FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Kim, Y
Kimball, JS
McDonald, KC
Glassy, J
AF Kim, Youngwook
Kimball, John S.
McDonald, Kyle C.
Glassy, Joseph
TI Developing a Global Data Record of Daily Landscape Freeze/Thaw Status
Using Satellite Passive Microwave Remote Sensing
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Earth system data record; freeze/thaw; Making Earth System Data Records
for Use in Research Environments; passive microwave remote sensing;
radiometry; soil moisture active passive; Special Sensor Microwave
Imager
ID NASA SCATTEROMETER NSCAT; SNOW-COVER; CARBON SEQUESTRATION; BOREAL;
THAW; FORESTS; CLIMATE; SSM/I; REANALYSIS; SCALE
AB The landscape freeze-thaw (F/T) state parameter derived from satellite microwave remote sensing is closely linked to the surface energy budget, hydrological activity, vegetation growing season dynamics, terrestrial carbon budgets, and land-atmosphere trace gas exchange. Satellite microwave remote sensing is well suited for global F/T monitoring due to its insensitivity to atmospheric contamination and solar illumination effects, and its strong sensitivity to the relationship between landscape dielectric properties and predominantly frozen and thawed conditions. We investigated the utility of multifrequency and dual polarization brightness temperature (T-b) measurements from the Special Sensor Microwave Imager (SSM/I) to map global patterns and daily variations in terrestrial F/T cycles. We defined a global F/T classification domain by examining biophysical cold temperature constraints to vegetation growing seasons. We applied a temporal change classification algorithm based on a seasonal thresholding scheme to classify daily F/T states from time series T-b measurements. The SSM/I F/T classification accuracy was assessed using in situ air temperature measurements from the global WMO weather station network. A single-channel classification of 37 GHz, V-polarization T-b time series provided generally improved performance over other SSM/I frequencies, polarizations and channel combinations. Mean annual F/T classification accuracies were 92.2 +/- 0.8 [SD] % and 85.0 +/- 0.7 [SD] % for respective SSM/I time series of P.M. and A.M. orbital nodes over the global domain and a 20-year (1988-2007) satellite record. The resulting database provides a continuous and relatively long-term record of daily F/T dynamics for the global biosphere with well-defined accuracy.
C1 [Kim, Youngwook] Univ Montana, FLBS NTSG, Missoula, MT 59812 USA.
[Kimball, John S.] Univ Montana, Div Biol Sci, Missoula, MT 59812 USA.
[McDonald, Kyle C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Glassy, Joseph] Lupine Log Inc, Missoula, MT 59812 USA.
RP Kim, Y (reprint author), Univ Montana, FLBS NTSG, Missoula, MT 59812 USA.
EM youngwook.kim@ntsg.umt.edu; johnk@ntsg.umt.edu;
kyle.c.mcdonald@jpl.nasa.gov; joe.glassy@ntsg.umt.edu
FU NASA [NNH06ZDA001N-MEaSUREs]
FX Manuscript received March 29, 2010; revised June 15, 2010; accepted
August 5, 2010. Date of publication October 14, 2010; date of current
version February 25, 2011. This work is supported in part by the NASA
Making Earth System Data Records for Use in Research Environments
(MEaSUREs) program under NNH06ZDA001N-MEaSUREs.
NR 65
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U1 3
U2 27
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2011
VL 49
IS 3
BP 949
EP 960
DI 10.1109/TGRS.2010.2070515
PG 12
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 725PN
UT WOS:000287658000005
ER
PT J
AU Arii, M
van Zyl, JJ
Kim, Y
AF Arii, Motofumi
van Zyl, Jakob J.
Kim, Yunjin
TI Adaptive Model-Based Decomposition of Polarimetric SAR Covariance
Matrices
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Adaptive nonnegative eigenvalue decomposition (NNED); model-based
decomposition; radar polarimetry
ID CLASSIFICATION; SCATTERING; AREAS
AB Previous model-based decomposition techniques are applicable to a limited range of vegetation types because of their specific assumptions about the volume scattering component. Furthermore, most of these techniques use the same model, or just a few models, to characterize the volume scattering component in the decomposition for all pixels in an image. In this paper, we extend the model-based decomposition idea by creating an adaptive model-based decomposition technique, allowing us to estimate both the mean orientation angle and a degree of randomness for the canopy scattering for each pixel in an image. No scattering reflection symmetry assumption is required to determine the volume contribution. We examined the usefulness of the proposed decomposition technique by decomposing the covariance matrix using the National Aeronautics and Space Administration/Jet Propulsion Laboratory Airborne Synthetic Aperture Radar data at the C-, L-, and P-bands. The randomness and mean orientation angle maps generated using our adaptive decomposition significantly improve the physical interpretation of the scattering observed at the three different frequencies.
