FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Romano, P
Sidoli, L
Cusumano, G
Evans, PA
Ducci, L
Krimm, HA
Vercellone, S
Page, KL
Beardmore, AP
Burrows, DN
Kennea, JA
Gehrels, N
La Parola, V
Mangano, V
AF Romano, P.
Sidoli, L.
Cusumano, G.
Evans, P. A.
Ducci, L.
Krimm, H. A.
Vercellone, S.
Page, K. L.
Beardmore, A. P.
Burrows, D. N.
Kennea, J. A.
Gehrels, N.
La Parola, V.
Mangano, V.
TI Multiple flaring activity in the supergiant fast X-ray transient IGR
J08408-4503 observed with Swift
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE X-rays: individual: IGR J08408-4503
ID CLUMPY STELLAR WINDS; NEUTRON-STAR; OUTBURST
AB IGR J08408-4503 is a supergiant fast X-ray transient discovered in 2006 with a confirmed association with a O8.5Ib(f) supergiant star, HD 74194. We report on the analysis of two outbursts caught by Swift/Burst Alert Telescope (BAT) on 2006 October 4 and 2008 July 5, and followed up at softer energies with Swift/X-ray Telescope (XRT). The 2008 XRT light curve shows a multiple-peaked structure with an initial bright flare that reached a flux of similar to 10(-9) erg cm(-2) s(-1) (2-10 keV), followed by two equally bright flares within 75 ks. The spectral characteristics of the flares differ dramatically, with most of the difference, as derived via time-resolved spectroscopy, being due to absorbing column variations. We observe a gradual decrease in the N(H), derived with a fit using absorbed power-law model, as time passes. We interpret these NH variations as due to an ionization effect produced by the first flare, resulting in a significant decrease in the measured column density towards the source. The durations of the flares as well as the times of the outbursts suggest that the orbital period is similar to 35 d, if the flaring activity is interpreted within the framework of the Sidoli et al. model with the outbursts triggered by the neutron star passage inside an equatorial wind inclined with respect to the orbital plane.
C1 [Romano, P.; Cusumano, G.; La Parola, V.; Mangano, V.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy.
[Sidoli, L.; Ducci, L.; Vercellone, S.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy.
[Evans, P. A.; Page, K. L.; Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Ducci, L.] Univ Insubria, Dipartimento Matemat & Fis, I-22100 Como, Italy.
[Krimm, H. A.] Univ Space Res Assoc, Columbia, MD USA.
[Krimm, H. A.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Burrows, D. N.; Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Romano, P (reprint author), Ist Astrofis Spaziale & Fis Cosm, INAF, Via U La Malfa 153, I-90146 Palermo, Italy.
EM romano@ifc.inaf.it
RI Gehrels, Neil/D-2971-2012;
OI Cusumano, Giancarlo/0000-0002-8151-1990; Sidoli,
Lara/0000-0001-9705-2883; Vercellone, Stefano/0000-0003-1163-1396; La
Parola, Valentina/0000-0002-8087-6488
FU Italy [ASI/INAFI/088/06/0, I/023/05/0]; Swift project; NASA [NAS5-00136]
FX We thank the Swift team for making these observations possible, the duty
scientists and science planners. We also thank the anonymous referee for
comments that helped improve the paper. This work was supported in Italy
by contracts ASI/INAFI/088/06/0 and I/023/05/0. APB, PAE and KLP
acknowledge STFC support. HAK was supported by the Swift project. DNB
and JAK acknowledge support from NASA contract NAS5-00136.
NR 33
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PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 1
PY 2009
VL 392
IS 1
BP 45
EP 51
DI 10.1111/j.1365-2966.2008.14050.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 392KX
UT WOS:000262302700004
ER
PT J
AU De Pasquale, M
Evans, P
Oates, S
Page, M
Zane, S
Schady, P
Breeveld, A
Holland, S
Kuin, P
Still, M
Roming, P
Ward, P
AF De Pasquale, M.
Evans, P.
Oates, S.
Page, M.
Zane, S.
Schady, P.
Breeveld, A.
Holland, S.
Kuin, P.
Still, M.
Roming, P.
Ward, P.
TI Jet breaks at the end of the slow decline phase of Swift GRB light
curves
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gamma-rays: bursts
ID GAMMA-RAY BURSTS; THEORETICAL IMPLICATIONS; AFTERGLOW EMISSION; ENERGY
RESERVOIR; FIREBALL MODEL; TELESCOPE; LONG; CALIBRATION; REDSHIFT
AB The Swift mission has discovered an intriguing feature of gamma-ray burst (GRBs) afterglows, a phase of shallow decline of the flux in the X-ray and optical light curves. This behaviour is typically attributed to energy injection into the burst ejecta. At some point this phase ends, resulting in a break in the light curve, which is commonly interpreted as the cessation of the energy injection. In a few cases, however, while breaks in the X-ray light curve are observed, optical emission continues its slow flux decline. This behaviour suggests a more complex scenario. In this paper, we present a model that invokes a double component outflow, in which narrowly collimated ejecta are responsible for the X-ray emission while a broad outflow is responsible for the optical emission. The narrow component can produce a jet break in the X-ray light curve at relatively early times, while the optical emission does not break due to its lower degree of collimation. In our model both components are subject to energy injection for the whole duration of the follow-up observations. We apply this model to GRBs with chromatic breaks, and we show how it might change the interpretation of the GRBs canonical light curve. We also study our model from a theoretical point of view, investigating the possible configurations of frequencies and the values of GRB physical parameters allowed in our model.
C1 [De Pasquale, M.; Oates, S.; Page, M.; Zane, S.; Schady, P.; Breeveld, A.; Kuin, P.; Still, M.; Ward, P.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Evans, P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Holland, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Roming, P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP De Pasquale, M (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM mdp@mssl.ucl.ac.uk
NR 55
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U1 0
U2 1
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 1
PY 2009
VL 392
IS 1
BP 153
EP 169
DI 10.1111/j.1365-2966.2008.13990.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 392KX
UT WOS:000262302700009
ER
PT J
AU Schurch, MPE
Coe, MJ
Galache, JL
Corbet, RHD
McGowan, KE
McBride, VA
Townsend, LJ
Udalski, A
Haberl, F
AF Schurch, M. P. E.
Coe, M. J.
Galache, J. L.
Corbet, R. H. D.
McGowan, K. E.
McBride, V. A.
Townsend, L. J.
Udalski, A.
Haberl, F.
TI High-mass X-ray binary SXP18.3 undergoes the longest type II outburst
ever seen in the Small Magellanic Cloud
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: emission-line, Be; Magellanic Clouds; X-rays: binaries
ID GRAVITATIONAL LENSING EXPERIMENT; PULSARS; CATALOG; SYSTEM
AB On 2006 August 30, SXP18.3 a high-mass X-ray binary (HMXB) in the Small Magellanic Cloud (SMC) with an 18.3 s pulse period was observed by Rossi X-ray Timing Explorer (RXTE). The source was seen continuously for the following 36 weeks. This is the longest type II outburst ever seen from a HMXB in the SMC. During the outburst, SXP18.3 was located from serendipitous XMM-Newton observations. The identification of the optical counterpart has allowed SXP18.3 to be classified as a Be/X-ray binary. This paper will report on the analysis of the optical and weekly RXTE X-ray data that span the last 10 yr. The extreme length of this outburst has for the first time enabled us to perform an extensive study of the pulse timing of a SMC Be/X-ray binary. We present a possible full orbital solution from the pulse timing data. An orbital period of 17.79 d is proposed from the analysis of the Optical Gravitational Lensing Experiment (OGLE) III light curve placing SXP18.3 on the boundary of known sources in the Corbet diagram.
C1 [Schurch, M. P. E.; Coe, M. J.; McGowan, K. E.; McBride, V. A.; Townsend, L. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Galache, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Corbet, R. H. D.] Univ Maryland Baltimore Cty, Xray Astrophys Lab, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Schurch, MPE (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
EM mpes@astro.soton.ac.uk
OI Haberl, Frank/0000-0002-0107-5237
FU National Aeronautics and Space Administration; National Science
Foundation; Polish MNiSW [N20303032/4275]
FX 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 paper utilizes
public domain data originally obtained by the MACHO Project, whose work
was performed under the joint auspices of the US Department of Energy,
National Nuclear Security Administration by the University of
California, Lawrence Livermore National Laboratory under contract number
W-7405-Eng- 48, the National Science Foundation through the Center for
Particle Astrophysics of the University of California under cooperative
agreement AST-8809616 and the Mount Stromlo and Siding Spring
Observatory, part of the Australian National University. This research
has made use of the SIMBAD data base, operated by CDS, Strasbourg,
France. We acknowledge support from the NASA Swift team in providing ToO
observations in order to locate the source. The OGLE project is
partially supported by the Polish MNiSW grant N20303032/4275.
NR 30
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U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN 1
PY 2009
VL 392
IS 1
BP 361
EP 366
DI 10.1111/j.1365-2966.2008.14048.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 392KX
UT WOS:000262302700027
ER
PT J
AU Xu, KM
AF Xu, Kuan-Man
TI Evaluation of Cloud Physical Properties of ECMWF Analysis and
Re-Analysis (ERA) against CERES Tropical Deep Convective Cloud Object
Observations
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID LARGE-SCALE MODELS; 1998 EL-NINO; STATISTICAL-ANALYSES; DIURNAL CYCLE;
PART I; SATELLITE; SCHEME; VALIDATION; CLIMATE; SURFACE
AB This study presents an approach that converts the vertical profiles of grid-averaged cloud properties from large-scale models to probability density functions (pdfs) of subgrid-cell cloud physical properties measured at satellite footprints. Cloud physical and radiative properties, rather than just cloud and precipitation occurrences, of assimilated cloud systems by the European Centre for Medium-Range Weather Forecasts (ECMWF) operational analysis (EOA) and 40-yr ECMWF Re-Analysis (ERA-40) are validated against those obtained from Earth Observing System satellite cloud object data for the January-August 1998 and March 2000 periods. These properties include the ice water path (IWP), cloud-top height and temperature, cloud optical depth, and solar and infrared radiative fluxes. Each cloud object, a contiguous region with similar cloud physical properties, is temporally and spatially matched with EOA and ERA-40 data. Results indicate that most pdfs of EOA and ERA-40 cloud physical and radiative properties agree with those of satellite observations of the tropical deep convective cloud object type for the January-August 1998 period. There are, however, significant discrepancies in selected ranges of the cloud property pdfs such as the upper range of EOA cloud-top height. A major discrepancy is that the dependence of the pdfs on the cloud object size for both EOA and ERA-40 is not as strong as in the observations. Modifications to the cloud parameterization in ECMWF that occurred in October 1999 eliminate the clouds near the tropopause but shift power of the pdf to lower cloud-top heights and greatly reduce the ranges of IWP and cloud optical depth pdfs. These features persist in ERA-40 due to the use of the same cloud parameterizations. The less sophisticated data assimilation technique and the lack of snow water content information in ERA-40, not the larger horizontal grid spacing, are also responsible for the disagreements with observed pdfs of cloud physical properties, although the detection rates of cloud object occurrence are improved for small-size categories. A possible improvement to the convective parameterization is to introduce a stronger dependence of updraft penetration heights on grid-cell dynamics.
C1 NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 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
FX The CERES data were obtained from the Atmospheric Sciences Data Center
at the NASA Langley Research Center. This research has been supported by
the NASA modeling, analysis, and prediction program and
interdisciplinary study program ( Drs. D. Anderson and H. Maring,
program managers). The author would like to thank Dr. Takmeng Wong, Mr.
Lindsay Parker, and Ms. Shengtao Dong for producing the cloud object
data and the matched ECMWF data. Discussions with Drs. Bruce Wielicki,
Takmeng Wong, and Zachary Eitzen are very helpful. Comments from Drs.
Martin Kuhler and Peter Bechtold of ECMWF and two anonymous reviewers
are greatly appreciated.
NR 60
TC 7
Z9 7
U1 0
U2 5
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 JAN
PY 2009
VL 137
IS 1
BP 207
EP 223
DI 10.1175/2008MWR2633.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 404VU
UT WOS:000263181900012
ER
PT J
AU Vj, L
Kobayashi, NP
Islam, MS
Wu, W
Chaturvedi, P
Fang, NX
Wang, SY
Williams, RS
AF Vj, Logeeswaran
Kobayashi, Nobuhiko P.
Islam, M. Saif
Wu, Wei
Chaturvedi, Pratik
Fang, Nicholas X.
Wang, Shih Yuan
Williams, R. Stanley
TI Ultrasmooth Silver Thin Films Deposited with a Germanium Nucleation
Layer
SO NANO LETTERS
LA English
DT Article
ID AG FILMS; MORPHOLOGY; GROWTH; INTERFACE; DIFFUSION; SURFACES; GOLD; SIO2
AB We demonstrate an effective method for depositing smooth silver (Ag) films on SiO/Si-2(100) substrates using a thin seed layer of evaporated germanium (Ge). The deposited Ag films exhibit smaller root-mean-square surface roughness, narrower peak-to-valley surface topological height distribution, smaller grain-size distribution, and smaller sheet resistance in comparison to those of Ag films directly deposited on SiO2/Si(100) substrates. Optically thin (similar to 10-20 nm) Ag films deposited with similar to 1-2 nm Ge nucleation layers show more than an order of magnitude improvement in the surface roughness. The presence of the thin layer of Ge changes the growth kinetics (nucleation and evolution) of the electron-beam-evaporated Ag, leading to Ag films with smooth surface morphology and high electrical conductivity. The demonstrated Ag thin films are very promising for large-scale applications as molecular anchors, optical metamaterials, plasmonic devices, and several areas of nanophotonics.
C1 [Vj, Logeeswaran; Islam, M. Saif] Univ Calif Davis, Dept Elect & Comp Engn, Davis, CA 95616 USA.
[Wu, Wei; Wang, Shih Yuan; Williams, R. Stanley] Hewlett Packard Labs, Informat & Quantum Syst Labs, Palo Alto, CA 94304 USA.
[Chaturvedi, Pratik; Fang, Nicholas X.] Univ Illinois, Dept Engn Sci & Mech, Urbana, IL 61801 USA.
[Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Jack Baskin Sch Engn, Santa Cruz, CA 95064 USA.
[Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, NECTAR, Adv Studies Labs, Santa Cruz, CA 95064 USA.
[Kobayashi, Nobuhiko P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Islam, MS (reprint author), Univ Calif Davis, Dept Elect & Comp Engn, Kemper Hall,1 Shields Ave, Davis, CA 95616 USA.
EM sislam@ucdavis.edu
RI Fang, Nicholas/A-5856-2008; Wang, Shih-Yuan/C-3889-2009; Chaturvedi,
Pratik/A-8922-2010; Wu, Wei/D-1908-2011; Williams, R.
Stanley/A-8281-2009; Kobayashi, Nobuhiko/E-3834-2012
OI Fang, Nicholas/0000-0001-5713-629X; Wang, Shih-Yuan/0000-0002-1212-3484;
Williams, R. Stanley/0000-0003-0213-4259;
FU Information and Quantum Systems Laboratories in Hewlett-Packard
Laboratories, Palo Alto CA; NSF [0547679]; UC Davis
FX The authors thank Zhiyong Li, Sagi Mathai, Xuema Li, Doug Ohlberg,
William Tong, and Denny Houng of Information and Quantum Systems
Laboratories in Hewlett-Packard Laboratories, Palo Alto CA, David A.
Horsley, Chan Mei-Lin, and Jack Skinner of UC DavisBerkeley Sensor &
Actuator Center, and A. Alec Talin from Sandia National
Laboratories-Livermore for valuable discussions. The work at UC Davis
was partially supported by NSF Grant #0547679 and a UC Davis research
grant.
NR 34
TC 34
Z9 34
U1 5
U2 44
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1530-6984
EI 1530-6992
J9 NANO LETT
JI Nano Lett.
PD JAN
PY 2009
VL 9
IS 1
BP 178
EP 182
DI 10.1021/nl8027476
PG 5
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied;
Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA 395IZ
UT WOS:000262519100033
ER
PT J
AU Whitelam, S
Rogers, C
Pasqua, A
Paavola, C
Trent, J
Geissler, PL
AF Whitelam, Stephen
Rogers, Carl
Pasqua, Andrea
Paavola, Chad
Trent, Jonathan
Geissler, Phillip L.
TI The Impact of Conformational Fluctuations on Self-Assembly: Cooperative
Aggregation of Archaeal Chaperonin Proteins
SO NANO LETTERS
LA English
DT Article
ID SULFOLOBUS-SHIBATAE; BUILDING-BLOCKS; DYNAMICS
AB Protein complexes called rosettasomes self-assemble in solution to form large-scale filamentous and planar structures. The relative abundance of these aggregates varies abruptly with environmental conditions and sample composition. Our simulations of a model of patchy nanoparticles can reproduce this sharp crossover, but only if particles are allowed to switch between two internal states favoring different geometries of local binding. These results demonstrate how local conformational adaptivity can fundamentally influence the cooperativity of pattern-forming dynamics.
C1 [Pasqua, Andrea; Geissler, Phillip L.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
[Whitelam, Stephen] Univ Warwick, Syst Biol Ctr, Coventry CV4 7AL, W Midlands, England.
[Rogers, Carl] Univ Calif Berkeley, Biophys Grad Grp, Berkeley, CA 94720 USA.
[Paavola, Chad; Trent, Jonathan] NASA, Ames Res Ctr, Bioengn Branch, Moffett Field, CA 94305 USA.
[Geissler, Phillip L.] Lawrence Berkeley Natl Lab, Div Mat Sci, Berkeley, CA 94720 USA.
[Geissler, Phillip L.] Lawrence Berkeley Natl Lab, Div Phys Biosci, Berkeley, CA 94720 USA.
[Geissler, Phillip L.] Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA.
RP Geissler, PL (reprint author), Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
EM geissler@berkeley.edu
FU U.S. Department of Energy [DE-AC02-05CH11231]; BioSim European Union
Network of Excellence [LSHB-CT-2004-005137]; NIH Molecular Biophysics
Training [T32GM08295]; Science Research Investment Fund
FX This work was supported by the Director, Office of Science, Office of
Basic Energy Sciences, Materials Sciences and Engineering Division, of
the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. S.W.
was supported by the BioSim European Union Network of Excellence
(LSHB-CT-2004-005137). C.R. was supported by a NIH Molecular Biophysics
Training Grant (T32GM08295). Computing facilities were provided in part
by the Centre for Scientific Computing at the University of Warwick with
support from the Science Research Investment Fund. We used
VMD22 to render simulation configurations.
NR 22
TC 15
Z9 15
U1 0
U2 12
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1530-6984
J9 NANO LETT
JI Nano Lett.
PD JAN
PY 2009
VL 9
IS 1
BP 292
EP 297
DI 10.1021/nl8029306
PG 6
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied;
Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA 395IZ
UT WOS:000262519100055
PM 19072304
ER
PT S
AU Andrews, RJ
AF Andrews, Russell J.
BE Sharma, HS
TI Neuromodulation: deep brain stimulation, sensory neuroprostheses, and
the neural-electrical interface
SO NANONEUROSCIENCE AND NANONEUROPHARMACOLOGY
SE Progress in Brain Research
LA English
DT Review; Book Chapter
DE brainstem implants; carbon nanotubes; cochlear implants; computational
analysis; deep brain stimulation; nanoelectrode arrays;
neural-electrical interface; neuromodulation; retinal implants; sensory
neuroprostheses
ID SUBTHALAMIC NUCLEUS; PARKINSONS-DISEASE; RELEASE; SYSTEM; PERFORMANCE;
PROSTHESIS; ASTROCYTES; IMPLANT; NEURONS; HEARING
AB Although neuromodulation with implanted brain electrodes (deep brain stimulation, DBS) has been increasingly effective in treating many patients with movement disorders (e.g., advanced Parkinson's disease) over the past 20 years, the techniques have changed little for more than 50 years. After summarizing the current state of DBS, this chapter considers (1) the advances being offered by computational analysis techniques as well as (2) the benefits of monitoring and modulating brain chemical activity in addition to brain electrical activity. A review of the current state of sensory neuroprostheses follows, with consideration of emerging data on the optimal configuration of micron-sized retinal prostheses as well as on the optimal site for stimulation of cells in the retina. Very recent findings on nanotechniques to enhance charge transfer from prosthesis to cell (neuronal or glial), that is, enhancement of the neural-electrical interface, are then reviewed. The final section summarizes areas of potential cross-fertilization between those centers developing sensory neuroprostheses and those centers developing nanotechniques for DBS.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Andrews, RJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM rja@russelljandrews.org
NR 28
TC 2
Z9 2
U1 2
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0079-6123
BN 978-0-444-53431-6
J9 PROG BRAIN RES
JI Prog. Brain Res.
PY 2009
VL 180
BP 127
EP 139
DI 10.1016/S0079-6123(08)80007-6
PG 13
WC Nanoscience & Nanotechnology; Neurosciences
SC Science & Technology - Other Topics; Neurosciences & Neurology
GA BQC14
UT WOS:000280620600008
PM 20302832
ER
PT S
AU Son, KA
Yang, BH
Prokopuk, N
Moon, JS
Liao, A
Gallegos, M
Yang, JW
Katona, T
Khan, MA
AF Son, K. -A.
Yang, B. H.
Prokopuk, N.
Moon, J. S.
Liao, A.
Gallegos, M.
Yang, J. W.
Katona, T.
Khan, M. A.
BE Nagarajan, R
Zukas, W
Hatton, TA
Lee, S
TI Novel GaN-based Chemical Sensors for Long-range Chemical Threat
Detection
SO NANOSCIENCE AND NANOTECHNOLOGY FOR CHEMICAL AND BIOLOGICAL DEFENSE
SE ACS Symposium Series
LA English
DT Proceedings Paper
CT 234th American-Chemical-Society National Meeting
CY AUG 17-19, 2007
CL Boston, MA
SP Amer Chem Soc, Div Colloid & Surface Chem
ID ELECTRON-MOBILITY-TRANSISTORS; FIELD-EFFECT TRANSISTORS; PIEZOELECTRIC
POLARIZATION; ALGAN/GAN HETEROSTRUCTURES; SF6
AB We are developing micro chemical sensor nodes consisting of GaN HEMT (High Electron Mobility Transistor) sensors and a RF communication link for long range chemical threat detection and early warning. In this paper, we discuss our research on (1) high selectivity detection of chemical agents (stimulants) using the GaN HEMT sensors, (2) the effects of the materials and design of the gate electrode on the sensitivity of the sensor, and (3) optimal operating parameters for high sensitivity detection.
C1 [Son, K. -A.; Yang, B. H.; Liao, A.; Gallegos, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Son, KA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 18
TC 0
Z9 0
U1 1
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 SIXTEENTH ST NW, WASHINGTON, DC 20036 USA
SN 0097-6156
BN 978-0-8412-6981-1
J9 ACS SYM SER
JI ACS Symp. Ser.
PY 2009
VL 1016
BP 155
EP 168
PG 14
WC Biochemistry & Molecular Biology; Chemistry, Multidisciplinary;
Nanoscience & Nanotechnology
SC Biochemistry & Molecular Biology; Chemistry; Science & Technology -
Other Topics
GA BVW58
UT WOS:000292990100012
ER
PT B
AU Vasquez, A
Ewert, M
Rowlands, J
Post, K
AF Vasquez, A.
Ewert, M.
Rowlands, J.
Post, K.
BE Laudon, M
Romanowicz, B
TI Johnson Space Center's Solar and Wind-based Renewable Energy System
SO NANOTECH CONFERENCE & EXPO 2009, VOL 3, TECHNICAL PROCEEDINGS
LA English
DT Proceedings Paper
CT Nanotech 2009 Conference
CY MAY 03-07, 2009
CL Houston, TX
SP Acctron AG, Adv Energy Consortium, Alliance NanoHealth, Appl Mat, Bayer MaterialScience, Buchanan Ingersoll & Rooney PC, Buhler PARTEC GmbH, Ctr Appl Nanotechnol GmbH, Ctr Biol & Environm Nanotechnol, Clean Technol & Sustainable Ind Org, CMP, CTC Nanotechnol GmbH, DREEBIT GmbH, ETH Zurich, ETH Transfer, ETH Zurich, MNSP, Folcy & Lardner LLP, FDA, Goodwin Procter LLC, HiNanoAnalytics, Houston Technol Ctr, Inno X GmbH, Innovat Alliance Carbon Nanotubes, Italian Tradde Commiss, Jackson Walket LLP, JENOPTIK, Lockheed Martin, Nano Sci & Technol Inst, nano tech 2009 Japan, NanoEurope Fair & Conf, Nanograde Llc, NanoInk, NANOSENSORS, NanoSPRINT, NanoWorld AG, NCI, NIH, Opportun Houston, OSEC, Pearland Econ Dev Corp, Res Germany Land Ideas, Richard Smalley Inst Nanoscale Sci & Technol, Taylor & Francis Grp LLC, CRC Press, TechConnect, Texas Nanotechnol Initiat, IEEE Stand Assoc, Russian Corp Nanotechnologies, TurboBeads Llc, Weidmann Plast Technol AG
DE renewable-energy; solar; photovoltaic; wind-turbine; space-exploration
power
AB The NASA Johnson Space Center (JSC) in Houston, Texas has a Sustainability Partnership team that seeks ways for earth-based sustainability practices to also benefit space exploration research. A renewable energy gathering system was installed in 2007 at the JSC Child Care Center (CCC) which also offers a potential test bed for space exploration power generation and remote monitoring and control concepts. The system comprises: 1) several different types of photovoltaic panels (29 M), 2) two wind-turbines (3.6 kW total), and 3) one roof-mounted solar thermal water heater and tank. A tie to the JSC local electrical grid was provided to accommodate excess power. The total first year electrical energy production was 53 megawatt-hours. A web-based real-time metering system collects and reports system performance and weather data. Improvements in areas of the CCC that were detected during subsequent energy analyses and some concepts for future efforts are also presented.
C1 [Vasquez, A.; Ewert, M.; Rowlands, J.; Post, K.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Vasquez, A (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM Arturo.Vasquez-1@nasa.gov; Michael.K.Ewert@nasa.gov;
Jerald.T.Rowlands@nasa.gov; Kevin.E.Post@nasa.gov
NR 1
TC 0
Z9 0
U1 0
U2 0
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-1-4398-1784-1
PY 2009
BP 137
EP 140
PG 4
WC Energy & Fuels; Nanoscience & Nanotechnology
SC Energy & Fuels; Science & Technology - Other Topics
GA BMQ04
UT WOS:000273331000033
ER
PT B
AU Wilson, WC
Atkinson, GM
AF Wilson, W. C.
Atkinson, G. M.
BE Laudon, M
Romanowicz, B
TI A Comparison of Surface Acoustic Wave Modeling Methods
SO NANOTECH CONFERENCE & EXPO 2009, VOL 3, TECHNICAL PROCEEDINGS
LA English
DT Proceedings Paper
CT Nanotech 2009 Conference
CY MAY 03-07, 2009
CL Houston, TX
SP Acctron AG, Adv Energy Consortium, Alliance NanoHealth, Appl Mat, Bayer MaterialScience, Buchanan Ingersoll & Rooney PC, Buhler PARTEC GmbH, Ctr Appl Nanotechnol GmbH, Ctr Biol & Environm Nanotechnol, Clean Technol & Sustainable Ind Org, CMP, CTC Nanotechnol GmbH, DREEBIT GmbH, ETH Zurich, ETH Transfer, ETH Zurich, MNSP, Folcy & Lardner LLP, FDA, Goodwin Procter LLC, HiNanoAnalytics, Houston Technol Ctr, Inno X GmbH, Innovat Alliance Carbon Nanotubes, Italian Tradde Commiss, Jackson Walket LLP, JENOPTIK, Lockheed Martin, Nano Sci & Technol Inst, nano tech 2009 Japan, NanoEurope Fair & Conf, Nanograde Llc, NanoInk, NANOSENSORS, NanoSPRINT, NanoWorld AG, NCI, NIH, Opportun Houston, OSEC, Pearland Econ Dev Corp, Res Germany Land Ideas, Richard Smalley Inst Nanoscale Sci & Technol, Taylor & Francis Grp LLC, CRC Press, TechConnect, Texas Nanotechnol Initiat, IEEE Stand Assoc, Russian Corp Nanotechnologies, TurboBeads Llc, Weidmann Plast Technol AG
DE Surface Acoustic Wave; SAW; transmission line models; Impulse Response
Method
AB Surface Acoustic Wave (SAW) technology is low cost, rugged, lightweight, extremely low power and call be used to develop passive wireless sensors. For these reasons, NASA is investigating the use of SAW technology for Integrated Vehicle Health Monitoring (IVHM) of aerospace structures. To facilitate rapid prototyping of passive SAW sensors for aerospace applications,, SAW models have been developed.
This paper reports oil the comparison of three methods of modeling SAWs. The three models are the Impulse Response Method a first order model, and two second order matrix methods; the conventional matrix approach, and a modified matrix approach that is extended to include internal finger reflections. The second order models are based upon matrices that were originally developed for analyzing microwave circuits using transmission line theory. Results from the models are presented with measured data from devices.
C1 [Wilson, W. C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Wilson, WC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM w.c.wilson@larc.nasa.gov; gmatkins@vcu.edu
NR 4
TC 1
Z9 1
U1 0
U2 0
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-1-4398-1784-1
PY 2009
BP 347
EP 350
PG 4
WC Energy & Fuels; Nanoscience & Nanotechnology
SC Energy & Fuels; Science & Technology - Other Topics
GA BMQ04
UT WOS:000273331000088
ER
PT J
AU Bleier, T
Dunson, C
Maniscalco, M
Bryant, N
Bambery, R
Freund, F
AF Bleier, T.
Dunson, C.
Maniscalco, M.
Bryant, N.
Bambery, R.
Freund, F.
TI Investigation of ULF magnetic pulsations, air conductivity changes, and
infra red signatures associated with the 30 October Alum Rock M5.4
earthquake
SO NATURAL HAZARDS AND EARTH SYSTEM SCIENCES
LA English
DT Article
ID CHI-CHI EARTHQUAKE; ELECTRIC-CURRENTS; CALIFORNIA; SIGNALS
AB Several electromagnetic signal types were observed prior to and immediately after 30 October 2007 (Local Time) M5.4 earthquake at Alum Rock, Ca with an epicenter similar to 15 km NE of San Jose Ca. The area where this event occurred had been monitored since November 2005 by a QuakeFinder magnetometer site, unit 609, 2 km from the epicenter. This instrument is one of 53 stations of the QuakeFinder (QF) California Magnetometer Network-CalMagNet. This station included an ultra low frequency (ULF) 3-axis induction magnetometer, a simple air conductivity sensor to measure relative airborne ion concentrations, and a geophone to identify the arrival of the P-wave from an earthquake. Similar in frequency content to the increased ULF activity reported two weeks prior to the Loma Prieta M7.0 quake in 1989 (Fraser-Smith, 1990, 1991), the QF station detected activity in the 0.01-12 Hz bands, but it consisted of an increasing number of short duration (1 to 30 s duration) pulsations. The pulsations peaked around 13 days prior to the event. The amplitudes of the pulses were strong, (3-20 nT), compared to the average ambient noise at the site, (10-250 pT), which included a component arising from the Bay Area Rapid Transit (BART) operations. The QF station also detected different pulse shapes, e. g. negative or positive only polarity, with some pulses including a combination of positive and negative. Typical pulse counts over the previous year ranged from 0-15 per day, while the count rose to 176 (east-west channel) on 17 October, 13 days prior to the quake. The air conductivity sensor saturated for over 14 h during the night and morning prior to the quake, which occurred at 20: 29 LT. Anomalous IR signatures were also observed in the general area, within 50 km of the epicenter, during the 2 weeks prior to the quake. These three simultaneous EM phenomena were compared with data collected over a 1-2-year period at the site. The data was also compared against accounts of air ionization reported to be associated with radon emission from the ground (Ouzounov, 2007), and a series of laboratory rock stressing experiments (Freund, 2006, 2007a, b, c) to determine if field data was consistent either of these accounts. We could not find a data set with pre-earthquake radon measurements taken near the Alum Rock epicenter to compare against our field data. However, based on the Alum Rock data set example and another data set at Parkfield, the field tests are at least consistent with the lab experiments showing currents, magnetic field disturbances, air conductivity changes, and IR signatures. This is encouraging, but more instrumented earthquake examples are needed to prove a repeating pattern for these types of pre-earthquake EM signatures.
C1 [Bleier, T.; Dunson, C.; Maniscalco, M.] QuakeFinder Inc, Palo Alto, CA 94306 USA.
[Bryant, N.; Bambery, R.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Freund, F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bleier, T (reprint author), QuakeFinder Inc, Palo Alto, CA 94306 USA.
EM tbleier@quakefinder.com
NR 19
TC 28
Z9 28
U1 0
U2 6
PU COPERNICUS PUBLICATIONS
PI KATHLENBURG-LINDAU
PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY
SN 1561-8633
J9 NAT HAZARD EARTH SYS
JI Nat. Hazards Earth Syst. Sci.
PY 2009
VL 9
IS 2
BP 585
EP 603
PG 19
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Water Resources
SC Geology; Meteorology & Atmospheric Sciences; Water Resources
GA 441BD
UT WOS:000265743400026
ER
PT J
AU Kirschbaum, DB
Adler, R
Hong, Y
Lerner-Lam, A
AF Kirschbaum, D. B.
Adler, R.
Hong, Y.
Lerner-Lam, A.
TI Evaluation of a preliminary satellite-based landslide hazard algorithm
using global landslide inventories
SO NATURAL HAZARDS AND EARTH SYSTEM SCIENCES
LA English
DT Article
ID DEBRIS FLOWS; SHALLOW LANDSLIDES; RAINFALL INTENSITY; DURATION CONTROL;
CENTRAL NEPAL; HONG-KONG; SUSCEPTIBILITY; GIS; PRODUCTS; MONSOON
AB Most landslide hazard assessment algorithms in common use are applied to small regions, where high-resolution, in situ, observables are available. A preliminary global landslide hazard algorithm has been developed to estimate areas of potential landslide occurrence in near real-time by combining a calculation of landslide susceptibility with satellite derived rainfall estimates to forecast areas with increased potential for landslide conditions. This paper presents a stochastic methodology to compare this new, landslide hazard algorithm for rainfall-triggered landslides with a newly available inventory of global landslide events, in order to determine the predictive skill and limitations of such a global estimation technique. Additionally, we test the sensitivity of the global algorithm to its input observables, including precipitation, topography, land cover and soil variables. Our analysis indicates that the current algorithm is limited by issues related to both the surface-based susceptibility map and the temporal resolution of rainfall information, but shows skill in determining general geographic and seasonal distributions of landslides. We find that the global susceptibility model has inadequate performance in certain locations, due to improper weighting of surface observables in the susceptibility map. This suggests that the relative contributions of topographic slope and soil conditions to landslide susceptibility must be considered regionally. The current, initial forecast system, although showing some overall skill, must be improved considerably if it is to be used for hazard warning or detailed studies. Surface and remote sensing observations at higher spatial resolution, together with improved landslide event catalogues, are required if global landslide hazard forecasts are to become an operational reality.
C1 [Kirschbaum, D. B.; Lerner-Lam, A.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA.
[Kirschbaum, D. B.; Lerner-Lam, A.] Columbia Univ, Dept Earth & Environm Sci, Palisades, NY USA.
[Kirschbaum, D. B.; Adler, R.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Adler, R.] Univ Maryland, ESSIC, College Pk, MD 20742 USA.
[Hong, Y.] Univ Oklahoma, Sch Civil Engn & Environm Sci, Natl Weather Ctr, Norman, OK 73019 USA.
RP Kirschbaum, DB (reprint author), Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA.
EM dbach@ldeo.columbia.edu
RI Hong, Yang/D-5132-2009; Kirschbaum, Dalia/F-9596-2012; Namikawa,
Laercio/C-5559-2013
OI Hong, Yang/0000-0001-8720-242X; Namikawa, Laercio/0000-0001-7847-1804
FU NASA [NNG05GN31H]; Lamont-Doherty Earth Observatory, Columbia University
FX The authors would like to thank Stephanie Hill and Lynne Shupp for their
help in preparing the landslide inventory database. This research was
supported by a grant from NASA Applied Sciences program, NASA Graduate
Fellowship ( Grant NNG05GN31H) and by the Lamont-Doherty Earth
Observatory, Columbia University.
NR 40
TC 29
Z9 29
U1 2
U2 23
PU COPERNICUS PUBLICATIONS
PI KATHLENBURG-LINDAU
PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY
SN 1561-8633
J9 NAT HAZARD EARTH SYS
JI Nat. Hazards Earth Syst. Sci.
PY 2009
VL 9
IS 3
BP 673
EP 686
PG 14
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Water Resources
SC Geology; Meteorology & Atmospheric Sciences; Water Resources
GA 464XP
UT WOS:000267543300003
ER
PT J
AU Bills, BG
AF Bills, Bruce G.
TI PLANETARY SCIENCE Tidal flows in satellite oceans
SO NATURE GEOSCIENCE
LA English
DT News Item
ID DISSIPATION; EUROPA
AB Sub-surface oceans probably exist on several large satellites of Jupiter and Saturn. An analysis of Europa's tides suggests that some of the Rossby waves are resonantly enhanced by the obliquity, producing sufficient heat and flow to keep the ocean liquid.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bills, BG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bruce.bills@jpl.nasa.gov
NR 11
TC 5
Z9 5
U1 1
U2 5
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 JAN
PY 2009
VL 2
IS 1
BP 13
EP 14
DI 10.1038/ngeo396
PG 3
WC Geosciences, Multidisciplinary
SC Geology
GA 397CB
UT WOS:000262638500010
ER
PT B
AU Hemmati, H
AF Hemmati, Hamid
BE Hemmati, H
TI Near-Earth Laser Communications
SO NEAR-EARTH LASER COMMUNICATIONS
SE Optical Science and Engineering-CRC
LA English
DT Article; Book Chapter
ID OPTICAL COMMUNICATIONS; SPACE COMMUNICATIONS; PERFORMANCE
C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
NR 61
TC 0
Z9 0
U1 0
U2 0
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-0-8247-5381-8
J9 OPT SCI ENG-CRC
PY 2009
BP 1
EP +
D2 10.1201/9781420015447
PG 31
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA BJV02
UT WOS:000267226700001
ER
PT B
AU Pribil, K
Hemmati, H
AF Pribil, Klaus
Hemmati, Hamid
BE Hemmati, H
TI Laser Transmitters: Coherent and Direct Detections
SO NEAR-EARTH LASER COMMUNICATIONS
SE Optical Science and Engineering-CRC
LA English
DT Article; Book Chapter
ID PHOTONIC CRYSTAL FIBERS; AMPLIFIERS; POWER
C1 [Pribil, Klaus] NewComp, Freienstein, Switzerland.
[Hemmati, Hamid] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA.
RP Pribil, K (reprint author), NewComp, Freienstein, Switzerland.
NR 20
TC 0
Z9 0
U1 0
U2 1
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-0-8247-5381-8
J9 OPT SCI ENG-CRC
PY 2009
BP 97
EP +
D2 10.1201/9781420015447
PG 46
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA BJV02
UT WOS:000267226700004
ER
PT B
AU Hemmati, H
AF Hemmati, Hamid
BE Hemmati, H
TI Flight Optomechanical Assembly
SO NEAR-EARTH LASER COMMUNICATIONS
SE Optical Science and Engineering-CRC
LA English
DT Article; Book Chapter
C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
NR 24
TC 0
Z9 0
U1 0
U2 0
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-0-8247-5381-8
J9 OPT SCI ENG-CRC
PY 2009
BP 143
EP 160
D2 10.1201/9781420015447
PG 18
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA BJV02
UT WOS:000267226700005
ER
PT B
AU Moision, B
Hamkins, J
AF Moision, Bruce
Hamkins, Jon
BE Hemmati, H
TI Coding and Modulation for Free-Space Optical Communications
SO NEAR-EARTH LASER COMMUNICATIONS
SE Optical Science and Engineering-CRC
LA English
DT Article; Book Chapter
ID CHANNEL; CODES; CAPACITY
C1 [Moision, Bruce; Hamkins, Jon] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
RP Moision, B (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
NR 29
TC 1
Z9 1
U1 0
U2 0
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-0-8247-5381-8
J9 OPT SCI ENG-CRC
PY 2009
BP 161
EP 187
D2 10.1201/9781420015447
PG 27
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA BJV02
UT WOS:000267226700006
ER
PT B
AU Piazzolla, S
AF Piazzolla, Sabino
BE Hemmati, H
TI Atmospheric Channel
SO NEAR-EARTH LASER COMMUNICATIONS
SE Optical Science and Engineering-CRC
LA English
DT Article; Book Chapter
ID OPTICAL SCINTILLATIONS; TURBULENT ATMOSPHERE; PROBABILITY-DENSITY;
FLUCTUATIONS; PROPAGATION; SYSTEMS; PATH
C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
RP Piazzolla, S (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
NR 34
TC 4
Z9 4
U1 0
U2 0
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-0-8247-5381-8
J9 OPT SCI ENG-CRC
PY 2009
BP 237
EP +
D2 10.1201/9781420015447
PG 37
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA BJV02
UT WOS:000267226700008
ER
PT B
AU Hemmati, H
AF Hemmati, Hamid
BE Hemmati, H
TI Reliability and Flight Qualification
SO NEAR-EARTH LASER COMMUNICATIONS
SE Optical Science and Engineering-CRC
LA English
DT Article; Book Chapter
ID GAMMA-IRRADIATION; LASER-DIODES; DOPED FIBERS; RADIATION; PERFORMANCE;
PHOTONICS; PROGRAM
C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
NR 52
TC 0
Z9 0
U1 0
U2 0
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-0-8247-5381-8
J9 OPT SCI ENG-CRC
PY 2009
BP 321
EP 343
D2 10.1201/9781420015447
PG 23
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA BJV02
UT WOS:000267226700010
ER
PT B
AU Hemmati, H
AF Hemmati, Hamid
BE Hemmati, H
TI Future Directions
SO NEAR-EARTH LASER COMMUNICATIONS
SE Optical Science and Engineering-CRC
LA English
DT Article; Book Chapter
ID OPTICAL COMMUNICATIONS DEMONSTRATOR
C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
NR 17
TC 0
Z9 0
U1 0
U2 0
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-0-8247-5381-8
J9 OPT SCI ENG-CRC
PY 2009
BP 369
EP 374
D2 10.1201/9781420015447
PG 6
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA BJV02
UT WOS:000267226700012
ER
PT B
AU Blackwell, WJ
Chen, FW
AF Blackwell, William J.
Chen, Frederick W.
BA Blackwell, WJ
Chen, FW
BF Blackwell, WJ
Chen, FW
TI Neural Networks in Atmospheric Remote Sensing Introduction
SO NEURAL NETWORKS IN ATMOSPHERIC REMOTE SENSING
SE Artech House Remote Sensing Library
LA English
DT Editorial Material; Book Chapter
ID ENVIRONMENTAL SCIENCES
C1 [Blackwell, William J.] NASA, AIRS NPP Sci Team, Washington, DC USA.
[Chen, Frederick W.] Signal Syst Corp, Severna Pk, MD USA.
[Chen, Frederick W.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Chen, Frederick W.] MIT, Lincoln Lab, Cambridge, MA 02139 USA.
NR 6
TC 19
Z9 19
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-59693-372-9
J9 ARTECH HSE REMOTE SE
PY 2009
BP 1
EP 5
PG 5
WC Remote Sensing
SC Remote Sensing
GA BKE03
UT WOS:000267849700001
ER
PT S
AU Zavlin, VE
AF Zavlin, Vyacheslav E.
BE Becker, W
TI Theory of Radiative Transfer in Neutron Star Atmospheres and Its
Applications
SO NEUTRON STARS AND PULSARS
SE Astrophysics and Space Science Library
LA English
DT Article; Book Chapter
ID MILLISECOND PULSAR J0437-4715; XMM-NEWTON OBSERVATIONS; X-RAY-EMISSION;
SUPERNOVA REMNANT IC-443; STRONG MAGNETIC-FIELDS; MODEL ATMOSPHERES;
ULTRAVIOLET EMISSION; CHANDRA OBSERVATIONS; THERMAL EMISSION; POLAR CAPS
C1 NASA, George C Marshall Space Flight Ctr, Space Sci Lab, Huntsville, AL 35805 USA.
RP Zavlin, VE (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Lab, SD59, Huntsville, AL 35805 USA.
EM vyacheslav.zavlin@msfc.nasa.gov
NR 101
TC 23
Z9 23
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 0067-0057
BN 978-3-540-76964-4
J9 ASTROPHYS SPACE SC L
PY 2009
VL 357
BP 181
EP 211
D2 10.1007/978-3-540-76965-1
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJO24
UT WOS:000266889500009
ER
PT S
AU Harding, AK
AF Harding, Alice K.
BE Becker, W
TI High-energy Emission from the Polar Cap and Slot Gap
SO NEUTRON STARS AND PULSARS
SE Astrophysics and Space Science Library
LA English
DT Article; Book Chapter
ID GAMMA-RAY PULSARS; INVERSE COMPTON-SCATTERING; STRONG MAGNETIC-FIELDS;
RADIATION PAIR FRONTS; MILLISECOND PULSARS; PARTICLE-ACCELERATION;
RADIO-EMISSION; YOUNG PULSARS; CREATION; MAGNETOSPHERES
C1 NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Washington, DC 20546 USA.
RP Harding, AK (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Washington, DC 20546 USA.
EM harding@twinkie.gsfc.nasa.gov
NR 79
TC 9
Z9 9
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 0067-0057
BN 978-3-540-76964-4
J9 ASTROPHYS SPACE SC L
PY 2009
VL 357
BP 521
EP 542
D2 10.1007/978-3-540-76965-1
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJO24
UT WOS:000266889500019
ER
PT S
AU Weisskopf, MC
Elsner, RF
Kaspi, VM
O'Dell, SL
George, GP
Ramsey, BD
AF Weisskopf, Martin C.
Elsner, Ronald F.
Kaspi, Victoria M.
O'Dell, Stephen L.
George, G. Pavlov
Ramsey, Brain D.
BE Becker, W
TI X-Ray Polarimetry and Its Potential Use for Understanding Neutron Stars
SO NEUTRON STARS AND PULSARS
SE Astrophysics and Space Science Library
LA English
DT Article; Book Chapter
ID SOFT GAMMA-REPEATERS; STRONGLY MAGNETIZED PLASMA; RAPIDLY SPINNING
PULSARS; COHERENT TIMING SOLUTION; COMPACT CENTRAL OBJECT; CRAB PULSAR;
OPTICAL POLARIZATION; OUTER MAGNETOSPHERE; ENERGETIC RADIATION;
SCATTERING FACTORS
C1 [Weisskopf, Martin C.; Elsner, Ronald F.; O'Dell, Stephen L.; Ramsey, Brain D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[George, G. Pavlov] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Weisskopf, MC (reprint author), NASA, George C Marshall Space Flight Ctr, VP62, Huntsville, AL 35812 USA.
EM martin@smoker.msfc.nasa.gov; ron.elsner@nasa.gov;
vkaspi@hep.physics.mcgill.ca; Steve.O'Dell@nasa.gov;
pavlov@astro.psu.edu; Brian.Ramsey@nasa.gov
OI O'Dell, Stephen/0000-0002-1868-8056
NR 90
TC 17
Z9 17
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 0067-0057
BN 978-3-540-76964-4
J9 ASTROPHYS SPACE SC L
PY 2009
VL 357
BP 589
EP 619
D2 10.1007/978-3-540-76965-1
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJO24
UT WOS:000266889500022
ER
PT S
AU Smith, DA
Thompson, DJ
AF Smith, David A.
Thompson, David J.
BE Becker, W
TI GeV Gamma-Ray Pulsar Detection
SO NEUTRON STARS AND PULSARS
SE Astrophysics and Space Science Library
LA English
DT Article; Book Chapter
ID ATMOSPHERIC CHERENKOV TELESCOPES; HIGH-ENERGY; IMAGING TELESCOPE;
CRAB-NEBULA; EMISSION; ARRAY; GLAST; DISCOVERY; ASTRONOMY; VERITAS
C1 [Smith, David A.] Univ Bordeaux 1, CENBG UMR 5797, CNRS, IN2P3, F-33175 Gradignan, France.
[Thompson, David J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20721 USA.
RP Smith, DA (reprint author), Univ Bordeaux 1, CENBG UMR 5797, CNRS, IN2P3, 1 Chemin Solarium BP120, F-33175 Gradignan, France.
EM smith@cenbg.in2p3.fr; David.J.Thompson@nasa.gov
NR 69
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 0067-0057
BN 978-3-540-76964-4
J9 ASTROPHYS SPACE SC L
PY 2009
VL 357
BP 621
EP 649
D2 10.1007/978-3-540-76965-1
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJO24
UT WOS:000266889500023
ER
PT J
AU Murphy, PJ
AF Murphy, P. J.
TI Extended Care
SO NEW ENGLAND REVIEW-MIDDLEBURY SERIES
LA English
DT Fiction, Creative Prose
C1 [Murphy, P. J.] Eastfield Coll, Mesquite, TX USA.
[Murphy, P. J.] NASA, Washington, DC USA.
[Murphy, P. J.] Univ Florida, Masters Program Forens Toxicol, Gainesville, FL 32611 USA.
RP Murphy, PJ (reprint author), Univ Florida, Alcohol Testing Program, Gainesville, FL 32611 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU MIDDLEBURY COLL PUBLICATIONS
PI MIDDLEBURY
PA MIDDLEBURY COLLEGE, MIDDLEBURY, VT 05753 USA
SN 1053-1297
J9 NEW ENGL REV-MIDDLEB
JI New Engl. Rev.-Middlebury Ser.
PY 2009
VL 30
IS 1
BP 167
EP 179
PG 13
WC Literary Reviews
SC Literature
GA 435NO
UT WOS:000265350800026
ER
PT S
AU Heap, S
Lindler, DJ
AF Heap, Sally
Lindler, Don J.
BE Dagostino, MC
Bertone, E
Gonzalez, DR
TI Constraining Galaxy Evolution With Hubble's Next Generation Spectral
Library
SO NEW QUESTS IN STELLAR ASTROPHYSICS II: ULTRAVIOLET PROPERTIES OF EVOLVED
STELLAR POPULATIONS
SE Astrophysics and Space Science Proceedings
LA English
DT Proceedings Paper
CT International Conference on Untraviolet Properties of Evolved Stellar
Populations
CY APR 16-20, 2007
CL Puerto Vallarta, MEXICO
SP Inst Nacl Astrofis, Opt & Elect, Univ Guadalajara
ID STARS; MASS
AB We present Hubble's Next Generation Spectral Library, a library of UV-optical spectra (0-2 - 1.0 mu) of 378 stars. We show that the mid-UV spectrum can be used to constrain the ages and metallicities of high-redshift galaxies presently being observed with large, ground-based telescopes.
C1 [Heap, Sally] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Lindler, Don J.] Sigma Space Corp, Lanham, MD USA.
RP Heap, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM Sally.Heap@nasa.gov; Don.J.Lindler@nasa.gov
RI heap, sara/E-2237-2012
NR 8
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 1570-6591
BN 978-0-387-87620-7
J9 ASTROPHYSICS SPACE
PY 2009
BP 273
EP +
DI 10.1007/978-0-387-87621-4_37
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJE77
UT WOS:000265216200037
ER
PT B
AU Boriah, S
Kumar, V
Steinbach, M
Tan, PN
Potter, C
Klooster, S
AF Boriah, Shyam
Kumar, Vipin
Steinbach, Michael
Tan, Pang-Ning
Potter, Christopher
Klooster, Steven
BE Kargupta, H
Han, J
Yu, PS
Motwani, R
Kumar, V
TI Detecting Ecosystem Disturbances and Land Cover Change Using Data Mining
SO NEXT GENERATION OF DATA MINING
SE Chapman & Hall-CRC Data Mining and Knowledge Discovery Series
LA English
DT Article; Book Chapter
ID DEFORESTATION; CLIMATE; SCALE
C1 [Boriah, Shyam; Kumar, Vipin; Steinbach, Michael; Tan, Pang-Ning] Univ Minnesota, Dept Comp Sci & Engn, Minneapolis, MN 55455 USA.
[Potter, Christopher] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Klooster, Steven] Calif State Univ, Monterey Bay Seaside, CA USA.
RP Boriah, S (reprint author), Univ Minnesota, Dept Comp Sci & Engn, Minneapolis, MN 55455 USA.
NR 10
TC 1
Z9 1
U1 0
U2 0
PU CHAPMAN & HALL/CRC PRESS
PI BOCA RATON
PA 6000 BROKEN SOUND PKWY, NW, STE 300, BOCA RATON, FL 33487 USA
BN 978-1-4200-8586-0
J9 CH CRC DATA MIN KNOW
PY 2009
BP 29
EP 47
PG 19
WC Computer Science, Artificial Intelligence; Computer Science, Information
Systems; Computer Science, Theory & Methods
SC Computer Science
GA BJR30
UT WOS:000267022300002
ER
PT J
AU Pickett, JS
Chen, LJ
Santolik, O
Grimald, S
Lavraud, B
Verkhoglyadova, OP
Tsurutani, BT
Lefebvre, B
Fazakerley, A
Lakhina, GS
Ghosh, SS
Grison, B
Decreau, PME
Gurnett, DA
Torbert, R
Cornilleau-Wehrlin, N
Dandouras, I
Lucek, E
AF Pickett, J. S.
Chen, L. -J.
Santolik, O.
Grimald, S.
Lavraud, B.
Verkhoglyadova, O. P.
Tsurutani, B. T.
Lefebvre, B.
Fazakerley, A.
Lakhina, G. S.
Ghosh, S. S.
Grison, B.
Decreau, P. M. E.
Gurnett, D. A.
Torbert, R.
Cornilleau-Wehrlin, N.
Dandouras, I.
Lucek, E.
TI Electrostatic solitary waves in current layers: from Cluster
observations during a super-substorm to beam experiments at the LAPD
SO NONLINEAR PROCESSES IN GEOPHYSICS
LA English
DT Article
CT Nonlinear Wave Workshop 2008
CY APR, 2008
CL Beaulieu, FRANCE
ID PROTON CYCLOTRON WAVES; PHASE-SPACE HOLES; ACOUSTIC WAVES;
ELECTRIC-FIELD; PLASMA; GENERATION; INSTABILITIES; RECONNECTION; NOISE;
POLAR
AB Electrostatic Solitary Waves (ESWs) have been observed by several spacecraft in the current layers of Earth's magnetosphere since 1982. ESWs are manifested as isolated pulses (one wave period) in the high time resolution waveform data obtained on these spacecraft. They are thus nonlinear structures generated out of nonlinear instabilities and processes. We report the first observations of ESWs associated with the onset of a super-substorm that occurred on 24 August 2005 while the Cluster spacecraft were located in the magnetotail at around 18-19 R(E) and moving northward from the plasma sheet to the lobes. These ESWs were detected in the waveform data of the WBD plasma wave receiver on three of the Cluster spacecraft. The majority of the ESWs were detected about 5 min after the super-substorm onset during which time 1) the PEACE electron instrument detected significant field-aligned electron fluxes from a few 100 eV to 3.5 keV, 2) the EDI instrument detected bursts of field-aligned electron currents, 3) the FGM instrument detected substantial magnetic fluctuations and the presence of Alfv,n waves, 4) the STAFF experiment detected broadband electric and magnetic waves, ion cyclotron waves and whistler mode waves, and 5) CIS detected nearly comparable densities of H+ and O+ ions and a large tailward H+ velocity. We compare the characteristics of the ESWs observed during this event to those created in the laboratory at the University of California-Los Angeles Plasma Device (LAPD) with an electron beam. We find that the time durations of both space and LAPD ESWs are only slightly larger than the respective local electron plasma periods, indicating that electron, and not ion, dynamics are responsible for generation of the ESWs. We have discussed possible mechanisms for generating the ESWs in space, including the beam and kinetic Buneman type instabilities and the acoustic instabilities. Future studies will examine these mechanisms in more detail using the space measurements as inputs to models, and better relate the ESW space measurements to the laboratory through PIC code models.
C1 [Pickett, J. S.; Santolik, O.; Gurnett, D. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Chen, L. -J.; Lefebvre, B.; Torbert, R.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Santolik, O.; Grison, B.] Inst Atmospher Phys, Prague, Czech Republic.
[Santolik, O.] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic.
[Grimald, S.; Fazakerley, A.] Univ Coll London, Mullard Space Sci Lab, Holmbury, England.
[Lavraud, B.; Dandouras, I.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, Toulouse, France.
[Lavraud, B.; Dandouras, I.] CNRS, UMR 5187, Toulouse, France.
[Verkhoglyadova, O. P.; Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Verkhoglyadova, O. P.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Lakhina, G. S.] Indian Inst Geomagnetism, Navi Mumbai, India.
[Grison, B.; Cornilleau-Wehrlin, N.] CNRS, LPP, Velizy Villacoublay, France.
[Decreau, P. M. E.] CNRS, LPC2E, F-45071 Orleans, France.
[Decreau, P. M. E.] Univ Orleans, Orleans, France.
[Grison, B.] Estec, ESA, Noordwijk, Netherlands.
[Cornilleau-Wehrlin, N.] Observ Paris, Stn Radioastron Nancay, Nancay, France.
[Lucek, E.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England.
RP Pickett, JS (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
EM pickett@uiowa.edu
RI Chen, Li-Jen/C-2106-2012; Lakhina, Gurbax /C-9295-2012; Ghosh,
Suktisama/J-8494-2013; Santolik, Ondrej/F-7766-2014; Grison,
Benjamin/G-9440-2014;
OI Grison, Benjamin/0000-0002-3440-6856; Dandouras,
Iannis/0000-0002-7121-1118; Lakhina, Gurbax /0000-0002-8956-486X;
Verkhoglyadova, Olga/0000-0002-9295-9539
NR 45
TC 11
Z9 11
U1 0
U2 1
PU COPERNICUS PUBLICATIONS
PI KATHLENBURG-LINDAU
PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY
SN 1023-5809
J9 NONLINEAR PROC GEOPH
JI Nonlinear Process Geophys.
PY 2009
VL 16
IS 3
BP 431
EP 442
PG 12
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 464XQ
UT WOS:000267543500006
ER
PT J
AU Cardace, D
Hoehler, TM
AF Cardace, Dawn
Hoehler, Tori M.
TI Serpentinizing Fluids Craft Microbial Habitat
SO NORTHEASTERN NATURALIST
LA English
DT Article; Proceedings Paper
CT 6th International Conference on Serpentine Ecology
CY JUN 16-23, 2008
CL Coll Atlantic, Bar Harbor, ME
HO Coll Atlantic
ID PARTIAL MOLAL PROPERTIES; HIGH-PRESSURES; TRANSPORT-PROPERTIES;
THERMODYNAMIC PROPERTIES; HYDROTHERMAL SYSTEMS; TEMPERATURES; STANDARD;
DEEP; SUBSURFACE; BACTERIA
AB Hydrogen produced by serpentinization has the potential to fuel subsurface microbial metabolisms. In the serpentinizing subsurface, the solids comprise ultramafic parent rocks derived from the Earth's mantle, serpentine minerals, veins of hydroxides, and accessory magnetite and/or other metal-rich grains. Fluid that occurs with these solids is altered seawater and/or meteoric water and is predicted to be reducing. Hydrogen, a powerful reducing agent, is generated when Fe(2+) in Fe(OH)(2) is oxidized to magnetite, coupled to the reduction of water. Theoretical considerations and experimental work suggest that serpentinization may generate fluid H(2) concentrations as high as approximate to 75 millimolar, and that related seeps on land should have approximate to 300 micromolar. Field observations have shown that submarine serpentinizing seeps contain fluid H(2) concentrations of 1 to 15 millimolar H(2), subseafloor sediments have approximate to 7-100 nanomolar H(2), and thermal springs have approximate to 13 nanomolar H(2). Fluid H(2) has the potential to drive a variety of metabolic processes in oxygen- and organic carbon-deprived environments, such that considerable interest has developed in the potential of serpentinizing systems as an abode of deep subsurface life. Based on empirical parameters, we have modeled the free-energy change for an array of metabolic reactions that may be associated with serpentinization, and find that metabolic niches do exist for methanogenesis, ferric iron reduction, sulfate reduction, and nitrate reduction, given environmentally realistic fluid chemistries.
C1 [Cardace, Dawn; Hoehler, Tori M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Cardace, D (reprint author), NASA, Ames Res Ctr, MS 239-4, Moffett Field, CA 94035 USA.
EM dawn.cardace-1@nasa.gov
NR 49
TC 12
Z9 13
U1 0
U2 12
PU HUMBOLDT FIELD RESEARCH INST
PI STEUBEN
PA PO BOX 9, STEUBEN, ME 04680-0009 USA
SN 1092-6194
J9 NORTHEAST NAT
JI Northeast. Nat
PY 2009
VL 16
SI 5
BP 272
EP 284
DI 10.1656/045.016.0520
PG 13
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 585GU
UT WOS:000276813900020
ER
PT J
AU Wargo, AM
Tilburg, CE
Driggers, WB
Sulikowski, JA
AF Wargo, Andrew M.
Tilburg, Charles E.
Driggers, William B.
Sulikowski, James A.
TI Observations on the Distribution of Ichthyoplankton within the Saco
River Estuary System
SO NORTHEASTERN NATURALIST
LA English
DT Article
ID LARVAL FISHES; MAINE; ABUNDANCE; DYNAMICS; GULF; BAY
AB Determining planktonic larval species composition and abundance data can serve to elucidate local patterns of distribution, determine an area's importance as a nursery ground, and help clarify broad-scale trends of adult distribution and spawning ranges. Although the Saco River and estuary is the fourth largest waterway system in Maine, this ecosystem has remained relatively unstudied over the last thirty years, and research describing the temporal ichthyoplankton composition and distribution is virtually absent. The present study examined the structure of the ichthyoplankton community and determined the temporal and spatial variation in species diversity and abundance within the Saco Bay estuary system. Weekly sampling trips during the months of June, July, and August in 2007 revealed ten species of ichthyoplankton present in the study area. Ulvaria subbifurcata (Radiated Shanny) and Tautogolabrus adsperus (Cunner) dominated the abundance data followed by Hippoglossoides platessoides (American Plaice) and Myoxocephalus octodecims-pinosus (Longhorn Sculpin).
C1 [Wargo, Andrew M.; Tilburg, Charles E.; Sulikowski, James A.] Univ New England, Ctr Marine Sci, Biddeford, ME 04005 USA.
[Driggers, William B.] SE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pascagoula, MS 39568 USA.
RP Sulikowski, JA (reprint author), Univ New England, Ctr Marine Sci, 11 Hills Beach Rd, Biddeford, ME 04005 USA.
EM jsulikowski@une.edu
FU University of New England Marine Science Center
FX We thank Tim Arienti, Nathan Furey, and Angela Cicia for their help in
sample collections. Thanks are further extended to Dr. John Olney for
his help in identification of the ichthyoplankton. This project was
supported by a University of New England Marine Science Center (MSC)
Summer Fellowship to J.A. Sulikowski and C.E. Tilburg. This manuscript
represents MSC contribution number 20.
NR 10
TC 3
Z9 3
U1 0
U2 4
PU HUMBOLDT FIELD RESEARCH INST
PI STEUBEN
PA PO BOX 9, STEUBEN, ME 04680-0009 USA
SN 1092-6194
J9 NORTHEAST NAT
JI Northeast. Nat
PY 2009
VL 16
IS 4
BP 647
EP 654
DI 10.1656/045.016.n414
PG 8
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 537IV
UT WOS:000273107500014
ER
PT B
AU Yee, HC
Sjogreen, B
AF Yee, H. C.
Sjoegreen, B.
BE Pogorelov, NV
Audit, E
Colella, P
Zank, GP
TI On Challenges for Hypersonic Turbulent Simulations
SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2008
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 3rd International Conference on Numerical Modeling of Space Plasma Flows
CY JUN 08-13, 2008
CL St Johns, VI
SP Univ Calif, Inst Geophys & Planetary Phys, Universe French Commiss Atom Energy, Inst Investigat Fundamental Laws
ID FINITE-DIFFERENCE SCHEMES; LARGE-EDDY SIMULATION; SOURCE TERMS;
NONOSCILLATORY SCHEMES; NUMERICAL-SOLUTIONS; HYPERBOLIC PROBLEMS;
WAVE-PROPAGATION; RESOLUTION; ALGORITHM; EQUATIONS
AB This short note discusses some of the challenges for design of suitable spatial numerical schemes for hypersonic turbulent flows, including combustion, and thermal and chemical nonequilibrium flows. Often, hypersonic turbulent flows around re-entry space vehicles and space physics involve mixed steady strong shocks and turbulence with unsteady shocklets. Material mixing in combustion poses additional computational challenges. Proper control of numerical dissipation in numerical methods beyond the standard shock-capturing dissipation at discontinuities is an essential element for accurate and stable simulations of the subject physics. On the one hand, the physics of strong steady shocks and unsteady turbulence/shocklet interactions under the nonequilibrium environment is not well understood. On the other hand, standard and newly developed high order accurate (fourth-order or higher) schemes were developed for homogeneous hyerbolic conservation laws and mixed hyperbolic and parabolic. p partial differential equations (PDEs) (without source terms). The majority of finite rate chemistry and thermal nonequilibrium simulations employ methods for homogeneous time-dependent PDEs with a pointwise evaluation of the source terms. The pointwise evaluation of the source term might not be the best choice for stability, accuracy and minimization of spurious numerics for the overall scheme.
C1 [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94040 USA.
[Sjoegreen, B.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
RP Yee, HC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94040 USA.
EM helen.m.yee@nasa.gov
FU NASA Fundamental Aeronautics Hypersonic; U.S. Department of Energy by
Lawrence Livermore National Laboratory [DE-AC52-07NA27344]
FX The financial support from the NASA Fundamental Aeronautics (Hypersonic)
program for the first author is gratefully acknowledged. This work
performed under the auspices of the U.S. Department of Energy by
Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344.
NR 69
TC 0
Z9 0
U1 0
U2 1
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-692-9
J9 ASTR SOC P
PY 2009
VL 406
BP 61
EP +
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJW00
UT WOS:000267287200009
ER
PT B
AU Usmanov, AV
Matthaeus, WH
Breech, B
Goldstein, ML
AF Usmanov, Arcadi V.
Matthaeus, William H.
Breech, Ben
Goldstein, Melvyn L.
BE Pogorelov, NV
Audit, E
Colella, P
Zank, GP
TI An MHD Solar Wind Model with Turbulence Transport
SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2008
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 3rd International Conference on Numerical Modeling of Space Plasma Flows
CY JUN 08-13, 2008
CL St Johns, VI
SP Univ Calif, Inst Geophys & Planetary Phys, Universe French Commiss Atom Energy, Inst Investigat Fundamental Laws
ID ALFVEN WAVES; FLUCTUATIONS; DISSIPATION; EVOLUTION
AB We present initial results from an axisymmetric steady-state solar wind model that describes properties of the large-scale solar wind, interplanetary magnetic field, and turbulence throughout the heliosphere from 0.3 AU to 100 AU. The model is based on numerical solutions of large-scale Reynolds-averaged magnetohydrodynamic (MHD) equations coupled with a set of small-scale transport equations for the turbulence energy, normalized cross-helicity, and correlation scale. The combined set of the time-dependent equations is solved in the frame of reference corotating with the Sun by a time-relaxation method. We use the model to study the global solar wind structure and the distribution of turbulence throughout the heliosphere.
C1 [Usmanov, Arcadi V.; Matthaeus, William H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Usmanov, Arcadi V.; Matthaeus, William H.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Usmanov, Arcadi V.; Breech, Ben; Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD USA.
RP Usmanov, AV (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
EM arcadi.usmanov@nasa.gov; melvyn.goldstein@gsfc.nasa.gov
RI Goldstein, Melvyn/B-1724-2008; Usmanov, Arcadi/A-9860-2013
NR 26
TC 9
Z9 9
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-692-9
J9 ASTR SOC P
PY 2009
VL 406
BP 160
EP +
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJW00
UT WOS:000267287200022
ER
PT B
AU Burlaga, LF
AF Burlaga, L. F.
BE Pogorelov, NV
Audit, E
Colella, P
Zank, GP
TI Tsallis Statistics for Models and Observations of the Heliospheric
Magnetic Field
SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2008
SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES
LA English
DT Proceedings Paper
CT 3rd International Conference on Numerical Modeling of Space Plasma Flows
CY JUN 08-13, 2008
CL St Johns, VI
SP Univ Cal, Inst Geophys & Planetary Phys, Universe French Commiss Atom Energy, Inst Investigat Fundamental Laws
ID SPEED FLUCTUATIONS; OUTER HELIOSPHERE; BOLTZMANN-GIBBS; 95 AU;
EVOLUTION; SCALES
AB The solar wind is a driven, open, non-linear, non-equilibrium, complex system. Streams, slow flows, ejecta, shocks, etc. produced near the Sun interact as they move away from the sun to create an evolving complex multiscale structure. During solar maximum, interaction regions merge with increasing distance from the sun, and these merged interaction regions coalesce form Global Merged Interaction Regions (GMIRs) which grow out to approximate to 45 AU and then decay out to 90 AU. One aspect of the statistical structure of the observed fluctuations of the magnetic strength B as a function of distance from the sun and scale can be described by the evolution of the probability distributions of increments of B, which can be described by the q-Gaussian functions of Tsallis statistics. These PDFs can be predicted by a deterministic 1-D multi-fluid MHD model with appropriate boundary conditions.
C1 NASA, Goddard Space Flight Ctr, Heliospher Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA.
RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Sci Div, Geospace Phys Lab, Code 673,Bldg 21,Rm 244, Greenbelt, MD 20771 USA.
EM leonard.f.burlaga@nasa.gov
NR 27
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-692-9
J9 ASTR SOC P
PY 2009
VL 406
BP 181
EP 188
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJW00
UT WOS:000267287200024
ER
PT B
AU Putman, WM
Lin, SJ
AF Putman, William M.
Lin, Shian-Jiann
BE Pogorelov, NV
Audit, E
Colella, P
Zank, GP
TI A Finite-Volume Dynamical Core on the Cubed-Sphere Grid
SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2008
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 3rd International Conference on Numerical Modeling of Space Plasma Flows
CY JUN 08-13, 2008
CL St Johns, VI
SP Univ Calif, Inst Geophys & Planetary Phys, Universe French Commiss Atom Energy, Inst Investigat Fundamental Laws
ID PARABOLIC METHOD PPM; TRANSPORT; EQUATIONS
AB The performance of a multidimensional finite-volume scheme for global atmospheric dynamics is evaluated on the cubed-sphere geometry. The development of the finite-volume dynamical core will be discussed from it's latitude-longitude based origins, to the recent implementation oil the cubed-sphere and future non-hydrostatic formulation. Baroclinic evaluation is performed via a recently developed deterministic initial value baroclinic test case from Jablonowski & Williamson (2006) to assess the evolution of ail idealized baroclinic wave in the Northern Hemisphere for global 3-dimensional atmospheric dynamical cores. Comparisons will be made to the traditional latitude-longitude discretization of the finite-volume dynamical core, as well as a spectral formulation for atmospheric dynamical cores. Finally, a glimpse at the achieved and potential scalability of the cubed-sphere finite-volume dynamical core is discussed.
C1 [Putman, William M.] NASA, Goddard Space Flight Ctr, Software Integrat & Visualizat Off, Mail Stop 610-3, Greenbelt, MD 20771 USA.
[Lin, Shian-Jiann] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
RP Putman, WM (reprint author), NASA, Goddard Space Flight Ctr, Software Integrat & Visualizat Off, Mail Stop 610-3, Greenbelt, MD 20771 USA.
EM william.m.putman@nasa.gov
NR 14
TC 15
Z9 15
U1 0
U2 2
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-692-9
J9 ASTR SOC P
PY 2009
VL 406
BP 268
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJW00
UT WOS:000267287200036
ER
PT B
AU Smith, SM
Zwart, SR
Kloeris, V
Heer, M
AF Smith, Scott M.
Zwart, Sara R.
Kloeris, Vickie
Heer, Martina
TI Nutritional Biochemistry of Space Flight
SO NUTRITIONAL BIOCHEMISTRY OF SPACE FLIGHT
SE Space Science Exploration and Policy
LA English
DT Editorial Material; Book
ID BONE-MINERAL DENSITY; SERUM TRANSFERRIN RECEPTOR; RENAL STONE FORMATION;
VITAMIN-D DEFICIENCY; PROLONGED BED REST; BODY IRON STORES; RED-CELL
MASS; LONG-DURATION SPACEFLIGHT; URINARY CALCIUM EXCRETION; CORONARY
HEART-DISEASE
C1 [Smith, Scott M.; Zwart, Sara R.] NASA, Lyndon B Johnson Space Ctr, Nutr Biochem Lab, Human Adaptat & Countermeasures Div,Univ Space Re, Houston, TX 77058 USA.
[Kloeris, Vickie] NASA, Lyndon B Johnson Space Ctr, Space Food Syst Lab, Habitabil & Environm Factors Div, Houston, TX 77058 USA.
[Heer, Martina] Profil Inst Metab Res, Neuss, Germany.
[Heer, Martina] DLR, Inst Aerosp Med, Cologne, Germany.
RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Nutr Biochem Lab, Human Adaptat & Countermeasures Div,Univ Space Re, Houston, TX 77058 USA.
EM scott.m.smith@nasa.gov; sara.zwart-1@nasa.gov;
vickie.l.kloeris@nasa.gov; Martina.Heer@profil-research.de
NR 763
TC 22
Z9 23
U1 0
U2 2
PU NOVA SCIENCE PUBLISHERS, INC
PI HAUPPAUGE
PA 400 OSER AVE, STE 1600, HAUPPAUGE, NY 11788-3635 USA
BN 978-1-60741-641-8
J9 SPACE SCI EXPLOR POL
PY 2009
BP 1
EP +
PG 166
WC Biochemistry & Molecular Biology; Nutrition & Dietetics
SC Biochemistry & Molecular Biology; Nutrition & Dietetics
GA BLS67
UT WOS:000270952200001
ER
PT B
AU MacLeod, TC
Sims, WH
Varnavas, KA
Sayyah, R
Ho, FD
AF MacLeod, Todd C.
Sims, W. Herb
Varnavas, Kosta A.
Sayyah, Rana
Ho, Fat D.
GP IEEE
TI Satellite Test of Radiation Impact on Ramtron 512K FRAM
SO NVMTS: 2009 10TH ANNUAL NON-VOLATILE MEMORY TECHNOLOGY SYMPOSIUM
LA English
DT Proceedings Paper
CT 10th Annual Non-Volatile Memory Technology Symposium
CY OCT 25-28, 2009
CL Portland, OR
DE component; FRAM; Satellite; Radiation Test
AB The Memory Test Experiment is a space test of a ferroelectric memory device on a low Earth orbit satellite. The test consists of writing and reading data with a ferroelectric based memory device. Any errors are detected and are stored on board the satellite. The data is send to the ground through telemetry once a day. Analysis of the data can determine the kind of error that was found and will lead to a better understanding of the effects of space radiation on memory systems. The test will be one of the first flight demonstrations of ferroelectric memory in a near polar orbit which allows testing in a varied radiation environment. The memory devices being tested is a Ramtron Inc. 512K memory device. This paper details the goals and purpose of this experiment as well as the development process. The process for analyzing the data to gain the maximum understanding of the performance of the ferroelectric memory device is detailed.
C1 [MacLeod, Todd C.; Sims, W. Herb; Varnavas, Kosta A.] NASA, Marshall Space Flight Ctr, Space Syst Dept, Huntsville, AL 35812 USA.
[Sayyah, Rana; Ho, Fat D.] Univ Alabama, Dept Elect Engn, Huntsville, AL USA.
RP MacLeod, TC (reprint author), NASA, Marshall Space Flight Ctr, Space Syst Dept, Huntsville, AL 35812 USA.
EM todd.macleod@nasa.gov
NR 4
TC 3
Z9 3
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4244-4953-8
PY 2009
BP 24
EP +
DI 10.1109/NVMT.2009.5429778
PG 2
WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA BPF44
UT WOS:000278758600005
ER
PT S
AU Gross, RS
Lavallee, DA
Blewitt, G
Clarke, PJ
AF Gross, Richard S.
Lavallee, David A.
Blewitt, Geoffrey
Clarke, Peter J.
BE Sideris, MG
TI Consistency of Earth Rotation, Gravity, and Shape Measurements
SO OBSERVING OUR CHANGING EARTH
SE International Association of Geodesy Symposia
LA English
DT Proceedings Paper
CT General Assembly of the International-Association-of-Geodesy/24th
General Assembly of the International-Union-of-Geodesy-and-Geophysics
CY JUL 02-13, 2007
CL Perugia, ITALY
SP Int Assoc Geodesy, Int Union Geodesy & Geophys
DE Earth rotation; Earth shape; Gravity; Surface mass density
ID OCEAN TIDES; SEA-LEVEL; MASS
AB Degree-2 spherical harmonic coefficients of the surface mass density determined from independent GRACE, SLR, GPS, and Earth rotation measurements are compared to each other and to a model of the surface mass density obtained by summing the contributions of atmospheric pressure, ocean-bottom pressure, land hydrology, and a mass-conserving term. In general, the independent measurements are found to be quite consistent with each other and with the model, with correlations being as high as 0.87 and with the model explaining as much as 88% of the observed variance. But no measurement technique is found to be best overall. For the different degree-2 coefficients, measurements from different techniques are found to agree best with the model. Thus, each measurement technique contributes to understanding the degree-2 surface mass density of the Earth.
C1 [Gross, Richard S.] CALTECH, Jet Prop Lab, Mail Stop 238-600,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Lavallee, David A.; Clarke, Peter J.] Newcastle Univ, Sch Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
[Blewitt, Geoffrey] Univ Nevada, Nevada Bur, Mines & Geol & Seismol Lab, Reno, NV 89557 USA.
RP Gross, RS (reprint author), CALTECH, Jet Prop Lab, Mail Stop 238-600,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Clarke, Peter/B-1783-2008; Symposia, IAG/K-2857-2012
OI Clarke, Peter/0000-0003-1276-8300;
FU Earth Surface and Interior Focus Area of NASA; NASA [NNG04G099G,
NAG5-13683]; UK Natural Environment Research Council
[NER/A/S/2001/01166]; Royal Society University Research Fellowship
FX We thank the IGS analysis center at Scripps Institution of Oceanography
for freely providing GPS SINEX files for use by the geodetic community.
The work of one of the authors (RSG) described in this paper was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. Support for the work of RSG was provided by the Earth
Surface and Interior Focus Area of NASA. Support for GB was provided by
NASA grants NNG04G099G and NAG5- 13683. PJC acknowledges grant
NER/A/S/2001/01166 from the UK Natural Environment Research Council, and
DAL was supported by a Royal Society University Research Fellowship.
NR 22
TC 3
Z9 3
U1 0
U2 1
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0939-9585
BN 978-3-540-85425-8
J9 IAG SYMP
PY 2009
VL 133
BP 463
EP +
PG 3
WC Geochemistry & Geophysics; Geology; Geosciences, Multidisciplinary
SC Geochemistry & Geophysics; Geology
GA BIT95
UT WOS:000262710400056
ER
PT S
AU Behrend, D
Bohm, J
Charlot, R
Clark, T
Corey, B
Gipson, J
Haas, R
Koyama, Y
MacMillan, D
Malkin, Z
Niell, A
Nilsson, T
Petrachenko, B
Rogers, A
Tuccari, G
Wresnik, J
AF Behrend, D.
Boehm, J.
Charlot, R.
Clark, T.
Corey, B.
Gipson, J.
Haas, R.
Koyama, Y.
MacMillan, D.
Malkin, Z.
Niell, A.
Nilsson, T.
Petrachenko, B.
Rogers, A.
Tuccari, G.
Wresnik, J.
BE Sideris, MG
TI Recent Progress in the VLBI2010 Development
SO OBSERVING OUR CHANGING EARTH
SE International Association of Geodesy Symposia
LA English
DT Proceedings Paper
CT General Assembly of the International-Association-of-Geodesy/24th
General Assembly of the International-Union-of-Geodesy-and-Geophysics
CY JUL 02-13, 2007
CL Perugia, ITALY
SP Int Assoc Geodesy, Int Union Geodesy & Geophys
DE Geodetic VLBI; Next generation VLBI2010; IVS; Monte Carlo simulations
ID GEODESY
AB From October 2003 to September 2005, the International VLBI Service for Geodesy and Astrometry (IVS) examined current and future requirements for geodetic VLBI, including all components from antennas to analysis. IVS Working Group 3 "VLBI 2010", which was tasked with this effort, concluded with recommendations for a new generation of VLBI systems. These recommendations were based on the goals of achieving I mm measurement accuracy on global baselines, performing continuous measurements for time series of station positions and Earth orientation parameters, and reaching a turnaround time from measurement to initial geodetic results of less than 24 It. To realize these recommendations and goals, along with the need for low cost of construction and operation, requires a complete examination of all aspects of geodetic VLBI including equipment, processes, and observational strategies. Hence, in October 2005, the IVS VLBI2010 Committee (V2C) commenced work on defining the VLBI2010 system specifications. In this paper we give a summary of the recent progress of the VLBI2010 project.
C1 [Behrend, D.; Clark, T.; Gipson, J.; MacMillan, D.] NASA, Goddard Space Flight Ctr, NVI Inc, Code 698, Greenbelt, MD 20771 USA.
[Boehm, J.] Vienna Univ Technol, Inst Geodesy & Geophys, AT-1040 Vienna, Austria.
[Charlot, R.] Observ Bordeaux, CNRS UMR 5804, F-33270 Floirac, France.
[Clark, T.; Gipson, J.; MacMillan, D.] NASA, Goddard Space Flight Ctr, NVI Inc, Greenbelt, MD 20771 USA.
[Corey, B.; Niell, A.; Rogers, A.] MIT, Haystack Observ, Westford, MA 01886 USA.
[Haas, R.; Nilsson, T.] Chalmers, Onala Space Observ, SE-43992 Onsala, Sweden.
[Koyama, Y.] Kashima Space Res Ctr, NICT, Kashima, Ibaraki 3148501, Japan.
[Malkin, Z.] Pulkovo Observ, St Petersburg 196140, Russia.
[Petrachenko, B.] Nat Resources Canada, Geodet Survey Div, Ottawa, ON K1A 0E9, Canada.
[Tuccari, G.] INFA, Inst Radioastronomia, IT-96017 Noto, Italy.
RP Behrend, D (reprint author), NASA, Goddard Space Flight Ctr, NVI Inc, Code 698, Greenbelt, MD 20771 USA.
RI Haas, Rudiger/G-1286-2010; Nilsson, Tobias/D-3764-2012; Symposia,
IAG/K-2857-2012; Bohm, Johannes/H-9161-2013; Malkin, Zinovy/C-1560-2008;
OI Haas, Rudiger/0000-0003-2681-9228; Nilsson, Tobias/0000-0003-4103-9078;
Bohm, Johannes/0000-0002-1208-5473; Malkin, Zinovy/0000-0002-5583-8391;
Tuccari, Gino/0000-0001-7175-1977
FU Austrian Science Fund (FWF) [P18404-N10]
FX J. Bohm and J. Wresnik are grateful to the Austrian Science Fund (FWF)
for supporting this work within Project P18404-N10.
NR 14
TC 9
Z9 9
U1 0
U2 4
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0939-9585
BN 978-3-540-85425-8
J9 IAG SYMP
PY 2009
VL 133
BP 833
EP +
PG 4
WC Geochemistry & Geophysics; Geology; Geosciences, Multidisciplinary
SC Geochemistry & Geophysics; Geology
GA BIT95
UT WOS:000262710400096
ER
PT S
AU Fisher, AD
VanZwieten, JH
VanZwieten, TS
AF Fisher, A. D.
VanZwieten, J. H., Jr.
VanZwieten, T. S.
GP IEEE
TI Adaptive Control of Small Outboard-Powered Boats for Survey Applications
SO OCEANS 2009, VOLS 1-3
SE OCEANS-IEEE
LA English
DT Proceedings Paper
CT Oceans 2009 Conference
CY OCT 26-29, 2009
CL Biloxi, MS
SP Marine Technol Soc, IEEE Ocean Engn Soc
DE Autopilot; Adaptive Control; Neuro-adaptive; Adaptive Augmentation;
Adaptive PID; Outboard Motor Control
AB Four autopilot controllers have been developed in this work that can both hold a desired heading and follow a straight line. These PID, adaptive PID, neuro-adaptive, and adaptive augmenting control algorithms have all been implemented into a numerical simulation of a 33-foot center console vessel with wind, waves, and current disturbances acting in the perpendicular (across-track) direction of the boat's desired trajectory. Each controller is tested for its ability to follow a desired heading in the presence of these disturbances and then to follow a straight line at two different throttle settings for the same disturbances. These controllers were tuned for an input thrust of 2000 N and all four controllers showed good performance with none of the controllers significantly outperforming the others when holding a constant heading and following a straight line at this engine thrust. Each controller was then tested for a reduced engine thrust of 1200 N per engine where each of the three adaptive controllers reduced heading error and across-track error by approximately 50% after a 300 second tuning period when compared to the fixed gain PID, showing that significant robustness to changes in throttle setting was gained by using an adaptive algorithm.
C1 [Fisher, A. D.; VanZwieten, J. H., Jr.] Florida Atlantic Univ, 101 N Beach Rd, Dania, FL 33004 USA.
[VanZwieten, T. S.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Fisher, AD (reprint author), Florida Atlantic Univ, 101 N Beach Rd, Dania, FL 33004 USA.
EM afishe14@fau.edu; jvanzwi@fau.edu; tannen.s.vanzwieten@nasa.gov
NR 14
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0197-7385
BN 978-1-4244-4960-6
J9 OCEANS-IEEE
PY 2009
BP 667
EP +
PG 2
WC Engineering, Ocean; Oceanography; Remote Sensing
SC Engineering; Oceanography; Remote Sensing
GA BPY34
UT WOS:000280322600099
ER
PT S
AU Small, RJ
Campbell, T
Teixeira, J
Smith, TA
Dykes, J
Chen, S
Allard, R
AF Small, R. J.
Campbell, T.
Teixeira, J.
Smith, T. A.
Dykes, J.
Chen, S.
Allard, R.
GP IEEE
TI Air-Sea Interaction In The Ligurian Sea: Numerical Simulations And
In-Situ Data In The Summer Of 2007
SO OCEANS 2009, VOLS 1-3
SE OCEANS-IEEE
LA English
DT Proceedings Paper
CT Oceans 2009 Conference
CY OCT 26-29, 2009
CL Biloxi, MS
SP Marine Technol Soc, IEEE Ocean Engn Soc
ID WESTERN MEDITERRANEAN-SEA; MODEL
AB In situ experimental data and numerical model results are presented from the Ligurian Sea in the north-western Mediterranean. Here surface winds are light in summer except during occasional Mistral events which are often associated with cyclogenesis in the lee of the Alps. The Ligurian Sea Air-Sea Interaction Experiment (LASIE07) took place in June 2007, with a focus on the coincident measurement of oceanic and atmospheric boundary layer properties.
To help interpret the observational results we use the Coupled Ocean-Atmosphere Mesoscale Prediction System (COAMPS (R)), developed at the Naval Research Laboratory. This system includes an atmospheric sigma coordinate, non-hydrostatic model, coupled to a hydrostatic sigma-z level ocean model (Naval Coastal Ocean Model), using the Earth System Modeling Framework (ESMF). Both models are at high resolution: the inner nest of the COAMPS domain is on a 4 km grid with 40 vertical levels, and that for NCOM on a 2km grid with 50 levels.
The coupled model system is evaluated for a month-long simulation which includes data assimilation in the atmosphere but not the ocean. Correlatation coefficients between model and observed values for near-surface wind speeds, and turbulent heat fluxes are above 0.5 (significant at 99%) at a deep water mooring.
A comparison of the coupled run with an uncoupled atmospheric run using analysis SST at the surface boundary, both of which use atmospheric data assimilation, does not reveal significant or systematic differences. Therefore a non-assimilating run for the period of a strong wind event (26-29 June), is performed to examine more closely the impact of coupling on the flux fields and SST. Here, the cooling of SST up to 3 degrees C over 72 hours in a fully coupled run affects the surface stress, which is reduced by similar to 20%, and the surface latent heat flux which is reduced by 50%, relative to an uncoupled simulation where the SST is kept fixed at the initial value of the coupled run. In other words, the coupling provides a negative feedback on the surface forcing under strong winds.
C1 [Small, R. J.; Campbell, T.; Smith, T. A.; Dykes, J.; Allard, R.] USN, Res Lab, Code 7320,Bldg 1009, Stennis Space Ctr, MS 39529 USA.
[Teixeira, J.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chen, S.] NRL Monterey, Monterey, CA 93943 USA.
RP Small, RJ (reprint author), USN, Res Lab, Code 7320,Bldg 1009, Stennis Space Ctr, MS 39529 USA.
FU High Performance Computing Modernization Program's Battlespace
Environments Institute and NRL's 6.2 Core Program "Battlespace
Environment Assessment for Situational Awareness" [PE 0602435N]
FX RJS, TC, TAS, and RA were supported by the High Performance Computing
Modernization Program's Battlespace Environments Institute and NRL's 6.2
Core Program "Battlespace Environment Assessment for Situational
Awareness"(Program Element PE 0602435N).
NR 13
TC 0
Z9 0
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0197-7385
BN 978-1-4244-4960-6
J9 OCEANS-IEEE
PY 2009
BP 676
EP +
PG 3
WC Engineering, Ocean; Oceanography; Remote Sensing
SC Engineering; Oceanography; Remote Sensing
GA BPY34
UT WOS:000280322600100
ER
PT S
AU Blonski, S
Holekamp, K
Spiering, BA
AF Blonski, Slawomir
Holekamp, Kara
Spiering, Bruce A.
GP IEEE
TI NASA Satellite Monitoring of Water Clarity in Mobile Bay for Nutrient
Criteria Development
SO OCEANS 2009, VOLS 1-3
SE OCEANS-IEEE
LA English
DT Proceedings Paper
CT Oceans 2009 Conference
CY OCT 26-29, 2009
CL Biloxi, MS
SP Marine Technol Soc, IEEE Ocean Engn Soc
ID ATMOSPHERIC CORRECTION; COASTAL WATERS; ABSORPTION-COEFFICIENTS;
CROSS-CALIBRATION; LANDSAT-7 ETM+; TIME-SERIES; MODIS; OCEAN; COLOR;
PHYTOPLANKTON
AB Water clarity controls the loss of sunlight reaching the underwater habitats. Because many organisms living in estuarine and coastal waters rely on photosynthesis, water clarity needs to be incorporated into protective water quality standards for these valued ecosystems. To develop the protective standards, a better understanding of causes and effects of water clarity variability at local and regional scales is needed. To that end, NASA remote sensing data are being used to monitor water clarity (measured by light attenuation) and the constituents that decrease water clarity (chlorophyll a, total suspended solids, and colored dissolved organic matter) in the estuarine and coastal systems of the northern Gulf of Mexico. The NASA measurements are intended to augment and extend temporal and spatial coverage of water clarity monitoring conducted by the Federal and State environmental agencies in the same areas. The main objective is to develop a methodology for and to demonstrate the feasibility of producing long-term (1984 to present) time series of the water clarity parameters based on combined satellite measurements from the Moderate Resolution Imaging Spectroradiometer (MODIS) instruments deployed on the Aqua and Terra spacecraft and from the Thematic Mapper (TM) and Enhanced Thematic Mapper Plus (ETM+) instruments from the Landsat 4/5 and Landsat 7 spacecraft, respectively. Aqua and Terra MODIS provide daily coverage dating from 2000, while Landsat TM/ETM+ data extend back to 1984, although with frequency of only once per 8 to 16 days. NASA Earth science research results that improved instrument calibration and data processing techniques have enabled merging the time series of observations from Landsat and MODIS. Algorithms for the retrieval of water clarity parameters from satellite data selected for this project are based on the inherent optical properties of water: absorption and scattering of light. The algorithms are refined based on comparison with field data collected during water quality monitoring in Mobile Bay, Alabama. Results of this project will support future interagency collaborative efforts to develop numeric nutrient criteria for estuarine and coastal waters in the Gulf of Mexico and will contribute to addressing the Gulf of Mexico Alliance priority issue of reducing nutrient inputs to coastal ecosystems.
C1 [Blonski, Slawomir; Holekamp, Kara] Sci Syst & Applicat Inc, Bldg 1105, Stennis Space Ctr, MS 39529 USA.
[Spiering, Bruce A.] NASA, Appl Sci & Technol Project Off, Stennis Space Ctr, MS 39529 USA.
RP Blonski, S (reprint author), Sci Syst & Applicat Inc, Bldg 1105, Stennis Space Ctr, MS 39529 USA.
FU Science Systems and Applications, Inc; NASA at the John C. Stennis Space
Center; Mississippi [NNS04AB54T]
FX Participation in this research by Science Systems and Applications,
Inc., was supported by NASA at the John C. Stennis Space Center,
Mississippi, under Task Order NNS04AB54T.
NR 19
TC 0
Z9 0
U1 1
U2 5
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0197-7385
BN 978-1-4244-4960-6
J9 OCEANS-IEEE
PY 2009
BP 1117
EP +
PG 2
WC Engineering, Ocean; Oceanography; Remote Sensing
SC Engineering; Oceanography; Remote Sensing
GA BPY34
UT WOS:000280322600165
ER
PT S
AU Kalcic, M
Hall, C
Russell, J
Fletcher, R
AF Kalcic, Maria
Hall, Callie
Russell, Jeff
Fletcher, Rose
GP IEEE
TI Monitoring Coastal Marshes for Persistent Saltwater Intrusion
SO OCEANS 2009, VOLS 1-3
SE OCEANS-IEEE
LA English
DT Proceedings Paper
CT Oceans 2009 Conference
CY OCT 26-29, 2009
CL Biloxi, MS
SP Marine Technol Soc, IEEE Ocean Engn Soc
AB Saltwater flooding of coastal marshes by storm surge, rising sea level, and subsidence is a primary cause of wetland deterioration and habitat loss. The objective of this study is to provide resource managers with remote sensing products that support ecosystem-forecasting models requiring inundation data. This investigation employed time-series indices derived from 250-meter NASA Moderate Resolution Imaging Spectroradiometer (MODIS) and 30-m Landsat imagery to map flooding and saltwater stress in the Sabine Basin in southwest Louisiana, before and after Hurricane Rita in 2005. After nearly 20 feet of storm surge inundated the area during Hurricane Rita, Hurricane Ike produced a storm surge of almost 14 feet in the same area and flooded areas as far as 30 miles inland. The study design of this investigation centered upon the use of vegetation and wetness (water) indicators to map flooded areas. The study team assigned a vegetation index to marsh areas of concomitant vegetation and water. We derived daily MODIS time series of Normalized Difference Vegetation Index, Normalized Difference Water Index, and Normalized Difference Soil Index from the NASA Stennis Space Center Time Series Product Tool, which provides the capability to compute phenological parameters and performs temporal modeling at ecosystem scales. We estimated the extent of flooding as the percentage of time the MODIS index was water; i.e., below a certain threshold. The percentages indicate areas of persistent flooding over certain time intervals, thereby informing planners of areas with a high probability of conversion to open water. The study team used Landsat 5 and 7 data for the years 2004 through 2006 to produce an 8-day time series of vegetation and wetness indices. We evaluated these Landsat-based flood maps with lidar data and in situ elevation data collected by the U.S. Geological Survey (USGS) and Louisiana Department of Natural Resources Coastwide Reference Monitoring System for the Sabine Basin. Finally, we combined salinity data collected in situ from the USGS and from the National Oceanic and Atmospheric Administration with our flooding estimates to map areas of persistent saltwater intrusion. The combination of these data are useful for habitat switching modules that predict the migration of marsh species from one salinity regime to another from estimates of the annual percent inundation and the mean annual salinity.
C1 [Kalcic, Maria; Fletcher, Rose] Sci Syst & Applicat Inc, Bldg 1105, John C Stennis Space Ctr, MS 39529 USA.
[Hall, Callie] NASA, Stennis Space Ctr, MS 39529 USA.
[Russell, Jeff] CSC, Stennis Space Ctr, MS 39529 USA.
RP Kalcic, M (reprint author), Sci Syst & Applicat Inc, Bldg 1105, John C Stennis Space Ctr, MS 39529 USA.
FU Science Systems and Applications, Inc; NASA at the John C. Stennis Space
Center, Mississippi [NNS04AB54T]
FX The authors wish to thank Mr. Abe Dailey, who worked at NASA/SSC as a
summer student from the University of Southern Maine. He was responsible
for compiling the many sources of data and for producing the salinity
data grids. Participation in this work by Science Systems and
Applications, Inc. was supported by NASA under Task Order NNS04AB54T at
the John C. Stennis Space Center, Mississippi.
NR 6
TC 0
Z9 0
U1 2
U2 5
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0197-7385
BN 978-1-4244-4960-6
J9 OCEANS-IEEE
PY 2009
BP 1150
EP +
PG 2
WC Engineering, Ocean; Oceanography; Remote Sensing
SC Engineering; Oceanography; Remote Sensing
GA BPY34
UT WOS:000280322600169
ER
PT S
AU Spruce, J
Ellis, J
Smoot, J
Swann, R
Graham, W
AF Spruce, Joseph
Ellis, Jean
Smoot, James
Swann, Roberta
Graham, William
GP IEEE
TI A Landsat-based Assessment of Mobile Bay Land Use and Land Cover Change
from 1974 to 2008
SO OCEANS 2009, VOLS 1-3
SE OCEANS-IEEE
LA English
DT Proceedings Paper
CT Oceans 2009 Conference
CY OCT 26-29, 2009
CL Biloxi, MS
SP Marine Technol Soc, IEEE Ocean Engn Soc
ID COASTAL; LOUISIANA
AB This paper discusses results of a Gulf of Mexico Application Pilot project conducted in 2008 to quantify and assess land use land cover (LULC) change from 1974 to 2008. Led by NASA Stennis Space Center, this project involved multiple Gulf of Mexico Alliance (GOMA) partners, including the Mobile Bay National Estuary Program (NEP), the U.S. Army Corps of Engineers, the National Oceanic and Atmospheric Administration's (NOAA's) National Coastal Data Development Center (NCDDC), and the NOAA Coastal Services Center. The Mobile Bay region provides great economic and ecologic benefits to the Nation, including important coastal habitat for a broad diversity of fisheries and wildlife. The Mobile Bay region has experienced considerable LULC change since the latter half of the 20th century. Accompanying this change has been urban expansion and a reduction of rural land uses. Much of this LULC change (largely urbanization) has reportedly occurred since the landfall of Hurricane Frederic in 1979. Regional urbanization threatens the estuary's water quality and aquatic-habitat dependent biota, including commercial fisheries and avian wildlife. Coastal conservation and urban land use planners require additional information on historical LULC change to support coastal habitat restoration and resiliency management efforts. This project quantified and assessed LULC change across the 34-year time frame and at decadal and mid-decadal scales. Nine Landsat images were employed to compute LULC products because of their availability and suitability for the application. The project also used Landsat-based national LULC products, including coastal LULC products from NOAA's Coastal Change & Analysis Program (C-CAP), available at 5-year intervals since 1995. Our study was initiated in part because C-CAP LULC products were not available to assess the region's urbanization prior to 1995 and subsequent to post-Hurricane Katrina in 2006.
The study area included the majority of Mobile and Baldwin counties that encompass Mobile Bay. Each date of Landsat data was classified using an end-user defined modified Anderson level 1 classification scheme. LULC classifications were refined using a decision rule approach in conjunction with available C-CAP products. Individual dates of LULC classifications were validated by image interpretation of stratified random locations on raw Landsat color composite imagery in combination with higher resolution remote sensing and in situ reference data. Overall classification accuracies for five separate single-date products ranged from 83% to 89%. The results of the LULC change analysis indicate that during the 34-year study period, urban areas increased from 96,688 to 150,227 acres, representing a 55.37% increase, or 1.63% per annum. Most of the identified urban expansion regarded the conversion of rural forest and agriculture to urban cover types. Final LULC mapping and metadata products were produced for the entire study area as well as for multiple watersheds of concern within the study area. The final project products, including LULC trend information, were incorporated into the Mobile Bay NEP State of the Bay report. Products and metadata were also transferred to NOAA NCDDC to allow free online accessibility and use by COMA partners and by the public.
C1 [Spruce, Joseph; Smoot, James] Sci Syst & Applicat Inc, Stennis Space Ctr, MS 39525 USA.
[Ellis, Jean] Univ South Carolina, Columbia, SC 29208 USA.
[Swann, Roberta] Mobile Bay Natl Estuary Program, Mobile, AL 36615 USA.
[Graham, William] NASA, Stennis Space Ctr, MS 39529 USA.
RP Spruce, J (reprint author), Sci Syst & Applicat Inc, Stennis Space Ctr, MS 39525 USA.
FU NASA's Applied Science and Technology Project Office
FX NASAs Applied Science and Technology Project Office supported J. Ellis.
T. McPherson assisted with project management.
NR 19
TC 0
Z9 0
U1 0
U2 4
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0197-7385
BN 978-1-4244-4960-6
J9 OCEANS-IEEE
PY 2009
BP 1185
EP +
PG 2
WC Engineering, Ocean; Oceanography; Remote Sensing
SC Engineering; Oceanography; Remote Sensing
GA BPY34
UT WOS:000280322600175
ER
PT S
AU Spruce, JP
Smoot, J
Graham, W
AF Spruce, J. P.
Smoot, J.
Graham, W.
GP IEEE
TI Developing New Coastal Forest Restoration Products Based on Landsat,
ASTER, and MODIS Data
SO OCEANS 2009, VOLS 1-3
SE OCEANS-IEEE
LA English
DT Proceedings Paper
CT Oceans 2009 Conference
CY OCT 26-29, 2009
CL Biloxi, MS
SP Marine Technol Soc, IEEE Ocean Engn Soc
ID EASTERN-UNITED-STATES; NOAA AVHRR; IMAGERY; TM; WETLANDS; IMPACT;
DAMAGE; COVER
AB This paper discusses an ongoing effort to develop new geospatial information products for aiding coastal forest restoration and conservation efforts in coastal Louisiana and Mississippi. This project employs Landsat, Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER), and Moderate Resolution Imaging Spectroradiometer (MODIS) satellite data in conjunction with airborne elevation data to compute coastal forest cover type maps and change detection products. Improved forest mapping products are needed to aid coastal forest restoration and management efforts of State and Federal agencies in the Northern Gulf of Mexico (NGOM) region. In particular, such products may aid coastal forest land acquisition and conservation easement procurements. This region's forests are often disturbed and subjected to multiple biotic and abiotic threats, including subsidence, salt water intrusion, hurricanes, sea-level rise, insect-induced defoliation and mortality, altered hydrology, wildfire, and conversion to non-forest land use. In some cases, such forest disturbance has led to forest loss or loss of regeneration capacity. In response, a case study was conducted to assess and demonstrate the potential of satellite remote sensing products for improving forest type maps and for assessing forest change over the last 25 years. Change detection products are needed for assessing risks for specific priority coastal forest types, such as live oak and baldcypress-dominated forest. Preliminary results indicate Landsat time series data are capable of generating the needed forest type and change detection products. Useful classifications were obtained using 2 strategies: 1) general forest classification based on use of 3 seasons of Landsat data from the same year; and 2) classification of specific forest types of concern using a single date of Landsat data in which a given targeted type is spectrally distinct compared to adjacent forested cover. When available, ASTER data was useful as a complement to Landsat data. Elevation data helped to define areas in which targeted forest types occur, such as live oak forests on natural levees. MODIS Normalized Difference Vegetation Index time series data aided visual assessments of coastal forest damage and recovery from hurricanes. Landsat change detection products enabled change to be identified at the stand level and at 10-year intervals with the earliest date preceding available change detection products from the National Oceanic and Atmospheric Administration and from the U.S. Geological Survey. Additional work is being done in collaboration with State and Federal agency partners in a follow-on NASA ROSES project to refine and validate these new, promising products. The products from the ROSES project will be available for aiding NGOM coastal forest restoration and conservation.
C1 [Spruce, J. P.; Smoot, J.] Sci Syst & Applicat Inc, Bldg 1105, Stennis Space Ctr, MS 39529 USA.
[Graham, W.] NASA, Appl Sci & Technol Project Off, Stennis Space Ctr, MS 39529 USA.
RP Spruce, JP (reprint author), Sci Syst & Applicat Inc, Bldg 1105, Stennis Space Ctr, MS 39529 USA.
FU NASA [NNS04AB54T]
FX Participation in this research by Science Systems and Applications,
Inc., was supported by NASA at the John C. Stennis Space Center,
Mississippi, under Task Order NNS04AB54T.
NR 27
TC 0
Z9 0
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0197-7385
BN 978-1-4244-4960-6
J9 OCEANS-IEEE
PY 2009
BP 1265
EP +
PG 3
WC Engineering, Ocean; Oceanography; Remote Sensing
SC Engineering; Oceanography; Remote Sensing
GA BPY34
UT WOS:000280322600187
ER
PT S
AU Alsweiss, S
Laupattarakasem, P
El-Nimri, S
Jones, WL
Veleva, S
Stiles, BW
Rodriguez, E
Gaston, RW
AF Alsweiss, Suleiman
Laupattarakasem, Peth
El-Nimri, Salem
Jones, W. Linwood
Veleva, Svetla
Stiles, Bryan W.
Rodriguez, Ernesto
Gaston, Robert W.
GP IEEE
TI Simulated OVW Retrievals in Tropical Cyclones for the Next Generation
Dual Frequency Scatterometer
SO OCEANS 2009, VOLS 1-3
SE OCEANS-IEEE
LA English
DT Proceedings Paper
CT Oceans 2009 Conference
CY OCT 26-29, 2009
CL Biloxi, MS
SP Marine Technol Soc, IEEE Ocean Engn Soc
AB The purpose of this study is to investigate the potential of the next generation Dual Frequency Scatterometer (DFS) proposed to fly onboard the Japanese Aerospace Exploration Agency (JAXA)/GCOM-W2 future mission to measure surface ocean vector winds. An end-to-end simulation was performed to retrieve ocean vector winds in extreme weather conditions, where high winds are usually associated with high rain rates. Both C- and Ku-bands DFS active measurements were combined in the retrieval algorithm. The simultaneous observations of JAXA's Advanced Microwave Scanning Radiometer (AMSR) were used to passively model both the atmospheric attenuation and rain volume backscatter to correct for rain effects and to further improve the retrievals range for tropical cyclones beyond that exhibited by the current operating scatterometers.
C1 [Alsweiss, Suleiman; Laupattarakasem, Peth; El-Nimri, Salem; Jones, W. Linwood] Univ Cent Florida, Cent Florida Remote Sensing Lab, Orlando, FL 32816 USA.
[Veleva, Svetla; Stiles, Bryan W.; Rodriguez, Ernesto; Gaston, Robert W.] Jet Propuls Lab, Pasadena, CA USA.
RP Alsweiss, S (reprint author), Univ Cent Florida, Cent Florida Remote Sensing Lab, Orlando, FL 32816 USA.
EM suleimanalsweiss@gmail.com
FU DFS Project of the Jet Propulsion Laboratory
FX This work was sponsored by the DFS Project of the Jet Propulsion
Laboratory, Pasadena, CA.
NR 8
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0197-7385
BN 978-1-4244-4960-6
J9 OCEANS-IEEE
PY 2009
BP 1903
EP +
PG 2
WC Engineering, Ocean; Oceanography; Remote Sensing
SC Engineering; Oceanography; Remote Sensing
GA BPY34
UT WOS:000280322601001
ER
PT S
AU Ladner, S
Arnone, R
Sandidge, J
Ko, DS
Casey, B
Hall, C
AF Ladner, Sherwin
Arnone, Robert
Sandidge, Juanita
Ko, DongShan
Casey, Brandon
Hall, Callie
GP IEEE
TI "Ocean Weather" in the Gulf of Mexico: Exploiting Real-Time Satellite
Ecological Properties and Circulation Models for Coastal Ocean
Monitoring
SO OCEANS 2009, VOLS 1-3
SE OCEANS-IEEE
LA English
DT Proceedings Paper
CT Oceans 2009 Conference
CY OCT 26-29, 2009
CL Biloxi, MS
SP Marine Technol Soc, IEEE Ocean Engn Soc
ID COLOR
AB The fusion of real-time remote sensing imagery with numerical ocean circulation models provides a unique capability for monitoring the coastal ocean. A real-time ocean monitoring system is currently operating in the Gulf of Mexico. Dynamic changes in the ocean environment occur on scales of hours, days, weeks and years, which influence biological, ecological and physical processes. By monitoring these processes at different spatial resolutions, new enhanced capability is available to coastal managers and researchers for making decisions.
Monitoring of physical processes and bio-optical responses are currently being done for the Gulf of Mexico. Open ocean eddies and loop current interact with coastal processes such as river plumes and tides and have significant impact on the biological and ecological processes along our shores. Until now we had no capability to routinely monitor these ocean conditions without insitu sensors and observations. Now the "weather" in the Gulf of Mexico is being monitored daily and provides coastal managers and researchers an edge in tracking or pin-pointing events. This information assists the decision maker in identifying how physical events are influencing the coastal ecosystem.
How is this being done? Improved bio-optical algorithms have been developed and applied to ocean color satellite imagery from NASA's Moderate Resolution Imaging Spectroradiometer (MOD'S) providing estimates of water constituents such as absorption properties from phytoplankton, color dissolved organic matter (CDOM), and detritus and backscattering properties related to sediment concentration. In addition, advances in numerical circulation modeling (Navy Coastal Ocean Model - NCOM) provide nowcasts and forecasts of coastal processes (currents, sea surface height, salinity and temperature). Physical ocean properties of temperature, salinity, and currents from NCOM are combined with daily latest pixel composite products of phytoplankton, CDOM, and detritus absorption, backscattering and sea surface temperature (SST). We demonstrate an advanced environmental monitoring capability available operationally that highlights the fusion of physical (model) and bio-optical properties (satellite).
The entire Gulf conditions are demonstrated daily in addition to higher resolution monitoring of coastal conditions. We will focus on Mississippi and Louisiana Coast using high resolution (250 meter resolution) MODIS imagery. We will demonstrate a capability of supporting coastal manager's and researchers integrating satellite bio-optical products, model circulation (current vectors), sea surface height (contours), salinity (contours) and temperature (contours) layers into Google Earth. In addition, we will demonstrate promising new research using satellite optics and numerical models to create surface optical forecast (hourly increments up to 48 hours) and a 3-D optical volume of the ocean derived from a physical (model) / optical (satellite) Gaussian relationship optimized using insitu profiles. By using these methods of fusing the satellite and ocean circulation model it will provide coastal zone managers with a new capability to assess, predict and track Harmful Algal Blooms, Hypoxia, and sediment discharge.
C1 [Ladner, Sherwin; Casey, Brandon] QinetiQ North Amer, Bldg 1009,Room 127A, Stennis Space Ctr, MS 39529 USA.
[Arnone, Robert; Sandidge, Juanita; Ko, DongShan] US Navy, Res Lab, Stennis Space Ctr, MS 39529 USA.
[Hall, Callie] NASA, Stennis Space Ctr, MS 39529 USA.
RP Ladner, S (reprint author), QinetiQ North Amer, Bldg 1009,Room 127A, Stennis Space Ctr, MS 39529 USA.
FU NOAA NCDDC; NOAA NOS; NOAA NESDIS; NASA Research; Applications Solution
Network (REASoN) [CAN-020ES-01]
FX The authors would like to thank NOAA NCDDC, NOAA NOS, and NOAA NESDIS
for all of their support during this project. Funding for this project
was provided by the NASA Research, Education, and Applications Solution
Network (REASoN) CAN-020ES-01.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0197-7385
BN 978-1-4244-4960-6
J9 OCEANS-IEEE
PY 2009
BP 2540
EP +
PG 2
WC Engineering, Ocean; Oceanography; Remote Sensing
SC Engineering; Oceanography; Remote Sensing
GA BPY34
UT WOS:000280322601101
ER
PT S
AU Dennis, SM
AF Dennis, Steven M.
GP IEEE
TI Coverage Metric for Acoustic Receiver Evaluation and Track Generation
SO OCEANS 2009, VOLS 1-3
SE OCEANS-IEEE
LA English
DT Proceedings Paper
CT Oceans 2009 Conference
CY OCT 26-29, 2009
CL Biloxi, MS
SP Marine Technol Soc, IEEE Ocean Engn Soc
AB Acoustic receiver track generation has been the subject of active research, both academic and operational, since at least 1946. In general, track generation algorithms operate by maximizing some measure of effectiveness or performance for a particular receiver in a particular environment. Current probability-based receiver performance measures are difficult to visualize, time consuming to calculate and are not easily subject to strict scientific analysis. Although great strides have been made in the ability to model and predict oceanography (temperature, salinity, currents, etc.) accurately, there exists the need to develop measures of receiver performance which more readily lend themselves to analysis of sensitivity to environmental variation or uncertainty.
With the increasing dependence on optimization algorithms in acoustic receiver placement and track generation in the presence of variable or uncertain environments, the desire for a more environmentally-sensitive metric of acoustic receiver performance has arisen. A measure of performance based upon acoustic coverage area has shown promise as a basis for acoustic receiver utilization and optimized track generation applications and is presented here. Coverage can be defined as the areas throughout which a receiver has a sufficiently high signal-to-noise ratio or, alternatively, probability of making positive observations. For the purposes of determining optimal receiver placement and track generation the area of interest is divided into a sufficiently sampled grid of calculation points. Computing and compiling acoustic receiver coverage area information for grid points throughout the area of interest into an acoustic receiver coverage map gives immediate visual feedback on locations of optimal performance for a specific acoustic receiver in use in the current ocean environment. By making use of multiple calculation layers in an N x 2-D fashion, acoustic coverage volumes can be constructed for the purposes of three dimensional receiver placement or track generation. The use of an acoustic coverage-based metric for optimal track generation is shown to compare favorably with current track optimizers which use cumulative probability measures of performance, offering faster calculation times and a stronger connection to the acoustic environment.
C1 USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
RP Dennis, SM (reprint author), USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0197-7385
BN 978-1-4244-4960-6
J9 OCEANS-IEEE
PY 2009
BP 2716
EP 2719
PG 4
WC Engineering, Ocean; Oceanography; Remote Sensing
SC Engineering; Oceanography; Remote Sensing
GA BPY34
UT WOS:000280322601126
ER
PT B
AU Jones, JA
Chao, Y
AF Jones, Jack A.
Chao, Yi
GP ASME
TI OFFSHORE HYDROKINETIC ENERGY CONVERSION FOR ONSHORE POWER GENERATION
SO OMAE 2009, VOL 4, PTS A AND B
LA English
DT Proceedings Paper
CT 28th International Conference on Ocean, Offshore and Arctic Engineering
CY MAY 31-JUN 05, 2009
CL Honolulu, HI
SP ASME, Ocean, Offshore & Arctic Engn Div
AB Design comparisons have been performed for a number of different tidal energy systems, including a fully submerged, horizontal-axis electro-turbine system, similar to Verdant Tidal Turbines in New York's East River, a platform-based Marine Current Turbine, now operating in Northern Ireland's Strangford Narrows, and the Rotech Lunar Energy system, to be installed off the South Korean Coast. A fourth type of tidal energy system studied is a novel JPL/Caltech hydraulic energy transfer system that uses submerged turbine blades which are mechanically attached to adjacent high-pressure pumps, instead of to adjacent electrical turbines. The generated high-pressure water streams are combined and transferred to an onshore hydroelectric plant by means of a closed-cycle pipeline. The hydraulic energy transfer system was found to be cost competitive, and it allows all electronics to be placed onshore, thus greatly reducing maintenance costs and corrosion problems. It also eliminates the expenses of conditioning and transferring multiple offshore power lines and of building offshore platforms embedded in the sea floor.
For time-dependent tidal energy, the pressurized hydraulic energy can be stored in an elevated onshore reservoir that can be used as per consumer energy demand, rather than as per tidal energy supply. This technology is a spinoff of a miniature ocean hydraulic energy transfer system that JPL is developing for the Office of Naval Research (ONR). The ONR device uses ocean temperature differences to provide pressurized hydraulic energy which supplies all electrical power for small submersibles. This type of hydraulic energy device is expected to allow submersibles to stay submerged for years. A three-month ocean endurance test is scheduled for late 2009.
Similar types of hydraulic energy transfer systems are potentially applicable to all types of hydrokinetic energy, including free-flowing rivers, ocean wave energy, and energy from ocean currents, such as the Gulf Stream. In each case, the corrosion-prone, submerged electrical turbines are replaced by all-mechanical water pumps without any electrical components, and the energy is hydraulically transferred to remote onshore hydroelectric plants by inexpensive pipes.
The submerged mechanical turbine blade/pump assemblies can be attached by long, small-diameter, flexible pressurized lines to the larger submerged, stationary pipe lines, thus allowing the submerged blade/pump assemblies to be lifted to the surface and serviced by boat. Check valves in the flexible lines allow damaged turbine blade/pump assemblies to be automatically taken off-line and later repaired or replaced as required.
C1 [Jones, Jack A.] CALTECH, Jet Prop Lab, Mech Syst Div, Pasadena, CA 91125 USA.
RP Jones, JA (reprint author), CALTECH, Jet Prop Lab, Mech Syst Div, Pasadena, CA 91125 USA.
NR 16
TC 0
Z9 0
U1 0
U2 11
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4344-4
PY 2009
BP 993
EP 1002
PG 10
WC Engineering, Ocean; Engineering, Mechanical
SC Engineering
GA BTB79
UT WOS:000286404300114
ER
PT B
AU VanZwieten, TS
VanZwieten, JH
Balas, MJ
Driscoll, FR
AF VanZwieten, Tannen S.
VanZwieten, James H.
Balas, Mark J.
Driscoll, Frederick R.
GP ASME
TI DIRECT ADAPTIVE REJECTION OF VORTEX-INDUCED DISTURBANCES FOR A POWERED
SPAR PLATFORM
SO OMAE 2009, VOL 5
LA English
DT Proceedings Paper
CT 28th International Conference on Ocean, Offshore and Arctic Engineering
CY MAY 31-JUN 05, 2009
CL Honolulu, HI
SP ASME, Ocean, Offshore & Arctic Engn Div
ID INDUCED VIBRATIONS
AB The Rapidly Deployable Stable Platform (RDSP) is a novel vessel designed to be a reconfigurable, stable at-sea platform. It consists of a detachable catamaran and spar, performing missions with the spar extending vertically below the catamaran and hoisting it completely out of the water. Multiple thrusters located along the spar allow it to be actively controlled in this configuration. A controller is presented in this work that uses an adaptive feedback algorithm in conjunction with Direct Adaptive Disturbance Rejection (DADR) to mitigate persistent, vortex-induced disturbances. Given the frequency of a disturbance, the nominal DADR scheme adaptively compensates for its unknown amplitude and phase. This algorithm is extended to adapt to a disturbance frequency that is only coarsely known by including a Phase Locked Loop (PLL). The PLL improves the frequency estimate on-line, allowing the modified controller to reduce vortex-induced motions by more than 95% using achievable thrust in-puts.
C1 [VanZwieten, Tannen S.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP VanZwieten, JH (reprint author), Florida Atlantic Univ, Dept Ocean Engn, Dania, FL 33004 USA.
EM tannen.s.vanzwieten@nasa.gov; jvanzwi@fau.edu; mbalas@uwyo.edu;
rdriscol@fau.edu
NR 36
TC 0
Z9 0
U1 1
U2 1
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4345-1
PY 2009
BP 487
EP 497
PG 11
WC Engineering, Marine; Engineering, Ocean
SC Engineering
GA BRL02
UT WOS:000282991700053
ER
PT S
AU Ansari, RR
Jones, JA
Pollonini, L
Rodriguez, M
Opperman, R
Hochstein, J
AF Ansari, Rafat R.
Jones, Jeffrey A.
Pollonini, Luca
Rodriguez, Mikael
Opperman, Roedolph
Hochstein, Jason
BE Cote, GL
TI A Non-Invasive Miniaturized-Wireless Laser-Doppler Fiber-Optic Sensor
for Understanding Distal Fingertip Injuries in Astronauts
SO OPTICAL DIAGNOSTICS AND SENSING IX
SE Proceedings of SPIE-The International Society for Optical Engineering
LA English
DT Proceedings Paper
CT Conference on Optical Diagnostics and Sensing IX
CY JAN 26-27, 2009
CL San Jose, CA
SP SPIE
AB During extra-vehicular activities (EVAs) or space walks astronauts over use their fingertips under pressure inside the confined spaces of gloves/space-suite. The repetitive hand motion is a probable cause for discomfort and injuries to the finger-tips. We describe a new wireless fiber-optic probe that can be integrated inside the astronaut glove for non-invasive blood perfusion measurements in distal finger tips. In this preliminary study, we present blood perfusion measurements while performing hand-grip exercises simulating the use of space tools.
C1 [Ansari, Rafat R.] NASA, Glenn Res Ctr, Cleveland, OH 44035 USA.
RP Ansari, RR (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44035 USA.
EM Rafat.R.Ansari@nasa.gov
RI Pollonini, Luca/J-9274-2014
OI Pollonini, Luca/0000-0003-2955-6355
NR 8
TC 0
Z9 0
U1 0
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7432-2
J9 P SOC PHOTO-OPT INS
PY 2009
VL 7186
AR 718609
DI 10.1117/12.809054
PG 9
WC Engineering, Biomedical; Remote Sensing; Optics
SC Engineering; Remote Sensing; Optics
GA BSS56
UT WOS:000285712100004
ER
PT S
AU Elsner, RF
O'Dell, SL
Ramsey, BD
Weisskopf, MC
AF Elsner, Ronald F.
O'Dell, Stephen L.
Ramsey, Brian D.
Weisskopf, Martin C.
BE O'Dell, SL
Pareschi, G
TI On the design of wide-field x-ray telescopes
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy IV
CY AUG 04-06, 2009
CL San Diego, CA
SP SPIE
DE X-ray astronomy; X-ray optics; ray trace; wide field-of-view
optimization
ID GRAZING-INCIDENCE OPTICS; OPTIMIZATION
AB X-ray telescopes having a relatively wide field-of-view and spatial resolution vs. polar off-axis angle curves much flatter than the parabolic dependence characteristic of Wolter I designs are of great interest for surveys of the X-ray sky and potentially for study of the Sun's X-ray emission. We discuss the various considerations affecting the design of such telescopes, including the possible use of polynomial mirror surface prescriptions, a method of optimizing the polynomial coefficients, scaling laws for mirror segment length vs. intersection radius, the loss of on-axis spatial resolution, and the positioning of focal plane detectors.
C1 [Elsner, Ronald F.; O'Dell, Stephen L.; Ramsey, Brian D.; Weisskopf, Martin C.] NASA Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
RP Elsner, RF (reprint author), NASA Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA.
EM ron.elsner@nasa.gov; steve.o'dell@nasa.gov; brian.ramsey@nasa.gov;
martin@smoker.msfc.nasa.gov; steve.o'dell@nasa.gov
NR 9
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7727-9
J9 PROC SPIE
PY 2009
VL 7437
AR 74370F
DI 10.1117/12.831262
PG 12
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BRX37
UT WOS:000283842600013
ER
PT S
AU Gubarev, MV
O'Dell, SL
Jones, WD
Kester, TJ
Griffith, CW
Zhang, WW
Saha, TT
Chan, KW
AF Gubarev, Mikhail V.
O'Dell, Stephen L.
Jones, William D.
Kester, Thomas J.
Griffith, Charles W.
Zhang, William W.
Saha, Timo T.
Chan, Kai-Wing
BE O'Dell, SL
Pareschi, G
TI A stainless-steel mandrel for slumping glass x-ray mirrors
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy IV
CY AUG 04-06, 2009
CL San Diego, CA
SP SPIE
DE mandrel fabrication; stainless-steel mandrels; metrology; x-ray mirrors;
thermal forming
ID OPTICS; MSFC
AB We have fabricated a precision full-cylinder stainless-steel mandrel at NASA Marshall Space Flight Center. The mandrel is figured for a 30-cm-diameter primary (paraboloid) mirror of an 840-cm focal-length Wolter-1 telescope. We have developed this mandrel for experiments in slumping-thermal forming at about 600 degrees C-of glass mirror segments at NASA Goddard Space Flight Center, in support of NASA's participation in the International X-ray Observatory (IXO). Precision turning of stainless-steel mandrels may offer a low-cost alternative to conventional figuring of fused-silica or other glassy forming mandrels. We report on the fabrication, metrology, and performance of this first mandrel; then we discuss plans and goals for stainless-steel mandrel technology.
C1 [Gubarev, Mikhail V.] NASA Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
RP Gubarev, MV (reprint author), NASA Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA.
EM mikhail.v.gubarev@nasa.gov
OI O'Dell, Stephen/0000-0002-1868-8056
NR 24
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7727-9
J9 PROC SPIE
PY 2009
VL 7437
AR 74370Z
DI 10.1117/12.831260
PG 12
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BRX37
UT WOS:000283842600032
ER
PT S
AU Lehan, JP
Atanossova, M
Chan, KW
Hadjimichael, T
Saha, TT
Hong, M
Zhang, WW
Blake, P
AF Lehan, J. P.
Atanossova, M.
Chan, K. -W.
Hadjimichael, T.
Saha, T. T.
Hong, M.
Zhang, W. W.
Blake, P.
BE O'Dell, SL
Pareschi, G
TI Progress toward a complete metrology set for the International X-ray
Observatory (IXO) soft x-ray mirrors
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy IV
CY AUG 04-06, 2009
CL San Diego, CA
SP SPIE
DE Optical metrology; x-ray optics; IXO
AB We present an overview update of the metrologic approach to be employed for the segmented mirror fabrication for the IXO soft x-ray telescope. We compare results achieved to date with mission requirements. This is discussed in terms of inherent capability versus in-practice capability of the metrology. We find that all the needed metrology equipment are in hand but that a number of the needed quantities remain too uncertain relative to mission requirements. This is driven by the mounting of the mirrors themselves. We then discuss some plans for addressing the mirror mounting issues. Finally, we also briefly discuss some promising mandrel metrology techniques.
C1 [Lehan, J. P.; Chan, K. -W.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA.
RP Lehan, JP (reprint author), NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
NR 11
TC 1
Z9 1
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7727-9
J9 PROC SPIE
PY 2009
VL 7437
AR 74370R
DI 10.1117/12.826625
PG 9
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BRX37
UT WOS:000283842600024
ER
PT S
AU Zhang, WW
AF Zhang, William W.
BE O'Dell, SL
Pareschi, G
TI Manufacture of Mirror Glass Substrates for The NUSTAR Mission
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy IV
CY AUG 04-06, 2009
CL San Diego, CA
SP SPIE
DE X-ray optics; lightweight optics; NuSTAR; Glass Slumping
AB The NuSTAR (Nuclear Spectroscopy Telescope Array) observatory (Harrison et al. 2009), expected to be launched into an equatorial low earth orbit in 2011, will have two mirror assemblies capable of imaging X-rays in the hard X-ray band between 5 keV and 80 keV. It will be the first X-ray observatory using multilayer coatings to significantly expand the bandwidth of the typical X-ray telescope of 0.1 keV to 10 keV. The mirror assemblies use a segmented design to simplify the construction process, as such they require 4,680 mirror substrates coated with appropriately designed multilayers to enhance reflectivity for hard X-rays. These substrates are produced by slumping commercially available thin glass sheets. In this paper we report on our work of manufacturing these substrates at NASA Goddard Space Flight Center.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhang, WW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 4
TC 13
Z9 13
U1 1
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7727-9
J9 PROC SPIE
PY 2009
VL 7437
AR 74370N
DI 10.1117/12.830225
PG 11
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BRX37
UT WOS:000283842600021
ER
PT S
AU Gizon, L
Schunker, H
Baldner, CS
Basu, S
Birch, AC
Bogart, RS
Braun, DC
Cameron, R
Duvall, TL
Hanasoge, SM
Jackiewicz, J
Roth, M
Stahn, T
Thompson, MJ
Zharkov, S
AF Gizon, L.
Schunker, H.
Baldner, C. S.
Basu, S.
Birch, A. C.
Bogart, R. S.
Braun, D. C.
Cameron, R.
Duvall, T. L., Jr.
Hanasoge, S. M.
Jackiewicz, J.
Roth, M.
Stahn, T.
Thompson, M. J.
Zharkov, S.
BE Thompson, MJ
Balogh, A
Culhane, JL
Nordlund, A
Solanki, SK
Zahn, JP
TI Helioseismology of Sunspots: A Case Study of NOAA Region 9787
SO ORIGIN AND DYNAMICS OF SOLAR MAGNETISM
SE Space Science Series of ISSI
LA English
DT Article; Book Chapter
DE Sun; Sunspots; Helioseismology
ID TIME-DISTANCE HELIOSEISMOLOGY; RING-DIAGRAM ANALYSIS; SOLAR ACTIVE
REGIONS; MODE TRAVEL-TIMES; LOCAL HELIOSEISMOLOGY; WAVE-PROPAGATION;
SOUND SPEED; P-MODES; FLOWS; INVERSION
AB Various methods of helioseismology are used to study the subsurface properties of the Sunspot in NOAA Active Region 9787. This sunspot was chosen because it is axisymmetric, shows little evolution during 20-28 January 2002, and was observed continuously by the MDI/SOHO instrument. AR 9787 is visible on helioseismic maps of the farside of the Sun from 15 January, i.e. days before it crossed the East limb.
Oscillations have reduced amplitudes in the sunspot at all frequencies, whereas a region of enhanced acoustic power above 5.5 mHz (above the quiet-Sun acoustic cutoff) is seen outside the sunspot and the plage region. This enhanced acoustic power has been Suggested to be caused by the conversion of acoustic waves into magneto-acoustic waves that are refracted back into the interior and re-emerge as acoustic waves in the quiet Sun. Observations show that the sunspot absorbs a significant fraction of the incoming p and f modes around 3 mHz. A numerical simulation of MHD wave propagation through a simple model of AR 9787 confirmed that wave absorption is likely to be due to the partial conversion of incoming waves into magneto-acoustic waves that propagate down the sunspot.
Wave travel times and mode frequencies are affected by the sunspot. In most cases, wave packets that propagate through the sunspot have reduced travel times. At short travel distances, however, the sign of the travel-time shifts appears to depend sensitively on how the data are processed and, in particular, on filtering in frequency-wavenumber space. We carry out two linear inversions for wave speed: one using travel-times and phase-speed filters and the other one using mode frequencies from ring analysis. These two inversions give subsurface wave-speed profiles with opposite signs and different amplitudes.
The travel-time measurements also imply different subsurface flow patterns in the surface layer depending on the filtering procedure that is used. Current sensitivity kernels are unable to reconcile these measurements, perhaps because they rely on imperfect models of the power spectrum of solar oscillations. We present a linear inversion for flows of ridge-filtered travel times. This inversion shows a horizontal outflow in the upper 4 Mill that is consistent with the moat flow deduced from the surface motion of moving magnetic features.
From this study of AR 9787, we conclude that we are currently unable to provide a unified description of the subsurface structure and dynamics of the sunspot.
C1 [Gizon, L.; Schunker, H.; Cameron, R.; Jackiewicz, J.; Roth, M.; Stahn, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Baldner, C. S.; Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Birch, A. C.; Braun, D. C.] Colorado Res Associates, Boulder, CO 80301 USA.
[Bogart, R. S.; Hanasoge, S. M.] Stanford Univ, Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Lab Solar Phys, Greenbelt, MD 20771 USA.
[Thompson, M. J.; Zharkov, S.] Univ Sheffield, Sch Math & Stat, Sheffield S3 7RH, S Yorkshire, England.
RP Gizon, L (reprint author), Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
EM gizon@mps.mpg.de
RI Basu, Sarbani/B-8015-2014
OI Basu, Sarbani/0000-0002-6163-3472
NR 65
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 1385-7525
BN 978-1-4419-0238-2
J9 SPACE SCI SER ISSI
PY 2009
VL 32
BP 249
EP 273
DI 10.1007/978-1-4419-0239-9_15
D2 10.1007/978-1-4419-0239-9
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BKH57
UT WOS:000268118700015
ER
PT S
AU Hathaway, DH
AF Hathaway, David H.
BE Thompson, MJ
Balogh, A
Culhane, JL
Nordlund, A
Solanki, SK
Zahn, JP
TI Solar Cycle Forecasting
SO ORIGIN AND DYNAMICS OF SOLAR MAGNETISM
SE Space Science Series of ISSI
LA English
DT Article; Book Chapter
DE Solar activity; Sunspot cycle; Solar cycle forecasting
ID FLUX; AMPLITUDE; DYNAMO; MINIMUM; MODELS; FIELD; SIZE
AB Predicting the behavior of a solar cycle after it is well underway (2-3 years after minimum) can be done with a fair degree of skill using auto-regression and curve fitting techniques that don't require any knowledge of the physics involved. Predicting the amplitude of a solar cycle near, or before, the time of solar cycle minimum can be done using precursors such as geomagnetic activity and polar fields that do have some connection to the physics but the connections are uncertain and the precursors provide less reliable forecasts. Predictions for the amplitude of cycle 24 using these precursor techniques give drastically different values. Recently, dynamo models have been used directly with assimilated data to predict the amplitude of sunspot cycle 24 but have also given significantly different predictions. While others have questioned both the predictability of the solar cycle and the ability of current dynamo models to provide predictions, it is clear that cycle 24 will help to discriminate between some opposing dynamo models.
C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM David.Hathaway@nasa.gov
NR 35
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 1385-7525
BN 978-1-4419-0238-2
J9 SPACE SCI SER ISSI
PY 2009
VL 32
BP 401
EP 412
DI 10.1007/978-1-4419-0239-9_20
D2 10.1007/978-1-4419-0239-9
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BKH57
UT WOS:000268118700020
ER
PT S
AU Lawson, PW
AF Lawson, Peter W.
BE Knudsen, EE
Michael, JH
TI What Are We Missing? Butterflies, Flowers, and Salmon Models
SO PACIFIC SALMON ENVIRONMENTAL AND LIFE HISTORY MODELS: ADVANCING SCIENCE
FOR SUSTAINABLE SALMON IN THE FUTURE
SE American Fisheries Society Symposium
LA English
DT Proceedings Paper
CT Symposium on Pacific Salmon Environmental and Life History Models
CY SEP 13-14, 2005
CL Anchorage, AK
SP Amer Fisheries Soc
ID NORTHEAST PACIFIC; SURVIVAL RATES; DYNAMICS; OREGON; PATTERNS
AB We understand our environment through our senses and tend to interpret the behavior of other animals in the context of the world we understand. Butterflies and flowers sometimes show distinctive patterns in ultraviolet light that are important to them but invisible to us. Likewise, the senses of fish and their experience of the world are very different from ours. Many aspects of a salmon's environment, such as olfactory stimuli, are completely invisible to us. Other factors, like certain aspects of habitat alteration, are visible but unnoticed because they occurred gradually or long ago. Like Poe's purloined letter they are cryptic-there for us to see if we only knew what to look for. As we build salmon models we base them on what we understand is important to the fish. However, our anthropocentric bias may cause us to overlook or misinterpret factors of importance. In addition, our necessarily simplified models, when applied to management, may result in a pernicious simplification of the salmon populations we wish to preserve. For example, if we model and manage for a dominant (or highly visible or easily monitored) salmon life history we may inadvertently eliminate other life histories of equal importance, or reduce diversity in ways that affect population viability. We should actively seek to identify important factors missing from our models and be aware of critical assumptions. Recognizing that our models are tools used to understand and manage salmon, we should try to understand the broader implications of these models to the future of the salmon we hope to preserve. In this essay, I offer speculation about what we may be missing in freshwater habitat, life history diversity, metapopulation dynamics, ocean survival, and water chemistry. I also consider the question of scale, and the effect our philosophical viewpoint may have on the direction and application of our modeling efforts and the likelihood of successful outcomes.
C1 Natl Marine Fisheries Serv, Newport Res Stn, Newport, OR 97365 USA.
RP Lawson, PW (reprint author), Natl Marine Fisheries Serv, Newport Res Stn, 2032 SE OSU Dr, Newport, OR 97365 USA.
EM peter.w.lawson@noaa.gov
NR 25
TC 1
Z9 1
U1 1
U2 1
PU AMER FISHERIES SOC
PI BETHESDA
PA 5410 GROSVENOR LANE, STE 110, BETHESDA, MD 20814-2199 USA
SN 0892-2284
BN 978-1-934874-09-7
J9 AM FISH S S
PY 2009
VL 71
BP 33
EP 44
PG 12
WC Fisheries
SC Fisheries
GA BLY21
UT WOS:000271411600003
ER
PT S
AU Munoz-Mari, J
Plaza, AJ
Gualtieri, JA
Camps-Valls, G
AF Munoz-Mari, Jordi
Plaza, Antonio J.
Gualtieri, J. Anthony
Camps-Valls, Gustavo
BE Xhafa, F
TI Parallel Implementations of SVM for Earth Observation
SO PARALLEL PROGRAMMING, MODELS AND APPLICATIONS IN GRID AND P2P SYSTEMS
SE Advances in Parallel Computing
LA English
DT Article; Book Chapter
DE Parallel processing; image classification; remote sensing; support
vector machine; multispectral; hyperspectral; kernel methods
ID HYPERSPECTRAL IMAGE CLASSIFICATION; SUPPORT VECTOR MACHINES; CLUSTER;
WORKSTATIONS; OPTIMIZATION; ALGORITHMS; NETWORKS
AB Imaging spectroscopy, also known as hyperspectral remote sensing, is concerned with the measurement, analysis, and interpretation of spectra acquired from a given scene (or specific object) at a short, medium or long distance by an airborne or satellite sensor. Analysis in a timely manner of the acquired multidimensional images allows to develop applications with high social impact, such as urban growing monitoring, crop fields identification, target detection for military and defense/security deployment, wildland fire detection and monitoring, biological threat detection, biophysical parameter estimation, or monitoring of oil spills and other types of chemical contamination.
In this context, support vector machines (SVM) [1, 2, 3] have become one of the state-of-the-art machine learning tools for hyperspectral image classification. However, its high computational cost for large scale applications makes the use of SVM limited to off-line processing scenarios. Certainly, with the recent explosion in the amount and complexity of hyperspectral data, parallel processing has soon become a requirement in many remote sensing missions, especially with the advent of low-cost systems such as commodity clusters and distributed networks of computers In order to address this relevant issue, this chapter explores the development of two parallel versions of SVMs for remote sensing image classification.
Sequential minimal optimization is a very popular algorithm for training SVMs, but it still requires a large amount of computation time for solving large size problems. In this work, we evaluate the performance of a parallel implementation of the SVM based on the parallelization of the incomplete Cholesky factorization and present novel parallel implementations that balance the load across the available processors through standard Master-Worker decompositions. Both methodologies are theoretically analyzed in terms of scalability, computational efficiency and time response. The impact of the multi-class scheme is also analyzed. Results on real multispectral and hyperspectral datasets illustrate the performance of the methods. We finally discuss the possibility of obtaining processing results quickly enough for practical use via the Marenostrum supercomputer available at the Barcelona Supercomputing Center in Spain, and other massively parallel facilities at NASA's Goddard Space Flight Center in Maryland.
C1 [Munoz-Mari, Jordi; Camps-Valls, Gustavo] Univ Valencia, IPL, Dept Elect Engn, E-46003 Valencia, Spain.
[Plaza, Antonio J.] Univ Extremadura, Dept Comp Sci, Caceres, Spain.
[Gualtieri, J. Anthony] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Munoz-Mari, J (reprint author), Univ Valencia, IPL, Dept Elect Engn, E-46003 Valencia, Spain.
EM jordi@uv.es; aplaza@unex.es; Anthony.Gualtieri@gst.com; gcamps@uv.es
OI Munoz-Mari, Jordi/0000-0002-3014-3921; Plaza,
Antonio/0000-0002-9613-1659
NR 60
TC 8
Z9 8
U1 0
U2 2
PU IOS PRESS
PI AMSTERDAM
PA NIEUWE HEMWEG 6B, 1013 BG AMSTERDAM, NETHERLANDS
SN 0927-5452
BN 978-1-60750-004-9
J9 ADV PARALLEL COMPUT
PY 2009
VL 17
BP 292
EP 312
DI 10.3233/978-1-60750-004-9-292
PG 21
WC Computer Science, Hardware & Architecture
SC Computer Science
GA BMB00
UT WOS:000271713700012
ER
PT J
AU Watson, AB
Ahumada, AJ
AF Watson, A. B.
Ahumada, A. J., Jr.
TI The image-based acuity model: A general model for image recognition
SO PERCEPTION
LA English
DT Meeting Abstract
C1 [Watson, A. B.; Ahumada, A. J., Jr.] NASA, Human Syst Integrat Div, Ames Res Ctr, Washington, DC USA.
EM andrew.b.watson@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 1
PU PION LTD
PI LONDON
PA 207 BRONDESBURY PARK, LONDON NW2 5JN, ENGLAND
SN 0301-0066
J9 PERCEPTION
JI Perception
PY 2009
VL 38
SU S
BP 60
EP 61
PG 2
WC Ophthalmology; Psychology; Psychology, Experimental
SC Ophthalmology; Psychology
GA V16YN
UT WOS:000207905000196
ER
PT J
AU Mortensen, DH
Bech, S
Begault, DR
Adelstein, BD
AF Mortensen, Ditte H.
Bech, Soren
Begault, Durand R.
Adelstein, Bernard D.
TI The relative importance of visual, auditory, and haptic information for
the user's experience of mechanical switches
SO PERCEPTION
LA English
DT Article
ID FEEDBACK; ILLUSIONS; TACTILE
AB While the use of hand tools and other everyday manually controlled devices is naturally accompanied by multisensory feedback, the deployment of fully multimodal virtual interfaces requires that haptic, acoustic, and visual cues be synthesised. The complexity and character of this synthesis will depend on a thorough understanding of the multimodal perceptual experience, including the interrelations between the individual sensory channels during manual interaction. In this study seventy participants were asked to rank the manual operation of ten electromechanical switches according to preference. The participants were randomly assigned in groups of ten to one of seven sensory presentation conditions. These conditions comprised six bit-nodal and unimodal sensory combinations created by selectively restricting the flow of haptic, auditory, and visual information, plus one condition in which ful sensory information was available. A principal components analysis on the obtained ranking data indicated that the sensory conditions with unimpeded haptic information were clearly distinct from those in which the haptic cues were impeded. The analysis also showed that, for switch use, the unimodal haptic condition most closely approached the condition with combined haptic, auditory, and visual feedback, compared with all of the conditions where haptic feedback was restricted.
C1 [Mortensen, Ditte H.; Bech, Soren] Bang & Olufsen As, Struer, Denmark.
[Begault, Durand R.; Adelstein, Bernard D.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
RP Mortensen, DH (reprint author), Bang & Olufsen As, Peter Bangs Vej 15, Struer, Denmark.
EM dhm@bang-olufsen.dk
RI Bech, Soren/L-4070-2015
OI Bech, Soren/0000-0002-0924-1914
NR 23
TC 1
Z9 1
U1 3
U2 7
PU PION LTD
PI LONDON
PA 207 BRONDESBURY PARK, LONDON NW2 5JN, ENGLAND
SN 0301-0066
J9 PERCEPTION
JI Perception
PY 2009
VL 38
IS 10
BP 1560
EP 1571
DI 10.1068/p5929
PG 12
WC Ophthalmology; Psychology; Psychology, Experimental
SC Ophthalmology; Psychology
GA 533WC
UT WOS:000272855100011
PM 19950486
ER
PT B
AU Tunstel, E
Dolan, JM
Fong, T
Schreckenghost, D
AF Tunstel, Edward
Dolan, John M.
Fong, Terrence
Schreckenghost, Debra
BE Madhavan, R
Tubstel, E
Messina, E
TI Mobile Robotic Surveying Performance for Planetary Surface Site
Characterization
SO PERFORMANCE EVALUATION AND BENCHMARKING OF INTELLIGENT SYSTEMS
LA English
DT Proceedings Paper
CT Workshop on Performance Metrics for Intelligent Systems (PerMIS 08)
CY AUG 19-21, 2008
CL Natl Inst Stand, Gaithersburg, MD
HO Natl Inst Stand
AB Robotic systems will perform mobile surveys for scientific and engineering purposes as part of future missions on lunar and planetary surfaces. With site characterization as a task objective various system configurations and surveying techniques are possible. This chapter describes several examples of mobile surveying approaches using local and remote sensing configurations. A geometric measure of area coverage performance is applied to each and relative performance in surveying a common area is characterized by expected performance trends. Performance metrics that solely express geometric aspects of the robotic task are limited in utility as decision aids to human mission operators. As such, the importance of enriching such metrics by incorporating additional attributes germane to surveying on planetary surfaces is highlighted. Examples of enriched metrics employed by recent NASA research work on human-supervised robotic surveying are provided.
C1 [Tunstel, Edward] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Johns Hopkins Rd, Laurel, MD 20723 USA.
[Dolan, John M.] Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA.
[Fong, Terrence] NASA Ames Res Ctr, Intelligent Robot Grp, Moffett Field, CA 94035 USA.
[Schreckenghost, Debra] TRACLabs Inc, Webster, NY USA.
RP Tunstel, E (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM edward.tunstel@jhuapl.edu; jmd@cs.cmu.edu; terry.fong@nasa.gov;
schreck@traclabs.com
FU NASA Astrobiology Science and Technology Instrument Development; NASA
Exploration Systems Technology Development Program under the
"Human-Robotic Systems" NASA Small Business Innovative Research(SBIR)
program; NASA Small Business Innovative Research(SBIR)
FX We thank Hans Utz, Tod Milam, David Lees, and Matt Deans for assisting
with the development and implementation of real-time robot performance
monitoring. This work was partially supported by the NASA Astrobiology
Science and Technology Instrument Development program, the NASA
Exploration Systems Technology Development Program under the
Human-Robotic Systems project and the NASA Small Business Innovative
Research(SBIR) program.
NR 23
TC 0
Z9 0
U1 0
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-1-4419-0491-1
PY 2009
BP 249
EP +
DI 10.1007/978-1-4419-0492-8_11
PG 3
WC Computer Science, Artificial Intelligence
SC Computer Science
GA BMM54
UT WOS:000272813500011
ER
PT S
AU Peterson, N
Anusuya-Rangappa, L
Shirazi, BA
Song, WZ
Huang, RJ
Tran, D
Chien, S
LaHusen, R
AF Peterson, Nina
Anusuya-Rangappa, Lohith
Shirazi, Behrooz A.
Song, WenZhan
Huang, Renjie
Tran, Daniel
Chien, Steve
LaHusen, Rick
BE Hassanien, AE
Abawajy, JH
Abraham, A
Hagras, H
TI Volcano Monitoring: A Case Study in Pervasive Computing
SO PERVASIVE COMPUTING: INNOVATIONS IN INTELLIGENT MULTIMEDIA AND
APPLICATIONS
SE Computer Communications and Networks Series
LA English
DT Article; Book Chapter
DE Wireless sensor networks; Pervasive computing; Environment monitoring;
Quality of service; Situation awareness
AB Recent advances in wireless sensor network technology have provided robust and reliable solutions for sophisticated pervasive computing applications such as inhospitable terrain environmental monitoring. We present a case study for developing a real-time pervasive computing system, called OASIS for optimized autonomous space in situ sensor-web, which combines ground assets (a sensor network) and space assets (NASA's earth observing (EO-1) satellite) to monitor volcanic activities at Mount St. Helens. OASIS's primary goals are: to integrate complementary space and in situ ground sensors into an interactive and autonomous sensorweb, to optimize power and communication resource management of the sensorweb and to provide mechanisms for seamless and scalable fusion of future space and in situ components. The OASIS in situ ground sensor network development addresses issues related to power management, bandwidth management, quality of service management, topology and routing management, and test-bed design. The space segment development consists of EO-1 architectural enhancements, feedback of EO-1 data into the in situ component, command and control integration, data ingestion and dissemination and field demonstrations.
C1 [Peterson, Nina; Anusuya-Rangappa, Lohith; Shirazi, Behrooz A.; Huang, Renjie] Washington State Univ, Sch Elect Engn & Comp Sci, Pullman, WA 99163 USA.
[LaHusen, Rick] USGS Cascades Volcano Observ, Vancouver, WA 98660 USA.
[Tran, Daniel; Chien, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Song, WenZhan] Washington State Univ, Sch Elect Engn & Comp Sci, Vancouver, WA 98686 USA.
RP Peterson, N (reprint author), Washington State Univ, Sch Elect Engn & Comp Sci, Pullman, WA 99163 USA.
EM npicone@eecs.wsu.edu
NR 29
TC 4
Z9 4
U1 0
U2 1
PU SPRINGER-VERLAG LONDON LTD
PI GODALMING
PA SWEETAPPLE HOUSE CATTESHALL RD FARNCOMBE, GODALMING GU7 1NH, SURREY,
ENGLAND
SN 1617-7975
BN 978-1-84882-598-7
J9 COMPUT COMMUN NETW S
PY 2009
BP 201
EP 230
DI 10.1007/978-1-84882-599-4_10
PG 30
WC Computer Science, Artificial Intelligence; Computer Science, Hardware &
Architecture
SC Computer Science
GA BLT76
UT WOS:000270992400010
ER
PT J
AU Pissulla, D
Seckmeyer, G
Cordero, RR
Blumthaler, M
Schallhart, B
Webb, A
Kift, R
Smedley, A
Bais, AF
Kouremeti, N
Cede, A
Herman, J
Kowalewskig, M
AF Pissulla, D.
Seckmeyer, G.
Cordero, R. R.
Blumthaler, M.
Schallhart, B.
Webb, A.
Kift, R.
Smedley, A.
Bais, A. F.
Kouremeti, N.
Cede, A.
Herman, J.
Kowalewskig, M.
TI Comparison of atmospheric spectral radiance measurements from five
independently calibrated systems
SO PHOTOCHEMICAL & PHOTOBIOLOGICAL SCIENCES
LA English
DT Article
ID SKY RADIANCE; IRRADIANCE; SPECTRORADIOMETERS; SENSITIVITY; UNCERTAINTY;
ULTRAVIOLET
AB A variety of instruments have been developed over the past 50 years to measure spectral radiance in absolute units at UV and visible wavelengths with high spectral resolution. While there is considerable experience in the measurement of spectral irradiance, less emphasis has been given to the reliable measurement of spectral radiance from ground observations. We discuss the methodology and calibration procedures for five instruments capable of making such measurements. Four of these instruments are based on double monochromators that scan each wavelength in turn, and one is based on a single monochromator with a charged coupled device (CCD) allowing the recording of all wavelengths simultaneously. The measured spectral radiance deviates between 3% and about 35% depending on the instruments. The results are compared with radiative transfer calculations when the aerosol characteristics of the atmosphere are known.
C1 [Pissulla, D.; Seckmeyer, G.] Leibniz Univ Hannover, Inst Meteorol & Climatol, Hannover, Germany.
[Cordero, R. R.] Univ Tecn Feder Santa Maria, Valparaiso, Chile.
[Cordero, R. R.] Univ Santiago Chile, Santiago, Chile.
[Blumthaler, M.; Schallhart, B.] Innsbruck Med Univ, Div Biomed Phys, Innsbruck, Austria.
[Blumthaler, M.; Schallhart, B.] Univ Manchester, Sch Earth Atmospher & Environm Sci, Manchester M13 9PL, Lancs, England.
[Bais, A. F.; Kouremeti, N.] Aristotle Univ Thessaloniki, Lab Atmospher Phys, Thessaloniki, Greece.
[Cede, A.; Herman, J.; Kowalewskig, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Pissulla, D (reprint author), Leibniz Univ Hannover, Inst Meteorol & Climatol, Hannover, Germany.
EM Pissulla@muk.uni-hannover.de
RI Bais, Alkiviadis/D-2230-2009; Smedley, Andrew/N-9865-2014;
OI Bais, Alkiviadis/0000-0003-3899-2001; Smedley,
Andrew/0000-0001-7137-6628; Herman, Jay/0000-0002-9146-1632; Kift,
Richard/0000-0003-1826-3653
FU WMO
FX Part of this study has been conducted in the framework of the EC
Integrated Project SCOUT-O3 (contract 505390-GOCE-CT2004). We would like
to thank WMO for providing financial support to groups taking part in
the Izana campaign. Furthermore, we are indebted to the director of the
Izana Observatory, Dr Emilio Cuevas for providing the facilities to host
the campaign and to Alberto Redondas for his continuous support during
the campaign.
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PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 1474-905X
EI 1474-9092
J9 PHOTOCH PHOTOBIO SCI
JI Photochem. Photobiol. Sci.
PY 2009
VL 8
IS 4
BP 516
EP 527
DI 10.1039/b817018e
PG 12
WC Biochemistry & Molecular Biology; Biophysics; Chemistry, Physical
SC Biochemistry & Molecular Biology; Biophysics; Chemistry
GA 426ZI
UT WOS:000264747000012
PM 19337666
ER
PT J
AU Boykin, TB
Kharche, N
Klimeck, G
AF Boykin, Timothy B.
Kharche, Neerav
Klimeck, Gerhard
TI Non-primitive rectangular cells for tight-binding electronic structure
calculations
SO PHYSICA E-LOW-DIMENSIONAL SYSTEMS & NANOSTRUCTURES
LA English
DT Article
DE Brillouin zone; Allowed wavevectors; Zone unfolding
AB Rectangular non-primitive unit cells are computationally convenient for use in nanodevice electronic structure and transport calculations. When these cells are used for Calculations of structures with periodicity, the resulting bands are zone-folded and must be unfolded in order to identify important gaps and masses. Before the zone-unfolding method can be applied, one must first determine the allowed wavevectors for the specific non-primitive cell. Because most computationally convenient non-primitive cells do not have axes parallel to the primitive cell direct lattice vectors, finding the allowed wavevectors is generally a non-trivial task. (Solid state texts generally treat only the simplest case in which the non-primitive and primitive cell axes are all aligned.) Rectangular non-primitive cells with one axis aligned along a specific direction are especially useful for obtaining the approximate random-alloy bands for a bulk crystal, a critical verification step in any randorn-alloy nanostructure calculation. Here, we present an easily implemented method for determining a non-primitive rectangular cell for the FCC lattice with an axis aligned in a desired direction and the associated allowed primitive cell wavevectors. We illustrate its use by unfolding the bands of Ge. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Boykin, Timothy B.] Univ Alabama, Dept Elect & Comp Engn, Huntsville, AL 35899 USA.
[Kharche, Neerav; Klimeck, Gerhard] Purdue Univ, Network Computat Nanotechnol, Sch Elect & Comp Engn, W Lafayette, IN 47907 USA.
[Klimeck, Gerhard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Boykin, TB (reprint author), Univ Alabama, Dept Elect & Comp Engn, Huntsville, AL 35899 USA.
EM boykin@ece.uah.edu
RI Kharche, Neerav/F-4331-2015; Klimeck, Gerhard/A-1414-2012
OI Kharche, Neerav/0000-0003-1014-6022; Klimeck,
Gerhard/0000-0001-7128-773X
FU Semiconductor Research Corporation; National Science Foundation
FX This work was supported by Semiconductor Research Corporation. The work
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, and jet
Propulsion Laboratory. nanohub.org Computational resources provided by
the Network for Computational Nanotechnology, funded by the National
Science Foundation were used.
