FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Akeson, RL
Chen, X
Ciardi, D
Crane, M
Good, J
Harbut, M
Jackson, E
Kane, SR
Laity, AC
Leifer, S
Lynn, M
McElroy, DL
Papin, M
Plavchan, P
Ramirez, SV
Rey, R
von Braun, K
Wittman, M
Abajian, M
Ali, B
Beichman, C
Beekley, A
Berriman, GB
Berukoff, S
Bryden, G
Chan, B
Groom, S
Lau, C
Payne, AN
Regelson, M
Saucedo, M
Schmitz, M
Stauffer, J
Wyatt, P
Zhang, A
AF Akeson, R. L.
Chen, X.
Ciardi, D.
Crane, M.
Good, J.
Harbut, M.
Jackson, E.
Kane, S. R.
Laity, A. C.
Leifer, S.
Lynn, M.
McElroy, D. L.
Papin, M.
Plavchan, P.
Ramirez, S. V.
Rey, R.
von Braun, K.
Wittman, M.
Abajian, M.
Ali, B.
Beichman, C.
Beekley, A.
Berriman, G. B.
Berukoff, S.
Bryden, G.
Chan, B.
Groom, S.
Lau, C.
Payne, A. N.
Regelson, M.
Saucedo, M.
Schmitz, M.
Stauffer, J.
Wyatt, P.
Zhang, A.
TI The NASA Exoplanet Archive: Data and Tools for Exoplanet Research
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE Astronomical Instrumentation
ID PLANET-DETECTION; VARIABLE-STARS; TIME-SERIES; CANDIDATES; VARIABILITY;
FIELD; SEARCH; PHOTOMETRY; PROJECT; 2MASS
AB We describe the contents and functionality of the NASA Exoplanet Archive, a database and toolset funded by NASA to support astronomers in the exoplanet community. The current content of the database includes interactive tables containing properties of all published exoplanets, Kepler planet candidates, threshold-crossing events, data validation reports and target stellar parameters, light curves from the Kepler and CoRoT missions and from several ground-based surveys, and spectra and radial velocity measurements from the literature. Tools provided to work with these data include a transit ephemeris predictor, both for single planets and for observing locations, light curve viewing and normalization utilities, and a periodogram and phased light curve service. The archive can be accessed at http://exoplanetarchive.ipac.caltech.edu.
C1 [Akeson, R. L.; Chen, X.; Ciardi, D.; Crane, M.; Good, J.; Kane, S. R.; Laity, A. C.; Leifer, S.; McElroy, D. L.; Papin, M.; Plavchan, P.; Ramirez, S. V.; von Braun, K.; Abajian, M.; Beichman, C.; Beekley, A.; Berriman, G. B.; Berukoff, S.; Chan, B.; Lau, C.; Payne, A. N.; Regelson, M.; Saucedo, M.; Wyatt, P.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Harbut, M.; Jackson, E.; Lynn, M.; Rey, R.; Wittman, M.; Ali, B.; Groom, S.; Schmitz, M.; Stauffer, J.; Zhang, A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91108 USA.
RP Akeson, RL (reprint author), CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
OI Ciardi, David/0000-0002-5741-3047
FU NASA's Exoplanet Exploration Program; National Aeronautics and Space
Administration; National Science Foundation; NASA [NAS5-26555]; NASA
Office of Space Science [NNX09AF08G]
FX The Exoplanet Archive is funded through NASA's Exoplanet Exploration
Program, administered by the Jet Propulsion Laboratory, California
Institute of Technology. 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 research has made use of the NASA's IPAC Infrared
Science Archive, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. The Kepler light curves 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. This research has made use of the SIMBAD
database, operated at CDS, Strasbourg, France.
NR 35
TC 75
Z9 75
U1 3
U2 23
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 AUG
PY 2013
VL 125
IS 930
BP 989
EP 999
DI 10.1086/672273
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205FR
UT WOS:000323428900008
ER
PT J
AU Baumgartner, WH
Tueller, J
Markwardt, CB
Skinner, GK
Barthelmy, S
Mushotzky, RF
Evans, PA
Gehrels, N
AF Baumgartner, W. H.
Tueller, J.
Markwardt, C. B.
Skinner, G. K.
Barthelmy, S.
Mushotzky, R. F.
Evans, P. A.
Gehrels, N.
TI THE 70 MONTH SWIFT-BAT ALL-SKY HARD X-RAY SURVEY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; surveys; X-rays: general
ID ACTIVE GALACTIC NUCLEI; INTEGRAL SOURCES; OPTICAL SPECTROSCOPY; CATALOG;
IDENTIFICATION; COUNTERPART; BINARIES; PULSAR; MISSION; PLANE
AB We present the catalog of sources detected in 70 months of observations with the Burst Alert Telescope (BAT) hard X-ray detector on the Swift gamma-ray burst observatory. The Swift-BAT 70 month survey has detected 1171 hard X-ray sources (more than twice as many sources as the previous 22 month survey) in the 14-195 keV band down to a significance level of 4.8 sigma, associated with 1210 counterparts. The 70 month Swift-BAT survey is the most sensitive and uniform hard X-ray all-sky survey and reaches a flux level of 1.03 x 10(-11) erg s(-1) cm(-2) over 50% of the sky and 1.34 x 10(-11) erg s(-1) cm(-2) over 90% of the sky. The majority of new sources in the 70 month survey continue to be active galactic nuclei, with over 700 in the catalog. As part of this new edition of the Swift-BAT catalog, we also make available eight-channel spectra and monthly sampled light curves for each object detected in the survey in the online journal and at the Swift-BAT 70 month Web site.
C1 [Baumgartner, W. H.; Tueller, J.; Markwardt, C. B.; Skinner, G. K.; Barthelmy, S.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Baumgartner, W. H.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Baumgartner, W. H.; Skinner, G. K.] CRESST, Columbia, MD 21044 USA.
[Skinner, G. K.; Mushotzky, R. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Skinner, G. K.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Evans, P. A.] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England.
RP Baumgartner, WH (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
EM whbaumga@alum.mit.edu
FU UKSA
FX We acknowledge the help of Mike Koss in obtaining optical spectra and
redshifts for many sources in the table. This work has made heavy use of
the NED, SIMBAD, and HEASRAC online databases as well as the private
Leicester database of automatic analyses of XRT data for the follow-up
observations of the BAT survey sources. And of course, this work could
not have been completed without the diligent effort of all the members
of the Swift team. Additionally, P.A.E. acknowledges support from UKSA.
NR 38
TC 169
Z9 169
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2013
VL 207
IS 2
AR UNSP 19
DI 10.1088/0067-0049/207/2/19
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 195NO
UT WOS:000322710000001
ER
PT J
AU Bock, J
Sullivan, I
Arai, T
Battle, J
Cooray, A
Hristov, V
Keating, B
Kim, MG
Lam, AC
Lee, DH
Levenson, LR
Mason, P
Matsumoto, T
Matsuura, S
Mitchell-Wynne, K
Nam, UW
Renbarger, T
Smidt, J
Suzuki, K
Tsumura, K
Wada, T
Zemcov, M
AF Bock, J.
Sullivan, I.
Arai, T.
Battle, J.
Cooray, A.
Hristov, V.
Keating, B.
Kim, M. G.
Lam, A. C.
Lee, D. H.
Levenson, L. R.
Mason, P.
Matsumoto, T.
Matsuura, S.
Mitchell-Wynne, K.
Nam, U. W.
Renbarger, T.
Smidt, J.
Suzuki, K.
Tsumura, K.
Wada, T.
Zemcov, M.
TI THE COSMIC INFRARED BACKGROUND EXPERIMENT (CIBER): THE WIDE-FIELD
IMAGERS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE dark ages, reionization, first stars; diffuse radiation; infrared:
diffuse background; instrumentation: miscellaneous; space vehicles:
instruments
ID NORTH ECLIPTIC POLE; MICROWAVE-ANISOTROPY-PROBE; DEEP GALAXY COUNTS;
DIRBE MINUS 2MASS; 3.5 MU-M; LUMINOSITY FUNCTIONS; EXPERIMENT SEARCH;
ZODIACAL LIGHT; POPULATION-III; SOURCE CATALOG
AB We have developed and characterized an imaging instrument to measure the spatial properties of the diffuse near-infrared extragalactic background light (EBL) in a search for fluctuations from z > 6 galaxies during the epoch of reionization. The instrument is part of the Cosmic Infrared Background Experiment (CIBER), designed to observe the EBL above Earth's atmosphere during a suborbital sounding rocket flight. The imaging instrument incorporates a 2 degrees x 2 degrees field of view to measure fluctuations over the predicted peak of the spatial power spectrum at 10 arcmin, and 7 '' x 7 '' pixels, to remove lower redshift galaxies to a depth sufficient to reduce the low-redshift galaxy clustering foreground below instrumental sensitivity. The imaging instrument employs two cameras with Delta lambda/lambda similar to 0.5 bandpasses centered at 1.1 mu m and 1.6 mu m to spectrally discriminate reionization extragalactic background fluctuations from local foreground fluctuations. CIBER operates at wavelengths where the electromagnetic spectrum of the reionization extragalactic background is thought to peak, and complements fluctuation measurements by AKARI and Spitzer at longer wavelengths. We have characterized the instrument in the laboratory, including measurements of the sensitivity, flat-field response, stray light performance, and noise properties. Several modifications were made to the instrument following a first flight in 2009 February. The instrument performed to specifications in three subsequent flights, and the scientific data are now being analyzed.
C1 [Bock, J.; Battle, J.; Zemcov, M.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, J.; Hristov, V.; Lam, A. C.; Levenson, L. R.; Mason, P.; Zemcov, M.] CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA.
[Sullivan, I.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Arai, T.; Matsuura, S.; Tsumura, K.; Wada, T.] Japan Aerosp Explorat Agcy JAXA, Dept Space Astron & Astrophys, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Arai, T.] Univ Tokyo, Dept Phys, Grad Sch Sci, Tokyo 1130033, Japan.
[Cooray, A.; Mitchell-Wynne, K.; Smidt, J.] Univ Calif Irvine, Ctr Cosmol, Irvine, CA 92697 USA.
[Keating, B.; Renbarger, T.] Univ Calif San Diego, Dept Phys, San Diego, CA 92093 USA.
[Kim, M. G.; Matsumoto, T.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea.
[Lee, D. H.; Matsumoto, T.] Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Nam, U. W.] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea.
[Suzuki, K.] Nagoya Univ, Ctr Tech, Instrument Dev Grp, Nagoya, Aichi 4648602, Japan.
RP Bock, J (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RI Matsuura, Shuji/B-5658-2016
OI Matsuura, Shuji/0000-0002-5698-9634
FU NASA APRA [NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, NNX10AE12G];
Jet Propulsion Laboratory's Director's Research and Development Fund;
National Aeronautics and Space Administration; National Science
Foundation; NSF CAREER award; JSPS Research Fellowship for Young
Scientists; UCSD Hellman Faculty Fellowship; NASA Postdoctoral Program
Fellowship
FX This work was supported by NASA APRA research grants NNX07AI54G,
NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was
provided by an award to J.B. from the Jet Propulsion Laboratory's
Director's Research and Development Fund. Japanese participation in
CIBER was supported by KAKENHI (20.34, 18204018, 19540250, 21340047, and
21111004) from the Japan Society for the Promotion of Science (JSPS) and
the Ministry of Education, Culture, Sports, Science, and Technology
(MEXT). Korean participation in CIBER was supported by the Pioneer
Project from the Korea Astronomy and Space Science Institute (KASI).;
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. This work made use
of images and/or data products provided by the NOAO Deep Wide-Field
Survey (NDWFS), which is supported by the National Optical Astronomy
Observatory, operated by AURA, Inc., under a cooperative agreement with
the National Science Foundation.; We would like to acknowledge the
dedicated efforts of the sounding rocket staff at the NASA Wallops
Flight Facility and the White Sands Missile Range. We also acknowledge
the work of the Genesia Corporation for technical support of the CIBER
optics. Our thanks to Y. Gong for sharing the REBL curves shown in
Figure 1. A. C. acknowledges support from an NSF CAREER award, B. K.
acknowledges support from a UCSD Hellman Faculty Fellowship, K. T.
acknowledges support from the JSPS Research Fellowship for Young
Scientists, and M.Z. acknowledges support from a NASA Postdoctoral
Program Fellowship.
NR 69
TC 10
Z9 10
U1 0
U2 6
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 AUG
PY 2013
VL 207
IS 2
AR UNSP 32
DI 10.1088/0067-0049/207/2/32
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 195NO
UT WOS:000322710000014
ER
PT J
AU Christiansen, JL
Clarke, BD
Burke, CJ
Jenkins, JM
Barclay, TS
Ford, EB
Haas, MR
Sabale, A
Seader, S
Smith, JC
Tenenbaum, P
Twicken, JD
Uddin, AK
Thompson, SE
AF Christiansen, Jessie L.
Clarke, Bruce D.
Burke, Christopher J.
Jenkins, Jon M.
Barclay, Thomas S.
Ford, Eric B.
Haas, Michael R.
Sabale, Anima
Seader, Shawn
Smith, Jeffrey Claiborne
Tenenbaum, Peter
Twicken, Joseph D.
Uddin, Akm Kamal
Thompson, Susan E.
TI MEASURING TRANSIT SIGNAL RECOVERY IN THE KEPLER PIPELINE. I. INDIVIDUAL
EVENTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE methods: data analysis; planets and satellites: detection
ID ADDITIONAL PLANETS; ERROR-CORRECTION; MISSION DATA; CANDIDATES; SEARCH;
QUARTERS; SCIENCE; SYSTEMS; STARS
AB The Kepler mission was designed to measure the frequency of Earth-size planets in the habitable zone of Sun-like stars. A crucial component for recovering the underlying planet population from a sample of detected planets is understanding the completeness of that sample-the fraction of the planets that could have been discovered in a given data set that actually were detected. Here, we outline the information required to determine the sample completeness, and describe an experiment to address a specific aspect of that question, i.e., the issue of transit signal recovery. We investigate the extent to which the Kepler pipeline preserves individual transit signals by injecting simulated transits into the pixel-level data, processing the modified pixels through the pipeline, and comparing the measured transit signal-to-noise ratio (S/N) to that expected without perturbation by the pipeline. We inject simulated transit signals across the full focal plane for a set of observations for a duration of 89 days. On average, we find that the S/N of the injected signal is recovered at MS = 0.9973(+/-0.0012) x BS-0.0151(+/-0.0049), where MS is the measured S/N and BS is the baseline, or expected, S/N. The 1 sigma width of the distribution around this correlation is +/-2.64%. This indicates an extremely high fidelity in reproducing the expected detection statistics for single transit events, and provides teams performing their own periodic transit searches the confidence that there is no systematic reduction in transit signal strength introduced by the pipeline. We discuss the pipeline processes that cause the measured S/N to deviate significantly from the baseline S/N for a small fraction of targets; these are primarily the handling of data adjacent to spacecraft re-pointings and the removal of harmonics prior to the measurement of the S/N. Finally, we outline the further work required to characterize the completeness of the Kepler pipeline.
C1 [Christiansen, Jessie L.; Clarke, Bruce D.; Burke, Christopher J.; Jenkins, Jon M.; Haas, Michael R.; Seader, Shawn; Smith, Jeffrey Claiborne; Tenenbaum, Peter; Twicken, Joseph D.; Thompson, Susan E.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas S.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA.
[Sabale, Anima; Uddin, Akm Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Christiansen, JL (reprint author), NASA, SETI Inst, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA.
EM jessie.l.christiansen@nasa.gov
OI /0000-0001-6545-639X
FU NASA's Science Mission Directorate
FX Funding for the Kepler Discovery Mission is provided by NASA's Science
Mission Directorate.
NR 33
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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 AUG
PY 2013
VL 207
IS 2
AR UNSP 35
DI 10.1088/0067-0049/207/2/35
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 195NO
UT WOS:000322710000017
ER
PT J
AU Guo, YC
Ferguson, HC
Giavalisco, M
Barro, G
Willner, SP
Ashby, MLN
Dahlen, T
Donley, JL
Faber, SM
Fontana, A
Galametz, A
Grazian, A
Huang, KH
Kocevski, DD
Koekemoer, AM
Koo, DC
McGrath, EJ
Peth, M
Salvato, M
Wuyts, S
Castellano, M
Cooray, AR
Dickinson, ME
Dunlop, JS
Fazio, GG
Gardner, JP
Gawiser, E
Grogin, NA
Hathi, NP
Hsu, LT
Lee, KS
Lucas, RA
Mobasher, B
Nandra, K
Newman, JA
van der Wel, A
AF Guo, Yicheng
Ferguson, Henry C.
Giavalisco, Mauro
Barro, Guillermo
Willner, S. P.
Ashby, Matthew L. N.
Dahlen, Tomas
Donley, Jennifer L.
Faber, Sandra M.
Fontana, Adriano
Galametz, Audrey
Grazian, Andrea
Huang, Kuang-Han
Kocevski, Dale D.
Koekemoer, Anton M.
Koo, David C.
McGrath, Elizabeth J.
Peth, Michael
Salvato, Mara
Wuyts, Stijn
Castellano, Marco
Cooray, Asantha R.
Dickinson, Mark E.
Dunlop, James S.
Fazio, G. G.
Gardner, Jonathan P.
Gawiser, Eric
Grogin, Norman A.
Hathi, Nimish P.
Hsu, Li-Ting
Lee, Kyoung-Soo
Lucas, Ray A.
Mobasher, Bahram
Nandra, Kirpal
Newman, Jeffery A.
van der Wel, Arjen
TI CANDELS MULTI-WAVELENGTH CATALOGS: SOURCE DETECTION AND PHOTOMETRY IN
THE GOODS-SOUTH FIELD
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; galaxies: high-redshift; galaxies: photometry; methods: data
analysis; techniques: image processing
ID ORIGINS DEEP SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION
HISTORY; SIMILAR-TO 2; GMASS ULTRADEEP SPECTROSCOPY; EXTRAGALACTIC
LEGACY SURVEY; REST-FRAME ULTRAVIOLET; UV LUMINOSITY FUNCTION;
HIGH-REDSHIFT GALAXIES; SPACE-TELESCOPE
AB We present a UV to mid-infrared multi-wavelength catalog in the CANDELS/GOODS-S field, combining the newly obtained CANDELS HST/WFC3 F105W, F125W, and F160W data with existing public data. The catalog is based on source detection in the WFC3 F160W band. The F160W mosaic includes the data from CANDELS deep and wide observations as well as previous ERS and HUDF09 programs. The mosaic reaches a 5 sigma limiting depth (within an aperture of radius 0 ''.17) of 27.4, 28.2, and 29.7 AB for CANDELS wide, deep, and HUDF regions, respectively. The catalog contains 34,930 sources with the representative 50% completeness reaching 25.9, 26.6, and 28.1 AB in the F160W band for the three regions. In addition to WFC3 bands, the catalog also includes data from UV (U band from both CTIO/MOSAIC and VLT/VIMOS), optical (HST/ACS F435W, F606W, F775W, F814W, and F850LP), and infrared (HST/WFC3 F098M, VLT/ISAAC K s, VLT/HAWK-I K s, and Spitzer/IRAC 3.6, 4.5, 5.8, 8.0 mu m) observations. The catalog is validated via stellar colors, comparison with other published catalogs, zero-point offsets determined from the best-fit templates of the spectral energy distribution of spectroscopically observed objects, and the accuracy of photometric redshifts. The catalog is able to detect unreddened star-forming (passive) galaxies with stellar mass of 10(10) M-circle dot at a 50% completeness level to z similar to 3.4 (2.8), 4.6 (3.2), and 7.0 (4.2) in the three regions. As an example of application, the catalog is used to select both star-forming and passive galaxies at z similar to 2-4 via the Balmer break. It is also used to study the color-magnitude diagram of galaxies at 0 < z < 4.
C1 [Guo, Yicheng; Barro, Guillermo; Faber, Sandra M.; Koo, David C.] Univ Calif Santa Cruz, Lick Observ, Dept Astron & Astrophys, UCO, Santa Cruz, CA 95064 USA.
[Guo, Yicheng; Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Ferguson, Henry C.; Dahlen, Tomas; Huang, Kuang-Han; Koekemoer, Anton M.; Lucas, Ray A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Willner, S. P.; Ashby, Matthew L. N.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Donley, Jennifer L.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Fontana, Adriano; Galametz, Audrey; Grazian, Andrea; Castellano, Marco] INAF, Osservatorio Astron, I-00040 Monte Porzio Catone, Italy.
[Huang, Kuang-Han; Peth, Michael] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Kocevski, Dale D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA.
[McGrath, Elizabeth J.] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA.
[Salvato, Mara; Wuyts, Stijn; Hsu, Li-Ting; Nandra, Kirpal] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Salvato, Mara] Excellence Cluster, D-85748 Garching, Germany.
[Cooray, Asantha R.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA.
[Dickinson, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Dunlop, James S.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Gardner, Jonathan P.] NASAs Goddard Space Flight Ctr, Astrophys Sci Div, Observat Cosmol Lab, Greenbelt, MD USA.
[Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, New Brunswick, NJ 08903 USA.
[Hathi, Nimish P.] Carnegie Observ, Pasadena, CA USA.
[Lee, Kyoung-Soo] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Newman, Jeffery A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Guo, YC (reprint author), Univ Calif Santa Cruz, Lick Observ, Dept Astron & Astrophys, UCO, Santa Cruz, CA 95064 USA.
EM ycguo@ucolick.org
RI Hathi, Nimish/J-7092-2014;
OI Hathi, Nimish/0000-0001-6145-5090; Castellano,
Marco/0000-0001-9875-8263; Koekemoer, Anton/0000-0002-6610-2048;
fontana, adriano/0000-0003-3820-2823
FU NASA through a grant from the Space Telescope Science Institute
[HST-GO-12060]; NASA [NAS5-26555]; NASA HST [GO-12060.10-A]; NSF
[AST-0808133]; European Research Council; Royal Society
FX We thank the anonymous referee for constructive comments that improve
this article. Support for program number HST-GO-12060 was provided by
NASA through a grant from the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in
Astronomy, Incorporated, under NASA contract NAS5-26555. Y.G. and the
authors from UCSC acknowledge support from NASA HST grant GO-12060.10-A
and NSF grant AST-0808133. J.S.D. acknowledges the support of the
European Research Council via the award of an Advanced Grant and the
support of the Royal Society via a Wolfson Research Merit Award. 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.
NR 84
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U1 0
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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 AUG
PY 2013
VL 207
IS 2
AR UNSP 24
DI 10.1088/0067-0049/207/2/24
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 195NO
UT WOS:000322710000006
ER
PT J
AU Hurley, K
Pal'shin, VD
Aptekar, RL
Golenetskii, SV
Frederiks, DD
Mazets, EP
Svinkin, DS
Briggs, MS
Connaughton, V
Meegan, C
Goldsten, J
Boynton, W
Fellows, C
Harshman, K
Mitrofanov, IG
Golovin, DV
Kozyrev, AS
Litvak, ML
Sanin, AB
Rau, A
von Kienlin, A
Zhang, X
Yamaoka, K
Fukazawa, Y
Hanabata, Y
Ohno, M
Takahashi, T
Tashiro, M
Terada, Y
Murakami, T
Makishima, K
Barthelmy, S
Cline, T
Gehrels, N
Cummings, J
Krimm, HA
Smith, DM
Del Monte, E
Feroci, M
Marisaldi, M
AF Hurley, K.
Pal'shin, V. D.
Aptekar, R. L.
Golenetskii, S. V.
Frederiks, D. D.
Mazets, E. P.
Svinkin, D. S.
Briggs, M. S.
Connaughton, V.
Meegan, C.
Goldsten, J.
Boynton, W.
Fellows, C.
Harshman, K.
Mitrofanov, I. G.
Golovin, D. V.
Kozyrev, A. S.
Litvak, M. L.
Sanin, A. B.
Rau, A.
von Kienlin, A.
Zhang, X.
Yamaoka, K.
Fukazawa, Y.
Hanabata, Y.
Ohno, M.
Takahashi, T.
Tashiro, M.
Terada, Y.
Murakami, T.
Makishima, K.
Barthelmy, S.
Cline, T.
Gehrels, N.
Cummings, J.
Krimm, H. A.
Smith, D. M.
Del Monte, E.
Feroci, M.
Marisaldi, M.
TI THE INTERPLANETARY NETWORK SUPPLEMENT TO THE FERMI GBM CATALOG OF COSMIC
GAMMA-RAY BURSTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; gamma-ray burst: general; techniques: miscellaneous
ID ARRIVAL-TIME LOCALIZATIONS; PIONEER-VENUS-ORBITER; 1ST 2 YEARS; ULYSSES
SUPPLEMENT; MISSION; MONITOR
AB We present Interplanetary Network (IPN) data for the gamma-ray bursts in the first Fermi Gamma-Ray Burst Monitor (GBM) catalog. Of the 491 bursts in that catalog, covering 2008 July 12 to 2010 July 11, 427 were observed by at least one other instrument in the nine-spacecraft IPN. Of the 427, the localizations of 149 could be improved by arrival time analysis (or "triangulation"). For any given burst observed by the GBM and one other distant spacecraft, triangulation gives an annulus of possible arrival directions whose half-width varies between about 0.'4 and 32 degrees, depending on the intensity, time history, and arrival direction of the burst, as well as the distance between the spacecraft. We find that the IPN localizations intersect the 1 sigma GBM error circles in only 52% of the cases, if no systematic uncertainty is assumed for the latter. If a 6 degrees systematic uncertainty is assumed and added in quadrature, the two localization samples agree about 87% of the time, as would be expected. If we then multiply the resulting error radii by a factor of three, the two samples agree in slightly over 98% of the cases, providing a good estimate of the GBM 3 sigma error radius. The IPN 3 sigma error boxes have areas between about 1 arcmin(2) and 110 deg(2), and are, on the average, a factor of 180 smaller than the corresponding GBM localizations. We identify two bursts in the IPN/GBM sample that did not appear in the GBM catalog. In one case, the GBM triggered on a terrestrial gamma flash, and in the other, its origin was given as "uncertain." We also discuss the sensitivity and calibration of the IPN.
C1 [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Pal'shin, V. D.; Aptekar, R. L.; Golenetskii, S. V.; Frederiks, D. D.; Mazets, E. P.; Svinkin, D. S.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
[Briggs, M. S.; Connaughton, V.] Univ Alabama, NSSTC, Huntsville, AL 35805 USA.
[Meegan, C.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA.
[Goldsten, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Boynton, W.; Fellows, C.; Harshman, K.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Mitrofanov, I. G.; Golovin, D. V.; Kozyrev, A. S.; Litvak, M. L.; Sanin, A. B.] Space Res Inst, Moscow 8432, Russia.
[Rau, A.; von Kienlin, A.; Zhang, X.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Yamaoka, K.] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Fukazawa, Y.; Hanabata, Y.; Ohno, M.] Hiroshima Univ, Dept Phys, Higashihiroshima, Hiroshima 7398526, Japan.
[Takahashi, T.] Inst Space & Astronaut Sci ISAS JAXA, Sagamihara, Kanagawa 2298510, Japan.
[Tashiro, M.; Terada, Y.] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan.
[Murakami, T.] Kanazawa Univ, Dept Phys, Kanazawa, Ishikawa 9201192, Japan.
[Makishima, K.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Barthelmy, S.; Cline, T.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cummings, J.] NASA, UMBC, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krimm, H. A.] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smith, D. M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Smith, D. M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Del Monte, E.; Feroci, M.] INAF IASF Roma, I-00133 Rome, Italy.
[Marisaldi, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Mazets, E. P.] Inst Phys & Chem Res RIKEN, Makishima Cosm Radiat Lab, Wako, Saitama 3510198, Japan.
[Cummings, J.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA.
RP Hurley, K (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM khurley@ssl.berkeley.edu
RI Svinkin, Dmitry/C-1934-2014; Frederiks, Dmitry/C-7612-2014; Pal'shin,
Valentin/F-3973-2014; Aptekar, Raphail/B-3456-2015; Golenetskii,
Sergey/B-3818-2015; Terada, Yukikatsu/A-5879-2013;
OI Terada, Yukikatsu/0000-0002-2359-1857; Frederiks,
Dmitry/0000-0002-1153-6340; Feroci, Marco/0000-0002-7617-3421;
Marisaldi, Martino/0000-0002-4000-3789
FU NASA [NNX09AU03G, NNX08AC90G, NNX08AX95G, NNX08AN23G, NNX09AO97G,
NNX08AZ85G, NNX09AV61G, NNX07AR71G]; JPL [1282043, Y503559]; Russian
Space Agency contract; RFBR [12-02-00032-a]
FX Support for the IPN was provided by NASA grants NNX09AU03G (Fermi),
NNX08AC90G and NNX08AX95G (INTEGRAL), NNX08AN23G and NNX09AO97G (Swift),
NNX08AZ85G and NNX09AV61G (Suzaku), NNX07AR71G (MESSENGER), and JPL
Contracts 1282043 and Y503559 (Odyssey). The Konus-Wind experiment is
supported by a Russian Space Agency contract and RFBR grant
12-02-00032-a. This research has made use of data and/or software
provided by the High Energy Astrophysics Science Archive Research Center
(HEASARC), which is a service of the Astrophysics Science Division at
NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian
Astrophysical Observatory.
NR 30
TC 9
Z9 9
U1 0
U2 10
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 AUG
PY 2013
VL 207
IS 2
AR UNSP 39
DI 10.1088/0067-0049/207/2/39
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 195NO
UT WOS:000322710000021
ER
PT J
AU Korngut, PM
Renbarger, T
Arai, T
Battle, J
Bock, J
Brown, SW
Cooray, A
Hristov, V
Keating, B
Kim, MG
Lanz, A
Lee, DH
Levenson, LR
Lykke, KR
Mason, P
Matsumoto, T
Matsuura, S
Nam, UW
Shultz, B
Smith, AW
Sullivan, I
Tsumura, K
Wada, T
Zemcov, M
AF Korngut, P. M.
Renbarger, T.
Arai, T.
Battle, J.
Bock, J.
Brown, S. W.
Cooray, A.
Hristov, V.
Keating, B.
Kim, M. G.
Lanz, A.
Lee, D. H.
Levenson, L. R.
Lykke, K. R.
Mason, P.
Matsumoto, T.
Matsuura, S.
Nam, U. W.
Shultz, B.
Smith, A. W.
Sullivan, I.
Tsumura, K.
Wada, T.
Zemcov, M.
TI THE COSMIC INFRARED BACKGROUND EXPERIMENT (CIBER): THE NARROW-BAND
SPECTROMETER
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE infrared: diffuse background; instrumentation: spectrographs; methods:
laboratory; space vehicles: instruments; techniques: spectroscopic;
zodiacal dust
ID DIRBE MINUS 2MASS; 3.5 MU-M; ZODIACAL LIGHT; INTERPLANETARY DUST;
EXPERIMENT SEARCH; DETECTIONS; SPECTRUM; DENSITY; SPACE
AB We have developed a near-infrared spectrometer designed to measure the absolute intensity of the solar 854.2 nm Ca II Fraunhofer line, scattered by interplanetary dust, in the zodiacal light (ZL) spectrum. Based on the known equivalent line width in the solar spectrum, this measurement can derive the zodiacal brightness, testing models of the ZL based on morphology that are used to determine the extragalactic background light in absolute photometry measurements. The spectrometer is based on a simple high-resolution tipped filter placed in front of a compact camera with wide-field refractive optics to provide the large optical throughput and high sensitivity required for rocket-borne observations. We discuss the instrument requirements for an accurate measurement of the absolute ZL brightness, the measured laboratory characterization, and the instrument performance in flight.
C1 [Korngut, P. M.; Bock, J.; Zemcov, M.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Korngut, P. M.; Battle, J.; Bock, J.; Hristov, V.; Lanz, A.; Levenson, L. R.; Mason, P.; Zemcov, M.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Renbarger, T.; Keating, B.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Arai, T.; Matsumoto, T.; Matsuura, S.; Tsumura, K.; Wada, T.] Japan Aerosp Explorat Agcy JAXA, Dept Space Astron & Astrophys, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Arai, T.] Univ Tokyo, Grad Sch Sci, Dept Phys, Tokyo 1130033, Japan.
[Brown, S. W.; Lykke, K. R.; Smith, A. W.] NIST, Sensor Sci Div, Gaithersburg, MD 20899 USA.
[Cooray, A.] Univ Calif Irvine, Ctr Cosmol, Irvine, CA 92697 USA.
[Kim, M. G.; Matsumoto, T.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea.
[Lee, D. H.; Nam, U. W.] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea.
[Matsumoto, T.] Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Shultz, B.] Materion Barr Precis Opt & Thin Film Coatings, Westford, MA 01886 USA.
[Sullivan, I.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
RP Korngut, PM (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
EM pkorngut@caltech.edu
RI Matsuura, Shuji/B-5658-2016
OI Matsuura, Shuji/0000-0002-5698-9634
FU NASA APRA [NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, NNX10AE12G];
Jet Propulsion Laboratory's Director's Research and Development Fund;
NSF CAREER award; UCSD Hellman Faculty Fellowship; JSPS Research
Fellowship for Young Scientists; NASA Postdoctoral Fellowships
FX This work was supported by NASA APRA research Grants NNX07AI54G,
NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was
provided by an award to J.B. from the Jet Propulsion Laboratory's
Director's Research and Development Fund. Japanese participation in
CIBER was supported by KAKENHI (20.34, 18204018, 19540250, 21340047, and
21111004) from the Japan Society for the Promotion of Science (JSPS) and
the Ministry of Education, Culture, Sports, Science, and Technology
(MEXT). Korean participation in CIBER was supported by the Pioneer
Project from the Korea Astronomy and Space science Institute (KASI).; We
acknowledge the dedicated efforts of the sounding rocket staff at the
NASA Wallops Flight Facility and the White Sands Missile Range. We also
acknowledge the work of the Genesia Corporation for technical support of
the CIBER optics. A. C. acknowledges support from an NSF CAREER award,
B. K. acknowledges support from a UCSD Hellman Faculty Fellowship, K. T.
acknowledges support from the JSPS Research Fellowship for Young
Scientists, and M.Z. and P. M. K acknowledge support from NASA
Postdoctoral Fellowships.
NR 37
TC 10
Z9 10
U1 0
U2 5
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 AUG
PY 2013
VL 207
IS 2
AR UNSP 34
DI 10.1088/0067-0049/207/2/34
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 195NO
UT WOS:000322710000016
ER
PT J
AU Pal'shin, VD
Hurley, K
Svinkin, DS
Aptekar, RL
Golenetskii, SV
Frederiks, DD
Mazets, EP
Oleynik, PP
Ulanov, MV
Cline, T
Mitrofanov, IG
Golovin, DV
Kozyrev, AS
Litvak, ML
Sanin, AB
Boynton, W
Fellows, C
Harshman, K
Trombka, J
McClanahan, T
Starr, R
Goldsten, J
Gold, R
Rau, A
von Kienlin, A
Savchenko, V
Smith, DM
Hajdas, W
Barthelmy, SD
Cummings, J
Gehrels, N
Krimm, H
Palmer, D
Yamaoka, K
Ohno, M
Fukazawa, Y
Hanabata, Y
Takahashi, T
Tashiro, M
Terada, Y
Murakami, T
Makishima, K
Briggs, MS
Kippen, RM
Kouveliotou, C
Meegan, C
Fishman, G
Connaughton, V
Boer, M
Guidorzi, C
Frontera, F
Montanari, E
Rossi, F
Feroci, M
Amati, L
Nicastro, L
Orlandini, M
DelMonte, E
Costa, E
Donnarumma, I
Evangelista, Y
Lapshov, I
Lazzarotto, F
Pacciani, L
Rapisarda, M
Soffitta, P
Di Cocco, G
Fuschino, F
Galli, M
Labanti, C
Marisaldi, M
Atteia, JL
Vanderspek, R
Ricker, G
AF Pal'shin, V. D.
Hurley, K.
Svinkin, D. S.
Aptekar, R. L.
Golenetskii, S. V.
Frederiks, D. D.
Mazets, E. P.
Oleynik, P. P.
Ulanov, M. V.
Cline, T.
Mitrofanov, I. G.
Golovin, D. V.
Kozyrev, A. S.
Litvak, M. L.
Sanin, A. B.
Boynton, W.
Fellows, C.
Harshman, K.
Trombka, J.
McClanahan, T.
Starr, R.
Goldsten, J.
Gold, R.
Rau, A.
von Kienlin, A.
Savchenko, V.
Smith, D. M.
Hajdas, W.
Barthelmy, S. D.
Cummings, J.
Gehrels, N.
Krimm, H.
Palmer, D.
Yamaoka, K.
Ohno, M.
Fukazawa, Y.
Hanabata, Y.
Takahashi, T.
Tashiro, M.
Terada, Y.
Murakami, T.
Makishima, K.
Briggs, M. S.
Kippen, R. M.
Kouveliotou, C.
Meegan, C.
Fishman, G.
Connaughton, V.
Boer, M.
Guidorzi, C.
Frontera, F.
Montanari, E.
Rossi, F.
Feroci, M.
Amati, L.
Nicastro, L.
Orlandini, M.
DelMonte, E.
Costa, E.
Donnarumma, I.
Evangelista, Y.
Lapshov, I.
Lazzarotto, F.
Pacciani, L.
Rapisarda, M.
Soffitta, P.
Di Cocco, G.
Fuschino, F.
Galli, M.
Labanti, C.
Marisaldi, M.
Atteia, J. -L.
Vanderspek, R.
Ricker, G.
TI INTERPLANETARY NETWORK LOCALIZATIONS OF KONUS SHORT GAMMA-RAY BURSTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; gamma-ray burst: general; techniques: miscellaneous
ID ARRIVAL-TIME LOCALIZATIONS; PIONEER-VENUS-ORBITER; ULYSSES SUPPLEMENT;
GIANT FLARE; LIGO OBSERVATIONS; GRB 051103; CATALOG; MISSION; BATSE;
SPECTROMETER
AB Between the launch of the Global Geospace Science Wind spacecraft in 1994 November and the end of 2010, the Konus-Wind experiment detected 296 short-duration gamma-ray bursts (including 23 bursts which can be classified as short bursts with extended emission). During this period, the Interplanetary Network (IPN) consisted of up to 11 spacecraft, and using triangulation, the localizations of 271 bursts were obtained. We present the most comprehensive IPN localization data on these events. The short burst detection rate, similar to 18 yr(-1), exceeds that of many individual experiments.
C1 [Pal'shin, V. D.; Svinkin, D. S.; Aptekar, R. L.; Golenetskii, S. V.; Frederiks, D. D.; Mazets, E. P.; Oleynik, P. P.; Ulanov, M. V.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
[Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Cline, T.; Trombka, J.; McClanahan, T.; Starr, R.; Barthelmy, S. D.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mitrofanov, I. G.; Golovin, D. V.; Kozyrev, A. S.; Litvak, M. L.; Sanin, A. B.] Space Res Inst, Moscow 117997, Russia.
[Boynton, W.; Fellows, C.; Harshman, K.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Goldsten, J.; Gold, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Rau, A.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Savchenko, V.] Univ Paris Diderot, Observ Paris, Francois Arago Ctr, APC,CNRS,CEA,Irfu,IN2P3, F-75205 Paris 13, France.
[Smith, D. M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Smith, D. M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Hajdas, W.] Paul Scherrer Inst, CH-5232 Villigen, Switzerland.
[Cummings, J.; Krimm, H.] NASA, UMBC, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cummings, J.] UMBC Phys Dept, Baltimore, MD 21250 USA.
[Krimm, H.] Univ Space Res Assoc, Columbia, MD 20144 USA.
[Palmer, D.; Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Yamaoka, K.; Takahashi, T.] Inst Space & Astronaut Sci ISAS JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ohno, M.; Fukazawa, Y.; Hanabata, Y.] Hiroshima Univ, Dept Phys, Hiroshima 7398526, Japan.
[Tashiro, M.; Terada, Y.] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan.
[Murakami, T.] Kanazawa Univ, Dept Phys, Kanazawa, Ishikawa 9201192, Japan.
[Makishima, K.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Briggs, M. S.; Connaughton, V.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Briggs, M. S.; Connaughton, V.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Kouveliotou, C.; Fishman, G.] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Meegan, C.] Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Boer, M.] Observ Haute Provence CNRS, F-04870 St Michel lObservatoire, France.
[Guidorzi, C.; Frontera, F.; Montanari, E.; Rossi, F.] Univ Ferrara, Dept Phys, I-44100 Ferrara, Italy.
[Frontera, F.; Amati, L.; Nicastro, L.; Orlandini, M.; Di Cocco, G.; Fuschino, F.; Labanti, C.; Marisaldi, M.] INAF, Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy.
[Montanari, E.] Ist IS Calvi, I-41034 Finale Emilia, MO, Italy.
[Feroci, M.; DelMonte, E.; Costa, E.; Donnarumma, I.; Evangelista, Y.; Lapshov, I.; Lazzarotto, F.; Pacciani, L.; Rapisarda, M.; Soffitta, P.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
[Galli, M.] ENEA Bologna, I-40129 Bologna, Italy.
[Atteia, J. -L.] Univ Toulouse, F-31400 Toulouse, France.
[Atteia, J. -L.] UPS OMP, F-31400 Toulouse, France.
[Atteia, J. -L.] CNRS, F-31400 Toulouse, France.
[Atteia, J. -L.] IRAP, F-31400 Toulouse, France.
[Vanderspek, R.; Ricker, G.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Pal'shin, VD (reprint author), AF Ioffe Phys Tech Inst, Politekhnicheskaya 26, St Petersburg 194021, Russia.
EM val@mail.ioffe.ru
RI Nicastro, Luciano/F-5866-2015; Amati, Lorenzo/N-5586-2015; Oleynik,
Philipp/C-1104-2014; Svinkin, Dmitry/C-1934-2014; Frederiks,
Dmitry/C-7612-2014; Pal'shin, Valentin/F-3973-2014; Orlandini,
Mauro/H-3114-2014; Ulanov, Mikhail/B-3467-2015; Aptekar,
Raphail/B-3456-2015; Golenetskii, Sergey/B-3818-2015; Terada,
Yukikatsu/A-5879-2013
OI Costa, Enrico/0000-0003-4925-8523; Donnarumma,
Immacolata/0000-0002-4700-4549; Marisaldi, Martino/0000-0002-4000-3789;
Labanti, Claudio/0000-0002-5086-3619; galli,
marcello/0000-0002-9135-3228; Pacciani, Luigi/0000-0001-6897-5996;
Frederiks, Dmitry/0000-0002-1153-6340; Feroci,
Marco/0000-0002-7617-3421; Soffitta, Paolo/0000-0002-7781-4104;
Fuschino, Fabio/0000-0003-2139-3299; Lazzarotto,
Francesco/0000-0003-4871-4072; Nicastro, Luciano/0000-0001-8534-6788;
Amati, Lorenzo/0000-0001-5355-7388; Orlandini,
Mauro/0000-0003-0946-3151; Ulanov, Mikhail/0000-0002-0076-5228; Terada,
Yukikatsu/0000-0002-2359-1857
FU Russian Space Agency; RFBR [12-02-00032a, 13-02-12017-ofi-m]; IPN under
NASA; IPN under JPL; IPN under MIT; JPL [958056, 1268385, 1282043];
[NNX07AH52G]; [NNX12AE41G]; [NAG5-12614]; [NNG04GM50G];
[NNG06GE69G]; [NNX07AQ22G]; [NNX08AC90G]; [NNX08AX95G];
[NNX09AR28G]; [NNG05GTF72G]; [NNG06GI89G]; [NNX07AJ65G];
[NNX08AN23G]; [NNX09AO97G]; [NNX10AI23G]; [NNX12AD68G]; [NAG5-3500];
[NAG5-9503]; [MIT-SC-R-293291]; [NAG5-11451]; [NNX06AI36G];
[NNX08AB84G]; [NNX08AZ85G]; [NNX09AV61G]; [NNX10AR12G];
[NNX09AU03G]; [NNX10AU34G]; [NNX11AP96G]; [NNX07AR71G]; [NAG5-7766];
[NAG5-9126]; [NAG5-10710]
FX The Konus-Wind experiment is supported by a Russian Space Agency
contract and RFBR grants 12-02-00032a and 13-02-12017-ofi-m. K. H. is
grateful for IPN support under the following NASA, JPL, and MIT grants
and contracts. JPL 958056 and 1268385 (Ulysses); NNX07AH52G and
NNX12AE41G (ADA and ADAP); NAG5-12614, NNG04GM50G, NNG06GE69G,
NNX07AQ22G, NNX08AC90G, NNX08AX95G and NNX09AR28G (INTEGRAL);
NNG05GTF72G, NNG06GI89G, NNX07AJ65G, NNX08AN23G, NNX09AO97G, NNX10AI23G,
and NNX12AD68G (Swift); NAG5-3500 and NAG5-9503 (NEAR); MIT-SC-R-293291
and NAG5-11451 (HETE-2); JPL 1282043 (Odyssey); NNX06AI36G, NNX08AB84G,
NNX08AZ85G, NNX09AV61G, NNX10AR12G (Suzaku); NNX09AU03G, NNX10AU34G, and
NNX11AP96G (Fermi); NNX07AR71G (MESSENGER); NAG5-7766, NAG5-9126, and
NAG5-10710 (BeppoSAX).
NR 65
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U1 1
U2 13
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 AUG
PY 2013
VL 207
IS 2
AR UNSP 38
DI 10.1088/0067-0049/207/2/38
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 195NO
UT WOS:000322710000020
ER
PT J
AU Tsumura, K
Arai, T
Battle, J
Bock, J
Brown, S
Cooray, A
Hristov, V
Keating, B
Kim, MG
Lee, DH
Levenson, LR
Lykke, K
Mason, P
Matsumoto, T
Matsuura, S
Murata, K
Nam, UW
Renbarger, T
Smith, A
Sullivan, I
Suzuki, K
Wada, T
Zemcov, M
AF Tsumura, K.
Arai, T.
Battle, J.
Bock, J.
Brown, S.
Cooray, A.
Hristov, V.
Keating, B.
Kim, M. G.
Lee, D. H.
Levenson, L. R.
Lykke, K.
Mason, P.
Matsumoto, T.
Matsuura, S.
Murata, K.
Nam, U. W.
Renbarger, T.
Smith, A.
Sullivan, I.
Suzuki, K.
Wada, T.
Zemcov, M.
TI THE COSMIC INFRARED BACKGROUND EXPERIMENT (CIBER): THE LOW RESOLUTION
SPECTROMETER
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic background radiation; infrared: diffuse background;
instrumentation: spectrographs; methods: laboratory; space vehicles:
instruments; techniques: spectroscopic
ID DEEP GALAXY COUNTS; DIRBE MINUS 2MASS; PRIMORDIAL STARS; 1ST DETECTIONS;
GAMMA-RAYS; LIGHT; BLAZARS; TELESCOPE; SPECTRUM; IMPRINT
AB Absolute spectrophotometric measurements of diffuse radiation at 1 mu m to 2 mu m are crucial to our understanding of the radiative content of the universe from nucleosynthesis since the epoch of reionization, the composition and structure of the zodiacal dust cloud in our solar system, and the diffuse galactic light arising from starlight scattered by interstellar dust. The Low Resolution Spectrometer (LRS) on the rocket-borne Cosmic Infrared Background Experiment is a lambda/Delta lambda similar to 15-30 absolute spectrophotometer designed to make precision measurements of the absolute near-infrared sky brightness between 0.75 mu m < lambda < 2.1 mu m. This paper presents the optical, mechanical, and electronic design of the LRS, as well as the ground testing, characterization, and calibration measurements undertaken before flight to verify its performance. The LRS is shown to work to specifications, achieving the necessary optical and sensitivity performance. We describe our understanding and control of sources of systematic error for absolute photometry of the near-infrared extragalactic background light.
C1 [Tsumura, K.; Arai, T.; Matsumoto, T.; Matsuura, S.; Murata, K.; Wada, T.] Japan Aerosp Explorat Agcy JAXA, Dept Space Astron & Astrophys, Inst Space & Astronout Sci, Sagamihara, Kanagawa 2525210, Japan.
[Arai, T.] Univ Tokyo, Grad Sch Sci, Dept Phys, Tokyo 1130033, Japan.
[Battle, J.; Bock, J.; Zemcov, M.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, J.; Hristov, V.; Levenson, L. R.; Mason, P.; Zemcov, M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Brown, S.; Lykke, K.; Smith, A.] NIST, Opt Technol Div, Gaithersburg, MD 20899 USA.
[Cooray, A.] Univ Calif Irvine, Ctr Cosmol, Irvine, CA 92697 USA.
[Keating, B.; Renbarger, T.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Kim, M. G.; Matsumoto, T.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea.
[Lee, D. H.; Nam, U. W.] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea.
[Murata, K.] Grad Univ Adv Studies, Sch Phys Sci, Dept Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Sullivan, I.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Suzuki, K.] Nagoya Univ, Ctr Tech, Instrument Dev Grp, Nagoya, Aichi 4648602, Japan.
RP Tsumura, K (reprint author), Japan Aerosp Explorat Agcy JAXA, Dept Space Astron & Astrophys, Inst Space & Astronout Sci, Sagamihara, Kanagawa 2525210, Japan.
EM tsumura@ir.isas.jaxa.jp
RI Matsuura, Shuji/B-5658-2016
OI Matsuura, Shuji/0000-0002-5698-9634
FU NASA APRA [NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G]; Jet
Propulsion Laboratory's Director's Research and Development Fund; JSPS
Research Fellowship for the Young Scientists; NASA Postdoctoral
Fellowship; NSF CAREER award
FX This work was supported by NASA APRA research grants NNX07AI54G,
NNG05WC18G, NNX07AG43G, and NNX07AJ24G. Initial support was provided by
an award to J.B. from the Jet Propulsion Laboratory's Director's
Research and Development Fund. Japanese participation in CIBER was
supported by KAKENHI (20.34, 18204018, 19540250, 21340047, 21111004, and
24111717) from the Japan Society for the Promotion of Science (JSPS) and
the Ministry of Education, Culture, Sports, Science, and Technology
(MEXT). Korean participation in CIBER was supported by the Pioneer
Project from the Korea Astronomy and Space science Institute (KASI).; We
would like to acknowledge the dedicated efforts of the sounding rocket
staff at the NASA Wallops Flight Facility and the White Sands Missile
Range. We also acknowledge the work of the Genesia Corporation for
technical support of the CIBER optics. K. T. acknowledges support from
the JSPS Research Fellowship for the Young Scientists, M.Z. acknowledges
support from a NASA Postdoctoral Fellowship, and A. C. acknowledges
support from an NSF CAREER award. We thank the referee for useful
suggestions which have improved this manuscript.
NR 44
TC 9
Z9 9
U1 1
U2 6
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 AUG
PY 2013
VL 207
IS 2
AR UNSP 33
DI 10.1088/0067-0049/207/2/33
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 195NO
UT WOS:000322710000015
ER
PT J
AU Zemcov, M
Arai, T
Battle, J
Bock, J
Cooray, A
Hristov, V
Keating, B
Kim, MG
Lee, DH
Levenson, LR
Mason, P
Matsumoto, T
Matsuura, S
Nam, UW
Renbarger, T
Sullivan, I
Suzuki, K
Tsumura, K
Wada, T
AF Zemcov, M.
Arai, T.
Battle, J.
Bock, J.
Cooray, A.
Hristov, V.
Keating, B.
Kim, M. G.
Lee, D. H.
Levenson, L. R.
Mason, P.
Matsumoto, T.
Matsuura, S.
Nam, U. W.
Renbarger, T.
Sullivan, I.
Suzuki, K.
Tsumura, K.
Wada, T.
TI THE COSMIC INFRARED BACKGROUND EXPERIMENT (CIBER): A SOUNDING ROCKET
PAYLOAD TO STUDY THE NEAR INFRARED EXTRAGALACTIC BACKGROUND LIGHT
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE dark ages, reionization, first stars; diffuse radiation; infrared:
diffuse background; instrumentation: spectrographs; space vehicles:
instruments; zodiacal dust
ID EMISSION; SEARCH
AB The Cosmic Infrared Background Experiment (CIBER) is a suite of four instruments designed to study the near infrared (IR) background light from above the Earth's atmosphere. The instrument package comprises two imaging telescopes designed to characterize spatial anisotropy in the extragalactic IR background caused by cosmological structure during the epoch of reionization, a low resolution spectrometer to measure the absolute spectrum of the extragalactic IR background, and a narrow band spectrometer optimized to measure the absolute brightness of the zodiacal light foreground. In this paper we describe the design and characterization of the CIBER payload. The detailed mechanical, cryogenic, and electrical design of the system are presented, including all system components common to the four instruments. We present the methods and equipment used to characterize the instruments before and after flight, and give a detailed description of CIBER's flight profile and configurations. CIBER is designed to be recoverable and has flown four times, with modifications to the payload having been informed by analysis of the first flight data. All four instruments performed to specifications during the subsequent flights, and the scientific data from these flights are currently being analyzed.
C1 [Zemcov, M.; Bock, J.; Hristov, V.; Levenson, L. R.; Mason, P.] CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA.
[Zemcov, M.; Battle, J.; Bock, J.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Arai, T.; Matsumoto, T.; Matsuura, S.; Tsumura, K.; Wada, T.] Japan Aerosp Explorat Agcy JAXA, Dept Space Astron & Astrophys, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Arai, T.] Univ Tokyo, Grad Sch Sci, Dept Phys, Tokyo 1130033, Japan.
[Cooray, A.] Univ Calif Irvine, Ctr Cosmol, Irvine, CA 92697 USA.
[Keating, B.; Renbarger, T.] Univ Calif San Diego, Dept Phys, San Diego, CA 92093 USA.
[Kim, M. G.; Matsumoto, T.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea.
[Lee, D. H.; Nam, U. W.] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea.
[Sullivan, I.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Suzuki, K.] Nagoya Univ, Ctr Tech, Instrument Dev Grp, Nagoya, Aichi 4648602, Japan.
RP Zemcov, M (reprint author), CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA.
EM zemcov@caltech.edu
RI Matsuura, Shuji/B-5658-2016
OI Matsuura, Shuji/0000-0002-5698-9634
FU NASA APRA [NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, NNX10AE12G];
Jet Propulsion Laboratory's Director's Research and Development Fund;
NASA Postdoctoral Fellowship; NSF CAREER award; UCSD Hellman Faculty
Fellowship; JSPS Research Fellowship for Young Scientists
FX This work was supported by NASA APRA research grants NNX07AI54G,
NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was
provided by an award to J.B. from the Jet Propulsion Laboratory's
Director's Research and Development Fund. Japanese participation in
CIBER was supported by KAKENHI (20.34, 18204018, 19540250, 21340047, and
21111004) from the Japan Society for the Promotion of Science (JSPS) and
the Ministry of Education, Culture, Sports, Science, and Technology
(MEXT). Korean participation in CIBER was supported by the Pioneer
Project from the Korea Astronomy and Space science Institute (KASI).; We
would like to acknowledge the dedicated efforts of the sounding rocket
staff at the NASA Wallops Flight Facility and the White Sands Missile
Range. We also acknowledge the work of the Genesia Corporation for
technical support of the CIBER optics, and M. C. Runyan and an anonymous
referee for helpful comments on this manuscript. M.Z. acknowledges
support from a NASA Postdoctoral Fellowship, A. C. acknowledges support
from an NSF CAREER award, B. K. acknowledges support from a UCSD Hellman
Faculty Fellowship, and K. T. acknowledges support from the JSPS
Research Fellowship for Young Scientists.
NR 20
TC 12
Z9 12
U1 0
U2 4
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 AUG
PY 2013
VL 207
IS 2
AR UNSP 31
DI 10.1088/0067-0049/207/2/31
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 195NO
UT WOS:000322710000013
ER
PT J
AU Booth, JF
Wang, SG
Polvani, L
AF Booth, James F.
Wang, Shuguang
Polvani, Lorenzo
TI Midlatitude storms in a moister world: lessons from idealized baroclinic
life cycle experiments
SO CLIMATE DYNAMICS
LA English
DT Article
DE Midlatitude storms; Baroclinic; Life cycles; Global warming; Moisture
ID EXTRATROPICAL CYCLONES; PRECIPITATION EXTREMES; NUMERICAL SIMULATIONS;
NORTHERN-HEMISPHERE; STATIC STABILITY; WARMER CLIMATE; CLOUD MODEL;
CYCLOGENESIS; SENSITIVITY; INSTABILITY
AB The response of midlatitude storms to global warming remains uncertain. This is due, in part, to the competing effects of a weaker meridional surface temperature gradient and a higher low-level moisture content, both of which are projected to occur as a consequence of increasing greenhouse gases. Here we address the latter of these two effects, and try to elucidate the effect of increased moisture on the development and evolution of midlatitude storms. We do this with a set of highly controlled, baroclinic lifecycle experiments, in which atmospheric moisture is progressively increased. To assess the robustness of the results, the moisture content is changed in two different ways: first by using different initial relative humidity, and second by varying a parameter that we insert into the Clausius-Clapeyron equation. The latter method allows us to artificially increase the moisture content above current levels while keeping the relative humidity constant. Irrespective of how moisture is altered, we find that nearly all important measures of storm strength increase as the moisture content rises. Specifically, we examine the storm's central pressure minimum, the strongest surface winds, and both extreme and accumulated precipitation rates. For all these metrics, increased moisture yields a stronger storm. Interestingly, we also find that when moisture is increased beyond current levels, the resulting storm has a reduced horizontal scale while its vertical extent increases. Finally, we note that for moisture increases comparable to those projected to occur by the end of the twentyfirst century, the actual amplitude of the increases in storm strength is relatively modest, irrespective of the specific measure one uses.
C1 [Booth, James F.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Wang, Shuguang; Polvani, Lorenzo] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
[Polvani, Lorenzo] Columbia Univ, Dept Earth & Environm Sci, Lamont Doherty Earth Observ, New York, NY 10027 USA.
RP Booth, JF (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM jbooth.atmos@gmail.com
RI Wang, Shuguang/C-2893-2011
OI Wang, Shuguang/0000-0003-1861-9285
FU LMP; US National Science Foundation; National Aeronautics and Space
Administration (NASA)
FX We acknowledge the World Climate Research Programme's Working Group on
Coupled Modeling, which is responsible for CMIP, and we thank the
climate modeling groups (listed in the Sect. Appendix) for producing and
making available their model output. For CMIP the U.S. Department of
Energy's PCMDU provides coordinating support and led development of
software infrastructure in partnership with the Global Organization for
Earth System Science Portals. The work of LMP is funded, in part, by a
grant from the US National Science Foundation. The work of JFB is funded
by the National Aeronautics and Space Administration (NASA) postdoctoral
program. SW thanks Jian Lu for discussions of experiment design at
earlier phase. We thank Heini Wernli and an anonymous reviewer for
useful suggestions that helped to clarify the presentation of the main
points of this work.
NR 44
TC 21
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U1 0
U2 20
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
J9 CLIM DYNAM
JI Clim. Dyn.
PD AUG
PY 2013
VL 41
IS 3-4
BP 787
EP 802
DI 10.1007/s00382-012-1472-3
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 194GQ
UT WOS:000322619500015
ER
PT J
AU Turyshev, SG
Williams, JG
Folkner, WM
Gutt, GM
Baran, RT
Hein, RC
Somawardhana, RP
Lipa, JA
Wang, SW
AF Turyshev, Slava G.
Williams, James G.
Folkner, William M.
Gutt, Gary M.
Baran, Richard T.
Hein, Randall C.
Somawardhana, Ruwan P.
Lipa, John A.
Wang, Suwen
TI Corner-cube retro-reflector instrument for advanced lunar laser ranging
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Lunar laser ranging; Laser corner-cube retro-reflector; Moon
ID TESTS
AB Lunar laser ranging (LLR) has made major contributions to our understanding of the Moon's internal structure and the dynamics of the Earth-Moon system. Because of the recent improvements of the ground-based laser ranging facilities, the present LLR measurement accuracy is limited by the retro-reflectors currently on the lunar surface, which are arrays of small corner-cubes. Because of lunar librations, the surfaces of these arrays do not, in general, point directly at the Earth. This effect results in a spread of arrival times, because each cube that comprises the retroreflector is at a slightly different distance from the Earth, leading to the reduced ranging accuracy. Thus, a single, wide aperture corner-cube could have a clear advantage. In addition, after nearly four decades of successful operations the retro-reflectors arrays currently on the Moon started to show performance degradation; as a result, they yield still useful, but much weaker return signals. Thus, fresh and bright instruments on the lunar surface are needed to continue precision LLR measurements. We have developed a new retro-reflector design to enable advanced LLR operations. It is based on a single, hollow corner cube with a large aperture for which preliminary thermal, mechanical, and optical design and analysis have been performed. The new instrument will be able to reach an Earth-Moon range precision of 1-mm in a single pulse while being subjected to significant thermal variations present on the lunar surface, and will have low mass to allow robotic deployment. Here we report on our design results and instrument development effort.
C1 [Turyshev, Slava G.; Williams, James G.; Folkner, William M.; Gutt, Gary M.; Baran, Richard T.; Hein, Randall C.; Somawardhana, Ruwan P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lipa, John A.; Wang, Suwen] Stanford Univ, Dept Phys, Hansen Expt Phys Lab, Stanford, CA 94305 USA.
RP Turyshev, SG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM turyshev@jpl.nasa.gov
NR 29
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Z9 3
U1 0
U2 17
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD AUG
PY 2013
VL 36
IS 1-2
BP 105
EP 135
DI 10.1007/s10686-012-9324-z
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 198HV
UT WOS:000322914200005
ER
PT J
AU Konovalenko, AA
Stanislavsky, AA
Rucker, HO
Lecacheux, A
Mann, G
Bougeret, JL
Kaiser, ML
Briand, C
Zarka, P
Abranin, EP
Dorovsky, VV
Koval, AA
Mel'nik, VN
Mukha, DV
Panchenko, M
AF Konovalenko, A. A.
Stanislavsky, A. A.
Rucker, H. O.
Lecacheux, A.
Mann, G.
Bougeret, J. -L.
Kaiser, M. L.
Briand, C.
Zarka, P.
Abranin, E. P.
Dorovsky, V. V.
Koval, A. A.
Mel'nik, V. N.
Mukha, D. V.
Panchenko, M.
TI Synchronized observations by using the STEREO and the largest
ground-based decametre radio telescope
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Solar corona; Solar radio radiation; Telescopes; Space vehicle
instruments
ID GALACTIC BACKGROUND-RADIATION; QUIET SUN; INTERPLANETARY SCINTILLATION;
SOLAR CORONA; EMISSION; BURSTS; MHZ; TEMPERATURE; WAVELENGTHS; ANTENNA
AB We consider the approach to simultaneous (synchronous) solar observations of radio emission by using the STEREO-WAVES instruments (frequency range 0.125-16 MHz) and the largest ground-based low-frequency radio telescope. We illustrate it by the UTR-2 radio telescope implementation (10-30 MHz). The antenna system of the radio telescope is a T-shape-like array of broadband dipoles and is located near the village Grakovo in the Kharkiv region (Ukraine). The third observation point on the ground in addition to two space-based ones improves the space-mission performance capabilities for the determination of radio-emission source directivity. The observational results from the high sensitivity antenna UTR-2 are particularly useful for analysis of STEREO data in the condition of weak event appearances during solar activity minima. In order to improve the accuracy of flux density measurements, we also provide simultaneous observations with a large part of the UTR-2 radio telescope array and its single dipole close to the STEREO-WAVES antennas in sensitivity. This concept has been studied by comparing the STEREO data with ground-based records from 2007-2011 and shown to be effective. The capabilities will be useful in the implementation of new instruments (LOFAR, LWA, MWA, etc.) and during the future Solar Orbiter mission.
C1 [Konovalenko, A. A.; Stanislavsky, A. A.; Abranin, E. P.; Dorovsky, V. V.; Koval, A. A.; Mel'nik, V. N.; Mukha, D. V.] Inst Radio Astron, UA-61002 Kharkov, Ukraine.
[Rucker, H. O.; Panchenko, M.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Lecacheux, A.] Observ Paris, CNRS, Dept Radioastron, UMR 8644, F-92195 Meudon, France.
[Mann, G.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany.
[Bougeret, J. -L.] Observ Paris Site Meudon, LESIA, F-92195 Meudon, France.
[Kaiser, M. L.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Briand, C.; Zarka, P.] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon 10 11, France.
RP Koval, AA (reprint author), Inst Radio Astron, 4 Chervonopraporna St, UA-61002 Kharkov, Ukraine.
EM akonov@ri.kharkov.ua; alexstan@ri.kharkov.ua; helmut.rucker@oeaw.ac.at;
alain.lecacheux@obspm.fr; GMann@aip.de; jean-louis.bougeret@obspm.fr;
michael.l.kaiser@nasa.gov; carine.briand@obspm.fr;
Philippe.Zarka@obspm.fr; koval2211@rambler.ru
RI Stanislavsky, Aleksander/C-5435-2015
OI Stanislavsky, Aleksander/0000-0003-4420-047X
FU NASU-CNRS PICS [1.33.11]; International Research Staff Exchange Scheme
"SOLSPANET"; Austrian "Fonds zur Foerderung der wissenschaftlichen
Forschung" [251 P20680-N16]
FX This work was supported in the frame of the NASU-CNRS PICS program
"Development of LF radioastronomy with ultrahigh sensitivity and
resolution" (Grant 1.33.11) and the International Research Staff
Exchange Scheme "SOLSPANET". The WAVES-STEREO and Wind WAVES instruments
are a joint effort of the Paris-Meudon Observatory, the University of
Minnesota, and the Goddard Space Flight Center. The authors are thankful
to the CDPP (Plasma Physics Data Center) team for the assistance with
STEREO/WAVES data access. The work of MP was supported by Austrian
"Fonds zur Foerderung der wissenschaftlichen Forschung" (project 251
P20680-N16). AS is grateful to the Mathematics Institute for pleasant
hospitality during his visit in University of St Andrews.
NR 58
TC 3
Z9 3
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD AUG
PY 2013
VL 36
IS 1-2
BP 137
EP 154
DI 10.1007/s10686-012-9326-x
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 198HV
UT WOS:000322914200006
ER
PT J
AU McEntaffer, R
DeRoo, C
Schultz, T
Gantner, B
Tutt, J
Holland, A
O'Dell, S
Gaskin, J
Kolodziejczak, J
Zhang, WW
Chan, KW
Biskach, M
McClelland, R
Iazikov, D
Wang, XP
Koecher, L
AF McEntaffer, Randall
DeRoo, Casey
Schultz, Ted
Gantner, Brennan
Tutt, James
Holland, Andrew
O'Dell, Stephen
Gaskin, Jessica
Kolodziejczak, Jeffrey
Zhang, William W.
Chan, Kai-Wing
Biskach, Michael
McClelland, Ryan
Iazikov, Dmitri
Wang, Xinpeng
Koecher, Larry
TI First results from a next-generation off-plane X-ray diffraction grating
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE X-ray spectroscopy; Off-plane reflection gratings; X-ray diffraction
ID IMPRINT LITHOGRAPHY; SPECTROSCOPY; TRANSMISSION; NANOIMPRINT;
PERFORMANCE; FABRICATION; RESOLUTION
AB Future NASA X-ray spectroscopy missions will require high throughput, high resolving power grating spectrometers. Off-plane reflection gratings are capable of meeting the performance requirements needed to realize the scientific goals of these missions. We have identified a novel grating fabrication method that utilizes common lithographic and microfabrication techniques to produce the high fidelity groove profile necessary to achieve this performance. Application of this process has produced an initial pre-master that exhibits a radial (variable line spacing along the groove dimension), high density (> 6000 grooves/mm), laminar profile. This pre-master has been tested for diffraction efficiency at the BESSY II synchrotron light facility and diffracts up to 55 % of incident light into usable spectral orders. Furthermore, tests of spectral resolving power show that these gratings are capable of obtaining resolving powers well above 1300 (lambda/Delta lambda) with limitations due to the test apparatus, not the gratings. Obtaining these results has provided confidence that this fabrication process is capable of producing off-plane reflection gratings for the next generation of X-ray observatories.
C1 [McEntaffer, Randall; DeRoo, Casey; Schultz, Ted; Gantner, Brennan] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Tutt, James; Holland, Andrew] Open Univ, Ctr Elect Imaging, Milton Keynes MK7 6AA, Bucks, England.
[O'Dell, Stephen; Gaskin, Jessica; Kolodziejczak, Jeffrey] NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Zhang, William W.; Chan, Kai-Wing; Biskach, Michael; McClelland, Ryan] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Iazikov, Dmitri] LightSmyth Technol Inc, Eugene, OR 97402 USA.
[Wang, Xinpeng; Koecher, Larry] Nanonex Corp, Monmouth Jct, NJ 08852 USA.
RP McEntaffer, R (reprint author), Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA.
EM randall-mcentaffer@uiowa.edu
RI Wang, Xinpeng/N-3876-2013;
OI O'Dell, Stephen/0000-0002-1868-8056
FU NASA [NNX12AF23G, NNX12AI16G]; University of Iowa
FX This work was supported by NASA grants NNX12AF23G and NNX12AI16G. We
would also like to acknowledge internal funding from the University of
Iowa in support of Casey DeRoo. Special thanks are due to several people
including Christian Laubis and his terrific support crew at PTB as well
as James Carter and Bill Jones at MSFC for support of the resolution
tests.
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD AUG
PY 2013
VL 36
IS 1-2
BP 389
EP 405
DI 10.1007/s10686-013-9338-1
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 198HV
UT WOS:000322914200014
ER
PT J
AU Hale, MC
Thrower, FP
Berntson, EA
Miller, MR
Nichols, KM
AF Hale, Matthew C.
Thrower, Frank P.
Berntson, Ewann A.
Miller, Michael R.
Nichols, Krista M.
TI Evaluating Adaptive Divergence Between Migratory and Nonmigratory
Ecotypes of a Salmonid Fish, Oncorhynchus mykiss
SO G3-GENES GENOMES GENETICS
LA English
DT Article
DE smoltification; life history variation; genomics; SNP; salmonids
ID GENOME-WIDE ASSOCIATION; QUANTITATIVE TRAIT LOCI; RAINBOW-TROUT GENOME;
GENETIC-BASIS; SNP DISCOVERY; POPULATION GENOMICS; NATURAL-SELECTION;
ANIMAL MIGRATION; ATLANTIC SALMON; STEELHEAD TROUT
AB Next-generation sequencing and the application of population genomic and association approaches have made it possible to detect selection and unravel the genetic basis to variable phenotypic traits. The use of these two approaches in parallel is especially attractive in nonmodel organisms that lack a sequenced and annotated genome, but only works well when population structure is not confounded with the phenotype of interest. Herein, we use population genomics in a nonmodel fish species, rainbow trout (Oncorhynchus mykiss), to better understand adaptive divergence between migratory and nonmigratory ecotypes and to further our understanding about the genetic basis of migration. Restriction site-associated DNA (RAD) tag sequencing was used to identify single-nucleotide polymorphisms (SNPs) in migrant and resident O. mykiss from two systems, one in Alaska and the other in Oregon. A total of 7920 and 6755 SNPs met filtering criteria in the Alaska and Oregon data sets, respectively. Population genetic tests determined that 1423 SNPs were candidates for selection when loci were compared between resident and migrant samples. Previous linkage mapping studies that used RAD DNA tag SNPs were available to determine the position of 1990 markers. Several significant SNPs are located in genome regions that contain quantitative trait loci for migratory-related traits, reinforcing the importance of these regions in the genetic basis of migration/residency. Annotation of genome regions linked to significant SNPs revealed genes involved in processes known to be important in migration (such as osmoregulatory function). This study adds to our growing knowledge on adaptive divergence between migratory and nonmigratory ecotypes of this species; across studies, this complex trait appears to be controlled by many loci of small effect, with some in common, but many loci not shared between populations studied.
C1 [Hale, Matthew C.; Nichols, Krista M.] Purdue Univ, Dept Biol Sci, W Lafayette, IN USA.
[Thrower, Frank P.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Ted Stevens Marine Inst, Juneau, AK 99801 USA.
[Berntson, Ewann A.; Nichols, Krista M.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA.
[Miller, Michael R.] Univ Calif Davis, Dept Anim Sci, Davis, CA 95616 USA.
RP Nichols, KM (reprint author), NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Conservat Biol Div, 2725 Montlake Blvd E, Seattle, WA 98112 USA.
EM krista.nichols@noaa.gov
RI chen, zhu/K-5923-2013
FU NSF [NSF-DEB-0845265]
FX We thank Nick Marra, Ashley Chin-Baarstad, Garrett McKinney, Julie
Scardina, Vanessa Reynolds Hale, Mike Ford, Jeff Hard, and anonymous
reviewers and editors for comments and suggestions on the manuscript.
Phillip San Miguel, Paul Parker, and Ann Feil were instrumental in the
sequencing of the Illumina RAD tag libraries. Garrett McKinney provided
assistance with Perl scripts to help parse and analyze the data. Charlie
Waters, John Colletti, and Michael Zanis provided field assistance in
the collection of Alaskan samples. Heather Holzhauer helped in
extracting the DNA from the Alaskan samples. Mike Flesher and his crew
helped collect samples from the Little Sheep Creek population. Yniv
Palti and Guangtu Guo were helpful in discussions on the scripts used to
construct the SNP databases. Funding was provided by an NSF Career award
to K.M.N. (NSF-DEB-0845265).
NR 67
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U2 134
PU GENETICS SOC AM
PI BETHESDA
PA 9650 ROCKVILLE AVE, BETHESDA, MD 20814 USA
SN 2160-1836
J9 G3-GENES GENOM GENET
JI G3-Genes Genomes Genet.
PD AUG 1
PY 2013
VL 3
IS 8
BP 1273
EP 1285
DI 10.1534/g3.113.006817
PG 13
WC Genetics & Heredity
SC Genetics & Heredity
GA 197BJ
UT WOS:000322822300010
PM 23797103
ER
PT J
AU Aydemir, A
Pronobis, A
Gobelbecker, M
Jensfelt, P
AF Aydemir, Alper
Pronobis, Andrzej
Gobelbecker, Moritz
Jensfelt, Patric
TI Active Visual Object Search in Unknown Environments Using Uncertain
Semantics
SO IEEE TRANSACTIONS ON ROBOTICS
LA English
DT Article
DE Active vision; semantic mapping; visual object search
ID PLACE CLASSIFICATION; MOBILE ROBOTS; RECOGNITION; SYSTEMS
AB In this paper, we study the problem of active visual search (AVS) in large, unknown, or partially known environments. We argue that by making use of uncertain semantics of the environment, a robot tasked with finding an object can devise efficient search strategies that can locate everyday objects at the scale of an entire building floor, which is previously unknown to the robot. To realize this, we present a probabilistic model of the search environment, which allows for prioritizing the search effort to those parts of the environment that are most promising for a specific object type. Further, we describe a method for reasoning about the unexplored part of the environment for goal-directed exploration with the purpose of object search. We demonstrate the validity of our approach by comparing it with two other search systems in terms of search trajectory length and time. First, we implement a greedy coverage-based search strategy that is found in previous work. Second, we let human participants search for objects as an alternative comparison for our method. Our results show that AVS strategies that exploit uncertain semantics of the environment are a very promising idea, and our method pushes the state-of-the-art forward in AVS.
C1 [Aydemir, Alper; Pronobis, Andrzej] Royal Inst Technol, Ctr Autonomous Syst, S-10044 Stockholm, Sweden.
[Gobelbecker, Moritz] Univ Freiburg, D-79110 Freiburg, Germany.
[Jensfelt, Patric] KTH Royal Inst Technol, Ctr Autonomous Syst, S-10044 Stockholm, Sweden.
RP Aydemir, A (reprint author), NASA, Jet Prop Lab, Comp Vis Grp, Los Angeles, CA 91109 USA.
EM aydemir@kth.se; pronobis@csc.kth.se;
goebelbe@informatik.uni-freiburg.de; patric@csc.kth.se
NR 55
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U1 1
U2 15
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 AUG
PY 2013
VL 29
IS 4
BP 986
EP 1002
DI 10.1109/TRO.2013.2256686
PG 17
WC Robotics
SC Robotics
GA 197FZ
UT WOS:000322836600014
ER
PT J
AU Heymsfield, GM
Tian, L
Li, LH
McLinden, M
Cervantes, JI
AF Heymsfield, Gerald M.
Tian, Lin
Li, Lihua
McLinden, Matthew
Cervantes, Jaime I.
TI Airborne Radar Observations of Severe Hailstorms: Implications for
Future Spaceborne Radar
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
DE Radars; Radar observations
ID GROUND-BASED RADAR; DOPPLER RADAR; CONVECTIVE STORMS; PRECIPITATION
RADAR; HAIL; THUNDERSTORMS; VELOCITY; MODEL; TRMM
AB A new dual-frequency (Ku and Ka band) nadir-pointing Doppler radar on the high-altitude NASA ER-2 aircraft, called the High-Altitude Imaging Wind and Rain Airborne Profiler (HIWRAP), has collected data over severe thunderstorms in Oklahoma and Kansas during the Midlatitude Continental Convective Clouds Experiment (MC3E). The overarching motivation for this study is to understand the behavior of the dual-wavelength airborne radar measurements in a global variety of thunderstorms and how these may relate to future spaceborne-radar measurements. HIWRAP is operated at frequencies that are similar to those of the precipitation radar on the Tropical Rainfall Measuring Mission (Ku band) and the upcoming Global Precipitation Measurement mission satellite's dual-frequency (Ku and Ka bands) precipitation radar. The aircraft measurements of strong hailstorms have been combined with ground-based polarimetric measurements to obtain a better understanding of the response of the Ku- and Ka-band radar to the vertical distribution of the hydrometeors, including hail. Data from two flight lines on 24 May 2011 are presented. Doppler velocities were similar to 39 m s(-1) at 10.7-km altitude from the first flight line early on 24 May, and the lower value of similar to 25 m s(-1) on a second flight line later in the day. Vertical motions estimated using a fall speed estimate for large graupel and hail suggested that the first storm had an updraft that possibly exceeded 60 m s(-1) for the more intense part of the storm. This large updraft speed along with reports of 5-cm hail at the surface, reflectivities reaching 70 dBZ at S band in the storm cores, and hail signals from polarimetric data provide a highly challenging situation for spaceborne-radar measurements in intense convective systems. The Ku- and Ka-band reflectivities rarely exceed similar to 47 and similar to 37 dBZ, respectively, in these storms.
C1 [Heymsfield, Gerald M.; Tian, Lin; Li, Lihua; McLinden, Matthew; Cervantes, Jaime I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tian, Lin] Morgan State Univ, Baltimore, MD 21239 USA.
[Cervantes, Jaime I.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Heymsfield, GM (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM gerald.heymsfield@nasa.gov
RI Measurement, Global/C-4698-2015
FU GPM Ground Validation; NASA Precipitation Measuring Mission (PMM); NASA
Instrument Incubator Program
FX This work was supported by the GPM Ground Validation (Drs. Matt
Schwaller and Walt Petersen) and by NASA Precipitation Measuring Mission
(PMM) funding. The U.S. DOE ARS was a major contributor in providing the
infrastructure for MC3E. Acknowledgment is given to the NASA Dryden ER-2
group that expeditiously integrated HIWRAP onto the ER-2 and conducted
the flights. HIWRAP was funded under the NASA Instrument Incubator
Program as a new technology instrument development. The authors thank
the anonymous reviewers for their thorough comments. We thank Dr. Andrew
Heymsfield for advice on the hail terminal velocities and Prof. Ramesh
Srivastava and Dr. Alexander Ryzhkov for insightful discussions on radar
hail observations and scattering aspects; Dr. Simone Tanelli provided
insightful comments on the manuscript, particularly with regard to
multiple-scattering processes. We also thank Dr. Stephen Guimond for his
comments on the manuscript, Mr. Martin Perrine and Mr. Michael Coon for
engineering support, and Dr. Amber Emory for field support and initial
analysis.
NR 42
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U1 3
U2 13
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 AUG
PY 2013
VL 52
IS 8
BP 1851
EP 1867
DI 10.1175/JAMC-D-12-0144.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 200BP
UT WOS:000323041800012
ER
PT J
AU Bosilovich, MG
AF Bosilovich, Michael G.
TI Regional Climate and Variability of NASA MERRA and Recent Reanalyses:
U.S. Summertime Precipitation and Temperature
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
DE Precipitation; Climate variability; Surface temperature; Climate
records; Reanalysis data
ID DATA ASSIMILATION SYSTEM; SEA-SURFACE TEMPERATURE; CENTRAL
UNITED-STATES; ENERGY; WATER; SEASONALITY; MOISTURE; BUDGETS; ERA-40;
TRENDS
AB Reanalyses have increasingly improved resolution and physical representation of regional climate and so may provide useful data in many regional applications. These data are not observations, however, and their limitations and uncertainties need to be closely investigated. The ability of reanalyses to reproduce the seasonal variations of precipitation and temperature over the United States during summer, when model forecasts have characteristically weak forecast skill, is assessed. Precipitation variations are reproduced well over much of the United States, especially in the Northwest, where ENSO contributes to the large-scale circulation. Some significant biases in the seasonal mean do exist. The weakest regions are the Midwest and Southeast, where land-atmosphere interactions strongly affect the physical parameterizations in the forecast model. In particular, the variance of the Modern-Era Retrospective Analysis for Research and Applications (MERRA) is too low (extreme seasonal averages are weak), and the variability of the Interim ECMWF Re-Analysis (ERA-Interim) is affected by spurious low-frequency trends. Surface temperature is generally robust among the reanalyses examined, though; reanalyses that assimilate near-surface observations have distinct advantages. Observations and forecast error from MERRA are used to assess the reanalysis uncertainty across U.S. regions. These data help to show where the reanalysis is realistically replicating physical processes, and they provide guidance on the quality of the data and needs for further development.
C1 NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bosilovich, MG (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM michael.bosilovich@nasa.gov
RI Bosilovich, Michael/F-8175-2012
FU NASA Energy and Water Cycle Studies Program (NEWS)
FX This work was supported as a NASA agency contribution to the National
Climate Assessment. Partial support was also contributed through the
NASA Energy and Water Cycle Studies Program (NEWS). MERRA was developed
and produced through the NASA Modeling, Analysis, and Prediction (MAP)
program. Arlindo da Silva developed the Gridded Innovations and
Observations (GIO) data used to evaluate the MERRA forecast error. The
author greatly appreciates useful discussions with Franklin R. Robertson
and Siegfried D. Schubert on the results of the study. Comments and
suggestions from Russel Vose and an anonymous reviewer contributed
greatly to the final form of this manuscript.
NR 36
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U1 0
U2 17
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 AUG
PY 2013
VL 52
IS 8
BP 1939
EP 1951
DI 10.1175/JAMC-D-12-0291.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 200BP
UT WOS:000323041800018
ER
PT J
AU Bilham, R
Fielding, E
AF Bilham, Roger
Fielding, Eric
TI Remote sensing and the search for surface rupture, Haiti 2010
SO NATURAL HAZARDS
LA English
DT Editorial Material
DE Remote sensing; Haiti earthquake; Surface deformation
ID EARTHQUAKE
AB Minutes after the January 12, 2010 Haiti earthquake, most geologists and seismologists assumed that from its shallow teleseismic location and its largely strike-slip mechanism that a significant rupture must have occurred on the transform plate boundary south and west of Port au Prince. Within hours, plans were being made by geologists to map the anticipated rupture and, if possible, to trench it to obtain a record of paleoseismic slip. However, remote sensing images available a few days after the earthquake revealed raised corals and no significant plate boundary slip, and we now know that shallow slip was transpressive and that no surface rupture occurred. A week after the earthquake, it was clear that scientific visits to the region would be much delayed by the continuing needs of emergency response teams and military support who had commandeered access to the airport at Port au Prince. Serendipitously on 20 January, one of the authors accompanied a film crew on a chartered flight from nearby Santo Domingo with the quest to record the tectonic reasons for the disaster and to document the details of structural damage. At the time, there was still no clear idea of whether the transform boundary had a surface rupture, but there was abundant evidence for surface deformation from Google Earth images showing raised corals and collapsed coastlines along the Leogane coast. This article briefly describes communications between remote geologists and the ground-based crew who were guided to critical areas in the search for surface deformation using remote sensing data.
C1 [Bilham, Roger] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Bilham, Roger] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Fielding, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bilham, R (reprint author), Univ Colorado, CIRES, Boulder, CO 80309 USA.
EM bilham@colorado.edu; Eric.Fielding@jpl.nasa.gov
RI Fielding, Eric/A-1288-2007;
OI Fielding, Eric/0000-0002-6648-8067; Bilham, Roger/0000-0002-5547-4102
NR 8
TC 1
Z9 1
U1 0
U2 20
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0921-030X
J9 NAT HAZARDS
JI Nat. Hazards
PD AUG
PY 2013
VL 68
IS 1
BP 213
EP 217
DI 10.1007/s11069-013-0550-0
PG 5
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Water Resources
SC Geology; Meteorology & Atmospheric Sciences; Water Resources
GA 195SN
UT WOS:000322724000017
ER
PT J
AU Jee, S
Mejia, ODL
Moser, RD
Muse, JA
Kutay, AT
Calise, AJ
AF Jee, SolKeun
Lopez Mejia, Omar D.
Moser, Robert D.
Muse, Jonathan A.
Kutay, Ali T.
Calise, Anthony J.
TI Simulation of Rapidly Maneuvering Airfoils with Synthetic Jet Actuators
SO AIAA JOURNAL
LA English
DT Article
ID EQUATION TURBULENCE MODEL; DETACHED-EDDY SIMULATION; AERODYNAMIC
FLOW-CONTROL; SEPARATION CONTROL; REYNOLDS
AB Synthetic jet actuators are investigated for rapidly maneuvering airfoils that are regulated by a closed-loop control system. To support active flow-control simulations performed here, the closed-loop system and vehicle dynamics are coupled with computational fluid dynamics. High-frequency sinusoidal pitching simulations with and without synthetic jet actuation indicate that the current synthetic jet actuators provide bidirectional change in aerodynamic forces during rapid maneuvers whose time scales are of the same order as the flow time scales. Responses of a wind-tunnel airfoil are well represented in the current simulations, which allows us to predict the response of the system for dynamic conditions representative of free flight. The control system is able to execute rapid free-flight maneuvers. It is observed that the controller is responding to small fluctuations caused by vortex shedding from the trailing-edge actuators.
C1 [Jee, SolKeun] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA.
[Lopez Mejia, Omar D.] Univ Andes, Dept Mech Engn, CO-0001 Bogota, Colombia.
[Moser, Robert D.] Univ Texas Austin, Dept Mech Engn, Inst Computat Engn & Sci, Austin, TX 78712 USA.
[Muse, Jonathan A.] US Air Force Res Lab, Air Vehicle Directorate, Dayton, OH 45433 USA.
[Kutay, Ali T.] Middle E Tech Univ, Dept Aerosp Engn, TR-06531 Ankara, Turkey.
[Calise, Anthony J.] Georgia Inst Technol, Sch Aerosp Engn, Atlanta, GA 30332 USA.
RP Jee, S (reprint author), NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA.
FU U.S. Air Force Office of Scientific Research [FA9550-05-1-0411];
Multidisciplinary University Research Initiative; NASA
FX This work was supported by the U.S. Air Force Office of Scientific
Research (grant FA9550-05-1-0411) and the Multidisciplinary University
Research Initiative. Although this study was finished during the
graduate study of the first author at the University of Texas at Austin,
the first author thanks the NASA Postdoctoral Program administrated by
Oak Ridge Associated Universities for supports to write this paper up at
the NASA Ames Research Center. The authors would like to thank Daniel
Brzozowski and An Glezer at the Georgia Institute of Technology for
providing the wind-tunnel experimental data. The authors also wish to
acknowledge Gianluca Iaccarino at Stanford University for providing
CDPv2.3.
NR 43
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U1 1
U2 16
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 AUG
PY 2013
VL 51
IS 8
BP 1883
EP 1897
DI 10.2514/1.J052080
PG 15
WC Engineering, Aerospace
SC Engineering
GA 193JZ
UT WOS:000322557400008
ER
PT J
AU Smee, SA
Gunn, JE
Uomoto, A
Roe, N
Schlegel, D
Rockosi, CM
Carr, MA
Leger, F
Dawson, KS
Olmstead, MD
Brinkmann, J
Owen, R
Barkhouser, RH
Honscheid, K
Harding, P
Long, D
Lupton, RH
Loomis, C
Anderson, L
Annis, J
Bernardi, M
Bhardwaj, V
Bizyaev, D
Bolton, AS
Brewington, H
Briggs, JW
Burles, S
Burns, JG
Castander, FJ
Connolly, A
Davenport, JRA
Ebelke, G
Epps, H
Feldman, PD
Friedman, SD
Frieman, J
Heckman, T
Hull, CL
Knapp, GR
Lawrence, DM
Loveday, J
Mannery, EJ
Malanushenko, E
Malanushenko, V
Merrelli, AJ
Muna, D
Newman, PR
Nichol, RC
Oravetz, D
Pan, K
Pope, AC
Ricketts, PG
Shelden, A
Sandford, D
Siegmund, W
Simmons, A
Smith, DS
Snedden, S
Schneider, DP
SubbaRao, M
Tremonti, C
Waddell, P
York, DG
AF Smee, Stephen A.
Gunn, James E.
Uomoto, Alan
Roe, Natalie
Schlegel, David
Rockosi, Constance M.
Carr, Michael A.
Leger, French
Dawson, Kyle S.
Olmstead, Matthew D.
Brinkmann, Jon
Owen, Russell
Barkhouser, Robert H.
Honscheid, Klaus
Harding, Paul
Long, Dan
Lupton, Robert H.
Loomis, Craig
Anderson, Lauren
Annis, James
Bernardi, Mariangela
Bhardwaj, Vaishali
Bizyaev, Dmitry
Bolton, Adam S.
Brewington, Howard
Briggs, John W.
Burles, Scott
Burns, James G.
Javier Castander, Francisco
Connolly, Andrew
Davenport, James R. A.
Ebelke, Garrett
Epps, Harland
Feldman, Paul D.
Friedman, Scott D.
Frieman, Joshua
Heckman, Timothy
Hull, Charles L.
Knapp, Gillian R.
Lawrence, David M.
Loveday, Jon
Mannery, Edward J.
Malanushenko, Elena
Malanushenko, Viktor
Merrelli, Aronne James
Muna, Demitri
Newman, Peter R.
Nichol, Robert C.
Oravetz, Daniel
Pan, Kaike
Pope, Adrian C.
Ricketts, Paul G.
Shelden, Alaina
Sandford, Dale
Siegmund, Walter
Simmons, Audrey
Smith, D. Shane
Snedden, Stephanie
Schneider, Donald P.
SubbaRao, Mark
Tremonti, Christy
Waddell, Patrick
York, Donald G.
TI THE MULTI-OBJECT, FIBER-FED SPECTROGRAPHS FOR THE SLOAN DIGITAL SKY
SURVEY AND THE BARYON OSCILLATION SPECTROSCOPIC SURVEY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE cosmology: observations; instrumentation: spectrographs; surveys
ID 9TH DATA RELEASE; SDSS-III; ACOUSTIC-OSCILLATIONS; TARGET SELECTION;
GALAXY SAMPLE; TELESCOPE; CALIBRATION; SYSTEM; STARS; CCDS
AB We present the design and performance of the multi-object fiber spectrographs for the Sloan Digital Sky Survey (SDSS) and their upgrade for the Baryon Oscillation Spectroscopic Survey (BOSS). Originally commissioned in Fall 1999 on the 2.5 m aperture Sloan Telescope at Apache Point Observatory, the spectrographs produced more than 1.5 million spectra for the SDSS and SDSS-II surveys, enabling a wide variety of Galactic and extra-galactic science including the first observation of baryon acoustic oscillations in 2005. The spectrographs were upgraded in 2009 and are currently in use for BOSS, the flagship survey of the third-generation SDSS-III project. BOSS will measure redshifts of 1.35 million massive galaxies to redshift 0.7 and Ly alpha absorption of 160,000 high redshift quasars over 10,000 deg(2) of sky, making percent level measurements of the absolute cosmic distance scale of the universe and placing tight constraints on the equation of state of dark energy. The twin multi-object fiber spectrographs utilize a simple optical layout with reflective collimators, gratings, all-refractive cameras, and state-of-the-art CCD detectors to produce hundreds of spectra simultaneously in two channels over a bandpass covering the near-ultraviolet to the near-infrared, with a resolving power R = lambda/FWHM similar to 2000. Building on proven heritage, the spectrographs were upgraded for BOSS with volume-phase holographic gratings and modern CCD detectors, improving the peak throughput by nearly a factor of two, extending the bandpass to cover 360 nm < lambda < 1000 nm, and increasing the number of fibers from 640 to 1000 per exposure. In this paper we describe the original SDSS spectrograph design and the upgrades implemented for BOSS, and document the predicted and measured performances.
C1 [Smee, Stephen A.; Barkhouser, Robert H.; Feldman, Paul D.; Heckman, Timothy] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Gunn, James E.; Carr, Michael A.; Lupton, Robert H.; Loomis, Craig; Knapp, Gillian R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Uomoto, Alan; Hull, Charles L.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Roe, Natalie; Schlegel, David] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Rockosi, Constance M.; Epps, Harland; Sandford, Dale] Univ Calif Santa Cruz, UC Observ, Santa Cruz, CA 95064 USA.
[Rockosi, Constance M.; Epps, Harland; Sandford, Dale] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Leger, French; Owen, Russell; Anderson, Lauren; Bhardwaj, Vaishali; Connolly, Andrew; Davenport, James R. A.; Mannery, Edward J.; Siegmund, Walter] Univ Washington, Dept Astron, Seattle, WA 09195 USA.
[Dawson, Kyle S.; Olmstead, Matthew D.; Bolton, Adam S.; Lawrence, David M.; Ricketts, Paul G.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Brinkmann, Jon; Long, Dan; Bizyaev, Dmitry; Brewington, Howard; Ebelke, Garrett; Malanushenko, Elena; Malanushenko, Viktor; Newman, Peter R.; Oravetz, Daniel; Pan, Kaike; Shelden, Alaina; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA.
[Honscheid, Klaus; Burns, James G.; Smith, D. Shane] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Honscheid, Klaus; Burns, James G.; Smith, D. Shane] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Harding, Paul] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA.
[Annis, James; Frieman, Joshua] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Bernardi, Mariangela; SubbaRao, Mark] Univ Penn, Dept Astron & Astrophys, Philadelphia, PA 19104 USA.
[Briggs, John W.] Mittelman Family Fdn, HUT Observ, Eagle, CO 81631 USA.
[Burles, Scott] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Javier Castander, Francisco] Inst Ciencies Espai IEEC CSIC, E-08193 Barcelona, Spain.
[Javier Castander, Francisco; Friedman, Scott D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Loveday, Jon] Univ Sussex, Ctr Astron, Brighton BN1 9QJ, E Sussex, England.
[Merrelli, Aronne James] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Muna, Demitri] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Nichol, Robert C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Pope, Adrian C.] Argonne Natl Lab, Div High Energy Phys, Lemont, IL 60439 USA.
[Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Tremonti, Christy] Univ Wisconsin, Dept Astron, Madison, WI 53703 USA.
[Waddell, Patrick] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[York, Donald G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[York, Donald G.] Univ Chicago, Fermi Inst, Chicago, IL 60637 USA.
RP Smee, SA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM smee@pha.jhu.edu
OI Davenport, James/0000-0002-0637-835X
FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department
of Energy Office of Science
FX Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, and the U.S. Department of Energy Office of Science. The
SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the
Astrophysical Research Consortium for the Participating Institutions of
the SDSS-III Collaboration including the University of Arizona, the
Brazilian Participation Group, Brookhaven National Laboratory,
University of Cambridge, Carnegie Mellon University, University of
Florida, the French Participation Group, the German Participation Group,
Harvard University, the Instituto de Astrofisica de Canarias, the
Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins
University, Lawrence Berkeley National Laboratory, Max Planck Institute
for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New
Mexico State University, New York University, Ohio State University,
Pennsylvania State University, University of Portsmouth, Princeton
University, the Spanish Participation Group, University of Tokyo,
University of Utah, Vanderbilt University, University of Virginia,
University of Washington, and Yale University.
NR 49
TC 223
Z9 223
U1 1
U2 17
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 AUG
PY 2013
VL 146
IS 2
AR 32
DI 10.1088/0004-6256/146/2/32
PG 40
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 183TW
UT WOS:000321841100014
ER
PT J
AU Martin, RA
AF Martin, Rodney A.
TI Optimal level-crossing prediction for jump linear MIMO dynamical systems
SO AUTOMATICA
LA English
DT Article
DE Alarm systems; Kalman filters; Prediction problems; Prediction methods;
Multivariable systems
ID SPEECH RECOGNITION; GAUSSIAN-PROCESSES
AB In this article, the theoretically optimal prediction of level-crossings for a jump linear MIMO (multi-input/multi-output) dynamical system driven by a control input is investigated. The study of this problem is motivated by the practical implications for design of an optimal alarm system as applied to the advance prediction of adverse events, which will elicit the fewest false alarms for a fixed detection probability. It was found that using an additional control input term results in increased uncertainty due to the associated model for the control. However, using the appropriate condition for optimality provides an accommodation for this uncertainty which does not translate into compromised predictive capability. For the given application, it was observed that modeling the control input as a linear dynamical system results in better prediction performance and qualitatively has a higher model fidelity than when using a hidden Markov model for the same function. Published by Elsevier Ltd
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Martin, RA (reprint author), NASA, Ames Res Ctr, Mail Stop 269-1,Bldg N269,Rm 260-17,POB 1, Moffett Field, CA 94035 USA.
EM rodney.martin@nasa.gov
FU Systemwide Safety Assurance Technologies (SSAT) project; Integrated
Vehicle Health Management (IVHM) project; Aviation Safety Program of
NASA's Aeronautics Research Mission Directorate
FX This work was supported in part by the Systemwide Safety Assurance
Technologies (SSAT) project and the Integrated Vehicle Health Management
(IVHM) project, funded by the Aviation Safety Program of NASA's
Aeronautics Research Mission Directorate. The material in this paper was
not presented at any conference. This paper was recommended for
publication in revised form by Associate Editor Martin Enqvist under the
direction of Editor Torsten Soderstrom.
NR 22
TC 2
Z9 2
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0005-1098
J9 AUTOMATICA
JI Automatica
PD AUG
PY 2013
VL 49
IS 8
BP 2440
EP 2445
DI 10.1016/j.automatica.2013.04.008
PG 6
WC Automation & Control Systems; Engineering, Electrical & Electronic
SC Automation & Control Systems; Engineering
GA 193LW
UT WOS:000322562300013
ER
PT J
AU Nitschke, W
McGlynn, SE
Milner-White, EJ
Russell, MJ
AF Nitschke, Wolfgang
McGlynn, Shawn E.
Milner-White, E. James
Russell, Michael J.
TI On the antiquity of metalloenzymes and their substrates in bioenergetics
SO BIOCHIMICA ET BIOPHYSICA ACTA-BIOENERGETICS
LA English
DT Article
DE Metal sulfide; ACS; CODH; Ni-Fe hydrogenase; Methane monooxygenase
ID IRON-SULFUR CLUSTERS; RESPIRATORY ARSENATE REDUCTASE; ANAEROBIC METHANE
OXIDATION; CITY HYDROTHERMAL FIELD; MID-ATLANTIC RIDGE; GREEN RUST;
EARLY EVOLUTION; NIFE HYDROGENASES; NICKELIAN MACKINAWITE; NITRATE
REDUCTION
AB Many metalloenzymes that inject and extract reducing equivalents at the beginning and the end of electron transport chains involved in chemiosmosis are suggested, through phylogenetic analysis, to have been present in the Last Universal Common Ancestor (LUCA). Their active centres are affine with the structures of minerals presumed to contribute to precipitate membranes produced on the mixing of hydrothermal solutions with the Hadean Ocean similar to 4 billion years ago. These mineral precipitates consist of transition element sulphides and oxides such as nickelian mackinawite ([Fe > Ni](2)S-2), a nickel-bearing greigite (similar to FeSS[Fe3NiS4]SSFe), violarite (similar to NiSS[Fe2Ni2S4]SSNi), a molybdenum bearing complex (similar to(Mo2Fe3S90/2-)-Fe-IV/VI) and green rust or fougerite (similar to[(FeFeIII)-Fe-II(OH)(4)](+)[OH](-)). They may be respectively compared with the active centres of Ni-Fe hydrogenase, carbon monoxide dehydrogenase (CODH), acetyl coenzyme-A synthase (ACS), the complex iron-sulphur molybdoenzyme (CISM) superfamily and methane monooxygenase (MMO). With the look of good catalysts - a suggestion that gathers some support from prebiotic hydrothermal experimentation - and sequestered by short peptides, they could be thought of as the original building blocks of proto-enzyme active centres. This convergence of the makeup of the LUCA-metalloenzymes with mineral structure and composition of hydrothermal precipitates adds credence to the alkaline hydrothermal (chemiosmotic) theory for the emergence of life, specifically to the possibility that the first metabolic pathway - the acetyl CoA pathway - was initially driven from either end, reductively from CO2 to CO and oxidatively and reductively from CH4 through to a methane thiol group, the two entities assembled with the help of a further thiol on a violarite cluster sequestered by peptides. By contrast the organic coenzymes were entirely a product of the first metabolic pathways. This article is part of a Special Issue entitled: Metals in Bioenergetics and Biomimetics Systems. Published by Elsevier B.V.
C1 [Nitschke, Wolfgang] CNRS, IFR88, UPR9036, Lab Bioenerget & Ingn Prot, F-13402 Marseille 20, France.
[McGlynn, Shawn E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Milner-White, E. James] Univ Glasgow, Coll Med Vet & Life Sci, Glasgow G12 8QQ, Lanark, Scotland.
[Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Russell, MJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM michael.j.russell@jpl.nasa.gov
OI Nitschke, Wolfgang/0000-0003-2084-3032
FU NASA Astrobiology Institute (Icy Worlds); US Government
FX We appreciate the help and stimulating discussions with Ariane Atteia,
Frauke Baymann, Robert van Us, Barbara Schoepp-Cothenet
(Marseilles/France), Lauren White and Isik Kanik (Pasadena/California),
Sebastien Gotti (Seraing/Belgium), George Helz (College Park/Maryland),
Nora de Leeuw (London, England) and Ines Pereira (Oeiras/Portugal).
MJR's contribution was made at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration with support by the NASA Astrobiology Institute
(Icy Worlds). US Government sponsorship acknowledged.
NR 159
TC 28
Z9 28
U1 4
U2 92
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0005-2728
J9 BBA-BIOENERGETICS
JI Biochim. Biophys. Acta-Bioenerg.
PD AUG-SEP
PY 2013
VL 1827
IS 8-9
SI SI
BP 871
EP 881
DI 10.1016/j.bbabio.2013.02.008
PG 11
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA 191LK
UT WOS:000322414300002
PM 23454059
ER
PT J
AU Burke, BJ
Liermann, MC
Teel, DJ
Anderson, JJ
AF Burke, Brian J.
Liermann, Martin C.
Teel, David J.
Anderson, James J.
TI Environmental and geospatial factors drive juvenile Chinook salmon
distribution during early ocean migration
SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES
LA English
DT Article
ID NORTHERN CALIFORNIA CURRENT; COHO ONCORHYNCHUS-KISUTCH; COLUMBIA RIVER
PLUME; WIRE TAG RECOVERIES; VERTICAL-DISTRIBUTION; SPATIAL-DISTRIBUTION;
COASTAL OCEAN; LIFE-HISTORY; SEA-TURTLES; TSHAWYTSCHA
AB Migrating animals rely on a variety of cues to guide them, but the relative importance of those signals may vary with size, life stage, or location. During their initial ocean migration, yearling Chinook salmon (Oncorhynchus tshawytcha) from the Columbia River have stock-specific spatial distributions that shift through time. We used a two-process mixture model to examine how the distribution of yearling migrants from three Chinook salmon stocks varies as a function of geospatial (e. g., latitude and distance from shore) and environmental (e. g., chlorophyll a and temperature) covariates. In this framework, one process described the probability of being inside the spatial, temporal, and environmental boundaries of the migration route, and one process described the patchy distribution of salmon abundance within that route. We found that both environmental and geospatial covariates explained substantial portions of observed spatial patterns in abundance, suggesting that these stocks responded to multiple cues during migration. However, model selection criteria indicated that fish distributions were more affected by geospatial than by environmental covariates. We conclude that during migration, behavioral responses to environmental variation are secondary to responses to geospatial variation, sometimes resulting in suboptimal environmental conditions. This may have sublethal effects on growth and could ultimately influence stock-specific responses to broad-scale climate changes.
C1 [Burke, Brian J.; Liermann, Martin C.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA.
[Teel, David J.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Manchester, WA 98353 USA.
[Anderson, James J.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA.
RP Burke, BJ (reprint author), NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, 2725 Montlake Blvd E, Seattle, WA 98112 USA.
EM brian.burke@noaa.gov
FU Bonneville Power Administration
FX Chinook salmon catch data were obtained during a survey funded by the
Bonneville Power Administration. Many people assisted with the project
organization and data collection, including but not limited to Ed
Casillas, Bill Peterson, Ric Brodeur, Bob Emmett, Kym Jacobson, Cheryl
Morgan, Jen Zamon, Brian Beckman, Laurie Weitkamp, Don Van Doornik,
David Kuligowski, Tom Wainwright, Joe Fisher, Susan Hinton, and Cindy
Bucher. Andre Punt contributed to the initial design of the model. We
also thank JoAnne Butzerin, James Faulkner, Bridget Ferris, Mark
Scheuerell, Rich Zabel, Aimee Fullerton, and two anonymous reviewers for
their constructive comments on earlier versions of this manuscript.
NR 58
TC 17
Z9 17
U1 1
U2 45
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA
SN 0706-652X
EI 1205-7533
J9 CAN J FISH AQUAT SCI
JI Can. J. Fish. Aquat. Sci.
PD AUG
PY 2013
VL 70
IS 8
BP 1167
EP 1177
DI 10.1139/cjfas-2012-0505
PG 11
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 193AF
UT WOS:000322528400006
ER
PT J
AU Trainer, MG
AF Trainer, Melissa G.
TI Atmospheric Prebiotic Chemistry and Organic Hazes
SO CURRENT ORGANIC CHEMISTRY
LA English
DT Article
DE Amino acid formation; Abiotic synthesis; Chemical evolution; Early earth
atmosphere; Organic haze; Prebiotic chemistry; Primitive earth
ID EARTHS EARLY ATMOSPHERE; CROSS-SECTION MEASUREMENTS; TITANS
UPPER-ATMOSPHERE; SPARK DISCHARGE EXPERIMENT; NEUTRAL MASS-SPECTROMETER;
MULTIPLE SULFUR ISOTOPES; CITY HYDROTHERMAL FIELD; AMINO-ACIDS;
TEMPERATURE-DEPENDENCE; ARCHEAN ATMOSPHERE
AB Earth's atmospheric composition at the time of the origin of life is not known, but it has often been suggested that chemical transformation of reactive species in the atmosphere was a significant source of prebiotic organic molecules. Experimental and theoretical studies over the past half century have shown that atmospheric synthesis can yield molecules such as amino acids and nucleobases, but these processes are very sensitive to gas composition and energy source. Abiotic synthesis of organic molecules is more productive in reduced atmospheres, yet the primitive Earth may not have been as reducing as earlier workers assumed, and recent research has reflected this shift in thinking. This work provides a survey of the range of chemical products that can be produced given a set of atmospheric conditions, with a particular focus on recent reports. Intertwined with the discussion of atmospheric synthesis is the consideration of an organic haze layer, which has been suggested as a possible ultraviolet shield on the anoxic early Earth. Since such a haze layer - if formed - would serve as a reservoir for organic molecules, the chemical composition of the aerosol should be closely examined. The results highlighted here show that a variety of products can be formed in mildly reducing or even neutral atmospheres, demonstrating that contributions of atmospheric synthesis to the organic inventory on early Earth should not be discounted. This review intends to bridge current knowledge of the range of possible atmospheric conditions in the prebiotic environment and pathways for synthesis under such conditions by examining the possible products of organic chemistry in the early atmosphere.
C1 NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA.
RP Trainer, MG (reprint author), NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Code 699, Greenbelt, MD 20771 USA.
EM melissa.trainer@nasa.gov
RI Trainer, Melissa/E-1477-2012
NR 167
TC 9
Z9 9
U1 5
U2 86
PU BENTHAM SCIENCE PUBL LTD
PI SHARJAH
PA EXECUTIVE STE Y-2, PO BOX 7917, SAIF ZONE, 1200 BR SHARJAH, U ARAB
EMIRATES
SN 1385-2728
EI 1875-5348
J9 CURR ORG CHEM
JI Curr. Org. Chem.
PD AUG
PY 2013
VL 17
IS 16
BP 1710
EP 1723
PG 14
WC Chemistry, Organic
SC Chemistry
GA 192XX
UT WOS:000322522400004
ER
PT J
AU Arumugam, DD
Ricketts, DS
AF Arumugam, D. D.
Ricketts, D. S.
TI Passive orientation measurement using magnetoquasistatic fields and
coupled magnetic resonances
SO ELECTRONICS LETTERS
LA English
DT Article
ID POSITION MEASUREMENT
AB A passive position orientation measurement method is presented which leverages the spatial variation of the reflected magnetoquasistatic field from a mobile loop to determine the loop's spatial orientation. The azimuthal orientation was measured from 0 degrees to 360 degrees at a distance of 1 m from the fixed measurement loop. Inverting the theoretical expressions to estimate orientation from measured field values resulted in an average and RMS error of 3.15 degrees and 4.55 degrees, respectively. This technique offers a means to accurately determine the orientation of the mobile loop through purely passive methods.
C1 [Arumugam, D. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ricketts, D. S.] N Carolina State Univ, Raleigh, NC 27695 USA.
RP Arumugam, DD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM darmindra.d.arumugam@jpl.nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 2
PU INST ENGINEERING TECHNOLOGY-IET
PI HERTFORD
PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND
SN 0013-5194
J9 ELECTRON LETT
JI Electron. Lett.
PD AUG 1
PY 2013
VL 49
IS 16
BP 999
EP 1000
DI 10.1049/el.2013.0766
PG 2
WC Engineering, Electrical & Electronic
SC Engineering
GA 195OG
UT WOS:000322712100019
ER
PT J
AU Xu, KM
Cheng, AN
AF Xu, Kuan-Man
Cheng, Anning
TI Evaluating Low-Cloud Simulation from an Upgraded Multiscale Modeling
Framework Model. Part I: Sensitivity to Spatial Resolution and
Climatology
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Climatology; Climate models; Cloud resolving models; General circulation
models; Model evaluation; performance; Multigrid models
ID BOUNDARY-LAYER CLOUDS; 3RD-ORDER TURBULENCE CLOSURES; SOUTHEAST PACIFIC;
RESOLVING MODEL; CONVECTION PARAMETERIZATION; STRATOCUMULUS CLOUDS;
PROJECT GPCP; PRECIPITATION; CUMULUS; SYSTEM
AB The multiscale modeling framework, which replaces traditional cloud parameterizations with a 2D cloud-resolving model (CRM) in each atmospheric column, is a promising approach to climate modeling. The CRM component contains an advanced third-order turbulence closure, helping it to better simulate low-level clouds. In this study, two simulations are performed with 1.9 degrees x 2.5 degrees grid spacing but they differ in the vertical resolution. The number of model layers below 700 hPa increases from 6 in one simulation (IP-6L) to 12 in another (IP-12L) to better resolve the boundary layer. The low-cloud horizontal distribution and vertical structures in IP-12L are more realistic and its global mean is higher than in IP-6L and closer to that of CloudSat/Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) observations. The spatial patterns of tropical precipitation are significantly improved; for example, a single intertropical convergence zone (ITCZ) in the Pacific, instead of double ITCZs in an earlier study that used coarser horizontal resolution and a different dynamical core in its host general circulation model (GCM), and the intensity of the South Pacific convergence zone (SPCZ), and the ITCZ in the Atlantic is more realistic. Many aspects of the global seasonal climatology agree well with observations except for excessive precipitation in the tropics. In terms of spatial correlations and patterns in the tropical/subtropical regions, most surface/vertically integrated properties show greater improvement over the earlier simulation than that with lower vertical resolution. The relationships between low-cloud amount and several large-scale properties are consistent with those observed in five low-cloud regions. There is an imbalance in the surface energy budget, which is an aspect of the model that needs to be improved in the future.
C1 [Xu, Kuan-Man; Cheng, Anning] NASA Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Cheng, Anning] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Xu, KM (reprint author), NASA Langley Res Ctr, Climate Sci Branch, Mail Stop 420, Hampton, VA 23681 USA.
EM kuan-man.xu@nasa.gov
RI Xu, Kuan-Man/B-7557-2013
OI Xu, Kuan-Man/0000-0001-7851-2629
FU NASA Modeling, Analysis, and Prediction program; DOE Atmospheric System
Research Program [DE-SC0005450]; NSF Science and Technology Center for
Multiscale Modeling of Atmospheric Processes (CMMAP); Colorado State
University [ATM-0425247]
FX This work has been supported by NASA Modeling, Analysis, and Prediction
program managed by Dr. David Considine. This work was also partially
supported by DOE Atmospheric System Research Program under Interagency
Agreement DE-SC0005450 and NSF Science and Technology Center for
Multiscale Modeling of Atmospheric Processes (CMMAP), managed by
Colorado State University under Cooperative Agreement ATM-0425247. The
computation resources from NCAR BlueGene supercomputer were provided by
the Teragrid organization. Special thanks go to Marat Khairoutdinov of
Stony Brook University for providing SPCAM, Seiji Kato for providing the
C3M data and EBAF-surface data, Drs. Zach Eitzen and Yunyan Zhang for
reading an earlier version of the manuscript, and two anonymous
reviewers for their valuable comments. The C3M data and CERES EBAF
version 2.6 data were obtained from the NASA Langley Research Center
CERES ordering tool (http://ceres.larc.nasa.gov/). The GPCP data are
downloaded from http://www.esrl.noaa.gov/psd/ maintained by
NOAA/OAR/ESRL PSD, Boulder, CO.
NR 55
TC 20
Z9 20
U1 2
U2 30
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 AUG
PY 2013
VL 26
IS 16
BP 5717
EP 5740
DI 10.1175/JCLI-D-12-00200.1
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 196FU
UT WOS:000322759700001
ER
PT J
AU Xu, KM
Cheng, AN
AF Xu, Kuan-Man
Cheng, Anning
TI Evaluating Low-Cloud Simulation from an Upgraded Multiscale Modeling
Framework Model. Part II: Seasonal Variations over the Eastern Pacific
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Clouds; Climate models; Cloud resolving models; Model evaluation;
performance; Numerical analysis; modeling; Subgrid-scale processes
ID SEA-SURFACE TEMPERATURE; BOUNDARY-LAYER CLOUDS; 3RD-ORDER TURBULENCE
CLOSURES; CLIMATOLOGY PROJECT GPCP; OCEAN-ATMOSPHERE MODEL; SOUTHEAST
PACIFIC; STRATOCUMULUS CLOUDS; RESOLVING MODEL; COUPLED OCEAN;
VOCALS-REX
AB The eastern Pacific is a climatologically important region. Conventional coupled atmosphere-ocean general circulation models produce positive sea surface temperature biases of 2-5 K in this region because of insufficient stratocumulus clouds. In this study, a global multiscale modeling framework (MMF), which replaces traditional cloud parameterizations with a 2D cloud-resolving model (CRM) in each atmospheric column, is used to examine the seasonal variations of this Pacific region. The CRM component contains an advanced third-order turbulence closure, helping it to better simulate boundary layer turbulence and low-level clouds. Compared to available satellite observations of cloud amount, liquid water path, cloud radiative effects, and precipitation, this MMF produces realistic seasonal variations of the eastern Pacific region, although there are some disagreements in the exact location of maximum cloudiness centers in the Peruvian region and the intensity of ITCZ precipitation. Analyses of profile- and subcloud-based decoupling measures reveal very small amplitudes of seasonal variations in the decoupling strength in the subtropics except for those regions off the subtropical coasts where the decoupling measures suggest that the boundary layers should be well coupled in all four seasons. In the Peruvian and Californian regions, the seasonal variations of low clouds are related to those in the boundary layer height and the strength of inversion. Factors that influence the boundary layer and the inversion, such as solar incident radiation, subcloud-layer turbulent mixing, and large-scale subsidence, can collectively explain the seasonal variations of low clouds rather than the deepening-warming mechanism of Bretherton and Wyant cited in earlier studies.
C1 [Xu, Kuan-Man; Cheng, Anning] NASA Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Cheng, Anning] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Xu, KM (reprint author), NASA Langley Res Ctr, Climate Sci Branch, Mail Stop 420, Hampton, VA 23681 USA.
EM kuan-man.xu@nasa.gov
RI Xu, Kuan-Man/B-7557-2013
OI Xu, Kuan-Man/0000-0001-7851-2629
FU NASA Modeling, Analysis, and Prediction program; DOE Atmospheric System
Research Program [DE-SC0005450]; NSF Science and Technology Center for
Multiscale Modeling of Atmospheric Processes (CMMAP); Colorado State
University [ATM-0425247]
FX This work has been supported by NASA Modeling, Analysis, and Prediction
program managed by Dr. David Considine. This work was also partially
supported by the DOE Atmospheric System Research Program under
Interagency Agreement DE-SC0005450 and NSF Science and Technology Center
for Multiscale Modeling of Atmospheric Processes (CMMAP), managed by
Colorado State University under Cooperative Agreement ATM-0425247. The
computation resources from NCAR BlueGene supercomputer were provided by
the Teragrid organization. Special thanks go to Marat Khairoutdinov of
Stony Brook University for providing SPCAM, Seiji Kato for providing the
C3M data and EBAF-surface data, Dr. Zach Eitzen for reading this
manuscript, and two anonymous reviewers for their valuable comments. The
C3M data and CERES EBAF version 2.6 data were obtained from the NASA
Langley Research Center CERES ordering tool at
http://ceres.larc.nasa.gov/. The GPCP data are downloaded from
http://www.esrl.noaa.gov/psd/ maintained by NOAA/OAR/ESRL PSD, Boulder,
CO.
NR 50
TC 18
Z9 18
U1 0
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 AUG
PY 2013
VL 26
IS 16
BP 5741
EP 5760
DI 10.1175/JCLI-D-12-00276.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 196FU
UT WOS:000322759700002
ER
PT J
AU Cheng, AN
Xu, KM
AF Cheng, Anning
Xu, Kuan-Man
TI Evaluating Low-Cloud Simulation from an Upgraded Multiscale Modeling
Framework Model. Part III: Tropical and Subtropical Cloud Transitions
over the Northern Pacific
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Boundary layer; Climate variability; Climate models; Cloud
parameterizations; Model evaluation; performance; Seasonal variability
ID COMMUNITY ATMOSPHERE MODEL; MARINE BOUNDARY-LAYER; 3RD-ORDER TURBULENCE
CLOSURES; ASTEX LAGRANGIAN EXPERIMENTS; SOUTHEAST PACIFIC; RESOLVING
MODEL; CLIMATE SIMULATIONS; LOWER TROPOSPHERE; VERSION 3;
PARAMETERIZATION
AB An analysis of simulated cloud regime transitions along a transect from the subtropical California coast to the tropics for the northern summer season (June-August) is presented in this study. The Community Atmosphere Model, version 5 (CAM5), superparameterized CAM (SPCAM), and an upgraded SPCAM with intermediately prognostic higher-order closure (SPCAM-IPHOC) are used to perform global simulations by imposing climatological sea surface temperature and sea ice distributions. The seasonal-mean properties are compared with recent observations of clouds, radiation, and precipitation and with multimodel intercomparison results. There are qualitative agreements in the characteristics of cloud regimes along the transect among the three models. CAM5 simulates precipitation and shortwave radiative fluxes well but the stratocumulus-to-cumulus transition occurs too close to the coast of California. SPCAM-IPHOC simulates longwave radiative fluxes and precipitable water well, but with systematic biases in shortwave radiative fluxes. The broad, stronger ascending band in SPCAM is related to the large biases in the convective region but the characteristics of the stratocumulus region are still more realistic and the transition occurs slightly farther away from the coast than in CAM5. Even though SPCAM-IPHOC produces the most realistic seasonal-mean transition, it underestimates the mean gradient in low-cloud cover (LCC) across the mean transition location because of an overestimate of LCC in the transition and convective regions that shifts the transition locations farther from the coast. Analysis of two decoupling measures shows consistency in the mean location and the histogram of decoupling locations with those of LCC transition. CAM5, however, lacks such a consistency, suggesting a need for further refinement of its boundary layer cloud parameterization.
C1 [Cheng, Anning; Xu, Kuan-Man] NASA Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Cheng, Anning] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Xu, KM (reprint author), NASA Langley Res Ctr, Climate Sci Branch, Mail Stop 420, Hampton, VA 23681 USA.
EM kuan-man.xu@nasa.gov
RI Xu, Kuan-Man/B-7557-2013
OI Xu, Kuan-Man/0000-0001-7851-2629
FU NASA Modeling, Analysis and Prediction program; U.S. Department of
Energy (DOE) Atmospheric System Research Program [DE-SC0005450]; NSF
Science and Technology Center for Multiscale Modeling of Atmospheric
Processes (CMMAP); Colorado State University [ATM-0425247]
FX This work has been supported by NASA Modeling, Analysis and Prediction
program managed by Dr. David Considine. This work was also partially
supported by the U.S. Department of Energy (DOE) Atmospheric System
Research Program under Interagency agreement DE-SC0005450 and NSF
Science and Technology Center for Multiscale Modeling of Atmospheric
Processes (CMMAP), managed by Colorado State University under
cooperative agreement ATM-0425247. The computation resources from NCAR
BlueGene supercomputer were provided by the Teragrid organization.
Special thanks go to Marat Khairoutdinov of Stony Brook University for
providing SPCAM, Seiji Kato for providing the C3M data and EBAF-surface
data, Dr. Zach Eitzen for reading this manuscript, and four anonymous
reviewers for their valuable comments. The C3M data and CERES EBAF
version 2.6 data were obtained from the NASA Langley Research Center
CERES ordering tool at http://ceres.larc.nasa.gov. The GPCP data are
downloaded from http://www.esrl.noaa.gov/psd/ maintained by
NOAA/OAR/ESRL PSD, Boulder, CO.
NR 58
TC 14
Z9 14
U1 0
U2 14
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 AUG
PY 2013
VL 26
IS 16
BP 5761
EP 5781
DI 10.1175/JCLI-D-12-00650.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 196FU
UT WOS:000322759700003
ER
PT J
AU Lee, T
Waliser, DE
Li, JLF
Landerer, FW
Gierach, MM
AF Lee, Tong
Waliser, Duane E.
Li, Jui-Lin F.
Landerer, Felix W.
Gierach, Michelle M.
TI Evaluation of CMIP3 and CMIP5 Wind Stress Climatology Using Satellite
Measurements and Atmospheric Reanalysis Products
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Fluxes; Atmosphere-ocean interaction; Sea level; Wind; Model evaluation;
performance; Seasonal cycle
ID OCEAN CIRCULATION; EL-NINO; TROPICAL PACIFIC; MODELS; VARIABILITY; ENSO;
SIMULATIONS; TEMPERATURE; PERFORMANCE; ANOMALIES
AB Wind stress measurements from the Quick Scatterometer (QuikSCAT) satellite and two atmospheric reanalysis products are used to evaluate the annual mean and seasonal cycle of wind stress simulated by phases 3 and 5 of the Coupled Model Intercomparison Project (CMIP3 and CMIP5). The ensemble CMIP3 and CMIP5 wind stresses are very similar to each other. Generally speaking, there is no significant improvement of CMIP5 over CMIP3. The CMIP ensemble-average zonal wind stress has eastward biases at midlatitude westerly wind regions (30 degrees-50 degrees N and 30 degrees-50 degrees S, with CMIP being too strong by as much as 55%), westward biases in subtropical-tropical easterly wind regions (15 degrees-25 degrees N and 15 degrees-25 degrees S), and westward biases at high-latitude regions (poleward of 55 degrees S and 55 degrees N). These biases correspond to too strong anticyclonic (cyclonic) wind stress curl over the subtropical (subpolar) ocean gyres, which would strengthen these gyres and influence oceanic meridional heat transport. In the equatorial zone, significant biases of CMIP wind exist in individual basins. In the equatorial Atlantic and Indian Oceans, CMIP ensemble zonal wind stresses are too weak and result in too small of an east-west gradient of sea level. In the equatorial Pacific Ocean, CMIP zonal wind stresses are too weak in the central and too strong in the western Pacific. These biases have important implications for the simulation of various modes of climate variability originating in the tropics. The CMIP as a whole overestimate the magnitude of seasonal variability by almost 50% when averaged over the entire global ocean. The biased wind stress climatologies in CMIP not only have implications for the simulated ocean circulation and climate variability but other air-sea fluxes as well.
C1 [Lee, Tong; Waliser, Duane E.; Li, Jui-Lin F.; Landerer, Felix W.; Gierach, Michelle M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lee, T (reprint author), CALTECH, Jet Prop Lab, MS300 323, Pasadena, CA 91109 USA.
EM tong.lee@jpl.nasa.gov
OI Gierach, Michelle/0000-0002-8161-4121; Landerer,
Felix/0000-0003-2678-095X
FU National Aeronautics and Space Administration
FX We acknowledge the GCM modeling groups, the Program for Climate Model
Diagnosis and Intercomparison (PCMDI), and the WCRP's Working Group on
Coupled Modeling for their roles in making available the WCRP CMIP3 and
CMIP5 multimodel datasets. Support of these data sets is provided by the
Office of Science, U.S. Department of Energy. This research was carried
out in part at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 51
TC 25
Z9 25
U1 1
U2 34
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 AUG
PY 2013
VL 26
IS 16
BP 5810
EP 5826
DI 10.1175/JCLI-D-12-00591.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 196FU
UT WOS:000322759700005
ER
PT J
AU Booth, JF
Naud, CM
Del Genio, AD
AF Booth, James F.
Naud, Catherine M.
Del Genio, Anthony D.
TI Diagnosing Warm Frontal Cloud Formation in a GCM: A Novel Approach Using
Conditional Subsetting
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Extratropical cyclones; Fronts; Clouds; Cloud tracking; cloud motion
winds; Climate models; Model evaluation; performance
ID MIDLATITUDE CYCLONES; PRECIPITATION; MODEL; CLIMATE; RADIATION;
PARAMETERIZATION; SIMULATION; NORTHERN; ENERGY; STORMS
AB This study analyzes characteristics of clouds and vertical motion across extratropical cyclone warm fronts in the NASA Goddard Institute for Space Studies general circulation model. The validity of the modeled clouds is assessed using a combination of satellite observations from CloudSat, Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO), Advanced Microwave Scanning Radiometer for Earth Observing System (AMSR-E), and the NASA Modern-Era Retrospective Analysis for Research and Applications (MERRA) reanalysis. The analysis focuses on developing cyclones, to test the model's ability to generate their initial structure. To begin, the extratropical cyclones and their warm fronts are objectively identified and cyclone-local fields are mapped into a vertical transect centered on the surface warm front. To further isolate specific physics, the cyclones are separated using conditional subsetting based on additional cyclone-local variables, and the differences between the subset means are analyzed. Conditional subsets are created based on 1) the transect clouds and 2) vertical motion; 3) the strength of the temperature gradient along the warm front, as well as the storm-local 4) wind speed and 5) precipitable water (PW). The analysis shows that the model does not generate enough frontal cloud, especially at low altitude. The subsetting results reveal that, compared to the observations, the model exhibits a decoupling between cloud formation at high and low altitudes across warm fronts and a weak sensitivity to moisture. These issues are caused in part by the parameterized convection and assumptions in the stratiform cloud scheme that are valid in the subtropics. On the other hand, the model generates proper covariability of low-altitude vertical motion and cloud at the warm front and a joint dependence of cloudiness on wind and PW.
C1 [Booth, James F.; Del Genio, Anthony D.] NASA Goddard Inst Space Studies, New York, NY USA.
[Booth, James F.; Naud, Catherine M.] Columbia Univ, New York, NY USA.
RP Booth, JF (reprint author), NASA GISS, 2880 Broadway, New York, NY 10025 USA.
EM jbooth.atmos@gmail.com
FU NASA Postdoctoral Program; NASA Modeling and Analysis Program; NASA
CloudSat-CALIPSO missions; NASA Terra-Aqua [NNX11AH22G]; NASA CloudSat
Science Team [NNX10AM20G]
FX This research was supported by the NASA Postdoctoral Program, the NASA
Modeling and Analysis Program, and the NASA CloudSat-CALIPSO missions.
CN was supported by the NASA Terra-Aqua Grant NNX11AH22G and the NASA
CloudSat Science Team Grant NNX10AM20G. Resources supporting this work
were provided by the NASA High-End Computing (HEC) Program through the
NASA Center for Climate Simulation (NCCS) at Goddard Space Flight
Center. AMSR-E data were obtained from the National Snow and Ice Data
Center and GEOPROF-lidar files were obtained from the CloudSat data
processing center. MERRA outputs were obtained from the Goddard Earth
Sciences Data and Information Services Center. The authors thank the
reviewers for suggestions that improved the presentation of this work.
The authors thank Mike Bauer for providing his cyclone tracking
algorithm and Maxwell Kelley and Yonghua Chen for help with the GISS
GCM.
NR 44
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Z9 9
U1 1
U2 10
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 AUG
PY 2013
VL 26
IS 16
BP 5827
EP 5845
DI 10.1175/JCLI-D-12-00637.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 196FU
UT WOS:000322759700006
ER
PT J
AU Nagao, TM
Suzuki, K
Nakajima, TY
AF Nagao, Takashi M.
Suzuki, Kentaroh
Nakajima, Takashi Y.
TI Interpretation of Multiwavelength-Retrieved Droplet Effective Radii for
Warm Water Clouds in Terms of In-Cloud Vertical Inhomogeneity by Using a
Spectral Bin Microphysics Cloud Model
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Cloud microphysics; Optical properties; Cloud retrieval; Satellite
observations
ID SOLAR-RADIATION MEASUREMENTS; EFFECTIVE PARTICLE RADIUS;
OPTICAL-THICKNESS; PRECIPITATION FORMATION; SATELLITE RETRIEVALS;
ENSEMBLE MODEL; SCATTERING; GROWTH; REFLECTANCE; ALGORITHMS
AB This study examines the impact of in-cloud vertical inhomogeneity on cloud droplet effective radii (CDERs) of water-phase cloud retrieved from 1.6-, 2.1-, and 3.7-m-band measurements (denoted by r(1.6), r(2.1), and r(3.7), respectively). Discrepancies between r(1.6), r(2.1), and r(3.7) due to in-cloud vertical inhomogeneity are simulated by using a spectral bin microphysics cloud model and one-dimensional (1D) remote sensing simulator under assumptions that cloud properties at the subpixel scale have horizontal homogeneity and 3D radiative transfer effects can be ignored. Two-dimensional weighting functions for the retrieved CDERs with respect to cloud optical depth and droplet size are introduced and estimated by least squares fitting to the relation between the model-simulated droplet size distribution functions and the retrieved CDERs. The results show that the 2D weighting functions can explain CDER discrepancies due to in-cloud vertical inhomogeneity and size spectrum characteristics. The difference between r(1.6) and r(2.1) is found to primarily depend on the vertical difference in droplet size distribution because the peak widths of their weighting functions differ in terms of cloud optical depth. The difference between r(3.7) and r(2.1), in contrast, is highly dependent on r(2.1) because the magnitude of its weighting function is always greater than that of r(3.7) over the entire range of optical depths and droplet sizes, except for the cloud top. The overestimation of retrieved CDER compared with in situ CDER in a typical adiabatic cloud case is also interpreted in terms of in-cloud vertical inhomogeneity based on the 2D weighting functions and simulation results.
C1 [Nagao, Takashi M.; Nakajima, Takashi Y.] Tokai Univ, Res & Informat Ctr, Tokyo 1510063, Japan.
[Suzuki, Kentaroh] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Nagao, TM (reprint author), Tokai Univ, Res & Informat Ctr, Shibuya Ku, 2-28-4 Tomigaya, Tokyo 1510063, Japan.
EM takashi.m.nagao@tokai-u.jp
RI Suzuki, Kentaroh/C-3624-2011; Nakajima, Takashi/C-2747-2009
FU Earth Cloud, Aerosol and Radiation Explorer (EarthCARE) Science Project
of the Japan Aerospace Exploration Agency (JAXA); Global Change
Observation Mission-Carbon Cycle (GCOM-C) Science Project of the Japan
Aerospace Exploration Agency (JAXA); Greenhouse Gases Observing
Satellite (GOSAT) Science Project of the National Institute of
Environmental Studies (NIES), Tsukuba, Japan; Japan Science and
Technology Agency (JST); Ministry of Education, Culture, Sports, Science
and Technology (MEXT), Japan [22340133]; National Aeronautics and Space
Administration; CREST
FX This work was supported by the Earth Cloud, Aerosol and Radiation
Explorer (EarthCARE) and Global Change Observation Mission-Carbon Cycle
(GCOM-C) Science Project of the Japan Aerospace Exploration Agency
(JAXA) and the Greenhouse Gases Observing Satellite (GOSAT) Science
Project of the National Institute of Environmental Studies (NIES),
Tsukuba, Japan. This work was also partly supported in part by the Japan
Science and Technology Agency (JST), CREST, and the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), Japan,
through a Grant-in-Aid for Scientific Research (B) (22340133). 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 5
Z9 5
U1 2
U2 13
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 AUG
PY 2013
VL 70
IS 8
BP 2376
EP 2392
DI 10.1175/JAS-D-12-0225.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 195RK
UT WOS:000322721100003
ER
PT J
AU Painemal, D
Minnis, P
O'Neill, L
AF Painemal, David
Minnis, Patrick
O'Neill, Larry
TI The Diurnal Cycle of Cloud-Top Height and Cloud Cover over the
Southeastern Pacific as Observed by GOES-10
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Cloud cover; Cloud retrieval; Remote sensing; Diurnal effects
ID SEA-SURFACE TEMPERATURE; VOCALS-REX; BOUNDARY-LAYER; STRATOCUMULUS
CLOUDS; SATELLITE MEASUREMENTS; MARINE STRATOCUMULUS; LOWER TROPOSPHERE;
MODEL; OCEAN; ATMOSPHERE
AB The diurnal cycles in cloud-top height H-top and cloud fraction (CF) in the southeastern Pacific stratocumulus region were determined for October-November 2008 by analyzing data from Geostationary Operational Environmental Satellite-10 (GOES-10) according to a diurnal/semidiurnal harmonic fitting technique. The value of H-top was obtained by applying a formula based on a linear regression of the differences between GOES-10 cloud-top temperature and Tropical Rainfall Measuring Mission (TRMM) Microwave Imager (TMI) satellite sea surface temperature, with a common 0.25 degrees x 0.25 degrees spatial resolution. A satellite liquid water path (LWP) climatology complemented this dataset.
Southwestward transects of H-top and LWP anomalies reveal a coherent propagating signal from the coast in the afternoon, with a typical phase speed of 25 m s(-1). This pattern is preceded by a subsidence wave that reaches its peak a few hours before the maximum in H-top and LWP anomalies. Coincident increases in LWP and H-top after the subsidence wave passes suggest that the boundary layer deepening promotes cloud thickening and increased LWP, which are likely maintained through a well-mixed boundary layer and sufficient moisture fluxes that can counteract the effect of dry air entrainment. The interference between the radiatively and subsidence wave-driven cycles gives rise to a semidiurnal cycle in H-top along the coast. While the semidiurnal amplitude is near 80 m close to the coast with a fraction of explained variance greater than 0.4, it decreases to 30 m offshore (80 degrees W). Similar to H-top, CF also exhibits contrasting zonal differences, but with a smaller semidiurnal component. The phase of the semidiurnal harmonic resembles the subsidence propagation westward, and the noticeable land-sea breeze circulation at 26 degrees S that extends 200 km offshore.
C1 [Painemal, David; Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[O'Neill, Larry] Oregon State Univ, Coll Earth & 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 NASA Langley Research Center; NASA
Modeling, Analysis, and Prediction Program; NASA CERES Program; U.S.
Department of Energy's Atmospheric Science Program Atmospheric System
Research Interagency [DE-SC0000991/003]; NASA's Ocean Vector Winds
Science Team [NNX11AF31G]; institutional fellowship through Oregon State
University
FX D. Painemal is supported by the NASA Postdoctoral Program at NASA
Langley Research Center, administered by Oak Ridge Associated
Universities (ORAU). P. Minnis is 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 is supported by Grant
NNX11AF31G through NASA's Ocean Vector Winds Science Team and an
institutional fellowship through Oregon State University. The comments
and suggestions of three anonymous reviewers are greatly acknowledged.
NR 42
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Z9 11
U1 0
U2 14
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 AUG
PY 2013
VL 70
IS 8
BP 2393
EP 2408
DI 10.1175/JAS-D-12-0325.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 195RK
UT WOS:000322721100004
ER
PT J
AU Jiang, X
Wang, JQ
Olsen, ET
Pagano, T
Chen, LL
Yung, YL
AF Jiang, Xun
Wang, Jingqian
Olsen, Edward T.
Pagano, Thomas
Chen, Luke L.
Yung, Yuk L.
TI Influence of Stratospheric Sudden Warming on AIRS Midtropospheric CO2
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Stratospheric circulation; Air pollution
ID ATMOSPHERIC INFRARED SOUNDER; NINO SOUTHERN OSCILLATION; CARBON-DIOXIDE;
INTERANNUAL VARIABILITY; NORTHERN-HEMISPHERE; EL-NINO; PART I;
EXTRATROPICAL OZONE; MAUNA-LOA; CLIMATE
AB Midtropospheric CO2 retrievals from the Atmospheric Infrared Sounder (AIRS) were used to explore the influence of stratospheric sudden warming (SSW) on CO2 in the middle to upper troposphere. To choose the SSW events that had strong coupling between the stratosphere and troposphere, the authors applied a principal component analysis to the NCEP/Department of Energy Global Reanalysis 2 (NCEP-2) geopotential height data at 17 pressure levels. Two events (April 2003 and March 2005) that have strong couplings between the stratosphere and troposphere were chosen to investigate the influence of SSW on AIRS midtropospheric CO2. The authors investigated the temporal and spatial variations of AIRS midtropospheric CO2 before and after the SSW events and found that the midtropospheric CO2 concentrations increased by 2-3 ppm within a few days after the SSW events. These results can be used to better understand how the chemical tracers respond to the large-scale dynamics in the high latitudes.
C1 [Jiang, Xun; Wang, Jingqian] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77004 USA.
[Olsen, Edward T.; Pagano, Thomas; Chen, Luke L.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA USA.
[Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Jiang, X (reprint author), Univ Houston, Dept Earth & Atmospher Sci, 4800 Calhoun Rd, Houston, TX 77004 USA.
EM xjiang7@uh.edu
FU JPL Grant [G99694]; OCO-2 project; National Aeronautics and Space
Administration
FX We thank M. Chahine, Q. Li, two anonymous reviewers, and the editor for
helpful comments. X. Jiang was supported by JPL Grant G99694. YLY was
supported by the OCO-2 project. 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 53
TC 4
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U1 0
U2 15
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD AUG
PY 2013
VL 70
IS 8
BP 2566
EP 2573
DI 10.1175/JAS-D-13-064.1
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 195RK
UT WOS:000322721100014
ER
PT J
AU Etiope, G
Vance, S
Christensen, LE
Marques, JM
da Costa, IR
AF Etiope, Giuseppe
Vance, Steve
Christensen, Lance E.
Marques, Jose M.
da Costa, Isabel Ribeiro
TI Methane in serpentinized ultramafic rocks in mainland Portugal
SO MARINE AND PETROLEUM GEOLOGY
LA English
DT Article
DE Methane; Serpentinization; Peridotites; Hyperalkaline waters; Igneous
reservoir rocks
ID HIGH-PH; OPHIOLITE; ALKANES; WATERS; GENOVA; DEEP
AB We report a new case of methane (CH4) of apparent abiotic origin in continental serpentinized ultramafic rocks. Multiple analytical techniques, on-site and in the laboratory, revealed methane and ethane degassing from hyperalkaline (pH > 11) Ca2+-OH- mineral waters in boreholes drilled in the Alter-do-Chao igneous intrusion, at Cabeco de Vide, in mainland Portugal. The C and H isotopic composition of CH4 (delta C-13 similar to -20 parts per thousand; delta H-2: -283 parts per thousand) suggests a dominant abiotic origin, although minor thermogenic contributions cannot be excluded. Similarly, low methane-to-ethane ratios suggest a predominantly non-microbial source, consistent with previous microbiological data showing the lack of methanogenic archaea in these waters. Heavier hydrocarbons, CO2 and H-2 are below detection limits. This case study confirms that CH4 from serpentinized ultramafic rocks can be transported by hyperalkaline fluids linked to deep circulation of meteoric waters. Maximum depth of Cabeco de Vide serpentinized rocks is less than 1 km, and present temperatures are likely lower than 50 degrees C. Serpentinization and related gas formation may have occurred at any time during thermal evolution of the igneous intrusion, so gas formation temperature cannot be easily determined. This case is an opportunity to test thermometry provided by CH4 isotopologue analyses. The existence of methane in continental serpentinized igneous rocks is more widespread than previously thought and petroleum systems with similar serpentinized ultramafics in reservoir rocks may have traces of the observed C-13-enriched CH4. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Etiope, Giuseppe] Ist Nazl Geofis & Vulcanol, Seze Roma 2, I-00143 Rome, Italy.
[Etiope, Giuseppe] Univ Babes Bolyai, Fac Environm Sci & Engn, R-3400 Cluj Napoca, Romania.
[Vance, Steve; Christensen, Lance E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Marques, Jose M.] Univ Tecn Lisboa, Ctr Petrol & Geochem CEPGIST, P-1100 Lisbon, Portugal.
[Marques, Jose M.] Univ Tecn Lisboa, Ctr Nat Resources & Environm CERENA, Inst Super Tecn, P-1100 Lisbon, Portugal.
[da Costa, Isabel Ribeiro] Univ Lisbon, Fac Ciencias, Dept Geol, CREMINER LARSyS Lab Associado, P-1699 Lisbon, Portugal.
RP Etiope, G (reprint author), Ist Nazl Geofis & Vulcanol, Seze Roma 2, Via V Murata 605, I-00143 Rome, Italy.
EM etiope@ingv.it
RI Etiope, Giuseppe/H-3343-2011; Marques, Jose/A-6595-2012
OI Etiope, Giuseppe/0000-0001-8614-4221; Marques, Jose/0000-0002-1644-7195
FU Centre for Petrology and Geochemistry of Instituto Superior Tecnico,
Portugal [PEst-OE/CTE/UI0098/2011]; FCT [PTDC/AAG-MAA/2891/2012]; INGV
project; NASA; NASA ASTEP Program; NASA Astrobiology Program
FX This study was partially funded by the Strategic Project
(PEst-OE/CTE/UI0098/2011) of the Centre for Petrology and Geochemistry
of Instituto Superior Tecnico, Portugal, and by the FCT Project
PTDC/AAG-MAA/2891/2012. Laboratory molecular and isotopic analyses were
performed by INGV project funds related to the institutional "Specific
Objective 4.5 - Natural degassing and petroleum gases". Work performed
at the Jet Propulsion Laboratory, California Institute of Technology,
was done under contract with NASA and funded by NASA ASTEP and
Astrobiology Programs.
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0264-8172
J9 MAR PETROL GEOL
JI Mar. Pet. Geol.
PD AUG
PY 2013
VL 45
BP 12
EP 16
DI 10.1016/j.marpetgeo.2013.04.009
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 186PM
UT WOS:000322056600003
ER
PT J
AU Gerousis, C
Grepiotis, A
AF Gerousis, C.
Grepiotis, A.
TI Reconfigurable gate array architecture for logic functions in tunneling
transistor technology
SO MICROELECTRONICS JOURNAL
LA English
DT Article
DE Single-electron transistor (SET); Reconfigurable SET logic; Circuit
simulation
ID ROOM-TEMPERATURE OPERATION; SINGLE-ELECTRON; CIRCUITS; SIMULATION;
DESIGN
AB This work describes the design of a reconfigurable logic gate array composed of single-electron tunneling (SET) transistors currently under investigation as potential post-CMOS candidates for future nano-scale integrated circuits for use in low-power embedded systems. A layer in the proposed array consists of a SET summing-inverter block replicated in subsequent blocks and extended to implement flexible logic functions in terms of the sum-of-products (Sop) and products-of-sum (PoS) forms. The reconfiguring of the array can be accomplished through the alteration of a block's logic function by way of a control voltage. The reconfigurable array can work normally at room temperature and can flexibly realize functions with better performance at lower power compared with pure MOSFET circuits. (c) 2013 Elsevier Ltd. All rights reserved.
C1 [Gerousis, C.] Christopher Newport Univ, Dept Phys Comp Sci & Engn, Newport News, VA 23606 USA.
[Grepiotis, A.] NASA Langley Res, Sci Syst & Applicat SSAI, Hampton, VA 23666 USA.
RP Gerousis, C (reprint author), Christopher Newport Univ, Dept Phys Comp Sci & Engn, Newport News, VA 23606 USA.
EM gerousis@cnu.edu
RI Arumugam, Thirumagal/C-3408-2014
NR 20
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0026-2692
EI 1879-2391
J9 MICROELECTRON J
JI Microelectron. J.
PD AUG
PY 2013
VL 44
IS 8
BP 706
EP 711
DI 10.1016/j.mejo.2013.05.002
PG 6
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology
SC Engineering; Science & Technology - Other Topics
GA 191LU
UT WOS:000322415300010
ER
PT J
AU Pawar, DD
Kalamkar, M
Altamirano, D
Linares, M
Shanthi, K
Strohmayer, T
Bhattacharya, D
van der Klis, M
AF Pawar, Devraj D.
Kalamkar, Maithili
Altamirano, Diego
Linares, Manuel
Shanthi, K.
Strohmayer, Tod
Bhattacharya, Dipankar
van der Klis, Michiel
TI Discovery of twin kHz quasi-periodic oscillations in the low-mass X-ray
binary XTE J1701-407
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: general; stars: individual: XTE J1701-407; stars: neutron;
X-rays: binaries
ID ENERGY-DEPENDENT VARIABILITY; ACCRETING MILLISECOND PULSAR; PROPORTIONAL
COUNTER ARRAY; NEUTRON-STAR SYSTEM; ATOLL SOURCE STATES; 4U 1608-52;
TIMING FEATURES; INTEGRAL OBSERVATIONS; SPECTRAL BEHAVIOR; FREQUENCY
AB We report the discovery of kHz quasi-periodic oscillations (QPOs) in three Rossi X-ray Timing Explorer observations of the low-mass X-ray binary XTE J1701-407. In one of the observations we detect a kHz QPO with a characteristic frequency of 1153 +/- 5 Hz, while in the other two observations we detect twin QPOs at characteristic frequencies of 740 +/- 5, 1112 +/- 17 Hz and 740 +/- 11, 1098 +/- 5 Hz. All detections happen when XTE J1701-407 was in its high-intensity soft state, and their single-trial significance is in the 3.1-7.5 Sigma range. The frequency difference in the centroid frequencies of the twin kHz QPOs (385 +/- 13 Hz) is one of the largest seen till date. The 3-30 keV fractional rms amplitude of the upper kHz QPO varies between similar to 18 and similar to 30 per cent. XTE J1701-407, with a persistent luminosity close to 1 per cent of the Eddington limit, is among the small group of low-luminosity kHz QPO sources and has the highest rms for the upper kHz QPO detected in any source. The X-ray spectral and variability characteristics of this source indicate its atoll source nature.
C1 [Pawar, Devraj D.] Ramniranjan Jhunjhunwala Coll, Bombay 400086, Maharashtra, India.
[Kalamkar, Maithili; Altamirano, Diego; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Linares, Manuel] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Shanthi, K.] Univ Bombay, UGC Acad Staff Coll, Bombay 400098, Maharashtra, India.
[Strohmayer, Tod] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Bhattacharya, Dipankar] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
RP Pawar, DD (reprint author), Ramniranjan Jhunjhunwala Coll, Bombay 400086, Maharashtra, India.
EM devrajdp@gmail.com
RI Bhattacharya, Dipankar/J-6927-2015
OI Bhattacharya, Dipankar/0000-0003-3352-3142
FU IUCAA, Pune, India; University of Amsterdam, Netherlands
FX DP and KS thank IUCAA, Pune, India, and University of Amsterdam,
Netherlands, for their support and thank Ranjeev Misra and Gulab
Dewangan for discussions during their visits to IUCAA. This research has
made use of NASA's Astrophysics Data System. This research has made use
of data obtained through the High Energy Astrophysics Science Archive
Research Center Online Service, provided by the NASA/Goddard Space
Flight Center.
NR 70
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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 AUG
PY 2013
VL 433
IS 3
BP 2436
EP 2444
DI 10.1093/mnras/stt919
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 191HK
UT WOS:000322403800055
ER
PT J
AU Brightman, M
Silverman, JD
Mainieri, V
Ueda, Y
Schramm, M
Matsuoka, K
Nagao, T
Steinhardt, C
Kartaltepe, J
Sanders, DB
Treister, E
Shemmer, O
Brandt, WN
Brusa, M
Comastri, A
Ho, LC
Lanzuisi, G
Lusso, E
Nandra, K
Salvato, M
Zamorani, G
Akiyama, M
Alexander, DM
Bongiorno, A
Capak, P
Civano, F
Del Moro, A
Doi, A
Elvis, M
Hasinger, G
Laird, ES
Masters, D
Mignoli, M
Ohta, K
Schawinski, K
Taniguchi, Y
AF Brightman, M.
Silverman, J. D.
Mainieri, V.
Ueda, Y.
Schramm, M.
Matsuoka, K.
Nagao, T.
Steinhardt, C.
Kartaltepe, J.
Sanders, D. B.
Treister, E.
Shemmer, O.
Brandt, W. N.
Brusa, M.
Comastri, A.
Ho, L. C.
Lanzuisi, G.
Lusso, E.
Nandra, K.
Salvato, M.
Zamorani, G.
Akiyama, M.
Alexander, D. M.
Bongiorno, A.
Capak, P.
Civano, F.
Del Moro, A.
Doi, A.
Elvis, M.
Hasinger, G.
Laird, E. S.
Masters, D.
Mignoli, M.
Ohta, K.
Schawinski, K.
Taniguchi, Y.
TI A statistical relation between the X-ray spectral index and Eddington
ratio of active galactic nuclei in deep surveys
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion; accretion discs; galaxies: active; galaxies: nuclei; quasars:
emission lines; quasars: general; X-rays: galaxies
ID FIELD-SOUTH SURVEY; SEYFERT 1 GALAXIES; NEWTON QUASAR SURVEY; MS SOURCE
CATALOGS; BLACK-HOLE MASSES; COSMOS SURVEY; XMM-COSMOS; EMISSION-LINE;
DATA RELEASE; LUMINOSITY
AB We present an investigation into how well the properties of the accretion flow on to a supermassive black hole may be coupled to those of the overlying hot corona. To do so, we specifically measure the characteristic spectral index, Gamma, of a power-law energy distribution, over an energy range of 2-10 keV, for X-ray selected, broad-lined radio-quiet active galactic nuclei (AGN) up to z similar to 2 in Cosmic Evolution Survey (COSMOS) and Extended Chandra Deep Field South (E-CDF-S). We test the previously reported dependence between Gamma and black hole mass, full width at half-maximum (FWHM) and Eddington ratio using a sample of AGN covering a broad range in these parameters based on both the Mg ii and H alpha emission lines with the later afforded by recent near-infrared spectroscopic observations using Subaru/Fibre Multi Object Spectrograph. We calculate the Eddington ratios, lambda(Edd), for sources where a bolometric luminosity (L-Bol) has been presented in the literature, based on spectral energy distribution fitting, or, for sources where these data do not exist, we calculate L-Bol using a bolometric correction to the X-ray luminosity, derived from a relationship between the bolometric correction and L-X/L-3000. From a sample of 69 X-ray bright sources (> 250 counts), where Gamma can be measured with greatest precision, with an estimate of L-Bol, we find a statistically significant correlation between Gamma and lambda(Edd), which is highly significant with a chance probability of 6.59x 10(-8). A statistically significant correlation between Gamma and the FWHM of the optical lines is confirmed, but at lower significance than with lambda(Edd) indicating that lambda(Edd) is the key parameter driving conditions in the corona. Linear regression analysis reveals that Gamma = (0.32 +/- 0.05) log(10)lambda(Edd) + (2.27 +/- 0.06) and Gamma = (-0.69 +/- 0.11) log(10)(FWHM/km s(-1)) + (4.44 +/- 0.42). Our results on Gamma-lambda(Edd) are in very good agreement with previous results. While the Gamma-lambda(Edd) relationship means that X-ray spectroscopy may be used to estimate black hole accretion rate, considerable dispersion in the correlation does not make this viable for single sources, however could be valuable for large X-ray spectral samples, such as those to be produced by eROSITA.
C1 [Brightman, M.; Brusa, M.; Lanzuisi, G.; Nandra, K.; Salvato, M.; Bongiorno, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Silverman, J. D.; Schramm, M.; Steinhardt, C.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Chiba 2778583, Japan.
[Mainieri, V.] European So Observ, D-85748 Garching, Germany.
[Ueda, Y.; Nagao, T.; Ohta, K.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Matsuoka, K.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea.
[Matsuoka, K.; Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan.
[Nagao, T.] Kyoto Univ, Hakubi Ctr Adv Res, Sakyo Ku, Kyoto 6068302, Japan.
[Kartaltepe, J.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Sanders, D. B.; Hasinger, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Shemmer, O.] Univ N Texas, Dept Phys, Denton, TX 76203 USA.
[Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Brusa, M.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Brusa, M.; Comastri, A.; Zamorani, G.; Mignoli, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Ho, L. C.; Masters, D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Lusso, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Akiyama, M.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Alexander, D. M.; Del Moro, A.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Bongiorno, A.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Capak, P.] CALTECH, NASA, JPL Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Doi, A.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuou Ku, Sagamihara, Kanagawa 2525210, Japan.
[Laird, E. S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Schawinski, K.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
RP Brightman, M (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
EM mbright@mpe.mpg.de
RI Lanzuisi, Giorgio/K-4378-2013; Brandt, William/N-2844-2015; Mignoli,
Marco/O-9426-2015; Comastri, Andrea/O-9543-2015;
OI Lanzuisi, Giorgio/0000-0001-9094-0984; Alexander,
David/0000-0002-5896-6313; Brandt, William/0000-0002-0167-2453; Mignoli,
Marco/0000-0002-9087-2835; Comastri, Andrea/0000-0003-3451-9970;
Bongiorno, Angela/0000-0002-0101-6624; Shemmer,
Ohad/0000-0003-4327-1460; Schawinski, Kevin/0000-0001-5464-0888;
Zamorani, Giovanni/0000-0002-2318-301X
FU Japan Society for the Promotion of Science (JSPS)
FX The authors would like to thank the anonymous referee for the careful
reading and constructive criticism of our manuscript. The authors would
also like to thank the builders and operators of XMM-Newton and Chandra
and all those involved in the COSMOS and E-CDF-S surveys. MB would like
to acknowledge the financial support at the start of this project from
the Japan Society for the Promotion of Science (JSPS).
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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 AUG
PY 2013
VL 433
IS 3
BP 2485
EP 2496
DI 10.1093/mnras/stt920
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 191HK
UT WOS:000322403800059
ER
PT J
AU Iyyani, S
Ryde, F
Axelsson, M
Burgess, JM
Guiriec, S
Larsson, J
Lundman, C
Moretti, E
McGlynn, S
Nymark, T
Rosquist, K
AF Iyyani, S.
Ryde, F.
Axelsson, M.
Burgess, J. M.
Guiriec, S.
Larsson, J.
Lundman, C.
Moretti, E.
McGlynn, S.
Nymark, T.
Rosquist, K.
TI Variable jet properties in GRB 110721A: time resolved observations of
the jet photosphere
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gamma-ray burst: individual: GRB 110721A
ID GAMMA-RAY-BURSTS; LARGE-AREA TELESCOPE; THERMAL EMISSION; PEAK ENERGY;
PROMPT EMISSION; BLACK-HOLE; ENERGETICS; EFFICIENCY; COMPONENT; OUTFLOWS
AB Fermi Gamma-ray Space Telescope observations of GRB 110721A have revealed two emission components from the relativistic jet: emission from the photosphere, peaking at similar to 100 keV, and a non-thermal component, which peaks at similar to 1000 keV. We use the photospheric component to calculate the properties of the relativistic outflow. We find a strong evolution in the flow properties: the Lorentz factor decreases with time during the bursts from G similar to 1000 to similar to 150 (assuming a redshift z = 2; the values are only weakly dependent on unknown efficiency parameters). Such a decrease is contrary to the expectations from the internal shocks and the isolated magnetar birth models. Moreover, the position of the flow nozzle measured from the central engine, r(0), increases by more than two orders of magnitude. Assuming a moderately magnetized outflow we estimate that r(0) varies from 10(6) to similar to 10(9) cm during the burst. We suggest that the maximal value reflects the size of the progenitor core. Finally, we show that these jet properties naturally explain the observed broken power-law decay of the temperature which has been reported as a characteristic for gamma-ray burst pulses.
C1 [Iyyani, S.; Ryde, F.; Axelsson, M.; Larsson, J.; Lundman, C.; Moretti, E.; Nymark, T.] AlbaNova Univ Ctr, KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden.
[Iyyani, S.; Ryde, F.; Axelsson, M.; Larsson, J.; Lundman, C.; Moretti, E.; Nymark, T.; Rosquist, K.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Iyyani, S.; Axelsson, M.; Rosquist, K.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Burgess, J. M.] Univ Alabama, Huntsville, AL 35899 USA.
[Guiriec, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McGlynn, S.] Tech Univ Munich, Excellence Cluster Universe, D-85748 Garching, Germany.
[McGlynn, S.] Univ Coll Dublin, Dublin 4, Ireland.
[Rosquist, K.] ICRANet, I-65122 Pescara, Italy.
RP Iyyani, S (reprint author), AlbaNova Univ Ctr, KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden.
EM shabuiyyani@particle.kth.se
RI Iyyani, Shabnam/D-8736-2017;
OI Iyyani, Shabnam/0000-0002-2525-3464; Burgess, James/0000-0003-3345-9515;
/0000-0003-0065-2933; Axelsson, Magnus/0000-0003-4378-8785; Moretti,
Elena/0000-0001-5477-9097
FU Swedish National Space Board; EACEA of the European Commission
[2011-1640]
FX We thank the referee, Peter Meszaros, and Martin Rees for useful
comments on the manuscript. We also thank Asaf Pe'er for useful
discussions. We acknowledge support from the Swedish National Space
Board. SI is supported by the Erasmus Mundus Joint Doctorate Program by
Grant Number 2011-1640 from the EACEA of the European Commission.
NR 56
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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 AUG
PY 2013
VL 433
IS 4
BP 2739
EP 2748
DI 10.1093/mnras/stt863
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 191IF
UT WOS:000322405900004
ER
PT J
AU Landry, D
Bonamente, M
Giles, P
Maughan, B
Joy, M
Murray, S
AF Landry, D.
Bonamente, M.
Giles, P.
Maughan, B.
Joy, M.
Murray, S.
TI Chandra measurements of a complete sample of X-ray luminous galaxy
clusters: the gas mass fraction
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: intracluster medium;
large-scale structure of Universe; X-rays: galaxies: clusters
ID ZELDOVICH EFFECT MEASUREMENTS; INTRACLUSTER MEDIUM; SUNYAEV-ZELDOVICH;
ANALYTIC MODEL; JOINT ANALYSIS; BARYON CONTENT; COMA CLUSTER; DARK
ENERGY; ROSAT; CONSTRAINTS
AB We present Chandra X-ray measurements of the gas mass fraction out to r(500) for a complete sample of the 35 most luminous clusters from the Brightest Cluster Sample and the Extended Brightest Cluster Sample at redshift z = 0.15-0.30. The sample includes relaxed and unrelaxed clusters, and the data were analysed independently using two pipelines and two different models for the gas density and temperature. We measure an average of f(gas)(r(500)) = 0.163 +/- 0.032, which is in agreement with the cosmic baryon fraction ((b)/(M) = 0.167 +/- 0.006) at the 1 Sigma level, after adding the stellar baryon fraction. Earlier studies reported gas mass fractions significantly lower than the cosmic baryon fraction at r(500), and in some cases higher values that are consistent with the cosmic baryon fraction towards the virial radius. In this paper, we show that the most X-ray luminous clusters in the redshift range z = 0.15-0.30 have a gas mass fraction that is consistent with the cosmic value at r(500).
C1 [Landry, D.; Bonamente, M.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Bonamente, M.; Joy, M.] NASA, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Giles, P.; Maughan, B.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Murray, S.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
RP Landry, D (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
EM d.landry@uah.edu
FU NASA through the Graduate Student Researchers Program at Marshall Space
Flight Center
FX We are grateful to the referee for his useful comments and suggestions.
DL was supported by NASA through the Graduate Student Researchers
Program at Marshall Space Flight Center.
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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 AUG
PY 2013
VL 433
IS 4
BP 2790
EP 2811
DI 10.1093/mnras/stt901
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 191IF
UT WOS:000322405900007
ER
PT J
AU Bendo, GJ
Griffin, MJ
Bock, JJ
Conversi, L
Dowell, CD
Lim, T
Lu, N
North, CE
Papageorgiou, A
Pearson, CP
Pohlen, M
Polehampton, ET
Schulz, B
Shupe, DL
Sibthorpe, B
Spencer, LD
Swinyard, BM
Valtchanov, I
Xu, CK
AF Bendo, G. J.
Griffin, M. J.
Bock, J. J.
Conversi, L.
Dowell, C. D.
Lim, T.
Lu, N.
North, C. E.
Papageorgiou, A.
Pearson, C. P.
Pohlen, M.
Polehampton, E. T.
Schulz, B.
Shupe, D. L.
Sibthorpe, B.
Spencer, L. D.
Swinyard, B. M.
Valtchanov, I.
Xu, C. K.
TI Flux calibration of the Herschel(star)-SPIRE photometer
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE instrumentation: photometers
ID SUBMILLIMETER; NEPTUNE; URANUS
AB We describe the procedure used to flux calibrate the three-band submillimetre photometer in the Spectral and Photometric Imaging Receiver instrument on the Herschel Space Observatory. This includes the equations describing the calibration scheme, a justification for using Neptune as the primary calibration source, a description of the observations and data processing procedures used to derive flux calibration parameters (for converting from voltage to flux density) for every bolometer in each array, an analysis of the error budget in the flux calibration for the individual bolometers and tests of the flux calibration on observations of primary and secondary calibrators. The procedure for deriving the flux calibration parameters is divided into two parts. In the first part, we use observations of astronomical sources in conjunction with the operation of the photometer internal calibration source to derive the unscaled derivatives of the flux calibration curves. To scale the calibration curves in Jy beam(-1) V-1, we then use observations of Neptune in which the beam of each bolometer is mapped using a very fine scan pattern. The total instrumental uncertainties in the flux calibration for most individual bolometers is similar to 0.5 per cent, although a few bolometers have uncertainties of similar to 1-5 per cent because of issues with the Neptune observations. Based on application of the flux calibration parameters to Neptune observations performed using typical scan map observing modes, we determined that measurements from each array as a whole have instrumental uncertainties of 1.5 per cent. This is considerably less than the absolute calibration uncertainty associated with the model of Neptune, which is estimated at 4 per cent.
C1 [Bendo, G. J.] Univ Manchester, Ctr Astrophys, Jodrell Bank, UK ALMA Reg Ctr Node,Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Griffin, M. J.; North, C. E.; Papageorgiou, A.; Spencer, L. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Bock, J. J.; Dowell, C. D.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Conversi, L.; Valtchanov, I.] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain.
[Lim, T.; Pearson, C. P.; Polehampton, E. T.; Swinyard, B. M.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
[Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] IPAC, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Pearson, C. P.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Pohlen, M.] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA.
[Sibthorpe, B.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Sibthorpe, B.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands.
[Swinyard, B. M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
RP Bendo, GJ (reprint author), Univ Manchester, Ctr Astrophys, Jodrell Bank, UK ALMA Reg Ctr Node,Sch Phys & Astron, Oxford Rd, Manchester M13 9PL, Lancs, England.
EM george.bendo@manchester.ac.uk
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); NASA (USA)
FX We thank the reviewer for the helpful comments on this paper. 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.
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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 AUG
PY 2013
VL 433
IS 4
BP 3062
EP 3078
DI 10.1093/mnras/stt948
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 191IF
UT WOS:000322405900024
ER
PT J
AU Waszczak, A
Ofek, EO
Aharonson, O
Kulkarni, SR
Polishook, D
Bauer, JM
Levitan, D
Sesar, B
Laher, R
Surace, J
AF Waszczak, A.
Ofek, E. O.
Aharonson, O.
Kulkarni, S. R.
Polishook, D.
Bauer, J. M.
Levitan, D.
Sesar, B.
Laher, R.
Surace, J.
CA PTF Team
TI Main-belt comets in the Palomar Transient Factory survey - I. The search
for extendedness
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; comets: general; minor planets; asteroids: general
ID TELESCOPE LEGACY SURVEY; ASTEROID P/2010 A2; R2 LA SAGRA; TERRESTRIAL
PLANETS; PHYSICAL-PROPERTIES; SYNOPTIC SURVEY; 596 SCHEILA; SKY SURVEY;
F5 GIBBS; 133P/ELST-PIZARRO
AB Cometary activity in main-belt asteroids probes the ice content of these objects and provides clues to the history of volatiles in the inner Solar system. We search the Palomar Transient Factory survey to derive upper limits on the population size of active main-belt comets (MBCs). From data collected from 2009 March through 2012 July, we extracted similar to 2 million observations of similar to 220 thousand known main-belt objects (40 per cent of the known population, down to similar to 1-km diameter) and discovered 626 new objects in multinight linked detections. We formally quantify the 'extendedness' of a small-body observation, account for systematic variation in this metric (e.g. due to on-sky motion) and evaluate this method's robustness in identifying cometary activity using observations of 115 comets, including two known candidate MBCs and six newly discovered non-MBCs (two of which were originally designated as asteroids by other surveys). We demonstrate a 66 per cent detection efficiency with respect to the extendedness distribution of the 115 sampled comets, and a 100 per cent detection efficiency with respect to extendedness levels greater than or equal to those we observed in the known candidate MBCs P/2010 R2 (La Sagra) and P/2006 VW139. Using a log-constant prior, we infer 95 per cent confidence upper limits of 33 and 22 active MBCs (per million main-belt asteroids down to similar to 1-km diameter), for detection efficiencies of 66 and 100 per cent, respectively. In a follow-up to this morphological search, we will perform a photometric (disc-integrated brightening) search for MBCs.
C1 [Waszczak, A.; Aharonson, O.; Kulkarni, S. R.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Ofek, E. O.] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Aharonson, O.] Weizmann Inst Sci, Helen Kimmel Ctr Planetary Sci, IL-76100 Rehovot, Israel.
[Kulkarni, S. R.; Levitan, D.; Sesar, B.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Polishook, D.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Bauer, J. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, J. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Laher, R.; Surace, J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Waszczak, A (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM waszczak@caltech.edu
FU Israeli Ministry of Science; NSF [AST-0507734]; AXA
FX We thank the referee for useful comments. This work is based on data
obtained with the 1.2-m Samuel Oschin Telescope at Palomar Observatory
as part of the Palomar Transient Factory project, a scientific
collaboration between the California Institute of Technology, Columbia
University, Las Cumbres Observatory, Lawrence Berkeley National
Laboratory, the National Energy Research Scientific Computing Center,
the University of Oxford and the Weizmann Institute of Science (WIS).
EOO is incumbent of the Arye Dissentshik career development chair and is
grateful for support via a grant from the Israeli Ministry of Science.
OA and EOO wish to thank the Helen Kimmel Center for Planetary Science
at WIS. SRK and his group are partially supported by NSF grant
AST-0507734. DP is grateful to the AXA research fund.
NR 90
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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 AUG
PY 2013
VL 433
IS 4
BP 3115
EP 3132
DI 10.1093/mnras/stt951
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 191IF
UT WOS:000322405900028
ER
PT J
AU Schweizer, T
Bucciantini, N
Idec, W
Nilsson, K
Tennant, A
Weisskopf, MC
Zanin, R
AF Schweizer, T.
Bucciantini, N.
Idec, W.
Nilsson, K.
Tennant, A.
Weisskopf, M. C.
Zanin, R.
TI Characterization of the optical and X-ray properties of the
north-western wisps in the Crab nebula
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; pulsars: individual: Crab; ISM:
supernova remnants
ID PULSAR WIND NEBULAE; RELATIVISTIC MHD SIMULATIONS; SUPERNOVA-REMNANTS;
SYNCHROTRON NEBULA; TORUS; ORIGIN; EMISSION; FLARES
AB We have studied the wisps to the north-west of the Crab pulsar as part of a multiwavelength campaign in the visible and in X-rays. Optical observations were obtained using the Nordic Optical Telescope in La Palma and X-ray observations were made with the Chandra X-ray Observatory. The observing campaign took place from 2010 October until 2012 September. About once per year we observe wisps forming and peeling off from (or near) the region commonly associated with the termination shock of the pulsar wind. We find that the exact locations of the north-western wisps in the optical and in X-rays are similar but not coincident, with X-ray wisps preferentially located closer to the pulsar. This suggests that the optical and X-ray wisps are not produced by the same particle distribution. Our measurements and their implications are interpreted in terms of a Doppler-boosted ring model that has its origin in magnetohydrodynamic (MHD) modelling. While the Doppler boosting factors inferred from the X-ray wisps are consistent with current MHD simulations of pulsar wind nebulae, the optical boosting factors are not, and typically exceed values from MHD simulations by about a factor of 3.
C1 [Schweizer, T.; Idec, W.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Bucciantini, N.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Bucciantini, N.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Florence, Italy.
[Idec, W.] Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland.
[Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Turku, Finland.
[Tennant, A.; Weisskopf, M. C.] NASA Marshall Space Flight Ctr, Space Sci Dept, Huntsville, AL 35812 USA.
[Zanin, R.] Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain.
RP Schweizer, T (reprint author), Max Planck Inst Phys & Astrophys, Foehringer Ring 6, D-80805 Munich, Germany.
EM tschweiz@googlemail.com
OI Bucciantini, Niccolo'/0000-0002-8848-1392
FU Chandra Project
FX The X-ray observations have been done with the Chandra X-ray satellite.
AT and MCW would like to acknowledge support from the Chandra Project.
We would also like to acknowledge the Director of the Chandra Science
Center for authorizing Director's Discretionary Time and Chandra
Proposal 1350025 for the remainder of the observations.
NR 25
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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 AUG
PY 2013
VL 433
IS 4
BP 3325
EP 3335
DI 10.1093/mnras/stt995
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 191IF
UT WOS:000322405900043
ER
PT J
AU Conley, CA
Rummel, JD
AF Conley, Catharine A.
Rummel, John D.
TI Appropriate protection of Mars
SO NATURE GEOSCIENCE
LA English
DT Editorial Material
C1 [Conley, Catharine A.] NASA Headquarters, Sci Mission Directorate, Washington, DC 20546 USA.
[Rummel, John D.] E Carolina Univ, Inst Coastal Sci & Policy, Greenville, NC 27858 USA.
RP Conley, CA (reprint author), NASA Headquarters, Sci Mission Directorate, Washington, DC 20546 USA.
EM rummelj@ecu.edu
NR 11
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U1 2
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PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD AUG
PY 2013
VL 6
IS 8
BP 587
EP 588
PG 2
WC Geosciences, Multidisciplinary
SC Geology
GA 191VK
UT WOS:000322441900002
ER
PT J
AU Goldblatt, C
Robinson, TD
Zahnle, KJ
Crisp, D
AF Goldblatt, Colin
Robinson, Tyler D.
Zahnle, Kevin J.
Crisp, David
TI Low simulated radiation limit for runaway greenhouse climates
SO NATURE GEOSCIENCE
LA English
DT Article
ID MOLECULAR SPECTROSCOPIC DATABASE; EARLY EARTH; VENUS; ATMOSPHERE; WATER;
TEMPERATURES; EQUILIBRIUM; EVOLUTION; SURFACE; MODEL
AB The atmospheres of terrestrial planets are expected to be in long-term radiation balance: an increase in the absorption of solar radiation warms the surface and troposphere, which leads to a matching increase in the emission of thermal radiation. Warming a wet planet such as Earth would make the atmosphere moist and optically thick such that only thermal radiation emitted from the upper troposphere can escape to space. Hence, for a hot moist atmosphere, there is an upper limit on the thermal emission that is unrelated to surface temperature. If the solar radiation absorbed exceeds this limit, the planet will heat uncontrollably and the entire ocean will evaporate-the so-called runaway greenhouse. Here we model the solar and thermal radiative transfer in incipient and complete runaway greenhouse atmospheres at line-by-line spectral resolution using a modern spectral database. We find a thermal radiation limit of 282 W m(-2) (lower than previously reported) and that 294 W m(-2) of solar radiation is absorbed (higher than previously reported). Therefore, a steam atmosphere induced by such a runaway greenhouse may be a stable state for a planet receiving a similar amount of solar radiation as Earth today. Avoiding a runaway greenhouse on Earth requires that the atmosphere is subsaturated with water, and that the albedo effect of clouds exceeds their greenhouse effect. A runaway greenhouse could in theory be triggered by increased greenhouse forcing, but anthropogenic emissions are probably insufficient.
C1 [Goldblatt, Colin] Univ Victoria, Sch Earth & Ocean Sci, Victoria, BC V8W 3V6, Canada.
[Robinson, Tyler D.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Zahnle, Kevin J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Crisp, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Goldblatt, C (reprint author), Univ Victoria, Sch Earth & Ocean Sci, POB 3065, Victoria, BC V8W 3V6, Canada.
EM czg@uvic.ca
FU NASA Planetary Atmospheres; NSERC; NASA Astrobiology Institute Virtual
Planetary Laboratory
FX We thank D. Catling, J. Kasting, R. Pierrehumbert and A. Watson for
discussions at various stages in the project, and D. Abbot for a
constructive review. Contributions to this work were financially
supported by NASA Planetary Atmospheres and NSERC Discovery grants
awarded to C. G. and by the NASA Astrobiology Institute Virtual
Planetary Laboratory.
NR 40
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U1 1
U2 28
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 AUG
PY 2013
VL 6
IS 8
BP 661
EP 667
DI 10.1038/NGEO1892
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 191VK
UT WOS:000322441900020
ER
PT J
AU Aasi, J
Abadie, J
Abbott, BP
Abbott, R
Abbott, TD
Abernathy, MR
Adams, C
Adams, T
Addesso, P
Adhikari, RX
Affeldt, C
Aguiar, OD
Ajith, P
Allen, B
Ceron, EA
Amariutei, D
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, C
Ast, S
Aston, SM
Atkinson, D
Aufmuth, P
Aulbert, C
Austin, L
Aylott, BE
Babak, S
Baker, PT
Ballmer, S
Bao, Y
Barayoga, JC
Barker, D
Barr, B
Barsotti, L
Barton, MA
Bartos, I
Bassiri, R
Batch, J
Bauchrowitz, J
Behnke, B
Bell, AS
Bell, C
Bergmann, G
Berliner, JM
Bertolini, A
Betzwieser, J
Beveridge, N
Beyersdorf, PT
Bhadbhade, T
Bilenko, IA
Billingsley, G
Birch, J
Biscans, S
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Bland, B
Bock, O
Bodiya, TP
Bogan, C
Bond, C
Bork, R
Born, M
Bose, S
Bowers, J
Brady, PR
Braginsky, VB
Brau, JE
Breyer, J
Bridges, DO
Brinkmann, M
Britzger, M
Brooks, AF
Brown, DA
Brown, DD
Buckland, K
Brueckner, F
Buchler, BC
Buonanno, A
Burguet-Castell, J
Byer, RL
Cadonati, L
Camp, JB
Campsie, P
Cannon, K
Cao, J
Capano, CD
Carbone, L
Caride, S
Castiglia, AD
Caudill, S
Cavaglia, M
Cepeda, C
Chalermsongsak, T
Chao, S
Charlton, P
Chen, X
Chen, Y
Cho, HS
Chow, JH
Christensen, N
Chu, Q
Chua, SSY
Chung, CTY
Ciani, G
Clara, F
Clark, DE
Clark, JA
Constancio, M
Cook, D
Corbitt, TR
Cordier, M
Cornish, N
Corsi, A
Costa, CA
Coughlin, MW
Countryman, S
Couvares, P
Coward, DM
Cowart, M
Coyne, DC
Craig, K
Creighton, JDE
Creighton, TD
Cumming, A
Cunningham, L
Dahl, K
Damjanic, M
Danilishin, SL
Danzmann, K
Daudert, B
Daveloza, H
Davies, GS
Daw, EJ
Dayanga, T
Deleeuw, E
Denker, T
Dent, T
Dergachev, V
DeRosa, R
DeSalvo, R
Dhurandhar, S
Di Palma, I
Diaz, M
Dietz, A
Donovan, F
Dooley, KL
Doravari, S
Drasco, S
Drever, RWP
Driggers, JC
Du, Z
Dumas, JC
Dwyer, S
Eberle, T
Edwards, M
Effler, A
Ehrens, P
Eikenberry, SS
Engel, R
Essick, R
Etzel, T
Evans, K
Evans, M
Evans, T
Factourovich, M
Fairhurst, S
Fang, Q
Farr, BF
Farr, W
Favata, M
Fazi, D
Fehrmann, H
Feldbaum, D
Finn, LS
Fisher, RP
Foley, S
Forsi, E
Fotopoulos, N
Frede, M
Frei, MA
Frei, Z
Freise, A
Frey, R
Fricke, TT
Friedrich, D
Fritschel, P
Frolov, VV
Fujimoto, MK
Fulda, PJ
Fyffe, M
Gair, J
Garcia, J
Gehrels, N
Gelencser, G
Gergely, LA
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Gil-Casanova, S
Gill, C
Gleason, J
Goetz, E
Gonzalez, G
Gordon, N
Gorodetsky, ML
Gossan, S
Gossler, S
Graef, C
Graff, PB
Grant, A
Gras, S
Gray, C
Greenhalgh, RJS
Gretarsson, AM
Griffo, C
Grote, H
Grover, K
Grunewald, S
Guido, C
Gustafson, EK
Gustafson, R
Hammer, D
Hammond, G
Hanks, J
Hanna, C
Hanson, J
Haris, K
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Hartman, MT
Haughian, K
Hayama, K
Heefner, J
Heintze, MC
Hendry, MA
Heng, IS
Heptonstall, AW
Heurs, M
Hewitson, M
Hild, S
Hoak, D
Hodge, KA
Holt, K
Holtrop, M
Hong, T
Hooper, S
Hough, J
Howell, EJ
Huang, V
Huerta, EA
Hughey, B
Huttner, SH
Huynh, M
Huynh-Dinh, T
Ingram, DR
Inta, R
Isogai, T
Ivanov, A
Iyer, BR
Izumi, K
Jacobson, M
James, E
Jang, H
Jang, YJ
Jesse, E
Johnson, WW
Jones, D
Jones, DI
Jones, R
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
Keitel, D
Kelley, DB
Kells, W
Keppel, DG
Khalaidovski, A
Khalili, FY
Khazanov, EA
Kim, BK
Kim, C
Kim, K
Kim, N
Kim, YM
King, PJ
Kinzel, DL
Kissel, JS
Klimenko, S
Kline, J
Kokeyama, K
Kondrashov, V
Koranda, S
Korth, WZ
Kozak, D
Kozameh, C
Kremin, A
Kringel, V
Krishnan, B
Kucharczyk, C
Kuehn, G
Kumar, P
Kumar, R
Kuper, BJ
Kurdyumov, R
Kwee, P
Lam, PK
Landry, M
Lantz, B
Lasky, PD
Lawrie, C
Lazzarini, A
Le Roux, A
Leaci, P
Lee, CH
Lee, HK
Lee, HM
Lee, J
Leong, JR
Levine, B
Lhuillier, V
Lin, AC
Litvine, V
Liu, Y
Liu, Z
Lockerbie, NA
Lodhia, D
Loew, K
Logue, J
Lombardi, AL
Lormand, M
Lough, J
Lubinski, M
Lueck, H
Lundgren, AP
Macarthur, J
Macdonald, E
Machenschalk, B
MacInnis, M
Macleod, DM
Magana-Sandoval, F
Mageswaran, M
Mailand, K
Manca, G
Mandel, I
Mandic, V
Marka, S
Marka, Z
Markosyan, AS
Maros, E
Martin, IW
Martin, RM
Martinov, D
Marx, JN
Mason, K
Matichard, F
Matone, L
Matzner, RA
Mavalvala, N
May, G
Mazzolo, G
McAuley, K
McCarthy, R
McClelland, DE
McGuire, SC
McIntyre, G
McIver, J
Meadors, GD
Mehmet, M
Meier, T
Melatos, A
Mendell, G
Mercer, RA
Meshkov, S
Messenger, C
Meyer, MS
Miao, H
Miller, J
Mingarelli, CMF
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Moe, B
Mokler, F
Mohapatra, SRP
Moraru, D
Moreno, G
Mori, T
Morriss, SR
Mossavi, K
Mow-Lowry, CM
Mueller, CL
Mueller, G
Mukherjee, S
Mullavey, A
Munch, J
Murphy, D
Murray, PG
Mytidis, A
Kumar, DN
Nash, T
Nayak, R
Necula, V
Newton, G
Nguyen, T
Nishida, E
Nishizawa, A
Nitz, A
Nolting, D
Normandin, ME
Nuttall, LK
O'Dell, J
O'Reilly, B
O'Shaughnessy, R
Ochsner, E
Oelker, E
Ogin, GH
Oh, JJ
Oh, SH
Ohme, F
Oppermann, P
Osthelder, C
Ott, CD
Ottaway, DJ
Ottens, RS
Ou, J
Overmier, H
Owen, BJ
Padilla, C
Pai, A
Pan, Y
Pankow, C
Papa, MA
Paris, H
Parkinson, W
Pedraza, M
Penn, S
Peralta, C
Perreca, A
Phelps, M
Pickenpack, M
Pierro, V
Pinto, IM
Pitkin, M
Pletsch, HJ
Pold, J
Postiglione, F
Poux, C
Predoi, V
Prestegard, T
Price, LR
Prijatelj, M
Privitera, S
Prokhorov, LG
Puncken, O
Quetschke, V
Quintero, E
Quitzow-James, R
Raab, FJ
Radkins, H
Raffai, P
Raja, S
Rakhmanov, M
Ramet, C
Raymond, V
Reed, CM
Reed, T
Reid, S
Reitze, DH
Riesen, R
Riles, K
Roberts, M
Robertson, NA
Robinson, EL
Roddy, S
Rodriguez, C
Rodriguez, L
Rodruck, M
Rollins, JG
Romie, JH
Ver, CR
Rowan, S
Rudiger, A
Ryan, K
Salemi, F
Sammut, L
Sandberg, V
Sanders, J
Sankar, S
Sannibale, V
Santamaria, L
Santiago-Prieto, I
Santostasi, G
Sathyaprakash, BS
Saulson, PR
Savage, RL
Schilling, R
Schnabel, R
Schofield, RMS
Schuette, D
Schulz, B
Schutz, BF
Schwinberg, P
Scott, J
Scott, SM
Seifert, F
Sellers, D
Sengupta, AS
Sergeev, A
Shaddock, DA
Shahriar, MS
Shaltev, M
Shao, Z
Shapiro, B
Shawhan, P
Shoemaker, DH
Sidery, TL
Siemens, X
Sigg, D
Simakov, D
Singer, A
Singer, L
Sintes, AM
Skelton, GR
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Smith, RJE
Smith-Lefebvre, ND
Son, EJ
Sorazu, B
Souradeep, T
Stefszky, M
Steinert, E
Steinlechner, J
Steinlechner, S
Steplewski, S
Stevens, D
Stochino, A
Stone, R
Strain, KA
Strigin, SE
Stroeer, AS
Stuver, AL
Summerscales, TZ
Susmithan, S
Sutton, PJ
Szeifert, G
Talukder, D
Tanner, DB
Tarabrin, SP
Taylor, R
Thomas, M
Thomas, P
Thorne, KA
Thorne, KS
Thrane, E
Tiwari, V
Tokmakov, KV
Tomlinson, C
Torres, CV
Torrie, CI
Traylor, G
Tse, M
Ugolini, D
Unnikrishnan, CS
Vahlbruch, H
Vallisneri, M
van der Sluys, MV
van Veggel, AA
Vass, S
Vaulin, R
Vecchio, A
Veitch, PJ
Veitch, J
Venkateswara, K
Verma, S
Vincent-Finley, R
Vitale, S
Vo, T
Vorvick, C
Vousden, WD
Vyatchanin, SP
Wade, A
Wade, L
Wade, M
Waldman, SJ
Wallace, L
Wan, Y
Wang, M
Wang, J
Wang, X
Wanner, A
Ward, RL
Was, M
Weinert, M
Weinstein, AJ
Weiss, R
Welborn, T
Wen, L
Wessels, P
West, M
Westphal, T
Wette, K
Whelan, JT
Whitcomb, SE
Wiseman, AG
White, DJ
Whiting, BF
Wiesner, K
Wilkinson, C
Willems, PA
Williams, L
Williams, R
Williams, T
Willis, JL
Willke, B
Wimmer, M
Winkelmann, L
Winkler, W
Wipf, CC
Wittel, H
Woan, G
Wooley, R
Worden, J
Yablon, J
Yakushin, I
Yamamoto, H
Yancey, CC
Yang, H
Yeaton-Massey, D
Yoshida, S
Yum, H
Zanolin, M
Zhang, F
Zhang, L
Zhao, C
Zhu, H
Zhu, XJ
Zotov, N
Zucker, ME
Zweizig, J
AF Aasi, J.
Abadie, J.
Abbott, B. P.
Abbott, R.
Abbott, T. D.
Abernathy, M. R.
Adams, C.
Adams, T.
Addesso, P.
Adhikari, R. X.
Affeldt, C.
Aguiar, O. D.
Ajith, P.
Allen, B.
Ceron, E. Amador
Amariutei, D.
Anderson, S. B.
Anderson, W. G.
Arai, K.
Araya, M. C.
Arceneaux, C.
Ast, S.
Aston, S. M.
Atkinson, D.
Aufmuth, P.
Aulbert, C.
Austin, L.
Aylott, B. E.
Babak, S.
Baker, P. T.
Ballmer, S.
Bao, Y.
Barayoga, J. C.
Barker, D.
Barr, B.
Barsotti, L.
Barton, M. A.
Bartos, I.
Bassiri, R.
Batch, J.
Bauchrowitz, J.
Behnke, B.
Bell, A. S.
Bell, C.
Bergmann, G.
Berliner, J. M.
Bertolini, A.
Betzwieser, J.
Beveridge, N.
Beyersdorf, P. T.
Bhadbhade, T.
Bilenko, I. A.
Billingsley, G.
Birch, J.
Biscans, S.
Black, E.
Blackburn, J. K.
Blackburn, L.
Blair, D.
Bland, B.
Bock, O.
Bodiya, T. P.
Bogan, C.
Bond, C.
Bork, R.
Born, M.
Bose, S.
Bowers, J.
Brady, P. R.
Braginsky, V. B.
Brau, J. E.
Breyer, J.
Bridges, D. O.
Brinkmann, M.
Britzger, M.
Brooks, A. F.
Brown, D. A.
Brown, D. D.
Buckland, K.
Brueckner, F.
Buchler, B. C.
Buonanno, A.
Burguet-Castell, J.
Byer, R. L.
Cadonati, L.
Camp, J. B.
Campsie, P.
Cannon, K.
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Chow, J. H.
Christensen, N.
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Chung, C. T. Y.
Ciani, G.
Clara, F.
Clark, D. E.
Clark, J. A.
Constancio, M., Jr.
Cook, D.
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Cornish, N.
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Winkler, W.
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Wittel, H.
Woan, G.
Wooley, R.
Worden, J.
Yablon, J.
Yakushin, I.
Yamamoto, H.
Yancey, C. C.
Yang, H.
Yeaton-Massey, D.
Yoshida, S.
Yum, H.
Zanolin, M.
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Zotov, N.
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Zweizig, J.
TI Enhanced sensitivity of the LIGO gravitational wave detector by using
squeezed states of light
SO NATURE PHOTONICS
LA English
DT Article
ID QUANTUM; INTERFEROMETER; METROLOGY; NOISE
AB Nearly a century after Einstein first predicted the existence of gravitational waves, a global network of Earth-based gravitational wave observatories(1-4) is seeking to directly detect this faint radiation using precision laser interferometry. Photon shot noise, due to the quantum nature of light, imposes a fundamental limit on the attometre-level sensitivity of the kilometre-scale Michelson interferometers deployed for this task. Here, we inject squeezed states to improve the performance of one of the detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) beyond the quantum noise limit, most notably in the frequency region down to 150 Hz, critically important for several astrophysical sources, with no deterioration of performance observed at any frequency. With the injection of squeezed states, this LIGO detector demonstrated the best broadband sensitivity to gravitational waves ever achieved, with important implications for observing the gravitational-wave Universe with unprecedented sensitivity.
C1 [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Ajith, P.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Buckland, K.; Cepeda, C.; Chalermsongsak, T.; Coyne, D. C.; Daudert, B.; Dergachev, V.; Doravari, S.; Driggers, J. C.; Ehrens, P.; Engel, R.; Etzel, T.; Fotopoulos, N.; Gustafson, E. K.; Harms, J.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lazzarini, A.; Litvine, V.; Mageswaran, M.; Mailand, K.; Maros, E.; Martinov, D.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Pedraza, M.; Phelps, M.; Poux, C.; Price, L. R.; Privitera, S.; Quintero, E.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Santamari, L.; Seifert, F.; Shao, Z.; Singer, A.; Singer, L.; Smith, M. R.; Smith-Lefebvre, N. D.; Taylor, R.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Williams, R.; Williams, T.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Barr, B.; Bassiri, R.; Bell, A. S.; Bell, C.; Beveridge, N.; Campsie, P.; Craig, K.; Cumming, A.; Cunningham, L.; Davies, G. S.; Evans, K.; Gill, C.; Gordon, N.; Grant, A.; Hammond, G.; Haughian, K.; Hendry, M. A.; Heng, I. S.; Hild, S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Lawrie, C.; Logue, J.; Macarthur, J.; Martin, I. W.; Murray, P. G.; Newton, G.; Pitkin, M.; Robertson, N. A.; Rowan, S.; Santiago-Prieto, I.; Scott, J.; Sorazu, B.; Strain, K. A.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Adams, C.; Aston, S. M.; Betzwieser, J.; 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.; Le Roux, A.; Lormand, M.; Meyer, M. S.; Nolting, D.; O'Reilly, B.; Overmier, H.; Ramet, C.; Raymond, V.; Riesen, R.; Roddy, S.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thomas, M.; Thorne, K. A.; Traylor, G.; Welborn, T.; Wooley, R.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA.
[Affeldt, C.; Allen, B.; Ast, S.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bergmann, G.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Damjanic, M.; Danzmann, K.; Denker, T.; Dent, T.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Heurs, M.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Keitel, D.; Keppel, D. G.; Khalaidovski, A.; Kringel, V.; Krishnan, B.; Kuehn, G.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mokler, F.; Mossavi, K.; Mow-Lowry, C. M.; Oppermann, P.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Ver, C. Ro; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schuette, D.; Schulz, B.; Shaltev, M.; Simakov, D.; Slutsky, J.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Vahlbruch, H.; Wanner, A.; Was, M.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Wiesner, K.; Willke, B.; Wimmer, M.; Winkelmann, L.; Winkler, W.; Wittel, H.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Allen, B.; Ceron, E. Amador; Anderson, W. G.; Brady, P. R.; Caudill, S.; Creighton, J. D. E.; Favata, M.; Giampanis, S.; Hammer, D.; Huynh, M.; Kline, J.; Koranda, S.; Mercer, R. A.; Moe, B.; O'Shaughnessy, R.; Ochsner, E.; Pankow, C.; Papa, M. A.; Siemens, X.; Skelton, G. R.; Wade, L.; Wade, M.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Bassiri, R.; Bhadbhade, T.; Byer, R. L.; Clark, D. E.; Kim, N.; Kucharczyk, C.; Kurdyumov, R.; Lantz, B.; Lin, A. C.; Markosyan, A. S.; Roberts, M.; Shapiro, B.] Stanford Univ, Stanford, CA 94305 USA.
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[Abbott, T. D.; Bowers, J.; Corbitt, T. R.; DeRosa, R.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Johnson, W. W.; Kokeyama, K.; May, G.; Mullavey, A.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
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[Affeldt, C.; Allen, B.; Ast, S.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bergmann, G.; Bertolini, A.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Damjanic, M.; Danzmann, K.; Denker, T.; Dent, T.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Heurs, M.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Keitel, D.; Keppel, D. G.; Khalaidovski, A.; Kringel, V.; Krishnan, B.; Kuehn, G.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mokler, F.; Mossavi, K.; Mow-Lowry, C. M.; Oppermann, P.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Ver, C. Ro; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schuette, D.; Schulz, B.; Shaltev, M.; Simakov, D.; Slutsky, J.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Vahlbruch, H.; Wanner, A.; Was, M.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Wiesner, K.; Willke, B.; Wimmer, M.; Winkelmann, L.; Winkler, W.; Wittel, H.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
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[McGuire, S. C.; Vincent-Finley, R.] Southern Univ, Baton Rouge, LA 70813 USA.
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[Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Burguet-Castell, J.; Gil-Casanova, S.; Sintes, A. M.] Univ Illes Balears, E-07122 Palma De Mallorca, Spain.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Khazanov, E. A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
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[Addesso, P.; DeSalvo, R.; Pierro, V.; Pinto, I. M.] INFN Sezione Napoli, Naples, Italy.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
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[Parkinson, W.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Cannon, K.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cho, H. -S.; Kim, Y. -M.; Lee, C. -H.] Pusan Natl Univ, Pusan, South Korea.
W Virginia Univ, Morgantown, WV 26505 USA.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Jang, H.; Kang, G.; Kim, B. K.; Kim, C.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Gergely, L. A.] Univ Szeged, H-6720 Szeged, Hungary.
[Holtrop, M.] Univ New Hampshire, Durham, NH 03824 USA.
[Coughlin, M. W.; Gair, J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Harry, G. M.] American Univ, Washington, DC 20016 USA.
[Aguiar, O. D.; Constancio, M., Jr.; Costa, C. A.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, Brazil.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Chao, S.; Huang, V.; Ou, J.; Wang, J.] Natl Tsing Hua Univ, Hsinchu 300, Taiwan.
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[Corsi, A.] George Washington Univ, Washington, DC 20052 USA.
[Iyer, B. R.] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Kozameh, C.] Univ Nacl Cordoba, RA-5000 Cordoba, Argentina.
[Nayak, R.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[Haris, K.; Pai, A.] IISER TVM, Trivandrum 695016, Kerala, India.
[Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India.
[Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India.
[Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Sergeev,
Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Ward, Robert/I-8032-2014;
Ottaway, David/J-5908-2015; Chen, Yanbei/A-2604-2013; Shaddock,
Daniel/A-7534-2011; Postiglione, Fabio/O-4744-2015; Gehring,
Tobias/A-8596-2016; Strain, Kenneth/D-5236-2011; Howell,
Eric/H-5072-2014; Bao, Yiliang/G-9848-2016; Zhu, Xingjiang/E-1501-2016;
Pinto, Innocenzo/L-3520-2016; Buchler, Ben/D-4581-2009; Bartos,
Imre/A-2592-2017; Chow, Jong/A-3183-2008; Kumar, Prem/B-6691-2009;
Huerta, Eliu/J-5426-2014; Lam, Ping Koy/A-5276-2008; Hild,
Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012; Lee,
Chang-Hwan/B-3096-2015; Khalili, Farit/D-8113-2012; McClelland,
David/E-6765-2010; Vecchio, Alberto/F-8310-2015; Mow-Lowry,
Conor/F-8843-2015; Finn, Lee Samuel/A-3452-2009; Sigg,
Daniel/I-4308-2015; Graef, Christian/J-3167-2015; Steinlechner,
Sebastian/D-5781-2013; Costa, Cesar/G-7588-2012; Strigin,
Sergey/I-8337-2012; Prokhorov, Leonid/I-2953-2012; Miao,
Haixing/O-1300-2013; Khazanov, Efim/B-6643-2014; Zhao,
Chunnong/C-2403-2013; Salemi, Francesco/F-6988-2014; Iyer, Bala
R./E-2894-2012; Gorodetsky, Michael/C-5938-2008; Mitrofanov,
Valery/D-8501-2012; Bell, Angus/E-7312-2011; Bilenko, Igor/D-5172-2012;
OI Farr, Ben/0000-0002-2916-9200; Pierro, Vincenzo/0000-0002-6020-5521;
Nishizawa, Atsushi/0000-0003-3562-0990; Lasky, Paul/0000-0003-3763-1386;
Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198;
Zweizig, John/0000-0002-1521-3397; Frey, Raymond/0000-0003-0341-2636;
Ciani, Giacomo/0000-0003-4258-9338; Whelan, John/0000-0001-5710-6576;
Matichard, Fabrice/0000-0001-8982-8418; Ward,
Robert/0000-0001-5503-5241; Pinto, Innocenzo M./0000-0002-2679-4457;
Shaddock, Daniel/0000-0002-6885-3494; Postiglione,
Fabio/0000-0003-0628-3796; Gehring, Tobias/0000-0002-4311-2593; Strain,
Kenneth/0000-0002-2066-5355; Howell, Eric/0000-0001-7891-2817; Zhu,
Xingjiang/0000-0001-7049-6468; Buchler, Ben/0000-0002-2852-7483; Chow,
Jong/0000-0002-2414-5402; Lam, Ping Koy/0000-0002-4421-601X; Danilishin,
Stefan/0000-0001-7758-7493; Lee, Chang-Hwan/0000-0003-3221-1171;
McClelland, David/0000-0001-6210-5842; Vecchio,
Alberto/0000-0002-6254-1617; Finn, Lee Samuel/0000-0002-3937-0688; Sigg,
Daniel/0000-0003-4606-6526; Graef, Christian/0000-0002-4535-2603;
Steinlechner, Sebastian/0000-0003-4710-8548; Miao,
Haixing/0000-0003-4101-9958; Zhao, Chunnong/0000-0001-5825-2401; Iyer,
Bala R./0000-0002-4141-5179; Gorodetsky, Michael/0000-0002-5159-2742;
Bell, Angus/0000-0003-1523-0821; O'Shaughnessy,
Richard/0000-0001-5832-8517; Fairhurst, Stephen/0000-0001-8480-1961;
Addesso, Paolo/0000-0003-0895-184X; Pitkin, Matthew/0000-0003-4548-526X;
Davies, Gareth/0000-0002-4289-3439; Kanner, Jonah/0000-0001-8115-0577
FU Australian Research Council; International Science Linkages programme 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; Royal Society;
Scottish Funding Council; Scottish Universities Physics Alliance;
National Aeronautics and Space Administration; National Research
Foundation of Korea; Ministry of Economic Development and Innovation,;
National Science and Engineering Research Council Canada; Carnegie
Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research
Corporation; Alfred P. Sloan Foundation
FX The authors acknowledge support from the United States National Science
Foundation for the construction and operation of the LIGO Laboratory,
and the Science and Technology Facilities Council of the United Kingdom,
the Max-Planck-Society and the State of Niedersachsen/Germany for
supporting the construction and operation of the GEO600 detector. The
authors also acknowledge support for the research, by these agencies and
by the Australian Research Council, the International Science Linkages
programme 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 Royal Society, the Scottish Funding Council, the
Scottish Universities Physics Alliance, The National Aeronautics and
Space Administration, the National Research Foundation of Korea,
Industry Canada and the Province of Ontario through the Ministry of
Economic Development and Innovation, the National Science and
Engineering Research Council Canada, the Carnegie Trust, the Leverhulme
Trust, the David and Lucile Packard Foundation, the Research Corporation
and the Alfred P. Sloan Foundation.
NR 31
TC 166
Z9 170
U1 24
U2 150
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1749-4885
EI 1749-4893
J9 NAT PHOTONICS
JI Nat. Photonics
PD AUG
PY 2013
VL 7
IS 8
BP 613
EP 619
DI 10.1038/NPHOTON.2013.177
PG 7
WC Optics; Physics, Applied
SC Optics; Physics
GA 191YD
UT WOS:000322450200012
ER
PT J
AU Su, Y
Veronig, AM
Holman, GD
Dennis, BR
Wang, TJ
Temmer, M
Gan, WQ
AF Su, Yang
Veronig, Astrid M.
Holman, Gordon D.
Dennis, Brian R.
Wang, Tongjiang
Temmer, Manuela
Gan, Weiqun
TI Imaging coronal magnetic-field reconnection in a solar flare
SO NATURE PHYSICS
LA English
DT Article
ID X-RAY SOURCE; CURRENT SHEET; EMISSION; OUTFLOWS; ERUPTION; INFLOW;
RHESSI
AB Magnetic-field reconnection is believed to play a fundamental role in magnetized plasma systems throughout the Universe(1), including planetary magnetospheres, magnetars and accretion disks around black holes. This letter presents extreme ultraviolet and X-ray observations of a solar flare showing magnetic reconnection with a level of clarity not previously achieved. The multi-wavelength extreme ultraviolet observations from SDO/AIA show inflowing cool loops and newly formed, outflowing hot loops, as predicted. RHESSI X-ray spectra and images simultaneously show the appearance of plasma heated to >10MK at the expected locations. These two data sets provide solid visual evidence of magnetic reconnection producing a solar flare, validating the basic physical mechanism of popular flare models. However, new features are also observed that need to be included in reconnection and flare studies, such as three-dimensional non-uniform, non-steady and asymmetric evolution.
C1 [Su, Yang; Veronig, Astrid M.; Temmer, Manuela] Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria.
[Holman, Gordon D.; Dennis, Brian R.; Wang, Tongjiang] NASA, Goddard Space Flight Ctr, Solar Phys Lab Code 671, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Wang, Tongjiang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Gan, Weiqun] Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210008, Jiangsu, Peoples R China.
RP Su, Y (reprint author), Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, Univ Pl 5-2, A-8010 Graz, Austria.
EM yang.su@uni-graz.at
RI Veronig, Astrid/B-8422-2009; Su, Yang/J-5381-2014;
OI Temmer, Manuela/0000-0003-4867-7558
FU NASA's Living With a Star (LWS) Program; European Community [263086];
NSFC [11233008]; NASA Guest Investigator; RHESSI programme; NASA
[NNX12AB34G, NNG11PL10A]; Austrian Science Fund (FWF) [V195-N16];
[2011CB811402]
FX The authors dedicate this paper to the late RHESSI PI, R. P. Lin, in
acknowledgement of his inspirational efforts that made possible the
high-quality solar X-ray data used in this paper. RHESSI is a NASA Small
Explorer Mission. The GOES is a joint effort of NASA and the National
Oceanic and Atmospheric Administration (NOAA). The SDO is a mission for
NASA's Living With a Star (LWS) Program. The work of Y.S. and A. M. V.
was supported by the European Community Framework Programme 7, High
Energy Solar Physics data in Europe (HESPE), grant agreement No. 263086.