C1 [Arii, Motofumi] Mitsubishi Space Software Co Ltd, Kamakura, Kanagawa 2470065, Japan.
[van Zyl, Jakob J.; Kim, Yunjin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Arii, M (reprint author), Mitsubishi Space Software Co Ltd, Kamakura, Kanagawa 2470065, Japan.
EM motofumi@gmail.com
NR 17
TC 82
Z9 94
U1 0
U2 12
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2011
VL 49
IS 3
BP 1104
EP 1113
DI 10.1109/TGRS.2010.2076285
PG 10
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 725PN
UT WOS:000287658000018
ER
PT J
AU Gabb, TP
Kantzos, PT
Telesman, J
Gayda, J
Sudbrack, CK
Palsa, B
AF Gabb, T. P.
Kantzos, P. T.
Telesman, J.
Gayda, J.
Sudbrack, C. K.
Palsa, B.
TI Fatigue resistance of the grain size transition zone in a dual
microstructure superalloy disk
SO INTERNATIONAL JOURNAL OF FATIGUE
LA English
DT Article
DE Superalloy; Disk; Dual microstructure; Transition zone; Fatigue
AB Mechanical property requirements vary with location in nickel-based superalloy disks In order to maximize the associated mechanical properties heat treatment methods have been developed for producing tailored microstructures In this study a specialized heat treatment method was applied to produce varying grain microstructures from the bore to the rim portions of a powder metallurgy processed nickel-based superalloy disk The bore of the contoured disk consisted of fine grains to maximize strength and fatigue resistance at lower temperatures The nm microstructure of the disk consisted of coarse grains for maximum resistance to creep and dwell crack growth at high temperatures up to 704 degrees C However the fatigue resistance of the grain size transition zone was unclear and needed to be evaluated This zone was located as a band in the disk web between the bore and rim Specimens were extracted parallel and transverse to the transition zone and multiple fatigue tests were performed at 427 degrees C and 704 degrees C Mean fatigue lives were lower at 427 degrees C than 704 degrees C Specimen failures often initiated at relatively large grains which failed on crystallographic facets Grain size distributions were characterized in the specimens and related to the grains initiating failures as well as location within the transition zone Fatigue life decreased with increasing maximum grain size Correspondingly mean fatigue resistance of the transition zone was slightly higher than that of the rim but lower than that of the bore The scatter in limited tests of replicates was comparable for all transition zone locations examined Published by Elsevier Ltd
C1 [Gabb, T. P.; Telesman, J.; Gayda, J.; Sudbrack, C. K.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Kantzos, P. T.] Honeywell Engine Syst, Phoenix, AZ 85034 USA.
[Palsa, B.] McGraw Hill Co Inc, Columbus, OH 43202 USA.
RP Gabb, TP (reprint author), NASA Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
FU NASA
FX The authors wish to acknowledge the support of the NASA Aviation Safety
program Disk forging was performed at PCC Wyman-Gordon Forgings under
the direction of Ian Dempster Disk heat treatments were performed at
Ladish Forgings Inc under the direction of Joe Lemsky and David Furrer
now at Rolls-Royce Aircraft Engines
NR 24
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U1 1
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0142-1123
J9 INT J FATIGUE
JI Int. J. Fatigue
PD MAR
PY 2011
VL 33
IS 3
BP 414
EP 426
DI 10.1016/j.ijfatigue.2010.09.022
PG 13
WC Engineering, Mechanical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 692QP
UT WOS:000285170500013
ER
PT J
AU Schwaller, MR
Morris, KR
AF Schwaller, Mathew R.
Morris, K. Robert
TI A Ground Validation Network for the Global Precipitation Measurement
Mission
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID RADAR OBSERVATIONS; TRMM SATELLITE; ORBIT; SITE
AB A prototype Validation Network (VN) is currently operating as part of the Ground Validation System for NASA's Global Precipitation Measurement (GPM) mission. The VN supports precipitation retrieval algorithm development in the GPM prelaunch era. Post launch, the VN will be used to validate GPM spacecraft instrument measurements and retrieved precipitation data products.
The period of record for the VN prototype starts on 8 August 2006 and runs to the present day. The VN database includes spacecraft data from the Tropical Rainfall Measuring Mission (TRMM) precipitation radar (PR) and coincident ground radar (GR) data from operational meteorological networks in the United States, Australia, Korea, and the Kwajalein Atoll in the Marshall Islands. Satellite and ground radar data products are collected whenever the PR satellite track crosses within 200 km of a VN ground radar, and these data are stored permanently in the VN database. VN products are generated from coincident PR and GR observations when a significant rain event occurs.