NR 14
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U1 0
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1386-9477
J9 PHYSICA E
JI Physica E
PD JAN
PY 2009
VL 41
IS 3
BP 490
EP 494
DI 10.1016/j.physe.2008.09.022
PG 5
WC Nanoscience & Nanotechnology; Physics, Condensed Matter
SC Science & Technology - Other Topics; Physics
GA 402LR
UT WOS:000263015700032
ER
PT J
AU Shaw, MD
Schneiderman, JF
Bueno, J
Palmer, BS
Delsing, P
Echternach, PM
AF Shaw, M. D.
Schneiderman, J. F.
Bueno, J.
Palmer, B. S.
Delsing, P.
Echternach, P. M.
TI Characterization of an entangled system of two superconducting qubits
using a multiplexed capacitance measurement
SO PHYSICAL REVIEW B
LA English
DT Article
DE capacitors; Cooper pairs; ground states; information theory; quantum
computing; quantum entanglement
ID CHARGE QUBITS; QUANTUM STATE; CAVITY
AB We characterize a pair of Cooper-pair boxes coupled with a fixed capacitor using spectroscopy and measurements of the ground-state quantum capacitance. We use the extracted parameters to estimate the concurrence or degree of entanglement between the two qubits. We also present a thorough demonstration of a multiplexed quantum capacitance measurement technique, which is in principle scalable to a large array of superconducting qubits.
C1 [Shaw, M. D.; Schneiderman, J. F.; Echternach, P. M.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
[Schneiderman, J. F.; Delsing, P.] Chalmers, S-41296 Gothenburg, Sweden.
[Bueno, J.; Delsing, P.; Echternach, P. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Palmer, B. S.] Lab Phys Sci, College Pk, MD 20740 USA.
RP Shaw, MD (reprint author), Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
RI Delsing, Per/F-7288-2010; Schneiderman, Justin/D-4508-2013
OI Delsing, Per/0000-0002-1222-3506; Schneiderman,
Justin/0000-0002-4441-2360
FU National Security Agency; NASA; University of Southern California
College of Arts and Sciences
FX We would like to thank Richard Muller for performing the electron-beam
lithography. This work was conducted at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration (NASA), and was funded by a grant
from the National Security Agency. J.B. acknowledges support from NASA.
M. S. acknowledges support from the University of Southern California
College of Arts and Sciences.
NR 25
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PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1098-0121
EI 1550-235X
J9 PHYS REV B
JI Phys. Rev. B
PD JAN
PY 2009
VL 79
IS 1
AR 014516
DI 10.1103/PhysRevB.79.014516
PG 8
WC Physics, Condensed Matter
SC Physics
GA 401XX
UT WOS:000262977900104
ER
PT J
AU Abbott, B
Abbott, R
Adhikari, R
Ajith, P
Allen, B
Allen, G
Amin, R
Anderson, DP
Anderson, SB
Anderson, WG
Arain, MA
Araya, M
Armandula, H
Armor, P
Aso, Y
Aston, S
Aufmuth, P
Aulbert, C
Babak, S
Ballmer, S
Bantilan, H
Barish, BC
Barker, C
Barker, D
Barr, B
Barriga, P
Barton, MA
Bastarrika, M
Bayer, K
Betzwieser, J
Beyersdorf, PT
Bilenko, IA
Billingsley, G
Biswas, R
Black, E
Blackburn, K
Blackburn, L
Blair, D
Bland, B
Bodiya, TP
Bogue, L
Bork, R
Boschi, V
Bose, S
Brady, PR
Braginsky, VB
Brau, JE
Brinkmann, M
Brooks, A
Brown, DA
Brunet, G
Bullington, A
Buonanno, A
Burmeister, O
Byer, RL
Cadonati, L
Cagnoli, G
Camp, JB
Cannizzo, J
Cannon, K
Cao, J
Cardenas, L
Casebolt, T
Castaldi, G
Cepeda, C
Chalkley, E
Charlton, P
Chatterji, S
Chelkowski, S
Chen, Y
Christensen, N
Clark, D
Clark, J
Cokelaer, T
Conte, R
Cook, D
Corbitt, T
Coyne, D
Creighton, JDE
Creighton, TD
Cumming, A
Cunningham, L
Cutler, RM
Dalrymple, J
Danzmann, K
Davies, G
DeBra, D
Degallaix, J
Degree, M
Dergachev, V
Desai, S
DeSalvo, R
Dhurandhar, S
Diaz, M
Dickson, J
Dietz, A
Donovan, F
Dooley, KL
Doomes, EE
Drever, RWP
Duke, I
Dumas, JC
Dupuis, RJ
Dwyer, JG
Echols, C
Effler, A
Ehrens, P
Ely, G
Espinoza, E
Etzel, T
Evans, T
Fairhurst, S
Fan, Y
Fazi, D
Fehrmann, H
Fejer, MM
Finn, LS
Flasch, K
Fotopoulos, N
Freise, A
Frey, R
Fricke, T
Fritschel, P
Frolov, VV
Fyffe, M
Garofoli, J
Gholami, I
Giaime, JA
Giampanis, S
Giardina, KD
Goda, K
Goetz, E
Goggin, L
Gonzalez, G
Gossler, S
Gouaty, R
Grant, A
Gras, S
Gray, C
Gray, M
Greenhalgh, RJS
Gretarsson, AM
Grimaldi, F
Grosso, R
Grote, H
Grunewald, S
Guenther, M
Gustafson, EK
Gustafson, R
Hage, B
Hallam, JM
Hammer, D
Hanna, C
Hanson, J
Harms, J
Harry, G
Harstad, E
Hayama, K
Hayler, T
Heefner, J
Heng, IS
Hennessy, M
Heptonstall, A
Hewitson, M
Hild, S
Hirose, E
Hoak, D
Hosken, D
Hough, J
Huttner, SH
Ingram, D
Ito, M
Ivanov, A
Johnson, B
Johnson, WW
Jones, DI
Jones, G
Jones, R
Ju, L
Kalmus, P
Kalogera, V
Kamat, S
Kanner, J
Kasprzyk, D
Katsavounidis, E
Kawabe, K
Kawamura, S
Kawazoe, F
Kells, W
Keppel, DG
Khalili, FY
Khan, R
Khazanov, E
Kim, C
King, P
Kissel, JS
Klimenko, S
Kokeyama, K
Kondrashov, V
Kopparapu, RK
Kozak, D
Kozhevatov, I
Krishnan, B
Kwee, P
Lam, PK
Landry, M
Lang, MM
Lantz, B
Lazzarini, A
Lei, M
Leindecker, N
Leonhardt, V
Leonor, I
Libbrecht, K
Lin, H
Lindquist, P
Lockerbie, NA
Lodhia, D
Lormand, M
Lu, P
Lubinski, M
Lucianetti, A
Luck, H
Machenschalk, B
MacInnis, M
Mageswaran, M
Mailand, K
Mandic, V
Marka, S
Marka, Z
Markosyan, A
Markowitz, J
Maros, E
Martin, I
Martin, RM
Marx, JN
Mason, K
Matichard, F
Matone, L
Matzner, R
Mavalvala, N
McCarthy, R
McClelland, DE
McGuire, SC
McHugh, M
McIntyre, G
McIvor, G
McKechan, D
McKenzie, K
Meier, T
Melissinos, A
Mendell, G
Mercer, RA
Meshkov, S
Messenger, CJ
Meyers, D
Miller, J
Minelli, J
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Miyakawa, O
Moe, B
Mohanty, S
Moreno, G
Mossavi, K
MowLowry, C
Mueller, G
Mukherjee, S
Mukhopadhyay, H
Muller-Ebhardt, H
Munch, J
Murray, P
Myers, E
Myers, J
Nash, T
Nelson, J
Newton, G
Nishizawa, A
Numata, K
O'Dell, J
Ogin, G
O'Reilly, B
O'Shaughnessy, R
Ottaway, DJ
Ottens, RS
Overmier, H
Owen, BJ
Pan, Y
Pankow, C
Papa, MA
Parameshwaraiah, V
Patel, P
Pedraza, M
Penn, S
Perreca, A
Petrie, T
Pinto, IM
Pitkin, M
Pletsch, HJ
Plissi, MV
Postiglione, F
Principe, M
Prix, R
Quetschke, V
Raab, F
Rabeling, DS
Radkins, H
Rainer, N
Rakhmanov, M
Ramsunder, M
Rehbein, H
Reid, S
Reitze, DH
Riesen, R
Riles, K
Rivera, B
Robertson, NA
Robinson, C
Robinson, EL
Roddy, S
Rodriguez, A
Rogan, AM
Rollins, J
Romano, JD
Romie, J
Route, R
Rowan, S
Rudiger, A
Ruet, L
Russell, P
Ryan, K
Sakata, S
Samidi, M
de la Jordana, LS
Sandberg, V
Sannibale, V
Saraf, S
Sarin, P
Sathyaprakash, BS
Sato, S
Saulson, PR
Savage, R
Savov, P
Schediwy, SW
Schilling, R
Schnabel, R
Schofield, R
Schutz, BF
Schwinberg, P
Scott, SM
Searle, AC
Sears, B
Seifert, F
Sellers, D
Sengupta, AS
Shawhan, P
Shoemaker, DH
Sibley, A
Siemens, X
Sigg, D
Sinha, S
Sintes, AM
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Smith, ND
Somiya, K
Sorazu, B
Stein, LC
Stochino, A
Stone, R
Strain, KA
Strom, DM
Stuver, A
Summerscales, TZ
Sun, KX
Sung, M
Sutton, PJ
Takahashi, H
Tanner, DB
Taylor, R
Taylor, R
Thacker, J
Thorne, KA
Thorne, KS
Thuring, A
Tokmakov, KV
Torres, C
Torrie, C
Traylor, G
Trias, M
Tyler, W
Ugolini, D
Ulmen, J
Urbanek, K
Vahlbruch, H
Van Den Broeck, C
van der Sluys, M
Vass, S
Vaulin, R
Vecchio, A
Veitch, J
Veitch, P
Vigeland, S
Villar, A
Vorvick, C
Vyachanin, SP
Waldman, SJ
Wallace, L
Ward, H
Ward, R
Weinert, M
Weinstein, A
Weiss, R
Wen, S
Wette, K
Whelan, JT
Whitbeck, DM
Whitcomb, SE
Whiting, BF
Wilkinson, C
Willems, PA
Williams, HR
Williams, L
Willke, B
Wilmut, I
Winkler, W
Wipf, CC
Wiseman, AG
Woan, G
Wooley, R
Worden, J
Wu, W
Yakushin, I
Yamamoto, H
Yan, Z
Yoshida, S
Zanolin, M
Zhang, J
Zhang, L
Zhao, C
Zotov, N
Zucker, M
Zweizig, J
AF Abbott, B.
Abbott, R.
Adhikari, R.
Ajith, P.
Allen, B.
Allen, G.
Amin, R.
Anderson, D. P.
Anderson, S. B.
Anderson, W. G.
Arain, M. A.
Araya, M.
Armandula, H.
Armor, P.
Aso, Y.
Aston, S.
Aufmuth, P.
Aulbert, C.
Babak, S.
Ballmer, S.
Bantilan, H.
Barish, B. C.
Barker, C.
Barker, D.
Barr, B.
Barriga, P.
Barton, M. A.
Bastarrika, M.
Bayer, K.
Betzwieser, J.
Beyersdorf, P. T.
Bilenko, I. A.
Billingsley, G.
Biswas, R.
Black, E.
Blackburn, K.
Blackburn, L.
Blair, D.
Bland, B.
Bodiya, T. P.
Bogue, L.
Bork, R.
Boschi, V.
Bose, S.
Brady, P. R.
Braginsky, V. B.
Brau, J. E.
Brinkmann, M.
Brooks, A.
Brown, D. A.
Brunet, G.
Bullington, A.
Buonanno, A.
Burmeister, O.
Byer, R. L.
Cadonati, L.
Cagnoli, G.
Camp, J. B.
Cannizzo, J.
Cannon, K.
Cao, J.
Cardenas, L.
Casebolt, T.
Castaldi, G.
Cepeda, C.
Chalkley, E.
Charlton, P.
Chatterji, S.
Chelkowski, S.
Chen, Y.
Christensen, N.
Clark, D.
Clark, J.
Cokelaer, T.
Conte, R.
Cook, D.
Corbitt, T.
Coyne, D.
Creighton, J. D. E.
Creighton, T. D.
Cumming, A.
Cunningham, L.
Cutler, R. M.
Dalrymple, J.
Danzmann, K.
Davies, G.
DeBra, D.
Degallaix, J.
Degree, M.
Dergachev, V.
Desai, S.
DeSalvo, R.
Dhurandhar, S.
Diaz, M.
Dickson, J.
Dietz, A.
Donovan, F.
Dooley, K. L.
Doomes, E. E.
Drever, R. W. P.
Duke, I.
Dumas, J.-C.
Dupuis, R. J.
Dwyer, J. G.
Echols, C.
Effler, A.
Ehrens, P.
Ely, G.
Espinoza, E.
Etzel, T.
Evans, T.
Fairhurst, S.
Fan, Y.
Fazi, D.
Fehrmann, H.
Fejer, M. M.
Finn, L. S.
Flasch, K.
Fotopoulos, N.
Freise, A.
Frey, R.
Fricke, T.
Fritschel, P.
Frolov, V. V.
Fyffe, M.
Garofoli, J.
Gholami, I.
Giaime, J. A.
Giampanis, S.
Giardina, K. D.
Goda, K.
Goetz, E.
Goggin, L.
Gonzalez, G.
Gossler, S.
Gouaty, R.
Grant, A.
Gras, S.
Gray, C.
Gray, M.
Greenhalgh, R. J. S.
Gretarsson, A. M.
Grimaldi, F.
Grosso, R.
Grote, H.
Grunewald, S.
Guenther, M.
Gustafson, E. K.
Gustafson, R.
Hage, B.
Hallam, J. M.
Hammer, D.
Hanna, C.
Hanson, J.
Harms, J.
Harry, G.
Harstad, E.
Hayama, K.
Hayler, T.
Heefner, J.
Heng, I. S.
Hennessy, M.
Heptonstall, A.
Hewitson, M.
Hild, S.
Hirose, E.
Hoak, D.
Hosken, D.
Hough, J.
Huttner, S. H.
Ingram, D.
Ito, M.
Ivanov, A.
Johnson, B.
Johnson, W. W.
Jones, D. I.
Jones, G.
Jones, R.
Ju, L.
Kalmus, P.
Kalogera, V.
Kamat, S.
Kanner, J.
Kasprzyk, D.
Katsavounidis, E.
Kawabe, K.
Kawamura, S.
Kawazoe, F.
Kells, W.
Keppel, D. G.
Khalili, F. Ya.
Khan, R.
Khazanov, E.
Kim, C.
King, P.
Kissel, J. S.
Klimenko, S.
Kokeyama, K.
Kondrashov, V.
Kopparapu, R. K.
Kozak, D.
Kozhevatov, I.
Krishnan, B.
Kwee, P.
Lam, P. K.
Landry, M.
Lang, M. M.
Lantz, B.
Lazzarini, A.
Lei, M.
Leindecker, N.
Leonhardt, V.
Leonor, I.
Libbrecht, K.
Lin, H.
Lindquist, P.
Lockerbie, N. A.
Lodhia, D.
Lormand, M.
Lu, P.
Lubinski, M.
Lucianetti, A.
Lueck, H.
Machenschalk, B.
MacInnis, M.
Mageswaran, M.
Mailand, K.
Mandic, V.
Marka, S.
Marka, Z.
Markosyan, A.
Markowitz, J.
Maros, E.
Martin, I.
Martin, R. M.
Marx, J. N.
Mason, K.
Matichard, F.
Matone, L.
Matzner, R.
Mavalvala, N.
McCarthy, R.
McClelland, D. E.
McGuire, S. C.
McHugh, M.
McIntyre, G.
McIvor, G.
McKechan, D.
McKenzie, K.
Meier, T.
Melissinos, A.
Mendell, G.
Mercer, R. A.
Meshkov, S.
Messenger, C. J.
Meyers, D.
Miller, J.
Minelli, J.
Mitra, S.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Miyakawa, O.
Moe, B.
Mohanty, S.
Moreno, G.
Mossavi, K.
MowLowry, C.
Mueller, G.
Mukherjee, S.
Mukhopadhyay, H.
Mueller-Ebhardt, H.
Munch, J.
Murray, P.
Myers, E.
Myers, J.
Nash, T.
Nelson, J.
Newton, G.
Nishizawa, A.
Numata, K.
O'Dell, J.
Ogin, G.
O'Reilly, B.
O'Shaughnessy, R.
Ottaway, D. J.
Ottens, R. S.
Overmier, H.
Owen, B. J.
Pan, Y.
Pankow, C.
Papa, M. A.
Parameshwaraiah, V.
Patel, P.
Pedraza, M.
Penn, S.
Perreca, A.
Petrie, T.
Pinto, I. M.
Pitkin, M.
Pletsch, H. J.
Plissi, M. V.
Postiglione, F.
Principe, M.
Prix, R.
Quetschke, V.
Raab, F.
Rabeling, D. S.
Radkins, H.
Rainer, N.
Rakhmanov, M.
Ramsunder, M.
Rehbein, H.
Reid, S.
Reitze, D. H.
Riesen, R.
Riles, K.
Rivera, B.
Robertson, N. A.
Robinson, C.
Robinson, E. L.
Roddy, S.
Rodriguez, A.
Rogan, A. M.
Rollins, J.
Romano, J. D.
Romie, J.
Route, R.
Rowan, S.
Ruediger, A.
Ruet, L.
Russell, P.
Ryan, K.
Sakata, S.
Samidi, M.
de la Jordana, L. Sancho
Sandberg, V.
Sannibale, V.
Saraf, S.
Sarin, P.
Sathyaprakash, B. S.
Sato, S.
Saulson, P. R.
Savage, R.
Savov, P.
Schediwy, S. W.
Schilling, R.
Schnabel, R.
Schofield, R.
Schutz, B. F.
Schwinberg, P.
Scott, S. M.
Searle, A. C.
Sears, B.
Seifert, F.
Sellers, D.
Sengupta, A. S.
Shawhan, P.
Shoemaker, D. H.
Sibley, A.
Siemens, X.
Sigg, D.
Sinha, S.
Sintes, A. M.
Slagmolen, B. J. J.
Slutsky, J.
Smith, J. R.
Smith, M. R.
Smith, N. D.
Somiya, K.
Sorazu, B.
Stein, L. C.
Stochino, A.
Stone, R.
Strain, K. A.
Strom, D. M.
Stuver, A.
Summerscales, T. Z.
Sun, K.-X.
Sung, M.
Sutton, P. J.
Takahashi, H.
Tanner, D. B.
Taylor, R.
Taylor, R.
Thacker, J.
Thorne, K. A.
Thorne, K. S.
Thuering, A.
Tokmakov, K. V.
Torres, C.
Torrie, C.
Traylor, G.
Trias, M.
Tyler, W.
Ugolini, D.
Ulmen, J.
Urbanek, K.
Vahlbruch, H.
Van Den Broeck, C.
van der Sluys, M.
Vass, S.
Vaulin, R.
Vecchio, A.
Veitch, J.
Veitch, P.
Vigeland, S.
Villar, A.
Vorvick, C.
Vyachanin, S. P.
Waldman, S. J.
Wallace, L.
Ward, H.
Ward, R.
Weinert, M.
Weinstein, A.
Weiss, R.
Wen, S.
Wette, K.
Whelan, J. T.
Whitbeck, D. M.
Whitcomb, S. E.
Whiting, B. F.
Wilkinson, C.
Willems, P. A.
Williams, H. R.
Williams, L.
Willke, B.
Wilmut, I.
Winkler, W.
Wipf, C. C.
Wiseman, A. G.
Woan, G.
Wooley, R.
Worden, J.
Wu, W.
Yakushin, I.
Yamamoto, H.
Yan, Z.
Yoshida, S.
Zanolin, M.
Zhang, J.
Zhang, L.
Zhao, C.
Zotov, N.
Zucker, M.
Zweizig, J.
CA LIGO Sci Collaboration
TI Einstein@Home search for periodic gravitational waves in LIGO S4 data
SO PHYSICAL REVIEW D
LA English
DT Article
ID PRECESSING NEUTRON-STARS; INSPIRALING BINARIES; RADIATION; TEMPLATES
AB A search for periodic gravitational waves, from sources such as isolated rapidly spinning neutron stars, was carried out using 510 h of data from the fourth LIGO science run (S4). The search was for quasimonochromatic waves in the frequency range from 50 to 1500 Hz, with a linear frequency drift f (measured at the solar system barycenter) in the range -f/tau < f < 0.1f/tau, where the minimum spin-down age tau was 1000 yr for signals below 300 Hz and 10 000 yr above 300 Hz. The main computational work of the search was distributed over approximately 100 000 computers volunteered by the general public. This large computing power allowed the use of a relatively long coherent integration time of 30 h, despite the large parameter space searched. No statistically significant signals were found. The sensitivity of the search is estimated, along with the fraction of parameter space that was vetoed because of contamination by instrumental artifacts. In the 100 to 200 Hz band, more than 90% of sources with dimensionless gravitational-wave strain amplitude greater than 10(-23) would have been detected.
C1 [Babak, S.; Chen, Y.; Degallaix, J.; Gholami, I.; Grunewald, S.; Krishnan, B.; Papa, M. A.; Schutz, B. F.; Sintes, A. M.; Somiya, K.; Takahashi, H.; Whelan, J. T.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Allen, B.; Aulbert, C.; Brinkmann, M.; Burmeister, O.; Danzmann, K.; Fehrmann, H.; Gossler, S.; Grote, H.; Harms, J.; Hewitson, M.; Lueck, H.; Machenschalk, B.; Messenger, C. J.; Mossavi, K.; Mueller-Ebhardt, H.; Pletsch, H. J.; Prix, R.; Rainer, N.; Rehbein, H.; Ruediger, A.; Schilling, R.; Schnabel, R.; Seifert, F.; Weinert, M.; Willke, B.; Winkler, W.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Dickson, J.; Gray, M.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; MowLowry, C.; Rabeling, D. S.; Searle, A. C.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Drever, R. W. P.] CALTECH, Pasadena, CA 91125 USA.
[Savov, P.; Thorne, K. S.] Caltech CaRT, Pasadena, CA 91125 USA.
[Cokelaer, T.; Davies, G.; Dietz, A.; Fairhurst, S.; Jones, G.; McKechan, D.; Robinson, C.; Sathyaprakash, B. S.; Sutton, P. J.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, Wales.
[Bantilan, H.; Christensen, N.; Ely, G.; Vigeland, S.] Carleton Coll, Northfield, MN 55057 USA.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Aso, Y.; Dwyer, J. G.; Kalmus, P.; Kamat, S.; Khan, R.; Marka, S.; Marka, Z.; Matone, L.; Rollins, J.] Columbia Univ, New York, NY 10027 USA.
[Gretarsson, A. M.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Khazanov, E.; Kozhevatov, I.] Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Dhurandhar, S.; Mitra, S.; Mukhopadhyay, H.] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Aufmuth, P.; Danzmann, K.; Hage, B.; Kwee, P.; Lueck, H.; Meier, T.; Thuering, A.; Vahlbruch, H.; Willke, B.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Abbott, B.; Abbott, R.; Adhikari, R.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, K.; Bork, R.; Boschi, V.; Brooks, A.; Cannon, K.; Cardenas, L.; Cepeda, C.; Chatterji, S.; Coyne, D.; DeSalvo, R.; Dupuis, R. J.; Echols, C.; Ehrens, P.; Espinoza, E.; Etzel, T.; Fazi, D.; Fricke, T.; Goggin, L.; Gustafson, E. K.; Heefner, J.; Ivanov, A.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Libbrecht, K.; Lindquist, P.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Meyers, D.; Miller, J.; Miyakawa, O.; Nash, T.; Ogin, G.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Samidi, M.; Sannibale, V.; Sears, B.; Sengupta, A. S.; Smith, M. R.; Stochino, A.; Taylor, R.; Tyler, W.; Vass, S.; Villar, A.; Waldman, S. J.; Wallace, L.; Ward, R.; Weinstein, A.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Bayer, K.; Blackburn, L.; Bodiya, T. P.; Brunet, G.; Cao, J.; Corbitt, T.; Donovan, F.; Duke, I.; Fritschel, P.; Goda, K.; Grimaldi, F.; Harry, G.; Katsavounidis, E.; MacInnis, M.; Markowitz, J.; Mason, K.; Mavalvala, N.; Mittleman, R.; Ottaway, D. J.; Ruet, L.; Sarin, P.; Shoemaker, D. H.; Smith, N. D.; Stein, L. C.; Weiss, R.; Wipf, C. C.; Zucker, M.] MIT, LIGO, Cambridge, MA 02139 USA.
[Barker, C.; Barker, D.; Bland, B.; Cook, D.; Effler, A.; Garofoli, J.; Gray, C.; Guenther, M.; Ingram, D.; Johnson, B.; Kawabe, K.; Landry, M.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moreno, G.; Myers, E.; Myers, J.; Parameshwaraiah, V.; Raab, F.; Radkins, H.; Rivera, B.; Ryan, K.; Sandberg, V.; Savage, R.; Schwinberg, P.; Sigg, D.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99325 USA.
[Bogue, L.; Evans, T.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Hoak, D.; Lormand, M.; O'Reilly, B.; Overmier, H.; Riesen, R.; Roddy, S.; Romie, J.; Sellers, D.; Sibley, A.; Stuver, A.; Thacker, J.; Torres, C.; Wooley, R.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA.
[Amin, R.; Giaime, J. A.; Gonzalez, G.; Gouaty, R.; Hanna, C.; Johnson, W. W.; Kissel, J. S.; Matichard, F.; Rodriguez, A.; Slutsky, J.; Sung, M.; Wen, S.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[McHugh, M.] Loyola Univ, New Orleans, LA 70118 USA.
[Bilenko, I. A.; Braginsky, V. B.; Khalili, F. Ya.; Mitrofanov, V. P.; Vyachanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia.
[Camp, J. B.; Cannizzo, J.; Numata, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kawamura, S.; Kawazoe, F.; Kokeyama, K.; Leonhardt, V.; Nishizawa, A.; Sakata, S.; Sato, S.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Kalogera, V.; Kim, C.; van der Sluys, M.] Northwestern Univ, Evanston, IL 60208 USA.
[Greenhalgh, R. J. S.; Hayler, T.; O'Dell, J.; Wilmut, I.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Beyersdorf, P. T.] San Jose State Univ, San Jose, CA 95192 USA.
[Saraf, S.] Sonoma State Univ, Rohnert Pk, CA 94928 USA.
[Rakhmanov, M.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Doomes, E. E.; McGuire, S. C.] So Univ & A& M Coll, Baton Rouge, LA 70813 USA.
[Allen, G.; Bullington, A.; Byer, R. L.; Casebolt, T.; Clark, D.; DeBra, D.; Degree, M.; Fejer, M. M.; Hennessy, M.; Lantz, B.; Leindecker, N.; Lu, P.; Markosyan, A.; Route, R.; Sinha, S.; Sun, K.-X.; Ulmen, J.; Urbanek, K.] Stanford Univ, Stanford, CA 94305 USA.
[Brown, D. A.; Dalrymple, J.; Hirose, E.; Saulson, P. R.; Smith, J. R.] Syracuse Univ, Syracuse, NY 13244 USA.
[Desai, S.; Finn, L. S.; Kopparapu, R. K.; Lang, M. M.; Minelli, J.; O'Shaughnessy, R.; Owen, B. J.; Petrie, T.; Ramsunder, M.; Thorne, K. A.; Whitbeck, D. M.; Williams, H. R.] Penn State Univ, University Pk, PA 16802 USA.
[Matzner, R.; McIvor, G.] Univ Texas Austin, Austin, TX 78712 USA.
[Creighton, T. D.; Diaz, M.; Grosso, R.; Hayama, K.; Mohanty, S.; Mukherjee, S.; Romano, J. D.; Stone, R.] Univ Texas Brownsville & Texas Southmost Coll, Brownsville, TX 78520 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[de la Jordana, L. Sancho; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain.
[Hosken, D.; Munch, J.; Veitch, P.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Aston, S.; Chelkowski, S.; Cutler, R. M.; Freise, A.; Hallam, J. M.; Hild, S.; Kasprzyk, D.; Lodhia, D.; Perreca, A.; Robinson, E. L.; Vecchio, A.; Veitch, J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Anderson, D. P.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Arain, M. A.; Dooley, K. L.; Klimenko, S.; Lin, H.; Lucianetti, A.; Martin, R. M.; Mercer, R. A.; Mitselmakher, G.; Mueller, G.; Ottens, R. S.; Pankow, C.; Quetschke, V.; Reitze, D. H.; Tanner, D. B.; Whiting, B. F.; Williams, L.; Wu, W.] Univ Florida, Gainesville, FL 32611 USA.
[Barr, B.; Barton, M. A.; Bastarrika, M.; Cagnoli, G.; Chalkley, E.; Clark, J.; Cumming, A.; Cunningham, L.; Grant, A.; Heng, I. S.; Heptonstall, A.; Hough, J.; Huttner, S. H.; Jones, R.; Martin, I.; Miller, J.; Murray, P.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Sorazu, B.; Strain, K. A.; Taylor, R.; Tokmakov, K. V.; Torrie, C.; Traylor, G.; Ward, H.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland.
[Buonanno, A.; Kanner, J.; Pan, Y.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA.
[Cadonati, L.] Univ Massachusetts, Amherst, MA 01003 USA.
[Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.; Zhang, J.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Brau, J. E.; Frey, R.; Harstad, E.; Ito, M.; Leonor, I.; Schofield, R.; Strom, D. M.] Univ Oregon, Eugene, OR 97403 USA.
[Mandic, V.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Fricke, T.; Giampanis, S.; Melissinos, A.] Univ Rochester, Rochester, NY 14627 USA.
[Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Fisciano, Salerno, Italy.
[Castaldi, G.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland.
[Barriga, P.; Blair, D.; Dumas, J.-C.; Fan, Y.; Gras, S.; Ju, L.; Schediwy, S. W.; Yan, Z.; Zhao, C.] Univ Western Australia, Nedlands, WA 6009, Australia.
[Allen, B.; Anderson, W. G.; Armor, P.; Biswas, R.; Brady, P. R.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Hammer, D.; Moe, B.; Papa, M. A.; Siemens, X.; Vaulin, R.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Bose, S.; Rogan, A. M.] Washington State Univ, Pullman, WA 99164 USA.
RP Abbott, B (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
RI Biswas, Rahul/H-7474-2016; Khalili, Farit/D-8113-2012; Vecchio,
Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Khan,
Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Postiglione,
Fabio/O-4744-2015; Sigg, Daniel/I-4308-2015; Pinto,
Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Frey,
Raymond/E-2830-2016; Ward, Robert/I-8032-2014; Finn, Lee
Samuel/A-3452-2009; Mitrofanov, Valery/D-8501-2012; Bilenko,
Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013;
Barker, David/A-5671-2013; Fricke, Thomas/B-6885-2013; Zhao,
Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Pitkin, Matthew/I-3802-2013;
Vyatchanin, Sergey/J-2238-2012; Khazanov, Efim/B-6643-2014; Lucianetti,
Antonio/G-7383-2014; Martin, Iain/A-2445-2010; Hild, Stefan/A-3864-2010;
Schutz, Bernard/B-1504-2010; Rowan, Sheila/E-3032-2010; Strain,
Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Lueck,
Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Freise,
Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Barriga,
Pablo/A-3929-2008; Lam, Ping Koy/A-5276-2008; McClelland,
David/E-6765-2010
OI Nishizawa, Atsushi/0000-0003-3562-0990; Zweizig,
John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517;
Freise, Andreas/0000-0001-6586-9901; Whiting, Bernard
F/0000-0002-8501-8669; Principe, Maria/0000-0002-6327-0628; Kanner,
Jonah/0000-0001-8115-0577; Whelan, John/0000-0001-5710-6576; Fairhurst,
Stephen/0000-0001-8480-1961; Boschi, Valerio/0000-0001-8665-2293;
Matichard, Fabrice/0000-0001-8982-8418; Pinto, Innocenzo
M./0000-0002-2679-4457; Minelli, Jeff/0000-0002-5330-912X; Hallam,
Jonathan Mark/0000-0002-7087-0461; Biswas, Rahul/0000-0002-0774-8906;
Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735;
Vecchio, Alberto/0000-0002-6254-1617; Khan, Rubab/0000-0001-5100-5168;
Postiglione, Fabio/0000-0003-0628-3796; Sigg,
Daniel/0000-0003-4606-6526; Frey, Raymond/0000-0003-0341-2636; Stein,
Leo/0000-0001-7559-9597; Ward, Robert/0000-0001-5503-5241; Finn, Lee
Samuel/0000-0002-3937-0688; Allen, Bruce/0000-0003-4285-6256; Zhao,
Chunnong/0000-0001-5825-2401; Pitkin, Matthew/0000-0003-4548-526X;
Strain, Kenneth/0000-0002-2066-5355; Lueck, Harald/0000-0001-9350-4846;
Lam, Ping Koy/0000-0002-4421-601X; McClelland, David/0000-0001-6210-5842
NR 48
TC 56
Z9 56
U1 2
U2 12
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 JAN
PY 2009
VL 79
IS 2
AR 022001
DI 10.1103/PhysRevD.79.022001
PG 29
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 401YK
UT WOS:000262979800005
ER
PT J
AU Abers, ES
Bhatia, AK
Dicus, DA
Repko, WW
Rosenbaum, DC
Teplitz, VL
AF Abers, E. S.
Bhatia, A. K.
Dicus, D. A.
Repko, W. W.
Rosenbaum, D. C.
Teplitz, V. L.
TI Charges on strange quark nuggets in space
SO PHYSICAL REVIEW D
LA English
DT Article
ID COLOR SUPERCONDUCTIVITY; E(+)E(-) EMISSION; MATTER SURFACES; STARS;
NUCLEARITES; RADIATION
AB Since Witten's seminal 1984 paper on the subject, searches for evidence of strange quark nuggets (SQNs) have proven unsuccessful. In the absence of experimental evidence ruling out SQNs, the validity of theories introducing mechanisms that increase their stability should continue to be tested. To stimulate electromagnetic SQN searches, particularly space searches, we estimate the net charge that would develop on a SQN in space exposed to various radiation baths (and showers) capable of liberating the SQN's less strongly bound electrons, taking into account recombination with ambient electrons. We consider, in particular, the cosmic microwave background, radiation from the sun, and diffuse galactic and extragalactic ultraviolet backgrounds. The largest charge, for the settings considered, develops on a solar system SQN exposed to a solar X-ray flare. A possible dramatic signal of SQNs in explosive astrophysical events is noted.
C1 [Abers, E. S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Bhatia, A. K.; Teplitz, V. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dicus, D. A.] Univ Texas Austin, Dept Phys, Austin, TX 78712 USA.
[Repko, W. W.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Rosenbaum, D. C.; Teplitz, V. L.] So Methodist Univ, Dept Phys, Dallas, TX 75275 USA.
RP Abers, ES (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
FU U. S. Department of Energy [DE-FG03-93ER40757]; National Science
Foundation [PHY-0555544]
FX L. T. very much appreciates a number of very helpful conversations with
Demos Kazanas, one with Floyd Stecker on Ref. [ 23] and one with M.
Alford on the effects of Cooper pairing. Dr. Alford kindly provided a
number of very helpful comments on the first version of this paper. D.
C. R. and V. L. T. are also grateful to Jonathan Gardner for calling
SN-2006gy to our attention, as well as C. Kilbourne for talking WHIM
with us. D. A. D. was supported in part by the U. S. Department of
Energy under Grant No. DE-FG03-93ER40757. W. W. R. was supported in part
by the National Science Foundation under Grant PHY-0555544.
NR 54
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U1 0
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PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD JAN
PY 2009
VL 79
IS 2
AR 023513
DI 10.1103/PhysRevD.79.023513
PG 11
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 401YK
UT WOS:000262979800023
ER
PT J
AU Mikellides, IG
AF Mikellides, Ioannis G.
TI Effects of viscosity in a partially ionized channel flow with thermionic
emission
SO PHYSICS OF PLASMAS
LA English
DT Article
DE channel flow; plasma collision processes; plasma flow; plasma
simulation; thermionic emission; viscosity
ID HOLLOW-CATHODE; MODEL
AB The flow of the partially ionized gas inside thermionic hollow cathodes spans a diverse range of theoretical disciplines in plasma physics and fluid mechanics. Understanding and predicting the evolution of such flows has many practical implications because hollow cathodes are critical components of electric propulsion systems used onboard scientific and commercial spacecraft presently in space or in the mission planning stages. As space missions become more demanding of the propulsion system in terms of throughput, understanding and predicting failure mechanisms of the system becomes imperative. Two-dimensional numerical simulations of the partially ionized gas generated by a thermionic hollow cathode have been performed to quantify the effects of viscosity inside the cylindrical channel of the device. A comparison of the inviscid and fully viscous flow fields shows that viscosity has a significant impact on the atomic species and a lesser effect on the ions. The internal pressure is determined to be more than 40% higher compared to the inviscid solution and the Reynolds number for the flow of atoms is found to be less than 20 inside the channel. Although the Mach number is computed to be < 0.1 for approximately 95% of the channel, the solution for the velocity flow field begins to deviate from the Poiseuille (parabolic) solution at about 50% of the channel due mainly to collisional drag with ions.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mikellides, IG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 23
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U1 2
U2 6
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD JAN
PY 2009
VL 16
IS 1
AR 013501
DI 10.1063/1.3056397
PG 10
WC Physics, Fluids & Plasmas
SC Physics
GA 401UM
UT WOS:000262967900035
ER
PT S
AU Lansbergen, GP
Rahman, R
Caro, J
Collaert, N
Biesemans, S
Klimeck, G
Hollenberg, LCL
Rogge, S
AF Lansbergen, G. P.
Rahman, R.
Caro, J.
Collaert, N.
Biesemans, S.
Klimeck, G.
Hollenberg, L. C. L.
Rogge, S.
BE Caldas, MJ
Studart, N
TI +Level Spectrum Of Single Gated As Donors
SO PHYSICS OF SEMICONDUCTORS
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 29th International Conference on Physics of Semiconductors
CY JUL 27-AUG 01, 2008
CL Rio de Janeiro, BRAZIL
DE Single donors; FinFET; Transport spectroscopy
ID SILICON; STATE
AB We study the electrical transport through single As donors incorporated in the channel of a FinFET, i.e. a donor in a three-terminal geometry. By means of spectroscopic measurements in conjuction with a NEMO-3D model, we can identify the excited states and associate them with either the donors Coulomb potential, a triangular well at the interface or a hybridized combination of the two. The correspondence between the transport measurements, the theoretical model and the local environment provides an atomic understanding of actual gated donors in a nanostructure.
C1 [Lansbergen, G. P.; Caro, J.; Rogge, S.] Delft Univ Technol, Kavli Inst Nanosci, Lorentzweg 1, NL-2628 CJ Delft, Netherlands.
[Rahman, R.; Klimeck, G.] Purdue Univ, Network Computat Nanotechnol, W Lafayette, IN 47907 USA.
[Hollenberg, L. C. L.] Univ Melbourne, Ctr Quantum Comp Technol, Sch Phys, Melbourne, Vic 3010, Australia.
[Collaert, N.; Biesemans, S.] IMEC, B-3001 Heverlee, Belgium.
[Klimeck, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lansbergen, GP (reprint author), Delft Univ Technol, Kavli Inst Nanosci, Lorentzweg 1, NL-2628 CJ Delft, Netherlands.
RI Hollenberg, Lloyd/B-2296-2010; Klimeck, Gerhard/A-1414-2012; Rogge,
Sven/G-3709-2010;
OI Klimeck, Gerhard/0000-0001-7128-773X; Rahman, Rajib/0000-0003-1649-823X
NR 13
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U1 0
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PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0736-7
J9 AIP CONF PROC
PY 2009
VL 1199
BP 93
EP +
PG 2
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA BQR10
UT WOS:000281590800044
ER
PT J
AU Turyshev, SG
AF Turyshev, S. G.
TI Experimental tests of general relativity: recent progress and future
directions
SO PHYSICS-USPEKHI
LA English
DT Review
ID INVERSE-SQUARE LAW; SOLAR GRAVITATIONAL DEFLECTION; PREFERRED-FRAME
THEORIES; FINE-STRUCTURE CONSTANT; PROBE WMAP OBSERVATIONS; ANGULAR
POWER SPECTRUM; LASER ASTROMETRIC TEST; ATOMIC CLOCK ENSEMBLE; NEWLY
RECOVERED DATA; SPACE-TIME FRAME
AB Einstein's general theory of relativity is the standard theory of gravity, especially where the needs of astronomy, astrophysics, cosmology, and fundamental physics are concerned. As such, this theory is used for many practical purposes involving spacecraft navigation, geodesy, and time transfer. We review the foundations of general relativity, discuss recent progress in tests of relativistic gravity, and present motivations for the new generation of high-accuracy tests of new physics beyond general relativity. Space-based experiments in fundamental physics are presently capable of uniquely addressing important questions related to the fundamental laws of nature. We discuss the advances in our understanding of fundamental physics that are anticipated in the near future and evaluate the discovery potential of a number of recently proposed space-based gravitational experiments.
C1 [Turyshev, S. G.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Turyshev, S. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Turyshev, SG (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prosp 13, Moscow 119992, Russia.
EM turyshev@jpl.nasa.gov
NR 476
TC 36
Z9 38
U1 0
U2 10
PU TURPION LTD
PI BRISTOL
PA C/O TURPION LTD, IOP PUBLISHING, TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1
6HG, ENGLAND
SN 1063-7869
EI 1468-4780
J9 PHYS-USP+
JI Phys. Usp.
PD JAN
PY 2009
VL 52
IS 1
BP 1
EP 27
DI 10.3367/UFNe.0179.200901a.0003
PG 27
WC Physics, Multidisciplinary
SC Physics
GA 454US
UT WOS:000266708800001
ER
PT J
AU Halekas, JS
Delory, GT
Lin, RP
Stubbs, TJ
Farrell, WM
AF Halekas, J. S.
Delory, G. T.
Lin, R. P.
Stubbs, T. J.
Farrell, W. M.
TI Lunar Prospector measurements of secondary electron emission from lunar
regolith
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Moon; Surface charging; Secondary electron emission; Lunar Prospector
AB We present the first in situ measurements of the secondary electron emission efficiency of lunar regolith, utilizing Lunar Prospector measurements of secondary electrons emitted from the negatively charged night side and accelerated upward by surface electric fields. By comparing measurements of secondary currents emitted from the surface and incident primary electron currents, we find that the secondary yield of lunar regolith is a factor of similar to 3 lower than that measured for samples in the laboratory. This lower yield significantly affects current balance at the lunar surface and the resulting equilibrium surface potentials. This information must be folded into models of the near-surface plasma sheath, in order to predict the effects on dust and other components of the lunar environment, and ultimately determine the importance for surface exploration and scientific investigations on the Moon. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Halekas, J. S.; Delory, G. T.; Lin, R. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Lin, R. P.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Stubbs, T. J.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Stubbs, T. J.; Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Halekas, JS (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM jazzman@ssi.berkeley.edu
RI Stubbs, Timothy/I-5139-2013; Farrell, William/I-4865-2013;
OI Stubbs, Timothy/0000-0002-5524-645X; Halekas, Jasper/0000-0001-5258-6128
FU NASA [NNG06GJ23G, NNX07AG10G]
FX This work was supported by the NASA grants NNG06GJ23G and NNX07AG10G.
NR 10
TC 25
Z9 26
U1 0
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD JAN
PY 2009
VL 57
IS 1
BP 78
EP 82
DI 10.1016/j.pss.2008.11.009
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409OK
UT WOS:000263515300010
ER
PT B
AU Khazanov, GV
Tel'nikhin, AA
Kronberg, TK
AF Khazanov, G. V.
Tel'nikhin, A. A.
Kronberg, T. K.
BE Gromov, SP
TI CHAOTIC MOTION OF RELATIVISTIC ELECTRONS DRIVEN BY WHISTLER WAVES
SO PLASMA PHYSICS RESEARCH ADVANCES
LA English
DT Article; Book Chapter
ID JOVIAN MAGNETOSPHERE; PARTICLE; ACCELERATION; DIFFUSION; JUPITER;
PACKET; FIELD
AB Canonical equations governing all electron motion in electromagnetic field of the whistler mode waves propagating along the direction of an ambient magnetic field are derived. The physical processes on which the equations of motion are based are identified. It is shown that relativistic electrons interacting with these fields demonstrate chaotic motion, which is accompanied by the particle stochastic heating and significant pitch angle diffusion. Evolution of distribution functions is described by the Fokker-Planck-Kolmogorov equations. A coefficient of diffusion is calculated from the equations of motion. Our results indicate that phase flow Of Our dynamical system is structural stable strange attractor. Chaotic motion on the attractor gives rise to an irreversible process (the so-called deterministic diffusion), which leads actually to establishing a steady-state energy spectra and results in such important and easily observable effects as the stochastic heating and pitch angle scattering of plasma particles. Under conditions typical of this mechanism, the heating region is determined by the boundaries of the attractor, and the heating rate is governed by the nature of the kinetics, which in turn depends on the canonical variables on the attractor. The same conditions impose limitations on the timescales of macroscopic effects and feasible extent of heating, so that understanding of this condition is of great practical interest. It is shown that the whistler mode waves could provide a viable mechanism for stochastic energization of electrons with energies up to 50 MeV in the Jovian magnetosphere.
C1 [Khazanov, G. V.] NASA Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Tel'nikhin, A. A.; Kronberg, T. K.] Altai State Univ, Barnaul 656049, Russia.
RP Khazanov, GV (reprint author), NASA Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
NR 27
TC 0
Z9 0
U1 0
U2 0
PU NOVA SCIENCE PUBLISHERS, INC
PI HAUPPAUGE
PA 400 OSER AVE, STE 1600, HAUPPAUGE, NY 11788-3635 USA
BN 978-1-60456-136-4
PY 2009
BP 333
EP 355
PG 23
WC Chemistry, Physical; Physics, Fluids & Plasmas
SC Chemistry; Physics
GA BKX66
UT WOS:000269533400010
ER
PT S
AU Quijada, MA
Waluschka, E
Wilson, M
McClain, CR
AF Quijada, Manuel A.
Waluschka, Eugene
Wilson, Mark
McClain, Charles R.
BE Shaw, JA
Tyo, JS
TI Measured Performance for Proposed Depolarizer for the Ocean Radiometer
for Carbon Assessment
SO POLARIZATION SCIENCE AND REMOTE SENSING IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Polarization Science and Remote Sensing IV
CY AUG 03-04, 2009
CL San Diego, CA
SP SPIE
DE ORCA; Polarimetry; depolarizer; birefringent materials; Mueller matrices
AB The Ocean Radiometer for Carbon Assessment (ORCA) is a new design concept for the next generation ocean biology and biogeochemistry satellite sensor. The wavelength range will be from the near UV, through the visible and to the Short Wave infrared. The challenge in this design is to remove the polarization effects from the optical performance of this hyper spectral observing instrument. In order to remove any polarization sensitivity during observation, the design calls for a front-end depolarizer that consists of two wedged birefringent magnesium fluoride crystals. Here we discuss the polarimetry measurements performed on this polarization scrambler, the depolarizer design and compare these results with model calculations.
C1 [Quijada, Manuel A.; Waluschka, Eugene; Wilson, Mark; McClain, Charles R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Quijada, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM manuel.a.quijada@nasa.gov
NR 6
TC 1
Z9 1
U1 0
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7751-4
J9 PROC SPIE
PY 2009
VL 7461
AR 746105
DI 10.1117/12.827427
PG 10
WC Remote Sensing; Optics
SC Remote Sensing; Optics
GA BCJ99
UT WOS:000310357000004
ER
PT S
AU Westl, E
Gary, GA
Cirtain, J
Davis, J
Kobayashi, K
Pietraszewski, C
AF Westl, Edward
Gary, G. Allen
Cirtain, Jonathan
Davis, John
Kobayashi, Ken
Pietraszewski, Chris
BE Shaw, JA
Tyo, JS
TI CIV Polarization Measurements using a Vacuum Ultraviolet Fabry-Perot
Interferometer
SO POLARIZATION SCIENCE AND REMOTE SENSING IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Polarization Science and Remote Sensing IV
CY AUG 03-04, 2009
CL San Diego, CA
SP SPIE
DE Fabry-Perot Interferometer; VUV Fabry-Perot; Vacuum Ultraviolet;
Polarization; CIV measurement
ID REGION
AB Marshall Space Flight Center's (MSFC) is developing a Vacuum Ultraviolet (VUV) Fabry-Perot Interferometer that will be launched on a sounding rocket for high throughput, high-cadence, extended field of view CIV (155nm) measurements. These measurements will provide (i) Dopplergrams for studies of waves, oscillations, explosive events, and mass motions through the transition region, and, (ii), polarization measurements to study the magnetic field in the transition region. This paper will describe the scientific goals of the instrument, a brief description of the optics and the polarization characteristics of the VUV Fabry Perot.
C1 [Westl, Edward; Cirtain, Jonathan; Davis, John] NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA.
[Gary, G. Allen; Kobayashi, Ken] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Pietraszewski, Chris] IC Opt Syst Ltd, Berkshire, England.
RP Westl, E (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA.
NR 17
TC 0
Z9 0
U1 0
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7751-4
J9 PROC SPIE
PY 2009
VL 7461
AR UNSP 746103
DI 10.1117/12.825718
PG 11
WC Remote Sensing; Optics
SC Remote Sensing; Optics
GA BCJ99
UT WOS:000310357000002
ER
PT J
AU Smith, TM
Williams, MK
Fesmire, JE
Sass, JP
Weiser, ES
AF Smith, Trent M.
Williams, Martha K.
Fesmire, James E.
Sass, Jared P.
Weiser, Erik S.
BE Mittal, KL
TI Polyimide-Aerogel Hybrid Foam Composites for Advanced Applications
SO POLYIMIDES AND OTHER HIGH-TEMPERATURE POLYMERS: SYNTHESIS,
CHARACTERIZATION AND APPLICATIONS, VOL 5
LA English
DT Proceedings Paper
CT 5th International Symposium on Polyimides and Other High-Temperature
Polymers - Synthesis, Characterization and Applications/MST Conferences
CY NOV 05-07, 2007
CL Orlando, FL
SP MST Conf
DE Polyimide; aerogel; foam; foam composite; aerospace insulation;
high-performance foam; TEEK
ID POLYURETHANE-BASED AEROGELS; COHERENT EXPANDED AEROGELS; LINKED SILICA
AEROGELS; THERMAL-RESISTANCE; INSULATION; PERFORMANCE; PRECURSORS;
DENSITY
AB NASA has had a growing need for high-performance polymer foams for cryogenic insulation, fireproofing, energy absorption and other applications. Commercially available foams, however, do not meet all of the requirements for surviving extreme environments. Most low-density foams crack at cryogenic temperatures, and the foams that can withstand extreme temperatures do not have the required structural integrity or thermal performance. Chemists and Engineers at NASA's Kennedy Space Center and Langley Research Center have collaborated in the development of a polyimide foam composite based on TEEK polyimide foam technology with enhanced thermal performance and vibration attenuation properties. The foam composites can be fabricated to target densities: high-density foam composites for structural applications and low-density foam composites where more flexibility might be advantageous. Heat transfer reduction is driven primarily by inorganic aerogel filler, with aerogel blanket composites having the most significant reduction in heat transfer and vibration attenuation. The TEEK composites are fire resistant and have excellent weather-resistant properties. This composite technology also lends itself to other foam systems. These materials may prove useful in process fluid piping, tanks for transporting and storing hot or cold fluids, ship and boat building and especially aerospace applications.
C1 [Smith, Trent M.; Williams, Martha K.; Fesmire, James E.; Sass, Jared P.] NASA, John F Kennedy Space Ctr, Spaceport Technol Div, Kennedy Space Ctr, FL 32899 USA.
RP Smith, TM (reprint author), NASA, John F Kennedy Space Ctr, Spaceport Technol Div, Kennedy Space Ctr, FL 32899 USA.
EM Trent.M.Smith@nasa.gov
NR 31
TC 0
Z9 0
U1 3
U2 26
PU E J BRILL
PI PA LEIDEN
PA PO BOX 9000, NL-2300 PA LEIDEN, NETHERLANDS
BN 978-90-474-2411-6
PY 2009
BP 295
EP 305
PG 11
WC Polymer Science
SC Polymer Science
GA BBY83
UT WOS:000308911600017
ER
PT S
AU Baran, O
DeGennaro, A
Rame, E
Wilkinson, A
AF Baran, Oleh
DeGennaro, Alfred
Rame, Enrique
Wilkinson, Allen
BE Nakagawa, M
Luding, S
TI DEM Simulation of a Schulze Ring Shear Tester
SO POWDERS AND GRAINS 2009
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 6th International Conference on the Micromechanics of Granular Media
CY JUL 13-17, 2009
CL Golden, CO
SP Assoc Study Micromech Granular Media, Univ Twente, Colorado Sch Mines
DE DEM; EDEM; granular flow; Schulze ring shear test
AB The Schulze ring shear tester allows measurement of yield loci for bulk granular solids and of the friction between the solids and the container wall material. These measurements are required inputs in a systematic design method for hoppers. The measurements are subject to test-to-test variations caused by the combined effects of several factors, such as cell filling technique, sampling technique, particle size and shape distribution of the loaded sample and cell size relative to the particle size. One difficulty for the experimenter is to decide which factors are most important in the shear test outcome. In this paper, we validate Discrete Element Model (DEM) simulation parameters with physical measurements of the JSC-1A lunar soil simulant, and inform about the relative impact of the various parameters to the shear test outcome. Specific tests will include sensitivity studies using DEM simulations that probe the effects of particle-to-cell size ratio, particle size distribution, particle shape, shear modulus and inter-particle adhesion and friction on shear failure.
C1 [Baran, Oleh] DEM Solut Inc, Lebanon, NH USA.
[DeGennaro, Alfred; Rame, Enrique; Wilkinson, Allen] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Baran, O (reprint author), DEM Solut Inc, Lebanon, NH USA.
NR 10
TC 0
Z9 0
U1 2
U2 6
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0682-7
J9 AIP CONF PROC
PY 2009
VL 1145
BP 409
EP +
PG 2
WC Materials Science, Multidisciplinary; Mechanics
SC Materials Science; Mechanics
GA BLN80
UT WOS:000270602900091
ER
PT S
AU Metzger, PT
Latta, RC
Schuler, JA
Immer, CD
AF Metzger, Philip T.
Latta, Robert C., III
Schuler, Jason A.
Immer, Christopher D.
BE Nakagawa, M
Luding, S
TI Craters Formed in Granular Beds by Impinging Jets of Gas
SO POWDERS AND GRAINS 2009
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 6th International Conference on the Micromechanics of Granular Media
CY JUL 13-17, 2009
CL Golden, CO
SP Assoc Study Micromech Granular Media, Univ Twente, Colorado Sch Mines
DE crater; erosion; scour hole; jet; bearing capacity; rocket exhaust;
martian soil; gravity
ID EROSION
AB When a jet of gas impinges vertically on a granular bed and forms a crater, the grains may be moved by several different mechanisms: viscous erosion, diffused gas eruption, bearing capacity failure, and/or diffusion-driven shearing. The relative importance of these mechanisms depends upon the flow regime of the gas, the mechanical state of the granular material, and other physical parameters. Here we report research in two specific regimes: viscous erosion forming scour holes as a function of particle size and gravity; and bearing capacity failure forming deep transient craters as a function of soil compaction.
C1 [Metzger, Philip T.] NASA, Granular Mech & Regolith Operat Lab, Kennedy Space Ctr, FL 32899 USA.
RP Metzger, PT (reprint author), NASA, Granular Mech & Regolith Operat Lab, Kennedy Space Ctr, FL 32899 USA.
OI Metzger, Philip/0000-0002-6871-5358
NR 8
TC 6
Z9 6
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0682-7
J9 AIP CONF PROC
PY 2009
VL 1145
BP 767
EP 770
PG 4
WC Materials Science, Multidisciplinary; Mechanics
SC Materials Science; Mechanics
GA BLN80
UT WOS:000270602900174
ER
PT B
AU Ryan, S
AF Ryan, Shannon
BE Hiermaier, S
TI Numerical Simulation in Micrometeoroid and Orbital Debris Risk
Assessment
SO PREDICTIVE MODELING OF DYNAMIC PROCESSES: A TRIBUTE TO PROFESSOR KLAUS
THOMA
LA English
DT Article; Book Chapter
ID BALLISTIC LIMIT; HYPERVELOCITY; SPACECRAFT; IMPACT; VELOCITIES
AB The threat of micrometeoroid and orbital debris (MMOD) impacts on space vehicles is assessed in terms of the probability of an impactor penetrating the spacecraft hull, and the probability of a penetrating impact resulting in catastrophic failure. These values are calculated in risk analysis codes which combine spacecraft geometry, debris environment models, and equations that define the penetration limits of the spacecraft outer structure (called ballistic limit equations, or BLEs). To characterize the performance of spacecraft structures under impact of MMOD particles at hypervelocity, experimental facilities such as two-stage light gas guns are commonly used. However, these facilities are only capable of reproducing approximately 40% of expected in-orbit impact conditions. As a result, numerical techniques are ideally suited for application in this field. The use of numerical hydrocodes in MMOD risk assessment is, historically, very limited. However, as code maturity continues to develop, their application becomes increasingly accepted. Within this chapter three examples are presented in which numerical hydrocodes were used in tandem with experimental testing for MMOD risk assessments. Beginning with the most simplistic application, i.e. derivation of perforation limits, the examples extend to the propagation of impact-induced dynamic disturbances through complex satellite structures.
C1 NASA, Johnson Space Ctr, Lunar & Planetary Inst, USRA, Washington, DC 20546 USA.
RP Ryan, S (reprint author), NASA, Johnson Space Ctr, Lunar & Planetary Inst, USRA, Washington, DC 20546 USA.
EM Shan-non.j.ryan@nasa.gov
NR 27
TC 2
Z9 2
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-1-4419-0726-4
PY 2009
BP 417
EP 446
DI 10.1007/978-1-4419-0727-1_22
D2 10.1007/978-1-4419-0727-1
PG 30
WC Engineering, Multidisciplinary; Engineering, Mechanical; Transportation
Science & Technology
SC Engineering; Transportation
GA BLA90
UT WOS:000269796700023
ER
PT S
AU Vetere, L
Burrows, DN
Gehrels, N
Meszaros, P
Wang, X
AF Vetere, L.
Burrows, D. N.
Gehrels, N.
Meszaros, P.
Wang, X.
BE Antonelli, LA
Limongi, M
Menci, N
Tornambe, A
Brocato, E
Raimondo, G
TI GRBs with no afterglow even in the Swift Era?
SO PROBING STELLAR POPULATIONS OUT TO THE DISTANT UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT International Conference on Probing Stellar Populations Out to the
Distant Universe
CY SEP 07-19, 2008
CL Cefalu, ITALY
SP Italian Inst Astrophys, Italian Inst Astrophys, Astron Observ Rome, Italian Inst Astrophys, Astron Observ Palermo, Italian Inst Astrophys, Astron Observ Teramo, Univ Cagliari, Dept Phys, Univ Palermo, Dept Phys & Astron Sci, Cefalu Local Author, Mondralisco Fdn, Assoc Cefalu & Astron
DE X-ray; gamma-ray; gamma-ray bursts
AB Thanks to its great capability Swift succeeds detecting an afterglow more than 93% of the time BAT triggers a new event. In a few cases, mainly Short GRBs or late observations, XRT did not detect any emission. However, for at least seven Long GRBs XRT could not measure any X-afterglow either, even as early as 100s after the BAT trigger. The detection of this new class of GRBs without any X-ray emission has raised many questions. Are these extreme naked GRB? Is this a completely new class of objects with an uncommon emission release? In this contribution we present a study on these unusual events. We analyse their peculiar behaviour in the Gamma and X-ray bands and discuss their singular origin.
C1 [Vetere, L.; Burrows, D. N.; Meszaros, P.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wang, X.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
RP Vetere, L (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM vetere@astro.psu.edu
RI Gehrels, Neil/D-2971-2012
NR 3
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0648-3
J9 AIP CONF PROC
PY 2009
VL 1111
BP 370
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJK00
UT WOS:000266597500061
ER
PT S
AU De Pasquale, M
Evans, P
Oates, S
Page, M
Zane, S
Breeveld, A
Holland, S
Still, A
AF De Pasquale, M.
Evans, P.
Oates, S.
Page, M.
Zane, S.
Breeveld, A.
Holland, S.
Still, A.
BE Antonelli, LA
Limongi, M
Menci, N
Tornambe, A
Brocato, E
Raimondo, G
TI Jet breaks at the end of the plateau phase of Swift GRB lightcurves
SO PROBING STELLAR POPULATIONS OUT TO THE DISTANT UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT International Conference on Probing Stellar Populations Out to the
Distant Universe
CY SEP 07-19, 2008
CL Cefalu, ITALY
SP Italian Inst Astrophys, Italian Inst Astrophys, Astron Observ Rome, Italian Inst Astrophys, Astron Observ Palermo, Italian Inst Astrophys, Astron Observ Teramo, Univ Cagliari, Dept Phys, Univ Palermo, Dept Phys & Astron Sci, Cefalu Local Author, Mondralisco Fdn, Assoc Cefalu & Astron
DE high energy astrophysics; relativistic outflows
AB An increasing sample of Swift GRBs show evidence of 'chromatic breaks', i.e. breaks that are present in the X-ray but not in the optical. Modelling the X-ray and optical data, we find that in a significant fraction of these GRB afterglows the component producing the X-ray emission cannot be responsible for the optical emission too. We propose that these afterglow lightcurves are the result of a two-component jet, in which both components are energy-injected for the whole observation and the X-ray break is due to a jet break in the narrow outflow. Bursts with chromatic breaks provide us with an explanation for another surprising finding, the paucity of late achromatic breaks. We show that our model may explain the behaviour of GRB emission in both X-ray and optical bands. Therefore, it can be a radical and noteworthy alternative to the current interpretation for the 'canonical' XRT and UVOT lightcurves, bearing fundamental implications for GRB physics.
C1 [De Pasquale, M.; Oates, S.; Page, M.; Zane, S.; Breeveld, A.; Still, A.] Univ Coll London, Mullard Space Lab, Holmbury Rd, Dorking RH5 6NT, Surrey, England.
[Evans, P.] Univ Leicester, Leicester LE1 7RH, Leics, England.
[Holland, S.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP De Pasquale, M (reprint author), Univ Coll London, Mullard Space Lab, Holmbury Rd, Dorking RH5 6NT, Surrey, England.
EM mpd@mssl.ucl.ac.uk
FU Royal Astronomical Society
FX The author could attend the Cefalu' conference and give his talk thanks
to a grant from Royal Astronomical Society.
NR 5
TC 0
Z9 0
U1 0
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0648-3
J9 AIP CONF PROC
PY 2009
VL 1111
BP 379
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJK00
UT WOS:000266597500063
ER
PT B
AU Boyle, RJ
Jones, SM
AF Boyle, R. J.
Jones, S. M.
GP ASME
TI Effects of Precooling Turbine Cooling Air on Engine Performance
SO PROCEEDINGS OF ASME TURBO EXPO 2009, VOL 4
LA English
DT Proceedings Paper
CT 54th ASME Turbo Expo 2009
CY JUN 08-12, 2009
CL Orlando, FL
SP ASME, Int Gas Turbine Inst
AB Approaches to improving gas turbine cycle efficiency by cooling the compressor discharge air used for turbine cooling are explored. From a turbine cycle standpoint, cooling the coolant air can improve cycle efficiency. A significant improvement in specific fuel consumption is achieved by raising the turbine rotor inlet temperature, and engine pressure ratio. Precooling compressor discharge air can enable rotor inlet temperature to increase up to 100 K at the same rotor cooling flow rate ratio. The efficiency gains from a 100 K rise in rotor inlet temperature translated into a fuel savings of 400 kg for a mission length of 5450 km. This fuel savings means about a 1200 kg savings in CO2 production. Compressor discharge air that passes through a heat exchanger may not have enough pressure to prevent hot gas ingestion through the cooling holes of the high pressure turbine stator. A stator analysis assuming a mixture of precooled and uncooled compressor discharge air showed only a 50 K rise in rotor inlet temperature due to precooling at the same cooling flow rate ratio.
C1 [Boyle, R. J.; Jones, S. M.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Boyle, RJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
EM Robert.J.Boyle@nasa.gov; Scott.M.Jones@nasa.gov
NR 16
TC 0
Z9 0
U1 0
U2 1
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4885-2
PY 2009
BP 495
EP 504
PG 10
WC Engineering, Mechanical; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Engineering; Materials Science; Metallurgy & Metallurgical Engineering
GA BON26
UT WOS:000277058700046
ER
PT B
AU Bruckner, RJ
AF Bruckner, Robert J.
GP ASME
TI WINDAGE POWER LOSS IN GAS FOIL BEARINGS AND THE ROTOR-STATOR CLEARANCE
OF HIGH SPEED GENERATORS OPERATING IN HIGH PRESSURE ENVIRONMENTS
SO PROCEEDINGS OF ASME TURBO EXPO 2009, VOL 5
LA English
DT Proceedings Paper
CT 54th ASME Turbo Expo 2009
CY JUN 08-12, 2009
CL Orlando, FL
SP ASME, Int Gas Turbine Inst
AB Closed Brayton Cycle (CBC) and Closed Supercritical Cycle (CSC) engines are prime candidates to convert heat from a reactor into electric power for robotic space exploration and habitation. These engine concepts incorporate a permanent magnet starter / generator mounted on the engine shaft along with the requisite turbomachinery. Successful completion of the long duration missions currently anticipated for these engines will require designs that adequately address all losses within the machine. The preliminary thermal management concept for these engine types is to use the cycle working fluid to provide the required cooling. In addition to providing cooling, the working fluid will also serve as the bearing lubricant. Additional requirements due to the unique application of these microturbines are zero contamination of the working fluid and entirely maintenance-free operation for many years. Losses in the gas foil bearings and within the rotor-stator gap of the generator become increasingly important as both rotational speed and mean operating pressure are increased. This paper presents the results of an experimental study, which obtained direct torque measurements on gas foil bearings and generator rotor-stator gaps. Test conditions for these measurements included rotational speeds up to 42000 revolutions per minute, pressures up to 45 atmospheres, and test gases of Nitrogen, Helium, and Carbon Dioxide. These conditions provided a maximum test Taylor number of nearly one million. The results show an exponential rise in power loss as mean operating density is increased for both the gas foil bearing and generator windage. These typical "secondary" losses can become larger than the total system output power if conventional design paradigms are followed. A non-dimensional analysis is presented to extend the experimental results into the CSC range for the generator windage.
C1 NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Bruckner, RJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
NR 22
TC 1
Z9 2
U1 0
U2 1
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4886-9
PY 2009
BP 263
EP 270
PG 8
WC Energy & Fuels; Engineering, Mechanical
SC Energy & Fuels; Engineering
GA BON28
UT WOS:000277059700027
ER
PT S
AU Eberspeaker, PJ
Gregory, DD
AF Eberspeaker, P. J.
Gregory, D. D.
BE Lacoste, H
TI AN OVERVIEW OF THE NASA SOUNDING ROCKETS AND BALLOON PROGRAMS
SO PROCEEDINGS OF THE 19TH ESA SYMPOSIUM ON EUROPEAN ROCKET AND BALLOON
PROGRAMMES AND RELATED RESEARCH
SE ESA Special Publications
LA English
DT Proceedings Paper
CT 19th ESA Symposium on European Rocket and Balloon Programmes and Related
Research
CY JUN 07-11, 2009
CL Bad Reichenhall, GERMANY
SP European Space Agcy (ESA)
AB The U. S. National Aeronautics and Space Administration (NASA) Sounding Rockets and Balloon Programs conduct a combined total of 40 to 50 missions per year in support of the NASA scientific community and other users. The NASA Sounding Rockets Program supports the science community by integrating their experiments into the sounding rocket payloads, and providing both the rocket vehicle and launch operations services. Flight operations have been conducted at Andoya Rocket Range, Poker Flat Research Range, Whites Sands Missile Range and Wallops Flight Facility. Development efforts include the Mesquito and Terrier-Improved Malemute launch vehicles as well as new attitude sensors and systems. The NASA Balloon Program provides balloons, data acquisition, and launch and flight operations support to the science community. Flight operations have been conducted in Antarctica; Sweden (Esrange); Palestine, Texas; and Ft. Sumner, New Mexico. Flights have included conventional and long duration balloons as well as a successful demonstration flight of the NASA Super Pressure Balloon. Technology initiatives include the development of parachute shock attenuation systems and an upgraded gondola automatic parachute release system.
C1 [Eberspeaker, P. J.] NASA, Sounding Rocket Program Off, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP Eberspeaker, PJ (reprint author), NASA, Sounding Rocket Program Off, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
EM philip.j.eberspeaker@nasa.gov
NR 4
TC 0
Z9 0
U1 0
U2 0
PU EUROPEAN SPACE AGENCY
PI PARIS
PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE
SN 0379-6566
BN 978-92-9221-235-3
J9 ESA SPEC PUBL
PY 2009
VL 671
BP 27
EP 34
PG 8
WC Engineering, Aerospace; Astronomy & Astrophysics; Meteorology &
Atmospheric Sciences
SC Engineering; Astronomy & Astrophysics; Meteorology & Atmospheric
Sciences
GA BBY59
UT WOS:000308797400006
ER
PT B
AU Aranki, N
Keymeulen, D
Bakhshi, A
Klimesh, M
AF Aranki, Nazeeh
Keymeulen, Didier
Bakhshi, Alireza
Klimesh, Matthew
GP IEEE/Computer Soc
TI Hardware Implementation of Lossless Adaptive and Scalable Hyperspectral
Data Compression for Space
SO PROCEEDINGS OF THE 2009 NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND
SYSTEMS
LA English
DT Proceedings Paper
CT 4th NASA/ESA Conference on Adaptive Hardware and Systems
CY JUL 29-AUG 01, 2009
CL Moscone Convention Ctr, San Francisco, CA
SP NASA Jet Propuls Lab, European Space Agcy, Univ Edinburgh
HO Moscone Convention Ctr
AB On-board lossless hyperspectral data compression reduces data volume in order to meet NASA and DoD limited downlink capabilities. The technique also improves signature extraction, object recognition and feature classification capabilities by providing exact reconstructed data on constrained downlink resources. At JPL a novel, adaptive and predictive technique for lossless compression of hyperspectral data was recently developed This technique uses an adaptive filtering method and achieves a combination of low complexity and compression effectiveness that far exceeds state-of-the-art techniques currently in use. The JPL-developed 'Fast Lossless' algorithm requires no training data or other specific information about the nature of the spectral bands for a fixed instrument dynamic range. It is of low computational complexity and thus well-suited for implementation in hardware. A modified form of the algorithm that is better suited for data from pushbroom instruments is generally appropriate for flight implementation. A scalable field programmable gate array (FPGA) hardware implementation was developed The FPGA implementation achieves a throughput performance of 58 Msamples/sec, which can be increased to over 100 Msamples/sec in a parallel implementation that uses twice the hardware resources This paper describes the hardware implementation of the 'Modified Fast Lossless' compression algorithm on an FPGA. The FPGA implementation targets the current state-of-the-art FPGAs (Xilinx Virtex IV and V families) and compresses one sample every clock cycle to provide a fast and practical real-time solution for space applications.
C1 [Aranki, Nazeeh; Keymeulen, Didier; Klimesh, Matthew] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Bakhshi, Alireza] B&A Engn Inc, San Dimas, CA 91773 USA.
RP Aranki, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM nazeeh.aranki@jpl.nasa.gov
FU Jet Propulsion Laboratory; California Institute of Technology; National
Aeronautics and Space Administration; Air Force Research Laboratory; JPL
FX The work 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. This
work was funded by Air Force Research Laboratory through the grant
entitled Fast Lossless On-Board Hyperspectral Data Compression. Special
thanks to Randy Odle, program manager, who also supported this research
at JPL, and to Ian Ferguson for his technical support to this research
NR 24
TC 6
Z9 6
U1 0
U2 5
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3714-6
PY 2009
BP 315
EP +
DI 10.1109/AHS.2009.66
PG 2
WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA BVA38
UT WOS:000290894400041
ER
PT B
AU Kizhner, S
Heinzen, K
AF Kizhner, Semion
Heinzen, Katherine
GP IEEE/Computer Soc
TI New Methodology for Reducing Sensor and Readout Electronics Circuitry
Noise in Digital Domain
SO PROCEEDINGS OF THE 2009 NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND
SYSTEMS
LA English
DT Proceedings Paper
CT 4th NASA/ESA Conference on Adaptive Hardware and Systems
CY JUL 29-AUG 01, 2009
CL Moscone Convention Ctr, San Francisco, CA
SP NASA Jet Propuls Lab, European Space Agcy, Univ Edinburgh
HO Moscone Convention Ctr
AB Upcoming NASA cosmology survey missions, such as Joint Dark Energy Mission (JDEM), carry instruments with multiple focal planes populated with many large sensor detector arrays. These sensors are passively cooled to low temperatures for low-level light and near-infrared (NIR) signal detection, and the sensor readout electronics circuitry must perform at extremely low noise levels to enable new required science measurements. Because we are at the technological edge of enhanced performance for sensors and readout electronics circuitry, as determined by thermal noise level at given temperature in analog domain, we must find new ways of further compensating for the noise in the signal digital domain. To facilitate this new approach, state-of-the-art sensors are augmented at their array hardware boundaries by non-illuminated or non-sensitive to photons reference pixels, which can be used to reduce noise attributed to sensor and readout electronics. There are a few proposed methodologies of processing in the digital domain the information carried by reference pixels. These methods involve using spatial and temporal global statistical scalar parameters derived from boundary reference pixel information to enhance the active pixels' signals. To make a step beyond this heritage methodology, we apply the NASA-developed technology known as the Hilbert-Huang Transform Data Processing System (HHT-DPS) to some component of reference pixel vectors' information. This allows to derive a noise correction array, which, in addition to the statistical parameter over the signal trend, is applied to the active pixel array.
C1 [Kizhner, Semion; Heinzen, Katherine] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kizhner, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Semion.Kizhner-1@nasa.gov
NR 8
TC 0
Z9 0
U1 0
U2 4
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3714-6
PY 2009
BP 323
EP 329
DI 10.1109/AHS.2009.15
PG 7
WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA BVA38
UT WOS:000290894400042
ER
PT J
AU Esterhuizen, S
Franklin, G
Hurst, K
Mannucci, A
Meehan, T
Webb, F
Young, L
AF Esterhuizen, Stephan
Franklin, Garth
Hurst, Ken
Mannucci, Anthony
Meehan, Tom
Webb, Frank
Young, Larry
BA Wang, J
Feng, Y
Wang, C
BF Wang, J
Feng, Y
Wang, C
TI TriG - A GNSS Precise Orbit and Radio Occultation Space Receiver
SO PROCEEDINGS OF THE 22ND INTERNATIONAL TECHNICAL MEETING OF THE SATELLITE
DIVISION OF THE INSTITUTE OF NAVIGATION (ION GNSS 2009)
LA English
DT Proceedings Paper
CT 22nd International Technical Meeting of the Satellite Division of the
Institute-of-Navigation (ION GNSS-09)
CY SEP 22-25, 2009
CL Savannah, GA
AB The GPS radio occultation (RO) technique [1] produces measurements in the ionosphere and neutral atmosphere [2] that contribute to monitoring space weather and climate change; and improving operational weather prediction. The high accuracy of RO soundings, traceable to SI standards, makes them ideal climate benchmark observations. For weather applications, RO observations improve the accuracy of weather forecasts by providing temperature and moisture profiles of sub-km vertical resolution, over land and ocean and in the presence of clouds.
JPL is currently flying a handful of RO instruments [3] on various satellites in Low Earth Orbit (LEO). Although these receivers have served to pioneer occultation measurements, various advances in technology and understanding of the RO technique along with availability of new signals from GPS and other GNSS satellites allow us to design an improved next generation space-based Precise Orbit Determination (POD) and RO receiver, the TriG receiver. The paper describes the architecture and implementation of the JPL TriG receiver as well as results obtained with a prototype receiver demonstrating key technologies necessary for a next-generation space science receiver.
C1 [Esterhuizen, Stephan; Franklin, Garth; Hurst, Ken; Mannucci, Anthony; Meehan, Tom; Webb, Frank; Young, Larry] CALTECH, JPL, Pasadena, CA 91125 USA.
RP Esterhuizen, S (reprint author), CALTECH, JPL, Pasadena, CA 91125 USA.
NR 6
TC 3
Z9 3
U1 0
U2 0
PU INST NAVIGATION
PI WASHINGTON
PA 815 15TH ST NW, STE 832, WASHINGTON, DC 20005 USA
PY 2009
BP 1442
EP 1446
PG 5
WC Computer Science, Artificial Intelligence; Telecommunications
SC Computer Science; Telecommunications
GA BSG19
UT WOS:000284356201048
ER
PT S
AU Roychoudhury, I
Biswas, G
Koutsoukos, X
AF Roychoudhury, Indranil
Biswas, Gautam
Koutsoukos, Xenofon
GP IEEE
TI Factoring Dynamic Bayesian Networks Based on Structural Observability
SO PROCEEDINGS OF THE 48TH IEEE CONFERENCE ON DECISION AND CONTROL, 2009
HELD JOINTLY WITH THE 2009 28TH CHINESE CONTROL CONFERENCE (CDC/CCC
2009)
SE IEEE Conference on Decision and Control
LA English
DT Proceedings Paper
CT Joint 48th IEEE Conference on Decision and Control (CDC) / 28th Chinese
Control Conference (CCC)
CY DEC 15-18, 2009
CL Shanghai, PEOPLES R CHINA
SP IEEE, Honeywell, Quanser, United Technologies, Googol Tech, MathWorks, Natl Instruments
ID LINEAR-SYSTEMS
AB Dynamic Bayesian Networks (DBNs) provide a systematic framework for robust online monitoring of dynamic systems. This paper presents an approach for increasing the efficiency of online estimation by partitioning a system DBN into a set of smaller factors, such that estimation algorithms can be applied to each factor independently. Our factoring scheme is based on the analysis of structural observability of the dynamic system. We establish the theoretical background for structural observability and derive an algorithm for generating the factors using structural observability analysis. We present experimental results to demonstrate the effectiveness of our factoring approach for accurate estimation of system behavior.
C1 [Roychoudhury, Indranil] NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA.
[Biswas, Gautam; Koutsoukos, Xenofon] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Inst Software Integrated Syst, Nashville, TN 37235 USA.
RP Roychoudhury, I (reprint author), NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA.
EM indranil.roychoudhury@nasa.gov; gautam.biswas@vanderbilt.edu;
xenofon.koutsoukos@vanderbilt.edu
FU National Science Foundation [CNS- 0615214]; NASA NRA [NNX07AD12A]
FX This work was supported by the National Science Foundation under Grant
CNS- 0615214 and NASA NRA NNX07AD12A.
NR 13
TC 1
Z9 1
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0743-1546
BN 978-1-4244-3872-3
J9 IEEE DECIS CONTR P
PY 2009
BP 244
EP 250
DI 10.1109/CDC.2009.5400689
PG 7
WC Automation & Control Systems; Engineering, Electrical & Electronic
SC Automation & Control Systems; Engineering
GA BA5OA
UT WOS:000336893600042
ER
PT B
AU Tinto, M
AF Tinto, M.
BE Maleki, L
TI SPACE SCIENCE APPLICATIONS OF FREQUENCY STANDARDS AND METROLOGY
SO PROCEEDINGS OF THE 7TH SYMPOSIUM FREQUENCY STANDARDS AND METROLOGY
LA English
DT Proceedings Paper
CT 7th Symposium on Frequency Standards and Metrology
CY OCT 05-11, 2008
CL Pacific Grove, CA
SP Jet Propuls Lab, Aerospace Corporat, Natl Inst Stand & Technol
DE Doppler tracking; Space-qualified atomic clocks; Radio science
experiments
ID GRAVITATIONAL-RADIATION; DOPPLER TRACKING
AB We are witnessing the beginning of a new era for space-qualified atomic clocks. These new instruments, characterized by low-mass, low-power consumption, and frequency stabilities comparable to those of ground-based clocks, will allow interplanetary spacecraft radio science experiments at unprecedented Doppler sensitivities.
By adding a digital receiver to the onboard instrumentation, it is possible to take advantage of the frequency stability of a space-qualified atomic clock by linearly combining digitally the multi-link Doppler measurements performed on the ground and onboard. This allows one to optimally suppress the frequency fluctuations of the Earth atmosphere, ionosphere and mechanical vibrations of the ground antenna (the dominant Doppler tracking noises) in the resulting Doppler data set.
After providing the general expression of the optimal combination of the ground and onboard Doppler data, we apply it, as an example, to interplanetary Doppler tracking searches for gravitational radiation. The resulting estimated sensitivity to milliHertz gravitational waves is about one order of magnitude better than that achievable by traditional two-way coherent Doppler experiments.
The Doppler tracking technique discussed in this article can be performed (at minimal additional cost) with future planned interplanetary missions, and extended to other experiments such as spacecraft Doppler tests of relativistic gravity, gravity field measurements, and radio occultations of planetary atmospheres and rings.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tinto, M (reprint author), CALTECH, Jet Prop Lab, MS 238-737, Pasadena, CA 91109 USA.
EM Massimo.Tinto@jpl.nasa.gov
NR 20
TC 0
Z9 0
U1 0
U2 0
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE
BN 978-981-283-821-6
PY 2009
BP 62
EP 70
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA BLM52
UT WOS:000270540200006
ER
PT B
AU Prestage, JD
Chung, S
Thompson, R
MacNeal, P
Le, T
AF Prestage, John D.
Chung, Sang
Thompson, Robert
MacNeal, Paul
Le, Thanh
BE Maleki, L
TI SMALL MERCURY MICROWAVE ION CLOCK FOR NAVIGATION AND RADIO-SCIENCE
SO PROCEEDINGS OF THE 7TH SYMPOSIUM FREQUENCY STANDARDS AND METROLOGY
LA English
DT Proceedings Paper
CT 7th Symposium on Frequency Standards and Metrology
CY OCT 05-11, 2008
CL Pacific Grove, CA
SP Jet Propuls Lab, Aerospace Corporat, Natl Inst Stand & Technol
AB We have recently completed a breadboard ion-clock physics package based on Hg ions shuttled between a quadrupole and a 16-pole rf trap. With this architecture we have demonstrated short-term stability similar to 1 -2x 10(-13) at 1 second, averaging to 10(-15) at 1 day. This development shows that H-maser quality stabilities can be produced in a small clock package, comparable in size to an ultra-stable quartz oscillator required for holding 1- 10(-13) at 1 second. This performance was obtained in a sealed vacuum configuration where only a getter pump was used to maintain vacuum. Because the tube is scaled, the Hg source and Neon buffer gas are held indefinitely, for the life of the tube. There is no consumption of Hg in this system unlike in a Cs beam tube where lifetime is often limited by Cs depletion. The vacuum tube containing the traps has now been under scaled vacuum conditions for over three years with no measurable degradation of ion trapping lifetimes or clock short-term performance. A 3-liter prototype physics package now in development will be described.
C1 [Prestage, John D.; Chung, Sang; Thompson, Robert; MacNeal, Paul; Le, Thanh] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Prestage, JD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 4
TC 0
Z9 0
U1 0
U2 2
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE
BN 978-981-283-821-6
PY 2009
BP 156
EP 165
PG 10
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA BLM52
UT WOS:000270540200016
ER
PT B
AU Burt, EA
Taghavi-Larigani, S
Prestage, JD
Tjoelker, RL
AF Burt, E. A.
Taghavi-Larigani, S.
Prestage, J. D.
Tjoelker, R. L.
BE Maleki, L
TI COMPENSATED MULTI-POLE MERCURY TRAPPED ION FREQUENCY STANDARD AND
STABILITY EVALUATION OF SYSTEMATIC EFFECTS
SO PROCEEDINGS OF THE 7TH SYMPOSIUM FREQUENCY STANDARDS AND METROLOGY
LA English
DT Proceedings Paper
CT 7th Symposium on Frequency Standards and Metrology
CY OCT 05-11, 2008
CL Pacific Grove, CA
SP Jet Propuls Lab, Aerospace Corporat, Natl Inst Stand & Technol
AB We have developed a compensated multi-pole Linear Ion Trap Standard (LITS) that eliminates nearly all frequency sensitivity to residual ion number variations. When operated with Hg-199(+), this trapped ion clock has recently demonstrated extremely good stability over a 9-month period. The short-term stability has been measured at 5x10(-14)/tau(1/2) and an upper limit on long-term fractional frequency deviations of <2.7x10(-17)/day was measured in comparison to the laser-cooled primary standards and to the post-processed ultra-stable version of TAI known as TTBIPM using GPS carrier phase time transfer. We have also made a first measurement of the Hg+/Hg collision shift and place a limit of +3.8(7.2)x10(-8)/Pa on the shift constant.
C1 [Burt, E. A.; Taghavi-Larigani, S.; Prestage, J. D.; Tjoelker, R. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Burt, EA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 16
TC 0
Z9 0
U1 0
U2 3
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE
BN 978-981-283-821-6
PY 2009
BP 321
EP 328
PG 8
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA BLM52
UT WOS:000270540200037
ER
PT B
AU Burt, EA
Taghavi-Larigani, S
Lea, SN
Prestage, JD
Tjoelker, RL
AF Burt, E. A.
Taghavi-Larigani, S.
Lea, S. N.
Prestage, J. D.
Tjoelker, R. L.
BE Maleki, L
TI EXPERIMENTS WITH A NEW (201)Hg(+) ION CLOCK
SO PROCEEDINGS OF THE 7TH SYMPOSIUM FREQUENCY STANDARDS AND METROLOGY
LA English
DT Proceedings Paper
CT 7th Symposium on Frequency Standards and Metrology
CY OCT 05-11, 2008
CL Pacific Grove, CA
SP Jet Propuls Lab, Aerospace Corporat, Natl Inst Stand & Technol
ID ATOMIC FREQUENCY STANDARDS; FUNDAMENTAL CONSTANTS; TIME-VARIATION;
LIMITS
AB in this paper we describe a new clock based on (201)Hg(+). All previous mercury ion clocks have been based on (199)Hg(+). We have recently completed construction of the (201)Hg(+) clock and will describe modifications to the design of our existing (199)Hg(+) clocks to accommodate the new isotope. We will also describe initial spectroscopic measurements of the hyperfine manifold, and possible future experiments. One experiment could place a limit on variations in the strong interaction fundamental constant ratio m(q)/Lambda(QCD).
C1 [Burt, E. A.; Taghavi-Larigani, S.; Prestage, J. D.; Tjoelker, R. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Burt, EA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
NR 15
TC 1
Z9 1
U1 0
U2 1
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE
BN 978-981-283-821-6
PY 2009
BP 358
EP 362
PG 5
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA BLM52
UT WOS:000270540200043
ER
PT B
AU Dick, J
Tu, M
Birnbaum, K
Strekalov, D
Yu, N
AF Dick, John
Tu, Meirong
Birnbaum, Kevin
Strekalov, Dmitry
Yu, Nan
BE Maleki, L
TI FUNDAMENTAL NOISE-LIMITED OPTICAL PHASE LOCKING AT FEMTOWATT LIGHT
LEVELS
SO PROCEEDINGS OF THE 7TH SYMPOSIUM FREQUENCY STANDARDS AND METROLOGY
LA English
DT Proceedings Paper
CT 7th Symposium on Frequency Standards and Metrology
CY OCT 05-11, 2008
CL Pacific Grove, CA
SP Jet Propuls Lab, Aerospace Corporat, Natl Inst Stand & Technol
AB We describe an optical phase lock loop (PLL) designed to recover an optical carrier at powers below one picowatt in a Deep Space optical transponder. Previous low power optical phase lock has been reported with powers down to about 1 pW. We report the demonstration and characterization of the optical phase locking at femtowatt levels. We achieved a phase slip rate below one cycle-slip/second at powers down to 60 femtowatts. This phase slip rate corresponds to a frequency stability Of 1x10(-14) at 1 s, a value better than any frequency standard available today for measuring times equal to a typical two-way delay between Earth and Mars. The PLL shows very robust stability at these power levels. We developed simulation software to optimize parameters of the second order PLL loop in the presence of laser flicker frequency noise and white phase (photon) noise, and verified the software with a white phase noise model by Viterbi. We also demonstrated precise Doppler tracking at femtowatt levels.
C1 [Dick, John; Tu, Meirong; Birnbaum, Kevin; Strekalov, Dmitry; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Dick, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 5
TC 0
Z9 0
U1 1
U2 1
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE
BN 978-981-283-821-6
PY 2009
BP 405
EP 416
PG 12
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA BLM52
UT WOS:000270540200050
ER
PT B
AU Tong, MT
Jones, SM
Haller, WJ
Handschuh, RF
AF Tong, Michael T.
Jones, Scott M.
Haller, William J.
Handschuh, Robert F.
GP ASME
TI ENGINE CONCEPTUAL DESIGN STUDIES FOR A HYBRID WING BODY AIRCRAFT
SO PROCEEDINGS OF THE ASME TURBO EXPO 2009, VOL 1
LA English
DT Proceedings Paper
CT 54th ASME Turbo Expo 2009
CY JUN 08-12, 2009
CL Orlando, FL
SP ASME, Int Gas Turbine Inst
DE hybrid wing body; fuel burn; noise; emissions
AB Worldwide concerns of air quality and climate change have made environmental protection one of the most critical issues in aviation today. NASA's current Fundamental Aeronautics research program is directed at three generations of aircraft in the near, mid and far term, with initial operating capability around 2015, 2020, and 2030, respectively. Each generation has associated goals for fuel burn, NO(x), noise, and field-length reductions relative to today's aircrafts. The research for the 2020 generation is directed at enabling a hybrid wing body (HWB) aircraft to meet NASA's aggressive technology goals. This paper presents the conceptual cycle and mechanical designs of the two engine concepts, podded and embedded systems, which were proposed for a HWB cargo freighter. They are expected to offer significant benefits in noise reductions without compromising the fuel burn.
C1 [Tong, Michael T.; Jones, Scott M.; Haller, William J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Tong, MT (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 16
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4882-1
PY 2009
BP 109
EP 117
PG 9
WC Energy & Fuels; Engineering, Mechanical
SC Energy & Fuels; Engineering
GA BON15
UT WOS:000277052900011
ER
PT B
AU Simon, DL
Garg, S
AF Simon, Donald L.
Garg, Sanjay
GP ASME
TI OPTIMAL TUNER SELECTION FOR KALMAN FILTER-BASED AIRCRAFT ENGINE
PERFORMANCE ESTIMATION
SO PROCEEDINGS OF THE ASME TURBO EXPO 2009, VOL 1
LA English
DT Proceedings Paper
CT 54th ASME Turbo Expo 2009
CY JUN 08-12, 2009
CL Orlando, FL
SP ASME, Int Gas Turbine Inst
AB A linear point design methodology for minimizing the error in on-line Kalman filter-based aircraft engine performance estimation applications is presented. This technique specifically addresses the underdetermined estimation problem, where there are more unknown parameters than available sensor measurements. A systematic approach is applied to produce a model tuning parameter vector of appropriate dimension to enable estimation by a Kalman filter, while minimizing the estimation error in the parameters of interest. Tuning parameter selection is performed using a multi-variable iterative search routine which seeks to minimize the theoretical mean-squared estimation error. This paper derives theoretical Kalman filter estimation error bias and variance values at steady-state operating conditions, and presents the tuner selection routine applied to minimize these values. Results from the application of the technique to an aircraft engine simulation are presented and compared to the conventional approach of tuner selection Experimental simulation results are found to be in agreement with theoretical predictions. The new methodology is shown to yield a significant improvement in on-line engine performance estimation accuracy.
C1 [Simon, Donald L.; Garg, Sanjay] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Simon, DL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4882-1
PY 2009
BP 659
EP 671
PG 13
WC Energy & Fuels; Engineering, Mechanical
SC Energy & Fuels; Engineering
GA BON15
UT WOS:000277052900065
ER
PT B
AU Shyam, V
Ameri, A
Luk, DF
Chen, JP
AF Shyam, Vikram
Ameri, Ali
Luk, Daniel F.
Chen, Jen-Ping
GP ASME
TI 3-D UNSTEADY SIMULATION OF A MODERN HIGH PRESSURE TURBINE STAGE USING
PHASE LAG PERIODICITY: ANALYSIS OF FLOW AND HEAT TRANSFER
SO PROCEEDINGS OF THE ASME TURBO EXPO 2009, VOL 3, PTS A AND B
LA English
DT Proceedings Paper
CT 54th ASME Turbo Expo 2009
CY JUN 08-12, 2009
CL Orlando, FL
SP ASME, Int Gas Turbine Inst
AB Unsteady 3-D RANS simulations have been performed on a highly loaded transonic turbine stage and results are compared to steady calculations as well as experiment. A low Reynolds number k-epsilon turbulence model is employed to provide closure for the RANS system. A phase-lag boundary condition is used in the periodic direction. This allows the unsteady simulation to be performed by using only one blade from each of the two rows. The objective of this paper is to study the effect of unsteadiness on rotor heat transfer and to glean any insight into unsteady flow physics. The role of the stator wake passing on the pressure distribution at the leading edge is also studied. The simulated heat transfer and pressure results agreed favorably with experiment. The time-averaged heat transfer predicted by the unsteady simulation is higher than the heat transfer predicted by the steady simulation everywhere except at the leading edge. The shock structure formed due to stator-rotor interaction was analyzed. Heat transfer and pressure at the hub and casing were also studied. Thermal segregation was observed that leads to the heat transfer patterns predicted by steady and unsteady simulations to be different.
C1 [Shyam, Vikram; Ameri, Ali] Ohio State Univ, NASA Glenn Res Ctr, Cleveland, OH USA.
RP Shyam, V (reprint author), Ohio State Univ, NASA Glenn Res Ctr, Cleveland, OH USA.
NR 20
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4884-5
PY 2009
BP 1039
EP 1049
PG 11
WC Energy & Fuels; Engineering, Mechanical
SC Energy & Fuels; Engineering
GA BON21
UT WOS:000277056900091
ER
PT J
AU Urzay, J
Nayagam, V
Williams, FA
AF Urzay, Javier
Nayagam, Vedha
Williams, Forman A.
TI Diffusion-flame extinction on a rotating porous-disk burner
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Laminar flames; Nonpremixed combustion; Asymptotic analysis; Extinction
ID ASYMPTOTIC STRUCTURE; EDGE-FLAMES; COUNTERFLOW; DYNAMICS
AB Flames advected by swirling flows are subject to large strain rates that may cause local extinction. In this investigation, a porous-disk burner is spun at a constant angular velocity in an otherwise quiescent oxidizing atmosphere. Gaseous methane is injected through the disk pores and burns in a flat diffusion flame adjacent to the disk, resulting in a variety of nonpremixed flame patterns for different combinations of the angular velocity and fuel flow rate. The method of activation-energy asymptotics is employed to address the transition from conditions under which a diffusion flame envelops the entire disk to conditions under which diffusion flames are present over only part of the disk, leading to the presence of edge flames. An expression for the extinction Damkohler number as a function of the fuel flow rate and angular velocity is derived and compared with experiments. Agreement is favorable when parameters for a one-step model of methane combustion are employed. (C) 2009 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Urzay, Javier; Williams, Forman A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA.
[Urzay, Javier; Williams, Forman A.] Univ Calif San Diego, Energy Res Ctr, La Jolla, CA 92093 USA.
[Nayagam, Vedha] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA.
RP Urzay, J (reprint author), Univ Calif San Diego, Dept Mech & Aerosp Engn, 9500 Gilman Dr, La Jolla, CA 92093 USA.
EM jurzay@ucsd.edu
RI Urzay, Javier /H-6029-2013
NR 13
TC 2
Z9 2
U1 0
U2 2
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2009
VL 32
BP 1219
EP 1226
DI 10.1016/j.proci.2008.06.016
PG 8
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA 427CG
UT WOS:000264756800140
ER
PT J
AU Bellan, J
Selle, LC
AF Bellan, J.
Selle, L. C.
TI Large Eddy Simulation composition equations for single-phase and
two-phase fully multicomponent flows
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Multicomponent LES equations
ID DIRECT NUMERICAL-SIMULATION; PLANE MIXING LAYER; EVAPORATING DROPS;
MIXTURES; TURBULENCE; LADEN; COMPONENTS; PARTICLES; NUMBER; MODEL
AB The Large Eddy Simulation (LES) equations for multicomponent (MC) fuel single-phase (SP) flow and two-phase (TP) flow with phase change are derived from the Direct Numerical Simulation (DNS) equations by filtering the DNS equations using a top-hat filter. Additional to the equations solved for single-component (SC) fuels, composition equations enter the formulation. The species composition is represented through a Probability Distribution Function (PDF), and DNS equations for the PDF moments are solved to find the composition. The TP filtered equations contain three categories of subgrid-scale (SGS) terms: ( 1) SGS-flux terms, (2) filtered Source terms (FSTs) and (3) terms representing the 'LES assumptions'. For SP flows no FSTs exist. The SGS terms in the LES equations must be either shown negligible or modeled. It is shown that for the composition equations, two equivalent forms of the DNS equations lead to two non-equivalent forms of the LES equations. Criteria are proposed to select the form best suited for LES. These criteria are used in conjunction with evaluations based oil a DNS database portraying mixing and phase change, and lead to choosing one of the LES forms which satisfies all criteria. It is shown that the LES assumptions lead to additional SGS terms which require modeling. Further considerations are made for reactive flows. (C) 2009 Published by Elsevier Inc. on behalf of The Combustion Institute.
C1 [Bellan, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bellan, J.; Selle, L. C.] CALTECH, Dept Mech Engn, Pasadena, CA 91125 USA.
RP Bellan, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 125-109, Pasadena, CA 91109 USA.
EM Josette.Bellan@jpl.nasa.gov
RI Selle, Laurent/I-6369-2013
OI Selle, Laurent/0000-0002-5997-3646
FU Jet Propulsion Laboratory (JPL); California Institute of Technology
(Caltech); American Chemical Society
FX This study was conducted at the Jet Propulsion Laboratory (JPL),
California Institute of Technology (Caltech), under the partial
sponsorship of the Donors of The Petroleum Research Fund administered by
the American Chemical Society through a grant (to J.B.) for Caltech Post
Doctoral Fellow (L.S.) Support, and of the Air Force Research
Laboratory. Wright Patterson Air Force Base with Dr. Tim Edwards as
technical monitor. Computational resources were provided by the
supercomputing facility at JPL.
NR 22
TC 4
Z9 4
U1 0
U2 9
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2009
VL 32
BP 2239
EP 2246
DI 10.1016/j.proci.2008.06.005
PG 8
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA 427CH
UT WOS:000264756900072
ER
PT J
AU Olson, SL
Miller, FJ
AF Olson, S. L.
Miller, F. J.
TI Experimental comparison of opposed and concurrent flame spread in a
forced convective microgravity environment
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Opposed flame spread; Concurrent flame spread; Microgravity; Normoxic
conditions; Recirculation cell
ID THIN; FLOW; FUEL
AB Flame spread experiments in both concurrent and opposed flow have been carried out in a 5.18-s drop tower with a thin cellulose fuel. Flame spread rate and flame length have been measured over a range 0-30 cm/s forced flow (in both directions), 3.6-14.7 psia, and oxygen mole fractions 0.24-0.85 in nitrogen. Results are presented for each of the three variables independently to elucidate their individual effects, with special emphasis on pressure/oxygen combinations that result in earth-equivalent oxygen partial pressures (normoxic conditions). Correlations using all three variables combined into a single parameter to predict flame spread rate are presented. The correlations are used to demonstrate that opposed flow flames in typical spacecraft ventilation flows (5-20 cm/s) spread faster than concurrent flow flames under otherwise similar conditions (pressure, oxygen concentration) in nearly all spacecraft atmospheres. This indicates that in the event of an actual fire aboard a spacecraft, the fire is likely to grow most quickly in the opposed mode as the upstream flame spreads faster and the downstream flame is inhibited by the vitiated atmosphere produced by the upstream flame. Additionally, an interesting phenomenon was observed at intermediate values of concurrent forced flow velocity where flow/flame interactions produced a recirculation downstream of the flame, which allowed an opposed flow leading edge to form there. Published by Elsevier Inc. on behalf of The Combustion Institute.
C1 [Olson, S. L.] NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA.
[Miller, F. J.] San Diego State Univ, Dept Mech Engn, San Diego, CA 92182 USA.
RP Olson, SL (reprint author), NASA, Glenn Res Ctr Lewis Field, MS 77-5, Cleveland, OH 44135 USA.
EM sandra.l.olson@nasa.gov
FU NASA's Fire Prevention, Detection, and Suppression Program
FX The research at NASA Glenn's Zero Gravity Research Facility was
supported by NASA's Fire Prevention, Detection, and Suppression Program.
We thank the personnel of the NASA Glenn Zero Gravity Research Facility
for upgrading the experiment apparatus and conducting the drop testing.
We thank Glenn's Spacecraft Fire Prevention team for reviewing this
work.
NR 21
TC 10
Z9 12
U1 2
U2 12
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2009
VL 32
BP 2445
EP 2452
DI 10.1016/j.proci.2008.05.081
PG 8
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA 427CH
UT WOS:000264756900097
ER
PT J
AU McAllister, S
Fernandez-Pello, C
Urban, D
Ruff, G
AF McAllister, Sara
Fernandez-Pello, Carlos
Urban, David
Ruff, Gary
TI Piloted ignition delay of PMMA in space exploration atmospheres
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Piloted ignition; Pressure; Oxygen; Exploration atmosphere
ID EXTINCTION; OXYGEN; FUELS
AB In order to reduce the risk of decompression sickness associated with extra-vehicular activity (EVA), NASA is designing the next generation of exploration vehicles and habitats with a different, cabin environment than used previously. The proposed environment uses a total cabin pressure of 52.7-58.6 kPa with all oxygen concentration of 30-34% by volume and was chosen with material flammability in mind. Because materials may burn differently under these conditions and there is little information oil how this new environment affects the flammability of the materials onboard, it is important to conduct material flammability experiments at the intended exploration atmosphere. One method to evaluate material flammability is by its ease of ignition. To this end, piloted ignition delay tests were conducted in the Forced Ignition and Spread Test (FIST) apparatus Subject to this new environment. In these tests, polymethylmethacylate (PMMA) was exposed to a range of oxidizer flow velocities and externally applied heat fluxes. Tests were conducted for a baseline case of normal pressure and oxygen concentration, low pressure (58.6 kPa) with normal oxygen (21%), and low pressure with 32% oxygen concentration conditions to determine the individual effect of pressure and the combined effect of pressure and oxygen concentration oil the ignition delay. It was found that reducing the pressure while keeping the oxygen concentration at 21%, reduced the ignition time by 17% on average. Increasing the oxygen concentration at low pressures reduced the ignition time by an additional 10%. It was also noted that the critical heat flux for ignition decreases at exploration atmospheres. These results show that tests conducted in standard atmospheric conditions will underpredict the ignition of materials intended for use on spacecraft and that, at these conditions, materials are more susceptible to ignition than at current spacecraft atmospheres. (C) 2009 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [McAllister, Sara; Fernandez-Pello, Carlos] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA.
[Urban, David; Ruff, Gary] NASA, John H Glenn Res Ctr, Cleveland, OH 44256 USA.
RP McAllister, S (reprint author), Univ Calif Berkeley, Dept Mech Engn, 60A Hesse Hall,Mailstop 1740, Berkeley, CA 94720 USA.
EM smcalliser@berkeley.edu
FU NASA [NNC-05GA02G]
FX This work was supported by NASA Grant NNC-05GA02G. The authors thank
Janice Lai, Sarah Scott, and Amelia Ramirez-Correa for their
indispensable assistance running the experiments: Chris Lautenberger for
his insightful (discussions and input; and Paul Ferkul for his unbiased
review of the manuscript.
NR 26
TC 12
Z9 12
U1 0
U2 5
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2009
VL 32
BP 2453
EP 2459
DI 10.1016/j.proci.2008.05.076
PG 7
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA 427CH
UT WOS:000264756900098
ER
PT J
AU Takahashi, F
Katta, VR
AF Takahashi, Fumiaki
Katta, Viswanath R.
TI Extinguishment of diffusion flames around a cylinder in a coaxial air
stream with dilution or water mist
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Fire suppression; Diffusion flame extinguishment; PMMA; Carbon dioxide;
Water mist
ID NON-PREMIXED FLAMES; CUP-BURNER FLAMES; SUPPRESSION EFFECTIVENESS;
DROPLETS
AB Extinguishment of methane and polymethylmethacrylate(PMMA) diffusion flames by gaseous and water mist fire-extinguishing agents has been studied experimentally and computationally using a cylindrical burner inserted downwardly into all upward coaxial air stream. Transient computations were performed for methane flames with full chemistry and a simple water- mist model to reveal the flame Structure and Suppression processes. For methane, as a gaseous agent (CO(2) or N(2)) or water mist (:approximate to 35 mu m number mean diameter) was added incrementally to the air stream: (1) a diffusion flame enveloping a Porous bottom surface or the cylinder extinguished first, resulting in a flame with its base(edge) anchored at the leading edge of the side of the porous cylinder; and (2) the flame base oscillated, detached, drifted downstream, and extinguished eventually. For PMMA. the flame base attached to the fuel Surface more closely than methane flames until detachment led to blowoff. The volume fractions of CO(2) or N(2) in the oxidizer stream at detachment and extinguishment were independent (or mild functions) of the mean oxidizer velocity (U(ox)). In computations, the initial envelope flame extinction led to extinguishment at the limits between the measured detachment and extinguishing conditions. The measured water flow rate at extinguishment was independent or U(ox); thus, the water mass fraction decreased dramatically with increasing U(ox), suggesting that the water mist was transported to the flame zone independently of the air flow. The calculated water mass fraction at extinguishment, by contrast, decreased only mildly with U(ox) because water mist was modeled as a gaseous species. The computation of the near-limit flames revealed that: (1) extinguishment occurred when the peak temperature decreased to approximate to 1600 K: (2) adding CO(2) or H(2)O exhibited chemical effects oil the flame structure; and (3) the stagnation-point-flow structure was nearly identical to that of a near-extinction counterflow diffusion flame. (c) 2009 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Takahashi, Fumiaki] NASA, Natl Ctr Space Explorat Res Fluids & Combust, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Katta, Viswanath R.] Innovat Sci Solut Inc, Dayton, OH 45440 USA.
RP Takahashi, F (reprint author), NASA, Natl Ctr Space Explorat Res Fluids & Combust, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA.
EM fxt13@case.edu
FU Office of Biological and Physical Research and the Fire Prevention,
Detection, and Suppression program; Exploration Technology Development
Program Office; National Aeronautics and Space Agency, Washington, DC
FX This research was supported by the Office of Biological and Physical
Research and the Fire Prevention, Detection, and Suppression program in
the Exploration Technology Development Program Office, National
Aeronautics and Space Agency, Washington, DC.
NR 29
TC 16
Z9 18
U1 2
U2 7
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2009
VL 32
BP 2615
EP 2623
DI 10.1016/j.proci.2008.05.028
PG 9
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA 427CH
UT WOS:000264756900118
ER
PT B
AU DellaCorte, C
AF DellaCorte, Christopher
GP ASME
TI TECHNICAL DEVELOPMENT PATH FOR FOIL GAS BEARINGS
SO PROCEEDINGS OF THE STLE/ASME INTERNATIONAL JOINT TRIBOLOGY CONFERENCE
2008
LA English
DT Proceedings Paper
CT STLE/ASME 2008 International Joint Tribology Conference
CY OCT 20-22, 2008
CL Miami, FL
SP Soc Tribologists & Lubricat Engineers, Amer Soc Mech Engineers
AB Foil gas bearings are in widespread commercial use in air cycle machines, turbocompressors and microturbine generators and are emerging in more challenging applications such as turbochargers, auxiliary power units and propulsion gas turbines. Though not well known, foil bearing technology is well over fifty years old. Recent technological developments indicate that their full potential has yet to be realized. This paper investigates the key technological developments that have characterized foil bearing advances. It is expected that a better understanding of foil gas bearing development path will aid in future development and progress towards more advanced applications.
C1 NASA, Glenn Res Ctr, Cleveland, OH USA.
RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
NR 20
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4336-9
PY 2009
BP 299
EP 302
PG 4
WC Engineering, Mechanical; Nanoscience & Nanotechnology; Materials
Science, Multidisciplinary; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Materials Science;
Physics
GA BJJ09
UT WOS:000266325200079
ER
PT B
AU Bruckner, RJ
AF Bruckner, Robert J.
GP ASME
TI EVALUATION OF SUPERCRITICAL CARBON DIOXIDE FOR USE IN FLUID FILM
BEARINGS FOR PROCESS FLUID LUBRICATED MACHINES
SO PROCEEDINGS OF THE STLE/ASME INTERNATIONAL JOINT TRIBOLOGY CONFERENCE
2008
LA English
DT Proceedings Paper
CT STLE/ASME 2008 International Joint Tribology Conference
CY OCT 20-22, 2008
CL Miami, FL
SP Soc Tribologists & Lubricat Engineers, Amer Soc Mech Engineers
C1 NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Bruckner, RJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4336-9
PY 2009
BP 407
EP 409
PG 3
WC Engineering, Mechanical; Nanoscience & Nanotechnology; Materials
Science, Multidisciplinary; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Materials Science;
Physics
GA BJJ09
UT WOS:000266325200106
ER
PT B
AU Dimofte, F
Ene, NM
Oswald, FB
AF Dimofte, Florin
Ene, Nicoleta M.
Oswald, Fred B.
GP ASME
TI OIL WAVE JOURNAL BEARING STEADY-STATE DATA FROM A NEW TEST RIG
SO PROCEEDINGS OF THE STLE/ASME INTERNATIONAL JOINT TRIBOLOGY CONFERENCE
2008
LA English
DT Proceedings Paper
CT STLE/ASME 2008 International Joint Tribology Conference
CY OCT 20-22, 2008
CL Miami, FL
SP Soc Tribologists & Lubricat Engineers, Amer Soc Mech Engineers
AB An oil lubricated wave bearing has been tested on a new rig for fluid film journal bearings at NASA Glenn Research Center in Cleveland, Ohio, USA. The tests are intended to evaluate the rig possibilities of running without misaligmnent. Data recorded under steady-state conditions included oil flow rate, input, output and oil supply temperatures, and shaft position. Two sets of data were collected: i) by varying the load to 9000 N at a constant shaft rotation speed of 8,000 RPM and ii) by varying the speed from 9,000 to 12,000 RPM at constant load of 6,700 N. The temperatures of the metal sleeves were also recorded. Vibration levels at four locations were displayed and recorded. These measurements indicated that damping from the wave bearings provides significant attenuation of the vibration generated by the air turbine that drives the rig.
C1 [Dimofte, Florin] Univ Toledo, NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Dimofte, F (reprint author), Univ Toledo, NASA, Glenn Res Ctr, Cleveland, OH USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4336-9
PY 2009
BP 415
EP 417
PG 3
WC Engineering, Mechanical; Nanoscience & Nanotechnology; Materials
Science, Multidisciplinary; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Materials Science;
Physics
GA BJJ09
UT WOS:000266325200108
ER
PT J
AU Meyyappan, M
AF Meyyappan, M.
TI Catalyzed chemical vapor deposition of one-dimensional nanostructures
and their applications
SO PROGRESS IN CRYSTAL GROWTH AND CHARACTERIZATION OF MATERIALS
LA English
DT Review
DE Nanostructures; One-dimensional nanomaterials; Low temperature plasma;
Catalyzed growth; Vapor-liquid-solid technique; Chemical vapor
deposition
ID CARBON NANOTUBE GROWTH; MULTILAYERED METAL-CATALYSTS; RANDOM-ACCESS
MEMORY; GERMANIUM NANOWIRES; SILICON NANOWIRES; SEMICONDUCTOR NANOWIRES;
THERMOELECTRIC FIGURE; SELECTIVE GROWTH; CRYSTAL-GROWTH; GAN NANOWIRES
AB This article reviews progress in the growth of one-dimensional nanomaterials such as carbon nanotubes and inorganic nanowires. Catalyzed chemical vapor deposition has been the preferred method to grow these materials for various applications requiring controlled growth on patterned and unpatterned substrates. Both thermal and plasma chemical vapor deposition techniques have been widely used in the case of carbon nanotubes. In addition to the discussion on growth, a review of applications for one-dimensional nanostructures and future directions is provided. Published by Elsevier Ltd.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Meyyappan, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM m.meyyappan@nasa.gov
NR 94
TC 19
Z9 19
U1 5
U2 29
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0960-8974
J9 PROG CRYST GROWTH CH
JI Prog. Cryst. Growth Charact. Mater.
PY 2009
VL 55
IS 1-2
BP 1
EP 21
DI 10.1016/j.pcrysgrow.2009.01.001
PG 21
WC Crystallography; Materials Science, Characterization & Testing
SC Crystallography; Materials Science
GA 440VD
UT WOS:000265726900001
ER
PT J
AU Phillips, AJ
Brodeur, RD
Suntsov, AV
AF Phillips, A. Jason
Brodeur, Richard D.
Suntsov, Andrey V.
TI Micronekton community structure in the epipelagic zone of the northern
California Current upwelling system
SO PROGRESS IN OCEANOGRAPHY
LA English
DT Review
DE Pacific Ocean; Marine micronekton; Lanternfish; Community composition;
Species diversity; California Current
ID VERTICAL-DISTRIBUTION; STENOBRACHIUS-LEUCOPSARUS; FISHERIES MANAGEMENT;
FEEDING-HABITS; COASTAL OCEAN; OREGON COAST; ECOSYSTEM; PACIFIC; USA;
MYCTOPHIDAE
AB Spatial and temporal variability in the micronekton community and in oceanographic conditions were evaluated from nighttime midwater trawl samples collected between Heceta Head, Oregon (44.0 degrees N) and Willapa Bay, Washington (46.6 degrees N). Collections from 13 cruises (176 trawls) from 2004 to 2006 yielded over 17,000,000 micronekton individuals (350,000 excluding euphausiids), representing 76 taxa and 43 families. The community was numerically dominated by euphausiids, followed in decreasing order by midwater shrimp (Sergestes similis), lanternfishes (Myctophidae), late larval/juvenile rockfishes (Sebastes spp.), age-0 Pacific hake (Merluccius productus), and pelagic squid (Abraliopsis felis). We used cluster analysis, ordinations, multi-response permutation procedures (MRPP), and indicator species analysis (ISA) to examine community structure of the 28 dominant taxa. Ordination and cluster results indicated that distance from shore and sea-floor depth best characterized habitats used by different assemblages of the micronekton community. Temperature and salinity at various depths influenced community structure to a lesser extent, along with Ekman transport. MRPP and ISA results indicated that nearly all dominant taxa were associated with cross-shelf gradients. Based upon a comparison between historical samples collected in 1976 and 1981 and comparable trawls from this survey, distinct decadal differences among micronektonic fish assemblages were observed, including more juvenile flatfishes and rockfishes but a lower diversity of mesopelagic fishes, which may be related to interdecadal environmental changes between the two time periods. This study represents the first examination of the relationships between both vertebrate and invertebrate members of the epipelagic nekton community. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Phillips, A. Jason] Oregon State Univ, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA.
[Brodeur, Richard D.; Suntsov, Andrey V.] NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
RP Phillips, AJ (reprint author), 104 COAS Adm Bldg, Corvallis, OR 97331 USA.
EM jphillip@coas.oregonstate.edu
FU NCAA Northwest Fisheries Science Center
FX We wish to thank Toby Auth, Paul Peterson, Jesse Lamb, Paul Bentley, Bob
Emmett, and the crew of the research and fishing vessels that
participated in the cruises and in processing of samples in the
laboratory. We would like to thank Bill Pearcy for providing unpublished
data. Also, we would like to thank Bill Pearcy, Toby Auth, Ed Casillas
and Doug Reese for comments on earlier versions of this manuscript.
Funding for the collection and analysis of the data comes from the NCAA
Northwest Fisheries Science Center and NCAA's Stock Assessment
Improvement Program.
NR 66
TC 12
Z9 12
U1 2
U2 18
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0079-6611
J9 PROG OCEANOGR
JI Prog. Oceanogr.
PD JAN-FEB
PY 2009
VL 80
IS 1-2
BP 74
EP 92
DI 10.1016/j.pocean.2008.12.001
PG 19
WC Oceanography
SC Oceanography
GA 425SO
UT WOS:000264657600004
ER
PT S
AU Golden, JL
Koontz, SL
Christiansen, EL
Graves, RF
Lorenz, MJ
Alred, JW
O'Rourke, MJE
AF Golden, Johnny L.
Koontz, Steven L.
Christiansen, Eric L.
Graves, Russell F.
Lorenz, Mary J.
Alred, John W.
O'Rourke, Mary Jane E.
BE Kleiman, JI
TI Spacecraft Materials in the Space Flight Environment: International
Space Station - May 2002 to May 2008
SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 9th International Conference on Protection of Materials and Structures
from Space Environment
CY MAY 20-23, 2008
CL Toronto, CANADA
SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab
ID LOW-EARTH-ORBIT; FIGURE; MERIT
AB The performance of ISS spacecraft materials and systems on prolonged exposure to the low-Earth orbit (LEO) space flight are reported in this paper. In-flight data, flight crew observations, and the results of ground-based test and analysis directly supporting programmatic and operational decision-making are described. The space flight environments definitions (both natural and induced) used for ISS design, material selection, and verification testing are shown, in most cases, to be more severe than the actual flight environment accounting, in parts for the outstandmig performance of ISS as a long mission duration spacecraft. No significant ISS material or system failures have been attributed to spacecraft-environments interactions. Nonetheless, ISS materials and systems performance data is contributing to our understanding of spacecraft material interactions with the spaceflight environment so as to reduce cost and risk for future spaceflight projects and programs.
C1 [Golden, Johnny L.; Lorenz, Mary J.] Boeing ISS Mat & Proc, Mail Code HB3-20,13100 Space Ctr Blvd, Houston, TX 77059 USA.
[Koontz, Steven L.; Alred, John W.; O'Rourke, Mary Jane E.] NASA, Johnson Space Ctr, Struct Engn Div, Houston, TX 77058 USA.
[Christiansen, Eric L.] NASA, Johnson Space Ctr, Solar Syst Explorat Div, Houston, TX 77058 USA.
[Graves, Russell F.] Boeing ISS Struct Mechanisms, Houston, TX 77059 USA.
RP Golden, JL (reprint author), Boeing ISS Mat & Proc, Mail Code HB3-20,13100 Space Ctr Blvd, Houston, TX 77059 USA.
EM johny.l.golden@boeing.com
NR 81
TC 2
Z9 2
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0619-3
J9 AIP CONF PROC
PY 2009
VL 1087
BP 3
EP +
PG 5
WC Engineering, Aerospace
SC Engineering
GA BIX44
UT WOS:000263582700001
ER
PT S
AU Stambler, AH
Inoshita, KE
Roberts, LM
Barbagallo, CE
de Groh, KK
Banks, BA
AF Stambler, Arielle H.
Inoshita, Karen E.
Roberts, Lily M.
Barbagallo, Claire E.
de Groh, Kim K.
Banks, Bruce A.
BE Kleiman, JI
TI Ground-Laboratory to In-Space Atomic Oxygen Correlation for the PEACE
Polymers
SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 9th International Conference on Protection of Materials and Structures
from Space Environment
CY MAY 20-23, 2008
CL Toronto, CANADA
SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab
AB The Materials International Space Station Experiment 2 (MISSE 2) Polymer Erosion and Contamination Experiment (PEACE) polymers were exposed to the environment of low Earth orbit (LEO) for 3.95 years from 2001 to 2005. There were forty-one different PEACE polymers, which were flown on the exterior of the International Space Station (ISS) in order to determine their atomic oxygen erosion yields. In LEO, atomic oxygen is an environmental durability threat, particularly for long duration mission exposures. Although space flight experiments, such as the MISSE 2 PEACE experiment, are ideal for determining LEO environmental durability of spacecraft materials, ground-laboratory testing is often relied upon for durability evaluation and prediction. Unfortunately, significant differences exist between LEO atomic oxygen exposure and atomic oxygen exposure in ground-laboratory facilities. These differences include variations in species, energies, thermal exposures and radiation exposures, all of which may result in different reactions and erosion rates. In an effort to improve the accuracy of ground-based durability testing, ground-l ab oratory to in-space atomic oxygen correlation experiments have been conducted. In these tests, the atomic oxygen erosion yields of the PEACE polymers were determined relative to Kapton H using a radio-frequency (RF) plasma asher (operated on air). The asher erosion yields were compared to the MISSE 2 PEACE erosion yields to determine the correlation between erosion rates in the two environments. This paper provides a summary of the MISSE 2 PEACE experiment; it reviews the specific polymers tested as well as the techniques used to determine erosion yield in the asher, and it provides a correlation between the space and ground-laboratory erosion yield values. Using the PEACE polymers' asher to in-space erosion yield ratios will allow more accurate in-space materials performance predictions to be made based on plasma asher durability evaluation.
C1 [Stambler, Arielle H.; Inoshita, Karen E.; Roberts, Lily M.; Barbagallo, Claire E.] Hathaway Brown Sch, 19600 N Pk Blvd, Shaker Hts, OH 44122 USA.
[de Groh, Kim K.] NASA, Lewis Res Ctr, Cleveland, OH 44135 USA.
[Banks, Bruce A.] NASA, Lewis Res Ctr, Consultant Alphaport InC, Cleveland, OH 44135 USA.
RP Stambler, AH (reprint author), Hathaway Brown Sch, 19600 N Pk Blvd, Shaker Hts, OH 44122 USA.
EM kim.k.degroh@nasa.gov; bruce.a.banks@nasa.gov
NR 13
TC 3
Z9 3
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0619-3
J9 AIP CONF PROC
PY 2009
VL 1087
BP 51
EP +
PG 3
WC Engineering, Aerospace
SC Engineering
GA BIX44
UT WOS:000263582700003
ER
PT S
AU Kauder, LR
AF Kauder, Lonny R.
BE Kleiman, JI
TI An Improved Formulation for Calorimetric Emittance Testing of Spacecraft
Thermal Control Coatings
SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 9th International Conference on Protection of Materials and Structures
from Space Environment
CY MAY 20-23, 2008
CL Toronto, CANADA
SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab
AB Spacecraft often rely heavily on passive thermal control to maintain operating temperature. An important parameter in the spacecraft heat balance equation is the emittance of thermal control coatings as a function of coating temperature. One method for determining the emittance of spacecraft thermal control from elevated temperature to cryogenic temperatures relies on a calorimetric technique. The fundamental equation governing this test method can be found in numerous places in the literature and although it generally provides reasonable results, its formulation is based on a conceptual flaw that only becomes apparent when the sample temperature approaches the wall temperature during testing. This paper investigates the cause for this error and develops the correct formulation for calorimetric emittance testing. Experimental data will also be presented that illustrates the difference between the two formulations and the resulting difference in the calculated emittance.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kauder, LR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 6
TC 1
Z9 1
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0619-3
J9 AIP CONF PROC
PY 2009
VL 1087
BP 117
EP 123
PG 7
WC Engineering, Aerospace
SC Engineering
GA BIX44
UT WOS:000263582700010
ER
PT S
AU Finckenor, M
AF Finckenor, Miria
BE Kleiman, JI
TI MISSE Thermal Control Materials with Comparison to Previous Flight
SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 9th International Conference on Protection of Materials and Structures
from Space Environment
CY MAY 20-23, 2008
CL Toronto, CANADA
SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab
AB Many different passive thermal control materials were flown as part of the Materials on International Space Station Experiment, including inorganic coatings, anodized aluminum, and multi-layer insulation materials. These and other material samples were exposed to the low Earth orbital environment of atomic oxygen, ultraviolet radiation, thermal cycling, and hard vacuum, though atomic oxygen exposure was limited for some samples. Materials flown on MISSE-1 and MISSE-2 were exposed to the space environment for nearly four years. Materials flown on MISSE-3, MISSE-4, and MISSE-5 were exposed to the space environment for one year.
Solar absorptance, infrared emittance, and mass measurements indicate the durability of these materials to withstand the space environment. Effects of short duration versus long duration exposure on ISS are explored, as well as comparable data from previous flight experiments, such as the Passive Optical Sample Assembly (POSA), Optical Properties Monitor (OPM), and Long Duration Exposure Facility (LDEF).
C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Finckenor, M (reprint author), NASA, George C Marshall Space Flight Ctr, Mail Code EM50, Huntsville, AL 35812 USA.
EM miria.finckenor@nasa.gov
NR 10
TC 1
Z9 1
U1 0
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0619-3
J9 AIP CONF PROC
PY 2009
VL 1087
BP 241
EP 248
PG 8
WC Engineering, Aerospace
SC Engineering
GA BIX44
UT WOS:000263582700021
ER
PT S
AU Jenkins, PP
Walters, RJ
Krasowski, MJ
Chapman, JJ
Ballard, PG
Vasquez, JA
Mahony, DR
LaCava, SN
Braun, WR
Skalitzky, R
Prokop, NF
Flatico, JM
Greer, LC
Gibson, KB
Kinard, WH
Pippin, HG
AF Jenkins, Phillip P.
Walters, Robert J.
Krasowski, Michael J.
Chapman, John J.
Ballard, Perry. G.
Vasquez, John A.
Mahony, Denis R.
LaCava, Susie N.
Braun, William R.
Skalitzky, Robert
Prokop, Norman F.
Flatico, Joseph M.
Greer, Lawrence C.
Gibson, Karen B.
Kinard, William H.
Pippin, H. Gary
BE Kleiman, JI
TI MISSE7: Building a Permanent Environmental Testbed for the International
Space Station
SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 9th International Conference on Protection of Materials and Structures
from Space Environment
CY MAY 20-23, 2008
CL Toronto, CANADA
SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab
AB The Materials on the International Space Station Experiments (MISSE) provide low-cost material exposure experiments on the exterior of the International Space Station (ISS). The original concept for a suitcase-like box bolted to the ISS to passively expose materials to space has grown to include increasingly complex in situ characterization. As the ISS completes construction, the facilities available to MISSE experiments will increase dramatically. MISSE7 is the first MISSE to take advantage of this new infrastructure. In addition to material exposure, MISSE7 will include characterization of single-event radiation effects on electronics and solar cell performance in LEO. MISSE7 will exploit the ISS Express Logistics Carrier power and data capabilities and will leave behind a MISSE specific infrastructure for future missions.
C1 [Jenkins, Phillip P.; Walters, Robert J.; Vasquez, John A.; LaCava, Susie N.; Braun, William R.; Skalitzky, Robert] USN, Res Lab, Washington, DC 20375 USA.
[Krasowski, Michael J.; Prokop, Norman F.; Greer, Lawrence C.] NASA, Glenn Res Ctr, Cleveland, OH USA.
[Chapman, John J.; Gibson, Karen B.; Kinard, William H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Ballard, Perry. G.] NASA, Johnson Space Ctr, Houston, TX USA.
[Mahony, Denis R.] Praxis Inc, Alexandria, VA USA.
[Flatico, Joseph M.] Ohio Aerosp Inst, Brookpark, OH USA.
[Pippin, H. Gary] Boeing Phantom Works, Seattle, WA USA.
RP Jenkins, PP (reprint author), USN, Res Lab, Washington, DC 20375 USA.
NR 9
TC 7
Z9 7
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0619-3
J9 AIP CONF PROC
PY 2009
VL 1087
BP 273
EP +
PG 2
WC Engineering, Aerospace
SC Engineering
GA BIX44
UT WOS:000263582700023
ER
PT S
AU Miller, SKR
Banks, BA
Tollis, G
AF Miller, Sharon K. R.
Banks, Bruce A.
Tollis, Greg
BE Kleiman, JI
TI MISSE Results used for RF Plasma Ground Testing-to-space-exposure
Correlation for Coated Kapton
SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 9th International Conference on Protection of Materials and Structures
from Space Environment
CY MAY 20-23, 2008
CL Toronto, CANADA
SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab
AB The ability to predict the durability of materials in the low Earth orbit (LEO) environment by exposing them in ground-based facilities is important because one can achieve test results sooner, expose more types of materials, and do it much more cost effectively than to test them in flight. However, flight experiments to determine the durability of groups or classes of materials that behave similarly are needed in order to provide correlations of how much time in ground-based facilities represents certain durations in LEO for the material type of interest. An experiment was designed and flown on the Materials International Space Station Experiment (MISSE) 2 (3.95 years in LEO) and MISSE 4 (1.04 years in LEO) in order to develop this type of correlation between ground-based RF plasma exposure and LEO exposure for coated Kapton. The experiment consisted of a sample of Kapton H (R) (DuPont) polyimide coated with 1300 Angstroms of silicon dioxide by Sheldahl Inc. The samples were exposed to atomic oxygen in a radio frequency (RF) generated atomic oxygen plasma. Mass change was measured for the samples and then the same samples were exposed in flight on MISSE and the mass change was again recorded post-flight. After documentation, the samples were exposed again in the ground-based RF plasma in order to determine if the erosion would be the same as it had been in the same facility pre-flight which would indicate whether or not the sample had been damaged during flight and if the defects on the surface were those that were there pre-flight. The slopes of the mass change versus fluence plots were then used to develop a correlation factor that can be used to help predict the durability of coated Kapton in ground-based isotropic atomic oxygen plasma systems. This paper describes the experiment and presents the correlation factor results.
C1 [Miller, Sharon K. R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Banks, Bruce A.] NASA, Consultant Alphaport Supporting, Washington, DC USA.
[Tollis, Greg] Cleveland State Univ, Cleveland, OH 44115 USA.
RP Miller, SKR (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM sharon.k.miller@nasa.gov
NR 10
TC 1
Z9 1
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0619-3
J9 AIP CONF PROC
PY 2009
VL 1087
BP 277
EP +
PG 2
WC Engineering, Aerospace
SC Engineering
GA BIX44
UT WOS:000263582700024
ER
PT S
AU Watson, KA
Ghose, S
Lillehei, PT
Smith, JG
Connell, JW
AF Watson, K. A.
Ghose, S.
Lillehei, P. T.
Smith, J. G., Jr.
Connell, J. W.
BE Kleiman, JI
TI Effect of LEO Exposure on Aromatic Polymers Containing Phenylphosphine
Oxide Groups
SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 9th International Conference on Protection of Materials and Structures
from Space Environment
CY MAY 20-23, 2008
CL Toronto, CANADA
SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab
ID POLY(ARYLENE ETHER HETEROCYCLE)S; ATOMIC OXYGEN EXPOSURE; CONTAINING
POLYIMIDES; PLASMA; FILMS; COPOLYMERS
AB As part of the Materials on The International Space Station Experiment (MISSE), aromatic polymers containing phenylphosphine oxide groups were exposed to low Earth orbit for similar to 4 years. All of the aromatic polymers containing phenylphosphine oxide groups survived the exposure despite the high fluence of atomic oxygen that completely eroded other polymer films such as Kapton (R) and Mylar (R) of comparable or greater thickness. The samples were characterized for changes in physical properties, thermal/optical properties surface chemistry, and surface topography. The data from the polymer samples on MISSE were compared to samples from the same batch of material stored under ambient conditions on Earth. In addition, comparisons were made between the MISSE samples and those subjected to shorter term space flight exposures. The results of these analyses will be presented.
C1 [Watson, K. A.; Ghose, S.] Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
[Lillehei, P. T.; Smith, J. G., Jr.; Connell, J. W.] Natl Aeronaut & Space Adm, Langley Res Ctr, Hampton, VA 23681 USA.
RP Watson, KA (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
NR 32
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0619-3
J9 AIP CONF PROC
PY 2009
VL 1087
BP 291
EP +
PG 3
WC Engineering, Aerospace
SC Engineering
GA BIX44
UT WOS:000263582700025
ER
PT S
AU Banks, BA
de Groh, KK
Miller, SK
Waters, DL
AF Banks, Bruce A.
de Groh, Kim K.
Miller, Sharon K.
Waters, Deborah L.
BE Kleiman, JI
TI Lessons Learned from Atomic Oxygen Interaction with Spacecraft Materials
in Low Earth Orbit
SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 9th International Conference on Protection of Materials and Structures
from Space Environment
CY MAY 20-23, 2008
CL Toronto, CANADA
SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab
ID RADIATION; FEP
AB There have been five Materials International Space Station Experiment (MISSE) passive experiment carriers (PECs) (MISSE 1-5) to date which have been launched, exposed in space on the exterior of International Space Station (ISS) and then returned to Earth for analysis. An additional four MISSE PECs (MISSE 6A, 6B, 7A & 7B) are in various stages of completion. The PECs are two-sided suitcase size sample carriers that are intended to provide information on the effects of the low Earth orbital environment on a wide variety of materials and components. As a result of post retrieval analyses of the retrieved MISSE 2 experiments and numerous prior space experiments, there have been valuable lessons learned and needs identified that are worthy of being documented so that planning, design, and analysis of future space environment experiments can benefit from the experience in order to maximize the knowledge gained. Some of the lessons learned involve the techniques, concepts, and issues associated with measuring atomic oxygen erosion yields. These are presented along with several issues to be considered when designing experiments, such as the uncertainty in mission duration, scattering and contamination effects on results, and the accuracy of measuring atomic oxygen erosion.
C1 [Banks, Bruce A.; de Groh, Kim K.; Miller, Sharon K.] NASA, Glenn Res Ctr, MS 309-2,21000 Brookpk Rd, Cleveland, OH 44135 USA.
[Waters, Deborah L.] Arctic Slope Reg Corp, Barrow, AL 99723 USA.
RP Banks, BA (reprint author), NASA, Glenn Res Ctr, MS 309-2,21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Bruce.A.Banks@nasa.gov
NR 19
TC 3
Z9 3
U1 0
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0619-3
J9 AIP CONF PROC
PY 2009
VL 1087
BP 312
EP +
PG 4
WC Engineering, Aerospace
SC Engineering
GA BIX44
UT WOS:000263582700027
ER
PT S
AU Edwards, DL
Cooke, W
Suggs, R
Moser, DE
AF Edwards, David L.
Cooke, William
Suggs, Rob
Moser, Danielle E.
BE Kleiman, JI
TI Analysis of Regolith Simulant Ejecta Distributions from Normal Incident
Hypervelocity Impact
SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 9th International Conference on Protection of Materials and Structures
from Space Environment
CY MAY 20-23, 2008
CL Toronto, CANADA
SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab
AB The National Aeronautics and Space Administration (NASA) has established the Constellation Program. The Constellation Program has defined one of its many goals as long-term lunar habitation. Critical to the design of a lunar habitat is an understanding of the lunar surface environment; of specific importance is the primary meteoroid and subsequent ejecta environment. The document, NASA SP-8013 "Meteoroid Environment Model Near Earth to Lunar Surface", was developed for the Apollo program in 1969 and contains the latest definition of the lunar ejecta environment. There is concern that NASA SP-8013 may overestimate the lunar ejecta environment. NASA's Meteoroid Environment Office (MEO) has initiated several tasks to improve the accuracy of our understanding of the lunar surface ejecta environment.
This paper reports the results of experiments on projectile impact into powdered pumice and unconsolidated JSC-1A Lunar Mare Regolith simulant targets. Projectiles were accelerated to velocities between 2.45 and 5.18 km/s and impacted the targets at normal incidence using the Ames Vertical Gun Range (AVGR). The ejected particles were detected by thin aluminum foil targets strategically placed around the impact site and angular ejecta distributions were determined. Assumptions were made to support the analysis which include; assuming ejecta spherical symmetry resulting from normal impact and all ejecta particles were of mean target particle size. This analysis produces a hemispherical flux density distribution of ejecta with sufficient velocity to penetrate the aluminum foil detectors.
C1 [Edwards, David L.; Cooke, William; Suggs, Rob] NASA, George C Marshall Space Flight Ctr, M-S EV44 MSFC, Huntsville, AL 35812 USA.
RP Edwards, DL (reprint author), NASA, George C Marshall Space Flight Ctr, M-S EV44 MSFC, Huntsville, AL 35812 USA.
NR 4
TC 0
Z9 0
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0619-3
J9 AIP CONF PROC
PY 2009
VL 1087
BP 559
EP +
PG 2
WC Engineering, Aerospace
SC Engineering
GA BIX44
UT WOS:000263582700050
ER
PT S
AU Kleiman, JI
Iskanderova, Z
Issoupov, V
Grigorevskiy, AV
Kiseleva, LV
Finckenor, M
Naumov, SF
Sokolova, SP
Kurilenok, AO
AF Kleiman, J. I.
Iskanderova, Z.
Issoupov, V.
Grigorevskiy, A. V.
Kiseleva, L. V.
Finckenor, M.
Naumov, S. F.
Sokolova, S. P.
Kurilenok, A. O.
BE Kleiman, JI
TI The Results of Ground-based and In-flight Testing of Charge-dissipative
and Conducting EKOM Thermal Control Paints
SO PROTECTION OF MATERIALS AND STRUCTURES FROM SPACE ENVIRONMENT
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 9th International Conference on Protection of Materials and Structures
from Space Environment
CY MAY 20-23, 2008
CL Toronto, CANADA
SP Canadian Space Agcy, Montana State Univ, Univ Toronto Inst Aerospac Studies, Integr Testing Lab
ID SURFACE MODIFICATION; SPACE DURABILITY; ENHANCEMENT
AB An international program on comparative evaluation of space durability of thermal control paints from a number of countries was initiated a few years ago at ITL with coatings from Russia, France and USA being studied. This paper describes the results of the study on space durability of three types of charge-dissipative and conductive Russian advanced polymer-based EKOM thermal control paints. Extensive ground-based testing in fast atomic oxygen (FAO) beam facilities was used to test the space durability of these paints and the enhancement of their atomic oxygen erosion resistance by a surface modification technology, Photosil (TM). All pristine EKOM paints were also tested in a direct materials exposure experiment on Russian module "Zvezda" onboard the International Space Station.
Space durability and change of the major physical properties were evaluated after these experiments using a number of analytical techniques. Both, the ground-based testing and the flight experiments indicated signs of surface erosion with some changes of thermal optical properties. Therefore, the paints were also modified by a surface treatment technology, Photosil (TM), to increase their erosion resistance to atomic oxygen, tested in the same ground-based FAO facilities up to high FAO fluencies and compared with testing results of pristine materials.
The comparison indicated that the surface-modified paints exhibit reduced mass loss, full stabilization and no surface morphology changes, thus indicating at full protection from the high FAO fluencies. It was demonstrated that the developed surface modification treatment could be applied successfully to charge dissipative and conductive paints, to enhance the low Earth orbit (LEO) environment resistance of external thermal control coatings in long-term space missions.
C1 [Kleiman, J. I.; Iskanderova, Z.; Issoupov, V.] Integr Testing Lab Inc, Markham, ON, Canada.
[Grigorevskiy, A. V.; Kiseleva, L. V.] JSC Kompozit Korolev, Moscow, Russia.
[Finckenor, M.] NASA, Marshall Space Fight Ctr, Huntsville, AL 35811 USA.
[Naumov, S. F.; Sokolova, S. P.; Kurilenok, A. O.] RSC Energia Korolev, Moscow, Russia.
RP Kleiman, JI (reprint author), Integr Testing Lab Inc, Markham, ON, Canada.
EM ziskanderova@itlinc.com
NR 10
TC 0
Z9 0
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0619-3
J9 AIP CONF PROC
PY 2009
VL 1087
BP 610
EP +
PG 3
WC Engineering, Aerospace
SC Engineering
GA BIX44
UT WOS:000263582700056
ER
PT S
AU Hays, CC
Kulleck, JG
Haines, BE
Narayan, SR
AF Hays, C. C.
Kulleck, J. G.
Haines, B. E.
Narayan, S. R.
BE Fuller, T
Uchida, H
Strasser, P
Shirvanian, P
Lamy, C
Hartnig, C
Gasteiger, HA
Zawodzinski, T
Jarvi, T
Bele, P
Ramani, V
Cleghorn, S
Jones, D
Zelenay, P
TI Thin Film Platinum Alloys For Use As Catalyst Materials In Fuel Cells
SO PROTON EXCHANGE MEMBRANE FUEL CELLS 9
SE ECS Transactions
LA English
DT Proceedings Paper
CT 9th Proton Exchange Membrane Fuel Cell Symposium (PEMFC) Conducted Under
the Auspices of the 216th Meeting of the Electrochemical-Society-Inc
CY OCT 04-09, 2009
CL Vienna, AUSTRIA
SP Electrochem Soc Inc, Electrochem Soc, Energy Technol Div, Electrochem Soc, Ind Electrochemistry & Electrochem Engn, Electrochem Soc, Phys & Analyt Electrochemistry Div, Electrochem Soc, Battery Div, Automot Fuel Cell Cooperat Corp, Ion Power, N E Chemcat Corp, Pine Res Instrumentat Inc, Tanaka Kikinzoku Kogyo, Toyota Motor Engn & Mfg Amer, Tokuyama Corp, Umicore AG & Co KG, UTC Power Corp
AB Measurements of the structural and electrochemical properties of nanostructured thin film alloys in the ternary series Pt-Co-Zr are presented. These alloys have been studied to determine the influence of early transition metal element additions on the catalytic response and chemical stability of platinum-group-metal (PGM) alloys in acid electrolytes. The thin film compositions in the Pt-Co-Zr system were prepared via co-sputtering and the films exhibit a (111) crystallographic orientation. Alloys with Pt-metal contents of less than 50 At. % are stable in 0.1 M perchloric acid electrolytes, and are electrochemically active for the oxygen reduction reaction (ORR). The ORR kinetic currents at 0.9 V are comparable to Pt. The alloys have been cycled over the range 0.0 to 1.2 V NHE, with no degradation of the electrode surface area or decrease in electrochemical performance observed. Our results suggest that Pt-Co-Zr alloys with reduced PGM contents may be competitive with Pt-catalysts.
C1 [Hays, C. C.; Kulleck, J. G.; Haines, B. E.; Narayan, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hays, CC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 2
TC 0
Z9 0
U1 0
U2 3
PU ELECTROCHEMICAL SOC INC
PI PENNINGTON
PA 65 S MAIN ST, PENNINGTON, NJ 08534-2839 USA
SN 1938-5862
BN 978-1-60768-088-8
J9 ECS TRANSACTIONS
PY 2009
VL 25
IS 1
BP 619
EP 623
DI 10.1149/1.3210613
PG 5
WC Electrochemistry; Energy & Fuels
SC Electrochemistry; Energy & Fuels
GA BJQ12
UT WOS:000329585500060
ER
PT S
AU Valdez, TI
Billings, KJ
Sakamoto, J
Mansfeld, F
Narayanan, SR
AF Valdez, Thomas I.
Billings, Keith J.
Sakamoto, Jeff
Mansfeld, Florian
Narayanan, S. R.
BE Fuller, T
Uchida, H
Strasser, P
Shirvanian, P
Lamy, C
Hartnig, C
Gasteiger, HA
Zawodzinski, T
Jarvi, T
Bele, P
Ramani, V
Cleghorn, S
Jones, D
Zelenay, P
TI Iridium and Lead Doped Ruthenium Oxide Catalysts for Oxygen Evolution
SO PROTON EXCHANGE MEMBRANE FUEL CELLS 9
SE ECS Transactions
LA English
DT Proceedings Paper
CT 9th Proton Exchange Membrane Fuel Cell Symposium (PEMFC) Conducted Under
the Auspices of the 216th Meeting of the Electrochemical-Society-Inc
CY OCT 04-09, 2009
CL Vienna, AUSTRIA
SP Electrochem Soc Inc, Electrochem Soc, Energy Technol Div, Electrochem Soc, Ind Electrochemistry & Electrochem Engn Div, Electrochem Soc, Phys & Analyt Electrochemistry Div, Electrochem Soc, Battery Div, Automot Fuel Cell Cooperat Corp, Ion Power, N E Chemcat Corp, Pine Res Instrumentat Inc, Tanaka Kikinzoku Kogyo, Toyota Motor Engn & Mfg Amer, Tokuyama Corp, Umicore AG & Co KG, UTC Power Corp
ID SOLID POLYMER ELECTROLYTE; WATER ELECTROLYSIS; ANODIC EVOLUTION;
ELECTROCATALYSIS; SURFACES
AB The performance of various ruthenium oxide-based oxygen evolution catalysts fabricated by various techniques has been studied. A thermal processing technique has been identified that can produce stable iridium and lead-doped ruthenium oxide catalysts. The best performance for the oxygen evolution reaction was obtained with iridium-doped ruthenium oxide catalyst containing nine-mole percent iridium. The cell voltage of the Ir(9%)-d-RuO2 catalyst at an applied current density of 200-mA/cm(2) was 1.45 Volts at 70 degrees C. The oxygen evolution Tafel slopes for the doped ruthenium oxide catalysts were in the range of 40 to 55-mV/decade.
C1 [Valdez, Thomas I.; Billings, Keith J.; Sakamoto, Jeff; Narayanan, S. R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Mansfeld, Florian] Univ So Calif, Los Angeles, CA 90089 USA.
RP Valdez, TI (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 15
TC 7
Z9 7
U1 0
U2 1
PU ELECTROCHEMICAL SOC INC
PI PENNINGTON
PA 65 S MAIN ST, PENNINGTON, NJ 08534-2839 USA
SN 1938-5862
BN 978-1-60768-088-8
J9 ECS TRANSACTIONS
PY 2009
VL 25
IS 1
BP 1371
EP 1382
DI 10.1149/1.3210693
PG 12
WC Electrochemistry; Energy & Fuels
SC Electrochemistry; Energy & Fuels
GA BJQ12
UT WOS:000329585500140
ER
PT J
AU Petrov, L
Phillips, C
Bertarini, A
Deller, A
Pogrebenko, S
Mujunen, A
AF Petrov, Leonid
Phillips, Chris
Bertarini, Alessandra
Deller, Adam
Pogrebenko, Sergei
Mujunen, Ari
TI Use of the Long Baseline Array in Australia for Precise Geodesy and
Absolute Astrometry
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
LA English
DT Article
DE instrumentation: interferometers; techniques: interferometric; reference
systems
ID VLBA CALIBRATOR SURVEY; HIGHER RADIO FREQUENCIES; INTERFEROMETRY; ICRF;
TITAN
AB We report the results of a successful 12-hour 22-GHz VLBI experiment using a heterogeneous network that includes radio telescopes of the Long Baseline Array (LBA) in Australia and several VLBI stations that regularly observe in geodetic VLBI campaigns. We have determined positions of three VLBI stations, ATCA-104, CEDUNA and MOPRA, with an accuracy of 4-30 mm using a novel technique of data analysis. These stations have never before participated in geodetic experiments. We observed 105 radio sources, and amongst them 5 objects which have not previously been observed with VLBI. We have determined positions of these new sources with the accuracy of 2-5 mas. We make the conclusion that the LBA network is capable of conducting absolute astrometry VLBI surveys with an accuracy better than 5 mas.
C1 [Petrov, Leonid] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA.
[Bertarini, Alessandra] Inst Geodesy & Geoinformat, Bonn, Germany.
[Deller, Adam] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3123, Australia.
[Mujunen, Ari] Helsinki Univ Technol, TKK, Metsahovi Radio Observ, FIN-02150 Espoo, Finland.
RP Petrov, L (reprint author), NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Code 610-2, Greenbelt, MD 20771 USA.
EM Leonid.Petrov@lpetrov.net
OI Deller, Adam/0000-0001-9434-3837
FU European Commission [026642]
FX EXPReS is an Integrated Infrastructure Initiative (I3), funded under the
European Commission's Sixth Framework Programme (FP6), contract number
026642, from March 2006 through February 2009. We greatly appreciate
Alan Fey and Roopesh Ojha who made digital images in FITS format from
the surveys publicly available and Robert Campbell for performing the
highly non-standard test correlations of LBA data at the JIVE
correlator.
NR 31
TC 5
Z9 5
U1 0
U2 1
PU CSIRO PUBLISHING
PI COLLINGWOOD
PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA
SN 1323-3580
J9 PUBL ASTRON SOC AUST
JI Publ. Astron. Soc. Aust.
PY 2009
VL 26
IS 1
BP 75
EP 84
DI 10.1071/AS08030
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 427EI
UT WOS:000264762200009
ER
PT J
AU Shaddock, DA
AF Shaddock, D. A.
TI An Overview of the Laser Interferometer Space Antenna
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
LA English
DT Article
DE gravitational waves; techniques: interferometric
ID FREQUENCY STABILIZATION; LISA ARM; LOCKING; DELAY
AB The Laser Interferometer Space Antenna (LISA) will detect gravitational waves with frequencies from 0.1 mHz to 1 Hz. This article provides a brief overview of LISA's science goals followed by a tutorial of the LISA measurement concept.
C1 [Shaddock, D. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Shaddock, D. A.] Australian Natl Univ, Ctr Gravitat Phys, Canberra, ACT 0200, Australia.
RP Shaddock, DA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM daniel.shaddock@jpl.nasa.gov
RI Shaddock, Daniel/A-7534-2011
OI Shaddock, Daniel/0000-0002-6885-3494
FU Australian Research Council [DP0666437]
FX I would like to thank the Astronomical Society of Australia for the
invitation to submit this paper as a result of an invited talk at the
ASM. The work reported on here is a summary of the work of the LISA
community and I gratefully acknowledge the hard work of many researchers
around the world. Parts of this research were performed at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. This
research was also supported by the Australian Research Council's
Discovery Projects funding scheme (project number DP0666437).
NR 27
TC 7
Z9 7
U1 0
U2 2
PU CSIRO PUBLISHING
PI COLLINGWOOD
PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA
SN 1323-3580
J9 PUBL ASTRON SOC AUST
JI Publ. Astron. Soc. Aust.
PY 2009
VL 26
IS 2
BP 128
EP 132
DI 10.1071/AS08059
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 462MS
UT WOS:000267358100004
ER
PT J
AU Sterling, NC
Dinerstein, HL
Hwang, S
Redfield, S
Aguilar, A
Witthoeft, MC
Esteves, D
Kilcoyne, ALD
Bautista, M
Phaneuf, R
Bilodeau, RC
Ballance, CP
McLaughlin, B
Norrington, PH
AF Sterling, N. C.
Dinerstein, H. L.
Hwang, S.
Redfield, S.
Aguilar, A.
Witthoeft, M. C.
Esteves, D.
Kilcoyne, A. L. D.
Bautista, M.
Phaneuf, R.
Bilodeau, R. C.
Ballance, C. P.
McLaughlin, B.
Norrington, P. H.
TI Improved Neutron-Capture Element Abundances in Planetary Nebulae
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
LA English
DT Article
DE planetary nebulae: general; nuclear reactions, nucleosynthesis,
abundances; stars: AGB and post-AGB; atomic data
ID ASYMPTOTIC GIANT BRANCH; S-PROCESS ABUNDANCES; R-MATRIX METHOD;
CHEMICAL-COMPOSITION; ELECTRON-SCATTERING; STARS; NUCLEOSYNTHESIS;
IDENTIFICATION; NGC-7027; KRYPTON
AB Spectroscopy of planetary nebulae (PNe) provides the means to investigate s-process enrichments of neutron(n)-capture elements that cannot be detected in Asymptotic Giant Branch (AGB) stars. However, accurate abundance determinations of these elements present a challenge. Corrections for unobserved ions can be large and uncertain, since in many PNe only one ion of a given n-capture element has been detected. Furthermore, the atomic data governing the ionization balance of these species are not well-determined, inhibiting the derivation of accurate ionization corrections. We present initial results of a program that addresses these challenges. Deep high-resolution optical spectroscopy of similar to 20 PNe has been performed to detect emission lines from trans-iron species including Se, Br, Kr, Rb and Xe. The optical spectral region provides access to multiple ions of these elements, which reduces the magnitude and importance of uncertainties in the ionization corrections. In addition, experimental and theoretical efforts are providing determinations of the photoionization cross sections and recombination rate coefficients of Se, Kr and Xe ions. These new atomic data will make it possible to derive robust ionization corrections for these elements. Together, our observational and atomic data results will enable n-capture element abundances to be determined with unprecedented accuracy in ionized nebulae.
C1 [Sterling, N. C.; Witthoeft, M. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dinerstein, H. L.; Hwang, S.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Redfield, S.] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA.
[Aguilar, A.; Kilcoyne, A. L. D.; Bilodeau, R. C.] Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94270 USA.
[Esteves, D.; Phaneuf, R.] Univ Nevada, Dept Phys, Reno, NV 89557 USA.
[Bautista, M.] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA.
[Ballance, C. P.] Auburn Univ, Dept Phys, Auburn, AL USA.
[McLaughlin, B.; Norrington, P. H.] Queens Univ Belfast, Sch Math & Phys, Ctr Atom Mol & Opt Phys, Belfast BT7 1NN, Antrim, North Ireland.
RP Sterling, NC (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
EM nicholas.c.sterling@nasa.gov
RI Kilcoyne, David/I-1465-2013;
OI Bilodeau, Rene/0000-0001-8607-2328; Redfield, Seth/0000-0003-3786-3486
FU US National Science Foundation [AST 0708245, 0406809]; US DOE
[DE-FG02-05R54819, DE-FG02-99ER54367]; NASA [06-APRA206-0049]
FX We gratefully acknowledge J. Bizau, who sent us experimental PI cross
section data for Xe3+ through Xe6+. N.C.S. is
supported by an appointment to the NASA Post-doctoral Program,
administered by Oak Ridge Associated Universities through a contract
with NASA. B. M. M. acknowledges support by the US National Science
Foundation through a grant to ITAMP at the Harvard-Smithsonian Center
for Astrophysics. C. P. B. is supported by US DOE grants
DE-FG02-05R54819 and DE-FG02-99ER54367. The DARC computations were
conducted at the National Energy Research Scientific Computing Center in
Oakland, CA. This work has been partially supported by NASA grant
06-APRA206-0049 and NSF grants AST 0708245 and 0406809.
NR 31
TC 19
Z9 19
U1 0
U2 2
PU CSIRO PUBLISHING
PI COLLINGWOOD
PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA
SN 1323-3580
J9 PUBL ASTRON SOC AUST
JI Publ. Astron. Soc. Aust.
PY 2009
VL 26
IS 3
BP 339
EP 344
DI 10.1071/AS08067
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 498ID
UT WOS:000270131300035
ER
PT J
AU Lawrence, JS
Ashley, MCB
Bailey, J
Navascues, DBY
Bedding, TR
Bland-Hawthorn, J
Bond, I
Boulanger, F
Bouwens, R
Bruntt, H
Bunker, A
Burgarella, D
Burton, MG
Busso, M
Coward, D
Cioni, MR
Durand, G
Eiroa, C
Epchtein, N
Gehrels, N
Gillingham, P
Glazebrook, K
Haynes, R
Kiss, L
Lagage, PO
Le Bertre, T
Mackay, C
Maillard, JP
McGrath, A
Minier, V
Mora, A
Olsen, K
Persi, P
Pimbblet, K
Quimby, R
Saunders, W
Schmidt, B
Stello, D
Storey, JWV
Tinney, C
Tremblin, P
Wheeler, JC
Yock, P
AF Lawrence, J. S.
Ashley, M. C. B.
Bailey, J.
Barrado y Navascues, D.
Bedding, T. R.
Bland-Hawthorn, J.
Bond, I.
Boulanger, F.
Bouwens, R.
Bruntt, H.
Bunker, A.
Burgarella, D.
Burton, M. G.
Busso, M.
Coward, D.
Cioni, M. -R.
Durand, G.
Eiroa, C.
Epchtein, N.
Gehrels, N.
Gillingham, P.
Glazebrook, K.
Haynes, R.
Kiss, L.
Lagage, P. O.
Le Bertre, T.
Mackay, C.
Maillard, J. P.