Y.S. also acknowledges NSFC 11233008. The work of G. H. was supported by
a NASA Guest Investigator Grant and the RHESSI programme. The work of T.
W. was supported by NASA grant NNX12AB34G and NASA Cooperative Agreement
NNG11PL10A to C. U. A. M. T. acknowledges the Austrian Science Fund
(FWF): V195-N16. W. G. acknowledges 2011CB811402 and NSFC 11233008.
NR 30
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U1 3
U2 23
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1745-2473
EI 1745-2481
J9 NAT PHYS
JI Nat. Phys.
PD AUG
PY 2013
VL 9
IS 8
BP 489
EP 493
DI 10.1038/NPHYS2675
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 193WK
UT WOS:000322592000018
ER
PT J
AU Wang, TY
Wei, ZG
Jiang, WY
Kuang, WJ
Ma, SZ
AF Wang TianYuan
Wei ZiGang
Jiang WeiYuan
Kuang WeiJia
Ma ShiZhuang
TI Martian magnetic field properties before the termination of its core
dynamo
SO SCIENCE CHINA-EARTH SCIENCES
LA English
DT Article
DE Mars; remnant magnetization; subcritical dynamo; dipolar
ID MARS; MAP; CONVECTION; STATE; MODEL
AB Observed Martian crustal magnetism shows that the Mars does not possess a global-scale, dynamo-driven intrinsic magnetic field. In addition, the remnant field at the surface is hemi-spherically asymmetric. Our earlier simulation results suggest that the Martian dynamo could be sub-critical near its end (the energy required to sustain a subcritical dynamo is less than that to excite the dynamo) and the generated field morphology is non-dipolar. We further the study to examine the characteristics of the magnetic field via Empirical Orthogonal Function (EOF) analysis on the subcritical dynamo solutions with the Rayleigh number R (th) = 2480 (below the critical point for the onset of the Martian dynamo). Our results show that the magnetic field is dominantly equatorial dipolar. Reversals and excursions occur frequently, and the magnetic dipole moment does not vary monotonically in time.
C1 [Wang TianYuan] Yunnan Univ, Sch Resource Environm & Earth Sci, Kunming 650091, Peoples R China.
[Wei ZiGang] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Jiang WeiYuan] NASA, Goddard Space Flight Ctr, SGT, Greenbelt, MD 20771 USA.
[Jiang WeiYuan; Kuang WeiJia] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Ma ShiZhuang] Chinese Acad Sci, Grad Univ, Lab Computat Geodynam, Beijing 100049, Peoples R China.
RP Wang, TY (reprint author), Yunnan Univ, Sch Resource Environm & Earth Sci, Kunming 650091, Peoples R China.
EM tywang@mails.gucas.ac.cn
RI Kuang, Weijia/K-5141-2012
OI Kuang, Weijia/0000-0001-7786-6425
NR 38
TC 1
Z9 1
U1 1
U2 4
PU SCIENCE PRESS
PI BEIJING
PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA
SN 1674-7313
J9 SCI CHINA EARTH SCI
JI Sci. China-Earth Sci.
PD AUG
PY 2013
VL 56
IS 8
BP 1452
EP 1458
DI 10.1007/s11430-012-4510-4
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 194IV
UT WOS:000322626300016
ER
PT J
AU Cerri, L
Lemoine, JM
Mercier, F
Zelensky, NP
Lemoine, FG
AF Cerri, L.
Lemoine, J. M.
Mercier, F.
Zelensky, N. P.
Lemoine, F. G.
TI DORIS-based point mascons for the long term stability of precise orbit
solutions
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE DORIS; POD; Altimetry; GRACE; Time Varying Gravity (TVG); MASCON
ID GRAVITY-FIELD MODELS; GRACE; PRESSURE; JASON-1
AB In recent years non-tidal Time Varying Gravity (TVG) has emerged as the most important contributor in the error budget of Precision Orbit Determination (POD) solutions for altimeter satellites' orbits. The Gravity Recovery And Climate Experiment (GRACE) mission has provided POD analysts with static and time-varying gravity models that are very accurate over the 2002-2012 time interval, but whose linear rates cannot be safely extrapolated before and after the GRACE lifespan. One such model based on a combination of data from GRACE and Lageos from 2002-2010, is used in the dynamic POD solutions developed for the Geophysical Data Records (GDRs) of the Jason series of altimeter missions and the equivalent products from lower altitude missions such as Envisat, Cryosat-2, and HY-2A. In order to accommodate long-term time-variable gravity variations not included in the background geopotential model, we assess the feasibility of using DORIS data to observe local mass variations using point mascons. In particular, we show that the point-mascon approach can stabilize the geographically correlated orbit errors which are of fundamental interest for the analysis of regional Mean Sea Level trends based on altimeter data, and can therefore provide an interim solution in the event of GRACE data loss. The time series of point-mass solutions for Greenland and Antarctica show good agreement with independent series derived from GRACE data, indicating a mass loss at rate of 210 Gt/year and 110 Gt/year respectively. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Cerri, L.; Mercier, F.] Ctr Natl Etud Spatiales, Orbitog Off, F-31055 Toulouse, France.
[Lemoine, J. M.] Ctr Natl Etud Spatiales, Grp Rech Geodesie Spatiale, F-31055 Toulouse, France.
[Zelensky, N. P.] SGT Inc, Greenbelt, MD USA.
[Lemoine, F. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Cerri, L (reprint author), Ctr Natl Etud Spatiales, Orbitog Off, 18 Ave Edouard Belin, F-31055 Toulouse, France.
EM luca.cerri@cnes.fr; jean-michel.lemoi-ne@cnes.fr;
flavien.mercier@cnes.fr; nze-lensky@sgt-inc.com;
frank.g.lemoine@nasa.gov
RI Lemoine, Frank/D-1215-2013
NR 25
TC 6
Z9 6
U1 2
U2 7
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD AUG 1
PY 2013
VL 52
IS 3
BP 466
EP 476
DI 10.1016/j.asr.2013.03.023
PG 11
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 187CU
UT WOS:000322095300012
ER
PT J
AU Michalek, G
Yashiro, S
AF Michalek, Grzegorz
Yashiro, Seiji
TI CMEs and active regions on the sun
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Sun; Solar activity; Coronal mass ejection
ID CORONAL MASS EJECTIONS
AB The relationship between active regions (ARs) and coronal mass ejections (CMEs) is studied. For this purpose a statistical analysis of 694 CMEs associated with ARs was carried out. We considered the relationship between properties of the CMEs and ARs characterized using the McIntosh classification. We demonstrated that CMEs are likely to be launched from ARs in the mature phase of their evolution when they have complex magnetic field. The fastest and halo CMEs can be ejected only from the most complex ARs (when an AR is a bipolar group of spots with large asymmetric penumbras around the main spot with many smaller spots in the group). We also showed that the wider events have a tendency to originate from uncomplicated magnetic structures. This tendency was used for estimation of the real angular widths of the halo CMEs. The probability of launching of fast CMEs increases together with increase of the complexity and size of ARs. The widest, but slow, CMEs originate from the simplest magnetic structure which are still able to produce CMEs. Our results could be useful for forecasting of space weather. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Michalek, Grzegorz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Yashiro, Seiji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yashiro, Seiji] Catholic Univ Amer, Washington, DC 20064 USA.
RP Michalek, G (reprint author), Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
EM michalek@oa.uj.edu.pl; seiji.yashiro@gmail.com
FU MNiSW [N203 023 31/3055]; NASA [NNX08AD60A]
FX Grzegorz Michalek was supported by MNiSW through the Grant N203 023
31/3055 and NASA (NNX08AD60A).
NR 15
TC 2
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U1 1
U2 2
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 AUG 1
PY 2013
VL 52
IS 3
BP 521
EP 527
DI 10.1016/j.asr.2013.04.001
PG 7
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 187CU
UT WOS:000322095300018
ER
PT J
AU Bernard, DE
Abelson, RD
Johannesen, JR
Lam, T
McAlpine, WJ
Newlin, LE
AF Bernard, Douglas E.
Abelson, Robert D.
Johannesen, Jennie R.
Lam, Try
McAlpine, William J.
Newlin, Laura E.
TI Europa planetary protection for Juno Jupiter Orbiter
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Juno; Jupiter; Planetary protection; Europa; Jet Propulsion Laboratory;
NASA
AB NASA's Juno mission launched in 2011 and will explore Jupiter and its near environment starting in 2016. Planetary protection requirements for avoiding the contamination of Europa have been taken into account in the Juno mission design. In particular Juno's polar orbit, which enables scientific investigations of parts of Jupiter's environment never before visited, also greatly assist avoiding close flybys of Europa and the other Galilean satellites.
The science mission is designed to conclude with a deorbit burn that disposes of the spacecraft in Jupiter's atmosphere. Compliance with planetary protection requirements is verified through a set of analyses including analysis of initial bioburden, analysis of the effect of bioburden reduction due to the space and Jovian radiation environments, probabilistic risk assessment of successful deorbit, Monte-Carlo orbit propagation, and bioburden reduction in the event of impact with an icy body. (C) 2013 Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Bernard, Douglas E.; Abelson, Robert D.; Johannesen, Jennie R.; Lam, Try; McAlpine, William J.; Newlin, Laura E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bernard, DE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM douglas.e.bernard@jpl.nasa.gov; robert.d.abelson@jpl.nasa.gov;
jennie.r.johannesen@jpl.nasa.gov; try.lam@jpl.nasa.gov;
william.j.mcalpine@jpl.nasa.gov; laura.e.newlin@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX Stuart Stephens of JPL contributed to the mission and trajectory design
portions of this paper including creating Figs. 1, 2 and 9 using SOAP
software. Amanda Briden and Chet Everline of JPL contributed technical
content to mission design and probabilistic risk analysis portions of
this paper, respectively. Steve Hancock of Foils Engineering helped the
wuno team appreciate the physical implications of high-speed impact into
an icy body and created Figs. 14-18. Lockheed Martin is the Juno
spacecraft developer and produced Figs. 3 and 4. 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 14
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U1 1
U2 17
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD AUG 1
PY 2013
VL 52
IS 3
BP 547
EP 568
DI 10.1016/j.asr.2013.03.015
PG 22
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 187CU
UT WOS:000322095300021
ER
PT J
AU Whiteman, DN
Venable, DD
Walker, M
Cadirola, M
Sakai, T
Veselovskii, I
AF Whiteman, David N.
Venable, Demetrius D.
Walker, Monique
Cadirola, Martin
Sakai, Tetsu
Veselovskii, Igor
TI Assessing the temperature dependence of narrow-band Raman water vapor
lidar measurements: a practical approach
SO APPLIED OPTICS
LA English
DT Article
ID ASYMMETRIC-TOP MOLECULES; CROSS-SECTIONS; UPPER TROPOSPHERE; H2O;
CALIBRATION; SCATTERING; EQUATIONS; AEROSOLS; SPECTRA; CLOUDS
AB Narrow-band detection of the Raman water vapor spectrum using the lidar technique introduces a concern over the temperature dependence of the Raman spectrum. Various groups have addressed this issue either by trying to minimize the temperature dependence to the point where it can be ignored or by correcting for whatever degree of temperature dependence exists. The traditional technique for performing either of these entails accurately measuring both the laser output wavelength and the water vapor spectral passband with combined uncertainty of approximately 0.01 nm. However, uncertainty in interference filter center wavelengths and laser output wavelengths can be this large or larger. These combined uncertainties translate into uncertainties in the magnitude of the temperature dependence of the Raman lidar water vapor measurement of 3% or more. We present here an alternate approach for accurately determining the temperature dependence of the Raman lidar water vapor measurement. This alternate approach entails acquiring sequential atmospheric profiles using the lidar while scanning the channel passband across portions of the Raman water vapor Q-branch. This scanning is accomplished either by tilt-tuning an interference filter or by scanning the output of a spectrometer. Through this process a peak in the transmitted intensity can be discerned in a manner that defines the spectral location of the channel passband with respect to the laser output wavelength to much higher accuracy than that achieved with standard laboratory techniques. Given the peak of the water vapor signal intensity curve, determined using the techniques described here, and an approximate knowledge of atmospheric temperature, the temperature dependence of a given Raman lidar profile can be determined with accuracy of 0.5% or better. A Mathematica notebook that demonstrates the calculations used here is available from the lead author. (C) 2013 Optical Society of America
C1 [Whiteman, David N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Venable, Demetrius D.; Walker, Monique] Howard Univ, Washington, DC 20059 USA.
[Cadirola, Martin] Ecotronics LLC, Clarksburg, MD 20871 USA.
[Sakai, Tetsu] Meteorol Res Inst, Tsukuba, Ibaraki 3050052, Japan.
[Veselovskii, Igor] Phys Instrumentat Ctr, Troitsk, Russia.
RP Whiteman, DN (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM david.n.whiteman@nasa.gov
FU NASA/Earth Science Technology Office; NASA Atmospheric Composition
Program
FX We thank Dr. Jose Maria Fernandez for fruitful discussions regarding the
absolute accuracy of the Avila et al. 2004 [20] cross section values.
The experimental technique of determining the FH curve
through tilt-tuning of interference filters was developed as part of the
NASA/Earth Science Technology Office funded Advanced Component
Technology Program involving Barr Associates and NASA/GSFC. This effort
has also been supported by the NASA Atmospheric Composition Program,
managed by Ken Jucks. The mention of a particular manufacturer does not
constitute an endorsement by NASA.
NR 32
TC 1
Z9 1
U1 0
U2 15
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
J9 APPL OPTICS
JI Appl. Optics
PD AUG 1
PY 2013
VL 52
IS 22
BP 5376
EP 5384
DI 10.1364/AO.52.005376
PG 9
WC Optics
SC Optics
GA 193OP
UT WOS:000322569800020
PM 23913054
ER
PT J
AU Ackermann, M
Ajello, M
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Bloom, ED
Bonamente, E
Borgland, AW
Brandt, TJ
Bregeon, J
Brez, A
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
Dermer, CD
de Palma, F
Digel, SW
Drell, PS
Dubois, R
Favuzzi, C
Ferrara, EC
Focke, WB
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashi, K
Hayashida, M
Hughes, RE
Itoh, R
Johannesson, G
Johnson, AS
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lee, SH
Llena-Garde, M
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Makeev, A
Martin, P
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Naumann-Godo, M
Nishino, S
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Parent, D
Pelassa, V
Pepe, M
Pesce-Rollins, M
Piron, F
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Ripken, J
Sada, T
Sadrozinski, HFW
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Strickman, MS
Strong, AW
Suson, DJ
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JB
Thompson, DJ
Tibaldo, L
Torres, DF
Tramacere, A
Uchiyama, Y
Uehara, T
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vilchez, N
Vitale, V
Vladimirov, AE
Waite, AP
Wang, P
Wood, KS
Yang, Z
Ziegler, M
AF Ackermann, M.
Ajello, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Brandt, T. J.
Bregeon, J.
Brez, A.
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.
Dermer, C. D.
de Palma, F.
Digel, S. W.
Drell, P. S.
Dubois, R.
Favuzzi, C.
Ferrara, E. C.
Focke, W. B.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashi, K.
Hayashida, M.
Hughes, R. E.
Itoh, R.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lee, S. -H.
Llena-Garde, M.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Makeev, A.
Martin, 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.
Naumann-Godo, M.
Nishino, S.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Parent, D.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Ripken, J.
Sada, T.
Sadrozinski, H. F. -W.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Strickman, M. S.
Strong, A. W.
Suson, D. J.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tramacere, A.
Uchiyama, Y.
Uehara, T.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vilchez, N.
Vitale, V.
Vladimirov, A. E.
Waite, A. P.
Wang, P.
Wood, K. S.
Yang, Z.
Ziegler, M.
TI CONSTRAINTS ON THE COSMIC-RAY DENSITY GRADIENT BEYOND THE SOLAR CIRCLE
FROM FERMI gamma-RAY OBSERVATIONS OF THE THIRD GALACTIC QUADRANT (vol
726, pg 81, 2011)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vladimirov, A. E.; Waite, A. P.; Wang, P.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vladimirov, A. E.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; 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.; Tibaldo, L.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brandt, T. J.; Knoedlseder, J.; Vilchez, N.] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Brandt, T. J.; Hughes, R. E.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[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.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] CSIC, Inst Ciencies Espai IEEC, E-08193 Barcelona, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Chekhtman, A.; Dermer, C. D.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, F-34095 Montpellier, France.
[Conrad, J.; Llena-Garde, M.; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.; Llena-Garde, M.; Ripken, J.; Yang, Z.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Ferrara, E. C.; Harding, A. K.; McEnery, J. E.; Thompson, D. J.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Itoh, R.; Katagiri, H.; Mizuno, T.; Nishino, S.; Sada, T.; Uehara, T.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Martin, P.; Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[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.
[Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, E-08010 Barcelona, Spain.
[Tramacere, A.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA.
[Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Ackermann, M (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM isabelle.grenier@cea.fr; mizuno@hep01.hepl.hiroshima-u.ac.jp;
luigi.tibaldo@pd.infn.it
RI Orlando, E/R-5594-2016; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016; Ozaki, Masanobu/K-1165-2013;
Rando, Riccardo/M-7179-2013; Johnson, Neil/G-3309-2014; Reimer,
Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Funk, Stefan/B-7629-2015;
Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015;
Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Torres,
Diego/O-9422-2016
OI Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario
/0000-0001-9325-4672; Reimer, Olaf/0000-0001-6953-1385; Morselli,
Aldo/0000-0002-7704-9553; 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; Torres, Diego/0000-0002-1522-9065
NR 1
TC 1
Z9 1
U1 0
U2 11
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 AUG 1
PY 2013
VL 772
IS 2
AR 154
DI 10.1088/0004-637X/772/2/154
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 186EL
UT WOS:000322024700076
ER
PT J
AU Green, JD
Ii, NJ
Kospal, A
Herczeg, G
Quanz, SP
Henning, T
van Kempen, TA
Lee, JE
Dunham, MM
Meeus, G
Bouwman, J
Chen, JH
Gudel, M
Skinner, SL
Liebhart, A
Merello, M
AF Green, Joel D.
Evans, Neal J., II
Kospal, Agnes
Herczeg, Gregory
Quanz, Sascha P.
Henning, Thomas
van Kempen, Tim A.
Lee, Jeong-Eun
Dunham, Michael M.
Meeus, Gwendolyn
Bouwman, Jeroen
Chen, Jo-hsin
Guedel, Manuel
Skinner, Stephen L.
Liebhart, Armin
Merello, Manuel
TI AN ANALYSIS OF THE ENVIRONMENTS OF FU ORIONIS OBJECTS WITH HERSCHEL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: jets and outflows; stars: individual (HBC 722, FU Orionis, V1057
Cyg, V1735 Cyg, V1331 Cyg, V1515 Cyg); stars: pre-main sequence; stars:
variables: T Tauri, Herbig Ae/Be; submillimeter: ISM
ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; LOW-MASS PROTOSTARS;
T-TAURI STARS; SPITZER-SPACE-TELESCOPE; MAIN-SEQUENCE STARS; LONG-TERM
EVOLUTION; BINARY-SYSTEM; EMBEDDED PROTOSTARS; PACS SPECTROSCOPY
AB We present Herschel-HIFI, SPIRE, and PACS 50-670 mu m imaging and spectroscopy of six FU Orionis-type objects and candidates (FU Orionis, V1735 Cyg, V1515 Cyg, V1057 Cyg, V1331 Cyg, and HBC 722), ranging in outburst date from 1936 to 2010, from the "FOOSH" (FU Orionis Objects Surveyed with Herschel) program, as well as ancillary results from Spitzer Infrared Spectrograph and the Caltech Submillimeter Observatory. In their system properties (L-bol, T-bol, and line emission), we find that FUors are in a variety of evolutionary states. Additionally, some FUors have features of both Class I and II sources: warm continuum consistent with Class II sources, but rotational line emission typical of Class I, far higher than Class II sources of similar mass/luminosity. Combining several classification techniques, we find an evolutionary sequence consistent with previous mid-IR indicators. We detect [O I] in every source at luminosities consistent with Class 0/I protostars, much greater than in Class II disks. We detect transitions of 13CO (J(up) of 5-8) around two sources (V1735 Cyg and HBC 722) but attribute them to nearby protostars. Of the remaining sources, three (FU Ori, V1515 Cyg, and V1331 Cyg) exhibit only low-lying CO, but one (V1057 Cyg) shows CO up to J = 23 -> 22 and evidence for H2O and OH emission, at strengths typical of protostars rather than T Tauri stars. Rotational temperatures for "cool" CO components range from 20 to 81 K, for similar to 10(50) total CO molecules. We detect [C I] and [N II] primarily as diffuse emission.
C1 [Green, Joel D.; Evans, Neal J., II; Merello, Manuel] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Kospal, Agnes] European Space Agcy ESA ESTEC, NL-2200 AG Noordwijk, Netherlands.
[Herczeg, Gregory] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Quanz, Sascha P.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Henning, Thomas; Bouwman, Jeroen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[van Kempen, Tim A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[van Kempen, Tim A.] Joint ALMA Off, Santiago, Chile.
[Lee, Jeong-Eun] Kyung Hee Univ, Dept Astron & Space Sci, Gyeonggi 446701, South Korea.
[Dunham, Michael M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Meeus, Gwendolyn] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Chen, Jo-hsin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Guedel, Manuel; Liebhart, Armin] Univ Vienna, Dept Astrophys, A-1010 Vienna, Austria.
[Skinner, Stephen L.] Univ Colorado, Ctr Astrophys & Space Astron CASA, Boulder, CO 80309 USA.
RP Green, JD (reprint author), Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA.
EM joel@astro.as.utexas.edu
RI Lee , Jeong-Eun/E-2387-2013; Guedel, Manuel/C-8486-2015;
OI Guedel, Manuel/0000-0001-9818-0588; Herczeg, Gregory/0000-0002-7154-6065
FU Herschel Open Time Key Project Program; NASA; Jet Propulsion Laboratory;
California Institute of Technology; Basic Science Research Program
through the National Research Foundation of Korea (NRF); Ministry of
Education, Science, and Technology [2012044689]; Austrian Research
Promotion Agency (FFG) through the ASAP initiative of the Austrian
Federal Ministry for Transport, Innovation, and Technology (BMVIT);
National Science Foundation [AST-0838261]; National Aeronautics; Space
Administration; National Science Foundation
FX Support for this work, part of the Herschel Open Time Key Project
Program, was provided by NASA through an award issued by the Jet
Propulsion Laboratory, California Institute of Technology. The authors
wish to acknowledge the Herschel Director, G.L. Pilbratt, for the timely
approval and execution of the Target of Opportunity program, and Ivan
Valtchanov and the Herschel Helpdesk for its assistance in timely data
reduction. The authors also thank Michelle Rascati and Roderik Overzier
for assistance in data reduction, and Colette Salyk, Amanda Heiderman,
Isa Oliveira, Tom Megeath, Will Fischer, Manoj Puravankara, and Geoff
Blake for helpful discussions, and the anonymous referee whose comments
greatly improved the manuscript. The research of J.E.L. is supported by
Basic Science Research Program through the National Research Foundation
of Korea (NRF) funded by the Ministry of Education, Science, and
Technology (No. 2012044689). The research of M.G. and A.L. has been
supported by the Austrian Research Promotion Agency (FFG) through the
ASAP initiative of the Austrian Federal Ministry for Transport,
Innovation, and Technology (BMVIT). This material is based upon work at
the Caltech Submillimeter Observatory, which is operated by the
California Institute of Technology under cooperative agreement with the
National Science Foundation (AST-0838261). 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 86
TC 11
Z9 11
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 AUG 1
PY 2013
VL 772
IS 2
AR UNSP 117
DI 10.1088/0004-637X/772/2/117
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 186EL
UT WOS:000322024700039
ER
PT J
AU Leenaarts, J
Pereira, TMD
Carlsson, M
Uitenbroek, H
De Pontieu, B
AF Leenaarts, J.
Pereira, T. M. D.
Carlsson, M.
Uitenbroek, H.
De Pontieu, B.
TI THE FORMATION OF IRIS DIAGNOSTICS. I. A QUINTESSENTIAL MODEL ATOM OF Mg
II AND GENERAL FORMATION PROPERTIES OF THE Mg II h&k LINES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radiative transfer; Sun: atmosphere; Sun: chromosphere
ID SOLAR TRANSITION REGION; RADIATIVE-TRANSFER; LPSP INSTRUMENT; PARTIAL
REDISTRIBUTION; HYDROGEN IONIZATION; RESONANCE LINES; ENERGY-BALANCE;
CALCIUM H; L-ALPHA; CHROMOSPHERE
AB NASA's Interface Region Imaging Spectrograph (IRIS) space mission will study how the solar atmosphere is energized. IRIS contains an imaging spectrograph that covers the Mg II h&k lines as well as a slit-jaw imager centered at Mg II k. Understanding the observations will require forward modeling of Mg II h&k line formation from three-dimensional (3D) radiation-MHD models. This paper is the first in a series where we undertake this forward modeling. We discuss the atomic physics pertinent to h&k line formation, present a quintessential model atom that can be used in radiative transfer computations, and discuss the effect of partial redistribution (PRD) and 3D radiative transfer on the emergent line profiles. We conclude that Mg II h&k can be modeled accurately with a four-level plus continuum Mg II model atom. Ideally radiative transfer computations should be done in 3D including PRD effects. In practice this is currently not possible. A reasonable compromise is to use one-dimensional PRD computations to model the line profile up to and including the central emission peaks, and use 3D transfer assuming complete redistribution to model the central depression.
C1 [Leenaarts, J.; Pereira, T. M. D.; Carlsson, M.; De Pontieu, B.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Pereira, T. M. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pereira, T. M. D.; De Pontieu, B.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Uitenbroek, H.] NSO Sacramento Peak, Sunspot, NM 88349 USA.
RP Leenaarts, J (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway.
EM jorritl@astro.uio.no; tiago.pereira@astro.uio.no;
mats.carlsson@astro.uio.no; huitenbroek@nso.edu; bdp@lmsal.com
RI Pereira, Tiago/G-4079-2014;
OI Pereira, Tiago/0000-0003-4747-4329; Leenaarts,
Jorrit/0000-0003-4936-4211
FU Netherlands Organization for Scientific Research (NWO); Research Council
of Norway through the European Research Council under the European Union
[291058]; Research Council of Norway; High End Computing Division of
NASA [s1061]; NASA Postdoctoral Program at Ames Research Center
[NNH06CC03B]; NASA [NNX08AH45G, NNX08BA99G, NNX11AN98G, NNG09FA40C]
FX J.L. recognizes support from the Netherlands Organization for Scientific
Research (NWO). This research was supported by the Research Council of
Norway through the grant "Solar Atmospheric Modeling," from the European
Research Council under the European Union's Seventh Framework Programme
(FP7/2007-2013)/ERC grant agreement No. 291058, and through grants of
computing time from the Programme for Supercomputing of the Research
Council of Norway and computing project s1061 from the High End
Computing Division of NASA. T.M.D.P. was supported by the NASA
Postdoctoral Program at Ames Research Center (grant NNH06CC03B). B.D.P.
acknowledges support from NASA grants NNX08AH45G, NNX08BA99G,
NNX11AN98G, and NNG09FA40C (IRIS). We thank Paul Barklem for pointing
out the paper on collisions with neutral hydrogen.
NR 54
TC 44
Z9 44
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 AUG 1
PY 2013
VL 772
IS 2
AR 89
DI 10.1088/0004-637X/772/2/89
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 186EL
UT WOS:000322024700011
ER
PT J
AU Leenaarts, J
Pereira, TMD
Carlsson, M
Uitenbroek, H
De Pontieu, B
AF Leenaarts, J.
Pereira, T. M. D.
Carlsson, M.
Uitenbroek, H.
De Pontieu, B.
TI THE FORMATION OF IRIS DIAGNOSTICS. II. THE FORMATION OF THE Mg II h&k
LINES IN THE SOLAR ATMOSPHERE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radiative transfer; Sun: atmosphere; Sun: chromosphere
ID RADIATIVE-TRANSFER; HIGH-RESOLUTION; STELLAR ATMOSPHERES; HYDROGEN
IONIZATION; CHROMOSPHERE; SIMULATIONS; QUIET; SCATTERING; PROFILES;
SPICULES
AB NASA's Interface Region Imaging Spectrograph (IRIS) small explorer mission will study how the solar atmosphere is energized. IRIS contains an imaging spectrograph that covers the Mg II h&k lines as well as a slit-jaw imager centered at Mg II k. Understanding the observations requires forward modeling of Mg II h&k line formation from three-dimensional (3D) radiation-magnetohydrodynamic (RMHD) models. This paper is the second in a series where we undertake this modeling. We compute the vertically emergent h&k intensity from a snapshot of a dynamic 3D RMHD model of the solar atmosphere, and investigate which diagnostic information about the atmosphere is contained in the synthetic line profiles. We find that the Doppler shift of the central line depression correlates strongly with the vertical velocity at optical depth unity, which is typically located less than 200 km below the transition region (TR). By combining the Doppler shifts of the h and k lines we can retrieve the sign of the velocity gradient just below the TR. The intensity in the central line depression is anti-correlated with the formation height, especially in subfields of a few square Mm. This intensity could thus be used to measure the spatial variation of the height of the TR. The intensity in the line-core emission peaks correlates with the temperature at its formation height, especially for strong emission peaks. The peaks can thus be exploited as a temperature diagnostic. The wavelength difference between the blue and red peaks provides a diagnostic of the velocity gradients in the upper chromosphere. The intensity ratio of the blue and red peaks correlates strongly with the average velocity in the upper chromosphere. We conclude that the Mg II h&k lines are excellent probes of the very upper chromosphere just below the TR, a height regime that is impossible to probe with other spectral lines. They also provide decent temperature and velocity diagnostics of the middle chromosphere.
C1 [Leenaarts, J.; Pereira, T. M. D.; Carlsson, M.; De Pontieu, B.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway.
[Pereira, T. M. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pereira, T. M. D.; De Pontieu, B.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Uitenbroek, H.] NSO Sacramento Peak, Sunspot, NM 88349 USA.
RP Leenaarts, J (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway.
EM jorritl@astro.uio.no; tiago.pereira@astro.uio.no;
mats.carlsson@astro.uio.no; huitenbroek@nso.edu; bdp@lmsal.com
RI Pereira, Tiago/G-4079-2014;
OI Pereira, Tiago/0000-0003-4747-4329; Leenaarts,
Jorrit/0000-0003-4936-4211
FU Netherlands Organization for Scientific Research (NWO); Research Council
of Norway; European Research Council under the European Union [291058];
High End Computing Division of NASA [s1061]; NASA Postdoctoral Program
at Ames Research Center [NNH06CC03B]; NASA [NNX08AH45G, NNX08BA99G,
NNX11AN98G, NNG09FA40C]
FX J.L. recognizes support from the Netherlands Organization for Scientific
Research (NWO). This research was supported by the Research Council of
Norway through the grant "Solar Atmospheric Modelling" and through
grants of computing time from the Programme for Supercomputing, by the
European Research Council under the European Union's Seventh Framework
Programme (FP7/2007-2013)/ERC Grant agreement No. 291058, and by the
computing project s1061 from the High End Computing Division of NASA.
T.M.D.P. was supported by the NASA Postdoctoral Program at Ames Research
Center (grant NNH06CC03B). B.D.P. acknowledges support from NASA grants
NNX08AH45G, NNX08BA99G, NNX11AN98G, and NNG09FA40C (IRIS).
NR 34
TC 57
Z9 57
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 AUG 1
PY 2013
VL 772
IS 2
AR 90
DI 10.1088/0004-637X/772/2/90
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 186EL
UT WOS:000322024700012
ER
PT J
AU Luo, B
Brandt, WN
Alexander, DM
Harrison, FA
Stern, D
Bauer, FE
Boggs, SE
Christensen, FE
Comastri, A
Craig, WW
Fabian, AC
Farrah, D
Fiore, F
Fuerst, F
Grefenstette, BW
Hailey, CJ
Hickox, R
Madsen, KK
Matt, G
Ogle, P
Risaliti, G
Saez, C
Teng, SH
Walton, DJ
Zhang, WW
AF Luo, B.
Brandt, W. N.
Alexander, D. M.
Harrison, F. A.
Stern, D.
Bauer, F. E.
Boggs, S. E.
Christensen, F. E.
Comastri, A.
Craig, W. W.
Fabian, A. C.
Farrah, D.
Fiore, F.
Fuerst, F.
Grefenstette, B. W.
Hailey, C. J.
Hickox, R.
Madsen, K. K.
Matt, G.
Ogle, P.
Risaliti, G.
Saez, C.
Teng, S. H.
Walton, D. J.
Zhang, W. W.
TI WEAK HARD X-RAY EMISSION FROM TWO BROAD ABSORPTION LINE QUASARS OBSERVED
WITH NuSTAR: COMPTON-THICK ABSORPTION OR INTRINSIC X-RAY WEAKNESS?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies: active; galaxies: nuclei; quasars:
absorption lines; quasars: emission lines; X-rays: general
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SPECTRAL
ENERGY-DISTRIBUTIONS; OPTICALLY SELECTED QUASARS; XMM-NEWTON
SPECTROSCOPY; HUBBLE-SPACE-TELESCOPE; ACCRETION DISK WINDS; RADIO-LOUD
QUASARS; SEYFERT 1 GALAXIES; 7TH DATA RELEASE
AB We present Nuclear Spectroscopic Telescope Array (NuSTAR) hard X-ray observations of two X-ray weak broad absorption line (BAL) quasars, PG 1004+130 (radio loud) and PG 1700+518 (radio quiet). Many BAL quasars appear X-ray weak, probably due to absorption by the shielding gas between the nucleus and the accretion-disk wind. The two targets are among the optically brightest BAL quasars, yet they are known to be significantly X-ray weak at rest-frame 2-10 keV (16-120 times fainter than typical quasars). We would expect to obtain approximate to 400-600 hard X-ray (greater than or similar to 10 keV) photons with NuSTAR, provided that these photons are not significantly absorbed (N-H less than or similar to 10(24) cm(-2)). However, both BAL quasars are only detected in the softer NuSTAR bands (e.g., 4-20 keV) but not in its harder bands (e.g., 20-30 keV), suggesting that either the shielding gas is highly Compton-thick or the two targets are intrinsically X-ray weak. We constrain the column densities for both to be N-H approximate to 7 x 10(24) cm(-2) if the weak hard X-ray emission is caused by obscuration from the shielding gas. We discuss a few possibilities for how PG 1004+130 could have Compton-thick shielding gas without strong Fe K alpha line emission; dilution from jet-linked X-ray emission is one likely explanation. We also discuss the intrinsic X-ray weakness scenario based on a coronal-quenching model relevant to the shielding gas and disk wind of BAL quasars. Motivated by our NuSTAR results, we perform a Chandra stacking analysis with the Large Bright Quasar Survey BAL quasar sample and place statistical constraints upon the fraction of intrinsically X-ray weak BAL quasars; this fraction is likely 17%-40%.
C1 [Luo, B.; Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Luo, B.; Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Alexander, D. M.; Hickox, R.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Harrison, F. A.; Fuerst, F.; Grefenstette, B. W.; Madsen, K. K.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, F. E.; Saez, C.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Comastri, A.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Fiore, F.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Hickox, R.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Ogle, P.] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Risaliti, G.] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Teng, S. H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Luo, B (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
RI Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015; Comastri,
Andrea/O-9543-2015;
OI Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453;
Comastri, Andrea/0000-0003-3451-9970; Risaliti,
Guido/0000-0002-3556-977X; Alexander, David/0000-0002-5896-6313; Fiore,
Fabrizio/0000-0002-4031-4157
FU California Institute of Technology (Caltech) NuSTAR [44A-1092750]; NASA
ADP Grant [NNX10AC99G]; Leverhulme trust; Science Technology and
Facilities Council; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT
1101024, Anillo ACT1101, FONDECYT 3120198]; NASA [NNG08FD60C]; National
Aeronautics and Space Administration
FX We acknowledge support from the California Institute of Technology
(Caltech) NuSTAR subcontract 44A-1092750 (B.L. and W.N.B.), NASA ADP
Grant NNX10AC99G (B.L. and W.N.B.), the Leverhulme trust and the Science
Technology and Facilities Council (D.M.A.), Basal-CATA Grant PFB-06/2007
and CONICYT-Chile Grants FONDECYT 1101024 and Anillo ACT1101 (F.E.B.),
and CONICYT-Chile Grant FONDECYT 3120198 (C.S.). We thank M. Young for
help with the planning of this project and K. Forster for help with the
NuSTAR data access, and we thank M. Balokovic, K. Boydstun, T. N. Lu, B.
P. Miller, Jianfeng Wu, and T. Yaqoob for helpful discussions. We thank
the referee, S. C. Gallagher, for carefully reviewing the manuscript and
providing helpful comments.; This work was supported under NASA contract
No. NNG08FD60C, and made use of data from the NuSTAR mission, a project
led by Caltech, managed by the Jet Propulsion Laboratory, and funded by
the National Aeronautics and Space Administration. We thank the NuSTAR
Operations, Software and Calibration teams for support with the
execution and analysis of these observations. This research has made use
of NuSTAR-DAS jointly developed by the ASI Science Data Center (ASDC,
Italy) and Caltech (USA).
NR 146
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2013
VL 772
IS 2
AR 153
DI 10.1088/0004-637X/772/2/153
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 186EL
UT WOS:000322024700075
ER
PT J
AU Takami, M
Karr, JL
Hashimoto, J
Kim, H
Wisniewski, J
Henning, T
Grady, CA
Kandori, R
Hodapp, KW
Kudo, T
Kusakabe, N
Chou, MY
Itoh, Y
Momose, M
Mayama, S
Currie, T
Follette, KB
Kwon, J
Abe, L
Brandner, W
Brandt, TD
Carson, J
Egner, SE
Feldt, M
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Ishii, M
Iye, M
Janson, M
Knapp, GR
Kuzuhara, M
McElwain, MW
Matsuo, T
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 Takami, Michihiro
Karr, Jennifer L.
Hashimoto, Jun
Kim, Hyosun
Wisniewski, John
Henning, Thomas
Grady, Carol A.
Kandori, Ryo
Hodapp, Klaus W.
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Chou, Mei-Yin
Itoh, Yoichi
Momose, Munetake
Mayama, Satoshi
Currie, Thayne
Follette, Katherine B.
Kwon, Jungmi
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph
Egner, Sebastian E.
Feldt, Markus
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko
Ishii, Miki
Iye, Masanori
Janson, Markus
Knapp, Gillian R.
Kuzuhara, Masayuki
McElwain, Michael W.
Matsuo, Taro
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Serabyn, Eugene
Suto, Hiroshi
Suzuki, Ryuji
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Watanabe, Makoto
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
Tamura, Motohide
TI HIGH-CONTRAST NEAR-INFRARED IMAGING POLARIMETRY OF THE PROTOPLANETARY
DISK AROUND RY TAU
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE polarization; protoplanetary disks; stars: individual (RY Tau); stars:
pre-main sequence
ID SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; 2-DIMENSIONAL
RADIATIVE-TRANSFER; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISK;
SCATTERED-LIGHT; PROTOSTELLAR ENVELOPES; TRANSITIONAL DISK;
OPTICAL-PROPERTIES; SIZE DISTRIBUTION
AB We present near-infrared coronagraphic imaging polarimetry of RY Tau. The scattered light in the circumstellar environment was imaged at the H band at a high resolution (similar to 0 ''.05) for the first time, using Subaru/HiCIAO. The observed polarized intensity (PI) distribution shows a butterfly-like distribution of bright emission with an angular scale similar to the disk observed at millimeter wavelengths. This distribution is offset toward the blueshifted jet, indicating the presence of a geometrically thick disk or a remnant envelope, and therefore the earliest stage of the Class II evolutionary phase. We perform comparisons between the observed PI distribution and disk models with (1) full radiative transfer code, using the spectral energy distribution (SED) to constrain the disk parameters; and (2) monochromatic simulations of scattered light which explore a wide range of parameters space to constrain the disk and dust parameters. We show that these models cannot consistently explain the observed PI distribution, SED, and the viewing angle inferred by millimeter interferometry. We suggest that the scattered light in the near-infrared is associated with an optically thin and geometrically thick layer above the disk surface, with the surface responsible for the infrared SED. Half of the scattered light and thermal radiation in this layer illuminates the disk surface, and this process may significantly affect the thermal structure of the disk.
C1 [Takami, Michihiro; Karr, Jennifer L.; Kim, Hyosun; Chou, Mei-Yin] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Hashimoto, Jun; Kandori, Ryo; Kusakabe, Nobuhiko; Kwon, Jungmi; Hayashi, Masahiko; Iye, Masanori; Miyama, Shoken; Morino, Jun-Ichi; Suto, Hiroshi; Suzuki, Ryuji; Takami, Hideki; Tamura, Motohide] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Henning, Thomas; Brandner, Wolfgang; Feldt, Markus] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA.
[Grady, Carol A.; Currie, Thayne; McElwain, Michael W.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Kudo, Tomoyuki; Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Ishii, Miki; Kuzuhara, Masayuki; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Usuda, Tomonori] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Itoh, Yoichi] Univ Hyogo, Ctr Astron, Nishi Harima Astron Observ, Sayo, Hyogo 6795313, Japan.
[Momose, Munetake] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
[Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Follette, Katherine B.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Kwon, Jungmi] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06108 Nice 2, France.
[Brandt, Timothy D.; Janson, Markus; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Kuzuhara, Masayuki] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Moro-Martin, Amaya] CAB CSIC INTA, Dept Astrophys, E-28850 Madrid, Spain.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Thalmann, Christian] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Takami, M (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
EM hiro@asiaa.sinica.edu.tw
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
FU National Science Council of Taiwan [100-2112-M-001-007-MY3]; NSF-AST
[1009314, 1009203, 1008440]
FX We are grateful to an anonymous referee for a thorough review and
valuable comments. We thank support from the Subaru Telescope staff,
especially from Michael Lemmen for making our observations successful.
We thank Drs. Shigehisa Takakuwa and Yasuhiro Hasegawa for useful
discussion. This research made use of the Simbad data base operated at
CDS, Strasbourg, France, and the NASA's Astrophysics Data System
Abstract Service. M. T. is supported from National Science Council of
Taiwan (grant No. 100-2112-M-001-007-MY3). J.P.W. is supported by
NSF-AST 1009314. J.C. was supported by NSF-AST 1009203. C. A. G.
acknowledges support under NSF AST 1008440.
NR 81
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2013
VL 772
IS 2
AR 145
DI 10.1088/0004-637X/772/2/145
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 186EL
UT WOS:000322024700067
ER
PT J
AU Brooks, DH
Warren, HP
Ugarte-Urra, I
Winebarger, AR
AF Brooks, David H.
Warren, Harry P.
Ugarte-Urra, Ignacio
Winebarger, Amy R.
TI HIGH SPATIAL RESOLUTION OBSERVATIONS OF LOOPS IN THE SOLAR CORONA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE magnetic fields; Sun: corona; Sun: UV radiation
ID ACTIVE-REGION LOOPS; TRANSITION-REGION; EXPLORER; TRACE; HINODE
AB Understanding how the solar corona is structured is of fundamental importance to determine how the Sun's upper atmosphere is heated to high temperatures. Recent spectroscopic studies have suggested that an instrument with a spatial resolution of 200 km or better is necessary to resolve coronal loops. The High Resolution Coronal Imager (Hi-C) achieved this performance on a rocket flight in 2012 July. We use Hi-C data to measure the Gaussian widths of 91 loops observed in the solar corona and find a distribution that peaks at about 270 km. We also use Atmospheric Imaging Assembly data for a subset of these loops and find temperature distributions that are generally very narrow. These observations provide further evidence that loops in the solar corona are often structured at a scale of several hundred kilometers, well above the spatial scale of many proposed physical mechanisms.
C1 [Brooks, David H.; Ugarte-Urra, Ignacio] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Warren, Harry P.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Winebarger, Amy R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Brooks, DH (reprint author), ISAS JAXA, Hinode Team, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
OI Ugarte-Urra, Ignacio/0000-0001-5503-0491
FU NASA Hinode program; Naval Research Laboratory
FX We acknowledge the High resolution Coronal Imager instrument team for
making the flight data publicly available. MSFC/NASA led the mission and
partners include the Smithsonian Astrophysical Observatory in Cambridge,
Massachusetts; Lockheed Martin's Solar Astrophysical Laboratory in
PaloAlto, California; the University of Central Lancashire in
Lancashire, England; and the Lebedev Physical Institute of the Russian
Academy of Sciences in Moscow. This work was performed under contract
with the Naval Research Laboratory and was funded by the NASA Hinode
program. 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).
NR 19
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 1
PY 2013
VL 772
IS 2
AR L19
DI 10.1088/2041-8205/772/2/L19
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 186CR
UT WOS:000322020000006
ER
PT J
AU Van Dyk, SD
Zheng, WK
Clubb, KI
Filippenko, AV
Cenko, SB
Smith, N
Fox, OD
Kelly, PL
Shivvers, I
Ganeshalingam, M
AF Van Dyk, Schuyler D.
Zheng, WeiKang
Clubb, Kelsey I.
Filippenko, Alexei V.
Cenko, S. Bradley
Smith, Nathan
Fox, Ori D.
Kelly, Patrick L.
Shivvers, Isaac
Ganeshalingam, Mohan
TI THE PROGENITOR OF SUPERNOVA 2011dh HAS VANISHED
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: individual (NGC 5194); stars: evolution; supernovae: general;
supernovae: individual (SN 2011dh)
ID RED SUPERGIANT PROGENITOR; SN 2011DH; IIB SUPERNOVA; EVOLUTION; 1993J;
STAR; M51; SPECTRA; COMPACT; SEARCH
AB We conducted Hubble Space Telescope (HST) Snapshot observations of the Type IIb supernova (SN) 2011dh in M51 at an age of similar to 641 days with the Wide Field Camera 3. We find that the yellow supergiant star, clearly detected in pre-SN HST images, has disappeared, implying that this star was almost certainly the progenitor of the SN. Interpretation of the early time SN data which led to the inference of a compact nature for the progenitor, and to the expected survival of this yellow supergiant, is now clearly incorrect. We also present ground-based UBVRI light curves obtained with the Katzman Automatic Imaging Telescope at Lick Observatory up to SN age similar to 70 days. From the light-curve shape including the very late time HST data, and from recent interacting binary models for SN 2011dh, we estimate that a putative surviving companion star to the now deceased yellow supergiant could be detectable by late 2013, especially in the ultraviolet. No obvious light echoes are detectable yet in the SN environment.
C1 [Van Dyk, Schuyler D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Zheng, WeiKang; Clubb, Kelsey I.; Filippenko, Alexei V.; Cenko, S. Bradley; Fox, Ori D.; Kelly, Patrick L.; Shivvers, Isaac] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85720 USA.
[Ganeshalingam, Mohan] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP Van Dyk, SD (reprint author), CALTECH, Spitzer Sci Ctr, Mailcode 220-6, Pasadena, CA 91125 USA.
EM vandyk@ipac.caltech.edu
OI Shivvers, Isaac/0000-0003-3373-8047; Van Dyk,
Schuyler/0000-0001-9038-9950
FU NASA [NAS 05-26555]; NASA from STScI [AR-12623, GO-13029]; Richard and
Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; NSF
[AST-1211916]
FX This work is based in part on observations made with the NASA/ESA Hubble
Space Telescope, obtained from the Data Archive at the Space Telescope
Science Institute (STScI), which is operated by the Association of
Universities for Research in Astronomy (AURA), Inc., under NASA contract
NAS 05-26555. KAIT and its ongoing research were made possible by
donations from Sun Microsystems, Inc., the Hewlett-Packard Company,
AutoScope Corporation, Lick Observatory, the NSF, the University of
California, the Sylvia & Jim Katzman Foundation, and the TABASGO
Foundation. Support for this research was provided by NASA through
grants AR-12623 and GO-13029 from STScI. A.V.F. and his group at UC
Berkeley also wish to acknowledge generous support from Gary and Cynthia
Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich
Fund, the TABASGO Foundation, and NSF grant AST-1211916.
NR 43
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 1
PY 2013
VL 772
IS 2
AR L32
DI 10.1088/2041-8205/772/2/L32
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 186CR
UT WOS:000322020000019
ER
PT J
AU Song, H
Lin, WY
Lin, YL
Wolf, AB
Neggers, R
Donner, LJ
Del Genio, AD
Liu, YG
AF Song, Hua
Lin, Wuyin
Lin, Yanluan
Wolf, Audrey B.
Neggers, Roel
Donner, Leo J.
Del Genio, Anthony D.
Liu, Yangang
TI Evaluation of Precipitation Simulated by Seven SCMs against the ARM
Observations at the SGP Site
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Model comparison; Model evaluation; performance; Single column models
ID SINGLE-COLUMN MODEL; GENERAL-CIRCULATION MODELS; LARGE-SCALE MODELS;
COMMUNITY ATMOSPHERE MODEL; DIURNAL CYCLE; CUMULUS PARAMETERIZATION;
CONVECTIVE PRECIPITATION; CLIMATE SIMULATIONS; MOIST CONVECTION;
GREAT-PLAINS
AB This study evaluates the performances of seven single-column models (SCMs) by comparing simulated surface precipitation with observations at the Atmospheric Radiation Measurement Program Southern Great Plains (SGP) site from January 1999 to December 2001. Results show that although most SCMs can reproduce the observed precipitation reasonably well, there are significant and interesting differences in their details. In the cold season, the model-observation differences in the frequency and mean intensity of rain events tend to compensate each other for most SCMs. In the warm season, most SCMs produce more rain events in daytime than in nighttime, whereas the observations have more rain events in nighttime. The mean intensities of rain events in these SCMs are much stronger in daytime, but weaker in nighttime, than the observations. The higher frequency of rain events during warm-season daytime in most SCMs is related to the fact that most SCMs produce a spurious precipitation peak around the regime of weak vertical motions but rich in moisture content. The models also show distinct biases between nighttime and daytime in simulating significant rain events. In nighttime, all the SCMs have a lower frequency of moderate-to-strong rain events than the observations for both seasons. In daytime, most SCMs have a higher frequency of moderate-to-strong rain events than the observations, especially in the warm season. Further analysis reveals distinct meteorological backgrounds for large underestimation and overestimation events. The former occur in the strong ascending regimes with negative low-level horizontal heat and moisture advection, whereas the latter occur in the weak or moderate ascending regimes with positive low-level horizontal heat and moisture advection.
C1 [Song, Hua; Lin, Wuyin; Lin, Yanluan; Liu, Yangang] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Lin, Yanluan; Donner, Leo J.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Wolf, Audrey B.] Columbia Univ, New York, NY USA.
[Neggers, Roel] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
[Del Genio, Anthony D.] NASA Goddard Inst Space Studies, New York, NY USA.
RP Song, H (reprint author), Brookhaven Natl Lab, Div Atmospher Sci, 75 Rutherford Dr,Bldg 815E, Upton, NY 11973 USA.
EM hsong@bnl.gov
RI Liu, Yangang/H-6154-2011; lin, yanluan/A-6333-2015
FU U.S. Department of Energy Earth System Modeling (ESM) program
FX This work is part of the FASTER project (http://www.bnl.gov/faster/)
supported by the U.S. Department of Energy Earth System Modeling (ESM)
program. The authors thank the two anonymous reviewers for their
constructive comments. The first author also would like to express her
sincere gratitude to her former advisor Dr. Minghua Zhang for his
incessant support and encouragement throughout her research.
NR 60
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U1 0
U2 16
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 AUG
PY 2013
VL 26
IS 15
BP 5467
EP 5492
DI 10.1175/JCLI-D-12-00263.1
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 190GP
UT WOS:000322327700010
ER
PT J
AU Kim, J
Waliser, DE
Mattmann, CA
Mearns, LO
Goodale, CE
Hart, AF
Crichton, DJ
McGinnis, S
Lee, H
Loikith, PC
Boustani, M
AF Kim, Jinwon
Waliser, Duane E.
Mattmann, Chris A.
Mearns, Linda O.
Goodale, Cameron E.
Hart, Andrew F.
Crichton, Dan J.
McGinnis, Seth
Lee, Huikyo
Loikith, Paul C.
Boustani, Maziyar
TI Evaluation of the Surface Climatology over the Conterminous United
States in the North American Regional Climate Change Assessment Program
Hindcast Experiment Using a Regional Climate Model Evaluation System
SO JOURNAL OF CLIMATE
LA English
DT Article
DE North America; Model errors; Model evaluation; performance; Policy;
Regional effects
ID PRECIPITATION REGIME; SEASON PRECIPITATION; VARIABILITY; CALIFORNIA;
SIMULATIONS; CIRCULATION; MONSOON; REGCM2
AB Surface air temperature, precipitation, and insolation over the conterminous United States region from the North American Regional Climate Change Assessment Program (NARCCAP) regional climate model (RCM) hindcast study are evaluated using the Jet Propulsion Laboratory (JPL) Regional Climate Model Evaluation System (RCMES). All RCMs reasonably simulate the observed climatology of these variables. RCM skill varies more widely for the magnitude of spatial variability than the pattern. The multimodel ensemble is among the best performers for all these variables. Systematic biases occur across these RCMs for the annual means, with warm biases over the Great Plains (GP) and cold biases in the Atlantic and the Gulf of Mexico (GM) coastal regions. Wet biases in the Pacific Northwest and dry biases in the GM/southern Great Plains also occur in most RCMs. All RCMs suffer problems in simulating summer rainfall in the Arizona-New Mexico region. RCMs generally overestimate surface insolation, especially in the eastern United States. Negative correlation between the biases in insolation and precipitation suggest that these two fields are related, likely via clouds. Systematic variations in biases for regions, seasons, variables, and metrics suggest that the bias correction in applying climate model data to assess the climate impact on various sectors must be performed accordingly. Precipitation evaluation with multiple observations reveals that observational data can be an important source of uncertainties in model evaluation; thus, cross examination of observational data is important for model evaluation.
C1 [Kim, Jinwon; Waliser, Duane E.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Waliser, Duane E.; Mattmann, Chris A.; Goodale, Cameron E.; Hart, Andrew F.; Crichton, Dan J.; Lee, Huikyo; Loikith, Paul C.; Boustani, Maziyar] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Mearns, Linda O.; McGinnis, Seth] Natl Ctr Atmospher Res, Inst Math Applicat Geosci, Boulder, CO 80307 USA.
RP Kim, J (reprint author), Univ Calif Los Angeles, JIFRESSE, 607 Charles E Young Dr East,Young Hall,Room 4242, Los Angeles, CA 90095 USA.
EM jkim@atmos.ucla.edu
OI McGinnis, Seth/0000-0001-8082-834X
FU American Recovery and Re-investment Act (ARRA); NASA AIST project
[AIST-QRS-12-0002]; NSF ExArch project [1125798]; NSF EaSM project
[2011-67004-30224]; NSF; U.S. Department of Energy; NOAA; U.S. EPA
Office of Research and Development; National Aeronautics and Space
Administration; NASA NCA project [11-NCA11-0028]
FX We thank Dr. Guan for making the Taylor diagrams. This study was
supported by the American Recovery and Re-investment Act (ARRA), NASA
NCA (ID 11-NCA11-0028), NASA AIST (AIST-QRS-12-0002), NSF ExArch (ID
1125798), and NSF EaSM (ID 2011-67004-30224) projects. The North
American Regional Climate Change Assessment Program (NARCCAP) is funded
by NSF, the U.S. Department of Energy, NOAA, and the U.S. EPA Office of
Research and Development. The contribution from D. E. Waliser, C.
Mattmann, C. Goodale, A. Hart, P. Zimdars, D. Crichton, H. Kyo, P.
Loikith, and M. Boustani to this study was performed on behalf of the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 53
TC 8
Z9 8
U1 2
U2 31
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 AUG
PY 2013
VL 26
IS 15
BP 5698
EP 5715
DI 10.1175/JCLI-D-12-00452.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 190GP
UT WOS:000322327700025
ER
PT J
AU Leppert, KD
Cecil, DJ
Petersen, WA
AF Leppert, Kenneth D., II
Cecil, Daniel J.
Petersen, Walter A.
TI Relation between Tropical Easterly Waves, Convection, and Tropical
Cyclogenesis: A Lagrangian Perspective
SO MONTHLY WEATHER REVIEW
LA English
DT Article
DE Convection; Cyclogenesis; cyclolysis; Lightning; Tropical cyclones
ID TRMM PRECIPITATION RADAR; OPTICAL TRANSIENT DETECTOR; RAIN-PROFILING
ALGORITHM; NUMERICAL-SIMULATION; PASSIVE MICROWAVE; HURRICANE SEASON;
HOT TOWERS; PART I; SYSTEMS; ATLANTIC
AB In this study, a wave-following Lagrangian framework was used to examine the evolution of tropical easterly wave structure, circulation, and convection in the days leading up to and including tropical cyclogenesis in the Atlantic and east Pacific basins. After easterly waves were separated into northerly, southerly, trough, and ridge phases using the National Centers for Environmental Prediction-National Center for Atmospheric Research reanalysis 700-hPa meridional wind, waves that developed a tropical cyclone [developing waves (DWs)] and waves that never developed a cyclone [nondeveloping waves (NDWs)] were identified. Day zero (D0) was defined as the day on which a tropical depression was identified for DWs or the day the waves achieved maximum 850-hPa vorticity for NDWs. Both waves types were then traced from five days prior to D0 (D - 5) through one day after D0. Results suggest that as genesis is approached for DWs, the coverage by convection and cold cloudiness (e.g., fractional coverage by infrared brightness temperatures 240 K) increases, while convective intensity (e.g., lightning flash rate) decreases. Therefore, the coverage by convection appears to be more important than the intensity of convection for tropical cyclogenesis. In contrast, convective coverage and intensity both increase from D - 5 to D0 for NDWs. Compared to NDWs, DWs are associated with significantly greater coverage by cold cloudiness, large-scale moisture throughout a deep layer, and large-scale, upper-level (similar to 200 hPa) divergence, especially within the trough and southerly phases, suggesting that these parameters are most important for cyclogenesis and for distinguishing DWs from NDWs.
C1 [Leppert, Kenneth D., II; Cecil, Daniel J.] Univ Alabama, Huntsville, AL 35899 USA.
[Petersen, Walter A.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP Leppert, KD (reprint author), NSSTC, 320 Sparkman Dr,Rm 4074, Huntsville, AL 35805 USA.
EM leppert@nsstc.uah.edu
FU NASA Earth and Space Science Fellowship [NNX09AO40H]
FX Funding for this research was generously provided through a NASA Earth
and Space Science Fellowship, Grant NNX09AO40H, in support of the lead
author's research for his doctoral degree. The authors wish to thank two
anonymous reviewers for their helpful comments and suggestions for
improving the manuscript. The authors would also like to gratefully
acknowledge the Goddard Earth Sciences Data and Information Services
Center for providing the TMI, PR, and IR brightness temperature data,
the NASA EOSDIS Global Hydrology Resource Center DAAC for providing the
LIS science data, and the NOAA/OAR/ESRL PSD for providing the NCEP-NCAR
re-analysis data.
NR 55
TC 5
Z9 5
U1 1
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD AUG
PY 2013
VL 141
IS 8
BP 2649
EP 2668
DI 10.1175/MWR-D-12-00217.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 188VR
UT WOS:000322225200005
ER
PT J
AU Sippel, JA
Braun, SA
Zhang, FQ
Weng, YH
AF Sippel, Jason A.
Braun, Scott A.
Zhang, Fuqing
Weng, Yonghui
TI Ensemble Kalman Filter Assimilation of Simulated HIWRAP Doppler Velocity
Data in a Hurricane
SO MONTHLY WEATHER REVIEW
LA English
DT Article
DE Ensembles; Numerical weather prediction; forecasting; Data assimilation;
Mesoscale models
ID SCALE DATA ASSIMILATION; CONVECTIVE PARAMETERIZATION; MODEL EXPERIMENTS;
MESOSCALE; PREDICTABILITY; TESTS
AB This study utilizes ensemble Kalman filter (EnKF) observing system simulation experiments (OSSEs) to analyze the potential impact of assimilating radial velocity observations of hurricanes from the High-altitude Imaging Wind and Rain Airborne Profiler (HIWRAP). HIWRAP is a new Doppler radar mounted on the NASA Global Hawk unmanned airborne system that flies at roughly 19-km altitude and has the benefit of a 25-30-h flight duration, which is 2-3 times that of conventional aircraft. This research is intended as a proof-of-concept study for future assimilation of real HIWRAP data. The most important result from this research is that HIWRAP data can potentially improve hurricane analyses and prediction. For example, by the end of a 12-h assimilation period, the analysis error is much lower than that in deterministic forecasts. As a result, subsequent forecasts initialized with the EnKF analyses also improve. Furthermore, analyses and forecasts clearly benefit more from a 12-h assimilation period than for shorter periods, which highlights a benefit of the Global Hawk's potentially long on-station times.
C1 [Sippel, Jason A.; Braun, Scott A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zhang, Fuqing; Weng, Yonghui] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
RP Sippel, JA (reprint author), NASA, GSFC, Code 612, Greenbelt, MD 20771 USA.
EM jason.sippel@nasa.gov
RI Zhang, Fuqing/E-6522-2010
OI Zhang, Fuqing/0000-0003-4860-9985
FU Oak Ridge Associated Universities; NASA
FX The authors benefited from discussions with Eugenia Kalnay, Altug Aksoy,
Sylvie Lorsolo, and Gerald Heymsfield on this research. We are also
sincerely thankful to three anonymous reviewers, who gave very useful
comments that improved this study. Work by the first author began under
the NASA Postdoctoral Program, sponsored by Oak Ridge Associated
Universities through a contract with NASA. The first author's work
continued through his employment at the Goddard Earth Sciences and
Technology Center and at Goddard Earth Sciences Technology and Research.
Funding for this work came from the NASA Hurricane Sciences Research
Program under Dr. Ramesh Kakar and from the Hurricane and Severe Storm
Sentinel Investigation under NASA's Earth Venture Program. The
simulations were conducted at NASA's Center for Computational Sciences
facilities.
NR 33
TC 7
Z9 7
U1 0
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD AUG
PY 2013
VL 141
IS 8
BP 2683
EP 2704
DI 10.1175/MWR-D-12-00157.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 188VR
UT WOS:000322225200007
ER
PT J
AU Fielding, EJ
Sladen, A
Li, ZH
Avouac, JP
Burgmann, R
Ryder, I
AF Fielding, Eric J.
Sladen, Anthony
Li, Zhenhong
Avouac, Jean-Philippe
Buergmann, Roland
Ryder, Isabelle
TI Kinematic fault slip evolution source models of the 2008 M7.9 Wenchuan
earthquake in China from SAR interferometry, GPS and teleseismic
analysis and implications for Longmen Shan tectonics
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Radar interferometry; Earthquake source observations; Seismicity and
tectonics; Body waves; Continental tectonics: compressional
ID W 7.9 WENCHUAN; TIBETAN PLATEAU; JOINT INVERSION; EASTERN MARGIN; INSAR
DATA; RADAR INTERFEROMETRY; SURFACE DEFORMATION; LANDERS EARTHQUAKE;
RUPTURE; SICHUAN
AB The M-w 7.9 2008 Wenchuan earthquake ruptured about 280 km of faults in the Longmen Shan of Sichuan province, China, at the eastern edge of the Tibetan Plateau. We use teleseismic waveforms with geodetic data from Global Positioning System, synthetic aperture radar interferometry and image amplitude correlation to produce a source model of this earthquake. The model describes evolution of fault slip during the earthquake. The geodetic data constrains the spatial distribution of fault slip and the seismic waveforms constrain mostly the time evolution of slip. We find that the earthquake started with largely thrust motion on an imbricate system of faults beneath the central Longmen Shan, including the Beichuan Fault and Pengguan Fault, with fault slip at depth extending up to 50 km northwest of the mountain front. The fault ruptures continued northeast along the Beichuan Fault with more oblique slip (right-lateral and thrust) and the proportion of lateral motion increasing in the northern Longmen Shan. The northernmost fault segment has a much steeper dip, consistent with nearly pure strike-slip motion. The kinematic source model shows that the rupture propagated to the northeast at about 2.5-3.0 km s(-1), producing a cascade of subevents with a total duration of about 110 s. The complex fault ruptures caused shortening and uplift of the extremely steep central Longmen Shan, which supports models where the steep edge of the plateau is formed by thrusting over the strong crust of the Sichuan Basin.
C1 [Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sladen, Anthony; Avouac, Jean-Philippe] CALTECH, Tecton Observ, Pasadena, CA 91125 USA.
[Li, Zhenhong] Univ Glasgow, Sch Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland.
[Buergmann, Roland; Ryder, Isabelle] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
RP Fielding, EJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-233, Pasadena, CA 91109 USA.
EM eric.j.fielding@jpl.nasa.gov
RI Li, Zhenhong/F-8705-2010; Avouac, Jean-Philippe/B-5699-2015; Fielding,
Eric/A-1288-2007; Sladen, Anthony/A-2532-2017
OI Li, Zhenhong/0000-0002-8054-7449; Avouac,
Jean-Philippe/0000-0002-3060-8442; Fielding, Eric/0000-0002-6648-8067;
Sladen, Anthony/0000-0003-4126-0020
FU European Space Agency [AOE-668, 5343]; Japanese Aerospace Exploration
Agency through the US Government Research Consortium Data Pool at the
Alaska Satellite Facility; METI through the US Government Research
Consortium Data Pool at the Alaska Satellite Facility; Japanese
Aerospace Exploration Agency through ALOS PI; METI through ALOS PI
[061]; NASA Earth Surface and Interior focus area; National Science
Foundation [EAR-1014880]; Gordon and Betty Moore Foundation through
Grant GBMF [423.01]; Natural Environmental Research Council through the
GAS project [NE/H001085/1]; National Centre of Earth Observation of
which the Centre for the Observation and Modelling of Earthquakes,
Volcanoes, and Tectonics (COMET+)
FX We thank many researchers for sharing their thoughts on this earthquake,
including Zheng-Kang Shen, Jing Liu-Zeng, Judith Hubbard, Chen Ji, Dan
McKenzie and Ken Hudnut. We thank Kiran Kumar Thingbaijam for help with
formatting our slip model results into the SRCMOD format. Envisat data
is copyright European Space Agency and provided under projects AOE-668
and Dragon-2 (ID: 5343). ALOS data is copyright Japanese Aerospace
Exploration Agency and METI and provided through the US Government
Research Consortium Data Pool at the Alaska Satellite Facility and
through ALOS PI project 061. Part of this research was supported by the
NASA Earth Surface and Interior focus area and performed at the Jet
Propulsion Laboratory, California Institute of Technology, Pasadena.
Additional support was provided by the National Science Foundation grant
EAR-1014880. This research was funded in part by the Gordon and Betty
Moore Foundation through Grant GBMF #423.01 to the Caltech Tectonics
Observatory. This work was supported in part by the Natural
Environmental Research Council through the GAS project (Reference:
NE/H001085/1), by the National Centre of Earth Observation of which the
Centre for the Observation and Modelling of Earthquakes, Volcanoes, and
Tectonics (COMET+) is a part. Caltech Tectonics Observatory Contribution
227.
NR 82
TC 20
Z9 20
U1 4
U2 29
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
EI 1365-246X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD AUG
PY 2013
VL 194
IS 2
BP 1138
EP 1166
DI 10.1093/gji/ggt155
PG 29
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 182VS
UT WOS:000321773500039
ER
PT J
AU Hegde, GM
Ye, C
Robinson, CA
Stroupe, A
Tunstel, E
AF Hegde, Guruprasad M.
Ye, Cang
Robinson, Christopher A.
Stroupe, Ashley
Tunstel, Edward
TI Computer-Vision-Based Wheel Sinkage Estimation for Robot Navigation on
Lunar Terrain
SO IEEE-ASME TRANSACTIONS ON MECHATRONICS
LA English
DT Article
DE Lunar robotics; normalized cuts; terrain interface angles; wheel sinkage
estimation; wheel-soil interaction
ID IMAGE SEGMENTATION; PLANETARY ROVERS; NORMALIZED CUTS; MOBILE ROBOTS;
SLIPPAGE
AB This paper presents a wheel sinkage detection method that may be used in robotic lunar exploration tasks. The method extracts the boundary line between a robot wheel and lunar soil by segmenting the wheel-soil image captured from a video camera that monitors wheel-soil interaction. The detected boundary is projected onto the soil-free image of the robot wheel to determine the parameters of wheel sinkage. The segmentation method is based on a graph theory. It first clusters a wheel-soil image into homogeneous regions called superpixels and constructs a graph on the superpixels. It then partitions the graph into segments by using normalized cuts. Compared with the existing wheel sinkage detection methods, the proposed algorithm is more robust to illumination condition, shadows, and dust (covering the wheel). The method's efficacy has been validated by experiments under various conditions.
C1 [Hegde, Guruprasad M.; Ye, Cang; Robinson, Christopher A.] Univ Arkansas, Dept Syst Engn, Little Rock, AR 72204 USA.
[Stroupe, Ashley] CALTECH, Jet Prop Lab, Adv Robot Control Grp, Mobil & Robot Syst Sect, Pasadena, CA 91109 USA.
[Tunstel, Edward] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
EM gmhegde@ualr.edu; cxye@ualr.edu; Christopher.joe.Robinson@gmail.com;
ashley.w.stroupe@jpl.nasa.gov; edward.tunstel@jhuapl.edu
FU NASA under the NASA EPSCoR RID Award; NASA EPSCoR Research Award
FX This work was supported in part by NASA under the NASA EPSCoR RID Award
and the NASA EPSCoR Research Award. An earlier version of this paper was
presented at the IEEE International Conference on Mechatronics and
Automation, Xi'an, China, August 4-7, 2010.
NR 23
TC 7
Z9 7
U1 2
U2 23
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1083-4435
J9 IEEE-ASME T MECH
JI IEEE-ASME Trans. Mechatron.
PD AUG
PY 2013
VL 18
IS 4
BP 1346
EP 1356
DI 10.1109/TMECH.2013.2264095
PG 11
WC Automation & Control Systems; Engineering, Manufacturing; Engineering,
Electrical & Electronic; Engineering, Mechanical
SC Automation & Control Systems; Engineering
GA 180YG
UT WOS:000321634500012
ER
PT J
AU Murman, SM
AF Murman, Scott M.
TI A scalar anisotropy model for turbulent eddy viscosity
SO INTERNATIONAL JOURNAL OF HEAT AND FLUID FLOW
LA English
DT Article
DE nu(2)-f; SSG; Pressure-strain; Separation
ID NEAR-WALL; BOUNDARY-LAYERS; SEPARATED FLOW; CHANNEL; COMPUTATIONS;
SIMULATION; EQUATION
AB A three-equation eddy-viscosity turbulence model using transport equations for the turbulent kinetic energy (k), dissipation rate (epsilon), and a scalar measure of the Reynolds-stress anisotropy is described. Away from walls, where the turbulence anisotropy goes to zero, the model naturally reverts to the isotropic k-epsilon formulation, with only a slightly modified value of the eddy-viscosity coefficient. This leverages the predictive capability of k-epsilon for free shear flows, while still providing accurate predictions of wall-bounded flows without resorting to wall-damping functions. The computed model predictions are compared against experimental Reynolds-stress measurements for a zero-pressure-gradient flat-plate boundary layer, a planar mixing-layer, and the separated flow over periodic hills. Further, the computed results show improvements over standard one- and two-equation models, most notably for the smooth-body separation and recirculation encountered in the flow over periodic hills. Published by Elsevier Inc.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Murman, SM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Scott.M.Murman@nasa.gov
NR 43
TC 2
Z9 2
U1 1
U2 12
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0142-727X
J9 INT J HEAT FLUID FL
JI Int. J. Heat Fluid Flow
PD AUG
PY 2013
VL 42
BP 115
EP 130
DI 10.1016/j.ijheatfluidflow.2013.02.007
PG 16
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA 182ES
UT WOS:000321725100010
ER
PT J
AU Spurr, R
Natraj, V
Lerot, C
Van Roozendael, M
Loyola, D
AF Spurr, R.
Natraj, V.
Lerot, C.
Van Roozendael, M.
Loyola, D.
TI Linearization of the Principal Component Analysis method for radiative
transfer acceleration: Application to retrieval algorithms and
sensitivity studies
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Radiative transfer; Principal Component Analysis; Analytic
linearization; Performance enhancement
ID TRANSFER MODEL; ABSORPTION; MISSION; GOME/ERS-2; SCATTERING; GOME
AB Principal Component Analysis (PCA) is a promising tool for enhancing radiative transfer (RT) performance. When applied to binned optical property data sets, PCA exploits redundancy in the optical data, and restricts the number of full multiple-scatter calculations to those optical states corresponding to the most important principal components, yet still maintaining high accuracy in the radiance approximations. We show that the entire PCA RT enhancement process is analytically differentiable with respect to any atmospheric or surface parameter, thus allowing for accurate and fast approximations of Jacobian matrices, in addition to radiances. This linearization greatly extends the power and scope of the PCA method to many remote sensing retrieval applications and sensitivity studies. In the first example, we examine accuracy for PCA-derived UV-backscatter radiance and Jacobian fields over a 290-340 nm window. In a second application, we show that performance for UV-based total ozone column retrieval is considerably improved without compromising the accuracy. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Spurr, R.] RT Solut Inc, Cambridge, MA 02138 USA.
[Natraj, V.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lerot, C.; Van Roozendael, M.] Belgian Inst Space Aeron, B-1180 Brussels, Belgium.
[Loyola, D.] German Aerosp Ctr DLR, D-82234 Oberpfaffenhofen, Germany.
RP Spurr, R (reprint author), RT Solut Inc, 9 Channing St, Cambridge, MA 02138 USA.
EM rtsolutions@verizon.net
FU NASA [1443017, 1408795]; German Aerospace Center (DLR); Belspo SPP
Science Policy "Chercheur Supplementaire" at the Belgian Institute for
Space Aeronomy (BIRA-IASB) [60.11.45.23]; Ozone_cci project (part of the
ESA Climate Change Initiative program)
FX Part of this work was funded through NASA JPL Sub-contract #1443017,
with additional support from NASA JPL Subcontract #1408795. Part of this
work was funded by a contract with the German Aerospace Center (DLR),
with additional support provided through the Belspo SPP Science Policy
"Chercheur Supplementaire" grant #60.11.45.23 at the Belgian Institute
for Space Aeronomy (BIRA-IASB). European support comes under the
umbrella of the Ozone_cci project (part of the ESA Climate Change
Initiative program). The authors would like to thank Mick Christi with
programming help on LIDORT and 2S model upgrades.
NR 29
TC 8
Z9 10
U1 0
U2 12
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 AUG
PY 2013
VL 125
BP 1
EP 17
DI 10.1016/j.jqsrt.2013.04.002
PG 17
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 181PR
UT WOS:000321681500001
ER
PT J
AU Stacy, A
Bromm, V
AF Stacy, Athena
Bromm, Volker
TI Constraining the statistics of Population III binaries
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation; stars: Population III; galaxies: formation; cosmology:
theory; dark ages, reionization, first stars; early Universe
ID GAMMA-RAY BURSTS; PRIMORDIAL STAR-FORMATION; 1ST SUPERNOVA EXPLOSIONS;
EARLY METAL ENRICHMENT; INITIAL MASS FUNCTION; MAIN-SEQUENCE STARS;
SMALL-SCALE DYNAMO; BLACK-HOLES; PROTOSTELLAR FEEDBACK; PREGALACTIC
OUTFLOWS
AB We perform a cosmological simulation in order to model the growth and evolution of Population III (Pop III) stellar systems in a range of host minihalo environments. A Pop III multiple system forms in each of the 10 minihaloes, and the overall mass function is top-heavy compared to the currently observed initial mass function in the Milky Way. Using a sink particle to represent each growing protostar, we examine the binary characteristics of the multiple systems, resolving orbits on scales as small as 20 au. We find a binary fraction of similar to 35 per cent, with semi-major axes as large as 3000 au. The distribution of orbital periods is slightly peaked at less than or similar to 900 yr, while the distribution of mass ratios is relatively flat. Of all sink particles formed within the 10 minihaloes, similar to 50 per cent are lost to mergers with larger sinks, and similar to 50 per cent of the remaining sinks are ejected from their star-forming discs. The large binary fraction may have important implications for Pop III evolution and nucleosynthesis, as well as the final fate of the first stars.
C1 [Stacy, Athena] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bromm, Volker] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Bromm, Volker] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA.
RP Stacy, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM athena.stacy@nasa.gov
FU JWST Postdoctoral Fellowship through the NASA Post-doctoral Program
(NPP); NASA through Astrophysics Theory and Fundamental Physics Program
[NNX09AJ33G]; NSF [AST-1009928]
FX The authors wish to thank John Mather for insightful discussion during
the development of this work. AS is grateful for support from the JWST
Postdoctoral Fellowship through the NASA Postdoctoral Program (NPP). VB
acknowledges support from NASA through Astrophysics Theory and
Fundamental Physics Program grant NNX09AJ33G and from NSF through grant
AST-1009928. Resources supporting this work were provided by the NASA
High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center.
NR 122
TC 38
Z9 38
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 AUG
PY 2013
VL 433
IS 2
BP 1094
EP 1107
DI 10.1093/mnras/stt789
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 178QK
UT WOS:000321462300015
ER
PT J
AU White, TR
Huber, D
Maestro, V
Bedding, TR
Ireland, MJ
Baron, F
Boyajian, TS
Che, X
Monnier, JD
Pope, BJS
Roettenbacher, RM
Stello, D
Tuthill, PG
Farrington, CD
Goldfinger, PJ
McAlister, HA
Schaefer, GH
Sturmann, J
Sturmann, L
ten Brummelaar, TA
Turner, NH
AF White, T. R.
Huber, D.
Maestro, V.
Bedding, T. R.
Ireland, M. J.
Baron, F.
Boyajian, T. S.
Che, X.
Monnier, J. D.
Pope, B. J. S.
Roettenbacher, R. M.
Stello, D.
Tuthill, P. G.
Farrington, C. D.
Goldfinger, P. J.
McAlister, H. A.
Schaefer, G. H.
Sturmann, J.
Sturmann, L.
ten Brummelaar, T. A.
Turner, N. H.
TI Interferometric radii of bright Kepler stars with the CHARA Array: theta
Cygni and 16 Cygni A and B
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: interferometric; stars: individual: theta Cygni; stars:
individual: 16 Cygni A; stars: individual: 16 Cygni B; stars:
oscillations
ID SOLAR-LIKE OSCILLATIONS; GENEVA-COPENHAGEN SURVEY; BASE-LINE
INTERFEROMETRY; VIRTUAL OBSERVATORY TOOL; EXOPLANET HOST STARS; ANGULAR
DIAMETERS; FUNDAMENTAL PROPERTIES; RED GIANTS; ULTRAVIOLET EXTINCTION;
SEARCHING CALIBRATORS
AB We present the results of long-baseline optical interferometry observations using the Precision Astronomical Visual Observations (PAVO) beam combiner at the Center for High Angular Resolution Astronomy (CHARA) Array to measure the angular sizes of three bright Kepler stars: theta Cygni, and both components of the binary system 16 Cygni. Supporting infrared observations were made with the Michigan Infrared Combiner (MIRC) and Classic beam combiner, also at the CHARA Array. We find limb-darkened angular diameters of 0.753 +/- 0.009 mas for theta Cyg, 0.539 +/- 0.007 mas for 16 Cyg A and 0.490 +/- 0.006 mas for 16 Cyg B. The Kepler Mission has observed these stars with outstanding photometric precision, revealing the presence of solar-like oscillations. Due to the brightness of these stars the oscillations have exceptional signal-to-noise, allowing for detailed study through asteroseismology, and are well constrained by other observations. We have combined our interferometric diameters with Hipparcos parallaxes, spectrophotometric bolometric fluxes and the asteroseismic large frequency separation to measure linear radii (theta Cyg: 1.48 +/- 0.02 R-circle dot, 16 Cyg A: 1.22 +/- 0.02 R-circle dot, 16 Cyg B: 1.12 +/- 0.02 R-circle dot), effective temperatures (theta Cyg: 6749 +/- 44 K, 16 Cyg A: 5839 +/- 42 K, 16 Cyg B: 5809 +/- 39 K) and masses (theta Cyg: 1.37 +/- 0.04 M-circle dot, 16 Cyg A: 1.07 +/- 0.05 M-circle dot, 16 Cyg B: 1.05 +/- 0.04 M-circle dot) for each star with very little model dependence. The measurements presented here will provide strong constraints for future stellar modelling efforts.
C1 [White, T. R.; Huber, D.; Maestro, V.; Bedding, T. R.; Ireland, M. J.; Pope, B. J. S.; Stello, D.; Tuthill, P. G.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[White, T. R.; Ireland, M. J.] Australian Astron Observ, Epping, NSW 1710, Australia.
[White, T. R.; Bedding, T. R.; Stello, D.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ireland, M. J.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Baron, F.; Che, X.; Monnier, J. D.; Roettenbacher, R. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Boyajian, T. S.; Farrington, C. D.; Goldfinger, P. J.; McAlister, H. A.; Schaefer, G. H.; Sturmann, J.; Sturmann, L.; ten Brummelaar, T. A.; Turner, N. H.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA.
[Boyajian, T. S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
RP White, TR (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
EM t.white@physics.usyd.edu.au
FU National Science Foundation [AST-0606958]; Georgia State University
through the College of Arts and Sciences; W.M. Keck Foundation;
Australian Research Council; The Danish National Research Foundation;
NASA's Science Mission Directorate; Australian Postgraduate Award;
University of Sydney Merit Award; Australian Astronomical Observatory
PhD Scholarship; Denison Merit Award; NASA
FX 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. We acknowledge the
support of the Australian Research Council. Funding for the Stellar
Astrophysics Centre is provided by The Danish National Research
Foundation. We also acknowledge the Kepler Science Team and all those
who have contributed to the Kepler Mission. Funding for the Kepler
Mission is provided by NASA's Science Mission Directorate. TRW is
supported by an Australian Postgraduate Award, a University of Sydney
Merit Award, an Australian Astronomical Observatory PhD Scholarship and
a Denison Merit Award. DH 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.
NR 93
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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 AUG
PY 2013
VL 433
IS 2
BP 1262
EP 1270
DI 10.1093/mnras/stt802
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 178QK
UT WOS:000321462300028
ER
PT J
AU Chappell, SP
Abercromby, AF
Gernhardt, ML
AF Chappell, Steven P.
Abercromby, Andrew F.
Gernhardt, Michael L.
TI NEEMO 15: Evaluation of human exploration systems for near-Earth
asteroids
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Underwater; Analogs; Aquarius; Asteroids; Exploration
ID OBJECTS
AB The NASA Extreme Environment Mission Operations (NEEMO) 15 mission was focused on evaluating techniques for exploring near-Earth asteroids (NEAs). It began with a University of Delaware autonomous underwater vehicle (AUV) systematically mapping the coral reef for hundreds of meters surrounding the Aquarius habitat. This activity is akin to the type of "far-field survey" approach that may be used by a robotic precursor in advance of a human mission to a NFA Data from the far-field survey were then examined by the NEEMO science team and follow-up exploration traverses were planned, which used Deepworker single-person submersibles. Science traverses at NEEMO 15 were planned according to a prioritized list of objectives developed by the science team. These objectives were based on review and discussion of previous related marine science research, including previous marine science saturation missions conducted at the Aquarius habitat. AUV data were used to select several areas of scientific interest. The Deepworker science traverses were then executed at these areas of interest during 4 days of the NEEMO 15 mission and provided higher resolution data such as coral species distribution and mortality. These traverses are analogous to the "near-field survey" approach that is expected to be performed by a Multi-Mission Space Exploration Vehicle (MMSEV) during a human mission to a NEA before extravehicular activities (EVAs) are conducted. In addition to the science objectives that were pursued, the NEEMO 15 traverses provided an opportunity to test newly developed software and techniques. Sample collection and instrument deployment on the NEA surface by EVA crew would follow the "near-field survey" in a human NEA mission. Sample collection was not necessary for the purposes of the NEEMO science objectives; however, the engineering and operations objectives during NEEMO 15 were to evaluate different combinations of vehicles, crew members, tools, and equipment that could be used to perform these science objectives on a NEA. Specifically, the productivity and acceptability of simulated NEA exploration activities were systematically quantified and compared when operating with different combinations of crew sizes and exploration systems including MMSEVs, EVA jet packs, and EVA translation devices. Data from NEEMO 15 will be used in conjunction with data from software simulations, parametric analysis, other analog field tests, anchoring models, and integrated testing at Johnson Space Center to inform the evolving architectures and exploration systems being developed by the Human Spaceflight Architecture Team. (C) 2013 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Chappell, Steven P.; Abercromby, Andrew F.] Wyle, Houston, TX 77058 USA.
[Gernhardt, Michael L.] NASA, Houston, TX 77058 USA.
RP Chappell, SP (reprint author), Wyle, 2101 NASA Pkwy,Mail Code WYLE HAC 37C, Houston, TX 77058 USA.
EM steven.p.chappell@nasa.gov; andrew.f.abercromby@nasa.gov;
michael.l.gemhardt@nasa.gov
FU NASA Directorate Integration Office; Advanced Exploration Systems
Analogs Project
FX The research summarized in this article was mainly funded by the NASA
Directorate Integration Office and Advanced Exploration Systems Analogs
Project. Representatives from both funding organizations participated in
the process of review and approval of the study design along with other
stakeholder organizations. Similarly, representatives from the funding
organizations participated in execution of the study and interpreting
the results, but not directly in collection and analysis of the data.
The writing of this article and decision for publication was performed
solely by the authors.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD AUG-SEP
PY 2013
VL 89
BP 166
EP 178
DI 10.1016/j.actaastro.2013.03.002
PG 13
WC Engineering, Aerospace
SC Engineering
GA 178AM
UT WOS:000321416500018
ER
PT J
AU Novotny, SC
Perusek, GP
Rice, AJ
Comstock, BA
Bansal, A
Cavanagh, PR
AF Novotny, Sara C.
Perusek, Gail P.
Rice, Andrea J.
Comstock, Bryan A.
Bansal, Aasthaa
Cavanagh, Peter R.
TI A harness for enhanced comfort and loading during treadmill exercise in
space
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Spaceflight; Treadmill; Running; Countermeasure; Comfort; Bone loss
ID SIMULATED MICROGRAVITY; DURATION SPACEFLIGHT; GRAVITY REPLACEMENT; FOOT
FORCES; LOCOMOTION; STATION; MUSCLE; CARRIAGE
AB . Introduction: Locomotor and some resistance exercises in space require a gravity replacement force in order to allow I g-like ground reaction forces to be generated. Currently bungee cords, or other loading devices, interface with the crew member through a harness with a waist belt and shoulder straps. Crew members often find the application of the required loads to be uncomfortable, particularly at the hips.
Methods: An experimental harness was built that differed from previous in-flight designs by having a wider, moldable waist belt and contoured shoulder straps with additional padding. Eight subjects ran at 100% body weight (BW) loading for a total duration of 30 min per day on 12 days over a 3-week period in simulated 0-g conditions using horizontal suspension. A 100 mm Visual Analog Scale (VAS)(1) was used to assess harness-related and lower extremity discomfort at the end of each run.
Results: The overall rating of harness discomfort decreased from 27 mm on the 100 mm scale on day I to 10 mm on day 12, with significant decreases recorded for the back and hip regions as well as the overall harness.
Discussion: The experimental harness allows for repeated exposure to 30-minute bouts of 100% BW loaded simulated 0-g running with levels of discomfort less than 30 mm on a VAS scale of 0-100 mm. We believe that the use of such a harness during on-orbit exercise countermeasures may allow exercise to be performed at levels which are more effective in preventing bone and muscle loss. (C) 2013 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Novotny, Sara C.; Rice, Andrea J.; Cavanagh, Peter R.] Univ Washington, Dept Orthopaed & Sports Med, Seattle, WA 98195 USA.
[Perusek, Gail P.] NASA John H Glenn Res Ctr, Cleveland, OH 44135 USA.
[Comstock, Bryan A.; Bansal, Aasthaa] Univ Washington, Dept Biostat, Seattle, WA 98195 USA.
RP Cavanagh, PR (reprint author), Univ Washington, Dept Orthopaed & Sports Med, BB 1065D,1959 NE Pacific St,Box 36500, Seattle, WA 98195 USA.
EM cavanagh@uw.edu
FU NASA [NNJ04HB08G]; John Glenn Biomedical Engineering Consortium
[NNC05AA56A]; National Space Biomedical Research Institute through NASA
[NCC 9-58]; NIH National Center for Research Resources [UL1RR025014]
FX This work was funded in part by NASA (NNJ04HB08G), the John Glenn
Biomedical Engineering Consortium (NNC05AA56A), and by the National
Space Biomedical Research Institute through NASA NCC 9-58. The
University of Washington Center for Biomedical Statistics is supported
by grant UL1RR025014 from the NIH National Center for Research
Resources. None of these organizations had any part in the analysis or
interpretation of the results.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD AUG-SEP
PY 2013
VL 89
BP 205
EP 214
DI 10.1016/j.actaastro.2013.03.010
PG 10
WC Engineering, Aerospace
SC Engineering
GA 178AM
UT WOS:000321416500022
ER
PT J
AU Lloyd, CW
Hackler, AS
Garcia, Y
Olivotto, C
Spiero, F
Boese, A
Galoforo, G
Mukai, C
Sentse, N
de Staerke, D
Moussine-Pouchkine, E
Gross, MG
Cortez, J
Llewellyn, A
Lorza-Pitt, R
Niihori, M
MacRae, H
Braeucker, R
Curtis, J
Gitsch, M
AF Lloyd, Charles W.
Hackler, Amanda Smith
Garcia, Yamil
Olivotto, Cristina
Spiero, Francois
Boese, Andrea
Galoforo, Germana
Mukai, Chiaki
Sentse, Nicole
de Staerke, Danielle
Moussine-Pouchkine, Elisabeth
Gonzalez Gross, Marcella
Cortez, Jaqueline
Llewellyn, Alicia
Lorza-Pitt, Rafael
Niihori, Maid
MacRae, Heather
Braeucker, Richard
Curtis, Jeremy
Gitsch, Michaela
TI IAC-11.E1-7.-A1.8.5 The Mission X: Train like an astronaut pilot study
(vol 81, pg 77, 2012)
SO ACTA ASTRONAUTICA
LA English
DT Correction
C1 [Lloyd, Charles W.] NASA, Houston, TX 77058 USA.
[Hackler, Amanda Smith] MEI Technol, Houston, TX USA.
[Garcia, Yamil; Cortez, Jaqueline] Wyle Integrated Sci & Engn Grp, Houston, TX USA.
[Olivotto, Cristina; Sentse, Nicole] ESA, Noordwijk, Netherlands.
[Spiero, Francois; Moussine-Pouchkine, Elisabeth] CNES, Paris, France.
[Boese, Andrea; Braeucker, Richard] Deutsch Zentrum Luft & Raumfahrt eV DLR, Cologne, Germany.
[Galoforo, Germana] ASI, Rome, Italy.
[Mukai, Chiaki; Niihori, Maid] Japan Aerosp Explorat Agcy JAXA, Tsukuba, Ibaraki, Japan.
[de Staerke, Danielle] CNES, Toulouse, France.
[Gonzalez Gross, Marcella] Univ Politecn Madrid, Madrid, Spain.
[Llewellyn, Alicia] Tietronix, Houston, TX USA.
[Lorza-Pitt, Rafael] ESA, Bogota, Colombia.
[MacRae, Heather] Venture Thinking, London, England.
[Curtis, Jeremy] UK Space Agcy, Didcot, Oxon, England.
[Gitsch, Michaela] FFG, Vienna, Austria.
RP Lloyd, CW (reprint author), NASA, Houston, TX 77058 USA.
EM charles.w.lloyd@nasa.gov
NR 1
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD AUG-SEP
PY 2013
VL 89
BP 215
EP 215
DI 10.1016/j.actaastro.2013.04.022
PG 1
WC Engineering, Aerospace
SC Engineering
GA 178AM
UT WOS:000321416500023
ER
PT J
AU Sherwood, B
McCleese, D
AF Sherwood, Brent
McCleese, Daniel
TI JPL Innovation Foundry
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Space science; Mission concepts; Concept engineering; JPL; Team X;
A-Team
AB Space science missions are increasingly challenged today: in ambition, by increasingly sophisticated hypotheses tested; in development, by the increasing complexity of advanced technologies; in budgeting, by the decline of flagship-class mission opportunities; in management, by expectations for breakthrough science despite a risk-averse programmatic climate; and in planning, by increasing competition for scarce resources. How are the space-science missions of tomorrow being formulated? The paper describes the JPL Innovation Foundry, created in am, to respond to this evolving context. The Foundry integrates methods, tools, and experts that span the mission concept lifecycle. Grounded in JPL's heritage of missions, flight instruments, mission proposals, and concept innovation, the Foundry seeks to provide continuity of support and cost-effective, on-call access to the right domain experts at the right time, as science definition teams and Principal Investigators mature mission ideas from "cocktail napkin" to PDR. The Foundry blends JPL capabilities in proposal development and concurrent engineering, including Team X, with new approaches for open-ended concept exploration in earlier, cost-constrained phases, and with ongoing research and technology projects. It applies complexity and cost models, project-formulation lessons learned, and strategy analyses appropriate to each level of concept maturity. The Foundry is organizationally integrated with JPL formulation program offices; staffed by JPL's line organizations for engineering, science, and costing; and overseen by senior Laboratory leaders to assure experienced coordination and review. Incubation of each concept is tailored depending on its maturity and proposal history, and its highest-leverage modeling and analysis needs. (C) 2013 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Sherwood, Brent; McCleese, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP McCleese, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM brent.sherwood@jpl.nasa.gov; danielj.mccleese@jpl.nasa.gov
NR 4
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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 AUG-SEP
PY 2013
VL 89
BP 236
EP 247
DI 10.1016/j.actaastro.2013.04.020
PG 12
WC Engineering, Aerospace
SC Engineering
GA 178AM
UT WOS:000321416500027
ER
PT J
AU Karaca, HE
Acar, E
Ded, GS
Basaran, B
Tobe, H
Noebe, RD
Bigelow, G
Chumlyakov, YI
AF Karaca, H. E.
Acar, E.
Ded, G. S.
Basaran, B.
Tobe, H.
Noebe, R. D.
Bigelow, G.
Chumlyakov, Y. I.
TI Shape memory behavior of high strength NiTiHfPd polycrystalline alloys
SO ACTA MATERIALIA
LA English
DT Article
DE Shape memory alloys; Phase transformation; High strength alloys;
Precipitation; Mechanical characterization
ID THERMOELASTIC MARTENSITIC TRANSFORMATIONS; SINGLE-CRYSTALS; TI-NI;
PHASE-TRANSFORMATION; ELECTRON-MICROSCOPY; HYSTERESIS; TEMPERATURES;
MICROSTRUCTURE; SUBSTRUCTURE; DEFORMATION
AB Systematic characterization of the shape memory properties of a quaternary Ni-45.3-Ti-29.7 Hf-20-Pd-5 (at.%) polycrystalline alloy was performed in compression after selected aging treatments. Precipitation characteristics were revealed by transmission electron microscopy. The effects of aging temperature and time on transformation temperatures, recoverable and residual strains, and temperature and stress hystereses were determined by differential scanning calorimetry, constant-load thermal cycling experiments and isothermal strain cycling (superelasticity) tests. The crystal structure and lattice parameters of the transforming phases were determined from X-ray diffraction analysis. It was revealed that precipitation hardening significantly improved the shape memory properties of the NiTiHfPd alloy. Under optimum aging conditions, shape memory strains of up to 4% under 1 GPa were possible, and superelasticity experiments resulted in full strain recovery without any plastic deformation, even at stress levels as high as 2 GPa. The NiTiHfPd polycrystalline alloy exhibited very high damping capacity/absorbed energy (30-34 J cm(-3)) and work output (30-35 J cm(-3)), which were attributed to the ability to operate at high stress levels without significant plastic deformation and to a high mechanical hysteresis (>900 MPa) at temperatures ranging from 20 degrees C to 80 degrees C. (C) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Karaca, H. E.; Acar, E.; Ded, G. S.; Basaran, B.; Tobe, H.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Noebe, R. D.; Bigelow, G.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Chumlyakov, Y. I.] Tomsk State Univ, Siberian Phys Tech Inst, Tomsk 634050, Russia.
[Basaran, B.] Univ Turkish Aeronaut Assoc, TR-06790 Ankara, Turkey.
RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
EM karaca@engr.uky.edu
RI Chumlyakov, Yuriy/R-6496-2016
FU NASA Fundamental Aeronautics Program; Aeronautical Sciences Project;
NASA EPSCOR program [NNX11AQ31A]; KY EPSCoR RID program [3049024332];
RFBR project [10-03-0154-a]
FX This work was supported in part by the NASA Fundamental Aeronautics
Program, Aeronautical Sciences Project and the NASA EPSCOR program under
Grant No: NNX11AQ31A, KY EPSCoR RID program under Grant No. 3049024332
and RFBR project with Grant No. 10-03-0154-a.
NR 58
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6454
J9 ACTA MATER
JI Acta Mater.
PD AUG
PY 2013
VL 61
IS 13
BP 5036
EP 5049
DI 10.1016/j.actamat.2013.04.039
PG 14
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 180NH
UT WOS:000321601400032
ER
PT J
AU Marinova, MM
McKay, CP
Pollard, WH
Heldmann, JL
Davila, AF
Andersen, DT
Jackson, WA
Lacelle, D
Paulsen, G
Zacny, K
AF Marinova, Margarita M.
McKay, Christopher P.
Pollard, Wayne H.
Heldmann, Jennifer L.
Davila, Alfonso F.
Andersen, Dale T.
Jackson, W. Andrew
Lacelle, Denis
Paulsen, Gale
Zacny, Kris
TI Distribution of depth to ice-cemented soils in the high-elevation
Quartermain Mountains, McMurdo Dry Valleys, Antarctica
SO ANTARCTIC SCIENCE
LA English
DT Article
DE dry permafrost; Mars; University Valley; vapour diffusion
ID MESOSCALE PREDICTION SYSTEM; SOUTHERN VICTORIA LAND; MIOCENE GLACIER
ICE; BEACON VALLEY; GROUND ICE; EAST ANTARCTICA; OLDEST ICE; STABILITY;
MARS; SUBLIMATION
AB We report on 475 measurements of depth to ice-cemented ground in four high-elevation valleys of the Quartermain Mountains, McMurdo Dry Valleys, Antarctica. These valleys have pervasive ice-cemented ground, and the depth to ice-cemented ground and the ice composition may be indicators of climate change. In University Valley, the measured depth to ice-cemented ground ranges from 0-98 cm. There is an overall trend of increasing depth to ice-cemented ground with distance from a small glacier at the head of the valley, with a slope of 32 cm depth per kilometre along the valley floor. For Farnell Valley, the depth to ice-cemented ground is roughly constant (c. 30 cm) in the upper and central parts of the valley, but increases sharply as the valley descends into Beacon Valley. The two valleys north of University Valley also have extensive ice-cemented ground, with depths of 20-40 cm, but exhibit no clear patterns of ice depth with location. For all valleys there is a tendency for the variability in depth to ice-cemented ground at a site to increase with increasing depth to ice. Snow recurrence, solar insolation, and surface albedo may all be factors that cause site to site variations in these valleys.
C1 [Marinova, Margarita M.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Marinova, Margarita M.; McKay, Christopher P.; Heldmann, Jennifer L.; Davila, Alfonso F.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Pollard, Wayne H.] McGill Univ, Dept Geog, Montreal, PQ H3A 2K6, Canada.
[Davila, Alfonso F.; Andersen, Dale T.] SETI Inst, Mountain View, CA 94043 USA.
[Jackson, W. Andrew] Texas Tech Univ, Lubbock, TX 79401 USA.
[Lacelle, Denis] Univ Ottawa, Dept Geog, Ottawa, ON K1N 6N5, Canada.
[Paulsen, Gale; Zacny, Kris] Honeybee Robot, Pasadena, CA 91103 USA.
RP Marinova, MM (reprint author), Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
EM margarita.m.marinova@gmail.com
RI Jackson, William/B-8999-2009;
OI Lacelle, Denis/0000-0002-6691-8717
FU NASA ASTEP program; US Antarctic Program; NSF Office of Polar Programs;
USAP [B-302]
FX This fieldwork and research was supported by the NASA ASTEP program, in
collaboration with the NSF Office of Polar Programs and the US Antarctic
Program. This work was conducted as part of USAP project B-302. We thank
the awesome USAP staff and helicopter crews for their extensive support.
We gratefully acknowledge the comments of the reviewers.
NR 38
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U1 0
U2 18
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0954-1020
J9 ANTARCT SCI
JI Antarct. Sci.
PD AUG
PY 2013
VL 25
IS 4
BP 575
EP 582
DI 10.1017/S095410201200123X
PG 8
WC Environmental Sciences; Geography, Physical; Geosciences,
Multidisciplinary
SC Environmental Sciences & Ecology; Physical Geography; Geology
GA 182QY
UT WOS:000321760000010
ER
PT J
AU Bell, AR
Osgood, DE
Cook, BI
Anchukaitis, KJ
McCarney, GR
Greene, AM
Buckley, BM
Cook, ER
AF Bell, Andrew R.
Osgood, Daniel E.
Cook, Benjamin I.
Anchukaitis, Kevin J.
McCarney, Geoffrey R.
Greene, Arthur M.
Buckley, Brendan M.
Cook, Edward R.
TI Paleoclimate histories improve access and sustainability in index
insurance programs
SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS
LA English
DT Article
DE Paleoclimate; Tree rings; Index insurance; Non-stationarity; Agriculture
ID CLIMATE-CHANGE; DROUGHT; MANAGEMENT; RISK
AB Proxy-based climate reconstructions can extend instrumental records by hundreds of years, providing a wealth of climate information at high temporal resolution. To date, however, their usefulness for informing climate risk and variability in policy and social applications has been understudied. Here, we apply tree-ring based reconstructions of drought for the last 700 years in a climate index insurance framework to show that additional information from long climate reconstructions significantly improves our understanding of the underlying climate distributions and variability. We further show that this added information can be used to better characterize risk to insurance providers, in many cases providing meaningful reductions in long-term contract costs to farmers in stand-alone policies. The impact of uncertainty on insurance premiums can also be reduced when insurers diversify portfolios, and the availability of long-term climate information from tree rings across a broad geographic range provides an opportunity to characterize spatial correlation in climate risk across geographic regions. Our results are robust to the range of climate variability experienced over the last 400 years and in model simulations of the twenty-first century, even within the context of changing baselines due to low frequency variability and secular climate trends. These results demonstrate the utility of longer-term climate histories in index insurance applications. Furthermore, they make the case from a climate-variability perspective for the continued importance of such approaches to improving the instrumental climate record, even into a non-stationary climate future. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Bell, Andrew R.] Int Food Policy Res Inst, Washington, DC 20006 USA.
[Osgood, Daniel E.; Greene, Arthur M.] Columbia Univ, Earth Inst, Int Res Inst Climate & Soc, Palisades, NY 10964 USA.
[Cook, Benjamin I.; Anchukaitis, Kevin J.; Buckley, Brendan M.; Cook, Edward R.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[McCarney, Geoffrey R.] Columbia Univ, Sch Int & Publ Affairs, New York, NY 10027 USA.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Anchukaitis, Kevin J.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
RP Bell, AR (reprint author), Int Food Policy Res Inst, Washington, DC 20006 USA.
EM a.bell@cgiar.org
RI Cook, Benjamin/H-2265-2012;
OI Bell, Andrew/0000-0002-1164-312X
FU NSF [AGS 0908971]
FX This work was funded by NSF grant AGS 0908971. We also gratefully
acknowledge Dr. Johann Jungclaus for making available the ECHAM5-MPIOM
simulation runs.
NR 44
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U1 2
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0959-3780
EI 1872-9495
J9 GLOBAL ENVIRON CHANG
JI Glob. Environ. Change-Human Policy Dimens.
PD AUG
PY 2013
VL 23
IS 4
BP 774
EP 781
DI 10.1016/j.gloenvcha.2013.03.003
PG 8
WC Environmental Sciences; Environmental Studies; Geography
SC Environmental Sciences & Ecology; Geography
GA 174LS
UT WOS:000321157600007
ER
PT J
AU Clifford, SM
Yoshikawa, K
Byrne, S
Durham, W
Fisher, D
Forget, F
Hecht, M
Smith, P
Tamppari, L
Titus, T
Zurek, R
AF Clifford, Stephen M.
Yoshikawa, Kenji
Byrne, Shane
Durham, William
Fisher, David
Forget, Francois
Hecht, Michael
Smith, Peter
Tamppari, Leslie
Titus, Timothy
Zurek, Richard
TI Introduction to the fifth Mars Polar Science special issue: Key
questions, needed observations, and recommended investigations
SO ICARUS
LA English
DT Editorial Material
ID EXPLORATION; FUTURE
C1 [Clifford, Stephen M.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Yoshikawa, Kenji] Univ Alaska Fairbanks, Water & Environm Res Ctr, Fairbanks, AK 99775 USA.
[Byrne, Shane; Smith, Peter] Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Durham, William] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Fisher, David] Univ Ottawa, Dept Geol, Ottawa, ON K1N 6N5, Canada.
[Forget, Francois] Inst Pierre Simon Laplace, Lab Meteorol Dynam, Paris, France.
[Hecht, Michael] MIT, Haystack Observ, Westford, MA 01886 USA.
[Tamppari, Leslie] CALTECH, Jet Prop Lab, Planetary & Earth Sci Sect, Pasadena, CA 91109 USA.
[Titus, Timothy] US Geol Survey, Flagstaff, AZ 86001 USA.
[Zurek, Richard] CALTECH, Jet Prop Lab, NASA Mars Program Off, Pasadena, CA 91109 USA.
RP Clifford, SM (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
EM clifford@lpi.usra.edu
NR 21
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U1 1
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD AUG
PY 2013
VL 225
IS 2
BP 864
EP 868
DI 10.1016/j.icarus.2013.04.005
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 183GL
UT WOS:000321802400001
ER
PT J
AU Thomas, PC
Calvin, WM
Gierasch, P
Haberle, R
James, PB
Sholes, S
AF Thomas, P. C.
Calvin, W. M.
Gierasch, P.
Haberle, R.
James, P. B.
Sholes, S.
TI Time scales of erosion and deposition recorded in the residual south
polar cap of Mars
SO ICARUS
LA English
DT Article
DE Mars, Polar caps; Mars, Atmosphere; Mars, Climate; Mars
ID GLOBAL DUST STORM; ICE; FEATURES
AB The residual south polar cap (RSPC) of Mars has been subject to competing processes during recent Mars years of high resolution image coverage: continuing erosion of scarps while the maximum extent grows as well as shrinks (Piqueux, S., Christensen, P.R. [2008]. J. Geophys. Res. (Planets) 113,2006; James, P.B., Thomas, P.C., Malin, M.C. [2010]. Icarus 208, 82-85). Additionally, the cap has a variety of morphologies and erosion (scarp retreat) rates (Thomas, P.C., James, P.B., Calvin, W.M., Haberle, R., Malin, M.C. [2009]. Icarus 203, 352-375). Do these different forms and competing processes indicate an aging and possibly disappearing cap, a growing cap, or a fluctuating cap, and is it possible to infer the timescales of the processes acting on the RSPC? Here we use the latest imaging data from Mars' southern summer in Mars year 30 (Calendar year 2011) to evaluate erosion rates of forms in the RSPC over 6 Mars years, and to map more fully features whose sizes can be used to predict deposit ages. Data through Mars year 30 show that scarp retreat rates in the RSPC have remained approximately the same for at least 6 Mars years and that these rates of erosion also apply approximately over the past 21 Mars years. The thicker units appear to have undergone changes in the locations of new pit formation about 30-50 Mars years ago. The thinner units have some areas that are possibly 80 Mars years old, with some younger materials having accumulated more than a meter in thickness since Mars year 9. Formation of the thicker units probably required over 100 Mars years. The upper surfaces of most areas, especially the thicker units, show little change at the few-cm level over the last 2 Mars years. This observation suggests that current conditions are substantially different from those when the thicker units were deposited. A prime characteristic of the evolution of the RSPC is that some changes are progressive, such as those involving scarp retreat, while others, such as the geography of initiation of new pits or the areal coverage of ice, appear to be more episodic. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Thomas, P. C.; Gierasch, P.; Sholes, S.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Calvin, W. M.] Univ Nevada, Dept Geol Sci, Reno, NV 89577 USA.
[Haberle, R.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[James, P. B.] Space Sci Inst, Boulder, CO 80301 USA.
RP Thomas, PC (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
EM pct2@cornell.edu
NR 24
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U1 0
U2 13
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD AUG
PY 2013
VL 225
IS 2
BP 923
EP 932
DI 10.1016/j.icarus.2012.08.038
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 183GL
UT WOS:000321802400006
ER
PT J
AU Benkrid, K
Keymeulen, D
Patel, UD
Merodio-Codinachs, D
AF Benkrid, Khaled
Keymeulen, Didier
Patel, Umeshkumar D.
Merodio-Codinachs, David
TI Guest Editors' Introduction: Special Section on Adaptive Hardware and
Systems
SO IEEE TRANSACTIONS ON COMPUTERS
LA English
DT Editorial Material
C1 [Benkrid, Khaled] Univ Edinburgh, Sch Engn, Edinburgh EH9 3JL, Midlothian, Scotland.
[Keymeulen, Didier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Patel, Umeshkumar D.] NASA, Goddard Space Flight Ctr, Electromech Syst Branch, Greenbelt, MD 20771 USA.
[Merodio-Codinachs, David] ESA ESTEC, European Space Agcy, Elect Engn Dept TEC EDM, NL-2201 AZ Noordwijk, Netherlands.
RP Benkrid, K (reprint author), Univ Edinburgh, Sch Engn, Kings Bldg,Faraday Bldg,Mayfield Rd, Edinburgh EH9 3JL, Midlothian, Scotland.
EM k.benkrid@ieee.org; didier.keymeulen@jpl.nasa.gov;
umeshkumar.d.patel@nasa.gov; david.merodio.codinachs@esa.int
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0018-9340
J9 IEEE T COMPUT
JI IEEE Trans. Comput.
PD AUG
PY 2013
VL 62
IS 8
BP 1478
EP 1480
PG 3
WC Computer Science, Hardware & Architecture; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA 175HH
UT WOS:000321221000001
ER
PT J
AU Lehnert, H
Stone, RP
Heimler, W
AF Lehnert, Helmut
Stone, Robert P.
Heimler, Wolfgang
TI Histodermella kagigunensis sp nov from the Gulf of Alaska and Aleutian
Islands; first records of the genus from the North Pacific
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
DE new species; Demospongiae; Coelosphaeridae; Histodermella; North
Pacific; Gulf of Alaska; Aleutian Islands
AB The genus Histodermella grows to four species with the addition of H. kagigunensis sp. nov. from the North Pacific. The new species is described and compared with all congeners. Histodermella kagigunensis shows affinities to H. ingolfi Lundbeck 1910 as it has the same spicule types but differs clearly in size, habitus and the dimensions of two occurring spicule types. The discovery of H. kagigunensis represents the first record of the genus Histodermella in the North Pacific Ocean.
C1 [Stone, Robert P.] Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, NOAA, Juneau, AK 99801 USA.
[Heimler, Wolfgang] Univ Erlangen Nurnberg, Inst Entwicklungsbiol, D-91054 Erlangen, Germany.
RP Lehnert, H (reprint author), Eichenstr 14, D-86507 Oberottmarshausen, Germany.
EM Lehnert@spongetaxonomics.de
FU Alaska Fisheries Science Center of NOAA/NMFS
FX We thank Roger N. Clark and Patrick Malecha for collecting the specimens
and William Austin for providing a first identification. H.L. was
supported by a contract from the Alaska Fisheries Science Center of
NOAA/NMFS. We thank the Institut fur Prozessmaschinen und Anlagentechnik
(IPAT), Universitat Erlangen for providing access to a scanning electron
microscope.
NR 7
TC 2
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U1 0
U2 5
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0025-3154
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD AUG
PY 2013
VL 93
IS 5
BP 1245
EP 1248
DI 10.1017/S0025315412001063
PG 4
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 179HI
UT WOS:000321510200009
ER
PT J
AU Werneth, CM
Maung, KM
Mead, LR
Blattnig, SR
AF Werneth, Charles M.
Maung, Khin Maung
Mead, Lawrence R.
Blattnig, Steve R.
TI Finite sum expressions for elastic and reaction cross sections
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article
DE Glauber theory; Eikonal approximation; Method of partial waves
ID MOMENTUM-SPACE; SCATTERING
AB Nuclear cross section calculations are often performed by using the partial wave method or the Eikonal method through Glauber theory. The expressions for the total cross section, total elastic cross section, and total reaction cross section in the partial wave method involve infinite sums and do not utilize simplifying approximations. Conversely, the Eikonal method gives these expressions in terms of integrals but utilizes the high energy and small angle approximations. In this paper, by using the fact that the lth partial wave component of the T-matrix can be very accurately approximated by its Born term, the infinite sums in each of the expressions for the differential cross section, total elastic cross section, total cross section, and total reaction cross section are re-written in terms of finite sums plus closed form expressions. The differential cross sections are compared to the Eikonal results for O-16 + O-16, C-12 + C-12, and p + C-12 elastic scattering. Total cross sections, total reaction cross sections, and total elastic cross sections are compared to the Eikonal results for C-12 + C-12 scattering. Published by Elsevier B.V.
C1 [Werneth, Charles M.; Blattnig, Steve R.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Maung, Khin Maung; Mead, Lawrence R.] Univ So Mississippi, Dept Phys & Astron, Hattiesburg, MS 39406 USA.
RP Werneth, CM (reprint author), NASA Langley Res Ctr, 2 West Reid St, Hampton, VA 23681 USA.
EM charles.m.werneth@nasa.gov; khin.maung@usm.edu; lawrence.mead@usm.edu;
steves.r.blattnig@nasa.gov
FU NASA (University of Southern Mississippi) [NNX09AE94A]; NASA (University
of Tennessee) [NNX10AD18A]
FX The authors thank Drs. Ryan Norman, Tony Slaba, Francis Badavi, John
Norbury, and Jonathan Ransom for reviewing this paper. This work was
supported in part by NASA grants NNX09AE94A (University of Southern
Mississippi) and NNX10AD18A (University of Tennessee).
NR 15
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U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD AUG 1
PY 2013
VL 308
BP 40
EP 45
DI 10.1016/j.nimb.2013.05.003
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 178YX
UT WOS:000321484400009
ER
PT J
AU Han, JW
Choi, BJ
Yang, JJ
Moon, DI
Choi, YK
Williams, RS
Meyyappan, M
AF Han, Jin-Woo
Choi, Byung Joon
Yang, J. Joshua
Moon, Dong-Il
Choi, Yang-Kyu
Williams, R. Stanley
Meyyappan, M.
TI A replacement of high-k process for CMOS transistor by atomic layer
deposition
SO SEMICONDUCTOR SCIENCE AND TECHNOLOGY
LA English
DT Article
AB A replacement of high-k process was implemented on an independent double gate FinFET, following the ordinary gate-first process with minor modifications. The present scheme involves neither exotic materials nor unprecedented processing. After the source/drain process, the sacrificial gate oxide was selectively substituted with amorphous Ta2O5 via conformal plasma enhanced atomic layer deposition. The present gate-first gate-dielectric-last scheme combines the advantages of the process and design simplicity of the gate-first approach and the control of the effective gate workfunction and the interfacial oxide of the gate-dielectric-last approach. Electrical characterization data and cross-sectional images are provided as evidence of the concept.
C1 [Han, Jin-Woo; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Choi, Byung Joon; Yang, J. Joshua; Williams, R. Stanley] Hewlett Packard Corp, Palo Alto, CA 94304 USA.
[Moon, Dong-Il; Choi, Yang-Kyu] Korea Adv Inst Sci & Technol, Dept Elect Engn, Taejon 305701, South Korea.
RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
EM jin-woo.han@nasa.gov
RI Choi, Byungjoon/H-4513-2011; Williams, R. Stanley/A-8281-2009
OI Williams, R. Stanley/0000-0003-0213-4259
NR 10
TC 3
Z9 3
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0268-1242
J9 SEMICOND SCI TECH
JI Semicond. Sci. Technol.
PD AUG
PY 2013
VL 28
IS 8
AR 082003
DI 10.1088/0268-1242/28/8/082003
PG 4
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA 181WP
UT WOS:000321701100003
ER
PT J
AU Duncan, C
Savage, K
Williams, M
Dickerson, B
Kondas, AV
Fitzpatrick, KA
Guerrero, JL
Spraker, T
Kersh, GJ
AF Duncan, C.
Savage, K.
Williams, M.
Dickerson, B.
Kondas, A. V.
Fitzpatrick, K. A.
Guerrero, J. L.
Spraker, T.
Kersh, G. J.
TI Multiple Strains of Coxiella burnetii are Present in the Environment of
St. Paul Island, Alaska
SO TRANSBOUNDARY AND EMERGING DISEASES
LA English
DT Article
DE Coxiella burnetii; environment; Alaska; marine mammals
ID SEAL CALLORHINUS-URSINUS; Q-FEVER; INFECTION; DNA
AB In 2010, Coxiella burnetii was identified at a high prevalence in the placentas of Northern fur seals (Callorhinus ursinus) collected at a single rookery on St. Paul Island Alaska; an area of the United States where the agent was not known to be present. As contamination was hypothesized as a potential cause of false positives, but nothing was known about environmental C.burnetii in the region, an environmental survey was conducted to look for the prevalence and distribution of the organism on the island. While environmental prevalence was low, two strains of the organism were identified using PCR targeting the COM1 and IS1111 genes. The two strains are consistent with the organism that has been increasingly identified in marine mammals as well as a strain type more commonly found in terrestrial environments and associated with disease in humans and terrestrial animals. Further work is needed to elucidate information regarding the ecology of this organism in this region, particularly in association with the coastal environment.
C1 [Duncan, C.; Spraker, T.] Colorado State Univ, Vet Diagnost Lab, Dept Microbiol Immunol & Pathol, Ft Collins, CO 80523 USA.
[Savage, K.; Williams, M.; Guerrero, J. L.] Alaska Reg Off, Natl Marine Fisheries Serv, Juneau, AK USA.
[Savage, K.; Williams, M.; Guerrero, J. L.] Alaska Reg Off, Natl Marine Fisheries Serv, Anchorage, AK USA.
[Dickerson, B.] Natl Marine Mammal Lab, Natl Marine Fisheries Serv, Seattle, WA USA.
[Kondas, A. V.; Fitzpatrick, K. A.; Kersh, G. J.] Ctr Dis Control & Prevent, Rickettsial Zoonoses Branch, Atlanta, GA USA.
RP Duncan, C (reprint author), Colorado State Univ, Vet Diagnost Lab, 300 West Drake, Ft Collins, CO 80523 USA.
EM colleen.duncan@colostate.edu
FU Centers for Disease Control and Prevention (CDC)
FX Sincere thanks to individuals who helped collect placental and
environmental samples for use in this study: Dr. Wendi Roe, Sophie
Peirszalowski, Kirsten Dullen and Dustin Carl. All tissue samples were
collected under authority of U.S. Marine Mammal Permit No. 782-1708
issued to the National Marine Mammal Lab, Seattle. A. V. K. was
supported by an appointment to the Emerging Infectious Diseases (EID)
Fellowship program administered by the Association of Public Health
Laboratories (APHL) and funded by the Centers for Disease Control and
Prevention (CDC). The findings and conclusions in this report are those
of the authors and do not necessarily represent the views of the CDC or
the Department of Health and Human Services.
NR 18
TC 5
Z9 5
U1 0
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1865-1674
J9 TRANSBOUND EMERG DIS
JI Transbound. Emerg. Dis.
PD AUG
PY 2013
VL 60
IS 4
BP 345
EP 350
DI 10.1111/j.1865-1682.2012.01353.x
PG 6
WC Infectious Diseases; Veterinary Sciences
SC Infectious Diseases; Veterinary Sciences
GA 178KT
UT WOS:000321447500007
PM 22747976
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 Travel distance and transformation of injected emulsified zerovalent
iron nanoparticles in the subsurface during two and half years
SO WATER RESEARCH
LA English
DT Article
DE Travel distance; Emulsified zerovalent iron; Pneumatic injection; Direct
injection; Nanoiron corrosion; Groundwater remediation; Magnetite;
Lepidocrocite; Ferrihydrite; Goethite
ID ZERO-VALENT IRON; MODIFIED FE-0 NANOPARTICLES; POROUS-MEDIA; PARTICLE
CONCENTRATION; SATURATED SAND; NANOSCALE; REACTIVITY; TRANSPORT;
REMEDIATION; LEPIDOCROCITE
AB Nanoscale zerovalent iron (NZVI) such as Toda Kogyo RNIP-10DS has been used for site remediation, yet information is lacking regarding how far injected NZVI can travel, how long it lasts, and how it transforms to other minerals in a groundwater system. Previously we reported effective mass destruction of chlorinated ethenes dominated by tetrachloroethene (PCE) using emulsified zerovalent iron (EZVI) nanoparticles of RNIP-10DS in a shallow aquifer (1-6 m below ground surface, BGS) at Site 45, Marine Corps Recruit Depot, Parris Island, South Carolina, USA. Here we report test results on transport and transformation of injected EZVI in the subsurface. We employed two EZVI delivery methods: pneumatic injection and direct injection. Effective delivery of EZVI to the targeted zone was achieved with pneumatic injection showing a travel distance from injection points of up to 2.1 m and direct injection showing a travel distance up to 0.89 m. X-ray diffraction and scanning electron microscopy studies on particles harvested from well purge waters indicated that injected black colored NZVI (alpha-Fe-0) was transformed largely to black colored cube-like and plate-like magnetites (Fe3O4, 0.1-1 mu m, 0-9 months), then to orange colored irregularly shaped lepidocrocite (gamma-FeOOH, 0.1-1 mu m, 9 months to 2.5 years), then to yellowish lath-like goethite (alpha-FeOOH, 2-5 mu m, 2.5 years) and ferrihydrite-like spherical particles (0.05-0.1 mu m) in the top portion of the aquifer (1-2 m BGS). No alpha-Fe-0 was found in most monitoring wells three months after injection. The formed iron oxides appeared to have a wider range of particle size (submicron to 5 mu m) than the pristine NZVI (35-140 nm). Injected NZVI was largely transformed to magnetite (0.1-1 mu m) during two and half years in the lower portion of the aquifer (3-6 m). 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.] Naval 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]; EPA; 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
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 and Ms. Lisa Donohoe 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, Lisa Constantino, and Kristie
Hargrove and Mr. Mark White of EPA for TOC/TIC and anions analysis, Mr.
Tony Lee of EPA for assistance with SEM analysis, Messrs. Steve Markham
and Andrew Greenwood of Shaw Environmental & Infrastructure, Inc. for
metals analysis, and three anonymous reviewers for their constructive
comments and suggestions that helped to improve the quality of this
paper.
NR 44
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U1 5
U2 71
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 AUG 1
PY 2013
VL 47
IS 12
SI SI
BP 4095
EP 4106
DI 10.1016/j.watres.2012.12.042
PG 12
WC Engineering, Environmental; Environmental Sciences; Water Resources
SC Engineering; Environmental Sciences & Ecology; Water Resources
GA 173MQ
UT WOS:000321084000024
PM 23562563
ER
PT J
AU Stenning, DC
Lee, TCM
van Dyk, DA
Kashyap, V
Sandell, J
Young, CA
AF Stenning, David C.
Lee, Thomas C. M.
van Dyk, David A.
Kashyap, Vinay
Sandell, Julia
Young, C. Alex
TI Morphological Feature Extraction for Statistical Learning With
Applications To Solar Image Data
SO STATISTICAL ANALYSIS AND DATA MINING
LA English
DT Article
DE mathematical morphology; image analysis; classification; sunspots;
coronal loops; skeletonization
AB Many areas of science are generating large volumes of digital image data. In order to take full advantage of the high-resolution and high-cadence images modern technology is producing, methods to automatically process and analyze large batches of such images are needed. This involves reducing complex images to simple representations such as binary sketches or numerical summaries that capture embedded scientific information. Using techniques derived from mathematical morphology, we demonstrate how to reduce solar images into simple 'sketch' representations and numerical summaries that can be used for statistical learning. We demonstrate our general techniques on two specific examples: classifying sunspot groups and recognizing coronal loop structures. Our methodology reproduces manual classifications at an overall rate of 90% on a set of 119 magnetogram and white light images of sunspot groups. We also show that our methodology is competitive with other automated algorithms at producing coronal loop tracings and demonstrate robustness through noise simulations. (C) 2013 Wiley Periodicals, Inc.
C1 [Stenning, David C.] Univ Calif Irvine, Dept Stat, Irvine, CA 92617 USA.
[Lee, Thomas C. M.] Univ Calif Davis, Dept Stat, Davis, CA 95616 USA.
[van Dyk, David A.] Univ London Imperial Coll Sci Technol & Med, Dept Math, Stat Sect, London SW7 2AZ, England.
[Kashyap, Vinay] Smithsonian Astrophys Observ, Div High Energy Astrophys, Cambridge, MA 02138 USA.
[Sandell, Julia] Univ Penn, Dept Phys, Philadelphia, PA 19104 USA.
[Young, C. Alex] NASA GSFC, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP van Dyk, DA (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Math, Stat Sect, Huxley Bldg, London SW7 2AZ, England.
EM dvandyk@imperial.ac.uk
NR 15
TC 5
Z9 5
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1932-1864
EI 1932-1872
J9 STAT ANAL DATA MIN
JI Stat. Anal. Data Min.
PD AUG
PY 2013
VL 6
IS 4
SI SI
BP 329
EP 345
DI 10.1002/sam.11200
PG 17
WC Computer Science, Artificial Intelligence; Computer Science,
Interdisciplinary Applications; Statistics & Probability
SC Computer Science; Mathematics
GA V41CX
UT WOS:000209525400006
ER
PT J
AU Munoz, C
Narkawicz, A
AF Munoz, Cesar
Narkawicz, Anthony
TI Formalization of Bernstein Polynomials and Applications to Global
Optimization
SO JOURNAL OF AUTOMATED REASONING
LA English
DT Article
DE Formal verification; Non-linear arithmetic; Global optimization;
Bernstein polynomials; Interactive theorem proving
AB This paper presents a formalization in higher-order logic of a practical representation of multivariate Bernstein polynomials. Using this representation, an algorithm for finding lower and upper bounds of the minimum and maximum values of a polynomial has been formalized and verified correct in the Prototype Verification System (PVS). The algorithm is used in the definition of proof strategies for formally and automatically solving polynomial global optimization problems.
C1 [Munoz, Cesar; Narkawicz, Anthony] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Munoz, C (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM Cesar.A.Munoz@nasa.gov; Anthony.Narkawicz@nasa.gov
NR 43
TC 14
Z9 14
U1 1
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0168-7433
J9 J AUTOM REASONING
JI J. Autom. Reasoning
PD AUG
PY 2013
VL 51
IS 2
BP 151
EP 196
DI 10.1007/s10817-012-9256-3
PG 46
WC Computer Science, Artificial Intelligence
SC Computer Science
GA 177RT
UT WOS:000321393800002
ER
PT J
AU Freund, F
AF Freund, Friedemann
TI Earthquake forewarning - A multidisciplinary challenge from the ground
up to space
SO ACTA GEOPHYSICA
LA English
DT Article
DE pre-earthquake signals; peroxy defects; positive holes; air ionization;
mesospheric lightning; ionospheric perturbations; Total Electron Content
ID MAGNESIUM-OXIDE; ELECTROMAGNETIC EMISSIONS; IONOSPHERIC ANOMALIES;
SATELLITE DETECTION; MAJOR EARTHQUAKES; IGNEOUS ROCKS; LOW-FREQUENCY;
PRECURSORS; SURFACE; HOLES
AB Most destructive earthquakes nucleate at between 5-7 km and about 35-40 km depth. Before earthquakes, rocks are subjected to increasing stress. Not every stress increase leads to rupture. To understand pre-earthquake phenomena we note that igneous and high-grade metamorphic rocks contain defects which, upon stressing, release defect electrons in the oxygen anion sublattice, known as positive holes. These charge carriers are highly mobile, able to flow out of stressed rocks into surrounding unstressed rocks. They form electric currents, which emit electromagnetic radiation, sometimes in pulses, sometimes sustained. The arrival of positive holes at the ground-air interface can lead to air ionization, often exclusively positive. Ionized air rising upward can lead to cloud condensation. The upward flow of positive ions can lead to instabilities in the mesosphere, to mesospheric lightning, to changes in the Total Electron Content (TEC) at the lower edge of the ionosphere, and electric field turbulences. Advances in deciphering the earthquake process can only be achieved in a broadly multidisciplinary spirit.
C1 [Freund, Friedemann] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Freund, Friedemann] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
[Freund, Friedemann] Carl Sagan Ctr, SETI Inst, Mountain View, CA USA.
RP Freund, F (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM friedemann.t.freund@nasa.gov
FU NASA Goddard Space Flight Center through its GEST Scholarship Program;
NASA Earth Surface and Interior program; NASA Exobiology Program; NASA
Ames Research Center
FX The work reported here has evolved over a period of more than 30 years.
It has benefited from innumerable discussions with students and
colleagues, whose names are listed in the referenced papers. In recent
years I acknowledge many fruitful discussions and joint experiments with
Dr. Akihiro Takeuchi, Dr. Bobby Lau, Dr. Robert Dahlgren, Dr. Stuart
Pilorz, and bright-eyed students. Much of the basic solid state physics
concept of positive hole charge carriers evolved through my
collaboration with Dr. Minoru Freund, my son who died in early 2012, in
the prime of his life, after a long, unwinnable battle with cancer. I
thank Marek Golkowski for permission to use his schematics for Fig. 6a.
My special thanks go to Morris Cohen, Georgia Institute of Technology,
for advice on the Global Electric Cirucit. Funding for this work has
come from NASA Goddard Space Flight Center through its GEST Scholarship
Program, from the NASA Earth Surface and Interior program (Dr. John
LaBrecque) and the NASA Exobiology Program (Dr. Michael New) as well as
from the NASA Ames Research Center under the leadership of Dr. Pete
Worden.
NR 94
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U1 4
U2 26
PU VERSITA
PI WARSAW
PA SOLIPSKA 14A-1, 02-482 WARSAW, POLAND
SN 1895-6572
J9 ACTA GEOPHYS
JI Acta Geophys.
PD AUG
PY 2013
VL 61
IS 4
BP 775
EP 807
DI 10.2478/s11600-013-0130-4
PG 33
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 163JG
UT WOS:000320331500002
ER
PT J
AU Moxley, FI
Chuss, DT
Dai, WZ
AF Moxley, Frederick Ira, III
Chuss, David T.
Dai, Weizhong
TI A generalized finite-difference time-domain scheme for solving nonlinear
Schrodinger equations
SO COMPUTER PHYSICS COMMUNICATIONS
LA English
DT Article
DE Finite-difference time-domain (FDTD) scheme; Nonlinear Schrodinger
equation; Soliton
ID DISCRETIZATION METHOD QDM; WAVES; MEDIA; BEAMS
AB Recently, we have developed a generalized finite-difference time-domain (G-FDTD) method for solving the time dependent linear Schrodinger equation. The G-FDTD is explicit and permits an accurate solution with simple computation, and also relaxes the stability condition as compared with the original FDTD scheme. In this article, we extend the G-FDTD scheme to solve nonlinear Schrodinger equations. Using the discrete energy method, the G-FDTD scheme is shown to satisfy a discrete analogous form of the conservation law. The obtained scheme is tested by three examples of soliton propagation, including bright and dark solitons as well as a 2D case. Compared with other popular existing methods, numerical results show that the present scheme provides a more accurate solution. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Moxley, Frederick Ira, III; Dai, Weizhong] Louisiana Tech Univ, Coll Engn & Sci, Ruston, LA 71272 USA.
[Chuss, David T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Dai, WZ (reprint author), Louisiana Tech Univ, Coll Engn & Sci, Ruston, LA 71272 USA.
EM dai@coes.latech.edu
FU NASA EPSCoR & LaSPACE, Louisiana
FX The research was supported by a grant from NASA EPSCoR & LaSPACE,
Louisiana.
NR 47
TC 5
Z9 5
U1 1
U2 27
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0010-4655
J9 COMPUT PHYS COMMUN
JI Comput. Phys. Commun.
PD AUG
PY 2013
VL 184
IS 8
BP 1834
EP 1841
DI 10.1016/j.cpc.2013.03.006
PG 8
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA 160VG
UT WOS:000320148000004
ER
PT J
AU Bretar, F
Arab-Sedze, M
Champion, J
Pierrot-Deseilligny, M
Heggy, E
Jacquemoud, S
AF Bretar, F.
Arab-Sedze, M.
Champion, J.
Pierrot-Deseilligny, M.
Heggy, E.
Jacquemoud, S.
TI An advanced photogrammetric method to measure surface roughness:
Application to volcanic terrains in the Piton de la Fournaise, Reunion
Island
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Surface roughness; Image correlation; Volcanic terrains; Roughness
anisotropy; Microtopography
ID FRACTAL DIMENSION; SOIL ROUGHNESS; RADAR; FEATURES; BACKSCATTERING;
RETRIEVAL; RAINFALL
AB We present a rapid in situ photogrammetric method to characterize surface roughness by taking overlapping photographs of a scene. The method uses a single digital camera to create a high-resolution digital terrain model (pixel size of similar to 1.32 mm) by means of a free open-source stereovision software. It is based on an auto-calibration process, which calculates the 3D geometry of the images, and an efficient multi-image correlation algorithm. The method is successfully applied to four different volcanic surfaces namely, a'a lava flows, pahoehoe lava flows, slabby pahoehoe lava flows, and lapilli deposits. These surfaces were sampled in the Piton de la Foumaise volcano (Reunion Island) in October, 2011, and displayed various terrain roughnesses. Our in situ measurements allow deriving digital terrain models that reproduce the millimeter-scale height variations of the surfaces over about 12 m(2). Five parameters characterizing surface topography are derived along unidirectional profiles: the root-mean-square height (xi), the correlation length (L-c), the ratio Z(s) = xi(2)/L-c, the tortuosity index (t), and the fractal dimension (D). Anisotropy in the surface roughness has been first investigated using 1-m-long profiles circularly arranged around a central point. The results show that L-c, Z(s) and D effectively catch preferential directions in the structure of bare surfaces. Secondly, we studied the variation of these parameters as a function of the profile length by drawing random profiles from 1 to 12 m in length. We verified that xi and L-c increase with the profile length and, therefore, are not appropriate to characterize surface roughness variation. We conclude that Z(s) and D are better suited to extract roughness information for multiple eruptive terrains with complex surface texture. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Bretar, F.] CETE Normandie Ctr, Lab Pouts & Chaussees, F-76121 Grand Quevilly, France.
[Arab-Sedze, M.; Champion, J.; Jacquemoud, S.] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, UMR CNRS 7154, F-75013 Paris, France.
[Arab-Sedze, M.] IGN, Lab MATIS, F-94160 St Mande, France.
[Pierrot-Deseilligny, M.] IGN ENSG, Lab Geomat Appl, F-77455 Marne La Vallee 2, France.
[Heggy, E.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bretar, F (reprint author), Consulat Gen France Shanghai, Serv Sci & Technol, Haitong Securities Bldg,2F,Suite 201,689 Guangdon, Shanghai 200001, Peoples R China.
EM frederic.bretar@ieee.org; sedze@ipgp.fr; champion@ipgp.fr;
marc.pierrot-deseilligny@ensg.eu; heggy@jpl.nasa.gov; jacquemoud@ipgp.fr
RI Jacquemoud, Stephane/F-8842-2010; Champion, Jason/O-4690-2014
OI Champion, Jason/0000-0002-9256-8917
FU CNES Terre Ocean Surfaces Continentales Atmosphere (TOSCA) program in
the frame of the DEVOIR (DEformation of active vegetated VOlcanos using
Insar and lidaR) project; DESDynI (Deformation, Ecosystem Structure and
Dynamics of Ice) team; National Aeronautics and Space Administration;
Observatoire Volcanologique du Piton de la Fournaise (IPGP)
FX This work was funded by the CNES Terre Ocean Surfaces Continentales
Atmosphere (TOSCA) program in the frame of the DEVOIR (DEformation of
active vegetated VOlcanos using Insar and lidaR) project. E. Heggy and
M. Arab-Sedze were also supported by the DESDynI (Deformation, Ecosystem
Structure and Dynamics of Ice) team. 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. We thank our colleagues from the Observatoire
Volcanologique du Piton de la Fournaise (IPGP) for their support during
the geophysical survey and M. Dechambre (LATMOS) for the fruitful
discussions about roughness. This paper is an IPGP contribution number
3379.
NR 39
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U1 1
U2 46
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD AUG
PY 2013
VL 135
BP 1
EP 11
DI 10.1016/j.rse.2013.03.026
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 164OJ
UT WOS:000320419100001
ER
PT J
AU Siegel, DA
Behrenfeld, M
Maritorena, S
McClain, CR
Antoine, D
Bailey, SW
Bontempi, PS
Boss, ES
Dierssen, HM
Doney, SC
Eplee, RE
Evans, RH
Feldman, GC
Fields, E
Franz, BA
Kuring, NA
Mengelt, C
Nelson, NB
Patt, FS
Robinson, WD
Sarmiento, JL
Swan, CM
Werdell, PJ
Westberry, TK
Wilding, JG
Yoder, JA
AF Siegel, D. A.
Behrenfeld, Mj.
Maritorena, S.
McClain, C. R.
Antoine, D.
Bailey, S. W.
Bontempi, P. S.
Boss, E. S.
Dierssen, H. M.
Doney, S. C.
Eplee, R. E., Jr.
Evans, R. H.
Feldman, G. C.
Fields, E.
Franz, B. A.
Kuring, N. A.
Mengelt, C.
Nelson, N. B.
Patt, F. S.
Robinson, W. D.
Sarmiento, J. L.
Swan, C. M.
Werdell, P. J.
Westberry, T. K.
Wilding, J. G.
Yoder, J. A.
TI Regional to global assessments of phytoplankton dynamics from the
SeaWiFS mission
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Ocean color; SeaWiFS; Phytoplankton; Colored dissolved organic matter;
Decadal trends
ID DISSOLVED ORGANIC-MATTER; PARTICULATE BEAM-ATTENUATION; CHLOROPHYLL-A
CONCENTRATION; INHERENT OPTICAL-PROPERTIES; CRITICAL DEPTH HYPOTHESIS;
OCEAN COLOR OBSERVATIONS; CASE-1 WATERS; SARGASSO SEA;
PHYSIOLOGICAL-RESPONSES; MULTISENSOR APPROACH
AB Photosynthetic production of organic matter by microscopic oceanic phytoplankton fuels ocean ecosystems and contributes roughly half of the Earth's net primary production. For 13 years, the Sea-viewing Wide Field-of-view Sensor (SeaWiFS) mission provided the first consistent, synoptic observations of global ocean ecosystems. Changes in the surface chlorophyll concentration, the primary biological property retrieved from SeaWiFS, have traditionally been used as a metric for phytoplankton abundance and its distribution largely reflects patterns in vertical nutrient transport. On regional to global scales, chlorophyll concentrations covary with sea surface temperature (SST) because SST changes reflect light and nutrient conditions. However, the ocean may be too complex to be well characterized using a single index such as the chlorophyll concentration. A semi-analytical bio-optical algorithm is used to help interpret regional to global SeaWiFS chlorophyll observations from using three independent, well-validated ocean color data products; the chlorophyll a concentration, absorption by CDM and particulate backscattering. First, we show that observed long-term, global-scale trends in standard chlorophyll retrievals are likely compromised by coincident changes in CDM. Second, we partition the chlorophyll signal into a component due to phytoplankton biomass changes and a component caused by physiological adjustments in intracellular chlorophyll concentrations to changes in mixed layer light levels. We show that biomass changes dominate chlorophyll signals for the high latitude seas and where persistent vertical upwelling is known to occur, while physiological processes dominate chlorophyll variability over much of the tropical and subtropical oceans. The SeaWiFS data set demonstrates complexity in the interpretation of changes in regional to global phytoplankton distributions and illustrates limitations for the assessment of phytoplankton dynamics using chlorophyll retrievals alone. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Siegel, D. A.; Maritorena, S.; Fields, E.; Nelson, N. B.; Swan, C. M.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA.
[Behrenfeld, Mj.; Westberry, T. K.] Oregon State Univ, Corvallis, OR 97331 USA.
[McClain, C. R.; Bailey, S. W.; Eplee, R. E., Jr.; Franz, B. A.; Kuring, N. A.; Patt, F. S.; Robinson, W. D.; Werdell, P. J.; Wilding, J. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Antoine, D.] Lab Oceanograp Villefranche, F-06238 Villefranche Sur Mer, France.
[Bontempi, P. S.] NASA Headquarters, Washington, DC 20546 USA.
[Boss, E. S.] Univ Maine, Orono, ME 04469 USA.
[Dierssen, H. M.] Univ Connecticut, Groton, CT 06340 USA.
[Doney, S. C.; Yoder, J. A.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Evans, R. H.] Univ Miami, Miami, FL 33149 USA.
[Mengelt, C.] Natl Acad, Ocean Studies Board, Washington, DC 20001 USA.
[Sarmiento, J. L.] Princeton Univ, Princeton, NJ 08540 USA.
RP Siegel, DA (reprint author), Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA.
EM davey@eri.ucsb.edu
RI Antoine, David/C-3817-2013; Doney, Scott/F-9247-2010; Siegel,
David/C-5587-2008; Nelson, Norman/B-7343-2014; Werdell,
Jeremy/D-8265-2012; Boss, Emmanuel/C-5765-2009; Franz,
Bryan/D-6284-2012; Bailey, Sean/D-3077-2017
OI Antoine, David/0000-0002-9082-2395; Doney, Scott/0000-0002-3683-2437;
Nelson, Norman/0000-0003-1767-7598; Boss, Emmanuel/0000-0002-8334-9595;
Franz, Bryan/0000-0003-0293-2082; Bailey, Sean/0000-0001-8339-9763
FU NASA Ocean Biology and Biogeochemistry program
FX The authors would like to acknowledge the NASA Ocean Biology and
Biogeochemistry program for its long-term support of satellite ocean
color research and the Orbital Sciences Corporation and GeoEye who were
responsible for the launch, satellite integration and on-orbit
management the SeaWiFS mission. The authors would also like to thank the
anonymous reviewers for their excellent and extremely helpful comments
on our manuscript.
NR 106
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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 AUG
PY 2013
VL 135
BP 77
EP 91
DI 10.1016/j.rse.2013.03.025
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 164OJ
UT WOS:000320419100007
ER
PT J
AU Crawford, CJ
Manson, SM
Bauer, ME
Hall, DK
AF Crawford, Christopher J.
Manson, Steven M.
Bauer, Marvin E.
Hall, Dorothy K.
TI Multitemporal snow cover mapping in mountainous terrain for Landsat
climate data record development
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Landsat; Multitemporal; Snow cover; Climate data record; Mountains
ID WESTERN UNITED-STATES; THEMATIC MAPPER; RADIOMETRIC CALIBRATION;
NORTH-AMERICA; CLOUD-COVER; TM DATA; MODIS; REFLECTANCE; VARIABILITY;
ACCURACY
AB A multitemporal method to map snow cover in mountainous terrain is proposed to guide Landsat climate data record (CDR) development. The Landsat image archive including MSS, TM, and ETM + imagery was used to construct a prototype Landsat snow cover CDR for the interior northwestern United States. Landsat snow cover CDRs are designed to capture snow-covered area (SCA) variability at discrete bi-monthly intervals that correspond to ground-based snow telemetry (SNOTEL) snow-water-equivalent (SWE) measurements. The June 1 bi-monthly interval was selected for initial CDR development, and was based on peak snowmelt timing for this mountainous region. Fifty-four Landsat images from 1975 to 2011 were preprocessed that included image registration, top-of-the-atmosphere (TOA) reflectance conversion, cloud and shadow masking, and topographic normalization. Snow covered pixels were retrieved using the normalized difference snow index (NDSI) and unsupervised classification, and pixels having greater (less) than 50% snow cover were classified presence (absence). A normalized SCA equation was derived to independently estimate SCA given missing image coverage and cloud-shadow contamination. Relative frequency maps of missing pixels were assembled to assess whether systematic biases were embedded within this Landsat CDR. Our results suggest that it is possible to confidently estimate historical bi-monthly SCA from partially cloudy Landsat images. This multitemporal method is intended to guide Landsat CDR development for freshwater-scarce regions of the western US to monitor climate-driven changes in mountain snowpack extent. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Crawford, Christopher J.; Manson, Steven M.] Univ Minnesota Twin Cities, Dept Geog, Minneapolis, MN 55455 USA.
[Bauer, Marvin E.] Univ Minnesota Twin Cities, Dept Forest Resources, St Paul, MN 55108 USA.
[Hall, Dorothy K.] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Crawford, CJ (reprint author), Univ Minnesota Twin Cities, Dept Geog, 414 Social Sci,267 19th Ave S, Minneapolis, MN 55455 USA.
EM crawf188@umn.edu
OI Manson, Steven/0000-0001-7697-5339
FU NASA Earth and Space Science Fellowship [NNX10A073H]; Association of
American Geographers Dissertation Research Grant; Association of
American Geographers Mountain Geography Specialty Group Research Grant
FX A NASA Earth and Space Science Fellowship grant number NNX10A073H, an
Association of American Geographers Dissertation Research Grant, and an
Association of American Geographers Mountain Geography Specialty Group
Research Grant funded this research. We would like to thank George
Riggs, James Foster, and Mike Mommsen for constructive feedback during
the development of this research and manuscript preparation. Additional
thanks are extended to Kurt Kipfmueller and Scott St. George for
assistance with MATLAB image processing code development. We are also
grateful for anonymous reviewer comments during manuscript preparation.
NR 64
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD AUG
PY 2013
VL 135
BP 224
EP 233
DI 10.1016/j.rse.2013.04.004
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 164OJ
UT WOS:000320419100019
ER
PT J
AU Xin, QC
Olofsson, P
Zhu, Z
Tan, B
Woodcock, CE
AF Xin, Qinchuan
Olofsson, Pontus
Zhu, Zhe
Tan, Bin
Woodcock, Curtis E.
TI Toward near real-time monitoring of forest disturbance by fusion of
MODIS and Landsat data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE MODIS; Landsat; Fusion; Time-series; Real-time; Change detection; Land
change; Forest disturbance; Point spread function
ID REMOTELY-SENSED DATA; SURFACE REFLECTANCE; SATELLITE DATA; COVER CHANGE;
SERIES; IMAGERY; IMPACT; DEFORESTATION; ACCURACY; PRODUCTS
AB Timely and accurate monitoring of forest disturbance is essential to help us understand how the Earth system is changing. MODIS (Moderate Resolution Imaging Spectroradiometer) imagery and subsequent MODIS products provide near-daily global coverage and have transformed the ways we study and monitor the Earth. To monitor forest disturbance, it is necessary to be able to compare observations of the same place from different times, but this is a challenging task using MODIS data as observations from different days have varying view angles and pixel sizes, and cover slightly different areas. In this paper, we propose a method to fuse MODIS and Landsat data in a way that allows for near real-time monitoring of forest disturbance. The method is based on using Landsat time-series images to predict the next MODIS image, which forms a stable basis for comparison with new MODIS acquisitions. The predicted MODIS images represent what the surface should look like assuming no disturbance, and the difference in the spectral signatures between predicted and observed MODIS images becomes the "signal" used for detecting forest disturbance. The method was able to detect subpixel forest disturbance with a producer's accuracy of 81% and a user's accuracy of 90%. Patches of forest disturbance as small as 5 to 7 ha in size were detected on a daily basis. The encouraging results indicate that the presented fusion method holds promise for improving monitoring of forest disturbance in near real-time. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Xin, Qinchuan] Tsinghua Univ, Ctr Earth Syst Sci, Minist Educ, Key Lab Earth Syst Modeling, Beijing 100084, Peoples R China.
[Xin, Qinchuan; Olofsson, Pontus; Zhu, Zhe; Woodcock, Curtis E.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Tan, Bin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Xin, QC (reprint author), Tsinghua Univ, Ctr Earth Syst Sci, Minist Educ, Key Lab Earth Syst Modeling, Beijing 100084, Peoples R China.
EM xqcchina@gmail.com
RI Zhu, Zhe/K-3518-2015; Xin, Qinchuan/O-3276-2014
OI Zhu, Zhe/0000-0001-8283-6407; Xin, Qinchuan/0000-0003-1146-4874
NR 52
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD AUG
PY 2013
VL 135
BP 234
EP 247
DI 10.1016/j.rse.2013.04.002
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 164OJ
UT WOS:000320419100020
ER
PT J
AU Kozachkov, H
Kolodziejska, J
Johnson, WL
Hofmann, DC
AF Kozachkov, Henry
Kolodziejska, Joanna
Johnson, William L.
Hofmann, Douglas C.
TI Effect of cooling rate on the volume fraction of B2 phases in a CuZrAlCo
metallic glass matrix composite
SO INTERMETALLICS
LA English
DT Article
DE Composites; Intermetallics; Elastic properties; Martensitic
transformations; Shape-memory effects; Casting
ID MECHANICAL-PROPERTIES; TENSILE DUCTILITY; MICROSTRUCTURE; DEFORMATION;
TRANSFORMATION; DENDRITES
AB The material properties of bulk metallic glass matrix composites (BMGMCs) depend strongly on the morphology and elastic constants of the included crystalline phase. Transformation induced plasticity (TRIP) BMGMCs based on the Cu-Zr system are alternatives to traditional dendrite-reinforced BMGMCs. Samples of a representative alloy, Zr48Cu47.5Al4Co0.5, are fabricated in various dimensions and characterized using DSC, SEM, and ultrasonic measurement of elastic constants. It is shown that the Cu-Zr system uniquely softens during crystallization, and the microstructure of the alloy depends strongly on the rate of cooling. We conclude by discussing how combinations of part design and alloy development could be used to utilize these alloys in applications. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Kozachkov, Henry; Kolodziejska, Joanna; Johnson, William L.; Hofmann, Douglas C.] CALTECH, Keck Lab Engn Mat, Pasadena, CA 91125 USA.
[Hofmann, Douglas C.] CALTECH, Jet Prop Lab, Engn & Sci Directorate, Pasadena, CA 91109 USA.
RP Hofmann, DC (reprint author), CALTECH, Keck Lab Engn Mat, Pasadena, CA 91125 USA.
EM dch@jpi.nasa.gov
FU National Aeronautics and Space Administration (NASA), Exploration
Systems Mission Directorate [MSFC-NRA10]; Air Force Office of Scientific
Research [RF01152700/PO60020925]; Office of Naval Research
[N0000-14-07-1-1115]
FX This work was supported by the National Aeronautics and Space
Administration (NASA), Exploration Systems Mission Directorate, under
Contract No. MSFC-NRA10, and the Air Force Office of Scientific Research
under grant no. RF01152700/PO60020925. Some graduate student support was
provided by the Office of Naval Research, under grant
N0000-14-07-1-1115.
NR 29
TC 9
Z9 10
U1 3
U2 83
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0966-9795
J9 INTERMETALLICS
JI Intermetallics
PD AUG
PY 2013
VL 39
BP 89
EP 93
DI 10.1016/j.intermet.2013.03.017
PG 5
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA 149HJ
UT WOS:000319309300014
ER
PT J
AU Echternach, PM
Stone, KJ
Bradford, CM
Day, PK
Wilson, DW
Megerian, KG
Llombart, N
Bueno, J
AF Echternach, P. M.
Stone, K. J.
Bradford, C. M.
Day, P. K.
Wilson, D. W.
Megerian, K. G.
Llombart, N.
Bueno, J.
TI Photon shot noise limited detection of terahertz radiation using a
quantum capacitance detector
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID SINGLE COOPER-PAIR; TES
AB We observed a sweep rate dependence of the quantum capacitance in a single Cooper-Pair box used as the readout of a Quantum Capacitance Detector. A model was developed that fits the data over five orders of magnitude in sweep rate and optical signal power and provides a natural calibration of the absorbed power. We are thereby able to measure the noise equivalent power of the detector as a function of absorbed power. We find that it is shot-noise-limited in detecting 1.5 THz photons with absorbed power ranging from 1 x 10(-22) W to 1 x 10(-17) W. (C) 2013 AIP Publishing LLC.
C1 [Echternach, P. M.; Stone, K. J.; Bradford, C. M.; Day, P. K.; Wilson, D. W.; Megerian, K. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Llombart, N.] Delft Univ Technol, Delft, Netherlands.
[Bueno, J.] Space Res Org Netherlands, Utrecht, Netherlands.
RP Echternach, PM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM pierre.m.echternach@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX We thank Richard Muller for electron beam lithography, Jonathan Kawamura
for assistance with optical alignment of the detectors, and Per Delsing
for fruitful discussions. 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 24
TC 4
Z9 4
U1 1
U2 10
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 JUL 29
PY 2013
VL 103
IS 5
AR 053510
DI 10.1063/1.4817585
PG 5
WC Physics, Applied
SC Physics
GA 195SD
UT WOS:000322723000112
ER
PT J
AU Zhai, PW
Hu, YX
Trepte, CR
Winker, DM
Josset, DB
Lucker, PL
Kattawar, GW
AF Zhai, Peng-Wang
Hu, Yongxiang
Trepte, Charles R.
Winker, David M.
Josset, Damien B.
Lucker, Patricia L.
Kattawar, George W.
TI Inherent optical properties of the coccolithophore: Emiliania huxleyi
SO OPTICS EXPRESS
LA English
DT Article
ID DISK-LIKE PARTICLES; TIME-DOMAIN METHOD; DISCRETE-DIPOLE APPROXIMATION;
LIGHT-SCATTERING; MUELLER MATRIX; SIZE DISTRIBUTIONS; SATELLITE DATA;
OCEAN; BACKSCATTERING; WATER
AB A realistic nonspherical model for Emiliania huxleyi (EHUX) is built, based on electron micrographs of coccolithophore cells. The Inherent Optical Properties (IOP) of the EHUX are then calculated numerically by using the discrete dipole approximation. The coccolithophore model includes a near-spherical core with the refractive index of 1.04+ m(i)j, and a carbonate shell formed by smaller coccoliths with refractive index of 1.2+ m(i)j, where m(i) = 0 or 0.01 and j(2) = -1. The reported IOP are the Mueller scattering matrix, backscattering probability, and depolarization ratio. Our calculation shows that the Mueller matrices of coccolithophores show different angular dependence from those of coccoliths. (C) 2013 Optical Society of America
C1 [Zhai, Peng-Wang; Josset, Damien B.; Lucker, Patricia L.] MS 475 NASA Langley Res Ctr, SSAI, Hampton, VA 23681 USA.
[Hu, Yongxiang; Trepte, Charles R.; Winker, David M.] MS 475 NASA 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), MS 475 NASA Langley Res Ctr, SSAI, Hampton, VA 23681 USA.
EM Pengwang.zhai-1@nasa.gov
RI Hu, Yongxiang/K-4426-2012
FU NASA; CALIPSO mission; ACE ocean lidar concept studies
FX This study is partially supported by the NASA Radiation Science program
administrated by Hal Maring and the Biogeochemistry program
administrated by Paula Bontempi. It is also partially supported by the
CALIPSO mission and the ACE ocean lidar concept studies. We thank two
anonymous reviewers for their insightful comments.
NR 39
TC 2
Z9 2
U1 0
U2 18
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD JUL 29
PY 2013
VL 21
IS 15
BP 17625
EP 17638
DI 10.1364/OE.21.017625
PG 14
WC Optics
SC Optics
GA 190UJ
UT WOS:000322366300024
PM 23938635
ER
PT J
AU Minazzoli, O
AF Minazzoli, Olivier
TI Conservation laws in theories with universal gravity/matter coupling
SO PHYSICAL REVIEW D
LA English
DT Article
ID MACHS PRINCIPLE; STRING THEORY; HISTORY
AB In this paper, we investigate the conservation laws of different types of particles in theories with a universal gravity/matter coupling. The result brings new insight about previous studies on universal gravity/matter theories. Especially, the paper demonstrates that, for perfect fluids, there is an equivalence between the assumption L-m = -is an element of, where is an element of is the total energy density, and the assumption that the matter fluid current is conserved [del(sigma)(rho u(sigma)) = 0, where rho is the rest mass density]. However, the main result is given in the general case in which one does not make any assumption on the conservation of the matter fluid current.
C1 [Minazzoli, Olivier] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, UMR ARTEMIS, F-06304 Nice 4, France.
[Minazzoli, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Minazzoli, O (reprint author), Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, UMR ARTEMIS, BP4229, F-06304 Nice 4, France.
EM ominazzoli@gmail.com
OI Minazzoli, Olivier/0000-0002-3151-7593
FU NASA; NASA Postdoctoral Program at the Jet Propulsion Laboratory,
California Institute of Technology
FX This research was partly done as an invited researcher of the
Observatoire de la Cote d'Azur. This research was partly 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. Government
sponsorship acknowledged. The author wants to thank Aurelien Hees,
Tiberiu Harko, Francisco Lobo and Viktor Toth for reading the paper and
for their interesting comments.
NR 50
TC 12
Z9 13
U1 0
U2 2
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 JUL 29
PY 2013
VL 88
IS 2
AR 027506
DI 10.1103/PhysRevD.88.027506
PG 5
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 193QU
UT WOS:000322577300011
ER
PT J
AU Shume, EB
Mannucci, AJ
AF Shume, E. B.
Mannucci, A. J.
TI First calculation of phase and coherence of longitudinally separated
L-band equatorial ionospheric scintillation
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE scintillation; forecast; plasma irregularities
ID IRREGULARITIES
AB We present the first calculation of phase and coherence of cross-wavelet transform applied to longitudinally separated L-band equatorial ionospheric scintillation observations received from Geostationary Earth Orbit (GEO) satellites. The phase and coherence analysis were employed on two pairs of observations: (1) SAo Luis and Rio Branco and (2) Alta Floresta and Huancayo. For these case studies, in statistically significant and high-coherence regions, scintillation observations over SAo Luis (Alta Floresta) lead that of Rio Branco (Huancayo) by approximate to 2 to 3 h with a 95%frequency. If L-band scintillation happens over SAo Luis (Alta Floresta), there is a 95%likelihood that scintillation would happen to the west over Rio Branco (Huancayo) after approximate to 2 to 3 h, suggesting that a forecast can be made ahead of scintillation occurrences. The phase and coherence relationships between the longitudinally separated scintillation-producing regions can be connected to the large-scale wave structures which are reported to be related to the generation of equatorial spread F and scintillation.
C1 [Shume, E. B.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Shume, EB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Esayas.B.Shume@jpl.nasa.gov
RI Shume, Esayas/I-3354-2013;
OI Shume, Esayas/0000-0002-4696-1283
FU NASA
FX The research was carried out at JPL, California Institute of Technology,
under a contract with NASA. E. Shume thanks the NPP administered by ORAU
under a contract with NASA. We thank Dr. C. E. Valladares for providing
the LISN data.
NR 14
TC 2
Z9 2
U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUL 28
PY 2013
VL 40
IS 14
BP 3496
EP 3501
DI 10.1002/grl.50702
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 204TP
UT WOS:000323392700002
ER
PT J
AU Grise, KM
Polvani, LM
Tselioudis, G
Wu, YT
Zelinka, MD
AF Grise, Kevin M.
Polvani, Lorenzo M.
Tselioudis, George
Wu, Yutian
Zelinka, Mark D.
TI The ozone hole indirect effect: Cloud-radiative anomalies accompanying
the poleward shift of the eddy-driven jet in the Southern Hemisphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ozone hole; cloud-radiative processes
ID CLIMATE; MODEL; ISCCP
AB This study quantifies the response of the clouds and the radiative budget of the Southern Hemisphere (SH) to the poleward shift in the tropospheric circulation induced by the development of the Antarctic ozone hole. Single forcing climate model integrations, in which only stratospheric ozone depletion is specified, indicate that (1) high-level and midlevel clouds closely follow the poleward shift in the SH midlatitude jet and that (2) low-level clouds decrease across most of the Southern Ocean. Similar cloud anomalies are found in satellite observations during periods when the jet is anomalously poleward. The hemispheric annual mean radiation response to the cloud anomalies is calculated to be approximately +0.25 W m(-2), arising largely from the reduction of the total cloud fraction at SH midlatitudes during austral summer. While these dynamically induced cloud and radiation anomalies are considerable and are supported by observational evidence, quantitative uncertainties remain from model biases in mean-state cloud-radiative processes.
C1 [Grise, Kevin M.; Polvani, Lorenzo M.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Polvani, Lorenzo M.; Tselioudis, George] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Polvani, Lorenzo M.; Tselioudis, George] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA.
[Tselioudis, George] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Wu, Yutian] NYU, Courant Inst Math Sci, Ctr Atmosphere Ocean Sci, New York, NY USA.
[Zelinka, Mark D.] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA USA.
RP Grise, KM (reprint author), Columbia Univ, Lamont Doherty Earth Observ, POB 1000,61 Rt 9W, Palisades, NY 10964 USA.
EM kgrise@ldeo.columbia.edu
RI Grise, Kevin/B-6939-2013; Zelinka, Mark/C-4627-2011
OI Grise, Kevin/0000-0003-0934-8129; Zelinka, Mark/0000-0002-6570-5445
FU National Science Foundation; U.S. Department of Energy (DOE) by Lawrence
Livermore National Laboratory [DE-AC52-07NA27344]; U.S. DOE's Office of
Science
FX We thank two anonymous reviewers for their helpful comments and G.J.P.
Correa for assistance with the model experiments. K. M. G. and L. M. P.
were supported by a National Science Foundation grant to Columbia
University. M.D.Z.'s contribution was performed under the auspices of
U.S. Department of Energy (DOE) by Lawrence Livermore National
Laboratory under contract DE-AC52-07NA27344 and was supported by the
Regional and Global Climate and Earth System Modeling programs of the
U.S. DOE's Office of Science.
NR 16
TC 23
Z9 23
U1 1
U2 37
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 JUL 28
PY 2013
VL 40
IS 14
BP 3688
EP 3692
DI 10.1002/grl.50675
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 204TP
UT WOS:000323392700036
ER
PT J
AU Loikith, PC
Lintner, BR
Kim, J
Lee, H
Neelin, JD
Waliser, DE
AF Loikith, P. C.
Lintner, B. R.
Kim, J.
Lee, H.
Neelin, J. D.
Waliser, D. E.
TI Classifying reanalysis surface temperature probability density functions
(PDFs) over North America with cluster analysis
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE surface temperature PDFs; cluster analysis; reanalysis; North America
ID PRECIPITATION; VARIABILITY; EXTREMES; MODELS
AB An important step in projecting future climate change impacts on extremes involves quantifying the underlying probability distribution functions (PDFs) of climate variables. However, doing so can prove challenging when multiple models and large domains are considered. Here an approach to PDF quantification using k-means clustering is considered. A standard clustering algorithm (with k=5 clusters) is applied to 33years of daily January surface temperature from two state-of-the-art reanalysis products, the North American Regional Reanalysis and the Modern Era Retrospective Analysis for Research and Applications. The resulting cluster assignments yield spatially coherent patterns that can be broadly related to distinct climate regimes over North America, e.g., low variability over the tropical oceans or temperature advection across stronger or weaker gradients. This technique has the potential to be a useful and intuitive tool for evaluation of model-simulated PDF structure and could provide insight into projections of future changes in temperature.
C1 [Loikith, P. C.; Lee, H.; Waliser, D. E.] NASA, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA.
[Lintner, B. R.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA.
[Kim, J.; Waliser, D. E.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Kim, J.; Neelin, J. D.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
RP Loikith, PC (reprint author), NASA, Jet Prop Lab, CALTECH, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM paul.c.loikith@jpl.nasa.gov
FU National Aeronautics and Space Administration; NSF [ExArch 1125798];
NOAA [NA11OAR4310099]; New Jersey Agricultural Experiment Station Hatch
grant [NJ07102]; NASA National Climate Assessment project
[11-NCA11-0028]; NASA AIST project [AIST-QRS-12-0002]
FX 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. Part of this research was funded
by NASA National Climate Assessment 11-NCA11-0028 and AIST
AIST-QRS-12-0002 projects, and the NSF ExArch 1125798 (P. C. L., J.K.,
H. L., and D. E. W). Part of this research was funded by NOAA
NA11OAR4310099 (J.D.N.) and New Jersey Agricultural Experiment Station
Hatch grant NJ07102 (B. R. L.). We thank Joyce Meyerson for her
assistance with figure visualization.
NR 18
TC 8
Z9 8
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUL 28
PY 2013
VL 40
IS 14
BP 3710
EP 3714
DI 10.1002/grl.50688
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 204TP
UT WOS:000323392700040
ER
PT J
AU Cooper, MJ
Martin, RV
Livesey, NJ
Degenstein, DA
Walker, KA
AF Cooper, Matthew J.
Martin, Randall V.
Livesey, Nathaniel J.
Degenstein, Doug A.
Walker, Kaley A.
TI Analysis of satellite remote sensing observations of low ozone events in
the tropical upper troposphere and links with convection
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ozone; convection; ENSO; upper troposphere
ID DEEP CONVECTION; OSCILLATION; CHEMISTRY; SPECTROMETER; CLIMATOLOGY;
VARIABILITY; RETRIEVALS; OSIRIS
AB Satellite observations from three instruments (Microwave Limb Sounder, Optical Spectrograph and Infrared Imaging System, and Atmospheric Chemistry Experiment Fourier Transform Spectrometer) reveal coherent patterns of low ozone events (<20 ppb) in the tropical upper troposphere. Using a chemical transport model (GEOS-Chem), we find that these events result from deep convective processes that rapidly transport air with low ozone concentrations from the marine boundary layer. These events occur with greater frequency over the tropical South Pacific warm pool, which is consistent with ozonesonde observations. The satellite observations indicate spatial shifts in the frequency of low ozone events that we attribute to changes in convection. As the location of the warm pool shifts eastward during El Nino events, the location of the most frequent low ozone events in the satellite record follows. Mapping of low ozone events over time reveals eastward propagating systems resembling the Madden-Julian Oscillation. These observations and analyses strengthen the link between deep convection and ozone concentrations in the tropical upper troposphere.
C1 [Cooper, Matthew J.; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Livesey, Nathaniel J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Degenstein, Doug A.] Univ Saskatchewan, Inst Space & Atmospher Sci, Dept Phys & Engn Phys, Saskatoon, SK, Canada.
[Walker, Kaley A.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Walker, Kaley A.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
RP Cooper, MJ (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
EM cooperm2@dal.ca
RI Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014
OI Martin, Randall/0000-0003-2632-8402;
FU NSERC; Canadian Space Agency
FX We thank Ian Folkins for helpful comments that improved the manuscript.
This research was supported by funding from the Canadian Space Agency.
MC was partially supported by an NSERC Fellowship.
NR 29
TC 7
Z9 7
U1 1
U2 16
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 JUL 28
PY 2013
VL 40
IS 14
BP 3761
EP 3765
DI 10.1002/grl.50717
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 204TP
UT WOS:000323392700049
ER
PT J
AU Mlynczak, MG
Hunt, LA
Marshall, BT
Mertens, CJ
Russell, JM
Siskind, D
Thompson, RE
Gordley, LL
AF Mlynczak, Martin G.
Hunt, Linda A.
Marshall, B. Thomas
Mertens, Christopher J.
Russell, James M., III
Siskind, David
Thompson, R. Earl
Gordley, Larry L.
TI Radiative constraints on the minimum atomic oxygen concentration in the
mesopause region
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE atomic oxygen; mesopause region; radiative constraints; energetics
ID ATMOSPHERE
AB Atomic oxygen [O] plays a fundamental role in the photochemistry and energy budget of the terrestrial mesopause region (80-100km). [O] is difficult to measure directly and is typically inferred at night from measurements of hydroxyl [OH] or molecular oxygen [O-2] emissions. During the day, measurements of ozone [O-3] concentration are used to infer [O]. These inferences carry significant uncertainties [Mlynczak et al., 2013a]. Recently, Mlynczak et al. [2013b] have used energy balance principles to set an upper limit on the annual global mean [O] concentration in the mesopause region. In this paper, we use night measurements of OH emission to set a lower limit on the global annual mean atomic oxygen concentration. These independent, radiatively constrained values of the maximum and minimum atomic oxygen concentration also place constraints on the magnitude of dynamical processes in the annual global mean energy budget of the mesopause region.
C1 [Mlynczak, Martin G.; Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Hunt, Linda A.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Marshall, B. Thomas; Thompson, R. Earl; Gordley, Larry L.] G&A Tech Software, Newport News, VA USA.
[Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Siskind, David] Naval Res Lab, Washington, DC USA.
RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM m.g.mlynczak@nasa.gov
FU NASA TIMED project; NASA Living with a Star program
FX The authors gratefully acknowledge support from the NASA TIMED project
and the NASA Living with a Star program.
NR 8
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
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUL 28
PY 2013
VL 40
IS 14
BP 3777
EP 3780
DI 10.1002/grl.50725
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 204TP
UT WOS:000323392700052
ER
PT J
AU Zimmerman, RK
AF Zimmerman, Robert K., Jr.
TI Reception of longitudinal vector potential radiation with a plasma
antenna
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
AB To help resolve the long-running debate between physicists and engineers regarding the existence of the magnetic vector potential, herewith we describe an experiment demonstrating reception of time-harmonic vector potential radiation at 1.3 GHz. (C) 2013 AIP Publishing LLC.
C1 NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
RP Zimmerman, RK (reprint author), NASA, Goddard Space Flight Ctr, Sigma Space Corp, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM rkzimmerman@gmail.com
NR 12
TC 0
Z9 0
U1 0
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD JUL 28
PY 2013
VL 114
IS 4
AR 044907
DI 10.1063/1.4816100
PG 5
WC Physics, Applied
SC Physics
GA 193DZ
UT WOS:000322539300112
ER
PT J
AU Arsenault, KR
Houser, PR
De Lannoy, GJM
Dirmeyer, PA
AF Arsenault, Kristi R.
Houser, Paul R.
De Lannoy, Gabrielle J. M.
Dirmeyer, Paul A.
TI Impacts of snow cover fraction data assimilation on modeled energy and
moisture budgets
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE snow cover; data assimilation; land surface model
ID LAND DATA ASSIMILATION; ENSEMBLE KALMAN FILTER; HYDROLOGIC DATA
ASSIMILATION; COMMUNITY CLIMATE MODEL; SURFACE MODEL;
INFORMATION-SYSTEM; WATER EQUIVALENT; SOIL-MOISTURE; MODIS; PREDICTION
AB Two data assimilation (DA) methods, a simple rule-based direct insertion (DI) approach and a one-dimensional ensemble Kalman filter (EnKF) method, are evaluated by assimilating snow cover fraction observations into the Community Land surface Model. The ensemble perturbation needed for the EnKF resulted in negative snowpack biases. Therefore, a correction is made to the ensemble bias using an approach that constrains the ensemble forecasts with a single unperturbed deterministic LSM run. This is shown to improve the final snow state analyses. The EnKF method produces slightly better results in higher elevation locations, whereas results indicate that the DI method has a performance advantage in lower elevation regions. In addition, the two DA methods are evaluated in terms of their overall impacts on the other land surface state variables (e.g., soil moisture) and fluxes (e.g., latent heat flux). The EnKF method is shown to have less impact overall than the DI method and causes less distortion of the hydrological budget. However, the land surface model adjusts more slowly to the smaller EnKF increments, which leads to smaller but slightly more persistent moisture budget errors than found with the DI updates. The DI method can remove almost instantly much of the modeled snowpack, but this also allows the model system to quickly revert to hydrological balance for nonsnowpack conditions.
C1 [Arsenault, Kristi R.] SAIC Inc, Beltsville, MD USA.
[Arsenault, Kristi R.; De Lannoy, Gabrielle J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Houser, Paul R.] George Mason Univ, Dept Geog & GeoInformat Sci, Fairfax, VA 22030 USA.
[De Lannoy, Gabrielle J. M.] USRA, Columbia, MD USA.
[Dirmeyer, Paul A.] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA.
[Dirmeyer, Paul A.] Ctr Ocean Land Atmosphere Studies, Calverton, MD USA.
RP Arsenault, KR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM kristi.r.arsenault@nasa.gov
RI Dirmeyer, Paul/B-6553-2016
OI Dirmeyer, Paul/0000-0003-3158-1752
FU NOAA [NA07OAR4310221]; NASA [NNX08AU51G, NNX08AV05H]
FX This work was funded by NOAA grant NA07OAR4310221 and NASA grants
NNX08AU51G, NNX08AV05H. The authors would like to thank Jagadish Shukla,
Zafer Boybeyi, and David Straus for their feedback and helpful
discussions. Computer resources were provided by the Institute of Global
Environment and Society. Gabrielle De Lannoy was a research fellow of
the Research Fund Flanders (Fonds Wetenschappelijk Onderzoek, FWO). We
greatly acknowledge Wade Crow and the three other anonymous reviewers
for their constructive comments.
NR 68
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUL 27
PY 2013
VL 118
IS 14
BP 7489
EP 7504
DI 10.1002/jgrd.50542
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 201DL
UT WOS:000323120800007
ER
PT J
AU Shi, MJ
Yang, ZL
Landerer, FW
AF Shi, Mingjie
Yang, Zong-Liang
Landerer, Felix W.
TI Representing and evaluating the landscape freeze/thaw properties and
their impacts on soil impermeability: Hydrological processes in the
community land model version 4
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE landscape frozen fraction; snow cover fraction; soil impermeability;
hydrological cycles; high-latitude regions; CLM4
ID GROUND THERMAL REGIME; SNOW COVER; RUNOFF; MANIPULATION; SIMULATION;
STORAGE; FROST
AB Snow cover at high latitudes is an excellent natural insulator that can maintain the underlying ground at a higher temperature than the overlying atmosphere. Soil impermeability usually varies when snow cover accumulates, which is closely related to soil and landscape freeze/thaw status. How snow cover affects the landscape frozen fraction and soil impermeability and how this impermeability regulates hydrological processes in cold regions have not been fully assessed and quantified. In order to understand these processes, this study performed a series of experiments by using the Community Land Model version 4 (CLM4). We first simulated the top-soil-layer ice, snow ice, and canopy ice to calculate the landscape frozen fraction, which was evaluated based on the Special Sensor Microwave/Imager (SSM/I) observed landscape freeze/thaw earth system data record (FT-ESDR) in two selected regions at high latitudes. Then two soil impermeability parameterizations were validated against various in situ and satellite observations. The results suggest the following: (1) compared to SSM/I FT-ESDR, CLM4 can capture the overall landscape freeze/thaw status in the regions north of 60 degrees N in boreal winter and spring; (2) as the snow cover fraction approaches unity, the CLM4-simulated landscape frozen fraction is mainly controlled by the snow ice amount, resulting in step changes between SSM/I FT-ESDR observed and CLM4-simulated landscape frozen fractions; and (3) in most of the cold regions, the timing of the boreal spring runoff simulations is improved by reducing the impermeable area in high landscape frozen fraction regions.
C1 [Shi, Mingjie; Yang, Zong-Liang] Univ Texas Austin, Dept Geol Sci, John A & Katherine G Jackson Sch Geosci, Austin, TX 78712 USA.
[Landerer, Felix W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Yang, ZL (reprint author), Univ Texas Austin, Dept Geol Sci, John A & Katherine G Jackson Sch Geosci, 1 Univ Stn C1100, Austin, TX 78712 USA.
EM liang@jsg.utexas.edu
RI Yang, Zong-Liang/B-4916-2011;
OI Landerer, Felix/0000-0003-2678-095X
FU U.S. National Aeronautics and Space Administration [NNX11AE42G]
FX This work was funded in part by the U.S. National Aeronautics and Space
Administration under the Interdisciplinary Science Project NNX11AE42G.
The computations were performed on Texas Advanced Computing Center and
the National Center for Atmospheric Research computer resources.
F.W.L.'s work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. We appreciate D. K. Hall for the
valuable suggestions, E. Podest for introducing SSM/I FT-ESDR, and S. C.
Swenson for providing the processed MERRA data. We also appreciate the
comments from three anonymous reviewers that led to significant
improvements of this paper. The authors would like to acknowledge the
language help from Patricia A. Bobeck and Adam R. Bowerman.
NR 35
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U2 22
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 JUL 27
PY 2013
VL 118
IS 14
BP 7542
EP 7557
DI 10.1002/jgrd.50576
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 201DL
UT WOS:000323120800011
ER
PT J
AU Lim, YK
Kim, HD
AF Lim, Young-Kwon
Kim, Hae-Dong
TI Impact of the dominant large-scale teleconnections on winter temperature
variability over East Asia
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE teleconnection; winter; temperature; East Asia
ID NORTHERN-HEMISPHERE WINTER; SOUTHERN-OSCILLATION; GEOPOTENTIAL HEIGHT;
UNITED-STATES; INTERANNUAL VARIATION; ARCTIC OSCILLATION; STATIONARY
WAVES; PRECIPITATION; PROPAGATION; FIELD
AB Monthly mean geopotential height for the past 33 DJF seasons archived in Modern Era Retrospective analysis for Research and Applications reanalysis is decomposed into the large-scale teleconnection patterns to explain their impacts on winter temperature variability over East Asia. Following Arctic Oscillation (AO) that explains the largest variance, East Atlantic/West Russia (EA/WR), West Pacific (WP) and El Nino-Southern Oscillation (ENSO) are identified as the first four leading modes that significantly explain East Asian winter temperature variation. While the northern part of East Asia north of 50 degrees N is prevailed by AO and EA/WR impacts, temperature in the midlatitudes (30 degrees N-50 degrees N), which include Mongolia, northeastern China, Shandong area, Korea, and Japan, is influenced by combined effect of the four leading teleconnections. ENSO impact on average over 33 winters is relatively weaker than the impact of the other three teleconnections. WP impact, which has received less attention than ENSO in earlier studies, characterizes winter temperatures over Korea, Japan, and central to southern China region south of 30 degrees N mainly by advective process from the Pacific. Upper level wave activity fluxes reveal that, for the AO case, the height and circulation anomalies affecting midlatitude East Asian winter temperature is mainly located at higher latitudes north of East Asia. Distribution of the fluxes also explains that the stationary wave train associated with EA/WR propagates southeastward from the western Russia, affecting the East Asian winter temperature. Investigation on the impact of each teleconnection for the selected years reveals that the most dominant teleconnection over East Asia is not the same at all years, indicating a great deal of interannual variability. Comparison in temperature anomaly distributions between observation and temperature anomaly constructed using the combined effect of four leading teleconnections clearly show a reasonable consistency between them, demonstrating that the seasonal winter temperature distributions over East Asia are substantially explained by these four large-scale circulation impacts.
C1 [Lim, Young-Kwon] NASA, Goddard Space Flight Ctr, Goddard Earth Sci Technol & Res, IM Syst Grp, Columbia, MD USA.
[Kim, Hae-Dong] Keimyung Univ, Coll Environm, Taegu, South Korea.
RP Kim, HD (reprint author), Keimyung Univ, Coll Environm, Taegu, South Korea.
EM khd@kmu.ac.kr
FU Keimyung University
FX This research was supported by the Scholar Research Grant of Keimyung
University in 2012.
NR 28
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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 JUL 27
PY 2013
VL 118
IS 14
BP 7835
EP 7848
DI 10.1002/jgrd.50462
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 201DL
UT WOS:000323120800032
ER
PT J
AU Sayer, AM
Hsu, NC
Bettenhausen, C
Jeong, MJ
AF Sayer, A. M.
Hsu, N. C.
Bettenhausen, C.
Jeong, M. -J.
TI Validation and uncertainty estimates for MODIS Collection 6 "Deep Blue"
aerosol data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol; MODIS; AERONET; Deep Blue; validation; Collection 6
ID OPTICAL DEPTH RETRIEVALS; DATA ASSIMILATION; BIDIRECTIONAL REFLECTANCE;
NORTH-AFRICA; MIDDLE-EAST; LAND; PRODUCTS; ALGORITHMS; INTENSITY;
AERONET
AB The Deep Blue aerosol optical depth (AOD) retrieval algorithm was introduced in Collection 5 of the Moderate Resolution Imaging Spectroradiometer (MODIS) product suite, and complemented the existing Dark Target land and ocean algorithms by retrieving AOD over bright arid land surfaces, such as deserts. The forthcoming Collection 6 of MODIS products will include a second generation Deep Blue algorithm, expanding coverage to all cloud-free and snow-free land surfaces. The Deep Blue dataset will also provide an estimate of the absolute uncertainty on AOD at 550 nm for each retrieval. This study describes the validation of Deep Blue Collection 6 AOD at 550 nm ((M)) from MODIS Aqua against Aerosol Robotic Network (AERONET) data from 60 sites to quantify these uncertainties. The highest quality (denoted quality assurance flag value 3) data are shown to have an absolute uncertainty of approximately (0.086+0.56(M))/AMF, where AMF is the geometric air mass factor. For a typical AMF of 2.8, this is approximately 0.03+0.20(M), comparable in quality to other satellite AOD datasets. Regional variability of retrieval performance and comparisons against Collection 5 results are also discussed.
C1 [Sayer, A. M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Greenbelt, MD USA.
[Sayer, A. M.; Hsu, N. C.; Bettenhausen, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bettenhausen, C.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Jeong, M. -J.] Gangneung Wonju Natl Univ, Gangneung City, South Korea.
RP Sayer, AM (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA.
EM andrew.sayer@nasa.gov
RI Sayer, Andrew/H-2314-2012
OI Sayer, Andrew/0000-0001-9149-1789
NR 32
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U1 8
U2 45
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 JUL 27
PY 2013
VL 118
IS 14
BP 7864
EP 7872
DI 10.1002/jgrd.50600
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 201DL
UT WOS:000323120800035
ER
PT J
AU Lang, TJ
Cummer, SA
Rutledge, SA
Lyons, WA
AF Lang, Timothy J.
Cummer, Steven A.
Rutledge, Steven A.
Lyons, Walter A.
TI The meteorology of negative cloud-to-ground lightning strokes with large
charge moment changes: Implications for negative sprites
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE negative sprites; charge moment change; negative lightning
ID MESOSCALE CONVECTIVE SYSTEMS; THUNDERSTORMS; DISCHARGES; INITIATION;
ELVES; RADAR; ARRAY
AB This study examined the meteorological characteristics of precipitation systems that produced 38 sprite-class negative cloud-to-ground (CG) strokes (i.e., peak currents in excess of 100kA and charge moment changes in excess of 800Ckm) as well as those that produced three confirmed negative sprites on 23 different days during 2009-2011. Within 15km of the negative sprite-parent/class stroke, the median characteristics for these systems were to produce negative CGs as 69.2% of all CGs, and for the 30dBZ radar reflectivity contour to reach on average 14.2km above mean sea level (MSL), during a 25min period encompassing the occurrence of the stroke. The median contiguous area of 30dBZ composite radar echo (i.e., maximum value in the vertical column) for these systems was 6.73x10(3)km(2). All but three of the discharges occurred in intense multicellular convection, with 30dBZ exceeding 10km MSL in altitude, while the others occurred in the stratiform regions of mesoscale convective systems. All but six of the systems produced greater than 50% negative CG lightning, though flash rates tended to be low near the stroke (1-2min(-1) on average). The results suggest that negative sprite-parent/class lightning typically occurs in precipitation systems of similar size and intensity as those that produce positive sprites, but not necessarily the same systems, and the negative lightning normally strikes ground in the convection rather than the stratiform precipitation. However, upper-level positive charge in the convection may play an important role in sprite-class/parent lightning of either polarity.
C1 [Lang, Timothy J.; Rutledge, Steven A.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Cummer, Steven A.] Duke Univ, Dept Elect & Comp Engn, Durham, NC USA.
[Lyons, Walter A.] FMA Res Inc, Ft Collins, CO USA.
RP Lang, TJ (reprint author), NASA, Marshall Space Flight Ctr ZP11, Huntsville, AL 35812 USA.
EM timothy.j.lang@nasa.gov
RI Cummer, Steven/A-6118-2008;
OI Cummer, Steven/0000-0002-0002-0613; Lang, Timothy/0000-0003-1576-572X
FU Defense Advanced Research Projects Agency under Nimbus program; National
Science Foundation [AGS-1010G6S7]
FX Vaisala supplied the NLDN flash-level data analyzed in this study and
also enables the CMCN by providing geolocation of high-iCMC strokes via
a real-time NLDN stroke-level data feed. These data were absolutely
critical to this study, and the authors offer their sincerest thanks to
Vaisala for providing them. Katherine Willingham provided the NMQ radar
mosaic data on behalf of NOAA. Bill McCaul of Universities Space
Research Association provided the NALMA data. Paul Hein of Colorado
State University assisted with the data analysis. The authors are
extremely grateful to all of these people and their agencies for their
gracious help in facilitating this research. The authors also thank the
journal editor and reviewers for their assistance with publishing this
study. This research was funded by the Defense Advanced Research
Projects Agency under the Nimbus program, as well as the National
Science Foundation under grant AGS-1010G6S7.
NR 41
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U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUL 27
PY 2013
VL 118
IS 14
BP 7886
EP 7896
DI 10.1002/jgrd.50595
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 201DL
UT WOS:000323120800037
ER
PT J
AU Bauer, SE
Bausch, A
Nazarenko, L
Tsigaridis, K
Xu, BQ
Edwards, R
Bisiaux, M
McConnell, J
AF Bauer, Susanne E.
Bausch, Alexandra
Nazarenko, Larissa
Tsigaridis, Kostas
Xu, Baiqing
Edwards, Ross
Bisiaux, Marion
McConnell, Joe
TI Historical and future black carbon deposition on the three ice caps: Ice
core measurements and model simulations from 1850 to 2100
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol; black carbon; deposition
ID GENERAL-CIRCULATION MODEL; GODDARD-INSTITUTE; CLIMATE; AEROSOLS;
ATMOSPHERE; SPACE; EMISSIONS; PLATEAU; RECORDS; SULFUR
AB Ice core measurements in conjunction with climate model simulations are of tremendous value when examining anthropogenic and natural aerosol loads and their role in past and future climates. Refractory black carbon (BC) records from the Arctic, the Antarctic, and the Himalayas are analyzed using three transient climate simulations performed with the Goddard Institute for Space Studies ModelE. Simulations differ in aerosol schemes (bulk aerosols vs. aerosol microphysics) and ocean couplings (fully coupled vs. prescribed ocean). Regional analyses for past (1850-2005) and future (2005-2100) carbonaceous aerosol simulations focus on the Antarctic, Greenland, and the Himalayas. Measurements from locations in the Antarctic show clean conditions with no detectable trend over the past 150years. Historical atmospheric deposition of BC and sulfur in Greenland shows strong trends and is primarily influenced by emissions from early twentieth century agricultural and domestic practices. Models fail to reproduce observations of a sharp eightfold BC increase in Greenland at the beginning of the twentieth century that could be due to the only threefold increase in the North American emission inventory. BC deposition in Greenland is about 10 times greater than in Antarctica and 10 times less than in Tibet. The Himalayas show the most complicated transport patterns, due to the complex terrain and dynamical regimes of this region. Projections of future climate based on the four CMIP5 Representative Concentration Pathways indicate further dramatic advances of pollution to the Tibetan Plateau along with decreasing BC deposition fluxes in Greenland and the Antarctic.
C1 [Bauer, Susanne E.; Bausch, Alexandra; Nazarenko, Larissa; Tsigaridis, Kostas] Columbia Univ, Earth Inst, Ctr Climate Syst Res, New York, NY 10025 USA.
[Bauer, Susanne E.; Nazarenko, Larissa; Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Xu, Baiqing] Chinese Acad Sci, Inst Tibetan Plateau Res, Key Lab Tibetan Environm Changes & Land Surface P, Beijing, Peoples R China.
[Edwards, Ross] Curtin Univ, Dept Imaging & Appl Phys, Bentley, WA, Australia.
[Bisiaux, Marion; McConnell, Joe] Univ Nevada, Desert Res Inst, Reno, NV 89506 USA.
RP Bauer, SE (reprint author), Columbia Univ, Earth Inst, Ctr Climate Syst Res, Broadway 2880, New York, NY 10025 USA.
EM Susanne.Bauer@Columbia.edu
RI Bauer, Susanne/P-3082-2014; Edwards, Ross/B-1433-2013
OI Edwards, Ross/0000-0002-9233-8775
FU NASA MAP program Modeling, Analysis and Prediction Climate Variability
and Change [NN-H-04-Z-YS-008-N, NN-H-08-Z-DA-001-N]; NSF; NOAA; NASA
FX This work has been supported by the NASA MAP program Modeling, Analysis
and Prediction Climate Variability and Change (NN-H-04-Z-YS-008-N and
NN-H-08-Z-DA-001-N). Resources supporting this work were provided by the
NASA High-End Computing (HEC) Program through the NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center. We acknowledge
the IMPROVE monitoring program. We acknowledge the use of HIPPO data
products (http://www.eol.ucar.edu/projects/hippo/). The HIPPO mission
was funded by NSF, NOAA, and NASA.
NR 37
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U1 2
U2 52
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUL 27
PY 2013
VL 118
IS 14
BP 7948
EP 7961
DI 10.1002/jgrd.50612
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 201DL
UT WOS:000323120800042
ER
PT J
AU Remsberg, E
Natarajan, M
Fairlie, TD
Wargan, K
Pawson, S
Coy, L
Lingenfelser, G
Kim, G
AF Remsberg, E.
Natarajan, M.
Fairlie, T. D.
Wargan, K.
Pawson, S.
Coy, L.
Lingenfelser, G.
Kim, G.
TI On the inclusion of Limb Infrared Monitor of the Stratosphere version 6
ozone in a data assimilation system
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE data assimilation; stratosphere; ozone
ID VARIATIONAL STATISTICAL-ANALYSIS; MICHELSON INTERFEROMETER; RECURSIVE
FILTERS; NUMERICAL ASPECTS; KALMAN FILTER; PART II; PROFILES;
COVARIANCES; MODEL; CONSTITUENTS
AB Version 6 ozone profiles for 1978-1979 from the Limb Infrared Monitor of the Stratosphere experiment on the NIMBUS 7 satellite (or LIMS v6) are assimilated into an updated version of the GEOS-5 model of NASA. First, an assimilation study is carried out using GEOS-5 version 7.2 (v7.2) and solar backscatter ultraviolet (SBUV) version 8.6 ozone profiles. Then, a second study is conducted that ingests both the LIMS and SBUV ozone, as weighted by their estimated absolute error vectors. Ozone from this second study compares well with independent observations from the Stratospheric Aerosol and Gas Experiment (SAGE I) and from the time series of ozonesonde data at Hohenpeissenberg and at Wallops Island. Assimilation of the LIMS data gives improved ozone distributions in the upper stratosphere (pressure<5 hPa) and in the polar night regionthe latter where solar backscatter ultraviolet (SBUV) is not observed. The LIMS ozone leads to improved total column ozone analyses in winter/spring outside of the tropics, based on independent comparisons with total ozone from the Total Ozone Mapping Spectrometer. The LIMS ozone also adds information in the tropics on coherent structural features at 20-30 hPa, related to the phase transition of the quasi-biennial oscillation wind field. It is affirmed that the process of data assimilation represents a cost-effective way of characterizing new and/or reprocessed satellite ozone data sets. It is concluded that the GEOS-5 v7.2 model with the addition of the LIMS data can improve analyses of ozone in 1978-1979.
C1 [Remsberg, E.; Natarajan, M.; Fairlie, T. D.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
[Wargan, K.; Pawson, S.; Coy, L.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Wargan, K.; Coy, L.; Lingenfelser, G.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Kim, G.] Ulsan Natl Inst Sci & Technol, Climate Environm Modeling Lab, Ulsan, South Korea.
RP Remsberg, E (reprint author), NASA, Sci Directorate, Langley Res Ctr, Mail Stop 401B, Hampton, VA 23681 USA.
EM Ellis.E.Remsberg@nasa.gov
RI Pawson, Steven/I-1865-2014;
OI Pawson, Steven/0000-0003-0200-717X; Wargan,
Krzysztof/0000-0002-3795-2983
FU Modeling, Analysis, and Prediction (MAP) within NASA's Science Mission
Directorate; Atmospheric Composition: Modeling and Analysis (ACMAP)
within NASA's Science Mission Directorate; NASA Langley by Malcolm Ko of
the Science Directorate
FX The authors gratefully acknowledge support from the Modeling, Analysis,
and Prediction (MAP: D. S. Considine) and the Atmospheric Composition:
Modeling and Analysis (ACMAP: R. S. Eckman) programs within NASA's
Science Mission Directorate. The data assimilation experiments were
performed using NASA's High-End Computing (HEC) resource allocations at
the NASA Center for Climate Studies (NCCS). SAGE I data were obtained
from the Atmospheric Science Data Center (ASDC) at the NASA Langley
Research Center (see also
http://eosweb.larc.nasa.gov/GUIDE/campaign_documents/sage1_project.html/
). We thank Randy Moore and Nina Iyer for assistance with the SAGE I
ozone data. We appreciate discussions with B. T. Marshall, regarding the
details of the LIMS v6 ozone retrieval algorithm. We appreciate the
insight and constructive comments from the three reviewers of the
manuscript. Ellis Remsberg is sponsored as a Distinguished Research
Associate (DRA) at NASA Langley by Malcolm Ko of the Science
Directorate.
NR 41
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U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUL 27
PY 2013
VL 118
IS 14
BP 7982
EP 8000
DI 10.1002/jgrd.50566
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 201DL
UT WOS:000323120800044
ER
PT J
AU McPeters, RD
Bhartia, PK
Haffner, D
Labow, GJ
Flynn, L
AF McPeters, Richard D.
Bhartia, P. K.
Haffner, D.
Labow, Gordon J.
Flynn, Larry
TI The version 8.6 SBUV ozone data record: An overview
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE ozone climatology
ID TEMPERATURE; RETRIEVAL; GOME
AB Under a NASA program to produce long-term data records from instruments on multiple satellites, data from a series of nine Solar Backscatter Ultraviolet (SBUV and SBUV/2) instruments have been reprocessed to create a coherent ozone time series. Data from the BUV instrument on Nimbus 4, SBUV on Nimbus 7, and SBUV/2 instruments on NOAA 9, 11, 14, 16, 17, 18, and 19 covering the period 1970-1972 and 1979-2011 were used to create a long-term data set. The goal is an ozone Earth Science Data Recorda consistent, calibrated ozone time series that can be used for trend analyses and other studies. In order to create this ozone data set, the radiances were adjusted and used to reprocess the entire data records for each of the nine instruments. Interinstrument comparisons during periods of overlap as well as comparisons with data from other satellite and ground-based instruments were used to evaluate the consistency of the record and make calibration adjustments as needed. Additional improvements in this version 8.6 processing included the use of the Brion, Daumont, and Malicet ozone cross sections, and a cloud-height climatology derived from Aura OMI measurements. Validation of the reprocessed ozone shows that total column ozone is consistent with the Brewer/Dobson network to within about 1% for the new time series. Comparisons with MLS, SAGE, sondes, and lidar show that ozone at individual levels in the stratosphere is generally consistent to within 5%.
C1 [McPeters, Richard D.; Bhartia, P. K.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Haffner, D.; Labow, Gordon J.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Flynn, Larry] NOAA NESDIS, College Pk, MD USA.
RP McPeters, RD (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 614, Greenbelt, MD 20771 USA.
EM Richard.D.McPeters@nasa.gov
RI Flynn, Lawrence/B-6321-2009; McPeters, Richard/G-4955-2013; Bhartia,
Pawan/A-4209-2016
OI Flynn, Lawrence/0000-0001-6856-2614; McPeters,
Richard/0000-0002-8926-8462; Bhartia, Pawan/0000-0001-8307-9137
NR 23
TC 36
Z9 40
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 JUL 27
PY 2013
VL 118
IS 14
BP 8032
EP 8039
DI 10.1002/jgrd.50597
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 201DL
UT WOS:000323120800048
ER
PT J
AU Pechony, O
Shindell, DT
Faluvegi, G
AF Pechony, Olga
Shindell, Drew T.
Faluvegi, Greg
TI Direct top-down estimates of biomass burning CO emissions using TES and
MOPITT versus bottom-up GFED inventory
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Carbon monoxide; Biomass burning emissions; MOPITT; TES; GFED; Climate
model
ID NADIR RETRIEVALS; CARBON-MONOXIDE; BURNED AREA; SATELLITE; SPECTROMETER;
VARIABILITY; POLLUTION; OZONE; SIMULATIONS; CHEMISTRY
AB In this study, we utilize near-simultaneous observations from two sets of multiple satellite sensors to segregate Tropospheric Emission Spectrometer (TES) and Measurements of Pollution in the Troposphere (MOPITT) CO observations over active fire sources from those made over clear background. Hence, we obtain direct estimates of biomass burning CO emissions without invoking inverse modeling as in traditional top-down methods. We find considerable differences between Global Fire Emissions Database (GFED) versions 2.1 and 3.1 and satellite-based emission estimates in many regions. Both inventories appear to greatly underestimate South and Southeast Asia emissions, for example. On global scales, however, CO emissions in both inventories and in the MOPITT-based analysis agree reasonably well, with the largest bias (30%) found in the Northern Hemisphere spring. In the Southern Hemisphere, there is a one-month shift between the GFED and MOPITT-based fire emissions peak. Afternoon tropical fire emissions retrieved from TES are about two times higher than the morning MOPITT retrievals. This appears to be both a real difference due to the diurnal fire activity variations, and a bias due to the scarcity of TES data.
C1 [Pechony, Olga; Shindell, Drew T.; Faluvegi, Greg] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Pechony, Olga; Shindell, Drew T.; Faluvegi, Greg] Columbia Earth Inst, New York, NY USA.
RP Pechony, O (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM pechony@gmail.com
RI Shindell, Drew/D-4636-2012
NR 45
TC 11
Z9 11
U1 0
U2 16
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 JUL 27
PY 2013
VL 118
IS 14
BP 8054
EP 8066
DI 10.1002/jgrd.50624
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 201DL
UT WOS:000323120800050
ER
PT J
AU Palumbo, D
AF Palumbo, Dan
TI The variance of convection velocity in the turbulent boundary layer and
its effect on coherence length
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
ID WALL-PRESSURE-FLUCTUATIONS; NUMBERS; FIELD
AB The Efimtsov model of coherence length and the Corcos cross spectrum model are commonly used to define the power spectra of the turbulent boundary layer near the wall. The models are useful for defining the pressure fields acting on structures such as aircraft fuselage and ship hulls as they move through fluid. In an effort to establish the validity of the models, the spectral definitions were used to synthesize time series data whose properties could then be compared to the actual data from which the model parameters were derived. Analysis of the synthesized time data indicated that the data contained coherence lengths longer than those specified in the models. The longer coherence lengths are shown to be related to the assumption of constant convection velocity that is fundamental to the Corcos model. A time domain technique is introduced by which the instantaneous convection velocity can be measured. Using this technique, statistics on the convection velocity for wall pressure data acquired during flight tests are shown to be normally distributed. Time data produced using a normally distributed convection velocity contains the specified coherence length, confirming that the assumption of constant convection velocity in the Corcos model was the source of the error. The coherence decay caused by convection velocity variance is shown to be Gaussian. A model is derived which divides the coherence decay into an exponential structural decay term and a Gaussian phase decay term. This is shown to be a good model for the coherence decay, except for frequencies around the peak in the power spectrum. The structural decay term is further divided into exponential and rectangular terms to represent inner layer and outer layer processes, respectively. The partitioned model is shown to correctly describe the coherence decay for the entire frequency band and provides a measure of the allocation of power between the inner and outer layer processes. It is concluded that the variance in the convection velocity has a significant effect on the decay of coherent power in the wall pressure of the turbulent boundary layer. Published by Elsevier Ltd.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Palumbo, D (reprint author), NASA, Langley Res Ctr, MS 463, Hampton, VA 23681 USA.
EM d.l.palumbo@nasa.gov
NR 9
TC 3
Z9 3
U1 0
U2 5
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 JUL 22
PY 2013
VL 332
IS 15
BP 3692
EP 3705
DI 10.1016/j.jsv.2013.02.010
PG 14
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA 148HS
UT WOS:000319236000007
ER
PT J
AU Ma, Q
Boulet, C
Tipping, RH
AF Ma, Q.
Boulet, C.
Tipping, R. H.
TI Refinement of the Robert-Bonamy formalism: Considering effects from the
line coupling
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID SEMICLASSICAL CALCULATIONS; BROADENING CALCULATIONS; SPECTRA;
RELAXATION; SHAPES; LINEWIDTHS; MICROWAVE; MIXTURES; QUANTUM; WIDTHS
AB Since it was developed in 1979, the Robert-Bonamy (RB) formalism has been widely used in calculating pressure broadened half-widths and induced shifts for many molecular systems. However, this formalism contains several approximations whose applicability has not been thoroughly justified. One of them is that lines of interest are well isolated. When these authors developed the formalism, they have relied on this assumption twice. First, in calculating the spectral density F(omega), they have only considered the diagonal matrix elements of the relaxation operator. Due to this simplification, effects from the line mixing are ignored. Second, when they applied the linked cluster theorem to remove the cutoff, they have assumed the matrix elements of the operator exp(-iS(1) - S-2) can be replaced by the exponential of the matrix elements of -iS(1) - S-2. With this replacement, effects from the line coupling are also ignored. Although both these two simplifications relied on the same approximation, their validity criteria are completely different and the latter is more stringent than the former. As a result, in many cases where the line mixing becomes negligible, significant effects from the line coupling have been completely missed. In the present study, we have developed a new method to evaluate the matrix elements of exp(-iS(1) - S-2) and have refined the RB formalism such that line coupling can be taken into account. Our numerical calculations of the half-widths for Raman Q lines of the N-2-N-2 pair have demonstrated that effects from the line coupling are important. In comparison with values derived from the RB formalism, new calculated values for these lines are significantly reduced. A recent study has shown that in comparison with the measurements and the most accurate close coupling calculations, the RB formalism overestimates the half-widths by a large amount. As a result, the refinement of the RB formalism goes in the right direction and these new calculated half-widths become closer to the "true" values. (C) 2013 AIP Publishing LLC.
C1 [Ma, Q.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Ma, Q.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Boulet, C.] CNRS, UMR8214, ISMO, F-91405 Orsay, France.
[Boulet, C.] Univ Paris 11, F-91405 Orsay, France.
[Tipping, R. H.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
RP Ma, Q (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
FU National Science Foundation (NSF) [1228861]; Office of Science of the
U.S. Department of Energy [DE-AC02-05CH11231]
FX We thank the two reviewers for their helpful comments on the manuscript.
Two of the authors (Q. Ma and R. H. Tipping) acknowledge financial
support from National Science Foundation (NSF) under Grant No. 1228861.
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.
NR 29
TC 7
Z9 7
U1 1
U2 12
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-9606
J9 J CHEM PHYS
JI J. Chem. Phys.
PD JUL 21
PY 2013
VL 139
IS 3
AR 034305
DI 10.1063/1.4813234
PG 16
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 188OT
UT WOS:000322203000024
PM 23883025
ER
PT J
AU Antiochos, SK
AF Antiochos, S. K.