The VN algorithm matches PR and GR radar data (including retrieved precipitation data in the case of the PR) by calculating averages of PR reflectivity (both raw and attenuation corrected) and rain rate, and GR reflectivity at the geometric intersection of the PR rays with the individual GR elevation sweeps. The algorithm thus averages the minimum PR and GR sample volumes needed to "matchup" the spatially coincident PR and GR data types. The result of this technique is a set of vertical profiles for a given rainfall event, with coincident PR and GR samples matched at specified heights throughout the profile.
VN data can be used to validate satellite measurements and to track ground radar calibration over time. A comparison of matched TRMM PR and GR radar reflectivity factor data found a remarkably small difference between the PR and GR radar reflectivity factor averaged over this period of record in stratiform and convective rain cases when samples were taken from high in the atmosphere. A significant difference in PR and GR reflectivity was found in convective cases, particularly in convective samples from the lower part of the atmosphere. In this case, the mean difference between PR and corrected GR reflectivity was -1.88 dBZ. The PR-GR bias was found to increase with the amount of PR attenuation correction applied, with the PR-GR bias reaching -3.07 dBZ in cases where the attenuation correction applied is >6 dBZ. Additional analysis indicated that the version 6 TRMM PR retrieval algorithm underestimates rainfall in case of convective rain in the lower part of the atmosphere by 30%-40%.
C1 [Schwaller, Mathew R.; Morris, K. Robert] NASA, Global Precipitat Measurement Project, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Morris, K. Robert] Sci Applicat Int Corp, Beltsville, MD USA.
RP Schwaller, MR (reprint author), NASA, Global Precipitat Measurement Project, Goddard Space Flight Ctr, Mail Code 422-587, Greenbelt, MD 20771 USA.
EM mathew.r.schwaller@nasa.gov
RI Measurement, Global/C-4698-2015
FU NASA's Global Precipitation Measuring Mission
FX The Validation Network is supported as part of NASA's Global
Precipitation Measuring Mission. The authors wish to acknowledge the
contributions of Jason Pippitt from the TRMM Ground Validation office,
who performs quality control of the ground radar data used in the VN. We
also gratefully acknowledge the ground radar data provided by Jun Park
and Mi-Lim Ou of the Korean Meteorological Administration (Gosan radar),
Walter Petersen of NASA's Marshall Space Flight Center (ARMOR radar),
Elizabeth Ebert from the Australian Bureau of Meteorology (Darwin
radar), and David Wolff of NASA's Goddard Space Flight Center (Kwajalein
radar).
NR 23
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U1 0
U2 12
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD MAR
PY 2011
VL 28
IS 3
BP 301
EP 319
DI 10.1175/2010JTECHA1403.1
PG 19
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 743VD
UT WOS:000289045900001
ER
PT J
AU Molthan, AL
Petersen, WA
AF Molthan, Andrew L.
Petersen, Walter A.
TI Incorporating Ice Crystal Scattering Databases in the Simulation of
Millimeter-Wavelength Radar Reflectivity
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID BULK PARAMETERIZATION; SIZE DISTRIBUTIONS; WATER-CONTENT; IN-SITU; PART
I; CLOUDS; SNOW; PRECIPITATION; MODEL; MICROPHYSICS
AB The Canadian Cloud/Sat/Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) Validation Project (C3VP) was designed to acquire aircraft, surface, and satellite observations of particle size distributions during cold season precipitation events for the purposes of validating and improving upon satellite-based retrievals of precipitation and the representation of cloud and precipitation processes within numerical weather prediction schemes. During an intensive observation period on 22 January 2007, an instrumented aircraft measured ice crystal size distributions, ice and liquid water contents, and atmospheric state parameters within a broad shield of precipitation generated by a passing midlatitude cyclone. The 94-GHz Cloud Sat radar acquired vertical profiles of radar reflectivity within light to moderate snowfall, coincident with C3VP surface and aircraft instrumentation. Satellite-based retrievals of cold season precipitation require relationships between remotely sensed quantities, such as radar reflectivity or brightness temperature, and the ice water content present within the sampled profile.
In this study, three methods for simulating Cloud Sat radar reflectivity are investigated by comparing Mie spheres, single dendrites, and fractal aggregates represented within scattering databases or parameterizations. It is demonstrated that calculations of radar backscatter from nonspherical crystal shapes are required to represent the vertical trend in CloudSat radar reflectivity for this particular event, as Mie resonance effects reduce the radar backscatter from precipitation-sized particles larger than 1 mm. Remaining differences between reflectivity from nonspherical shapes and observations are attributed to uncertainty in the mass diameter relationships for observed crystals and disparities between naturally occurring crystals and shapes assumed in the development of ice crystal scattering databases and parameterizations.