McGrath, A.
Minier, V.
Mora, A.
Olsen, K.
Persi, P.
Pimbblet, K.
Quimby, R.
Saunders, W.
Schmidt, B.
Stello, D.
Storey, J. W. V.
Tinney, C.
Tremblin, P.
Wheeler, J. C.
Yock, P.
TI The Science Case for PILOT I: Summary and Overview
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
LA English
DT Editorial Material
DE cosmology: observations; early universe; instrumentation: high angular
resolution; site testing; stars: formation; telescopes
ID INFRARED SKY BRIGHTNESS; SPITZER-SPACE-TELESCOPE; HIGH-ANTARCTIC
PLATEAU; DOME-C; SOUTH-POLE; RADIO OBSERVATIONS; ASTRONOMY; ARRAY;
TURBULENCE; UNIVERSE
AB PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. Conditions at Dome C are known to be exceptional for astronomy. The seeing (above similar to 30m height), coherence time, and isoplanatic angle are all twice as good as at typical mid-latitude sites, while the water-vapour column, and the atmosphere and telescope thermal emission are all an order of magnitude better. These conditions enable a unique scientific capability for PILOT, which is addressed in this series of papers. The current paper presents an overview of the optical and instrumentation suite for PILOT and its expected performance, a summary of the key science goals and observational approach for the facility, a discussion of the synergies between the science goals for PILOT and other telescopes, and a discussion of the future of Antarctic astronomy. Paper II and Paper III present details of the science projects divided, respectively, between the distant Universe (i.e. studies of first light, and the assembly and evolution of structure) and the nearby Universe (i.e. studies of Local Group galaxies, the Milky Way, and the Solar System).
C1 [Lawrence, J. S.; Ashley, M. C. B.; Bailey, J.; Burton, M. G.; Storey, J. W. V.; Tinney, C.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Barrado y Navascues, D.] Lab Astrofis Espacial & Fis Fundamental INTA, Madrid 28080, Spain.
[Bedding, T. R.; Bland-Hawthorn, J.; Bruntt, H.; Kiss, L.; Stello, D.] Univ Sydney, Sch Phys, Inst Astron, Sydney, NSW 2006, Australia.
[Bond, I.] Massey Univ, Auckland 0745, New Zealand.
[Boulanger, F.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Bouwens, R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Bunker, A.; Gillingham, P.; Haynes, R.; McGrath, A.; Saunders, W.] Anglo Australian Observ, Epping, NSW 1710, Australia.
[Busso, M.] Univ Perugia, Dept Phys, I-06123 Perugia, Italy.
[Burgarella, D.] Univ Aix Marseille, Observ Astron Marseille Provence, F-13388 Marseille, France.
[Coward, D.] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia.
[Cioni, M. -R.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Durand, G.; Lagage, P. O.; Minier, V.; Tremblin, P.] CEA Saclay, Serv Astrophys, F-91191 Saclay, France.
[Eiroa, C.; Mora, A.] Univ Autonoma Madrid, Dept Fis Teor C 11, E-28049 Madrid, Spain.
[Epchtein, N.] UNSA, CNRS Fizeau, F-06108 Nice, France.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Glazebrook, K.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Le Bertre, T.] Observ Paris, F-75014 Paris, France.
[Mackay, C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HE, England.
[Maillard, J. P.] Inst Astrophys, F-75014 Paris, France.
[Olsen, K.] Natl Opt Astron Observ, Kitt Peak Natl Observ, Tucson, AZ 85719 USA.
[Persi, P.] Ist Astrofis Spaziale & Fis Cosm INAF, I-00100 Rome, Italy.
[Pimbblet, K.] Univ Queensland, Dept Phys, Brisbane, Qld 4072, Australia.
[Quimby, R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Yock, P.] Univ Auckland, Auckland 1142, New Zealand.
RP Lawrence, JS (reprint author), Macquarie Univ, Dept Phys & Engn, N Ryde, NSW 2109, Australia.
EM jsl@science.mq.edu.au
RI Gehrels, Neil/D-2971-2012; Glazebrook, Karl/N-3488-2015; Barrado
Navascues, David/C-1439-2017; Busso, Maurizio Maria/K-7075-2015;
OI Glazebrook, Karl/0000-0002-3254-9044; Barrado Navascues,
David/0000-0002-5971-9242; Busso, Maurizio Maria/0000-0001-8944-5820;
Burton, Michael/0000-0001-7289-1998; Schmidt, Brian/0000-0001-6589-1287;
Tremblin, Pascal/0000-0001-6172-3403; Tinney,
Christopher/0000-0002-7595-0970
NR 82
TC 10
Z9 11
U1 0
U2 4
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1323-3580
EI 1448-6083
J9 PUBL ASTRON SOC AUST
JI Publ. Astron. Soc. Aust.
PY 2009
VL 26
IS 4
BP 379
EP 396
DI 10.1071/AS08048
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 514SM
UT WOS:000271415900001
ER
PT J
AU Lawrence, JS
Ashley, MCB
Bunker, A
Bouwens, R
Burgarella, D
Burton, MG
Gehrels, N
Glazebrook, K
Pimbblet, K
Quimby, R
Saunders, W
Storey, JWV
Wheeler, JC
AF Lawrence, J. S.
Ashley, M. C. B.
Bunker, A.
Bouwens, R.
Burgarella, D.
Burton, M. G.
Gehrels, N.
Glazebrook, K.
Pimbblet, K.
Quimby, R.
Saunders, W.
Storey, J. W. V.
Wheeler, J. C.
TI The Science Case for PILOT II: the Distant Universe
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
LA English
DT Review
DE early universe; cosmology: observations; galaxies: clusters: general;
galaxies: high-redshift; large-scale structure of universe; supernovae:
general; telescopes
ID GAMMA-RAY BURST; COLOR-DENSITY RELATION; HIGH-REDSHIFT UNIVERSE; GALAXY
STAR-FORMATION; DOME-C; MASSIVE GALAXIES; POPULATION-III; IA SUPERNOVAE;
1ST STARS; ENVIRONMENTAL DEPENDENCE
AB PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. The atmospheric conditions at Dome C deliver a high sensitivity, high photometric precision, wide-field, high spatial resolution, and high-cadence imaging capability to the PILOT telescope. These capabilities enable a unique scientific potential for PILOT, which is addressed in this series of papers. The current paper presents a series of projects dealing with the distant (redshift > 1) Universe, that have been identified as key science drivers for the PILOT facility. The potential for PILOT to detect the first populations of stars to form in the early Universe, via infrared projects searching for pair-instability supernovae and gamma-ray burst afterglows, is investigated. Two projects are proposed to examine the assembly and evolution of structure in the Universe: an infrared survey searching for the first evolved galaxies at high redshift, and an optical survey aimed at characterising moderate-redshift galaxy clusters. Finally, a large-area weak-lensing survey and a program to obtain supernova infrared light-curves are proposed to examine the nature and evolution of dark energy and dark matter.
C1 [Lawrence, J. S.; Ashley, M. C. B.; Burton, M. G.; Storey, J. W. V.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Bunker, A.; Saunders, W.] Anglo Australian Observ, Epping, NSW 1710, Australia.
[Bouwens, R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Burgarella, D.] Univ Aix Marseille, Observ Astron Marseille Provence, F-13388 Marseille, France.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Glazebrook, K.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Pimbblet, K.] Univ Queensland, Dept Phys, Brisbane, Qld 4072, Australia.
[Quimby, R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Lawrence, JS (reprint author), Macquarie Univ, Dept Phys & Engn, N Ryde, NSW 2109, Australia.
EM jsl@science.mq.edu.au
RI Gehrels, Neil/D-2971-2012; Glazebrook, Karl/N-3488-2015;
OI Glazebrook, Karl/0000-0002-3254-9044; Burton,
Michael/0000-0001-7289-1998
FU Australian Department of Education, Science, and Training through the
National Collaborative Research Infrastructure Strategy (NCRIS);
University of New South Wales through the UNSW PILOT Science Office;
European Commission [RICA26150]
FX The PILOT Science Case, presented here, was produced as part of the
PILOT conceptual design study, funded through the Australian Department
of Education, Science, and Training through the National Collaborative
Research Infrastructure Strategy (NCRIS) scheme, and the University of
New South Wales through the UNSW PILOT Science Office. The European
contribution has been supported by the ARENA network of the European
Commission FP6 under contract RICA26150.
NR 106
TC 6
Z9 7
U1 0
U2 1
PU CSIRO PUBLISHING
PI COLLINGWOOD
PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA
SN 1323-3580
J9 PUBL ASTRON SOC AUST
JI Publ. Astron. Soc. Aust.
PY 2009
VL 26
IS 4
BP 397
EP 414
DI 10.1071/AS08049
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 514SM
UT WOS:000271415900002
ER
PT J
AU Shao, M
Nemati, B
AF Shao, M.
Nemati, B.
TI Sub-Microarcsecond Astrometry with SIM-Lite: A Testbed-based Performance
Assessment
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
AB SIM-Lite is an astrometric interferometer being designed for sub-microarcsecond astrometry, with a wide range of applications from searches for Earth-analogs to determining the distribution of dark matter. SIM-Lite measurements can be limited by random and systematic errors, as well as astrophysical noise. In this paper we focus on instrument systematic errors and report results from SIM-Lite's interferometer testbed. We find that, for narrow-angle astrometry such as used for planet finding, the end-of-mission noise floor for SIM-Lite is below 0.035 mu as.
C1 [Shao, M.; Nemati, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Shao, M (reprint author), CALTECH, Jet Prop Lab, MS 301-486, Pasadena, CA 91125 USA.
FU Copyright 2008 California Institute of Technology
FX The research described in this article was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
Copyright 2008 California Institute of Technology. Government
sponsorship acknowledged.
NR 10
TC 9
Z9 9
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD JAN
PY 2009
VL 121
IS 875
BP 41
EP 44
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 404LF
UT WOS:000263152600005
ER
PT J
AU Myhre, G
Berglen, TF
Hoyle, CR
Christopher, SA
Coe, H
Crosier, J
Formenti, P
Haywood, JM
Johnsrud, M
Jones, TA
Loeb, N
Osborne, S
Remer, LA
AF Myhre, G.
Berglen, T. F.
Hoyle, C. R.
Christopher, S. A.
Coe, H.
Crosier, J.
Formenti, P.
Haywood, J. M.
Johnsrud, M.
Jones, T. A.
Loeb, N.
Osborne, S.
Remer, L. A.
TI Modelling of chemical and physical aerosol properties during the ADRIEX
aerosol campaign
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE aircraft measurements; secondary organic aerosols; radiative forcing
ID SECONDARY ORGANIC AEROSOL; INDIAN-OCEAN EXPERIMENT; DUST EXPERIMENT
SHADE; RADIATIVE IMPACT; OPTICAL-PROPERTIES; TRANSPORT MODEL; GLOBAL
AEROSOL; AIR-POLLUTION; OSLO CTM2; SEA-SALT
AB A global aerosol model with relatively high resolution is used to simulate the distribution and radiative effect of aerosols during the Aerosol Direct Radiative Impact Experiment (ADRIEX) campaign in August and September 2004. The global chemical transport model Oslo CTM2 includes detailed chemistry, which is coupled to aerosol partitioning of sulphate, nitrate and secondary organic aerosols. In accordance with aircraft observations the aerosol model simulates a dominance of secondary aerosols compared to primary aerosols in the ADRIEX study region. The model underestimates the aerosol optical depth (AOD) at 550 nm in the main region of the campaign around Venice. This underestimation mainly occurs during a 3-4 day period of highest AODs. At two AERONET (Aerosol Robotic Network) stations related to the ADRIEX campaign outside the Po valley area, the model compares very well with the observed AOD. Comparisons with observed chemical composition show that the model mainly underestimates organic carbon, with better agreement for other aerosol species. The model simulations indicate that the emission of aerosols and their precursors may be underestimated in the Po valley. Recent results show a large spread in radiative forcing due to the direct aerosol effect in global aerosol models, which is likely linked to large. differences in the vertical profile of aerosols and aerosol absorption. The modelled vertical profile of aerosol compares reasonably well to the aircraft measurements as was the case in two earlier campaigns involving biomass burning and dust aerosols. The radiative effect of aerosols over the northern part of the Adriatic Sea agrees well with the mean of three satellite-derived estimates despite large differences between the satellite-derived data. The difference between the model and the mean of the satellite data is within 10% for the radiative effect. The radiative forcing due to anthropogenic aerosols is simulated to be negative in the ADRIEX region with values between -5 and -2 W m(-2). Copyright (C) 2008 Royal Meteorological Society and Crown Copyright
C1 [Myhre, G.; Berglen, T. F.; Hoyle, C. R.] Univ Oslo, Dept Geosci, N-0315 Oslo, Norway.
[Myhre, G.] Ctr Int Climate & Environm Res, Oslo, Norway.
[Christopher, S. A.; Jones, T. A.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA.
[Coe, H.; Crosier, J.] Univ Manchester, Manchester M13 9PL, Lancs, England.
[Formenti, P.] Univ Paris 12, LISA, Creteil, France.
[Formenti, P.] Univ Paris 07, LISA, Creteil, France.
[Haywood, J. M.; Osborne, S.] Met Off, Exeter, Devon, England.
[Johnsrud, M.] Norwegian Inst Air Res NILU, Kjeller, Norway.
[Loeb, N.] NASA, Langley Atmospher Res Ctr LaRC, Hampton, VA USA.
[Remer, L. A.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
RP Myhre, G (reprint author), Univ Oslo, Dept Geosci, POB 1022, N-0315 Oslo, Norway.
EM gunnar.myhre@geo.uio.no
RI Myhre, Gunnar/A-3598-2008; Crosier, Jonathan/G-8952-2011; Christopher,
Sundar/E-6781-2011; Coe, Hugh/C-8733-2013; Hoyle,
Christopher/B-7786-2008;
OI Myhre, Gunnar/0000-0002-4309-476X; Hoyle,
Christopher/0000-0002-1369-9143; Crosier, Jonathan/0000-0002-3086-4729;
Coe, Hugh/0000-0002-3264-1713
FU Norwegian Research Council
FX We appreciate the useful and constructive comments and suggestions from
two reviewers. This study has received support from the Norwegian
Research Council.
NR 67
TC 7
Z9 7
U1 0
U2 5
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 JAN
PY 2009
VL 135
IS 638
BP 53
EP 66
DI 10.1002/qj.350
PN A
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 435WV
UT WOS:000265374900004
ER
PT J
AU Allen, G
Vaughan, G
Brunner, D
May, PT
Heyes, W
Minnis, P
Ayers, JK
AF Allen, G.
Vaughan, G.
Brunner, D.
May, P. T.
Heyes, W.
Minnis, P.
Ayers, J. K.
TI Modulation of tropical convection by breaking Rossby waves
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE convection; tropopause fold; Rossby waves; stratosphere to troposphere
exchange
ID DRY-AIR; TROPOSPHERE; PACIFIC; INTRUSION; MONSOON; OZONE
AB This work discusses observations of both the convective-inhibiting and convective-promoting properties associated with Rossby waves that break in the extratropics and extend into the tropics. Two tropical drought periods - times of reduced tropical cloudiness and rainfall - were observed during mid to late November 2005 over a wide area of northwest Australia, with an observed eruption of a nearby synoptic tropical cloud band in between times. Both convective inhibition and promotion appear to be linked to the descent of dry upper tropospheric air within a series of tropopause folds; convective inhibition was observed within the dry pool itself, whilst convective promotion was observed on the high moisture gradient at the leading edge of an advancing dry slot. A range of satellite images, surface rain gauges, radiosonde and ozonesonde data are used in conjunction with back trajectories and European Centre for Medium-Range Weather Forecasts (ECMWF) analysis fields to investigate the origins and dynamics associated with these convective events, showing each to be ultimately linked to breaking Rossby wave activity on the southern subtropical jet. Together, these observations support a growing number of studies linking midlatitude tropopause-level dynamics with the modulation of tropical deep convection, an influence that is poorly characterized when considering the climatology of tropical cloudiness and rainfall. Copyright (C) 2008 Royal Meteorological Society
C1 [Allen, G.; Vaughan, G.; Heyes, W.] Univ Manchester, Ctr Atmospher Sci, Manchester M13 9PL, Lancs, England.
[Brunner, D.] Swiss Fed Inst Mat Testing & Res, EMPA, Dubendorf, Switzerland.
[May, P. T.] Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia.
[Minnis, P.; Ayers, J. K.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA.
RP Allen, G (reprint author), Univ Manchester, Ctr Atmospher Sci, Oxford Rd, Manchester M13 9PL, Lancs, England.
EM grant.allen@manchester.ac.uk
RI Brunner, Dominik/A-1255-2009; Allen, Grant /A-7737-2013; Minnis,
Patrick/G-1902-2010; Vaughan, Geraint/O-2459-2015
OI Brunner, Dominik/0000-0002-4007-6902; Allen, Grant /0000-0002-7070-3620;
Minnis, Patrick/0000-0002-4733-6148; Vaughan,
Geraint/0000-0002-0885-0398
NR 27
TC 15
Z9 15
U1 0
U2 9
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD JAN
PY 2009
VL 135
IS 638
BP 125
EP 137
DI 10.1002/qj.349
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 435WV
UT WOS:000265374900010
ER
PT J
AU Newman, SM
Knuteson, RO
Zhou, DK
Larar, AM
Smith, WL
Taylor, JP
AF Newman, Stuart M.
Knuteson, Robert O.
Zhou, Daniel K.
Larar, Allen M.
Smith, William L.
Taylor, Jonathan P.
TI Radiative transfer validation study from the European Aqua Thermodynamic
Experiment
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Review
DE remote sensing; AIRS; airborne measurements; spectroscopy
ID SPECTROSCOPIC DATABASE; TESTBED INTERFEROMETER; RADIANCES; EAQUATE;
SURFACE
AB The European AQUA Thermodynamic Experiment (EAQUATE) brought together collocated hyperspectral measurements from the Atmospheric Infrared Sounder (AIRS) on NASA's Aqua satellite, as well as three airborne interferometers operating in the troposphere and stratosphere. Simultaneous observations of temperature, water vapour and trace gases have been used to constrain the atmospheric state, for validation of radiometric accuracy and radiative transfer modelling. The close agreement of observations with model spectra, in the 800-1200 cm(-1) region, indicates that the accuracy of modelling AIRS spectra is sufficient for beneficial use of the data in operational weather forecasting. The variability of atmospheric water vapour was found to be a fundamental constraint in the modelling of the 1400-1600 cm(-1) region, emphasising the requirement for a high density of observations in future validation campaigns. Copyright (C) Royal Meterological Society and Crown Copyright, 2009.
C1 [Newman, Stuart M.; Taylor, Jonathan P.] Met Off, Exeter EX1 3PB, Devon, England.
[Knuteson, Robert O.] Univ Wisconsin, Ctr Space Sci & Engn, Cooperat Inst Meteorol Sounding Studies, Madison, WI 53706 USA.
[Zhou, Daniel K.; Larar, Allen M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Smith, William L.] Hampton Univ, Hampton, VA 23668 USA.
RP Newman, SM (reprint author), Met Off, FitzRoy Rd, Exeter EX1 3PB, Devon, England.
EM stu.newman@metoffice.gov.uk
RI Zhang, YIng/F-5751-2011; Taylor, Jonathan/B-3786-2013
FU NPOESS IPO; NASA; Met Office; Natural Environment Research Council
FX We thank Walter Wolf at NOAA/NESDIS and the AIRS science team for
facilitating our use and analysis of AIRS data. We also thank two
anonyrnous reviewers for their thorough critiques which led to
improvements in the final manuscript. The NAST-I programme is supported
by the NPOESS IPO, NASA Headquarters, and NASA Langley Research Center.
FAAM (http://www.faam.ac.uk/) is jointly funded by the Met Office and
the Natural Environment Research Council.
NR 21
TC 3
Z9 3
U1 0
U2 4
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 JAN
PY 2009
VL 135
IS 639
BP 277
EP 290
DI 10.1002/qj.382
PN B
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 435WX
UT WOS:000265375100001
ER
PT B
AU Bartelmann, M
Bennett, CL
Burigana, C
Chiosi, C
D'Onofrio, M
Dressler, A
Gioia, I
Hasinger, G
Macias-Perez, JF
Madau, P
Marziani, P
Mather, J
Matteucci, F
Olive, K
Peacock, J
Reich, W
Robitaille, PM
Rowan-Robinson, M
Steigman, G
Steinmetz, M
Sulentic, JW
Turatto, M
White, SDM
AF Bartelmann, Matthias
Bennett, Charles L.
Burigana, Carlo
Chiosi, Cesare
D'Onofrio, Mauro
Dressler, Alan
Gioia, Isabella
Hasinger, Guenther
Macias-Perez, Juan Francisco
Madau, Piero
Marziani, Paola
Mather, John
Matteucci, Francesca
Olive, Keith
Peacock, John
Reich, Wolfgang
Robitaille, Pierre-Marie
Rowan-Robinson, Michael
Steigman, Gary
Steinmetz, Matthias
Sulentic, Jack W.
Turatto, Massimo
White, Simon D. M.
BE DOnofrio, M
Burigana, C
TI Fundamental Cosmological Observations and Data Interpretation
SO QUESTIONS OF MODERN COSMOLOGY: GALILEO'S LEGACY
LA English
DT Article; Book Chapter
ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; X-RAY-CLUSTERS; MICROWAVE
BACKGROUND-RADIATION; ACTIVE GALACTIC NUCLEI; COLD DARK-MATTER;
PRIMORDIAL HELIUM ABUNDANCE; PROBE WMAP OBSERVATIONS; MEDIUM-SENSITIVITY
SURVEY; STAR-FORMATION HISTORY
C1 [Bartelmann, Matthias] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Chiosi, Cesare; D'Onofrio, Mauro] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Burigana, Carlo] INAF Bologna, Ist Astrofis Spaziale & Fis Cosm IASF, I-40129 Bologna, Italy.
[Bennett, Charles L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Dressler, Alan] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Gioia, Isabella] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[Hasinger, Guenther] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Macias-Perez, Juan Francisco] Lab Phys Subatom & Cosmol, F-38026 Grenoble, France.
[Madau, Piero] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Marziani, Paola] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Mather, John] NASA, GSFC, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Matteucci, Francesca] Univ Trieste, I-34131 Trieste, Italy.
[Olive, Keith] Univ Minnesota, Sch Phys & Astron, Fine Theoret Phys Inst, Minneapolis, MN 55455 USA.
[Peacock, John] Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Reich, Wolfgang] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Robitaille, Pierre-Marie] Ohio State Univ, Dept Radiol, Columbus, OH 43210 USA.
[Rowan-Robinson, Michael] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England.
[Steigman, Gary] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Steinmetz, Matthias] Astrophys Inst Potzdam, D-14482 Potsdam, Germany.
[Sulentic, Jack W.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Turatto, Massimo] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy.
[White, Simon D. M.] Max Planck Inst Astrophys, D-85740 Garching, Germany.
RP Bartelmann, M (reprint author), Heidelberg Univ, Inst Theoret Astrophys, Albert Uberle Str 2, D-69120 Heidelberg, Germany.
EM mbartelmann@ita.uni-heidelberg.de; cbennett@jhu.edu;
burigana@iasfbo.inaf.it; cesare.chiosi@unipd.it;
mauro.donofrio@unipd.it; dressler@ociw.edu; gioia@ira.inaf.it;
ghasinger@mpe.mpg.de; macias@lpsc.in2p3.fr; pmadau@ucolick.org;
paola.marziani@oapd.inaf.it; john.c.mather@nasa.gov;
matteucci@oats.inaf.it; olive@physics.umn.edu; jap@roe.ac.uk;
wreich@mpifr-bonn.mpg.de; robitaille.1@osu.edu; m.rrobinson@ic.ac.uk;
steigman@mps.ohio-state.edu; msteinmetz@aip.de; jsulenti@bama.ua.edu;
Massimo.Turatto@oact.inaf.it; swhite@mpa-garching.mpg.de
OI Turatto, Massimo/0000-0002-9719-3157; Marziani,
Paola/0000-0002-6058-4912
NR 599
TC 3
Z9 3
U1 1
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-3-642-00791-0
PY 2009
BP 7
EP 201
DI 10.1007/978-3-642-00792-7_2
D2 10.1007/978-3-642-00792-7
PG 195
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BKX82
UT WOS:000269558100002
ER
PT B
AU Balbi, A
Bennett, CL
Bucher, M
Burigana, C
Coles, P
D'Onofrio, M
Durrer, R
Mather, J
Naselsky, P
Perrotta, F
Popa, LA
Spergel, D
Subramanian, K
Vittorio, N
AF Balbi, Amedeo
Bennett, Charles L.
Bucher, Martin
Burigana, Carlo
Coles, Peter
D'Onofrio, Mauro
Durrer, Ruth
Mather, John
Naselsky, Pavel
Perrotta, Francesca
Popa, Lucia A.
Spergel, David
Subramanian, Kandaswamy
Vittorio, Nicola
BE DOnofrio, M
Burigana, C
TI Astrophysical Cosmology
SO QUESTIONS OF MODERN COSMOLOGY: GALILEO'S LEGACY
LA English
DT Article; Book Chapter
ID MICROWAVE-ANISOTROPY-PROBE; LARGE-SCALE STRUCTURE; PRIMORDIAL
MAGNETIC-FIELDS; COLD DARK-MATTER; BIG-BANG NUCLEOSYNTHESIS; DIGITAL SKY
SURVEY; DOUBLE-BETA DECAY; MINIMAL ISOCURVATURE MODEL; NONZERO LEPTON
NUMBERS; GALAXY REDSHIFT SURVEY
C1 [Balbi, Amedeo] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[D'Onofrio, Mauro] Univ Padua, Dip Astron, I-35122 Padua, Italy.
[Burigana, Carlo] INAF Bologna, Ist Astrofis Spaziale & Fis Cosm IASF, I-40129 Bologna, Italy.
[Bennett, Charles L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bucher, Martin] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France.
[Coles, Peter] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Naselsky, Pavel] Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Perrotta, Francesca] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Popa, Lucia A.] Inst Space Sci, Bucharest 76900, Romania.
[Spergel, David] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Subramanian, Kandaswamy] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Vittorio, Nicola] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Durrer, Ruth] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland.
[Mather, John] NASA, Astrophys Sci Div, GSFC, Greenbelt, MD 20771 USA.
RP Balbi, A (reprint author), Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci, I-00133 Rome, Italy.
EM amedeo.balbi@roma2.infn.it; cbennett@jhu.edu; bucher@th.u-psud.fr;
burigana@iasfbo.inaf.it; Peter.Coles@astro.cf.ac.uk;
mauro.donofrio@unipd.it; Ruth.Durrer@physics.unige.ch;
john.c.mather@nasa.gov; naselsky@nbi.dk; perrotta@oats.inaf.it;
lpopa@venus.nipne.ro; Dns@astro.princeton.edu; kandu@iucaa.ernet.in;
nicola.vittorio@roma2.infn.it
RI popa, lucia/B-4718-2012
NR 276
TC 1
Z9 1
U1 0
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-3-642-00791-0
PY 2009
BP 203
EP 299
DI 10.1007/978-3-642-00792-7_3
D2 10.1007/978-3-642-00792-7
PG 97
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BKX82
UT WOS:000269558100003
ER
PT B
AU Bartelmann, M
Bennett, CL
Bucher, M
Burigana, C
Capaccioli, M
D'Onofrio, M
Durrer, R
Gioia, I
Hasinger, G
Lawrence, C
Longo, G
Macias-Perez, JF
Madau, P
Mather, J
Peacock, J
Popa, LA
Rebolo, R
Reich, W
Steinmetz, M
Turatto, M
White, SDM
AF Bartelmann, Matthias
Bennett, Charles L.
Bucher, Martin
Burigana, Carlo
Capaccioli, Massimo
D'Onofrio, Mauro
Durrer, Ruth
Gioia, Isabella
Hasinger, Guenther
Lawrence, Charles
Longo, Giuseppe
Macias-Perez, Juan Francisco
Madau, Piero
Mather, John
Peacock, John
Popa, Lucia A.
Rebolo, Rafael
Reich, Wolfgang
Steinmetz, Matthias
Turatto, Massimo
White, Simon D. M.
BE DOnofrio, M
Burigana, C
TI Next Challenges
SO QUESTIONS OF MODERN COSMOLOGY: GALILEO'S LEGACY
LA English
DT Article; Book Chapter
ID DIGITAL-SKY-SURVEY; MICROWAVE BACKGROUND-RADIATION; SURVEY COMMISSIONING
DATA; DARK-MATTER SUBSTRUCTURE; RAY GALAXY CLUSTERS; INFLATIONARY
UNIVERSE; HIGH-REDSHIFT; COSMIC STRINGS; SCALE STRUCTURE; DATA-FLOW
C1 [Bartelmann, Matthias] Univ Heidelberg, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[D'Onofrio, Mauro] Univ Padua, Dip Astron, I-35122 Padua, Italy.
[Burigana, Carlo] INAF Bologna, Ist Astrofis Spaziale & Fis Cosm IASF, I-40129 Bologna, Italy.
[Bennett, Charles L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bucher, Martin] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France.
[Capaccioli, Massimo] Osserv Astron Capodimonte, VST Ctr, INAF, I-80131 Naples, Italy.
[Durrer, Ruth] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland.
[Gioia, Isabella] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[Hasinger, Guenther] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Lawrence, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Longo, Giuseppe] Univ Naples Federico 2, Dept Phys Sci, I-80126 Naples, Italy.
[Macias-Perez, Juan Francisco] Lab Phys Subatom & Cosmol, F-38026 Grenoble, France.
[Madau, Piero] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Mather, John] NASA, Astrophys Sci Div, GSFC, Greenbelt, MD 20771 USA.
[Peacock, John] Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Popa, Lucia A.] Inst Space Sci, Bucharest 76900, Romania.
[Rebolo, Rafael] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Reich, Wolfgang] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Steinmetz, Matthias] Astrophys Inst Potzdam, D-14482 Potsdam, Germany.
[Turatto, Massimo] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy.
[White, Simon D. M.] Max Planck Inst Astrophys, D-85740 Garching, Germany.
RP Bartelmann, M (reprint author), Univ Heidelberg, Inst Theoret Astrophys, Albert Uberle Str 2, D-69120 Heidelberg, Germany.
EM mbartelmann@ita.uni-heidelberg.de; cbennett@jhu.edu;
bucher@th.u-psud.fr; burigana@iasfbo.inaf.it; mc@na.infn.it;
mauro.donofrio@unipd.it; Ruth.Durrer@physics.unige.ch;
gioia@ira.inaf.it; ghasinger@mpe.mpg.de;
Charles.R.Lawrence@jpl.nasa.gov; longo@na.infn.it; macias@lpsc.in2p3.fr;
pmadau@ucolick.org; john.c.mather@nasa.gov; jap@roe.ac.uk;
lpopa@venus.nipne.ro; rrl@iac.es; wreich@mpifr-bonn.mpg.de;
msteinmetz@aip.de; Massimo.Turatto@oact.inaf.it;
swhite@mpa-garching.mpg.de; burigana@iasfbo.inaf.it
RI popa, lucia/B-4718-2012;
OI Turatto, Massimo/0000-0002-9719-3157
NR 150
TC 0
Z9 0
U1 0
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-3-642-00791-0
PY 2009
BP 429
EP 501
DI 10.1007/978-3-642-00792-7_5
PG 73
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BKX82
UT WOS:000269558100005
ER
PT J
AU Marchetti, AA
McAninch, JE
Rugel, G
Ruhm, W
Korschinek, G
Martinelli, RE
Faestermann, T
Knie, K
Egbert, SD
Wallner, A
Wallner, C
Tanaka, K
Endo, S
Hoshi, M
Shizuma, K
Fujita, S
Hasai, H
Imanaka, T
Straume, T
AF Marchetti, A. A.
McAninch, J. E.
Rugel, G.
Ruehm, W.
Korschinek, G.
Martinelli, R. E.
Faestermann, T.
Knie, K.
Egbert, S. D.
Wallner, A.
Wallner, C.
Tanaka, K.
Endo, S.
Hoshi, M.
Shizuma, K.
Fujita, S.
Hasai, H.
Imanaka, T.
Straume, T.
TI Fast Neutrons Measured in Copper from the Hiroshima Atomic Bomb Dome
SO RADIATION RESEARCH
LA English
DT Article
ID ACCELERATOR MASS-SPECTROMETRY; NI-63; EU-152; CO-60
AB The first measurements of (63)Ni produced by A-bomb fast neutrons (above similar to 1 MeV) in copper samples from Hiroshima encompassed distances from similar to 380 to 5062 m front the hypocenter (the point on the ground directly under the bomb). They included the region of interest to survivor studies (similar to 900 to 1500 m) and provided the first direct validation of fast neutrons in that range. However, a significant measurement gap remained between the hypocenter and 380 m. Measurements close to the hypocenter are important as a high-value anchor for the slope of the curve for neutron activation as a function of distance. Here we report measurements of (63)Ni in copper samples from the historic Hiroshima Atomic Bomb Dome, which is located similar to 150 m front the hypocenter. These measurements extend the range of our previously published data for (63)Ni providing a more comprehensive and consistent A-bomb activation curve. The results are also in good agreement with calculations based on the current dosimetry system (DS02) and give further experimental support to the accuracy of this system that forms the basis for radiation risk estimates worldwide. (C) 2009 by Radiation Research Society.
C1 [Marchetti, A. A.; Martinelli, R. E.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[McAninch, J. E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Rugel, G.; Korschinek, G.; Faestermann, T.; Knie, K.; Wallner, A.; Wallner, C.] Tech Univ Munich, Fak Phys, D-85748 Garching, Germany.
[Ruehm, W.] German Res Ctr Environm Hlth, Helmholtz Zentrum Munchen, D-85764 Neuherberg, Germany.
[Egbert, S. D.] Sci Applicat Int Corp, San Diego, CA 92121 USA.
[Tanaka, K.; Endo, S.; Hoshi, M.; Shizuma, K.] Hiroshima Univ, Hiroshima, Japan.
[Fujita, S.] Radiat Effects Res Fdn, Hiroshima, Japan.
[Hasai, H.] Hiroshima Kokusai Gakuin Univ, Hiroshima, Japan.
[Imanaka, T.] Kyoto Univ, Inst Res Reactor, Kyoto 6068501, Japan.
[Straume, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Marchetti, AA (reprint author), Lawrence Livermore Natl Lab, L-096,7000 East Ave, Livermore, CA 94550 USA.
EM marchetti@llnl.gov
RI Wallner, Anton/G-1480-2011; Endo, Satoru/D-9091-2012;
OI Wallner, Anton/0000-0003-2804-3670; Endo, Satoru/0000-0001-5961-681X;
Faestermann, Thomas/0000-0002-6603-8787
FU U.S. Department of Energy [DEFG0300ER62963, DEFC0397SF21354]; U.S.
National Academy of Sciences [E215099]; U.S. Army Surgeon General's
Office; European Commission [FIGD-CT20000079]; German Federal Ministry
of Environment; Nature Conservation and Nuclear Safety [StSch4235];
Lawrence Livermore National Laboratory [DE-AC52-07NA27344]
FX We thank the Radiation Effects Research Foundation, Hiroshima
University, and Hiroshima Kokusai Gakuin University for generously
providing copper samples and related sample information for this study.
We also thank the following organizations for supporting this work: the
U.S. Department of Energy (grant DEFG0300ER62963, contract
DEFC0397SF21354, TS), the U.S. National Academy of Sciences (grant
E215099, TS), the U.S. Army Surgeon General's Office (TS), the European
Commission (FIGD-CT20000079), the German Federal Ministry of
Environment, Nature Conservation and Nuclear Safety (StSch4235). One of
us (GR) would like to thank the Bavarian Government for a grant.
Portions of this work were performed under the auspices of the U.S.
Department of Energy by the Lawrence Livermore National Laboratory under
contract DE-AC52-07NA27344.
NR 17
TC 4
Z9 4
U1 1
U2 3
PU RADIATION RESEARCH SOC
PI LAWRENCE
PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA
SN 0033-7587
J9 RADIAT RES
JI Radiat. Res.
PD JAN
PY 2009
VL 171
IS 1
BP 118
EP 122
DI 10.1667/RR1436.1
PG 5
WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology,
Nuclear Medicine & Medical Imaging
GA 390TX
UT WOS:000262187700012
PM 19138052
ER
PT S
AU Liechty, DS
AF Liechty, Derek S.
BE Abe, T
TI Modifications to Axially Symmetric Simulations Using New DSMC (2007)
Algorithms
SO RAREFIED GAS DYNAMICS
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 26th International Symposium on Rarefied Gas Dynamics (RGD26)
CY JUN 20-JUL 25, 2008
CL Kyoto, JAPAN
SP Japan Soc Promot Sci, Japan Aerosp Explorat Agcy, Soc Promot Space Sci, Iwantani Naoji Fdn, Inoue Fdn Sci, Casio Sci Promot Fdn, Kaijma Fdn, IHI Corp, IHI Aerosp Engn Co Ltd, Osaka Vaccuun Ltd, Nissin Inc
DE Monte Carlo; particle methods; nonequilibrium fluid.
AB Several modifications aimed at improving physical accuracy are proposed for solving axially symmetric problems building on the DSMC (2007) algorithms introduced by Bird. Originally developed to solve nonequilibrium, rarefied flows, the DSMC method is now regularly used to solve complex problems over a wide range of Knudsen numbers. These new algorithms include features such as nearest neighbor collisions excluding the previous collision partners, separate collision and sampling cells, automatically adaptive variable time steps, a modified no-time counter procedure for collisions, and discontinuous and event-driven physical processes. Axially symmetric solutions require radial weighting for the simulated molecules since the molecules near the axis represent fewer real molecules than those farther away from the axis due to the difference in volume of the cells. In the present methodology, these radial weighting factors are continuous, linear functions that vary with the radial position of each simulated molecule. It is shown that how one defines the number of tentative collisions greatly influences the mean collision time near the axis. The method by which the grid is treated for axially symmetric problems also plays an important role near the axis, especially for scalar pressure. A new method to treat how the molecules are traced through the grid is proposed to alleviate the decrease in scalar pressure at the axis near the surface. Also, a modification to the duplication baffler is proposed to vary the duplicated molecular velocities while retaining the molecular kinetic energy and axially symmetric nature of the problem.
C1 NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
RP Liechty, DS (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
NR 7
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0615-5
J9 AIP CONF PROC
PY 2009
VL 1084
BP 251
EP 256
PG 6
WC Engineering, Aerospace; Physics, Fluids & Plasmas
SC Engineering; Physics
GA BJF97
UT WOS:000265564800040
ER
PT S
AU Goldstein, DB
Summy, D
Colaprete, A
Varghese, PL
Trafton, LM
AF Goldstein, D. B.
Summy, D.
Colaprete, A.
Varghese, P. L.
Trafton, L. M.
BE Abe, T
TI Modeling the Vapor and Dust Dynamics Due to the Impact of the LCROSS
Spacecraft on the Moon.
SO RAREFIED GAS DYNAMICS
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 26th International Symposium on Rarefied Gas Dynamics (RGD26)
CY JUN 20-JUL 25, 2008
CL Kyoto, JAPAN
SP Japan Soc Promot Sci, Japan Aerosp Explorat Agcy, Soc Promot Space Sci, Iwantani Naoji Fdn, Inoue Fdn Sci, Casio Sci Promot Fdn, Kaijma Fdn, IHI Corp, IHI Aerosp Engn Co Ltd, Osaka Vaccuun Ltd, Nissin Inc
DE Collisionless atmosphere; exosphere; lunar atmosphere; lunar impact
ID LUNAR SOUTH-POLE; WATER ICE; COLD TRAP; DEPOSITS; PROSPECTOR; SEARCH
AB The implications of possibly large volatile reservoirs on the Moon are significant for the future of manned activity there and for space science and exploration in general. In autumn of 2008 NASA will launch the LCROSS mission to impact two spacecraft into a permanently shadowed crater-a cold trap - at the south pole of the Moon. The lead spacecraft will excavate its own several meter crater. The process will be observed by the following smaller vehicle and by orbiting and Earth-based instruments in hopes of observing the release of volatiles-predominantly water -- from the lunar soil. The following vehicle will then impact as well. We examine the plausible vapor dynamics following the impacts and concentrate on the observability of the gas from Earth or lunar orbit. In the free-molecular computational model of the vapor motion, water and OH molecules move ballistically, have a temperature-dependent surface residence time, and are subject to photo-dissociation and ionization losses. Sunlight shadowing, separation of the vapor from the dust grains, dust thermodynamics and different impact plume models are considered.
C1 [Goldstein, D. B.; Summy, D.; Varghese, P. L.; Trafton, L. M.] Univ Texas Austin, Austin, TX 78712 USA.
[Colaprete, A.] NASA, Ames Res Ctr, Moffett Field, CA USA.
RP Goldstein, DB (reprint author), Univ Texas Austin, Austin, TX 78712 USA.
FU NASA [NNG04GQ66G, NNX08AZ42A]
FX This work was supported in part by NASA grants NNG04GQ66G and
NNX08AZ42A.
NR 24
TC 2
Z9 2
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0615-5
J9 AIP CONF PROC
PY 2009
VL 1084
BP 1061
EP +
PG 2
WC Engineering, Aerospace; Physics, Fluids & Plasmas
SC Engineering; Physics
GA BJF97
UT WOS:000265564800170
ER
PT B
AU Scimemi, SJ
AF Scimemi, Samuel J.
BE Kurnaz, S
Ince, F
Onbasioglu, S
Basturk, S
TI Human Space Flight Docking Interoperability
SO RAST 2009: PROCEEDINGS OF THE 4TH INTERNATIONAL CONFERENCE ON RECENT
ADVANCES IN SPACE TECHNOLOGIES
LA English
DT Proceedings Paper
CT 4th International Conference on Recent Advances in Space Technologies
CY JUN 11-13, 2009
CL Istanbul, TURKEY
SP turkish Air Force Acad, Istanbul Tech Univ, Bogazici Univ, Marmara Univ, Bahcesehir Univ, Istanbul Commerce Univ, Halic Univ, Yeditepe Univ, IEEE, AIAA
C1 NASA Headquarters, Washington, DC 20009 USA.
RP Scimemi, SJ (reprint author), NASA Headquarters, 300 E St SW,Suite 7A16, Washington, DC 20009 USA.
EM sam.scimemi@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4244-3626-2
PY 2009
BP 167
EP 169
DI 10.1109/RAST.2009.5158189
PG 3
WC Engineering, Aerospace
SC Engineering
GA BLZ72
UT WOS:000271613000034
ER
PT S
AU Dorodnitsyn, A
Kallman, T
AF Dorodnitsyn, A.
Kallman, T.
BE Hubeny, I
Stone, JM
MacGregor, K
Werner, K
TI The formation of narrow X-ray line spectra from realistic hydrodynamical
models: applications to the problem of warm absorbers
SO RECENT DIRECTIONS IN ASTROPHYSICAL QUANTITATIVE SPECTROSCOPY AND
RADIATION HYDRODYNAMICS
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference on Recent Directions in Astrophysical Quantitative
Spectroscopy and Radiation Hydrodynamics held in honor of Dimitri
Mihalas
CY MAR 30-APR 03, 2009
CL Boulder, CO
SP Natl Ctr Atmospher Res
DE Document processing; Class file writing; LATEX2 epsilon
AB We calculate a series of synthetic spectra from outflows originating from the obscuring torus in active galactic nuclei (AGN). Such modeling includes 2.5D hydrodynamical simulations of an X-ray excited torus wind, including the effects of X-ray heating, ionization, and radiation pressure. 3D radiation transfer calculations are performed in the 3D Sobolev approximation. Synthetic X-ray line spectra and individual profiles of several strong lines are shown at different inclination angles, observing times, and for different characteristics of the torus.
C1 [Dorodnitsyn, A.; Kallman, T.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
RP Dorodnitsyn, A (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.
NR 2
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0710-7
J9 AIP CONF PROC
PY 2009
VL 1171
BP 304
EP 308
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQB69
UT WOS:000280587500027
ER
PT S
AU Garcia, J
Kallman, T
AF Garcia, Javier
Kallman, Tim
BE Hubeny, I
Stone, JM
MacGregor, K
Werner, K
TI Comptonized Fe K-lines in the X-ray spectra of Low-Mass X-ray Binaries
SO RECENT DIRECTIONS IN ASTROPHYSICAL QUANTITATIVE SPECTROSCOPY AND
RADIATION HYDRODYNAMICS
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference on Recent Directions in Astrophysical Quantitative
Spectroscopy and Radiation Hydrodynamics held in honor of Dimitri
Mihalas
CY MAR 30-APR 03, 2009
CL Boulder, CO
SP Natl Ctr Atmospher Res
DE accretion, accretion disks; line: formation; radiative transfer; X-rays:
binaries
ID IRON; PHOTOIONIZATION; REFLECTION
AB We present new models for the vertical structure of accretion disks illuminated by X-rays. The chief advance is the inclusion of the most recent atomic data for the inner-shell of the iron isonuclear sequence. We also include the redistribution of the photons due to Compton scattering. By performing detailed ID radiative transfer calculations, we have computed the reflected spectra from constant density slabs for different degrees of ionization. Our results show that Comptonization can be responsible for a significant fraction of the broadening of the Fe K-line. This is of interest in view of recent observations which have revealed broad and asymmetric iron emission line profiles in some neutron star Low Mass X-Ray Binaries (LMXBs). Although these resemble the broadened lines observed in some active galactic nuclei, and which are likely due to the Doppler effect and gravitational redshift, we examine the contribution to the Fe K-line broadening by Comptonization in a disk atmosphere. Using simulated Suzaku observations, we compare our models with the current
C1 [Garcia, Javier] Catholic Univ Amer, IACS, Dept Phys, Washington, DC 20064 USA.
[Kallman, Tim] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Garcia, J (reprint author), Catholic Univ Amer, IACS, Dept Phys, Washington, DC 20064 USA.
NR 7
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0710-7
J9 AIP CONF PROC
PY 2009
VL 1171
BP 363
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQB69
UT WOS:000280587500042
ER
PT S
AU Shen, SH
Leptoukh, G
Loboda, T
Csiszar, I
Romanov, P
Gerasimov, I
AF Shen, Suhung
Leptoukh, Gregory
Loboda, Tatiana
Csiszar, Ivan
Romanov, Peter
Gerasimov, Irina
BE Groisman, PY
Ivanov, SV
TI The NASA NEESPI Data Portal to Support Studies of Climate and
Environmental Changes in Non-boreal Europe
SO REGIONAL ASPECTS OF CLIMATE-TERRESTRIAL-HYDROLOGIC INTERACTIONS IN
NON-BOREAL EASTERN EUROPE
SE NATO Science for Peace and Security Series C-Environmental Security
LA English
DT Proceedings Paper
CT NATO Advanced Research Workshop on Regional Aspects of
Climate-Terrestrial-Hydrologic Interactions in Non-boreal Eastern Europe
CY AUG 23-28, 2008
CL Odessa, UKRAINE
SP NATO, No Eurasia Earth Sci Partnership Initiat
DE remote sensing; online visualization; data analysis; fire; NDVI
AB Goddard Interactive Online Visualization ANd aNalysis Infrastructure (Giovanni) data portal is ready to support NEESPI studies in Northern Eurasia with high quality remote sensing information.
C1 [Shen, Suhung] George Mason Univ, Data & Informat Serv Ctr, NASA, GSFC, Code 610-2, Greenbelt, MD 20771 USA.
[Leptoukh, Gregory] NASA, GSFC, Greenbelt, MD 20771 USA.
[Loboda, Tatiana; Csiszar, Ivan; Romanov, Peter] Univ Maryland, College Pk, MD 20742 USA.
[Gerasimov, Irina] NASA, GSFC, ADNET, Greenbelt, MD 20771 USA.
RP Shen, SH (reprint author), George Mason Univ, Data & Informat Serv Ctr, NASA, GSFC, Code 610-2, Greenbelt, MD 20771 USA.
EM suhung.shen-1@nasa.gov
RI Csiszar, Ivan/D-2396-2010; Romanov, Peter/F-5622-2010
OI Romanov, Peter/0000-0002-2153-8307
FU NASA through ROSES [NNH05ZDA001N-ACCESS]
FX The project is supported by NASA through ROSES 2005 NNH05ZDA001N-ACCESS.
The authors wish to express great appreciation for the technical support
of the Giovanni software development and S4PA data ingest working groups
at NASA GES-DISC.
NR 9
TC 1
Z9 1
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 1871-4668
BN 978-481-2241-7; 978-90-481-2240-0
J9 NATO SCI PEACE SECUR
JI NATO Sci. Peace Secur. Ser. C- Environ. Secur.
PY 2009
BP 9
EP +
DI 10.1007/978-90-481-2283-7_2
PG 2
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA BJK38
UT WOS:000266662700002
ER
PT S
AU Gutman, G
AF Gutman, Garik
BE Groisman, PY
Ivanov, SV
TI The NASA Land-Cover/Land-Use Change (LCLUC) Program's Support of the
Northern Eurasia Earth Science Partnership Initiative (NEESPI): Focus on
Non-boreal Europe
SO REGIONAL ASPECTS OF CLIMATE-TERRESTRIAL-HYDROLOGIC INTERACTIONS IN
NON-BOREAL EASTERN EUROPE
SE NATO Science for Peace and Security Series C - Environmental Security
LA English
DT Proceedings Paper
CT NATO Advanced Research Workshop on Regional Aspects of
Climate-Terrestrial-Hydrologic Interactions in Non-boreal Eastern Europe
CY AUG 23-28, 2008
CL Odessa, UKRAINE
SP NATO, No Eurasia Earth Sci Partnership Initiat
DE land cover; land use change; non-boreal Eastern Europe
ID BIOOPTICAL PARAMETER VARIABILITY; CHLOROPHYLL-A CONCENTRATION; TURBID
PRODUCTIVE WATERS; GYPSY-MOTH DEFOLIATION; REMOTE ESTIMATION; FOREST
DISTURBANCE
AB Currently, the Northern Eurasia Earth Science Partnership Initiative (NEESPI) includes over 120 international projects involving more than 200 scientific institutions from over 30 countries. The program involves national government agencies, academia and private organizations in the U.S., Europe, Japan and Northern Eurasia (Gutman 2007). The NEESPI science is directed at evaluating the role of anthropogenic impacts on the Northern Eurasia ecosystems, the hemispheric-scale interaction and assessing how future human actions would affect the global climate and ecosystems of the region. Projections of the consequences of global changes for regional environment in Northern Eurasia are also in the center of the scientific foci of this initiative. The Land-Cover/Land-Use Change (LCLUC) Program is an interdisciplinary science program in the Earth Science Division of the Science Mission Directorate supporting several regional initiatives, including NEESPI. The NASA LCLUC currently funds over 30 NEESPI projects. The NEESPI program links to several international projects, such as GLP, iLEAPS and others, under major international programs: IGBP and WCRP. The NEESPI covers a large geographic domain, which includes the former Soviet Union, northern China, Mongolia, Scandinavia and Eastern Europe. This contribution provides a short description of the ongoing NEESPI studies in the non-boreal European sub-region of the NEESPI geographic domain that are supported by the NASA LCLUC program. More information on the projects can be found at http://neespi.org and http://lcluc.hq.nasa.gov.
C1 NASA Headquarters, Land Cover Land Use Change Program, Washington, DC 20546 USA.
RP Gutman, G (reprint author), NASA Headquarters, Land Cover Land Use Change Program, 300 E St SW, Washington, DC 20546 USA.
EM ggutman@noaa.gov
NR 18
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 1871-4668
BN 978-481-2241-7
J9 NATO SCI PEACE SECUR
PY 2009
BP 117
EP 122
DI 10.1007/978-90-481-2283-7_13
PG 6
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA BJK38
UT WOS:000266662700013
ER
PT S
AU Ramesham, R
AF Ramesham, Rajeshuni
BE Kullberg, RC
Ramesham, R
TI Environmental Testing of COTS Components for Space Applications
SO RELIABILITY, PACKAGING, TESTING, AND CHARACTERIZATION OF MEMS/MOEMS AND
NANODEVICES VIII
SE Proceedings of SPIE-The International Society for Optical Engineering
LA English
DT Proceedings Paper
CT Conference on Reliability, Packaging, Testing, and Characterization of
MEMS/MOEMS and Nanodevices VIII
CY JAN 28-29, 2009
CL San Jose, CA
SP SPIE, Texas Instruments Inc, Nanoink Inc, Photon Ctr Boston Univ, Ozen Engn Inc
DE COTS; MEMS; Life testing; Protoflight qualification; Valves; Pumps; and
Reliability
ID RELIABILITY; MEMS
AB Research and development of microelectromechanical systems (MEMS) has shown a significant promise for a variety of commercial applications. For example, accelerometers are widely used for air bags in automobiles, MEMS inkjet print heads are used for printers, gyroscopes for guidance and navigation and pressure sensors for various industrial applications. Some of the MEMS devices have potential to become the commercial-off-the-shelf (COTS) components. Aerospace requires more sophisticated technology development to achieve significant cost savings if they could utilize COTS components in their systems.
A miniature gas chromatograph instrument designed as a space station project will provide on-orbit detection, identification, and quantification of potentially toxic trace volatile organic compounds in the human-supporting environment. The instrument consists of several commercial off-the-shelf (COTS) valves, pumps and sensors. This paper describes the thermal environmental requirements and protoflight/qualification thermal test results for the COTS parts at cold and hot temperature extremes. The objective of this study is to qualify several COTS components for specific thermal/dynamic environments to assess their reliability. All COTS components life tested were believed to meet the 3x mission operational life requirements. Test results will be presented.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ramesham, R (reprint author), CALTECH, Jet Prop Lab, 125-204D,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Rajeshuni.ramesham@jpl.nasa.gov; Rajeshuni.ramesham@jpl.nasa.gov
NR 30
TC 0
Z9 0
U1 1
U2 4
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7452-0
J9 P SOC PHOTO-OPT INS
PY 2009
VL 7206
AR 72060H
DI 10.1117/12.813408
PG 11
WC Nanoscience & Nanotechnology; Materials Science, Characterization &
Testing; Optics
SC Science & Technology - Other Topics; Materials Science; Optics
GA BSP99
UT WOS:000285331000016
ER
PT S
AU Lin, B
Fan, TF
AF Lin, Bing
Fan, Tai-Fang (Alice)
BE Revetria, R
Mladenov, V
Mastorakis, N
TI Global Atmospheric Heat Distributions Observed From Space
SO REMOTE'09: PROCEEDINGS OF THE 5TH WSEAS INTERNATIONAL CONFERENCE ON
REMOTE SENSING
SE Mathematics and Computers in Science and Engineering
LA English
DT Proceedings Paper
CT 5th WSEAS International Conference on Remote Sensing (REMOTE '09)
CY OCT 17-19, 2009
CL Univ Genova, Genoa, ITALY
SP WSEAS
HO Univ Genova
DE radiation; latent heat; sensible heat; satellite observation
AB This study focuses on the observations of global atmospheric heat distributions using satellite measurements. Major heat components such as radiation energy, latent heat and sensible heat are considered. The uncertainties and error sources are assessed. Results show that the atmospheric heat is basically balanced, and the observed patterns of radiation and latent heat from precipitation are clearly related to general circulation.
C1 [Lin, Bing] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
[Fan, Tai-Fang (Alice)] SSSAI, Hampton, VA 23666 USA.
RP Lin, B (reprint author), NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
EM Bing.Lin@nasa.gov; Tai-Fang.Fan-1@nasa.gov
NR 2
TC 0
Z9 0
U1 0
U2 0
PU WORLD SCIENTIFIC AND ENGINEERING ACAD AND SOC
PI ATHENS
PA AG LOANNOU THEOLOGOU 17-23, 15773 ZOGRAPHOU, ATHENS, GREECE
SN 1792-4308
BN 978-960-474-129-8
J9 MATH COMPUT SCI ENG
PY 2009
BP 19
EP 21
PG 3
WC Remote Sensing
SC Remote Sensing
GA BOF41
UT WOS:000276454400002
ER
PT B
AU Hu, YX
AF Hu, Yongxiang
BE Revetria, R
Mladenov, V
Mastorakis, N
TI Ocean, Land and Meteorology Studies Using Space-Based Lidar Measurements
SO REMOTE'09: PROCEEDINGS OF THE 5TH WSEAS INTERNATIONAL CONFERENCE ON
REMOTE SENSING
SE Mathematics and Computers in Science and Engineering
LA English
DT Proceedings Paper
CT 5th WSEAS International Conference on Remote Sensing (REMOTE '09)
CY OCT 17-19, 2009
CL Univ Genova, Genoa, ITALY
SP WSEAS
HO Univ Genova
DE lidar ocean wind aerosol temperature altimetry
ID SURFACE
AB CALIPSO's main mission objective is studying the climate impact of clouds and aerosols in the atmosphere. CALIPSO also collects information about other components of the Earth's ecosystem, such as oceans and land. This paper introduces the physics concepts and presents preliminary results for the valueadded CALIPSO Earth system science products. These include ocean surface wind speeds, column atmospheric optical depths, ocean subsurface backscatter, land surface elevations, atmospheric temperature profiles, and A-train data fusion products.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Hu, YX (reprint author), NASA, Langley Res Ctr, MS 475, Hampton, VA 23681 USA.
EM Yongxiang.hu-1@nasa.gov
RI Hu, Yongxiang/K-4426-2012
NR 6
TC 0
Z9 0
U1 0
U2 0
PU WORLD SCIENTIFIC AND ENGINEERING ACAD AND SOC
PI ATHENS
PA AG LOANNOU THEOLOGOU 17-23, 15773 ZOGRAPHOU, ATHENS, GREECE
BN 978-960-474-129-8
J9 MATH COMPUT SCI ENG
PY 2009
BP 47
EP 50
PG 4
WC Remote Sensing
SC Remote Sensing
GA BOF41
UT WOS:000276454400007
ER
PT B
AU Xu, KM
Su, WY
Eitzen, Z
AF Xu, Kuan-Man
Su, Wenying
Eitzen, Zachary
BE Revetria, R
Mladenov, V
Mastorakis, N
TI Use of CERES Cloud and Radiation Data for Model Evaluation and Cloud
Feedback Studies
SO REMOTE'09: PROCEEDINGS OF THE 5TH WSEAS INTERNATIONAL CONFERENCE ON
REMOTE SENSING
SE Mathematics and Computers in Science and Engineering
LA English
DT Proceedings Paper
CT 5th WSEAS International Conference on Remote Sensing (REMOTE '09)
CY OCT 17-19, 2009
CL Univ Genova, Genoa, ITALY
SP WSEAS
HO Univ Genova
DE CERES; Cloud Feedback; Cloud Radiative Effects
ID SURFACE-TEMPERATURE
AB The availability of enormous amounts of satellite remote sensing data provides a golden opportunity to improve the capability of climate models for projecting future climate change. In this study, we will present recent progress in using CERES (Clouds and the Earth's Radiant Energy System) satellite data to evaluate model performance with regards to the vertical structures of radiative fluxes and cloud radiative effects and to provide an unambiguous estimate of the magnitude of low cloud feedbacks.
C1 [Xu, Kuan-Man; Su, Wenying; Eitzen, Zachary] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 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; Wenying.Su-1@nasa.gov; Zachary.A.Eitzen@nasa.gov
RI Xu, Kuan-Man/B-7557-2013
OI Xu, Kuan-Man/0000-0001-7851-2629
NR 16
TC 0
Z9 0
U1 0
U2 3
PU WORLD SCIENTIFIC AND ENGINEERING ACAD AND SOC
PI ATHENS
PA AG LOANNOU THEOLOGOU 17-23, 15773 ZOGRAPHOU, ATHENS, GREECE
BN 978-960-474-129-8
J9 MATH COMPUT SCI ENG
PY 2009
BP 56
EP 61
PG 6
WC Remote Sensing
SC Remote Sensing
GA BOF41
UT WOS:000276454400009
ER
PT S
AU Taranik, JV
Coolbaugh, MF
Vaughan, RG
AF Taranik, James V.
Coolbaugh, Mark F.
Vaughan, R. Greg
BE Bedell, R
Crosta, AP
Grunsky, E
TI An Overview of Thermal Infrared Remote Sensing with Applications to
Geothermal and Mineral Exploration in the Great Basin, Western United
States
SO REMOTE SENSING AND SPECTRAL GEOLOGY
SE Reviews in Economic Geology
LA English
DT Article; Book Chapter
ID REFLECTION RADIOMETER ASTER; MULTISPECTRAL SCANNER; VIRGINIA RANGE;
DEATH-VALLEY; LAVA FLOWS; IMAGES; NEVADA; CALIFORNIA; EMISSION; AIRBORNE
AB The physics of thermal infrared aerospace measurements is based on Planck's Radiation law,, Wien's Displacement law, and Kirchoff's law. The electromagnetic spectrum for thermal infrared aerospace measurements includes measurements beyond the reflected short- (2.5 mu m) to the long-wave infrared (14 mu m).
Thermal infrared sensors measure thermal emission from the Earths surface in single wavelength bands (broadband), tens of bands (multiband), and in hundreds of hands (hyperspectral). Broadband thermal infrared measurement techniques include surface temperature Mapping and thermal inertia mapping. Multiband and hyperspectral techniques involve mapping of changes in thermal emission at different wavelengths (emissivity mapping). Today, broadband surface temperature mapping is mostly done with satellite sensors. Thermal inertia mapping is done using broadband measurements taken during the day and night. Emissivity mapping is done using tens to hundreds of hands, and it requires sensors capable of measuring small changes in radiant emittance. Sensor systems discussed in this study include: Thermal Infrared Multispectral Scanner (TIMS), the Moderate Resolution Imaging Spectroradiometer (MODIS), Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) Simulator (MASTER), the Spatially Enhanced Broadband Array Spectrograph System (SEBASS) and the ASTER satellite sensor.
Several areas of Nevada, such as Brady's Hot Springs, Steamboat Springs, Geiger Grade, and Virginia City, were used as sites for demonstrating the geologic applications of thermal infrared remote sensing. Corrected day and night images over Steamboat Springs were acquired by TIMS. These day-night images were combined together to produce a final processed temperature image, in which the temperature effects of albedo, topographic slope, and thermal inertia were minimized to facilitate the detection of geothermal anomalies. Spectral variations in emitted thermal energy were detected over the Geiger Grade and Virginia City areas Using the MODIS-ASTER Simulator (MASTER) and (SEBASS). MASTER thermal infrared image data allowed two primary mineralogic units in the Steamboat. Springs area to he identified: sinter and/or chalcedony deposits and quartz-alunite allteration, which have spectral emissivity features around 9.0 mu m; and clay-rich soil and clay alteration, which have spectral emissivity features around 9.7 mu m. The higher spatial and spectral resolution SEBASS data allowed six different alteration assemblages to be identified: quartz, alunite, pyrophyllite, feldspar, kaolinite, and montmorillonite and/or illite.
C1 [Taranik, James V.] Univ Nevada, Arthur Brant Lab Explorat Geophys, Mackay Sch Earth Sci & Engn, Reno, NV 89557 USA.
[Vaughan, R. Greg] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Taranik, James V.] NASA Headquarters, Off Space & Terr Applicat, Washington, DC USA.
[Vaughan, R. Greg] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Taranik, James V.] NASA, Washington, DC USA.
[Coolbaugh, Mark F.] Univ Nevada, Great Basin Ctr Geothermal Energy, Reno, NV 89557 USA.
RP Taranik, JV (reprint author), Univ Nevada, Arthur Brant Lab Explorat Geophys, Mackay Sch Earth Sci & Engn, Reno, NV 89557 USA.
EM jtaraink@mines.unr.edu
NR 80
TC 3
Z9 3
U1 1
U2 5
PU SOC ECONOMIC GEOLOGISTS, INC
PI LITTLETON
PA 7811 SHAFFER PKWY, LITTLETON, CO 80127 USA
SN 0741-0123
BN 978-1-934969-13-7
J9 REV ECON GEOL
PY 2009
VL 16
BP 41
EP 57
PG 17
WC Geology; Remote Sensing; Mining & Mineral Processing
SC Geology; Remote Sensing; Mining & Mineral Processing
GA BKK76
UT WOS:000268394400006
ER
PT S
AU Taranik, JV
Aslett, ZL
AF Taranik, James V.
Aslett, Zan L.
BE Bedell, R
Crosta, AP
Grunsky, E
TI Development of Hyperspectral Imaging for Mineral Exploration
SO REMOTE SENSING AND SPECTRAL GEOLOGY
SE Reviews in Economic Geology
LA English
DT Article; Book Chapter
ID SPECTROMETER AVIRIS; EO-1 HYPERION; AIRBORNE; SPECTROSCOPY; EARTH;
SPECTRORADIOMETER; NEVADA; IMAGES
AB The emergence of hyperspectral image data to remotely map minerals oil the surface of the Earth is the result of decades of laboratory, engineering, and physics research conducted by both commercial and government sectors. We present a synopsis of major events which culminated ill the development of mature hyperspectral reflectance and thermal emissivity data collection capabilities that are Currently available in worldwide capacity. Laboratory and field measurement efforts in the 1960s produced a foundation of knowledge pertaining to mineral spectral phenomenology. This in turn spurred the creation of first broadband multispectral and then hyperspectral data via airborne and spaceborne sensors to capitalize on mineral characteristics. Highly accurate radiometric calibration and atmospheric corrections allow remote measurements to closely emulate ground or laboratory measurements, while commercial hyperspectral data processing software enables timely analysis of the data. Increasing amounts of image data have been collected by a variety of commercial and government sensors, of which mineral exploration is a predominant application. The differences in sensor mid image data acquisition parameters directly affect the ability to map minerals. A brief analysis of Cuprite, Nevada, using multiple sensors is used as all example to illuminate factors of importance.
C1 [Taranik, James V.; Aslett, Zan L.] Univ Nevada, Arthur Brant Lab Explorat Geophys ABLE, Mackay Sch Earth Sci & Engn, Reno, NV 89557 USA.
[Taranik, James V.] NASA Headquarters, Off Space & Terr Applicat, Washington, DC USA.
[Taranik, James V.] NASA, Washington, DC USA.
RP Taranik, JV (reprint author), Univ Nevada, Arthur Brant Lab Explorat Geophys ABLE, Mackay Sch Earth Sci & Engn, Mail Stop 168, Reno, NV 89557 USA.
EM jtaranik@mines.unr.edu
NR 43
TC 7
Z9 7
U1 0
U2 2
PU SOC ECONOMIC GEOLOGISTS, INC
PI LITTLETON
PA 7811 SHAFFER PKWY, LITTLETON, CO 80127 USA
SN 0741-0123
BN 978-1-934969-13-7
J9 REV ECON GEOL
PY 2009
VL 16
BP 83
EP 95
PG 13
WC Geology; Remote Sensing; Mining & Mineral Processing
SC Geology; Remote Sensing; Mining & Mineral Processing
GA BKK76
UT WOS:000268394400008
ER
PT S
AU Gentile, A
Pierce, L
Ciraolo, G
Zhang, G
La Loggia, G
Nemani, R
AF Gentile, A.
Pierce, L.
Ciraolo, G.
Zhang, G.
La Loggia, G.
Nemani, R.
BE Neale, CMU
Maltese, A
TI Comparison between energy balance and mass balance models for actual
evapotranspiration assessment
SO REMOTE SENSING FOR AGRICULTURE, ECOSYSTEMS, AND HYDROLOGY XI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Remote Sensing for Agriculture, Ecosystems and Hydrology
XI as Part of the 16th International Symposium on Remote Sensing
CY AUG 31-SEP 03, 2009
CL Berlin, GERMANY
SP SPIE Europe
DE evapotranspiration; surface energy balance; water balance; viticulture;
Landsat 5
ID MAPPING EVAPOTRANSPIRATION; VINEYARD; SOIL
AB The assessment of the water needs for a specific crop has a fundamental importance in the management of water resources. The application of empirical models able to retrieve estimates of the actual evapotranspiration (ETa) to assess the need for water could give a valid tool for the planning of water supply, avoiding unnecessary water losses. In this context, two independent models for estimating actual evapotranspiration were compared. The first model is based on an energy balance and uses remotely sensed data and ancillary data from weather stations to assess the ETa. The second model also uses remotely sensed data and climatic data on a daily basis from a weather network. Field measurements are needed to calibrate both models. The study was conducted in a commercial vineyard located in Napa Valley (California). The observed range of ETdaily is included within the values measured by other authors. The results retrieved from both models show actual ETdaily values with a different trend over time; after mid-summer (early July) VSIM estimates of ETdaily trend downwards, while SEBAL estimates remain fairly constant.
This disagreement illustrate the difficulty in estimating the actual evapotranspiration at the end of season, when soil moisture gets low and vine water stress increases due to reducing stomatal conductance.
C1 [Gentile, A.; Ciraolo, G.; La Loggia, G.] Univ Palermo, DIIAA, Dept Hydraul Engn & Environm Applicat, I-90133 Palermo, Italy.
[Pierce, L.] Calif State Univ Monterey Bay, Div Sci & Environm Policy, Monterey, CA 93933 USA.
[Zhang, G.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA.
[Nemani, R.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
RP Gentile, A (reprint author), Univ Palermo, DIIAA, Dept Hydraul Engn & Environm Applicat, I-90133 Palermo, Italy.
OI Ciraolo, Giuseppe/0000-0001-6627-0175
NR 22
TC 0
Z9 0
U1 1
U2 4
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7777-4
J9 PROC SPIE
PY 2009
VL 7472
AR 747212
DI 10.1117/12.830229
PG 12
WC Agricultural Engineering; Remote Sensing; Optics
SC Agriculture; Remote Sensing; Optics
GA BDH76
UT WOS:000313294600025
ER
PT S
AU Kassianov, E
Ovchinnikov, M
Berg, LK
McFarlane, SA
Flynn, C
Ferrare, R
Hostetler, C
AF Kassianov, Evgueni
Ovchinnikov, Mikhail
Berg, Larry K.
McFarlane, Sally A.
Flynn, Connor
Ferrare, Richard
Hostetler, Chris
BE Picard, RH
Schafer, K
Comeron, A
Kassianov, E
Mertens, CJ
TI The 3D Radiative Effects of Clouds in Aerosol Retrieval: Can we Remove
Them?
SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XIV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT 14th Conference on Remote Sensing of Clouds and the Atmosphere
CY AUG 31-SEP 01, 2009
CL Berlin, GERMANY
SP SPIE Europe
DE Aerosol optical depth; cumulus clouds; multi-spectral reflectance; Monte
Carlo radiative transfer calculations; aircraft observations
ID SPECTRAL-RESOLUTION LIDAR; MODIS
AB We outline a new method, called the ratio method, developed to retrieve aerosol optical depth (AOD) under broken cloud conditions and present validation results from sensitivity and case studies. Results of the sensitivity study demonstrate that the ratio method, which exploits ratios of reflectances in the visible spectral range, has the potential for accurate AOD retrievals under different observational conditions and random errors in input data. Also, we examine the performance of the ratio method using aircraft data collected during the Cloud and Land Surface Interaction Campaign (CLASIC) and the Cumulus Humilis Aerosol Processing Study (CHAPS). Results of the case study suggest that the ratio method has the ability to retrieve AOD from multi-spectral aircraft observations of the reflected solar radiation.
C1 [Kassianov, Evgueni; Ovchinnikov, Mikhail; Berg, Larry K.; McFarlane, Sally A.; Flynn, Connor] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Ferrare, Richard; Hostetler, Chris] NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Kassianov, E (reprint author), Pacific NW Natl Lab, Richland, WA 99352 USA.
EM Evgueni.Kassianov@pnl.gov
RI Berg, Larry/A-7468-2016
OI Berg, Larry/0000-0002-3362-9492
FU National Aeronautics and Space Administration ( NASA) through the
Radiation Sciences Program; Office of Biological and Environmental
Research ( OBER) of the U. S. Department of Energy ( DOE) as part of the
Atmospheric Radiation Measurement ( ARM) Program; Atmospheric Science
Program ( ASP); Battelle for the DOE [DE- AC0676RLO 1830]; OE, OBER and
located at PNNL
FX This work was supported by the National Aeronautics and Space
Administration ( NASA) through the Radiation Sciences Program and the
Office of Biological and Environmental Research ( OBER) of the U. S.
Department of Energy ( DOE) as part of the Atmospheric Radiation
Measurement ( ARM) Program and Atmospheric Science Program ( ASP). The
Pacific Northwest National Laboratory ( PNNL) is operated by Battelle
for the DOE under contract DE- AC0676RLO 1830. This research was
performed in part using the Molecular Science Computing Facility ( MSCF)
in the Environmental Molecular Sciences Laboratory ( EMSL), a national
scientific user facility sponsored by the U. S. DOE, OBER and located at
PNNL.
NR 14
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7780-4
J9 PROC SPIE
PY 2009
VL 7475
AR UNSP 74750I
DI 10.1117/12.830179
PG 7
WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics
SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics
GA BA7EJ
UT WOS:000337499500013
ER
PT S
AU Krueger, A
Yang, K
Krotkov, N
AF Krueger, Arlin
Yang, Kai
Krotkov, Nickolay
BE Picard, RH
Schafer, K
Comeron, A
Kassianov, E
Mertens, CJ
TI Enhanced monitoring of sulfur dioxide sources with hyperspectral UV
sensors
SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XIV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT 14th Conference on Remote Sensing of Clouds and the Atmosphere
CY AUG 31-SEP 01, 2009
CL Berlin, GERMANY
SP SPIE Europe
DE Hyperspectral; Remote Sensing; UV spectrometer; Sulfur Dioxide; Volcanic
emissions; Air quality; Aviation hazards
ID OZONE MAPPING SPECTROMETER; EL-CHICHON; INSTRUMENT; GOME; TOMS
AB Sulfur dioxide, a short-lived atmospheric constituent, is oxidized to sulfate aerosols, a climate agent. Main sources are volcanoes, smelters, and fossil fuel combustion. Satellite monitoring of SO2 began with TOMS data in 1978 that detected volcanic eruption clouds. Hyperspectral instruments, like OMI and GOME, have a twenty-fold improvement in sensitivity. Degassing volcanoes, smelters, and large power plants are now monitored for a database of SO2 emission to the atmosphere. SO2 is a distinctive marker for volcanic ash clouds, a hazard to aircraft.
C1 [Krueger, Arlin] Univ Maryland Baltimore Cty, Joint Ctr Earth Sci Technol, Baltimore, MD 21250 USA.
[Yang, Kai; Krotkov, Nickolay] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA.
RP Krueger, A (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Sci Technol, Baltimore, MD 21250 USA.
EM akrueger@umbc.edu
RI Krotkov, Nickolay/E-1541-2012
OI Krotkov, Nickolay/0000-0001-6170-6750
FU NASA TOMS and OMI Science Teams; NASA Applications Program Cooperative
Agreement Grant [NNS06AA05G]
FX This work was supported by NASA TOMS and OMI Science Teams and by the
NASA Applications Program Cooperative Agreement Grant NNS06AA05G (NASA
research volcanic emissions data for Aviation Hazards). In-kind support
has been provided by NOAA/NESDIS and USGS.
NR 15
TC 0
Z9 0
U1 1
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7780-4
J9 PROC SPIE
PY 2009
VL 7475
AR UNSP 74750Y
DI 10.1117/12.830142
PG 9
WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics
SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics
GA BA7EJ
UT WOS:000337499500026
ER
PT S
AU Mertens, CJ
Xu, X
Fernandez, JR
Bilitza, D
Russell, JM
Mlynczak, MG
AF Mertens, C. J.
Xu, X.
Fernandez, J. R.
Bilitza, D.
Russell, J. M., III
Mlynczak, M. G.
BE Picard, RH
Schafer, K
Comeron, A
Kassianov, E
Mertens, CJ
TI Development of a Geomagnetic Storm Correction to the International
Reference Ionosphere E-Region Electron Densities Using TIMED/SABER
Observations
SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XIV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT 14th Conference on Remote Sensing of Clouds and the Atmosphere
CY AUG 31-SEP 01, 2009
CL Berlin, GERMANY
SP SPIE Europe
ID KINETIC TEMPERATURE; CORRECTION MODEL; CARBON-DIOXIDE; EMISSION; IRI2000
AB Auroral infrared emission observed from the TIMED/SABER broadband 4.3 um channel is used to develop an empirical geomagnetic storm correction to the International Reference Ionosphere (IRI) E-region electron densities. The observation-based proxy used to develop the storm model is SABER-derived NO+(v) 4.3 um volume emission rates (VER). A correction factor is defined as the ratio of storm-time NO+(v) 4.3 um VER to a quiet-time climatological averaged NO+(v) 4.3 um VER, which is linearly fit to available geomagnetic activity indices. The initial version of the E-region storm model, called STORM-E, is most applicable within the auroral oval region. The STORM-E predictions of E-region electron densities are compared to incoherent scatter radar electron density measurements during the Halloween 2003 storm events. Future STORM-E updates will extend the model outside the auroral oval.
C1 [Mertens, C. J.; Fernandez, J. R.; Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Xu, X.] SSAI Inc, Hampton, VA USA.
[Bilitza, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Russell, J. M., III] Hampton Univ, Hampton, VA 23668 USA.
RP Mertens, CJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
FU National Aeronautics and Space Administration [NNH06DA001N]
FX This material is based upon work supported by the National Aeronautics
and Space Administration under grant NNH06DA001N issued through the
Science Mission Directorate's Living With A Star Targeted Research and
Technology Program.
NR 14
TC 1
Z9 1
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7780-4
J9 PROC SPIE
PY 2009
VL 7475
AR UNSP 747508
DI 10.1117/12.829976
PG 12
WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics
SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics
GA BA7EJ
UT WOS:000337499500006
ER
PT S
AU Sano, I
Mukai, S
Mukai, M
Holben, B
Slutsker, I
AF Sano, I.
Mukai, S.
Mukai, M.
Holben, B.
Slutsker, I.
BE Picard, RH
Schafer, K
Comeron, A
Kassianov, E
Mertens, CJ
TI Estimation algorithm for aerosol properties from CAI on GOSAT
SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XIV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT 14th Conference on Remote Sensing of Clouds and the Atmosphere
CY AUG 31-SEP 01, 2009
CL Berlin, GERMANY
SP SPIE Europe
DE Aerosols; absorbing particles; GOSAT; CAI; GLI; MODIS; POLDER
ID OPTICAL-PROPERTIES; DIELECTRIC-CONSTANT; LAND SURFACES; SMOKE
AB Green house gases observational satellite (GOSAT) was successfully launched on 23 January in 2009 by JAXA. The satellite carries two sensors, Fourier Transform Spectrometer (FTS) and Cloud Aerosol Imager (CAI). The CAI has four observing wavelengths as 0.38, 0.67, 0.87 and 1.6 mu m. It is shown here that this CAI/0.38 mu m is a unique observing band among usual sensors as MODIS and so on, and it is useful to distinguish the aerosol characteristics of absorbing (e. g., biomass burning) or non-absorbing (e. g., sulfate). In other word, this work proposed a space based retrieval algorithm for atmospheric aerosols including estimation of the optical constant for biomass burning particles. Our algorithm aims to apply the combination use of near UV data with GOAT/CAI, the violet data with Aqua/MODIS and near-IR polarization data with PARASOL/POLDER. In practice the algorithm has been partly examined by using ADEOS-2 / GLI data.
C1 [Sano, I.; Mukai, S.] Kinki Univ, Fac Sci & Technol, 3-4-1 Kowakae, Higashi Osaka 5778502, Japan.
[Mukai, M.] Japan Aerosp Explorat Agcy, EORC, Tsukuba, Ibaraki 3058505, Japan.
[Holben, B.; Slutsker, I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sano, I (reprint author), Kinki Univ, Fac Sci & Technol, 3-4-1 Kowakae, Higashi Osaka 5778502, Japan.
FU GOSAT/CAI (NIES, Japan); GCOM-C/SGLI (JAXA, Japan); Ministry of
Education, Culture, Sports, Science and Technology in Japan [21120509]
FX The authors gratefully acknowledge the JAXA/EORC for GLI data
processing. This work was supported in part by grant for GOSAT/CAI
(NIES, Japan), GCOM-C/SGLI (JAXA, Japan), and by a Grant-in-Aid for
Scientific Research from the Ministry of Education, Culture, Sports,
Science and Technology in Japan (No. 21120509).
NR 18
TC 0
Z9 0
U1 1
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7780-4
J9 PROC SPIE
PY 2009
VL 7475
AR UNSP 74751E
DI 10.1117/12.830155
PG 8
WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics
SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics
GA BA7EJ
UT WOS:000337499500040
ER
PT S
AU Szewczyk, ZP
Priestley, KJ
AF Szewczyk, Z. Peter
Priestley, Kory J.
BE Picard, RH
Schafer, K
Comeron, A
Kassianov, E
Mertens, CJ
TI CERES (FM2) Field Campaigns of 2008
SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XIV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT 14th Conference on Remote Sensing of Clouds and the Atmosphere
CY AUG 31-SEP 01, 2009
CL Berlin, GERMANY
SP SPIE Europe
AB A Clouds and the Earth's Radiant Energy System instrument (FM2) on board the Terra satellite has been used in field campaigns to provide TOA radiance measurements. Using a special programmable azimuth plan scan (PAPS) mode, a scanner collects data over a specified Earth target or of a prescribed spatial orientation. This paper covers operational aspects of four field campaigns in which FM2 participated in 2008. These include the annual CERES/GERB comparison campaign carried out at the summer and winter solstices, an aerosol campaign over Beijing ran before, during and after Summer Olympics, calibration and validation of GERB radiances at the ground station in Alacante/Spain, and also a bi-weekly true long-track scan for comparison to true nadir instruments.
C1 [Szewczyk, Z. Peter] SAIC, Hampton, VA 23666 USA.
[Priestley, Kory J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Szewczyk, ZP (reprint author), SAIC, Hampton, VA 23666 USA.
EM z.peter.szewczyk@nasa.gov; kory.j.priestley@nasa.gov
NR 12
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7780-4
J9 PROC SPIE
PY 2009
VL 7475
AR UNSP 74750E
DI 10.1117/12.829854
PG 10
WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics
SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics
GA BA7EJ
UT WOS:000337499500010
ER
PT S
AU Cantrell, JH
AF Cantrell, John H.
BE Thompson, DO
Chimenti, DE
TI NONDESTRUCTIVE EVALUATION OF METAL FATIGUE USING NONLINEAR ACOUSTICS
SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 28A
AND 28B
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 35th Annual Review of Progress in Quantitative Nondestructive Evaluation
CY JUL 20-25, 2008
CL Univ Chicago, Chicago, IL
HO Univ Chicago
DE Nonlinear Acoustics; Metal Fatigue; Microelastic-Plastic Nonlinearity;
Dislocation Substructures
ID WAVY SLIP METALS; HARMONIC-GENERATION; ULTRASONIC-WAVES; DAMAGE
ACCUMULATION; SOLIDS
AB Safe-life and damage-tolerant design philosophies of high performance structures have driven the development of various methods to evaluate nondestructively the accumulation of damage in such structures resulting from cyclic loading. Although many techniques have proven useful, none has been able to provide an unambiguous, quantitative assessment of damage accumulation at each stage of fatigue from the virgin state to fracture. A method based on nonlinear acoustics is shown to provide such a means to assess the state of metal fatigue. The salient features of an analytical model are presented of the microelastic-plastic nonlinearities resulting from the interaction of an acoustic wave with fatigue-generated dislocation substructures and cracks that predictably evolve during the metal fatigue process. The interaction is quantified by the material (acoustic) nonlinearity parameter beta extracted from acoustic harmonic generation measurements. The beta parameters typically increase monotonically by several hundred percent over the fatigue life of the metal, thus providing a unique measure of the state of fatigue. Application of the model to aluminum alloy 2024-T4 and 410Cb stainless steel specimens fatigued using different loading conditions yields good agreement between theory and experiment. Application of the model and measurement technique to the on-site inspection of steam turbine blades is discussed.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA.
NR 22
TC 5
Z9 5
U1 0
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0629-2
J9 AIP CONF PROC
PY 2009
VL 1096
BP 19
EP 32
PG 14
WC Materials Science, Characterization & Testing; Physics, Applied
SC Materials Science; Physics
GA BKO01
UT WOS:000268740800002
ER
PT S
AU Cantrell, JH
AF Cantrell, John H.
BE Thompson, DO
Chimenti, DE
TI ACOUSTIC RECTIFICATION IN DISPERSIVE MEDIA
SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 28A
AND 28B
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 35th Annual Review of Progress in Quantitative Nondestructive Evaluation
CY JUL 20-25, 2008
CL Univ Chicago, Chicago, IL
HO Univ Chicago
DE Radiation-Induced Static Pulses; Dispersive Media; Solitons
ID RADIATION STRESS; SOLIDS
AB It is shown that the shapes of acoustic radiation-induced static strain and displacement pulses (rectified acoustic pulses) are defined locally by the energy density of the generating waveform. Dispersive properties are introduced analytically by assuming that the rectified pulses are functionally dependent on a phase factor that includes both dispersive and nonlinear terms. The dispersion causes an evolutionary change in the shape of the energy density profile that leads to the generation of solitons experimentally observed in fused silica.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA.
NR 7
TC 0
Z9 0
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0629-2
J9 AIP CONF PROC
PY 2009
VL 1096
BP 217
EP 223
PG 7
WC Materials Science, Characterization & Testing; Physics, Applied
SC Materials Science; Physics
GA BKO01
UT WOS:000268740800025
ER
PT S
AU Wincheski, B
Simpson, J
Hall, G
AF Wincheski, Buzz
Simpson, John
Hall, George
BE Thompson, DO
Chimenti, DE
TI EDDY CURRENT SYSTEM FOR DETECTION OF CRACKING BENEATH BRAIDING IN
CORRUGATED METAL HOSE
SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 28A
AND 28B
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 35th Annual Review of Progress in Quantitative Nondestructive Evaluation
CY JUL 20-25, 2008
CL Univ Chicago, Chicago, IL
HO Univ Chicago
DE Eddy Current; Fatigue Crack; Corrugated Metal Hose; Flex Hose; Space
Shuttle
AB In this paper an eddy current system for the detection of partially-through-the-thickness cracks in corrugated metal hose is presented. Design criteria based upon the geometry and conductivity of the part are developed and applied to the fabrication of a prototype inspection system. Experimental data are used to highlight the capabilities of the system and an image processing technique is presented to improve flaw detection capabilities. A case study for detection of cracking damage in a space shuttle radiator retract flex hoses is also presented.
C1 [Wincheski, Buzz] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Simpson, John] Lockheed Martin Space Operat, Hampton, VA 23681 USA.
[Hall, George] George Washington Univ, Washington, DC 20052 USA.
RP Wincheski, B (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
NR 5
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0629-2
J9 AIP CONF PROC
PY 2009
VL 1096
BP 371
EP +
PG 2
WC Materials Science, Characterization & Testing; Physics, Applied
SC Materials Science; Physics
GA BKO01
UT WOS:000268740800045
ER
PT S
AU Roth, DJ
Tokars, RP
Martin, RE
Rauser, RW
Aldrin, JC
AF Roth, D. J.
Tokars, R. P.
Martin, R. E.
Rauser, R. W.
Aldrin, J. C.
BE Thompson, DO
Chimenti, DE
TI ULTRASONIC PHASED ARRAY SIMULATIONS OF WELDED COMPONENTS AT NASA
SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 28A
AND 28B
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 35th Annual Review of Progress in Quantitative Nondestructive Evaluation
CY JUL 20-25, 2008
CL Univ Chicago, Chicago, IL
HO Univ Chicago
DE Nondestructive Evaluation; Computational Simulation; Ultrasonics; Weld;
Modeling; Phased Array
AB Comprehensive and accurate inspections of welded components have become of increasing importance as NASA develops new hardware such as Ares rocket segments for future exploration missions. Simulation and modeling will play an increasing role in the future for nondestructive evaluation in order to better understand the physics of the inspection process, to prove or disprove the feasibility for an inspection method or inspection scenario, for inspection optimization, for better understanding of experimental results, and for assessment of probability of detection. This study presents simulation and experimental results for an ultrasonic phased array inspection of a critical welded structure important for NASA future exploration vehicles.
C1 [Roth, D. J.; Tokars, R. P.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Rauser, R. W.] Univ Toledo, Toledo, OH USA.
RP Roth, DJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 13
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0629-2
J9 AIP CONF PROC
PY 2009
VL 1096
BP 1190
EP +
PG 2
WC Materials Science, Characterization & Testing; Physics, Applied
SC Materials Science; Physics
GA BKO01
UT WOS:000268740800151
ER
PT S
AU Johnston, PH
AF Johnston, P. H.
BE Thompson, DO
Chimenti, DE
TI ADDRESSING THE LIMIT OF DETECTABILITY OF RESIDUAL OXIDE DISCONTINUITIES
IN FRICTION STIR BUTT WELDS OF ALUMINUM USING PHASED ARRAY ULTRASOUND
SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 28A
AND 28B
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 35th Annual Review of Progress in Quantitative Nondestructive Evaluation
CY JUL 20-25, 2008
CL Univ Chicago, Chicago, IL
HO Univ Chicago
DE Ultrasonic NDE; Friction Stir Weld; Residual Oxide Discontinuity
AB This activity seeks to estimate a theoretical upper bound of detectability for a layer of oxide embedded in a friction stir weld in aluminum. The oxide is theoretically modeled as an ideal planar layer of aluminum oxide, oriented normal to an interrogating ultrasound beam. Experimentally-measured grain scattering level is used to represent the practical noise floor. Echoes from naturally-occurring oxides will necessarily fall below this theoretical limit, and must be above the measurement noise to be potentially detectable.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Johnston, PH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
NR 3
TC 1
Z9 2
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0629-2
J9 AIP CONF PROC
PY 2009
VL 1096
BP 1902
EP 1909
PG 8
WC Materials Science, Characterization & Testing; Physics, Applied
SC Materials Science; Physics
GA BKO01
UT WOS:000268740800243
ER
PT J
AU Keiser, GM
Adams, M
Bencze, WJ
Brumley, RW
Buchman, S
Clarke, B
Conklin, J
DeBra, DB
Dolphin, M
Hipkins, DN
Holmes, T
Everitt, CWF
Goebel, JH
Gill, D
Green, GB
Heifetz, M
Kolodziejczak, J
Li, J
Lipa, J
Lockhart, JM
Mester, JC
Muhlfelder, B
Ohshima, Y
Parkinson, BW
Salomon, M
Shestople, P
Silbergleit, AS
Stahl, K
Taber, MA
Turneaure, JP
Wang, S
Worden, P
AF Keiser, G. M.
Adams, M.
Bencze, W. J.
Brumley, R. W.
Buchman, S.
Clarke, B.
Conklin, J.
DeBra, D. B.
Dolphin, M.
Hipkins, D. N.
Holmes, T.
Everitt, C. W. F.
Goebel, J. H.
Gill, D.
Green, G. B.
Heifetz, M.
Kolodziejczak, J.
Li, J.
Lipa, J.
Lockhart, J. M.
Mester, J. C.
Muhlfelder, B.
Ohshima, Y.
Parkinson, B. W.
Salomon, M.
Shestople, P.
Silbergleit, A. S.
Stahl, K.
Taber, M. A.
Turneaure, J. P.
Wang, S.
Worden, P.
TI Gravity Probe B(*)
SO RIVISTA DEL NUOVO CIMENTO
LA English
DT Article
ID B RELATIVITY MISSION; GYROSCOPE; PERFORMANCE; SATELLITE; MOTION; ROTOR
AB This paper describes the flight hardware. on-orbit operations. and preliminary data analysis for the Gravity Probe B satellite.
C1 [Keiser, G. M.; Adams, M.; Bencze, W. J.; Brumley, R. W.; Buchman, S.; Clarke, B.; Conklin, J.; DeBra, D. B.; Dolphin, M.; Hipkins, D. N.; Holmes, T.; Everitt, C. W. F.; Goebel, J. H.; Gill, D.; Green, G. B.; Heifetz, M.; Li, J.; Lipa, J.; Mester, J. C.; Muhlfelder, B.; Ohshima, Y.; Parkinson, B. W.; Salomon, M.; Shestople, P.; Silbergleit, A. S.; Stahl, K.; Taber, M. A.; Turneaure, J. P.; Wang, S.; Worden, P.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Kolodziejczak, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Lockhart, J. M.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
RP Keiser, GM (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
NR 61
TC 8
Z9 8
U1 0
U2 1
PU SOC ITALIANA FISICA
PI BOLOGNA
PA VIA SARAGOZZA, 12, I-40123 BOLOGNA, ITALY
SN 0393-697X
EI 1826-9850
J9 RIV NUOVO CIMENTO
JI Riv. Nuovo Cimento
PY 2009
VL 32
IS 11
BP 555
EP 589
DI 10.1393/ncr/i2009-10049-y
PG 35
WC Physics, Multidisciplinary
SC Physics
GA 544RS
UT WOS:000273677400001
ER
PT S
AU Barringer, H
Havelund, K
Rydeheard, D
Groce, A
AF Barringer, Howard
Havelund, Klaus
Rydeheard, David
Groce, Alex
BE Bensalem, S
Peled, DA
TI Rule Systems for Runtime Verification: A Short Tutorial
SO RUNTIME VERIFICATION
SE Lecture Notes in Computer Science
LA English
DT Proceedings Paper
CT 9th International Workshop on Runtime Verification
CY JUN 26-28, 2009
CL Grenoble, FRANCE
DE Runtime verification; rule systems; temporal logic; code
instrumentation; log file analysis; Java; AspectJ; Python
AB In this tutorial, we introduce two rule-based systems for on and off-line trace analysis, RULER and LOGSCOPE. RULER is a conditional rule-based system, which has a simple and easily implemented algorithm for effective runtime verification, and into which one can compile a wide range of temporal logics and other specification formalisms used for runtime verification. Specifications can be parameterized with data, or even with specifications, allowing for temporal logic combinators to be defined. We outline a number of simple syntactic extensions of core RULER that can lead to further conciseness of specification but still enabling easy and efficient implementation. RuleR is implemented in Java and we will demonstrate its ease of use in monitoring Java programs. LOGSCOPE is a derivation of RULER adding a simple very user-friendly temporal logic. It was developed in Python, specifically for Supporting testing of spacecraft flight software for NASA's next 2011 Mars mission MSL (Mars Science Laboratory). The system has been applied by test engineers to analysis of log files generated by running the flight software. Detailed logging is already part of the system design approach, and hence there is no added instrumentation overhead caused by this approach. While post-mortem log analysis prevents the autonomous reaction to problems possible with traditional runtime verification, it provides a powerful tool for test automation. A new system is being developed that integrates features from both RULER and LOGSCOPE.
C1 [Barringer, Howard; Rydeheard, David] Univ Manchester, Sch Comp Sci, Oxford Rd, Manchester M13 9PL, Lancs, England.
[Havelund, Klaus] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Groce, Alex] Oregon State Univ, Sch Elect Engn & Comp Sci, Corvallis, OR 97331 USA.
RP Barringer, H (reprint author), Univ Manchester, Sch Comp Sci, Oxford Rd, Manchester M13 9PL, Lancs, England.
EM Howard.Barringer@manchester.ac.uk; Klaus.Havelund@jpl.nasa.gov;
David.Rydeheard@manchester.ac.uk; Alex@eecs.oregonstate.edu
NR 21
TC 5
Z9 5
U1 0
U2 0
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0302-9743
BN 978-3-642-04693-3
J9 LECT NOTES COMPUT SC
PY 2009
VL 5779
BP 1
EP +
PG 3
WC Computer Science, Hardware & Architecture; Computer Science, Theory &
Methods
SC Computer Science
GA BMU92
UT WOS:000273623300001
ER
PT S
AU Tran, D
Chien, S
Rabideau, G
Cichy, B
AF Tran, Daniel
Chien, Steve
Rabideau, Gregg
Cichy, Benjamin
BE Barley, M
Mouratidis, H
Unruh, A
Spears, D
Scerri, P
Massacci, F
TI Safe Agents in Space: Preventing and Responding to Anomalies in the
Autonomous Sciencecraft Experiment
SO SAFETY AND SECURITY IN MULTIAGENT SYSTEMS: RESEARCH RESULTS FROM
2004-2006
SE Lecture Notes in Artificial Intelligence
LA English
DT Article; Book Chapter
AB This paper describes the design of the Autonomous Sciencecraft Experiment, a software agent that has been running on-board the EO-1 spacecraft since 2003. The agent recognizes science events, retargets the spacecraft to respond to the science events, and reduces data downlink to only the highest value science data. The autonomous science agent was designed using a layered architectural approach with specific redundant safeguards to reduce the risk of an agent malfunction to the EO-1 spacecraft. The agent was designed to be "safe" by first preventing anomalies, then by automatically detecting and responding to them when possible. This paper describes elements of the design that increase the safety of the agent, several of the anomalies that occurred during the experiment, and how the agent responded to these anomalies.
C1 [Tran, Daniel; Chien, Steve; Rabideau, Gregg; Cichy, Benjamin] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Tran, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Daniel.Tran@jpl.nasa.gov; Steve.Chien@jpl.nasa.gov;
Gregg.Rabideau@jpl.nasa.gov; Benjamin.Cichy@jpl.nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 1
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0302-9743
BN 978-3-642-04878-4
J9 LECT NOTES ARTIF INT
PY 2009
VL 4324
BP 147
EP 161
D2 10.1007/978-3-642-04879-1
PG 15
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA BLW07
UT WOS:000271196900011
ER
PT S
AU Martin, C
Schreckenghost, D
Bonasso, P
AF Martin, Cheryl
Schreckenghost, Debra
Bonasso, Pete
BE Barley, M
Mouratidis, H
Unruh, A
Spears, D
Scerri, P
Massacci, F
TI Command and Authorization Services for Multiple Humans Interacting with
a Software Control Agent for Advanced Life Support
SO SAFETY AND SECURITY IN MULTIAGENT SYSTEMS: RESEARCH RESULTS FROM
2004-2006
SE Lecture Notes in Artificial Intelligence
LA English
DT Article; Book Chapter
ID INTELLIGENT CONTROL; SPACE
AB This paper describes current work developing command and authorization services to support the coordination of multiple humans and an autonomous control agent working on the same underlying advanced life support system. The primary goal of these services is to prevent unknowing or accidental conflicts from arising as a result of issuing commands or taking action on the system. Avoiding such conflicts minimizes the risk of interfering with the work of another agent or putting the system into an unsafe operating state. This paper provides an overview of the advanced life support system at NASA to which this work has been applied and then discusses details for authorization, overrides, and system reconfiguration for commanding.
C1 [Martin, Cheryl] Univ Texas Austin, Appl Res Labs, Austin, TX 78713 USA.
[Schreckenghost, Debra; Bonasso, Pete] NASA, Lyndon B Johnson Space Ctr, TRACLabs, Houston, TX 77058 USA.
RP Martin, C (reprint author), Univ Texas Austin, Appl Res Labs, POB 8029, Austin, TX 78713 USA.
EM cmartin@arlut.utexas.edu; ghost@ieee.org; r.p.bonasso@jsc.nasa.gov
NR 29
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0302-9743
BN 978-3-642-04878-4
J9 LECT NOTES ARTIF INT
PY 2009
VL 4324
BP 225
EP 240
D2 10.1007/978-3-642-04879-1
PG 16
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA BLW07
UT WOS:000271196900016
ER
PT J
AU Marshall, YY
AF Marshall, Yolanda Y.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Introduction to Space Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Editorial Material; Book Chapter
C1 NASA, Safety & Mission Assurance Directorate, Johnson Space Ctr, Houston, TX USA.
RP Marshall, YY (reprint author), NASA, Safety & Mission Assurance Directorate, Johnson Space Ctr, Houston, TX USA.
NR 2
TC 1
Z9 1
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 1
EP 5
DI 10.1016/B978-0-7506-8580-1.00001-4
PG 5
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700003
ER
PT B
AU O'Connor, B
AF O'Connor, Bryan
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Safety Design for Space Systems Preface
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Editorial Material; Book Chapter
C1 NASA, Washington, DC 20546 USA.
RP O'Connor, B (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP XXIII
EP XXIII
DI 10.1016/B978-0-7506-8580-1.00031-2
PG 1
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700001
ER
PT B
AU Musgrave, GE
AF Musgrave, Gary Eugene
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Safety Design for Space Systems Introduction
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Editorial Material; Book Chapter
C1 [Musgrave, Gary Eugene] NASA, NASA Payload Safety Review Panel, Johnson Space Ctr, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP XXV
EP XXV
DI 10.1016/B978-0-7506-8580-1.00032-4
PG 1
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700002
ER
PT J
AU Sgobba, T
Larsen, AM
Musgrave, GE
AF Sgobba, Tommaso
Larsen, Axel M. (Skip), Jr.
Musgrave, Gary E.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Basic Principles of Space Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 [Sgobba, Tommaso] European Space Agcy, European Space Res & Technol Ctr, Independent Flight Safety Off, NL-2200 AG Noordwijk, Netherlands.
[Larsen, Axel M. (Skip), Jr.; Musgrave, Gary E.] NASA, NASA Payload Safety Review Panel, Johnson Space Ctr, Houston, TX USA.
RP Sgobba, T (reprint author), European Space Agcy, European Space Res & Technol Ctr, Independent Flight Safety Off, NL-2200 AG Noordwijk, Netherlands.
NR 5
TC 1
Z9 1
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 163
EP 174
DI 10.1016/B978-0-7506-8580-1.00004-X
PG 12
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700006
ER
PT B
AU Prokhorov, KS
AF Prokhorov, Kimberlee S.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Life Support Systems Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 NASA, ISS Common Environm Team, Johnson Space Ctr, Houston, TX USA.
RP Prokhorov, KS (reprint author), NASA, ISS Common Environm Team, Johnson Space Ctr, Houston, TX USA.
NR 42
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 185
EP 224
DI 10.1016/B978-0-7506-8580-1.00006-3
PG 40
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700008
ER
PT B
AU Goodman, JR
Grosveld, FW
AF Goodman, Jerry R.
Grosveld, Ferdinand W.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Noise Control Design
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 [Goodman, Jerry R.] NASA, Acoust Working Grp, Houston, TX USA.
[Goodman, Jerry R.] NASA, Johnson Space Ctr, Houston, TX USA.
[Grosveld, Ferdinand W.] NASA Langley Res Ctr, Acoust & Fluid Mech Lockheed Martin Mission Serv, Houston, TX USA.
[Grosveld, Ferdinand W.] Univ Kansas, Lawrence, KS 66045 USA.
[Grosveld, Ferdinand W.] Old Dominion Univ, Norfolk, VA 23529 USA.
RP Goodman, JR (reprint author), NASA, Johnson Space Ctr, Houston, TX USA.
NR 20
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 341
EP 357
DI 10.1016/B978-0-7506-8580-1.00011-7
PG 17
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700013
ER
PT B
AU Pedley, MD
AF Pedley, Michael D.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Materials Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 NASA, Mat & Proc Branch, Johnson Space Ctr, Houston, TX USA.
RP Pedley, MD (reprint author), NASA, Mat & Proc Branch, Johnson Space Ctr, Houston, TX USA.
NR 20
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 359
EP 374
DI 10.1016/B978-0-7506-8580-1.00012-9
PG 16
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700014
ER
PT B
AU Pedley, MD
AF Pedley, Michael D.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Oxygen Systems Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 NASA, Mat & Proc Branch, Johnson Space Ctr, Houston, TX USA.
RP Pedley, MD (reprint author), NASA, Mat & Proc Branch, Johnson Space Ctr, Houston, TX USA.
NR 22
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 375
EP 402
DI 10.1016/B978-0-7506-8580-1.00013-0
PG 28
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700015
ER
PT B
AU Tadlock, DE
AF Tadlock, David E.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Avionics Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 [Tadlock, David E.] NASA, Operat Space Syst Support Off, Johnson Space Ctr, Houston, TX USA.
NR 25
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 403
EP 474
DI 10.1016/B978-0-7506-8580-1.00014-2
PG 72
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700016
ER
PT J
AU Leveson, NG
Weiss, KA
AF Leveson, Nancy G.
Weiss, Kathryn Anne
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Software System Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 [Leveson, Nancy G.] MIT, Boston, MA USA.
[Weiss, Kathryn Anne] CALTECH, NASA Jet Prop Lab, Flight Software & Data Syst Sect, Pasadena, CA 91125 USA.
RP Leveson, NG (reprint author), MIT, Boston, MA USA.
NR 32
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 475
EP 505
DI 10.1016/B978-0-7506-8580-1.00015-4
PG 31
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700017
ER
PT J
AU Jeevarajan, JA
AF Jeevarajan, Judith A.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Battery Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
ID LITHIUM-ION BATTERIES; CELLS; MECHANISMS; VOLTAGE
C1 NASA, Power Syst Branch, Johnson Space Ctr, Houston, TX USA.
RP Jeevarajan, JA (reprint author), NASA, Power Syst Branch, Johnson Space Ctr, Houston, TX USA.
NR 57
TC 1
Z9 1
U1 0
U2 1
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 507
EP 548
DI 10.1016/B978-0-7506-8580-1.00016-6
PG 42
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700018
ER
PT B
AU Moreland, DW
AF Moreland, Dean W.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Mechanical Systems Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 NASA, Payload Safety Review Panel, Johnson Space Ctr, Houston, TX USA.
RP Moreland, DW (reprint author), NASA, Payload Safety Review Panel, Johnson Space Ctr, Houston, TX USA.
NR 28
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 549
EP 606
DI 10.1016/B978-0-7506-8580-1.00017-8
PG 58
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700019
ER
PT B
AU Baumer, GJ
AF Baumer, Gregg John
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Failure Tolerance Design
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 [Baumer, Gregg John] NASA, Int Space Stn Safety Review Panel, Johnson Space Ctr, Houston, TX USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 653
EP 660
DI 10.1016/B978-0-7506-8580-1.00019-1
PG 8
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700021
ER
PT B
AU Van Tassel, KE
AF Van Tassel, Keith E.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Pyrotechnic Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 NASA, Johnson Space Ctr, Houston, TX USA.
RP Van Tassel, KE (reprint author), NASA, Johnson Space Ctr, Houston, TX USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 695
EP 704
DI 10.1016/B978-0-7506-8580-1.00021-X
PG 10
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700023
ER
PT B
AU Hornyak, D
AF Hornyak, David
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Emergency, Caution, and Warning System
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 NASA, Johnson Space Ctr, Houston, TX USA.
RP Hornyak, D (reprint author), NASA, Johnson Space Ctr, Houston, TX USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 725
EP 732
DI 10.1016/B978-0-7506-8580-1.00023-3
PG 8
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700025
ER
PT B
AU Victor, JM
AF Victor, Joe M.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Laser Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Victor, JM (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 733
EP 744
DI 10.1016/B978-0-7506-8580-1.00024-5
PG 12
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700026
ER
PT B
AU Kirkpatrick, P
Palo, T
AF Kirkpatrick, Paul
Palo, Thomas
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Safety Considerations for the Ground Environment
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 [Kirkpatrick, Paul] Ground Safety Review Panel, Kennedy Space Ctr, FL USA.
[Kirkpatrick, Paul; Palo, Thomas] NASA, Kennedy Space Ctr, FL USA.
RP Kirkpatrick, P (reprint author), Ground Safety Review Panel, Kennedy Space Ctr, FL USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 817
EP 828
DI 10.1016/B978-0-7506-8580-1.00026-9
PG 12
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700028
ER
PT J
AU Ruff, GA
Urban, DL
Pedley, MD
Johnson, PT
AF Ruff, Gary A.
Urban, David L.
Pedley, Michael D.
Johnson, Paul T.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Fire Safety
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
ID JET DIFFUSION FLAMES; LOW-VELOCITY FLOWS; PILOTED IGNITION;
CARBON-DIOXIDE; MICROGRAVITY; COMBUSTION; GRAVITY; SPREAD; FUELS; SMOKE
C1 [Ruff, Gary A.] NASA, Adv Capabil Project Off, Glenn Res Ctr, Cleveland, OH USA.
[Urban, David L.] NASA, Combust & Reacting Syst Branch, Space Proc & Experiments Div, Glenn Res Ctr, Cleveland, OH USA.
[Pedley, Michael D.] NASA, Mat & Proc Branch, Lyndon B Johnson Space Ctr, Houston, TX USA.
[Johnson, Paul T.] Boeing Co, Safety & Reliabil, Huntsville, AL USA.
RP Ruff, GA (reprint author), NASA, Adv Capabil Project Off, Glenn Res Ctr, Cleveland, OH USA.
NR 104
TC 1
Z9 1
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 829
EP 883
DI 10.1016/B978-0-7506-8580-1.00027-0
PG 55
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700029
ER
PT B
AU Baumer, GJ
AF Baumer, Gregg John
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Safe Without Services Design
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 [Baumer, Gregg John] Int Space Stn Safety Review Panel, Houston, TX USA.
[Baumer, Gregg John] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Baumer, GJ (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 885
EP 888
DI 10.1016/B978-0-7506-8580-1.00028-2
PG 4
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700030
ER
PT B
AU Stamatelatos, MG
Vesely, WE
Prassinos, PG
AF Stamatelatos, Michael G.
Vesely, William E.
Prassinos, Peter G.
BE Musgrave, GE
Larsen, AM
Sgobba, T
TI Probabilistic Risk Assessment with Emphasis on Design
SO SAFETY DESIGN FOR SPACE SYSTEMS
LA English
DT Article; Book Chapter
C1 [Stamatelatos, Michael G.; Vesely, William E.; Prassinos, Peter G.] NASA, Off Safety & Mission Assurance, Washington, DC 20546 USA.
RP Stamatelatos, MG (reprint author), NASA, Off Safety & Mission Assurance, Washington, DC 20546 USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER BUTTERWORTH-HEINEMANN
PI BURLINGTON
PA 30 CORPORATE DRIVE, STE 400, BURLINGTON, MA 01803 USA
BN 978-0-08-055922-3
PY 2009
BP 889
EP 911
DI 10.1016/B978-0-7506-8580-1.00029-4
PG 23
WC Engineering, Aerospace
SC Engineering
GA BGC95
UT WOS:000322363700031
ER
PT B
AU Russell, M
Lecakes, GD
Mandayam, S
Morris, JA
Turowski, M
Schmalzel, JL
AF Russell, Michael
Lecakes, George D., Jr.
Mandayam, Shreekanth
Morris, Jonathan A.
Turowski, Mark
Schmalzel, John L.
GP IEEE
TI Acquisition, Interfacing and Analysis of Sensor Measurements in a VR
Environment for Integrated Systems Health Management in Rocket Engine
Tests
SO SAS 2009 - IEEE SENSORS APPLICATIONS SYMPOSIUM, PROCEEDINGS
LA English
DT Proceedings Paper
CT 4th IEEE Sensors Applications Symposium
CY FEB 17-19, 2009
CL New Orleans, LA
SP IEEE Instrumentat & Measurement Soc
DE Data Acquisition; Network Interface; Failure Analysis; Virtual Reality;
Visualization
AB This paper presents our ongoing work in the area of using virtual reality (VR) environments for the integrated systems health management of complex test environments, such as those found in a rocket engine test stand. Specifically, the paper focuses on the design, development and implementation of a hardware-software framework for acquiring, interfacing, integrating and analyzing multiple sensor measurements for display inside of a VR environment. IEEE and OSA-CBM standards are used to design the acquisition and interface methods. Commercial off-the-shelf software is used for analysis and integration. Results demonstrating the application of our method to a rocket engine test stand are presented.
C1 [Russell, Michael; Lecakes, George D., Jr.; Mandayam, Shreekanth] Rowan Univ, Dept Elect & Comp Engn, Glassboro, NJ 08028 USA.
[Morris, Jonathan A.; Turowski, Mark; Schmalzel, John L.] NASA, Stennis Space Ctr, Bay St Louis, MS 39529 USA.
RP Russell, M (reprint author), Rowan Univ, Dept Elect & Comp Engn, Glassboro, NJ 08028 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4244-2786-4
PY 2009
BP 128
EP +
DI 10.1109/SAS.2009.4801792
PG 2
WC Engineering, Electrical & Electronic; Instruments & Instrumentation;
Remote Sensing
SC Engineering; Instruments & Instrumentation; Remote Sensing
GA BKL67
UT WOS:000268444000027
ER
PT B
AU Lecakes, GD
Russell, M
Mandayam, S
Morris, JA
Schmalzel, JL
AF Lecakes, George D., Jr.
Russell, Michael
Mandayam, Shreekanth
Morris, Jonathan A.
Schmalzel, John L.
GP IEEE
TI Visualization of Multiple Sensor Measurements in a VR Environment for
Integrated Systems Health Management in Rocket Engine Tests
SO SAS 2009 - IEEE SENSORS APPLICATIONS SYMPOSIUM, PROCEEDINGS
LA English
DT Proceedings Paper
CT 4th IEEE Sensors Applications Symposium
CY FEB 17-19, 2009
CL New Orleans, LA
SP IEEE Instrumentat & Measurement Soc
DE Virtual Reality; Visualization; Virtual Instrumentation; Condition Based
Monitoring; Graphical User Interface; Modeling and Simulation
AB This paper presents our continuing work in the area of using virtual reality (VR) environments for the integrated systems health management of complex test environments, such as those found in a rocket engine test stand. Specifically, the paper focuses on the design and development of a software framework for integrating and displaying multiple sensor measurements. Various forms of data are displayed inside the VR environment in conjunction with the associated graphics which correspond to the physical structure of the test-stand (piping, valves, sensors, etc.). Results demonstrating the application of our method for visualizing scalar, vector and system-state data are presented.
C1 [Lecakes, George D., Jr.; Russell, Michael; Mandayam, Shreekanth] Rowan Univ, Dept Elect & Comp Engn, Glassboro, NJ 08028 USA.
[Morris, Jonathan A.; Schmalzel, John L.] NASA, Stennis Space Ctr, Bay St Louis, MS 39529 USA.
RP Lecakes, GD (reprint author), Rowan Univ, Dept Elect & Comp Engn, Glassboro, NJ 08028 USA.
FU NASA, Space Center [NNS06AC08P, NNX07AO92H]
FX This work is supported by NASA John C. Stennis Space Center under Order
No. NNS06AC08P and Grant No. NNX07AO92H.
NR 8
TC 1
Z9 1
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4244-2786-4
PY 2009
BP 132
EP +
DI 10.1109/SAS.2009.4801793
PG 2
WC Engineering, Electrical & Electronic; Instruments & Instrumentation;
Remote Sensing
SC Engineering; Instruments & Instrumentation; Remote Sensing
GA BKL67
UT WOS:000268444000028
ER
PT B
AU Wang, CT
Woodard, SE
Taylor, BD
AF Wang, Chuantong
Woodard, Stanley E.
Taylor, Bryant D.
GP IEEE
TI Sensing of Multiple Unrelated Tire Parameters Using Electrically Open
Circuit Sensors Having no Electrical Connections
SO SAS 2009 - IEEE SENSORS APPLICATIONS SYMPOSIUM, PROCEEDINGS
LA English
DT Proceedings Paper
CT 4th IEEE Sensors Applications Symposium
CY FEB 17-19, 2009
CL New Orleans, LA
SP IEEE Instrumentat & Measurement Soc
DE Electrically open-circuit sensor; tire safety monitoring; magnetic field
response sensor; LC resonator; multifunctional tire sensor; SansEC
AB All sensors or sensor systems previously used for tire measurements have one common feature - the sensors are part of electrically closed circuits and electrical connections are used to form the closed circuits. In this paper, we present a new tire safety monitoring system using a recently developed method for designing, powering and interrogating sensors developed at NASA. In lieu of sensors being a collection of components assembled using electrical connections, the sensors are patterns of electrically conductive material that can store electric fields and magnetic fields without electrical connections. They are powered using oscillating magnetic fields and respond with their own magnetic fields whose signatures give information about the measured parameters. Because no electrical connections are used to power, communicate with the sensor or to make the sensor, there is no point on the sensor that if damaged, renders the sensor non-functional. Many damage events simply shift the sensor's frequency range. Survivability of the sensor allows it to continue measurement while damaged. The physical quantities to be measured are correlated to the sensor's magnetic field response amplitude, frequency and bandwidth. The proposed method measures wheel speed, rotation angle, direction, acceleration, temperature, damage and wear of tread element by using two or more sensors. In this study, two sensors are used. One of the sensors is coated with temperature sensitive dielectric material. The two sensors working cooperatively are able to measure the seven parameters. The results and multifunctional measurement strategies are presented.
C1 [Wang, Chuantong] Natl Inst Aerosp, Hampton, VA 23630 USA.
[Woodard, Stanley E.] NASA, Langley Res Ctr, Hampton, VA 23630 USA.
[Taylor, Bryant D.] ATK Space Div Res, Hampton, VA 23630 USA.
RP Wang, CT (reprint author), Natl Inst Aerosp, Hampton, VA 23630 USA.
EM C.Wang@nianet.org; Stanley.E.Woodard@nasa.gov; Bryant.D.Taylor@nasa.gov
NR 16
TC 1
Z9 1
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4244-2786-4
PY 2009
BP 142
EP +
PG 2
WC Engineering, Electrical & Electronic; Instruments & Instrumentation;
Remote Sensing
SC Engineering; Instruments & Instrumentation; Remote Sensing
GA BKL67
UT WOS:000268444000030
ER
PT B
AU Orton, GS
Baines, KH
Cruikshank, D
Cuzzi, JN
Krimigis, SM
Miller, S
Lellouch, E
AF Orton, Glenn S.
Baines, Kevin H.
Cruikshank, Dale
Cuzzi, Jeffrey N.
Krimigis, Stamatios M.
Miller, Steve
Lellouch, Emmanuel
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Review of Knowledge Prior to the Cassini-Huygens Mission and Concurrent
Research
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Review; Book Chapter
ID HUBBLE-SPACE-TELESCOPE; RESOLVED INFRARED OBSERVATIONS; 1990 EQUATORIAL
DISTURBANCE; OUTER SOLAR-SYSTEM; RADIO ASTRONOMY OBSERVATIONS;
PARTICLE-SIZE DISTRIBUTIONS; PLANETARY RING-SYSTEMS; SEASONAL CLIMATE
MODEL; SATURNS H-3(+) AURORA; AMMONIA ICE PARTICLES
AB The scientific achievements of the Cassini-Huygens mission have been based on previous decades of investigations from ground-based observations, an intensive 2-year time span of exploration by three spacecraft (Pioneer Saturn, Voyagers 1 and 2) in 1979-1981, and observations by the Infrared Space Observatory, the International Ultraviolet Explorer, and Hubble Space Telescope. We review both these and research concurrent with the nominal mission which often provided directly supporting results. Saturn's "bulk" composition remains uncertain. Its few discrete cloud features include a hexagon near the sorth pole, and a major episodic storm at the equator. A heterogeneous cloud field at depth was uncovered at 5 mu m. Temperatures are enhanced at Saturn's south pole both from seasonal variations of sunlight and from dynamical forcing. Zonal winds peak near Saturn's equator. Saturn possesses a well-defined ionosphere, but with significant structure and variability. The magnetic field is aligned to within a degree of Saturn's rotation axis. An equatorial ring current of similar to 10(7) A has been inferred, with inner and outer radii of similar to 8 and similar to 16 R-S. Radiation belts at Saturn are well-established up to the edge of the outer rings, and the higherenergy (>1 meV) proton component is readily absorbed by the inner satellites. The magnetosphere includes both a well-developed plasma sheet and a magneto-tail. Radio emissions and plasma waves exist throughout, and the auroral kilometric radiation (SKR), modulated at 10 h 39.4 min, has been widely adopted as a measure of the internal rotation. The plasma population consists principally of protons, but with a heavier component close to the equatorial plane widely assumed to be nitrogen or oxygen. Saturn's ring system is the most accessible in the solar system and consists of three primary components, the A, B and C rings. The A ring contains a large number of spiral density wages generated by gravitational interactions with Saturn's satellites. Other rings include the tenuous D, E, and G rings, and the narrow F ring. Voyager imaging detected "spokes" in the rings and, through occultation studies, an intricate detailed radial structure. Spectroscopic information on the icy satellites reveals the presence of crystalline water ice, mixed with a non-ice surface component with strong UV absorption. Detailed information on the geology of, Saturn's eight largest icy satellites before the Cassini arrival was based entirely on Voyager observations. They were found to be surprisingly heterogeneous, with implied internal activity in Enceladus and the dichotomous albedo of Iapetus being two of the biggest mysteries. Among the smaller satellites are those embedded in Saturn's rings and irregular captured satellites outside the orbits of the co-planar satellites.
C1 [Orton, Glenn S.; Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cruikshank, Dale; Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Krimigis, Stamatios M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Krimigis, Stamatios M.] Acad Athens, Athens 10679, Greece.
[Miller, Steve] Univ London Imperial Coll Sci Technol & Med, London WC1E 6BT, England.
[Lellouch, Emmanuel] Observ Paris, F-92195 Meudon, France.
RP Orton, GS (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 363
TC 4
Z9 4
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 9
EP 54
DI 10.1007/978-1-4020-9217-6_2
D2 10.1007/978-1-4020-9217-6
PG 46
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000002
ER
PT B
AU Johnson, TV
Estrada, PR
AF Johnson, Torrence V.
Estrada, Paul R.
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Origin of the Saturn System
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID OUTER SOLAR-SYSTEM; DIFFERENTIATED INTERNAL STRUCTURE; CASSINI IMAGING
SCIENCE; LATE HEAVY BOMBARDMENT; GRAVITY-FIELD; GIANT PLANETS; IRREGULAR
SATELLITES; INTERIOR STRUCTURE; KUIPER-BELT; COLLISIONAL EVOLUTION
AB Cassini mission results are providing new insights into the origin of the Saturn system and giant planet satellite systems generally. The chapter discusses current models for the formation of giant planets and their satellites and reviews major Cassini findings which help advance our understanding of the system's formation and evolution to its current state.
C1 [Johnson, Torrence V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Estrada, Paul R.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
RP Johnson, TV (reprint author), CALTECH, Jet Prop Lab, MS 301-345E,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Torrence.V.Johnson@jpl.nasa.gov; Paul.R.Estrada@nasa.gov
NR 148
TC 7
Z9 7
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 55
EP 74
DI 10.1007/978-1-4020-9217-6_3
D2 10.1007/978-1-4020-9217-6
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000003
ER
PT B
AU Hubbard, WB
Dougherty, MK
Gautier, D
Jacobson, R
AF Hubbard, William B.
Dougherty, Michele K.
Gautier, Daniel
Jacobson, Robert
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI The Interior of Saturn
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
DE Saturn interior; Saturn atmosphere; Saturn rotation; Jupiter interior
ID INTERNAL STRUCTURE; GIANT PLANETS; HELIUM; HYDROGEN; OCCULTATION;
ATMOSPHERE; ABUNDANCE; PRESSURE; EQUATION; JUPITER
AB A source of uncertainty in Saturn interior models is the lack of a unique rotation rate to be ascribed to the deep (metallic-hydrogen) interior. As a result, models are not uniquely constrained by measured gravitational multiple coefficients. Further uncertainty is associated with the effect of a multiplicity of rotation periods due to zonal flows of unknown magnitude and depth (and therefore unknown mass). Nevertheless, the inference that Saturn has a large core of mass 15-20 ME (Earth masses) is robust. The equation of state of dense hydrogen-helium mixtures is one area where uncertainty has been much reduced, thanks to new first-principles simulations. However, because there is still uncertainty in Saturn's interior temperature profile, a variety of mantle metallicities and core masses could still fit the constraints, and the question of interior helium separation is still unsettled.
C1 [Hubbard, William B.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Dougherty, Michele K.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London, England.
[Jacobson, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Gautier, Daniel] Observ Paris Site Meudon, Paris, France.
RP Hubbard, WB (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
NR 22
TC 9
Z9 9
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 75
EP 81
DI 10.1007/978-1-4020-9217-6_4
D2 10.1007/978-1-4020-9217-6
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000004
ER
PT B
AU Del Genio, AD
Achterberg, RK
Baines, KH
Flasar, FM
Read, PL
Sanchez-Lavega, A
Showman, AP
AF Del Genio, Anthony D.
Achterberg, Richard K.
Baines, Kevin H.
Flasar, F. Michael
Read, Peter L.
Sanchez-Lavega, Agustin
Showman, Adam P.
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Saturn Atmospheric Structure and Dynamics
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID SHALLOW-WATER TURBULENCE; HUBBLE-SPACE-TELESCOPE; NORTH POLAR SPOT;
GREAT RED SPOT; VOYAGER INFRARED MEASUREMENTS; POTENTIAL-VORTICITY
DYNAMICS; 1990 EQUATORIAL DISTURBANCE; ROTATING SPHERICAL-SHELLS;
JUPITER UPPER TROPOSPHERE; LARGE-SCALE INSTABILITIES
AB Saturn inhabits a dynamical regime of rapidly rotating, internally heated atmospheres similar to Jupiter. Zonal winds have remained fairly steady since the time of Voyager except in the equatorial zone and slightly stronger winds occur at deeper levels. Eddies supply energy to the jets at a rate somewhat less than on Jupiter and mix potential vorticity near westward jets. Convective clouds exist preferentially in cyclonic shear regions as on Jupiter but also near jets, including major outbreaks near 35 S associated with Saturn electrostatic discharges, and in sporadic giant equatorial storms perhaps generated froth frequent events at depth. The implied meridional circulation at and below the visible cloud tops consists of upwelling (downwelling) at cyclonic (anti-cyclonic) shear latitudes. Thermal winds decay upward above the clouds, implying a reversal of the circulation there. Warm-core vortices with associated cyclonic circulations exist at both poles, including surrounding thick high clouds at the south pole. Disequilibrium gas concentrations in the tropical upper troposphere imply rising motion there. The radiative-convective boundary and tropopause occur at higher pressure in the southern (summer) hemisphere due to greater penetration of solar heating there. A temperature "knee" of warm air below the tropopause, perhaps due to haze heating, is stronger in the summer hemisphere as well. Saturn's south polar stratosphere is warmer than predicted by radiative models and enhanced in ethane, suggesting subsidence-driven adiabatic warming there. Recent modeling advances suggest that shallow weather layer theories of jet pumping may be viable if water condensation is the source of energy input driving the flow, and that deep convective cylinder models with a sufficiently large tangent cylinder radius can reproduce observed flow features as well.
C1 [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Achterberg, Richard K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sanchez-Lavega, Agustin] Univ Basque Country, Dept Fis Aplicada, Bilbao 48013, Spain.
[Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Read, Peter L.] Clarendon Lab, Oxford OX1 3PU, England.
RP Del Genio, AD (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
RI Flasar, F Michael/C-8509-2012;
OI Sanchez-Lavega, Agustin/0000-0001-7355-1522
NR 225
TC 26
Z9 26
U1 1
U2 6
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 113
EP 159
DI 10.1007/978-1-4020-9217-6_6
D2 10.1007/978-1-4020-9217-6
PG 47
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000006
ER
PT B
AU West, RA
Baines, KH
Karkoschka, E
Sanchez-Lavega, A
AF West, R. A.
Baines, K. H.
Karkoschka, E.
Sanchez-Lavega, A.
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Clouds and Aerosols in Saturn's Atmosphere
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID 1990 EQUATORIAL DISTURBANCE; SPACE TELESCOPE OBSERVATIONS; NEAR-IR
SPECTROPHOTOMETRY; AMMONIA ICE; JOVIAN PLANETS; VERTICAL STRUCTURE;
UPPER TROPOSPHERE; HAZE FORMATION; JUPITER; PHOTOMETRY
AB In this chapter we review the photochemical and thermochemical equilibrium theories for the formation of condensate clouds and photochemical haze in Saturn's upper troposphere and stratosphere and show the relevant observations from ground-based and spacecraft instruments. Based on thermochemical equilibrium models we expect ammonia ice crystals to dominate in the high troposphere. There is very little spectral evidence to confirm this idea. Thanks to a stellar occultation observed by the Cassini VIMS instrument we now have spectral evidence for a hydrocarbon stratospheric haze component, and we still seek evidence for an expected diphosphine stratospheric haze component. The vertical distributions of stratospheric and upper tropospheric hazes have been mapped well with ground-based and Hubble Space telescope data, and Cassini data are beginning to add to this picture. Polar stratospheric aerosols are dark at UV wavelengths and exhibit strong Rayleigh-like polarization which suggests that auroral processes are important for their formation as is the case for the jovian polar stratospheric haze. The cloud and haze structure exhibits a variety of temporal variation, including seasonal change, long-term secular change near the equator, and short-term changes with a complicated latitudinal structure, and still not understood. Cassini instruments, especially the VIMS instrument, show an abundance of small-scale structure (convective clouds) at a pressure near 2 bar.
C1 [West, R. A.; Baines, K. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Karkoschka, E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Sanchez-Lavega, A.] Univ Basque Country, ETS Ingenieros, Dept Fis Aplicada 1, E-48080 Bilbao, Spain.
RP West, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
OI Sanchez-Lavega, Agustin/0000-0001-7355-1522
NR 59
TC 26
Z9 26
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 161
EP 179
DI 10.1007/978-1-4020-9217-6_7
D2 10.1007/978-1-4020-9217-6
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000007
ER
PT B
AU Nagy, AF
Kliore, AJ
Mendillo, M
Miller, S
Moore, L
Moses, JI
Muller-Wodarg, I
Shemansky, D
AF Nagy, Andrew F.
Kliore, Arvydas J.
Mendillo, Michael
Miller, Steve
Moore, Luke
Moses, Julianne I.
Mueller-Wodarg, Ingo
Shemansky, Don
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Upper Atmosphere and Ionosphere of Saturn
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID EXTREME-ULTRAVIOLET OBSERVATIONS; JOVIAN UPPER-ATMOSPHERE;
PLANETARY-ATMOSPHERES; OCCULTATION MEASUREMENTS; THERMAL PROFILES;
CROSS-SECTIONS; OUTER PLANETS; JUPITER; H-3(+); THERMOSPHERE
AB This chapter summarizes our current understanding of the upper atmosphere and ionosphere of Saturn. We summarize the available observations and the various relevant models associated with these regions. We describe what is currently known, outline any controversies and indicate how future observations can help in advancing our understanding of the various controlling physical and chemical processes.
C1 [Nagy, Andrew F.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Kliore, Arvydas J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mendillo, Michael; Moore, Luke] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Miller, Steve] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Moses, Julianne I.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Mueller-Wodarg, Ingo] Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England.
[Shemansky, Don] Planetary & Space Sci Div, Pasadena, CA 91107 USA.
RP Nagy, AF (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RI Mendillo, Michael /H-4397-2014; Moses, Julianne/I-2151-2013
OI Moses, Julianne/0000-0002-8837-0035
NR 106
TC 28
Z9 28
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 181
EP 201
DI 10.1007/978-1-4020-9217-6_8
D2 10.1007/978-1-4020-9217-6
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000008
ER
PT B
AU Mauk, BH
Hamilton, DC
Hill, TW
Hospodarsky, GB
Johnson, RE
Paranicas, C
Roussos, E
Russell, CT
Shemansky, DE
Sittler, EC
Thorne, RM
AF Mauk, B. H.
Hamilton, D. C.
Hill, T. W.
Hospodarsky, G. B.
Johnson, R. E.
Paranicas, C.
Roussos, E.
Russell, C. T.
Shemansky, D. E.
Sittler, E. C., Jr.
Thorne, R. M.
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Fundamental Plasma Processes in Saturn's Magnetosphere
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID NARROWBAND ELECTROMAGNETIC EMISSIONS; NONTHERMAL CONTINUUM RADIATION;
INTERPLANETARY MAGNETIC-FIELD; RADIO ASTRONOMY OBSERVATIONS; ENERGETIC
CHARGED-PARTICLES; PITCH-ANGLE DIFFUSION; NEUTRAL CLOUD THEORY;
ION-CYCLOTRON WAVES; DEPLETED FLUX TUBES; JOVIAN MAGNETOSPHERE
AB In this chapter, we review selected fundamental plasma processes that control the extensive space environment, or magnetosphere, of Saturn (see Chapter 9, for the global context). This writing occurs at a point in time when some measure of maturity has been achieved in our understanding of the operations of Saturn's magnetosphere and its relationship to those of Earth and Jupiter. Our understanding of planetary magnetospheres has exploded in the past decade or so partly because of the presence of orbiting spacecraft (Galileo and Cassini) as well as remote sensing assets (e.g., Hubble Space Telescope). This book and chapter are intended to take stock of where we are in our understanding of Saturn's magnetosphere following the successful return and analysis of extensive sets of Cassini data. The end of the prime mission provides us with an opportunity to consolidate older and newer work to provide guidance for continuing investigations.
C1 [Mauk, B. H.; Paranicas, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Hamilton, D. C.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Hill, T. W.] Rice Univ, Dept Phys & Astron, Houston, TX USA.
[Hospodarsky, G. B.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Johnson, R. E.] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA USA.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Shemansky, D. E.] Planetary & Space Sci Div, Pasadena, CA USA.
[Sittler, E. C., Jr.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Thorne, R. M.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90024 USA.
[Roussos, E.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
RP Mauk, BH (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
EM Barry.mauk@jhuapl.edu
RI Paranicas, Christopher/B-1470-2016; Mauk, Barry/E-8420-2017;
OI Paranicas, Christopher/0000-0002-4391-8255; Mauk,
Barry/0000-0001-9789-3797; Hamilton, Douglas/0000-0001-6103-8019;
Hospodarsky, George/0000-0001-9200-9878; Roussos,
Elias/0000-0002-5699-0678; Russell, Christopher/0000-0003-1639-8298
NR 310
TC 47
Z9 47
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 281
EP 331
DI 10.1007/978-1-4020-9217-6_11
D2 10.1007/978-1-4020-9217-6
PG 51
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000011
ER
PT B
AU Schmidt, J
Ohtsuki, K
Rappaport, N
Salo, H
Spahn, F
AF Schmidt, Juergen
Ohtsuki, Keiji
Rappaport, Nicole
Salo, Heikki
Spahn, Frank
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Dynamics of Saturn's Dense Rings
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID PARTICLE-SIZE DISTRIBUTIONS; AZIMUTHAL BRIGHTNESS VARIATIONS; VOYAGER-1
RADIO OCCULTATION; SELF-GRAVITATING PARTICLES; NARROW PLANETARY RINGS;
OPTICAL DEPTH PROFILE; N-BODY SIMULATIONS; NEARBY GAP EDGE; F-RING;
B-RING
AB The Cassini mission to Saturn opened a new era in the research of planetary rings, bringing data in unprecedented detail, monitoring the structure and properties of Saturn's ring system. The question of ring dynamics is to identify and understand underlying physical processes and to connect them to the observations in terms of mathematical models and computer simulations. For Saturn's dense rings important physical processes are dissipative collisions between ring particles, their motion in Saturn's gravity field, their mutual self-gravity, and the gravitational interaction with Saturn's moons, exterior to or embedded in the rings.
The importance of the rings' self-gravity became strikingly clear from the identification of gravitational wakes in Cassini data nearly everywhere in the A and B rings. Self-gravity wakes imply that the rings are in a flat, dynamically cold state, ring particles colliding very dissipatively, being densely packed in the ring plane, continuously forming transient gravitationally bound opaque clumps, that are disrupted again by shear on orbital timescales. Current mathematical dynamical models usually treat self-gravity in an approximate manner, which does not lead to a wake state.
The dense packing of ring particles, in turn, strongly influences the collisional dynamics, since the mean free path of the particles is then comparable to or smaller than the particle size. This leads to a strong nonlocal component of pressure and momentum transport, which determines the viscous evolution of the rings, the damping of density waves, as well as the stability properties of the ring's flow. A strong nonlocal contribution to viscosity is, for instance, favorable for viscous overstability, leading to axisymmetric waves of about 100 m wavelength. Such wavelike perturbations in the ring's opacity, consistent with overstability, are seen in Cassini stellar and radio occultations.
A classical topic of ring dynamics is the interaction of moons and rings. On the one hand, there are exterior moons with resonances in the rings, creating numerous density and bending waves. With the large sets of Cassini occultation and imaging data, improved estimates of the ring surface mass density and viscosity are obtained from fits of the observations to dynamical models. On the other hand, the embedded moons Pan and Daphnis open the Encke and Keeler gaps, respectively, and moonlets in the rings, too small to open a circumferential gap, are found to produce a characteristic propeller structure.
Comparison between theoretical studies and Cassini observations of thermal emission from the rings provides constraints on spin rates of ring particles, which are otherwise not directly observable. The size distribution of particles and small moonlets embedded in the rings, together with the observed shapes and internal densities of small moons just exterior to the rings, underline the importance of accretion and fragmentation for the dynamical evolution of Saturn's ring system.
C1 [Schmidt, Juergen; Spahn, Frank] Univ Potsdam, Inst F Phys & Astron, Potsdam, Germany.
[Rappaport, Nicole] JPL, Pasadena, CA USA.
[Salo, Heikki] Univ Oulu, Div Astron, Dept Phys Sci, Oulu, Finland.
[Ohtsuki, Keiji] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Ohtsuki, Keiji] Kobe Univ, Dept Earth & Planet Sci, Kobe, Hyogo, Japan.
[Ohtsuki, Keiji] Kobe Univ, Ctr Planet Sci, Kobe, Hyogo, Japan.
RP Schmidt, J (reprint author), Univ Potsdam, Inst F Phys & Astron, Potsdam, Germany.
NR 278
TC 34
Z9 34
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 413
EP 458
DI 10.1007/978-1-4020-9217-6_14
D2 10.1007/978-1-4020-9217-6
PG 46
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000014
ER
PT B
AU Cuzzi, J
Clark, R
Filacchione, G
French, R
Johnson, R
Marouf, E
Spilker, L
AF Cuzzi, Jeff
Clark, Roger
Filacchione, Gianrico
French, Richard
Johnson, Robert
Marouf, Essam
Spilker, Linda
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Ring Particle Composition and Size Distribution
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; SATURNS MAIN RINGS; POLYCYCLIC
AROMATIC-HYDROCARBONS; VOYAGER-1 RADIO OCCULTATION; INFRARED
OPTICAL-PROPERTIES; SOLAR-SYSTEM BODIES; WATER-VAPOR PLUME;
CASSINI-VIMS; PLANETARY RINGS; PHASE CURVES
AB We review recent progress concerning the composition and size distribution of the particles in Saturn's main ring system, and describe how these properties vary from place to place. We discuss how the particle size distribution is measured, and how it varies radially. We note the discovery of unusually large "particles" in restricted radial bands. We discuss the properties of the grainy regoliths of the ring particles. We review advances in understanding of ring particle composition from spectrophotometry at UV, visual and near-IR wavelengths, multicolor photometry at visual wavelengths, and thermal emission. We discuss the observed ring atmosphere and its interpretation and, briefly, models of the evolution of ring composition. We connect the ring composition with what has been learned recently about the composition of other icy objects in the Saturn system and beyond. Because the rings are so thoroughly and rapidly structurally evolved, the composition of the rings may be our best clue as to their origin; however, the evolution of ring particle composition over time must first be understood.
C1 [Cuzzi, Jeff] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Clark, Roger] US Geol Survey, Denver, CO 80225 USA.
[French, Richard] Wellesley Coll, Wellesley, MA 02181 USA.
[Johnson, Robert] Univ Virginia, Charlottesville, VA USA.
[Marouf, Essam] San Jose State Univ, San Jose, CA 95192 USA.
[Spilker, Linda] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Filacchione, Gianrico] Ist Astrofis Spaziale & Fis Cosm, Rome, Italy.
RP Cuzzi, J (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
OI Filacchione, Gianrico/0000-0001-9567-0055
NR 197
TC 57
Z9 57
U1 0
U2 8
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 459
EP 509
DI 10.1007/978-1-4020-9217-6_15
D2 10.1007/978-1-4020-9217-6
PG 51
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000015
ER
PT B
AU Matson, DL
Castillo-Rogez, JC
Schubert, G
Sotin, C
McKinnon, WB
AF Matson, Dennis L.
Castillo-Rogez, Julie C.
Schubert, Gerald
Sotin, Christophe
McKinnon, William B.
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI The Thermal Evolution and Internal Structure of Saturn's Mid-Sized Icy
Satellites
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID TEMPERATURE-DEPENDENT VISCOSITY; INFINITE PRANDTL NUMBER; STAGNANT LID
CONVECTION; CHONDRITE PARENT BODIES; LATE HEAVY BOMBARDMENT; OUTER
SOLAR-SYSTEM; INTERIOR STRUCTURE; LIQUID WATER; GALILEAN SATELLITES;
TERRESTRIAL PLANETS
AB The Cassini-Huygens mission is returning new geophysical data for the midsize, icy satellites of Saturn (i.e., satellites with radii between 100 and 1,000 km). These data have enabled a new generation of geophysical model studies for Phoebe, Iapetus, Rhea, Mimas, Tethys, Dione, as well as Enceladus (which is addressed in a separate chapter in this book). In the present chapter we consider the new model studies that have reported significant results elucidating the evolutionary histories and internal structures of these satellites. Those results have included their age, the development of their internal structures and mineralogies, which for greatest fidelity must be done concomitantly with coupled dynamical evolutions. Surface areas, volumes, bulk densities, spin rates, orbit inclinations, eccentricities, and distance from Saturn have changed as the satellites have aged. Heat is required to power the satellites' evolution, but is not overly abundant for the midsized satellites. All sources of heat must be evaluated and taken into account. This includes their intensities and when they occur and are available to facilitate evolution, both internal and dynamical. The mechanisms of heat transport must also be included. However, to model these to high fidelity the material properties of the satellite interiors must be accurately known. This is not the case. Thus, much of the chapter is devoted to discussion of what is known about these properties and how the uncertainties affect the estimation of heat sources, transport processes, and the consequential changes in composition and evolution. Phoebe has an oblate shape that may be in equilibrium with its spin period of similar to 9.3 h. Its orbital properties suggest that it is not one of the regular satellites, but is a captured body. Its density is higher than that of the other satellites, consistent with formation in the solar nebula rather than from material around Saturn. Oblate shape and high density are unusual for objects in this size range, and may indicate that Phoebe was heated by Al-26 decay soon after its formation, which is consistent with some models of the origin of Kuiper-Belt objects. lapetus has the shape of a hydrostatic body with a rotation period of 16 h. It subsequently despun to its current synchronous rotation state, similar to 79 day period. These observations are sufficient to constrain the required heating in Iapetus' early history, suggesting that it formed several My after CAI condensation. Since Saturn had to be present for Iapetus to form, this date also constrains the age of Saturn and how long it took to form. Both shape and gravitational data are available for Rhea. Gravity data were obtained from the single Cassini flyby during the prime mission and within the uncertainties cannot distinguish between hydrostatic and non-hydrostatic gravitational fields. Both Dione and Tethys display evidence of smooth terrains, with Dione's appearing considerably younger. Both are conceivably linked to tidal heating in the past, but the low rock abundance within Tethys and the lack of eccentricity excitation of Tethys' orbit today make explaining this satellite's geology challenging.
C1 [Matson, Dennis L.; Castillo-Rogez, Julie C.; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schubert, Gerald] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[McKinnon, William B.] Washington Univ, St Louis, MO 63139 USA.
RP Matson, DL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 178
TC 17
Z9 17
U1 2
U2 3
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 577
EP 612
DI 10.1007/978-1-4020-9217-6_18
D2 10.1007/978-1-4020-9217-6
PG 36
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000018
ER
PT B
AU Dones, L
Chapman, CR
McKinnon, WB
Melosh, HJ
Kirchoff, MR
Neukum, G
Zahnle, KJ
AF Dones, Luke
Chapman, Clark R.
McKinnon, William B.
Melosh, H. Jay
Kirchoff, Michelle R.
Neukum, Gerhard
Zahnle, Kevin J.
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Icy Satellites of Saturn: Impact Cratering and Age Determination
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID LATE HEAVY BOMBARDMENT; JUPITER-FAMILY COMETS; TERRESTRIAL PLANET
FORMATION; JOVIAN TROJAN ASTEROIDS; TRANS-NEPTUNIAN BODIES; KUIPER-BELT
OBJECTS; SHORT-PERIOD COMETS; OUTER SOLAR-SYSTEM; SHOEMAKER-LEVY 9;
IRREGULAR SATELLITES
AB Saturn is the first giant planet to be visited by an orbiting spacecraft that can transmit large amounts of data to Earth. Crater counts on satellites from Phoebe inward to the regular satellites and ring moons are providing unprecedented insights into the origin and time histories of the impacting populations. Many Voyager-era scientists concluded that the satellites had been struck by at least two populations of impactors. In this view, the Population I impactors, which were generally judged to be "comets" orbiting the Sun, formed most of the larger and older craters, while Population II impactors, interpreted as Saturn-orbiting ejecta from impacts on satellites, produced most of the smaller and younger craters. Voyager data also implied that all of the "ring moons;" and probably some of the mid-sized classical moons, had been catastrophically disrupted and reaccreted since they formed. We examine models of the primary impactor populations in the Saturn system. At the present time, "ecliptic comets," which likely originate in the Kuiper Belt/Scattered Disk, are predicted to dominate impacts on the regular satellites and ring moons, but the models require extrapolations in size (from the observed Kuiper Belt Objects to the much smaller bodies that produce the craters) or in distance (from the known active Jupiter family comets to 9.5 AU). Phoebe, Iapetus, and perhaps even moons closer to Saturn have been struck by irregular satellites as well. We describe the Nice model, which provides a plausible mechanism by which the entire Solar System might have experienced an era of heavy bombardment long after the planets formed. We then discuss the three cratering chronologies, including one based upon the Nice model, that have been used to infer surface ages from crater densities on the saturnian satellites. After reviewing scaling relations between the properties of impactors and the craters they produce, we provide model estimates of the present-day rate at which comets impact, and catastrophically disrupt, the saturnian moons. Finally, we present crater counts on the satellites from two different groups. Many of the heavily cratered terrains appear to be nearly saturated, so it is difficult to infer the provenance of the impactors from crater counts alone. More large craters have been found on Iapetus than on any other satellite. Enceladus displays an enormous range of surface ages, ranging from the old mid-latitude plains to the extremely young South Polar Terrain. Cassini images provide some evidence for the reality of "Population II". Most of the observed craters may have formed in one or more "cataclysms," but more work is needed to determine the roles of heliocentric and planetocentric bodies in creating the craters.
C1 [Dones, Luke; Chapman, Clark R.] SW Res Inst, Boulder, CO 80302 USA.
[McKinnon, William B.] Washington Univ, St Louis, MO 63130 USA.
[Melosh, H. Jay] Univ Arizona, Tucson, AZ 85721 USA.
[Kirchoff, Michelle R.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Neukum, Gerhard] Free Univ Berlin, D-12249 Berlin, Germany.
[Zahnle, Kevin J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Dones, L (reprint author), SW Res Inst, Boulder, CO 80302 USA.
NR 194
TC 30
Z9 30
U1 1
U2 2
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 613
EP 635
DI 10.1007/978-1-4020-9217-6_19
D2 10.1007/978-1-4020-9217-6
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000019
ER
PT B
AU Jaumann, R
Clark, RN
Nimmo, F
Hendrix, AR
Buratti, BJ
Denk, T
Moore, JM
Schenk, PM
Ostro, SJ
Srama, R
AF Jaumann, Ralf
Clark, Roger N.
Nimmo, Francis
Hendrix, Amanda R.
Buratti, Bonnie J.
Denk, Tilmann
Moore, Jeffrey M.
Schenk, Paul M.
Ostro, Steve J.
Srama, Ralf
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Icy Satellites: Geological Evolution and Surface Processes
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID INFRARED MAPPING SPECTROMETER; CASSINI IMAGING SCIENCE; BIDIRECTIONAL
REFLECTANCE SPECTROSCOPY; GALILEO ULTRAVIOLET SPECTROMETER; SATURNS
SMALL SATELLITES; TITAN RADAR MAPPER; E-RING; WATER VOLCANISM; DARK
MATERIAL; POLAR WANDER
AB The sizes of the Saturnian icy satellites range from similar to 1,500 km in diameter (Rhea) to similar to 20 km (Calypso), and even smaller 'rocks' of only a kilometer in diameter are common in the system. All these bodies exhibit remarkable, unique features and unexpected diversity. In this chapter, we will mostly focus on the 'medium-sized icy objects' Mimas, Tethys, Dione, Rhea, Iapetus, Phoebe and Hyperion, and consider small objects only where appropriate, whereas Titan and Enceladus will be described in separate chapters. Mimas and Tethys show impact craters caused by bodies that were almost large enough to break them apart. Iapetus is unique in the Saturnian system because of its extreme global brightness dichotomy. Tectonic activity varies widely - from inactive Mimas through extensional terrains on Rhea and Dione to the current cryovolcanic eruptions on Enceladus - and is not necessarily correlated with predicted tidal stresses. Likely sources of stress include impacts, despinning, reorientation and volume changes. Accretion of dark material originating from outside the Saturnian system may explain the surface contamination that prevails in the whole satellite system, while coating by Saturn's E-ring particles brightens the inner satellites.
So far, among the surprising Cassini discoveries are the volcanic activity on Enceladus, the sponge-like appearance of Hyperion and the equatorial ridge on Iapetus - unique features in the solar system. The bright-ray system on Rhea was caused by a relatively recent medium impact which formed a similar to 40 km crater at 12 degrees S latitude, 112 degrees W longitude, while the wispy streaks on Dione and Rhea are of tectonic origin. Compositional mapping shows that the dark material on Iapetus is composed of organics, CO2 mixed with H2O ice, and metallic iron, and also exhibits possible signatures of ammonia, bound water, H-2 or OH-bearing minerals, and a number of as-yet unidentified substances. The spatial pattern, Rayleigh scattering effect, and spectral properties argue that the dark material on Iapetus is only a thin coating on its surface. Radar data indicate that the thickness of the dark layers can be no more than a few decimeters; this is also consistent with the discovery of small bright-ray and bright-floor craters within the dark terrain. Moreover, several spectral features of the dark material match those seen on Phoebe, Iapetus, Hyperion, Dione and Epimetheus as well as in the F-ring and the Cassini Division, implying that throughout the Saturnian system. All dark material appears to have a high content of metallic iron and a small content of nano-phase hematite. However, the complete composition of the dark material is still unresolved, and additional laboratory work is required. As previously concluded for Phoebe, the dark material appears to have originated external to the Saturnian system.
The icy satellites of Saturn offer an unrivalled natural laboratory for understanding the geological diversity of different-sized icy satellites and their interactions within a complex planetary system.
C1 [Jaumann, Ralf] Inst Planetary Res, DLR, D-12489 Berlin, Germany.
[Jaumann, Ralf; Denk, Tilmann] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany.
[Clark, Roger N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA.
[Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Hendrix, Amanda R.; Buratti, Bonnie J.; Ostro, Steve J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Moore, Jeffrey M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schenk, Paul M.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Srama, Ralf] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
RP Jaumann, R (reprint author), Inst Planetary Res, DLR, Rutherfordstr 2, D-12489 Berlin, Germany.
NR 300
TC 28
Z9 28
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 637
EP 681
DI 10.1007/978-1-4020-9217-6_20
D2 10.1007/978-1-4020-9217-6
PG 45
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000020
ER
PT B
AU Spencer, JR
Barr, AC
Esposito, LW
Helfenstein, P
Ingersoll, AP
Jaumann, R
McKay, CP
Nimmo, F
Waite, JH
AF Spencer, John R.
Barr, Amy C.
Esposito, Larry W.
Helfenstein, Paul
Ingersoll, Andrew P.
Jaumann, Ralf
McKay, Christopher P.
Nimmo, Francis
Waite, J. Hunter
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI Enceladus: An Active Cryovolcanic Satellite
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID SATURNS E-RING; OUTER SOLAR-SYSTEM; NEAR-INFRARED SPECTRA; SOUTH-POLAR
FRACTURES; TIDAL DISSIPATION; ICY SATELLITES; HYDROTHERMAL SYSTEMS;
VISCOELASTIC MODELS; INTERNAL STRUCTURE; DUST MEASUREMENTS
AB Enceladus is one of the most remarkable satellites in the solar system, as revealed by Cassini's detection of active plumes erupting from warm fractures near its south pole. This discovery makes Enceladus the only icy satellite known to exhibit ongoing internally driven geological activity. The activity is presumably powered by tidal heating maintained by Enceladus' 2:1 mean-motion resonance with Dione, but many questions remain. For instance, it appears difficult or impossible to maintain the currently observed radiated power (probably at least 6 GW) in steady state. It is also not clear how Enceladus first entered its current self-maintaining warm and dissipative state-initial heating from non-tidal sources is probably required. There are also many unanswered questions about Enceladus' interior. The silicate fraction inferred from its density of 1.68 g cm(-2) is probably differentiated into a core, though we have not direct evidence for differentiation. Above the core there is probably a global or regional liquid water layer, inferred from several models of tidal heating, and an ice shell thick enough to support the similar to 1 km amplitude topography seen on Enceladus. It is possible that dissipation is largely localized beneath the south polar region. Enceladus' surface geology, ranging from moderately cratered terrain to the virtually crater-free active south polar region, is highly diverse, tectonically complex, and remarkably symmetrical about the rotation axis and the direction to Saturn. South polar activity is concentrated along the four "tiger stripe" fractures, which radiate heat at temperatures up to at least 167 K and are the source of multiple plumes ejecting similar to 200 kg s(-1) of H2O vapor along with significant N-2 (or C2H4), CO2, CH4, NH3, and higher-mass hydrocarbons. The escaping gas maintains Saturn's neutral gas torus, and the plumes also eject a large number of micron-sized H2O ice grains that populate Saturn's E-ring. The mechanism that powers the plumes is not well understood, and whether liquid water is involved is a subject of active debate. Enceladus provides perhaps the most promising potential habitat for life in the outer solar system, and the active plumes allow the unique opportunity for direct sampling of that zone. Enceladus is thus a prime target for Cassini's continued exploration of the Saturn system, and will be a tempting target for future missions.
C1 [Spencer, John R.; Barr, Amy C.] SW Res Inst, Boulder, CO USA.
[Waite, J. Hunter] SW Res Inst, San Antonio, TX USA.
[Esposito, Larry W.] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Helfenstein, Paul] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Ingersoll, Andrew P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Jaumann, Ralf] DLR, Inst Planetary Res, Berlin, Germany.
[McKay, Christopher P.] NASA, Ames Res Ctr, Mountain View, CA USA.
[Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
RP Spencer, JR (reprint author), SW Res Inst, Boulder, CO USA.
NR 170
TC 61
Z9 61
U1 2
U2 14
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 683
EP 724
DI 10.1007/978-1-4020-9217-6_21
D2 10.1007/978-1-4020-9217-6
PG 42
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000021
ER
PT B
AU Seal, DA
Buffington, BB
AF Seal, David A.
Buffington, Brent B.
BE Dougherty, MK
Esposito, LW
Krimigis, SM
TI The Cassini Extended Mission
SO SATURN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
AB Based on the overwhelming success of the Cassini/Huygens 4-year tour of Saturn from July 2004 to June 2008, NASA Headquarters approved at least two years of extended mission for continued study of the target-rich Saturnian system. After a rigorous phase of science objective definition and trajectory design and analysis, the Cassini project initiated an efficient, scientifically intense and operationally challenging mission phase, including 60 orbits around Saturn. 26 close Titan flybys, and 10 close icy satellite flybys - including seven more flybys of Enceladus. At the conclusion of the 2-year extended mission, substantial operating margins should be present with some fascinating options for further extensions.
C1 [Seal, David A.; Buffington, Brent B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Seal, DA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 20
TC 4
Z9 4
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9216-9
PY 2009
BP 725
EP 744
DI 10.1007/978-1-4020-9217-6_22
D2 10.1007/978-1-4020-9217-6
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMO21
UT WOS:000273026000022
ER
PT J
AU Kharuk, VI
Ranson, KJ
Im, ST
Dvinskaya, ML
AF Kharuk, Viacheslav I.