TI HELICITY CONDENSATION AS THE ORIGIN OF CORONAL AND SOLAR WIND STRUCTURE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; Sun: corona
ID MAGNETIC-FIELD; FLUX EMERGENCE; PHOTOSPHERIC NETWORK; ACTIVE REGIONS;
POLAR CROWN; RECONNECTION; PROMINENCES; DYNAMICS; ATMOSPHERE; FILAMENTS
AB Three of the most important and most puzzling features of the Sun's atmosphere are the smoothness of the closed-field corona (the so-called coronal loops), the accumulation of magnetic shear at photospheric polarity inversion lines (PILs; filament channels), and the complex dynamics of the slow wind. We propose that a single process, helicity condensation, is the physical mechanism giving rise to all three features. A simplified model is presented for how helicity is injected and transported in the closed corona by magnetic reconnection. With this model, we demonstrate that magnetic shear must accumulate at PILs and coronal hole boundaries, and estimate the rate of shear growth at PILs and the loss to the wind. Our results can account for many of the observed properties of the corona and wind.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Antiochos, SK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM spiro.antiochos@nasa.gov
RI Antiochos, Spiro/D-4668-2012
OI Antiochos, Spiro/0000-0003-0176-4312
FU NASA
FX This work has been supported, in part, by the NASA TR&T and SR&T
Programs. The work has benefited greatly from the authors' participation
in the NASA TR&T focused science teams on multiscale coupling and the
slow solar wind. The author thanks C. R. DeVore, J. T. Karpen, and J. A.
Klimchuk for invaluable scientific discussions and J. T. Karpen for help
with the graphics.
NR 74
TC 11
Z9 11
U1 1
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2013
VL 772
IS 1
AR 72
DI 10.1088/0004-637X/772/1/72
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700072
ER
PT J
AU Assef, RJ
Stern, D
Kochanek, CS
Blain, AW
Brodwin, M
Brown, MJI
Donoso, E
Eisenhardt, PRM
Jannuzi, BT
Jarrett, TH
Stanford, SA
Tsai, CW
Wu, J
Yan, L
AF Assef, R. J.
Stern, D.
Kochanek, C. S.
Blain, A. W.
Brodwin, M.
Brown, M. J. I.
Donoso, E.
Eisenhardt, P. R. M.
Jannuzi, B. T.
Jarrett, T. H.
Stanford, S. A.
Tsai, C. -W.
Wu, J.
Yan, L.
TI MID-INFRARED SELECTION OF ACTIVE GALACTIC NUCLEI WITH THE WIDE-FIELD
INFRARED SURVEY EXPLORER. II. PROPERTIES OF WISE-SELECTED ACTIVE
GALACTIC NUCLEI IN THE NDWFS BOOTES FIELD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; methods: statistical; quasars: general
ID QUASAR LUMINOSITY FUNCTION; SPITZER-SPACE-TELESCOPE; IRAC SHALLOW
SURVEY; SUPERMASSIVE BLACK-HOLES; ARRAY CAMERA IRAC; X-RAY SURVEY;
SIMILAR-TO 4; UNIFIED SCHEMES; SKY SURVEY; PHOTOMETRIC REDSHIFTS
AB Stern et al. presented a study of Wide-field Infrared Survey Explorer (WISE) selection of active galactic nuclei (AGNs) in the 2 deg(2) COSMOS field, finding that a simple criterion W1-W2 >= 0.8 provides a highly reliable and complete AGN sample for W2 < 15.05, where the W1 and W2 passbands are centered at 3.4 mu m and 4.6 mu m, respectively. Here we extend this study using the larger 9 deg(2) NOAO Deep Wide-Field Survey Bootes field which also has considerably deeper WISE observations than the COSMOS field, and find that this simple color cut significantly loses reliability at fainter fluxes. We define a modified selection criterion combining the W1-W2 color and the W2 magnitude to provide highly reliable or highly complete AGN samples for fainter WISE sources. In particular, we define a color-magnitude cut that finds 130 +/- 4 deg(-2) AGN candidates for W2 < 17.11 with 90% reliability. Using the extensive UV through mid-IR broadband photometry available in this field, we study the spectral energy distributions of WISE AGN candidates. We find that, as expected, the WISE AGN selection can identify highly obscured AGNs, but that it is biased toward objects where the AGN dominates the bolometric luminosity output. We study the distribution of reddening in the AGN sample and discuss a formalism to account for sample incompleteness based on the step-wise maximum-likelihood method of Efstathiou et al. The resulting dust obscuration distributions depend strongly on AGN luminosity, consistent with the trend expected for a receding torus. At L-AGN similar to 3 x 10(44) erg s(-1), 29% +/- 7% of AGNs are observed as Type 1, while at similar to 4 x 10(45) erg s(-1) the fraction is 64% +/- 13%. The distribution of obscuration values suggests that dust in the torus is present as both a diffuse medium and in optically thick clouds.
C1 [Assef, R. J.; Stern, D.; Jannuzi, B. T.; Tsai, C. -W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Blain, A. W.] Univ Leicester, Leicester LE1 7RH, Leics, England.
[Brown, M. J. I.] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA.
[Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Donoso, E.; Jarrett, T. H.; Yan, L.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Donoso, E.] ICATE, RA-5400 San Juan, Argentina.
[Jannuzi, B. T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Jarrett, T. H.] Univ Cape Town, Dept Astron, ZA-7700 Rondebosch, South Africa.
[Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Wu, J.] UCLA Astron, Los Angeles, CA 90095 USA.
EM roberto.j.assef@jpl.nasa.gov
RI Brown, Michael/B-1181-2015
OI Brown, Michael/0000-0002-1207-9137
FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; NASA; W.M.
Keck Foundation
FX We thank M. Dickinson, A. H. Gonzalez, J. Kartaltepe, B. Mobasher, H.
Nayyeri, K. Penner, and G. Zeimann for helping us obtain some of the
Keck spectroscopic observations used in this work. We thank M. Elitzur
for an insightful discussion about dust properties in AGNs. We thank the
NDWFS, NEWFIRM, and MAGES survey teams for providing their respective
data sets over the Bootes field. We thank the anonymous referee for
suggestions that helped improve our work. R. J. A. and C.-W.T. are
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. 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. 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.
NR 85
TC 106
Z9 106
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 JUL 20
PY 2013
VL 772
IS 1
AR 26
DI 10.1088/0004-637X/772/1/26
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700026
ER
PT J
AU Dahle, H
Sarazin, CL
Lopez, LA
Kouveliotou, C
Patel, SK
Rol, E
van der Horst, AJ
Fynbo, J
Wijers, RAMJ
Burrows, DN
Gehrels, N
Grupe, D
Ramirez-Ruiz, E
Michalowski, MJ
AF Dahle, H.
Sarazin, C. L.
Lopez, L. A.
Kouveliotou, C.
Patel, S. K.
Rol, E.
van der Horst, A. J.
Fynbo, J.
Wijers, R. A. M. J.
Burrows, D. N.
Gehrels, N.
Grupe, D.
Ramirez-Ruiz, E.
Michalowski, M. J.
TI THE BURST CLUSTER: DARK MATTER IN A CLUSTER MERGER ASSOCIATED WITH THE
SHORT GAMMA-RAY BURST, GRB 050509B
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (ZwCl 1234.0+02916, NSC J123610+285901);
gamma-ray burst: individual (GRB 050509B)
ID LENSING MASS RECONSTRUCTION; INTERACTION CROSS-SECTION;
HUBBLE-SPACE-TELESCOPE; GALAXY CLUSTER; GLOBULAR-CLUSTERS; MERGING
CLUSTER; STELLAR MASS; HOST GALAXY; SUBMILLIMETER GALAXIES; TEMPERATURE
RELATION
AB We have identified a merging galaxy cluster with evidence of two distinct subclusters. The X-ray and optical data suggest that the subclusters are presently moving away from each other after closest approach. This cluster merger was discovered from observations of the first well-localized short-duration gamma-ray burst (GRB), GRB 050509B. The Swift/Burst Alert Telescope error position of the source is coincident with a cluster of galaxies ZwCl 1234.0+02916, while the subsequent Swift/X-Ray Telescope localization of the X-ray afterglow found the GRB coincident with 2MASX J12361286+2858580, a giant red elliptical galaxy in the cluster. Deep multi-epoch optical images were obtained in this field to constrain the evolution of the GRB afterglow, including a total of 27,480 s exposure in the F814W band with Hubble Space Telescope Advanced Camera for Surveys, among the deepest imaging ever obtained toward a known galaxy cluster in a single passband. We perform a weak gravitational lensing analysis based on these data, including mapping of the total mass distribution of the merger system with high spatial resolution. When combined with Chandra X-ray Observatory Advanced CCD Imaging Spectrometer and Swift/XRT observations, we are able to investigate the dynamical state of the merger to better understand the nature of the dark matter component. Our weak gravitational lensing measurements reveal a separation of the X-ray centroid of the western subcluster from the center of the mass and galaxy light distributions, which is somewhat similar to that of the famous "Bullet cluster," and we conclude that this "Burst cluster" adds another candidate to the previously known merger systems for determining the nature of dark matter, as well as for studying the environment of a short GRB. Finally, we discuss potential connections between the cluster dynamical state and/or matter composition, and compact object mergers, which is currently the leading model for the origin of short GRBs. We also present our results from a weak-lensing survey based on archival Very Large Telescope images in the areas of five other short GRBs, which do not provide any firm detections of mass concentrations representative of rich clusters.
C1 [Dahle, H.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway.
[Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Lopez, L. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Kouveliotou, C.] NASA, Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Patel, S. K.] Opt Sci Corp, Huntsville, AL 35806 USA.
[Rol, E.; van der Horst, A. J.; Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
[Fynbo, J.; Michalowski, M. J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Burrows, D. N.; Grupe, D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ramirez-Ruiz, E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95060 USA.
[Michalowski, M. J.] Univ Edinburgh, Royal Observ, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland.
RP Dahle, H (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway.
EM hdahle@astro.uio.no
RI Fynbo, Johan/L-8496-2014;
OI Fynbo, Johan/0000-0002-8149-8298; Wijers, Ralph/0000-0002-3101-1808
FU Research Council of Norway; National Aeronautics and Space
Administration through Chandra awards [GO7-8129X, GO8-9085X, GO9-0135X,
GO9-0148X, GO1-12169X]; National Aeronautics and Space Administration
through HST awards [HST-GO-10582.02-A, HST-GO-10835.01-A,
HST-GO-11679.01, HST-GO-12012.02-A, HST-GO-12202.0-A]; NASA through the
Einstein Fellowship Program [PF1-120085]; Pappalardo Fellowship in
Physics at MIT; Danish National Research Foundation; Netherlands
foundation for Scientific Research; [075.D-0261]; [075.D-0415];
[075.D-0468]; [075.D-0787]; [076.D-0612]
FX We thank A. von der Linden for her detailed and critical remarks on the
paper. H. D. acknowledges support from the Research Council of Norway,
including a postdoctoral research fellowship. C. L. S. was supported by
the National Aeronautics and Space Administration through Chandra awards
GO7-8129X, GO8-9085X, GO9-0135X, GO9-0148X, and GO1-12169X, and through
HST awards HST-GO-10582.02-A, HST-GO-10835.01-A, HST-GO-11679.01,
HST-GO-12012.02-A, and HST-GO-12202.0-A. Support for L. A. L. was
provided by NASA through the Einstein Fellowship Program, grant
PF1-120085; L. A. L. also acknowledges support by the Pappalardo
Fellowship in Physics at MIT. C. K. thanks the Dark Cosmology Center,
who provided the nourishing environment for the final stages of this
paper. A.J.vdH. was supported by an appointment to the NASA Postdoctoral
Program at the MSFC, administered by Oak Ridge Associated Universities
through a contract with NASA. The Dark Cosmology Center is funded by the
Danish National Research Foundation. The WSRT is operated by ASTRON
(Netherlands Institute for Radio Astronomy) with support from the
Netherlands foundation for Scientific Research. Some of the results were
based on observations made with ESO Telescopes at the La Silla or
Paranal Observatories under program IDs 075.D-0261, 075.D-0415,
075.D-0468, 075.D-0787, 076.D-0612.
NR 95
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
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2013
VL 772
IS 1
AR 23
DI 10.1088/0004-637X/772/1/23
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700023
ER
PT J
AU Donaldson, JK
Lebreton, J
Roberge, A
Augereau, JC
Krivov, AV
AF Donaldson, J. K.
Lebreton, J.
Roberge, A.
Augereau, J. -C.
Krivov, A. V.
TI MODELING THE HD 32297 DEBRIS DISK WITH FAR-INFRARED HERSCHEL DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars
ID BETA-PICTORIS DISK; AU MICROSCOPII; CIRCUMSTELLAR DISK; SURROUNDING
HD-32297; INTERSTELLAR DUST; PLANET FORMATION; YOUNG STARS; GAS;
EVOLUTION; SYSTEM
AB HD 32297 is a young A-star (similar to 30 Myr) 112 pc away with a bright edge-on debris disk that has been resolved in scattered light. We observed the HD 32297 debris disk in the far-infrared and sub-millimeter with the Herschel Space Observatory PACS and SPIRE instruments, populating the spectral energy distribution (SED) from 63 to 500 mu m. We aimed to determine the composition of dust grains in the HD 32297 disk through SED modeling, using geometrical constraints from the resolved imaging to break the degeneracies inherent in SED modeling. We found the best fitting SED model has two components: an outer ring centered around 110 AU, seen in the scattered light images, and an inner disk near the habitable zone of the star. The outer disk appears to be composed of grains >2 mu m consisting of silicates, carbonaceous material, and water ice with an abundance ratio of 1: 2: 3 respectively and 90% porosity. These grains appear consistent with cometary grains, implying the underlying planetesimal population is dominated by comet-like bodies. We also discuss the 3.7 sigma detection of [C II] emission at 158 mu m with the Herschel PACS instrument, making HD 32297 one of only a handful of debris disks with circumstellar gas detected.
C1 [Donaldson, J. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Lebreton, J.; Augereau, J. -C.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France.
[Roberge, A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Krivov, A. V.] Univ Jena, Inst Astrophys, D-07745 Jena, Germany.
RP Donaldson, JK (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM jessd@astro.umd.edu
RI Roberge, Aki/D-2782-2012
OI Roberge, Aki/0000-0002-2989-3725
FU NASA through JPL/Caltech; PNP-CNES
FX This work is based on observations made with Herschel, a European Space
Agency Cornerstone Mission with significant participation by NASA.
Support for this work was provided by NASA through an award issued by
JPL/Caltech. J.L. and J.C.A. thank the PNP-CNES for financial support.
We also wish to thank the anonymous referee for a very thorough review
that helped improve this paper.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2013
VL 772
IS 1
AR 17
DI 10.1088/0004-637X/772/1/17
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700017
ER
PT J
AU Fortenberry, RC
Huang, XC
Crawford, TD
Lee, TJ
AF Fortenberry, Ryan C.
Huang, Xinchuan
Crawford, T. Daniel
Lee, Timothy J.
TI HIGH-ACCURACY QUARTIC FORCE FIELD CALCULATIONS FOR THE SPECTROSCOPIC
CONSTANTS AND VIBRATIONAL FREQUENCIES OF 1(1)A ' l-C3H-: A POSSIBLE LINK
TO LINES OBSERVED IN THE HORSEHEAD NEBULA PHOTODISSOCIATION REGION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: individual objects (Horsehead nebula); ISM: lines
and bands; ISM: molecules; molecular data; radio lines: ISM
ID CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; ASTRONOMICAL
DETECTION; ELECTRON-ATTACHMENT; INTERSTELLAR CLOUDS; EXCITED-STATES;
ANIONS; C4H; ATOMS; ENERGY
AB It has been shown that rotational lines observed in the Horsehead nebula photodissociation region (PDR) are probably not caused by l-C3H+, as was originally suggested. In the search for viable alternative candidate carriers, quartic force fields are employed here to provide highly accurate rotational constants, as well as fundamental vibrational frequencies, for another candidate carrier: 1(1)A'C3H-. The ab initio computed spectroscopic constants provided in this work are, compared to those necessary to define the observed lines, as accurate as the computed spectroscopic constants for many of the known interstellar anions. Additionally, the computed D-eff for C3H is three times closer to the D deduced from the observed Horsehead nebula lines relative to l-C3H+. As a result, 1(1)A'C3H- is a more viable candidate for these observed rotational transitions. It has been previously proposed that at least C6H- may be present in the Horsehead nebular PDR formed by way of radiative attachment through its dipole-bound excited state. C3H- could form in a similar way through its dipole-bound state, but its valence excited state increases the number of relaxation pathways possible to reach the ground electronic state. In turn, the rate of formation for C3H- could be greater than the rate of its destruction. C3H- would be the seventh confirmed interstellar anion detected within the past decade and the first CnH- molecular anion with an odd n.
C1 [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
[Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA.
RP Fortenberry, RC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; Crawford,
Thomas/A-9271-2017
OI Crawford, Thomas/0000-0002-7961-7016
FU NASA; NASA/SETI Institute [NNX12AG96A]; NASA's Laboratory Astrophysics
"Carbon in the Galaxy" Consortium Grant [NNH10ZDA001N]; U.S. National
Science Foundation (NSF) Multi-User Chemistry Research Instrumentation
and Facility (CRIF:MU) award [CHE-0741927]; [NSF-1058420]
FX R.C.F. is currently supported on a NASA Postdoctoral Program Fellowship
administered by Oak Ridge Associated Universities. NASA/SETI Institute
Cooperative Agreement NNX12AG96A has funded the work undertaken by X. H.
Support from NASA's Laboratory Astrophysics "Carbon in the Galaxy"
Consortium Grant (NNH10ZDA001N) is gratefully acknowledged. The U.S.
National Science Foundation (NSF) Multi-User Chemistry Research
Instrumentation and Facility (CRIF:MU) award CHE-0741927 provided the
computational hardware, and award NSF-1058420 has supported T. D. C. The
CheMVP program was used to create Figure 1. The authors also acknowledge
many others for their contributions to our astronomical understanding of
this subject. These include, most notably: Dr. Michael C. McCarthy of
the Harvard-Smithsonian Center for Astrophysics, Dr. Naseem Rangwala of
the University of Colorado, Dr. Lou Allamandola of the NASA Ames
Research Center, and Dr. Christiaan Boersma of the NASA Ames Research
Center and San Jose State University.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2013
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DI 10.1088/0004-637X/772/1/39
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SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700039
ER
PT J
AU Jang-Condell, H
Turner, NJ
AF Jang-Condell, Hannah
Turner, Neal J.
TI GAPS IN PROTOPLANETARY DISKS AS SIGNATURES OF PLANETS. II. INCLINED
DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planet-disk interactions; planets and satellites: detection;
protoplanetary disks; radiative transfer; stars: individual (LkCa 15)
ID TRANSITIONAL DISK; CIRCUMSTELLAR DISKS; LKCA 15; RADIATIVE-TRANSFER;
MASS PLANETS; STARS; EVOLUTION; PERTURBATIONS; ACCRETION; MWC-480
AB We examine the observational appearance of partial gaps being opened by planets in protoplanetary disks, considering the effects of the inclination relative to the line of sight. We model the disks with static alpha-models with detailed radiative transfer, parameterizing the shape and size of the partially cleared gaps based on the results of hydrodynamic simulations. As in previous work, starlight falling across the gap leads to high surface brightness contrasts. The gap's trough is darkened by both shadowing and cooling, relative to the uninterrupted disk. The gap's outer wall is brightened by direct illumination and also by heating, which puffs it up so that it intercepts more starlight. In this paper, we examine the effects of inclination on resolved images of disks with and without gaps at a wide range of wavelengths. The scattering surface's offset from the disk midplane creates a brightness asymmetry along the axis of inclination, making the disk's near side appear brighter than the far side in scattered light. Finite disk thickness also causes the projected distances of equidistant points on the disk surface to be smaller on the near side of the disk as compared to the far side. Consequently, the gap shoulder on the near side of the disk should appear brighter and closer to the star than on the far side. However, if the angular resolution of the observation is coarser than the width of the brightened gap shoulder, then the gap shoulder on the far side may appear brighter because of its larger apparent size. We present a formula to recover the scale height and inclination angle of an imaged disk using simple geometric arguments and measuring disk asymmetries. Resolved images of circumstellar disks have revealed clearings and gaps, such as the transitional disk in LkCa 15. Models created using our synthetic imaging attempting to match the morphology of observed scattered light images of LkCa 15 indicate that the H-band flux deficit in the inner similar to 0.'' 5 of the disk can be explained with a planet if mass is greater than 0.5 Jupiter mass.
C1 [Jang-Condell, Hannah] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Turner, Neal J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Jang-Condell, H (reprint author), Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
OI Jang-Condell, Hannah/0000-0002-7639-1322; Turner,
Neal/0000-0001-8292-1943
FU NASA Astrophysics Theory Program [NNX12AD43G]; Michelson Fellowship
Program under Jet Propulsion Laboratory (JPL); NASA; NASA Origins of
Solar Systems program [09-SSO09-0046]; Humboldt Foundation
FX The authors thank C. A. Grady and A. Hubbard for helpful discussions in
the preparation of this paper. We also thank an anonymous referee for
constructive comments that greatly improved this paper. H.J.-C.
acknowledges support from the NASA Astrophysics Theory Program through
grant NNX12AD43G and the Michelson Fellowship Program under contract
with the Jet Propulsion Laboratory (JPL) funded by NASA. N.J.T. was
employed by JPL, which is managed for NASA by the California Institute
of Technology. He was supported by the NASA Origins of Solar Systems
program through grant 09-SSO09-0046, and by the Humboldt Foundation
through a Fellowship for Experienced Researchers.
NR 46
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
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SC Astronomy & Astrophysics
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UT WOS:000321673700034
ER
PT J
AU Krivov, AV
Eiroa, C
Lohne, T
Marshall, JP
Montesinos, B
del Burgo, C
Absil, O
Ardila, D
Augereau, JC
Bayo, A
Bryden, G
Danchi, W
Ertel, S
Lebreton, J
Liseau, R
Mora, A
Mustill, AJ
Mutschke, H
Neuhauser, R
Pilbratt, GL
Roberge, A
Schmidt, TOB
Stapelfeldt, KR
Thebault, P
Vitense, C
White, GJ
Wolf, S
AF Krivov, A. V.
Eiroa, C.
Loehne, T.
Marshall, J. P.
Montesinos, B.
del Burgo, C.
Absil, O.
Ardila, D.
Augereau, J. -C.
Bayo, A.
Bryden, G.
Danchi, W.
Ertel, S.
Lebreton, J.
Liseau, R.
Mora, A.
Mustill, A. J.
Mutschke, H.
Neuhaeuser, R.
Pilbratt, G. L.
Roberge, A.
Schmidt, T. O. B.
Stapelfeldt, K. R.
Thebault, Ph.
Vitense, Ch.
White, G. J.
Wolf, S.
TI HERSCHEL's "COLD DEBRIS DISKS": BACKGROUND GALAXIES OR QUIESCENT RIMS OF
PLANETARY SYSTEMS?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; galaxies: statistics; planets and satellites:
formation; protoplanetary disks; stars: individual (HIP 29271, HIP
49908, HIP 109378, HIP 92043, HIP 171, HIP 73100)
ID INTERSTELLAR DUST GRAINS; KUIPER-BELT OBJECTS; MAIN-SEQUENCE STARS;
PROTOPLANETARY DISKS; SIZE DISTRIBUTION; NEARBY STARS; COLLISIONAL
EVOLUTION; GROWTH PEBBLES; ALL-SKY; CATASTROPHIC DISRUPTIONS
AB Infrared excesses associated with debris disk host stars detected so far peak at wavelengths around similar to 100 mu m or shorter. However, 6 out of 31 excess sources studied in the Herschel Open Time Key Programme, DUNES, have been seen to show significant-and in some cases extended-excess emission at 160 mu m, which is larger than the 100 mu m excess. This excess emission has been attributed to circumstellar dust and has been suggested to stem from debris disks colder than those known previously. Since the excess emission of the cold disk candidates is extremely weak, challenging even the unrivaled sensitivity of Herschel, it is prudent to carefully consider whether some or even all of them may represent unrelated galactic or extragalactic emission, or even instrumental noise. We re-address these issues using several distinct methods and conclude that it is highly unlikely that none of the candidates represents a true circumstellar disk. For true disks, both the dust temperatures inferred from the spectral energy distributions and the disk radii estimated from the images suggest that the dust is nearly as cold as a blackbody. This requires the grains to be larger than similar to 100 mu m, even if they are rich in ices or are composed of any other material with a low absorption in the visible. The dearth of small grains is puzzling, since collisional models of debris disks predict that grains of all sizes down to several times the radiation pressure blowout limit should be present. We explore several conceivable scenarios: transport-dominated disks, disks of low dynamical excitation, and disks of unstirred primordial macroscopic grains. Our qualitative analysis and collisional simulations rule out the first two of these scenarios, but show the feasibility of the third one. We show that such disks can indeed survive for gigayears, largely preserving the primordial size distribution. They should be composed of macroscopic solids larger than millimeters, but smaller than a few kilometers in size. If larger planetesimals were present, then they would stir the disk, triggering a collisional cascade and thus causing production of small debris, which is not seen. Thus, planetesimal formation, at least in the outer regions of the systems, has stopped before "cometary" or "asteroidal" sizes were reached.
C1 [Krivov, A. V.; Loehne, T.; Mutschke, H.; Neuhaeuser, R.; Schmidt, T. O. B.; Vitense, Ch.] Univ Jena, Inst Astrophys, D-07745 Jena, Germany.
[Krivov, A. V.; Loehne, T.; Mutschke, H.; Neuhaeuser, R.; Schmidt, T. O. B.; Vitense, Ch.] Univ Jena, Univ Sternwarte, D-07745 Jena, Germany.
[Eiroa, C.; Marshall, J. P.; Mustill, A. J.] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain.
[Montesinos, B.] CSIC INTA, Ctr Astrobiol CAB, Dept Astrofis, E-28691 Madrid, Spain.
[del Burgo, C.] INAOE, Puebla 72000, Mexico.
[Absil, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Ardila, D.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Augereau, J. -C.; Ertel, S.; Lebreton, J.] UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France.
[Bayo, A.] European So Observ, Santiago 19, Chile.
[Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Danchi, W.; Roberge, A.; Stapelfeldt, K. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Liseau, R.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
[Mora, A.] ESA ESAC Gaia SOC, E-28691 Madrid, Spain.
[Pilbratt, G. L.] ESTEC SRE SA, ESA Astrophys & Fundamental Phys Missions Div, NL-2201 AZ Noordwijk, Netherlands.
[Thebault, Ph.] Observ Paris, LESIA, F-92195 Meudon, France.
[White, G. J.] Open Univ, Dept Phys & Astrophys, Milton Keynes MK7 6AA, Bucks, England.
[White, G. J.] Rutherford Appleton Lab, Chilton OX11 0QX, England.
[Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany.
[Bayo, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Krivov, AV (reprint author), Univ Jena, Inst Astrophys, Schillergasschen 2-3, D-07745 Jena, Germany.
EM krivov@astro.uni-jena.de
RI Roberge, Aki/D-2782-2012; Montesinos, Benjamin/C-3493-2017;
OI Roberge, Aki/0000-0002-2989-3725; Montesinos,
Benjamin/0000-0002-7982-2095; Marshall, Jonathan/0000-0001-6208-1801;
Mustill, Alexander James/0000-0002-2086-3642
FU Deutsche Forschungsgemeinschaft [Kr 2164/10-1, Lo 1715/1-1, Wo 857/7-1];
Spanish grant [AYA 2011-26202]; CNES-PNP; French National Research
Agency (ANR) [ANR-2010 BLAN-0505-01]; Marie Curie Actions of the
European Commission
FX We are grateful to the referee for useful comments that greatly helped
to improve the manuscript. A. V. K. and T. L. thank Jurgen Blum and
Carsten Guttler for their explanations on collisional outcomes and
Ludwig Trepl for discussions on the ROSAT data. The work of A. V. K., T.
L., and S. W. was partly funded by the Deutsche Forschungsgemeinschaft
(grants Kr 2164/10-1, Lo 1715/1-1, and Wo 857/7-1). C. E., J.P.M., and
B. M. were partly supported by Spanish grant AYA 2011-26202. J.-C.A. and
S. E. acknowledge financial support of the CNES-PNP. S. E. also thanks
the French National Research Agency (ANR) for financial support through
contract ANR-2010 BLAN-0505-01 (EXOZODI). A. B. was co-funded under the
Marie Curie Actions of the European Commission (FP7-COFUND).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2013
VL 772
IS 1
AR 32
DI 10.1088/0004-637X/772/1/32
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700032
ER
PT J
AU Kuiper, R
Yorke, HW
AF Kuiper, R.
Yorke, H. W.
TI ON THE SIMULTANEOUS EVOLUTION OF MASSIVE PROTOSTARS AND THEIR HOST CORES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; methods: numerical; stars: evolution; stars:
formation; stars: pre-main sequence
ID RADIATION-HYDRODYNAMIC SIMULATIONS; (PROTO)STAR IRAS 20126+4104; YOUNG
STELLAR OBJECTS; H II REGIONS; STAR-FORMATION; MOLECULAR OUTFLOWS; DISK
ACCRETION; ROTATING-DISK; IONIZED JETS; AFGL-490
AB Studies of the evolution of massive protostars and the evolution of their host molecular cloud cores are commonly treated as separate problems. However, interdependencies between the two can be significant. Here, we study the simultaneous evolution of massive protostars and their host molecular cores using a multi-dimensional radiation hydrodynamics code that incorporates the effects of the thermal pressure and radiative acceleration feedback of the centrally forming protostar. The evolution of the massive protostar is computed simultaneously using the stellar evolution code STELLAR, modified to include the effects of variable accretion. The interdependencies are studied in three different collapse scenarios. For comparison, stellar evolutionary tracks at constant accretion rates and the evolution of the host cores using pre-computed stellar evolutionary tracks are computed. The resulting interdependencies of the protostellar evolution and the evolution of the environment are extremely diverse and depend on the order of events, in particular the time of circumstellar accretion disk formation with respect to the onset of the bloating phase of the star. Feedback mechanisms affect the instantaneous accretion rate and the protostar's radius, temperature, and luminosity on timescales t <= 5 kyr, corresponding to the accretion timescale and Kelvin-Helmholtz contraction timescale, respectively. Nevertheless, it is possible to approximate the overall protostellar evolution in many cases by pre-computed stellar evolutionary tracks assuming appropriate constant average accretion rates.
C1 [Kuiper, R.; Yorke, H. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kuiper, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Rolf.Kuiper@jpl.nasa.gov; Harold.W.Yorke@jpl.nasa.gov
FU German Academy of Science Leopoldina within the Leopoldina Fellowship
program [LPDS 2011-5]; National Aeronautics and Space Administration
(NASA)
FX This research project was financially supported by the German Academy of
Science Leopoldina within the Leopoldina Fellowship program, grant No.
LPDS 2011-5. We thank our colleague Takashi Hosokawa for fruitful
discussions and support. R.K. thanks Arjan Bik, Hendrik Linz, and Henrik
Beuther for discussing the observational chances and most promising
techniques toward detecting massive protostars during their bloating
phase. This work was conducted at the Jet Propulsion Laboratory,
California Institute of Technology, operating under a contract with the
National Aeronautics and Space Administration (NASA).
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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UT WOS:000321673700061
ER
PT J
AU Pirzkal, N
Rothberg, B
Ly, C
Malhotra, S
Rhoads, JE
Grogin, NA
Dahlen, T
Noeske, KG
Meurer, GR
Walsh, JR
Hathi, NP
Cohen, SH
Bellini, A
Holwerda, BW
Straughn, AN
Mechtley, M
Windhorst, RA
AF Pirzkal, Nor
Rothberg, Barry
Ly, Chun
Malhotra, Sangeeta
Rhoads, James E.
Grogin, Norman A.
Dahlen, Tomas
Noeske, Kai G.
Meurer, Gerhardt R.
Walsh, Jeremy R.
Hathi, Nimish P.
Cohen, Seth H.
Bellini, Andrea
Holwerda, Benne W.
Straughn, Amber N.
Mechtley, Matthew
Windhorst, Rogier A.
TI EMISSION-LINE GALAXIES FROM THE HUBBLE SPACE TELESCOPE PROBING EVOLUTION
AND REIONIZATION SPECTROSCOPICALLY (PEARS) GRISM SURVEY. II. THE
COMPLETE SAMPLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; galaxies: evolution; galaxies: luminosity function, mass
function; line: identification
ID ULTRA DEEP FIELD; STAR-FORMING GALAXIES; LUMINOSITY FUNCTION; POPULATION
SYNTHESIS; TIME-SCALES; RESOLUTION; DISCREPANCY; EXTRACTION; MORPHOLOGY;
REDSHIFTS
AB We present a full analysis of the Probing Evolution And Reionization Spectroscopically (PEARS) slitess grism spectroscopic data obtained with the Advanced Camera for Surveys on board Hubble Space Telescope. PEARS covers fields within both the Great Observatories Origins Deep Survey (GOODS) North and South fields, making it ideal as a random survey of galaxies, as well as the availability of a wide variety of ancillary observations complemented by the spectroscopic results. Using the PEARS data, we are able to identify star-forming galaxies (SFGs) within the redshift volume 0 < z < 1.5. Star-forming regions in the PEARS survey are pinpointed independently of the host galaxy. This method allows us to detect the presence of multiple emission-line regions (ELRs) within a single galaxy. We identified a total of 1162 H alpha [O III], and/or [O II] emission lines in the PEARS sample of 906 galaxies to a limiting flux of similar to 10(-18) erg s(-1) cm(-2). The ELRs have also been compared to the properties of the host galaxy, including morphology, luminosity, and mass. From this analysis, we find three key results: (1) the computed line luminosities show evidence of a flattening in the luminosity function with increasing redshift; (2) the star-forming systems show evidence of complex morphologies with star formation occurring predominantly within one effective (half-light) radius. However, the morphologies show no correlation with host stellar mass. (3) Also, the number density of SFGs with M-* >= 10(9) M-circle dot decreases by an order of magnitude at z <= 0.5 relative to the number at 0.5 < z < 0.9, supporting the argument of galaxy downsizing.
C1 [Pirzkal, Nor; Rothberg, Barry; Ly, Chun; Grogin, Norman A.; Dahlen, Tomas; Noeske, Kai G.; Bellini, Andrea] Space Telescope Sci Inst, Baltimore, MD 21210 USA.
[Rothberg, Barry] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA.
[Rothberg, Barry] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Malhotra, Sangeeta; Rhoads, James E.; Cohen, Seth H.; Mechtley, Matthew; Windhorst, Rogier A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Meurer, Gerhardt R.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia.
[Walsh, Jeremy R.] European So Observ, D-85748 Garching, Germany.
[Hathi, Nimish P.] Carnegie Observ, Pasadena, CA 91101 USA.
[Holwerda, Benne W.] ESA ESTEC, NL-2200 AG Noordwijk, Netherlands.
[Straughn, Amber N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Pirzkal, N (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21210 USA.
RI Hathi, Nimish/J-7092-2014;
OI Hathi, Nimish/0000-0001-6145-5090; Mechtley, Matt/0000-0001-6462-6190;
Ly, Chun/0000-0002-4245-2318; Holwerda, Benne/0000-0002-4884-6756
NR 47
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2013
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IS 1
AR 48
DI 10.1088/0004-637X/772/1/48
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700048
ER
PT J
AU Rigliaco, E
Pascucci, I
Gorti, U
Edwards, S
Hollenbach, D
AF Rigliaco, E.
Pascucci, I.
Gorti, U.
Edwards, S.
Hollenbach, D.
TI UNDERSTANDING THE ORIGIN OF THE [O I] LOW-VELOCITY COMPONENT FROM T
TAURI STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; protoplanetary disks; stars: formation;
stars: pre-main sequence; ultraviolet: stars
ID MAIN-SEQUENCE STARS; LOW-MASS STARS; PHOTOEVAPORATING PROTOPLANETARY
DISCS; FORBIDDEN-LINE EMISSION; HUBBLE-SPACE-TELESCOPE; X-RAY; YOUNG
STARS; RU-LUPI; OBSERVATIONAL CONSTRAINTS; CIRCUMSTELLAR DISKS
AB The formation time, masses, and location of planets are strongly impacted by the physical mechanisms that disperse protoplanetary disks and the timescale over which protoplanetary material is cleared out. Accretion of matter onto the central star, protostellar winds/jets, magnetic disk winds, and photoevaporative winds operate concurrently. Hence, disentangling their relative contribution to disk dispersal requires identifying diagnostics that trace different star-disk environments. Here, we analyze the low-velocity component (LVC) of the oxygen optical forbidden lines, which is found to be blueshifted by a few km s(-1) with respect to the stellar velocity. We find that the [O I] LVC profiles are different from those of [Ne II] at 12.81 mu m and CO at 4.7 mu m lines pointing to different origins for these gas lines. We report a correlation between the luminosity of the [O I] LVC and the accretion luminosity L-acc. We do not find any correlation with the X-ray luminosity, while we find that the higher is the stellar far-UV (FUV) luminosity, the higher is the luminosity of the [O I] LVC. In addition, we show that the [O I] lambda 6300/lambda 5577 ratio is low (ranging between 1 and 8). These findings favor an origin of the [O I] LVC in a region where OH is photodissociated by stellar FUV photons and argue against thermal emission from an X-ray-heated layer. Detailed modeling of two spectra with the highest S/N and resolution shows that there are two components within the LVC: a broad, centrally peaked component that can be attributed to gas arising in a warm disk surface in Keplerian rotation (with FWHM between similar to 40 and similar to 60 km s(-1)), and a narrow component (with FWHM similar to 10 km s(-1) and small blueshifts of similar to 2 km s(-1)) that may arise in a cool (<= 1000 K) molecular wind.
C1 [Rigliaco, E.; Pascucci, I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Gorti, U.; Hollenbach, D.] SETI Inst, Mountain View, CA USA.
[Gorti, U.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Edwards, S.] Smith Coll, Dept Astron, Northampton, MA 01063 USA.
RP Rigliaco, E (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM rigliaco@lpl.arizona.edu
FU Astronomy and Astrophysics research grant [AST0908479]; NASA ADAP grant
[NNX09AC78G]
FX The authors thank Jeanette Bast for providing us with the CO line
profiles, and Germano Sacco for providing us with the [Ne II] line
profiles. We also thank Barbara Ercolano and James Owen for useful
discussions about the X-ray photoevaporation. Support for E.R. was
provided by Astronomy and Astrophysics research grant to I.P. (ID:
AST0908479). U.G. acknowledges support from a NASA ADAP grant
(NNX09AC78G). The authors thank the anonymous referee for helpful
comments that improved the clarity of this paper.
NR 94
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U1 0
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2013
VL 772
IS 1
AR UNSP 60
DI 10.1088/0004-637X/772/1/60
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700060
ER
PT J
AU Sifon, C
Menanteau, F
Hasselfield, M
Marriage, TA
Hughes, JP
Barrientos, LF
Gonzalez, J
Infante, L
Addison, GE
Baker, AJ
Battaglia, N
Bond, JR
Crichton, D
Das, S
Devlin, MJ
Dunkley, J
Dunner, R
Gralla, MB
Hajian, A
Hilton, M
Hincks, AD
Kosowsky, AB
Marsden, D
Moodley, K
Niemack, MD
Nolta, MR
Page, LA
Partridge, B
Reese, ED
Sehgal, N
Sievers, J
Spergel, DN
Staggs, ST
Thornton, RJ
Trac, H
Wollack, EJ
AF Sifon, Cristobal
Menanteau, Felipe
Hasselfield, Matthew
Marriage, Tobias A.
Hughes, John P.
Felipe Barrientos, L.
Gonzalez, Jorge
Infante, Leopoldo
Addison, Graeme E.
Baker, Andrew J.
Battaglia, Nick
Bond, J. Richard
Crichton, Devin
Das, Sudeep
Devlin, Mark J.
Dunkley, Joanna
Duenner, Rolando
Gralla, Megan B.
Hajian, Amir
Hilton, Matt
Hincks, Adam D.
Kosowsky, Arthur B.
Marsden, Danica
Moodley, Kavilan
Niemack, Michael D.
Nolta, Michael R.
Page, Lyman A.
Partridge, Bruce
Reese, Erik D.
Sehgal, Neelima
Sievers, Jon
Spergel, David N.
Staggs, Suzanne T.
Thornton, Robert J.
Trac, Hy
Wollack, Edward J.
TI THE ATACAMA COSMOLOGY TELESCOPE: DYNAMICAL MASSES AND SCALING RELATIONS
FOR A SAMPLE OF MASSIVE SUNYAEV-ZEL'DOVICH EFFECT SELECTED GALAXY
CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; galaxies:
clusters: general; galaxies: distances and redshifts
ID SOUTH-POLE TELESCOPE; X-RAY-PROPERTIES; DIGITAL SKY SURVEY; RICH
CLUSTERS; VELOCITY DISPERSIONS; OBSERVED GROWTH; 148 GHZ;
PHYSICAL-PROPERTIES; LINEAR-REGRESSION; ASTRONOMICAL DATA
AB We present the first dynamical mass estimates and scaling relations for a sample of Sunyaev-Zel'dovich effect (SZE) selected galaxy clusters. The sample consists of 16 massive clusters detected with the Atacama Cosmology Telescope (ACT) over a 455 deg(2) area of the southern sky. Deep multi-object spectroscopic observations were taken to secure intermediate-resolution (R similar to 700-800) spectra and redshifts for approximate to 60 member galaxies on average per cluster. The dynamical masses M-200c of the clusters have been calculated using simulation-based scaling relations between velocity dispersion and mass. The sample has a median redshift z = 0.50 and a median mass M-200c similar or equal to 12 x 10(14) h(70)(-1) M-circle dot with a lower limit M-200c similar or equal to 6 x 10(14)h(70)(-1) M-circle dot, consistent with the expectations for the ACT southern sky survey. These masses are compared to the ACT SZE properties of the sample, specifically, the match-filtered central SZE amplitude (y) over tilde (0), the central Compton parameter y(0), and the integrated Compton signal Y-200c, which we use to derive SZE-mass scaling relations. All SZE estimators correlate with dynamical mass with low intrinsic scatter (less than or similar to 20%), in agreement with numerical simulations. We explore the effects of various systematic effects on these scaling relations, including the correlation between observables and the influence of dynamically disturbed clusters. Using the three-dimensional information available, we divide the sample into relaxed and disturbed clusters and find that similar to 50% of the clusters are disturbed. There are hints that disturbed systems might bias the scaling relations, but given the current sample sizes, these differences are not significant; further studies including more clusters are required to assess the impact of these clusters on the scaling relations.
C1 [Sifon, Cristobal; Felipe Barrientos, L.; Gonzalez, Jorge; Infante, Leopoldo; Duenner, Rolando] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Sifon, Cristobal] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Menanteau, Felipe; Hughes, John P.; Baker, Andrew J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Marriage, Tobias A.; Crichton, Devin; Gralla, Megan B.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Addison, Graeme E.; Dunkley, Joanna] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
[Battaglia, Nick; Bond, J. Richard; Hajian, Amir; Hincks, Adam D.; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Das, Sudeep] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Devlin, Mark J.; Reese, Erik D.; Thornton, Robert J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Hincks, Adam D.; Page, Lyman A.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Kosowsky, Arthur B.] 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, Sch Math Sci, ZA-4041 Durban, South Africa.
[Niemack, Michael D.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Sehgal, Neelima; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Thornton, Robert J.] W Chester Univ, Dept Phys, W Chester, PA 19383 USA.
[Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Trac,
Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Menanteau, Felipe/0000-0002-1372-2534; Sievers,
Jonathan/0000-0001-6903-5074; Sifon, Cristobal/0000-0002-8149-1352
FU European Organisation for Astronomical Research in the Southern
Hemisphere, Chile [084.A-0577, 086.A-0425]; Programa de Astronomia de la
Comision Nacional de Investigacion Cientifica y Tecnologica de Chile
(CONICYT); U.S. National Science Foundation [AST-0408698, AST-0965625,
PHY-0855887, PHY-1214379, AST-0707731, PIRE-0507768, OISE-0530095];
Princeton University; University of Pennsylvania; Canada Foundation for
Innovation (CFI); CFI; Compute Canada; Government of Ontario; Ontario
Research Fund-Research Excellence; University of Toronto; Centro de
Astrofisica FONDAP [15010003]; Centro BASAL-CATA; FONDECYT [1120676,
1085286]; ALMA-CONICYT [31090002, 31100003]
FX Based in part on observations collected at the European Organisation for
Astronomical Research in the Southern Hemisphere, Chile, under programs
084.A-0577 and 086.A-0425.; ACT operates in the Parque Astronomico
Atacama in northern Chile under the auspices of Programa de Astronomia
de la Comision Nacional de Investigacion Cientifica y Tecnologica de
Chile (CONICYT). This work was supported by the U.S. National Science
Foundation through awards AST-0408698 and AST-0965625 for the ACT
project, and PHY-0855887, PHY-1214379, AST-0707731, and PIRE-0507768
(award No. OISE-0530095). Funding was also provided by Princeton
University, the University of Pennsylvania, and a Canada Foundation for
Innovation (CFI) award to UBC. 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. This research is partially funded by "Centro de Astrofisica
FONDAP" 15010003, Centro BASAL-CATA, by FONDECYT under projects 1120676
and 1085286 and by ALMA-CONICYT under projects 31090002 and 31100003.
NR 126
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U2 10
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2013
VL 772
IS 1
AR 25
DI 10.1088/0004-637X/772/1/25
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700025
ER
PT J
AU Tazaki, F
Ueda, Y
Terashima, Y
Mushotzky, RF
Tombesi, F
AF Tazaki, Fumie
Ueda, Yoshihiro
Terashima, Yuichi
Mushotzky, Richard F.
Tombesi, Francesco
TI SUZAKU VIEW OF THE SWIFT/BAT ACTIVE GALACTIC NUCLEI. V. TORUS STRUCTURE
OF TWO LUMINOUS RADIO-LOUD ACTIVE GALACTIC NUCLEI (3C 206 AND PKS
0707-35)
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (3C 206, PKS 0707-35); X-rays:
galaxies
ID X-RAY-EMISSION; DISK-JET CONNECTION; SEYFERT-GALAXIES; REFLECTION
SPECTRA; MODELS; ABSORPTION; QUASARS; EVOLUTION; BEPPOSAX; CLUSTERS
AB We present the results from broadband X-ray spectral analysis of 3C 206 and PKS 0707-35 with Suzaku and Swift/BAT, two of the most luminous unobscured and obscured radio-loud active galactic nuclei (AGNs) with hard X-ray luminosities of 10(45.5) erg s(-1) and 10(44.9) erg s(-1) (14-195 keV), respectively. Based on the radio core luminosity, we estimate that the X-ray spectrum of 3C 206 contains a significant (similar to 60% in the 14-195 keV band) contribution from the jet, while it is negligible in PKS 0707-35. We can successfully model the spectra with the jet component (for 3C 206), the transmitted emission, and two reflection components from the torus and the accretion disk. The reflection strengths from the torus are found to be R-torus(equivalent to Omega/2 pi) = 0.29 +/- 0.18 and 0.41 +/- 0.18 for 3C 206 and PKS 0707-35, respectively, which are smaller than those in typical Seyfert galaxies. Utilizing the torus model by Ikeda et al., we quantify the relation between the half-opening angle of a torus (theta(oa)) and the equivalent width of an iron-K line. The observed equivalent width of 3C 206, < 71 eV, constrains the column density in the equatorial plane to N-H(eq) < 10(23) cm(-2), or the half-opening angle to theta(oa) > 80 degrees if N-H(eq) = 10(24) cm(-2) is assumed. That of PKS 0707-35, 72 +/- 36 eV, is consistent with N-H(eq) similar to 10(23) cm(-2). Our results suggest that the tori in luminous radio-loud AGNs are only poorly developed. The trend is similar to that seen in radio-quiet AGNs, implying that the torus structure is not different between AGNs with jets and without jets.
C1 [Tazaki, Fumie; Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan.
[Terashima, Yuichi] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan.
[Mushotzky, Richard F.; Tombesi, Francesco] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Tombesi, Francesco] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Tombesi, Francesco] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
RP Tazaki, F (reprint author), Kyoto Univ, Dept Astron, Kyoto 6068502, Japan.
RI XRAY, SUZAKU/A-1808-2009
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT) of
Japan; [23540265]
FX We thank the anonymous referee for many useful comments. This work was
partly supported by the Grant-in-Aid for JSPS Fellows for young
researchers (F. T.) and for Scientific Research 23540265 (Y.U.), and by
the Grant-in-Aid for the Global COE Program "The Next Generation of
Physics, Spun from Universality and Emergence" from the Ministry of
Education, Culture, Sports, Science and Technology (MEXT) of Japan.
NR 64
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U1 0
U2 2
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2013
VL 772
IS 1
AR 38
DI 10.1088/0004-637X/772/1/38
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700038
ER
PT J
AU Viero, MP
Wang, L
Zemcov, M
Addison, G
Amblard, A
Arumugam, V
Aussel, H
Bethermin, M
Bock, J
Boselli, A
Buat, V
Burgarella, D
Casey, CM
Clements, DL
Conley, A
Conversi, L
Cooray, A
De Zotti, G
Dowell, CD
Farrah, D
Franceschini, A
Glenn, J
Griffin, M
Hatziminaoglou, E
Heinis, S
Ibar, E
Ivison, RJ
Lagache, G
Levenson, L
Marchetti, L
Marsden, G
Nguyen, HT
O'Halloran, B
Oliver, SJ
Omont, A
Page, MJ
Papageorgiou, A
Pearson, CP
Perez-Fournon, I
Pohlen, M
Rigopoulou, D
Roseboom, IG
Rowan-Robinson, M
Schulz, B
Scott, D
Seymour, N
Shupe, DL
Smith, AJ
Symeonidis, M
Vaccari, M
Valtchanov, I
Vieira, JD
Wardlow, J
Xu, CK
AF Viero, M. P.
Wang, L.
Zemcov, M.
Addison, G.
Amblard, A.
Arumugam, V.
Aussel, H.
Bethermin, M.
Bock, J.
Boselli, A.
Buat, V.
Burgarella, D.
Casey, C. M.
Clements, D. L.
Conley, A.
Conversi, L.
Cooray, A.
De Zotti, G.
Dowell, C. D.
Farrah, D.
Franceschini, A.
Glenn, J.
Griffin, M.
Hatziminaoglou, E.
Heinis, S.
Ibar, E.
Ivison, R. J.
Lagache, G.
Levenson, L.
Marchetti, L.
Marsden, G.
Nguyen, H. T.
O'Halloran, B.
Oliver, S. J.
Omont, A.
Page, M. J.
Papageorgiou, A.
Pearson, C. P.
Perez-Fournon, I.
Pohlen, M.
Rigopoulou, D.
Roseboom, I. G.
Rowan-Robinson, M.
Schulz, B.
Scott, D.
Seymour, N.
Shupe, D. L.
Smith, A. J.
Symeonidis, M.
Vaccari, M.
Valtchanov, I.
Vieira, J. D.
Wardlow, J.
Xu, C. K.
TI HerMES: COSMIC INFRARED BACKGROUND ANISOTROPIES AND THE CLUSTERING OF
DUSTY STAR-FORMING GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: formation; galaxies: halos; large-scale structure of universe
ID 160 MU-M; SUBMILLIMETER-SELECTED GALAXIES; MULTIBAND IMAGING PHOTOMETER;
ATACAMA COSMOLOGY TELESCOPE; FORMATION-DENSITY RELATION; SOUTH-POLE
TELESCOPE; SIMILAR-TO 2; LESS-THAN 2; HERSCHEL-ATLAS; POWER SPECTRUM
AB We present measurements of the auto-and cross-frequency power spectra of the cosmic infrared background (CIB) at 250, 350, and 500 mu m (1200, 860, and 600 GHz) from observations totaling similar to 70 deg(2) made with the SPIRE instrument aboard the Herschel Space Observatory. We measure a fractional anisotropy delta I/I = 14% +/- 4%, detecting signatures arising from the clustering of dusty star-forming galaxies in both the linear (2-halo) and nonlinear (1-halo) regimes; and that the transition from the 2- to 1-halo terms, below which power originates predominantly from multiple galaxies within dark matter halos, occurs at k(theta) similar to 0.10-0.12 arcmin(-1) (l similar to 2160-2380), from 250 to 500 mu m. New to this paper is clear evidence of a dependence of the Poisson and 1-halo power on the flux-cut level of masked sources-suggesting that some fraction of the more luminous sources occupy more massive halos as satellites, or are possibly close pairs. We measure the cross-correlation power spectra between bands, finding that bands which are farthest apart are the least correlated, as well as hints of a reduction in the correlation between bands when resolved sources are more aggressively masked. In the second part of the paper, we attempt to interpret the measurements in the framework of the halo model. With the aim of fitting simultaneously with one model the power spectra, number counts, and absolute CIB level in all bands, we find that this is achievable by invoking a luminosity-mass relationship, such that the luminosity-to-mass ratio peaks at a particular halo mass scale and declines toward lower and higher mass halos. Our best-fit model finds that the halo mass which is most efficient at hosting star formation in the redshift range of peak star-forming activity, z similar to 1-3, is log( M-peak/M-circle dot) similar to 12.1 +/- 0.5, and that the minimum halo mass to host infrared galaxies is log(Mmin/M-circle dot) similar to 10.1 +/- 0.6.
C1 [Viero, M. P.; Zemcov, M.; Bock, J.; Cooray, A.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Vieira, J. D.; Xu, C. K.] CALTECH, Pasadena, CA 91125 USA.
[Wang, L.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Wang, L.; Farrah, D.; Oliver, S. J.; Roseboom, I. G.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Zemcov, M.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Addison, G.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Amblard, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Arumugam, V.; Ivison, R. J.; Roseboom, I. G.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Aussel, H.; Bethermin, M.] Univ Paris Diderot, CNRS, CEA, Lab AIM Paris Saclay,DSM Irfu, F-91191 Gif Sur Yvette, France.
[Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Bethermin, M.; Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France.
[Boselli, A.; Buat, V.; Burgarella, D.; Heinis, S.] Univ Aix Marseille, LAM, F-13388 Marseille, France.
[Casey, C. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Clements, D. L.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Conversi, L.] European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain.
[Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[De Zotti, G.] INAF Osservatorio Astronomico Padova, Vicolo Osservatorio, I-35122 Padua, Italy.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Marchetti, L.] Univ Padua, Dipartimento Astron, Vicolo Osservatorio, I-35122 Padua, Italy.
[Glenn, J.] Univ Colorado, CASA 389, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Ibar, E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile.
[Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Omont, A.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Page, M. J.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Pearson, C. P.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Perez-Fournon, I.] IAC, E-38205 San Cristobal la Laguna, Tenerife, Spain.
[Perez-Fournon, I.] ULL, Dept Astrofis, E-38205 San Cristobal la Laguna, Tenerife, Spain.
[Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Bellville, Cape Town, South Africa.
RP Viero, MP (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM marco.viero@caltech.edu
RI amblard, alexandre/L-7694-2014; Wardlow, Julie/C-9903-2015; Ivison,
R./G-4450-2011; Vaccari, Mattia/R-3431-2016;
OI amblard, alexandre/0000-0002-2212-5395; Wardlow,
Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Vaccari,
Mattia/0000-0002-6748-0577; De Zotti, Gianfranco/0000-0003-2868-2595;
Scott, Douglas/0000-0002-6878-9840; Marchetti,
Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536; Casey,
Caitlin/0000-0002-0930-6466; Bethermin, Matthieu/0000-0002-3915-2015
FU UK's Science and Technology Facilities Council [ST/F002858/1]; ERC StG
[DEGAS-259586]; CSA (Canada); NAOC (China); CEA, CNES, CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); NASA (USA)
FX L.W. acknowledges support from UK's Science and Technology Facilities
Council grant ST/F002858/1 and an ERC StG grant (DEGAS-259586). 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).
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2013
VL 772
IS 1
AR 77
DI 10.1088/0004-637X/772/1/77
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181NG
UT WOS:000321673700077
ER
PT J
AU Dragomir, D
Matthews, JM
Eastman, JD
Cameron, C
Howard, AW
Guenther, DB
Kuschnig, R
Moffat, AFJ
Rowe, JF
Rucinski, SM
Sasselov, D
Weiss, WW
AF Dragomir, Diana
Matthews, Jaymie M.
Eastman, Jason D.
Cameron, Chris
Howard, Andrew W.
Guenther, David B.
Kuschnig, Rainer
Moffat, Anthony F. J.
Rowe, Jason F.
Rucinski, Slavek M.
Sasselov, Dimitar
Weiss, Werner W.
TI MOST* DETECTS TRANSITS OF HD 97658b, A WARM, LIKELY VOLATILE-RICH
SUPER-EARTH
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: formation; planets and satellites: interiors;
stars: individual (HD 97658); techniques: photometric
ID Y-2 ISOCHRONES; EXOPLANETS; PHOTOMETRY; SPACE
AB Through photometric monitoring of the extended transit window of HD 97658b with the MOST space telescope, we have found that this exoplanet transits with an ephemeris consistent with that predicted from radial velocity measurements. The mid-transit times are 5.6 sigma earlier than those of the unverified transit-like signals reported in 2011, and we find no connection between the two sets of events. The transit depth together with our determined stellar radius (R-star = 0.703(-0.034)(+0.039) R-circle dot) indicates a 2.34(-0.15)(+0.18) R-circle plus super-Earth. When combined with the radial velocity determined mass of 7.86 +/- 0.73 M-circle plus, our radius measure allows us to derive a planet density of 3.44(-0.82)(+0.91) g cm(-3). Models suggest that a planet with our measured density has a rocky core that is enveloped in an atmosphere composed of lighter elements. The star of the HD 97658 system is the second brightest known to host a transiting super-Earth, facilitating follow-up studies of this not easily daunted, warm and likely volatile-rich exoplanet.
C1 [Dragomir, Diana; Eastman, Jason D.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Dragomir, Diana; Eastman, Jason D.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA USA.
[Matthews, Jaymie M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Cameron, Chris] Cape Breton Univ, Dept Math Phys & Geol, Sydney, NS B1P 6L2, Canada.
[Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Guenther, David B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Moffat, Anthony F. J.] Obs Mont Megant, Notre Dame Des Bois, PQ J0B 2E0, Canada.
[Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA.
[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), Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr Suite 102, Goleta, CA 93117 USA.
EM diana@lcogt.net
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Eastman, Jason/0000-0003-3773-5142;
Dragomir, Diana/0000-0003-2313-467X
FU Natural Sciences and Engineering Research Council of Canada; FQRNT
(Quebec); Austrian Science Fund [P22691-N16]; Austrian Research
Promotion Agency-ALR
FX 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 21
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 20
PY 2013
VL 772
IS 1
AR L2
DI 10.1088/2041-8205/772/1/L2
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181VC
UT WOS:000321696500002
ER
PT J
AU France, K
Nell, N
Kane, R
Burgh, EB
Beasley, M
Green, JC
AF France, Kevin
Nell, Nicholas
Kane, Robert
Burgh, Eric B.
Beasley, Matthew
Green, James C.
TI H-2 EXCITATION STRUCTURE ON THE SIGHTLINES TO delta SCORPII AND zeta
OPHIUCI: FIRST RESULTS FROM THE SUB-ORBITAL LOCAL INTERSTELLAR CLOUD
EXPERIMENT
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE instrumentation: spectrographs; ISM: molecules; stars: individual (eta
Uma (HD 120315), alpha Vir (HD 116658), delta Sco (HD 143275), zeta Oph
(HD 149757))
ID MOLECULAR-HYDROGEN; ROTATIONAL-EXCITATION; PHYSICAL CONDITIONS; COLUMN
DENSITIES; BOW SHOCK; H2; LINES; ABSORPTION; ABUNDANCES; EMISSION
AB We present the first science results from the Sub-orbital Local Interstellar Cloud Experiment (SLICE): moderate resolution 1020-1070 angstrom spectroscopy of four sightlines through the local interstellar medium. High signal-to-noise (S/N) spectra of eta Uma, alpha Vir, delta Sco, and zeta Oph were obtained during a 2013 April 21 rocket flight. The SLICE observations constrain the density, molecular photoexcitation rates, and physical conditions present in the interstellar material toward delta Sco and zeta Oph. Our spectra indicate a factor of two lower total N(H-2) than previously reported for delta Sco, which we attribute to higher S/N and better scattered light control in the new SLICE observations. We find N(H-2) = 1.5 x 10(19) cm(-2) on the delta Sco sightline, with kinetic and excitation temperatures of 67 and 529 K, respectively, and a cloud density of n(H) = 56 cm(-3). Our observations of the bulk of the molecular sightline toward zeta Oph are consistent with previous measurements (N(H-2) approximate to 3 x 10(20) cm(-2) at T-01(H-2) = 66 K and T-exc = 350 K). However, we detect significantly more rotationally excited H-2 toward zeta Oph than previously observed. We infer a cloud density in the rotationally excited component of n(H) approximate to 7600 cm(-3) and suggest that the increased column densities of excited H-2 are a result of the ongoing interaction between zeta Oph and its environment; also manifest as the prominent mid-IR bowshock observed by WISE and the presence of vibrationally excited H-2 molecules observed by the Hubble Space Telescope.
C1 [France, Kevin; Nell, Nicholas; Kane, Robert; Green, James C.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Burgh, Eric B.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Beasley, Matthew] Planetary Resources Inc, Seattle, WA 98104 USA.
RP France, K (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA.
EM kevin.france@colorado.edu
FU NASA Wallops Flight Facility/NSROC payload team; Physical Sciences
Laboratory at New Mexico State University; Navy team at WSMR; NASA Nancy
Grace Roman Fellowship; NASA [NNX10AC66G, NNX13AF55G]
FX We acknowledge the hard work and dedication of the NASA Wallops Flight
Facility/NSROC payload team, the Physical Sciences Laboratory at New
Mexico State University, and the Navy team at WSMR that supported the
36.271 mission. We are indebted to Ted Schultz for assistance with the
design and fabrication of the SLICE electronics package. K.F.
acknowledges support through a NASA Nancy Grace Roman Fellowship during
a portion of this work. This work was further supported by NASA grants
NNX10AC66G and NNX13AF55G to the University of Colorado at Boulder.
NR 29
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 20
PY 2013
VL 772
IS 1
AR L9
DI 10.1088/2041-8205/772/1/L9
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181VC
UT WOS:000321696500009
ER
PT J
AU Kreimeyer, K
Veilleux, S
AF Kreimeyer, Kory
Veilleux, Sylvain
TI MMTF DISCOVERY OF GIANT IONIZATION CONES IN MR 2251-178: IMPLICATIONS
FOR QUASAR RADIATIVE FEEDBACK
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE diffuse radiation; galaxies: halos; intergalactic medium; quasars:
general; quasars: individual (MR 2251-178)
ID ACTIVE GALACTIC NUCLEI; ALPHA EMISSION; GAS FRACTIONS; HIGH-REDSHIFT;
IONIZED-GAS; GALAXIES; REIONIZATION; QSO; TELESCOPE; PROBE
AB We report the discovery of giant ionization cones in the 140 kpc nebula around quasar MR 2251-178 based on deep [O III] lambda 5007/H beta and [N II] lambda 6583/H alpha flux ratio maps obtained with the Maryland-Magellan Tunable Filter on the Baade-Magellan 6.5 m Telescope. These cones are aligned with the weak double-lobed radio source observed on smaller scale (<30 kpc). They have an opening angle similar to 120 degrees +/- 10 degrees and subtend similar to 65%-90% of 4 pi sr, where the uncertainty takes into account possible projection effects. The material in the outer ionization cones is matter-bounded, indicating that all ionizing photons emitted through the cones escape from the system. The quasar ionizing flux is similar to 2-3 times fainter outside of these cones, despite the largely symmetric geometry of the nebula in [O III]. Overall, adding up the contributions from both inside and outside the cones, we find that similar to 65%-95% of the quasar ionizing radiation makes its way out of the system. These results emphasize the need for line ratio maps to quantify the escape fraction of ionizing radiation from quasars and the importance of quasar radiative feedback on the intergalactic medium.
C1 [Kreimeyer, Kory; Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Veilleux, Sylvain] NASA, Astroparticle Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Veilleux, Sylvain] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Kreimeyer, K (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM kory@astro.umd.edu; veilleux@astro.umd.edu
FU NSF grant [AST-10009583]; Senior NASA Postdoctoral Program award;
Alexander von Humboldt Foundation
FX We thank M. McDonald for help with data acquisition and reduction, and
the referee, M. Villar-Martin, for a thoughtful report. This work was
funded through NSF grant AST-10009583 (K.K. and S.V.), a Senior NASA
Postdoctoral Program award (S.V.), and the Alexander von Humboldt
Foundation (S.V.).
NR 39
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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 JUL 20
PY 2013
VL 772
IS 1
AR L11
DI 10.1088/2041-8205/772/1/L11
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181VC
UT WOS:000321696500011
ER
PT J
AU Wang, ZJ
Fidkowski, K
Abgrall, R
Bassi, F
Caraeni, D
Cary, A
Deconinck, H
Hartmann, R
Hillewaert, K
Huynh, HT
Kroll, N
May, G
Persson, PO
van Leer, B
Visbal, M
AF Wang, Z. J.
Fidkowski, Krzysztof
Abgrall, Remi
Bassi, Francesco
Caraeni, Doru
Cary, Andrew
Deconinck, Herman
Hartmann, Ralf
Hillewaert, Koen
Huynh, H. T.
Kroll, Norbert
May, Georg
Persson, Per-Olof
van Leer, Bram
Visbal, Miguel
TI High-order CFD methods: current status and perspective
SO INTERNATIONAL JOURNAL FOR NUMERICAL METHODS IN FLUIDS
LA English
DT Review
DE High-order methods; CFD
ID FINITE-DIFFERENCE SCHEMES; NAVIER-STOKES EQUATIONS; ESSENTIALLY
NONOSCILLATORY SCHEMES; COMPUTATIONAL FLUID-DYNAMICS; RUNGE-KUTTA
SCHEMES; ELEMENT-METHOD; UNSTRUCTURED GRIDS; ACCURATE; RESOLUTION;
ACOUSTICS
AB After several years of planning, the 1st International Workshop on High-Order CFD Methods was successfully held in Nashville, Tennessee, on January 7-8, 2012, just before the 50th Aerospace Sciences Meeting. The American Institute of Aeronautics and Astronautics, the Air Force Office of Scientific Research, and the German Aerospace Center provided much needed support, financial and moral. Over 70 participants from all over the world across the research spectrum of academia, government labs, and private industry attended the workshop. Many exciting results were presented. In this review article, the main motivation and major findings from the workshop are described. Pacing items requiring further effort are presented. Copyright (c) 2013 John Wiley & Sons, Ltd.
C1 [Wang, Z. J.] Iowa State Univ, Dept Aerosp Engn, Ames, IA USA.
[Fidkowski, Krzysztof] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
[Abgrall, Remi] INRIA, Dept Math, Bordeaux, France.
[Bassi, Francesco] Univ Bergamo, I-24044 Bergamo, Italy.
[Huynh, H. T.] NASA Glenn Res Ctr, Washington, DC USA.
[May, Georg] Rhein Westfal TH Aachen, Aachen, Germany.
[Persson, Per-Olof] Univ Calif Berkeley, Berkeley, CA USA.
[van Leer, Bram] Univ Michigan, Ann Arbor, MI 48109 USA.
RP Fidkowski, K (reprint author), Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
EM kfid@umich.edu
RI Wang, Z.J./A-9628-2010;
OI Wang, Z.J./0000-0002-6203-6303; Hartmann, Ralf/0000-0002-0403-1221;
BASSI, Francesco/0000-0003-0504-390X
FU Air Force Office of Scientific Research; AIAA FDTC; DLR
FX We gratefully acknowledge the support by the Air Force Office of
Scientific Research, AIAA FDTC, and DLR.
NR 38
TC 97
Z9 100
U1 12
U2 67
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0271-2091
J9 INT J NUMER METH FL
JI Int. J. Numer. Methods Fluids
PD JUL 20
PY 2013
VL 72
IS 8
BP 811
EP 845
DI 10.1002/fld.3767
PG 35
WC Computer Science, Interdisciplinary Applications; Mathematics,
Interdisciplinary Applications; Mechanics; Physics, Fluids & Plasmas
SC Computer Science; Mathematics; Mechanics; Physics
GA 157DJ
UT WOS:000319875700001
ER
PT J
AU Zamanian-Daryoush, M
Lindner, D
Tallant, TC
Wang, ZN
Buffa, J
Klipfell, E
Parker, Y
Hatala, D
Parsons-Wingerter, P
Rayman, P
Yusufishaq, MSS
Fisher, EA
Smith, JD
Finke, J
DiDonato, JA
Hazen, SL
AF Zamanian-Daryoush, Maryam
Lindner, Daniel
Tallant, Thomas C.
Wang, Zeneng
Buffa, Jennifer
Klipfell, Elizabeth
Parker, Yvonne
Hatala, Denise
Parsons-Wingerter, Patricia
Rayman, Pat
Yusufishaq, Mohamed Sharif S.
Fisher, Edward A.
Smith, Jonathan D.
Finke, Jim
DiDonato, Joseph A.
Hazen, Stanley L.
TI The Cardioprotective Protein Apolipoprotein A1 Promotes Potent
Anti-tumorigenic Effects
SO JOURNAL OF BIOLOGICAL CHEMISTRY
LA English
DT Article
ID HIGH-DENSITY-LIPOPROTEIN; RANDOMIZED CONTROLLED-TRIAL; APOA-I; MATRIX
METALLOPROTEINASES; CORONARY ATHEROSCLEROSIS; LIQUID-CHROMATOGRAPHY;
TUMOR ANGIOGENESIS; OXIDATIVE STRESS; MYELOID CELLS; HUMAN SERUM
AB Here, we show that apolipoprotein A1 (apoA1), the major protein component of high density lipoprotein (HDL), through both innate and adaptive immune processes, potently suppresses tumor growth and metastasis in multiple animal tumor models, including the aggressive B16F10L murine malignant melanoma model. Mice expressing the human apoA1 transgene (A1Tg) exhibited increased infiltration of CD11b(+) F4/80(+) macrophages with M1, anti-tumor phenotype, reduced tumor burden and metastasis, and enhanced survival. In contrast, apoA1-deficient (A1KO) mice showed markedly heightened tumor growth and reduced survival. Injection of human apoA1 into A1KO mice inoculated with tumor cells remarkably reduced both tumor growth and metastasis, enhanced survival, and promoted regression of both tumor and metastasis burden when administered following palpable tumor formation and metastasis development. Studies with apolipoprotein A2 revealed the anti-cancer therapeutic effect was specific to apoA1. In vitro studies ruled out substantial direct suppressive effects by apoA1 or HDL on tumor cells. Animal models defective in different aspects of immunity revealed both innate and adaptive arms of immunity contribute to complete apoA1 anti-tumor activity. This study reveals a potent immunomodulatory role for apoA1 in the tumor microenvironment, altering tumor-associated macrophages from a pro-tumor M2 to an anti-tumor M1 phenotype. Use of apoA1 to redirect in vivo elicited tumor-infiltrating macrophages toward tumor rejection may hold benefit as a potential cancer therapeutic.
C1 [Zamanian-Daryoush, Maryam; Tallant, Thomas C.; Wang, Zeneng; Buffa, Jennifer; Klipfell, Elizabeth; Yusufishaq, Mohamed Sharif S.; Smith, Jonathan D.; DiDonato, Joseph A.; Hazen, Stanley L.] Cleveland Clin, Dept Cellular & Mol Med, Cleveland, OH 44195 USA.
[Zamanian-Daryoush, Maryam; Tallant, Thomas C.; Wang, Zeneng; Buffa, Jennifer; Klipfell, Elizabeth; DiDonato, Joseph A.; Hazen, Stanley L.] Cleveland Clin, Ctr Cardiovasc Diagnost & Prevent, Cleveland, OH 44195 USA.
[Lindner, Daniel; Parker, Yvonne] Cleveland Clin, Taussig Canc Ctr, Cleveland, OH 44195 USA.
[Hatala, Denise] Cleveland Clin, Imaging Core, Cleveland, OH 44195 USA.
[Rayman, Pat; Finke, Jim] Cleveland Clin, Dept Immunol, Cleveland, OH 44195 USA.
[Smith, Jonathan D.; Hazen, Stanley L.] Cleveland Clin, Dept Cardiovasc Med, Cleveland, OH 44195 USA.
[Parsons-Wingerter, Patricia] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
[Fisher, Edward A.] NYU, Sch Med, Dept Cell Biol, New York, NY 10016 USA.
[Fisher, Edward A.; Hazen, Stanley L.] NYU, Sch Med, Dept Med, Leon H Charney Div Cardiol, New York, NY 10016 USA.
RP Hazen, SL (reprint author), Cleveland Clin, Dept Cellular & Mol Med, 9500 Euclid Ave,NC-10, Cleveland, OH 44195 USA.
EM hazens@ccf.org
OI Fisher, Edward/0000-0001-9802-143X
FU National Institutes of Health [P01HL098055, P01HL076491, HL094525];
LeDucq Fondation; Abbott; Cleveland Heart Lab; Esperion; Lilly;
Liposcience Inc.; Merck Co., Inc.; Pfizer Inc.
FX This work was supported, in whole or in part, by National Institutes of
Health Grants P01HL098055, P01HL076491, and HL094525. This work was also
supported in part by a grant from the LeDucq Fondation. Drs.
Zamanian-Daryoush, DiDonato, and Hazen report being listed as
co-inventors on pending and issued patents held by the Cleveland Clinic.
Dr. Hazen reports having been paid as a consultant for the following
companies: Abbott, Cleveland Heart Lab, Esperion, Lilly, Liposcience
Inc., Merck & Co., Inc., and Pfizer Inc. and receiving research funds
from Abbott, Cleveland Heart Lab, Liposcience Inc., and Pfizer Inc.
NR 65
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U1 0
U2 7
PU AMER SOC BIOCHEMISTRY MOLECULAR BIOLOGY INC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3996 USA
SN 0021-9258
J9 J BIOL CHEM
JI J. Biol. Chem.
PD JUL 19
PY 2013
VL 288
IS 29
BP 21237
EP 21252
DI 10.1074/jbc.M113.468967
PG 16
WC Biochemistry & Molecular Biology
SC Biochemistry & Molecular Biology
GA 186AU
UT WOS:000322014400045
PM 23720750
ER
PT J
AU Webster, CR
Mahaffy, PR
Flesch, GJ
Niles, PB
Jones, JH
Leshin, LA
Atreya, SK
Stern, JC
Christensen, LE
Owen, T
Franz, H
Pepin, RO
Steele, A
AF Webster, Chris R.
Mahaffy, Paul R.
Flesch, Gregory J.
Niles, Paul B.
Jones, John H.
Leshin, Laurie A.
Atreya, Sushil K.
Stern, Jennifer C.
Christensen, Lance E.
Owen, Tobias
Franz, Heather
Pepin, Robert O.
Steele, Andrew
CA MSL Sci Team
TI Isotope Ratios of H, C, and O in CO2 and H2O of the Martian Atmosphere
SO SCIENCE
LA English
DT Article
ID METEORITE ALH84001; CLIMATE HISTORY; SNC METEORITES; WATER CYCLE; MARS;
ENVIRONMENTS; D/H; GEOCHEMISTRY; CARBONATES; EVOLUTION
AB Stable isotope ratios of H, C, and O are powerful indicators of a wide variety of planetary geophysical processes, and for Mars they reveal the record of loss of its atmosphere and subsequent interactions with its surface such as carbonate formation. We report in situ measurements of the isotopic ratios of D/H and O-18/O-16 in water and C-13/C-12, O-18/O-16, O-17/O-16, and (CO)-C-13-O-18/(CO)-C-12-O-16 in carbon dioxide, made in the martian atmosphere at Gale Crater from the Curiosity rover using the Sample Analysis at Mars (SAM)'s tunable laser spectrometer (TLS). Comparison between our measurements in the modern atmosphere and those of martian meteorites such as ALH 84001 implies that the martian reservoirs of CO2 and H2O were largely established similar to 4 billion years ago, but that atmospheric loss or surface interaction may be still ongoing.
C1 [Webster, Chris R.; Flesch, Gregory J.; Christensen, Lance E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mahaffy, Paul R.; Stern, Jennifer C.; Franz, Heather] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Leshin, Laurie A.] Rensselaer Polytech Inst, Troy, NY 12180 USA.
[Atreya, Sushil K.] Univ Michigan, Ann Arbor, MI 48105 USA.
[Owen, Tobias] Univ Hawaii, Honolulu, HI 96822 USA.
[Niles, Paul B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Jones, John H.] Univ Arizona, Tucson, AZ 85721 USA.
[Pepin, Robert O.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Steele, Andrew] Carnegie Inst Sci, Washington, DC 20015 USA.
RP Webster, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM chris.r.webster@jpl.nasa.gov
RI szopa, cyril/C-6865-2015; Martin-Torres, Francisco Javier/G-6329-2015;
Blanco, Juan Jose/E-3627-2014; Harri, Ari-Matti/C-7142-2012; Zorzano,
Maria-Paz/F-2184-2015; Dworkin, Jason/C-9417-2012; Stern,
Jennifer/E-3135-2012; Gonzalez, Rafael/D-1748-2009; Rodriguez-Manfredi,
Jose/L-8001-2014; Hayes, Alexander/P-2024-2014; Zorzano,
Maria-Paz/C-5784-2015; Lemmon, Mark/E-9983-2010; Balic-Zunic,
Tonci/A-6362-2013; de Pablo, Miguel Angel/J-6442-2014; Gomez-Elvira,
Javier/K-5829-2014; Ramos, Miguel/K-2230-2014; Gomez, Felipe/L-7315-2014
OI szopa, cyril/0000-0002-0090-4056; Martin-Torres, Francisco
Javier/0000-0001-6479-2236; Blanco, Juan Jose/0000-0002-8666-0696;
Harri, Ari-Matti/0000-0001-8541-2802; Zorzano,
Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997;
Stern, Jennifer/0000-0002-0162-8807; Rodriguez-Manfredi,
Jose/0000-0003-0461-9815; Hayes, Alexander/0000-0001-6397-2630; Zorzano,
Maria-Paz/0000-0002-4492-9650; Lemmon, Mark/0000-0002-4504-5136;
Balic-Zunic, Tonci/0000-0003-1687-1233; de Pablo, Miguel
Angel/0000-0002-4496-2741; Gomez-Elvira, Javier/0000-0002-9068-9846;
Ramos, Miguel/0000-0003-3648-6818; Gomez, Felipe/0000-0001-9977-7060
NR 35
TC 74
Z9 76
U1 17
U2 132
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD JUL 19
PY 2013
VL 341
IS 6143
BP 260
EP 263
DI 10.1126/science.1237961
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 185HV
UT WOS:000321959300038
PM 23869013
ER
PT J
AU Mahaffy, PR
Webster, CR
Atreya, SK
Franz, H
Wong, M
Conrad, PG
Harpold, D
Jones, JJ
Leshin, LA
Manning, H
Owen, T
Pepin, RO
Squyres, S
Trainer, M
AF Mahaffy, Paul R.
Webster, Christopher R.
Atreya, Sushil K.
Franz, Heather
Wong, Michael
Conrad, Pamela G.
Harpold, Dan
Jones, John J.
Leshin, Laurie A.
Manning, Heidi
Owen, Tobias
Pepin, Robert O.
Squyres, Steven
Trainer, Melissa
CA MSL Sci Team
TI Abundance and Isotopic Composition of Gases in the Martian Atmosphere
from the Curiosity Rover
SO SCIENCE
LA English
DT Article
ID TRAPPED NOBLE-GASES; SNC METEORITES; HERSCHEL/HIFI OBSERVATIONS;
CARBON-DIOXIDE; MARS; ORIGIN; NITROGEN; SHERGOTTITES; EETA-79001;
COMPONENTS
AB Volume mixing and isotope ratios secured with repeated atmospheric measurements taken with the Sample Analysis at Mars instrument suite on the Curiosity rover are: carbon dioxide (CO2), 0.960(+/-0.007); argon-40 (Ar-40), 0.0193(+/-0.0001); nitrogen (N-2), 0.0189(+/-0.0003); oxygen, 1.45(+/-0.09) x 10(-3); carbon monoxide, < 1.0 x 10(-3); and Ar-40/Ar-36, 1.9(+/-0.3) x 10(3). The Ar-40/N-2 ratio is 1.7 times greater and the Ar-40/Ar-36 ratio 1.6 times lower than values reported by the Viking Lander mass spectrometer in 1976, whereas other values are generally consistent with Viking and remote sensing observations. The Ar-40/Ar-36 ratio is consistent with martian meteoritic values, which provides additional strong support for a martian origin of these rocks. The isotopic signature delta C-13 from CO2 of similar to 45 per mil is independently measured with two instruments. This heavy isotope enrichment in carbon supports the hypothesis of substantial atmospheric loss.
C1 [Mahaffy, Paul R.; Franz, Heather; Conrad, Pamela G.; Harpold, Dan; Trainer, Melissa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Webster, Christopher R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Atreya, Sushil K.; Wong, Michael] Univ Michigan, Ann Arbor, MI 48109 USA.
[Jones, John J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Leshin, Laurie A.] Rensselaer Polytech Inst, Troy, NY 12180 USA.
[Manning, Heidi] Concordia Coll, Moorhead, MN 56562 USA.
[Owen, Tobias] Univ Hawaii, Honolulu, HI 96822 USA.
[Pepin, Robert O.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Squyres, Steven] Cornell Univ, Ithaca, NY 14853 USA.
RP Mahaffy, PR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM paul.r.mahaffy@nasa.gov
RI Martin-Torres, Francisco Javier/G-6329-2015; Blanco, Juan
Jose/E-3627-2014; Harri, Ari-Matti/C-7142-2012; Zorzano,
Maria-Paz/F-2184-2015; Dworkin, Jason/C-9417-2012; Gonzalez,
Rafael/D-1748-2009; Lemmon, Mark/E-9983-2010; Balic-Zunic,
Tonci/A-6362-2013; de Pablo, Miguel Angel/J-6442-2014; Gomez-Elvira,
Javier/K-5829-2014; Ramos, Miguel/K-2230-2014; Gomez,
Felipe/L-7315-2014; Rodriguez-Manfredi, Jose/L-8001-2014; Hayes,
Alexander/P-2024-2014; Zorzano, Maria-Paz/C-5784-2015; szopa,
cyril/C-6865-2015
OI Martin-Torres, Francisco Javier/0000-0001-6479-2236; Blanco, Juan
Jose/0000-0002-8666-0696; Harri, Ari-Matti/0000-0001-8541-2802; Zorzano,
Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997;
Muller, Jan-Peter/0000-0002-5077-3736; Lemmon, Mark/0000-0002-4504-5136;
Balic-Zunic, Tonci/0000-0003-1687-1233; de Pablo, Miguel
Angel/0000-0002-4496-2741; Gomez-Elvira, Javier/0000-0002-9068-9846;
Ramos, Miguel/0000-0003-3648-6818; Gomez, Felipe/0000-0001-9977-7060;
Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Hayes,
Alexander/0000-0001-6397-2630; Zorzano, Maria-Paz/0000-0002-4492-9650;
szopa, cyril/0000-0002-0090-4056
NR 41
TC 80
Z9 83
U1 14
U2 138
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 JUL 19
PY 2013
VL 341
IS 6143
BP 263
EP 266
DI 10.1126/science.1237966
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 185HV
UT WOS:000321959300039
PM 23869014
ER
PT J
AU Rignot, E
Jacobs, S
Mouginot, J
Scheuchl, B
AF Rignot, E.
Jacobs, S.
Mouginot, J.
Scheuchl, B.
TI Ice-Shelf Melting Around Antarctica
SO SCIENCE
LA English
DT Article
ID PINE ISLAND GLACIER; MASS-BALANCE; SHEET; CIRCULATION; THICKNESS; CAVITY
AB We compare the volume flux divergence of Antarctic ice shelves in 2007 and 2008 with 1979 to 2010 surface accumulation and 2003 to 2008 thinning to determine their rates of melting and mass balance. Basal melt of 1325 +/- 235 gigatons per year (Gt/year) exceeds a calving flux of 1089 +/- 139 Gt/year, making ice-shelf melting the largest ablation process in Antarctica. The giant cold-cavity Ross, Filchner, and Ronne ice shelves covering two-thirds of the total ice-shelf area account for only 15% of net melting. Half of the meltwater comes from 10 small, warm-cavity Southeast Pacific ice shelves occupying 8% of the area. A similar high melt/area ratio is found for six East Antarctic ice shelves, implying undocumented strong ocean thermal forcing on their deep grounding lines.
C1 [Rignot, E.; Mouginot, J.; Scheuchl, B.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Rignot, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jacobs, S.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
RP Rignot, E (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM erignot@uci.edu
RI Rignot, Eric/A-4560-2014; Mouginot, Jeremie/G-7045-2015;
OI Rignot, Eric/0000-0002-3366-0481; Mouginot, Jeremie/0000-0001-9155-5455
FU NASA's Cryospheric Science Program; NASA's Operation IceBridge (OIB);
National Science Foundation; National Oceanic and Atmospheric
Administration
FX We thank three anonymous reviewers for their constructive criticism of
the manuscript. This work was performed at the University of California,
Irvine, and at the Jet Propulsion Laboratory, California Institute of
Technology, under grants from NASA's Cryospheric Science Program and
Operation IceBridge (OIB) and at the Lamont-Doherty Earth Observatory of
Columbia University under grants from the National Science Foundation
and the National Oceanic and Atmospheric Administration.
NR 35
TC 209
Z9 215
U1 12
U2 130
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 JUL 19
PY 2013
VL 341
IS 6143
BP 266
EP 270
DI 10.1126/science.1235798
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 185HV
UT WOS:000321959300040
PM 23765278
ER
PT J
AU Nitschke, W
Russell, MJ
AF Nitschke, Wolfgang
Russell, Michael J.
TI Beating the acetyl coenzyme A-pathway to the origin of life
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE bioenergetics; origin of life; carbon fixation; alkaline hydrothermal
vent; methanotrophy; Wood-Ljungdahl pathways
ID METHYLOBACTERIUM-EXTORQUENS AM1; CITY HYDROTHERMAL FIELD; ANAEROBIC
METHANE OXIDATION; BANDED IRON FORMATIONS; METHANOGENIC ARCHAEA;
METHYLOTROPHIC BACTERIA; VOLCANIC EMISSIONS; DEPENDENT ENZYMES; EARLY
EVOLUTION; CARBON-DIOXIDE
AB Attempts to draft plausible scenarios for the origin of life have in the past mainly built upon palaeogeochemical boundary conditions while, as detailed in a companion article in this issue, frequently neglecting to comply with fundamental thermodynamic laws. Even if demands from both palaeogeochemistry and thermodynamics are respected, then a plethora of strongly differing models are still conceivable. Although we have no guarantee that life at its origin necessarily resembled biology in extant organisms, we consider that the only empirical way to deduce how life may have emerged is by taking the stance of assuming continuity of biology from its inception to the present day. Building upon this conviction, we have assessed extant types of energy and carbon metabolism for their appropriateness to conditions probably pertaining in those settings of the Hadean planet that fulfil the thermodynamic requirements for life to come into being. Wood-Ljungdahl (WL) pathways leading to acetyl CoA formation are excellent candidates for such primordial metabolism. Based on a review of our present understanding of the biochemistry and biophysics of acetogenic, methanogenic and methanotrophic pathways and on a phylogenetic analysis of involved enzymes, we propose that a variant of modern methanotrophy is more likely than traditional WL systems to date back to the origin of life. The proposed model furthermore better fits basic thermodynamic demands and palaeogeochemical conditions suggested by recent results from extant alkaline hydrothermal seeps.
C1 [Nitschke, Wolfgang] CNRS AMU, Bioenerget & Ingn Prot UMR7281, Marseille, France.
[Russell, Michael J.] CALTECH, Jet Prop Lab, Planetary Sci Sect 3225, Pasadena, CA 91109 USA.
RP Nitschke, W (reprint author), CNRS AMU, Bioenerget & Ingn Prot UMR7281, FR3479, Marseille, France.
EM nitschke@imm.cnrs.fr
OI Nitschke, Wolfgang/0000-0003-2084-3032
FU National Aeronautics and Space Administration; NASA Astrobiology
Institute (Icy Worlds); French Agence Nationale pour la Recherche
[ANR-Blanc-MC2]; U.S. Government
FX We appreciate help from Elbert Branscomb (Urbana-Champaign/Illinois),
Isik Kanik (Pasadena/California), Shawn McGlynn (Pasadena/California),
Barbara Schoepp-Cothenet (Marseilles/France), Anne-Lise Ducluzeau
(Lincoln/Nebraska), Frauke Baymann (Marseilles/France) and Robert van
Lis (Marseilles/France). The research described for this publication was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration with support by the NASA Astrobiology Institute (Icy
Worlds) and by the French Agence Nationale pour la Recherche
(ANR-Blanc-MC2). U.S. Government sponsorship is acknowledged.
NR 112
TC 26
Z9 28
U1 5
U2 96
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8436
EI 1471-2970
J9 PHILOS T R SOC B
JI Philos. Trans. R. Soc. B-Biol. Sci.
PD JUL 19
PY 2013
VL 368
IS 1622
AR 20120258
DI 10.1098/rstb.2012.0258
PG 15
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 160GF
UT WOS:000320105200005
PM 23754811
ER
PT J
AU Russell, MJ
Nitschke, W
Branscomb, E
AF Russell, Michael J.
Nitschke, Wolfgang
Branscomb, Elbert
TI The inevitable journey to being
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE origin of life; carbon fixation; alkaline hydrothermal; disequilibria;
pyrophosphatase
ID CITY HYDROTHERMAL FIELD; HYDROTALCITE-LIKE COMPOUNDS; MINERAL INDUCED
FORMATION; EAST PACIFIC RISE; GREEN RUST; POURBAIX-DIAGRAMS;
CONFORMATIONAL-CHANGES; PREBIOTIC SYNTHESIS; CRYSTAL-STRUCTURE;
OXIDATION-STATE
AB Life is evolutionarily the most complex of the emergent symmetry-breaking, macroscopically organized dynamic structures in the Universe. Members of this cascading series of disequilibria-converting systems, or engines in Cottrell's terminology, become ever more complicated-more chemical and less physical-as each engine extracts, exploits and generates ever lower grades of energy and resources in the service of entropy generation. Each one of these engines emerges spontaneously from order created by a particular mother engine or engines, as the disequilibrated potential daughter is driven beyond a critical point. Exothermic serpentinization of ocean crust is life's mother engine. It drives alkaline hydrothermal convection and thereby the spontaneous production of precipitated submarine hydrothermal mounds. Here, the two chemical disequilibria directly causative in the emergence of life spontaneously arose across the mineral precipitate membranes separating the acidulous, nitrate-bearing CO2-rich, Hadean sea from the alkaline and CH4/H-2-rich serpentinization-generated effluents. Essential redox gradients-involving hydrothermal CH4 and H-2 as electron donors, CO2 and nitrate, nitrite, and ferric iron from the ambient ocean as acceptors-were imposed which functioned as the original 'carbon-fixing engine'. At the same time, a post-critical-point (milli) voltage pH potential (proton concentration gradient) drove the condensation of orthophosphate to produce a high energy currency: 'the pyrophosphatase engine'.
C1 [Russell, Michael J.] CALTECH, Jet Prop Lab, Planetary Sci Sect 3225, Pasadena, CA 91109 USA.
[Nitschke, Wolfgang] CNRS AMU, Bioenerget & Ingn Prot UMR7281, FR3479, Marseille, France.
[Branscomb, Elbert] Univ Illinois, Inst Genom Biol, Urbana, IL 61801 USA.
RP Russell, MJ (reprint author), CALTECH, Jet Prop Lab, Planetary Sci Sect 3225, 800 Oak Grove Dr,MS 183-301, Pasadena, CA 91109 USA.
EM michael.j.russell@jpl.nasa.gov
OI Nitschke, Wolfgang/0000-0003-2084-3032
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute [NNA13AA91A]; French Agence Nationale pour la
Recherche [ANR-Blanc-MC2]; U.S. Government
FX We appreciate help from Jan Amend, Nick Arndt, Laurie Barge,
GiuseppeEtiope, Nigel Goldenfeld, Elizabeth Jagger, Isik Kanik, Richard
Kidd, Nick Lane, Ole Lutjens, Tom McCollom, Shawn McGlynn, Randall
Mielke, James Milner-White, Andrew Russell, Bob Shapiro, Takazo Shibuya
and Lauren White. We also thank Dr Carl Pilcher and the members of the
NAI-sponsored Thermodynamics Disequilibrium and Evolution Focus Group
for discussions. The research described for this publication was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration with support by the NASA Astrobiology Institute (Icy
Worlds); at the Institute for Genomic Biology, UIUC with partial support
of the National Aeronautics and Space Administration through the NASA
Astrobiology Institute under Cooperative Agreement No. NNA13AA91A issued
through the Science Mission Directorate, and at Bioenergetique et
Ingenierie des Proteines, CNRS supported by the French Agence Nationale
pour la Recherche (ANR-Blanc-MC2). U.S. Government sponsorship is
acknowledged.
NR 201
TC 28
Z9 28
U1 9
U2 113
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8436
EI 1471-2970
J9 PHILOS T R SOC B
JI Philos. Trans. R. Soc. B-Biol. Sci.
PD JUL 19
PY 2013
VL 368
IS 1622
AR 20120254
DI 10.1098/rstb.2012.0254
PG 19
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 160GF
UT WOS:000320105200002
PM 23754808
ER
PT J
AU Lamsal, LN
Martin, RV
Parrish, DD
Krotkov, NA
AF Lamsal, L. N.
Martin, R. V.
Parrish, D. D.
Krotkov, N. A.
TI Scaling Relationship for NO2 Pollution and Urban Population Size: A
Satellite Perspective
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; FINE PARTICULATE MATTER; UNITED-STATES;
NITROGEN-DIOXIDE; AIR-POLLUTION; NORTH-AMERICA; GLOBAL BURDEN;
POWER-PLANTS; EMISSIONS; MORTALITY
AB Concern is growing about the effects of urbanization on air pollution and health. Nitrogen dioxide (NO2) released primarily from combustion processes, such as traffic, is a short-lived atmospheric pollutant that serves as an air-quality indicator and is itself a health concern. We derive a global distribution of ground-level NO2 concentrations from tropospheric NO2 columns retrieved from the Ozone Monitoring Instrument (OMI). Local scaling factors from a three-dimensional chemistry-transport model (GEOS-Chem) are used to relate the OMI NO2 columns to ground-level concentrations. The OMI-derived surface NO2 data are significantly correlated (r = 0.69) with in situ surface measurements. We examine how the OMI-derived ground-level NO2 concentrations, OMI NO2 columns, and bottom-up NOx emission inventories relate to urban population. Emission hot spots, such as power plants, are excluded to focus on urban relationships. The correlation of surface NO2 with population is significant for the three countries and one continent examined here: United States (r = 0.71), Europe (r = 0.67), China (r = 0.69), and India (r = 0.59). Urban NO2 pollution, like other urban properties, is a power law scaling function of the population size: NO2 concentration increases proportional to population raised to an exponent. The value of the exponent varies by region from 0.36 for India to 0.66 for China, reflecting regional differences in industrial development and per capita emissions. It has been generally established that energy efficiency increases and, therefore, per capita NO emissions decrease with urban population; here, we show how outdoor ambient NO2 concentrations depend upon urban population in different global regions.
C1 [Lamsal, L. N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA.
[Lamsal, L. N.; Krotkov, N. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
[Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Parrish, D. D.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA.
RP Lamsal, LN (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA.
EM lok.lamsal@nasa.gov
RI Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; Parrish,
David/E-8957-2010; Krotkov, Nickolay/E-1541-2012; Manager, CSD
Publications/B-2789-2015
OI Martin, Randall/0000-0003-2632-8402; Parrish, David/0000-0001-6312-2724;
Krotkov, Nickolay/0000-0001-6170-6750;
FU NASA's Earth Science Directorate Atmospheric Composition Program;
Natural Sciences and Engineering Research Council of Canada
FX We thank Aaron van Donkelaar for performing the GEOS-Chem nested
simulation. The work was supported by NASA's Earth Science Directorate
Atmospheric Composition Program and the Natural Sciences and Engineering
Research Council of Canada.
NR 53
TC 36
Z9 39
U1 5
U2 87
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD JUL 16
PY 2013
VL 47
IS 14
BP 7855
EP 7861
DI 10.1021/es400744g
PG 7
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 186QS
UT WOS:000322059800036
PM 23763377
ER
PT J
AU Tao, WK
Wu, D
Matsui, T
Peters-Lidard, C
Lang, S
Hou, A
Rienecker, M
Petersen, W
Jensen, M
AF Tao, Wei-Kuo
Wu, Di
Matsui, Toshihisa
Peters-Lidard, Christa
Lang, Stephen
Hou, Arthur
Rienecker, Michele
Petersen, Walter
Jensen, Michael
TI Precipitation intensity and variation during MC3E: A numerical modeling
study
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE precipitation; numerical modeling; diurnal variation
ID MESOSCALE CONVECTIVE SYSTEM; CLOUD-RESOLVING SIMULATIONS; TROPICAL
OCEANIC CONVECTION; WARM-SEASON PRECIPITATION; CONTINENTAL
UNITED-STATES; MIDLATITUDE SQUALL LINE; DIURNAL CYCLE; STRATIFORM
PRECIPITATION; PREDICTION MODELS; DOPPLER RADAR
AB Previous observational studies have identified three different types of diurnal precipitation variation over the conterminous U.S.: localized afternoon rainfall maxima over the Mississippi and Ohio valleys, propagating mesoscale convective systems (MCSs) from the Rocky Mountain region, and propagating MCSs over the Appalachian Mountains. This study focuses on the second type, which involves nocturnal rainfall maxima from eastward-propagating MCSs on the lee side of the Rocky Mountains. This study evaluates model simulations with regard to rainfall using observations and assesses the impact of microphysics, surface fluxes, radiation, and terrain on the simulated diurnal rainfall variation. A regional high-resolution model was used to conduct a series of real-time forecasts during the Midlatitude Continental Convective Clouds Experiment (MC3E) in 2011 over the Southern Great Plains. The model ably captured most heavy precipitation events. When all forecast days are composited, the mean forecast depicts accurate, propagating precipitation features and thus the overall diurnal variation. However, individual forecasts tend to overestimate the rainfall for light precipitation events, have location errors, and misrepresent convection in some cases. A post mission case study is performed on one multi-cell, eastward-propagating MCS event; the results suggest that cold-pool dynamics were an important physical process. Model results also indicate that terrain effects are important during the initial stages of MCS development. By increasing the terrain height by 10%, the simulated rainfall is increased and in better agreement with observations. On the other hand, surface fluxes, and radiation processes only have a secondary effect for short-term simulations.
C1 [Tao, Wei-Kuo; Wu, Di; Matsui, Toshihisa; Lang, Stephen; Hou, Arthur] NASA, Mesoscale Atmospher Processes Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wu, Di; Lang, Stephen] Sci Syst & Applicat Inc, Lanham, MD USA.
[Matsui, Toshihisa] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Peters-Lidard, Christa] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rienecker, Michele] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Petersen, Walter] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
[Jensen, Michael] Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Tao, WK (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM Wei-Kuo.Tao-1@nasa.gov
RI Peters-Lidard, Christa/E-1429-2012; Measurement, Global/C-4698-2015
OI Peters-Lidard, Christa/0000-0003-1255-2876;
FU NASA Precipitation Measurement Mission (PMM); NASA Modeling Analysis
Prediction (MAP); Office of Science (BER); U.S. Department of
Energy/Atmospheric System Research (DOE/ASR) Interagency
[DE-AI02-04ER63755]
FX The authors appreciate the hard work and effort of all those who planned
and participated in the MC3E field campaign. We thank R. Johnson and S.
Rutledge at Colorado State University for discussions on stratiform rain
amounts. We would also like to thank Anil Kumar at Goddard for providing
the LIS spin-up data sets. Carrie Langston at the National Severe Storm
Laboratory provided invaluable help in the NEXRAD NMQ data product. The
authors acknowledge the NASA Ames Research Center and the NASA Goddard
Space Flight Center for the computer time used in this research. We also
thank three anonymous reviewers for their constructive comments that
improved this paper significantly. This research was supported by NASA
Precipitation Measurement Mission (PMM), NASA Modeling Analysis
Prediction (MAP), and the Office of Science (BER), U.S. Department of
Energy/Atmospheric System Research (DOE/ASR) Interagency Agreement
DE-AI02-04ER63755. MC3E is a NASA-DOE joint field campaign.
NR 69
TC 15
Z9 15
U1 0
U2 15
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 JUL 16
PY 2013
VL 118
IS 13
BP 7199
EP 7218
DI 10.1002/jgrd.50410
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 188KP
UT WOS:000322192200021
ER
PT J
AU Hashino, T
Satoh, M
Hagihara, Y
Kubota, T
Matsui, T
Nasuno, T
Okamoto, H
AF Hashino, Tempei
Satoh, Masaki
Hagihara, Yuichiro
Kubota, Takuji
Matsui, Toshihisa
Nasuno, Tomoe
Okamoto, Hajime
TI Evaluating cloud microphysics from NICAM against CloudSat and CALIPSO
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE global cloud-resolving model; active satellite measurements; cloud
microphysics; satellite data simulator
ID PARTICLE-SIZE DISTRIBUTIONS; SATELLITE-OBSERVATIONS; PASSIVE MICROWAVE;
RADAR OBSERVATIONS; STRATIFORM CLOUD; FRONTAL CLOUDS; WINTER STORM;
IN-SITU; MODEL; PRECIPITATION
AB We describe a method to evaluate cloud microphysics simulated with a global cloud-resolving model against CloudSat and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) satellite data. Output from the Nonhydrostatic Icosahedral Atmospheric Model (NICAM) is run through a satellite-sensor simulator (Joint Simulator for Satellite Sensors), then directly compared to the radar and lidar signals from CloudSat and CALIPSO. The forward approach allows for consistency in cloud microphysical assumption involved in the evaluation. To investigate the dependence of the signals on the temperature, we use temperature extensively as the vertical coordinate. The global statistical analysis of the radar reflectivity shows that the simulation overestimates all the percentiles above -50 degrees C and that snow category contributes significantly to low reflectivity values between -80 and -40 degrees C. The simulated lidar signals have two modes associated with cloud ice and snow categories, though the observations have only one mode. The synergetic use of radar reflectivity and lidar backscatter enables us to determine the relative magnitudes of ice/liquid water contents and effective radii without use of retrievals. The radar-and-lidar diagnosis for cloud tops shows that, due to snow category, NICAM overestimates the mass-equivalent effective radius and underestimates ice water content. Also, the diagnosis was shown to be useful to investigate sensitivities of the parameters of bulk microphysical schemes on the water contents and sizes. The nonspherical scattering of ice particles was shown to affect the above radar-and-lidar diagnosis for large reflectivity ranges but not to alter most of the other diagnoses for this simulation.
C1 [Hashino, Tempei; Satoh, Masaki] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778568, Japan.
[Hagihara, Yuichiro; Okamoto, Hajime] Kyushu Univ, Res Inst Appl Mech, Fukuoka, Japan.
[Kubota, Takuji] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki, Japan.
[Matsui, Toshihisa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nasuno, Tomoe] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa, Japan.
RP Hashino, T (reprint author), Univ Tokyo, Atmosphere & Ocean Res Inst, 5-1-5 Kashiwano Ha, Kashiwa, Chiba 2778568, Japan.
EM hashino@aori.u-tokyo.ac.jp
RI Kubota, Takuji/E-6024-2011; Okamoto, Hajime/E-6510-2010; Kyushu,
RIAM/F-4018-2015; Satoh, Masaki/G-3325-2015; U-ID, Kyushu/C-5291-2016
OI Kubota, Takuji/0000-0003-0282-1075; Okamoto, Hajime/0000-0002-4540-1698;
Satoh, Masaki/0000-0003-3580-8897;
FU JAXA/EarthCARE 1st Research Announcement
FX This research was supported by the JAXA/EarthCARE 1st Research
Announcement. We thank Chihiro Kodama and Alessandro Battaglia for
valuable discussions, leading to a better manuscript. We also appreciate
the valuable comments and suggestions by the anonymous reviewers. The
NICAM simulations were done using the Earth Simulator at the Japan
Agency for Marine-Earth Science and Technology (JAMSTEC).
NR 56
TC 21
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U1 0
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUL 16
PY 2013
VL 118
IS 13
BP 7273
EP 7292
DI 10.1002/jgrd.50564
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 188KP
UT WOS:000322192200025
ER
PT J
AU Chen, XH
Huang, XL
Liu, X
AF Chen, Xiuhong
Huang, Xianglei
Liu, Xu
TI Non-negligible effects of cloud vertical overlapping assumptions on
longwave spectral fingerprinting studies
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Radiative processes; Global climate models; Remote sensing; Clouds and
aerosols
ID MOLECULAR SPECTROSCOPIC DATABASE; TESTING CLIMATE MODELS;
RADIATIVE-TRANSFER; INFRARED-SPECTRA; PART I; PARAMETERIZATION;
TEMPERATURE
AB In order to monitor and attribute secular changes from outgoing spectral radiances, spectral fingerprints need to be constructed first. Large-scale model outputs are usually used to derive such spectral fingerprints. Different models make different assumptions on vertical overlapping of subgrid clouds. We explore the extent to which the spectral fingerprints constructed under different cloud vertical overlapping assumptions can affect such spectral fingerprinting studies. Utilizing a principal component-based radiative transfer model with high computational efficiency, we build an OSSE (Observing System Simulation Experiment) with full treatment of subgrid cloud variability to study this issue. We first show that the OLR (outgoing longwave radiation) computed from this OSSE is consistent with the OLR directly output from the parent large-scale models. We then examine the differences in spectral fingerprints due to cloud overlapping assumptions alone. Different cloud overlapping assumptions have little effect on the spectral fingerprints of temperature and humidity. However, the amplitude of the spectral fingerprints due to the same amount of cloud fraction change can differ as much as a factor of two between maximum random versus random overlap assumptions, especially for middle and low clouds. We further examine the impact of cloud overlapping assumptions on the results of linear regression of spectral differences with respect to predefined spectral fingerprints. Cloud-relevant regression coefficients are affected more by different cloud overlapping assumptions than regression coefficients of other geophysical variables. These findings highlight the challenges in constructing realistic longwave spectral fingerprints and in detecting climate change using all-sky observations.
C1 [Chen, Xiuhong; Huang, Xianglei] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Liu, Xu] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Huang, XL (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward St, Ann Arbor, MI 48109 USA.
EM xianglei@umich.edu
RI Huang, Xianglei/G-6127-2011; Chen, Xiuhong/P-4030-2014; Richards,
Amber/K-8203-2015
OI Huang, Xianglei/0000-0002-7129-614X;
FU NASA [NNX11AE68G, NNX12AG66G]
FX We wish to thank three anonymous reviewers for their constructive
suggestions, which improved the clarity and readability of the paper. We
are thankful to one reviewer for pointing out the importance of the ERO
assumption in current modeling developments. We thank S. Klein for
informative discussions on the satellite simulator in model assessment.
The AM2 simulations were carried out on NOAA GFDL computing facility.
The research is supported by NASA CLARREO project via NASA NNX11AE68G
awarded to the University of Michigan. X.L. Huang also acknowledges the
support from NASA NNX12AG66G. The ECMWF data were obtained from
http://data-portal.ecmwf.int/data/d/interim_daily/.
NR 47
TC 9
Z9 9
U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUL 16
PY 2013
VL 118
IS 13
BP 7309
EP 7320
DI 10.1002/jgrd.50562
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 188KP
UT WOS:000322192200027
ER
PT J
AU Rosenfeld, D
Bell, TL
AF Rosenfeld, Daniel
Bell, Thomas L.
TI "Why do tornados and hailstorms rest on weekends?" Reply
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Severe storms; weekly cycle; aerosols
ID CLOUDS
C1 [Rosenfeld, Daniel] Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel.
[Bell, Thomas L.] NASA, Climate & Radiat Branch, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Rosenfeld, D (reprint author), Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel.
EM daniel.rosenfeld@huji.ac.il
RI Rosenfeld, Daniel/F-6077-2016
OI Rosenfeld, Daniel/0000-0002-0784-7656
NR 13
TC 1
Z9 1
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUL 16
PY 2013
VL 118
IS 13
BP 7339
EP 7343
DI 10.1002/jgrd.50539
PG 5
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 188KP
UT WOS:000322192200030
ER
PT J
AU Bergamaschi, P
Houweling, S
Segers, A
Krol, M
Frankenberg, C
Scheepmaker, RA
Dlugokencky, E
Wofsy, SC
Kort, EA
Sweeney, C
Schuck, T
Brenninkmeijer, C
Chen, H
Beck, V
Gerbig, C
AF Bergamaschi, P.
Houweling, S.
Segers, A.
Krol, M.
Frankenberg, C.
Scheepmaker, R. A.
Dlugokencky, E.
Wofsy, S. C.
Kort, E. A.
Sweeney, C.
Schuck, T.
Brenninkmeijer, C.
Chen, H.
Beck, V.
Gerbig, C.
TI Atmospheric CH4 in the first decade of the 21st century: Inverse
modeling analysis using SCIAMACHY satellite retrievals and NOAA surface
measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE atmospheric CH4; CH4 emissions; interannual variability and trends
ID GROWTH-RATE; METHANE EMISSIONS; CARBON-DIOXIDE; NORTHERN-HEMISPHERE;
DATA ASSIMILATION; TRANSPORT MODEL; VARIABILITY; CHEMISTRY; CLIMATE;
TROPOSPHERE
AB The causes of renewed growth in the atmospheric CH4 burden since 2007 are still poorly understood and subject of intensive scientific discussion. We present a reanalysis of global CH4 emissions during the 2000s, based on the TM5-4DVAR inverse modeling system. The model is optimized using high-accuracy surface observations from NOAA ESRL's global air sampling network for 2000-2010 combined with retrievals of column-averaged CH4 mole fractions from SCIAMACHY onboard ENVISAT (starting 2003). Using climatological OH fields, derived global total emissions for 2007-2010 are 16-20 Tg CH4/yr higher compared to 2003-2005. Most of the inferred emission increase was located in the tropics (9-14 Tg CH4/yr) and mid- latitudes of the northern hemisphere (6-8 Tg CH4/yr), while no significant trend was derived for Arctic latitudes. The atmospheric increase can be attributed mainly to increased anthropogenic emissions, but the derived trend is significantly smaller than estimated in the EDGARv4.2 emission inventory. Superimposed on the increasing trend in anthropogenic CH4 emissions are significant inter-annual variations (IAV) of emissions from wetlands (up to +/- 10 Tg CH4/yr), and biomass burning (up to +/- 7 Tg CH4/yr). Sensitivity experiments, which investigated the impact of the SCIAMACHY observations (versus inversions using only surface observations), of the OH fields used, and of a priori emission inventories, resulted in differences in the detailed latitudinal attribution of CH4 emissions, but the IAV and trends aggregated over larger latitude bands were reasonably robust. All sensitivity experiments show similar performance against independent shipboard and airborne observations used for validation, except over Amazonia where satellite retrievals improved agreement with observations in the free troposphere.
C1 [Bergamaschi, P.; Segers, A.] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21020 Ispra, Italy.
[Houweling, S.; Krol, M.; Scheepmaker, R. A.] SRON, Netherlands Inst Space Res, Utrecht, Netherlands.
[Houweling, S.; Krol, M.] Inst Marine & Atmospher Res Utrecht IMAU, Utrecht, Netherlands.
[Segers, A.] TNO, Netherlands Org Appl Sci Res, Utrecht, Netherlands.
[Krol, M.] Univ Wageningen & Res Ctr, Meteorol & Air Qual Dept, Wageningen, Netherlands.
[Frankenberg, C.; Kort, E. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Dlugokencky, E.; Sweeney, C.; Chen, H.] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO USA.
[Wofsy, S. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Wofsy, S. C.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Sweeney, C.; Chen, H.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Schuck, T.; Brenninkmeijer, C.] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Chen, H.] Univ Groningen, Ctr Isotope Res, Groningen, Netherlands.
[Beck, V.; Gerbig, C.] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
RP Bergamaschi, P (reprint author), Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21020 Ispra, Italy.
EM peter.bergamaschi@jrc.ec.europa.eu
RI Kort, Eric/F-9942-2012; Chen, Huilin/J-9479-2012; Gerbig,
Christoph/L-3532-2013; Krol, Maarten/E-3414-2013; Frankenberg,
Christian/A-2944-2013
OI Kort, Eric/0000-0003-4940-7541; Chen, Huilin/0000-0002-1573-6673;
Gerbig, Christoph/0000-0002-1112-8603; Frankenberg,
Christian/0000-0002-0546-5857
FU European Commission [218793]; MACC-2 [283576]; Office of Biological and
Environmental Research of the U.S. Department of Energy
[DE-AC02-05CH11231]
FX This work has been supported by the European Commission's Seventh
Framework Programme (FP7/2007-2013) projects MACC under grant agreement
218793 and MACC-2 under grant agreement 283576. We are grateful to
Philippe Le Sager for preprocessing the ECMWF meteorological data as TM5
input. We thank Greet Janssens-Maenhout for providing the EDGARv4.2
emission inventory and for the helpful comments on the manuscript and
Christoph Bruhl for providing the stratospheric CH4 sinks
from the ECHAM5/MESSy1 model. We thank ECMWF for providing computing
resources under the special projects "Inverse Modelling of Atmospheric
CH4 and N2O" (2009-2011) and "Global and Regional Inverse
Modeling of Atmospheric CH4 and N2O" (2012-2014).
Aircraft observations over SGP were supported by the Office of
Biological and Environmental Research of the U.S. Department of Energy
under contract DE-AC02-05CH11231 as part of the Atmospheric Radiation
Measurement Program (ARM), ARM Aerial Facility, and Terrestrial
Ecosystem Science Program.
NR 70
TC 72
Z9 77
U1 1
U2 76
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 JUL 16
PY 2013
VL 118
IS 13
BP 7350
EP 7369
DI 10.1002/jgrd.50480
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 188KP
UT WOS:000322192200032
ER
PT J
AU Labow, GJ
McPeters, RD
Bhartia, PK
Kramarova, N
AF Labow, Gordon J.
McPeters, Richard D.
Bhartia, Pawan K.
Kramarova, Natalya
TI A comparison of 40 years of SBUV measurements of column ozone with data
from the Dobson/Brewer network
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE ozone
ID SOLAR BACKSCATTER ULTRAVIOLET; RAMAN-SCATTERING; CALIBRATION; BREWER
AB Total column ozone data from the Nimbus-4 Backscatter UltraViolet (BUV) instrument, Nimbus-7 Solar Backscatter Ultraviolet (SBUV) instrument, as well as from seven NOAA SBUV/2 instruments have been newly reprocessed with the Version 8.6 ozone retrieval algorithm. This yields a coherent data set that, unlike the Total Ozone Mapping Spectrometer ozone record, has no data gaps or significant time periods with large uncertainties due to calibration issues from 1979 to the present. The column ozone data from the first 3 years of the BUV record (1970-1972) is of high quality and can be used to extend the satellite ozone record back over 40 years. With the new algorithm, an improved total column ozone value is calculated by summing up the profile information as opposed to a single direct column measurement, and the algorithm is optimized for the detection of long-term trends. The results from this processing of these data have been systematically compared to total ozone data from Brewer and Dobson spectrophotometers for many individual ground stations as a function of time, satellite solar zenith angle, and latitude. The time series comparisons show an agreement within +/- 1% over the past 40 years with the bias approaching zero over the last decade. The aerosols associated with the eruption of Mt Pinatubo in 1991 produced an underestimation of ozone for our retrievals at high slant columns while the near-nadir values were relatively unaffected. There is very little systematic offset between the satellite and ground-based measurements as a function of latitude with the Nimbus-4 BUV data (1970-1976) showing the largest offsets. The comparisons as a function of satellite solar zenith angle show consistent behavior for all instruments. Comparisons with ozonesonde data show good agreement in the integrated column up to 25 hPa with differences of no more than 5%.
C1 [Labow, Gordon J.; Kramarova, Natalya] Sci Syst & Applicat Inc, Lanham, MD USA.
[McPeters, Richard D.; Bhartia, Pawan K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Labow, GJ (reprint author), NASA, Goddard Space Flight Ctr, Code 613-3 Mailstop 613-3, Greenbelt, MD 20771 USA.
EM gordon.j.labow@nasa.gov
RI Kramarova, Natalya/D-2270-2014; McPeters, Richard/G-4955-2013; Bhartia,
Pawan/A-4209-2016
OI Kramarova, Natalya/0000-0002-6083-8548; McPeters,
Richard/0000-0002-8926-8462; Bhartia, Pawan/0000-0001-8307-9137
NR 30
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Z9 18
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUL 16
PY 2013
VL 118
IS 13
BP 7370
EP 7378
DI 10.1002/jgrd.50503
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 188KP
UT WOS:000322192200033
ER
PT J
AU Oetjen, H
Baidar, S
Krotkov, NA
Lamsal, LN
Lechner, M
Volkamer, R
AF Oetjen, Hilke
Baidar, Sunil
Krotkov, Nickolay A.
Lamsal, Lok N.
Lechner, Michael
Volkamer, Rainer
TI Airborne MAX-DOAS measurements over California: Testing the NASA OMI
tropospheric NO2 product
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Nitrogen dioxide; Air Quality; satellite; DOAS
ID OZONE MONITORING INSTRUMENT; IN-SITU MEASUREMENTS; COLUMN DENSITIES;
NITROGEN-DIOXIDE; ABSORPTION-MEASUREMENTS; SATELLITE VALIDATION; AEROSOL
EXTINCTION; GOME MEASUREMENTS; TRACE GASES; EMISSIONS
AB Airborne Multi-AXis Differential Optical Absorption Spectroscopy (AMAX-DOAS) measurements of NO2 tropospheric vertical columns were performed over California for two months in summer 2010. The observations are compared to the NASA Ozone Monitoring Instrument (OMI) tropospheric vertical columns (data product v2.1) in two ways: (1) Median data were compared for the whole time period for selected boxes, and the agreement was found to be fair (R = 0.97, slope = 1.4 +/- 0.1, N= 10). (2) A comparison was performed on the mean of coincident AMAX-DOAS measurements within the area of the corresponding OMI pixels with the tropospheric NASA OMI NO2 assigned to that pixel. The effects of different data filters were assessed. Excellent agreement and a strong correlation (R = 0.85, slope = 1.05 +/- 0.09, N= 56) was found for (2) when the data were filtered to eliminate large pixels near the edge of the OMI orbit, the cloud radiance fraction was <50%, the OMI overpass occurred within 2 h of the AMAX-DOAS measurements, the flight altitude was > 2 km, and a representative sample of the footprint was taken by the AMAX-DOAS instrument. The AMAX-DOAS and OMI data sets both show a reduction of NO2 tropospheric columns on weekends by 38 +/- 24% and 33 +/- 11%, respectively. The assumptions in the tropospheric satellite air mass factor simulations were tested using independent measurements of surface albedo, aerosol extinction, and NO2 profiles for Los Angeles for July 2010 indicating an uncertainty of 12%.
C1 [Oetjen, Hilke; Baidar, Sunil; Lechner, Michael; Volkamer, Rainer] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Baidar, Sunil; Volkamer, Rainer] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Krotkov, Nickolay A.; Lamsal, Lok N.; Lechner, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lamsal, Lok N.] Univ Space Res Assoc, Columbia, MD 90034 USA.
RP Volkamer, R (reprint author), Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA.
EM rainer.volkamer@colorado.edu
RI Volkamer, Rainer/B-8925-2016; Krotkov, Nickolay/E-1541-2012; Oetjen,
Hilke/H-3708-2016
OI Volkamer, Rainer/0000-0002-0899-1369; Krotkov,
Nickolay/0000-0001-6170-6750; Oetjen, Hilke/0000-0002-3542-1337
FU California Air Resource Board [09-317]; National Science Foundation
[ATM-847793]; CU start-up funds; ESRL-CIRES graduate fellowship
FX This study was supported by the California Air Resource Board contract
09-317, the National Science Foundation CAREER award ATM-847793, CU
start-up funds (RV) and an ESRL-CIRES graduate fellowship (SB). We thank
T. Deutschmann (University of Heidelberg, Germany) for providing
McArtim, C. Fayt and M. v. Roozendael (IASB-BIRA, Belgium) for WinDOAS,
S.-W. Kim, A. O. Langford, and C. J. Senff (NOAA, Boulder) for
discussions, A. Schneider for the GPS visualizer
(http://www.gpsvisualizer.com/), and the NOAA Twin Otter flight crew for
their support during the campaigns. We acknowledge Jochen Stutz for
providing AERONET data from the Caltech site.
NR 67
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U1 2
U2 22
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 JUL 16
PY 2013
VL 118
IS 13
BP 7400
EP 7413
DI 10.1002/jgrd.50550
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 188KP
UT WOS:000322192200036
ER
PT J
AU Colas, F
Wang, XC
Capet, X
Chao, Y
McWilliams, JC
AF Colas, Francois
Wang, Xiaochun
Capet, Xavier
Chao, Yi
McWilliams, James C.
TI Untangling the roles of wind, run-off and tides in Prince William Sound
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
DE Regional modeling; Prince William Sound; Circulation variability;
Run-off; Tides
ID ALASKA COASTAL CURRENT; NORTHERN GULF; OCEAN CIRCULATION; MODELING
SYSTEM; SURFACE; VARIABILITY; TOPOGRAPHY; SATELLITE; EDDIES; FLOW
AB Prince William Sound (PWS) oceanic circulation is driven by a combination of local wind, large run-off and strong tides. Using a regional oceanic model of the Gulf of Alaska, adequately resolving the mean circulation and mesoscale eddies, we configure a series of three nested domains. The inner domain zooms in on Prince William Sound with a 1-km horizontal grid resolution. We analyze a set of four experiments with different combinations of run-off, wind and tides to demonstrate the relative influence of these forcing on the central Sound mean circulation cell and its seasonal variability. The mean circulation in the central PWS region is generally characterized by a cyclonic cell. When forced only by the wind, the circulation is cyclonic in winter and fall and strongly anticyclonic in summer. The addition of freshwater run-off greatly enhances the eddy kinetic energy in PWS partly through near-surface baroclinic instabilities. This leads to a much more intermittent circulation in the central Sound, with the presence of intense small-scale turbulence and a disappearance of the summer wind-forced anticyclonic cell. The addition of tides reduces the turbulence intensity (relatively to the experiment with run-off only), particularly in the central Sound. The generation of turbulent motions by baroclinic processes is lowered by tidal mixing and by modification of the exchange at Hinchinbrook Entrance. Tides have an overall stabilizing effect on the central Sound circulation. Tidal rectification currents help maintain a mean cyclonic circulation throughout the year. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Colas, Francois; McWilliams, James C.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Wang, Xiaochun; Chao, Yi] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Capet, Xavier] IFREMER, Lab Phys Oceans, Plouzane, France.
[Chao, Yi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Colas, F (reprint author), Univ Paris 06, LOCEAN, IPSL, Paris, France.
EM francois@atmos.ucla.edu
RI Colas, Francois/B-4920-2012
OI Colas, Francois/0000-0002-5859-6586
FU Alaska Ocean Observing System (AOOS); Oil Spill Recovery Institute
(OSRI) [OSRI-06-10-04]; Office of Naval Research (ONR)
[N00014-08-1-0597]; National Aeronautics and Space Administration (NASA)
FX The authors wish to thank Peter Olsson for providing the RAMS outputs,
Xin Jin for his work on the freshwater discharge model, Hongchun Zhang
for her help with the model runs and Carl Schoch for his support and his
dedication. The authors also greatly appreciated, during the course of
this work, discussions with Thomas Royer, Steve Okkonen, Claude
Belanger, Shelton Gay and Alexander Shchepetkin. The authors thank the
two anonymous reviewers for their constructive comments. This research
was supported by the Alaska Ocean Observing System (AOOS), the Oil Spill
Recovery Institute (OSRI) under the contract OSRI-06-10-04 and the
Office of Naval Research (ONR), Grant N00014-08-1-0597. The research was
carried out, in part, by the Jet Propulsion Laboratory (JPL), California
Institute of Technology, under contract with the National Aeronautics
and Space Administration (NASA). Computations were made at the National
Center for Supercomputing Applications (NCSA) and on computers provided
by the JPL Supercomputer Project and the NASA Advanced Supercomputing
Division at Ames Research Center.
NR 54
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U1 1
U2 13
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0278-4343
J9 CONT SHELF RES
JI Cont. Shelf Res.
PD JUL 15
PY 2013
VL 63
SU S
SI SI
BP S79
EP S89
DI 10.1016/j.csr.2012.05.002
PG 11
WC Oceanography
SC Oceanography
GA 202BP
UT WOS:000323188800008
ER
PT J
AU Farrara, JD
Chao, Y
Li, ZJ
Wang, XC
Jin, X
Zhang, HC
Li, P
Vu, Q
Olsson, PQ
Schoch, GC
Halverson, M
Moline, MA
Ohlmann, C
Johnson, M
McWilliams, JC
Colas, FA
AF Farrara, John D.
Chao, Yi
Li, Zhijin
Wang, Xiaochun
Jin, Xin
Zhang, Hongchun
Li, Peggy
Quoc Vu
Olsson, Peter Q.
Schoch, G. Carl
Halverson, Mark
Moline, Mark A.
Ohlmann, Carter
Johnson, Mark
McWilliams, James C.
Colas, Francois A.
TI A data-assimilative ocean forecasting system for the Prince William
sound and an evaluation of its performance during sound Predictions 2009
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
DE Ocean modeling; Data assimilation; Prince William Sound; Real-time ocean
forecasts
ID CIRCULATION MODEL; NORTHERN GULF; ALASKA; TIDES; IMPLEMENTATION;
CALIFORNIA; SURFACE; COAST; WATER
AB The development and implementation of a three-dimensional ocean modeling system for the Prince William Sound (PWS) is described. The system consists of a regional ocean model component (ROMS) forced by output from a regional atmospheric model component (the Weather Research and Forecasting Model, WRF). The ROMS ocean model component has a horizontal resolution of 1 km within PWS and utilizes a recently-developed multi-scale 3DVAR data assimilation methodology along with freshwater runoff from land obtained via real-time execution of a digital elevation model. During the Sound Predictions Field Experiment (July 19-August 3, 2009) the system was run in real-time to support operations and incorporated all available real-time streams of data. Nowcasts were produced every 6 h and a 48-h forecast was performed once a day. In addition, a sixteen-member ensemble of forecasts was executed on most days. All results were published at a web portal (http://ourocean.jpl.nasa.gov/PWS) in real time to support decision making.
The performance of the system during Sound Predictions 2009 is evaluated. The ROMS results are first compared with the assimilated data as a consistency check. RMS differences of about 0.7 degrees C were found between the ROMS temperatures and the observed vertical profiles of temperature that are assimilated. The ROMS salinities show greater discrepancies, tending to be too salty near the surface. The overall circulation patterns observed throughout the Sound are qualitatively reproduced, including the following evolution in time. During the first week of the experiment, the weather was quite stormy with strong southeasterly winds. This resulted in strong north to northwestward surface flow in much of the central PWS. Both the observed drifter trajectories and the ROMS nowcasts showed strong surface inflow into the Sound through the Hinchinbrook Entrance and strong generally northward to northwestward flow in the central Sound that was exiting through the Knight Island Passage and Montague Strait entrance. During the latter part of the second week when surface winds were light and southwesterly, the mean surface flow at the Hinchinbrook Entrance reversed to weak outflow and a cyclonic eddy formed in the central Sound. Overall, RMS differences between ROMS surface currents and observed HF radar surface currents in the central Sound were generally between 5 and 10 cm/s, about 20-40% of the time mean current speeds.
The ROMS reanalysis is then validated against independent observations. A comparison of the ROMS currents with observed vertical current profiles from moored ADCPs in the Hinchinbrook Entrance and Montague Strait shows good qualitative agreement and confirms the evolution of the near surface inflow/outflow at these locations described above. A comparison of the ROMS surface currents with drifter trajectories provided additional confirmation that the evolution of the surface flow described above was realistic. Forecasts of drifter locations had RMS errors of less than 10 km for up to 36 h. One and two-day forecasts of surface temperature, salinity and current fields were more skillful than persistence forecasts. In addition, ensemble mean forecasts were found to be slightly more skillful than single forecasts. Two case studies demonstrated the system's qualitative skill in predicting subsurface changes within the mixed layer measured by ships and autonomous underwater vehicles. In summary, the system is capable of producing a realistic evolution of the near-surface circulation within PWS including forecasts of up to two days of this evolution. Use of the products provided by the system during the experiment as part of the asset deployment decision making process demonstrated the value of accurate regional ocean forecasts in support of field experiments. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Farrara, John D.; Chao, Yi; Li, Zhijin; Wang, Xiaochun; Jin, Xin; Zhang, Hongchun] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Li, Zhijin; Li, Peggy; Quoc Vu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Olsson, Peter Q.] Univ Alaska Anchorage, Alaska Expt Forecast Facil, Anchorage, AK 99501 USA.
[Olsson, Peter Q.] Univ Alaska Anchorage, Alaska State Climate Ctr, Environm & Nat Resources Inst, Anchorage, AK 99508 USA.
[Olsson, Peter Q.] Alaska Ocean Observing Syst, Anchorage, AK 99501 USA.
[Schoch, G. Carl] Coastwise Serv, Homer, AK 99603 USA.
[Halverson, Mark] Prince William Sound Sci Ctr, Cordova, AK 99574 USA.
[Moline, Mark A.] Univ Delaware, Sch Marine Sci & Policy, Lewes, DE 19958 USA.
[Ohlmann, Carter] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Chao, Yi; Johnson, Mark] Univ Alaska, Inst Marine Sci, Fairbanks, AK 99775 USA.
[Chao, Yi; McWilliams, James C.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Colas, Francois A.] Remote Sensing Solut Inc, Pasadena, CA 91107 USA.
RP Farrara, JD (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
EM jfarrara@jpl.nasa.gov
RI Colas, Francois/B-4920-2012
OI Colas, Francois/0000-0002-5859-6586
FU National Aeronautics and Space Administration; Alaska Ocean Observing
System (AOOS)/Prince William Sound Science Center [09-25-03:1];
NASA/University of Washington [313081]; Bureau of Ocean Energy
Management; Oil Spill Recovery Institute (OSRI); Exxon Valdez Oil Spill
Trustee Council
FX The research was carried out, in part, by the Jet Propulsion Laboratory
(JPL), California Institute of Technology, under contract with the
National Aeronautics and Space Administration. We are grateful to Dr.
Jia Wang for sharing his hydrological model codes and Dr. Sharan
Majumdar, RSMAS for his assistance in developing the ensemble
forecasting methodology used here. Support from the Alaska Ocean
Observing System (AOOS)/Prince William Sound Science Center under Award
number 09-25-03:1 and the assistance of Dr. W. Scott Pegau of PWSSC.
Support from NASA/University of Washington under Award number 313081 is
also gratefully acknowledged. The HF radar was provided by the
University of Alaska HF Radar group led by Dr. Tom Weingartner with
support from the Bureau of Ocean Energy Management (then Minerals
Management Service). We are grateful for the expertise of Hank
Statscewich and Rachel Potter at the University of Alaska Fairbanks for
on-site logistics and data collection that made this portion possible.
Funding for the subsurface moorings in the Hinchinbrook Entrance and
Montague Strait from the Oil Spill Recovery Institute (OSRI) is
gratefully acknowledged. The subsurface moorings in Hinchinbrook
Entrance and Montague Strait were funded by a grant to the Prince
William Sound Science Center PWSSC from the Exxon Valdez Oil Spill
Trustee Council. We are grateful to Eoin Howlett (ASA) and Art Allen for
providing the U. S. Coast Guard drifter dataset and Ian Robbins (Calpoly
SLO) for the REMUS and glider deployments and datasets. The
computational resources required to perform the ensemble forecasts were
provided by the JPL Supercomputing Project. We wish to especially thank
Molly McCammon of AOOS for her continuous support throughout the
project.
NR 38
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0278-4343
J9 CONT SHELF RES
JI Cont. Shelf Res.
PD JUL 15
PY 2013
VL 63
SU S
SI SI
BP S193
EP S208
DI 10.1016/j.csr.2012.11.008
PG 16
WC Oceanography
SC Oceanography
GA 202BP
UT WOS:000323188800016
ER
PT J
AU Li, ZJ
Chao, Y
Farrara, JD
McWilliams, JC
AF Li, Zhijin
Chao, Yi
Farrara, John D.
McWilliams, James C.
TI Impacts of distinct observations during the 2009 Prince William Sound
field experiment: A data assimilation study
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
DE Variational data assimilation; Observing system experiment; Field
experiment; Coastal ocean; Prince William Sound
ID OCEAN MODELING SYSTEM; PART I; ALASKA; CIRCULATION; SURFACE; SCHEME;
BIAS; ROMS
AB A set of data assimilation experiments, known as Observing System Experiments (OSEs) are performed to assess the relative impacts of different types of observations acquired during the 2009 Prince William Sound Field Experiment. The observations assimilated consist primarily of two types: High Frequency (HF) radar surface velocities and vertical profiles of temperature/salinity (T/S) measured by ships, moorings, an Autonomous Underwater Vehicle and a glider. The impact of all the observations, HF radar surface velocities, and T/S profiles is assessed. Without data assimilation, a frequently occurring cyclonic eddy in the central Sound is overly persistent and intense. The assimilation of the HF radar velocities effectively reduces these biases and improves the representation of the velocities as well as the T/S fields in the Sound. The assimilation of the T/S profiles improves the large scale representation of the temperature/salinity and also the velocity field in the central Sound. The combination of the HF radar surface velocities and sparse T/S profiles results in an observing system capable of representing the circulation in the Sound reliably and thus producing analyses and forecasts with useful skill. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Li, Zhijin; Chao, Yi; Farrara, John D.; McWilliams, James C.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Chao, Yi; McWilliams, James C.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Chao, Yi] Remote Sensing Solut Inc, Pasadena, CA USA.
RP Li, ZJ (reprint author), CALTECH, Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM zhijin.li@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); Alaska Ocean
Observing System (AOOS)/Prince William Sound Science Center [09-25-03:1]
FX The research described in this publication was carried out, in part, at
the Jet Propulsion Laboratory (JPL), California Institute of Technology,
under a contract with the National Aeronautics and Space Administration
(NASA). Support was provided by the Alaska Ocean Observing System
(AOOS)/Prince William Sound Science Center under Award number
09-25-03:1. We thank Molly McCammon and G. Carl Schoch of AOOS for their
continuous support throughout the project. Contributions from Peggy Li,
Quoc Vu at JPL, and Hongchun Zhang, Xiaochun Wang, Xin Jin, and Francois
A. Colas at University of California, Los Angeles, in data processing
and system testing are gratefully acknowledged. Computations were
performed on the SGI Altix computer through the JPL Supercomputing
Project. The authors thank an anonymous reviewer for comments, which
were helpful in improving the manuscript.
NR 36
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0278-4343
J9 CONT SHELF RES
JI Cont. Shelf Res.
PD JUL 15
PY 2013
VL 63
SU S
SI SI
BP S209
EP S222
DI 10.1016/j.csr.2012.06.018
PG 14
WC Oceanography
SC Oceanography
GA 202BP
UT WOS:000323188800017
ER
PT J
AU Wang, XC
Chao, Y
Thompson, DR
Chien, SA
Farrara, J
Li, P
Vu, Q
Zhang, HC
Levin, JC
Gangopadhyay, A
AF Wang, Xiaochun
Chao, Yi
Thompson, David R.
Chien, Steve A.
Farrara, John
Li, Peggy
Quoc Vu
Zhang, Hongchun
Levin, Julia C.
Gangopadhyay, Avijit
TI Multi-model ensemble forecasting and glider path planning in the
Mid-Atlantic Bight
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
DE Mid-Atlantic Bight; Ensemble forecasting; Objective weighting method;
Equal weighting method; Glider path planning
ID CIRCULATION MODELING SYSTEM; MAINE/GEORGES BANK REGION; DATA
ASSIMILATION; PART I; OCEAN; PREDICTION; FORMULATION; SURFACE; SHELF;
GULF
AB During the first two weeks of November 2009, a field experiment was conducted in the Mid-Atlantic Bight region to demonstrate a coastal ocean observatory that can collect observations from heterogeneous platforms and forecast fields from four different ocean models, provide multi-model ensemble forecasts based on either an equal weighting (EQ) or objective weighting (OBJ) method, and use model forecasts in a path planning system to relocate autonomous gliders. This experiment is a prototype for the command and control component of cyberinfrastructure of the Ocean Observatories Initiative funded by the National Science Foundation. The four individual models use different forcing fields, boundary conditions and data assimilation techniques, and have resolutions varying from 2 km to 15 km. Our results indicate that for sea surface temperature and surface currents, the OBJ ensemble outperforms the four individual models, while the EQ ensemble can also provide an effective way to improve individual model forecasts. In terms of glider path planning, the OBJ ensemble has a performance similar to the best individual model, which has the finest horizontal resolution. This field experiment demonstrates the first-ever use of ensemble current forecasts to guide glider path planning in the context of real-time data collection and ocean model forecasting. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Wang, Xiaochun; Chao, Yi; Farrara, John; Zhang, Hongchun] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Wang, Xiaochun; Thompson, David R.; Chien, Steve A.; Li, Peggy; Quoc Vu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chao, Yi] Remote Sensing Solut Inc, Pasadena, CA 91107 USA.
[Levin, Julia C.] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08901 USA.
[Gangopadhyay, Avijit] Univ Massachusetts Dartmouth, Sch Marine Sci & Technol, New Bedford, MA 02744 USA.
RP Wang, XC (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, 9258 Boelter Hall,Box 957288, Los Angeles, CA 90095 USA.
EM xcwang@jifresse.ucla.edu
FU National Aeronautics and Space Administration
FX The research was carried out, in part, by the Jet Propulsion Laboratory
(JPL), California Institute of Technology, under contract with the
National Aeronautics and Space Administration. The insightful comments
on an early draft of the paper from Drs. Alan Blumberg, Richard Signell,
and John Warner are appreciated. We would like to thank the four
modeling groups from Woods Hole Science Center, USGS (COAWST), Institute
of Marine and Coastal Sciences, Rutgers University (ESPRESSO), Center
for Maritime Systems, Stevens Institute of Technology (NYHOPS), and
School of Marine Science and Technology, University of Massachusetts
Dartmouth (SMAST-HOPS) for providing their forecasts to the JPL web
portal. The participating glider teams were the Rutgers Coastal Ocean
Observation Lab (Drs. Oscar Schofield and Scott Glenn) and the
University of Delaware (Dr. Matthew Oliver). The Rutgers team also
provided the glider position and observation to the web portal. The
detailed and insightful comments from two anonymous reviewers and the
editor helped us to restructure the paper.
NR 43
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U2 14
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0278-4343
J9 CONT SHELF RES
JI Cont. Shelf Res.
PD JUL 15
PY 2013
VL 63
SU S
SI SI
BP S223
EP S234
DI 10.1016/j.csr.2012.07.006
PG 12
WC Oceanography
SC Oceanography
GA 202BP
UT WOS:000323188800018
ER
PT J
AU Wang, XC
Chao, Y
Zhang, HC
Farrara, J
Li, ZJ
Jin, X
Park, K
Colas, F
McWilliams, JC
Paternostro, C
Shum, CK
Yi, YC
Schoch, C
Olsson, P
AF Wang, Xiaochun
Chao, Yi
Zhang, Hongchun
Farrara, John
Li, Zhijin
Jin, Xin
Park, Kyungeen
Colas, Francois
McWilliams, James C.
Paternostro, Chris
Shum, C. K.
Yi, Yuchan
Schoch, Carl
Olsson, Peter
TI Modeling tides and their influence on the circulation in Prince William
Sound, Alaska
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
DE Prince William Sound; Tides; Cyclonic gyre
ID COASTAL OCEAN MODEL; CENTRAL CALIFORNIA; BOUNDARY-CONDITION; SYSTEM;
IMPLEMENTATION; FLOW; VARIABILITY; FORMULATION; SIMULATION; CURRENTS
AB In the process of developing a real-time data-assimilating coastal ocean forecasting system for Prince William Sound, Alaska, tidal signal was added to a three-domain nested model for the region. The model, which is configured from the Regional Ocean Modeling System (ROMS), has 40 levels in the vertical direction and horizontal resolutions of 10.6 km, 3.6 km and 1.2 km for its three nested domains, respectively. In the present research, the ROMS tidal solution was validated using data from coastal tide gauges, satellite altimeters, high-frequency coastal radars, and Acoustic Doppler Current Profiler (ADCP) current surveys. The error of barotropic tides, as measured by the total root mean square discrepancy of eight major tidal constituents is 5.3 cm, or 5.6% of the tidal sea surface height variability in the open ocean. Along the coastal region, the total discrepancy is 9.6 cm, or 8.2% of the tidal sea surface height variability. Model tidal currents agree reasonably well with the observations. The influence of tides on the circulation was also investigated using numerical experiments. Besides tides, other types of forcing fields (heat flux, wind stress, evaporation minus precipitation, and freshwater discharge) were also included in the model. Our results indicate that tides play a significant role in shaping the mean circulation of the region. For the summer months, the tidal residual circulation tends to generate a cyclonic gyre in the central Sound. The net transport into the Sound through Hinchinbrook Entrance is reduced. Tides also increase the mixed layer depth in the Sound, especially during the winter months. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Wang, Xiaochun; Chao, Yi; Zhang, Hongchun; Farrara, John; Li, Zhijin; Jin, Xin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Chao, Yi] Remote Sensing Solut Inc, Pasadena, CA 91107 USA.
[Li, Zhijin; Park, Kyungeen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Colas, Francois; McWilliams, James C.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Paternostro, Chris] NOAA, Ctr Operat Oceanog Prod & Serv, NOS, Silver Spring, MD 20910 USA.
[Shum, C. K.; Yi, Yuchan] Ohio State Univ, Columbus, OH 43210 USA.
[Schoch, Carl] Alaska Ocean Observing Syst, Anchorage, AK 99501 USA.
[Olsson, Peter] Univ Alaska Anchorage, Alaska Expt Forecast Facil, Anchorage, AK 99501 USA.
RP Wang, XC (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, 607 Charles E Young Dr East,Young Hall,Room 4242, Los Angeles, CA 90095 USA.
EM xcwang@jifresse.ucla.edu
RI Colas, Francois/B-4920-2012
OI Colas, Francois/0000-0002-5859-6586
FU Alaska Ocean Observing System (AOOS); NASA's Physical Oceanography
Program under the Ocean Topography Science Team; PWSSC Project
[10-10-09]; National Aeronautics and Space Administration (NASA)
FX The research was carried out, in part, by the Jet Propulsion Laboratory
(JPL), California Institute of Technology, under contract with the
National Aeronautics and Space Administration (NASA). The financial
support was provided by the Alaska Ocean Observing System (AOOS). Dr.
Jia Wang generously shared his code of the hydrological digital
elevation model, which was modified and used in the present research.
The IT support to the ROMS group at JPL was provided by Drs. Peggy Li
and Quoc Vu. The Ohio State University research is supported by NASA's
Physical Oceanography Program under the Ocean Topography Science Team.
The long-term support from Drs. Emily Greene and Michael Lampel at the
Pasadena office of Raytheon is acknowledged. Computations were performed
on computers provided by the JPL Supercomputer Project and the NASA
Advanced Supercomputing Division at Ames Research Center. Wang would
like to acknowledge the support from PWSSC Project 10-10-09 and the
support from Profs. Guoxiong Wu and Yimin Liu from Institute of
Atmospheric Physics, Chinese Academy of Sciences during the summer of
2012. The comments from anonymous reviewers and the editor helped us
greatly during the revision process.
NR 54
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U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0278-4343
J9 CONT SHELF RES
JI Cont. Shelf Res.
PD JUL 15
PY 2013
VL 63
SU S
SI SI
BP S126
EP S137
DI 10.1016/j.csr.2012.08.016
PG 12
WC Oceanography
SC Oceanography
GA 202BP
UT WOS:000323188800011
ER
PT J
AU Grudinin, IS
Lin, GP
Yu, N
AF Grudinin, Ivan S.
Lin, Guoping
Yu, Nan
TI Polarization conversion loss in birefringent crystalline resonators
SO OPTICS LETTERS
LA English
DT Article
ID WHISPERING-GALLERY MODES
AB Whispering gallery modes in birefringent crystalline resonators are investigated. We experimentally investigate the XY-cut resonators made with LiNbO3, LiTaO3, and BBO and observe strong influence of the resonator's shape and birefringence on the quality factor of the extraordinary polarized modes. We show that extraordinary modes can have lower Q and even be suppressed owing to polarization conversion loss. The ordinary ray modes retain the high Q due to inhibited reflection phenomenon. (C) 2013 Optical Society of America
C1 [Grudinin, Ivan S.; Lin, Guoping; 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
RI Lin, Guoping/I-3381-2015
OI Lin, Guoping/0000-0003-4007-1850
FU NASA Center Innovation Fund; JPL Research and Technology Development
Program; National Aeronautics and Space Administration
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 support from NASA Center Innovation Fund
and JPL Research and Technology Development Program.
NR 11
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U1 1
U2 13
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 JUL 15
PY 2013
VL 38
IS 14
BP 2410
EP 2412
DI 10.1364/OL.38.002410
PG 3
WC Optics
SC Optics
GA 182UT
UT WOS:000321770900013
PM 23939064
ER
PT J
AU Liewer, K
Martin, S
Serabyn, E
AF Liewer, K.
Martin, S.
Serabyn, E.
TI Demonstration of coherent imaging through a phased array of single-mode
optical fibers
SO OPTICS LETTERS
LA English
DT Article
ID HIGH-CONTRAST; TELESCOPE
AB We demonstrate coherent imaging through a phased array of single-mode optical fibers. Specifically, we show that two laboratory point sources located within the individual-fiber single-mode acceptance angle can be resolved. Such techniques could eventually enable direct imaging with arrays of small collecting telescopes. (c) 2013 Optical Society of America
C1 [Liewer, K.; Martin, S.; Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Liewer, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kurt.liewer@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration.
NR 6
TC 0
Z9 0
U1 0
U2 2
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 JUL 15
PY 2013
VL 38
IS 14
BP 2452
EP 2454
DI 10.1364/OL.38.002452
PG 3
WC Optics
SC Optics
GA 182UT
UT WOS:000321770900027
PM 23939078
ER
PT J
AU Collier, MR
Farrell, WM
Stubbs, TJ
AF Collier, Michael R.
Farrell, William M.
Stubbs, Timothy J.
TI The lunar dust pendulum
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Lunar dust; Electrostatic transport; Lunar surface potential
ID PHOTOELECTRON SHEATH; TRANSPORT; SURFACE; GRAINS; LEVITATION; MOTION;
SPACE; EROS
AB An analytic model for the motion of a positively charged lunar dust grain in the presence of a shadowed crater at a negative potential in vacuum is presented. It is shown that the dust grain executes oscillatory trajectories, and an expression is derived for the period of oscillation. Simulations used to verify the analytic expression also show that because the trajectories are unstable, dust grains are either ejected from the crater's vicinity or deposited into the crater forming "dust ponds." The model also applies to other airless bodies in the solar system, such as asteroids, and predicts that under certain conditions, particularly near lunar sunset, oscillating dust "canopies" or "swarms" will form over negatively charged craters. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Collier, Michael R.; Farrell, William M.; Stubbs, Timothy J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stubbs, Timothy J.] Univ Maryland, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA.
[Farrell, William M.; Stubbs, Timothy J.] NASA, Ames Res Ctr, NASAs Lunar Sci Inst, Moffett Field, CA 94035 USA.
RP Collier, MR (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA.
EM michael.r.collier@nasa.gov; william.m.farrell@nasa.gov;
timothy.j.stubbs@nasa.gov
RI Collier, Michael/I-4864-2013; Stubbs, Timothy/I-5139-2013; Farrell,
William/I-4865-2013
OI Collier, Michael/0000-0001-9658-6605; Stubbs,
Timothy/0000-0002-5524-645X;
FU Dynamic Response of the Environment At the Moon (DREAM) NASA Lunar
Science Institute; NASA [NNX08AN76G (LROPS)]; NASA LASER
[132438.01.15.01.06]; Exploration Systems Mission Directorate/Advanced
Capabilities Division
FX This work was supported through the Dynamic Response of the Environment
At the Moon (DREAM) NASA Lunar Science Institute team and NASA Grant
NNX08AN76G (LROPS) as well as by NASA LASER 132438.01.15.01.06 issued
through the Science Mission Directorate/Planetary Science Division and
Exploration Systems Mission Directorate/Advanced Capabilities Division.
Special thanks to Greg Delory for pointing out relevant references and
to Dennis Chornay and John Keller for helpful discussions.
NR 42
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U2 12
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 JUL 15
PY 2013
VL 52
IS 2
BP 251
EP 261
DI 10.1016/j.asr.2012.09.044
PG 11
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 174LQ
UT WOS:000321157400003
ER
PT J
AU Araki, H
Noda, H
Tazawa, S
Ishihara, Y
Goossens, S
Sasaki, S
AF Araki, Hiroshi
Noda, Hirotomo
Tazawa, Seiichi
Ishihara, Yoshiaki
Goossens, Sander
Sasaki, Sho
TI Lunar laser topography by LALT on board the KAGUYA lunar explorer -
Operational history, new topographic data, peak height analysis of laser
echo pulses
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE KAGUYA; LALT; Laser; Lunar topography; Operational history; Peak height
ID ALTIMETER; SELENE
AB In this paper we review the lunar laser ranging conducted by the laser altimeter (LALT) on board the KAGUYA lunar explorer (2007-2009). Five aspects of LALT measurements are described: (1) General operational history, (2) Laser shot and data statistics, (3) Revisions to LALT topographic data, (4) Variations in laser output energy, and (5) Peak height analysis of laser echo pulses. LALT was able to range to the lunar surface despite some troubles with respect to laser output energy in the middle of the KAGUYA mission. The time series topographic data set was revised (Ver. 2) by incorporating new lunar gravity model based on KAGUYA and other historical lunar satellite's orbit data, along with other improvements, for example by incorporating the accurate position of the laser collimator on board the KAGUYA; however, more than half of the acquired range data could not be converted properly due to problems with orbit accuracy during the extended phase of the mission. The spherical harmonic coefficients and the basic lunar figure parameters derived from LALT_LGT_TS agree very well with LRO-LOLA and the Chang'E-1 LAM model. It is possible that partial failure to the laser diode was responsible for the gradual degradation of laser power (0.835 mJ per million shots) and the rapid decrease that occurred over April 9-14, 2008. The laser power also proved to be extremely sensitive to the temperature of the laser oscillator. The peak height ratio that is peak height telemetry data divided by calculated ratio - is about 19% on average using the mean slope and albedo data from LALT and Spectral Profiler on KAGUYA space craft, respectively, which suggests the performance of peak height measurement is more than 1/5 for more than 70 km altitude, if compared with calculated one. The peak height ratio may be better if we take the effect of small scale topography within a footprint into account. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Araki, Hiroshi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Noda, Hirotomo; Sasaki, Sho] Natl Astron Observ Japan, Ohshu, Iwate 0230861, Japan.
[Tazawa, Seiichi] Natl Astron Observ Japan, Hilo, HI 96720 USA.
[Ishihara, Yoshiaki] Natl Inst Adv Ind Sci & Technol, Tsukuba, Ibaraki 3058568, Japan.
[Goossens, Sander] NASA, Goddard Space Flight Ctr, CRESST Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Araki, H (reprint author), Natl Astron Observ Japan, 2-21-1 Mitaka, Mitaka, Tokyo 1818588, Japan.
EM araki.hiroshi@nao.ac.jp; hirotomo.noda@nao.ac.jp;
tazawa.seiichi@nao.ac.jp; ishihara.yoshiaki@aist.go.jp;
sander.j.goossens@nasa.gov; sasaki.sho@nao.ac.jp
RI Goossens, Sander/K-2526-2015;
OI Goossens, Sander/0000-0002-7707-1128; Ishihara,
Yoshiaki/0000-0002-0375-6300
NR 16
TC 2
Z9 2
U1 0
U2 9
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD JUL 15
PY 2013
VL 52
IS 2
BP 262
EP 271
DI 10.1016/j.asr.2013.02.018
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 174LQ
UT WOS:000321157400004
ER
PT J
AU Burns, JO
Kring, DA
Hopkins, JB
Norris, S
Lazio, TJW
Kasper, J
AF Burns, Jack O.
Kring, David A.
Hopkins, Joshua B.
Norris, Scott
Lazio, T. Joseph W.
Kasper, Justin
TI A lunar L2-Farside exploration and science mission concept with the
Orion Multi-Purpose Crew Vehicle and a teleoperated lander/rover
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Human cis-lunar missions; Moon; Planets and satellites: formation,
Surfaces; Radio astronomy; Space vehicles: instruments; Telerobotics
ID POLE-AITKEN BASIN; SCHRODINGER-BASIN; ATMOSPHERE; UNIVERSE; SURFACE;
SCALE
AB A novel concept is presented in this paper for a human mission to the lunar L2 (Lagrange) point that would be a proving ground for future exploration missions to deep space while also overseeing scientifically important investigations. In an L2 halo orbit above the lunar farside, the astronauts aboard the Orion Crew Vehicle would travel 15% farther from Earth than did the Apollo astronauts and spend almost three times longer in deep space. Such a mission would serve as a first step beyond low Earth orbit and prove out operational spaceflight capabilities such as life support, communication, high speed re-entry, and radiation protection prior to more difficult human exploration missions. On this proposed mission, the crew would teleoperate landers/rovers on the unexplored lunar farside, which would obtain samples from the geologically interesting farside and deploy a low radio frequency telescope. Sampling the South Pole-Aitken basin, one of the oldest impact basins in the solar system, is a key science objective of the 2011 Planetary Science Decadal Survey. Observations at low radio frequencies to track the effects of the Universe's first stars/galaxies on the intergalactic medium are a priority of the 2010 Astronomy and Astrophysics Decadal Survey. Such telerobotic oversight would also demonstrate capability for human and robotic cooperation on future, more complex deep space missions such as exploring Mars. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Burns, Jack O.] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Burns, Jack O.; Kring, David A.; Lazio, T. Joseph W.; Kasper, Justin] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94089 USA.
[Kring, David A.] USRA Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA.
[Hopkins, Joshua B.; Norris, Scott] CO TSB, Lockheed Martin Space Syst, Denver, CO 80127 USA.
[Lazio, T. Joseph W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kasper, Justin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Burns, JO (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, 593 UCB, Boulder, CO 80309 USA.
EM jack.burns@colorado.edu
RI Kasper, Justin/D-1152-2010
OI Kasper, Justin/0000-0002-7077-930X
FU Lunar University Network for Astrophysics Research; NASA Lunar Science
Institute [NNA09DB30A, NNA09DB33A]; NASA
FX The development of this mission concept was supported by the Lunar
University Network for Astrophysics Research
(http://lunar.colorado.edu), headquartered at the University of Colorado
Boulder, and the LPI-JSC Center for Lunar Science and Exploration in
Houston (http://www.lpi.usra.edu/nlsi/), both funded by the NASA Lunar
Science Institute (NASA Cooperative Agreements NNA09DB30A and
NNA09DB33A, respectively). Part of this research was conducted at the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA. We thank Y. Takahashi for the use of his
electromagnetic propagation code to study diffraction effects at
locations on the lunar farside and A. Datta for porting/running the code
at U. Colorado. We also thank Mattie Toll for her editorial assistance
and Terry Fong for insightful discussions on telerobotics In addition,
we are grateful to Dan Lester for helpful comments on an earlier draft
of this paper.
NR 46
TC 17
Z9 18
U1 0
U2 24
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 JUL 15
PY 2013
VL 52
IS 2
BP 306
EP 320
DI 10.1016/j.asr.2012.11.016
PG 15
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 174LQ
UT WOS:000321157400007
ER
PT J
AU Burlaga, LF
Ness, NF
Stone, EC
AF Burlaga, L. F.
Ness, N. F.
Stone, E. C.
TI Magnetic Field Observations as Voyager 1 Entered the Heliosheath
Depletion Region
SO SCIENCE
LA English
DT Article
ID TERMINATION SHOCK; HELIOSPHERE; VELOCITY; PLASMA; SYSTEM; FLOW; AU
AB Magnetic fields measured by Voyager 1 (V1) show that the spacecraft crossed the boundary of an unexpected region five times between days 210 and similar to 238 in 2012. The magnetic field strength B increased across this boundary from approximate to 0.2 to approximate to 0.4 nanotesla, and B remained near 0.4 nanotesla until at least day 270, 2012. The strong magnetic fields were associated with unusually low counting rates of >0.5 mega-electron volt per nuclear particle. The direction of B did not change significantly across any of the five boundary crossings; it was very uniform and very close to the spiral magnetic field direction, which was observed throughout the heliosheath. The observations indicate that V1 entered a region of the heliosheath (the heliosheath depletion region), rather than the interstellar medium.
C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ness, N. F.] Catholic Univ Amer, Washington, DC 20064 USA.
[Stone, E. C.] CALTECH, Pasadena, CA 91125 USA.
RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM lburlagahsp@verizon.net
FU NASA [NNX12AC63G, NNG11PN48P]
FX T. McClanahan and S. Kramer provided support in the processing of the
data and D. Berdichevsky computed correction tables for the three
sensors on each of the two magnetometers. N.F.N. was partially supported
by NASA grant NNX12AC63G to the Catholic University of America. L. F. B.
was supported by NASA contract NNG11PN48P. The data are available at
NASA's Virtual Heliospheric Observatory (http://vho.nasa.gov/),
maintained within the Heliospheric Physics Laboratory at NASA's Goddard
Space Flight Center.
NR 27
TC 64
Z9 64
U1 1
U2 16
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 JUL 12
PY 2013
VL 341
IS 6142
BP 147
EP 150
DI 10.1126/science.1235451
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 185KA
UT WOS:000321965300035
PM 23811226
ER
PT J
AU Stone, EC
Cummings, AC
McDonald, FB
Heikkila, BC
Lal, N
Webber, WR
AF Stone, E. C.
Cummings, A. C.
McDonald, F. B.
Heikkila, B. C.
Lal, N.
Webber, W. R.
TI Voyager 1 Observes Low-Energy Galactic Cosmic Rays in a Region Depleted
of Heliospheric Ions
SO SCIENCE
LA English
DT Article
ID HELIOPAUSE; SPECTRUM; MODULATION
AB On 25 August 2012, Voyager 1 was at 122 astronomical units when the steady intensity of low-energy ions it had observed for the previous 6 years suddenly dropped for a third time and soon completely disappeared as the ions streamed away into interstellar space. Although the magnetic field observations indicate that Voyager 1 remained inside the heliosphere, the intensity of cosmic ray nuclei from outside the heliosphere abruptly increased. We report the spectra of galactic cosmic rays down to similar to 3 x 10(6) electron volts per nucleon, revealing H and He energy spectra with broad peaks from 10 x 10(6) to 40 x 10(6) electron volts per nucleon and an increasing galactic cosmic-ray electron intensity down to similar to 10 x 10(6) electron volts.
C1 [Stone, E. C.; Cummings, A. C.] CALTECH, Pasadena, CA 91125 USA.
[McDonald, F. B.] Univ Maryland, College Pk, MD 20742 USA.
[Heikkila, B. C.; Lal, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Webber, W. R.] New Mexico State Univ, Las Cruces, NM 88003 USA.
RP Stone, EC (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM ecs@srl.caltech.edu
FU NASA [NNN12A012]
FX This work was supported by NASA (NNN12A012). This paper is dedicated to
the memory of Frank McDonald, whose leadership in the cosmic-ray
investigation on Voyager began in 1972. His contributions continued
until the day of his passing, just after Voyager 1 durably entered the
depletion region and fulfilled his vision of observing low-energy
galactic cosmic rays from the local interstellar medium. This paper
benefited substantially from discussions during meetings of the
International Team on the Physics of the Heliopause at the International
Space Science Institute in Bern, Switzerland.
NR 21
TC 127
Z9 128
U1 1
U2 10
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 JUL 12
PY 2013
VL 341
IS 6142
BP 150
EP 153
DI 10.1126/science.1236408
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 185KA
UT WOS:000321965300036
PM 23811227
ER
PT J
AU Lyra, W
Kuchner, M
AF Lyra, W.
Kuchner, M.
TI Formation of sharp eccentric rings in debris disks with gas but without
planets
SO NATURE
LA English
DT Article
ID PICTORIS CIRCUMSTELLAR DISK; BETA-PICTORIS; FOMALHAUT B; DUST;
TURBULENCE; SIMULATIONS; INSTABILITY; MORPHOLOGY; ORIGIN; SYSTEM
AB 'Debris disks' around young stars (analogues of the Kuiper Belt in our Solar System) show a variety of non-trivial structures attributed to planetary perturbations and used to constrain the properties of those planets(1-3). However, these analyses have largely ignored the fact that some debris disks are found to contain small quantities of gas(4-9), a component that all such disks should contain at some level(10,11). Several debris disks have been measured with a dust-to-gas ratio of about unity(4-9), at which the effect of hydrodynamics on the structure of the disk cannot be ignored(12,13). Here we report linear and nonlinear modelling that shows that dust-gas interactions can produce some of the key patterns attributed to planets. We find a robust clumping instability that organizes the dust into narrow, eccentric rings, similar to the Fomalhaut debris disk(14). The conclusion that such disks might contain planets is not necessarily required to explain these systems.
C1 [Lyra, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lyra, W.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Lyra, W.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
[Kuchner, M.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 21230 USA.
RP Lyra, W (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM wlyra@caltech.edu; marc.j.kuchner@nasa.gov
FU National Science Foundation [AST10-09802]; National Aeronautics and
Space Administration; National Science Foundation; NASA Astrobiology
Institute through the Goddard Center for Astrobiology
FX We thank H. Latter and G. Stewart for discussions. The writing of this
paper started at the American Museum of Natural History, with financial
support by the National Science Foundation under grant no. AST10-09802,
and was completed at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration. This research was supported by an allocation of advanced
computing resources supported by the National Science Foundation. The
computations were performed on the Kraken system at the National
Institute for Computational Sciences. W. L. is a Carl Sagan fellow. M.
K. is supported in part by the NASA Astrobiology Institute through the
Goddard Center for Astrobiology.
NR 30
TC 37
Z9 37
U1 0
U2 8
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUL 11
PY 2013
VL 499
IS 7457
BP 184
EP 187
DI 10.1038/nature12281
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 179YA
UT WOS:000321557600056
PM 23846656
ER
PT J
AU Magnotti, G
Cutler, AD
Danehy, PM
AF Magnotti, Gaetano
Cutler, Andrew D.
Danehy, Paul M.
TI Development of a dual-pump coherent anti-Stokes Raman spectroscopy
system for measurements in supersonic combustion
SO APPLIED OPTICS
LA English
DT Article
ID NONRESONANT 3RD-ORDER SUSCEPTIBILITIES; FLAT-FLAME BURNER; CARS
TEMPERATURE-MEASUREMENTS; SCATTERING MEASUREMENTS; HIGH-RESOLUTION;
THERMOMETRY; GASES; PRECISION; N2; CALIBRATION
AB This work describes the development of a dual-pump coherent anti-Stokes Raman spectroscopy system for simultaneous measurements of the temperature and the absolute mole fraction of N-2, O-2, and H-2 in supersonic combusting flows. Changes to the experimental setup and the data analysis to improve the quality of the measurements in this turbulent, high-temperature reacting flow are described. The accuracy and precision of the instrument have been determined using data collected in a Hencken burner flame. For temperatures above 800 K, errors in the absolute mole fraction are within 1.5%, 0.5%, and 1% of the total composition for N-2, O-2, and H-2, respectively. Standard deviations based on 500 single shots are between 10 and 65 K for the temperature, between 0.5% and 1.7% of the total composition for O-2, and between 1.5% and 3.4% for N-2. The standard deviation of H-2 is similar to 10% of the average measured mole fraction. (C) 2013 Optical Society of America
C1 [Magnotti, Gaetano] Sandia Natl Labs, Combust Res Facil, Livermore, CA 94550 USA.
[Cutler, Andrew D.] George Washington Univ, MAE Dept, Newport News, VA 23602 USA.
[Danehy, Paul M.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurements Branch, Hampton, VA 23681 USA.
RP Magnotti, G (reprint author), Sandia Natl Labs, Combust Res Facil, 7011 East Ave, Livermore, CA 94550 USA.
EM gaetanomagnotti@gmail.com
OI Magnotti, Gaetano/0000-0002-1723-5258
FU NASA Fundamental Aeronautics Program, Hypersonics Project; NASA AFOSR
[FA 9550-09-1-0611]
FX This work was supported by the NASA Fundamental Aeronautics Program,
Hypersonics Project, and the NASA AFOSR-sponsored National Center for
Hypersonic Combined Cycle Propulsion (grant no. FA 9550-09-1-0611 with
technical monitors Chiping Li, AFOSR, and Aaron Auslender and Rick
Gaffney, NASA). The authors would like to thank Lloyd G. Wilson and
Sarah A. Tedder for assistance in performing these experiments.
NR 48
TC 4
Z9 4
U1 1
U2 33
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
J9 APPL OPTICS
JI Appl. Optics
PD JUL 10
PY 2013
VL 52
IS 20
BP 4779
EP 4791
DI 10.1364/AO.52.004779
PG 13
WC Optics
SC Optics
GA 180TH
UT WOS:000321619500002
PM 23852189
ER
PT J
AU Everett, ME
Howell, SB
Silva, DR
Szkody, P
AF Everett, Mark E.
Howell, Steve B.
Silva, David R.
Szkody, Paula
TI SPECTROSCOPY OF FAINT KEPLER MISSION EXOPLANET CANDIDATE HOST STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: fundamental parameters;
stars: fundamental parameters; surveys
ID FALSE-POSITIVE RATE; BRIGHT F-STAR; K-DWARF; PLANET CANDIDATES;
ECCENTRIC ORBIT; HOT JUPITER; TRANSITING PLANET; INPUT CATALOG; COOL
STARS; STELLAR
AB Stellar properties are measured for a large set of Kepler mission exoplanet candidate host stars. Most of these stars are fainter than 14th magnitude, in contrast to other spectroscopic follow-up studies. This sample includes many high-priority Earth-sized candidate planets. A set of model spectra are fitted to R similar to 3000 optical spectra of 268 stars to improve estimates of T-eff, log( g), and [Fe/H] for the dwarfs in the range 4750 <= T-eff <= 7200 K. These stellar properties are used to find new stellar radii and, in turn, new radius estimates for the candidate planets. The result of improved stellar characteristics is a more accurate representation of this Kepler exoplanet sample and identification of promising candidates for more detailed study. This stellar sample, particularly among stars with T-eff greater than or similar to 5200 K, includes a greater number of relatively evolved stars with larger radii than assumed by the mission on the basis of multi-color broadband photometry. About 26% of the modeled stars require radii to be revised upward by a factor of 1.35 or greater, and modeling of 87% of the stars suggest some increase in radius. The sample presented here also exhibits a change in the incidence of planets larger than 3-4 R-circle plus as a function of metallicity. Once [Fe/H] increases to >= -0.05, large planets suddenly appear in the sample while smaller planets are found orbiting stars with a wider range of metallicity. The modeled stellar spectra, as well as an additional 84 stars of mostly lower effective temperatures, are made available to the community.
C1 [Everett, Mark E.; Silva, David R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
RP Everett, ME (reprint author), Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA.
FU NASA Kepler Mission [AST-0950945]
FX Our work was made possible through the efforts of many others. Among
them are those in the Kepler Science Office and science team. At the
telescope we always received excellent help from our observing
assistants, and help from additional observers Jay Holberg, Ken Mighell,
and Jason Rowe. Codes used in our modeling were adopted from work by
Greg Doppmann and we received help to compile a list of properties for
our test star sample from Lars Buchhave and Thomas Kallinger. We also
thank the referee for helpful suggestions that were incorporated into
this work. Financial support for the work was provided by the NASA
Kepler Mission and Cooperative Agreement AST-0950945 to NOAO.
NR 51
TC 29
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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 JUL 10
PY 2013
VL 771
IS 2
AR 107
DI 10.1088/0004-637X/771/2/107
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176XS
UT WOS:000321340700032
ER
PT J
AU Fujii, Y
Kawahara, H
Suto, Y
Fukuda, S
Nakajima, T
Livengood, TA
Turner, EL
AF Fujii, Yuka
Kawahara, Hajime
Suto, Yasushi
Fukuda, Satoru
Nakajima, Teruyuki
Livengood, Timothy A.
Turner, Edwin L.
TI COLORS OF A SECOND EARTH. II. EFFECT OF CLOUDS ON PHOTOMETRIC
CHARACTERIZATION OF EARTH-LIKE EXOPLANETS (vol 738, pg 184, 2011)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Fujii, Yuka; Suto, Yasushi; Turner, Edwin L.] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
[Kawahara, Hajime] Tokyo Metropolitan Univ, Dept Phys, Hachioji, Tokyo 1920397, Japan.
[Suto, Yasushi] Univ Tokyo, Grad Sch Sci, Res Ctr Early Universe, Tokyo 1130033, Japan.
[Suto, Yasushi; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Fukuda, Satoru; Nakajima, Teruyuki] Univ Tokyo, Ctr Climate Syst Res, Kashiwa, Chiba 2778568, Japan.
[Livengood, Timothy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Turner, Edwin L.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
RP Fujii, Y (reprint author), Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
EM yuka.fujii@utap.phys.s.u-tokyo.ac.jp
RI Nakajima, Teruyuki/H-2370-2013
OI Nakajima, Teruyuki/0000-0002-9042-504X
NR 1
TC 0
Z9 0
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 JUL 10
PY 2013
VL 771
IS 2
AR 139
DI 10.1088/0004-637X/771/2/139
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176XS
UT WOS:000321340700064
ER
PT J
AU Landry, R
Dodson-Robinson, SE
Turner, NJ
Abram, G
AF Landry, Russell
Dodson-Robinson, Sarah E.
Turner, Neal J.
Abram, Greg
TI PROTOSTELLAR DISK EVOLUTION OVER MILLION-YEAR TIMESCALES WITH A
PRESCRIPTION FOR MAGNETIZED TURBULENCE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; instabilities; magnetic fields;
magnetohydrodynamics (MHD); protoplanetary disks; stars: formation
ID YOUNG STELLAR OBJECTS; T-TAURI DISKS; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC
SIMULATIONS; ROSSBY-WAVE INSTABILITY; ACCRETION DISKS; PROTOPLANETARY
DISKS; MAGNETOROTATIONAL-INSTABILITY; SNOW LINE; LAYERED ACCRETION;
GIANT PLANETS
AB Magnetorotational instability (MRI) is the most promising mechanism behind accretion in low-mass protostellar disks. Here we present the first analysis of the global structure and evolution of non-ideal MRI-driven T-Tauri disks on million-year timescales. We accomplish this in a 1+1D simulation by calculating magnetic diffusivities and utilizing turbulence activity criteria to determine thermal structure and accretion rate without resorting to a three-dimensional magnetohydrodynamical (MHD) simulation. Our major findings are as follows. First, even for modest surface densities of just a few times the minimum-mass solar nebula, the dead zone encompasses the giant planet-forming region, preserving any compositional gradients. Second, the surface density of the active layer is nearly constant in time at roughly 10 g cm(-2), which we use to derive a simple prescription for viscous heating in MRI-active disks for those who wish to avoid detailed MHD computations. Furthermore, unlike a standard disk with constant-alpha viscosity, the disk midplane does not cool off over time, though the surface cools as the star evolves along the Hayashi track. Instead, the MRI may pile material in the dead zone, causing it to heat up over time. The ice line is firmly in the terrestrial planet-forming region throughout disk evolution and can move either inward or outward with time, depending on whether pileups form near the star. Finally, steady-state mass transport is an extremely poor description of flow through an MRI-active disk, as we see both the turnaround in the accretion flow required by conservation of angular momentum and peaks in (M) over dot(R) bracketing each side of the dead zone. We caution that MRI activity is sensitive to many parameters, including stellar X-ray flux, grain size, gas/small grain mass ratio and magnetic field strength, and we have not performed an exhaustive parameter study here. Our 1+1D model also does not include azimuthal information, which prevents us from modeling the effects of Rossby waves.
C1 [Landry, Russell] Univ Texas Dallas, Dept Phys, Richardson, TX 75080 USA.
[Dodson-Robinson, Sarah E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Abram, Greg] Univ Texas Austin, Texas Adv Comp Ctr, Austin, TX 78758 USA.
RP Landry, R (reprint author), Univ Texas Dallas, Dept Phys, Richardson, TX 75080 USA.
EM russell.landry@gmail.com
OI Turner, Neal/0000-0001-8292-1943
FU NASA [NNX10AH28G]; University of Texas; National Science Foundation;
NASA
FX Funding for this work was provided by NASA through grant NNX10AH28G to
S.D.R. and N.J.T., and by University of Texas through a startup grant to
S.D.R. Computing and visualization support were provided by the Texas
Advanced Computing Center, which is funded by the National Science
Foundation. N.J.T. carried out his work at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA.
NR 91
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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 JUL 10
PY 2013
VL 771
IS 2
AR 80
DI 10.1088/0004-637X/771/2/80
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176XS
UT WOS:000321340700005
ER
PT J
AU Lehmer, BD
Wik, DR
Hornschemeier, AE
Ptak, A
Antoniou, V
Argo, MK
Bechtol, K
Boggs, S
Christensen, FE
Craig, WW
Hailey, CJ
Harrison, FA
Krivonos, R
Leyder, JC
Maccarone, TJ
Stern, D
Venters, T
Zezas, A
Zhang, WW
AF Lehmer, B. D.
Wik, D. R.
Hornschemeier, A. E.
Ptak, A.
Antoniou, V.
Argo, M. K.
Bechtol, K.
Boggs, S.
Christensen, F. E.
Craig, W. W.
Hailey, C. J.
Harrison, F. A.
Krivonos, R.
Leyder, J-C
Maccarone, T. J.
Stern, D.
Venters, T.
Zezas, A.
Zhang, W. W.
TI NuSTAR AND CHANDRA INSIGHT INTO THE NATURE OF THE 3-40 keV NUCLEAR
EMISSION IN NGC 253
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 253); galaxies: star
formation; galaxies: starburst; X-rays: galaxies
ID STARBURST GALAXY NGC-253; X-RAY OBSERVATIONS; XMM-NEWTON OBSERVATIONS;
ACTIVE GALACTIC NUCLEI; CATALOG; COMPLEX; REGION; DISK; RESOLUTION;
BINARIES
AB We present results from three nearly simultaneous Nuclear Spectroscopic Telescope Array (NuSTAR) and Chandra monitoring observations between 2012 September 2 and 2012 November 16 of the local star-forming galaxy NGC 253. The 3-40 keV intensity of the inner similar to 20 arcsec (similar to 400 pc) nuclear region, as measured by NuSTAR, varied by a factor of similar to 2 across the three monitoring observations. The Chandra data reveal that the nuclear region contains three bright X-ray sources, including a luminous (L2-10 (keV) similar to few x 10(39) erg s(-1)) point source located similar to 1 arcsec from the dynamical center of the galaxy (within the 3 sigma positional uncertainty of the dynamical center); this source drives the overall variability of the nuclear region at energies greater than or similar to 3 keV. We make use of the variability to measure the spectra of this single hard X-ray source when it was in bright states. The spectra are well described by an absorbed (N-H approximate to 1.6 x 10(23) cm(-2)) broken power-law model with spectral slopes and break energies that are typical of ultraluminous X-ray sources (ULXs), but not active galactic nuclei (AGNs). A previous Chandra observation in 2003 showed a hard X-ray point source of similar luminosity to the 2012 source that was also near the dynamical center (theta approximate to 0.4 arcsec); however, this source was offset from the 2012 source position by approximate to 1 arcsec. We show that the probability of the 2003 and 2012 hard X-ray sources being unrelated is >> 99.99% based on the Chandra spatial localizations. Interestingly, the Chandra spectrum of the 2003 source (3-8 keV) is shallower in slope than that of the 2012 hard X-ray source. Its proximity to the dynamical center and harder Chandra spectrum indicate that the 2003 source is a better AGN candidate than any of the sources detected in our 2012 campaign; however, we were unable to rule out a ULX nature for this source. Future NuSTAR and Chandra monitoring would be well equipped to break the degeneracy between the AGN and ULX nature of the 2003 source, if again caught in a high state.
C1 [Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Lehmer, B. D.; Wik, D. R.; Hornschemeier, A. E.; Ptak, A.; Leyder, J-C; Venters, T.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Antoniou, V.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Argo, M. K.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Bechtol, K.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Boggs, S.; Craig, W. W.; Krivonos, R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94720 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Harrison, F. A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Leyder, J-C] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Maccarone, T. J.] Univ Southampton, Sch Phys & Astron, Highfield SO17 1BJ, Hants, England.
[Maccarone, T. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zezas, A.] Univ Crete, Dept Phys, Iraklion, Greece.
RP Lehmer, BD (reprint author), Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA.
RI Boggs, Steven/E-4170-2015; Zezas, Andreas/C-7543-2011; Antoniou,
Vallia/E-3837-2013;
OI Boggs, Steven/0000-0001-9567-4224; Zezas, Andreas/0000-0001-8952-676X;
Antoniou, Vallia/0000-0001-7539-1593; Argo, Megan/0000-0003-3594-0214
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration
FX We thank the anonymous referee for helpful comments, which have improved
the quality of this paper. This work was supported under NASA Contract
No. NNG08FD60C, and made use of data from the NuSTAR mission, a project
led by the California Institute of Technology, managed by the Jet
Propulsion Laboratory, and funded by the National Aeronautics and Space
Administration. We thank the NuSTAR operations, software, and
calibration teams for support with the execution and analysis of these
observations. This research has made use of the NuSTAR Data Analysis
Software (NuSTARDAS) jointly developed by the ASI Science Data Center
(ASDC, Italy) and the California Institute of Technology (USA). We thank
the Chandra X-ray Center staff for providing faster than usual
processing of the Chandra data.
NR 36
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U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2013
VL 771
IS 2
AR 134
DI 10.1088/0004-637X/771/2/134
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176XS
UT WOS:000321340700059
ER
PT J
AU Masson, S
Antiochos, SK
DeVore, CR
AF Masson, S.
Antiochos, S. K.
DeVore, C. R.
TI A MODEL FOR THE ESCAPE OF SOLAR-FLARE-ACCELERATED PARTICLES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); methods: numerical; Sun: coronal mass
ejections (CMEs); Sun: flares; Sun: magnetic topology; Sun: particle
emission
ID CORONAL MASS EJECTIONS; FIELD LINE SHRINKAGE; X-RAY; MAGNETIC
RECONNECTION; ENERGETIC PARTICLES; NULL-POINT; NUMERICAL SIMULATIONS;
BREAKOUT MODEL; FLUX EMERGENCE; 3 DIMENSIONS
AB We address the problem of how particles are accelerated by solar flares can escape into the heliosphere on timescales of an hour or less. Impulsive solar energetic particle (SEP) bursts are generally observed in association with so-called eruptive flares consisting of a coronal mass ejection (CME) and a flare. These fast SEPs are believed to be accelerated directly by the flare, rather than by the CME shock. However, the precise mechanism by which the particles are accelerated remains controversial. Regardless of the origin of the acceleration, the particles should remain trapped in the closed magnetic fields of the coronal flare loops and the ejected flux rope, given the magnetic geometry of the standard eruptive-flare model. In this case, the particles would reach the Earth only after a delay of many hours to a few days (coincident with the bulk ejecta arriving at Earth). We propose that the external magnetic reconnection intrinsic to the breakout model for CME initiation can naturally account for the prompt escape of flare-accelerated energetic particles onto open interplanetary magnetic flux tubes. We present detailed 2.5-dimensional magnetohydrodynamic simulations of a breakout CME/flare event with a background isothermal solar wind. Our calculations demonstrate that if the event occurs sufficiently near a coronal-hole boundary, interchange reconnection between open and closed fields can occur. This process allows particles from deep inside the ejected flux rope to access solar wind field lines soon after eruption. We compare these results to standard observations of impulsive SEPs and discuss the implications of the model on further observations and calculations.
C1 [Masson, S.; Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[DeVore, C. R.] Naval Res Lab, Lab Computat Phys & Fluid Dynam, Washington, DC 20375 USA.
RP Masson, S (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM sophie.masson@nasa.gov
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
FX S.M. gratefully acknowledges support from the NASA Post-doctoral
Program, administered by Oak Ridge Associated Universities through a
contract with NASA, during her stay at NASA Goddard Space Flight Center.
This work was supported, in part, by the NASA TR&T and SR&T Programs.
NR 98
TC 17
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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 JUL 10
PY 2013
VL 771
IS 2
AR 82
DI 10.1088/0004-637X/771/2/82
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176XS
UT WOS:000321340700007
ER
PT J
AU Pasham, DR
Strohmayer, TE
AF Pasham, Dheeraj R.
Strohmayer, Tod E.
TI ON THE NATURE OF THE mHz X-RAY QUASI-PERIODIC OSCILLATIONS FROM
ULTRALUMINOUS X-RAY SOURCE M82 X-1: SEARCH FOR TIMING-SPECTRAL
CORRELATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; methods: data analysis; X-rays: binaries
ID NOVA XTE J1550-564; BLACK-HOLE CANDIDATES; NGC 5408 X-1; GRS 1915+105;
RXTE OBSERVATIONS; TERM VARIABILITY; QPO FREQUENCY; XMM-NEWTON; IRON
LINE; DISCOVERY
AB Using all the archival XMM-Newton X-ray (3-10 keV) observations of the ultraluminous X-ray source (ULX) M82 X-1, we searched for a correlation between its variable mHz quasi-periodic oscillation (QPO) frequency and its hardness ratio (5-10 keV/3-5 keV), an indicator of the energy spectral power-law index. When stellar-mass black holes (StMBHs) exhibit type-C low-frequency QPOs (similar to 0.2-15 Hz), the centroid frequency of the QPO is known to correlate with the energy spectral index. The detection of such a correlation would strengthen the identification of M82 X-1's mHz QPOs as type-C and enable a more reliable mass estimate by scaling its QPO frequencies to those of type-C QPOs in StMBHs of known mass. We resolved the count rates and the hardness ratios of M82 X-1 and a nearby bright ULX (source 5/X42.3+59) through surface brightness modeling. We detected QPOs in the frequency range of 36-210 mHz during which M82 X-1's hardness ratio varied from 0.42 to 0.47. Our primary results are (1) that we do not detect any correlation between the mHz QPO frequency and the hardness ratio (a substitute for the energy spectral power-law index) and (2) similar to some accreting X-ray binaries, we find that M82 X-1's mHz QPO frequency increases with its X-ray count rate (Pearson's correlation coefficient = +0.97). The apparent lack of a correlation between the QPO centroid frequency and the hardness ratio poses a challenge to the earlier claims that the mHz QPOs of M82 X-1 are the analogs of the type-C low-frequency QPOs of StMBHs. On the other hand, it is possible that the observed relation between the hardness ratio and the QPO frequency represents the saturated portion of the correlation seen in type-C QPOs of StMBHs-in which case M82 X-1's mHz QPOs can still be analogous to type-C QPOs.
C1 [Pasham, Dheeraj R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Strohmayer, Tod E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Pasham, DR (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM dheeraj@astro.umd.edu; tod.strohmayer@nasa.gov
NR 55
TC 9
Z9 9
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 JUL 10
PY 2013
VL 771
IS 2
AR 101
DI 10.1088/0004-637X/771/2/101
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176XS
UT WOS:000321340700026
ER
PT J
AU Rappazzo, AF
Velli, M
Einaudi, G
AF Rappazzo, A. F.
Velli, M.
Einaudi, G.
TI FIELD LINES TWISTING IN A NOISY CORONA: IMPLICATIONS FOR ENERGY STORAGE
AND RELEASE, AND INITIATION OF SOLAR ERUPTIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); Sun:corona; Sun:coronal mass ejections
(CMEs); Sun:magnetic topology; turbulence
ID DRIVEN VORTEX FLOWS; MAGNETOHYDRODYNAMIC TURBULENCE; REDUCED
MAGNETOHYDRODYNAMICS; KINK INSTABILITY; MASS EJECTIONS; LOOPS;
RECONNECTION; RELAXATION; NANOFLARES; EQUATIONS
AB We present simulations modeling closed regions of the solar corona threaded by a strong magnetic field where localized photospheric vortical motions twist the coronal field lines. The linear and nonlinear dynamics are investigated in the reduced magnetohydrodynamic regime in Cartesian geometry. Initially the magnetic field lines get twisted and the system becomes unstable to the internal kink mode, confirming and extending previous results. As typical in this kind of investigations, where initial conditions implement smooth fields and flux-tubes, we have neglected fluctuations and the fields are laminar until the instability sets in. However, previous investigations indicate that fluctuations, excited by photospheric motions and coronal dynamics, are naturally present at all scales in the coronal fields. Thus, in order to understand the effect of a photospheric vortex on a more realistic corona, we continue the simulations after kink instability sets in, when turbulent fluctuations have already developed in the corona. In the nonlinear stage the system never returns to the simple initial state with ordered twisted field lines, and kink instability does not occur again. Nevertheless, field lines get twisted, although in a disordered way, and energy accumulates at large scales through an inverse cascade. This energy can subsequently be released in micro-flares or larger flares, when interaction with neighboring structures occurs or via other mechanisms. The impact on coronal dynamics and coronal mass ejections initiation is discussed.
C1 [Rappazzo, A. F.] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA.
[Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Einaudi, G.] Berkeley Res Associates Inc, Beltsville, MD 20705 USA.
RP Rappazzo, AF (reprint author), Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA.
EM rappazzo@udel.edu
FU NASA; NASA [NNX11AJ44G, 11-2331, 12-3188]; NSF [AGS-1063439,
AGS-1156094]
FX This work was carried out in part at the Jet Propulsion Laboratory under
a contract with NASA. This research supported in part by the NASA
Heliophysics Theory program NNX11AJ44G, and by the NSF Solar Terrestrial
and SHINE programs (AGS-1063439 and AGS-1156094), by the NASA MMS and
Solar probe Plus Projects. Simulations have been performed through the
NASA Advanced Supercomputing SMD awards 11-2331 and 12-3188.
NR 55
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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 JUL 10
PY 2013
VL 771
IS 2
AR 76
DI 10.1088/0004-637X/771/2/76
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176XS
UT WOS:000321340700001
ER
PT J
AU Viall, NM
Klimchuk, JA
AF Viall, Nicholeen M.
Klimchuk, James A.
TI MODELING THE LINE-OF-SIGHT INTEGRATED EMISSION IN THE CORONA:
IMPLICATIONS FOR CORONAL HEATING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona
ID ACTIVE-REGION LOOPS; X-RAY TELESCOPE; IMAGING SPECTROMETER; PLASMA;
EVOLUTION; HINODE; TRACE; CORE; CONSTRAINTS; EXPLORER
AB One of the outstanding problems in all of space science is uncovering how the solar corona is heated to temperatures greater than 1 MK. Though studied for decades, one of the major difficulties in solving this problem has been unraveling the line-of-sight (LOS) effects in the observations. The corona is optically thin, so a single pixel measures counts from an indeterminate number (perhaps tens of thousands) of independently heated flux tubes, all along that pixel's LOS. In this paper we model the emission in individual pixels imaging the active region corona in the extreme ultraviolet. If LOS effects are not properly taken into account, erroneous conclusions regarding both coronal heating and coronal dynamics may be reached. We model the corona as an LOS integration of many thousands of completely independently heated flux tubes. We demonstrate that despite the superposition of randomly heated flux tubes, nanoflares leave distinct signatures in light curves observed with multi-wavelength and high time cadence data, such as those data taken with the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. These signatures are readily detected with the time-lag analysis technique of Viall & Klimchuk in 2012. Steady coronal heating leaves a different and equally distinct signature that is also revealed by the technique.
C1 [Viall, Nicholeen M.; Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Viall, NM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Klimchuk, James/D-1041-2012
OI Klimchuk, James/0000-0003-2255-0305
FU NASA
FX This research was supported by the NASA Supporting Research and
Technology program. We thank the reviewer for their helpful comments and
suggestions. The data are courtesy of NASA/SDO and the AIA science team.
This work benefited greatly from the International Space Science
Institute team meeting "Coronal Heating-Using Observables to Settle the
Question of Steady vs. Impulsive Heating" led by Stephen Bradshaw and
Helen Mason.
NR 46
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U1 1
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2013
VL 771
IS 2
AR 115
DI 10.1088/0004-637X/771/2/115
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176XS
UT WOS:000321340700040
ER
PT J
AU Parks, GK
Lee, E
Lin, N
Fu, SY
McCarthy, M
Cao, JB
Hong, J
Liu, Y
Shi, JK
Goldstein, ML
Canu, P
Dandouras, I
Reme, H
AF Parks, G. K.
Lee, E.
Lin, N.
Fu, S. Y.
McCarthy, M.
Cao, J. B.
Hong, J.
Liu, Y.
Shi, J. K.
Goldstein, M. L.
Canu, P.
Dandouras, I.
Reme, H.
TI REINTERPRETATION OF SLOWDOWN OF SOLAR WIND MEAN VELOCITY IN NONLINEAR
STRUCTURES OBSERVED UPSTREAM OF EARTH'S BOW SHOCK
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; shock waves; solar wind
ID DIAMAGNETIC CAVITIES UPSTREAM; HOT FLOW ANOMALIES; DENSITY HOLES
AB Two of the many features associated with nonlinear upstream structures are (1) the solar wind (SW) mean flow slows down and deviates substantially and (2) the temperature of the plasma increases in the structure. In this Letter, we show that the SW beam can be present throughout the entire upstream event maintaining a nearly constant beam velocity and temperature. The decrease of the velocity is due to the appearance of new particles moving in the opposite direction that act against the SW beam and reduce the mean velocity as computed via moments. The new population, which occupies a larger velocity space, also contributes to the second moment, increasing the temperature. The new particles include the reflected SW beam at the bow shock and another population of lower energies, accelerated nearby at the shock or at the boundary of the nonlinear structures.
C1 [Parks, G. K.; Lin, N.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Lee, E.; Hong, J.] Kyung Hee Univ, Sch Space Res, Yongin, Gyeonggi, South Korea.
[Fu, S. Y.] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
[McCarthy, M.] Univ Washington, Seattle, WA 98195 USA.
[Cao, J. B.] Beijing Univ Aeronaut & Astronaut, Beijing 100190, Peoples R China.
[Liu, Y.; Shi, J. K.] Natl Space Sci Ctr, Beijing, Peoples R China.
[Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Canu, P.] Ecole Polytech, Plasma Phys Lab, F-75230 Paris, France.
[Dandouras, I.] IRAP, CNRS, Toulouse, France.
[Reme, H.] Univ Toulouse, UPS OMP, IRAP, CNRS, Toulouse, France.
RP Parks, GK (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM parks@ssl.berkeley.edu
OI Dandouras, Iannis/0000-0002-7121-1118; Liu, Ying/0000-0002-3483-5909
FU NASA [NNX11AD49G-2/14]; WCU program through NRF [R31-10016]; MEST of
Korea
FX The research was supported in part by a NASA grant to the University of
California, Berkeley NNX11AD49G-2/14 and at Kyung Hee University by WCU
program (Grant No. R31-10016) through NRF funded by MEST of Korea.
NR 10
TC 1
Z9 1
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 JUL 10
PY 2013
VL 771
IS 2
AR L39
DI 10.1088/2041-8205/771/2/L39
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 172WI
UT WOS:000321036000021
ER
PT J
AU Pasham, DR
Strohmayer, TE
Mushotzky, RF
AF Pasham, Dheeraj R.
Strohmayer, Tod E.
Mushotzky, Richard F.
TI DISCOVERY OF A 7 mHz X-RAY QUASI-PERIODIC OSCILLATION FROM THE MOST
MASSIVE STELLAR-MASS BLACK HOLE IC 10 X-1
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE black hole physics; X-rays: binaries; X-rays: individual (IC 10 X-1)
ID GRS 1915+105; HIGH-FREQUENCY; XTE J1550-564; 4U 1608-52; VARIABILITY;
CANDIDATE; ACCRETION; DISK; QPOS; INSTABILITIES
AB We report the discovery with XMM-Newton of an approximate to 7 mHz X-ray (0.3-10.0 keV) quasi-periodic oscillation (QPO) from the eclipsing, high-inclination black hole binary IC 10 X-1. The QPO is significant at >4.33 sigma confidence level and has a fractional amplitude (% rms) and a quality factor, Q nu/Delta nu of approximate to 11 and 4, respectively. The overall X-ray (0.3-10.0 keV) power spectrum in the frequency range 0.0001-0.1 Hz can be described by a power-law with an index of approximate to-2, and a QPO at 7 mHz. At frequencies greater than or similar to 0.02 Hz there is no evidence for significant variability. The fractional amplitude (rms) of the QPO is roughly energy-independent in the energy range of 0.3-1.5 keV. Above 1.5 keV the low signal-to-noise ratio of the data does not allow us to detect the QPO. By directly comparing these properties with the wide range of QPOs currently known from accreting black hole and neutron stars, we suggest that the 7 mHz QPO of IC 10 X-1 may be linked to one of the following three categories of QPOs: (1) the "heartbeat" mHz QPOs of the black hole sources GRS 1915+105 and IGR J17091-3624, or (2) the 0.6-2.4 Hz "dipper QPOs" of high-inclination neutron star systems, or (3) the mHz QPOs of Cygnus X-3.
C1 [Pasham, Dheeraj R.; Mushotzky, Richard F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Strohmayer, Tod E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Pasham, DR (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM dheeraj@astro.umd.edu; tod.strohmayer@nasa.gov; richard@astro.umd.edu
NR 41
TC 5
Z9 5
U1 1
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 JUL 10
PY 2013
VL 771
IS 2
AR L44
DI 10.1088/2041-8205/771/2/L44
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 172WI
UT WOS:000321036000026
ER
PT J
AU Cuero, R
Mckay, DS
AF Cuero, Raul
McKay, David S.
TI Induction and construct UV protective yeast plasmid
SO JOURNAL OF BIOTECHNOLOGY
LA English
DT Article
DE Plasmid; Anti-UV; HSP (heat shock protein); Alcohol dehydrogenase (ADH);
Kinase and skin cells
ID TANDEM MASS-SPECTROMETRY; STATISTICAL-MODEL; BACILLUS-SUBTILIS;
PROTEINS; IDENTIFICATION; DISRUPTION; RADIATION; DATABASE; STRESS
AB In this study, we apply concepts of synthetic biology in combination with conventional methods to assemble different genetic components to construct yeast resistant to UV radiation, and to induce production of anti-UV proteins. This work combines sequences of different promoters, STRESS-proteins, heat shock protein (HSP), kinase proteins, alcohol dehydrogenase protein (ADH), ribosomal binding sites, fluorescent reporter proteins, terminators, and a synthetic ribosomal switch. The aim of this investigation was to induce an anti-UV proteins, and to construct an anti-UV yeast plasmid to be used for protection of skin cells against UV radiation. This investigation demonstrates induction and construction of anti-UV genes and production of their corresponding proteins. Cultures of Saccharomyces cerevisiae (ATCC # 66348) were exposed to short-wave UV radiation and were then subjected to time-PCR to assess specific gene expression. Proteins were identified using two dimensional difference gel electrophoresis (2D DIGE) and LC-MS/MS. Different up-regulated and down-regulated proteins were identified. Highly expressed identified proteins were cloned into S. cerevisiae using a synthetic biology approach. Extracts from UV-induced genetically transformed yeasts were used to protect skin cell cultures (ATCC #2522-CRL) in vitro. Both microscopic analysis and an apoptosis assay showed protection of the skin cell cultures against UV radiation. (c) 2013 Elsevier B.V. All rights reserved.
C1 [Cuero, Raul] Prairie View A&M Univ, CARC, Prairie View, TX 77446 USA.
[McKay, David S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Cuero, R (reprint author), 7219 Prairie Village, Parc Of Creativity Cypre, TX 77433 USA.
EM olimpa@aol.com
FU SynBERC-NSF; NASA-JSC-Houston; CARC-Prairie View AM University
FX The authors are indebted to SynBERC-NSF, NASA-JSC-Houston, and
CARC-Prairie View A&M University for providing research funding, and to
CloneTex Systems, Inc., for providing the synthesized gene sequences and
technical assistance.
NR 27
TC 0
Z9 0
U1 1
U2 32
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1656
J9 J BIOTECHNOL
JI J. Biotechnol.
PD JUL 10
PY 2013
VL 166
IS 3
BP 76
EP 83
DI 10.1016/j.jbiotec.2013.05.003
PG 8
WC Biotechnology & Applied Microbiology
SC Biotechnology & Applied Microbiology
GA 173YR
UT WOS:000321120200002
PM 23665192
ER
PT J
AU Ricklin, ME
Lorscheider, J
Waschbisch, A
Paroz, C
Mehta, SK
Pierson, DL
Kuhle, J
Fischer-Barnicol, B
Sprenger, T
Lindberg, RLP
Kappos, L
Derfuss, T
AF Ricklin, Meret E.
Lorscheider, Johannes
Waschbisch, Anne
Paroz, Cecile
Mehta, Satish K.
Pierson, Duane L.
Kuhle, Jens
Fischer-Barnicol, Bettina
Sprenger, Till
Lindberg, Raija L. P.
Kappos, Ludwig
Derfuss, Tobias
TI T-cell response against varicella-zoster virus in fingolimod-treated MS
patients
SO NEUROLOGY
LA English
DT Article
ID RELAPSING MULTIPLE-SCLEROSIS; HUMAN TRIGEMINAL GANGLIA; LYMPHOCYTE
EGRESS; ORAL FINGOLIMOD; FTY720; SUBSETS; THERAPY; BLOOD
AB Objective: To study the immune response against varicella-zoster virus (VZV) in patients with multiple sclerosis before and during fingolimod therapy.
Methods: The VZV-specific immune response was studied using interferon (IFN)-gamma enzyme-linked immunosorbent spot assay, proliferation assays, and upregulation of T-cell activation markers in patients before (n = 38) and after 3 months of fingolimod therapy (n = 34), in untreated (n 5 33) and IFN-beta-treated (n = 25) patients with multiple sclerosis, and in healthy controls (n 5 22). Viral replication was analyzed by using real-time PCR in 76 peripheral blood mononuclear cell samples and 146 saliva samples.
Results: Treatment with fingolimod led to a marked reduction of CD3(+) T cells with a relative decrease of naive and central memory T cells and an increase of effector memory T cells. Expression of the activation markers CD137 and CD69 upon VZV stimulation was unaltered by fingolimod. However, the absolute number of cells proliferating upon VZV stimulation was reduced in the blood of patients treated with fingolimod. Also, VZV-specific and Epstein-Barr virus (EBV)-specific IFN-gamma-producing cells were reduced after fingolimod therapy. Seven of the 35 patients treated with fingolimod showed signs of VZV or EBV reactivation in saliva compared with 3 of the 111 controls. None of the 76 tested samples showed signs of viral reactivation in the peripheral blood mononuclear cells.
Conclusion: Patients treated with fingolimod show a slightly reduced antiviral T-cell response. This reduced response is accompanied by a subclinical reactivation of VZV or EBV in the saliva of 20% of patients treated with fingolimod.
C1 [Ricklin, Meret E.; Lorscheider, Johannes; Paroz, Cecile; Kuhle, Jens; Lindberg, Raija L. P.; Kappos, Ludwig; Derfuss, Tobias] Univ Basel, Dept Biomed, CH-4003 Basel, Switzerland.
[Sprenger, Till] Univ Basel, Div Diagnost, Dept Radiol & Nucl Med, CH-4003 Basel, Switzerland.
[Sprenger, Till] Univ Basel, Div Intervent Neuroradiol, Dept Radiol & Nucl Med, CH-4003 Basel, Switzerland.
[Lorscheider, Johannes; Kuhle, Jens; Fischer-Barnicol, Bettina; Sprenger, Till; Kappos, Ludwig; Derfuss, Tobias] Univ Basel Hosp, Dept Neurol, Basel, Switzerland.
[Waschbisch, Anne] Univ Hosp Erlangen, Dept Neurol, Erlangen, Germany.
[Mehta, Satish K.] NASA, Lyndon B Johnson Space Ctr, Microbiol Lab, Houston, TX 77058 USA.
RP Derfuss, T (reprint author), Univ Basel, Dept Biomed, CH-4003 Basel, Switzerland.
EM tobias.derfuss@usb.ch
OI Sprenger, Till/0000-0002-5390-819X
FU Novartis
FX The study was partly funded by a research grant from Novartis.
NR 17
TC 28
Z9 28
U1 1
U2 2
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0028-3878
EI 1526-632X
J9 NEUROLOGY
JI Neurology
PD JUL 9
PY 2013
VL 81
IS 2
BP 174
EP 181
PG 8
WC Clinical Neurology
SC Neurosciences & Neurology
GA 304JJ
UT WOS:000330742600015
PM 23700335
ER
PT J
AU Moya, PS
Navarro, R
Munoz, V
Valdivia, JA
AF Moya, Pablo S.
Navarro, Roberto
Munoz, Victor
Alejandro Valdivia, J.
TI Comment on "Sensitive Test for Ion-Cyclotron Resonant Heating in the
Solar Wind"
SO PHYSICAL REVIEW LETTERS
LA English
DT Editorial Material
ID THERMAL ANISOTROPY; INSTABILITY
C1 [Moya, Pablo S.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Moya, Pablo S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Navarro, Roberto; Munoz, Victor; Alejandro Valdivia, J.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile.
RP Moya, PS (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Mail Code 673, Greenbelt, MD 20771 USA.
EM pablo.s.moyafuentes@nasa.gov
RI Munoz, Victor/A-2255-2008; Navarro, Roberto/F-7045-2014; Moya,
Pablo/C-3163-2011; Valdivia, Juan/A-3631-2008
OI Navarro, Roberto/0000-0003-0782-1904; Moya, Pablo/0000-0002-9161-0888;
Valdivia, Juan/0000-0003-3381-9904
NR 7
TC 5
Z9 5
U1 0
U2 4
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 JUL 9
PY 2013
VL 111
IS 2
AR 029001
DI 10.1103/PhysRevLett.111.029001
PG 2
WC Physics, Multidisciplinary
SC Physics
GA 182OE
UT WOS:000321752400048
PM 23889454
ER
PT J
AU Wejinya, UC
Chalamalasetty, SNS
Dong, ZX
Meyyappan, M
Iyuke, SE
AF Wejinya, Uchechukwu C.
Chalamalasetty, Siva Naga Sandeep
Dong, Zhuxin
Meyyappan, Meyya
Iyuke, Sunny E.
TI Dimensional Analysis of Acid Etching Effects on Vertically Grown Carbon
Nanofibers Using Atomic Force Microscopy
SO NANOMATERIALS AND NANOTECHNOLOGY
LA English
DT Article
DE Decentralized control; High-Order Neural Networks; Extended Kalman
Filter; Backstepping
ID NANOELECTRODE ARRAYS; FABRICATION
AB This paper presents a discrete-time decentralized control scheme for trajectory tracking of a two degrees of freedom (DOF) robot manipulator. A high order neural network (HONN) is used to approximate a decentralized control law designed by the backstepping technique as applied to a block strict feedback form (BSFF). The weights for each neural network are adapted online by an extended Kalman filter training algorithm. The motion for each joint is controlled independently using only local angular position and velocity measurements. The stability analysis for the closed-loop system via the Lyapunov approach is included. Finally, the real-time results show the feasibility of the proposed control scheme robot manipulator.
C1 [Wejinya, Uchechukwu C.; Dong, Zhuxin] Univ Arkansas, Dept Mech Engn, Fayetteville, AR 72701 USA.
[Chalamalasetty, Siva Naga Sandeep] Univ Arkansas, Dept Microelect & Photon, Fayetteville, AR 72701 USA.
[Meyyappan, Meyya] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Iyuke, Sunny E.] Univ Witwatersrand, Sch Chem & Met Engn, Johannesburg, South Africa.
RP Wejinya, UC (reprint author), Univ Arkansas, Dept Mech Engn, Fayetteville, AR 72701 USA.
EM uwejinya@uark.edu
FU University of Arkansas, College of Engineering External Mentoring Award
Program
FX The authors wish to express their sincere gratitude to Dr. Jessica
Koehne and Dr. PrabhuArmugam of NASA Ames Research Center for supplying
the fabricated chips and for their timely support and knowledgeable
discussions throughout the project. This project is partly supported by
University of Arkansas, College of Engineering External Mentoring Award
Program.
NR 16
TC 0
Z9 0
U1 1
U2 1
PU INTECH EUROPE
PI RIJEKA
PA JANEZA TRDINE 9, RIJEKA, 51000, CROATIA
SN 1847-9804
J9 NANOMATER NANOTECHNO
JI Nanomater. Nanotechnol.
PD JUL 8
PY 2013
VL 3
AR 9
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA AA5XW
UT WOS:000331173900001
ER
PT J
AU Pendo, L
Handberg, EM
Smelyanskiy, VN
Petukhov, AG
AF Pendo, Luke
Handberg, E. M.
Smelyanskiy, V. N.
Petukhov, A. G.
TI Large Stark effect for Li donor spins in Si
SO PHYSICAL REVIEW B
LA English
DT Article
ID SINGLE-ELECTRON SPIN; LATTICE RELAXATION; PERTURBATION-THEORY; EXCITED
STATES; SHALLOW DONORS; GROUND-STATE; QUANTUM DOTS; SILICON; GERMANIUM;
RESONANCE
AB We study the effect of a static electric field on lithium donor spins in silicon. The anisotropy of the effective mass leads to the anisotropy of the quadratic Stark susceptibility, which we determined using the Dalgarno-Lewis exact summation method. The theory is asymptotically exact in the field domain below Li-donor ionization threshold, relevant to the Stark-tuning electron spin resonance experiments. To obtain the generalized Stark susceptibilities at arbitrary fields, we propose a new variational wave function, which reproduces the exact results in the low-field limit. With the calculated susceptibilities at hand, we are able to predict and analyze several important physical effects. First, we observe that the energy level shifts due to the quadratic Stark effect for Li donors in Si are equivalent to, and can be mapped onto, those produced by an external stress. Second, we demonstrate that the Stark effect anisotropy, combined with the unique valley-orbit splitting of a Li donor in Si, spin-orbit interaction, and specially tuned external stress may lead to a very strong modulation of the donor spin g factor by the electric field. Third, we investigate the influence of random strains on the g factor shifts and quantify the random strain limits and requirements to Si material purity necessary to observe the g-factor Stark shifts experimentally. Finally, we discuss possible implications of our results for quantum information processing with Li spin qubits in Si.
C1 [Pendo, Luke; Handberg, E. M.; Petukhov, A. G.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Smelyanskiy, V. N.] NASA Ames Res Ctr, Moffett Field, CA 94043 USA.
RP Pendo, L (reprint author), South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
EM andre.petukhov@sdsmt.edu
FU NASA [NNX10AJ58A]; US Department of Energy, Office of Basic Energy
Sciences, Division of Materials Sciences and Engineering [ER46781]; US
National Security Agency; Mines Medal Fellowship
FX We are grateful to Stephen Lyon and Alexei Tyryshkin for multiple
stimulating discussions. Research supported by NASA under Award No.
NNX10AJ58A, by the US Department of Energy, Office of Basic Energy
Sciences, Division of Materials Sciences and Engineering under Award No.
ER46781 (L. P., E. M. H., and A. G. P.), by the US National Security
Agency (V. N. S.), and by a Mines Medal Fellowship (E. M. H.).
NR 50
TC 4
Z9 4
U1 0
U2 13
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1098-0121
J9 PHYS REV B
JI Phys. Rev. B
PD JUL 8
PY 2013
VL 88
IS 4
AR 045307
DI 10.1103/PhysRevB.88.045307
PG 19
WC Physics, Condensed Matter
SC Physics
GA 181LZ
UT WOS:000321670400011
ER
PT J
AU Aartsen, MG
Abbasi, R
Abdou, Y
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Altmann, D
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Bechet, S
Tjus, JB
Becker, KH
Bell, M
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Bertrand, D
Besson, DZ
Binder, G
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohaichuk, S
Bohm, C
Bose, D
Boeser, S
Botner, O
Brayeur, L
Bretz, HP
Brown, AM
Bruijn, R
Brunner, J
Carson, M
Casey, J
Casier, M
Chirkin, D
Christov, A
Christy, B
Clark, K
Clevermann, F
Coenders, S
Cohen, S
Cowen, DF
Silva, AHC
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
De Ridder, S
Desiati, P
De With, M
DeYoung, T
Diaz-Velez, JC
Dunkman, M
Eagan, R
Eberhardt, B
Eisch, J
Ellsworth, RW
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
Gluesenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Goodman, JA
Gora, D
Grant, D
Gross, A
Gurtner, M
Ha, C
Ismail, AH
Hallen, P
Hallgren, A
Halzen, F
Hanson, K
Heereman, D
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
Jagielski, K
Japaridze, GS
Jero, K
Jlelati, O
Kaminsky, B
Kappes, A
Karg, T
Karle, A
Kelley, JL
Kiryluk, J
Kislat, F
Klaes, J
Klein, SR
Koehne, JH
Kohnen, G
Kolanoski, H
Koepke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krasberg, M
Krings, K
Kroll, G
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Landsman, H
Larson, MJ
Lesiak-Bzdak, M
Leuermann, M
Leute, J
Luenemann, 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
Nahnhauer, R
Naumann, U
Niederhausen, H
Nowicki, SC
Nygren, DR
Obertacke, A
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Paul, L
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pinat, E
Pirk, N
Posselt, J
Price, PB
Przybylski, GT
Raedel, L
Rameez, M
Rawlins, K
Redl, P
Reimann, R
Resconi, E
Rhode, W
Ribordy, M
Richman, M
Riedel, B
Rodrigues, JP
Rott, C
Ruhe, T
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
Schoeneberg, S
Schoenwald, A
Schukraft, A
Schulte, L
Schulz, O
Seckel, D
Sestayo, Y
Seunarine, S
Sheremata, C
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
Tesic, G
Tilav, S
Toale, PA
Toscano, S
Usner, M
van der Drift, D
van Eijndhoven, N
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Waldenmaier, T
Wallraff, M
Wasserman, R
Weaver, C
Wellons, M
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
Zierke, S
Zilles, A
Zoll, M
AF Aartsen, M. G.
Abbasi, R.
Abdou, Y.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Altmann, D.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Baum, V.
Bay, R.
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.
Bernhard, A.
Bertrand, D.
Besson, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohaichuk, S.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Brayeur, L.
Bretz, H. -P.
Brown, A. M.
Bruijn, R.
Brunner, J.
Carson, M.
Casey, J.
Casier, M.
Chirkin, D.
Christov, A.
Christy, B.
Clark, K.
Clevermann, F.
Coenders, S.
Cohen, S.
Cowen, D. F.
Silva, A. H. Cruz
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
De Ridder, S.
Desiati, P.
De With, M.
DeYoung, T.
Diaz-Velez, J. C.
Dunkman, M.
Eagan, R.
Eberhardt, B.
Eisch, J.
Ellsworth, R. W.
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.
Golup, G.
Gonzalez, J. G.
Goodman, J. A.
Gora, D.
Grant, D.
Gross, A.
Gurtner, M.
Ha, C.
Ismail, A. Haj
Hallen, P.
Hallgren, A.
Halzen, F.
Hanson, K.
Heereman, D.
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.
Jagielski, K.
Japaridze, G. S.
Jero, K.
Jlelati, O.
Kaminsky, B.
Kappes, A.
Karg, T.
Karle, A.
Kelley, J. L.
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.
Krings, K.
Kroll, G.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Landsman, H.
Larson, M. J.
Lesiak-Bzdak, M.
Leuermann, M.
Leute, J.
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.
Nahnhauer, R.
Naumann, U.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Obertacke, A.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Paul, L.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pinat, E.
Pirk, N.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Raedel, L.
Rameez, M.
Rawlins, K.
Redl, P.
Reimann, R.
Resconi, E.
Rhode, W.
Ribordy, M.
Richman, M.
Riedel, B.
Rodrigues, J. P.
Rott, C.
Ruhe, T.
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.
Schoenwald, A.
Schukraft, A.
Schulte, L.
Schulz, O.
Seckel, D.
Sestayo, Y.
Seunarine, S.
Sheremata, C.
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.
Tesic, G.
Tilav, S.
Toale, P. A.
Toscano, S.
Usner, M.
van der Drift, D.
van Eijndhoven, N.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Wasserman, R.
Weaver, Ch
Wellons, M.
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.
Zierke, S.
Zilles, A.
Zoll, M.
CA IceCube Collaboration
TI First Observation of PeV-Energy Neutrinos with IceCube
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID ATMOSPHERIC MUON; PERFORMANCE; SCATTERING; SELECTION; SPECTRUM; SYSTEM;
CHARM; ICE
AB We report on the observation of two neutrino-induced events which have an estimated deposited energy in the IceCube detector of 1.04 +/- 0.16 and 1.14 +/- 0.17 PeV, respectively, the highest neutrino energies observed so far. These events are consistent with fully contained particle showers induced by neutral-current nu(e,mu,tau) ((nu) over bar (e,mu,tau)) or charged-current nu(e) ((nu) over bar (e)) interactions within the IceCube detector. The events were discovered in a search for ultrahigh energy neutrinos using data corresponding to 615.9 days effective live time. The expected number of atmospheric background is 0.082 +/- 0.004(stat)(-0.057)(+0.041)(syst). The probability of observing two or more candidate events under the atmospheric background-only hypothesis is 2.9 x 10(-3) (2.8 sigma) taking into account the uncertainty on the expected number of background events. These two events could be a first indication of an astrophysical neutrino flux; the moderate significance, however, does not permit a definitive conclusion at this time.
C1 [Bissok, M.; Blumenthal, J.; Coenders, S.; Euler, S.; Hallen, P.; Heinen, D.; Jagielski, K.; Krings, K.; Leuermann, M.; Paul, L.; Raedel, L.; Reimann, R.; Scheel, M.; Schoenen, S.; Schukraft, A.; Soiron, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zierke, S.; Zilles, A.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Aartsen, M. G.; Hill, G. C.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[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.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; van der Drift, D.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Binder, G.; 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.
[Altmann, D.; De With, M.; Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Tjus, J. Becker; Fedynitch, A.; Olivo, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Schulte, L.; Stasik, A.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Bechet, S.; Bertrand, D.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Bruxelles, Sci Fac CP230, B-1050 Brussels, Belgium.
[Bose, D.; Brayeur, L.; Casier, M.; De Clercq, C.; Golup, G.; Kunnen, J.; Labare, M.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Brown, A. M.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[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.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, 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.
[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.
[Bohaichuk, S.; Grant, D.; Nowicki, S. C.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Aguilar, J. A.; Christov, A.; Montaruli, T.; Rameez, M.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[Abdou, Y.; Carson, M.; De Ridder, S.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Ryckbosch, D.; Van Overloop, A.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kelley, J. L.; 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; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kelley, J. L.; 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; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Baum, V.; Eberhardt, B.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Bernhard, A.; Gross, A.; Leute, J.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; 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.; Gonzalez, J. G.; 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.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[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.
[Cowen, D. F.; Meszaros, P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Bell, M.; Clark, K.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Eagan, R.; Koskinen, D. J.; Meszaros, P.; Salameh, T.; Smith, M. W. E.; Tesic, G.; Wasserman, R.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Boersma, D. J.; Botner, O.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[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.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy.
[Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ishihara, A (reprint author), Chiba Univ, Dept Phys, Chiba 2638522, Japan.
EM aya@hepburn.s.chiba-u.ac.jp
RI Taavola, Henric/B-4497-2011; Aguilar Sanchez, Juan Antonio/H-4467-2015;
Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty,
James/D-9310-2011; Tjus, Julia/G-8145-2012; Wiebusch,
Christopher/G-6490-2012; Auffenberg, Jan/D-3954-2014; Koskinen,
David/G-3236-2014; Brunner, Juergen/G-3540-2015
OI Taavola, Henric/0000-0002-2604-2810; Carson,
Michael/0000-0003-0400-7819; Perez de los Heros,
Carlos/0000-0002-2084-5866; Benabderrahmane, Mohamed
Lotfi/0000-0003-4410-5886; Aguilar Sanchez, Juan
Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X;
Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952;
Rott, Carsten/0000-0002-6958-6033; Ter-Antonyan,
Samvel/0000-0002-5788-1369; Schukraft, Anne/0000-0002-9112-5479;
Wiebusch, Christopher/0000-0002-6418-3008; Auffenberg,
Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Brunner,
Juergen/0000-0002-5052-7236
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin-Madison; Open Science Grid
(OSG) grid infrastructure; U.S. Department of Energy; National Energy
Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI) grid computing resources; Natural Sciences and
Engineering Research Council of Canada; Compute Canada; Compute West
High Performance Computing; Swedish Research Council, Sweden; Swedish
Polar Research Secretariat, Sweden; Swedish National Infrastructure for
Computing (SNIC), Sweden; Knut and Alice Wallenberg Foundation, Sweden;
German Ministry for Education and Research (BMBF), Germany; Deutsche
Forschungsgemeinschaft (DFG), Germany; Helmholtz Alliance for
Astroparticle Physics (HAP), Germany; 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 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; Natural Sciences and Engineering
Research Council of Canada, Compute Canada, and Compute West High
Performance Computing; 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),
Helmholtz Alliance for Astroparticle Physics (HAP), 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 25
TC 243
Z9 244
U1 1
U2 23
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 JUL 8
PY 2013
VL 111
IS 2
AR 021103
DI 10.1103/PhysRevLett.111.021103
PG 7
WC Physics, Multidisciplinary
SC Physics
GA 181NN
UT WOS:000321674500001
PM 23889381
ER
PT J
AU Thornton, D
Stappers, B
Bailes, M
Barsdell, B
Bates, S
Bhat, NDR
Burgay, M
Burke-Spolaor, S
Champion, DJ
Coster, P
D'Amico, N
Jameson, A
Johnston, S
Keith, M
Kramer, M
Levin, L
Milia, S
Ng, C
Possenti, A
van Straten, W
AF Thornton, D.
Stappers, B.
Bailes, M.
Barsdell, B.
Bates, S.
Bhat, N. D. R.
Burgay, M.
Burke-Spolaor, S.
Champion, D. J.
Coster, P.
D'Amico, N.
Jameson, A.
Johnston, S.
Keith, M.
Kramer, M.
Levin, L.
Milia, S.
Ng, C.
Possenti, A.
van Straten, W.
TI A Population of Fast Radio Bursts at Cosmological Distances
SO SCIENCE
LA English
DT Article
ID GAMMA-RAY BURSTS; MULTIBEAM PULSAR SURVEY; REIONIZATION HISTORY;
ENVIRONMENT; DISPERSION; DISCOVERY; ORIGINS; SEARCH; GALAXY; STARS
AB Searches for transient astrophysical sources often reveal unexpected classes of objects that are useful physical laboratories. In a recent survey for pulsars and fast transients, we have uncovered four millisecond-duration radio transients all more than 40 degrees from the Galactic plane. The bursts' properties indicate that they are of celestial rather than terrestrial origin. Host galaxy and intergalactic medium models suggest that they have cosmological redshifts of 0.5 to 1 and distances of up to 3 gigaparsecs. No temporally coincident x- or gamma-ray signature was identified in association with the bursts. Characterization of the source population and identification of host galaxies offers an opportunity to determine the baryonic content of the universe.
C1 [Thornton, D.; Stappers, B.; Kramer, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Thornton, D.; Coster, P.; Johnston, S.; Keith, M.] Commonwealth Sci & Ind Res Org CSIRO Astron & Spa, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Bailes, M.; Barsdell, B.; Bhat, N. D. R.; Coster, P.; Jameson, A.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Bailes, M.; Barsdell, B.; Bhat, N. D. R.; Jameson, A.; van Straten, W.] Australian Res Council Ctr Excellence All Sky Ast, Hawthorn, Vic 3122, Australia.
[Bates, S.; Levin, L.] W Virginia Univ, Ctr Astrophys, Morgantown, WV 26506 USA.
[Bhat, N. D. R.] Curtin Univ, Fac Sci & Engn, Dept Imaging & Appl Phys, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Burgay, M.; D'Amico, N.; Milia, S.; Possenti, A.] Osservatorio Astron Cagliari, Ist Nazl Astrofis, I-09012 Capoterra, CA, Italy.
[Burke-Spolaor, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91104 USA.
[Champion, D. J.; Kramer, M.; Ng, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[D'Amico, N.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy.
RP Thornton, D (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
EM thornton@jb.man.ac.uk
OI Champion, David/0000-0003-1361-7723; Burgay, Marta/0000-0002-8265-4344;
van Straten, Willem/0000-0003-2519-7375
FU NASA; Commonwealth of Australia; CAASTRO [CE110001020]; Science and
Technology Facilities Council; CSIRO Astronomy and Space Science; Curtin
Research Fellowship [CRF12228]
FX This research has made use of the NASA/IPAC (Infrared Processing and
Analysis Center) Extragalactic Database (NED), which is operated by the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA. This research has made use of data obtained from the
High Energy Astrophysics Science Archive Research Center, provided by
NASA's Goddard Space Flight Center. Part of this research was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. The Parkes radio telescope 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. Part of this research was conducted because of the
support of CAASTRO through project number CE110001020. D. T. gratefully
acknowledges the support of the Science and Technology Facilities
Council and CSIRO Astronomy and Space Science in his Ph.D. studentship.
N.D.R.B. is supported by a Curtin Research Fellowship (CRF12228).
NR 26
TC 224
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U1 2
U2 15
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 JUL 5
PY 2013
VL 341
IS 6141
BP 53
EP 56
DI 10.1126/science.1236789
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 176GL
UT WOS:000321291700044
PM 23828936
ER
PT J
AU Meibom, S
Torres, G
Fressin, F
Latham, DW
Rowe, JF
Ciardi, DR
Bryson, ST
Rogers, LA
Henze, CE
Janes, K
Barnes, SA
Marcy, GW
Isaacson, H
Fischer, DA
Howell, SB
Horch, EP
Jenkins, JM
Schuler, SC
Crepp, J
AF Meibom, Soren
Torres, Guillermo
Fressin, Francois
Latham, David W.
Rowe, Jason F.
Ciardi, David R.
Bryson, Steven T.
Rogers, Leslie A.
Henze, Christopher E.
Janes, Kenneth
Barnes, Sydney A.
Marcy, Geoffrey W.
Isaacson, Howard
Fischer, Debra A.
Howell, Steve B.
Horch, Elliott P.
Jenkins, Jon M.
Schuler, Simon C.
Crepp, Justin
TI The same frequency of planets inside and outside open clusters of stars
SO NATURE
LA English
DT Article
ID INTERMEDIATE-MASS STARS; STELLAR CLUSTERS; NGC 6811; KEPLER; SYSTEMS;
ISOCHRONES; DYNAMICS; FIELD
AB Most stars and their planets form in open clusters. Over 95 per cent of such clusters have stellar densities too low (less than a hundred stars per cubic parsec) to withstand internal and external dynamical stresses and fall apart within a few hundred million years(1). Older open clusters have survived by virtue of being richer and denser in stars (1,000 to 10,000 per cubic parsec) when they formed. Such clusters represent a stellar environment very different from the birthplace of the Sun and other planet-hosting field stars. So far more than 800 planets have been found around Sun-like stars in the field(2). The field planets are usually the size of Neptune or smaller(3-5). In contrast, only four planets have been found orbiting stars in open clusters(6-8), all with masses similar to or greater than that of Jupiter. Here we report observations of the transits of two Sun-like stars by planets smaller than Neptune in the billion-year-old open cluster NGC6811. This demonstrates that small planets can form and survive in a dense cluster environment, and implies that the frequency and properties of planets in open clusters are consistent with those of planets around field stars in the Galaxy.
C1 [Meibom, Soren; Torres, Guillermo; Fressin, Francois; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rowe, Jason F.; Bryson, Steven T.; Henze, Christopher E.; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Rogers, Leslie A.] CALTECH, Pasadena, CA 91125 USA.
[Janes, Kenneth] Boston Univ, Boston, MA 02215 USA.
[Barnes, Sydney A.] Leibniz Inst Astrophys, D-14467 Potsdam, Germany.
[Barnes, Sydney A.] Space Sci Inst, Boulder, CO 80301 USA.
[Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Fischer, Debra A.] Yale Univ, New Haven, CT 06520 USA.
[Horch, Elliott P.] So Connecticut State Univ, New Haven, CT 06515 USA.
[Jenkins, Jon M.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schuler, Simon C.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Crepp, Justin] Univ Notre Dame, Notre Dame, IN 46556 USA.
RP Meibom, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM smeibom@cfa.harvard.edu
OI Ciardi, David/0000-0002-5741-3047; Schuler, Simon/0000-0001-7203-8014;
Fischer, Debra/0000-0003-2221-0861
FU NASA's Science Mission Directorate; NASA [NNX09AH18A, HF-51313.01-A, NAS
5-26555]; Kepler mission via NASA Cooperative Agreement [NCC2-1390];
NASA's Kepler Participating Scientist Program [NNX12AC75G]; Space
Telescope Science Institute
FX Kepler was competitively selected as the tenth Discovery mission.
Funding for this mission is provided by NASA's Science Mission
Directorate. S. M. acknowledges support through NASA grant NNX09AH18A
(The Kepler Cluster Study) and from the Kepler mission via NASA
Cooperative Agreement NCC2-1390. G. T. acknowledges support through
NASA's Kepler Participating Scientist Program grant NNX12AC75G. L. A. R.
acknowledges NASA support through Hubble Fellowship grant HF-51313.01-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.
NR 27
TC 37
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U1 0
U2 9
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUL 4
PY 2013
VL 499
IS 7456
BP 55
EP 58
DI 10.1038/nature12279
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 176ED
UT WOS:000321285600031
PM 23803764
ER
PT J
AU Marchi, S
Chapman, CR
Fassett, CI
Head, JW
Bottke, WF
Strom, RG
AF Marchi, Simone
Chapman, Clark R.
Fassett, Caleb I.
Head, James W.
Bottke, W. F.
Strom, Robert G.
TI Global resurfacing of Mercury 4.0-4.1 billion years ago by heavy
bombardment and volcanism
SO NATURE
LA English
DT Article
ID INNER SOLAR-SYSTEM; NEAR-EARTH OBJECTS; CRATER CHRONOLOGY; LUNAR;
STRATIGRAPHY; MESSENGER; IMPACTS; ORIGIN; MOON; AGES
AB The most heavily cratered terrains on Mercury have been estimated to be about 4 billion years (Gyr) old(1-4), but this was based on images of only about 45 per cent of the surface; even older regions could have existed in the unobserved portion. These terrains have a lower density of craters less than 100 km in diameter than does the Moon(1,3,5), an observation attributed to preferential resurfacing on Mercury. Here we report global crater statistics of Mercury's most heavily cratered terrains on the entire surface. Applying a recent model for early lunar crater chronology(6) and an updated dynamical extrapolation to Mercury(7), we find that the oldest surfaces were emplaced just after the start of the Late Heavy Bombardment (LHB) about 4.0-4.1 Gyr ago. Mercury's global record of large impact basins(8), which has hitherto not been dated, yields a similar surface age. This agreement implies that resurfacing was global and was due to volcanism, as previously suggested(1,5). This activity ended during the tail of the LHB, within about 300-400 million years after the emplacement of the oldest terrains on Mercury. These findings suggest that persistent volcanism could have been aided by the surge of basin-scale impacts during this bombardment.
C1 [Marchi, Simone] NASA, Lunar Sci Inst, SW Res Inst, Boulder, CO 80302 USA.
[Chapman, Clark R.; Bottke, W. F.] SW Res Inst, Boulder, CO 80302 USA.
[Fassett, Caleb I.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
[Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Strom, Robert G.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
RP Marchi, S (reprint author), NASA, Lunar Sci Inst, SW Res Inst, Boulder, CO 80302 USA.
EM marchi@boulder.swri.edu
OI Fassett, Caleb/0000-0001-9155-3804
FU NASA Lunar Science Institute (Center for Lunar Origin and Evolution at
the Southwest Research Institute in Boulder, Colorado-NASA)
[NNA09DB32A]; NASA [NASW-00002, NAS5-97271]; NASA Lunar Science
Institute (Center for Lunar Science and Exploration at the Lunar and
Planetary Institute in Houston, Texas)
FX The contributions of S. M. and W. F. B. were supported by the NASA Lunar
Science Institute (Center for Lunar Origin and Evolution at the
Southwest Research Institute in Boulder, Colorado-NASA Grant NNA09DB32A;
Center for Lunar Science and Exploration at the Lunar and Planetary
Institute in Houston, Texas). S. M. is grateful for being welcomed as a
collaborator with the Geology Discipline Group of MESSENGER. C.R.C.'s
contribution was supported by the MESSENGER Project. 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 31
TC 44
Z9 44
U1 3
U2 39
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUL 4
PY 2013
VL 499
IS 7456
BP 59
EP 61
DI 10.1038/nature12280
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 176ED
UT WOS:000321285600032
PM 23823793
ER
PT J
AU Miller, LG
Baesman, SM
Kirshtein, J
Voytek, MA
Oremland, RS
AF Miller, Laurence G.
Baesman, Shaun M.
Kirshtein, Julie
Voytek, Mary A.
Oremland, Ronald S.
TI A Biogeochemical and Genetic Survey of Acetylene Fermentation by
Environmental Samples and Bacterial Isolates
SO GEOMICROBIOLOGY JOURNAL
LA English
DT Article
DE acetylene; Enceladus; fermentation; Pelobacter; sediment
ID EARTHS EARLY ATMOSPHERE; PELOBACTER-ACETYLENICUS; SP-NOV; RIBOSOMAL-RNA;
MONO LAKE; REDUCTION; METABOLISM; HYDRATASE; METHANE; TITAN
AB Anoxic samples (sediment and groundwater) from 13 chemically diverse field sites were assayed for their ability to consume acetylene (C2H2). Over incubation periods ranging from approximate to 10 to 80days, selected samples from 7 of the 13 tested sites displayed significant C2H2 removal. No significant formation of ethylene was noted in these incubations; therefore, C2H2 consumption could be attributed to acetylene hydratase (AH) rather than nitrogenase activity. This putative AH (PAH) activity was observed in only 21% of the total of assayed samples, while amplification of AH genes from extracted DNA using degenerate primers derived from Pelobacter acetylenicus occurred in even fewer (9.8%) samples. Acetylene-fermenting bacteria were isolated as a pure culture from the sediments of a tidal mudflat in San Francisco Bay (SFB93) and as an enrichment culture from freshwater Searsville Lake (SV7). Comparison of 16S rDNA clone libraries revealed that SFB93 was closely related to P. carbolinicus, while SV7 consisted of several unrelated bacteria. AH gene was amplified from SFB93 but not SV7. The inability of the primers to generate amplicons in the SV7 enrichment, as well as from several of the environmental samples that displayed PAH activity, implied that either the primers were too highly constrained in their specificity or that there was a different type of AH gene in these environmental samples than occurs in P. acetylenicus. The significance of this work with regard to the search for life in the outer Solar System, where C2H2 is abundant, is discussed.
C1 [Miller, Laurence G.; Baesman, Shaun M.; Oremland, Ronald S.] USGS, Menlo Pk, CA 94015 USA.
[Kirshtein, Julie; Voytek, Mary A.] US Geol Survey, Reston, VA 22092 USA.
[Voytek, Mary A.] NASA Headquarters, Washington, DC USA.
RP Miller, LG (reprint author), USGS, Mail Stop 480,345 Middlefield Rd, Menlo Pk, CA 94015 USA.
EM lgmiller@usgs.gov
FU National Research Program of the US Geological Survey; Exobiology
Program of NASA
FX We are grateful to S. E. Hoeft, S. Bennett and K. M. Charles for
technical assistance. Environmental samples were provided by A.
Amirbahman, T. Imbrigiotta, S. B. Joye, K. Wolf, and R. B. Thomas. This
research was supported by the National Research Program of the US
Geological Survey, and by a grant from the Exobiology Program of NASA.
NR 61
TC 8
Z9 8
U1 0
U2 19
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 0149-0451
J9 GEOMICROBIOL J
JI Geomicrobiol. J.
PD JUL 3
PY 2013
VL 30
IS 6
BP 501
EP 516
DI 10.1080/01490451.2012.732662
PG 16
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 145TV
UT WOS:000319041700005
ER
PT J
AU Knyazikhin, Y
Lewis, P
Disney, MI
Mottus, M
Rautiainen, M
Stenberg, P
Kaufmann, RK
Marshak, A
Schull, MA
Carmona, PL
Vanderbilt, V
Davis, AB
Baret, F
Jacquemoud, S
Lyapustin, A
Yang, Y
Myneni, RB
AF Knyazikhin, Yuri
Lewis, Philip
Disney, Mathias I.
Mottus, Matti
Rautiainen, Miina
Stenberg, Pauline
Kaufmann, Robert K.
Marshak, Alexander
Schull, Mitchell A.
Carmona, Pedro Latorre
Vanderbilt, Vern
Davis, Anthony B.
Baret, Frederic
Jacquemoud, Stephane
Lyapustin, Alexei
Yang, Yan
Myneni, Ranga B.
TI Reply to Ollinger et al.: Remote sensing of leaf nitrogen and emergent
ecosystem properties
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Letter
C1 [Knyazikhin, Yuri; Kaufmann, Robert K.; Yang, Yan; Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Lewis, Philip; Disney, Mathias I.] UCL, Dept Geog, London WC1E 6BT, England.
[Lewis, Philip; Disney, Mathias I.] UCL, Natl Ctr Earth Observat, London WC1E 6BT, England.
[Mottus, Matti] Univ Helsinki, Dept Geosci & Geog, FI-00014 Helsinki, Finland.
[Rautiainen, Miina; Stenberg, Pauline] Univ Helsinki, Dept Forest Sci, FI-00014 Helsinki, Finland.
[Marshak, Alexander; Lyapustin, Alexei] NASA, Climate & Radiat Lab, Goddard Flight Ctr, Greenbelt, MD 20771 USA.
[Schull, Mitchell A.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Carmona, Pedro Latorre] Univ Jaume 1, Dept Lenguajes & Sistemas Informat, Castellon de La Plana 12071, Spain.
[Vanderbilt, Vern] NASA, Biospher Sci Branch, Div Earth Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Baret, Frederic] INRA Site Agroparc, Unite Mixte Rech Environm Mediterraneen & Modelis, F-84914 Avignon, France.
[Jacquemoud, Stephane] Univ Paris Diderot, Inst Phys Globe Paris, Sorbonne Paris Cite, Unite Mixte Rech Ctr Natl Rech Sci 7154, F-75013 Paris, France.
RP Knyazikhin, Y (reprint author), Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
EM jknjazi@bu.edu
RI Rautiainen, Miina/A-4208-2009; Mottus, Matti/A-4130-2009; Marshak,
Alexander/D-5671-2012; Myneni, Ranga/F-5129-2012; Lyapustin,
Alexei/H-9924-2014; Disney, Mathias/C-1889-2008; Jacquemoud,
Stephane/F-8842-2010; Baret, Fred/C-4135-2011
OI Rautiainen, Miina/0000-0002-6568-3258; Mottus,
Matti/0000-0002-2745-1966; Lyapustin, Alexei/0000-0003-1105-5739; Baret,
Fred/0000-0002-7655-8997
NR 5
TC 4
Z9 4
U1 0
U2 43
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 JUL 2
PY 2013
VL 110
IS 27
BP E2438
EP E2438
DI 10.1073/pnas.1305930110
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 185OF
UT WOS:000321978000002
PM 23980281
ER
PT J
AU George, KA
Hada, M
Chappell, L
Cucinotta, FA
AF George, Kerry A.
Hada, Megumi
Chappell, Lori
Cucinotta, Francis A.
TI Biological Effectiveness of Accelerated Particles for the Induction of
Chromosome Damage: Track Structure Effects
SO RADIATION RESEARCH
LA English
DT Article
ID HUMAN-LYMPHOCYTES; HEAVY-IONS; MAMMALIAN-CELLS; MUTATION-INDUCTION;
CHARGED-PARTICLES; SPACE EXPLORATION; MEV PROTONS; TIME-COURSE; V79
CELLS; HIGH-LET
AB We have investigated how radiation quality affects the induction of chromosomal aberrations in human cells. Human lymphocytes were irradiated in vitro with various energies of accelerated high charge and energy (HZE) particles including oxygen, neon, silicon, titanium and iron. Chromosome damage was assessed using three-color FISH chromosome painting in chemically induced premature chromosome condensation samples collected at first cell division after irradiation. The LET values for these particles ranged from 30 to 195 keV/mu m, and their energies ranged from about 55 MeV/u to more than 1,000 MeV/u. The 89 and 142 MeV/u neon particles produced the most simple-type reciprocal exchanges per unit dose. For complex-type exchanges, 64 MeV/u neon and 450 MeV/u iron were equally effective and induced the greatest amount of complex damage. Track structure models predict that at a fixed value of LET, particles with lower charge number (Z) will have a higher biological effectiveness compared to particles with a higher Z, and that a saturation cross section will be observed for different radiation qualities. Our results are consistent with model expectations within the limitation of experimental error, and provide the most extensive data that have been reported on the radiation quality dependences of chromosomal aberrations. (C) 2013 by Radiation Research Society
C1 [George, Kerry A.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
[Hada, Megumi; Chappell, Lori] Univ Space Res Assoc, Houston, TX 77058 USA.
[Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP George, KA (reprint author), Wyle Integrated Sci & Engn Grp, Mail Code Wyle HAC-37A,1290 Hercules Dr, Houston, TX 77058 USA.
EM kerry.a.george@nasa.gov
NR 33
TC 9
Z9 9
U1 0
U2 5
PU RADIATION RESEARCH SOC
PI LAWRENCE
PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA
SN 0033-7587
EI 1938-5404
J9 RADIAT RES
JI Radiat. Res.
PD JUL
PY 2013
VL 180
IS 1
BP 25
EP 33
DI 10.1667/RR3291.1
PG 9
WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology,
Nuclear Medicine & Medical Imaging
GA AA3JD
UT WOS:000330987800004
PM 23692480
ER
PT J
AU Huang, HY
Hall, A
Teixeira, J
AF Huang, Hsin-Yuan
Hall, Alex
Teixeira, Joao
TI Evaluation of the WRF PBL Parameterizations for Marine Boundary Layer
Clouds: Cumulus and Stratocumulus
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID EDDY-DIFFUSIVITY/MASS-FLUX; YAMADA LEVEL-3 MODEL; SHALLOW CUMULUS; BULK
PARAMETERIZATION; VERTICAL DIFFUSION; CLOSURE-MODEL; MASS; CONVECTION;
SCHEME; OCEAN
AB The performance of five boundary layer parameterizations in the Weather Research and Forecasting Model is examined for marine boundary layer cloud regions running in single-column mode. Most parameterizations show a poor agreement of the vertical boundary layer structure when compared with large-eddy simulation models. These comparisons against large-eddy simulation show that a parameterization based on the eddy-diffusivity/mass-flux approach provides a better performance. The results also illustrate the key role of boundary layer parameterizations in model performance.
C1 [Huang, Hsin-Yuan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Hall, Alex] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Huang, HY (reprint author), Univ Calif Los Angeles, 7343 Math Sci Bldg, Los Angeles, CA 90095 USA.
EM hyhuang@ucla.edu
RI Hall, Alex/D-8175-2014
FU Department of Energy [DE-SC0001467]
FX This work was supported by the Department of Energy Grant DE-SC0001467.
The authors thank Dr. Wayne Angevine at the National Oceanic and
Atmospheric Administration and Dr. Thorsten Mauritsen at the Max Planck
Institute for Meteorology for their invaluable discussions on this work.
We also thank Dr. Joshua Hacker at the Naval Postgraduate School for his
help on WRF single-column model simulations. Help and discussion from
Dr. Kay Suselj at the Caltech Jet Propulsion Laboratory are also greatly
acknowledged.
NR 43
TC 11
Z9 11
U1 1
U2 19
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD JUL
PY 2013
VL 141
IS 7
BP 2265
EP 2271
DI 10.1175/MWR-D-12-00292.1
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 301ET
UT WOS:000330516300007
ER
PT J
AU Jones, TA
Stensrud, DJ
Minnis, P
Palikonda, R
AF Jones, Thomas A.
Stensrud, David J.
Minnis, Patrick
Palikonda, Rabindra
TI Evaluation of a Forward Operator to Assimilate Cloud Water Path into
WRF-DART
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID ENSEMBLE KALMAN FILTER; NUMERICAL WEATHER PREDICTION; INFRARED SATELLITE
RADIANCES; SSI ANALYSIS SYSTEM; BULK MICROPHYSICS; PART I; MODIS DATA;
RADAR DATA; MODEL; THUNDERSTORM
AB Assimilating satellite-retrieved cloud properties into storm-scale models has received limited attention despite its potential to provide a wide array of information to a model analysis. Available retrievals include cloud water path (CWP), which represents the amount of cloud water and cloud ice present in an integrated column, and cloud-top and cloud-base pressures, which represent the top and bottom pressure levels of the cloud layers, respectively. These interrelated data are assimilated into an Advanced Research Weather Research and Forecasting Model (ARW-WRF) 40-member ensemble with 3-km grid spacing using the Data Assimilation Research Testbed (DART) ensemble Kalman filter. A new CWP forward operator combines the satellite-derived cloud information with similar variables generated by WRF. This approach is tested using a severe weather event on 10 May 2010. One experiment only assimilates conventional (CONV) observations, while the second assimilates the identical conventional observations and the satellite-derived CWP (PATH).
Comparison of the CWP observations at 2045 UTC to CONV and PATH analyses shows that PATH has an improved representation of both the magnitude and spatial orientation of CWP compared to CONV. Assimilating CWP acts both to suppress convection in the model where none is present in satellite data and to encourage convection where it is observed. Oklahoma Mesonet observations of downward shortwave flux at 2100 UTC indicate that PATH reduces the root-mean-square difference errors in downward shortwave flux by 75 W m(-2) compared to CONV. Reduction in model error is generally maximized during the initial 30-min forecast period with the impact of CWP observations decreasing for longer forecast times.
C1 [Jones, Thomas A.] Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Norman, OK 73072 USA.
[Stensrud, David J.] NOAA, OAR, Natl Severe Storms Lab, Norman, OK 73072 USA.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Palikonda, Rabindra] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Jones, TA (reprint author), Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Norman, OK 73072 USA.
EM thomas.jones@noaa.gov
RI Minnis, Patrick/G-1902-2010
OI Minnis, Patrick/0000-0002-4733-6148
FU NOAA/National Environmental Satellite, Data, and Information Service;
NOAA/Office of Oceanic and Atmospheric Research under NOAA-University of
Oklahoma [NA17RJ1227]; NOAA/Office of Oceanic and Atmospheric Research
under U.S. Department of Commerce; NASA Modeling, Analysis, and
Prediction (MAP) Program; GOES-R Program; Department of Energy
Atmospheric Science Research Program [DE-SC0000991/003]
FX We appreciate the two anonymous reviewers whose comments improved the
quality of this work. Weather Surveillance Radar-1988 Doppler (WSR-88D)
level 2 radar reflectivity were retrieved from National Climatic Data
Center archives. Mesonet data were kindly provided by the Oklahoma
Climatological Survey. Nancy Collins at the University Corporation for
Atmospheric Research provided invaluable assistance in helping debug
certain parts of the new CWP forward operator. This research was
supported by the NOAA/National Environmental Satellite, Data, and
Information Service. Partial funding for this research was also provided
by NOAA/Office of Oceanic and Atmospheric Research under NOAA-University
of Oklahoma Cooperative Agreement NA17RJ1227, under the U.S. Department
of Commerce. P. Minnis and R. Palikonda are supported by the NASA
Modeling, Analysis, and Prediction (MAP) Program, the GOES-R Program,
and by the Department of Energy Atmospheric Science Research Program
under Interagency Agreement DE-SC0000991/003. (The near-real-time
satellite analyses can be accessed for a variety of domains at
http://angler.larc.nasa.gov/.)
NR 62
TC 13
Z9 13
U1 0
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD JUL
PY 2013
VL 141
IS 7
BP 2272
EP 2289
DI 10.1175/MWR-D-12-00238.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 301ET
UT WOS:000330516300008
ER
PT J
AU Kao, DL
Wong, PC
AF Kao, David L.
Wong, Pak Chung
TI Special issue of selected articles from visualization and data analysis
2012
SO INFORMATION VISUALIZATION
LA English
DT Editorial Material
C1 [Kao, David L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wong, Pak Chung] Pacific NW Natl Lab, Richland, WA 99352 USA.
RP Kao, DL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM David.L.Kao@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 1
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1473-8716
EI 1473-8724
J9 INFORM VISUAL
JI Inf. Vis.
PD JUL
PY 2013
VL 12
IS 3-4
SI SI
BP 219
EP 220
DI 10.1177/1473871613491563
PG 2
WC Computer Science, Software Engineering
SC Computer Science
GA 287WJ
UT WOS:000329572700001
ER
PT J
AU Yeh, CK
Liu, ZP
Kao, DL
Lee, TY
AF Yeh, Chih-Kuo
Liu, Zhanping
Kao, David L.
Lee, Tong-Yee
TI Animating streamlines with orthogonal advancing waves
SO INFORMATION VISUALIZATION
LA English
DT Article
DE Flow visualization; evenly spaced streamlines; animation; repeated
asymmetric patterns; color map
ID LINE INTEGRAL CONVOLUTION; FLOW VISUALIZATION; FIELDS
AB Self-animating image of flow through repeated asymmetric patterns (RAPs) is an innovative approach for creating illusory motion using a single image. In this paper, we present a smooth cyclic variable-speed RAP animation model that emulates orthogonal advancing waves from a geometry-based flow representation. It enables dense, accurate visualization of complex real-world flows using animated streamlines of an elegant placement coupled with visually appealing orthogonal advancing waves. The animation model first performs velocity (magnitude) integral luminance transition on individual streamlines. Then, inter-streamline synchronization in luminance varying along the tangential direction is imposed. Next, tangential flow streaks are constructed using evenly spaced hue differing in the orthogonal direction. In addition, an energy-decreasing strategy is proposed that adopts an iterative yet efficient procedure for determining the luminance phase and hue of each streamline in HSL (hue, saturation, and lightness or brightness) color space. To increase the contrast between flow streaks, adaptive luminance interleaving in the direction perpendicular to the flow is further applied. We demonstrate the effectiveness of the animation model using some synthetic and real flows. Color figures, images, and accompanying animations are available at http://graphics.csie.ncku.edu.tw/flowvis.
C1 [Yeh, Chih-Kuo; Lee, Tong-Yee] Natl Cheng Kung Univ, Dept Comp Sci & Informat Engn, Tainan 701, Taiwan.
[Liu, Zhanping] Kentucky State Univ, Dept Comp Sci, Frankfort, KY USA.
[Kao, David L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lee, TY (reprint author), Natl Cheng Kung Univ, Dept Comp Sci & Informat Engn, 1 Univ Rd, Tainan 701, Taiwan.
EM tonylee@mail.ncku.edu.tw
FU National Science Council, Taiwan [NSC-99-2221-E-006-066-MY3,
NSC-100-2221-E-006-188-MY3, NSC-100-2628-E-006-031-MY3]
FX This work was supported in part by the National Science Council
(contracts NSC-99-2221-E-006-066-MY3, NSC-100-2221-E-006-188-MY3 and
NSC-100-2628-E-006-031-MY3), Taiwan.
NR 23
TC 1
Z9 1
U1 0
U2 2
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1473-8716
EI 1473-8724
J9 INFORM VISUAL
JI Inf. Vis.
PD JUL
PY 2013
VL 12
IS 3-4
SI SI
BP 257
EP 272
DI 10.1177/1473871612458507
PG 16
WC Computer Science, Software Engineering
SC Computer Science
GA 287WJ
UT WOS:000329572700004
ER
PT J
AU Churnside, JH
McCarty, BJ
Lu, XM
AF Churnside, James H.
McCarty, Brandi J.
Lu, Xiaomei
TI Subsurface Ocean Signals from an Orbiting Polarization Lidar
SO REMOTE SENSING
LA English
DT Article
DE CALIPSO; CALIOP; ocean lidar; phytoplankton; polarization; lidar; ocean
color; chlorophyll
ID OCEANOGRAPHIC LIDAR; SCATTERING LAYERS; AIRBORNE LIDAR; SEA; BUBBLES;
TAIL; GULF; FISH
AB Detection of subsurface returns from the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) on the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) satellite were demonstrated. Despite the coarse range resolution of this aerosol lidar, evidence of subsurface scattering was observed as a delay and broadening of the cross-polarized signal relative to the co-polarized signal in the three near-surface range bins. These two effects contributed to an increased depolarization at the nominal depth of 25 m. These features were all correlated with near-surface chlorophyll concentrations. An increase in the depolarization was also seen at a depth of 50 m under certain conditions, suggesting that chlorophyll concentration at that depth could be estimated if an appropriate retrieval technique can be developed. At greater depths, the signal is dominated by the temporal response of the detectors, which was approximated by an analytical expression. The depolarization caused by aerosols in the atmosphere was calculated and eliminated as a possible artifact.
C1 [Churnside, James H.] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
[McCarty, Brandi J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80305 USA.
[Lu, Xiaomei] NASA, Langley Res Ctr, Hampton, VA 23666 USA.
RP Churnside, JH (reprint author), NOAA, Earth Syst Res Lab, 325 Broadway, Boulder, CO 80305 USA.
EM james.h.churnside@noaa.gov; brandi.mccarty@noaa.gov; xiaomei.lu@nasa.gov
RI Churnside, James/H-4873-2013; Manager, CSD Publications/B-2789-2015
FU NASA [NNH10AO57I]
FX This work was partially supported by NASA under project number
NNH10AO57I. CALIOP data were obtained from NASA Langley Research Center
Atmospheric Science Data Center. MODIS AQUA chlorophyll concentrations
were obtained from NASA Goddard Space Flight Center. Chlorophyll
profiles were provided by the NOAA World Ocean Database. We would like
to thank Yongxiang Hu for helpful discussions.
NR 33
TC 7
Z9 7
U1 1
U2 11
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JUL
PY 2013
VL 5
IS 7
BP 3457
EP 3475
DI 10.3390/rs5073457
PG 19
WC Remote Sensing
SC Remote Sensing
GA 274SH
UT WOS:000328626000016
ER
PT J
AU von Rosenvinge, T
Coplan, M
AF von Rosenvinge, Tycho
Coplan, Michael
TI Frank Bethune McDonald obituary
SO PHYSICS TODAY
LA English
DT Biographical-Item
C1 [von Rosenvinge, Tycho] Goddard Space Flight Ctr, Greenbelt, MD USA.
[Coplan, Michael] Univ Maryland, College Pk, MD 20742 USA.
RP von Rosenvinge, T (reprint author), Goddard Space Flight Ctr, Greenbelt, MD USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0031-9228
EI 1945-0699
J9 PHYS TODAY
JI Phys. Today
PD JUL
PY 2013
VL 66
IS 7
BP 61
EP 62
PG 2
WC Physics, Multidisciplinary
SC Physics
GA 252RP
UT WOS:000327027700021
ER
PT J
AU Allen, CC
AF Allen, Carlton C.
TI ADVANCED CURATION OF CURRENT AND FUTURE EXTRATERRESTRIAL SAMPLES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Allen, Carlton C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM carlton.c.allen@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A43
EP A43
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800013
ER
PT J
AU Aoyagi, Y
Mikouchi, T
Goodrich, CA
Zolensky, ME
AF Aoyagi, Y.
Mikouchi, T.
Goodrich, C. A.
Zolensky, M. E.
TI MINERALOGY OF GRAIN BOUNDARY METAL IN UREILITIC FRAGMENTS OF ALMAHATA
SITTA
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Aoyagi, Y.; Mikouchi, T.] Univ Tokyo, Dept Earth & Planet Sci, Tokyo 1130033, Japan.
[Goodrich, C. A.] Planet Sci Inst, Tucson, AZ 85719 USA.
[Zolensky, M. E.] NASA JSC, Houston, TX 77058 USA.
EM aoyagi@eps.s.u-tokyo.ac.jp
NR 5
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A46
EP A46
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800016
ER
PT J
AU Bell, MS
AF Bell, M. S.
TI CONSTRAINING ALTERATION CONDITIONS ON MARS FROM EXPERIMENTALLY SHOCKED
AND ALTERED BASALT
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Bell, M. S.] Jacobs NASA, Lyndon B Johnson Space Ctr, Houston, TX USA.
EM msbell@nasa.gov
NR 7
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A53
EP A53
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800023
ER
PT J
AU Bigolski, JN
Frank, DR
Zolensky, ME
Weisberg, MK
Ebel, DS
Rahman, Z
AF Bigolski, J. N.
Frank, D. R.
Zolensky, M. E.
Weisberg, M. K.
Ebel, D. S.
Rahman, Z.
TI A MICROANALYTICAL (TEM) STUDY OF FINE-GRAINED CHOND RULE RIMS IN NWA
5717.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Bigolski, J. N.; Weisberg, M. K.] CUNY, Kingsborough Coll, Dept Phys Sci, Bklyn, NY 11235 USA.
[Bigolski, J. N.; Weisberg, M. K.] CUNY, Grad Ctr, Dept Earth & Envi Sci, New York, NY 10016 USA.
[Bigolski, J. N.; Weisberg, M. K.; Ebel, D. S.] Amer Museum Nat Hist, Dept Earth & Planet Sci, New York, NY 10024 USA.
[Frank, D. R.; Rahman, Z.] NASA, Lyndon B Johnson Space Ctr, ESCG, Houston, TX 77058 USA.
[Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A59
EP A59
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800029
ER
PT J
AU Calaway, MJ
Allen, CC
Allton, JH
AF Calaway, M. J.
Allen, C. C.
Allton, J. H.
TI REDUCING ORGANIC CONTAMINATION IN NASA JSC ASTROMATERIAL CURATION
FACILITY.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Calaway, M. J.] NASA Johnson Space Ctr, Jacobs Technol JETS, Astromat Acquisit & Curat Off, Houston, TX USA.
[Allen, C. C.; Allton, J. H.] NASA Johnson Space Ctr, Astromat Acquisit & Curat Off, Houston, TX USA.
EM mi-chael.calaway@nasa.gov
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A80
EP A80
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800050
ER
PT J
AU Calaway, MJ
Allen, CC
AF Calaway, M. J.
Allen, C. C.
TI CRYOGENIC CURATION: ISOLATION TECHNOLOGY AND MISSION OPERATIONAL
REQUIREMENTS FOR SAMPLE RETURN.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Calaway, M. J.] NASA Johnson Space Ctr, Jacobs Technol JETS, Astromat Acquisit & Curat Off, Houston, TX USA.
[Allen, C. C.] NASA Johnson Space Ctr, Astromat Acquisit & Curat Off, Houston, TX USA.
EM michael.calaway@nasa.gov
NR 1
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A79
EP A79
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800049
ER
PT J
AU Evans, CA
Todd, NS
Allen, CC
AF Evans, C. A.
Todd, N. S.
Allen, C. C.
TI ASTROMATERIALS INFORMATICS-AN INTEGRAL COMPONENT OF ADVANCED CURATION OF
EXTRATERRESTRIAL SAMPLES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Evans, C. A.; Allen, C. C.] NASA, Lyndon B Johnson Space Ctr, MC KT, Houston, TX 77058 USA.
[Todd, N. S.] NASA, Lyndon B Johnson Space Ctr, Jacobs JETS, Houston, TX 77058 USA.
EM Cindy.evans-l@nasa.gov
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A115
EP A115
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800085
ER
PT J
AU Flynn, GJ
Wirick, S
Keller, LP
AF Flynn, George J.
Wirick, Sue
Keller, Lindsay P.
TI A CARBON-XANES STUDY OF IDP ORGANIC DIVERSITY: EVIDENCE FOR MULTIPLE
SOURCES OF EARLY SOLAR SYSTEM ORGANIC MATTER
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID INTERPLANETARY DUST
C1 [Flynn, George J.] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA.
[Wirick, Sue] Univ Chicago, CARS, Chicago, IL 60637 USA.
[Keller, Lindsay P.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A126
EP A126
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800096
ER
PT J
AU Frank, DR
Zolensky, ME
Le, L
AF Frank, D. R.
Zolensky, M. E.
Le, L.
TI DECIPHERING KBO FROM ASTEROIDAL MATERIAL: WHAT OLIVINE AND PYROXENE
COMPOSITIONS FROM WILD 2 AND CHONDRITE MATRIX REVEAL.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Frank, D. R.; Le, L.] NASA, JETS, Johnson Space Ctr, Houston, TX USA.
[Zolensky, M. E.] NASA, ARES, Johnson Space Ctr, Houston, TX USA.
EM david.r.frank@nasa.gov
NR 8
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A131
EP A131
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800101
ER
PT J
AU Hallis, LJ
Huss, GR
Taylor, GJ
Nagashima, K
Halldorsson, SA
Hilton, DR
Sobolev, N
AF Hallis, L. J.
Huss, G. R.
Taylor, G. J.
Nagashima, K.
Halldorsson, S. A.
Hilton, D. R.
Sobolev, N.
TI THE D/H RATIO OF THE EARTH'S DEEP MANTLE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Hallis, L. J.; Huss, G. R.; Taylor, G. J.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Hallis, L. J.; Huss, G. R.; Taylor, G. J.; Nagashima, K.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Halldorsson, S. A.; Hilton, D. R.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92037 USA.
[Sobolev, N.] Russsian Acad Sci, Siberian Branch, Sobolev Inst Geol & Mineral, Novosibirsk 630090, Russia.
RI Halldorsson, Saemundur/L-9560-2015
OI Halldorsson, Saemundur/0000-0002-9311-7704
NR 11
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A152
EP A152
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800122
ER
PT J
AU Joy, KH
Messenger, S
Zolensky, ME
Frank, DR
Kring, DA
AF Joy, K. H.
Messenger, S.
Zolensky, M. E.
Frank, D. R.
Kring, D. A.
TI BENCH CRATER METEORITE: HYDRATED ASTEROIDAL MATERIAL DELIVERED TO THE
MOON
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID WATER
C1 [Joy, K. H.; Kring, D. A.] Univ Manchester, SEAES, Manchester M13 9PL, Lancs, England.
[Joy, K. H.; Kring, D. A.] LPI USRA, CLSE, Houston, TX 77058 USA.
[Messenger, S.; Zolensky, M. E.; Frank, D. R.] NASA Johnson Space Ctr, ARES, Houston, TX 77058 USA.
EM Katherine.Joy@manchester.ac.uk
NR 8
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A195
EP A195
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800165
ER
PT J
AU Keller, LP
Needham, AW
Messenger, S
AF Keller, L. P.
Needham, A. W.
Messenger, S.
TI A FIB/TEM STUDY OF A COMPLEX WARK-LOVERING RIM ON A VIGARANO CAI
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID SOLAR NEBULA
C1 [Keller, L. P.; Messenger, S.] NASA JSC, Robert M Walker Lab Space Sci, Code KR, ARES, Houston, TX 77058 USA.
[Needham, A. W.] LPI, Houston, TX 77058 USA.
EM Lind-say.P.Keller@nasa.gov
NR 7
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A197
EP A197
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800167
ER
PT J
AU Kring, DA
Swindle, TD
Zolensky, ME
AF Kring, D. A.
Swindle, T. D.
Zolensky, M. E.
TI BRECCIATED CHELYABINSK NEAR-EARTH ASTEROID AND ITS CATASTROPHIC AIR
BURST
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID ITOKAWA
C1 [Kring, D. A.] Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX USA.
[Zolensky, M. E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM kring@lpi.usra.edu
NR 7
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A211
EP A211
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800181
ER
PT J
AU Liu, Y
Day, JMD
Ma, C
Hand, KP
Pokhilenko, NP
Taylor, LA
AF Liu, Y.
Day, J. M. D.
Ma, C.
Hand, K. P.
Pokhilenko, N. P.
Taylor, L. A.
TI CHELYABINSK: AN ORDINARY CHONDRITE FROM A SPECTACULAR FALL IN RUSSIA
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Liu, Y.; Hand, K. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Day, J. M. D.] UCSD, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Ma, C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Pokhilenko, N. P.] Russian Acad Sci, Siberian Branch, Novosibirsk, Russia.
[Taylor, L. A.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
EM yangliu@jpl.nasa.gov
RI Pokhilenko, Nikolay/B-3211-2014
NR 1
TC 1
Z9 1
U1 0
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A225
EP A225
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800195
ER
PT J
AU Mane, P
Wadhwa, M
Keller, LP
AF Mane, P.
Wadhwa, M.
Keller, L. P.
TI TRACE ELEMENT ABUNDANCES IN AN UNUSUAL HIBONITE-PEROVSKITE REFRACTORY
INCLUSION FROM ALLENDE
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID CHONDRITE
C1 [Mane, P.; Wadhwa, M.] Arizona State Univ, Ctr Meteorite Studies, Tempe, AZ 85287 USA.
[Keller, L. P.] NASA, Robert M Walker Lab Space Sci, Code KR, ARES,JSC, Houston, TX 77058 USA.
EM Prajkta.Mane@asu.edu
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 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A231
EP A231
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800201
ER
PT J
AU Mikouchi, T
Aoyagi, Y
Goodrich, CA
Yubuta, K
Sugiyama, K
Zolensky, ME
Goldstein, JI
AF Mikouchi, T.
Aoyagi, Y.
Goodrich, C. A.
Yubuta, K.
Sugiyama, K.
Zolensky, M. E.
Goldstein, J. I.
TI COOLING HISTORY OF ALMAHATA SITTA UREILITE AS INFERRED FROM TRANSMISSION
ELECTRON MICROSCOPY OF IRON METAL
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Mikouchi, T.; Aoyagi, Y.] Univ Tokyo, Dept Earth & Planet Sci, Tokyo 1130033, Japan.
[Goodrich, C. A.] Planet Sci Inst, Tucson, AZ 85719 USA.
[Yubuta, K.; Sugiyama, K.] Tohoku Univ, Inst Mat Res, Sendai, Miyagi 9808577, Japan.
[Zolensky, M. E.] NASA, ARES, JSC, Houston, TX 77058 USA.
[Goldstein, J. I.] Univ Massachusetts, Amherst, MA 01003 USA.
EM mikouchi@eps.s.u-tokyo.ac.jp
RI Yubuta, Kunio/B-8124-2011; Sugiyama, Kazumasa/B-3447-2010
OI Yubuta, Kunio/0000-0002-3401-6874;
NR 5
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A247
EP A247
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800217
ER
PT J
AU Mittlefehldt, DW
Mertzman, SA
Peng, ZX
Mertzman, KR
AF Mittlefehldt, D. W.
Mertzman, S. A.
Peng, Z. X.
Mertzman, K. R.
TI PETROLOGIC AND CHEMICAL CHARACTERIZATION OF A SUITE OF ANTARCTIC
DIOGENITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID GENESIS
C1 [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Mertzman, S. A.; Mertzman, K. R.] Franklin & Marshall Coll, Lancaster, PA 17604 USA.
[Peng, Z. X.] Engn & Sci Contract Grp, Houston, TX USA.
EM david.w.mittlefehldt@nasa.gov
NR 6
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A250
EP A250
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800220
ER
PT J
AU Mittlefehldt, DW
Ammannito, E
Hiroi, T
De Angelis, S
Di Iorio, T
Pieters, CM
De Sanctis, MC
AF Mittlefehldt, D. W.
Ammannito, E.
Hiroi, T.
De Angelis, S.
Di Iorio, T.
Pieters, C. M.
De Sanctis, M. C.
TI TOWARDS CALIBRATING THE VESTAN REGOLITH: CORRELATING THE PETROLOGY,
CHEMISTRY AND SPECTROSCOPY OF HOWARDITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Ammannito, E.; De Angelis, S.; Di Iorio, T.; De Sanctis, M. C.] INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy.
[Hiroi, T.; Pieters, C. M.] Brown Univ, Providence, RI 02912 USA.
EM da-vid.w.mittlefehldt@nasa.gov
RI De Sanctis, Maria Cristina/G-5232-2013; Di Iorio, Tatiana/O-8700-2015
OI De Sanctis, Maria Cristina/0000-0002-3463-4437; Di Iorio,
Tatiana/0000-0001-8872-8917
NR 6
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A249
EP A249
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800219
ER
PT J
AU Nakamura-Messenger, K
Clemett, SJ
Nguyen, AN
Berger, EL
Keller, LP
Messenger, S
AF Nakamura-Messenger, K.
Clemett, S. J.
Nguyen, A. N.
Berger, E. L.
Keller, L. P.
Messenger, S.
TI SYSTEMATIC EXAMINATION OF STARDUST BULBOUS TRACK WALL MATERIALS.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID COMET 81P/WILD-2; MINERALOGY; PARTICLES
C1 [Nakamura-Messenger, K.; Clemett, S. J.; Nguyen, A. N.; Berger, E. L.; Keller, L. P.; Messenger, S.] JETS, Houston, TX USA.
[Nakamura-Messenger, K.; Clemett, S. J.; Nguyen, A. N.] NASA JSC, Robert M Walker Lab Space Sci, Houston, TX USA.
EM kei-ko.nakamura-1@nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A259
EP A259
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800229
ER
PT J
AU Needham, AW
Messenger, S
Keller, LP
AF Needham, A. W.
Messenger, S.
Keller, L. P.
TI OXYGEN ISOTOPE MAPPING OF THE INTERIOR AND RIM OF A MASS DEPENDENTLY
FRACTIONATED CAI.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID SOLAR NEBULA
C1 [Needham, A. W.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Needham, A. W.; Messenger, S.; Keller, L. P.] NASA JSC, Robert M Walker Lab Space Sci, ARES, Houston, TX 77058 USA.
EM andrew.w.needham@nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A261
EP A261
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800231
ER
PT J
AU Norman, MD
Nemchin, AA
Grange, ML
Zeigler, RA
Whitehouse, MJ
Muhling, JR
Merle, RE
AF Norman, M. D.
Nemchin, A. A.
Grange, M. L.
Zeigler, R. A.
Whitehouse, M. J.
Muhling, J. R.
Merle, R. E.
TI U-PB AGES AND COMPOSITIONS OF APOLLO 14 REGOLITH GLASSES.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID IMPACT GLASSES
C1 [Norman, M. D.] Australian Natl Univ, RSES, Canberra, ACT 0200, Australia.
[Nemchin, A. A.; Grange, M. L.; Merle, R. E.] Curtin Univ, Bentley, WA 6845, Australia.
[Zeigler, R. A.] NASA JSC, Houston, TX 77058 USA.
[Whitehouse, M. J.] Swedish Museum Nat Hist, S-10405 Stockholm, Sweden.
[Muhling, J. R.] Univ Western Australia, Crawley, WA 6009, Australia.
EM marc.norman@anu.edu.au
RI Muhling, Janet/C-4687-2011
OI Muhling, Janet/0000-0003-1890-9119
NR 5
TC 0
Z9 0
U1 0
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A267
EP A267
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800237
ER
PT J
AU Nuevo, M
Sandford, SA
Flynn, GJ
Wirick, S
AF Nuevo, M.
Sandford, S. A.
Flynn, G. J.
Wirick, S.
TI MID-INFRARED STUDY OF STONES FROM THE SUTTER'S MILL METEORITE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Nuevo, M.; Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Nuevo, M.] SETI Inst, Mountain View, CA USA.
[Flynn, G. J.] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA.
[Wirick, S.] Univ Chicago, CARS, Chicago, IL 60637 USA.
EM michel.nuevo-1@nasa.gov
NR 2
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A268
EP A268
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800238
ER
PT J
AU Nuth, JA
Paquette, JA
Johnson, NM
AF Nuth, J. A.
Paquette, J. A.
Johnson, N. M.
TI CO SELF SHIELDING AS A MECHANISM TO MAKE O-16 ENRICHED SOLIDS IN THE
SOLAR NEBULA.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID OXYGEN-ISOTOPIC COMPOSITION; SYSTEM; METEORITES; ORIGIN; DUST
C1 [Nuth, J. A.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Paquette, J. A.; Johnson, N. M.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Paquette, J. A.] NASA, Greenbelt, MD 20771 USA.
EM joseph.a.nuth@nasa.gov
RI Johnson, Natasha/E-3093-2012
NR 15
TC 0
Z9 0
U1 2
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A269
EP A269
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800239
ER
PT J
AU Nyquist, LE
Shih, CY
Peng, ZX
Agee, C
AF Nyquist, L. E.
Shih, C. -Y.
Peng, Z. X.
Agee, C.
TI NWA 7034 MARTIAN BRECCIA: DISTURBED Rb-Sr SYSTEMATICS, PRELIMINARY
similar to 4.4 Ga Sm-Nd AGE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Nyquist, L. E.] NASA Johnson Space Ctr, KR, Houston, TX 77058 USA.
[Shih, C. -Y.; Peng, Z. X.] NASA JSC JETS, Houston, TX 77058 USA.
[Agee, C.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
[Agee, C.] Univ New Mexico, Dept Earth Planet Sci, Albuquerque, NM 87131 USA.
EM lau-rence.e.nyquist@nasa.gov
NR 2
TC 1
Z9 1
U1 1
U2 8
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A270
EP A270
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800240
ER
PT J
AU Paquette, JA
Nuth, JA
AF Paquette, J. A.
Nuth, J. A.
TI HOW MUCH DUST IS PROCESSED BY A SINGLE LIGHTNING BOLT IN THE PROTO-SOLAR
NEBULA?
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Paquette, J. A.; Nuth, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM john.a.paquette@nasa.gov
NR 5
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A276
EP A276
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800246
ER
PT J
AU Park, J
Herzog, GF
Nyquist, LE
Shih, CY
Turrin, B
Lindsay, FN
Delaney, JS
Swisher, CC
Agee, C
AF Park, J.
Herzog, G. F.
Nyquist, L. E.
Shih, C. -Y.
Turrin, B.
Lindsay, F. N.
Delaney, J. S.
Swisher, C. C., III
Agee, C.
TI Ar-Ar AND Rb-Sr AGES OF THE TISSINT OLIVINE- PHYRIC MARTIAN SHERGOTTITE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Park, J.; Herzog, G. F.; Turrin, B.; Lindsay, F. N.; Delaney, J. S.; Swisher, C. C., III] Rutgers State Univ, Piscataway, NJ 08854 USA.
[Park, J.; Herzog, G. F.; Lindsay, F. N.; Delaney, J. S.] Dept Chem & Chem Biol, Houston, TX 77058 USA.
[Park, J.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Nyquist, L. E.] KR NASA Johnson Space Ctr, Houston, TX 77058 USA.
[Shih, C. -Y.] NASA JSC JETS, Houston, TX 77058 USA.
[Turrin, B.; Swisher, C. C., III; Agee, C.] Univ New Mexico, Dept Earth Planet Sci, Albuquerque, NM 87131 USA.
[Agee, C.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
EM jisun.park@rutgers.edu
NR 10
TC 0
Z9 0
U1 1
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A279
EP A279
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800249
ER
PT J
AU Pillinger, CT
Greenwood, RC
Gibson, JM
Gibson, EK
AF Pillinger, C. T.
Greenwood, R. C.
Gibson, J. M.
Gibson, E. K.
TI WEATHERING EFFECTS IN THE HOLBROOK METEORITE AND THEIR POSSIBLE REMOVAL
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Pillinger, C. T.; Greenwood, R. C.; Gibson, J. M.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Gibson, E. K.] NASA, Astromat Res Off, KR, Johnson Space Ctr, Houston, TX 77058 USA.
EM c.t.pillinger@open.ac.uk
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A282
EP A282
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800252
ER
PT J
AU Righter, K
Harrington, R
Schroder, C
Morris, RV
AF Righter, K.
Harrington, R.
Schroeder, C.
Morris, R. V.
TI NON-DESTRUCTIVE CLASSIFICATION APPROACHES FOR EQUILIBRATED ORDINARY
CHONDRITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Righter, K.; Morris, R. V.] NASA, JSC, Houston, TX 77058 USA.
[Harrington, R.] NASA, Jacobs Technol, JSC, Houston, TX 77058 USA.
[Schroeder, C.] Univ Stirling, Stirling FK9 4LA, Scotland.
EM kevin.righter-1@nasa.gov
RI Schroder, Christian/B-3870-2009
OI Schroder, Christian/0000-0002-7935-6039
NR 4
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A297
EP A297
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800267
ER
PT J
AU Righter, K
Nakamura-Messenger, K
Lauretta, DS
AF Righter, K.
Nakamura-Messenger, K.
Lauretta, D. S.
CA OSIRIS-REx Curation Working Grp
TI CURATION OF OSIRIS-REx ASTEROID SAMPLES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Righter, K.] NASA, JSC, Houston, TX 77058 USA.
[Nakamura-Messenger, K.] NASA, Jacobs Technol, JSC, Houston, TX 77058 USA.
[Lauretta, D. S.] Univ Arizona, LPL, Tucson, AZ 85721 USA.
NR 4
TC 1
Z9 1
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A298
EP A298
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800268
ER
PT J
AU Righter, K
Fries, MD
Gibson, EK
Harrington, R
Keller, LP
McCoy, TJ
Morris, RV
Nagao, K
Nakamura-Messenger, K
Niles, P
Nyquist, L
Park, J
Peng, ZX
Shih, CY
Simon, JI
Zeigler, RA
AF Righter, K.
Fries, M. D.
Gibson, E. K.
Harrington, R.
Keller, L. P.
McCoy, T. J.
Morris, R. V.
Nagao, K.
Nakamura-Messenger, K.
Niles, P.
Nyquist, L.
Park, J.
Peng, Z. X.
Shih, C-Y
Simon, J. I.
Zeigler, R. A.
TI CONSORTIUM STUDY OF THE CHELYABINSK METEORITE
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Righter, K.; Fries, M. D.; Gibson, E. K.; Keller, L. P.; Morris, R. V.; Niles, P.; Nyquist, L.; Simon, J. I.; Zeigler, R. A.] NASA, JSC, Houston, TX 77058 USA.
[Harrington, R.; Nakamura-Messenger, K.; Peng, Z. X.; Shih, C-Y] NASA, JSC, JETS, Houston, TX 77058 USA.
[McCoy, T. J.] Smithsonian Inst, Washington, DC 20560 USA.
[Nagao, K.] Univ Tokyo, Earthquake Chem Lab, Bunkyo Ku, Tokyo 1130033, Japan.
[Park, J.] Rutgers State Univ, Dept Chem, Wright Labs, Piscataway, NJ USA.
NR 2
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A296
EP A296
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800266
ER
PT J
AU Sandford, SA
Nuevo, M
Elsila, JE
AF Sandford, S. A.
Nuevo, M.
Elsila, J. E.
TI PHOTO-INDUCED DEUTERIUM ENRICHMENT IN A RESIDUE PRODUCED FROM THE UV
IRRADIATION OF PYRIMIDINE IN H2O+NH3 ICES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID ULTRAVIOLET PHOTOIRRADIATION
C1 [Sandford, S. A.; Nuevo, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Nuevo, M.] SETI Inst, Mountain View, CA USA.
[Elsila, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Scott.A.Sandford@nasa.gov
RI Elsila, Jamie/C-9952-2012
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A305
EP A305
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800275
ER
PT J
AU Sears, DWG
AF Sears, D. W. G.
TI TWO MAJOR NEW FINDS OF ANTARCTIC CO CHONDRITES (DOM 08004 AND MIL
07531): THEIR ORBITS, TERRESTRIAL AGE, AND PETROGRAPHIC TYPE.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Sears, D. W. G.] NASA, Ames Res Ctr, BAER Inst, Mountain View, CA 94035 USA.
EM Derek.Sears@NASA.gov
NR 6
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A313
EP A313
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800283
ER
PT J
AU Smith, T
Nakamura-Messenger, K
Messenger, S
Keller, LP
Khodja, H
Raepsaet, C
Wirick, S
Flynn, GJ
Taylor, S
Engrand, C
Duprat, J
Herzog, GF
AF Smith, T.
Nakamura-Messenger, K.
Messenger, S.
Keller, L. P.
Khodja, H.
Raepsaet, C.
Wirick, S.
Flynn, G. J.
Taylor, S.
Engrand, C.
Duprat, J.
Herzog, G. F.
TI C/N AND OTHER ELEMENTAL RATIOS OF CHONDRITIC POROUS IDPS AND A FLUFFY
CONCORDIA MICROMETEORITE
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID SNOW
C1 [Smith, T.; Khodja, H.; Raepsaet, C.] CEA Saclay, Gif Sur Yvette, France.
[Smith, T.] U Bern, Bern, Switzerland.
[Nakamura-Messenger, K.; Messenger, S.; Keller, L. P.] NASA JSC, Houston, TX 77058 USA.
[Wirick, S.] U Chicago, CARS, Chicago, IL 60637 USA.
[Flynn, G. J.] SUNY Coll Plattsburgh, Plattsburgh, NY 12901 USA.
[Taylor, S.] CRREL, Hanover, NH 03755 USA.
[Engrand, C.; Duprat, J.] U Paris Sud, CSNSM CNRS, Orsay, France.
[Herzog, G. F.] Rutgers U, Piscataway, NJ 08854 USA.
RI Khodja, Hicham/A-1869-2016
NR 8
TC 0
Z9 0
U1 0
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A322
EP A322
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800292
ER
PT J
AU Telus, M
Huss, GR
Nagashima, K
Ogliore, RC
Chen, JH
Papanastassiou, DA
AF Telus, M.
Huss, G. R.
Nagashima, K.
Ogliore, R. C.
Chen, J. H.
Papanastassiou, D. A.
TI 60Fe-60Ni SYSTEMATICS OF CHONDRULES FROM UOC QUE97008: COMPARING RESULTS
FROM IN SITU AND BULK ANALYSES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID RATIO ESTIMATION
C1 [Telus, M.; Huss, G. R.; Nagashima, K.; Ogliore, R. C.] Univ Hawaii Manoa, HIGP, Honolulu, HI 96822 USA.
[Chen, J. H.; Papanastassiou, D. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM telus@higp.hawaii.edu
NR 7
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A336
EP A336
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800306
ER
PT J
AU Thomas-Keprta, KL
Clemett, S
Ross, DK
Le, L
Rahman, Z
McKay, DS
Gibson, EK
Gonzalez, C
AF Thomas-Keprta, K. L.
Clemett, S.
Ross, D. K.
Le, L.
Rahman, Z.
McKay, D. S.
Gibson, E. K.
Gonzalez, C.
TI ALLOCHTHONOUS ADDITION OF METEORITIC ORGANICS TO THE LUNAR REGOLITH
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Thomas-Keprta, K. L.; Clemett, S.; Ross, D. K.; Le, L.; Rahman, Z.; Gonzalez, C.] JETS NASA JSC, Houston, TX 77058 USA.
[Gibson, E. K.] NASA JSC, Houston, TX 77058 USA.
EM kathie.thomas-keprta-1@nasa.gov
NR 3
TC 0
Z9 0
U1 0
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A338
EP A338
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800308
ER
PT J
AU Todd, NS
Satterwhite, CE
Righter, K
AF Todd, N. S.
Satterwhite, C. E.
Righter, K.
TI Enhancements to the Antarctic Meteorite Classification and Petrographic
Database Update
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Todd, N. S.; Satterwhite, C. E.] NASA, Lyndon B Johnson Space Ctr, Jacobs JETS, MC KT, Houston, TX 77058 USA.
[Righter, K.] NASA, Lyndon B Johnson Space Ctr, MC KT, Houston, TX 77058 USA.
EM nan-cy.s.todd@nasa.gov
NR 3
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A341
EP A341
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800311
ER
PT J
AU Velbel, MA
Tonui, EK
Zolensky, ME
AF Velbel, M. A.
Tonui, E. K.
Zolensky, M. E.
TI COMPOSITIONS OF PARTLY ALTERED OLIVINE AND REPLACEMENT SERPENTINE IN THE
CM2 CHONDRITE QUE 93005
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Velbel, M. A.] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA.
[Tonui, E. K.] BP Amer Inc, Houston, TX USA.
[Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Off, Houston, TX 77058 USA.
EM velbel@msu.edu
NR 0
TC 1
Z9 1
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A360
EP A360
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800330
ER
PT J
AU Yada, T
Zolensky, ME
Abe, M
Okada, T
Uesugi, M
Karouji, Y
Ishibashi, Y
AF Yada, T.
Zolensky, M. E.
Abe, M.
Okada, T.
Uesugi, M.
Karouji, Y.
Ishibashi, Y.
TI A CONSORTIUM STUDY OF A POSSIBLE ITOKAWA PARTICLE BEARING HALITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
ID ORDINARY CHONDRITES; HAYABUSA SAMPLES; DUST PARTICLES; REGOLITH; GASES
C1 [Yada, T.; Abe, M.; Okada, T.; Uesugi, M.; Karouji, Y.; Ishibashi, Y.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Zolensky, M. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM yada@planeta.sci.isas.jaxa.jp
NR 12
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A380
EP A380
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800350
ER
PT J
AU Zeigler, RA
Righter, K
Allen, CC
AF Zeigler, R. A.
Righter, K.
Allen, C. C.
TI Nondestructive Analysis of Astromaterials by Micro-CT and Micro-XRF
Analysis for PET Examination
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Zeigler, R. A.; Righter, K.; Allen, C. C.] NASA JSC, Houston, TX 77058 USA.
EM ryan.a.zeigler@nasa.gov
NR 2
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A388
EP A388
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800358
ER
PT J
AU Zolensky, M
Fries, M
Bodnar, R
Yurimoto, H
Itoh, S
Steele, A
Mikouchi, T
Hagiya, K
Ohsumi, K
Le, L
Rahman, Z
AF Zolensky, M.
Fries, M.
Bodnar, R.
Yurimoto, H.
Itoh, S.
Steele, A.
Mikouchi, T.
Hagiya, K.
Ohsumi, K.
Le, L.
Rahman, Z.
TI EARLY SOLAR SYSTEM CRYOVOLCANICS IN THE LABORATORY
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 76th Annual Meeting of the Meteoritical-Society
CY JUL 29-AUG 02, 2013
CL Edmonton, CANADA
SP Meteorit Soc
C1 [Zolensky, M.; Fries, M.] NASA JSC, Houston, TX USA.
[Bodnar, R.] Virginia Tech, Blacksburg, VA USA.
[Yurimoto, H.; Itoh, S.] Hokkaido Univ, Sapporo, Hokkaido 060, Japan.
[Steele, A.] Carnegie Inst Sci, Washington, DC 20005 USA.
[Mikouchi, T.] Univ Tokyo, Tokyo 1138654, Japan.
[Hagiya, K.] Univ Hyogo, Kobe, Hyogo 6500044, Japan.
[Le, L.; Rahman, Z.] JETS NASA, Houston, TX USA.
EM michael.e.-zolensky@nasa.gov
NR 11
TC 0
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U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2013
VL 48
SU 1
SI SI
BP A392
EP A392
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 237JN
UT WOS:000325865800362
ER
PT J
AU Bezirgiannidis, N
Burleigh, S
Tsaoussidis, V
AF Bezirgiannidis, Nikolaos
Burleigh, Scott
Tsaoussidis, Vassilis
TI Delivery Time Estimation for Space Bundles
SO IEEE TRANSACTIONS ON AEROSPACE AND ELECTRONIC SYSTEMS
LA English
DT Article
ID WEIGHTED MOVING AVERAGES; PROTOCOL; LINKS
AB We present a method for predicting delivery time of bundles in space internetworks. The bundle delivery time estimation (BDTE) tool exploits contact graph routing (CGR), predicts bundle route, and calculates plausible arrival times along with the corresponding probabilities. Latency forecasts are performed in an administrative node with access to an instrumentation database (DB) appropriate for statistical processing. Through both analysis and experimentation, we demonstrate that estimates of bundle earliest plausible delivery time and destination arrival probabilities can be provided.
C1 [Bezirgiannidis, Nikolaos; Tsaoussidis, Vassilis] Democritus Univ Thrace, Dept Elect & Comp Engn, GR-67100 Xanthi, Greece.
[Burleigh, Scott] Jet Prop Lab, Pasadena, CA 91101 USA.
RP Bezirgiannidis, N (reprint author), Democritus Univ Thrace, Dept Elect & Comp Engn, Bldg A,Kimmeria Campus, GR-67100 Xanthi, Greece.
EM nbezirgi@ee.duth.gr
FU European Community [FP7/2007-2013_FP7-REGPOT-2010-1, 264226]; National
Aeronautics and Space Administration
FX The research leading to these results received funding from the European
Community's Seventh Framework Programme
(FP7/2007-2013_FP7-REGPOT-2010-1, SP4 Capacities, Coordination and
Support Actions) under Grant Agreement 264226 (project title: Space
Internetworking Center-SPICE). Also, some of the research described in
this paper was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 22
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U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9251
EI 1557-9603
J9 IEEE T AERO ELEC SYS
JI IEEE Trans. Aerosp. Electron. Syst.
PD JUL
PY 2013
VL 49
IS 3
BP 1897
EP 1910
PG 14
WC Engineering, Aerospace; Engineering, Electrical & Electronic;
Telecommunications
SC Engineering; Telecommunications
GA 235ZG
UT WOS:000325761900033
ER
PT J
AU Brown, CA
AF Brown, Clifford A.
TI Jet-Surface Interaction Test: Far-Field Noise Results
SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE
ASME
LA English
DT Article
ID TRAILING-EDGE; TURBULENT-FLOW; AERODYNAMIC NOISE; SOUND
AB Many configurations proposed for the next generation of aircraft rely on the wing or other aircraft surfaces to shield the engine noise from the observers on the ground. However, the ability to predict the shielding effect and any new noise sources that arise from the high-speed jet flow interacting with a hard surface is currently limited. Furthermore, quality experimental data from jets with surfaces nearby suitable for developing and validating noise prediction methods are usually tied to a particular vehicle concept and, therefore, very complicated. The Jet-Surface Interaction Tests are intended to supply a high quality set of data covering a wide range of surface geometries and positions and jet flows to researchers developing aircraft noise prediction tools. The initial goal is to measure the noise of a jet near a simple planar surface while varying the surface length and location in order to: (1) validate noise prediction schemes when the surface is acting only as a jet noise shield and when the jet-surface interaction is creating additional noise, and (2) determine regions of interest for future, more detailed, tests. To meet these objectives, a flat plate was mounted on a two-axis traverse in two distinct configurations: (1) as a shield between the jet and the observer and (2) as a reflecting surface on the opposite side of the jet from the observer. The surface length was varied between 2 and 20 jet diameters downstream of the nozzle exit. Similarly, the radial distance from the jet centerline to the surface face was varied between 1 and 16 jet diameters. Far-field and phased array noise data were acquired at each combination of surface length and radial location using two nozzles operating at jet exit conditions across several flow regimes: subsonic cold, subsonic hot, underexpanded, ideally expanded, and overexpanded supersonic. The far-field noise results, discussed here, show where the jet noise is partially shielded by the surface and where jet-surface interaction noise dominates the low frequency spectrum as a surface extends downstream and approaches the jet plume.
C1 NASA, Acoust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Brown, CA (reprint author), NASA, Acoust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Clifford.A.Brown@nasa.gov
FU NASA
FX This work was supported by the NASA Fundamental Aeronautics Program,
Subsonic Fixed Wing Project. Special thanks to James Bridges for
reviewing the work and to the staff at the AAPL for their work on this
project.
NR 24
TC 4
Z9 4
U1 1
U2 5
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0742-4795
EI 1528-8919
J9 J ENG GAS TURB POWER
JI J. Eng. Gas. Turbines Power-Trans. ASME
PD JUL
PY 2013
VL 135
IS 7
AR 071201
DI 10.1115/1.4023605
PG 7
WC Engineering, Mechanical
SC Engineering
GA 241HL
UT WOS:000326157000001
ER
PT J
AU Simon, DL
Armstrong, JB
AF Simon, Donald L.
Armstrong, Jeffrey B.
TI An Integrated Approach for Aircraft Engine Performance Estimation and
Fault Diagnostics
SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE
ASME
LA English
DT Article
AB A Kalman filter-based approach for integrated on-line aircraft engine performance estimation and gas path fault diagnostics is presented. This technique is specifically designed for underdetermined estimation problems where there are more unknown system parameters representing deterioration and faults than available sensor measurements. A previously developed methodology is applied to optimally design a Kalman filter to estimate a vector of tuning parameters, appropriately sized to enable estimation. The estimated tuning parameters can then be transformed into a larger vector of health parameters representing system performance deterioration and fault effects. The results of this study show that basing fault isolation decisions solely on the estimated health parameter vector does not provide ideal results. Furthermore, expanding the number of the health parameters to address additional gas path faults causes a decrease in the estimation accuracy of those health parameters representative of turbomachinery performance deterioration. However, improved fault isolation performance is demonstrated through direct analysis of the estimated tuning parameters produced by the Kalman filter. This was found to provide equivalent or superior accuracy compared to the conventional fault isolation approach based on the analysis of sensed engine outputs, while simplifying online implementation requirements. Results from the application of these techniques to an aircraft engine simulation are presented and discussed.
C1 [Simon, Donald L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Armstrong, Jeffrey B.] ASRC Aerosp Corp, Cleveland, OH 44135 USA.
RP Simon, DL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd,MS 77-1, Cleveland, OH 44135 USA.
NR 21
TC 6
Z9 6
U1 1
U2 9
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0742-4795
EI 1528-8919
J9 J ENG GAS TURB POWER
JI J. Eng. Gas. Turbines Power-Trans. ASME
PD JUL
PY 2013
VL 135
IS 7
AR 071203
DI 10.1115/1.4023902
PG 10
WC Engineering, Mechanical
SC Engineering
GA 241HL
UT WOS:000326157000003
ER
PT J
AU Zinnecker, H
AF Zinnecker, H.
TI SOFIA: first science highlights and future science potential
SO ASTRONOMISCHE NACHRICHTEN
LA English
DT Article
DE infrared: general; instrumentation: miscellaneous; techniques:
spectroscopic; telescopes
ID INTERSTELLAR DUST GRAINS; MU-M; PHOTODISSOCIATION REGIONS; MOLECULAR
CLOUD; ORION NEBULA; M17 SW; ABSORPTION; LINE; CO; OH
AB SOFIA, the Stratospheric Observatory for Infrared Astronomy, is a joint project between NASA and the German Aerospace Agency (DLR) to develop and operate a 2.5 m airborne telescope in a highly modified Boeing 747SP aircraft that can fly as high as 45000 feet (13.7 km). This is above 99.8 % of the precipitable water vapor which blocks much of the midand far-infrared radiation from reaching ground-based telescopes. In this review, we briefly discuss the characteristics of the Observatory and present a number of early science highlights obtained with the FORCAST camera in 5-40 micron spectral region and with the GREAT heterodyne spectrometer in the 130-240 micron spectral region. The FORCAST images in Orion show the discovery of a new high-mass protostar (IRc4), while GREAT observations at 1 km s-1 velocity resolution detected velocity-resolved, redshifted ammonia spectra at 1.81 THz in absorption against several strong farinfrared dust continuum sources, clear evidence of substantial protostellar infall onto massive (non-ionizing) protostars. These powerful new data allow us to determine how massive stars form in our Galaxy. Another highlight is the stunning image taken by FORCAST that reveals the transient circumnuclear 1.5 pc radius (dust) ring around our Galactic center, heated by hundreds of massive stars in the young nuclear star cluster. The GREAT heterodyne spectrometer also observed the circumnuclear ring in highly excited CO rotational lines, indicative of emission from warm dense molecular gas with broad velocity structure, perhaps due to local shock heating. GREAT also made superb mapping observations of the [C II] fine structure cooling line at 158 microns, for example in M17-SW molecular cloud-star cluster interface, observations which disprove the simple canonical photodissociation models. The much better baseline stability of the GREAT receivers (compared to Herschel HIFI) allows efficient on-the-fly mapping of extended [C II] emission in our galaxy and also in other nearby spiral galaxies. Of particular note is the GREAT discovery of two new molecules outside the solar system: OD (the deuterated OH hydroxyl radical) as well as mercapto radical SH, both in absorption near 1.4 THz, a frequency gap where Herschel was blind. A special highlight was the 2011 June 23 UT stellar occultation by Pluto using the HIPO high speed photometer and the FDC fast diagnostic camera. This difficult but successful observation, which was both space-critical (within 100 km) and time-critical (within 1 min), proved that SOFIA can be in the right place at the right time, when important transient events occur. ((c) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
C1 NASA, SOFIA Sci Ctr, Deutsch SOFIA Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Zinnecker, H (reprint author), NASA, SOFIA Sci Ctr, Deutsch SOFIA Inst, Ames Res Ctr, MS 232-12, Moffett Field, CA 94035 USA.
EM hzinnecker@sofia.usra.edu
NR 41
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Z9 5
U1 0
U2 7
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 0004-6337
EI 1521-3994
J9 ASTRON NACHR
JI Astro. Nachr.
PD JUL
PY 2013
VL 334
IS 6
SI SI
BP 558
EP 575
DI 10.1002/asna.201311908
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 237IN
UT WOS:000325862900011
ER
PT J
AU van der Dussen, JJ
de Roode, SR
Ackerman, AS
Blossey, PN
Bretherton, CS
Kurowski, MJ
Lock, AP
Neggers, RAJ
Sandu, I
Siebesma, AP
AF van der Dussen, J. J.
de Roode, S. R.
Ackerman, A. S.
Blossey, P. N.
Bretherton, C. S.
Kurowski, M. J.
Lock, A. P.
Neggers, R. A. J.
Sandu, I.
Siebesma, A. P.
TI The GASS/EUCLIPSE model intercomparison of the stratocumulus transition
as observed during ASTEX: LES results
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
DE stratocumulus transition; model intercomparison; ASTEX; large-eddy
simulation (LES); GASS; EUCLIPSE
ID MARINE BOUNDARY-LAYER; LARGE-EDDY SIMULATIONS; ADVECTION TRANSPORT
ALGORITHM; SHALLOW CUMULUS CONVECTION; AIRCRAFT OBSERVATIONS; LAGRANGIAN
EXPERIMENTS; STRATIFORM CLOUDS; SCALAR ADVECTION; STRONG INVERSION;
MIXED-LAYER
AB Large-eddy simulations of a Lagrangian transition from a vertically well-mixed stratocumulus-topped boundary layer to a situation in which shallow cumuli penetrate an overlying layer of thin and broken stratocumulus are compared with aircraft observations collected during the Atlantic Stratocumulus Transition Experiment. Despite the complexity of the case and the long simulation period of 40 h, the six participating state-of-the-art models skillfully and consistently represent the observed gradual deepening of the boundary layer, a negative buoyancy flux at the top of the subcloud layer and the development of a double-peaked vertical velocity variance profile. The moisture flux from the subcloud to the stratocumulus cloud layer by cumulus convection exhibits a distinct diurnal cycle. During the night the moisture flux at the stratocumulus cloud base exceeds the surface evaporation flux, causing a net drying of the subcloud layer, and vice versa during daytime. The spread in the liquid water path (LWP) among the models is rather large during the first 12 h. From additional sensitivity experiments it is demonstrated that this spread is mainly attributable to differences in the parameterized precipitation rate. The LWP differences are limited through a feedback mechanism in which enhanced drizzle fluxes result in lower entrainment rates and subsequently a reduced drying at cloud top. The spread is furthermore reduced during the day as cloud layers with a greater LWP absorb more solar radiation and hence evaporate more.
C1 [van der Dussen, J. J.; de Roode, S. R.; Siebesma, A. P.] Delft Univ Technol, Dept Geosci & Remote Sensing, NL-2628 CN Delft, Netherlands.
[Ackerman, A. S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Blossey, P. N.; Bretherton, C. S.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Kurowski, M. J.] Univ Warsaw, Fac Phys, Inst Geophys, Warsaw, Poland.
[Kurowski, M. J.] Natl Res Inst, Inst Meteorol & Water Management, Warsaw, Poland.
[Lock, A. P.] Met Off, Fdn Sci, Exeter, Devon, England.
[Neggers, R. A. J.] Royal Netherlands Meteorol Inst, Dept Reg Climate, NL-3730 AE De Bilt, Netherlands.
[Neggers, R. A. J.] Univ Cologne, Inst Geophys & Meteorol, Cologne, Germany.
[Sandu, I.] Max Planck Inst Meteorol, Dept Atmosphere Earth Syst, D-20146 Hamburg, Germany.
[Sandu, I.] European Ctr Medium Range Weather Forecasts, Sect Phys Aspects, Reading RG2 9AX, Berks, England.
[Siebesma, A. P.] Royal Netherlands Meteorol Inst, Div Atmospher Res, NL-3730 AE De Bilt, Netherlands.
RP van der Dussen, JJ (reprint author), Delft Univ Technol, Dept Geosci & Remote Sensing, Stevinweg 1, NL-2628 CN Delft, Netherlands.
EM j.j.vanderdussen@tudelft.nl
RI Ackerman, Andrew/D-4433-2012
OI Ackerman, Andrew/0000-0003-0254-6253
FU European Union [244067]; National Computing Facilities Foundation (NCF)
FX The research leading to these results has received funding from the
European Union, Seventh Framework Programme (FP7/2007-2013) under grant
agreement 244067. ECMWF ERA-Interim data used in this project have been
obtained from the ECMWF data server. The work was sponsored by the
National Computing Facilities Foundation (NCF) for the use of
supercomputer facilities. We kindly thank Coen Hennipman and Arjan van
Leeuwen for providing analysis used in this paper and Gunilla Svensson
for helpful suggestions regarding the setup of the case. We also thank
two anonymous reviewers whose comments helped to improve the quality of
the manuscript.
NR 67
TC 15
Z9 15
U1 1
U2 18
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD JUL
PY 2013
VL 5
IS 3
BP 483
EP 499
DI 10.1002/jame.20033
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 238HB
UT WOS:000325934100002
ER
PT J
AU Rothschild, LJ
AF Rothschild, L. J.
TI EXTREMOPHILES AND THE SEARCH FOR LIFE IN THE UNIVERSE
SO PHYCOLOGIA
LA English
DT Meeting Abstract
C1 [Rothschild, L. J.] NASA Ames Res Ctr, Washington, DC USA.
EM lynn.j.rothschild@nasa.gov
NR 0
TC 0
Z9 0
U1 2
U2 11
PU INT PHYCOLOGICAL SOC
PI LAWRENCE
PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0031-8884
J9 PHYCOLOGIA
JI Phycologia
PD JUL
PY 2013
VL 52
IS 4
SU S
MA 248
BP 94
EP 95
PG 2
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 238QV
UT WOS:000325963600249
ER
PT J
AU Previdi, M
Liepert, BG
Peteet, D
Hansen, J
Beerling, DJ
Broccoli, AJ
Frolking, S
Galloway, JN
Heimann, M
Le Quere, C
Levitus, S
Ramaswamy, V
AF Previdi, M.
Liepert, B. G.
Peteet, D.
Hansen, J.
Beerling, D. J.
Broccoli, A. J.
Frolking, S.
Galloway, J. N.
Heimann, M.
Le Quere, C.
Levitus, S.
Ramaswamy, V.
TI Climate sensitivity in the Anthropocene
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Review
DE climate sensitivity; radiative forcing; radiative feedbacks; carbon
cycle; Anthropocene
ID SEA-LEVEL; CARBON-DIOXIDE; EARTH-SYSTEM; ENVIRONMENTAL-CHANGE; METHANE
EMISSIONS; SOIL RESPIRATION; NITROGEN-CYCLE; MASS-LOSS; FEEDBACKS;
TEMPERATURE
AB Climate sensitivity in its most basic form is defined as the equilibrium change in global surface temperature that occurs in response to a climate forcing, or externally imposed perturbation of the planetary energy balance. Within this general definition, several specific forms of climate sensitivity exist that differ in terms of the types of climate feedbacks they include. Based on evidence from Earth's history, we suggest here that the relevant form of climate sensitivity in the Anthropocene (e.g. from which to base future greenhouse gas (GHG) stabilization targets) is the Earth system sensitivity including fast feedbacks from changes in water vapour, natural aerosols, clouds and sea ice, slower surface albedo feedbacks from changes in continental ice sheets and vegetation, and climate-GHG feedbacks from changes in natural (land and ocean) carbon sinks. Traditionally, only fast feedbacks have been considered (with the other feedbacks either ignored or treated as forcing), which has led to estimates of the climate sensitivity for doubled CO2 concentrations of about 3 degrees C. The 2xCO(2) Earth system sensitivity is higher than this, being approximate to 4-6 degrees C if the ice sheet/vegetation albedo feedback is included in addition to the fast feedbacks, and higher still if climate-GHG feedbacks are also included. The inclusion of climate-GHG feedbacks due to changes in the natural carbon sinks has the advantage of more directly linking anthropogenic GHG emissions with the ensuing global temperature increase, thus providing a truer indication of the climate sensitivity to human perturbations. The Earth system climate sensitivity is difficult to quantify due to the lack of palaeo-analogues for the present-day anthropogenic forcing, and the fact that ice sheet and climate-GHG feedbacks have yet to become globally significant in the Anthropocene. Furthermore, current models are unable to adequately simulate the physics of ice sheet decay and certain aspects of the natural carbon and nitrogen cycles. Obtaining quantitative estimates of the Earth system sensitivity is therefore a high priority for future work.
C1 [Previdi, M.; Peteet, D.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Liepert, B. G.] NW Res Associates Inc, Redmond, WA USA.
[Peteet, D.; Hansen, J.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Hansen, J.] Columbia Univ, Earth Inst, New York, NY USA.
[Beerling, D. J.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
[Broccoli, A. J.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA.
[Frolking, S.] Univ New Hampshire, Inst Study Earth Oceans & Space, Earth Syst Res Ctr, Durham, NH 03824 USA.
[Galloway, J. N.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA.
[Heimann, M.] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
[Le Quere, C.] Univ E Anglia, Tyndall Ctr Climate Change Res, Norwich NR4 7TJ, Norfolk, England.
[Levitus, S.] NOAA, Natl Oceanog Data Ctr, Silver Spring, MD USA.
[Ramaswamy, V.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
RP Previdi, M (reprint author), Columbia Univ, Lamont Doherty Earth Observ, 61 Route 9W, Palisades, NY 10964 USA.
EM mprevidi@ldeo.columbia.edu
RI Broccoli, Anthony/D-9186-2014; Beerling, David/C-2840-2009; Heimann,
Martin/H-7807-2016; Le Quere, Corinne/C-2631-2017
OI Broccoli, Anthony/0000-0003-2619-1434; Beerling,
David/0000-0003-1869-4314; Heimann, Martin/0000-0001-6296-5113; Le
Quere, Corinne/0000-0003-2319-0452
FU LDEO/GISS Climate Center
FX We thank two anonymous reviewers whose comments significantly improved
the manuscript. We also thank Reto Knutti, Susan Solomon and Steve
Schwartz for helpful comments on an earlier version of the manuscript.
This work was funded by a grant from the LDEO/GISS Climate Center, and
was motivated by discussions that took place at a meeting titled
'Climate Sensitivity Extremes: Assessing the Risk' that was held at NASA
GISS during April 2010.
NR 87
TC 8
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U1 5
U2 78
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD JUL
PY 2013
VL 139
IS 674
BP 1121
EP 1131
DI 10.1002/qj.2165
PN A
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 240MV
UT WOS:000326101800001
ER
PT J
AU Errico, RM
Yang, RH
Prive, NC
Tai, KS
Todling, R
Sienkiewicz, ME
Guo, J
AF Errico, Ronald M.
Yang, Runhua
Prive, Nikki C.
Tai, King-Sheng
Todling, Ricardo
Sienkiewicz, Meta E.
Guo, Jing
TI Development and validation of observing-system simulation experiments at
NASA's Global Modeling and Assimilation Office
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE OSSE; data assimilation; atmospheric observations
ID ERROR CHARACTERISTICS
AB Initial design and validation of baseline Observing System Simulation Experiments (OSSEs) at NASA's Global Modeling and Assimilation Office (GMAO) are described. The OSSEs mimic the procedures used to analyze global observations for specifying states of the atmosphere. As simulations, however, OSSEs are not only confined to already existing observations and they provide a perfect description of the true state being analyzed. These two properties of the simulations can be exploited to improve both existing and envisioned observing systems and the algorithms to analyze them. Preliminary to any applications, however, the OSSE framework must be adequately validated. This first version of the simulated observations is drawn from a 13 month simulation of nature produced by the European Center for Medium-Range Weather Forecasts. These observations include simulated errors of both instruments and representativeness. Since the statistics of analysis and forecast errors are partially determined by these observational errors, their appropriate modelling can be crucial for validating the realism of the OSSE. That validation is performed by comparing the statistics of the results of assimilating these simulated observations for one summer month compared with the corresponding statistics obtained from assimilating real observations during the same time of year. The assimilation system is the three-dimensional variational analysis (GSI) scheme used at both the National Centers for Environmental Prediction and GMAO. Here, only statistics concerning observation innovations or analysis increments within the troposphere are considered for the validation. In terms of the examined statistics, the OSSE is validated remarkably well, even with some simplifications currently employed. In order to obtain this degree of success, it was necessary to employ horizontally correlated observation errors for both atmospheric motion vectors and some satellite observed radiances. The simulated observations with added observation errors appear suitable for some initial OSSE applications.
C1 [Errico, Ronald M.; Prive, Nikki C.] Morgan State Univ, Goddard Earth Sci Technol & Res Ctr, Baltimore, MD 21239 USA.
[Errico, Ronald M.; Prive, Nikki C.; Todling, Ricardo] NASA, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Yang, Runhua] IM Syst Grp Inc, Rockville, MD USA.
[Tai, King-Sheng; Sienkiewicz, Meta E.; Guo, Jing] Sci Syst & Applicat Inc, Greenbelt, MD USA.
RP Errico, RM (reprint author), NASA GSFC Code 610 1, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
EM ronald.m.errico@nasa.gov
RI Sienkiewicz, Meta/P-8168-2016;
OI Sienkiewicz, Meta/0000-0002-9267-4568; Prive, Nikki/0000-0001-8309-8741
FU National Aeronautics and Space Administration [WBS 802678.02.17.01.06,
MAP/04-0000-0080]; National Science Foundation [ATM-0745906]
FX The authors benefited from many conversations with Ronald Gelaro, Will
McCarty and Arlindo da Silva. Joanna Joiner suggested using an elevated
surface to provide a cloud effect for IR radiances. Steve Bloom and Tong
Zhu provided some useful software. Ravi Govindaraju, Joesph Stassi and
Thomas Owens provided some additional necessary datasets. The ECMWF
nature run was provided by Erik Andersson through arrangements made by
Michiko Masutani. Support for this project was encouraged by Michele
Rienecker and provided by grant numbers WBS 802678.02.17.01.06 and
MAP/04-0000-0080 from the National Aeronautics and Space Administration
and grant number ATM-0745906 from the National Science Foundation.
NR 21
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U1 0
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD JUL
PY 2013
VL 139
IS 674
BP 1162
EP 1178
DI 10.1002/qj.2027
PN A
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 240MV
UT WOS:000326101800003
ER
PT J
AU Schleeweis, K
Goward, SN
Huang, CQ
Masek, JG
Moisen, G
Kennedy, RE
Thomas, NE
AF Schleeweis, Karen
Goward, Samuel N.
Huang, Chengquan
Masek, Jeffrey G.
Moisen, Gretchen
Kennedy, Robert E.
Thomas, Nancy E.
TI Regional dynamics of forest canopy change and underlying causal
processes in the contiguous US
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
DE Forest disturbance; harvest; time-series; NAFD; Landsat
ID EASTERN UNITED-STATES; TERRESTRIAL CARBON STORAGE; NORTH-AMERICAN
FORESTS; NATURAL DISTURBANCES; LANDSCAPE PATTERNS; CLIMATE-CHANGE;
CATASTROPHIC WIND; MAPPING WILDFIRE; FIRE MANAGEMENT; LANDSAT IMAGERY
AB The history of forest change processes is written into forest age and distribution and affects earth systems at many scales. No one data set has been able to capture the full forest disturbance and land use record through time, so in this study, we combined multiple lines of evidence to examine trends, for six US regions, in forest area affected by harvest, fire, wind, insects, and forest conversion to urban/surburban use. We built an integrated geodatabase for the contiguous U.S. (CONUS) with data spanning the nation and decades, from remote sensing observations of forest canopy dynamics, geospatial data sets on disturbance and conversion, and statistical inventories, to evaluate relationships between canopy change observations and casual processes at multiple scales. Results show the variability of major change processes through regions across decades. Harvest affected more forest area than any other major change processes in the North East, North Central, Southeast, and South central regions. In the Pacific Coast and Intermountain West, more forest area was affected by harvest than forest fires. Canopy change rates at regional scales confounded the trends of individual forest change processes, showing the importance of landscape scale data. Local spikes in observed canopy change rates were attributed to wind and fire events, as well as volatile harvest regimes. This study improves the geographic model of forest change processes by updating regional trends for major disturbance and conversion processes and combining data on the dynamics of fire, wind, insects, harvest, and conversion into one integrated geodatabase for the CONUS.
C1 [Schleeweis, Karen; Moisen, Gretchen] US Forest Serv, Rocky Mt Res Stn, USDA, Ogden, UT 84401 USA.
[Schleeweis, Karen; Goward, Samuel N.; Huang, Chengquan; Thomas, Nancy E.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Kennedy, Robert E.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Kennedy, Robert E.] Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA.
[Thomas, Nancy E.] Stanford Univ, Dept Environm Earth Syst Sci, Stanford, CA 94305 USA.
RP Schleeweis, K (reprint author), US Forest Serv, Rocky Mt Res Stn, USDA, Ogden, UT 84401 USA.
EM kgschleeweis@fs.fed.us
RI Masek, Jeffrey/D-7673-2012;
OI Huang, Chengquan/0000-0003-0055-9798
FU NASA's Carbon Cycle Science Program [NNG05GE55G, NNX08AI26G, NNX11AJ78G]
FX The study contributes to the North American Carbon Program (NACP), with
grant support from NASA's Carbon Cycle Science Program (NNG05GE55G,
NNX08AI26G, and NNX11AJ78G). The authors thank Brad Smith, the editor,
and anonymous reviewers for their comments and feedback.
NR 127
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U1 2
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-8953
EI 2169-8961
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD JUL
PY 2013
VL 118
IS 3
BP 1035
EP 1053
DI 10.1002/jgrg.20076
PG 19
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 233EV
UT WOS:000325549900007
ER
PT J
AU Hakkinen, S
Rhines, PB
Worthen, DL
AF Haekkinen, Sirpa
Rhines, Peter B.
Worthen, Denise L.
TI Northern North Atlantic sea surface height and ocean heat content
variability
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE multidecadal variability; sea surface height; ocean heat content
ID MERIDIONAL OVERTURNING CIRCULATION; THERMOHALINE CIRCULATION; SUBPOLAR
GYRE; INTERANNUAL VARIABILITY; ATMOSPHERIC BLOCKING; OSCILLATION;
FREQUENCY; CLIMATE
AB The evolution of nearly 20 years of altimetric sea surface height (SSH) is investigated to understand its association with decadal to multidecadal variability of the North Atlantic heat content. Altimetric SSH is dominated by an increase of about 14 cm in the Labrador and Irminger seas from 1993 to 2011, while the opposite has occurred over the Gulf Stream region over the same time period. During the altimeter period the observed 0-700 m ocean heat content (OHC) in the subpolar gyre mirrors the increased SSH by its dominantly positive trend. Over a longer period, 1955-2011, fluctuations in the subpolar OHC reflect Atlantic multidecadal variability (AMV) and can be attributed to advection driven by the wind stress gyre mode bringing more subtropical waters into the subpolar gyre. The extended subpolar warming evident in SSH and OHC during the altimeter period represents transition of the AMV from cold to warm phase. In addition to the dominant trend, the first empirical orthogonal function SSH time series shows an abrupt change 2009-2010 reaching a new minimum in 2010. The change coincides with the change in the meridional overturning circulation at 26.5 degrees N as observed by the RAPID (Rapid Climate Change) project, and with extreme behavior of the wind stress gyre mode and of atmospheric blocking. While the general relationship between northern warming and Atlantic meridional overturning circulation (AMOC) volume transport remains undetermined, the meridional heat and salt transport carried by AMOC's arteries are rich with decade-to-century timescale variability.
C1 [Haekkinen, Sirpa; Worthen, Denise L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rhines, Peter B.] Univ Washington, Sch Oceanog, Seattle, WA 98195 USA.
[Worthen, Denise L.] Wyle ITS, Greenbelt, MD USA.
RP Hakkinen, S (reprint author), NASA, Goddard Space Flight Ctr, Code 615, Greenbelt, MD 20771 USA.
EM sirpa.hakkinen@nasa.gov
FU NASA Headquarters Physical Oceanography Program; OSTM Science Team; NASA
through the OSTM Science Team; NASA's MEaSUREs program
FX S.H. and D. L. W. gratefully acknowledge the support from NASA
Headquarters Physical Oceanography Program and OSTM Science Team for
this work. P. B. R. is supported by NASA through the OSTM Science Team.
Altimeter data were provided by Brian Beckely, supported by NASA's
MEaSUREs program. Also, we thank the two anonymous reviewers for
constructive and helpful comments.
NR 36
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U1 9
U2 31
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 JUL
PY 2013
VL 118
IS 7
BP 3670
EP 3678
DI 10.1002/jgrc.20268
PG 9
WC Oceanography
SC Oceanography
GA 224KY
UT WOS:000324885400028
ER
PT J
AU John, R
Chen, JQ
Ou-Yang, ZT
Xiao, JF
Becker, R
Samanta, A
Ganguly, S
Yuan, WP
Batkhishig, O
AF John, Ranjeet
Chen, Jiquan
Ou-Yang, Zu-Tao
Xiao, Jingfeng
Becker, Richard
Samanta, Arindam
Ganguly, Sangram
Yuan, Wenping
Batkhishig, Ochirbat
TI Vegetation response to extreme climate events on the Mongolian Plateau
from 2000 to 2010
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE Mongolian Plateau; vegetation indices; extreme climate; drought; land
surface temperature; MODIS; EVI; EVI2; dzud
ID INNER-MONGOLIA; ATMOSPHERIC CIRCULATION; SATELLITE DATA; LAND-USE;
CHINA; DROUGHT; VARIABILITY; AMAZON; INDEX; GRASSLAND
AB Climate change has led to more frequent extreme winters (aka, dzud) and summer droughts on the Mongolian Plateau during the last decade. Among these events, the 2000-2002 combined summer drought-dzud and 2010 dzud were the most severe on vegetation. We examined the vegetation response to these extremes through the past decade across the Mongolian Plateau as compared to decadal means. We first assessed the severity and extent of drought using the Tropical Rainfall Measuring Mission (TRMM) precipitation data and the Palmer drought severity index (PDSI). We then examined the effects of drought by mapping anomalies in vegetation indices (EVI, EVI2) and land surface temperature derived from MODIS and AVHRR for the period of 2000-2010. We found that the standardized anomalies of vegetation indices exhibited positively skewed frequency distributions in dry years, which were more common for the desert biome than for grasslands. For the desert biome, the dry years (2000-2001, 2005 and 2009) were characterized by negative anomalies with peak values between -1.5 and -0.5 and were statistically different (P < 0.001) from relatively wet years (2003, 2004 and 2007). Conversely, the frequency distributions of the dry years were not statistically different (p < 0.001) from those of the relatively wet years for the grassland biome, showing that they were less responsive to drought and more resilient than the desert biome. We found that the desert biome is more vulnerable to drought than the grassland biome. Spatially averaged EVI was strongly correlated with the proportion of land area affected by drought (PDSI < -1) in Inner Mongolia (IM) and Outer Mongolia (OM), showing that droughts substantially reduced vegetation activity. The correlation was stronger for the desert biome (R-2 = 65 and 60, p < 0.05) than for the IM grassland biome (R-2 = 53, p < 0.05). Our results showed significant differences in the responses to extreme climatic events (summer drought and dzud) between the desert and grassland biomes on the Plateau.
C1 [John, Ranjeet; Chen, Jiquan; Ou-Yang, Zu-Tao; Becker, Richard] Univ Toledo, Dept Environm Sci, Toledo, OH 43606 USA.
[Chen, Jiquan] Chinese Acad Sci, Inst Bot, Beijing 100093, Peoples R China.
[Xiao, Jingfeng] Univ New Hampshire, Inst Study Earth Oceans & Space, Earth Syst Res Ctr, Durham, NH 03824 USA.
[Samanta, Arindam] Atmospher & Environm Res Inc, Boston, MA USA.
[Ganguly, Sangram] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Ganguly, Sangram] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Yuan, Wenping] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
[Batkhishig, Ochirbat] Mongolian Acad Sci, Inst Geog, Ulaanbaatar 210620, Mongol Peo Rep.
RP John, R (reprint author), Univ Toledo, Dept Environm Sci, 2801 W Bancroft St, Toledo, OH 43606 USA.
EM ranjeet.john@utoledo.edu
RI Chen, Jiquan/D-1955-2009; Becker, Richard/A-9120-2010; ganguly,
sangram/B-5108-2010;
OI Becker, Richard/0000-0003-2514-2040; John, Ranjeet/0000-0002-0150-8450
FU NASA-NEWS Program [NN-H-04-705 Z-YS-005-N]; Natural Science Foundation
of China [31229001]; Outstanding Overseas Scientists Team Project of the
Chinese Academy of Sciences; State Key Basic Research Development
Program of China [2007CB106800]; National Science Foundation (NSF)
[1065777]; NASA [NNX11AL32G]
FX This study was supported by the NASA-NEWS Program (NN-H-04-705
Z-YS-005-N), the Natural Science Foundation of China (31229001), the
Outstanding Overseas Scientists Team Project of the Chinese Academy of
Sciences and the State Key Basic Research Development Program of China
(2007CB106800). J Xiao was partly supported by the National Science
Foundation (NSF) through MacroSystems Biology (award number 1065777) and
NASA through the Carbon Monitoring System (NNX11AL32G). We would like to
thank Lisa Delp Taylor and Dee Becker who proofread the manuscript at
various stages, Mohamed Abd salam El Vilaly and Kirk Zmijewski for RS
data processing suggestions and Kamel Didan for kindly providing travel
support to the VIP data workshop at the University of Arizona in January
2013.
NR 67
TC 14
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U1 10
U2 95
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 JUL-SEP
PY 2013
VL 8
IS 3
AR UNSP 035033
DI 10.1088/1748-9326/8/3/035033
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 229FL
UT WOS:000325247100078
ER
PT J
AU Silva, RA
West, JJ
Zhang, YQ
Anenberg, SC
Lamarque, JF
Shindell, DT
Collins, WJ
Dalsoren, S
Faluvegi, G
Folberth, G
Horowitz, LW
Nagashima, T
Naik, V
Rumbold, S
Skeie, R
Sudo, K
Takemura, T
Bergmann, D
Cameron-Smith, P
Cionni, I
Doherty, RM
Eyring, V
Josse, B
MacKenzie, IA
Plummer, D
Righi, M
Stevenson, DS
Strode, S
Szopa, S
Zeng, G
AF Silva, Raquel A.
West, J. Jason
Zhang, Yuqiang
Anenberg, Susan C.
Lamarque, Jean-Francois
Shindell, Drew T.
Collins, William J.
Dalsoren, Stig
Faluvegi, Greg
Folberth, Gerd
Horowitz, Larry W.
Nagashima, Tatsuya
Naik, Vaishali
Rumbold, Steven
Skeie, Ragnhild
Sudo, Kengo
Takemura, Toshihiko
Bergmann, Daniel
Cameron-Smith, Philip
Cionni, Irene
Doherty, Ruth M.
Eyring, Veronika
Josse, Beatrice
MacKenzie, I. A.
Plummer, David
Righi, Mattia
Stevenson, David S.
Strode, Sarah
Szopa, Sophie
Zeng, Guang
TI Global premature mortality due to anthropogenic outdoor air pollution
and the contribution of past climate change
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE climate change; air pollution; ozone; particulate matter; human health;
premature mortality
ID INTERCOMPARISON PROJECT ACCMIP; ATMOSPHERIC CHEMISTRY; TROPOSPHERIC
OZONE; HEALTH IMPACTS; EXPOSURE; PREINDUSTRIAL; SIMULATIONS; DISEASE;
BURDEN; EMISSIONS
AB Increased concentrations of ozone and fine particulate matter (PM2.5) since preindustrial times reflect increased emissions, but also contributions of past climate change. Here we use modeled concentrations from an ensemble of chemistry-climate models to estimate the global burden of anthropogenic outdoor air pollution on present-day premature human mortality, and the component of that burden attributable to past climate change. Using simulated concentrations for 2000 and 1850 and concentration-response functions (CRFs), we estimate that, at present, 470 000 (95% confidence interval, 140 000 to 900 000) premature respiratory deaths are associated globally and annually with anthropogenic ozone, and 2.1 (1.3 to 3.0) million deaths with anthropogenic PM2.5-related cardiopulmonary diseases (93%) and lung cancer (7%). These estimates are smaller than ones from previous studies because we use modeled 1850 air pollution rather than a counterfactual low concentration, and because of different emissions. Uncertainty in CRFs contributes more to overall uncertainty than the spread of model results. Mortality attributed to the effects of past climate change on air quality is considerably smaller than the global burden: 1500 (-20 000 to 27 000) deaths yr(-1) due to ozone and 2200 (-350 000 to 140 000) due to PM2.5. The small multi-model means are coincidental, as there are larger ranges of results for individual models, reflected in the large uncertainties, with some models suggesting that past climate change has reduced air pollution mortality.
C1 [Silva, Raquel A.; West, J. Jason; Zhang, Yuqiang] Univ N Carolina, Chapel Hill, NC 27599 USA.
[Anenberg, Susan C.] US EPA, Washington, DC 20004 USA.
[Lamarque, Jean-Francois] Natl Ctr Atmospher Res, NCAR Earth Syst Lab, Boulder, CO 80301 USA.
[Shindell, Drew T.; Faluvegi, Greg] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Shindell, Drew T.; Faluvegi, Greg] Columbia Earth Inst, New York, NY USA.
[Collins, William J.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Dalsoren, Stig; Skeie, Ragnhild] Ctr Int Climate & Environm Res Oslo, CICERO, Oslo, Norway.
[Folberth, Gerd; Rumbold, Steven] Hadley Ctr Climate Predict, Met Off, Exeter, Devon, England.
[Horowitz, Larry W.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
[Nagashima, Tatsuya] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan.
[Naik, Vaishali] UCAR NOAA Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
[Sudo, Kengo] Nagoya Univ, Grad Sch Environm Studies, Nagoya, Aichi 4648601, Japan.
[Takemura, Toshihiko] Kyushu Univ, Appl Mech Res Inst, Fukuoka 8168580, Japan.
[Bergmann, Daniel; Cameron-Smith, Philip] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Cionni, Irene] Agenzia Nazl Nuove Tecnol Energia & Sviluppo Econ, Bologna, Italy.
[Doherty, Ruth M.; MacKenzie, I. A.; Stevenson, David S.] Univ Edinburgh, Sch GeoSci, Edinburgh, Midlothian, Scotland.
[Eyring, Veronika; Righi, Mattia] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Phys Atmosphare, Oberpfaffenhofen, Germany.
[Josse, Beatrice] CNRS Ctr Natl Rech Meteorolg, Meteo France, GAME CNRM, Toulouse, France.
[Plummer, David] Environm Canada, Canadian Ctr Climate Modeling & Anal, Victoria, BC, Canada.
[Strode, Sarah] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Strode, Sarah] Univ Space Res Assoc, Columbia, MD USA.
[Szopa, Sophie] LSCE CEA CNRS UVSQ, Lab Sci Climat & Environm, Gif Sur Yvette, France.
[Zeng, Guang] Natl Inst Water & Atmospher Res, Lauder, New Zealand.
RP West, JJ (reprint author), Univ N Carolina, Chapel Hill, NC 27599 USA.
EM jjwest@email.unc.edu
RI Strode, Sarah/H-2248-2012; U-ID, Kyushu/C-5291-2016; Eyring,
Veronika/O-9999-2016; Zhang, Yuqiang/P-2682-2016; Zhang,
Yuqiang/C-5027-2015; Shindell, Drew/D-4636-2012; Stevenson,
David/C-8089-2012; Horowitz, Larry/D-8048-2014; Bergmann,
Daniel/F-9801-2011; Naik, Vaishali/A-4938-2013; Takemura,
Toshihiko/C-2822-2009; Collins, William/A-5895-2010; Righi,
Mattia/I-5120-2013; Lamarque, Jean-Francois/L-2313-2014; Cameron-Smith,
Philip/E-2468-2011; Kyushu, RIAM/F-4018-2015; West, Jason/J-2322-2015;
Szopa, Sophie/F-8984-2010
OI Strode, Sarah/0000-0002-8103-1663; Eyring, Veronika/0000-0002-6887-4885;
Zhang, Yuqiang/0000-0002-9161-7086; Zhang, Yuqiang/0000-0002-9161-7086;
Folberth, Gerd/0000-0002-1075-440X; Skeie, Ragnhild/0000-0003-1246-4446;
Righi, Mattia/0000-0003-3827-5950; Stevenson, David/0000-0002-4745-5673;
Horowitz, Larry/0000-0002-5886-3314; Bergmann,
Daniel/0000-0003-4357-6301; Naik, Vaishali/0000-0002-2254-1700;
Takemura, Toshihiko/0000-0002-2859-6067; Collins,
William/0000-0002-7419-0850; Lamarque,
Jean-Francois/0000-0002-4225-5074; Cameron-Smith,
Philip/0000-0002-8802-8627; West, Jason/0000-0001-5652-4987; Szopa,
Sophie/0000-0002-8641-1737
FU Portuguese Foundation for Science and Technology (FCT)
[SFRH/BD/62759/2009]; International Council for Clean Transportation
FX This work was supported by fellowship SFRH/BD/62759/2009 (to RAS) from
the Portuguese Foundation for Science and Technology (FCT), and by the
International Council for Clean Transportation. Acknowledgments of
funding for the modeling groups participating in ACCMIP can be found in
previous publications (e.g., Lamarque et al 2013).
NR 33
TC 75
Z9 80
U1 19
U2 140
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 JUL-SEP
PY 2013
VL 8
IS 3
AR UNSP 034005
DI 10.1088/1748-9326/8/3/034005
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 229FL
UT WOS:000325247100011
ER
PT J
AU Konopliv, AS
Park, RS
Yuan, DN
Asmar, SW
Watkins, MM
Williams, JG
Fahnestock, E
Kruizinga, G
Paik, M
Strekalov, D
Harvey, N
Smith, DE
Zuber, MT
AF Konopliv, Alex S.
Park, Ryan S.
Yuan, Dah-Ning
Asmar, Sami W.
Watkins, Michael M.
Williams, James G.
Fahnestock, Eugene
Kruizinga, Gerhard
Paik, Meegyeong
Strekalov, Dmitry
Harvey, Nate
Smith, David E.
Zuber, Maria T.
TI The JPL lunar gravity field to spherical harmonic degree 660 from the
GRAIL Primary Mission
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Moon; gravity; GRAIL
ID TRACKING DATA; MOON; PROSPECTOR; CLEMENTINE; RECOVERY; CRUST; MODEL
AB The lunar gravity field and topography provide a way to probe the interior structure of the Moon. Prior to the Gravity Recovery and Interior Laboratory (GRAIL) mission, knowledge of the lunar gravity was limited mostly to the nearside of the Moon, since the farside was not directly observable from missions such as Lunar Prospector. The farside gravity was directly observed for the first time with the SELENE mission, but was limited to spherical harmonic degree n <= 70. The GRAIL Primary Mission, for which results are presented here, dramatically improves the gravity spectrum by up to similar to 4 orders of magnitude for the entire Moon and for more than 5 orders-of-magnitude over some spectral ranges by using interspacecraft measurements with near 0.03 m/s accuracy. The resulting GL0660B (n=660) solution has 98% global coherence with topography to n=330, and has variable regional surface resolution between n=371 (14.6km) and n=583 (9.3km) because the gravity data were collected at different spacecraft altitudes. The GRAIL data also improve low-degree harmonics, and the uncertainty in the lunar Love number has been reduced by similar to 5x to k(2)=0.02405 +/- 0.00018. The reprocessing of the Lunar Prospector data indicates similar to 3x improved orbit uncertainty for the lower altitudes to similar to 10 m, whereas the GRAIL orbits are determined to an accuracy of 20cm.
C1 [Konopliv, Alex S.; Park, Ryan S.; Yuan, Dah-Ning; Asmar, Sami W.; Watkins, Michael M.; Williams, James G.; Fahnestock, Eugene; Kruizinga, Gerhard; Paik, Meegyeong; Strekalov, Dmitry; Harvey, Nate] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
RP Konopliv, AS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM Alexander.S.Konopliv@jpl.nasa.gov
NR 50
TC 50
Z9 59
U1 0
U2 10
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 JUL
PY 2013
VL 118
IS 7
BP 1415
EP 1434
DI 10.1002/jgre.20097
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 224TH
UT WOS:000324911800001
ER
PT J
AU Lillis, RJ
Robbins, S
Manga, M
Halekas, JS
Frey, HV
AF Lillis, Robert J.
Robbins, Stuart
Manga, Michael
Halekas, Jasper S.
Frey, Herbert V.
TI Time history of the Martian dynamo from crater magnetic field analysis
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; dynamo; crater; magnetic; age; history
ID IMPACT DEMAGNETIZATION; ELECTRON REFLECTOMETRY; CRUSTAL MAGNETIZATION;
ATMOSPHERIC LOSS; MARS; EVOLUTION; ROCKS; SHOCK; CONSTRAINTS; CHRONOLOGY
AB Large impacts simultaneously reset both the surface age and the magnetization of the entire depth of crust over areas comparable to the final size of the resulting craters. These properties make large impact craters (>300km in diameter) ideal magnetic markers for constraining the history of the Martian core dynamo. However, the relationship between crustal magnetization and magnetic field measured in orbit is nonunique, making the measured magnetic field signature of an impact crater only a proxy for the magnetization (or lack thereof) below. Using Monte Carlo Fourier domain modeling of subsurface magnetization, we calculate probability distributions of the magnetic field signatures of partially and completely demagnetized craters. We compare these distributions to measured magnetic field signatures of 41 old impact craters on Mars larger than 300km in diameter and calculate probabilities of their magnetization state. We compare these probabilities to cratering densities and absolute model ages and in this manner arrive at a robust time history of Martian large-crater magnetization and hence of the Martian dynamo. We conclude that the most likely scenario was a Mars dynamo active when the oldest detectable basins formed, ceasing before the Hellas and Utopia impacts, between 4.0 and 4.1Ga (in model age) and not thereafter restarting. The Mars atmosphere was thereafter exposed directly to erosion by the solar wind, significantly altering the path of climate evolution. Further improvements to the history of the Martian dynamo will require better crater age estimates and lower altitude magnetic field data.
C1 [Lillis, Robert J.; Halekas, Jasper S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Robbins, Stuart] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Manga, Michael] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Frey, Herbert V.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM rlillis@ssl.berkeley.edu
RI Lillis, Robert/A-3281-2008;
OI Lillis, Robert/0000-0003-0578-517X; Manga, Michael/0000-0003-3286-4682;
Halekas, Jasper/0000-0001-5258-6128
FU NASA Mars Data Analysis program [NNX07AN94G, NNX11AI85G]
FX This work was supported by the NASA Mars Data Analysis program (grants
NNX07AN94G and NNX11AI85G).
NR 74
TC 13
Z9 13
U1 1
U2 9
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 JUL
PY 2013
VL 118
IS 7
BP 1488
EP 1511
DI 10.1002/jgre.20105
PG 24
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 224TH
UT WOS:000324911800005
ER
PT J
AU Thejappa, G
MacDowall, RJ
Bergamo, M
AF Thejappa, G.
MacDowall, R. J.
Bergamo, M.
TI Observational evidence for the collapsing Langmuir wave packet in a
solar type III radio burst
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE solar flares; solar wind; solar radio bursts
ID INTERPLANETARY PLASMA; HARMONIC STRUCTURE; ENVELOPE SOLITONS; SPATIAL
COLLAPSE; SOURCE REGIONS; TURBULENCE; EMISSION; WIND; RADIATION;
STABILIZATION
AB High time resolution observations from the STEREO spacecraft show that in solar type III radio bursts, Langmuir waves often occur as very intense one-dimensional magnetic field aligned field structures. One of these events represents the most intense Langmuir wave packet with W-L/n(e)T(e)similar to 7.2x10(-3) ever detected in a type III radio burst until now (W-L is the peak energy density, and n(e) and T-e are the electron density and temperature, respectively). The detailed analysis of this wave packet indicates that (1) its peak intensity is well above the threshold for the oscillating two-stream instability (OTSI) and supersonic collapse; (2) its peak intensity and spatial scale satisfy the criterion for it to be a collapsing envelope soliton; (3) its low-frequency components provide evidence for a density cavity, whose depth, width, and temporal coincidence indicate that probably it is the ponderomotive force generated density cavity; and (4) its spectrum contains harmonic peaks at 2f(pe) and 3f(pe) (in addition to the main Langmuir wave peak at the electron plasma frequency, f(pe)), which, as indicated by the bispectral analysis, probably are of the electromagnetic waves generated as a result of coalescence of two oppositely propagating Langmuir waves, and a Langmuir wave and a second harmonic electromagnetic wave, respectively. These characteristics strongly suggest that this wave packet and its associated density cavity represent the collapsing envelope soliton-caviton pair formed as a result of OTSI, and in the present case, the strong turbulence processes probably play key roles in the beam stabilization as well as conversion of Langmuir waves into escaping radiation at 2f(pe) and 3f(pe).
C1 [Thejappa, G.; Bergamo, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Thejappa, G (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM thejappa.golla@nasa.gov
FU NASA [NNX09AB19G, NNX12AH47G]
FX The research of G. T. is supported by NASA grants NNX09AB19G and
NNX12AH47G. The SWAVES instruments include contributions from the
Observatoire de Paris, the University of Minnesota, the University of
California, Berkeley, and NASA/GSFC. We thank the referees for very
helpful and constructive comments.
NR 71
TC 8
Z9 8
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JUL
PY 2013
VL 118
IS 7
BP 4039
EP 4052
DI 10.1002/jgra.50441
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 226YN
UT WOS:000325073600010
ER
PT J
AU Hwang, KJ
Goldstein, ML
Wendel, DE
Fazakerley, AN
Gurgiolo, C
AF Hwang, K-J.
Goldstein, M. L.
Wendel, D. E.
Fazakerley, A. N.
Gurgiolo, C.
TI Cluster observations near reconnection X lines in Earth's magnetotail
current sheet
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE reconnection; electron diffusion region; X line; neutral sheet
ID COLLISIONLESS MAGNETIC RECONNECTION; FIELD; ACCELERATION; REGION; TAIL
AB Magnetic reconnection is an efficient way to convert magnetic energy into particle energy. In this paper, we use Cluster thermal electron and ion measurements in the vicinity of a reconnection X line to delineate the structure of the reconnection current sheet. Multispacecraft observations made by Cluster on 18 August 2002 indicate that an X line drifted close to the spacecraft, about 3.4 R-E earthward of the position where another X line had been observed earlier. Comparison of the Hall magnetic and electric field geometry and the observed properties of energetic electron beams streaming along the separatrix between the Cluster spacecraft indicates that the second X line formed within 20 s of the observation of the first X line. Repeated flow reversals and Hall field geometry together with the presence of a magnetic island embedded in the outflow region downstream of the first X line suggest that the initial current sheet was unstable, perhaps to the tearing mode. We identify a region with a thickness of 0.72 ion inertial lengths (29 electron inertial lengths, d(e)) of super-Alfvenic electron outflow (greater than the ion in-flow Alfven speed) during the period when the spacecraft was in the vicinity of the neutral sheet. Slightly below the neutral sheet, Cluster observed asymmetric counter-streaming electrons with a loss of axisymmetry in the electron (V-1,V-2) distribution functions over a thin boundary with a thickness of several d(e). This electron-scale transition layer was embedded in a much wider region where both the ion and electron Walen tests failed, and the electron super-Alfvenic bulk outflow jets with high-energy electron beams were detected. Those phenomena provide details of the substructure of the reconnection current sheet and suggest that the spacecraft traversed or skimmed the tailward edge of an elongated electron current layer. We also note that this event differs from a previously reported reconnection event in that strong electron temperature anisotropy (T-vertical bar>T) is observed both in the inflow region and in the exhaust, where the anisotropy appears to be associated with the elongated electron outflow jets.
C1 [Hwang, K-J.; Goldstein, M. L.; Wendel, D. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hwang, K-J.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Fazakerley, A. N.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Gurgiolo, C.] Bitterroot Basic Res, Hamilton, MT USA.
RP Hwang, KJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM kyoung-joo.hwang@nasa.gov
RI Wendel, Deirdre/D-4429-2012
OI Wendel, Deirdre/0000-0002-1925-9413
FU NASA's Magnetospheric Multiscale Mission Interdisciplinary Science
grant; Cluster mission; NASA [NXX10AQ46G]; UK STFC [ST/H00260X/1]
FX We acknowledge helpful comments by J. Egedal as well as the
Cluster-PEACE, FGM, CIS, EFW, and STAFF teams along with the Cluster
Active Archive for providing the data used in this study. K.-J. Hwang,
M. L. Goldstein, and D. E. Wendel were supported, in part, by NASA's
Magnetospheric Multiscale Mission Interdisciplinary Science grant to the
Goddard Space Flight Center and by the Cluster mission. C. Gurgiolo was
supported, in part, by NASA grant NXX10AQ46G. A. N. Fazakerley was
supported, in part, by UK STFC grant ST/H00260X/1.
NR 40
TC 10
Z9 10
U1 0
U2 7
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 JUL
PY 2013
VL 118
IS 7
BP 4199
EP 4209
DI 10.1002/jgra.50403
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 226YN
UT WOS:000325073600023
ER
PT J
AU Trattner, KJ
Allegrini, F
Dayeh, MA
Funsten, HO
Fuselier, SA
Heirtzler, D
Janzen, P
Kucharek, H
McComas, DJ
Mobius, E
Moore, TE
Petrinec, SM
Reisenfeld, DB
Schwadron, NA
Wurz, P
AF Trattner, K. J.
Allegrini, F.
Dayeh, M. A.
Funsten, H. O.
Fuselier, S. A.
Heirtzler, D.
Janzen, P.
Kucharek, H.
McComas, D. J.
Moebius, E.
Moore, T. E.
Petrinec, S. M.
Reisenfeld, D. B.
Schwadron, N. A.
Wurz, P.
TI The free escape continuum of diffuse ions upstream of the Earth's
quasi-parallel bow shock
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE shock acceleration; free escape boundary; energetic ions
ID HYDROMAGNETIC WAVE EXCITATION; MULTI-SPACECRAFT OBSERVATIONS; ENERGETIC
IONS; SOLAR-WIND; PARTICLE EVENTS; ACCELERATION; PROTONS; POPULATIONS;
MAGNETOTAIL; DOWNSTREAM
AB The Earth's bow shock is very efficient in accelerating ions out of the incident solar wind distribution to high energies (approximate to 200keV/e). Fluxes of energetic ions accelerated at the quasi-parallel bow shock, also known as diffuse ions, are best represented by exponential spectra in energy/charge, which require additional assumptions to be incorporated into these model spectra. One of these assumptions is a so-called free escape boundary along the interplanetary magnetic field into the upstream direction. Locations along the IBEX orbit are ideally suited for in situ measurements to investigate the existence of an upstream free escape boundary for bow shock accelerated ions. In this study we use 2years of ion measurements from the background monitor on the IBEX spacecraft, supported by ACE solar wind observations. The IBEX Background Monitor is sensitive to protons >14keV, which includes the energy of the maximum flux for diffuse ions. With increasing distance from the bow shock along the interplanetary magnetic field, the count rates for diffuse ions stay constant for ions streaming away from the bow shock, while count rates for diffuse ions streaming toward the shock gradually decrease from a maximum value to similar to 1/e at distances of about 10 R-E to 14 R-E. These observations of a gradual decrease support the transition to a free escape continuum for ions of energy >14keV at distances from 10 R-E to 14 R-E from the bow shock.
C1 [Trattner, K. J.; Petrinec, S. M.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA.
[Allegrini, F.; Dayeh, M. A.; Fuselier, S. A.; McComas, D. J.] SW Res Inst, San Antonio, TX USA.
[Allegrini, F.; McComas, D. J.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA.
[Funsten, H. O.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Heirtzler, D.; Kucharek, H.; Moebius, E.; Schwadron, N. A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Janzen, P.; Reisenfeld, D. B.] Univ Montana, Dept Phys & Astron, Missoula, MT 59812 USA.
[Moore, T. E.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Wurz, P.] Univ Bern, Inst Phys, Bern, Switzerland.
RP Trattner, KJ (reprint author), Lockheed Martin Adv Technol Ctr, 3251 Hanover St, Palo Alto, CA 94304 USA.
EM trattner@spasci.com
RI Funsten, Herbert/A-5702-2015; Reisenfeld, Daniel/F-7614-2015;
OI Funsten, Herbert/0000-0002-6817-1039; Moebius,
Eberhard/0000-0002-2745-6978
FU IBEX mission as a part of NASA's Explorer program; NASA [599769Q,
NNX08AF35G, NNX09AM72G, NNX11AJ09G, NNG05GE15G]; National Science
Foundation [1102572]
FX We acknowledge the use of ISTP KP database. Solar wind observations were
provided by the ACE Solar Wind Experiment (ACE/SWE) [McComas et al.,
1998]. The IMF measurements are provided by the ACE Magnetic Field
Instrument (ACE/MFI) [Smith et al., 1998]. Support for this study comes
from the IBEX mission as a part of NASA's Explorer program. IBEX is the
result of efforts from a large number of scientists, engineers, and
others; all who contributed to this mission share in its success. The
work at Lockheed Martin was supported by NASA contracts 599769Q,
NNX08AF35G, NNX09AM72G, NNX11AJ09G, and NNG05GE15G and by grant 1102572
from the National Science Foundation.
NR 41
TC 1
Z9 1
U1 0
U2 3
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 JUL
PY 2013
VL 118
IS 7
BP 4425
EP 4434
DI 10.1002/jgra.50447
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 226YN
UT WOS:000325073600043
ER
PT J
AU Morgan, DD
Gurnett, DA
Kirchner, DL
Fox, JL
Nielsen, E
Plaut, JJ
AF Morgan, D. D.
Gurnett, D. A.
Kirchner, D. L.
Fox, J. L.
Nielsen, E.
Plaut, J. J.
TI Variation of the Martian ionospheric electron density from Mars Express
radar soundings (vol 118, pg 4710, 2013)
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Correction
DE Mars; ionosphere; radar
C1 [Morgan, D. D.; Gurnett, D. A.; Kirchner, D. L.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Fox, J. L.] Wright State Univ, Dept Phys, Dayton, OH 45435 USA.
[Nielsen, E.] Max Plank Inst Solar Syst Studies, Katlenburg Lindau, Germany.
[Plaut, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Morgan, DD (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
NR 1
TC 2
Z9 2
U1 0
U2 0
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 JUL
PY 2013
VL 118
IS 7
BP 4710
EP 4710
DI 10.1002/jgra.50369
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 226YN
UT WOS:000325073600066
ER
PT J
AU Katzberg, SJ
Dunion, J
Ganoe, GG
AF Katzberg, Stephen J.
Dunion, Jason
Ganoe, George G.
TI The use of reflected GPS signals to retrieve ocean surface wind speeds
in tropical cyclones
SO RADIO SCIENCE
LA English
DT Article
DE GPS reflection
ID GLOBAL POSITIONING SYSTEM; SEA-SURFACE; AIRCRAFT; DROPWINDSONDE;
HURRICANES; SCATTERING
AB Since the first intentional acquisition of GPS signals reflected from water bodies, one of the objectives which has driven the research is to determine whether the acquired signal can provide useful geophysical information about the reflecting surface. One obvious condition of considerable interest is ocean surface wind speed. Theory suggested that the reflection technique, a form of bistatic RADAR, would be sensitive to surface roughness which in turn is driven by wind speed. This paper reports the results derived from data acquired over the past decade of applying the GPS reflection technique to ocean surface winds, particularly ocean surface winds in tropical cyclones. Examples of wind speed retrievals will be given for some illustrative cases of hurricanes and tropical storms. The results from several hurricanes and tropical storms on how the signal was calibrated will be presented. In addition, a quantitative comparison will be given between dropsondes deployed by NOAA during the storms and GPS reflection derived wind speeds taken at the same time. Conditions in which the GPS technique offers excellent comparisons as well as examples where the comparison is not so good will be presented. Suggestions will be given as to when the GPS technique can be used with confidence and when it is likely to be at variance with other methods.
C1 [Katzberg, Stephen J.; Ganoe, George G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Dunion, Jason] Univ Miami, CIMAS, Coral Gables, FL 33124 USA.
[Dunion, Jason] NOAA, Hurricane Res Div, AOML, Miami, FL USA.
RP Katzberg, SJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM Stephen.J.Katzberg@nasa.gov
RI Dunion, Jason/B-1352-2014
OI Dunion, Jason/0000-0001-7489-0569
NR 29
TC 13
Z9 13
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
J9 RADIO SCI
JI Radio Sci.
PD JUL
PY 2013
VL 48
IS 4
BP 371
EP 387
DI 10.1002/rds.20042
PG 17
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA 224WF
UT WOS:000324921400002
ER
PT J
AU Ngwira, CM
Klenzing, J
Olwendo, J
D'ujanga, FM
Stoneback, R
Baki, P
AF Ngwira, Chigomezyo M.
Klenzing, Jeff
Olwendo, Joseph
D'ujanga, Florence M.
Stoneback, Russell
Baki, Paul
TI A study of intense ionospheric scintillation observed during a quiet day
in the East African low-latitude region
SO RADIO SCIENCE
LA English
DT Article
DE ionosphere; amplitude scintillation; total electron content; equatorial
plasma bubbles
ID EQUATORIAL PLASMA BUBBLES; TOTAL ELECTRON-CONTENT; SPREAD-F; DRIFT
VELOCITY; GPS; SATELLITE; IRREGULARITIES; SPECIFICATION; FLUCTUATIONS;
SYSTEMS
AB Ionospheric plasma density irregularities are a common feature of the equatorial and low-latitude ionosphere. These irregularities are known to cause fading and phase fluctuation (scintillation) of L-band radio navigation signals such as those used by Global Navigation Satellite Systems. This study investigates the occurrence of intense ionospheric scintillation in the postsunset period during a geomagnetically quiet day on 8 April 2011. In particular, we use Global Positioning System (GPS) derived observations, i.e., total electron content (TEC) and amplitude scintillation intensity index, S4, to examine the occurrence of intense scintillations at two low-latitude stations in the East African sector. Deep TEC depletions, in some cases roughly 40 TECU, are observed consistently with the occurrence of intense scintillations. In addition, we compare the GPS-based observations to the Communication/Navigation Outage Forecasting System (C/NOFS) satellite plasma data. The intense scintillation events also correspond well with plasma depletion structures present on the C/NOFS observations and can be attributed to strong plasma bubble activity. The C/NOFS data also provide evidence of strong upward drift velocities (> 60 m/s) associated with the depletions, which may have contributed to the generation of the strong irregularities.
C1 [Ngwira, Chigomezyo M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ngwira, Chigomezyo M.; Klenzing, Jeff] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Olwendo, Joseph] Pwani Univ Coll, Dept Math & Phys, Kilifi, Kenya.
[Olwendo, Joseph] Univ Nairobi, Dept Phys, Nairobi, Kenya.
[D'ujanga, Florence M.] Makerere Univ, Dept Phys, Kampala, Uganda.
[Stoneback, Russell] Univ Texas Dallas, WB Hanson Ctr Space Sci, Richardson, TX 75083 USA.
[Baki, Paul] Kenya Polytech Univ Coll, Sch Pure & Appl Sci, Nairobi, Kenya.
RP Ngwira, CM (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM chigomezyo.ngwira@nasa.gov
RI Klenzing, Jeff/E-2406-2011; ngwira, chigomezyo/D-7310-2012;
OI Klenzing, Jeff/0000-0001-8321-6074; Stoneback,
Russell/0000-0001-7216-4336
NR 42
TC 1
Z9 2
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
EI 1944-799X
J9 RADIO SCI
JI Radio Sci.
PD JUL
PY 2013
VL 48
IS 4
BP 396
EP 405
DI 10.1002/rds.20045
PG 10
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA 224WF
UT WOS:000324921400004
ER
PT J
AU Arevalo, R
McDonough, WF
Stracke, A
Willbold, M
Ireland, TJ
Walker, RJ
AF Arevalo, Ricardo, Jr.
McDonough, William F.
Stracke, Andreas
Willbold, Matthias
Ireland, Thomas J.
Walker, Richard J.
TI Simplified mantle architecture and distribution of radiogenic power
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
DE OIB; mantle; hotspot; source; radiogenic heat; mass balance
ID OCEAN ISLAND BASALTS; TRACE ELEMENT FRACTIONATION; TH-PA-RA; EARTHS
MANTLE; ISOTOPIC EVIDENCE; FRENCH-POLYNESIA; CENTRAL PACIFIC;
U-235-PA-231 DISEQUILIBRIA; HETEROGENEOUS MANTLE; ABYSSAL PERIDOTITES
AB The mantle components that represent the source region of ocean island basalts (OIB) and feed hotspot volcanism are predicted to contain 160 +/- 20 (2 sigma(m)) ng/g Th, a heat-producing element. This critical model composition indicates that the OIB source region (OSR) comprises a significant amount of recycled oceanic crust and constitutes 19(-2)(+3) (2 sigma(m))% of the mantle by mass. The mass fraction of this reservoir supports a mantle architecture with a basal thermochemical layering at an average depth of 2000 +/- 100 (2 sigma(m)) km or two thermochemical piles that extend up to midmantle levels. The hotspot source described here generates 10 pW/kg of radiogenic heat and supplies 7.3 TW to the planet's total surface heat flux. Given that the silicate portion of the Earth produces some 20.4 TW of radiogenic power, with 7.2 TW derived from the continental crust, the mantle source responsible for mid-ocean ridge volcanism provides only 5.9 TW of radiogenic power (or <2 pW/kg). As a result, the source of hotspots generates >5x more radiogenic heat than the source of mid-ocean ridges, thus contributing to the energetics that drive mantle convection and potentially the formation of long-lived plumes via bottom heating of the modern mantle. The potential for a sequestered or unsampled mantle reservoir would impact the relative mass fractions of the source regions of OIB and mid-ocean ridge volcanism but not the compositional model of the OSR presented here.
C1 [Arevalo, Ricardo, Jr.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD USA.
[McDonough, William F.; Walker, Richard J.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA.
[Stracke, Andreas] Univ Munster, Inst Mineral, D-48149 Munster, Germany.
[Willbold, Matthias] Univ Bristol, Sch Earth Sci, Bristol, Avon, England.
[Ireland, Thomas J.] Boston Univ, Dept Earth Sci, Boston, MA 02215 USA.
RP Arevalo, R (reprint author), NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD USA.
EM ricardo.d.arevalo@nasa.gov
RI Walker, Richard/K-6869-2016; McDonough, William/I-7720-2012;
OI Walker, Richard/0000-0003-0348-2407; McDonough,
William/0000-0001-9154-3673; Willbold, Matthias/0000-0003-2178-2470
FU NSF [EAR-0739006]; NSF CSEDI grant [0757808]
FX We thank Bill White, Emily Klein, and an anonymous reviewer for their
insightful comments regarding this work. This study was funded by NSF
grant EAR-0739006 (to W. F. M.) and NSF CSEDI grant 0757808 (to R.J.W.).
NR 145
TC 5
Z9 5
U1 0
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD JUL
PY 2013
VL 14
IS 7
BP 2265
EP 2285
DI 10.1002/ggge.20152
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 210JP
UT WOS:000323828800012
ER
PT J
AU Duan, HY
Xu, R
Li, JC
Yuan, YG
Wang, QX
Hadi, NI
AF Duan Huanyun
Xu Rui
Li Jianchang
Yuan Yage
Wang Qiuxia
Hadi, Nomana Intekhab
TI Analysis on sustainable development countermeasures and barriers of
rural household biogas in China
SO JOURNAL OF RENEWABLE AND SUSTAINABLE ENERGY
LA English
DT Article
AB The paper has been designed based on the experimental survey and questionnaires to 797 farmers, 25 technicians in 41 villages, and 8 towns of Yuxi region, Yunnan, China-to analyze the universal problems in biogas utilization process, including (a) low biogas utilization rate, critical dysfunctional phenomenon; (b) poor comprehensive utilization of biogas, bio-slurry, and residue; and (c) imperfect post-installation service system. Combined with the investigated findings, the article has analyzed the main causes and influencing factors which lead to the different problems. In the end, having based on the adequate interpretation about the studying conclusion, recommendations and countermeasures for the future sustainable development of China's rural household biogas proper measures can be put forward onto consideration table, which includes (a) encourage joint household biogas construction; (b) carry out comprehensive utilization demonstration actively; (c) establish a relatively complete post-installation service system by encouraging technicians to get involved in the maintenance and management initiations. The establishment of incentive systems and co-operative approaches can help to achieve the ultimate target of appropriately "biogas-designed" that are sustainably developed and constructed in China. (C) 2013 AIP Publishing LLC.
C1 [Duan Huanyun; Xu Rui; Li Jianchang; Yuan Yage; Wang Qiuxia] Yannan Normal Univ, Solar Energy Inst, Coll Energy & Environm Sci, Kunming 650092, Peoples R China.
[Hadi, Nomana Intekhab] NASA, Ames Res Ctr, SETI Inst Affiliat, Moffett Field, CA 94035 USA.
RP Duan, HY (reprint author), Yannan Normal Univ, Solar Energy Inst, Coll Energy & Environm Sci, Kunming 650092, Peoples R China.
EM duanhuanyun@gmail.com; ecowatch.xr@gmail.com; jclee94213@yahoo.com.cn;
yuanyage@sina.cn; 798606608@qq.com; nomana.i.hadi@gmail.com
FU National Natural Science Foundation [51166014]; Wisions; Blue Moon Fund;
Global Environmental Institute; Nexus
FX We are thankful to Eco-Watch Institute and Yunnan Normal University
Solar Energy Research Institute Laboratory and staffs (Wang Fuxian,
Zhang Zhengyun, Liu Yanting, Li Yongbo, Leng Congbing, Luo Fei), as well
as the Yuxi Rural Energy Stations for helping in carrying out such
outstanding baseline project survey. We also want to mention
wholehearted gratitude towards Wisions, Blue Moon Fund, Global
Environmental Institute, and Nexus for sponsoring throughout the project
to get properly driven. This research was also funded by National
Natural Science Foundation (51166014). Nomana Intekhab Hadi a NASA Ames
Research Center USA research associate, who helps a lot in the project
and paper to be well reporter. Thanks to the entire team for their
outstanding supports in the project.
NR 7
TC 3
Z9 3
U1 1
U2 25
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1941-7012
J9 J RENEW SUSTAIN ENER
JI J. Renew. Sustain. Energy
PD JUL 1
PY 2013
VL 5
IS 4
AR 043116
DI 10.1063/1.4816690
PG 12
WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Energy & Fuels
SC Science & Technology - Other Topics; Energy & Fuels
GA 211XO
UT WOS:000323945600041
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneers A Series of Interviews With Significant Contributors
to Terahertz Science and Technology
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91109 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91109 USA.
[Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91109 USA.
NR 0
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 JUL
PY 2013
VL 3
IS 4
BP 347
EP 347
DI 10.1109/TTHZ.2013.2260372
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 210MD
UT WOS:000323836700002
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneer: Philippe Goy "If You Agree With the Majority, You
Might be Wrong"
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Biographical-Item
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
[Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA.
EM phs@caltech.edu
NR 0
TC 1
Z9 1
U1 0
U2 6
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 JUL
PY 2013
VL 3
IS 4
BP 348
EP 353
DI 10.1109/TTHZ.2013.2260373
PG 6
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 210MD
UT WOS:000323836700003
ER
PT J
AU Vaishampayan, P
Moissl-Eichinger, C
Puka, R
Schumann, P
Sproer, C
Augustus, A
Roberts, AH
Namba, G
Cisneros, J
Salmassi, T
Venkateswaran, K
AF Vaishampayan, Parag
Moissl-Eichinger, Christine
Puka, Ruediger
Schumann, Peter
Sproeer, Cathrin
Augustus, Angela
Roberts, Anne Hayden
Namba, Greg
Cisneros, Jessica
Salmassi, Tina
Venkateswaran, Kasthuri
TI Description of Tersicoccus phoenicis gen. nov., sp nov isolated from
spacecraft assembly clean room environments
SO INTERNATIONAL JOURNAL OF SYSTEMATIC AND EVOLUTIONARY MICROBIOLOGY
LA English
DT Article
ID POLAR LIPID-COMPOSITION; TAXONOMIC IMPLICATIONS; CLINICAL SPECIMENS; DNA
HYBRIDIZATION; COMB. NOV; COHN 1872; ARTHROBACTER; BACTERIA;
CLASSIFICATION; MICROORGANISMS
AB Two strains of aerobic, non-motile, Gram-reaction-positive cocci were independently isolated from geographically distinct spacecraft assembly clean room facilities (Kennedy Space Center, Florida, USA and Centre Spatial Guyanais, Kourou, French Guiana). A polyphasic study was carried out to delineate the taxonomic identity of these two isolates (1P05MA(T) and KO_PS43). The 16S rRNA gene sequences exhibited a high similarity when compared to each other (100%) and lower than 96.7% relatedness with Arthrobacter crystallopoietes ATCC 15481(T), Arthrobacter luteolus ATCC BAA-272(T), Arthrobacter tumbae DSM 16406(T) and Arthrobacter subterraneus DSM 17585(T). In contrast with previously described Arthrobacter species, the novel isolates maintained their coccidal morphology throughout their growth and did not exhibit the rod coccus life cycle typically observed in nearly all Arthrobacter species, except A. agilis. The distinct taxonomic identity of the novel isolates was confirmed based on their unique cell-wall peptidoglycan type (A.11.20; Lys-Ser-Ala(2)) and polar lipid profile (presence of phosphatidylglycerol, diphosphatidylglycerol, phosphatidylinositol, an unknown phospholipid and two unknown glycolipids). The G+C content of the genomic DNA was 70.6 mol%. The novel strains revealed MK-9(H-2) and MK-8(H-2) as dominant menaquinones and exhibited fatty acid profiles consisting of major amounts of anteiso-C-15:0 and anteiso-(17:0) and moderate amounts of iso-C-15:0 discriminating them again from closely related Arthrobacter species. Based on these observations, the authors propose that strains 1P05MA(T) and KO_PS43 be assigned into a separate genus Tersicoccus gen. nov. For this new taxon, comprising strains 1P05MA(T) and KO_PS43, we propose the name Tersicoccus phoenicis gen. nov., sp. nov. (the type species of Tersicoccus), represented by the type strain Tersicoccus phoenicis 1P05MA(T) (=NRRL B-59547(T)=DSM 30849(T)).
C1 [Vaishampayan, Parag; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA.
[Moissl-Eichinger, Christine] Univ Regensburg, Inst Microbiol, D-93053 Regensburg, Germany.
[Moissl-Eichinger, Christine] Univ Regensburg, Archaea Ctr, D-93053 Regensburg, Germany.
[Puka, Ruediger; Schumann, Peter; Sproeer, Cathrin] Leibniz Inst DSMZ German Collect Microorganisms &, D-38124 Braunschweig, Germany.
[Augustus, Angela; Roberts, Anne Hayden; Namba, Greg; Cisneros, Jessica; Salmassi, Tina] Calif State Univ Los Angeles, Dept Biol Sci, Los Angeles, CA 90032 USA.
RP Vaishampayan, P (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM vaishamp@jpl.nasa.gov
RI Moissl-Eichinger, Christine/A-6682-2015
OI Moissl-Eichinger, Christine/0000-0001-6755-6263
FU National Aeronautics and Space Administration; NRA ROSES grant; NAI-MIRS
grant; European Space Agency [20508/07/NL/EK]
FX The research described in this publication was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. Part of
this research was funded by a 2007 NRA ROSES grant to K. V., at
California State University Los Angeles funded by NAI-MIRS grant to T.
S. and at the Regensburg University (CME) under a contract with the
European Space Agency (no. 20508/07/NL/EK). The authors extend thanks to
Shariff Osman (JPL) and Petra Schwendner (DLR) for sampling and
cultivation as well as to Anika Wasner, Melanie Duckstein, Bettina
Straubler (all DSMZ) for excellent technical assistance.
NR 36
TC 4
Z9 4
U1 9
U2 35
PU SOC GENERAL MICROBIOLOGY
PI READING
PA MARLBOROUGH HOUSE, BASINGSTOKE RD, SPENCERS WOODS, READING RG7 1AG,
BERKS, ENGLAND
SN 1466-5026
EI 1466-5034
J9 INT J SYST EVOL MICR
JI Int. J. Syst. Evol. Microbiol.
PD JUL
PY 2013
VL 63
BP 2463
EP 2471
DI 10.1099/ijs.0.047134-0
PN 7
PG 9
WC Microbiology
SC Microbiology
GA 200QD
UT WOS:000323083100015
PM 23223813
ER
PT J
AU Bristow, TF
Grotzinger, JP
AF Bristow, Thomas F.
Grotzinger, John P.
TI Sulfate availability and the geological record of cold-seep deposits
SO GEOLOGY
LA English
DT Article
ID CARBONATE CRUST FORMATION; LOW MARINE SULFATE; SNOWBALL EARTH; GAS
HYDRATE; VENT SITES; METHANE; OXIDATION; OCEAN; OXYGENATION; CONSORTIUM
AB Cold-seep deposits are the remnants of ancient chemosynthetic ecosystems that derive energy from microbial anaerobic oxidation of methane (AOM) using seawater sulfate. They provide a physical record of a microbial process that plays a critical role in regulating biospheric methane. Although highly C-13-depleted kerogen suggests that AOM dates back 2.7 b.y., puzzlingly, the oldest reported cold seeps only appear at 635 Ma and lack carbon isotopic signals (<-30% Peedee belemnite) that are diagnostic of AOM in examples younger than 350 Ma. Using a one-dimensional biogeochemical reaction-transport model, we confirm that these discrepancies are an expected consequence of changes in seawater chemistry. More specifically, sub-millimolar (mM) to millimolar seawater sulfate concentrations ([SO42-](SW)) and elevated concentrations of dissolved inorganic carbon that characterized seawater through much of the Precambrian limited AOM-driven carbonate supersaturation and C-13 depletion, making seep carbonates less likely to form and more challenging to identify. Moderate 13C depletions observed in 420-370-m.y.-old cold-seep carbonates (independently identified by fossil assemblages and contextual and textural observations) indicate [SO42-](SW) < 5 mM in this interval. This is significant because low [SO42-](SW) has been linked to widespread ocean anoxia in the early Paleozoic, an environmental condition thought to have influenced the evolution, extinction, and recovery of early animals.
C1 [Bristow, Thomas F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Grotzinger, John P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Bristow, TF (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU NASA
FX This work was supported by a NASA Postdoctoral Fellowship to Bristow. We
thank M. Alperin, K. Soetaert, and F. Meysman for discussions and
several anonymous reviewers for their comments.
NR 34
TC 6
Z9 6
U1 4
U2 38
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD JUL
PY 2013
VL 41
IS 7
BP 811
EP 814
DI 10.1130/G34265.1
PG 4
WC Geology
SC Geology
GA 203EB
UT WOS:000323272400023
ER
PT J
AU Guingla, DAP
De Keyser, R
De Lannoy, GJM
Giustarini, L
Matgen, P
Pauwels, VRN
AF Guingla, Douglas A. Plaza
De Keyser, Robin
De Lannoy, Gabrielle J. M.
Giustarini, Laura
Matgen, Patrick
Pauwels, Valentijn R. N.
TI Improving particle filters in rainfall-runoff models: Application of the
resample-move step and the ensemble Gaussian particle filter
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE data assimilation; ensemble Kalman filter; particle filter;
rainfall-runoff models; Gaussian particle filter
ID SEQUENTIAL DATA ASSIMILATION; MONTE-CARLO METHODS; KALMAN FILTER; STATE
ESTIMATION; UNCERTAINTY; CALIBRATION; SYSTEMS
AB The objective of this paper is to analyze the improvement in the performance of the particle filter by including a resample-move step or by using a modified Gaussian particle filter. Specifically, the standard particle filter structure is altered by the inclusion of the Markov chain Monte Carlo move step. The second choice adopted in this study uses the moments of an ensemble Kalman filter analysis to define the importance density function within the Gaussian particle filter structure. Both variants of the standard particle filter are used in the assimilation of densely sampled discharge records into a conceptual rainfall-runoff model. The results indicate that the inclusion of the resample-move step in the standard particle filter and the use of an optimal importance density function in the Gaussian particle filter improve the effectiveness of particle filters. Moreover, an optimization of the forecast ensemble used in this study allowed for a better performance of the modified Gaussian particle filter compared to the particle filter with resample-move step.
C1 [Guingla, Douglas A. Plaza; De Lannoy, Gabrielle J. M.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
[Guingla, Douglas A. Plaza; De Keyser, Robin] Univ Ghent, Dept Elect Energy Syst & Automat, B-9000 Ghent, Belgium.
[De Lannoy, Gabrielle J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[De Lannoy, Gabrielle J. M.] Univ Space Res Assoc, Columbia, MD 90034 USA.
[Giustarini, Laura; Matgen, Patrick] Publ Res Ctr Gabriel Lippmann, Dept Environm & Agrobiotechnol, Luxembourg, Luxembourg.
[Pauwels, Valentijn R. N.] Monash Univ, Dept Civil Engn, Clayton, Vic 3168, Australia.
RP Guingla, DAP (reprint author), Univ Ghent, Lab Hydrol & Water Management, Coupure Links 653, B-9000 Ghent, Belgium.
EM DouglasAntonio.PlazaGuingla@UGent.be
OI Pauwels, Valentijn/0000-0002-1290-9313
FU Belgian Science Policy in the frame of the STEREO II programme;
Secretaria de Educacion Superior en Ciencia y Tecnologia (SENESCYT);
Escuela Superior Politecnica del Litoral (ESPOL Guayaquil-Ecuador);
Foundation of Scientific Research of the Flemish Community
(FWO-Vlaanderen)
FX The work in this paper has been funded mainly by the Belgian Science
Policy for the HYDRASENS project in the frame of the STEREO II programme
and partly by Secretaria de Educacion Superior en Ciencia y Tecnologia
(SENESCYT). The first author would like to express his gratitude to
Escuela Superior Politecnica del Litoral (ESPOL Guayaquil-Ecuador) for
the support during the initial phase of his postgraduate studies.
Gabrielle De Lannoy was a postdoctoral researcher funded by the
Foundation of Scientific Research of the Flemish Community
(FWO-Vlaanderen). The authors are very grateful to the Associate Editor
Hamid Moradkhani, the reviewer Nataliya Bulygina, and three anonymous
reviewers for the valuable contribution to the development of this
paper.
NR 52
TC 4
Z9 4
U1 1
U2 24
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 JUL
PY 2013
VL 49
IS 7
BP 4005
EP 4021
DI 10.1002/wrcr.20291
PG 17
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 205CP
UT WOS:000323419100009
ER
PT J
AU Risi, C
Noone, D
Frankenberg, C
Worden, J
AF Risi, Camille
Noone, David
Frankenberg, Christian
Worden, John
TI Role of continental recycling in intraseasonal variations of continental
moisture as deduced from model simulations and water vapor isotopic
measurements
SO WATER RESOURCES RESEARCH
LA English
DT Review
DE continental recycling; remote-sensing; water isotopes; moisture tracking
ID GENERAL-CIRCULATION MODEL; ATMOSPHERE COUPLING EXPERIMENT; BOUNDARY
LAYER INTERACTIONS; GLOBAL VEGETATION MODEL; LAND-SURFACE PROCESSES;
SOIL-MOISTURE; PART II; HYDROLOGIC-CYCLE; CLIMATE-CHANGE; UNITED-STATES
AB Climate models suggest an important role for land-atmosphere feedbacks on climate, but exhibit a large dispersion in the simulation of this role. We focus here on the role of continental recycling in the intraseasonal variability of continental moisture, and we explore the possibility of using water isotopic measurements to observationally constrain this role. Based on water tagging, we design a diagnostic, named D1, to estimate the role of continental recycling on the intraseasonal variability of continental moisture simulated by the general circulation model LMDZ. In coastal regions, the intraseasonal variability of continental moisture is mainly driven by the variability in oceanic moisture convergence. More inland, the role of continental recycling becomes important. The simulation of this role is sensitive to model parameters modulating evapotranspiration. Then we show that D in the low-level water vapor is a good tracer for continental recycling, due to the enriched signature of transpiration. Over tropical land regions, the intraseasonal relationship between D and precipitable water, named D1_iso, is a good observational proxy for D1. We test the possibility of using D1_iso for model evaluation using two satellite data sets: GOSAT and TES. LMDZ captures well the spatial patterns of D1_iso, but underestimates its values. However, a more accurate description of how atmospheric processes affect the isotopic composition of water vapor is necessary before concluding with certitude that LMDZ underestimates the role of continental recycling.
C1 [Risi, Camille] CNRS, IPSL, LMD, F-75005 Paris, France.
[Noone, David] Univ Colorado, Dept Atmospher & Ocean Sci, CIRES, Boulder, CO 80309 USA.
[Frankenberg, Christian; Worden, John] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Risi, C (reprint author), CNRS, IPSL, LMD, F-75005 Paris, France.
EM camille.risi@lmd.jussieu.fr
RI Frankenberg, Christian/A-2944-2013
OI Frankenberg, Christian/0000-0002-0546-5857
NR 152
TC 29
Z9 29
U1 3
U2 47
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 JUL
PY 2013
VL 49
IS 7
BP 4136
EP 4156
DI 10.1002/wrcr.20312
PG 21
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 205CP
UT WOS:000323419100018
ER
PT J
AU Almenara, JM
Bouchy, F
Gaulme, P
Deleuil, M
Havel, M
Gandolfi, D
Deeg, HJ
Wuchterl, G
Guillot, T
Gardes, B
Pasternacki, T
Aigrain, S
Alonso, R
Auvergne, M
Baglin, A
Bonomo, AS
Borde, P
Cabrera, J
Carpano, S
Cochran, WD
Csizmadia, S
Damiani, C
Diaz, RF
Dvorak, R
Endl, M
Erikson, A
Ferraz-Mello, S
Fridlund, M
Hebrard, G
Gillon, M
Guenther, E
Hatzes, A
Leger, A
Lammer, H
MacQueen, PJ
Mazeh, T
Moutou, C
Ollivier, M
Ofir, A
Patzold, M
Parviainen, H
Queloz, D
Rauer, H
Rouan, D
Santerne, A
Samuel, B
Schneider, J
Tal-Or, L
Tingley, B
Weingrill, J
AF Almenara, J. M.
Bouchy, F.
Gaulme, P.
Deleuil, M.
Havel, M.
Gandolfi, D.
Deeg, H. J.
Wuchterl, G.
Guillot, T.
Gardes, B.
Pasternacki, T.
Aigrain, S.
Alonso, R.
Auvergne, M.
Baglin, A.
Bonomo, A. S.
Borde, P.
Cabrera, J.
Carpano, S.
Cochran, W. D.
Csizmadia, Sz.
Damiani, C.
Diaz, R. F.
Dvorak, R.
Endl, M.
Erikson, A.
Ferraz-Mello, S.
Fridlund, M.
Hebrard, G.
Gillon, M.
Guenther, E.
Hatzes, A.
Leger, A.
Lammer, H.
MacQueen, P. J.
Mazeh, T.
Moutou, C.
Ollivier, M.
Ofir, A.
Paetzold, M.
Parviainen, H.
Queloz, D.
Rauer, H.
Rouan, D.
Santerne, A.
Samuel, B.
Schneider, J.
Tal-Or, L.
Tingley, B.
Weingrill, J.
TI Transiting exoplanets from the CoRoT space mission
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planetary systems; techniques: photometric; techniques: radial
velocities; techniques: spectroscopic
ID EXTRASOLAR PLANETS; HOT-JUPITER; GIANT PLANET; SUPER-EARTH; ORBIT;
STARS; METALLICITY; EVOLUTION; MASSES; SEARCH
AB We report the discovery of two transiting exoplanets, CoRoT-25b and CoRoT-26b, both of low density, one of which is in the Saturn mass-regime. For each star, ground-based complementary observations through optical photometry and radial velocity measurements secured the planetary nature of the transiting body and allowed us to fully characterize them. For CoRoT-25b we found a planetary mass of 0.27 similar to 0.04 M-Jup, a radius of 1.08(-0.10)(+0.3) R-Jup and hence a mean density of 0.15(-0.06)(+ 0.15) g cm(-3). The planet orbits an F9 mainsequence star in a 4.86-day period, that has a V magnitude of 15.0, solar metallicity, and an age of 4.5(-2.0) (+1.8)-Gyr. CoRoT-26b orbits a slightly evolved G5 star of 9.06 +/- 1.5-Gyr age in a 4.20-day period that has solar metallicity and a V magnitude of 15.8. With a mass of 0.52 +/- 0.05 MJup, a radius of 1.26(-0.07)(+0.13) R-Jup, and a mean density of 0.28(-0.07)(+0.09) g cm(-3), it belongs to the low-mass hot-Jupiter population. Planetary evolution models allowed us to estimate a core mass of a few tens of Earth mass for the two planets with heavy-element mass fractions of 0.52(-0.15)(+0.08) and 0.26(-0.08)(+0.05), respectively, assuming that a small fraction of the incoming flux is dissipated at the center of the planet. In addition, these models indicate that CoRoT-26b is anomalously large compared with what standard models could account for, indicating that dissipation from stellar heating could cause this size.
C1 [Almenara, J. M.; Bouchy, F.; Deleuil, M.; Gardes, B.; Bonomo, A. S.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Bouchy, F.; Hebrard, G.] Inst Astrophys Paris, F-75014 Paris, France.
[Gaulme, P.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Havel, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wuchterl, G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Deeg, H. J.] Inst Astrofis Canarias, Tenerife 38205, Spain.
[Alonso, R.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany.
[Alonso, R.] Lab Cassiopee, Observ Cote Azur, F-06304 Nice 4, France.
[Guenther, E.; Hatzes, A.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany.
[Guillot, T.] Univ Oxford, Dept Phys, Oxford, England.
[Csizmadia, Sz.; Erikson, A.] Observ Univ Geneva, CH-1290 Sauverny, Switzerland.
[MacQueen, P. J.] LESIA, Obs Paris, F-92195 Meudon, France.
[Paetzold, M.] INAF Osservatorio Astron Torino, I-10025 Pino, Torinese, Italy.
[Endl, M.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Dvorak, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Leger, A.] Univ Sao Paulo, IAG, BR-05508 Sao Paulo, Brazil.
[Lammer, H.] Univ Gottingen, Inst Astrophys, D-37073 Gottingen, Germany.
[Rauer, H.] Univ Cologne, Rhein Inst Umweltforsch, D-50931 Cologne, Germany.
[Paetzold, M.] TU Berlin, Ctr Astron & Astrophys, D-10623 Berlin, Germany.
[Ofir, A.] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92195 Meudon, France.
[Mazeh, T.; Tingley, B.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
RP Almenara, JM (reprint author), Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
EM josemanuel.almenara@oamp.fr
RI Santerne, Alexandre/M-9265-2013; Alonso, Roi/D-8799-2014; Tingley,
Brandon/E-5146-2014; Ferraz-Mello, Sylvio/B-7529-2013;
OI Santerne, Alexandre/0000-0002-3586-1316; Alonso,
Roi/0000-0001-8462-8126; Tingley, Brandon/0000-0003-4483-2661; Gandolfi,
Davide/0000-0001-8627-9628; Parviainen, Hannu/0000-0001-5519-1391; Deeg,
Hans-Jorg/0000-0003-0047-4241
FU Spanish Ministerio de Economia y Competividad [AYA2010-20982-C02-02,
AYA2012-39346-C02-02]; NASA Keck PI Data Award; NASA Exoplanet Science
Institute; W.M. Keck Foundation; NASA Postdoctoral Program at the Ames
Research Center; Oak Ridge Associated Universities through a contract
with NASA
FX The team at IAC acknowledges support by grants AYA2010-20982-C02-02 and
AYA2012-39346-C02-02 of the Spanish Ministerio de Economia y
Competividad. Some of the data presented was acquired with the IAC80
telescope operated at Teide Observatory on the island of Tenerife by the
Instituto de Astrofisica de Canarias. This research has made use of the
Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.
org. Part of this work was supported by a NASA Keck PI Data Award,
administered by the NASA Exoplanet Science Institute. Some of the data
presented herein were obtained at the W.M. Keck Observatory from
telescope time allocated to the National Aeronautics and Space
Administration through the agency's scientific partnership with the
California Institute of Technology and the University of California. The
Observatory was made possible by the generous financial support of the
W.M. Keck Foundation. The authors wish to recognize and acknowledge the
very significant cultural role and reverence that the summit of Mauna
Kea has always had within the indigenous Hawaiian community. We are most
fortunate to have the opportunity to conduct observations from this
mountain. This research was supported by an appointment to the NASA
Postdoctoral Program at the Ames Research Center, administered by Oak
Ridge Associated Universities through a contract with NASA.
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SC Astronomy & Astrophysics
GA 185YV
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ER
PT J
AU Aurass, H
Holman, G
Braune, S
Mann, G
Zlobec, P
AF Aurass, H.
Holman, G.
Braune, S.
Mann, G.
Zlobec, P.
TI Radio evidence for breakout reconnection in solar eruptive events
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: radio radiation; Sun: X-rays, gamma rays; Sun: coronal mass
ejections (CMEs); Sun: magnetic topology; Sun: flares; Sun: corona
ID CORONAL MASS EJECTION; 03 NOVEMBER 2003; X-RAY SOURCES; MAGNETIC
RECONNECTION; FLARE; MODEL; BURST; EMISSION; PHASE; WAVES
AB Context. Magnetic reconnection is understood to be fundamental to energy release in solar eruptive events (SEEs). In these events reconnection produces a magnetic flux rope above an arcade of hot flare loops. Breakout reconnection, a secondary reconnection high in the corona between this flux rope and the overlying magnetic field, has been hypothesized. Direct observational evidence for breakout reconnection has been elusive, however.
Aims. The aim of this study is to establish a plausible interpretation of the combined radio and hard X-ray (HXR) emissions observed during the impulsive phase of the near-limb X3.9-class SEE on 2003 November 03.
Methods. We study radio spectra (AIP), simultaneous radio images (Nancay Multi-frequency Radio Heliograph, NRH), and single-frequency polarimeter data (OAT). The radio emission is nonthermal plasma radiation with a complex structure in frequency and time. Emphasis is on the time interval when the HXR flare loop height was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI) to be at its minimum and an X-ray source was observed above the top of the arcade loops.
Results. Two stationary, meter-wavelength sources are observed radially aligned at 0.18 and 0.41 R-circle dot above the active region and HXR sources. The lower source is apparently associated with the upper reconnection jet of the flare current sheet (CS), and the upper source is apparently associated with breakout reconnection. Sources observed at lower radio frequencies surround the upper source at the expected locations of the breakout reconnection jets.
Conclusions. We believe the upper radio source is the most compelling evidence to date for the onset of breakout reconnection during a SEE. The height stationarity of the breakout sources and their dynamic radio spectrum discriminate them from propagating disturbances. Timing and location arguments reveal for the first time that both the earlier described above the flare loop top HXR source and the lower radio source are emission from the upper reconnection jet above the vertical flare CS.
C1 [Aurass, H.; Braune, S.; Mann, G.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Holman, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zlobec, P.] INAF Trieste Astron Observ OAT, I-34143 Trieste, Italy.
RP Aurass, H (reprint author), Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
EM haurass@aip.de
FU RHESSI Project; NASA Guest Investigator Grant; EU FP7-SPACE-1-program
[262773]; DLR grant [50QL0901]
FX The authors acknowledge the use of radio imaging data of the French
Multi-Frequency Radioheliograph in Nancay, and the open data policy of
the team running this instrument. H.A. thanks A. Kerdraon for advice
concerning the NRH data. We are also obliged to A. Veronig and S.
Krucker (RHESSI data), H. Meszarosova, M. Karlicky (Astronomical
Observatory Ondrejov, Czech Republic), and W. Potzi (Univ. Graz, Obs.
Kanzelhohe, Austria) for information about observations. We took profit
from the use of SOHO and GOES-SXI data. The authors gratefully
acknowledge the helpful comments of an unknown referee. G.D.H.
acknowledges support from the RHESSI Project and a NASA Guest
Investigator Grant. This work was stimulated by the participation of
H.A. and S.B. in the EU FP7-SPACE2010-1-program under grant no. 262773.
The work of S.B. was also supported by the DLR grant No. 50QL0901.
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SC Astronomy & Astrophysics
GA 185YV
UT WOS:000322008600040
ER
PT J
AU Benoit-Levy, A
Dechelette, T
Benabed, K
Cardoso, JF
Hanson, D
Prunet, S
AF Benoit-Levy, A.
Dechelette, T.
Benabed, K.
Cardoso, J. -F.
Hanson, D.
Prunet, S.
TI Full-sky CMB lensing reconstruction in presence of sky-cuts
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing: weak; methods: data analysis; cosmic background
radiation
ID POWER SPECTRUM; MICROWAVE; MAPS; PLANCK
AB We consider the reconstruction of the CMB lensing potential and its power spectrum on the full sphere in presence of sky-cuts due to point sources and Galactic contamination. These two effects are treated separately. Small regions contaminated by point sources are filled in using constrained Gaussian realizations. The Galactic plane is simply removed using an apodized mask before lensing reconstruction. This algorithm recovers the power spectrum of the lensing potential with no significant bias.
C1 [Benoit-Levy, A.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Benoit-Levy, A.; Dechelette, T.; Benabed, K.; Cardoso, J. -F.; Prunet, S.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Cardoso, J. -F.] Univ Paris 06, CNRS, UMR 7164, F-75013 Paris, France.
[Cardoso, J. -F.] CNRS, Lab Traitement & Informat, UMR 5141, F-75634 Paris 13, France.
[Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France.
[Hanson, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hanson, D.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
RP Benoit-Levy, A (reprint author), UCL, Dept Phys & Astron, London WC1E 6BT, England.
EM benoitl@star.ucl.ac.uk
FU Leverhulme Trust; STFC; CITA National Fellowship
FX A.B.L. acknowledges fruitful discussions with E. Hivon. A.B.L. wishes to
thank the Jet Propulsion Laboratory (JPL), where part of this work was
carried, for kind hospitality. A.B.L. is supported by the Leverhulme
Trust and STFC. D.H. acknowledges the support of a CITA National
Fellowship. Part of this work has been initiated within the CMB lensing
working group of the Planck Collaboration. We also acknowledge the use
of the HEALPix package and the cosmological code CAMB.
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PT J
AU Benvenuto, F
Schwartz, R
Piana, M
Massone, AM
AF Benvenuto, F.
Schwartz, R.
Piana, M.
Massone, A. M.
TI Expectation maximization for hard X-ray count modulation profiles
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE methods: statistical; techniques: image processing; Sun: flares; Sun:
X-rays, gamma rays
ID MULTIRESOLUTION IMAGE-RECONSTRUCTION; SOLAR-SPECTROSCOPIC-IMAGER;
VISIBILITIES; LIKELIHOOD; RHESSI; FLARES
AB Context. This paper is concerned with the image reconstruction problem when the measured data are solar hard X-ray modulation profiles obtained from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) instrument.
Aims. Our goal is to demonstrate that a statistical iterative method classically applied to the image deconvolution problem is very effective when utilized to analyze count modulation profiles in solar hard X-ray imaging based on rotating modulation collimators.
Methods. The algorithm described in this paper solves the maximum likelihood problem iteratively and encodes a positivity constraint into the iterative optimization scheme. The result is therefore a classical expectation maximization method this time applied not to an image deconvolution problem but to image reconstruction from count modulation profiles. The technical reason that makes our implementation particularly effective in this application is the use of a very reliable stopping rule which is able to regularize the solution providing, at the same time, a very satisfactory Cash-statistic (C-statistic).
Results. The method is applied to both reproduce synthetic flaring configurations and reconstruct images from experimental data corresponding to three real events. In this second case, the performance of expectation maximization, when compared to Pixon image reconstruction, shows a comparable accuracy and a notably reduced computational burden; when compared to CLEAN, shows a better fidelity with respect to the measurements with a comparable computational effectiveness.
Conclusions. If optimally stopped, expectation maximization represents a very reliable method for image reconstruction in the RHESSI context when count modulation profiles are used as input data.
C1 [Benvenuto, F.; Piana, M.] Univ Genoa, Dipartimento Matemat, I-16146 Genoa, Italy.
[Schwartz, R.] Catholic Univ, Greenbelt, MD 20771 USA.
[Schwartz, R.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Piana, M.; Massone, A. M.] CNR SPIN, I-16146 Genoa, Italy.
RP Benvenuto, F (reprint author), Univ Genoa, Dipartimento Matemat, Via Dodecaneso 35, I-16146 Genoa, Italy.
EM piana@dima.unige.it
RI piana, michele/H-9376-2015;
OI PIANA, MICHELE/0000-0003-1700-991X
FU European Community [263086]
FX The experiment with synthetic data in Sect. 4 was conceived in
collaboration with A. G. Emslie and G. H. Hurford, who are kindly
acknowledged. This work was supported by the European Community
Framework Program 7, "High Energy Solar Physics Data in Europe (HESPE)",
Grant Agreement No. 263086.
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ER
PT J
AU Bouret, JC
Lanz, T
Martins, F
Marcolino, WLF
Hillier, DJ
Depagne, E
Hubeny, I
AF Bouret, J. -C.
Lanz, T.
Martins, F.
Marcolino, W. L. F.
Hillier, D. J.
Depagne, E.
Hubeny, I.
TI Massive stars at low metallicity Evolution and surface abundances of O
dwarfs in the SMC
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: early-type; stars: fundamental parameters; stars: rotation;
stars: abundances; Magellanic Clouds
ID SMALL-MAGELLANIC-CLOUD; VLT-FLAMES SURVEY; ELECTRON-IMPACT-EXCITATION;
B-TYPE STARS; MAIN-SEQUENCE STARS; ULTRAVIOLET SPECTRAL MORPHOLOGY;
PHOTOIONIZATION CROSS-SECTIONS; EFFECTIVE COLLISION STRENGTHS; BLANKETED
MODEL ATMOSPHERES; EFFECTIVE TEMPERATURE SCALE
AB Aims. We aim to study the properties of massive stars at low metallicity, with an emphasis on their evolution, rotation, and surface abundances. We focus on O-type dwarfs in the Small Magellanic Cloud. These stars are expected to have weak winds that do not remove significant amounts of their initial angular momentum.
Methods. We analyzed the UV and optical spectra of twenty-three objects using the NLTE stellar atmosphere code CMFGEN and derived photospheric and wind properties.
Results. The observed binary fraction of the sample is approximate to 26%, which is consistent with more systematic studies if one considers that the actual binary fraction is potentially larger owing to low-luminosity companions and that the sample was biased because it excluded obvious spectroscopic binaries. The location of the fastest rotators in the Hertzsprung-Russell (H-R) diagram built with fast-rotating evolutionary models and isochrones indicates that these could be several Myr old. The off set in the position of these fast rotators compared with the other stars confirms the predictions of evolutionary models that fast-rotating stars tend to evolve more vertically in the H-R diagram. Only one star of luminosity class Vz, expected to best characterize extreme youth, is located on the zero-age main sequence, the other two stars are more evolved. We found that the distribution of O and B stars in the epsilon(N) - v sin i diagram is the same, which suggests that the mechanisms responsible for the chemical enrichment of slowly rotating massive stars depend only weakly on the star's mass. We furthermore confirm that the group of slowly rotating N-rich stars is not reproduced by the evolutionary tracks. Even for more massive stars and faster rotators, our results call for stronger mixing in the models to explain the range of observed N abundances. All stars have an N/C ratio as a function of stellar luminosity that match the predictions of the stellar evolution models well. More massive stars have a higher N/C ratio than the less massive stars. Faster rotators show on average a higher N/C ratio than slower rotators, again consistent with the expected trend of stronger mixing as rotation increases. When comparing the N/O versus N/C ratios with those of stellar evolution models, the same global qualitative agreement is reached. The only discrepant behavior is observed for the youngest two stars of the sample, which both show very strong signs of mixing, which is unexpected for their evolutionary status.
C1 [Bouret, J. -C.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Bouret, J. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lanz, T.] Univ Nice Sophia Antipolis, CNRS, Lab JL Lagrange, Observ Cote Azur,UMR 7293, F-06304 Nice 4, France.
[Martins, F.] Univ Montpellier 2, LUPM UMR 5299, F-34095 Montpellier 5, France.
[Martins, F.] CNRS, F-34095 Montpellier 5, France.
[Marcolino, W. L. F.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, Brazil.
[Hillier, D. J.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Hillier, D. J.] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA.
[Depagne, E.] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany.
[Hubeny, I.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Bouret, JC (reprint author), Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
EM Jean-Claude.Bouret@oamp.fr; Thierry.Lanz@oca.eu;
fabrice.martins@univ-montp2.fr; wagner@astro.ufrj.br; hillier@pitt.edu;
edepagne@aip.de; hubeny@as.arizona.edu
RI Marcolino, Wagner/M-7428-2014
FU French Agence Nationale de la Recherche (ANR); NASA [NAS5-26555,
NNX08AC146]; STScI theory grants [HST-AR-11756.01.A, HST-AR-12640.01.A]
FX We thank the referee for helpful comments and suggestions. We are
grateful to P. Crowther, C. Evans and P. Massey who provided several
optical spectra most useful to this work. We thank the French Agence
Nationale de la Recherche (ANR) for financial support under Programme
Blanc MaSiLU. This research has made use of the SIMBAD database,
operated at CDS, Strasbourg, France. STScI is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. J.-C. Bouret is indebted to George Sonneborn for
his invitation to work at NASA/GSFC when this work was initiated. This
work was supported by NASA grant NNX08AC146 to the University of
Colorado at Boulder. D.J.H. acknowledges support from STScI theory
grants HST-AR-11756.01.A and HST-AR-12640.01.A.
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GA 185YV
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ER
PT J
AU Eiroa, C
Marshall, JP
Mora, A
Montesinos, B
Absil, O
Augereau, JC
Bayo, A
Bryden, G
Danchi, W
del Burgo, C
Ertel, S
Fridlund, M
Heras, AM
Krivov, AV
Launhardt, R
Liseau, R
Lohne, T
Maldonado, J
Pilbratt, GL
Roberge, A
Rodmann, J
Sanz-Forcada, J
Solano, E
Stapelfeldt, K
Thebault, P
Wolf, S
Ardila, D
Arevalo, M
Beichmann, C
Faramaz, V
Gonzalez-Garcia, BM
Gutierrez, R
Lebreton, J
Martinez-Arnaiz, R
Meeus, G
Montes, D
Olofsson, G
Su, KYL
White, GJ
Barrado, D
Fukagawa, M
Grun, E
Kamp, I
Lorente, R
Morbidelli, A
Muller, S
Mutschke, H
Nakagawa, T
Ribas, I
Walker, H
AF Eiroa, C.
Marshall, J. P.
Mora, A.
Montesinos, B.
Absil, O.
Augereau, J. Ch.
Bayo, A.
Bryden, G.
Danchi, W.
del Burgo, C.
Ertel, S.
Fridlund, M.
Heras, A. M.
Krivov, A. V.
Launhardt, R.
Liseau, R.
Loehne, T.
Maldonado, J.
Pilbratt, G. L.
Roberge, A.
Rodmann, J.
Sanz-Forcada, J.
Solano, E.
Stapelfeldt, K.
Thebault, P.
Wolf, S.
Ardila, D.
Arevalo, M.
Beichmann, C.
Faramaz, V.
Gonzalez-Garcia, B. M.
Gutierrez, R.
Lebreton, J.
Martinez-Arnaiz, R.
Meeus, G.
Montes, D.
Olofsson, G.
Su, K. Y. L.
White, G. J.
Barrado, D.
Fukagawa, M.
Gruen, E.
Kamp, I.
Lorente, R.
Morbidelli, A.
Mueller, S.
Mutschke, H.
Nakagawa, T.
Ribas, I.
Walker, H.
TI DUst around NEarby Stars. The survey observational results
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE circumstellar matter; planetary systems; infrared: stars
ID SOLAR-TYPE STARS; MAIN-SEQUENCE STARS; KUIPER DEBRIS DISK; SUN-LIKE
STARS; BETA-PICTORIS; PLANETARY SYSTEMS; TEMPERATURE MINIMUM; MODEL
ATMOSPHERES; MASSIVE PLANETS; NSTARS PROJECT
AB Context. Debris discs are a consequence of the planet formation process and constitute the fingerprints of planetesimal systems. Their solar system counterparts are the asteroid and Edgeworth-Kuiper belts.
Aims. The DUNES survey aims at detecting extra-solar analogues to the Edgeworth-Kuiper belt around solar-type stars, putting in this way the solar system into context. The survey allows us to address some questions related to the prevalence and properties of planetesimal systems.
Methods. We used Herschel/PACS to observe a sample of nearby FGK stars. Data at 100 and 160 mu m were obtained, complemented in some cases with observations at 70 mu m, and at 250, 350 and 500 mu m using SPIRE. The observing strategy was to integrate as deep as possible at 100 mu m to detect the stellar photosphere.
Results. Debris discs have been detected at a fractional luminosity level down to several times that of the Edgeworth-Kuiper belt. The incidence rate of discs around the DUNES stars is increased from a rate of similar to 12.1% +/- 5% before Herschel to similar to 20.2% +/- 2%. A significant fraction (similar to 52%) of the discs are resolved, which represents an enormous step ahead from the previously known resolved discs. Some stars are associated with faint far-IR excesses attributed to a new class of cold discs. Although it cannot be excluded that these excesses are produced by coincidental alignment of background galaxies, statistical arguments suggest that at least some of them are true debris discs. Some discs display peculiar SEDs with spectral indexes in the 70-160 mu m range steeper than the Rayleigh-Jeans one. An analysis of the debris disc parameters suggests that a decrease might exist of the mean black body radius from the F-type to the K-type stars. In addition, a weak trend is suggested for a correlation of disc sizes and an anticorrelation of disc temperatures with the stellar age.
C1 [Eiroa, C.; Marshall, J. P.; Maldonado, J.; Meeus, G.] Univ Autonoma Madrid, Fac Ciencias, Dpto Fis Teor, E-28049 Madrid, Spain.
[Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain.
[Montesinos, B.; Sanz-Forcada, J.; Solano, E.; Arevalo, M.; Gutierrez, R.; Barrado, D.] Ctr Astrobiol INTA CSIC, Madrid 28691, Spain.
[Absil, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium.
[Augereau, J. Ch.; Ertel, S.; Faramaz, V.; Lebreton, J.] UJF Grenoble 1 CNRS INSU, IPAG, F-38041 Grenoble, France.
[Bayo, A.] European Space Observ, Santiago 19, Chile.
[Bayo, A.; Launhardt, R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Danchi, W.; Roberge, A.; Stapelfeldt, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[del Burgo, C.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico.
[Fridlund, M.; Heras, A. M.; Pilbratt, G. L.] ES TEC SRE, ESA Astrophys & Fundamental Phys Miss Div, NL-2201 AZ Noordwijk, Netherlands.
[Krivov, A. V.; Loehne, T.; Mueller, S.; Mutschke, H.] Inst Astrophys, D-07745 Jena, Germany.
[Krivov, A. V.; Loehne, T.; Mueller, S.; Mutschke, H.] Univ Jena, D-07745 Jena, Germany.
[Liseau, R.] Onsala Space Observ, Chalmers Univ Technol, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
[Rodmann, J.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Thebault, P.] LESIA, Observ Paris, F-92195 Meudon, France.
[Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany.
[Ardila, D.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Beichmann, C.] CALTECH, NASA, ExoPlanet Sci Inst, Pasadena, CA 91125 USA.
[Gonzalez-Garcia, B. M.] ISDEFE ESAC, Madrid 28691, Spain.
[Martinez-Arnaiz, R.; Montes, D.] Univ Complutense Madrid, Fac Ciencias Fis, Dpt Astrofis, E-28040 Madrid, Spain.
[Olofsson, G.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden.
[Su, K. Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[White, G. J.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[White, G. J.; Walker, H.] Open Univ, Dept Phys & Astrophys, Milton Keynes MK7 6AA, Bucks, England.
[Barrado, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain.
[Fukagawa, M.] Nagoya Univ, Nagoya, Aichi 4648601, Japan.
[Gruen, E.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Kamp, I.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Lorente, R.] ESAC ESA, Herschel Sci Ctr, Madrid 28691, Spain.
[Morbidelli, A.] Observ Cote Azur, F-06304 Nice 4, France.
[Nakagawa, T.] Japan Aerosp Explorat Agcy JAXA, ISAS, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ribas, I.] Inst Ciencies Espai CSIC IEEC, Fac Ciencias, Barcelona 08193, Spain.
[Arevalo, M.] ESA ESAC, Sci Arch Team, Madrid 28691, Spain.
RP Eiroa, C (reprint author), Univ Autonoma Madrid, Fac Ciencias, Dpto Fis Teor, Modulo 15,Campus Cantoblanco, E-28049 Madrid, Spain.
EM carlos.eiroa@uam.es
RI Montes, David/B-9329-2014; Roberge, Aki/D-2782-2012; Ribas,
Ignasi/M-2134-2014; Barrado Navascues, David/C-1439-2017; Sanz-Forcada,
Jorge/C-3176-2017; Montesinos, Benjamin/C-3493-2017;
OI Montes, David/0000-0002-7779-238X; Roberge, Aki/0000-0002-2989-3725;
Ribas, Ignasi/0000-0002-6689-0312; Barrado Navascues,
David/0000-0002-5971-9242; Sanz-Forcada, Jorge/0000-0002-1600-7835;
Montesinos, Benjamin/0000-0002-7982-2095; Su, Kate/0000-0002-3532-5580;
Marshall, Jonathan/0000-0001-6208-1801
FU Spanish grant [AYA2008-01727, AYA2011-26202, AYA2008-02038,
AYA2011-30147-C03-03]; Marie Curie Actions of the European Commision;
German DFG [Kr 2164/10-1, Lo 1715/1-1]; JPL/Caltech
FX C. Eiroa, J. Maldonado, J. P. Marshall, G. Meeus and B. Montesinos were
supported by the Spanish grants AYA2008-01727 and AYA2011-26202. A. Bayo
was partly supported by the Marie Curie Actions of the European
Commision (FT7-COFUND). J. Sanz was supported by Spanish grants
AYA2008-02038 and AYA2011-30147-C03-03. A. V. Krivov and T. Lohne
acknowledge support by the German DFG, grants Kr 2164/10-1 and Lo
1715/1-1. NASA support for this work (D. Ardila, Ch. Beichmann, G.
Bryden, W. Danchi, A. Roberge, K. Stapelfeldt) was provided through an
award issued by JPL/Caltech.
NR 108
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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 JUL
PY 2013
VL 555
AR A11
DI 10.1051/0004-6361/201321050
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 185YV
UT WOS:000322008600011
ER
PT J
AU Fioretti, V
Angelini, L
Mushotzky, RF
Koss, M
Malaguti, G
AF Fioretti, V.
Angelini, L.
Mushotzky, R. F.
Koss, M.
Malaguti, G.
TI X-ray view of four high-luminosity Swift/BAT AGN: Unveiling obscuration
and reflection with Suzaku
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: galaxies; galaxies: active
ID ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXIES; SUPERMASSIVE BLACK-HOLES; II
RADIO GALAXIES; DEEP FIELD-SOUTH; ABSORBING COLUMN DENSITIES;
HIGH-RESOLUTION MAPS; LOW-REDSHIFT; SPECTRAL PROPERTIES; HOST GALAXIES
AB Aims. A complete census of obscured active galactic nuclei (AGN) is necessary to reveal the history of the super massive black hole (SMBH) growth and galaxy evolution in the Universe given the complex feedback processes and the fact that much of this growth occurs in an obscured phase. In this context, hard X-ray surveys and dedicated follow-up observations represent a unique tool for selecting highly absorbed AGN and for characterizing the obscuring matter surrounding the SMBH. Here we focus on the absorption and reflection occurring in highly luminous, quasar-like AGN, to study the relation between the geometry of the absorbing matter and the AGN nature (e.g. X-ray, optical, and radio properties), and to help to determine the column density dependency on the AGN luminosity.
Methods. The Swift/BAT nine-month survey observed 153 AGN, all with ultra-hard X-ray BAT fluxes in excess of 10(-11) erg cm(-2) s(-1) and an average redshift of 0.03. Among them, four of the most luminous BAT AGN (44.73 < Log L-BAT < 45.31) were selected as targets of Suzaku follow-up observations: J2246.0+3941 (3C 452), J0407.4+0339 (3C 105), J0318.7+6828, and J0918.5+0425. The column density, scattered/reflected emission, the properties of the Fe K line, and a possible variability are fully analyzed. For the latter, the spectral properties from Chandra, XMM-Newton and Swift/XRT public observations were compared with the present Suzaku analysis, adding an original spectral analysis when none was available from the literature.
Results. Of our sample, 3C 452 is the only certain Compton-thick AGN candidate because of i) the high absorption (N-H similar to 4 x 10(23) cm(-2)) and strong Compton reflection; ii) the lack of variability; iii) the "buried" nature, i.e. the low scattering fraction (<0.5%) and the extremely low relative [OIII] luminosity. In contrast 3C 105 is not reflection-dominated, despite the comparable column density, X-ray luminosity and radio morphology, but shows a strong long-term variability in flux and scattering fraction, consistent with the soft emission being scattered from a distant region (e.g., the narrow emission line region). The sample presents high (> 100) X-to-[OIII] luminosity ratios, with an extreme value of R-[OIII](X) similar to 800 for 3C 452, confirming the [OIII] luminosity to be affected by residual extinction in presence of mild absorption, especially for "buried" AGN such as 3C 452. Three of our targets are powerful FRII radio galaxies, which is shown by their high luminosity and absorption; this makes them the most luminous and absorbed AGN of the BAT Seyfert survey despite the inversely proportional N-H - L-X relation.
C1 [Fioretti, V.; Malaguti, G.] INAF Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy.
[Fioretti, V.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Angelini, L.; Mushotzky, R. F.; Koss, M.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fioretti, V (reprint author), INAF Ist Astrofis Spaziale & Fis Cosm, Via Gobetti 101, I-40129 Bologna, Italy.
EM fioretti@iasfbo.inaf.it
RI Koss, Michael/B-1585-2015; Fioretti, Valentina/N-5589-2015; XRAY,
SUZAKU/A-1808-2009;
OI Koss, Michael/0000-0002-7998-9581; Fioretti,
Valentina/0000-0002-6082-5384; Malaguti, Giuseppe/0000-0001-9872-3378
FU Thales Alenia Space Italy Ph.D. fellowship; University Space Research
Association (USRA); Center for Research and Exploration in Space Science
and Technology (CRESST) [NNG06EO90A]; NASA/GSFC
FX We thank the anonymous referee for useful suggestions to improve the
paper. This work was supported by the Thales Alenia Space Italy Ph.D.
fellowship and the University Space Research Association (USRA), and it
was hosted by the Center for Research and Exploration in Space Science
and Technology (CRESST, Contract NNG06EO90A) and the NASA/GSFC. V.F.
gratefully acknowledges G.G.C. Palumbo for his constant scientific
support and P. Grandi for her extensive paper reading.
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2013
VL 555
AR A44
DI 10.1051/0004-6361/201219460
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 185YV
UT WOS:000322008600044
ER
PT J
AU Kuhnel, M
Muller, S
Kreykenbohm, I
Furst, F
Pottschmidt, K
Rothschild, RE
Caballero, I
Grinberg, V
Schonherr, G
Shrader, C
Klochkov, D
Staubert, R
Ferrigno, C
Torrejon, JM
Martinez-Nunez, S
Wilms, J
AF Kuehnel, M.
Mueller, S.
Kreykenbohm, I.
Fuerst, F.
Pottschmidt, K.
Rothschild, R. E.
Caballero, I.
Grinberg, V.
Schoenherr, G.
Shrader, C.
Klochkov, D.
Staubert, R.
Ferrigno, C.
Torrejon, J. -M.
Martinez-Nunez, S.
Wilms, J.
TI GRO J1008-57: an (almost) predictable transient X-ray binary
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: binaries; pulsars: individual: GRO J1008-57; accretion,
accretion disks; ephemerides
ID CYGNUS X-1; TIMING-EXPLORER; NEUTRON-STAR; PULSARS; OUTBURSTS;
ACCRETION; EMISSION; ORBIT; COMPTONIZATION; SPECTROSCOPY
AB A study of archival RXTE, Swift, and Suzaku pointed observations of the transient high-mass X-ray binary GRO J1008-57 is presented. A new orbital ephemeris based on pulse arrival-timing shows the times of maximum luminosities during outbursts of GRO J1008-57 to be close to periastron at orbital phase -0.03. This makes the source one of a few for which outburst dates can be predicted with very high precision. Spectra of the source in 2005, 2007, and 2011 can be well described by a simple power law with high-energy cutoff and an additional black body at lower energies. The photon index of the power law and the black-body flux only depend on the 15-50 keV source flux. No apparent hysteresis effects are seen. These correlations allow us to predict the evolution of the pulsar's X-ray spectral shape over all outbursts as a function of just one parameter, the source's flux. If modified by an additional soft component, this prediction even holds during GRO J1008-57's 2012 type II outburst.
C1 [Kuehnel, M.; Mueller, S.; Kreykenbohm, I.; Grinberg, V.; Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
[Kuehnel, M.; Mueller, S.; Kreykenbohm, I.; Grinberg, V.; Wilms, J.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
[Fuerst, F.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Pottschmidt, K.] UMBC, Ctr Space Sci & Technol, CRESST, Baltimore, MD 21250 USA.
[Pottschmidt, K.; Shrader, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rothschild, R. E.] Univ Calif San Diego, Ctr Astron & Space Sci, La Jolla, CA 92093 USA.
[Caballero, I.] Univ Paris 07, CNRS, CEA, CEA Saclay,DSM IRFU SAp UMR AIM 7158, F-91191 Gif Sur Yvette, France.
[Schoenherr, G.] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany.
[Shrader, C.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Klochkov, D.; Staubert, R.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Ferrigno, C.] ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland.