Ranson, Kenneth J.
Im, Sergey T.
Dvinskaya, Maria L.
TI Response of Pinus sibirica and Larix sibirica to climate change in
southern Siberian alpine forest-tundra ecotone
SO SCANDINAVIAN JOURNAL OF FOREST RESEARCH
LA English
DT Article
DE Climate change; forest-tundra ecotone; larch; Siberian pine; tree line
ID SWEDISH SCANDES; TREE-LINE; HEIGHT GROWTH; SYLVESTRIS; VEGETATION;
IMPACTS; 20TH-CENTURY; PERSPECTIVE; MOUNTAINS; RUSSIA
AB A warming climate provides competitive advantages to Siberian pine (Pinus sibirica Du Tour) in areas with sufficient precipitation. The warmer temperatures observed in central Siberia over the past three decades appear to have had a noticeable effect on growth of Siberian pine and larch (Larix sibirica Ledeb.) in the south Siberian Mountain forest-tundra ecotone. Larch is more tolerant of harsh climates and exhibits an arboreal growth form, whereas Siberian pine is in krummholz form. Larch also has an advantage at the upper tree limit and in areas with low precipitation. Since the mid-1980s there have been measurable increases in growth increments, stand densification, regeneration propagation into the alpine tundra and transformation of krummholz into arboreal forms. Warming winter temperatures have been sufficient for increased survival of regeneration. Regeneration responded to temperature increase of 1C by migration to areas 10-40 m higher in elevation. Regeneration has propagated into the alpine tundra at the rate of similar to 1.0-2.0 m year-1. Siberian pine and larch regeneration surpassed their upper historical limit by 10-80 m in elevation. While increased tree growth and migration into alpine tundra areas affect the regional carbon balance, it will also decrease albedo, which may increase warming at the regional level.
C1 [Kharuk, Viacheslav I.; Im, Sergey T.; Dvinskaya, Maria L.] VN Sukachev Inst Forest, Krasnoyarsk, Russia.
[Ranson, Kenneth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kharuk, VI (reprint author), VN Sukachev Inst Forest, Krasnoyarsk, Russia.
EM kharuk@ksc.krasn.ru
RI Ranson, Kenneth/G-2446-2012; Im, Sergei/J-2736-2016
OI Ranson, Kenneth/0000-0003-3806-7270; Im, Sergei/0000-0002-5794-7938
FU Terrestrial Ecology and Cryospheric Sciences Programs and Russian Fund
for Fundamental Investigations [06-05-64939]
FX This research was supported in part by the NASA Science Mission
Directorate, Terrestrial Ecology and Cryospheric Sciences Programs and
Russian Fund for Fundamental Investigations No. 06-05-64939. Special
thanks to Joanne Howl, DVM, for assisting with final preparation of the
manuscript.
NR 42
TC 27
Z9 27
U1 2
U2 11
PU TAYLOR & FRANCIS AS
PI OSLO
PA KARL JOHANS GATE 5, NO-0154 OSLO, NORWAY
SN 0282-7581
J9 SCAND J FOREST RES
JI Scand. J. Forest Res.
PY 2009
VL 24
IS 2
BP 130
EP 139
AR PII 911108538
DI 10.1080/02827580902845823
PG 10
WC Forestry
SC Forestry
GA 445ER
UT WOS:000266033100004
ER
PT J
AU Liu, Y
Chen, D
Kahn, RA
He, KB
AF Liu Yang
Chen Dan
Kahn, Ralph A.
He KeBin
TI Review of the applications of Multiangle Imaging SpectroRadiometer to
air quality research
SO SCIENCE IN CHINA SERIES D-EARTH SCIENCES
LA English
DT Article
DE aerosol remote sensing; MISR; multiangle imaging; aerosol optical
thickness; particulate matters; PM2.5; PM10; air pollution
ID AEROSOL OPTICAL DEPTH; MATTER COMPONENT CONCENTRATIONS; GROUND-LEVEL
PM2.5; DUST AEROSOLS; MISR; MODIS; DISTRIBUTIONS; RETRIEVAL; THICKNESS;
AERONET
AB The Multiangle Imaging SpectroRadiometer (MISR) launched by NASA in late 1999 has a unique multiangle design, which points nine cameras at fixed angles along the satellite flight track and collects reflected solar radiation simultaneously. This design allows the retrieval of a rich dataset of particle abundance, shape and composition over both land and ocean. Some of its capabilities have not been seen by any currently operating satellite aerosol sensors. Since MISR is sensitive to fine particles, it provides a new data source to study the spatial and temporal characteristics of air quality over large geographical regions. We first briefly introduce the MISR instrument, the retrieval and structure of MISR aerosol data, and then review the applications of MISR aerosol data in various aspects of air quality research since its launch. These include the spatial distributions of particle pollution events such as dust storms, wild fires, and urban pollution. Because of the high quality of MISR aerosol data, they can be used as quantitative indicators of particle pollution levels. We review the current modeling studies of surface level particle concentrations. Next, we introduce research results using MISR's advanced data such as the plume heights, and particle microphysical properties. In the discussion, we compare MISR research with current MODIS research to the best of our ability as MODIS data have been more extensively explored by the Chinese scientific community. Finally, we summarize the advantages and disadvantages of MISR data related to its applications to the air quality research. Given the highly quantitative measurements and comprehensive aerosol information MISR can provide, we believe that it will provide great values to advance our understanding of the particle air pollution in China.
C1 [Chen Dan; He KeBin] Tsinghua Univ, Dept Environm Engn & Sci, Beijing 100084, Peoples R China.
[Liu Yang] Harvard Univ, Sch Publ Hlth, Boston, MA 02215 USA.
[Kahn, Ralph A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP He, KB (reprint author), Tsinghua Univ, Dept Environm Engn & Sci, Beijing 100084, Peoples R China.
EM hekb@tsinghua.edu.cn
RI Kahn, Ralph/D-5371-2012; Chen, Dan/R-4486-2016
OI Kahn, Ralph/0000-0002-5234-6359;
FU Harvard-EPA Center on Particle Health Effects [R-827353, R-832416];
NASA's Climate and Radiation Research and Analysis Program; National
High Technology Research and Development Program of China [2006AA06A305]
FX Supported by Harvard-EPA Center on Particle Health Effects (Grant Nos.
R-827353 and R-832416), NASA's Climate and Radiation Research and
Analysis Program, the EOS-MISR Instrument Project and the National High
Technology Research and Development Program of China (Grant No.
2006AA06A305).
NR 61
TC 9
Z9 9
U1 2
U2 13
PU SCIENCE PRESS
PI BEIJING
PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA
SN 1006-9313
J9 SCI CHINA SER D
JI Sci. China Ser. D-Earth Sci.
PD JAN
PY 2009
VL 52
IS 1
BP 132
EP 144
DI 10.1007/s11430-008-0149-6
PG 13
WC Geosciences, Multidisciplinary
SC Geology
GA 429XI
UT WOS:000264953000013
ER
PT S
AU Normand, E
Grant, K
Ioup, E
Sample, J
AF Normand, Eric
Grant, Kevin
Ioup, Elias
Sample, John
BE Winslett, M
TI Improving Relation Extraction by Exploiting Properties of the Target
Relation
SO SCIENTIFIC AND STATISTICAL DATABASE MANAGEMENT, PROCEEDINGS
SE Lecture Notes in Computer Science
LA English
DT Proceedings Paper
CT 21st International Conference on Scientific and Statistical Database
Management
CY JUN 02-04, 2009
CL New Orleans, LA
SP LATG, Diamond Data Syst, Sun Microsyst, NOVACES, Univ New Orleans
AB In this paper we demonstrate and quantify the advantage gained by allowing relation extraction algorithms to make use of information about the cardinality of the target, relation. The two algorithms presented herein differ only in their assumption about the nature of the target relation (one-to-many or many-to-many). The algorithms are tested on the same relation to show the degree of advantage gained by their differing assumptions. Comparison of the performance of the two algorithms oil a one-to-many domain demonstrates the existence of several, previously undocumented behaviors which can he used to improve the performance of relation extraction algorithms. The first is a distinct, inverted u-shape in the initial portion of the recall Curve of the many-to-many algorithm. The second is that, as the number of seeds increases, the rate of improvement of the two algorithms descreases to approach the rate at which new information is added via the seeds.
C1 [Normand, Eric; Grant, Kevin; Ioup, Elias; Sample, John] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
RP Normand, E (reprint author), USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
EM enormand@nrlssc.navy.mil; kevin.grant.ctr@nrlssc.navy.mil;
eioup@nrlssc.navy.mil; john.sample@nrlssc.navy.mil
NR 14
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0302-9743
BN 978-3-642-02278-4
J9 LECT NOTES COMPUT SC
PY 2009
VL 5566
BP 553
EP 561
PG 9
WC Computer Science, Information Systems; Computer Science, Theory &
Methods
SC Computer Science
GA BKL72
UT WOS:000268444900037
ER
PT B
AU Wang, TJ
Ofman, L
Davila, JM
AF Wang, T. J.
Ofman, L.
Davila, J. M.
BE Lites, B
Cheung, M
Magara, T
Mariska, J
Reeves, K
TI Hinode/EIS Observations of Propagating Slow Magnetoacoustic Waves in a
Coronal Loop
SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 2nd Hinode Science Meeting
CY SEP 29-OCT 03, 2008
CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO
HO Natl Ctr Atmospher Res, Ctr Green Campus
ID OSCILLATIONS; TRACE
AB We present the first Hinode/EIS observations of 5 min quasi-periodic oscillations detected in the transition region and corona at the footpoint of a coronal loop. The oscillations are characterized by a series of wave packets with nearly constant period, typically persisting for 4-6 cycles. There is an in-phase relation between Doppler shift and intensity oscillations, indicating upwardly propagating slow magnetoacoustic waves in the loop. We find that the oscillations detected in the five coronal lines are highly correlated, and the amplitude decreases with increasing temperature. These oscillations may be caused by the leakage of the photospheric p-modes through the chromosphere and transition region into the corona, which has been suggested as the source for intensity oscillations previously observed by TRACE. The temperature dependence of the oscillation amplitudes can be explained by damping of the waves traveling along the loop with multithread structure near the footpoint.
C1 [Wang, T. J.; Ofman, L.] Catholic Univ Amer, Dept Phys, Code 671,Bldg 21-RM 177B, Greenbelt, MD 20770 USA.
[Wang, T. J.; Ofman, L.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Wang, TJ (reprint author), Catholic Univ Amer, Dept Phys, Code 671,Bldg 21-RM 177B, Greenbelt, MD 20770 USA.
EM wangtj@helio.gsfc.nasa.gov
FU NRL [NO0173-06-1-G033]
FX Hinode is a Japanese mission developed and launched by ISAS/JAXA in
partnership with NAOJ, NASA, and STFC (UK). The work of LO and TJW was
supported by NRL grant NO0173-06-1-G033.
NR 9
TC 1
Z9 1
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-710-0
J9 ASTR SOC P
PY 2009
VL 415
BP 28
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL19
UT WOS:000281239000005
ER
PT B
AU Kitiashvili, I
Jacoutot, L
Kosovichev, A
Wray, A
Mansour, N
AF Kitiashvili, Irina
Jacoutot, Laetitia
Kosovichev, Alexander
Wray, Alan
Mansour, Nagi
BE Lites, B
Cheung, M
Magara, T
Mariska, J
Reeves, K
TI Realistic Numerical Modeling of Solar Magnetoconvection and Oscillations
SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 2nd Hinode Science Meeting
CY SEP 29-OCT 03, 2008
CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO
HO Natl Ctr Atmospher Res, Ctr Green Campus
ID MAGNETIC-FIELDS; P-MODES; CONVECTION; EXCITATION; MISSION
AB We have developed 3D, compressible, non-linear radiative MHD simulations to study the influence of magnetic fields of various strengths and geometries on the turbulent convective cells and on the excitation mechanisms of the acoustic oscillations. The results reveal substantial changes of the granulation structure with increased magnetic field, and a frequency-dependent reduction in the oscillation power. These simulation results reproduce the enhanced high-frequency acoustic emission observed at the boundaries of active region ("acoustic halo" phenomenon). In the presence of inclined magnetic field the solar convection develops filamentary structure with flows concentrated along magnetic filaments, and also exhibits behavior of running magnetoconvective waves, resembling recent observations of the sunspot penumbra dynamics from Hinode/SOT.
C1 [Kitiashvili, Irina; Jacoutot, Laetitia] Stanford Univ, Ctr Turbulence Res, 488 Escandido Mall, Stanford, CA 94305 USA.
[Kosovichev, Alexander; Wray, Alan] Stanford Univ, HEPL, Stanford, CA 94305 USA.
[Mansour, Nagi] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kitiashvili, I (reprint author), Stanford Univ, Ctr Turbulence Res, 488 Escandido Mall, Stanford, CA 94305 USA.
EM irinasun@stanford.edu; sasha@sun.stanford.edu
NR 11
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-710-0
J9 ASTR SOC P
PY 2009
VL 415
BP 83
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL19
UT WOS:000281239000016
ER
PT B
AU Straus, T
Fleck, B
Jefferies, SM
McIntosh, SW
Severino, G
Steffen, M
Tarbell, TD
AF Straus, Thomas
Fleck, Bernhard
Jefferies, Stuart M.
McIntosh, Scott W.
Severino, Giuseppe
Steffen, Matthias
Tarbell, Theodore D.
BE Lites, B
Cheung, M
Magara, T
Mariska, J
Reeves, K
TI On the Role of Acoustic-Gravity Waves in the Energetics of the Solar
Atmosphere
SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 2nd Hinode Science Meeting
CY SEP 29-OCT 03, 2008
CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO
HO Natl Ctr Atmospher Res, Ctr Green Campus
ID CHROMOSPHERE; FLUX
AB In a recent paper (Straus et al. 2008) we determined the energy flux of internal gravity waves in the lower solar atmosphere using a combination of 3D numerical simulations and observations obtained with the IBIS instrument operated at the Dunn Solar Telescope and the Michelson Doppler Imager (MDI) on SOHO. In this paper we extend these studies using coordinated observations from SOT/NFI and SOT/SP on Hinode and MDI. The new measurements confirm that gravity waves are the dominant phenomenon in the quiet middle/upper photosphere and that they transport more mechanical energy than the high-frequency (> 5 mHz) acoustic waves, even though we find an acoustic flux 3-5 times larger than the upper limit estimate of Possum and Carlsson (2005). It therefore appears justified to reconsider the significance of (non-M)HD waves for the energy balance of the solar chromosphere.
C1 [Straus, Thomas; Severino, Giuseppe] Osserv Astron Capodimonte, INAF, Via Moiariello 16, I-80131 Naples, Italy.
[Fleck, Bernhard] NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA.
[Jefferies, Stuart M.] Univ Hawaii, Inst Astron, Pukalani, HI 96768 USA.
[McIntosh, Scott W.] High Altitude Observ, Boulder, CO 80307 USA.
[Steffen, Matthias] Astrophys Inst Potsdam, D-14482 Potsdam, Germany.
[Tarbell, Theodore D.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
RP Straus, T (reprint author), Osserv Astron Capodimonte, INAF, Via Moiariello 16, I-80131 Naples, Italy.
EM bfleck@esa.nascom.nasa.gov; mscott@ucar.edu; tarbell@lmsal.com
RI Fleck, Bernhard/C-9520-2012
NR 11
TC 9
Z9 9
U1 1
U2 1
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-710-0
J9 ASTR SOC P
PY 2009
VL 415
BP 95
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL19
UT WOS:000281239000019
ER
PT B
AU Panasenco, O
Velli, M
AF Panasenco, Olga
Velli, Marco
BE Lites, B
Cheung, M
Magara, T
Mariska, J
Reeves, K
TI Plasma Motions in Prominences Observed by Hinode/SOT
SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 2nd Hinode Science Meeting
CY SEP 29-OCT 03, 2008
CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO
HO Natl Ctr Atmospher Res, Ctr Green Campus
ID MAGNETIC-FIELD; INSTABILITY
AB We analyze the plasma motions inside prominences observed by Hinode/SOT during 2006-2007 with focus on the two spectacular examples from 25 April 2007 in H alpha line and 30 November 2006 in the CaH line. It is now well-known that most filaments (prominences on the limb) are composed of fine threads of similar dimensions. Recent observations of counter-streaming motions together with oscillations along the threads provide strong evidence that the threads are field aligned. To more correctly interpret the nature of observed downward flows of dense and cool plasma as well as the upward dark flows of less dense plasma, we take into account the geometry of the prominence structures and the viewing angle. Basic plasma physical considerations lead one to conclude that the magnetic field for the SOT observations considered above must be mainly orthogonal to the plane of the sky.
C1 [Panasenco, Olga] Helio Res, 5212 Maryland Ave, La Crescenta, CA 91214 USA.
[Velli, Marco] Jet Prop Lab, Pasadena, CA USA.
RP Panasenco, O (reprint author), Helio Res, 5212 Maryland Ave, La Crescenta, CA 91214 USA.
EM OlgaPanasenco@aol.com; velli@arcetri.astro.it
NR 10
TC 1
Z9 1
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-710-0
J9 ASTR SOC P
PY 2009
VL 415
BP 196
EP +
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL19
UT WOS:000281239000038
ER
PT B
AU Klimchuk, JA
AF Klimchuk, James A.
BE Lites, B
Cheung, M
Magara, T
Mariska, J
Reeves, K
TI Coronal Loop Models and Those Annoying Observations! (Keynote)
SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 2nd Hinode Science Meeting
CY SEP 29-OCT 03, 2008
CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO
HO Natl Ctr Atmospher Res, Ctr Green Campus
ID ACTIVE-REGION LOOPS; X-RAY; SPECTROSCOPIC OBSERVATIONS; IMAGING
SPECTROMETER; HOT PLASMA; HINODE; TELESCOPE; EXPLORER; MOTIONS; TRACE
AB It was once thought that all coronal loops are in static equilibrium, but observational and modeling developments over the past decade have shown that this is clearly not the case. It is now established that warm (similar to 1 MK) loops observed in the EUV are explainable as bundles of unresolved strands that are heated impulsively by storms of nanoflares. A raging debate concerning the multi-thermal versus isothermal nature of the loops can be reconciled in terms of the duration of the storm. We show that short and long storms produce narrow and broad thermal distributions, respectively. We also examine the possibility that warm loops can be explained with thermal nonequilibrium, a process by which steady heating produces dynamic behavior whenever the heating is highly concentrated near the loop footpoints. We conclude that this is not a viable explanation for monolithic loops under the conditions we have considered, but that it may have application to multi-stranded loops. Serious questions remain, however.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Klimchuk, JA (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
EM James.A.Klimchuk@nasa.gov
RI Klimchuk, James/D-1041-2012
OI Klimchuk, James/0000-0003-2255-0305
NR 36
TC 42
Z9 42
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-710-0
J9 ASTR SOC P
PY 2009
VL 415
BP 221
EP 233
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL19
UT WOS:000281239000043
ER
PT B
AU Reale, F
Klimchuk, JA
Parenti, S
Testa, P
AF Reale, Fabio
Klimchuk, James A.
Parenti, Susanna
Testa, Paola
BE Lites, B
Cheung, M
Magara, T
Mariska, J
Reeves, K
TI XRT Detection of Hot Plasma in Active Regions and Nanoflare Heating
SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 2nd Hinode Science Meeting
CY SEP 29-OCT 03, 2008
CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO
HO Natl Ctr Atmospher Res, Ctr Green Campus
ID CORONA; LOOPS
AB Nanoflares occurring in sub-resolution strands have been long invoked as strong candidates for the heating of active region (AR) coronal loops. However, the frequent occurrence of nanoflares requires the steady presence of flare-hot plasma in the active region, which has been difficult to detect so far. We report on the analysis of multi-filter Hinode/XRT observations of an active region, which may show the widespread presence of 10 MK plasma.
C1 [Reale, Fabio] Univ Palermo, Dipartimento Sci Fis & Astron, Sez Astron, Piazza Parlamento 1, I-90134 Palermo, Italy.
[Reale, Fabio] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy.
[Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Parenti, Susanna] Observ Royal Belgique, B-1180 Brussels, Belgium.
[Testa, Paola] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Reale, F (reprint author), Univ Palermo, Dipartimento Sci Fis & Astron, Sez Astron, Piazza Parlamento 1, I-90134 Palermo, Italy.
EM reale@astropa.unipa.it; James.A.Klimchuk@nasa.gov;
ptesta@cfa.harvard.edu
RI Klimchuk, James/D-1041-2012
OI Klimchuk, James/0000-0003-2255-0305
FU Italian Ministero dell'Universita e Ricerca and Agenzia Spaziale
Italiana (ASI) [I/015/07/0]; NASA [NNM07AA02C]; Belgian Federal Science
Policy Office; International Space Science Institute
FX 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). FR acknowledges support from Italian Ministero
dellUniversita e Ricerca and Agenzia Spaziale Italiana (ASI) contract
I/015/07/0. US members of the XRT team are supported by NASA contract
NNM07AA02C to SAO. SP acknowledge the support from the Belgian Federal
Science Policy Office through the ESA-PRODEX program. This work was
partially supported by the International Space Science Institute in the
framework of an international working team.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-710-0
J9 ASTR SOC P
PY 2009
VL 415
BP 256
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL19
UT WOS:000281239000048
ER
PT B
AU Del Zanna, G
Bradshaw, SJ
AF Del Zanna, G.
Bradshaw, S. J.
BE Lites, B
Cheung, M
Magara, T
Mariska, J
Reeves, K
TI Coronal Loops: New Insights from EIS Observations
SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 2nd Hinode Science Meeting
CY SEP 29-OCT 03, 2008
CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO
HO Natl Ctr Atmospher Res, Ctr Green Campus
ID HINODE EIS
AB Multi-instrument observations of coronal loops of different active regions have been studied. The general features discussed in Del Zanna (2003) and Del Zanna and Mason (2003) based on SOHO/CDS are confirmed. Hinnode/EIS high-cadence observations clearly show how dynamic loops are at all temperatures. This clearly reflects the fast changes in the photospheric magnetic fields measured by SOT over a minute timescale. Despite that, persistent patterns are present. In particular, the pattern of Doppler shifts and non-thermal widths, found for the first time in NOAA 10926 (cf. Del Zanna 2007, 2008), is actually a common feature in all active regions. It is likely that the majority of cool (0.5-1 MK) loops are observed during their radiatively cooling phase.
C1 [Del Zanna, G.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
[Del Zanna, G.] DAMPT, Ctr Math Sci, Cambridge CB3 0WA, England.
[Bradshaw, S. J.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Bradshaw, S. J.] George Mason Univ, Dept Comp & Data Sci, Fairfax, VA 22030 USA.
RP Del Zanna, G (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM gdz@mssl.ucl.ac.uk
NR 6
TC 2
Z9 2
U1 2
U2 2
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-710-0
J9 ASTR SOC P
PY 2009
VL 415
BP 264
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL19
UT WOS:000281239000050
ER
PT B
AU McIntosh, SW
Burkepile, J
Leamon, RJ
AF McIntosh, Scott W.
Burkepile, Joan
Leamon, Robert J.
BE Lites, B
Cheung, M
Magara, T
Mariska, J
Reeves, K
TI More of the Inconvenient Truth About Coronal Dimmings
SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 2nd Hinode Science Meeting
CY SEP 29-OCT 03, 2008
CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO
HO Natl Ctr Atmospher Res, Ctr Green Campus
ID MASS EJECTIONS; HINODE; MISSION
AB We continue the investigation of a CME-driven coronal dimming from December 14 2006 using unique high resolution imaging of the chromosphere and corona from the Hinode spacecraft. Over the course of the dimming event we observe the dynamic increase of non-thermal line broadening of multiple emission lines as the CME is released and the corona opens; reaching levels seen in coronal holes. As the corona begins to close, refill and brighten, we see a reduction of the non-thermal broadening towards the pre-eruption level. The dynamic evolution of non-thermal broadening is consistent with the expected change of Alfven wave amplitudes in the magnetically open rarefied dimming region, compared to the dense closed corona prior to the CME. The presented data reinforce the belief that coronal dimmings must be temporary sources of the fast solar wind. It is unclear if such a rapid transition in the thermodynamics of the corona to a solar wind state has an effect on the CME itself.
C1 [McIntosh, Scott W.; Burkepile, Joan] Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA.
[Leamon, Robert J.] Adnet Syst Inc, NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP McIntosh, SW (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA.
EM mscott@ucar.edu; iguana@ucar.edu
NR 12
TC 1
Z9 1
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-710-0
J9 ASTR SOC P
PY 2009
VL 415
BP 393
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL19
UT WOS:000281239000077
ER
PT B
AU Wang, TJ
Sui, L
Qiu, J
AF Wang, T. J.
Sui, L.
Qiu, J.
BE Lites, B
Cheung, M
Magara, T
Mariska, J
Reeves, K
TI Direct Observation of High-Speed Reconnection Outflows With SOHO/SUMER,
TRACE and RHESSI
SO SECOND HINODE SCIENCE MEETING: BEYOND DISCOVERY-TOWARD UNDERSTANDING
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 2nd Hinode Science Meeting
CY SEP 29-OCT 03, 2008
CL Natl Ctr Atmospher Res, Ctr Green Campus, Boulder, CO
HO Natl Ctr Atmospher Res, Ctr Green Campus
ID MAGNETIC RECONNECTION; SOLAR-FLARES
AB Spectroscopic observations of a solar limb flare recorded by SUMER on SOHO reveal, for the first time, hot fast magnetic reconnection outflows in the corona. The observations from TRACE and RHESSI allow us to determine the location of magnetic reconnection region. We find that as the reconnection site rises across the SUMER spectrometer slit, significant blue- and red-shift signatures are observed in the Fe XIX line, reflecting upflows and downflows of hot plasma jets, respectively. With the projection effect corrected, the measured outflow speed is between about 900-3500 km/s, consistent with theoretical predictions. This study provides an important guidance to the future observation with Hinode/EIS.
C1 [Wang, T. J.; Sui, L.] Catholic Univ Amer, Dept Phys, Code 671, Greenbelt, MD 20770 USA.
[Wang, T. J.; Sui, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Qiu, J.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
RP Wang, TJ (reprint author), Catholic Univ Amer, Dept Phys, Code 671, Greenbelt, MD 20770 USA.
EM wangtj@helio.gsfc.nasa.gov
NR 5
TC 1
Z9 1
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-710-0
J9 ASTR SOC P
PY 2009
VL 415
BP 447
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL19
UT WOS:000281239000087
ER
PT S
AU Eggert, J
Ryan, SJ
Ramesh, KT
Funk, D
Proud, W
AF Eggert, J.
Ryan, S. J.
Ramesh, K. T.
Funk, D.
Proud, W. G.
BE Elert, ML
Buttler, WT
Furnish, MD
Anderson, WW
Proud, WG
TI TOWN HALL MEETING - SCCM 2009
SO SHOCK COMPRESSION OF CONDENSED MATTER - 2009, PTS 1 AND 2
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 16th Conference of the American-Physical-Society-Topical-Group on Shock
Compression of Condensed Matter
CY JUN 28-JUL 03, 2009
CL Nashville, TN
SP Amer Phys Soc, Topical Grp
DE communication satellites; nanoscale materials and structures; metrology
AB The following article contains the summary of the discussion held at the Shock Compression of Condensed Matter Town Hall Meeting. This was held on Tuesday afternoon of the meeting and attracted 100+ attendees. This meeting, chaired by John Eggert, was planned to introduce challenges in selected topics relevant to shock wave science. The three subjects and speakers were: space research introduced by Shannon Ryan, nanotechnology presented by Kaliat T. Ramesh, and compression tools delivered by Dave Funk. After each presentation there were a number of questions.
C1 [Eggert, J.] Lawrence Livermore Natl Lab, POB 808, Livermore, CA 94551 USA.
[Ryan, S. J.] HITF, NASA Johnson Space Ctr, Houston, TX USA.
[Ramesh, K. T.] Johns Hopkins Univ, Dept Mech Engn, Baltimore, MD 21218 USA.
[Funk, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Proud, W. G.] Fracture & Shock Phys Grp, Cavendish Lab, Cambridge CB30HE, England.
RP Eggert, J (reprint author), Lawrence Livermore Natl Lab, POB 808, Livermore, CA 94551 USA.
NR 1
TC 0
Z9 0
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0732-9
J9 AIP CONF PROC
PY 2009
VL 1195
BP 26
EP +
PG 2
WC Physics, Condensed Matter
SC Physics
GA BOG48
UT WOS:000276574100004
ER
PT S
AU Ryan, SJ
Christiansen, EL
Lear, DM
AF Ryan, S. J.
Christiansen, E. L.
Lear, D. M.
BE Elert, ML
Buttler, WT
Furnish, MD
Anderson, WW
Proud, WG
TI DEVELOPMENT OF THE NEXT GENERATION OF METEOROID AND ORBITAL DEBRIS
SHIELDS
SO SHOCK COMPRESSION OF CONDENSED MATTER - 2009, PTS 1 AND 2
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 16th Conference of the American-Physical-Society-Topical-Group on Shock
Compression of Condensed Matter
CY JUN 28-JUL 03, 2009
CL Nashville, TN
SP Amer Phys Soc, Topical Grp
DE Hypervelocity impact; aluminum: foam; penetration
ID SPACECRAFT
AB The novel structure of metallic foams is of interest in the design of next-generation debris shields as it introduces physical mechanisms that are advantageous to hypervelocity impact shielding (e.g. increased fragmentation/melt/vaporization, energy dissipation, etc.). Preliminary investigations have shown improved shielding capability over traditional spacecraft primary structures. In this paper, the results of a current hypervelocity impact test program on metallic open-cell foam core sandwich panels are reported. A preliminary ballistic limit equation has been derived from the experimental results, and is presented in a form suitable for implementation in risk assessment software codes.
C1 [Ryan, S. J.] USRA Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
[Christiansen, E. L.; Lear, D. M.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
RP Ryan, SJ (reprint author), USRA Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
NR 10
TC 1
Z9 1
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0732-9
J9 AIP CONF PROC
PY 2009
VL 1195
BP 1417
EP +
PG 2
WC Physics, Condensed Matter
SC Physics
GA BOG48
UT WOS:000276574100334
ER
PT S
AU Sankrit, R
Williams, BJ
Borkowski, KJ
Raymond, JC
Gaetz, TJ
Blair, WP
Ghavamian, P
Long, KS
Reynolds, SP
AF Sankrit, Ravi
Williams, Brian J.
Borkowski, Kazimierz J.
Raymond, John C.
Gaetz, Terrance J.
Blair, William P.
Ghavamian, Parviz
Long, Knox S.
Reynolds, Stephen P.
BE Ao, X
Burrows, R
Zank, GP
TI Dust Destruction in a Nonradiative Shock in the Cygnus Loop Supernova
Remnant
SO SHOCK WAVES IN SPACE AND ASTROPHYSICAL ENVIRONMENTS
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 8th Annual International Astrophysics Conference
CY MAY 01-07, 2009
CL Kona, HI
SP Univ Alabama Huntsville, Ctr Space Plasma & Aeronom Res
DE Dust; Shocks; Supernova Remnants
ID LARGE-MAGELLANIC-CLOUD; SPECTRA
AB We present 24 mu m and 70 mu m images of a non-radiative shock in the Cygnus Loop supernova remnant, obtained with the Multiband Imaging Photometer on board the Spitzer Space Telescope. The observed emission is from dust grains heated in the post-shock region. The 70 mu m to 24 mu m flux ratio depends on the dust heating and the dust destruction rates, and thereby it is a sensitive tracer of the gas density and temperature in the shocked plasma. We model the dust emission and grain destruction in the post-shock flow, and find that the observed 70 mu m to 24 mu m flux ratios are produced for post-shock densities, n(H) similar to 2.0 cm(-3) and electron temperatures of about 0.20 keV. We find that about 35% of the dust has been destroyed in the shock, and that non-thermal sputtering (i.e. sputtering due to bulk motion of the grains relative to the gas) contributes significantly to the dust destruction.
C1 [Sankrit, Ravi] NASA, SOFIA, Ames Res Ctr, M-S 211-3, Moffett Field, CA 94041 USA.
[Williams, Brian J.; Borkowski, Kazimierz J.; Reynolds, Stephen P.] North Carolina State Univ, Raleigh, NC 27695 USA.
[Raymond, John C.; Gaetz, Terrance J.] Smithsonian Astrophys Observ, Cambridge, MA USA.
[Blair, William P.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Ghavamian, Parviz; Long, Knox S.] STScI, Baltimore, MD USA.
RP Sankrit, R (reprint author), NASA, SOFIA, Ames Res Ctr, M-S 211-3, Moffett Field, CA 94041 USA.
FU JPL [1278412]; SOFIA Science Center/USRA
FX This work was supported in part by JPL Award 1278412 to the University
of California, Berkeley and North Carolina State University. RS
acknowledges support from the SOFIA Science Center/USRA.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0724-4
J9 AIP CONF PROC
PY 2009
VL 1183
BP 95
EP +
PG 2
WC Astronomy & Astrophysics; Physics, Applied
SC Astronomy & Astrophysics; Physics
GA BPZ45
UT WOS:000280435400012
ER
PT B
AU Liou, MS
Chang, CH
Chen, H
Hu, JJ
AF Liou, M. -S.
Chang, C. -H.
Chen, H.
Hu, J. -J.
BE Hannemann, K
Seiler, F
TI Numerical study of shock-driven deformation of interfaces
SO SHOCK WAVES, VOL 2, PROCEEDINGS
LA English
DT Proceedings Paper
CT 26th International Symposium on Shock Waves
CY JUL 15-20, 2007
CL Gottingen, GERMANY
SP German Aerosp Ctr, French German Res Inst St Louis
ID 2-PHASE FLOW; WAVES
AB We employ AUSM(+)-up to obtain numerical results for studying the deformation of a droplet and an air bubble impacted initially by a passing shock wave, which triggers sequences of all enormously complicated flowfield. Multiplicate shock and rarefaction waves, and contact/slip surfaces have developed and interacted with each other, resulting in incredibly fine structures. Further analysis of the results yields useful insight into the behavior of interface dynamics, providing a new light oil the path to understanding of droplet breakup and jet formation.
C1 [Liou, M. -S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Chang, C. -H.] Univ Calif, Ctr Risk Stud & Safety, Goleta, CA 93117 USA.
[Chen, H.] Leader Univ, Tainan 70970, Taiwan.
[Hu, J. -J.] Shu Te Univ, Kaohsiung 82445, Taiwan.
RP Liou, MS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 16
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
BN 978-3-540-85180-6
PY 2009
BP 919
EP +
DI 10.1007/978-3-540-85181-3_20
PG 2
WC Engineering, Mechanical; Mechanics; Physics, Applied; Physics,
Multidisciplinary
SC Engineering; Mechanics; Physics
GA BKZ48
UT WOS:000269687500020
ER
PT S
AU Spry, DJ
Neudeck, PG
Chen, LY
Beheim, GM
Okojie, RS
Chang, CW
Meredith, RD
Ferrier, TL
Evans, LJ
AF Spry, David J.
Neudeck, Philip G.
Chen, Liang-Yu
Beheim, Glenn M.
Okojie, Robert S.
Chang, Carl W.
Meredith, Roger D.
Ferrier, Terry L.
Evans, Laura J.
BE Suzuki, A
Okumura, H
Kimoto, T
Fuyuki, T
Fukuda, K
Nishizawa, S
TI Fabrication and Testing of 6H-SiC JFETs for Prolonged 500 degrees C
Operation in Air Ambient
SO SILICON CARBIDE AND RELATED MATERIALS 2007, PTS 1 AND 2
SE Materials Science Forum
LA English
DT Proceedings Paper
CT 12th International Conference on Silicon Carbide and Related Materials
CY OCT 14-19, 2007
CL Otsu, JAPAN
SP Japan Soc Appl Phys, Assoc Promot Elect, Elect & Informat Engn, Ceram Soc Japan, IEEE EDS, Kansai Chapter, IEEJ, Inst Elect, Informat & Commun Engineers, Japanese Assoc Crystal Growth, Surface Sci Soc Japan, Vacuum Soc Japan
DE 6H-SiC; JFET; Junction Field Effect; Transistor; Durability;
Reliability; High Temperature; Amplifier; Differential Amplifier;
Packaging
AB This paper reports on the fabrication and testing of 6H-SiC junction field effect transistors (JFETs) and a simple differential amplifier integrated circuit that have demonstrated 2000 hours of electrical operation at 500 degrees C without degradation. The high-temperature ohmic contacts, dielectric passivation, and packaging technology that enabled such 500 degrees C durability are briefly described. Key JFET parameters of threshold voltage, on-state resistance, transconductance, and on-state current, as well as the gain of the differential amplifier integrated circuit, exhibited less than 7% change over the first 2000 hours of 500 degrees C operational testing.
C1 [Spry, David J.; Chen, Liang-Yu] NASA Glenn, OAI, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA.
[Neudeck, Philip G.; Beheim, Glenn M.; Okojie, Robert S.; Meredith, Roger D.; Ferrier, Terry L.; Evans, Laura J.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Chang, Carl W.] ASRC Aerosp Corp, Cleveland, OH 44135 USA.
RP Spry, DJ (reprint author), NASA Glenn, OAI, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA.
EM David.J.Spry@nasa.gov; Philip.G.Neudeck@nasa.gov;
Liangyu.Chen@grc.nasa.gov
FU NASA Aeronautics Research Mission Directorate; Fundamental Aeronautics
Programs under the Integrated Vehicle Health Management, Subsonic Fixed
Wing; Supersonics Projects; NASA
FX This work is presently funded by the NASA Aeronautics Research Mission
Directorate in both the Aviation Safety and Fundamental Aeronautics
Programs under the Integrated Vehicle Health Management, Subsonic Fixed
Wing, and Supersonics Projects. Prior-year NASA funding for this work
included the Glennan Microsystems Initiative, Ultra Efficient Engine
Technology, Propulsion 21, and NASA electronics Parts and Packaging
programs. Work was carried out by NASA Glenn Research Center with
assistance of D. Lukco, A. Trunek, D. Androjna, K. Laster, J. Gonzalez,
R. Lotenero, M. Mrdenovich, B. Osborn, G. Hunter, and L. Matus.
NR 6
TC 6
Z9 6
U1 0
U2 0
PU TRANS TECH PUBLICATIONS LTD
PI DURNTEN-ZURICH
PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND
SN 0255-5476
J9 MATER SCI FORUM
PY 2009
VL 600-603
BP 1079
EP +
PN 1-2
PG 2
WC Materials Science, Ceramics; Materials Science, Multidisciplinary
SC Materials Science
GA BIX26
UT WOS:000263555300258
ER
PT S
AU Patil, A
Fu, XA
Neudeck, P
Beheim, G
Mehregany, M
Garverick, S
AF Patil, Amita
Fu, Xiao-an
Neudeck, Philip
Beheim, Glenn
Mehregany, Mehran
Garverick, Steven
BE Suzuki, A
Okumura, H
Kimoto, T
Fuyuki, T
Fukuda, K
Nishizawa, S
TI Silicon Carbide Differential Amplifiers for High-Temperature Sensing
SO SILICON CARBIDE AND RELATED MATERIALS 2007, PTS 1 AND 2
SE Materials Science Forum
LA English
DT Proceedings Paper
CT 12th International Conference on Silicon Carbide and Related Materials
CY OCT 14-19, 2007
CL Otsu, JAPAN
SP Japan Soc Appl Phys, Assoc Promot Elect, Elect & Informat Engn, Ceram Soc Japan, IEEE EDS, Kansai Chapter, IEEJ, Inst Elect, Informat & Commun Engineers, Japanese Assoc Crystal Growth, Surface Sci Soc Japan, Vacuum Soc Japan
DE Junction field effect transistors; silicon carbide electronics;
high-temperature electronics; sensor interface circuits; differential
amplifiers
AB This paper presents silicon carbide sensor interface circuits and techniques for MEMS-based sensors operating in harsh environments. More specifically, differential amplifiers were constructed using integrated, depletion-mode, n-channel, 6H-SiC JFETs and off-chip passive components. A three-stage voltage amplifier has a differential voltage gain of similar to 50 dB and a gain-bandwidth of similar to 200 kHz at 450 degrees C, as limited by test parasitics. Such an amplifier could be used to amplify the signals produced by a piezoresistive Wheatstone bridge sensor, for example. Design considerations for 6H-SiC JFET transimpedance amplifiers appropriate for capacitance sensing and for frequency readout from a micromechanical resonator are also presented.
C1 [Patil, Amita; Fu, Xiao-an; Mehregany, Mehran; Garverick, Steven] Case Western Reserve Univ, Cleveland, OH 44106 USA.
[Neudeck, Philip; Beheim, Glenn] NASA Glenn Res Ctr, Cleveland, OH USA.
RP Patil, A (reprint author), Case Western Reserve Univ, Cleveland, OH 44106 USA.
EM amita.patil@case.edu; xiao-an.fu@case.edu; Philip.G.Neudeck@nasa.gov;
glenn.m.beheim@nasa.gov; mehran@case.edu; steven.garverick@case.edu
FU DARPA [NBCH1050002]; Glennan Microsystems Initiative and the Integrated
Vehicle Health Management Project under the Aviation Safety Program
FX This work was supported by DARPA under award #NBCH1050002. Work at NASA
Glenn Research Center was supported by the Glennan Microsystems
Initiative and the Integrated Vehicle Health Management Project under
the Aviation Safety Program.
NR 8
TC 5
Z9 5
U1 0
U2 0
PU TRANS TECH PUBLICATIONS LTD
PI DURNTEN-ZURICH
PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND
SN 0255-5476
J9 MATER SCI FORUM
PY 2009
VL 600-603
BP 1083
EP +
PN 1-2
PG 2
WC Materials Science, Ceramics; Materials Science, Multidisciplinary
SC Materials Science
GA BIX26
UT WOS:000263555300259
ER
PT S
AU Fu, XA
Patil, A
Neudeck, PG
Beheim, GM
Garverick, SL
Mehregany, M
AF Fu, Xiao-An
Patil, Amita
Neudeck, Philip G.
Beheim, Glenn M.
Garverick, Steven L.
Mehregany, Mehran
BE Suzuki, A
Okumura, H
Kimoto, T
Fuyuki, T
Fukuda, K
Nishizawa, S
TI 6H-SiC Lateral JFETs for Analog Integrated Circuits
SO SILICON CARBIDE AND RELATED MATERIALS 2007, PTS 1 AND 2
SE Materials Science Forum
LA English
DT Proceedings Paper
CT 12th International Conference on Silicon Carbide and Related Materials
CY OCT 14-19, 2007
CL Otsu, JAPAN
SP Japan Soc Appl Phys, Assoc Promot Elect, Elect & Informat Engn, Ceram Soc Japan, IEEE EDS, Kansai Chapter, IEEJ, Inst Elect, Informat & Commun Engineers, Japanese Assoc Crystal Growth, Surface Sci Soc Japan, Vacuum Soc Japan
DE JFET; high temperature electronics; 6H-SiC; device physics; device
fabrication
ID TEMPERATURE
AB This paper reports fabrication and electrical characterization of 6H-SiC n-channel, depletion-mode, junction-field-effect transistors (JFETs) for use in high-temperature analog integrated circuits for sensing and control in propulsion, power systems, and geothermal exploration. Electrical characteristics of the resulting MET devices have been measured across the wafer as a function of temperature, from room temperature to 450 degrees C. The results indicate that the JFETs are suitable for high-gain amplifiers in high-temperature sensor signal processing circuits.
C1 [Fu, Xiao-An; Patil, Amita; Garverick, Steven L.; Mehregany, Mehran] Case Western Reserve Univ, Dept Elect Engn & Comp Sci, Cleveland, OH 44106 USA.
[Neudeck, Philip G.; Beheim, Glenn M.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Fu, XA (reprint author), Case Western Reserve Univ, Dept Elect Engn & Comp Sci, Cleveland, OH 44106 USA.
EM xxf@case.edu; amita@case.edu; Philip.G.Neudeck@nasa.gov;
Glenn.M.Beheim@nasa.gov; steven.garverick@case.edu; mehran@case.edu
FU DARPA [NBCH1050002]; Glennan Microsystems Initiative; Integrated Vehicle
Health Management Project under the Aviation Safety Program
FX The authors would like to thank Mr. David Spry for technical
contributions to NASA Glenns SiC electronics research. This work was
supported by DARPA under award #NBCH1050002. Work at NASA Glenn Research
Center was supported by the Glennan Microsystems Initiative and the
Integrated Vehicle Health Management Project under the Aviation Safety
Program.
NR 7
TC 1
Z9 1
U1 0
U2 0
PU TRANS TECH PUBLICATIONS LTD
PI DURNTEN-ZURICH
PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND
SN 0255-5476
J9 MATER SCI FORUM
PY 2009
VL 600-603
BP 1099
EP +
PN 1-2
PG 2
WC Materials Science, Ceramics; Materials Science, Multidisciplinary
SC Materials Science
GA BIX26
UT WOS:000263555300263
ER
PT S
AU Neudeck, PG
Spry, DJ
Trunek, AJ
Evans, LJ
Chen, LY
Hunter, GW
Androjna, D
AF Neudeck, Philip G.
Spry, David J.
Trunek, Andrew J.
Evans, Laura J.
Chen, Liang-Yu
Hunter, Gary W.
Androjna, Drago
BE Suzuki, A
Okumura, H
Kimoto, T
Fuyuki, T
Fukuda, K
Nishizawa, S
TI Hydrogen Gas Sensors Fabricated on Atomically Flat 4H-SiC Webbed
Cantilevers
SO SILICON CARBIDE AND RELATED MATERIALS 2007, PTS 1 AND 2
SE Materials Science Forum
LA English
DT Proceedings Paper
CT 12th International Conference on Silicon Carbide and Related Materials
CY OCT 14-19, 2007
CL Otsu, JAPAN
SP Japan Soc Appl Phys, Assoc Promot Elect, Elect & Informat Engn, Ceram Soc Japan, IEEE EDS, Kansai Chapter, IEEJ, Inst Elect, Informat & Commun Engineers, Japanese Assoc Crystal Growth, Surface Sci Soc Japan, Vacuum Soc Japan
DE Gas Sensor; Hydrogen; Webbed Cantilevers; Hydrogen Sensor; Atomically
Flat; On-axis; Step-free Surface; Schottky Diode; Platinum
AB This paper reports on initial results from the first device tested of a "second generation" Pt-SiC Schottky diode hydrogen gas sensor that: 1) resides on the top of atomically flat 4H-SiC webbed cantilevers, 2) has integrated heater resistor, and 3) is bonded and packaged. With proper selection of heater resistor and sensor diode biases, rapid detection of H-2 down to concentrations of 20 ppm was achieved. A stable sensor current gain of 125 +/- 11 standard deviation was demonstrated during 250 hours of cyclic test exposures to 0.5% H-2 and N-2/air.
C1 [Neudeck, Philip G.; Evans, Laura J.; Hunter, Gary W.] NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA.
[Spry, David J.; Trunek, Andrew J.; Chen, Liang-Yu] NASA, OAI, Cleveland, OH 44135 USA.
[Androjna, Drago] Sierra Lobo Inc, NASA, Cleveland, OH 44135 USA.
RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA.
EM Neudeck@nasa.gov; David.J.Spry@nasa.gov; Gary.W.Hunter@nasa.gov
FU NASA Aeronautics Research Mission Directorate in the Fundamental
Aeronautics Program, Supersonics Project
FX The authors thank J. Xu, M. Artale, P. Lampard, B. Osborn, M.
Mrdenovich, G. Beheim, R. Okojie, J. A. Powell, and L. Matus at NASA
Glenn Research Center for their assistance. This work was funded by the
NASA Aeronautics Research Mission Directorate in the Fundamental
Aeronautics Program, Supersonics Project.
NR 6
TC 8
Z9 8
U1 0
U2 1
PU TRANS TECH PUBLICATIONS LTD
PI DURNTEN-ZURICH
PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND
SN 0255-5476
J9 MATER SCI FORUM
PY 2009
VL 600-603
BP 1199
EP +
PN 1-2
PG 2
WC Materials Science, Ceramics; Materials Science, Multidisciplinary
SC Materials Science
GA BIX26
UT WOS:000263555300288
ER
PT S
AU Trunek, AJ
Powell, JA
Neudeck, PG
Mrdenovich, M
AF Trunek, A. J.
Powell, J. A.
Neudeck, P. G.
Mrdenovich, M.
BE PerezTomas, A
Godignon, P
Vellvehi, M
Brosselard, P
TI HCl Etching Behavior on Low-Tilt-Angle and Step-Free 4H-SiC Surfaces
SO SILICON CARBIDE AND RELATED MATERIALS 2008
SE Materials Science Forum
LA English
DT Proceedings Paper
CT 7th European Conference on Silicon Carbide and Related Materials
CY SEP 07-11, 2008
CL Barcelona, SPAIN
SP Minist Educ & Cienc, ACCIO, Generalitat Catalunya, ACREO, Aixtron, Cree Inc, Dow Corning, D plus T Microelect, Ion Beam Serv, SiCED, SiCrystal AG
DE HCl etching; on-axis; mesa; cold wall
ID CONTROLLED GROWTH; EPITAXIAL-GROWTH; 6H-SIC(0001); HOMOEPITAXY; MESAS
AB We report on new observations made, when 4H-SiC, Si-face Substrate mesas, having either low tilt-angle (< 1 degrees) with steps or step-free top surfaces, were exposed to three separate HCl etching conditions for five minutes at temperatures of 1130 degrees C, 1240 degrees C and 1390 degrees C. We observed that HCl was ineffective at 1130 degrees C, as etching was incomplete with abundant surface contamination. At 1240 degrees C. screw dislocations were aggressively etched by HCl, while multiple shallow flat-bottomed etch pits were formed oil step-free mesa surfaces. At 1390 degrees C, step-flow etching dominated as large etch pits were formed at screw dislocations and previously step-free surfaces etched inward from mesa edges to form parallel rows of organized steps.
C1 [Trunek, A. J.] OAI, Cleveland, OH 44135 USA.
[Powell, J. A.] Est Inc, Cleveland, OH 44135 USA.
[Neudeck, P. G.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Mrdenovich, M.] Sierra Lobo, Cleveland, OH 44135 USA.
RP Trunek, AJ (reprint author), OAI, MS 77-1,21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM andrew.j.trunek@nasa.gov; j.a.powell@nasa.gov
NR 8
TC 2
Z9 2
U1 0
U2 0
PU TRANS TECH PUBLICATIONS LTD
PI STAFA-ZURICH
PA LAUBLSRUTISTR 24, CH-8717 STAFA-ZURICH, SWITZERLAND
SN 0255-5476
J9 MATER SCI FORUM
PY 2009
VL 615-617
BP 593
EP 596
PG 4
WC Engineering, Electrical & Electronic; Materials Science, Ceramics;
Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA BJH84
UT WOS:000265961100143
ER
PT S
AU Rowland, LB
Wyatt, JL
Fronheiser, JA
Vert, AV
Sandvik, PM
Borsa, T
Van Zeghbroeck, J
Van Zeghbroeck, B
Babu, S
AF Rowland, L. B.
Wyatt, J. L.
Fronheiser, J. A.
Vert, A. V.
Sandvik, P. M.
Borsa, T.
Van Zeghbroeck, J.
Van Zeghbroeck, B.
Babu, S.
BE PerezTomas, A
Godignon, P
Vellvehi, M
Brosselard, P
TI 6H and 4H-SiC Avalanche Photodiodes
SO SILICON CARBIDE AND RELATED MATERIALS 2008
SE Materials Science Forum
LA English
DT Proceedings Paper
CT 7th European Conference on Silicon Carbide and Related Materials
CY SEP 07-11, 2008
CL Barcelona, SPAIN
SP Minist Educ & Cienc, ACCIO, Generalitat Catalunya, ACREO, Aixtron, Cree Inc, Dow Corning, D plus T Microelect, Ion Beam Serv, SiCED, SiCrystal AG
DE avalanche photodiode; APD; a-plane; 11-20; photodiode; ultraviolet;
sensor
AB We report on the fabrication and testing of SiC p-i-n avalanche photodiodes. APDs of 0.25 mm(2) area on a-plane (11 (2) over bar0) 6H-SiC as well as off-axis Si face 6H and 4H-SiC were Successfully fabricated. A beveled mesa was used as edge termination. Recessed windows were formed using reactive ion etching to enhance low-wavelength UV performance. We performed current-voltage tests with and without UV illumination to determine dark current, photocurrent, and gain on selected devices. Dark Current was less than 1 pA at 0.5V(br) on multiple devices. Quantum efficiency of 40% or greater was observed for all orientations and polytypes.
C1 [Rowland, L. B.; Wyatt, J. L.] Aymont Technol Inc, Ballston Spa, NY 12020 USA.
[Fronheiser, J. A.; Vert, A. V.; Sandvik, P. M.] GE Global Res, Niskayuna, NY 12309 USA.
[Borsa, T.; Van Zeghbroeck, J.; Van Zeghbroeck, B.] Univ Colorado, Boulder, CO 80301 USA.
[Babu, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rowland, LB (reprint author), Aymont Technol Inc, 30 Saratoga Ave,Suite 6H, Ballston Spa, NY 12020 USA.
EM rowland@aymont.com
RI Rowland, Larry/C-4487-2008
NR 8
TC 2
Z9 2
U1 0
U2 2
PU TRANS TECH PUBLICATIONS LTD
PI STAFA-ZURICH
PA LAUBLSRUTISTR 24, CH-8717 STAFA-ZURICH, SWITZERLAND
SN 0255-5476
J9 MATER SCI FORUM
PY 2009
VL 615-617
BP 869
EP 872
PG 4
WC Engineering, Electrical & Electronic; Materials Science, Ceramics;
Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA BJH84
UT WOS:000265961100211
ER
PT S
AU Neudeck, PG
Spry, DJ
Chen, LY
Chang, CW
Beheim, GM
Okojie, RS
Evans, LJ
Meredith, RD
Ferrier, TL
Krasowski, MJ
Prokop, NF
AF Neudeck, Philip G.
Spry, David J.
Chen, Liang-Yu
Chang, Carl W.
Beheim, Glenn M.
Okojie, Robert S.
Evans, Laura J.
Meredith, Roger D.
Ferrier, Terry L.
Krasowski, Michael J.
Prokop, Norman F.
BE PerezTomas, A
Godignon, P
Vellvehi, M
Brosselard, P
TI Prolonged 500 degrees C Operation of 6H-SiC JFET Integrated Circuitry
SO SILICON CARBIDE AND RELATED MATERIALS 2008
SE Materials Science Forum
LA English
DT Proceedings Paper
CT 7th European Conference on Silicon Carbide and Related Materials
CY SEP 07-11, 2008
CL Barcelona, SPAIN
SP Minist Educ & Cienc, ACCIO, Generalitat Catalunya, ACREO, Aixtron, Cree Inc, Dow Corning, D plus T Microelect, Ion Beam Serv, SiCED, SiCrystal AG
DE 6H-SiC; JFET; high temperature; integrated circuit; amplifier; logic
gate
ID 500-DEGREES-C
AB This paper updates the long-term 500 degrees C electrical testing results from 6H-SiC junction field effect transistors (JFETs) and small integrated circuits that were introduced at ICSCRM-2007. Two packaged JFETs have now been operated in excess of 7000 hours at 500 degrees C with less than 10% degradation in linear I-V characteristics. Several simple digital and analog demonstration integrated circuits Successfully operated for 2000-6500 hours at 500 degrees C before failure.
C1 [Neudeck, Philip G.; Spry, David J.; Beheim, Glenn M.; Okojie, Robert S.; Evans, Laura J.; Meredith, Roger D.; Ferrier, Terry L.; Krasowski, Michael J.; Prokop, Norman F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Chen, Liang-Yu] NASA Glenn, OAI, Cleveland, OH 44135 USA.
[Chang, Carl W.] ASRC Aerosp Corp, Cleveland, OH 44135 USA.
RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA.
EM neudeck@nasa.gov; david.j.spry@nasa.gov; liangyu.chen-1@nasa.gov
RI Vellvehi, Miquel/J-8009-2014
OI Vellvehi, Miquel/0000-0002-0127-4690
NR 8
TC 12
Z9 12
U1 0
U2 0
PU TRANS TECH PUBLICATIONS LTD
PI STAFA-ZURICH
PA LAUBLSRUTISTR 24, CH-8717 STAFA-ZURICH, SWITZERLAND
SN 0255-5476
J9 MATER SCI FORUM
PY 2009
VL 615-617
BP 929
EP 932
PG 4
WC Engineering, Electrical & Electronic; Materials Science, Ceramics;
Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA BJH84
UT WOS:000265961100225
ER
PT S
AU Malaguti, G
Angelini, L
Raimondi, L
Moretti, A
Trifoglio, M
AF Malaguti, G.
Angelini, L.
Raimondi, L.
Moretti, A.
Trifoglio, M.
BE Ferrando, P
Rodriguez, J
TI Simbol-X Telescope Scientific Calibrations: Requirements and Plans
SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 2nd International Simbol-X Symposium
CY DEC 02-05, 2008
CL Paris, FRANCE
SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR
DE Simbol-X; calibrations; end-to-end test
AB The Simbol-X telescope characteristics and the mission scientific requirements impose a challenging calibration plan with a number of unprecedented issues. The 20 m focal length implies for the incoming X-ray beam a divergence comparable to the incidence angle of the mirror surface also for 100 m-long facilities. Moreover this is the first time that a direct focussing X-ray telescope will be calibrated on an energy band covering about three decades, and with a complex focal plane. These problems require a careful plan and organization of the measurements, together with an evaluation of the calibration needs in terms of both hardware and software.
C1 [Malaguti, G.; Raimondi, L.; Trifoglio, M.] INAF IASF, Bologna, Italy.
[Angelini, L.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Moretti, A.] INAF OABrera, Milan, Italy.
RP Malaguti, G (reprint author), INAF IASF, Bologna, Italy.
RI Trifoglio, Massimo/F-5302-2015
OI Malaguti, Giuseppe/0000-0001-9872-3378; moretti,
alberto/0000-0002-9770-0315; Trifoglio, Massimo/0000-0002-2505-3630
NR 3
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0662-9
J9 AIP CONF PROC
PY 2009
VL 1126
BP 85
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJM09
UT WOS:000266785900021
ER
PT S
AU Gehrels, N
Cannizzo, JK
AF Gehrels, Neil
Cannizzo, John K.
BE Ferrando, P
Rodriguez, J
TI The Hard X-ray Sky: Recent Observational Progress
SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 2nd International Simbol-X Symposium
CY DEC 02-05, 2008
CL Paris, FRANCE
SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR
DE X- and gamma-rays: telescopes and instrumentation, observations; Sky
surveys; X-ray binaries; The Galaxy: center; disk; Galaxies: AGN;
Seyfert
ID GALACTIC-CENTER; MILKY-WAY; CATALOG
AB The last fifty years have witnessed the birth, development, and maturation to full potential of hard X-ray astrophysics. The primary force driving the history of the field has been the development of space-based instrumentation optimized for getting the maximum science out of observations of high-energy photons from astrophysical sources. Hard X-ray telescopes are leading research in areas such as galactic diffuse emission, galactic transients, and active galactic nuclei.
C1 [Gehrels, Neil] NASA, GSFC, ASD, Code 661, Greenbelt, MD 20071 USA.
[Cannizzo, John K.] CRESST, UMBC, GSFC, ASD, Greenbelt, MD 20071 USA.
RP Gehrels, N (reprint author), NASA, GSFC, ASD, Code 661, Greenbelt, MD 20071 USA.
RI Gehrels, Neil/D-2971-2012
NR 10
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0662-9
J9 AIP CONF PROC
PY 2009
VL 1126
BP 99
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJM09
UT WOS:000266785900025
ER
PT S
AU Beckmann, V
Courvoisier, TJL
Gehrels, N
Lubinski, P
Malzac, J
Petrucci, PO
Shrader, CR
Soldi, S
AF Beckmann, V.
Courvoisier, T. J. -L.
Gehrels, N.
Lubinski, P.
Malzac, J.
Petrucci, P. O.
Shrader, C. R.
Soldi, S.
BE Ferrando, P
Rodriguez, J
TI Compton Reflection in AGN with Simbol-X
SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 2nd International Simbol-X Symposium
CY DEC 02-05, 2008
CL Paris, FRANCE
SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR
DE Galaxies: active; Galaxies: Seyfert; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; LUMINOSITY FUNCTION; SPECTRUM; GALAXIES; ORIGIN
AB AGN exhibit complex hard X-ray spectra. Our current understanding is that the emission is dominated by inverse Compton processes which take place in the corona above the accretion disk, and that absorption and reflection in a distant absorber play a major role. These processes can be directly observed through the shape of the continuum, the Compton reflection hump around 30 keV, and the iron fluorescence line at 6.4 keV. We demonstrate the capabilities of Simbol-X to constrain complex models for cases like MCG-05-23-016, NGC 4151, NGC 2110, and NGC 4051 in short (10 ksec) observations. We compare the simulations with recent observations on these sources by INTEGRAL, Swift and Suzaku. Constraining reflection models for AGN with Simbol-X will help us to get a clear view of the processes and geometry near to the central engine in AGN, and will give insight to which sources are responsible for the Cosmic X-ray background at energies > 20keV.
C1 [Beckmann, V.; Courvoisier, T. J. -L.; Soldi, S.] ISDC Data Ctr Astrophys, Ch Ecogia 16, CH-1290 Versoix, Switzerland.
[Gehrels, N.; Shrader, C. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lubinski, P.] Centrum Astronomiczne, PL-00716 Warsaw, Poland.
[Malzac, J.] CNRS, CESR, F-31028 Toulouse, France.
[Petrucci, P. O.] CNRS, Lab Astrophys Grenoble, F-38041 Grenoble, France.
RP Beckmann, V (reprint author), ISDC Data Ctr Astrophys, Ch Ecogia 16, CH-1290 Versoix, Switzerland.
RI Gehrels, Neil/D-2971-2012
NR 18
TC 1
Z9 1
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0662-9
J9 AIP CONF PROC
PY 2009
VL 1126
BP 141
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJM09
UT WOS:000266785900034
ER
PT S
AU Raimondi, L
Malaguti, G
Angelini, L
Cappi, M
Grandi, P
Palumbo, GGC
Puccetti, S
AF Raimondi, L.
Malaguti, G.
Angelini, L.
Cappi, M.
Grandi, P.
Palumbo, G. G. C.
Puccetti, S.
BE Ferrando, P
Rodriguez, J
TI The Galactic Center View with Simbol-X
SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 2nd International Simbol-X Symposium
CY DEC 02-05, 2008
CL Paris, FRANCE
SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR
DE Simbol-X; simulations; Galactic Centre; diffuse emission
AB The nature of the hard X-ray emission above 3 keV of the Galactic Centre (GC) is still source of controversy. Recent observations with Chandra are consistent with either a population of discrete sources or with a diffuse non thermal emission or, most likely, a combination of the two. The Simbol-X mission will be equipped with a grazing incident telescope imaging up to similar to 80 keV, providing an improvement of three orders of magnitude in sensitivity and angular resolution compared with the instruments that have operated so far above 10 keV. This capability will enable to directly disentangle between the discrete source versus the diffuse emission scenarios. This is demonstrated by the Simbol-X simulations of the GC shown here, where the input model includes a list of both diffuse and point sources (both resolved and unresolved) using the input spectrum observed with presently operating X-ray telescopes.
C1 [Raimondi, L.; Malaguti, G.; Cappi, M.; Grandi, P.] IASF Bologna, INAF, Bologna, Italy.
[Angelini, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Palumbo, G. G. C.] Univ Bologna, I-40126 Bologna, Italy.
[Puccetti, S.] ASI Sci Data Ctr, Rome, Italy.
RP Raimondi, L (reprint author), IASF Bologna, INAF, Bologna, Italy.
RI Cappi, Massimo/F-4813-2015;
OI Cappi, Massimo/0000-0001-6966-8920; Malaguti,
Giuseppe/0000-0001-9872-3378; Grandi, Paola/0000-0003-1848-6013;
Puccetti, Simonetta/0000-0002-2734-7835
FU Italian Space Agency; ASI INAF [ASI- 1/088/06/0]
FX We thank the Italian Space Agency for support under contract ASI INAF
ASI- 1/088/06/0.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0662-9
J9 AIP CONF PROC
PY 2009
VL 1126
BP 153
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJM09
UT WOS:000266785900037
ER
PT S
AU Migliori, G
Grandi, P
Angelini, L
Raimondi, L
Torresi, E
Palumbo, GGC
AF Migliori, G.
Grandi, P.
Angelini, L.
Raimondi, L.
Torresi, E.
Palumbo, G. G. C.
BE Ferrando, P
Rodriguez, J
TI Powerful Radio Galaxies with Simbol-X: Lobes and Hot Spots
SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 2nd International Simbol-X Symposium
CY DEC 02-05, 2008
CL Paris, FRANCE
SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR
DE galaxies: active; galaxies: individual (Pictor A); radiation mechanisms:
non thermal
ID RAY-EMISSION; PICTOR-A
AB We present here the first Simbol-X simulations of the extended components, lobes and hot spots, of the radio galaxies. We use the paradigmatic case of Pictor A to test the capabilities of Simbol-X in this field of studies. Simulations demonstrate that Simbol-X will be able not only to perform spatially resolved studies on the lobes of radio galaxies below 10 keV but also to observe, for the first time, hard X-ray emission from the hot spots. These extremely promising results show the considerable potentiality of Simbol-X in studying interaction phenomena between relativistic plasma and surrounding environment.
C1 [Migliori, G.] ISAS, SISSA, Via Beirut 2-4, I-34014 Trieste, Italy.
[Grandi, P.; Raimondi, L.; Torresi, E.] INAF, IASF Bologna, I-34014 Trieste, Italy.
[Angelini, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Palumbo, G. G. C.] Univ Bologna, Dipartimento Astronomia, I-40126 Bologna, Italy.
RP Migliori, G (reprint author), ISAS, SISSA, Via Beirut 2-4, I-34014 Trieste, Italy.
OI Grandi, Paola/0000-0003-1848-6013; TORRESI, ELEONORA/0000-0002-5201-010X
FU Asi Science Data Center
FX The authors thank S. Puccetti (Asi Science Data Center) for the support
provided in the simulations.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0662-9
J9 AIP CONF PROC
PY 2009
VL 1126
BP 156
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJM09
UT WOS:000266785900038
ER
PT S
AU de Martino, D
Anzolin, G
Bonnet-Bidaud, JM
Falanga, M
Matt, G
Mouchet, M
Mukai, K
Masetti, N
AF de Martino, D.
Anzolin, G.
Bonnet-Bidaud, J. -M.
Falanga, M.
Matt, G.
Mouchet, M.
Mukai, K.
Masetti, N.
BE Ferrando, P
Rodriguez, J
TI Exploring the Hard and Soft X-ray Emission of Magnetic Cataclysmic
Variables
SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 2nd International Simbol-X Symposium
CY DEC 02-05, 2008
CL Paris, FRANCE
SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR
DE X-rays; Accretion and Accretion Disks; Cataclysmic Binaries
ID INTERMEDIATE POLAR; WHITE-DWARF; IDENTIFICATION
AB A non-negligible fraction of galactic hard (>20keV) X-ray sources were identified as CVs of the magnetic Intermediate Polar type in INTEGRAL, SWIFT and RXTE surveys, that suggests a still hidden but potentially important population of faint hard X-ray sources. Simbol-X has the unique potential to simultaneously characterize their variable and complex soft and hard X-ray emission thus allowing to understand their putative role in galactic populations of X-ray sources.
C1 [de Martino, D.; Anzolin, G.] INAF Osservatorio Astron Capodimonte, Via Moiariello 16, I-80131 Naples, Italy.
[Bonnet-Bidaud, J. -M.; Falanga, M.] Saclay Gif Sur Yvette, Serv Astrophys, Gif Sur Yvette, France.
[Matt, G.] Univ Rome Tre, Dipartmento Fis, Rome, Italy.
[Mouchet, M.] Univ Paris 07, Lab APC, Paris, France.
[Mukai, K.] NASA, GSFC, CRESST & X Ray Astrophys Lab, Greenbelt, MD 20771 USA.
[Masetti, N.] INAF IASF Bologna, Bologna, Italy.
RP de Martino, D (reprint author), INAF Osservatorio Astron Capodimonte, Via Moiariello 16, I-80131 Naples, Italy.
OI de Martino, Domitilla/0000-0002-5069-4202
FU ASI [1/023/05/06, 1/088/06/0]; INAF [PRIN-INAF/2007/17]
FX We acknowledge financial support from ASI under contracts 1/023/05/06
and 1/088/06/0 and INAF under contract PRIN-INAF/2007/17.
NR 25
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0662-9
J9 AIP CONF PROC
PY 2009
VL 1126
BP 210
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJM09
UT WOS:000266785900052
ER
PT S
AU Paizis, A
Farinelli, R
Titarchuk, L
Frontera, F
Cocchi, M
Ferrigno, C
AF Paizis, A.
Farinelli, R.
Titarchuk, L.
Frontera, F.
Cocchi, M.
Ferrigno, C.
BE Ferrando, P
Rodriguez, J
TI A New Comptonization Model for Weakly Magnetized Accreting NS LMXBs
SO SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 2nd International Simbol-X Symposium
CY DEC 02-05, 2008
CL Paris, FRANCE
SP CNES, ASI, CEA, CNRS, Univ Paris, GDR-PCHE, IN2P3, CESR
DE X-ray binaries; Accretion and accretion disks; Neutron stars
ID X-RAY BINARIES; NEUTRON-STAR; FLOW
AB We have developed a new Comptonization model to propose, for the first time, a self consistent physical interpretation of the complex spectral evolution seen in NS LMXBs. The model and its application to LMXBs are presented and compared to the Simbol-X expected capabilities.
C1 [Paizis, A.] INAF IASF Milano, Milan, Italy.
[Farinelli, R.; Titarchuk, L.; Frontera, F.] Univ Ferrara, Dept Fis, I-44100 Ferrara, Italy.
[Titarchuk, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cocchi, M.] INAF IASF, Rome, Italy.
[Ferrigno, C.] INTEGRAL Sci Data Ctr, Geneva, Switzerland.
RP Paizis, A (reprint author), INAF IASF Milano, Milan, Italy.
OI Paizis, Adamantia/0000-0001-5067-0377
FU ASI [1/008/07/0]; "Bulk motion Comptonization models in XRBs: from
phenomenology to physics", Italian [PRIN-INAF]
FX AP acknowledges ASI financial and programmatic support
(contract1/008/07/0). This work has been partially supported by the
Italian PRIN-INAF 2007 grant, "Bulk motion Comptonization models in
XRBs: from phenomenology to physics", PI M. Cocchi.
NR 11
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0662-9
J9 AIP CONF PROC
PY 2009
VL 1126
BP 316
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJM09
UT WOS:000266785900076
ER
PT B
AU Clancey, WJ
AF Clancey, William J.
BA Turkle, S
BF Turkle, S
TI BECOMING A ROVER
SO SIMULATION AND ITS DISCONTENTS
SE Simplicity-Design Technology Business Life
LA English
DT Article; Book Chapter
C1 [Clancey, William J.] NASA, Ames Res Ctr, Washington, DC 20546 USA.
RP Clancey, WJ (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA.
NR 6
TC 2
Z9 2
U1 0
U2 0
PU M I T PRESS
PI CAMBRIDGE
PA FIVE CAMBRIDGE CENTER, CAMBRIDGE, MA 02142 USA
BN 978-0-262-01270-6
J9 SIMPLICITY-DES TECHN
PY 2009
BP 107
EP +
PG 25
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods; Operations Research & Management Science
SC Computer Science; Operations Research & Management Science
GA BOZ16
UT WOS:000278096100007
ER
PT B
AU Matsko, AB
Maleki, L
AF Matsko, Andrey B.
Maleki, Lute
BE Khurgin, JB
Tucker, RS
TI Resonator-Mediated Slow Light: Novel Structures, Applications and
Tradeoffs
SO SLOW LIGHT: SCIENCE AND APPLICATIONS
SE Optical Science and Engineering-CRC
LA English
DT Article; Book Chapter
ID OPTOELECTRONIC MICROWAVE-OSCILLATOR; ELECTROMAGNETICALLY INDUCED
TRANSPARENCY; OPTICAL WAVE-GUIDES; GROUP-VELOCITY; ATOMIC GAS; DELAY;
FILTERS; TRANSMISSION; PROPAGATION; SYSTEMS
C1 [Matsko, Andrey B.; Maleki, Lute] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Matsko, AB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 62
TC 0
Z9 0
U1 0
U2 1
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-1-4200-6151-2
J9 OPT SCI ENG-CRC
PY 2009
VL 140
BP 101
EP 117
PG 17
WC Engineering, Electrical & Electronic; Optics; Physics, Applied; Physics,
Particles & Fields
SC Engineering; Optics; Physics
GA BJU13
UT WOS:000267161300006
ER
PT B
AU Boroson, DM
Scozzafava, JJ
Murphy, DV
Robinson, BS
Shaw, H
AF Boroson, D. M.
Scozzafava, J. J.
Murphy, D. V.
Robinson, B. S.
Shaw, H.
GP IEEE COMPUTER SOC
TI The Lunar Laser Communications Demonstration (LLCD)
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
AB NASA is presently overseeing a project to create the world's first free-space laser communications system that can be operated over a range ten times larger than the near-earth ranges that have been demonstrated to date. To be flown on the Lunar Atmosphere and Dust Environment Explorer (LADEE), which is planned for launch by NASA in 2012, it will demonstrate high-rate laser communications from Lunar orbit to a transportable ground terminal on the Earth. To support up to 622 Mbps over the approximately 400 thousand kilometer link, the system will make use of a high peak-power doped-fiber transmitter, a hybrid pointing and tracking system, high efficiency modulation and coding techniques, superconducting photon-counting detectors, and a scalable optical collector architecture. It also will support up to 20 Mbps on the optical uplink, plus a highly accurate continuous two-way time-of-flight measurement capability with the potential to perform ranging with sub-centimeter accuracy to the moving spacecraft. The project is being undertaken by MIT Lincoln Laboratory (MIT/LL) and the NASA Goddard Space Flight Center (GSFC.)
C1 [Boroson, D. M.; Scozzafava, J. J.; Murphy, D. V.; Robinson, B. S.] MIT, Lincoln Lab, 244 Wood St, Lexington, MA 02173 USA.
[Shaw, H.] NASA, Goddard Space Flight cTR, Greenbelt, MD USA.
RP Boroson, DM (reprint author), MIT, Lincoln Lab, 244 Wood St, Lexington, MA 02173 USA.
EM boroson@ll.mit.edu
NR 10
TC 12
Z9 13
U1 2
U2 12
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 23
EP +
DI 10.1109/SMC-IT.2009.57
PG 3
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700003
ER
PT B
AU Wang, SY
Torgerson, JL
Schoolcraft, J
Brenman, Y
AF Wang, Shin-Ywan (Cindy)
Torgerson, J. Leigh
Schoolcraft, Joshua
Brenman, Yan
GP IEEE COMPUTER SOC
TI The Deep Impact Network Experiment Operations Center Monitor and Control
System
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE Deep Impack Network (DINET); Delay/Disruption Tolerant Network (DTN);
Interplanetary Overlay Network (ION); Bundle Protocol (BP); Experiment
Operations Center (EOC); Asynchronous Message System (AMS); Protocol
Technology Lab (PTL)
AB The Interplanetary Overlay Network (ION) software at JPL is an implementation of Delay/Disruption Tolerant Networking (DTN) which has been proposed as an interplanetary protocol to support space communication. The JPL Deep Impact Network (DINET) is a technology development experiment intended to increase the technical readiness of the JPL implemented ION suite. The DINET Experiment Operations Center (EOC) developed by JPL's Protocol Technology Lab (PTL) was critical in accomplishing the experiment. EOC, containing all end nodes of simulated spaces and one administrative node, exercised publish and subscribe functions for payload data among all end nodes to verify the effectiveness of data exchange over ION protocol stacks. A Monitor and Control System was created and installed on the administrative node as a multi-tiered internet-based Web application to support the Deep Impact Network Experiment by allowing monitoring and analysis of the data delivery and statistics from ION. This Monitor and Control System includes the capability of receiving protocol status messages, classifying and storing status messages into a database from the ION simulation network, and providing web interfaces for viewing the live results in addition to interactive database queries.
C1 [Wang, Shin-Ywan (Cindy); Torgerson, J. Leigh; Schoolcraft, Joshua; Brenman, Yan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wang, SY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Shin-Ywan.Wang@jpl.nasa.gov; Jordan.L.Torgerson@jpl.nasa.gov;
Joshua.Schoolcraft@jpl.nasa.gov; Bremann.Yan@jpl.nasa.gov
NR 5
TC 2
Z9 2
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 34
EP 40
DI 10.1109/SMC-IT.2009.13
PG 7
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700005
ER
PT B
AU Wang, YF
Schrock, M
Baldwin, J
Rangel, G
Borden, C
AF Wang, Yeou-Fang
Schrock, Mitchell
Baldwin, John
Rangel, Gabriel
Borden, Chester
GP IEEE COMPUTER SOC
TI Web 2.0 for Ground Resource Allocation
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE resource management; planning; Internet
AB A set of analysis tools has been created in a community-based team environment to support NASA ground resource allocation and planning. This new tool, called GRAPE (Ground Resource Allocation and Planning Environment), combines analysis, monitoring, and search capabilities into an existing community environment where wikis, blogs, document libraries, calendars, discussion forums, lists, progress management, and email repositories are available in a web site which assists users with their communication, operation, analysis, and collaboration needs.
C1 [Wang, Yeou-Fang; Schrock, Mitchell; Baldwin, John; Rangel, Gabriel; Borden, Chester] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Wang, YF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Yeou-Fang.Wang@jpl.nasa.gov
NR 1
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 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 51
EP 57
DI 10.1109/SMC-IT.2009.15
PG 7
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700007
ER
PT B
AU Policella, N
Oliveira, H
Siili, T
AF Policella, Nicola
Oliveira, Henrique
Siili, Tero
GP IEEE COMPUTER SOC
TI SKEYP: AI applied to SOHO Keyhole Operations
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
AB The Solar and Heliospheric Observatory's (SOHO) mission operations team has - due to a spacecraft malfunction - had to deal with the Keyhole Periods problem since 2003. This combinatorial problem arises from the conflict between limited telemetry downlink capabilities during keyhole periods and the need to maximize the return of science data while respecting other constraints, such as limited on-board storage capacity. Until recently, this problem has been addressed by manually generating data production and downlink plans. This work presents the SOHO Keyhole Planner (SKEYP), a software tool designed to improve on the manual workflow for plan generation by shortening the time needed and reduce significance of the learning curve associated with this process.
C1 [Policella, Nicola; Oliveira, Henrique] European Space Agcy, European Space Operat Ctr, Darmstadt, Germany.
[Siili, Tero] Goddard Space Flight Ctr, European Space Agcy, SOHO Team, Greenbelt, MD USA.
RP Policella, N (reprint author), European Space Agcy, European Space Operat Ctr, Darmstadt, Germany.
EM nicola.policella@esa.int; henrique.oliveira@esa.int; tero.siili@esa.int
NR 7
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 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 58
EP +
DI 10.1109/SMC-IT.2009.16
PG 2
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700008
ER
PT B
AU Morris, R
Dungan, J
Votava, P
AF Morris, Robert
Dungan, Jennifer
Votava, Petr
GP IEEE COMPUTER SOC
TI A Workflow Model for Earth Observation Sensor Webs
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE Sensor Webs; Workflow Management System
AB An Earth science sensor web consists of a distributed collection of sensors, Earth science models, human scientists and information technologists, and data archives. The scientific use of the sensor web consists broadly of seeking to improve the understanding of natural processes occurring on the Earth's surface or in the atmosphere. Sensor measurements serve to quantify aspects of these processes that allow Earth science models to make predictions of scientific and social value. The management problem for sensor webs considered here is the problem of reconfiguring the sensor web in order to answer new science questions. The notion of reconfiguration is used broadly here to describe a set of actions for retargeting sensors, querying databases for image data, or executing functions foe analyzing acquired data. This paper describes a workflow model and architecture for a workflow management system for reconfiguring sensor webs.
C1 [Morris, Robert; Dungan, Jennifer; Votava, Petr] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Morris, R (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM robert.a.morris@nasa.gov; jennifer.l.dungan@nasa.gov;
petr.votava@nasa.gov
OI /0000-0002-4863-1616
NR 8
TC 3
Z9 3
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 69
EP 76
DI 10.1109/SMC-IT.2009.60
PG 8
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700009
ER
PT B
AU Pasareanu, CS
Schumann, J
Mehlitz, P
Lowry, M
Karsai, G
Nine, H
Neema, S
AF Pasareanu, Corina S.
Schumann, Johann
Mehlitz, Peter
Lowry, Mike
Karsai, Gabor
Nine, Harmon
Neema, Sandeep
GP IEEE COMPUTER SOC
TI Model Based Analysis and Test Generation for Flight Software
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
ID SEMANTICS
AB We describe a framework for model-based analysis and test case generation in the context of a heterogeneous model-based development paradigm that uses and combines MathWorks and UML 2.0 models and the associated code generation tools. This paradigm poses novel challenges to analysis and test case generation that, to the best of our knowledge, have not been addressed before. The framework is based on a common intermediate representation for different modeling formalisms and leverages and extends model checking and symbolic execution tools for model analysis and test case generation, respectively. We discuss the application of our framework to software models for a NASA flight mission.
C1 [Pasareanu, Corina S.; Schumann, Johann; Mehlitz, Peter; Lowry, Mike] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Karsai, Gabor; Nine, Harmon; Neema, Sandeep] Vanderbilt Univ, ISIS, Nashville, TN 37235 USA.
RP Pasareanu, CS (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM CORINASPASAREANU@nasa.gov; JOHANNSCHUMANN@nasa.gov;
PETERMEHLITZ@nasa.gov; MIKELOWRY@nasa.gov; gabor@isis.vanderbilt.edu;
hnine@isis.vanderbilt.edu; sandeep@isis.vanderbilt.edu
NR 15
TC 5
Z9 5
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 83
EP +
DI 10.1109/SMC-IT.2009.18
PG 3
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700011
ER
PT B
AU Barry, M
Horvath, G
AF Barry, Matthew
Horvath, Gregory
GP IEEE COMPUTER SOC
TI Prototype Implementation of a Goal-Based Software Health Management
Service
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
AB The FAILSAFE project is developing concepts and prototype implementations for software health management in mission-critical real-time embedded systems. The project unites features of the industry standard ARINC 653 Avionics Application Software Standard Interface and JPL's Mission Data System (MDS) technology. The ARINC 653 standard establishes requirements for the services provided by partitioned real-time operating systems. The MDS technology provides a state analysis method, canonical architecture, and software framework that facilitates the design and implementation of software-intensive complex systems. We use the MDS technology to provide the health management function for an ARINC 653 application implementation. In particular, we focus on showing how this combination enables reasoning about and recovering from application software problems.
Our prototype application software mimics the Space Shuttle orbiter's abort control sequencer software task, which provides safety-related functions to manage vehicle performance during launch aborts. We turned this task into a goal-based function that, when working in concert with the software health manager, aims to work around software and hardware problems in order to maximize abort performance results. In order to make it a compelling demonstration for current aerospace initiatives, we additionally imposed on our prototype a number of requirements derived from NASA's Constellation Program. Lastly, the ARINC 653 standard imposes a number of requirements on the system integrator for developing the requisite error handier process. Under ARINC 653, the health monitoring (HM) service is invoked by an application calling the application error service or by the operating system or hardware detecting a fault. It is these HM and error process details that we implement with the MDS technology, showing how a state-analytic approach is appropriate for identifying fault determination details, and showing how the framework supports acting upon state estimation and control features in order to achieve safety-related goals.
We describe herein the requirements, design, and implementation of our software health manager and the software under control. We provide details of the analysis and design for the Phase II prototype, and describe future directions for the remainder of Phase II and the new topics we plan to address in Phase III.
C1 [Barry, Matthew] Kestrel Technol LLC, 4984 El Camino Real, Los Altos, CA 94022 USA.
[Horvath, Gregory] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Barry, M (reprint author), Kestrel Technol LLC, 4984 El Camino Real, Los Altos, CA 94022 USA.
EM mrbarry@kestreltechnology.com; gregory.a.horvath@jpl.nasa.gov
FU NASA Small Business Technology Transfer (STTR) [NNA07AA24C]
FX The Failsafe project is sponsored by a NASA Small Business Technology
Transfer (STTR) Phase II award under contract NNA07AA24C.
NR 5
TC 2
Z9 2
U1 0
U2 2
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 117
EP +
DI 10.1109/SMC-IT.2009.21
PG 2
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700015
ER
PT B
AU Granat, R
Wagstaff, KL
Bornstein, B
Tang, BY
Turmon, M
AF Granat, Robert
Wagstaff, Kiri L.
Bornstein, Benjamin
Tang, Benyang
Turmon, Michael
GP IEEE COMPUTER SOC
TI Simulating and Detecting Radiation-Induced Errors for Onboard Machine
Learning
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
ID ALGORITHMIC FAULT TOLERANCE; NETWORKS
AB Spacecraft processors and memory are subjected to high radiation doses and therefore employ radiation-hardened components. However, these components are orders of magnitude more expensive than typical desktop components, and they lag years behind in terms of speed and size. We have integrated algorithm-based fault tolerance (ABFT) methods into onboard data analysis algorithms to detect radiation-induced errors, which ultimately may permit the use of spacecraft memory that need not be fully hardened, reducing cost and increasing capability at the same time. We have also developed a lightweight software radiation simulator, BITFLIPS, that permits evaluation of error detection strategies in a controlled fashion, including the specification of the radiation rate and selective exposure of individual data structures. Using BITFLIPS, we evaluated our error detection methods when using a support vector machine to analyze data collected by the Mars Odyssey spacecraft. We observed good performance from both an existing ABFT method for matrix multiplication and a novel ABFT method for exponentiation. These techniques bring us a step closer to "rad-hard" machine learning algorithms.
C1 [Granat, Robert; Wagstaff, Kiri L.; Bornstein, Benjamin; Tang, Benyang; Turmon, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Granat, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.granat@jpl.nasa.gov; kiri.wagstaff@jpl.nasa.gov;
benjamin.bornstein@jpl.nasa.gov; benyang.tang@jpl.nasa.gov;
michael.turmon@jpl.nasa.gov
OI Wagstaff, Kiri/0000-0003-4401-5506
NR 24
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 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 125
EP 131
DI 10.1109/SMC-IT.2009.22
PG 7
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700016
ER
PT B
AU Zima, HP
James, ML
AF Zima, Hans P.
James, Mark L.
GP IEEE COMPUTER SOC
TI Introspection-Based Verification and Validation
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
AB Future missions of deep-space exploration will require an on-board computational capability that can support autonomy and enhanced science processing. The integration of emerging commodity multi-core technology into space-borne systems can provide the required performance; however, protecting such systems against faults has become a critical research issue. In this paper we present an approach to fault tolerance based On a newly developed introspection framework that supports runtime monitoring of program execution and feedback-oriented recovery. We discuss the relationship of this approach to traditional Verification. and Validation (V&V) and propose methods for the automatic generation of assertions front static and dynamic analysis.
C1 [Zima, Hans P.; James, Mark L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zima, HP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM zima@jpl.nasa.gov; mjames@jpl.nasa.gov
NR 23
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 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 132
EP 139
DI 10.1109/SMC-IT.2009.23
PG 8
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700017
ER
PT B
AU Smith, TB
Chavez-Clemente, D
AF Smith, Tristan B.
Chavez-Clemente, Daniel
GP IEEE COMPUTER SOC
TI A Practical Comparison of Motion Planning Techniques for Robotic Legs in
Environments with Obstacles
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
AB ATHLETE is a large six-legged tele-operated robot. Each foot is a wheel; travel can be achieved by walking, rolling, or some combination of the two. Operators control ATHLETE by selecting parameterized commands front a command dictionary. While rolling can be done efficiently, any motion involving steps is cumbersome - each step can require multiple commands and take many minutes to complete. In this paper we consider four different algorithms that generate a sequence of commands to take a step. We consider a baseline heuristic, a randomized motion planning algorithm, and two variants of A* search. Results for a variety of terrains are presented, and we discuss the quantitative and qualitative tradeoffs between the approaches.
C1 [Smith, Tristan B.] NASA, Ames Res Ctr, Mission Crit Technol Inc, Moffett Field, CA 94035 USA.
[Chavez-Clemente, Daniel] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
RP Smith, TB (reprint author), NASA, Ames Res Ctr, Mission Crit Technol Inc, Moffett Field, CA 94035 USA.
EM tristan.b.smith@nasa.gov; dchavez@stanford.edu
NR 11
TC 0
Z9 1
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 155
EP +
DI 10.1109/SMC-IT.2009.26
PG 2
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700020
ER
PT B
AU Mattmann, CA
Freeborn, D
Crichton, D
Foster, B
Hart, A
Woollard, D
Hardman, S
Ramirez, P
Kelly, S
Chang, AY
Miller, CE
AF Mattmann, Chris A.
Freeborn, Dana
Crichton, Dan
Foster, Brian
Hart, Andrew
Woollard, David
Hardman, Sean
Ramirez, Paul
Kelly, Sean
Chang, Albert Y.
Miller, Charles E.
GP IEEE COMPUTER SOC
TI A Reusable Process Control System Framework for the Orbiting Carbon
Observatory and NPP Sounder PEATE missions
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
AB We describe a reusable architecture and implementation framework for managing science processing pipelines for mission ground data systems. Our system, dubbed "PCS", for Process Control System, improves upon an existing software component, the OODT Catalog and Archive (CAS), which has already supported the QuikSCAT SeaWinds and AMT earth. science missions. This paper focuses on PCS within the context of two current earth science missions: the Orbiting Carbon Observatory (OCO), and NPP Sounder PEATE projects.
C1 [Mattmann, Chris A.; Freeborn, Dana; Crichton, Dan; Foster, Brian; Hart, Andrew; Woollard, David; Hardman, Sean; Ramirez, Paul; Kelly, Sean; Chang, Albert Y.; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mattmann, CA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mattmann@jpl.nasa.gov
NR 12
TC 8
Z9 8
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 165
EP 172
DI 10.1109/SMC-IT.2009.27
PG 8
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700021
ER
PT B
AU Topousis, DE
Means, EK
Murphy, KS
Yew, M
AF Topousis, Daria E.
Means, Erin K.
Murphy, Keri S.
Yew, Manson
GP IEEE COMPUTER SOC
TI Enhancing Collaboration Among NASA Engineers through a Knowledge Sharing
System
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE Communities of practice; information retrieval; knowledge based systems
AB Because solar system exploration often involves highly complex missions, a strong infrastructure to support knowledge sharing among engineers is critical to facilitate problem solving and preserve solutions for future work. Any system developed to meet these needs must include the ability to rapidly disseminate content, connect users to the right information regardless of where it is stored, and connect people with the experts and they need. This paper describes the knowledge sharing solution called the NASA Engineering Network, which includes a faceted search, communities of practice, an expertise locator, and a centralized engineering portal. The paper includes details on how the components were developed and provides best practices that other aerospace organizations might use when implementing similar systems.
C1 [Topousis, Daria E.; Means, Erin K.; Murphy, Keri S.; Yew, Manson] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Topousis, DE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM daria.e.topousis@jpl.nasa.gov; erin.means@jpl.nasa.gov;
keri.s.murphy@jpl.nasa.gov; manson.yew@jpl.nasa.gov
NR 13
TC 0
Z9 0
U1 0
U2 6
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 187
EP 192
DI 10.1109/SMC-IT.2009.29
PG 6
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700024
ER
PT B
AU Troglio, G
Benediktsson, JA
Troglio, G
Moser, G
Serpico, SB
Le Moigne, J
AF Troglio, G.
Benediktsson, J. A.
Troglio, G.
Moser, G.
Serpico, S. B.
Le Moigne, J.
GP IEEE COMPUTER SOC
TI Automatic Extraction of Planetary Image Features
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE Crater detection; feature extraction; image segmentation; image
registration
ID CLASSIFICATION
AB With the launch of several Lunar missions such as the Lunar Reconnaissance Orbiter (LRO) and Chandrayaan-1, a large amount of Lunar images will be acquired and will need to be analyzed. Although many automatic feature extraction methods have been proposed and utilized for Earth remote sensing images, these methods are not always applicable to Lunar data that often present low contrast and uneven illumination characteristics. In this paper, we propose a new method for the extraction of features from the Lunar surface, based on the combination of several image processing techniques, including a watershed segmentation and the generalized Hough Transform. The method has many applications, among which image registration, and can be generalized to other planetary images as well.
C1 [Troglio, G.; Benediktsson, J. A.] Univ Iceland, Dept Elect & Comp Engn, Reykjavik, Iceland.
[Troglio, G.; Moser, G.; Serpico, S. B.] Univ Genoa, Dept Biophys & Elect Engn, Genoa, Italy.
[Le Moigne, J.] NASA, Goddard Space Flight Ctr, Software Engn Div, GSFC Code 580, Greenbelt, MD USA.
RP Troglio, G (reprint author), Univ Iceland, Dept Elect & Comp Engn, Reykjavik, Iceland.
EM benedikt@hi.is; sebastiano.serpico@unige.it;
Jacqueline.LeMoigne@nasa.gov
RI Benediktsson, Jon/F-2861-2010
OI Benediktsson, Jon/0000-0003-0621-9647
FU University of Iceland; NASA Goddard Space Flight Center
FX This work was supported by the Research of Fund of the University of
Iceland and was performed at NASA Goddard Space Flight Center.
NR 13
TC 1
Z9 1
U1 0
U2 2
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 211
EP +
DI 10.1109/SMC-IT.2009.32
PG 3
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700027
ER
PT B
AU Lim, CS
Jain, A
AF Lim, Christopher S.
Jain, Abhinandan
GP IEEE COMPUTER SOC
TI Dshell plus plus : A Component Based, Reusable Space System Simulation
Framework
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE Aerospace simulation software
AB This paper describes the multi-mission Dshell++ simulation framework for high fidelity, physics-based simulation of spacecraft, robotic manipulation and mobility systems. Dshell++ is a C++/Python library which uses modern script-driven object-oriented techniques to allow component reuse and a dynamic run-time interface for complex, high-fidelity simulation of spacecraft and robotic systems. The goal of the Dshell++ architecture is to manage the inherent complexity of physics-based simulations while supporting component model reuse across missions. The framework provides several features that support a large degree of simulation configurability and usability.
C1 [Lim, Christopher S.; Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA.
RP Lim, CS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91009 USA.
EM Christopher.S.Lim@jpl.nasa.gov
NR 19
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 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 229
EP 236
DI 10.1109/SMC-IT.2009.35
PG 8
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700030
ER
PT B
AU Pomerantz, MI
Jain, A
Myint, S
AF Pomerantz, Marc I.
Jain, Abhinandan
Myint, Steven
GP IEEE COMPUTER SOC
TI Dspace: Real-time 3D Visualization System for Spacecraft Dynamics
Simulation
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
AB The multi-mission Dshell++ simulation framework has formed the basis for high-performance, physics-based simulations for a large variety of space mission simulations including cruise and orbiter spacecraft, Entry, Descent, Landing (EDL) missions as well as for planetary surface rovers. The Dspace interactive, reusable 3D visualization system has been developed to support the diverse visualization needs of such complex real-time simulations
C1 [Pomerantz, Marc I.; Jain, Abhinandan; Myint, Steven] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pomerantz, MI (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Marc.I.Pomerantz@jpl.nasa.gov
NR 16
TC 1
Z9 1
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 237
EP 245
DI 10.1109/SMC-IT.2009.36
PG 9
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700031
ER
PT B
AU Estlin, T
Castano, R
Bornstein, B
Gaines, D
Anderson, RC
de Granville, C
Thompson, D
Burl, M
Judd, M
Chien, S
AF Estlin, Tara
Castano, Rebecca
Bornstein, Benjamin
Gaines, Daniel
Anderson, Robert C.
de Granville, Charles
Thompson, David
Burl, Michael
Judd, Michele
Chien, Steve
GP IEEE COMPUTER SOC
TI Automated Targeting for the MER Rovers
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
AB The Autonomous Exploration for Gathering Increased Science System (AEGIS) will soon provide automated targeting for remote sensing instruments on the Mars Exploration Rover (MER) mission, which currently has two rovers exploring the surface of Mars. Targets for rover remote-sensing instruments, especially narrow field-of-view instruments (such as the MER Mini-TES spectrometer or the 2011 Mars Science Laboratory (MSL) Mission ChemCam Spectrometer), are typically selected manually based on imagery already on the ground with the operations team. AEGIS enables the rover flight software to analyze imagery onboard in order to autonomously select and sequence targeted remote-sensing observations in an opportunistic fashion
In this paper, we first provide background information on the larger autonomous science framework in which AEGIS was developed. We then describe how AEGIS was specifically developed and tested on the JPL FIDO rover. Finally we discuss how AEGIS will be uploaded and used on the Mars Exploration Rover (MER) mission in mid 2009.
C1 [Estlin, Tara; Castano, Rebecca; Bornstein, Benjamin; Gaines, Daniel; Anderson, Robert C.; de Granville, Charles; Thompson, David; Burl, Michael; Judd, Michele; Chien, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Estlin, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM tara.estlin@jpl.nasa.gov; rebecca.castano@jpl.nasa.gov;
benjamin.bornstein@jpl.nasa.gov; daniel.gaines@jpl.nasa.gov;
robert.anderson@jpl.nasa.gov; charles.degranville@jpl.nasa.gov;
david.thompson@jpl.nasa.gov; michael.burl@jpl.nasa.gov;
michele.judd@jpl.nasa.gov; steve.chien@jpl.nasa.gov
NR 9
TC 0
Z9 0
U1 0
U2 2
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 257
EP 263
DI 10.1109/SMC-IT.2009.38
PG 7
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700033
ER
PT B
AU Gaines, D
Estlin, T
Schaffer, S
Chouinard, C
Elfes, A
AF Gaines, Daniel
Estlin, Tara
Schaffer, Steve
Chouinard, Caroline
Elfes, Alberto
GP IEEE COMPUTER SOC
TI Autonomous Planning and Execution for a Future Titan Aerobot
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
AB We are developing onboard planning and execution technologies to provide robust and opportunistic mission operations for a future Titan aerobot. Aerobot have the potential for collecting a vast amount of high priority science data. However, to be effective, an aerobot must address several challenges including communication constraints, extended periods without contact with Earth, uncertain and changing environmental conditions, maneuvarability constraints and potentially short-lived science opportunities. We are developing the AerOASIS system to develop and test technology to support autonomous science operations for a future Titan Aerobot. The planning and execution component of AerOASIS is able to generate mission operations plans that achieve science and engineering objectives while respecting mission and resource constraints as well as adapt the plan to respond to new science opportunities. Our technology leverages prior work on the OASIS system for autonomous rover exploration. In this paper we describe how the OASIS planning component was adapted to address the unique challenges of a Titan Aerobot and we describe a field demonstration of the system with the JPL prototype aerobot.
C1 [Gaines, Daniel; Estlin, Tara; Schaffer, Steve; Chouinard, Caroline; Elfes, Alberto] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gaines, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM daniel.gaines@jpl.nasa.gov; tara.estlin@jpl.nasa.gov;
steve.schaffer@jpl.nasa.gov; caroline.chouinard@jpl.nasa.gov;
alberto.elfes@jpl.nasa.gov
RI Elfes, Alberto/E-2463-2011
OI Elfes, Alberto/0000-0003-2433-995X
NR 8
TC 0
Z9 0
U1 0
U2 1
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 264
EP 269
DI 10.1109/SMC-IT.2009.39
PG 6
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700034
ER
PT B
AU Hanna, RA
AF Hanna, Robert A.
GP IEEE COMPUTER SOC
TI Earned Value Management Software Projects
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE Cost; Schedule; Software; Management
AB JPL has been attempting to apply EVM techniques for the last 15 years with mixed success, especially when applied to software tasks. One of the main causes is that software presents particular challenges that were not considered during the genesis of EVM. A small number of tasks have been able to use EVM effectively and derive great benefits. This paper discusses challenges specific to software management and how they can be successfully addressed. Specifically, it details lessons learned from the $28 million dollar Next Generation Navigation Software Project that replaced NASA's deep space navigation software for operations. The project was able to successfully use EVM techniques during a four year period, producing 12 releases on their promised delivery dates and projects actual costs that were within 0.3% of the planned budget (under), in contrast to performance before the techniques were put into practice.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Hanna, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Robert.A.Hanna@jpl.nasa.gov
NR 6
TC 2
Z9 2
U1 2
U2 3
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 297
EP 304
DI 10.1109/SMC-IT.2009.42
PG 8
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700038
ER
PT B
AU Fijany, A
Barrett, A
Vatan, F
AF Fijany, Amir
Barrett, Anthony
Vatan, Farrokh
GP IEEE COMPUTER SOC
TI A Novel Efficient Method for Conflicts Set Generation for Model-Based
Diagnosis
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE model-based diagnosis; fault detection; conflict; analytical redundancy
relation; hitting set problem
ID ANALYTICAL REDUNDANCY RELATIONS
AB In this paper we present a new efficient algorithmic method for generating the conflicts set for model-based diagnosis. Our new method combines the strength of the two different approaches proposed in the literature, that is, the Fault Detection and Isolation (FDI), which is based on automatic control theory and statistical decision theory, and the other one, known as DX, which is based on artificial intelligence techniques. The first building block in our method is a new efficient algorithm for generation of the complete set of Analytical redundancy Relations (ARRs) for the system in an implicit form. For the diagnosis, our method first performs (similar to DX approaches) a system simulation to calculate the expected values of the measurements. Any discrepancy, i.e., the difference between expected and actual value of measurement, would trigger our diagnosis process. To this end, only those ARRs which involve the measurement with discrepancy are checked for consistency which lead a to a significant reduction in the number of consistency checks usually performed by DX approaches. We demonstrate the efficiency of our new method by its application to several synthetic systems and compare it with that of GDE.
C1 [Fijany, Amir] Italian Inst Technol, Genoa, Italy.
[Barrett, Anthony; Vatan, Farrokh] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Fijany, A (reprint author), Italian Inst Technol, Genoa, Italy.
EM Amir.Fijany@iit.it; Anthony.C.Barrett@jpl.nasa.gov;
Farrokh.Vatan@jpl.nasa.gov
NR 9
TC 1
Z9 2
U1 0
U2 4
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 346
EP +
DI 10.1109/SMC-IT.2009.58
PG 2
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700044
ER
PT B
AU Duong, TA
Duong, VA
AF Duong, Tuan A.
Duong, Vu A.
GP IEEE COMPUTER SOC
TI Sequential Principal Component Analysis-A Hardware-Implementable
Transform for Image Compression
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE Sequential Principal Component Analysis; Image compression; JPEG2000;
hardware implementation
AB This paper presents the JPL-developed Sequential Principal Component Analysis (SPCA) algorithm for feature extraction / image compression, based on "dominant-term selection" unsupervised learning technique that requires an order-of-magnitude lesser computation and has simpler architecture compared to the state of the art gradient-descent techniques. This algorithm is inherently amenable to a compact, low power and high speed VLSI hardware embodiment. The paper compares the lossless image compression performance of the JPL's SPCA algorithm with the state of the art JPEG2000, widely used due to its simplified hardware implementability. JPEG2000 is not an optimal data compression technique because of its fixed transform characteristics, regardless of its data structure. On the other hand, conventional Principal Component Analysis based transform (PCA-transform) is a data-dependent-structure transform. However, it is not easy to implement the PCA in compact VLSI hardware, due to its highly computational and architectural complexity. In contrast, the JPL's "dominant-term selection" SPCA algorithm allows, for the first time, a compact, low-power hardware implementation of the powerful PCA algorithm. This paper presents a direct comparison of the JPL's SPCA versus JPEG2000, incorporating the Huffman and arithmetic coding for completeness of the data compression operation. The simulation results show that JPL's SPCA algorithm is superior as an optimal data-dependent-transform over the state of tire art JPEG2000. When implemented in hardware, this technique is projected to be ideally suited to future NASA missions for autonomous on-board image data processing to improve the bandwidth of communication.
C1 [Duong, Tuan A.; Duong, Vu A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Duong, TA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM taduong@jpl.nasa.gov; vaduong@jpl.nasa.gov
NR 17
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 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 362
EP 366
DI 10.1109/SMC-IT.2009.49
PG 5
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700046
ER
PT B
AU Daugherty, SC
Cervantes, BW
AF Daugherty, Sarah C.
Cervantes, Benjamin W.
GP IEEE COMPUTER SOC
TI The Mission Planning Lab: A Visualization and Analysis Tool
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE modeling; simulation; software integration; visualization
AB Simulation and visualization are powerful decision making tools that are time-saving and cost-effiective. Space missions pose testing and evaluation challenges that can be overcome through modeling, simulation, and visualization Of mission parameters. The National Aeronautics and Space Administration's (NASA) Wallops Flight Facility (WFF) capitalizes on the benefits of modeling, simulation, and visualization tools through a project initiative called The Mission Planning Lab (MPL).
C1 [Daugherty, Sarah C.; Cervantes, Benjamin W.] NASA, Wallops Flight Facil, Wallops Syst Software Engn Branch, Wallops Isl, VA USA.
RP Daugherty, SC (reprint author), NASA, Wallops Flight Facil, Wallops Syst Software Engn Branch, Wallops Isl, VA USA.
EM Sarah.C.Daugherty@nasa.gov; Benjamin.W.Cervantes@nasa.gov
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 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 369
EP 375
DI 10.1109/SMC-IT.2009.51
PG 7
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700047
ER
PT B
AU Barrett, A
Dvorak, D
AF Barrett, Anthony
Dvorak, Daniel
GP IEEE COMPUTER SOC
TI A Combinatorial Test Suite Generator for Gray-Box Testing
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE software testing; combinatorial testing; gray-box testing
ID DESIGN
AB In black-box testing, the system being tested is typically characterized as a number of inputs, where each input can take one of a number of values. Thus each test is a vector of input settings, and the set of possible tests is an N dimensional space, where N is the number of inputs. For example, an instance of a simulation of a Crew Exploration Vehicle's (CEV) launch pad abort scenario can have 76 floating-point inputs. Unfortunately, for such a large number of inputs only a small percentage of the test space can be actually tested. This paper characterizes levels of partial test space coverage and presents Testgen, a tool for generating a suite of tests that guarantees a level of test space coverage, which a user can adapt to take advantage of knowledge of system internals. This ability to adapt coverage makes Testgen a gray-box testing tool.
C1 [Barrett, Anthony; Dvorak, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Barrett, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM anthony.barrett@jpl.nasa.gov; daniel.dvorak@jpl.nasa.gov
NR 16
TC 3
Z9 3
U1 0
U2 1
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 387
EP 393
DI 10.1109/SMC-IT.2009.53
PG 7
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700049
ER
PT B
AU Nikora, AP
Balcom, G
AF Nikora, Allen P.
Balcom, Galen
GP IEEE COMPUTER SOC
TI Improving the Accuracy of Space Mission Software Anomaly Frequency
Estimates
SO SMC-IT 2009: THIRD IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION
CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS
LA English
DT Proceedings Paper
CT 3rd IEEE International Conference on Space Mission Challenges for
Information Technology
CY JUL 19-23, 2009
CL Pasadena, CA
SP IEEE
DE error estimation; failure analysis; software reliability; text
processing
AB Anomaly data can be used to estimate baseline values for operational mission software anomaly frequencies; these estimates can be used for future missions to determine whether software reliability is improving. The accuracy of anomaly frequency estimates can be affected by characteristics of the anomaly data and the problem reporting system maintaining that data. We have been using text mining and machine learning techniques to address one of these issues, in which the number of software-related anomalies is incorrectly reported because the problem reporting system does not tag them correctly. Results to date indicate that these techniques may substantially increase the accuracy of anomaly frequency estimates.
C1 [Nikora, Allen P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Balcom, Galen] Calif State Univ Fresno, Dept Comp Sci, Fresno, CA 93740 USA.
RP Nikora, AP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Allen.P.Nikora@jpl.nasa.gov; gbalcom@csufresno.edu
NR 17
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 90720-1264 USA
BN 978-0-7695-3637-8
PY 2009
BP 402
EP +
DI 10.1109/SMC-IT.2009.55
PG 3
WC Engineering, Aerospace
SC Engineering
GA BMO51
UT WOS:000273122700051
ER
PT J
AU Yasunari, TJ
Yamazaki, K
AF Yasunari, Teppei J.
Yamazaki, Koji
TI Origins of Air Masses over an Alaskan Glacier and Implications for Ice
Core Studies in the North Pacific Region
SO SOLA
LA English
DT Article
ID STRATOSPHERE; CLIMATE; AEROSOLS; CANADA; YUKON; DUST
AB Simulations of 10-day backward trajectories of air masses from Mount Wrangell, an Alaskan ice core site, were calculated for 11 years on a daily basis. Results were analyzed statistically in order to interpret monthly air mass contributions over the ice core site and to discuss implications for ice core studies in the North Pacific Region (NPR).
Increases in tropospheric air mass transport from EA in spring suggest favorable transport conditions for Asian dust during this season. The stratospheric air mass (< 300 hPa) over the ice core site increases in winter and that from East Asia (EA) to the North Pacific Ocean in late spring. The tritium peaks observed in the ice core in late spring were discussed in the context of the present results with two possibilities on the time lag of tritium transportation in the stratosphere and the seasonal variations of water vapor amount in the troposphere. Increases in air masses originating from Siberia, Alaska and Canada in summer-fall favor the transport of black carbon due to forest fires over the ice core site. These results allow advanced interpretation of the origin and transport processes of materials in the ice core proxies in the NPR.
C1 [Yasunari, Teppei J.] NASA, Goddard Space Flight Ctr, GEST, UMBC, Greenbelt, MD 20771 USA.
[Yamazaki, Koji] Hokkaido Univ, Grad Sch Environm Sci, Sapporo, Hokkaido, Japan.
RP Yasunari, TJ (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, UMBC,GEST Ctr, Code 613-2, Greenbelt, MD 20771 USA.
EM tj.yasunari@gmail.com
RI Yasunari, Teppei/E-5374-2010
OI Yasunari, Teppei/0000-0002-9896-9404
NR 26
TC 5
Z9 5
U1 0
U2 5
PU METEOROLOGICAL SOC JPN
PI TOKYO
PA C/O JPN METEOROL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO, 100-0004,
JAPAN
SN 1349-6476
J9 SOLA
JI SOLA
PY 2009
VL 5
BP 77
EP 80
DI 10.2151/sola.2009-020
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 545PG
UT WOS:000273746300020
ER
PT J
AU Irie, H
Kanaya, Y
Takashima, H
Gleason, JF
Wang, ZF
AF Irie, Hitoshi
Kanaya, Yugo
Takashima, Hisahiro
Gleason, James F.
Wang, Zifa
TI Characterization of OMI Tropospheric NO2 Measurements in East Asia Based
on a Robust Validation Comparison
SO SOLA
LA English
DT Article
ID MAX-DOAS
AB In the period from June 2006 to December 2008, we measured the tropospheric nitrogen dioxide (NO2) column by ground-based Multi-Axis Differential Optical Absorption Spectroscopy (MAX-DOAS) at an urban site in China (Tai'an) and three sites in Japan, covering urban (Yokosuka), suburban (Tsukuba), and remote areas (Hedo). This robust dataset is used to characterize Ozone Monitoring Instrument (OMI) tropospheric NO2 column data (the standard product, version 3). Correlations between MAX-DOAS and OMI data, both of which show very low NO2 at Hedo and moderate/high levels at the other sites, have correlation coefficients (R-2) as high as 0.64, indicating that relative changes in OMI NO2 data are reliable. However, OMI data have a negative bias of 31% on average. Assuming that these results are valid for OMI data taken over China, we find an increasing trend in tropospheric column NO2 at about 5% per year on average in the industrial areas of China (30 degrees-40 degrees N and 110 degrees-123 degrees E) over 2005. 2008, but its spatial distribution is highly inhomogeneous.
C1 [Irie, Hitoshi; Kanaya, Yugo; Takashima, Hisahiro] JAMSTEC, Res Inst Global Change, Yokohama, Kanagawa, Japan.
[Gleason, James F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wang, Zifa] Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China.
RP Irie, H (reprint author), Japan Agcy Marine Earth Sci & Technol, Res Inst Global Change, Kanazawa Ku, 3173-25 Showa Machi, Kanagawa 2360001, Japan.
EM irie@jamstec.go.jp
RI Kanaya, Yugo/C-7446-2012; Wang, ZF/D-7202-2012; Gleason,
James/E-1421-2012; Wang, Zifa/B-5799-2011
OI Wang, ZF/0000-0002-7062-6012;
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT);
Ministry of the Environment, Japan [S-7]
FX We thank PREDE, Co., Ltd for their technical assistance in developing
the MAX-DOAS instruments. We are grateful to NIES for supporting
measurements at Tsukuba and Hedo. This work was supported by the Japan
EOS (Earth Observation System) Promotion Program of the Ministry of
Education, Culture, Sports, Science and Technology (MEXT). This work was
supported by the Global Environment Research Fund (S-7) of the Ministry
of the Environment, Japan.
NR 14
TC 11
Z9 13
U1 1
U2 8
PU METEOROLOGICAL SOC JPN
PI TOKYO
PA C/O JPN METEOROL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO, 100-0004,
JAPAN
SN 1349-6476
J9 SOLA
JI SOLA
PY 2009
VL 5
BP 117
EP 120
DI 10.2151/sola.2009-030
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 545PG
UT WOS:000273746300030
ER
PT B
AU Zhao, J
Hartlep, T
Kosovichev, AG
Mansour, NN
AF Zhao, J.
Hartlep, T.
Kosovichev, A. G.
Mansour, N. N.
BE Dikpati, M
Arentoft, T
Hernandez, IG
Lindsey, C
Hill, F
TI Time-Distance Helioseismic Imaging of a Numerically Simulated Solar
Tachocline
SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG
2008/SOHO 21
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and
Asteroseismology (GONG 2008/SOHO 21)
CY AUG 11-15, 2008
CL High Altitude Observ, Boulder, CO
HO High Altitude Observ
ID ROTATION; INTERIOR
AB The solar tachocline, located near the bottom of the convection zone, is a very important region for solar dynamics and the solar dynamo. We develop a time-distance helioseismology technique, including both surface- and deep-focusing measurements, together with inversions, to derive the interior image of the sound speed perturbation at the tachocline with a latitudinal dependence. We test the technique on numerically simulated global wavefields and find that the technique is able to recover the major features that are preset in the numerical model, though a bit more widespread into the deeper interior. This measurement and inversion technique will be applied to MDI observations to derive the structures of solar tachocline.
C1 [Zhao, J.; Kosovichev, A. G.] Stanford Univ, WW Hansen Expt Phys Lab, Room 130-452 Lomita Mall, Stanford, CA 94305 USA.
[Hartlep, T.; Mansour, N. N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Zhao, J (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Room 130-452 Lomita Mall, Stanford, CA 94305 USA.
EM junwei@solar.stanford.edu; thartlep@solar.stanford.edu;
akosovichev@solar.stanford.edu
NR 10
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-712-4
J9 ASTR SOC P
PY 2009
VL 416
BP 25
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL27
UT WOS:000281240900003
ER
PT B
AU Jacoutot, L
Kosovichev, A
Wray, A
Mansour, N
AF Jacoutot, L.
Kosovichev, A.
Wray, A.
Mansour, N.
BE Dikpati, M
Arentoft, T
Hernandez, IG
Lindsey, C
Hill, F
TI Realistic MHD Simulations of Solar Convection and Oscillations in
Magnetic Regions: Mode Excitation and Effects of Acoustic Halos
SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG
2008/SOHO 21
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and
Asteroseismology (GONG 2008/SOHO 21)
CY AUG 11-15, 2008
CL High Altitude Observ, Boulder, CO
HO High Altitude Observ
ID P-MODES; TURBULENT CONVECTION; RADIAL OSCILLATIONS; SUN
AB We have used a 3D, compressible, non-linear radiative magnetohydrodynamics code developed at the NASA Ames Research Center to model solar convection and oscillations in magnetic regions. This code takes into account several physical phenomena: compressible fluid flow in a highly stratified medium, sub-grid scale turbulence models, radiative energy transfer, and a real-gas equation of state. We have studied the influence of the magnetic field of various strength on the convective cells and on the excitation mechanisms of the acoustic oscillations by calculating spectral properties of the convective motions and oscillations. The results reveal substantial changes of the granulation structure with increased magnetic field, and a frequency-dependent reduction in the oscillation power in a good agreement with solar observations. The simulations provide a solution to the long-standing problem of enhanced high-frequency acoustic emission at the boundaries of active region ("acoustic halos"), suggesting that this phenomenon is caused by the changes of the spatial-temporal spectrum of the turbulent convection in magnetic field, resulting in turbulent motions of smaller scales and higher frequencies than in quiet Sun regions. These simulation results may have also important implications for understanding high-frequency oscillations of magnetic stars.
C1 [Jacoutot, L.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA.
[Kosovichev, A.] Stanford Univ, HEPL, Stanford, CA 94305 USA.
[Wray, A.; Mansour, N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Jacoutot, L (reprint author), Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA.
EM akosovichev@solar.stanford.edu
NR 17
TC 1
Z9 1
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-712-4
J9 ASTR SOC P
PY 2009
VL 416
BP 67
EP +
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL27
UT WOS:000281240900009
ER
PT B
AU Duvall, TL
Hanasoge, SM
AF Duvall, T. L., Jr.
Hanasoge, S. M.
BE Dikpati, M
Arentoft, T
Hernandez, IG
Lindsey, C
Hill, F
TI Measuring Meridional Circulation in the Sun
SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG
2008/SOHO 21
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and
Asteroseismology (GONG 2008/SOHO 21)
CY AUG 11-15, 2008
CL High Altitude Observ, Boulder, CO
HO High Altitude Observ
ID TIME-DISTANCE HELIOSEISMOLOGY
AB Measuring the depth variation of the meridional flows is important for understanding the solar cycle, at least according to a number of dynamo models. While attempting to extend the early observations of Giles (2000) of time-distance measurements of flow, we have stumbled upon some systematic errors that can affect these measurements: 1) the additional distance traveled by radiation coming from points away from disk center causes an apparent 'shrinking' Sun, that is an apparent flow towards the disk center and 2) in measurements away from the central longitude, the rotation signal can leak into meridional flow signals. Attempts to understand and overcome these systematic problems will be presented. Forward models based on ray theory have been applied in order to test the sensitivity of travel times to various models.
C1 [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Hanasoge, S. M.] Stanford Univ, W W Hansen Expt Phys Lab, Stanford, CA 94305 USA.
RP Duvall, TL (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
EM tduvall@solar.stanford.edu; hanasoge@gmail.com
RI Duvall, Thomas/C-9998-2012
NR 11
TC 11
Z9 11
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-712-4
J9 ASTR SOC P
PY 2009
VL 416
BP 103
EP +
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL27
UT WOS:000281240900015
ER
PT B
AU Beck, JG
Duvall, TL
Zhao, J
AF Beck, J. G.
Duvall, T. L., Jr.
Zhao, J.
BE Dikpati, M
Arentoft, T
Hernandez, IG
Lindsey, C
Hill, F
TI Travel-Time Errors Due To Data Gaps
SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG
2008/SOHO 21
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and
Asteroseismology (GONG 2008/SOHO 21)
CY AUG 11-15, 2008
CL High Altitude Observ, Boulder, CO
HO High Altitude Observ
AB Time-distance measurements of wave packet travel times can be used to determine various properties of the plasma through which the p modes propagate, however, missing data can introduce significant errors in the travel time measurements. We find that the magnitude of the error depends on the amount of missing data, the temporal position of the data gaps, and the travel distance, but not on the continuity of data gaps. Further, apodizing the data gaps or linearly filling the gaps fails to reduce the errors.
C1 [Beck, J. G.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford Solar Observ, Room 130-452 Lomita Mall, Stanford, CA 94305 USA.
[Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Beck, JG (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford Solar Observ, Room 130-452 Lomita Mall, Stanford, CA 94305 USA.
EM jbeck@solar.stanford.edu; tduvall@solar.stanford.edu;
junwei@solar.stanford.edu
RI Duvall, Thomas/C-9998-2012
FU NASA [NAG5-8878]
FX This work was supported by NASA grant NAG5-8878.
NR 3
TC 0
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U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-712-4
J9 ASTR SOC P
PY 2009
VL 416
BP 135
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL27
UT WOS:000281240900022
ER
PT B
AU Hartlep, T
Kosovichev, AG
Zhao, J
Mansour, NN
AF Hartlep, T.
Kosovichev, A. G.
Zhao, J.
Mansour, N. N.
BE Dikpati, M
Arentoft, T
Hernandez, IG
Lindsey, C
Hill, F
TI Signatures of Emerging Subsurface Structures in Acoustic Power Maps
SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG
2008/SOHO 21
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and
Asteroseismology (GONG 2008/SOHO 21)
CY AUG 11-15, 2008
CL High Altitude Observ, Boulder, CO
HO High Altitude Observ
ID NUMERICAL SIMULATIONS; SOLAR; SUN
AB We show that under suitable conditions subsurface structures can alter the average acoustic power observed at the photosphere. By using numerical simulations of wave propagation, we investigate whether this effect can be used to detect emerging active regions before they appear on the surface. In the simulations, subsurface structures are modeled as regions with enhanced or reduced acoustic wave speed. We show how the acoustic power above a subsurface region depends on the sign, depth and strength of the wave speed perturbation. For comparison, we analyze observations from SOHO/MDI of the emergence of active region NOAA 10488.
C1 [Hartlep, T.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA.
[Kosovichev, A. G.; Zhao, J.] Stanford Univ, W W Hansen Expt Phys, Stanford, CA 94305 USA.
[Mansour, N. N.] NASA Ames Res Ctr, Moffett Field, CA USA.
RP Hartlep, T (reprint author), Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA.
EM thartlep@solar.stanford.edu; akosovichev@solar.stanford.edu;
junwei@solar.stanford.edu
NR 8
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-712-4
J9 ASTR SOC P
PY 2009
VL 416
BP 147
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL27
UT WOS:000281240900025
ER
PT B
AU Ilonidis, S
Zhao, J
Hartlep, T
AF Ilonidis, S.
Zhao, J.
Hartlep, T.
BE Dikpati, M
Arentoft, T
Hernandez, IG
Lindsey, C
Hill, F
TI Time-Distance Solar Far-Side Imaging Using Three-Skip Acoustic Signals
SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG
2008/SOHO 21
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and
Asteroseismology (GONG 2008/SOHO 21)
CY AUG 11-15, 2008
CL High Altitude Observ, Boulder, CO
HO High Altitude Observ
ID SUN
AB The purpose of this work is to image the solar far-side active regions using acoustic signals with three skips. The mapping of the far-side active regions was first made possible (Lindsey & Braun 2000) using helioseismic holography technique by use of four-skip acoustic signals. The quality of far-side images was later improved with the combination of four- and five-skip signals using the time-distance technique (Zhao 2007). In this work, we further explore the possibility of making three-skip far-side images of active regions, and improving the image quality by combining the three-skip images with the images obtained from existing techniques.
C1 [Ilonidis, S.; Zhao, J.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Zhao, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hartlep, T.] Stanford Univ, W W Hansen Expt Phys Lab, Stanford, CA 94305 USA.
RP Ilonidis, S (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM ilonidis@solar.stanford.edu; junwei@solar.stanford.edu;
thartlep@solar.stanford.edu
FU NASA Living With a Star program and the NASA Postdoctoral Program
administered by Oak Ridge Associated Universities under contract with
NASA
FX The numerical simulations used in this paper were performed at NASA Ames
Research Center. T.H. was supported by the NASA Living With a Star
program and the NASA Postdoctoral Program administered by Oak Ridge
Associated Universities under contract with NASA.
NR 8
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-712-4
J9 ASTR SOC P
PY 2009
VL 416
BP 163
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL27
UT WOS:000281240900029
ER
PT B
AU Hathaway, DH
Williams, PE
Cuntz, M
AF Hathaway, D. H.
Williams, P. E.
Cuntz, M.
BE Dikpati, M
Arentoft, T
Hernandez, IG
Lindsey, C
Hill, F
TI The Advection of Supergranules by Large-Scale Flows
SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG
2008/SOHO 21
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and
Asteroseismology (GONG 2008/SOHO 21)
CY AUG 11-15, 2008
CL High Altitude Observ, Boulder, CO
HO High Altitude Observ
ID SPHERICAL HARMONIC-ANALYSIS; STEADY PHOTOSPHERIC FLOWS; MICHELSON
DOPPLER IMAGER; SOLAR PHOTOSPHERE; VELOCITY-FIELDS; ROTATION
AB We produce a 10-day series of simulated Doppler images at a 15-minute cadence that reproduces the spatial and temporal characteristics seen in the SOHO/MDI Doppler data. Our simulated data contains a spectrum of cellular flows with but two necessary components-a granule component that peaks at wavenumbers of about 4000 and a supergranule component that peaks at wavenumbers of about 110. We include the advection of these cellular components by a differential rotation profile that depends on latitude and wavenumber (depth). We further mimic the evolution of the cellular pattern by introducing random variations to the amplitudes and phases of the spectral components at rates that reproduce the level of cross-correlation as a function of time and latitude. Our simulated data do not include any wave-like characteristics for the supergranules yet can accurately reproduce the rotation characteristics previously attributed to wave-like characteristics.
C1 [Hathaway, D. H.] NASA, George C Marshall Space Flight Ctr, Code ES-82, Huntsville, AL 35812 USA.
[Williams, P. E.; Cuntz, M.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA.
RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, Code ES-82, Huntsville, AL 35812 USA.
EM david.hathaway@msfc.nasa.gov
FU NASA Marshall Space Flight Center; University of Texas Arlington
FX We would like to thank NASA for its support of this research through a
grant from the Heliophysics Guest Investigator Program to NASA Marshall
Space Flight Center and The University of Texas Arlington. We would also
like to thank the SOHO/MDI team for the critical role they played in
producing the raw MDI data and John Beck in particular for implementing
the temporal averaging of that data to remove the p-mode noise.
NR 18
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-712-4
J9 ASTR SOC P
PY 2009
VL 416
BP 495
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL27
UT WOS:000281240900086
ER
PT B
AU Svanda, M
Kosovichev, AG
Klvana, M
Sobotka, M
Duvall, TL
AF Svanda, M.
Kosovichev, A. G.
Klvana, M.
Sobotka, M.
Duvall, T. L., Jr.
BE Dikpati, M
Arentoft, T
Hernandez, IG
Lindsey, C
Hill, F
TI Transport of Supergranules and their Vertical Coherence
SO SOLAR-STELLAR DYNAMOS AS REVEALED BY HELIO AND ASTEROSEISMOLOGY: GONG
2008/SOHO 21
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Workshop on Solar-Stellar Dynamos as Revealed by Helio and
Asteroseismology (GONG 2008/SOHO 21)
CY AUG 11-15, 2008
CL High Altitude Observ, Boulder, CO
HO High Altitude Observ
ID TIME-DISTANCE HELIOSEISMOLOGY; SOLAR SUPERGRANULATION; FLOWS
AB In recent papers, we have introduced a method for measuring the photospheric flow field that is based on the tracking of supergranular structures. Here, in combination with helioseismic data, we are able to estimate the depth in the solar convection envelope to which the detected large-scale flow field is coherent. We show that the upper 10 Mm in the convection zone depicts similar features in horizontal velocity. Our interpretation of this observation is that the supergranulation is a coherent structure 10 Mm deep and is subject to large-scale transport by the underlying velocity field.
C1 [Svanda, M.] Charles Univ Prague, Astron Inst, V Holesovickach 2, Prague, Czech Republic.
[Svanda, M.; Klvana, M.; Sobotka, M.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, CZ-25165 Ondrejov, Czech Republic.
[Kosovichev, A. G.] Stanford Univ, HEPL, Stanford, CA 94305 USA.
[Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Svanda, M (reprint author), Charles Univ Prague, Astron Inst, V Holesovickach 2, Prague, Czech Republic.
EM akosovichev@solar.stanford.edu; tduvall@solar.stanford.edu
RI Svanda, Michal/A-6576-2008; Duvall, Thomas/C-9998-2012; Sobotka,
Michal/G-9042-2014
OI Svanda, Michal/0000-0002-6345-1007; Sobotka, Michal/0000-0001-5439-7822
FU Agency of Academy of Science of the Czech Republic [IAA30030808];
Astronomical Institute of Charles University [MSM0021620860]; Ministry
of Education of CR
FX M.S, M. K.,and M. S. were supported by the Grant Agency of Academy of
Science of the Czech Republic under grant IAA30030808. The Astronomical
Institute of Charles University works on the Research program
MSM0021620860 (Ministry of Education of CR).
NR 7
TC 1
Z9 1
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-712-4
J9 ASTR SOC P
PY 2009
VL 416
BP 547
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL27
UT WOS:000281240900095
ER
PT S
AU Prasad, NS
Trivedi, S
Kutcher, S
Wang, CC
Kim, JS
Hommerich, U
Shukla, V
Sadangi, R
AF Prasad, Narasimha S.
Trivedi, Sudhir
Kutcher, Susan
Wang, Chen-Chia
Kim, Joo-Soo
Hommerich, Uwe
Shukla, Vijay
Sadangi, Rajendra
BE Clarkson, WA
Hodgson, N
Shori, RK
TI Development of ceramic solid-state laser host materials
SO SOLID STATE LASERS XVIII: TECHNOLOGY AND DEVICES
SE Proceedings of SPIE-The International Society for Optical Engineering
LA English
DT Proceedings Paper
CT Conference on Solid State Lasers XVIII - Technology and Devices
CY JAN 25-29, 2009
CL San Jose, CA
SP SPIE, Coherent, Inc
DE Solid-state lasers; ceramic laser host materials; Neodymium doped
Yttria; Ytterbium Yttria; Erbium Yttria; Scandium Oxide; Lutesium Oxide
ID TRANSFORMATION-ASSISTED CONSOLIDATION
AB Polycrystalline ceramic laser materials are gaining importance in the development of novel diode-pumped solid-state lasers. Compared to single-crystals, ceramic laser materials offer advantages in terms of ease of fabrication, shape, size, and control of dopant concentrations. Recently, we have developed Neodymium doped Yttria (Nd:Y(2)O(3)) as a solid-state ceramic laser material. A scalable production method was utilized to make spherical non agglomerated and monodisperse metastable ceramic powders of compositions that were used to fabricate polycrystalline ceramic material components. This processing technique allowed for higher doping concentrations without the segregation problems that are normally encountered in single crystalline growth. We have successfully fabricated undoped and Neodymium doped Yttria material up to 2 '' in diameter, Ytterbium doped Yttria, and erbium doped Yttria. We are also in the process of developing other sesquioxides such as scandium Oxide (Sc(2)O(3)) and Lutesium Oxide (Lu(2)O(3)) doped with Ytterbium, erbium and thulium dopants. In this paper, we present our initial results on the material, optical, and spectroscopic properties of the doped and undoped sesquioxide materials. Polycrystalline ceramic lasers have enormous potential applications including remote sensing, chem.-bio detection, and space exploration research. It is also potentially much less expensive to produce ceramic laser materials compared to their single crystalline counterparts because of the shorter fabrication time and the potential for mass production in large sizes.
C1 [Prasad, Narasimha S.] NASA, Langley Res Ctr, Laser Remote Sensing Branch, Hampton, VA 23681 USA.
RP Prasad, NS (reprint author), NASA, Langley Res Ctr, Laser Remote Sensing Branch, 5 N Dryden St,MS 468, Hampton, VA 23681 USA.
EM Narasimha.s.prasad@nasa.gov
NR 6
TC 0
Z9 0
U1 0
U2 6
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7439-1
J9 P SOC PHOTO-OPT INS
PY 2009
VL 7193
AR 71931X
DI 10.1117/12.813785
PG 11
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BSL69
UT WOS:000284870500055
ER
PT S
AU Prasad, NS
AF Prasad, Narasimha S.
BE Clarkson, WA
Hodgson, N
Shori, RK
TI Some Activities of MISSE 6 Mission
SO SOLID STATE LASERS XVIII: TECHNOLOGY AND DEVICES
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Solid State Lasers XVIII - Technology and Devices
CY JAN 25-29, 2009
CL San Jose, CA
SP SPIE, Coherent Inc
DE MISSE 6; Space Qualification; Laser components; International Space
Station; STS-123
AB The objective of the Materials International Space Station Experiment (MISSE) is to study the performance of novel materials when subjected to the synergistic effects of the harsh space environment for several months. In this paper, a few laser and optical elements from NASA Langley Research Center (LaRC) that have been flown on MISSE 6 mission will be discussed. These items were characterized and packed inside a ruggedized Passive Experiment Container (PEC) that resembles a suitcase. The PEC was tested for survivability due to launch conditions. Subsequently, the MISSE 6 PEC was transported by the STS-123 mission to International Space Station (ISS) on March 11, 2008. The astronauts successfully attached the PEC to external handrails and opened the PEC for long term exposure to the space environment. The plan is to retrieve the MISSE 6 PEC by STS-128 mission in August 2009.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Prasad, NS (reprint author), NASA, Langley Res Ctr, 5 N Dryden St,MS 468, Hampton, VA 23681 USA.
EM narasimha.s.prasad@nasa.gov
NR 7
TC 0
Z9 0
U1 0
U2 1
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7439-1
J9 PROC SPIE
PY 2009
VL 7193
AR 719304
DI 10.1117/12.814870
PG 7
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BSL69
UT WOS:000284870500001
ER
PT S
AU Shaw, GB
Stephen, MA
Troupaki, E
Vasilyev, AA
Yu, AW
AF Shaw, George B.
Stephen, Mark A.
Troupaki, Elisavet
Vasilyev, Aleksey A.
Yu, Anthony W.
BE Clarkson, WA
Hodgson, N
Shori, RK
TI Longevity validation of the LOLA laser design by extended vacuum testing
of the LOLA engineering model laser
SO SOLID STATE LASERS XVIII: TECHNOLOGY AND DEVICES
SE Proceedings of SPIE-The International Society for Optical Engineering
LA English
DT Proceedings Paper
CT Conference on Solid State Lasers XVIII - Technology and Devices
CY JAN 25-29, 2009
CL San Jose, CA
SP SPIE, Coherent, Inc
DE Lunar Orbiter Laser Altimeter; LOLA; Laser; Nd:YAG; Topography; LIDAR;
Altimeter; Space laser
ID MISSION
AB The Lunar Orbiter Laser Altimeter (LOLA) is one of seven instruments aboard the Lunar Reconnaissance Orbiter (LRO) spacecraft with the objectives to determine the global topography of the lunar surface at high resolution, measure landing site slopes and search for polar ices in shadowed regions. The LOLA laser transmitter is a passively Q-switched crossed-Porro resonator. All components used in the laser have space flight heritage. The flight laser bench houses two oscillators (a primary and a cold spare) that are designed to operate sequentially during the mission. If the primary laser can no longer provide adequate scientific data products, the secondary laser will be turned on. The baseline mission calls for LOLA (and LRO) to spend about one year studying the Moon. Since LOLA operates at 28 Hz, the laser system needs to produce approximately one billion pulses during the primary one year mission. To validate that the LOLA laser design is capable of meeting this requirement, the LOLA Engineering Model (EM) laser has been subjected to extended operation testing in vacuum. In this paper we will summarize the longevity validation test effort of the LOLA EM laser.
C1 [Shaw, George B.; Stephen, Mark A.; Troupaki, Elisavet; Vasilyev, Aleksey A.; Yu, Anthony W.] NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, Greenbelt, MD 20771 USA.
RP Shaw, GB (reprint author), NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, MC554, Greenbelt, MD 20771 USA.
NR 6
TC 2
Z9 2
U1 1
U2 2
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7439-1
J9 P SOC PHOTO-OPT INS
PY 2009
VL 7193
AR 719306
DI 10.1117/12.814883
PG 12
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BSL69
UT WOS:000284870500003
ER
PT S
AU Yu, AW
Li, SX
Shaw, GB
Seas, A
Stephen, MA
Troupaki, E
Vasilyev, A
Ramos-Izquierdo, L
Lukemier, A
Mamakos, W
Melak, A
Guzek, J
Rosanova, A
AF Yu, Anthony W.
Li, Steve X.
Shaw, George B.
Seas, Antonios
Stephen, Mark A.
Troupaki, Elisavet
Vasilyev, Aleksey
Ramos-Izquierdo, Luis
Lukemier, Alan
Mamakos, William
Melak, Anthony
Guzek, Jeff
Rosanova, Alberto
BE Clarkson, WA
Hodgson, N
Shori, RK
TI Overview of Space Qualified Solid-State Lasers Development at NASA
Goddard Space Flight Center
SO SOLID STATE LASERS XVIII: TECHNOLOGY AND DEVICES
SE Proceedings of SPIE-The International Society for Optical Engineering
LA English
DT Proceedings Paper
CT Conference on Solid State Lasers XVIII - Technology and Devices
CY JAN 25-29, 2009
CL San Jose, CA
SP SPIE, Coherent, Inc
DE Topography; LIDAR; Remote Sensing; Space Laser Systems; Laser Altimeter;
Space-Qualified Lasers
ID MESSENGER MISSION; MERCURY; ALTIMETER; TRANSMITTER; MARS
AB NASA Goddard Space Flight Center (GSFC) has been engaging in Earth and planetary science instruments development for many years. With stunning topographic details of the Mars surface to Earth's surface maps and ice sheets dynamics of recent years, NASA GSFC has provided vast amount of scientific data products that gave detailed insights into Earth's and planetary sciences. In this paper we will review the past and present of space-qualified laser programs at GSFC and offer insights into future laser based science instrumentations.
C1 [Yu, Anthony W.; Li, Steve X.; Shaw, George B.; Seas, Antonios; Stephen, Mark A.; Troupaki, Elisavet; Vasilyev, Aleksey; Ramos-Izquierdo, Luis; Lukemier, Alan; Mamakos, William; Melak, Anthony; Guzek, Jeff; Rosanova, Alberto] NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, Greenbelt, MD 20771 USA.
RP Yu, AW (reprint author), NASA, Goddard Space Flight Ctr, Laser & Electroopt Branch, Greenbelt, MD 20771 USA.
NR 28
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Z9 5
U1 1
U2 3
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7439-1
J9 P SOC PHOTO-OPT INS
PY 2009
VL 7193
AR 719305
DI 10.1117/12.814954
PG 7
WC Instruments & Instrumentation; Optics
SC Instruments & Instrumentation; Optics
GA BSL69
UT WOS:000284870500002
ER
PT S
AU Loewenstein, M
AF Loewenstein, Michael
BE Cline, DB
TI Suzaku search for evidence of sterile neutrinos in the Ursa Minor dwarf
spheroidal galaxy
SO SOURCES AND DETECTION OF DARK MATTER AND DARK ENERGY IN THE UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 8th UCLA Symposium on Sources and Detection of Dark Matter and Dark
Energy in the Universe
CY FEB 20-22, 2008
CL Marina del Rey, CA
SP Univ Calif Los Angeles
DE sterile neutrinos; dark matter
ID WARM DARK-MATTER; X-RAY; MILKY-WAY; OSCILLATIONS; SUPERNOVA; KICKS; XIS
AB We present results of our search for X-ray line emission associated with the radiative decay of the sterile neutrino, a well-motivated dark matter candidate, in Suzaku Observatory spectra of the Ursa Minor dwarf spheroidal galaxy. These data represent the first deep observation of one of these extreme mass-to-light systems and the first dedicated dark matter search using an X-ray telescope. No such emission line is positively detected; and, we derive new upper limits that match or approach the best previous results over the entire 1-20 ke V mass range from a single Suzaku observation. These are used to place constraints on the existence of sterile neutrinos with given combinations of mass and active-sterile neutrino oscillation mixing angle in the general case, and in the case where they are assumed to constitute all of the dark matter. The allowed range implies that sterile neutrinos remain a viable candidate to make up some - or all - of the dark matter and also explain pulsar kicks and various other astrophysical phenomena.
C1 [Loewenstein, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Loewenstein, M (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
NR 27
TC 0
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U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0703-9
J9 AIP CONF PROC
PY 2009
VL 1166
BP 185
EP 190
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BPR82
UT WOS:000279741300025
ER
PT S
AU Abers, ES
Bhatia, AK
Dicus, DA
Repko, WW
Rosenbaum, DC
Teplitz, VL
AF Abers, E. S.
Bhatia, A. K.
Dicus, D. A.
Repko, W. W.
Rosenbaum, D. C.
Teplitz, V. L.
BE Cline, DB
TI Strange Quark Nuggets in Space: Charges in Seven Settings
SO SOURCES AND DETECTION OF DARK MATTER AND DARK ENERGY IN THE UNIVERSE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 8th UCLA Symposium on Sources and Detection of Dark Matter and Dark
Energy in the Universe
CY FEB 20-22, 2008
CL Marina del Rey, CA
SP Univ Calif Los Angeles
ID NUCLEARITES; MATTER
AB We have computed the charge that develops on an SQN in space as a result of balance between the rates of ionization by ambient gammas and capture of ambient electrons. We have also computed the tin-as for achieving that equilibrium and binding energy of the least bound SQN electrons. We have done this for seven different settings. We sketch the calculations here and give their results in the Figure and Table II; details are in the Physical Review D.79.023513 (2009).
C1 [Abers, E. S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Bhatia, A. K.; Teplitz, V. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dicus, D. A.] Univ Texas Austin, Dept Phys, Austin, TX 78712 USA.
[Repko, W. W.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Rosenbaum, D. C.; Teplitz, V. L.] Southern Methodist Univ, Dept Phys, Dallas, TX 75275 USA.
RP Abers, ES (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
FU U.S. Department of Energy [DE-FG03-93ER40757]; National Science
Foundation [PHY-0555544]
FX VLT very much appreciates a number of very helpful conversations with
Demos Kazanas, one with Floyd Stecker on the diffuse gamma ray spectrum
and one with M. Alford on effects of Cooper pairing. Dr. Alford kindly
provided a number of insightful comments on the first version of this
paper. DCR and VLT are also grateful to Jonathan Gardner for calling
SN-2006gy to our attention, as well as C. Kilbourne for talking WHIM
with us. DAD was supported in part by the U.S. Department of Energy
under Grant No. DE-FG03-93ER40757. WWR was supported in part by the
National Science Foundation under Grant PHY-0555544.
NR 17
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PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0703-9
J9 AIP CONF PROC
PY 2009
VL 1166
BP 242
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BPR82
UT WOS:000279741300034
ER
PT B
AU Moltz, JC
AF Moltz, James Clay
BE Coletta, D
Pilch, FT
TI Russia and China Strategic choices in space
SO SPACE AND DEFENSE POLICY
SE Space Power and Politics
LA English
DT Article; Book Chapter
C1 [Moltz, James Clay] NASA, Space Futures Working Grp, Ames Res Ctr, Washington, DC USA.
[Moltz, James Clay] Monterey Inst Int Studies, CNS, Monterey, CA USA.
NR 15
TC 0
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PU ROUTLEDGE
PI LONDON
PA 11 NEW FETTER LANE, LONDON EC4P 4EE, ENGLAND
BN 978-0-203-88306-8
J9 SPACE POWER POLIT
PY 2009
BP 269
EP 289
PG 21
WC International Relations; Political Science
SC International Relations; Government & Law
GA BNL06
UT WOS:000274836500013
ER
PT B
AU Souza, KA
Ilyin, EA
Sychev, VN
Jahns, GC
AF Souza, Kenneth A.
Ilyin, Eugene A.
Sychev, Vladimir N.
Jahns, Gary C.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Biological Research in Space
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
ID MESSENGER-RNA LEVELS; ALTERED GRAVITATIONAL-FIELDS; PERIPHERAL-BLOOD
LEUKOCYTES; LOCUS-COERULEUS NEURONS; BONE-MATRIX PROTEINS;
LIFE-SUPPORT-SYSTEM; SKELETAL-MUSCLE; GENE-EXPRESSION; SPACEFLIGHT
CONDITIONS; ESCHERICHIA-COLI
C1 [Souza, Kenneth A.] NASA, Ames Res Ctr, Mail Code SC, Mountain View, CA 94035 USA.
[Ilyin, Eugene A.; Sychev, Vladimir N.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
[Jahns, Gary C.] NASA, Ames Res Ctr, Mail Code VB, Mountain View, CA 94035 USA.
RP Souza, KA (reprint author), NASA, Ames Res Ctr, Mail Code SC, Mountain View, CA 94035 USA.
EM Kenneth.A.Souza@nasa.gov; ilyine@imbp.ru; Gary.c.jahns@nasa.gov
NR 291
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PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 1
EP 43
PG 43
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900002
ER
PT B
AU House, NG
Samarin, GI
AF House, Nancy G.
Samarin, G. I.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Biomedical Research in Spaceflight
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
ID INTERNATIONAL-SPACE-STATION; ORTHOSTATIC HYPOTENSION; BONE METABOLISM;
ASTRONAUTS; FLIGHT
C1 [House, Nancy G.] NASA, Lyndon B Johnson Space Ctr, Stinger Ghaffarian Technol Mail Code ZB, Houston, TX 77058 USA.
[Samarin, G. I.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
RP House, NG (reprint author), NASA, Lyndon B Johnson Space Ctr, Stinger Ghaffarian Technol Mail Code ZB, Houston, TX 77058 USA.
EM Nancy.g.house@nasa.gov; samarin@imbp.ru; Nancy.g.house@nasa.gov
NR 36
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PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 69
EP 194
PG 126
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900004
ER
PT B
AU Katuntsev, VP
Osipov, YY
Gernhardt, M
Dervay, J
Thomas, KS
Reeves, JM
AF Katuntsev, V. P.
Osipov, Yu Yu.
Gernhardt, M.
Dervay, J.
Thomas, K. S.
Reeves, J. M.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Extravehicular Activity
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
ID DECOMPRESSION-SICKNESS; ALTITUDE DECOMPRESSION; EVA; PRESSURE; SUPPORT;
MIR
C1 [Katuntsev, V. P.; Osipov, Yu Yu.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
[Gernhardt, M.] NASA, Lyndon B Johnson Space Ctr, Mail Code CB, Houston, TX 77058 USA.
[Thomas, K. S.] Hamilton Sundstrand Corp, Windsor Locks, CT 06096 USA.
[Dervay, J.] NASA, Lyndon B Johnson Space Ctr, Mail Code SD2, Houston, TX 77058 USA.
[Reeves, J. M.] NASA, Lyndon B Johnson Space Ctr, Muniz Engn Inc, Mail Code SK, Houston, TX 77058 USA.
RP Katuntsev, VP (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia.
EM katuntsev@imbp.ru; osipov@imbp.ru; michael.l.gernhardt@nasa.gov;
joseph.p.dervay@nasa.gov; jacqueline.m.reeves@nasa.gov
NR 47
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PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 195
EP 233
PG 39
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900005
ER
PT B
AU Baranov, VM
Mccoy, JT
Agureev, AN
AF Baranov, V. M.
McCoy, J. Torin
Agureev, Aleksandr N.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Habitable Environment of the International Space Station Overview
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Editorial Material; Book Chapter
C1 [Baranov, V. M.; Agureev, Aleksandr N.] Russian Acad Sci, State Res Ctr, Inst Biomed Problems, Moscow 123007, Russia.
[McCoy, J. Torin] NASA, Lyndon B Johnson Space Ctr, Environm Factors Branch, Space & Life Sci Directorate, Washington, DC USA.
RP Baranov, VM (reprint author), Russian Acad Sci, State Res Ctr, Inst Biomed Problems, 76A Khoroshevskoye Shosse, Moscow 123007, Russia.
EM baranov@imbp.ru; aagureev@imbp.ru
NR 0
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U2 0
PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 235
EP 236
PG 2
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900006
ER
PT B
AU Bogatova, RI
Allen, CS
Kutina, IV
Goodman, JR
AF Bogatova, R. I.
Allen, C. S.
Kutina, I. V.
Goodman, J. R.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Microclimate, Acoustic Environment, and Lighting Conditions
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
C1 [Bogatova, R. I.; Kutina, I. V.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
[Allen, C. S.; Goodman, J. R.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF2, Houston, TX 77058 USA.
RP Bogatova, RI (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia.
EM rimma@imbp.ru; christopher.s.allen@nasa.gov; jerry.r.goodman@nasa.gov
NR 30
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PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 237
EP 248
PG 12
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900007
ER
PT B
AU Mukhamedieva, LN
James, JT
Aksel-Rubinstein, VZ
Solomin, GI
AF Mukhamedieva, L. N.
James, J. T.
Aksel-Rubinstein, V. Z.
Solomin, G. I.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Toxicology of the International Space Station Atmosphere
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
C1 [Mukhamedieva, L. N.; Solomin, G. I.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
[Aksel-Rubinstein, V. Z.] Minist Hlth Russian Federat, GUP Sci Res Inst Ind & Marine Med, St Petersburg 196143, Russia.
[James, J. T.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF, Houston, TX 77058 USA.
RP Mukhamedieva, LN (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia.
EM moukhamedieva@imbp.ru; john.t.james@nasa.gov
NR 23
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PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 249
EP 262
PG 14
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900008
ER
PT B
AU Novikova, ND
Pierson, DL
Poddubko, SV
Deshevaya, YA
Ott, CM
Castro, VA
Bruce, RJ
AF Novikova, N. D.
Pierson, D. L.
Poddubko, S. V.
Deshevaya, Ye. A.
Ott, C. M.
Castro, V. A.
Bruce, R. J.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Microbiology of the International Space Station
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
ID ASTRONAUTS; SPACEFLIGHT; REACTIVATION; BACTERIA; SYSTEM
C1 [Novikova, N. D.; Poddubko, S. V.; Deshevaya, Ye. A.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
[Bruce, R. J.] NASA, Lyndon B Johnson Space Ctr, Enterprise Advisory Serv Inc, Mail Code SF, Houston, TX 77058 USA.
[Pierson, D. L.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF2, Houston, TX 77058 USA.
RP Novikova, ND (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia.
EM novikova@imbp.ru; duane.l.pierson@nasa.gov; poddubko@imbp.ru;
charlie.m.ott@nasa.gov; victoria.a.castro@nasa.gov;
rebekah.j.bruce@nasa.gov
NR 51
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PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 263
EP 278
PG 16
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900009
ER
PT B
AU Petrov, VA
Cucinotta, FA
AF Petrov, V. A.
Cucinotta, F. A.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Radiation Safety of International Space Station Crews
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
ID GALACTIC COSMIC-RAYS; CHROMOSOME-ABERRATIONS; BLOOD-LYMPHOCYTES; CANCER;
PROTECTION; ASTRONAUTS; EQUIVALENT; DEPENDENCE; SPECTRA; RISK
C1 [Petrov, V. A.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
[Cucinotta, F. A.] NASA, Lyndon B Johnson Space Ctr, Mail Code SK, Houston, TX 77058 USA.
RP Petrov, VA (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia.
EM petrov@pike.net.ru; francis.a.cucinotta@nasa.gov
NR 44
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PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 279
EP 299
PG 21
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900010
ER
PT B
AU Skuratov, VM
Mudgett, PD
Bobe, LS
Andreichuk, PO
Schultz, JR
AF Skuratov, V. M.
Mudgett, P. D.
Bobe, L. S.
Andreichuk, P. O.
Schultz, J. R.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Water Supply on the International Space Station Station Water Supply
System and Operating Results November 2, 2000-April 20, 2007 (Increments
ISS-1-ISS-14)
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
C1 [Skuratov, V. M.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
[Bobe, L. S.] OAO Sci Res Inst KhimMash, Moscow 127015, Russia.
[Andreichuk, P. O.] Energiya Rocket Space Corp, Sci Prod Org, Korolev 141070, Moscovskaya Obl, Russia.
[Mudgett, P. D.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF2, Houston, TX 77058 USA.
[Schultz, J. R.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF, Houston, TX 77058 USA.
RP Skuratov, VM (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia.
EM paul.d.mudgett@nasa.gov; l_bobe@niichimmash.ru; john.r.schultz@nasa.gov
NR 16
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PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 301
EP 311
PG 11
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900011
ER
PT B
AU Agureev, AN
Kloeris, V
Zwart, SR
Smith, SM
AF Agureev, A. N.
Kloeris, V.
Zwart, S. R.
Smith, S. M.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Nutrition for International Space Station Crews
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
ID VITAMIN-K; FLIGHT; ASTRONAUTS; METABOLISM; MARKERS
C1 [Agureev, A. N.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
[Kloeris, V.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF3, Houston, TX 77058 USA.
[Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Mail Code SK3, Houston, TX 77058 USA.
[Zwart, S. R.] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Mail Code SK, Houston, TX 77058 USA.
RP Agureev, AN (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia.
EM aagureev@imbp.ru; vickie.l.kloeris@nasa.gov; sara.zwart-1@nasa.gov;
scott.m.smith@nasa.gov
NR 44
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PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 313
EP 324
PG 12
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900012
ER
PT B
AU Shumilina, GA
Villarreal, JD
AF Shumilina, G. A.
Villarreal, J. D.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Personal Hygiene for International Space Station Crewmembers
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
C1 [Villarreal, J. D.] NASA, Lyndon B Johnson Space Ctr, Mail Code EC1, Houston, TX 77058 USA.
EM jennifer.d.villarreal@nasa.gov
NR 20
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PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 325
EP 330
PG 6
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900013
ER
PT B
AU Bogomolov, VV
Duncan, JM
Sargsyan, AE
Pool, SL
AF Bogomolov, V. V.
Duncan, J. M.
Sargsyan, A. E.
Pool, S. L.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Medical Support for Crewmembers of the International Space Station
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
ID MIR; FLIGHT; SPACEFLIGHT; LONG; QUALIFICATION; MICROGRAVITY;
SHUTTLE/MIR; EXPERIENCES; PROGRAM; HEALTH
C1 [Bogomolov, V. V.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
[Duncan, J. M.] NASA, Lyndon B Johnson Space Ctr, Mail Code SD, Houston, TX 77058 USA.
[Sargsyan, A. E.] NASA, Lyndon B Johnson Space Ctr, Mail Code SD2, Houston, TX 77058 USA.
RP Bogomolov, VV (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia.
EM vvb@imbp.ru; james.m.duncan@nasa.gov; ashot.sargsyan-1@nasa.gov;
SLPool@earthlink.net
NR 59
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PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 331
EP 394
PG 64
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900014
ER
PT B
AU Grigoriev, AI
Potapov, AN
Jones, JA
Sullivan, TA
Scheuring, RA
AF Grigoriev, A. I.
Potapov, A. N.
Jones, J. A.
Sullivan, T. A.
Scheuring, R. A.
BE Sawin, CF
Hanson, SI
House, NG
Pestov, ID
TI Medical Support for Interplanetary Human Spaceflights
SO SPACE BIOLOGY AND MEDICINE, VOL 5: U.S. AND RUSSIAN COOPERATION IN SPACE
BIOLOGY AND MEDICINE
SE Library of Flight
LA English
DT Article; Book Chapter
ID INTERNATIONAL-SPACE-STATION; LONG-DURATION SPACEFLIGHT; MICROGRAVITY;
ASTRONAUTS; MISSION; RISK; COUNTERMEASURE; PARTICLES; RADIATION; ABOARD
C1 [Grigoriev, A. I.; Potapov, A. N.] Inst Biomed Problems, State Res Ctr, Moscow 123007, Russia.
[Jones, J. A.] NASA, Lyndon B Johnson Space Ctr, Mail Code SD2, Houston, TX 77058 USA.
[Sullivan, T. A.] NASA, Lyndon B Johnson Space Ctr, Mail Code SF, Houston, TX 77058 USA.