[Torrejon, J. -M.; Martinez-Nunez, S.] Univ Alicante, Inst Fis Aplicada Ciencias & Tecnol, E-03080 Alicante, Spain.
RP Kuhnel, M (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany.
EM matthias.kuehnel@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013; Torrejon, Jose /K-6395-2014; XRAY,
SUZAKU/A-1808-2009
OI Wilms, Joern/0000-0003-2065-5410; Torrejon, Jose /0000-0002-5967-5163;
FU Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum
fur Luft- und Raumfahrt [50OR0808, 50OR0905, 50OR1113]; Deutscher
Akademischer Austauschdienst; Spanish Ministerio de Ciencia e Innovacion
[AYA2010-15431, AIB2010DE-00054]
FX We thank the RXTE-, Swift- and Suzaku-teams for their role in scheduling
all observations used within this paper and for accepting our proposals.
We especially thank Evan Smith for his help in scheduling the RXTE
observations in 2011 April. Many thanks to Hans Krimm for providing the
BAT-spectrum during the 2012 giant outburst. We acknowledge funding by
the Bundesministerium fur Wirtschaft und Technologie under Deutsches
Zentrum fur Luft- und Raumfahrt grants 50OR0808, 50OR0905, 50OR1113, and
the Deutscher Akademischer Austauschdienst. This work has been partially
supported by the Spanish Ministerio de Ciencia e Innovacion through
projects AYA2010-15431 and AIB2010DE-00054. All figures shown in this
paper were produced using the SLXfig module, developed by John E. Davis.
We thank the referee for her/his helpful comments and suggestions.
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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 JUL
PY 2013
VL 555
AR A95
DI 10.1051/0004-6361/201321203
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 185YV
UT WOS:000322008600095
ER
PT J
AU Lebreton, J
van Lieshout, R
Augereau, JC
Absil, O
Mennesson, B
Kama, M
Dominik, C
Bonsor, A
Vandeportal, J
Beust, H
Defrere, D
Ertel, S
Faramaz, V
Hinz, P
Kral, Q
Lagrange, AM
Liu, W
Thebault, P
AF Lebreton, J.
van Lieshout, R.
Augereau, J. -C.
Absil, O.
Mennesson, B.
Kama, M.
Dominik, C.
Bonsor, A.
Vandeportal, J.
Beust, H.
Defrere, D.
Ertel, S.
Faramaz, V.
Hinz, P.
Kral, Q.
Lagrange, A. -M.
Liu, W.
Thebault, P.
TI An interferometric study of the Fomalhaut inner debris disk III.
Detailed models of the exozodiacal disk and its origin
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: interferometric; zodiacal dust; infrared: planetary systems;
stars: individual: Fomalhaut; radiative transfer; circumstellar matter
ID DUST RING FORMATION; KUIPER-BELT; CIRCUMSTELLAR MATERIAL;
RADIATIVE-TRANSFER; PLANETARY SYSTEM; SPACE-TELESCOPE; HOT DUST; STARS;
GRAINS; SUBLIMATION
AB Context. Debris disks are thought to be extrasolar analogs to the solar system planetesimal belts. The star Fomalhaut harbors a cold debris belt at 140 AU comparable to the Edgeworth-Kuiper belt, as well as evidence of a warm dust component, unresolved by single-dish telescopes, which is suspected of being a bright analog to the solar system's zodiacal dust.
Aims. Interferometric observations obtained with the VLTI/VINCI instrument and the Keck Interferometer Nuller have identified near- and mid-infrared excesses attributed respectively to hot and warm exozodiacal dust residing in the inner few AU of the Fomalhaut environment. We aim to characterize the properties of this double inner dust belt and to unveil its origin.
Methods. We performed parametric modeling of the exozodiacal disk ("exozodi") using the GRaTeR radiative transfer code to reproduce the interferometric data, complemented by mid-to far-infrared photometric measurements from Spitzer and Herschel(star star). A detailed treatment of sublimation temperatures was introduced to explore the hot population at the size-dependent sublimation rim. We then used an analytical approach to successively testing several source mechanisms for the dust and suspected parent bodies.
Results. A good fit to the multiwavelength data is found by two distinct dust populations: (1) a population of very small (0.01 to 0.5 mu m), hence unbound, hot dust grains confined in a narrow region (similar to 0.1-0.3 AU) at the sublimation rim of carbonaceous material; (2) a population of bound grains at similar to 2 AU that is protected from sublimation and has a higher mass despite its fainter flux level. We propose that the hot dust is produced by the release of small carbon grains following the disruption of dust aggregates that originate in the warm component. A mechanism, such as gas braking, is required to further confine the small grains for a long enough time. In situ dust production could hardly be ensured for the age of the star, so we conclude that the observed amount of dust is triggered by intense dynamical activity.
Conclusions. Fomalhaut may be representative of exozodis that are currently being surveyed at near and mid-infrared wavelengths worldwide. We propose a framework for reconciling the "hot exozodi phenomenon" with theoretical constraints: the hot component of Fomalhaut is likely the "tip of the iceberg" since it could originate in the more massive, but fainter, warm dust component residing near the ice line. This inner disk exhibits interesting morphology and can be considered a prime target for future exoplanet research.
C1 [Lebreton, J.; Augereau, J. -C.; Bonsor, A.; Vandeportal, J.; Beust, H.; Ertel, S.; Faramaz, V.; Lagrange, A. -M.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France.
[van Lieshout, R.; Kama, M.; Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Absil, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium.
[Mennesson, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Vandeportal, J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Vandeportal, J.] Univ Montreal, Observ Mt Megantic, Montreal, PQ H3C 3J7, Canada.
[Defrere, D.; Hinz, P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Kral, Q.; Thebault, P.] Observ Paris, Sect Meudon, F-92195 Meudon, France.
[Liu, W.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Lebreton, J (reprint author), UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France.
EM jeremy.lebreton@obs.ujf-grenoble.fr
OI Kama, Mihkel/0000-0003-0065-7267
FU European Community [226604]; French National Research Agency (ANR)
[ANR-2010 BLAN-0505-01]; Programme National de Planetologie (PNP); CNES
FX We would like to acknowledge Paul Kalas, James Graham, Kate Su and
Alexis Brandeker, for contributing to interesting discussions on various
aspects of this study, as well as the anonymous referee for the valuable
advices he provided. The research leading to these results has received
funding from the European Community's Seventh Framework Programme under
Grant Agreement 226604. We also thank the French National Research
Agency (ANR) for financial support through contract ANR-2010
BLAN-0505-01 (EXOZODI), the Programme National de Planetologie (PNP) and
the CNES for supporting part of this research.
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SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2013
VL 555
AR A146
DI 10.1051/0004-6361/201321415
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 185YV
UT WOS:000322008600146
ER
PT J
AU Nesci, R
Tosti, G
Pursimo, T
Ojha, R
Kadler, M
AF Nesci, R.
Tosti, G.
Pursimo, T.
Ojha, R.
Kadler, M.
TI Near-infrared and gamma-ray monitoring of TANAMI gamma-ray bright
sources
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE BL Lacertae objects: general; radiation mechanisms: non-thermal; gamma
rays: galaxies
ID LARGE-AREA TELESCOPE; BL-LACERTAE OBJECTS; RELATIVISTIC JETS; DETECTED
BLAZARS; X-RAY; CATALOG; VARIABILITY; GALAXIES; EMISSION
AB Context. Spectral energy distribution and its variability are basic tools for understanding the physical processes operating in active galactic nuclei (AGN).
Aims. In this paper we report the results of a one-year near-infrared (NIR) and optical monitoring of a sample of 22 AGN known to be gamma-ray emitters, aimed at discovering correlations between optical and gamma-ray emission.
Methods. We observed our objects with the Rapid Eye Mount (REM) telescope in J, H, K, and R bands nearly twice every month during their visibility window and derived light curves and spectral indexes. We also analyzed the gamma-ray data from the Fermi gamma-ray Space Telescope, making weekly averages.
Results. Six sources were never detected during our monitoring, proving to be fainter than their historical Two micron all sky survey (2MASS) level. All of the sixteen detected sources showed marked flux density variability, while the spectral indexes remained unchanged within our sensitivity limits. Steeper sources showed, on average, a larger variability. From the NIR light curves we also computed a variability speed index for each detected source. Only one source (PKS 0208-512) underwent an NIR flare during our monitoring. Half of the sources showed a regular flux density trend on a one-year time scale, but do not show any other peculiar characteristic. The broadband spectral index alpha(ro) appears to be a good proxy of the NIR spectral index only for BL Lac objects. No clear correlation between NIR and gamma-ray data is evident in our data, save for PKS 0537-441, PKS 0521-360, PKS 2155-304, and PKS 1424-418. The gamma-ray/NIR flux ratio showed a large spread, QSO being generally gamma-louder than BL Lac, with a marked correlation with the estimated peak frequency (nu(peak)) of the synchrotron emission.
C1 [Nesci, R.] INAF IAPS, I-00133 Rome, Italy.
[Nesci, R.] Univ Roma La Sapienza, I-00133 Rome, Italy.
[Tosti, G.] Univ Perugia, I-06023 Perugia, Italy.
[Pursimo, T.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Santa Cruz De T, Spain.
[Ojha, R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Ojha, R.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, Lehrstuhl Astron, D-97074 Wurzburg, Germany.
[Kadler, M.] Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany.
RP Nesci, R (reprint author), INAF IAPS, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
EM roberto.nesci@uniroma1.it
OI Kadler, Matthias/0000-0001-5606-6154
FU NASA [NNH09ZDA001N, 31263, NNH10ZDA001N, 41213]; University of
Massachusetts; Infrared Processing and Analysis Center/California
Institute of Technology
FX This research was funded in part by NASA through Fermi Guest
Investigator grant NNH09ZDA001N (proposal number 31263) and grant
NNH10ZDA001N (proposal number 41213). This research was supported by an
appointment to the NASA Postdoctoral Program at the Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. This research has made use of the SIMBAD database,
operated at CDS, Strasbourg, France, and also of the Two Micron All-Sky
Survey database, which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology. This research has made use of NASA's
Astrophysics Data System Bibliographic Services. 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.
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2013
VL 555
AR A2
DI 10.1051/0004-6361/201321094
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 185YV
UT WOS:000322008600002
ER
PT J
AU O'Flannagain, AM
Gallagher, PT
Brown, JC
Milligan, RO
Holman, GD
AF O'Flannagain, A. M.
Gallagher, P. T.
Brown, J. C.
Milligan, R. O.
Holman, G. D.
TI Solar flare X-ray source motion as a response to electron spectral
hardening
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: particle emission; Sun: flares; Sun: X-rays, gamma rays
ID LOW-ENERGY CUTOFFS; CHROMOSPHERIC EVAPORATION; PARTICLE-ACCELERATION;
NUMERICAL SIMULATIONS; NONTHERMAL ELECTRONS; DENSITY-MEASUREMENTS;
IMPULSIVE PHASE; RHESSI; EMISSION; TARGET
AB Context. Solar flare hard X-rays (HXRs) are thought to be produced by nonthermal coronal electrons stopping in the chromosphere or remaining trapped in the corona. The collisional thick target model (CTTM) predicts that more energetic electrons penetrate to greater column depths along the flare loop. This requires that sources produced by harder power-law injection spectra should appear further down the legs or footpoints of a flareloop. Therefore, the frequently observed hardening of the injected power-law electron spectrum during flare onset should be concurrent with a descending hard X-ray source.
Aims. We test this implication of the CTTM by comparing its predicted HXR source locations with those derived from observations of a solar flare which exhibits a nonthermally-dominated spectrum before the peak in HXRs, known as an early impulsive event.
Methods. The HXR images and spectra of an early impulsive C-class flare were obtained using the Ramaty High-Energy Solar Spectroscopic Imager (RHESSI). Images were reconstructed to produce HXR source height evolutions for three energy bands. Spatially integrated spectral analysis was performed to isolate nonthermal emission and to determine the power-law index of the electron injection spectrum. The observed height-time evolutions were then fitted with CTTM-based simulated heights for each energy, using the electron spectral indices derived from the RHESSI spectra.
Results. The flare emission was found to be dominantly nonthermal above similar to 7 keV, with emission of thermal and nonthermal X-rays likely to be simultaneously observable below that energy. The density structure required for a good match between model and observed source heights agreed with previous studies of flare loop densities.
Conclusions. The CTTM has been used to produce a descent of model HXR source heights that compares well with observations of this event. Based on this interpretation, downward motion of nonthermal sources should occur in any flare where there is spectral hardening in the electron distribution during a flare. However, this is often masked by thermal emission associated with flare plasma preheating. To date, flare models that predict transfer of energy from the corona to the chromosphere by means other than a flux of nonthermal electrons do not predict this observed source descent. Therefore, flares such as this will be key in explaining this elusive energy transfer process.
C1 [O'Flannagain, A. M.; Gallagher, P. T.] Univ Dublin Trinity Coll, Sch Phys, Astrophys Res Grp, Dublin 2, Ireland.
[Brown, J. C.] Univ Glasgow, Sch Phys & Astron, Astron & Astrophys Grp, Glasgow G12 8QQ, Lanark, Scotland.
[Milligan, R. O.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Holman, G. D.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP O'Flannagain, AM (reprint author), Univ Dublin Trinity Coll, Sch Phys, Astrophys Res Grp, Dublin 2, Ireland.
EM oflannaa@tcd.ie
RI Gallagher, Peter/C-7717-2011
OI Gallagher, Peter/0000-0001-9745-0400
FU Government of Ireland Studentship (AMO'F) from the Irish Research
Council for Science, Engineering and Technology (IRCSET); Visiting
Fellowship by TCD; NASA Heliophysics Guest Investigator Program; RHESSI
project
FX The author would like to thank Brian Dennis and the RHESSI team for
their hospitality and input during this research. This work has been
supported by a Government of Ireland Studentship (AMO'F) from the Irish
Research Council for Science, Engineering and Technology (IRCSET) and a
Visiting Fellowship by TCD (JCB). G.D.H. acknowledges support from the
NASA Heliophysics Guest Investigator Program and the RHESSI project. The
authors also thank the anonymous referee for comments which greatly
improved the accuracy and clarity of the paper.
NR 52
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2013
VL 555
AR A21
DI 10.1051/0004-6361/201220368
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 185YV
UT WOS:000322008600021
ER
PT J
AU Rezac, L
Kutepov, AA
Faure, A
Hartogh, P
Feofilov, AG
AF Rezac, L.
Kutepov, A. A.
Faure, A.
Hartogh, P.
Feofilov, A. G.
TI Rotational non-LTE in HCN in the thermosphere of Titan: Implications for
the radiative cooling
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE radiation mechanisms: non-thermal; line: formation; planets and
satellites: atmospheres
ID ACCELERATED LAMBDA ITERATION; HYPERFINE EXCITATION; PHOTOCHEMICAL MODEL;
UPPER-ATMOSPHERE; TEMPERATURE; ESCAPE; LINES; GAS; HNC; CN
AB Context. The thermal structure of Titan's thermosphere is determined by the balance between several heating and cooling processes. These processes must be accurately modeled to correctly interpret the available measurements and enhance our understanding of the formation and evolution of this atmosphere. One of the most important thermospheric cooling process for Titan is emission in the HCN rotational band.
Aims. We aim to determine the validity of local thermodynamic equilibrium (LTE) for the HCN rotational distribution in the thermosphere of Titan and the impact of its breakdown on the HCN radiative cooling rate in the thermosphere.
Methods. A general non-LTE radiative transfer code for rotational lines based on the accelerated lambda iteration (ALI) was used to calculate the excitation of HCN rotational levels in Titan's atmosphere. These level populations were then used to calculate the associated cooling rate.
Results. We show that the common assumption in the models of Titan's thermospheric energy balance, namely the LTE distribution of rotational lines of HCN, is generally not valid above about 1100 km, or similar to 0.025 nbar, which will affect the derived thermospheric cooling rates. The effect of non-LTE is to reduce the cooling rate to 15% of the LTE value at around the exobase altitudes depending on the given density of HCN and collisional partners (N-2, CH4, H-2, and electrons). Since collision state-to-state quenching rates of HCN rotational levels are poorly known, a sensitivity analysis of our results to these rates is also presented.
C1 [Rezac, L.; Hartogh, P.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Kutepov, A. A.] Catholic Univ Amer, Washington, DC 20064 USA.
[Kutepov, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Faure, A.] Univ Grenoble 1, CNRS, UMR 5571, Astrophys Lab, F-38041 Grenoble 9, France.
[Feofilov, A. G.] Ecole Polytech, CNRS, Meteorol Dynam Lab, F-91128 Palaiseau, France.
RP Rezac, L (reprint author), Max Planck Inst Solar Syst Res, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
EM rezac@mps.mpg.de
RI Feofilov, Artem/A-2271-2015
OI Feofilov, Artem/0000-0001-9924-4846
FU German Deutsche Forschungsgemeinschaft, DFG [HA 3261/7-1]
FX This work was supported by the German Deutsche Forschungsgemeinschaft,
DFG project number HA 3261/7-1.
NR 34
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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 JUL
PY 2013
VL 555
AR A122
DI 10.1051/0004-6361/201321231
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 185YV
UT WOS:000322008600122
ER
PT J
AU Riviere-Marichalar, P
Pinte, C
Barrado, D
Thi, WF
Eiroa, C
Kamp, I
Montesinos, B
Donaldson, J
Augereau, JC
Huelamo, N
Roberge, A
Ardila, D
Sandell, G
Williams, JP
Dent, WRF
Menard, F
Lillo-Box, J
Duchene, G
AF Riviere-Marichalar, P.
Pinte, C.
Barrado, D.
Thi, W. F.
Eiroa, C.
Kamp, I.
Montesinos, B.
Donaldson, J.
Augereau, J. C.
Huelamo, N.
Roberge, A.
Ardila, D.
Sandell, G.
Williams, J. P.
Dent, W. R. F.
Menard, F.
Lillo-Box, J.
Duchene, G.
TI Gas and dust in the TW Hydrae association as seen by the Herschel Space
Observatory
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; astrochemistry; protoplanetary disks; circumstellar
matter; zodiacal dust; planetary systems
ID LOW-MASS STARS; 4796A CIRCUMSTELLAR DISK; TAURI STARS; DEBRIS DISKS;
YOUNG STARS; PROTOPLANETARY DISKS; HYA ASSOCIATION; HR 4796A; HD 98800;
CIRCUMBINARY DISK
AB Context. Circumstellar discs are the places where planets form, therefore knowledge of their evolution is crucial for our understanding of planet formation. The Herschel Space Observatory is providing valuable data for studying disc systems, thanks to its sensitivity and wavelength coverage. This paper is one of several devoted to analysing and modelling Herschel-PACS observations of various young stellar associations from the GASPS open time key programme.
Aims. The aim of this paper is to elucidate the gas and dust properties of circumstellar discs in the similar to 10 Myr TW Hya association (TWA) using new far-infrared (IR) imaging and spectroscopy from Herschel-PACS.
Methods. We obtained far-IR photometric data at 70, 100, and 160 mu m of 14 TWA members; spectroscopic observations centred on the [OI] line at 63.18 mu m were also obtained for 9 of the 14. The new photometry for each star was incorporated into its full spectral energy distribution.
Results. We detected excess IR emission that is characteristic of circumstellar discs from five TWA members, and computed upper limits for another nine. Two TWA members (TWA 01 and TWA 04B) also show [OI] emission at 63.18 mu m. Discs in the TWA association display a variety of properties, with a wide range of dust masses and inner radii, based on modified blackbody modelling. Both transitional and debris discs are found in the sample. Models for sources with a detected IR excess give dust masses in the range from similar to 0.15 M-circle plus to similar to 63 M-circle plus.
C1 [Riviere-Marichalar, P.; Barrado, D.; Montesinos, B.; Huelamo, N.; Lillo-Box, J.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Villanueva De La Canada 28691, Spain.
[Pinte, C.; Thi, W. F.; Augereau, J. C.; Menard, F.; Duchene, G.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys IPAG, UMR 5274, F-38041 Grenoble, France.
[Menard, F.] Univ Chile, CNRS, Lab Franco Chileno Astron, PUC U Concept,UMI 3386, Santiago, Chile.
[Barrado, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain.
[Riviere-Marichalar, P.; Eiroa, C.] UAM, Fac Ciencia, Dept Fis Teor, Madrid 28049, Spain.
[Kamp, I.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Donaldson, J.] Univ Maryland, Dept Astron, College Pk, MD USA.
[Roberge, A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Ardila, D.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Washington, DC USA.
[Williams, J. P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Dent, W. R. F.] ALMA, Santiago, Chile.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Riviere-Marichalar, P (reprint author), CSIC INTA, Ctr Astrobiol, Dept Astrofis, ESAC Campus,POB 78, Villanueva De La Canada 28691, Spain.
EM riviere@cab.inta-csic.es; barrado@cab.inta-csic.es
RI Roberge, Aki/D-2782-2012; Lillo-Box, Jorge/I-2841-2015; Barrado
Navascues, David/C-1439-2017; Huelamo, Nuria/C-3042-2017; Montesinos,
Benjamin/C-3493-2017;
OI Roberge, Aki/0000-0002-2989-3725; Lillo-Box, Jorge/0000-0003-3742-1987;
Barrado Navascues, David/0000-0002-5971-9242; Huelamo,
Nuria/0000-0002-2711-8143; Montesinos, Benjamin/0000-0002-7982-2095;
Williams, Jonathan/0000-0001-5058-695X
FU ANR [ANR-07-BLAN-0221]; PNPS of CNRS/INSU, France; European Commission
[PERG06-GA-2009-256513]; Agence Nationale pour la Recherche (ANR) of
France [ANR-2010-JCJC-0504-01]; EU (DIANA project) [284405]; PNP-CNES;
Millennium Science Initiative (Chilean Ministry of Economy) [Nucleus
P10-022-F]; [AYA 2010-21161-C02-02]; [AYA2012-38897-C02-01];
[AYA2011-26202 CDS2006-00070]; [PRICIT-S2009/ESP-1496]
FX This research has been funded by Spanish grants AYA 2010-21161-C02-02,
AYA2012-38897-C02-01, AYA2011-26202 CDS2006-00070, and
PRICIT-S2009/ESP-1496. We also acknowledge support from ANR (contract
ANR-07-BLAN-0221) and PNPS of CNRS/INSU, France. C. Pinte acknowledges
funding from the European Commission's 7th Framework programme (contract
PERG06-GA-2009-256513) and from Agence Nationale pour la Recherche (ANR)
of France under contract ANR-2010-JCJC-0504-01. W.F.T. thanks the CNES
for a post-doctoral position. W.F.T., F.M. and I.K. acknowledge funding
from the EU FP7-2011 under Grant Agreement nr. 284405 (DIANA project).
J.C.A. acknowledges the PNP-CNES for financial support. F.M. acknowledge
support from the Millennium Science Initiative (Chilean Ministry of
Economy), through grant "Nucleus P10-022-F".
NR 85
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U1 0
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2013
VL 555
AR A67
DI 10.1051/0004-6361/201321506
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 185YV
UT WOS:000322008600067
ER
PT J
AU Tran, TT
Li, HX
Ru, GY
Kerczewski, RJ
Liu, LJ
Khan, SU
AF Tran, Tuan T.
Li, Hongxiang
Ru, Guanying
Kerczewski, Robert J.
Liu, Lingjia
Khan, Samee U.
TI Secure Wireless Multicast for Delay-Sensitive Data via Network Coding
SO IEEE TRANSACTIONS ON WIRELESS COMMUNICATIONS
LA English
DT Article
DE Wireless multicast; network coding; Markov decision process; security;
denied-of-service attack
AB Wireless multicast for delay-sensitive data is challenging because of the heterogeneity effect where each receiver may experience different packet losses. Fortunately, network coding, a new advanced routing protocol, offers significant advantages over the traditional Automatic Repeat reQuest (ARQ) protocols in that it mitigates the need for retransmission and has the potential to approach the min-cut capacity. Network-coded multicast would be, however, vulnerable to false packet injection attacks, in which the adversary injects bogus packets to prevent receivers from correctly decoding the original data. Without a right defense in place, even a single bogus packet can completely change the decoding outcome. Existing solutions either incur high computation cost or cannot withstand high packet loss. In this paper, we propose a novel scheme to defend against false packet injection attacks on network-coded multicast for delay-sensitive data. Specifically, we propose an efficient authentication mechanism based on null space properties of coded packets, aiming to enable receivers to detect any bogus packets with high probability. We further design an adaptive scheduling algorithm based on the Markov Decision Processes (MDP) to maximize the number of authenticated packets received within a given time constraint. Both analytical and simulation results have been provided to demonstrate the efficacy and efficiency of our proposed scheme.
C1 [Tran, Tuan T.; Li, Hongxiang; Ru, Guanying] Univ Louisville, JB Speed Sch Engn, Dept Elect & Comp Engn, Louisville, KY 40292 USA.
[Kerczewski, Robert J.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Liu, Lingjia] Univ Kansas, Dept Elect Engn & Comp Sci, Lawrence, KS 66045 USA.
[Khan, Samee U.] N Dakota State Univ, Dept Elect & Comp Engn, Fargo, ND 58102 USA.
RP Tran, TT (reprint author), InfoBeyond Technol LLC, Louisville, KY 40223 USA.
EM ttran10@asu.edu; h.li@louisville.edu; g0ru0001@louisville.edu;
RKerczewski@nasa.gov; lingjialiu@ittc.ku.edu; Samee.Khan@ndsu.edu
FU US National Science Foundation [1156395, 1228071]; Kentucky NASA EPSCoR
Research Infrastructure Development Grant
FX This work was supported by US National Science Foundation (1156395 &
1228071) and Kentucky NASA EPSCoR 2012 Research Infrastructure
Development Grant. This paper was presented in part at the IEEE
International Conference on Communications (ICC), June, 2012.
NR 42
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U1 1
U2 16
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1536-1276
EI 1558-2248
J9 IEEE T WIREL COMMUN
JI IEEE Trans. Wirel. Commun.
PD JUL
PY 2013
VL 12
IS 7
BP 3372
EP 3387
DI 10.1109/TWC.2013.062413.121557
PG 16
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 194VQ
UT WOS:000322661200023
ER
PT J
AU Mulani, SB
Bird, RK
Kapania, RK
Bird, RK
Kapania, RK
Robert, O
AF Mulani, Sameer B.
Bird, R. Keith
Kapania, Rakesh K.
Bird, R. Keith
Kapania, Rakesh K.
Robert, Olliffe
TI Design, Optimization, and Evaluation of Al-2139 Compression Panel with
Integral T-Stiffeners
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB A T-stiffened panel was designed and optimized for minimum mass subjected to constraints on buckling load, yielding, and crippling or local stiffener failure using a new analysis and design tool named EBF3PanelOpt. The panel was designed for a compression loading configuration, a realistic load case for a typical aircraft skin-stiffened panel. The panel was integrally machined from a 2139 aluminum alloy plate and was tested in compression. The panel was loaded beyond buckling and strains, and out-of-plane displacements were extracted from 36 strain gages and one linear variable displacement transducer. A digital photogrammetric system was used to obtain full-field displacements and strains on the smooth (unstiffened) side of the panel. The experimental data were compared with the strains and out-of-plane deflections from a high-fidelity nonlinear finite element analysis. The test data indicated that the panel buckled at the linear elastic buckling eigenvalue predicted for the panel. The out-of-plane displacement measured by the digital photogrammetric system compared well both qualitatively and quantitatively with the nonlinear finite element solution in the postbuckling regime. Furthermore, the experimental strains compared well with both the linear and nonlinear finite element models before buckling. The weight of the optimized panel was 20% less than that of a T-stiffened panel optimized using conventional design techniques.
C1 [Mulani, Sameer B.] Virginia Polytech Inst & State Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24061 USA.
[Bird, R. Keith] Lockheed Martin Aeronaut Co, ADP Technol Dev & Integrat, Marietta, GA 30063 USA.
[Bird, R. Keith] NASA Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23666 USA.
[Kapania, Rakesh K.] Virginia Polytech Inst & State Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24061 USA.
[Robert, Olliffe] Lockheed Martin Aeronaut Co, ADP Technol Dev & Integrat, Marietta, GA 30063 USA.
RP Mulani, SB (reprint author), Virginia Polytech Inst & State Univ, Dept Aerosp & Ocean Engn, 215 Randolph Hall 0203, Blacksburg, VA 24061 USA.
FU NASA Subsonic Fixed Wing Hybrid Body Technologies NRA [NASA NNL08AA02C]
FX The work presented here was funded under NASA Subsonic Fixed Wing Hybrid
Body Technologies NRA (NASA NNL08AA02C) with Karen M. Brown Taminger as
the NASA Technical Lead. The authors are thankful to K. M. Brown
Taminger for her suggestions. The authors would like to thank our
partners in the NRA project, John Barnes and Steve Englestad of Lockheed
Martin Aeronautics Company of Marietta, GA, for technical discussions.
NR 22
TC 1
Z9 2
U1 1
U2 10
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD JUL-AUG
PY 2013
VL 50
IS 4
BP 1275
EP 1286
DI 10.2514/1.C032199
PG 12
WC Engineering, Aerospace
SC Engineering
GA 196VR
UT WOS:000322806000026
ER
PT J
AU Gregorio, A
Cuttaia, F
Mennella, A
Bersanelli, M
Maris, M
Meinhold, P
Sandri, M
Terenzi, L
Tomasi, M
Villa, F
Frailis, M
Morgante, G
Pearson, D
Zacchei, A
Battaglia, P
Butler, RC
Davis, R
Franceschet, C
Franceschi, E
Galeotta, S
Leonardi, R
Lowe, S
Mandolesi, N
Melot, F
Mendes, L
Stassi, P
Stringhetti, L
Tavagnacco, D
Zonca, A
Wilkinson, A
Wilson, P
Charra, M
Maciaszek, T
Foley, S
Watson, CJ
Casale, M
Laureijs, R
Tauber, J
Texier, D
Baker, M
Cuevas, LP
Krassenburg, M
Rihet, P
AF Gregorio, A.
Cuttaia, F.
Mennella, A.
Bersanelli, M.
Maris, M.
Meinhold, P.
Sandri, M.
Terenzi, L.
Tomasi, M.
Villa, F.
Frailis, M.
Morgante, G.
Pearson, D.
Zacchei, A.
Battaglia, P.
Butler, R. C.
Davis, R.
Franceschet, C.
Franceschi, E.
Galeotta, S.
Leonardi, R.
Lowe, S.
Mandolesi, N.
Melot, F.
Mendes, L.
Stassi, P.
Stringhetti, L.
Tavagnacco, D.
Zonca, A.
Wilkinson, A.
Wilson, P.
Charra, M.
Maciaszek, T.
Foley, S.
Watson, C. J.
Casale, M.
Laureijs, R.
Tauber, J.
Texier, D.
Baker, M.
Cuevas, L. Perez
Krassenburg, M.
Rihet, P.
TI In-flight calibration and verification of the Planck-LFI instrument
SO JOURNAL OF INSTRUMENTATION
LA English
DT Article
DE Instrument optimisation; Space instrumentation; Microwave radiometers;
Instruments for CMB observations
ID PRE-LAUNCH STATUS; RADIOMETERS
AB In this paper we discuss the Planck-LFI in-flight calibration campaign. After a brief overview of the ground test campaigns, we describe in detail the calibration and performance verification (CPV) phase, carried out in space during and just after the cool-down of LFI. We discuss in detail the functionality verification, the tuning of the front-end and warm electronics, the preliminary performance assessment and the thermal susceptibility tests. The logic, sequence, goals and results of the in-flight tests are discussed. All the calibration activities were successfully carried out and the instrument response was comparable to the one observed on ground. For some channels the in-flight tuning activity allowed us to improve significantly the noise performance.
C1 [Gregorio, A.; Tavagnacco, D.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Gregorio, A.; Tavagnacco, D.] INAF OATS Trieste, I-34143 Trieste, Italy.
[Cuttaia, F.; Terenzi, L.; Morgante, G.; Butler, R. C.; Franceschi, E.; Mandolesi, N.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Mennella, A.; Bersanelli, M.; Tomasi, M.; Villa, F.; Battaglia, P.; Franceschet, C.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy.
[Meinhold, P.; Zonca, A.] UCSB, Dept Phys, Santa Barbara, CA USA.
[Pearson, D.; Wilson, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Davis, R.] JBO, Manchester, Lancs, England.
[Leonardi, R.; Mendes, L.; Casale, M.; Laureijs, R.; Tauber, J.; Texier, D.] European Space Astron Ctr, PSO, Madrid, Spain.
[Stassi, P.] INPG, UJF Grenoble 1, LPSC, CNRS IN2P3, Grenoble, France.
[Lowe, S.] LCOGT, Goleta, CA USA.
[Charra, M.] Univ Paris 11, IAS, Paris, France.
[Maciaszek, T.] CNES, Paris, France.
[Foley, S.; Watson, C. J.] European Space Technol Ctr, MOC, Darmstadt, Germany.
[Baker, M.; Cuevas, L. Perez; Krassenburg, M.] Estec, Noordwijk, Netherlands.
[Rihet, P.] Thales Alenia Space, F-06150 Cannes, France.
RP Gregorio, A (reprint author), Univ Trieste, Dipartimento Fis, Via Valerio 2, I-34127 Trieste, Italy.
EM Anna.Gregorio@ts.infn.it
RI Butler, Reginald/N-4647-2015; Tomasi, Maurizio/I-1234-2016;
OI Gregorio, Anna/0000-0003-4028-8785; Butler,
Reginald/0000-0003-4366-5996; Cuttaia, Francesco/0000-0001-6608-5017;
Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379;
Zacchei, Andrea/0000-0003-0396-1192; Tomasi,
Maurizio/0000-0002-1448-6131; Lowe, Stuart/0000-0002-2975-9032;
Galeotta, Samuele/0000-0002-3748-5115; Stringhetti,
Luca/0000-0002-3961-9068; Frailis, Marco/0000-0002-7400-2135; Maris,
Michele/0000-0001-9442-2754; Sandri, Maura/0000-0003-4806-5375;
Franceschi, Enrico/0000-0002-0585-6591; Morgante,
Gianluca/0000-0001-9234-7412
FU ESA; ASI-E2 phase of the Planck contract; NASA Science Mission
Directorate; Finnish Funding Agency for Technology and Innovation
(Tekes); ESA Mission Operation Centre; ESA Planck Science Office; ESA
Planck Project
FX Planck is a project of the European Space Agency with instruments funded
by ESA member states, and with special contributions from Denmark and
NASA (USA). The Planck LFI project is developed by an International
Consortium lead by Italy and involving Canada, Finland, Germany, Norway,
Spain, Switzerland, UK, USA. The Italian contribution to Planck is
supported by the Italian Space Agency (ASI). The work in this paper has
been supported by in the framework of the ASI-E2 phase of the Planck
contract. The US Planck Project is supported by the NASA Science Mission
Directorate. In Finland, the Planck LFI 70 GHz work was supported by the
Finnish Funding Agency for Technology and Innovation (Tekes).; During
the ground tests and the full in-flight operations, the LFI instrument
team is supported by the HFI team, in particular for what regards the
cryogenic chain operations, by the ESA Mission Operation Centre, by the
ESA Planck Science Office and by the ESA Planck Project.
NR 30
TC 0
Z9 0
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-0221
J9 J INSTRUM
JI J. Instrum.
PD JUL
PY 2013
VL 8
AR T07001
DI 10.1088/1748-0221/8/07/T07001
PG 100
WC Instruments & Instrumentation
SC Instruments & Instrumentation
GA 193PO
UT WOS:000322572900033
ER
PT J
AU Wang, TS
Lin, J
Guidos, M
AF Wang, Ten-See
Lin, Jeff
Guidos, Mike
TI Transient Side-Load Analysis of Out-of-Round Film-Cooled Nozzle
Extensions
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article; Proceedings Paper
CT 48th AIAA/ASME/SAE/ASEE Joint Propulsion Conference and Exhibit / 10th
International Energy Conversion Engineering Conference
CY JUL 29-AUG 03, 2012
CL Atlanta, GA
SP AIAA, ASME, SAE, ASEE
ID BASE-HEATING ENVIRONMENT; FLOW SEPARATION; ENGINE NOZZLE; PERFORMANCE;
SIMULATION; REGIME
AB Understanding the impact of out-of-round nozzle extension on the nozzle side load during engine transient startup operations has garnered special interest from design engineers of late. The out-of-round nozzle extension could be the result of asymmetric internal stresses, deformation induced by previous tests, and asymmetric loads induced by hardware attached to the nozzle. The objective of this study was to computationally investigate the effect of out-of-round nozzle extension on the nozzle side loads during an engine startup transient. The rocket engine studied encompasses a regeneratively cooled chamber and nozzle, along with a film-cooled nozzle extension. The computational methodology is based on an unstructured-grid pressure-based computational fluid dynamics formulation, and on transient inlet boundary flow properties derived from an engine system simulation. Six three-dimensional cases were performed, with the out of roundness achieved by three different degrees of ovalization, elongated on lateral y and z axes: one slightly ovalized, one more ovalized, and one significantly ovalized. The results show that the separation line jump was the primary peak side-load physics. Compared with the peak side load of the perfectly round nozzle, the peak side loads increased most for the slightly ovalized nozzle extensions. The peak side loads then reduced moderately from the slightly ovalized nozzle extensions to the more ovalized nozzle extensions. For the significantly ovalized nozzle extensions, the peak side loads dropped substantially from those of the slightly ovalized nozzle extensions, due to increased flow directionality.
C1 [Wang, Ten-See; Lin, Jeff] NASA, Marshall Space Flight Ctr, Fluid Dynam Branch, Struct Thermal & Fluids Anal Div, Huntsville, AL USA.
[Guidos, Mike] NASA, Marshall Space Flight Ctr, Liquid Engine & Main Prop Syst Branch, Prop Syst Design & Integrat Div, Huntsville, AL USA.
RP Wang, TS (reprint author), NASA, Marshall Space Flight Ctr, Fluid Dynam Branch, Struct Thermal & Fluids Anal Div, Huntsville, AL USA.
NR 36
TC 4
Z9 5
U1 1
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD JUL-AUG
PY 2013
VL 29
IS 4
BP 855
EP 866
DI 10.2514/1.B34812
PG 12
WC Engineering, Aerospace
SC Engineering
GA 186PR
UT WOS:000322057100011
ER
PT J
AU Thomas, RE
Burton, RL
Polzin, KA
AF Thomas, Robert E.
Burton, Rodney L.
Polzin, Kurt A.
TI Performance Characteristics of an Ablative Gallium Electromagnetic
Accelerator
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article; Proceedings Paper
CT 46th AIAA/ASME/SAE/ASEE Joint Propulsion Conference and Exhibit
CY JUL 25-29, 2010
CL Nashville, TN
SP AIAA, ASME, SAE, ASEE, Israel Minist Sci, Culture & Sport
ID MAGNETOPLASMADYNAMIC THRUSTER; PLASMA; PROBE
AB Experimental performance measurements are presented for an ablative gallium electromagnetic accelerator driven by a 50 its flat-top current pulse, with gallium supplied to the discharge by evaporation of the central cathode. The arc impedance, exhaust velocity, and electron temperature are measured for discharge currents in the range of ;6-24 kA and an electrode radius ratio of r(a)/r(c) = 3.4. The arc voltage is found to vary linearly with the discharge current, giving an arc impedance of 6-7 m Omega. An exhaust velocity of u(e) = 16 km/s is found by using the mass bit and computing the electromagnetic thrust from the discharge current data. This value is invariant with the discharge current and is within the experimental error of the velocities measured using electrostatic probes. Triple probe measurements yield on-axis electron temperatures in the range of 0.8-3.8 eV and electron densities in the range of 0.16-2.1 x 10(22) m(-3). Magnetic induction probe measurements in the interelectrode region yield a peak magnetic field of 0.8 Tat 24 kA and no evidence of the spoking instability. An efficiency of 25% at 1600 s is calculated for r(a)/r(c) = 3.4 using the mass bit and discharge current data assuming the cathode has a flat tip. The efficiency scaling predicts that changing to a conical tip cathode and increasing the radius ratio r(a)/r(c) to 10 will result in an efficiency of 52% at an I-sp of 3200s.
C1 [Thomas, Robert E.] Univ Illinois, Prop & Propellants Branch, NASA Glenn Res Center, Urbana, IL 61801 USA.
[Burton, Rodney L.] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.
[Polzin, Kurt A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Thomas, RE (reprint author), Univ Illinois, Prop & Propellants Branch, NASA Glenn Res Center, Urbana, IL 61801 USA.
NR 25
TC 1
Z9 1
U1 1
U2 4
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 JUL-AUG
PY 2013
VL 29
IS 4
BP 930
EP 937
DI 10.2514/1.B34256
PG 8
WC Engineering, Aerospace
SC Engineering
GA 186PR
UT WOS:000322057100018
ER
PT J
AU DeLaat, JC
Kopasakis, G
Saus, JR
Chang, CT
Wey, C
AF DeLaat, John C.
Kopasakis, George
Saus, Joseph R.
Chang, Clarence T.
Wey, Changlie
TI Active Combustion Control for a Low-Emissions Aircraft Engine Combustor
Prototype: Experimental Results
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article; Proceedings Paper
CT 50th AIAA Aerospace Sciences Meeting and Exhibit including the New
Horizons Forum and Aerospace Exposition
CY JAN 06-13, 2012
CL Nashville, TN
SP AIAA, US AF Off Sci Res
ID INSTABILITY
AB Lean combustion concepts for aircraft engines are more susceptible to combustion instabilities. Prior activity has demonstrated active control to suppress combustion instabilities with a conventional rich-front-end combustor. The current effort is developing further understanding of the problem specifically as applied to future lean-burning, very low-emissions aircraft engine combustors. A prototype low-emissions aircraft engine combustor with a combustion instability has been identified and previous work has characterized the combustor's dynamic behavior. The combustor exhibits thermoacoustic instabilities related to increasing fuel flow that prevent full-power operation. Active combustion instability suppression using the adaptive sliding phasor average control method has been demonstrated experimentally with this combustor prototype in a combustion test cell operating at engine pressures, temperatures, and flows. A high-frequency fuel valve perturbed the combustor fuel flow. Successful instability suppression was shown using a dynamic pressure sensor in the combustor for controller feedback. Instability control was also shown with a pressure feedback sensor in the lower temperature region, upstream of the combustor. It was also demonstrated that the controller can prevent the instability from occurring while combustor operation was transitioning from a stable low-power condition to a normally unstable high-power condition, thus enabling the high-power condition.
C1 [DeLaat, John C.; Kopasakis, George; Saus, Joseph R.; Chang, Clarence T.] NASA, H Glenn Res Ctr Lewis Field, Controls & Dynam Branch, Cleveland, OH 44135 USA.
[Wey, Changlie] Vantage Partners LLC, Brookpark, OH 44142 USA.
RP DeLaat, JC (reprint author), NASA, H Glenn Res Ctr Lewis Field, Controls & Dynam Branch, Brookpk Rd,MS77 1, Cleveland, OH 44135 USA.
NR 27
TC 0
Z9 0
U1 0
U2 6
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 JUL-AUG
PY 2013
VL 29
IS 4
BP 991
EP 1000
DI 10.2514/1.B34653
PG 10
WC Engineering, Aerospace
SC Engineering
GA 186PR
UT WOS:000322057100024
ER
PT J
AU Dec, JA
Braun, RD
AF Dec, John A.
Braun, Robert D.
TI Three-Dimensional Finite Element Ablative Thermal Response and Design of
Thermal Protection Systems
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 42nd AIAA Thermophysics Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA, NASA Ames Res Ctr (ARC), NASA Strateg Capabilities Assests Program
AB A finite element ablation and thermal response program for the simulation of three-dimensional transient thermostructural analysis has been developed. The three-dimensional governing differential equations and finite element formulation are summarized. A novel probabilistic design methodology for thermal protection systems has been developed. The design methodology is an eight step process beginning with a parameter sensitivity study and is followed by a deterministic analysis whereby an optimum design can determined. The design process concludes with a Monte Carlo simulation where the probabilities of exceeding design specifications are estimated. The design methodology is demonstrated by applying the methodology to the carbon phenolic compression pads of the Crew Exploration Vehicle. The maximum allowed values of bondline temperature and tensile stress are used as the design specifications in this study. Using the design methodology, the probability of exceeding these design specifications was shown to be low and within an acceptable range.
C1 [Dec, John A.] NASA, Langley Res Ctr, Struct & Thermal Syst Branch, Hampton, VA 23681 USA.
[Braun, Robert D.] Georgia Inst Technol, Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA.
RP Dec, JA (reprint author), NASA, Langley Res Ctr, Struct & Thermal Syst Branch, MS 431, Hampton, VA 23681 USA.
NR 13
TC 0
Z9 0
U1 1
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JUL-AUG
PY 2013
VL 50
IS 4
BP 725
EP 734
DI 10.2514/1.A32313
PG 10
WC Engineering, Aerospace
SC Engineering
GA 197KS
UT WOS:000322850700001
ER
PT J
AU Agrawal, P
Chavez-Garcia, JF
Pham, J
AF Agrawal, Parul
Chavez-Garcia, Jose F.
John Pham
TI Fracture in Phenolic Impregnated Carbon Ablator
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 42nd AIAA Thermophysics Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA, NASA Ames Res Ctr (ARC), NASA Strateg Capabilities Assests Program
AB This paper describes the development of a novel technique to understand the failure mechanisms inside thermal protection materials. The focus of this research is on the class of materials known as phenolic impregnated carbon ablators. It has successfully flown on the Stardust spacecraft and is the thermal protection system material chosen for the Mars Science Laboratory and SpaceX Dragon spacecraft. Although it has good thermal properties, structurally, it is a weak material. To understand failure mechanisms in carbon ablators, fracture tests were performed on FiberForm (R) (precursor), virgin, and charred ablator materials. Several samples of these materials were tested to investigate failure mechanisms at a microstructural scale. Stress-strain data were obtained simultaneously to estimate the tensile strength and toughness. It was observed that cracks initiated and grew in the FiberForm when a critical stress limit was reached such that the carbon fibers separated from the binder. However, both for virgin and charred carbon ablators, crack initiation and growth occurred in the matrix (phenolic) phase. Both virgin and charred carbon ablators showed greater strength values compared with FiberForm samples, confirming that the presence of the porous matrix helps in absorbing the fracture energy.
C1 [Agrawal, Parul; Chavez-Garcia, Jose F.] NASA, Ames Res Ctr, ERC Corp, Thermal Protect Mat & Syst Branch, Moffett Field, CA 94035 USA.
[John Pham] NASA, Ames Res Ctr, Univ Space Res Associates, Thermal Protect Mat & Syst Branch, Moffett Field, CA 94035 USA.
RP Agrawal, P (reprint author), NASA, Ames Res Ctr, ERC Corp, Thermal Protect Mat & Syst Branch, MS 234-1, Moffett Field, CA 94035 USA.
NR 14
TC 3
Z9 5
U1 6
U2 13
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JUL-AUG
PY 2013
VL 50
IS 4
BP 735
EP 741
DI 10.2514/1.A32389
PG 7
WC Engineering, Aerospace
SC Engineering
GA 197KS
UT WOS:000322850700002
ER
PT J
AU Bopp, MS
Ruffin, SM
Braun, RD
Clark, IG
Theisinger, JE
AF Bopp, Matthew S.
Ruffin, Stephen M.
Braun, Robert D.
Clark, Ian G.
Theisinger, John E.
TI Multi-Fidelity Approach to Estimate Heating for Three-Dimensional
Hypersonic Aeroshells
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 42nd AIAA Thermophysics Conference
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA, NASA Ames Res Ctr (ARC), NASA Strateg Capabilities Assests Program
ID EQUATIONS; ENTRY; FLOWS
AB In the early stages of aeroshell shape design, it is important to strike an appropriate balance between analysis fidelity and computational effort. Because the prediction of aerodynamic heating for axisymmetric flows is significantly faster than for three-dimensional flows, it is advantageous to employ an axisymmetric analysis method. The current work couples an equivalent axisymmetric body technique with different axisymmetric analysis methods, using a series of axisymmetric bodies to approximate the three-dimensional heating. Three levels of fidelity are considered: 1) a Newtonian inviscid solution coupled with an axisymmetric integral boundary layer approach, 2) an Euler solution coupled with an axisymmetric integral boundary-layer approach, and 3) a Navier Stokes solution applied to each equivalent axisymmetric body. Approximate solutions for three-dimensional flows were compared with high-fidelity computational and experimental data, establishing the accuracy for various levels of fidelity. The multi-fidelity analysis showed that significant decreases in computational times could be achieved, at the same time maintaining sufficient accuracy to perform shape optimization.
C1 [Bopp, Matthew S.; Ruffin, Stephen M.; Braun, Robert D.] Georgia Inst Technol, Sch Aerosp Engn, Atlanta, GA 30332 USA.
[Clark, Ian G.] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Theisinger, John E.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Bopp, MS (reprint author), Georgia Inst Technol, Sch Aerosp Engn, 270 Ferst Drive, Atlanta, GA 30332 USA.
NR 24
TC 0
Z9 0
U1 0
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JUL-AUG
PY 2013
VL 50
IS 4
BP 754
EP 762
DI 10.2514/1.A32211
PG 9
WC Engineering, Aerospace
SC Engineering
GA 197KS
UT WOS:000322850700004
ER
PT J
AU Johansen, CT
Danehy, PM
Ashcraft, SW
Bathel, BF
Inman, JA
Jones, SB
AF Johansen, C. T.
Danehy, P. M.
Ashcraft, S. W.
Bathel, B. F.
Inman, J. A.
Jones, S. B.
TI Planar Laser-Induced Fluorescence of Mars Science Laboratory Reaction
Control System Jets
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 41st AIAA Fluid Dynamics Conference and Exhibit
CY JUN 27-30, 2011
CL Honolulu, HI
SP AIAA, US Army Res Off
ID VISUALIZATION; LAMINAR; FLOWS
AB Nitric-oxide planar laser-induced fluorescence was used to visualize the flow in the wake of a Mars Science Laboratory entry capsule with activated reaction control system jets in NASA Langley Research Center's 31 in. Mach 10 air tunnel facility. Images were processed using the virtual diagnostics interface method, which brings out the three-dimensional nature of the flow visualization data while showing the relative location of the data with respect to the model. Comparison of wind-on and wind-off results illustrates the effect that the hypersonic crossflow has on the trajectory and structure of individual reaction control system jets. The visualization and comparison of both single and multiple activated jets indicate low levels of jet-jet interaction. Quantitative streamwise velocity was also obtained via molecular tagging velocimetry.
C1 [Johansen, C. T.] NASA, Langley Res Ctr, Natl Inst Aerosp, Hampton, VA 23681 USA.
[Johansen, C. T.; Danehy, P. M.; Ashcraft, S. W.; Bathel, B. F.; Inman, J. A.; Jones, S. B.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA.
[Johansen, C. T.] Univ Calgary, Calgary, AB T2N 1N4, Canada.
[Ashcraft, S. W.] Univ Kentucky, Lexington, KY 40506 USA.
[Bathel, B. F.] Univ Virginia, Charlottesville, VA 22904 USA.
RP Johansen, CT (reprint author), NASA, Langley Res Ctr, Natl Inst Aerosp, MS 493, Hampton, VA 23681 USA.
NR 29
TC 2
Z9 2
U1 1
U2 4
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JUL-AUG
PY 2013
VL 50
IS 4
BP 781
EP 792
DI 10.2514/1.A32214
PG 12
WC Engineering, Aerospace
SC Engineering
GA 197KS
UT WOS:000322850700007
ER
PT J
AU Hill, J
Wang, KW
Fang, H
AF Hill, J.
Wang, K. W.
Fang, H.
TI Advances of Surface Control Methodologies for Flexible Space Reflectors
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID SHAPE CONTROL; MEMBRANE REFLECTORS
AB With the advances in deployable membrane technologies, the possibility of developing large, lightweight reflectors has greatly improved. However, to achieve the required accuracy, precision surface control is needed. The goal of this research was to investigate the feasibility of applying distributed polyvinylidene fluoride actuators and domain control on a flexible reflector and address some of the technical challenges. An analytical model of the integrated reflector-actuator system was developed. A Kapton reflector with polyvinylidene fluoride actuators was experimentally tested and compared with the model. A new least-squares control law is designed to ensure optimal solutions are derived in a rigorous manner when constraints are applied. The model is exercised using individually controlled polyvinylidene fluoride actuators on a large-scale reflector under thermal load. Although the results are promising with the large number of actuators applied, the major challenge is that it is unrealistic to have the same number of power supplies as actuators in actual applications. To resolve this issue, a new optimization methodology was developed, designated as the en masse elimination algorithm, which finds the global optimal solution that groups the actuators to match the limited number of power supplies and achieve minimum surface error.
C1 [Hill, J.; Wang, K. W.] Univ Michigan, Dept Mech Engn, Ann Arbor, MI 48109 USA.
[Fang, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hill, J (reprint author), Univ Michigan, Dept Mech Engn, 2350 Hayward St, Ann Arbor, MI 48109 USA.
FU NASA
FX Part of the research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA.
NR 19
TC 8
Z9 8
U1 1
U2 10
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JUL-AUG
PY 2013
VL 50
IS 4
BP 816
EP 828
DI 10.2514/1.A32231
PG 13
WC Engineering, Aerospace
SC Engineering
GA 197KS
UT WOS:000322850700011
ER
PT J
AU Yunis, I
AF Yunis, Isam
TI Standard Deviation of Launch Vehicle Vibration and Acoustic Environments
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB Statistical analyses are used for the development of the acoustic, vibration, and shock environments on launch vehicles. The standard deviation of these environments is critical for deriving accurate statistical extrema. However, often very little measured data exist in order to define the standard deviation. In many cases, the use of a typical standard deviation is better than the use of one derived from a few measurements. Extensive Space Shuttle Program and Expendable Launch Vehicle flight data are used in this paper to define a typical standard deviation for acoustics and random vibrations. The results suggest that, in the absence of sufficient data, 3 dB is a practical selection for the standard deviation of these environments. Further, the data are used to show that a standard deviation of 3 dB should be used for cases in which there are less than five data sets because there is not enough information to supersede the 3 dB estimate.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Yunis, I (reprint author), NASA, Langley Res Ctr, Mail Stop 431, Hampton, VA 23681 USA.
NR 4
TC 1
Z9 1
U1 0
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JUL-AUG
PY 2013
VL 50
IS 4
BP 829
EP 837
DI 10.2514/1.A32375
PG 9
WC Engineering, Aerospace
SC Engineering
GA 197KS
UT WOS:000322850700012
ER
PT J
AU Gaier, JR
Hicks, MC
Misconin, RM
AF Gaier, James R.
Hicks, Michael C.
Misconin, Robert M.
TI Studies of Simulated Lunar Dust on the Properties of Thermal-Control
Surfaces
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB A study was carried out to examine several factors that can influence how dust can degrade thermal-control surfaces on the moon. The most important factor, besides how much dust covers the thermal-control surface, was the solar absorptance a and, to a lesser extent, the thermal emittance e of the dust covering the surface. Full coverage of the lightest and darkest dust degraded the alpha/epsilon of the surface by a factor of about 1.5 and 5.8 respectively. Silver-backed fluoroethylene propylene exhibited the least amount of degradation by lightest-colored dust, and although its fractional degradation for the darkest-colored dust was the highest, the absolute value of the alpha/epsilon was still lower than that of white thermal-control paint (AZ93) or aluminized fluoroethylene propylene. Neither illumination angle nor particle size (for particles less than 50 mu m) were found to degrade the alpha/epsilon of thermal-control surfaces in an important way. The degradation in alpha/epsilon by complete monolayer coverage was much less than would be predicted from a simple rule of mixtures. Development of effective mitigation strategies will be essential to avoid prohibitive mass penalties for thermal-control systems that must work in a dusty environment.
C1 [Gaier, James R.; Hicks, Michael C.] NASA, John H Glenn Res Ctr Lewis Field, Space Environm & Expt Branch, Cleveland, OH 44135 USA.
[Hicks, Michael C.] NASA, John H Glenn Res Ctr Lewis Field, Combust & Reacting Syst Branch, Cleveland, OH 44135 USA.
[Misconin, Robert M.] Ohio Aerosp Inst, 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.
FU Exploration Technology Development Program's Dust Mitigation Project;
Advanced Thermal Control Project
FX This work is the result of a great deal of effort by a sizable team of
dedicated professionals from many organizations. Edward A. Sechkar of
the Arctic Slope Research Corporation (ASRC) and Frank P. Lam (Jacobs
Sverdrup) provided engineering and technical support of the LDAB
facility. Scott R. Panko (ASRC) provided both electrical engineering and
test engineering support for the LDAB. An expanded expert team did the
thermal modeling led by Michael C. Hicks, and including Robert J.
Christie, Lauren K. Clayman, and George R. Harpster (NASA John H. Glenn
Research Center at Lewis Field). Don Jaworske (NASA John H. Glenn
Research Center at Lewis Field) oversaw the fabrication of the test
samples and acted as a general resource on the behavior of
thermal-control coatings. Technical, programmatic, and financial support
was provided by the Exploration Technology Development Program's Dust
Mitigation Project (Mark J. Hyatt, NASA John H. Glenn Research Center at
Lewis Field) and Advanced Thermal Control Project (Ryan A. Stephan, NASA
Johnson Space Center).
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PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JUL-AUG
PY 2013
VL 50
IS 4
BP 848
EP 852
DI 10.2514/1.A32135
PG 5
WC Engineering, Aerospace
SC Engineering
GA 197KS
UT WOS:000322850700014
ER
PT J
AU Osipov, V
Muratov, C
Hafiychuk, H
Ponizovskaya-Devine, E
Smelyanskiy, V
Mathias, D
Lawrence, S
Werkheiser, M
AF Osipov, Viatcheslav
Muratov, Cyrill
Hafiychuk, Halyna
Ponizovskaya-Devine, Ekaterina
Smelyanskiy, Vadim
Mathias, Donovan
Lawrence, Scott
Werkheiser, Mary
TI Explosion Hazard from a Propellant-Tank Breach in Liquid Hydrogen-Oxygen
Rockets
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID DETONATION
AB An engineering risk assessment of the conditions for massive explosions of cryogenic liquid hydrogen-oxygen rockets during launch accidents is presented. The assessment is based on the analysis of the data of purposeful rupture experiments with liquid oxygen and hydrogen tanks and on an interpretation of these data via analytical semiquantitative estimates and numerical simulations of simplified models for the whole range of the physical phenomena governing the outcome of a propellant-tank breach. The following sequence of events is reconstructed: rupture of fuel tanks, escape of the fluids from the ruptured tanks, liquid film boiling, fragmentation of liquid flow, formation of aerosol oxygen and hydrogen clouds, mixing of the clouds, droplet evaporation, self-ignition of the aerosol clouds, and aerosol combustion. The power of the explosion is determined by a small fraction of the escaped cryogens that become well mixed within the aerosol cloud during the delay time between rupture and ignition. Several scenarios of cavitation-induced self-ignition of the cryogenic hydrogen/oxygen mixture are discussed. The explosion parameters in a particular accident are expected to be highly varied and unpredictable due to randomness of the processes of formation, mixing, and ignition of oxygen and hydrogen clouds. Under certain conditions rocket accidents may result in very strong explosions with blast pressures from a few atm up to 100 atm. The most dangerous situations and the foreseeable risks for space missions are uncovered.
C1 [Osipov, Viatcheslav; Muratov, Cyrill; Hafiychuk, Halyna; Ponizovskaya-Devine, Ekaterina; Smelyanskiy, Vadim; Mathias, Donovan; Lawrence, Scott; Werkheiser, Mary] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Osipov, V (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU NASA [NNX10AC65G]
FX We acknowledge Frank Benz from NASA Johnson Space Center White Sands
Test Facility for providing the test data for Hydrogen-Oxygen vertical
impact tests performed at the facility and for valuable discussions. The
work of CBM was supported by NASA via grant number NNX10AC65G.
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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 JUL-AUG
PY 2013
VL 50
IS 4
BP 860
EP 871
DI 10.2514/1.A32277
PG 12
WC Engineering, Aerospace
SC Engineering
GA 197KS
UT WOS:000322850700016
ER
PT J
AU Townsend, LJ
Drave, SP
Hill, AB
Coe, MJ
Corbet, RHD
Bird, AJ
Schurch, MPE
AF Townsend, L. J.
Drave, S. P.
Hill, A. B.
Coe, M. J.
Corbet, R. H. D.
Bird, A. J.
Schurch, M. P. E.
TI Contrasting behaviour from two Be/X-ray binary pulsars: insights into
differing neutron star accretion modes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: emission-line, Be; Magellanic Clouds; X-rays: binaries
ID SMALL-MAGELLANIC-CLOUD; PHOTON IMAGING CAMERA; XMM-NEWTON; FUNDAMENTAL
PARAMETERS; ECLIPSING BINARIES; CATALOG; STREAM; DISTANCE; SMC
AB In this paper we present the identification of two periodic X-ray signals coming from the direction of the Small Magellanic Cloud (SMC). On detection with the Rossi X-ray Timing Explorer (RXTE), the 175.4 s and 85.4 s pulsations were considered to originate from new Be/ X-ray binary (BeXRB) pulsars with unknown locations. Using rapid follow-up INTEGRAL and XMM-Newton observations, we show the first pulsar (designated SXP175) to be coincident with a candidate high-mass X-ray binary (HMXB) in the northern bar region of the SMC undergoing a small Type II outburst. The orbital period (87 d) and spectral class (B0-B0.5IIIe) of this system are determined and presented here for the first time. The second pulsar is shown not to be new at all, but is consistent with being SXP91.1 - a pulsar discovered at the very beginning of the 13 year long RXTE key monitoring programme of the SMC. Whilst it is theoretically possible for accreting neutron stars to change spin period so dramatically over such a short time, the X-ray and optical data available for this source suggest this spin-up is continuous during long phases of X-ray quiescence, where accretion-driven spin-up of the neutron star should be minimal.
C1 [Townsend, L. J.; Drave, S. P.; Hill, A. B.; Coe, M. J.; Bird, A. J.] Univ Southampton, Fac Phys & Appl Sci, Southampton SO17 1BJ, Hants, England.
[Hill, A. B.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Hill, A. B.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Corbet, R. H. D.] Univ Maryland Baltimore Cty, Xray Astrophys Lab, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schurch, M. P. E.] Univ Cape Town, Dept Astron, ACGC, ZA-7701 Rondebosch, South Africa.
RP Townsend, LJ (reprint author), Univ Southampton, Fac Phys & Appl Sci, Southampton SO17 1BJ, Hants, England.
EM ljt203@soton.ac.uk
OI Hill, Adam/0000-0003-3470-4834
FU University of Southampton; Claude Leon Foundation; NRF of South Africa;
La Silla Observatory [079. D-0371(A)]; Marie Curie International
Outgoing Fellowship within the 7th European Community Framework
Programme [275861]
FX LJT is supported by a Mayflower scholarship from the University of
Southampton. MPES is funded through the Claude Leon Foundation and the
NRF of South Africa. We are grateful to the staff at SAAO, and Tetsuya
Nagata, for support during the 1.9-m and IRSF telescope runs. This work
is based on observations made with ESO Telescopes at the La Silla
Observatory under programme ID 079. D-0371(A). ABH acknowledges that
this research was supported by a Marie Curie International Outgoing
Fellowship within the 7th European Community Framework Programme
(FP7/2007-2013) under grant agreement no. 275861. We thank Helen Klus
for her help with some of the data analysis and the referee for their
comments on which this paper has benefitted.
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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 JUL
PY 2013
VL 433
IS 1
BP 23
EP 35
DI 10.1093/mnras/stt646
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 178PZ
UT WOS:000321461200002
ER
PT J
AU Burgay, M
Bailes, M
Bates, SD
Bhat, NDR
Burke-Spolaor, S
Champion, DJ
Coster, P
D'Amico, N
Johnston, S
Keith, MJ
Kramer, M
Levin, L
Lyne, AG
Milia, S
Ng, C
Possenti, A
Stappers, BW
Thornton, D
Tiburzi, C
van Straten, W
Bassa, CG
AF Burgay, M.
Bailes, M.
Bates, S. D.
Bhat, N. D. R.
Burke-Spolaor, S.
Champion, D. J.
Coster, P.
D'Amico, N.
Johnston, S.
Keith, M. J.
Kramer, M.
Levin, L.
Lyne, A. G.
Milia, S.
Ng, C.
Possenti, A.
Stappers, B. W.
Thornton, D.
Tiburzi, C.
van Straten, W.
Bassa, C. G.
TI The High Time Resolution Universe Pulsar Survey - VII. Discovery of five
millisecond pulsars and the different luminosity properties of binary
and isolated recycled pulsars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE pulsars: individual: PSR J1431-5740; pulsars: individual: PSR
J1545-4550; pulsars: individual: PSR J1825-0319; pulsars: individual:
PSR J1832-0836; pulsars: individual: PSR J2236-5527
ID GALACTIC MAGNETIC-FIELD; LARGE-AREA TELESCOPE; RADIO PULSARS;
GLOBULAR-CLUSTERS; ROTATION MEASURES; TIMING ANALYSIS; FREE-ELECTRONS;
POLARIZATION; EMISSION; SEARCH
AB This paper presents the discovery and timing parameters for five millisecond pulsars (MSPs), four in binary systems with probable white dwarf companions and one isolated, found in ongoing processing of the High Time Resolution Universe Pulsar (HTRU) survey. We also present high-quality polarimetric data on four of them. These further discoveries confirm the high potential of our survey in finding pulsars with very short spin periods. At least two of these five MSPs are excellent candidates to be included in the pulsar timing array projects. Thanks to the wealth of MSP discoveries in the HTRU survey, we revisit the question of whether the luminosity distributions of isolated and binary MSPs are different. Using the Cordes and Lazio distance model and our new and catalogue flux density measurements, we find that 41 of the 42 most luminous MSPs in the Galactic disc are in binaries, and a statistical analysis suggests that the luminosity functions differ with 99.9 per cent significance. We conclude that the formation process that leads to solitary MSPs affects their luminosities, despite their period and period derivatives being similar to those of pulsars in binary systems.
C1 [Burgay, M.; D'Amico, N.; Milia, S.; Possenti, A.; Tiburzi, C.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy.
[Bailes, M.; Bhat, N. D. R.; Coster, P.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Bailes, M.] ARC Ctr Excellence All Sky Astrophys, Sydney, NSW 2016, Australia.
[Bates, S. D.; Levin, L.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[Bhat, N. D. R.] Curtin Univ Technol, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia.
[Burke-Spolaor, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91104 USA.
[Champion, D. J.; Kramer, M.; Ng, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Coster, P.; Johnston, S.; Keith, M. J.; Thornton, D.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[D'Amico, N.; Tiburzi, C.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, Italy.
[Kramer, M.; Lyne, A. G.; Stappers, B. W.; Thornton, D.; Bassa, C. G.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
RP Burgay, M (reprint author), INAF Osservatorio Astron Cagliari, Str 54, I-09012 Capoterra, Italy.
EM burgay@oa-cagliari.inaf.it
OI Champion, David/0000-0003-1361-7723; Burgay, Marta/0000-0002-8265-4344;
van Straten, Willem/0000-0003-2519-7375
FU Commonwealth of Australia; National Aeronautics and Space
Administration; ASI [I/047/08/0-WP3000]
FX The Parkes radio telescope is part of the Australia Telescope which is
funded by the Commonwealth of Australia for operation as a National
Facility managed by CSIRO.; 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.; MBu
and AP have been partly funded under the ASI contract I/047/08/0-WP3000
(Fermi).
NR 66
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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 JUL
PY 2013
VL 433
IS 1
BP 259
EP 269
DI 10.1093/mnras/stt721
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 178PZ
UT WOS:000321461200022
ER
PT J
AU Burningham, B
Cardoso, CV
Smith, L
Leggett, SK
Smart, RL
Mann, AW
Dhital, S
Lucas, PW
Tinney, CG
Pinfield, DJ
Zhang, Z
Morley, C
Saumon, D
Aller, K
Littlefair, SP
Homeier, D
Lodieu, N
Deacon, N
Marley, MS
van Spaandonk, L
Baker, D
Allard, F
Andrei, AH
Canty, J
Clarke, J
Day-Jones, AC
Dupuy, T
Fortney, JJ
Gomes, J
Ishii, M
Jones, HRA
Liu, M
Magazzu, A
Marocco, F
Murray, DN
Rojas-Ayala, B
Tamura, M
AF Burningham, Ben
Cardoso, C. V.
Smith, L.
Leggett, S. K.
Smart, R. L.
Mann, A. W.
Dhital, S.
Lucas, P. W.
Tinney, C. G.
Pinfield, D. J.
Zhang, Z.
Morley, C.
Saumon, D.
Aller, K.
Littlefair, S. P.
Homeier, D.
Lodieu, N.
Deacon, N.
Marley, M. S.
van Spaandonk, L.
Baker, D.
Allard, F.
Andrei, A. H.
Canty, J.
Clarke, J.
Day-Jones, A. C.
Dupuy, T.
Fortney, J. J.
Gomes, J.
Ishii, M.
Jones, H. R. A.
Liu, M.
Magazzu, A.
Marocco, F.
Murray, D. N.
Rojas-Ayala, B.
Tamura, M.
TI 76 T dwarfs from the UKIDSS LAS: benchmarks, kinematics and an updated
space density
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; brown dwarfs; stars: low-mass
ID INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; GALACTIC CLUSTERS SURVEY;
INFRARED-SURVEY-EXPLORER; INTEGRAL-FIELD SPECTROGRAPH; COOLEST BROWN
DWARFS; EARLY DATA RELEASE; LARGE-AREA SURVEY; SOLAR NEIGHBORHOOD; L/T
TRANSITION
AB We report the discovery of 76 new T dwarfs from the UKIRT Infrared Deep Sky Survey (UKIDSS) Large Area Survey (LAS). Near-infrared broad- and narrow-band photometry and spectroscopy are presented for the new objects, along with Wide-field Infrared Survey Explorer (WISE) and warm-Spitzer photometry. Proper motions for 128 UKIDSS T dwarfs are presented from a new two epoch LAS proper motion catalogue. We use these motions to identify two new benchmark systems: LHS 6176AB, a T8p+M4 pair and HD 118865AB, a T5.5+F8 pair. Using age constraints from the primaries and evolutionary models to constrain the radii, we have estimated their physical properties from their bolometric luminosity. We compare the colours and properties of known benchmark T dwarfs to the latest model atmospheres and draw two principal conclusions. First, it appears that the H - [4.5] and J - W2 colours are more sensitive to metallicity than has previously been recognized, such that differences in metallicity may dominate over differences in T-eff when considering relative properties of cool objects using these colours. Secondly, the previously noted apparent dominance of young objects in the late-T dwarf sample is no longer apparent when using the new model grids and the expanded sample of late-T dwarfs and benchmarks. This is supported by the apparently similar distribution of late-T dwarfs and earlier type T dwarfs on reduced proper motion diagrams that we present. Finally, we present updated space densities for the late-T dwarfs, and compare our values to simulation predictions and those from WISE.
C1 [Burningham, Ben; Cardoso, C. V.; Smith, L.; Lucas, P. W.; Pinfield, D. J.; Zhang, Z.; van Spaandonk, L.; Baker, D.; Canty, J.; Clarke, J.; Day-Jones, A. C.; Gomes, J.; Jones, H. R. A.; Marocco, F.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Burningham, Ben; Andrei, A. H.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil.
[Cardoso, C. V.; Smart, R. L.; Andrei, A. H.] Osserv Astron Torino, Ist Nazl Astrofis, I-10025 Pino Torinese, Italy.
[Leggett, S. K.] Gemini Observ, Hilo, HI 96720 USA.
[Mann, A. W.; Aller, K.; Liu, M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Dhital, S.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Tinney, C. G.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia.
[Tinney, C. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Morley, C.; Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Saumon, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Littlefair, S. P.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
[Homeier, D.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Homeier, D.] Ecole Normale Super Lyon, CRAL, CNRS, UMR 5574, F-69364 Lyon, France.
[Lodieu, N.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Lodieu, N.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Deacon, N.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Marley, M. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Andrei, A. H.] Shanghai Astron Observatory, CAS, Shanghai 200030, Peoples R China.
[Andrei, A. H.] Univ Fed Rio de Janeiro, Observat Valongo, BR-20080090 Rio de Janeiro, Brazil.
[Day-Jones, A. C.] Univ Chile, Camino Observ, Santiago, Chile.
[Dupuy, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ishii, M.] Subaru Telescope, Hilo, HI 96720 USA.
[Magazzu, A.] INAF, Fundac Galileo Galilei, E-38700 Santa Cruz De La Palma, Spain.
[Rojas-Ayala, B.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
[Tamura, M.] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan.
RP Burningham, B (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
EM b.burningham@herts.ac.uk
RI Rojas-Ayala, Barbara/G-4382-2015;
OI Leggett, Sandy/0000-0002-3681-2989; Rojas-Ayala,
Barbara/0000-0002-0149-1302; Littlefair, Stuart/0000-0001-7221-855X;
Smart, Richard/0000-0002-4424-4766; Burningham, Ben/0000-0003-4600-5627;
Fortney, Jonathan/0000-0002-9843-4354; Homeier,
Derek/0000-0002-8546-9128; Magazzu, Antonio/0000-0003-1259-4371; Allard,
France/0000-0003-1929-9340; Mann, Andrew/0000-0003-3654-1602; Marley,
Mark/0000-0002-5251-2943; Tinney, Christopher/0000-0002-7595-0970
FU Marie Curie 7th European Community Framework Programme [247593];
Fondecyt postdoctorado fellowship [3100098]; proyecto Basal [PB06
(CATA)]; Joint Committee ESO-Government Chile; CNPq [PQ306775/2009-3];
SHAO/CAS; ARC [DP0774000]; Gemini Observatory; RoPACS; Marie Curie
Initial Training Network; European Commission; Spanish Ministry of
Science and Innovation through the Ramon y Cajal fellowship
[08-303-01-02, AYA2010-19136]
FX We thank our referee, J. Davy Kirkpatrick, for a helpful review which
substantially improved the quality of this manuscript. Based on
observations made under project A22TAC96 on the Italian Telescopio
Nazionale Galileo (TNG) operated on the island of La Palma by the
Fundacin Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica)
at the Spanish Observatorio del Roque de los Muchachos of the Instituto
de Astrofisica de Canarias. Based on observations obtained at the Gemini
Observatory, which is operated by the Association of Universities for
Research in Astronomy, Inc., under a cooperative agreement with the NSF
on behalf of the Gemini partnership: the National Science Foundation
(United States), the Science and Technology Facilities Council (United
Kingdom), the National Research Council (Canada), CONICYT (Chile), the
Australian Research Council (Australia), Ministerio da Ciencia e
Tecnologia (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion
Productiva (Argentina). We would like to acknowledge the support of the
Marie Curie 7th European Community Framework Programme grant no. 247593
Interpretation and Parametrization of Extremely Red COOL dwarfs
(IPERCOOL) International Research Staff Exchange Scheme. ADJ is
supported by a Fondecyt postdoctorado fellowship, under project number
3100098, and is also partially supported by the proyecto Basal PB06
(CATA) and the Joint Committee ESO-Government Chile. AHA thanks CNPq
grant PQ306775/2009-3 and SHAO/CAS Visiting Professorship grant. CGT is
supported by ARC grant DP0774000. SKL's research is supported by the
Gemini Observatory. JG is supported by RoPACS, a Marie Curie Initial
Training Network funded by the European Commission's Seventh Framework
Programme. NL acknowledges funding from the Spanish Ministry of Science
and Innovation through the Ramon y Cajal fellowship number 08-303-01-02
and the project number AYA2010-19136. 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 the SIMBAD data base, operated at CDS,
Strasbourg, France, and has benefited from the SpeX Prism Spectral
Libraries, maintained by Adam Burgasser at
http://www.browndwarfs.org/spexprism. 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 124
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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 JUL
PY 2013
VL 433
IS 1
BP 457
EP 497
DI 10.1093/mnras/stt740
PG 41
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 178PZ
UT WOS:000321461200038
ER
PT J
AU Lidman, C
Iacobuta, G
Bauer, AE
Barrientos, LF
Cerulo, P
Couch, WJ
Delaye, L
Demarco, R
Ellingson, E
Faloon, AJ
Gilbank, D
Huertas-Company, M
Mei, S
Meyers, J
Muzzin, A
Noble, A
Nantais, J
Rettura, A
Rosati, P
Sanchez-Janssen, R
Strazzullo, V
Webb, TMA
Wilson, G
Yan, R
Yee, HKC
AF Lidman, C.
Iacobuta, G.
Bauer, A. E.
Barrientos, L. F.
Cerulo, P.
Couch, W. J.
Delaye, L.
Demarco, R.
Ellingson, E.
Faloon, A. J.
Gilbank, D.
Huertas-Company, M.
Mei, S.
Meyers, J.
Muzzin, A.
Noble, A.
Nantais, J.
Rettura, A.
Rosati, P.
Sanchez-Janssen, R.
Strazzullo, V.
Webb, T. M. A.
Wilson, G.
Yan, R.
Yee, H. K. C.
TI The importance of major mergers in the build up of stellar mass in
brightest cluster galaxies at z=1
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: general; galaxies: evolution; galaxies:
high-redshift
ID COLOR-MAGNITUDE DIAGRAM; SIMILAR-TO 1; X-RAY; SPECTROSCOPIC
CONFIRMATION; CLOSE COMPANIONS; HIGH-REDSHIFT; HAWK-I; EVOLUTION;
MATTER; DISCOVERY
AB Recent independent results from numerical simulations and observations have shown that brightest cluster galaxies (BCGs) have increased their stellar mass by a factor of almost 2 between z similar to 0.9 and z similar to 0.2. The numerical simulations further suggest that more than half this mass is accreted through major mergers. Using a sample of 18 distant galaxy clusters with over 600 spectroscopically confirmed cluster members between them, we search for observational evidence that major mergers do play a significant role. We find a major merger rate of 0.38 +/- 0.14 mergers per Gyr at z similar to 1. While the uncertainties, which stem from the small size of our sample, are relatively large, our rate is consistent with the results that are derived from numerical simulations. If we assume that this rate continues to the present day and that half of the mass of the companion is accreted on to the BCG during these mergers, then we find that this rate can explain the growth in the stellar mass of the BCGs that is observed and predicted by simulations. Major mergers therefore appear to be playing an important role, perhaps even the dominant one, in the build up of stellar mass in these extraordinary galaxies.
C1 [Lidman, C.; Iacobuta, G.; Bauer, A. E.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Iacobuta, G.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Cerulo, P.; Couch, W. J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Delaye, L.; Huertas-Company, M.; Mei, S.] Observ Paris, GEPI, F-70514 Paris, France.
[Demarco, R.; Nantais, J.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Ellingson, E.] Univ Colorado, Dept Astrophys & Planetary Sci, UCB 389, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Faloon, A. J.; Noble, A.; Webb, T. M. A.] McGill Univ, Montreal, PQ H3A 2T8, Canada.
[Gilbank, D.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Huertas-Company, M.; Mei, S.] Univ Paris Denis Diderot, Paris 13, France.
[Meyers, J.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Muzzin, A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Rettura, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rosati, P.] European So Observ, D-85748 Garching, Germany.
[Sanchez-Janssen, R.] European So Observ, Santiago 19, Chile.
[Strazzullo, V.] Univ Paris Diderot, CEA Saclay, Irfu Serv Astrophys, Lab AIM Paris Saclay,CEA DSM CNRS, F-91191 Gif Sur Yvette, France.
[Wilson, G.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Yan, R.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA.
[Yee, H. K. C.] Univ Toronto, Dept Phys & Astron, Toronto M5S 3H4, ON, Canada.
RP Lidman, C (reprint author), Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia.
EM clidman@aao.gov.au
FU Australian Research Council [FT0992259, DP0877642]; Fondo National de
Desarollo Cientifico y Tecnologico (FONDECYT) [1085286, 1120676];
FONDECYT [3120233, 1100540]; National Science Foundation [AST-0909198]
FX The authors thank Chris Collins, John Stott, Adam Duffy and Darren
Croton for useful discussions, and Adam Stanford for making available
the redshifts for XMMXCS 2215. The data in this paper were based in part
on observations obtained at the ESO Paranal Observatory (ESO programmes
060.A-9284(H) and 084.A-0214). CL is the recipient of an Australian
Research Council Future Fellowship (programme number FT0992259). LFB was
supported by Fondo National de Desarollo Cientifico y Tecnologico
(FONDECYT) grants No. 1085286 and 1120676. WJC is the recipient of an
Australian Research Council Professorial Fellowship (programme number
DP0877642). JN acknowledges the support provided from FONDECYT research
grant number 3120233. RD acknowledges the support provided from FONDECYT
research grant number 1100540. GW gratefully acknowledges support from
National Science Foundation grant AST-0909198.
NR 71
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Z9 45
U1 0
U2 1
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 JUL
PY 2013
VL 433
IS 1
BP 825
EP 837
DI 10.1093/mnras/stt777
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 178PZ
UT WOS:000321461200068
ER
PT J
AU Semboloni, E
Hoekstra, H
Huang, Z
Cardone, VF
Cropper, M
Joachimi, B
Kitching, T
Kuijken, K
Lombardi, M
Maoli, R
Mellier, Y
Miller, L
Rhodes, J
Scaramella, R
Schrabback, T
Velander, M
AF Semboloni, E.
Hoekstra, H.
Huang, Z.
Cardone, V. F.
Cropper, M.
Joachimi, B.
Kitching, T.
Kuijken, K.
Lombardi, M.
Maoli, R.
Mellier, Y.
Miller, L.
Rhodes, J.
Scaramella, R.
Schrabback, T.
Velander, M.
TI On the shear estimation bias induced by the spatial variation of colour
across galaxy profiles
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; surveys
ID HUBBLE-SPACE-TELESCOPE; WEAK LENSING SURVEYS; EXTRAGALACTIC LEGACY
SURVEY; IMAGE-ANALYSIS COMPETITION; POINT-SPREAD FUNCTION; SHAPE
MEASUREMENT; COSMIC SHEAR; GREAT08 CHALLENGE; GROTH STRIP; NOISE BIAS
AB The spatial variation of the colour of a galaxy may introduce a bias in the measurement of its shape if the point spread function (PSF) profile depends on wavelength. We study how this bias depends on the properties of the PSF and the galaxies themselves. The bias depends on the scales used to estimate the shape, which may be used to optimize methods to reduce the bias. Here, we develop a general approach to quantify the bias. Although applicable to any weak lensing survey, we focus on the implications for the ESA Euclid mission.
Based on our study of synthetic galaxies, we find that the bias is a few times 10(-3) for a typical galaxy observed by Euclid. Consequently, it cannot be neglected and needs to be accounted for. We demonstrate how one can do so using spatially resolved observations of galaxies in two filters. We show that Hubble Space Telescope (HST) observations in the F606W and F814W filters allow us to model and reduce the bias by an order of magnitude, sufficient to meet Euclid's scientific requirements. The precision of the correction is ultimately determined by the number of galaxies for which spatially resolved observations in at least two filters are available. We use results from the Millennium simulation to demonstrate that archival HST data will be sufficient for the tomographic cosmic shear analysis with the Euclid data set.
C1 [Semboloni, E.; Hoekstra, H.; Kuijken, K.; Velander, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Huang, Z.; Cardone, V. F.; Scaramella, R.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Cropper, M.; Kitching, T.] Univ Coll London, Mullard Space Lab, Dorking RH5 6NT, Surrey, England.
[Joachimi, B.; Kitching, T.] Univ Edinburgh, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Lombardi, M.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy.
[Maoli, R.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Mellier, Y.] Univ Paris 06, CNRS UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Miller, L.; Velander, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Rhodes, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schrabback, T.] Argelander Inst Astron, D-53121 Bonn, Germany.
[Schrabback, T.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
RP Semboloni, E (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM sembolon@strw.leidenuniv.nl
OI Scaramella, Roberto/0000-0003-2229-193X; LOMBARDI,
MARCO/0000-0002-3336-4965; Hoekstra, Henk/0000-0002-0641-3231
FU Netherlands Organization for Scientific Research (NWO); European
Research Council [279396]; UK Space Agency; STFC [ST/J001422/1]; Royal
Society University Research Fellowship; JPL; NSF [AST-0444059-001]; SAO
[GO0-11147A]; DLR [FKZ 50 QE 1103]; Beecroft Institute for Particle
Astrophysics and Cosmology; National Science Foundation [1066293]
FX We would like to thank Gary Bernstein, Christopher Hirata, Jerome
Amiaux, Frederic Courbin and Edo van Uitert and in general, the members
of the Euclid Consortium for helpful discussions. We would also like to
thank the anonymous referee who helped us to improve the quality of this
manuscript. ES and HH acknowledge the support of the Netherlands
Organization for Scientific Research (NWO) through a VIDI grant and the
support from the European Research Council under FP7 grant number
279396. BJ acknowledges support by a UK Space Agency Euclid grant and by
STFC Consolidated Grant ST/J001422/1. TK was supported by a Royal
Society University Research Fellowship. JR was supported by JPL, run by
Caltech under a contract for NASA. TS acknowledges support from NSF
through grant AST-0444059-001, SAO through grant GO0-11147A, and DLR
through grant FKZ 50 QE 1103. MV acknowledges support from the
Netherlands Organization for Scientific Research (NWO) and from the
Beecroft Institute for Particle Astrophysics and Cosmology. This
material is based upon work supported in part by the National Science
Foundation under Grant No. 1066293 and the hospitality of the Aspen
Center for Physics.
NR 48
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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 JUL
PY 2013
VL 432
IS 3
BP 2385
EP 2401
DI 10.1093/mnras/stt602
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 165AW
UT WOS:000320455800040
ER
PT J
AU Mazer, SJ
Travers, SE
Cook, BI
Davies, TJ
Bolmgren, K
Kraft, NJB
Salamin, N
Inouye, DW
AF Mazer, Susan J.
Travers, Steven E.
Cook, Benjamin I.
Davies, T. Jonathan
Bolmgren, Kjell
Kraft, Nathan J. B.
Salamin, Nicolas
Inouye, David W.
TI FLOWERING DATE OF TAXONOMIC FAMILIES PREDICTS PHENOLOGICAL SENSITIVITY
TO TEMPERATURE: IMPLICATIONS FOR FORECASTING THE EFFECTS OF CLIMATE
CHANGE ON UNSTUDIED TAXA
SO AMERICAN JOURNAL OF BOTANY
LA English
DT Article
ID LONG-TERM; PLANT PHENOLOGY; CENTRAL-EUROPE; LIFE-HISTORY; PHENOTYPIC
PLASTICITY; TEMPORAL VARIABILITY; TROPHIC INTERACTIONS; SPRING
PHENOLOGY; RAPID EVOLUTION; THOREAUS WOODS
AB Premise of the study: Numerous long-term studies in seasonal habitats have tracked interannual variation in first flowering date (FFD) in relation to climate, documenting the effect of warming on the FFD of many species. Despite these efforts, long-term phenological observations are still lacking for many species. If we could forecast responses based on taxonomic affinity, however, then we could leverage existing data to predict the climate-related phenological shifts of many taxa not yet studied.
Methods: We examined phenological time series of 1226 species occurrences (1031 unique species in 119 families) across seven sites in North America and England to determine whether family membership (or family mean FFD) predicts the sensitivity of FFD to standardized interannual changes in temperature and precipitation during seasonal periods before flowering and whether families differ significantly in the direction of their phenological shifts.
Key results: Patterns observed among species within and across sites are mirrored among family means across sites; early-flowering families advance their FFD in response to warming more than late-flowering families. By contrast, we found no consistent relationships among taxa between mean FFD and sensitivity to precipitation as measured here.
Conclusions: Family membership can be used to identify taxa of high and low sensitivity to temperature within the seasonal, temperate zone plant communities analyzed here. The high sensitivity of early-flowering families (and the absence of early-flowering families not sensitive to temperature) may reflect plasticity in flowering time, which may be adaptive in environments where early-season conditions are highly variable among years.
C1 [Mazer, Susan J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
[Mazer, Susan J.] Stellenbosch Inst Adv Study STIAS, ZA-7602 Stellenbosch, South Africa.
[Travers, Steven E.] N Dakota State Univ, Dept Biol Sci, Fargo, ND 58102 USA.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Cook, Benjamin I.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Davies, T. Jonathan] McGill Univ, Dept Biol, Montreal, PQ H3A 0G4, Canada.
[Bolmgren, Kjell] Lund Univ, Theoret Populat Ecol & Evolut Grp, S-22100 Lund, Sweden.
[Bolmgren, Kjell] Swedish Univ Agr Sci, Swedish Natl Phenol Network, SE-36030 Lammhult, Sweden.
[Kraft, Nathan J. B.; Inouye, David W.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Salamin, Nicolas] Swiss Inst Bioinformat, CH-1015 Lausanne, Switzerland.
[Inouye, David W.] Rocky Mt Biol Labs, Crested Butte, CO 81224 USA.
RP Mazer, SJ (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
EM mazer@lifesci.ucsb.edu
RI Kraft, Nathan/A-2817-2012; Cook, Benjamin/H-2265-2012; Inouye,
David/C-2997-2011; Bolmgren, Kjell/E-1459-2016
OI Kraft, Nathan/0000-0001-8867-7806; Inouye, David/0000-0003-2076-7834;
Bolmgren, Kjell/0000-0001-9552-9684
FU NSF [EF-0553768]; University of California, Santa Barbara; State of
California; National Center for Ecological Analysis and Synthesis
FX We are indebted to those who contributed the phenological time series
analyzed here, including the many scientists and volunteers who recorded
field data or who managed subsets of the data, particularly A. H.
Fitter, R. S. R. Fitter (Chinnor), David Inouye (Gothic), John O'Keefe
(Harvard Forest), and Paul Huth, Shana Smiley, and John Thompson
(Mohonk, NY). The observational studies examined here were originally
designed by investigators and supported by funding sources listed in the
online Supplemental Data (Appendix S1). Special thanks are due to the
National Center for Ecological Analysis and Synthesis (funded by NSF
EF-0553768, the University of California, Santa Barbara, and the State
of California) for supporting the working group on "Forecasting
Phenology". The Stellenbosch Institute for Advanced Study graciously
hosted S. J. M. during the preparation of this manuscript.
NR 86
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U1 0
U2 92
PU BOTANICAL SOC AMER INC
PI ST LOUIS
PA PO BOX 299, ST LOUIS, MO 63166-0299 USA
SN 0002-9122
J9 AM J BOT
JI Am. J. Bot.
PD JUL
PY 2013
VL 100
IS 7
BP 1381
EP 1397
DI 10.3732/ajb.1200455
PG 17
WC Plant Sciences
SC Plant Sciences
GA 182TF
UT WOS:000321766600013
PM 23752756
ER
PT J
AU Wolkovich, EM
Davies, TJ
Schaefer, H
Cleland, EE
Cook, BI
Travers, SE
Willis, CG
Davis, CC
AF Wolkovich, Elizabeth M.
Davies, T. Jonathan
Schaefer, Hanno
Cleland, Elsa E.
Cook, Benjamin I.
Travers, Steven E.
Willis, Charles G.
Davis, Charles C.
TI TEMPERATURE-DEPENDENT SHIFTS IN PHENOLOGY CONTRIBUTE TO THE SUCCESS OF
EXOTIC SPECIES WITH CLIMATE CHANGE
SO AMERICAN JOURNAL OF BOTANY
LA English
DT Article
DE non-native species; flowering time; introduced species; invasion
biology; plant phenology; temperate grasslands; North American prairies
ID DARWINS NATURALIZATION HYPOTHESIS; FLOWERING PHENOLOGY; PHENOTYPIC
PLASTICITY; DECIDUOUS FOREST; ADAPTIVE EVOLUTION; TALLGRASS PRAIRIE;
INVASIVE PLANT; LEAF PHENOLOGY; THOREAUS WOODS; GLOBAL CHANGE
AB Premise of the study: The study of how phenology may contribute to the assembly of plant communities has a long history in ecology. Climate change has brought renewed interest in this area, with many studies examining how phenology may contribute to the success of exotic species. In particular, there is increasing evidence that exotic species occupy unique phenological niches and track climate change more closely than native species.
Methods: Here, we use long-term records of species' first flowering dates from five northern hemisphere temperate sites (Chinnor, UK and in the United States, Concord, Massachusetts; Fargo, North Dakota; Konza Prairie, Kansas; and Washington, D. C.) to examine whether invaders have distinct phenologies. Using a broad phylogenetic framework, we tested for differences between exotic and native species in mean annual flowering time, phenological changes in response to temperature and precipitation, and longer-term shifts in first flowering dates during recent pronounced climate change ("flowering time shifts").
Key results: Across North American sites, exotic species have shifted flowering with climate change while native species, on average, have not. In the three mesic systems, exotic species exhibited higher tracking of interannual variation in temperature, such that flowering advances more with warming, than native species. Across the two grassland systems, however, exotic species differed from native species primarily in responses to precipitation and soil moisture, not temperature.
Conclusions: Our findings provide cross-site support for the role of phenology and climate change in explaining species' invasions. Further, they support recent evidence that exotic species may be important drivers of extended growing seasons observed with climate change in North America.
C1 [Wolkovich, Elizabeth M.] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V5Z 1M9, Canada.
[Wolkovich, Elizabeth M.; Cleland, Elsa E.] Univ Calif San Diego, Div Biol Sci, La Jolla, CA 92093 USA.
[Davies, T. Jonathan] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
[Schaefer, Hanno; Davis, Charles C.] Harvard Univ Herbaria, Dept Organism & Evolutionary Biol, Cambridge, MA USA.
[Schaefer, Hanno] Tech Univ Munich, D-80290 Munich, Germany.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Cook, Benjamin I.] Lamont Doherty Earth Observ, Palisades, NY USA.
[Travers, Steven E.] N Dakota State Univ, Dept Biol Sci, Fargo, ND 58105 USA.
[Willis, Charles G.] Duke Univ, Dept Biol, Durham, NC USA.
RP Wolkovich, EM (reprint author), Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V5Z 1M9, Canada.
EM lizzie@biodiversity.ubc.ca
RI Cook, Benjamin/H-2265-2012
FU NSERC CREATE training program in biodiversity research
FX The authors thank all data collectors and contributors for sharing their
data and R. Abbott, R. FitzJohn, N. Salamin, and W. Wen for data
collection and analysis help. Comments from J. Craine, H. Kharouba, R.
Primack. S. Weller, and two anonymous reviewers improved the manuscript.
This work was conducted while E. M. W. was a National Science Foundation
Postdoctoral Research Fellow in Biology (DBI-0905806) and also while she
was supported by the NSERC CREATE training program in biodiversity
research.
NR 92
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U1 11
U2 198
PU BOTANICAL SOC AMER INC
PI ST LOUIS
PA PO BOX 299, ST LOUIS, MO 63166-0299 USA
SN 0002-9122
J9 AM J BOT
JI Am. J. Bot.
PD JUL
PY 2013
VL 100
IS 7
BP 1407
EP 1421
DI 10.3732/ajb.1200478
PG 15
WC Plant Sciences
SC Plant Sciences
GA 182TF
UT WOS:000321766600015
PM 23797366
ER
PT J
AU Paletz, SBF
Kim, KH
Schunn, CD
Tollinger, I
Vera, A
AF Paletz, Susannah B. F.
Kim, Kevin H.
Schunn, Christian D.
Tollinger, Irene
Vera, Alonso
TI Reuse and Recycle: The Development of Adaptive Expertise, Routine
Expertise, and Novelty in a Large Research Team
SO APPLIED COGNITIVE PSYCHOLOGY
LA English
DT Article
ID MENTAL MODELS; ORGANIZATIONAL ROUTINES; PERFORMANCE; CREATIVITY;
KNOWLEDGE; INNOVATION; AMBIDEXTERITY; EXPLOITATION; ENVIRONMENTS;
FLEXIBILITY
AB Combining innovation and efficiency is ideal in many organizational settings. Adaptive expertise represents a cognitive explanation of how individuals and teams can learn to achieve simultaneous innovation and efficiency. In 2004, scientists led twin rovers on Mars in the search for historical water. The science team experienced a remarkable increase in efficiency, adapting with flexibility to unexpected events and dynamic, dwindling resources. After discussing the conceptual differences between adaptive expertise and related team learning and innovation concepts, we examine longitudinal behavioral data on novelty, routine and adaptive expertise. Sequential time series ARIMA analyses reveal that novelty fluctuated randomly, but both routine and adaptive expertise significantly increased over time. In addition, novelty, routine expertise, and adaptive expertise did not significantly predict each other directly or at a lag, suggesting that these are indeed three distinct constructs. Implications for theory and research on efficiency and innovation are discussed. Copyright (C) 2013 John Wiley & Sons, Ltd.
C1 [Paletz, Susannah B. F.] Univ Maryland, Ctr Adv Study Language, College Pk, MD 20742 USA.
[Kim, Kevin H.] Univ Pittsburgh, Sch Educ, Pittsburgh, PA 15260 USA.
[Schunn, Christian D.] Univ Pittsburgh, Learning Res & Dev Ctr, Pittsburgh, PA USA.
[Tollinger, Irene; Vera, Alonso] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
RP Paletz, SBF (reprint author), Univ Maryland, Ctr Adv Study Language, 7005 52nd Ave, College Pk, MD 20742 USA.
EM sbfpaletz@gmail.com
OI Schunn, Christian/0000-0003-3589-297X
NR 78
TC 3
Z9 3
U1 5
U2 31
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0888-4080
J9 APPL COGNITIVE PSYCH
JI Appl. Cogn. Psychol.
PD JUL
PY 2013
VL 27
IS 4
BP 415
EP 428
DI 10.1002/acp.2928
PG 14
WC Psychology, Experimental
SC Psychology
GA 188UU
UT WOS:000322221400001
ER
PT J
AU Kowalski, AF
Hawley, SL
Wisniewski, JP
Osten, RA
Hilton, EJ
Holtzman, JA
Schmidt, SJ
Davenport, JRA
AF Kowalski, Adam F.
Hawley, Suzanne L.
Wisniewski, John P.
Osten, Rachel A.
Hilton, Eric J.
Holtzman, Jon A.
Schmidt, Sarah J.
Davenport, James R. A.
TI TIME-RESOLVED PROPERTIES AND GLOBAL TRENDS IN dMe FLARES FROM
SIMULTANEOUS PHOTOMETRY AND SPECTRA
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE stars: atmospheres; stars: flare
ID WHITE-LIGHT FLARES; LOW-MASS STARS; YZ CANIS MINORIS; RADIATIVE
HYDRODYNAMIC MODELS; EXTREME-ULTRAVIOLET-EXPLORER; GAMMA-RAY BURSTS;
M-DWARF FLARES; UV CETI STARS; SOLAR-FLARE; X-RAY
AB We present a homogeneous analysis of line and continuum emission from simultaneous high-cadence spectra and photometry covering near-ultraviolet and optical wavelengths for 20 M dwarf flares. These data were obtained to study the white-light continuum components at bluer and redder wavelengths than the Balmer jump. Our goals were to break the degeneracy between emission mechanisms that have been fit to broadband colors of flares and to provide constraints for radiative-hydrodynamic (RHD) flare models that seek to reproduce the white-light flare emission. The main results from the analysis are the following: (1) the detection of Balmer continuum (in emission) that is present during all flares and with a wide range of relative contributions to the continuum flux at bluer wavelengths than the Balmer jump; (2) a blue continuum at flare maximum that is linearly decreasing with wavelength from lambda = 4000-4800 angstrom, indicative of hot, blackbody emission with typical temperatures of T-BB similar to 9000-14,000 K; (3) a redder continuum apparent at wavelengths longer than H beta (lambda greater than or similar to 4900 angstrom) which becomes relatively more important to the energy budget during the late gradual phase. The hot blackbody component and redder continuum component have been detected in previous studies of flares. However, we have found that although the hot blackbody emission component is relatively well-represented by a featureless, single-temperature Planck function, this component includes absorption features and has a continuum shape strikingly similar to the spectrum of an A-type star as directly observed in our flare spectra. New model constraints are presented for the time evolution among the hydrogen Balmer lines and between Ca II K and the blackbody continuum emission. We calculate Balmer jump flux ratios and compare to the solar-type flare heating predictions from RHD models. The model ratios are too large and the blue-optical (lambda = 4000-4800 angstrom) slopes are too red in both the impulsive and gradual decay phases of all 20 flares. This discrepancy implies that further work is needed to understand the heating at high column mass during dMe flares.
C1 [Kowalski, Adam F.; Hawley, Suzanne L.; Davenport, James R. A.] Univ Washington, Dept Astron, Uw Seattle, WA 98195 USA.
[Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Osten, Rachel A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hilton, Eric J.] Universe Sandbox, Seattle, WA USA.
[Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Schmidt, Sarah J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
RP Kowalski, AF (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
EM adam.f.kowalski@nasa.gov
OI Schmidt, Sarah/0000-0002-7224-7702; Davenport, James/0000-0002-0637-835X
FU NSF [AST08-07205]; NASA [Kepler GO NNX11AB71G]; ORAU/NASA; K-Unit
FX We thank an anonymous referee for helpful suggestions that improved this
paper. This work resulted from the PhD Dissertation of A. F. K. at the
University of Washington Department of Astronomy. We thank M. Giampapa
for suggesting to investigate flare speeds and H. Lamers for insight
that contributed to the ideas developed in this section. We acknowledge
many helpful discussions at L. Fletcher's International Space Sciences
Institute (ISSI) "Solar Chromospheric Flares" team meetings, in
particular with L. Fletcher, H. Hudson, P. Heinzel, G. Cauzzi, and M.
Carlsson. We thank M. Mathioudakis for useful discussions. We thank K.
Covey for the use of his PyRAF spectral reduction software. We thank N.
Ule for obtaining data. We thank J. Allred for the use of his flare
model results. We would like to thank the staff at the Apache Point
Observatory and especially the Observing Specialists (R. McMillan, W.
Ketzeback, J. Huehnerhoff, G. Sarage, and J. Dembicky) at the 3.5 m for
assistance with data acquisition and data calibration feedback. We also
thank the SDSS 2.5 m observers at the Apache Point Observatory for
on-site assistance with the ARCSAT 0.5 m telescope. Finally, we thank E.
Agol for useful discussions and feedback on this work. A. F. K.
acknowledges support from NSF grant AST08-07205, NASA Kepler GO
NNX11AB71G, the ORAU/NASA Postdoctoral Program, and the K-Unit.
NR 139
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUL
PY 2013
VL 207
IS 1
AR UNSP 15
DI 10.1088/0067-0049/207/1/15
PG 57
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 194KJ
UT WOS:000322631500015
ER
PT J
AU Robberto, M
Soderblom, DR
Bergeron, E
Kozhurina-Platais, V
Makidon, RB
McCullough, PR
McMaster, M
Panagia, N
Reid, IN
Levay, Z
Frattare, L
Da Rio, N
Andersen, M
O'Dell, CR
Stassun, KG
Simon, M
Feigelson, ED
Stauffer, JR
Meyer, M
Reggiani, M
Krist, J
Manara, CF
Romaniello, M
Hillenbrand, LA
Ricci, L
Palla, F
Najita, JR
Ananna, TT
Scandariato, G
Smith, K
AF Robberto, M.
Soderblom, D. R.
Bergeron, E.
Kozhurina-Platais, V.
Makidon, R. B.
McCullough, P. R.
McMaster, M.
Panagia, N.
Reid, I. N.
Levay, Z.
Frattare, L.
Da Rio, N.
Andersen, M.
O'Dell, C. R.
Stassun, K. G.
Simon, M.
Feigelson, E. D.
Stauffer, J. R.
Meyer, M.
Reggiani, M.
Krist, J.
Manara, C. F.
Romaniello, M.
Hillenbrand, L. A.
Ricci, L.
Palla, F.
Najita, J. R.
Ananna, T. T.
Scandariato, G.
Smith, K.
TI THE HUBBLE SPACE TELESCOPE TREASURY PROGRAM ON THE ORION NEBULA CLUSTER
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE brown dwarfs; ISM: individual objects (M42); stars: formation; stars:
low-mass; stars: pre-main sequence
ID LOW-MASS STARS; T-TAURI STARS; MULTICOLOR OPTICAL SURVEY; BROWN DWARFS;
TRAPEZIUM CLUSTER; CIRCUMSTELLAR DISKS; PROTOPLANETARY DISKS;
EVOLUTIONARY MODELS; ACCRETION RATES; EMISSION-LINES
AB The Hubble Space Telescope (HST) Treasury Program on the Orion Nebula Cluster (ONC) has used 104 orbits of HST time to image the Great Orion Nebula region with the Advanced Camera for Surveys (ACS), the Wide-Field/PlanetaryCamera 2 (WFPC2), and the Near-Infrared Camera and Multi-Object Spectrograph (NICMOS) instrument in 11 filters ranging from the U band to the H band equivalent of HST. The program has been intended to perform the definitive study of the stellar component of the ONC at visible wavelengths, addressing key questions like the cluster initial mass function, age spread, mass accretion, binarity, and cirumstellar disk evolution. The scanning pattern allowed us to cover a contiguous field of approximately 600 arcmin(2) with both ACS and WFPC2, with a typical exposure time of approximately 11 minutes per ACS filter, corresponding to a point source depth AB(F435W) = 25.8 and AB(F775W) = 25.2 with 0.2 mag of photometric error. We describe the observations, data reduction, and data products, including images, source catalogs, and tools for quick look preview. In particular, we provide ACS photometry for 3399 stars, most of them detected at multiple epochs; WFPC2 photometry for 1643 stars, 1021 of them detected in the U band; and NICMOS JH photometry for 2116 stars. We summarize the early science results that have been presented in a number of papers. The final set of images and the photometric catalogs are publicly available through the archive as High Level Science Products at the STScI Multimission Archive hosted by the Space Telescope Science Institute.
C1 [Robberto, M.; Soderblom, D. R.; Bergeron, E.; Kozhurina-Platais, V.; Makidon, R. B.; McCullough, P. R.; McMaster, M.; Panagia, N.; Reid, I. N.; Levay, Z.; Frattare, L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Panagia, N.; Scandariato, G.] INAF CT Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Da Rio, N.; Andersen, M.] European Space Agcy, NL-2200 AG Noordwijk, Netherlands.
[O'Dell, C. R.; Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Stassun, K. G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
[Stassun, K. G.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Simon, M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Feigelson, E. D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Stauffer, J. R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Meyer, M.; Reggiani, M.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Krist, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Manara, C. F.; Romaniello, M.] European So Observ, D-85748 Garching, Germany.
[Hillenbrand, L. A.; Ricci, L.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Palla, F.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Najita, J. R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Ananna, T. T.] Bryn Mawr Coll, Bryn Mawr, PA 19010 USA.
[Smith, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Robberto, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM robberto@stsci.edu
OI palla, francesco/0000-0002-3321-0456
FU NASA/ESA Hubble Space Telescope under the GO program [10246]; NASA [NAS
5-26555]
FX Based on observations made with the NASA/ESA Hubble Space Telescope
under the GO program No. 10246, 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 No. 10246.
NR 83
TC 12
Z9 12
U1 1
U2 8
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 JUL
PY 2013
VL 207
IS 1
AR UNSP 10
DI 10.1088/0067-0049/207/1/10
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 194KJ
UT WOS:000322631500010
ER
PT J
AU Buccello-Stout, RR
Cromwell, RL
Bloomberg, JJ
Whorton, EB
AF Buccello-Stout, Regina R.
Cromwell, Ronita L.
Bloomberg, Jacob J.
Whorton, Elbert B.
TI Sensorimotor Adaptation Training's Effect on Head Stabilization in
Response to a Lateral Perturbation in Older Adults
SO JOURNAL OF AGING AND PHYSICAL ACTIVITY
LA English
DT Article
DE postural stability; falls in older adults; balance control
ID VISUAL RISK-FACTORS; MOTOR SKILL; VIRTUAL ENVIRONMENT; OBSTACLE
AVOIDANCE; ADAPTIVE-CONTROL; LOCOMOTOR TASKS; HIP FRACTURE; WALKING;
FALLS; PEOPLE
AB The goal of this study was to determine if exposure to sensorimotor adaptation training improved head stabilization in older adults. Sixteen participants, age 66-81 yr, were assigned at random to the control group (n = 8) or the experimental group (n = 8). Both groups first completed 6 trials of walking a foam pathway consisting of a moveable platform that induced a lateral perturbation during walking. Head-in-space and trunk-in-space angular velocities were collected. Participants from both groups then trained twice per week for 4 wk. Both groups walked on a treadmill for 20 min. The control group viewed a static scene. The experimental group viewed a rotating visual scene that provided a perceptual-motor mismatch. After training, both groups were retested on the perturbation pathway test. The experimental group used a movement strategy that preserved head stabilization compared with the controls (p < .05). This training effect was not retained after 4 wk.
C1 [Buccello-Stout, Regina R.] Wyle Integrated Sci & Engn, Neurosci Labs, Houston, TX USA.
[Cromwell, Ronita L.] Univ Space Res Assoc, Div Flight Analogs, Houston, TX USA.
[Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA.
[Whorton, Elbert B.] Galveston Natl Lab, Inst Human Infect & Immun, Galveston, TX USA.
RP Buccello-Stout, RR (reprint author), Wyle Integrated Sci & Engn, Neurosci Labs, Houston, TX USA.
FU National Aeronautics and Space Administration [NASA-NNJ05JG67H];
National Space Biomedical Research Institute through NASA NCC [9-58]
FX This research was supported by both a grant from the National
Aeronautics and Space Administration Graduate Student Researchers
Program (NASA-NNJ05JG67H) and the National Space Biomedical Research
Institute through NASA NCC 9-58.
NR 53
TC 2
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U1 3
U2 8
PU HUMAN KINETICS PUBL INC
PI CHAMPAIGN
PA 1607 N MARKET ST, PO BOX 5076, CHAMPAIGN, IL 61820-2200 USA
SN 1063-8652
J9 J AGING PHYS ACTIV
JI J. Aging Phys. Act.
PD JUL
PY 2013
VL 21
IS 3
BP 272
EP 289
PG 18
WC Geriatrics & Gerontology; Gerontology; Sport Sciences
SC Geriatrics & Gerontology; Sport Sciences
GA 190QI
UT WOS:000322354900003
PM 23006335
ER
PT J
AU Dunkley, J
Calabrese, E
Sievers, J
Addison, GE
Battaglia, N
Battistelli, ES
Bond, JR
Das, S
Devlin, MJ
Dunner, R
Fowler, JW
Gralla, M
Hajian, A
Halpern, M
Hasselfield, M
Hincks, AD
Hlozek, R
Hughes, JP
Irwin, KD
Kosowsky, A
Louis, T
Marriage, TA
Marsden, D
Menanteau, F
Moodley, K
Niemack, M
Nolta, MR
Page, LA
Partridge, B
Sehgal, N
Spergel, DN
Staggs, ST
Switzer, ER
Trac, H
Wollack, E
AF Dunkley, J.
Calabrese, E.
Sievers, J.
Addison, G. E.
Battaglia, N.
Battistelli, E. S.
Bond, J. R.
Das, S.
Devlin, M. J.
Duenner, R.
Fowler, J. W.
Gralla, M.
Hajian, A.
Halpern, M.
Hasselfield, M.
Hincks, A. D.
Hlozek, R.
Hughes, J. P.
Irwin, K. D.
Kosowsky, A.
Louis, T.
Marriage, T. A.
Marsden, D.
Menanteau, F.
Moodley, K.
Niemack, M.
Nolta, M. R.
Page, L. A.
Partridge, B.
Sehgal, N.
Spergel, D. N.
Staggs, S. T.
Switzer, E. R.
Trac, H.
Wollack, E.
TI The Atacama Cosmology Telescope: likelihood for small-scale CMB data
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE cosmological parameters from CMBR; CMBR experiments; Sunyaev-Zeldovich
effect
ID SOUTH-POLE TELESCOPE; PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND
ANISOTROPIES; ZELDOVICH POWER SPECTRUM; STAR-FORMING GALAXIES;
SUNYAEV-ZELDOVICH; CLUSTER PHYSICS; 148 GHZ; PARAMETERS; REIONIZATION
AB The Atacama Cosmology Telescope has measured the angular power spectra of microwave fluctuations to arcminute scales at frequencies of 148 and 218 GHz, from three seasons of data. At small scales the fluctuations in the primordial Cosmic Microwave Background (CMB) become increasingly obscured by extragalactic foregounds and secondary CMB signals. We present results from a nine-parameter model describing these secondary effects, including the thermal and kinematic Sunyaev-Zel'dovich (tSZ and kSZ) power; the clustered and Poisson-like power from Cosmic Infrared Background (CIB) sources, and their frequency scaling; the tSZ-CIB correlation coefficient; the extragalactic radio source power; and thermal dust emission from Galactic cirrus in two different regions of the sky. In order to extract cosmological parameters, we describe a likelihood function for the ACT data, fitting this model to the multi-frequency spectra in the multipole range 500 < l < 10000. We extend the likelihood to include spectra from the South Pole Telescope at frequencies of 95, 150, and 220 GHz. Accounting for different radio source levels and Galactic cirrus emission, the same model provides an excellent fit to both datasets simultaneously, with chi(2)/dof= 675/697 for ACT, and 96/107 for SPT. We then use the multi-frequency likelihood to estimate the CMB power spectrum from ACT in bandpowers, marginalizing over the secondary parameters. This provides a simplified 'CMB-only' likelihood in the range 500 < l < 3500 for use in cosmological parameter estimation.
C1 [Dunkley, J.; Calabrese, E.; Addison, G. E.; Louis, T.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
[Sievers, J.; Hlozek, R.; Marriage, T. A.; Page, L. A.; Staggs, S. T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Addison, G. E.; Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Battaglia, N.; Trac, H.] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Battistelli, E. S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Bond, J. R.; Hajian, A.; Hincks, A. D.; Nolta, M. R.; Switzer, E. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Das, S.] Argonne Natl Lab, Div High Energy Phys, Lemont, IL 60439 USA.
[Das, S.] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Das, S.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Devlin, M. J.; Marsden, D.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Duenner, R.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Fowler, J. W.; Irwin, K. D.; Niemack, M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA.
[Gralla, M.; Marriage, T. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hasselfield, M.; Hlozek, R.; Marriage, T. A.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hughes, J. P.; Menanteau, F.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Kosowsky, A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Marsden, D.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Moodley, K.] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Niemack, M.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Partridge, B.] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Sehgal, N.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Dunkley, J (reprint author), Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England.
EM j.dunkley@physics.ox.ac.uk
RI Spergel, David/A-4410-2011; Trac, Hy/N-8838-2014; Wollack,
Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Menanteau, Felipe/0000-0002-1372-2534; Sievers,
Jonathan/0000-0001-6903-5074
FU U.S. National Science Foundation [AST-0408698, AST-0965625, PHY-0855887,
PHY-1214379]; Princeton University; University of Pennsylvania; Canada
Foundation for Innovation (CFI); Comision Nacional de Investigacion
Cientifica y Tecnologica de Chile (CONICYT); CFI; Government of Ontario;
Ontario Research Fund - Research Excellence; University of Toronto; ERC
grant [259505]; NASA Office of Space Science; Compute Canada
FX This work was supported by the U.S. National Science Foundation through
awards AST-0408698 and AST-0965625 for the ACT project, as well as
awards PHY-0855887 and PHY-1214379. Funding was also provided by
Princeton University, the University of Pennsylvania, and a Canada
Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque
Astronomico Atacama in northern Chile under the auspices 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. Funding from ERC grant 259505
supports JD, EC, and TL. We thank George Efstathiou and Steven Gratton
for useful discussions, and Christian Reichardt for help with the SPT
data. We acknowledge the use of the Legacy Archive for Microwave
Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the
NASA Office of Space Science. The likelihood codes will be made public
through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT
website(http://www.physics.princeton.edu/act/).
NR 73
TC 42
Z9 42
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD JUL
PY 2013
IS 7
AR 025
DI 10.1088/1475-7516/2013/07/025
PG 32
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 193SO
UT WOS:000322582000026
ER
PT J
AU Hasselfield, M
Hilton, M
Marriage, TA
Addison, GE
Barrientos, LF
Battaglia, N
Battistelli, ES
Bond, JR
Crichton, D
Das, S
Devlin, MJ
Dicker, SR
Dunkley, J
Dunner, R
Fowler, JW
Gralla, MB
Hajian, A
Halpern, M
Hincks, AD
Hlozek, R
Hughes, JP
Infante, L
Irwin, KD
Kosowsky, A
Marsden, D
Menanteau, F
Moodley, K
Niemack, MD
Nolta, MR
Page, LA
Partridge, B
Reese, ED
Schmitt, BL
Sehgal, N
Sherwin, BD
Sievers, J
Sifon, C
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Thornton, R
Trac, H
Wollack, EJ
AF Hasselfield, Matthew
Hilton, Matt
Marriage, Tobias A.
Addison, Graeme E.
Barrientos, L. Felipe
Battaglia, Nicholas
Battistelli, Elia S.
Bond, J. Richard
Crichton, Devin
Das, Sudeep
Devlin, Mark J.
Dicker, Simon R.
Dunkley, Joanna
Duenner, Rolando
Fowler, Joseph W.
Gralla, Megan B.
Hajian, Amir
Halpern, Mark
Hincks, Adam D.
Hlozek, Renee
Hughes, John P.
Infante, Leopoldo
Irwin, Kent D.
Kosowsky, Arthur
Marsden, Danica
Menanteau, Felipe
Moodley, Kavilan
Niemack, Michael D.
Nolta, Michael R.
Page, Lyman A.
Partridge, Bruce
Reese, Erik D.
Schmitt, Benjamin L.
Sehgal, Neelima
Sherwin, Blake D.
Sievers, Jon
Sifon, Cristobal
Spergel, David N.
Staggs, Suzanne T.
Swetz, Daniel S.
Switzer, Eric R.
Thornton, Robert
Trac, Hy
Wollack, Edward J.
TI The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy
clusters at 148 GHz from three seasons of data
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE galaxy clusters; Sunyaev-Zeldovich effect
ID SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; GREATER-THAN 1; MICROWAVE
BACKGROUND ANISOTROPIES; DARK-ENERGY CONSTRAINTS;
HUBBLE-SPACE-TELESCOPE; X-RAY DATA; SCALING RELATIONS; POWER SPECTRUM;
RICH CLUSTERS
AB We present a catalog of 68 galaxy clusters, of which 19 are new discoveries, detected via the Sunyaev-Zel'dovich effect (SZ) at 148 GHz in the Atacama Cosmology Telescope (ACT) survey on the celestial equator. With this addition, the ACT collaboration has reported a total of 91 optically confirmed, SZ detected clusters. The 504 square degree survey region includes 270 square degrees of overlap with SDSS Stripe 82, permitting the confirmation of SZ cluster candidates in deep archival optical data. The subsample of 48 clusters within Stripe 82 is estimated to be 90% complete for M-500c > 4.5 x 10(14)M(circle dot) and redshifts 0.15 < z < 0.8. While a full suite of matched filters is used to detect the clusters, the sample is studied further through a "Profile Based Amplitude Analysis" using a statistic derived from a single filter at a fixed theta(500) = 5'.9 angular scale. This new approach incorporates the cluster redshift along with prior information on the cluster pressure profile to fix the relationship between the cluster characteristic size (R-500) and the integrated Compton parameter (Y-500). We adopt a one-parameter family of "Universal Pressure Profiles" (UPP) with associated scaling laws, derived from X-ray measurements of nearby clusters, as a baseline model. Three additional models of cluster physics are used to investigate a range of scaling relations beyond the UPP prescription. Assuming a concordance cosmology, the UPP scalings are found to be nearly identical to an adiabatic model, while a model incorporating non-thermal pressure better matches dynamical mass measurements and masses from the South Pole Telescope. A high signal to noise ratio subsample of 15 ACT clusters with complete optical follow-up is used to obtain cosmological constraints. We demonstrate, using fixed scaling relations, how the constraints depend on the assumed gas model if only SZ measurements are used, and show that constraints from SZ data are limited by uncertainty in the scaling relation parameters rather than sample size or measurement uncertainty. We next add in seven clusters from the ACT Southern survey, including their dynamical mass measurements, which are based on galaxy velocity dispersions and thus are independent of the gas physics. In combination with WMAP7 these data simultaneously constrain the scaling relation and cosmological parameters, yielding 68% confidence ranges described by sigma(8) = 0.829 +/- 0.024 and Omega(m) = 0.292 +/- 0.025. We consider these results in the context of constraints from CMB and other cluster studies. The constraints arise mainly due to the inclusion of the dynamical mass information and do not require strong priors on the SZ scaling relation parameters. The results include marginalization over a 15% bias in dynamical masses relative to the true halo mass. In an extension to Lambda CDM that incorporates non-zero neutrino mass density, we combine our data with WMAP7, Baryon Acoustic Oscillation data, and Hubble constant measurements to constrain the sum of the neutrino mass species to be Sigma(nu)m(nu) < 0.29eV (95% confidence limit).
C1 [Hasselfield, Matthew; Hlozek, Renee; Sievers, Jon; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hasselfield, Matthew; Addison, Graeme E.; Battistelli, Elia S.; Halpern, Mark] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England.
[Marriage, Tobias A.; Crichton, Devin; Gralla, Megan B.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Addison, Graeme E.; Dunkley, Joanna] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Barrientos, L. Felipe; Duenner, Rolando; Infante, Leopoldo] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Battaglia, Nicholas; Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Battaglia, Nicholas; Bond, J. Richard; Hajian, Amir; Hincks, Adam D.; Nolta, Michael R.; Sievers, Jon; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Das, Sudeep] Argonne Natl Lab, Div High Energy Phys, Lemont, IL 60439 USA.
[Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Devlin, Mark J.; Dicker, Simon R.; Marsden, Danica; Reese, Erik D.; Schmitt, Benjamin L.; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Fowler, Joseph W.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA.
[Fowler, Joseph W.; Niemack, Michael D.; Sherwin, Blake D.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 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.
[Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Sehgal, Neelima] Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Sifon, Cristobal] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Thornton, Robert] West Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA.
[Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hasselfield, M (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
EM mhasse@astro.princeton.edu; hiltonm@ukzn.ac.za; marriage@pha.jhu.edu
RI Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Trac,
Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Menanteau, Felipe/0000-0002-1372-2534; Sievers,
Jonathan/0000-0001-6903-5074; Sifon, Cristobal/0000-0002-8149-1352
FU U.S. National Science Foundation [AST-0408698, AST-0965625, PHY-0855887,
PHY-1214379]; Princeton University; University of Pennsylvania; Canada
Foundation for Innovation (CFI) award; Comision Nacional de
Investigacion Cientifica y Tecnologica de Chile (CONICYT); CFI;
Government of Ontario; Ontario Research Fund - Research Excellence;
University of Toronto; Compute Canada
FX This work was supported by the U.S. National Science Foundation through
awards AST-0408698 and AST-0965625 for the ACT project, as well as
awards PHY-0855887 and PHY-1214379. Funding was also provided by
Princeton University, the University of Pennsylvania, and a Canada
Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque
Astronomico Atacama in northern Chile under the auspices 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 126
TC 144
Z9 145
U1 0
U2 12
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 JUL
PY 2013
IS 7
AR 008
DI 10.1088/1475-7516/2013/07/008
PG 62
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 193SO
UT WOS:000322582000009
ER
PT J
AU Sepulveda, HH
Marchesiello, P
Li, ZJ
AF Sepulveda, Hector H.
Marchesiello, Patrick
Li, Zhijin
TI Oceanic data assimilation study in northern Chile: use of a 3DVAR method
SO LATIN AMERICAN JOURNAL OF AQUATIC RESEARCH
LA English
DT Article
DE ocean forecast; observational system simulation; data assimilation;
northern Chile
ID FORECASTING SYSTEM; MODELING SYSTEM; ROMS
AB We report the use of a 3-dimensional variational (3DVAR) data assimilation method as part of a numerical model off northern Chile. The numerical model is part of an ocean forecasting project that aims to understand the impact of environmental variability on the distribution of biological species in the area. We assimilated data from a simulated ocean observing system to recover a known state, obtaining a significantly smaller error when compared to a numerical run with no assimilation. Our results validate the computational implementation of the code, and allow us to evaluate the impact of the choice of data in the assimilation process: the assimilation of sea surface height being particularly important. We note that the assimilation of surface data propagates properly to greater depths and reduces the error with reference to the known state. This was possible by using covariance error matrices calculated previously for the California coastal area. The implementation of the data assimilation module is relatively simple and permits its use in operational forecasting systems, and for the design and evaluation of future ocean observational systems.
C1 [Sepulveda, Hector H.] Univ Concepcion, Dept Geophys, Concepcion, Chile.
[Marchesiello, Patrick] Lab Etudes Geophys & Oceanog Spatiale, IRD, Toulouse, France.
[Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Sepulveda, HH (reprint author), Univ Concepcion, Dept Geophys, POB 160-C, Concepcion, Chile.
EM andres@dgeo.udec.cl
RI Sepulveda, Hector/C-3712-2011
OI Sepulveda, Hector/0000-0002-0131-6627
FU project "Implementation de ROMS-3DVAR pour affiner le downscaling des
previsions MERCATOR (projet previ-ROMS)"; project INNOVA-CORFO
[07CN13IXM-A 150]
FX Funding provided by project "Implementation de ROMS-3DVAR pour affiner
le downscaling des previsions MERCATOR (projet previ-ROMS)". MERCATOR,
Fr. and project INNOVA-CORFO 07CN13IXM-A 150.
NR 13
TC 0
Z9 0
U1 1
U2 6
PU UNIV CATOLICA DE VALPARAISO
PI VALPARAISO
PA AV BRASIL 2950, PO BOX 4059, VALPARAISO, CHILE
SN 0718-560X
J9 LAT AM J AQUAT RES
JI Lat. Am. J. Aquat. Res.
PD JUL
PY 2013
VL 41
IS 3
BP 570
EP 575
DI 10.3856/vol41-issue3-fulltext-18
PG 6
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 189IY
UT WOS:000322262000018
ER
PT J
AU Shariff, K
Manning, TA
AF Shariff, Karim
Manning, Ted A.
TI A ray tracing study of shock leakage in a model supersonic jet
SO PHYSICS OF FLUIDS
LA English
DT Article
ID RECTANGULAR JET; SCREECH TONES; MIXING LAYER; SHEAR-LAYER; TRANSPORT
AB Recent work has described screech noise from a supersonic jet as being due to leakage of a wave that is otherwise trapped in the jet's interior. In that work, the simplest of many techniques used is ray tracing for a single shear-layer modeled as a row of Stuart vortices. In the present work, a lower row of vortices is added to form a plane jet. Instead of plotting ray paths, a technique of visualization analogous to streaklines is used that better corresponds to instantaneous density fields as observed, for instance, by the Schlieren method. This produces striking images that show leakage of waves at each internal reflection resulting in a row of acoustic sources as envisioned since the 1950s. However, the sources are not isotropic and each has a zone of silence in the downstream direction. Leakage creates a fold in the wave pattern internal to the jet which leads to fine scale features. Reported experiments have also observed fine scale features (described as splitting) in the shock-cell pattern; they may be related to those observed here. Internally reflected rays also undergo a diffusive process as they propagate down the jet. In particular, each successive internal reflection at an unsteady shear-layer scatters rays along a wider range of wave angle and makes them more susceptible to leakage at the next reflection. It also causes more downstream directivity for the more downstream sources. An important result is that as the Mach number M-j is varied, maxima in leakage rate and mean acoustic amplitude occur at (near) resonances between the Mach-wave and shear-layer periods. Maxima in sound pressure level versus M-j have also been reported for laboratory round jets. Finally, as the shear-layer thickness is increased, a minimum in the rate of leakage (correlated with a minimum in radiation amplitude) occurs due to the competing effects of increased shear-layer penetration versus reduced eddy passage frequency.
C1 [Shariff, Karim; Manning, Ted A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Shariff, K (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
OI Shariff, Karim/0000-0002-7256-2497
NR 27
TC 3
Z9 3
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 1070-6631
J9 PHYS FLUIDS
JI Phys. Fluids
PD JUL
PY 2013
VL 25
IS 7
AR 076103
DI 10.1063/1.4813630
PG 20
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 192XL
UT WOS:000322521100053
ER
PT J
AU Thompson, MA
Kirkpatrick, D
Mace, GN
Cushing, MC
Gelino, CR
Griffith, RL
Skrutskie, MF
Eisenhardt, PRM
Wright, EL
Marsh, KA
Mix, KJ
Beichman, CA
Faherty, JK
Toloza, O
Ferrara, J
Apodaca, B
Mclean, IS
Bloom, JS
AF Thompson, Maggie A.
Kirkpatrick, Davy
Mace, Gregory N.
Cushing, Michael C.
Gelino, Christopher R.
Griffith, Roger L.
Skrutskie, Michael F.
Eisenhardt, Peter R. M.
Wright, Edward L.
Marsh, Kenneth A.
Mix, Katholeen J.
Beichman, Charles A.
Faherty, Jacqueline K.
Toloza, Odette
Ferrara, Jocelyn
Apodaca, Brian
Mclean, Ian S.
Bloom, Joshua S.
TI Nearby M, L, and T Dwarfs Discovered by the Wide-field Infrared Survey
Explorer (WISE)
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID DIGITAL SKY SURVEY; ULTRACOOL BROWN DWARFS; SPECTRAL TYPE-L; LOW-MASS
STARS; PROPER MOTIONS; COOL NEIGHBORS; LUMINOSITY FUNCTION; TELESCOPE
FACILITY; SURVEY 2MASS; DATA RELEASE
AB In our effort to complete the census of low-mass stars and brown dwarfs in the immediate solar neighborhood, we present spectra, photometry, proper motions, and distance estimates for 42 low-mass star and brown dwarf candidates discovered by the Wide-field Infrared Survey Explorer (WISE). We also present additional follow-up information on 12 candidates selected using WISE data but previously published elsewhere. The new discoveries include 15 M dwarfs, 17 L dwarfs, five T dwarfs, and five objects of other types. Among these discoveries is a newly identified "unusually red L dwarf" (WISE J223527.07 + 451140.9), four peculiar L dwarfs whose spectra are most readily explained as unresolved L + T binary systems, and a T9 dwarf (WISE J124309.61 + 844547.8). We also show that the recently discovered red L dwarf WISEP J004701.06 + 680352.1 may be a low-gravity object and hence young and potentially low-mass (<25 M-Jup).
C1 [Thompson, Maggie A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kirkpatrick, Davy; Mace, Gregory N.; Gelino, Christopher R.; Griffith, Roger L.; Mix, Katholeen J.; Beichman, Charles A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Mace, Gregory N.; Wright, Edward L.; Mclean, Ian S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Marsh, Kenneth A.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Faherty, Jacqueline K.] Univ Chile Cerro Calan, Dept Astron, Las Condes CF24 3AA, S Glam, Wales.
[Toloza, Odette] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile.
[Ferrara, Jocelyn] Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Apodaca, Brian] Calif State Polytech Univ Pomona, Pomona, CA 91768 USA.
[Bloom, Joshua S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Thompson, MA (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall,4 Ivy Lane, Princeton, NJ 08544 USA.
EM mat3@princeton.edu
FU National Aeronautics and Space Administration (NASA); NASA [NNG06GH50G];
National Science Foundation; 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; Space Telescope Science Institute under U.S. Government [NAG
W-2166]; NASA by JPL/Caltech [70062, 80109]; Harvard University Milton
Fund; National Science Foundation, a PAARE Grant for the
California-Arizona Minority Partnership for Astronomy Research and
Education (CAMPARE) [AST-0847170]
FX We thank David Ciardi and Gerard van Belle for their help in acquiring
the 2013 February 21 Keck/NIRSPEC observations, and we thank our
anonymous referee for a timely and helpful report. 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 data products from 2MASS, SDSS, and DSS.
2MASS is a joint project of the University of Massachusetts and the
Infrared Processing and Analysis Center/California Institute of
Technology, funded by NASA and the National Science Foundation. SDSS is
funded 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 DSS were produced at the Space Telescope
Science Institute under U.S. Government grant NAG W-2166. The images of
these surveys are based on photographic data obtained using the Oschin
Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. 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 to programs
70062 and 80109 by JPL/Caltech. 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 NASA. This research has also benefitted from the M, L, and
T dwarf compendium housed at DwarfArchives.org; from the SIMBAD
database, operated at CDS, Strasbourg, France; and from NASA's
Astrophysics Data System. We acknowledge support from the Steward/Mount
Bigelow staff for use of the 2MASS imager at the Bigelow 61 inch
telescope. We acknowledge use of PAIRITEL, which is operated by the
Smithsonian Astrophysical Observatory (SAO) and was made possible by a
grant from the Harvard University Milton Fund, the camera loaned from
the University of Virginia, and the continued support of the SAO and UC
Berkeley. The PAIRITEL project is supported by NASA Grant NNG06GH50G.
This material is based on work supported by the National Science
Foundation under Award No. AST-0847170, a PAARE Grant for the
California-Arizona Minority Partnership for Astronomy Research and
Education (CAMPARE). Any opinions, findings, and conclusions or
recommendations expressed in this material are those of the authors and
do not necessarily reflect the views of the National Science Foundation.
NR 89
TC 24
Z9 24
U1 0
U2 7
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 JUL
PY 2013
VL 125
IS 929
BP 809
EP 837
DI 10.1086/671426
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 188TT
UT WOS:000322217800007
ER
PT J
AU Nicol, SJ
Allain, V
Pilling, GM
Polovina, J
Coll, M
Bell, J
Dalzell, P
Sharples, P
Olson, R
Griffiths, S
Dambacher, JM
Young, J
Lewis, A
Hampton, J
Molina, JJ
Hoyle, S
Briand, K
Bax, N
Lehodey, P
Williams, P
AF Nicol, Simon J.
Allain, Valerie
Pilling, Graham M.
Polovina, Jeff
Coll, Marta
Bell, Johann
Dalzell, Paul
Sharples, Peter
Olson, Robert
Griffiths, Shane
Dambacher, Jeffrey M.
Young, Jock
Lewis, Antony
Hampton, John
Molina, Jesus Jurado
Hoyle, Simon
Briand, Karine
Bax, Nic
Lehodey, Patrick
Williams, Peter
TI An ocean observation system for monitoring the affects of climate change
on the ecology and sustainability of pelagic fisheries in the Pacific
Ocean
SO CLIMATIC CHANGE
LA English
DT Article
ID MARINE ECOSYSTEMS; EASTERN AUSTRALIA; TROPHIC CASCADES; TOP PREDATORS;
FOOD-WEB; EL-NINO; DYNAMICS; ECOPATH; MODEL; BIODIVERSITY
AB Climate change presents an emerging challenge to the sustainable management of tuna fisheries, and robust information is essential to ensure future sustainability. Climate and harvest affect tuna stocks, populations of non-target, dependent species and the ecosystem. To provide relevant advice we need an improved understanding of oceanic ecosystems and better data to parameterise the models that forecast the impacts of climate change. Currently ocean-wide data collection in the Pacific Ocean is primarily restricted to oceanographic data. However, the fisheries observer programs that operate in the region offer an opportunity to collect the additional information on the mid and upper trophic levels of the ecosystem that is necessary to complement this physical data, including time-series of distribution, abundance, size, composition and biological information on target and non-target species and mid trophic level organisms. These observer programs are in their infancy, with limited temporal and spatial distribution but recent international and national policy decisions have been made to expand their coverage. We identify a number of actions to initiate this monitoring including: consolidating collaborations to ensure the use of best quality data; developing consistency between sub-regional observer programmes to ensure that they meet the objectives of ecosystem monitoring; interrogating of existing time series to determine the most appropriate spatial template for monitoring; and exploring existing ecosystem models to identify suitable indicators of ecosystem status and change. The information obtained should improve capacity to develop fisheries management policies that are resilient and can be adapted to climate change.
C1 [Nicol, Simon J.; Allain, Valerie; Pilling, Graham M.; Polovina, Jeff; Sharples, Peter; Lewis, Antony; Hampton, John; Molina, Jesus Jurado; Hoyle, Simon; Briand, Karine; Williams, Peter] Secretariat Pacific Community, Noumea 98848, New Caledonia.
[Polovina, Jeff] Natl Marine Fisheries Serv, Honolulu, HI 96822 USA.
[Coll, Marta] Inst Ciencias Mar, Barcelona 08003, Spain.
[Dalzell, Paul] Western Pacific Reg Fisheries Management Council, Honolulu, HI 96813 USA.
[Olson, Robert] Interamer Trop Tuna Commiss, La Jolla, CA 92037 USA.
[Griffiths, Shane] Commonwealth Sci & Ind Res Org, Dutton Pk, Qld 4102, Australia.
[Dambacher, Jeffrey M.; Young, Jock; Bax, Nic] Commonwealth Sci & Ind Res Org, Hobart, Tas 7001, Australia.
[Lehodey, Patrick] CLS, Space Oceanog Div, F-31520 Ramonville St Agne, Saint Agne, France.
RP Nicol, SJ (reprint author), Secretariat Pacific Community, BP D5, Noumea 98848, New Caledonia.
EM simonn@spc.int
RI Bax, Nicholas/A-2321-2012
OI Bax, Nicholas/0000-0002-9697-4963
FU Global Environment Facility Pacific Islands Oceanic Fisheries Management
project; 9th European Union Development Fund (SCIFISH project); 10th
European Union Development Fund (SCICOFISH project); Australian
Government Overseas Aid Program (AusAID); Deutsche Gesellschaft fur
Internationale Zusammenarbeit (GIZ)
FX Financial support was provided by the Global Environment Facility
Pacific Islands Oceanic Fisheries Management project, the 9th European
Union Development Fund (SCIFISH project), the 10th European Union
Development Fund (SCICOFISH project), Australian Government Overseas Aid
Program (AusAID) and Deutsche Gesellschaft fur Internationale
Zusammenarbeit (GIZ). We would like to thank the following persons for
the provision of data and information on observer programmes: Nick
Vogel, Stephen Brouwer, Karl Staisch, Tim Park, Stuart Arceneaux, Lesley
Jantz, Eric Forney, John D. Kelly and Kevin Busscher.
NR 69
TC 13
Z9 13
U1 3
U2 63
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0165-0009
J9 CLIMATIC CHANGE
JI Clim. Change
PD JUL
PY 2013
VL 119
IS 1
SI SI
BP 131
EP 145
DI 10.1007/s10584-012-0598-y
PG 15
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 185GC
UT WOS:000321953700011
ER
PT J
AU Gnoffo, PA
Fay, CC
AF Gnoffo, Peter A.
Fay, Catharine C.
TI Laser Vaporization and Plume Chemistry in a Boron Nitride Nanotube
Production Rig
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
ID COLLISION INTEGRALS; SCHEMES; EARTH; MARS
AB Flow in a pressurized, vapor condensation boron nitride nanotube production rig is modeled. A laser provides a thermal energy source to the tip of a boron fiber bundle in a high-pressure nitrogen chamber causing a plume of boron-rich gas to rise. The buoyancy-driven flow is modeled as a mixture of thermally perfect gases (B, B-2, N, N-2, BN) in either thermochemical equilibrium or chemical nonequilibrium, assuming steady-state melt and vaporization from a 1 mm radius spot at the axis of an axisymmetric chamber. The simulation is intended to define the macroscopic thermochemical environment from which boron-rich species, including nanotubes, condense out of the plume. Simulations indicate a high-temperature environment (T > 4400 K) for elevated pressures within 1 mm of the surface, sufficient to dissociate molecular nitrogen and form BN at the base of the plume. Modifications to the program LAURA, a finite volume-based solver for hypersonic flows including coupled radiation and ablation, are described to enable this simulation. High-pressure synthesis conditions enable formation of BN vapor in the plume, which may serve to enhance formation of exceptionally long nanotubes in the pressurized vapor condensation process.
C1 [Gnoffo, Peter A.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Fay, Catharine C.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
RP Gnoffo, PA (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
NR 27
TC 3
Z9 3
U1 1
U2 16
PU AMER INST AERONAUTICS ASTRONAUTICS
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 JUL-SEP
PY 2013
VL 27
IS 3
BP 369
EP 381
DI 10.2514/1.T3996
PG 13
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 187FG
UT WOS:000322101700001
ER
PT J
AU Daryabeigi, K
Cunnington, GR
Knutson, JR
AF Daryabeigi, Kamran
Cunnington, George R.
Knutson, Jeffrey R.
TI Heat Transfer Modeling for Rigid High-Temperature Fibrous Insulation
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
ID RADIATION; CONDUCTION
AB Combined radiation and conduction heat transfer through a high-temperature, high-porosity, rigid multiple-fiber fibrous insulation was modeled using a thermal model previously used to model heat transfer in flexible single-fiber fibrous insulation. The rigid insulation studied was alumina enhanced thermal barrier at densities between 130-260 k g/m(3). The model consists of using the diffusion approximation for radiation heat transfer, a semi-empirical solid conduction model, and a standard gas conduction model. The relevant parameters needed for the heat transfer model were estimated from steady-state thermal measurements in nitrogen gas at various temperatures and environmental pressures. The heat transfer modeling methodology was evaluated by comparison with standard thermal conductivity measurements, and steady-state thermal measurements in argon and carbon dioxide gases. The heat transfer model is applicable over the temperature range of 300-1360 K, pressure range of 0.133 to 101.3 x 10(3) Pa, and over the insulation density range of 130-260 k g/m(3) in various gaseous environments.
C1 [Daryabeigi, Kamran] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
[Cunnington, George R.] Cunnington & Associates, Palo Alto, CA 94303 USA.
[Knutson, Jeffrey R.] NASA, Langley Res Ctr, Syst Integrat & Test Branch, Hampton, VA 23681 USA.
RP Daryabeigi, K (reprint author), NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Mail Stop 190, Hampton, VA 23681 USA.
NR 29
TC 3
Z9 3
U1 0
U2 16
PU AMER INST AERONAUTICS ASTRONAUTICS
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 JUL-SEP
PY 2013
VL 27
IS 3
BP 414
EP 421
DI 10.2514/1.T3998
PG 8
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 187FG
UT WOS:000322101700005
ER
PT J
AU Blosser, ML
AF Blosser, Max L.
TI Analytical Solution for Transient Thermal Response of an Insulated
Structure
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
AB An analytical solution was derived for the transient response of an insulated aerospace vehicle structure subjected to a simplified heat pulse. This simplified problem approximates the thermal response of a thermal protection system of an atmospheric entry vehicle. The exact analytical solution is solely a function of two nondimensional parameters. A simpler function of these two parameters was developed to approximate the maximum structural temperature over a wide range of parameter values. Techniques were developed to choose constant, effective properties to represent the relevant temperature and pressure-dependent properties for the insulator and structure. A technique was also developed to map a time-varying surface temperature history to an equivalent square heat pulse. Using these techniques, the maximum structural temperature rise was calculated using the analytical solutions and shown to typically agree with finite element simulations within 10-20% over the relevant range of parameters studied.
C1 NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Blosser, ML (reprint author), NASA Langley Res Ctr, Struct Mech & Concepts Branch, Stop 190, Hampton, VA 23681 USA.
NR 13
TC 1
Z9 1
U1 1
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
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 JUL-SEP
PY 2013
VL 27
IS 3
BP 422
EP 428
DI 10.2514/1.T4007
PG 7
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 187FG
UT WOS:000322101700006
ER
PT J
AU Blosser, ML
AF Blosser, Max L.
TI Mass Efficiency Considerations for Thermally Insulated Structural Skin
of an Aerospace Vehicle
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
AB An approximate equation was derived to predict the mass of insulation required to limit the maximum temperature reached by an insulated structure subjected to a transient heating pulse. In the course of the derivation, two figures of merit were identified. One figure of merit correlates to the effectiveness of the heat capacity of the underlying structural material in reducing the amount of required insulation. The second figure of merit provides an indicator of the mass efficiency of the insulator material. An iterative one-dimensional finite element analysis was used to size the external insulation required to protect the structure at a single location on the space shuttle orbiter and a reusable launch vehicle. Required insulation masses were calculated for a range of different materials for both structure and insulator. The required insulation masses calculated using the approximate equation were shown to typically agree with finite element results within 10-20% over the range of parameters studied. Finite element results closely followed the trends indicated by both figures of merit.
C1 NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Blosser, ML (reprint author), NASA Langley Res Ctr, Struct Mech & Concepts Branch, Mail Stop 190, Hampton, VA 23681 USA.
NR 11
TC 0
Z9 0
U1 1
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
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 JUL-SEP
PY 2013
VL 27
IS 3
BP 429
EP 434
DI 10.2514/1.T4008
PG 6
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 187FG
UT WOS:000322101700007
ER
PT J
AU Gokcen, T
Alunni, AI
AF Goekcen, Tahir
Alunni, Antonella I.
TI On Laminar-to-Turbulent Transition of Arc-Jet Flow in the NASA Panel
Test Facility
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
AB This paper provides experimental evidence and supporting computational analysis to characterize the laminar-to-turbulent flow transition in a high-enthalpy arc-jet facility at NASA Ames Research Center. The arc-jet test data obtained in the 20 MW Panel Test Facility include measurements of surface pressure and heat flux on a water-cooled calibration plate and measurements of surface temperature on a tile plate with reaction-cured glass-coating. Computational fluid dynamics simulations are performed to characterize the arc-jet test environment and estimate its parameters consistent with the facility and calibration measurements. The present analysis is composed of simulations of the nonequilibrium flowfleld in the facility nozzle, test box, and flowfield over test articles. Both laminar and turbulent simulations are performed, and the computed results are compared with the experimental measurements, including Stanton number dependence on Reynolds number. Comparisons of computed and measured surface heat fluxes (and temperatures), along with the accompanying analysis, confirm that the boundary layer in the Panel Test Facility flow is transitional at certain arc-heater conditions.
C1 [Goekcen, Tahir; Alunni, Antonella I.] NASA, Ames Res Ctr, ERC Inc, Moffett Field, CA 94035 USA.
RP Gokcen, T (reprint author), NASA, Ames Res Ctr, ERC Inc, MS 230-2, Moffett Field, CA 94035 USA.
NR 18
TC 0
Z9 0
U1 1
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
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 JUL-SEP
PY 2013
VL 27
IS 3
BP 549
EP 562
DI 10.2514/1.T3984
PG 14
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 187FG
UT WOS:000322101700021
ER
PT J
AU Hahn, PV
Frendi, A
AF Hahn, Philip V.
Frendi, Abdelkader
TI Interaction of Three-Dimensional Protuberances with a Supersonic
Turbulent Boundary Layer
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 18th AIAA/CEAS Aeroacoustics Conference / 33rd AIAA Aeroacoustics
Conference
CY JUN 04-06, 2012
CL Colorado Springs, CO
SP AIAA, CEAS
ID WALL-PRESSURE-FLUCTUATIONS; FREQUENCY SPECTRUM; CHANNEL FLOW; NUMBER;
FIELD; MODEL
AB A comprehensive computational fluid dynamics study of the surface-pressure fluctuations induced by a cylindrical protuberance in a supersonic turbulent boundary layer is presented. The effects of two important parameters on the surface-pressure fluctuations are investigated: protuberance height to boundary-layer thickness and surface curvature. The turbulent boundary layer is modeled using a hybrid Reynolds-averaged Navier-Stokes and large-eddy-simulation approach known as detached-eddy simulation. At first extensive comparisons to experimental data for the surface-pressure coefficient and the unsteady surface-pressure coefficient were performed. Results from our computational-fluid-dynamics computations compared well to the experimental data in the wake region downstream of the protuberance and in the vicinity of the protuberance at other locations. Increasing the protuberance height relative to the boundary-layer thickness resulted in higher sound-pressure levels on the surface. In addition, the surface-pressure fluctuation showed more coherence in the spanwise direction ahead of the protuberance and immediately downstream of it. Increasing the surface curvature lowered the sound-pressure levels on the surface and resulted in stretched coherent structures in the spanwise direction. Convection velocities of the turbulent structures increased away from the protuberance and were in agreement with published literature.
C1 [Hahn, Philip V.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35811 USA.
[Frendi, Abdelkader] Univ Alabama, Huntsville, AL 35899 USA.
RP Hahn, PV (reprint author), Blue Origin, Kent, WA 98032 USA.
NR 32
TC 3
Z9 3
U1 0
U2 5
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 JUL
PY 2013
VL 51
IS 7
BP 1657
EP 1666
DI 10.2514/1.J052101
PG 10
WC Engineering, Aerospace
SC Engineering
GA 181PL
UT WOS:000321680900011
ER
PT J
AU Kless, JE
Aftosmis, MJ
Ning, SA
Nemec, M
AF Kless, James E.
Aftosmis, Michael J.
Ning, S. Andrew
Nemec, Marian
TI Inviscid Analysis of Extended-Formation Flight
SO AIAA JOURNAL
LA English
DT Article
AB Flying airplanes in extended formations, with separation distances of tens of wingspans, significantly improves safety while maintaining most of the fuel savings achieved in close formations. The present study investigates the impact of roll trim and compressibility at a fixed lift coefficient on the benefits of extended-formation flight. An Euler solver with adjoint-based mesh refinement combined with a wake propagation model is used to analyze a two-body echelon formation at a separation distance of 30 spans. Two geometries are examined: a simple wing and a wing-body geometry. Energy savings, quantified by both formation drag fraction and span efficiency factor, are investigated at subsonic and transonic speeds for a matrix of vortex locations. The results show that, at fixed lift and trimmed for roll, the optimal location of vortex impingement is about 10% inboard of the trailing airplane's wing tip. Interestingly, the improvement in drag fraction is relatively robust in the vicinity of the optimal position. Over 90% of energy benefits can be obtained with a 5% variation in vertical and 10% variation in spanwise positions. Control surface deflections required to achieve roll trim reduce the benefits of formation flight by 3-5% at subsonic speeds and 9-11% at transonic speeds. Overall, simulations show peak induced drag saving for the trail aircraft are 54% in subsonic flow and 35% in transonic flow while accounting for trim.
C1 [Kless, James E.; Nemec, Marian] Sci & Technol Corp, NASA, Ames Supercomp Div, Moffett Field, CA 94035 USA.
[Aftosmis, Michael J.] NASA, Ames Res Ctr, Ames Supercomp Div, Moffett Field, CA 94035 USA.
[Ning, S. Andrew] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
RP Kless, JE (reprint author), Sci & Technol Corp, NASA, Ames Supercomp Div, Moffett Field, CA 94035 USA.
EM james.kless-1@nasa.gov; michael.aftosmis@nasa.gov; aning@stanford.edu;
marian.nemec@nasa.gov
OI Ning, Andrew/0000-0003-2190-823X
FU NASA Ames Research Center [NNA10DF26C]; Subsonic Fixed Wing Project of
NASA's Fundamental Aeronautics Program
FX This work was supported by the NASA Ames Research Center contract
NNA10DF26C, and the Subsonic Fixed Wing Project of NASA's Fundamental
Aeronautics Program. Marsha Berger contributed significant time and
effort into enabling anisotropic streamwise Cartesian meshing, for which
the authors are extremely thankful.
NR 19
TC 10
Z9 11
U1 0
U2 6
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 JUL
PY 2013
VL 51
IS 7
BP 1703
EP 1715
DI 10.2514/1.J052224
PG 13
WC Engineering, Aerospace
SC Engineering
GA 181PL
UT WOS:000321680900016
ER
PT J
AU Balla, RJ
AF Balla, R. Jeffrey
TI Iodine Tagging Velocimetry in a Mach 10 Wake
SO AIAA JOURNAL
LA English
DT Article
ID DENSITY-MEASUREMENTS; FLUORESCENCE; I-2; AIR
C1 NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA.
RP Balla, RJ (reprint author), NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, MS 493, Hampton, VA 23681 USA.
EM robert.j.balla@nasa.gov
NR 11
TC 4
Z9 4
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 JUL
PY 2013
VL 51
IS 7
BP 1783
EP 1786
DI 10.2514/1.J052416
PG 4
WC Engineering, Aerospace
SC Engineering
GA 181PL
UT WOS:000321680900024
ER
PT J
AU Ziolkowski, LA
Wierzchos, J
Davila, AF
Slater, GF
AF Ziolkowski, Lori A.
Wierzchos, Jacek
Davila, Alfonso F.
Slater, Gregory F.
TI Radiocarbon Evidence of Active Endolithic Microbial Communities in the
Hyperarid Core of the Atacama Desert
SO ASTROBIOLOGY
LA English
DT Article
DE Endoliths; Extremophile; Carbon isotopes; Radiocarbon; Lipids
ID CARBON-SOURCES; LIFE; SEDIMENTS; MARS; FRACTIONATION; LIPIDS; HALITE;
C-14; CO2; SUBSTRATE
AB The hyperarid core of the Atacama Desert is one of the driest and most inhospitable places on Earth, where life is most commonly found in the interior of rocks (i.e., endolithic habitats). Due to the extreme dryness, microbial activity in these habitats is expected to be low; however, the rate of carbon cycling within these microbial communities remains unknown. We address this issue by characterizing the isotopic composition (C-13 and C-14) of phospholipid fatty acids (PLFA) and glycolipid fatty acids (GLFA) in colonized rocks from four different sites inside the hyperarid core. delta C-13 results suggest that autotrophy and/or quantitative conversion of organic matter to CO2 are the dominant processes occurring with the rock. Most Delta C-14 signatures of PLFA and GLFA were consistent with modern atmospheric CO2, indicating that endoliths are using atmospheric carbon as a primary carbon source and are also cycling carbon quickly. However, at one site the PLFA contained C-14 from atmospheric nuclear weapons testing that occurred during the 1950s and 1960s, indicating a decadal rate of carbon cycling. At the driest site (Yungay), based on the relative abundance and C-14 content of GLFA and PLFA, there was evidence of possible preservation. Hence, in low-moisture conditions, glycolipids may persist while phospholipids are preferentially hydrolyzed.
C1 [Ziolkowski, Lori A.; Slater, Gregory F.] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON L8S 4L8, Canada.
[Wierzchos, Jacek] MNCN CSIC, Museo Nacl Ciencias Nat, Madrid, Spain.
[Davila, Alfonso F.] NASA Ames Res Ctr, Moffett Field, CA USA.
RP Ziolkowski, LA (reprint author), McMaster Univ, Sch Geog & Earth Sci, GSB 322A,1280 Main St West, Hamilton, ON L8S 4L8, Canada.
EM lorized@gmail.com
RI Ziolkowski, Lori/C-6752-2012
OI Ziolkowski, Lori/0000-0002-1799-385X
FU Canadian Astrobiology Training Program; McMaster University Origins
Institute; Natural Science and Engineering Council grant [288309-09];
NASA Exobiology Program; Spanish Ministry of Science and Innovation
[CGL2010-16004]
FX Jennie Kirby, Martin Knyf, and Sheila Griffin for technical assistance.
Funding to L.A.Z. from the Canadian Astrobiology Training Program and
McMaster University Origins Institute. Funding to G.F.S. from Natural
Science and Engineering Council grant 288309-09. Funding to A.F.D. from
the NASA Exobiology Program. Funding to J.W. from grant CGL2010-16004
from the Spanish Ministry of Science and Innovation. Two anonymous
reviewers and Dr. Sherry Cady for providing helpful suggestions that
improved this manuscript.
NR 49
TC 12
Z9 13
U1 6
U2 45
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 JUL
PY 2013
VL 13
IS 7
BP 607
EP 616
DI 10.1089/ast.2012.0854
PG 10
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 184NA
UT WOS:000321896100002
PM 23848470
ER
PT J
AU Abbey, W
Salas, E
Bhartia, R
Beegle, LW
AF Abbey, William
Salas, Everett
Bhartia, Rohit
Beegle, Luther W.
TI The Mojave Vadose Zone: A Subsurface Biosphere Analogue for Mars
SO ASTROBIOLOGY
LA English
DT Article
DE Mars; Search for extraterrestrial life; Evolution and distribution of
life; Mars analogues on Earth
ID SUBSEAFLOOR MICROBIAL-CELLS; LANDSCAPE EVOLUTION; UNSATURATED ZONE;
NORTHERN PLAINS; CO2 PRODUCTION; SOIL PROFILES; DESERT SOIL; WATER;
SURFACE; ICE
AB If life ever evolved on the surface of Mars, it is unlikely that it would still survive there today, but as Mars evolved from a wet planet to an arid one, the subsurface environment may have presented a refuge from increasingly hostile surface conditions. Since the last glacial maximum, the Mojave Desert has experienced a similar shift from a wet to a dry environment, giving us the opportunity to study here on Earth how subsurface ecosystems in an arid environment adapt to increasingly barren surface conditions. In this paper, we advocate studying the vadose zone ecosystem of the Mojave Desert as an analogue for possible subsurface biospheres on Mars. We also describe several examples of Mars-like terrain found in the Mojave region and discuss ecological insights that might be gained by a thorough examination of the vadose zone in these specific terrains. Examples described include distributary fans (deltas, alluvial fans, etc.), paleosols overlain by basaltic lava flows, and evaporite deposits.
C1 [Abbey, William; Salas, Everett; Bhartia, Rohit; Beegle, Luther W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Beegle, LW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-601, Pasadena, CA 91109 USA.
EM Luther.Beegle@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract from the National
Aeronautics and Space Administration. The authors would like to thank
Chris McKay (NASA Ames), Norm Sleep (Stanford), and an anonymous
reviewer for their thoughtful critiques, as well as Ann Copin and Mickey
Honchell of JPL Library Services for their timely help with gathering
references.
NR 112
TC 1
Z9 1
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
EI 1557-8070
J9 ASTROBIOLOGY
JI Astrobiology
PD JUL
PY 2013
VL 13
IS 7
BP 637
EP 646
DI 10.1089/ast.2012.0948
PG 10
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 184NA
UT WOS:000321896100005
PM 23848498
ER
PT J
AU Gerakines, PA
Hudson, RL
AF Gerakines, Perry A.
Hudson, Reggie L.
TI Glycine's Radiolytic Destruction in Ices: First in situ Laboratory
Measurements for Mars
SO ASTROBIOLOGY
LA English
DT Article
DE Mars; Ice; Radiolysis; In situ measurement; Laboratory investigations
ID AMINO-ACIDS; IONIZING-RADIATION; MARTIAN SURFACE; UV PHOTOLYSIS;
METEORITE; PHOTOSTABILITY; ANALOGS
AB We report new laboratory studies of the radiation-induced destruction of glycine-containing ices for a range of temperatures and compositions that allow extrapolation to martian conditions. In situ infrared spectroscopy was used to study glycine decay rates as a function of temperature (from 15 to 280 K) and initial glycine concentrations in six mixtures whose compositions ranged from dry glycine to H2O+glycine (300:1). Results are presented in several systems of units, with cautions concerning their use. The half-life of glycine under the surface of Mars is estimated as an extrapolation of this data set to martian conditions, and trends in decay rates are described as are applications to Mars' near-surface chemistry.
C1 [Gerakines, Perry A.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
RP Gerakines, PA (reprint author), NASA, Goddard Space Flight Ctr, Code 691-1, Greenbelt, MD 20771 USA.
EM perry.a.gerakines@nasa.gov
RI Gerakines, Perry/D-2226-2012
OI Gerakines, Perry/0000-0002-9667-5904
FU NASA Astrobiology Institute; NASA's Exobiology Program
FX Marla Moore and Jan-Luca Bell contributed some of the early measurements
of glycine and H2O+glycine used in this study. Mark Loeffler
is recognized for substantial assistance in day-to-day operations of the
equipment in our laboratory. Zan Peeters constructed and tested the
sublimation oven we used. The authors wish to acknowledge support from
the NASA Astrobiology Institute through a grant to the Goddard Center
for Astrobiology. The support of NASA's Exobiology Program also is
gratefully acknowledged. Finally, we thank Steve Brown, Tom Ward, and
Eugene Gerashchenko, members of the Radiation Effects Facility at the
NASA Goddard Space Flight Center, for operation of the proton
accelerator.
NR 26
TC 16
Z9 16
U1 1
U2 18
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 JUL
PY 2013
VL 13
IS 7
BP 647
EP 655
DI 10.1089/ast.2012.0943
PG 9
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 184NA
UT WOS:000321896100006
PM 23848469
ER
PT J
AU Ackermann, M
Ajello, M
Albert, A
Allafort, A
Antolini, E
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Blandford, RD
Bloom, ED
Bonamente, E
Bottacini, E
Bouvier, A
Brandt, TJ
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Cavazzuti, E
Cecchi, C
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cutini, S
Dalton, M
D'Ammando, F
de Angelis, A
de Palma, F
Dermer, CD
Di Venere, L
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Franckowiak, A
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grondin, MH
Grove, JE
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashida, M
Hays, E
Hewitt, J
Hill, AB
Horan, D
Hou, X
Hughes, RE
Inoue, Y
Jackson, MS
Jogler, T
Johannesson, G
Johnson, WN
Kamae, T
Kataoka, J
Kawano, T
Knoedlseder, J
Kuss, M
Lande, J
Larsson, S
Latronico, L
Lemoine-Goumard, M
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Mayer, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nemmen, R
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Panetta, JH
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Romoli, C
Roth, M
Sanchez-Conde, M
Scargle, JD
Schulz, A
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Suson, DJ
Takahashi, H
Takeuchi, Y
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Tronconi, V
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Winer, BL
Wood, KS
Wood, M
Yang, Z
AF Ackermann, M.
Ajello, M.
Albert, A.
Allafort, A.
Antolini, E.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Bottacini, E.
Bouvier, A.
Brandt, T. J.
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.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
Dalton, M.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Dermer, C. D.
Di Venere, L.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grondin, M-H.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashida, M.
Hays, E.
Hewitt, J.
Hill, A. B.
Horan, D.
Hou, X.
Hughes, R. E.
Inoue, Y.
Jackson, M. S.
Jogler, T.
Johannesson, G.
Johnson, W. N.
Kamae, T.
Kataoka, J.
Kawano, T.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Latronico, L.
Lemoine-Goumard, M.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nemmen, R.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Panetta, J. H.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Romoli, C.
Roth, M.
Sanchez-Conde, M.
Scargle, J. D.
Schulz, A.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Suson, D. J.
Takahashi, H.
Takeuchi, Y.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Tronconi, V.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Winer, B. L.
Wood, K. S.
Wood, M.
Yang, Z.
TI THE FERMI ALL-SKY VARIABILITY ANALYSIS: A LIST OF FLARING GAMMA-RAY
SOURCES AND THE SEARCH FOR TRANSIENTS IN OUR GALAXY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; BL Lacertae objects: general; catalogs; galaxies:
active; stars: flare; surveys
ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; ETA-CARINAE; CRAB-NEBULA;
SOURCE CATALOG; LS 5039; EMISSION; BINARY; DISCOVERY; HESS
AB In this paper, we present the Fermi All-sky Variability Analysis (FAVA), a tool to systematically study the variability of the gamma-ray sky measured by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. For each direction on the sky, FAVA compares the number of gamma-rays observed in a given time window to the number of gamma-rays expected for the average emission detected from that direction. This method is used in weekly time intervals to derive a list of 215 flaring gamma-ray sources. We proceed to discuss the 27 sources found at Galactic latitudes smaller than 10 degrees and show that, despite their low latitudes, most of them are likely of extragalactic origin.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Albert, A.; Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA.
[Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Inoue, Y.; Jogler, T.; Kamae, T.; 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.; Sanchez-Conde, M.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA.
[Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Inoue, Y.; Jogler, T.; Kamae, T.; 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.; Sanchez-Conde, M.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Grenier, I. A.] Univ Paris Diderot, Lab AIM, CEA IRFU, CNRS,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.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.; Romoli, C.; Tronconi, V.] 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.; Razzano, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Bouvier, A.; Razzano, M.] 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.; Horan, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, 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.
[Chekhtman, A.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA.
[Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy.
[Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS IN2P3, Montpellier, France.
[Conrad, J.; Larsson, S.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[Dalton, M.; Hou, X.; Lemoine-Goumard, M.; Lott, B.] Univ Bordeaux 1, CNRS IN2p3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Grp Collegato Udine, Ist Nazl Fis Nucl, I-33100 Udine, Italy.
[Fukazawa, Y.; Hanabata, Y.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Grondin, M-H.; Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Grondin, M-H.; Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Jackson, M. S.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kataoka, J.; Takeuchi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[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.
[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.
[Perkins, J. S.] Univ Maryland Baltimore Cty, 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.
[Scargle, J. D.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] Inst Catalana Recerca & Estudis Avancats ICREA, Barcelona, Spain.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Conrad, J.] Royal Swedish Acad Sci, Stockholm, Sweden.
[Troja, E.] NASA, Postdoctoral Program, Washington, DC USA.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM allafort@stanford.edu; rolf.buehler@desy.de
RI Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Di Venere,
Leonardo/C-7619-2017; Rando, Riccardo/M-7179-2013; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016; Hays, Elizabeth/D-3257-2012;
Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen,
Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; 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
OI Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti,
monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852;
Gasparrini, Dario/0000-0002-5064-9495; Baldini,
Luca/0000-0002-9785-7726; Torres, Diego/0000-0002-1522-9065; Di Venere,
Leonardo/0000-0003-0703-824X; Inoue, Yoshiyuki/0000-0002-7272-1136;
Giordano, Francesco/0000-0002-8651-2394; De Angelis,
Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018;
Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864;
Rando, Riccardo/0000-0001-6992-818X; Hill, Adam/0000-0003-3470-4834;
Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577;
Mazziotta, Mario /0000-0001-9325-4672; Reimer, Olaf/0000-0001-6953-1385;
Morselli, Aldo/0000-0002-7704-9553; 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
FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes
Spatiales in France
FX Rolf Buhler acknowledges generous support from the Fermi guest
investigator program. 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.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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ER
PT J
AU Debes, JH
Jang-Condell, H
Weinberger, AJ
Roberge, A
Schneider, G
AF Debes, John H.
Jang-Condell, Hannah
Weinberger, Alycia J.
Roberge, Aki
Schneider, Glenn
TI THE 0.5-2.22 mu m SCATTERED LIGHT SPECTRUM OF THE DISK AROUND TW Hya:
DETECTION OF A PARTIALLY FILLED DISK GAP AT 80 AU
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planet-disk interactions; protoplanetary disks; radiative transfer;
stars: individual (TW Hya)
ID PROTOPLANETARY DISKS; CIRCUMSTELLAR DISK; ACCRETION DISKS; HYDRAE
ASSOCIATION; YOUNG OBJECTS; DUST EMISSION; EFFECTIVE TEMPERATURES;
SUBMILLIMETER ARRAY; PLANETARY SYSTEM; MAGNETIC-FIELD
AB We present a 0.5-2.2 mu m scattered light spectrum of the circumstellar disk around TW Hya from a combination of spatially resolved Hubble Space Telescope STIS spectroscopy and NICMOS coronagraphic images of the disk. We investigate the morphology of the disk at distances >40 AU over this wide range of wavelengths, and identify the presence of a depression in surface brightness at similar to 80 AU that could be caused by a gap in the disk. Additionally, we quantify the surface brightness, azimuthal symmetry, and spectral character of the disk as a function of radius. Our analysis shows that the scattering efficiency of the dust is largely neutral to blue over the observed wavelengths. We model the disk as a steady alpha-disk with an ad hoc gap structure. The thermal properties of the disk are self-consistently calculated using a three-dimensional radiative transfer code that uses ray tracing to model the heating of the disk interior and scattered light images. We find a good fit to the data over a wide range of distances from the star if we use a model disk with a partially filled gap of 30% depth at 80 AU and with a self-similar truncation knee at 100 AU. The origin of the gap is unclear, but it could arise from a transition in the nature of the disk's dust composition or the presence of a planetary companion. Based on scalings to previous hydrodynamic simulations of gap-opening criteria for embedded proto-planets, we estimate that a planetary companion forming the gap could have a mass between 6 and 28M(circle plus).
C1 [Debes, John H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Jang-Condell, Hannah] Univ Wyoming, Laramie, WY 82071 USA.
[Weinberger, Alycia J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Roberge, Aki] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schneider, Glenn] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Debes, JH (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RI Roberge, Aki/D-2782-2012;
OI Roberge, Aki/0000-0002-2989-3725; Jang-Condell,
Hannah/0000-0002-7639-1322
FU NASA through a grant from the Space Telescope Science Institute;
Association of Universities for Research in Astronomy, Inc., under NASA
[NAS 5-26555]; NASA Astrophysics Theory Program [NNX12AD43G]; Michelson
Fellowship Program; Jet Propulsion Laboratory (JPL); NASA
FX The authors thank the anonymous referee for several helpful suggestions,
including a suggestion to investigate the spectral type of TW Hya. We
also thank Ted Bergin, Diego Munoz, and Ruobing Dong for enlightening
conversations on alternative origins for disk gaps, as well as A.
Meredith Hughes for discussions of TW Hya CO data. Support for program
10167 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.
H.J.-C. acknowledges support from the NASA Astrophysics Theory Program
through grant NNX12AD43G, and the Michelson Fellowship Program under
contract with the Jet Propulsion Laboratory (JPL) funded by NASA. JPL is
managed for NASA by the California Institute of Technology.
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ER
PT J
AU Farhang, M
Bond, JR
Dore, O
Netterfield, CB
AF Farhang, M.
Bond, J. R.
Dore, O.
Netterfield, C. B.
TI PRIMORDIAL GRAVITATIONAL WAVE DETECTABILITY WITH DEEP SMALL-SKY COSMIC
MICROWAVE BACKGROUND EXPERIMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmological parameters; cosmology: theory;
methods: numerical
ID PROBE WMAP OBSERVATIONS; POLARIZATION POWER SPECTRA; INFLATIONARY
UNIVERSE; COSMOLOGICAL PARAMETERS; DENSITY PERTURBATIONS; 2003 FLIGHT;
FOREGROUND EMISSION; ANISOTROPY; CMB; TEMPERATURE
AB We use the Bayesian estimation on direct T-Q-U cosmic microwave background (CMB) polarization maps to forecast errors on the tensor-to-scalar power ratio r, and hence on primordial gravitational waves, as a function of sky coverage f(sky). This map-based likelihood filters the information in the pixel-pixel space into the optimal combinations needed for r detection for cut skies, providing enhanced information over a first-step linear separation into a combination of E, B, and mixed modes, and ignoring the latter. With current computational power and for typical resolutions appropriate for r detection, the large matrix inversions required are accurate and fast. Our simulations explore two classes of experiments, with differing bolometric detector numbers, sensitivities, and observational strategies. One is motivated by a long duration balloon experiment like Spider, with pixel noise proportional to root f(sky) for a specified observing period. This analysis also applies to ground-based array experiments. We find that, in the absence of systematic effects and foregrounds, an experiment with Spider-like noise concentrating on f(sky) similar to 0.02-0.2 could place a 2 sigma(r) approximate to 0.014 boundary (similar to 95% confidence level), which rises to 0.02 with an l-dependent foreground residual left over from an assumed efficient component separation. We contrast this with a Planck-like fixed instrumental noise as f(sky) varies, which gives a Galaxy-masked (f(sky) = 0.75) 2 sigma(r) approximate to 0.015, rising to approximate to 0.05 with the foreground residuals. Using as the figure of merit the (marginalized) one-dimensional Shannon entropy of r, taken relative to the first 2003 WMAP CMB-only constraint, gives -2.7 bits from the 2012 WMAP9+ACT+SPT+LSS data, and forecasts of -6 bits from Spider (+ Planck); this compares with up to -11 bits for CMBPol, COrE, and PIXIE post-Planck satellites and -13 bits for a perfectly noiseless cosmic variance limited experiment. We thus confirm the wisdom of the current strategy for r detection of deeply probed patches covering the f(sky) minimum-error trough with balloon and ground experiments.
C1 [Farhang, M.; Bond, J. R.; Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Farhang, M.; Dore, O.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Dore, O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dore, O.] CALTECH, Pasadena, CA 91125 USA.
[Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
RP Farhang, M (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George, Toronto, ON M5S 3H4, Canada.
FU NSERC; Canadian Institute for Advanced Research; Canadian Space Agency
FX We thank our many Spider, ABS, and Planck collaborators for many
stimulating discussions about the experimental assault on CMB tensor
mode detection. We thank William C. Jones for his helpful comments on
the text. We thank Marc Antoine Miville Deschenes for advice and aid on
foregrounds. Support from NSERC, the Canadian Institute for Advanced
Research, and the Canadian Space Agency (for PlanckHFI and Spider work)
is gratefully acknowledged. 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 large matrix computations were performed using the
SciNET facility at the University of Toronto. Some of the results in
this paper have been derived using the HEALPix package (Gorski et al.
2005), http://healpix.jpl.nasa.gov.
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EI 1538-4357
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ER
PT J
AU Lin, YT
Brodwin, M
Gonzalez, AH
Bode, P
Eisenhardt, PRM
Stanford, SA
Vikhlinin, A
AF Lin, Yen-Ting
Brodwin, Mark
Gonzalez, Anthony H.
Bode, Paul
Eisenhardt, Peter R. M.
Stanford, S. A.
Vikhlinin, Alexey
TI THE STELLAR MASS GROWTH OF BRIGHTEST CLUSTER GALAXIES IN THE IRAC
SHALLOW CLUSTER SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: elliptical and lenticular, cD;
galaxies: evolution; galaxies: luminosity function, mass function
ID X-RAY DATA; LUMINOSITY FUNCTION; EVOLUTION; SIMULATIONS; POPULATION;
COSMOLOGY; REDSHIFT; SCATTER
AB The details of the stellar mass assembly of brightest cluster galaxies (BCGs) remain an unresolved problem in galaxy formation. We have developed a novel approach that allows us to construct a sample of clusters that form an evolutionary sequence, and have applied it to the Spitzer IRAC Shallow Cluster Survey (ISCS) to examine the evolution of BCGs in progenitors of present-day clusters with mass of (2.5-4.5) x 10(14) M-circle dot. We follow the cluster mass growth history extracted from a high resolution cosmological simulation, and then use an empirical method that infers the cluster mass based on the ranking of cluster luminosity to select high-z clusters of appropriate mass from ISCS to be progenitors of the given set of z = 0 clusters. We find that, between z = 1.5 and 0.5, the BCGs have grown in stellar mass by a factor of 2.3, which is well-matched by the predictions from a state-of-the-art semi-analytic model. Below z = 0.5 we see hints of differences in behavior between the model and observation.
C1 [Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Lin, Yen-Ting] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, Kashiwa, Chiba, Japan.
[Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Bode, Paul] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lin, YT (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
EM ytl@asiaa.sinica.edu.tw
FU National Science Council [NSC 102-2112-M-001-001-MY3]; WPI Research
Center Initiative, MEXT, Japan; National Science Foundation
[AST-0707731, AST-0908292]; Pittsburgh Supercomputing Center
[AST070015]; NASA
FX We thank Laurie Shaw and Antonio Vale for constructing the merger trees
used in this work. We are grateful to the anonymous referee for a report
that improved the paper. Y.T.L. thanks Gabriella De Lucia, David
Spergel, and Jerry Ostriker for helpful discussions, and I. H. for
constant encouragement. Y.T.L. acknowledges supports from the National
Science Council grant NSC 102-2112-M-001-001-MY3, as well as WPI
Research Center Initiative, MEXT, Japan, during the course of this work.
This work was supported by National Science Foundation grants
AST-0707731 and AST-0908292. Computer simulations and analysis were
supported by the NSF through resources provided by XSEDE and the
Pittsburgh Supercomputing Center, under grant AST070015; computations
were also performed at the TIGRESS high performance computer center at
Princeton University, which is jointly supported by the Princeton
Institute for Computational Science and Engineering and the Princeton
University Office of Information Technology. This work is based in part
on observations made with the Spitzer Space Telescope, which is operated
by the JPL/Caltech under a contract with NASA. This publication makes
use of data products from WISE, a joint project of UCLA and JPL/Caltech,
funded by NASA. The Millennium Simulation databases were constructed as
part of the activities of the GAVO.
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SC Astronomy & Astrophysics
GA 176AD
UT WOS:000321274200061
ER
PT J
AU Martinez-Sykora, J
De Pontieu, B
Leenaarts, J
Pereira, TMD
Carlsson, M
Hansteen, V
Stern, JV
Tian, H
McIntosh, SW
van der Voort, LR
AF Martinez-Sykora, Juan
De Pontieu, Bart
Leenaarts, Jorrit
Pereira, Tiago M. D.
Carlsson, Mats
Hansteen, Viggo
Stern, Julie V.
Tian, Hui
McIntosh, Scott W.
van der Voort, Luc Rouppe
TI A DETAILED COMPARISON BETWEEN THE OBSERVED AND SYNTHESIZED PROPERTIES OF
A SIMULATED TYPE II SPICULE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); radiative transfer; Sun: atmosphere; Sun:
chromosphere; Sun: corona; Sun: transition region
ID HIGH-RESOLUTION OBSERVATIONS; FLUX TUBE EMERGENCE; TRANSITION REGION;
SOLAR CORONA; EXTREME-ULTRAVIOLET; ALFVENIC WAVES; MAGNETOHYDRODYNAMIC
SIMULATIONS; NONEQUILIBRIUM IONIZATION; NUMERICAL SIMULATIONS; HYDROGEN
IONIZATION
AB We have performed a three-dimensional radiative MHD simulation of the solar atmosphere. This simulation shows a jet-like feature that shows similarities to the type II spicules observed for the first time with Hinode's Solar Optical Telescope. Rapid blueshifted events (RBEs) on the solar disk are associated with these spicules. Observational results suggest they may contribute significantly in supplying the corona with hot plasma. We perform a detailed comparison of the properties of the simulated jet with those of type II spicules (observed with Hinode) and RBEs (with ground-based instruments). We analyze a wide variety of synthetic emission and absorption lines from the simulations including chromospheric (Ca II 8542 angstrom, Ca II H, and H alpha) to transition region and coronal temperatures (10,000 K to several million K). We compare their synthetic intensities, line profiles, Doppler shifts, line widths, and asymmetries with observations from Hinode/SOT and EIS, SOHO/SUMER, the Swedish 1 m Solar Telescope, and SDO/AIA. Many properties of the synthetic observables resemble the observations, and we describe in detail the physical processes that lead to these observables. Detailed analysis of the synthetic observables provides insight into how observations should be analyzed to derive information about physical variables in such a dynamic event. For example, we find that line-of-sight superposition in the optically thin atmosphere requires the combination of Doppler shifts and spectral line asymmetry to determine the velocity in the jet. In our simulated type II spicule, the lifetime of the asymmetry of the transition region lines is shorter than that of the coronal lines. Other properties differ from the observations, especially in the chromospheric lines. The mass density of the part of the spicule with a chromospheric temperature is too low to produce significant opacity in chromospheric lines. The synthetic Ca II 8542 angstrom and H alpha profiles therefore do not show signal resembling RBEs. These and other discrepancies are described in detail, and we discuss which mechanisms and physical processes may need to be included in the MHD simulations to mimic the thermodynamic processes of the chromosphere and corona, in particular to reproduce type II spicules.
C1 [Martinez-Sykora, Juan; De Pontieu, Bart; Pereira, Tiago M. D.; Stern, Julie V.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Martinez-Sykora, Juan; Leenaarts, Jorrit; Carlsson, Mats; Hansteen, Viggo; van der Voort, Luc Rouppe] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Martinez-Sykora, Juan] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Pereira, Tiago M. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Tian, Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[McIntosh, Scott W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
RP Martinez-Sykora, J (reprint author), Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
EM j.m.sykora@astro.uio.no
RI Pereira, Tiago/G-4079-2014;
OI Pereira, Tiago/0000-0003-4747-4329; Leenaarts,
Jorrit/0000-0003-4936-4211
FU European Research Council under the European Union's Seventh Framework
Programme/ERC [291058]; NASA [NNX08AH45G, NNX08BA99G, NNX11AN98G,
NNM07AA01C, NNG09FA40C]; NASA Post-doctoral Program at Ames Research
Center [NNH06CC03B]; Lockheed-Martin [8100002705]; High End Computing
(HEC) division of NASA [s1061]; Research Council of Norway [170935/V30];
Programme for Supercomputing
FX The research leading to these results has received funding from the
European Research Council under the European Union's Seventh Framework
Programme (FP7/2007-2013)/ERC grant agreement No. 291058. We gratefully
acknowledge support by NASA grants NNX08AH45G, NNX08BA99G, NNX11AN98G,
NNM07AA01C (Hinode), and NNG09FA40C (IRIS). T.M.D.P.'s research was
supported by the NASA Post-doctoral Program at Ames Research Center
through Contract No. NNH06CC03B. H.T.'s work at CfA is supported under
contract 8100002705 from Lockheed-Martin to SAO. The 3D simulation and
synthesis have been run on clusters from the Notur project, and the
Pleiades cluster through the computing project s1061 from the High End
Computing (HEC) division of NASA. We thankfully acknowledge the computer
and super-computer resources of the Research Council of Norway through
grant 170935/V30 and through grants of computing time from the Programme
for Supercomputing. The Swedish 1 m Solar Telescope is operated by the
Institute for Solar Physics of the Royal Swedish Academy of Sciences in
the Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofisica de Canarias.
NR 74
TC 8
Z9 8
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2013
VL 771
IS 1
AR 66
DI 10.1088/0004-637X/771/1/66
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176AD
UT WOS:000321274200066
ER
PT J
AU Mukadam, AS
Bischoff-Kim, A
Fraser, O
Corsico, AH
Montgomery, MH
Kepler, SO
Romero, AD
Winget, DE
Hermes, JJ
Riecken, TS
Kronberg, ME
Winget, KI
Falcon, RE
Chandler, DW
Kuehne, JW
Sullivan, DJ
Reaves, D
von Hippel, T
Mullally, F
Shipman, H
Thompson, SE
Silvestri, NM
Hynes, RI
AF Mukadam, Anjum S.
Bischoff-Kim, Agnes
Fraser, Oliver
Corsico, A. H.
Montgomery, M. H.
Kepler, S. O.
Romero, A. D.
Winget, D. E.
Hermes, J. J.
Riecken, T. S.
Kronberg, M. E.
Winget, K. I.
Falcon, Ross E.
Chandler, D. W.
Kuehne, J. W.
Sullivan, D. J.
Reaves, D.
von Hippel, T.
Mullally, F.
Shipman, H.
Thompson, S. E.
Silvestri, N. M.
Hynes, R. I.
TI MEASURING THE EVOLUTIONARY RATE OF COOLING OF ZZ Ceti
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: evolution; stars: individual (ZZ Ceti, R548); stars: oscillations
(including pulsations); stars: variables: general; white dwarfs
ID PULSATING WHITE-DWARF; WHOLE EARTH TELESCOPE; INSTABILITY STRIP; PERIOD
CHANGE; DIFFERENTIAL ROTATION; MAGNETIC-FIELDS; TIME-SCALE; AXION MASS;
STARS; G117-B15A
AB We have finally measured the evolutionary rate of cooling of the pulsating hydrogen atmosphere (DA) white dwarf ZZ Ceti (Ross 548), as reflected by the drift rate of the 213.13260694 s period. Using 41 yr of time-series photometry from 1970 November to 2012 January, we determine the rate of change of this period with time to be dP/dt = (5.2 +/- 1.4) x 10(-15) s s(-1) employing the O - C method and (5.45 +/- 0.79) x 10(-15) s s(-1) using a direct nonlinear least squares fit to the entire lightcurve. We adopt the dP/dt obtained from the nonlinear least squares program as our final determination, but augment the corresponding uncertainty to a more realistic value, ultimately arriving at the measurement of dP/dt = (5.5 +/- 1.0) x 10(-15) s s(-1). After correcting for proper motion, the evolutionary rate of cooling of ZZ Ceti is computed to be (3.3 +/- 1.1) x 10(-15) s s(-1). This value is consistent within uncertainties with the measurement of (4.19 +/- 0.73) x 10(-15) s s(-1) for another similar pulsating DA white dwarf, G 117-B15A. Measuring the cooling rate of ZZ Ceti helps us refine our stellar structure and evolutionary models, as cooling depends mainly on the core composition and stellar mass. Calibrating white dwarf cooling curves with this measurement will reduce the theoretical uncertainties involved in white dwarf cosmochronometry. Should the 213.13 s period be trapped in the hydrogen envelope, then our determination of its drift rate compared to the expected evolutionary rate suggests an additional source of stellar cooling. Attributing the excess cooling to the emission of axions imposes a constraint on the mass of the hypothetical axion particle.
C1 [Mukadam, Anjum S.; Fraser, Oliver; Riecken, T. S.; Kronberg, M. E.; Silvestri, N. M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Mukadam, Anjum S.; Fraser, Oliver; Riecken, T. S.; Kronberg, M. E.; Silvestri, N. M.] Apache Point Observ, Sunspot, NM 88349 USA.
[Bischoff-Kim, Agnes] Georgia Coll & State Univ, Milledgeville, GA 31061 USA.
[Corsico, A. H.] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina.
[Corsico, A. H.] Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina.
[Montgomery, M. H.; Winget, D. E.; Hermes, J. J.; Winget, K. I.; Falcon, Ross E.; Reaves, D.] Univ Texas Austin, Dept Astron, Austin, TX 78759 USA.
[Montgomery, M. H.; Shipman, H.] Mt Cuba Observ, Delaware Asteroseism Res Ctr, Greenville, DE 19807 USA.
[Montgomery, M. H.; Winget, D. E.; Hermes, J. J.; Winget, K. I.; Falcon, Ross E.; Kuehne, J. W.; Reaves, D.] McDonald Observ, Ft Davis, TX 79734 USA.
[Kepler, S. O.; Romero, A. D.] Univ Fed Rio Grande do Sul, BR-91501970 Porto Alegre, RS, Brazil.
[Chandler, D. W.] Cent Texas Astron Soc, Meyer Observ, Temple, TX 76504 USA.
[Sullivan, D. J.] Victoria Univ Wellington, Wellington, New Zealand.
[von Hippel, T.] Embry Riddle Aeronaut Univ, Daytona Beach, FL 32114 USA.
[Mullally, F.; Thompson, S. E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Shipman, H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Hynes, R. I.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
RP Mukadam, AS (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA.
RI Kepler, S. O. /H-5901-2012; Romero, Alejandra/G-1644-2016
OI Kepler, S. O. /0000-0002-7470-5703;
FU NSF [AST-1008734, AST-0909107]; Norman Hackerman Advanced Research
Program [003658-0252-2009]
FX We gratefully thank the countless astronomers who observed this star
since 1970 and passed on the data that have made this measurement
possible. A. S. M. acknowledges NSF for the grant AST-1008734 that
provided funding for this project. M. H. M., D. E. W., and J.J.H.
acknowledge support from the NSF under grant AST-0909107 and the Norman
Hackerman Advanced Research Program under grant 003658-0252-2009. Based
on observations obtained with the Apache Point Observatory 3.5 m
telescope, which is owned and operated by the Astrophysical Research
Consortium.
NR 59
TC 9
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U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2013
VL 771
IS 1
AR 17
DI 10.1088/0004-637X/771/1/17
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176AD
UT WOS:000321274200017
ER
PT J
AU Rietmeijer, FJM
Nuth, JA
AF Rietmeijer, Frans J. M.
Nuth, Joseph A.
TI PETROLOGIC CONSTRAINTS ON AMORPHOUS AND CRYSTALLINE MAGNESIUM SILICATES:
DUST FORMATION AND EVOLUTION IN SELECTED HERBIG Ae/Be SYSTEMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; methods: laboratory; methods: observational;
protoplanetary disks; stars: variables: T Tauri, Herbig Ae/Be
ID METASTABLE EUTECTIC CONDENSATION; MIDINFRARED SPECTRAL EVOLUTION;
CIRCUMSTELLAR DUST; SOLID CONDENSATION; ISO SPECTROSCOPY;
INFRARED-SPECTRA; COMETARY DUST; HD 163296; AB AUR; MINERALOGY
AB The Infrared Space Observatory, Spitzer Space Telescope, and Herschel Space Observatory surveys provided a wealth of data on the Mg-silicate minerals (forsterite, enstatite), silica, and "amorphous silicates with olivine and pyroxene stoichiometry" around Herbig Ae/Be stars. These incredible findings do not resonate with the mainstream Earth Sciences because of (1) disconnecting "astronomical nomenclature" and the long existing mineralogical and petrologic terminology of minerals and amorphous materials, and (2) the fact that Earth scientists (formerly geologists) are bound by the "Principle of Actualism" that was put forward by James Hutton (1726-1797). This principle takes a process-oriented approach to understanding mineral and rock formation and evolution. This paper will (1) review and summarize the results of laboratory-based vapor phase condensation and thermal annealing experiments, (2) present the pathways of magnesiosilica condensates to Mg-silicate mineral (forsterite, enstatite) formation and processing, and (3) present mineralogical and petrologic implications of the properties and compositions of the infrared-observed crystalline and amorphous dust for the state of circumstellar disk evolution. That is, the IR-observation of smectite layer silicates in HD142527 suggests the break-up of asteroid-like parent bodies that had experienced aqueous alteration. We discuss the persistence of amorphous dust around some young stars and an ultrafast amorphous to crystalline dust transition in HD 163296 that leads to forsterite grains with numerous silica inclusions. These dust evolution processes to form forsterite, enstatite +/- tridymite could occur due to amorphous magnesiosilica dust precursors with a serpentine- or smectite-dehydroxylate composition.
C1 [Rietmeijer, Frans J. M.] 1 Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Nuth, Joseph A.] NASA, Astrochem Lab, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rietmeijer, FJM (reprint author), 1 Univ New Mexico, Dept Earth & Planetary Sci, MSC 03 2040, Albuquerque, NM 87131 USA.
EM fransjmr@unm.edu
FU NASA Cosmochemistry Program [NNX10AK28G]; NASA LARS Program
[NNX11AC36G]; NASA Exobiology Program
FX We are grateful for the unfortunately anonymous reviewer whose work
helped us to greatly improve our original submission. F.J.M.R. was
supported by grant NNX10AK28G (PI: J.A. Nuth) through the NASA
Cosmochemistry Program, and grant NNX11AC36G through the NASA LARS
Program. J.A.N. acknowledges the support of the NASA Exobiology Program.
NR 73
TC 4
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U1 1
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 JUL 1
PY 2013
VL 771
IS 1
AR 34
DI 10.1088/0004-637X/771/1/34
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176AD
UT WOS:000321274200034
ER
PT J
AU Roberge, A
Kamp, I
Montesinos, B
Dent, WRF
Meeus, G
Donaldson, JK
Olofsson, J
Moor, A
Augereau, JC
Howard, C
Eiroa, C
Thi, WF
Ardila, DR
Sandell, G
Woitke, P
AF Roberge, A.
Kamp, I.
Montesinos, B.
Dent, W. R. F.
Meeus, G.
Donaldson, J. K.
Olofsson, J.
Moor, A.
Augereau, J. -C.
Howard, C.
Eiroa, C.
Thi, W. -F.
Ardila, D. R.
Sandell, G.
Woitke, P.
TI HERSCHEL OBSERVATIONS OF GAS AND DUST IN THE UNUSUAL 49 Ceti DEBRIS DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; Kuiper belt: general; protoplanetary disks; stars:
individual (49 Ceti)
ID PICTORIS CIRCUMSTELLAR DISK; RADIATION THERMOCHEMICAL MODELS;
MAIN-SEQUENCE STARS; A-TYPE STARS; BETA-PICTORIS; PROTOPLANETARY DISCS;
PLANET FORMATION; MOLECULAR GAS; HERBIG AE/BE; EVOLUTION
AB We present far-IR/sub-mm imaging and spectroscopy of 49 Ceti, an unusual circumstellar disk around a nearby young A1V star. The system is famous for showing the dust properties of a debris disk, but the gas properties of a low-mass protoplanetary disk. The data were acquired with the Herschel Space Observatory PACS and SPIRE instruments, largely as part of the "Gas in Protoplanetary Systems" (GASPS) Open Time Key Programme. Disk dust emission is detected in images at 70, 160, 250, 350, and 500 mu m; 49 Cet is significantly extended in the 70 mu m image, spatially resolving the outer dust disk for the first time. Spectra covering small wavelength ranges centered on eight atomic and molecular emission lines were obtained, including [O I] 63 mu m and [C II] 158 mu m. The C II line was detected at the 5 sigma level-the first detection of atomic emission from the disk. No other emission lines were seen, despite the fact that the O I line is the brightest one observed in Herschel protoplanetary disk spectra. We present an estimate of the amount of circumstellar atomic gas implied by the C II emission. The new far-IR/sub-mm data fills in a large gap in the previous spectral energy distribution (SED) of 49 Cet. A simple model of the new SED confirms the two-component structure of the disk: warm inner dust and cold outer dust that produces most of the observed excess. Finally, we discuss preliminary thermochemical modeling of the 49 Cet gas/dust disk and our attempts to match several observational results simultaneously. Although we are not yet successful in doing so, our investigations shed light on the evolutionary status of the 49 Cet gas, which might not be primordial gas but rather secondary gas coming from comets.
C1 [Roberge, A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Kamp, I.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Montesinos, B.] Centro Astrobiol INTA CSIC, Dept Astrofis, E-28691 Madrid, Spain.
[Dent, W. R. F.] ALMA, Santiago, Chile.
[Meeus, G.; Eiroa, C.] Univ Autonoma Madrid, Dept Fis Teor, Fac Ciencias, E-28049 Madrid, Spain.
[Donaldson, J. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Olofsson, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Moor, A.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary.
[Augereau, J. -C.; Thi, W. -F.] UJF Grenoble 1, CNRS, INSU, Inst Planetol & Astrophys Grenoble,UMR 5274, F-38041 Grenoble, France.
[Howard, C.; Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Ardila, D. R.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Woitke, P.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria.
RP Roberge, A (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
EM Aki.Roberge@nasa.gov
RI Roberge, Aki/D-2782-2012; Montesinos, Benjamin/C-3493-2017
OI Roberge, Aki/0000-0002-2989-3725; Montesinos,
Benjamin/0000-0002-7982-2095
FU NASA Herschel Science Center through JPL/Caltech; Goddard Center for
Astrobiology, NASA Astrobiology Institute; CNES-PNP; [AYA 2011-26202]
FX Herschel is an ESA space observatory with science instruments provided
by European-led Principal Investigator consortia and with important
participation from NASA. Support for this work was provided by the NASA
Herschel Science Center through an award issued by JPL/Caltech. A.
Roberge also acknowledges support by the Goddard Center for
Astrobiology, part of the NASA Astrobiology Institute. J.-C. Augereau
thanks the CNES-PNP for financial support. C. Eiroa, G. Meeus, and B.
Montesinos were partly supported by Spanish grant AYA 2011-26202.
NR 60
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2013
VL 771
IS 1
AR 69
DI 10.1088/0004-637X/771/1/69
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176AD
UT WOS:000321274200069
ER
PT J
AU Scargle, JD
Keil, SL
Worden, SP
AF Scargle, Jeffrey D.
Keil, Stephen L.
Worden, Simon P.
TI SOLAR CYCLE VARIABILITY AND SURFACE DIFFERENTIAL ROTATION FROM Ca II
K-LINE TIME SERIES DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: statistical; Sun: chromosphere; Sun:
rotation
ID UNEVENLY SPACED DATA; SPECTRAL-ANALYSIS; PERIODICITIES; STAR; PERIOD;
SUN
AB Analysis of over 36 yr of time series data from the NSO/AFRL/Sac Peak K-line monitoring program elucidates 5 components of the variation of the 7 measured chromospheric parameters: (a) the solar cycle (period similar to 11 yr), (b) quasi-periodic variations (periods similar to 100 days), (c) a broadband stochastic process (wide range of periods), (d) rotational modulation, and (e) random observational errors, independent of (a)-(d). Correlation and power spectrum analyses elucidate periodic and aperiodic variation of these parameters. Time-frequency analysis illuminates periodic and quasi-periodic signals, details of frequency modulation due to differential rotation, and in particular elucidates the rather complex harmonic structure (a) and (b) at timescales in the range similar to 0.1-10 yr. These results using only full-disk data suggest that similar analyses will be useful for detecting and characterizing differential rotation in stars from stellar light curves such as those being produced by NASA's Kepler observatory. Component (c) consists of variations over a range of timescales, in the manner of a 1/f random process with a power-law slope index that varies in a systematic way. A time-dependent Wilson-Bappu effect appears to be present in the solar cycle variations (a), but not in the more rapid variations of the stochastic process (c). Component (d) characterizes differential rotation of the active regions. Component (e) is of course not characteristic of solar variability, but the fact that the observational errors are quite small greatly facilitates the analysis of the other components. The data analyzed in this paper can be found at the National Solar Observatory Web site http://nsosp.nso.edu/cak_mon/, or by file transfer protocol at ftp://ftp.nso.edu/idl/cak.parameters.
C1 [Scargle, Jeffrey D.; Worden, Simon P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Keil, Stephen L.] Natl Solar Observ, Sunspot, NM 88349 USA.
RP Scargle, JD (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU NASA Applied Information Systems Research Program
FX We are grateful to Alexander Kosovichev, Kira Rehfeld, and Luca Bertello
for helpful comments, and to Joe Bredekamp and the NASA Applied
Information Systems Research Program for encouragement and support. The
observations used herein were obtained at the Evans Solar Facility of
the National Solar Observatory. We are grateful for the assistance of
NSO personnel, especially John Cornett, Timothy Henry, and Lou Gilliam
for observing and reduction of the raw data to produce the Ca II K-line
data archive. The NSO is operated by the Association of Universities for
Research in Astronomy, Inc. (AURA), for the National Science Foundation.
NR 36
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2013
VL 771
IS 1
AR 33
DI 10.1088/0004-637X/771/1/33
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176AD
UT WOS:000321274200033
ER
PT J
AU Winebarger, AR
Walsh, RW
Moore, R
De Pontieu, B
Hansteen, V
Cirtain, J
Golub, L
Kobayashi, K
Korreck, K
DeForest, C
Weber, M
Title, A
Kuzin, S
AF Winebarger, Amy R.
Walsh, Robert W.
Moore, Ronald
De Pontieu, Bart
Hansteen, Viggo
Cirtain, Jonathan
Golub, Leon
Kobayashi, Ken
Korreck, Kelly
DeForest, Craig
Weber, Mark
Title, Alan
Kuzin, Sergey
TI DETECTING NANOFLARE HEATING EVENTS IN SUBARCSECOND INTER-MOSS LOOPS
USING Hi-C
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona
ID ACTIVE-REGION LOOPS; TRANSITION-REGION; CORONAL-EXPLORER; ATMOSPHERIC
LOOP; SOLAR CORONA; TRACE; TEMPERATURE; HINODE; CONSTRAINTS; EVOLUTION
AB The High-resolution Coronal Imager (Hi-C) flew aboard a NASA sounding rocket on 2012 July 11 and captured roughly 345 s of high-spatial and temporal resolution images of the solar corona in a narrowband 193 angstrom channel. In this paper, we analyze a set of rapidly evolving loops that appear in an inter-moss region. We select six loops that both appear in and fade out of the Hi-C images during the short flight. From the Hi-C data, we determine the size and lifetimes of the loops and characterize whether these loops appear simultaneously along their length or first appear at one footpoint before appearing at the other. Using co-aligned, co-temporal data from multiple channels of the Atmospheric Imaging Assembly on the Solar Dynamics Observatory, we determine the temperature and density of the loops. We find the loops consist of cool (similar to 10(5) K), dense (similar to 10(10) cm(-3)) plasma. Their required thermal energy and their observed evolution suggest they result from impulsive heating similar in magnitude to nanoflares. Comparisons with advanced numerical simulations indicate that such dense, cold and short-lived loops are a natural consequence of impulsive magnetic energy release by reconnection of braided magnetic field at low heights in the solar atmosphere.
C1 [Winebarger, Amy R.; Moore, Ronald; Cirtain, Jonathan] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Walsh, Robert W.] Univ Cent Lancashire, Preston PR1 2HE, Lancs, England.
[De Pontieu, Bart; Title, Alan] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Hansteen, Viggo] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Golub, Leon; Korreck, Kelly; Weber, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kobayashi, Ken] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
[DeForest, Craig] Southwest Res Inst, Boulder, CO 80302 USA.
[Kuzin, Sergey] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia.
RP Winebarger, AR (reprint author), NASA, George C Marshall Space Flight Ctr, ZP 13, Huntsville, AL 35812 USA.
EM amy.r.winebarger@nasa.gov
RI Kuzin, Sergey/M-3435-2015
FU NASA
FX We acknowledge the High-resolution Coronal Imager instrument grant
funded by the NASA's Low Cost Access to Space program. MSFC/NASA led the
mission and partners include the Smithsonian Astrophysical Observatory
in Cambridge, Massachusetts; Lockheed Martin's Solar Astrophysical
Laboratory in Palo Alto, California; the University of Central
Lancashire in Lancashire, England; and the Lebedev Physical Institute of
the Russian Academy of Sciences in Moscow.
NR 37
TC 26
Z9 26
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 JUL 1
PY 2013
VL 771
IS 1
AR 21
DI 10.1088/0004-637X/771/1/21
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 176AD
UT WOS:000321274200021
ER
PT J
AU Stubenrauch, CJ
Rossow, WB
Kinne, S
Ackerman, S
Cesana, G
Chepfer, H
Di Girolamo, L
Getzewich, B
Guignard, A
Heidinger, A
Maddux, BC
Menzel, WP
Minnis, P
Pearl, C
Platnick, S
Poulsen, C
Riedi, J
Sun-Mack, S
Walther, A
Winker, D
Zeng, S
Zhao, G
AF Stubenrauch, C. J.
Rossow, W. B.
Kinne, S.
Ackerman, S.
Cesana, G.
Chepfer, H.
Di Girolamo, L.
Getzewich, B.
Guignard, A.
Heidinger, A.
Maddux, B. C.
Menzel, W. P.
Minnis, P.
Pearl, C.
Platnick, S.
Poulsen, C.
Riedi, J.
Sun-Mack, S.
Walther, A.
Winker, D.
Zeng, S.
Zhao, G.
TI Assessment of Global Cloud Datasets from Satellites: Project and
Database Initiated by the GEWEX Radiation Panel
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID MICROPHYSICAL PROPERTIES; STATISTICAL-ANALYSIS; IMAGERS ISCCP; LEVEL
CLOUDS; SOUNDERS 3I; WATER PATH; A-TRAIN; PART I; MODIS; CIRRUS
AB Clouds cover about 70% of Earth's surface and play a dominant role in the energy and water cycle of our planet. Only satellite observations provide a continuous survey of the state of the atmosphere over the entire globe and across the wide range of spatial and temporal scales that compose weather and climate variability. Satellite cloud data records now exceed more than 25 years; however, climate data records must be compiled from different satellite datasets and can exhibit systematic biases. Questions therefore arise as to the accuracy and limitations of the various sensors and retrieval methods. The Global Energy and Water Cycle Experiment (GEWEX) Cloud Assessment, initiated in 2005 by the GEWEX Radiation Panel (GEWEX Data and Assessment Panel since 2011), provides the first coordinated intercomparison of publicly available, standard global cloud products (gridded monthly statistics) retrieved from measurements of multispectral imagers (some with multiangle view and polarization capabilities), IR sounders, and lidar. Cloud properties under study include cloud amount, cloud height (in terms of pressure, temperature, or altitude), cloud thermodynamic phase, and cloud radiative and bulk microphysical properties (optical depth or emissivity, effective particle radius, and water path). Differences in average cloud properties, especially in the amount of high-level clouds, are mostly explained by the inherent instrument measurement capability for detecting and/or identifying optically thin cirrus, especially when overlying low-level clouds. The study of long-term variations with these datasets requires consideration of many factors. The monthly gridded database presented here facilitates further assessments, climate studies, and the evaluation of climate models.
C1 [Stubenrauch, C. J.; Chepfer, H.; Guignard, A.] Ecole Polytech, Lab Meteorol Dynam, UPMC, CNRS,IPSL, F-91128 Palaiseau, France.
[Rossow, W. B.; Pearl, C.] CUNY, CREST Inst, New York, NY 10021 USA.
[Kinne, S.] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
[Ackerman, S.; Maddux, B. C.; Menzel, W. P.; Walther, A.] Univ Wisconsin, CIMSS, Madison, WI USA.
[Di Girolamo, L.; Zhao, G.] Univ Illinois, Dept Atmospher Sci, Urbana, IL USA.
[Getzewich, B.; Sun-Mack, S.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Heidinger, A.] STAR, NESDIS, NOAA, Madison, WI USA.
[Minnis, P.; Winker, D.] NASA Langley Res Ctr, Hampton, VA USA.
[Platnick, S.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Poulsen, C.] Rutherford Appleton Lab, Chilton, England.
[Riedi, J.; Zeng, S.] Inst Pasteur, Ctr Immunol & Biol Parasitaire, CNRS, Opt Atmospher Lab, F-59019 Lille, France.
RP Stubenrauch, CJ (reprint author), Ecole Polytech, Lab Meteorol Dynam, F-91128 Palaiseau, France.
EM stubenrauch@lmd.polytechnique.fr
RI Zeng, Shan/C-1520-2014; Menzel, W. Paul/B-8306-2011; Platnick,
Steven/J-9982-2014; Heidinger, Andrew/F-5591-2010; Rossow,
William/F-3138-2015; Ackerman, Steven/G-1640-2011; Minnis,
Patrick/G-1902-2010
OI Zeng, Shan/0000-0002-3540-1811; Menzel, W. Paul/0000-0001-5690-1201;
Platnick, Steven/0000-0003-3964-3567; Heidinger,
Andrew/0000-0001-7631-109X; Ackerman, Steven/0000-0002-4476-0269;
Minnis, Patrick/0000-0002-4733-6148
NR 63
TC 99
Z9 102
U1 3
U2 57
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 JUL
PY 2013
VL 94
IS 7
BP 1031
EP 1049
DI 10.1175/BAMS-D-12-00117.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 188LU
UT WOS:000322195300006
ER
PT J
AU Bois, P
Gunapala, SD
AF Bois, Philippe
Gunapala, Sarath D.
TI Preface
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Editorial Material
C1 [Bois, Philippe] Thales Res & Technol, Lab 3 5, F-91767 Palaiseau, France.
[Gunapala, Sarath D.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
RP Bois, P (reprint author), Thales Res & Technol, Lab 3 5, Campus Polytech,1 Av A Fresnel, F-91767 Palaiseau, France.
EM philippe.bois@thalesgroup.com; sarath.d.gunapala@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 3
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 JUL
PY 2013
VL 59
BP 1
EP 1
DI 10.1016/j.infrared.2013.02.001
PG 1
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA 172BL
UT WOS:000320974800001
ER
PT J
AU Gunapala, SD
Rafol, SB
Ting, DZ
Soibel, A
Liu, JK
Khoshakhlagh, A
Keo, SA
Mumolo, JM
Nguyen, J
AF Gunapala, S. D.
Rafol, S. B.
Ting, D. Z.
Soibel, A.
Liu, J. K.
Khoshakhlagh, A.
Keo, S. A.
Mumolo, J. M.
Nguyen, J.
TI Modulation transfer function of QWIP and superlattice focal plane arrays
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Article; Proceedings Paper
CT International Conference on Quantum Structure Infrared Photodetector
(QSIP)
CY JUN 18-22, 2012
CL Inst Etudes Sci Cargese, FRANCE
SP III V Lab, JPL, Acreo, ONERA, Aselsan, Pulse Instruments, FLIR, Qmagiq, Intelli EPI, Sofradir, Wafer Technol Ltd, Thales, Collectivite Territoriale Corse
HO Inst Etudes Sci Cargese
DE QWIPs; Superlattices; Focal Plane Arrays; Modulation Transfer Function
AB Modulation transfer function (MTF) is the ability of an imaging system to faithfully image a given object. The MTF of an imaging system quantifies the ability of the system to resolve or transfer spatial frequencies. In this paper we will discuss the detail MTF measurements of a 1024 x 1024 pixel multi-band quantum well infrared photodetector and 320 x 256 pixel long-wavelength InAs/GaSb superlattice infrared focal plane arrays. (c) 2013 Elsevier B.V. All rights reserved.
C1 [Gunapala, S. D.; Rafol, S. B.; Ting, D. Z.; Soibel, A.; Liu, J. K.; Khoshakhlagh, A.; Keo, S. A.; Mumolo, J. M.; Nguyen, J.] CALTECH, Jet Prop Lab, Ctr Infrared Sensors, Pasadena, CA 91109 USA.
RP Gunapala, SD (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Sensors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sarath.d.gunapala@jpl.nasa.gov
RI Soibel, Alexander/A-1313-2007
NR 10
TC 2
Z9 2
U1 2
U2 20
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 JUL
PY 2013
VL 59
BP 64
EP 71
DI 10.1016/j.infrared.2012.12.016
PG 8
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA 172BL
UT WOS:000320974800012
ER
PT J
AU Ting, DZY
Soibel, A
Khoshakhlagh, A
Keo, SA
Nguyen, J
Hoglund, L
Mumolo, JM
Liu, JK
Rafol, B
Hill, CJ
Gunapala, SD
AF Ting, David Z. -Y.
Soibel, Alexander
Khoshakhlagh, Arezou
Keo, Sam A.
Nguyen, Jean
Hoeglund, Linda
Mumolo, Jason M.
Liu, John K.
Rafol, B.
Hill, Cory J.
Gunapala, Sarath D.
TI Complementary barrier infrared detector (CBIRD) with double tunnel
junction contact and quantum dot barrier infrared detector (QD-BIRD)
SO INFRARED PHYSICS & TECHNOLOGY
LA English
DT Article; Proceedings Paper
CT International Conference on Quantum Structure Infrared Photodetector
(QSIP)
CY JUN 18-22, 2012
CL Inst Etudes Sci Cargese, FRANCE
SP III V Lab, JPL, Acreo, ONERA, Aselsan, Pulse Instruments, FLIR, Qmagiq, Intelli EPI, Sofradir, Wafer Technol Ltd, Thales, Collectivite Territoriale Corse
HO Inst Etudes Sci Cargese
DE Infrared detector; Antimonide; Type-II superlattice; Quantum dot;
Unipolar barrier
ID PHOTODIODES; PHOTODETECTORS; SUPERLATTICES; PERFORMANCE
AB The InAs/GaSb type-II superlattice based complementary barrier infrared detector (CBIRD) has already demonstrated very good performance in long-wavelength infrared (LWIR) detection. In this work, we describe results on a modified CBIRD device that incorporates a double tunnel junction contact designed for robust device and focal plane array processing. The new device also exhibited reduced turn-on voltage. We also report results on the quantum dot barrier infrared detector (QD-BIRD). By incorporating self-assembled InSb quantum dots into the InAsSb absorber of the standard nBn detector structure, the QD-BIRD extend the detector cutoff wavelength from similar to 4.2 mu m to 6 mu m, allowing the coverage of the mid-wavelength infrared (MWIR) transmission window. The device has been observed to show infrared response at 225 K. (c) 2013 Elsevier B.V. All rights reserved.
C1 [Ting, David Z. -Y.; Soibel, Alexander; Khoshakhlagh, Arezou; Keo, Sam A.; Nguyen, Jean; Hoeglund, Linda; Mumolo, Jason M.; Liu, John K.; Rafol, B.; Hill, Cory J.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Ctr Infrared Sensors, Pasadena, CA 91109 USA.
RP Ting, DZY (reprint author), CALTECH, Jet Prop Lab, M-S 302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM David.Z.Ting@jpl.nasa.gov
RI Soibel, Alexander/A-1313-2007
NR 28
TC 2
Z9 2
U1 3
U2 31
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 JUL
PY 2013
VL 59
BP 146
EP 151
DI 10.1016/j.infrared.2012.12.030
PG 6
WC Instruments & Instrumentation; Optics; Physics, Applied
SC Instruments & Instrumentation; Optics; Physics
GA 172BL
UT WOS:000320974800026
ER
PT J
AU Sakai, T
Whiteman, DN
Russo, F
Turner, DD
Veselovskii, I
Melfi, SH
Nagai, T
Mano, Y
AF Sakai, Tetsu
Whiteman, David N.
Russo, Felicita
Turner, David D.
Veselovskii, Igor
Melfi, S. Harvey
Nagai, Tomohiro
Mano, Yuzo
TI Liquid Water Cloud Measurements Using the Raman Lidar Technique: Current
Understanding and Future Research Needs
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
DE Cloud retrieval; Lidars; Lidar observations
ID EMITTED RADIANCE INTERFEROMETER; GROUND-BASED MEASUREMENTS; VAPOR
MIXING-RATIO; CROSS-SECTIONS; ATMOSPHERIC AEROSOLS; FLUORESCENCE;
SCATTERING; BACKSCATTER; PERFORMANCE; TROPOSPHERE
AB This paper describes recent work in the Raman lidar liquid water cloud measurement technique. The range-resolved spectral measurements at the National Aeronautics and Space Administration Goddard Space Flight Center indicate that the Raman backscattering spectra measured in and below low clouds agree well with theoretical spectra for vapor and liquid water. The calibration coefficients of the liquid water measurement for the Raman lidar at the Atmospheric Radiation Measurement Program Southern Great Plains site of the U.S. Department of Energy were determined by comparison with the liquid water path (LWP) obtained with Atmospheric Emitted Radiance Interferometer (AERI) and the liquid water content (LWC) obtained with the millimeter wavelength cloud radar and water vapor radiometer (MMCR-WVR) together. These comparisons were used to estimate the Raman liquid water cross-sectional value. The results indicate a bias consistent with an effective liquid water Raman cross-sectional value that is 28%-46% lower than published, which may be explained by the fact that the difference in the detectors' sensitivity has not been accounted for. The LWP of a thin altostratus cloud showed good qualitative agreement between lidar retrievals and AERI. However, the overall ensemble of comparisons of LWP showed considerable scatter, possibly because of the different fields of view of the instruments, the 350-m distance between the instruments, and the horizontal inhomogeneity of the clouds. The LWC profiles for a thick stratus cloud showed agreement between lidar retrievals and MMCR-WVR between the cloud base and 150 m above that where the optical depth was less than 3. Areas requiring further research in this technique are discussed.
C1 [Sakai, Tetsu; Nagai, Tomohiro; Mano, Yuzo] Meteorol Res Inst, Tsukuba, Ibaraki 3050052, Japan.
[Whiteman, David N.; Melfi, S. Harvey] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Russo, Felicita] Italian Natl Agcy New Technol, Bologna, Italy.
[Turner, David D.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
[Veselovskii, Igor] Russian Acad Sci, Inst Gen Phys, Phys Instrumentat Ctr, Moscow, Russia.
RP Sakai, T (reprint author), Meteorol Res Inst, 1-1 Nagamine, Tsukuba, Ibaraki 3050052, Japan.
EM tetsu@mri-jma.go.jp
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT)
FX This work was supported by the Ministry of Education, Culture, Sports,
Science and Technology (MEXT).
NR 50
TC 4
Z9 4
U1 2
U2 25
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD JUL
PY 2013
VL 30
IS 7
BP 1337
EP 1353
DI 10.1175/JTECH-D-12-00099.1
PG 17
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 187NP
UT WOS:000322126100006
ER
PT J
AU Xu, ZG
Song, YT
AF Xu, Zhigang
Song, Y. Tony
TI Combining the All-Source Green's Functions and the GPS-Derived Source
Functions for Fast Tsunami PredictionsIllustrated by the March 2011
Japan Tsunami
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
DE Shallow-water equations; Global positioning systems (GPS); In situ
oceanic observations; Differential equations; Numerical analysis;
modeling; Ocean models
ID DECEMBER 2004 TSUNAMI; WAVE-FORMS; EARTHQUAKE; INVERSION
AB This paper proposes an effective approach on how to predict tsunamis rapidly following a submarine earthquake by combining a real-time GPS-derived tsunami source function with a set of precalculated all-source Green's functions (ASGFs). The approach uses the data from both teleseismic and coastal GPS networks to constrain a tsunami source function consisting of both sea surface elevation and horizontal velocity field, and uses the ASGFs to instantaneously transfer the source function to the arrival time series at the destination points. The ASGF can take a tsunami source of arbitrary geographic origin and resolve it as fine as the native resolution of a tsunami propagation model from which the ASGF is derived. This new approach is verified by the 2011 Tohoku tsunami using data measured by the Deep-Ocean Assessment and Reporting of Tsunamis (DART) buoys.
C1 [Xu, Zhigang] Fisheries & Oceans Canada, Maurice Lamontagne Inst, Mont Joli, PQ G5H 3Z4, Canada.
[Song, Y. Tony] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Xu, ZG (reprint author), Fisheries & Oceans Canada, Maurice Lamontagne Inst, 850 Route Mer,POB 1000, Mont Joli, PQ G5H 3Z4, Canada.
EM zhigang.xu@dfo-mpo.gc.ca
NR 35
TC 3
Z9 3
U1 0
U2 9
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 JUL
PY 2013
VL 30
IS 7
BP 1542
EP 1554
DI 10.1175/JTECH-D-12-00201.1
PG 13
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 187NP
UT WOS:000322126100019
ER
PT J
AU Suselj, K
Teixeira, J
Chung, D
AF Suselj, Kay
Teixeira, Joao
Chung, Daniel
TI A Unified Model for Moist Convective Boundary Layers Based on a
Stochastic Eddy-Diffusivity/Mass-Flux Parameterization
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Boundary layer; Convective parameterization; Cumulus clouds;
Parameterization; Stochastic models
ID SHALLOW CUMULUS CONVECTION; GENERAL-CIRCULATION MODELS; PDF-BASED MODEL;
PART II; MIXING SCHEME; CLOUDS; STRATOCUMULUS; SIMULATIONS; ENTRAINMENT;
TRANSITION
AB A single-column model (SCM) is developed for representing moist convective boundary layers. The key component of the SCM is the parameterization of subgrid-scale vertical mixing, which is based on a stochastic eddy-diffusivity/mass-flux (EDMF) approach. In the EDMF framework, turbulent fluxes are calculated as a sum of the turbulent kinetic energy-based eddy-diffusivity component and a mass-flux component. The mass flux is modeled as a fixed number of steady-state plumes. The main challenge of the mass-flux model is to properly represent cumulus clouds, which are modeled as moist plumes. The solutions have to account for a realistic representation of condensation within the plumes and of lateral entrainment into the plumes. At the level of mean condensation within the updraft, the joint pdf of moist conserved variables and vertical velocity is used to estimate the proportion of dry and moist plumes and is sampled in a Monte Carlo way creating a predefined number of plumes. The lateral entrainment rate is modeled as a stochastic process resulting in a realistic decrease of the convective cloudiness with height above cloud base. In addition to the EDMF scheme, the following processes are included in the SCM: a pdf-based parameterization of subgrid-scale condensation, a simple longwave radiation, and one-dimensional dynamics. Note that in this approach there are two distinct pdfs, one representing the variability of updraft properties and the other one the variability of thermodynamic properties of the surrounding environment. The authors show that the model is able to capture the essential features of moist boundary layers, ranging from stratocumulus to shallow-cumulus regimes. Detailed comparisons, which include pdfs, profiles, and integrated budgets with the Barbados Oceanographic and Meteorological Experiment (BOMEX), Dynamics and Chemistry of Marine Stratocumulus (DYCOMS), and steady-state large-eddy simulation (LES) cases, are discussed to confirm the quality of the present approach.
C1 [Suselj, Kay; Teixeira, Joao; Chung, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Teixeira, Joao] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Chung, Daniel] Univ Melbourne, Dept Mech Engn, Melbourne, Vic, Australia.
RP Suselj, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kay.suselj@jpl.nasa.gov
RI Chung, Daniel/F-4468-2016
OI Chung, Daniel/0000-0003-3732-364X
FU Office of Naval Research, Marine Meteorology Program [N0001411IP20087,
N0001411IP20069]; NASA MAP Program; NOAA/CPO MAPP Program; National
Aeronautics and Space Administration
FX The valuable comments of the three anonymous reviewers contributed to
the improvement of the original manuscript. We acknowledge the support
provided by the Office of Naval Research, Marine Meteorology Program
under Awards N0001411IP20087 and N0001411IP20069, the NASA MAP Program
and the NOAA/CPO MAPP 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 66
TC 16
Z9 16
U1 2
U2 23
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD JUL
PY 2013
VL 70
IS 7
BP 1929
EP 1953
DI 10.1175/JAS-D-12-0106.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187NK
UT WOS:000322125600005
ER
PT J
AU Garfinkel, CI
Oman, LD
Barnes, EA
Waugh, DW
Hurwitz, MH
Molod, AM
AF Garfinkel, Chaim I.
Oman, Luke D.
Barnes, Elizabeth A.
Waugh, Darryn W.
Hurwitz, Margaret H.
Molod, Andrea M.
TI Connections between the Spring Breakup of the Southern Hemisphere Polar
Vortex, Stationary Waves, and Air-Sea Roughness
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Stationary waves; Stratospheric circulation; Wind waves;
Stratophere-troposphere coupling; Air-sea interaction
ID SURFACE FRICTION; PLANETARY-WAVES; MOMENTUM FLUXES; LATITUDE; JET;
STRATOSPHERE; PROPAGATION; CIRCULATION; TROPOSPHERE; ATMOSPHERE
AB A robust connection between the drag on surface-layer winds and the stratospheric circulation is demonstrated in NASA's Goddard Earth Observing System Chemistry-Climate Model (GEOSCCM). Specifically, an updated parameterization of roughness at the air-sea interface, in which surface roughness is increased for moderate wind speeds (4-20 m s(-1)), leads to a decrease in model biases in Southern Hemispheric ozone, polar cap temperature, stationary wave heat flux, and springtime vortex breakup. A dynamical mechanism is proposed whereby increased surface roughness leads to improved stationary waves. Increased surface roughness leads to anomalous eddy momentum flux convergence primarily in the Indian Ocean sector (where eddies are strongest climatologically) in September and October. The localization of the eddy momentum flux convergence anomaly in the Indian Ocean sector leads to a zonally asymmetric reduction in zonal wind and, by geostrophy, to a wavenumber-1 stationary wave pattern. This tropospheric stationary wave pattern leads to enhanced upward wave activity entering the stratosphere. The net effect is an improved Southern Hemisphere vortex: the vortex breaks up earlier in spring (i.e., the spring late-breakup bias is partially ameliorated) yet is no weaker in midwinter. More than half of the stratospheric biases appear to be related to the surface wind speed biases. As many other chemistry-climate models use a similar scheme for their surface-layer momentum exchange and have similar biases in the stratosphere, the authors expect that results from GEOSCCM may be relevant for other climate models.
C1 [Garfinkel, Chaim I.; Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Oman, Luke D.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
[Barnes, Elizabeth A.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Hurwitz, Margaret H.] Morgan State Univ, NASA Goddard Earth Sci Technol & Res GESTAR, Baltimore, MD 21239 USA.
[Hurwitz, Margaret H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Molod, Andrea M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Molod, Andrea M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Garfinkel, CI (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
EM cig4@jhu.edu
RI Oman, Luke/C-2778-2009; garfinkel, chaim/H-6215-2012; Barnes,
Elizabeth/O-1790-2014; Waugh, Darryn/K-3688-2016
OI Oman, Luke/0000-0002-5487-2598; garfinkel, chaim/0000-0001-7258-666X;
Barnes, Elizabeth/0000-0003-4284-9320; Waugh, Darryn/0000-0001-7692-2798
FU NASA [NNX06AE70G]; NSF [ATM 0905863, AGS 0938325]; NOAA Climate & Global
Change Fellowship through the University Corporation of Atmospheric
Research Visiting Science Program
FX This work was supported by NASA Grant NNX06AE70G and NSF Grants ATM
0905863 and AGS 0938325. EAB is funded by a NOAA Climate & Global Change
Fellowship through the University Corporation of Atmospheric Research
Visiting Science Program. We thank Greg Bodeker of Bodeker Scientific
for providing the combined total column ozone database, In-Sun Song for
helpful conversations and for advice regarding the experiments described
in section 6, and the two anonymous reviewers for their helpful
comments. The simulations were performed at the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center.
NR 42
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U1 0
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD JUL
PY 2013
VL 70
IS 7
BP 2137
EP 2151
DI 10.1175/JAS-D-12-0242.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187NK
UT WOS:000322125600016
ER
PT J
AU Apple, TM
Cantrell, JH
Amaro, CM
Mayer, CR
Yost, WT
Agnew, SR
Howe, JM
AF Apple, T. M.
Cantrell, J. H.
Amaro, C. M.
Mayer, C. R.
Yost, W. T.
Agnew, S. R.
Howe, J. M.
TI Acoustic harmonic generation from fatigue-generated dislocation
substructures in copper single crystals
SO PHILOSOPHICAL MAGAZINE
LA English
DT Article
DE fatigue; ultrasonics; transmission electron microscopy; materials
characterisation; dislocation structures; dislocation dynamics;
deformation; mechanical property evaluation
ID PERSISTENT SLIP BANDS; CYCLIC DEFORMATION; DAMAGE ACCUMULATION; CRACK
INITIATION; ULTRASONIC-WAVES; ELASTIC-CONSTANTS; ALUMINUM-ALLOY;
WEAK-BEAM; STRAIN; AMPLITUDE
AB Dislocations generated during cyclic loading of metals self-organize into substructures that produce substantial changes in the nonlinear response. The nonlinearity is quantified by the material nonlinearity parameter extracted from acoustic harmonic generation measurements. Measurements of on copper single crystals oriented for single-slip ([123] loading axis) and fatigued in plastic strain control are compared to calculations of obtained from the Cantrell model for which measured values of model parameters associated with the substructures are required. Transmission electron microscopy measurements of the volume fractions of veins and persistent slip bands, dislocation loop lengths, dipole heights and the densities of primary and secondary dislocations in the fatigue-generated substructures are obtained for input into the model calculations. The model predictions agree with the values observed experimentally. In particular, the experimental data show an increase in proportional to where is the cumulative plastic strain and m is 0.7 and 0.4, respectively, for acoustic wave propagation along the and crystal axes. Such dependence is consistent with the Cantrell model and at variance with models, based on assumed variations in the third-order elastic constants, which predict an exponential dependence on Gamma.
C1 [Apple, T. M.; Amaro, C. M.; Mayer, C. R.; Agnew, S. R.; Howe, J. M.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22904 USA.
[Cantrell, J. H.; Yost, W. T.] NASA Langley Res Ctr, Res Div, Hampton, VA 23681 USA.
RP Cantrell, JH (reprint author), NASA Langley Res Ctr, Res Div, Hampton, VA 23681 USA.
EM john.h.cantrell@nasa.gov
FU NASA [NNX07AU57A]; NASA Langley Research Centre, Hampton, VA
FX This work was supported by NASA Grant No. NNX07AU57A, NASA Langley
Research Centre, Hampton, VA.
NR 70
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Z9 4
U1 2
U2 26
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 1478-6435
J9 PHILOS MAG
JI Philos. Mag.
PD JUL 1
PY 2013
VL 93
IS 21
BP 2802
EP 2825
DI 10.1080/14786435.2013.789144
PG 24
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering; Physics, Applied; Physics, Condensed Matter
SC Materials Science; Metallurgy & Metallurgical Engineering; Physics
GA 184LI
UT WOS:000321890800004
ER
PT J
AU Kitiashvili, IN
Abramenko, VI
Goode, PR
Kosovichev, AG
Lele, SK
Mansour, NN
Wray, AA
Yurchyshyn, VB
AF Kitiashvili, I. N.
Abramenko, V. I.
Goode, P. R.
Kosovichev, A. G.
Lele, S. K.
Mansour, N. N.
Wray, A. A.
Yurchyshyn, V. B.
TI Turbulent kinetic energy spectra of solar convection from New Solar
Telescope observations and realistic magnetohydrodynamic simulations
SO PHYSICA SCRIPTA
LA English
DT Article; Proceedings Paper
CT 3rd International Conference on Turbulent Mixing and Beyond
CY AUG 21-28, 2011
CL Trieste, ITALY
ID POWER SPECTRA; BRIGHT POINTS; QUIET SUN; GRANULATION; PHOTOSPHERE;
EXCITATION; MOTION; STATE; MODEL
AB Turbulent properties of the quiet Sun represent the basic state of surface conditions and a background for various processes of solar activity. Therefore, understanding the properties and dynamics of this 'basic' state is important for the investigation of more complex phenomena, the formation and development of observed phenomena in the photosphere and atmosphere. For the characterization of turbulent properties, we compare the kinetic energy spectra on granular and sub-granular scales obtained from infrared TiO observations with the New Solar Telescope (Big Bear Solar Observatory) and from three-dimensional radiative magnetohydrodynamic (MHD) numerical simulations ('SolarBox' code). We find that the numerical simulations require high spatial resolution with a 10-25 km grid step in order to reproduce the inertial (Kolmogorov) turbulence range. The observational data require an averaging procedure to remove noise and potential instrumental artifacts. The resulting kinetic energy spectra reveal good agreement between the simulations and the observations, opening up new perspectives for detailed joint analyses of more complex turbulent phenomena on the Sun and possibly on other stars. In addition, using the simulations and observations, we investigate the effects of a background magnetic field, which is concentrated in self-organized complicated structures in intergranular lanes, and observe an increase of the small-scale turbulence energy and its decrease at larger scales due to magnetic field effects.
C1 [Kitiashvili, I. N.; Kosovichev, A. G.] Stanford Univ, W W Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Kitiashvili, I. N.; Lele, S. K.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA.
[Kitiashvili, I. N.] Kazan Fed Univ, Kazan 420008, Russia.
[Abramenko, V. I.; Goode, P. R.; Yurchyshyn, V. B.] New Jersey Inst Technol, Big Bear Solar Observ, Big Bear Lake, CA 92315 USA.
[Lele, S. K.] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
[Mansour, N. N.; Wray, A. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kitiashvili, IN (reprint author), Stanford Univ, W W Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM irinasun@stanford.edu
FU NASA [NNX10AC55G]; International Space Science Institute (Bern); Nordita
(Stockholm)
FX This work was partially supported by the NASA grant no. NNX10AC55G, the
International Space Science Institute (Bern) and Nordita (Stockholm).
NR 31
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U1 1
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0031-8949
EI 1402-4896
J9 PHYS SCRIPTA
JI Phys. Scr.
PD JUL
PY 2013
VL T155
AR UNSP 014025
DI 10.1088/0031-8949/2013/T155/014025
PG 8
WC Physics, Multidisciplinary
SC Physics
GA 184CC
UT WOS:000321863000027
ER
PT J
AU Van Bossuyt, DL
Tumer, IY
Wall, SD
AF Van Bossuyt, Douglas L.
Tumer, Irem Y.
Wall, Stephen D.
TI A case for trading risk in complex conceptual design trade studies
SO RESEARCH IN ENGINEERING DESIGN
LA English
DT Article
DE Trade study; Complex system design; Risk; Collaborative Design Center
risk trading
ID PRODUCT DEVELOPMENT; ENGINEERING DESIGN; DECISION-MAKING; EXPERT
JUDGMENT; ROBUST DESIGN; EXPLORATION; SYSTEM; ARCHITECTURE; METHODOLOGY;
UNCERTAINTY
AB Complex conceptual system design trade studies traditionally consider risk after a conceptual design has been created. Further, one person is often tasked with collecting risk information and managing it from each subsystem. This paper proposes a method to explicitly consider and trade risk on the same level as other important system-level variables during the creation of conceptual designs in trade studies. The proposed risk trading method advocates putting each subsystem engineer in control of risk for each subsystem. A risk vector is proposed that organizes many different risk metrics for communication between subsystems. A method of coupling risk models to dynamic subsystem models is presented. Several risk visualization techniques are discussed. A trade study example is presented based upon a simplified spacecraft model. Results from introducing the risk trading methodology into a simulated Collaborative Design Center are presented. The risk trading method offers an approach to more thoroughly consider risk during the creation of conceptual designs in trade studies.
C1 [Van Bossuyt, Douglas L.; Tumer, Irem Y.] Oregon State Univ, Sch Mech Ind & Mfg Engn, Corvallis, OR 97331 USA.
[Wall, Stephen D.] CALTECH, Jet Prop Lab, Syst Modeling & Anal Program Off, Pasadena, CA 91019 USA.
RP Van Bossuyt, DL (reprint author), Oregon State Univ, Sch Mech Ind & Mfg Engn, Corvallis, OR 97331 USA.
EM Douglas.VanBossuyt@gmail.com; Irem.Tumer@oregonstate.edu;
Stephen.D.Wall@jpl.nasa.gov
RI Van Bossuyt, Douglas/B-5884-2014
OI Van Bossuyt, Douglas/0000-0001-9910-371X
FU NASA
FX This research was carried out in part at JPL, Caltech, under contract
with NASA. Special thanks goes to Scott Ragon, Taurik Elgabrowny, and
others at Phoenix Integration Inc. for donating software and providing
technical support, and Steve Cornford at JPL for providing valuable
feedback and inspiration. The study protocol was reviewed and approved
by the Institutional Review Board, Study 4611, at Oregon State
University. The opinions and findings of this work are the
responsibility of the authors and do not necessarily reflect the views
of the sponsors or collaborators.
NR 74
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U1 1
U2 13
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0934-9839
J9 RES ENG DES
JI Res. Eng. Design
PD JUL
PY 2013
VL 24
IS 3
BP 259
EP 275
DI 10.1007/s00163-012-0142-0
PG 17
WC Engineering, Multidisciplinary; Engineering, Industrial; Engineering,
Manufacturing
SC Engineering
GA 181HU
UT WOS:000321659400004
ER
PT J
AU Zwart, SR
Morgan, JLL
Smith, SM
AF Zwart, Sara R.
Morgan, Jennifer L. L.
Smith, Scott M.
TI Iron status and its relations with oxidative damage and bone loss during
long-duration space flight on the International Space Station
SO AMERICAN JOURNAL OF CLINICAL NUTRITION
LA English
DT Article
ID HUMAN-IMMUNODEFICIENCY-VIRUS; RED-BLOOD-CELL; BODY IRON;
NUTRITIONAL-STATUS; TRANSFERRIN RECEPTOR; CALCIUM-METABOLISM;
SPACEFLIGHT; FERRITIN; OVERLOAD; STRESS
AB Background: Increases in stored iron and dietary intake of iron during space flight have raised concern about the risk of excess iron and oxidative damage, particularly in bone.
Objectives: The objectives of this study were to perform a comprehensive assessment of iron status in men and women before, during, and after long-duration space flight and to quantify the association of iron status with oxidative damage and bone loss.
Design: Fasting blood and 24-h urine samples were collected from 23 crew members before, during, and after missions lasting 50 to 247 d to the International Space Station.
Results: Serum ferritin and body iron increased early in flight, and transferrin and transferrin receptors decreased later, which indicated that early increases in body iron stores occurred through the mobilization of iron to storage tissues. Acute phase proteins indicated no evidence of an inflammatory response during flight. Serum ferritin was positively correlated with the oxidative damage markers 8-hydroxy-2'-deoxyguanosine (r = 0.53, P < 0.001) and prostaglandin F2 alpha (r = 0.26, P < 0.001), and the greater the area under the curve for ferritin during flight, the greater the decrease in bone mineral density in the total hip (P = 0.031), trochanter (P = 0.006), hip neck (P = 0.044), and pelvis (P = 0.049) after flight.
Conclusion: Increased iron stores may be a risk factor for oxidative damage and bone resorption.
C1 [Zwart, Sara R.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA.
[Morgan, Jennifer L. L.] Oak Ridge Associated Univ, NASA, Houston, TX USA.
[Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Human Hlth & Performance Directorate, Houston, TX 77058 USA.
RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA.
EM scott.m.smith@nasa.gov
FU National Aeronautics and Space Administration Human Research Program;
Oak Ridge Associated Universities/National Aeronautics and Space
Administration
FX Supported by the National Aeronautics and Space Administration Human
Research Program and the Oak Ridge Associated Universities/National
Aeronautics and Space Administration Postdoctoral Fellowship (JLLM).
NR 45
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U1 1
U2 14
PU AMER SOC NUTRITION-ASN
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 0002-9165
J9 AM J CLIN NUTR
JI Am. J. Clin. Nutr.
PD JUL
PY 2013
VL 98
IS 1
BP 217
EP 223
DI 10.3945/ajcn.112.056465
PG 7
WC Nutrition & Dietetics
SC Nutrition & Dietetics
GA 171EZ
UT WOS:000320909200026
PM 23719548
ER
PT J
AU Abshire, JB
Riris, H
Weaver, CJ
Mao, JP
Allan, GR
Hasselbrack, WE
Browell, EV
AF Abshire, James B.
Riris, Haris
Weaver, Clark J.
Mao, Jianping
Allan, Graham R.
Hasselbrack, William E.
Browell, Edward V.
TI Airborne measurements of CO2 column absorption and range using a pulsed
direct-detection integrated path differential absorption lidar
SO APPLIED OPTICS
LA English
DT Article
ID GASES OBSERVING SATELLITE; ATMOSPHERIC CO2; REFLECTED SUNLIGHT; COHERENT
DETECTION; CARBON-DIOXIDE; SENSITIVITY; SPECTROMETER; BUDGET; BAND; CH4
AB We report on airborne CO2 column absorption measurements made in 2009 with a pulsed direct-detection lidar operating at 1572.33 nm and utilizing the integrated path differential absorption technique. We demonstrated these at different altitudes from an aircraft in July and August in flights over four locations in the central and eastern United States. The results show clear CO2 line shape and absorption signals, which follow the expected changes with aircraft altitude from 3 to 13 km. The lidar measurement statistics were also calculated for each flight as a function of altitude. The optical depth varied nearly linearly with altitude, consistent with calculations based on atmospheric models. The scatter in the optical depth measurements varied with aircraft altitude as expected, and the median measurement precisions for the column varied from 0.9 to 1.2 ppm. The altitude range with the lowest scatter was 8-10 km, and the majority of measurements for the column within it had precisions between 0.2 and 0.9 ppm.
C1 [Abshire, James B.; Riris, Haris] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Weaver, Clark J.; Mao, Jianping] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Allan, Graham R.; Hasselbrack, William E.] Sigma Space Corp, Lanham, MD 20706 USA.
[Browell, Edward V.] NASA, Langley Res Ctr, STARSS Affiliate 2, Hampton, VA 23681 USA.
RP Abshire, JB (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM James.B.Abshire@nasa.gov
RI Abshire, James/I-2800-2013; Riris, Haris/D-1004-2013
FU NASA Earth Science Technology Office; NASA ASCENDS Mission Definition
activity; NASA Goddard IRAD program
FX We are grateful for the support of the NASA Earth Science Technology
Office's Advanced Instrument Technology and Instrument Incubator
Programs, the NASA ASCENDS Mission Definition activity, and the NASA
Goddard IRAD program. We greatly appreciate the work of other members of
the Goddard CO2 Sounder team. We also appreciate the
collaborations with James Demers, Alan Mickleright, and Steven Hughell
of NASA Glenn, the in situ atmospheric measurements from Susan Kooi of
NASA LaRC, and the many helpful comments and recommendations from the
reviewers.
NR 33
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U1 2
U2 12
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
J9 APPL OPTICS
JI Appl. Optics
PD JUL 1
PY 2013
VL 52
IS 19
BP 4446
EP 4461
DI 10.1364/AO.52.004446
PG 16
WC Optics
SC Optics
GA 176FS
UT WOS:000321289700006
PM 23842238
ER
PT J
AU Hui, HJ
Neal, CR
Shih, CY
Nyquist, LE
AF Hui, Hejiu
Neal, Clive R.
Shih, Chi-Yu
Nyquist, Laurence E.
TI Petrogenetic association of the oldest lunar basalts: Combined Rb-Sr
isotopic and trace element constraints
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Apollo 14; high-Al basalt; Rb-Sr isotopic system; radiometric age;
incompatible trace element; mixing
ID ALUMINOUS MARE BASALTS; FRA MAURO FORMATION; APOLLO-14 MISSION; MAGMA
OCEAN; HALF-LIFE; MOON; AGE; CHRONOLOGY; KREEP; ROCKS
AB We report a new radiometric Rb-Sr age determination of 4.03 +/- 0.04 Ga for high-Al basaltic clast 14321,1353, which is a Group B Apollo 14 high-Al basalt based on its whole-rock incompatible-trace-element chemistry. In addition, available literature Rb-Sr isotope data for Apollo 14 high-Al basalts were reprocessed using the same decay constant and data reduction protocol as used for sample 14321,1353. The Rb-Sr isotopic ages of high-Al basalts range from 431 +/- 0.17 to 3.93 +/- 0.06 Ga. The trace element and Rb-Sr isotopic compositions of high-Al basalts are distinct from those of Apollo 14 aluminous impact melts that crystallized at 3.86 +/- 0.01 Ga. The Rb-Sr isotope systematics, coupled with incompatible-trace-element data are consistent with the parental melts of Apollo 14 high-Al basalts being derived from sources consisting of primitive crystallization products of the lunar magma ocean that were variably metasomatized by late-stage KREEP-rich fluids. Our new Rb-Sr isotopic age for 14321,1353 suggests that the KREEP metasomatism must occur in the lunar mantle no later than 4.03 +/- 0.04 Ga. Collectively, the Apollo 14 high-Al basalts represent the earliest known volcanic products from the Moon and place a time constraint on the formation of the high-Al basalt source through the crystallization of the lunar magma ocean. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Hui, Hejiu; Neal, Clive R.] Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA.
[Shih, Chi-Yu] Jacobs Technol, ESCG, Houston, TX 77058 USA.
[Nyquist, Laurence E.] NASA, ARES, Johnson Space Ctr, Mail Code KR, Houston, TX 77058 USA.
RP Hui, HJ (reprint author), Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA.
EM hhui@nd.edu
RI Hui, Hejiu/D-2912-2011
OI Hui, Hejiu/0000-0003-2733-5794
FU NASA [NNX09AB92G]
FX This work was supported by the NASA Cosmochemistry Grant NNX09AB92G to
CRN. The informal review by Tony Simonetti significantly clarified the
manuscript. The constructive reviews by the editor Tim Elliott and two
anonymous reviewers were invaluable in improving this paper.
NR 76
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Z9 2
U1 2
U2 17
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD JUL 1
PY 2013
VL 373
BP 150
EP 159
DI 10.1016/j.epsl.2013.04.034
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 181PF
UT WOS:000321680300016
ER
PT J
AU Bandfield, JL
Wolff, MJ
Smith, MD
Schofield, JT
McCleese, DJ
AF Bandfield, Joshua L.
Wolff, Michael J.
Smith, Michael D.
Schofield, John T.
McCleese, Daniel J.
TI Radiometric comparison of Mars Climate Sounder and Thermal Emission
spectrometer measurements
SO ICARUS
LA English
DT Article
DE Mars, Climate; Infrared observations; Mars, Atmosphere
ID MARTIAN ATMOSPHERE; GLOBAL SURVEYOR; WATER-VAPOR; ICE CLOUDS;
INTERANNUAL VARIABILITY; INFRARED MEASUREMENTS; MGS TES; SURFACE;
TEMPERATURES; APHELION
AB Mars Climate Sounder (MCS) nadir oriented thermal infrared and solar channel measurements are compared with Thermal Emission Spectrometer (TES) measurements across multiple Mars years. Thermal infrared measurements were compared by convolving the TES data using the MCS spectral band passes. The MCS solar channel measurements were calibrated using Compact Reconnaissance Imaging Spectrometer for Mars observations to provide the proper gain factor (3.09 x 10(-3) W sr(-1) m(-2) mu m(-1)). The comparisons of the datasets show that day and night surface and atmospheric temperatures are within 3 K over the course of 5 martian years, after accounting for the local time differences. Any potential interannual variations in global average temperature are masked by calibration and modeling uncertainties. Previous work attributed apparent interannual global surface and atmospheric temperature variations to major dust storm activity; however, this variation has since been attributed to a calibration error in the TES dataset that has been corrected. MCS derived Lambert albedos are slightly higher than TES measurements acquired over the same season and locations. Most of this difference can be attributed to the spectral response functions of MCS and TES. Consistent with previous work, global albedo is highly variable (similar to 6%) and this variability must be taken into account when determining long term global trends. Vertical aerosol distributions were also derived from the calibrated MCS visible channel limb measurements, demonstrating the utility of the MCS visible channel data for monitoring of aerosols. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Bandfield, Joshua L.] Univ Washington, Seattle, WA 98195 USA.
[Wolff, Michael J.] Space Sci Inst, Boulder, CO 80301 USA.
[Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Schofield, John T.; McCleese, Daniel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bandfield, JL (reprint author), Univ Washington, Seattle, WA 98195 USA.
EM joshband@u.washington.edu
FU MRO; JPL [130685]
FX We would like to thank the MGS and MRO spacecraft operations teams for
ensuring successful science investigations. J.-B. Madeleine and an
anonymous reviewer provided helpful and constructive comments that
significantly improved this manuscript. This work was partially funded
by the MRO Participating Scientist program and JPL Contract 130685 to
J.L.B.
NR 48
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U1 0
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 28
EP 39
DI 10.1016/j.icarus.2013.03.007
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800003
ER
PT J
AU Robbins, SJ
Hynek, BM
Lillis, RJ
Bottke, WF
AF Robbins, Stuart J.
Hynek, Brian M.
Lillis, Robert J.
Bottke, William F.
TI Large impact crater histories of Mars: The effect of different model
crater age techniques
SO ICARUS
LA English
DT Article
DE Mars; Cratering; Mars, Surface; Asteroids, Dynamics; Magnetic fields
ID INNER SOLAR-SYSTEM; MARTIAN HIGHLANDS; FLUVIAL PROCESSES; GALE CRATER;
EVOLUTION; BASINS; ORIGIN; STRATIGRAPHY; CONSTRAINTS
AB Impact events that produce large craters primarily occurred early in the Solar System's history because the largest bolides were remnants from planetary formation. Determining when large impacts occurred on a planetary surface such as Mars can yield clues to the flux of material in the early inner Solar System which, in turn, can constrain other planetary processes such as the timing and magnitude of resurfacing and the history of the martian core dynamo. We have used a large, global planetary database in conjunction with geomorphologic mapping to identify craters superposed on the rims of 78 larger craters with diameters D >= 150 km on Mars, approximate to 78% of which have not been previously dated in this manner. The densities of superposed craters with diameters larger than 10, 16, 25, and 50 km, as well as isochron fits were used to derive model crater ages of these larger craters and basins from which we derived an impact flux. In discussing these ages, we point out several internal inconsistencies of crater-age modeling techniques and chronology systems and, all told, we explain why we think isochron-fitting is the most reliable indicator of an age. Our results point to a mostly obliterated crater record prior to similar to 4.0 Ga with the oldest preserved mappable craters on Mars dating to similar to 4.3-4.35 Ga. We have used our results to constrain the cessation time of the martian core dynamo which we found to have occurred between the formation of Ladon and Prometheus basins, approximately 4.06-4.09 Ga. We also show that, overall, surfaces on Mars older than similar to 4.0-4.1 Ga have experienced >1 km of resurfacing, while those younger than similar to 3.8-3.9 Ga have experienced significantly less. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Robbins, Stuart J.; Hynek, Brian M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Hynek, Brian M.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Lillis, Robert J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bottke, William F.] SW Res Inst, Boulder, CO 80302 USA.
[Bottke, William F.] NASA, Lunar Sci Inst, Boulder, CO 80302 USA.
RP Robbins, SJ (reprint author), Univ Colorado, Atmospher & Space Phys Lab, 3665 Discovery Dr, Boulder, CO 80309 USA.
EM stuart.robbins@colorado.edu; hynek@lasp.color-ado.edu;
rlillis@ssl.berkeley.edu; bottke@boulder.swri.edu
RI Lillis, Robert/A-3281-2008
OI Lillis, Robert/0000-0003-0578-517X
FU NASA [NNX10AL65G]; MDAP [NNX11AI85G]; NASA's Lunar Science Institute
(Center for Lunar Origin and Evolution) [NNA09DB32A]; NSF's Planetary
Astronomy Program
FX Thanks to E.B. Bierhaus and H.V. Frey for providing detailed and helpful
comments on the manuscript. Support for Robbins and Hynek was through
NASA's Mars Data Analysis Program (MDAP) Award NNX10AL65G. Support for
Lillis was through MDAP Award NNX11AI85G. Support for Bottke was
provided by NASA's Lunar Science Institute (Center for Lunar Origin and
Evolution, Grant Number NNA09DB32A) and by NSF's Planetary Astronomy
Program.
NR 45
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U1 0
U2 14
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 173
EP 184
DI 10.1016/j.icarus.2013.03.019
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800015
ER
PT J
AU Bergonio, JR
Rottas, KM
Schorghofer, N
AF Bergonio, Justin R.
Rottas, Kimberly M.
Schorghofer, Norbert
TI Properties of martian slope streak populations
SO ICARUS
LA English
DT Article
DE Mars, Surface; Mars, Atmosphere; Geologic processes
ID MARS; DUST
AB Slope streaks are down-slope mass movements on the surface of Mars that are among the few known examples of contemporary geologic activity on Mars. Here we study slope streak activity over three decades, based on overlapping images in the Lycus Sulci region taken by the Context Camera (CTX) 2007-2010 and the Viking Orbiter Camera in 1977. The number of disappeared slope streaks is nearly equal the number of newly formed slope streaks, suggesting the streak population is balanced. The turnover time of the population is estimated to be four decades. Slope streaks fade gradually over time, with islands of persistence. We also determine the number of observable slope streaks as a function of image resolution based on images by the High Resolution Imaging Science Experiment (HiRISE) camera, and find that the number of discernible slope streaks can increase rapidly with spatial resolution. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Bergonio, Justin R.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Rottas, Kimberly M.] Univ Hawaii, Dept Geol & Geophys, Honolulu, HI 96822 USA.
[Schorghofer, Norbert] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Schorghofer, Norbert] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
RP Schorghofer, N (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM norbert@hawaii.edu
RI Schorghofer, Norbert/A-1194-2007
FU NASA through the Mars Data Analysis Program [NNX09AH54G]; Space Grant
Consortium; Mars Data Analysis Program
FX This material is based upon work supported by NASA under Grant No.
NNX09AH54G issued through the Mars Data Analysis Program. K.M.R. and
J.R.B. were supported by the Space Grant Consortium. This research has
made use of the USGS Integrated Software for Imagers and Spectrometers
(ISIS).
NR 14
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Z9 7
U1 0
U2 5
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 194
EP 199
DI 10.1016/j.icarus.2013.03.023
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800017
ER
PT J
AU Wendt, L
Bishop, JL
Neukum, G
AF Wendt, Lorenz
Bishop, Janice L.
Neukum, Gerhard
TI Knob fields in the Terra Cimmeria/Terra Sirenum region of Mars:
Stratigraphy, mineralogy and morphology
SO ICARUS
LA English
DT Article
DE Mars, Surface; Mineralogy; Spectroscopy
ID ORBITER LASER ALTIMETER; CLAY-MINERALS; SPECTROSCOPY; HISTORY; ORIGIN;
CAMERA; BASIN; CRISM
AB We investigate the stratigraphy, morphology and mineralogy of five major knob fields in the region between Terra Cimmeria and Terra Sirenum on Mars based on HRSC, CTX, MOC and HiRISE imagery together with hyperspectral data from CRISM. The knob fields comprise Ariadnes Colles, Atlantis Chaos and Gorgonum Chaos and further, unnamed fields of mounds. They have been mapped in previous studies as Hesperian or Amazonian units and are located within the shoreline of the proposed "Eridania lake", the putative source of Ma'adim Vallis. The mounds contain Mg/Fe-bearing phyllosilicates and locally Al-rich phyllosilicates. Our geological mapping shows that the knob fields have a late Noachian age, which indicates later phyllosilicate formation than typically observed on Mars. The knob fields formed by alteration of the "Electris deposit", an airfall deposit possibly rich in basaltic glass (Grant, J.A., Schultz, P.H. [1990]. Icarus 84, 166-195), in local depressions, possibly in the Eridania lake. The spectroscopic detection of phyllosilicates here may indicate that liquid water persisted longer in this region than elsewhere on Mars. The knob fields are embayed by the Hesperian ridged plains. Numerous valleys carve into the ridged plains and document that the aqueous history of this region continued into the Hesperian and Amazonian. The study area is traversed by the Sirenum Fossae. These graben appear to post-date the aqueous activity in the study area except in the Gorgonum basin, where a lake developed after their formation. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Wendt, Lorenz; Neukum, Gerhard] Free Univ Berlin, Inst Geol Sci, Planetary Sci & Remote Sensing Grp, D-12249 Berlin, Germany.
[Bishop, Janice L.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Wendt, L (reprint author), Free Univ Berlin, Inst Geol Sci, Planetary Sci & Remote Sensing Grp, Malteserstr 74-100D, D-12249 Berlin, Germany.
EM lorenz.wendt@fu-berlin.de; jbishop@seti.org; gerhard.neukum@fu-berlin.de
FU German Space Agency (DLR Bonn) on behalf of the German Federal Ministry
of Economics and Technology [50QM1001]
FX We thank two anonymous reviewers for their constructive remarks and
comments, which helped improving the manuscript. The work has been
financially supported by the German Space Agency (DLR Bonn) Grant
50QM1001 "HRSC on Mars Express" on behalf of the German Federal Ministry
of Economics and Technology. We thank S. Walter from the Freie
Universitat Berlin for the processing of several datasets and mosaics.
NR 56
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 200
EP 215
DI 10.1016/j.icarus.2013.03.020
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800018
ER
PT J
AU Sinclair, JA
Irwin, PGJ
Fletcher, LN
Moses, JI
Greathouse, TK
Friedson, AJ
Hesman, B
Hurley, J
Merlet, C
AF Sinclair, J. A.
Irwin, P. G. J.
Fletcher, L. N.
Moses, J. I.
Greathouse, T. K.
Friedson, A. J.
Hesman, B.
Hurley, J.
Merlet, C.
TI Seasonal variations of temperature, acetylene and ethane in Saturn's
atmosphere from 2005 to 2010, as observed by Cassini-CIRS
SO ICARUS
LA English
DT Article
DE Abundances, Atmospheres; Atmospheres, Composition; Saturn, Atmosphere;
Atmospheres, Dynamics; Infrared observations
ID RESOLVED INFRARED OBSERVATIONS; QUASI-BIENNIAL OSCILLATION; MERIDIONAL
DISTRIBUTION; GENERAL-CIRCULATION; CIRS/CASSINI LIMB; THERMAL STRUCTURE;
STRATOSPHERE; TRANSPORT; SPECTROMETER; SCANS
AB Acetylene (C2H2) and ethane (C2H6) are by-products of complex photochemistry in the stratosphere of Saturn. Both hydrocarbons are important to the thermal balance of Saturn's stratosphere and serve as tracers of vertical motion in the lower stratosphere. Earlier studies of Saturn's hydrocarbons using Cassini-CIRS observations have provided only a snapshot of their behaviour. Following the vernal equinox in August 2009, Saturn's northern and southern hemispheres have entered spring and autumn, respectively, however the response of Saturn's hydrocarbons to this seasonal shift remains to be determined. In this paper, we investigate how the thermal structure and concentrations of acetylene and ethane have evolved with the changing season on Saturn. We retrieve the vertical temperature profiles and acetylene and ethane volume mixing ratios from Delta(nu) over tilde = 15.5 cm(-1) Cassini-CIRS observations. In comparing 2005 (solar longitude, L-s similar to 308 degrees), 2009 (L-s similar to 3 degrees) and 2010 (L-s similar to 15 degrees) results, we observe the disappearance of Saturn's warm southern polar hood with cooling of up to 17.1 K +/- 0.8 K at 1.1 mbar at high-southern latitudes. Comparison of the derived temperature trend in this region with a radiative climate model (Section 4 of Fletcher et al., 2010 and Greathouse et al. (2013, in preparation)) indicates that this cooling is radiative although dynamical changes in this region cannot be ruled out. We observe a 21 +/- 12% enrichment of acetylene and a 29 +/- 11% enrichment of ethane at 25 degrees N from 2005 to 2009, suggesting downwelling at this latitude. At 15 S, both acetylene and ethane exhibit a decrease in concentration of 6 +/- 11% and 17 +/- 9% from 2005 to 2010, respectively, which suggests upwelling at this latitude (though a statistically significant change is only exhibited by ethane). These implied vertical motions at 15 degrees S and 25 degrees N are consistent with a recently-developed global circulation model of Saturn's tropopause and stratosphere(Friedson and Moses, 2012), which predicts this pattern of upwelling and downwelling as a result of a seasonally-reversing Hadley circulation. Ethane exhibits a general enrichment at mid-northern latitudes from 2005 to 2009. As the northern hemisphere approaches summer solstice in 2017, this feature might indicate an onset of a meridional enrichment of ethane, as has been observed in the southern hemisphere during/after southern summer solstice. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Sinclair, J. A.; Irwin, P. G. J.; Fletcher, L. N.; Hurley, J.; Merlet, C.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England.
[Moses, J. I.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Greathouse, T. K.] SW Res Inst, San Antonio, TX 28510 USA.
[Friedson, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hesman, B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Sinclair, JA (reprint author), Univ Oxford, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England.
EM j.a.sinclair@atm.ox.ac.uk
RI Moses, Julianne/I-2151-2013; Fletcher, Leigh/D-6093-2011;
OI Moses, Julianne/0000-0002-8837-0035; Fletcher,
Leigh/0000-0001-5834-9588; Irwin, Patrick/0000-0002-6772-384X
FU Royal Society
FX UK authors acknowledge the STFC (Science and Technology Facilities
Council) who have made this study possible. Fletcher was supported by a
Royal Society research fellowship. We thank the Cassini-CIRS team for
their planning and calibration of this data. Many thanks also to
Sandrine Guerlet for providing results from limb observations in
2005/2006 and for also discussing unpublished results from limb
observations in 2010. We also thank both anonymous reviewers for their
helpful and constructive feedback of this study.
NR 39
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 257
EP 271
DI 10.1016/j.icarus.2013.03.011
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800023
ER
PT J
AU Lorenz, RD
Stiles, BW
Aharonson, O
Lucas, A
Hayes, AG
Kirk, RL
Zebker, HA
Turtle, EP
Neish, CD
Stofan, ER
Barnes, JW
AF Lorenz, Ralph D.
Stiles, Bryan W.
Aharonson, Oded
Lucas, Antoine
Hayes, Alexander G.
Kirk, Randolph L.
Zebker, Howard A.
Turtle, Elizabeth P.
Neish, Catherine D.
Stofan, Ellen R.
Barnes, Jason W.
CA Cassini RADAR Team
TI A global topographic map of Titan
SO ICARUS
LA English
DT Article
DE Titan; Geological processes
ID SHAPE; ALTIMETER; MARS
AB Cassini RADAR SARtopo and altimetry data are used to construct a global gridded 1 x 1 degrees elevation map, for use in Global Circulation Models, hydrological models and correlative studies. The data are sparse, and so most of the map domain (similar to 90%) is populated with interpolated values using a spline algorithm. The highest (similar to+520 m) gridded point observed is at 48 degrees S, 12 degrees W. The lowest point observed (similar to 1700 m below a 2575 km sphere) is at 59 degrees S, 317 degrees W: this may be a basin where liquids presently in the north could have resided in the past. If the deepest point were once a sea with the areal extent of present-day Ligeia Mare, it would be similar to 1000 m deep. We find four prominent topographic rises, each similar to 200 km wide, radar-bright and heavily dissected, distributed over a similar to 3000 km arc in the southeastern quadrant of Titan (similar to 40-60 degrees S, 15-150 degrees W). (C) 2013 Elsevier Inc. All rights reserved.
C1 [Lorenz, Ralph D.; Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
[Stiles, Bryan W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Aharonson, Oded] Weizmann Inst Sci, Helen Kimmel Ctr Planetary Sci, IL-76100 Rehovot, Israel.
[Lucas, Antoine] Univ Paris 07, Lab AIM, CNRS, CEA, F-91191 Gif Sur Yvette, France.
[Hayes, Alexander G.] Cornell Univ, Ithaca, NY 14853 USA.
[Kirk, Randolph L.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Zebker, Howard A.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
[Neish, Catherine D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stofan, Ellen R.] Proxemy Res, Rectortown, VA 20140 USA.
[Barnes, Jason W.] Univ Idaho, Moscow, ID 83844 USA.
RP Lorenz, RD (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM ralph.lorenz@jhuapl.edu
RI Barnes, Jason/B-1284-2009; Neish, Catherine/G-6321-2012; Lucas,
Antoine/A-9752-2009; Hayes, Alexander/P-2024-2014; Turtle,
Elizabeth/K-8673-2012; Lorenz, Ralph/B-8759-2016
OI Barnes, Jason/0000-0002-7755-3530; Lucas, Antoine/0000-0003-2192-4416;
Hayes, Alexander/0000-0001-6397-2630; Turtle,
Elizabeth/0000-0003-1423-5751; Lorenz, Ralph/0000-0001-8528-4644
FU NASA; European Space Agency (ESA); Italian Space Agency (ASI); NASA
[NNX13AH14G]
FX This work was supported by the Cassini/Huygens mission, which is a joint
endeavor of NASA, the European Space Agency (ESA), and the Italian Space
Agency (ASI) and is managed by JPL/Caltech under a contract with NASA.
RI, was supported by NASA Grant NNX13AH14G.
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 367
EP 377
DI 10.1016/j.icarus.2013.04.002
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800031
ER
PT J
AU Swain, M
Deroo, P
Tinetti, G
Hollis, M
Tessenyi, M
Line, M
Kawahara, H
Fujii, Y
Showman, AP
Yurchenko, SN
AF Swain, Mark
Deroo, Pieter
Tinetti, Giovanna
Hollis, Morgan
Tessenyi, Marcell
Line, Michael
Kawahara, Hajime
Fujii, Yuka
Showman, Adam P.
Yurchenko, Sergey N.
TI Probing the extreme planetary atmosphere of WASP-12b
SO ICARUS
LA English
DT Article
DE Extrasolar planets; Eclipses; Spectroscopy; Jovian planets; Atmospheres,
Composition
ID TRANSITING EXTRASOLAR PLANET; COLLISION-INDUCED ABSORPTION; SECONDARY
ECLIPSE; THERMAL EMISSION; BROWN DWARF; H-2 PAIRS; TEMPERATURE;
OPACITIES; SPECTRA; SPECTROSCOPY
AB We report near-infrared measurements of the terminator region transmission spectrum and dayside emission spectrum of the exoplanet WASP-12b obtained using the HST WFC3 instrument. The disk-average dayside brightness temperature averages about 2900 K, peaking to 3200 K around 1.46 mu m. We modeled a range of atmospheric cases for both the emission and transmission spectrum and confirm the recent finding by Crossfield et al. (Crossfield, L, Barman, T., Hansen, B., Tanaka, I., Kodama, T. [2012b]. arXiv: 1210.4836C) that there is no evidence for C/O > 1 in the atmosphere of WASP-12b. Assuming a physically plausible atmosphere, we find evidence that the presence of a number of molecules is consistent with the data, but the justification for inclusion of these opacity sources based on the Bayesian Information Criterion (BIC) is marginal. We also find the near-infrared primary eclipse light curve is consistent with small amounts of prolate distortion. As part of the calibration effort for these data, we conducted a detailed study of instrument systematics using 65 orbits of WFC3-IR grims observations. The instrument systematics are dominated by detector-related affects, which vary significantly depending on the detector readout mode. The 256 x 256 subarray observations of WASP-12 produced spectral measurements within 15% of the photon-noise limit using a simple calibration approach. Residual systematics are estimated to be <= 70 ppm. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Swain, Mark; Deroo, Pieter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tinetti, Giovanna; Hollis, Morgan; Tessenyi, Marcell; Yurchenko, Sergey N.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Line, Michael] CALTECH, Pasadena, CA 91106 USA.
[Kawahara, Hajime] Tokyo Metropolitan Univ, Dept Phys, Hachioji, Tokyo 1920397, Japan.
[Fujii, Yuka] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
[Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Swain, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Mark.R.Swain@jpl.nasa.gov
RI Yurchenko, Sergey/G-9929-2012;
OI Yurchenko, Sergey/0000-0001-9286-9501; Hollis,
Morgan/0000-0002-8058-9075; Tinetti, Giovanna/0000-0001-6058-6654;
Kawahara, Hajime/0000-0003-3309-9134
FU National Aeronautics and Space Administration; JSPS (Japan Society for
the Promotion of Science) [DC:23-6070, PD:22-5467]
FX The research described in this publication was carried out in part at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration. Y.F.
and H.K. are supported by JSPS (Japan Society for the Promotion of
Science) Fellowship for Research, DC:23-6070 and PD:22-5467,
respectively. We thank Nikku Madhusudhan for kindly providing the data
for a previously published theoretical model for comparison with these
observations. We are grateful to Rachel Akeson and Thomas Green for
useful discussions and suggestions on improving the manuscript.
Copyright 2012. All rights reserved.
NR 36
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 432
EP 445
DI 10.1016/j.icarus.2013.04.003
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800037
ER
PT J
AU Kelley, MS
Fernandez, YR
Licandro, J
Lisse, CM
Reach, WT
A'Hearn, MF
Bauer, J
Campins, H
Fitzsimmons, A
Groussin, O
Lamy, PL
Lowry, SC
Meech, KJ
Pittichova, J
Snodgrass, C
Toth, I
Weaver, HA
AF Kelley, Michael S.
Fernandez, Yanga R.
Licandro, Javier
Lisse, Carey M.
Reach, William T.
A'Hearn, Michael F.
Bauer, James
Campins, Humberto
Fitzsimmons, Alan
Groussin, Olivier
Lamy, Philippe L.
Lowry, Stephen C.
Meech, Karen J.
Pittichova, Jana
Snodgrass, Colin
Toth, Imre
Weaver, Harold A.
TI The persistent activity of Jupiter-family comets at 3-7 AU
SO ICARUS
LA English
DT Article
DE Comets; Comets, Dust; Comets, Coma; Infrared observations
ID SPITZER-SPACE-TELESCOPE; SHORT-PERIOD COMETS; DEEP IMPACT; 103P/HARTLEY
2; SOLAR-SYSTEM; INNER COMA; NUCLEI; DUST; 9P/TEMPEL-1; PHOTOMETRY
AB We present an analysis of comet activity based on the Spitzer Space Telescope component of the Survey of the Ensemble Physical Properties of Cometary Nuclei. We show that the survey is well suited to measuring the activity of Jupiter-family comets at 3-7 AU from the Sun. Dust was detected in 33 of 89 targets (37 +/- 6%), and we conclude that 21 comets (24 +/- 5%) have morphologies that suggest ongoing or recent cometary activity. Our dust detections are sensitivity limited, therefore our measured activity rate is necessarily a lower limit. All comets with small perihelion distances (q < 1.8 AU) are inactive in our survey, and the active comets in our sample are strongly biased to post-perihelion epochs. We introduce the quantity epsilon f rho, intended to be a thermal emission counterpart to the often reported Af rho, and find that the comets with large perihelion distances likely have greater dust production rates than other comets in our survey at 3-7 AU from the Sun, indicating a bias in the discovered Jupiter-family comet population. By examining the orbital history of our survey sample, we suggest that comets perturbed to smaller perihelion distances in the past 150 yr are more likely to be active, but more study on this effect is needed. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Kelley, Michael S.; A'Hearn, Michael F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kelley, Michael S.; Fernandez, Yanga R.; Campins, Humberto] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Licandro, Javier] Inst Astrofis Canarias, Tenerife 38205, Spain.
[Lisse, Carey M.; Weaver, Harold A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Reach, William T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA.
[Bauer, James] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fitzsimmons, Alan] Queens Univ Belfast, Astrophys Res Ctr, Sch Phys & Astron, Belfast BT7 1NN, Antrim, North Ireland.
[Groussin, Olivier; Lamy, Philippe L.] Aix Marseille Univ, CNRS, LAM UMR 7326, F-13388 Marseille, France.
[Lowry, Stephen C.] Univ Kent, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England.
[Meech, Karen J.; Pittichova, Jana] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Snodgrass, Colin] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Toth, Imre] Konkoly Observ Budapest, H-1525 Budapest, Hungary.
RP Kelley, MS (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM msk@astro.umd.edu; yfernandez@physics.ucf.edu
RI Weaver, Harold/D-9188-2016; Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Fernandez, Yanga/0000-0003-1156-9721;
Kelley, Michael/0000-0002-6702-7676; Reach, William/0000-0001-8362-4094;
Snodgrass, Colin/0000-0001-9328-2905
FU NASA; NASA through JPL/Caltech; European Union [268421]
FX The authors appreciate Paul Weissman's careful review of our manuscript.
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, in part, provided by NASA through an award issued by
JPL/Caltech. CS has received funding from the European Union Seventh
Framework Programme (FP7/2007-2013) under Grant Agreement No. 268421.
NR 61
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 475
EP 494
DI 10.1016/j.icarus.2013.04.012
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800039
ER
PT J
AU Diniega, S
Hansen, CJ
McElwaine, JN
Hugenholtz, CH
Dundas, CM
McEwen, AS
Bourke, MC
AF Diniega, S.
Hansen, C. J.
McElwaine, J. N.
Hugenholtz, C. H.
Dundas, C. M.
McEwen, A. S.
Bourke, M. C.
TI A new dry hypothesis for the formation of martian linear gullies
SO ICARUS
LA English
DT Article
DE Mars, Surface; Geological processes; Ices
ID DEBRIS FLOWS; SAND DUNES; MARS; WATER; DEPTH
AB Long, narrow grooves found on the slopes of martian sand dunes have been cited as evidence of liquid water via the hypothesis that melt-water initiated debris flows eroded channels and deposited lateral levees. However, this theory has several short-comings for explaining the observed morphology and activity of these linear gullies. We present an alternative hypothesis that is consistent with the observed morphology, location, and current activity: that blocks of CO2 ice break from over-steepened cornices as sublimation processes destabilize the surface in the spring, and these blocks move downslope, carving out leveed grooves of relatively uniform width and forming terminal pits. To test this hypothesis, we describe experiments involving water and CO2 blocks on terrestrial dunes and then compare results with the martian features. Furthermore, we present a theoretical model of the initiation of block motion due to sublimation and use this to quantitatively compare the expected behavior of blocks on the Earth and Mars. The model demonstrates that CO2 blocks can be expected to move via our proposed mechanism on the Earth and Mars, and the experiments show that the motion of these blocks will naturally create the main morphological features of linear gullies seen on Mars. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Diniega, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hansen, C. J.; McElwaine, J. N.; Bourke, M. C.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[McElwaine, J. N.] SLF WSL, CH-2740 Davos, Switzerland.
[Hugenholtz, C. H.] Univ Lethbridge, Dept Geog, Lethbridge, AB T1K 3M4, Canada.
[Hugenholtz, C. H.] Univ Calgary, Fac Environm Design, Calgary, AB T2N 1N4, Canada.
[Dundas, C. M.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[McEwen, A. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Bourke, M. C.] Univ Dublin Trinity Coll, Dept Geog, Sch Nat Sci, Dublin 2, Ireland.
RP Diniega, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-250D, Pasadena, CA 91109 USA.
EM serina.diniega@jpl.nasa.gov
RI Bourke, Mary/I-4387-2012;
OI Bourke, Mary/0000-0002-0424-0322; Dundas, Colin/0000-0003-2343-7224
FU NASA
FX Diniega was supported by an appointment to the NASA Postdoctoral
Program, administered by Oak Ridge Associated Universities, at the
California Institute of Technology Jet Propulsion Laboratory under a
contract with NASA.
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 526
EP 537
DI 10.1016/j.icarus.2013.04.006
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800043
ER
PT J
AU Klaasen, KP
A'Hearn, M
Besse, S
Bodewits, D
Carcich, B
Farnham, T
Feaga, L
Groussin, O
Hampton, D
Huisjen, M
Kelley, MS
McLaughlin, S
Merlin, F
Protopapa, S
Sunshine, J
Thomas, P
Wellnitz, D
AF Klaasen, Kenneth P.
A'Hearn, Michael
Besse, Sebastian
Bodewits, Dennis
Carcich, Brian
Farnham, Tony
Feaga, Lori
Groussin, Olivier
Hampton, Donald
Huisjen, Marty
Kelley, Michael S.
McLaughlin, Stephanie
Merlin, Frederic
Protopapa, Silvia
Sunshine, Jessica
Thomas, Peter
Wellnitz, Dennis
TI EPOXI instrument calibration
SO ICARUS
LA English
DT Article
DE Instrumentation; Data reduction techniques; Infrared observations
ID STELLAR SPECTRA; MISSION
AB NASA's EPOXI mission used the Deep Impact (DI) Flyby spacecraft to deliver a payload of three scientific instruments, two visible cameras and an IR spectrometer, to a close flyby of Comet 103P/Hartley 2 in November 2010. Interpretation of the scientific measurements made using these instruments depends on accurate calibration of the instruments' performance. Updates to the instrument calibrations achieved during the Deep Impact primary mission and results of continued monitoring of their performance during EPOXI are reported here. The instruments' performance has remained remarkably stable over the nearly 7 years of flight. Significant improvements in the understanding and calibration of the IR spectrometer response non-linearity, time-varying background level, flat field, wavelength map, and absolute spectral response have been achieved. Techniques for reducing some semi-coherent horizontal noise stripes in the visible cameras' readouts were developed, and some adjustments have been made to their absolute radiometric conversion constants. The data processing pipeline has been updated to incorporate the improvements in the instrument calibrations. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Klaasen, Kenneth P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[A'Hearn, Michael; Besse, Sebastian; Bodewits, Dennis; Farnham, Tony; Feaga, Lori; Kelley, Michael S.; McLaughlin, Stephanie; Merlin, Frederic; Protopapa, Silvia; Sunshine, Jessica; Wellnitz, Dennis] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Carcich, Brian; Thomas, Peter] Cornell Univ, Ithaca, NY 14853 USA.
[Groussin, Olivier] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Hampton, Donald] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Huisjen, Marty] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA.
RP Klaasen, KP (reprint author), CALTECH, Jet Prop Lab, Mail Stop 306-392,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kenneth.p.klaasen@jpl.nasa.gov
OI Kelley, Michael/0000-0002-6702-7676; Bodewits,
Dennis/0000-0002-2668-7248; Besse, Sebastien/0000-0002-1052-5439
FU National Aeronautics and Space Administration [NNM07AA99C]; Centre
National d'Etudes Spatiales (CNES) in France; [NMO711002]
FX This work was supported by National Aeronautics and Space
Administration's Discovery Program through Contract NNM07AA99C to the
University of Maryland and by task order NMO711002 to the Jet Propulsion
Laboratory, California Institute of Technology. The contributions of O.
Groussin and F. Merlin to this project were funded by the Centre
National d'Etudes Spatiales (CNES) in France. We appreciate the data
processing contributions of David Brown, Peter Kim, Nick Mastrodemos,
Nelly Mouawad, and Brian Prager and the Project flight team efforts of
Tim Larson, Al Nakata, Steve Wissler, Greg LaBorde, Rich Rieber, Steve
Collins, and Amy Walsh in collecting the data. Valuable review comments
were provided by Dr. David Humm of the Applied Physics Lab.
NR 18
TC 5
Z9 5
U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 643
EP 680
DI 10.1016/j.icarus.2013.03.024
PG 38
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800053
ER
PT J
AU Farrand, WH
Bell, JF
Johnson, JR
Rice, MS
Hurowitz, JA
AF Farrand, William H.
Bell, James F., III
Johnson, Jeffrey R.
Rice, Melissa S.
Hurowitz, Joel A.
TI VNIR multispectral observations of rocks at Cape York, Endeavour crater,
Mars by the Opportunity rover's Pancam
SO ICARUS
LA English
DT Article
DE Mars; Mars, Surface; Spectroscopy
ID MERIDIANI-PLANUM; SPECTROMETER
AB From its arrival at the portion of the rim of Endeavour crater known informally as Cape York, the Mars Exploration Rover Opportunity has made numerous visible and near infrared (VNIR) multispectral observations of rock surfaces. This paper describes multispectral observations from Opportunity's arrival at Cape York to its winter-over location at Greeley Haven. Averages of pixels from the Pancam's left and right eyes were joined to form 11 point spectra from numerous observations and were examined via a number of techniques. These included principal components analysis, a sequential maximum angle convex cone approach, examination of spectral parameters, and a hierarchical clustering approach. The end result of these analyses was the determination of six primary spectral (PS) classes describing spectrally unique materials observed on Cape York. These classes consisted of a "standard" outcrop spectrum that was observed on the clasts and matrix comprising the upper unit of the Shoemaker formation, a class representing rock surfaces exposed around Odyssey crater and typified by the rocks of the Tisdale series, pebbles occurring in and weathered out of the upper unit of the Shoemaker formation that appear red in 1009, 904, 754 nm color composites, patches on Tisdale rocks exhibiting a 864 nm band minimum that were spectrally anomalous in root mean square error images derived from spectral mixture analyses, clasts with a high 904 nm band depth occurring in the Greeley Haven location, and gypsum veins typified by the vein Homestake. Comparisons of three of these classes that had well defined band minima between 800 and 1009 nm with spectral library spectra of ferrous silicates and ferric oxide, oxyhydroxide and ferric sulfate minerals indicated tentative matches of the "red" pebbles with orthopyroxenes, of the spectrally anomalous 864 nm band minimum material with hematite or ferric sulfates, and of the high 904 nm band depth material with an orthopyroxene-clinopyroxene mixture. The spectral properties of rock surfaces on Cape York are distinct from those of Burns Formation outcrops observed on the Meridiani Plains. The Cape York outcrop is Noachian in age and study of these materials provides insight into less acidic environmental conditions extant before the formation of the Burns Formation. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Farrand, William H.] Space Sci Inst, Boulder, CO 80031 USA.
[Bell, James F., III] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Johnson, Jeffrey R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Rice, Melissa S.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Hurowitz, Joel A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Farrand, WH (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80031 USA.
EM farrand@spacescience.org
RI Johnson, Jeffrey/F-3972-2015
FU NASA through Cornell University; Jet Propulsion Laboratory
FX Funding for Athena science team members was provided by NASA contracts
through Cornell University and the Jet Propulsion Laboratory. We are
grateful to helpful reviews by Edward Cloutis and Eldar Noe Dobrea.
NR 21
TC 7
Z9 7
U1 1
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 709
EP 725
DI 10.1016/j.icarus.2013.04.014
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800057
ER
PT J
AU Rampe, EB
Kraft, MD
Sharp, TG
AF Rampe, Elizabeth B.
Kraft, Michael D.
Sharp, Thomas G.
TI Deriving chemical trends from thermal infrared spectra of weathered
basalt: Implications for remotely determining chemical trends on Mars
SO ICARUS
LA English
DT Article
DE Infrared observations; Mars, Surface; Mineralogy; Regoliths;
Spectroscopy
ID EMISSION SPECTROMETER DATA; MINI-TES EXPERIMENT; MERIDIANI-PLANUM;
MARTIAN SURFACE; SPIRIT ROVER; GUSEV CRATER; MINERALOGY; SPECTROSCOPY;
CHEMISTRY; SILICA
AB Variations in chemical composition over a planetary surface can be used to study petrologic and aqueous alteration processes. The desire for such data on Mars has prompted investigators to derive chemistry from models of Thermal Emission Spectrometer data. Although chemistry derived from thermal infrared spectral models is reportedly reliable for unaltered igneous rocks, the martian surface has experienced chemical weathering, which can adversely affect models. Here, we examine weathered basalts from Baynton, Australia, for which chemical weathering trends have been previously characterized, to test how well chemistry and chemical trends can be determined from TIR spectra of weathered rocks. The mineralogy of variably weathered rocks was derived from TIR spectra by linear mixing, and major-element chemistry was calculated from those mineral models. Derived chemistries and trends were compared to those measured by X-ray fluorescence. TIR spectroscopy is sensitive to weathering products in weathering rinds because the products are present in a coating geometry, making it a useful technique for remotely detecting weathered surfaces on planetary surfaces such as Mars. This sensitivity results in significant modeled abundances of weathering products (>80% of all phases) from TIR spectra of weathered Baynton surfaces, despite evidence from microscopy and X-ray diffraction showing that igneous minerals dominate the weathering rind. Measured chemical weathering trends show loss of MgO, CaO, Na2O, and K2O and relative enrichment in Al2O3 and FeOT. The modeled trends are similar to the measured trends, but a closer look at the modeled oxide abundances demonstrates that most oxides (i.e., alkalis, SiO2, and FeOT) are not well modeled, especially for weathered surfaces. The reasons for this are: (1) non-linear mixing and the presence of secondary coatings causes the overestimation of secondary phases in spectral models, and (2) spectral libraries generally lack poorly crystalline and amorphous secondary phases that are common in weathering rinds so that crystalline phases such as phyllosilicates are selected. The martian surface has likely been weathered less pervasively than the Baynton rocks and, therefore, weathering products may be dominated by poorly crystalline and amorphous phases, rather than crystalline phyllosilicates. Adding these phases to spectral libraries could improve bulk chemistry derived from the martian surface; however, if the secondary phases are present in a coating geometry, the derived chemistry will reflect the composition of the coating, and it may be difficult to infer the chemistry of the parent rock. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Rampe, Elizabeth B.] NASA, Lyndon B Johnson Space Ctr, ARES Mail Code KA, Houston, TX 77058 USA.
[Rampe, Elizabeth B.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Kraft, Michael D.; Sharp, Thomas G.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Rampe, EB (reprint author), NASA, Lyndon B Johnson Space Ctr, ARES Mail Code KA, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM elizabeth.b.rampe@nasa.gov
FU NASA GSRP [NNX07AP11H]
FX We gratefully acknowledge Phil Christensen and the Mars Space Flight
Facility for the use of the TIR emission spectrometer, the LeRoy Eyring
Center for Solid State Science at Arizona State University and Emmanuel
Soignard for the use of the XRD, Anne Piesler and Lone Li at NASA
Johnson Space Center for help on the electron microprobe and sample
preparation, and Allan Treiman at the Lunar and Planetary Institute for
the use of the petrographic microscope. We thank Deanne Rogers for
providing a spectral library and Cheryl Replogle for her dedicated work
in the laboratory. Many people have added to this manuscript by
thoughtful discussions, including Deanne Rogers, Phil Christensen, Rick
Hervig, Everett Shock, and Lynda Williams. We thank Katie Alexander,
Deanne Rogers, Joseph Michalski, and two anonymous reviewers for their
comments on this manuscript. This work was funded by NASA GSRP Grant
NNX07AP11H.
NR 66
TC 2
Z9 2
U1 0
U2 8
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUL
PY 2013
VL 225
IS 1
BP 749
EP 762
DI 10.1016/j.icarus.2013.05.005
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 174ND
UT WOS:000321161800060
ER
PT J
AU Johnson, SM
Madsen, LD
Freiman, S
AF Johnson, Sylvia M.
Madsen, Lynnette D.
Freiman, Stephen
TI Nanoscale Ceramics: Environmental, Health, and Safety (EHS) Implications
SO INTERNATIONAL JOURNAL OF APPLIED CERAMIC TECHNOLOGY
LA English
DT Article
ID MONOCYTE-DERIVED CELLS; ATHEROSCLEROSIS; EMIGRATION; SILICA
AB Part of the symposium on Nanostructured Materials at the Fourth International Congress on Ceramics (ICC4) dealt with health aspects related to these materials. Major issues discussed included definitions and measurements of nanoparticles, best test protocols, collaboration and communication between, for example, materials scientists and biologists, and the plethora of information and regulations (that is sometimes even conflicting). Emerging opportunities were identified in terms of obtaining uniformity of nomenclature and testing standards, education and training of a new generation of multidisciplinary researchers, and understanding and then fully exploiting the positive aspects of nanomaterials, including improvements to human health.
C1 [Johnson, Sylvia M.] NASA, Ames Res Ctr, Moffett Field, CA 94610 USA.
[Madsen, Lynnette D.] Natl Sci Fdn, Div Mat Res, Arlington, VA 22230 USA.
[Freiman, Stephen] Freiman Consulting, Potomac, MD 20854 USA.
RP Johnson, SM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94610 USA.
EM sylvia.m.johnson@nasa.gov
RI Madsen, Lynnette/F-8323-2012
OI Madsen, Lynnette/0000-0001-5449-4825
NR 11
TC 1
Z9 1
U1 1
U2 13
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1546-542X
J9 INT J APPL CERAM TEC
JI Int. J. Appl. Ceram. Technol.
PD JUL
PY 2013
VL 10
IS 4
BP 577
EP 583
DI 10.1111/ijac.12079
PG 7
WC Materials Science, Ceramics
SC Materials Science
GA 173UL
UT WOS:000321106400002
ER
PT J
AU Mosier, KL
Rettenmaier, P
McDearmid, M
Wilson, J
Mak, S
Raj, L
Orasanu, J
AF Mosier, Kathleen L.
Rettenmaier, Paula
McDearmid, Matthew
Wilson, Jordan
Mak, Stanton
Raj, Lakshmi
Orasanu, Judith
TI Pilot-ATC Communication Conflicts: Implications for NextGen
SO INTERNATIONAL JOURNAL OF AVIATION PSYCHOLOGY
LA English
DT Article
ID DECISION-MAKING; ANGER
AB In the planned NextGen aviation operations, it will be critical to ensure shared situational understanding and cooperative problem solving between aircrews and air traffic controllers (ATC). A first step in predicting how future changes will impact flight crews and ATC is to examine the current system and to pinpoint problematic areas that could be ameliorated or exacerbated by advanced automation and heavier traffic density. In this study, we coded Aviation Safety Reporting System (ASRS) reports identified as having communication conflicts between pilots and ATC. Results describe types of conflict, operational context, phase of flight, operator states, and situations conducive to communication conflicts, risk perception differences, and inappropriate resolution strategies. Reports suggest that high workload approach and landing phases are conducive to communication conflicts, that different interpretations of the same information might lead to conflict, and that operator state could impact communication and collaboration between flight crews and ATC. A specific problem was noted when reporters felt that the affective response of the other party was not appropriate to the situation. Although this study reflects the limitations inherent in ASRS data, it can provide insights into potential problem areas and conflict triggers in NextGen operations. This research will enable us to better predict NextGen aircrew-ATC communication breakdowns and conflicts resulting from specific situations or operator states.
C1 [Mosier, Kathleen L.; Rettenmaier, Paula; McDearmid, Matthew; Wilson, Jordan; Mak, Stanton; Raj, Lakshmi] San Francisco State Univ, Dept Psychol, San Francisco, CA 94132 USA.
[Orasanu, Judith] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Mosier, KL (reprint author), San Francisco State Univ, Dept Psychol, 1600 Holloway Ave, San Francisco, CA 94132 USA.
EM kmosier@sfsu.edu
NR 22
TC 1
Z9 2
U1 1
U2 7
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 1050-8414
J9 INT J AVIAT PSYCHOL
JI Int. J. Aviat. Psychol.
PD JUL 1
PY 2013
VL 23
IS 3
BP 213
EP 226
DI 10.1080/10508414.2013.799350
PG 14
WC Psychology, Applied
SC Psychology
GA 175NN
UT WOS:000321237500002
ER
PT J
AU Pineda, EJ
Waas, AM
AF Pineda, Evan J.
Waas, Anthony M.
TI Numerical implementation of a multiple-ISV thermodynamically-based work
potential theory for modeling progressive damage and failure in
fiber-reinforced laminates
SO INTERNATIONAL JOURNAL OF FRACTURE
LA English
DT Article
ID FINITE-ELEMENT-ANALYSIS; THERMOMECHANICAL CONSTITUTIVE THEORY; CROSS-PLY
LAMINATE; MATRIX CRACKING; ANISOTROPIC DAMAGE; PHENOMENOLOGICAL MODELS;
VARIATIONAL APPROACH; STIFFNESS REDUCTION; TRANSVERSE CRACKING;
COMPOSITE-MATERIALS
AB A thermodynamically-based work potential theory for modeling progressive damage and failure in fiber-reinforced laminates is presented. The current, multiple-internal state variable (ISV) formulation, referred to as enhanced Schapery theory, utilizes separate ISVs for modeling the effects of damage and failure. Damage is considered to be the effect of any structural changes in a material that manifest as pre-peak non-linearity in the stress versus strain response. Conversely, failure is taken to be the effect of the evolution of any mechanisms that results in post-peak strain softening, resulting in a negative tangent stiffness. It is assumed that matrix microdamage is the dominant damage mechanism in continuous fiber-reinforced polymer matrix laminates, and its evolution is controlled with a single ISV. Three additional ISVs are introduced to account for failure due to mode I transverse cracking, mode II transverse cracking, and mode I axial failure. Typically, failure evolution (i.e., post-peak strain softening characterized through a negative tangent stiffness) results in pathologically mesh dependent solutions within a finite element (FE) framework. Therefore, consistent characteristic lengths are introduced into the formulation to govern the evolution of the three failure ISVs. Using the stationarity of the total work potential with respect to each ISV, a set of thermodynamically consistent evolution equations for the ISVs are derived. The theory is implemented in association with the commercial FE software, Abaqus. Objectivity of total energy dissipated during the failure process, with regards to refinements in the FE mesh, is demonstrated. The model is also verified against experimental results from two laminated, T800/3900-2 panels containing a central notch and different fiber-orientation stacking sequences. Global load versus displacement, global load versus local strain gage data, and macroscopic failure paths obtained from the models are compared against the experimental results.
C1 [Pineda, Evan J.] NASA, Glenn Res Ctr, Mech & Life Predict Branch, Cleveland, OH 44135 USA.
[Waas, Anthony M.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
[Waas, Anthony M.] Univ Michigan, Dept Mech Engn, Ann Arbor, MI 48109 USA.
RP Waas, AM (reprint author), Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
EM evan.j.pineda@nasa.gov; dcw@umich.edu
NR 118
TC 14
Z9 14
U1 1
U2 19
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0376-9429
J9 INT J FRACTURE
JI Int. J. Fract.
PD JUL
PY 2013
VL 182
IS 1
BP 93
EP 122
DI 10.1007/s10704-013-9860-1
PG 30
WC Materials Science, Multidisciplinary; Mechanics
SC Materials Science; Mechanics
GA 179MO
UT WOS:000321524600006
ER
PT J
AU Cook, BI
Seager, R
Miller, RL
Mason, JA
AF Cook, Benjamin I.
Seager, Richard
Miller, Ron L.
Mason, Joseph A.
TI Intensification of North American Megadroughts through Surface and Dust
Aerosol Forcing
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Atmosphere-land interaction; Drought; Paleoclimate; Dust or dust storms
ID EL-NINO/SOUTHERN-OSCILLATION; HOLOCENE DUNE ACTIVITY; CENTRAL
GREAT-PLAINS; NEBRASKA SAND HILLS; TROPICAL PACIFIC; LAST MILLENNIUM;
UNITED-STATES; CLIMATE SIMULATIONS; MEDIEVAL DROUGHT; SOIL-MOISTURE
AB Tree-ring-based reconstructions of the Palmer drought severity index (PDSI) indicate that, during the Medieval Climate Anomaly (MCA), the central plains of North America experienced recurrent periods of drought spanning decades or longer. These megadroughts had exceptional persistence compared to more recent events, but the causes remain uncertain. The authors conducted a suite of general circulation model experiments to test the impact of sea surface temperature (SST) and land surface forcing on the MCA megadroughts over the central plains. The land surface forcing is represented as a set of dune mobilization boundary conditions, derived from available geomorphological evidence and modeled as increased bare soil area and a dust aerosol source (32 degrees-44 degrees N, 105 degrees-95 degrees W). In the experiments, cold tropical Pacific SST forcing suppresses precipitation over the central plains but cannot reproduce the overall drying or persistence seen in the PDSI reconstruction. Droughts in the scenario with dust aerosols, however, are amplified and have significantly longer persistence than in other model experiments, more closely matching the reconstructed PDSI. This additional drying occurs because the dust increases the shortwave planetary albedo, reducing energy inputs to the surface and boundary layer. The energy deficit increases atmospheric stability, inhibiting convection and reducing cloud cover and precipitation over the central plains. Results from this study provide the first model-based evidence that dust aerosol forcing and land surface changes could have contributed to the intensity and persistence of the central plains megadroughts, although uncertainties remain in the formulation of the boundary conditions and the future importance of these feedbacks.
C1 [Cook, Benjamin I.; Miller, Ron L.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Cook, Benjamin I.; Seager, Richard] Lamont Doherty Earth Observ, Palisades, NY USA.
[Miller, Ron L.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Mason, Joseph A.] Univ Wisconsin, Madison, WI USA.
RP Cook, BI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM benjamin.i.cook@nasa.gov
RI Miller, Ron/E-1902-2012; Cook, Benjamin/H-2265-2012
FU National Aeronautics and Space Administration (NASA) High-End Computing
(HEC) Program through the NASA Center for Climate Simulation (NCCS) at
Goddard Space Flight Center; NSF Grant [ATMO9-02716, ATM-06-20066]; NOAA
Grant [NA100AR-4310137]; NASA Atmospheric Composition Program; NASA
Modeling, Analysis and Prediction (MAP) Program
FX Resources supporting this work were provided by the National Aeronautics
and Space Administration (NASA) High-End Computing (HEC) Program through
the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight
Center. The authors acknowledge the support of NSF Grant ATMO9-02716;
NOAA Grant NA100AR-4310137; NSF Grant ATM-06-20066; the NASA Atmospheric
Composition Program; and the NASA Modeling, Analysis and Prediction
(MAP) Program. Jonathan Overpeck and one anonymous reviewer provided
feedback that greatly improved the quality of this manuscript.
NR 83
TC 10
Z9 10
U1 2
U2 46
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 JUL
PY 2013
VL 26
IS 13
BP 4414
EP 4430
DI 10.1175/JCLI-D-12-00022.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 175UL
UT WOS:000321259000003
ER
PT J
AU Brown, DR
Day, T
Caillat, T
Snyder, GJ
AF Brown, David R.
Day, Tristan
Caillat, Thierry
Snyder, G. Jeffrey
TI Chemical Stability of (Ag,Cu)(2)Se: a Historical Overview
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article
ID SELENIDE; COPPER
AB Recent work on Cu2-x Se has caused strong interest in this material due to its high reported peak zT (1.5) and the reduction of thermal conductivity through the mechanism of liquid-like suppression of heat capacity. In the 1960s, 3M patented Cu1.97Ag0.03Se as "TPM-217." Over the following decade it was tested and developed by the 3M Corporation, at the National Aeronautics and Space Administration (NASA) Jet Propulsion Laboratory, Teledyne Energy Systems, and the General Atomics Corporation for use as a next-generation thermoelectric material. During these tests, extreme problems with material loss through Se vaporization and chemical reactions between the material and the device contacts were found. These problems were especially severe while operating under conditions of high As a result, the material system was abandoned. The results of these reports are discussed. A simple test of degradation of Cu2Se under conditions of applied current and thermal gradient was performed and showed results compatible with the work done by General Atomics.
C1 [Brown, David R.; Day, Tristan; Snyder, G. Jeffrey] CALTECH, Dept Appl Phys & Mat Sci, Pasadena, CA 91125 USA.
[Caillat, Thierry] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Brown, DR (reprint author), CALTECH, Dept Appl Phys & Mat Sci, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
EM db@caltech.edu
RI Snyder, G. Jeffrey/E-4453-2011; Snyder, G/I-2263-2015
OI Snyder, G. Jeffrey/0000-0003-1414-8682;
FU Resnick Institute; Air Force Office of Science Research
FX D.R.B. would like to acknowledge the support of the Resnick Institute.
T.D. and G.J.S. would like to acknowledge the support of the Air Force
Office of Science Research. Part of this work was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 21
TC 26
Z9 26
U1 5
U2 99
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD JUL
PY 2013
VL 42
IS 7
BP 2014
EP 2019
DI 10.1007/s11664-013-2506-2
PG 6
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA 170YJ
UT WOS:000320890800116
ER
PT J
AU Mondelo, JM
Broschart, SB
Villac, BF
AF Mondelo, Josep-Maria
Broschart, Stephen B.
Villac, Benjamin F.
TI Ballistic Transfers Across the 1: 1 Resonance Around Vesta Following
Invariant Manifolds
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT AIAA/AAS Astrodynamics Specialist Conference
CY AUG 02-05, 2010
CL Toronto, CANADA
SP Amer Inst Aeronaut & Astronaut (AIAA), Amer Astronaut Soc (AAS)
ID RESTRICTED 3-BODY PROBLEM; PERIODIC-ORBITS; EXPLORATION; ASTEROIDS;
DYNAMICS; DAWN
AB Motivated by the challenging crossing of the 1 : 1 resonance planned for the Dawn mission a general transfer design strategy is developed using the manifold structure of near-synchronous, unstable periodic orbits. Two families of transfers across the 1 : 1 resonance at the asteroid Vesta demonstrate the approach. A family of low-inclination low-energy transfers follows the stable and unstable manifolds of the libration orbits near Vesta's equilibrium points (in a surface-fixed rotating frame). A high-inclination family of transfers arises similarly from the manifold structure of near-polar near-circular orbits. Ballistic resonance, crossing transfers near Vesta are presented and characterized. This transfer design methodology applies well to any solar system body where the dynamics are dominated by gravitational acceleration from a nonspherical central-body potential.
C1 [Mondelo, Josep-Maria] Univ Autonoma Barcelona, Dept Matemat, E-08193 Barcelona, Spain.
[Mondelo, Josep-Maria] Univ Autonoma Barcelona, Inst Estudis Espacials Catalunya, E-08193 Barcelona, Spain.
[Broschart, Stephen B.] CALTECH, Jet Prop Lab, Nav & Mission Design Sect, Pasadena, CA 91109 USA.
[Villac, Benjamin F.] Univ Calif Irvine, Irvine, CA 92697 USA.
RP Mondelo, JM (reprint author), Univ Autonoma Barcelona, Dept Matemat, E-08193 Barcelona, Spain.
EM jmm@mat.uab.cat; Stephen.B.Broschart@jpl.nasa.gov; bvillac@uci.edu
NR 21
TC 2
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U1 1
U2 7
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 JUL-AUG
PY 2013
VL 36
IS 4
BP 1119
EP 1133
DI 10.2514/1.57494
PG 15
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 179PY
UT WOS:000321535000018
ER
PT J
AU Barber, ZW
Dahl, JR
Sharpe, TL
Erkmen, BI
AF Barber, Zeb W.
Dahl, Jason R.
Sharpe, Tia L.
Erkmen, Baris I.
TI Shot noise statistics and information theory of sensitivity limits in
frequency-modulated continuous-wave ladar
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA A-OPTICS IMAGE SCIENCE AND
VISION
LA English
DT Article
ID LASER; LIDAR
AB A theoretical analysis and experimental verification of the sensitivity limits of frequency-modulated continuous-wave (FMCW) ladar in the limit of a strong local oscillator is presented. The single-photon sensitivity of coherent heterodyne detection in this shot-noise dominated limit is verified to extend to linearly chirped waveforms. An information theoretic analysis is presented to estimate the information efficiency of received photons for the task of locating the range to single and multiple targets. It is found that the optimum receive signal level is proportional to the logarithm of the number of resolvable range locations and the maximum theoretical photon information efficiency for FMCW ranging with coherent fields is log(e) approximate to 1.44 bits per received photon. (C) 2013 Optical Society of America
C1 [Barber, Zeb W.; Dahl, Jason R.; Sharpe, Tia L.] Montana State Univ, Spectrum Lab, Bozeman, MT 59717 USA.
[Erkmen, Baris I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Barber, ZW (reprint author), Montana State Univ, Spectrum Lab, POB 173510, Bozeman, MT 59717 USA.
EM barber@spectrum.montana.edu
FU DARPA InPho program under Army Research Office grant at MSU
[W911NF-11-1-0540]
FX This work was performed as part of the DARPA InPho program under Army
Research Office grant W911NF-11-1-0540 at MSU and PROP, and 81-17433 at
JPL.
NR 18
TC 6
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U1 1
U2 23
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1084-7529
J9 J OPT SOC AM A
JI J. Opt. Soc. Am. A-Opt. Image Sci. Vis.
PD JUL
PY 2013
VL 30
IS 7
BP 1335
EP 1341
DI 10.1364/JOSAA.30.001335
PG 7
WC Optics
SC Optics
GA 176WG
UT WOS:000321336400006
PM 24323147
ER
PT J
AU Jimenez, C
Gulkis, S
Beaudin, G
Encrenaz, T
Eriksson, P
Kamp, L
Lee, S
Buehler, SA
AF Jimenez, C.
Gulkis, S.
Beaudin, G.
Encrenaz, T.
Eriksson, P.
Kamp, L.
Lee, S.
Buehler, S. A.
CA MIRO Team
TI Sub-millimeter observations of the terrestrial atmosphere during an
Earth flyby of the MIRO sounder on the Rosetta spacecraft
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Microwave sounder; Cometary observations; Gravitational flyby;
Terrestrial atmospheric temperature; Atmospheric radiative transfer;
Inversion theory
ID INSTRUMENT; RETRIEVAL; MILLIMETER; TEMPERATURE; SIMULATIONS; PARAMETERS;
SATELLITE; PROFILES; DATABASE; ARTS
AB Sub-millimeter spectra recorded by the MIRO sounder aboard the Rosetta spacecraft have been used at the time of an Earth flyby (November 2007) to check the consistency and validity of the instrumental data. High-resolution spectroscopic data were recorded in 8 channels in the vicinity of the strong water line at 557 GHz, and in a broad band continuum channel at 570 GHz. An atmospheric radiative transfer code (ARTS) and standard terrestrial atmospheres have been used to simulate the expected observational results. Differences with the MIRO spectra suggest an anomaly in the behavior of four spectroscopic channels. Further technical investigations have shown that a large part of the anomalies are associated with an instability of one of the amplifiers. The quality of the MIRO data has been further tested by inverting the spectra with an atmospheric inversion tool (Qpack) in order to derive a mesospheric temperature profile. The retrieved profile is in good agreement with the one inferred from the Earth Observing System Microwave Limb Sounder (EOS-MLS). This work illustrates the interest of validating instruments aboard planetary or cometary spacecraft by using data acquired during Earth flybys. (c) 2013 Elsevier Ltd. All rights reserved.
C1 [Jimenez, C.; Beaudin, G.; Encrenaz, T.] Observ Paris, Lab Etud Rayonnement & Matiere Astrophys, F-75014 Paris, France.
[Gulkis, S.; Kamp, L.; Lee, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Buehler, S. A.] Lulea Univ Technol, Dept Comp Sci Elect & Space Engn, S-98128 Kiruna, Sweden.
[Eriksson, P.] Chalmers, Dept Earth & Space Sci, SE-41296 Gothenburg, Sweden.
RP Jimenez, C (reprint author), Observ Paris, Lab Etud Rayonnement & Matiere Astrophys, 61 Ave Observ, F-75014 Paris, France.
EM carlos.jimenez@obspm.fr
RI Eriksson, Patrick/A-5321-2009; Buehler, Stefan Alexander/A-4056-2009
OI Eriksson, Patrick/0000-0002-8475-0479; Buehler, Stefan
Alexander/0000-0001-6389-1160
FU ESA Rosetta Project Team; Rosetta Science Operation Center; Rosetta
Mission Operations Center
FX We are thankful to Catherine Prigent from the Observatoire de Paris, for
constructive discussions concerning this work. We are grateful to the
EOS-MLS for making their data accessible. The ARTS community is
acknowledged for their efforts toward developing the model. The MIRO
Team thanks the ESA Rosetta Project Team, the Rosetta Science Operation
Center and the Rosetta Mission Operations Center for their support.
NR 31
TC 2
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U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD JUL
PY 2013
VL 82-83
BP 99
EP 112
DI 10.1016/j.pss.2013.03.016
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 173OI
UT WOS:000321088400009
ER
PT J
AU Fielding, EJ
Lundgren, PR
Taymaz, T
Yolsal-Cevikbilen, S
Owen, SE
AF Fielding, Eric J.
Lundgren, Paul R.
Taymaz, Tuncay
Yolsal-Cevikbilen, Seda
Owen, Susan E.
TI Fault-Slip Source Models for the 2011 M 7.1 Van Earthquake in Turkey
from SAR Interferometry, Pixel Offset Tracking, GPS, and Seismic
Waveform Analysis
SO SEISMOLOGICAL RESEARCH LETTERS
LA English
DT Article
ID ANATOLIAN PLATEAU TURKEY; TELESEISMIC BODY WAVES; SOURCE PARAMETERS;
ACTIVE TECTONICS; RUPTURE PROCESS; FAULT ZONE; SURROUNDING REGIONS;
CRUSTAL STRUCTURE; JOINT INVERSION; IRANIAN PLATEAU
C1 [Fielding, Eric J.; Lundgren, Paul R.; Owen, Susan E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Taymaz, Tuncay; Yolsal-Cevikbilen, Seda] Istanbul Tech Univ, Fac Mines, Dept Geophys Engn, TR-34469 Istanbul, Turkey.
RP Fielding, EJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-233, Pasadena, CA 91109 USA.
RI Fielding, Eric/A-1288-2007
OI Fielding, Eric/0000-0002-6648-8067
FU Istanbul Technical University Research Fund (ITU-BAP); Turkish National
Scientific, Technological Foundation (TUBITAK); Turkish Academy of
Sciences (TUBA) [TT-TUBA-GEBIP 2001-2-17]; Alexander von
Humboldt-Stiftung (AvH); NASA Earth Surface and Interior focus area
FX We thank an anonymous reviewer for detailed comments on earlier versions
of our manuscript that helped us to improve it. We thank M. Barazangi,
Z. Liu, S. Akciz, E. Hauksson, J. Elliott, and K. Hudnut for
discussions. We thank S. Ergintav for helping to arrange the sharing of
the GPS data on the Geohazards Supersite. We thank B. Dogan for sending
pre-prints of papers in advance of publication. We would like to thank
Istanbul Technical University Research Fund (ITU-BAP), Turkish National
Scientific, Technological Foundation (TUBITAK), Turkish Academy of
Sciences (TUBA) in the framework for Young Scientist Award Program
(TT-TUBA-GEBIP 2001-2-17), and Alexander von Humboldt-Stiftung (AvH) for
their support. Generic Mapping Tools (GMT; Wessel and Smith, 1998) and
SAC2000 software packages (Goldstein et al., 2003) were used to prepare
figures and to process conventional earthquake data, respectively. We
are thankful to Yesim Cubuk for her help in generating Figure 1 and
Table 1. The teleseismic body waves used in this study are from the
International Federation of Digital Seismograph Networks (FDSN), the
Global Digital Seismograph Network (GDSN) stations and archived at the
IRIS-DMC. COSMO-SkyMed (CSK) original data are copyright 2011 by the
Italian Space Agency and was provided under CSK AO PI project 2271.
Envisat original data are copyright 2010-2011 by the European Space
Agency and was delivered under the Group on Earth Observation (GEO)
Geohazards Supersite program. Part of this research was sponsored by the
NASA Earth Surface and Interior focus area and performed at the Jet
Propulsion Laboratory, California Institute of Technology.
NR 69
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U1 3
U2 15
PU SEISMOLOGICAL SOC AMER
PI ALBANY
PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA
SN 0895-0695
EI 1938-2057
J9 SEISMOL RES LETT
JI Seismol. Res. Lett.
PD JUL-AUG
PY 2013
VL 84
IS 4
BP 579
EP 593
DI 10.1785/0220120164
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 176PH
UT WOS:000321316100003
ER
PT J
AU Joshi, NC
Uddin, W
Srivastava, AK
Chandra, R
Gopalswamy, N
Manoharan, PK
Aschwanden, MJ
Choudhary, DP
Jain, R
Nitta, NV
Xie, H
Yashiro, S
Akiyama, S
Makela, P
Kayshap, P
Awasthi, AK
Dwivedi, VC
Mahalakshmi, K
AF Joshi, N. C.
Uddin, W.
Srivastava, A. K.
Chandra, R.
Gopalswamy, N.
Manoharan, P. K.
Aschwanden, M. J.
Choudhary, D. P.
Jain, R.
Nitta, N. V.
Xie, H.
Yashiro, S.
Akiyama, S.
Maekelae, P.
Kayshap, P.
Awasthi, A. K.
Dwivedi, V. C.
Mahalakshmi, K.
TI A multiwavelength study of eruptive events on January 23, 2012
associated with a major solar energetic particle event
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Sun; Solar flares; Coronal mass ejections; Solar energetic particles;
Geomagnetic storm
ID CORONAL MASS EJECTIONS; II RADIO-BURSTS; FLARE; ACCELERATION;
HELIOSPHERE; SCINTILLATION; CONNECTION; ORIGIN; STORM; EARTH
AB We use multiwavelength data from space and ground based instruments to study the solar flares and coronal mass ejections (CMEs) on January 23, 2012 that were responsible for one of the largest solar energetic particle (SEP) events of solar cycle 24. The eruptions consisting of two fast CMEs (approximate to 1400 km s(-1) and approximate to 2000 km s(-1)) and M-class flares that occurred in active region 11402 located at approximate to N28 W36. The two CMEs occurred in quick successions, so they interacted very close to the Sun. The second CME caught up with the first one at a distance of approximate to 11-12 R-sun. The CME interaction may be responsible for the elevated SEP flux and significant changes in the intensity profile of the SEP event. The compound CME resulted in a double-dip moderate geomagnetic storm (Dst similar to -73 nT). The two dips are due to the southward component of the interplanetary magnetic field in the shock sheath and the ICME intervals. One possible reason for the lack of a stronger geomagnetic storm may be that the ICME delivered a glancing blow to Earth. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Joshi, N. C.; Uddin, W.; Srivastava, A. K.; Kayshap, P.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263002, India.
[Chandra, R.] Kumaun Univ, Dept Phys, Naini Tal 263002, India.
[Gopalswamy, N.; Xie, H.; Yashiro, S.; Akiyama, S.; Maekelae, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Manoharan, P. K.; Dwivedi, V. C.; Mahalakshmi, K.] Tata Inst Fundamental Res, Radio Astron Ctr, Ooty 643001, India.
[Aschwanden, M. J.; Nitta, N. V.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Choudhary, D. P.] Calif State Univ Northridge, Deptartment Phys & Astrophys, Northridge, CA 91330 USA.
[Jain, R.; Awasthi, A. K.] Phys Res Lab, Dept Space, Ahmadabad 380009, Gujarat, India.
RP Joshi, NC (reprint author), Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263002, India.
EM navin@aries.res.in; wahab@aries.res.in; aks@aries.res.in;
rchandra.ntl@gmail.com; Nat.Gopalswamy@nasa.gov; mano@ncra.tifr.res.in;
aschwanden@lm-sal.com; debiprasad.choudhary@csun.edu; rajmal@prl.res.in;
nitta@lmsal.com; hong.xie-1@nasa.gov; seiji.yashiro@nasa.gov;
sachiko.akiyama@nasa.gov; pertti.makela@nasa.gov;
pradeep.kashyap@aries.res.in; awasthi@prl.res.in;
vidya_charan2000@yahoo.com; kmahee@gmail.com
RI Awasthi, Arun/H-5596-2016
OI Awasthi, Arun/0000-0001-5313-1125
FU IUSSTF/JC-Solar Eruptive Phenomena project on "Multiwavelength Study of
Solar Eruptive Phenomena and their Interplanetary Responses"; Aryabhatta
Research Institute of Observational Sciences (ARIES), Nainital; NASA LWS
program; ISRO/RESPOND Project [ISRO/RES/2/379/12-13]
FX We thank the anonymous referees for their valuable comments and
suggestions. We thank IUSSTF/JC-Solar Eruptive
Phenomena/99-2010/2011-2012 project on "Multiwavelength Study of Solar
Eruptive Phenomena and their Interplanetary Responses" for its support
to this study during our bilateral collaboration. We acknowledge the
Wind/WAVES and SDO's AIA and HMI teams for providing their data. SOHO is
a project of international cooperation between ESA and NASA. The STEREO
Science Center made available the data used in this work. N.C.J thanks
Aryabhatta Research Institute of Observational Sciences (ARIES),
Nainital for providing Post Doctoral Grant. This work was partly
supported by NASA LWS program. RC, AKS and WU acknowledge ISRO/RESPOND
Project no. ISRO/RES/2/379/12-13. We also acknowledge the NoRH, GOES,
HiRAS and GONG teams for providing their data.
NR 40
TC 14
Z9 14
U1 1
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD JUL 1
PY 2013
VL 52
IS 1
BP 1
EP 14
DI 10.1016/j.asr.2013.03.009
PG 14
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 167NQ
UT WOS:000320639100001
ER
PT J
AU Slaba, TC
Blattnig, SR
Reddell, B
Bahadori, A
Norman, RB
Badavi, FF
AF Slaba, Tony C.
Blattnig, Steve R.
Reddell, Brandon
Bahadori, Amir
Norman, Ryan B.
Badavi, Francis F.
TI Pion and electromagnetic contribution to dose: Comparisons of HZETRN to
Monte Carlo results and ISS data
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE HZETRN; Geant4; FLUKA; PHITS; Space radiation; Galactic cosmic rays
ID RADIATION; TRANSPORT; VALIDATION; MODEL; CODE; ENVIRONMENT;
BENCHMARKING; SPECTRA; SHUTTLE; BOARD
AB Recent work has indicated that pion production and the associated electromagnetic (EM) cascade may be an important contribution to the total astronaut exposure in space. Recent extensions to the deterministic space radiation transport code, HZETRN, allow the production and transport of pions, muons, electrons, positrons, and photons. In this paper, the extended code is compared to the Monte Carlo codes, Geant4, PHITS, and FLUKA, in slab geometries exposed to galactic cosmic ray (GCR) boundary conditions. While improvements in the HZETRN transport formalism for the new particles are needed, it is shown that reasonable agreement on dose is found at larger shielding thicknesses commonly found on the International Space Station (ISS). Finally, the extended code is compared to ISS data on a minute-by-minute basis over a seven day period in 2001. The impact of pion/EM production on exposure estimates and validation results is clearly shown. The Badhwar-O'Neill (BO) 2004 and 2010 models are used to generate the GCR boundary condition at each time-step allowing the impact of environmental model improvements on validation results to be quantified as well. It is found that the updated BO2010 model noticeably reduces overall exposure estimates from the BO2004 model, and the additional production mechanisms in HZETRN provide some compensation. It is shown that the overestimates provided by the BO2004 GCR model in previous validation studies led to deflated uncertainty estimates for environmental, physics, and transport models, and allowed an important physical interaction (pi/EM) to be overlooked in model development. Despite the additional pi/EM production mechanisms in HZETRN, a systematic under-prediction of total dose is observed in comparison to Monte Carlo results and measured data. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Slaba, Tony C.; Blattnig, Steve R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Reddell, Brandon] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Bahadori, Amir] Univ Houston, Houston, TX USA.
[Norman, Ryan B.] Univ Tennessee, Knoxville, TN USA.
[Badavi, Francis F.] Old Dominion Univ, Norfolk, VA USA.
RP Slaba, TC (reprint author), NASA, Langley Res Ctr, Mail Stop 188E,2 West Reid St B1205,Rm 281, Hampton, VA 23681 USA.
EM Tony.C.Slaba@nasa.gov; Steve.R.Blattnig@nasa.gov;
Brandon.D.Reddell@nasa.gov; Amir.A.Bahadori@nasa.gov;
Ryan.B.Norman@nasa.gov; Francis.F.Badavi@nasa.gov
RI Norman, Ryan/D-5095-2017
OI Norman, Ryan/0000-0002-9103-7225
FU Human Research Program in the Advanced Capabilities Division under the
Human Exploration and Operations Mission Directorate of NASA; NASA
Bioastronautics Contract [NAS 9-02078]
FX This work was supported by the Human Research Program in the Advanced
Capabilities Division under the Human Exploration and Operations Mission
Directorate of NASA. The authors would like to thank Nicholas Stale,
Robert Rutledge, Kerry Lee, and Neal Zapp for the TEPC data and Tsvetan
Dachev and Borislav Tomov for the Liulin data. The PHITS simulations for
this work were supported by NASA Bioastronautics Contract NAS 9-02078.
NR 51
TC 12
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U1 0
U2 5
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 JUL 1
PY 2013
VL 52
IS 1
BP 62
EP 78
DI 10.1016/j.asr.2013.02.015
PG 17
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 167NQ
UT WOS:000320639100007
ER
PT J
AU Nobili, AM
Lucchesi, DM
Crosta, MT
Shao, M
Turyshev, SG
Peron, R
Catastini, G
Anselmi, A
Zavattini, G
AF Nobili, A. M.
Lucchesi, D. M.
Crosta, M. T.
Shao, M.
Turyshev, S. G.
Peron, R.
Catastini, G.
Anselmi, A.
Zavattini, G.
TI On the universality of free fall, the equivalence principle, and the
gravitational redshift
SO AMERICAN JOURNAL OF PHYSICS
LA English
DT Article
ID INERTIAL MASS; RELATIVITY; ANISOTROPY; GRAVITY; ENERGY; BODY
AB Through the contributions of Galileo, Newton, and Einstein, we recall the universality of free fall (UFF), the weak equivalence principle (WEP), and the strong equivalence principle (SEP), in order to stress that general relativity requires all test masses to be equally accelerated in a gravitational field; that is, it requires UFF and WEP to hold. The possibility of testing this crucial fact with null, highly sensitive experiments makes these the most powerful tests of the theory. Following Schiff, we derive the gravitational redshift from the WEP and special relativity and show that, as long as clocks are affected by a gravitating body like normal matter, measurement of the redshift is a test of UFF/WEP but cannot compete with direct null tests. A new measurement of the gravitational redshift based on free-falling cold atoms and an absolute gravimeter is not competitive either. Finally, we compare UFF/WEP experiments using macroscopic masses as test bodies in one case and cold atoms in the other. We conclude that there is no difference in the nature of the test and that the merit of any such experiment rests on the accuracy it can achieve and on the physical differences between the elements it can test, macroscopic proof masses being superior in both respects. (C) 2013 American Association of Physics Teachers.
C1 [Nobili, A. M.] Univ Pisa, Dept Phys E Fermi, I-56127 Pisa, Italy.
[Nobili, A. M.; Lucchesi, D. M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Lucchesi, D. M.; Peron, R.] IAPS, INAF, I-00133 Rome, Italy.
[Crosta, M. T.] Osservatorio Astrofis Torino, INAF, Turin, Italy.
[Shao, M.; Turyshev, S. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Catastini, G.; Anselmi, A.] Thales Alenia Space Italia, I-10146 Turin, Italy.
[Zavattini, G.] Univ Ferrara, Dept Phys, I-44122 Ferrara, Italy.
[Zavattini, G.] Ist Nazl Fis Nucl, Sez Ferrara, I-44122 Ferrara, Italy.
RP Nobili, AM (reprint author), Univ Pisa, Dept Phys E Fermi, Largo Bruno Pontecorvo 3, I-56127 Pisa, Italy.
OI Lucchesi, David/0000-0002-7057-4785; Peron, Roberto/0000-0002-1774-5725
FU ASI (Agenzia Spaziale Italiana); INFN
FX This work was supported by ASI (Agenzia Spaziale Italiana) and INFN, and
it was performed in part at JPL, Caltech, under a contract with NASA.
Thanks are due to F. Pegoraro for helping to present this work in the
context of the current debate.
NR 53
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U1 2
U2 10
PU AMER ASSOC PHYSICS TEACHERS AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0002-9505
J9 AM J PHYS
JI Am. J. Phys.
PD JUL
PY 2013
VL 81
IS 7
BP 527
EP 536
DI 10.1119/1.4798583
PG 10
WC Education, Scientific Disciplines; Physics, Multidisciplinary
SC Education & Educational Research; Physics
GA 167ED
UT WOS:000320612800006
ER
PT J
AU Borkowski, KJ
Reynolds, SP
Hwang, U
Green, DA
Petre, R
Krishnamurthy, K
Willett, R
AF Borkowski, Kazimierz J.
Reynolds, Stephen P.
Hwang, Una
Green, David A.
Petre, Robert
Krishnamurthy, Kalyani
Willett, Rebecca
TI SUPERNOVA EJECTA IN THE YOUNGEST GALACTIC SUPERNOVA REMNANT G1.9+0.3
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual objects (G1.9+0.3); ISM: supernova remnants; nuclear
reactions, nucleosynthesis, abundances; X-rays: ISM
ID RISING LIGHT CURVES; IA SUPERNOVAE; NUCLEOSYNTHESIS; CONSTRAINTS;
EXPANSION; EMISSION; SPECTRUM; MODELS
AB G1.9+0.3 is the youngest known Galactic supernova remnant (SNR), with an estimated supernova (SN) explosion date of similar to 1900, and most likely located near the Galactic center. Only the outermost ejecta layers with freeexpansion velocities greater than or similar to 18,000 km s(-1) have been shocked so far in this dynamically young, likely Type Ia SNR. A long (980 ks) Chandra observation in 2011 allowed spatially resolved spectroscopy of heavy-element ejecta. We denoised Chandra data with the spatio-spectral method of Krishnamurthy et al., and used a wavelet-based technique to spatially localize thermal emission produced by intermediate-mass elements (IMEs; Si and S) and iron. The spatial distribution of both IMEs and Fe is extremely asymmetric, with the strongest ejecta emission in the northern rim. Fe K alpha emission is particularly prominent there, and fits with thermalmodels indicate strongly oversolar Fe abundances. In a localized, outlying region in the northern rim, IMEs are less abundant than Fe, indicating that undiluted Fe-group elements (including Ni-56) with velocities > 18,000 km s(-1) were ejected by this SN. However, in the inner west rim, we find Si-and S-rich ejecta without any traces of Fe, so high-velocity products of O-burning were also ejected. G1.9+0.3 appears similar to energetic Type Ia SNe such as SN 2010jn where iron-group elements at such high free-expansion velocities have been recently detected. The pronounced asymmetry in the ejecta distribution and abundance inhomogeneities are best explained by a strongly asymmetric SN explosion, similar to those produced in some recent three-dimensional delayed-detonation Type Ia models.
C1 [Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Hwang, Una] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Green, David A.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krishnamurthy, Kalyani; Willett, Rebecca] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
RP Borkowski, KJ (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
EM kborkow@unity.ncsu.edu
RI Green, David/E-9609-2010;
OI Green, David/0000-0003-3189-9998; Willett, Rebecca/0000-0002-8109-7582
FU NASA through Chandra General Observer Program [SAO G01-12098A, SAO
G01-12098B]
FX This work was supported by NASA through Chandra General Observer Program
grants SAO G01-12098A and B.
NR 27
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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 JUL 1
PY 2013
VL 771
IS 1
AR L9
DI 10.1088/2041-8205/771/1/L9
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 169WL
UT WOS:000320811300009
ER
PT J
AU Cernicharo, J
Tercero, B
Fuente, A
Domenech, JL
Cueto, M
Carrasco, E
Herrero, VJ
Tanarro, I
Marcelino, N
Roueff, E
Gerin, M
Pearson, J
AF Cernicharo, J.
Tercero, B.
Fuente, A.
Domenech, J. L.
Cueto, M.
Carrasco, E.
Herrero, V. J.
Tanarro, I.
Marcelino, N.
Roueff, E.
Gerin, M.
Pearson, J.
TI DETECTION OF THE AMMONIUM ION IN SPACE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: abundances; ISM: individual objects (B1-bS); ISM: molecules; line:
identification molecular data
ID INTERSTELLAR DEUTERATED AMMONIA; PRE-PROTOSTELLAR COLLAPSE; 1ST ISM
DETECTION; TO-PARA RATIO; ROTATIONAL SPECTRUM; DARK CLOUDS; MOLECULAR
CLOUDS; BARNARD-1 CLOUD; ETHYL CYANIDE; CHEMISTRY
AB We report on the detection of a narrow feature at 262816.73 MHz toward Orion and the cold prestellar core B1-bS which we attribute to the 1(0)-0(0) line of the deuterated ammonium ion, NH3D+. The observations were performed with the IRAM 30 m radio telescope. The carrier has to be a light molecular species as it is the only feature detected over 3.6 GHz of bandwidth. The hyperfine structure is not resolved, indicating a very low value for the electric quadrupolar coupling constant of nitrogen which is expected for NH3D+ as the electric field over the N nucleus is practically zero. Moreover, the feature is right at the predicted frequency for the 1(0)-0(0) transition of the ammonium ion, 262817 +/- 6MHz (3 sigma), using rotational constants derived from new infrared data obtained in our laboratory in Madrid. The estimated column density is (1.1 +/- 0.2) x 10(12) cm(-2). Assuming a deuterium enhancement similar to that of NH2D, we derive N(NH4+) similar or equal to 2.6 x 10(13) cm(-2), i.e., an abundance for ammonium of a few 10(-11).
C1 [Cernicharo, J.; Tercero, B.] CSIC, CAB, INTA, Deparment Astrophys, E-28850 Madrid, Spain.
[Fuente, A.] Observ Astron Nacl, E-28803 Alcala De Henares, Spain.
[Domenech, J. L.; Cueto, M.; Carrasco, E.; Herrero, V. J.; Tanarro, I.] CSIC, IEM, E-28006 Madrid, Spain.
[Marcelino, N.] NRAO, Charlottesville, VA 22902 USA.
[Roueff, E.] CNRS, Observ Paris, UMR8102, F-92190 Meudon, France.
[Gerin, M.] CNRS, Observ Paris, LERMA, UMR8112, F-75014 Paris, France.
[Gerin, M.] Ecole Normale Super, F-75014 Paris, France.
[Pearson, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cernicharo, J (reprint author), CSIC, CAB, INTA, Deparment Astrophys, Crta Torrejon Ajalvir Km 4, E-28850 Madrid, Spain.
EM jcernicharo@cab.inta-csic.es
RI Herrero, Victor/G-1369-2016; Fuente, Asuncion/G-1468-2016; Domenech,
Jose/F-5561-2013; Carrasco, Esther/F-2927-2016
OI Fuente, Asuncion/0000-0001-6317-6343; Domenech,
Jose/0000-0001-8629-2566; Carrasco, Esther/0000-0002-2278-8930
FU Spanish MICINN [AYA2009-07304, CSD2009-00038, Fis2010-16455,
Fis2012-38175]; French national PCMI program
FX The Spanish authors thank the Spanish MICINN for funding support through
grants, AYA2009-07304, CSD2009-00038, Fis2010-16455, and Fis2012-38175.
M. Gerin and E. Roueff acknowledge support from the French national PCMI
program. J. Cernicharo thanks U. Paris Est for an invited professor
position during the completion of this work.
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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 JUL 1
PY 2013
VL 771
IS 1
AR L10
DI 10.1088/2041-8205/771/1/L10
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 169WL
UT WOS:000320811300010
ER
PT J
AU Holder, GP
Viero, MP
Zahn, O
Aird, KA
Benson, BA
Bhattacharya, S
Bleem, LE
Bock, J
Brodwin, M
Carlstrom, JE
Chang, CL
Cho, HM
Conley, A
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Dudley, J
George, EM
Halverson, NW
Holzapfel, WL
Hoover, S
Hou, Z
Hrubes, JD
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Marsden, G
Marrone, DP
McMahon, JJ
Mehl, J
Meyer, SS
Millea, M
Mohr, JJ
Montroy, TE
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Ruhl, JE
Sayre, JT
Schaffer, KK
Schulz, B
Shaw, L
Shirokoff, E
Spieler, HG
Staniszewski, Z
Stark, AA
Story, KT
van Engelen, A
Vanderlinde, K
Vieira, JD
Williamson, R
Zemcov, M
AF Holder, G. P.
Viero, M. P.
Zahn, O.
Aird, K. A.
Benson, B. A.
Bhattacharya, S.
Bleem, L. E.
Bock, J.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Cho, H-M.
Conley, A.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Dudley, J.
George, E. M.
Halverson, N. W.
Holzapfel, W. L.
Hoover, S.
Hou, Z.
Hrubes, J. D.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
Marsden, G.
Marrone, D. P.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Millea, M.
Mohr, J. J.
Montroy, T. E.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Ruhl, J. E.
Sayre, J. T.
Schaffer, K. K.
Schulz, B.
Shaw, L.
Shirokoff, E.
Spieler, H. G.
Staniszewski, Z.
Stark, A. A.
Story, K. T.
van Engelen, A.
Vanderlinde, K.
Vieira, J. D.
Williamson, R.
Zemcov, M.
TI A COSMIC MICROWAVE BACKGROUND LENSING MASS MAP AND ITS CORRELATION WITH
THE COSMIC INFRARED BACKGROUND
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmic background radiation; galaxies: structure
ID SOUTH-POLE TELESCOPE; GALAXIES
AB We use a temperature map of the cosmic microwave background (CMB) obtained using the South Pole Telescope at 150 GHz to construct a map of the gravitational convergence to z similar to 1100, revealing the fluctuations in the projected mass density. This map shows individual features that are significant at the similar to 4 sigma level, providing the first image of CMB lensing convergence. We cross-correlate this map with Herschel/SPIRE maps covering 90 deg(2) at wavelengths of 500, 350, and 250 mu m. We show that these submillimeter (submm) wavelength maps are strongly correlated with the lensing convergence map, with detection significances in each of the three submm bands ranging from 6.7 sigma to 8.8 sigma. We fit the measurement of the cross power spectrum assuming a simple constant bias model and infer bias factors of b = 1.3-1.8, with a statistical uncertainty of 15%, depending on the assumed model for the redshift distribution of the dusty galaxies that are contributing to the Herschel/SPIRE maps.
C1 [Holder, G. P.; de Haan, T.; Dobbs, M. A.; Dudley, J.; Shaw, L.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Viero, M. P.; Bock, J.; Lueker, M.; Padin, S.; Schulz, B.; Vieira, J. D.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
[Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA.
[Benson, B. A.; Bhattacharya, S.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K. T.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bhattacharya, S.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60440 USA.
[Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Keisler, R.; Meyer, S. S.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.; Mehl, J.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cho, H-M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Hou, Z.; Knox, L.; Millea, M.] 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.
[Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; 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.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Schulz, B.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Holder, GP (reprint author), McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Reichardt,
Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996;
Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518
FU National Science Foundation [ANT-0638937]; NSF [PHY-1125897,
AST-1009811]; Kavli Foundation; Gordon and Betty Moore Foundation;
National Sciences and Engineering Research Council of Canada; Canada
Research Chairs program; Canadian Institute for Advanced Research; NASA
Hubble Fellowship [HF-51275.01]; KICP Fellowship; Alfred P. Sloan
Research Fellowship; BCCP fellowship; [AST-1009012]
FX The SPT is supported by the National Science Foundation through grant
ANT-0638937, with partial support provided by NSF grant PHY-1125897, the
Kavli Foundation, and the Gordon and Betty Moore Foundation. 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. Work at Harvard is supported
by grant AST-1009012. S. Bhattacharya acknowledges support from NSF
grant AST-1009811, R. Keisler from NASA Hubble Fellowship grant
HF-51275.01, B. Benson from a KICP Fellowship, M. Dobbs from an Alfred
P. Sloan Research Fellowship, and O. Zahn from a BCCP fellowship.
NR 26
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 1
PY 2013
VL 771
IS 1
AR L16
DI 10.1088/2041-8205/771/1/L16
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 169WL
UT WOS:000320811300016
ER
PT J
AU Hsieh, HH
Kaluna, HM
Novakovic, B
Yang, B
Haghighipour, N
Micheli, M
Denneau, L
Fitzsimmons, A
Jedicke, R
Kleyna, J
Veres, P
Wainscoat, RJ
Ansdell, M
Elliott, GT
Keane, JV
Meech, KJ
Moskovitz, NA
Riesen, TE
Sheppard, SS
Sonnett, S
Tholen, DJ
Urban, L
Kaiser, N
Chambers, KC
Burgett, WS
Magnier, EA
Morgan, JS
Price, PA
AF Hsieh, Henry H.
Kaluna, Heather M.
Novakovic, Bojan
Yang, Bin
Haghighipour, Nader
Micheli, Marco
Denneau, Larry
Fitzsimmons, Alan
Jedicke, Robert
Kleyna, Jan
Veres, Peter
Wainscoat, Richard J.
Ansdell, Megan
Elliott, Garrett T.
Keane, Jacqueline V.
Meech, Karen J.
Moskovitz, Nicholas A.
Riesen, Timm E.
Sheppard, Scott S.
Sonnett, Sarah
Tholen, David J.
Urban, Laurie
Kaiser, Nick
Chambers, K. C.
Burgett, William S.
Magnier, Eugene A.
Morgan, Jeffrey S.
Price, Paul A.
TI MAIN-BELT COMET P/2012 T1 (PANSTARRS)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE comets: general; minor planets; asteroids: general
ID ASTEROID FAMILIES; F5 GIBBS; 133P/ELST-PIZARRO; BODIES; VW139; WATER;
DISRUPTION; COLLISION; ORIGIN; SYSTEM
AB We present initial results from observations and numerical analyses aimed at characterizing the main-belt comet P/2012 T1 (PANSTARRS). Optical monitoring observations were made between 2012 October and 2013 February using the University of Hawaii 2.2 m telescope, the Keck I telescope, the Baade and Clay Magellan telescopes, Faulkes Telescope South, the Perkins Telescope at Lowell Observatory, and the Southern Astrophysical Research Telescope. The object's intrinsic brightness approximately doubles from the time of its discovery in early October until mid-November and then decreases by similar to 60% between late December and early February, similar to photometric behavior exhibited by several other main-belt comets and unlike that exhibited by disrupted asteroid (596) Scheila. We also used Keck to conduct spectroscopic searches for CN emission as well as absorption at 0.7 mu m that could indicate the presence of hydrated minerals, finding an upper limit CN production rate of Q(CN) < 1.5 x 10(23) mol s(-1), from which we infer a water production rate of Q(H2O) < 5 x 10(25) mol s(-1), and no evidence of the presence of hydrated minerals. Numerical simulations indicate that P/2012 T1 is largely dynamically stable for > 100 Myr and is unlikely to be a recently implanted interloper from the outer solar system, while a search for potential asteroid family associations reveals that it is dynamically linked to the similar to 155 Myr old Lixiaohua asteroid family.
C1 [Hsieh, Henry H.; Kaluna, Heather M.; Yang, Bin; Haghighipour, Nader; Micheli, Marco; Denneau, Larry; Jedicke, Robert; Kleyna, Jan; Veres, Peter; Wainscoat, Richard J.; Ansdell, Megan; Elliott, Garrett T.; Keane, Jacqueline V.; Meech, Karen J.; Riesen, Timm E.; Sonnett, Sarah; Tholen, David J.; Urban, Laurie; Kaiser, Nick; Chambers, K. C.; Burgett, William S.; Magnier, Eugene A.; Morgan, Jeffrey S.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Novakovic, Bojan] Univ Belgrade, Fac Math, Dept Astron, Belgrade 11000, Serbia.
[Fitzsimmons, Alan] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Moskovitz, Nicholas A.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Sheppard, Scott S.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Price, Paul A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kaluna, Heather M.; Yang, Bin; Haghighipour, Nader; Kleyna, Jan; Ansdell, Megan; Keane, Jacqueline V.; Meech, Karen J.; Riesen, Timm E.; Urban, Laurie] NASA, Astrobiol Inst, Washington, DC USA.
RP Hsieh, HH (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM hsieh@ifa.hawaii.edu
OI Novakovic, Bojan/0000-0001-6349-6881; Chambers, Kenneth
/0000-0001-6965-7789; Micheli, Marco/0000-0001-7895-8209
FU NASA [HF-51274.01, NAS 5-26555, NNX08AR22G]; Space Telescope Science
Institute; NASA Astrobiology Institute [NNA09DA77A]; Ministry of
Education and Science of Serbia [176011]; NSF [AST-1010059]; Alfred P.
Sloan Foundation; Participating Institutions; NSF; U.S. Department of
Energy Office of Science
FX H.H.H. is supported by NASA through the Hubble Fellowship grant
HF-51274.01 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. H.M.K., B.Y., N.H., and
K.J.M. acknowledge support through the NASA Astrobiology Institute under
cooperative agreement NNA09DA77A. B.N. is supported by the Ministry of
Education and Science of Serbia under Project 176011. J.K., M.A.,
J.V.K., T.R., and L.U. acknowledge support through NSF grant
AST-1010059. We thank Larry Wasserman and Brian Taylor at Lowell for
assistance in obtaining observations. Some data presented were acquired
using the PS1 System operated by the PS1 Science Consortium (PS1SC) and
its member institutions. The PS1 survey was made possible by
contributions from PS1SC member institutions and NASA through grant
NNX08AR22G issued through the Planetary Science Division of the NASA
Science Mission Directorate. SDSS-III (http://www.sdss3.org/) is funded
by the Alfred P. Sloan Foundation, the Participating Institutions, NSF,
and the U.S. Department of Energy Office of Science, and managed by the
Astrophysical Research Consortium for the SDSS-III Collaboration.
NR 47
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 1
PY 2013
VL 771
IS 1
AR L1
DI 10.1088/2041-8205/771/1/L1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 169WL
UT WOS:000320811300001
ER
PT J
AU Mills, RD
Glazner, AF
AF Mills, Ryan D.
Glazner, Allen F.
TI Experimental study on the effects of temperature cycling on coarsening
of plagioclase and olivine in an alkali basalt
SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY
LA English
DT Article
DE Crystal growth; Basalt; Temperature cycling; Crystal size distribution;
Phenocrysts
ID CRYSTAL SIZE-DISTRIBUTION; MAGMA CHAMBERS; CONTINENTAL-CRUST;
PHASE-EQUILIBRIA; DISTRIBUTION CSD; KILAUEA VOLCANO; GROWTH;
CRYSTALLIZATION; DISTRIBUTIONS; ORIGIN
AB We conducted experiments on an alkali basalt at 1-atmosphere in order to investigate the effects of temperature cycling on crystal coarsening. Experiments at 1,150 A degrees C near the Ni-NiO buffer indicate that coarsening of plagioclase and olivine crystals is greatly accentuated by temperature cycling. For a given experiment duration, crystal number density decreases with temperature cycle amplitude and average crystal size increases with increasing amplitude. We observed little correlation between cycle period and crystal number density or average crystal size. We suggest that dissolution and size-proportional crystal growth during repeated heating and cooling decrease crystal number density and increase average crystal size. These experiments indicate that the texture of silicate minerals can be modified by temperature cycling and that phenocrysts may develop quicker in silicate magmas when the magma temperature is cycled.
C1 [Mills, Ryan D.; Glazner, Allen F.] Univ N Carolina, Chapel Hill, NC 27599 USA.
RP Mills, RD (reprint author), NASA JSC, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA.
EM ryan.d.mills@nasa.gov
FU National Science Foundation [EAR-1052813]; NASA Postdoctoral Program;
Justin Simon
FX This research was supported by National Science Foundation Grant
EAR-1052813. The Martin Fund of the Department of Geological Sciences at
the University of North Carolina, the Geological Society of America,
Sigma Xi, and the Mary Lily Kenan Flagler Bingham Professorship. R. M.
acknowledges the NASA Postdoctoral Program and Justin Simon for support.
Colin McKinney provided expertise with control systems. Kent Ross
assisted with the FE-SEM work. Informal reviews by Alan Boudreau, Drew
Coleman, Ryan Frazer, and Breck Johnson on earlier versions of this
manuscript helped clarify the content. Journal reviews by Ariel Provost,
Pietro Armienti, and editor Jon Blundy greatly improved the quality of
the final publication. We also thank Jon Blundy for his editorial
handling of the manuscript.
NR 68
TC 11
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U1 0
U2 17
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0010-7999
J9 CONTRIB MINERAL PETR
JI Contrib. Mineral. Petrol.
PD JUL
PY 2013
VL 166
IS 1
BP 97
EP 111
DI 10.1007/s00410-013-0867-4
PG 15
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 167SU
UT WOS:000320655900006
ER
PT J
AU Colliander, A
Xu, XL
AF Colliander, Andreas
Xu, Xiaolan
TI Normalized Residual Scattering Index Applied to Aquarius L-Band
Measurements
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Active; Aquarius; European Centre for Medium-range Weather Forecasts;
GlobSnow; Global Multiresolution Terrain Elevation Data 2010; microwave;
passive; vegetation
ID SNOW WATER EQUIVALENT; ACTIVE L-BAND; SOIL-MOISTURE; AMSR-E; MICROWAVE
SENSOR; VEGETATION
AB A normalized residual scattering index is introduced. This index is based on the relationship between coincident microwave-backscatter and brightness-temperature observations. In this letter, the L-band NRSI is shown to correlate with vegetation cover conditions on a global scale. The interpretation of global observations from the Aquarius satellite is based on Passive Active L-band System airborne data collected during field experiments together with ground truth. The benefit of the method is that it is sensitive to land-cover features affecting both active and passive measurements while being insensitive to surface effects such as soil moisture.
C1 [Colliander, Andreas; Xu, Xiaolan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Colliander, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM andreas.colliander@jpl.nasa.gov; xiaolan.xu@jpl.nasa.gov
NR 23
TC 4
Z9 4
U1 0
U2 17
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD JUL
PY 2013
VL 10
IS 4
BP 890
EP 894
DI 10.1109/LGRS.2012.2226559
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 168QJ
UT WOS:000320720300027
ER
PT J
AU Josset, D
Tanelli, S
Hu, Y
Pelon, J
Zhai, P
AF Josset, D.
Tanelli, S.
Hu, Y.
Pelon, J.
Zhai, P.
TI Analysis of Water Vapor Correction for CloudSat W-Band Radar
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Laser radar; radar; remote sensing; water vapor
ID MILLIMETER-WAVE-PROPAGATION; SURFACE WIND; AIRBORNE; CALIBRATION;
ABSORPTION; CONTINUUM; MODELS; LIDAR; ICE
AB We analyzed different models to estimate absorption at W-band by gaseous species by taking advantage of the collocated CloudSat-Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) measurements. We used the power backscattered by the surface in the green visible wavelength of the lidar of CALIPSO as a reference to infer CloudSat's 94-GHz ocean surface backscatter in clear air and infer the attenuation introduced by gaseous absorption. Different millimeter-wave propagation models (MPMs) and different sources to determine the profile of atmospheric thermodynamic state are used to estimate CloudSat attenuation. These estimates are compared to the observations to calculate the residual dispersion. We show here that we need to adjust the empirical constants of preexisting water vapor absorption models to minimize the dispersion. Our results indicate an overestimation of absorption by the water vapor continuum at 94 GHz in Liebe-based MPM. We also propose a new empirical model to better represent the absorption of the water vapor continuum near 94 GHz. When this model is used in combination with the Advanced Microwave Scanning Radiometer for the Earth Observing System water vapor path and the Global Modeling and Assimilation Office water vapor vertical profile distribution, it leads to the lowest dispersion of the data on a statistical basis (global data over one month). The improved model is expected to optimize water vapor correction applied to CloudSat data and, potentially, also to improve interpretation of brightness temperature measurements in the W-band (e. g., 85- and 98-GHz radiometric channels).
C1 [Josset, D.; Zhai, P.] Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
[Tanelli, S.] CALTECH, Jet Prop Lab, Radar Sci & Engn Sect, Pasadena, CA 91109 USA.
[Hu, Y.] NASA, Atmospher Composit Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Pelon, J.] Univ Paris 06, Inst Pierre Simon Laplace, Ctr Natl Rech Sci, Lab Atmospheres, F-75252 Paris, France.
RP Josset, D (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
EM damien.b.josset@nasa.gov; simone.tanelli@jpl.nasa.gov;
yongxiang.hu-1@nasa.gov; jacques.pelon@latmos.ipsl.fr;
pengwang.zhai-1@nasa.gov
RI Hu, Yongxiang/K-4426-2012
FU NASA; CNES; Science System and Applications, Inc. in the frame of the
CALIPSO mission; ICARE French Archive Center for the MODerate-resolution
Imaging Spectroradiometer (MODIS) collocation (CALTRACK product)
FX This work was supported by NASA, CNES and Science System and
Applications, Inc. in the frame of the CALIPSO mission.; The authors
would like to thank the ICARE French Archive
(http://www.icare.univ-lille1.fr/) Center for the MODerate-resolution
Imaging Spectroradiometer (MODIS) collocation (CALTRACK product), the
NASA and CNES for their support and data availability for the CALIPSO,
CloudSat, MODIS, and AMSR-E project, and two anonymous reviewers for
their useful comments. The contributions by Simone Tanelli were
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration for the CloudSat mission. Special kudos must go to H. J.
Liebe for his outstanding contribution to science and for the creation
of the millimeter-wave propagation models.
NR 33
TC 2
Z9 2
U1 1
U2 15
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 JUL
PY 2013
VL 51
IS 7
BP 3812
EP 3825
DI 10.1109/TGRS.2012.2228659
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 171PX
UT WOS:000320942600003
ER
PT J
AU King, MD
Platnick, S
Menzel, WP
Ackerman, SA
Hubanks, PA
AF King, Michael D.
Platnick, Steven
Menzel, W. Paul
Ackerman, Steven A.
Hubanks, Paul A.
TI Spatial and Temporal Distribution of Clouds Observed by MODIS Onboard
the Terra and Aqua Satellites
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aqua; cloud remote sensing; clouds; Moderate Resolution Imaging
Spectroradiometer (MODIS); satellite applications; Terra; terrestrial
atmosphere.
ID SOLAR-RADIATION MEASUREMENTS; LIQUID WATER CLOUDS; OPTICAL-THICKNESS;
PART II; DROPLET GROWTH; LAND PRODUCTS; STATISTICS; ISCCP; VAPOR; HIRS
AB Cloud properties have been retrieved from the Moderate Resolution Imaging Spectroradiometer (MODIS) over 12 years of continuous observations from Terra and over nine years from Aqua. Results include the spatial and temporal distribution of cloud fraction, the cloud top pressure and cloud top temperature, and the cloud optical thickness and effective radius of both liquid water and ice clouds. Globally, the cloud fraction derived by the MODIS cloud mask is similar to 67%, with somewhat more clouds over land during the afternoon and less clouds over ocean in the afternoon, with very little difference in global cloud cover between Terra and Aqua. Overall, the cloud fraction over land is similar to 55%, with a distinctive seasonal cycle, whereas the ocean cloudiness is much higher, around 72%, with much reduced seasonal variation. Aqua and Terra have comparable zonal cloud top pressures, with Aqua having somewhat higher clouds (cloud top pressures lower by 100 hPa) over land due to afternoon deep convection. The coldest cloud tops (colder than 230 K) generally occur over Antarctica and the high clouds in the tropics. The cloud effective particle radius of liquid water clouds is significantly larger over ocean (mode 12-13 mu m) than land (mode 10-11 mu m), consistent with the variation in hygroscopic aerosol concentrations that provide cloud condensation nuclei necessary for cloud formation. We also find the effective radius to be 2-3 mu m larger in the southern hemisphere than in the northern hemisphere, likely reflecting differences in sources of cloud condensation nuclei.
C1 [King, Michael D.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Platnick, Steven] NASA, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Menzel, W. Paul; Ackerman, Steven A.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA.
[Hubanks, Paul A.] Wyle Informat Syst LLC, Lanham, MD 20706 USA.
RP King, MD (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
EM michael.king@lasp.colorado.edu
RI King, Michael/C-7153-2011; Ackerman, Steven/G-1640-2011; Menzel, W.
Paul/B-8306-2011; Platnick, Steven/J-9982-2014
OI King, Michael/0000-0003-2645-7298; Ackerman, Steven/0000-0002-4476-0269;
Menzel, W. Paul/0000-0001-5690-1201; Platnick,
Steven/0000-0003-3964-3567
FU National Aeronautics and Space Administration (NASA) [NNX11AF28G,
NNX11AH62G]
FX This work was supported by the National Aeronautics and Space
Administration (NASA) through the MODIS Science Team. The work of M. D.
King was supported by NASA under Grant NNX11AF28G to the University of
Colorado. The work of W. P. Menzel and S. A. Ackerman was supported by
NASA under Grant NNX11AH62G to the University of Wisconsin.
NR 58
TC 59
Z9 60
U1 5
U2 50
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 JUL
PY 2013
VL 51
IS 7
BP 3826
EP 3852
DI 10.1109/TGRS.2012.2227333
PN 1
PG 27
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 171PX
UT WOS:000320942600004
ER
PT J
AU Jethva, H
Torres, O
Remer, LA
Bhartia, PK
AF Jethva, Hiren
Torres, Omar
Remer, Lorraine A.
Bhartia, Pawan K.
TI A Color Ratio Method for Simultaneous Retrieval of Aerosol and Cloud
Optical Thickness of Above-Cloud Absorbing Aerosols From Passive
Sensors: Application to MODIS Measurements
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aerosol absorption; aerosols above cloud; color ratio; Moderate
Resolution Imaging Spectroradiometer (MODIS); Ozone Monitoring
Instrument (OMI)
ID DEPTH
AB The presence of absorbing aerosols above cloud decks reduces the amount of upwelling ultraviolet (UV), visible (VIS), and shortwave infrared radiation reaching the top of atmosphere. This effect is often referred to as "cloud darkening," which can be seen by eye in images and quantitatively in the spectral reflectance measurements made by passive sensors such as the Moderate Resolution Imaging Spectroradiometer (MODIS) in the regions where light-absorbing carbonaceous and dust aerosols overlay low-level clouds. Radiative transfer simulations support the observational evidence and further reveal that the reduction in the spectral reflectance and color ratio between a pair of wavelengths is a function of both aerosol and cloud optical thickness (AOT and COT). For a prescribed set of aerosol and cloud properties and their vertical profiles, thus, the measured reflectance can be associated with a pair of AOT and COT. Based on these results, a retrieval technique has been developed, which is named as the "color ratio method," which utilizes the measurements at a shorter (470 nm) and a longer (860 nm) wavelength for the simultaneous derivation of AOT and COT. The retrieval technique has been applied to the MODIS 1-km reflectance measurements for the two distinct above-cloud smoke and dust aerosols events. This study is an extension of the previously developed near-UV method to the VIS spectral region. However, it constitutes the first attempt to use non-UV wavelengths to retrieve above-cloud AOT by a passive nonpolarized sensor. An uncertainty analysis has been presented, which estimates the expected error associated with these retrievals.
C1 [Jethva, Hiren] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Jethva, Hiren; Torres, Omar; Bhartia, Pawan K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Remer, Lorraine A.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
RP Jethva, H (reprint author), Univ Space Res Assoc, Columbia, MD 21044 USA.
EM hiren.t.jethva@nasa.gov
RI Torres, Omar/G-4929-2013; Bhartia, Pawan/A-4209-2016
OI Bhartia, Pawan/0000-0001-8307-9137
NR 20
TC 24
Z9 24
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 JUL
PY 2013
VL 51
IS 7
BP 3862
EP 3870
DI 10.1109/TGRS.2012.2230008
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 171PX
UT WOS:000320942600006
ER
PT J
AU Bateni, SM
Huang, CL
Margulis, SA
Podest, E
McDonald, K
AF Bateni, S. Mohyeddin
Huang, Chunlin
Margulis, Steven A.
Podest, Erika
McDonald, Kyle
TI Feasibility of Characterizing Snowpack and the Freeze-Thaw State of
Underlying Soil Using Multifrequency Active/Passive Microwave Data
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Active microwave data; data assimilation (DA); passive microwave data;
snow cover; snow water equivalent (SWE); soil freeze-thaw
ID QUASI-CRYSTALLINE APPROXIMATION; ARTIFICIAL NEURAL-NETWORK; 1ST-YEAR
SEA-ICE; SIR-C/X-SAR; WATER EQUIVALENT; DATA ASSIMILATION; GRAIN-SIZE;
ENVIRONMENTAL-CONDITIONS; SCATTEROMETER DATA; LAYERED SNOWPACKS
AB An ensemble-based data assimilation approach is developed to characterize the snow water equivalent (SWE) and underlying soil freeze-thaw state (including the soil surface temperature and both soil ice and liquid water content) using multifrequency passive and active microwave remote-sensing measurements. Its feasibility was examined using a synthetic test where passive microwave (1.4, 18.7, and 36.5 GHz) and active microwave [L-band (1.4 GHz), C-band (5.4 GHz), and Ku-band (12 GHz)] measurements at the point scale were individually and simultaneously assimilated to estimate the SWE and soil freeze-thaw state using an Ensemble Batch Smoother framework. The contribution of each channel in retrieving the true SWE, soil surface temperature, soil liquid water and ice content was investigated at the local-scale observation site of the National Aeronautics and Space Administration Cold Land Processes Experiments Field Campaign in northern Colorado during both the snow accumulation (Fall 2002-Winter 2003) and melt (Spring 2003) periods. All of the utilized passive and active measurements were found to contain valuable and complementary information for characterizing the SWE and freeze-thaw state of the underlying soil. L-band measurements were most effective for soil freeze-thaw state estimation, whereas higher frequencies were more effective at SWE characterization. In addition, results from the simultaneous assimilation of passive and active microwave data were compared to those from a modeling approach without assimilating microwave data (open loop). It was found that assimilating both passive and active microwave data decreased the errors that are associated with the open-loop approach. Finally, passive and active measurements were undersampled as expected from the overpasses of current and future satellite platforms. It was observed that the developed method can reliably estimate the soil freeze-thaw state and SWE, even with measurement sequences anticipated from the temporal frequency of existing and future satellites such as the Special Sensor Microwave/Imager, Soil Moisture Active Passive Mission, and Cold Regions Hydrology High-Resolution Observatory.
C1 [Bateni, S. Mohyeddin; Margulis, Steven A.] Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA 90095 USA.
[Huang, Chunlin] Chinese Acad Sci, Cold & Arid Reg Environm & Engn Res Inst, Lanzhou 730000, Peoples R China.
[Podest, Erika; McDonald, Kyle] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McDonald, Kyle] CUNY City Coll, Dept Earth & Atmospher Sci, New York, NY 10016 USA.
RP Bateni, SM (reprint author), Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA 90095 USA.
RI Huang, Chunlin/G-6715-2011; westgis.CAREERI, SCI paper/O-2255-2013
OI Huang, Chunlin/0000-0002-1366-5170; westgis.CAREERI, SCI
paper/0000-0001-5298-1494
NR 79
TC 12
Z9 12
U1 0
U2 34
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 JUL
PY 2013
VL 51
IS 7
BP 4085
EP 4102
DI 10.1109/TGRS.2012.2229466
PN 2
PG 18
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 171QI
UT WOS:000320943700002
ER
PT J
AU Skofronick-Jackson, GM
Johnson, BT
Munchak, SJ
AF Skofronick-Jackson, Gail M.
Johnson, Benjamin T.
Munchak, S. Joseph
TI Detection Thresholds of Falling Snow From Satellite-Borne Active and
Passive Sensors
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Clouds; Earth; remote sensing; water resources
ID LAND-SURFACE EMISSIVITY; MILLIMETER WAVELENGTHS; DATA ASSIMILATION;
IN-ORBIT; MICROWAVE; RETRIEVAL; RADAR; RADIOMETER; PARTICLES; SYSTEM
AB There is an increased interest in detecting and estimating the amount of falling snow reaching the Earth's surface in order to fully capture the global atmospheric water cycle. An initial step toward global spaceborne falling snow algorithms for current and future missions includes determining the thresholds of detection for various active and passive sensor channel configurations and falling snow events over land surfaces and lakes. In this paper, cloud resolving model simulations of lake effect and synoptic snow events were used to determine the minimum amount of snow (threshold) that could be detected by the following instruments: the W-band radar of CloudSat, Global Precipitation Measurement (GPM) Dual-Frequency Precipitation Radar (DPR) Ku- and Ka-bands, and the GPM Microwave Imager. Eleven different nonspherical snowflake shapes were used in the analysis. Notable results include the following: 1) The W-band radar has detection thresholds more than an order of magnitude lower than the future GPM radars; 2) the cloud structure macrophysics influences the thresholds of detection for passive channels (e.g., snow events with larger ice water paths and thicker clouds are easier to detect); 3) the snowflake microphysics (mainly shape and density) plays a large role in the detection threshold for active and passive instruments; 4) with reasonable assumptions, the passive 166-GHz channel has detection threshold values comparable to those of the GPM DPR Ku- and Ka-band radars with similar to 0.05 g . m(-3) detected at the surface, or an similar to 0.5-1.0-mm . h(-1) melted snow rate. This paper provides information on the light snowfall events missed by the sensors and not captured in global estimates.
C1 [Skofronick-Jackson, Gail M.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Branch, Greenbelt, MD 20771 USA.
[Johnson, Benjamin T.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Munchak, S. Joseph] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Skofronick-Jackson, GM (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Branch, Greenbelt, MD 20771 USA.
EM Gail.S.Jackson@nasa.gov; Benjamin.T.Johnson@nasa.gov;
s.j.munchak@nasa.gov
RI Skofronick-Jackson, Gail/D-5354-2012; Measurement, Global/C-4698-2015;
Johnson, Benjamin/E-8557-2015
OI Johnson, Benjamin/0000-0003-3444-9669
FU National Aeronautics and Space Administration Headquarters
FX Manuscript received May 3, 2012; revised September 17, 2012; accepted
October 14, 2012. Date of publication February 1, 2013; date of current
version June 20, 2013. This work was supported in part by Dr. Ramesh
Kakar and in part by Dr. Hal Maring at the National Aeronautics and
Space Administration Headquarters through Precipitation Measurement
Mission funding and CloudSat funding, respectively.
NR 35
TC 5
Z9 5
U1 1
U2 26
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 JUL
PY 2013
VL 51
IS 7
BP 4177
EP 4189
DI 10.1109/TGRS.2012.2227763
PN 2
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 171QI
UT WOS:000320943700008
ER
PT J
AU Wu, AS
Xiong, XX
Doelling, DR
Morstad, D
Angal, A
Bhatt, R
AF Wu, Aisheng
Xiong, Xiaoxiong
Doelling, David R.
Morstad, Daniel
Angal, Amit
Bhatt, Rajendra
TI Characterization of Terra and Aqua MODIS VIS, NIR, and SWIR Spectral
Bands' Calibration Stability
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aqua; calibration; MODIS; stability; Terra
ID REFLECTIVE SOLAR BANDS; INTERSATELLITE CALIBRATION; AEROSOL PROPERTIES;
VISIBLE CHANNEL; TEMPERATURE; INSTRUMENT; SATELLITES; ATMOSPHERE;
CLOUDS; SYSTEM
AB The Moderate Resolution Imaging Spectroradiometer (MODIS) has successfully operated onboard the Terra spacecraft for more than 12 years and the Aqua spacecraft for more than ten years. It has 20 reflective solar bands covering the visible (VIS), near infrared (NIR), and short-wave infrared (SWIR) spectral regions. They are calibrated on orbit using regularly scheduled solar diffuser measurements and lunar observations. In recent years, observations over selected ground targets are also used to monitor detector responses at different angles of incidence. This paper provides a brief description of MODIS on-orbit calibration and characterization methodologies and examines the calibration stability of the VIS, NIR, and SWIR spectral bands over the entire missions of both instruments. Results obtained from four different vicarious approaches (deserts, Dome Concordia, deep convective cloud, and simultaneous nadir overpass) show that Terra MODIS VIS and NIR spectral bands have a wavelength-dependent drift in reflectance with a drop up to 8% in the shortest wavelength region. All four approaches have a relative agreement to within 2.0% with an uncertainty of less than 1.5% for most bands. It is anticipated that the improvements made in the MODIS Collection 6, with additional corrections based on the desert reflectance trending results, will significantly reduce, if not completely remove, some of the trending drifts identified in the Collection-5 data product.
C1 [Wu, Aisheng] Sigma Space Corp, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Doelling, David R.] NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23630 USA.
[Morstad, Daniel; Bhatt, Rajendra] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Angal, Amit] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Wu, AS (reprint author), Sigma Space Corp, Lanham, MD 20706 USA.
EM aisheng.wu@sigmaspace.com; Xiaoxiong.Xiong-1@nasa.gov;
david.r.doelling@nasa.gov; daniel.morstad@nasa.gov;
amit.angal@ssaihq.com; rajendra.bhatt@nasa.gov
NR 29
TC 31
Z9 34
U1 1
U2 22
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 JUL
PY 2013
VL 51
IS 7
BP 4330
EP 4338
DI 10.1109/TGRS.2012.2226588
PN 2
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 171QI
UT WOS:000320943700020
ER
PT J
AU Venters, TM
Pavlidou, V
AF Venters, T. M.
Pavlidou, V.
TI Probing the intergalactic magnetic field with the anisotropy of the
extragalactic gamma-ray background
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE magnetic fields; galaxies: active; BL Lacertae objects: general;
galaxies: starburst; diffuse radiation
ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES;
ELECTROMAGNETIC CASCADES; TEV BLAZARS; FERMI; RADIATION; CONSTRAINTS;
EMISSION; UNIVERSE
AB The intergalactic magnetic field (IGMF) may leave an imprint on the angular anisotropy of the extragalactic gamma-ray background through its effect on electromagnetic cascades triggered by interactions between very high energy photons and the extragalactic background light. A strong IGMF will deflect secondary particles produced in these cascades and will thus tend to isotropize lower energy cascade photons, thereby inducing a modulation in the anisotropy energy spectrum of the gamma-ray background. Here, we present a simple, proof-of-concept calculation of the magnitude of this effect and demonstrate that current Fermi data already seem to prefer non-negligible IGMF values. The anisotropy energy spectrum of the Fermi gamma-ray background could thus be used as a probe of the IGMF strength.
C1 [Venters, T. M.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pavlidou, V.] Max Planck Inst Radioastron, DE-53121 Bonn, Germany.
[Pavlidou, V.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
RP Venters, TM (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
EM tonia.m.venters@nasa.gov; pavlidou@physics.uoc.gr
RI Pavlidou, Vasiliki/C-2944-2011
OI Pavlidou, Vasiliki/0000-0002-0870-1368
NR 60
TC 6
Z9 6
U1 0
U2 4
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 JUL
PY 2013
VL 432
IS 4
BP 3485
EP 3494
DI 10.1093/mnras/stt697
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 173BR
UT WOS:000321053500071
ER
PT J
AU Huang, H
Ren, YX
Yan, Y
Ahmed, N
Yue, Y
Bozovich, A
Erkmen, BI
Birnbaum, K
Dolinar, S
Tur, M
Willner, AE
AF Huang, Hao
Ren, Yongxiong
Yan, Yan
Ahmed, Nisar
Yue, Yang
Bozovich, Amanda
Erkmen, Baris I.
Birnbaum, Kevin
Dolinar, Sam
Tur, Moshe
Willner, Alan E.
TI Phase-shift interference-based wavefront characterization for orbital
angular momentum modes
SO OPTICS LETTERS
LA English
DT Article
ID INTERFEROMETRY; SINGULARITIES; SENSOR
AB Wavefront characterization for orbital angular momentum (OAM) modes is demonstrated using quadrature phase-shift interference. The phase fronts and intensity profiles of OAM(-2), OAM(-4), OAM(-6), and OAM(-8) are measured. Wavefront correlations between the experimental results and the pure Laguerre-Gaussian modes are calculated to evaluate the measurement. The measured results are in reasonable agreement with the anticipated results based on simulations. (C) 2013 Optical Society of America
C1 [Huang, Hao; Ren, Yongxiong; Yan, Yan; Ahmed, Nisar; Yue, Yang; Bozovich, Amanda; Willner, Alan E.] Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
[Erkmen, Baris I.; Birnbaum, Kevin; Dolinar, Sam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tur, Moshe] Tel Aviv Univ, Sch Elect Engn, IL-69978 Tel Aviv, Israel.
RP Huang, H (reprint author), Univ So Calif, Dept Elect Engn, Los Angeles, CA 90089 USA.
EM haoh@usc.edu
FU DARPA under InPho (Information in a Photon) program
FX We acknowledge the support of DARPA under InPho (Information in a
Photon) program.
NR 17
TC 14
Z9 14
U1 0
U2 17
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 JUL 1
PY 2013
VL 38
IS 13
BP 2348
EP 2350
DI 10.1364/OL.38.002348
PG 3
WC Optics
SC Optics
GA 175VU
UT WOS:000321262500062
PM 23811924
ER
PT J
AU Tsuchiya, H
Enoto, T
Iwata, K
Yamada, S
Yuasa, T
Kitaguchi, T
Kawaharada, M
Nakazawa, K
Kokubun, M
Kato, H
Okano, M
Tamagawa, T
Makishima, K
AF Tsuchiya, H.
Enoto, T.
Iwata, K.
Yamada, S.
Yuasa, T.
Kitaguchi, T.
Kawaharada, M.
Nakazawa, K.
Kokubun, M.
Kato, H.
Okano, M.
Tamagawa, T.
Makishima, K.
TI Hardening and Termination of Long-Duration gamma Rays Detected Prior to
Lightning
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID ELECTRIC-FIELDS; X-RAYS; THUNDERSTORM; AIR; THUNDERCLOUDS; BURSTS
AB We report the first observation of 3-30 MeV prolonged gamma-ray emission that was abruptly terminated by lightning. The gamma-ray detection was made during winter thunderstorms on December 30, 2010, by the Gamma-Ray Observation of Winter Thunderclouds experiment carried out in a coastal area along the Sea of Japan. The gamma-ray flux lasted for less than 3 min, continuously hardening closer to the lightning occurrence. The hardening at energies of 3-10 MeV energies was most prominent. The gamma-ray flux abruptly ceased less than 800 ms before the lightning flash that occurred over 5 km away from the experimental site. In addition, we observed a clear difference in the duration of the 3-10 MeV gamma rays and those >10 MeV, suggesting that the area of >10 MeV gamma-ray emission is considerably smaller than that of the lower-energy gamma rays. This work may give a manifestation that a local region emitting prolonged gamma rays connects with a distant region to initiate lightning.
C1 [Tsuchiya, H.] Japan Atom Energy Agcy, Tokai, Ibaraki 3191195, Japan.
[Tsuchiya, H.; Enoto, T.; Yamada, S.; Kitaguchi, T.; Kato, H.; Okano, M.; Tamagawa, T.] RIKEN, High Energy Astrophys Lab, Wako, Saitama 3510198, Japan.
[Enoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Iwata, K.] Shibaura Inst Techmol, Saitama 3378570, Japan.
[Yuasa, T.; Kawaharada, M.; Kokubun, M.] JAXA, Inst Space & Astronaut Sci, Dept High Energy Astrophys, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Nakazawa, K.; Makishima, K.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
RP Tsuchiya, H (reprint author), Japan Atom Energy Agcy, Tokai, Ibaraki 3191195, Japan.
OI Tsuchiya, Harufumi/0000-0002-5581-0006
FU Suimitomo Foundation; Special Postdoctoral Research Project for Basic
Science in RIKEN; [24740183]
FX We deeply thank members of radiation safety group of Kashiwazaki-Kariwa
power station, TEPCO. The present work is supported in part by the
Suimitomo Foundation, the Special Postdoctoral Research Project for
Basic Science in RIKEN, and the Grant-in-Aid for Young Scientists No.
24740183.
NR 26
TC 8
Z9 8
U1 0
U2 8
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 JUL 1
PY 2013
VL 111
IS 1
AR 015001
DI 10.1103/PhysRevLett.111.015001
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 174BB
UT WOS:000321126500007
PM 23863005
ER
PT J
AU Lin, SY
Splinter, SC
Tarkenton, C
Paddock, DA
Smeltzer, SS
Ghose, S
Guzman, JC
McCarville, DA
Sutkus, DJ
AF Lin, S. -Y.
Splinter, S. C.
Tarkenton, C.
Paddock, D. A.
Smeltzer, S. S.
Ghose, S.
Guzman, J. C.
McCarville, D. A.
Sutkus, D. J.
TI Fabrication and Testing of Durable Redundant and Fluted-Core Joints for
Composite Sandwich Structures
SO SAMPE JOURNAL
LA English
DT Article
AB The development of durable bonded joint technology for assembling composite structures is an essential component of future space technologies. While NASA is working toward providing an entirely new capability for human space exploration beyond low Earth orbit, the objective of this project is to design, fabricate, analyze, and test a NASA patented durable redundant joint (DRJ) and a NASA/Boeing co-designed fluted-core joint (FCJ). The potential applications include a wide range of sandwich structures for NASA's future launch vehicles.
Three types of joints were studied splice joint (Si, as baseline), DRJ, and FCJ. Tests included tension, after-impact tension, and compression: Teflon strips were used at the joint area to increase failure strength by shifting stress concentration to a less sensitive area. Test results were compared to those of pristine coupons fabricated utilizing the same methods. Tensile test results indicated that the DRJ design was stiffer, stronger, and more impact resistant than other designs. The drawbacks of the DRJ design were extra mass and complex fabrication processes. The FCJ was lighter than the DRJ but less impact resistant. With barely visible but detectable impact damages, all three joints showed no sign of tensile strength reduction. No compression test was conducted on any impact-damaged sample due to limited scope and resource. Failure modes and damage propagation were also studied to support progressive damage modeling of the Si and the DRJ.
C1 [Lin, S. -Y.; Splinter, S. C.; Tarkenton, C.; Paddock, D. A.; Smeltzer, S. S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Ghose, S.; Guzman, J. C.; McCarville, D. A.] Boeing Co, Seattle, WA USA.
[Sutkus, D. J.] Mosley Tech Serv, Huntsville, AL USA.
RP Lin, SY (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 7
TC 0
Z9 0
U1 0
U2 2
PU SAMPE PUBLISHERS
PI COVINA
PA 1161 PARKVIEW DRIVE, COVINA, CA 91722 USA
SN 0091-1062
J9 SAMPE J
JI Sampe J.
PD JUL-AUG
PY 2013
VL 49
IS 4
BP 30
EP 39
PG 10
WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 171FN
UT WOS:000320910600004
ER
PT J
AU Moore, TE
Burch, JL
Daughton, WS
Fuselier, SA
Hasegawa, H
Petrinec, SM
Pu, ZY
AF Moore, T. E.
Burch, J. L.
Daughton, W. S.
Fuselier, S. A.
Hasegawa, H.
Petrinec, S. M.
Pu, Zuyin
TI Multiscale studies of the three-dimensional dayside X-line
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Reconnection; Magnetosphere; Multiscale; Plasma; Magnetic
ID MAGNETIC RECONNECTION; CLUSTER OBSERVATIONS; MAGNETOPAUSE; FIELD;
BOUNDARY
AB We review recent experience from the Cluster, Double Star, and THEMIS missions for lessons that apply to the upcoming Magnetospheric Multiscale Mission (MMS) being developed for launch in 2014. On global scales, simulation and statistical studies lead to mean configurations of dayside reconnection, implying specific relative alignments of the inflow magnetic fields and X-line, with implications for MMS operations designed to maximize the number of close encounters with the diffusion region. At intermediate MHD-to-ion scales, reconstruction of features created by one or two X-lines have developed to the point where data from a cluster of spacecraft can determine their temporal trends and the approximate three-dimensional X-line structure. Recent petascale particle-in-cell (PIC) simulations of reconnection encompass three spatial dimensions with excellent resolution, and make striking predictions of electron scale physics that creates complex interacting flux ropes under component reconnection. High time resolution measurements from MMS will determine the detailed electron scale kinetics embedded within the global and MHD-ion scale contexts. These developments will lead to the refinement of our three-dimensional multiscale picture of reconnection, yielding improved understanding of the global, MHD, and local physics controlling the onset or quenching, variability, and mean rate of reconnection. This in turn will enable improved predictability of the structural features created by transient reconnection, and their space weather consequences. Published by Elsevier Ltd.
C1 [Moore, T. E.] NASA, Goddard SFC, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Burch, J. L.; Fuselier, S. A.] Southwest Res Inst, San Antonio, TX 78238 USA.
[Daughton, W. S.] Los Alamos Natl Labs, Los Alamos, NM 87545 USA.
[Petrinec, S. M.] Lockheed Martin ATC, Palo Alto, CA 94304 USA.
[Pu, Zuyin] Beijing Univ, Dept Geophys, Beijing 100871, Peoples R China.
RP Moore, TE (reprint author), NASA, Goddard SFC, Heliophys Sci Div, Code 670,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM t.e.moore@nasa.gov; jburch@swri.org; daughton@lanl.gov;
hase@stp.isas.jaxa.jp; steven.m.petrinec@lmco.com; zypu@pku.edu.cn
RI Hasegawa, Hiroshi/A-1192-2007; Moore, Thomas/D-4675-2012; Daughton,
William/L-9661-2013; NASA MMS, Science Team/J-5393-2013
OI Hasegawa, Hiroshi/0000-0002-1172-021X; Moore,
Thomas/0000-0002-3150-1137; NASA MMS, Science Team/0000-0002-9504-5214
FU NASA Magnetospheric Multiscale project at Goddard Space Flight Center
FX This work was supported by the NASA Magnetospheric Multiscale project at
Goddard Space Flight Center. The authors are grateful to the ISROSES
Conference organizers for the opportunity to present this material in
draft form there.
NR 39
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U1 0
U2 15
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 JUL
PY 2013
VL 99
SI SI
BP 32
EP 40
DI 10.1016/j.jastp.2012.10.004
PG 9
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 165OS
UT WOS:000320493800005
ER
PT J
AU Budak, S
Parker, R
Smith, C
Muntele, C
Heidary, K
Johnson, RB
Ila, D
AF Budak, Satilmis
Parker, Robert
Smith, Cydale
Muntele, Claudiu
Heidary, Kaveh
Johnson, Ralph B.
Ila, Daryush
TI Superlattice multinanolayered thin films of SiO2/SiO2 + Ge for
thermoelectric device applications
SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES
LA English
DT Article; Proceedings Paper
CT 6th Annual Energy Harvesting Workshop
CT 6th Annual Energy Harvesting Workshop
CY AUG 07-11, 2011
CY AUG 07-11, 2011
CL Roanoke, VA
CL Roanoke, VA
DE Ion bombardment; thermoelectric properties; transport properties;
multinanolayers; figure of merit
ID THERMOELECTRIC PROPERTIES; POWER-GENERATION; NANOSTRUCTURES; SIO2;
EFFICIENCY; GROWTH
AB Thermoelectric generators convert heat to electricity. Effective thermoelectric materials and devices have a low thermal conductivity and a high electrical conductivity. The performance of thermoelectric materials and devices is shown by a dimensionless figure of merit, ZT = S-2 sigma T/K, where S is the Seebeck coefficient, sigma is the electrical conductivity, T is the absolute temperature, and K is the thermal conductivity. We have prepared 100 alternating layers of SiO2/SiO2+ Ge superlattice thin films using ion beam-assisted deposition for the thermoelectric generator device application. The 5 MeV Si ion bombardments were performed using the Center for Irradiation Materials' Pelletron ion beam accelerator to form quantum dots and/or quantum clusters in the multinanolayer superlattice thin films to decrease the cross-plane thermal conductivity and increase the cross-plane Seebeck coefficient and cross-plane electrical conductivity. The thermoelectric and transport properties have been characterized for SiO2/SiO2+ Ge superlattice thin films.
C1 [Budak, Satilmis; Heidary, Kaveh] Alabama A&M Univ, Dept Elect Engn & Comp Sci, Normal, AL 35762 USA.
[Parker, Robert] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Smith, Cydale] Alabama A&M Univ, CIM, Normal, AL 35762 USA.
[Muntele, Claudiu] Cygnus Sci Serv, Huntsville, AL USA.
[Johnson, Ralph B.] Alabama A&M Univ, Dept Phys, Normal, AL 35762 USA.
[Ila, Daryush] Fayetteville State Univ, Dept Chem & Phys, Fayetteville, NC USA.
RP Budak, S (reprint author), Alabama A&M Univ, Dept Elect Engn & Comp Sci, 4900 Meridian St,POB 1955, Normal, AL 35762 USA.
EM satilmis.budak@aamu.edu
FU Center for Irradiation of Materials (CIM); National Science Foundation
under NSF-EPSCOR R-II-3 Grant [EPS-0814103]; DOD under Nanotechnology
Infrastructure Development for Education and Research through the Army
Research Office [W911 NF-08-1-0425]; DOD Army Research Office [W911
NF-12-1-0063]
FX This research was sponsored by the Center for Irradiation of Materials
(CIM), National Science Foundation under NSF-EPSCOR R-II-3 Grant No.
EPS-0814103, DOD under Nanotechnology Infrastructure Development for
Education and Research through the Army Research Office # W911
NF-08-1-0425, and DOD Army Research Office # W911 NF-12-1-0063.
NR 36
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U1 0
U2 23
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1045-389X
EI 1530-8138
J9 J INTEL MAT SYST STR
JI J. Intell. Mater. Syst. Struct.
PD JUL
PY 2013
VL 24
IS 11
SI SI
BP 1357
EP 1364
DI 10.1177/1045389X13483022
PG 8
WC Materials Science, Multidisciplinary
SC Materials Science
GA 175AX
UT WOS:000321202700009
ER
PT J
AU Zhang, ZW
Lehner, MJ
Wang, JH
Wen, CY
Wang, SY
King, SK
Granados, AP
Alcock, C
Axelrod, T
Bianco, FB
Byun, YI
Chen, WP
Coehlo, NK
Cook, KH
de Pater, I
Kim, DW
Lee, T
Lissauer, JJ
Marshall, SL
Protopapas, P
Rice, JA
Schwamb, ME
AF Zhang, Z. -W.
Lehner, M. J.
Wang, J. -H.
Wen, C. -Y.
Wang, S. -Y.
King, S. -K.
Granados, A. P.
Alcock, C.
Axelrod, T.
Bianco, F. B.
Byun, Y. -I.
Chen, W. P.
Coehlo, N. K.
Cook, K. H.
de Pater, I.
Kim, D. -W.
Lee, T.
Lissauer, J. J.
Marshall, S. L.
Protopapas, P.
Rice, J. A.
Schwamb, M. E.
TI THE TAOS PROJECT: RESULTS FROM SEVEN YEARS OF SURVEY DATA
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE comets: general; Kuiper Belt: general; occultations; planets and
satellites: formation
ID KUIPER-BELT OBJECTS; JUPITER-FAMILY COMETS; TRANS-NEPTUNIAN OBJECTS;
OUTER SOLAR-SYSTEM; AMERICAN OCCULTATION SURVEY; SIZE DISTRIBUTION;
STELLAR OCCULTATIONS; COLLISIONAL EVOLUTION; LUMINOSITY FUNCTION;
MILLISECOND DIPS
AB The Taiwanese-American Occultation Survey (TAOS) aims to detect serendipitous occultations of stars by small (similar to 1 km diameter) objects in the Kuiper Belt and beyond. Such events are very rare (<10(-3) events per star per year) and short in duration (similar to 200 ms), so many stars must be monitored at a high readout cadence. TAOS monitors typically similar to 500 stars simultaneously at a 5 Hz readout cadence with four telescopes located at Lulin Observatory in central Taiwan. In this paper, we report the results of the search for small Kuiper Belt objects (KBOs) in seven years of data. No occultation events were found, resulting in a 95% c. l. upper limit on the slope of the faint end of the KBO size distribution of q = 3.34-3.82, depending on the surface density at the break in the size distribution at a diameter of about 90 km.
C1 [Zhang, Z. -W.; Lehner, M. J.; Wang, J. -H.; Wen, C. -Y.; Wang, S. -Y.; King, S. -K.; Cook, K. H.; Lee, T.] Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Lehner, M. J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Lehner, M. J.; Alcock, C.; Protopapas, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Granados, A. P.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico.
[Axelrod, T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bianco, F. B.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Byun, Y. -I.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea.
[Byun, Y. -I.] Yonsei Univ, Univ Observ, Seoul 120749, South Korea.
[Chen, W. P.] Natl Cent Univ, Inst Astron, Jhongli 320, Taoyuan County, Taiwan.
[Coehlo, N. K.; Rice, J. A.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA.
[de Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kim, D. -W.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Lissauer, J. J.] NASA, Space Sci & Astrobiol Div 245 3, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Marshall, S. L.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Protopapas, P.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA.
[Schwamb, M. E.] Yale Univ, Dept Phys, New Haven, CT 06511 USA.
[Schwamb, M. E.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
RP Zhang, ZW (reprint author), Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan.
EM zwzhang@asiaa.sinica.edu.tw
RI Lee, Typhoon/N-8347-2013;
OI Lehner, Matthew/0000-0003-4077-0985; Schwamb, Megan/0000-0003-4365-1455
FU thematic research program [AS-88-TP-A02]; NSF [AST-0501681,
DMS-0636667]; NASA [NNG04G113G]; NRF [2011-0030875]; USDOE
[DE-AC02-76SF00515]; NASA's Planetary Geology and Geophysics Program;
[NSC101-2628-M-008-002]; [NSC 96-2112-M-008-024-MY3]
FX Work at ASIAA was supported in part by the thematic research program
AS-88-TP-A02. Work at NCU and at Lulin Observatory was supported in part
by grant NSC101-2628-M-008-002. Work at the CfA was supported in part by
the NSF under grant AST-0501681 and by NASA under grant NNG04G113G. Work
at Yonsei was supported by the NRF grant 2011-0030875. Work at NCU was
supported by the grant NSC 96-2112-M-008-024-MY3. Work at Berkeley was
supported in part by NSF grant DMS-0636667. Work at SLAC was performed
under USDOE contract DE-AC02-76SF00515. Work at NASA Ames was supported
by NASA's Planetary Geology and Geophysics Program.
NR 56
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUL
PY 2013
VL 146
IS 1
AR 14
DI 10.1088/0004-6256/146/1/14
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 166JP
UT WOS:000320551000014
ER
PT J
AU He, CM
Zeng, XW
Wilkinson, A
AF He, Chunmei
Zeng, Xiangwu
Wilkinson, Allen
TI Geotechnical Properties of GRC-3 Lunar Simulant
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Space exploration; Moon; Lunar materials; Soil properties; Exploration;
Geotechnical; Lunar simulant
ID SOIL
AB Geotechnical properties of the lunar regolith are critical parameters in the design of equipment for in situ resource utilization (ISRU) on the Moon. It is imperative to simulate the geotechnical behavior of the lunar soil properly in the development of such equipment. Soil strength depends on the preparation method as well as the properties of the granular raw material. To execute the many small- and large-scale equipment tests planned for ISRU, it is necessary to develop a simulant that is inexpensive and can be produced in large quantities. This paper presents the methodology behind developing such a lunar-like geotechnical soil, GRC-3, and compares the properties of this soil with those of lunar regolith. The results show that particle size distribution, specific gravity, bulk density, and shear strength parameters for several preparation protocols are similar to that of lunar soil. Therefore, GRC-3 can be used in future large-scale experiments to predict the performance of ISRU equipment on the Moon.
C1 [He, Chunmei] Barr & Prevost Inc, Columbus, OH 43231 USA.
[Zeng, Xiangwu] Case Western Reserve Univ, Dept Civil Engn, Cleveland, OH 44106 USA.
[Wilkinson, Allen] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP He, CM (reprint author), Barr & Prevost Inc, 2800 Corp Exchange Dr,Suite 240, Columbus, OH 43231 USA.
EM springmay_he@hotmail.com
FU NASA [NNX07A078G, NNX07AM35A]
FX The work reported here was carried out with support from NASA Grant
NNX07A078G and NNX07AM35A. The opinions expressed in this paper are that
of the authors and do not represent the official policies of the funding
agency.
NR 20
TC 4
Z9 5
U1 1
U2 12
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD JUL 1
PY 2013
VL 26
IS 3
BP 528
EP 534
DI 10.1061/(ASCE)AS.1943-5525.0000162
PG 7
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 163VZ
UT WOS:000320366900002
ER
PT J
AU Fisher, JB
Malhi, Y
Torres, IC
Metcalfe, DB
van de Weg, MJ
Meir, P
Silva-Espejo, JE
Huasco, WH
AF Fisher, Joshua B.
Malhi, Yadvinder
Cuba Torres, Israel
Metcalfe, Daniel B.
van de Weg, Martine J.
Meir, Patrick
Silva-Espejo, Javier E.
Huaraca Huasco, Walter
TI Nutrient limitation in rainforests and cloud forests along a 3,000-m
elevation gradient in the Peruvian Andes
SO OECOLOGIA
LA English
DT Article
DE Fertilization; Forest; Montane; Nitrogen; Phosphorus; Tropical
ID TROPICAL MONTANE FOREST; N-P RATIOS; TREE GROWTH; PHOSPHORUS
FERTILIZATION; PRIMARY PRODUCTIVITY; PLANT FERTILIZATION;
MINERAL-NUTRITION; SOIL RESPIRATION; LEAF TRAITS; NITROGEN
AB We report results from a large-scale nutrient fertilization experiment along a "megadiverse" (154 unique species were included in the study) 3,000-m elevation transect in the Peruvian Andes and adjacent lowland Amazonia. Our objectives were to test if nitrogen (N) and phosphorus (P) limitation shift along this elevation gradient, and to determine how an alleviation of nutrient limitation would manifest in ecosystem changes. Tree height decreased with increasing elevation, but leaf area index (LAI) and diameter at breast height (DBH) did not vary with elevation. Leaf N:P decreased with increasing elevation (from 24 at 200 m to 11 at 3,000 m), suggesting increased N limitation and decreased P limitation with increasing elevation. After 4 years of fertilization (N, P, N + P), plots at the lowland site (200 m) fertilized with N + P showed greater relative growth rates in DBH than did the control plots; no significant differences were evident at the 1,000 m site, and plots fertilized with N at the highest elevation sites (1,500, 3,000 m) showed greater relative growth rates in DBH than did the control plots, again suggesting increased N constraint with elevation. Across elevations in general N fertilization led to an increase in microbial respiration, while P and N + P addition led to an increase in root respiration and corresponding decrease in hyphal respiration. There was no significant canopy response (LAI, leaf nutrients) to fertilization, suggesting that photosynthetic capacity was not N or P limited in these ecosystems. In sum, our study significantly advances ecological understanding of nutrient cycling and ecosystem response in a region where our collective knowledge and data are sparse: we demonstrate N limitation in high elevation tropical montane forests, N and P co-limitation in lowland Amazonia, and a nutrient limitation response manifested not in canopy changes, but rather in stem and belowground changes.
C1 [Fisher, Joshua B.; Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England.
[Cuba Torres, Israel; Silva-Espejo, Javier E.; Huaraca Huasco, Walter] Univ San Antonio, Dept Biol, Abad Del Cusco, Cusco, Peru.
[Metcalfe, Daniel B.] Swedish Univ Agr Sci, Dept Forest Ecol & Management, S-90660 Umea, Sweden.
[van de Weg, Martine J.] Vrije Univ Amsterdam, Amsterdam Global Change Inst, NL-1081 HV Amsterdam, Netherlands.
[Meir, Patrick] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9XP, Midlothian, Scotland.
RP Fisher, JB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM joshbfisher@gmail.com
RI Meir, Patrick/J-8344-2012;
OI Fisher, Joshua/0000-0003-4734-9085
FU NERC [NE/D014174/1, NE/F002149/1]; Gordon and Betty Moore foundation;
Andes Biodiversity and Ecosystem Research Group (ABERG); Jackson
Foundation; Royal Society of Edinburgh; Amazon Basin Conservation
Association (ACCA); Wayqecha field station; Explorers' Inn at Tambopata
FX This project was supported by a NERC-funded grant (NE/D014174/1) and by
the Gordon and Betty Moore foundation, and is a product of the Andes
Biodiversity and Ecosystem Research Group (ABERG). Y.M. was supported by
the Jackson Foundation. P. M. was supported by the Royal Society of
Edinburgh and NERC Grant NE/F002149/1. We thank INRENA and Manu National
Park for permits to work in the area, the Amazon Basin Conservation
Association (ACCA) and their Wayqecha field station, and the Explorers'
Inn at Tambopata for supporting our work in Peru. We are grateful to, F.
F. Amezquita, L.E.O.C. Aragao, L. D. Baca, K. G. Cabrera, R. Ccacya, K.
Clark, C.A.J. Girardin, J.A.Q. Loayza, A. A. V. Maucaylla, J.K. Mamani,
T. Marthews, P.O.C. Porroa, V. Qquellon, A.J.C. Quispe, J.S. Quispe,
M.N.R. Quisiyupanqui, W. F. Rios, N. Salinas, J.F.M. Solorzano, M. M.
Solorzano, M. I. A. Soto, S.-Y. Tan, S. Ynuma, and M. Zimmermann for
assistance and field work help. Two anonymous reviewers and the journal
editors provided invaluable suggestions that substantially improved the
manuscript.
NR 85
TC 51
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U1 11
U2 137
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD JUL
PY 2013
VL 172
IS 3
BP 889
EP 902
DI 10.1007/s00442-012-2522-6
PG 14
WC Ecology
SC Environmental Sciences & Ecology
GA 164KX
UT WOS:000320409100024
PM 23180422
ER
PT J
AU LeBlanc, A
Matsumoto, T
Jones, J
Shapiro, J
Lang, T
Shackelford, L
Smith, SM
Evans, H
Spector, E
Ploutz-Snyder, R
Sibonga, J
Keyak, J
Nakamura, T
Kohri, K
Ohshima, H
AF LeBlanc, A.
Matsumoto, T.
Jones, J.
Shapiro, J.
Lang, T.
Shackelford, L.
Smith, S. M.
Evans, H.
Spector, E.
Ploutz-Snyder, R.
Sibonga, J.
Keyak, J.
Nakamura, T.
Kohri, K.
Ohshima, H.
TI Bisphosphonates as a supplement to exercise to protect bone during
long-duration spaceflight
SO OSTEOPOROSIS INTERNATIONAL
LA English
DT Article
DE Bisphosphonates; Bone loss; Computed bone strength; Exercise; QCT;
Spaceflight
ID PROXIMAL FEMORAL STRENGTH; RENAL STONE FORMATION; TERM BED REST;
SPACE-FLIGHT; RESISTIVE EXERCISE; FEMUR FRACTURES; BODY SCANS;
OSTEONECROSIS; ASTRONAUTS; PRECISION
AB We report the results of alendronate ingestion plus exercise in preventing the declines in bone mass and strength and elevated levels of urinary calcium and bone resorption in astronauts during 5.5 months of spaceflight.
This investigation was an international collaboration between NASA and the JAXA space agencies to investigate the potential value of antiresorptive agents to mitigate the well-established bone changes associated with long-duration spaceflight.
We report the results from seven International Space Station (ISS) astronauts who spent a mean of 5.5 months on the ISS and who took an oral dose of 70 mg of alendronate weekly starting 3 weeks before flight and continuing throughout the mission. All crewmembers had available for exercise a treadmill, cycle ergometer, and a resistance exercise device. Our assessment included densitometry of multiple bone regions using X-ray absorptiometry (DXA) and quantitative computed tomography (QCT) and assays of biomarkers of bone metabolism.
In addition to pre- and post-flight measurements, we compared our results to 18 astronauts who flew ISS missions and who exercised using an early model resistance exercise device, called the interim resistance exercise device, and to 11 ISS astronauts who exercised using the newer advanced resistance exercise device (ARED). Our findings indicate that the ARED provided significant attenuation of bone loss compared with the older device although post-flight decreases in the femur neck and hip remained. The combination of the ARED and bisphosphonate attenuated the expected decline in essentially all indices of altered bone physiology during spaceflight including: DXA-determined losses in bone mineral density of the spine, hip, and pelvis, QCT-determined compartmental losses in trabecular and cortical bone mass in the hip, calculated measures of fall and stance computed bone strength of the hip, elevated levels of bone resorption markers, and urinary excretion of calcium.
The combination of exercise plus an antiresoptive drug may be useful for protecting bone health during long-duration spaceflight.
C1 [LeBlanc, A.; Ploutz-Snyder, R.] Univ Space Res Assoc, Houston, TX 77058 USA.
[Matsumoto, T.] Univ Tokushima, Grad Sch Med Sci, Dept Med & Bioregulatory Sci, Tokushima 7708503, Japan.
[Jones, J.] Baylor Coll Med, Ctr Space Med, Houston, TX 77030 USA.
[Shapiro, J.] Kennedy Krieger Inst, Baltimore, MD 21205 USA.
[Lang, T.] Univ Calif San Francisco, Dept Radiol, San Francisco, CA 94143 USA.
[Shackelford, L.; Smith, S. M.; Sibonga, J.] NASA, Lyndon B Johnson Space Ctr, Human & Adaptat Countermeasure Div, Houston, TX 77058 USA.
[Evans, H.; Spector, E.] Wyle, Houston, TX 77058 USA.
[Keyak, J.] Univ Calif Irvine, Dept Radiol Sci, Irvine, CA 92697 USA.
[Nakamura, T.] Univ Occupat & Environm, Dept Orthoped Surg, Kitakyushu, Fukuoka, Japan.
[Kohri, K.] Nagoya City Univ, Dept Nephrol, Nagoya, Aichi, Japan.
[Ohshima, H.] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki, Japan.
RP LeBlanc, A (reprint author), Univ Space Res Assoc, 3600 Bay Area Blvd, Houston, TX 77058 USA.
EM leblanc@dsls.usra.edu
FU National Aeronautic Space Administration; Japan Aerospace Exploration
Agency
FX This project was supported by the Human Research Program at the National
Aeronautic Space Administration and the Japan Aerospace Exploration
Agency. We wish to thank Curtis Kershner, Karen Lawrence, and Michelle
Lawless of Lockheed Martin for their help in managing the experiment
documentation, along with Lisa King and Scott A Smith of Wyle for their
help in acquiring the DXA and pQCT data. The authors would especially
like to thank the astronauts who participated in this research project.
NR 41
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U1 4
U2 29
PU SPRINGER LONDON LTD
PI LONDON
PA 236 GRAYS INN RD, 6TH FLOOR, LONDON WC1X 8HL, ENGLAND
SN 0937-941X
J9 OSTEOPOROSIS INT
JI Osteoporosis Int.
PD JUL
PY 2013
VL 24
IS 7
BP 2105
EP 2114
DI 10.1007/s00198-012-2243-z
PG 10
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA 162RQ
UT WOS:000320283300018
PM 23334732
ER
PT J
AU Goodloe, AE
Munoz, CA
AF Goodloe, Alwyn E.
Munoz, Cesar A.
TI Compositional verification of a communication protocol for a remotely
operated aircraft
SO SCIENCE OF COMPUTER PROGRAMMING
LA English
DT Article
DE Protocol verification; Interactive theorem proving; Compositional
reasoning
ID SLIDING WINDOW PROTOCOL; ISABELLE/HOL; OWICKI/GRIES; PVS
AB This paper presents the formal specification and verification of a communication protocol between a ground station and a remotely operated aircraft. The protocol can be seen as the vertical composition of protocol layers, where each layer performs input and output message processing, and the horizontal composition of different processes concurrently inhabiting the same layer, where each process should satisfy a distinct delivery requirement. A compositional technique is used to formally prove that the protocol satisfies these requirements. Although the protocol itself is not novel, the methodology employed in its verification extends existing techniques by automating the tedious and usually cumbersome part of the proof, thereby making the iterative design process of protocols feasible. Published by Elsevier B.V.
C1 [Goodloe, Alwyn E.; Munoz, Cesar A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Goodloe, AE (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM a.goodloe@nasa.gov; Cesar.A.Munoz@nasa.gov
FU National Aeronautics and Space Administration under the NASA
[NNX08AE37A]
FX This work was supported by the National Aeronautics and Space
Administration under the NASA Cooperative Agreement NNX08AE37A awarded
to the National Institute of Aerospace (NIA) while the authors were
resident at the NIA. Authors are listed in alphabetical order.
NR 34
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-6423
J9 SCI COMPUT PROGRAM
JI Sci. Comput. Program.
PD JUL 1
PY 2013
VL 78
IS 7
BP 813
EP 827
DI 10.1016/j.scico.2011.10.011
PG 15
WC Computer Science, Software Engineering
SC Computer Science
GA 164PJ
UT WOS:000320421700004
ER
PT J
AU Jahanshahi, MR
Masri, SF
AF Jahanshahi, Mohammad R.
Masri, Sami F.
TI Parametric Performance Evaluation of Wavelet-Based Corrosion Detection
Algorithms for Condition Assessment of Civil Infrastructure Systems
SO JOURNAL OF COMPUTING IN CIVIL ENGINEERING
LA English
DT Article
DE Corrosion; Imaging techniques; Algorithms; Infrastructure; Parameters;
Corrosion detection; Color texture analysis; Multiresolution wavelet
analysis; Image processing
ID TEXTURE CLASSIFICATION; IMAGE SEGMENTATION; COLOR; DAMAGE
AB Corrosion is a crucial defect in structural systems that can lead to catastrophic effects if neglected. Current structure inspection standards require an inspector to visually assess the conditions of a target structure. A less time-consuming and inexpensive alternative to current monitoring methods is to use a robotic system, which can inspect structures more frequently and perform autonomous damage detection. The feasibility of using image processing techniques to detect corrosion in structures has been acknowledged by leading experts in the field; however, there has not been a systematic study to evaluate the effects of different parameters on the performance of vision-based corrosion detection systems. This study evaluates several parameters that can affect the performance of color wavelet-based texture analysis algorithms for detecting corrosion. Furthermore, an approach is proposed to utilize the depth perception for corrosion detection. The proposed approach improves the reliability of the corrosion detection algorithm. The integration of depth perception with pattern classification algorithms, which has never been reported in published studies, is part of the contribution of the current study. Several quantitative evaluations are presented to scrutinize the performance of the investigated approaches.
C1 [Jahanshahi, Mohammad R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jahanshahi, Mohammad R.; Masri, Sami F.] Univ So Calif, Viterbi Sch Engn, Sonny Astani Dept Civil & Environm Engn, Los Angeles, CA 90089 USA.
RP Jahanshahi, MR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 198-235, Pasadena, CA 91109 USA.
EM mohammad@caltech.edu; masri@usc.edu
FU U.S. National Science Foundation
FX This study was supported in part by grants from the U.S. National
Science Foundation. The authors would like to thank Dr. Zahra Tehrani
for her critical reading of the manuscript, and Prof. Antonio Ortega,
Prof. Gerard Medioni and Prof. Jay Kuo from the Department of Electrical
Engineering at University of Southern California for their constructive
feedback on this study.
NR 32
TC 0
Z9 0
U1 2
U2 8
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0887-3801
J9 J COMPUT CIVIL ENG
JI J. Comput. Civil. Eng.
PD JUL 1
PY 2013
VL 27
IS 4
BP 345
EP 357
DI 10.1061/(ASCE)CP.1943-5487.0000225
PG 13
WC Computer Science, Interdisciplinary Applications; Engineering, Civil
SC Computer Science; Engineering
GA 160FL
UT WOS:000320102700002
ER
PT J
AU Jolitz, RD
McKay, CP
AF Jolitz, Rebecca D.
McKay, Christopher P.
TI Quantitative 3D Model of Light Transmittance Through Translucent Rocks
Applied to the Hypolithic Microbial Community
SO MICROBIAL ECOLOGY
LA English
DT Article
ID DESERT; CYANOBACTERIA; HOT; PHOTOSYNTHESIS; COLONIZATION; ENVIRONMENT
AB In extreme desert environments, photosynthetic microorganisms often live on the buried undersides of translucent rocks. Computing the light level reaching these locations requires 3D modeling of a finite rock. We report on Monte Carlo calculations of skylight and sunlight transmission through a partially buried flat cylindrical rock using one billion photons per simulation. Transmitted light level drops inversely with increasing rock opacity, as expected for purely scattering media. For a half-buried rock with an extinction coefficient of 0.1 cm(-1) (opacity of 0.2), transmission at the bottom is 64 % for sunlight at a solar zenith angle of 60A degrees and 82 % for skylight. Transmitted light level increases slowly with increasing scattering asymmetry factor of the rock independent of illumination or depth buried. Transmitted sunlight at zenith through a thick half-buried rock (opacity of 0.6) is six times brighter at the bottom than the subsurface sides. Skylight transmits equally to the subsurface sides and bottom. When the sun is not straight overhead, the sunward side of the rock is brighter than the underside of the rock. Compared to the sunlight transmitted to the bottom, transmitted sunlight inclined at 60A degrees is 24 times brighter at the subsurface side towards the sun and 14 times brighter at the subsurface side 70A degrees away from the sun. Transmitted sunlight emitted from zenith and skylight is uniformly bright at the bottom regardless of how deeply the rock is buried. Sunlight not at zenith transmits preferentially to the sunward bottom edge depending on the depth the rock is buried.
C1 [Jolitz, Rebecca D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Jolitz, RD (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
EM rjolitz@berkeley.edu
FU NASA's Astrobiology Program; Davidson Foundation
FX This research was supported by NASA's Astrobiology Program. R. D. J.
acknowledges support from the Davidson Foundation.
NR 26
TC 1
Z9 1
U1 4
U2 10
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0095-3628
J9 MICROB ECOL
JI Microb. Ecol.
PD JUL
PY 2013
VL 66
IS 1
BP 112
EP 119
DI 10.1007/s00248-013-0242-z
PG 8
WC Ecology; Marine & Freshwater Biology; Microbiology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology;
Microbiology
GA 159LX
UT WOS:000320048000012
PM 23666241
ER
PT J
AU Joshi, RP
Qiu, H
Tripathi, RK
AF Joshi, Ravindra P.
Qiu, Hao
Tripathi, Ram K.
TI Configuration studies for active electrostatic space radiation shielding
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Radiation; Shielding; Electrostatic; Toroidal geometry; Deep-space;
Spacecraft
ID MAGNETIC-FIELD; PROTECTION
AB Developing successful and optimal solutions to mitigating the hazards of severe space radiation in deep space long duration missions is critical for the success of deep-space explorations. Space crews traveling aboard interplanetary spacecraft will be exposed to a constant flux of galactic cosmic rays (GCR), as well as intense fluxes of charged particles during solar particle events (SPEs). A recent report (Tripathi et al., Adv. Space Res. 42 (2008) 1043-1049), had explored the feasibility of using electrostatic shielding in concert with the state-of-the-art materials shielding technologies. Here we continue to extend the electrostatic shielding strategy and quantitatively examine a different configuration based on multiple toroidal rings. Our results show that SPE radiation can almost be eliminated by these electrostatic configurations. Also, penetration probabilities for novel structures such as toroidal rings are shown to be substantially reduced as compared to the simpler all-sphere geometries. More interestingly, the dimensions and aspect ratio of the toroidal rings could be altered and optimized to achieve an even higher degree of radiation protection. (C) 2013 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Joshi, Ravindra P.; Qiu, Hao] Old Dominion Univ, Dept Elect & Comp Engn, Norfolk, VA 23529 USA.
[Tripathi, Ram K.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Joshi, RP (reprint author), Old Dominion Univ, Dept Elect & Comp Engn, Norfolk, VA 23529 USA.
EM rjoshi@odu.edu
FU NASA Innovative Advanced Concept (NIAC) Program; NASA Langley Research
Center [NNX11AG71G]
FX This work was supported in part by NASA Innovative Advanced Concept
(NIAC) Program. The team at Old Dominion University (RDJ and HQ)
acknowledges the NASA Langley Research Center for partial support
through grant no. NNX11AG71G. Finally, we would like to thank an unknown
reviewer for a particularly insightful and useful comment.
NR 28
TC 2
Z9 2
U1 1
U2 11
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 JUL-AUG
PY 2013
VL 88
BP 138
EP 145
DI 10.1016/j.actaastro.2013.03.011
PG 8
WC Engineering, Aerospace
SC Engineering
GA 151WG
UT WOS:000319490500013
ER
PT J
AU Lepot, K
Williford, KH
Ushikubo, T
Sugitani, K
Mimura, K
Spicuzza, MJ
Valley, JW
AF Lepot, Kevin
Williford, Kenneth H.
Ushikubo, Takayuki
Sugitani, Kenichiro
Mimura, Koichi
Spicuzza, Michael J.
Valley, John W.
TI Texture-specific isotopic compositions in 3.4 Gyr old organic matter
support selective preservation in cell-like structures
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID STRELLEY POOL FORMATION; ION MASS-SPECTROMETRY; INDIVIDUAL PRECAMBRIAN
MICROFOSSILS; MICROBIAL SULFATE REDUCTION; BARBERTON GREENSTONE-BELT;
EARLY ARCHEAN ERA; WESTERN-AUSTRALIA; PILBARA CRATON; APEX CHERT;
CARBONACEOUS-MATERIAL
AB Abundant cell-like organic structures have been proposed as microfossils in Paleoarchean (3.2-3.5 Ga) cherts. The wide range of delta C-13(org) values recorded in Paleoarchean organic matter (OM), including some of these possible microfossils, is difficult to reconcile with the smaller range observed in living cells and younger microfossils. Metamorphic and metasomatic effects on delta C-13(org) have been recognized in Paleoarchean rocks, but have never been assessed for cell-like structures. Migrations of OM, of which the textures can mimic microfossils, are also difficult to constrain in Paleoarchean cherts that are often cut by submillimeter-to meter-scale OM-bearing veins.
Here, we present the results of petrography, Raman microspectroscopy, and in situ analyses of delta C-13(org) and H/C using secondary ion mass spectrometry (SIMS) of diverse organic microstructures, including possible microfossils, from two localities of the 3.4-billion-year-old Strelley Pool Formation (Western Australia, SPF). For the first time, we show that the wide range of delta C-13(org) values recorded at the micrometer scale correlates with specific OM-texture types in the SPF. The cross-cutting texture and lower structural order show that the OM in micro-veins of one sample from the Goldsworthy greenstone belt (WF4) post-dates all other OM-texture types. Possible microfossils (spheres, lenses), clots and micrometer-scale globules all show a higher structural order reached during peak metamorphism. Other than late micro-veins, textures indicative of OM migration beyond the millimeter-scale are absent; hence the source of clots, lenses, spheres and globules is indigenous to the cherts. A weak positive relation between delta C-13(org) and H/C demonstrates that the 10 parts per thousand range in delta C-13(org) recorded in indigenous OM is not metamorphic or metasomatic in origin. Texture-specific isotopic compositions strongly argue against fully abiotic OM synthesis. Spherical cell-like structures have distinct delta C-13(org) values compared to all other organic textures: their distribution peaks between -35 parts per thousand and -36 parts per thousand in WF4 and averages -35.7 parts per thousand in sample PAN1-1A from the Panorama greenstone belt. Lenses are composed of a network of nanoscale OM with a relatively high H/C and delta C-13(org) (average -32 parts per thousand in WF4), and include globules with lower H/C and delta C-13(org) down to -40 parts per thousand. Similar globules also appear as isolated clusters. In both WF4 and PAN1-1A, delta C-13(org) of OM clots shows a bimodal distribution, the lower values overlapping with those of lenses. These heterogeneities can be explained by different carbon-fixation metabolisms, e.g. photosynthetic high delta C-13(org) lenses versus methanogenic low delta C-13(org) spheres. Alternatively, heterogeneities can be explained by selective diagenetic preservation of the distinct isotopic fractionations inherited from different precursor biomolecules. Selective preservation is supported by (i) coupled delta C-13(org)-H/C heterogeneities, (ii) the delta C-13(org) differences between cell-like structures and recondensed clots, (iii) internal isotopic heterogeneities in SPF lenses similar to heterogeneities in modern and fossil cells. These results support the interpretation of biogenicity of morphologically cellular structures in the SPF. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Lepot, Kevin; Williford, Kenneth H.; Ushikubo, Takayuki; Spicuzza, Michael J.; Valley, John W.] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, WiscSIMS, Madison, WI 53706 USA.
[Lepot, Kevin] Univ Lille 1, CNRS, UMR8217, Lab Geosyst, F-59655 Villeneuve Dascq, France.
[Williford, Kenneth H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sugitani, Kenichiro] Nagoya Univ, Grad Sch Environm Studies, Dept Environm Engn & Architecture, Nagoya, Aichi 4648601, Japan.