[Scheuring, R. A.] NASA, Lyndon B Johnson Space Ctr, Mail Code SD, Houston, TX 77058 USA.
RP Grigoriev, AI (reprint author), Inst Biomed Problems, State Res Ctr, 76A Khoroshevskoye Shosse, Moscow 123007, Russia.
EM grigoriev@imbp.ru; potapov@imbp.ru; jeffrey.a.jones@nasa.gov;
thomas.a.suilivan@nasa.gov; richard.a.scheuring@nasa.gov
NR 167
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PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-996-0
J9 LIBR FLIGHT
PY 2009
BP 395
EP 454
PG 60
WC Engineering, Aerospace; Biology; Medicine, Research & Experimental
SC Engineering; Life Sciences & Biomedicine - Other Topics; Research &
Experimental Medicine
GA BKU32
UT WOS:000269263900015
ER
PT B
AU Jones, SM
AF Jones, Steven M.
BE Denis, JH
Aldridge, PD
TI SPACE SCIENCE APPLICATIONS OF AEROGELS
SO SPACE EXPLORATION RESEARCH
SE Space Science Exploration and Policy
LA English
DT Article; Book Chapter
ID SOL-GEL PROCESS; SILICA AEROGEL; COMET 81P/WILD-2; IMPACT FEATURES;
STARDUST; DUST; IDENTIFICATION; CHEMISTRY
AB The unique physical properties of aerogels have provided enabling technologies to a variety of both flight and proposed space science missions. The extremely low values of the density and corresponding high values of the porosity of aerogels make them suitable for stopping high velocity particles, as highly efficient thermal barriers and as a porous medium for the containment of cryogenic fluids. The use of silica aerogel as a hypervelocity particle capture and return medium for the Stardust Mission, which launched in 1999 and returned to earth in 2006, has drawn the attention of the scientific community, as well as the public, to these fascinating materials. Aerogels are currently being used as the thermal insulation material in the 2003 Mars Exploration Rovers and will be used on the 2009 Mars Science Laboratory rover, as well. The SCIM (Sample Collection for the Investigation of Mars) and the STEP (Satellite Test of the Equivalence Principle) Missions are proposed scientific missions, in which the use of aerogel is critical to their overall design and success. Composite materials comprised of silica aerogel and oxide powders are currently under development for use in a new generation of thermoelectric devices that are planned for use in future mission designs. Work is ongoing in the development and production of non-silicate and composite aerogels to extend the range of useful physical properties, and thus, the applications of aerogels in future space science missions.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Jones, SM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Steven.M.Jones@jpl.nasa.gov
NR 43
TC 0
Z9 0
U1 0
U2 0
PU NOVA SCIENCE PUBLISHERS, INC
PI HAUPPAUGE
PA 400 OSER AVE, STE 1600, HAUPPAUGE, NY 11788-3635 USA
BN 978-1-60692-264-4
J9 SPACE SCI EXPLOR POL
PY 2009
BP 361
EP 384
PG 24
WC Engineering, Aerospace; Astronomy & Astrophysics
SC Engineering; Astronomy & Astrophysics
GA BNV31
UT WOS:000275662600014
ER
PT S
AU Bugby, D
Seghi, S
Kroliczek, E
Pauken, M
AF Bugby, D.
Seghi, S.
Kroliczek, E.
Pauken, M.
BE Robertson, GA
TI Novel Architecture for a Long-Life, Lightweight Venus Lander
SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 13th Conference on Thermophysics Applications in Microgravity/6th
Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on
Astrosociology
CY FEB 24-26, 2009
CL Huntsville, AL
SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst
DE Spacecraft; Venus; Lander; Long-Life; Lightweight; Thermal;
Architecture; Evaporation; Water; Insulation
AB This paper describes a novel concept for an extended lifetime, lightweight Venus lander. Historically, to operate in the 480 degrees C, 90 atm, corrosive, mostly CO2 Venus surface environment, previous landers have relied on thick Ti spherical outer shells and thick layers of internal insulation. But even the most resilient of these landers operated for only about 2 hours before succumbing to the environment. The goal on this project is to develop an architecture that extends lander lifetime to 20-25 hours and also reduces mass compared to the Pioneer Venus mission architecture. The idea for reducing mass is to: (a) contain the science instruments within a spherical high strength lightweight polymer matrix composite (PMC) tank; (b) surround the PMC tank with an annular shell of high performance insulation pre-pressurized to a level that (after landing) will exceed the external Venus surface pressure; and (c) surround the insulation with a thin Ti outer shell that contains only a net internal pressure, eliminating buckling overdesign mass. The combination of the PMC inner tank and thin Ti outer shell is lighter than a single thick Ti outer shell. The idea for extending lifetime is to add the following three features: (i) an expendable water supply that is placed within the insulation or is contained in an additional vessel within the PMC tank; (ii) a thin spherical evaporator shell placed within the insulation a short radial distance from the outer shell; and (iii) a thin heat-intercepting liquid cooled shield placed inboard of the evaporator shell. These features lower the temperature of the insulation below what it would have been with the insulation alone, reducing the internal heat leak and lengthening lifetime. The use of phase change materials (PCMs) inside the PMC tank is also analyzed as a lifetime-extending design option. The paper describes: (1) analytical modeling to demonstrate reduced mass and extended life; (2) thermal conductivity testing of high performance insulation as a function of temperature and pressure; (3) a bench-top ambient pressure thermal test of the evaporation system; and (4) a higher fidelity test, to be conducted in a high pressure, high temperature inert gas test chamber, of a small-scale Venus lander prototype (made from two hemispherical interconnecting halves) that includes all of the aforesaid features. 22 CFR 125.4(b)(13) applicable
C1 [Bugby, D.] ATK Space, 5050 Powder Mill Rd, Beltsville, MD 20705 USA.
[Seghi, S.] Ceram Compos Inc, Annapolis, MD 21401 USA.
[Kroliczek, E.] B & K Engn, Davidsonville, MD USA.
[Pauken, M.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Bugby, D (reprint author), ATK Space, 5050 Powder Mill Rd, Beltsville, MD 20705 USA.
EM david.bugby@atk.com
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0639-1
J9 AIP CONF PROC
PY 2009
VL 1103
BP 39
EP 50
PG 12
WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels
SC Engineering; Astronomy & Astrophysics; Energy & Fuels
GA BJG15
UT WOS:000265592900005
ER
PT S
AU Williams, GJ
Gilland, JH
AF Williams, George J., Jr.
Gilland, James H.
BE Robertson, GA
TI Propulsion Utilizing Laser-Driven Ponderomotive Fields for Deep-Space
Missions
SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 13th Conference on Thermophysics Applications in Microgravity/6th
Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on
Astrosociology
CY FEB 24-26, 2009
CL Huntsville, AL
SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst
DE Laser Propulsion; Ponderomotive; Interstellar Propulsion
AB The generation of large amplitude electric fields in plasmas by high-power lasers has been studied for several years in the context of high-energy particle acceleration. Fields on the order of GeV/m are generated in the plasma wake of the laser by non-linear ponderomotive forces. The laser fields generate longitudinal and translational electron plasma waves with phase velocities close to the speed of light. These fields and velocities offer the potential to revolutionize spacecraft propulsion, leading to extended deep space robotic probes. Based on these initial calculations, plasma acceleration by means of laser-induced ponderomotive forces appears to offer significant potential for spacecraft propulsion. Relatively high-efficiencies appear possible with proper beam conditioning, resulting in an order of magnitude more thrust than alternative concepts for high I(sp) (>10(5) s) and elimination of the primary life-limiting erosion phenomena associated with conventional electric propulsion systems. Ponderomotive propulsion readily lends itself to beamed power which might overcome some of the constraints of power-limited propulsion concepts. A preliminary assessment of the impact of these propulsion systems for several promising configurations on mission architectures has been conducted. Emphasizing interstellar and interstellar-precursor applications, performance and technical requirements are identified for a number of missions. The use of in-situ plasma and gas for propellant is evaluated as well.
C1 [Williams, George J., Jr.; Gilland, James H.] NASA, Ohio Aerosp Inst, GRCMS 16 1, Cleveland, OH 44135 USA.
RP Williams, GJ (reprint author), NASA, Ohio Aerosp Inst, GRCMS 16 1, Cleveland, OH 44135 USA.
EM George.J.Williams@nasa.gov; James.H.Gilland@nasa.gov
NR 22
TC 0
Z9 0
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0639-1
J9 AIP CONF PROC
PY 2009
VL 1103
BP 175
EP 184
PG 10
WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels
SC Engineering; Astronomy & Astrophysics; Energy & Fuels
GA BJG15
UT WOS:000265592900021
ER
PT S
AU Swanson, TD
AF Swanson, Theodore D.
BE Robertson, GA
TI Space Exploration and the Greenland Norse; A Comparative Study on the
Application of Technology for Exploration
SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 13th Conference on Thermophysics Applications in Microgravity/6th
Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on
Astrosociology
CY FEB 24-26, 2009
CL Huntsville, AL
SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst
DE Exploration; Space; Greenland Norse; Technology; Survival
AB During the mid to late Middle Ages a group of intrepid explorers from Scandinavia established two colonies in the harsh environment of Greenland. These people were known as the Greenland Norse. While their colonies made a determined effort and survived for about 500 years, they never really flourished and struggled just to survive in their harsh environment. Eventually they disappeared, despite the fact that a neighboring group, the Inuits, was successful in surviving into the modem era. Hence, while survival was very difficult due to a variety of factors, it was possible depending on how the society dealt with the environment. There are a number of interesting parallels between this Greenland Norse experiment and the modem era of space exploration. While comparisons from the past to present day plans must certainly be made with caution, there may be interesting lessons to learn. Specifically, the role of technology and innovation by the Greenland Norse is addressed in this comparative study.
C1 NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA.
RP Swanson, TD (reprint author), NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA.
EM Theodore.D.Swanson@nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0639-1
J9 AIP CONF PROC
PY 2009
VL 1103
BP 407
EP 413
PG 7
WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels
SC Engineering; Astronomy & Astrophysics; Energy & Fuels
GA BJG15
UT WOS:000265592900049
ER
PT S
AU Clark, PE
Millar, PS
Beaman, B
Choi, M
Cooper, L
Feng, S
King, R
Leshin, L
Lewis, R
Yeh, PS
Young, E
Lorenz, J
AF Clark, P. E.
Millar, P. S.
Beaman, B.
Choi, M.
Cooper, L.
Feng, S.
King, R.
Leshin, L.
Lewis, R.
Yeh, P. S.
Young, E.
Lorenz, J.
BE Robertson, GA
TI Enabling Technology for Lunar Surface Science
SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 13th Conference on Thermophysics Applications in Microgravity/6th
Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on
Astrosociology
CY FEB 24-26, 2009
CL Huntsville, AL
SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst
DE Moon; Lunar Surface; Instrumentation; Space Physics; Space Environment;
Space Radiation; Atmosphere; Magnetic Field; Plasma; Dust; Geophysics;
Interior; Heat Flow; Seismometry; Astrophysics
AB Implementation of Lunar Exploration Initiative goals will require deployment of science packages at sites with the appropriate vantage point for obtaining the desired measurements and remote from potential (human) sources of contamination, thus requiring stand alone operation. Chief instruments/instrument package candidates include those which could provide long-term monitoring of the surface and subsurface environments for fundamental lunar science and crew safety. The major challenge such packages face will be operating during long periods of darkness in extreme cold potentially without the Pu238 based power and thermal systems available to Apollo era packages (ALSEP). The initial attempt to design a 10 instrument environmental monitoring package with a solar/battery based power system led to a package with a unacceptably large mass (500 kg) of which over half was battery mass. We achieved considerable reduction in this mass, first through the introduction of high performance electronics capable of operating at far lower temperature, reducing the initial mass estimate by a factor of 2, and then through the use of innovative thermal balance strategies involving the use of multi-layer thin materials and gravity-assisted heat pipes, reducing the initial mass estimate by a factor of 5. Yet to be implemented are strategies involving the universal incorporation of ULT/ULP (Ultra Low Temperature/Ultra Low Power) digital and analog electronics, distributed or non-conventionally packaged power systems, and state of the art solar power technology. These strategies will be required to meet the far more challenging thermal requirements of operating through a normal 28 day diurnal cycle. Limited battery survival temperature range remains the largest obstacle.
C1 [Clark, P. E.; Millar, P. S.; Beaman, B.; Choi, M.; Cooper, L.; Feng, S.; King, R.; Leshin, L.; Lewis, R.; Yeh, P. S.; Young, E.; Lorenz, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Clark, PE (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD USA.
EM 301-286-7457.pamela.e.clark@nasa.gov; john.e.lorenz@nasa.gov
RI Millar, Pamela/B-4426-2013
NR 12
TC 0
Z9 0
U1 0
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0639-1
J9 AIP CONF PROC
PY 2009
VL 1103
BP 599
EP 607
PG 9
WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels
SC Engineering; Astronomy & Astrophysics; Energy & Fuels
GA BJG15
UT WOS:000265592900071
ER
PT S
AU Clark, PE
Curtis, SA
Minetto, F
Cheung, CY
Keller, JF
Moore, M
Calle, CI
AF Clark, P. E.
Curtis, S. A.
Minetto, F.
Cheung, C. Y.
Keller, J. F.
Moore, M.
Calle, C. I.
BE Robertson, GA
TI SPARCLE: Electrostatic Tool for Lunar Dust Control
SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 13th Conference on Thermophysics Applications in Microgravity/6th
Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on
Astrosociology
CY FEB 24-26, 2009
CL Huntsville, AL
SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst
DE Lunar Surface; Dust Control; Sampling; Electrostatic; Mechanical;
Exploration
ID SPACECRAFT; SURFACE; WAKE
AB Successful exploration of most planetary surfaces, with their impact-generated dusty regoliths, will depend on the capabilities to keep surfaces free of the dust which could compromise performance and to collect dust for characterization. Solving the dust problem is essential before we return to the Moon. During the Apollo missions, the discovery was made that regolith fines, or dust, behaved like abrasive velcro, coating surfaces, clogging mechanisms, and making movement progressively more difficult as it was mechanically stirred up during surface operations, and abrading surfaces, including spacesuits, when attempts were made to remove it manually. In addition, some of the astronauts experienced breathing difficulties when exposed to dust that got into the crew compartment. The successful strategy will deal with dust dynamics resulting from interaction between mechanical and electrostatic forces. Here we will describe the surface properties of dust particles, the basis for their behavior, and an electrostatically-based approach and methodology for addressing this issue confirmed by our preliminary results. Our device concept utilizes a focused electron beam to control the electrostatic potential of the surface. A plate of the opposite potential is then used to induce dust migration in the presence of an electrical field. Our goal is a compact device of < 5 kg mass and using <5 watts of power to be operational in <5 years with heritage from ionic sweepers for active spacecraft potential control (e.g., on POLAR). Rovers could be fitted with devices that could harness the removal of dust for sampling as part of the extended exploration process on Mercury, Mars, asteroids or outer solar system satellites, as well as the Moon.
C1 [Clark, P. E.] Catholic Univ Amer, Washington, DC 20064 USA.
[Clark, P. E.; Curtis, S. A.; Minetto, F.; Keller, J. F.; Moore, M.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Calle, C. I.] NASA KSC, Code KT E, FL-32899 Cape Kennedy, Florida.
RP Clark, PE (reprint author), Catholic Univ Amer, Washington, DC 20064 USA.
EM pamela.clark@gsfc.nasa.gov
RI Keller, John/I-5097-2013
FU NASA ESMD ETDP; NASA/KSC; NASA/GSDC IRAD; GSFC [695, 588]
FX We would like to acknowledge the important discussion pertaining to this
work we have had with our collegues William Farrell, David Carrier and
Otto Berg. We thank NASA ESMD ETDP, NASA/KSC, NASA/GSDC IRAD, GSFC Codes
695, and 588 for their support.
NR 30
TC 1
Z9 1
U1 0
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0639-1
J9 AIP CONF PROC
PY 2009
VL 1103
BP 608
EP 614
PG 7
WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels
SC Engineering; Astronomy & Astrophysics; Energy & Fuels
GA BJG15
UT WOS:000265592900072
ER
PT S
AU Howard, RT
Bryan, TC
AF Howard, Richard T.
Bryan, Thomas C.
BE Robertson, GA
TI The Next Generation Advanced Video Guidance Sensor: Flight Heritage and
Current Development
SO SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM SPESIF-2009
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 13th Conference on Thermophysics Applications in Microgravity/6th
Symposium on New Frontiers in Space Propulsion Sciences/1st Symposium on
Astrosociology
CY FEB 24-26, 2009
CL Huntsville, AL
SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Astrosociol Res Inst
DE Sensors; Docking; Automated; Proximity Operations; Relative Navigation;
Rendezvous; Video
AB The Next Generation Advanced Video Guidance Sensor (NGAVGS) is the latest in a line of sensors that have flown four times in the last 10 years. The NGAVGS has been under development for the last two years as a long-range proximity operations and docking sensor for use in an Automated Rendezvous and Docking (AR&D) system. The first autonomous rendezvous and docking in the history of the U.S. Space Program was successfully accomplished by Orbital Express, using the Advanced Video Guidance Sensor (AVGS) as the primary docking sensor. That flight proved that the United States now has a mature and flight proven sensor technology for supporting Crew Exploration Vehicles (CEV) and Commercial Orbital Transport Systems (COTS) Automated Rendezvous and Docking (AR&D). NASA video sensors have worked well in the past: the AVGS used on the Demonstration of Autonomous Rendezvous Technology (DART) mission operated successfully in "spot mode" out to 2 km, and the first generation rendezvous and docking sensor, the Video Guidance Sensor (VGS), was developed and successfully flown on Space Shuttle flights in 1997 and 1998.
This paper presents the flight heritage and results of the sensor technology, some hardware trades for the current sensor, and discusses the needs of future vehicles that may rendezvous and dock with the International Space Station (ISS) and other Constellation vehicles. It also discusses approaches for upgrading AVGS to address parts obsolescence, and concepts for minimizing the sensor footprint, weight, and power requirements. In addition, the testing of the various NGAVGS development units will be discussed along with the use of the NGAVGS as a proximity operations and docking sensor.
C1 [Howard, Richard T.; Bryan, Thomas C.] NASA, Automated Rendezvous & Docking Dev & Test Branch, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Howard, RT (reprint author), NASA, Automated Rendezvous & Docking Dev & Test Branch, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM ricky.howard@nasa.gov
NR 1
TC 0
Z9 0
U1 1
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0639-1
J9 AIP CONF PROC
PY 2009
VL 1103
BP 615
EP 621
PG 7
WC Engineering, Aerospace; Astronomy & Astrophysics; Energy & Fuels
SC Engineering; Astronomy & Astrophysics; Energy & Fuels
GA BJG15
UT WOS:000265592900073
ER
PT S
AU Broschart, SB
Villac, BF
AF Broschart, Stephen B.
Villac, Benjamin F.
BE Segerman, AM
Lai, PC
Wilkins, MP
Pittelkau, ME
TI IDENTIFICATION OF NON-CHAOTIC TERMINATOR ORBITS NEAR 6489 GOLEVKA
SO SPACEFLIGHT MECHANICS 2009, VOL 134, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA 19th Space Flight Mechanics Meeting
CY FEB 08-12, 2009
CL Savannah, GA
SP AAS, AIAA
ID RADIATION PRESSURE; SATELLITE DYNAMICS; SOLAR-RADIATION; 2-BODY PROBLEM;
STABILITY; ASTEROIDS; PARTICLES; MOTION
AB Terminator orbits are an attractive class of quasi-periodic orbits for missions to small bodies because they exhibit stable behavior in the presence of a strong solar radiation pressure perturbation and robustness against uncertainty in the gravitational environment. Here, a numerical procedure is demonstrated for extracting long-term stability characteristics of terminator orbit dynamics. This approach yields a quantitative description of the region in state space that results in long-term stable terminator orbit dynamics in a high-fidelity dynamical model. These body-specific results complement the more generalized analytical results by providing more detail on the orbit stability properties in a particular situation of interest and stability information when the implicit assumptions of the analytical results do not apply.
The procedure first identifies periodic orbits in the augmented Hill problem numerically, then evaluates the long-term behavior of nearby initial conditions using the Fast Lyapunov Indicator of chaoticity in a high-fidelity dynamical model that includes solar radiation pressure, an elliptical heliocentric small-body orbit, and a irregular rotating small-body gravity field. The procedure is successfully demonstrated on a model of the asteroid 6489 Golevka and results are compared with existing analytical results. This approach also has application to the study of orbiting particles and moons.
C1 [Broschart, Stephen B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Broschart, SB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-150, Pasadena, CA 91109 USA.
EM Stephen.B.Broschart@ipl.nasa.gov; bvillac@uci.edu
NR 28
TC 4
Z9 4
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-554-1
J9 ADV ASTRONAUT SCI
PY 2009
VL 134
BP 861
EP 880
PN I-III
PG 20
WC Engineering, Aerospace
SC Engineering
GA BOE66
UT WOS:000276394400052
ER
PT S
AU Pelletier, FJ
Antreasian, PG
Ardalan, SM
Criddle, KE
Ionasescu, R
Jacobson, RA
Jones, JB
Parcher, DW
Roth, DC
Thompson, PF
AF Pelletier, Frederic J.
Antreasian, Peter G.
Ardalan, Shadan M.
Criddle, Kevin E.
Ionasescu, Rodica
Jacobson, Robert A.
Jones, Jeremy B.
Parcher, Daniel W.
Roth, Duane C.
Thompson, Paul F.
BE Segerman, AM
Lai, PC
Wilkins, MP
Pittelkau, ME
TI FLYING BY TITAN
SO SPACEFLIGHT MECHANICS 2009, VOL 134, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA 19th Space Flight Mechanics Meeting
CY FEB 08-12, 2009
CL Savannah, GA
SP AAS, AIAA
AB The Cassini spacecraft encounters the massive Titan about once every month. These encounters are essential to the mission as Titan is the only satellite of Saturn that can provide enough gravity assist to shape the orbit tour, which will allow outstanding science for many years. From a navigation point of view, these encounters provide many challenges. In particular, those that fly close enough to the surface for the atmospheric drag to perturb the orbit. This paper discusses the dynamic models developed to successfully navigate Cassini and determine its trajectory. This includes the moon's gravity pull with its second degree zonal harmonics, J(2), the attitude control perturbations and the acceleration of drag.
C1 [Pelletier, Frederic J.; Antreasian, Peter G.; Ardalan, Shadan M.; Criddle, Kevin E.; Ionasescu, Rodica; Jacobson, Robert A.; Jones, Jeremy B.; Parcher, Daniel W.; Roth, Duane C.; Thompson, Paul F.] CALTECH, Jet Prop Lab, Guidance Nav & Control Sect, Pasadena, CA 91109 USA.
RP Pelletier, FJ (reprint author), CALTECH, Jet Prop Lab, Guidance Nav & Control Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 14
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-554-1
J9 ADV ASTRONAUT SCI
PY 2009
VL 134
BP 1457
EP 1471
PN I-III
PG 15
WC Engineering, Aerospace
SC Engineering
GA BOE66
UT WOS:000276394400088
ER
PT S
AU Williams, PN
Ballard, CG
Gist, EM
Goodson, TD
Hahn, Y
Stumpf, PW
Wagner, SV
AF Williams, Powtawche N.
Ballard, Christopher G.
Gist, Emily M.
Goodson, Troy D.
Hahn, Yungsun
Stumpf, Paul W.
Wagner, Sean V.
BE Segerman, AM
Lai, PC
Wilkins, MP
Pittelkau, ME
TI FLIGHT PATH CONTROL DESIGN FOR THE CASSINI EQUINOX MISSION
SO SPACEFLIGHT MECHANICS 2009, VOL 134, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA 19th Space Flight Mechanics Meeting
CY FEB 08-12, 2009
CL Savannah, GA
SP AAS, AIAA
AB The Cassini-Huygens spacecraft has successfully completed its four-year Prime Mission and began a two-year extended mission on July 1, 2008. Officially named the "Equinox Mission", the extended mission includes 95 orbit trim maneuvers designed to achieve flybys of Titan, Enceladus, Rhea, and Dione. This paper gives an overview of maneuver statistical predictions and analysis for the Equinox Mission.
C1 [Williams, Powtawche N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Williams, PN (reprint author), CALTECH, Jet Prop Lab, Mail Stop 230-205,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Powtawche.N.Williams@jpl.nasa.gov
NR 15
TC 0
Z9 0
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-554-1
J9 ADV ASTRONAUT SCI
PY 2009
VL 134
BP 1851
EP 1865
PN I-III
PG 15
WC Engineering, Aerospace
SC Engineering
GA BOE66
UT WOS:000276394400111
ER
PT B
AU Wyatt, J
Burleigh, S
Jones, R
Torgerson, L
Wissler, S
AF Wyatt, Jay
Burleigh, Scott
Jones, Ross
Torgerson, Leigh
Wissler, Steve
GP IEEE
TI Disruption Tolerant Networking Flight Validation Experiment on NASA's
EPOXI Mission
SO SPACOMN: 2009 FIRST INTERNATIONAL CONFERENCE ON ADVANCES IN SATELLITE
AND SPACE COMMUNICATIONS
LA English
DT Proceedings Paper
CT 1st International Conference on Advances in Satellite and Space
Communications
CY JUL 20-25, 2009
CL Colmar, FRANCE
DE DTN; EPOXI; networking; protocols
AB In October and November of 2008, the Jet Propulsion Laboratory installed and tested essential elements of Delay/Disruption Tolerant Networking (DTN) technology on the Deep Impact spacecraft. This experiment, called Deep Impact Network Experiment (DINET), was performed in close cooperation with the EPOXI project which has responsibility for the spacecraft. During DINET some 300 images were transmitted from the JPL nodes to the spacecraft. Then they were automatically forwarded from the spacecraft back to the JPL nodes, exercising DTN's bundle origination, transmission, acquisition, dynamic route computation, congestion control, prioritization, custody transfer, and automatic retransmission procedures, both on the spacecraft and on the ground, over a period of 27 days. All transmitted bundles were successfully received, without corruption. The DINET experiment demonstrated DTN readiness for operational use in space missions. This activity was part of a larger NASA space DTN development program to mature DTN to flight readiness for a wide variety of mission types by the end of 2011. This paper describes the DTN protocols, the flight demo implementation, validation metrics which were created for the experiment, and validation results.
C1 [Wyatt, Jay; Burleigh, Scott; Jones, Ross; Torgerson, Leigh; Wissler, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wyatt, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM E.Jay.Wyatt@jpl.nasa.gov; Scott.C.Burleigh@jpl.nasa.gov;
Ross.M.Jones@jpl.nasa.gov; Jordan.L.Torgerson@jpl.nasa.gov;
Steven.S.Wissler@jpl.nasa.gov
NR 5
TC 11
Z9 11
U1 0
U2 2
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4244-4426-7
PY 2009
BP 187
EP 196
DI 10.1109/SPACOMM.2009.39
PG 10
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA BOZ33
UT WOS:000278100200033
ER
PT S
AU Cohn, SE
AF Cohn, Stephen E.
BE Temam, RM
Tribbia, JJ
TI Energetic Consistency and Coupling of the Mean and Covariance Dynamics
SO SPECIAL VOLUME: COMPUTATIONAL METHODS FOR THE ATMOSPHERE AND THE OCEANS
SE Handbook of Numerical Analysis
LA English
DT Article; Book Chapter
ID ADJOINT VORTICITY EQUATION; VARIATIONAL ASSIMILATION; METEOROLOGICAL
OBSERVATIONS; TRANSPORT SCHEMES; PREDICTION; CIRCULATION; MODEL
C1 NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Cohn, SE (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
NR 17
TC 2
Z9 2
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1570-8659
BN 978-0-08-093103-6
J9 HANDB NUM ANAL
PY 2009
VL 14
BP 443
EP 478
DI 10.1016/S1570-8659(08)00210-x
PG 36
WC Mathematics
SC Mathematics
GA BCT26
UT WOS:000311344600012
ER
PT J
AU Enya, K
Kotani, T
Nakagawa, T
Kataza, H
Haze, K
Higuchi, S
Miyata, T
Sako, S
Nakamura, T
Yamashita, T
Narita, N
Tamura, M
Nishikawa, J
Hayano, H
Oya, S
Itoh, Y
Fukagawa, M
Shibai, H
Honda, M
Baba, N
Murakami, N
Takami, M
Matsuo, T
Ida, S
Abe, L
Guyon, O
Venet, M
Yamamuro, T
Bierden, P
AF Enya, K.
Kotani, T.
Nakagawa, T.
Kataza, H.
Haze, K.
Higuchi, S.
Miyata, T.
Sako, S.
Nakamura, T.
Yamashita, T.
Narita, N.
Tamura, M.
Nishikawa, J.
Hayano, H.
Oya, S.
Itoh, Y.
Fukagawa, M.
Shibai, H.
Honda, M.
Baba, N.
Murakami, N.
Takami, M.
Matsuo, T.
Ida, S.
Abe, L.
Guyon, O.
Venet, M.
Yamamuro, T.
Bierden, P.
CA SPICA Coronagraph Team
BE Heras, AM
swinyard, BM
Isaak, KG
Goicoechea, JR
TI SPICA CORONAGRAPH INSTRUMENT (SCI) FOR THE DIRECT IMAGING AND
SPECTROSCOPY OF EXO-PLANETS
SO SPICA JOINT EUROPEAN/JAPANESE WORKSHOP
LA English
DT Proceedings Paper
CT Joint European/Japanese Workshop on Space Infrared Telescope for
Cosmology and Astrophysics
CY JUL 06-08, 2009
CL Oxford, ENGLAND
SP Daiwa Anglo-Japanese Fdn, Great Britain SASAKAWA Fdn
DE SPICA; coronagraph; instrument; exo-planet; transit; spectroscopy
ID STAR
AB We present the SPICA Coronagraph Instrument (SCI) for the direct imaging and spectroscopy of exo-planets. The SPICA mission gives us a unique opportunity for high-contrast observations because of the large telescope aperture, the simple pupil shape, and the capability for infrared observations from space. The primary target of SCI is Jovian exo-planets. Using the spectroscopy mode of SCI, we will try the detection and the characterization of mid-infrared line features of the atmosphere of exo-planets. The specifications, performance and the design of the instrument are shown. The main wavelengths and the contrast required for the observations are 3.5-27 mu m, and 10(-6), respectively. We also show the progress of the development of key technology to realize SCI. Laboratory demonstration of the principle of coronagraph, realistic design and fabrication of masks, and the development of cryogenic active optics have been carried out, or are successfully ongoing. We are preparing a cryogenic chamber for the tests of the whole infrared coronagraph. A potentially important by-product of the instrument, transit monitoring for characterization of exo-planets, is also described. We expect that SCI will provide drastic progress in the understanding of various planetary systems and will be a unique capability in the SPICA era.
C1 [Enya, K.; Kotani, T.; Nakagawa, T.; Kataza, H.; Haze, K.; Higuchi, S.] ISAS JAXA, 3-1-1 Yoshinodai, Kanagawa 2298510, Japan.
[Haze, K.] Grad Univ Adv Studies, Dept Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Higuchi, S.] Univ Tokyo, Grad Sch Sci, Dept Phys, Tokyo 1130033, Japan.
[Miyata, T.; Sako, S.; Nakamura, T.] Univ Tokyo, Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan.
[Yamashita, T.; Narita, N.; Tamura, M.; Nishikawa, J.; Hayano, H.; Oya, S.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Itoh, Y.] Kobe Univ, Grad Sch Sci, Kobe, Hyogo 6578501, Japan.
[Fukagawa, M.; Shibai, H.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Honda, M.] Kanagawa Univ, Dept Informat Sci, Hiratsuka, Kanagawa 2591293, Japan.
[Baba, N.; Murakami, N.] Hokkaido Univ, Div Appl Sci, Sapporo, Hokkaido 0608628, Japan.
[Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan.
[Matsuo, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ida, S.] Tokyo Inst Technol, Dept Earth & Space Sci, Tokyo 1528551, Japan.
[Abe, L.] Univ Nice, CNRS, Lab AH Fizeau, F-06108 Nice, France.
[Guyon, O.] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Venet, M.] Observ Astron Marseille Provence, F-13388 Marseille, France.
[Yamamuro, T.; Bierden, P.] Optcraft Corp, Sagamihara, Kanagawa 2291104, Japan.
[SPICA Coronagraph Team] Boston Micromachines Corp, Cambridge, MA 02138 USA.
RP Enya, K (reprint author), ISAS JAXA, 3-1-1 Yoshinodai, Kanagawa 2298510, Japan.
NR 11
TC 0
Z9 0
U1 1
U2 1
PU E D P SCIENCES
PI CEDEX A
PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A,
FRANCE
BN 978-2-7598-0493-1
PY 2009
AR UNSP 01004
DI 10.1051/spica/200901004
PG 6
WC Astronomy & Astrophysics; Instruments & Instrumentation
SC Astronomy & Astrophysics; Instruments & Instrumentation
GA BUU69
UT WOS:000290389800004
ER
PT S
AU Nixon, DD
Johnson, CD
AF Nixon, D. D.
Johnson, C. D.
GP IEEE
TI Numerical Evaluation of the "Dual-Kernel, Counter-flow" Matric
Convolution Integral that Arises in Discrete/Continuous (D/C) Control
Theory
SO SSST: 2009 41ST SOUTHEASTERN SYMPOSIUM ON SYSTEM THEORY
SE Southeastern Symposium on System Theory
LA English
DT Proceedings Paper
CT 41st Southeastern Symposium on System Theory
CY MAR 15-17, 2009
CL Tullahoma, TN
AB Discrete/Continuous (D/C) control theory is a new generalized theory of discrete-time control that expands the concept of conventional (exact) discrete-time control so that actuator commands need not be constant between control decisions, but can be more generally defined and implemented as functions that vary with time across each sample period in some beneficial manner. Because the plant/control system construct contains two linear subsystems arranged in tandem, a novel "dual-kernel counter-flow" convolution integral appears in the formulation; and, as part of the D/C control design and implementation process, numerical evaluation of that integral over each sample period is required. Three fundamentally different evaluation methods and associated algorithms are derived for the constant-coefficient case, and numerical results are matched against three available examples that have closed-form solutions.
C1 [Nixon, D. D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Johnson, C. D.] Univ Alabama, Elect & Comp Engn, Huntsville, AL 35899 USA.
RP Nixon, DD (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM douglas.d.nixon@nasa.gov; johnson@ece.uah.edu
NR 9
TC 1
Z9 1
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0094-2898
BN 978-1-4244-3324-7
J9 SE SYM SYS THRY
PY 2009
BP 285
EP +
PG 2
WC Computer Science, Artificial Intelligence; Computer Science, Hardware &
Architecture; Computer Science, Theory & Methods; Robotics
SC Computer Science; Robotics
GA BKN37
UT WOS:000268672400057
ER
PT S
AU Hannan, MR
Johnson, CD
AF Hannan, Michael R.
Johnson, C. D.
GP IEEE
TI Simulation and Animation of Coffee Sloshing in a Cup; A Testbed for
Control Design
SO SSST: 2009 41ST SOUTHEASTERN SYMPOSIUM ON SYSTEM THEORY
SE Southeastern Symposium on System Theory
LA English
DT Proceedings Paper
CT 41st Southeastern Symposium on System Theory
CY MAR 15-17, 2009
CL Tullahoma, TN
DE Dual-Mode Control; Disturbance-Observer; Disturbance-Accommodation;
Animation; GUI; LQR; Controls Education; Simulink
AB This paper describes a software tool useful for gaining insight into the trade-offs encountered in any control system design and to the benefits of a dual-mode control when needed The plant is a relatively simple two body problem (two masses coupled with a spring & damper). A GUI interfaces with a Simulink (R) model of the plant and two control options. The GUI makes it possible to switch controllers as the simulation is running and illustrates the trade-offs between performance (output tracking) and control energy management. The dynamics are presented in the form of coffee sloshing in a cup to give the user a familiar physical interpretation.
C1 [Hannan, Michael R.] NASA MSFC, Huntsville, AL 35811 USA.
[Johnson, C. D.] Univ Alabama, ECE Dept, Huntsville, AL USA.
RP Hannan, MR (reprint author), NASA MSFC, Huntsville, AL 35811 USA.
NR 5
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0094-2898
BN 978-1-4244-3324-7
J9 SE SYM SYS THRY
PY 2009
BP 317
EP +
DI 10.1109/SSST.2009.4806826
PG 2
WC Computer Science, Artificial Intelligence; Computer Science, Hardware &
Architecture; Computer Science, Theory & Methods; Robotics
SC Computer Science; Robotics
GA BKN37
UT WOS:000268672400063
ER
PT S
AU Creech-Eakman, MJ
Hora, J
Ivezic, Z
Jurgenson, C
Luttermoser, D
Marengo, M
Speck, A
Stencel, R
Thompson, RR
AF Creech-Eakman, M. J.
Hora, J.
Ivezic, Z.
Jurgenson, C.
Luttermoser, D.
Marengo, M.
Speck, A.
Stencel, R.
Thompson, R. R.
BE Guzik, JA
Bradley, PA
TI Multiwavelength Study of Pulsation and Dust Production in Mira Variables
Using Optical Interferometry for Constraints
SO STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT International Conference on Stellar Pulsation - Challenges for Theory
and Observation
CY MAY 31-JUN 05, 2009
CL Santa Fe, NM
SP Los Alamos Natl Lab, Ctr Space Sci & Explorat, Inst Geophys & Planetary Phys, TAE Photo & Design, La Fonda Plaza
DE mira variables; dust production; infrared spectroscopy; optical/infrared
interferometry; facility: Spitzer Space Telescope facility: Palomar
Testbed Interferometer
ID TIME-VARIATION; STARS
AB Optical interferometry is a technique by which the diameters and indeed the direct pulsations of stars are routinely being measured. As a follow-on to a 7 year interferometric campaign to measure the pulsations of over 100 mira variables, our team has been using the Spitzer Space Telescope to obtain 95 mid-infrared spectra of 25 miras during their pulsations over one year while simultaneously ascertaining their near-infrared diameters using the Palomar Testbed Interferometer. These data will then be combined with modeling from NLTE and radiative transfer codes to place hard constraints on our understanding of these stars and their circumstellar environments. We present some initial results from this work and discuss the next steps toward fully characterizing the atmosphere, molecular photosphere and dust production in mira variables.
C1 [Creech-Eakman, M. J.] New Mexico Inst Min & Technol, Dept Phys, 801 Leroy Pl, Socorro, NM 87801 USA.
[Creech-Eakman, M. J.; Jurgenson, C.] Magdalena Ridge Observ Interferometer, Socorro, NM 87801 USA.
[Hora, J.; Marengo, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ivezic, Z.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Luttermoser, D.] East Tennessee State Univ, Dept Phys, Johnson City, TN 37614 USA.
[Marengo, M.] Iowa State Univ, Dept Phys, Ames, IA 50011 USA.
[Speck, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[Stencel, R.] Univ Denver, Dept Phys & Astrophys, Denver, CO 80208 USA.
[Thompson, R. R.] NASA, Opt Sci Corp, SOFIA Project, Dryden Aircraft Operat Fac, Palmdal, CA 93550 USA.
RP Creech-Eakman, MJ (reprint author), New Mexico Inst Min & Technol, Dept Phys, 801 Leroy Pl, Socorro, NM 87801 USA.
OI Hora, Joseph/0000-0002-5599-4650
FU NASA grant to the PI and team associated with Spitzer program [GO50717]
FX Some of the work on this project was supported through a NASA grant to
the PI and team associated with Spitzer program GO50717.
NR 14
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA
SN 0094-243X
BN 978-0-7354-0707-7
J9 AIP CONF PROC
PY 2009
VL 1170
BP 137
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BPW04
UT WOS:000280126200030
ER
PT J
AU Kaul, UK
AF Kaul, Upender K.
TI Modeling and Simulation of Normal and Damage Vibration Signatures of
Idealized Gears
SO STRUCTURAL HEALTH MONITORING-AN INTERNATIONAL JOURNAL
LA English
DT Article
DE wave-based structural health monitoring; damage vibration signatures;
finite-difference modeling; elastodynamic partial differential equations
ID WAVE PROPAGATION; MEDIA
AB A physics-based first principles approach is adopted in this study to simulate vibration signatures from an idealized gear such as a thin spur gear under plane dynamic stresses induced by an impulsive rotation. The governing equations of velocity-stress are solved using a finite-difference formulation in generalized curvilinear coordinates and a fully characteristic set of boundary conditions based on the theory of hyperbolic systems. The vibration signatures are thus directly obtained in the time domain. A second-order accurate in time and space, time-staggered leapfrog scheme, is used to integrate the time-dependent partial differential equations. Normal as well as damage signatures are obtained and compared; normal signatures correspond to uniform material properties of the gear, and damage signatures correspond to one of the gear teeth being made less rigid in a certain fashion so as to mimic a damage such as due to impact-induced pitting, deformation or incipient crack formation. It is observed that significant deviations from the normal signature occur in amplitude due to this seeded damage. Using this approach, baseline or reference vibration signatures can be obtained for any structural subsystem to aid in its health monitoring.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kaul, UK (reprint author), NASA, Ames Res Ctr, MS 258-5, Moffett Field, CA 94035 USA.
EM Upender.K.Kaul@nasa.gov
FU NASA Computing, Information and Communications Technology (CICT) Program
FX This work was supported by the NASA Computing, Information and
Communications Technology (CICT) Program.
NR 17
TC 2
Z9 2
U1 0
U2 1
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1475-9217
J9 STRUCT HEALTH MONIT
JI Struct. Health Monit.
PD JAN
PY 2009
VL 8
IS 1
BP 17
EP 28
DI 10.1177/1475921708094791
PG 12
WC Engineering, Multidisciplinary; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 398XB
UT WOS:000262763700002
ER
PT J
AU Crespo, LG
Giesy, DP
Kenny, SP
AF Crespo, Luis G.
Giesy, Daniel P.
Kenny, Sean P.
TI Reliability-based analysis and design via failure domain bounding
SO STRUCTURAL SAFETY
LA English
DT Article
DE Reliability; Bounds; Failure probability; Optimization
ID ALGORITHM; SYSTEMS
AB This paper proposes a methodology for bounding and approximating failure probabilities for systems with parametric uncertainty that are subject to multiple design requirements. The two fundamental developments in this work are (1) a method to explicitly compute upper bounds on failure probability based on solving an optimization problem, and (2) a hybrid method, utilizing the upper bounds together with conditional sampling, to achieve highly accurate estimates of failure probabilities. The computation of failure probability bounds is accomplished by the deformation of hyper-spherical or hyper-rectangular sets in the standard normal space and utilizes a combination of numerical optimization and analytic tools. The methods for calculating these bounds are applicable to systems having multiple limit state functions and are not subject to difficulties when there are multiple critical parameter points. Numerical experiments are presented to demonstrate that the gains in accuracy and efficiency of the method are considerable when compared to alternative methods. The tools proposed are especially suited for design optimization due to their efficiency and the resulting continuity of the upper bounds. Since only standard optimization algorithms are required for implementation, these strategies are easily applicable to a variety of complex engineering problems. Published by Elsevier Ltd.
C1 [Crespo, Luis G.] Natl Inst Aerospace, Hampton, VA 23666 USA.
[Giesy, Daniel P.; Kenny, Sean P.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Crespo, LG (reprint author), Natl Inst Aerospace, 100 Explorat Way, Hampton, VA 23666 USA.
EM lgcrespo@nianet.org; daniel.p.giesy@nasa.gov; sean.p.kenny@nasa.gov
NR 24
TC 7
Z9 7
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-4730
J9 STRUCT SAF
JI Struct. Saf.
PY 2009
VL 31
IS 4
BP 306
EP 315
DI 10.1016/j.strusafe.2008.09.001
PG 10
WC Engineering, Civil
SC Engineering
GA 448IG
UT WOS:000266255700005
ER
PT B
AU Lis, DC
Goldsmith, PF
Bergin, EA
Falgarone, E
Gerin, M
Roueff, E
AF Lis, Dariusz C.
Goldsmith, Paul F.
Bergin, Edwin A.
Falgarone, Edith
Gerin, Maryvonne
Roueff, Evelyne
BE Lis, DC
Vaillancourt, JE
Goldsmith, PF
Bell, TA
Scoville, NZ
Zmuidzinas, J
TI Hydrides in Space: Past, Present, and Future
SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS
G. PHILLIPS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Symposium on Submillimeter Astrophysics and Technology held in honor of
Thomas G Philllips
CY FEB 23-24, 2009
CL Calif Inst Technol, Pasadena, CA
HO Calif Inst Technol
ID O1 HALE-BOPP; DENSE INTERSTELLAR CLOUDS; 1996 B2 HYAKUTAKE; PRESTELLAR
CORES; DEUTERIUM FRACTIONATION; PHYSICAL CONDITIONS; DEUTERATED AMMONIA;
HYDROGEN-CHLORIDE; STARLESS CORES; CO DEPLETION
AB One of the central questions of modern astrophysics concerns the life cycle of molecules in the Universe-from the diffuse interstellar medium to planetary systems-and the chemical pathways leading from simple atoms and diatomic molecules to complex organic species. In the past two decades, the Caltech Submillimeter Observatory (CSO) has contributed a number of key discoveries on these topics. Light hydrides are of particular interest for astrochemistry, as the basic building blocks of the chemical networks in both diffuse and dense clouds. Ongoing and planned submillimeter wide-field continuum surveys will yield hundreds of potential galactic targets suitable for detailed spectroscopic follow-ups. Recent advances in detector and digital spectrometer technologies promise to truly revolutionize further the field of high-resolution submillimeter spectroscopy and its application to the study of the life cycle of molecules. This will greatly improve our understanding of astrochemistry, astrobiology, the origin of life on Earth, and allow assessing the possibilities of life in other planetary systems.
C1 [Lis, Dariusz C.] CALTECH, MS 301-17, Pasadena, CA 91125 USA.
[Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bergin, Edwin A.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Falgarone, Edith; Gerin, Maryvonne] CNRS, LERMA, F-75231 Paris, France.
[Falgarone, Edith; Gerin, Maryvonne] Ecole Normale Super, F-75231 Paris, France.
[Roueff, Evelyne] Observ Paris, F-92195 Meudon, France.
RP Lis, DC (reprint author), CALTECH, MS 301-17, Pasadena, CA 91125 USA.
EM dcl@caltech.edu; paul.f.goldsmith@jpl.nasa.gov; ebergin@umich.edu;
edith@lra.ens.fr; gerin@lra.ens.fr
FU NSF [AST-0540882]
FX The Caltech submillimted Observatory is supported by NSF grant
AST-0540882.
NR 52
TC 9
Z9 9
U1 0
U2 4
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-714-8
J9 ASTR SOC P
PY 2009
VL 417
BP 23
EP +
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL34
UT WOS:000281244000003
ER
PT B
AU Langer, WD
AF Langer, William D.
BE Lis, DC
Vaillancourt, JE
Goldsmith, PF
Bell, TA
Scoville, NZ
Zmuidzinas, J
TI The Lifecycle of Carbon in the Interstellar Medium
SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS
G. PHILLIPS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Symposium on Submillimeter Astrophysics and Technology held in honor of
Thomas G Philllips
CY FEB 23-24, 2009
CL Calif Inst Technol, Pasadena, CA
HO Calif Inst Technol
ID GALACTIC PLANE SURVEY; MOLECULAR CLOUDS; ATOMIC CARBON; CO SURVEY;
CHEMISTRY; LINE
AB This review summarizes the role of gaseous carbon in the Galactic interstellar medium (ISM) as a tracer of its different phases and as a primary gas coolant. Carbon in one of its many gaseous atomic and molecular forms has proven to be critical to our ability to trace the chemical and physical states of the cloud. This review covers the important role that Professor Tom Phillips has played in the study of key carbon species in the ISM.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Langer, WD (reprint author), CALTECH, Jet Prop Lab, MS 180-500,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM william.langer@jpl.nasa.gov
NR 22
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-714-8
J9 ASTR SOC P
PY 2009
VL 417
BP 71
EP 82
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL34
UT WOS:000281244000006
ER
PT B
AU Becklin, EE
Gehrz, RD
AF Becklin, E. E.
Gehrz, R. D.
BE Lis, DC
Vaillancourt, JE
Goldsmith, PF
Bell, TA
Scoville, NZ
Zmuidzinas, J
TI SOFIA: Stratospheric Observatory for Infrared Astronomy
SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS
G. PHILLIPS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Symposium on Submillimeter Astrophysics and Technology held in honor of
Thomas G Philllips
CY FEB 23-24, 2009
CL Calif Inst Technol, Pasadena, CA
HO Calif Inst Technol
ID SPACE-TELESCOPE; MISSION
AB The NASA/DLR. Stratospheric Observatory for Infrared Astronomy (SOFIA) is a 2.5 m infrared telescope in a Boeing 747SP. Flying at altitudes as high as 45,000 feet, it will enable 0.3 mu m - 1.6 mm observations with an average transmission of >= 80%. We describe the key role that Toni Phillips played in the early days of airborne astronomy that culminated in the development of SOFIA. The facility design and status are described. Nine first generation instruments that will fly on SOFIA include broadband imaging cameras, moderate resolution spectrographs capable of resolving emission features due to dust and large molecules, and high resolution spectrometers suitable for kinematical studies of molecular and atomic gas lines at km s(-1) resolution. World-wide deployments will provide access to the entire sky and enable timely observations of transient events. SOFIA's sensitivity for imaging and spectroscopy is similar to that of the space observatory ISO. Its telescope is diffraction-limited beyond 25 mu m, making its iinages 3 times sharper than those obtained by the Spitzer Space Telescope at these wavelengths. We describe the characteristics of the observatory and give several examples of science opportunities with SOFIA.
C1 [Becklin, E. E.] NASA, Univ Space Res Assoc, Ames Res Ctr, MS 211-3, Moffett Field, CA 94035 USA.
RP Becklin, EE (reprint author), NASA, Univ Space Res Assoc, Ames Res Ctr, MS 211-3, Moffett Field, CA 94035 USA.
EM becklin@astro.ucla.edu
NR 10
TC 4
Z9 4
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-714-8
J9 ASTR SOC P
PY 2009
VL 417
BP 101
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL34
UT WOS:000281244000009
ER
PT B
AU Benford, DJ
AF Benford, Dominic J.
BE Lis, DC
Vaillancourt, JE
Goldsmith, PF
Bell, TA
Scoville, NZ
Zmuidzinas, J
TI The SOFIA/SAFIRE Far-Infrared Spectrometer: Highlighting Submillimeter
Astrophysics and Technology
SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS
G. PHILLIPS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Symposium on Submillimeter Astrophysics and Technology held in honor of
Thomas G Philllips
CY FEB 23-24, 2009
CL Calif Inst Technol, Pasadena, CA
HO Calif Inst Technol
AB The Submillimeter and Far-InfraRed Experiment (SAFIRE) on the SOFIA airborne observatory is an imaging spectrometer for wavelengths between 28 mu m and 440 mu m. Our design is a dual-band long-slit grating spectrometer, which provides broadband (similar to 4000 km/s) observations in two lines simultaneously over a field of view roughly 10 '' wide by 320 '' long. The low backgrounds in spectroscopy require very sensitive detectors with noise equivalent powers of order 10(-18) W/root Hz. We are developing a kilopixel, filled detector array for SAFIRE in a 32 x 40 format. The detector consists of a transition edge sensor (TES) bolometer array, a per-pixel broadband absorbing backshort array, and a NIST SQUID multiplexer readout array. This general type of array has been used successfully in the GISMO instrument, so we extrapolate to the sensitivity needed for airborne spectroscopy. Much of the cryogenic, electronics, and software infrastructure for SAFIRE have been developed. I provide here an overview of the progress on SAFIRE.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Benford, DJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM dominic.benford@nasa.gov
RI Benford, Dominic/D-4760-2012
OI Benford, Dominic/0000-0002-9884-4206
NR 6
TC 0
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U1 0
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PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-714-8
J9 ASTR SOC P
PY 2009
VL 417
BP 137
EP 142
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL34
UT WOS:000281244000013
ER
PT B
AU Goldsmith, PF
Velusamy, T
Li, D
Langer, W
AF Goldsmith, Paul F.
Velusamy, T.
Li, Di
Langer, William
BE Lis, DC
Vaillancourt, JE
Goldsmith, PF
Bell, TA
Scoville, NZ
Zmuidzinas, J
TI H-2 in Molecular Clouds
SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS
G. PHILLIPS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Symposium on Submillimeter Astrophysics and Technology held in honor of
Thomas G Philllips
CY FEB 23-24, 2009
CL Calif Inst Technol, Pasadena, CA
HO Calif Inst Technol
ID HYDROGEN; GAS
AB We report the detection of the S(0) and S(1) pure rotational transitions of H-2 in emission from a boundary layer of the Taurus molecular cloud. These lines were observed with the Spitzer Infrared Spectrograph (IRS), and are very weak, with maximum specific intensity <= 0.4 MJy sr(-1). The emission is strongest 8.5' (0.33 pc) outside the edge of the cloud defined by the (CO)-C-13. We see H2 emission towards the bulk of the cloud at a lower level, suggestive of limb brightening of an envelope around the purely molecular cloud. The peak column densities looking directly towards the cloud are N(J = 3) = 1.3x10(17) cm(-2), and N(J = 2) = 2.2x10(18) cm(-2). Towards the maximum of the rotationally excited H-2 emission, N(J = 3) = 5.2x10(17) cm(-2) and N(J = 2) = 4.4x10(18) cm(-2). Interpreting the ratio is made difficult by the not well determined ortho- to para-H-2 ratio (OPR), but for reasonable values of the OPR, we can constrain the characteristics of the region responsible for the H2 emission. For example, for OPR = 3 and n(H-2) = 100 cm(-3), T-K must be greater than approximately 200 K. We have used the Meudon PDR code to model the H-2 emission from the cloud edge, and find that while the column density in J = 2 can be reproduced with reasonable parameters for the region and its environment, the column density in J = 3 that is predicted falls more than a factor of 5 below that observed. This suggests that an additional source of H-2 excitation is present. Further data and modeling are required to understand this issue, which will improve our understanding of cloud structure and the physics of H-2 formation.
C1 [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Oak Grove Dr,MS 180-703, Pasadena, CA 91103 USA.
RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, Oak Grove Dr,MS 180-703, Pasadena, CA 91103 USA.
EM paul.f.goldsmith@jpl.nasa.gov; velusamy@jpl.nasa.gov; dili@jpl.nasa.gov;
william.langer@jpl.nasa.gov
NR 13
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-714-8
J9 ASTR SOC P
PY 2009
VL 417
BP 177
EP +
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL34
UT WOS:000281244000017
ER
PT B
AU Pearson, JC
Brauer, CS
Drouin, BJ
Yu, S
AF Pearson, J. C.
Brauer, C. S.
Drouin, B. J.
Yu, S.
BE Lis, DC
Vaillancourt, JE
Goldsmith, PF
Bell, TA
Scoville, NZ
Zmuidzinas, J
TI Better Spectrometers, Beautiful Spectra, and Confusion for All
SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS
G. PHILLIPS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Symposium on Submillimeter Astrophysics and Technology held in honor of
Thomas G Philllips
CY FEB 23-24, 2009
CL Calif Inst Technol, Pasadena, CA
HO Calif Inst Technol
ID ORION
AB The confluence of enormous improvements in submillimeter receivers and the development of powerful large scale observatories is about to force astrophysics and the sciences that support it to develop novel approaches for interpretation of data. The historical method of observing one or two lines and carefully analyzing them in the context of a simple model is now only applicable for distant objects where only a few lines are strong enough to be observable. Modern observatories collect many GHz of high signal-to-noise spectra in a single observation and, in many cases, at sufficiently high spatial resolution to start resolving chemically distinct regions. The observatories planned for the near future and the inevitable upgrades of existing facilities will make large spectral data sets the rule rather than the exception in many areas of molecular astrophysics. The methodology and organization required to fully extract the available information and interpret these beautiful spectra represents a challenge to submillimeter astrophysics similar in magnitude to the last few decades of effort in improving receivers. The quality and abundance of spectra effectively prevents line-by-line analysis from being a time efficient proposition, however, global analysis of complex spectra is a science in its infancy. Spectroscopy at several other wavelengths has developed a number of techniques to analyze complex spectra, which can provide a great deal of guidance to the molecular astrophysics community on how to attack the complex spectrum problem. Ultimately, the challenge is one of organization, similar to building observatories, requiring teams of specialists combining their knowledge of dynamical, structural, chemical and radiative models with detailed knowledge in molecular physics and gas and grain surface chemistry to extract and exploit the enormous information content of complex spectra. This paper presents a spectroscopist's view of the necessary elements in a tool for complex spectral analysis.
C1 [Pearson, J. C.; Brauer, C. S.; Drouin, B. J.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pearson, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM john.c.pearson@jpl.nasa.gov
NR 8
TC 0
Z9 0
U1 0
U2 1
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-714-8
J9 ASTR SOC P
PY 2009
VL 417
BP 191
EP 202
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL34
UT WOS:000281244000018
ER
PT B
AU Bradford, CM
Aguirre, JE
Bock, JJ
Earle, L
Glenn, J
Inami, H
Kamenetzky, J
Maloney, PR
Matsuhara, H
Naylor, BJ
Nguyen, HT
Zmuidzinas, J
AF Bradford, C. M.
Aguirre, J. E.
Bock, J. J.
Earle, L.
Glenn, J.
Inami, H.
Kamenetzky, J.
Maloney, P. R.
Matsuhara, H.
Naylor, B. J.
Nguyen, H. T.
Zmuidzinas, J.
BE Lis, DC
Vaillancourt, JE
Goldsmith, PF
Bell, TA
Scoville, NZ
Zmuidzinas, J
TI Survey Spectroscopy in the Submillimeter and Millimeter, from the CSO to
CCAT
SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS
G. PHILLIPS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Symposium on Submillimeter Astrophysics and Technology held in honor of
Thomas G Philllips
CY FEB 23-24, 2009
CL Calif Inst Technol, Pasadena, CA
HO Calif Inst Technol
ID INITIAL MASS FUNCTION; CLOVERLEAF QUASAR; STAR-FORMATION; MOLECULAR GAS;
BROAD-BAND; Z-SPEC; SPECTROMETER; EMISSION; REDSHIFT; GALAXIES
AB I outline some results from the Z-Spec instrument at the CSO and present a concept for CCAT survey spectrometer.
C1 [Bradford, C. M.; Bock, J. J.; Naylor, B. J.; Nguyen, H. T.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, JPL Mail Code 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Bradford, C. M.; Bock, J. J.; Naylor, B. J.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA.
[Aguirre, J. E.; Earle, L.; Glenn, J.; Kamenetzky, J.; Maloney, P. R.] Univ Colorado, Boulder, CO 80303 USA.
[Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA.
[Inami, H.; Matsuhara, H.] Japan Aerosp & Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan.
RP Bradford, CM (reprint author), CALTECH, Jet Prop Lab, JPL Mail Code 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bradford@submm.caltech.edu; jason.glenn@colorado.edu;
jonas@submm.caltech.edu
NR 21
TC 3
Z9 3
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-714-8
J9 ASTR SOC P
PY 2009
VL 417
BP 341
EP +
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL34
UT WOS:000281244000034
ER
PT B
AU Staguhn, J
Benford, D
Allen, C
Arendt, R
George, J
Fixsen, D
Maher, S
Sharp, E
Ames, T
Chuss, D
Dwek, E
Marx, C
Miller, T
Moseley, SH
Navarro, S
Schinnerer, E
Sievers, A
Walter, F
Wollack, E
AF Staguhn, Johannes
Benford, Dominic
Allen, Christine
Arendt, Rick
George, Jithin
Fixsen, Dale
Maher, Stephen
Sharp, Elmer
Ames, Troy
Chuss, David
Dwek, Eli
Marx, Catherine
Miller, Tim
Moseley, S. Harvey
Navarro, Santiago
Schinnerer, Eva
Sievers, Albrecht
Walter, Fabian
Wollack, Edward
BE Lis, DC
Vaillancourt, JE
Goldsmith, PF
Bell, TA
Scoville, NZ
Zmuidzinas, J
TI New Results from GISMO, a 2 mm Camera Using a Backshort-Under-Grid TES
Bolometer Array
SO SUBMILLIMETER ASTROPHYSICS AND TECHNOLOGY: A SYMPOSIUM HONORING THOMAS
G. PHILLIPS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Symposium on Submillimeter Astrophysics and Technology held in honor of
Thomas G Philllips
CY FEB 23-24, 2009
CL Calif Inst Technol, Pasadena, CA
HO Calif Inst Technol
AB In October 2008, we demonstrated for the second time our 2 mm bolometer camera GISMO (the Goddard IRAM Superconducting 2 Millimeter Observer) for astronomical observations at the IRAM 30 m telescope in Spain. GISMO uses a monolithic 8 x 16 Backshort Under Grid (BUG) array with superconducting Transition Edge Sensors (TES). The instrument's fast beam yields 0.9 lambda/D pixel sampling, which optimizes GISMO for detecting sources serendipitously in large sky surveys, while the capability for diffraction limited imaging is preserved. In order to ensure GISMO's operation under all weather conditions, we used a 40% neutral density filter at 4 K. In less than ideal weather conditions we obtained map sensitivities for the working pixels of between 40 mJy s(-1/2) and 50 mJy s(-1/2). These numbers are consistent with our atmospheric model calculations. The predicted map NEFDs range from 28 to 56 mJy s(-1/2) for GISMO's optical configuration (including the 40% neutral density filter) and observing conditions ranging between 10% and 40% line of sight opacities. With an optimized observing strategy for point sources of known position, this sensitivity can further be increased by a factor of 1.5, which we demonstrate by means of analyzing of our signal to noise ratio achieved for point source crossings in the time stream data. The noise in our co-added maps (with few thousand seconds of integration time) scales very well with the square root of time clown to sub-mJy levels. We have now designed a cryogenic mechanism that will allow us to move neutral density filters in or out of the beam during future observations. Our simulations indicate that we will gain a factor of 2.4 in observing efficiency if we take out the neutral density filter under good weather conditions. Under typical conditions (20% line of sight sky opacity) we expect to achieve a good pixel map sensitivity of 22 mJy s(-1/2) and a map NEFD of 1 mJy in an observation lasting about 8 minutes.
C1 [Staguhn, Johannes; Benford, Dominic; Allen, Christine; Arendt, Rick; Fixsen, Dale; Maher, Stephen; Sharp, Elmer; Ames, Troy; Chuss, David; Dwek, Eli; Marx, Catherine; Miller, Tim; Moseley, S. Harvey; Wollack, Edward] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
RP Staguhn, J (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM johannes.g.staguhn@nasa.gov; dominic.benford@nasa.gov;
harvey.moseley@nasa.gov
RI Dwek, Eli/C-3995-2012; Benford, Dominic/D-4760-2012; Moseley,
Harvey/D-5069-2012; Chuss, David/D-8281-2012; Wollack,
Edward/D-4467-2012
OI Benford, Dominic/0000-0002-9884-4206; Wollack,
Edward/0000-0002-7567-4451
FU NSF [0705185]
FX THis work was sipported in party by NSF Grant AST 0705185
NR 8
TC 1
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U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-714-8
J9 ASTR SOC P
PY 2009
VL 417
BP 451
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BQL34
UT WOS:000281244000041
ER
PT B
AU Ghais, AF
AF Ghais, Ahmad F.
BE Sachdev, DK
TI INMARSAT: A SUCCESS STORY
SO SUCCESS STORIES IN SATELLITE SYSTEMS
SE Library of Flight
LA English
DT Article; Book Chapter
C1 [Ghais, Ahmad F.] INMARSAT, Engn & Operat, London, England.
[Ghais, Ahmad F.] NASA, Washington, DC USA.
RP Ghais, AF (reprint author), NASA, Washington, DC USA.
NR 0
TC 1
Z9 1
U1 0
U2 0
PU AMER INST AERONAUTICS & ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DR, STE 500, RESTON, VA 20191-4344 USA
BN 978-1-56347-966-3
J9 LIBR FLIGHT
PY 2009
BP 95
EP +
PG 26
WC Engineering, Aerospace
SC Engineering
GA BKF81
UT WOS:000267990500005
ER
PT J
AU Atlas, RM
AF Atlas, Ronald M.
GP Natl Res Council
TI A SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE
SCIENCES A Collaborative Effort of the National Research Council and the
American Association for the Advancement of Science Summary
SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE
SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND
THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE
LA English
DT Editorial Material; Book Chapter
ID BIOLOGICAL WEAPONS; ETHICAL-ISSUES; SCIENTIFIC-RESEARCH; RESEARCH NORMS;
1918 FLU; VIRUS; GENETICS; CODES; INDUSTRY; FACULTY
C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
[Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA.
[Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA.
[Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA.
[Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA.
[Atlas, Ronald M.] ASM, Madison, WI USA.
[Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA.
[Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway.
[Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England.
RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
NR 168
TC 1
Z9 1
U1 0
U2 0
PU NATL ACADEMIES PRESS
PI WASHINGTON
PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA
BN 978-0-309-12510-9
PY 2009
BP 1
EP +
PG 20
WC Education & Educational Research
SC Education & Educational Research
GA BC4IZ
UT WOS:000352554100002
ER
PT J
AU Atlas, RM
AF Atlas, Ronald M.
GP Natl Res Council
TI A SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE
SCIENCES A Collaborative Effort of the National Research Council and the
American Association for the Advancement of Science Preface and
Acknowledgments
SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE
SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND
THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE
LA English
DT Editorial Material; Book Chapter
C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
[Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA.
[Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA.
[Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA.
[Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA.
[Atlas, Ronald M.] ASM, Madison, WI USA.
[Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA.
[Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway.
[Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England.
RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU NATL ACADEMIES PRESS
PI WASHINGTON
PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA
BN 978-0-309-12510-9
PY 2009
BP VII
EP IX
PG 3
WC Education & Educational Research
SC Education & Educational Research
GA BC4IZ
UT WOS:000352554100001
ER
PT J
AU Atlas, RM
AF Atlas, Ronald M.
GP Natl Res Council
TI A SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE
SCIENCES A Collaborative Effort of the National Research Council and the
American Association for the Advancement of Science Overview
SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE
SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND
THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE
LA English
DT Editorial Material; Book Chapter
C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
[Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA.
[Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA.
[Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA.
[Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA.
[Atlas, Ronald M.] ASM, Madison, WI USA.
[Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA.
[Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway.
[Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England.
RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU NATL ACADEMIES PRESS
PI WASHINGTON
PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA
BN 978-0-309-12510-9
PY 2009
BP 11
EP 41
PG 31
WC Education & Educational Research
SC Education & Educational Research
GA BC4IZ
UT WOS:000352554100003
ER
PT J
AU Atlas, RM
AF Atlas, Ronald M.
GP Natl Res Council
TI Approach
SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE
SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND
THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE
LA English
DT Article; Book Chapter
C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
[Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA.
[Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA.
[Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA.
[Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA.
[Atlas, Ronald M.] ASM, Madison, WI USA.
[Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA.
[Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway.
[Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England.
RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU NATL ACADEMIES PRESS
PI WASHINGTON
PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA
BN 978-0-309-12510-9
PY 2009
BP 43
EP 61
PG 19
WC Education & Educational Research
SC Education & Educational Research
GA BC4IZ
UT WOS:000352554100004
ER
PT J
AU Atlas, RM
AF Atlas, Ronald M.
GP Natl Res Council
TI Results of the Survey
SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE
SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND
THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE
LA English
DT Article; Book Chapter
C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
[Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA.
[Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA.
[Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA.
[Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA.
[Atlas, Ronald M.] ASM, Madison, WI USA.
[Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA.
[Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway.
[Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England.
RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU NATL ACADEMIES PRESS
PI WASHINGTON
PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA
BN 978-0-309-12510-9
PY 2009
BP 63
EP 113
PG 51
WC Education & Educational Research
SC Education & Educational Research
GA BC4IZ
UT WOS:000352554100005
ER
PT J
AU Atlas, RM
AF Atlas, Ronald M.
GP Natl Res Council
TI A SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE
SCIENCES A Collaborative Effort of the National Research Council and the
American Association for the Advancement of Science Conclusions and
Recommendations
SO SURVEY OF ATTITUDES AND ACTIONS ON DUAL USE RESEARCH IN THE LIFE
SCIENCES: A COLLABORATIVE EFFORT OF THE NATIONAL RESEARCH COUNCIL AND
THE AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCIENCE
LA English
DT Editorial Material; Book Chapter
C1 [Atlas, Ronald M.] Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
[Atlas, Ronald M.] Univ Louisville, Ctr Hlth Hazards Preparedness, Louisville, KY 40292 USA.
[Atlas, Ronald M.] NASA, Planetary Protect Board, Washington, DC USA.
[Atlas, Ronald M.] Wellcome Trust Infect Immunol & Populat Hlth Stra, Baltimore, MD USA.
[Atlas, Ronald M.] ASM Task Force Biodef, Boston, MA USA.
[Atlas, Ronald M.] ASM, Madison, WI USA.
[Atlas, Ronald M.] NIH, Recombinant DNA Advisory Comm, Baltimore, MD USA.
[Atlas, Ronald M.] Dept Homeland Secur Sci & Technol Advisory Comm, Oslo, Norway.
[Atlas, Ronald M.] Fed Bur Invest Sci Working Grp Bioforens, London, England.
RP Atlas, RM (reprint author), Univ Louisville, Biol & Publ Hlth, Louisville, KY 40292 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU NATL ACADEMIES PRESS
PI WASHINGTON
PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA
BN 978-0-309-12510-9
PY 2009
BP 115
EP 122
PG 8
WC Education & Educational Research
SC Education & Educational Research
GA BC4IZ
UT WOS:000352554100006
ER
PT J
AU Feidas, H
Kokolatos, G
Negri, A
Manyin, M
Chrysoulakis, N
Kamarianakis, Y
AF Feidas, H.
Kokolatos, G.
Negri, A.
Manyin, M.
Chrysoulakis, N.
Kamarianakis, Y.
TI Validation of an infrared-based satellite algorithm to estimate
accumulated rainfall over the Mediterranean basin
SO THEORETICAL AND APPLIED CLIMATOLOGY
LA English
DT Article
ID PRECIPITATION ESTIMATION; RETRIEVAL ALGORITHMS; CLOUD; IMAGERY;
MICROWAVE; PENINSULA; RADAR
AB The potential of an infrared-based satellite rainfall algorithm, the well-known Convective-Stratiform technique (CST), to estimate accumulated rainfall in the Mediterranean basin is tested. The CST, calibrated by coincident, physically retrieved rainfall rates from the Tropical Rainfall Measuring Mission (TRMM) Precipitation Radar (PR), is applied over the central-eastern Mediterranean region for the twelve-month period September 2004-August 2005. Estimates from this technique are verified over a 1A degrees x1A degrees gridded precipitation dataset, based on rain gauge data only, for different time scales (monthly, seasonal and annual). The comparisons between satellite-derived precipitation estimates and validation data provide a high correlation coefficient (0.88) and low biases only for the summer season. In contrast, the comparison statistics for winter demonstrate the shortcomings of the CST algorithm in reproducing adequately the precipitation field in the mid-latitudes during this season. Although the correlations for spring and annual precipitation are relatively high (0.76 and 0.73, respectively), a strong positive bias exists. Rainfall variability is less adequately reproduced for the autumn, but the errors are within an acceptable range. A comparison test conducted in the different climate zones of the study area indicated that the calibrated CST performs better in the sub-tropical deserts and steppes of northern Africa and in humid, continental climates. Mediterranean climates produce higher correlations for autumn, summer and spring precipitation, whereas humid sub-tropical climates present the lowest correlation coefficients. Finally, the potential of the CST technique in climatic studies was demonstrated by studying the diurnal variability of precipitation at high spatial and temporal resolutions.
C1 [Feidas, H.] Aristotle Univ Thessaloniki, Dept Geol, Div Meteorology Climatol, Thessaloniki 54124, Greece.
[Kokolatos, G.] Univ Aegean, Dept Geog, Mitilini, Greece.
[Negri, A.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Manyin, M.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Chrysoulakis, N.; Kamarianakis, Y.] Fdn Res & Technol Hellas, Reg Anal Div, Inst Appl & Computat Math, Iraklion, Crete, Greece.
RP Feidas, H (reprint author), Aristotle Univ Thessaloniki, Dept Geol, Div Meteorology Climatol, Thessaloniki 54124, Greece.
EM xfeidas@geo.aegean.gr
RI Manyin, Michael/D-7756-2012
FU Ministry of Development of Greece.
FX This work was conducted as part of the SATERM (A Satellite Technique for
Estimating Rainfall over the Mediterranean basin) project funded by the
Project "Competitiveness'', Action 4.3.6.1d "Cooperation with R&T
institutions in non-European countries'' of the General Secretary of
Research and Technology, Ministry of Development of Greece.
NR 50
TC 11
Z9 12
U1 0
U2 1
PU SPRINGER WIEN
PI WIEN
PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA
SN 0177-798X
J9 THEOR APPL CLIMATOL
JI Theor. Appl. Climatol.
PD JAN
PY 2009
VL 95
IS 1-2
BP 91
EP 109
DI 10.1007/s00704-007-0360-y
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 396FI
UT WOS:000262577200008
ER
PT B
AU Lunine, J
Choukroun, M
Stevenson, D
Tobie, G
AF Lunine, Jonathan
Choukroun, Mathieu
Stevenson, David
Tobie, Gabriel
BE Brown, RH
Lebreton, JP
Waite, JH
TI The Origin and Evolution of Titan
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID GIANT PLANET FORMATION; LARGE ICY SATELLITES; OUTER SOLAR-SYSTEM;
PROTOPLANETARY DISKS; GALILEAN SATELLITES; INTERNAL STRUCTURE; THERMAL
EVOLUTION; HIGH-PRESSURE; THERMODYNAMIC PROPERTIES; ATMOSPHERIC METHANE
AB Titan was formed as a regular satellite in a disk that was the outgrowth of the formation of Saturn itself. Unlike the Jovian system, Titan is alone in terms of its size and mass, not part of a system gradational in density and hence rock abundance, perhaps reflecting a smaller disk and greater importance of stochastic events during satellite assembly. Accretional heating of Titan was enough to melt an outer layer of water (a water "magma ocean") and sustain for a short period an environment in which exposed water or water-ammonia liquid was in contact with organic molecules. Initial warm surface conditions are supported by direct samplings of Titan's atmosphere by the mass spectrometers on board Cassini and Huygens, which provide circumstantial evidence that ammonia (NH(3)) is the primordial Source of Titan's atmospheric molecular nitrogen. Ammonia can be extracted from the liquid phase only if the surface temperature is above the melting point of the mixture, thus implying warm accretion.
The carbon isotopic ratio (13)C/(12)C in hydrocarbon molecules measured by the GCMS on Huygens reflects a bulk carbon inventory that did not participate in the massive escape phase of the ancient post-accretional atmosphere, in contrast to nitrogen, whose isotopic ratio (15)N/(14)N is modestly enhanced and thus suggests escape, though how much depends on the mechanism. The presence of a significant amount of the (40)K decay daughter (40)Ar strongly suggests that internal outgassing of volatiles, including methane and argon, has occurred through Titan's history.
Different models of the thermal and structure evolution of Titan's interior have been proposed to explain the persistence of methane at the surface over the age of the solar system (of order 100 times the lifetime of the known reservoirs of methane in the surface and atmosphere), and a modest dearth of impact craters consistent with a surface age of about a billion years. A first post-Cassini-Huygens model suggests that the formation of thin crust enriched in methane clathrate, owing to interactions between the primordial ocean and the primitive atmosphere as well as release of volatiles from the deep interior, could have delayed the crystallization of the internal ocean, favoring outgassing of methane at different epochs.
C1 [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Choukroun, Mathieu] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stevenson, David] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Tobie, Gabriel] Univ Nantes, Lab Planetol & Geodynam, F-44312 Nantes 3, France.
RP Lunine, J (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM jlunine@lpl.arizona.edu
RI Choukroun, Mathieu/F-3146-2017
OI Choukroun, Mathieu/0000-0001-7447-9139
NR 148
TC 18
Z9 18
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 35
EP 59
DI 10.1007/978-1-4020-9215-2_3
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300003
ER
PT B
AU Sotin, C
Mitri, G
Rappaport, N
Schubert, G
Stevenson, D
AF Sotin, Christophe
Mitri, Giuseppe
Rappaport, Nicole
Schubert, Gerald
Stevenson, David
BE Brown, RH
Lebreton, JP
Waite, JH
TI Titan's Interior Structure
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID LARGE VISCOSITY VARIATIONS; LARGE ICY SATELLITES; INTERNAL STRUCTURE;
THERMAL-CONVECTION; HUYGENS PROBE; PHYSICAL-CHARACTERISTICS; GALILEAN
SATELLITES; TIDAL DISSIPATION; ATMOSPHERE; SHELL
AB The goal of this chapter is to give a description of Titan's interior that is consistent with the new constraints provided by the Cassini mission. As the Cassini mission proceeds into its first extended phase, the data obtained during the nominal mission suggest that Titan is at least partially differentiated. An ocean would be present some tens of kilometers below the surface. By comparison with the Galilean icy satellites Ganymede and Callisto, Titan would be composed of a metal/silicate rich core and a H2O rich outer layer. These conclusions are drawn from the interpretation of the gravity data, the geological data and the presence of a Schumann resonance which has been inferred from the measurement of electric signals during the descent of the Huygens probe into Titan's atmosphere. Titan's high eccentricity implies that the interior has not been very dissipative, there is little tidal heating available for internal dynamics, and the ice layer is cold, which can be achieved if the ocean under the ice layer contains ammonia. This paper also describes observations and interpretations which seem difficult to reconcile with our present understanding of Titan's interior structure and evolution such as the shape of the planet or the obliquity. The last part of the chapter describes heat transfer models which suggest that the lower part of the ice crust could be convective. The NH3-H2O phase diagram indicates that the ocean is decoupled from the silicate-rich core by a layer of high-pressure ices. However, the interior model is largely uncertain because the interpretation of the data is still debated at present time. The additional information that will be acquired during the Cassini Solstice Mission should allow us to answer some of the questions.
C1 [Sotin, Christophe; Mitri, Giuseppe; Rappaport, Nicole] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schubert, Gerald] Univ Calif Los Angeles, Los Angeles, CA USA.
RP Sotin, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 183-301, Pasadena, CA 91109 USA.
EM christophe.sotin@jpl.nasa.gov
NR 58
TC 16
Z9 16
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 61
EP 73
DI 10.1007/978-1-4020-9215-2_4
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300004
ER
PT B
AU Jaumann, R
Kirk, RL
Lorenz, RD
Lopes, RMC
Stofan, E
Turtle, EP
Keller, HU
Wood, CA
Sotin, C
Soderblom, LA
Tomasko, MG
AF Jaumann, Ralf
Kirk, Randolph L.
Lorenz, Ralph D.
Lopes, Rosaly M. C.
Stofan, Ellen
Turtle, Elizabeth P.
Keller, Horst Uwe
Wood, Charles A.
Sotin, Christophe
Soderblom, Laurence A.
Tomasko, Martin G.
BE Brown, RH
Lebreton, JP
Waite, JH
TI Geology and Surface Processes on Titan
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID HUYGENS LANDING SITE; BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DESCENT
IMAGER/SPECTRAL RADIOMETER; CASSINI RADAR OBSERVATIONS; MAPPING
SPECTROMETER VIMS; ADAPTIVE OPTICS; TIDAL DISSIPATION; IMAGING SCIENCE;
SATURN SYSTEM; MU-M
AB The surface of Titan has been revealed globally, if incompletely, by Cassini observations at infrared and radar wavelengths as well as locally by the instruments on the Huygens probe. Extended dune fields, lakes, mountainous terrain, dendritic erosion patterns and erosional remnants indicate dynamic surface processes. Valleys, small-scale gullies and rounded cobbles such as those observed at the Huygens landing site require erosion by energetic flow of a liquid. There is strong evidence that liquid hydrocarbons are ponded on the surface in high-latitude lakes, predominantly, but not exclusively, at high northern latitudes. A variety of features including extensive flows and caldera-like constructs are interpreted to be cryovolcanic in origin. Chains and isolated blocks of rugged terrain rising from smoother areas are best described as mountains and might be related to tectonic processes. Finally, impact craters are observed but their small numbers indicate that the crater retention age is very young overall. In general, Titan exhibits a geologically active surface indicating significant endogenic and exogenic processes, with diverse geophysical and atmospheric processes reminiscent of those on Earth.
C1 [Jaumann, Ralf] DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Jaumann, Ralf] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany.
[Kirk, Randolph L.; Soderblom, Laurence A.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Lorenz, Ralph D.; Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
[Lopes, Rosaly M. C.; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stofan, Ellen] Proxemy Res, Rectortown, VA 20140 USA.
[Keller, Horst Uwe] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
[Wood, Charles A.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Tomasko, Martin G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Jaumann, R (reprint author), DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
EM ralf.jaumann@dlr.de
RI Turtle, Elizabeth/K-8673-2012; Lorenz, Ralph/B-8759-2016
OI Turtle, Elizabeth/0000-0003-1423-5751; Lorenz, Ralph/0000-0001-8528-4644
NR 230
TC 18
Z9 18
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 75
EP 140
DI 10.1007/978-1-4020-9215-2_5
PG 66
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300005
ER
PT B
AU Soderblom, LA
Barnes, JW
Brown, RH
Clark, RN
Janssen, MA
McCord, TB
Niemann, HB
Tomasko, MG
AF Soderblom, L. A.
Barnes, J. W.
Brown, R. H.
Clark, R. N.
Janssen, M. A.
McCord, T. B.
Niemann, H. B.
Tomasko, M. G.
BE Brown, RH
Lebreton, JP
Waite, JH
TI Composition of Titan's Surface
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID HUYGENS LANDING SITE; DESCENT IMAGER/SPECTRAL RADIOMETER; MAPPING
SPECTROMETER VIMS; COMPLEX ORGANIC-MATTER; CASSINI RADAR; ICY
SATELLITES; MU-M; DIELECTRIC-PROPERTIES; INFRARED OBSERVATIONS;
REFLECTANCE SPECTRA
AB The Huygens Probe returned the first in situ data on Titan's surface composition in January 2005. Although Huygens landed on a dry plain, the Gas Chromatograph Mass Spectrometer (GCMS) showed evidence of methane moisture in the near subsurface suggesting methane precipitation at some time in the past. Heavier organic molecules were not found to be abundant in the atmosphere or at the surface, but the GCMS surface results did show ethane to be present and tentatively identified cyanogen, benzene, and carbon dioxide. During descent, aerosol particles were processed with the Aerosol Collector and Pyroliser; results suggested that the aerosols contain both nitrites and hydrocarbons. The Descent Imager/Spectral Radiometer (DISR also carried by the probe) measured the visible and near-infrared spectral reflectance of the dark plain surface at the landing site. Those data suggest a mixture of water ice, tholin-like materials, and dark neutral material with a blue slope in the near infrared; identification of water ice is suggested but inconclusive. Most remarkably DISR did not detect spectral features, beyond those for methane, for a wide range of spectrally active hydrocarbon and nitrile compounds that had been expected to be present on the surface.
C1 [Soderblom, L. A.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86004 USA.
[Barnes, J. W.] Univ Idaho, Moscow, ID 83844 USA.
[Brown, R. H.; Tomasko, M. G.] Univ Arizona, Tucson, AZ 85721 USA.
[Clark, R. N.] US Geol Survey, Denver, CO 80225 USA.
[Janssen, M. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McCord, T. B.] Bear Fight Ctr, Winthrop, WA 98862 USA.
[Niemann, H. B.] NASA, Greenbelt, MD 20771 USA.
RP Soderblom, LA (reprint author), US Geol Survey, Astrogeol Team, Flagstaff, AZ 86004 USA.
EM lsoderblom@usgs.gov
NR 128
TC 8
Z9 8
U1 2
U2 3
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 141
EP 175
DI 10.1007/978-1-4020-9215-2_6
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300006
ER
PT B
AU Waite, JH
Young, DT
Westlake, JH
Lunine, JI
McKay, CP
Lewis, WS
AF Waite, J. H., Jr.
Young, D. T.
Westlake, J. H.
Lunine, J. I.
McKay, C. P.
Lewis, W. S.
BE Brown, RH
Lebreton, JP
Waite, JH
TI High-Altitude Production of Titan's Aerosols
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID UPPER-ATMOSPHERE; HAZE FORMATION; COUPLING PHOTOCHEMISTRY; INFRARED
OBSERVATIONS; ORGANIC-CHEMISTRY; SATURNIAN SYSTEM; MODEL; VOYAGER-1;
THOLIN; ION
AB Measurements with the Cassini Ion and Neutral Mass Spectrometer (INMS) and two Cassini Plasma Spectrometer (CAPS) sensors, the Ion beam Spectrometer (IBS) and the Electron Spectrometer (ELS), have revealed the presence of a significant population of heavy hydrocarbon and nitrile species well above the homopause, with masses as large as several thousand Daltons (Da). The INMS ion and neutral spectra cover the mass range 1-100 Da. The IBS has measured positive ions up to 350 Da, while the ELS has detected concentrations of negative ions as high as 20% of the total negatively charged ionosphere component extending to over 13,000 Da. These measurements have motivated the development of new atmospheric models and have significant implications for our knowledge and understanding of Titan's haze layers.
C1 [Waite, J. H., Jr.; Young, D. T.; Westlake, J. H.; Lewis, W. S.] SW Res Inst, San Antonio, TX 78228 USA.
[Waite, J. H., Jr.; Westlake, J. H.] Univ Texas San Antonio, San Antonio, TX 78249 USA.
[Lunine, J. I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[McKay, C. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Waite, JH (reprint author), SW Res Inst, PO Drawer 28510, San Antonio, TX 78228 USA.
EM hwaite@swri.edu
RI Westlake, Joseph/G-2732-2015
OI Westlake, Joseph/0000-0003-0472-8640
NR 64
TC 11
Z9 11
U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 201
EP 214
DI 10.1007/978-1-4020-9215-2_8
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300008
ER
PT B
AU Raulin, F
McKay, C
Lunine, J
Owen, T
AF Raulin, F.
McKay, C.
Lunine, J.
Owen, T.
BE Brown, RH
Lebreton, JP
Waite, JH
TI Titan's Astrobiology
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID PHOTOCHEMICAL KINETICS UNCERTAINTIES; ATMOSPHERIC CHEMISTRY; HAZE
FORMATION; ORGANIC HAZE; EARLY EARTH; PRIMITIVE EARTH; IN-SITU; COUPLING
PHOTOCHEMISTRY; LABORATORY SIMULATIONS; HETEROGENEOUS REACTION
AB This chapter describes the aspects of Saturn's moon Titan of astrobiological interest. Titan's prebiotic-like chemistry is reviewed, from the high atomosphere to the surface and subsurface, using the Cassini-Huygens data, with the help of theoretical modeling and experimental simulations. Similarities with and differences from the environment of the pre-biotic Earth are presented, and the lessons to be learned for Earth's organic chemical evolution on the prebiotic Earth discussed. The question of habitability and life on and in Titan is then considered, including the possibility of an exotic type of life that might exist in the liquid methane/ethane lakes. Finally. the relation between Titan and the destiny of life on Earth is discussed.
C1 [Raulin, F.] Univ Paris, LISA, Paris 12, France.
[Raulin, F.] Univ Paris, LISA, Paris 7, France.
[McKay, C.] NASA Ames, Ames, IA USA.
[Lunine, J.] Univ Arizona, LPL, Tucson, AZ USA.
[Owen, T.] Univ Hawaii, Honolulu, HI 96822 USA.
RP Raulin, F (reprint author), Univ Paris, LISA, Paris 12, France.
EM raulin@lisa.univ-paris12.fr
NR 133
TC 14
Z9 15
U1 2
U2 11
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 215
EP 233
DI 10.1007/978-1-4020-9215-2_9
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300009
ER
PT B
AU Strobel, DF
Atreya, SK
Bezard, B
Ferri, F
Flasar, FM
Fulchignoni, M
Lellouch, E
Muller-Wodarg, I
AF Strobel, Darrell F.
Atreya, Sushil K.
Bezard, Bruno
Ferri, Francesca
Flasar, F. Michael
Fulchignoni, Marcello
Lellouch, Emmanuel
Mueller-Wodarg, Ingo
BE Brown, RH
Lebreton, JP
Waite, JH
TI Atmospheric Structure and Composition
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID TITANS UPPER-ATMOSPHERE; HYDRODYNAMICALLY ESCAPING ATMOSPHERE; VOYAGER-1
RADIO-OCCULTATION; ISOTOPIC-RATIOS; CASSINI CIRS; STRATOSPHERIC
TEMPERATURE; HETEROGENEOUS REACTION; LATITUDINAL VARIATIONS; INFRARED
OBSERVATIONS; HYPOTHESIZED OCEAN
AB Titan's atmosphere is predominantly N-2 with CH4 the next most abundant molecule. It has a mole fraction of 0.05 just above the surface decreasing to 0.014 in the stratosphere. Above the homopause (similar to 800-850 km), it increases to 0.12 at the exobase. The third abundant molecule is H-2 with a tropospheric mole fraction of 0.001 increasing to 0.004 at similar to 1000 km and similar to 0.02 at the exobase (similar to 1500-1600 km). This chapter reviews the various measurements acquired by the Voyager flybys, Huygens Probe, orbiting Cassini spacecraft. ground-based and orbiting telescopes of the large suite of hydrocarbons, nitriles, other nitrogen and also oxygen bearing compounds. Titan possesses a mostly stable troposphere with a well defined tropopause (T similar to 70 K at similar to 44 km) and a lower stratosphere with a high static stability, which is extremely cold over the winter polar region (currently northern hemisphere) and warm over the summer pole. Remarkably in the middle stratosphere, the warmest temperatures occur at the equator and the largest meridional temperature gradients are found in the winter hemisphere. The stratopause from the summer pole to about 45 degrees N remains at a relatively constant pressure of 0.1 mbar/300 km and then it rises rapidly upward to similar to 0.01 mbar/400 km at the winter north pole, where it is the warmest region in the entire atmosphere. One possible interpretation of the Huygens Atmospheric Structure Instrument (HASI) temperature profile is that Titan's atmosphere is essentially isothermal similar to 170 K from 500-1100 km, with large amplitude thermal waves (10 K) superimposed. The existence and location of a well defined mesopause is an open question.
The chemistry of Titan's atmosphere is driven by CH4 photolysis in the thermosphere and catalytic reactions in the stratosphere, and by N-2 dissociation due to both UV photons and energetic electrons. Ethane is the most abundant gas product and HCN is the dominant nitrile. The mixing ratios of all photochemical species, except C2H4, increase with altitude at equatorial and Southern latitudes, indicative of transport from a high-altitude source to a condensation sink in the lower stratosphere. Northward of 45 degrees N, most product compounds are enriched as a consequence of subsidence in the winter polar vortex, particularly for nitriles and more complex hydrocarbons than C2H6 and C2H2. North of 45 degrees N, most products have lower increases with attitude than at low latitudes.
C1 [Strobel, Darrell F.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Atreya, Sushil K.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Bezard, Bruno; Fulchignoni, Marcello; Lellouch, Emmanuel] Observ Paris, LESIA, F-92195 Meudon, France.
[Ferri, Francesca] Univ Padua, CISAS G Colombo, I-35131 Padua, Italy.
[Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mueller-Wodarg, Ingo] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2BW, England.
RP Strobel, DF (reprint author), Johns Hopkins Univ, Baltimore, MD 21218 USA.
EM strobel@jhu.edu; atreya@umich.edu; Bruno.Bezard@obspm.fr;
francesca.ferri@unipd.it; f.m.flasar@nasa.gov;
marcello.fulchignoni@obspm.fr; emmanuel.lellouch@obspm.fr;
i.mueller-wodarg@imperial.ac.uk
RI Flasar, F Michael/C-8509-2012
NR 104
TC 24
Z9 24
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 235
EP 257
DI 10.1007/978-1-4020-9215-2_10
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300010
ER
PT B
AU Tomasko, MG
West, RA
AF Tomasko, Martin G.
West, Robert A.
BE Brown, RH
Lebreton, JP
Waite, JH
TI Aerosols in Titan's Atmosphere
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID IMAGER/SPECTRAL RADIOMETER DISR; NORTH POLAR STRATOSPHERE;
GENERAL-CIRCULATION; AGGREGATE PARTICLES; MIDLATITUDE CLOUDS;
OPTICAL-PROPERTIES; CONDENSATE CLOUDS; ORGANIC-CHEMISTRY;
HYDROGEN-CYANIDE; HUYGENS PROBE
AB Aerosols in Titan's atmosphere play important roles in the transfer of solar and thermal radiation, in Titan's heat balance, in forcing atmospheric dynamics, and as a sink for photochemical reactions. In this chapter we briefly summarize the history of our knowledge of their distribution and optical properties before concentrating in greater detail on current knowledge of their properties and roles in the physics and chemistry in Titan's atmosphere. We discuss the size, shape, optical properties, and the vertical distribution of Titan's aerosols. We discuss variations of the optical properties of the aerosols with wavelength, variations of the distribution of the aerosols over the disk of Titan, and the seasonal and long-term variations in structure. We discuss the visible and thermal opacity of the aerosols, and their roles in Titan's heat balance. We summarize the history and current state of laboratory simulations of these particles, and present our understanding of their formation and life cycles in one and two-dimensional microphysical models. We also discuss the presence, location, and variations in condensation clouds over Titan's disk. Finally, we indicate the prospects for further progress in understanding the origin, distribution, and properties of Titan's aerosols in the future.
C1 [Tomasko, Martin G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[West, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tomasko, MG (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM mtomasko@lpl.arizona.edu
NR 89
TC 10
Z9 10
U1 3
U2 3
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 297
EP 321
DI 10.1007/978-1-4020-9215-2_12
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300012
ER
PT B
AU Flasar, FM
Baines, KH
Bird, MK
Tokano, T
West, RA
AF Flasar, F. M.
Baines, K. H.
Bird, M. K.
Tokano, T.
West, R. A.
BE Brown, RH
Lebreton, JP
Waite, JH
TI Atmospheric Dynamics and Meteorology
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID COMPOSITE INFRARED SPECTROMETER; VOYAGER-1 RADIO-OCCULTATION; TITANS
MIDLATITUDE CLOUDS; GENERAL-CIRCULATION MODEL; HUYGENS PROBE; ZONAL
WINDS; EQUATORIAL SUPERROTATION; TROPOSPHERIC CLOUDS; CASSINI RADAR;
LATITUDINAL VARIATIONS
AB Titan, after Venus, is the second example in the solar system of an atmosphere with a global cyclostrophic circulation, but in this case a circulation that has a strong seasonal modulation in the middle atmosphere. Direct measurement of Titan's winds., particularly observations tracking the Huygens probe at 10 degrees S, indicate that the zonal winds are mostly in the sense of the satellite's rotation. They generally increase with altitude and become cyclostrophic near 35 km above the surface. An exception to this is a sharp minimum centered near 75 km, where the wind velocity decreases to nearly zero. Zonal winds derived from temperatures retrieved from Cassini orbiter measurements, using the thermal wind equation, indicate a strong winter circumpolar vortex, with maximum winds of 190 m s(-1) at mid northern latitudes near 300 kin. Above this level, the vortex decays. Curiously, the stratospheric zonal winds and temperatures in both hemispheres are symmetric about a pole that is offset from the surface pole by similar to 4 degrees. The cause of this is not well understood, but it may reflect the response of a cyclostrophic circulation to the offset between the equator, where the distance to the rotation axis is Greatest, and the seasonally varying subsolar latitude. The mean meridional circulation can be inferred from the temperature field and the meridional distribution of organic molecules and condensates and hazes. Both the warm temperatures near 400 km and the enhanced concentration of several organic molecules suggest subsidence in the north-polar region during winter and early spring. Stratospheric condensates are localized at high northern latitudes, with a sharp cut-off near 50 degrees N. Titan's winter polar vortex appears to share many of the same characteristics of isolating high and low-latitude air masses as do the winter polar vortices on Earth that envelop the ozone holes. Global mapping of temperatures, winds, and composition in the troposphere, by contrast, is incomplete. The few suitable discrete clouds that have been found for tracking indicate smaller velocities than aloft, consistent with the Huygens measurements. Along the descent trajectory, the Huygens measurements indicate eastward zonal winds down to 7 km, where they shift westward, and then eastward again below 1 km down to the surface. The low-latitude dune fields seen in Cassini RADAR images have been interpreted as longitudinal dunes occurring in a mean eastward zonal wind. This is not like Earth, where the low-latitude winds are westward above the surface. Because the net zonal-mean time-averaged torque exerted by the surface on the atmosphere should vanish, there must be westward flow over part of the surface; the question is where and when. The meridional contrast in tropospheric temperatures, deduced from radio occultations at low, mid, and high latitudes, is small, similar to 5 K at the tropopause and similar to 3 K at the surface. This implies efficient heat transport, probably by axisymmetric meridional circulations. The effect of the methane "hydrological" cycle on the atmospheric circulation is not well constrained by existing measurements. Understanding the nature of the surface-atmosphere coupling will be critical to elucidating the atmospheric transports of momentum, heat, and volatiles.
C1 [Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baines, K. H.; West, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Bird, M. K.] Univ Bonn, D-5300 Bonn, Germany.
[Tokano, T.] Univ Cologne, D-5000 Cologne 41, Germany.
RP Flasar, FM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM f.m.flasar@nasa.gov
RI Flasar, F Michael/C-8509-2012
NR 141
TC 8
Z9 8
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 323
EP 352
DI 10.1007/978-1-4020-9215-2_13
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300013
ER
PT B
AU Lorenz, RD
Brown, ME
Flasar, FM
AF Lorenz, Ralph D.
Brown, Michael E.
Flasar, F. Michael
BE Brown, RH
Lebreton, JP
Waite, JH
TI Seasonal Change on Titan
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID HUBBLE-SPACE-TELESCOPE; ZONAL WINDS; GENERAL-CIRCULATION; MIDLATITUDE
CLOUDS; CASSINI/CIRS DATA; LOWER ATMOSPHERE; SATURN SYSTEM; SURFACE;
MODEL; STRATOSPHERE
AB Titan displays seasonal changes in the distribution of gas and hazes in its atmosphere, in the character of its methane clouds, and in its temperatures and winds. While Cassini has observed some of these changes in detail, some are observable from Earth, and the period of most rapid change may be just about to begin in the years after equinox.
C1 [Lorenz, Ralph D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Brown, Michael E.] CALTECH, Pasadena, CA 91125 USA.
[Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lorenz, RD (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
EM ralph.lorenz@jhuapl.edu
RI Flasar, F Michael/C-8509-2012; Lorenz, Ralph/B-8759-2016
OI Lorenz, Ralph/0000-0001-8528-4644
NR 108
TC 7
Z9 7
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 353
EP 372
DI 10.1007/978-1-4020-9215-2_14
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300014
ER
PT B
AU Johnson, RE
Tucker, OJ
Michael, M
Sittler, EC
Smith, HT
Young, DT
Waite, JH
AF Johnson, R. E.
Tucker, O. J.
Michael, M.
Sittler, E. C.
Smith, H. T.
Young, D. T.
Waite, J. H.
BE Brown, RH
Lebreton, JP
Waite, JH
TI Mass Loss Processes in Titan's Upper Atmosphere
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID HYDRODYNAMICALLY ESCAPING ATMOSPHERE; PICK-UP IONS; SATURNS
MAGNETOSPHERE; ENCELADUS; NITROGEN; PLASMA; SPECTROMETER; EVOLUTION;
VOYAGER-1; EXOSPHERE
AB Although Titan's atmospheric column density is about ten times that of the Earth's, its measured N-15/N-14 ratio suggests that considerable escape has occurred or that Titan's original material had a ratio closer to that of cometary materials. A number of active escape processes have been proposed: thermal escape, chemical-induced escape, slow hydrodynamic escape, pick-up ion loss, ionospheric outflow and plasma-ion-induced atmospheric sputtering. These loss processes and relevant simulations are reviewed in light of recent Cassini data.
Analysis of Cassini data collected in Titan's thermosphere and corona indicate that thermal loss of hydrogen occurs at a rate comparable to pre-Cassini estimates. This escape of hydrogen is accompanied by a significant loss of methane due to formation and precipitation of hydrocarbons (similar to 2 x 10(29) amu/s). However, there is much less agreement on the rates for the escape of methane and nitrogen. Recent estimates, similar to 0.3-5 x 10(28) amu/s, are much larger than the pre-Cassini estimates and also much larger than the measured ion loss rates (similar to 1-5 x 10(26) amu/s). If the largest heavy molecule escape rates are assumed, a significant fraction of the present atmosphere would have been lost to space in 4 Gyr. Because understanding the nature of the active escape processes is critical, a number of data sets were used to model the methane and nitrogen escape rates. The solar heating/cooling rate and the nitrogen density profile vs altitude were used in a fluid dynamic model to extract an average net upward flux below the exobase; the altitude dependence of the diffusion of methane through nitrogen was described below the exobase allowing for upward flow and escape; the coronal structure above the exobase was simulated by plasma and photon-induced hot particle production; and measurements of the emission from excited-dissociation products were used to estimate escape. In the latter two models, hot recoils from photochemistry or plasma-ion-induced heating lead to escape, whereas in the first two models heat conduction from below was assumed to enhance Jeans escape, a process referred to as slow hydrodynamic escape. These models are compared to each other and to recent simulations of Titan's exobase region. It is found that these simulations are inconsistent with the slow hydrodynamic escape model and that the composition of the magnetospheric plasma at Titan's orbit is inconsistent with the largest carbon loss rates suggested.
C1 [Johnson, R. E.; Tucker, O. J.] Univ Virginia, Charlottesville, VA 22904 USA.
[Johnson, R. E.; Tucker, O. J.] NYU, Dept Phys, New York, NY 10003 USA.
[Michael, M.] Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India.
[Sittler, E. C.] GSFC, Greenbelt, MD USA.
[Smith, H. T.] JHUAPL, Laurel, MD USA.
[Young, D. T.; Waite, J. H.] SwRI, San Antonio, TX USA.
RP Tucker, OJ (reprint author), Univ Virginia, Charlottesville, VA 22904 USA.
EM rej@virginia.edu
RI Smith, Howard/H-4662-2016
OI Smith, Howard/0000-0003-3537-3360
NR 88
TC 26
Z9 26
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 373
EP 391
DI 10.1007/978-1-4020-9215-2_15
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300015
ER
PT B
AU Sittler, EC
Hartle, RE
Bertucci, C
Coates, A
Cravens, T
Dandouras, I
Shemansky, D
AF Sittler, Edward C.
Hartle, R. E.
Bertucci, Cesar
Coates, Andrew
Cravens, Thomas
Dandouras, Iannis
Shemansky, Don
BE Brown, RH
Lebreton, JP
Waite, JH
TI Energy Deposition Processes in Titan's Upper Atmosphere and Its Induced
Magnetosphere
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID FAR-ULTRAVIOLET SPECTROPHOTOMETRY; POLYCYCLIC AROMATIC-HYDROCARBONS;
CASSINI PLASMA SPECTROMETER; FULLERENE RADICAL CATIONS; STRUCTURE
INSTRUMENT HASI; MAGNETIC-FIELD; SATURNS MAGNETOSPHERE; E-RING;
ELECTRICAL-CONDUCTIVITY; DUST MEASUREMENTS
AB Most of Titan's atmospheric organic and nitrogen chemistry, aerosol formation, and atmospheric loss are driven from external energy sources such as Solar UV, Saturn's magnetosphere, solar wind and galactic cosmic rays. The Solar UV tends to dominate the energy input at lower altitudes similar to 1,200 km but which can extend down to similar to 400 km, while the plasma interaction from Saturn's magnetosphere, Saturn's magnetosheath or solar wind are more important at higher altitudes similar to 1,400 km, but the heavy ion plasma (O+) similar to 5 keV and energetic ions (H+) similar to 30 keV or higher from Saturn's magnetosphere can penetrate below 950 km. Cosmic rays with energies >1 GeV can penetrate much deeper into Titan's atmosphere with most of its energy deposited similar to 70 km altitude. Haze layers are observed in scattered solar photons starting at 510 km, but aerosols are broadly distributed and measured in extinction from 1,000 km downward, diffusively separated to 400 km. The induced magnetic field from Titan's interaction with the external plasma can be very complex and will tend to channel the flow of energy into Titan's upper atmosphere. Cassini observations combined with advanced hybrid simulations of the plasma interaction with Titan's upper atmosphere show significant changes in the character of the interaction with Saturn local time at Titan's orbit where the magnetosphere displays large and systematic changes with local time. The external solar wind can also drive sub-storms within the magnetosphere which can then modify the magnetospheric interaction with Titan. Another important parameter is solar zenith angle (SZA) with respect to the co-rotation direction of the magnetospheric flow which is referred to as the solar incidence-ram angle. Titan's interaction can contribute to atmospheric loss via pickup ion loss, scavenging of Titan's ionospheric plasma, loss of ionospheric plasma down its induced magnetotail via an ionospheric wind, and non-thermal loss of the atmosphere via heating and sputtering induced by the bombardment of magnetospheric keV ions and electrons. This energy input evidently drives the large positive and negative ions observed below similar to 1,100 km altitude with ion masses exceeding 10,000 Da. We refer to these ions as seed particles for the aerosols observed below 1,000 km altitude. These seed particles can be formed, for example, from the polymerization of acetylene (C2H2) and benzene (C6H6) molecules in Titan's upper atmosphere to form polycyclic aromatic hydrocarbons (PAH) and/or fullerenes (C-60). In the case of fullerenes, which are hollow spherical carbon shells, magnetospheric keV O+ ions can become trapped inside the fullerenes and eventually find themselves inside the aerosols as free oxygen. The aerosols are then expected to fall to Titan's surface as polymerized hydrocarbons with trapped free oxygen where unknown surface chemistry can take place.
C1 [Sittler, Edward C.; Hartle, R. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bertucci, Cesar] Inst Astron & Space Phys IAFE, Buenos Aires, DF, Argentina.
[Coates, Andrew] UCL, Mullard Space Sci Lab, London WC1E 6BT, England.
[Cravens, Thomas] Univ Kansas, Lawrence, KS 66045 USA.
[Dandouras, Iannis] Ctr Etud Spatiale Rayonnements Lab, CNRS, Toulouse, France.
[Shemansky, Don] Univ So Calif, Dept Aerosp & Mech Engn, Los Angeles, CA USA.
RP Sittler, EC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Edward.C.Sittler@nasa.gov
RI Coates, Andrew/C-2396-2008
OI Coates, Andrew/0000-0002-6185-3125
NR 213
TC 40
Z9 40
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 393
EP 453
DI 10.1007/978-1-4020-9215-2_16
PG 61
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300016
ER
PT B
AU Hansen, CJ
Waite, JH
Bolton, SJ
AF Hansen, C. J.
Waite, J. H.
Bolton, S. J.
BE Brown, RH
Lebreton, JP
Waite, JH
TI Titan in the Cassini-Huygens Extended Mission
SO TITAN FROM CASSINI-HUYGENS
LA English
DT Article; Book Chapter
ID ATMOSPHERIC TEMPERATURES; RADAR OBSERVATIONS; LANDING SITE; SURFACE;
WINDS; SPECTROMETER; TOPOGRAPHY; IMAGES; ETHANE; OCEAN
C1 [Hansen, C. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Waite, J. H.; Bolton, S. J.] SW Res Inst, San Antonio, TX 78238 USA.
RP Hansen, CJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Candice.j.Hansen@jpl.nasa.gov
NR 43
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-1-4020-9214-5
PY 2009
BP 455
EP 477
DI 10.1007/978-1-4020-9215-2_17
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BMN07
UT WOS:000272894300017
ER
PT B
AU Makeev, MA
Lawson, JW
Srivastava, D
AF Makeev, Maxim A.
Lawson, John W.
Srivastava, Deepak
GP TMS
TI KINETICS OF FORMATION AND THERMAL AND MECHANICAL PROPERTIES OF CHAR
OBTAINED BY ULTRA-HIGH TEMPERATURE PYROLYSIS OF POLYETHYLENE VIA
MOLECULAR DYNAMICS SIMULATIONS
SO TMS 2009 138TH ANNUAL MEETING & EXHIBITION - SUPPLEMENTAL PROCEEDINGS,
VOL 2: MATERIALS CHARACTERIZATION, COMPUTATION AND MODELING
LA English
DT Proceedings Paper
CT 138th TMS Annual Meeting and Exhibition
CY FEB 15-19, 2009
CL San Francisco, CA
DE pyrolytic char; atomistic simulations; elastic properties; thermal
conductivity
ID FLAMMABILITY PROPERTIES; CONDUCTIVITY; NANOCOMPOSITES; NETWORKS; FILMS
AB We report results of a molecular dynamics simulation study of the high-temperature pyrolysis of polyethylene (PE) and the mechanical and thermal properties of the resultant carbonaceous char. The microstructure of pyrolyzed PE samples was monitored during the simulation. Mechanical properties of the resultant char were studied for char samples with varied microstructure (average coordination number and ring-size distributions) to establish structure-property relationships between mechanical (thermal) response properties and microstructure. We found that this relationship can be established based upon the random network theory of amorphous media, if additional topological constraints due to rings are taken into account. Thermal conductivity of pyrolytic char is investigated for samples with different microstructures for a wide range of temperatures. Similar to the mechanical response, the thermal response properties are correlated to microstructure. It is shown that the behavior of the thermal conductivity can be well described by Einstein's heat transfer theory, if microstructure effecs are taken into account.
C1 [Makeev, Maxim A.; Lawson, John W.; Srivastava, Deepak] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Makeev, MA (reprint author), NASA, Ames Res Ctr, Mail Stop 229-1, Moffett Field, CA 94035 USA.
NR 14
TC 0
Z9 0
U1 4
U2 10
PU MINERALS, METALS & MATERIALS SOC
PI WARRENDALE
PA 184 THORN HILL RD, WARRENDALE, PA 15086-7514 USA
BN 978-0-87339-739-1
PY 2009
BP 79
EP 86
PG 8
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering; Materials Science, Characterization & Testing; Mineralogy
SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy
GA BJC16
UT WOS:000264674700011
ER
PT S
AU Rowe, JF
Matthews, JM
Seager, S
Sasselov, D
Kuschnig, R
Guenther, DB
Moffat, AFJ
Rucinski, SM
Walker, GAH
Weiss, WW
AF Rowe, Jason F.
Matthews, Jaymie M.
Seager, Sara
Sasselov, Dimitar
Kuschnig, Rainer
Guenther, David B.
Moffat, Anthony F. J.
Rucinski, Slavek M.
Walker, Gordon A. H.
Weiss, Werner W.
BE Pont, F
Sasselov, D
Holman, M
TI Towards the Albedo of an Exoplanet: MOST Satellite Observations of
Bright Transiting Exoplanetary Systems
SO TRANSITING PLANETS, PROCEEDINGS
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 253th Symposium of the International-Astronomical-Union
CY MAY 19-23, 2008
CL Cambridge, MA
SP Int Astron Union
ID HD 209458B; ATMOSPHERES; PHOTOMETRY; CLOUDS; SPACE
AB The Canadian MOST satellite is a unique platform for observations of bright transiting exoplanetary systems. Providing nearly continuous photometric observations for lip to 4 weeks, MOST can produce important observational data, to hell) us learn about the properties of exosolar planets. We review our current, observations of HD 209458 and HD 189733 with implications for the albedo and our progress towards detecting reflected light from an exoplanet.
C1 [Rowe, Jason F.; Matthews, Jaymie M.; Seager, Sara; Sasselov, Dimitar; Kuschnig, Rainer; Guenther, David B.; Moffat, Anthony F. J.; Rucinski, Slavek M.; Walker, Gordon A. H.; Weiss, Werner W.] NASA, Moffett Field, CA 94035 USA.
RP Rowe, JF (reprint author), NASA, Ames Res Pk,MS-244-30, Moffett Field, CA 94035 USA.
EM jasonfrowe@gmail.com; matthews@astro.ubc.ca; seager@mit.edu;
dsasselov@cfa.harvard.edu; dsasselov@cfa.harvard.edu
NR 11
TC 0
Z9 0
U1 0
U2 0
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND
SN 1743-9213
BN 978-0-521-88984-1
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2009
VL 4
IS 253
BP 121
EP 127
DI 10.1017/S1743921308026318
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJD37
UT WOS:000264979500014
ER
PT S
AU Deming, D
AF Deming, Drake
BE Pont, F
Sasselov, D
Holman, M
TI Emergent Exoplanet Flux: Review of the Spitzer Results
SO TRANSITING PLANETS, PROCEEDINGS
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 253th Symposium of the International-Astronomical-Union
CY MAY 19-23, 2008
CL Cambridge, MA
SP Int Astron Union
ID PLANET HD 189733B; TRANSITING EXTRASOLAR PLANET; HOT JUPITERS;
SPACE-TELESCOPE; ATMOSPHERIC CIRCULATION; THERMAL EMISSION; INFRARED
RADIUS; 209458B; SPECTRUM; WATER
AB Observations using the Spitzer Space Telescope provided the first; detections of photons from extrasolar planets. Spitzer observations are allowing us to infer the temperature structure, composition, and dynamics of exoplanet atmospheres. The Spitzer studies extend from many hot Jupiters to the hot Neptune orbiting GJ 436. Here I review the current status of Spitzer secondary eclipse observations, and summarize the results from the viewpoint, of what is robust, what needs more work, and what the observations are telling us about the physical nature of exoplanet atmospheres.
C1 NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.
RP Deming, D (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Code 693, Greenbelt, MD 20771 USA.
EM ddeming@pop600.gsfc.nasa.gov
NR 43
TC 0
Z9 0
U1 0
U2 0
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND
SN 1743-9213
BN 978-0-521-88984-1
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2009
VL 4
IS 253
BP 197
EP 207
DI 10.1017/S1743921308026410
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJD37
UT WOS:000264979500023
ER
PT S
AU Borucki, W
Koch, D
Batalha, N
Caldwell, D
Christensen-Dalsgaard, J
Cochran, WD
Dunham, E
Gautier, TN
Geary, J
Gilliland, R
Jenkins, J
Kjeldsen, H
Lissauer, JJ
Rowe, J
AF Borucki, William
Koch, David
Batalha, Natalie
Caldwell, Douglas
Christensen-Dalsgaard, Jorgen
Cochran, William D.
Dunham, Edward
Gautier, Thomas N.
Geary, John
Gilliland, Ronald
Jenkins, Jon
Kjeldsen, Hans
Lissauer, Jack J.
Rowe, Jason
BE Pont, F
Sasselov, D
Holman, M
TI KEPLER: Search for Earth-Size Planets in the Habitable Zone
SO TRANSITING PLANETS, PROCEEDINGS
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 253th Symposium of the International-Astronomical-Union
CY MAY 19-23, 2008
CL Cambridge, MA
SP Int Astron Union
ID PHOTOMETRIC-METHOD; COMPANION; SYSTEMS; STARS
AB The Kepler Mission is a space-based mission whose primary goal is to determine the frequency of Earth-size and larger planets in the habitable zone of solar-like stars. The mission will monitor more than 100,000 stars for patterns of transits with a differential photometric precision of 20 ppm at V = 12 for a 6.5 hour transit. It will also provide asteroseismic results on several thousand dwarf stars. It is specifically designed to continuously observe a single field of view of greater than 100 square degrees for 3.5 or more years.
This paper provides a short overview of the mission, a brief history of the mission development, expected results, new investigations by the recently chosen Participating Scientists, and the plans for the Guest Observer and Astrophysical Data, Programs.
C1 [Borucki, William; Koch, David; Lissauer, Jack J.; Rowe, Jason] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Borucki, W (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM henry.w.daniels-l@nasa.gov; dkoch@mail.arc.nasa.gov;
Thomas.N.Gautier@jpl.nasa.gov; gillil@stsci.edu; hans@phys.au.dk;
jlissauer@mail.arc.nasa.gov; jasonfrowe@gmail.com
RI Caldwell, Douglas/L-7911-2014
OI Caldwell, Douglas/0000-0003-1963-9616
NR 21
TC 5
Z9 5
U1 1
U2 1
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND
SN 1743-9213
BN 978-0-521-88984-1
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2009
VL 4
IS 253
BP 289
EP 299
DI 10.1017/S1743921308026513
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJD37
UT WOS:000264979500033
ER
PT S
AU Iro, N
Deming, D
AF Iro, Nicolas
Deming, Drake
BE Pont, F
Sasselov, D
Holman, M
TI A time-dependent radiative model for the atmosphere of the eccentric
transiting planets
SO TRANSITING PLANETS, PROCEEDINGS
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 253th Symposium of the International-Astronomical-Union
CY MAY 19-23, 2008
CL Cambridge, MA
SP Int Astron Union
AB We present a time-dependent radiative model for the atmosphere of the transiting planets that takes into account the eccentricity of their orbit. We investigate the temporal temperature and flux variations due to the planet-star distance variability. We will also discuss observational aspects with Spitzer measurements.
C1 [Iro, Nicolas; Deming, Drake] NASA, GSFC Planetary Syst Lab Code 693 0, Greenbelt, MD 20770 USA.
RP Iro, N (reprint author), NASA, GSFC Planetary Syst Lab Code 693 0, Greenbelt, MD 20770 USA.
EM nicolas.iro@nasa.gov; leo.d.deming@nasa.gov
NR 7
TC 0
Z9 0
U1 0
U2 0
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND
SN 1743-9213
BN 978-0-521-88984-1
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2009
VL 4
IS 253
BP 516
EP 519
DI 10.1017/S1743921308027099
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJD37
UT WOS:000264979500090
ER
PT S
AU O'Donovan, FT
Charbonneau, D
Harrington, J
Seager, S
Deming, D
Knutson, HA
AF O'Donovan, Francis T.
Charbonneau, David
Harrington, Joseph
Seager, Sara
Deming, Drake
Knutson, Heather A.
BE Pont, F
Sasselov, D
Holman, M
TI Detection of Planetary Emission from TrES-2 using Spitzer/IRAC
SO TRANSITING PLANETS, PROCEEDINGS
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 253th Symposium of the International-Astronomical-Union
CY MAY 19-23, 2008
CL Cambridge, MA
SP Int Astron Union
ID TRANSITS; PROJECT
AB We present here results from observations of TrES-2 made using the Infrared Array Camera on the Spitzer Space Telescope. We monitored this transiting system during two secondary eclipses, when the planetary emission is blocked by the star. The resulting decrease in flux is 0.135 +/- 0.036%, 0.245 +/- 0.027%, 0.162 +/- 0.064%, and 0.295 +/- 0.066%, at 3.6-mu m, 4.5-mu m, 5.8-mu m, and 8.0-mu m, respectively. We find evidence for a temperature inversion in the atmosphere of TrES-2. which is predicted by Fortney and collaborators based on the proposed importance of TiO and VO opacities for this highly irradiated gas giant. We also find the time of the center of the eclipse to be consistent with predictions from transit timing observations of TrES-2. This implies that TrES-2 most likely has a circular orbit, and thus does not obtain additional thermal energy from tidal dissipation of a non-zero orbital eccentricity, a proposed explanation of the large planetary radius.
C1 [O'Donovan, Francis T.; Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP O'Donovan, FT (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM francis.odonovan@nasa.gov; dcharbonneau@cfa.harvard.edu;
jh@physics.ucf.edu; seager@mit.edu; leo.d.deming@nasa.gov;
hknutson@cfa.harvard.edu
OI Charbonneau, David/0000-0002-9003-484X
NR 8
TC 0
Z9 0
U1 0
U2 0
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND
SN 1743-9213
BN 978-0-521-88984-1
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2009
VL 4
IS 253
BP 536
EP 539
DI 10.1017/S1743921308027142
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJD37
UT WOS:000264979500095
ER
PT J
AU Ducluzeau, AL
van Lis, R
Duval, S
Schoepp-Cothenet, B
Russell, MJ
Nitschke, W
AF Ducluzeau, Anne-Lise
van Lis, Robert
Duval, Simon
Schoepp-Cothenet, Barbara
Russell, Michael J.
Nitschke, Wolfgang
TI Was nitric oxide the first deep electron sink?
SO TRENDS IN BIOCHEMICAL SCIENCES
LA English
DT Review
ID COPPER OXYGEN REDUCTASES; CYTOCHROME-C-OXIDASE; ACTIVE-SITE RESIDUE;
NITROGEN-FIXATION; CBB(3) OXIDASES; OXIDATION-STATE; EARLY EVOLUTION;
EARLY EARTH; ATMOSPHERE; REDOX
AB Evolutionary histories of enzymes involved in chemiosmotic energy conversion indicate that a strongly oxidizing substrate was available to the last universal common ancestor before the divergence of Bacteria and Archaea. According to palaeogeochemical evidence, 02 was not present beyond trace amounts on the early Earth. Based on recent phylogenetic, enzymatic and geochemical results, we propose that, in the earliest Archaean, nitric oxide (NO) and its derivatives nitrate and nitrite served as strongly oxidizing substrates driving the evolution of a bioenergetic pathway related to modern dissimilatory denitrification. Aerobic respiration emerged later from within this ancestral pathway via adaptation of the enzyme NO reductase to its new substrate, dioxygen.
C1 [Ducluzeau, Anne-Lise; van Lis, Robert; Duval, Simon; Schoepp-Cothenet, Barbara; Nitschke, Wolfgang] CNRS, Lab Bioenerget & Ingn Prot, UPR9036, IFR77, F-13402 Marseille 20, France.
[Russell, Michael J.] CALTECH, Jet Prop Lab, Sect 3220, Pasadena, CA 91109 USA.
RP Nitschke, W (reprint author), CNRS, Lab Bioenerget & Ingn Prot, UPR9036, IFR77, 31 Chemin Joseph Aiguier, F-13402 Marseille 20, France.
EM nitschke@ibsm.cnrs-mrs.fr
OI Nitschke, Wolfgang/0000-0003-2084-3032
FU French Agence Nationale pour la Recherche [ANR-06-BLAN-0384]; National
Aeronautics and Space Administration
FX We thank Christaphe Leger (Marseille) and Chris Boxe (Jet Propulsion
Laboratory) for stimulating discussions, Our work was financially
supported by the French Agence Nationale pour la Recherche
(ANR-06-BLAN-0384 and ERRMoE; www.agence-nationale-recherche.fr).
M.J.R.'s research described here was carried out at the Jet Propulsion
Laboratory, California Institute of Technology (www.jpl.nasa.gov) under
a contract with the National Aeronautics and Space Administration
(www.nasa.gov).
NR 49
TC 68
Z9 69
U1 3
U2 25
PU ELSEVIER SCIENCE LONDON
PI LONDON
PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND
SN 0968-0004
J9 TRENDS BIOCHEM SCI
JI Trends Biochem.Sci.
PD JAN
PY 2009
VL 34
IS 1
BP 9
EP 15
DI 10.1016/j.tibs.2008.10.005
PG 7
WC Biochemistry & Molecular Biology
SC Biochemistry & Molecular Biology
GA 402HY
UT WOS:000263006000006
PM 19008107
ER
PT J
AU Dellacorte, C
AF Dellacorte, Christopher
TI History's ultimate lube job
SO TRIBOLOGY & LUBRICATION TECHNOLOGY
LA English
DT Article
C1 NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Dellacorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
EM christopher.dellocorte@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS
PI PARK RIDGE
PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA
SN 1545-858X
J9 TRIBOL LUBR TECHNOL
JI Tribol. Lubr. Technol.
PD JAN
PY 2009
VL 65
IS 1
BP 26
EP 27
PG 2
WC Engineering, Mechanical
SC Engineering
GA 397RL
UT WOS:000262679700008
ER
PT J
AU Stanford, MK
AF Stanford, Malcolm K.
TI Dimensional Stability, Microstructure, and Cohesion Strength of
Composite Solid Lubricant Coatings after Heat Treatment
SO TRIBOLOGY TRANSACTIONS
LA English
DT Article
DE Plasma Spray Coatings; Lubrication; Cohesion; Metallography; Oxidation
ID TEMPERATURE; PS304
AB PS304 is a plasma spray deposited coating composed of Ni-Cr, Cr(2)O(3), Ag, and BaF(2)-CaF(2) that has been developed for reduction of friction and wear at high temperatures. Physical properties of the coating after varying heat treatments and using varying weight percentages of chromium in the Ni-Cr constituent have been investigated. Dimensional stability was reduced with increasing heat treatment temperature and the coating growth rate decreased with time. The dimensional stability was also reduced as the Cr content in the Ni-Cr constituent increased from 10 to 30 wt%. Coating growth was due to oxidation of the Ni-Cr constituent. The optimum cohesion strength for PS304 was essentially the same after heat treatment at 650 or 725 degrees C for 100 h. Further investigation indicated that heat treatment at 725 degrees C for 100 h increases the dimensional stability in a high temperature service environment.
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Stanford, MK (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 14
TC 1
Z9 1
U1 1
U2 2
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 1040-2004
J9 TRIBOL T
JI Tribol. Trans.
PY 2009
VL 52
IS 2
BP 269
EP 276
DI 10.1080/10402000802527781
PG 8
WC Engineering, Mechanical
SC Engineering
GA 424GR
UT WOS:000264554600004
ER
PT J
AU Morales, W
Handschuh, RF
Krantz, TL
AF Morales, Wilfredo
Handschuh, Robert F.
Krantz, Timothy L.
TI Feasibility Study of Vapor-Mist Phase Reaction Lubrication using a
Thioether Liquid
SO TRIBOLOGY TRANSACTIONS
LA English
DT Article
DE Gears; Vapor Phase Lubrication
ID IRON
AB Aerospace drive systems are required to survive a loss-of-lubrication test for qualification. In many cases emergency lubrication systems need to be designed and utilized to permit the drive system to pass this difficult requirement. The weight of emergency systems can adversely affect the mission capabilities of the aircraft. The possibility to reduce the emergency system weight using vapor-mist phase lubrication (VMPL) technology has been considered by NASA and the Army Research Laboratory (ARL). Phosphate esters have been the lubricant of choice in most VMPL studies primarily because they do provide adequate lubrication for short periods of time. However, during the lubrication process, the phosphate esters react continuously with the surface iron in gears and bearings, resulting in excessive wear. To minimize this problem an alternative non-phosphate liquid, a thioether, was used to mist phase lubricate a spur gearbox rig operating at 10,000 rpm under highly loaded conditions. After 21 million shaft revolutions of operation the gears exhibited only minor wear.
C1 [Morales, Wilfredo] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Handschuh, Robert F.; Krantz, Timothy L.] US Army Res Lab, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Morales, W (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 11
TC 1
Z9 2
U1 0
U2 3
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 1040-2004
J9 TRIBOL T
JI Tribol. Trans.
PY 2009
VL 52
IS 3
BP 370
EP 375
DI 10.1080/10402000802563448
PG 6
WC Engineering, Mechanical
SC Engineering
GA 424GS
UT WOS:000264554700004
ER
PT J
AU Oswald, FB
Zaretsky, EV
Poplawski, JV
AF Oswald, Fred B.
Zaretsky, Erwin V.
Poplawski, Joseph V.
TI Interference-Fit Life Factors for Roller Bearings
SO TRIBOLOGY TRANSACTIONS
LA English
DT Article
DE Interference Fit; Cylindrical Roller Bearings; Rolling Bearings; Fatigue
Analysis; Contacts; Life Prediction Methods; Maintenance; Rolling
Bearings; Rolling-Contact Fatigue; Wear; Stress Analysis; Contacts
ID PREDICTION; PROFILE
AB The effect of hoop stresses in reducing cylindrical roller bearing fatigue life was determined for various classes of inner-ring interference fit. Calculations were performed for up to seven fit classes for each of the 10 bearing sizes. The hoop stresses were superimposed on the Hertzian principal stresses created by the applied radial load to calculate roller bearing fatigue life. A method was developed through a series of equations to calculate the life reduction for cylindrical roller bearings. All calculated lives are for zero initial internal clearance. Any reduction in bearing clearance due to interference fit would be compensated by increasing the initial (unmounted) clearance. The results are presented as tables and charts of life factors for bearings with light, moderate, and heavy loads and interference fits ranging from extremely light to extremely heavy for bearing accuracy class RBEC-5 (ISO class 5). Interference fits on the inner ring of a cylindrical roller bearing can significantly reduce bearing fatigue life. In general, life factors are smaller (lower life) for bearings running under a light load where the unfactored life is the highest. The various bearing series within a particular bore size had almost identical interference-fit life factors for a particular fit. The tightest fit at the high end of the tolerance band produces a life factor of approximately 0.40 for an inner-race maximum Hertz stress of 1200 MPa (175 ksi) and a life factor of 0.60 for an inner-race maximum Hertz stress of 2200 MPa (320 ksi). Interference fits also impact the maximum Hertz stress-life relation.
C1 [Oswald, Fred B.; Zaretsky, Erwin V.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Poplawski, Joseph V.] JV Poplawski & Associates, Bethlehem, PA 18018 USA.
RP Oswald, FB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
NR 19
TC 6
Z9 8
U1 0
U2 4
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 1040-2004
J9 TRIBOL T
JI Tribol. Trans.
PY 2009
VL 52
IS 4
BP 415
EP 426
AR PII 910296043
DI 10.1080/10402000802687890
PG 12
WC Engineering, Mechanical
SC Engineering
GA 434VK
UT WOS:000265302000001
ER
PT J
AU Miller, BA
Howard, SA
AF Miller, Brad A.
Howard, Samuel A.
TI Identifying Bearing Rotor-Dynamic Coefficients Using an Extended Kalman
Filter
SO TRIBOLOGY TRANSACTIONS
LA English
DT Article
DE Hydrodynamic Bearings; Journal Bearings; Dynamic Modeling
ID 2 JOURNAL BEARINGS; SUPPORT PARAMETERS; FIELD METHODS; IDENTIFICATION;
RESPONSES
AB An extended Kalman filter is developed to estimate the linearized direct and indirect stiffness and damping force coefficients for bearings in rotor-dynamic applications from noisy measurements of the shaft displacement in response to imbalance and impact excitation. The bearing properties are modeled as stochastic random variables using a Gauss-Markov model. Noise terms are introduced into the system model to account for all of the estimation error, including modeling errors and uncertainties and the propagation of measurement errors into the parameter estimates. The system model contains two user-defined parameters that can be tuned to improve the filter's performance; these parameters correspond to the covariance of the system and measurement noise variables. The filter is also strongly influenced by the initial values of the states and the error covariance matrix. The filter is demonstrated using numerically simulated data for a rotor-bearing system with two identical bearings, which reduces the number of unknown linear dynamic coefficients to eight. The filter estimates the direct damping coefficients and all four stiffness coefficients correlated well with actual values, whereas the estimates the cross-coupled damping coefficients were the least accurate.
C1 [Miller, Brad A.] Harding Univ, Dept Engn & Phys, Searcy, AR 72149 USA.
[Howard, Samuel A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Miller, BA (reprint author), Harding Univ, Dept Engn & Phys, 915 E Market Ave, Searcy, AR 72149 USA.
FU NASA [NNC06GA20G]
FX The material is based upon work supported by NASA under award No.
NNC06GA20G.
NR 19
TC 2
Z9 2
U1 0
U2 1
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 1040-2004
J9 TRIBOL T
JI Tribol. Trans.
PY 2009
VL 52
IS 5
BP 671
EP 679
AR PII 913558721
DI 10.1080/10402000902913295
PG 9
WC Engineering, Mechanical
SC Engineering
GA 481RZ
UT WOS:000268830700003
ER
PT S
AU Goldstein, ML
AF Goldstein, Melvyn L.
BE Hasan, SS
Gangadhara, RT
Krishan, V
TI Observations and Modeling of Turbulence in the Solar Wind
SO TURBULENCE, DYNAMOS, ACCRETION DISKS, PULSARS AND COLLECTIVE PLASMA
PROCESSES
SE Astrophysics and Space Science Proceedings
LA English
DT Proceedings Paper
CT 1st Kodai-Trieste Workshop on Plasma Astrophysics
CY AUG 27-SEP 07, 2007
CL Kodaikanal, INDIA
SP Indian Inst Astrophys, Kodaikanal Observatory, Abdus Salam Int Ctr Theoret Phys
DE Magnetohydrodynamics-solar wind; Turbulence-simulations
ID INTERPLANETARY MAGNETIC-FIELD; FLUX-CORRECTED TRANSPORT;
MAGNETOHYDRODYNAMIC FLUCTUATIONS; HELIOS OBSERVATIONS; VELOCITY SHEAR;
ALFVEN WAVES; EVOLUTION; SIMULATION; ANISOTROPY; LATITUDES
AB Alfvenic fluctuations are a ubiquitous component of the solar wind. Evidence from many spacecrafts indicate that the fluctuations are convected out of the solar corona with relatively flat power spectra and constitute a source of free energy for a turbulent cascade of magnetic and kinetic energy to high wave numbers. Observations and simulations support the conclusion that the cascade evolves most, rapidly in the vicinity of velocity shears and current sheets. Numerical solutions of the magnetohydrodynamic equations have elucidated the role of expansion on the evolution of the turbulence. Such studies are clarifying not only how a turbulent cascade develops, but, also the nature of the symmetries of the turbulence.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Goldstein, ML (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM melvyn.l.goldstein@nasa.gov
RI Goldstein, Melvyn/B-1724-2008
NR 44
TC 1
Z9 1
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 1570-6591
BN 978-1-4020-8867-4
J9 ASTROPHYSICS SPACE
PY 2009
BP 21
EP 33
PG 13
WC Astronomy & Astrophysics; Physics, Fluids & Plasmas
SC Astronomy & Astrophysics; Physics
GA BIY36
UT WOS:000263688100002
ER
PT S
AU Chiuderi, C
Velli, M
AF Chiuderi, C.
Velli, M.
BE Vlahos, L
Cargill, P
TI Solar MHD: An Introduction
SO TURBULENCE IN SPACE PLASMAS
SE Lecture Notes in Physics
LA English
DT Article; Book Chapter
ID ALFVEN WAVES; MAGNETOHYDRODYNAMIC TURBULENCE; CORONA; ENERGY; FIELDS;
LOOPS
C1 [Chiuderi, C.] Univ Florence, Dipartimento Astron, I-50125 Florence, Italy.
[Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Chiuderi, C (reprint author), Univ Florence, Dipartimento Astron, Largo Enrico Fermi 5, I-50125 Florence, Italy.
EM chiuderi@arcetri.astro.it; velli@arcetri.astro.it
NR 38
TC 0
Z9 0
U1 1
U2 2
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0075-8450
BN 978-3-642-00209-0
J9 LECT NOTES PHYS
PY 2009
VL 778
BP 45
EP 69
DI 10.1007/978-3-642-00210-6_2
D2 10.1007/978-3-642-00210-6
PG 25
WC Astronomy & Astrophysics; Physics, Fluids & Plasmas
SC Astronomy & Astrophysics; Physics
GA BJZ20
UT WOS:000267515600003
ER
PT S
AU Velli, M
AF Velli, M.
BE Vlahos, L
Cargill, P
TI Physical Processes in the Solar Wind
SO TURBULENCE IN SPACE PLASMAS
SE Lecture Notes in Physics
LA English
DT Article; Book Chapter
ID INTERPLANETARY ALFVENIC FLUCTUATIONS; MHD TURBULENCE;
MAGNETOHYDRODYNAMIC TURBULENCE; HYDROMAGNETIC TURBULENCE; STELLAR WINDS;
CORONAL HOLE; WAVES; ATMOSPHERE; EVOLUTION; DYNAMICS
C1 [Velli, M.] Univ Florence, Dipartimento Astron, I-50125 Florence, Italy.
[Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Velli, M (reprint author), Univ Florence, Dipartimento Astron, Largo Enrico Fermi 5, I-50125 Florence, Italy.
EM velli@arcetri.astro.it
NR 51
TC 1
Z9 1
U1 1
U2 1
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0075-8450
BN 978-3-642-00209-0
J9 LECT NOTES PHYS
PY 2009
VL 778
BP 247
EP 268
DI 10.1007/978-3-642-00210-6_7
D2 10.1007/978-3-642-00210-6
PG 22
WC Astronomy & Astrophysics; Physics, Fluids & Plasmas
SC Astronomy & Astrophysics; Physics
GA BJZ20
UT WOS:000267515600008
ER
PT B
AU Kurylo, MJ
AF Kurylo, Michael J.
BE Zerefos, C
Contopoulos, G
Skalkeas, G
TI The Role of Airborne Science in the Study of Polar Ozone
SO TWENTY YEARS OF OZONE DECLINE
LA English
DT Proceedings Paper
CT Symposium for the 20th Anniversary of the Montreal Protocol 2007
CY SEP, 2007
CL Athens, GREECE
SP United Nat Environm Programme, Int Ozone Commiss, Acad Athens, Mariolopoulos-Kanaginis Fdn
DE Airborne science; integrated observations; ozone depletion; ozone hole;
Polar Ozone
ID ANTARCTICA
AB This chapter will provide a brief historical perspective of the Antarctic ozone hole and the role that 1986-1987 ground-based and aircraft studies played in linking its formation to reactions involving chlorine and bromine radicals resulting from the degradation of halocarbon source gases (emitted in large part from human activities). The results from later aircraft campaigns focused oil understanding ozone production and loss within the Arctic stratosphere will also be highlighted. These results affirm the continuing need in ozone research for the integration of synoptic scale satellite measurements with ground-based, balloon-borne, and aircraft measurements having a unique temporal and spatial resolution.
C1 NASA Headquarters, Sci Miss Directorate, Washington, DC USA.
RP Kurylo, MJ (reprint author), NASA Headquarters, Sci Miss Directorate, Washington, DC USA.
EM Michael.J.Kurylo@nasa.gov
RI Kurylo, Michael/H-2201-2012
NR 2
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-90-481-2468-8
PY 2009
BP 173
EP 182
DI 10.1007/978-90-481-2469-5_12
PG 10
WC Geochemistry & Geophysics; Environmental Sciences; Meteorology &
Atmospheric Sciences
SC Geochemistry & Geophysics; Environmental Sciences & Ecology; Meteorology
& Atmospheric Sciences
GA BKP72
UT WOS:000268885100012
ER
PT B
AU Bhartia, PK
AF Bhartia, Pawan K.
BE Zerefos, C
Contopoulos, G
Skalkeas, G
TI Role of Satellite Measurements in the Discovery of Stratospheric Ozone
Depletion
SO TWENTY YEARS OF OZONE DECLINE
LA English
DT Proceedings Paper
CT Symposium for the 20th Anniversary of the Montreal Protocol 2007
CY SEP, 2007
CL Athens, GREECE
SP United Nat Environm Programme, Int Ozone Commiss, Acad Athens, Mariolopoulos-Kanaginis Fdn
DE Ozone hole; satellite algorithm; TOMS; total ozone; UVB
AB This chapter discusses the role satellite total ozone measuring instruments have played in the study of stratospheric ozone depletion. By the early 1980s total ozone measured from two NASA satellites had produced a record that spanned more than a decade, with quality comparable with best ground-based stations. It was therefore a puzzle to many why NASA did not report the discovery of the Antarctic ozone depletion until late 1985. This was initially described as a computer error and continues to be described that way in both scientific and popular media. This simplistic labelling has unfortunately served to hide deeper issues about the ability of satellite instruments in making new scientific discoveries as the nature of the satellite retrieval problems make them critically dependent on the availability of prior information. Lack of such prior information and the unavailability of "ground-truth" data were key contributing factors that caused the delay in reporting the discovery of the Antarctic ozone hole, though it was clearly seen in the data by the summer of 1984. The strength of the satellite instruments is their capability to expand the limited view provided by ground-based and aircraft instruments into a global view. This view played a crucial role in making the public and policy makers aware of the seriousness of the ozone depletion problem that led to the phase-out of the ozone-destroying chemicals. This case is even stronger for the surface UV radiation where large spatial and temporal variability due to clouds and aerosols make it very difficult to see patterns in the data without the perspective that only satellites can provide.
C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
RP Bhartia, PK (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
EM Pawiin.Bhartia@nast.gov
RI Bhartia, Pawan/A-4209-2016
OI Bhartia, Pawan/0000-0001-8307-9137
NR 13
TC 0
Z9 0
U1 0
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-90-481-2468-8
PY 2009
BP 183
EP 189
DI 10.1007/978-90-481-2469-5_13
PG 7
WC Geochemistry & Geophysics; Environmental Sciences; Meteorology &
Atmospheric Sciences
SC Geochemistry & Geophysics; Environmental Sciences & Ecology; Meteorology
& Atmospheric Sciences
GA BKP72
UT WOS:000268885100013
ER
PT B
AU Newman, PA
Nash, ER
Douglass, AR
Nielsen, JE
Stolarski, RS
AF Newman, Paul A.
Nash, Eric R.
Douglass, Anne R.
Nielsen, J. Eric
Stolarski, Richard S.
BE Zerefos, C
Contopoulos, G
Skalkeas, G
TI Estimating When the Antarctic Ozone Hole will Recover
SO TWENTY YEARS OF OZONE DECLINE
LA English
DT Proceedings Paper
CT Symposium for the 20th Anniversary of the Montreal Protocol 2007
CY SEP, 2007
CL Athens, GREECE
SP United Nat Environm Programme, Int Ozone Commiss, Acad Athens, Mariolopoulos Kanaginis Fdn
DE Antarctic; ozone depletion; ozone hole; recovery; stratosphere
ID CHLORINE; LOSSES
AB The Antarctic ozone hole develops during the Austral winter and reaches its deepest levels by early spring (late September to early October). The severity of the hole has been assessed from satellites by calculating the average aerial coverage of depletion during the September-October period. Profile information shows that ozone is completely destroyed in the 14-21 km layer by early October. This ozone is mainly destroyed by halogen (chlorine and bromine) catalytic cycles, and these losses are modulated by temperature variations.
Because atmospheric halogen levels are responding to international agreements that limit or phase out production, the amount of halogens in the stratosphere should considerably decrease over the next few decades. Using projections of halogen levels combined with age-of-air estimates, we find that the ozone hole is recovering at an extremely slow rate and that large ozone holes will regularly recur over the next 2 decades. We estimate that the ozone hole will begin to show first signs of area decrease in about 2023, and the hole will fully recover to pre-1980 levels in approximately 2070. Estimates of the ozone hole's recovery from models reveal important uncertainties in recovery as a result of climate change.
C1 [Newman, Paul A.; Douglass, Anne R.; Stolarski, Richard S.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Code 613-3, Greenbelt, MD 20771 USA.
[Nash, Eric R.; Nielsen, J. Eric] Sci Syst & Appl Inc, Lanham, MD 20706 USA.
RP Newman, PA (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Code 613-3, Greenbelt, MD 20771 USA.
EM Paul.A.Newman@nasa.gov
RI Newman, Paul/D-6208-2012; Douglass, Anne/D-4655-2012; Stolarski,
Richard/B-8499-2013
OI Newman, Paul/0000-0003-1139-2508; Stolarski, Richard/0000-0001-8722-4012
FU NASA
FX This analysis work was mainly supported under a NASA grant for the
Atmospheric Chemistry and Analysis Program (ACMAP), while the GEOS CCM
modeling work was supported under a grant from the NASA Modeling,
Analysis and Prediction (MAP) Program
NR 24
TC 0
Z9 1
U1 1
U2 14
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-90-481-2468-8
PY 2009
BP 191
EP +
DI 10.1007/978-90-481-2469-5_14
PG 3
WC Geochemistry & Geophysics; Environmental Sciences; Meteorology &
Atmospheric Sciences
SC Geochemistry & Geophysics; Environmental Sciences & Ecology; Meteorology
& Atmospheric Sciences
GA BKP72
UT WOS:000268885100014
ER
PT B
AU Douglass, AR
AF Douglass, Anne R.
BE Zerefos, C
Contopoulos, G
Skalkeas, G
TI Global Observations-The Key to Model Development and Improved
Assessments
SO TWENTY YEARS OF OZONE DECLINE
LA English
DT Proceedings Paper
CT Symposium for the 20th Anniversary of the Montreal Protocol 2007
CY SEP, 2007
CL Athens, GREECE
SP United Nat Environm Programme, Int Ozone Commiss, Acad Athens, Mariolopoulos-Kanaginis Fdn
DE Constituent correlations; numerical transport; stratospheric
constituents; stratospheric models
ID CONSTITUENT TRANSPORT CALCULATIONS; NITROUS-OXIDE; TOTAL OZONE;
STRATOSPHERE; CHEMISTRY; SCHEME
AB The stratospheric models used to predict changes in the ozone due to changes in the atmospheric composition and climate have developed from the one-dimensional models of the 1970s to the three-dimensional models ill use today. Observations have played an obvious key role in model development, as they lead to the development and refinement of the conceptual model that underlies the computational model used in prediction. Observations also played another role. For example, a model failure to produce observed correlations between long-lived constituents in the lower stratosphere first led to an improvement in the numerical scheme transport algorithm and then inspired changes in the approach used to solve the equations of motion in a general circulation model. This led to improvements in several aspects of the simulation, including realistic propagation of the tape recorder signature in the tropical water vapor and a realistic distribution for lower stratospheric age-of-air.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Douglass, AR (reprint author), NASA, Goddard Space Flight Ctr, Code 613-3, Greenbelt, MD 20771 USA.
EM Anne.R.Douglass@nasa.gov
RI Douglass, Anne/D-4655-2012
NR 32
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-90-481-2468-8
PY 2009
BP 251
EP 259
DI 10.1007/978-90-481-2469-5_18
PG 9
WC Geochemistry & Geophysics; Environmental Sciences; Meteorology &
Atmospheric Sciences
SC Geochemistry & Geophysics; Environmental Sciences & Ecology; Meteorology
& Atmospheric Sciences
GA BKP72
UT WOS:000268885100018
ER
PT B
AU Schoeberl, MR
Rodriguez, JM
AF Schoeberl, Mark R.
Rodriguez, Jose M.
BE Zerefos, C
Contopoulos, G
Skalkeas, G
TI The Rise and Fall of Dynamical Theories of the Ozone Hole
SO TWENTY YEARS OF OZONE DECLINE
LA English
DT Proceedings Paper
CT Symposium for the 20th Anniversary of the Montreal Protocol 2007
CY SEP, 2007
CL Athens, GREECE
SP United Nat Environm Programme, Int Ozone Commiss, Acad Athens, Mariolopoulos Kanaginis Fdn
DE Antarctic lower stratosphere; observations ozone hole; ozone hole
theory; TOMS
ID ANTARCTIC TOTAL-OZONE; STRATOSPHERIC TEMPERATURE; SATELLITE
MEASUREMENTS; DEPLETION; CHLORINE; STATION; TRENDS; VAPOR; HCL
AB During the late 1980's the appearance of the rapid spring decrease in Antarctic stratospheric ozone (the ozone hole) produced a large number of hypotheses. The two main contenders were the chemical hypothesis involving unmeasured chemical reactions, and the dynamical hypothesis involving a potential systematic change in Antarctic circulation. The strong observed correlation between column ozone changes and lower stratospheric temperature trends gave weight to the dynamical theory. However, after pioneering ground based and aircraft observations, it became clear that the Antarctic circulation was not changing during the column ozone decrease period as predicted by the dynamical hypothesis. These same observations showed significant chemical changes in the Antarctic lower stratosphere, which, along with focused laboratory chemical measurements showed that a variation of the original the chemical hypothesis explained the ozone hole phenomena.
C1 [Schoeberl, Mark R.; Rodriguez, Jose M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Schoeberl, MR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM mark.r.schoeberl@nasa.gov
RI Rodriguez, Jose/G-3751-2013
OI Rodriguez, Jose/0000-0002-1902-4649
NR 32
TC 0
Z9 0
U1 1
U2 3
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-90-481-2468-8
PY 2009
BP 263
EP +
DI 10.1007/978-90-481-2469-5_19
PG 4
WC Geochemistry & Geophysics; Environmental Sciences; Meteorology &
Atmospheric Sciences
SC Geochemistry & Geophysics; Environmental Sciences & Ecology; Meteorology
& Atmospheric Sciences
GA BKP72
UT WOS:000268885100019
ER
PT S
AU Davila, JM
Gopalswamy, N
Thompson, BJ
AF Davila, Joseph M.
Gopalswamy, Nat
Thompson, Barbara J.
BE Gopalswamy, N
Webg, DF
TI Universal processes in heliophysics
SO UNIVERSAL HELIOPHYSICAL PROCESSES
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 257th Symposium of the International-Astronomical-Union
CY SEP 15-19, 2008
CL Ioannina, GREECE
SP Int Astron Union, Univ Ioannina, Greek Minist Educ & Religious Affairs, Greek Minist Culture, Int Heliophys Year, NASA
DE Sun: general; interplanetary medium; solar system: general
AB The structure of the Universe is determined primarily by the interplay of gravity which is dominant in condensed objects, and the magnetic force which is dominant in the rarefied medium between condensed objects. Each of these forces orders the matter into a, set of characteristic structures each with the ability to store and release energy in response to changes in the external environment. For the most part, the storage and release of energy proceeds through a number of Universal Processes. The coordinated study of these processes in different settings provides a deeper understanding of the underlying physics governing Universal Processes in astrophysics.
C1 [Davila, Joseph M.; Gopalswamy, Nat; Thompson, Barbara J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Davila, JM (reprint author), NASA, Goddard Space Flight Ctr, Code 670, Greenbelt, MD 20771 USA.
EM Joseph.M.Davila@nasa.gov; Nat.Gopalswamy@nasa.gov;
Barbara.J.Thompson@nasa.gov; Nat.Gopalswamy@nasa.gov
RI Gopalswamy, Nat/D-3659-2012; Thompson, Barbara/C-9429-2012
NR 5
TC 1
Z9 1
U1 0
U2 1
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND
SN 1743-9213
BN 978-0-521-88988-9
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2009
VL 4
IS 257
BP 11
EP 16
DI 10.1017/S1743921309029032
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJH42
UT WOS:000265828300002
ER
PT S
AU Gopalswamy, N
Akiyama, S
Yashiro, S
AF Gopalswamy, N.
Akiyama, S.
Yashiro, S.
BE Gopalswamy, N
Webg, DF
TI Major solar flares without coronal mass ejections
SO UNIVERSAL HELIOPHYSICAL PROCESSES
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 257th Symposium of the International-Astronomical-Union
CY SEP 15-19, 2008
CL Ioannina, GREECE
SP Int Astron Union, Univ Ioannina, Greek Minist Educ & Religious Affairs, Greek Minist Culture, Int Heliophys Year, NASA
DE coronal mass ejections (CMEs); flares; particle emission; radio
radiation
ID ASSOCIATION
AB We examine the source properties of X-class soft X-ray flares that were not associated with coronal mass ejections (CMEs). All the Hares were associated with intense microwave bursts implying the production of high energy electrons. However, most (85%) of the flares were not associated with metric type III bursts, even though open field lines existed in all but two of the active regions. The X-class flares seem to be truly confined because there was no material ejection (thermal or nonthermal) away from the flaring region into space.
C1 [Gopalswamy, N.; Akiyama, S.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM nat.gopalswamy@nasa.gov; sachiko.akiyama@nasa.gov;
seiji.yashiro@nasa.gov
RI Gopalswamy, Nat/D-3659-2012
NR 11
TC 3
Z9 3
U1 0
U2 2
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND
SN 1743-9213
BN 978-0-521-88988-9
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2009
VL 4
IS 257
BP 283
EP 286
DI 10.1017/S174392130902941X
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJH42
UT WOS:000265828300037
ER
PT S
AU MacDowall, RJ
Richardson, IG
Hess, RA
Thejappa, G
AF MacDowall, R. J.
Richardson, I. G.
Hess, R. A.
Thejappa, G.
BE Gopalswamy, N
Webg, DF
TI Re-examining the correlation of complex solar type III radio bursts and
solar energetic particles
SO UNIVERSAL HELIOPHYSICAL PROCESSES
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 257th Symposium of the International-Astronomical-Union
CY SEP 15-19, 2008
CL Ioannina, GREECE
SP Int Astron Union, Univ Ioannina, Greek Minist Educ & Religious Affairs, Greek Minist Culture, Int Heliophys Year, NASA
DE acceleration of particles; shock waves; Sun: radio radiation; Sun:
coronal mass ejections (CMEs); Sun: flares
ID ACCELERATION; ELECTRONS; EVENTS
AB Interplanetary radio observations provide important information on particle acceleration processes at the Sun and propagation of the accelerated particles in the solar wind. Cane et al. (2002) have drawn attention to a, class of prominent radio bursts that accompany > 20 MeV solar proton events. They call these bursts 'type III-L' because: they are fast, drifting (like normal type III bursts associated with electrons accelerated at impulsive solar flares); they are Long-lasting compared to normal type III bursts: they occur Late compared to the onset of the related solar event; and, they commence at Lower frequencies (similar to 100 MHz) than normal type III bursts, suggesting that they originate higher in the corona at similar to 0.5 R(s) above the Sun. We report, on all analysis of the correlated radio and SEP events during 1996-2006 using the Wind Waves and near-Earth SEP data sets, and discuss whether the characteristics of the complex type III bursts (at less than 14 MHz) will permit them to serve as proxies for SEP event occurrence and intensity.
C1 [MacDowall, R. J.; Richardson, I. G.; Hess, R. A.; Thejappa, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP MacDowall, RJ (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA.
EM robert.macdowall@nasa.gov; ian.g.richardson@nasa.gov;
roger.hess@nasa.gov; thejappa.golla@nasa.gov
RI MacDowall, Robert/D-2773-2012; Gopalswamy, Nat/D-3659-2012;
OI Richardson, Ian/0000-0002-3855-3634
NR 11
TC 1
Z9 1
U1 0
U2 0
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND
SN 1743-9213
BN 978-0-521-88988-9
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2009
VL 4
IS 257
BP 335
EP 340
DI 10.1017/S1743921309029512
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJH42
UT WOS:000265828300046
ER
PT S
AU Grebowsky, JM
Aikin, AC
AF Grebowsky, Joseph M.
Aikin, Arthur C.
BE Gopalswamy, N
Webg, DF
TI Planetary ionospheres - sources and dynamic drivers
SO UNIVERSAL HELIOPHYSICAL PROCESSES
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 257th Symposium of the International-Astronomical-Union
CY SEP 15-19, 2008
CL Ioannina, GREECE
SP Int Astron Union, Univ Ioannina, Greek Minist Educ & Religious Affairs, Greek Minist Culture, Int Heliophys Year, NASA
DE earth; meteors; meteoroids; planets and satellites: general; magnetic
fields
ID RADIO OCCULTATIONS; MARS; ATMOSPHERE; JUPITER; EUROPA; VENUS
AB External energy inputs into all planetary tipper atmospheres (including more than a half dozen moons with atmospheres) are comprised of combinations of solar EUV, soft x-rays, solar energetic particles, solar wind charged particles, magnetospherically accelerated particles, solar wind electric field, interplanetary dust particles as well as propagating lower atmosphere disturbances. Each input, has analogous physical interactions with all planetary ionospheres and upper atmospheres, but the integrated consequences of the multiple energy inputs vary from planet to planet. The Earth forms the framework for most fundamental processes because of extensive measurements of the effects of each of the inputs. However the conditions at Earth are far different from those at the carbon dioxide atmosphere of magnetic field-free, slow-rotating Venus, the carbon dioxide atmosphere of Mars with patchy remnant magnetic fields, while the outer planets have hydrogen atmospheres, are fast rotating with intrinsic magnetic fields, and encompass moons that interact with the magnetospheres and have exotic atmospheres. Although the physical processes are known, our understanding of our solar system's ionospheres diminishes with increasing distance from the Sun.