[Mimura, Koichi] Nagoya Univ, Grad Sch Environm Studies, Dept Earth & Environm Sci, Nagoya, Aichi 4648601, Japan.
RP Lepot, K (reprint author), Univ Lille 1, CNRS, UMR8217, Lab Geosyst, Batiment SN5, F-59655 Villeneuve Dascq, France.
EM kevin.lepot@univ-lille1.fr
RI Lepot, Kevin/C-7072-2014; Valley, John/B-3466-2011
OI Lepot, Kevin/0000-0003-0556-0405; Valley, John/0000-0003-3530-2722
FU NSF-EAR [0319230, 0744079, 1053466]; Japan Society for Promotion of
Science [22340149, 24654162]; CNRS-INSU INTERRVIE; NASA Astrobiology
Institute
FX We thank Noriko Kita, Jim Kern and Kouki Kitajima for assistance with
SIMS analyses, Brian Hess for expert SIMS mount preparation, Tsutomu
Nagaoka for thin section preparation, Christopher House (Penn State
University) for providing the PPRG215-1 standard, Myriam Moreau for
assistance with Raman analyses, and Sandra Ventalon for assistance with
CL imaging. We thank A. Nemchin (associate editor) and two anonymous
reviewers for constructive comments. Funding was provided by the NASA
Astrobiology Institute. The WiscSIMS Lab is partially funded by NSF-EAR
(0319230, 0744079, 1053466). Kenichiro Sugitani was funded by Japan
Society for Promotion of Science (Nos. 22340149 and 24654162). Raman
analyses were funded by CNRS-INSU INTERRVIE (K.L.).
NR 95
TC 16
Z9 17
U1 5
U2 60
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 JUL 1
PY 2013
VL 112
BP 66
EP 86
DI 10.1016/j.gca.2013.03.004
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 144WP
UT WOS:000318972800005
ER
PT J
AU Atli, KC
Franco, BE
Karaman, I
Gaydosh, D
Noebe, RD
AF Atli, K. C.
Franco, B. E.
Karaman, I.
Gaydosh, D.
Noebe, R. D.
TI Influence of crystallographic compatibility on residual strain of TiNi
based shape memory alloys during thermo-mechanical cycling
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE Shape memory alloys; Dimensional stability; Thermo-mechanical cycling;
Crystallographic compatibility; NiTi; NiTiPd
ID SEVERE PLASTIC-DEFORMATION; ZN-AL ALLOY; FUNCTIONAL STABILITY;
HEAT-TREATMENT; NITI ALLOY; HYSTERESIS; TRANSFORMATION; BEHAVIOR; PHASE
AB The primary focus of this study was to determine the influence of the inherent microstructure, specifically the crystallographic compatibility between martensite and austenite during the transformation process, on residual strain and strain evolution during isobaric thermal cycling. A series of predominantly single-phase Ti-rich TiNi based shape memory alloys (SMAs), including binary Ti50.1Ni49.9, two ternary TiNiPd25 compositions with slightly different Ni contents, Ti50.5Ni28.5Pt21, and a quaternary Ti50Ni24.5Pd25Sc0.5 alloy, were thermally cycled nominally 100 times at different stress levels. In all cases, the amount of residual strain per cycle was found to decrease asymptotically with increasing number of cycles to some finite value that was related to the compatibility of the transforming phases as determined by the middle eigenvalue of the transformation stretch tensor. In addition, the amount of residual strain generated during the early thermal cycles was also dependent on the resistance of the SMAs against defect propagation, which can be controlled by initial dislocation density and grain size among other factors. In light of these findings, it was concluded that a dimensionally stable SMA actuator for multiple cycle operation should have compatible transforming phases to reduce the generation of defects and a high resistance against defect propagation. (c) 2013 Elsevier B.V. All rights reserved.
C1 [Atli, K. C.; Franco, B. E.; Karaman, I.] Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA.
[Karaman, I.] Texas A&M Univ, Mat Sci & Engn Program, College Stn, TX 77843 USA.
[Gaydosh, D.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Gaydosh, D.; Noebe, R. D.] NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
RP Karaman, I (reprint author), Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA.
EM ikaraman@tamu.edu
RI Karaman, Ibrahim/E-7450-2010; Atli, Kadri/D-6978-2013
OI Karaman, Ibrahim/0000-0001-6461-4958; Atli, Kadri/0000-0002-4807-2113
FU NASA Fundamental Aeronautics Program (FAP), Subsonic Fixed Wing Project
[NNX07AB56A]; FAP Aeronautical Sciences Project
FX This study has been supported by the NASA Fundamental Aeronautics
Program (FAP), Subsonic Fixed Wing Project through Cooperative Agreement
no. NNX07AB56A, with additional support from the FAP Aeronautical
Sciences Project.
NR 29
TC 17
Z9 18
U1 7
U2 50
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD JUL 1
PY 2013
VL 574
BP 9
EP 16
DI 10.1016/j.msea.2013.02.035
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 146JT
UT WOS:000319088100002
ER
PT J
AU Faghihi, A
Tesch, J
Gibson, S
AF Faghihi, Azin
Tesch, Jonathan
Gibson, Steve
TI Identified state-space prediction model for aero-optical wavefronts
SO OPTICAL ENGINEERING
LA English
DT Article
DE system identification; prediction filter; optimal control; adaptive
optics; aero-optics
ID MULTICHANNEL LATTICE FILTER; DRIVEN H-2-OPTIMAL CONTROL; ADAPTIVE
OPTICS; PHASE SCREENS
AB A state-space disturbance model and associated prediction filter for aero-optical wavefronts are described. The model is computed by system identification from a sequence of wavefronts measured in an airborne laboratory. Estimates of the statistics and flow velocity of the wavefront data are shown and can be computed from the matrices in the state-space model without returning to the original data. Numerical results compare velocity values and power spectra computed from the identified state-space model with those computed from the aero-optical data. (C) 2013 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Faghihi, Azin; Gibson, Steve] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Tesch, Jonathan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Faghihi, A (reprint author), Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
EM gibson@ucla.edu
FU High Energy Laser Joint Technology Office; U.S. Office of Naval Research
[N00014 07-1-1063]; Air Force Office of Scientific Research
[FA9550-12-1-0375]
FX This work was supported by the High Energy Laser Joint Technology Office
and the U.S. Office of Naval Research under grant N00014 07-1-1063 and
the Air Force Office of Scientific Research under grant
FA9550-12-1-0375. The authors of this paper are indebted to the
University of Notre Dame aero-optical research group12-15 for
the aero-optical data used here and indispensable assistance with
interpreting the data.
NR 18
TC 4
Z9 4
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
J9 OPT ENG
JI Opt. Eng.
PD JUL
PY 2013
VL 52
IS 7
AR 071419
DI 10.1117/1.OE.52.7.071419
PG 10
WC Optics
SC Optics
GA 151FJ
UT WOS:000319445800019
ER
PT J
AU Tesch, J
Gibson, S
Verhaegen, M
AF Tesch, Jonathan
Gibson, Steve
Verhaegen, Michel
TI Receding-horizon adaptive control of aero-optical wavefronts
SO OPTICAL ENGINEERING
LA English
DT Article
DE adaptive control; adaptive optics; adaptive filtering; aero-optics
ID DRIVEN H-2-OPTIMAL CONTROL; PHASE SCREENS; OPTICS; RECONSTRUCTION
AB A new method for adaptive prediction and correction of wavefront errors in adaptive optics (AO) is introduced. The new method is based on receding-horizon control design and an adaptive lattice filter. Experimental results presented illustrate the capability of the new adaptive controller to predict and correct aero-optical wavefronts derived from recent flight-test data. The experimental results compare the performance of the new adaptive controller the performance of a minimum-variance adaptive controller previously used in AO. These results demonstrate the reduced sensitivity of the receding-horizon adaptive controller to high-frequency sensor noise. (C) 2013 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Tesch, Jonathan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gibson, Steve] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Verhaegen, Michel] Delft Univ Technol, Delft Ctr Syst & Control, NL-2628 CD Delft, Netherlands.
RP Tesch, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Jonathan.A.Tesch@jpl.nasa.gov; gibson@ucla.edu
FU High Energy Laser Joint Technology Office; U.S. Office of Naval Research
[00014 07-1-1063]
FX This work was supported by the High Energy Laser Joint Technology Office
and the U.S. Office of Naval Research under Grant No. 00014 07-1-1063.
The authors of this paper are indebted to the authors of Refs. 18, 27-29
for the aero-optical data and indispensable assistance with interpreting
the data.
NR 30
TC 2
Z9 2
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
J9 OPT ENG
JI Opt. Eng.
PD JUL
PY 2013
VL 52
IS 7
AR 071406
DI 10.1117/1.OE.52.7.071406
PG 13
WC Optics
SC Optics
GA 151FJ
UT WOS:000319445800006
ER
PT J
AU Gutman, G
Huang, CQ
Chander, G
Noojipady, P
Masek, JG
AF Gutman, Garik
Huang, Chengquan
Chander, Gyanesh
Noojipady, Praveen
Masek, Jeffrey G.
TI Assessment of the NASA-USGS Global Land Survey (GLS) datasets
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Global Land Surveys; Landsat; Quality assessment
ID THEMATIC MAPPER DATA; RADIOMETRIC CALIBRATION; UNITED-STATES; DATA SET;
COVER; RECORD; EARTH; TM; IMAGERY; FUTURE
AB The Global Land Survey (GLS) datasets are a collection of orthorectified, cloud-minimized Landsat-type satellite images, providing near complete coverage of the global land area decadally since the early 1970s. The global mosaics are centered on 1975, 1990, 2000, 2005, and 2010, and consist of data acquired from four sensors: Enhanced Thematic Mapper Plus, Thematic Mapper, Multispectral Scanner, and Advanced Land Imager. The GLS datasets have been widely used in land-cover and land-use change studies at local, regional, and global scales. This study evaluates the GLS datasets with respect to their spatial coverage, temporal consistency, geodetic accuracy, radiometric calibration consistency, image completeness, extent of cloud contamination, and residual gaps. In general, the three latest GLS datasets are of a better quality than the GLS-1990 and GLS-1975 datasets, with most of the imagery (85%) having cloud cover of less than 10%, the acquisition years clustered much more tightly around their target years, better co-registration relative to GLS-2000, and better radiometric absolute calibration. Probably, the most significant impediment to scientific use of the datasets is the variability of image phenology (i.e., acquisition day of year). This paper provides end-users with an assessment of the quality of the GLS datasets for specific applications, and where possible, suggestions for mitigating their deficiencies. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Gutman, Garik] NASA Headquarters, Washington, DC 20546 USA.
[Huang, Chengquan; Noojipady, Praveen] Univ Maryland, Dept Geog Sci, Global Land Cover Facil, College Pk, MD 20742 USA.
[Chander, Gyanesh] US Geol Survey, SGT Inc, Earth Resources Observat & Sci EROS Ctr, Sioux Falls, SD 57198 USA.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gutman, G (reprint author), NASA Headquarters, Washington, DC 20546 USA.
EM ggutman@nasa.gov; cqhuang@umd.edu; gchander@usgs.gov;
Jeffrey.G.Masek@nasa.gov
RI Masek, Jeffrey/D-7673-2012;
OI Huang, Chengquan/0000-0003-0055-9798
FU NASA [NNH06ZDA001N-MEASURES]; USGS [G10PC00044]
FX This study was supported by grants from NASA's Land-Cover/Land-Use
Change, Terrestrial Ecology, Carbon Cycle Science, and Applied Sciences
Programs, and by NASA's funding opportunity NNH06ZDA001N-MEASURES. The
SGT Inc, work was performed under USGS contract G10PC00044. DoHyung Kim,
Joe Sexton, and Saurabh Channan of the GLCF provided significant support
in evaluating the cloud cover of the GLS-2000 and phenological
suitability of the GLS images. Aparajithan Sampath and Rajagopalan
Rengarajan from SGT provided significant support to the geodetic
assessment of the GLS datasets. Special thanks go to Steven Covington
(Aerospace), Rachel Headley, John Dwyer, and Ray Byrnes (USGS) for
helping with the creation of the GLS datasets. We appreciate Rachel
Headley's help with reviewing this manuscript and providing us useful
feedback. We are also grateful to the four anonymous reviewers whose
constructive criticisms helped to improve the text substantially. Any
use of trade, product, or firm names is for descriptive purposes only
and does not imply endorsement by the US Government.
NR 44
TC 32
Z9 37
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 JUL
PY 2013
VL 134
BP 249
EP 265
DI 10.1016/j.rse.2013.02.026
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 148GS
UT WOS:000319233200019
ER
PT J
AU Feng, M
Sexton, JO
Huang, CQ
Masek, JG
Vermote, EF
Gao, F
Narasimhan, R
Channan, S
Wolfe, RE
Townshend, JR
AF Feng, Min
Sexton, Joseph O.
Huang, Chengquan
Masek, Jeffrey G.
Vermote, Eric F.
Gao, Feng
Narasimhan, Raghuram
Channan, Saurabh
Wolfe, Robert E.
Townshend, John R.
TI Global surface reflectance products from Landsat: Assessment using
coincident MODIS observations
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Landsat; Surface reflectance; Global; MODIS; Quality assessment
ID LEAF-AREA-INDEX; ATMOSPHERIC CORRECTION; BOREAL FOREST; ABSORBED PAR;
EOS-MODIS; ETM+ DATA; COVER; CLASSIFICATION; PERFORMANCE; METHODOLOGY
AB Global, long-term monitoring of changes in Earth's land surface requires quantitative comparisons of satellite images acquired under widely varying atmospheric conditions. Although physically based estimates of surface reflectance (SR) ultimately provide the most accurate representation of Earth's surface properties, there has never been a globally consistent SR dataset at the spatial resolution (<1 ha) or temporal extent (similar to 40 years) of the Landsat mission. To increase the consistency and robustness of Landsat-based land cover monitoring, we atmospherically corrected the Global Land Survey (GLS) Landsat dataset using the Landsat Ecosystem Disturbance Adaptive Processing System (LEDAPS) implementation of the Second Simulation of the Satellite Signal in the Solar Spectrum ( 6S) radiative transfer model. The GLS provides synoptic, orthorectified, cloud-free Landsat coverage of Earth's land area in four nominal epochs (1975, 1990, 2000, and 2005). This paper presents the resulting GLS surface reflectance dataset and a global assessment of the 2000- and 2005-epoch data against coincident Moderate Resolution Imaging Spectroradiometer (MODIS) daily SR and Normalized Bidirectional Distribution Function-Adjusted Reflectance (NBAR) measurements. Agreement with respect to MODIS SR and NBAR data is very high, with overall discrepancies (Root-Mean-Squared Deviation (RMSD)) between 1.3 and 2.8 percent reflectance for Landsat-7 Enhanced Thematic Mapper Plus (ELM +) and between 2.2 and 3.5 percent reflectance for Landsat-5 Thematic Mapper (TM). The resulting Landsat surface reflectance dataset and the associated quality metrics for each image are hosted on the Global Land Cover Facility web site for free download (http://www.landcover.org/data/gls_SR). This new repository will provide consistent, calibrated, multi-decadal image data for robust land cover change detection and monitoring across the Earth sciences. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Feng, Min; Sexton, Joseph O.; Huang, Chengquan; Narasimhan, Raghuram; Channan, Saurabh; Townshend, John R.] Univ Maryland, Dept Geog, Global Land Cover Facil, College Pk, MD 20742 USA.
[Masek, Jeffrey G.] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Vermote, Eric F.; Wolfe, Robert E.] NASA, Terr Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gao, Feng] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA.
RP Feng, M (reprint author), Univ Maryland, Dept Geog, Global Land Cover Facil, College Pk, MD 20742 USA.
EM feng.tank@gmail.com
RI Masek, Jeffrey/D-7673-2012; Wolfe, Robert/E-1485-2012;
OI Wolfe, Robert/0000-0002-0915-1855; Huang, Chengquan/0000-0003-0055-9798
FU NASA [NNH06ZDA001N-MEASURES, NNH07ZDA001N-LCLUC, NNH06ZDA001N-EOS]
FX Funding support for this study was provided by the following NASA
programs: Making Earth System Data Records for Use in Research
Environments (NNH06ZDA001N-MEASURES), Land Cover and Land Use Change
(NNH07ZDA001N-LCLUC), and Earth System Science Research Using Data and
Products from Terra, Aqua, and Acrimsat Satellites (NNH06ZDA001N-EOS).
The MODIS daily products used in this study were obtained from Greg
Ederer and Robert Wolfe (NASA Goddard Space Flight Center). The GLS
datasets were sent to GLCF by Rachel Headley (USGS). We also acknowledge
the three anonymous reviewers for their helpful comments on earlier
versions of the manuscript.
NR 50
TC 34
Z9 35
U1 5
U2 51
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD JUL
PY 2013
VL 134
BP 276
EP 293
DI 10.1016/j.rse.2013.02.031
PG 18
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 148GS
UT WOS:000319233200021
ER
PT J
AU Huang, WL
Sun, GQ
Dubayah, R
Cook, B
Montesano, P
Ni, WJ
Zhang, ZY
AF Huang, Wenli
Sun, Guoqing
Dubayah, Ralph
Cook, Bruce
Montesano, Paul
Ni, Wenjian
Zhang, Zhiyu
TI Mapping biomass change after forest disturbance: Applying LiDAR
footprint-derived models at key map scales
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Above-ground biomass; Scale; Disturbance; Waveform LiDAR; LVIS
ID WAVE-FORM LIDAR; ABOVEGROUND BIOMASS; AIRBORNE LIDAR; CARBON STOCKS;
BOREAL FOREST; LASER; VALIDATION; ESTIMATORS; VEGETATION; REGIONS
AB Accurate estimate of biomass and its changes at local to regional scales are important for a better understanding of ecosystem function, biodiversity and sustainability. In this study we explored the forest biomass prediction and dynamic monitoring from Light detection and ranging (LiDAR) waveform metrics at different key map scales. NASA's Laser Vegetation Imaging Sensor (LVIS) data were acquired in Penobscot County, Maine, USA, during August 2003 and 2009 airborne campaigns in the New England region. Field data were collected in 2003, and 2009 to 2011. Regression models developed at the scale of footprint were applied to all LVIS waveforms within the two study sites: Howland Forest (HF) and Penobscot Experiment Forest (PEF). The effect of forest disturbances on LVIS biomass prediction models was investigated. Two types of models, i. e. combined model without consideration of disturbances and disturbance-specific models were developed and compared. Field data from nested field plots of 0.25 ha, 0.5 ha and 1.0 ha were used to evaluate the averaged, footprint-level (similar to 0.03 ha, 20 m diameter) estimates in these plots. The results demonstrate that: 1) prediction model at the scale of individual LVIS footprints is reliable when the geolocations of the measured footprints were determined by DGPS with a best accuracy of 0.5-1.0 m. 2) The differences between biomass prediction models for disturbed and undisturbed forests were statistically significant (p < 0.001) at the scale of footprint, and the disturbance-specific models performed slightly better (R-2 = 0.89, RMSE = 27.9 Mg.ha(-1), and relative error of 22.6%) than the combined model (R-2 = 0.86, RMSE = 31.0 Mg.ha(-1), 25.1%). 3) The evaluation using field plot data showed that the predictions of biomass were improved markedly with the increase of plot sizes from 0.25 ha to 1.0 ha and that the effect of disturbance was not strong. At 1.0 ha plot-level, both disturbance-specific and combined models agreed well with field estimates (R-2 = 0.91, 23.1 Mg.ha(-1), 16.1%; and R-2 = 0.91, 22.4 Mg.ha(-1), 15.6%). 4) Sensitivity analysis on levels of variation and error to footprint density suggests that a certain density of LVIS footprints is required for biomass mapping. The errors were minimized when footprint coverage approached about 50% of the area of 1.0 ha plots (16 footprints). 5) By applying the footprint-level models developed from 2009 LVIS data to both 2009 and 2003 LVIS data, the change of biomass from 2003 to 2009 could be assessed. The average annual biomass reduction rate from forest disturbance at two sites is -7.0 Mg.ha(-1) and -6.2 Mg.ha(-1), the average annual biomass accumulation from regrowth is +4.4 Mg.ha(-1) and +5.2 Mg.ha(-1), respectively. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Huang, Wenli; Sun, Guoqing; Dubayah, Ralph; Montesano, Paul; Ni, Wenjian] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Cook, Bruce] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ni, Wenjian; Zhang, Zhiyu] Chinese Acad Sci, Inst Remote Sensing Applicat, Beijing 100101, Peoples R China.
RP Huang, WL (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
EM wlhuang@umd.edu
RI Cook, Bruce/M-4828-2013; Beckley, Matthew/D-4547-2013
OI Cook, Bruce/0000-0002-8528-000X;
FU NASA Terrestrial Ecology Program [NNX09AG66G]; University of Maryland
(UMD), College Park; NASA
FX This work was done with financial support from the NASA Terrestrial
Ecology Program (no. NNX09AG66G). LiDAR datasets were provided by the
LVIS team in the Laser Remote Sensing Branch at NASA GSFC with supports
from University of Maryland (UMD), College Park. Field data were
collected by teams from NASA GSFC, JPL, UMD, and University of Maine in
October 2003, August 2009 to 2011 funded by NASA. The authors would like
to thank Prof. John Lee for collection of forest management maps and
assistance in field measurements, and Prof. Chengquan Huang for
acquisition and processing of LTSS-VCT disturbance product over the
study area.
NR 50
TC 21
Z9 21
U1 5
U2 62
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 JUL
PY 2013
VL 134
BP 319
EP 332
DI 10.1016/j.rse.2013.03.017
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 148GS
UT WOS:000319233200024
ER
PT J
AU Rybicki, NB
Kirshtein, JD
Voytek, MA
AF Rybicki, Nancy B.
Kirshtein, Julie D.
Voytek, Mary A.
TI Molecular techniques to distinguish morphologically similar Hydrilla
verticillata, Egeria densa, Elodea nuttallii, and Elodea canadensis
SO JOURNAL OF AQUATIC PLANT MANAGEMENT
LA English
DT Article
DE Chesapeake Bay; exotic; misidentification; polymerase chain reaction;
submerged aquatic vegetation
AB The four submerged aquatic species, hydrilla (Hydrilla verticillata [monoecious and dioecious]), Brazilian waterweed (Egeria densa), Canadian waterweed (Elodea canadensis), and western waterweed (Elodea nuttallii), are difficult to positively identify because of their morphological similarity to each other, resulting in possible misidentification. This limits our ability to understand their past and present distribution, which is important in aquatic plant management. We investigated a molecular technique to identify these species, which are problematic because of their invasive nature on multiple continents. Approximately 100 samples of these species, ranging in age from 40-yr-old herbarium samples to recently collected plants, were collected from regions across the United States. The distribution and range of the samples collected in this research were compared to those reported in the literature. We confirmed information on the current wide distribution of both hydrilla biotypes in the United States and discovered that hydrilla had actually invaded the waterways near Washington, DC 6 yr earlier than originally reported. In addition, we found evidence of the confusion, dating back to the 1980s, between Canadian waterweed and western waterweed in the mid-Atlantic region of the United States. Canadian waterweed was previously reported as common and western waterweed as rare; however, our samples indicate the opposite is true. This information indicates there is a need for investigators to anticipate the spread of hydrilla populations to northern U.S. waterways, where it will compete with existing plant species, including Canadian and western waterweeds. Our ability to confirm distribution and pace of spread of invasive and noninvasive species will improve with increased application of molecular techniques.
C1 [Rybicki, Nancy B.; Kirshtein, Julie D.] US Geol Survey, Natl Ctr 430, Reston, VA 20192 USA.
[Voytek, Mary A.] Natl Aeronaut & Space Adm, Astrobiol, Washington, DC 20546 USA.
RP Rybicki, NB (reprint author), US Geol Survey, Natl Ctr 430, Reston, VA 20192 USA.
EM nrybicki@usgs.gov
NR 35
TC 3
Z9 3
U1 2
U2 6
PU AQUATIC PLANT MANAGEMENT SOC, INC
PI VICKSBURG
PA PO BOX 821265, VICKSBURG, MS 39182 USA
SN 0146-6623
J9 J AQUAT PLANT MANAGE
JI J. Aquat. Plant Manage.
PD JUL
PY 2013
VL 51
BP 94
EP 102
PG 9
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA V41TH
UT WOS:000209568000004
ER
PT J
AU Spitsberg, I
Brahmandam, S
Verti, MJ
Coulston, GW
AF Spitsberg, Irene
Brahmandam, Sudhir
Verti, Michael J.
Coulston, George W.
TI Technology Landscape Mapping At the Heart of Open Innovation
SO RESEARCH-TECHNOLOGY MANAGEMENT
LA English
DT Article
DE Technology scouting; Technology landscape map
AB Open innovation efforts traditionally focus on sourcing external solutions against known needs. This approach, while helping the organization to close gaps in internal capabilities, has only limited impact on ideation and strategy. A broader awareness of technology and market trends can itself become a powerful source of new and differentiating ideas. Because of this, a systematic process for building technology awareness and articulating and disseminating knowledge within the organization is critical for enabling a collaborative cross-functional ideation process. This can be accomplished through systematic, proactive scouting and technology landscape maps, which, for a given technology domain, identify technology drivers, critical technology attributes, related existing and emerging technologies with their commercial readiness levels, and the opportunity space enabled by these technologies. We are sharing a new framework, with associated processes and tools that we developed at Kennametal. This process addresses a broader set of objectives than targeted technology searches and is versatile enough to be applied to any technology domain.
C1 [Spitsberg, Irene; Verti, Michael J.] Kennametal Inc, Innovat Ventures Grp, Latrobe, PA 15650 USA.
[Spitsberg, Irene] GE Aviat, Cincinnati, OH USA.
[Spitsberg, Irene] Natl Govt Labs, Pittsburgh, PA USA.
[Spitsberg, Irene] NASA, Washington, DC USA.
[Verti, Michael J.] Hewlett Packard Corp, Palo Alto, CA USA.
[Verti, Michael J.] Lucent Technol, Bonn, Germany.
[Verti, Michael J.] Kennametal, Latrobe, PA USA.
[Coulston, George W.] Kennametal Inc, Innovat Ventures, Latrobe, PA USA.
[Coulston, George W.] Adv Mat Solut Grp, Latrobe, PA USA.
[Coulston, George W.] Breakthrough Technol, Evanston, IL USA.
[Coulston, George W.] DuPont Co Inc, R&D, Wilmington, DE USA.
RP Spitsberg, I (reprint author), Kennametal Inc, Innovat Ventures Grp, Latrobe, PA 15650 USA.
EM Irene.Spitsberg@kennametal.com; Sudhir.Brahmandam@kennametal.com;
Michael.Verti@kennametal.com; George.Coulston@kennametal.com
NR 16
TC 3
Z9 3
U1 3
U2 26
PU INDUSTRIAL RESEARCH INST, INC
PI ARLINGTON
PA 2200 CLARENDON BLVD, STE 1102, ARLINGTON, VA 22201 USA
SN 0895-6308
EI 1930-0166
J9 RES TECHNOL MANAGE
JI Res.-Technol. Manage.
PD JUL-AUG
PY 2013
VL 56
IS 4
BP 27
EP +
DI 10.5437/08956308X5604107
PG 9
WC Business; Engineering, Industrial; Management
SC Business & Economics; Engineering
GA AI8XS
UT WOS:000337210900008
ER
PT J
AU Masud, MM
Chen, Q
Khan, L
Aggarwal, CC
Gao, J
Han, JW
Srivastava, A
Oza, NC
AF Masud, Mohammad M.
Chen, Qing
Khan, Latifur
Aggarwal, Charu C.
Gao, Jing
Han, Jiawei
Srivastava, Ashok
Oza, Nikunj C.
TI Classification and Adaptive Novel Class Detection of Feature-Evolving
Data Streams
SO IEEE TRANSACTIONS ON KNOWLEDGE AND DATA ENGINEERING
LA English
DT Article
DE Data stream; concept-evolution; novel class; outlier
AB Data stream classification poses many challenges to the data mining community. In this paper, we address four such major challenges, namely, infinite length, concept-drift, concept-evolution, and feature-evolution. Since a data stream is theoretically infinite in length, it is impractical to store and use all the historical data for training. Concept-drift is a common phenomenon in data streams, which occurs as a result of changes in the underlying concepts. Concept-evolution occurs as a result of new classes evolving in the stream. Feature-evolution is a frequently occurring process in many streams, such as text streams, in which new features (i.e., words or phrases) appear as the stream progresses. Most existing data stream classification techniques address only the first two challenges, and ignore the latter two. In this paper, we propose an ensemble classification framework, where each classifier is equipped with a novel class detector, to address concept-drift and concept-evolution. To address feature-evolution, we propose a feature set homogenization technique. We also enhance the novel class detection module by making it more adaptive to the evolving stream, and enabling it to detect more than one novel class at a time. Comparison with state-of-the-art data stream classification techniques establishes the effectiveness of the proposed approach.
C1 [Masud, Mohammad M.] United Arab Emirates Univ, Fac Informat Technol, Al Ain, U Arab Emirates.
[Chen, Qing] Richfit IT LLC, China Natl Petr Co, Beijing 100007, Peoples R China.
[Khan, Latifur] Univ Texas Dallas, Erik Jonsson Sch Engn & Comp Sci, Dept Comp Sci, UTD Data Min Lab, Richardson, TX 75083 USA.
[Aggarwal, Charu C.] IBM Corp, Thomas J Watson Res Ctr, Yorktown Hts, NY 10598 USA.
[Gao, Jing] SUNY Buffalo, Dept Comp Sci & Engn, Buffalo, NY 14260 USA.
[Han, Jiawei] Univ Illinois, Siebel Ctr Comp Sci, Dept Comp Sci, Urbana, IL 61801 USA.
[Srivastava, Ashok] NASA, Ames Res Ctr, Intelligent Data Understanding Grp Lead, Moffett Field, CA 94035 USA.
[Oza, Nikunj C.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Masud, MM (reprint author), United Arab Emirates Univ, Fac Informat Technol, POB 17551, Al Ain, U Arab Emirates.
EM m.masud@uaeu.ac.ae; peterchq@hotmail.com; lkhan@utdallas.edu;
charu@us.ibm.com; jing@buffalo.edu; hanj@cs.uiuc.edu;
Ashok.N.Srivastava@nasa.gov; Nikunj.C.Oza@nasa.gov
OI Masud, Mohammad/0000-0002-5274-5982
FU AFOSR [FA9550-08-1-0260]; NASA [2008-00867-01]
FX This material is based upon work supported by the AFOSR under Award No.
FA9550-08-1-0260 and NASA under Award No. 2008-00867-01.
NR 24
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Z9 14
U1 2
U2 20
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1041-4347
J9 IEEE T KNOWL DATA EN
JI IEEE Trans. Knowl. Data Eng.
PD JUL
PY 2013
VL 25
IS 7
BP 1484
EP 1497
DI 10.1109/TKDE.2012.109
PG 14
WC Computer Science, Artificial Intelligence; Computer Science, Information
Systems; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA 151LK
UT WOS:000319461800004
ER
PT J
AU Mishchenko, MI
Kahnert, M
Mackowski, DW
Wriedt, T
AF Mishchenko, Michael I.
Kahnert, Michael
Mackowski, Daniel W.
Wriedt, Thomas
TI Peter Waterman and his scientific legacy
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
ID MATRIX REFERENCE DATABASE; UPDATE
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Kahnert, Michael] Swedish Meteorol & Hydrol Inst, SE-60176 Norrkoping, Sweden.
[Mackowski, Daniel W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
[Wriedt, Thomas] Inst Werkstofftech, D-28359 Bremen, Germany.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM michael.i.mishchenko@nasa.gov; michael.kahnert@smhi.se;
mackodw@auburn.edu; thw@iwt.uni-bremen.de
RI Mackowski, Daniel/K-1917-2013; Kahnert, Michael/A-3275-2009; Mishchenko,
Michael/D-4426-2012
OI Kahnert, Michael/0000-0001-5695-1356;
NR 8
TC 2
Z9 2
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUL
PY 2013
VL 123
SI SI
BP 1
EP 1
DI 10.1016/j.jqsrt.2013.01.025
PG 1
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 146MN
UT WOS:000319095300001
ER
PT J
AU Mishchenko, MI
Martin, PA
AF Mishchenko, M. I.
Martin, P. A.
TI Peter Waterman and T-matrix methods
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Acoustic scattering; Electromagnetic scattering; Elastodynamic
scattering; Discrete random media; Extended boundary condition method;
T-matrix; Superposition T-matrix method; Radiative transfer
ID MULTIPLE-SCATTERING; EM WAVES; SPHERES
AB This paper summarizes the scientific legacy of Peter C. Waterman (1928-2012) who introduced concepts and theoretical techniques that have had a major impact on the. fields of scattering by particles and particle groups, optical particle characterization, radiative transfer, and remote sensing. A biographical sketch is also included. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Mishchenko, M. I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Martin, P. A.] Colorado Sch Mines, Dept Appl Math & Stat, Golden, CO 80401 USA.
RP Martin, PA (reprint author), Colorado Sch Mines, Dept Appl Math & Stat, Golden, CO 80401 USA.
EM michael.i.mishchenko@nasa.gov; pamartin@mines.edu
RI Martin, Paul/D-3398-2009; Mishchenko, Michael/D-4426-2012
NR 16
TC 3
Z9 4
U1 0
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUL
PY 2013
VL 123
SI SI
BP 2
EP 7
DI 10.1016/j.jqsrt.2012.10.025
PG 6
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 146MN
UT WOS:000319095300002
ER
PT J
AU Bi, L
Yang, P
Kattawar, GW
Mishchenko, MI
AF Bi, Lei
Yang, Ping
Kattawar, George W.
Mishchenko, Michael I.
TI A numerical combination of extended boundary condition method and
invariant imbedding method applied to light scattering by large
spheroids and cylinders
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Light scattering; T-matrix; Extended boundary condition method;
Invariant imbedding method
ID T-MATRIX METHOD; ELECTROMAGNETIC SCATTERING; PARTICLES
AB The extended boundary condition method (EBCM) and invariant imbedding method (IIM) are two fundamentally different T-matrix methods for the solution of light scattering by nonspherical particles. The standard EBCM is very efficient but encounters a loss of precision when the particle size is large, the maximum size being sensitive to the particle aspect ratio. The IIM can be applied to particles in a relatively large size parameter range but requires extensive computational time due to the number of spherical layers in the particle volume discretization. A numerical combination of the EBCM and the IIM (hereafter, the EBCM+IIM) is proposed to overcome the aforementioned disadvantages of each method. Even though the EBCM can fail to obtain the T-matrix of a considered particle, it is valuable for decreasing the computational domain (i.e., the number of spherical layers) of the IIM by providing the initial T-matrix associated with an iterative procedure in the IIM. The EBCM+IIM is demonstrated to be more efficient than the IIM in obtaining the optical properties of large size parameter particles beyond the convergence limit of the EBCM. The numerical performance of the EBCM+IIM is illustrated through representative calculations in spheroidal and cylindrical particle cases. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Bi, Lei; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Kattawar, George W.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Bi, L (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM bilei@neo.tamu.edu
RI Yang, Ping/B-4590-2011; Mishchenko, Michael/D-4426-2012; Bi,
Lei/B-9242-2011
FU National Science Foundation [ATMO-0803779, OCE-1130906]; NASA
[NNX11AK37G]; David Bullock Harris Chair in Geosciences at the College
of Geosciences, Texas AM University
FX This research is supported by the National Science Foundation; PY
(ATMO-0803779) and GWK (OCE-1130906), NASA (NNX11AK37G and the Remote
Sensing Theory Program), and the endowment funds associated with the
David Bullock Harris Chair in Geosciences at the College of Geosciences,
Texas A&M University. The numerical computations were performed using
the EOS supercomputer at Texas A&M University. We thank two anonymous
referees for helpful comments.
NR 17
TC 17
Z9 18
U1 0
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUL
PY 2013
VL 123
SI SI
BP 17
EP 22
DI 10.1016/j.jqsrt.2012.11.033
PG 6
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 146MN
UT WOS:000319095300004
ER
PT J
AU Mackowski, DW
Mishchenko, MI
AF Mackowski, D. W.
Mishchenko, M. I.
TI Direct simulation of extinction in a slab of spherical particles
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Electromagnetic scattering; Random media; Radiative transfer
ID MULTIPLE-SCATTERING; MEDIA; WAVE; ATTENUATION
AB The exact multiple sphere superposition method is used to calculate the coherent and incoherent contributions to the ensemble-averaged electric field amplitude and Poynting vector in systems of randomly positioned nonabsorbing spherical particles. The target systems consist of cylindrical volumes, with radius several times larger than length, containing spheres with positional configurations generated by a Monte Carlo sampling method. Spatially dependent values for coherent electric field amplitude, coherent energy flux, and diffuse energy flux, are calculated by averaging of exact local field and flux values over multiple configurations and over spatially independent directions for fixed target geometry, sphere properties, and sphere volume fraction. Our results reveal exponential attenuation of the coherent field and the coherent energy flux inside the particulate layer and thereby further corroborate the general methodology of the microphysical radiative transfer theory. An effective medium model based on plane wave transmission and reflection by a plane layer is used to model the dependence of the coherent electric field on particle packing density. The effective attenuation coefficient of the random medium, computed from the direct simulations, is found to agree closely with effective medium theories and with measurements. In addition, the simulation results reveal the presence of a counter-propagating component to the coherent field, which arises due to the internal reflection of the main coherent field component by the target boundary. The characteristics of the diffuse flux are compared to, and found to be consistent with, a model based on the diffusion approximation of the radiative transfer theory. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Mackowski, D. W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
[Mishchenko, M. I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Mackowski, DW (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
EM mackodw@auburn.edu
RI Mackowski, Daniel/K-1917-2013; Mishchenko, Michael/D-4426-2012
NR 20
TC 10
Z9 10
U1 1
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 JUL
PY 2013
VL 123
SI SI
BP 103
EP 112
DI 10.1016/j.jqsrt.2013.02.008
PG 10
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 146MN
UT WOS:000319095300012
ER
PT J
AU Mackowski, DW
Kahnert, FM
Mishchenko, MI
AF Mackowski, D. W.
Kahnert, F. M.
Mishchenko, M. I.
TI A T matrix method based upon scalar basis functions
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Electromagnetic scattering; T matrix method; Volume integral equation
formulation; Vector spherical wave functions; Scalar Helmholtz equation
ID DISCRETE-DIPOLE APPROXIMATION; ELECTROMAGNETIC SCATTERING
AB A surface integral formulation is developed for the T matrix of a homogenous and isotropic particle of arbitrary shape, which employs scalar basis functions represented by the translation matrix elements of the vector spherical wave functions. The formulation begins with the volume integral equation for scattering by the particle, which is transformed so that the vector and dyadic components in the equation are replaced with associated dipole and multipole level scalar harmonic wave functions. The approach leads to a volume integral formulation for the T matrix, which can be extended, by the use of Green's identities, to the surface integral formulation. The result is shown to be equivalent to the traditional surface integral formulas based on the VSWF basis. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Mackowski, D. W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
[Kahnert, F. M.] Swedish Meteorol & Hydrol Inst, Res Dept, SE-60176 Norrkoping, Sweden.
[Kahnert, F. M.] Chalmers, Dept Earth & Space Sci, SE-41296 Gothenburg, Sweden.
[Mishchenko, M. I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Mackowski, DW (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
EM mackodw@auburn.edu
RI Mackowski, Daniel/K-1917-2013; Kahnert, Michael/A-3275-2009; Mishchenko,
Michael/D-4426-2012
OI Kahnert, Michael/0000-0001-5695-1356;
FU US Department of Energy [DE-NA 0001709]; NASA Radiation Sciences
Program; Hal Maring and the NASA Remote Sensing Theory Program; Swedish
Research Council [621-2011-3346]
FX D.W.M. acknowledges funding from the US Department of Energy, Project
DE-NA 0001709, David LaGraffe, Program Manager. M.I.M. acknowledges
funding from the NASA Radiation Sciences Program managed by Hal Maring
and the NASA Remote Sensing Theory Program managed by Lucia Tsaoussi.
F.M.K. acknowledges funding from the Swedish Research Council (project
621-2011-3346).
NR 16
TC 1
Z9 1
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUL
PY 2013
VL 123
SI SI
BP 113
EP 121
DI 10.1016/j.jqsrt.2013.02.029
PG 9
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 146MN
UT WOS:000319095300013
ER
PT J
AU Mishchenko, MI
AF Mishchenko, Michael I.
TI Measurement of electromagnetic energy flow through a sparse particulate
medium: A perspective
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Electromagnetic scattering; Directional radiometry; Radiative transfer;
Optical particle characterization; Remote sensing; Macroscopic Maxwell
equations
ID ANGULAR-DISTRIBUTION; RADIATIVE-TRANSFER; SPIN POLARIZATION; OPTICAL
THEOREM; PHOTOELECTRONS; PHOTOEMISSION; EXTINCTION; PARTICLES; PARADIGM;
FIELD
AB First-principle analysis of the functional design of a well-collimated radiometer (WCR) reveals that in general, this instrument does not record the instantaneous directional flow of electromagnetic energy. Only in special cases can a sequence of measurements with a WCR yield the magnitude and direction of the local time-averaged Poynting vector. Our analysis demonstrates that it is imperative to clearly formulate the physical nature of the actual measurement afforded by a directional radiometer rather than presume desirable measurement capabilities. Only then can the directional radiometer be considered a legitimate part of physically based remote sensing and radiation-budget applications. We also emphasize the need for a better understanding of the nature of measurements with panoramic radiometers. Published by Elsevier Ltd.
C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM michael.i.mishchenko@nasa.gov
RI Mishchenko, Michael/D-4426-2012
FU NASA Remote Sensing Theory Program; NASA Radiation Sciences Program
FX I appreciate numerous illuminating discussions with Matthew Berg, Brian
Cairns, Michael Kahnert, and Daniel Mackowski as well as helpful
comments by two anonymous referees. This research was funded by the NASA
Remote Sensing Theory Program managed by Lucia Tsaoussi and the NASA
Radiation Sciences Program managed by Hal Maring.
NR 35
TC 3
Z9 3
U1 1
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUL
PY 2013
VL 123
SI SI
BP 122
EP 134
DI 10.1016/j.jqsrt.2013.01.006
PG 13
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 146MN
UT WOS:000319095300014
ER
PT J
AU Mishchenko, MI
Liu, L
Mackowski, DW
AF Mishchenko, Michael I.
Liu, Li
Mackowski, Daniel W.
TI T-matrix modeling of linear depolarization by morphologically complex
soot and soot-containing aerosols
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Soot aggregates; Optical cross sections; Linear depolarization; Remote
sensing; Atmospheric radiation
ID LIGHT ABSORBING CARBON; OPTICAL-PROPERTIES; RADIATIVE PROPERTIES;
SCATTERING PROPERTIES; BLACK CARBON; ELECTROMAGNETIC SCATTERING;
SOUTHERN AFRICA; TAR BALLS; ABSORPTION; PARTICLES
AB We use state-of-the-art public-domain Fortran codes based on the T-matrix method to calculate orientation and ensemble averaged scattering matrix elements for a variety of morphologically complex black carbon (BC) and BC-containing aerosol particles, with a special emphasis on the linear depolarization ratio (LDR). We explain theoretically the quasi-Rayleigh LDR peak at side-scattering angles typical of low-density soot fractals and conclude that the measurement of this feature enables one to evaluate the compactness state of BC clusters and trace the evolution of low-density fluffy fractals into densely packed aggregates. We show that small backscattering LDRs measured with ground-based, airborne, and spaceborne lidars for fresh smoke generally agree with the values predicted theoretically for fluffy BC fractals and densely packed near-spheroidal BC aggregates. To reproduce higher lidar LDRs observed for aged smoke, one needs alternative particle models such as shape mixtures of BC spheroids or cylinders. Published by Elsevier Ltd.
C1 [Mishchenko, Michael I.; Liu, Li] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Liu, Li] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Mackowski, Daniel W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM michael.i.mishchenko@nasa.gov
RI Mackowski, Daniel/K-1917-2013; Mishchenko, Michael/D-4426-2012
FU NASA Radiation Sciences Program; NASA Remote Sensing Theory Program
FX We thank W. Patrick Arnott, Rajan Chakrabarty, Hans Moosmuller, and
Andrew Lacis for useful discussions and two anonymous referees for
constructive and helpful comments. This research was funded by the NASA
Radiation Sciences Program managed by Hal Mating and by the NASA Remote
Sensing Theory Program managed by Lucia Tsaoussi.
NR 124
TC 24
Z9 25
U1 6
U2 40
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 JUL
PY 2013
VL 123
SI SI
BP 135
EP 144
DI 10.1016/j.jqsrt.2012.11.012
PG 10
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 146MN
UT WOS:000319095300015
ER
PT J
AU Mishchenko, MI
Videen, G
Khlebtsov, NG
Wriedt, T
AF Mishchenko, Michael I.
Videen, Gorden
Khlebtsov, Nikolai G.
Wriedt, Thomas
TI Comprehensive T-matrix reference database: A 2012-2013 update
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Electromagnetic scattering; T-matrix method; Complex scattering objects
ID MULTIPLE-SCATTERING THEORY; DISCRETE DIPOLE APPROXIMATION;
LIGHT-SCATTERING; ELECTROMAGNETIC SCATTERING; ATTENUATION CORRECTION;
COLLOIDAL CLUSTERS; OPTICAL-PROPERTIES; DIELECTRIC BODIES; SIZE
DISTRIBUTION; IRREGULAR SHAPE
AB The T-matrix method is one of the most versatile, efficient, and accurate theoretical techniques widely used for numerically exact computer calculations of electromagnetic scattering by single and composite particles, discrete random media, and particles imbedded in complex environments. This paper presents the fifth update to the comprehensive database of peer-reviewed T-matrix publications initiated by us in 2004 and includes relevant publications that have appeared since 2012. It also lists several earlier publications not incorporated in the original database, including Peter Waterman's reports from the 1960s illustrating the history of the T-matrix approach and demonstrating that John Fikioris and Peter Waterman were the true pioneers of the multi-sphere method otherwise known as the generalized Lorenz-Mie theory. Published by Elsevier Ltd.
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Videen, Gorden] USA, Res Lab, AMSRL IS EE, Adelphi, MD 20783 USA.
[Khlebtsov, Nikolai G.] Russian Acad Sci, Inst Biochem & Physiol Plants & Microorganisms, Saratov 410015, Russia.
[Wriedt, Thomas] Inst Werkstofftech, D-28359 Bremen, Germany.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM michael.i.mishchenko@nasa.gov
RI Mishchenko, Michael/D-4426-2012; Khlebtsov, Nikolai/D-6199-2017; Pylaev,
Timofey/A-8401-2016;
OI Pylaev, Timofey/0000-0002-2701-3333; Khlebtsov,
Nikolai/0000-0002-2055-7784
FU NASA Radiation Sciences Program; NASA Remote Sensing Theory Project
FX We thank Josefina Mora, Zoe Wai, and Nadia Zakharova for technical
assistance. This project was sponsored by the NASA Radiation Sciences
Program managed by Hal Maring and the NASA Remote Sensing Theory Project
managed by Lucia Tsaoussi.
NR 131
TC 20
Z9 21
U1 3
U2 23
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 JUL
PY 2013
VL 123
SI SI
BP 145
EP 152
DI 10.1016/j.jqsrt.2013.01.024
PG 8
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 146MN
UT WOS:000319095300016
ER
PT J
AU Nemeth, N
Walker, A
Baker, E
Murthy, P
Bratton, R
AF Nemeth, Noel
Walker, Andrew
Baker, Eric
Murthy, Pappu
Bratton, Robert
TI Large-scale Weibull analysis of H-451 nuclear-grade graphite rupture
strength
SO CARBON
LA English
DT Article
ID POLYGRANULAR GRAPHITES; FRACTURE STATISTICS; CERAMICS
AB A Weibull analysis was performed of the strength distribution and size effects for 2000 specimens of H-451 nuclear-grade graphite. The data, generated elsewhere, measured the tensile and four-point-flexure room-temperature rupture strength of specimens cut from a single extruded graphite log. Strength variation versus specimen location, size, and orientation relative to the parent body were compared. In our study, data were progressively and extensively pooled into larger data sets to discriminate overall trends from local variations and investigate the strength distribution. Issues regarding size effect, Weibull parameter consistency, and nonlinear stress-strain response were investigated using the Ceramics Analysis and Reliability Evaluation of Structures Life Prediction Program (CARES/Life) and WeibPar codes. Overall, the Weibull distribution described the behavior of the pooled data very well. The Weibull modulus was shown to be clearly consistent between different tensile specimen sizes and orientations. However, the issue regarding the smaller-than-expected size effect remained. This exercise illustrated that a conservative approach using a two-parameter Weibull distribution is best for designing graphite components with low probability of failure for the in-core structures in the proposed Generation IV high-temperature gas-cooled nuclear reactors. This exercise also demonstrated the continuing need to better understand the mechanisms driving stochastic strength response. Published by Elsevier Ltd.
C1 [Nemeth, Noel; Murthy, Pappu] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Walker, Andrew] Wright State Univ, Dayton, OH 45435 USA.
[Baker, Eric] Connecticut Reserve Technol, Gates Mills, OH 44040 USA.
[Bratton, Robert] US DOE, Idaho Natl Lab, Idaho Falls, ID 83415 USA.
RP Nemeth, N (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM noel.n.nemeth@nasa.gov
NR 33
TC 7
Z9 7
U1 1
U2 17
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0008-6223
J9 CARBON
JI Carbon
PD JUL
PY 2013
VL 58
BP 208
EP 225
DI 10.1016/j.carbon.2013.02.054
PG 18
WC Chemistry, Physical; Materials Science, Multidisciplinary
SC Chemistry; Materials Science
GA 142ZB
UT WOS:000318835000021
ER
PT J
AU Yurchak, BS
AF Yurchak, Boris S.
TI Radar specular return waveform from a planar surface
SO REMOTE SENSING LETTERS
LA English
DT Article
ID IMPULSE-RESPONSE
AB A model of the specular component of a radar return waveform from a planar surface is presented for narrowband rectangular probe pulse and Gaussian antenna pattern for beam- and pulse-limited modes. Comparison of the derived model with a conventional incoherent model has been carried out.
C1 Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Yurchak, BS (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
EM yurboris@umbc.edu
FU NASA's Cryospheric Science Program
FX This work was supported by NASA's Cryospheric Science Program. The
author is grateful to two anonymous reviewers for their comments, which
improved the manuscript.
NR 11
TC 0
Z9 0
U1 0
U2 8
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 2150-704X
J9 REMOTE SENS LETT
JI Remote Sens. Lett.
PD JUL 1
PY 2013
VL 4
IS 7
BP 715
EP 724
DI 10.1080/2150704X.2013.790572
PG 10
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA 139OP
UT WOS:000318592600011
ER
PT J
AU Habbal, SR
Morgan, H
Druckmuller, M
Ding, A
Cooper, JF
Daw, A
Sittler, EC
AF Habbal, S. Rifai
Morgan, H.
Druckmueller, M.
Ding, A.
Cooper, J. F.
Daw, A.
Sittler, E. C., Jr.
TI Probing the Fundamental Physics of the Solar Corona with Lunar Solar
Occultation Observations
SO SOLAR PHYSICS
LA English
DT Article
DE Corona; Eclipse; Solar wind
ID WHITE-LIGHT IMAGES; MAGNETIC-FIELD; ELECTRON-TEMPERATURE; ECLIPSE
OBSERVATIONS; WIND; SPECTROMETER; POLARIZATION; LINE; ENHANCEMENTS;
IONIZATION
AB Imaging and spectroscopy of the solar corona, coupled with polarimetry, are the only tools available at present to capture signatures of physical processes responsible for coronal heating and solar wind acceleration within the first few solar radii above the solar limb. With the recent advent of improved detector technology and image processing techniques, broad-band white light and narrow-band multi-wavelength observations of coronal forbidden lines, made during total solar eclipses, have started to yield new views about the thermodynamic and magnetic properties of coronal structures. This paper outlines these unique capabilities, which until present, have been feasible primarily with observations during natural total solar eclipses. This work also draws attention to the exciting possibility of greatly increasing the frequency and duration of solar eclipse observations with Moon orbiting observatories utilizing lunar limb occultation of the solar disk for coronal measurements.
C1 [Habbal, S. Rifai; Morgan, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Druckmueller, M.] Brno Univ Technol, Brno 61669, Czech Republic.
[Ding, A.] Tech Univ Berlin, Inst Opt & Atom Phys, Berlin, Germany.
[Ding, A.] Inst Tech Phys, Berlin, Germany.
[Cooper, J. F.; Daw, A.; Sittler, E. C., Jr.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Habbal, SR (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM shadia@ifa.hawaii.edu; hmorgan@ifa.hawaii.edu; druckmuller@fme.vutbr.cz;
adalbert.ding@gmx.de; john.f.cooper@nasa.gov; adrian.daw@nasa.gov;
ed.sittler@nasa.gov
RI Cooper, John/D-4709-2012;
OI Morgan, Huw/0000-0002-6547-5838
FU NASA [NNX08AQ29G]; NSF [AGS 08-02520]
FX S.R. Habbal and H. Morgan were supported by funding from NASA Grants
NNX08AQ29G and NSF grant AGS 08-02520 to the University of Hawaii.
NR 49
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U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD JUL
PY 2013
VL 285
IS 1-2
BP 9
EP 24
DI 10.1007/s11207-012-0115-5
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 138OS
UT WOS:000318518600002
ER
PT J
AU Muller, D
Marsden, RG
St Cyr, OC
Gilbert, HR
AF Muller, D.
Marsden, R. G.
St Cyr, O. C.
Gilbert, H. R.
TI Solar Orbiter Exploring the Sun-Heliosphere Connection
SO SOLAR PHYSICS
LA English
DT Article
DE Sun; Heliosphere; Corona; Dynamics; Magnetic fields
ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLE EVENTS; OPEN MAGNETIC-FLUX;
TEMPERATURE ANISOTROPY; DIFFERENTIAL ROTATION; WIND ACCELERATION;
TRANSITION REGION; DRIVEN SHOCKS; MISSION; FIELDS
AB The heliosphere represents a uniquely accessible domain of space, where fundamental physical processes common to solar, astrophysical and laboratory plasmas can be studied under conditions impossible to reproduce on Earth and unfeasible to observe from astronomical distances. Solar Orbiter, the first mission of ESA's Cosmic Vision 2015 -aEuro parts per thousand 2025 programme, will address the central question of heliophysics: How does the Sun create and control the heliosphere? In this paper, we present the scientific goals of the mission and provide an overview of the mission implementation.
C1 [Muller, D.; Marsden, R. G.] European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands.
[St Cyr, O. C.; Gilbert, H. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Muller, D (reprint author), European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands.
EM Daniel.Mueller@esa.int; Richard.Marsden@esa.int; Chris.StCyr@nasa.gov;
Holly.R.Gilbert@nasa.gov
NR 127
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD JUL
PY 2013
VL 285
IS 1-2
BP 25
EP 70
DI 10.1007/s11207-012-0085-7
PG 46
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 138OS
UT WOS:000318518600003
ER
PT J
AU Webb, DF
Mostl, C
Jackson, BV
Bisi, MM
Howard, TA
Mulligan, T
Jensen, EA
Jian, LK
Davies, JA
de Koning, CA
Liu, Y
Temmer, M
Clover, JM
Farrugia, CJ
Harrison, RA
Nitta, N
Odstrcil, D
Tappin, SJ
Yu, HS
AF Webb, D. F.
Moestl, C.
Jackson, B. V.
Bisi, M. M.
Howard, T. A.
Mulligan, T.
Jensen, E. A.
Jian, L. K.
Davies, J. A.
de Koning, C. A.
Liu, Y.
Temmer, M.
Clover, J. M.
Farrugia, C. J.
Harrison, R. A.
Nitta, N.
Odstrcil, D.
Tappin, S. J.
Yu, H-S
TI Heliospheric Imaging of 3D Density Structures During the Multiple
Coronal Mass Ejections of Late July to Early August 2010
SO SOLAR PHYSICS
LA English
DT Article
ID IN-SITU OBSERVATIONS; CME-CME INTERACTION; SOLAR-WIND; WHITE-LIGHT;
3-DIMENSIONAL RECONSTRUCTION; IMAGER SMEI; 1 AU; SPACECRAFT;
PROPAGATION; INSTRUMENT
AB It is usually difficult to gain a consistent global understanding of a coronal mass ejection (CME) eruption and its propagation when only near-Sun imagery and the local measurements derived from single-spacecraft observations are available. Three-dimensional (3D) density reconstructions based on heliospheric imaging allow us to "fill in" the temporal and spatial gaps between the near-Sun and in situ data to provide a truly global picture of the propagation and interactions of the CME as it moves through the inner heliosphere. In recent years the heliospheric propagation of dense structures has been observed and measured by the heliospheric imagers of the Solar Mass Ejection Imager (SMEI) and on the twin Solar TErrestrial RElations Observatory (STEREO) spacecraft. We describe the use of several 3D reconstruction techniques based on these heliospheric imaging data sets to distinguish and track the propagation of multiple CMEs in the inner heliosphere during the very active period of solar activity in late July -aEuro parts per thousand early August 2010. We employ 3D reconstruction techniques used at the University of California, San Diego (UCSD) based on a kinematic solar wind model, and also the empirical Tappin-Howard model. We compare our results with those from other studies of this active period, in particular the heliospheric simulations made with the ENLIL model by Odstrcil et al. (J. Geophys. Res., 2013) and the in situ results from multiple spacecraft provided by Mostl et al. (Astrophys. J. 758, 10 -aEuro parts per thousand 28, 2012). We find that the SMEI results in particular provide an overall context for the multiple-density flows associated with these CMEs. For the first time we are able to intercompare the 3D reconstructed densities with the timing and magnitude of in situ density structures at five spacecraft spread over 150A degrees in ecliptic longitude and from 0.4 to 1 AU in radial distance. We also model the magnetic flux-rope structures at three spacecraft using both force-free and non-force-free modelling, and compare their timing and spatial structure with the reconstructed density flows.
C1 [Webb, D. F.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02167 USA.
[Moestl, C.; Temmer, M.] Graz Univ, Inst Phys, A-8010 Graz, Austria.
[Moestl, C.; Liu, Y.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Jackson, B. V.; Clover, J. M.; Yu, H-S] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Bisi, M. M.] Aberystwyth Univ, Inst Math & Phys, Aberystwyth, Ceredigion, Wales.
[Howard, T. A.] SW Res Inst, Boulder, CO USA.
[Mulligan, T.] Aerosp Corp, Dept Space Sci, SSAL, Los Angeles, CA 90009 USA.
[Jensen, E. A.] ACS Consulting, Houston, TX USA.
[Jian, L. K.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Davies, J. A.; Harrison, R. A.] RAL Space, Didcot, Oxon, England.
[de Koning, C. A.] NOAA, Space Weather Predict Ctr, Boulder, CO USA.
[Farrugia, C. J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Farrugia, C. J.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Nitta, N.] Lockheed Martin Adv Technol Ctr, Solar & Astrophys Lab, Palo Alto, CA USA.
[Odstrcil, D.] George Mason Univ, Dept Computat & Data Sci, Fairfax, VA 22030 USA.
[Odstrcil, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tappin, S. J.] Natl Solar Observ, Sunspot, NM 88349 USA.
RP Webb, DF (reprint author), Boston Coll, Inst Sci Res, Chestnut Hill, MA 02167 USA.
EM david.WEBB@hanscom.af.mil
RI Jian, Lan/B-4053-2010;
OI Jian, Lan/0000-0002-6849-5527; Liu, Ying/0000-0002-3483-5909; Moestl,
Christian/0000-0001-6868-4152; Temmer, Manuela/0000-0003-4867-7558
FU Air Force [AF19628-00-K-0073, FA8718-04-C-0006]; Navy contracts
[N00173-07-1-G016, N00173-10-1-G001]; European Union [263252]; Marie
Curie International Outgoing Fellowship within the 7th European
Community Framework Programme; Austrian Science Fund (FWF) [FWF
V195-N16]; UCSD NSF [M-0852246, AGS-1053766, ATM-0925023]; NASA
[NNX11AB50G, NX10AQ29G]; AFOSR [11NE043]; UK STFC Standard Grant;
NSF/SHINE Competition [0849916]; NASA Heliophysics program [NNX10AC05G];
NSF [AGS-1140211]
FX We acknowledge the organisers of and the beneficial discussions at the
three August 2010 events workshops, held in January 2011 in Abingdon,
England, March 2011 in Graz, Austria, and June 2011 in Aberystwyth,
Wales, which were vital in producing this paper. The Solar Mass Ejection
Imager (SMEI) instrument is a collaborative project of the U. S. Air
Force Research Laboratory, NASA, the University of California at San
Diego, the University of Birmingham, UK, Boston College, and Boston
University. The STEREO SECCHI Heliospheric Imager (HI) instrument was
developed by a collaboration that included the Rutherford Appleton
Laboratory and the University of Birmingham, both in the United Kingdom,
the Centre Spatial de Liege (CSL), Belgium, and the US Naval Research
Laboratory (NRL), Washington DC, USA. The SECCHI project is an
international consortium of the Naval Research Laboratory, Lockheed
Martin Solar and Astrophysics Lab, NASA Goddard Space Flight Center,
Rutherford Appleton Laboratory, University of Birmingham,
Max-Planck-Institut fur Sonnensystemforschung, Centre Spatial de Liege,
Institut d'Optique Theorique et Appliquee, and Institut d'Astrophysique
Spatiale. We also benefited from data from the SOHO mission, which is an
international collaboration between NASA and ESA, and also from the
SOHO/LASCO CME catalog, generated and maintained by the Center for Solar
Physics and Space Weather, The Catholic University of America in
cooperation with NRL and NASA. The work of DFW was supported at Boston
College by Air Force contracts AF19628-00-K-0073 and FA8718-04-C-0006
and Navy contracts N00173-07-1-G016 and N00173-10-1-G001. The work of CM
was supported by the European Union Seventh Framework Programme
(FP7/2007-2013) under grant agreement no. 263252 (COMESEP), and by a
Marie Curie International Outgoing Fellowship within the 7th European
Community Framework Programme. MT acknowledges the Austrian Science Fund
(FWF): FWF V195-N16. BVJ, JMC, and H-SY were supported by UCSD NSF
grants ATM-0852246 and AGS-1053766, NASA grant NNX11AB50G, and AFOSR
grant 11NE043. MMB acknowledges support on these analyses from UCSD NSF
grant ATM-0925023, and also from a UK STFC Standard Grant to Aberystwyth
University for continued CME and heliospheric interplanetary
scintillation (IPS) and white-light analyses. TAH was partially
supported by the NSF/SHINE Competition (Award 0849916) and the NASA
Heliophysics program (grant NNX10AC05G). CJF was supported by NASA grant
NX10AQ29G and NSF grant AGS-1140211.
NR 63
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD JUL
PY 2013
VL 285
IS 1-2
BP 317
EP 348
DI 10.1007/s11207-013-0260-5
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 138OS
UT WOS:000318518600019
ER
PT J
AU Tang, XW
Cattell, C
Dombeck, J
Dai, L
Wilson, LB
Breneman, A
Hupach, A
AF Tang, Xiangwei
Cattell, Cynthia
Dombeck, John
Dai, Lei
Wilson, Lynn B., III
Breneman, Aaron
Hupach, Adam
TI THEMIS observations of the magnetopause electron diffusion region: Large
amplitude waves and heated electrons
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE magnetic reconnection; electron diffusion region; waves; magnetopause
ID MAGNETIC-FIELD RECONNECTION; HYBRID-DRIFT INSTABILITY; PLASMA-WAVES;
DAYSIDE MAGNETOPAUSE; EARTHS MAGNETOPAUSE; MAGNETOTAIL; INSTRUMENT; MODE
AB We present the first observations of large amplitude waves in a well-defined electron diffusion region based on the criteria described by Scudder et al. [2012] at the subsolar magnetopause using data from one Time History of Events and Macroscale Interactions during Substorms (THEMIS) satellite. These waves identified as whistler mode waves, electrostatic solitary waves, lower hybrid waves, and electrostatic electron cyclotron waves, are observed in the same 12 s waveform capture and in association with signatures of active magnetic reconnection. The large amplitude waves in the electron diffusion region are coincident with abrupt increases in electron parallel temperature suggesting strong wave heating. The whistler mode waves, which are at the electron scale and which enable us to probe electron dynamics in the diffusion region were analyzed in detail. The energetic electrons (similar to 30keV) within the electron diffusion region have anisotropic distributions with T-e perpendicular to/T-e vertical bar > 1 that may provide the free energy for the whistler mode waves. The energetic anisotropic electrons may be produced during the reconnection process. The whistler mode waves propagate away from the center of the X-line along magnetic field lines, suggesting that the electron diffusion region is a possible source region of the whistler mode waves.
C1 [Tang, Xiangwei; Cattell, Cynthia; Dombeck, John; Dai, Lei; Breneman, Aaron; Hupach, Adam] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Wilson, Lynn B., III] NASA Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD USA.
RP Tang, XW (reprint author), Univ Minnesota, Sch Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA.
EM xtangphysics@gmail.com
RI Wilson III, Lynn/D-4425-2012;
OI Wilson III, Lynn/0000-0002-4313-1970; Cattell,
Cynthia/0000-0002-3805-320X
FU APL; NASA [NAS5-02099]; German Ministry for Economy and Technology;
German Center for Aviation and Space (DLR) [50 OC 0302]; [NNX08AF28];
[NNX13AE16G]
FX At the University of Minnesota, this work was supported by NNX08AF28,
NNX13AE16G, and a contract from APL for the development of RBSP/EFW. The
authors acknowledge NASA contract NAS5-02099 and V. Angelopoulos for use
of data from the THEMIS Mission, specifically: J. W. Bonnell and F. S.
Mozer for use of EFI data; D. Larson and R. P. Lin for use of SST data;
C. W. Carlson and J. P. McFadden for use of ESA data; A. Roux and O.
LeContel for use of SCM data; and K. H. Glassmeier, U. Auster, and W.
Baumjohann for the use of FGM data provided under the lead of the
Technical University of Braunschweig and with financial support through
the German Ministry for Economy and Technology and the German Center for
Aviation and Space (DLR) under contract 50 OC 0302. The authors are
grateful for discussion and comments from S. Thaller, K. Kersten, and C.
Colpitts.
NR 42
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U1 2
U2 15
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 JUN 28
PY 2013
VL 40
IS 12
BP 2884
EP 2890
DI 10.1002/grl.50565
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 185FJ
UT WOS:000321951300002
ER
PT J
AU Hodyss, R
Choukroun, M
Sotin, C
Beauchamp, P
AF Hodyss, Robert
Choukroun, Mathieu
Sotin, Christophe
Beauchamp, Patricia
TI The solubility of Ar-40 and Kr-84 in liquid hydrocarbons: Implications
for Titan's geological evolution
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Titan
ID NOBLE-GASES; COUPLING PHOTOCHEMISTRY; HAZE FORMATION; METHANE CYCLE;
LAKES; ATMOSPHERE; REMOVAL; OCEAN
AB The solubility of argon and krypton in methane and ethane has been experimentally determined at Titan-relevant temperatures. At typical Titan surface temperature (94K), argon and krypton solubilities are very large (47% in methane and 15% in ethane for Ar, 29% in methane and 43% in ethane for Kr), making liquid alkanes on Titan an important potential reservoir of Ar-40 and other noble gases. Large subsurface reservoirs of liquid ethane and methane could be sufficient to trap much of the argon outgassing from Titan's interior, which can help explain the discrepancy between the potential amount of Ar-40 produced inside Titan's interior and the amount observed in the atmosphere by Cassini-Huygens. Consequently, on Titan, liquid hydrocarbons may function as a buffer in the outgassing of volatiles from the interior, and they may strongly influence the evolution of the atmosphere's composition through the release of soluble gases upon evaporation and/or intake upon condensation.
C1 [Hodyss, Robert; Choukroun, Mathieu; Sotin, Christophe; Beauchamp, Patricia] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hodyss, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Robert.P.Hodyss@jpl.nasa.gov
RI Choukroun, Mathieu/F-3146-2017
OI Choukroun, Mathieu/0000-0001-7447-9139
FU NASA Astrobiology Institute; National Aeronautics and Space
Administration
FX Support from the NASA Astrobiology Institute is gratefully acknowledged.
This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. Government sponsorship acknowledged.
NR 32
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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 JUN 28
PY 2013
VL 40
IS 12
BP 2935
EP 2940
DI 10.1002/grl.50630
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 185FJ
UT WOS:000321951300011
ER
PT J
AU Velicogna, I
Wahr, J
AF Velicogna, I.
Wahr, J.
TI Time-variable gravity observations of ice sheet mass balance: Precision
and limitations of the GRACE satellite data
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ice mass balance; sea level; time variable gravity
ID LAST GLACIAL MAXIMUM; SEA-LEVEL; GREENLAND; MODEL; GRAVIMETRY; SURFACE;
SYSTEM; FIELD
AB [1]Time-variable gravity data from the Gravity Recovery and Climate Experiment (GRACE) mission have been available since 2002 to estimate the mass balance of the Greenland and Antarctic Ice Sheets. We analyze current progress and uncertainties in GRACE estimates of ice sheet mass balance. We discuss the impacts of errors associated with spherical harmonic truncation, spatial averaging, temporal sampling, and leakage from other time-dependent signals (e.g., glacial isostatic adjustment (GIA)). The largest sources of error for Antarctica are the GIA correction, the omission of l=1 terms, nontidal changes in ocean mass, and measurement errors. For Greenland, the errors come mostly from the uncertainty in the scaling factor. Using Release 5.0 (RL05) GRACE fields for January 2003 through November 2012, we find a mass change of -258 +/- 41Gt/yr for Greenland, with an acceleration of -31 +/- 6Gt/yr(2), and a loss that migrated clockwise around the ice sheet margin to progressively affect the entire periphery. For Antarctica, we report changes of -83 +/- 49 and -147 +/- 80Gt/yr for two GIA models, with an acceleration of -12 +/- 9Gt/yr(2) and a dominance from the southeast pacific sector of West Antarctica and the Antarctic Peninsula.
C1 [Velicogna, I.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Velicogna, I.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wahr, J.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Wahr, J.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
RP Velicogna, I (reprint author), Univ Calif Irvine, 226 Croul Hall, Irvine, CA 92697 USA.
EM isabella@uci.edu
FU NASA's Cryospheric Science Program; Solid Earth and Natural Hazards
Program; Terrestrial Hydrology Program; IDS Program; MEaSUREs Program
FX This work was performed at the University of California Irvine, the Jet
Propulsion Laboratory, California Institute of Technology, and the
University of Colorado, and was supported by grants from NASA's
Cryospheric Science Program, Solid Earth and Natural Hazards Program,
Terrestrial Hydrology Program, IDS Program, and MEaSUREs Program. We
thank the editor and one anonymous reviewer for their advice.
NR 42
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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 JUN 28
PY 2013
VL 40
IS 12
BP 3055
EP 3063
DI 10.1002/grl.50527
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA 185FJ
UT WOS:000321951300032
ER
PT J
AU Lau, WKM
Wu, HT
Kim, KM
AF Lau, William K. -M.
Wu, H. -T.
Kim, K. -M.
TI A canonical response of precipitation characteristics to global warming
from CMIP5 models
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE precipitation; global warming
ID TROPICAL PRECIPITATION; INTENSE PRECIPITATION; 21ST-CENTURY CLIMATE;
SIMULATIONS; MECHANISMS; EXTREMES; IMPACTS; TRENDS
AB In this study, we find from analyses of projections of 14 CMIP5 models a robust, canonical global response in rainfall characteristics to a warming climate. Under a scenario of 1% increase per year of CO2 emission, the model ensemble projects globally more heavy precipitation (+7 +/- 2.4%K-1), less moderate precipitation (-2.5 +/- 0.6%K-1), more light precipitation (+1.8 +/- 1.3%K-1), and increased length of dry (no-rain) periods (+4.7 +/- 2.1%K-1). Regionally, a majority of the models project a consistent response with more heavy precipitation over climatologically wet regions of the deep tropics, especially the equatorial Pacific Ocean and the Asian monsoon regions, and more dry periods over the land areas of the subtropics and the tropical marginal convective zones. Our results suggest that increased CO2 emissions induce a global adjustment in circulation and moisture availability manifested in basic changes in global precipitation characteristics, including increasing risks of severe floods and droughts in preferred geographic locations worldwide.
C1 [Lau, William K. -M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Wu, H. -T.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Kim, K. -M.] Morgan State Univ, Baltimore, MD 21239 USA.
RP Lau, WKM (reprint author), NASA, Goddard Space Flight Ctr, Div Earth Sci, Code 613,Bldg 33,Rm C121, Greenbelt, MD 20771 USA.
EM William.K.Lau@nasa.gov
RI Kim, Kyu-Myong/G-5398-2014; Lau, William /E-1510-2012
OI Lau, William /0000-0002-3587-3691
FU Precipitation Measurement Missions (PMM); CMIP5 Diagnostic Project,
Modeling and Analysis Program (MAP), NASA headquarters; Korea
Meteorological Administration Research and Development Program [CATER
2012-2062]
FX This work is partially funded by the Precipitation Measurement Missions
(PMM) and the CMIP5 Diagnostic Project, Modeling and Analysis Program
(MAP), NASA headquarters. K.-M. Kim was also supported by the Korea
Meteorological Administration Research and Development Program under
grant CATER 2012-2062.
NR 35
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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 JUN 28
PY 2013
VL 40
IS 12
BP 3163
EP 3169
DI 10.1002/grl.50420
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 185FJ
UT WOS:000321951300051
ER
PT J
AU Watanabe, M
Kamae, Y
Yoshimori, M
Oka, A
Sato, M
Ishii, M
Mochizuki, T
Kimoto, M
AF Watanabe, Masahiro
Kamae, Youichi
Yoshimori, Masakazu
Oka, Akira
Sato, Makiko
Ishii, Masayoshi
Mochizuki, Takashi
Kimoto, Masahide
TI Strengthening of ocean heat uptake efficiency associated with the recent
climate hiatus
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE climate hiatus; ocean heat uptake; GCM; surface temperature; energy
budget
ID EARTHS ENERGY; SENSITIVITY; AOGCM
AB The rate of increase of global-mean surface air temperature (SAT(g)) has apparently slowed during the last decade. We investigated the extent to which state-of-the-art general circulation models (GCMs) can capture this hiatus period by using multimodel ensembles of historical climate simulations. While the SAT(g) linear trend for the last decade is not captured by their ensemble means regardless of differences in model generation and external forcing, it is barely represented by an 11-member ensemble of a GCM, suggesting an internal origin of the hiatus associated with active heat uptake by the oceans. Besides, we found opposite changes in ocean heat uptake efficiency (), weakening in models and strengthening in nature, which explain why the models tend to overestimate the SAT(g) trend. The weakening of commonly found in GCMs seems to be an inevitable response of the climate system to global warming, suggesting the recovery from hiatus in coming decades.
C1 [Watanabe, Masahiro; Yoshimori, Masakazu; Oka, Akira; Kimoto, Masahide] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778568, Japan.
[Kamae, Youichi] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan.
[Sato, Makiko] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Sato, Makiko] Columbia Univ, Earth Inst, New York, NY USA.
[Ishii, Masayoshi] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki, Japan.
[Mochizuki, Takashi] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa, Japan.
RP Watanabe, M (reprint author), Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778568, Japan.
EM hiro@aori.u-tokyo.ac.jp
RI Kamae, Youichi/L-6694-2013; Mochizuki, Takashi/C-7466-2013; kimoto,
masahide/P-9077-2014
OI Kamae, Youichi/0000-0003-0461-5718; Mochizuki,
Takashi/0000-0001-7884-6717;
FU Program for Risk Information on Climate Change (SOUSEI project); MEXT,
Japan [23310014, 23340137]
FX The authors are grateful to G. A. Meehl and an anonymous reviewer for
their encouraging comments. This work was supported by the Program for
Risk Information on Climate Change (SOUSEI project) and Grants-in-Aid
23310014 and 23340137 from MEXT, Japan.
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PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUN 28
PY 2013
VL 40
IS 12
BP 3175
EP 3179
DI 10.1002/grl.50541
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 185FJ
UT WOS:000321951300053
ER
PT J
AU Minnis, P
Bedka, ST
Duda, DP
Bedka, KM
Chee, T
Ayers, JK
Palikonda, R
Spangenberg, DA
Khlopenkov, KV
Boeke, R
AF Minnis, Patrick
Bedka, Sarah T.
Duda, David P.
Bedka, Kristopher M.
Chee, Thad
Ayers, J. Kirk
Palikonda, Rabindra
Spangenberg, Douglas A.
Khlopenkov, Konstantin V.
Boeke, Robyn
TI Linear contrail and contrail cirrus properties determined from satellite
data
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE contrails; contrail cirrus; clouds; optical depth
ID AQUA MODIS DATA; NORTHERN-HEMISPHERE; CLIMATE; GROWTH
AB The properties of contrail cirrus clouds are retrieved through analysis of Terra and Aqua Moderate Resolution Imaging Spectroradiometer data for 21 cases of spreading linear contrails. For these cases, contrail cirrus enhanced the linear contrail coverage by factors of 2.4-7.6 depending on the contrail mask sensitivity. In dense air traffic areas, linear contrail detection sensitivity is apparently reduced when older contrails overlap and thus is likely diminished during the afternoon. The mean optical depths and effective particle sizes of the contrail cirrus were 2-3 times and 20% greater, respectively, than the corresponding values retrieved for the adjacent linear contrails. When contrails form below, in, or above existing cirrus clouds, the column cloud optical depth is increased and particle size is decreased. Thus, even without increased cirrus coverage, contrails will affect the radiation balance. These results should be valuable for refining model characterizations of contrail cirrus needed to fully assess the climate impacts of contrails.
C1 [Minnis, Patrick] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Bedka, Sarah T.; Duda, David P.; Bedka, Kristopher M.; Chee, Thad; Ayers, J. Kirk; Palikonda, Rabindra; Spangenberg, Douglas A.; Khlopenkov, Konstantin V.; Boeke, Robyn] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Minnis, P (reprint author), NASA, Climate Sci Branch, Langley Res Ctr, MS 420,21 Langley Blvd, Hampton, VA 23681 USA.
EM p.minnis@nasa.gov
RI Minnis, Patrick/G-1902-2010
OI Minnis, Patrick/0000-0002-4733-6148
FU Aviation Climate Change Research Initiative (ACCRI) [DTRT57-10-X-70020];
DOT
FX This work was supported by the Aviation Climate Change Research
Initiative (ACCRI) under contract DTRT57-10-X-70020 with the DOT. The
waypoint data used for this work were provided by U. S. DOT Volpe Center
and are based on data provided by the U. S. FAA and EUROCONTROL in
support of the objectives of the International Civil Aviation
Organization Committee on Aviation Environmental Protection
CO2 Task Group. Any opinions, findings, and conclusions or
recommendations expressed in this material are those of the authors and
do not necessarily reflect the views of the U. S. DOT Volpe Center, the
U. S. FAA, or EUROCONTROL.
NR 19
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U2 11
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 JUN 28
PY 2013
VL 40
IS 12
BP 3220
EP 3226
DI 10.1002/grl.50569
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 185FJ
UT WOS:000321951300061
ER
PT J
AU Yang, WD
Marshak, A
Kostinski, AB
Varnai, T
AF Yang, Weidong
Marshak, Alexander
Kostinski, Alexander B.
Varnai, Tamas
TI Shape-induced gravitational sorting of Saharan dust during transatlantic
voyage: Evidence from CALIOP lidar depolarization measurements
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Saharan dust; transport; CALIPSO; remote sensing; particle shape;
depolarization
ID MINERALOGICAL COMPOSITION; SAMUM 2006; PARTICLES; AEROSOL; WAVELENGTHS
AB Motivated by the physical picture of shape-dependent air resistance and, consequently, shape-induced differential sedimentation of dust particles, we searched for and found evidence of dust particle asphericity affecting the evolution and distribution of dust-scattered light depolarization ratio (). Specifically, we examined a large data set of Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) observations of Saharan dust from June to August 2007. Observing along a typical transatlantic dust track, we find that (1) median is uniformly distributed between 2 and 5km altitudes as the elevated dust leaves the west coast of Africa, thereby indicating uniformly random mixing of particle shapes with height; (2) vertical homogeneity of median breaks down during the westward transport: between 2 and 5km increases with altitude and this increase becomes more pronounced with westward progress; (3) tends to increase at higher altitude (>4km) and decrease at lower altitude (<4km) during the westward transport. All these features are captured qualitatively by a minimal model (two shapes only), suggesting that shape-induced differential settling and consequent sorting indeed contribute significantly to the observed temporal evolution and vertical stratification of dust properties. By implicating particle shape as a likely cause of gravitational sorting, these results will affect the estimates of radiative transfer through Saharan dust layers.
C1 [Yang, Weidong] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA.
[Yang, Weidong; Marshak, Alexander; Varnai, Tamas] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kostinski, Alexander B.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA.
[Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP Yang, WD (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA.
EM Weidong.Yang@nasa.gov
RI Marshak, Alexander/D-5671-2012
FU NASA; NSF [AGS-1119164]
FX We gratefully acknowledge support for this research by the NASA
Radiation Sciences Program managed by Hal Maring, by the NASA CALIPSO
project supervised by Charles Trepte as the technical officer, and by
NSF through grant AGS-1119164. We also thank Peter Colarco, Ralph Kahn,
Robert Levy, Zhaoyan Liu, Yuekui Yang, Hongbin Yu, and Tianle Yuan for
their helpful suggestions. We are also grateful for the insightful
comments by the anonymous referees.
NR 22
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U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUN 28
PY 2013
VL 40
IS 12
BP 3281
EP 3286
DI 10.1002/grl.50603
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 185FJ
UT WOS:000321951300072
ER
PT J
AU Li, T
Calvo, N
Yue, J
Dou, XK
Russell, JM
Mlynczak, MG
She, CY
Xue, XH
AF Li, Tao
Calvo, Natalia
Yue, Jia
Dou, Xiankang
Russell, J. M., III
Mlynczak, M. G.
She, Chiao-Yao
Xue, Xianghui
TI Influence of El Nino-Southern Oscillation in the mesosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE El Nino-Southern Oscillation; mesospheric temperature; SABER; WACCM
ID TEMPERATURES; STRATOSPHERE; MODEL; ENSO; CLIMATE; SIGNAL
AB Using the middle atmosphere temperature data set observed by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) satellite experiment between 2002 and 2012, and temperatures simulated by the Whole Atmospheric Community Climate Model version 3.5 (WACCM3.5) between 1953 and 2005, we studied the influence of El Nino-Southern Oscillation (ENSO) on middle atmosphere temperature during the Northern Hemisphere (NH) wintertime. For the first time, a significant winter temperature response to ENSO in the middle mesosphere has been observed, with an anomalous warming of 1.0K/MEI (Multivariate ENSO Index) in the tropics and an anomalous cooling of -2.0K/MEI in the NH middle latitudes. The observed temperature responses to ENSO in the mesosphere are opposite to those in the stratosphere, in agreement with previous modeling studies. Temperature responses to ENSO observed by SABER show similar patterns to those simulated by the WACCM3.5 model. Analysis of the WACCM3.5 residual mean meridional circulation response to ENSO reveals a significant downwelling in the tropical mesosphere and upwelling in the NH middle and high latitudes during warm ENSO events, which is mostly driven by anomalous eastward gravity wave forcing in the NH mesosphere.
C1 [Li, Tao; Dou, Xiankang; Xue, Xianghui] Univ Sci & Technol China, Dept Geophys & Planetary Sci, CAS Key Lab Geospace Environm, Hefei 230026, Anhui, Peoples R China.
[Calvo, Natalia] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Calvo, Natalia] Natl Ctr Atmospher Res, Adv Study Program, Boulder, CO 80307 USA.
[Yue, Jia; Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA USA.
[She, Chiao-Yao] Colorado State Univ, Dept Phys, Ft Collins, CO 80523 USA.
RP Li, T (reprint author), Univ Sci & Technol China, Dept Geophys & Planetary Sci, CAS Key Lab Geospace Environm, Hefei 230026, Anhui, Peoples R China.
EM litao@ustc.edu.cn
RI Yue, Jia/D-8177-2011; Dou, xiankang/M-9106-2013; Li, Tao/J-8950-2014;
Xue, Xianghui/E-1225-2012;
OI Li, Tao/0000-0002-5100-4429; Xue, Xianghui/0000-0002-4541-9900; CALVO
FERNANDEZ, NATALIA/0000-0001-6213-1864
FU National Natural Science Foundation of China [41225017, 41074108,
41127901, 41025016, 41121003]; Chinese Academy of Sciences [KZZD-EW-01];
Fundamental Research Funds for the Central Universities; Spanish
Ministry of Science [CSD 2007-00050]; NSF/AGS [1136082]
FX This work was carried out at the University of Science and Technology of
China, with support from the National Natural Science Foundation of
China grants (41225017, 41074108, 41127901, 41025016, 41121003), the
Chinese Academy of Sciences Key Research Program KZZD-EW-01, and the
Fundamental Research Funds for the Central Universities. N.C.'s work was
partly supported by the Spanish Ministry of Science through the project
Supercomputing and e-Science, Consolider CSD 2007-00050. C.Y.S.'s work
was supported by NSF/AGS grant 1136082. We are grateful to the SABER
retrieval team for producing a high-quality data set that is made
readily available to the scientific community. The SABER data were
downloaded from http://saber.gats-inc.com/.
NR 23
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U1 0
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUN 28
PY 2013
VL 40
IS 12
BP 3292
EP 3296
DI 10.1002/grl.50598
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 185FJ
UT WOS:000321951300074
ER
PT J
AU Britch, SC
Binepal, YS
Ruder, MG
Kariithi, HM
Linthicum, KJ
Anyamba, A
Small, JL
Tucker, CJ
Ateya, LO
Oriko, AA
Gacheru, S
Wilson, WC
AF Britch, Seth C.
Binepal, Yatinder S.
Ruder, Mark G.
Kariithi, Henry M.
Linthicum, Kenneth J.
Anyamba, Assaf
Small, Jennifer L.
Tucker, Compton J.
Ateya, Leonard O.
Oriko, Abuu A.
Gacheru, Stephen
Wilson, William C.
TI Rift Valley Fever Risk Map Model and Seroprevalence in Selected Wild
Ungulates and Camels from Kenya
SO PLOS ONE
LA English
DT Article
ID SAUDI-ARABIA; VERTICAL TRANSMISSION; VEGETATION INDEX; AFRICAN BUFFALO;
VIRUS; OUTBREAK; ANTIBODY; HUMANS; PREVALENCE; PREVENTION
AB Since the first isolation of Rift Valley fever virus (RVFV) in the 1930s, there have been multiple epizootics and epidemics in animals and humans in sub-Saharan Africa. Prospective climate-based models have recently been developed that flag areas at risk of RVFV transmission in endemic regions based on key environmental indicators that precede Rift Valley fever (RVF) epizootics and epidemics. Although the timing and locations of human case data from the 2006-2007 RVF outbreak in Kenya have been compared to risk zones flagged by the model, seroprevalence of RVF antibodies in wildlife has not yet been analyzed in light of temporal and spatial predictions of RVF activity. Primarily wild ungulate serum samples from periods before, during, and after the 2006-2007 RVF epizootic were analyzed for the presence of RVFV IgM and/or IgG antibody. Results show an increase in RVF seropositivity from samples collected in 2007 (31.8%), compared to antibody prevalence observed from 2000-2006 (3.3%). After the epizootic, average RVF seropositivity diminished to 5% in samples collected from 2008-2009. Overlaying maps of modeled RVF risk assessments with sampling locations indicated positive RVF serology in several species of wild ungulate in or near areas flagged as being at risk for RVF. Our results establish the need to continue and expand sero-surveillance of wildlife species Kenya and elsewhere in the Horn of Africa to further calibrate and improve the RVF risk model, and better understand the dynamics of RVFV transmission.
C1 [Britch, Seth C.; Linthicum, Kenneth J.] ARS, Ctr Med Agr & Vet Entomol, USDA, Gainesville, FL USA.
[Binepal, Yatinder S.; Kariithi, Henry M.; Ateya, Leonard O.; Oriko, Abuu A.] Kenya Agr Res Inst, Ctr Biotechnol, Nairobi, Kenya.
[Ruder, Mark G.; Wilson, William C.] ARS, Arthropod Borne Anim Dis Res Unit, Ctr Grain & Anim Hlth Res, USDA, Manhattan, KS USA.
[Anyamba, Assaf; Small, Jennifer L.; Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gacheru, Stephen] Vet Serv, Kabete, Kenya.
RP Wilson, WC (reprint author), ARS, Arthropod Borne Anim Dis Res Unit, Ctr Grain & Anim Hlth Res, USDA, Manhattan, KS USA.
EM william.wilson@ars.usda.gov
FU International Atomic Energy Agency (IAEA); US Department of Agriculture,
Agricultural Research Service Project [58-5430-005-00D]; Science and
Technology Directorate of the U.S. Department of Homeland Security
[HSHQDC-07-00982]; Department of Defense-Armed Forces Health
Surveillance Center; United States Department of Agriculture
-Agricultural Research Service, Division of GEIS Operations
FX We are indebted to the International Atomic Energy Agency (IAEA) for the
initial funding of this study. This project was also support in part by
the US Department of Agriculture, Agricultural Research Service Project
#58-5430-005-00D through an interagency agreement with the Science and
Technology Directorate of the U.S. Department of Homeland Security under
Award Number HSHQDC-07-00982. The Department of Defense-Armed Forces
Health Surveillance Center, Division of GEIS Operations and the United
States Department of Agriculture -Agricultural Research Service
supported the RVF Monitoring and Risk Mapping project. The funders had
no role in study design, data collection and analysis, decision to
publish, or preparation of the manuscript.
NR 52
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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 JUN 28
PY 2013
VL 8
IS 6
AR e66626
DI 10.1371/journal.pone.0066626
PG 14
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 174IH
UT WOS:000321148400018
PM 23840512
ER
PT J
AU Melosh, HJ
Freed, AM
Johnson, BC
Blair, DM
Andrews-Hanna, JC
Neumann, GA
Phillips, RJ
Smith, DE
Solomon, SC
Wieczorek, MA
Zuber, MT
AF Melosh, H. J.
Freed, Andrew M.
Johnson, Brandon C.
Blair, David M.
Andrews-Hanna, Jeffrey C.
Neumann, Gregory A.
Phillips, Roger J.
Smith, David E.
Solomon, Sean C.
Wieczorek, Mark A.
Zuber, Maria T.
TI The Origin of Lunar Mascon Basins
SO SCIENCE
LA English
DT Article
ID INTERNAL STRUCTURE; GRAVITY-FIELD; MOON; IMPACTS; SIMULATIONS; MISSION;
MERCURY; GRAIL; CRUST; MODEL
AB High-resolution gravity data from the Gravity Recovery and Interior Laboratory spacecraft have clarified the origin of lunar mass concentrations (mascons). Free-air gravity anomalies over lunar impact basins display bull's-eye patterns consisting of a central positive (mascon) anomaly, a surrounding negative collar, and a positive outer annulus. We show that this pattern results from impact basin excavation and collapse followed by isostatic adjustment and cooling and contraction of a voluminous melt pool. We used a hydrocode to simulate the impact and a self-consistent finite-element model to simulate the subsequent viscoelastic relaxation and cooling. The primary parameters controlling the modeled gravity signatures of mascon basins are the impactor energy, the lunar thermal gradient at the time of impact, the crustal thickness, and the extent of volcanic fill.
C1 [Melosh, H. J.; Freed, Andrew M.; Blair, David M.] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA.
[Melosh, H. J.; Johnson, Brandon C.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Andrews-Hanna, Jeffrey C.] Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA.
[Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA.
[Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 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 10964 USA.
[Wieczorek, Mark A.] Univ Paris Diderot, Inst Phys Globe Paris, Sorbonne Paris Cite, F-75205 Paris 13, France.
RP Melosh, HJ (reprint author), Purdue Univ, Dept Earth Atmospher & Planetary Sci, 550 Stadium Mall Dr, W Lafayette, IN 47907 USA.
EM jmelosh@purdue.edu
RI Wieczorek, Mark/G-6427-2010; Neumann, Gregory/I-5591-2013;
OI Wieczorek, Mark/0000-0001-7007-4222; Neumann,
Gregory/0000-0003-0644-9944; Johnson, Brandon/0000-0002-4267-093X
FU NASA
FX The GRAIL mission is supported by NASA's Discovery Program and is
performed under contract to the Massachusetts Institute of Technology
and the Jet Propulsion Laboratory. The Lunar Reconnaissance Orbiter LOLA
investigation is supported by the NASA Science Mission Directorate under
contract to the NASA Goddard Space Flight Center and Massachusetts
Institute of Technology. Data from the GRAIL and LOLA missions have been
deposited in the Geosciences Node of NASA's Planetary Data System.
NR 22
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U2 26
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 JUN 28
PY 2013
VL 340
IS 6140
BP 1552
EP 1555
DI 10.1126/science.1235768
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 172ME
UT WOS:000321007000036
PM 23722426
ER
PT J
AU Wen, GY
Cahalan, RF
Haigh, JD
Pilewskie, P
Oreopoulos, L
Harder, JW
AF Wen, Guoyong
Cahalan, Robert F.
Haigh, Joanna D.
Pilewskie, Peter
Oreopoulos, Lazaros
Harder, Jerald W.
TI Reconciliation of modeled climate responses to spectral solar forcing
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE SORCE; SSI; RCM
ID STRATOSPHERIC OZONE; ATMOSPHERE; CYCLE; IRRADIANCE; VARIABILITY;
EQUILIBRIUM; RADIATION; MISSIONS; IMPACT; ATLAS
AB The SIM (Spectral Irradiance Monitor) on SORCE (Solar Radiation and Climate Experiment) provides more spectrally complete daily SSI (spectral solar irradiance) measurements than ever before, allowing us to explore chemical and physical processes in the Earth's ocean and atmosphere system. However, the newly observed SSI instigated controversies in the Sun-climate community on whether the SIM-observed trends are true solar variations and on whether climate responses are in phase or out of phase with solar forcing. In this study, we focus on resolving two apparently contradictory results published on possible temperature responses to SIM-derived solar forcing. When applying extreme scenarios of SIM-based spectral solar forcing in a radiative-convective model (RCM), we find that some apparently contradictory results can be explained by the different methods used to apply the SIM SSI data. It is clear that accurate SSI data are essential for accurate climate simulations and that climate modelers need to take care how they apply these data.
C1 [Wen, Guoyong; Cahalan, Robert F.; Oreopoulos, Lazaros] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wen, Guoyong] Morgan State Univ, Baltimore, MD 21239 USA.
[Haigh, Joanna D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England.
[Pilewskie, Peter] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
RP Wen, GY (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
EM Guoyong.Wen-1@nasa.gov
RI Oreopoulos, Lazaros/E-5868-2012; Haigh, Joanna/F-6847-2014
OI Oreopoulos, Lazaros/0000-0001-6061-6905; Haigh,
Joanna/0000-0001-5504-4754
FU NASA's Living With a Star program
FX This research was supported by NASA's Living With a Star program managed
by M. Guhathakurta. We also thank A. Arking, J. Lean, W. Ridgway, and D.
Rind for helpful discussions.
NR 39
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U2 12
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 JUN 27
PY 2013
VL 118
IS 12
BP 6281
EP 6289
DI 10.1002/jgrd.50506
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600027
ER
PT J
AU de Boer, G
Bauer, SE
Toto, T
Menon, S
Vogelmann, AM
AF de Boer, G.
Bauer, S. E.
Toto, T.
Menon, Surabi
Vogelmann, A. M.
TI Evaluation of aerosol-cloud interaction in the GISS ModelE using ARM
observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE climate model; aerosol cloud interactions; model evaluation; remote
sensing
ID GLOBAL CLIMATE MODELS; GENERAL-CIRCULATION MODEL; GROUND-BASED
MEASUREMENTS; EFFECTIVE RADIUS; SATELLITE DATA; WATER CLOUDS;
PARAMETERIZATION; MICROPHYSICS; SIMULATIONS; VAPOR
AB Observations from the US Department of Energy's Atmospheric Radiation Measurement (ARM) program are used to evaluate the ability of the NASA GISS ModelE global climate model in reproducing observed interactions between aerosols and clouds. Included in the evaluation are comparisons of basic meteorology and aerosol properties, droplet activation, effective radius parameterizations, and surfacebased evaluations of aerosolcloud interactions (ACI). Differences between the simulated and observed ACI are generally large, but these differences may result partially from vertical distribution of aerosol in the model, rather than the representation of physical processes governing the interactions between aerosols and clouds. Compared to the current observations, the ModelE often features elevated droplet concentrations for a given aerosol concentration, indicating that the activation parameterizations used may be too aggressive. Additionally, parameterizations for effective radius commonly used in models were tested using ARM observations, and there was no clear superior parameterization for the cases reviewed here. This lack of consensus is demonstrated to result in potentially large, statistically significant differences to surface radiative budgets, should one parameterization be chosen over another.
C1 [de Boer, G.] Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[de Boer, G.] NOAA Earth Syst Res Lab, Div Phys Sci, Boulder, CO USA.
[de Boer, G.; Menon, Surabi] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Bauer, S. E.] Columbia Univ, Earth Inst, New York, NY USA.
[Bauer, S. E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Toto, T.; Vogelmann, A. M.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Menon, Surabi] ClimateWorks Fdn, San Francisco, CA USA.
RP de Boer, G (reprint author), Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
EM gijs.deboer@colorado.edu
RI Vogelmann, Andrew/M-8779-2014; Bauer, Susanne/P-3082-2014
OI Vogelmann, Andrew/0000-0003-1918-5423;
FU Office of Science, Office of Biological and Environmental Research of
the U.S. Department of Energy as part of their Climate and Earth System
Modeling Program [DE-AC02-05CH11231]; FASTER project; National Oceanic
and Atmospheric Administration, U.S. Department of Commerce
[NA17RJ1229]; National Science Foundation [ARC-1203902]; US Department
of Energy [DE-SC0008794]; U.S. DOE [DE-AC02-98CH10886]; NASA High-End
Computing (HEC) Program through the NASA Center for Climate Simulation
(NCCS) at Goddard Space Flight Center; U.S. Department of Energy, Office
of Science, Office of Biological and Environmental Research, Climate and
Environmental Sciences Division
FX This research was supported by the Director, Office of Science, Office
of Biological and Environmental Research of the U.S. Department of
Energy under Contract DE-AC02-05CH11231 as part of their Climate and
Earth System Modeling Program and through the FASTER project. LBNL is
managed by the University of California under the same grant. This work
was prepared in part at the Cooperative Institute for Research in
Environmental Sciences (CIRES) with support in part from the National
Oceanic and Atmospheric Administration, U.S. Department of Commerce,
under cooperative agreement NA17RJ1229 and other grants. The statements,
findings, conclusions, and recommendations are those of the authors and
do not necessarily reflect the views of the National Oceanic and
Atmospheric Administration or the Department of Commerce. GB was
supported in part by the National Science Foundation (ARC-1203902) and
US Department of Energy (DE-SC0008794). Computing resources were
provided by NASA and the US Department of Energy. A.V. wishes to
acknowledge funding from the U.S. DOE (contract DE-AC02-98CH10886).
2NFOV retrievals were generously provided by Christine Chiu, and China
AMF data were provided by Maureen Cribb and Zanquing Li. Resources
supporting this work were provided by the NASA High-End Computing (HEC)
Program through the NASA Center for Climate Simulation (NCCS) at Goddard
Space Flight Center. Data were obtained from the Atmospheric Radiation
Measurement (ARM) Program sponsored by the U.S. Department of Energy,
Office of Science, Office of Biological and Environmental Research,
Climate and Environmental Sciences Division.
NR 45
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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 JUN 27
PY 2013
VL 118
IS 12
BP 6383
EP 6395
DI 10.1002/jgrd.50460
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600035
ER
PT J
AU Eck, TF
Holben, BN
Reid, JS
Mukelabai, MM
Piketh, SJ
Torres, O
Jethva, HT
Hyer, EJ
Ward, DE
Dubovik, O
Sinyuk, A
Schafer, JS
Giles, DM
Sorokin, M
Smirnov, A
Slutsker, I
AF Eck, T. F.
Holben, B. N.
Reid, J. S.
Mukelabai, M. M.
Piketh, S. J.
Torres, O.
Jethva, H. T.
Hyer, E. J.
Ward, D. E.
Dubovik, O.
Sinyuk, A.
Schafer, J. S.
Giles, D. M.
Sorokin, M.
Smirnov, A.
Slutsker, I.
TI A seasonal trend of single scattering albedo in southern African
biomass-burning particles: Implications for satellite products and
estimates of emissions for the world's largest biomass-burning source
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol absorption; biomass burning; southern Africa
ID AEROSOL OPTICAL DEPTH; OZONE MONITORING INSTRUMENT; SKY RADIANCE
MEASUREMENTS; SAFARI 2000; WAVELENGTH DEPENDENCE; ATMOSPHERIC AEROSOLS;
PHYSICAL-PROPERTIES; AERONET; MODIS; SMOKE
AB As a representative site of the southern African biomass-burning region, sun-sky data from the 15 year Aerosol Robotic Network (AERONET) deployment at Mongu, Zambia, was analyzed. For the biomass-burning season months (July-November), we investigate seasonal trends in aerosol single scattering albedo (SSA), aerosol size distributions, and refractive indices from almucantar sky scan retrievals. The monthly mean single scattering albedo at 440nm in Mongu was found to increase significantly from similar to 0.84 in July to similar to 0.93 in November (from 0.78 to 0.90 at 675nm in these same months). There was no significant change in particle size, in either the dominant accumulation or secondary coarse modes during these months, nor any significant trend in the Angstrom exponent (440-870nm; r(2)=0.02). A significant downward seasonal trend in imaginary refractive index (r(2)=0.43) suggests a trend of decreasing black carbon content in the aerosol composition as the burning season progresses. Similarly, burning season SSA retrievals for the Etosha Pan, Namibia AERONET site also show very similar increasing single scattering albedo values and decreasing imaginary refractive index as the season progresses. Furthermore, retrievals of SSA at 388nm from the Ozone Monitoring Instrument satellite sensor show similar seasonal trends as observed by AERONET and suggest that this seasonal shift is widespread throughout much of southern Africa. A seasonal shift in the satellite retrieval bias of aerosol optical depth from the Moderate Resolution Imaging Spectroradiometer collection 5 dark target algorithm is consistent with this seasonal SSA trend since the algorithm assumes a constant value of SSA. Multi-angle Imaging Spectroradiometer, however, appears less sensitive to the absorption-induced bias.
C1 [Eck, T. F.; Jethva, H. T.] Univ Space Res Assoc, Columbia, MD USA.
[Eck, T. F.; Holben, B. N.; Torres, O.; Jethva, H. T.; Sinyuk, A.; Schafer, J. S.; Giles, D. M.; Sorokin, M.; Smirnov, A.; Slutsker, I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Reid, J. S.; Hyer, E. J.] Naval Res Lab, Monterey, CA USA.
[Mukelabai, M. M.] Zambian Meteorol Dept, Lusaka, Zambia.
[Piketh, S. J.] North West Univ, Sch Geo & Spatial Sci, Potchefstroom, South Africa.
[Ward, D. E.] White Salmon, Enviropyron, Washington, DC USA.
[Dubovik, O.] Univ Lille, Villeneuve Dascq, France.
[Sinyuk, A.; Schafer, J. S.; Giles, D. M.; Sorokin, M.; Smirnov, A.; Slutsker, I.] Sigma Space Corp, Lanham, MD USA.
RP Eck, TF (reprint author), NASA, Goddard Space Flight Ctr, Code 618, Greenbelt, MD 20771 USA.
EM thomas.f.eck@nasa.gov
RI Dubovik, Oleg/A-8235-2009; Reid, Jeffrey/B-7633-2014; Hyer,
Edward/E-7734-2011; Torres, Omar/G-4929-2013; Smirnov,
Alexander/C-2121-2009
OI Dubovik, Oleg/0000-0003-3482-6460; Reid, Jeffrey/0000-0002-5147-7955;
Hyer, Edward/0000-0001-8636-2026; Smirnov, Alexander/0000-0002-8208-1304
NR 79
TC 29
Z9 29
U1 1
U2 40
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 JUN 27
PY 2013
VL 118
IS 12
BP 6414
EP 6432
DI 10.1002/jgrd.50500
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600037
ER
PT J
AU Huang, JF
Hsu, NC
Tsay, SC
Liu, ZY
Jeong, MJ
Hansell, RA
Lee, J
AF Huang, Jingfeng
Hsu, N. Christina
Tsay, Si-Chee
Liu, Zhaoyan
Jeong, Myeong-Jae
Hansell, Richard A.
Lee, Jaehwa
TI Use of spaceborne lidar for the evaluation of thin cirrus contamination
and screening in the Aqua MODIS Collection 5 aerosol products
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE thin cirrus; aerosol; AQUA-MODIS; CALIPSO; VFM; cirrus screening
ID OPTICAL DEPTH; CLOUD CONTAMINATION; CALIPSO; SATELLITE; ALGORITHM;
RETRIEVALS; 1.38-MU-M; CHANNELS; OCEAN; RATIO
AB Cloud contamination from subvisual thin cirrus clouds is still a challenging issue for operational satellite aerosol retrievals. In the A-Train constellation, concurrent high-sensitivity cirrus observations from the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) provide us with an unprecedented opportunity to examine the susceptibility of the Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) aerosol retrievals to thin cirrus contamination and to evaluate the robustness of various cirrus screening techniques. Quantitative evaluations indicate that the current cirrus screening schemes in the MODIS Dark Target and Deep Blue Collection 5 aerosol retrievals can effectively remove most cirrus signals while some residual thin cirrus signals still exist with strong spatial and seasonal variability. Results also show significant linkage between thin cirrus occurrence frequency and the susceptibility of aerosol retrievals to thin cirrus contamination. Using the CALIPSO cirrus observations as a reference, we also examined the effectiveness and robustness of eight MODIS-derived cirrus screening parameters. These parameters include apparent reflectance at 1.38 mu m (R1.38), cirrus reflectance at 0.66 mu m (CR0.66), CR0.66 cirrus flag (CF), reflectance ratio between 1.38 mu m and 0.66 mu m (RR1.38/0.66), reflectance ratio between 1.38 mu m and 1.24 mu m (RR1.38/1.24), brightness temperature difference between 8.6 mu m and 11 mu m (BTD8.6-11), brightness temperature difference between 11 mu m and 12 mu m (BTD11-12), and cloud phase infrared approach (CPIR). Among these parameters, RR1.38/0.66 achieves the best overall performance, followed by the BTD11-12. Results from several test cases suggest that the cirrus screening schemes in the operational MODIS aerosol retrieval algorithms can be further improved to reduce thin cirrus contamination.
C1 [Huang, Jingfeng; Hansell, Richard A.; Lee, Jaehwa] UMD, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA.
[Huang, Jingfeng] NOAA, Ctr Satellite Applicat & Res, NESDIS, College Pk, MD 20740 USA.
[Hsu, N. Christina; Tsay, Si-Chee; Hansell, Richard A.; Lee, Jaehwa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Liu, Zhaoyan] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Liu, Zhaoyan] Sci Syst & Applicat Inc, Hampton, VA USA.
[Jeong, Myeong-Jae] Gangneung Wonju Natl Univ, Dept Atmospher & Environm Sci, Kangnung, South Korea.
RP Huang, JF (reprint author), NOAA, Ctr Satellite Applicat & Res, NESDIS, 5825 Univ Res Court, College Pk, MD 20740 USA.
EM jingfeng.huang@noaa.gov
RI Huang, Jingfeng/D-7336-2012; Liu, Zhaoyan/B-1783-2010; Tsay,
Si-Chee/J-1147-2014; Hansell, Richard/J-2065-2014
OI Huang, Jingfeng/0000-0002-8779-2922; Liu, Zhaoyan/0000-0003-4996-5738;
FU NASA EOS Program
FX This work is supported by grant from the NASA EOS Program, managed by
Hal Maring. Authors thank Brent N. Holben, Alexander Smirnov, Ellsworth
J. Welton, Robert C. Levy, David M. Giles, Bo-Cai Gao, Steve Ou, James
R. Campbell, and Zhien Wang for their constructive comments on the use
of in situ and satellite data, analysis methodology, and cirrus
climatology. The authors thank three anonymous reviewers for their
constructive and insightful comments that lead to the significant
improvements of the paper. Aqua MODIS L1B and L2 data were obtained from
NASA L1 and Atmosphere Archive and Distribution System (LAADS). CALIPSO
data were obtained from the NASA Langley Research Center Atmospheric
Science Data Center.
NR 37
TC 4
Z9 4
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 27
PY 2013
VL 118
IS 12
BP 6444
EP 6453
DI 10.1002/jgrd.50504
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600039
ER
PT J
AU Wu, LT
Su, H
Jiang, JH
AF Wu, Longtao
Su, Hui
Jiang, Jonathan H.
TI Regional simulation of aerosol impacts on precipitation during the East
Asian summer monsoon
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol impacts on precipitation; East Asian summer monsoon; WRF-Chem
ID CLIMATE-CHEMISTRY/AEROSOL MODEL; GENERAL-CIRCULATION MODEL;
ANTHROPOGENIC AEROSOLS; SULFATE AEROSOLS; BLACK CARBON; CHINA; CLOUDS;
POLLUTION; VARIABILITY; INHIBITION
AB The Weather Research and Forecasting model with Chemistry is used to examine aerosol impacts on precipitation over China during the East Asian summer monsoon (EASM). In the first EASM phase (6 May to 13 June), monsoonal rainband is located to the south of high aerosol areas. The surface cooling by the aerosol radiative effect induces an anticyclonic circulation in northern China, causing a precipitation decrease over southern China. The aerosol microphysical effect tends to broaden the precipitation region. In the second EASM phase (14 June to 5 August), the precipitation band jumps to northern China, where heavy pollution locates. By serving as cloud condensation nuclei, the aerosol microphysical effect causes a reduction of local cloudiness and induces ascent to the north and descent to the south, leading to a precipitation shift from south to north. The aerosol radiative effect strengthens such a meridional asymmetry. Moisture budget analysis shows that the aerosol-induced anomalies of precipitation in both phases are mainly contributed by the changes in vertical velocity associated with convection, while the horizontal advection of moisture plays a nonnegligible role. Our study highlights that aerosol effects on EASM precipitation depend on the location of monsoon precipitation band and its relative location to aerosols, which may be the main factor that contributed to the discrepancy in literature regarding the aerosol impacts on the so-called southern flood and northern flood over China.
C1 [Wu, Longtao] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Wu, Longtao; Su, Hui; Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Wu, LT (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
EM longtao.wu@jpl.nasa.gov
FU NASA AST program; NASA
FX The MODIS and TRMM data used in this study were produced with the
Giovanni online data system, developed and maintained by the National
Aeronautics and Space Administration (NASA) GES DISC. We acknowledge the
MODIS and TRMM teams for the data used. We thank the PIs for their
efforts in establishing and maintaining the AERONET sites at Beijing,
Xianghe, and Taihu. The CALIPSO data were obtained from the NASA Langley
Research Center Atmospheric Science Data Center. The ERA-Interim data
were downloaded from the UCAR website
http://rda.ucar.edu/datasets/ds627.0. The valuable comments and
suggestions from three anonymous reviewers are appreciated. This study
is supported by NASA AST program. This research was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with NASA.
NR 56
TC 19
Z9 20
U1 4
U2 52
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 27
PY 2013
VL 118
IS 12
BP 6454
EP 6467
DI 10.1002/jgrd.50527
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600040
ER
PT J
AU Millan, L
Read, W
Kasai, Y
Lambert, A
Livesey, N
Mendrok, J
Sagawa, H
Sano, T
Shiotani, M
Wu, DL
AF Millan, L.
Read, W.
Kasai, Y.
Lambert, A.
Livesey, N.
Mendrok, J.
Sagawa, H.
Sano, T.
Shiotani, M.
Wu, D. L.
TI SMILES ice cloud products
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE SMILES; retrievals; IWC; pIWP
ID TROPICAL UPPER TROPOSPHERE; RADIATIVE-TRANSFER; DIURNAL CYCLE; CIRRUS
CLOUDS; PARTICLE-SIZE; 183 GHZ; MISSION; CLIMATE; PARAMETERIZATION;
SIMULATIONS
AB Upper tropospheric water vapor and clouds play an important role in Earth's climate, but knowledge of them, in particular diurnal variation in deep convective clouds, is limited. An essential variable to understand them is cloud ice water content. The Japanese Superconducting Submillimeter-Wave Limb-Emission Sounder (SMILES) on board the International Space Station (ISS) samples the atmosphere at different local times allowing the study of diurnal variability of atmospheric parameters. We describe a new ice cloud data set consisting of partial Ice Water Path and Ice Water Content. Preliminary comparisons with EOS-MLS, CloudSat-CPR and CALIOP-CALIPSO are presented. Then, the diurnal variation over land and over open ocean for partial ice water path is reported. Over land, a pronounced diurnal variation peaking strongly in the afternoon/early evening was found. Over the open ocean, little temporal dependence was encountered. This data set is publicly available for download in HDF5 format.
C1 [Millan, L.; Read, W.; Lambert, A.; Livesey, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Kasai, Y.; Mendrok, J.; Sagawa, H.] Nat Inst Informat & Commun Technol, Tokyo, Japan.
[Mendrok, J.] Lulea Univ Technol, Kiruna, Sweden.
[Sano, T.] Japan Aerosp Explorat Agcy, Tokyo, Japan.
[Shiotani, M.] Kyoto Univ, Kyoto, Japan.
[Wu, D. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Millan, L (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM lmillan@jpl.nasa.gov
RI Mendrok, Jana/D-9349-2013; Millan, Luis/J-2759-2015
OI Mendrok, Jana/0000-0002-0032-2021;
FU National Aeronautics and Space Administration
FX The research described in this paper was carried out by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
JEM/SMILES mission is a joint project of Japan Aerospace Exploration
Agency (JAXA) and National Institute of Information and Communications
Technology (NICT).
NR 52
TC 8
Z9 8
U1 0
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 27
PY 2013
VL 118
IS 12
BP 6468
EP 6477
DI 10.1002/jgrd.50322
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600041
ER
PT J
AU Menut, L
Perez, C
Haustein, K
Bessagnet, B
Prigent, C
Alfaro, S
AF Menut, Laurent
Perez, Carlos
Haustein, Karsten
Bessagnet, Bertrand
Prigent, Catherine
Alfaro, Stephane
TI Impact of surface roughness and soil texture on mineral dust emission
fluxes modeling
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE mineral dust; emissions fluxes; transport modeling
ID GENERAL-CIRCULATION MODEL; DRY DEPOSITION; GOCART MODEL; AEROSOLS; WIND;
DISTRIBUTIONS; SENSITIVITY; SIMULATION; AEROCOM; DESERT
AB Dust production models (DPM) used to estimate vertical fluxes of mineral dust aerosols over arid regions need accurate data on soil and surface properties. The Laboratoire Inter-Universitaire des Systemes Atmospheriques (LISA) data set was developed for Northern Africa, the Middle East, and East Asia. This regional data set was built through dedicated field campaigns and include, among others, the aerodynamic roughness length, the smooth roughness length of the erodible fraction of the surface, and the dry (undisturbed) soil size distribution. Recently, satellite-derived roughness length and high-resolution soil texture data sets at the global scale have emerged and provide the opportunity for the use of advanced schemes in global models. This paper analyzes the behavior of the ERS satellite-derived global roughness length and the State Soil Geographic data base-Food and Agriculture Organization of the United Nations (STATSGO-FAO) soil texture data set (based on wet techniques) using an advanced DPM in comparison to the LISA data set over Northern Africa and the Middle East. We explore the sensitivity of the drag partition scheme (a critical component of the DPM) and of the dust vertical fluxes (intensity and spatial patterns) to the roughness length and soil texture data sets. We also compare the use of the drag partition scheme to a widely used preferential source approach in global models. Idealized experiments with prescribed wind speeds show that the ERS and STATSGO-FAO data sets provide realistic spatial patterns of dust emission and friction velocity thresholds in the region. Finally, we evaluate a dust transport model for the period of March to July 2011 with observed aerosol optical depths from Aerosol Robotic Network sites. Results show that ERS and STATSGO-FAO provide realistic simulations in the region.
C1 [Menut, Laurent] Ecole Polytech, Meteorol Dynam Lab, CNRS, Institut PS Laplace,UMR 8539, Palaiseau, France.
[Perez, Carlos] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Perez, Carlos] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Haustein, Karsten] Barcelona Supercomp Ctr, Div Earth Sci, Barcelona, Spain.
[Haustein, Karsten] Univ Oxford, Sch Geog & Environm, Oxford, England.
[Bessagnet, Bertrand] Inst Natl Environm Ind & Risques, INERIS, Verneuil En Halatte, France.
[Prigent, Catherine] Observ Paris, CNRS UMR 8112, Lab Etud Rayonnement & Matiere Astrophys, F-75014 Paris, France.
[Alfaro, Stephane] Univ Paris Diderot, Univ Parie Est Creteil, Lab Interuniv Syst Atmospher, CNRS UMR 7583, Creteil, France.
RP Menut, L (reprint author), Ecole Polytech, Meteorol Dynam Lab, Palaiseau, France.
EM menut@lmd.polytechnique.fr
RI Menut, Laurent/O-2296-2016; Bessagnet, Bertrand/O-2969-2016
OI Menut, Laurent/0000-0001-9776-0812; Perez Garcia-Pando,
Carlos/0000-0002-4456-0697; Bessagnet, Bertrand/0000-0003-2062-4681
FU French Ministry in charge of Ecology
FX This study was partly funded by the French Ministry in charge of
Ecology. We thank the principal investigators and their staff for
establishing and maintaining the AERONET sites used in this study:
Didier Tanre for Banizoumbou, Capo Verde and Dakar; Bernadette Chatenet
and Jean-Louis Rajot for Zinder and Cinzana; and Daniela Meloni for
Lampedusa.
NR 61
TC 26
Z9 26
U1 1
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 27
PY 2013
VL 118
IS 12
BP 6505
EP 6520
DI 10.1002/jgrd.50313
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600044
ER
PT J
AU Lebsock, M
Morrison, H
Gettelman, A
AF Lebsock, Matthew
Morrison, Hugh
Gettelman, Andrew
TI Microphysical implications of cloud-precipitation covariance derived
from satellite remote sensing
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE accretion; autoconversion; sub-grid correlation; scale dependence
ID BOUNDARY-LAYER CLOUDS; COMMUNITY ATMOSPHERE MODEL; GENERAL-CIRCULATION
MODEL; SUBGRID-SCALE VARIABILITY; MARINE STRATOCUMULUS; PART I; SPATIAL
VARIABILITY; MODIS; PARAMETERIZATION; SCHEME
AB Covariance between cloud and precipitation water in shallow marine boundary layer clouds is assessed using collocated satellite observations from CloudSat and the moderate resolution imaging spectroradiometer (MODIS) at spatial scales typical of global models. An analytic construct is presented, which suggests that global models that do not take subgrid scale cloud-precipitation covariance into account in their microphysical parameterizations may significantly underestimate grid mean microphysical process rates in warm clouds. The proposed framework indicates a mean bias in autoconversion rates of 129% when subgrid scale cloud water variability is neglected and bias in accretion rates of 60% when subgrid cloud-precipitation covariability is neglected at a model grid resolution of 141km. The bias in accretion rate is dependent on the significant correlation () found between cloud and precipitation, which in the global mean is found to be =0.44. The regional distribution of the process rate biases is largely governed by the spatial pattern of cloud water variance. Specific areas of low cloud water variance are found in the subtropical eastern ocean basins and the high latitudes, whereas much of the tropics display relatively larger cloud water variance. These regional distinctions in cloud water variance are associated with commensurate regionality in the process rate biases. The magnitude of the bias has a scale dependence that is governed by the spatial scaling behavior of the cloud and precipitation variances, which follow a power law scaling with exponent of 2/3 at scales below about 10km and decreasing exponent above this length scale. While the parametric framework reduces biases in the accretion rate estimated from the grid-mean values of cloud and precipitation water, it is shown that it still undercorrects the accretion rate because it neglects the fact that the precipitation fractional area is less than the cloud fractional area and is preferentially colocated with the highest cloud water concentrations. These results imply that (1) predicting the appropriate balance of autoconversion to accretion in global models requires not only the subgrid scale cloud water variability but also the subgrid scale covariability of cloud and precipitation water and (2) the ability of a global model to calculate the correct regional variation in process rates depends crucially on the fidelity of that model to predict or diagnose the spatial distribution of the variance in cloud water.
C1 [Lebsock, Matthew] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morrison, Hugh; Gettelman, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Lebsock, M (reprint author), CALTECH, Jet Prop Lab, M-S 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM matthew.d.lebsock@jpl.nasa.gov
FU U.S. National Science Foundation; NSF Climate Process Team [0968648,
0968657]
FX 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 National Center for
Atmospheric Research (NCAR) is sponsored by the U.S. National Science
Foundation. This work was also supported by an NSF Climate Process Team,
grants 0968648 to Colorado State University and 0968657 to NCAR.
CloudSat data were acquired through the DPC and can be accessed through
their Web site http://www.cloudsat.cira.colostate.edu. MODIS products
were obtained from the Goddard Distributed Active Archive Center (DAAC).
Finally, we acknowledge the insightful critiques of three anonymous
reviewers whose comments greatly improved the manuscript.
NR 45
TC 19
Z9 21
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 JUN 27
PY 2013
VL 118
IS 12
BP 6521
EP 6533
DI 10.1002/jgrd.50347
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600045
ER
PT J
AU Davies, L
Jakob, C
Cheung, K
Del Genio, A
Hill, A
Hume, T
Keane, RJ
Komori, T
Larson, VE
Lin, Y
Liu, X
Nielsen, BJ
Petch, J
Plant, RS
Singh, MS
Shi, X
Song, X
Wang, W
Whitall, MA
Wolf, A
Xie, S
Zhang, G
AF Davies, L.
Jakob, C.
Cheung, K.
Del Genio, A.
Hill, A.
Hume, T.
Keane, R. J.
Komori, T.
Larson, V. E.
Lin, Y.
Liu, X.
Nielsen, B. J.
Petch, J.
Plant, R. S.
Singh, M. S.
Shi, X.
Song, X.
Wang, W.
Whitall, M. A.
Wolf, A.
Xie, S.
Zhang, G.
TI A single-column model ensemble approach applied to the TWP-ICE
experiment
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE TWP-ICE; Single Column Model; Ensemble
ID CLOUD-RESOLVING MODELS; GENERAL-CIRCULATION MODELS; LARGE-SCALE MODELS;
BOUNDARY-LAYER; PART I; RADIATIVE PROPERTIES; CONVECTION SCHEME; MOIST
CONVECTION; VERSION-3 CAM3; CLIMATE MODELS
AB Single-column models (SCM) are useful test beds for investigating the parameterization schemes of numerical weather prediction and climate models. The usefulness of SCM simulations are limited, however, by the accuracy of the best estimate large-scale observations prescribed. Errors estimating the observations will result in uncertainty in modeled simulations. One method to address the modeled uncertainty is to simulate an ensemble where the ensemble members span observational uncertainty. This study first derives an ensemble of large-scale data for the Tropical Warm Pool International Cloud Experiment (TWP-ICE) based on an estimate of a possible source of error in the best estimate product. These data are then used to carry out simulations with 11 SCM and two cloud-resolving models (CRM). Best estimate simulations are also performed. All models show that moisture-related variables are close to observations and there are limited differences between the best estimate and ensemble mean values. The models, however, show different sensitivities to changes in the forcing particularly when weakly forced. The ensemble simulations highlight important differences in the surface evaporation term of the moisture budget between the SCM and CRM. Differences are also apparent between the models in the ensemble mean vertical structure of cloud variables, while for each model, cloud properties are relatively insensitive to forcing. The ensemble is further used to investigate cloud variables and precipitation and identifies differences between CRM and SCM particularly for relationships involving ice. This study highlights the additional analysis that can be performed using ensemble simulations and hence enables a more complete model investigation compared to using the more traditional single best estimate simulation only.
C1 [Davies, L.] Monash Univ, Sch Math, Melbourne, Vic 3004, Australia.
[Jakob, C.] Monash Univ, ARC Ctr Excellence Climate Syst Sci, Melbourne, Vic 3004, Australia.
[Cheung, K.] Bur Meteorol, Melbourne, Vic, Australia.
[Del Genio, A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Hill, A.; Petch, J.] Met Off, Exeter, Devon, England.
[Hume, T.] Bur Meteorol, Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia.
[Keane, R. J.] Univ Munich, Inst Meteorol, D-80539 Munich, Germany.
[Komori, T.] Japan Meteorol Agcy, Tokyo, Japan.
[Larson, V. E.; Nielsen, B. J.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Lin, Y.] Univ Corp Atmospher Res, Boulder, CO USA.
[Lin, Y.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Liu, X.; Shi, X.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Plant, R. S.; Whitall, M. A.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Singh, M. S.] MIT, Cambridge, MA 02139 USA.
[Song, X.; Zhang, G.] Univ Calif San Diego, San Diego, CA 92103 USA.
[Wang, W.] NOAA, IMSG, Natl Ctr Environm Predict, College Pk, MD USA.
[Wolf, A.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Xie, S.] Lawrence Livermore Natl Lab, Livermore, CA USA.
RP Davies, L (reprint author), Univ Melbourne, Sch Earth Sci, Melbourne, Vic 3010, Australia.
EM laura.davies@unimelb.edu.au
RI Liu, Xiaohong/E-9304-2011; lin, yanluan/A-6333-2015; Xie,
Shaocheng/D-2207-2013; Jakob, Christian/A-1082-2010
OI Liu, Xiaohong/0000-0002-3994-5955; Plant, Robert/0000-0001-8808-0022;
Xie, Shaocheng/0000-0001-8931-5145; Jakob, Christian/0000-0002-5012-3207
FU Office of Science (BER); U.S. Department of Energy [DE-SC0002731]; U.S.
Department of Energy Atmospheric System Research Program; United States
Department of Energy [DE-SC0006927, DE-SC0008668]; National Science
Foundation [AGS-0968640]; U.S. Department of Energy (DOE), Office of
Science, Atmospheric System Research (ASR) program; Battelle Memorial
Institute [DE-AC06-76RLO 1830]; National Natural Science Foundation of
China [41075039]; U.S. Department of Energy (DOE), Office of Science,
Office of Biological and Environmental Research by Lawrence Livermore
National Laboratory [DE-AC52-07NA27344]; Atmospheric Radiation
Measurement Program of the Office of Science at the DOE
FX Davies and Jakob are supported by the Office of Science (BER), U.S.
Department of Energy, under grant DE-SC0002731. Many of the other
coauthors also participated through support from the U.S. Department of
Energy Atmospheric System Research Program. V. Larson and B. Nielsen are
grateful for financial support from the United States Department of
Energy (grants DE-SC0006927 and DE-SC0008668) and the National Science
Foundation (grant AGS-0968640). Support for X. Liu was provided by the
U.S. Department of Energy (DOE), Office of Science, Atmospheric System
Research (ASR) program. The Pacific Northwest National Laboratory is
operated for DOE by Battelle Memorial Institute under contract
DE-AC06-76RLO 1830. Dr. Weiguo Wang is partly supported by the National
Natural Science Foundation of China under Grant No. 41075039. The
contributions of S. Xie to this work were performed under the auspices
of the U.S. Department of Energy (DOE), Office of Science, Office of
Biological and Environmental Research by Lawrence Livermore National
Laboratory under contract No. DE-AC52-07NA27344 and supported by the
Atmospheric Radiation Measurement Program of the Office of Science at
the DOE.
NR 88
TC 13
Z9 13
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 27
PY 2013
VL 118
IS 12
BP 6544
EP 6563
DI 10.1002/jgrd.50450
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600047
ER
PT J
AU Lu, GP
Cummer, SA
Li, JB
Zigoneanu, L
Lyons, WA
Stanley, MA
Rison, W
Krehbiel, PR
Edens, HE
Thomas, RJ
Beasley, WH
Weiss, SA
Blakeslee, RJ
Bruning, EC
MacGorman, DR
Meyer, TC
Palivec, K
Ashcraft, T
Samaras, T
AF Lu, Gaopeng
Cummer, Steven A.
Li, Jingbo
Zigoneanu, Lucian
Lyons, Walter A.
Stanley, Mark A.
Rison, William
Krehbiel, Paul R.
Edens, Harald E.
Thomas, Ronald J.
Beasley, William H.
Weiss, Stephanie A.
Blakeslee, Richard J.
Bruning, Eric C.
MacGorman, Donald R.
Meyer, Tiffany C.
Palivec, Kevin
Ashcraft, Thomas
Samaras, Tim
TI Coordinated observations of sprites and in-cloud lightning flash
structure
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Review
DE red sprite; positive cloud-to-ground ( plus CG) stroke; Lightning
Mapping Array; lightning charge transfer; in-cloud lightning structure;
mesoscale convective system
ID MESOSCALE CONVECTIVE SYSTEMS; CHARGE MOMENT CHANGES; RED SPRITES;
THUNDERSTORM ELECTRIFICATION; ELECTRICAL STRUCTURES; CONTINUING CURRENT;
POSITIVE CHARGE; SPACE-SHUTTLE; ELF RADIATION; DISCHARGES
AB The temporal and spatial development of sprite-producing lightning flashes is examined with coordinated observations over an asymmetric mesoscale convective system (MCS) on 29 June 2011 near the Oklahoma Lightning Mapping Array (LMA). Sprites produced by a total of 26 lightning flashes were observed simultaneously on video from Bennett, Colorado and Hawley, Texas, enabling a triangulation of sprites in comparison with temporal development of parent lightning (in particular, negatively charged stepped leaders) in three-dimensional space. In general, prompt sprites produced within 20ms after the causative stroke are less horizontally displaced (typically <30km) from the ground stroke than delayed sprites, which usually occur over 40ms after the stroke with significant lateral offsets (>30km). However, both prompt and delayed sprites are usually centered within 30km of the geometric center of relevant LMA sources (with affinity to negative stepped leaders) during the prior 100ms interval. Multiple sprites appearing as dancing/jumping events associated with a single lightning flash could be produced either by distinct strokes of the flash, by a single stroke through a series of current surges superposed on an intense continuing current, or by both. Our observations imply that sprites elongated in one direction are sometimes linked to in-cloud leader structure with the same elongation, and sprites that were more symmetric were produced above the progression of multiple negative leaders. This suggests that the large-scale structure of sprites could be affected by the in-cloud geometry of positive charge removal. Based on an expanded dataset of 39 sprite-parent flashes by including more sprites recorded by one single camera over the same MCS, the altitude (above mean sea level, MSL) of positively charged cloud region tapped by sprite-producing strokes declined gradually from similar to 10km MSL (-35 degrees C) to around 6km MSL (-10 degrees C) as the MCS evolved through the mature stage. On average, the positive charge removal by causative strokes of sprites observed on 29 June is centered at 3.6km above the freezing level or at 7.9km above ground level.
C1 [Lu, Gaopeng; Cummer, Steven A.; Li, Jingbo; Zigoneanu, Lucian] Duke Univ, Dept Elect & Comp Engn, Durham, NC USA.
[Lyons, Walter A.] FMA Res Inc, Ft Collins, CO USA.
[Stanley, Mark A.; Rison, William; Krehbiel, Paul R.; Edens, Harald E.; Thomas, Ronald J.] New Mexico Inst Min & Technol, Langmuir Lab, Socorro, NM 87801 USA.
[Beasley, William H.; Weiss, Stephanie A.] Univ Oklahoma, Sch Meteorol, Norman, OK 73019 USA.
[Blakeslee, Richard J.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
[Bruning, Eric C.] Texas Tech Univ, Dept Geosci, Lubbock, TX 79409 USA.
[MacGorman, Donald R.] Natl Severe Storms Lab, Norman, OK 73069 USA.
[Meyer, Tiffany C.] Natl Weather Serv, Warning Decis Training Branch, Norman, OK USA.
[Ashcraft, Thomas] Heliotown Observ, Lamy, NM USA.
[Samaras, Tim] Samaras Technol, Bennett, CO USA.
RP Lu, GP (reprint author), Chinese Acad Sci, Inst Atmospher Phys, Lab Middle Atmosphere & Global Environm Observat, Beijing 100029, Peoples R China.
EM gaopenglu@gmail.com
RI Lu, Gaopeng/D-9011-2012; Cummer, Steven/A-6118-2008;
OI Cummer, Steven/0000-0002-0002-0613; MacGorman,
Donald/0000-0002-2395-8196
FU DARPA Nimbus program; NSF Physical and Dynamic Meteorology program;
William P. Winn of Langmuir Laboratory; Matuszeski Graduate Research
Fund of New Mexico Tech.
FX We wish to dedicate this paper to the memory of contributor Tim Samaras,
who tragically perished along with his son Paul Samaras and fellow
severe storm researcher Carl Young during the El Reno, Oklahoma EF-5
tornado on 31 May 2013 while collecting vital in-situ measurements. This
work was supported by the DARPA Nimbus program and the NSF Physical and
Dynamic Meteorology program. Many people offered help to install and
operate SpriteCam and LF systems, including Eric Cramer, Shahab
Arabshahi, and Joseph Dwyer from Florida Institute of Technology; Thomas
C. Marshall, Maribeth Stolzenburg, and Sumedhe Karunarathne from
University of Mississippi; James Roberts and Krokhin Arkadii from
University of North Texas; and Ruth Douglas Miller and Liang-Wu Cai from
Kansas State University. Danyal Petersen provided the access to OKLMA
data. The work of Gaopeng Lu on sprites was supported by William P. Winn
of Langmuir Laboratory and the Matuszeski Graduate Research Fund of New
Mexico Tech.
NR 105
TC 23
Z9 24
U1 1
U2 18
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 JUN 27
PY 2013
VL 118
IS 12
BP 6607
EP 6632
DI 10.1002/jgrd.50459
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600051
ER
PT J
AU Ghan, SJ
Smith, SJ
Wang, MH
Zhang, K
Pringle, KJ
Carslaw, KS
Pierce, JR
Bauer, SE
Adams, PJ
AF Ghan, Steven J.
Smith, Steven J.
Wang, Minghuai
Zhang, Kai
Pringle, Kirsty J.
Carslaw, Kenneth S.
Pierce, Jeffrey R.
Bauer, Susanne E.
Adams, Peter J.
TI A simple model of global aerosol indirect effects
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol; cloud; interactions; indirect; climate
ID CLOUD CONDENSATION NUCLEI; GENERAL-CIRCULATION MODEL; CARBON-CYCLE
MODELS; CLIMATE MODEL; ORGANIC AEROSOL; MARINE STRATOCUMULUS;
UNCERTAINTY ANALYSIS; MICROPHYSICS MODEL; ATMOSPHERE-OCEAN; SENSITIVITY
AB Most estimates of the global mean indirect effect of anthropogenic aerosol on the Earth's energy balance are from simulations by global models of the aerosol lifecycle coupled with global models of clouds and the hydrologic cycle. Extremely simple models have been developed for integrated assessment models, but lack the flexibility to distinguish between primary and secondary sources of aerosol. Here a simple but more physically based model expresses the aerosol indirect effect (AIE) using analytic representations of cloud and aerosol distributions and processes. Although the simple model is able to produce estimates of AIEs that are comparable to those from some global aerosol models using the same global mean aerosol properties, the estimates by the simple model are sensitive to preindustrial cloud condensation nuclei concentration, preindustrial accumulation mode radius, width of the accumulation mode, size of primary particles, cloud thickness, primary and secondary anthropogenic emissions, the fraction of the secondary anthropogenic emissions that accumulates on the coarse mode, the fraction of the secondary mass that forms new particles, and the sensitivity of liquid water path to droplet number concentration. Estimates of present-day AIEs as low as -5 W m(-2) and as high as -0.3 W m(-2) are obtained for plausible sets of parameter values. Estimates are surprisingly linear in emissions. The estimates depend on parameter values in ways that are consistent with results from detailed global aerosol-climate simulation models, which adds to understanding of the dependence on AIE uncertainty on uncertainty in parameter values.
C1 [Ghan, Steven J.; Smith, Steven J.; Wang, Minghuai; Zhang, Kai] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Pringle, Kirsty J.; Carslaw, Kenneth S.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England.
[Pierce, Jeffrey R.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Bauer, Susanne E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Adams, Peter J.] Carnegie Mellon Univ, Ctr Atmospher Particle Studies, Pittsburgh, PA 15213 USA.
RP Ghan, SJ (reprint author), Pacific NW Natl Lab, 902 Battelle Blvd, Richland, WA 99352 USA.
EM steve.ghan@pnnl.gov
RI Wang, Minghuai/E-5390-2011; Pierce, Jeffrey/E-4681-2013; Carslaw,
Ken/C-8514-2009; Adams, Peter/D-7134-2013; Zhang, Kai/F-8415-2010; Ghan,
Steven/H-4301-2011
OI Wang, Minghuai/0000-0002-9179-228X; Pierce, Jeffrey/0000-0002-4241-838X;
Carslaw, Ken/0000-0002-6800-154X; Adams, Peter/0000-0003-0041-058X;
Zhang, Kai/0000-0003-0457-6368; Ghan, Steven/0000-0001-8355-8699
FU Office of Science of the U.S. Department of Energy as part of the
Atmospheric System Research Program; U.S. Environmental Protection
Agency, Climate Change Division; DOE by Battelle Memorial Institute
[DE-AC06-76RLO 1830]
FX The authors thank colleague Ben Kravitz and reviewers Rob Wood and Chris
Golaz for helpful comments. Support for S. Ghan, M. Wang, and K. Zhang
was provided by the Office of Science of the U.S. Department of Energy
as part of the Atmospheric System Research Program. Support for S. Smith
was provided by the U.S. Environmental Protection Agency, Climate Change
Division. The Pacific Northwest National Laboratory (PNNL) is operated
for the DOE by Battelle Memorial Institute under contract DE-AC06-76RLO
1830.
NR 84
TC 19
Z9 19
U1 2
U2 44
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 JUN 27
PY 2013
VL 118
IS 12
BP 6688
EP 6707
DI 10.1002/jgrd.50567
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 187OY
UT WOS:000322129600057
ER
PT J
AU Iwahashi, T
Enoto, T
Yamada, S
Nishioka, H
Nakazawa, K
Tamagawa, T
Makishima, K
AF Iwahashi, Takanori
Enoto, Teruaki
Yamada, Shin'ya
Nishioka, Hiroyuki
Nakazawa, Kazuhiro
Tamagawa, Toru
Makishima, Kazuo
TI Suzaku Follow-Up Observation of the Activated Magnetar 1E 1547.0-5408
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE pulsars: individual (1E 1547.0-5408, SGR J1550-5418, PSR 1550-5418);
star: pulsar: general
ID X-RAY PULSAR; SOFT GAMMA-REPEATERS; SGR 0501+4516; BOARD SUZAKU;
SUPERNOVA REMNANT; RXTE OBSERVATIONS; NEUTRON-STARS; SHORT BURSTS; 4U
0142+61; DISCOVERY
AB We present broadband X-ray analyses of the magnetar 1E 1547.0-5408 observed with Suzaku on 2010 August 7, nearly one and a half years after an intense outburst in 2009 January. The 2-10 keV flux decreased to (1.06 +/- 0.01) x 10(-11) erg cm(-2) s(-1), while the hard X-ray detection was 3.5 sigma (18-40 keV) and 2.4 sigma (18-35 keV) significance levels, where the former includes only the 2% systematic error of the non X-ray background, and the latter further takes into account possible near-by contaminating sources, respectively. Our confirmation of both soft and hard X-ray components during the late phase of the outburst strengthened the possibility that most magnetars are composed of the two spectral components, both in burst-active and less-active states. Together with a similar decay speed between the soft and hard components, their radiation mechanisms are suggested to be tightly related to each other. The 1-40 keV broadband spectrum was successfully fitted with the same model as used in the fit just after the onset of the outburst in 2009: a surface blackbody radiation with photoelectric absorption and a hard power-law. The blackbody flux decreased to be similar to 30% of that in 2009 while keeping its temperature at kT = 0.65 keV, suggesting a shrinking hotspot on the magnetar surface by a factor of 0.3. The hard power-law extended up to at least similar to 35 keV with a photon index of Gamma = 1.1 +/- 0.4, which was consistent with the 2009 value. The flux ratio, xi, of the 1-60 keV power-law to 1-60 keV thermal component was calculated to be xi = 1.2 +/- 0.7 at the late phase of the outburst for the first time. The obtained value follows the previously known negative correlation with the characteristic age, implying that the correlation holds for most of the magnetar states: no burst, onset and late phase of outbursts.
C1 [Iwahashi, Takanori; Enoto, Teruaki; Yamada, Shin'ya; Tamagawa, Toru; Makishima, Kazuo] Inst Phys & Chem Res, High Energy Astrophys Lab, Wako, Saitama 3510198, Japan.
[Iwahashi, Takanori; Tamagawa, Toru] Tokyo Univ Sci, Dept Phys, Shinjyuku Ku, Tokyo 1628601, Japan.
[Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nishioka, Hiroyuki; Nakazawa, Kazuhiro; Makishima, Kazuo] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
RP Iwahashi, T (reprint author), Inst Phys & Chem Res, High Energy Astrophys Lab, 2-1 Hirosawa, Wako, Saitama 3510198, Japan.
EM iwahashi@crab.riken.jp
RI XRAY, SUZAKU/A-1808-2009
FU Special Postdoctoral Researchers Program in RIKEN; JSPS KAKENHI Grant
[24740129]; [22.7385]
FX The authors would like to express their hearty thanks to the Suzaku team
members. We are grateful to Professor S. Shibata for his useful
suggestions. The research presented in this paper has been financed by a
Grant-in-Aid for JSPS Fellows (22.7385). T.E. is supported by a
Grant-in-Aid for superlative JSPS Fellows. S.Y. is supported by the
Special Postdoctoral Researchers Program in RIKEN and JSPS KAKENHI Grant
Number 24740129.
NR 53
TC 1
Z9 1
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD JUN 25
PY 2013
VL 65
IS 3
AR 52
DI 10.1093/pasj/65.3.52
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 181PW
UT WOS:000321682000009
ER
PT J
AU Lee, JE
Frankenberg, C
van der Tol, C
Berry, JA
Guanter, L
Boyce, CK
Fisher, JB
Morrow, E
Worden, JR
Asefi, S
Badgley, G
Saatchi, S
AF Lee, Jung-Eun
Frankenberg, Christian
van der Tol, Christiaan
Berry, Joseph A.
Guanter, Luis
Boyce, C. Kevin
Fisher, Joshua B.
Morrow, Eric
Worden, John R.
Asefi, Salvi
Badgley, Grayson
Saatchi, Sassan
TI Forest productivity and water stress in Amazonia: observations from
GOSAT chlorophyll fluorescence
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE chlorophyll fluorescence; Amazon; water stress; drought
ID STOMATAL CONDUCTANCE; CO2 ASSIMILATION; CARBON-DIOXIDE; SEVERE DROUGHT;
CLIMATE-CHANGE; RAIN-FOREST; PHOTOSYNTHESIS; MODEL; CANOPY; PLANTS
AB It is unclear to what extent seasonal water stress impacts on plant productivity over Amazonia. Using new Greenhouse gases Observing SATellite (GOSAT) satellite measurements of sun-induced chlorophyll fluorescence, we show that midday fluorescence varies with water availability, both of which decrease in the dry season over Amazonian regions with substantial dry season length, suggesting a parallel decrease in gross primary production (GPP). Using additional SeaWinds Scatterometer onboard QuikSCAT satellite measurements of canopy water content, we found a concomitant decrease in daily storage of canopy water content within branches and leaves during the dry season, supporting our conclusion. A large part (r(2) = 0.75) of the variance in observed monthly midday fluorescence from GOSAT is explained by water stress over moderately stressed evergreen forests over Amazonia, which is reproduced by model simulations that include a full physiological representation of photosynthesis and fluorescence. The strong relationship between GOSAT and model fluorescence (r(2) = 0.79) was obtained using a fixed leaf area index, indicating that GPP changes are more related to environmental conditions than chlorophyll contents. When the dry season extended to drought in 2010 over Amazonia, midday basin-wide GPP was reduced by 15 per cent compared with 2009.
C1 [Lee, Jung-Eun; Frankenberg, Christian; Fisher, Joshua B.; Worden, John R.; Badgley, Grayson; Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[van der Tol, Christiaan] Univ Twente, Fac Geoinformat Sci & Earth Observat, NL-7500 AE Enschede, Netherlands.
[Berry, Joseph A.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Guanter, Luis] Free Univ Berlin, Inst Space Sci, Berlin, Germany.
[Boyce, C. Kevin] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Morrow, Eric] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Asefi, Salvi] Arizona State Univ, Sch Life Sci, Tempe, AZ USA.
RP Lee, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM jung-eun.lee@jpl.nasa.gov
RI Guanter, Luis/I-1588-2015; van der Tol, Christiaan/A-2403-2010;
Frankenberg, Christian/A-2944-2013;
OI Guanter, Luis/0000-0002-8389-5764; van der Tol,
Christiaan/0000-0002-2484-8191; Frankenberg,
Christian/0000-0002-0546-5857; Fisher, Joshua/0000-0003-4734-9085
FU Emmy Noether Programme of the German Research Foundation (GlobFluo
project); Carbon Cycle; NASA under terrestrial ecology; National
Aeronautics and Space Administration; W.M. Keck Institute for Space
Studies
FX We acknowledge the entire GOSAT team for having designed and built the
instrument and especially A. Kuze and H. Suto for their tremendous
efforts in helping understand GOSAT calibration in the O2 A-band. We
acknowledge all MODIS land product science team members for providing an
invaluable public dataset. ECMWF ERA-Interim data used in this study
have been provided by ECMWF. We thank M. Zhao (University of Montana)
for providing the updated LAI and GPP products and M. Jung and M.
Reichstein for providing the MPI-BGC dataset. We also thank anonymous
reviewers and S. Saleska for providing careful and constructive comments
on our manuscript. L.G.'s work has been funded by the Emmy Noether
Programme of the German Research Foundation (GlobFluo project), and S.S.
acknowledges the support by Carbon Cycle funding from NASA under
terrestrial ecology. This research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration, and is supported in
part by the W.M. Keck Institute for Space Studies.
NR 49
TC 44
Z9 44
U1 7
U2 119
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
EI 1471-2954
J9 P ROY SOC B-BIOL SCI
JI Proc. R. Soc. B-Biol. Sci.
PD JUN 22
PY 2013
VL 280
IS 1761
AR 20130171
DI 10.1098/rspb.2013.0171
PG 9
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 141XS
UT WOS:000318760500001
PM 23760636
ER
PT J
AU Dugaiczyk, L
Ngo-Duc, TT
Gacusan, J
Singh, K
Yang, J
Santhanam, S
Han, JW
Koehne, JE
Kobayashi, NP
Meyyappan, M
Oye, MM
AF Dugaiczyk, Lars
Tam-Triet Ngo-Duc
Gacusan, Jovi
Singh, Karandeep
Yang, Jonathan
Santhanam, Sarnath
Han, Jin-Woo
Koehne, Jessica E.
Kobayashi, Nobuhiko P.
Meyyappan, M.
Oye, Michael M.
TI Resistive switching in single vertically-aligned ZnO nanowire grown
directly on Cu substrate
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
ID MEMORY
AB We report unipolar resistive switching measurements from single vertical ZnO nanowires grown directly on a copper substrate. Electrical measurements using a conductive atomic force microscope show conductive filament formation at 30 kV/cm, which is an order of magnitude lower field than that for bulk films and suggest a preferential filament formation likely on the surface of the nanowires. A high resistive ratio of three orders of magnitude was observed between the high and low resistive memory states. (C) 2013 Elsevier B. V. All rights reserved.
C1 [Dugaiczyk, Lars; Tam-Triet Ngo-Duc; Gacusan, Jovi; Singh, Karandeep; Yang, Jonathan; Han, Jin-Woo; Koehne, Jessica E.; Meyyappan, M.; Oye, Michael M.] NASA, Ames Res Ctr, Ames Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Dugaiczyk, Lars; Tam-Triet Ngo-Duc; Gacusan, Jovi; Singh, Karandeep; Yang, Jonathan; Santhanam, Sarnath; Han, Jin-Woo; Koehne, Jessica E.; Kobayashi, Nobuhiko P.; Oye, Michael M.] NASA, Ames Res Ctr, UCSC NASA ARC Adv Studies Labs, Moffett Field, CA 94035 USA.
[Dugaiczyk, Lars; Santhanam, Sarnath; Kobayashi, Nobuhiko P.; Oye, Michael M.] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA.
RP Oye, MM (reprint author), NASA, Ames Res Ctr, Ames Ctr Nanotechnol, Moffett Field, CA 94035 USA.
EM Michael.M.Oye@nasa.gov
RI Kobayashi, Nobuhiko/E-3834-2012
FU NASA [NNX09AQ44A]
FX NASA grant NNX09AQ44A to UCSC is acknowledged for instruments in UCSC
MACS Facility within UCSC/NASA-ARC Advanced Studies Laboratories. L. D.,
K. S., J.Y. are student interns. T.-T. N.-D., J.G., M.O. are employed by
ELORET Corporation at NASA Ames.
NR 23
TC 7
Z9 7
U1 5
U2 62
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2614
EI 1873-4448
J9 CHEM PHYS LETT
JI Chem. Phys. Lett.
PD JUN 21
PY 2013
VL 575
BP 112
EP 114
DI 10.1016/j.cplett.2013.05.005
PG 3
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 168QL
UT WOS:000320720500021
ER
PT J
AU Radue, E
Crisman, E
Wang, L
Kittiwatanakul, S
Lu, J
Wolf, SA
Wincheski, R
Lukaszew, RA
Novikova, I
AF Radue, E.
Crisman, E.
Wang, L.
Kittiwatanakul, S.
Lu, J.
Wolf, S. A.
Wincheski, R.
Lukaszew, R. A.
Novikova, I.
TI Effect of a substrate-induced microstructure on the optical properties
of the insulator-metal transition temperature in VO2 thin films
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID VANADIUM DIOXIDE; PHASE-TRANSITION; DEPOSITION
AB Using both Raman spectroscopy and direct laser reflectivity measurements, we investigate the optical properties of vanadium dioxide (VO2) thin films deposited on different substrates as they undergo the thermally induced insulator to metal phase transition. Comparing similarly prepared VO2 films grown on quartz, sapphire, and rutile substrates, we observed a significant difference in the transition temperatures without hysteresis loop broadening after heating and cooling the samples. We attribute these different transition temperatures to differences in the VO2 microstructure, mainly the difference in average grain sizes. We also observed variations in the contrast of the detected Raman resonances using different wavelengths for the excitation laser, and found that in all cases a longer wavelength (in our case 785 nm) yielded the clearest VO2 Raman spectra. (C) 2013 AIP Publishing LLC.
C1 [Radue, E.; Crisman, E.; Wang, L.; Lukaszew, R. A.; Novikova, I.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Kittiwatanakul, S.; Wolf, S. A.] Univ Virginia, Dept Phys, Charlottesville, VA 22904 USA.
[Lu, J.; Wolf, S. A.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22904 USA.
[Wincheski, R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Radue, E (reprint author), Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
EM elradue@email.wm.edu
OI Wang, Lei/0000-0002-1767-5202
FU NSF [DMR-1006013]; NRI/SRC
FX This work was financed by NSF, DMR-1006013: Plasmon Resonances and Metal
Insulator Transitions in Highly Correlated Thin Film Systems. We also
acknowledge support from the NRI/SRC sponsored ViNC center and the
Commonwealth of Virginia through the Virginia Micro-Electronics
Consortium (VMEC).
NR 21
TC 17
Z9 17
U1 1
U2 76
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD JUN 21
PY 2013
VL 113
IS 23
AR 233104
DI 10.1063/1.4811689
PG 6
WC Physics, Applied
SC Physics
GA 172NT
UT WOS:000321011700005
ER
PT J
AU Giacintucci, S
Kale, R
Wik, DR
Venturi, T
Markevitch, M
AF Giacintucci, Simona
Kale, Ruta
Wik, Daniel R.
Venturi, Tiziana
Markevitch, Maxim
TI DISCOVERY OF A GIANT RADIO HALO IN A NEW PLANCK GALAXY CLUSTER
PLCKG171.9-40.7 (vol 766, pg 18, 2013)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
ID SUNYAEV-ZELDOVICH
C1 [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Giacintucci, Simona] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Kale, Ruta; Venturi, Tiziana] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Kale, Ruta] Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Wik, Daniel R.; Markevitch, Maxim] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Giacintucci, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM simona@astro.umd.edu
NR 5
TC 0
Z9 0
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR 161
DI 10.1088/0004-637X/770/2/161
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG2KE
UT WOS:000335244400007
ER
PT J
AU Schmelz, JT
Winebarger, AR
Kimble, JA
Pathak, S
Golub, L
Jenkins, BS
Worley, BT
AF Schmelz, J. T.
Winebarger, A. R.
Kimble, J. A.
Pathak, S.
Golub, L.
Jenkins, B. S.
Worley, B. T.
TI BRIGHT POINTS: MULTITHERMAL ANALYSIS AS A TEST OF STEADY HEATING MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: fundamental parameters; Sun: UV radiation
ID X-RAY TELESCOPE; EUV IMAGING SPECTROMETER; PLASMA FILLING FACTOR;
ACTIVE-REGION CORE; ATOMIC DATA; DENSITY-MEASUREMENTS; RATE
COEFFICIENTS; CORONAL-EXPLORER; EMISSION-MEASURE; MAGNETIC-FIELDS
AB X-ray bright points are small, million-degree features in the solar atmosphere composed of short coronal loops. They are magnetically driven structures associated with photospheric magnetic bipoles. Their relatively small size and simple structure suggest they are ideal candidates for comparisons with coronal heating models. In this paper, we present the analysis of 12 bright points using data from the EUV Imaging Spectrometer on Hinode and the Michelson Doppler Imager on Solar and Heliospheric Observatory. Using the spectroscopy data, we construct differential emission measure (DEM) curves, calculate the electron density, and find DEM-weighted temperatures. In addition, we determine the most likely ionization balance. Using the magnetic field observations, we complete potential field extrapolations of the magnetograms and estimate the loop lengths. Using this information, we construct models assuming the bright points are formed of hundreds of strands, each heated steadily and uniformly. We formulate the models so that the observed emission measure distribution is matched within a few percent. We then compare the densities determined from the models, (1.4-5.0) x 10(9), to those calculated from spectral data, (0.6-2.0) x 10(9). We find the majority of bright points do not agree with steady uniform heating models; instead they are underdense relative to their expected density by a factor of 0.16-0.82.
C1 [Schmelz, J. T.; Kimble, J. A.; Pathak, S.; Jenkins, B. S.; Worley, B. T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
[Winebarger, A. R.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
EM jschmelz@memphis.edu
FU Hinode subcontract from NASA/SAO; NSF [ATM-0402729]
FX The authors would like to thank Steve Saar of CfA and Jim Klimchuk of
GSFC for useful discussions on BPs. 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 the NSC (Norway). CHIANTI is a
collaborative project involving the NRL (USA), the Universities of
Florence (Italy) and Cambridge (UK), and George Mason University (USA).
Solar physics research at the University of Memphis is supported by a
Hinode subcontract from NASA/SAO as well as NSF ATM-0402729.
NR 51
TC 2
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR 160
DI 10.1088/0004-637X/770/2/160
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG2KE
UT WOS:000335244400006
ER
PT J
AU Seo, BJ
Nissly, C
Troy, M
Angeli, G
Bernier, R
Stepp, L
Williams, E
AF Seo, Byoung-Joon
Nissly, Carl
Troy, Mitchell
Angeli, George
Bernier, Robert
Stepp, Larry
Williams, Eric
TI Estimation of normalized point-source sensitivity of segment surface
specifications for extremely large telescopes
SO APPLIED OPTICS
LA English
DT Article
AB We present a method which estimates the normalized point-source sensitivity (PSSN) of a segmented telescope when only information from a single segment surface is known. The estimation principle is based on a statistical approach with an assumption that all segment surfaces have the same power spectral density (PSD) as the given segment surface. As presented in this paper, the PSSN based on this statistical approach represents a worst-case scenario among statistical random realizations of telescopes when all segment surfaces have the same PSD. Therefore, this method, which we call the vendor table, is expected to be useful for individual segment specification such as the segment polishing specification. The specification based on the vendor table can be directly related to a science metric such as PSSN and provides the mirror vendors significant flexibility by specifying a single overall PSSN value for them to meet. We build a vendor table for the Thirty Meter Telescope (TMT) and test it using multiple mirror samples from various mirror vendors to prove its practical utility. Accordingly, TMT has a plan to adopt this vendor table for its M1 segment final mirror polishing requirement. (C) 2013 Optical Society of America
C1 [Seo, Byoung-Joon; Nissly, Carl; Troy, Mitchell] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Seo, Byoung-Joon; Nissly, Carl; Troy, Mitchell] CALTECH, Pasadena, CA 91125 USA.
[Angeli, George; Bernier, Robert; Stepp, Larry; Williams, Eric] Thirty Meter Telescope Observ, Pasadena, CA 91107 USA.
RP Seo, BJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Byoung-Joon.Seo@jpl.nasa.gov
FU California Institute of Technology; National Aeronautics and Space
Administration; TMT partner institutions; Association of Canadian
Universities for Research in Astronomy (ACURA); University of
California; Gordon and Betty Moore Foundation; Canada Foundation for
Innovation; Ontario Ministry of Research and Innovation; National
Research Council of Canada; Natural Sciences and Engineering Research
Council of Canada; British Columbia Knowledge Development Fund;
Association of Universities for Research in Astronomy (AURA); U.S.
National Science Foundation
FX This research was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, and was sponsored by the California
Institute of Technology and the National Aeronautics and Space
Administration. The authors gratefully acknowledge the support of the
TMT partner institutions. They are the Association of Canadian
Universities for Research in Astronomy (ACURA), the California Institute
of Technology, and the University of California. This work was supported
as well by the Gordon and Betty Moore Foundation, the Canada Foundation
for Innovation, the Ontario Ministry of Research and Innovation, the
National Research Council of Canada, the Natural Sciences and
Engineering Research Council of Canada, the British Columbia Knowledge
Development Fund, the Association of Universities for Research in
Astronomy (AURA), and the U.S. National Science Foundation.
NR 12
TC 1
Z9 2
U1 1
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
J9 APPL OPTICS
JI Appl. Optics
PD JUN 20
PY 2013
VL 52
IS 18
BP 4111
EP 4122
DI 10.1364/AO.52.004111
PG 12
WC Optics
SC Optics
GA 168LX
UT WOS:000320708500005
PM 23842151
ER
PT J
AU Kane, SR
Barclay, T
Gelino, DM
AF Kane, Stephen R.
Barclay, Thomas
Gelino, Dawn M.
TI A POTENTIAL SUPER-VENUS IN THE KEPLER-69 SYSTEM
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrobiology; planetary systems; stars: individual (Kepler-69)
ID MAIN-SEQUENCE STARS; SUN-LIKE STAR; HABITABLE-ZONE; TRANSMISSION
SPECTRUM; PLANET; EARTH; CANDIDATES; EXOPLANET; TERRESTRIAL; RADIUS
AB Transiting planets have greatly expanded and diversified the exoplanet field. These planets provide greater access to characterization of exoplanet atmospheres and structure. The Kepler mission has been particularly successful in expanding the exoplanet inventory, even to planets smaller than the Earth. The orbital period sensitivity of the Kepler data is now extending into the habitable zones of their host stars, and several planets larger than the Earth have been found to lie therein. Here we examine one such proposed planet, Kepler-69c. We provide new orbital parameters for this planet and an in-depth analysis of the habitable zone. We find that, even under optimistic conditions, this 1.7 R-circle plus planet is unlikely to be within the habitable zone of Kepler-69. Furthermore, the planet receives an incident flux of 1.91 times the solar constant, which is similar to that received by Venus. We thus suggest that this planet is likely a super-Venus rather than a super-Earth in terms of atmospheric properties and habitability, and we propose follow-up observations to disentangle the ambiguity.
C1 [Kane, Stephen R.; Gelino, Dawn M.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kane, SR (reprint author), CALTECH, NASA, Exoplanet Sci Inst, MS 100-22,770 South Wilson Ave, Pasadena, CA 91125 USA.
EM skane@ipac.caltech.edu
NR 29
TC 12
Z9 13
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 JUN 20
PY 2013
VL 770
IS 2
AR L20
DI 10.1088/2041-8205/770/2/L20
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 168MJ
UT WOS:000320709900004
ER
PT J
AU Kennea, JA
Burrows, DN
Kouveliotou, C
Palmer, DM
Gogus, E
Kaneko, Y
Evans, PA
Degenaar, N
Reynolds, MT
Miller, JM
Wijnands, R
Mori, K
Gehrels, N
AF Kennea, J. A.
Burrows, D. N.
Kouveliotou, C.
Palmer, D. M.
Gogus, E.
Kaneko, Y.
Evans, P. A.
Degenaar, N.
Reynolds, M. T.
Miller, J. M.
Wijnands, R.
Mori, K.
Gehrels, N.
TI SWIFT DISCOVERY OF A NEW SOFT GAMMA REPEATER, SGR J1745-29, NEAR
SAGITTARIUS A*
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE pulsars: general; pulsars: individual (SGR J1745-29); stars: neutron;
X-rays: bursts
ID X-RAY PULSARS; GALACTIC-CENTER; TELESCOPE; BURSTS; GRBS
AB Starting in 2013 February, Swift has been performing short daily monitoring observations of the G2 gas cloud near Sgr A* with the X-Ray Telescope to determine whether the cloud interaction leads to an increase in the flux from the Galactic center. On 2013 April 24 Swift detected an order of magnitude rise in the X-ray flux from the region near Sgr A*. Initially thought to be a flare from Sgr A*, the detection of a short hard X-ray burst from the same region by the Burst Alert Telescope suggested that the flare was from an unresolved new Soft Gamma Repeater, SGR J1745-29. Here we present the discovery of SGR J1745-29 by Swift, including analysis of data before, during, and after the burst. We find that the spectrum in the 0.3-10 keV range is well fit by an absorbed blackbody model with kT(BB) similar or equal to 1 keV and absorption consistent with previously measured values from the quiescent emission from Sgr A*, strongly suggesting that this source is at a similar distance. Only one SGR burst has been detected so far from the new source, and the persistent light curve shows little evidence of decay in approximately two weeks of monitoring after outburst. We discuss this light curve trend and compare it with those of other well covered SGR outbursts. We suggest that SGR J1745-29 belongs to an emerging subclass of magnetars characterized by low burst rates and prolonged steady X-ray emission one to two weeks after outburst onset.
C1 [Kennea, J. A.; Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Sci & Technol Off, Huntsville, AL 35812 USA.
[Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Gogus, E.; Kaneko, Y.] Sabanci Univ, TR-34956 Istanbul, Turkey.
[Evans, P. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Degenaar, N.; Reynolds, M. T.; Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Mori, K.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Kennea, JA (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM kennea@swift.psu.edu
FU NASA grant through the Swift Guest Investigator Program [NAS5-00135]
FX This work was supported by NASA grant NAS5-00135 through the Swift Guest
Investigator Program. This work made use of data supplied by the UK
Swift Science Data Centre at the University of Leicester. We acknowledge
the use of public data from the Swift data archive. This research has
made use of the XRT Data Analysis Software (XRTDAS) developed under the
responsibility of the ASI Science Data Center (ASDC), Italy.
NR 39
TC 45
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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 JUN 20
PY 2013
VL 770
IS 2
AR L24
DI 10.1088/2041-8205/770/2/L24
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 168MJ
UT WOS:000320709900008
ER
PT J
AU Mori, K
Gotthelf, EV
Zhang, S
An, HJ
Baganoff, FK
Barriere, NM
Beloborodov, AM
Boggs, SE
Christensen, FE
Craig, WW
Dufour, F
Grefenstette, BW
Hailey, CJ
Harrison, FA
Hong, J
Kaspi, VM
Kennea, JA
Madsen, KK
Markwardt, CB
Nynka, M
Stern, D
Tomsick, JA
Zhang, WW
AF Mori, Kaya
Gotthelf, Eric V.
Zhang, Shuo
An, Hongjun
Baganoff, Frederick K.
Barriere, Nicolas M.
Beloborodov, Andrei M.
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Dufour, Francois
Grefenstette, Brian W.
Hailey, Charles J.
Harrison, Fiona A.
Hong, Jaesub
Kaspi, Victoria M.
Kennea, Jamie A.
Madsen, Kristin K.
Markwardt, Craig B.
Nynka, Melania
Stern, Daniel
Tomsick, John A.
Zhang, William W.
TI NuSTAR DISCOVERY OF A 3.76 s TRANSIENT MAGNETAR NEAR SAGITTARIUS A*
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Galaxy: center; pulsars: general; pulsars: individual (SGR J1745-29);
stars: neutron
ID X-RAY PULSARS; SOFT GAMMA-REPEATERS; GALACTIC-CENTER; NEUTRON-STARS;
RADIO PULSATIONS; EMISSION; OUTBURST; TELESCOPE; MECHANISM; DISK
AB We report the discovery of 3.76 s pulsations from a new burst source near Sgr A* observed by the NuSTAR observatory. The strong signal from SGR J1745-29 presents a complex pulse profile modulated with pulsed fraction 27% +/- 3% in the 3-10 keV band. Two observations spaced nine days apart yield a spin-down rate of (P) over dot = (6.5 +/- 1.4) x 10(-12). This implies a magnetic field B = 1.6 x 10(14) G, spin-down power (E) over dot = 5 x 10(33) erg s(-1), and characteristic age P/2(P) over dot = 9 x 10(3) yr for the rotating dipole model. However, the current (P) over dot may be erratic, especially during outburst. The flux and modulation remained steady during the observations and the 3-79 keV spectrum is well fitted by a combined blackbody plus power-law model with temperature kT(BB) = 0.96 +/- 0.02 keV and photon index Gamma = 1.5 +/- 0.4. The neutral hydrogen column density (N-H similar to 1.4 x 10(23) cm(-2)) measured by NuSTAR and Swift suggests that SGR J1745-29 is located at or near the Galactic center. The lack of an X-ray counterpart in the published Chandra survey catalog sets a quiescent 2-8 keV luminosity limit of Lx less than or similar to 10(32) erg s(-1). The bursting, timing, and spectral properties indicate a transient magnetar undergoing an outburst with 2-79 keV luminosity up to 3.5 x 10(35) erg s(-1) for a distance of 8 kpc. SGR J1745-29 joins a growing subclass of transient magnetars, indicating that many magnetars in quiescence remain undetected in the X-ray band or have been detected as high-B radio pulsars. The peculiar location of SGR J1745-29 has important implications for the formation and dynamics of neutron stars in the Galactic center region.
C1 [Mori, Kaya; Gotthelf, Eric V.; Zhang, Shuo; Beloborodov, Andrei M.; Hailey, Charles J.; Nynka, Melania] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[An, Hongjun; Dufour, Francois; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Barriere, Nicolas M.; Boggs, Steven E.; Craig, William W.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hong, Jaesub] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kennea, Jamie A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Markwardt, Craig B.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mori, K (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
EM kaya@astro.columbia.edu
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Madsen, Kristin/0000-0003-1252-4891
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration
FX This work was supported under NASA Contract No. NNG08FD60C, and made use
of data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration. The authors
thank Arash Bodaghee and Clio Sleator for their assistance with data
analysis and Brian Metzger for helpful discussions.
NR 47
TC 68
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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 JUN 20
PY 2013
VL 770
IS 2
AR L23
DI 10.1088/2041-8205/770/2/L23
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 168MJ
UT WOS:000320709900007
ER
PT J
AU Whitaker, KE
van Dokkum, PG
Brammer, G
Momcheva, IG
Skelton, R
Franx, M
Kriek, M
Labbe, I
Fumagalli, M
Lundgren, BF
Nelson, EJ
Patel, SG
Rix, HW
AF Whitaker, Katherine E.
van Dokkum, Pieter G.
Brammer, Gabriel
Momcheva, Ivelina G.
Skelton, Rosalind
Franx, Marijn
Kriek, Mariska
Labbe, Ivo
Fumagalli, Mattia
Lundgren, Britt F.
Nelson, Erica J.
Patel, Shannon G.
Rix, Hans-Walter
TI QUIESCENT GALAXIES IN THE 3D-HST SURVEY: SPECTROSCOPIC CONFIRMATION OF A
LARGE NUMBER OF GALAXIES WITH RELATIVELY OLD STELLAR POPULATIONS AT z
similar to 2
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift
ID HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; RED-SEQUENCE;
ABSORPTION-LINE; DEEP-FIELD; MASS-SIZE; X-RAY; EVOLUTION; AGN;
Z-SIMILAR-TO-2.3
AB Quiescent galaxies at z similar to 2 have been identified in large numbers based on rest-frame colors, but only a small number of these galaxies have been spectroscopically confirmed to show that their rest-frame optical spectra show either strong Balmer or metal absorption lines. Here, we median stack the rest-frame optical spectra for 171 photometrically quiescent galaxies at 1.4 < z < 2.2 from the 3D-HST grism survey. In addition to H beta (lambda 4861 angstrom), we unambiguously identify metal absorption lines in the stacked spectrum, including the G band (lambda 4304 angstrom), Mg I (lambda 5175 angstrom), and Na I (lambda 5894 angstrom). This finding demonstrates that galaxies with relatively old stellar populations already existed when the universe was similar to 3 Gyr old, and that rest-frame color selection techniques can efficiently select them. We find an average age of 1.3(-0.3)(+0.1) Gyr when fitting a simple stellar population to the entire stack. We confirm our previous result from medium-band photometry that the stellar age varies with the colors of quiescent galaxies: the reddest 80% of galaxies are dominated by metal lines and have a relatively old mean age of 1.6(-0.4)(+0.5) Gyr, whereas the bluest (and brightest) galaxies have strong Balmer lines and a spectroscopic age of 0.9(-0.1)(+0.2) Gyr. Although the spectrum is dominated by an evolved stellar population, we also find [O III] and H beta emission. Interestingly, this emission is more centrally concentrated than the continuum with L-OIII = 1.7 +/- 0.3 x 10(40) erg s(-1), indicating residual central star formation or nuclear activity.
C1 [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[van Dokkum, Pieter G.; Momcheva, Ivelina G.; Skelton, Rosalind; Nelson, Erica J.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Brammer, Gabriel] European So Observ, Santiago 19001, Chile.
[Franx, Marijn; Labbe, Ivo; Fumagalli, Mattia; Patel, Shannon G.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[Kriek, Mariska] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Lundgren, Britt F.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Whitaker, KE (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
EM kate.whitaker@nasa.gov
FU NASA; STScI grant [GO-12177]; NASA ADAP grant [NNX11AB08G]
FX We sincerely thank the referee for the thorough review of the
manuscript. 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. Support
from STScI grant GO-12177 and NASA ADAP grant NNX11AB08G is gratefully
acknowledged.
NR 34
TC 42
Z9 42
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 JUN 20
PY 2013
VL 770
IS 2
AR L39
DI 10.1088/2041-8205/770/2/L39
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 168MJ
UT WOS:000320709900023
ER
PT J
AU Fu, H
Cooray, A
Feruglio, C
Ivison, RJ
Riechers, DA
Gurwell, M
Bussmann, RS
Harris, AI
Altieri, B
Aussel, H
Baker, AJ
Bock, J
Boylan-Kolchin, M
Bridge, C
Calanog, JA
Casey, CM
Cava, A
Chapman, SC
Clements, DL
Conley, A
Cox, P
Farrah, D
Frayer, D
Hopwood, R
Jia, J
Magdis, G
Marsden, G
Martinez-Navajas, P
Negrello, M
Neri, R
Oliver, SJ
Omont, A
Page, MJ
Perez-Fournon, I
Schulz, B
Scott, D
Smith, A
Vaccari, M
Valtchanov, I
Vieira, JD
Viero, M
Wang, L
Wardlow, JL
Zemcov, M
AF Fu, Hai
Cooray, Asantha
Feruglio, C.
Ivison, R. J.
Riechers, D. A.
Gurwell, M.
Bussmann, R. S.
Harris, A. I.
Altieri, B.
Aussel, H.
Baker, A. J.
Bock, J.
Boylan-Kolchin, M.
Bridge, C.
Calanog, J. A.
Casey, C. M.
Cava, A.
Chapman, S. C.
Clements, D. L.
Conley, A.
Cox, P.
Farrah, D.
Frayer, D.
Hopwood, R.
Jia, J.
Magdis, G.
Marsden, G.
Martinez-Navajas, P.
Negrello, M.
Neri, R.
Oliver, S. J.
Omont, A.
Page, M. J.
Perez-Fournon, I.
Schulz, B.
Scott, D.
Smith, A.
Vaccari, M.
Valtchanov, I.
Vieira, J. D.
Viero, M.
Wang, L.
Wardlow, J. L.
Zemcov, M.
TI The rapid assembly of an elliptical galaxy of 400 billion solar masses
at a redshift of 2.3
SO NATURE
LA English
DT Article
ID STAR-FORMING GALAXIES; H-2 CONVERSION FACTOR; SUBMILLIMETER GALAXIES;
MOLECULAR GAS; MODEL; SIMULATIONS; EMISSION; MERGERS; HERMES; GROWTH
AB Stellar archaeology(1) shows that massive elliptical galaxies formed rapidly about ten billion years ago with star-formation rates of above several hundred solar masses per year. Their progenitors are probably the submillimetre bright galaxies(2) at redshifts z greater than 2. Although the mean molecular gas mass(3) (5 x 10(10) solar masses) of the submillimetre bright galaxies can explain the formation of typical elliptical galaxies, it is inadequate to form elliptical galaxies(4) that already have stellar masses above 2 x 10(11) solar masses at z approximate to 2. Here we report multi-wavelength high-resolution observations of a rare merger of two massive submillimetre bright galaxies at z approximate to 2.3. The system is seen to be forming stars at a rate of 2,000 solar masses per year. The star-formation efficiency is an order of magnitude greater than that of normal galaxies, so the gas reservoir will be exhausted and star formation will be quenched in only around 200 million years. At a projected separation of 19 kiloparsecs, the two massive starbursts are about to merge and form a passive elliptical galaxy with a stellar mass of about 4 x 10(11) solar masses. We conclude that gas-rich major galaxy mergers with intense star formation can form the most massive elliptical galaxies by z approximate to 1.5.
C1 [Fu, Hai; Cooray, Asantha; Boylan-Kolchin, M.; Calanog, J. A.; Jia, J.; Wardlow, J. L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Feruglio, C.; Cox, P.; Neri, R.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
[Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Riechers, D. A.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Gurwell, M.; Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Altieri, B.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain.
[Aussel, H.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA Saclay, CEA,DSM,Irfu,SAp,CNRS, F-91191 Gif Sur Yvette, France.
[Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, J.; Bridge, C.; Vieira, J. D.; Viero, M.] CALTECH, Pasadena, CA 91125 USA.
[Casey, C. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Cava, A.] Univ Complutense Madrid, Fac Ciencias Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
[Clements, D. L.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Marsden, G.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Martinez-Navajas, P.; Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Martinez-Navajas, P.; Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Negrello, M.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Oliver, S. J.; Smith, A.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Omont, A.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Schulz, B.] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa.
RP Fu, H (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
EM haif@uci.edu; acooray@uci.edu
RI Magdis, Georgios/C-7295-2014; Wardlow, Julie/C-9903-2015; Ivison,
R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017;
OI Magdis, Georgios/0000-0002-4872-2294; Wardlow,
Julie/0000-0003-2376-8971; Boylan-Kolchin, Michael/0000-0002-9604-343X;
Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577;
Cava, Antonio/0000-0002-4821-1275; Scott, Douglas/0000-0002-6878-9840;
Casey, Caitlin/0000-0002-0930-6466; Altieri, Bruno/0000-0003-3936-0284
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA)
FX Herschel is an ESA space observatory with science instruments provided
by European-led Principal Investigator consortia and with important
participation from NASA. This research has made use of data from the
HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key
Programme using Guaranteed Time from the SPIRE instrument team, ESAC
scientists and a mission scientist. 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, IPAC and the University of
Colorado (USA). This development has been supported by the following
national funding agencies: CSA (Canada); NAOC (China); CEA, CNES and
CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and
NASA (USA). The data presented in this paper will be released through
the HeDaM Database in Marseille at http://hedam.oamp.fr/HerMES.
NR 30
TC 53
Z9 53
U1 1
U2 18
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUN 20
PY 2013
VL 498
IS 7454
BP 338
EP 341
DI 10.1038/nature12184
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 166XI
UT WOS:000320592900034
PM 23698363
ER
PT J
AU Aliu, E
Archambault, S
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bird, R
Bouvier, A
Bradbury, SM
Buckley, JH
Bugaev, V
Byrum, K
Cannon, A
Cesarini, A
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickherber, R
Duke, C
Dumm, J
Dwarkadas, VV
Errando, M
Falcone, A
Federici, S
Feng, Q
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gillanders, GH
Godambe, S
Gotthelf, EV
Griffin, S
Grube, J
Gyuk, G
Hanna, D
Holder, J
Huan, H
Hughes, G
Humensky, TB
Kaaret, P
Karlsson, N
Kertzman, M
Khassen, Y
Kieda, D
Krawczynski, H
Krennrich, F
Lang, MJ
Lee, K
Madhavan, AS
Maier, G
Majumdar, P
McArthur, S
McCann, A
Millis, J
Moriarty, P
Mukherjee, R
Nelson, T
de Bhroithe, AO
Ong, RA
Orr, M
Otte, AN
Pandel, D
Park, N
Perkins, JS
Pohl, M
Popkow, A
Prokoph, H
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Ruppel, J
Saxon, DB
Schroedter, M
Sembroski, GH
Senturk, GD
Skole, C
Telezhinsky, I
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Tyler, J
Varlotta, A
Vassiliev, VV
Vincent, S
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Weisgarber, T
Welsing, R
Williams, DA
Zitzer, B
AF Aliu, E.
Archambault, S.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Bird, R.
Bouvier, A.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cannon, A.
Cesarini, A.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickherber, R.
Duke, C.
Dumm, J.
Dwarkadas, V. V.
Errando, M.
Falcone, A.
Federici, S.
Feng, Q.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gillanders, G. H.
Godambe, S.
Gotthelf, E. V.
Griffin, S.
Grube, J.
Gyuk, G.
Hanna, D.
Holder, J.
Huan, H.
Hughes, G.
Humensky, T. B.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
Lee, K.
Madhavan, A. S.
Maier, G.
Majumdar, P.
McArthur, S.
McCann, A.
Millis, J.
Moriarty, P.
Mukherjee, R.
Nelson, T.
de Bhroithe, A. O'Faolain
Ong, R. A.
Orr, M.
Otte, A. N.
Pandel, D.
Park, N.
Perkins, J. S.
Pohl, M.
Popkow, A.
Prokoph, H.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Ruppel, J.
Saxon, D. B.
Schroedter, M.
Sembroski, G. H.
Sentuerk, G. D.
Skole, C.
Telezhinsky, I.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Tyler, J.
Varlotta, A.
Vassiliev, V. V.
Vincent, S.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
Weisgarber, T.
Welsing, R.
Williams, D. A.
Zitzer, B.
TI DISCOVERY OF TeV GAMMA-RAY EMISSION TOWARD SUPERNOVA REMNANT SNR
G78.2+2.1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; cosmic rays; gamma rays: general; ISM:
supernova remnants
ID PARTICLE-ACCELERATION; FERMI; HESS; SEARCH; COUNTERPART; 2CG078+2;
CATALOG; ORIGIN
AB We report the discovery of an unidentified, extended source of very-high-energy gamma-ray emission, VER J2019+407, within the radio shell of the supernova remnant SNR G78.2+2.1, using 21.4 hr of data taken by the VERITAS gamma-ray observatory in 2009. These data confirm the preliminary indications of gamma-ray emission previously seen in a two-year (2007-2009) blind survey of the Cygnus region by VERITAS. VER J2019+407, which is detected at a post-trials significance of 7.5 standard deviations in the 2009 data, is localized to the northwestern rim of the remnant in a region of enhanced radio and X-ray emission. It has an intrinsic extent of 0 degrees.23 +/- 0 degrees.03(stat-0 degrees.02sys)(+0 degrees.04) and its spectrum is well-characterized by a differential power law (dN/dE = N-0 x (E/TeV)-Gamma) with a photon index of Gamma = 2.37 +/- 0.14(stat) +/- 0.20(sys) and a flux normalization of N-0 = 1.5 +/- 0.2(stat) +/- 0.4(sys) x 10(-12) photon TeV-1 cm(-2) s(-1). This yields an integral flux of 5.2 +/- 0.8(stat) +/- 1.4(sys) x 10(-12) photon cm(-2) s(-1) above 320 GeV, corresponding to 3.7% of the Crab Nebula flux. We consider the relationship of the TeV gamma-ray emission with the GeV gamma-ray emission seen from SNR G78.2+2.1 as well as that seen from a nearby cocoon of freshly accelerated cosmic rays. Multiple scenarios are considered as possible origins for the TeV gamma-ray emission, including hadronic particle acceleration at the SNR shock.
C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Tesic, G.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Arlen, T.; Aune, T.; Majumdar, P.; Ong, R. A.; Popkow, 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.; Thibadeau, S.; Ward, J. E.] 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.
[Bird, R.; Cannon, A.; Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Byrum, K.; 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.
[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.
[Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 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.; Vincent, S.; 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.] 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.
[Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Holder, J.; Saxon, D. B.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Saxon, D. B.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Huan, H.; McArthur, S.; Park, N.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Humensky, T. B.; Sentuerk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India.
[McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 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.
[Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA.
[Perkins, J. S.] NASA GSFC, 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.
RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
EM amandajw@iastate.edu
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;
Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201; Bird,
Ralph/0000-0002-4596-8563
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]; Science and Technology Facilities Council
in the UK; NASA [NNX11A086G]
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 the Science Foundation
Ireland (SFI 10/RFP/AST2748) and by the Science and Technology
Facilities Council 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. Dr. Weinstein and Dr. Dwarkadas' research was also supported
in part by NASA grant NNX11A086G.
NR 35
TC 17
Z9 17
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 JUN 20
PY 2013
VL 770
IS 2
AR 93
DI 10.1088/0004-637X/770/2/93
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200011
ER
PT J
AU Bodenheimer, P
D'Angelo, G
Lissauer, JJ
Fortney, JJ
Saumon, D
AF Bodenheimer, Peter
D'Angelo, Gennaro
Lissauer, Jack J.
Fortney, Jonathan J.
Saumon, Didier
TI DEUTERIUM BURNING IN MASSIVE GIANT PLANETS AND LOW-MASS BROWN DWARFS
FORMED BY CORE-NUCLEATED ACCRETION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; brown dwarfs; planets and satellites:
formation; planets and satellites: individual (beta Pictoris b); planets
and satellites: physical evolution
ID PROTOPLANETARY ATMOSPHERES; BETA-PICTORIS; HR 8799; EVOLUTION; JUPITER;
MODELS; OPACITIES; GRAINS; DISKS; GAS
AB Using detailed numerical simulations, we study the formation of bodies near the deuterium-burning limit according to the core-nucleated giant planet accretion scenario. The objects, with heavy-element cores in the range 5-30 M-circle plus, are assumed to accrete gas up to final masses of 10-15 Jupiter masses (M-Jup). After the formation process, which lasts 1-5 Myr and which ends with a "cold-start," low-entropy configuration, the bodies evolve at constant mass up to an age of several Gyr. Deuterium burning via proton capture is included in the calculation, and we determined the mass, M-50, above which more than 50% of the initial deuterium is burned. This often-quoted borderline between giant planets and brown dwarfs is found to depend only slightly on parameters, such as core mass, stellar mass, formation location, solid surface density in the protoplanetary disk, disk viscosity, and dust opacity. The values for M-50 fall in the range 11.6-13.6 M-Jup, in agreement with previous determinations that do not take the formation process into account. For a given opacity law during the formation process, objects with higher core masses form more quickly. The result is higher entropy in the envelope at the completion of accretion, yielding lower values of M-50. For masses above M-50, during the deuterium-burning phase, objects expand and increase in luminosity by one to three orders of magnitude. Evolutionary tracks in the luminosity versus time diagram are compared with the observed position of the companion to Beta Pictoris.
C1 [Bodenheimer, Peter] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[D'Angelo, Gennaro; Lissauer, Jack J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[D'Angelo, Gennaro] SETI Inst, Mountain View, CA 94043 USA.
RP Bodenheimer, P (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
EM peter@ucolick.org; gennaro.dangelo@nasa.gov; Jack.J.Lissauer@nasa.gov;
jfortney@ucolick.org; dsaumon@lanl.gov
RI D'Angelo, Gennaro/L-7676-2014;
OI D'Angelo, Gennaro/0000-0002-2064-0801; Fortney,
Jonathan/0000-0002-9843-4354
FU NASA [NNX11AK54G, NNX11AD20G, NNH11AQ54I, NNH12AT89I]; NSF [AST0908807]
FX Primary funding for this project was provided by the NASA Origins of
Solar Systems Program grant NNX11AK54G (P.B., G.D., J.L.). G.D.
acknowledges additional support from NASA grant NNX11AD20G. P.B.
acknowledges additional support from NSF grant AST0908807. D.S. is
supported in part by NASA grants NNH11AQ54I and NNH12AT89I. The authors
are indebted to Gilles Chabrier for the use of his nuclear screening
factors. The 3D hydrodynamical simulations reported in this work were
performed using resources provided by the NASA High-End Computing (HEC)
Program through the NASA Advanced Supercomputing (NAS) Division at Ames
Research Center. G.D. thanks Los Alamos National Laboratory for its
hospitality. The authors thank the referee Dr. Christoph Mordasini for a
detailed and constructive review.
NR 54
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR 120
DI 10.1088/0004-637X/770/2/120
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200038
ER
PT J
AU Chapman, NL
Davidson, JA
Goldsmith, PF
Houde, M
Kwon, W
Li, ZY
Looney, LW
Matthews, B
Matthews, TG
Novak, G
Peng, RS
Vaillancourt, JE
Volgenau, NH
AF Chapman, Nicholas L.
Davidson, Jacqueline A.
Goldsmith, Paul F.
Houde, Martin
Kwon, Woojin
Li, Zhi-Yun
Looney, Leslie W.
Matthews, Brenda
Matthews, Tristan G.
Novak, Giles
Peng, Ruisheng
Vaillancourt, John E.
Volgenau, Nikolaus H.
TI ALIGNMENT BETWEEN FLATTENED PROTOSTELLAR INFALL ENVELOPES AND AMBIENT
MAGNETIC FIELDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: jets and outflows; ISM: magnetic fields; stars: formation;
techniques: polarimetric
ID 2-DIMENSIONAL RADIATIVE-TRANSFER; SINGULAR ISOTHERMAL TOROIDS; MOLECULAR
CLOUD CORES; SMALL-SCALE STRUCTURE; CLASS 0 PROTOSTARS; STAR-FORMATION;
BOK GLOBULES; INTERSTELLAR CLOUDS; YOUNG STARS; SHARC-II
AB We present 350 mu m polarization observations of four low-mass cores containing Class 0 protostars: L483, L1157, L1448-IRS2, and Serp-FIR1. This is the second paper in a larger survey aimed at testing magnetically regulated models for core-collapse. One key prediction of these models is that the mean magnetic field in a core should be aligned with the symmetry axis (minor axis) of the flattened young stellar object inner envelope (aka pseudodisk). Furthermore, the field should exhibit a pinched or hourglass-shaped morphology as gravity drags the field inward toward the central protostar. We combine our results for the four cores with results for three similar cores that were published in the first paper from our survey. An analysis of the 350 mu m polarization data for the seven cores yields evidence of a positive correlation between mean field direction and pseudodisk symmetry axis. Our rough estimate for the probability of obtaining by pure chance a correlation as strong as the one we found is about 5%. In addition, we combine together data for multiple cores to create a source-averaged magnetic field map having improved signal-to-noise ratio, and this map shows good agreement between mean field direction and pseudodisk axis (they are within 15 degrees). We also see hints of a magnetic pinch in the source-averaged map. We conclude that core-scale magnetic fields appear to be strong enough to guide gas infall, as predicted by the magnetically regulated models. Finally, we find evidence of a positive correlation between core magnetic field direction and bipolar outflow axis.
C1 [Chapman, Nicholas L.; Matthews, Tristan G.; Novak, Giles] Northwestern Univ, CIERA, Evanston, IL 60208 USA.
[Chapman, Nicholas L.; Matthews, Tristan G.; Novak, Giles] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Davidson, Jacqueline A.] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia.
[Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada.
[Houde, Martin] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Kwon, Woojin; Looney, Leslie W.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Kwon, Woojin] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands.
[Li, Zhi-Yun] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Matthews, Brenda] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Matthews, Brenda] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada.
[Peng, Ruisheng] Caltech Submillimeter Observ, Hilo, HI 96720 USA.
[Vaillancourt, John E.] NASA, Ames Res Ctr, Univ Space Res Assoc, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Volgenau, Nikolaus H.] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA.
RP Chapman, NL (reprint author), Northwestern Univ, CIERA, 2145 Sheridan Rd, Evanston, IL 60208 USA.
RI Goldsmith, Paul/H-3159-2016
FU National Science Foundation [AST-0838261, AST-0909030]; NASA
FX We thank the anonymous referee for providing useful feedback that
improved the statistical analysis in this paper. This material is based
upon work at the Caltech Submillimeter Observatory, which is operated by
the California Institute of Technology under cooperative agreement with
the National Science Foundation (AST-0838261). This research was carried
out in part at the Jet Propulsion Laboratory, which is operated by the
California Institute of Technology under contract with NASA. We are
grateful to the National Science Foundation for supporting the operation
of SHARP via grant AST-0909030. N.L.C. is also supported under this
grant.
NR 71
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR 151
DI 10.1088/0004-637X/770/2/151
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200069
ER
PT J
AU Harrison, FA
Craig, WW
Christensen, FE
Hailey, CJ
Zhang, WW
Boggs, SE
Stern, D
Cook, WR
Forster, K
Giommi, P
Grefenstette, BW
Kim, Y
Kitaguchi, T
Koglin, JE
Madsen, KK
Mao, PH
Miyasaka, H
Mori, K
Perri, M
Pivovaroff, MJ
Puccetti, S
Rana, VR
Westergaard, NJ
Willis, J
Zoglauer, A
An, HJ
Bachetti, M
Barriere, NM
Bellm, EC
Bhalerao, V
Brejnholt, NF
Fuerst, F
Liebe, CC
Markwardt, CB
Nynka, M
Vogel, JK
Walton, DJ
Wik, DR
Alexander, DM
Cominsky, LR
Hornschemeier, AE
Hornstrup, A
Kaspi, VM
Madejski, GM
Matt, G
Molendi, S
Smith, DM
Tomsick, JA
Ajello, M
Ballantyne, DR
Balokovic, M
Barret, D
Bauer, FE
Blandford, RD
Brandt, WN
Brenneman, LW
Chiang, J
Chakrabarty, D
Chenevez, J
Comastri, A
Dufour, F
Elvis, M
Fabian, AC
Farrah, D
Fryer, CL
Gotthelf, EV
Grindlay, JE
Helfand, DJ
Krivonos, R
Meier, DL
Miller, JM
Natalucci, L
Ogle, P
Ofek, EO
Ptak, A
Reynolds, SP
Rigby, JR
Tagliaferri, G
Thorsett, SE
Treister, E
Urry, CM
AF Harrison, Fiona A.
Craig, William W.
Christensen, Finn E.
Hailey, Charles J.
Zhang, William W.
Boggs, Steven E.
Stern, Daniel
Cook, W. Rick
Forster, Karl
Giommi, Paolo
Grefenstette, Brian W.
Kim, Yunjin
Kitaguchi, Takao
Koglin, Jason E.
Madsen, Kristin K.
Mao, Peter H.
Miyasaka, Hiromasa
Mori, Kaya
Perri, Matteo
Pivovaroff, Michael J.
Puccetti, Simonetta
Rana, Vikram R.
Westergaard, Niels J.
Willis, Jason
Zoglauer, Andreas
An, Hongjun
Bachetti, Matteo
Barriere, Nicolas M.
Bellm, Eric C.
Bhalerao, Varun
Brejnholt, Nicolai F.
Fuerst, Felix
Liebe, Carl C.
Markwardt, Craig B.
Nynka, Melania
Vogel, Julia K.
Walton, Dominic J.
Wik, Daniel R.
Alexander, David M.
Cominsky, Lynn R.
Hornschemeier, Ann E.
Hornstrup, Allan
Kaspi, Victoria M.
Madejski, Greg M.
Matt, Giorgio
Molendi, Silvano
Smith, David M.
Tomsick, John A.
Ajello, Marco
Ballantyne, David R.
Balokovic, Mislav
Barret, Didier
Bauer, Franz E.
Blandford, Roger D.
Brandt, W. Niel
Brenneman, Laura W.
Chiang, James
Chakrabarty, Deepto
Chenevez, Jerome
Comastri, Andrea
Dufour, Francois
Elvis, Martin
Fabian, Andrew C.
Farrah, Duncan
Fryer, Chris L.
Gotthelf, Eric V.
Grindlay, Jonathan E.
Helfand, David J.
Krivonos, Roman
Meier, David L.
Miller, Jon M.
Natalucci, Lorenzo
Ogle, Patrick
Ofek, Eran O.
Ptak, Andrew
Reynolds, Stephen P.
Rigby, Jane R.
Tagliaferri, Gianpiero
Thorsett, Stephen E.
Treister, Ezequiel
Urry, C. Megan
TI THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY
MISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE space vehicles: instruments; X-rays: general
ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLE; DEEP FIELD-SOUTH;
SUPERNOVA REMNANT G1.9+0.3; SOFT GAMMA-REPEATERS; MS SOURCE CATALOGS;
BROAD IRON LINES; XMM-NEWTON; ASCA OBSERVATIONS; NEUTRON-STAR
AB The Nuclear Spectroscopic Telescope Array (NuSTAR) mission, launched on 2012 June 13, is the first focusing high-energy X-ray telescope in orbit. NuSTAR operates in the band from 3 to 79 keV, extending the sensitivity of focusing far beyond the similar to 10 keV high-energy cutoff achieved by all previous X-ray satellites. The inherently low background associated with concentrating the X-ray light enables NuSTAR to probe the hard X-ray sky with a more than 100-fold improvement in sensitivity over the collimated or coded mask instruments that have operated in this bandpass. Using its unprecedented combination of sensitivity and spatial and spectral resolution, NuSTAR will pursue five primary scientific objectives: (1) probe obscured active galactic nucleus (AGN) activity out to the peak epoch of galaxy assembly in the universe (at z less than or similar to 2) by surveying selected regions of the sky; (2) study the population of hard X-ray-emitting compact objects in the Galaxy by mapping the central regions of the Milky Way; (3) study the non-thermal radiation in young supernova remnants, both the hard X-ray continuum and the emission from the radioactive element Ti-44; (4) observe blazars contemporaneously with ground-based radio, optical, and TeV telescopes, as well as with Fermi and Swift, to constrain the structure of AGN jets; and (5) observe line and continuum emission from core-collapse supernovae in the Local Group, and from nearby Type Ia events, to constrain explosion models. During its baseline two-year mission, NuSTAR will also undertake a broad program of targeted observations. The observatory consists of two co-aligned grazing-incidence X-ray telescopes pointed at celestial targets by a three-axis stabilized spacecraft. Deployed into a 600 km, near-circular, 6 degrees inclination orbit, the observatory has now completed commissioning, and is performing consistent with pre-launch expectations. NuSTAR is now executing its primary science mission, and with an expected orbit lifetime of 10 yr, we anticipate proposing a guest investigator program, to begin in late 2014.
C1 [Harrison, Fiona A.; Cook, W. Rick; Forster, Karl; Grefenstette, Brian W.; Madsen, Kristin K.; Mao, Peter H.; Miyasaka, Hiromasa; Rana, Vikram R.; Bellm, Eric C.; Bhalerao, Varun; Fuerst, Felix; Walton, Dominic J.; Balokovic, Mislav] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Craig, William W.; Pivovaroff, Michael J.; Vogel, Julia K.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Craig, William W.; Boggs, Steven E.; Zoglauer, Andreas; Barriere, Nicolas M.; Tomsick, John A.; Ajello, Marco; Krivonos, Roman] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, Finn E.; Westergaard, Niels J.; Brejnholt, Nicolai F.; Hornstrup, Allan; Chenevez, Jerome] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark.
[Hailey, Charles J.; Koglin, Jason E.; Mori, Kaya; Nynka, Melania; Gotthelf, Eric V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Zhang, William W.; Markwardt, Craig B.; Wik, Daniel R.; Hornschemeier, Ann E.; Ptak, Andrew; Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stern, Daniel; Kim, Yunjin; Willis, Jason; Liebe, Carl C.; Meier, David L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Giommi, Paolo; Perri, Matteo; Puccetti, Simonetta] ESRIN, ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Kitaguchi, Takao] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Koglin, Jason E.; Madejski, Greg M.] RIKEN, Wako, Saitama 3510198, Japan.
[Perri, Matteo; Puccetti, Simonetta; Blandford, Roger D.; Chiang, James] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[An, Hongjun; Kaspi, Victoria M.; Dufour, Francois] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Bachetti, Matteo; Barret, Didier] Univ Toulouse, IRAP, UPS OMP, Toulouse, France.
[Bachetti, Matteo; Barret, Didier] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
[Bhalerao, Varun] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Alexander, David M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Cominsky, Lynn R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA.
[Matt, Giorgio] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Molendi, Silvano] INAF, IASF Milano, I-20133 Milan, Italy.
[Smith, David M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Smith, David M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Ballantyne, David R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Bauer, Franz E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Brandt, W. Niel] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Brandt, W. Niel] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brenneman, Laura W.; Elvis, Martin; Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Comastri, Andrea] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Farrah, Duncan] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Fryer, Chris L.] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA.
[Helfand, David J.] Quest Univ Canada, Squamish, BC V8B 0N8, Canada.
[Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Natalucci, Lorenzo] INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
[Ogle, Patrick] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Ofek, Eran O.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Reynolds, Stephen P.] NC State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Tagliaferri, Gianpiero] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Thorsett, Stephen E.] Willamette Univ, Dept Phys, Salem, OR 97301 USA.
[Treister, Ezequiel] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Urry, C. Megan] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Urry, C. Megan] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
RP Harrison, FA (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
EM fiona@srl.caltech.edu
RI Urry, Claudia/G-7381-2011; Rigby, Jane/D-4588-2012; Pivovaroff,
Michael/M-7998-2014; Boggs, Steven/E-4170-2015; Brandt,
William/N-2844-2015; Comastri, Andrea/O-9543-2015;
OI Bachetti, Matteo/0000-0002-4576-9337; Rana, Vikram/0000-0003-1703-8796;
Alexander, David/0000-0002-5896-6313; Molendi,
Silvano/0000-0002-2483-278X; Tagliaferri, Gianpiero/0000-0003-0121-0723;
Puccetti, Simonetta/0000-0002-2734-7835; Urry,
Claudia/0000-0002-0745-9792; Rigby, Jane/0000-0002-7627-6551;
Pivovaroff, Michael/0000-0001-6780-6816; Boggs,
Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453;
Comastri, Andrea/0000-0003-3451-9970; Thorsett,
Stephen/0000-0002-2025-9613; giommi, paolo/0000-0002-2265-5003;
Bhalerao, Varun/0000-0002-6112-7609; Perri, Matteo/0000-0003-3613-4409
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
National Space Institute, Technical University of Denmark; Italian Space
Agency (ASI); Centre National d'Etudes Spatiales (CNES); NASA
Postdoctoral Program; Leverhulme Research Fellowship; U.S. DOE/LLNL;
NSERC; CIFAR; FQRNT; Killam Research Fellowship; Science and Technology
Facilities Council; NSF AST
FX This work was supported under NASA No. NNG08FD60C and made use of data
from the Nuclear Spectroscopic Telescope Array (NuSTAR) mission, a
project led by Caltech, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration. Additional
support for development was provided by the National Space Institute,
Technical University of Denmark. The Malindi ground station is provided
by the Italian Space Agency (ASI) and support for science software
development by the ASI Science Data Center (ASDC). Science team members
acknowledge support from Centre National d'Etudes Spatiales (CNES)
(D.B., M.B.), the NASA Postdoctoral Program (D.R.W.), Leverhulme
Research Fellowship and Science and Technology Facilities Council
(D.M.A), NSF AST (D.R.B.), U.S. DOE/LLNL (W.W.C., M.P., J.V.), NSERC,
CIFAR, FQRNT, and Killam Research Fellowship (V.K.). We thank David
Burrows (PSU) for useful comments which improved the quality of the
manuscript.
NR 155
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR UNSP 103
DI 10.1088/0004-637X/770/2/103
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200021
ER
PT J
AU Konstantopoulos, IS
Maybhate, A
Charlton, JC
Fedotov, K
Durrell, PR
Mulchaey, JS
English, J
Desjardins, TD
Gallagher, SC
Walker, LM
Johnson, KE
Tzanavaris, P
Gronwall, C
AF Konstantopoulos, I. S.
Maybhate, A.
Charlton, J. C.
Fedotov, K.
Durrell, P. R.
Mulchaey, J. S.
English, J.
Desjardins, T. D.
Gallagher, S. C.
Walker, L. M.
Johnson, K. E.
Tzanavaris, P.
Gronwall, C.
TI STELLAR POPULATIONS IN COMPACT GALAXY GROUPS: A MULTI-WAVELENGTH STUDY
OF HCGs 16, 22, AND 42, THEIR STAR CLUSTERS, AND DWARF GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: groups: individual (HCG
16, HCG 22, HCG 42); galaxies: interactions; galaxies: star clusters:
general; intergalactic medium
ID X-RAY-EMISSION; GEMINI SPECTROSCOPIC SURVEY; DIGITAL SKY SURVEY;
LUMINOSITY FUNCTION; GLOBULAR-CLUSTERS; INTERACTING GALAXIES;
STEPHAN-QUINTET; DIFFUSE LIGHT; NEARBY GROUPS; TIDAL TAILS
AB We present a multi-wavelength analysis of three compact galaxy groups, Hickson compact groups (HCGs) 16, 22, and 42, which describe a sequence in terms of gas richness, from space- (Swift, Hubble Space Telescope (HST), and Spitzer) and ground-based (Las Campanas Observatory and Cerro Tololo Inter-American Observatory) imaging and spectroscopy. We study various signs of past interactions including a faint, dusty tidal feature about HCG 16A, which we tentatively age-date at <1 Gyr. This represents the possible detection of a tidal feature at the end of its phase of optical observability. Our HST images also resolve what were thought to be double nuclei in HCG 16C and D into multiple, distinct sources, likely to be star clusters. Beyond our phenomenological treatment, we focus primarily on contrasting the stellar populations across these three groups. The star clusters show a remarkable intermediate-age population in HCG 22, and identify the time at which star formation was quenched in HCG 42. We also search for dwarf galaxies at accordant redshifts. The inclusion of 33 members and 27 "associates" (possible members) radically changes group dynamical masses, which in turn may affect previous evolutionary classifications. The extended membership paints a picture of relative isolation in HCGs 16 and 22, but shows HCG 42 to be part of a larger structure, following a dichotomy expected from recent studies. We conclude that (1) star cluster populations provide an excellent metric of evolutionary state, as they can age-date the past epochs of star formation; and (2) the extended dwarf galaxy population must be considered in assessing the dynamical state of a compact group.
C1 [Konstantopoulos, I. S.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Maybhate, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Charlton, J. C.; Gronwall, C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Fedotov, K.; Desjardins, T. D.; Gallagher, S. C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Fedotov, K.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Durrell, P. R.] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA.
[Mulchaey, J. S.] Carnegie Observ, Pasadena, CA 91101 USA.
[English, J.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada.
[Walker, L. M.; Johnson, K. E.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Johnson, K. E.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Tzanavaris, P.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA.
[Tzanavaris, P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Gronwall, C.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
RP Konstantopoulos, IS (reprint author), Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia.
EM iraklis@aao.gov.au
OI Konstantopoulos, Iraklis/0000-0003-2177-0146
FU Science and Industry Research Fund; National Science Foundation
[AST-0908984]; NASA through grant from the Space Telescope Science
Institute [HST-GO-10787.15-A]; NASA [NAS 5-26555]; Natural Science and
Engineering Research Council of Canada; Ontario Early Researcher Award
Program; Alfred P. Sloan Foundation; Participating Institutions;
National Science Foundation; U.S. Department of Energy; Japanese
Monbukagakusho; Max Planck Society
FX I.S.K. is the recipient of a John Stocker Postdoctoral Fellowship from
the Science and Industry Research Fund.; We thank the anonymous referee
for the enthusiastic reception of our work and for suggestions that
improved the manuscript. Funding was provided at PSU by the National
Science Foundation under award AST-0908984. Support for this work was
provided by NASA through grant No. HST-GO-10787.15-A from the Space
Telescope Science Institute which is operated by AURA, Inc., under NASA
contract NAS 5-26555. K.F. and S.C.G. thank the Natural Science and
Engineering Research Council of Canada and the Ontario Early Researcher
Award Program for support. This paper makes use of publicly available
SDSS imaging and spectroscopy. Funding for the creation and distribution
of the SDSS Archive has been provided by the Alfred P. Sloan Foundation,
the Participating Institutions, the National Aeronautics and Space
Administration, the National Science Foundation, the U.S. Department of
Energy, the Japanese Monbukagakusho, and the Max Planck Society. The
SDSS Web site is http://www.sdss.org/. The SDSS is managed by the
Astrophysical Research Consortium (ARC) for the Participating
Institutions. The Participating Institutions are The University of
Chicago, Fermilab, the Institute for Advanced Study, the Japan
Participation Group, The Johns Hopkins University, Los Alamos National
Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), NewMexico State University,
Princeton University, the United States Naval Observatory, and the
University of Washington. 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 90
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR 114
DI 10.1088/0004-637X/770/2/114
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200032
ER
PT J
AU Lave, KA
Wiedenbeck, ME
Binns, WR
Christian, ER
Cummings, AC
Davis, AJ
de Nolfo, GA
Israel, MH
Leske, RA
Mewaldt, RA
Stone, EC
von Rosenvinge, TT
AF Lave, K. A.
Wiedenbeck, M. E.
Binns, W. R.
Christian, E. R.
Cummings, A. C.
Davis, A. J.
de Nolfo, G. A.
Israel, M. H.
Leske, R. A.
Mewaldt, R. A.
Stone, E. C.
von Rosenvinge, T. T.
TI GALACTIC COSMIC-RAY ENERGY SPECTRA AND COMPOSITION DURING THE 2009-2010
SOLAR MINIMUM PERIOD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; Galaxy: abundances; Sun: activity
ID ADVANCED COMPOSITION EXPLORER; PARTIAL CROSS-SECTIONS; ISOTOPIC
COMPOSITION; CHARGE COMPOSITION; NUCLEUS REACTIONS; SECONDARY;
PROPAGATION; HELIOSPHERE; MODULATION; ELEMENTS
AB We report new measurements of the elemental energy spectra and composition of galactic cosmic rays during the 2009-2010 solar minimum period using observations from the Cosmic Ray Isotope Spectrometer (CRIS) onboard the Advanced Composition Explorer. This period of time exhibited record-setting cosmic-ray intensities and very low levels of solar activity. Results are given for particles with nuclear charge 5 <= Z <= 28 in the energy range similar to 50-550 MeV nucleon(-1). Several recent improvements have been made to the earlier CRIS data analysis, and therefore updates of our previous observations for the 1997-1998 solar minimum and 2001-2003 solar maximum are also given here. Formost species, the reported intensities changed by less than similar to 7%, and the relative abundances changed by less than similar to 4%. Compared with the 1997-1998 solar minimum relative abundances, the 2009-2010 abundances differ by less than 2 sigma, with a trend of fewer secondary species observed in the more recent time period. The new 2009-2010 data are also compared with results of a simple "leaky-box" galactic transport model combined with a spherically symmetric solar modulation model. We demonstrate that this model is able to give reasonable fits to the energy spectra and the secondary-to-primary ratios BC and (Sc+Ti+V)/Fe. These results are also shown to be comparable to a GALPROP numerical model that includes the effects of diffusive reacceleration in the interstellar medium.
C1 [Lave, K. A.; Binns, W. R.; Israel, M. H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Lave, K. A.; Binns, W. R.; Israel, M. H.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Christian, E. R.; de Nolfo, G. A.; von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cummings, A. C.; Davis, A. J.; Leske, R. A.; Mewaldt, R. A.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA.
RP Lave, KA (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA.
RI Christian, Eric/D-4974-2012; de Nolfo, Georgia/E-1500-2012
OI Christian, Eric/0000-0003-2134-3937;
FU NASA at the California Institute of Technology [NNX08AI11G, NNX10AE45G];
Goddard Space Flight Center; Jet Propulsion Laboratory; Washington
University in Saint Louis
FX This work was supported by NASA at the California Institute of
Technology (under grants NNX08AI11G and NNX10AE45G), the Goddard Space
Flight Center, the Jet Propulsion Laboratory, and Washington University
in Saint Louis. We also acknowledge Dr. Nasser Barghouty for his vital
help in updating the semi-empirical nuclear production cross sections
used in our interstellar transport code.
NR 36
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR 117
DI 10.1088/0004-637X/770/2/117
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200035
ER
PT J
AU Lee, CF
Yang, CH
Sahai, R
Contreras, CS
AF Lee, Chin-Fei
Yang, Chun-Hui
Sahai, Raghvendra
Sanchez Contreras, Carmen
TI MAPPING THE CENTRAL REGION OF THE PPN CRL 618 AT SUBARCSECOND RESOLUTION
AT 350 GHz
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary nebulae: general; stars: AGB and
post-AGB; stars: individual (CRL 618); stars: mass-loss
ID PROTOPLANETARY NEBULA CRL-618; MOLECULAR LINE SURVEY; PLANETARY-NEBULAE;
PHYSICAL STRUCTURE; MILLIMETER-WAVE; SUBMILLIMETER; SPECTROSCOPY;
CARBON; ABUNDANCES; ENVELOPE
AB CRL 618 is a well-studied pre-planetary nebula. We have mapped its central region in continuum and molecular lines with the Submillimeter Array at 350 GHz at similar to 0 ''.3-0 ''.5 resolutions. Two components are seen in the 350 GHz continuum: (1) a compact emission at the center tracing the dense inner part of the Hii region previously detected in a 23 GHz continuum and it may trace a fast ionized wind at the base; and (2) an extended thermal dust emission surrounding the Hii region, tracing the dense core previously detected in HC3N at the center of the circumstellar envelope. The dense core is dusty and may contain millimeter-sized dust grains. It may have a density enhancement in the equatorial plane. It is also detected in carbon chain molecules HC3N and HCN and their isotopologues, with higher excitation lines tracing closer to the central star. It is also detected in CH2CHCN toward the innermost part. Most of the emission detected here arises within similar to 630 AU (0 ''.7) of the central star. A simple radiative transfer model is used to derive the kinematics, physical conditions, and the chemical abundances in the dense core. The dense core is expanding and accelerating, with the velocity increasing roughly linearly from similar to 3 km s(-1) in the innermost part to similar to 16 km s(-1) at 630 AU. The mass-loss rate in the dense core is extremely high with a value of similar to 1.15 x 10(-3) M circle dot yr(-1). The dense core has a mass of similar to 0.47 M circle dot and a dynamical age of similar to 400 yr. It could result from a recent enhanced heavy mass-loss episode that ends the asymptotic giant branch phase. The isotopic ratios of C-12/C-13 and N-14/N-15 are 9 +/- 4 and 150 +/- 50, respectively, both lower than the solar values.
C1 [Lee, Chin-Fei; Yang, Chun-Hui] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Sahai, Raghvendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sanchez Contreras, Carmen] Astrobiol Ctr CSIC INTA, E-28691 Madrid, Spain.
RP Lee, CF (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan.
RI Sanchez-Contreras, Carmen/N-3718-2015
OI Sanchez-Contreras, Carmen/0000-0002-6341-592X
FU National Science Council of Taiwan [NSC 99-2112-M-001-007-MY2, NSC
101-2119-M- 001-002-MY3]; Spanish MICINN/MINECO [AYA2009-07304,
AYA2012-32032]; CONSOLIDER INGENIO for the team "Molecular Astrophysics:
The Herschel and ALMA Era-ASTROMOL" [CDS2009-00038]
FX We thank the anonymous referee for valuable and insightful comments. We
thank the SMA staff for their efforts in running and maintaining the
array. C.-F. Lee and C.-H. Yang acknowledge grants from the National
Science Council of Taiwan (NSC 99-2112-M-001-007-MY2 and NSC 101-2119-M-
001-002-MY3). CSC has been partially supported by the Spanish
MICINN/MINECO through grants AYA2009-07304, AYA2012-32032, and
CONSOLIDER INGENIO 2010 for the team "Molecular Astrophysics: The
Herschel and ALMA Era-ASTROMOL" (ref.: CDS2009-00038).
NR 40
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR UNSP 153
DI 10.1088/0004-637X/770/2/153
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200071
ER
PT J
AU Lissauer, JJ
Jontof-Hutter, D
Rowe, JF
Fabrycky, DC
Lopez, ED
Agol, E
Marcy, GW
Deck, KM
Fischer, DA
Fortney, JJ
Howell, SB
Isaacson, H
Jenkins, JM
Kolbl, R
Sasselov, D
Short, DR
Welsh, WF
AF Lissauer, Jack J.
Jontof-Hutter, Daniel
Rowe, Jason F.
Fabrycky, Daniel C.
Lopez, Eric D.
Agol, Eric
Marcy, Geoffrey W.
Deck, Katherine M.
Fischer, Debra A.
Fortney, Jonathan J.
Howell, Steve B.
Isaacson, Howard
Jenkins, Jon M.
Kolbl, Rea
Sasselov, Dimitar
Short, Donald R.
Welsh, William F.
TI ALL SIX PLANETS KNOWN TO ORBIT KEPLER-11 HAVE LOW DENSITIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE celestial mechanics; ephemerides; planets and satellites: composition;
planets and satellites: dynamical evolution and stability; planets and
satellites: fundamental parameters
ID TRANSITING SUPER-EARTH; SUN-LIKE STAR; EXTRASOLAR PLANETS; THERMAL
EVOLUTION; TIMING VARIATIONS; WARM-SPITZER; CANCRI E; LOW-MASS; SYSTEM;
POPULATIONS
AB The Kepler-11 planetary system contains six transiting planets ranging in size from 1.8 to 4.2 times the radius of Earth. Five of these planets orbit in a tightly packed configuration with periods between 10 and 47 days. We perform a dynamical analysis of the system based upon transit timing variations observed in more than three years of Kepler photometric data. Stellar parameters are derived using a combination of spectral classification and constraints on the star's density derived from transit profiles together with planetary eccentricity vectors provided by our dynamical study. Combining masses of the planets relative to the star from our dynamical study and radii of the planets relative to the star from transit depths together with deduced stellar properties yields measurements of the radii of all six planets, masses of the five inner planets, and an upper bound to the mass of the outermost planet, whose orbital period is 118 days. We find mass-radius combinations for all six planets that imply that substantial fractions of their volumes are occupied by constituents that are less dense than rock. Moreover, we examine the stability of these envelopes against photoevaporation and find that the compositions of at least the inner two planets have likely been significantly sculpted by mass loss. The Kepler-11 system contains the lowest mass exoplanets for which both mass and radius have been measured.
C1 [Lissauer, Jack J.; Jontof-Hutter, Daniel; Rowe, Jason F.; Howell, Steve B.; Jenkins, Jon M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rowe, Jason F.; Jenkins, Jon M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Lopez, Eric D.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Marcy, Geoffrey W.; Isaacson, Howard; Kolbl, Rea] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Deck, Katherine M.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Deck, Katherine M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Short, Donald R.] San Diego State Univ, Dept Math, San Diego, CA 92182 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Jack.Lissauer@nasa.gov
OI Fortney, Jonathan/0000-0002-9843-4354; /0000-0002-0802-9145; Fabrycky,
Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NSF [AST-0645416, AST-1109928];
Kepler Participating Scientist Program via NASA [NNX12AD23G]
FX Kepler was competitively selected as the tenth Discovery mission.
Funding for this mission is provided by NASA's Science Mission
Directorate. E.A.'s work was supported by NSF Career grant AST-0645416.
W.F.W. gratefully acknowledges support from the Kepler Participating
Scientist Program via NASA grant NNX12AD23G, and from the NSF via grant
AST-1109928. D.J. gratefully acknowledges a Fellowship from the NASA
Postdoctoral Program. We thank Jerome Orosz and Gur Windmiller for
assistance in developing D.S.'s method for measuring transit times and
Tony Dobrovolskis, Darin Ragozzine, and Billy Quarles for helpful
comments on the manuscript.
NR 36
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR UNSP 131
DI 10.1088/0004-637X/770/2/131
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200049
ER
PT J
AU Lopez-Puertas, M
Dinelli, BM
Adriani, A
Funke, B
Garcia-Comas, M
Moriconi, ML
D'Aversa, E
Boersma, C
Allamandola, LJ
AF Lopez-Puertas, M.
Dinelli, B. M.
Adriani, A.
Funke, B.
Garcia-Comas, M.
Moriconi, M. L.
D'Aversa, E.
Boersma, C.
Allamandola, L. J.
TI LARGE ABUNDANCES OF POLYCYCLIC AROMATIC HYDROCARBONS IN TITAN'S UPPER
ATMOSPHERE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE molecular processes; planets and satellites: atmospheres; planets and
satellites: composition; planets and satellites: individual (Titan);
radiation mechanisms: non-thermal
ID SPECTROSCOPIC DATABASE; INFRARED-SPECTROSCOPY; MU-M; EMISSION; AEROSOLS;
MODEL; CASSINI/VIMS; SPECTRA
AB In this paper, we analyze the strong unidentified emission near 3.28 mu m in Titan's upper daytime atmosphere recently discovered by Dinelli et al. We have studied it by using the NASA Ames PAH IR Spectroscopic Database. The polycyclic aromatic hydrocarbons (PAHs), after absorbing UV solar radiation, are able to emit strongly near 3.3 mu m. By using current models for the redistribution of the absorbed UV energy, we have explained the observed spectral feature and have derived the vertical distribution of PAH abundances in Titan's upper atmosphere. PAHs have been found to be present in large concentrations, about (2-3) x 10(4) particles cm(-3). The identified PAHs have 9-96 carbons, with a concentration-weighted average of 34 carbons. The mean mass is similar to 430 u; the mean area is about 0.53 nm(2); they are formed by 10-11 rings on average, and about one-third of them contain nitrogen atoms. Recently, benzene together with light aromatic species as well as small concentrations of heavy positive and negative ions have been detected in Titan's upper atmosphere. We suggest that the large concentrations of PAHs found here are the neutral counterpart of those positive and negative ions, which hence supports the theory that the origin of Titan main haze layer is located in the upper atmosphere.
C1 [Lopez-Puertas, M.; Funke, B.; Garcia-Comas, M.] Inst Astrofis Andalucia CSIC, E-18080 Granada, Spain.
[Dinelli, B. M.] ISAC CNR, I-40129 Bologna, Italy.
[Adriani, A.; D'Aversa, E.] IAPS INAF, I-00133 Rome, Italy.
[Moriconi, M. L.] ISAC CNR, I-00133 Rome, Italy.
[Boersma, C.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lopez-Puertas, M (reprint author), Inst Astrofis Andalucia CSIC, E-18080 Granada, Spain.
EM puertas@iaa.es
RI Lopez Puertas, Manuel/M-8219-2013; Garcia-Comas, Maya/E-4050-2014;
moriconi, maria luisa/B-7201-2009; Funke, Bernd/C-2162-2008; Boersma,
Christiaan/L-7696-2014; Dinelli, Bianca Maria/C-1212-2015;
OI Adriani, Alberto/0000-0003-4998-8008; Dinelli, Bianca
Maria/0000-0002-1218-0008; Lopez Puertas, Manuel/0000-0003-2941-7734;
Garcia-Comas, Maya/0000-0003-2323-4486; moriconi, maria
luisa/0000-0003-2609-2620; Funke, Bernd/0000-0003-0462-4702; Boersma,
Christiaan/0000-0002-4836-217X; D'Aversa, Emiliano/0000-0002-5842-5867
FU Italian Space Agency [ASI I/015/09]; Spanish MINECO [AYA2011-23552];
CONSOLIDER program [CSD2009-00038]; EC FEDER funds; MINECO under its
"Ramon y Cajal" subprogram; NASA Postdoctoral Program at the Ames
Research Center; NASA
FX Special thanks are given to the Cassini/VIMS team for planning the VIMS
observations and to Nick Teanby for looking at and providing the CIRS
high-altitude spectra. The activities of the Italian authors have been
supported by the Italian Space Agency under the grant ASI I/015/09. The
IAA team was supported by the Spanish MINECO under grant AYA2011-23552,
the CONSOLIDER program CSD2009-00038, and EC FEDER funds. M.G.C. is also
financially supported by MINECO under its "Ramon y Cajal" subprogram.
C.B.' s work was supported by an appointment to the NASA Postdoctoral
Program at the Ames Research Center, administered by Oak Ridge
Associated Universities through a contract with NASA.
NR 38
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR UNSP 132
DI 10.1088/0004-637X/770/2/132
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200050
ER
PT J
AU Plagge, TJ
Marrone, DP
Abdulla, Z
Bonamente, M
Carlstrom, JE
Gralla, M
Greer, CH
Joy, M
Lamb, JW
Leitch, EM
Mantz, A
Muchovej, S
Woody, D
AF Plagge, Thomas J.
Marrone, Daniel P.
Abdulla, Zubair
Bonamente, Massimiliano
Carlstrom, John E.
Gralla, Megan
Greer, Christopher H.
Joy, Marshall
Lamb, James W.
Leitch, Erik M.
Mantz, Adam
Muchovej, Stephen
Woody, David
TI CARMA MEASUREMENTS OF THE SUNYAEV-ZEL'DOVICH EFFECT IN RX J1347.5-1145
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general
ID GALAXY CLUSTER; SKY SURVEY; RX-J1347.5-1145; UNCERTAINTIES;
RX-J1347-1145; J1347-1145; BARYONS; MASS; GHZ; MAP
AB We demonstrate the Sunyaev-Zel'dovich (SZ) effect imaging capabilities of the Combined Array for Research in Millimeter-wave Astronomy (CARMA) by presenting an SZ map of the galaxy cluster RX J1347.5-1145. By combining data from multiple CARMA bands and configurations, we are able to capture the structure of this cluster over a wide range of angular scales, from its bulk properties to its core morphology. We find that roughly 9% of this cluster's thermal energy is associated with sub-arcminute-scale structure imparted by a merger, illustrating the value of high-resolution SZ measurements for pursuing cluster astrophysics and for understanding the scatter in SZ scaling relations. We also find that the cluster's SZ signal is lower in amplitude than suggested by a spherically symmetric model derived from X-ray data, consistent with compression along the line of sight relative to the plane of the sky. Finally, we discuss the impact of upgrades currently in progress that will further enhance CARMA's power as an SZ imaging instrument.
C1 [Plagge, Thomas J.; Marrone, Daniel P.; Abdulla, Zubair; Carlstrom, John E.; Gralla, Megan; Greer, Christopher H.; Leitch, Erik M.; Mantz, Adam] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Marrone, Daniel P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bonamente, Massimiliano] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Bonamente, Massimiliano; Joy, Marshall] NASA, Space Sci VP62, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Carlstrom, John E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Carlstrom, John E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Gralla, Megan] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lamb, James W.; Muchovej, Stephen; Woody, David] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA.
RP Plagge, TJ (reprint author), Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
OI Marrone, Daniel/0000-0002-2367-1080
FU Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris
Foundation; James S. McDonnell Foundation; Associates of the California
Institute of Technology; University of Chicago; state of California;
state of Illinois; state of Maryland; National Science Foundation;
National Science Foundation at the University of Chicago [AST-0838187];
CARMA; NSF Physics Frontier Center grant [PHY-1125897]; NASA through
Hubble Fellowship grant [HST-HF-51259.01]
FX Support for CARMA construction was derived from the Gordon and Betty
Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the
James S. McDonnell Foundation, the Associates of the California
Institute of Technology, the University of Chicago, the states of
California, Illinois, and Maryland, and the National Science Foundation.
Ongoing CARMA development and operations are supported by the National
Science Foundation under a cooperative agreement, including grant
AST-0838187 at the University of Chicago, and by the CARMA partner
universities. Partial support is provided by NSF Physics Frontier Center
grant PHY-1125897 to the Kavli Institute of Cosmological Physics. D.P.M.
was supported for part of this work by NASA through Hubble Fellowship
grant HST-HF-51259.01.
NR 33
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2013
VL 770
IS 2
AR 112
DI 10.1088/0004-637X/770/2/112
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200030
ER
PT J
AU Sitarski, BN
Morris, MR
Lu, JR
Duchene, G
Stolte, A
Becklin, EE
Ghez, AM
Zinnecker, H
AF Sitarski, Breann N.
Morris, Mark R.
Lu, Jessica R.
Duchene, Gaspard
Stolte, Andrea
Becklin, E. E.
Ghez, Andrea M.
Zinnecker, Hans
TI KECK ADAPTIVE OPTICS OBSERVATIONS OF THE PROTOSTELLAR DISK AROUND RADIO
SOURCE I IN THE ORION KLEINMANN-LOW NEBULA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; ISM: individual objects (Orion); stars: pre-main
sequence
ID EDGE-ON DISK; CIRCUMSTELLAR DISK; YOUNG STARS; MU-M; MOLECULAR CLOUD;
GALACTIC-CENTER; STELLAR ORBITS; MASSIVE STARS; BN/KL REGION; RESOLUTION
AB We have made the first detection of a near-infrared counterpart associated with the disk around Radio Source "I," a massive protostar in the Kleinmann-Low nebula in Orion, using imaging with laser guide star adaptive optics on the Keck II telescope. The infrared emission is evident in images acquired using L' (3.8 mu m) and Ms (4.7 mu m) filters and is not detectable at K' (2.1 mu m). The observed morphology strongly suggests that we are seeing some combination of scattered and thermal light emanating from the disk. The disk is also manifest in the L'/Ms flux ratio image. We interpret the near-infrared emission as the illuminated surface of a nearly edge-on disk, oriented so that only the northern face is visible; the opposite surface remains hidden by the disk. We do not see infrared radiation associated directly with the star proposed to be associated with Source "I." The data also suggest that there is a cavity above and below the disk that is oriented perpendicular to the disk and is sculpted by the known, strong outflow from the inner disk of Source I. We compare our data to models of a protostar with a surrounding disk, envelope, and wind-blown cavity in order to elucidate the nature of the disk around Radio Source I.
C1 [Sitarski, Breann N.; Morris, Mark R.; Becklin, E. E.; Ghez, Andrea M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Lu, Jessica R.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Duchene, Gaspard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Duchene, Gaspard] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, F-38041 Grenoble, France.
[Stolte, Andrea] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Becklin, E. E.; Zinnecker, Hans] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Zinnecker, Hans] Astrophys Inst Potsdam, D-14482 Potsdam, Germany.
[Zinnecker, Hans] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
RP Sitarski, BN (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, 430 Portola Plaza, Los Angeles, CA 90095 USA.
EM bsitarski@astro.ucla.edu
OI Lu, Jessica/0000-0001-9611-0009
FU Universities Space Research Association (USRA) grant [USRA850005];
German Science Foundation Emmy Noether program [DFG STO 496-3]; NSF
Astronomy and Astrophysics Postdoctoral Fellow program [AST-1102791]; W.
M. Keck Foundation
FX Support for this work was provided by a Universities Space Research
Association (USRA) grant to UCLA (grant USRA850005). A.S. acknowledges
support from the German Science Foundation Emmy Noether program under
grant DFG STO 496-3. J.R.L. acknowledges support from the NSF Astronomy
and Astrophysics Postdoctoral Fellow program (AST-1102791).; Data
presented herein were taken at the W. M. Keck Observatory. The W. M.
Keck Observatory 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. We acknowledge the significant cultural role that the summit
of Mauna Kea has always had for the indigenous Hawaiian community. We
are most fortunate to have the opportunity to conduct observations from
this mountain.
NR 58
TC 5
Z9 5
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 JUN 20
PY 2013
VL 770
IS 2
AR UNSP 134
DI 10.1088/0004-637X/770/2/134
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200052
ER
PT J
AU Williams, BJ
Borkowski, KJ
Ghavamian, P
Hewitt, JW
Mao, SA
Petre, R
Reynolds, SP
Blondin, JM
AF Williams, Brian J.
Borkowski, Kazimierz J.
Ghavamian, Parviz
Hewitt, John W.
Mao, S. Alwin
Petre, Robert
Reynolds, Stephen P.
Blondin, John M.
TI AZIMUTHAL DENSITY VARIATIONS AROUND THE RIM OF TYCHO's SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: supernova remnants
ID LARGE-MAGELLANIC-CLOUD; BRAHES 1572 SUPERNOVA; IA SUPERNOVA; DUST
GRAINS; NONRADIATIVE SHOCKS; OPTICAL-PROPERTIES; SPITZER; EMISSION;
SPECTROSCOPY; EXPANSION
AB Spitzer images of Tycho's supernova remnant in the mid-infrared reveal limb-brightened emission from the entire periphery of the shell and faint filamentary structures in the interior. As with other young remnants, this emission is produced by dust grains, warmed to similar to 100 K in the post-shock environment by collisions with energetic electrons and ions. The ratio of the 70 to 24 mu m fluxes is a diagnostic of the dust temperature, which in turn is a sensitive function of the plasma density. We find significant variations in the 70/24 flux ratio around the periphery of Tycho's forward shock, implying order-of-magnitude variations in density. While some of these are likely localized interactions with dense clumps of the interstellar medium (ISM), we find an overall gradient in the ambient density surrounding Tycho, with densities 3-10 times higher in the northeast than in the southwest. This large density gradient is qualitatively consistent with the variations in the proper motion of the shock observed in radio and X-ray studies. Overall, the mean ISM density around Tycho is quite low (similar to 0.1-0.2 cm(-3)), consistent with the lack of thermal X-ray emission observed at the forward shock. We perform two-dimensional hydrodynamic simulations of a Type Ia supernova expanding into a density gradient in the ISM, and find that the overall round shape of the remnant is still easily achievable, even for explosions into significant gradients. However, this leads to an offset of the center of the explosion from the geometric center of the remnant of up to 20%, although lower values of 10% are preferred. The best match with hydrodynamical simulations is achieved if Tycho is located at a large (3-4 kpc) distance in a medium with a mean preshock density of similar to 0.2 cm(-3). Such preshock densities are obtained for highly (greater than or similar to 50%) porous ISM grains.
C1 [Williams, Brian J.; Hewitt, John W.; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Borkowski, Kazimierz J.; Mao, S. Alwin; Reynolds, Stephen P.; Blondin, John M.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Ghavamian, Parviz] Towson Univ, Dept Phys Astron & Geosci, Towson, MD 21252 USA.
[Mao, S. Alwin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Williams, BJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM brian.j.williams@nasa.gov
FU NASA [NNX11AB14G]; NASA Archival Data Analysis Program [12-ADAP12-0168];
NSF's REU [AST-1032736]
FX We thank the anonymous referee for a careful reading of the text. We
thank P. F. Winkler for the H alpha image. This work is partly based on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology under
a contract with NASA. This work was supported by NASA Archival Data
Analysis Program grant 12-ADAP12-0168. B.J.W. acknowledges support from
the NASA Postdoctoral Program Fellowship. K.J.B. and S.P.R. acknowledge
support from NASA through grant NNX11AB14G. A.M. acknowledges support
through NSF's REU award AST-1032736 to NC State University.
NR 62
TC 19
Z9 19
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 JUN 20
PY 2013
VL 770
IS 2
AR 129
DI 10.1088/0004-637X/770/2/129
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 160HZ
UT WOS:000320111200047
ER
PT J
AU Acar, E
Karaca, HE
Basaran, B
Yang, F
Mills, MJ
Noebe, RD
Chumlyakov, YI
AF Acar, E.
Karaca, H. E.
Basaran, B.
Yang, F.
Mills, M. J.
Noebe, R. D.
Chumlyakov, Y. I.
TI Role of aging time on the microstructure and shape memory properties of
NiTiHfPd single crystals
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE Aging; Elastic energy; NiTiHfPd; Single crystals; Shape memory alloy
ID MARTENSITIC-TRANSFORMATION; ALLOYS; BEHAVIOR; DEPENDENCE; PARTICLES; AL
AB Shape memory properties of [111] oriented NiTiHfPd single crystals aged at 600 degrees C for 48 and 72 h were investigated through isobaric thermal cycling and superelasticity experiments in compression. A maximum transformation strain of 2.6% at 1000 MPa compressive stress was attained above 100 degrees C. It was observed that precipitate size and interparticle distances were strong functions of aging time and subsequently govern the shape memory responses of the NiTiHfPd single crystals. Moreover, it was revealed that the elastic energy storage highly depends on precipitate characteristics. (c) 2013 Elsevier B.V. All rights reserved.
C1 [Acar, E.; Karaca, H. E.; Basaran, B.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Yang, F.; Mills, M. J.] Ohio State Univ, Dept Mat Sci, Columbus, OH 43210 USA.
[Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Chumlyakov, Y. I.] Siberian Phys Tech Inst, Tomsk 634050, Russia.
RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
EM karaca@engr.uky.edu
RI Mills, Michael/I-6413-2013; Chumlyakov, Yuriy/R-6496-2016
FU NASA Fundamental Aeronautics Program; Aeronautical Sciences Project;
NASA EPSCOR Program [NNX11AQ31A]; KY EPSCoR RID Program [3049024332];
RFBR Project [10-03-0154-a]; US Department of Energy, Office of Basic
Energy Sciences
FX This work was supported in part by the NASA Fundamental Aeronautics
Program, Aeronautical Sciences Project and the NASA EPSCOR Program under
Grant No NNX11AQ31A and KY EPSCoR RID Program under Grant No 3049024332
and RFBR Project with Grant no 10-03-0154-a. FY and MJM acknowledge the
support of the US Department of Energy, Office of Basic Energy Sciences.
NR 34
TC 15
Z9 15
U1 0
U2 19
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD JUN 20
PY 2013
VL 573
BP 161
EP 165
DI 10.1016/j.msea.2013.02.016
PG 5
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 152PU
UT WOS:000319544400023
ER
PT J
AU Yu, J
Liu, AK
Yang, Y
Zhao, Y
AF Yu, J.
Liu, A. K.
Yang, Y.
Zhao, Y.
TI Analysis of sea ice motion and deformation using AMSR-E data from 2005
to 2007
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID WAVELET ANALYSIS; SAR IMAGERY; TRACKING; SYSTEM; BUOY
AB Dynamics of Arctic sea ice, including motion and deformation, are studied utilizing data from the Advanced Microwave Scanning Radiometer for the Earth Observing System (EOS) (AMSR-E) during 2005 and 2007. We first derive sea ice motion maps from the satellite data in a grid of 100 kmx100 km using a two-dimensional wavelet method. These sea ice motion results are compared with those derived from buoy data from the International Arctic Buoy Programme. Secondly, it is well known that sea ice deformation can be characterized by a strain-rate tensor calculated from the ice velocity field. Two components of the strain-rate tensor quantify the divergence and the shearing of the ice field, respectively. Daily maps for both sea ice motion and strain-rate tensor, as well as monthly averages and spatial sums, are computed and analysed. Comparison of the monthly ice motion maps for May 2005 and May 2007 indicates that the anti-cyclonic Beaufort Gyre and Transpolar Drift Stream in the western Arctic are relatively stronger during 2007 than 2005. Different patterns in the spring months' sea ice deformation rates as characterized by the absolute values of the strain-rate tensor are observed when we compare the data of 2007 with those of 2005 and 2006. The sea ice deformation activities in the spring of 2007 happen earlier and are relatively stronger than that of 2005 and 2006. These results might help to explain why the sea ice extent in the summer of 2007 is unprecedentedly low.
C1 [Yu, J.; Yang, Y.] Univ Vermont, Dept Math & Stat, Burlington, VT 05405 USA.
[Liu, A. K.; Zhao, Y.] NASA, Lab Hydrospher Proc, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Yu, J (reprint author), Univ Vermont, Dept Math & Stat, Burlington, VT 05405 USA.
EM Jun.Yu@uvm.edu
FU Vermont Space Grant Consortium; Vermont NASA
FX This work was supported by the Vermont Space Grant Consortium and the
Vermont NASA Experimental Program to Stimulate Competitive Research
grant.
NR 20
TC 1
Z9 2
U1 0
U2 35
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD JUN 20
PY 2013
VL 34
IS 12
BP 4127
EP 4141
DI 10.1080/01431161.2013.772314
PG 15
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA 109UR
UT WOS:000316395000001
ER
PT J
AU Shapiro, MG
Priest, MF
Siegel, PH
Bezanilla, F
AF Shapiro, Mikhail G.
Priest, Michael F.
Siegel, Peter H.
Bezanilla, Francisco
TI Thermal Mechanisms of Millimeter Wave Stimulation of Excitable Cells
SO BIOPHYSICAL JOURNAL
LA English
DT Article
ID NA+/K+-ATPASE; TEMPERATURE; INACTIVATION; CHANNELS; CURRENTS; SQUID;
STATE
AB Interactions between millimeter waves (MMWs) and biological systems have received increasing attention due to the growing use of MMW radiation in technologies ranging from experimental medical devices to telecommunications and airport security. Studies have shown that MMW exposure alters cellular function, especially in neurons and muscles. However, the biophysical mechanisms underlying such effects are still poorly understood. Due to the high aqueous absorbance of MMW, thermal mechanisms are likely. However, nonthermal mechanisms based on resonance effects have also been postulated. We studied MMW stimulation in a simplified preparation comprising Xenopus laevis oocytes expressing proteins that underlie membrane excitability. Using electrophysiological recordings simultaneously with 60 GHz stimulation, we observed changes in the kinetics and activity levels of voltage-gated potassium and sodium channels and a sodium-potassium pump that are consistent with a thermal mechanism. Furthermore, we showed that MMW stimulation significantly increased the action potential firing rate in oocytes coexpressing voltage-gated sodium and potassium channels, as predicted by thermal terms in the Hodgkin-Huxley model of neurons. Our results suggest that MMW stimulation produces significant thermally mediated effects on excitable cells via basic thermodynamic mechanisms that must be taken into account in the study and use of MMW radiation in biological systems.
C1 [Shapiro, Mikhail G.] Univ Calif Berkeley, Miller Res Inst, Berkeley, CA 94720 USA.
[Shapiro, Mikhail G.] Univ Calif Berkeley, Dept Bioengn, Berkeley, CA 94720 USA.
[Shapiro, Mikhail G.] Univ Calif Berkeley, Dept Mol & Cell Biol, Berkeley, CA 94720 USA.
[Priest, Michael F.] Univ Chicago, Comm Neurobiol, Chicago, IL 60637 USA.
[Priest, Michael F.; Bezanilla, Francisco] Univ Chicago, Dept Biochem & Mol Biol, Chicago, IL 60637 USA.
CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA.
RP Shapiro, MG (reprint author), Univ Calif Berkeley, Miller Res Inst, Berkeley, CA 94720 USA.
EM mikhail@caltech.edu; fbezanilla@peds.bsd.uchicago.edu
OI Shapiro, MIkhail/0000-0002-0291-4215
FU Miller Research Institute; NIH [GM030376, F31 NIH-NS081954]
FX This research was supported by the Miller Research Institute (to MGS),
NIH grant GM030376 (to FB) and F31 NIH-NS081954 (to MFP).
NR 27
TC 5
Z9 5
U1 2
U2 14
PU CELL PRESS
PI CAMBRIDGE
PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA
SN 0006-3495
EI 1542-0086
J9 BIOPHYS J
JI Biophys. J.
PD JUN 18
PY 2013
VL 104
IS 12
BP 2622
EP 2628
DI 10.1016/j.bpj.2013.05.014
PG 7
WC Biophysics
SC Biophysics
GA 169DI
UT WOS:000320757100007
PM 23790370
ER
PT J
AU Kharecha, PA
Hansen, JE
AF Kharecha, Pushker A.
Hansen, James E.
TI Response to Comment on "Prevented Mortality and Greenhouse Gas Emissions
from Historical and Projected Nuclear Power"
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Editorial Material
ID ENERGY
C1 [Kharecha, Pushker A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
Columbia Univ, Earth Inst, New York, NY 10025 USA.
RP Kharecha, PA (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM pushker@giss.nasa.gov
NR 14
TC 1
Z9 1
U1 2
U2 17
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD JUN 18
PY 2013
VL 47
IS 12
BP 6718
EP 6719
DI 10.1021/es402211m
PG 2
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 169AJ
UT WOS:000320749000082
PM 23697846
ER
PT J
AU Bennett, CJ
Brotton, SJ
Jones, BM
Misra, AK
Sharma, SK
Kaiser, RI
AF Bennett, Chris J.
Brotton, Stephen J.
Jones, Brant M.
Misra, Anupam K.
Sharma, Shiv K.
Kaiser, Ralf I.
TI High-Sensitivity Raman Spectrometer To Study Pristine and Irradiated
Interstellar Ice Analogs
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID MICROPROBE SPECTROSCOPY; INFRARED INTENSITIES; ORGANIC-MATTER;
CROSS-SECTION; SURFACE; SCATTERING; SYSTEM; MOLECULES; ISOMER;
PREDICTION
AB We discuss the novel design of a sensitive, normal-Raman spectrometer interfaced to an ultra-high vacuum chamber (5 X 10(-11) Torr) utilized to investigate the interaction of ionizing radiation with low temperature ices relevant to the solar system and interstellar medium. The design is based on a pulsed Nd:YAG laser which takes advantage of gating techniques to isolate the scattered Raman signal from the competing fluorescence signal. The setup incorporates innovations to achieve maximum sensitivity without detectable heating of the sample. Thin films of carbon dioxide (CO2) ices of 10 to 396 nm thickness were prepared and characterized using both Fourier transform infrared (FT-IR) spectroscopy and HeNe interference techniques. The nu(+) and nu(-) Fermi resonance bands of CO2 ices were observed by Raman spectroscopy at 1385 and 1278 cm(-1), respectively, and the band areas showed a linear dependence on ice thickness. Preliminary irradiation experiments are conducted on a 450 nm thick sample of CO2 ice using energetic electrons. Both carbon monoxide (CO) and the infrared inactive molecular oxygen (O-2) products are readily detected from their characteristic Raman bands at 2145 and 1545 cm(-1), respectively. Detection limits of 4 +/- 3 and 6 4 monolayers of CO and O-2 were derived, demonstrating the unique power to detect newly formed molecules in irradiated ices in situ. The setup is universally applicable to the detection of low-abundance species, since no Raman signal enhancement is required, demonstrating Raman spectroscopy as a reliable alternative, or complement, to FT-IR spectroscopy in space science applications.
C1 [Bennett, Chris J.; Brotton, Stephen J.; Jones, Brant M.; Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
[Bennett, Chris J.; Brotton, Stephen J.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
[Jones, Brant M.; Kaiser, Ralf I.] Univ Hawaii Manoa, WM Keck Res Lab Astrochem, Honolulu, HI 96822 USA.
[Misra, Anupam K.; Sharma, Shiv K.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
RP Kaiser, RI (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
EM ralfk@hawaii.edu
OI Bennett, Christopher/0000-0002-4181-6976
FU W. M. Keck Foundation; National Aeronautics and Space Administration
through the NASA Astrobiology Institute (Office of Space Science)
[NNA09DA77A]
FX This project was made possible by the generous financial support of the
W. M. Keck Foundation. C.J.B. would like to acknowledge support from the
National Aeronautics and Space Administration through the NASA
Astrobiology Institute (Cooperative Agreement No. NNA09DA77A issued
through the Office of Space Science). We thank the anonymous referee for
their valuable suggestions to this work. We also thank Patrick Gasda for
his contributions to the initial design and testing of the Raman
spectrometer.
NR 69
TC 12
Z9 12
U1 1
U2 31
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
EI 1520-6882
J9 ANAL CHEM
JI Anal. Chem.
PD JUN 18
PY 2013
VL 85
IS 12
BP 5659
EP 5665
DI 10.1021/ac303259y
PG 7
WC Chemistry, Analytical
SC Chemistry
GA 169AL
UT WOS:000320749200010
PM 23662702
ER
PT J
AU Dowsett, HJ
Foley, KM
Stoll, DK
Chandler, MA
Sohl, LE
Bentsen, M
Otto-Bliesner, BL
Bragg, FJ
Chan, WL
Contoux, C
Dolan, AM
Haywood, AM
Jonas, JA
Jost, A
Kamae, Y
Lohmann, G
Lunt, DJ
Nisancioglu, KH
Abe-Ouchi, A
Ramstein, G
Riesselman, CR
Robinson, MM
Rosenbloom, NA
Salzmann, U
Stepanek, C
Strother, SL
Ueda, H
Yan, Q
Zhang, ZS
AF Dowsett, Harry J.
Foley, Kevin M.
Stoll, Danielle K.
Chandler, Mark A.
Sohl, Linda E.
Bentsen, Mats
Otto-Bliesner, Bette L.
Bragg, Fran J.
Chan, Wing-Le
Contoux, Camille
Dolan, Aisling M.
Haywood, Alan M.
Jonas, Jeff A.
Jost, Anne
Kamae, Youichi
Lohmann, Gerrit
Lunt, Daniel J.
Nisancioglu, Kerim H.
Abe-Ouchi, Ayako
Ramstein, Gilles
Riesselman, Christina R.
Robinson, Marci M.
Rosenbloom, Nan A.
Salzmann, Ulrich
Stepanek, Christian
Strother, Stephanie L.
Ueda, Hiroaki
Yan, Qing
Zhang, Zhongshi
TI Sea Surface Temperature of the mid-Piacenzian Ocean: A Data-Model
Comparison
SO SCIENTIFIC REPORTS
LA English
DT Article
ID NORTH-ATLANTIC OCEAN; PLIOMIP EXPERIMENTAL-DESIGN; GENERAL-CIRCULATION
MODEL; PMIP2 COUPLED SIMULATIONS; LAST GLACIAL MAXIMUM; PLIOCENE
CLIMATE; BOUNDARY-CONDITIONS; UNITED-STATES; JOINT INVESTIGATIONS; WARM
PERIOD
AB The mid-Piacenzian climate represents the most geologically recent interval of long-term average warmth relative to the last million years, and shares similarities with the climate projected for the end of the 21st century. As such, it represents a natural experiment from which we can gain insight into potential climate change impacts, enabling more informed policy decisions for mitigation and adaptation. Here, we present the first systematic comparison of Pliocene sea surface temperature (SST) between an ensemble of eight climate model simulations produced as part of PlioMIP (Pliocene Model Intercomparison Project) with the PRISM (Pliocene Research, Interpretation and Synoptic Mapping) Project mean annual SST field. Our results highlight key regional and dynamic situations where there is discord between the palaeoenvironmental reconstruction and the climate model simulations. These differences have led to improved strategies for both experimental design and temporal refinement of the palaeoenvironmental reconstruction.
C1 [Dowsett, Harry J.; Foley, Kevin M.; Stoll, Danielle K.; Riesselman, Christina R.; Robinson, Marci M.; Strother, Stephanie L.] US Geol Survey, Reston, VA 20192 USA.
[Chandler, Mark A.; Sohl, Linda E.; Jonas, Jeff A.] Columbia Univ, NASA GISS, New York, NY USA.
[Bentsen, Mats; Nisancioglu, Kerim H.; Zhang, Zhongshi] Bjerknes Ctr Climate Res, Bergen, Norway.
[Otto-Bliesner, Bette L.; Rosenbloom, Nan A.] Natl Ctr Atmospher Res, Boulder, CO 80305 USA.
[Bragg, Fran J.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Chan, Wing-Le; Abe-Ouchi, Ayako] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778564, Japan.
[Contoux, Camille; Ramstein, Gilles] UMR CEA CNRS UVSQ, Lab Sci Climat & Environnem IPSL, F-91191 Gif Sur Yvette, France.
[Contoux, Camille; Jost, Anne] Univ Paris 06, F-75005 Sisyphe, France.
[Contoux, Camille; Jost, Anne] CNRS, F-75005 Sisyphe, France.
[Dolan, Aisling M.; Haywood, Alan M.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England.
[Kamae, Youichi; Ueda, Hiroaki] Univ Tsukuba, Grad Sch Life & Environm Sci, Tsukuba, Ibaraki, Japan.
[Lohmann, Gerrit; Stepanek, Christian] Alfred Wegener Inst Polar & Marine Res, Bremerhaven, Germany.
[Abe-Ouchi, Ayako] Japan Agcy Marine Earth Sci & Technol, Res Inst forGlobal Change, Yokohama, Kanagawa, Japan.
[Salzmann, Ulrich; Strother, Stephanie L.] Northumbria Univ, Fac Engn & Environm, Dept Geog, Newcastle Upon Tyne NE1 8ST, Tyne & Wear, England.
[Yan, Qing; Zhang, Zhongshi] Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China.
RP Dowsett, HJ (reprint author), US Geol Survey, Reston, VA 20192 USA.
EM hdowsett@usgs.gov
RI Lunt, Daniel/G-9451-2011; Kamae, Youichi/L-6694-2013; Abe-Ouchi,
Ayako/M-6359-2013; Ramstein, Gilles/L-3328-2014; Zhang,
Zhongshi/L-2891-2013; Yan, Qing/C-5413-2013;
OI Bragg, Fran/0000-0002-8179-4214; Dowsett, Harry/0000-0003-1983-7524;
Lunt, Daniel/0000-0003-3585-6928; Lohmann, Gerrit/0000-0003-2089-733X;
Kamae, Youichi/0000-0003-0461-5718; Abe-Ouchi,
Ayako/0000-0003-1745-5952; Ramstein, Gilles/0000-0002-1522-917X; Zhang,
Zhongshi/0000-0002-2354-1622; Yan, Qing/0000-0001-5299-7824; Dolan,
Aisling/0000-0002-9585-9648
FU U.S. Geological Survey Climate and Land Use Change Research and
Development Program; PlioMIP initiative; USGS Mendenhall Post-doctoral
Fellowship Program; NASA; NASA High-End Computing (HEC) Program through
the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight
Center; Natural Environment Research Council, NERC [NE/I016287/1,
NE/H006273/1]; U.S. National Science Foundation (NSF); NSF; European
Research Council under the European Union/ERC [278636]; UK Natural
Environment Research Council; AWI; Helmholz; Japan Society for the
Promotion of Science and computing resources at the Earth Simulator
Center, JAMSTEC
FX HJD, KMF, DKS and MMR acknowledge the continued support of the U.S.
Geological Survey Climate and Land Use Change Research and Development
Program; HJD, MAC and MMR thank the USGS John Wesley Powell Center for
Analysis and Synthesis for support of the PlioMIP initiative; HJD and
CRR acknowledge support from the USGS Mendenhall Post-doctoral
Fellowship Program; MAC and LES acknowledge support from the NASA
Climate Modeling Program, and the NASA High-End Computing (HEC) Program
through the NASA Center for Climate Simulation (NCCS) at Goddard Space
Flight Center. Financial support was provided by grants to US and AMH
from the Natural Environment Research Council, NERC (NE/I016287/1); DJL
and FJB acknowledge NERC grant NE/H006273/1. BLO and NAR recognize NCAR
is sponsored by the U.S. National Science Foundation (NSF) and computing
resources were provided by the Climate Simulation Laboratory at NCAR's
Computational and Information Systems Laboratory (CISL) sponsored by the
NSF and other agencies. AMH and AMD acknowledge research leading to
these results received funding from the European Research Council under
the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC
grant agreement no. 278636. AMD acknowledges the UK Natural Environment
Research Council for the provision of a Doctoral Training Grant. CS and
GL received funding from AWI and Helmholz through the programmes POLMAR,
PACES and REKLIM. WLC and AAO acknowledge financial support from the
Japan Society for the Promotion of Science and computing resources at
the Earth Simulator Center, JAMSTEC. This research used samples and/or
data provided by the Ocean Drilling Program (ODP). This is a product of
the PRISM Project.
NR 69
TC 39
Z9 39
U1 3
U2 49
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD JUN 18
PY 2013
VL 3
AR 2013
DI 10.1038/srep02013
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 165RJ
UT WOS:000320500900010
PM 23774736
ER
PT J
AU Chen, YJ
Birnbaum, KM
Hemmati, H
AF Chen, Yijiang
Birnbaum, Kevin M.
Hemmati, Hamid
TI Active laser ranging over planetary distances with millimeter accuracy
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID MARS; GRAVITY; INSTRUMENT; RELATIVITY; SUPERNOVAE; OPERATION; TRACKING;
APOLLO; TESTS
AB Precision laser ranging between planetary bodies will allow advances in the study of fundamental physics and solar system dynamics. Current precision ranging techniques based on retro-reflectors are limited to the Earth-Moon distance. We present a method of active laser ranging over interplanetary distances with asynchronous two-way ranging. The method is validated in real time laboratory experiments and field tests. Sub-millimeter accuracy has been achieved in real-time active laser ranging for interplanetary distances, providing precision improvement well above three orders of magnitude over the current RF techniques. An instrument developed with the approach and deployed in future planetary missions will significantly advance planetary sciences and fundamental physics. For example, implemented in a future Mars lander mission our approach will clarify the Mars interior (liquid or solid), which is still an open question due to limitation of RF ranging precision although extensive efforts have been made over years with numerous missions since 1970s. (C) 2013 AIP Publishing LLC.
C1 [Chen, Yijiang; Birnbaum, Kevin M.; Hemmati, Hamid] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Chen, YJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 33
TC 7
Z9 7
U1 2
U2 8
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 JUN 17
PY 2013
VL 102
IS 24
AR 241107
DI 10.1063/1.4810906
PG 5
WC Physics, Applied
SC Physics
GA 171XC
UT WOS:000320962400007
ER
PT J
AU Venturelli, D
Fazio, R
Giovannetti, V
AF Venturelli, Davide
Fazio, Rosario
Giovannetti, Vittorio
TI Minimal Self-Contained Quantum Refrigeration Machine Based on Four
Quantum Dots
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID ANDERSON; PHYSICS
AB We present a theoretical study of an electronic quantum refrigerator based on four quantum dots arranged in a square configuration, in contact with as many thermal reservoirs. We show that the system implements the minimal mechanism for acting as a self-contained quantum refrigerator, by demonstrating heat extraction from the coldest reservoir and the cooling of the nearby quantum dot.
C1 [Venturelli, Davide; Fazio, Rosario; Giovannetti, Vittorio] Scuola Normale Super Pisa, NEST, Piazza Cavalieri 7, I-56127 Pisa, Italy.
[Venturelli, Davide; Fazio, Rosario; Giovannetti, Vittorio] CNR, Ist Nanosci, I-56127 Pisa, Italy.
[Venturelli, Davide] NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab, Moffett Field, CA 94035 USA.
RP Venturelli, D (reprint author), Scuola Normale Super Pisa, NEST, Piazza Cavalieri 7, I-56127 Pisa, Italy.
RI Fazio, rosario/M-1742-2013;
OI Fazio, rosario/0000-0002-7793-179X; GIOVANNETTI,
VITTORIO/0000-0002-7636-9002
FU MIUR through the FIRB-IDEAS Project [RBID08B3FM]; EU through the Project
IP-SOLID; Sandia National Laboratories
FX We acknowledge useful discussions with C. W. J. Beenakker, M. Carroll,
F. Giazotto, F. Mazza, and J. Pekola and support from MIUR through the
FIRB-IDEAS Project No. RBID08B3FM, by the EU through the Project
IP-SOLID, and by Sandia National Laboratories.
NR 28
TC 40
Z9 40
U1 2
U2 17
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 JUN 17
PY 2013
VL 110
IS 25
AR 256801
DI 10.1103/PhysRevLett.110.256801
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 167EM
UT WOS:000320613800009
PM 23829751
ER
PT J
AU Kovalskyy, V
Henebry, GM
Roy, DP
Adusei, B
Hansen, M
Senay, G
Mocko, DM
AF Kovalskyy, V.
Henebry, G. M.
Roy, D. P.
Adusei, B.
Hansen, M.
Senay, G.
Mocko, D. M.
TI Evaluation of a coupled event-driven phenology and evapotranspiration
model for croplands in the United States northern Great Plains
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE comparison of modeled ET; phenology in ET
ID LAND-SURFACE MODEL; ASSIMILATION SYSTEM NLDAS; TIME-SERIES; MONITORING
VEGETATION; ENERGY-BALANCE; CLIMATE MODELS; SATELLITE DATA; MODIS;
RESOLUTION; SIMULATION
AB A new model coupling scheme with remote sensing data assimilation was developed for estimation of daily actual evapotranspiration (ET). The scheme consists of the VegET, a model to estimate ET from meteorological and water balance data, and an Event Driven Phenology Model (EDPM), an empirical crop specific model trained on multiple years of flux tower data transformed into six types of environmental forcings that are called events to emphasize their temporally discrete character, which has advantages for modeling multiple contingent influences. The EDPM in prognostic mode supplies seasonal trajectories of normalized difference vegetation index (NDVI); whereas in diagnostic mode, it can adjust the NDVI prediction with assimilated remotely sensed observations. The scheme was deployed within the croplands of the Northern Great Plains. The evaluation used 2007-2009 land surface forcing data from the North American Land Data Assimilation System and crop maps derived from remotely sensed data of NASA's Moderate Resolution Imaging Spectroradiometer (MODIS). We compared the NDVI produced by the EDPM with NDVI data derived from the MODIS nadir bidirectional reflectance distribution function adjusted reflectance product. The EDPM performance in prognostic mode yielded a coefficient of determination (r(2)) of 0.80.15and the root mean square error (RMSE) of 0.10.035 across the entire study area. Retrospective correction of canopy attributes using assimilated MODIS NDVI values improved EDPM NDVI estimates, bringing the errors down to the average level of 0.1. The ET estimates produced by the coupled scheme were compared with the MODIS evapotranspiration product and with ET from NASA's Mosaic land surface model. The expected r(2)=0.70.15 and RMSE=11.24mm per 8days achieved in earlier point-based validations were met in this study by the coupling scheme functioning in both prognostic and retrospective modes. Coupled model performance was diminished at the periphery of the study area where r(2) values were about 0.5 and RMSEs up to 15 +/- 5mm per 8days. This performance degradation can be attributed both to insufficient EDPM training and to spatial heterogeneity in the accuracy of the crop maps. Overall, the experiment provided sufficient evidence of soundness of the EDPM and VegET coupling scheme, assuring its potential for spatially explicit applications.
C1 [Kovalskyy, V.; Henebry, G. M.; Roy, D. P.; Adusei, B.; Hansen, M.] S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA.
[Senay, G.] US Geol Survey, Ctr Earth Resources Observat & Sci, Sioux Falls, SD USA.
[Mocko, D. M.] NASA Goddard Space Flight Ctr, SAIC Hydrol Sci Lab, Greenbelt, MD USA.
[Mocko, D. M.] NASA Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
RP Kovalskyy, V (reprint author), S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA.
EM Valeriy.Kovalskyy@sdstate.edu
OI Henebry, Geoffrey/0000-0002-8999-2709
FU NASA [NNX07AT61A, NNH07ZDA001N, NNX08AL93A]
FX This research was supported in part by NASA grants NNX07AT61A,
NNH07ZDA001N, and NNX08AL93A. The NLDAS data used in this study were
acquired as part of the activities of NASA's Science Mission
Directorate, archived, and distributed by the Goddard Earth Sciences
(GES) Data and Information Services Center (DISC). The authors are also
grateful to the two anonymous reviewers for insightful comments and
suggestions to improve the clarity of this manuscript.
NR 75
TC 2
Z9 2
U1 1
U2 15
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 JUN 16
PY 2013
VL 118
IS 11
BP 5065
EP 5081
DI 10.1002/jgrd.50387
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600001
ER
PT J
AU Prive, NC
Errico, RM
Tai, KS
AF Prive, N. C.
Errico, R. M.
Tai, K. -S.
TI The influence of observation errors on analysis error and forecast skill
investigated with an observing system simulation experiment
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE data assimilation; observing system simulation experiment; observation
error
ID ATMOSPHERIC DATA ASSIMILATION; IMPACT; PREDICTABILITY; SENSITIVITY;
MODELS
AB The National Aeronautics and Space Administration Global Modeling and Assimilation Office (NASA/GMAO) observing system simulation experiment (OSSE) framework is used to explore the response of analysis error and forecast skill to observation quality. In an OSSE, synthetic observations may be created that have much smaller error than real observations, and precisely quantified error may be applied to these synthetic observations. Three experiments are performed in which synthetic observations with magnitudes of applied observation error that vary from zero to twice the estimated realistic error are ingested into the Goddard Earth Observing System Model (GEOS-5) with Gridpoint Statistical Interpolation (GSI) data assimilation for a 1month period representing July. The analysis increment and observation innovation are strongly impacted by observation error, with much larger variances for increased observation error. The analysis quality is degraded by increased observation error, but the change in root-mean-square error of the analysis state is small relative to the total analysis error. Surprisingly, in the 120h forecast, increased observation error only yields a slight decline in forecast skill in the extratropics and no discernible degradation of forecast skill in thetropics.
C1 [Prive, N. C.; Errico, R. M.] Morgan State Univ, Goddard Earth Sci Technol & Res Ctr, Baltimore, MD 21239 USA.
[Tai, K. -S.] Sci Syst & Applicat Inc, Greenbelt, MD USA.
[Prive, N. C.; Errico, R. M.; Tai, K. -S.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Prive, NC (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM nikki.prive@nasa.gov
OI Prive, Nikki/0000-0001-8309-8741
FU GMAO
FX The ECMWF Nature Run was provided by Erik Andersson through arrangements
made by Michiko Masutani. Support for this project was encouraged by
Michele Rienecker and provided by GMAO core funding.
NR 21
TC 7
Z9 7
U1 0
U2 3
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 JUN 16
PY 2013
VL 118
IS 11
BP 5332
EP 5346
DI 10.1002/jgrd.50452
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600021
ER
PT J
AU Jensen, EJ
Lawson, RP
Bergman, JW
Pfister, L
Bui, TP
Schmitt, CG
AF Jensen, E. J.
Lawson, R. P.
Bergman, J. W.
Pfister, L.
Bui, T. P.
Schmitt, C. G.
TI Physical processes controlling ice concentrations in synoptically
forced, midlatitude cirrus
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE cirrus
ID CLOUD FORMATION; AEROSOLS; NUCLEATION; NUCLEI; PARAMETERIZATION;
SIMULATIONS; MODEL; TEMPERATURE; SENSITIVITY; DENSITIES
AB Numerical simulations and airborne measurements are used to evaluate the impact of physical processes on synoptically forced, midlatitude cirrus ice concentrations. The agreement within a factor of 2 between ice concentrations measured with independent techniques (replicators and optical imaging probes) provides confidence in the accuracy of the in situ measurements. We use a computationally efficient modeling approach that incorporates the key cirrus physical processes, such that thousands of cloud cases can be simulated and the model results can be statistically compared with observations. One-dimensional simulations with detailed treatments of cloud microphysical processes are driven by temperatures and vertical winds extracted from meteorological analyses. Small-scale temperature and vertical wind perturbations associated with mesoscale waves are superimposed on the analysis fields. We find that in simulations with only homogeneous freezing nucleation, ice concentration statistics are very sensitive to the specified mesoscale wave vertical wind perturbations. With the frequency distribution of vertical winds adjusted to agree with aircraft observations, we obtain good agreement between the simulated and observed ice concentration frequency distributions. Both the observations and simulations indicate that relatively high ice concentrations (1000L(-1)) occur rarely in these clouds (less than 1% of the time). Simulations including both homogeneous and heterogeneous nucleation indicate that even with moderate concentrations of ice nuclei (20L(-1)), heterogeneous nucleation is an important ice production process, particularly for relatively low ice concentrations and warm temperatures. With enhanced ice nuclei concentrations (100L(-1)), heterogeneous nucleation dominates ice production in the model. We find that it is critically important to include the impact of sedimentation on the evolution of ice concentrations when comparing model results with observations. Ice crystal collection efficiencies are poorly constrained at low temperatures, and we find that aggregation can significantly reduce ice concentrations. Sensitivity tests indicate that neither the agreement between observed and simulated ice crystal statistics nor the sensitivities indicated by the simulations are significantly affected by model assumptions such as the time periods simulated, geographic domain covered, trajectory paths calculated, or ice crystal habit assumed.
C1 [Jensen, E. J.; Pfister, L.; Bui, T. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bergman, J. W.] Bay Area Environm Res Inst, Sonoma, CA USA.
[Lawson, R. P.] Spec Inc, Boulder, CO USA.
[Bergman, J. W.; Schmitt, C. G.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Jensen, EJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM eric.j.jensen@nasa.gov
RI Schmitt, Carl/P-5490-2015;
OI Schmitt, Carl/0000-0003-3829-6970
FU NASA Radiation Science Programs; DOE Atmospheric System Research Program
FX This work was supported by the NASA Radiation Science Programs and the
DOE Atmospheric System Research Program.
NR 39
TC 21
Z9 21
U1 1
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 16
PY 2013
VL 118
IS 11
BP 5348
EP 5360
DI 10.1002/jgrd.50421
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600023
ER
PT J
AU Bond, TC
Doherty, SJ
Fahey, DW
Forster, PM
Berntsen, T
DeAngelo, BJ
Flanner, MG
Ghan, S
Karcher, B
Koch, D
Kinne, S
Kondo, Y
Quinn, PK
Sarofim, MC
Schultz, MG
Schulz, M
Venkataraman, C
Zhang, H
Zhang, S
Bellouin, N
Guttikunda, SK
Hopke, PK
Jacobson, MZ
Kaiser, JW
Klimont, Z
Lohmann, U
Schwarz, JP
Shindell, D
Storelvmo, T
Warren, SG
Zender, CS
AF Bond, T. C.
Doherty, S. J.
Fahey, D. W.
Forster, P. M.
Berntsen, T.
DeAngelo, B. J.
Flanner, M. G.
Ghan, S.
Kaercher, B.
Koch, D.
Kinne, S.
Kondo, Y.
Quinn, P. K.
Sarofim, M. C.
Schultz, M. G.
Schulz, M.
Venkataraman, C.
Zhang, H.
Zhang, S.
Bellouin, N.
Guttikunda, S. K.
Hopke, P. K.
Jacobson, M. Z.
Kaiser, J. W.
Klimont, Z.
Lohmann, U.
Schwarz, J. P.
Shindell, D.
Storelvmo, T.
Warren, S. G.
Zender, C. S.
TI Bounding the role of black carbon in the climate system: A scientific
assessment
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Review
DE black carbon; climate forcing; aerosol
ID AEROSOL LIGHT-ABSORPTION; GENERAL-CIRCULATION MODEL; BIOMASS BURNING
EMISSIONS; CIRRUS CLOUD FORMATION; GREENHOUSE-GAS EMISSIONS; AIRBORNE
PARTICULATE MATTER; GLOBAL WARMING POTENTIALS; INDIAN-OCEAN EXPERIMENT;
FOSSIL-FUEL COMBUSTION; CHEMICAL MASS-BALANCE
AB Black carbon aerosol plays a unique and important role in Earth's climate system. Black carbon is a type of carbonaceous material with a unique combination of physical properties. This assessment provides an evaluation of black-carbon climate forcing that is comprehensive in its inclusion of all known and relevant processes and that is quantitative in providing best estimates and uncertainties of the main forcing terms: direct solar absorption; influence on liquid, mixed phase, and ice clouds; and deposition on snow and ice. These effects are calculated with climate models, but when possible, they are evaluated with both microphysical measurements and field observations. Predominant sources are combustion related, namely, fossil fuels for transportation, solid fuels for industrial and residential uses, and open burning of biomass. Total global emissions of black carbon using bottom-up inventory methods are 7500 Gg yr(-1) in the year 2000 with an uncertainty range of 2000 to 29000. However, global atmospheric absorption attributable to black carbon is too low in many models and should be increased by a factor of almost 3. After this scaling, the best estimate for the industrial-era (1750 to 2005) direct radiative forcing of atmospheric black carbon is +0.71 W m(-2) with 90% uncertainty bounds of (+0.08, +1.27) W m(-2). Total direct forcing by all black carbon sources, without subtracting the preindustrial background, is estimated as +0.88 (+0.17, +1.48) W m(-2). Direct radiative forcing alone does not capture important rapid adjustment mechanisms. A framework is described and used for quantifying climate forcings, including rapid adjustments. The best estimate of industrial-era climate forcing of black carbon through all forcing mechanisms, including clouds and cryosphere forcing, is +1.1 W m(-2) with 90% uncertainty bounds of +0.17 to +2.1 W m(-2). Thus, there is a very high probability that black carbon emissions, independent of co-emitted species, have a positive forcing and warm the climate. We estimate that black carbon, with a total climate forcing of +1.1 W m(-2), is the second most important human emission in terms of its climate forcing in the present-day atmosphere; only carbon dioxide is estimated to have a greater forcing. Sources that emit black carbon also emit other short-lived species that may either cool or warm climate. Climate forcings from co-emitted species are estimated and used in the framework described herein. When the principal effects of short-lived co-emissions, including cooling agents such as sulfur dioxide, are included in net forcing, energy-related sources (fossil fuel and biofuel) have an industrial-era climate forcing of +0.22 (-0.50 to +1.08) W m(-2) during the first year after emission. For a few of these sources, such as diesel engines and possibly residential biofuels, warming is strong enough that eliminating all short-lived emissions from these sources would reduce net climate forcing (i.e., produce cooling). When open burning emissions, which emit high levels of organic matter, are included in the total, the best estimate of net industrial-era climate forcing by all short-lived species from black-carbon-rich sources becomes slightly negative (-0.06 W m(-2) with 90% uncertainty bounds of -1.45 to +1.29 W m(-2)).
The uncertainties in net climate forcing from black-carbon-rich sources are substantial, largely due to lack of knowledge about cloud interactions with both black carbon and co-emitted organic carbon. In prioritizing potential black-carbon mitigation actions, non-science factors, such as technical feasibility, costs, policy design, and implementation feasibility play important roles. The major sources of black carbon are presently in different stages with regard to the feasibility for near-term mitigation. This assessment, by evaluating the large number and complexity of the associated physical and radiative processes in black-carbon climate forcing, sets a baseline from which to improve future climate forcing estimates.
C1 [Bond, T. C.] Univ Illinois, Urbana, IL 61801 USA.
[Doherty, S. J.] Univ Washington, Joint Inst Study Atmosphere & Ocean, Seattle, WA 98195 USA.
[Fahey, D. W.; Schwarz, J. P.] Univ Colorado, NOAA Earth Syst Res Lab, Boulder, CO 80309 USA.
[Fahey, D. W.; Schwarz, J. P.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Forster, P. M.] Univ Leeds, Leeds, W Yorkshire, England.
[Berntsen, T.] Univ Oslo, Ctr Int Climate & Environm Res Oslo, Oslo, Norway.
[Berntsen, T.] Univ Oslo, Dept Geosci, Oslo, Norway.
[DeAngelo, B. J.; Sarofim, M. C.] US EPA, Washington, DC 20460 USA.
[Flanner, M. G.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Ghan, S.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Kaercher, B.] Deutsch Zentrum Luft & Raumfahrt Oberpfaffenhofen, Wessling, Germany.
[Koch, D.] US DOE, Washington, DC 20585 USA.
[Kinne, S.] Max Planck Inst, Hamburg, Germany.
[Kondo, Y.] Univ Tokyo, Tokyo, Japan.
[Quinn, P. K.] NOAA Pacific Marine Environm Lab, Seattle, WA USA.
[Schultz, M. G.] Forschungszentrum Julich, D-52425 Julich, Germany.
[Schulz, M.] Norwegian Meteorol Inst, Oslo, Norway.
[Venkataraman, C.] Indian Inst Technol, Bombay 400076, Maharashtra, India.
[Zhang, H.] China Meteorol Adm, Beijing, Peoples R China.
[Zhang, S.] Peking Univ, Beijing 100871, Peoples R China.
[Bellouin, N.] Met Off Hadley Ctr, Exeter, Devon, England.
[Guttikunda, S. K.] Univ Nevada, Desert Res Inst, Div Atmospher Sci, Reno, NV 89506 USA.
[Hopke, P. K.] Clarkson Univ, Potsdam, NY USA.
[Jacobson, M. Z.] Stanford Univ, Stanford, CA 94305 USA.
[Kaiser, J. W.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Kaiser, J. W.] Kings Coll London, London, England.
[Kaiser, J. W.] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Klimont, Z.] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria.
[Lohmann, U.] ETH, Zurich, Switzerland.
[Shindell, D.] NASA Goddard Inst Space Studies, New York, NY USA.
[Storelvmo, T.] Yale Univ, New Haven, CT USA.
[Warren, S. G.] Univ Washington, Seattle, WA 98195 USA.
[Zender, C. S.] Univ Calif Irvine, Irvine, CA USA.
RP Bond, TC (reprint author), Univ Illinois, Urbana, IL 61801 USA.
EM yark@uiuc.edu
RI Fahey, David/G-4499-2013; Quinn, Patricia/R-1493-2016; Forster,
Piers/F-9829-2010; Schultz, Martin/I-9512-2012; Manager, CSD
Publications/B-2789-2015; Zender, Charles/D-4485-2012; schwarz,
joshua/G-4556-2013; Flanner, Mark/C-6139-2011; Kaiser,
Johannes/A-7057-2012; Shindell, Drew/D-4636-2012; Karcher,
Bernd/D-5325-2014; Kondo, Yutaka/D-1459-2012; Bond, Tami/A-1317-2013;
Doherty, Sarah/D-5592-2015; Lohmann, Ulrike/B-6153-2009; Schulz,
Michael/A-6930-2011; Klimont, Zbigniew/P-7641-2015; Ghan,
Steven/H-4301-2011; Hopke, Philip/C-6020-2008
OI Fahey, David/0000-0003-1720-0634; Quinn, Patricia/0000-0003-0337-4895;
Forster, Piers/0000-0002-6078-0171; Schultz, Martin/0000-0003-3455-774X;
Zender, Charles/0000-0003-0129-8024; schwarz,
joshua/0000-0002-9123-2223; Flanner, Mark/0000-0003-4012-174X; Kaiser,
Johannes/0000-0003-3696-9123; Karcher, Bernd/0000-0003-0278-4980; Bond,
Tami/0000-0001-5968-8928; Doherty, Sarah/0000-0002-7796-6968; Lohmann,
Ulrike/0000-0001-8885-3785; Schulz, Michael/0000-0003-4493-4158;
Klimont, Zbigniew/0000-0003-2630-198X; Ghan, Steven/0000-0001-8355-8699;
Hopke, Philip/0000-0003-2367-9661
FU International Global Atmospheric Chemistry (IGAC) project; Climate
Program Office of the National Oceanic and Atmospheric Administration
(NOAA); Radiation Sciences Program of the National Aeronautic and Space
Administration (NASA); CSC; Tully Graphics; IGAC via the Joint Institute
for the Study of the Atmosphere and Ocean (JISAO) under NOAA
[NA10OAR4320148, 2035]; U.S. EPA [RD-83503401]; NASA [RD-83503401]; NSF
[ATM 08-52775]; DOE [DE-SC0006689, DE-AC06-76RLO 1830]; Royal Society
Wolfson Research Merit award; Joint DECC/Defra Met Office Hadley Centre
Climate Programme [GA01101]; U.S. Department of Energy (DOE), Office of
Science, Scientific Discovery through Advanced Computing (SciDAC)
program; DOE Decadal and Regional Climate Prediction using Earth System
Models (EaSM) program; Ministry of Education, Culture, Sports, Science,
and Technology (MEXT); Japan Science and Technology Agency (JST); global
environment research fund of the Japanese Ministry of the Environment
[A-1101]; EUCAARI project (EU-FP6) [34684]; U.S. National Science
Foundation; European Union Seventh Research Framework Programme (MACC
project) [218793]; U.S. NSF [ARC-06-12636]; National Basic Research
Program of China [2011CB403405]
FX This assessment is a contribution of the IGBP-IGAC/WCRP-SPARC
Atmospheric Chemistry and Climate Initiative (AC&C). The authors
acknowledge financial and technical support from the International
Global Atmospheric Chemistry (IGAC) project
(http://igac.jisao.washington.edu/index.php), C. Koblinsky of the
Climate Program Office of the National Oceanic and Atmospheric
Administration (NOAA), H. Maring of the Radiation Sciences Program of
the National Aeronautic and Space Administration (NASA), Rose Kendall of
CSC, and Beth Tully of Tully Graphics. IGAC funding for this project is
via the Joint Institute for the Study of the Atmosphere and Ocean
(JISAO) under NOAA Cooperative Agreement NA10OAR4320148, Contribution
No. 2035. The authors are grateful to Ray Minjares and the International
Council on Clean Transportation (ICCT) and Catherine Witherspoon of the
ClimateWorks Foundation for encouragement to undertake this effort. The
authors wish to thank the AeroCom modeling community and the AERONET
data providers for their great help in providing basic data sets,
further analyzed here. Olivier Boucher is thanked for his substantial
contribution to section 9 and his careful review and subsequent
discussion with the author team on the entire manuscript. We also thank
N. Riemer of the University of Illinois for particle-resolved simulation
results in Figure 6, N. Mahowald of Cornell University for dust fields
in Figure 12, and D. M. Winker of NASA for providing the CALIPSO data in
Figure 16. A. Heil is thanked for providing information on biomass fuel
loads and M. O. Andreae for providing updates of his biomass burning
emission factor compilation. E. Baum, J. Bachmann, R. Minjares, K. Ram,
V. Ramanathan, and D. Zaelke are thanked for reading and providing
comments that improved the document. T. C. Bond acknowledges support for
related work under U.S. EPA RD-83503401, NASA RD-83503401, NSF ATM
08-52775, and DOE DE-SC0006689. Piers Forster acknowledges support from
a Royal Society Wolfson Research Merit award. N. Bellouin was supported
by the Joint DECC/Defra Met Office Hadley Centre Climate Programme
(GA01101). S. Ghan was supported by the U.S. Department of Energy (DOE),
Office of Science, Scientific Discovery through Advanced Computing
(SciDAC) program, and the DOE Decadal and Regional Climate Prediction
using Earth System Models (EaSM) program. The Pacific Northwest National
Laboratory is operated for the DOE by Battelle Memorial Institute under
contract DE-AC06-76RLO 1830. Y. Kondo was supported by the Ministry of
Education, Culture, Sports, Science, and Technology (MEXT), strategic
international cooperative program of Japan Science and Technology Agency
(JST), and the global environment research fund of the Japanese Ministry
of the Environment (A-1101). For P. K. Quinn's work, this is NOAA PMEL
contribution no. 3786. M. Schulz received funding support through the
EUCAARI project (EU-FP6 Contract 34684). M. Z. Jacobson received funding
from the U.S. National Science Foundation. J. W. Kaiser was supported by
the European Union Seventh Research Framework Programme (MACC project,
contract number 218793). S. G. Warren acknowledges support from U.S. NSF
grant ARC-06-12636. H. Zhang was funded by the National Basic Research
Program of China (2011CB403405). The views expressed in this paper are
those of the authors and do not necessarily reflect the views or
policies of the U.S. Environmental Protection Agency.
NR 867
TC 936
Z9 961
U1 126
U2 719
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 JUN 16
PY 2013
VL 118
IS 11
BP 5380
EP 5552
DI 10.1002/jgrd.50171
PG 173
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600025
ER
PT J
AU van Donkelaar, A
Martin, RV
Spurr, RJD
Drury, E
Remer, LA
Levy, RC
Wang, J
AF van Donkelaar, Aaron
Martin, Randall V.
Spurr, Robert J. D.
Drury, Easan
Remer, Lorraine A.
Levy, Robert C.
Wang, Jun
TI Optimal estimation for global ground-level fine particulate matter
concentrations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE PM2.5; AOD; Optimal Estimation; AERONET; CALIOP; MODIS
ID AEROSOL OPTICAL DEPTH; UNITED-STATES; AIR-POLLUTION; SATELLITE
RETRIEVALS; RADIATIVE-TRANSFER; ALGORITHM; PM2.5; REFLECTANCE; LONG;
VISIBILITY
AB We develop an optimal estimation (OE) algorithm based on top-of-atmosphere reflectances observed by the MODIS satellite instrument to retrieve near-surface fine particulate matter (PM2.5). The GEOS-Chem chemical transport model is used to provide prior information for the Aerosol Optical Depth (AOD) retrieval and to relate total column AOD to PM2.5. We adjust the shape of the GEOS-Chem relative vertical extinction profiles by comparison with lidar retrievals from the CALIOP satellite instrument. Surface reflectance relationships used in the OE algorithm are indexed by land type. Error quantities needed for this OE algorithm are inferred by comparison with AOD observations taken by a worldwide network of sun photometers (AERONET) and extended globally based upon aerosol speciation and cross correlation for simulated values, and upon land type for observational values. Significant agreement in PM2.5 is found over North America for 2005 (slope=0.89; r=0.82; 1-sigma error=1 mu g/m(3)+27%), with improved coverage and correlation relative to previous work for the same region and time period, although certain subregions, such as the San Joaquin Valley of California are better represented by previous estimates. Independently derived error estimates of the OE PM2.5 values at in situ locations over North America (of (2.5 mu g/m(3)+31%) and Europe of (3.5 mu g/m(3)+30%) are corroborated by comparison with in situ observations, although globally (error estimates of (3.0 mu g/m(3)+35%), may be underestimated. Global population-weighted PM2.5 at 50% relative humidity is estimated as 27.8 mu g/m(3) at 0.1 degrees x0.1 degrees resolution.
C1 [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Spurr, Robert J. D.] RT Solut Inc, Cambridge, MA USA.
[Drury, Easan] Natl Renewable Energy Lab, Golden, CO USA.
[Remer, Lorraine A.] Univ Maryland, JCET, Baltimore, MD 21201 USA.
[Levy, Robert C.] Inc Lanham, Sci Syst & Applicat, Greenbelt, MD USA.
[Levy, Robert C.] NASA, Goddard Space Flight Ctr, Earth Sci Div, Greenbelt, MD 20771 USA.
[Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA.
RP van Donkelaar, A (reprint author), Dalhousie Univ, 6300 Coburg Rd, Halifax, NS B3H 3J5, Canada.
EM Aaron.van.Donkelaar@dal.ca
RI Levy, Robert/M-7764-2013; Martin, Randall/C-1205-2014; Chem,
GEOS/C-5595-2014; Wang, Jun/A-2977-2008
OI Levy, Robert/0000-0002-8933-5303; Martin, Randall/0000-0003-2632-8402;
Wang, Jun/0000-0002-7334-0490
FU Health Canada; Natural Sciences and Engineering Research Council of
Canada
FX We are grateful to the CALIOP, AERONET, NAPS, and AQS teams for making
available data used here. This work was funded by Health Canada and the
Natural Sciences and Engineering Research Council of Canada.
NR 63
TC 32
Z9 32
U1 7
U2 44
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 JUN 16
PY 2013
VL 118
IS 11
BP 5621
EP 5636
DI 10.1002/jgrd.50479
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600030
ER
PT J
AU Mlynczak, MG
Hunt, LA
Mast, JC
Marshall, BT
Russell, JM
Smith, AK
Siskind, DE
Yee, JH
Mertens, CJ
Martin-Torres, FJ
Thompson, RE
Drob, DP
Gordley, LL
AF Mlynczak, Martin G.
Hunt, Linda A.
Mast, Jeffrey C.
Marshall, B. Thomas
Russell, James M., III
Smith, Anne K.
Siskind, David E.
Yee, Jeng-Hwa
Mertens, Christopher J.
Martin-Torres, F. Javier
Thompson, R. Earl
Drob, Douglas P.
Gordley, Larry L.
TI Atomic oxygen in the mesosphere and lower thermosphere derived from
SABER: Algorithm theoretical basis and measurement uncertainty
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Atomic oxygen; Mesopause; Airglow; Ozone; Energy budget
ID VIBRATIONALLY EXCITED OH; KINETIC-PARAMETERS; MIDDLE ATMOSPHERE;
HYDROXYL AIRGLOW; MOLECULAR-OXYGEN; LOWER IONOSPHERE; MU-M; NIGHTGLOW;
OZONE; ROCKET
AB Atomic oxygen (O) is a fundamental component in chemical aeronomy of Earth's mesosphere and lower thermosphere region extending from approximately 50km to over 100km in altitude. Atomic oxygen is notoriously difficult to measure, especially with remote sensing techniques from orbiting satellite sensors. It is typically inferred from measurements of the ozone concentration in the day or from measurements of the Meinel band emission of the hydroxyl radical (OH) at night. The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on the NASA Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics (TIMED) satellite measures OH emission and ozone for the purpose of determining the O-atom concentration. In this paper, we present the algorithms used in the derivation of day and night atomic oxygen from these measurements. We find excellent consistency between the day and night O-atom concentrations from daily to annual time scales. We also examine in detail the collisional relaxation of the highly vibrationally excited OH molecule at night measured by SABER. Large rate coefficients for collisional removal of vibrationally excited OH molecules by atomic oxygen are consistent with the SABER observations if the deactivation of OH(9) proceeds solely by collisional quenching. An uncertainty analysis of the derived atomic oxygen is also given. Uncertainty in the rate coefficient for recombination of O and molecular oxygen is shown to be the largest source of uncertainty in the derivation of atomic oxygen day or night.
C1 [Mlynczak, Martin G.; Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Hunt, Linda A.; Mast, Jeffrey C.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Marshall, B. Thomas; Thompson, R. Earl; Gordley, Larry L.] G&A Tech Software, Newport News, VA USA.
[Russell, James M., III] Hampton Univ, Hampton, VA 23668 USA.
[Smith, Anne K.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Siskind, David E.; Drob, Douglas P.] Naval Res Lab, Washington, DE USA.
[Yee, Jeng-Hwa] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Martin-Torres, F. Javier] Ctr Astrobiol CSIC INTA, Madrid, Spain.
RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM m.g.mlynczak@nasa.gov
RI Drob, Douglas/G-4061-2014; Martin-Torres, Francisco Javier/G-6329-2015
OI Drob, Douglas/0000-0002-2045-7740; Martin-Torres, Francisco
Javier/0000-0001-6479-2236
NR 46
TC 25
Z9 25
U1 3
U2 15
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 JUN 16
PY 2013
VL 118
IS 11
BP 5724
EP 5735
DI 10.1002/jgrd.50401
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600037
ER
PT J
AU Imai, K
Manago, N
Mitsuda, C
Naito, Y
Nishimoto, E
Sakazaki, T
Fujiwara, M
Froidevaux, L
von Clarmann, T
Stiller, GP
Murtagh, DP
Rong, PP
Mlynczak, MG
Walker, KA
Kinnison, DE
Akiyoshi, H
Nakamura, T
Miyasaka, T
Nishibori, T
Mizobuchi, S
Kikuchi, K
Ozeki, H
Takahashi, C
Hayashi, H
Sano, T
Suzuki, M
Takayanagi, M
Shiotani, M
AF Imai, Koji
Manago, Naohiro
Mitsuda, Chihiro
Naito, Yoko
Nishimoto, Eriko
Sakazaki, Takatoshi
Fujiwara, Masatomo
Froidevaux, Lucien
von clarmann, Thomas
Stiller, Gabriele P.
Murtagh, Donal P.
Rong, Ping-ping
Mlynczak, Martin G.
Walker, Kaley A.
Kinnison, Douglas E.
Akiyoshi, Hideharu
Nakamura, Tetsu
Miyasaka, Takayuki
Nishibori, Toshiyuki
Mizobuchi, Satoko
Kikuchi, Ken-ichi
Ozeki, Hiroyuki
Takahashi, Chikako
Hayashi, Hiroo
Sano, Takuki
Suzuki, Makoto
Takayanagi, Masahiro
Shiotani, Masato
TI Validation of ozone data from the Superconducting Submillimeter-Wave
Limb-Emission Sounder (SMILES)
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE middle atmosphere; atmospheric composition; ozone chemistry; atmospheric
transport
ID CHEMISTRY EXPERIMENT ACE; ATMOSPHERIC CHEMISTRY; MIPAS; TEMPERATURE;
RETRIEVAL; PROFILES; STRATOSPHERE; JEM/SMILES; RADIOMETER; MODEL
AB The Superconducting Submillimeter-Wave Limb-Emission Sounder (SMILES) onboard the International Space Station provided global measurements of ozone profiles in the middle atmosphere from 12 October 2009 to 21 April 2010. We present validation studies of the SMILES version 2.1 ozone product based on coincidence statistics with satellite observations and outputs of chemistry and transport models (CTMs). Comparisons of the stratospheric ozone with correlative data show agreements that are generally within 10%. In the mesosphere, the agreement is also good and better than 30% even at a high altitude of 73km, and the SMILES measurements with their local time coverage also capture the diurnal variability very well. The recommended altitude range for scientific use is from 16 to 73km. We note that the SMILES ozone values for altitude above 26km are smaller than some of the correlative satellite datasets; conversely the SMILES values in the lower stratosphere tend to be larger than correlative data, particularly in the tropics, with less than 8% difference below similar to 24km. The larger values in the lower stratosphere are probably due to departure of retrieval results between two detection bands at altitudes below 28km; it is similar to 3% at 24km and is increasing rapidly down below.
C1 [Imai, Koji; Nishibori, Toshiyuki; Sano, Takuki; Suzuki, Makoto; Takayanagi, Masahiro; Shiotani, Masato] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Manago, Naohiro] Chiba Univ, Ctr Environm Remote Sensing, Chiba, Japan.
[Mitsuda, Chihiro; Miyasaka, Takayuki; Takahashi, Chikako; Hayashi, Hiroo] Fujitsu FIP Corp, Tokyo, Japan.
[Naito, Yoko; Nishimoto, Eriko] Kyoto Univ, Fac Sci, Kyoto, Japan.
[Sakazaki, Takatoshi; Fujiwara, Masatomo] Hokkaido Univ, Grad Sch Environm Sci, Sapporo, Hokkaido, Japan.
[Froidevaux, Lucien] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[von clarmann, Thomas; Stiller, Gabriele P.] Karlsruhe Inst Technol, Inst Meteorol & Klimaforsch, D-76021 Karlsruhe, Germany.
[Murtagh, Donal P.] Chalmers, Dept Radio & Space Sci, S-41296 Gothenburg, Sweden.
[Rong, Ping-ping; Mlynczak, Martin G.] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Walker, Kaley A.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Walker, Kaley A.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Kinnison, Douglas E.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Akiyoshi, Hideharu; Nakamura, Tetsu] Natl Inst Environm Studies, Ctr Global Environm Res, Tsukuba, Ibaraki, Japan.
[Nakamura, Tetsu] Natl Inst Polar Res, Arctic Environm Res Ctr, Tachikawa, Tokyo, Japan.
[Mizobuchi, Satoko] Syst Engn Consultants Co LTD, Tokyo, Japan.
[Kikuchi, Ken-ichi] Natl Inst Informat & Communicat Technol, Appl Electromagnet Res Inst, Koganei, Tokyo, Japan.
[Ozeki, Hiroyuki] Toho Univ, Fac Sci, Dept Environm Sci, Funabashi, Chiba 274, Japan.
[Shiotani, Masato] Kyoto Univ, Res Inst Sustainable Humanosphere, Uji, Kyoto, Japan.
RP Imai, K (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
EM imai.koji@jaxa.jp
RI Kikuchi, Kenichi/H-3382-2011; Stiller, Gabriele/A-7340-2013; Nakamura,
Tetsu/M-7914-2015; Murtagh, Donal/F-8694-2011
OI Kikuchi, Kenichi/0000-0002-2088-0717; Stiller,
Gabriele/0000-0003-2883-6873; Nakamura, Tetsu/0000-0002-2056-7392;
Murtagh, Donal/0000-0003-1539-3559
FU Japanese Ministry of Education, Culture, Sports, Science and Technology
(MEXT) [22310010]; ISS Science Project Office of ISAS/JAXA; Global
Environment Research Fund of the Japanese Ministry of the Environment
[A-0903]; Canadian Space Agency; Natural Sciences and Engineering
Research Council of Canada; U.S. National Science Foundation
FX This study was supported in part by the Japanese Ministry of Education,
Culture, Sports, Science and Technology (MEXT) through a Grant-in-Aid
for Scientific Research (22310010), the ISS Science Project Office of
ISAS/JAXA, and the Global Environment Research Fund of the Japanese
Ministry of the Environment (A-0903). SMILES data obtained from Data
Archives and Transmission System (DARTS), provided by Center for
Science-satellite Operation and Data Archive (C-SODA) at ISAS/JAXA. The
Atmospheric Chemistry Experiment (ACE), also known as SCISAT, is a
Canadian-led mission mainly supported by the Canadian Space Agency and
the Natural Sciences and Engineering Research Council of Canada.
Computations for MIROC3.2-CTM were made on the NEC SX-8R computers at
the Center for Global Environmental Research (CGER), National Institute
for Environmental Studies (NIES). The authors also thank the MIROC model
development group at AORI in the University of Tokyo, JAMSTEC, and NIES,
and K. Sudo in Nagoya University. The National Center for Atmospheric
Research (NCAR) is sponsored by U.S. National Science Foundation.
NR 70
TC 15
Z9 16
U1 1
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 16
PY 2013
VL 118
IS 11
BP 5750
EP 5769
DI 10.1002/jgrd.50434
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600039
ER
PT J
AU Ren, XR
van Duin, D
Cazorla, M
Chen, S
Mao, JQ
Zhang, L
Brune, WH
Flynn, JH
Grossberg, N
Lefer, BL
Rappengluck, B
Wong, KW
Tsai, C
Stutz, J
Dibb, JE
Jobson, BT
Luke, WT
Kelley, P
AF Ren, Xinrong
van Duin, Diana
Cazorla, Maria
Chen, Shuang
Mao, Jingqiu
Zhang, Li
Brune, William H.
Flynn, James H.
Grossberg, Nicole
Lefer, Barry L.
Rappenglueck, Bernhard
Wong, Kam W.
Tsai, Catalina
Stutz, Jochen
Dibb, Jack E.
Jobson, B. Thomas
Luke, Winston T.
Kelley, Paul
TI Atmospheric oxidation chemistry and ozone production: Results from SHARP
2009 in Houston, Texas
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Photochemsitry; Ozone Production; Houston; SHARP
ID LASER-INDUCED FLUORESCENCE; VOLATILE ORGANIC-COMPOUNDS; MASTER CHEMICAL
MECHANISM; PEROXY RADICAL CHEMISTRY; MISSING OH SOURCE; MCM V3 PART; HO2
CONCENTRATIONS; TROPOSPHERIC DEGRADATION; FIELD CAMPAIGN; MODELED OH
AB Ozone (O-3) and secondary fine particles come from the atmospheric oxidation chemistry that involves the hydroxyl radical (OH) and hydroperoxyl radical (HO2), which are together called HOx. Radical precursors such as nitrous acid (HONO) and formaldehyde (HCHO) significantly affect the HOx budget in urban environments. These chemical processes connect surface anthropogenic and natural emissions to local and regional air pollution. Using the data collected during the Study of Houston Atmospheric Radical Precursors (SHARP) in spring 2009, we examine atmospheric oxidation chemistry and O-3 production in this polluted urban environment. A numerical box model with five different chemical mechanisms was used to simulate the oxidation processes and thus OH and HO2 in this study. In general, the model reproduced the measured OH and HO2 with all five chemical mechanisms producing similar levels of OH and HO2, although midday OH was overpredicted and nighttime OH and HO2 were underpredicted. The calculated HOx production was dominated by HONO photolysis in the early morning and by the photolysis of O-3 and oxygenated volatile organic compounds (OVOCs) in the midday. On average, the daily HOx production rate was 24.6 ppbv d(-1), of which 30% was from O-3 photolysis, 22% from HONO photolysis, 15% from the photolysis of OVOCs (other than HCHO), 14% from HCHO photolysis, and 13% from O-3 reactions with alkenes. The O-3 production was sensitive to volatile organic compounds (VOCs) in the early morning but was sensitive to NOx for most of afternoon. This is similar to the behavior observed in two previous summertime studies in Houston: the Texas Air Quality Study in 2000 (TexAQS 2000) and the TexAQS II Radical and Aerosol Measurement Project in 2006 (TRAMP 2006). Ozone production in SHARP exhibits a longer NOx-sensitive period than TexAQS 2000 and TRAMP 2006, indicating that NOx control may be an efficient approach for the O-3 control in springtime for Houston. Results from this study provide additional support for regulatory actions to reduce NOx and reactive VOCs in Houston in order to reduce O-3 and other secondary pollutants.
C1 [Ren, Xinrong] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Ren, Xinrong; Luke, Winston T.; Kelley, Paul] NOAA, Air Resources Lab, College Pk, MD USA.
[van Duin, Diana; Cazorla, Maria; Chen, Shuang; Zhang, Li; Brune, William H.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Cazorla, Maria] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
[Mao, Jingqiu] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Flynn, James H.; Grossberg, Nicole; Lefer, Barry L.; Rappenglueck, Bernhard] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX USA.
[Wong, Kam W.; Tsai, Catalina; Stutz, Jochen] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Wong, Kam W.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Dibb, Jack E.] Univ New Hampshire, Climate Change Res Ctr, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Jobson, B. Thomas] Washington State Univ, Dept Civil & Environm Engn, Seattle, WA USA.
RP Ren, XR (reprint author), NOAA, Air Resources Lab, College Pk, MD USA.
EM Xinrong.Ren@noaa.gov
RI Kelley, Paul/C-9155-2016; Mao, Jingqiu/F-2511-2010; Ren,
Xinrong/E-7838-2015; Stutz, Jochen/K-7159-2014; Lefer,
Barry/B-5417-2012; Luke, Winston/D-1594-2016
OI Cazorla, Maria/0000-0001-5295-2968; Mao, Jingqiu/0000-0002-4774-9751;
Ren, Xinrong/0000-0001-9974-1666; Lefer, Barry/0000-0001-9520-5495;
Luke, Winston/0000-0002-1993-2241
FU Houston Advanced Research Center (HARC); Texas Commission for
Environmental Quality (TCEQ) through Air Quality Research Program (AQRP)
at University of Texas-Austin
FX The authors thank Houston Advanced Research Center (HARC) and Texas
Commission for Environmental Quality (TCEQ) through Air Quality Research
Program (AQRP) at University of Texas-Austin for funding, other SHARP
participating groups for the use of their data in the study, and W.
Goliff for providing the RACM2 mechanism. Although this article has been
subject to the reviews by TCEQ and NOAA Air Resources Laboratory, it
does not necessarily reflect the views of the Agencies and no official
endorsement should be inferred.
NR 59
TC 18
Z9 18
U1 9
U2 82
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 JUN 16
PY 2013
VL 118
IS 11
BP 5770
EP 5780
DI 10.1002/jgrd.50342
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600040
ER
PT J
AU Mlynczak, MG
Hunt, LH
Mertens, CJ
Marshall, BT
Russell, JM
Puertas, ML
Smith, AK
Siskind, DE
Mast, JC
Thompson, RE
Gordley, LL
AF Mlynczak, Martin G.
Hunt, Linda H.
Mertens, Christopher J.
Marshall, B. Thomas
Russell, James M., III
Puertas, Manuel Lopez
Smith, Anne K.
Siskind, David E.
Mast, Jeffrey C.
Thompson, R. Earl
Gordley, Larry L.
TI Radiative and energetic constraints on the global annual mean atomic
oxygen concentration in the mesopause region
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE atomic oxygen; energy balance; radiative constraints; mesopause;
airglow; ozone
ID MIDDLE ATMOSPHERE; BANDS; MODEL; TEMPERATURE; PHOTOLYSIS
AB We present a new approach to constrain and validate atomic oxygen (O) concentrations in the mesopause region (similar to 80 to similar to 100 km). In a prior companion paper [Mlynczak et al., ], we presented O-atom concentrations in the mesopause region inferred from measurements of day ozone and night hydroxyl emission rates made by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument. The approach presented here uses the constraint of global, annual mean energy balance to derive atomic oxygen concentrations, consistent with rates of radiative cooling by carbon dioxide (CO2) and solar heating due to molecular oxygen (O-2). The mathematical difference between these cooling and heating rates, on a global annual mean basis, effectively constrains the maximum heating rate for the sum of all other processes. The remaining terms, solar heating due to ozone plus a series of exothermic chemical reactions can be expressed as functions of O. This new approach enables a simple mathematical expression that yields the vertical profile of global annual mean radiatively constrained atomic oxygen in the mesopause region. The radiatively constrained atomic oxygen depends only on the CO2 cooling rates, O-2 solar heating rates, and standard reaction rate coefficients and enthalpies. Radiative cooling and solar heating rates used in these analyses are derived from measurements made by the SABER instrument on the NASA Thermosphere Ionosphere Mesosphere Energetics and Dynamics satellite. There is excellent agreement between the SABER radiatively constrained atomic oxygen and that derived from the SABER ozone and OH emission measurements over most of the mesopause region. Radiatively constrained atomic oxygen represents an upper limit on the global average O-atom concentration in the mesopause region.
C1 [Mlynczak, Martin G.; Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Hunt, Linda H.; Mast, Jeffrey C.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Marshall, B. Thomas; Thompson, R. Earl; Gordley, Larry L.] G&A Tech Software, Newport News, VA USA.
[Russell, James M., III] Hampton Univ, Hampton, VA 23668 USA.
[Puertas, Manuel Lopez] IAA CSIC, Granada, Spain.
[Smith, Anne K.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Siskind, David E.] Naval Res Lab, Washington, DC USA.
RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM m.g.mlynczak@nasa.gov
RI Lopez Puertas, Manuel/M-8219-2013
OI Lopez Puertas, Manuel/0000-0003-2941-7734
NR 13
TC 7
Z9 7
U1 0
U2 3
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 JUN 16
PY 2013
VL 118
IS 11
BP 5796
EP 5802
DI 10.1002/jgrd.50400
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600042
ER
PT J
AU Smith, AK
Harvey, VL
Mlynczak, MG
Funke, B
Garcia-Comas, M
Hervig, M
Kaufmann, M
Kyrola, E
Lopez-Puertas, M
McDade, I
Randall, CE
Russell, JM
Sheese, PE
Shiotani, M
Skinner, WR
Suzuki, M
Walker, KA
AF Smith, A. K.
Harvey, V. L.
Mlynczak, M. G.
Funke, B.
Garcia-Comas, M.
Hervig, M.
Kaufmann, M.
Kyrola, E.
Lopez-Puertas, M.
McDade, I.
Randall, C. E.
Russell, J. M., III
Sheese, P. E.
Shiotani, M.
Skinner, W. R.
Suzuki, M.
Walker, K. A.
TI Satellite observations of ozone in the upper mesosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE ozone; mesosphere; SABER
ID NONLOCAL THERMODYNAMIC-EQUILIBRIUM; HALOGEN OCCULTATION EXPERIMENT;
VIBRATIONALLY EXCITED OZONE; MIDDLE ATMOSPHERE; LOWER THERMOSPHERE; LIMB
EMISSION; GOMOS DATA; MU-M; VALIDATION; MIPAS
AB Ozone profiles in the upper mesosphere (70-100km) retrieved from nine instruments are compared. Ozone from the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument is used as the basis of comparison. Other measurements are from the Halogen Occultation Experiment, the High Resolution Doppler Imager, the Michelson Interferometer for Passive Atmospheric Sounding, the Global Ozone Monitoring by Occultation of Stars, the Atmospheric Chemistry ExperimentFourier Transform Spectrometer, the Solar Occultation For Ice Experiment, the Optical Spectrograph and InfraRed Imaging System, and the Superconducting Submillimeter-Wave Limb-Emission Sounder. Comparisons of each data set with SABER using coincident profiles indicate agreement in the basic vertical profile of ozone but also some systematic differences in daytime ozone. Ozone from the SABER 9.6m channel is higher than the other measurements over the altitude range 60-80km by 20-50%. Nighttime comparisons indicate better relative agreement (<10% difference). Taking all the data, not limited to coincidences, shows the global and seasonal distributions of ozone in the upper mesosphere from each instrument. The average maximum in ozone mixing ratio is around 90-92km during daytime and 95km at night. There is a maximum in ozone density at night (approximate to 90km) and during some hours of the day. The latitude structure of ozone has appreciable variations with season, particularly in the tropical upper mesosphere. The basic latitude-altitude structure of ozone depends on local time, even when the analysis is restricted to day-only observations.
C1 [Smith, A. K.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Harvey, V. L.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Funke, B.; Garcia-Comas, M.; Lopez-Puertas, M.] Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Hervig, M.] GATS Inc, Driggs, ID USA.
[Kaufmann, M.] Forschungszentrum Julich, D-52425 Julich, Germany.
[Kyrola, E.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[McDade, I.] York Univ, Dept Earth & Space Sci & Engn, Toronto, ON M3J 2R7, Canada.
[Randall, C. E.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Sheese, P. E.; Walker, K. A.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Shiotani, M.] Kyoto Univ, Res Inst Sustainable Humanosphere, Uji, Kyoto, Japan.
[Skinner, W. R.] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA.
[Suzuki, M.] Japan Aerosp Explorat Agcy, Sagamihara, Kanagawa, Japan.
RP Smith, AK (reprint author), Natl Ctr Atmospher Res, Div Atmospher Chem, POB 3000, Boulder, CO 80307 USA.
EM aksmith@ucar.edu
RI Lopez Puertas, Manuel/M-8219-2013; Kyrola, Erkki/E-1835-2014;
Garcia-Comas, Maya/E-4050-2014; Funke, Bernd/C-2162-2008; Randall,
Cora/L-8760-2014
OI Lopez Puertas, Manuel/0000-0003-2941-7734; Garcia-Comas,
Maya/0000-0003-2323-4486; Funke, Bernd/0000-0003-0462-4702; Randall,
Cora/0000-0002-4313-4397
FU National Science Foundation; NASA Heliospheric Guest Investigator
Program; Spanish MCINN [AYA2011-23552]; EC FEDER; MINECO under Ramon y
Cajal subprogram; Canadian Space Agency; Natural Sciences and
Engineering Research Council of Canada; Japan Aerospace Exploration
Agency (JAXA); National Institute of Information and Communications
Technology (NICT)
FX The National Center for Atmospheric Research is sponsored by the
National Science Foundation. Support for this work was also provided by
the NASA Heliospheric Guest Investigator Program. The IAA team was
supported by the Spanish MCINN under grant AYA2011-23552 and EC FEDER
funds. MGC is financially supported by the MINECO under its Ramon y
Cajal subprogram. The Atmospheric Chemistry Experiment (ACE), also known
as SCISAT, is a Canadian-led mission mainly supported by the Canadian
Space Agency and the Natural Sciences and Engineering Research Council
of Canada. JEM/SMILES mission is a joint project of Japan Aerospace
Exploration Agency (JAXA) and National Institute of Information and
Communications Technology (NICT).
NR 60
TC 15
Z9 15
U1 3
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 16
PY 2013
VL 118
IS 11
BP 5803
EP 5821
DI 10.1002/jgrd.50445
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600043
ER
PT J
AU Ryerson, TB
Andrews, AE
Angevine, WM
Bates, TS
Brock, CA
Cairns, B
Cohen, RC
Cooper, OR
de Gouw, JA
Fehsenfeld, FC
Ferrare, RA
Fischer, ML
Flagan, RC
Goldstein, AH
Hair, JW
Hardesty, RM
Hostetler, CA
Jimenez, JL
Langford, AO
McCauley, E
McKeen, SA
Molina, LT
Nenes, A
Oltmans, SJ
Parrish, DD
Pederson, JR
Pierce, RB
Prather, K
Quinn, PK
Seinfeld, JH
Senff, CJ
Sorooshian, A
Stutz, J
Surratt, JD
Trainer, M
Volkamer, R
Williams, EJ
Wofsy, SC
AF Ryerson, T. B.
Andrews, A. E.
Angevine, W. M.
Bates, T. S.
Brock, C. A.
Cairns, B.
Cohen, R. C.
Cooper, O. R.
de Gouw, J. A.
Fehsenfeld, F. C.
Ferrare, R. A.
Fischer, M. L.
Flagan, R. C.
Goldstein, A. H.
Hair, J. W.
Hardesty, R. M.
Hostetler, C. A.
Jimenez, J. L.
Langford, A. O.
McCauley, E.
McKeen, S. A.
Molina, L. T.
Nenes, A.
Oltmans, S. J.
Parrish, D. D.
Pederson, J. R.
Pierce, R. B.
Prather, K.
Quinn, P. K.
Seinfeld, J. H.
Senff, C. J.
Sorooshian, A.
Stutz, J.
Surratt, J. D.
Trainer, M.
Volkamer, R.
Williams, E. J.
Wofsy, S. C.
TI The 2010 California Research at the Nexus of Air Quality and Climate
Change (CalNex) field study
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Review
DE California; air quality; climate change; field study; CalNex
ID VOLATILE ORGANIC-COMPOUNDS; IONIZATION-MASS-SPECTROMETRY; MARINE
BOUNDARY-LAYER; AEROSOL OPTICAL-PROPERTIES; MILAGRO 2006 CAMPAIGN;
IN-SITU MEASUREMENTS; LOS-ANGELES BASIN; 2-DIMENSIONAL
GAS-CHROMATOGRAPHY; POLLUTED URBAN-ENVIRONMENT; SPECTRAL-RESOLUTION
LIDAR
AB The California Research at the Nexus of Air Quality and Climate Change (CalNex) field study was conducted throughout California in May, June, and July of 2010. The study was organized to address issues simultaneously relevant to atmospheric pollution and climate change, including (1) emission inventory assessment, (2) atmospheric transport and dispersion, (3) atmospheric chemical processing, and (4) cloud-aerosol interactions and aerosol radiative effects. Measurements from networks of ground sites, a research ship, tall towers, balloon-borne ozonesondes, multiple aircraft, and satellites provided in situ and remotely sensed data on trace pollutant and greenhouse gas concentrations, aerosol chemical composition and microphysical properties, cloud microphysics, and meteorological parameters. This overview report provides operational information for the variety of sites, platforms, and measurements, their joint deployment strategy, and summarizes findings that have resulted from the collaborative analyses of the CalNex field study. Climate-relevant findings from CalNex include that leakage from natural gas infrastructure may account for the excess of observed methane over emission estimates in Los Angeles. Air-quality relevant findings include the following: mobile fleet VOC significantly declines, and NOx emissions continue to have an impact on ozone in the Los Angeles basin; the relative contributions of diesel and gasoline emission to secondary organic aerosol are not fully understood; and nighttime NO3 chemistry contributes significantly to secondary organic aerosol mass in the San Joaquin Valley. Findings simultaneously relevant to climate and air quality include the following: marine vessel emissions changes due to fuel sulfur and speed controls result in a net warming effect but have substantial positive impacts on local air quality.
C1 [Ryerson, T. B.; Angevine, W. M.; Brock, C. A.; Cooper, O. R.; de Gouw, J. A.; Langford, A. O.; McKeen, S. A.; Parrish, D. D.; Senff, C. J.; Trainer, M.; Williams, E. J.] NOAA, Div Chem Sci, Boulder, CO USA.
[Andrews, A. E.] NOAA, Global Monitoring Div, Boulder, CO USA.
[Angevine, W. M.; Cooper, O. R.; de Gouw, J. A.; Fehsenfeld, F. C.; Hardesty, R. M.; Jimenez, J. L.; McKeen, S. A.; Oltmans, S. J.; Senff, C. J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Bates, T. S.; Quinn, P. K.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA.
[Cairns, B.] NASA, Goddard Inst Space Studies, Greenbelt, MD USA.
[Cohen, R. C.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
[Ferrare, R. A.; Hair, J. W.; Hostetler, C. A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Fischer, M. L.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Environm Energy Technol Div, Berkeley, CA 94720 USA.
[Flagan, R. C.; Seinfeld, J. H.] CALTECH, Dept Chem Engn, Pasadena, CA 91125 USA.
[Goldstein, A. H.] Univ Calif Berkeley, Dept Civil & Environm Engn, Berkeley, CA 94720 USA.
[Jimenez, J. L.; Volkamer, R.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[McCauley, E.; Pederson, J. R.] Calif Air Resources Board, Atmospher Processes Res Sect, Sacramento, CA USA.
[Molina, L. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
[Molina, L. T.] Molina Ctr Energy & Environm, La Jolla, CA USA.
[Nenes, A.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Pierce, R. B.] NOAA, Natl Environm Satellite Data & Informat Serv, Madison, WI USA.
[Prather, K.] Univ Calif San Diego, Dept Chem & Biochem, San Diego, CA 92103 USA.
[Sorooshian, A.] Univ Arizona, Tucson, AZ USA.
[Stutz, J.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Surratt, J. D.] Univ N Carolina, Chapel Hill, NC USA.
[Wofsy, S. C.] Harvard Univ, Boston, MA 02115 USA.
RP Ryerson, TB (reprint author), NOAA, Div Chem Sci, Boulder, CO USA.
EM thomas.b.ryerson@noaa.gov
RI Ryerson, Tom/C-9611-2009; Stutz, Jochen/K-7159-2014; de Gouw,
Joost/A-9675-2008; Volkamer, Rainer/B-8925-2016; Bates,
Timothy/L-6080-2016; Quinn, Patricia/R-1493-2016; Manager, CSD
Publications/B-2789-2015; Prather, Kimberly/A-3892-2008; Jimenez,
Jose/A-5294-2008; Langford, Andrew/D-2323-2009; Cohen,
Ronald/A-8842-2011; Pierce, Robert Bradley/F-5609-2010; Cooper,
Owen/H-4875-2013; Angevine, Wayne/H-9849-2013; Goldstein,
Allen/A-6857-2011; Parrish, David/E-8957-2010; Andrews,
Arlyn/K-3427-2012; Brock, Charles/G-3406-2011; Surratt,
Jason/D-3611-2009; Trainer, Michael/H-5168-2013; Senff,
Christoph/I-2592-2013
OI de Gouw, Joost/0000-0002-0385-1826; Volkamer,
Rainer/0000-0002-0899-1369; Quinn, Patricia/0000-0003-0337-4895;
Prather, Kimberly/0000-0003-3048-9890; Cairns,
Brian/0000-0002-1980-1022; Sorooshian, Armin/0000-0002-2243-2264;
Jimenez, Jose/0000-0001-6203-1847; Langford, Andrew/0000-0002-2932-7061;
Cohen, Ronald/0000-0001-6617-7691; Pierce, Robert
Bradley/0000-0002-2767-1643; Angevine, Wayne/0000-0002-8021-7116;
Goldstein, Allen/0000-0003-4014-4896; Parrish,
David/0000-0001-6312-2724; Brock, Charles/0000-0002-4033-4668; Surratt,
Jason/0000-0002-6833-1450;
FU NOAA Air Quality program; California Air Resources Board; NOAA Climate
Change program [NA090AR4310128]; DOE Atmospheric Systems Research
Program; NASA Radiation Sciences and Tropospheric Chemistry programs;
NOAA Office of Global Programs; California Energy Commission (CEC)
Public Interest Environmental Research Program; LBNL Laboratory Directed
Research through the U.S. Department of Energy [DE-AC02-05CH11231]; US
Department of Energy; US National Science Foundation
FX We thank L. Dolislager (CARB) for the description of existing long-term
criteria pollutant, greenhouse gas, and meteorological measurement sites
in California. We also thank G. Sanger and B. Ochs (NWS San Joaquin
Valley/Hanford Weather Forecast Office) and L. Dolislager and J.
Pederson (CARB) for meteorological forecast summaries. The R/V Atlantis
cruise and NOAA P-3 flights were supported, in part, by the NOAA Climate
Change and, in part, by the NOAA Air Quality programs. NOAA Twin Otter
flights were supported by the NOAA Air Quality program and the
California Air Resources Board. CIRPAS Twin Otter flights were supported
by the NOAA Climate Change program under contract NA090AR4310128. NASA
B200 flights were supported by the DOE Atmospheric Systems Research
Program and the NASA Radiation Sciences and Tropospheric Chemistry
programs. Data collection at the CALGEM tall tower sites was supported
by the NOAA Office of Global Programs, the California Energy Commission
(CEC) Public Interest Environmental Research Program, and LBNL
Laboratory Directed Research through the U.S. Department of Energy under
contract DE-AC02-05CH11231. Researchers at the ground sites were
supported by the California Air Resources Board, the NOAA Office of
Global Programs, the US Department of Energy, and the US National
Science Foundation.
NR 279
TC 77
Z9 77
U1 9
U2 144
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 JUN 16
PY 2013
VL 118
IS 11
BP 5830
EP 5866
DI 10.1002/jgrd.50331
PG 37
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 228TG
UT WOS:000325212600045
ER
PT J
AU Parazoo, NC
Bowman, K
Frankenberg, C
Lee, JE
Fisher, JB
Worden, J
Jones, DBA
Berry, J
Collatz, GJ
Baker, IT
Jung, M
Liu, JJ
Osterman, G
O'Dell, C
Sparks, A
Butz, A
Guerlet, S
Yoshida, Y
Chen, HL
Gerbig, C
AF Parazoo, Nicholas C.
Bowman, Kevin
Frankenberg, Christian
Lee, Jung-Eun
Fisher, Joshua B.
Worden, John
Jones, Dylan B. A.
Berry, Joseph
Collatz, G. James
Baker, Ian T.
Jung, Martin
Liu, Junjie
Osterman, Gregory
O'Dell, Chris
Sparks, Athena
Butz, Andre
Guerlet, Sandrine
Yoshida, Yukio
Chen, Huilin
Gerbig, Christoph
TI Interpreting seasonal changes in the carbon balance of southern Amazonia
using measurements of XCO2 and chlorophyll fluorescence from GOSAT
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE carbon cycle; amazon; satellite remote sensing; GOSAT; chlorophyll
fluorescence; biomass burning
ID CO2 RETRIEVAL ALGORITHM; ATMOSPHERIC CO2; RAIN-FOREST; DROUGHT; DIOXIDE;
DIEBACK; SPACE; LAND
AB Amazon forests exert a major influence on the global carbon cycle, but quantifying the impact is complicated by diverse landscapes and sparse data. Here we examine seasonal carbon balance in southern Amazonia using new measurements of column-averaged dry air mole fraction of CO2 (XCO2) and solar induced chlorophyll fluorescence (SIF) from the Greenhouse Gases Observing Satellite (GOSAT) from July 2009 to December 2010. SIF, which reflects gross primary production (GPP), is used to disentangle the photosynthetic component of land-atmosphere carbon exchange. We find that tropical transitional forests in southern Amazonia exhibit a pattern of low XCO2 during the wet season and high XCO2 in the dry season that is robust to retrieval methodology and with seasonal amplitude double that of cerrado ecosystems to the east (4ppm versus 2ppm), including enhanced dilution of 2.5ppm in the wet season. Concomitant measurements of SIF, which are inversely correlated with XCO2 in southern Amazonia (r=-0.53, p<0.001), indicate that the enhanced variability is driven by seasonal changes in GPP due to coupling of strong vertical mixing with seasonal changes in underlying carbon exchange. This finding is supported by forward simulations of the Goddard Chemistry Transport Model (GEOS-Chem) which show that local carbon uptake in the wet season and loss in the dry season due to emissions by ecosystem respiration and biomass burning produces best agreement with observed XCO2. We conclude that GOSAT provides critical measurements of carbon exchange in southern Amazonia, but more samples are needed to examine moist Amazon forests farther north
C1 [Parazoo, Nicholas C.; Bowman, Kevin; Frankenberg, Christian; Lee, Jung-Eun; Fisher, Joshua B.; Worden, John; Liu, Junjie; Osterman, Gregory; Sparks, Athena] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Parazoo, Nicholas C.; Bowman, Kevin; Jones, Dylan B. A.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Jones, Dylan B. A.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Berry, Joseph] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA.
[Collatz, G. James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baker, Ian T.; O'Dell, Chris] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Jung, Martin; Gerbig, Christoph] Max Planck Inst Biogeochem, Dept Biogeochem Syst, D-07745 Jena, Germany.
[Butz, Andre] Karlsruhe Inst Technol, IMK ASF, Leopoldshafen, Germany.
[Guerlet, Sandrine] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[Yoshida, Yukio] Natl Inst Environm Studies, Ctr Global Environm Res, Tsukuba, Ibaraki, Japan.
[Chen, Huilin] NOAA Earth Syst Res Lab, Boulder, CO USA.
RP Parazoo, NC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Nicholas.C.Parazoo@jpl.nasa.gov
RI Gerbig, Christoph/L-3532-2013; Butz, Andre/A-7024-2013; Chem,
GEOS/C-5595-2014; collatz, george/D-5381-2012; Chen, Huilin/J-9479-2012;
Jones, Dylan/O-2475-2014; Frankenberg, Christian/A-2944-2013
OI Gerbig, Christoph/0000-0002-1112-8603; Butz, Andre/0000-0003-0593-1608;
Chen, Huilin/0000-0002-1573-6673; Jones, Dylan/0000-0002-1935-3725;
Frankenberg, Christian/0000-0002-0546-5857
FU ESA's CCI on GHGs; European Commission [218793]; DFG [BU2599/1-1]; NASA
FX ACOS b2.9 XCO2 data were produced by the ACOS/OCO-2 project
at the Jet Propulsion Laboratory, CalTech, and obtained from the
ACOS/OCO-2 data archive maintained at the NASA GES DISC. Development of
RemoTeC algorithm is partly funded from ESA's CCI on GHGs and the
European Commission's seventh framework program under grant agreement
218793 and by the Emmy-Noether programme of DFG through grant
BU2599/1-1. CarbonTracker 2011 results provided by NOAA ESRL, Boulder,
Colorado, USA from the website at http://carbontracker.noaa.gov. We
thank Prof. Dr. Paulo Artaxo, Dr. Kenia Wiedemann, Fernando Morais,
Alcides Ribeiro, University of Sao Paulo, Brazil, and Livia Oliveira,
INPA, Brazil, for their assistance and support in installing and
operating the Picarro instrument at the TT34 tower. Part of this
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA (c) 2013. All rights
reserved.
NR 30
TC 29
Z9 29
U1 3
U2 70
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 JUN 16
PY 2013
VL 40
IS 11
BP 2829
EP 2833
DI 10.1002/grl.50452
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 175VL
UT WOS:000321261600064
ER
PT J
AU Davis, SM
Liang, CK
Rosenlof, KH
AF Davis, Sean M.
Liang, Calvin K.
Rosenlof, Karen H.
TI Interannual variability of tropical tropopause layer clouds
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE TTL; cirrus; ENSO; QBO; Brewer Dobson Circulation
ID STRATOSPHERIC TEMPERATURES; WATER-VAPOR; CIRCULATION; CALIPSO; BALANCE;
CYCLE
AB The quasi-biennial oscillation (QBO), El Nino Southern Oscillation (ENSO), and upwelling in the tropical branch of the Brewer-Dobson circulation (BDC) impact tropical tropopause layer (TTL, 14-19km) temperature (T) and relative humidity (RH), and thus it is likely that they also affect the TTL cloud distribution. Satellite data reveal extreme interannual variability in the zonal-mean TTL cloud occurrence frequency (CF) in the deep tropics (10 degrees S-10 degrees N). This zonal-mean interannual variability is related to the QBO and BDC, with a relatively minor role for ENSO. However, over the whole tropics (30 degrees S-30 degrees N), the dominant mode of variability in the longitudinally resolved CF field is an ENSO-related dipole pattern of positive and negative anomalies centered over the Pacific that mimics the RH/T fields. The ENSO effects largely cancel in the zonal mean, although El Nino is weakly associated with enhanced zonal-mean cloudiness in the uppermost TTL over the short satellite record.
C1 [Davis, Sean M.; Rosenlof, Karen H.] NOAA Earth Syst Res Lab ESRL, Boulder, CO 80305 USA.
[Davis, Sean M.] Univ Colorado Boulder, CIRES, Boulder, CO USA.
[Liang, Calvin K.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Davis, SM (reprint author), NOAA Earth Syst Res Lab ESRL, 325 S Broadway, Boulder, CO 80305 USA.
EM sean.m.davis@noaa.gov
RI Davis, Sean/C-9570-2011; Rosenlof, Karen/B-5652-2008; Manager, CSD
Publications/B-2789-2015
OI Davis, Sean/0000-0001-9276-6158; Rosenlof, Karen/0000-0002-0903-8270;
FU NASA [NNX09AO04H]; Northrop Grumman Aerospace Systems fellowship; NOAA
FX The authors would like to thank B. Kahn, A. Eldering, A. Dessler, A.
Gettleman, B. Rossow, and E. Fetzer for helpful discussions. CKL was
supported by a NASA Earth and Space Science Fellowship (NNX09AO04H) and
the Northrop Grumman Aerospace Systems fellowship. CloudSat and CALIPSO
data were obtained through the CloudSat Data Processing Center
(http://www.cloudsat.cira.colostate.edu/). SMD and KHR are supported by
the NOAA Atmospheric Composition and Climate Program.
NR 26
TC 6
Z9 6
U1 1
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JUN 16
PY 2013
VL 40
IS 11
BP 2862
EP 2866
DI 10.1002/grl.50512
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 175VL
UT WOS:000321261600070
ER
PT J
AU Norman, RB
Slaba, TC
Blattnig, SR
AF Norman, R. B.
Slaba, T. C.
Blattnig, S. R.
TI An extension of HZETRN for cosmic ray initiated electromagnetic cascades
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Cosmic rays; Space radiation; Electron; Positron; Pion; Muon
ID TRANSPORT; PROPAGATION; VALIDATION
AB Safe and efficient mission operations in space require an accurate understanding of the physical interactions of space radiation. As the primary space radiation interacts with intervening materials, the composition and spectrum of the radiation environment changes. The production of secondary particles can make a significant contribution to radiation exposure. In this work, the NASA space radiation transport code, HZETRN, is extended to include the transport of electrons, positrons, and photons. The production of these particles is coupled to the initial cosmic ray radiation environment through the decay of neutral pions, which produce high energy photons, and through the decay of muons, which produce electrons and positrons. The photons, electrons, and positrons interact with materials producing more photons, electrons and positrons generating an electromagnetic cascade. The relevant cross sections, transport equation, and solution method are introduced. Electron and positron production in Earth's atmosphere is investigated and compared to experimental balloon-flight measurements. Reasonable agreement is seen between HZETRN and data. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Norman, R. B.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA.
[Slaba, T. C.; Blattnig, S. R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Norman, RB (reprint author), Univ Tennessee, Dept Nucl Engn, 211 Pasqua Engn Bldg, Knoxville, TN 37996 USA.
EM ryan.b.norman@nasa.gov; tony.c.slaba@nasa.gov; steve.r.blattnig@nasa.gov
RI Norman, Ryan/D-5095-2017
OI Norman, Ryan/0000-0002-9103-7225
NR 32
TC 12
Z9 12
U1 0
U2 0
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD JUN 15
PY 2013
VL 51
IS 12
BP 2251
EP 2260
DI 10.1016/j.asr.2013.01.021
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 168DN
UT WOS:000320686000007
ER
PT J
AU Beaudet, RA
AF Beaudet, Robert A.
TI The statistical treatment implemented to obtain the planetary protection
bioburdens for the Mars Science Laboratory mission
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Planetary protection; Mars Science Laboratory; MSL; Bioburden; Bioburden
density; Mars
AB NASA Planetary Protection Policy requires that Category IV missions such as those going to the surface of Mars include detailed assessment and documentation of the bioburden on the spacecraft at launch. In the prior missions to Mars, the approaches used to estimate the bioburden could easily be conservative without penalizing the project because spacecraft elements such as the descent and landing stages had relatively small surface areas and volumes. With the advent of a large spacecraft such as Mars Science Laboratory (MSL), it became necessary for a modified-still conservative but more pragmatic-statistical treatment be used to obtain the standard deviations and the bioburden densities at about the 99.9% confidence limits. This article describes both the Gaussian and Poisson statistics that were implemented to analyze the bioburden data from the MSL spacecraft prior to launch. The standard deviations were weighted by the areas sampled with each swab or wipe. Some typical cases are given and discussed. Published by Elsevier Ltd. on behalf of COSPAR.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Beaudet, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Robert.A.Beaudet@jpl.nasa.gov
FU National Aeronautics and Space Administration; MSL project; Mars
Technology Program
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. I would like to thank Dr. Jack
Barengoltz who first suggested the weighting scheme (equivalent number
of swabs per wipe) and who reviewed this manuscript in detail. Also, I
would like to thank Robert Koukol, Fabian Morales, Wayne Schubert, J.
Nick Benardini, J.Andy Spry and Karen Buxbaum for reading and reviewing
this manuscript and offering their constructive suggestions prior to
submission. The original program in MS Access was written by Dr.
Jennifer Law. This work was funded by the MSL project and the Mars
Technology Program.
NR 5
TC 5
Z9 5
U1 0
U2 1
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 JUN 15
PY 2013
VL 51
IS 12
BP 2261
EP 2268
DI 10.1016/j.asr.2013.01.026
PG 8
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 168DN
UT WOS:000320686000008
ER
PT J
AU Brunini, C
Conte, JF
AzpilicuetaA, F
Bilitza, D
AF Brunini, Claudio
Federico Conte, J.
AzpilicuetaA, Francisco
Bilitza, Dieter
TI A different method to update monthly median h(m)F2 values
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE h(m)F2; Electron density profile; ITU-R database; Ionosphere
ID IONOSPHERE; MODEL; HEIGHT; GPS
AB The height, h(m)F2, and the electron density, N(m)F2, of the F2 peak are key model parameters to characterize the actual state of the ionosphere. These parameters, or alternatively the propagation factor, M3000F2, and the critical frequency, f(o)F2, of the F2 peak, which are related to h(m)F2 and N(m)F2, are used to anchor the electron density vertical profile computed with different models such as the International Reference Ionosphere (Bilitza, 2002), as well as for radio propagation forecast purposes. Long time series of these parameters only exist in an inhomogeneous distribution of points over the surface of Earth, where dedicated instruments (typically ionosondes) have been working for many years. A commonly used procedure for representing median values of the aforementioned parameters all over the globe is the one recommended by the ITU-R (ITU-R, 1997). This procedure, known as the Jones and Gallet mapping technique, was based on ionosondes measurements gathered from 1954 to 1958 by a global network of around 150 ionospheric stations (Jones and Gallet, 1962; Jones and Obitts, 1970). Even though several decades have passed since the development of that innovative work, only few efforts have been dedicated to establish a new mapping technique for computing h(m)F2 and N(m)F2 median values at global scale or to improve the old method using the increased observational database. Therefore, in this work three different procedures to describe the daily and global behavior of the height of the F2 peak are presented. All of them represent a different and simplified method to estimate h(m)F2 and are based on different mathematical expressions. The advantages and disadvantages of these three techniques are analyzed, leading to the conclusion that the recommended procedure to represent h(m)F2 is best characterized by a Spherical Harmonics expansion of degree and order equal to 15, since the differences between the h(m)F2 values obtained with the Jones and Gallet technique and those obtained using the abovementioned procedure are of only 1%. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Brunini, Claudio; Federico Conte, J.; AzpilicuetaA, Francisco] UNLP, Fac Ciencias Astron & Geofis, Space Geodesy & Aeron GESA Dept, La Plata, Buenos Aires, Argentina.
[Bilitza, Dieter] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Conte, JF (reprint author), UNLP, Fac Ciencias Astron & Geofis, Space Geodesy & Aeron GESA Dept, Paseo Basque S-N,B1900, La Plata, Buenos Aires, Argentina.
EM fconte@fcaglp.unlp.edu.ar
NR 24
TC 10
Z9 10
U1 0
U2 0
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 JUN 15
PY 2013
VL 51
IS 12
BP 2322
EP 2332
DI 10.1016/j.asr.2013.01.027
PG 11
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 168DN
UT WOS:000320686000015
ER
PT J
AU Chen, YJ
Hemmati, H
Some, R
AF Chen, Yijiang
Hemmati, Hamid
Some, Raphael
TI Multi-Gb/s Fiberoptic Physical Layer for Spacecraft Interconnects
SO JOURNAL OF LIGHTWAVE TECHNOLOGY
LA English
DT Article
DE Optical communications; optical fiber bus; protocol; space avionics
AB We report on the development of a fiberoptic physical layer bus with RapidIO-protocol for spacecraft avionics interconnects. To emulate spacecraft instrument data transmission, dynamic routing of real-time live camera data packets is demonstrated through a switch-based network. For real-time instrument data input/output, an interface bridge between Ethernet protocol and RapidIO protocol is developed. RapidIO-based fiberoptic avionic system is compared with 1393 ring protocol based interconnect in terms of performance, flexibility, mass/power/size, and suitability for different mission applications. Fault tolerant architectures for RapidIO and 1393 ring-protocol-based spacecraft buses are also presented.
C1 [Chen, Yijiang; Hemmati, Hamid; Some, Raphael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Chen, YJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM yijiang.chen@jpl.nasa.gov
NR 5
TC 0
Z9 0
U1 1
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0733-8724
J9 J LIGHTWAVE TECHNOL
JI J. Lightwave Technol.
PD JUN 15
PY 2013
VL 31
IS 12
BP 1899
EP 1905
DI 10.1109/JLT.2013.2261050
PG 7
WC Engineering, Electrical & Electronic; Optics; Telecommunications
SC Engineering; Optics; Telecommunications
GA 151KO
UT WOS:000319459600002
ER
PT J
AU Guanter, L
Rossini, M
Colombo, R
Meroni, M
Frankenberg, C
Lee, JE
Joiner, J
AF Guanter, Luis
Rossini, Micol
Colombo, Roberto
Meroni, Michele
Frankenberg, Christian
Lee, Jung-Eun
Joiner, Joanna
TI Using field spectroscopy to assess the potential of statistical
approaches for the retrieval of sun-induced chlorophyll fluorescence
from ground and space
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Fluorescence retrieval; Fraunhofer-line approach; GOSAT-FTS; Singular
vector decomposition; O(2)A-band
ID VEGETATION FLUORESCENCE; STRESS DETECTION; WATER-STRESS; SIMULATIONS;
INSTRUMENT; EMISSION; PLATFORM; CAMERA; SENSOR; PLANTS
AB Sun-induced chlorophyll fluorescence (F-s) is an electromagnetic signal emitted in the 650-800 nm spectral window by the chlorophyll-a of green leaves. Previous studies demonstrated the retrieval of F-s on a global scale using high spectral resolution measurements by the Fourier Transform Spectrometer (FTS) on board the greenhouse gases observing satellite (GOSAT). The retrieval of F-s from GOSAT-FTS data is based on the modeling of the in-filling of solar Fraunhofer lines by F-s. The first Fs retrieval methods for GOSAT-FTS measurements were based on physical formulations of the radiative transfer between the atmosphere, the surface and the instrument including the F-s emission. As an alternative, a statistical method was also successfully applied to GOSAT data. This method is based on a singular vector decomposition (SVD) technique producing a basis of spectral functions able to model the contribution of the reflected solar radiation to the top-of-atmosphere measurement in a linear way. The F-s signal is included in the forward model as an extra parameter adding to the reflected solar radiation. Here, we use field spectroscopy measurements to provide further experimental evidence on the retrieval of F-s with statistical approaches in both Fraunhofer lines and atmospheric oxygen and water vapor bands. The statistical retrieval method used with GOSAT-FTS data has been adapted to a set of ground-based spectro-radiometer measurements in the 717-780 nm range. Retrieval results in the 745-759 nm window, which contains only Fraunhofer lines, support the overall approach of estimating F-s from space measurements in that spectral window. Furthermore, the application of the method to broader fitting windows including both Fraunhofer lines and and (oxygen and water vapor) atmospheric bands atmospheric bands has been proven to be very effective to reduce the retrieval noise and has also shown a good comparison with reference O(2)A-based retrievals. This allows consideration of statistical methods as a powerful option for F-s retrieval from broad-band space-based measurements in the near-infrared. (c) 2013 Published by Elsevier Inc.
C1 [Guanter, Luis] Free Univ Berlin, Inst Space Sci, Berlin, Germany.
[Meroni, Michele] Univ Studi Milano Bicocca, DISAT, Remote Sensing Environm Dynam Lab, Milan, Italy.
[Meroni, Michele] Inst Environm & Sustainabil, DG JRC, European Commiss, Ispra, Varese, Italy.
[Frankenberg, Christian; Lee, Jung-Eun] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Joiner, Joanna] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Guanter, L (reprint author), Free Univ Berlin, Inst Space Sci, Berlin, Germany.
EM luis.guanter@wew.fu-berlin.de
RI Joiner, Joanna/D-6264-2012; Guanter, Luis/I-1588-2015; Frankenberg,
Christian/A-2944-2013;
OI Guanter, Luis/0000-0002-8389-5764; Frankenberg,
Christian/0000-0002-0546-5857; Rossini, Micol/0000-0002-6052-3140
FU European Commission through the 7th Framework Marie Curie Actions
Programme; Emmy Noether Programme of the German Research Foundation
FX This research has been funded by the European Commission through the 7th
Framework Marie Curie Actions Programme and the Emmy Noether Programme
of the German Research Foundation. The authors thank Albert
Porcar-Castell from the University of Helsinki for his comments on an
earlier version of the manuscript. We acknowledge the staff of the
Remote Sensing of Environmental Dynamic Laboratory, DISAT, UNIMIB (S.
Cogliati, M. Migliavacca) for their support during the field campaigns.
NR 35
TC 33
Z9 34
U1 7
U2 76
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD JUN 15
PY 2013
VL 133
BP 52
EP 61
DI 10.1016/j.rse.2013.01.017
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 130TD
UT WOS:000317942100004
ER
PT J
AU Fortenberry, RC
Huang, XC
Yachmenev, A
Thiel, W
Lee, TJ
AF Fortenberry, Ryan C.
Huang, Xinchuan
Yachmenev, Andrey
Thiel, Walter
Lee, Timothy J.
TI On the use of quartic force fields in variational calculations
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
DE Ryan C. Fortenberry a; Xinchuan Huang b; Andrey Yachmenev cri; Walter
Thiel C; Timothy J. Lee
ID POTENTIAL-ENERGY SURFACES; CORRELATED MOLECULAR CALCULATIONS; TRANSFORM
INFRARED-SPECTROSCOPY; AB-INITIO CALCULATION; GAUSSIAN-BASIS SETS;
VIBRATIONAL FREQUENCIES; POLYATOMIC-MOLECULES; ROVIBRATIONAL ENERGIES;
EQUILIBRIUM STRUCTURE; TETRATOMIC MOLECULES
AB Quartic force fields (QFFs) have been shown to be one of the most effective ways to efficiently compute vibrational frequencies for small molecules. In this letter we discuss how the simple-internal or bond-length bond-angle (BLBA) coordinates can be transformed into Morse-cosine (-sine) coordinates which produce potential energy surfaces from QFFs that possess proper limiting behavior and can describe the vibrational (or rovibrational) energy levels of an arbitrary molecular system to 5 cm(-1) or better compared to experiment. We investigate parameter scaling in the Morse coordinate, symmetry considerations, and examples of transformed QFFs making use of the MULTIMODE, TROVE, and VTET variational vibrational methods. (c) 2013 Elsevier B.V. All rights reserved.
C1 [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
[Yachmenev, Andrey; Thiel, Walter] Max Planck Inst Kohlenforsch, D-45470 Mulheim, Germany.
RP Lee, TJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; Thiel,
Walter/A-5677-2016
OI Thiel, Walter/0000-0001-6780-0350
FU NASA [08-APRA08-0050, 10-APRA10-0167]; NASA's Laboratory Astrophysics
'Carbon in the Galaxy' Consortium [NNH10ZDA001N]; NASA/SETI Institute
[NNX09AI49A, NNX12AG96A]
FX The authors gratefully acknowledge support from NASA Grants
08-APRA08-0050 and 10-APRA10-0167 as well as NASA's Laboratory
Astrophysics 'Carbon in the Galaxy' Consortium Grant (NNH10ZDA001N).
R.C.F. is funded by the NASA Postdoctoral Program administered through
Oak Ridge Associated Universities. X.H. acknowledges financial support
by NASA/SETI Institute Cooperative Agreements NNX09AI49A and NNX12AG96A.
Helpful comments from Dr. Stuart Carter and Professor Joel Bowman are
gratefully acknowledged.
NR 86
TC 28
Z9 28
U1 1
U2 28
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2614
J9 CHEM PHYS LETT
JI Chem. Phys. Lett.
PD JUN 14
PY 2013
VL 574
BP 1
EP 12
DI 10.1016/j.cplett.2013.03.078
PG 12
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 164SW
UT WOS:000320430800001
ER
PT J
AU Tirumalai, MR
Rastogi, R
Zamani, N
Williams, EO
Allen, S
Diouf, F
Kwende, S
Weinstock, GM
Venkateswaran, KJ
Fox, GE
AF Tirumalai, Madhan R.
Rastogi, Rajat
Zamani, Nader
Williams, Elisha O'Bryant
Allen, Shamail
Diouf, Fatma
Kwende, Sharon
Weinstock, George M.
Venkateswaran, Kasthuri J.
Fox, George E.
TI Candidate Genes That May Be Responsible for the Unusual Resistances
Exhibited by Bacillus pumilus SAFR-032 Spores
SO PLOS ONE
LA English
DT Article
ID SPACECRAFT ASSEMBLY FACILITY; DNA-REPAIR PATHWAYS; SUBTILIS SPORES;
SP-NOV.; STRUCTURAL COMPONENTS; PHOTOPRODUCT LYASE; IONIZING-RADIATION;
ESCHERICHIA-COLI; UV RESISTANCE; PROTECTION
AB The spores of several Bacillus species, including Bacillus pumilus SAFR-032 and B. safensis FO-36b, which were isolated from the spacecraft assembly facility at NASA's Jet Propulsion Laboratory, are unusually resistant to UV radiation and hydrogen peroxide. In order to identify candidate genes that might be associated with these resistances, the whole genome of B. pumilus SAFR-032, and the draft genome of B. safensis FO-36b were compared in detail with the very closely related type strain B. pumilus ATCC7061(T). 170 genes are considered characteristic of SAFR-032, because they are absent from both FO-36b and ATCC7061(T). Forty of these SAFR-032 characteristic genes are entirely unique open reading frames. In addition, four genes are unique to the genomes of the resistant SAFR-032 and FO-36b. Fifty three genes involved in spore coat formation, regulation and germination, DNA repair, and peroxide resistance, are missing from all three genomes. The vast majority of these are cleanly deleted from their usual genomic context without any obvious replacement. Several DNA repair and peroxide resistance genes earlier reported to be unique to SAFR-032 are in fact shared with ATCC7061 (T) and no longer considered to be promising candidates for association with the elevated resistances. Instead, several SAFR-032 characteristic genes were identified, which along with one or more of the unique SAFR-032 genes may be responsible for the elevated resistances. These new candidates include five genes associated with DNA repair, namely, BPUM_0608 a helicase, BPUM_0652 an ATP binding protein, BPUM_0653 an endonuclease, BPUM_0656 a DNA cytosine-5-methyltransferase, and BPUM_3674 a DNA helicase. Three of these candidate genes are in immediate proximity of two conserved hypothetical proteins, BPUM_0654 and BPUM_0655 that are also absent from both FO-36b and ATCC7061(T). This cluster of five genes is considered to be an especially promising target for future experimental work.
C1 [Tirumalai, Madhan R.; Rastogi, Rajat; Zamani, Nader; Williams, Elisha O'Bryant; Fox, George E.] Univ Houston, Dept Biol & Biochem, Houston, TX 77004 USA.
[Allen, Shamail; Diouf, Fatma; Kwende, Sharon] Texas So Univ, Dept Biol, Houston, TX 77004 USA.
[Weinstock, George M.] Washington Univ, Sch Med, Genome Inst, St Louis, MO USA.
[Venkateswaran, Kasthuri J.] CALTECH, NASA, Jet Prop Labs, Biotechnol & Planetary Protect Grp, Pasadena, CA 91125 USA.
RP Fox, GE (reprint author), Univ Houston, Dept Biol & Biochem, Houston, TX 77004 USA.
EM gefox@central.uh.edu
OI R Tirumalai, Madhan/0000-0002-5999-333X
FU Institute of Space Systems Operations at the University of Houston;
Center for Bio-nanotechnology and Environmental Research at Texas
Southern University (NASA) [NNX08B4A47A]; Center for Ribosomal Evolution
and Adaptation at the Georgia Institute of Technology (NASA)
[NNA09DA78A]; National Science Foundation [414410]
FX This work was supported by grants from the Institute of Space Systems
Operations at the University of Houston, the Center for
Bio-nanotechnology and Environmental Research at Texas Southern
University (NASA Cooperative agreement NNX08B4A47A) and the Center for
Ribosomal Evolution and Adaptation at the Georgia Institute of
Technology (NASA Cooperative Agreement NNA09DA78A) to George E. Fox and
National Science Foundation grant -414410 to George M. Weinstock. The
funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 59
TC 11
Z9 11
U1 0
U2 13
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 JUN 14
PY 2013
VL 8
IS 6
AR e66012
DI 10.1371/journal.pone.0066012
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 163UV
UT WOS:000320363300059
PM 23799069
ER
PT J
AU Famiglietti, JS
Rodell, M
AF Famiglietti, James S.
Rodell, Matthew
TI Water in the Balance
SO SCIENCE
LA English
DT Editorial Material
ID GROUNDWATER DEPLETION; GRACE; CYCLE
C1 [Famiglietti, James S.] Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA 92697 USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA.
[Rodell, Matthew] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Famiglietti, JS (reprint author), Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA 92697 USA.
EM jfamigli@uci.edu
RI Rodell, Matthew/E-4946-2012
OI Rodell, Matthew/0000-0003-0106-7437
NR 15
TC 94
Z9 96
U1 5
U2 124
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD JUN 14
PY 2013
VL 340
IS 6138
BP 1300
EP 1301
DI 10.1126/science.1236460
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 163FC
UT WOS:000320320200034
PM 23766323
ER
PT J
AU Cziczo, DJ
Froyd, KD
Hoose, C
Jensen, EJ
Diao, MH
Zondlo, MA
Smith, JB
Twohy, CH
Murphy, DM
AF Cziczo, Daniel J.
Froyd, Karl D.
Hoose, Corinna
Jensen, Eric J.
Diao, Minghui
Zondlo, Mark A.
Smith, Jessica B.
Twohy, Cynthia H.
Murphy, Daniel M.
TI Clarifying the Dominant Sources and Mechanisms of Cirrus Cloud Formation
SO SCIENCE
LA English
DT Article
ID ICE NUCLEATION; BIOLOGICAL PARTICLES; MIXED-PHASE; AEROSOLS; NUCLEI;
DUST; LEAD
AB Formation of cirrus clouds depends on the availability of ice nuclei to begin condensation of atmospheric water vapor. Although it is known that only a small fraction of atmospheric aerosols are efficient ice nuclei, the critical ingredients that make those aerosols so effective have not been established. We have determined in situ the composition of the residual particles within cirrus crystals after the ice was sublimated. Our results demonstrate that mineral dust and metallic particles are the dominant source of residual particles, whereas sulfate and organic particles are underrepresented, and elemental carbon and biological materials are essentially absent. Further, composition analysis combined with relative humidity measurements suggests that heterogeneous freezing was the dominant formation mechanism of these clouds.
C1 [Cziczo, Daniel J.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Froyd, Karl D.; Murphy, Daniel M.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA.
[Froyd, Karl D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Hoose, Corinna] Karlsruhe Inst Technol, Inst Meteorol & Climate Res Atmospher Aerosol Res, D-76021 Karlsruhe, Germany.
[Jensen, Eric J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Diao, Minghui; Zondlo, Mark A.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[Smith, Jessica B.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Twohy, Cynthia H.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
RP Cziczo, DJ (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM djcziczo@mit.edu
RI Murphy, Daniel/J-4357-2012; Froyd, Karl/H-6607-2013; Hoose,
Corinna/A-4295-2009; Diao, Minghui/A-4437-2015; Zondlo,
Mark/R-6173-2016; Manager, CSD Publications/B-2789-2015
OI Murphy, Daniel/0000-0002-8091-7235; Hoose, Corinna/0000-0003-2827-5789;
Diao, Minghui/0000-0003-0324-0897; Zondlo, Mark/0000-0003-2302-9554;
FU NSF [AGS-0840732, AGS-1036275]; NASA [NNX07AL11G, NNX08AH57G]; NASA
Earth Science Division Atmospheric Composition program [NNH11AQ58UI]
FX We thank D. S. Thomson and G. Kulkarni for assistance with the
measurements; S. Solomon for advice on manuscript preparation; all
participants of the field studies for their efforts, in particular the
air and ground crews of the NASA WB-57F and DC-8 and NSF G-V; and O.
Seland, D. Olivie, and A. Kirkevag for providing particle surface area
densities from CAM4-Oslo simulations. The MDC12C1 2011 Land Cover Type
data were obtained through the online Data Pool at the NASA Land
Processes Distributed Active Archive Center, U.S. Geological
Survey/Earth Resources Observation and Science Center, Sioux Falls,
South Dakota (https://lpdaac.usgs.gov/get_data). M.A.Z. acknowledges
support from NSF AGS-0840732 and AGS-1036275, M. D. acknowledges a NASA
Earth and Space Science Graduate Fellowship, and C. H. T. acknowledges
support from the NASA Radiation Sciences Program award numbers
NNX07AL11G and NNX08AH57G. This research was supported by the NASA Earth
Science Division Atmospheric Composition program award number
NNH11AQ58UI. Author contributions: single-particle MS, EM, data
analysis, and paper writing (D.J.C.); counterflow virtual impactor
development, mass spectrometer development, single-particle MS, data
analysis, and paper writing (K. D. F.); compilation of INAS densities
from laboratory data, deriving the model-based estimates of upper
tropospheric IN, and paper writing (C. H.); measurement of water vapor
mixing ratio, analysis of relative humidity data, and paper writing
(J.B.S., M.A.Z, and M. D.); mission planning, data analysis, and paper
writing (E.J.J); TC4 instrument design and data acquisition, paper
writing (C. H. T.); and mass spectrometer development, single-particle
MS, data analysis, and paper writing (D.M.M.).
NR 31
TC 147
Z9 147
U1 18
U2 182
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD JUN 14
PY 2013
VL 340
IS 6138
BP 1320
EP 1324
DI 10.1126/science.1234145
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 163FC
UT WOS:000320320200042
PM 23661645
ER
PT J
AU Gehrels, N
Cannizzo, JK
AF Gehrels, Neil
Cannizzo, John K.
TI High-energy transients
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Review
DE gamma rays; general; telescopes; bursts; galactic transients
ID GAMMA-RAY BURST; MASSIVE BLACK-HOLE; TIDALLY DISRUPTED STAR; X-RAY;
RADIATIVE MECHANISM; NEUTRON-STAR; GRB 101225A; EV-LACERTAE; SGR
1900+14; JET BREAKS
AB We present an overview of high-energy transients in astrophysics, highlighting important advances over the past 50 years. We begin with early discoveries of gamma-ray transients, and then delve into physical details associated with a variety of phenomena. We discuss some of the unexpected transients found by Fermi and Swift, many of which are not easily classifiable or in some way challenge conventional wisdom. These objects are important insofar as they underscore the necessity of future, more detailed studies.
C1 [Gehrels, Neil; Cannizzo, John K.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Div, Greenbelt, MD 20771 USA.
[Cannizzo, John K.] Univ Maryland Baltimore Cty, CRESST Joint Ctr Astrophys, Baltimore, MD 21250 USA.
RP Gehrels, N (reprint author), NASA, Goddard Space Flight Ctr, Astroparticle Phys Div, Greenbelt, MD 20771 USA.
EM gehrels@milkyway.gsfc.nasa.gov
NR 87
TC 3
Z9 3
U1 0
U2 3
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-503X
EI 1471-2962
J9 PHILOS T R SOC A
JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci.
PD JUN 13
PY 2013
VL 371
IS 1992
AR 20120270
DI 10.1098/rsta.2012.0270
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 133TB
UT WOS:000318162100008
PM 23630376
ER
PT J
AU Seo, BJ
Nissly, C
Troy, M
Angeli, G
Ford, V
Stepp, L
Williams, E
AF Seo, Byoung-Joon
Nissly, Carl
Troy, Mitchell
Angeli, George
Ford, Virginia
Stepp, Larry
Williams, Eric
TI Approximation of normalized point source sensitivity using power
spectral density and slopes of wavefront aberration
SO APPLIED OPTICS
LA English
DT Article
AB We have investigated two approximation methods for estimating the normalized point source sensitivity (PSSN), which is a recently developed optical performance metric for telescopes. One is an approximation based on the power spectral density (PSD) of the wavefront error. The other is the root-square-sum of the wavefront slope. We call these approximations beta approximation and SlopeRMS approximation, respectively. Our analysis shows that for the Thirty Meter Telescope (TMT), the uncertainty of the beta approximation is less than 1 x 10(-3) if the PSSN is better than 0.95, assuming the input PSD estimation is accurate. In addition, we find that the SlopeRMS approximation is a simple method for estimating the worst-case PSSN value in the specific situation when the PSSN is dominated by low-frequency aberrations. Therefore, the SlopeRMS approximation is expected to be useful for specifying a mirror surface for mirror vendors. Accordingly, TMT has a plan to adopt the SlopeRMS approximation for its M2 and M3 polishing specification. (C) 2013 Optical Society of America
C1 [Seo, Byoung-Joon; Nissly, Carl; Troy, Mitchell] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Angeli, George; Ford, Virginia; Stepp, Larry; Williams, Eric] Thirty Meter Telescope Observ, Pasadena, CA 91107 USA.
RP Seo, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Byoung-Joon.Seo@jpl.nasa.gov
FU California Institute of Technology; National Aeronautics and Space
Administration; TMT partner institutions; Gordon and Betty Moore
Foundation; Canada Foundation for Innovation; Ontario Ministry of
Research and Innovation; National Research Council of Canada; Natural
Sciences and Engineering Research Council of Canada; British Columbia
Knowledge Development Fund; Association of Universities for Research in
Astronomy (AURA); U.S. National Science Foundation
FX This research was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, and was sponsored by the California
Institute of Technology and the National Aeronautics and Space
Administration. The authors gratefully acknowledge the support of the
TMT partner institutions. They are the Association of Canadian
Universities for Research in Astronomy (ACURA), the California Institute
of Technology, and the University of California. This work was supported
as well by the Gordon and Betty Moore Foundation, the Canada Foundation
for Innovation, the Ontario Ministry of Research and Innovation, the
National Research Council of Canada, the Natural Sciences and
Engineering Research Council of Canada, the British Columbia Knowledge
Development Fund, the Association of Universities for Research in
Astronomy (AURA), and the U.S. National Science Foundation.
NR 13
TC 0
Z9 1
U1 1
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
J9 APPL OPTICS
JI Appl. Optics
PD JUN 10
PY 2013
VL 52
IS 17
BP 3910
EP 3922
DI 10.1364/AO.52.003910
PG 13
WC Optics
SC Optics
GA 160HW
UT WOS:000320110900003
PM 23759838
ER
PT J
AU Yao, HM
Wright, MW
Marciante, JR
AF Yao, Haomin
Wright, Malcolm W.
Marciante, John R.
TI Optimization of resonantly cladding-pumped erbium-doped fiber amplifiers
for space-borne applications
SO APPLIED OPTICS
LA English
DT Article
ID LARGE-MODE-AREA; OUTPUT POWER; LASER; EFFICIENCY
AB Lasers for use in space-borne applications require ultrahigh efficiency due to limited heat dissipation and power generation capacity. In particular, interplanetary optical communication systems require high-efficiency, moderate-power (>4 W) optical transmitters in the 1600 nm wavelength range. Resonantly pumped dual-clad erbium-doped fiber lasers are best suited for this purpose. Parametric numerical optimizations are performed using a two-level propagation model modified to include spatial effects specific to large-mode-area fibers. Propagation loss mechanisms are found to be limiting factors due to the relatively low cross-sections and low quenching-free doping densities of erbium. Although experimental reports have demonstrated efficiencies up to 33%, simulation results indicate that over 53% power-conversion efficiency can be achieved using commercial fibers, and over 75% can be achieved using custom fibers employing propagation-loss mitigation strategies. (C) 2013 Optical Society of America
C1 [Yao, Haomin; Marciante, John R.] Univ Rochester, Inst Opt, Rochester, NY 14627 USA.
[Wright, Malcolm W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yao, HM (reprint author), Univ Rochester, Inst Opt, Rochester, NY 14627 USA.
EM hayao@optics.rochester.edu
FU NASA/JPL [1440052]
FX H. Yao and J. R. Marciante were supported in part by NASA/JPL under
Subcontract No. 1440052. The work of M. W. Wright was carried out at the
Jet Propulsion Laboratory, California Institute of Technology under
contract with the National Aeronautics and Space Administration. H. Yao
thanks Jordan Leidner for helpful discussions.
NR 29
TC 2
Z9 2
U1 0
U2 6
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
J9 APPL OPTICS
JI Appl. Optics
PD JUN 10
PY 2013
VL 52
IS 17
BP 3923
EP 3930
DI 10.1364/AO.52.003923
PG 8
WC Optics
SC Optics
GA 160HW
UT WOS:000320110900004
PM 23759839
ER
PT J
AU Bautista, MA
Fivet, V
Quinet, P
Dunn, J
Gull, TR
Kallman, TR
Mendoza, C
AF Bautista, M. A.
Fivet, V.
Quinet, P.
Dunn, J.
Gull, T. R.
Kallman, T. R.
Mendoza, C.
TI UNCERTAINTIES IN ATOMIC DATA AND THEIR PROPAGATION THROUGH SPECTRAL
MODELS. I.
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atomic data; atomic processes; line: formation; methods: data analysis;
molecular data; molecular processes; techniques: spectroscopic
ID FORBIDDEN LINES; FE II; IRON
AB We present a method for computing uncertainties in spectral models, i.e., level populations, line emissivities, and emission line ratios, based upon the propagation of uncertainties originating from atomic data. We provide analytic expressions, in the form of linear sets of algebraic equations, for the coupled uncertainties among all levels. These equations can be solved efficiently for any set of physical conditions and uncertainties in the atomic data. We illustrate our method applied to spectral models of O III and Fe II and discuss the impact of the uncertainties on atomic systems under different physical conditions. As to intrinsic uncertainties in theoretical atomic data, we propose that these uncertainties can be estimated from the dispersion in the results from various independent calculations. This technique provides excellent results for the uncertainties in A-values of forbidden transitions in [Fe II].
C1 [Bautista, M. A.; Fivet, V.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Fivet, V.; Quinet, P.] Univ Mons UMONS, B-7000 Mons, Belgium.
[Fivet, V.; Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium.
[Dunn, J.] Georgia Perimeter Coll, Dept Phys Sci, Dunwoody, GA 30338 USA.
[Gull, T. R.] NASA, Code 667, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kallman, T. R.] NASA, Code 662, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mendoza, C.] IVIC, Ctr Fis, Caracas 1020A, Venezuela.
RP Bautista, MA (reprint author), Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
EM manuel.bautista@wmich.edu
FU NASA Astronomy and Physics Research and Analysis Program [NNX09AB99G]
FX We acknowledge financial support from grants from the NASA Astronomy and
Physics Research and Analysis Program (award NNX09AB99G). The Belgian
FRS-FNRS is also acknowledged.
NR 10
TC 9
Z9 9
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 JUN 10
PY 2013
VL 770
IS 1
AR 15
DI 10.1088/0004-637X/770/1/15
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400015
ER
PT J
AU Cordiner, MA
Buckle, JV
Wirstrom, ES
Olofsson, AOH
Charnley, SB
AF Cordiner, M. A.
Buckle, J. V.
Wirstrom, E. S.
Olofsson, A. O. H.
Charnley, S. B.
TI ON THE UBIQUITY OF MOLECULAR ANIONS IN THE DENSE INTERSTELLAR MEDIUM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: clouds; ISM: molecules; stars:
formation
ID CARBON-CHAIN MOLECULES; STAR-FORMATION; NEGATIVE-IONS; LINE
OBSERVATIONS; DARK CLOUDS; CORES; CHEMISTRY; TMC-1; MILLIMETER; C6H
AB Results are presented from a survey for molecular anions in seven nearby Galactic star-forming cores and molecular clouds. The hydrocarbon anion C6H- is detected in all seven target sources, including four sources where no anions have been previously detected: L1172, L1389, L1495B, and TMC-1C. The C6H-/C6H column density ratio is greater than or similar to 1.0% in every source, with a mean value of 3.0% (and standard deviation 0.92%). Combined with previous detections, our results show that anions are ubiquitous in dense clouds wherever C6H is present. The C6H-/C6H ratio is found to show a positive correlation with molecular hydrogen number density, and with the apparent age of the cloud. We also report the first detection of C4H- in TMC-1 (at 4.8 sigma confidence), and derive an anion-to-neutral ratio C4H-/C4H = (1.2 +/- 0.4) x 10(-5)(= 0.0012% +/- 0.0004%). Such a low value compared with C6H- highlights the need for a revised radiative electron attachment rate for C4H. Chemical model calculations show that the observed C4H- could be produced as a result of reactions of oxygen atoms with C5H- and C6H-.
C1 [Cordiner, M. A.; Wirstrom, E. S.; Charnley, S. B.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cordiner, M. A.; Wirstrom, E. S.; Charnley, S. B.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cordiner, M. A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Buckle, J. V.] Univ Cambridge, Cavendish Astrophys Grp, Cambridge CB3 0HE, England.
[Buckle, J. V.] Univ Cambridge, Inst Astron, Kavli Inst Cosmol, Cambridge CB3 0HE, England.
[Wirstrom, E. S.; Olofsson, A. O. H.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
RP Cordiner, MA (reprint author), NASA, Astrochem Lab, Goddard Space Flight Ctr, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM martin.cordiner@nasa.gov
OI Wirstrom, Eva/0000-0002-0656-876X
FU NASA Exobiology Program through the Goddard Center for Astrobiology;
NASA Astrobiology Institute through the Goddard Center for Astrobiology
FX This research was supported by the NASA Exobiology Program and the NASA
Astrobiology Institute through the Goddard Center for Astrobiology. We
gratefully acknowledge the assistance of Tom Millar and Catherine Walsh
during the 2010 Onsala HC3N observing run. J.V.B. thanks John
Richer for support. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc.
NR 52
TC 16
Z9 16
U1 2
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 JUN 10
PY 2013
VL 770
IS 1
AR 48
DI 10.1088/0004-637X/770/1/48
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400048
ER
PT J
AU Guiriec, S
Daigne, F
Hascoet, R
Vianello, G
Ryde, F
Mochkovitch, R
Kouveliotou, C
Xiong, S
Bhat, PN
Foley, S
Gruber, D
Burgess, JM
McGlynn, S
McEnery, J
Gehrels, N
AF Guiriec, S.
Daigne, F.
Hascoet, R.
Vianello, G.
Ryde, F.
Mochkovitch, R.
Kouveliotou, C.
Xiong, S.
Bhat, P. N.
Foley, S.
Gruber, D.
Burgess, J. M.
McGlynn, S.
McEnery, J.
Gehrels, N.
TI EVIDENCE FOR A PHOTOSPHERIC COMPONENT IN THE PROMPT EMISSION OF THE
SHORT GRB 120323A AND ITS EFFECTS ON THE GRB HARDNESS-LUMINOSITY
RELATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; cosmology: miscellaneous; gamma-ray burst:
individual (GRB 120323A); gamma rays: stars; radiation mechanisms:
non-thermal; radiation mechanisms: thermal
ID GAMMA-RAY-BURSTS; INTERNAL SHOCK MODEL; PEAK ENERGY; FERMI OBSERVATIONS;
THERMAL EMISSION; SPECTRAL CATALOG; BATSE OBSERVATIONS; NEUTRON-STARS;
BLACK-HOLES; EVOLUTION
AB The short GRB 120323A had the highest flux ever detected with the Gamma-Ray Burst Monitor on board the Fermi Gamma-Ray Space Telescope. Here we study its remarkable spectral properties and their evolution using two spectral models: (1) a single emission component scenario, where the spectrum is modeled by the empirical Band function (a broken power law), and (2) a two-component scenario, where thermal (a Planck-like function) emission is observed simultaneously with a non-thermal component (a Band function). We find that the latter model fits the integrated burst spectrum significantly better than the former, and that their respective spectral parameters are dramatically different: when fit with a Band function only, the E-peak of the event is unusually soft for a short gamma-ray burst (GRB; 70 keV compared to an average of 300 keV), while adding a thermal component leads to more typical short GRB values (E-peak similar to 300 keV). Our time-resolved spectral analysis produces similar results. We argue here that the two-component model is the preferred interpretation for GRB 120323A based on (1) the values and evolution of the Band function parameters of the two component scenario, which are more typical for a short GRB, and (2) the appearance in the data of a significant hardness-intensity correlation, commonly found in GRBs, when we employee two-component model fits; the correlation is non-existent in the Band-only fits. GRB 110721A, a long burst with an intense photospheric emission, exhibits the exact same behavior. We conclude that GRB 120323A has a strong photospheric emission contribution, observed for the first time in a short GRB. Magnetic dissipation models are difficult to reconcile with these results, which instead favor photospheric thermal emission and fast cooling synchrotron radiation from internal shocks. Finally, we derive a possibly universal hardness-luminosity relation in the source frame using a larger set of GRBs (L-i(Band) = (1.59 +/- 0.84) x 10(50)(E (rest)(peak,i))(1.33 +/- 0.07) erg s(-1)), which could be used as a possible redshift estimator for cosmology.
C1 [Guiriec, S.; McEnery, J.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Daigne, F.; Hascoet, R.; Mochkovitch, R.] Univ Paris 06, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Daigne, F.; Hascoet, R.; Mochkovitch, R.] CNRS, F-75014 Paris, France.
[Vianello, G.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Ryde, F.] AlbaNova, Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden.
[Ryde, F.] AlbaNova, Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden.
[Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Off Sci & Technol, Huntsville, AL 35812 USA.
[Xiong, S.; Bhat, P. N.; Burgess, J. M.] Univ Alabama, NSSTC, Huntsville, AL 35805 USA.
[Foley, S.; McGlynn, S.] Univ Coll Dublin, UCD Sch Phys, Dublin 4, Ireland.
[Gruber, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[McEnery, J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Guiriec, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM sylvain.guiriec@nasa.gov
OI Burgess, James/0000-0003-3345-9515
FU NASA Postdoctoral Program (NPP) at the NASA/Goddard Space Flight Center;
NASA; Cycle-4 NASA Fermi Guest Investigator program; Irish Research
Council for Science, Engineering, and Technology; Marie Curie Actions
FX S.G. was supported by the NASA Postdoctoral Program (NPP) at the
NASA/Goddard Space Flight Center, administered by the Oak Ridge
Associated Universities through a contract with NASA. S.G. acknowledges
financial support through the Cycle-4 NASA Fermi Guest Investigator
program. S.F. acknowledges the support of the Irish Research Council for
Science, Engineering, and Technology, cofunded by Marie Curie Actions
under FP7. We thank Valentin Pal'shin for his private communication on
the propagation time between the WIND and Fermi spacecraft as well as
Adam Goldstein, Michael Briggs, and Valerie Connaughton for their useful
comments which helped to improve the quality of the manuscript. Finally,
we thank the referee and the editor for their useful comments, which
increased the quality of the article.
NR 112
TC 45
Z9 45
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 JUN 10
PY 2013
VL 770
IS 1
AR 32
DI 10.1088/0004-637X/770/1/32
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400032
ER
PT J
AU Hoard, DW
Debes, JH
Wachter, S
Leisawitz, DT
Cohen, M
AF Hoard, D. W.
Debes, John H.
Wachter, Stefanie
Leisawitz, David T.
Cohen, Martin
TI THE WIRED SURVEY. IV. NEW DUST DISKS FROM THE McCOOK & SION WHITE DWARF
CATALOG
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; surveys; white dwarfs
ID ALL-SKY SURVEY; EXCESS INFRARED RADIATION; SPITZER-SPACE-TELESCOPE;
PALOMAR-GREEN SURVEY; DEBRIS DISKS; SPECTROSCOPIC ANALYSIS;
PLANETARY-NEBULAE; DATA RELEASE; CIRCUMSTELLAR DUST; COOL COMPANIONS
AB We have compiled photometric data from the Wide-field Infrared Survey Explorer All Sky Survey and other archival sources for the more than 2200 objects in the original McCook & Sion Catalog of Spectroscopically Identified White Dwarfs. We applied color-selection criteria to identify 28 targets whose infrared spectral energy distributions depart from the expectation for the white dwarf (WD) photosphere alone. Seven of these are previously known WDs with circumstellar dust disks, five are known central stars of planetary nebulae, and six were excluded for being known binaries or having possible contamination of their infrared photometry. We fit WD models to the spectral energy distributions of the remaining ten targets, and find seven new candidates with infrared excess suggesting the presence of a circumstellar dust disk. We compare the model dust disk properties for these new candidates with a comprehensive compilation of previously published parameters for known WDs with dust disks. It is possible that the current census of WDs with dust disks that produce an excess detectable at K-band and shorter wavelengths is close to complete for the entire sample of known WDs to the detection limits of existing near-IR all-sky surveys. The WD dust disk candidates now being found using longer wavelength infrared data are drawn from a previously underrepresented region of parameter space, in which the dust disks are overall cooler, narrower in radial extent, and/or contain fewer emitting grains.
C1 [Hoard, D. W.; Wachter, Stefanie] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Hoard, D. W.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Debes, John H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Leisawitz, David T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cohen, Martin] Monterey Inst Res Astron, Marina, CA 93933 USA.
EM hoard@mpia.de
OI Hoard, Donald W./0000-0002-6800-6519
FU National Aeronautics and Space Administration (NASA); National Science
Foundation (NSF); The American Association of Variable Star Observers
(AAVSO) Photometric All-Sky Survey (APASS); Robert Martin Ayers Sciences
Fund; NASA's Astrophysics Data System; The Galaxy Evolution Explorer
(GALEX); NASA by Caltech under NASA contract [NAS-98034]; Research in
Astronomy, Inc., under NASA contract [NAS5-26555]; NASA Office of Space
Science [NNX09AF08G]; NASA; Alfred P. Sloan Foundation; Participating
Institutions; NSF; U. S. Department of Energy; Japanese Monbukagakusho;
Max Planck Society; Higher Education Funding Council for England
FX This work is based on data, data products, and other resources obtained
from (1) the Two Micron All Sky Survey (2MASS), a joint project of the
University of Massachusetts and the Infrared Processing and Analysis
Center (IPAC)/California Institute of Technology (Caltech), funded by
the National Aeronautics and Space Administration (NASA) and the
National Science Foundation (NSF). (2) The American Association of
Variable Star Observers (AAVSO) Photometric All-Sky Survey (APASS),
funded by the Robert Martin Ayers Sciences Fund. (3) NASA's Astrophysics
Data System. (4) The Galaxy Evolution Explorer (GALEX), a NASA Small
Explorer launched in 2003 April and operated for NASA by Caltech under
NASA contract NAS-98034. The GALEX data products were obtained from the
Multimission Archive at the Space Telescope Science Institute (MAST).
STScI is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for
non-HST data is provided by the NASA Office of Space Science via grant
NNX09AF08G and by other grants and contracts. (5) The NASA/IPAC Infrared
Science Archive (IRSA), which is operated by the Jet Propulsion
Laboratory (JPL), Caltech, under a contract with NASA, including the
Spitzer Enhanced Imaging Products based on observations obtained with
the Spitzer Space Telescope, which is operated by JPL, Caltech, under a
contract with NASA. (6) The SIMBAD database, operated at CDS,
Strasbourg, France. (7) The Sloan Digital Sky Survey (SDSS and SDSS-II),
whose funding has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the NSF, the U. S. Department of Energy,
NASA, 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. (8) The
Wide-field Infrared Survey Explorer (WISE), which is a joint project of
the University of California, Los Angeles, and JPL, Caltech, funded by
NASA.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2013
VL 770
IS 1
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DI 10.1088/0004-637X/770/1/21
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400021
ER
PT J
AU Kitiashvili, IN
Kosovichev, AG
Lele, SK
Mansour, NN
Wray, AA
AF Kitiashvili, I. N.
Kosovichev, A. G.
Lele, S. K.
Mansour, N. N.
Wray, A. A.
TI UBIQUITOUS SOLAR ERUPTIONS DRIVEN BY MAGNETIZED VORTEX TUBES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; magnetohydrodynamics (MHD); methods: numerical;
plasmas; Sun: chromosphere; Sun: photosphere; turbulence
ID RESOLUTION OBSERVATIONS; NUMERICAL-SIMULATION; SMALL-SCALE; CONVECTION;
SPICULES; OSCILLATIONS; CORONA; SUN; GRANULATION; PHOTOSPHERE
AB The solar surface is covered by high-speed jets transporting mass and energy into the solar corona and feeding the solar wind. The most prominent of these jets have been known as spicules. However, the mechanism initiating these eruption events is still unknown. Using realistic numerical simulations we find that small-scale eruptions are produced by ubiquitous magnetized vortex tubes generated by the Sun's turbulent convection in subsurface layers. The swirling vortex tubes (resembling tornadoes) penetrate into the solar atmosphere, capture and stretch background magnetic field, and push the surrounding material up, generating shocks. Our simulations reveal complicated high-speed flow patterns and thermodynamic and magnetic structure in the erupting vortex tubes. The main new results are: (1) the eruptions are initiated in the subsurface layers and are driven by high-pressure gradients in the subphotosphere and photosphere and by the Lorentz force in the higher atmosphere layers; (2) the fluctuations in the vortex tubes penetrating into the chromosphere are quasi-periodic with a characteristic period of 2-5 minutes; and (3) the eruptions are highly non-uniform: the flows are predominantly downward in the vortex tube cores and upward in their surroundings; the plasma density and temperature vary significantly across the eruptions.
C1 [Kitiashvili, I. N.; Kosovichev, A. G.] Stanford Univ, Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Kitiashvili, I. N.; Lele, S. K.; Mansour, N. N.; Wray, A. A.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA.
[Kitiashvili, I. N.] Kazan Fed Univ, Kazan 420008, Russia.
[Lele, S. K.] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
[Mansour, N. N.; Wray, A. A.] NASA, Ames Res Ctr, Mountain View, CA 94040 USA.
RP Kitiashvili, IN (reprint author), Stanford Univ, Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM irinasun@stanford.edu
FU NASA [NNX10AC55G]; International Space Science Institute (Bern); Nordita
(Stockholm)
FX The simulation results were obtained on the NASA's Pleiades
supercomputer at the NASA Ames Research Center. This work was partially
supported by the NASA grant NNX10AC55G, the International Space Science
Institute (Bern) and Nordita (Stockholm).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2013
VL 770
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AR 37
DI 10.1088/0004-637X/770/1/37
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400037
ER
PT J
AU Kopparapu, RK
Ramirez, R
Kasting, JF
Eymet, V
Robinson, TD
Mahadevan, S
Terrien, RC
Domagal-Goldman, S
Meadows, V
Deshpande, R
AF Kopparapu, Ravi Kumar
Ramirez, Ramses
Kasting, James F.
Eymet, Vincent
Robinson, Tyler D.
Mahadevan, Suvrath
Terrien, Ryan C.
Domagal-Goldman, Shawn
Meadows, Victoria
Deshpande, Rohit
TI HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES (vol 765, pg
131, 2013)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
ID CLIMATES; SCATTERING; STABILITY; PLANET
C1 [Kopparapu, Ravi Kumar; Ramirez, Ramses; Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Kopparapu, Ravi Kumar; Ramirez, Ramses; Kasting, James F.] Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA.
[Kopparapu, Ravi Kumar; Ramirez, Ramses; Kasting, James F.; Mahadevan, Suvrath; Terrien, Ryan C.; Deshpande, Rohit] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Eymet, Vincent] Univ Bordeaux 1, Lab Astrophys Bordeaux, UMR 5804, F-33270 Floirac, France.
[Robinson, Tyler D.; Meadows, Victoria] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Robinson, Tyler D.; Mahadevan, Suvrath; Terrien, Ryan C.; Deshpande, Rohit] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Domagal-Goldman, Shawn] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA.
RP Kopparapu, RK (reprint author), Penn State Univ, Dept Geosci, 443 Deike Bldg, University Pk, PA 16802 USA.
RI Domagal-Goldman, Shawn/F-3521-2012
OI Domagal-Goldman, Shawn/0000-0003-0354-9325
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2013
VL 770
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AR 82
DI 10.1088/0004-637X/770/1/82
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400082
ER
PT J
AU Laming, JM
Moses, JD
Ko, YK
Ng, CK
Rakowski, CE
Tylka, AJ
AF Laming, J. Martin
Moses, J. Daniel
Ko, Yuan-Kuen
Ng, Chee K.
Rakowski, Cara E.
Tylka, Allan J.
TI ON THE REMOTE DETECTION OF SUPRATHERMAL IONS IN THE SOLAR CORONA AND
THEIR ROLE AS SEEDS FOR SOLAR ENERGETIC PARTICLE PRODUCTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; shock waves; Sun: corona; Sun: coronal mass
ejections (CMEs)
ID NON-WKB MODELS; MAGNETIC RECONNECTION; SHOCK-WAVES; ELECTRON
ACCELERATION; STOCHASTIC ACCELERATION; PERPENDICULAR SHOCKS;
ASTROPHYSICAL SHOCKS; MASS EJECTIONS; OBLIQUE SHOCKS; CHARGE STATES
AB Forecasting large solar energetic particle (SEP) events associated with shocks driven by fast coronal mass ejections (CMEs) poses a major difficulty in the field of space weather. Besides issues associated with CME initiation, the SEP intensities are difficult to predict, spanning three orders of magnitude at any given CME speed. Many lines of indirect evidence point to the pre-existence of suprathermal seed particles for injection into the acceleration process as a key ingredient limiting the SEP intensity of a given event. This paper outlines the observational and theoretical basis for the inference that a suprathermal particle population is present prior to large SEP events, explores various scenarios for generating seed particles and their observational signatures, and explains how such suprathermals could be detected through measuring the wings of the H I Ly alpha line.
C1 [Laming, J. Martin; Moses, J. Daniel; Ko, Yuan-Kuen] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ng, Chee K.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Tylka, Allan J.] NASA, GSFC, Greenbelt, MD 20771 USA.
RP Laming, JM (reprint author), USN, Res Lab, Div Space Sci, Code 7684, Washington, DC 20375 USA.
RI Tylka, Allan/G-9592-2014
FU Office of Naval Research; NASA Astrophysics Data Analysis Program
[NNH10A009I]
FX This work was supported by basic research funds of the Office of Naval
Research. J.M.L. and C.E.R. also acknowledge support under grant
NNH10A009I from the NASA Astrophysics Data Analysis Program. We also
thank Ron Murphy for reading a draft of the paper and providing many
helpful comments.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2013
VL 770
IS 1
AR 73
DI 10.1088/0004-637X/770/1/73
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400073
ER
PT J
AU Leutenegger, MA
Cohen, DH
Sundqvist, JO
Owocki, SP
AF Leutenegger, Maurice A.
Cohen, David H.
Sundqvist, Jon O.
Owocki, Stanley P.
TI CONSTRAINTS ON POROSITY AND MASS LOSS IN O-STAR WINDS FROM THE MODELING
OF X-RAY EMISSION LINE PROFILE SHAPES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radiative transfer; stars: early-type; stars: individual (zeta Puppis);
stars: mass-loss; stars: winds, outflows; X-rays: stars
ID REFLECTION GRATING SPECTROMETER; DRIVEN STELLAR WINDS; ZETA-PUPPIS;
XMM-NEWTON; HOT STARS; SPECTROSCOPY; EVOLUTION; SPECTRA; I.
AB We fit X-ray emission line profiles in high resolution XMM-Newton and Chandra grating spectra of the early O supergiant zeta Pup with models that include the effects of porosity in the stellar wind. We explore the effects of porosity due to both spherical and flattened clumps. We find that porosity models with flattened clumps oriented parallel to the photosphere provide poor fits to observed line shapes. However, porosity models with isotropic clumps can provide acceptable fits to observed line shapes, but only if the porosity effect is moderate. We quantify the degeneracy between porosity effects from isotropic clumps and the mass-loss rate inferred from the X-ray line shapes, and we show that only modest increases in the mass-loss rate (less than or similar to 40%) are allowed if moderate porosity effects (h(infinity) less than or similar to R-*) are assumed to be important. Large porosity lengths, and thus strong porosity effects, are ruled out regardless of assumptions about clump shape. Thus, X-ray mass-loss rate estimates are relatively insensitive to both optically thin and optically thick clumping. This supports the use of X-ray spectroscopy as a mass-loss rate calibration for bright, nearby O stars.
C1 [Leutenegger, Maurice A.] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Leutenegger, Maurice A.] NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Leutenegger, Maurice A.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Cohen, David H.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA.
[Sundqvist, Jon O.; Owocki, Stanley P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Sundqvist, Jon O.] Univ Sternwarte Munchen, D-81679 Munich, Germany.
RP Leutenegger, MA (reprint author), NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Maurice.A.Leutenegger@nasa.gov
FU National Aeronautics and Space Administration through Chandra award
[AR7-8002X]; ADAP award [NNX11AD26G]; NASA [ATP NNX11AC40G]; DFG
[Pu117/8-1]
FX We acknowledge the comments of the referee, Achim Feldmeier, which
significantly improved the presentation of this article. Support for
this work was provided by the National Aeronautics and Space
Administration through Chandra award number AR7-8002X and ADAP award
number NNX11AD26G to Swarthmore College. J.O.S. and S.P.O. acknowledge
support from NASA award ATP NNX11AC40G to the University of Delaware.
J.O.S. also acknowledges current support from DFG-grant Pu117/8-1.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2013
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DI 10.1088/0004-637X/770/1/80
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400080
ER
PT J
AU Masiero, JR
Mainzer, AK
Bauer, JM
Grav, T
Nugent, CR
Stevenson, R
AF Masiero, Joseph R.
Mainzer, A. K.
Bauer, J. M.
Grav, T.
Nugent, C. R.
Stevenson, R.
TI ASTEROID FAMILY IDENTIFICATION USING THE HIERARCHICAL CLUSTERING METHOD
AND WISE/NEOWISE PHYSICAL PROPERTIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets; asteroids: general
ID MAIN BELT ASTEROIDS; INFRARED-SURVEY-EXPLORER; SIZE DISTRIBUTION;
ELEMENTS; NEOWISE; VESTA; DISTRIBUTIONS; SIMULATIONS; IMPACTS; COLOR
AB Using albedos from WISE/NEOWISE to separate distinct albedo groups within the Main Belt asteroids, we apply the Hierarchical Clustering Method to these subpopulations and identify dynamically associated clusters of asteroids. While this survey is limited to the similar to 35% of known Main Belt asteroids that were detected by NEOWISE, we present the families linked from these objects as higher confidence associations than can be obtained from dynamical linking alone. We find that over one-third of the observed population of the Main Belt is represented in the high-confidence cores of dynamical families. The albedo distribution of family members differs significantly from the albedo distribution of background objects in the same region of the Main Belt; however, interpretation of this effect is complicated by the incomplete identification of lower-confidence family members. In total we link 38,298 asteroids into 76 distinct families. This work represents a critical step necessary to debias the albedo and size distributions of asteroids in the Main Belt and understand the formation and history of small bodies in our solar system.
C1 [Masiero, Joseph R.; Mainzer, A. K.; Bauer, J. M.; Nugent, C. R.; Stevenson, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, J. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91109 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ USA.
[Nugent, C. R.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
RP Masiero, JR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-601, Pasadena, CA 91109 USA.
EM Joseph.Masiero@jpl.nasa.gov; amainzer@jpl.nasa.gov;
James.Bauer@jpl.nasa.gov; tgrav@psi.edu; cnugent@ucla.edu;
Rachel.Stevenson@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU NASA Postdoctoral Program at JPL; National Aeronautics and Space
Administration; Planetary Science Division of the National Aeronautics
and Space Administration
FX J.M. was partially supported by an appointment to the NASA Postdoctoral
Program at JPL, administered by Oak Ridge Associated Universities
through a contract with NASA. The authors thank the referee Alberto
Cellino for comments that greatly improved the paper, and John Dailey
for helpful discussions on implementation of algorithms. 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. We
gratefully acknowledge the extraordinary services specific to NEOWISE
contributed by the International Astronomical Union's Minor Planet
Center, operated by the Harvard-Smithsonian Center for Astrophysics, and
the Central Bureau for Astronomical Telegrams, operated by Harvard
University.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2013
VL 770
IS 1
AR 7
DI 10.1088/0004-637X/770/1/7
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400007
ER
PT J
AU Oemler, A
Dressler, A
Gladders, MG
Rigby, JR
Bai, L
Kelson, D
Villanueva, E
Fritz, J
Rieke, G
Poggianti, BM
Vulcani, B
AF Oemler, Augustus, Jr.
Dressler, Alan
Gladders, Michael G.
Rigby, Jane R.
Bai, Lei
Kelson, Daniel
Villanueva, Edward
Fritz, Jacopo
Rieke, George
Poggianti, Bianca M.
Vulcani, Benedetta
TI THE IMACS CLUSTER BUILDING SURVEY. I. DESCRIPTION OF THE SURVEY AND
ANALYSIS METHODS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: evolution; galaxies: photometry;
galaxies: star formation
ID STAR-FORMATION RATES; MULTIBAND IMAGING PHOTOMETER; FORMATION RATE
INDICATORS; DISK GALAXIES; RICH CLUSTERS; STARBURST GALAXIES; INFRARED
GALAXIES; DISTANT CLUSTERS; FORMING GALAXIES; S0 GALAXIES
AB The IMACS Cluster Building Survey uses the wide field spectroscopic capabilities of the IMACS spectrograph on the 6.5 m Baade Telescope to survey the large-scale environment surrounding rich intermediate-redshift clusters of galaxies. The goal is to understand the processes which may be transforming star-forming field galaxies into quiescent cluster members as groups and individual galaxies fall into the cluster from the surrounding supercluster. This first paper describes the survey: the data taking and reduction methods. We provide new calibrations of star formation rates (SFRs) derived from optical and infrared spectroscopy and photometry. We demonstrate that there is a tight relation between the observed SFR per unit B luminosity, and the ratio of the extinctions of the stellar continuum and the optical emission lines. With this, we can obtain accurate extinction-corrected colors of galaxies. Using these colors as well as other spectral measures, we determine new criteria for the existence of ongoing and recent starbursts in galaxies.
C1 [Oemler, Augustus, Jr.; Dressler, Alan; Kelson, Daniel; Villanueva, Edward] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Gladders, Michael G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Bai, Lei] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Fritz, Jacopo] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Rieke, George] Univ Arizona, Steward Observ, Tucson, AZ USA.
[Poggianti, Bianca M.; Vulcani, Benedetta] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Vulcani, Benedetta] Univ Padua, Dept Astron, I-35122 Padua, Italy.
RP Oemler, A (reprint author), Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA.
EM oemler@obs.carnegiescience.edu
RI Rigby, Jane/D-4588-2012;
OI Rigby, Jane/0000-0002-7627-6551; Vulcani, Benedetta/0000-0003-0980-1499
FU NSF [AST-0407343]; NASA; ASI [I/016/07/0]; ASI-INAF [I/009/10/0];
National Aeronautics and Space Administration
FX Oemler and Dressler acknowledge support of the NSF Grant AST-0407343.
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 to A.D., A.O., J.R.R., L.B., and G.R. by NASA
through an award issued by JPL/Caltech. Support for this work was
provided by NASA to J.R.R. through the Spitzer Space Telescope
Fellowship Program, through a contract issued by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. B.V. and B.M.P. acknowledge financial support from ASI contract
I/016/07/0 and ASI-INAF I/009/10/0. 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. We have
made extensive use of Ned Wright's Online Cosmological Calculator
(Wright 2006).
NR 59
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2013
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IS 1
AR 61
DI 10.1088/0004-637X/770/1/61
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400061
ER
PT J
AU Rea, N
Israel, GL
Pons, JA
Turolla, R
Vigano, D
Zane, S
Esposito, P
Perna, R
Papitto, A
Terreran, G
Tiengo, A
Salvetti, D
Girart, JM
Palau, A
Possenti, A
Burgay, M
Gogus, E
Caliandro, GA
Kouveliotou, C
Gotz, D
Mignani, RP
Ratti, E
Stella, L
AF Rea, N.
Israel, G. L.
Pons, J. A.
Turolla, R.
Vigano, D.
Zane, S.
Esposito, P.
Perna, R.
Papitto, A.
Terreran, G.
Tiengo, A.
Salvetti, D.
Girart, J. M.
Palau, Aina
Possenti, A.
Burgay, M.
Gogus, E.
Caliandro, G. A.
Kouveliotou, C.
Goetz, D.
Mignani, R. P.
Ratti, E.
Stella, L.
TI THE OUTBURST DECAY OF THE LOW MAGNETIC FIELD MAGNETAR SGR 0418+5729
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: individual (SGR 0418+5729); stars: magnetic field; stars: neutron
ID RESONANT CYCLOTRON SCATTERING; PHOTON IMAGING CAMERA; SOFT
GAMMA-REPEATERS; LARGE-AREA TELESCOPE; X-RAY-EMISSION; NEUTRON-STARS;
SWIFT J1822.3-1606; FALLBACK DISKS; XMM-NEWTON; SPIN-DOWN
AB We report on the long-term X-ray monitoring of the outburst decay of the low magnetic field magnetar SGR 0418+5729 using all the available X-ray data obtained with RXTE, Swift, Chandra, and XMM-Newton observations from the discovery of the source in 2009 June up to 2012 August. The timing analysis allowed us to obtain the first measurement of the period derivative of SGR 0418+5729: (P) over dot = 4(1) x 10(-15) s s(-1), significant at a similar to 3.5 sigma confidence level. This leads to a surface dipolar magnetic field of B-dip similar or equal to 6 x 10(12) G. This measurement confirms SGR 0418+5729 as the lowest magnetic field magnetar. Following the flux and spectral evolution from the beginning of the outburst up to similar to 1200 days, we observe a gradual cooling of the tiny hot spot responsible for the X-ray emission, from a temperature of similar to 0.9 to 0.3 keV. Simultaneously, the X-ray flux decreased by about three orders of magnitude: from about 1.4 x 10(-11) to 1.2 x 10(-14) erg s(-1) cm(-2). Deep radio, millimeter, optical, and gamma-ray observations did not detect the source counterpart, implying stringent limits on its multi-band emission, as well as constraints on the presence of a fossil disk. By modeling the magneto-thermal secular evolution of SGR 0418+5729, we infer a realistic age of similar to 550 kyr, and a dipolar magnetic field at birth of similar to 10(14) G. The outburst characteristics suggest the presence of a thin twisted bundle with a small heated spot at its base. The bundle untwisted in the first few months following the outburst, while the hot spot decreases in temperature and size. We estimate the outburst rate of low magnetic field magnetars to be about one per year per galaxy, and we briefly discuss the consequences of such a result in several other astrophysical contexts.
C1 [Rea, N.; Papitto, A.; Terreran, G.; Girart, J. M.; Palau, Aina; Caliandro, G. A.] Inst Space Sci CSIC IEEC, Fac Sci, E-08193 Barcelona, Spain.
[Israel, G. L.; Stella, L.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Pons, J. A.; Vigano, D.] Univ Alicante, Dept Fis Aplicada, E-03080 Alicante, Spain.
[Turolla, R.; Terreran, G.] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy.
[Turolla, R.; Zane, S.; Mignani, R. P.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Esposito, P.; Tiengo, A.; Salvetti, D.; Mignani, R. P.] INAF Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy.
[Perna, R.] Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA.
[Perna, R.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Tiengo, A.] IUSS Ist Univ Studi Super, I-27100 Pavia, Italy.
[Tiengo, A.; Salvetti, D.] INFN Ist Nazl Fis Nucl, Sez Pavia, I-27100 Pavia, Italy.
[Salvetti, D.] Univ Pavia, Dipartimento Fis Nucl & Teor, I-27100 Pavia, Italy.
[Possenti, A.; Burgay, M.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy.
[Gogus, E.] Sabanci Univ, TR-34956 Istanbul, Turkey.
[Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Goetz, D.] Univ Paris Diderot, DSM CNRS, UMR CEA 7158, AIM,Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Mignani, R. P.] Univ Zielona Gora, Kepler Inst Astron, PL-65265 Zielona Gora, Poland.
[Ratti, E.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
RP Rea, N (reprint author), Inst Space Sci CSIC IEEC, Fac Sci, Campus UAB,Torre C5-Parell, E-08193 Barcelona, Spain.
RI PONS, JOSE/D-4687-2012; Girart, Josep/O-1638-2014; Rea,
Nanda/I-2853-2015;
OI PONS, JOSE/0000-0003-1018-8126; Girart, Josep/0000-0002-3829-5591; Rea,
Nanda/0000-0003-2177-6388; Israel, GianLuca/0000-0001-5480-6438; Burgay,
Marta/0000-0002-8265-4344; Tiengo, Andrea/0000-0002-6038-1090; Esposito,
Paolo/0000-0003-4849-5092
FU Ramon y Cajal Research Fellowship; INAF PRIN grant; JAE-Doc CSIC
fellowship; European Social Fund under the program "Junta para la
Ampliacion de Estudios"; Spanish MICINN [AYA2011-30228-C03-02]; FEDER
funds; AGAUR grant (Catalonia) [2009SGR1172]; [AYA2009-07391];
[AYA2012-39303]; [SGR2009-811]; [TW2010005]; [iLINK 2011-0303]; [AYA
2010-21097-C03-02]; [Prometeo/2009/103]
FX We are indebted to the Chandra, Swift, XMM-Newton, GBT, WHT, and PdBI
support teams, with a special thank to Michael Bremer, for the
extraordinary job in planning the PdB observations presented in this
paper. We thank S. Mereghetti and H. Tong for their valuable comments on
the manuscript. N.R. is supported by a Ramon y Cajal Research
Fellowship, and by grants AYA2009-07391, AYA2012-39303, SGR2009-811,
TW2010005, and iLINK 2011-0303. J.A.P. and D.V. acknowledge support from
the grants AYA 2010-21097-C03-02 and Prometeo/2009/103. R.T. and S.M.
are partially funded through an INAF 2011 PRIN grant. A.P. is supported
by a JAE-Doc CSIC fellowship co-funded with the European Social Fund
under the program "Junta para la Ampliacion de Estudios," by the Spanish
MICINN grant AYA2011-30228-C03-02 (co-funded with FEDER funds), and by
the AGAUR grant 2009SGR1172 (Catalonia).
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SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2013
VL 770
IS 1
AR 65
DI 10.1088/0004-637X/770/1/65
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400065
ER
PT J
AU Richey, CR
Kinzer, RE
Cataldo, G
Wollack, EJ
Nuth, JA
Benford, DJ
Silverberg, RF
Rinehart, SA
AF Richey, C. R.
Kinzer, R. E.
Cataldo, G.
Wollack, E. J.
Nuth, J. A.
Benford, D. J.
Silverberg, R. F.
Rinehart, S. A.
TI OPTICAL PROPERTIES OF IRON SILICATES IN THE INFRARED TO MILLIMETER AS A
FUNCTION OF WAVELENGTH AND TEMPERATURE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: ISM; methods: laboratory; submillimeter:
ISM; techniques: spectroscopic
ID METASTABLE EUTECTIC CONDENSATION; COSMIC DUST ANALOGS; GRAINS;
ABSORPTION; DEPENDENCE; SPECTRA; REGION; SMOKES
AB The Optical Properties of Astronomical Silicates with Infrared Techniques program utilizes multiple instruments to provide spectral data over a wide range of temperatures and wavelengths. Experimental methods include Vector Network Analyzer and Fourier transform spectroscopy transmission, and reflection/scattering measurements. From this data, we can determine the optical parameters for the index of refraction, n, and the absorption coefficient, k. The analysis of the laboratory transmittance data for each sample type is based upon different mathematical models, which are applied to each data set according to their degree of coherence. Presented here are results from iron silicate dust grain analogs, in several sample preparations and at temperatures ranging from 5 to 300 K, across the infrared and millimeter portion of the spectrum (from 2.5 to 10,000 mu m or 4000 to 1 cm(-1)).
C1 [Richey, C. R.; Kinzer, R. E.; Cataldo, G.; Wollack, E. J.; Nuth, J. A.; Benford, D. J.; Silverberg, R. F.; Rinehart, S. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Richey, CR (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 665, Greenbelt, MD 20771 USA.
EM christina.r.richey@nasa.gov
RI Wollack, Edward/D-4467-2012; Benford, Dominic/D-4760-2012
OI Wollack, Edward/0000-0002-7567-4451; Benford,
Dominic/0000-0002-9884-4206
FU NASA Science Mission Directorate through the ROSES/APRA program; NASA
through the NASA Herschel Science Center Laboratory Astrophysics
Program; NASA Postdoctoral Program at GSFC; NASA; USRP program
FX The material presented in this paper is based upon work supported by
NASA Science Mission Directorate through the ROSES/APRA program.
Additional support for this work was provided by NASA through the NASA
Herschel Science Center Laboratory Astrophysics Program. Work by C.
Richey and R. Kinzer was supported by appointments to the NASA
Postdoctoral Program at GSFC, administered by the Oak Ridge Associated
Universities under contract with NASA. Contributions to this project
were also made by several students funded through the USRP program:
Nathan Lourie, Caleb Wheeler, Jordan Wheeler, Nicole Mihalko, Tyler
Chisholm, Bethany Niedzielski, John Cognetti, Alex Tinguely, and Meghan
Burleigh. Laboratory support provided by Manuel Quijada and the use of
the Fourier transform spectrometers in the Optics Branch (Code 551) at
GSFC is gratefully acknowledged.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2013
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DI 10.1088/0004-637X/770/1/46
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SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400046
ER
PT J
AU Rothschild, R
Markowitz, A
Hemphill, P
Caballero, I
Pottschmidt, K
Kuhnel, M
Wilms, J
Furst, F
Doroshenko, V
Camero-Arranz, A
AF Rothschild, Richard
Markowitz, Alex
Hemphill, Paul
Caballero, Isabel
Pottschmidt, Katja
Kuehnel, Matthias
Wilms, Joern
Fuerst, Felix
Doroshenko, Victor
Camero-Arranz, Ascension
TI OBSERVATIONS OF THE HIGH-MASS X-RAY BINARY A 0535+26 IN QUIESCENCE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: general; stars: individual (A 0535+26); stars: neutron; X-rays:
stars
ID TRANSIENT; ACCRETION; STARS; A0535+26; PULSARS; WINDS
AB We have analyzed three observations of the high-mass X-ray binary A 0535+26 performed by the Rossi X-Ray Timing Explorer (RXTE) three, five, and six months after the last outburst in 2011 February. We detect pulsations only in the second observation. The 3-20 keV spectra can be fit equally well with either an absorbed power law or absorbed thermal bremsstrahlung model. Reanalysis of two earlier RXTE observations made 4 yr after the 1994 outburst, original BeppoSAX observations 2 yr later, reanalysis of four EXOSAT observations made 2 yr after the last 1984 outburst, and a recent XMM-Newton observation in 2012 reveal a stacked, quiescent flux level decreasing from similar to 2 to <1 x 10(-11) erg cm(-2) s(-1) over 6.5 yr after outburst. The detection of pulsations during half of the quiescent observations would imply that accretion onto the magnetic poles of the neutron star continues despite the fact that the circumstellar disk may no longer be present. The accretion could come from material built up at the corotation radius or from an isotropic stellar wind.
C1 [Rothschild, Richard; Markowitz, Alex; Hemphill, Paul] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Markowitz, Alex; Kuehnel, Matthias; Wilms, Joern] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
[Markowitz, Alex; Wilms, Joern; Fuerst, Felix] ECAP, D-96049 Bamberg, Germany.
[Caballero, Isabel] Univ P Diderot, CEA, UMR AIM CNRS 7158, CEA Saclay,DSM,IRFU,SAp, F-91191 Gif Sur Yvette, France.
[Pottschmidt, Katja] UMBC, CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, Katja] NASA GSFC, Code 661, Greenbelt, MD 20771 USA.
[Fuerst, Felix] CALTECH, Space Radiat Lab, MC Cahill 290 17, Pasadena, CA 91125 USA.
[Doroshenko, Victor] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Camero-Arranz, Ascension] IEEC CSIC, Inst Ciencies Espai, Fac Ciencies, E-08193 Barcelona, Spain.
RP Rothschild, R (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA.
EM rrothschild@ucsd.edu
RI Wilms, Joern/C-8116-2013;
OI Wilms, Joern/0000-0003-2065-5410; Doroshenko,
Victor/0000-0001-8162-1105; Hemphill, Paul/0000-0002-1676-6954
FU Bundesministerium fur Wirtschaft und Technologie through DLR [50 OR
1113]; [AYA2012-39303]; [SGR2009- 811]; [iLINK2011-0303]
FX We acknowledge the assistance and mentoring of Eric Michelsen concerning
Lomb-Scargle analysis and its interpretation, along with use of his
program. Thanks go out to Ron Remillard for supplying the weekly A
0535+26 ASM data for the duration of the RXTE mission. These results
were provided by the ASM/RXTE teams at MIT and at the RXTE SOF and GOF
at NASA's GSFC. We thank Evan Smith for his excellent efforts in
scheduling the RXTE observations. We thank ISSI for hosting and
financing international group meetings on modeling and observations of
cyclotron lines in high-mass X-ray binaries. We acknowledge the GSFC
HEASARC for providing extracted spectra and response files for the
EXOSAT observations that allowed for the reanalysis of the A0535+26
observations. This work was supported by the Bundesministerium fur
Wirtschaft und Technologie through DLR grant 50 OR 1113. We thank J. E.
Davis for the slxfig module which was used to create some of the plots
through out this paper. A.C.A. acknowledges the support from grants
AYA2012-39303, SGR2009- 811, and iLINK2011-0303.
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SC Astronomy & Astrophysics
GA 158QD
UT WOS:000319986400019
ER
PT J
AU Russell, CT
Mewaldt, RA
Luhmann, JG
Mason, GM
von Rosenvinge, TT
Cohen, CMS
Leske, RA
Gomez-Herrero, R
Klassen, A
Galvin, AB
Simunac, KDC
AF Russell, C. T.
Mewaldt, R. A.
Luhmann, J. G.
Mason, G. M.
von Rosenvinge, T. T.
Cohen, C. M. S.
Leske, R. A.
Gomez-Herrero, R.
Klassen, A.
Galvin, A. B.
Simunac, K. D. C.
TI THE VERY UNUSUAL INTERPLANETARY CORONAL MASS EJECTION OF 2012 JULY 23: A
BLAST WAVE MEDIATED BY SOLAR ENERGETIC PARTICLES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; solar-terrestrial relations; solar wind; Sun:
coronal mass ejections (CMEs); Sun: flares
ID MAGNETOSHEATH
AB The giant, superfast, interplanetary coronal mass ejection, detected by STEREO A on 2012 July 23, well away from Earth, appears to have reached 1 AU with an unusual set of leading bow waves resembling in some ways a subsonic interaction, possibly due to the high pressures present in the very energetic particles produced in this event. Eventually, a front of record high-speed flow reached STEREO. The unusual behavior of this event is illustrated using the magnetic field, plasma, and energetic ion observations obtained by STEREO. Had the Earth been at the location of STEREO, the large southward-oriented magnetic field component in the event, combined with its high speed, would have produced a record storm.
C1 [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Mewaldt, R. A.; Cohen, C. M. S.; Leske, R. A.] CALTECH, Pasadena, CA 91125 USA.
[Luhmann, J. G.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Mason, G. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gomez-Herrero, R.] Univ Alcala de Henares, E-28871 Alcala De Henares, Spain.
[Klassen, A.] Univ Kiel, D-24118 Kiel, Germany.
[Galvin, A. B.; Simunac, K. D. C.] Univ New Hampshire, Durham, NH 03824 USA.
RP Russell, CT (reprint author), Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
EM ctrussell@igpp.ucla.edu
RI Gomez-Herrero, Raul/B-7346-2011
OI Gomez-Herrero, Raul/0000-0002-5705-9236
FU National Aeronautics and Space Administration under NASA Grant
[NAS5-00133]
FX This work was supported by the National Aeronautics and Space
Administration under NASA Grant NAS5-00133, administered by the
University of California, Berkeley.
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UT WOS:000319986400038
ER
PT J
AU Valencic, LA
Smith, RK
AF Valencic, Lynne A.
Smith, Randall K.
TI INTERSTELLAR ABUNDANCES TOWARD X Per, REVISITED
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: abundances
ID ABSORPTION-LINE OBSERVATIONS; RAY SPECTROSCOPY; CHEMICAL-COMPOSITION;
GALACTIC DISK; TEMPERATURE-FLUCTUATIONS; PLANETARY-NEBULAE;
FINE-STRUCTURE; STELLAR WINDS; NEUTRON-STAR; CRAB-NEBULA
AB The nearby X-ray binary X Per (HD 24534) provides a useful beacon with which to examine dust grain types and measure elemental abundances in the local interstellar medium (ISM). The absorption features of O, Fe, Mg, and Si along this line of sight were measured using spectra from the Chandra X-Ray Observatory's LETG/ACIS-S and XMM-Newton's RGS instruments, and the Spex software package. The spectra were fit with dust analogs measured in the laboratory. The O, Mg, and Si abundances were compared to those from standard references, and the O abundance was compared to that along lines of sight toward other X-ray binaries. The results are as follows. First, it was found that a combination of MgSiO3 (enstatite) and Mg1.6Fe0.4SiO4 (olivine) provided the best fit to the O K edge, with N(MgSiO3)/N(Mg1.6Fe0.4SiO4) = 3.4. Second, the Fe L edge could be fit with models that included metallic iron, but it was not well described by the laboratory spectra currently available. Third, the total abundances of O, Mg, and Si were in very good agreement with that of recently re-analyzed B stars, suggesting that they are good indicators of abundances in the local ISM, and the depletions were also in agreement with expected values for the diffuse ISM. Finally, the O abundances found from X-ray binary absorption spectra show a similar correlation with Galactocentric distances as seen in other objects.
C1 [Valencic, Lynne A.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Valencic, Lynne A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smith, Randall K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Valencic, LA (reprint author), Johns Hopkins Univ, Baltimore, MD 21218 USA.
FU Chandra Award [GO1-12052A]
FX The authors are grateful to an anonymous referee, whose thoughtful
comments improved this work. This work was supported by Chandra Award
No. GO1-12052A.
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SC Astronomy & Astrophysics
GA 158QD
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EF