C1 [Grebowsky, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Grebowsky, JM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM joseph.m.grebowsky@nasa.gov; aaikin1@verizon.net
RI Gopalswamy, Nat/D-3659-2012; Grebowsky, Joseph/I-7185-2013
NR 19
TC 0
Z9 0
U1 0
U2 1
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND
SN 1743-9213
BN 978-0-521-88988-9
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2009
VL 4
IS 257
BP 499
EP 510
DI 10.1017/S1743921309029780
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJH42
UT WOS:000265828300069
ER
PT S
AU Rankin, AL
Huertas, A
Matthies, LH
AF Rankin, Arturo L.
Huertas, Andres
Matthies, Larry H.
BE Gerhart, GR
Gage, DW
Shoemaker, CM
TI Stereo vision based terrain mapping for off-road autonomous navigation
SO UNMANNED SYSTEMS TECHNOLOGY XI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Unmanned Systems Technology XI
CY APR 17-17, 2009
CL Orlando, FL
SP SPIE
DE Terrain mapping; stereo vision; passive perception; autonomous
navigation
ID MAP
AB Successful off-road autonomous navigation by an unmanned ground vehicle (UGV) requires reliable perception and representation of natural terrain. While perception algorithms are used to detect driving hazards, terrain mapping algorithms are used to represent the detected hazards in a world model a UGV can use to plan safe paths. There are two primary ways to detect driving hazards with perception sensors mounted to a UGV: binary obstacle detection and traversability cost analysis. Binary obstacle detectors label terrain as either traversable or non-traversable, whereas, traversability cost analysis assigns a cost to driving over a discrete patch of terrain. In uncluttered environments where the non-obstacle terrain is equally traversable, binary obstacle detection is sufficient. However, in cluttered environments, some form of traversability cost analysis is necessary. The Jet Propulsion Laboratory (JPL) has explored both approaches using stereo vision systems. A set of binary detectors has been implemented that detect positive obstacles, negative obstacles, tree trunks, tree lines, excessive slope, low overhangs, and water bodies. A compact terrain map is built from each frame of stereo images. The mapping algorithm labels cells that contain obstacles as no-go regions, and encodes terrain elevation, terrain classification, terrain roughness, traversability cost, and a confidence value. The single frame maps are merged into a world map where temporal filtering is applied. In previous papers, we have described our perception algorithms that perform binary obstacle detection. In this paper, we summarize the terrain mapping capabilities that JPL has implemented during several UGV programs over the last decade and discuss some challenges to building terrain maps with stereo range data.
C1 [Rankin, Arturo L.; Huertas, Andres; Matthies, Larry H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rankin, AL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 23
TC 5
Z9 5
U1 0
U2 6
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-7598-5
J9 PROC SPIE
PY 2009
VL 7332
AR 733210
DI 10.1117/12.819099
PG 17
WC Computer Science, Artificial Intelligence; Computer Science, Information
Systems; Robotics; Optics
SC Computer Science; Robotics; Optics
GA BVS50
UT WOS:000292646300024
ER
PT J
AU Jones, JA
Ciftcioglu, N
Schmid, JF
Barr, YR
Griffith, D
AF Jones, Jeffrey A.
Ciftcioglu, Neva
Schmid, Josef F.
Barr, Yael R.
Griffith, Donald
TI Calcifying Nanoparticles (Nanobacteria): An Additional Potential Factor
for Urolithiasis in Space Flight Crews
SO UROLOGY
LA English
DT Article
ID KIDNEY-STONE FORMATION; METABOLISM; CALCIUM; DISEASE
AB Space flight-induced microgravity appears to be a risk factor for the development of urinary calculi, resulting in urolithiasis during and after spaceflight. Calcifying nanoparticles, or nanobacteria, multiply more rapidly in simulated microgravity and create external shells of calcium phosphate. The question arises whether calcifying nanoparticles are nidi for calculi and contribute to the development of clinically significant urolithiasis in those who are predisposed to the development Of urinary calculi because of intrinsic or extrinsic factors. This case report describes a calculus recovered after flight from an astronaut that, on morphologic and immunochemical analysis (including specific monoclonal antibody staining), demonstrated characteristics of calcifying nanoparticles. UROLOGY 73: 210.e11-210.e13, 2009. (C) 2009 Elsevier Inc.
C1 [Jones, Jeffrey A.] NASA, Lyndon B Johnson Space Ctr, SD, Houston, TX 77058 USA.
Baylor Coll Med, Houston, TX 77030 USA.
Vet Affairs Med Ctr, Houston, TX 77030 USA.
Univ Texas Med Branch, Galveston, TX USA.
RP Jones, JA (reprint author), NASA, Lyndon B Johnson Space Ctr, SD, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM jeffrey.a.jones@nasa.gov
NR 15
TC 5
Z9 6
U1 0
U2 6
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0090-4295
J9 UROLOGY
JI Urology
PD JAN
PY 2009
VL 73
IS 1
AR 210.e11
DI 10.1016/j.urology.2008.01.033
PG 3
WC Urology & Nephrology
SC Urology & Nephrology
GA 393NJ
UT WOS:000262379700054
PM 18718644
ER
PT B
AU Kouveliotou, C
AF Kouveliotou, C.
BE Stanek, KZ
TI Bohdan Paczynski and Gamma-Ray Bursts
SO VARIABLE UNIVERSE: A CELEBRATION OF BOHDAN PACZYNSKI
SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES
LA English
DT Proceedings Paper
CT Symposium on the Variable Universe - A Celebration of Bohdan Paczynski
CY SEP 29-30, 2007
CL Princeton Univ, Princeton, NJ
HO Princeton Univ
ID EMISSION PROPERTIES; SPECTRAL CATALOG; HUBBLE DIAGRAM; RADIO;
SUPERNOVAE; AFTERGLOW; BATSE; DISCOVERY; REDSHIFT; ORIGIN
C1 NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA.
RP Kouveliotou, C (reprint author), NASA, George C Marshall Space Flight Ctr, NSSTC, 320 Sparkman Dr, Huntsville, AL 35805 USA.
NR 63
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-682-0
J9 ASTR SOC P
PY 2009
VL 403
BP 150
EP 170
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BJC81
UT WOS:000264849400010
ER
PT B
AU Spera, DA
AF Spera, David A.
BE Spera, DA
TI Introduction to Modern Wind Turbines
SO WIND TURBINE TECHNOLOGY: FUNDAMENTAL CONCEPTS OF WIND TURBINE
ENGINEERING, SECOND EDITION
LA English
DT Editorial Material; Book Chapter
C1 [Spera, David A.] NASA, Wind Energy Projects, Glenn Res Ctr, Cleveland, OH USA.
[Spera, David A.] DASCON Engn LLC, Bonita Springs, FL USA.
RP Spera, DA (reprint author), DASCON Engn LLC, Bonita Springs, FL USA.
NR 15
TC 2
Z9 2
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-0260-1
PY 2009
BP 47
EP 103
DI 10.1115/1.802601.ch2
D2 10.1115/1.802601
PG 57
WC Energy & Fuels; Engineering, Mechanical
SC Energy & Fuels; Engineering
GA BGT44
UT WOS:000324080100002
ER
PT B
AU Hubbard, HH
Shepherd, KP
AF Hubbard, Harvey H.
Shepherd, Kevin P.
BE Spera, DA
TI Wind Turbine Acoustics
SO WIND TURBINE TECHNOLOGY: FUNDAMENTAL CONCEPTS OF WIND TURBINE
ENGINEERING, SECOND EDITION
LA English
DT Article; Book Chapter
ID NOISE
C1 [Hubbard, Harvey H.; Shepherd, Kevin P.] NASA Langley Res Ctr, Hampton, VA USA.
RP Hubbard, HH (reprint author), NASA Langley Res Ctr, Hampton, VA USA.
NR 61
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-0260-1
PY 2009
BP 413
EP 465
DI 10.1115/1.802601.ch7
D2 10.1115/1.802601
PG 53
WC Energy & Fuels; Engineering, Mechanical
SC Energy & Fuels; Engineering
GA BGT44
UT WOS:000324080100009
ER
PT B
AU Thresher, RW
Mirandy, LP
Carne, TG
Lobitz, DW
James, GH
AF Thresher, Robert W.
Mirandy, Louis P.
Carne, Thomas G.
Lobitz, Donald W.
James, George H., III
BE Spera, DA
TI Structural Dynamic Behavior of Wind Turbines
SO WIND TURBINE TECHNOLOGY: FUNDAMENTAL CONCEPTS OF WIND TURBINE
ENGINEERING, SECOND EDITION
LA English
DT Article; Book Chapter
ID BLADE
C1 [Thresher, Robert W.] Natl Renewable Energy Lab, Golden, CO USA.
[Mirandy, Louis P.] GE Co, King Of Prussia, PA USA.
[Carne, Thomas G.; Lobitz, Donald W.] Sandia Natl Labs, Albuquerque, NM 87185 USA.
[James, George H., III] NASA Johnson Space Ctr, Houston, TX USA.
RP Thresher, RW (reprint author), Natl Renewable Energy Lab, Golden, CO USA.
NR 41
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-0260-1
PY 2009
BP 605
EP 662
DI 10.1115/1.802601.ch11
D2 10.1115/1.802601
PG 58
WC Energy & Fuels; Engineering, Mechanical
SC Energy & Fuels; Engineering
GA BGT44
UT WOS:000324080100013
ER
PT B
AU Spera, DA
AF Spera, David A.
BE Spera, DA
TI Fatigue Design of Wind Turbines
SO WIND TURBINE TECHNOLOGY: FUNDAMENTAL CONCEPTS OF WIND TURBINE
ENGINEERING, SECOND EDITION
LA English
DT Article; Book Chapter
C1 [Spera, David A.] NASA, Wind Energy Projects, Glenn Res Ctr, Cleveland, OH USA.
[Spera, David A.] DASCON Engn LLC, Bonita Springs, FL USA.
RP Spera, DA (reprint author), DASCON Engn LLC, Bonita Springs, FL USA.
NR 66
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-0260-1
PY 2009
BP 663
EP 719
DI 10.1115/1.802601.ch12
D2 10.1115/1.802601
PG 57
WC Energy & Fuels; Engineering, Mechanical
SC Energy & Fuels; Engineering
GA BGT44
UT WOS:000324080100014
ER
PT J
AU Banks, ME
McEwen, AS
Kargel, JS
Baker, VR
Strom, RG
Mellon, MT
Gulick, VC
Keszthelyi, L
Herkenhoff, KE
Pelletier, JD
Jaeger, WL
AF Banks, Maria E.
McEwen, Alfred S.
Kargel, Jeffrey S.
Baker, Victor R.
Strom, Robert G.
Mellon, Michael T.
Gulick, Virginia C.
Keszthelyi, Laszlo
Herkenhoff, Kenneth E.
Pelletier, Jon D.
Jaeger, Windy L.
TI High Resolution Imaging Science Experiment (HiRISE) observations of
glacial and periglacial morphologies in the circum-Argyre Planitia
highlands, Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID ORBITER LASER ALTIMETER; NORTH-POLAR CAP; VALLES MARINERIS; ROCK
GLACIERS; DEBRIS APRONS; ICE; DEPOSITS; HISTORY; WATER; FLOW
AB The landscape of the Argyre Planitia and adjoining Charitum and Nereidum Montes in the southern hemisphere of Mars has been heavily modified since formation of the Argyre impact basin. This study examines morphologies in the Argyre region revealed in images acquired by the High Resolution Imaging Science Experiment ( HiRISE) camera and discusses the implications for glacial and periglacial processes. Distinctive features such as large grooves, semicircular embayments in high topography, and streamlined hills are interpreted as glacially eroded grooves, cirques, and whalebacks or roche moutonnee, respectively. Large boulders scattered across the floor of a valley may be ground moraine deposited by ice ablation. Glacial interpretations are supported by the association of these features with other landforms typical of glaciated landscapes such as broad valleys with parabolic cross sections and stepped longitudinal profiles, lobate debris aprons interpreted as remnant debris covered glaciers or rock glaciers, and possible hanging valleys. Aligned boulders observed on slopes may also indicate glacial processes such as fluting. Alternatively, boulders aligned on slopes and organized in clumps and polygonal patterns on flatter surfaces may indicate periglacial processes, perhaps postglaciation, that form patterned ground. At least portions of the Argyre region appear to have been modified by processes of ice accumulation, glacial flow, erosion, sediment deposition, ice stagnation and ablation, and perhaps subsequent periglacial processes. The type of bedrock erosion apparent in images suggests that glaciers were, at times, wet based. The number of superposed craters is consistent with geologically recent glacial activity, but may be due to subsequent modification.
C1 [Banks, Maria E.; Pelletier, Jon D.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[McEwen, Alfred S.; Strom, Robert G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Kargel, Jeffrey S.; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Mellon, Michael T.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Gulick, Virginia C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gulick, Virginia C.] SETI Inst, Moffett Field, CA 94035 USA.
[Keszthelyi, Laszlo; Herkenhoff, Kenneth E.; Jaeger, Windy L.] USGS, Astrogeol Team, Flagstaff, AZ 86001 USA.
RP Banks, ME (reprint author), Univ Arizona, Dept Geosci, 1040 E 4th St, Tucson, AZ 85721 USA.
EM mbanks@email.arizona.edu
RI Mellon, Michael/C-3456-2016
FU NASA
FX We gratefully acknowledge the invaluable assistance of the entire HiRISE
team, including the software developers, the uplink and downlink teams,
and the science team. This paper also benefited from detailed reviews by
G. Komatsu and an anonymous reviewer. This work was supported by the
NASA Mars Reconnaissance Orbiter project managed through the California
Institute of Technology's Jet Propulsion Laboratory.
NR 86
TC 26
Z9 26
U1 2
U2 11
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 DEC 31
PY 2008
VL 113
IS E12
AR E12015
DI 10.1029/2007JE002994
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 390OC
UT WOS:000262172600001
ER
PT J
AU Hashimoto, GL
Roos-Serote, M
Sugita, S
Gilmore, MS
Kamp, LW
Carlson, RW
Baines, KH
AF Hashimoto, George L.
Roos-Serote, Maarten
Sugita, Seiji
Gilmore, Martha S.
Kamp, Lucas W.
Carlson, Robert W.
Baines, Kevin H.
TI Felsic highland crust on Venus suggested by Galileo Near-Infrared
Mapping Spectrometer data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID RADAR REFLECTIVITY; DEEP ATMOSPHERE; LANDING SITES; SURFACE; WATER;
NIGHTSIDE; EARTH; REFLECTANCE; MAGELLAN; CLIMATE
AB We evaluated the spatial variation of Venusian surface emissivity at 1.18 mu m wavelength and that of near-surface atmospheric temperature using multispectral images obtained by the Near-Infrared Mapping Spectrometer (NIMS) on board the Galileo spacecraft. The Galileo NIMS observed the nightside thermal emission from the surface and the deep atmosphere of Venus, which is attenuated by scattering from the overlying clouds. To analyze the NIMS data, we used a radiative transfer model based on the adding method. Although there is still an uncertainty in the results owing to the not well known parameters of the atmosphere, our analysis revealed that the horizontal temperature variation in the near-surface atmosphere is no more than +/- 2 K on the Venusian nightside and also suggests that the majority of lowlands likely has higher emissivity compared to the majority of highlands. One interpretation for the latter result is that highland materials are generally composed of felsic rocks. Since formation of a large body of granitic magmas requires water, the presence of granitic terrains would imply that Venus may have had an ocean and a mechanism to recycle water into the mantle in the past.
C1 [Hashimoto, George L.] Kobe Univ, Org Adv Sci & Technol, Lab Earth & Planetary Atmospher Sci, Nada Ku, Kobe, Hyogo 6578501, Japan.
[Kamp, Lucas W.; Carlson, Robert W.; Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilmore, Martha S.] Wesleyan Univ, Dept Earth & Environm Sci, Middletown, CT 06459 USA.
[Roos-Serote, Maarten] Lisbon Astron Observ, P-1349018 Lisbon, Portugal.
[Sugita, Seiji] Univ Tokyo, Grad Sch Frontier Sci, Dept Complex Sci & Engn, Chiba 2778561, Japan.
RP Hashimoto, GL (reprint author), Kobe Univ, Org Adv Sci & Technol, Lab Earth & Planetary Atmospher Sci, Nada Ku, 1-1 Rokkodai, Kobe, Hyogo 6578501, Japan.
EM george@kobe-u.ac.jp; maarten@lightcurvefilms.com;
sugita@k.u-tokyo.ac.jp; mgilmore@wesleyan.edu; lwk@mipl.jpl.nasa.gov;
rcarlson@lively.jpl.nasa.gov; kbaines@scn.jpl.nasa.gov
RI Gilmore, Martha/G-5856-2011; HASHIMOTO, George/B-1529-2011
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT);
Portuguese FCT [PDCTE/FNU/49822/2003, BSAB/584/2006]
FX The authors express their thanks to anonymous reviewers for their
constructive comments on this manuscript. G. L. H. would like to thank
Teruyuki Nakajima for detailed discussion of radiative transfer
modeling, Naomoto Iwagami for helpful discussion of gas absorption,
Yutaka Abe for fruitful discussion of early evolution of terrestrial
planets, Yukari Tsutsumi for her help in developing computational code,
and Constantine Tsang for his technical aid in preparing figures. G. L.
H. and S. S. thank Grants-in-Aid for Scientific Research and The 21st
Century COE Program of Origin and Evolution of Planetary Systems of
Ministry of Education, Culture, Sports, Science and Technology (MEXT)
for support. M. R. S. is supported by Portuguese FCT project
PDCTE/FNU/49822/2003 and FCT scholarship BSAB/584/2006.
NR 65
TC 28
Z9 28
U1 2
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 31
PY 2008
VL 113
AR E00B24
DI 10.1029/2008JE003134
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 390NX
UT WOS:000262172100001
ER
PT J
AU Andre, N
Blanc, M
Maurice, S
Schippers, P
Pallier, E
Gombosi, TI
Hansen, KC
Young, DT
Crary, FJ
Bolton, S
Sittler, EC
Smith, HT
Johnson, RE
Baragiola, RA
Coates, AJ
Rymer, AM
Dougherty, MK
Achilleos, N
Arridge, CS
Krimigis, SM
Mitchell, DG
Krupp, N
Hamilton, DC
Dandouras, I
Gurnett, DA
Kurth, WS
Louarn, P
Srama, R
Kempf, S
Waite, HJ
Esposito, LW
Clarke, JT
AF Andre, N.
Blanc, M.
Maurice, S.
Schippers, P.
Pallier, E.
Gombosi, T. I.
Hansen, K. C.
Young, D. T.
Crary, F. J.
Bolton, S.
Sittler, E. C.
Smith, H. T.
Johnson, R. E.
Baragiola, R. A.
Coates, A. J.
Rymer, A. M.
Dougherty, M. K.
Achilleos, N.
Arridge, C. S.
Krimigis, S. M.
Mitchell, D. G.
Krupp, N.
Hamilton, D. C.
Dandouras, I.
Gurnett, D. A.
Kurth, W. S.
Louarn, P.
Srama, R.
Kempf, S.
Waite, H. J.
Esposito, L. W.
Clarke, J. T.
TI IDENTIFICATION OF SATURN'S MAGNETOSPHERIC REGIONS AND ASSOCIATED PLASMA
PROCESSES: SYNOPSIS OF CASSINI OBSERVATIONS DURING ORBIT INSERTION
SO REVIEWS OF GEOPHYSICS
LA English
DT Review
ID NEUTRAL MASS-SPECTROMETER; KILOMETRIC RADIATION; ROTATION PERIOD;
SOLAR-WIND; IO TORUS; THERMAL PLASMA; ENCELADUS; RADIO; FIELD; DYNAMICS
AB Saturn's magnetosphere is currently studied from the microphysical to the global scale by the Cassini-Huygens mission. During the first half of 2004, in the approach phase, remote sensing observations of Saturn's magnetosphere gave access to its auroral, radio, UV, energetic neutral atom, and dust emissions. Then, on 1 July 2004, Cassini Saturn orbit insertion provided us with the first in situ exploration of Saturn's magnetosphere since Voyager. To date, Saturn orbit insertion is the only Cassini orbit to have been described in common by all field and particle instruments. We use the comprehensive suite of magnetospheric and plasma science instruments to give a unified description of the large-scale structure of the magnetosphere during this particular orbit, identifying the different regions and their boundaries. These regions consist of the Saturnian ring system region 1, within 3 Saturn radii R-S)) and the cold plasma torus region 2, within 5-6 R-S) in the inner magnetosphere, a dynamic and extended plasma sheet region 3), and an outer high-latitude magnetosphere region 4, beyond 12-14 R-S). We compare these observations to those made at the time of the Voyager encounters. Then, we identify some of the dominant chemical characteristics and dynamical phenomena in each of these regions. The inner magnetosphere is characterized by the presence of the dominant plasma and neutral sources of the Saturnian system, giving birth to a very special magnetosphere dominated by water products. The extended plasma sheet, where the ring current resides, is a variable region with stretched magnetic field lines and contains a mixture of cold and hot plasma populations resulting from plasma transport processes. The outer high-latitude magnetosphere is characterized by a quiet magnetic field and an absence of plasma. Saturn orbit insertion observations enabled us to capture a snapshot of the large-scale structure of the Saturnian magnetosphere and of some of the main plasma processes operating in this complex environment. The analysis of the broad diversity of these interaction processes will be one of the main themes of magnetospheric and plasma science during the Cassini mission.
C1 [Andre, N.] European Space Agcy, Res & Sci Support Dept, NL-2200 Noordwijk, Netherlands.
[Dougherty, M. K.; Achilleos, N.; Arridge, C. S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England.
[Smith, H. T.; Johnson, R. E.; Baragiola, R. A.] Univ Virginia, Engn Phys Program, Charlottesville, VA 22904 USA.
[Smith, H. T.; Johnson, R. E.; Baragiola, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Blanc, M.; Maurice, S.; Schippers, P.; Pallier, E.; Dandouras, I.; Louarn, P.] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France.
[Young, D. T.; Crary, F. J.; Bolton, S.; Waite, H. J.] SW Res Inst, San Antonio, TX 78238 USA.
[Clarke, J. T.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Coates, A. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Esposito, L. W.] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Gombosi, T. I.; Hansen, K. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
[Gurnett, D. A.; Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Hamilton, D. C.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Srama, R.; Kempf, S.] Max Planck Nucl Phys, D-69117 Heidelberg, Germany.
[Rymer, A. M.; Krimigis, S. M.; Mitchell, D. G.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Krupp, N.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Sittler, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Andre, N (reprint author), European Space Agcy, Res & Sci Support Dept, Keplerlaan 1,POB 299, NL-2200 Noordwijk, Netherlands.
EM nandre@rssd.esa.int
RI Arridge, Christopher/A-2894-2009; Gombosi, Tamas/G-4238-2011; Achilleos,
Nicholas/C-1647-2008; Hansen, Kenneth/F-3693-2011; Clarke,
John/C-8644-2013; Coates, Andrew/C-2396-2008; Smith, Howard/H-4662-2016
OI Arridge, Christopher/0000-0002-0431-6526; Gombosi,
Tamas/0000-0001-9360-4951; Dandouras, Iannis/0000-0002-7121-1118; KEMPF,
SASCHA/0000-0001-5236-3004; Hamilton, Douglas/0000-0001-6103-8019;
Achilleos, Nicholas/0000-0002-5886-3509; Kurth,
William/0000-0002-5471-6202; Hansen, Kenneth/0000-0002-8502-1980;
Coates, Andrew/0000-0002-6185-3125; Smith, Howard/0000-0003-3537-3360
FU Science and Technology Facilities Council [PP/D00084X/1]
NR 119
TC 13
Z9 13
U1 3
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 8755-1209
EI 1944-9208
J9 REV GEOPHYS
JI Rev. Geophys.
PD DEC 31
PY 2008
VL 46
IS 4
AR RG4008
DI 10.1029/2007RG000238
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 390PF
UT WOS:000262175500001
ER
PT J
AU Bozzolo, G
Mosca, HO
del Grosso, MF
AF Bozzolo, G.
Mosca, H. O.
del Grosso, M. F.
TI Surface structure and composition of Ni-Ti alloys and their influence on
the temperature-dependent segregation behavior
SO APPLIED SURFACE SCIENCE
LA English
DT Article
DE Surface Segregation; Ni-Ti alloys; Computer simulation; Semi-empirical
methods
ID SHAPE-MEMORY ALLOY; OXIDATION BEHAVIOR; LAYER
AB Atomistic modeling of segregation in Ni-Ti alloys is performed using the Bozzolo-Ferrante-Smith (BFS) method for alloys. It is found that Ti segregation to the surface decreases rapidly even for small increases in Ni concentration. A competing process is identified in the vicinity of surface defects, leading to excess Ti coverage of the exposed surface and the creation of Ti-covered pits. A simple explanation based on an atom-by-atom energy analysis is found to satisfactorily explain the observed effects. (C) 2008 Elsevier B.gV. All rights reserved.
C1 [Bozzolo, G.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Bozzolo, G.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Mosca, H. O.; del Grosso, M. F.] UA Fis, Comis Nacl Energia Atom, San Martin, Argentina.
[Mosca, H. O.; del Grosso, M. F.] FRG Pacheco, GCMM, UTN, Gral Pacheco, Argentina.
RP Bozzolo, G (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
EM GuillermoBozzolo@oai.org
FU NASA Fundamental Aeronautics
FX Fruitful discussions with N. Bozzolo are gratefully acknowledged. This
work was partially sponsored by the NASA Fundamental Aeronautics
NR 19
TC 2
Z9 2
U1 1
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-4332
J9 APPL SURF SCI
JI Appl. Surf. Sci.
PD DEC 30
PY 2008
VL 255
IS 5
BP 3004
EP 3010
DI 10.1016/j.apsusc.2008.08.060
PG 7
WC Chemistry, Physical; Materials Science, Coatings & Films; Physics,
Applied; Physics, Condensed Matter
SC Chemistry; Materials Science; Physics
GA 378CR
UT WOS:000261299200078
ER
PT J
AU Jiang, X
Li, QB
Liang, MC
Shia, RL
Chahine, MT
Olsen, ET
Chen, LL
Yung, YL
AF Jiang, Xun
Li, Qinbin
Liang, Mao-Chang
Shia, Run-Lie
Chahine, Moustafa T.
Olsen, Edward T.
Chen, Luke L.
Yung, Yuk L.
TI Simulation of upper tropospheric CO2 from chemistry and transport models
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
ID CARBON-DIOXIDE; ATMOSPHERIC CO2; VARIABILITY; SENSITIVITY; SINKS; FLUX;
PARAMETERIZATION; CONVECTION; TRACERS; GASES
AB The California Institute of Technology/Jet Propulsion Laboratory two-dimensional (2-D), three-dimensional (3-D) GEOS-Chem, and 3-D MOZART- 2 chemistry and transport models (CTMs), driven respectively by NCEP2, GEOS-4, and NCEP1 reanalysis data, have been used to simulate upper tropospheric CO2 from 2000 to 2004. Model results of CO2 mixing ratios agree well with monthly mean aircraft observations at altitudes between 8 and 13 km ( Matsueda et al., 2002) in the tropics. The upper tropospheric CO2 seasonal cycle phases are well captured by the CTMs. Model results have smaller seasonal cycle amplitudes in the Southern Hemisphere compared with those in the Northern Hemisphere, which are consistent with the aircraft data. Some discrepancies are evident between the model and aircraft data in the midlatitudes, where models tend to underestimate the amplitude of CO2 seasonal cycle. Comparison of the simulated vertical profiles of CO2 between the different models reveals that the convection in the 3-D models is likely too weak in boreal winter and spring. Model sensitivity studies suggest that convection mass flux is important for the correct simulation of upper tropospheric CO2.
C1 [Jiang, Xun; Li, Qinbin; Chahine, Moustafa T.; Olsen, Edward T.; Chen, Luke L.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA.
[Liang, Mao-Chang] Acad Sinica, Environm Res Ctr, Taipei 115, Taiwan.
[Liang, Mao-Chang] Natl Cent Univ, Grad Inst Astron, Jhongli, Taiwan.
[Liang, Mao-Chang; Shia, Run-Lie; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Jiang, X (reprint author), CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM xun@gps.caltech.edu
RI Chem, GEOS/C-5595-2014
FU NASA [102438-01.01.01]; NSF [ATM-9903790]; NSC [96-2628-M-001-018]
FX This work is performed at JPL under contract with NASA and is supported
by project 102438-01.01.01. We thank J. Randerson for useful inputs and
helpful comments, two anonymous reviewers, and C. L. Quere for helpful
comments. Our special thanks to Bob Yantosca at Harvard University for
the help on the GEOS-Chem model and to Peter Hess, Larry Horowitz, and
Jean-Francois Lamar on the MOZART-2 model. R. L. Shia and Y. L. Yung are
supported by NSF grant ATM-9903790. M. C. Liang also would like to
acknowledge the support from an NSC grant 96-2628-M-001-018 to Academia
Sinica.
NR 48
TC 13
Z9 13
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0886-6236
EI 1944-9224
J9 GLOBAL BIOGEOCHEM CY
JI Glob. Biogeochem. Cycle
PD DEC 30
PY 2008
VL 22
IS 4
AR GB4025
DI 10.1029/2007GB003049
PG 11
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA 390MU
UT WOS:000262169200001
ER
PT J
AU Su, H
Jiang, JH
Vane, DG
Stephens, GL
AF Su, Hui
Jiang, Jonathan H.
Vane, Deborah G.
Stephens, Graeme L.
TI Observed vertical structure of tropical oceanic clouds sorted in
large-scale regimes
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB The CloudSat cloud water content (CWC) profiles are sorted by a number of large-scale parameters obtained from reanalysis and satellite observations, including 500 hPa vertical velocity, sea surface temperature and its gradient, surface divergence, precipitation, water vapor path, convective available potential energy and lower tropospheric static stability. The sorting is physics-based and phenomenon-oriented. We find different degrees of clustering of cloud vertical structure in various large-scale regimes. The dominant modes are the deep and shallow clouds with peak CWC above 7 km and below 2 km, respectively, corresponding to distinctly different large-scale regimes. A middle-level peak of CWC around 5-7 km is discernible associated with the large-scale conditions similar to the shallow clouds. This study provides the first quantitative and comprehensive view of tropical CWC distributions in large-scale regimes. These results offer insights into cloud parameterizations and serve as new observational metrics for evaluation of cloud simulations in models. Citation: Su, H., J. H. Jiang, D. G. Vane, and G. L. Stephens (2008), Observed vertical structure of tropical oceanic clouds sorted in large-scale regimes, Geophys. Res. Lett., 35, L24704, doi: 10.1029/2008GL035888.
C1 [Su, Hui; Jiang, Jonathan H.; Vane, Deborah G.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Stephens, Graeme L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
RP Su, H (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM hui.su@jpl.nasa.gov
FU JPL RTD
FX We thank the JPL R&TD FY08 funding support, discussions with J. Teixeira
and X. Huang, and helpful comments from the two reviewers. This work is
conducted at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA.
NR 8
TC 25
Z9 27
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 27
PY 2008
VL 35
IS 24
AR L24704
DI 10.1029/2008GL035888
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 388SW
UT WOS:000262040500001
ER
PT J
AU Hamilton, VE
Morris, RV
Gruener, JE
Mertzman, SA
AF Hamilton, Victoria E.
Morris, Richard V.
Gruener, John E.
Mertzman, Stanley A.
TI Visible, near-infrared, and middle infrared spectroscopy of altered
basaltic tephras: Spectral signatures of phyllosilicates, sulfates, and
other aqueous alteration products with application to the mineralogy of
the Columbia Hills of Gusev Crater, Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Review
ID THERMAL EMISSION-SPECTROSCOPY; REMOTE-SENSING APPLICATIONS; HAWAIIAN
PALAGONITIC SOIL; MINI-TES EXPERIMENT; MAUNA-KEA VOLCANO; MARTIAN
SURFACE; REFLECTANCE SPECTROSCOPY; MERIDIANI-PLANUM; MU-M; MOSSBAUER
SPECTROMETER
AB We studied visible to near-infrared (VNIR, 0.35-2.5 mu m) and middle infrared (MIR, 1800-250 cm(-1), also called thermal infrared and vibrational) spectra of basaltic tephras from Mauna Kea volcano that were altered under ambient, hydrothermal ( hydrolytic and acid sulfate), and dry heat conditions. Although models of MIR spectra of altered tephras generally produce fits whose quality is reduced compared to deconvolutions of primary lithologies, they successfully identify major alteration phases (cristobalite, oxide, phyllosilicate, and sulfate) except in palagonites. MIR spectra of the < 45 mu m fraction of all altered tephra samples exhibit an H2O peak at similar to 1640 cm(-1), but it cannot be used as an indicator of H2O content. This feature is present with band strengths > 1% in spectra of the 500-1000 mu m fraction only if phyllosilicates are present. Although Mauna Kea palagonitic tephra is considered a VNIR analog to Martian dust, comparison of MIR altered tephra spectra (< 45 mu m fraction) to dust spectra retrieved from Mars Global Surveyor and Mars Exploration Rover instruments do not provide good spectral matches. The best MIR match is a tephra that has a strong plagioclase feldspar transparency feature and was altered under dry, high-temperature, oxidizing conditions. This sample is not a VNIR analog and is not a process analog, but it emphasizes the mineralogical importance of plagioclase feldspar in Martian dust. No single tephra is a good spectral analog across the VNIR and MIR. We found no evidence for substantial sulfates or phyllosilicates in Mini-Thermal Emission Spectrometer (Mini-TES) spectra from Gusev Crater.
C1 [Hamilton, Victoria E.] SW Res Inst, Boulder, CO 80302 USA.
[Morris, Richard V.; Gruener, John E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Mertzman, Stanley A.] Franklin & Marshall Coll, Dept Earth & Environm, Lancaster, PA 17604 USA.
RP Hamilton, VE (reprint author), SW Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
EM hamilton@boulder.swri.edu
FU NASA's Mars Fundamental Research and Planetary Geology and Geophysics
programs; NASA Mars Exploration Rover Project; NASA Mars Reconnaissance
Orbiter (CRISM) Project; NASA Johnson Space Center
FX We thank Joe Michalski for providing several phyllosilicate and silica
phase spectra and Ray Arvidson and Patrick McGuire for calculation of
the transmission spectrum of H2O vapor. Steve Ruff provided
Mini-TES spectra of dust and rocks in Gusev Crater. Jim Gooding
collected the samples from Puu Pohaku, and Doug Ming and Trevor Graff
assisted with collection of samples from Puu Poliahu and Puu Waiau. Some
VNIR spectra were acquired with an ASD spectrometer provided by Ray
Arvidson. Funding to V. E. H. for this work was provided in part by
NASA's Mars Fundamental Research and Planetary Geology and Geophysics
programs. R. V. M. acknowledges support of the NASA Mars Exploration
Rover Project, the NASA Mars Reconnaissance Orbiter (CRISM) Project, and
the NASA Johnson Space Center. We thank Gregg Swayze and Steve Ruff for
their careful and detailed reviews, which have resulted in
clarifications and other improvements to the manuscript.
NR 109
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Z9 20
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 27
PY 2008
VL 113
IS E12
AR E12S43
DI 10.1029/2007JE003049
PG 30
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 388UC
UT WOS:000262043700001
ER
PT J
AU Galli, A
Wurz, P
Kallio, E
Ekenback, A
Holmstrom, M
Barabash, S
Grigoriev, A
Futaana, Y
Fok, MC
Gunell, H
AF Galli, A.
Wurz, P.
Kallio, E.
Ekenback, A.
Holmstrom, M.
Barabash, S.
Grigoriev, A.
Futaana, Y.
Fok, M. -C.
Gunell, H.
TI Tailward flow of energetic neutral atoms observed at Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID SOLAR-WIND INTERACTION; SUBSOLAR ENA JET; 1ST-ENA OBSERVATIONS; ASPERA-3
OBSERVATIONS; UPPER-ATMOSPHERE; CHARGE-EXCHANGE; EXPRESS MISSION; SPACE
PLASMAS; HYDROGEN; DISTRIBUTIONS
AB The ASPERA-3 experiment on Mars Express provides the first measurements of energetic neutral atoms (ENAs) from Mars. These measurements are used to study the global structure of the interaction of the solar wind with the Martian atmosphere. In this study we describe the tailward ENA flow observed at the nightside of Mars. After characterizing energy spectra of hydrogen ENA signals, we present composite images of the ENA intensities and compare them to theoretical predictions (empirical and MHD models). We find that the tailward flow of hydrogen ENAs is mainly generated by shocked solar wind protons. Despite intensive search, no oxygen ENAs above the instrument threshold are detected. The results challenge existing plasma models and constrain the hydrogen exospheric densities and atmospheric hydrogen and oxygen loss rates at low solar activity.
C1 [Galli, A.; Wurz, P.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Kallio, E.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Ekenback, A.; Holmstrom, M.; Barabash, S.; Grigoriev, A.; Futaana, Y.] Inst Rymdfys, SE-98128 Kiruna, Sweden.
[Fok, M. -C.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Gunell, H.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
RP Galli, A (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
EM galli@space.unibe.ch; peter.wurz@space.unibe.ch
RI Fok, Mei-Ching/D-1626-2012; Gunell, Herbert/D-5611-2013; Futaana,
Yoshifumi/P-5899-2014; Kallio, Esa/F-9410-2014;
OI Futaana, Yoshifumi/0000-0002-7056-3517; Kallio, Esa/0000-0002-9791-804X;
Gunell, Herbert/0000-0001-5379-1158
FU Swiss National Science Foundation
FX We thank Y. Ma and A. F. Nagy for providing the ion fluxes from their
MHD model that we used to compute the ENA fluxes. This work is supported
by the Swiss National Science Foundation.
NR 33
TC 10
Z9 10
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 25
PY 2008
VL 113
IS E12
AR E12012
DI 10.1029/2008JE003139
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 388UB
UT WOS:000262043600001
ER
PT J
AU Haba, Y
Liebmann, AC
Fukumura, K
Kunieda, H
Tsuruta, S
AF Haba, Yoshito
Liebmann, Andrew C.
Fukumura, Keigo
Kunieda, Hideyo
Tsuruta, Sachiko
TI XMM-Newton Observations of NGC 4051: Temporal Flux and Spectral
Variability during Transition to the Faintest Phase in NGC 4051
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 4051); galaxies: Seyfert;
X-rays: galaxies
ID LINE SEYFERT-1 GALAXY; ULTRALUMINOUS INFRARED GALAXIES; DENSE MOLECULAR
GAS; X-RAY-SPECTRUM; ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATE; ASCA
OBSERVATIONS; ACCRETION FLOW; BLACK-HOLE; SWAN SONG
AB We report on the results from temporal and spectral analyses of NGC 4051 observed with XMM-Newton. The X-ray variabilities in the higher-flux states are well explained by the combination of a variable, direct power law and a temporally stable, absorbed component. In low-flux states, however, spectral variations are mainly due to flux changes of the absorbed component. Furthermore, when the source enters into the lowest-flux state, the absorbed component no longer appears. One promising interpretation is that part of the central emission region is covered by a temporally stable material, while the size of the emission region varies so as to produce a flux variation predominantly in direct power-law component. Once the emission region becomes smaller than the size of the absorber, however. the absorbed flux also begins to decrease. Finally, when the emission region is reduced sufficiently, both the direct and absorbed components disappear (i.e., "switched off" state). In this state, we found the signature of thermal emission, whose temperature of 0.8 keV is in agreement with the average value obtained from statistical analyses of Seyfert 2, galaxies with starburst activity. This could suggest that NGC 4051 possesses a nuclear starburst region.
C1 [Haba, Yoshito; Kunieda, Hideyo] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Liebmann, Andrew C.; Tsuruta, Sachiko] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
[Fukumura, Keigo] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
RP Haba, Y (reprint author), Nagoya Univ, Dept Phys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan.
FU Ministry of Education, Culture, Sports, Science and Technology
FX We are deeply grateful to the whole XMM-Newton team for building,
launching, calibrating, and operating the spacecraft and instruments. We
thank an anonymous referee for useful comments that make our
presentations clearer and more meaningful. Y. H. is supported by a
Grant-in-Aid for the 21st Century COE "The Origin of the Universe and
Matter: Physical Elucidation of the Cosmic History" from the Ministry of
Education, Culture, Sports, Science and Technology.
NR 50
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 DEC 25
PY 2008
VL 60
IS 6
BP 1257
EP 1266
DI 10.1093/pasj/60.6.1257
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 433ZJ
UT WOS:000265244100006
ER
PT J
AU Wen, GY
Marshak, A
Cahalan, RF
AF Wen, Guoyong
Marshak, Alexander
Cahalan, Robert F.
TI Importance of molecular Rayleigh scattering in the enhancement of clear
sky reflectance in the vicinity of boundary layer cumulus clouds
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID AEROSOL OPTICAL-THICKNESS; MODIS; PRODUCTS; TERRA; OCEAN; LAND;
ATMOSPHERES; RETRIEVAL; TRANSPORT; DATASETS
AB Clouds increase the complexity of atmospheric radiative transfer processes, particularly for aerosol retrievals in clear regions in the vicinity of clouds. This study focuses on identifying mechanisms responsible for the enhancement of nadir reflectance in clear regions in the vicinity of cumulus clouds and quantifies the relative importance of each mechanism. Using cloud optical properties and surface albedo derived from Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) and Moderate Resolution Imaging Spectroradiometer (MODIS), we performed extensive Monte Carlo simulations of radiative transfer in two cumulus scenes in a biomass burning region in Brazil. The results show that the scattering of radiation by clouds, followed by upward Rayleigh scattering by molecules above cloud top over clear gaps, is the dominant mechanism for the enhancement of visible reflectance in clear regions in boundary layer cumulus field over dark surfaces with aerosols trapped in the boundary layer. The Rayleigh scattering contributes similar to 80% and similar to 50% to the total enhancement for wavelengths 0.47 mu m (with aerosol optical thickness 0.2) and 0.66 mu m (with aerosol optical thickness 0.1), respectively. Out of the total contribution of molecular scattering, similar to 90% arises from the clear atmosphere above cloud top height. The mechanism is valid for a large range of aerosol optical thicknesses (up to 1 in this study) for 0.47 mu m, and for aerosol optical thickness up to 0.2 for 0.66 mu m. Our results provide a basis to develop simplifications for future aerosol remote sensing from satellite.
C1 [Wen, Guoyong; Marshak, Alexander; Cahalan, Robert F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wen, Guoyong] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Wen, GY (reprint author), NASA, Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA.
EM Guoyong.Wen-1@nasa.gov
RI Marshak, Alexander/D-5671-2012; Cahalan, Robert/E-3462-2012
OI Cahalan, Robert/0000-0001-9724-1270
FU NASA GSFC [DE-AI02-95ER6I96I]; NASA's Radiation Sciences Program
[921266]
FX This research was supported by the Department of Energy (under grant
DE-AI02-95ER6I96I to NASA GSFC) as part of the Atmospheric Radiation
Measurement (ARM) program, by NASA's Radiation Sciences Program (under
grant 921266), and we thank program manager Hal Maring. We thank J.
Coakley, N. Loeb, L. Remer, and T. Varnai for useful discussions. The
authors were greatly inspired by our colleague Yoram J. Kaufman in
aerosol research.
NR 35
TC 18
Z9 18
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD DEC 24
PY 2008
VL 113
AR D24207
DI 10.1029/2008JD010592
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 388TG
UT WOS:000262041500003
ER
PT J
AU Yang, FH
Zhu, AX
Ichii, K
White, MA
Hashimoto, H
Nemani, RR
AF Yang, Feihua
Zhu, A-Xing
Ichii, Kazuhito
White, Michael A.
Hashimoto, Hirofumi
Nemani, Ramakrishna R.
TI Assessing the representativeness of the AmeriFlux network using MODIS
and GOES data
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID LAND-SURFACE TEMPERATURE; GROSS PRIMARY PRODUCTION; SUPPORT VECTOR
MACHINE; VEGETATION INDEXES; COMBINING MODIS; FLUXES; ECOSYSTEM;
EVAPOTRANSPIRATION; VALIDATION; CARBON
AB The AmeriFlux network of eddy covariance towers has played a critical role in the analysis of terrestrial water and carbon dynamics. It has been used to understand the general principles of ecosystem behaviors and to scale up those principles from sites to regions. To support the generalization from individual sites to large regions, it is essential that all major ecoregions in North America are represented in the AmeriFlux network. In this study, we examined the representativeness of the AmeriFlux network by comparing the climate and vegetation across the coterminous United States in 2004 with those at the AmeriFlux network in 2000-2004 on the basis of remote sensing products. We found that the AmeriFlux network generally captured the climatic and vegetation characteristics in the coterminous United States with under-representations in the Rocky Mountain evergreen needleleaf forest, the Sierra Nevada Mountains, the Sonora desert, the northern Great Plains, the Great Basin Desert, and New England. In terms of site representativeness, our analysis suggested that Indiana Morgan Monroe State Forest, Indiana, and Harvard Forest, Massachusetts, were among the forest sites with high representativeness extents; while Audubon Research Ranch, Arizona, and Sky Oaks Young Chaparral were among the nonforest sites with high representativeness extents.
C1 [Yang, Feihua] Univ Wisconsin, Dept Geog, Madison, WI 53706 USA.
[Yang, Feihua; Ichii, Kazuhito; Hashimoto, Hirofumi; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ichii, Kazuhito] Fukushima Univ, Fac Symbiot Syst Sci, Fukushima 9601296, Japan.
[White, Michael A.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA.
[Hashimoto, Hirofumi] Calif State Univ, Div Sci & Environm Policy, Seaside, CA USA.
[Zhu, A-Xing] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, State Key Lab Resources & Environm Informat Syst, Beijing, Peoples R China.
RP Yang, FH (reprint author), Univ Wisconsin, Dept Geog, 426 Sci Hall,550 N Pk St, Madison, WI 53706 USA.
EM feihuayang@wisc.edu
RI Ichii, Kazuhito/D-2392-2010;
OI Ichii, Kazuhito/0000-0002-8696-8084; White, Michael/0000-0002-0238-8913
FU Chinese Academy of Sciences International Partnership Project
[CXTD-Z2005-1]; National Basic Research Program of China [2007CB407207];
Chinese Academy of Sciences; NASA New Investigator Program; EOS; REASON;
Department of Energy; National Oceanic and Atmospheric Administration;
National Aeronautics and Space Administration; National Science
Foundation
FX The funding from the Chinese Academy of Sciences International
Partnership Project (Human Activities and Ecosystem Changes (project
CXTD-Z2005-1)), National Basic Research Program of China (2007CB407207),
and the Chinese Academy of Sciences through the One-Hundred Talents
Program to A-Xing Zhu was appreciated. M. A. White was supported by the
NASA New Investigator Program. NASA's Science Mission Directorate funded
part of this research through EOS and REASON grants to RRN. The authors
also thank John W. Norman, James E. Burt, David J. Page, and John W.
William for inspirations of this research. AmeriFlux was funded by the
Department of Energy, the National Oceanic and Atmospheric
Administration, the National Aeronautics and Space Administration, and
the National Science Foundation. Special thanks to all scientists and
supporting staffs at AmeriFlux sites.
NR 26
TC 8
Z9 8
U1 0
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD DEC 24
PY 2008
VL 113
IS G4
AR G04036
DI 10.1029/2007JG000627
PG 11
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 388TS
UT WOS:000262042700001
ER
PT J
AU Crooker, NU
Kahler, SW
Gosling, JT
Lepping, RP
AF Crooker, N. U.
Kahler, S. W.
Gosling, J. T.
Lepping, R. P.
TI Evidence in magnetic clouds for systematic open flux transport on the
Sun
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTIONS; SOLAR-WIND; ELECTRONS; TOPOLOGY; DEPLETIONS;
EVENTS
AB Most magnetic clouds encountered by spacecraft at 1 AU display a mix of unidirectional suprathermal electrons signaling open field lines and counterstreaming electrons signaling loops connected to the Sun at both ends. Assuming the open fields were originally loops that underwent interchange reconnection with open fields at the Sun, we determine the sense of connectedness of the open fields found in 72 of 97 magnetic clouds identified by the Wind spacecraft in order to obtain information on the location and sense of the reconnection and resulting flux transport at the Sun. The true polarity of the open fields in each magnetic cloud was determined from the direction of the suprathermal electron flow relative to the magnetic field direction. Results indicate that the polarity of all open fields within a given magnetic cloud is the same 89% of the time, implying that interchange reconnection at the Sun most often occurs in only one leg of a flux rope loop, thus transporting open flux in a single direction, from a coronal hole near that leg to the foot point of the opposite leg. This pattern is consistent with the view that interchange reconnection in coronal mass ejections systematically transports an amount of open flux sufficient to reverse the polarity of the heliospheric field through the course of the solar cycle. Using the same electron data, we also find that the fields encountered in magnetic clouds are only a third as likely to be locally inverted as not. While one might expect inversions to be equally as common as not in flux rope coils, consideration of the geometry of spacecraft trajectories relative to the modeled magnetic cloud axes leads us to conclude that the result is reasonable.
C1 [Crooker, N. U.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Gosling, J. T.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
[Kahler, S. W.] USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA.
[Lepping, R. P.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
RP Crooker, NU (reprint author), Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
EM crooker@bu.edu
FU NASA [NNG06GC18G]
FX This paper is based upon work supported by NASA under grant NNG06GC18G.
NR 20
TC 10
Z9 10
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD DEC 24
PY 2008
VL 113
IS A12
AR A12107
DI 10.1029/2008JA013628
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 388UH
UT WOS:000262044200001
ER
PT J
AU Morris, RV
Klingelhofer, G
Schroder, C
Fleischer, I
Ming, DW
Yen, AS
Gellert, R
Arvidson, RE
Rodionov, DS
Crumpler, LS
Clark, BC
Cohen, BA
Mccoy, TJ
Mittlefehldt, DW
Schmidt, ME
de Souza, PA
Squyres, SW
AF Morris, R. V.
Klingelhoefer, G.
Schroeder, C.
Fleischer, I.
Ming, D. W.
Yen, A. S.
Gellert, R.
Arvidson, R. E.
Rodionov, D. S.
Crumpler, L. S.
Clark, B. C.
Cohen, B. A.
Mccoy, T. J.
Mittlefehldt, D. W.
Schmidt, M. E.
de Souza, P. A., Jr.
Squyres, S. W.
TI Iron mineralogy and aqueous alteration from Husband Hill through Home
Plate at Gusev Crater, Mars: Results from the Mossbauer instrument on
the Spirit Mars Exploration Rover
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MARTIAN SOIL; SPECTROMETER; METEORITES; HEMATITE; ROCKS; DUST;
PATHFINDER; VOLCANO; ANALOG
AB Spirit's Mossbauer (MB) instrument determined the Fe mineralogy and oxidation state of 71 rocks and 43 soils during its exploration of the Gusev plains and the Columbia Hills (West Spur, Husband Hill, Haskin Ridge, northern Inner Basin, and Home Plate) on Mars. The plains are predominantly float rocks and soil derived from olivine basalts. Outcrops at West Spur and on Husband Hill have experienced pervasive aqueous alteration as indicated by the presence of goethite. Olivine-rich outcrops in a possible mafic/ultramafic horizon are present on Haskin Ridge. Relatively unaltered basalt and olivine basalt float rocks occur at isolated locations throughout the Columbia Hills. Basalt and olivine basalt outcrops are found at and near Home Plate, a putative hydrovolcanic structure. At least three pyroxene compositions are indicated by MB data. MB spectra of outcrops Barnhill and Torquas resemble palagonitic material and thus possible supergene aqueous alteration. Deposits of Fe3+-sulfate soil, located at Paso Robles, Arad, and Tyrone, are likely products of acid sulfate fumarolic and/or hydrothermal activity, possibly in connection with Home Plate volcanism. Hematite-rich outcrops between Home Plate and Tyrone (e. g., Montalva) may also be products of this aqueous activity. Low water-to-rock ratios (isochemical alteration) are implied during palagonite, goethite, and hematite formation because bulk chemical compositions are basaltic (SO3-free basis). High water-to-rock ratios (leaching) under acid sulfate conditions are implied for the high-SiO2 rock and soil in Eastern Valley and the float rock FuzzySmith, which has possible pyrite/marcasite as a hydrothermal alteration product.
C1 [Morris, R. V.; Schroeder, C.; Ming, D. W.; Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Clark, B. C.] Lockheed Martin Corp, Littleton, CO 80127 USA.
[Cohen, B. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Crumpler, L. S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA.
[de Souza, P. A., Jr.] CSIRO, Tasmanian ICT Ctr, Hobart, Tas 7000, Australia.
[Klingelhoefer, G.; Fleischer, I.; Rodionov, D. S.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55128 Mainz, Germany.
[Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada.
[Mccoy, T. J.; Schmidt, M. E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
[Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Yen, A. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rodionov, D. S.] Moscow Space Res Inst, Moscow 117810, Russia.
RP Morris, RV (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM richard.v.morris@nasa.gov
RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009; Centre,
TasICT/D-1212-2011
OI de Souza, Paulo/0000-0002-0091-8925; Schroder,
Christian/0000-0002-7935-6039;
FU NASA Mars Exploration Rover Project; NASA Johnson Space Center; German
Space Agency [50QM 99022]; Technical University of Darmstadt; University
of Mainz
FX R. V. M. and D. W. M. acknowledge support of the NASA Mars Exploration
Rover Project and the NASA Johnson Space Center. C. S. acknowledges
support by an appointment to the NASA Postdoctoral Program at the
Johnson Space Center, administered by Oak Ridge Associated Universities
through a contract with NASA. The MER MIMOS II Mossbauer spectrometers
were developed and built with funding provided by the German Space
Agency under contract 50QM 99022 and with additional support from the
Technical University of Darmstadt and the University of Mainz. A portion
of the work described in this paper was conducted at the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. We acknowledge the unwavering support, dedication, and attention
to detail of JPL engineering and MER operations staff and the MER Athena
Science Team. We thank D. Agresti and Brad Jolliff for thoughtful and
detailed reviews of the manuscript.
NR 63
TC 70
Z9 72
U1 2
U2 32
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 23
PY 2008
VL 113
IS E12
AR E12S42
DI 10.1029/2008JE003201
PG 43
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 388UA
UT WOS:000262043500001
ER
PT J
AU van der Werf, GR
Dempewolf, J
Trigg, SN
Randerson, JT
Kasibhatla, PS
Gigliof, L
Murdiyarso, D
Peters, W
Morton, DC
Collatz, GJ
Dolman, AJ
DeFries, RS
AF van der Werf, G. R.
Dempewolf, J.
Trigg, S. N.
Randerson, J. T.
Kasibhatla, P. S.
Gigliof, L.
Murdiyarso, D.
Peters, W.
Morton, D. C.
Collatz, G. J.
Dolman, A. J.
DeFries, R. S.
TI Climate regulation of fire emissions and deforestation in equatorial
Asia
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE climate change; feedbacks; biomass burning; Indonesia; global carbon
cycle
ID SOUTHEAST-ASIA; MODIS; VEGETATION; INDONESIA; PEAT; ALGORITHM; DATASET;
BORNEO; POLICY; HAZE
AB Drainage of peatlands and deforestation have led to large-scale fires in equatorial Asia, affecting regional air quality and global concentrations of greenhouse gases. Here we used several sources of satellite data with biogeochemical and atmospheric modeling to better understand and constrain fire emissions from Indonesia, Malaysia, and Papua New Guinea during 2000-2006. We found that average fire emissions from this region [128 +/- 51 (1 sigma) Tg carbon (C) year(-1), T = 1012] were comparable to fossil fuel emissions. In Borneo, carbon emissions from fires were highly variable, fluxes during the moderate 2006 El Nino more than 30 times greater than those during the 2000 La Nina (and with a 2000-2006 mean of 74 +/- 33 Tg C yr(-1)). Higher rates of forest loss and larger areas of peatland becoming vulnerable to fire in drought years caused a strong nonlinear relation between drought and fire emissions in southern Borneo. Fire emissions from Sumatra showed a positive linear trend, increasing at a rate of 8 Tg C year(-2) (approximately doubling during 2000-2006). These results highlight the importance of including deforestation in future climate agreements. They also imply that land manager responses to expected shifts in tropical precipitation may critically determine the strength of climate-carbon cycle feedbacks during the 21st century.
C1 [van der Werf, G. R.; Dolman, A. J.] Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands.
[Dempewolf, J.; Morton, D. C.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Trigg, S. N.] Cranfield Univ, Integrated Earth Syst Sci Inst, Cranfield MK43 0AL, Beds, England.
[Randerson, J. T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Kasibhatla, P. S.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Gigliof, L.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Murdiyarso, D.] JI CIFOR, Ctr Int Forestry Res, Bogor 16680, Indonesia.
[Peters, W.] Univ Wageningen & Res Ctr, Dept Meteorol & Air Qual, NL-6700 AA Wageningen, Netherlands.
[Collatz, G. J.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[DeFries, R. S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
RP van der Werf, GR (reprint author), Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands.
EM guido.van.der.werf@falw.vu.nl
RI Peters, Wouter/B-8305-2008; Kasibhatla, Prasad/A-2574-2010; collatz,
george/D-5381-2012; Morton, Douglas/D-5044-2012; Xiongfei,
Zhao/G-7690-2015; van der Werf, Guido/M-8260-2016;
OI Peters, Wouter/0000-0001-8166-2070; van der Werf,
Guido/0000-0001-9042-8630; Kasibhatla, Prasad/0000-0003-3562-3737;
Dolman, A.J./0000-0003-0099-0457
FU National Aeronautics and Space Administration [NNG05GD20G, NNG04GK49G,
NNG04GD89G]; Netherlands Organization for Scientific Research
FX This research was supported by National Aeronautics and Space
Administration grants NNG05GD20G, NNG04GK49G, and NNG04GD89G. G.R.v.d.W.
was supported by a Veni grant from the Netherlands Organization for
Scientific Research.
NR 38
TC 133
Z9 136
U1 5
U2 81
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 DEC 23
PY 2008
VL 105
IS 51
BP 20350
EP 20355
DI 10.1073/pnas.0803375105
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 388BP
UT WOS:000261995600031
PM 19075224
ER
PT J
AU Abbott, B
Abbott, R
Adhikari, R
Ajith, P
Allen, B
Allen, G
Amin, R
Anderson, SB
Anderson, WG
Arain, MA
Araya, M
Armandula, H
Armor, P
Aso, Y
Aston, S
Aufmuth, P
Aulbert, C
Babak, S
Ballmer, S
Bantilan, H
Barish, BC
Barker, C
Barker, D
Barr, B
Barriga, P
Barton, MA
Bartos, I
Bastarrika, M
Bayer, K
Betzwieser, J
Beyersdorf, PT
Bilenko, IA
Billingsley, G
Biswas, R
Black, E
Blackburn, K
Blackburn, L
Blair, D
Bland, B
Bodiya, TP
Bogue, L
Bork, R
Boschi, V
Bose, S
Brady, PR
Braginsky, VB
Brau, JE
Brinkmann, M
Brooks, A
Brown, DA
Brunet, G
Bullington, A
Buonanno, A
Burmeister, O
Byer, RL
Cadonati, L
Cagnoli, G
Camp, JB
Cannizzo, J
Cannon, K
Cao, J
Cardenas, L
Casebolt, T
Castaldi, G
Cepeda, C
Chalkley, E
Charlton, P
Chatterji, S
Chelkowski, S
Chen, Y
Christensen, N
Clark, D
Clark, J
Cokelaer, T
Conte, R
Cook, D
Corbitt, T
Coyne, D
Creighton, JDE
Cumming, A
Cunningham, L
Cutler, RM
Dalrymple, J
Danzmann, K
Davies, G
DeBra, D
Degallaix, J
Degree, M
Dergachev, V
Desai, S
DeSalvo, R
Dhurandhar, S
Diaz, M
Dickson, J
Di Credico, A
Dietz, A
Donovan, F
Dooley, KL
Doomes, EE
Drever, RWP
Duke, I
Dumas, JC
Dupuis, RJ
Dwyer, JG
Echols, C
Effler, A
Ehrens, P
Espinoza, E
Etzel, T
Evans, T
Fairhurst, S
Fan, Y
Fazi, D
Fehrmann, H
Fejer, MM
Finn, LS
Flasch, K
Fotopoulos, N
Freise, A
Frey, R
Fricke, T
Fritschel, P
Frolov, VV
Fyffe, M
Garofoli, J
Gholami, I
Giaime, JA
Giampanis, S
Giardina, KD
Goda, K
Goetz, E
Goggin, L
Gonzalez, G
Gossler, S
Gouaty, R
Grant, A
Gras, S
Gray, C
Gray, M
Greenhalgh, RJS
Gretarsson, AM
Grimaldi, F
Grosso, R
Grote, H
Grunewald, S
Guenther, M
Gustafson, EK
Gustafson, R
Hage, B
Hallam, JM
Hammer, D
Hanna, C
Hanson, J
Harms, J
Harry, G
Harstad, E
Hayama, K
Hayler, T
Heefner, J
Heng, IS
Hennessy, M
Heptonstall, A
Hewitson, M
Hild, S
Hirose, E
Hoak, D
Hosken, D
Hough, J
Hughey, B
Huttner, SH
Ingram, D
Ito, M
Ivanov, A
Johnson, B
Johnson, WW
Jones, DI
Jones, G
Jones, R
Ju, L
Kalmus, P
Kalogera, V
Kamat, S
Kanner, J
Kasprzyk, D
Katsavounidis, E
Kawabe, K
Kawamura, S
Kawazoe, F
Kells, W
Keppel, DG
Khalili, FY
Khan, R
Khazanov, E
Kim, C
King, P
Kissel, JS
Klimenko, S
Kokeyama, K
Kondrashov, V
Kopparapu, RK
Kozak, D
Kozhevatov, I
Krishnan, B
Kwee, P
Lam, PK
Landry, M
Lang, MM
Lantz, B
Lazzarini, A
Lei, M
Leindecker, N
Leonhardt, V
Leonor, I
Libbrecht, K
Lin, H
Lindquist, P
Lockerbie, NA
Lodhia, D
Lormand, M
Lu, P
Lubinski, M
Lucianetti, A
Luck, H
Machenschalk, B
MacInnis, M
Mageswaran, M
Mailand, K
Mandic, V
Marka, S
Marka, Z
Markosyan, A
Markowitz, J
Maros, E
Martin, I
Martin, RM
Marx, JN
Mason, K
Matichard, F
Matone, L
Matzner, R
Mavalvala, N
McCarthy, R
McClelland, DE
McGuire, SC
McHugh, M
McIntyre, G
McIvor, G
McKechan, D
McKenzie, K
Meier, T
Melissinos, A
Mendell, G
Mercer, RA
Meshkov, S
Messenger, CJ
Meyers, D
Miller, J
Minelli, J
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Miyakawa, O
Moe, B
Mohanty, S
Moreno, G
Mossavi, K
MowLowry, C
Mueller, G
Mukherjee, S
Mukhopadhyay, H
Muller-Ebhardt, H
Munch, J
Murray, P
Myers, E
Myers, J
Nash, T
Nelson, J
Newton, G
Nishizawa, A
Numata, K
O'Dell, J
Ogin, G
O'Reilly, B
O'Shaughnessy, R
Ottaway, DJ
Ottens, RS
Overmier, H
Owen, BJ
Pan, Y
Pankow, C
Papa, MA
Parameshwaraiah, V
Patel, P
Pedraza, M
Penn, S
Perreca, A
Petrie, T
Pinto, IM
Pitkin, M
Pletsch, HJ
Plissi, MV
Postiglione, F
Principe, M
Prix, R
Quetschke, V
Raab, F
Rabeling, DS
Radkins, H
Rainer, N
Rakhmanov, M
Ramsunder, M
Rehbein, H
Reid, S
Reitze, DH
Riesen, R
Riles, K
Rivera, B
Robertson, NA
Robinson, C
Robinson, EL
Roddy, S
Rodriguez, A
Rogan, AM
Rollins, J
Romano, JD
Romie, J
Route, R
Rowan, S
Rudiger, A
Ruet, L
Russell, P
Ryan, K
Sakata, S
Samidi, M
de la Jordana, LS
Sandberg, V
Sannibale, V
Saraf, S
Sarin, P
Sathyaprakash, BS
Sato, S
Saulson, PR
Savage, R
Savov, P
Schediwy, SW
Schilling, R
Schnabel, R
Schofield, R
Schutz, BF
Schwinberg, P
Scott, SM
Searle, AC
Sears, B
Seifert, F
Sellers, D
Sengupta, AS
Shawhan, P
Shoemaker, DH
Sibley, A
Siemens, X
Sigg, D
Sinha, S
Sintes, AM
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Smith, ND
Somiya, K
Sorazu, B
Stein, LC
Stochino, A
Stone, R
Strain, KA
Strom, DM
Stuver, A
Summerscales, TZ
Sun, KX
Sung, M
Sutton, PJ
Takahashi, H
Tanner, DB
Taylor, R
Taylor, R
Thacker, J
Thorne, KA
Thorne, KS
Thuering, A
Tinto, M
Tokmakov, KV
Torres, C
Torrie, C
Traylor, G
Trias, M
Tyler, W
Ugolini, D
Ulmen, J
Urbanek, K
Vahlbruch, H
Van Den Broeck, C
van der Sluys, M
Vass, S
Vaulin, R
Vecchio, A
Veitch, J
Veitch, P
Villar, A
Vorvick, C
Vyachanin, SP
Waldman, SJ
Wallace, L
Ward, H
Ward, R
Weinert, M
Weinstein, A
Weiss, R
Wen, S
Wette, K
Whelan, JT
Whitcomb, SE
Whiting, BF
Wilkinson, C
Willems, PA
Williams, HR
Williams, L
Willke, B
Wilmut, I
Winkler, W
Wipf, CC
Wiseman, AG
Woan, G
Wooley, R
Worden, J
Wu, W
Yakushin, I
Yamamoto, H
Yan, Z
Yoshida, S
Zanolin, M
Zhang, J
Zhang, L
Zhao, C
Zotov, N
Zucker, M
Zweizig, J
AF Abbott, B.
Abbott, R.
Adhikari, R.
Ajith, P.
Allen, B.
Allen, G.
Amin, R.
Anderson, S. B.
Anderson, W. G.
Arain, M. A.
Araya, M.
Armandula, H.
Armor, P.
Aso, Y.
Aston, S.
Aufmuth, P.
Aulbert, C.
Babak, S.
Ballmer, S.
Bantilan, H.
Barish, B. C.
Barker, C.
Barker, D.
Barr, B.
Barriga, P.
Barton, M. A.
Bartos, I.
Bastarrika, M.
Bayer, K.
Betzwieser, J.
Beyersdorf, P. T.
Bilenko, I. A.
Billingsley, G.
Biswas, R.
Black, E.
Blackburn, K.
Blackburn, L.
Blair, D.
Bland, B.
Bodiya, T. P.
Bogue, L.
Bork, R.
Boschi, V.
Bose, S.
Brady, P. R.
Braginsky, V. B.
Brau, J. E.
Brinkmann, M.
Brooks, A.
Brown, D. A.
Brunet, G.
Bullington, A.
Buonanno, A.
Burmeister, O.
Byer, R. L.
Cadonati, L.
Cagnoli, G.
Camp, J. B.
Cannizzo, J.
Cannon, K.
Cao, J.
Cardenas, L.
Casebolt, T.
Castaldi, G.
Cepeda, C.
Chalkley, E.
Charlton, P.
Chatterji, S.
Chelkowski, S.
Chen, Y.
Christensen, N.
Clark, D.
Clark, J.
Cokelaer, T.
Conte, R.
Cook, D.
Corbitt, T.
Coyne, D.
Creighton, J. D. E.
Cumming, A.
Cunningham, L.
Cutler, R. M.
Dalrymple, J.
Danzmann, K.
Davies, G.
DeBra, D.
Degallaix, J.
Degree, M.
Dergachev, V.
Desai, S.
DeSalvo, R.
Dhurandhar, S.
Diaz, M.
Dickson, J.
Di Credico, A.
Dietz, A.
Donovan, F.
Dooley, K. L.
Doomes, E. E.
Drever, R. W. P.
Duke, I.
Dumas, J-C
Dupuis, R. J.
Dwyer, J. G.
Echols, C.
Effler, A.
Ehrens, P.
Espinoza, E.
Etzel, T.
Evans, T.
Fairhurst, S.
Fan, Y.
Fazi, D.
Fehrmann, H.
Fejer, M. M.
Finn, L. S.
Flasch, K.
Fotopoulos, N.
Freise, A.
Frey, R.
Fricke, T.
Fritschel, P.
Frolov, V. V.
Fyffe, M.
Garofoli, J.
Gholami, I.
Giaime, J. A.
Giampanis, S.
Giardina, K. D.
Goda, K.
Goetz, E.
Goggin, L.
Gonzalez, G.
Gossler, S.
Gouaty, R.
Grant, A.
Gras, S.
Gray, C.
Gray, M.
Greenhalgh, R. J. S.
Gretarsson, A. M.
Grimaldi, F.
Grosso, R.
Grote, H.
Grunewald, S.
Guenther, M.
Gustafson, E. K.
Gustafson, R.
Hage, B.
Hallam, J. M.
Hammer, D.
Hanna, C.
Hanson, J.
Harms, J.
Harry, G.
Harstad, E.
Hayama, K.
Hayler, T.
Heefner, J.
Heng, I. S.
Hennessy, M.
Heptonstall, A.
Hewitson, M.
Hild, S.
Hirose, E.
Hoak, D.
Hosken, D.
Hough, J.
Hughey, B.
Huttner, S. H.
Ingram, D.
Ito, M.
Ivanov, A.
Johnson, B.
Johnson, W. W.
Jones, D. I.
Jones, G.
Jones, R.
Ju, L.
Kalmus, P.
Kalogera, V.
Kamat, S.
Kanner, J.
Kasprzyk, D.
Katsavounidis, E.
Kawabe, K.
Kawamura, S.
Kawazoe, F.
Kells, W.
Keppel, D. G.
Khalili, F. Ya
Khan, R.
Khazanov, E.
Kim, C.
King, P.
Kissel, J. S.
Klimenko, S.
Kokeyama, K.
Kondrashov, V.
Kopparapu, R. K.
Kozak, D.
Kozhevatov, I.
Krishnan, B.
Kwee, P.
Lam, P. K.
Landry, M.
Lang, M. M.
Lantz, B.
Lazzarini, A.
Lei, M.
Leindecker, N.
Leonhardt, V.
Leonor, I.
Libbrecht, K.
Lin, H.
Lindquist, P.
Lockerbie, N. A.
Lodhia, D.
Lormand, M.
Lu, P.
Lubinski, M.
Lucianetti, A.
Lueck, H.
Machenschalk, B.
MacInnis, M.
Mageswaran, M.
Mailand, K.
Mandic, V.
Marka, S.
Marka, Z.
Markosyan, A.
Markowitz, J.
Maros, E.
Martin, I.
Martin, R. M.
Marx, J. N.
Mason, K.
Matichard, F.
Matone, L.
Matzner, R.
Mavalvala, N.
McCarthy, R.
McClelland, D. E.
McGuire, S. C.
McHugh, M.
McIntyre, G.
McIvor, G.
McKechan, D.
McKenzie, K.
Meier, T.
Melissinos, A.
Mendell, G.
Mercer, R. A.
Meshkov, S.
Messenger, C. J.
Meyers, D.
Miller, J.
Minelli, J.
Mitra, S.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Miyakawa, O.
Moe, B.
Mohanty, S.
Moreno, G.
Mossavi, K.
MowLowry, C.
Mueller, G.
Mukherjee, S.
Mukhopadhyay, H.
Mueller-Ebhardt, H.
Munch, J.
Murray, P.
Myers, E.
Myers, J.
Nash, T.
Nelson, J.
Newton, G.
Nishizawa, A.
Numata, K.
O'Dell, J.
Ogin, G.
O'Reilly, B.
O'Shaughnessy, R.
Ottaway, D. J.
Ottens, R. S.
Overmier, H.
Owen, B. J.
Pan, Y.
Pankow, C.
Papa, M. A.
Parameshwaraiah, V.
Patel, P.
Pedraza, M.
Penn, S.
Perreca, A.
Petrie, T.
Pinto, I. M.
Pitkin, M.
Pletsch, H. J.
Plissi, M. V.
Postiglione, F.
Principe, M.
Prix, R.
Quetschke, V.
Raab, F.
Rabeling, D. S.
Radkins, H.
Rainer, N.
Rakhmanov, M.
Ramsunder, M.
Rehbein, H.
Reid, S.
Reitze, D. H.
Riesen, R.
Riles, K.
Rivera, B.
Robertson, N. A.
Robinson, C.
Robinson, E. L.
Roddy, S.
Rodriguez, A.
Rogan, A. M.
Rollins, J.
Romano, J. D.
Romie, J.
Route, R.
Rowan, S.
Ruediger, A.
Ruet, L.
Russell, P.
Ryan, K.
Sakata, S.
Samidi, M.
de la Jordana, L. Sancho
Sandberg, V.
Sannibale, V.
Saraf, S.
Sarin, P.
Sathyaprakash, B. S.
Sato, S.
Saulson, P. R.
Savage, R.
Savov, P.
Schediwy, S. W.
Schilling, R.
Schnabel, R.
Schofield, R.
Schutz, B. F.
Schwinberg, P.
Scott, S. M.
Searle, A. C.
Sears, B.
Seifert, F.
Sellers, D.
Sengupta, A. S.
Shawhan, P.
Shoemaker, D. H.
Sibley, A.
Siemens, X.
Sigg, D.
Sinha, S.
Sintes, A. M.
Slagmolen, B. J. J.
Slutsky, J.
Smith, J. R.
Smith, M. R.
Smith, N. D.
Somiya, K.
Sorazu, B.
Stein, L. C.
Stochino, A.
Stone, R.
Strain, K. A.
Strom, D. M.
Stuver, A.
Summerscales, T. Z.
Sun, K-X
Sung, M.
Sutton, P. J.
Takahashi, H.
Tanner, D. B.
Taylor, R.
Taylor, R.
Thacker, J.
Thorne, K. A.
Thorne, K. S.
Thuering, A.
Tinto, M.
Tokmakov, K. V.
Torres, C.
Torrie, C.
Traylor, G.
Trias, M.
Tyler, W.
Ugolini, D.
Ulmen, J.
Urbanek, K.
Vahlbruch, H.
Van Den Broeck, C.
van der Sluys, M.
Vass, S.
Vaulin, R.
Vecchio, A.
Veitch, J.
Veitch, P.
Villar, A.
Vorvick, C.
Vyachanin, S. P.
Waldman, S. J.
Wallace, L.
Ward, H.
Ward, R.
Weinert, M.
Weinstein, A.
Weiss, R.
Wen, S.
Wette, K.
Whelan, J. T.
Whitcomb, S. E.
Whiting, B. F.
Wilkinson, C.
Willems, P. A.
Williams, H. R.
Williams, L.
Willke, B.
Wilmut, I.
Winkler, W.
Wipf, C. C.
Wiseman, A. G.
Woan, G.
Wooley, R.
Worden, J.
Wu, W.
Yakushin, I.
Yamamoto, H.
Yan, Z.
Yoshida, S.
Zanolin, M.
Zhang, J.
Zhang, L.
Zhao, C.
Zotov, N.
Zucker, M.
Zweizig, J.
CA LIGO Sci Collaboration
TI First joint search for gravitational-wave bursts in LIGO and GEO 600
data
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID SCIENCE RUN; INVERSE PROBLEM; DETECTOR; GEO-600; ALGORITHM
AB We present the results of the first joint search for gravitational-wave bursts by the LIGO and GEO 600 detectors. We search for bursts with characteristic central frequencies in the band 768-2048 Hz in the data acquired between 22 February and 23 March, 2005 (fourth LSC Science Run-S4). We discuss the inclusion of the GEO 600 data in the Waveburst-CorrPower pipeline that first searches for coincident excess power events without taking into account differences in the antenna responses or strain sensitivities of the various detectors. We compare the performance of this pipeline to that of the coherent Waveburst pipeline based on the maximum likelihood statistic. This likelihood statistic is derived from a coherent sum of the detector data streams that takes into account the antenna patterns and sensitivities of the different detectors in the network. We find that the coherent Waveburst pipeline is sensitive to signals of amplitude 30-50% smaller than the Waveburst-CorrPower pipeline. We perform a search for gravitational-wave bursts using both pipelines and find no detection candidates in the S4 data set when all four instruments were operating stably.
C1 [Abbott, B.; Abbott, R.; Adhikari, R.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, K.; Bork, R.; Boschi, V.; Brooks, A.; Cannon, K.; Cardenas, L.; Cepeda, C.; Chatterji, S.; Coyne, D.; DeSalvo, R.; Dupuis, R. J.; Echols, C.; Ehrens, P.; Espinoza, E.; Etzel, T.; Fazi, D.; Fricke, T.; Goggin, L.; Gustafson, E. K.; Heefner, J.; Ivanov, A.; Kells, W.; Keppel, D. G.; King, P.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Libbrecht, K.; Lindquist, P.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; Meshkov, S.; Meyers, D.; Miller, J.; Miyakawa, O.; Ogin, G.; Patel, P.; Pedraza, M.; Robertson, N. A.; Russell, P.; Samidi, M.; Sannibale, V.; Sears, B.; Sengupta, A. S.; Smith, M. R.; Stochino, A.; Tinto, M.; Tyler, W.; Vass, S.; Villar, A.; Waldman, S. J.; Wallace, L.; Ward, R.; Weinstein, A.; Whitcomb, S. E.; Willems, P. A.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Ajith, P.; Allen, B.; Aulbert, C.; Brinkmann, M.; Burmeister, O.; Fehrmann, H.; Gossler, S.; Grote, H.; Harms, J.; Hewitson, M.; Lueck, H.; Machenschalk, B.; Messenger, C. J.; Mossavi, K.; Mueller-Ebhardt, H.; Pletsch, H. J.; Prix, R.; Ruediger, A.; Schilling, R.; Schnabel, R.; Seifert, F.; Somiya, K.; Weinert, M.; Winkler, W.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Allen, B.; Anderson, W. G.; Armor, P.; Biswas, R.; Brady, P. R.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Hammer, D.; Moe, B.; Papa, M. A.; Siemens, X.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Allen, G.; Bullington, A.; Byer, R. L.; Casebolt, T.; Clark, D.; DeBra, D.; Degree, M.; Fejer, M. M.; Hennessy, M.; Lantz, B.; Leindecker, N.; Lu, P.; Markosyan, A.] Stanford Univ, Stanford, CA 94305 USA.
[Amin, R.; Giaime, J. A.; Gouaty, R.; Hanna, C.; Johnson, W. W.; Kissel, J. S.; Matichard, F.; Rodriguez, A.; Sung, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Arain, M. A.; Klimenko, S.; Lin, H.; Lucianetti, A.; Mercer, R. A.; Mitselmakher, G.; Ottens, R. S.; Pankow, C.; Quetschke, V.; Reitze, D. H.; Tanner, D. B.; Whiting, B. F.; Wu, W.] Univ Florida, Gainesville, FL 32611 USA.
[Aso, Y.; Bartos, I.; Dwyer, J. G.; Kalmus, P.; Kamat, S.; Khan, R.; Marka, S.; Marka, Z.; Matone, L.; Rollins, J.] Columbia Univ, New York, NY 10027 USA.
[Aston, S.; Cutler, R. M.; Hild, S.; Lodhia, D.; Perreca, A.; Robinson, E. L.; Vecchio, A.; Veitch, J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Aufmuth, P.; Danzmann, K.; Hage, B.; Thuering, A.; Vahlbruch, H.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Babak, S.; Chen, Y.; Degallaix, J.; Gholami, I.; Krishnan, B.; Papa, M. A.; Sintes, A. M.; Somiya, K.; Takahashi, H.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Bantilan, H.; Christensen, N.] Carleton Coll, Northfield, MN 55057 USA.
[Barker, C.; Barker, D.; Garofoli, J.; Guenther, M.; Ingram, D.; Johnson, B.; Kawabe, K.; Landry, M.; Lubinski, M.; Mendell, G.; Moreno, G.; Myers, J.; Parameshwaraiah, V.; Raab, F.; Radkins, H.; Rivera, B.; Sandberg, V.; Schwinberg, P.; Sigg, D.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA.
[Barr, B.; Barton, M. A.; Bastarrika, M.; Clark, J.; Cunningham, L.; Grant, A.; Heng, I. S.; Heptonstall, A.; Hough, J.; Huttner, S. H.; Jones, R.; Miller, J.; Murray, P.; Pitkin, M.; Reid, S.; Robertson, N. A.; Rowan, S.; Strain, K. A.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland.
[Barriga, P.; Dumas, J-C; Fan, Y.; Gras, S.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia.
[Bayer, K.; Blackburn, L.; Bodiya, T. P.; Brunet, G.; Cao, J.; Corbitt, T.; Donovan, F.; Fritschel, P.; Goda, K.; Grimaldi, F.; Harry, G.; Hughey, B.; Katsavounidis, E.; Markowitz, J.; Mason, K.; Mavalvala, N.; Mittleman, R.; Ruet, L.; Sarin, P.; Shoemaker, D. H.; Smith, N. D.; Weiss, R.] MIT, LIGO, Cambridge, MA 02139 USA.
[Beyersdorf, P. T.] San Jose State Univ, San Jose, CA 95192 USA.
[Bilenko, I. A.; Braginsky, V. B.; Khalili, F. Ya; Mitrofanov, V. P.; Vyachanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia.
[Bogue, L.; Evans, T.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Lormand, M.; O'Reilly, B.; Overmier, H.; Roddy, S.; Romie, J.; Sellers, D.; Sibley, A.; Stuver, A.; Thacker, J.; Traylor, G.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA.
[Bose, S.; Rogan, A. M.] Washington State Univ, Pullman, WA 99164 USA.
[Brau, J. E.; Frey, R.; Leonor, I.] Univ Oregon, Eugene, OR 97403 USA.
[Dalrymple, J.; Hirose, E.; Saulson, P. R.; Smith, J. R.] Syracuse Univ, Syracuse, NY 13244 USA.
[Buonanno, A.; Kanner, J.; Pan, Y.] Univ Maryland, College Pk, MD 20742 USA.
[Cadonati, L.] Univ Massachusetts, Amherst, MA 01003 USA.
[Camp, J. B.; Cannizzo, J.; Numata, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Castaldi, G.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, Y.; Savov, P.] CALTECH CaRT, Pasadena, CA 91125 USA.
[Cokelaer, T.; Davies, G.; Fairhurst, S.; Jones, G.; McKechan, D.; Robinson, C.; Schutz, B. F.; Sutton, P. J.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, Wales.
[Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy.
[Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.; Zhang, J.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Desai, S.; Finn, L. S.; Kopparapu, R. K.; Lang, M. M.; Minelli, J.; O'Shaughnessy, R.; Thorne, K. A.] Penn State Univ, University Pk, PA 16802 USA.
[Dhurandhar, S.; Mukhopadhyay, H.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Diaz, M.; Grosso, R.; Hayama, K.; Mohanty, S.; Mukherjee, S.; Romano, J. D.; Stone, R.] Univ Texas Brownsville & Texas Southmost Coll, Brownsville, TX 78520 USA.
[Dickson, J.; Lam, P. K.; McClelland, D. E.; McKenzie, K.; Rabeling, D. S.; Scott, S. M.; Searle, A. C.; Slagmolen, B. J. J.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Doomes, E. E.; McGuire, S. C.] Southern Univ, Baton Rouge, LA 70813 USA.
[Doomes, E. E.; McGuire, S. C.] A & M Coll, Baton Rouge, LA 70813 USA.
[Fricke, T.; Melissinos, A.] Univ Rochester, Rochester, NY 14627 USA.
[Hayler, T.; O'Dell, J.; Wilmut, I.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Gretarsson, A. M.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Hosken, D.; Munch, J.; Veitch, P.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Hosken, D.; Munch, J.; Veitch, P.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Kalogera, V.; Kanner, J.; Kim, C.] Northwestern Univ, Evanston, IL 60208 USA.
[Kawamura, S.; Kokeyama, K.; Leonhardt, V.; Nishizawa, A.; Sakata, S.; Sato, S.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Khazanov, E.; Kozhevatov, I.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Lockerbie, N. A.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland.
[Mandic, V.] Univ Minnesota, Minneapolis, MN 55455 USA.
[McIvor, G.] Univ Texas Austin, Austin, TX 78712 USA.
[McHugh, M.] Loyola Univ, New Orleans, LA 70118 USA.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[de la Jordana, L. Sancho; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain.
[Saraf, S.] Sonoma State Univ, Rohnert Pk, CA 94928 USA.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
RP Abbott, B (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
EM i.heng@physics.gla.ac.uk
RI Ward, Robert/I-8032-2014; Vecchio, Alberto/F-8310-2015; Mow-Lowry,
Conor/F-8843-2015; Khan, Rubab/F-9455-2015; Ottaway, David/J-5908-2015;
Postiglione, Fabio/O-4744-2015; Biswas, Rahul/H-7474-2016; Sigg,
Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms,
Jan/J-4359-2012; Bartos, Imre/A-2592-2017; Frey, Raymond/E-2830-2016;
Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen,
Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013;
Fricke, Thomas/B-6885-2013; Zhao, Chunnong/C-2403-2013; Ju,
Li/C-2623-2013; Pitkin, Matthew/I-3802-2013; Vyatchanin,
Sergey/J-2238-2012; Khazanov, Efim/B-6643-2014; Lucianetti,
Antonio/G-7383-2014; Khalili, Farit/D-8113-2012; Hild,
Stefan/A-3864-2010; Schutz, Bernard/B-1504-2010; Rowan,
Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab,
Frederick/E-2222-2011; Lueck, Harald/F-7100-2011; Kawazoe,
Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Kawabe,
Keita/G-9840-2011; Finn, Lee Samuel/A-3452-2009; Lam, Ping
Koy/A-5276-2008; McClelland, David/E-6765-2010; Martin, Iain/A-2445-2010
OI Veitch, John/0000-0002-6508-0713; Principe, Maria/0000-0002-6327-0628;
Papa, M.Alessandra/0000-0002-1007-5298; Kanner,
Jonah/0000-0001-8115-0577; Nishizawa, Atsushi/0000-0003-3562-0990;
Zweizig, John/0000-0002-1521-3397; O'Shaughnessy,
Richard/0000-0001-5832-8517; Aulbert, Carsten/0000-0002-1481-8319;
Freise, Andreas/0000-0001-6586-9901; Whiting, Bernard
F/0000-0002-8501-8669; Ward, Robert/0000-0001-5503-5241; Whelan,
John/0000-0001-5710-6576; Fairhurst, Stephen/0000-0001-8480-1961;
Boschi, Valerio/0000-0001-8665-2293; Matichard,
Fabrice/0000-0001-8982-8418; Pinto, Innocenzo M./0000-0002-2679-4457;
Minelli, Jeff/0000-0002-5330-912X; Sorazu, Borja/0000-0002-6178-3198;
Hallam, Jonathan Mark/0000-0002-7087-0461; Vecchio,
Alberto/0000-0002-6254-1617; Khan, Rubab/0000-0001-5100-5168;
Postiglione, Fabio/0000-0003-0628-3796; Biswas,
Rahul/0000-0002-0774-8906; Sigg, Daniel/0000-0003-4606-6526; Frey,
Raymond/0000-0003-0341-2636; Stein, Leo/0000-0001-7559-9597; Allen,
Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin,
Matthew/0000-0003-4548-526X; Strain, Kenneth/0000-0002-2066-5355; Lueck,
Harald/0000-0001-9350-4846; Finn, Lee Samuel/0000-0002-3937-0688; Lam,
Ping Koy/0000-0002-4421-601X; McClelland, David/0000-0001-6210-5842;
FU United States National Science Foundation for the construction and
operation of the LIGO Laboratory; Science and Technology Facilities
Council of the United Kingdom; Max-Planck-Society; State of
Niedersachsen/Germany; Australian Research Council; Council of
Scientific and Industrial Research of India; Istituto Nazionale di
Fisica Nucleare of Italy; Spanish Ministerio de Educacion y Ciencia;
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;
Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation;
Research Corporation; Alfred P Sloan Foundation; LIGO Laboratory
[LIGO-P080008-B-Z]
FX The authors gratefully acknowledge the support of 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 support of the construction and operation of
the GEO600 detector. The authors also gratefully acknowledge the support
of the research by these agencies and by the Australian Research
Council, the Council of Scientific and Industrial Research of India, the
Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio
de Educacion y Ciencia, 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 Carnegie Trust, the
Leverhulme Trust, the David and Lucile Packard Foundation, the Research
Corporation, and the Alfred P Sloan Foundation. This document has been
assigned LIGO Laboratory document number LIGO-P080008-B-Z.
NR 29
TC 19
Z9 19
U1 3
U2 14
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD DEC 21
PY 2008
VL 25
IS 24
AR 245008
DI 10.1088/0264-9381/25/24/245008
PG 21
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 379GD
UT WOS:000261383800008
ER
PT J
AU Hoskinson, AR
Hershkowitz, N
Ashpis, DE
AF Hoskinson, A. R.
Hershkowitz, N.
Ashpis, D. E.
TI Force measurements of single and double barrier DBD plasma actuators in
quiescent air
SO JOURNAL OF PHYSICS D-APPLIED PHYSICS
LA English
DT Article
ID ATMOSPHERIC-PRESSURE; DISCHARGE PLASMA; SURFACE PLASMA; MECHANISMS;
RESPONSES
AB We present the results of our experimental measurements of how variations in the discharge geometry of surface-mounted dielectric barrier discharges (DBDs) affect the force transferred to atmospheric pressure air. Our studies include both single barrier plasma actuators (one electrode insulated) and double barrier plasma actuators (both electrodes insulated) operated in quiescent air. Stagnation probe measurements of the induced air flow and direct force measurements using an electronic balance show that, for both actuator types, parallel time-averaged forces increase as the high voltage electrode diameter decreases. For single barrier actuators, this increase is exponential rather than linear as previously reported in the literature. The data from the two measurement techniques are directly proportional to one another. When the variation of velocity and pressure on all sides of an actuator are considered, the techniques show quantitative agreement.
C1 [Hoskinson, A. R.; Hershkowitz, N.] Univ Wisconsin, Dept Engn Phys, Madison, WI 53706 USA.
[Ashpis, D. E.] NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA.
RP Hoskinson, AR (reprint author), Univ Wisconsin, Dept Engn Phys, 1500 Engn Dr, Madison, WI 53706 USA.
EM arhoskinson@wisc.edu; hershkowitz@engr.wisc.edu
RI Hoskinson, Alan/F-9752-2013;
OI Ashpis, David/0000-0003-4193-6174
FU NASA [NNX07AB84A]; Air Force Office of Scientific Research (AFOSR)
[FA9550-07-1-0025]
FX This work was supported by the NASA under Cooperative Agreement
NNX07AB84A and the Air Force Office of Scientific Research (AFOSR) under
grant FA9550-07-1-0025. The authors thank Dr Riccardo Bonazza for
several helpful discussions regarding the stagnation probe calculations
and Dr Jon Ahn for helpful suggestions about pressure sensor set up.
NR 24
TC 34
Z9 36
U1 1
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0022-3727
J9 J PHYS D APPL PHYS
JI J. Phys. D-Appl. Phys.
PD DEC 21
PY 2008
VL 41
IS 24
AR 245209
DI 10.1088/0022-3727/41/24/245209
PG 9
WC Physics, Applied
SC Physics
GA 379GC
UT WOS:000261383700029
ER
PT J
AU Fischer, CF
Rubin, RH
Rodriguez, M
AF Fischer, C. Froese
Rubin, R. H.
Rodriguez, M.
TI Multiconfiguration Dirac-Hartree-Fock energy levels and transition
probabilities for 3d(5) in Fe IV
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE atomic data; atomic processes
ID IRON PROJECT; ATOMIC DATA; NEBULA; EXCITATION
AB Multiconfiguration Dirac-Hartree-Fock electric quadrupole (E2) and magnetic dipole (M1) transition probabilities are reported for transitions between levels of 3d(5) in [Fe IV]. The accuracy of the ab initio energy levels and the agreement in the length and velocity forms of the line strength for the E2 transitions are used as indicators of accuracy. The present E2 and M1 transition probabilities are compared with earlier Breit-Pauli results and other theories. An extensive set of transition probabilities with indicators of accuracy are reported in Appendices A and B. Recommended values of A(E2) + A(M1) are listed in Appendix C.
C1 [Fischer, C. Froese] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA.
[Rubin, R. H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rubin, R. H.] Orion Enterprises, Moffett Field, CA 94035 USA.
[Rubin, R. H.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Rodriguez, M.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico.
RP Fischer, CF (reprint author), Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA.
EM charlotte.fischer@nist.gov
FU NASA [HST-AR-10973.01-A, NAS5-26555]; Mexican CONACYT [50359-F]
FX Support for this publication was provided by NASA through programme
number HST-AR-10973.01-A (PI RR) from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, under NASA contract NAS5-26555. MR acknowledges
support from Mexican CONACYT project 50359-F.
NR 23
TC 8
Z9 8
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 21
PY 2008
VL 391
IS 4
BP 1828
EP 1837
DI 10.1111/j.1365-2966.2008.13997.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 382PD
UT WOS:000261617000026
ER
PT J
AU Helling, C
Ackerman, A
Allard, F
Dehn, M
Hauschildt, P
Homeier, D
Lodders, K
Marley, M
Rietmeijer, F
Tsuji, T
Woitke, P
AF Helling, Ch.
Ackerman, A.
Allard, F.
Dehn, M.
Hauschildt, P.
Homeier, D.
Lodders, K.
Marley, M.
Rietmeijer, F.
Tsuji, T.
Woitke, P.
TI A comparison of chemistry and dust cloud formation in ultracool dwarf
model atmospheres
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: atmospheres; stars: low-mass; brown dwarfs
ID LOW-MASS STARS; BROWN DWARFS; T-DWARFS; PHOTOSPHERIC ENVIRONMENT;
CHEMICAL-COMPOSITION; CIRCUMSTELLAR DUST; PHOTOMETRIC SYSTEM;
CONDENSATION; TEMPERATURE; ABUNDANCES
AB The atmospheres of substellar objects contain clouds of oxides, iron, silicates and other refractory condensates. Water clouds are expected in the coolest objects. The opacity of these 'dust' clouds strongly affects both the atmospheric temperature-pressure profile and the emergent flux. Thus, any attempt to model the spectra of these atmospheres must incorporate a cloud model. However, the diversity of cloud models in atmospheric simulations is large and it is not always clear how the underlying physics of the various models compare. Likewise, the observational consequences of different modelling approaches can be masked by other model differences, making objective comparisons challenging. In order to clarify the current state of the modelling approaches, this paper compares five different cloud models in two sets of tests. Test case 1 tests the dust cloud models for a prescribed L-, L-T and T-dwarf atmospheric ( temperature T, pressure p, convective velocity v(conv)) structures. Test case 2 compares complete model atmosphere results for given ( effective temperature T(eff), surface gravity log g). All models agree on the global cloud structure but differ in opacity relevant details such as grain size, amount of dust, dust and gas-phase composition. These models can loosely be grouped into high- and low-altitude cloud models whereas the first appears generally redder in near-infrared colours than the latter. Comparisons of synthetic photometric fluxes translate into a modelling uncertainty in apparent magnitudes for our L-dwarf (T-dwarf) test case of 0.25 <= Delta m <= 0.875 (0.1 <= Delta m <= 1.375), taking into account the Two-Micron All Sky Survey, the UKIRT WFCAM, the Spitzer IRAC and VLT VISIR filters with UKIRT WFCAM being the most challenging for the models. Future developments will need closer links with laboratory astrophysics, and a consistent treatment of the cloud chemistry and turbulence.
C1 [Helling, Ch.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Ackerman, A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Allard, F.] Univ Lyon, Ecole Normale Super Lyon, CNRS, Ctr Rech Astrophys Lyon,UMR5574, F-69634 Lyon, France.
[Allard, F.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Dehn, M.; Hauschildt, P.] Hamburger Sternwarte, D-21029 Hamburg, Germany.
[Homeier, D.] Univ Gottingen, Inst Astrophys, D-137077 Gottingen, Germany.
[Lodders, K.] Washington Univ, Dept Earth & Planetary Sci, Planetary Chem Lab, St Louis, MO 63130 USA.
[Marley, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rietmeijer, F.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Tsuji, T.] Univ Tokyo, Inst Astron, Tokyo 1810015, Japan.
[Woitke, P.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
RP Helling, C (reprint author), Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
EM Christiane.Helling@st-and.ac.uk
RI Ackerman, Andrew/D-4433-2012; Marley, Mark/I-4704-2013;
OI Ackerman, Andrew/0000-0003-0254-6253; Homeier, Derek/0000-0002-8546-9128
FU Lorentz Center of the University Leiden; Nederlandse Organisatie voor
Wetenschappelijk Onderzoek; The Netherlands research School for
Astronomy; Scottish University Physics Alliance and European Space
Agency
FX We thank the anonymous referee for the valuable report. ChH thanks Alkes
Scholz and Soren Witte for helpful discussions on the manuscript. We
thank the participants of the workshop From Brown Dwarfs to Planets:
Chemistry and Cloud Formation which was supported by the Lorentz Center
of the University Leiden, Nederlandse Organisatie voor Wetenschappelijk
Onderzoek, The Netherlands research School for Astronomy, the Scottish
University Physics Alliance and European Space Agency.
NR 92
TC 96
Z9 97
U1 2
U2 5
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 21
PY 2008
VL 391
IS 4
BP 1854
EP 1873
DI 10.1111/j.1365-2966.2008.13991.x
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 382PD
UT WOS:000261617000028
ER
PT J
AU Rucinski, SM
Matthews, JM
Kuschnig, R
Pojmanski, G
Rowe, J
Guenther, DB
Moffat, AFJ
Sasselov, D
Walker, GAH
Weiss, WW
AF Rucinski, Slavek M.
Matthews, Jaymie M.
Kuschnig, Rainer
Pojmanski, Grzegorz
Rowe, Jason
Guenther, David B.
Moffat, Anthony F. J.
Sasselov, Dimitar
Walker, Gordon A. H.
Weiss, Werner W.
TI Photometric variability of the T Tauri star TW Hya on time-scales of
hours to years
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: pre-main-sequence; stars: variables: other
ID SKY AUTOMATED SURVEY; HYDRAE ASSOCIATION; SOUTHERN-HEMISPHERE;
VARIABLE-STARS; CATALOG; DISK; DISCOVERY; MEMBERS; CANDIDATE; QUARTER
AB Microvariability & Oscillations of STars ( MOST) and All Sky Automated Survey (ASAS) observations have been used to characterize photometric variability of TW Hya on time-scales from a fraction of a day to 7.5 weeks and from a few days to 8 yr, respectively. The two data sets have very different uncertainties and temporal coverage properties and cannot be directly combined, nevertheless, they suggest a global variability spectrum with 'flicker-noise' properties, that is with amplitudes a alpha 1/root f, over >4 decades in frequency, in the range f = 0.0003-10 cd(-1). A 3.7 d period is clearly present in the continuous 11 d, 0.07 d time resolution, observations by MOST in 2007. Brightness extrema coincide with zero-velocity crossings in periodic (3.56 d) radial-velocity variability detected in contemporaneous spectroscopic observations of Setiawan et al. and interpreted as caused by a planet. The 3.56/3.7 d periodicity was entirely absent in the second, 4 times longer MOST run in 2008, casting doubt on the planetary explanation. Instead, a spectrum of unstable single periods within the range of 2-9 d was observed; the tendency of the periods to progressively shorten was well traced using the wavelet analysis. The evolving periodicities and the overall flicker-noise characteristics of the TW Hya variability suggest a combination of several mechanisms, with the dominant ones probably related to the accretion processes from the disc around the star.
C1 [Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Matthews, Jaymie M.; Kuschnig, Rainer; Walker, Gordon A. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Pojmanski, Grzegorz] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Rowe, Jason] NASA Ames Res Pk, Moffett Field, CA 94035 USA.
[Guenther, David B.] St Marys Univ, Inst Computat Astrophys, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Moffat, Anthony F. J.] Ctr Res Astrophys Quebec, Quebec City, PQ, Canada.
[Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
RP Rucinski, SM (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
EM rucinski@astro.utoronto.ca
FU Natural Sciences and Engineering Research Council of Canada; AFJM; FQRNT
(Quebec); Canadian Space Agency; Austrian Space Agency; Austrian Science
Fund; Polish Ministry of Science [N20300731/1328]
FX The Natural Sciences and Engineering Research Council of Canada supports
the research of DBG, JMM, AFJM and SMR. Additional support for AFJM
comes from FQRNT (Quebec). RK is supported by the Canadian Space Agency
and WWW is supported by the Austrian Space Agency and the Austrian
Science Fund. GP acknowledges the research grant N20300731/1328 from
Polish Ministry of Science.; Special thanks are extended to Ray
Jayawardhana, Marten van Kerkwijk and Alexis Brandeker for very useful
comments and to John Percy for an excellent review.; This research has
made use of the SIMBAD data base, operated at CDS, Strasbourg, France
and NASA's Astrophysics Data System ( ADS) Bibliographic Services.
NR 34
TC 44
Z9 44
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 21
PY 2008
VL 391
IS 4
BP 1913
EP 1924
DI 10.1111/j.1365-2966.2008.14014.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 382PD
UT WOS:000261617000033
ER
PT J
AU Maraschi, L
Foschini, L
Ghisellini, G
Tavecchio, F
Sambruna, RM
AF Maraschi, L.
Foschini, L.
Ghisellini, G.
Tavecchio, F.
Sambruna, R. M.
TI Testing the blazar spectral sequence: X-ray-selected blazars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; galaxies: active; galaxies: jets
ID RADIO-LOUD QUASARS; BL LACERTAE OBJECTS; FLUX-DENSITY VARIATIONS; ACTIVE
GALACTIC NUCLEI; MEDIUM-SENSITIVITY SURVEY; LINE SEYFERT-1 GALAXIES;
BURST ALERT TELESCOPE; JET-DISK CONNECTION; LOW-ENERGY CUTOFFS;
GAMMA-RAYS
AB We present simultaneous optical and X-ray data from Swift for a sample of radio-loud flat-spectrum quasars selected from the Einstein Medium Sensitivity Survey (EMSS). We present also a complete analysis of Swift and INTEGRAL data on four blazars recently discussed as possibly challenging the trends of the hypothesized 'blazar spectral sequence'. The spectral energy distributions (SEDs) of all these objects are modelled in terms of a general theoretical scheme, applicable to all blazars, leading to an estimate of the jets' physical parameters. Our results show that, in the case of the EMSS broad line blazars, X-ray selection does not lead to find sources with synchrotron peaks in the UV/X-ray range, as was the case for X-ray-selected BL Lacs. Instead, for a wide range of radio powers all the sources with broad emission lines show similar SEDs, with synchrotron components peaking below the optical/UV range. The SED models suggest that the associated inverse Compton (IC) emission should peak below the GeV range, but could be detectable in some cases by the Fermi Gamma-ray Space Telescope. Of the remaining four 'anomalous' blazars, two highly luminous sources with broad lines, claimed to possibly emit synchrotron X-rays, are shown to be better described with IC models for their X-ray emission. For one source with weak emission lines ( a BL Lac object) a synchrotron peak in the soft X-ray range is confirmed, while for the fourth source, exhibiting narrow emission lines typical of narrow-line Seyfert 1 galaxies, no evidence of X-ray emission from a relativistic jet is found. We re-examine the standing and interpretation of the original 'blazar spectral sequence' and suggest that the photon ambient, in which the particle acceleration and emission occur, is likely the main factor determining the shape of the blazar SED. A connection between SED shape and jet power/luminosity can however result through the link between the mass and accretion rate of the central black hole and the radiative efficiency of the resulting accretion flow, thus involving at least two parameters.
C1 [Maraschi, L.; Ghisellini, G.; Tavecchio, F.] Osserv Astron Brera, INAF, I-20100 Milan, Italy.
[Foschini, L.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Sambruna, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Maraschi, L (reprint author), Osserv Astron Brera, INAF, V Brera 28, I-20100 Milan, Italy.
EM laura.maraschi@brera.inaf.it
RI Foschini, Luigi/H-3833-2012;
OI Foschini, Luigi/0000-0001-8678-0324; Ghisellini,
Gabriele/0000-0002-0037-1974
FU Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration; Alfred P. Sloan Foundation;
Participating Institutions; National Science Foundation; US Department
of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education
Funding Council for England; American Museum of Natural History;
Astrophysical Institute Potsdam; University of Basel; University of
Cambridge; Case Western Reserve University; University of Chicago,
Drexel University, Fermilab; Institute for Advanced Study; Japan
Participation Group; Johns Hopkins University; Joint Institute for
Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and
Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST),
Los Alamos National Laboratory; Max-Planck-Institute for Astronomy
(MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington; ASI/INAF [I/088/06/0]
FX We acknowledge funding from ASI/INAF with contract I/088/06/0.
NR 75
TC 29
Z9 29
U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 21
PY 2008
VL 391
IS 4
BP 1981
EP 1993
DI 10.1111/j.1365-2966.2008.14030.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 382PD
UT WOS:000261617000040
ER
PT J
AU Hair, JW
Hostetler, CA
Cook, AL
Harper, DB
Ferrare, RA
Mack, TL
Welch, W
Izquierdo, LR
Hovis, FE
AF Hair, Johnathan W.
Hostetler, Chris A.
Cook, Anthony L.
Harper, David B.
Ferrare, Richard A.
Mack, Terry L.
Welch, Wayne
Izquierdo, Luis Ramos
Hovis, Floyd E.
TI Airborne High Spectral Resolution Lidar for profiling aerosol optical
properties
SO APPLIED OPTICS
LA English
DT Article
ID SINGLE-FREQUENCY OPERATION; IODINE ABSORPTION FILTER; RAYLEIGH-MIE
LIDAR; ND-YAG LASERS; RAMAN LIDAR; SCATTERING PROPERTIES; ATMOSPHERIC
AEROSOLS; EXTINCTION; STABILIZATION; CALIBRATION
AB A compact, highly robust airborne High Spectral Resolution Lidar (HSRL) that provides measurements of aerosol backscatter and extinction coefficients and aerosol depolarization at two wavelengths has been developed, tested, and deployed on nine field experiments (over 650 flight hours). A unique and advantageous design element of the HSRL system is the ability to radiometrically calibrate the instrument internally, eliminating any reliance on vicarious calibration from atmospheric targets for which aerosol loading must be estimated. This paper discusses the design of the airborne HSRL, the internal calibration and accuracy of the instrument, data products produced, and observations and calibration data from the first two field missions: the Joint Intercontinental Chemical Transport Experiment-Phase B (INTEX-B)/Megacity Aerosol Experiment-Mexico City (MAX-Mex)/Megacities Impacts on Regional and Global Environment (MILAGRO) field mission (hereafter MILAGRO) and the Gulf of Mexico Atmospheric Composition and Climate Study/Texas Air Quality Study II (hereafter GoMACCS/TexAQS II). (C) 2008 Optical Society of America
C1 [Hair, Johnathan W.; Hostetler, Chris A.; Cook, Anthony L.; Harper, David B.; Ferrare, Richard A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Mack, Terry L.] Langley Res Ctr, Hampton, VA 23681 USA.
[Welch, Wayne] Welch Mech Designs LLC, Havre De Grace, MD 21078 USA.
[Izquierdo, Luis Ramos] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hovis, Floyd E.] Fibertek Inc, Herndon, VA 20170 USA.
RP Hair, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM johnathan.w.hair@nasa.gov
FU NASA LaRC; NASA HQ Science Mission Directorate; NASA CALIPSO Project;
U.S. Department of Energy's Atmospheric Science Program
[DE-AI02-05ER63985]; NASA LaRC Research Services Directorate
FX The authors thank the two reviewers for their detailed reviews that
improved the manuscript. We also acknowledge the support of the NASA
LaRC, NASA HQ Science Mission Directorate, and the NASA CALIPSO Project
for funding the development of the HSRL instrument. The deployment of
the HSRL in these field experiments were supported in part by the U.S.
Department of Energy's Atmospheric Science Program (Office of Science,
BER, Grant DE-AI02-05ER63985). We also acknowledge the aircraft flight
support provided by personnel in the NASA LaRC Research Services
Directorate.
NR 44
TC 177
Z9 187
U1 3
U2 40
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD DEC 20
PY 2008
VL 47
IS 36
BP 6734
EP 6752
DI 10.1364/AO.47.006734
PG 19
WC Optics
SC Optics
GA 395AQ
UT WOS:000262494800006
PM 19104525
ER
PT J
AU Kwiatkowska, EJ
Franz, BA
Meister, G
McClain, CR
Xiong, XX
AF Kwiatkowska, Ewa J.
Franz, Bryan A.
Meister, Gerhard
McClain, Charles R.
Xiong, Xiaoxiong
TI Cross calibration of ocean-color bands from Moderate Resolution Imaging
Spectroradiometer on Terra platform
SO APPLIED OPTICS
LA English
DT Article
ID ON-ORBIT CALIBRATION; REFLECTIVE SOLAR BANDS; WATER-LEAVING RADIANCE;
ATMOSPHERIC CORRECTION; POLARIZATION-SENSITIVITY; SPECTRAL REFLECTANCE;
SEAWIFS; ALGORITHM; INSTRUMENT; SENSORS
AB Ocean-color applications require maxi main uncertainties in blue-wavelength water-leaving radiances in oligotrophic ocean of approximately 5%. Water-leaving radiances from Moderate Resolution Imaging Spectroradiometer (MODIS) on the Terra satellite, however, exhibit temporal drift of the order of 15% as well as sensor changes in response versus scan and polarization sensitivity, which cannot be tracked by onboard calibrators. This paper introduces an instrument characterization approach that uses Earth-view data as a calibration source. The approach models the top of the atmosphere signal over ocean that the instrument is expected to measure, including its polarization, with water-leaving radiances coming from another well-calibrated global sensor. The cross calibration allows for significant improvement in derived MODIS-Terra ocean-color products, with largest changes in the blue wavelengths. (C) 2008 Optical Society of America
C1 [Kwiatkowska, Ewa J.; Franz, Bryan A.; Meister, Gerhard; McClain, Charles R.] NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA.
[Kwiatkowska, Ewa J.; Franz, Bryan A.] Sci Applicat Int Corp, Beltsville, MD 20705 USA.
[Meister, Gerhard] Futuretech Corp, Greenbelt, MD 20770 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Moderate Resolut Imaging Spectroradiometer Charac, Greenbelt, MD 20771 USA.
RP Kwiatkowska, EJ (reprint author), NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA.
EM ewa.kwiatkowska@gmail.com
RI Franz, Bryan/D-6284-2012; Meister, Gerhard/F-7159-2012
OI Franz, Bryan/0000-0003-0293-2082;
FU NASA Research Opportunities in Space and Earth Sciences (ROSES);
validation solicitation funding
FX This work was supported under the NASA Research Opportunities in Space
and Earth Sciences (ROSES) 2006 calibration and validation solicitation
funding.
NR 45
TC 43
Z9 43
U1 1
U2 5
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD DEC 20
PY 2008
VL 47
IS 36
BP 6796
EP 6810
DI 10.1364/AO.47.006796
PG 15
WC Optics
SC Optics
GA 395AQ
UT WOS:000262494800012
PM 19104531
ER
PT J
AU Numata, K
Camp, J
AF Numata, Kenji
Camp, Jordan
TI Interferometric testbed for nanometer level stabilization of
environmental motion over long time scales
SO APPLIED OPTICS
LA English
DT Article
AB We developed an interferometric testbed to stabilize environmental motions over time scales of several hours and a length scale of 1 m. Typically, thermal and seismic motions on the ground are larger than 1 mu m over these scales, affecting the precision of more sensitive measurements. To suppress such motions, we built an active stabilization system composed of interferometric sensors, a hexapod actuator, and a frequency-stabilized laser. With this stabilized testbed, environmental motions were Suppressed down to the nanometer level. This system will allow us to perform sensitive measurements, such as ground testing of the Laser Interferometer Space Antenna, in the presence of enviromental noise. (C) 2008 Optical Society of America
C1 [Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Numata, Kenji; Camp, Jordan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Numata, K (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM Kenji.Numata@nasa.gov
NR 15
TC 6
Z9 6
U1 0
U2 4
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD DEC 20
PY 2008
VL 47
IS 36
BP 6832
EP 6841
DI 10.1364/AO.47.006832
PG 10
WC Optics
SC Optics
GA 395AQ
UT WOS:000262494800015
PM 19104534
ER
PT J
AU Campbell, J
AF Campbell, Joel
TI Synthetic quadrature phase detector/demodulator for Fourier transform
spectrometers
SO APPLIED OPTICS
LA English
DT Article
ID DEMODULATION
AB A method is developed to demodulate (velocity correct) Fourier transform spectrometer data that are taken with an analog to digital converter that digitizes equally spaced in time. This method makes it possible to use simple low-cost, high-resolution audio digitizers to record high-quality data without the need For an event timer or quadrature laser hardware and makes it possible to use a metrology laser of any wavelength. The reduced parts count and simple implementation make it an attractive alternative in space-based applications when compared to previous methods such as the Brault algorithm. (C) 2008 Optical Society of America
C1 NASA, Langley Res Ctr, Hampton, VA 23662 USA.
RP Campbell, J (reprint author), NASA, Langley Res Ctr, MS 488, Hampton, VA 23662 USA.
EM joel.f.campbell@nasa.gov
NR 12
TC 5
Z9 6
U1 1
U2 1
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD DEC 20
PY 2008
VL 47
IS 36
BP 6889
EP 6894
DI 10.1364/AO.47.006889
PG 6
WC Optics
SC Optics
GA 395AQ
UT WOS:000262494800023
PM 19104542
ER
PT J
AU MacTavish, CJ
Ade, PAR
Battistelli, ES
Benton, S
Bihary, R
Bock, JJ
Bond, JR
Brevik, J
Bryan, S
Contaldi, CR
Crill, BP
Dore, O
Fissel, L
Golwala, SR
Halpern, M
Hilton, G
Holmes, W
Hristov, VV
Irwin, K
Jones, WC
Kuo, CL
Lange, AE
Lawrie, C
Martin, TG
Mason, P
Montroy, TE
Netterfield, CB
Riley, D
Ruhl, JE
Runyan, M
Trangsrud, A
Tucker, C
Turner, A
Viero, M
Wiebe, D
AF MacTavish, C. J.
Ade, P. A. R.
Battistelli, E. S.
Benton, S.
Bihary, R.
Bock, J. J.
Bond, J. R.
Brevik, J.
Bryan, S.
Contaldi, C. R.
Crill, B. P.
Dore, O.
Fissel, L.
Golwala, S. R.
Halpern, M.
Hilton, G.
Holmes, W.
Hristov, V. V.
Irwin, K.
Jones, W. C.
Kuo, C. L.
Lange, A. E.
Lawrie, C.
Martin, T. G.
Mason, P.
Montroy, T. E.
Netterfield, C. B.
Riley, D.
Ruhl, J. E.
Runyan, M.
Trangsrud, A.
Tucker, C.
Turner, A.
Viero, M.
Wiebe, D.
TI SPIDER OPTIMIZATION: PROBING THE SYSTEMATICS OF A LARGE-SCALE B-MODE
EXPERIMENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic microwave background; gravitational waves; methods: data
analysis; polarization
ID BACKGROUND POLARIZATION MEASUREMENTS; TRANSITION-EDGE SENSORS; 2003
FLIGHT; WMAP OBSERVATIONS; POWER SPECTRUM; CMB TEMPERATURE; ANISOTROPY;
BOOMERANG; MULTIPLEXER; INFLATION
AB Spider is a long-duration, balloon-borne polarimeter designed to measure large-scale cosmic microwave background (CMB) polarization with very high sensitivity and control of systematics. The instrument will map over half the sky with degree angular resolution in the I, Q, and U Stokes parameters in four frequency bands from 96 to 275 GHz. Spider's ultimate goal is to detect the primordial gravity-wave signal imprinted on the CMB B-mode polarization. One of the challenges in achieving this goal is the minimization of the contamination of B-modes by systematic effects. This paper explores a number of instrument systematics and observing strategies in order to optimize B-mode sensitivity. This is done by injecting realistic-amplitude, time-varying systematics into a set of simulated time streams. Tests of the impact of detector noise characteristics, pointing jitter, payload pendulations, polarization angle offsets, beam systematics, and receiver gain drifts are shown. Spider's default observing strategy is to spin continuously in azimuth, with polarization modulation achieved by either a rapidly spinning half-wave plate or a rapidly spinning gondola and a slowly stepped half-wave plate. Although the latter is more susceptible to systematics, the results shown here indicate that either mode of operation can be used by Spider.
C1 [MacTavish, C. J.; Bond, J. R.; Crill, B. P.; Dore, O.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Ade, P. A. R.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Battistelli, E. S.; Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Benton, S.; Netterfield, C. B.; Wiebe, D.] Univ Toronto, Dept Phys, Toronto, ON M5S 3H8, Canada.
[Bihary, R.; Bryan, S.; Lawrie, C.; Montroy, T. E.; Riley, D.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Bock, J. J.; Brevik, J.; Holmes, W.; Jones, W. C.; Turner, A.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, J. J.; Golwala, S. R.; Hristov, V. V.; Jones, W. C.; Kuo, C. L.; Lange, A. E.; Mason, P.; Runyan, M.; Trangsrud, A.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Contaldi, C. R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2A, England.
[Crill, B. P.; Fissel, L.; Netterfield, C. B.; Viero, M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Hilton, G.; Irwin, K.] Natl Inst Stand & Technol, Boulder, CO 80305 USA.
[Martin, T. G.] Univ Toronto, Dept Mech & Ind Engn, Toronto, ON M5S 3G8, Canada.
RP MacTavish, CJ (reprint author), Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
FU Canada Foundation for Innovation
FX This research used the McKenzie cluster at CITA, funded by the Canada
Foundation for Innovation. Some of the results in this paper have been
derived using the HEALPix package (Gorski et al. 2005), as well as the
FFTW package (Frigo & Johnson 2005). We thank the anonymous referee for
helpful comments and corrections.
NR 49
TC 15
Z9 15
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 DEC 20
PY 2008
VL 689
IS 2
BP 655
EP 665
DI 10.1086/592732
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 376NF
UT WOS:000261189600001
ER
PT J
AU Ajello, M
Greiner, J
Sato, G
Willis, DR
Kanbach, G
Strong, AW
Diehl, R
Hasinger, G
Gehrels, N
Markwardt, CB
Tueller, J
AF Ajello, M.
Greiner, J.
Sato, G.
Willis, D. R.
Kanbach, G.
Strong, A. W.
Diehl, R.
Hasinger, G.
Gehrels, N.
Markwardt, C. B.
Tueller, J.
TI COSMIC X-RAY BACKGROUND AND EARTH ALBEDO SPECTRA WITH SWIFT BAT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology observations; diffuse radiation; Earth; galaxies: active;
X-rays: diffuse background
ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; XMM-NEWTON; BLACK-HOLES;
GAMMA-RAYS; CHANDRA; AGNS; SPECTROMETERS; POPULATION; TELESCOPE
AB We use Swift BAT Earth occultation data at different geomagnetic latitudes to derive a sensitive measurement of the cosmic X-ray background (CXB) and of the Earth albedo emission in the 15-200 keV band. We compare our CXB spectrum with recent (INTEGRAL, BeppoSAX) and past results (HEAO-1) and find good agreement. Using an independent measurement of the CXB spectrum we are able to confirm our results. This study shows that the BAT CXB spectrum has a normalization similar to 8% +/- 3% larger than the HEAO-1 measurement. The BAT accurate Earth albedo spectrum can be used to predict the level of photon background for satellites in low Earth and mid inclination orbits.
C1 [Ajello, M.; Greiner, J.; Willis, D. R.; Kanbach, G.; Strong, A. W.; Diehl, R.; Hasinger, G.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Sato, G.; Gehrels, N.; Markwardt, C. B.; Tueller, J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Ajello, M (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany.
RI Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012
FU DFG Leibniz-Prize [HA 1850/28-1]
FX We are grateful to S. Barthelmy, J. Cummings and H. Krimm for all the
effort spent in keeping the BAT perfectly operating. M. A. acknowledges
the useful suggestions of R. Mushotzky and the help of C. Gordon for
adapting XSPEC to the purposes of this analysis. The anonymous referee
is acknowledged for his/her helpful comments which improved the
manuscript. M. A. is grateful to S. Sazonov and A. Zoglauer for
interesting discussions about the Earth emission. This research has made
use of data obtained from the High Energy Astrophysics Science Archive
Research Center (HEASARC) provided by NASA's Goddard Space Flight
Center. M.A. acknowledges funding from the DFG Leibniz-Prize to G.H. (HA
1850/28-1).
NR 44
TC 86
Z9 86
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2008
VL 689
IS 2
BP 666
EP 677
DI 10.1086/592595
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 376NF
UT WOS:000261189600002
ER
PT J
AU Gehrels, N
Barthelmy, SD
Burrows, DN
Cannizzo, JK
Chincarini, G
Fenimore, E
Kouveliotou, C
O'Brien, P
Palmer, DM
Racusin, J
Roming, PWA
Sakamoto, T
Tueller, J
Wijers, RAMJ
Zhang, B
AF Gehrels, N.
Barthelmy, S. D.
Burrows, D. N.
Cannizzo, J. K.
Chincarini, G.
Fenimore, E.
Kouveliotou, C.
O'Brien, P.
Palmer, D. M.
Racusin, J.
Roming, P. W. A.
Sakamoto, T.
Tueller, J.
Wijers, R. A. M. J.
Zhang, B.
TI CORRELATIONS OF PROMPT AND AFTERGLOW EMISSION IN SWIFT LONG AND SHORT
GAMMA-RAY BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE gamma rays: bursts
ID SPECTRAL-ENERGY CORRELATIONS; X-RAY; OPTICAL AFTERGLOW; LIGHT CURVES;
HOST GALAXY; XRT DATA; MULTIWAVELENGTH AFTERGLOW; COMPREHENSIVE
ANALYSIS; CHROMATIC BREAKS; SHALLOW DECAY
AB Correlation studies of prompt and afterglow emission from gamma-ray bursts (GRBs) between different spectral bands have been difficult to do in the past because few bursts had comprehensive and comparable afterglow measurements. In this paper we present a large and uniform data set for correlation analysis based on bursts detected by the Swift mission. For the first time, short and long bursts can be analyzed and compared. It is found for both classes that the optical, X-ray, and gamma-ray emission are linearly correlated, but with a large spread about the correlation line; stronger bursts tend to have brighter afterglow, and bursts with brighter X-ray afterglow tend to have brighter optical afterglow. Short bursts are, on average, weaker in both prompt and afterglow emission. No short bursts are seen with extremely low optical Y to YX-ray ratios, as occurs for "dark'' long bursts. Although statistics are still poor for short bursts, there is no evidence yet for a subgroup of short bursts with high extinction, as there is for long bursts. Long bursts are detected in the dark category in the same fraction as pre-Swift bursts. Interesting cases of long bursts that are detected in the optical, and yet have a low enough optical Y to YX-ray ratio to be classified as dark, are discovered. For the prompt emission, short and long bursts have different average tracks on flux versus fluence plots. In Swift, GRB detections tend to be fluence-limited for short bursts and flux-limited for long events.
C1 [Gehrels, N.; Barthelmy, S. D.; Cannizzo, J. K.; Sakamoto, T.; Tueller, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Burrows, D. N.; Racusin, J.; Roming, P. W. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Cannizzo, J. K.; Sakamoto, T.] Univ Maryland Baltimore Cty, CRESST, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Chincarini, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Chincarini, G.] Univ Milan, I-20126 Milan, Italy.
[Fenimore, E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Kouveliotou, C.] NSSTC, NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[O'Brien, P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, Fac Sci, NL-1098 SJ Amsterdam, Netherlands.
[Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
RP Gehrels, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM neil.gehrels@nasa.gov
RI Racusin, Judith/D-2935-2012; Barthelmy, Scott/D-2943-2012; Gehrels,
Neil/D-2971-2012; Tueller, Jack/D-5334-2012;
OI Wijers, Ralph/0000-0002-3101-1808
NR 119
TC 65
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U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2008
VL 689
IS 2
BP 1161
EP 1172
DI 10.1086/592766
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 376NF
UT WOS:000261189600038
ER
PT J
AU Sahai, R
Findeisen, K
De Paz, AG
Contreras, CS
AF Sahai, R.
Findeisen, K.
De Paz, A. Gil
Contreras, C. Sanchez
TI BINARITY IN COOL ASYMPTOTIC GIANT BRANCH STARS: A GALEX SEARCH FOR
ULTRAVIOLET EXCESSES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; circumstellar matter; planetary nebulae: general;
stars: AGB and post-AGB; stars: mass loss
ID HUBBLE-SPACE-TELESCOPE; PLANETARY-NEBULAE; MIRA-B; H-2 EMISSION;
V-HYDRAE; OUTFLOW; SPECTRA; DISK; CLASSIFICATION; PERFORMANCE
AB The search for binarity in AGB stars is of critical importance for our understanding of how planetary nebulae acquire the dazzling variety of aspherical shapes which characterizes this class. However, detecting binary companions in such stars has been severely hampered due to their extreme luminosities and pulsations. We have carried out a small imaging survey of AGB stars in ultraviolet light (using GALEX), where these cool objects are very faint, in order to search for hotter companions. We report the discovery of significant far-ultraviolet excesses toward nine of these stars. The far-ultraviolet excess most likely results either directly from the presence of a hot binary companion or indirectly from a hot accretion disk around the companion.
C1 [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Findeisen, K.] Cornell Univ, Ithaca, NY 14853 USA.
[De Paz, A. Gil] Univ Complutense Madrid, Dept Astrofis, E-28040 Madrid, Spain.
[Contreras, C. Sanchez] CSIC, Inst Estructura Mat, Dept Astrofis Mol & Infraroja, E-28006 Madrid, Spain.
RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-900, Pasadena, CA 91109 USA.
RI Sanchez-Contreras, Carmen/N-3718-2015; Gil de Paz, Armando/J-2874-2016;
OI Sanchez-Contreras, Carmen/0000-0002-6341-592X; Gil de Paz,
Armando/0000-0001-6150-2854; Findeisen, Krzysztof/0000-0003-1898-5760
FU Spanish Ramon y Cajal program; Programa Nacional de Astronomia y
Astrofisica [AYA 2006-02358]; Spanish MCyT [AYA 2006-14876]; Spanish MEC
[PIE 200750I028]
FX We would like to thank an anonymous referee for his/ her thoughtful
review of our paper. We acknowledge discussions with Patrick Morrissey
related to the possibility of red leaks in the GALEX FUV and NUV bands.
R. S.' s contribution to the research described in this publication was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. R. S. thanks NASA for financial
support via a GALEX award and an LTSA award. K. F. was partially funded
by a SURF scholarship and through the Cornell Presidential Research
Scholars (CPRS) program. A. G. d. P. is partially financed by the
Spanish Ramon y Cajal program and the Programa Nacional de Astronomia y
Astrofisica under grant AYA 2006-02358. C. S. C. is partially funded for
this work by the Spanish MCyT under project AYA 2006-14876 and the
Spanish MEC under project PIE 200750I028.
NR 34
TC 21
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2008
VL 689
IS 2
BP 1274
EP 1278
DI 10.1086/592559
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 376NF
UT WOS:000261189600047
ER
PT J
AU Saumon, D
Marley, MS
AF Saumon, D.
Marley, Mark S.
TI THE EVOLUTION OF L AND T DWARFS IN COLOR-MAGNITUDE DIAGRAMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE stars: atmospheres; stars: evolution; stars: low-mass, brown dwarfs
ID LOW-MASS STARS; EXTRASOLAR GIANT PLANETS; COLLISION-INDUCED ABSORPTION;
BROWN DWARFS; STELLAR ATMOSPHERES; SUBSTELLAR OBJECTS; L/T TRANSITION;
INFRARED PHOTOMETRY; THERMAL STRUCTURE; ULTRACOOL DWARFS
AB We present new evolution sequences for very low mass stars, brown dwarfs, and giant planets and use them to explore a variety of influences on the evolution of these objects. While the predicted adiabatic evolution of luminosity with time is very similar to results of previous work, the remaining disagreements reveal the magnitude of current uncertainty in brown dwarf evolution theory. We discuss the sources of those differences and argue for the importance of the surface boundary condition provided by atmosphere models including clouds. The L- to T-type ultracool dwarf transition can be accommodated within the Ackerman and Marley cloud model by varying the cloud sedimentation parameter. We develop a simple model for the evolution across the L/T transition. By combining the evolution calculation and our atmosphere models, we generate colors and magnitudes of synthetic populations of ultracool dwarfs in the field and in Galactic clusters. We focus on near-infrared color-magnitude diagrams (CMDs) and on the nature of the "second parameter'' that is responsible for the scatter of colors along the T(eff) sequence. Instead of a single second parameter we find that variations in metallicity and cloud parameters, unresolved binaries, and possibly a relatively young population all play a role in defining the spread of brown dwarfs along the cooling sequence. We also find that the transition from cloudy L dwarfs to cloudless T dwarfs slows down the evolution and causes a pileup of substellar objects in the transition region, in contradiction with previous studies. However, the same model is applied to the Pleiades brown dwarf sequence with less success. Taken at face value, the present Pleiades data suggest that the L/T transition occurs at lower T(eff) for lower gravity objects, such as those found in young Galactic clusters. The simulated populations of brown dwarfs also reveal that the phase of deuterium burning produces a distinctive feature in CMDs that should be detectable in similar to 50-100 Myr old clusters.
C1 [Saumon, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Saumon, D (reprint author), Los Alamos Natl Lab, POB 1663,Mail Stop F663, Los Alamos, NM 87545 USA.
EM dsaumon@lanl.gov; mark.s.marley@nasa.gov
RI Marley, Mark/I-4704-2013
NR 105
TC 218
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2008
VL 689
IS 2
BP 1327
EP 1344
DI 10.1086/592734
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 376NF
UT WOS:000261189600051
ER
PT J
AU Rowe, JF
Matthews, JM
Seager, S
Miller-Ricci, E
Sasselov, D
Kuschnig, R
Guenther, DB
Moffat, AFJ
Rucinski, SM
Walker, GAH
Weiss, WW
AF Rowe, Jason F.
Matthews, Jaymie M.
Seager, Sara
Miller-Ricci, Eliza
Sasselov, Dimitar
Kuschnig, Rainer
Guenther, David B.
Moffat, Anthony F. J.
Rucinski, Slavek M.
Walker, Gordon A. H.
Weiss, Werner W.
TI THE VERY LOW ALBEDO OF AN EXTRASOLAR PLANET: MOST(1) SPACE-BASED
PHOTOMETRY OF HD 209458
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HD 209458); techniques:
photometric
ID GIANT PLANETS; THERMAL EMISSION; HOT JUPITERS; ATMOSPHERES; MODELS;
SATELLITE; INVERSION; HD-209458; SPECTRUM; SEARCH
AB Measuring the albedo of an extrasolar planet provides insight into its atmospheric composition and its global thermal properties, including heat dissipation and weather patterns. Such a measurement requires very precise photometry of a transiting system, fully sampling many phases of the secondary eclipse. Space-based optical photometry of the transiting system HD 209458 from the MOST (Microvariablity and Oscillations of Stars) satellite, spanning 14 and 44 days in 2004 and 2005, respectively, allows us to set a sensitive limit on the optical eclipse of the hot exosolar giant planet in this system. Our best fit to the observations yields a flux ratio of the planet and star of 7 +/- 9 ppm ( parts per million), which corresponds to a geometric albedo through the MOST bandpass (400-700 nm) of A(g) = 0.038 +/- 0.045. This gives a 1 sigma upper limit of 0.08 for the geometric albedo and a 3 sigma upper limit of 0.17. HD 209458b is significantly less reflective than Jupiter ( for which A(g)would be about 0.5). This low geometric albedo rules out the presence of bright reflective clouds in this exoplanet's atmosphere. We determine refined parameters for the star and exoplanet in the HD 209458 system based on a model fit to the MOST light curve.
C1 [Rowe, Jason F.] NASA, Moffett Field, CA 94035 USA.
[Seager, Sara] MIT, Cambridge, MA 02159 USA.
[Miller-Ricci, Eliza; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kuschnig, Rainer; Walker, Gordon A. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Guenther, David B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Rucinski, Slavek M.] Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada.
[Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
RP Rowe, JF (reprint author), NASA, Ames Res Pk,Mail Stop 244-30, Moffett Field, CA 94035 USA.
EM jasonfrowe@gmail.com
FU Natural Sciences and Engineering Research Council (NSERC) Canada;
Canadian Space Agency; Austrian Science Promotion Agency (FFG-MOST);
Austrian Science Fonds [FWF-P17580]
FX The contributions of J.M.M., D. B. G., A. F. J. M., S. M. R., and G. A.
H. W. are supported by funding from the Natural Sciences and Engineering
Research Council (NSERC) Canada. R. K. is funded by the Canadian Space
Agency. W. W. W. received financial support from the Austrian Science
Promotion Agency (FFG-MOST) and the Austrian Science Fonds (FWF-P17580).
NR 33
TC 114
Z9 115
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2008
VL 689
IS 2
BP 1345
EP 1353
DI 10.1086/591835
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 376NF
UT WOS:000261189600052
ER
PT J
AU Hartlep, T
Zhao, JW
Mansour, NN
Kosovichev, AG
AF Hartlep, Thomas
Zhao, Junwei
Mansour, Nagi N.
Kosovichev, Alexander G.
TI VALIDATING TIME-DISTANCE FAR-SIDE IMAGING OF SOLAR ACTIVE REGIONS
THROUGH NUMERICAL SIMULATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: numerical; Sun: helioseismology; Sun: oscillations; sunspots
ID SUN; HELIOSEISMOLOGY; INVERSION; OSCILLATIONS; SUNSPOTS
AB Far-side imaging using time-distance helioseismology methods is assessed using numerically generated artificial data. The data are generated using direct numerical simulations of acoustic oscillations in a spherical solar model. Localized variations of the sound speed in the surface and subsurface layers are used to model the perturbations associated with sunspots and active regions. The accuracy of acoustic travel-time far-side maps is shown to depend on the size and location of active regions. Potential artifacts in the far-side imaging procedure, such as those caused by the presence of active regions on the solar near side, are also investigated.
C1 [Hartlep, Thomas; Mansour, Nagi N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Zhao, Junwei; Kosovichev, Alexander G.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
RP Hartlep, T (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RI Zhao, Junwei/A-1177-2007;
OI Hartlep, Thomas/0000-0002-5062-9507
FU NASA's; NASA Postdoctoral Program; Oak Ridge Associated Universities;
NASA's "Columbia''; NASA Science Mission Directorate (SMD) High-End
Computing (HEC)
FX This work was supported by NASA's "Living With a Star'' program. Support
from the NASA Postdoctoral Program administered by Oak Ridge Associated
Universities is gratefully acknowledged. Simulations were performed on
NASA's "Columbia'' supercomputer system. Support by NASA Science Mission
Directorate (SMD) High-End Computing (HEC) is gratefully acknowledged.
NR 29
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U1 1
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 DEC 20
PY 2008
VL 689
IS 2
BP 1373
EP 1378
DI 10.1086/592721
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 376NF
UT WOS:000261189600054
ER
PT J
AU Falconer, DA
Moore, RL
Gary, GA
AF Falconer, D. A.
Moore, R. L.
Gary, G. A.
TI MAGNETOGRAM MEASURES OF TOTAL NONPOTENTIALITY FOR PREDICTION OF SOLAR
CORONAL MASS EJECTIONS FROM ACTIVE REGIONS OF ANY DEGREE OF MAGNETIC
COMPLEXITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: coronal mass ejections (CMEs); Sun: magnetic fields
ID FLARES
AB For investigating the magnetic causes of coronal mass ejections (CMEs) and for forecasting the CME productivity of active regions, in previous work we have gauged the total nonpotentiality of a whole active region by either of two measures, L(SSM) and L(SGM), two measures of the magnetic field along the main neutral line in a vector magnetogram of the active region. This previous work was therefore restricted to nominally bipolar active regions, active regions that have a clearly identifiable main neutral line. In the present paper, we show that our work can be extended to include multipolar active regions of any degree of magnetic complexity by replacing L(SSM) and L(SGM) with their generalized counterparts, WL(SS) and WL(SG), which are corresponding integral measures covering all neutral lines in an active region instead of only the main neutral line. In addition, we show that for active regions within 30 heliocentric degrees of disk center, WL(SG) can be adequately measured from line-of-sight magnetograms instead of vector magnetograms. This approximate measure of active-region total nonpotentiality, (L)WL(SG), with the extensive set of 96 minute cadence full-disk line-of-sight magnetograms from SOHO MDI, can be used to study the evolution of active-region total nonpotentiality leading to the production of CMEs.
C1 [Falconer, D. A.; Moore, R. L.; Gary, G. A.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
RP Falconer, DA (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
EM david.a.falconer@nasa.gov; ron.moore@nasa.gov; allen.gary@nasa.gov
FU NSF's Division of Atmospheric Sciences through its SHINE and Space
Weather; NASA's Science Mission Directorate through the Living With a
Star Targeted Research and Technology
FX This work was supported by funding from NSF's Division of Atmospheric
Sciences through its SHINE and Space Weather programs, and by NASA's
Science Mission Directorate through the Living With a Star Targeted
Research and Technology program of its Heliophysics Division. We
acknowledge the use of the SOHO LASCO CME Catalog generated and
maintained by the Center of Solar Physics and Space Weather of the
Catholic University of America in cooperation with the Naval Research
Laboratory and NASA. SOHO is a project of international cooperation
between ESA and NASA.
NR 26
TC 26
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2008
VL 689
IS 2
BP 1433
EP 1442
DI 10.1086/591045
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 376NF
UT WOS:000261189600060
ER
PT J
AU Rodgers, SD
Charnley, SB
AF Rodgers, S. D.
Charnley, S. B.
TI NITROGEN ISOTOPIC FRACTIONATION OF INTERSTELLAR NITRILES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; comets: general; ISM: molecules; meteors, meteoroids;
molecular processes
ID GAS-PHASE REACTIONS; BOPP C/1995 O1; MOLECULAR CLOUDS; PRESTELLAR CORES;
GRAIN PROCESSES; UMIST DATABASE; ORGANIC-MATTER; STAR-FORMATION;
SOLID-PHASE; SOLAR-WIND
AB In light of recent measurement of nitrogen isotope ratios in CN and HCN in several comets, and the correlation between (15)N excess and the presence of nitrile (-CN) functional groups in meteoritic samples, we have reassessed the potential of interstellar chemistry to directly fractionate nitriles. We focus in particular on the (15)N chemistry in selective depletion cores where O-bearing molecules are depleted yet N- and C-bearing species remain in the gas, as revealed by the recent detection of CN in dense CO-depleted cores. We show that large HC(15)N/HC(14)N ratios can be generated if the reaction of CN with N has a barrier, and suggest that cometary HCN and CN may trace material originally formed in dense interstellar clouds.
C1 [Rodgers, S. D.; Charnley, S. B.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
RP Rodgers, SD (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA.
EM rodgers@dusty.arc.nasa.gov
RI Charnley, Steven/C-9538-2012
FU NASA's Origins of Solar Systems Program through NASA Ames Cooperative
[NNX07AO86A]; SETI Institute
FX This work was supported by NASA's Origins of Solar Systems Program
through NASA Ames Cooperative agreement NNX07AO86A with the SETI
Institute.
NR 70
TC 32
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2008
VL 689
IS 2
BP 1448
EP 1455
DI 10.1086/592195
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 376NF
UT WOS:000261189600062
ER
PT J
AU Hailey-Dunsheath, S
Nikola, T
Stacey, GJ
Oberst, TE
Parshley, SC
Bradford, CM
Ade, PAR
Tucker, CE
AF Hailey-Dunsheath, S.
Nikola, T.
Stacey, G. J.
Oberst, T. E.
Parshley, S. C.
Bradford, C. M.
Ade, P. A. R.
Tucker, C. E.
TI DETECTION OF THE (CO)-C-13 J=6 -> 5 TRANSITION IN THE STARBURST GALAXY
NGC 253
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: individual (NGC 253); galaxies: ISM; galaxies: nuclei;
galaxies: starburst; ISM: molecules; submillimeter
ID WARM MOLECULAR GAS; INTER-STELLAR CLOUDS; DENSE GAS; CIRCUMNUCLEAR DISK;
INFRARED-EMISSION; NUCLEAR STARBURST; THERMAL BALANCE; NEARBY GALAXIES;
CARBON-MONOXIDE; VELOCITY-FIELD
AB We report the detection of (CO)-C-13 J = 6 -> 5 emission from the nucleus of the starburst galaxy NGC 253 with the redshift (z) and Early Universe Spectrometer (ZEUS), a new submillimeter grating spectrometer. This is the first extragalactic detection of the (CO)-C-13 J = 6 -> 5 transition, which traces warm, dense molecular gas. We employ a multiline LVG analysis and find approximate to 35%-60% of the molecular interstellar medium is both warm (T similar to 110 K) and dense (n(H2) similar to 10(4) cm(-3)). We analyze the potential heat sources and conclude that ultraviolet and X-ray photons are unlikely to be energetically important. Instead, the molecular gas is most likely heated by an elevated density of cosmic rays or by the decay of supersonic turbulence through shocks. If the cosmic rays and turbulence are created by stellar feedback within the starburst, then our analysis suggests the starburst may be self-limiting.
C1 [Hailey-Dunsheath, S.; Nikola, T.; Stacey, G. J.; Oberst, T. E.; Parshley, S. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ade, P. A. R.; Tucker, C. E.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
RP Hailey-Dunsheath, S (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM steve@astro.cornell.edu
FU NSF [AST 00-96881, AST 03-52855, AST 07-05256, AST 07-22220]; NASA [NGT
05-50470, NNG 05-GK70H]
FX This work was supported by NSF grants AST 00-96881, AST 03-52855, AST
07-05256, and AST 07-22220, and by NASA grants NGT 05-50470 and NNG
05-GK70H. We are indebted to the GSFC group (C. A. Allen, S. H. Moseley,
D. J. Benford, and J. G. Staguhn) for their sensitive bolometers. We
also thank the CSO staff for their support of ZEUS operations and an
anonymous referee for many helpful comments on an earlier draft of this
manuscript.
NR 38
TC 31
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 20
PY 2008
VL 689
IS 2
BP L109
EP L112
DI 10.1086/595840
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 398LQ
UT WOS:000262734000008
ER
PT J
AU Krennrich, F
Dwek, E
Imran, A
AF Krennrich, F.
Dwek, E.
Imran, A.
TI CONSTRAINTS ON ENERGY SPECTRA OF BLAZARS BASED ON RECENT EBL LIMITS FROM
GALAXY COUNTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE BL Lacertae objects: individual (1ES 1218+30.4, 1ES 1101-232; 1ES
0229+200)
ID EXTRAGALACTIC BACKGROUND LIGHT; SPITZER-SPACE-TELESCOPE; VHE GAMMA-RAYS;
TEV BLAZARS; MU-M; DISCOVERY; RADIATION; ACCELERATION; EVOLUTION;
EMISSION
AB We combine the recent estimate of the contribution of galaxies to the 3.6 mu m intensity of the extragalactic background light (EBL) with optical and near-infrared (IR) galaxy counts to set new limits on intrinsic spectra of some of the most distant TeV blazars, 1ES 0229+200, 1ES 1218+30.4, and 1ES 1101-232, located at redshifts 0.1396, 0.182, and 0.186, respectively. The new lower limit on the 3.6 mm EBL intensity is significantly higher than the previous one set by the cumulative emission from resolved Spitzer galaxies. Correcting for attenuation by the revised EBL, we show that the differential spectral index of the intrinsic spectrum of the three blazars is or harder. These results present blazar emission models with the challenge of producing 1.28 +/- 0.20 extremely hard intrinsic spectra in the sub-TeV to multi-TeV regime. These results also question the reliability of recently derived upper limits on the near-IR EBL intensity that are solely based on the assumption that intrinsic blazar spectra should not be harder than 1.50.
C1 [Krennrich, F.; Imran, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Dwek, E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
RP Krennrich, F (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
EM krennrich@iastate.edu; eli.dwek@nasa.gov
RI Dwek, Eli/C-3995-2012
FU US Department of Energy; NASA [LTSA 03-0000-065]
FX This research is supported by grants from the US Department of Energy.
The authors thank W. Benbow and W. Hofmann for providing the spectral
data for 1ES 1101-232 and 1ES 0229+200. We also thank P. Fortin and the
VERITAS collaboration for providing the 1ES 1218+30.4 data. E. D.
acknowledges the support of NASA LTSA 03-0000-065.
NR 33
TC 19
Z9 19
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 20
PY 2008
VL 689
IS 2
BP L93
EP L96
DI 10.1086/595960
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 398LQ
UT WOS:000262734000004
ER
PT J
AU Campbell, B
Carter, L
Phillips, R
Plaut, J
Putzig, N
Safaeinili, A
Seu, R
Biccari, D
Egan, A
Orosei, R
AF Campbell, Bruce
Carter, Lynn
Phillips, Roger
Plaut, Jeffrey
Putzig, Nathaniel
Safaeinili, Ali
Seu, Roberto
Biccari, Daniela
Egan, Anthony
Orosei, Roberto
TI SHARAD radar sounding of the Vastitas Borealis Formation in Amazonis
Planitia
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID ORBITER LASER ALTIMETER; NORTHERN LOWLANDS; FLOOD LAVAS; MOLA DATA;
MARS; VOLCANISM; DEPOSITS; PLAINS; FATE
AB Amazonis Planitia has undergone alternating episodes of sedimentary and volcanic infilling, forming an interleaved sequence with an upper surface that is very smooth at the kilometer scale. Earlier work interprets the near-surface materials as either young, rough lava flows or ice-rich sediment layers, overlying a basement comprising the Vastitas Borealis Formation and earlier Hesperian plains. Sounding radar profiles across Amazonis Planitia from the Shallow Radar (SHARAD) instrument on the Mars Reconnaissance Orbiter reveal a subsurface dielectric interface that increases in depth toward the north along most orbital tracks. The maximum depth of detection is 100-170 m, depending upon the real dielectric permittivity of the materials, but the interface may persist at greater depth to the north if the reflected energy is attenuated below the SHARAD noise floor. The dielectric horizon likely marks the boundary between sedimentary material of the Vastitas Borealis Formation and underlying Hesperian volcanic plains. The SHARAD-detected interface follows the surface topography across at least one of the large wrinkle ridges in north central Amazonis Planitia. This conformality suggests that Vastitas Borealis sediments, at least in this region, were emplaced prior to compressional tectonic deformation. The change in radar echo strength with time delay is consistent with a loss tangent of 0.005-0.012 for the column of material between the surface and the reflector. These values are consistent with dry, moderate-density sediments or the lower end of the range of values measured for basalts. While a component of distributed ice in a higher-loss matrix cannot be ruled out, we do not find evidence for a dielectric horizon within the Vastitas Borealis Formation that might suggest an abrupt change from an upper dry layer to an ice-rich lower deposit.
C1 [Campbell, Bruce; Carter, Lynn] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
[Seu, Roberto; Biccari, Daniela] Univ Roma La Sapienza, INFOCOM, I-00184 Rome, Italy.
[Phillips, Roger; Putzig, Nathaniel; Egan, Anthony] SW Res Inst, Boulder, CO 80302 USA.
[Orosei, Roberto] Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
[Plaut, Jeffrey; Safaeinili, Ali] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Campbell, B (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA.
EM campbellb@si.edu
RI Carter, Lynn/D-2937-2012
NR 26
TC 18
Z9 18
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 20
PY 2008
VL 113
IS E12
AR E12010
DI 10.1029/2008JE003177
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 386MI
UT WOS:000261886900002
ER
PT J
AU Yingst, RA
Crumpler, L
Farrand, WH
Li, R
Cabrol, NA
Neakrase, LD
AF Yingst, R. A.
Crumpler, L.
Farrand, W. H.
Li, R.
Cabrol, N. A.
Neakrase, L. D.
TI Morphology and texture of particles along the Spirit rover traverse from
sol 450 to sol 745
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID PATHFINDER LANDING SITE; GUSEV CRATER; ROCK PARTICLES; MARS; SHAPE;
ROUNDNESS; SIZE; DISTRIBUTIONS; INDICATORS; PLANETARY
AB We quantified and classified the shape, roundness, size, and texture of 935 loose surface particles along the Spirit rover traverse from sols 450-745 to assess origin, transport, and other alteration mechanisms that altered particles during and after formation. Variation in particle morphologic parameters along traverse is consistent with crossing mapped geologic unit boundaries. Texture is divided into four types: vesicular, smooth and flat-faceted, rough and flat-faceted, and very rough. Sphericity and roundness are intermediate and low, respectively, comparable to particles moved by high-energy transport or to crushed particles. This indicates intermittent, high-energy emplacement or modification of a single lithology, rather than systematic, continuous low-energy abrasion or wear over time. Comparison with particle morphology at other Mars landing sites is consistent with the hypothesis that no secondary systematic transport or wide-scale chemical alteration was active at a significant enough level to alter macromorphology. In particular, particle morphology at the Mars Pathfinder site shows stronger evidence of abrasion than along the Spirit traverse, suggesting Mars Pathfinder particles have undergone abrasion processes that particles in this study area have not. Additionally, morphology indices have correlation coefficients near zero, indicating that a fluvial transport mechanism is likely not responsible for morphology. Morphology and texture are instead related to origin and composition rather than subsequent modification. Morphology and texture support a volcanic origin, possibly without modification, but most likely altered primarily by ballistic impact, implying that the Spirit landing site and traverse may be utilized in the future as a standard site for characterization of impact-derived morphology.
C1 [Yingst, R. A.] Univ Wisconsin Green Bay, Dept Nat & Appl Sci, Green Bay, WI 54311 USA.
[Cabrol, N. A.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Crumpler, L.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA.
[Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA.
[Li, R.] Ohio State Univ, Dept Civil Engn, Columbus, OH 43210 USA.
[Neakrase, L. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Yingst, RA (reprint author), Univ Wisconsin Green Bay, Dept Nat & Appl Sci, 2420 Nicolet Dr, Green Bay, WI 54311 USA.
EM yingsta@uwgb.edu
FU Mars Exploration Rover Program through JPL [1278721]
FX We gratefully acknowledge the constructive reviews of J. Zimbelman and
B. Ehlmann, whose comments greatly improved this manuscript.
Undergraduates Cassandra Marnocha and Zachary Christman collected
portions of the data. This research was supported by the Mars
Exploration Rover Program through JPL contract 1278721 to R.A.Y.
NR 73
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U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 20
PY 2008
VL 113
IS E12
AR E12S41
DI 10.1029/2008JE003179
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 386MI
UT WOS:000261886900003
ER
PT J
AU Miyashita, Y
Hosokawa, K
Hori, T
Kamide, Y
Yukimatu, AS
Fujimoto, M
Mukai, T
Machida, S
Sato, N
Saito, Y
Shinohara, I
Sigwarth, JB
AF Miyashita, Y.
Hosokawa, K.
Hori, T.
Kamide, Y.
Yukimatu, A. S.
Fujimoto, M.
Mukai, T.
Machida, S.
Sato, N.
Saito, Y.
Shinohara, I.
Sigwarth, J. B.
TI Response of large-scale ionospheric convection to substorm expansion
onsets: A case study
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID HIGH-LATITUDE CONVECTION; EARTHWARD FLOW BURSTS; SHEET BOUNDARY-LAYER;
AURORAL RADAR NETWORK; THIN CURRENT SHEETS; PLASMA SHEET; MAGNETOSPHERIC
SUBSTORMS; MIDDISTANT MAGNETOTAIL; GEOTAIL OBSERVATIONS; CURRENT
SIGNATURES
AB We have studied the response of large-scale ionospheric convection to substorm expansion onsets on the basis of two weak substorms of 1 May 2001, during which a large part of the dawn cell of the two-cell ionospheric convection pattern was monitored by the SuperDARN radars. Ionospheric convection began to enhance first in a localized region of the equatorward part of the dawn cell similar to 2 minutes before the expansion onsets of both substorms and then enhanced in the entire dawn cell successively. The enhanced convection persisted throughout their expansion phase, possibly even near the footprint of a plasma sheet region without fast flows observed by Geotail. These observations suggest that ionospheric convection begins to enhance just before substorm expansion onset and then enhances in the entire cell, possibly regardless of the presence of fast earthward flows in the corresponding plasma sheet region of the magnetotail. The global enhancement of ionospheric convection is consistent with that of magnetotail convection, which also begins just before onset.
C1 [Miyashita, Y.; Fujimoto, M.; Mukai, T.; Saito, Y.; Shinohara, I.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Hosokawa, K.] Univ Electrocommun, Dept Informat & Commun Engn, Tokyo 1828585, Japan.
[Hori, T.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Kamide, Y.] Kyoto Univ, Res Inst Sustainable Humanosphere, Kyoto 6110011, Japan.
[Yukimatu, A. S.; Sato, N.] Natl Inst Polar Res, Itabashi Ku, Tokyo 1738515, Japan.
[Machida, S.] Kyoto Univ, Dept Geophys, Sakyo Ku, Kyoto 6068502, Japan.
[Sigwarth, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Miyashita, Y (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
EM miyasita@stp.isas.jaxa.jp
OI Hori, Tomoaki/0000-0001-8451-6941
FU University of Iowa; National Aeronautics and Space Administration
[NAG5-11528]
FX We thank S. Kokubun and T. Nagai for providing the Geotail MGF magnetic
field data. We also thank R. W. McEntire, S. P. Christon, and A. T. Y.
Lui for the Geotail EPIC-STICS high-energy particle data and M. Nose, D.
Nagata, and Y. Ono for preparing them. The ACE SWEPAM plasma data, the
ACE MAG magnetic field data, and the GOES magnetic field data were
provided by D. J. McComas, N. Ness, and H. J. Singer, respectively,
through the Coordinated Data Analysis Web (CDAWeb) at NASA. The CANOPUS
MSP auroral data were provided by F. Creutzberg and E. Donovan, and the
CANOPUS and CANMOS geomagnetic field data were provided by I. Mann and
D. Boteler, respectively, through the Canadian Space Science Data Portal
(CSSDP). The Sym-H and Dst indices were provided by World Data Center
for Geomagnetism, Kyoto. The Polar UVI auroral imager data were provided
by K. Liou and G. K. Parks. The IMAGE FUV auroral imager data were
provided by S. B. Mende. We thank all the staff who contributed to the
operation of the SuperDARN radars. We also thank F. Creutzberg for his
useful comments. This research was supported in part at the University
of Iowa by the National Aeronautics and Space Administration under
NAG5-11528.
NR 63
TC 12
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U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD DEC 20
PY 2008
VL 113
IS A12
AR A12309
DI 10.1029/2008JA013586
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 386MT
UT WOS:000261888000001
ER
PT J
AU Singh, M
Asthana, R
Shpargel, TP
AF Singh, M.
Asthana, R.
Shpargel, T. P.
TI Brazing of ceramic-matrix composites to Ti and Hastealloy using Ni-base
metallic glass interlayers
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article; Proceedings Paper
CT 2nd International Conference on Recent Advances in Composite Materials
CY FEB 20-23, 2007
CL New Delhi, INDIA
SP India Habitat Ctr
DE Metallic glass; Brazing; C-C composite; C-SiC composite; SiC-SiC
composite; Scanning electron microscopy; Energy dispersive spectroscopy;
Knoop microhardness
ID CARBON-CARBON COMPOSITES; TITANIUM
AB Carbon-carbon, carbon-silicon carbide, and silicon carbide-silicon carbide composites were vacuum brazed to Ti and Hastealloy X using Ni-base metallic glass braze foils (MBF-20 and MBF-30). Scanning electron microscopy (SEM) and energy-dispersive X-ray spectroscopy (EDS) of the joints showed that compositional changes due to substrate dissolution led to secondary-phase precipitation which aided interfacial bonding although inter-laminar shear failure occurred within some composites. Residual thermal stresses in the joint led to hardness gradients; however, stress accommodation by the brazes prevented interfacial cracking. The peak Knoop microhardness in the joints was as high as 1165-1294 KHN. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Singh, M.] NASA, Glenn Res Ctr, Ohio Aerosp Inst, ASRC Aerosp, Cleveland, OH 44135 USA.
[Asthana, R.] Univ Wisconsin Stout, Dept Engn & Technol, Menomonie, WI 54751 USA.
RP Singh, M (reprint author), NASA, Glenn Res Ctr, Ohio Aerosp Inst, ASRC Aerosp, Cleveland, OH 44135 USA.
EM Mrityunjay.Singh-1@grc.nasa.gov
NR 22
TC 56
Z9 66
U1 3
U2 17
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 DEC 20
PY 2008
VL 498
IS 1-2
SI SI
BP 19
EP 30
DI 10.1016/j.msea.2007.11.150
PG 12
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 379UA
UT WOS:000261420500005
ER
PT J
AU Singh, M
Morscher, GN
Shpargel, TP
Asthana, R
AF Singh, M.
Morscher, Gregory N.
Shpargel, Tarah P.
Asthana, Rajiv
TI Active metal brazing of titanium to high-conductivity carbon-based
sandwich structures
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article; Proceedings Paper
CT 2nd International Conference on Recent Advances in Composite Materials
CY FEB 20-23, 2007
CL New Delhi, INDIA
SP India Habitat Ctr
DE Brazing; Carbon foam; C-C composite; Shear stress; Knoop microhardness;
Scanning electron microscopy; Energy-dispersive spectroscopy
AB Reactive brazing technology was developed and processing parameters were optimized for the bonding of titanium tubes, graphite foam, and high-conductivity carbon-carbon composite face sheets using the active braze Cusil-ABA paste and foils. The microstructure and composition of the joints, examined using scanning electron microscopy coupled with energy-dispersive spectroscopy, showed good bonding and braze penetration in all systems when braze paste was used. The hardness values of the brazed joints were consistent for the different specimen stacking configurations. Mechanical testing of Ti tube/foam/C-C composite structures both in tension and shear showed that failure always occurred in the foam material demonstrating that the brazed joint was sufficient for these types of sandwich structures. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Singh, M.; Morscher, Gregory N.] NASA, Glenn Res Ctr, Ohio Aerosp Inst, ASRC Aerosp, Cleveland, OH 44135 USA.
[Asthana, Rajiv] Univ Wisconsin Stout, Dept Engn & Technol, Menomonie, WI 54751 USA.
RP Singh, M (reprint author), NASA, Glenn Res Ctr, Ohio Aerosp Inst, ASRC Aerosp, MS 106-5, Cleveland, OH 44135 USA.
EM Mrityunjay.Singh@grc.nasa.gov
NR 5
TC 22
Z9 23
U1 2
U2 9
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD DEC 20
PY 2008
VL 498
IS 1-2
SI SI
BP 31
EP 36
DI 10.1016/j.msea.2007.11.151
PG 6
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 379UA
UT WOS:000261420500006
ER
PT J
AU Kalashnikova, OV
Kahn, RA
AF Kalashnikova, Olga V.
Kahn, Ralph A.
TI Mineral dust plume evolution over the Atlantic from MISR and MODIS
aerosol retrievalsy
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID REMOTE-SENSING OBSERVATIONS; OPTICAL DEPTH; SAHARAN DUST; INTERANNUAL
VARIABILITY; FORECAST MODEL; ART.; SENSITIVITY; AERONET; SIMULATIONS;
ASSESSMENTS
AB We demonstrate how Multiangle Imaging Spectroradiometer ( MISR) and Moderate Resolution Imaging Spectroradiometer ( MODIS) space-based aerosol products provide complementary information, characterizing ( 1) transported desert dust plume extent over water, ( 2) aerosol optical thickness ( AOT) evolution, and ( 3) particle size sensitivity and fraction spherical evolution for the thicker parts of these plumes. MODIS provides more extensive coverage, whereas MISR's multiangle retrievals include dust properties and fill in areas where glint precludes MODIS optical depth retrievals, increasing by up to 50% dust plume surface area coverage compared to MODIS-only observations. These results can be used to improve dust aerosol representations in climate, forecast, and transport models. Extensive comparison of MISR and MODIS AOT retrievals with Aerosol Robotic Network ( AERONET) observations in dusty regions show accuracies of about 20%; MISR Angstrom exponent is predominantly less than 1, in reasonably good agreement with AERONET. For four selected North African dust transport events, combined MISR and MODIS observations map systematic changes in retrieved plume surface area, on the basis of AOT contours; these reflect differences in aerosol dispersion and removal rates that must be reproduced by models. Within MISR retrieval uncertainties, Angstrom exponent and AOT fraction spherical are lower in the optically thicker parts of the plume by up to 30% and increase as the plume is transported across the ocean, as would be expected; retrieved single-scattering albedo values are similar to 0.98 for all stages of plume evolution. For the cases studied, AERONET shows similar property patterns at points on either side of the Atlantic and indicates similar to 15% decrease in aerosol coarse mode effective radius during transoceanic transport.
C1 [Kalashnikova, Olga V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kahn, Ralph A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kalashnikova, OV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM olga.v.kalashnikova@jpl.nasa.gov
RI Kahn, Ralph/D-5371-2012
OI Kahn, Ralph/0000-0002-5234-6359
FU NASA Earth Sciences Division
FX We thank Michael Garay for creating tools for collocating MISR and MODIS
aerosol retrievals; Amy Braverman, PI of AMAPS project, for her help in
developing tools for obtaining and comparing MISR, MODIS, and AERONET
data; and the AERONET project and the Saharan AERONET stations principal
investigators for their efforts in establishing and maintaining the nine
sites used in this investigation. We thank Jeffrey Reid and Douglas
Westphal for sharing NAAPS data and the MISR team for providing
facilities, access to data, and useful discussions. The work of O.
Kalashnikova is supported by a grant from the NASA Earth Sciences
Division, Climate and Radiation program, under H. Maring. The work of R.
Kahn is supported in part by the NASA Climate and Radiation Research and
Analysis program under H. Maring, the Atmospheric Composition program
under Phil DeCola, and the EOS- MISR instrument project. This work was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA and at the NASA Goddard Space
Flight Center. The MISR data were obtained from the NASA Langley
Research Center Atmospheric Sciences Data Center.
NR 49
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U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD DEC 19
PY 2008
VL 113
AR D24204
DI 10.1029/2008JD010083
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 386LC
UT WOS:000261883700004
ER
PT J
AU Lee, T
Wang, O
Tang, WQ
Liu, WT
AF Lee, Tong
Wang, Ou
Tang, Wenqing
Liu, W. Timothy
TI Wind stress measurements from the QuikSCAT-SeaWinds scatterometer tandem
mission and the impact on an ocean model
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID INDIAN-OCEAN; SURFACE WIND; SEMIDIURNAL VARIATIONS; PACIFIC-OCEAN;
HEAT-FLUX; CIRCULATION; PARAMETERIZATION; VARIABILITY; BOUNDARY; FIELDS
AB We examine diurnal signals captured by the QuikSCAT-SeaWinds scatterometer tandem mission (April-October 2003) and their impact on ocean model simulation. The diurnal variability captured by twice-daily scatterometer wind from the tandem mission is substantially larger than that estimated by the National Centers for Environmental Prediction (NCEP) reanalysis product (even with a 6-hourly interval in the latter). Consequently, the impact of diurnal wind on model sea surface temperature (SST) is significantly larger with scatterometer than with NCEP winds because of stronger vertical mixing caused by the twice-daily scatterometer wind. This is consistent with previous studies that high-frequency wind at the ocean's inertial frequencies enhances vertical mixing through resonant inertial oscillations. The weak vertical mixing associated with daily scatterometer winds causes warm bias of SST (relative to that resulting from twice-daily scatterometer wind) and larger deviation from observations. The warm bias reaches several degrees Celsius in midlatitude oceans during summertime and can accumulate with time. Heat flux correction that attempts to account for the feedback of SST would propagate the error in wind and vertical mixing to heat flux without correcting the error source. Because of this error compensation, caution is needed in the interpretation of SST budget resulting from ocean models and data assimilation outputs based on wind products that do not adequately resolve diurnal variability. Our findings highlight the need to resolve diurnal wind in future scatterometer missions. Our study assumes that wind differences between the two scatterometers are primarily due to the sampling of diurnal cycle at different times. However, potential bias between the two needs further investigations.
C1 [Lee, Tong; Wang, Ou; Tang, Wenqing; Liu, W. Timothy] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
RP Lee, T (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM tong.lee@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); Physical
Oceanography Distributed Active Archive Center (PO. DAAC); NASA Jet
Propulsion Laboratory, Pasadena, CA
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration (NASA).
The scatterometer data used for the analysis were obtained from the
Physical Oceanography Distributed Active Archive Center (PO. DAAC) at
the NASA Jet Propulsion Laboratory, Pasadena, CA (data are available at
http://podaac.jpl.nasa.gov). The model sensitivity experiments were
performed on the supercomputers of the JPL Super-computing Project and
NASA Ames Research Center.
NR 30
TC 8
Z9 8
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD DEC 19
PY 2008
VL 113
IS C12
AR C12019
DI 10.1029/2008JC004855
PG 14
WC Oceanography
SC Oceanography
GA 386LX
UT WOS:000261885800002
ER
PT J
AU Ming, DW
Gellert, R
Morris, RV
Arvidson, RE
Brukner, J
Clark, BC
Cohen, BA
d'Uston, C
Economou, T
Fleischer, I
Klingelhofer, G
McCoy, TJ
Mittlefehldt, DW
Schmidt, ME
Schroder, C
Squyres, SW
Treguier, E
Yen, AS
Zipfel, J
AF Ming, D. W.
Gellert, R.
Morris, R. V.
Arvidson, R. E.
Bruekner, J.
Clark, B. C.
Cohen, B. A.
d'Uston, C.
Economou, T.
Fleischer, I.
Klingelhoefer, G.
McCoy, T. J.
Mittlefehldt, D. W.
Schmidt, M. E.
Schroeder, C.
Squyres, S. W.
Treguier, E.
Yen, A. S.
Zipfel, J.
TI Geochemical properties of rocks and soils in Gusev Crater, Mars: Results
of the Alpha Particle X-Ray Spectrometer from Cumberland Ridge to Home
Plate
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MAGNETIC-PROPERTIES EXPERIMENTS; FLUID INCLUSIONS; SPIRIT ROVER;
MINERALOGY; CHEMISTRY; MISSION; DUST
AB Geochemical diversity of rocks and soils has been discovered by the Alpha Particle X-Ray Spectrometer ( APXS) during Spirit's journey over Husband Hill and down into the Inner Basin from sol 470 to 1368. The APXS continues to operate nominally with no changes in calibration or spectral degradation over the course of the mission. Germanium has been added to the Spirit APXS data set with the confirmation that it occurs at elevated levels in many rocks and soils around Home Plate. Twelve new rock classes and two new soil classes have been identified at the Spirit landing site since sol 470 on the basis of the diversity in APXS geochemistry. The new rock classes are Irvine ( alkaline basalt), Independence ( low Fe outcrop), Descartes ( outcrop similar to Independence with higher Fe and Mn), Algonquin ( mafic-ultramafic igneous sequence), Barnhill ( volcaniclastic sediments enriched in Zn, Cl, and Ge), Fuzzy Smith ( high Si and Ti rock), Elizabeth Mahon ( high Si, Ni, and Zn outcrop and rock), Halley ( hematite-rich outcrop and rock), Montalva ( high K, hematite-rich rock), Everett ( high Mg, magnetite-rich rock), Good Question ( high Si, low Mn rock), and Torquas ( high K, Zn, and Ni magnetite-rich rock). New soil classes are Gertrude Weise ( very high Si soil) and Eileen Dean ( high Mg, magnetite-rich soil). Aqueous processes have played a major role in the formation and alteration of rocks and soils on Husband Hill and in the Inner Basin.
C1 [Ming, D. W.; Morris, R. V.; Mittlefehldt, D. W.; Schroeder, C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada.
[Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Bruekner, J.] Max Planck Inst Chem, D-55128 Mainz, Germany.
[Clark, B. C.] Space Sci Inst, Boulder, CO 80301 USA.
[Cohen, B. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[d'Uston, C.; Treguier, E.] Univ Toulouse 3, CNRS, Ctr Etud Spatiale Rayonnements, OMP, F-31028 Toulouse, France.
[Economou, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Fleischer, I.; Klingelhoefer, G.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55128 Mainz, Germany.
[McCoy, T. J.; Schmidt, M. E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
[Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Yen, A. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zipfel, J.] Forschungsinst, D-60325 Frankfurt, Germany.
[Zipfel, J.] Nat Museum Senckenberg, D-60325 Frankfurt, Germany.
RP Ming, DW (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM douglas.w.ming@nasa.gov
RI Schroder, Christian/B-3870-2009;
OI Schroder, Christian/0000-0002-7935-6039; Treguier,
Erwan/0000-0002-7347-2805
FU NASA; Canadian Space Agency
FX We thank the members of the MER project who enable daily science
observations at the Spirit landing site. The work described in this
paper was conducted at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA. D. W. M. and R. V.
M. acknowledge support of the NASA Mars Fundamental Research Program and
the NASA Johnson Space Center. R. G. acknowledges support from the
Canadian Space Agency. C. S. acknowledges support by an appointment to
the NASA Postdoctoral Program at the Johnson Space Center, administered
by Oak Ridge Associated Universities through a contract with NASA. We
thank David Vaniman and an anonymous reviewer for detailed reviews.
NR 44
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U2 26
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 19
PY 2008
VL 113
IS E12
AR E12S39
DI 10.1029/2008JE003195
PG 28
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 386MH
UT WOS:000261886800002
ER
PT J
AU Ehlmann, BL
Mustard, JF
Murchie, SL
Poulet, F
Bishop, JL
Brown, AJ
Calvin, WM
Clark, RN
Des Marais, DJ
Milliken, RE
Roach, LH
Roush, TL
Swayze, GA
Wray, JJ
AF Ehlmann, Bethany L.
Mustard, John F.
Murchie, Scott L.
Poulet, Francois
Bishop, Janice L.
Brown, Adrian J.
Calvin, Wendy M.
Clark, Roger N.
Des Marais, David J.
Milliken, Ralph E.
Roach, Leah H.
Roush, Ted L.
Swayze, Gregg A.
Wray, James J.
TI Orbital Identification of Carbonate-Bearing Rocks on Mars
SO SCIENCE
LA English
DT Article
ID MINERALS; CLIMATE; PHYLLOSILICATES; TEMPERATURE; PRODUCTS; SULFATES;
OLIVINE; SPECTRA; SYSTEM; MODEL
AB Geochemical models for Mars predict carbonate formation during aqueous alteration. Carbonate- bearing rocks had not previously been detected on Mars' surface, but Mars Reconnaissance Orbiter mapping reveals a regional rock layer with near- infrared spectral characteristics that are consistent with the presence of magnesium carbonate in the Nili Fossae region. The carbonate is closely associated with both phyllosilicate- bearing and olivine- rich rock units and probably formed during the Noachian or early Hesperian era from the alteration of olivine by either hydrothermal fluids or near- surface water. The presence of carbonate as well as accompanying clays suggests that waters were neutral to alkaline at the time of its formation and that acidic weathering, proposed to be characteristic of Hesperian Mars, did not destroy these carbonates and thus did not dominate all aqueous environments.
C1 [Ehlmann, Bethany L.; Mustard, John F.; Roach, Leah H.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Poulet, Francois] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Bishop, Janice L.; Brown, Adrian J.] SETI Inst, Mountain View, CA 94043 USA.
[Bishop, Janice L.; Brown, Adrian J.; Des Marais, David J.; Roush, Ted L.] NASA, Ames Res Ctr, Mountain View, CA 94043 USA.
[Calvin, Wendy M.] Univ Nevada, Dept Geol Sci & Engn, Reno, NV 89557 USA.
[Clark, Roger N.; Swayze, Gregg A.] US Geol Survey, Lakewood, CO 80225 USA.
[Milliken, Ralph E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wray, James J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Ehlmann, BL (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
RI Wray, James/B-8457-2008; Murchie, Scott/E-8030-2015
OI Wray, James/0000-0001-5559-2179; Murchie, Scott/0000-0002-1616-8751
FU NASA/Keck Reflectance Experiment Laboratory (RELAB) spectral database
FX We thank R. Arvidson, R. Morris, N. Mangold, A. Baldridge, J.-P.
Bibring, D. Jouglet, A. Fraeman, S. Wiseman, A. McEwen, G. Marzo, P.
McGuire, and M. Wyatt for thoughtful discussions during manuscript
preparation and E. Cloutis and others who have made quality spectral
libraries available and contributed to the building of the NASA/Keck
Reflectance Experiment Laboratory (RELAB) spectral database. We are
grateful for the ongoing efforts of the MRO science and engineering
teams, in particular the CRISM team, which enable these discoveries.
NR 45
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U1 10
U2 63
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 DEC 19
PY 2008
VL 322
IS 5909
BP 1828
EP 1832
DI 10.1126/science.1164759
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 385FF
UT WOS:000261799400050
PM 19095939
ER
PT J
AU Hofton, MA
Blair, JB
Luthcke, SB
Rabine, DL
AF Hofton, M. A.
Blair, J. B.
Luthcke, S. B.
Rabine, D. L.
TI Assessing the performance of 20-25 m footprint waveform lidar data
collected in ICESat data corridors in Greenland
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LASER ALTIMETER; VEGETATION; ACCURACY
AB The precision and accuracy of surface elevation measurements of the Greenland ice sheet provided by 20 25 m-footprint waveform laser altimetry is assessed using data collected by NASA's LVIS airborne lidar in September 2007. Repeated data acquisitions from two similar to 850 km long transects over the ice sheet and a similar to 30 km-long transect in the Summit area are evaluated for consistency and compared to in situ data for validation. Comparisons to data collected by NASA's ICESat system reveal good agreement. In the Summit area, differences are better than 0.07 m (1 sigma) (except for L3C where it is 0.13 m), with mean offsets of -0.09 to 0.16 m depending on the campaign. Within the feeder zone to Jakobshavn Glacier, ice elevation decreases of up to 12 m, 2004-2008, are observed. The results suggest that 25 m waveform lidar can measure ice sheet elevation precisely and accurately and that the measurement scheme could be used to complement the legacy ICESat measurements. Citation: Hofton, M. A., J. B. Blair, S. B. Luthcke, and D. L. Rabine (2008), Assessing the performance of 20-25 m footprint waveform lidar data collected in ICESat data corridors in Greenland, Geophys. Res. Lett., 35, L24501, doi: 10.1029/2008GL035774.
C1 [Hofton, M. A.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Blair, J. B.; Luthcke, S. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rabine, D. L.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Hofton, MA (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
EM Mhofton@umd.edu; Bryan.Blair@nasa.gov; Scott.B.Luthcke@nasa.gov;
David.Rabine@nasa.gov
RI Khachadourian, Diana/C-8513-2012; Luthcke, Scott/D-6283-2012; Rabine,
David/C-9626-2013; Blair, James/D-3881-2013
FU GSFC IRAD; NASA [NNX08AI50G]
FX We would like to thank J. Sauber, an anonymous reviewer, R.
Bindschadler, R. Ray, E. Frederick, J. Sonntag, J. Yungel, C. Shuman,
and B. Hawley. Funding for this project was provided by a GSFC IRAD, and
NASA grant NNX08AI50G. The LVIS data are available at
https://lvis.gsfc.nasa.gov.
NR 10
TC 15
Z9 15
U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 18
PY 2008
VL 35
IS 24
AR L24501
DI 10.1029/2008GL035774
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 386KO
UT WOS:000261882300004
ER
PT J
AU Jeong, MJ
Hsu, NC
AF Jeong, Myeong-Jae
Hsu, N. Christina
TI Retrievals of aerosol single-scattering albedo and effective aerosol
layer height for biomass-burning smoke: Synergy derived from "A-Train"
sensors
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SUN
AB In this paper, we present results from a new algorithm which provides aerosol layer height (ALH) as well as single-scattering albedo (SSA) for biomass-burning smoke aerosols by merging measurements from three of the "A-Train" satellite sensors: MODIS, OMI, and CALIOP. This algorithm has been applied successfully to biomass burning episodes over North America and Southeast Asia, and the corresponding SSA retrievals show good agreement with those from the AERONET. Furthermore, by combining ALH information from CALIOP with the retrieved SSA, extended information of ALH over wide areas can be obtained outside the CALIPSO track. Even when CALIPSO data are not available, this algorithm will still allow for the separation of aerosols residing within the boundary layer from those elevated in the free troposphere by combining only MODIS and OMI data. Results from this study will provide a better understanding of the height of smoke layers generated from biomass burning and thus improve aerosol models and the prediction of smoke aerosol transport. Citation: Jeong, M.-J., and N. C. Hsu (2008), Retrievals of aerosol single-scattering albedo and effective aerosol layer height for biomass-burning smoke: Synergy derived from "A-Train" sensors, Geophys. Res. Lett., 35, L24801, doi: 10.1029/2008GL036279.
C1 [Jeong, Myeong-Jae] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Jeong, Myeong-Jae; Hsu, N. Christina] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Jeong, MJ (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
EM myeong-jae.jeong-1@nasa.gov
RI Jeong, Myeong/B-8803-2008; Hsu, N. Christina/H-3420-2013
FU NASA Applied Sciences Program
FX This work is supported by grant from the NASA Applied Sciences Program,
under L. Friedl. We thank grant PI John McHenry of Baron Advanced
Meteorological Systems for useful discussions during this research.
CALIPSO data were obtained from the NASA Langley Research Center
Atmospheric Science Data Center. The OMI L1B data were acquired from the
Goddard Earth Sciences Distributed Active Archive Center,
http://disc.gsfc.nasa.gov. We thank many AERONET principal investigators
and their staff for establishing and maintaining the AERONET sites used
in this study. We are also grateful to the MODAPS team for producing and
distributing the MODIS products.
NR 13
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U1 1
U2 8
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 DEC 18
PY 2008
VL 35
IS 24
AR L24801
DI 10.1029/2008GL036279
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 386KO
UT WOS:000261882300006
ER
PT J
AU Marzo, GA
Roush, TL
Blanco, A
Fonti, S
Orofino, V
AF Marzo, G. A.
Roush, T. L.
Blanco, A.
Fonti, S.
Orofino, V.
TI Statistical exploration and volume reduction of planetary remote sensing
spectral data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID THERMAL EMISSION SPECTROMETER; SURFACE COMPOSITIONS; MARTIAN SURFACE;
MGS-TES; MARS; IDENTIFICATION; MINERALS
AB Modern planetary scientific experiments are providing a huge amount of information that requires extensive analysis and evaluation in order to understand its scientific content. In this work we evaluate the ability of a previously developed and evaluated technique to explore a large data set in order to identify the cluster representatives of the spectral variability of a selected Martian region and obtain a reduction of the original data volume similar to 2 x 10(4). We also demonstrate that the cluster centroids are able to quantitatively reproduce previously interpreted atmospheric, topographic, and compositional properties. The results build additional confidence in the application of the statistical techniques.
C1 [Marzo, G. A.; Roush, T. L.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Blanco, A.; Fonti, S.; Orofino, V.] Univ Salento, Dept Phys, I-73100 Lecce, Italy.
RP Marzo, GA (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Mail Stop 245-3, Moffett Field, CA 94035 USA.
EM giuseppe.a.marzo@nasa.gov
RI Marzo, Giuseppe/A-9765-2015
FU NASA; Oak Ridge Associated Universities
FX 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. T. L. R.
acknowledges research support from NASA's Planetary Geology and
Geophysics Program.
NR 30
TC 9
Z9 9
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 18
PY 2008
VL 113
IS E12
AR E12009
DI 10.1029/2008JE003219
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 386MG
UT WOS:000261886700001
ER
PT J
AU Fairen, AG
AF Fairen, Alberto G.
TI Finding of unusual soil on Mars could stem from tools used
SO NATURE
LA English
DT Letter
C1 [Fairen, Alberto G.] NASA, Ames Res Ctr, Space Sci & Astrogbiol Div, Moffett Field, CA 94035 USA.
RP Fairen, AG (reprint author), NASA, Ames Res Ctr, Space Sci & Astrogbiol Div, MS 245-3, Moffett Field, CA 94035 USA.
EM afairen@arc.nasa.gov
NR 1
TC 0
Z9 0
U1 0
U2 3
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD DEC 18
PY 2008
VL 456
IS 7224
BP 870
EP 870
DI 10.1038/456870c
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 384TY
UT WOS:000261768300014
PM 19092906
ER
PT J
AU Garcia-Comas, M
Lopez-Puertas, M
Marshall, BT
Wintersteiner, PP
Funke, B
Bermejo-Pantaleon, D
Mertens, CJ
Remsberg, EE
Gordley, LL
Mlynczak, MG
Russell, JM
AF Garcia-Comas, M.
Lopez-Puertas, M.
Marshall, B. T.
Wintersteiner, P. P.
Funke, B.
Bermejo-Pantaleon, D.
Mertens, C. J.
Remsberg, E. E.
Gordley, L. L.
Mlynczak, M. G.
Russell, J. M., III
TI Errors in Sounding of the Atmosphere using Broadband Emission Radiometry
(SABER) kinetic temperature caused by
non-local-thermodynamic-equilibrium model parameters
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CO2 15-MU-M EMISSION; VIBRATIONAL DEACTIVATION; MU-M; COLLISIONAL
DEACTIVATION; LOWER THERMOSPHERE; ENERGY-TRANSFER; CARBON-DIOXIDE;
ATOMIC OXYGEN; LIMB EMISSION; RATE-CONSTANT
AB The vast set of near-global and continuous atmospheric measurements made by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument since 2002, including daytime and nighttime kinetic temperature (T-k) from 20 to 105 km, is available to the scientific community. The temperature is retrieved from SABER measurements of the atmospheric 15 mu m CO2 limb emission. This emission separates from local thermodynamic equilibrium (LTE) conditions in the rarefied mesosphere and thermosphere, making it necessary to consider the CO2 vibrational state non-LTE populations in the retrieval algorithm above 70 km. Those populations depend on kinetic parameters describing the rate at which energy exchange between atmospheric molecules take place, but some of these collisional rates are not well known. We consider current uncertainties in the rates of quenching of CO2(v(2)) by N-2, O-2 and O, and the CO2(v(2)) vibrational-vibrational exchange to estimate their impact on SABER T-k for different atmospheric conditions. The T-k is more sensitive to the uncertainty in the latter two, and their effects depend on altitude. The T-k combined systematic error due to non-LTE kinetic parameters does not exceed +/- 1.5 K below 95 km and +/- 4-5 K at 100 km for most latitudes and seasons (except for polar summer) if the T-k profile does not have pronounced vertical structure. The error is +/- 3 K at 80 km, +/- 6 K at 84 km and +/- 18 K at 100 km under the less favorable polar summer conditions. For strong temperature inversion layers, the errors reach +/- 3 K at 82 km and +/- 8 K at 90 km. This particularly affects tide amplitude estimates, with errors of up to +/- 3 K.
C1 [Garcia-Comas, M.; Lopez-Puertas, M.; Funke, B.; Bermejo-Pantaleon, D.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Marshall, B. T.; Gordley, L. L.] G & A Tech Software, Newport News, VA 23606 USA.
[Mertens, C. J.; Remsberg, E. E.; Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Wintersteiner, P. P.] ARCON Corp, Waltham, MA 02154 USA.
RP Garcia-Comas, M (reprint author), CSIC, Inst Astrofis Andalucia, Apartado Correos 3004, E-18080 Granada, Spain.
EM maya@iaa.es; puertas@iaa.es; b.t.marshall@gats-inc.com;
winters@arcon.com; bernd@iaa.es; diego@iaa.es;
christopher.j.mertens@nasa.gov; ellis.e.remsberg@nasa.gov;
l.l.gordley@gats-inc.com; Martin.G.Mlynczak@nasa.gov;
james.russell@hamptonu.edu
RI Mlynczak, Martin/K-3396-2012; Lopez Puertas, Manuel/M-8219-2013;
Garcia-Comas, Maya/E-4050-2014; Funke, Bernd/C-2162-2008
OI Lopez Puertas, Manuel/0000-0003-2941-7734; Garcia-Comas,
Maya/0000-0003-2323-4486; Funke, Bernd/0000-0003-0462-4702
FU Spanish project [ESP2004-01556]; EC FEDER; NASA TIMED mission; Air Force
Office of Scientific Research
FX The IAA team was partially supported by the Spanish project
ESP2004-01556 and EC FEDER funds. The SABER science team acknowledges
support from NASA TIMED mission under its SABER project. PPW also
acknowledges support from Air Force Office of Scientific Research. The
authors thank A. K. Smith for her valuable help in the estimation of
tidal effects on atomic oxygen, and the anonymous reviewers of this
manuscript, who helped to improve its quality with their thoughtful
comments and suggestions.
NR 42
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Z9 44
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD DEC 17
PY 2008
VL 113
AR D24106
DI 10.1029/2008JD010105
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 386LA
UT WOS:000261883500002
ER
PT J
AU Schoeberl, MR
Douglass, AR
Stolarski, RS
Pawson, S
Strahan, SE
Read, W
AF Schoeberl, M. R.
Douglass, A. R.
Stolarski, R. S.
Pawson, S.
Strahan, S. E.
Read, W.
TI Comparison of lower stratospheric tropical mean vertical velocities
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; TROPOPAUSE TEMPERATURES; ANNUAL CYCLE;
WATER-VAPOR; TRANSPORT MODEL; AIR; CIRCULATION; CHEMISTRY; DIAGNOSTICS;
ATMOSPHERE
AB We have analyzed 13 years (1993-2005) of tropical stratospheric water vapor data from the Halogen Occultation Experiment and over 3 years of data (October 2004 through November 2007) from the Aura Microwave Limb Sounder. By correlating the phase lag of the water vapor "tape recorder'' signal between levels we estimate the time mean vertical velocity. Our estimated vertical velocity compares well with calculations from the Goddard Earth Observing System (GEOS) chemistry-climate model (CCM) and from the GEOS data assimilation system. Between 18 and 26 km both the GEOS CCM simulations and water vapor observations agree that the vertical velocity is below 0.04 cm/s, with a minimum near 20 km of 0.03 cm/s. Vertical velocities deduced from water vapor observations are higher than those from the GEOS CCM in the region 16-18 km (0.04 cm/s) and above 26-30 km (up to 0.07 cm/s). These estimates are close to earlier estimates from a shorter water vapor record and radiative transfer models. No evidence is found for velocities as high as 0.15 cm/s as was recently estimated from aircraft CO2 measurements in the upper troposphere/lower stratosphere. Further diagnosis of the aircraft CO2 data and model simulations of CO2 show that while the CO2 data give an apparent upward transport velocity of similar to 0.06 cm/s, about half of this is due to vertical and horizontal eddy transport. Accounting for the eddy terms gives a CO2-based estimate of the vertical velocity of similar to 0.03 cm/s, in much closer agreement with that estimated from water vapor.
C1 [Schoeberl, M. R.; Douglass, A. R.; Stolarski, R. S.; Pawson, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Read, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Strahan, S. E.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Schoeberl, MR (reprint author), NASA, Goddard Space Flight Ctr, Mail Stop 613-3,Code 910, Greenbelt, MD 20771 USA.
EM mark.r.schoeberl@nasa.gov
RI Douglass, Anne/D-4655-2012; Strahan, Susan/H-1965-2012; Stolarski,
Richard/B-8499-2013; Pawson, Steven/I-1865-2014
OI Stolarski, Richard/0000-0001-8722-4012; Pawson,
Steven/0000-0003-0200-717X
FU NASA
FX The authors would like to acknowledge funding for this research from the
NASA Earth Sciences Program.
NR 41
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Z9 53
U1 0
U2 4
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 DEC 17
PY 2008
VL 113
AR D24109
DI 10.1029/2008JD010221
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 386LA
UT WOS:000261883500003
ER
PT J
AU Su, WY
Schuster, GL
Loeb, NG
Rogers, RR
Ferrare, RA
Hostetler, CA
Hair, JW
Obland, MD
AF Su, Wenying
Schuster, Gregory L.
Loeb, Norman G.
Rogers, Raymond R.
Ferrare, Richard A.
Hostetler, Chris A.
Hair, Johnathan W.
Obland, Michael D.
TI Aerosol and cloud interaction observed from high spectral resolution
lidar data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TO-BACKSCATTER RATIO; PARTICLE-PRODUCTION; OPTICAL-PROPERTIES; RAMAN
LIDAR; EXTINCTION; MICROPHYSICS; ATMOSPHERE; PRODUCTS; OCEAN; CERES
AB Recent studies utilizing satellite retrievals have shown a strong correlation between aerosol optical depth (AOD) and cloud cover. However, these retrievals from passive sensors are subject to many limitations, including cloud adjacency (or three-dimensional) effects, possible cloud contamination, uncertainty in the AOD retrieval. Some of these limitations do not exist in High Spectral Resolution Lidar (HSRL) observations; for instance, HSRL observations are not affected by cloud adjacency effects, are less prone to cloud contamination, and offer accurate aerosol property measurements (backscatter coefficient, extinction coefficient, lidar ratio, backscatter Angstrom exponent, and aerosol optical depth) at a fine spatial resolution (< 100 m) in the vicinity of clouds. Hence the HSRL provides an important data set for studying aerosol and cloud interaction. In this study, we statistically analyze aircraft-based HSRL profiles according to their distance from the nearest cloud, assuring that all profile comparisons are subject to the same largescale meteorological conditions. Our results indicate that AODs from HSRL are about 8 17% higher in the proximity of clouds (similar to 100 m) than far away from clouds (4.5 km), which is much smaller than the reported cloud three-dimensional effect on AOD retrievals. The backscatter and extinction coefficients also systematically increase in the vicinity of clouds, which can be explained by aerosol swelling in the high relative humidity (RH) environment and/or aerosol growth through in-cloud processing (albeit not conclusively). On the other hand, we do not observe a systematic trend in lidar ratio; we hypothesize that this is caused by the opposite effects of aerosol swelling and aerosol in-cloud processing on the lidar ratio. Finally, the observed backscatter Angstrom exponent (BAE) does not show a consistent trend because of the complicated relationship between BAE and RH. We demonstrate that BAE should not be used as a surrogate for Angstrom exponent, especially at high RH.
C1 [Su, Wenying; Rogers, Raymond R.; Obland, Michael D.] Sci Syst & Applications Inc, Hampton, VA 23666 USA.
[Schuster, Gregory L.; Loeb, Norman G.; Ferrare, Richard A.; Hostetler, Chris A.; Hair, Johnathan W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Su, WY (reprint author), Sci Syst & Applications Inc, 1 Enterprise Pkwy, Hampton, VA 23666 USA.
EM wenying.su-1@nasa.gov
FU NASA CALIPSO program
FX The authors thank the support from NASA CALIPSO program and NASA
Interdisciplinary Research in Earth Science under the direction of Dr.
Hal Maring. Wenying Su thanks Bill Smith Jr. for discussions on GOES
image. At the time this research was performed, Michael Obland was a
NASA postdoctoral fellow at NASA Langley Research Center, administered
by Oak Ridge Associated Universities through a contract with NASA.
NR 41
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Z9 49
U1 1
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 DEC 17
PY 2008
VL 113
AR D24202
DI 10.1029/2008JD010588
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 386LA
UT WOS:000261883500006
ER
PT J
AU Willis, JK
Fu, LL
AF Willis, Josh K.
Fu, Lee-Lueng
TI Combining altimeter and subsurface float data to estimate the
time-averaged circulation in the upper ocean
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID DEPTH CIRCULATION; STERIC HEIGHT; NORTH PACIFIC; SOUTH-PACIFIC;
GULF-STREAM; VARIABILITY; TRANSPORT; LABRADOR; HEAT
AB A new technique is presented for estimating time-averaged, upper ocean geostrophic velocity from a combination of altimeter data and subsurface float data. The technique makes uses of the strong relationship between sea-surface height anomaly and anomalous velocity at depth to reduce mesoscale eddy variability in subsurface float displacements. The technique is demonstrated on a region in the North Atlantic that was well sampled by Argo floats. The 2004 through 2006 time-averaged density field was estimated from the surface to 2000 db by combining altimeter and hydrographic data from the floats. In addition, a reference velocity field was estimated at 1000 db based on a combination of altimeter data and subsurface float displacements. The reference velocity field was combined with geostrophic shear based on the density field to produce a three-dimensional estimate of geostrophic velocity from the surface to 2000 db. The Gulf Stream transport in the upper 2000 db is estimated to be 76 Sv at 73 degrees W. In addition, an estimate of the 3-year average dynamic height at the surface was computed by combining the 1000-db reference dynamic height and the time-averaged density field.
C1 [Willis, Josh K.; Fu, Lee-Lueng] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Willis, JK (reprint author), CALTECH, Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jwillis@caltech.edu
FU CNES
FX The altimeter products were produced by Ssalto/Duacs and distributed by
Aviso with support from CNES. Rio05 [Rio and Hernandez, 2004] was
produced by the CLS Space Oceanography Division. The 1992 - 2002 mean
ocean dynamic topography data has been obtained from Nikolai Maximenko
(IPRC) and Peter Niiler (SIO). Thanks to S. Jayne for generously
providing his estimate of surface dynamic height. Float data were
collected and made freely available by Argo (a pilot program of the
Global Ocean Observing System) and contributing national programs
(http://www.argo.net/). 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 27
TC 32
Z9 34
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD DEC 17
PY 2008
VL 113
IS C12
AR C12017
DI 10.1029/2007JC004690
PG 15
WC Oceanography
SC Oceanography
GA 386LP
UT WOS:000261885000002
ER
PT J
AU Alexeev, II
Belenkaya, ES
Bobrovnikov, SY
Slavin, JA
Sarantos, M
AF Alexeev, I. I.
Belenkaya, E. S.
Bobrovnikov, S. Yu.
Slavin, J. A.
Sarantos, M.
TI Paraboloid model of Mercury's magnetosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND INTERACTION; MESSENGERS 1ST FLYBY; MAGNETIC-FIELD; HERMEAN
MAGNETOSPHERE; TERRESTRIAL PLANETS; SODIUM EXOSPHERE; ELECTRIC-FIELDS;
SURFACE; MAGNETOPAUSE; MISSION
AB A new "Paraboloidal'' model of Mercury's magnetospheric magnetic field based upon the earlier terrestrial model and using similar techniques is developed. The model describes the field of Mercury's dipole, which is considered to be offset from the planet's center; the magnetopause currents driven by the solar wind; and the tail current system including the cross-tail currents and their closure currents at the magnetopause. The effect of the interplanetary magnetic field (IMF) is modeled as a partial penetration of the IMF into the magnetosphere. The goals of the present work are (1) to develop an easily usable, yet robust model of Mercury's magnetospheric magnetic field and (2) to produce an improved "unified'' determination of Mercury's magnetic dipole moment which fits the measurements taken during both Mariner 10's first and third flybys. This new model of Mercury's magnetosphere is described and used to determine a best Mercury magnetic dipole moment of 192 nT R-M(3), from the two Mariner 10 flybys, a value which is intermediate between the various estimates produced by previous models. The best fit to the Mariner 10 measurements gives the dipole offset 0.18 R-M above the equatorial plane. The new Paraboloidal model is used to predict the configuration of this miniature magnetosphere under average and extreme solar wind conditions.
C1 [Alexeev, I. I.; Belenkaya, E. S.; Bobrovnikov, S. Yu.] Moscow MV Lomonosov State Univ, Inst Nucl Phys, Moscow, Russia.
[Slavin, J. A.; Sarantos, M.] NASA, GSFC, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Alexeev, II (reprint author), Moscow MV Lomonosov State Univ, Inst Nucl Phys, POB 119991, Moscow, Russia.
EM james.a.slavin@nasa.gov
RI Belenkaya, Elena/D-6940-2012; Slavin, James/H-3170-2012; Alexeev,
Igor/G-8773-2011; Sarantos, Menelaos/H-8136-2013
OI Slavin, James/0000-0002-9206-724X;
FU RFBR [07-05-00529]; NASA
FX Work at the Institute of Nuclear Physics, Moscow State University, was
supported by the RFBR Grant 07-05-00529. MS was supported by the NASA
Postdoctoral Program (NPP).; Wolfgang Baumjohann thanks the reviewers
for their assistance in evaluating this paper.
NR 76
TC 31
Z9 32
U1 2
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD DEC 17
PY 2008
VL 113
IS A12
AR A12210
DI 10.1029/2008JA013368
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 386MQ
UT WOS:000261887700001
ER
PT J
AU Liston, DB
Stone, LS
AF Liston, Dorion B.
Stone, Leland S.
TI Effects of Prior Information and Reward on Oculomotor and Perceptual
Choices
SO JOURNAL OF NEUROSCIENCE
LA English
DT Article
DE saccade; attention; basal ganglia; superior colliculus; frontal eye
field; lateral intraparietal area
ID FRONTAL EYE FIELD; SUPERIOR COLLICULUS; SPATIAL ATTENTION;
CAUDATE-NUCLEUS; RESPONSE BIAS; VISUAL-SEARCH; AREA V4; MACAQUE;
MOVEMENTS; DECISION
AB Expectations about the environment influence motor behavior. In simple tasks, for example, prior knowledge about which stimulus event will likely occur or which response will likely be rewarded induces a tendency to take the favored action (i.e., a motor or response bias), especially when sensory information is sparse or ambiguous. Models of choice behavior account for this bias by weighting decision alternatives unequally, either at an early sensory-input stage or at a downstream motor-output stage. These two alternatives can be distinguished empirically; the former predicts an altered percept that correlates with motor bias, the latter predicts no perceptual effect. By varying the prior probability of target or reward location, we induced biased oculomotor responses in a brightness selection task with human subjects. We found that the induced motor bias was correlated with an amplification of both the sensory signals and internal noise underlying brightness perception, without a systematic change in perceived overall brightness. We also found that the magnitude of the sensory amplification was correlated with the amount of noise in the brightness percept, consistent with a multiplicative weighting factor located downstream from the limiting internal sensory noise. Our data demonstrate that prior knowledge (about target location or reward) shapes visual signals for perception and action in parallel but does not improve the quality (i.e., signal-to-noise ratio) of sensory processing.
C1 [Liston, Dorion B.; Stone, Leland S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Liston, Dorion B.] San Jose State Univ, San Jose, CA 95192 USA.
RP Liston, DB (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2, Moffett Field, CA 94035 USA.
EM dorion.b.liston@nasa.gov
FU NASA's Space Human Factors Engineering Program
FX This work was supported by NASA's Space Human Factors Engineering
Program. We are grateful to Al Ahumada for suggesting the continuous
analysis and to Miguel Eckstein, Brent Beutter, and Barbara Chapman for
helpful feedback on a previous draft of this manuscript. We also thank
the two anonymous reviewers for their insightful feedback and helpful
suggestions and Rami Ersheid for technical support.
NR 58
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U1 0
U2 2
PU SOC NEUROSCIENCE
PI WASHINGTON
PA 11 DUPONT CIRCLE, NW, STE 500, WASHINGTON, DC 20036 USA
SN 0270-6474
J9 J NEUROSCI
JI J. Neurosci.
PD DEC 17
PY 2008
VL 28
IS 51
BP 13866
EP 13875
DI 10.1523/JNEUROSCI.3120-08.2008
PG 10
WC Neurosciences
SC Neurosciences & Neurology
GA 384YM
UT WOS:000261780100016
PM 19091976
ER
PT J
AU Rind, D
Lean, J
Lerner, J
Lonergan, P
Leboissitier, A
AF Rind, D.
Lean, J.
Lerner, J.
Lonergan, P.
Leboissitier, A.
TI Exploring the stratospheric/tropospheric response to solar forcing
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; TROPOSPHERE-STRATOSPHERE SYSTEM; UV
VARIABILITY; CLIMATE VARIATIONS; OCEAN TEMPERATURE; EARTHS ATMOSPHERE;
CYCLE VARIABILITY; JULY-AUGUST; SIGNAL; OZONE
AB We use the new Goddard Institute for Space Studies Global Climate Middle Atmosphere Model 3 with four different resolutions to investigate various aspects of solar cycle influence on the troposphere/stratosphere system. Three different configurations of sea surface temperatures are used to help determine whether the tropospheric response is due to forcing from above (UV variations impacting the stratosphere) or below (total solar irradiance changes acting through the surface temperature field). The results show that the stratospheric response is highly repeatable and significant. With the more active sun, the annual residual circulation change features relative increased upwelling in the Southern Hemisphere and downwelling in the Northern Hemisphere. Stratospheric west wind increases extend down into the troposphere, especially during Southern Hemisphere winter, and in some runs the jet stream weakens and moves poleward. The predominant tropospheric response consists of warming in the troposphere, with precipitation decreases south of the equator and in the Northern Hemisphere subtropics and midlatitudes, with increases north of the equator especially over southern Asia. The tropospheric response is often not significant, but is fairly robust among the different simulations. These features, which have been reported in observations and other model studies, appear to be driven both from the stratosphere and the surface; nevertheless, they account for only a small percentage of the total variance. More accurate simulations of the solar cycle stratospheric ozone response, the quasi-biennial oscillation, and coupled atmosphere-ocean dynamics are necessary before any conclusions can be deemed definitive.
C1 [Rind, D.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Lean, J.] USN, Res Lab, Washington, DC 20375 USA.
[Lerner, J.; Lonergan, P.; Leboissitier, A.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
RP Rind, D (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM drind@giss.nasa.gov
OI Lean, Judith/0000-0002-0087-9639
FU NASA
FX This work was supported by the NASA Living With A Star program and the
NASA Atmospheric Composition focus area. Computer time was provided by
the NASA NCCS high-speed computing program. Climate modeling at GISS in
general is supported by the NASA Climate Variability and Climate Change
focus area.
NR 63
TC 45
Z9 51
U1 2
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 DEC 16
PY 2008
VL 113
AR D24103
DI 10.1029/2008JD010114
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 386KY
UT WOS:000261883300003
ER
PT J
AU Farrand, WH
Bell, JF
Johnson, JR
Arvidson, RE
Crumpler, LS
Hurowitz, JA
Schroder, C
AF Farrand, W. H.
Bell, J. F., III
Johnson, J. R.
Arvidson, R. E.
Crumpler, L. S.
Hurowitz, J. A.
Schroder, C.
TI Rock spectral classes observed by the Spirit Rover's Pancam on the Gusev
Crater Plains and in the Columbia Hills
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MARS; HEMATITE; ANALOG; SOIL
AB This paper examines the ferrous and ferric iron mineralogy of rocks inferred from 246 visible/near-infrared (430-1010 nm) multispectral observations made by the Mars Exploration Rover Spirit's Pancam on its traverse from its landing site to its second Winter Haven location. Principal component, correspondence analyses, and a sequential maximum angle convex cone technique were used to identify 14 candidate classes. Spectra from the West Spur of Husband Hill and the Watchtower area had the highest 535 and 601 nm band depths indicating that these areas were more oxidized. Differences in the depth and band center of a near infrared (NIR) absorption feature were observed using 904 nm band depth and 803: 904 nm ratio and parameters gauging the 754-864 and 754-1009 nm slopes. Spectra of rocks from the southern flank of Husband Hill had negative 754-1009 nm slopes and a broad NIR absorption consistent with high olivine abundances. Rocks observed on the lower West Spur, at the Cumberland Ridge locale, at the Husband Hill summit, and at the Haskin Ridge locale had deep 904 nm band depths and steep 754-864 nm slopes consistent with greater pyroxene abundances. These observations are consistent with results on iron-bearing mineralogy from Spirit's Mossbauer spectrometer. Comparisons of these rock spectral classes with a set of terrestrial analog samples found similarities between the West Spur and Watchtower classes and red hematite-bearing impact melts. Fewer similarities were found in comparisons of the Columbia Hills classes with basaltic hydrovolcanic tephras.
C1 [Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA.
[Bell, J. F., III] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Johnson, J. R.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA.
[Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Crumpler, L. S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA.
[Hurowitz, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schroder, C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Farrand, WH (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
EM farrand@spacescience.org
RI Schroder, Christian/B-3870-2009; Johnson, Jeffrey/F-3972-2015
OI Schroder, Christian/0000-0002-7935-6039;
NR 51
TC 24
Z9 24
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 16
PY 2008
VL 113
IS E12
AR E12S38
DI 10.1029/2008JE003237
PG 25
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 386ME
UT WOS:000261886500001
ER
PT J
AU Prather, MJ
Zhua, X
Strahan, SE
Steenrod, SD
Rodriguez, JM
AF Prather, Michael J.
Zhua, Xin
Strahan, Susan E.
Steenrod, Stephen D.
Rodriguez, Jose M.
TI Quantifying errors in trace species transport modeling
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE biogeochemical cycles; model errors; source inversions; uncertainties
ID GENERAL-CIRCULATION MODEL; ATMOSPHERIC TRANSPORT; NUMERICAL ADVECTION;
INITIATIVE ASSESSMENT; CO2; CHEMISTRY; FORMULATIONS; SIMULATIONS;
SENSITIVITY; DYNAMICS
AB One expectation when computationally solving an Earth system model is that a correct answer exists, that with adequate physical approximations and numerical methods our solutions will converge to that single answer. With such hubris, we performed a controlled numerical test of the atmospheric transport of CO2 using 2 models known for accurate transport of trace species. Resulting differences were unexpectedly large, indicating that in some cases, scientific conclusions may err because of lack of knowledge of the numerical errors in tracer transport models. By doubling the resolution, thereby reducing numerical error, both models show some convergence to the same answer. Now, under realistic conditions, we identify a practical approach for finding the correct answer and thus quantifying the advection error.
C1 [Prather, Michael J.; Zhua, Xin] Univ Calif Irvine, Earth Syst Sci Dept, Irvine, CA 92697 USA.
[Strahan, Susan E.; Steenrod, Stephen D.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA.
[Rodriguez, Jose M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Prather, MJ (reprint author), Univ Calif Irvine, Earth Syst Sci Dept, 3329 Croul Hall, Irvine, CA 92697 USA.
EM mprather@uci.edu
RI Strahan, Susan/H-1965-2012; Steenrod, Stephen/H-2218-2012
FU National Aeronautics and Space Administration [NNG06GB84G, NNG04GA09G];
National Science Foundation [NSF ATM-0550234]; Kavli Foundation
FX We thank 2 referees for their insightful comments. This work was
supported at the University of California, Irvine, by National
Aeronautics and Space Administration Grants NNG06GB84G and NNG04GA09G,
National Science Foundation Grant NSF ATM-0550234, and the Kavli
Foundation.
NR 30
TC 28
Z9 28
U1 1
U2 4
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 DEC 16
PY 2008
VL 105
IS 50
BP 19617
EP 19621
DI 10.1073/pnas.0806541106
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 385GI
UT WOS:000261802300011
PM 19066224
ER
PT J
AU Levine, LH
Kasahara, H
Kopka, J
Erban, A
Fehrl, I
Kaplan, F
Zhao, W
Littell, RC
Guy, C
Wheeler, R
Sager, J
Mills, A
Levine, HG
AF Levine, Lanfang H.
Kasahara, Hirokazu
Kopka, Joachim
Erban, Alexander
Fehrl, Ines
Kaplan, Fatma
Zhao, Wei
Littell, Ramon C.
Guy, Charles
Wheeler, Raymond
Sager, John
Mills, Aaron
Levine, Howard G.
TI Physiologic and metabolic responses of wheat seedlings to elevated and
super-elevated carbon dioxide
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Elevated carbon dioxide; Evapotranspiration (ET); Metabolite profile;
Primary metabolites; Secondary metabolites; Super-elevated carbon
dioxide; Wheat (Triticum aestivum)
ID CHROMATOGRAPHY-MASS SPECTROMETRY; CO2 ENRICHMENT; STOMATAL CONDUCTANCE;
FEEDBACK-REGULATION; LEAF SENESCENCE; GENE-EXPRESSION; ATMOSPHERIC CO2;
LOTUS-JAPONICUS; PHOTOSYNTHESIS; ACCLIMATION
AB The metabolic consequence Of suboptimal (400 mu mol mol(-1) or ppm), near-optimal (1500 ppm)and supra-optimal (10,000 ppm) atmospheric carbon dioxide concentrations [CO(2)] Wits investigated in an attempt to reveal plausible underlying mechanisms for the differential physiological and developmental responses to increasing [CO(2)] Both non-targeted and targeted metabolite profiling by GC-MS and LC-MS were employed to examine primary and secondary metabolites in wheat (Triticum aestivum, cv Yocoro rojo) continuously exposed to these [CO(2)] levels for 14, 21 and 28 days. Metabolite profile wits altered by both [CO(2)] and physiological age. In general, plants grown under high [CO(2)] exhibited a metabolite profile characteristic of older plants under ambient CO(2) Elevated [CO(2)] resulted in higher levels of phosphorylated sugar intermediates, though no clear trend in the content of reducing sugars was observed. Transient starch content was enhanced by increasing [CO(2)] to it Much greater extent at 10,000 ppm CO(2) than at 1500 ppm CO(2). The percentage increase of starch content resulting from CO(2) enrichment declined as plants develope. In contrast, elevated [CO(2)] promoted the accumulation of secondary metabolites (flavonoids) progressively to it greater extent as plants became mature. Elevated [CO(2)] to 1500 ppm induced it higher initial growth rate, while super-elevated [CO(2)] appeared to negate such initial growth promotion. However, after 4 weeks, there was no difference in vegetative growth between 1500 and 10,000 ppm CO(2)-grown plants, both elevated CO(2) levels resulted in all overall 25% increase in biomass over the control plants. More interestingly, elevated atmospheric [CO(2)] reduced evapotranspiration rate (ET), but further increase to the supra-optimal level resulted in increased ET (it reversed trend), i.e. ET at 1500 ppm < ET at 10,000 ppm < ET at 400 ppm. the differential effect of elevated and super-elevated CO(2) oil plants was further reflected in the nitrogen dynamics. These results provide the potential metabolic basis for the differential productivity and stomatal function of plants grown under elevated and super-elevated CO(2) levels. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Levine, Lanfang H.] Dynamac Corp, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA.
[Kasahara, Hirokazu] Hokkaido Tokai Univ, Sch Engn, Dept Biosci & Technol, Sapporo, Hokkaido, Japan.
[Kopka, Joachim; Erban, Alexander; Fehrl, Ines] Max Planck Inst Mol Pflanzenphysiol, D-14476 Golm, Germany.
[Kaplan, Fatma; Guy, Charles] Univ Florida, Dept Environm Hort, Plant Mol & Cellular Biol Program, Gainesville, FL 32611 USA.
[Zhao, Wei; Littell, Ramon C.] Univ Florida, Inst Food & Agr Sci, Dept Stat, Gainesville, FL 32611 USA.
[Wheeler, Raymond; Sager, John; Mills, Aaron; Levine, Howard G.] NASA, Sustainable Syst Div, Kennedy Space Ctr, FL 32899 USA.
RP Levine, LH (reprint author), Dynamac Corp, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA.
EM lanfang.h.levine@nasa.gov
OI Kopka, Joachim/0000-0001-9675-4883
FU NASA NRA [NCC 10-5, NAG10-316]; KSC Center Director Discretionary Fund
FX We acknowledge Gerogiana Tynes for her assistance in plant cultivation
and sampling. This work was supported by: (1) NASA NRA Grant NCC 10-5,
(2) it metabolomics initiative via SABRE/UF from NASA Grant NAG10-316,
and (3) the KSC Center Director Discretionary Fund 2005.
NR 51
TC 21
Z9 24
U1 1
U2 15
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 DEC 15
PY 2008
VL 42
IS 12
BP 1917
EP 1928
DI 10.1016/j.asr.2008.07.014
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 384FD
UT WOS:000261728800005
ER
PT J
AU Drysdale, A
Nakamura, T
Yorio, N
Sager, J
Wheeler, R
AF Drysdale, Alan
Nakamura, Takashi
Yorio, Neil
Sager, John
Wheeler, Ray
TI Use of sunlight for plant lighting in a bioregenerative life support
system - Equivalent system mass calculations
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Space life sciences; Bioregenerative systems; Plant lighting systems
AB Plant lighting is it critical issue for cost effectiveness of bioregenerative systems. A plant lighting system using sunlight has been investigated and compared to systems using electrical lighting. Co-generation of electricity and use of in situ resource utilization (ISRU) were also considered. The fixed part of equivalent system mass was found to be reduced by factors of from 3.1 to 3.9, according to the mission assumptions. The time-dependent part of equivalent system mass was reduced by it smaller value, of about 1.05. Cost effectiveness of bioregeneration hits been compared to the cost of shipping food. Break-even times for different Lunar and Mars missions were generally in the order of 2-10 years, and were quite sensitive to the assumptions. There is significant scope for future refinement of these values, and work is ongoing. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Nakamura, Takashi] Phys Sci Inc, New England Business Ctr 20, Andover, MA 01810 USA.
[Yorio, Neil] Dynamac Corp, DYN 3, Kennedy Space Ctr, FL 32815 USA.
[Sager, John; Wheeler, Ray] NASA, Kennedy Space Ctr, FL 32815 USA.
RP Drysdale, A (reprint author), 6208 Windover Way, Titusville, FL 32780 USA.
EM gnrlact@cfl.rr.com; nakamura@psicorp.com; neil.c.yorio@nasa.gov;
john.c.sager@nasa.gov; raymond.m.wheeler@nasa.gov
FU SBIR [NNK060M15C]
FX This work was supported by SBIR Grant NNK060M15C.
NR 25
TC 4
Z9 4
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 DEC 15
PY 2008
VL 42
IS 12
BP 1929
EP 1943
DI 10.1016/j.asr.2008.09.020
PG 15
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 384FD
UT WOS:000261728800006
ER
PT J
AU Ito, M
Messenger, S
AF Ito, Motoo
Messenger, Scott
TI Isotopic imaging of refractory inclusions in meteorites with the
NanoSIMS 50L
SO APPLIED SURFACE SCIENCE
LA English
DT Article
DE NanoSIMS 50L; Ca, Al-rich inclusions (CAIs); Oxygen isotope image;
Isotopic measurement; Cooling rate; Extraterrestrial material
ID AL-RICH INCLUSIONS; SOLAR-SYSTEM; ALLENDE; ORIGIN; CA; ANOMALIES;
HETEROGENEITY; CHONDRITES; NEBULA; RATIOS
AB Oxygen isotopic micro-distributions within and among silicate and oxide minerals in a meteorite were measured with the JSC NanoSIMS 50L by isotopic imaging. High precision isotopic images with micrometer-scale resolution revealed detailed O isotope distributions within CAI minerals. Small-scale heterogeneous distributions of O isotopes constrain the history of isotopic exchange mechanisms in the CAI during and since its formation in the early solar system. We describe the development O isotopic imaging of insulating minerals with high precision of +/-6 and 3 parts per thousand for delta(17)O and delta(18)O, respectively. Published by Elsevier B.V.
C1 [Ito, Motoo; Messenger, Scott] NASA, Lyndon B Johnson Space Ctr, ARES, Robert M Walker Lab Space Sci, Houston, TX 77573 USA.
RP Ito, M (reprint author), NASA, Lyndon B Johnson Space Ctr, ARES, Robert M Walker Lab Space Sci, 2101 NASA Pkwy, Houston, TX 77573 USA.
EM motoo.ito-1@nasa.gov; scott.r.messenger@nasa.gov
NR 28
TC 5
Z9 5
U1 0
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-4332
J9 APPL SURF SCI
JI Appl. Surf. Sci.
PD DEC 15
PY 2008
VL 255
IS 4
BP 1446
EP 1450
DI 10.1016/j.apsusc.2008.05.095
PG 5
WC Chemistry, Physical; Materials Science, Coatings & Films; Physics,
Applied; Physics, Condensed Matter
SC Chemistry; Materials Science; Physics
GA 460UX
UT WOS:000267217500062
ER
PT J
AU Solaimanzadeh, I
Schlegel, TT
Feiveson, AH
Greco, EC
Depalma, JL
Starc, V
Marthol, H
Tutaj, M
Buechner, S
Axelrod, FB
Hilz, MJ
AF Solaimanzadeh, I.
Schlegel, T. T.
Feiveson, A. H.
Greco, E. C.
Depalma, J. L.
Starc, V.
Marthol, H.
Tutaj, M.
Buechner, S.
Axelrod, F. B.
Hilz, M. J.
TI Advanced electrocardiographic predictors of mortality in familial
dysautonomia
SO AUTONOMIC NEUROSCIENCE-BASIC & CLINICAL
LA English
DT Article
DE Heart rate variability; Bradycardia; Signal averaged ECG; QT interval;
QRS-T angle; T-wave morphology; Hypoxia; Left ventricular hypertrophy
ID LEFT-VENTRICULAR HYPERTROPHY; HEART-RATE-VARIABILITY; OBSTRUCTIVE
SLEEP-APNEA; QT INTERVAL VARIABILITY; SUDDEN CARDIAC DEATH; T-WAVE
MORPHOLOGY; MYOCARDIAL-INFARCTION; BLOOD-PRESSURE; REPOLARIZATION
LABILITY; ATRIOVENTRICULAR-BLOCK
AB Objective: To identify electrocardiographic predictors of mortality in patients with familial dysautonomia (FD). Methods: Ten-minute resting high-fidelity 12-lead electrocardiograms (ECGs) were obtained from 14 FD patients and 14 age/gender-matched healthy subjects. Multiple conventional and advanced ECG parameters were Studied for their ability to predict mortality over a subsequent 4.5-year period, including representative parameters of heart rate variability (HRV), QT variability (QTV), T-wave complexity, signal averaged ECG, and 3-dimensional ECG.
Results: Four of the 14 FD patients died during the follow-up period, three with concomitant pulmonary disorder. Of the ECG parameters Studied, increased non-HRV-correlated QTV and decreased HRV were the most predictive of death. Compared to controls as a group, FD patients also had significantly increased ECG voltages. JTc intervals and waveform complexity, suggggestive of structural heart disease.
Conclusion: Increased QTV and decreased HRV are markers for increased risk of death in FD patients. When present, both markets may reflect concurrent pathological processes, especially hypoxia due to pulmonary disorders and sleep apnea.
C1 [Schlegel, T. T.; Feiveson, A. H.; Greco, E. C.; Depalma, J. L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Solaimanzadeh, I.] Natl Space Biomed Res Inst, Houston, TX USA.
[Solaimanzadeh, I.] CUNY Queens Coll, Flushing, NY USA.
[Starc, V.] Univ Ljubljana, Inst Physiol, Ljubljana, Slovenia.
[Marthol, H.] Univ Erlangen Nurnberg, Dept Neurol, D-8520 Erlangen, Germany.
[Tutaj, M.] Jagiellonian Univ, Dept Neurol, Krakow, Poland.
[Buechner, S.] Reg Gen Hosp, Dept Neurol, Bolzano, Italy.
[Axelrod, F. B.; Hilz, M. J.] NYU, Med Ctr, Dept Neurol, New York, NY 10016 USA.
RP Schlegel, TT (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code SK3, Houston, TX 77058 USA.
EM todd.t.schlegel@nasa.gov
FU National Space Biomedical Research Institute; Johnson Space Center
Technology Investment Fund; Johnson Space Center Summer Faculty
Fellowship; USA-Slovenia Cooperation in Science and Technology;
Kosciuszko Foundation; Dysautonomia Foundation, Inc.
FX This research was supported by grants front the National Space
Biomedical Research Institute (Student Internship Program, Mr.
Solaimanzadeh), the Johnson Space Center Technology Investment Fund (Dr.
Schlegel), the Johnson Space Center Summer Faculty Fellowship program
(Drs. Greco and DePalma), the USA-Slovenia Cooperation in Science and
Technology (Drs. Starc and Schlegel), the Kosciuszko Foundation (Dr.
Tutaj), and the Dysautonomia Foundation, Inc. (Drs. Axelrod, Hilz,
Marthol, Buechner). The advanced ECG hardware and software were provided
Courtesy of CardioSoft and Enhanced Cardiology, Houston, TX.
NR 70
TC 16
Z9 16
U1 1
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1566-0702
J9 AUTON NEUROSCI-BASIC
JI Auton. Neurosci-Basic Clin.
PD DEC 15
PY 2008
VL 144
IS 1-2
BP 76
EP 82
DI 10.1016/j.autneu.2008.08.016
PG 7
WC Neurosciences
SC Neurosciences & Neurology
GA 386BM
UT WOS:000261857300009
PM 18851930
ER
PT J
AU Sawakuchi, GO
Yukihara, EG
McKeever, SWS
Benton, ER
Gaza, R
Uchihori, Y
Yasuda, N
Kitamura, H
AF Sawakuchi, G. O.
Yukihara, E. G.
McKeever, S. W. S.
Benton, E. R.
Gaza, R.
Uchihori, Y.
Yasuda, N.
Kitamura, H.
TI Relative optically stimulated luminescence and thermoluminescence
efficiencies of Al2O3:C dosimeters to heavy charged particles with
energies relevant to space and radiotherapy dosimetry
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
DE aerospace biophysics; alumina; carbon; dosimetry; photoluminescence;
radiation therapy; thermoluminescent dosimeters
ID THERMO-LUMINESCENCE; RADIATION-DOSIMETRY; OSL; ION; DETECTORS; TRACK;
LIF; IRRADIATION; STATION; SYSTEM
AB This article presents a comprehensive characterization of the thermoluminescence (TL) and optically stimulated luminescence (OSL) relative luminescence efficiencies of carbon-doped aluminum (Al2O3:C) for heavy charged particles (HCPs) with atomic numbers ranging from 1 (proton) to 54 (xenon) and energies ranging from 7 to 1000 MeV/u, and investigates the dependence of the Al2O3:C response on experimental conditions. Relative luminescence efficiency values are presented for 19 primary charge/energy combinations, plus 31 additional charge/energy combinations obtained by introducing absorbers in the primary beam. Our results show that for energies of hundreds of MeV/u the data can be described by a single curve of relative luminescence efficiency versus linear energy transfer (LET). This information is needed to compensate for the reduced OSL efficiency to high-LET particles in such applications as space dosimetry. For lower energies, the relative luminescence efficiency as function of LET cannot be described by a single curve; instead, it separates into different components corresponding to different particles. We also present data on the low-LET dose response of Al2O3:C, measured under the same experimental conditions in which the relative luminescence efficiencies to HCPs were obtained, providing information relevant to future theoretical investigations of HCP energy deposition and luminescence production in Al2O3:C.
C1 [Uchihori, Y.; Yasuda, N.; Kitamura, H.] Natl Inst Radiol Sci, Chiba 2638555, Japan.
[Sawakuchi, G. O.; Yukihara, E. G.; McKeever, S. W. S.; Benton, E. R.] Oklahoma State Univ, Dept Phys, Radiat Dosimetry Lab, Stillwater, OK 74078 USA.
[Gaza, R.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
[Gaza, R.] NASA, Lyndon B Johnson Space Ctr, Space Radiat Anal Grp, Houston, TX 77058 USA.
RP Sawakuchi, GO (reprint author), Univ Texas MD Anderson Canc Ctr, Dept Radiat Phys, Unit 94,1515 Holcombe Blvd, Houston, TX 77030 USA.
EM gsawakuchi@mdanderson.org; eduardo.yukihara@okstate.edu
RI Sawakuchi, Gabriel/A-8961-2009; Yukihara, Eduardo/F-1345-2014
OI Yukihara, Eduardo/0000-0002-4615-6698
NR 52
TC 18
Z9 18
U1 2
U2 14
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD DEC 15
PY 2008
VL 104
IS 12
AR 124903
DI 10.1063/1.3041655
PG 10
WC Physics, Applied
SC Physics
GA 391HT
UT WOS:000262225100127
ER
PT J
AU Gruszczynski, M
Marshall, JD
Goldring, R
Coleman, ML
Malkowski, K
Gazdzicka, E
Semil, J
Gatt, P
AF Gruszczynski, Michal
Marshall, Jim D.
Goldring, Roland
Coleman, Max L.
Malkowski, Krzysztof
Gazdzicka, Elzbieta
Semil, Julia
Gatt, Peter
TI Hiatal surfaces from the Miocene Globigerina Limestone Formation of
Malta: Biostratigraphy, sedimentology, trace fossils and early
diagenesis
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article; Proceedings Paper
CT Symposium on Biotic-Sediment Interactions in honor of Roland Goldring
CY JUL 20-22, 2006
CL Univ Reading, Reading, ENGLAND
SP Ichron Ltd, BG Grp, Palaeontol Assoc
HO Univ Reading
DE Hardgrounds and firmgrounds; Carbon and oxygen stable isotopes; Calcite
and dolomite cementation
ID CALCAREOUS NANNOFOSSIL BIOSTRATIGRAPHY; ORDOVICIAN HARDGROUND COMMUNITY;
ISLAND SOUND SEDIMENTS; SUBMARINE LITHIFICATION; MEDITERRANEAN REGION;
CARBONATE SEDIMENTS; BEAR-ISLAND; ENVIRONMENTS; BASIN; SEA
AB The Miocene Globigerina Limestone of the Maltese islands contains widespread omission surfaces with very different characteristics and origins.
The terminal Lower Globigerina Limestone hardground (TLGLHg) formed during a period of falling sea level. Coccolith assemblages suggest shallowness. Sedimentary structures and trace fossil assemblages, indicate increasing frequency of storm events and erosional episodes, towards the surface. Calcite cementation which took place around Thalassinoides burrows and formed irregular nodules was followed by dissolution of aragonite. It is suggested that lithification was linked to microbial reactions involving organic matter.
In contrast two later surfaces, the terminal Middle Globigerina Limestone omissionground (TMGLOg), which marks the Lower to Middle Miocene boundary, and the Fomm-ir-Rih local hardground (FiRLHg) both contain early diagenetic dolomite. Lithification took place in two phases. The dolomite is interpreted to have formed beneath the sea floor: it was subsequently exhumed and partially corroded as the precipitation of calcitic and phosphatic cements took place around burrows open to the circulation of sea water. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Gruszczynski, Michal] Uniwersytet Jana Kochanowskiego, Inst Geog, PL-25406 Kielce, Poland.
[Gruszczynski, Michal; Malkowski, Krzysztof] Polish Acad Sci, Inst Paleobiol, PL-00818 Warsaw, Poland.
[Marshall, Jim D.] Univ Liverpool, Liverpool L69 3GP, Merseyside, England.
[Goldring, Roland; Coleman, Max L.] Univ Reading, Sch Human & Environm Sci, Reading RG6 6AB, Berks, England.
[Coleman, Max L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gazdzicka, Elzbieta] Panstwowy Inst Geol, PL-00975 Warsaw, Poland.
[Semil, Julia] Univ Warsaw, Wydzial Geol, PL-02089 Warsaw, Poland.
[Gatt, Peter] Univ Malta, Dept Civil Engn, Msida, Malta.
RP Gruszczynski, M (reprint author), Uniwersytet Jana Kochanowskiego, Inst Geog, Swietokrzyska 15, PL-25406 Kielce, Poland.
EM beerbear@onet.eu
RI Coleman, Max/A-1303-2007
OI Coleman, Max/0000-0002-5514-1826
NR 75
TC 9
Z9 10
U1 0
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-0182
J9 PALAEOGEOGR PALAEOCL
JI Paleogeogr. Paleoclimatol. Paleoecol.
PD DEC 15
PY 2008
VL 270
IS 3-4
BP 239
EP 251
DI 10.1016/j.palaeo.2008.01.035
PG 13
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA 386AE
UT WOS:000261853900004
ER
PT J
AU Brown, CA
Huot, Y
Werdell, PJ
Gentili, B
Claustre, H
AF Brown, Catherine A.
Huot, Yannick
Werdell, P. Jeremy
Gentili, Bernard
Claustre, Herve
TI The origin and global distribution of second order variability in
satellite ocean color and its potential applications to algorithm
development
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Remote sensing; MODIS; Optical properties; Backscattering; CDOM; Ocean
color; Bio-optics
ID INHERENT OPTICAL-PROPERTIES; ANTARCTIC PENINSULA WATERS; CASE-I WATERS;
CASE-1 WATERS; BIOOPTICAL PROPERTIES; CHLOROPHYLL-A; PHYTOPLANKTON
PIGMENTS; MULTISENSOR APPROACH; REFLECTANCE MODEL; COASTAL WATERS
AB Empirical algorithms based on first order relationships between ocean color and the chlorophyll concentration ([ChI]; mg m(-3)) are widely used, but cannot explain the statistical dispersion or "anomalies" around the mean trends. We use an empirical approach that removes the first order effects of [ChI] from satellite ocean color, thus allowing us to quantify the impact on the ocean color signal of optical anomalies that vary independently of the global mean trends with remotely sensed [ChI]. We then present statistical and modeling analyses to interpret the observed anomalies in terms of their optical sources (i.e. absorption and backscattering coefficients). We identify two main sources of second order variability for a given [ChI]: 1) the amount of non-algal absorption, especially due to colored dissolved organic matter; and 2) the amplitude of the backscattering coefficient of particles. The global distribution of the anomalies displays significant regional and seasonal trends, providing important information for characterizing the marine optical environment and for inferring biogeochemical influences. We subsequently use our empirically determined anomalies to estimate the backscattering coefficient of particles and the combined absorption coefficient for colored detrital and dissolved materials. This purely empirical approach provides an independent assessment of second order optical variability for comparison with existing methods that are generally based on semi-analytical models. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Brown, Catherine A.; Huot, Yannick; Gentili, Bernard; Claustre, Herve] CNRS, UMR 7093, Oceanog Lab, F-06230 Villefranche Sur Mer, France.
[Brown, Catherine A.; Huot, Yannick; Gentili, Bernard; Claustre, Herve] Univ Paris 06, UMR 7093, Oceanog Lab, F-06230 Villefranche Sur Mer, France.
[Werdell, P. Jeremy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Brown, CA (reprint author), CNRS, UMR 7093, Oceanog Lab, F-06230 Villefranche Sur Mer, France.
EM brown@obs-vlfr.fr
RI Werdell, Jeremy/D-8265-2012; Huot, Yannick/B-4497-2008; CLAUSTRE,
Herve/E-6877-2011
OI Huot, Yannick/0000-0003-1793-761X; CLAUSTRE, Herve/0000-0001-6243-0258
NR 64
TC 47
Z9 48
U1 1
U2 13
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 DEC 15
PY 2008
VL 112
IS 12
BP 4186
EP 4203
DI 10.1016/j.rse.2008.06.008
PG 18
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 373AD
UT WOS:000260942500002
ER
PT J
AU Bindschadler, R
Vornberger, P
Fleming, A
Fox, A
Mullins, J
Binnie, D
Paulsen, SJ
Granneman, B
Gorodetzky, D
AF Bindschadler, Robert
Vornberger, Patricia
Fleming, Andrew
Fox, Adrian
Mullins, Jerry
Binnie, Douglas
Paulsen, Sara Jean
Granneman, Brian
Gorodetzky, David
TI The Landsat Image Mosaic of Antarctica
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Landsat; Antarctica; Ice sheet
ID BIDIRECTIONAL REFLECTANCE; SNOW
AB The Landsat Image Mosaic of Antarctica (LIMA) is the first true-color, high-spatial-resolution image of the seventh continent. It is constructed from nearly 1100 individually selected Landsat-7 ETM+ scenes. Each image was orthorectified and adjusted for geometric, sensor and illumination variations to a standardized, almost seamless surface reflectance product. Mosaicing to avoid clouds produced a high quality, nearly cloud-free benchmark data set of Antarctica for the International Polar Year from images collected primarily during 1999-2003. Multiple color composites and enhancements were generated to illustrate additional characteristics of the multispectral data including: the true appearance of the surface: discrimination between snow and bare ice; reflectance variations within bright snow; recovered reflectance values in regions of sensor saturation; and subtle topographic variations associated with ice flow. LIMA is viewable and individual scenes or user defined portions of the mosaic are downloadable at http://Iima.usgs.gov. Educational materials associated with LIMA are available at http://Iima.nasa.gov. Published by Elsevier Inc.
C1 [Bindschadler, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fleming, Andrew; Fox, Adrian] British Antarctic Survey, Cambridge, England.
RP Bindschadler, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Robert.A.Bindschadler@nasa.gov
FU National Science Foundation [0541544, 0233246H]; British Antarctic
Survey
FX This project was supported by the National Science Foundation through
grants #0541544 to NASA and #0233246H to USGS and by the British
Antarctic Survey. It is regarded as a major benchmark data set of the
International Polar Year.
NR 8
TC 70
Z9 72
U1 1
U2 12
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 DEC 15
PY 2008
VL 112
IS 12
BP 4214
EP 4226
DI 10.1016/j.rse.2008.07.006
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 373AD
UT WOS:000260942500004
ER
PT J
AU Ganguly, S
Samanta, A
Schull, MA
Shabanov, NV
Milesi, C
Nemani, RR
Knyazikhin, Y
Myneni, RB
AF Ganguly, Sangram
Samanta, Arindam
Schull, Mitchell A.
Shabanov, Nikolay V.
Milesi, Cristina
Nemani, Ramakrishna R.
Knyazikhin, Yuri
Myneni, Ranga B.
TI Generating vegetation leaf area index Earth system data record from
multiple sensors. Part 2: Implementation, analysis and validation
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Leaf area index; Validation; Accuracy; Climate data; Long term data
record; AVHRR LAI; MODIS LAI; CYCLOPES; Spectral invariants; Recollision
probability; Radiative transfer; Scaling; Single scattering albedo; Data
uncertainties
ID CYCLOPES GLOBAL PRODUCTS; LAND-SURFACE; PHOTOSYNTHETIC TRENDS;
SPOT-VEGETATION; SATELLITE DATA; AFRICAN SAHEL; WHITE SPRUCE; LAI
PRODUCTS; NDVI DATA; MODIS
AB The evaluation of a new global monthly leaf area index (LAI) data set for the period July 1981 to December 2006 derived from AVHRR Normalized Difference Vegetation Index (NDVI) data is described. The physically based algorithm is detailed in the first of the two part series. Here, the implementation, production and evaluation of the data set are described. The data set is evaluated both by direct comparisons to ground data and indirectly through inter-comparisons with similar data sets. This indirect validation showed satisfactory agreement with existing LAI products, importantly MODIS, at a range of spatial scales, and significant correlations with key climate variables in areas where temperature and precipitation limit plant growth. The data set successfully reproduced well-documented spatio-temporal trends and inter-annual variations in vegetation activity in the northern latitudes and semi-arid tropics. Comparison with plot scale field measurements over homogeneous vegetation patches indicated a 7% underestimation when all major vegetation types are taken into account. The error in mean values obtained from distributions of AVHRR LAI and high-resolution field LAI maps for different biomes is within 0.5 LAI for six out of the ten selected sites. These validation exercises though limited by the amount of field data, and thus less than comprehensive, indicated satisfactory agreement between the LAI product and field measurements. Overall, the inter-comparison with short-term LAI data sets, evaluation of long term trends with known variations in climate variables, and validation with field measurements together build confidence in the utility of this new 26 year LAI record for long term vegetation monitoring and modeling studies. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Ganguly, Sangram; Samanta, Arindam; Schull, Mitchell A.; Knyazikhin, Yuri; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Shabanov, Nikolay V.] NOAA NEDIS, Camp Springs, MD 20746 USA.
[Milesi, Cristina; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Ecosyst Sci & Technol Branch, Moffett Field, CA 94035 USA.
RP Ganguly, S (reprint author), Boston Univ, Dept Geog & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA.
EM sganguly@bu.edu
RI Schull, Mitch/D-1663-2010; Samanta, Arindam/B-9550-2009; Myneni,
Ranga/F-5129-2012
FU NASA Earth Science Enterprise
FX This research was funded by NASA Earth Science Enterprise. We thank Dr.
C. J. Tucker of NASA GSFC for making the GIMMS NDVI data available.
NR 64
TC 52
Z9 60
U1 2
U2 33
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 DEC 15
PY 2008
VL 112
IS 12
BP 4318
EP 4332
DI 10.1016/j.rse.2008.07.013
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 373AD
UT WOS:000260942500011
ER
PT J
AU Ganguly, S
Schull, MA
Samanta, A
Shabanov, NV
Milesi, C
Nemani, RR
Knyazikhin, Y
Myneni, RB
AF Ganguly, Sangram
Schull, Mitchell A.
Samanta, Arindam
Shabanov, Nikolay V.
Milesi, Cristina
Nemani, Ramakrishna R.
Knyazikhin, Yuri
Myneni, Ranga B.
TI Generating vegetation leaf area index earth system data record from
multiple sensors. Part 1: Theory
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Leaf area index; Spectral invariant; Recollision probability; Radiative
transfer; Long-term data record; AVHRR; MODIS; Scaling; Single
scattering albedo; Data uncertainties
ID SPECTRAL INVARIANTS; RADIATIVE-TRANSFER; SATELLITE DATA; MODIS DATA;
NDVI DATA; CANOPY; ALGORITHM; MODEL; LAI; PARAMETERIZATION
AB The generation of multi-decade long Earth System Data Records (ESDRs) of Leaf Area Index (LAI) and Fraction of Photosynthetically Active Radiation absorbed by vegetation (FPAR) from remote sensing measurements of multiple sensors is key to monitoring long-term changes in vegetation due to natural and anthropogenic influences. Challenges in developing such ESDRs include problems in remote sensing science (modeling of variability in global vegetation, scaling, atmospheric correction) and sensor hardware (differences in spatial resolution, spectral bands, calibration, and information content). In this paper, we develop a physically based approach for deriving LAI and FPAR products from the Advanced Very High Resolution Radiometer (AVHRR) data that are of comparable quality to the Moderate resolution Imaging Spectroradiometer (MODIS) LAI and FPAR products, thus realizing the objective of producing a long (multi-decadal) time series of these products. The approach is based on the radiative transfer theory of canopy spectral invariants which facilitates parameterization of the canopy spectral bidirectional reflectance factor (BRF). The methodology permits decoupling of the structural and radiometric components and obeys the energy conservation law. The approach is applicable to any optical sensor, however, it requires selection of sensor-specific values of configurable parameters, namely, the single scattering albedo and data uncertainty. According to the theory of spectral invariants, the single scattering albedo is a function of the spatial scale, and thus, accounts for the variation in BRF with sensor spatial resolution. Likewise, the single scattering albedo accounts for the variation in spectral BRF with sensor bandwidths. The second adjustable parameter is data uncertainty. which accounts for varying information content of the remote sensing measurements, i.e., Normalized Difference Vegetation Index (NDVI, low information content), vs. spectral BRF (higher information content). Implementation of this approach indicates good consistency in LAI values retrieved from NDVI (AVHRR-mode) and spectral BRF (MODIS-mode). Specific details of the implementation and evaluation of the derived products are detailed in the second part of this two-paper series. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Ganguly, Sangram; Schull, Mitchell A.; Samanta, Arindam; Knyazikhin, Yuri; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Shabanov, Nikolay V.] NOAA NESDIS, Camp Springs, MD 20746 USA.
[Milesi, Cristina; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Ecosyst Sci & Technol Branch, Moffett Field, CA 94035 USA.
RP Ganguly, S (reprint author), Boston Univ, Dept Geog & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA.
EM sganguly@bu.edu
RI Schull, Mitch/D-1663-2010; Samanta, Arindam/B-9550-2009; ganguly,
sangram/B-5108-2010; Myneni, Ranga/F-5129-2012
FU NASA Earth Science Enterprise
FX This research was funded by NASA Earth Science Enterprise. We thank Dr.
C. J. Tucker of NASA GSFC for making the GIMMS NDVI data available.
NR 50
TC 67
Z9 75
U1 1
U2 28
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 DEC 15
PY 2008
VL 112
IS 12
BP 4333
EP 4343
DI 10.1016/j.rse.2008.07.014
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 373AD
UT WOS:000260942500012
ER
PT J
AU Li, LM
Gierasch, PJ
Achterberg, RK
Conrath, BJ
Flasar, FM
Vasavada, AR
Ingersoll, AP
Banfield, D
Simon-Miller, AA
Fletcher, LN
AF Li Liming
Gierasch, Peter J.
Achterberg, Richard K.
Conrath, Barney J.
Flasar, F. Michael
Vasavada, Ashwin R.
Ingersoll, Andrew P.
Banfield, Don
Simon-Miller, Amy A.
Fletcher, Leigh N.
TI Strong jet and a new thermal wave in Saturn's equatorial stratosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; CLOUD LEVEL; UPPER TROPOSPHERE; ROTATION
PERIOD; ATMOSPHERE; JUPITER; TEMPERATURES; SYSTEM; SPOTS; FIELD
AB The strong jet, with a speed between 500 and 600 m/s, is inferred in the equatorial region of Saturn by combining the nadir and limb observations of Composite Infrared Spectrometer (CIRS) aboard the Cassini spacecraft. A similar jet was discovered on Jupiter (F. M. Flasar et al., 2004a). These discoveries raise the possibility that intense jets are common in the equatorial stratospheres of giant planets. An equatorial wave with wavenumber similar to 9 is revealed in the stratosphere of Saturn by the CIRS high spatial-resolution thermal maps. Our discussion based on the phase velocity suggests that the equatorial wave is probably a Rossby-gravity wave. The discovery of an equatorial wave in the stratosphere suggests that Saturn's equatorial oscillations (T. Fouchet et al., 2008; G. S. Orton et al., 2008) may be driven by vertically propagating waves, the same mechanism that drives the quasi-biennial oscillation (QBO) on Earth.
C1 [Li Liming; Gierasch, Peter J.; Conrath, Barney J.; Banfield, Don] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Achterberg, Richard K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Flasar, F. Michael; Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Vasavada, Ashwin R.; Fletcher, Leigh N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ingersoll, Andrew P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Li, LM (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM liming@astro.cornell.edu
RI Fletcher, Leigh/D-6093-2011; Flasar, F Michael/C-8509-2012; Simon,
Amy/C-8020-2012;
OI Fletcher, Leigh/0000-0001-5834-9588; Simon, Amy/0000-0003-4641-6186;
Banfield, Don/0000-0003-2664-0164
NR 31
TC 5
Z9 5
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 13
PY 2008
VL 35
IS 23
AR L23208
DI 10.1029/2008GL035515
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 383JG
UT WOS:000261669300002
ER
PT J
AU Lau, KM
Zhou, YP
Wu, HT
AF Lau, K. -M.
Zhou, Y. P.
Wu, H. -T.
TI Have tropical cyclones been feeding more extreme rainfall?
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID WESTERN NORTH PACIFIC; ATLANTIC HURRICANE SEASON; GLOBAL CLIMATE-CHANGE;
UNITED-STATES; INTERANNUAL VARIABILITY; CLIMATOLOGICAL RAINFALL; SURFACE
TEMPERATURE; STRONG ASSOCIATION; AFRICAN RAINFALL; EL-NINO
AB We have conducted a study of the relationship between tropical cyclone (TC) and extreme rain events using GPCP and TRMM rainfall data, and storm track data for July through November (JASON) in the North Atlantic (NAT) and the western North Pacific (WNP). Extreme rain events are defined in terms of percentile rainrate, and TC-rain by rainfall associated with a named TC. Results show that climatologically, 8% of rain events and 17% of the total rain amount in NAT are accounted by TCs, compared to 9% of rain events, and 21% of rain amount in WNP. The fractional contribution of accumulated TC-rain to total rain, Omega, increases nearly linearly as a function of rainrate. Extending the analyses using GPCP pentad data for 1979-2005, and for the post-SSM/I period (1988-2005), we find that while there is no significant trend in the total JASON rainfall over NAT or WNP, there is a positive significant trend in heavy rain over both basins for the 1979-2005 period, but not for the post-SSM/I period. Trend analyses of Omega for both periods indicate that TCs have been feeding increasingly more to rainfall extremes in NAT, where the expansion of the warm pool area can explain slightly more than 50% of the change in observed trend in total TC rainfall. In WNP, trend signals for Omega are mixed, and the long-term relationship between TC rain and warm pool area is strongly influenced by interannual and interdecadal variability.
C1 [Lau, K. -M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Zhou, Y. P.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Catonsville, MD USA.
[Wu, H. -T.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Lau, KM (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613, Greenbelt, MD 20771 USA.
EM william.k.lau@nasa.gov; yaping.zhou-1@nasa.gov;
hueytzu.wu-1@mail.nasa.gov
RI Lau, William /E-1510-2012
OI Lau, William /0000-0002-3587-3691
FU Precipitation Measuring Mission, NASA Earth Science Division
FX This work is supported by the Precipitation Measuring Mission
(Headquarter Manager: Dr. R. Kakar), NASA Earth Science Division. We
thank Dr. Chris Landsea and two anonymous reviewers for constructive
comments that have improved the manuscript.
NR 54
TC 32
Z9 32
U1 0
U2 4
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 DEC 13
PY 2008
VL 113
IS D23
AR D23113
DI 10.1029/2008JD009963
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 383KE
UT WOS:000261671700002
ER
PT J
AU Matsoukas, C
Banks, AC
Pavlakis, KG
Hatzianastassiou, N
Stackhouse, PW
Vardavas, I
AF Matsoukas, C.
Banks, A. C.
Pavlakis, K. G.
Hatzianastassiou, N.
Stackhouse, P. W., Jr.
Vardavas, I.
TI Reply to comment by Kara and Barron on "Seasonal heat budgets of the Red
and Black seas''
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Editorial Material
ID GLOBAL DISTRIBUTION; RADIATION BUDGET; MODEL
C1 [Matsoukas, C.] Univ Aegean, Dept Environm, GR-81100 Mitilini, Greece.
[Banks, A. C.] Hellen Ctr Marine Res, GR-71003 Iraklion, Greece.
[Hatzianastassiou, N.] Univ Ioannina, Dept Phys, Lab Meteorol, GR-45110 Ioannina, Greece.
[Pavlakis, K. G.] Technol Educ Inst Crete, Dept Gen Appl Sci, GR-71110 Iraklion, Greece.
[Stackhouse, P. W., Jr.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Vardavas, I.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
RP Matsoukas, C (reprint author), Univ Aegean, Dept Environm, Xenia Bldg,Univ Hill, GR-81100 Mitilini, Greece.
EM matsoukas@aegean.gr
RI Vardavas, Ilias/G-7310-2011
NR 13
TC 0
Z9 0
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD DEC 13
PY 2008
VL 113
IS C12
AR C12009
DI 10.1029/2008JC004917
PG 3
WC Oceanography
SC Oceanography
GA 383KX
UT WOS:000261673600004
ER
PT J
AU Hong, G
Yang, P
Minnis, P
Hu, YX
North, G
AF Hong, Gang
Yang, Ping
Minnis, Patrick
Hu, Yong X.
North, Gerald
TI Do contrails significantly reduce daily temperature range?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID UNITED-STATES; CLIMATE; CIRRUS; WEATHER; CLOUDS; TRENDS; IMPACT; CLEAR
AB One of the most visible anthropogenic phenomena in the atmosphere is the occurrence of contrails. The direct effects of contrails on surface temperature are investigated on the basis of the data sets for the cloud cover and surface temperature over the conterminous United States for the period 1971-2001. It is shown that the increase of the average daily temperature range (DTR) over the United States during the three-day grounding period of 11-14 September 2001 cannot be attributed to the absence of contrails, a subject was debated in several previous studies. The present analysis suggests that the DTR is attributed to the change of low cloudiness. Citation: Hong, G., P. Yang, P. Minnis, Y. X. Hu, and G. North (2008), Do contrails significantly reduce daily temperature range?, Geophys. Res. Lett., 35, L23815, doi:10.1029/2008GL036108.
C1 [Hong, Gang; Yang, Ping; North, Gerald] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Minnis, Patrick; Hu, Yong X.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Hong, G (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM hong@ariel.met.tamu.edu
RI Minnis, Patrick/G-1902-2010; Yang, Ping/B-4590-2011; North,
Gerald/G-1019-2011; Hong, Gang/A-2323-2012; Hu, Yongxiang/K-4426-2012
OI Minnis, Patrick/0000-0002-4733-6148;
FU U.S.Department of Transportation; Volpe National Transportation System
Center [DTRT57-08-C-10005]; National Science Foundation [ATM-0239605]
FX This study is partly supported by U.S.Department of Transportation (DOT)
Volpe National Transportation System Center under contract
DTRT57-08-C-10005 managed by Mohan Gupta and the National Science
Foundation under ATM-0239605 managed by Bradley Smull. ECMWF ERA-40 data
used in this study/project have been provided by ECMWF/ have been
obtained from the ECMWF Data Server. The ISCCP D1 data were obtained
from the International Satellite Cloud Climatology Project web site
http:// isccp.giss.nasa.gov maintained by the ISCCP research group at
the NASA Goddard Institute for Space Studies, New York, NY on January,
2005. Data set 3200 (DSI-3200) was obtained from National Climatic Data
Center, Asheville, NC. G. Hong gratefully thanks W. Spangler at
NCAR/CISL/DSS for accessing the data set DSI3200. We also thank the two
reviewers for their constructive comments.
NR 17
TC 6
Z9 8
U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 12
PY 2008
VL 35
IS 23
AR L23815
DI 10.1029/2008GL036108
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 383JD
UT WOS:000261669000004
ER
PT J
AU Briggs, RW
Sieh, K
Amidon, WH
Galetzka, J
Prayudi, D
Suprihanto, I
Sastra, N
Suwargadi, B
Natawidjaja, D
Farr, TG
AF Briggs, Richard W.
Sieh, Kerry
Amidon, William H.
Galetzka, John
Prayudi, Dudi
Suprihanto, Imam
Sastra, Nugraha
Suwargadi, Bambang
Natawidjaja, Danny
Farr, Thomas G.
TI Persistent elastic behavior above a megathrust rupture patch: Nias
island, West Sumatra
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID CASCADIA SUBDUCTION ZONE; SEA-LEVEL CHANGES; 1964 ALASKA EARTHQUAKE;
MALAY-THAI PENINSULA; SIMEULUE EARTHQUAKE; CRUSTAL DEFORMATION;
SOUTHWEST JAPAN; COASTAL DEFORMATION; ANDAMAN EARTHQUAKE; TECTONIC
MOVEMENTS
AB We quantify fore-arc deformation using fossil reefs to test the assumption commonly made in seismic cycle models that anelastic deformation of the fore arc is negligible. Elevated coral microatolls, paleoreef flats, and chenier plains show that the Sumatran outer arc island of Nias has experienced a complex pattern of relatively slow long-term uplift and subsidence during the Holocene epoch. This same island rose up to 2.9 m during the M-w 8.7 Sunda megathrust rupture in 2005. The mismatch between the 2005 and Holocene uplift patterns, along with the overall low rates of Holocene deformation, reflects the dominance of elastic strain accumulation and release along this section of the Sunda outer arc high and the relatively subordinate role of upper plate deformation in accommodating long-term plate convergence. The fraction of 2005 uplift that will be retained permanently is generally <4% for sites that experienced more than 0.25 m of coseismic uplift. Average uplift rates since the mid-Holocene range from 1.5 to -0.2 mm/a and are highest on the eastern coast of Nias, where coseismic uplift was nearly zero in 2005. The pattern of long-term uplift and subsidence is consistent with slow deformation of Nias along closely spaced folds in the north and trenchward dipping back thrusts in the southeast. Low Holocene tectonic uplift rates provide for excellent geomorphic and stratigraphic preservation of the mid-Holocene relative sea level high, which was under way by similar to 7.3 ka and persisted until similar to 2 ka.
C1 [Briggs, Richard W.; Sieh, Kerry; Amidon, William H.; Galetzka, John] CALTECH, Div Geol & Planetary Sci, Tecton Observ, Pasadena, CA 91125 USA.
[Farr, Thomas G.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Prayudi, Dudi; Sastra, Nugraha; Suwargadi, Bambang; Natawidjaja, Danny] Indonesian Inst Sci, Res Ctr Geotechnol, Bandung 40135, Indonesia.
RP Briggs, RW (reprint author), US Geol Survey, Geol Hazards Team, MS 966,Box 25046, Golden, CO 80225 USA.
EM rbriggs@usgs.gov
RI Briggs, Richard/A-1348-2013;
OI Briggs, Richard/0000-0001-8108-0046; Farr, Thomas/0000-0001-5406-2096
FU NSF [EAR-0610078]; Gordon and Betty Moore Foundation
FX We thank the Captain and crew of the Mentawai Indah. Thanks to Hong-Wei
Chiang and Larry Edwards for the U-Th dates. Dick Peltier and Rosemarie
Drummond kindly provided predictions from the ICE-5G (VM2) model, and
Aron Meltzner generously provided tide model calculations. We benefited
greatly from discussions with Mike Gagan, Jean-Philippe Avouac, Glenn
Milne, Chris Goldfinger, Harvey Kelsey, Ben Horton, and Heidrun Kopp. We
also thank Daniel Melnick, Alan Nelson, two anonymous reviewers, and
Associate Editor Greg Moore for their reviews and discussion of our
manuscript. This work was supported by NSF (EAR-0610078) and a grant
from the Gordon and Betty Moore Foundation. This is Caltech Tectonics
Observatory contribution 80.
NR 94
TC 19
Z9 19
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD DEC 12
PY 2008
VL 113
IS B12
AR B12406
DI 10.1029/2008JB005684
PG 28
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 383QK
UT WOS:000261688200001
ER
PT J
AU Wilson, JW
Ott, CM
Quick, L
Davis, R
Bentrup, KHZ
Crabbe, A
Richter, E
Sarker, S
Barrila, J
Porwollik, S
Cheng, P
McClelland, M
Tsaprailis, G
Radabaugh, T
Hunt, A
Shah, M
Nelman-Gonzalez, M
Hing, S
Parra, M
Dumars, P
Norwood, K
Bober, R
Devich, J
Ruggles, A
CdeBaca, A
Narayan, S
Benjamin, J
Goulart, C
Rupert, M
Catella, L
Schurr, MJ
Buchanan, K
Morici, L
McCracken, J
Porter, MD
Pierson, DL
Smith, SM
Mergeay, M
Leys, N
Stefanyshyn-Piper, HM
Gorie, D
Nickerson, CA
AF Wilson, James W.
Ott, C. Mark
Quick, Laura
Davis, Richard
Bentrup, Kerstin Hoener zu
Crabbe, Aurelie
Richter, Emily
Sarker, Shameema
Barrila, Jennifer
Porwollik, Steffen
Cheng, Pui
McClelland, Michael
Tsaprailis, George
Radabaugh, Timothy
Hunt, Andrea
Shah, Miti
Nelman-Gonzalez, Mayra
Hing, Steve
Parra, Macarena
Dumars, Paula
Norwood, Kelly
Bober, Ramona
Devich, Jennifer
Ruggles, Ashleigh
CdeBaca, Autumn
Narayan, Satro
Benjamin, Joseph
Goulart, Carla
Rupert, Mark
Catella, Luke
Schurr, Michael J.
Buchanan, Kent
Morici, Lisa
McCracken, James
Porter, Marc D.
Pierson, Duane L.
Smith, Scott M.
Mergeay, Max
Leys, Natalie
Stefanyshyn-Piper, Heidemarie M.
Gorie, Dominic
Nickerson, Cheryl A.
TI Media Ion Composition Controls Regulatory and Virulence Response of
Salmonella in Spaceflight
SO PLOS ONE
LA English
DT Article
AB The spaceflight environment is relevant to conditions encountered by pathogens during the course of infection and induces novel changes in microbial pathogenesis not observed using conventional methods. It is unclear how microbial cells sense spaceflight-associated changes to their growth environment and orchestrate corresponding changes in molecular and physiological phenotypes relevant to the infection process. Here we report that spaceflight-induced increases in Salmonella virulence are regulated by media ion composition, and that phosphate ion is sufficient to alter related pathogenesis responses in a spaceflight analogue model. Using whole genome microarray and proteomic analyses from two independent Space Shuttle missions, we identified evolutionarily conserved molecular pathways in Salmonella that respond to spaceflight under all media compositions tested. Identification of conserved regulatory paradigms opens new avenues to control microbial responses during the infection process and holds promise to provide an improved understanding of human health and disease on Earth.
C1 [Quick, Laura; Davis, Richard; Crabbe, Aurelie; Richter, Emily; Sarker, Shameema; Barrila, Jennifer; Nickerson, Cheryl A.] Arizona State Univ, Ctr Infect Dis & Vaccinol, Biodesign Inst, Tempe, AZ 85287 USA.
[Wilson, James W.; Quick, Laura] Villanova Univ, Dept Biol, Villanova, PA 19085 USA.
[Ott, C. Mark; Pierson, Duane L.] NASA, Johnson Space Center, Habitabil & Environm Factors Div, Houston, TX USA.
[Bentrup, Kerstin Hoener zu; Morici, Lisa] Tulane Univ, Hlth Sci Ctr, New Orleans, LA 70118 USA.
[Crabbe, Aurelie] Free Univ Brussels, Flanders Inst Biotechnol, B-1050 Brussels, Belgium.
[Crabbe, Aurelie; Mergeay, Max; Leys, Natalie] Belgian Nuclear Res Ctr, Mol, Belgium.
[Porwollik, Steffen; Cheng, Pui; McClelland, Michael] Sidney Kimmel Canc Ctr, San Diego, CA USA.
[Tsaprailis, George; Radabaugh, Timothy; Hunt, Andrea] Univ Arizona, Ctr Toxicol, Tucson, AZ 85721 USA.
[Shah, Miti] Arizona State Univ, Ctr Glycosci Technol, Biodesign Inst, Tempe, AZ 85287 USA.
[Nelman-Gonzalez, Mayra] Wyle Lab, Houston, TX USA.
[Hing, Steve; Parra, Macarena; Dumars, Paula] NASA, Ames Res Ctr, Moffett Field, CA USA.
[Norwood, Kelly; Bober, Ramona; Devich, Jennifer; Ruggles, Ashleigh; CdeBaca, Autumn; Narayan, Satro; Benjamin, Joseph; Catella, Luke] Kennedy Space Ctr, Space Life Sci Lab, Cape Canaveral, FL USA.
[Goulart, Carla; Rupert, Mark] Univ Colorado, Boulder, CO 80309 USA.
[Schurr, Michael J.] Univ Colorado, Sch Med, Aurora, CO USA.
[Buchanan, Kent] Oklahoma City Univ, Oklahoma City, OK USA.
[McCracken, James] Univ Chicago, Sect Gen Surg, Chicago, IL 60637 USA.
[Porter, Marc D.] Univ Utah, Dept Chem, Chem Engn & Bioengn, Salt Lake City, UT 84112 USA.
[Smith, Scott M.] Natl Aeronaut & Space Adm, Johnson Space Ctr, Human Adapt & Countermeasures Div, Houston, TX USA.
[Stefanyshyn-Piper, Heidemarie M.; Gorie, Dominic] NASA, Johnson Space Ctr, Astronaut Office, Houston, TX USA.
RP Wilson, JW (reprint author), Arizona State Univ, Ctr Infect Dis & Vaccinol, Biodesign Inst, Tempe, AZ 85287 USA.
EM Cheryl.A.Nickerson@asu.edu
RI McClelland, Michael/A-8583-2011; Mergeay, Max/H-2003-2011;
OI McClelland, Michael/0000-0003-1788-9347
FU NASA [NCC2-1362]; NIEHS [ES06694]; NIH/NCI [CA023074]; BIO5 Institute of
the University of Arizona; King Baudouin Foundation [Henri Benedictus
Fellowship]; Belgian American Educational Foundation
FX This work was supported by NASA grant NCC2-1362 to CAN; Arizona
Proteomics Consortium supported by NIEHS grant ES06694 to the SWEHSC,
NIH/NCI grant CA023074 to the AZCC, and by the BIO5 Institute of the
University of Arizona; AC supported by Henri Benedictus Fellowship of
the King Baudouin Foundation and the Belgian American Educational
Foundation (B.A.E.F.). The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 33
TC 47
Z9 53
U1 0
U2 20
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD DEC 12
PY 2008
VL 3
IS 12
AR e3923
DI 10.1371/journal.pone.0003923
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 436ZW
UT WOS:000265456300003
PM 19079590
ER
PT J
AU Huang, J
Minnis, P
Chen, B
Huang, ZW
Liu, ZY
Zhao, QY
Yi, YH
Ayers, JK
AF Huang, Jianping
Minnis, Patrick
Chen, Bin
Huang, Zhongwei
Liu, Zhaoyan
Zhao, Qingyun
Yi, Yuhong
Ayers, J. Kirk
TI Long-range transport and vertical structure of Asian dust from CALIPSO
and surface measurements during PACDEX
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID APRIL 1998; LIDAR OBSERVATIONS; LOESS PLATEAU; MINERAL DUST; SAHARAN
DUST; EAST-ASIA; AEROSOLS; CLIMATE; NETWORK; EVENTS
AB Knowledge of long-range transport and vertical distribution of Asian dust aerosols in the free troposphere is important for estimating their impact on climate. Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO), surface micropulse lidar (MPL), and standard surface measurements are used to directly observe the long-range transport and vertical distribution of Asian dust aerosols in the free troposphere during the Pacific Dust Experiment (PACDEX). The MPL measurements were made at the Loess Plateau (35.95 degrees N, 104.1 degrees E) near the major dust source regions of the Taklamakan and Gobi deserts. Dust events are more frequent in the Taklamakan, where floating dust dominates, while more intensive, less frequent dust storms are more common in the Gobi region. The vertical distribution of the CALIPSO backscattering/depolarization ratios indicate that nonspherically shaped dust aerosols floated from near the ground to an altitude of approximately 9 km around the source regions. This suggests the possible long-range transport of entrained dust aerosols via upper tropospheric westerly jets. A very distinct large depolarization layer was also identified between 8 and 10 km over eastern China and the western Pacific Ocean corresponding to dust aerosols transported from the Taklamakan and Gobi areas, as confirmed by back trajectory analyses. The combination of these dust sources results in a two-layer or multilayered dust structure over eastern China and the western Pacific Ocean.
C1 [Huang, Jianping; Chen, Bin; Huang, Zhongwei] Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China.
[Yi, Yuhong; Ayers, J. Kirk] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Liu, Zhaoyan] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23666 USA.
[Zhao, Qingyun] Gansu Meteorol Bur, Lanzhou 730000, Peoples R China.
RP Huang, J (reprint author), Lanzhou Univ, Coll Atmospher Sci, Lanzhou 730000, Peoples R China.
EM hjp@lzu.edu.cn
RI Liu, Zhaoyan/A-9604-2009; Liu, Zhaoyan/B-1783-2010; Minnis,
Patrick/G-1902-2010; Huang, Zhongwei/K-5484-2013
OI Liu, Zhaoyan/0000-0003-4996-5738; Minnis, Patrick/0000-0002-4733-6148;
FU National Science Foundation of China [40628005, 40633017]; NASA Science
Mission Directorate
FX This research is supported by National Science Foundation of China under
grants 40628005 and 40633017 and the NASA Science Mission Directorate
through the CALIPSO Project and the Radiation Sciences Program. The
CALIPSO data were obtained from the NASA Langley Atmospheric Science
Data Center (ASDC).
NR 42
TC 123
Z9 139
U1 9
U2 29
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 DEC 11
PY 2008
VL 113
IS D23
AR D23212
DI 10.1029/2008JD010620
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 383JQ
UT WOS:000261670300003
ER
PT J
AU Xi, DJ
Zhang, H
Furst, S
Chen, B
Pei, QB
AF Xi, Dongjuan
Zhang, Han
Furst, Stephen
Chen, Bin
Pei, Qibing
TI Electrochemical Synthesis and Photovoltaic Property of Cadmium
Sulfide-Polybithiophene Interdigitated Nanohybrid Thin Films
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Article
ID HYBRID SOLAR-CELLS; BULK-HETEROJUNCTION; CONJUGATED-POLYMER;
POLYTHIOPHENE FILMS; MESOPOROUS TITANIA; CONTROLLED GROWTH;
NANOCRYSTALS; RAMAN; NANOPARTICLES; COMPOSITES
AB Interdigitated hybrid films consisting of cadmium sulfide (CdS) nanorod arrays and interpenetrating polybithiophene have been synthesized by electrochemical depositions. The vertically aligned CdS nanorods were self-assembled on gold-coated glass substrates through a simple cathodic process of an electrolyte solution containing cadmium sulfate and potassium thiocyanate, without the use of any templates. The conjugated polymer polybithiophene was deposited into the nanorod arrays by in situ electrochemical polymerization. The resulting interdigitated nanohybrid films showed dense packing of the polymer in the nanorod arrays with a filling ratio estimated to be 76%. Raman spectroscopy and Fourier transform infrared revealed charge-transfer between the polymer and the CdS nanorods, consistent with the high filling ratio and improved polymer-CdS interface. Solar cells based on these hybrid films with vapor-deposited aluminum cathode exhibited a diode characteristic with a rectification ratio of 10(3) at +/- 1 V. The measured open-circuit voltage was 0.84 V, and the short-circuit current was 0.52 mA/cm(2). The overall power conversion efficiency was 0.38%.
C1 [Xi, Dongjuan; Zhang, Han; Pei, Qibing] Univ Calif Los Angeles, Dept Mat Sci & Engn, Henry Samueli Sch Engn & Appl Sci, Los Angeles, CA 90095 USA.
[Furst, Stephen] N Carolina State Univ, NASA, Dept Elect Engn, Space Program, Moffett Field, CA 94035 USA.
[Chen, Bin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Pei, QB (reprint author), Univ Calif Los Angeles, Dept Mat Sci & Engn, Henry Samueli Sch Engn & Appl Sci, Los Angeles, CA 90095 USA.
EM qpei@seas.ucla.edu
RI Pei, Qibing/N-7497-2015
FU National Science Foundation [0507294]; Defense Threat Reduction Agency
[HDTRA1-07-1-0028]
FX The authors would like to thank Dr. Haizheng Zhong for valuable
discussions. This work is financially supported by the National Science
Foundation under Grant No. 0507294 and the Defense Threat Reduction
Agency Grant No. HDTRA1-07-1-0028.
NR 52
TC 19
Z9 21
U1 2
U2 18
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1932-7447
J9 J PHYS CHEM C
JI J. Phys. Chem. C
PD DEC 11
PY 2008
VL 112
IS 49
BP 19765
EP 19769
DI 10.1021/jp807868j
PG 5
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA 379WJ
UT WOS:000261426600085
ER
PT J
AU Perera, TA
Chapin, EL
Austermann, JE
Scott, KS
Wilson, GW
Halpern, M
Pope, A
Scott, D
Yun, MS
Lowenthal, JD
Morrison, G
Aretxaga, I
Bock, JJ
Coppin, K
Crowe, M
Frey, L
Hughes, DH
Kang, Y
Kim, S
Mauskopf, PD
AF Perera, T. A.
Chapin, E. L.
Austermann, J. E.
Scott, K. S.
Wilson, G. W.
Halpern, M.
Pope, A.
Scott, D.
Yun, M. S.
Lowenthal, J. D.
Morrison, G.
Aretxaga, I.
Bock, J. J.
Coppin, K.
Crowe, M.
Frey, L.
Hughes, D. H.
Kang, Y.
Kim, S.
Mauskopf, P. D.
TI An AzTEC 1.1 mm survey of the GOODS-N field - I. Maps, catalogue and
source statistics
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE instrumentation: detectors; galaxies: high redshift; galaxies:
starburst; submillimetre
ID DEGREE EXTRAGALACTIC SURVEY; SCUBA SUPER-MAP; DEEP SUBMILLIMETER SURVEY;
1200-MU-M MAMBO SURVEY; NUMBER COUNTS; HIGH-REDSHIFT; LOCKMAN HOLE;
COSMOS FIELD; GALAXIES; NORTH
AB We have conducted a deep and uniform 1.1 mm survey of the Great Observatories Origins Deep Survey-North (GOODS-N) field with AzTEC on the James Clerk Maxwell Telescope. Here, we present the first results from this survey including maps, the source catalogue and 1.1 mm number counts. The results presented here were obtained from a 245 arcmin(2) region with a near uniform coverage to a depth of 0.96-1.16 mJy beam(-1). Our robust catalogue contains 28 source candidates detected with S/N >= 3.75, only similar to 1-2 of which are expected to be spurious detections. Of these source candidates, eight are also detected by Submillimetre Common-User Bolometer Array ( SCUBA) at 850 mu m in regions where there is a good overlap between the two surveys. The major advantage of our survey over that with SCUBA is the uniformity of coverage. We calculate number counts using two different techniques: the first using a frequentist parameter estimation and the second using a Bayesian method. The two sets of results are in good agreement. We find that the 1.1 mm differential number counts are well described in the 2-6 mJy range by the functional form dN/dS = N'(S'/S) exp(-S/S') with fitted parameters S' = 1.25 +/- 0.38 mJy and dN/dS = 300 +/- 90 mJy(-1) deg(-2) at 3 mJy.
C1 [Perera, T. A.; Austermann, J. E.; Scott, K. S.; Wilson, G. W.; Yun, M. S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Chapin, E. L.; Halpern, M.; Pope, A.; Scott, D.; Crowe, M.; Frey, L.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Pope, A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Lowenthal, J. D.] Smith Coll, Dept Astron, Northampton, MA 01063 USA.
[Morrison, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Morrison, G.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA.
[Aretxaga, I.; Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico.
[Bock, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Coppin, K.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Kang, Y.; Kim, S.] Sejong Univ, Dept Astron & Space Sci, Seoul, South Korea.
[Mauskopf, P. D.] Cardiff Univ, Cardiff, S Glam, Wales.
RP Perera, TA (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
EM perera@astro.umass.edu
OI Scott, Douglas/0000-0002-6878-9840
FU NSF [AST 05-40852]; Korea Science & Engineering Foundation (KOSEF);
Astrophysical Research Center of the Structure and Evolution of the
Cosmos (ARCSEC); CONACT [60878, 50786]; NASA through the Spitzer Space
Telescope Fellowship Program; Jet Propulsion Laboratory; California
Institute of Technology; Science and Technology Facilities Council;
Natural Sciences and Engineering Research Council of Canada
FX The authors are grateful to J. Aguirre, J. Karakla, K. Souccar, I.
Coulson, R. Tilanus, R. Kackley, D. Haig, S. Doyle, and the observatory
staff at the JCMT who made these observations possible. Support for this
work was provided, in part, by the NSF grant AST 05-40852 and the grant
from the Korea Science & Engineering Foundation (KOSEF) under a
cooperative Astrophysical Research Center of the Structure and Evolution
of the Cosmos (ARCSEC). DHH and IA acknowledge partial support by CONACT
from research grants 60878 and 50786. AP acknowledges support provided
by NASA 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. KC acknowledges support from
the Science and Technology Facilities Council. DS and MH acknowledge
support from the Natural Sciences and Engineering Research Council of
Canada.
NR 37
TC 86
Z9 86
U1 1
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC 11
PY 2008
VL 391
IS 3
BP 1227
EP 1238
DI 10.1111/j.1365-2966.2008.13902.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 377QK
UT WOS:000261265500016
ER
PT J
AU Deming, D
AF Deming, Drake
TI ASTROPHYSICS Quest for a habitable world
SO NATURE
LA English
DT Editorial Material
ID EXTRASOLAR PLANET; HD 189733B; WATER; ATMOSPHERE; SPECTRUM; STAR
C1 NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Deming, D (reprint author), NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA.
EM leo.d.deming@nasa.gov
NR 11
TC 1
Z9 1
U1 0
U2 2
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD DEC 11
PY 2008
VL 456
IS 7223
BP 714
EP 715
DI 10.1038/456714a
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 381TX
UT WOS:000261559900029
PM 19079042
ER
PT J
AU Abe, K
Fuke, H
Haino, S
Hams, T
Itazaki, A
Kim, KC
Kumazawa, T
Lee, MH
Makida, Y
Matsuda, S
Matsumoto, K
Mitchell, JW
Moiseev, AA
Myers, Z
Nishimura, J
Nozaki, M
Orito, R
Ormes, JF
Sasaki, M
Seo, ES
Shikaze, Y
Streitmatter, RE
Suzuki, J
Takasugi, Y
Takeuchi, K
Tanaka, K
Yamagami, T
Yamamoto, A
Yoshida, T
Yoshimura, K
AF Abe, K.
Fuke, H.
Haino, S.
Hams, T.
Itazaki, A.
Kim, K. C.
Kumazawa, T.
Lee, M. H.
Makida, Y.
Matsuda, S.
Matsumoto, K.
Mitchell, J. W.
Moiseev, A. A.
Myers, Z.
Nishimura, J.
Nozaki, M.
Orito, R.
Ormes, J. F.
Sasaki, M.
Seo, E. S.
Shikaze, Y.
Streitmatter, R. E.
Suzuki, J.
Takasugi, Y.
Takeuchi, K.
Tanaka, K.
Yamagami, T.
Yamamoto, A.
Yoshida, T.
Yoshimura, K.
TI Measurement of the cosmic-ray low-energy antiproton spectrum with the
first BESS-Polar Antarctic flight
SO PHYSICS LETTERS B
LA English
DT Article
DE Cosmic-ray antiproton; Solar modulation; Superconducting spectrometer
ID SECONDARY ANTIPROTONS; PARTICLE ASTROPHYSICS; SOLAR MINIMUM; CURRENT
SHEET; BLACK-HOLES; SPECTROMETER; PROTON; FLUX; PROGRESS; MODEL
AB The BESS-Polar spectrometer had its first successful balloon flight over Antarctica in December 2004. During the 8.5-day long-duration flight, almost 0.9 billion events were recorded and 1,520 antiprotons were detected in the energy range 0.1-4.2 GeV. In this Letter, we report the antiproton spectrum obtained, discuss the origin of cosmic-ray antiprotons, and use antiproton data to probe the effect of charge-sign-dependent drift in the solar modulation. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Abe, K.; Itazaki, A.; Orito, R.; Shikaze, Y.; Takasugi, Y.; Takeuchi, K.] Kobe Univ, Kobe, Hyogo 6578501, Japan.
[Fuke, H.; Yamagami, T.; Yoshida, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Haino, S.; Kumazawa, T.; Makida, Y.; Matsuda, S.; Matsumoto, K.; Nozaki, M.; Suzuki, J.; Tanaka, K.; Yamamoto, A.; Yoshimura, K.] High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan.
[Hams, T.; Mitchell, J. W.; Moiseev, A. A.; Sasaki, M.; Streitmatter, R. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kim, K. C.; Lee, M. H.; Myers, Z.; Seo, E. S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[Nishimura, J.] Univ Tokyo, Bunkyo Ku, Tokyo 1130033, Japan.
[Ormes, J. F.] Univ Denver, Denver, CO 80208 USA.
[Hams, T.; Sasaki, M.] CRESST USRA, Columbia, MD 21044 USA.
RP Haino, S (reprint author), Ist Nazl Fis Nucl, I-06123 Perugia, Italy.
EM haino@post.kek.jp
OI Seo, Eun-Suk/0000-0001-8682-805X
FU ISAS/JAXA; KEK; National Science Foundation (NSF), USA; Raytheon Polar
Service Company; MEXT in Japan [KAKENHI-13001004, KAKENHI-15340077,
KAKENHI-181040006]; NASA in the USA
FX The authors thank NASA Headquarters for continuous encouragement in this
US-Japan cooperative project. Sincere thanks are expressed to the NASA
Balloon Programs Office at GSFC/WFF and to the NASA Columbia Scientific
Balloon Facility for their experienced support. They also thank
ISAS/JAXA and KEK for their continuous support and encouragement.
Special thanks go to the National Science Foundation (NSF), USA, and
Raytheon Polar Service Company for their professional support in the USA
and in Antarctica. The authors would thank the BESS-Polar II
collaborators M. Hasegawa, A. Horikoshi, K. Sakai, and N. Thakur for
their contribution to the instrument performance evaluation and further
cooperation. The BESS-Polar experiment is being carried out as a
Japan-US Collaboration. It is supported by MEXT grants
(KAKENHI-13001004, 15340077, and 181040006) in Japan, and by NASA grants
in the USA.
NR 45
TC 46
Z9 46
U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0370-2693
J9 PHYS LETT B
JI Phys. Lett. B
PD DEC 11
PY 2008
VL 670
IS 2
BP 103
EP 108
DI 10.1016/j.physletb.2008.10.053
PG 6
WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 385NJ
UT WOS:000261820600002
ER
PT J
AU Tedder, SA
Weikl, MC
Seeger, T
LeipertZ, A
AF Tedder, Sarah A.
Weikl, Markus C.
Seeger, Thomas
LeipertZ, Alfred
TI Determination of probe volume dimensions in coherent measurement
techniques
SO APPLIED OPTICS
LA English
DT Article
ID STOKES-RAMAN SCATTERING; SPECTROSCOPY; BOXCARS; FLAME
AB When investigating combustion phenomena with pump-probe techniques, the spatial resolution is given by the overlapping region of the laser beams and thus defines the probe volume size. The size of this probe volume becomes important when the length scales of interest are on the same order or smaller. We present a new approach to measure the probe volume in three dimensions, which can be used to determine the probe volume length, diameter, and shape. The optical arrangement and data evaluation are demonstrated for a dual-pump dual-broadband coherent anti-Stokes Raman scattering setup that is used for combustion diagnostics. This new approach offers a simple, quick alternative with more capabilities than formerly used probe volume measurement methods. (c) 2008 Optical Society of America.
C1 [Tedder, Sarah A.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA.
[Weikl, Markus C.; Seeger, Thomas; LeipertZ, Alfred] Lehrstuhl Tech Thermodynam, D-91058 Erlangen, Germany.
[Weikl, Markus C.; Seeger, Thomas; LeipertZ, Alfred] Erlangen Grad Sch Adv Opt Technol SAOT, D-91052 Erlangen, Germany.
RP Tedder, SA (reprint author), NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, 12 Langley Blvd, Hampton, VA 23681 USA.
EM sarah.a.tedder@nasa.gov
RI Seeger, Thomas/C-3951-2017;
OI Seeger, Thomas/0000-0002-9145-5910; Weikl, Markus/0000-0002-8570-3842
FU School in Advanced Optical Technologies (SAOT); German National Science
Foundation (DFG)
FX The authors gratefully acknowledge funding of the Erlangen Graduate
School in Advanced Optical Technologies (SAOT) by the German National
Science Foundation (DFG) in the framework of the excellence initiative.
The authors would also like to thank Greg Herring and Dimitrii Kozlov
for advice and direction regarding CARS probe volume theory.
NR 13
TC 12
Z9 12
U1 0
U2 1
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD DEC 10
PY 2008
VL 47
IS 35
BP 6601
EP 6605
DI 10.1364/AO.47.006601
PG 5
WC Optics
SC Optics
GA 391NR
UT WOS:000262240500017
PM 19079469
ER
PT J
AU Vanderveld, RA
AF Vanderveld, R. Ali
TI QUANTIFYING PARAMETER ERRORS DUE TO THE PECULIAR VELOCITIES OF TYPE Ia
SUPERNOVAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; cosmology: observations; cosmology: theory;
supernovae: general
ID HIGH-REDSHIFT SUPERNOVAE; HUBBLE-SPACE-TELESCOPE; OMEGA(LAMBDA);
CONSTRAINTS; EVOLUTION; OMEGA(M); SET
AB The fitting of the observed redshifts and magnitudes of Type Ia supernovae to what we would see in homogeneous cosmological models has led to constraints on cosmological parameters. However, in performing such fits it is assumed that the sampled supernovae are moving with the Hubble flow, or namely that their peculiar velocities are zero. In reality, peculiar velocities will modify supernova data in a way that can impact best-fit cosmological parameters. We theoretically quantify this effect in the nonlinear regime with a Monte Carlo analysis, using data from semi-analytical galaxy catalogs built from the Millennium N-body simulation. We find scaling relations for the errors in best-fit parameters resulting solely from peculiar velocities, as a function of the total number of sources in a supernova survey N and its maximum redshift zmax. For low-redshift surveys, we find that these errors can be of the same order of magnitude as the errors due to an intrinsic magnitude scatter of 0.1 mag. For a survey with N = 2000 and z(max) = 1.7, we estimate that the expected peculiar velocity-induced errors in the best-fit cosmological constant density and equation of state can be sigma(Lambda) approximate to 0.009 and sigma(w) approximate to 0.01, respectively, which are subdominant to the errors due to the intrinsic scatter. We further find that throwing away supernova data below a redshift z approximate to 0.01-0.02 can reduce the combined error due to peculiar velocities and the intrinsic scatter, but by only about 10%.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Vanderveld, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM rav@caltech.edu
NR 15
TC 3
Z9 3
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2008
VL 689
IS 1
BP 49
EP 52
DI 10.1086/592396
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 401GV
UT WOS:000262929000003
ER
PT J
AU Graff, PB
Georganopoulos, M
Perlman, ES
Kazanas, D
AF Graff, Philip B.
Georganopoulos, Markos
Perlman, Eric S.
Kazanas, Demosthenes
TI A MULTIZONE MODEL FOR SIMULATING THE HIGH-ENERGY VARIABILITY OF TeV
BLAZARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; quasars: general; radiation mechanisms: nonthermal;
X-rays: galaxies
ID SELF-COMPTON MODEL; RAPID NONTHERMAL FLARES; BL LACERTAE OBJECTS;
SIMULTANEOUS X-RAY; MULTIWAVELENGTH OBSERVATIONS; SPECTRAL EVOLUTION;
MARKARIAN 421; PKS 2155-304; CORRELATED VARIABILITY; SYNCHROTRON
EMISSION
AB We present a time-dependent multizone code for simulating the variability of synchrotron self-Compton (SSC) sources. The code adopts a multizone pipe geometry for the emission region, appropriate for simulating emission from a standing or propagating shock in a collimated jet. Variations in the injection of relativistic electrons in the inlet propagate along the length of the pipe, cooling radiatively. Our code for the first time takes into account the nonlocal, time-retarded nature of SSC losses that are thought to be dominant in TeV blazars. The observed synchrotron and SSC emission is followed self-consistently, taking into account light-travel time delays. At any given time, the emitting portion of the pipe depends on the frequency and the nature of the variation followed. Our simulation employs only one additional physical parameter relative to one-zone models, that of the pipe length, and is computationally very efficient, using simplified expressions for the SSC processes. The code will be useful for observers modeling Fermi, TeV, and X-ray observations of SSC blazars.
C1 [Graff, Philip B.; Georganopoulos, Markos] Univ Maryland, Joint Ctr Astrophys, Dept Phys, Baltimore, MD 21250 USA.
[Georganopoulos, Markos; Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
RP Graff, PB (reprint author), Univ Maryland, Joint Ctr Astrophys, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
OI Perlman, Eric/0000-0002-3099-1664
NR 44
TC 32
Z9 33
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2008
VL 689
IS 1
BP 68
EP 78
DI 10.1086/592427
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 401GV
UT WOS:000262929000006
ER
PT J
AU Melendez, M
Kraemer, SB
Schmitt, HR
Crenshaw, DM
Deo, RP
Mushotzky, RF
Bruhweiler, FC
AF Melendez, M.
Kraemer, S. B.
Schmitt, H. R.
Crenshaw, D. M.
Deo, R. P.
Mushotzky, R. F.
Bruhweiler, F. C.
TI CONSTRAINING THE ACTIVE GALACTIC NUCLEUS CONTRIBUTION IN A
MULTIWAVELENGTH STUDY OF SEYFERT GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: Seyfert; Galaxy: stellar content; infrared: galaxies
ID SPITZER-SPACE-TELESCOPE; LUMINOUS INFRARED GALAXIES; NARROW-LINE REGION;
X-RAY-EMISSION; STAR-FORMATION; MU-M; ENERGY-DISTRIBUTIONS; NEARBY
GALAXIES; SAMPLE; SPECTRA
AB We have studied the relationship between the high- and low-ionization [O IV] lambda 25.89 mu m, [Ne III] lambda 115.56 mu m, and [ Ne ii] lambda 12.81 mu m emission lines with the aim of constraining the active galactic nuclei (AGNs) and star formation contributions for a sample of 103 Seyfert galaxies. We use the [O iv] and [Ne ii] emission as tracers for the AGN power and star formation to investigate the ionization state of the emission- line gas. We find that Seyfert 2 galaxies have, on average, lower [O IV]/[ Ne II] ratios than Seyfert 1 galaxies. This result suggests two possible scenarios: (1) Seyfert 2 galaxies have intrinsically weakerAGNs, or (2) Seyfert 2 galaxies have relatively higher star formation rates than Seyfert 1 galaxies. We estimate the fraction of [Ne II] directly associated with the AGNs and find that Seyfert 2 galaxies have a larger contribution from star formation, by a factor of similar to 1.5 on average, than what is found in Seyfert 1 galaxies. Using the stellar component of [Ne II] as a tracer of the current star formation, we found similar star formation rates in Seyfert 1 and Seyfert 2 galaxies. We examined the mid- and far- infrared continua and found that [Ne II] iswell correlatedwith the continuum luminosity at 60 mu m and that both [Ne III] and [O IV] are better correlated with the 25 mu m luminosities than with the continuum at longer wavelengths, suggesting that the mid- infrared continuum luminosity is dominated by the AGN, while the far- infrared luminosity is dominated by star formation. Overall, these results test the unified model of AGNs and suggest that the differences between Seyfert galaxies cannot be solely due to viewing angle dependence.
C1 [Melendez, M.; Kraemer, S. B.; Bruhweiler, F. C.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Schmitt, H. R.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
[Schmitt, H. R.] Interferometrics Inc, Herndon, VA 20171 USA.
[Crenshaw, D. M.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA.
[Deo, R. P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
[Mushotzky, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Melendez, M (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
EM 07melendez@cua.edu
NR 63
TC 47
Z9 47
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2008
VL 689
IS 1
BP 95
EP 107
DI 10.1086/592724
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 401GV
UT WOS:000262929000008
ER
PT J
AU Marrero, AYR
Torres, DF
del Pozo, ED
Reimer, O
Cillis, AN
AF Rodriguez Marrero, Ana Y.
Torres, Diego F.
de Cea del Pozo, Elsa
Reimer, Olaf
Cillis, Analia N.
TI DIFFUSION OF COSMIC RAYS AND THE GAMMA-RAY LARGE AREA TELESCOPE:
PHENOMENOLOGY AT THE 1-100 GeV REGIME
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: observations; gamma rays: theory
ID EMISSION; RADIATION; EGRET
AB This paper analyzes astrophysical scenarios that may be detected at the upper end of the energy range of the Gamma-Ray Large Area Space Telescope (GLAST), as a result of cosmic-ray (CR) diffusion in the interstellar medium (ISM). Hadronic processes are considered the source of gamma-ray photons from localized molecular enhancements nearby accelerators. Two particular cases are presented: (1) the possibility of detecting spectral energy distributions (SEDs) with maxima above 1 GeV, which may be constrained by detection or nondetection at very high energies (VHEs) with observations by ground-based Cerenkov telescopes, and (2) the possibility of detecting V-shaped, inverted spectra, due to confusion of a nearby (to the line of sight) arrangement of accelerator/target scenarios with different characteristic properties. We show that finding these signatures (in particular, a peak at the 1-100 GeVenergy region) indicates the underlying mechanism producing the gamma-rays that is realized by nature, which accelerator (age and relative position to the target cloud) and under which diffusion properties CRs propagate.
C1 [Rodriguez Marrero, Ana Y.; Torres, Diego F.; de Cea del Pozo, Elsa] Campus UAB, Fac Sci, Inst Ciencies Espai, IEEC CSIC, Barcelona 08193, Spain.
[Reimer, Olaf] Stanford Univ, WW Hansen Expt Phys Lab HEPL, Stanford, CA 94305 USA.
[Reimer, Olaf] Stanford Univ, KIPAC, Stanford, CA 94305 USA.
[Cillis, Analia N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Marrero, AYR (reprint author), Campus UAB, Fac Sci, Inst Ciencies Espai, IEEC CSIC, Torre C5,Parell,2a Planta, Barcelona 08193, Spain.
EM arodrig@ieec.uab.es; decea@ieec.uab.es; dtorres@ieec.uab.es;
olr@stanford.edu; analia.n.cillis@nasa.gov
RI Reimer, Olaf/A-3117-2013; Torres, Diego/O-9422-2016
OI Reimer, Olaf/0000-0001-6953-1385; Torres, Diego/0000-0002-1522-9065
NR 16
TC 13
Z9 13
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2008
VL 689
IS 1
BP 213
EP 218
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 401GV
UT WOS:000262929000018
ER
PT J
AU Katsuda, S
Tsunemi, H
Uchida, H
Kimura, M
AF Katsuda, S.
Tsunemi, H.
Uchida, H.
Kimura, M.
TI FORWARD SHOCK PROPER MOTIONS OF KEPLER'S SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual (Kepler's Supernova); shock waves; supernova remnants;
X-rays: ISM
ID X-RAY; EXPANSION; EMISSION; EVOLUTION
AB The X-ray structure of Kepler's supernova remnant shows a rounded shape delineated by forward shocks. We measure proper motions of the forward shocks on overall rims of the remnant, by using archival Chandra data taken in two epochs with time difference of 6.09 yr. The proper motions of the forward shocks on the northern rim are measured to be 0.076 '' (+/- 0.032 '' +/- 0.016 '') to 0.11 '' (+/- 0.014 '' +/- 0.016 '') yr(-1), while those on the rest of the rims are measured to be 0.15 '' (+/- 0.017 '' +/- 0.016 '') to 0.30 '' (+/- 0.048 '' +/- 0.016 '') yr(-1); here the first-termerrors are statistical uncertainties and the second-term errors are systematic uncertainties. Combining the best-estimated shock velocity of 1660 +/- 120 km s(-1) measured for Balmer-dominated filaments in the northern and central portions of the remnant (Sankrit et al. 2005) with the proper motions derived for the forward shocks on the northern rim, we estimate a distance of 3.3(-0.4)(+1.6) kpc to the remnant. We measure the expansion indices, m (defined as R alpha t(m)), to be 0.47-0.82 for most of the rims. These values are consistent with those expected in Type Ia SN explosion models, in which the ejecta and the circumstellar medium have power-law density profiles whose indices are 5-7 and 0-2, respectively. In addition, we should note the slower expansion on the northern rim than that on the southern rim. This is likely caused by the inhomogeneous circumstellar medium; the density of the circumstellar medium is higher in the north than that in the south of the remnant. The newly estimated geometric center, around which we believe the explosion point exists, is located at similar to 5 '' offset to the north of the radio center.
C1 [Katsuda, S.; Tsunemi, H.; Uchida, H.; Kimura, M.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Katsuda, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Katsuda, S (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama, Osaka 5600043, Japan.
EM satoru.katsuda@nasa.gov; tsunemi@ess.sci.osaka-u.ac.jp;
uchida@ess.sci.osaka-u.ac.jp; mkimura@ess.sci.osaka-u.ac.jp
NR 25
TC 12
Z9 12
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2008
VL 689
IS 1
BP 225
EP 230
DI 10.1086/592376
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 401GV
UT WOS:000262929000020
ER
PT J
AU Krco, M
Goldsmith, PF
Brown, RL
Li, D
AF Krco, Marko
Goldsmith, Paul F.
Brown, Robert L.
Li, D.
TI AN IMPROVED TECHNIQUE FOR MEASUREMENT OF COLD H I IN MOLECULAR CLOUD
CORES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: evolution; line: profiles; molecular processes
ID NARROW SELF-ABSORPTION; GALACTIC PLANE SURVEY; DARK CLOUDS; NEUTRAL
HYDROGEN; ATOMIC-HYDROGEN; RADIO-CONTINUUM; DUST; TAURUS; GAS; COMPLEX
AB The presence of atomic gas mixed with molecular species in a "molecular" cloud may significantly affect its chemistry, the excitation of some species, and can serve as probe of the cloud's evolution. Cold neutral atomic hydrogen (H I) in molecular clouds is revealed by its self absorption of background galactic H I 21 cm emission. The properties of this gas can be investigated quantitatively through observation of H I narrow self-absorption (HINSA). In this paper we present a new technique for measuring atomic gas physical parameters from HINSA observations that utilizes molecular tracers to guide the HINSA extraction. This technique offers a significant improvement in the precision with which H I column densities can be determined over previous methods, and it opens several new avenues of study of relevance to the field of star formation.
C1 [Krco, Marko; Goldsmith, Paul F.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Goldsmith, Paul F.; Li, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brown, Robert L.] Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA.
RP Krco, M (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM marko@astro.cornell.edu
RI Goldsmith, Paul/H-3159-2016
NR 26
TC 11
Z9 11
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2008
VL 689
IS 1
BP 276
EP 289
DI 10.1086/592553
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 401GV
UT WOS:000262929000025
ER
PT J
AU Liu, Y
Luhmann, JG
Muller-Mellin, R
Schroeder, PC
Wang, L
Lin, RP
Bale, SD
Li, Y
Acuna, MH
Sauvaud, JA
AF Liu, Y.
Luhmann, J. G.
Mueller-Mellin, R.
Schroeder, P. C.
Wang, L.
Lin, R. P.
Bale, S. D.
Li, Y.
Acuna, M. H.
Sauvaud, J. -A.
TI A COMPREHENSIVE VIEW OF THE 2006 DECEMBER 13 CME: FROM THE SUN TO
INTERPLANETARY SPACE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE shock waves; solar-terrestrial relations; solar wind; Sun: coronal mass
ejections (CMEs); Sun: particle emission; Sun: radio radiation
ID CORONAL MASS EJECTIONS; MAGNETIC-FIELD; SOLAR-WIND; RADIO; EMISSION;
ULYSSES; PROPAGATION; ELECTRONS; ORIGIN; EVENT
AB The biggest halo coronal mass ejection (CME) since the Halloween storm in 2003, which occurred on 2006 December 13, is studied in terms of its solar source and heliospheric consequences. The CME was accompanied by an X3.4 flare, EUV dimmings, and coronal waves. It generated significant space weather effects such as an interplanetary shock, radio bursts, major solar energetic particle (SEP) events, and a magnetic cloud (MC) that were detected by a fleet of spacecraft including STEREO, ACE, WIND, and Ulysses. Reconstruction of the MC with the Grad-Shafranov (GS) method yields an axis orientation oblique to the flare ribbons. Observations of the SEP intensities and anisotropies show that the particles can be trapped, deflected, and reaccelerated by the large-scale transient structures. The CME-driven shock was observed at both the Earth and Ulysses when they were separated by 74 degrees in latitude and 117 degrees in longitude, which is the largest shock extent ever detected. The ejecta seem to have been missed at Ulysses. The shock arrival time at Ulysses is well predicted by an MHD model that can propagate the 1 AU data outward. The CME/shock is tracked remarkably well from the Sun all the way to Ulysses by coronagraph images, type II frequency drift, in situ measurements, and the MHD model. These results reveal a technique that combines MHD propagation of the solar wind and type II emissions to predict the shock arrival time at the Earth, which is a significant advance for space weather forecasting, especially when in situ data become available from the Solar Orbiter and Solar Sentinels.
C1 [Liu, Y.; Luhmann, J. G.; Schroeder, P. C.; Wang, L.; Lin, R. P.; Bale, S. D.; Li, Y.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Liu, Y.] Chinese Acad Sci, State Key Lab Space Weather, Beijing 100080, Peoples R China.
[Mueller-Mellin, R.] Univ Kiel, Inst Expt & Angewandte Phys, D-24098 Kiel, Germany.
[Acuna, M. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sauvaud, J. -A.] CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
RP Liu, Y (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM liuxying@ssl.berkeley.edu
RI Bale, Stuart/E-7533-2011; Wang, Linghua/C-4938-2014;
OI Bale, Stuart/0000-0002-1989-3596; Wang, Linghua/0000-0001-7309-4325;
Liu, Ying/0000-0002-3483-5909
FU STEREO [NAS5-03131]; NNSFC [40621003]
FX The research was supported by the STEREO project under grant NAS5-03131.
We acknowledge the use of SOHO, GOES, ACE, WIND, and Ulysses data and
CME parameters from the LASCO CME catalog maintained by NASA and the
Catholic University of America in cooperation with the Naval Research
Laboratory ( RL). We thank C. T. Russell for helping to maintain the
STEREOMAG data and are grateful to the referee for his or her helpful
suggestions. This work was also supported in part by grant NNSFC
40621003.
NR 47
TC 55
Z9 58
U1 2
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2008
VL 689
IS 1
BP 563
EP 571
DI 10.1086/592031
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 401GV
UT WOS:000262929000049
ER
PT J
AU Remijan, AJ
Milam, SN
Womack, M
Apponi, AJ
Ziurys, LM
Wyckoff, S
A'Hearn, MF
de Pater, I
Forster, JR
Friedel, DN
Palmer, P
Snyder, LE
Veal, JM
Woodney, LM
Wright, MCH
AF Remijan, Anthony J.
Milam, Stefanie N.
Womack, Maria
Apponi, A. J.
Ziurys, L. M.
Wyckoff, Susan
A'Hearn, M. F.
de Pater, Imke
Forster, J. R.
Friedel, D. N.
Palmer, Patrick
Snyder, L. E.
Veal, J. M.
Woodney, L. M.
Wright, M. C. H.
TI THE DISTRIBUTION, EXCITATION, AND FORMATION OF COMETARY MOLECULES:
METHANOL, METHYL CYANIDE, AND ETHYLENE GLYCOL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; comets: individual (Hale Bopp [C/1995 01], LINEAR [C/2002
T7]); molecular processes; radio lines: solar system; techniques:
interferometric
ID O1 HALE-BOPP; C/1995 O1; C/2001 Q4; SPECTROSCOPY; FORMALDEHYDE; REGIONS;
CH3CN; CORE; NEAT; HOT
AB We present an interferometric and single-dish study of small organic species toward Comets C/1995 O1 (Hale-Bopp) and C/2002 T7 (LINEAR) using the BIMA interferometer at 3 mm and the ARO 12 m telescope at 2 mm. For Comet Hale-Bopp, both the single-dish and interferometer observations of CH(3)OH indicate an excitation temperature of 105 +/- 5 K and an average production rate ratio Q(CH(3)OH)/Q(H(2)O) similar to 1.3% at similar to 1 AU. In addition, the aperture synthesis observations of CH(3)OH suggest a distribution well described by a spherical outflow and no evidence of significant extended emission. Single-dish observations of CH(3)CN in Comet Hale-Bopp indicate an excitation temperature of 200 +/- 10 K and a production rate ratio of Q(CH(3)CN)/Q(H(2)O) similar to 0.017% at similar to 1 AU. The nondetection of a previously claimed transition of cometary (CH(2)OH)(2) toward Comet Hale-Bopp with the 12 m telescope indicates a compact distribution of emission, D < 9 '' (< 8500 km). For the single-dish observations of Comet T7 LINEAR, we find an excitation temperature of CH(3)OH of 35 +/- 5 K and a CH(3)OH production rate ratio of Q(CH(3)OH)/Q(H(2)O) similar to 1.5% at similar to 0.3 AU. Our data support current chemical models that CH(3)OH, CH(3)CN, and (CH(2)OH)(2) are parent nuclear species distributed into the coma via direct sublimation off cometary ices from the nucleus with no evidence of significant production in the outer coma.
C1 [Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22901 USA.
[Milam, Stefanie N.; Apponi, A. J.; Ziurys, L. M.] Univ Arizona, Dept Chem, NASA, Astrobiol Inst, Tucson, AZ 85721 USA.
[Womack, Maria] St Cloud State Univ, Dept Phys & Astron, St Cloud, MN 56301 USA.
[Wyckoff, Susan] Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA.
[A'Hearn, M. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[de Pater, Imke; Forster, J. R.; Wright, M. C. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Friedel, D. N.; Snyder, L. E.; Veal, J. M.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Palmer, Patrick] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Woodney, L. M.] Calif State Univ San Bernardino, Dept Phys, San Bernardino, CA 92407 USA.
RP Remijan, AJ (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22901 USA.
EM aremijan@nrao.edu; stefanie.n.milam@nasa.gov; mwomack@stcloudstate.edu;
aapponi@as.arizona.edu; lziurys@as.arizona.edu; wyckoff@asu.edu;
ma@astro.umd.edu; imke@floris.berkeley.edu; rforster@astro.berkeley.edu;
friedel@astro.uiuc.edu; ppalmer@oskar.uchicago.edu;
snyder@astro.uiuc.edu; jveal@swccd.edu; woodney@csusb.edu;
wright@astro.berkeley.edu
RI Milam, Stefanie/D-1092-2012;
OI Milam, Stefanie/0000-0001-7694-4129; Womack, Maria/0000-0003-4659-8653
NR 35
TC 9
Z9 9
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2008
VL 689
IS 1
BP 613
EP 621
DI 10.1086/592242
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 401GV
UT WOS:000262929000053
ER
PT J
AU Bentz, MC
Walsh, JL
Barth, AJ
Baliber, N
Bennert, N
Canalizo, G
Filippenko, AV
Ganeshalingam, M
Gates, EL
Greene, JE
Hidas, MG
Hiner, KD
Lee, N
Li, WD
Malkan, MA
Minezaki, T
Serduke, FJD
Shiode, JH
Silverman, JM
Steele, TN
Stern, D
Street, RA
Thornton, CE
Treu, T
Wang, XF
Woo, JH
Yoshii, Y
AF Bentz, Misty C.
Walsh, Jonelle L.
Barth, Aaron J.
Baliber, Nairn
Bennert, Nicola
Canalizo, Gabriela
Filippenko, Alexei V.
Ganeshalingam, Mohan
Gates, Elinor L.
Greene, Jenny E.
Hidas, Marton G.
Hiner, Kyle D.
Lee, Nicholas
Li, Weidong
Malkan, Matthew A.
Minezaki, Takeo
Serduke, Frank J. D.
Shiode, Joshua H.
Silverman, Jeffrey M.
Steele, Thea N.
Stern, Daniel
Street, Rachel A.
Thornton, Carol E.
Treu, Tommaso
Wang, Xiaofeng
Woo, Jong-Hak
Yoshii, Yuzuru
TI FIRST RESULTS FROM THE LICK AGN MONITORING PROJECT: THE MASS OF THE
BLACK HOLE IN ARP 151
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: individual (Arp 151); galaxies: nuclei;
galaxies: Seyfert
ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; SEYFERT-GALAXIES; EMISSION;
REVERBERATION; VARIABILITY; CONTINUUM; NGC-5548; QUASARS; SIZES
AB We have recently completed a 64 night spectroscopic monitoring campaign at the Lick Observatory 3 m Shane telescope with the aim of measuring the masses of the black holes in 13 nearby (z < 0.05) Seyfert 1 galaxies with with expected masses in the range similar to 10(6)-10(7) M(circle dot). We present here the first results from this project-the mass, of the central black hole in Arp 151. Strong variability throughout the campaign led to an exceptionally clean H beta lag measurement in this object of 4.25(-0.66)(+0.68) days in the observed frame. Coupled with the width of the H beta emission line in the variable spectrum, we determine a black hole mass of (7.1 +/- 1.2) x 10(6) M(circle dot), assuming the Onken et al. normalization for reverberation-based virial masses. We also find velocity-resolved lag information within the H beta emission line which clearly shows infalling gas in the H beta-emitting region. Further detailed analysis may lead to a full model of the geometry and kinematics of broad line region gas around the central black hole in Arp 151.
C1 [Bentz, Misty C.; Walsh, Jonelle L.; Barth, Aaron J.; Thornton, Carol E.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Baliber, Nairn; Bennert, Nicola; Hidas, Marton G.; Street, Rachel A.; Treu, Tommaso; Woo, Jong-Hak] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Baliber, Nairn; Hidas, Marton G.; Street, Rachel A.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Bennert, Nicola; Canalizo, Gabriela; Hiner, Kyle D.] Univ Calif Riverside, Inst Geophys & Planetary Phys, Riverside, CA 92521 USA.
[Canalizo, Gabriela; Hiner, Kyle D.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Filippenko, Alexei V.; Ganeshalingam, Mohan; Lee, Nicholas; Li, Weidong; Serduke, Frank J. D.; Shiode, Joshua H.; Silverman, Jeffrey M.; Steele, Thea N.; Wang, Xiaofeng] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Gates, Elinor L.] Lick Observ, Mt Hamilton, CA 95140 USA.
[Greene, Jenny E.] Princeton Univ Observ, Princeton, NJ 08544 USA.
[Malkan, Matthew A.; Woo, Jong-Hak] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90024 USA.
[Minezaki, Takeo; Yoshii, Yuzuru] Univ Tokyo, Sch Sci, Inst Astron, Tokyo 1810015, Japan.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China.
[Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China.
[Yoshii, Yuzuru] Univ Tokyo, Sch Sci, Res Ctr Early Univ, Tokyo 1130033, Japan.
RP Bentz, MC (reprint author), Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA.
EM mbentz@uci.edu
RI Woo, Jong-Hak/A-2790-2014; Wang, Xiaofeng/J-5390-2015
FU NSF [AST 0548198, AST 0607485, AST 0642621, AST 0507450]; TABASGO
Foundation
FX We thank the Lick Observatory staff for their tireless support during
this project. We also thank Brad Peterson for helpful conversations and
the use of his analysis software. This work was supported by NSF grants
AST 0548198 (UC Irvine), AST 0607485 (UC Berkeley), AST 0642621 (UC
Santa Barbara), and AST 0507450 (UC Riverside), as well as the TABASGO
Foundation (UC Berkeley).
NR 23
TC 40
Z9 40
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 10
PY 2008
VL 689
IS 1
BP L21
EP L24
DI 10.1086/595719
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 398LO
UT WOS:000262733800006
ER
PT J
AU Burgasser, AJ
Tinney, CG
Cushing, MC
Saumon, D
Marley, MS
Bennett, CS
Kirkpatrick, JD
AF Burgasser, Adam J.
Tinney, C. G.
Cushing, Michael C.
Saumon, Didier
Marley, Mark S.
Bennett, Clara S.
Kirkpatrick, J. Davy
TI 2MASS J09393548-2448279: THE COLDEST AND LEAST LUMINOUS BROWN DWARF
BINARY KNOWN?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: close; stars: fundamental parameters; stars: individual (2MASS
J04151954-0935066 2MASS J09393548-2448279); stars: low-mass, brown
dwarfs
ID SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; T-DWARFS; SPECTRAL
CLASSIFICATION; ADAPTIVE OPTICS; FILTER SET; SPECTROGRAPH; TRANSITION;
SEARCH; ATMOSPHERES
AB Determinations of the luminosity and atmospheric properties of the T8 brown dwarf 2MASS J09393548 - 2448279 are presented, based on Spitzer IRAC and IRS observations and ground-based astrometry. We find log(10) (L(bol)/L(circle dot)) = -5.69 +/- 0.03 for this source, comparable to the current low-luminosity record holder 2MASS J04151954 - 0935066. However, modeling of near- and mid-infrared spectral data indicates an effective temperature of 600 +/- 35 K, roughly 100 K cooler than 2M0415. These parameters require a highly inflated radius for 2M0939 (R approximate to 0.13 R(circle dot)) which cannot be reconciled with brown dwarf structure models. However, if this source is an unresolved, equal-mass binary, then the reduced luminosity of each component (L(bol) approximate to 10(-6) L(circle dot)) can be brought into agreement with the inferred atmospheric parameters for an age of 0.4-12 Gyr and component masses of 0.01-0.05 M(circle dot). This hypothesis can be tested through future high-resolution imaging and/or spectroscopic observations.
C1 [Burgasser, Adam J.; Bennett, Clara S.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Tinney, C. G.] Univ New S Wales, Sch Phys, Dept Astrophys, Sydney, NSW 2052, Australia.
[Saumon, Didier] Los Alamos Natl Lab, Div Appl Phys, Los Alamos, NM 87545 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kirkpatrick, J. Davy] CALTECH, Infrared Proc Anal Ctr, Pasadena, CA 91125 USA.
RP Burgasser, AJ (reprint author), MIT, Kavli Inst Astrophys & Space Res, Bldg 37,Room 664B,77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM ajb@mit.edu
RI Marley, Mark/I-4704-2013
FU NASA [DP0774000]; NSF
FX This publication makes use of data 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 (IPAC), and funded by NASA
and the NSF. The 2MASS data were obtained from the NASA/IPAC Infrared
Science Archive, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology (JPL/Caltech), under contract with
NASA. This work is also based in part on observations made with the
Spitzer Space Telescope, which is operated by JPL/Caltech under a
contract with NASA. Support for this work was provided by NASA through
an award issued by JPL/Caltech. C. G. T. acknowledges support from ARC
grant DP0774000. Support for D. S.'s work, part of the Spitzer Space
Telescope Theoretical Research Program, was provided by NASA. We thank
our anonymous referee for her/his prompt review of our original
manuscript.
NR 35
TC 31
Z9 31
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 10
PY 2008
VL 689
IS 1
BP L53
EP L56
DI 10.1086/595747
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 398LO
UT WOS:000262733800014
ER
PT J
AU Meijerink, R
Poelman, DR
Spaans, M
Tielens, AGGM
Glassgold, AE
AF Meijerink, R.
Poelman, D. R.
Spaans, M.
Tielens, A. G. G. M.
Glassgold, A. E.
TI ROTATIONAL LINE EMISSION FROM WATER IN PROTOPLANETARY DISKS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; infrared: stars; planetary systems:
protoplanetary disks; radiative transfer; stars: pre-main-sequence;
X-rays: stars
ID ACCRETION DISKS; SNOW LINE; GAS TEMPERATURE; YOUNG OBJECTS; H2O;
IRRADIATION; EXCITATION; LOCATION; REGION; MODELS
AB Circumstellar disks provide the material reservoir for the growth of young stars and for planet formation. We combine a high-level radiative transfer program with a thermal-chemical model of a typical T Tauri star disk to investigate the diagnostic potential of the far-infrared lines of water for probing disk structure. We discuss the observability of pure rotational H(2)O lines with the Herschel Space Observatory, specifically the residual gas where water is mainly frozen out. We find that measuring both the line profile of the ground 1(10)-1(01) ortho-H(2)O transition and the ratio of this line to the 3(12)-3(03) and 2(21)-2(12) lines can provide information on the gas-phase water between 5 and 100 AU, but not on the snow line which is expected to occur at smaller radii.
C1 [Meijerink, R.; Glassgold, A. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Poelman, D. R.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Scotland.
[Spaans, M.; Tielens, A. G. G. M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Tielens, A. G. G. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Meijerink, R (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM rowin@gps.caltech.edu
FU NSF [AST 05-07423]; NASA [NNG06GF88G]
FX This work has been supported by NSF grant AST 05-07423 and NASA grant
NNG06GF88G to UC Berkeley. We thank F. van der Tak, P. d'Alessio, and
the anonymous referee for their invaluable contributions.
NR 26
TC 13
Z9 13
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 10
PY 2008
VL 689
IS 1
BP L57
EP L60
DI 10.1086/595726
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 398LO
UT WOS:000262733800015
ER
PT J
AU Comstock, JM
Lin, RF
Starr, DO
Yang, P
AF Comstock, Jennifer M.
Lin, Ruei-Fong
Starr, David O'C.
Yang, Ping
TI Understanding ice supersaturation, particle growth, and number
concentration in cirrus clouds
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Review
ID WATER-VAPOR MEASUREMENTS; DELIQUESCENT MIXED CCN; ART. NO. 2230; IN-SITU
DATA; RELATIVE-HUMIDITY; RADIATIVE PROPERTIES; CLIMATE MODELS;
MICROPHYSICAL PROPERTIES; UPPER-TROPOSPHERE; RAMAN LIDAR
AB Many factors control the ice supersaturation and microphysical properties in cirrus clouds. We explore the effects of dynamic forcing, ice nucleation mechanisms, and ice crystal growth rate on the evolution and distribution of water vapor and cloud properties in nighttime cirrus clouds using a one-dimensional cloud model with bin microphysics and remote sensing measurements obtained at the Department of Energy's Atmospheric Radiation Measurement (ARM) Climate Research Facility located near Lamont, OK. We forced the model using both large-scale vertical ascent and, for the first time, mean mesoscale velocity derived from radar Doppler velocity measurements. Both heterogeneous and homogeneous nucleation processes are explored, where a classical theory heterogeneous scheme is compared with empirical representations. We evaluated model simulations by examining both bulk cloud properties and distributions of measured radar reflectivity, lidar extinction, and water vapor profiles, as well as retrieved cloud microphysical properties. Our results suggest that mesoscale variability is the primary mechanism needed to reproduce observed quantities. Model sensitivity to the ice growth rate is also investigated. The most realistic simulations as compared with observations are forced using mesoscale waves, include fast ice crystal growth, and initiate ice by either homogeneous or heterogeneous nucleation. Simulated ice crystal number concentrations (tens to hundreds particles per liter) are typically two orders of magnitude smaller than previously published results based on aircraft measurements in cirrus clouds, although higher concentrations are possible in isolated pockets within the nucleation zone.
C1 [Comstock, Jennifer M.] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA.
[Lin, Ruei-Fong] Univ Maryland, NASA, Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA.
[Starr, David O'C.] NASA, Goddard Space Flight Ctr, Atmospher & Space Phys Lab, Greenbelt, MD 20771 USA.
[Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
RP Comstock, JM (reprint author), Pacific NW Natl Lab, Atmospher Sci & Global Change Div, POB 999,MSIN K9-24, Richland, WA 99352 USA.
EM jennifer.comstock@pnl.gov
RI Yang, Ping/B-4590-2011
FU DOE Office of Science; Atmospheric Radiation Measurement (ARM) Program
FX Research performed by Jennifer M. Comstock was supported by the DOE
Office of Science, Atmospheric Radiation Measurement (ARM) Program.
NR 101
TC 23
Z9 23
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 DEC 10
PY 2008
VL 113
IS D23
AR D23211
DI 10.1029/2008JD010332
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 383JO
UT WOS:000261670100009
ER
PT J
AU Stephens, GL
Vane, DG
Tanelli, S
Im, E
Durden, S
Rokey, M
Reinke, D
Partain, P
Mace, GG
Austin, R
L'Ecuyer, T
Haynes, J
Lebsock, M
Suzuki, K
Waliser, D
Wu, D
Kay, J
Gettelman, A
Wang, Z
Marchand, R
AF Stephens, Graeme L.
Vane, Deborah G.
Tanelli, Simone
Im, Eastwood
Durden, Stephen
Rokey, Mark
Reinke, Don
Partain, Philip
Mace, Gerald G.
Austin, Richard
L'Ecuyer, Tristan
Haynes, John
Lebsock, Matthew
Suzuki, Kentaroh
Waliser, Duane
Wu, Dong
Kay, Jen
Gettelman, Andrew
Wang, Zhien
Marchand, Rojer
TI CloudSat mission: Performance and early science after the first year of
operation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID COMMUNITY ATMOSPHERE MODEL; RADIATIVE PROPERTIES; MICROPHYSICS SCHEME;
CLIMATE SYSTEM; VERSION-3 CAM3; RADAR; AIRBORNE; PRECIPITATION;
CLOUDINESS; SPACE
AB This paper reports on the early mission performance of the radar and other major aspects of the CloudSat mission. The Cloudsat cloud profiling radar (CPR) has been operating since 2 June 2006 and has proven to be remarkably stable since turn-on. A number of products have been developed using these space-borne radar data as principal inputs. Combined with other A-Train sensor data, these new observations offer unique, global views of the vertical structure of clouds and precipitation jointly. Approximately 11% of clouds detected over the global oceans produce precipitation that, in all likelihood, reaches the surface. Warm precipitating clouds are both wetter and composed of larger particles than nonprecipitating clouds. The frequency of precipitation increases significantly with increasing cloud depth, and the increased depth and water path of precipitating clouds leads to increased optical depths and substantially more sunlight reflected from precipitating clouds compared to than nonprecipitating warm clouds. The CloudSat observations also provide an authoritative estimate of global ice water paths. The observed ice water paths are larger than those predicted from most climate models. CloudSat observations also indicate that clouds radiatively heat the global mean atmospheric column (relative to clear skies) by about 10 Wm(-2). Although this heating appears to be contributed almost equally by solar and infrared absorption, the latter contribution is shown to vary significantly with latitude being influenced by the predominant cloud structures of the different region in questions.
C1 [Stephens, Graeme L.; Austin, Richard; L'Ecuyer, Tristan; Haynes, John; Lebsock, Matthew; Suzuki, Kentaroh] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Vane, Deborah G.; Tanelli, Simone; Im, Eastwood; Durden, Stephen; Rokey, Mark; Waliser, Duane; Wu, Dong] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kay, Jen; Gettelman, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80305 USA.
[Mace, Gerald G.] Univ Utah, Dept Meteorol, Salt Lake City, UT 84112 USA.
[Marchand, Rojer] Univ Washington, Joint Inst Study Atmosphere & Ocean, Seattle, WA 98195 USA.
[Partain, Philip] MetSat, Sci Technol Corp, Ft Collins, CO 80323 USA.
[Reinke, Don] Colorado State Univ, CIRA, Ft Collins, CO 80523 USA.
[Wang, Zhien] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
RP Stephens, GL (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
EM stephens@atmos.colostate.edu; dvane@jpl.nasa.gov;
simone.tanelli@jpl.nasa.gov; eastwood.im@jpl.nasa.gov;
stephen.durden@jpl.nasa.gov; mark.rokey@jpl.nasa.gov;
reinke@cira.colostate.edu; partain@cira.colostate.edu;
mace@met.utah.edu; Austin@atmos.colostate.edu;
Tristan@atmos.colostate.edu; Haynes@atmos.colostate.edu;
lebsock@atmos.colostate.edu; kenta@atmos.colostate.edu;
duane.waliser@jpl.nasa.gov; Dong.L.Wu@jpl.nasa.gov; jenkay@cgd.ucar.edu;
andrew@ucar.edu; zwang@uwyo.edu; rojmarch@u.washington.edu
RI Suzuki, Kentaroh/C-3624-2011; Wang, Zhien/F-4857-2011; Kay,
Jennifer/C-6042-2012; L'Ecuyer, Tristan/C-7040-2013; L'Ecuyer,
Tristan/E-5607-2012; Wu, Dong/D-5375-2012
OI L'Ecuyer, Tristan/0000-0002-7584-4836;
FU NASA [NNX07AR11G]
FX This study was supported by NASA grant NNX07AR11G.
NR 40
TC 258
Z9 266
U1 9
U2 45
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 DEC 10
PY 2008
VL 113
IS D23
AR D00A18
DI 10.1029/2008JD009982
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 383JO
UT WOS:000261670100004
ER
PT J
AU Taha, G
Jaross, G
Fussen, D
Vanhellemont, F
Kyrola, E
McPeters, RD
AF Taha, Ghassan
Jaross, Glen
Fussen, Didier
Vanhellemont, Filip
Kyroelae, Erkki
McPeters, Richard D.
TI Ozone profile retrieval from GOMOS limb scattering measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OSIRIS INSTRUMENT; ODIN SATELLITE; SAGE-II; SCIAMACHY; RADIATION;
MISSION; ENVISAT
AB We analyzed a set of Global Ozone Monitoring by Occultation of Stars (GOMOS) bright limb measurements with solar zenith angles less than 85 degrees and within 150 km of Stratospheric Aerosol and Gas Experiment II (SAGE II) measurements. In order to perform any species retrieval, GOMOS measurements were first corrected for stray light contamination. GOMOS pointing was analyzed using scene-based tangent height algorithms, and the best results were achieved using similar to 350 nm (Rayleigh) pixels that were consistent with GOMOS known accurate pointing. In order to demonstrate GOMOS bright limb capabilities, ozone profile retrievals were performed using GOMOS measurements of limb-scattered radiances with the Ozone Mapping and Profiler Suite limb profiler algorithm. The algorithm performs a simultaneous optimal estimation inversion of both Hartley-Huggins and Chappuis band radiances. We restricted our GOMOS ozone retrievals to the range 25-53 km, a region of relatively constant measurement uncertainty. In this first look at GOMOS limb data, the retrieved ozone profiles agree with collocated SAGE II measurements on average to within 10-15% and with a standard deviation of 10%. Retrieval results were consistent for both upper and lower GOMOS detector bands.
C1 [Taha, Ghassan; Jaross, Glen] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Fussen, Didier; Vanhellemont, Filip] Belgian Inst Space Aeron, B-1180 Brussels, Belgium.
[Kyroelae, Erkki] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[McPeters, Richard D.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
RP Taha, G (reprint author), Sci Syst & Applicat Inc, Suite 500,10210 Greenbelt Rd, Lanham, MD 20706 USA.
EM ghassan_taha@ssaihq.com; glen.jaross@nasa.gov;
didier.fussen@aeronomie.be; filip.vanhellemont@aeronomie.be;
erkki.kyrola@fmi.fi; richard.d.mcpeters@nasa.gov
RI Kyrola, Erkki/E-1835-2014; McPeters, Richard/G-4955-2013
OI McPeters, Richard/0000-0002-8926-8462
NR 26
TC 8
Z9 8
U1 0
U2 0
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 DEC 10
PY 2008
VL 113
IS D23
AR D23307
DI 10.1029/2007JD009409
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 383JO
UT WOS:000261670100001
ER
PT J
AU Jeon, KJ
Jeun, M
Lee, E
Lee, JM
Lee, KI
von Allmen, P
Lee, A
AF Jeon, Kye Jin
Jeun, Minhong
Lee, Eunsongyi
Lee, Jun Min
Lee, Kyoung-Il
von Allmen, Paul
Lee, Wooyoung
TI Finite size effect on hydrogen gas sensing performance in single Pd
nanowires
SO NANOTECHNOLOGY
LA English
DT Article
ID SENSOR; PERMEATION; MEMBRANES; SYSTEMS; ARRAYS
AB We present the hydrogen sensing performance of individual Pd nanowires grown by electrodeposition into nanochannels of anodized aluminum oxide (AAO) templates investigated as a function of the nanowire diameter. Four-terminal devices based on individual Pd nanowires were found to successfully detect hydrogen gas (H(2)). Our experimental results show that the H2 sensing sensitivity increases and the response time decreases with decreasing diameter of Pd nanowires with d = 400, 200, 80 and 20 nm, due to the high surface-to-volume ratio and short diffusion paths, respectively. This is in qualitatively good agreement with simulated results obtained from a theoretical model based on a combination of the rate equation and diffusion equation.
C1 [Jeon, Kye Jin; Jeun, Minhong; Lee, Eunsongyi; Lee, Jun Min; Lee, Kyoung-Il; Lee, Wooyoung] Yonsei Univ, Dept Mat Sci & Engn, Seoul 120749, South Korea.
[von Allmen, Paul] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lee, A (reprint author), Yonsei Univ, Dept Mat Sci & Engn, 134 Shinchon, Seoul 120749, South Korea.
EM wooyoung@yonsei.ac.kr
RI Lee, Eunsongyi/B-5162-2011
FU KOSEF [R15-2004024-00000-0]; Seoul Research and Business Development
Program [10816]; Agency for Defense Development through the Defense Nano
Technology Application Center
FX This work was supported by KOSEF through the National Core Research
Center for Nanomedical Technology (R15-2004024-00000-0), the Seoul
Research and Business Development Program (10816) and the Agency for
Defense Development through the Defense Nano Technology Application
Center.
NR 15
TC 27
Z9 28
U1 3
U2 17
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD DEC 10
PY 2008
VL 19
IS 49
AR 495501
DI 10.1088/0957-4484/19/49/495501
PG 6
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 374KW
UT WOS:000261043300014
PM 21730673
ER
PT J
AU Masse, M
Le Mouelic, S
Bourgeois, O
Combe, JP
Le Deit, L
Sotin, C
Bibring, JP
Gondet, B
Langevin, Y
AF Masse, M.
Le Mouelic, S.
Bourgeois, O.
Combe, J. -P.
Le Deit, L.
Sotin, C.
Bibring, J. -P.
Gondet, B.
Langevin, Y.
TI Mineralogical composition, structure, morphology, and geological history
of Aram Chaos crater fill on Mars derived from OMEGA Mars Express data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MERIDIANI-PLANUM; OPPORTUNITY ROVER; THERMAL INERTIA; HEMATITE; SURFACE;
DEPOSITS; SPECTROMETER; EVOLUTION; SULFATES; TERRAINS
AB Aram Chaos is a crater 280 km in diameter centered at 2.5 degrees N, 338.5 degrees E. It is filled by chaotic terrains overlain by a dome-shaped, layered 900 m thick formation displaying spectral signatures of ferric oxides on Thermal Emission Spectrometer (TES) and Observatoire pour la Mineralogie, L'Eau, les Glaces et L'Activite (OMEGA) medium spatial resolution data. We describe in detail the mineralogical composition, structure, and morphology of this crater fill using high-resolution data (OMEGA, Mars Orbiter Laser Altimeter, Mars Orbiter Camera, TES, Thermal Emission Imaging System, and High-Resolution Imaging Science Experiment). We infer the following formation scenario: the crater was first filled by a geological formation, the composition of which remains unclear because it is covered by dust. Widespread fracturing of this formation led to the development of chaotic terrains. Later, a second layered formation, presently dome shaped, was emplaced unconformably on the chaotic terrains. This younger unit is composed of a bright, poorly consolidated material that contains both monohydrated sulfates and ferric oxides according to OMEGA data. The surface of this formation is partially covered by dust and displays landforms indicating that the bright material has been mobilized by wind during or after its deposition. After its emplacement, this formation has been grooved down to various depths by large eolian erosion corridors. In these corridors, eolian removal of the bright material with a sulfate-rich matrix has left debris fans, sand sheets, and dunes, which display some of the strongest spectral signatures of ferric oxides on Mars. Similar residual deposits enriched in ferric oxides, overlying a layered formation containing both ferric oxides and sulfates, have been observed by the Opportunity rover in Meridiani Planum, suggesting a common formation process.
C1 [Masse, M.; Le Mouelic, S.; Bourgeois, O.; Le Deit, L.] Univ Nantes, CNRS, UMR6112, Lab Planetol & Geodynam, F-44322 Nantes 3, France.
[Bibring, J. -P.; Gondet, B.; Langevin, Y.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Combe, J. -P.] Bear Fight Ctr, Winthrop, WA 98862 USA.
[Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Masse, M (reprint author), Univ Nantes, CNRS, UMR6112, Lab Planetol & Geodynam, 2 Chemin Houssiniere,BP 92205, F-44322 Nantes 3, France.
EM marion.masse@univ-nantes.fr
FU Centre National de la Recherche Scientifique; Institut National des
Sciences de l'Univers; Centre National d'Etudes Spatiales; French
government
FX This work benefited from financial supports from the Centre National de
la Recherche Scientifique, Institut National des Sciences de l'Univers
(Programme National de Planetologie), and from the Centre National
d'Etudes Spatiales. M. Masse is supported by a Ph. D. research grant
from the French government (Ministere de l'Enseignement Superieur et de
la Recherche). We thank W. H. Farrand and an anonymous reviewer for
their insightful comments. Thorough advice from D. Mege, S. Pochat, and
A. Bargery greatly improved the quality of this article.
NR 57
TC 25
Z9 25
U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 9
PY 2008
VL 113
IS E12
AR E12006
DI 10.1029/2008JE003131
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 383QD
UT WOS:000261687500002
ER
PT J
AU Huang, XC
Schwenke, DW
Lee, TJ
AF Huang, Xinchuan
Schwenke, David W.
Lee, Timothy J.
TI An accurate global potential energy surface, dipole moment surface, and
rovibrational frequencies for NH(3)
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
DE ab initio calculations; ammonia; correlation methods; coupled cluster
calculations; excited states; functional analysis; molecular moments;
perturbation theory; potential energy surfaces; rotational-vibrational
states
ID AB-INITIO; VARIATIONAL CALCULATIONS; PROJECTION OPERATORS; INTERSTELLAR
AMMONIA; GIANT PLANETS; HOT AMMONIA; GLIESE 570D; FORCE-FIELD;
EQUILIBRIUM; WATER
AB A global potential energy surface (PES) that includes short and long range terms has been determined for the NH(3) molecule. The singles and doubles coupled-cluster method that includes a perturbational estimate of connected triple excitations and the internally contracted averaged coupled-pair functional electronic structure methods have been used in conjunction with very large correlation-consistent basis sets, including diffuse functions. Extrapolation to the one-particle basis set limit was performed and core correlation and scalar relativistic contributions were included directly, while the diagonal Born-Oppenheimer correction was added. Our best purely ab initio PES, denoted "mixed," is constructed from two PESs which differ in whether the ic-ACPF higher-order correlation correction was added or not. Rovibrational transition energies computed from the mixed PES agree well with experiment and the best previous theoretical studies, but most importantly the quality does not deteriorate even up to 10 300 cm(-1) above the zero-point energy (ZPE). The mixed PES was improved further by empirical refinement using the most reliable J=0-2 rovibrational transitions in the HITRAN 2004 database. Agreement between high-resolution experiment and rovibrational transition energies computed from our refined PES for J=0-6 is excellent. Indeed, the root mean square (rms) error for 13 HITRAN 2004 bands for J=0-2 is 0.023 cm(-1) and that for each band is always <= 0.06 cm(-1). For J=3-5 the rms error is always <= 0.15 cm(-1). This agreement means that transition energies computed with our refined PES should be useful in the assignment of new high-resolution NH(3) spectra and in correcting mistakes in previous assignments. Ideas for further improvements to our refined PES and for extension to other isotopolog are discussed.
C1 [Huang, Xinchuan; Schwenke, David W.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Schwenke, DW (reprint author), NASA, Ames Res Ctr, Mail Stop T27B-1, Moffett Field, CA 94035 USA.
EM xinchuan.huang-1@nasa.gov; timothy.j.lee@nasa.gov;
timothy.j.lee@nasa.gov
RI HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012; schwenke,
david/I-3564-2013
FU NASA; Spitzer Space Telescope GO program
FX X. H. acknowledges the support by an appointment to the NASA
Postdoctoral Program at the Ames Research Center, administered by Oak
Ridge Associated Universities through a contract with NASA. Support from
the Spitzer Space Telescope GO program (Cycle 4 ) is gratefully
acknowledged. Professor Joel Bowman is thanked for insightful
discussions and significant assistance in the early stages of this
study. Helpful comments from Dr. Wesley Allen and encouragement from Dr.
John Pearson and Dr. Mark Marley are gratefully acknowledged.
NR 51
TC 43
Z9 43
U1 2
U2 20
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-9606
J9 J CHEM PHYS
JI J. Chem. Phys.
PD DEC 7
PY 2008
VL 129
IS 21
AR 214304
DI 10.1063/1.3025885
PG 16
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 379XW
UT WOS:000261430900022
PM 19063558
ER
PT J
AU Russell, P
Thomas, N
Byrne, S
Herkenhoff, K
Fishbaugh, K
Bridges, N
Okubo, C
Milazzo, M
Daubar, I
Hansen, C
McEwen, A
AF Russell, Patrick
Thomas, Nicolas
Byrne, Shane
Herkenhoff, Kenneth
Fishbaugh, Kathryn
Bridges, Nathan
Okubo, Chris
Milazzo, Moses
Daubar, Ingrid
Hansen, Candice
McEwen, Alfred
TI Seasonally active frost-dust avalanches on a north polar scarp of Mars
captured by HiRISE
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID REGION
AB North-polar temporal monitoring by the High Resolution Imaging Science Experiment (HiRISE) orbiting Mars has discovered new, dramatic examples that Mars' CO2-dominated seasonal volatile cycle is not limited to quiet deposition and sublimation of frost. In early northern martian spring, 2008, HiRISE captured several cases of CO2 frost and dust cascading down a steep, polar scarp in discrete clouds. Analysis of morphology and process reveals these events to be similar to terrestrial powder avalanches, sluffs, and falls of loose, dry snow. Potential material sources and initiating mechanisms are discussed in the context of the Martian polar spring environment and of additional, active, aeolian processes observed on the plateau above the scarp. The scarp events are identified as a trigger for mass wasting of bright, fractured layers within the basal unit, and may indirectly influence the retreat rate of steep polar scarps in competing ways. Citation: Russell, P., et al. (2008), Seasonally active frost-dust avalanches on a north polar scarp of Mars captured by HiRISE, Geophys. Res. Lett., 35, L23204, doi: 10.1029/2008GL035790.
C1 [Russell, Patrick; Thomas, Nicolas] Univ Bern, Inst Phys, Dept Space Res & Planetary Sci, CH-3012 Bern, Switzerland.
[Bridges, Nathan; Hansen, Candice] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Daubar, Ingrid; McEwen, Alfred] Univ Arizona, Lunar & Planetary Lab, HiRISE Operat Ctr, Tucson, AZ 85721 USA.
[Fishbaugh, Kathryn] Smithsonian Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20024 USA.
[Herkenhoff, Kenneth; Okubo, Chris; Milazzo, Moses] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA.
RP Russell, P (reprint author), Univ Bern, Inst Phys, Dept Space Res & Planetary Sci, Sidlerstr 5, CH-3012 Bern, Switzerland.
EM patrick.russell@space.unibe.ch; nicolas.thomas@space.unibe.ch;
shane@lpl.arizona.edu; kherkenhoff@usgs.gov; fishbaughke@si.edu;
nathan.t.bridges@jpl.nasa.gov; cokubo@usgs.gov; moses@usgs.gov;
ingrid@pirl.lpl.arizona.edu; candice.j.hansen@jpl.nasa.gov;
mcewen@pirl.lpl.arizona.edu
RI Byrne, Shane/B-8104-2012; Daubar, Ingrid/N-1408-2013
FU Swiss National Science Foundation
FX Thank you to P. Thomas and M. Koutnik for helpful reviews, the HiRISE
and HiROC teams for help and discussions, and Sarah Mattson for jitter
analysis. This work was supported in part by the Swiss National Science
Foundation.
NR 12
TC 16
Z9 16
U1 2
U2 9
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 DEC 6
PY 2008
VL 35
IS 23
AR L23204
DI 10.1029/2008GL035790
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 380NA
UT WOS:000261471200004
ER
PT J
AU L'Ecuyer, TS
Wood, NB
Haladay, T
Stephens, GL
Stackhouse, PW
AF L'Ecuyer, Tristan S.
Wood, Norman B.
Haladay, Taryn
Stephens, Graeme L.
Stackhouse, Paul W., Jr.
TI Impact of clouds on atmospheric heating based on the R04 CloudSat fluxes
and heating rates data set
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID EARTH RADIATION BUDGET; GENERAL-CIRCULATION MODEL; ISCCP DATA SETS;
ENERGY BUDGET; CIRRUS CLOUDS; PART I; INTERANNUAL VARIATIONS;
SEASONAL-VARIATION; AFRICAN CONTINENT; SOLAR IRRADIANCE
AB Among the largest uncertainties in quantifying the radiative impacts of clouds are those that arise from the inherent difficulty in precisely specifying the vertical distribution of cloud optical properties using passive satellite measurements. Motivated by the need to address this problem, CloudSat was launched in April 2006 carrying into orbit the first millimeter wavelength cloud radar to be flown in space. Retrieved profiles of liquid and ice cloud microphysical properties from this Cloud Profiling Radar form the basis of the CloudSat's fluxes and heating rates algorithm, 2B-FLXHR, a standard product that provides high vertical resolution profiles of radiative fluxes and atmospheric heating rates on the global scale. This paper describes the physical basis of the 2B-FLXHR algorithm and documents the first year of 2B-FLXHR data in the context of assessing the radiative impact of clouds on global and regional scales. The analysis confirms that cloud contributions to atmospheric radiative heating are small on the global scale because of a cancelation of the much larger regional heating from high clouds in the tropics and cooling from low clouds at higher latitudes. Preliminary efforts to assess the accuracy of the 2B-FLXHR product using coincident CERES data demonstrate that outgoing longwave fluxes are better represented than those in the shortwave but both exhibit good agreement with CERES on scales longer than 5 days and larger than 5 degrees. Colocated CALIPSO observations of clouds that are undetected by CloudSat further indicate that while thin cirrus can introduce modest uncertainty in the products, low clouds that are obscured by ground clutter represent a far more important source of error in the current 2B-FLXHR product that must be addressed in subsequent versions of the algorithm.
C1 [L'Ecuyer, Tristan S.; Wood, Norman B.; Haladay, Taryn; Stephens, Graeme L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Stackhouse, Paul W., Jr.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP L'Ecuyer, TS (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
EM tristan@atmos.colostate.edu
RI L'Ecuyer, Tristan/C-7040-2013; L'Ecuyer, Tristan/E-5607-2012
OI L'Ecuyer, Tristan/0000-0002-7584-4836
FU NASA CloudSat Mission [NAS5-99237]; NASA Energy and Water [NAG06GC46G]
FX This research was supported by NASA CloudSat Mission grant NAS5-99237
and NASA Energy and Water cycle Sponsored research (NEWS) grant
NAG06GC46G. The authors thank the staff at the CloudSat Data Processing
Center (DPC) and, in particular, Philip Partain for their assistance in
implementing the FLXHR algorithm. All CloudSat data presented here were
acquired through the DPC and can be accessed through their Web site
http://www.cloudsat.cira.colostate.edu. The authors would also like to
acknowledge Ed Eloranta and the University of Wisconsin Lidar Group
(http://lidar.ssec.wisc.edu/) for graciously providing the AHSRL and
MMCR data used in this study.
NR 51
TC 67
Z9 68
U1 2
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD DEC 6
PY 2008
VL 113
AR D00A15
DI 10.1029/2008JD009951
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 380NN
UT WOS:000261472500002
ER
PT J
AU Huang, D
Liu, YG
Wiscombe, W
AF Huang, Dong
Liu, Yangang
Wiscombe, Warren
TI Cloud tomography: Role of constraints and a new algorithm
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID INVERSION
AB Retrieving spatial distributions of cloud liquid water content from limited-angle emission data (passive microwave cloud tomography) is ill-posed, and a small inaccuracy in the data and/or numerical treatments may result in a large error in the retrieval. Proper handling of the ill-posedness is an ongoing challenge to the atmospheric remote sensing community. In this paper we first analyze the major regularization methods that each apply a single but different constraint to their retrievals and extend these methods to allow for multiple constraints. We then develop a new iterative algorithm that can also incorporate complex physical constraints with great flexibility. To understand the influences of different constraints on the retrievals, we use the new iterative algorithm with various combinations of constraints to retrieve a stratocumulus cloud simulated with a large-eddy-simulation model. For this relatively homogeneous cloud case, the standard least squares method with no constraints, as expected, performs very poorly, and yields a very large retrieval error, making this method nearly useless. Adding a nonnegativity constraint reduces the mean retrieval error by a factor of 6 but the internal structure of the cloud is still not reproduced in the retrieval. Adding a smoothness constraint dramatically improves the retrieved spatial structure of the cloud, and brings the mean error down further, although the retrieved cloud top edges are still considerably blurred. Further adding the so-called double-side constraint (based on scaled adiabatic profiles) produces the best result; the retrieval faithfully reproduces the cloud water structure with a mean retrieval error of only one third of that of the nonnegativity and smoothness constrained method.
C1 [Huang, Dong; Liu, Yangang; Wiscombe, Warren] Brookhaven Natl Lab, Dept Environm Sci, Upton, NY 11973 USA.
[Wiscombe, Warren] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Huang, D (reprint author), Brookhaven Natl Lab, Dept Environm Sci, 75 Rutherford Dr, Upton, NY 11973 USA.
EM dhuang@bnl.gov
RI Liu, Yangang/H-6154-2011; Wiscombe, Warren/D-4665-2012; Huang,
Dong/H-7318-2014
OI Wiscombe, Warren/0000-0001-6844-9849; Huang, Dong/0000-0001-9715-6922
NR 20
TC 5
Z9 7
U1 2
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD DEC 5
PY 2008
VL 113
AR D23203
DI 10.1029/2008JD009952
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 380NL
UT WOS:000261472300004
ER
PT J
AU Lui, ATY
Angelopoulos, V
LeContel, O
Frey, H
Donovan, E
Sibeck, DG
Liu, W
Auster, HU
Larson, D
Li, X
Nose, M
Fillingim, MO
AF Lui, A. T. Y.
Angelopoulos, V.
LeContel, O.
Frey, H.
Donovan, E.
Sibeck, D. G.
Liu, W.
Auster, H. U.
Larson, D.
Li, X.
Nose, M.
Fillingim, M. O.
TI Determination of the substorm initiation region from a major conjunction
interval of THEMIS satellites
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EARTH PLASMA SHEET; MAGNETIC-FIELD OBSERVATIONS; THIN CURRENT SHEETS;
BURSTY BULK FLOWS; BALLOONING INSTABILITY; CURRENT DISRUPTION; NEUTRAL
LINE; PRESSURE-GRADIENT; AURORAL SUBSTORM; EXPANSION PHASE
AB We investigate in detail the time history of substorm disturbances in the magnetotail observed during a major tail conjunction of Time History of Events and Macroscale Interactions during Substorms (THEMIS) satellites on 29 January 2008, 0700-0900 UT. During this interval, all THEMIS satellites were closely aligned along the tail axis near midnight and were bracketed in local time by GOES 11 and 12. The radial distance covered ranges from the geosynchronous altitude to similar to 30 R-E in the tail. This interval consists of three activations detected by the THEMIS satellites with good ground all-sky-camera observations of auroral activity. The first activation is a small substorm with spatially limited disturbance in the tail. The onset arc was equatorward of an undisturbed arc. The second activation is a moderate size substorm with the onset arc also being equatorward of an undisturbed arc. The third activation is an intensification of the substorm with its onset indicated by the second activation. The active auroral arc for this intensification was near the poleward boundary of the auroral oval. Analysis of these observations indicates that the first activation is a small substorm initiated in the near-Earth plasma sheet and does not involve magnetic reconnection of open magnetic field lines. Magnetic reconnection on closed field lines can be ruled out for this substorm because it cannot generate the observed high-speed plasma flow. The second and third activations are part of a moderate size substorm initiated also in the near-Earth plasma sheet, with a subsequent substorm intensification involving activity initiated tailward of similar to 30 R-E. Overall, the time history of substorm activity for these two substorms is consistent with the near-Earth initiation model.
C1 [Lui, A. T. Y.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Nose, M.] Kyoto Univ, Dept Geophys, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Laurel, MD 20723 USA.
[Liu, W.; Li, X.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
[LeContel, O.] Ctr Etud Environm Terr & Planetaires, Inst Pierre Simon Laplace, F-78140 Velizy Villacoublay, France.
[Frey, H.; Larson, D.; Fillingim, M. O.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Donovan, E.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Auster, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany.
[Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
RP Lui, ATY (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM tony.lui@jhuapl.edu
RI Sibeck, David/D-4424-2012; Liu, Wenlong/G-5585-2013; Nose,
Masahito/B-1900-2015
OI Liu, Wenlong/0000-0001-7991-5067; Nose, Masahito/0000-0002-2789-3588
FU NASA [NAS5-02099, NNX07AU74G]; NSF [ATM-0630912]; German Zentrum fur
Luft- und Raumfahrt [50QP0402]
FX We thank J.P. McFadden, J.W. Bonnell, and H. Singer for availability of
THEMIS ESA data, THEMIS EFI data, and GOES magnetometer data,
respectively. This work was supported by the NASA contract NAS5-02099 to
University of California, Berkeley, by the NSF grant ATM-0630912 and
NASA grant NNX07AU74G to The Johns Hopkins University Applied Physics
Laboratory, and by the German Ministerium fur Wirtschaft und Technologie
and the German Zentrum fur Luft- und Raumfahrt under grant 50QP0402.
NR 68
TC 34
Z9 34
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD DEC 5
PY 2008
VL 113
AR A00C04
DI 10.1029/2008JA013424
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 380PC
UT WOS:000261476600001
ER
PT J
AU Lawson, JW
Bauschlicher, CW
Toulouse, J
Filippi, C
Umrigar, CJ
AF Lawson, John W.
Bauschlicher, Charles W., Jr.
Toulouse, Julien
Filippi, Claudia
Umrigar, C. J.
TI Quantum Monte Carlo study of the cooperative binding of NO(2) to
fragment models of carbon nanotubes
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
ID CORRELATION-ENERGY; DENSITY; PSEUDOPOTENTIALS; EXCHANGE; ACCURATE
AB Previous calculations on model systems for the cooperative binding of two NO(2) molecules to carbon nanotubes using density functional theory and second order Moller-Plesset perturbation theory gave results differing by 30 kcal/mol. Quantum Monte Carlo calculations are performed to study the role of electronic correlations in these systems and resolve the discrepancy between these previous calculations. Compared to QMC binding energies, MP2 and LDA are shown to overbind, while B3LYP and BPW91 underbind. PW91 gives the best agreement with QMC with a binding energy differing by only 3 kcal/mol. Basis set effects are also shown to be important. Published by Elsevier B. V.
C1 [Lawson, John W.] NASA, Ames Res Ctr, Space Technol, Moffett Field, CA 94035 USA.
[Toulouse, Julien] Univ Paris 06, Chim Theor Lab, Paris, France.
[Toulouse, Julien] CNRS, Paris, France.
[Filippi, Claudia] Leiden Univ, Inst Lorentz, NL-2300 RA Leiden, Netherlands.
[Filippi, Claudia] Univ Twente, Fac Sci & Technol, NL-7500 AE Enschede, Netherlands.
[Filippi, Claudia] Univ Twente, MESA Res Inst, NL-7500 AE Enschede, Netherlands.
[Umrigar, C. J.] Cornell Univ, Atom & Solid State Phys Lab, Ithaca, NY 14853 USA.
RP Lawson, JW (reprint author), NASA, Ames Res Ctr, Space Technol, Mail Stop 229-1, Moffett Field, CA 94035 USA.
EM John.W.Lawson@nasa.gov
RI Toulouse, Julien/A-1376-2010
FU NASA Ames DDF; European Marie Curie Outgoing International Fellowship
[039750-QMC-DFT]; NSF; DOE
FX J.W.L. and C. W. B. are civil servants in the TS Division ( Mail Stop
229-1). This work was funded in part by grants from the NASA Ames DDF,
European Marie Curie Outgoing International Fellowship (039750-QMC-DFT),
the NSF and the DOE.
NR 29
TC 7
Z9 7
U1 0
U2 3
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 DEC 4
PY 2008
VL 466
IS 4-6
BP 170
EP 175
DI 10.1016/j.cplett.2008.10.066
PG 6
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 376LC
UT WOS:000261184100014
ER
PT J
AU Zeng, N
Yoon, JH
Vintzileos, A
Collatz, GJ
Kalnay, E
Mariotti, A
Kumar, A
Busalacchi, A
Lord, S
AF Zeng, Ning
Yoon, Jin-Ho
Vintzileos, Augustin
Collatz, G. James
Kalnay, Eugenia
Mariotti, Annarita
Kumar, Arun
Busalacchi, Antonio
Lord, Stephen
TI Dynamical prediction of terrestrial ecosystems and the global carbon
cycle: A 25-year hindcast experiment
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
ID NINO-SOUTHERN-OSCILLATION; EQUATORIAL PACIFIC; FORECAST SYSTEM;
ATMOSPHERIC CO2; MODEL; SIMULATION; ENSO
AB Using a 25-year hindcast experiment, we explore the possibility of seasonal-interannual prediction of terrestrial ecosystems and the global carbon cycle. This has been achieved using a prototype forecasting system in which the dynamic vegetation and terrestrial carbon cycle model VEGAS was forced with 15-member ensemble climate predictions generated by the NOAA/NCEP coupled climate forecasting system (CFS) for the period 1981-2005, with lead times up to 9 months. The results show that the predictability is dominated by the ENSO signal with its major influence on the tropical and subtropical regions, including South America, Indonesia, southern Africa, eastern Australia, western United States, and central Asia. There is also important non-ENSO related predictability such as that associated with midlatitude drought. Comparison of the dynamical prediction results with benchmark statistical prediction methods such as anomaly persistence and damping show that the dynamical method performs significantly better. The hindcasted ecosystem variables and carbon flux show significantly slower decrease in skill at longer lead time compared to the climate forcing variables, partly because of the memories in land and vegetation processes that filter out the higher-frequency noise and sustain the signal.
C1 [Zeng, Ning; Yoon, Jin-Ho; Kalnay, Eugenia; Busalacchi, Antonio] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Zeng, Ning; Mariotti, Annarita; Busalacchi, Antonio] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Collatz, G. James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kumar, Arun] NOAA, Climate Predict Ctr, Camp Springs, MD 20746 USA.
[Vintzileos, Augustin; Lord, Stephen] NOAA, Environm Modeling Ctr, Camp Springs, MD 20746 USA.
[Mariotti, Annarita] ENEA Casaccia, Rome, Italy.
RP Zeng, N (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM zeng@atmos.umd.edu
RI Kalnay, Eugenia/F-4393-2010; collatz, george/D-5381-2012; Zeng,
Ning/A-3130-2008; YOON, JIN-HO/A-1672-2009;
OI Zeng, Ning/0000-0002-7489-7629; YOON, JIN-HO/0000-0002-4939-8078;
Kalnay, Eugenia/0000-0002-9984-9906
FU NOAA [NA04OAR4310091, NA04OAR4310114]; NSF [ATM0739677]; NASA
[407191AG7]
FX We thank S. Saha for discussion on CFS and NOAA/NCEP for making the CFS
data available. Discussions with K. Mitchell and W. Higgins were helpful
in improving our manuscript. The manuscript was significantly improved
because of the comments from the Associate Editor Jim Randerson, Peter
Rayner, and another anonymous reviewer. This research was supported by
NOAA grants NA04OAR4310091 and NA04OAR4310114, NSF grant ATM0739677, and
NASA grant 407191AG7.
NR 32
TC 2
Z9 2
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0886-6236
EI 1944-9224
J9 GLOBAL BIOGEOCHEM CY
JI Glob. Biogeochem. Cycle
PD DEC 4
PY 2008
VL 22
IS 4
AR GB4015
DI 10.1029/2008GB003183
PG 13
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA 380MT
UT WOS:000261470500003
ER
PT J
AU Sergienko, OV
Bindschadler, RA
Vornberger, PL
MacAyeal, DR
AF Sergienko, O. V.
Bindschadler, R. A.
Vornberger, P. L.
MacAyeal, D. R.
TI Ice stream basal conditions from block-wise surface data inversion and
simple regression models of ice stream flow: Application to Bindschadler
Ice Stream
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
ID WEST ANTARCTICA; BENEATH; SHEET
AB [1] Widespread basal conditions controlling ice stream flows are still beyond the scope of direct observation, thus knowledge of their magnitudes and variabilities comes from inversion of surface measurements: ice velocities, surface elevations, and thicknesses. We present a new approach to implement a widely accepted inverse method on regular (10 x 10 km) blocks, smaller than the whole domain, to enhance the spatial resolution of calculated basal conditions. Inverted basal friction coefficients and calculated shear stress have sharp transitions and large variations in small areas. Overall, the obtained basal shear stress is very small in regions of fast flowing ice. The results of the inversion, along with the surface variables, are used to construct two simple regression models of Bindschadler Ice Stream ( former Ice Stream D) that reproduce 96% of observed velocity variations. While highly idealized, these regression models are sufficiently informative to be considered as parameterizations for ice stream flow in large-scale ice sheet models which lack the spatial and temporal resolution necessary to simulate ice stream dynamics in detail.
C1 [Sergienko, O. V.] Portland State Univ, Dept Geol, Portland, OR 97207 USA.
[Bindschadler, R. A.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[MacAyeal, D. R.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Vornberger, P. L.] Sci Applicat Int Corp, Beltsville, MD 20705 USA.
RP Sergienko, OV (reprint author), Portland State Univ, Dept Geol, POB 751, Portland, OR 97207 USA.
EM sergienk@pdx.edu
OI MacAyeal, Douglas/0000-0003-0647-6176
FU NASA Postdoctoral Program at the Goddard Space Flight Center; Oak Ridge
Associated Universities; NSF [OPP-0632168, OPP-0229546]
FX We thank the associated editor, Shawn Marshall, Hilmar Gudmundsson, and
anonymous reviewer for insightful comments and valuable suggestions that
helped to improve the manuscript. O.V.S. 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, and by NSF grant OPP-0632168. D. R. M.' s participation was
supported by NSF OPP- 0229546.
NR 21
TC 11
Z9 11
U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9003
EI 2169-9011
J9 J GEOPHYS RES-EARTH
JI J. Geophys. Res.-Earth Surf.
PD DEC 4
PY 2008
VL 113
IS F4
AR F04010
DI 10.1029/2008JF001004
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA 380OF
UT WOS:000261474300001
ER
PT J
AU Konca, AO
Avouac, JP
Sladen, A
Meltzner, AJ
Sieh, K
Fang, P
Li, ZH
Galetzka, J
Genrich, J
Chlieh, M
Natawidjaja, DH
Bock, Y
Fielding, EJ
Ji, C
Helmberger, DV
AF Konca, A. Ozgun
Avouac, Jean-Philippe
Sladen, Anthony
Meltzner, Aron J.
Sieh, Kerry
Fang, Peng
Li, Zhenhong
Galetzka, John
Genrich, Jeff
Chlieh, Mohamed
Natawidjaja, Danny H.
Bock, Yehuda
Fielding, Eric J.
Ji, Chen
Helmberger, Don V.
TI Partial rupture of a locked patch of the Sumatra megathrust during the
2007 earthquake sequence
SO NATURE
LA English
DT Article
ID SUBDUCTION ZONE EARTHQUAKES; ANDAMAN EARTHQUAKE; DEFORMATION; ASPERITY;
MODEL; SLIP
AB The great Sumatra - Andaman earthquake and tsunami of 2004 was a dramatic reminder of the importance of understanding the seismic and tsunami hazards of subduction zones(1-4). In March 2005, the Sunda megathrust ruptured again, producing an event(5) of moment magnitude (M(w)) 8.6 south of the 2004 rupture area, which was the site of a similar event in 1861 (ref. 6). Concern was then focused on the Mentawai area, where large earthquakes had occurred in 1797 ( M(w) = 8.8) and 1833 (M(w) = 9.0)(6,7). Two earthquakes, one of M(w) = 8.4 and, twelve hours later, one of M(w) = 7.9, indeed occurred there on 12 September 2007. Here we show that these earthquakes ruptured only a fraction of the area ruptured in 1833 and consist of distinct asperities within a patch of the megathrust that had remained locked in the interseismic period. This indicates that the same portion of a megathrust can rupture in different patterns depending on whether asperities break as isolated seismic events or cooperate to produce a larger rupture. This variability probably arises from the influence of non- permanent barriers, zones with locally lower pre- stress due to the past earthquakes. The stress state of the portion of the Sunda megathrust that had ruptured in 1833 and 1797 was probably not adequate for the development of a single large rupture in 2007. Themoment released in 2007 amounts to only a fraction both of that released in 1833 and of the deficit of moment that had accumulated as a result of interseismic strain since 1833. The potential for a large megathrust event in the Mentawai area thus remains large.
C1 [Konca, A. Ozgun; Avouac, Jean-Philippe; Sladen, Anthony; Meltzner, Aron J.; Sieh, Kerry; Galetzka, John; Genrich, Jeff; Natawidjaja, Danny H.; Helmberger, Don V.] CALTECH, Tecton Observ, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Fang, Peng; Bock, Yehuda] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Li, Zhenhong] Univ Glasgow, COMET, Dept Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland.
[Chlieh, Mohamed] Univ Nice Sophia Antipolis, Inst Rech Dev, Observ Cote Azur, F-06560 Valbonne, France.
[Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ji, Chen] Univ Calif Santa Barbara, Dept Geol Sci, Santa Barbara, CA 94106 USA.
RP Avouac, JP (reprint author), CALTECH, Tecton Observ, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM avouac@gps.caltech.edu
RI Meltzner, Aron/A-5585-2009; Li, Zhenhong/F-8705-2010; Avouac,
Jean-Philippe/B-5699-2015; Fielding, Eric/A-1288-2007; Sladen,
Anthony/A-2532-2017
OI Meltzner, Aron/0000-0002-2955-0896; 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 NSF [EAR-0538333]; Gordon and Betty Moore Foundation
FX This study was partly funded by the NSF (grant EAR-0538333) and the
Gordon and Betty Moore Foundation. This is Caltech Tectonics Observatory
contribution no. 93. We thank R. Burgmann for comments and suggestions.
NR 30
TC 141
Z9 145
U1 0
U2 27
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD DEC 4
PY 2008
VL 456
IS 7222
BP 631
EP 635
DI 10.1038/nature07572
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 378QW
UT WOS:000261340000039
PM 19052626
ER
PT J
AU Plante, I
Cucinotta, FA
AF Plante, Ianik
Cucinotta, Francis A.
TI Ionization and excitation cross sections for the interaction of HZE
particles in liquid water and application to Monte Carlo simulation of
radiation tracks
SO NEW JOURNAL OF PHYSICS
LA English
DT Article
ID ELECTRONS; RANGE; IONS
AB Relativistic heavy ions of high charge (Z) and energy (E) (HZE) in galactic cosmic rays (GCR) are important contributors to space radiation risk because they cannot be shielded completely and their relative biological effectiveness is very high. To understand these risks, Monte Carlo track structure simulations by radiation transport codes are widely used in radiation biology to provide information on energy deposition and production of radiolytic species that damage cellular structures. In this paper, we show that relativistic corrections can be applied to existing semi-empirical cross section models for the ionization and excitation of water molecules by ions to extend the validity of their energy range up to similar to 10(4) MeV amu(-1). Similarly, an effective charge value correction is applied for Z > 2 ions. Simulations of HZE tracks have been performed by a new C++ Monte Carlo transport code, named RITRACKS, that uses these cross sections to calculate the stopping power, radial dose, XY-plane projections of track segments and radial distributions of primary radiolytic species (H-center dot, (OH)-O-center dot, H-2, H2O2 and e(aq)(-)) at similar to 10(-12) s. These new data will be useful to understand results from experiments performed at ion accelerators by discriminating the role of the so-called core and penumbra of the tracks.
C1 [Plante, Ianik; Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Plante, Ianik] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
RP Plante, I (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM Ianik.Plante@USherbrooke.ca; Francis.A.Cucinotta@nasa.gov
FU NASA Space Radiation Risk Assessment Project
FX This research was supported by the NASA Space Radiation Risk Assessment
Project.
NR 21
TC 32
Z9 33
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1367-2630
J9 NEW J PHYS
JI New J. Phys.
PD DEC 4
PY 2008
VL 10
AR 125020
DI 10.1088/1367-2630/10/12/125020
PG 15
WC Physics, Multidisciplinary
SC Physics
GA 380MQ
UT WOS:000261470200004
ER
PT J
AU Palacios, C
Zettler, E
Amils, R
Amaral-Zettler, L
AF Palacios, Carmen
Zettler, Erik
Amils, Ricardo
Amaral-Zettler, Linda
TI Contrasting Microbial Community Assembly Hypotheses: A Reconciling Tale
from the Rio Tinto
SO PLOS ONE
LA English
DT Article
ID EXTREME ACIDIC ENVIRONMENT; SPECIES RICHNESS; DIVERSITY; RIVER; ECOLOGY;
SPAIN; BACTERIOPLANKTON; SEQUENCES; CHANCE; UNITS
AB Background: The Rio Tinto (RT) is distinguished from other acid mine drainage systems by its natural and ancient origins. Microbial life from all three domains flourishes in this ecosystem, but bacteria dominate metabolic processes that perpetuate environmental extremes. While the patchy geochemistry of the RT likely influences the dynamics of bacterial populations, demonstrating which environmental variables shape microbial diversity and unveiling the mechanisms underlying observed patterns, remain major challenges in microbial ecology whose answers rely upon detailed assessments of community structures coupled with fine-scale measurements of physico-chemical parameters.
Methodology/Principal Findings: By using high-throughput environmental tag sequencing we achieved saturation of richness estimators for the first time in the RT. We found that environmental factors dictate the distribution of the most abundant taxa in this system, but stochastic niche differentiation processes, such as mutation and dispersal, also contribute to observed diversity patterns.
Conclusions/Significance: We predict that studies providing clues to the evolutionary and ecological processes underlying microbial distributions will reconcile the ongoing debate between the Baas Becking vs. Hubbell community assembly hypotheses.
C1 [Palacios, Carmen; Amaral-Zettler, Linda] Josephine Bay Paul Ctr Comparat Mol Biol & Evolut, Marine Biol Lab, Woods Hole, MA USA.
[Palacios, Carmen; Amaral-Zettler, Linda] NASA Astrobiol Inst, Marine Biol Lab, Woods Hole, MA USA.
[Zettler, Erik; Amils, Ricardo] Univ Autonoma Madrid, Ctr Biol Mol, E-28049 Madrid, Spain.
[Zettler, Erik] Sea Educ Assoc, Woods Hole, MA USA.
[Amils, Ricardo] INTA CSIC, Ctr Astrobiol, Torrejon de Ardoz, Spain.
RP Palacios, C (reprint author), Univ Perpignan Via Domitia, CNRS EPHE UPVD, UMR 5244, Ctr Biol & Ecol Trop & Mediterraneenne,Equipe Par, Perpignan, France.
EM amaral@mbl.edu
RI Palacios, Carmen/A-6255-2010
FU NASA Astrobiology Institute [NC-1054 LAZ]; Ministry of Science and
Education [CGL2006/02534/BOS RA]; Spanish Centro de Astrobiologia
FX This work was supported by grants from NASA Astrobiology Institute
(NC-1054 LAZ) and from the Ministry of Science and Education
(CGL2006/02534/BOS RA) and support to CP by the Spanish Centro de
Astrobiologia. The funders had no role in study design, data collection
and analysis, decision to publish, or preparation of the manuscript.
NR 52
TC 24
Z9 24
U1 2
U2 18
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD DEC 4
PY 2008
VL 3
IS 12
AR e3853
DI 10.1371/journal.pone.0003853
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 436YO
UT WOS:000265452200006
PM 19052647
ER
PT J
AU Famiglietti, JS
Ryu, D
Berg, AA
Rodell, M
Jackson, TJ
AF Famiglietti, James S.
Ryu, Dongryeol
Berg, Aaron A.
Rodell, Matthew
Jackson, Thomas J.
TI Reply to comment by H. Vereecken et al. on "Field observations of soil
moisture variability across scales"
SO WATER RESOURCES RESEARCH
LA English
DT Editorial Material
C1 [Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Berg, Aaron A.] Univ Guelph, Dept Geog, Guelph, ON N1G 2W1, Canada.
[Ryu, Dongryeol; Jackson, Thomas J.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA.
[Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP Famiglietti, JS (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
RI Rodell, Matthew/E-4946-2012; Ryu, Dongryeol/C-5903-2008
OI Rodell, Matthew/0000-0003-0106-7437; Ryu, Dongryeol/0000-0002-5335-6209
NR 6
TC 2
Z9 2
U1 1
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
J9 WATER RESOUR RES
JI Water Resour. Res.
PD DEC 4
PY 2008
VL 44
IS 12
AR W12602
DI 10.1029/2008WR007323
PG 2
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 380PV
UT WOS:000261478500004
ER
PT J
AU Kuhlman, KR
Venkat, P
La Duc, MT
Kuhlman, GM
Mckay, CP
AF Kuhlman, Kimberly R.
Venkat, Parth
La Duc, Myron T.
Kuhlman, Gregory M.
Mckay, Christopher P.
TI Evidence of a microbial community associated with rock varnish at
Yungay, Atacama Desert, Chile
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Review
ID BIOLOGICAL SOIL CRUSTS; RIBOSOMAL-RNA ANALYSIS; PROJECT RDP-II;
HYPERARID CORE; RADIOCARBON MEASUREMENTS; PHYLOGENETIC DIVERSITY;
SUPEROXIDE-DISMUTASE; RADIATION-RESISTANCE; MICROCOLONIAL FUNGI; WHIPPLE
MOUNTAINS
AB Rock varnish is a very slow-growing nanostratigraphic coating consisting of approximately 70% fine-grained clay and 30% iron and manganese oxides that forms on the surfaces of rocks in arid and semiarid climates. The microbial diversity associated with rock varnish collected from the hyperarid Yungay region of the Atacama Desert was investigated using culture-independent biomolecular methods and an adenosine triphosphate (ATP) assay. The extraction of DNA from rock varnish collected at Yungay, a region in which little to no DNA has been extracted from the surface soil (<1 cm) to date, indicates that rock varnish may provide a niche habitat for microbial life where water is essentially absent. The clone library constructed suggests the presence of numerous phylogenetically distinct microorganisms, ranging in diversity from Cyanobacterial to a a-proteobacteria lineages. The findings also show that only a few micrometers of varnish material are enough to shelter microbes like Chroococcidiopsis spp. from the intense ultraviolet radiation present in the Atacama Desert. Whether or not microorganisms are involved in its nucleation and/or growth, rock varnish appears to provide a microhabitat resembling cryptoendolithic communities seen on a larger scale.
C1 [Kuhlman, Kimberly R.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Kuhlman, Gregory M.] Univ Wisconsin, Madison, WI 53706 USA.
[La Duc, Myron T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Venkat, Parth] CALTECH, Pasadena, CA 91106 USA.
RP Kuhlman, KR (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA.
EM kim@psi.edu; parthvenkat@gmail.com; myron.t.laduc@jpl.nasa.gov;
gmkuhlman@wisc.edu; cmckay@arc.nasa.gov
FU Jet Propulsion Laboratory's Director's Research and Development Fund
(DRDF); NASA's Astrobiology Science and Technology Instrument
Development (ASTID) Program
FX We wish to thank Diana Northup, University of New Mexico, Ronald
Crawford, University of Idaho, and Janice Strap, University of Ontario
Institute of Technology, for constructive critical reviews of this work.
We also wish to thank Tanzhou Liu for his artful fabrication and imaging
of ultra-thin petrographic thin sections of rock varnish from Yungay.
This work was funded by the Jet Propulsion Laboratory's Director's
Research and Development Fund (DRDF) and by NASA's Astrobiology Science
and Technology Instrument Development (ASTID) Program.
NR 119
TC 19
Z9 19
U1 1
U2 26
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD DEC 3
PY 2008
VL 113
IS G4
AR G04022
DI 10.1029/2007JG000677
PG 14
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 380NW
UT WOS:000261473400001
ER
PT J
AU Galli, A
Fok, MC
Wurz, P
Barabash, S
Grigoriev, A
Futaana, Y
Holmstrom, M
Ekenback, A
Kallio, E
Gunell, H
AF Galli, A.
Fok, M. -C.
Wurz, P.
Barabash, S.
Grigoriev, A.
Futaana, Y.
Holmstroem, M.
Ekenbaeck, A.
Kallio, E.
Gunell, H.
TI Tailward flow of energetic neutral atoms observed at Venus
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID 1ST-ENA OBSERVATIONS; UPPER-ATMOSPHERE; MARS; HYDROGEN; ASPERA-4; OXYGEN
AB The Analyzer of Space Plasma and Energetic Atoms (ASPERA-4) experiment on Venus Express provides the first measurements of energetic neutral atoms (ENAs) from Venus. The results improve our knowledge on the interaction of the solar wind with a nonmagnetized planet and they present an observational constraint to existing plasma models. We characterize the tailward flow of hydrogen ENAs observed on the nightside by providing global images of the ENA intensity. The images show a highly concentrated tailward flow of hydrogen ENAs tangential to the Venus limb around the Sun's direction. No oxygen ENAs above the instrument threshold are detected. The observed ENA intensities are reproduced with a simple ENA model within a factor of 2, indicating that the observed hydrogen ENAs originate from shocked solar wind protons that charge exchange with the neutral hydrogen exosphere.
C1 [Galli, A.; Wurz, P.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Fok, M. -C.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Gunell, H.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[Kallio, E.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Barabash, S.; Grigoriev, A.; Futaana, Y.; Holmstroem, M.; Ekenbaeck, A.] Inst Rymdfys, Kiruna, Sweden.
RP Galli, A (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
EM wurz@space.unibe.ch
RI Fok, Mei-Ching/D-1626-2012; Gunell, Herbert/D-5611-2013; Kallio,
Esa/F-9410-2014;
OI Kallio, Esa/0000-0002-9791-804X; Gunell, Herbert/0000-0001-5379-1158
FU Swiss National Science Foundation
FX The ASPERA-4 experiment on the ESA Venus Express mission is a joint
effort between 16 laboratories in 11 countries, all sponsored by their
national agencies. We thank all these agencies as well as the various
departments/institutes hosting these efforts. The lead author wishes to
acknowledge the support of the Swiss National Science Foundation.
NR 25
TC 12
Z9 13
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 2
PY 2008
VL 113
AR E00B15
DI 10.1029/2008JE003096
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 380OM
UT WOS:000261475000001
ER
PT J
AU Teanby, NA
de Kok, R
Irwin, PGJ
Osprey, S
Vinatier, S
Gierasch, PJ
Read, PL
Flasar, FM
Conrath, BJ
Achterberg, RK
Bezard, B
Nixon, CA
Calcutt, SB
AF Teanby, N. A.
de Kok, R.
Irwin, P. G. J.
Osprey, S.
Vinatier, S.
Gierasch, P. J.
Read, P. L.
Flasar, F. M.
Conrath, B. J.
Achterberg, R. K.
Bezard, B.
Nixon, C. A.
Calcutt, S. B.
TI Titan's winter polar vortex structure revealed by chemical tracers
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID COMPOSITE INFRARED SPECTROMETER; GENERAL-CIRCULATION MODEL; MIDDLE
ATMOSPHERE; MERIDIONAL CIRCULATION; POTENTIAL-VORTICITY;
RADIATIVE-TRANSFER; CASSINI/CIRS DATA; GRAVITY-WAVES; STRATOSPHERE;
DYNAMICS
AB The winter polar vortex on Saturn's largest moon Titan has profound effects on atmospheric circulation and chemistry and for the current northern midwinter season is the major dynamical feature of Titan's stratosphere and mesosphere. We use 2 years of observations from Cassini's composite infrared spectrometer to determine cross sections of five independent chemical tracers (HCN, HC3N, C2H2, C3H4, and C4H2), which are then used to probe dynamical processes occurring within the vortex. Our results provide compelling evidence that the vortex acts as a strong mixing barrier in the stratosphere and mesosphere, effectively separating a tracer-enriched air mass in the north from air at lower latitudes. In the mesosphere, above the level of the vortex jet, a tracer-depleted zone extends away from the north pole toward the equator and enrichment is confined to high northern latitudes. However, below this level, mixing processes cause tongues of gas to extend away from the polar region toward the equator. These features are not reproduced by current general circulation models and suggest that a residual polar circulation is present and that waves and instabilities form a more important part of Titan's atmospheric dynamics than previously thought. We also observe an unexpected enrichment of C4H2 in the northern stratosphere, which suggests photochemical polymerization of C2H2. Our observations provide stringent new constraints for dynamical and photochemical models and identify key polar processes for the first time. Some of the processes we see have analogues in Earth's polar vortex, while others are unique to Titan.
C1 [de Kok, R.; Irwin, P. G. J.; Osprey, S.; Read, P. L.; Calcutt, S. B.] Univ Oxford, Oxford OX1 3PU, England.
[Achterberg, R. K.; Nixon, C. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Vinatier, S.; Bezard, B.] Observ Paris, LESIA, F-92195 Meudon, France.
[Gierasch, P. J.; Conrath, B. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Teanby, NA (reprint author), Univ Oxford, Oxford OX1 3PU, England.
EM teanby@atm.ox.ac.uk
RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Osprey,
Scott/P-6621-2016;
OI Nixon, Conor/0000-0001-9540-9121; Osprey, Scott/0000-0002-8751-1211;
Calcutt, Simon/0000-0002-0102-3170; Teanby,
Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X
FU UK Science and Technology Facilities Council
FX This research was funded by the UK Science and Technology Facilities
Council. The authors would like to thank the Cassini-CIRS instrument
team, without which this research would not have been possible. We also
thank Bryan Lawrence at the British Atmospheric Data Centre for
supplying the gravity wave parameterization code.
NR 59
TC 33
Z9 33
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD DEC 2
PY 2008
VL 113
IS E12
AR E12003
DI 10.1029/2008JE003218
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 380OO
UT WOS:000261475200003
ER
PT J
AU Soares, MCR
Rabiu, AB
Gopalswamy, N
Thompson, BJ
Davila, JM
Sobrinho, AA
AF Soares, M. C. Rabello
Rabiu, A. B.
Gopalswamy, N.
Thompson, B. J.
Davila, J. M.
Sobrinho, A. A.
TI Outreach activities during the 2006 total solar eclipse sponsored by the
International Heliophysical Year
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Solar eclipse; Education; Sun; Solar-terrestrial relations; Solar
system; Africa; Asia; South America
AB The International Heliophysical Year (IHY) is an international program of scientific research to advance our understanding of the physical processes that govern the Sun, Earth and heliosphere. It has a strong educational component, linking research and education. Here, we describe the outreach activities during the 2006 total solar eclipse sponsored by IHY. (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Soares, M. C. Rabello] Stanford Univ, HEPL Solar Phys, Stanford, CA 94305 USA.
[Rabiu, A. B.] Fed Univ Technol Akure, Dept Phys, Akure, Nigeria.
[Gopalswamy, N.; Thompson, B. J.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Solar Phys Branch, Greenbelt, MD 20771 USA.
[Sobrinho, A. A.] Ctr Fed Educ Tecnol Rio Grande do Norte, Natal, RN, Brazil.
RP Soares, MCR (reprint author), Stanford Univ, HEPL Solar Phys, 445 Via Palou, Stanford, CA 94305 USA.
EM csoares@sun.stanford.edu; tunderabiu@yahoo.com; antonioaraujo@cefetrn.br
RI Gopalswamy, Nat/D-3659-2012; Thompson, Barbara/C-9429-2012;
OI Rabello Soares, Maria Cristina/0000-0003-0172-3713
NR 11
TC 0
Z9 0
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 DEC 1
PY 2008
VL 42
IS 11
BP 1792
EP 1799
DI 10.1016/j.asr.2007.04.014
PG 8
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 381NP
UT WOS:000261543500003
ER
PT J
AU Mitchell, SE
Drobnes, E
Colina-Trujillo, MS
Noel-Storr, J
AF Mitchell, Sara E.
Drobnes, Emilie
Colina-Trujillo, M. Sol
Noel-Storr, Jacob
TI NASA Family Science Night: Changing perceptions one family at a time
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Family; Science; Parents; Parental involvement; Out-of-school;
Perceptions; Engagement; Middle school; Informal education
AB Parents and families have the greatest influence on children's attitudes towards education and career choices. If students' attitudes towards science, particularly the physical sciences, are not influenced positively by parental/familial attitudes, efforts to improve the quality of content and teaching of these subjects in school may be futile. Research shows that parental involvement increases student achievement outcomes, and family-oriented programs have a direct impact on student performance.
Based on this premise, the NASA Goddard Space Flight Center started a series of Family Science Nights for middle school students and their families. The program provides a non-threatening venue for families to explore the importance of science and technology in our daily lives by engaging in learning activities that change their perception and understanding of science - making it more practical and approachable for participants of all ages. Family Science Night strives to change the way that students and their families participate in science, within the program and beyond. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Mitchell, Sara E.] NASA, Goddard Space Flight Ctr, SP Syst & Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Drobnes, Emilie; Colina-Trujillo, M. Sol] NASA, Goddard Space Flight Ctr, ADNET & Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Noel-Storr, Jacob] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
RP Mitchell, SE (reprint author), NASA, Goddard Space Flight Ctr, SP Syst & Astrophys Sci Div, Code 660-1, Greenbelt, MD 20771 USA.
EM sara.mitchell@nasa.gov; emilie.drob-nes@nasa.gov;
mcolina@pop400.gsfc.nasa.gov; jake@cis.rit.edu
NR 5
TC 0
Z9 0
U1 2
U2 7
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 DEC 1
PY 2008
VL 42
IS 11
BP 1844
EP 1847
DI 10.1016/j.asr.2008.01.004
PG 4
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 381NP
UT WOS:000261543500010
ER
PT J
AU Beck-Winchatz, B
Riccobono, MA
AF Beck-Winchatz, Bernhard
Riccobono, Mark A.
TI Advancing participation of blind students in Science, Technology,
Engineering, and Math
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Science education; Special needs; Diversity; Blindness
AB Like their sighted peers, many blind students in elementary, middle, and high school are naturally interested in space. This interest can motivate them to learn fundamental scientific, quantitative, and critical thinking skills, and sometimes even lead to careers in Science, Technology, Engineering, and Math (STEM) disciplines. However, these students are often at a disadvantage in science because of the ubiquity of important graphical information that is generally not available in accessible formats, the unfamiliarity of teachers with non-visual teaching methods, lack of access to blind role models, and the low expectations of their teachers and parents. We discuss joint efforts by the National Aeronautics and Space Administration (NASA) and the National Federation of the Blind's (NFB) National Center for Blind Youth in Science (NCBYS) to develop and implement strategies to promote opportunities for blind youth in science. These include the development of tactile space science books and curriculum materials, science academies for blind middle school and high school students, and college-level internship and mentoring programs. The partnership with the NFB exemplifies the effectiveness of collaborations between NASA and consumer-directed organizations to improve opportunities for underserved and underrepresented individuals. (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Beck-Winchatz, Bernhard] De Paul Univ, NASA, SMD Broker Facilitator Program, Chicago, IL 60614 USA.
[Riccobono, Mark A.] Jernigan Inst, Baltimore, MD 21230 USA.
RP Beck-Winchatz, B (reprint author), De Paul Univ, NASA, SMD Broker Facilitator Program, 990 Fullerton,Suite 4400, Chicago, IL 60614 USA.
EM bbeckwin@depaul.edu
RI Duello, Theresa/P-5752-2015
NR 17
TC 9
Z9 9
U1 1
U2 23
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 DEC 1
PY 2008
VL 42
IS 11
BP 1855
EP 1858
DI 10.1016/j.asr.2007.05.080
PG 4
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 381NP
UT WOS:000261543500012
ER
PT J
AU Bering, EA
Bacon, L
Copper, KK
Hansen, LJ
Sanchez, MJ
AF Bering, E. A., III
Bacon, L.
Copper, K. K.
Hansen, L. J.
Sanchez, M. J.
TI The American Institute of Aeronautics and Astronautics pre-college
outreach program
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Education; Pre-college; National program
ID ASPIRATIONS; STUDENTS; ATTITUDE; SCIENCE; ADOLESCENTS; SCHOOL; FAMILY
AB Many United States, school children perceive science, technology, engineering, and mathematics (STEM) as difficult, boring and often irrelevant subjects. The possible reasons for this problem are endlessly debated. However, the economic, social, and overall national importance of producing graduates who are technically literate and enthusiastic in their support of a rational scientific world is essential to our nation. This apparent STEM crisis should motivate the many scientific and engineering societies to develop STEM outreach programs aimed at students, parents, teachers and schools (grades K-12).
The American Institute of Aeronautics and Astronautics (AIAA) is among those organizations that have identified the need to educate students and teachers about STEM current events and their direct effects on the United States population in a way that motivates both. The AIAA has established a pre-college outreach program that has several major elements that will be described in this paper. Elements focused on the teachers include a pre-college Educator Associate Membership program, classroom grants to support hands-on learning activities, Educator of the Year awards and recognition program and two national workshop events. The first workshop event, Passport to the Future, is held annually in conjunction with the Joint Propulsion Conference. It is intended to provide summertime training in Aerospace science education to classroom teachers, in conjunction with a national professional conference. The second workshop, Education Alley, is held in the fall in conjunction with the "Space" series of conferences. This program is aimed at direct outreach to local students in the conference host city, providing fun, interesting, and educational events that promote STEM. The AIAA also encourages and supports pre-college outreach activities sponsored by the local AIAA sections through leadership training, activity and material support. (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Bering, E. A., III] Univ Houston, Dept Phys, Houston, TX 77204 USA.
[Bering, E. A., III] Univ Houston, Dept Elect & Comp Engn, Houston, TX 77204 USA.
[Bacon, L.] Amer Inst Aeronaut & Astronaut, Reston, VA 20191 USA.
[Copper, K. K.] IDS, Boeing, Ofallon, MO 63366 USA.
[Hansen, L. J.] HRP Syst Inc, Torrance, CA 90503 USA.
[Sanchez, M. J.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
RP Bering, EA (reprint author), Univ Houston, Dept Phys, 617 Sci & Res Bldg 1, Houston, TX 77204 USA.
EM eabering@uh.edu; lisab@aiaa.org; karen.k.copper@boeing.com;
hansen@hrpsystems.com; merri.j.sanchez@nasa.gov
NR 16
TC 0
Z9 0
U1 1
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 DEC 1
PY 2008
VL 42
IS 11
BP 1869
EP 1878
DI 10.1016/j.asr.2007.11.009
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 381NP
UT WOS:000261543500015
ER
PT J
AU Thomas, JL
Diskin, B
Rumsey, CL
AF Thomas, James L.
Diskin, Boris
Rumsey, Christopher L.
TI Toward Verification of Unstructured-Grid Solvers
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT AIAA 46th Aerospace Sciences Meeting and Exhibit
CY JAN 07-10, 2008
CL Reno, NV
SP Amer Inst Aeronaut & Astronaut
ID NONUNIFORM MESHES; SCHEMES; ACCURACY; FLOWS
AB New methodology for verification of finite volume computational methods using unstructured grids is presented. The discretization-order properties are studied in computational windows, easily constructed within a collection of grids or a single grid. Tests are performed within each window and address a combination of problem-, solution-, and discretization/grid-related features affecting discretization-error convergence. The windows can be adjusted to isolate particular elements of the computational scheme, such as the interior discretization, the boundary discretization, or singularities. Studies can use traditional grid-refinement computations within a fixed window or downscaling, a recently introduced technique in which computations are made within windows contracting toward a focal point of interest. Grids within the windows are constrained to be consistently refined, allowing a meaningful assessment of asymptotic error convergence on unstructured grids. Demonstrations of the method are shown, including a comparative accuracy assessment of commonly used schemes on general mixed grids and the identification of local accuracy deterioration at boundary intersections. Recommendations to enable attainment of design-order discretization errors for large-scale computational simulations are given.
C1 [Thomas, James L.; Rumsey, Christopher L.] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA.
[Diskin, Boris] Natl Inst Aerosp, Hampton, VA 23666 USA.
RP Thomas, JL (reprint author), NASA, Langley Res Ctr, Computat Aerosci Branch, Mail Stop 128, Hampton, VA 23681 USA.
EM James.L.Thomas@nasa.gov; bdiskin@nianet.org; c.l.rumsey@nasa.gov
NR 24
TC 16
Z9 16
U1 2
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD DEC
PY 2008
VL 46
IS 12
BP 3070
EP 3079
DI 10.2514/1.36655
PG 10
WC Engineering, Aerospace
SC Engineering
GA 381IA
UT WOS:000261528000008
ER
PT J
AU Nichols, RH
Tramel, RW
Buning, PG
AF Nichols, Robert H.
Tramel, Robert W.
Buning, Pieter G.
TI Evaluation of Two High-Order Weighted Essentially Nonoscillatory Schemes
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT AIAA 25th Applied Aerodynamics Conference
CY JUN 25-28, 2007
CL Miami, FL
SP Amer Inst Aeronaut & Astronaut
ID EFFICIENT IMPLEMENTATION; CONSERVATION-LAWS; COMPUTATIONS; CYLINDER;
FLOWS; GRIDS; FORM
AB Two fifth-order spatial weighted essentially nonoscillatory schemes for the convective terms were added to the OVERFLOW 2 implicit overset Navier-Stokes flow solver. The method used to incorporate the schemes is similar to a monotone upstream-centered scheme for conservation laws and requires no modification of the viscous terms, transport equations, or turbulence models in the code. The new flux calculation schemes were applied to problems involving vortex convection, strong shocks, and large scale unsteady flows. The weighted essentially nonoscillatory schemes were found to have much lower numerical dissipation/dispersion than traditional third-order spatial monotone upstream-centered schemes for conservation laws. Both weighted essentially nonoscillatory schemes were numerically robust over a wide range of Mach numbers when solved using the existing implicit schemes within OVERFLOW 2. The weighted essentially nonoscillatory schemes also provided improved numerical accuracy over traditional third-order spatial monotone upstream-centered schemes for conservation laws on the same computational grid for all the applications examined here. The weighted essentially nonoscillatory schemes are 10-30% more expensive than the third-order spatial monotone upstream-centered schemes for conservation laws depending on choice of implicit solver.
C1 [Nichols, Robert H.] Univ Alabama Birmingham, Dept Mech Engn, Birmingham, AL 35294 USA.
[Tramel, Robert W.] Digital Fus Inc, Huntsville, AL 35806 USA.
[Buning, Pieter G.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
RP Nichols, RH (reprint author), Univ Alabama Birmingham, Dept Mech Engn, Birmingham, AL 35294 USA.
NR 34
TC 10
Z9 13
U1 0
U2 2
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 DEC
PY 2008
VL 46
IS 12
BP 3090
EP 3102
DI 10.2514/1.36849
PG 13
WC Engineering, Aerospace
SC Engineering
GA 381IA
UT WOS:000261528000010
ER
PT J
AU Kojima, J
Nguyen, QV
AF Kojima, Jun
Nguyen, Quang-Viet
TI Observation of Turbulent Mixing in Lean-Direct-Injection Combustion at
Elevated Pressure
SO AIAA JOURNAL
LA English
DT Article
ID SPONTANEOUS RAMAN-SCATTERING; LARGE-EDDY SIMULATION; TURBINE MODEL
COMBUSTOR; SIMULTANEOUS TEMPERATURE; HYDROCARBON FLAMES; LASER
DIAGNOSTICS; DIFFUSION FLAME; SWIRL FLAMES; GAS; SPECTROSCOPY
AB We report the first quantitative single-shot multiscalar data obtained from a realistic air-fed lean-direct-injection burner operating on gaseous methane (CH(4)) fuel at elevated pressure (5 atm) using single-shot spontaneous Raman spectroscopy. From a statistical analysis of the multiscalar data, we present spatially mapped probability density functions of the concentration of CH(4) and O(2), and the instantaneous temperature. The measured three-scalar correlations and probability density functions provide insights into the nature and extent of the mixing process and its impact on the subsequent combustion process. The data will also be useful for comparison with the various turbulence-chemistry interaction models such as large-eddy simulation. The swirl-stabilized flame investigated in this paper was characterized as operating in a partially premixed combustion regime that was dominated by turbulent mixing provided by the lean-direct-injection configuration. Although a majority of the single-shot data indicated complete or near-complete reactions including stoichiometric combustion, a considerable number of the data points exhibited incomplete combustion characterized by a substantial amount of residual fuel at intermediate temperatures or were simply unreacted with little or no preheating of the mixture.
C1 [Kojima, Jun] Ohio Aerosp Inst, Turbomachinery & Prop Syst Team, Cleveland, OH 44142 USA.
[Nguyen, Quang-Viet] NASA, John H Glenn Res Ctr Lewis Field, Combust Branch, Cleveland, OH 44135 USA.
RP Kojima, J (reprint author), Ohio Aerosp Inst, Turbomachinery & Prop Syst Team, Cleveland, OH 44142 USA.
FU NASA
FX The authors acknowledge financial support by the Supersonics program and
the Subsonic Fixed Wing program under Fundamental Aeronautics at NASA
John H. Glenn Research Center at Lewis Field. The authors also
acknowledge Gregg Calhoun for his assistance in the operation of the
facilities.
NR 51
TC 6
Z9 6
U1 1
U2 7
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD DEC
PY 2008
VL 46
IS 12
BP 3116
EP 3127
DI 10.2514/1.37433
PG 12
WC Engineering, Aerospace
SC Engineering
GA 381IA
UT WOS:000261528000012
ER
PT J
AU Yung, PT
Ponce, A
AF Yung, Pun To
Ponce, Adrian
TI Fast Sterility Assessment by Germinable-Endospore Biodosimetry
SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY
LA English
DT Article
ID BACTERIAL-SPORES; MEDICAL DEVICES; INACTIVATION; RESISTANCE; MODEL
AB The increased demand for sterile products has created the need for rapid technologies capable of validating the hygiene of industrial production processes. Bacillus endospores are in standard use as biological indicators for evaluating the effectiveness of sterilization processes. Currently, culture-based methods, requiring more than 2 days before results become available, are employed to verify endospore inactivation. We describe a rapid, microscopy-based endospore viability assay (mu EVA) capable of enumerating germinable endospores in less than 15 min. mu EVA employs time-gated luminescence microscopy to enumerate single germinable endospores via terbium-dipicolinate (Tb-DPA) luminescence, which is triggered under UV excitation as 10(8) DPA molecules are released during germination on agarose containing Tb(3+) and a germinant (e. g., L-alanine). Inactivation of endospore populations to sterility was monitored with mu EVA as a function of thermal and UV dosage. A comparison of culturing results yielded nearly identical decimal reduction values, thus validating mu EVA as a rapid biodosimetry method for monitoring sterilization processes. The simple Tb-DPA chemical test for germinability is envisioned to enable fully automated instrumentation for in-line monitoring of hygiene in industrial production processes.
C1 [Yung, Pun To; Ponce, Adrian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ponce, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM adrian.ponce@jpl.nasa.gov
FU NASA; National Aeronautic and Space Administration; NASA's Astrobiology
and Planetary Protection Programs; Department of Homeland Security's
Chemical and Biological Research & Development Program
FX P. T. Y. acknowledges support from the NASA postdoctoral program. The
research described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautic and Space Administration and was sponsored by NASA's
Astrobiology and Planetary Protection Programs and by the Department of
Homeland Security's Chemical and Biological Research & Development
Program.
NR 32
TC 18
Z9 18
U1 0
U2 8
PU AMER SOC MICROBIOLOGY
PI WASHINGTON
PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA
SN 0099-2240
J9 APPL ENVIRON MICROB
JI Appl. Environ. Microbiol.
PD DEC
PY 2008
VL 74
IS 24
BP 7669
EP 7674
DI 10.1128/AEM.01437-08
PG 6
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA 381CU
UT WOS:000261513700027
PM 18836020
ER
PT J
AU Osipov, VV
Muratov, CB
AF Osipov, V. V.
Muratov, C. B.
TI Dynamic condensation blocking in cryogenic refueling
SO APPLIED PHYSICS LETTERS
LA English
DT Article
DE condensation; cryogenics; heat conduction
ID EVAPORATION
AB We demonstrate that a negative feedback between vapor pressure and condensation rate may be established in two-phase systems during vapor compression with rates of practical importance. As a result, dynamic condensation blocking occurs. The effect is studied numerically in the case of filling a no-vent insulated tank by liquid hydrogen. It is shown that the filling dynamics quite sensitively depends on the filling rate, and for sufficiently fast filling rates consist of a fast stage dominated by gas compression and a slow stage governed by heat conduction in the liquid.
C1 [Osipov, V. V.] Mission Crit Technol Inc, El Segundo, CA 90245 USA.
[Osipov, V. V.] NASA, Ames Res Ctr, Intelligent Syst Div, D&SH Branch, Moffett Field, CA 94035 USA.
[Muratov, C. B.] New Jersey Inst Technol, Dept Math Sci, Newark, NJ 07102 USA.
RP Osipov, VV (reprint author), Mission Crit Technol Inc, 2041 Rosecrans Ave,Suite 225, El Segundo, CA 90245 USA.
EM muratov@njit.edu
FU NSF [DMS-0718027]
FX We are grateful to V.N. Smelyanskiy for suggesting this problem to us.
The work of C. B. M. was supported, in part, by NSF via Grant No.
DMS-0718027.
NR 13
TC 3
Z9 3
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 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD DEC 1
PY 2008
VL 93
IS 22
AR 224105
DI 10.1063/1.3025674
PG 3
WC Physics, Applied
SC Physics
GA 379XT
UT WOS:000261430600095
ER
PT J
AU Mouroulis, P
van Gorp, B
Blaney, D
Green, RO
AF Mouroulis, Pantazis
van Gorp, Byron
Blaney, Diana
Green, Robert O.
TI Reflectance Microspectroscopy of Natural Rock Samples in the Visible and
Near Infrared
SO APPLIED SPECTROSCOPY
LA English
DT Article
DE Reflectance spectroscopy; Microspectroscopy; Near-infrared region
ID IMAGING SPECTROSCOPY; SURFACE
AB We have collected reflectance spectra of various unprocessed rock samples in the 450-1650 nm wavelength range with a spatial resolution of 60 and 120 mu m (diameter) and using three illumination modes. Spectra taken in diffuse reflectance (dark field) mode are comparable to those obtained from macroscopic measurements and can provide the basis for mineral detection at that spatial scale. The spectral discrimination of the dark field mode is demonstrated to be consistent with the spatial resolution of the microscope for the samples examined. These results support the conclusion that reflectance microspectroscopy in the visible and near-infrared regions can be a valuable tool for understanding mineral formation at the spatial scale of tens of micrometers.
C1 [Mouroulis, Pantazis; van Gorp, Byron; Blaney, Diana; Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mouroulis, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM zakos@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research described here has been performed at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 22
TC 4
Z9 4
U1 1
U2 7
PU SOC APPLIED SPECTROSCOPY
PI FREDERICK
PA 201B BROADWAY ST, FREDERICK, MD 21701 USA
SN 0003-7028
J9 APPL SPECTROSC
JI Appl. Spectrosc.
PD DEC
PY 2008
VL 62
IS 12
BP 1370
EP 1377
PG 8
WC Instruments & Instrumentation; Spectroscopy
SC Instruments & Instrumentation; Spectroscopy
GA 382GT
UT WOS:000261594500013
PM 19094397
ER
PT J
AU Datiles, MB
Ansari, RR
Suh, KI
Vitale, S
Reed, GF
Zigler, JS
Ferris, FL
AF Datiles, Manuel B., III
Ansari, Rafat R.
Suh, Kwang I.
Vitale, Susan
Reed, George F.
Zigler, J. Samuel, Jr.
Ferris, Frederick L., III
TI Clinical Detection of Precataractous Lens Protein Changes Using Dynamic
Light Scattering
SO ARCHIVES OF OPHTHALMOLOGY
LA English
DT Article; Proceedings Paper
CT Annual Meeting of the
Association-for-Research-in-Vision-and-Ophthalmology
CY MAY 06-10, 2007
CL Ft Lauderdale, FL
SP Assoc Res Vis & Ophthalmol
ID BOVINE ALPHA-CRYSTALLIN; AGE-RELATED-CHANGES; LIVING HUMAN LENS;
MOLECULAR CHAPERONE; CATARACT FORMATION; GLUTATHIONE-REDUCTASE; NUCLEAR
CATARACT; FUNCTIONAL-ROLE; OPACIFICATION; EYE
AB Objective: To use dynamic light scattering to clinically assess early precataractous lens protein changes.
Methods: We performed a cross-sectional study in 380 eyes of 235 patients aged 7 to 86 years with Age-Related Eye Disease Study clinical nuclear lens opacity grades 0 to 3.8. A dynamic light-scattering device was used to assess alpha-crystallin, a molecular chaperone protein shown to bind other damaged lens proteins, preventing their aggregation. The outcome measure was the alpha-crystallin index, a measure of unbound alpha-crystallin in each lens. The association of the alpha-crystallin index with increasing nuclear opacity and aging was determined.
Results: There was a significant decrease in the alpha-crystallin index associated with increasing nuclear lens opacity grades (P<.001). There were significant losses of alpha-crystallin even in clinically clear lenses associated with aging (P<.001). The standard error of measurement was 3%.
Conclusions: Dynamic light scattering clinically detects alpha-crystallin protein loss even in clinically clear lenses. alpha-Crystallin index measurements may be useful in identifying patients at high risk for cataracts and as an outcome variable in clinical lens studies.
C1 [Datiles, Manuel B., III; Vitale, Susan; Reed, George F.; Zigler, J. Samuel, Jr.; Ferris, Frederick L., III] NEI, NIH, Bethesda, MD 20892 USA.
[Ansari, Rafat R.] NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH USA.
[Suh, Kwang I.] Ohio Aerosp Inst, Cleveland, OH USA.
RP Datiles, MB (reprint author), NEI, NIH, 10 Ctr Dr,Bldg 10,Room 10N226, Bethesda, MD 20892 USA.
EM DatilesM@NEI.NIH.GOV
OI Datiles, Manuel III B./0000-0003-4660-1664
FU Intramural NIH HHS [Z99 EY999999]
NR 52
TC 36
Z9 37
U1 1
U2 6
PU AMER MEDICAL ASSOC
PI CHICAGO
PA 515 N STATE ST, CHICAGO, IL 60610-0946 USA
SN 0003-9950
J9 ARCH OPHTHALMOL-CHIC
JI Arch. Ophthalmol.
PD DEC
PY 2008
VL 126
IS 12
BP 1687
EP 1693
DI 10.1001/archophthalmol.2008.507
PG 7
WC Ophthalmology
SC Ophthalmology
GA 380RA
UT WOS:000261481700011
PM 19064850
ER
PT J
AU Hausrath, EM
Treiman, AH
Vicenzi, E
Bish, DL
Blake, D
Sarrazin, P
Hoehler, T
Midtkandal, I
Steele, A
Brantley, SL
AF Hausrath, E. M.
Treiman, A. H.
Vicenzi, E.
Bish, D. L.
Blake, D.
Sarrazin, P.
Hoehler, T.
Midtkandal, I.
Steele, A.
Brantley, S. L.
TI Short- and Long-Term Olivine Weathering in Svalbard: Implications for
Mars
SO ASTROBIOLOGY
LA English
DT Article
DE Olivine; Weathering; Mars; Glass; Hydrothermal; CheMin
ID FORSTERITE DISSOLUTION RATES; ARCTIC ALPINE ENVIRONMENT; AQUEOUS
ALTERATION; NORTHERN SCANDINAVIA; SILICATE SURFACES; RIND DEVELOPMENT;
SWEDISH LAPLAND; ORGANIC-ACIDS; GUSEV CRATER; PH
AB Liquid water is essential to life as we know it on Earth; therefore, the search for water on Mars is a critical component of the search for life. Olivine, a mineral identified as present on Mars, has been proposed as an indicator of the duration and characteristics of water because it dissolves quickly, particularly under low-pH conditions. The duration of olivine persistence relative to glass under conditions of aqueous alteration reflects the pH and temperature of the reacting fluids. In this paper, we investigate the utility of 3 methodologies to detect silicate weathering in a Mars analog environment (Sverrefjell volcano, Svalbard). CheMin, a miniature Xray diffraction instrument developed for flight on NASA's upcoming Mars Science Laboratory, was deployed on Svalbard and was successful in detecting olivine and weathering products. The persistence of olivine and glass in Svalbard rocks was also investigated via laboratory observations of weathered hand samples as well as an in situ burial experiment. Observations of hand samples are consistent with the inference that olivine persists longer than glass at near-zero temperatures in the presence of solutions at pH similar to 7-9 on Svalbard, whereas in hydrothermally altered zones, glass has persisted longer than olivine in the presence of fluids at similar pH at similar to 50 degrees C. Analysis of the surfaces of olivine and glass samples, which were buried on Sverrefjell for 1 year and then retrieved, documented only minor incipient weathering, though these results suggest the importance of biological impacts. The 3 types of observations ( CheMin, laboratory observations of hand samples, burial experiments) of weathering of olivine and glass at Svalbard show promise for interpretation of weathering on Mars. Furthermore, the weathering relationships observed on Svalbard are consistent with laboratory-measured dissolution rates, which suggests that relative mineral dissolution rates in the laboratory, in concert with field observations, can be used to yield valuable information regarding the pH and temperature of reacting martian fluids.
C1 [Hausrath, E. M.; Brantley, S. L.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Hausrath, E. M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Treiman, A. H.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Vicenzi, E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Bish, D. L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Blake, D.; Hoehler, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sarrazin, P.] InXitu Inc, Mountain View, CA USA.
[Midtkandal, I.] Univ Oslo, Dept Geosci, Oslo, Norway.
[Steele, A.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA.
RP Hausrath, EM (reprint author), Univ Nevada, Dept Geosci, 4505 S Maryland Pkwy, Las Vegas, NV 89154 USA.
EM Elisabeth.Hausrath@unlv.edu
FU World Universities Network, BRIE [DGE-9972759]; Pennsylvania State
Astrobiology Research Center, NASA [NNG05GN72G]; NAI Research
Fellowship; NSF Graduate Research Fellowship Program
FX We would like to thank B. Abbey, M. Angelone, J. Cantolina, D. Voight,
C. Lernhihan, A. Barnes, V. Bojan, T. Daniels, C. Winslow, V. Starke,
and AMASE. We appreciate the thoughtful reviews by two anonymous
reviewers and Hojatollah Vali. This work was supported by funding from
the World Universities Network, BRIE [ Pennsylvania State NSF (IGERT)
grant DGE-9972759], Pennsylvania State Astrobiology Research Center,
NASA Grant NNG05GN72G, and the NAI Research Fellowship. E. M. H. is
grateful for support from the NSF Graduate Research Fellowship Program.
NR 77
TC 19
Z9 19
U1 3
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 DEC
PY 2008
VL 8
IS 6
BP 1079
EP 1092
DI 10.1089/ast.2007.0195
PG 14
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 409OX
UT WOS:000263516800003
PM 19191538
ER
PT J
AU Allen, CC
Oehler, DZ
AF Allen, Carlton C.
Oehler, Dorothy Z.
TI A Case for Ancient Springs in Arabia Terra, Mars
SO ASTROBIOLOGY
LA English
DT Article
DE Mars; Martian; Vernal Crater; Arabia Terra; Springs; Thermal springs;
Warm springs; Spring mounds; HiRISE; Hot springs; Astrobiology
ID HOT-SPRINGS; MERIDIANI PLANUM; THERMAL SPRINGS; IMPACT CRATER; DEPOSITS;
LIFE; PRESERVATION; SEARCH; SILICIFICATION; MORPHOLOGIES
AB Based on new image data from the High Resolution Imaging Science Experiment (HiRISE) on Mars Reconnaissance Orbiter (MRO), a case can be made that several structures in Vernal Crater, Arabia Terra are ancient springs. This interpretation is based on comprehensive geomorphologic analysis coupled with assessment of multiple hypotheses. The structures identified extend across several kilometers and are exceptional in that nothing with their detail and scale has been reported from Mars. The deposits are associated with an extensive fracture system that may have facilitated upward flow of warm fluids. Several additional spring-like features occur in Vernal Crater, and it is possible that these are part of a major province of spring activity. Since springs are environments where life could have evolved on Mars, where that life could have found refuge as the climate became colder and drier, and where signatures of that life may be preserved, Vernal Crater may be a site of major astrobiological importance.
C1 [Allen, Carlton C.; Oehler, Dorothy Z.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA.
RP Allen, CC (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA.
EM carlton.c.allen@nasa.gov
FU NASA; Astromaterials Research and Exploration Science Directorate;
Johnson Space Center (JSC); NASA fellowship
FX We thank NASA and the Astromaterials Research and Exploration Science
Directorate at the Johnson Space Center (JSC) for support. We are
grateful to Dr. Adrian Brown ( NASA Ames Research Center and SETI
Institute) for assistance with CRISM interpretation, Dr. Mary Bourke (
Planetary Science Institute) and Ms. Jaclyn Allen ( JSC) for examining
images of the spring-like features in Vernal Crater, Dr. Devon Burr for
helpful comments and insights, and Mr. Orrin Thomas ( JSC Image Science
and Analysis Group) for 3-D analysis of CTX images. The manuscript was
reviewed by Dr. Stephen Grasby ( Geological Survey of Canada), Dr. Larry
Crumpler ( New Mexico Museum of Natural History and Science), and an
anonymous reviewer, all of whom made important comments and suggestions.
We are grateful to Dr. David Beaty (NASA-JPL) for helpful discussions,
Dr. M. A. (Rien) Habermehl ( Australian Government Department of
Agriculture, Fisheries and Forestry) for providing information about
springs in the Great Artesian Basin and at Dalhousie, and Dr. Malcolm
Walter ( Australian Centre for Astrobiology) for encouragement. We thank
Google Earth for permission to use some of their images. This work was
partially funded by a NASA fellowship to D. Z. O.
NR 83
TC 39
Z9 40
U1 2
U2 10
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 DEC
PY 2008
VL 8
IS 6
BP 1093
EP 1112
DI 10.1089/ast.2008.0239
PG 20
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 409OX
UT WOS:000263516800004
PM 19093802
ER
PT J
AU Kempf, MJ
Schubert, WW
Beaudet, RA
AF Kempf, M. J.
Schubert, W. W.
Beaudet, R. A.
TI Determination of Lethality Rate Constants and D-Values for Bacillus
atrophaeus (ATCC 9372) Spores Exposed to Dry Heat from 115 degrees C to
170 degrees C
SO ASTROBIOLOGY
LA English
DT Article
DE Bacillus atrophaeus spores; Planetary protection; Dry heat microbial
reduction
ID SUBTILIS VAR NIGER; AIRBORNE BACTERIAL-SPORES; THERMAL-RESISTANCE; WATER
ACTIVITIES; INACTIVATION; KINETICS; MICROORGANISMS; STERILIZATION;
REQUIREMENTS; HUMIDITY
AB Dry heat microbial reduction is the NASA-approved sterilization method to reduce the microbial bioburden on spaceflight hardware for missions with planetary protection requirements. The method involves heating the spaceflight hardware to temperatures between 104 degrees C and 125 degrees C for up to 50 hours, while controlling the humidity to very low values. Collection of lethality data at temperatures above 125 degrees C and with ambient ( uncontrolled) humidity conditions would establish whether any microbial reduction credit can be offered to the flight project for processes that occur at temperatures greater than 125 degrees C. The goal of this research is to determine the survival rates of Bacillus atrophaeus ( ATCC 9372) spores subjected to temperatures higher than 125 degrees C under both dry (controlled) and room ambient humidity (36-66% relative humidity) conditions. Spores were deposited inside thin, stainless steel thermal spore exposure vessels (TSEVs) and heated under ambient or controlled humidity conditions from 115 degrees C to 170 degrees C. After the exposures, the TSEVs were cooled rapidly, and the spores were recovered and plated. Survivor ratios, lethality rate constants, and D-values were calculated at each temperature. At 115 degrees C and 125 degrees C, the controlled humidity lethality rate constant was faster than the ambient humidity lethality rate constant. At 135 degrees C, the ambient and controlled humidity lethality rate constants were statistically identical. At 150 degrees C and 170 degrees C, the ambient humidity lethality rate constant was slightly faster than the controlled humidity lethality rate constant. These results provide evidence for possibly modifying the NASA dry heat microbial reduction specification.
C1 [Kempf, M. J.; Schubert, W. W.; Beaudet, R. A.] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA USA.
RP Kempf, MJ (reprint author), Univ Tennessee, Dept Biol Sci, 574 Univ St,228 Brehm Hall, Martin, TN 38238 USA.
EM mkempf@utm.edu
NR 37
TC 11
Z9 11
U1 1
U2 10
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 DEC
PY 2008
VL 8
IS 6
BP 1169
EP 1182
DI 10.1089/ast.2007.0208
PG 14
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 409OX
UT WOS:000263516800009
PM 19191542
ER
PT J
AU Mengel, S
Lehnert, MD
Thatte, N
Whitmore, B
Vacca, WD
Chandar, R
AF Mengel, S.
Lehnert, M. D.
Thatte, N.
Whitmore, B.
Vacca, W. D.
Chandar, R.
TI Young star clusters in the Antennae galaxies and NGC 1487
SO ASTRONOMISCHE NACHRICHTEN
LA English
DT Article
DE galaxies: individual (Antennae, NGC 1487); galaxies: kinematics and
dynamics; galaxies: star clusters
ID STELLAR CLUSTERS; MASS-LOSS; NGC-4038/4039; M82; SPECTROSCOPY;
DESTRUCTION; STARBURST; IMPACT; SIZES
AB We estimate the dynamical masses of several young (approximate to 10 Myr) massive star clusters in two interacting galaxies, NGC 4038/4039 ("The Antennae") and NGC 1487, under the assumption of virial equilibrium. These are compared with photometric mass estimates. A dynamical mass substantially higher than the photometric estimate could indicate non-virial motion of the stars in the cluster, and potentially lead to cluster disruption. All but one of the Antennae clusters have dynamical and photometric mass estimates which are within a factor approximate to 2 of one another, implying both that standard IMFs provide a good approximation to the IMF of these clusters, and that there is no significant extra-virial motion, as would be expected if they were rapidly dispersing. These results suggest that almost all of the clusters in our sample have survived the gas removal phase as bound or marginally bound objects. But a few targets (two in NGC 1487 and one in the Antennae) have M(dyn) estimates which are significantly larger than the photometric mass estimates. At least two of those clusters may be actively in the process of dissolving. The dissolution candidates in both galaxies are amongst the clusters with the lowest pressures/densities measured in our sample. (C) 2008 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim
C1 [Mengel, S.] European So Observ, D-85748 Garching, Germany.
[Lehnert, M. D.] Univ Paris 07, CNRS, Observ Paris, F-92190 Meudon, France.
[Thatte, N.] Univ Oxford, Dept Astrophys, Gb Oxford OX1 3RH, England.
[Whitmore, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Vacca, W. D.] Univ Space Res Assoc, NASA, Ames Res Ctr, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA.
[Chandar, R.] Univ Toledo, Toledo, OH 43606 USA.
RP Mengel, S (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM smengel@eso.org
NR 25
TC 0
Z9 0
U1 0
U2 1
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY
SN 0004-6337
J9 ASTRON NACHR
JI Astro. Nachr.
PD DEC
PY 2008
VL 329
IS 9-10
BP 944
EP 947
DI 10.1002/asna.200811072
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 399IY
UT WOS:000262794800017
ER
PT J
AU Krucker, S
Battaglia, M
Cargill, PJ
Fletcher, L
Hudson, HS
MacKinnon, AL
Masuda, S
Sui, L
Tomczak, M
Veronig, AL
Vlahos, L
White, SM
AF Krucker, S.
Battaglia, M.
Cargill, P. J.
Fletcher, L.
Hudson, H. S.
MacKinnon, A. L.
Masuda, S.
Sui, L.
Tomczak, M.
Veronig, A. L.
Vlahos, L.
White, S. M.
TI Hard X-ray emission from the solar corona
SO ASTRONOMY AND ASTROPHYSICS REVIEW
LA English
DT Review
DE Sun; Corona; Hard X-rays
ID HIGH-ENERGY ELECTRONS; COLLAPSING MAGNETIC TRAPS; FAST-MODE WAVES;
LOOP-TOP SOURCE; 2002 JULY 23; PARTICLE-ACCELERATION; IMPULSIVE PHASE;
SPECTRAL EVOLUTION; STOCHASTIC ACCELERATION; CURRENT SHEETS
AB This review surveys hard X-ray emissions of non-thermal electrons in the solar corona. These electrons originate in flares and flare-related processes. Hard X-ray emission is the most direct diagnostic of electron presence in the corona, and such observations provide quantitative determinations of the total energy in the non-thermal electrons. The most intense flare emissions are generally observed from the chromosphere at footpoints of magnetic loops. Over the years, however, many observations of hard X-ray and even gamma-ray emission directly from the corona have also been reported. These coronal sources are of particular interest as they occur closest to where the electron acceleration is thought to occur. Prior to the actual direct imaging observations, disk occultation was usually required to study coronal sources, resulting in limited physical information. Now RHESSI has given us a systematic view of coronal sources that combines high spatial and spectral resolution with broad energy coverage and high sensitivity. Despite the low density and hence low bremsstrahlung efficiency of the corona, we now detect coronal hard X-ray emissions from sources in all phases of solar flares. Because the physical conditions in such sources may differ substantially from those of the usual "footpoint" emission regions, we take the opportunity to revisit the physics of hard X-radiation and relevant theories of particle acceleration.
C1 [Krucker, S.; Hudson, H. S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Battaglia, M.] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland.
[Cargill, P. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England.
[MacKinnon, A. L.] Univ Glasgow, Dept Phys & Astron, DACE, Glasgow G12 8QQ, Lanark, Scotland.
[Masuda, S.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Sui, L.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Tomczak, M.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland.
[Veronig, A. L.] Graz Univ, Inst Phys, IGAM, A-8010 Graz, Austria.
[Vlahos, L.] Univ Thessaloniki, Dept Phys, Thessaloniki 54124, Greece.
[White, S. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Krucker, S (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM krucker@ssl.berkeley.edu
RI Veronig, Astrid/B-8422-2009;
OI Battaglia, Marina/0000-0003-1438-9099
NR 221
TC 110
Z9 110
U1 1
U2 6
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0935-4956
EI 1432-0754
J9 ASTRON ASTROPHYS REV
JI Astron. Astrophys. Rev.
PD DEC
PY 2008
VL 16
IS 3-4
BP 155
EP 208
DI 10.1007/s00159-008-0014-9
PG 54
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 379WL
UT WOS:000261426800001
ER
PT J
AU Beckmann, V
Courvoisier, TJL
Gehrels, N
Lubinski, P
Malzac, J
Petrucci, PO
Shrader, CR
Soldi, S
AF Beckmann, V.
Courvoisier, T. J. -L.
Gehrels, N.
Lubinski, P.
Malzac, J.
Petrucci, P. -O.
Shrader, C. R.
Soldi, S.
TI The efficient low-mass Seyfert MCG-05-23-016
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; X-rays: galaxies; galaxies:
individual: MCG-05-23-016; accretion, accretion discs
ID ACTIVE GALACTIC NUCLEI; X-RAY SOURCES; BLACK-HOLE MASS; BEPPOSAX
OBSERVATIONS; INTEGRAL OBSERVATIONS; VELOCITY DISPERSION; GALAXY
MCG-5-23-16; COMPTON REFLECTION; EMISSION; SPECTRA
AB Aims. The Seyfert 1.9 galaxy MCG-05-23-016 has been shown to exhibit a complex X-ray spectrum. This source has moderate X-ray luminosity, hosts a comparably low-mass black hole, but accretes at a high Eddington rate, and allows us to study a super massive black hole in an early stage.
Methods. Three observations of the INTEGRAL satellite simultaneous with pointed Swift/XRT observations performed from December 2006 to June 2007 are used in combination with public data from the INTEGRAL archive to study the variability of the hard X-ray components and to generate a high-quality spectrum from 1 to 150 keV.
Results. The AGN shows little variability in the hard X-ray spectrum, with some indication of a variation in the high-energy cut-of energy ranging from 50 keV to >> 100 keV, with an electron plasma temperature in the 10-90 keV range. The reflection component is not evident and, if present, the reflected fraction can be constrained to R < 0.3 for the combined data set. Comparison to previous observations shows that the reflection component has to be variable. No variability in the UV and optical range is observed on a time scale of 1.5 years.
Conclusions. The hard X-ray spectrum of MCG-05-23-016 appears to be stable with the luminosity and underlying power law varying moderately and the optical/UV flux staying constant. The reflection component and the iron K alpha line seem to have decreased between December 2005 and the observations presented here. The spectral energy distribution appears to be similar to that of Galactic black hole systems, e. g. XTE 1118+ 480 in the low state. The AGN exhibits a remarkably high Eddington ratio of L-bol/L-Edd greater than or similar to 0.8 (or L-bol/L-Edd greater than or similar to 0.1, if we consider a higher mass of the central engine) and, at the same time, a low cut-off energy around 70 keV. Objects like MCG-05-23-016 might indicate the early stages of super massive black holes, in which a strong accretion flow feeds the central engine.
C1 [Beckmann, V.; Courvoisier, T. J. -L.; Lubinski, P.; Soldi, S.] ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland.
[Beckmann, V.; Courvoisier, T. J. -L.; Soldi, S.] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland.
[Beckmann, V.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Gehrels, N.; Shrader, C. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Lubinski, P.] Ctr Astron M Kopernika, PL-00716 Warsaw, Poland.
[Malzac, J.] CNRS, UPS, OMP, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Petrucci, P. -O.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, F-38041 Grenoble, France.
RP Beckmann, V (reprint author), ISDC Data Ctr Astrophys, Chemin Ecogia 16, CH-1290 Versoix, Switzerland.
EM Volker.Beckmann@unige.ch
RI Gehrels, Neil/D-2971-2012
NR 52
TC 8
Z9 8
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD DEC
PY 2008
VL 492
IS 1
BP 93
EP 99
DI 10.1051/0004-6361:200810674
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 377LQ
UT WOS:000261253100015
ER
PT J
AU Kreykenbohm, I
Wilms, J
Kretschmar, P
Torrejon, JM
Pottschmidt, K
Hanke, M
Santangelo, A
Ferrigno, C
Staubert, R
AF Kreykenbohm, I.
Wilms, J.
Kretschmar, P.
Torrejon, J. M.
Pottschmidt, K.
Hanke, M.
Santangelo, A.
Ferrigno, C.
Staubert, R.
TI High variability in Vela X-1: giant flares and off states
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Review
DE X-rays: stars; stars: flare; stars: pulsars: individual: Vela X-1;
stars: magnetic fields
ID X-RAY PULSARS; QUASI-PERIODIC OSCILLATIONS; CYCLOTRON-LINE FEATURES;
CLUMPY STELLAR WINDS; INTEGRAL OBSERVATION; NEUTRON-STAR; CIRCUMSTELLAR
MATTER; MAGNETIC-FIELDS; OUTER EVOLUTION; ACCRETION FLOW
AB Aims. We investigate the spectral and temporal behavior of the high mass X-ray binary Vela X-1 during a phase of high activity, with special focus on the observed giant flares and off states.
Methods. INTEGRAL observed Vela X-1 in a long almost uninterrupted observation for two weeks in 2003 Nov/Dec. The data were analyzed with OSA 7.0 and FTOOLS 6.2. We derive the pulse period, light curves, spectra, hardness ratios, and hardness intensity diagrams, and study the eclipse.
Results. In addition to an already high activity level, Vela X-1 exhibited several intense flares, the brightest ones reaching a maximum intensity of more than 5 Crab in the 20-40 keV band and several off states where the source was no longer detected by INTEGRAL. We determine the pulse period to be 283.5320 +/- 0.0002 s, which is stable throughout the entire observation. Analyzing the eclipses provided an improvement in the ephemeris. Spectral analysis of the flares indicates that there appear to be two types of flares: relatively brief flares, which can be extremely intense and show spectral softening, in contrast to high intensity states, which are longer and show no softening.
Conclusions. Both flares and off states are interpreted as being due to a strongly structured wind of the optical companion. When Vela X-1 encounters a cavity with strongly reduced density, the flux will drop triggering the onset of the propeller effect, which inhibits further accretion, giving rise to off states. The sudden decrease in the density of the material required to trigger the propeller effect in Vela X-1 is of the same order as predicted by theoretical papers about the densities in OB star winds. A similarly structured wind can produce giant flares when Vela X-1 encounters a dense blob in the wind.
C1 [Kreykenbohm, I.; Wilms, J.; Hanke, M.] Dr Karl Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany.
[Kreykenbohm, I.; Wilms, J.; Hanke, M.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Kreykenbohm, I.; Santangelo, A.; Ferrigno, C.; Staubert, R.] Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany.
[Kreykenbohm, I.; Ferrigno, C.] INTEGRAL Sci Data Ctr, CH-1290 Chavannes Des Bois, Switzerland.
[Kretschmar, P.] European Space Astron Ctr, European Space Agcy, Madrid 28691, Spain.
[Torrejon, J. M.] Univ Alicante, Escuela Politecn Super, Dept Fis Ingn Sistemas & Teoria Senal, Alicante 03080, Spain.
[Torrejon, J. M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Pottschmidt, K.] Univ Maryland, CRESST, Baltimore, MD 21250 USA.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Ferrigno, C.] IASF INAF, I-90136 Palermo, Italy.
RP Kreykenbohm, I (reprint author), Dr Karl Remeis Sternwarte Bamberg, Sternwartstr 7, D-96049 Bamberg, Germany.
EM Ingo.Kreykenbohm@sternwarte.uni-erlangen.de
RI Ferrigno, Carlo/H-4139-2012; Wilms, Joern/C-8116-2013; Kreykenbohm,
Ingo/H-9659-2013; Torrejon, Jose /K-6395-2014;
OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803;
Torrejon, Jose /0000-0002-5967-5163; Kretschmar,
Peter/0000-0001-9840-2048
NR 115
TC 63
Z9 63
U1 0
U2 1
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 DEC
PY 2008
VL 492
IS 2
BP 511
EP 525
DI 10.1051/0004-6361:200809956
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 379YC
UT WOS:000261431500023
ER
PT J
AU Piranomonte, S
Ward, PA
Fiore, F
Vergani, SD
D'Elia, V
Krongold, Y
Nicastro, F
Meurs, EJA
Chincarini, G
Covino, S
Della Valle, M
Fugazza, D
Norci, L
Sbordone, L
Stella, L
Tagliaferri, G
Burrows, DN
Gehrels, N
Goldoni, P
Malesani, D
Mirabel, IF
Pellizza, LJ
Perna, R
AF Piranomonte, S.
Ward, P. A.
Fiore, F.
Vergani, S. D.
D'Elia, V.
Krongold, Y.
Nicastro, F.
Meurs, E. J. A.
Chincarini, G.
Covino, S.
Della Valle, M.
Fugazza, D.
Norci, L.
Sbordone, L.
Stella, L.
Tagliaferri, G.
Burrows, D. N.
Gehrels, N.
Goldoni, P.
Malesani, D.
Mirabel, I. F.
Pellizza, L. J.
Perna, R.
TI Probing the complex environments of GRB host galaxies and intervening
systems: high resolution spectroscopy of GRB050922C
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gamma rays: bursts; cosmology: observations; galaxies: abundances;
galaxies: ISM
ID GAMMA-RAY BURSTS; PHOTOCHEMICAL EVOLUTION; PHYSICAL CONDITIONS; LEVEL
POPULATIONS; ELLIPTIC GALAXIES; AFTERGLOW; GRB-021004; PROGENITOR;
REDSHIFT; PHOTOIONIZATION
AB Aims. The aim of this paper is to investigate the environment of gamma ray bursts (GRBs) and the interstellar matter of their host galaxies.
Methods. To this purpose we use high resolution spectroscopic observations of the afterglow of GRB050922C, obtained with UVES/VLT similar to 3.5 h after the GRB event.
Results. We found that, as for most high resolution spectra of GRBs, the spectrum of the afterglow of GRB050922C is complex. At least seven components contribute to the main absorption system at z = 2.1992. The detection of lines of neutral elements like MgI and the detection of fine-structure levels of the ions FeII, SiII and CII allows us to separate components in the GRB ISM along the line of sight. Moreover, in addition to the main system, we analyzed the five intervening systems between z = 2.077 and z = 1.5664 identified along the GRB line of sight.
Conclusions. GRB afterglow spectra are very complex, but full of information. This can be used to disentangle the contribution of the different parts of the GRB host galaxy and to study their properties. Our metallicity estimates agree with the scenario of GRBs exploding in low metallicity galaxies
C1 [Piranomonte, S.; Fiore, F.; D'Elia, V.; Nicastro, F.; Stella, L.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy.
[Ward, P. A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Vergani, S. D.; Norci, L.] Dublin Inst Adv Studies, Dublin 2, Ireland.
[Vergani, S. D.; Meurs, E. J. A.] Dublin City Univ, Sch Phys Sci, Dublin 9, Ireland.
[Vergani, S. D.; Meurs, E. J. A.] Dublin City Univ, NCPST, Dublin 9, Ireland.
[Vergani, S. D.; Chincarini, G.; Covino, S.; Fugazza, D.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy.
[Krongold, Y.] Univ Nacl Autonoma Mexico, Astron Inst, Mexico City 04510, DF, Mexico.
[Chincarini, G.] Univ Milan, I-20126 Milan, Italy.
[Della Valle, M.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Della Valle, M.] Int Ctr Relativist Astrophys Network, I-65122 Pescara, Italy.
[Della Valle, M.] European So Observ, D-85748 Garching, Germany.
[Sbordone, L.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France.
[Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Goldoni, P.] Lab Astroparticule & Cosmol, UMR 7164, APC, F-75231 Paris 05, France.
[Goldoni, P.] CEA Saclay, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Malesani, D.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Mirabel, I. F.] European So Observ, Santiago 19, Chile.
[Pellizza, L. J.] Inst Astron & Fis Espacio, CONICET, UBA, RA-1428 Buenos Aires, DF, Argentina.
[Perna, R.] Univ Colorado, JILA, Boulder, CO 80309 USA.
RP Piranomonte, S (reprint author), Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy.
EM piranomonte@oa-roma.inaf.it
RI Gehrels, Neil/D-2971-2012;
OI Nicastro, Fabrizio/0000-0002-6896-1364; D'Elia,
Valerio/0000-0002-7320-5862; Della Valle, Massimo/0000-0003-3142-5020;
Fiore, Fabrizio/0000-0002-4031-4157
FU MIUR [COFIN-03-02-23, INAF/PRIN270/2003]; ASI [ASI/I/R/039/04,
ASI/I/R/023/05/0]; SFI
FX We thank an anonymous referee for comments that improved the
presentation. We thank C. Porciani, V. D'Odorico, H.-W. Chen, J. X.
Prochaska and P. M. Vreeswijk for useful discussions. Part of this work
was supported by MIUR COFIN-03-02-23 and INAF/PRIN270/2003 and ASI
contracts ASI/I/R/039/04 and ASI/I/R/023/05/0. S. P. and V. D.
acknowledge support from ASI grants. S. P., S. D. V. and M. D. V. thank
the Dark Cosmology Centre of Copenhagen, where part of this work was
done, for the friendly and creative atmosphere. D. M. acknowledges the
Instrument Center for Danish Astrophysics for support and thanks the
Dark Cosmology Centre (funded by the DNRF). S. D. V. is supported by
SFI.
NR 43
TC 28
Z9 28
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD DEC
PY 2008
VL 492
IS 3
BP 775
EP 785
DI 10.1051/0004-6361:20079015
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 383UA
UT WOS:000261697900020
ER
PT J
AU Goad, MR
Tyler, LG
Beardmore, AP
Evans, PA
Rosen, SR
Osborne, JP
Starling, RLC
Marshall, FE
Yershov, V
Burrows, DN
Gehrels, N
Roming, PWA
Moretti, A
Capalbi, M
Hill, JE
Kennea, J
Koch, S
Berk, DV
AF Goad, M. R.
Tyler, L. G.
Beardmore, A. P.
Evans, P. A.
Rosen, S. R.
Osborne, J. P.
Starling, R. L. C.
Marshall, F. E.
Yershov, V.
Burrows, D. N.
Gehrels, N.
Roming, P. W. A.
Moretti, A.
Capalbi, M.
Hill, J. E.
Kennea, J.
Koch, S.
Berk, D. Vanden
TI Accurate early positions for Swift GRBs: enhancing X-ray positions with
UVOT astrometry (vol 476, pg 1401, 2007)
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Correction
DE gamma rays: bursts; astrometry; errata, addenda
C1 [Goad, M. R.; Tyler, L. G.; Beardmore, A. P.; Evans, P. A.; Rosen, S. R.; Osborne, J. P.; Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Marshall, F. E.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rosen, S. R.; Yershov, V.] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England.
[Burrows, D. N.; Roming, P. W. A.; Kennea, J.; Koch, S.; Berk, D. Vanden] Penn State Univ, University Pk, PA 16802 USA.
[Moretti, A.] INAF Osservatorio Astronom Brera, I-23807 Merate, Lc, Italy.
[Capalbi, M.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Hill, J. E.] Univ Space Res Assoc, Columbia, MD 21044 USA.
RP Goad, MR (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM mrg@star.le.ac.uk
RI Gehrels, Neil/D-2971-2012
NR 1
TC 2
Z9 2
U1 0
U2 1
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 DEC
PY 2008
VL 492
IS 3
BP 873
EP 873
DI 10.1051/0004-6361:20078436e
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 383UA
UT WOS:000261697900029
ER
PT J
AU Smith, DA
Guillemot, L
Camilo, F
Cognard, I
Dumora, D
Espinoza, C
Freire, PCC
Gotthelf, EV
Harding, AK
Hobbs, GB
Johnston, S
Kaspi, VM
Kramer, M
Livingstone, MA
Lyne, AG
Manchester, RN
Marshall, FE
McLaughlin, MA
Noutsos, A
Ransom, SM
Roberts, MSE
Romani, RW
Stappers, BW
Theureau, G
Thompson, DJ
Thorsett, SE
Wang, N
Weltevrede, P
AF Smith, D. A.
Guillemot, L.
Camilo, F.
Cognard, I.
Dumora, D.
Espinoza, C.
Freire, P. C. C.
Gotthelf, E. V.
Harding, A. K.
Hobbs, G. B.
Johnston, S.
Kaspi, V. M.
Kramer, M.
Livingstone, M. A.
Lyne, A. G.
Manchester, R. N.
Marshall, F. E.
McLaughlin, M. A.
Noutsos, A.
Ransom, S. M.
Roberts, M. S. E.
Romani, R. W.
Stappers, B. W.
Theureau, G.
Thompson, D. J.
Thorsett, S. E.
Wang, N.
Weltevrede, P.
TI Pulsar timing for the Fermi gamma-ray space telescope
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE space vehicles: instruments; stars: pulsars: general; gamma-rays:
observations; ephemerides
ID RAPIDLY SPINNING PULSARS; GIANT RADIO PULSES; MILLISECOND PULSARS;
HIGH-ENERGY; BINARY PULSAR; CRAB PULSAR; PRECISION; RADIATION; MODEL;
DISCOVERY
AB We describe a comprehensive pulsar monitoring campaign for the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope ( formerly GLAST). The detection and study of pulsars in gamma rays give insights into the populations of neutron stars and supernova rates in the Galaxy, into particle acceleration mechanisms in neutron star magnetospheres, and into the "engines" driving pulsar wind nebulae. LAT's unprecedented sensitivity between 20 MeV and 300 GeV together with its 2.4 sr field-of-view makes detection of many gamma-ray pulsars likely, justifying the monitoring of over two hundred pulsars with large spin-down powers. To search for gamma-ray pulsations from most of these pulsars requires a set of phase-connected timing solutions spanning a year or more to properly align the sparse photon arrival times. We describe the choice of pulsars and the instruments involved in the campaign. Attention is paid to verifications of the LAT pulsar software, using for example giant radio pulses from the Crab and from PSR B1937+21 recorded at Nancay, and using X-ray data on PSR J0218+4232 from XMM-Newton. We demonstrate accuracy of the pulsar phase calculations at the microsecond level.
C1 [Smith, D. A.; Guillemot, L.; Dumora, D.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France.
[Smith, D. A.; Guillemot, L.; Dumora, D.] Ctr Etud Nucl Bordeaux Gradignan, IN2P3, CNRS, UMR 5797, F-33175 Gradignan, France.
[Camilo, F.; Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Cognard, I.; Theureau, G.] CNRS INSU, UMR 6115, LPCE, F-45071 Orleans, France.
[Cognard, I.; Theureau, G.] CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France.
[Theureau, G.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France.
[Espinoza, C.; Kramer, M.; Lyne, A. G.; Noutsos, A.; Stappers, B. W.] Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England.
[Freire, P. C. C.] Arecibo Observ, Arecibo, PR 00612 USA.
[Harding, A. K.; Marshall, F. E.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hobbs, G. B.; Johnston, S.; Manchester, R. N.; Weltevrede, P.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Kaspi, V. M.; Livingstone, M. A.] McGill Univ, Montreal, PQ, Canada.
[McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Roberts, M. S. E.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Romani, R. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Thorsett, S. E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Wang, N.] Chinese Acad Sci, Natl Astron Observ, Urumqi 830011, Peoples R China.
RP Smith, DA (reprint author), Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France.
EM smith@cenbg.in2p3.fr
RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012;
OI Thompson, David/0000-0001-5217-9135; Thorsett,
Stephen/0000-0002-2025-9613; Roberts, Mallory/0000-0002-9396-9720;
Ransom, Scott/0000-0001-5799-9714
NR 80
TC 77
Z9 78
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD DEC
PY 2008
VL 492
IS 3
BP 923
EP 931
DI 10.1051/0004-6361:200810285
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 383UA
UT WOS:000261697900032
ER
PT J
AU Hartman, RC
Kadler, M
Tueller, J
AF Hartman, R. C.
Kadler, M.
Tueller, J.
TI GAMMA-RAY EMISSION FROM THE BROAD-LINE RADIO GALAXY 3C 111
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (3C 111); gamma rays:
observations
ID SEYFERT-GALAXIES; SKY SURVEY; M87 JET; MISSION; TELESCOPE; CATALOG;
3C-111; CLOUD
AB The broad-line radio galaxy 3C 111 has been suggested as the counterpart of the gamma-ray source 3EG J0416+3650. While 3C 111 meets most of the criteria for a high-probability identification, like a bright flat-spectrum radio core and a blazar-like broadband SED, in the Third EGRET Catalog, the large positional offset of about 1.5 degrees put 3C 111 outside the 99% probability region for 3EG J0416+3650, making this association questionable. We present a reanalysis of all available data for 3C 111 from the EGRET archives, resulting in probable detection of high-energy gamma-ray emission above 1000 MeV from a position close to the nominal position of 3C 111, in two separate viewing periods (VPs), at a 3 sigma level in each. A new source, GRO J0426+3747, appears to be present nearby, seen only in the >1000 MeV data. For >100 MeV, the data are in agreement with only one source ( at the original catalog position) accounting for most of the EGRET-detected emission of 3EG J0416+3650. A follow-up Swift UVOT/XRT observation reveals one moderately bright X-ray source in the error box of 3EG J0416+3650, but because of the large EGRET position uncertainty, it is not certain that the X-ray and gamma-ray sources are associated. A Swift observation of GRO J0426+3747 detected no X-ray source nearby.
C1 [Hartman, R. C.; Tueller, J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Kadler, M.] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
[Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA.
RP Hartman, RC (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA.
RI Tueller, Jack/D-5334-2012;
OI Kadler, Matthias/0000-0001-5606-6154
FU NASA Postdoctoral Program at the Goddard Space Flight Center; NSF;
Smithsonian Institution; Academia Sinica
FX We thank Goro Sato, Francesco Verrecchia, Svetlana Jorstad, and Chris
Shrader for their help and advice in compiling the SED data for this
study. Steve Drake and Rachel Osten have kindly provided insight
regarding X-ray emission from stars. M. K. has been supported by 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 data obtained from the High
Energy Astrophysics Science Archive Research Center (HEASARC), provided
by the NASA Goddard Space Flight Center, and the NASA/IPAC Extragalactic
Database (NED), operated by the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. We have also made use
of data products from the Two Micron All Sky Survey, a joint project of
the University of Massachusetts and the Infrared Processing and Analysis
Center, California Institute of Technology, funded by NASA and NSF.
Submillimeter flux ranges for 3C 111 were obtained from the online
archives of the Submillimeter Array ( SMA), a joint project between the
Smithsonian Astrophysical Observatory and the Academia Sinica Institute
of Astronomy and Astrophysics, funded by the Smithsonian Institution and
the Academia Sinica.
NR 29
TC 17
Z9 17
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2008
VL 688
IS 2
BP 852
EP 858
DI 10.1086/592138
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 373VU
UT WOS:000261002400012
ER
PT J
AU Higdon, JL
Higdon, SJU
Willner, SP
Brown, MJI
Stern, D
Le Floc'h, E
Eisenhardt, P
AF Higdon, J. L.
Higdon, S. J. U.
Willner, S. P.
Brown, M. J. I.
Stern, D.
Le Floc'h, E.
Eisenhardt, P.
TI RADIO AND INFRARED SELECTED OPTICALLY INVISIBLE SOURCES IN THE BOOTES
NDWFS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: high-redshift; galaxies: starburst;
infrared: galaxies; radio continuum: galaxies
ID SPITZER-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; SPECTRAL
ENERGY-DISTRIBUTIONS; STAR-FORMATION HISTORY; HUBBLE DEEP FIELD; ARRAY
CAMERA IRAC; HIGH-REDSHIFT; LUMINOUS GALAXIES; ELLIPTIC GALAXIES;
FORMING GALAXIES
AB We have combined data from the NOAO Deep Wide-Field Survey in Bootes and the Spitzer Space Telescope to determine basic properties for 16 optically "invisible'' MIPS 24 mu m and 35 optically invisible radio sources (OIMSs and OIRSs, respectively), including their spectral energy distributions (SEDs) and luminosities. Most OIMSs possess steep power-law SEDs over lambda(rest) = 1-10 mu m, indicating the presence of obscured AGNs in agreement with Spitzer spectroscopy. These objects are extremely luminous at rest-frame near- and mid-IR [vLv(5 mu m) approximate to 10(38)-10(39) W], consistent with accretion near the Eddington limit and further implying that they host buried QSOs. The majority of the IRAC-detected OIRSs have flat 3.6-24 mu m SEDs, implying comparable emission from stellar photospheres and hot AGN-illuminated dust. This may reflect relatively small amounts of dust close to the central engine or current low mass accretion rates. A small subset of OIRSs appear to be starburst-dominated with photometric redshifts from 1.0 to 4.5. The OIMSs and OIRSs with significant starburst components have similar L-K and stellar masses (M* approximate to 10(11) M-circle dot) assuming minimal AGN contribution. Roughly half of the OIRSs are not detected by Spitzer IRAC or MIPS. These are most likely z >= 2 radio galaxies. The IRAC-detected OIRSs are more likely than OIMSs to appear nonpointlike in the 3.6 and 4.5 mu m images, suggesting that interactions play a role in triggering their activity. The AGN-powered OIMSs may represent submillimeter galaxies making the transition from starburst to accretion dominance in their evolution to current-epoch massive ellipticals.
C1 [Higdon, J. L.; Higdon, S. J. U.] Georgia So Univ, Dept Phys, Statesboro, GA 30460 USA.
[Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Stern, D.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Le Floc'h, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Le Floc'h, E.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Higdon, JL (reprint author), Georgia So Univ, Dept Phys, Statesboro, GA 30460 USA.
RI Brown, Michael/B-1181-2015
OI Brown, Michael/0000-0002-1207-9137
FU NASA through awards issued by JPL/Caltech; NASA/IPAC Extragalactic
Database (NED); Jet Propulsion Laboratory; California Institute of
Technology; National Aeronautics and Space Administration
FX We wish to thank Terry Herter for valuable discussions relating to the
template-fitting routines, as well as Julien Devriendt and Kevin Xu for
access to their libraries of galaxy SEDs. We also wish to thank the
anonymous referee for helpful suggestions and comments. 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 awards issued by JPL/Caltech. 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 69
TC 7
Z9 7
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2008
VL 688
IS 2
BP 885
EP 904
DI 10.1086/591069
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 373VU
UT WOS:000261002400015
ER
PT J
AU Trinchieri, G
Pellegrini, S
Fabbiano, G
Fu, R
Brassington, NJ
Zezas, A
Kim, DW
Gallagher, J
Angelini, L
Davies, RL
Kalogera, V
King, AR
Zepf, S
AF Trinchieri, G.
Pellegrini, S.
Fabbiano, G.
Fu, R.
Brassington, N. J.
Zezas, A.
Kim, D. -W.
Gallagher, J.
Angelini, L.
Davies, R. L.
Kalogera, V.
King, A. R.
Zepf, S.
TI DISCOVERY OF HOT GAS IN OUTFLOW IN NGC 3379
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC
3379); X-rays: galaxies; X-rays: ISM
ID EARLY-TYPE GALAXIES; CCD SURFACE PHOTOMETRY; X-RAY-EMISSION; TO-LIGHT
RATIO; ELLIPTIC GALAXIES; DARK-MATTER; STELLAR POPULATION; BLACK-HOLES;
GLOBULAR-CLUSTERS; DEEP CHANDRA
AB We report the discovery of a faint (L-X similar to 4 +/- 1.5 x 10(37) ergs s(-1), 0.5-2 keV), outflowing gaseous hot interstellar medium (ISM) in NGC 3379. This represents the lowest X-ray luminosity ever measured from a hot phase of the ISM in a nearby early-type galaxy. The discovery of the hot ISM in a very deep Chandra observation was possible thanks to its unique spectral and spatial signatures, which distinguish it from the integrated stellar X-ray emission, responsible for most of the unresolved emission in the Chandra data. This hot component is found in a region of similar to 800 pc in radius at the center of the galaxy and has a total mass M similar to 3 +/- 1 x 10(5) M-circle dot. Independent theoretical prediction of the characteristics of an ISM in this galaxy, based on the intrinsic properties of NGC 3379, reproduce well the observed luminosity, temperature, and radial distribution and mass of the hot gas, and indicate that the gas is in an outflowing phase, predicted by models but not observed in any system so far.
C1 [Trinchieri, G.] Osserv Astron Brera, INAF, I-20212 Milan, Italy.
[Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Fabbiano, G.; Fu, R.; Brassington, N. J.; Zezas, A.; Kim, D. -W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Angelini, L.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA.
[Davies, R. L.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
[Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[King, A. R.] Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England.
[Zepf, S.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
RP Trinchieri, G (reprint author), Osserv Astron Brera, INAF, Via Brera 28, I-20212 Milan, Italy.
EM ginevra.trinchieri@brera.inaf.it
RI Zezas, Andreas/C-7543-2011;
OI Zezas, Andreas/0000-0001-8952-676X; Trinchieri,
Ginevra/0000-0002-0227-502X
FU Chandra X-Ray Center (CXC) CIAO software and CALDB; SAOImage DS9;
Smithsonian Astrophysical Observatory; Chandra GO [G06-7079A]; NASA LTSA
[NAG5-13056]; Italian Space Agency ASI (Agenzia Spaziale Italiana)
through grant ASI-INAF [I/023/05/0]; [NAS8-39073]
FX We thank Stefano Andreon for many interesting discussions on the
statistical aspects of the data analysis, and Terry Gaetz and Diab
Jerius for their help in understanding the PSF issues. We thank the
referee for raising the issue of the effects of the PSF, which prompted
us to better investigate the reliability of the results. The data
analysis was supported by the Chandra X-Ray Center (CXC) CIAO software
and CALDB, and has made use of the SAOImage DS9 and funtools softwares,
developed by the Smithsonian Astrophysical Observatory. We have used the
NASA NED and ADS facilities, and have extracted archival data from the
Chandra, HST, and 2MASS archives. This work was supported by the Chandra
GO grant G06-7079A ( PI: G. Fabbiano) and subcontract G06-7079B ( PI: V.
Kalogera). We acknowledge partial support from NASA contract NAS8-39073
(CXC); A. Zezas acknowledges support from NASA LTSA grant NAG5-13056; S.
Pellegrini acknowledges partial financial support from the Italian Space
Agency ASI (Agenzia Spaziale Italiana) through grant ASI-INAF
I/023/05/0.
NR 66
TC 22
Z9 22
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 DEC 1
PY 2008
VL 688
IS 2
BP 1000
EP 1008
DI 10.1086/592287
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 373VU
UT WOS:000261002400022
ER
PT J
AU Abdo, AA
Allen, B
Aune, T
Berley, D
Blaufuss, E
Casanova, S
Chen, C
Dingus, BL
Ellsworth, RW
Fleysher, L
Fleysher, R
Gonzalez, MM
Goodman, JA
Hoffman, CM
Huntemeyer, PH
Kolterman, BE
Lansdell, CP
Linnemann, JT
McEnery, JE
Mincer, AI
Moskalenko, IV
Nemethy, P
Noyes, D
Porter, TA
Pretz, J
Ryan, JM
Parkinson, PMS
Shoup, A
Sinnis, G
Smith, AJ
Strong, AW
Sullivan, GW
Vasileiou, V
Walker, GP
Williams, DA
Yodh, GB
AF Abdo, A. A.
Allen, B.
Aune, T.
Berley, D.
Blaufuss, E.
Casanova, S.
Chen, C.
Dingus, B. L.
Ellsworth, R. W.
Fleysher, L.
Fleysher, R.
Gonzalez, M. M.
Goodman, J. A.
Hoffman, C. M.
Huentemeyer, P. H.
Kolterman, B. E.
Lansdell, C. P.
Linnemann, J. T.
McEnery, J. E.
Mincer, A. I.
Moskalenko, I. V.
Nemethy, P.
Noyes, D.
Porter, T. A.
Pretz, J.
Ryan, J. M.
Parkinson, P. M. Saz
Shoup, A.
Sinnis, G.
Smith, A. J.
Strong, A. W.
Sullivan, G. W.
Vasileiou, V.
Walker, G. P.
Williams, D. A.
Yodh, G. B.
TI MEASUREMENT OF THE SPATIAL DISTRIBUTION OF DIFFUSE TeV GAMMA-RAY
EMISSION FROM THE GALACTIC PLANE WITH MILAGRO
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: observations
ID COSMIC-RAY; GALAXY; J2032+4130; DISCOVERY; SPECTRUM; CYGNUS; EXCESS;
MATTER; RIDGE
AB Diffuse gamma-ray emission produced by the interaction of cosmic-ray particles with matter and radiation in the Galaxy can be used to probe the distribution of cosmic rays and their sources in different regions of the Galaxy. With its large field of view and long observation time, the Milagro Gamma Ray Observatory is an ideal instrument for surveying large regions of the northern hemisphere sky and for detecting diffuse gamma-ray emission at very high energies. Here the spatial distribution and the flux of the diffuse gamma-ray emission in the TeV energy range with a median energy of 15 TeV for Galactic longitude between 30 degrees and 110 degrees and between 136 degrees and 216 degrees and for Galactic latitude between -10 degrees and 10 degrees are determined. The measured fluxes are consistent with predictions of the GALPROP model everywhere, except for the Cygnus region (l is an element of[65 degrees, 85 degrees]). For the Cygnus region, the flux is twice the predicted value. This excess can be explained by the presence of active cosmic-ray sources accelerating hadrons, which interact with the local dense interstellar medium and produce gamma rays through pion decay.
C1 [Abdo, A. A.] USN, Res Lab, Washington, DC 20375 USA.
[Allen, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Aune, T.; Porter, T. A.; Parkinson, P. M. Saz; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Berley, D.; Blaufuss, E.; Goodman, J. A.; Noyes, D.; Smith, A. J.; Sullivan, G. W.; Vasileiou, V.] Univ Maryland, College Pk, MD 20742 USA.
[Casanova, S.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Chen, C.; Yodh, G. B.] Univ Calif Irvine, Irvine, CA USA.
[Dingus, B. L.; Hoffman, C. M.; Huentemeyer, P. H.; Pretz, J.; Sinnis, G.; Walker, G. P.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Ellsworth, R. W.] George Mason Univ, Fairfax, VA 22030 USA.
[Fleysher, L.; Fleysher, R.; Kolterman, B. E.; Mincer, A. I.; Nemethy, P.] NYU, New York, NY USA.
[Gonzalez, M. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Lansdell, C. P.] Inst Def Anal, Alexandria, VA USA.
[Linnemann, J. T.] Michigan State Univ, E Lansing, MI 48824 USA.
[McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Moskalenko, I. V.] Stanford Univ, HEPL, Stanford, CA 94305 USA.
[Moskalenko, I. V.] Stanford Univ, KIPAC, Stanford, CA 94305 USA.
[Ryan, J. M.] Univ New Hampshire, Durham, NH 03824 USA.
[Shoup, A.] Ohio State Univ, Lima, OH 45804 USA.
[Strong, A. W.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany.
RP Abdo, AA (reprint author), USN, Res Lab, Washington, DC 20375 USA.
RI McEnery, Julie/D-6612-2012; Casanova, Sabrina/J-8935-2013; Moskalenko,
Igor/A-1301-2007;
OI Casanova, Sabrina/0000-0002-6144-9122; Moskalenko,
Igor/0000-0001-6141-458X; Dingus, Brenda/0000-0001-8451-7450
FU National Science Foundation [PHY-0245234, PHY-0302000, PHY-0400424,
PHY-0504201, PHY-0601080, ATM-0002744]; Department of Energy (Office of
High Energy Physics); Los Alamos National Laboratory; University of
California; Institute for Geophysics and Planetary Physics at Los Alamos
National Laboratory; NASA APRA
FX We thank Scott Delay, Michael Schneider, and Owen Marshall for their
dedicated efforts on the Milagro experiment. We also gratefully
acknowledge the financial support of the National Science Foundation
(under grants PHY-0245234, -0302000, -0400424, -0504201, -0601080, and
ATM-0002744), the Department of Energy (Office of High Energy Physics),
Los Alamos National Laboratory, the University of California, and the
Institute for Geophysics and Planetary Physics at Los Alamos National
Laboratory. I.V. Moskalenko acknowledges partial support from the NASA
APRA grant.
NR 35
TC 65
Z9 67
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2008
VL 688
IS 2
BP 1078
EP 1083
DI 10.1086/592213
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 373VU
UT WOS:000261002400028
ER
PT J
AU Uchida, H
Tsunemi, H
Katsuda, S
Kimura, M
AF Uchida, Hiroyuki
Tsunemi, Hiroshi
Katsuda, Satoru
Kimura, Masashi
TI THE PLASMA STRUCTURE OF THE SOUTHWESTERN REGION OF THE CYGNUS LOOP WITH
THE XMM-NEWTON OBSERVATORY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: abundances; ISM: individual (Cygnus Loop); supernova remnants;
X-rays: ISM
ID SUPERNOVA-REMNANTS; NORTHEASTERN RIM; NUCLEOSYNTHESIS; EXPLOSION;
EMISSION; SUZAKU; FRONT
AB We observed the southwestern region of the Cygnus Loop in two pointings with XMM-Newton. The region observed is called the "blow-out'' region, which is extended further in the south. The origin of the "blow out'' is not well understood, but it is suggested that there is another supernova remnant here in radio observation. To investigate in detail the structure of this region in X-ray, we divided our fields of view into 33 box regions. The spectra are well fitted by a two-component nonequilibrium ionization model. The emission measure distributions of heavy elements decrease from the inner region to the outer region of the Loop. Then, we also divided our fields of view into 26 annular sectors to examine the radial plasma structure. Judging from the metal abundances obtained, it is consistent that the X-ray emission is of Cygnus Loop origin, and we conclude that the high-kT(e) component (similar to 0.4 keV) originates from the ejecta, while the low-kT(e) component (similar to 0.2 keV) is derived from the swept-up interstellar medium. The flux of the low-kT(e) component is much less than that of high-kT(e) component, suggesting that the ISM component is very thin. Also, the relative abundances in the ejecta component show values similar to those obtained from previous observations of the Cygnus Loop. We find no evidence in X-ray that the nature of the "blow-out'' region originated from the extra supernova remnant. From the ejecta component, we calculated the masses for various metals and estimated the origin of the Cygnus Loop as a core-collapse explosion rather than a Type Ia supernova.
C1 [Uchida, Hiroyuki; Tsunemi, Hiroshi; Katsuda, Satoru; Kimura, Masashi] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Katsuda, Satoru] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Uchida, H (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan.
EM uchida@ess.sci.osaka-u.ac.jp; tsunemi@ess.sci.osaka-u.ac.jp;
satoru.katsuda@nasa.gov; mkimura@ess.sci.osaka-u.ac.jp
RI XRAY, SUZAKU/A-1808-2009
FU Ministry of Education, Culture, Sports, Science and Technology
[16002004]; JSPS Research Fellowship for Young Scientists
FX We thank H. Kosugi's careful reading of the manuscript. This work is
partly supported by a Grant-in-Aid for Scientific Research by the
Ministry of Education, Culture, Sports, Science and Technology
(16002004). This study is also carried out as part of the 21st Century
COE Program, "Towards a New Basic Science: Depth and Snthesis.'' H. U.
and S. K. are supported by JSPS Research Fellowship for Young
Scientists.
NR 21
TC 11
Z9 11
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2008
VL 688
IS 2
BP 1102
EP 1111
DI 10.1086/592398
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 373VU
UT WOS:000261002400030
ER
PT J
AU Bauer, FE
Dwarkadas, VV
Brandt, WN
Immler, S
Smartt, S
Bartel, N
Bietenholz, MF
AF Bauer, F. E.
Dwarkadas, V. V.
Brandt, W. N.
Immler, S.
Smartt, S.
Bartel, N.
Bietenholz, M. F.
TI SUPERNOVA 1996cr: SN 1987A's WILD COUSIN?
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE circumstellar matter; supernovae: general; supernovae: individual (SN
1996cr); X-rays: individual (SN 1996cr)
ID GAMMA-RAY BURST; RAPID PRESUPERNOVA EVOLUTION; WIND-DRIVEN BUBBLES; II
SUPERNOVAE; CIRCUMSTELLAR MEDIUM; MASSIVE STARS; IA SUPERNOVA; RADIO
OBSERVATIONS; CIRCINUS GALAXY; LIGHT ECHOES
AB We report on new VLT optical spectroscopic and multiwavelength archival observations of SN 1996cr, a previously identified ultraluminous X-ray source known as Circinus galaxy X-2. Our optical spectrum confirms SN 1996cr as a bona fide Type IIn supernova, while archival imaging from the Anglo-Australian Telescope archive isolates the explosion date to between 1995 February 28 and 1996 March 16. SN 1996cr is one of the closest SNe (approximate to 3.8 Mpc) in the last several decades, and in terms of flux ranks among the brightest radio and X-ray SNe ever detected. The wealth of optical, X-ray, and radio observations that exist for this source provide relatively detailed constraints on its postexplosion expansion and progenitor history, including a preliminary angular size constraint from VLBI. Archival X-ray and radio data imply that the progenitor of SN 1996cr evacuated a large cavity just prior to exploding: the blast wave likely spent similar to 1-2 yr in relatively uninhibited expansion before eventually striking the dense circumstellar material which surrounds SN 1996cr. The X-ray and radio emission, which trace the progenitor mass-loss rate, have respectively risen by a factor of greater than or similar to 2 and remained roughly constant over the past 7 years. This behavior is reminiscent of the late rise of SN 1987A, but 1000 times more luminous and much more rapid to onset. SN 1996cr may likewise provide us with a younger example of SN 1978K and SN 1979C, both of which exhibit flat X-ray evolution at late times. Complex oxygen line emission hints at a possible concentric shell or ringlike structure. The discovery of SN 1996cr suggests that a substantial fraction of the closest SNe observed in the last several decades have occurred in wind-blown bubbles, and argues for the phenomena being widespread.
C1 [Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Immler, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smartt, S.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Bartel, N.; Bietenholz, M. F.] York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada.
[Bietenholz, M. F.] Hartebeesthoek Radio Observ, ZA-1740 Krugersdorp, South Africa.
EM feb@astro.columbia.edu
RI Brandt, William/N-2844-2015
OI Brandt, William/0000-0002-0167-2453
FU Chandra Postdoctoral Fellowship Award [PF4- 50032]; NSF award [AST-
0319261]; NASA STScI [HST- AR- 10649]; NASA LTSA [NAG5- 13035];
Leverhulme Trust; ESF EURYI scheme
FX We thank Bjorn Emonts and Bryan Gaensler for help in reducing archival
ATCA observations, Roger Chevalier, Claes Frannson, Dick McCray, Kurt
Weiler, and Christopher Stockdale for useful discussions about the
nature of the multiwavelength emission, Baerbel Koribalski for
increasing our awareness of Australian online archives and access to
proprietary ATCA observations, Ernesto Oliva and Alessandro Marconi for
access to reduced NTT data, Bruno Leibundgut and Rob Fesen for their
spectra of SN 1986J and SN 1979C, Philip Edwards, Steven Tingay, and
Tasso Tzioumis for support of the VLBI observations, Kevin Hurley for
directing us to revised IPN results which allowed us to reject an
otherwise tentative GRB identification, John Raymond for helping to
improve our emission- line tables, and the anonymous referee for useful
comments that improved the content and presentation of the paper. We
gratefully acknowledge the financial support of Chandra Postdoctoral
Fellowship Award PF4- 50032 (F.E.B.), NSF award AST- 0319261 (V.V.D.),
NASA STScI grant HST- AR- 10649 (V.V.D.), NASA LTSA grant NAG5- 13035
(W.N.B.), the Leverhulme Trust (S.J.S.) and the ESF EURYI scheme
(S.J.S.).
NR 134
TC 30
Z9 30
U1 0
U2 4
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2008
VL 688
IS 2
BP 1210
EP 1234
DI 10.1086/589761
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 373VU
UT WOS:000261002400039
ER
PT J
AU Bitner, MA
Richter, MJ
Lacy, JH
Herczeg, GJ
Greathouse, TK
Jaffe, DT
Salyk, C
Blake, GA
Hollenbach, DJ
Doppmann, GW
Najita, JR
Currie, T
AF Bitner, Martin A.
Richter, Matthew J.
Lacy, John H.
Herczeg, Gregory J.
Greathouse, Thomas K.
Jaffe, Daniel T.
Salyk, Colette
Blake, Geoffrey A.
Hollenbach, David J.
Doppmann, Greg W.
Najita, Joan R.
Currie, Thayne
TI THE TEXES SURVEY FOR H-2 EMISSION FROM PROTOPLANETARY DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE circumstellar matter; infrared: stars; planetary systems: protoplanetary
disks; stars: individual (AB Aur, DoAr 21, Elias 29, GSS 30 IRS 1, GV
Tau N, HL Tau); stars: pre-main-sequence
ID T-TAURI STARS; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS;
MOLECULAR-HYDROGEN EMISSION; RHO-OPHIUCHI CLOUD; CO LINE EMISSION;
SPACE-OBSERVATORY OBSERVATIONS; X-RAY OBSERVATIONS; HERBIG AE STARS;
HIGH-RESOLUTION
AB We report the results of a search for pure rotational molecular hydrogen emission from the circumstellar environments of young stellar objects with disks using the Texas Echelon Cross Echelle Spectrograph (TEXES) on the NASA Infrared Telescope Facility and the Gemini North Observatory. We searched for mid-infrared H-2 emission in the S(1), S(2), and S(4) transitions. Keck/NIRSPEC observations of the H-2 S(9) transition were included for some sources as an additional constraint on the gas temperature. We detected H-2 emission from 6 of 29 sources observed: AB Aur, DoAr 21, Elias 29, GSS 30 IRS 1, GV Tau N, and HL Tau. Four of the six targets with detected emission are class I sources that show evidence for surrounding material in an envelope in addition to a circumstellar disk. In these cases, we show that accretion shock heating is a plausible excitation mechanism. The detected emission lines are narrow (similar to 10 km s(-1)), centered at the stellar velocity, and spatially unresolved at scales of 0.4 '', which is consistent with origin from a disk at radii 10-50 AU from the star. In cases where we detect multiple emission lines, we derive temperatures greater than or similar to 500 K from similar to 1 M-circle plus of gas. Our upper limits for the nondetections place upper limits on the amount of H-2 gas with T > 500 K of less than a few Earth masses. Such warm gas temperatures are significantly higher than the equilibrium dust temperatures at these radii, suggesting that the gas is decoupled from the dust in the regions that we are studying and that processes such as UV, X-ray, and accretion heating may be important.
C1 [Bitner, Martin A.; Lacy, John H.; Jaffe, Daniel T.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Richter, Matthew J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Herczeg, Gregory J.; Salyk, Colette; Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Greathouse, Thomas K.] SW Res Inst, San Antonio, TX 78209 USA.
[Hollenbach, David J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Doppmann, Greg W.; Najita, Joan R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Currie, Thayne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Bitner, MA (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
EM mbitner@astro.as.utexas.edu
OI Greathouse, Thomas/0000-0001-6613-5731; Herczeg,
Gregory/0000-0002-7154-6065
FU NSF [AST 06-07312, AST 07-08074]; NASA [NNG04GG92G]
FX 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. We thank the
Gemini staff, and John White in particular, for their support of TEXES
observations on Gemini North. The development of TEXES was supported by
grants from the NSF and the NASA/USRA SOFIA project. Modification of
TEXES for use on Gemini was supported by Gemini Observatory.
Observations with TEXES were supported by NSF grant AST 06-07312. M.J.R.
acknowledges support from NSF grant AST 07-08074 and NASA grant
NNG04GG92G. 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. This work is 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 Particle Physics and Astronomy Research Council
(United Kingdom), the National Research Council (Canada), CONICYT
(Chile), the Australian Research
NR 145
TC 30
Z9 30
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2008
VL 688
IS 2
BP 1326
EP 1344
DI 10.1086/592317
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 373VU
UT WOS:000261002400049
ER
PT J
AU Dodson-Robinson, SE
Bodenheimer, P
Laughlin, G
Willacy, K
Turner, NJ
Beichman, CA
AF Dodson-Robinson, Sarah E.
Bodenheimer, Peter
Laughlin, Gregory
Willacy, Karen
Turner, Neal J.
Beichman, C. A.
TI SATURN FORMS BY CORE ACCRETION IN 3.4 Myr
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: formation; planets and satellites: individual
(Saturn)
ID GIANT PLANETS; OLIGARCHIC GROWTH; SOLAR-SYSTEM; JUPITER; MODELS; DISKS;
GAS; PROTOPLANETS; CLOUD
AB We present two new in situ core accretion simulations of Saturn with planet formation timescales of 3.37 Myr (model S0) and 3.48 Myr (model S1), consistent with observed protostellar disk lifetimes. In model S0, we assume rapid grain settling reduces opacity due to grains from full interstellar values. In model S1, we do not invoke grain settling, instead assigning full interstellar opacities to grains in the envelope. Surprisingly, the two models produce nearly identical formation timescales and core/atmosphere mass ratios. We therefore observe a new manifestation of core accretion theory: at large heliocentric distances, the solid core growth rate (limited by Keplerian orbital velocity) controls the planet formation timescale. We argue that this paradigm should apply to Uranus and Neptune as well.
C1 [Dodson-Robinson, Sarah E.; Beichman, C. A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Bodenheimer, Peter; Laughlin, Gregory] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Willacy, Karen; Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Dodson-Robinson, SE (reprint author), CALTECH, NASA, Exoplanet Sci Inst, 770 S Wilson Ave, Pasadena, CA 91125 USA.
EM sdr@ipac.caltech.edu; chas@ipac.caltech.edu
FU NSF Career [AST-0449986]; NASA Planetary Geology and Geophysics Program
[NNG04GK19G]; NSF [AST-0507424]; NASA [NNX08AH82G]; National Aeronautics
and Space Administration; JPL Research and Technology Development
Program
FX We thank Geoff Bryden and Jonathan Fortney for helpful conversations and
the anonymous referee for suggesting model S1. This research was
supported by a scholarship award from the Achievement Rewards for
College Scientists Foundation to S. D. R.; by NSF Career Grant
AST-0449986 and NASA Planetary Geology and Geophysics Program Grant
NNG04GK19G to G. L.; and by NSF Grant AST-0507424 and NASA Origins Grant
NNX08AH82G to P. B. The work of K. W. and N. T. was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration, with
funding provided by the JPL Research and Technology Development Program.
NR 28
TC 31
Z9 31
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 1
PY 2008
VL 688
IS 2
BP L99
EP L102
DI 10.1086/595616
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 398LG
UT WOS:000262733000011
ER
PT J
AU Jess, DB
Mathioudakis, M
Crockett, PJ
Keenan, FP
AF Jess, D. B.
Mathioudakis, M.
Crockett, P. J.
Keenan, F. P.
TI DO ALL FLARES HAVE WHITE-LIGHT EMISSION?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: activity; Sun: evolution; Sun: flares; Sun: photosphere; sunspots
ID CONTINUUM EMISSION; INFRARED CONTINUUM; TRANSITION-REGION;
CORONAL-EXPLORER; SOLAR-FLARES; YOHKOH; RESOLUTION; TELESCOPE; SUNSPOTS;
HINODE
AB High-cadence, multiwavelength optical observations of a solar active region (NOAA AR 10969), obtained with the Swedish Solar Telescope, are presented. Difference imaging of white light continuum data reveals a white-light brightening, 2 minutes in duration, linked to a cotemporal and cospatial C2.0 flare event. The flare kernel observed in the white-light images has a diameter of 300 km, thus rendering it below the resolution limit of most space-based telescopes. Continuum emission is present only during the impulsive stage of the flare, with the effects of chromospheric emission subsequently delayed by approximate to 2 minutes. The localized flare emission peaks at 300% above the quiescent flux. This large, yet tightly confined, increase in emission is only resolvable due to the high spatial resolution of the Swedish Solar Telescope. An investigation of the line-of-sight magnetic field derived from simultaneous MDI data shows that the continuum brightening is located very close to a magnetic polarity inversion line. In addition, an Ha flare ribbon is directed along a region of rapid magnetic energy change, with the footpoints of the ribbon remaining cospatial with the observed white-light brightening throughout the duration of the flare. The observed flare parameters are compared with current observations and theoretical models for M- and X-class events and we determine the observed white-light emission is caused by radiative back-warming. We suggest that the creation of white-light emission is a common feature of all solar flares.
C1 [Jess, D. B.; Mathioudakis, M.; Crockett, P. J.; Keenan, F. P.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Jess, D. B.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Jess, DB (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
EM djess01@qub.ac.uk
FU Northern Ireland Department for Employment and Learning studentship;
Optical Infrared Coordination network (OPTICON); Research
Infrastructures Programme of the European Commissions Sixth Framework
Programme
FX D. B. J. is supported by a Northern Ireland Department for Employment
and Learning studentship. D. B. J. additionally thanks NASA Goddard
Space Flight Center for a CAST studentship. F. P. K. is grateful to A.
W. E. Aldermaston for the award of aWilliam Penney Fellowship. The
Swedish 1 m Solar Telescope is operated on the island of La Palma 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. These observations have been funded by the
Optical Infrared Coordination network (OPTICON), a major international
collaboration supported by the Research Infrastructures Programme of the
European Commissions Sixth Framework Programme.
NR 33
TC 50
Z9 50
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 1
PY 2008
VL 688
IS 2
BP L119
EP L122
DI 10.1086/595588
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 398LG
UT WOS:000262733000016
ER
PT J
AU Velusamy, T
Peng, R
Li, D
Goldsmith, PF
Langer, WD
AF Velusamy, T.
Peng, R.
Li, D.
Goldsmith, P. F.
Langer, William D.
TI DICHOTOMY IN THE DYNAMICAL STATUS OF MASSIVE CORES IN ORION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: clouds; ISM: individual (Orion); ISM: kinematics and dynamics; ISM:
molecules; stars: formation
ID PROTOSTELLAR COLLAPSE; STARLESS CORES; QUIESCENT CORES; INFALL MOTIONS;
LINE-PROFILES; CLOUD CORES; OBJECTS; SEARCH; STARS; B335
AB To study the evolution of high-mass cores, we have searched for evidence of collapse motions in a large sample of starless cores in the Orion molecular cloud. We used the Caltech Submillimeter Observatory telescope to obtain spectra of the optically thin (H(13)CO(+)) and optically thick (HCO(+)) high-density tracer molecules in 27 cores with masses >1 M(circle dot). The red-and blue-asymmetries seen in the line profiles of the optically thick line, with respect to the optically thin line indicate that 2/3 of these cores are not static. We detect evidence for infall (inward motions) in 9 cores and outward motions for 10 cores, suggesting a dichotomy in the kinematic state of the nonstatic cores in this sample. Our results provide an important observational constraint on the fraction of collapsing (inward motions) versus noncollapsing (reexpanding) cores for comparison with model simulations.
C1 [Velusamy, T.; Li, D.; Goldsmith, P. F.; Langer, William D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Peng, R.] Caltech Submillimeter Observ, Hilo, HI 96720 USA.
RP Velusamy, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Velusamy@jpl.nasa.gov; peng@submm.caltech.edu
RI Goldsmith, Paul/H-3159-2016
FU NASA Astronomy and Physics Research and Analysis Program; NSF
[AST-0229008]
FX Letter was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration and supported by a grant from NASA Astronomy
and Physics Research and Analysis Program. Research at the Caltech
Submillimeter Observatory is supported by NSF grant AST-0229008.
NR 21
TC 13
Z9 13
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 1
PY 2008
VL 688
IS 2
BP L87
EP L90
DI 10.1086/595585
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 398LG
UT WOS:000262733000008
ER
EF