C1 [Molthan, Andrew L.] NASA, Earth Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35802 USA.
RP Molthan, AL (reprint author), NASA, Earth Sci Off, George C Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35802 USA.
EM andrew.molthan@nasa.gov
FU NASA; Canadian Space Agency; NASA Marshall Space Flight Center
FX Petersen acknowledges funding from the NASA Precipitation Measurement
Mission via Dr. Ramesh Kakar, and the Global Precipitation Mission
Science Project Scientist (Dr. Arthur Hou) and Project Offices (Dr.
Mathew Schwaller). Prime funding for aircraft studies during the
Canadian CloudSat/CALIPSO Validation Project was provided by the
Canadian Space Agency. The lead author was supported in part by the
Cooperative Education Program at NASA Marshall Space Flight Center, and
thanks three anonymous reviewers for constructive comments that improved
the clarity of the final published manuscript.
NR 33
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U1 3
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD MAR
PY 2011
VL 28
IS 3
BP 337
EP 351
DI 10.1175/2010JTECHA1511.1
PG 15
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 743VD
UT WOS:000289045900003
ER
PT J
AU Gibert, F
Koch, GJ
Beyon, JY
Hilton, TW
Davis, KJ
Andrews, A
Flamant, PH
Singh, UN
AF Gibert, Fabien
Koch, Grady J.
Beyon, Jeffrey Y.
Hilton, Timothy W.
Davis, Kenneth J.
Andrews, Arlyn
Flamant, Pierre H.
Singh, Upendra N.
TI Can CO2 Turbulent Flux Be Measured by Lidar? A Preliminary Study
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID CONVECTIVE BOUNDARY-LAYER; DIFFERENTIAL ABSORPTION; DOPPLER LIDAR;
CARBON-DIOXIDE; MIXING-RATIO; WATER-VAPOR; (CO2)-C-12-O-16;
OPTIMIZATION; STATISTICS; PARAMETERS
AB The vertical profiling of CO2 turbulent fluxes in the atmospheric boundary layer (ABL) is investigated using a coherent differential absorption lidar (CDIAL) operated nearby a tall tower in Wisconsin during June 2007. A CDIAL can perform simultaneous range-resolved CO2 DIAL and velocity measurements. The lidar eddy covariance technique is presented. The aims of the study are (i) an assessment of performance and current limitation of available CDIAL for CO2 turbulent fluxes and (ii) the derivation of instrument specifications to build a future CDIAL to perform accurate range-resolved CO2 fluxes. Experimental lidar CO2 mixing ratio and vertical velocity profiles are successfully compared with in situ sensors measurements. Time a.-id space integral scales of turbulence in the AB L are addressed that result in limitation for time averaging and range accumulation. A first attempt to infer CO2 fluxes using an eddy covariance technique with currently available 2-mu m CDIAL dataset is reported.
C1 [Gibert, Fabien; Flamant, Pierre H.] Ecole Polytech, IPSL, LMD, Palaiseau, France.
[Gibert, Fabien; Hilton, Timothy W.; Davis, Kenneth J.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Koch, Grady J.; Beyon, Jeffrey Y.; Singh, Upendra N.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Andrews, Arlyn] NOAA, Earth Syst Res Lab, Boulder, CO USA.
RP Gibert, F (reprint author), Ecole Polytech, IPSL, LMD, Palaiseau, France.
EM fabien.gibert@lmd.polytechnique.fr
RI Andrews, Arlyn/K-3427-2012;
OI Hilton, Timothy/0000-0001-9575-9850
FU NASA
FX This research was funded by the NASA Instrument Incubator Program and
NASA Laser Risk Reduction Program. We thank R. Strand and J. Ayers of
the Wisconsin Educational Communications Board for hosting the lidar at
the WLEF tower.
NR 29
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U1 0
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD MAR
PY 2011
VL 28
IS 3
BP 365
EP 377
DI 10.1175/2010JTECHA1446.1
PG 13
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 743VD
UT WOS:000289045900005
ER
PT J
AU Semedo, A
Suselj, K
Rutgersson, A
Sterl, A
AF Semedo, Alvaro
Suselj, Kay
Rutgersson, Anna
Sterl, Andreas
TI A Global View on the Wind Sea and Swell Climate and Variability from
ERA-40
SO JOURNAL OF CLIMATE
LA English
DT Article
ID MARINE BOUNDARY-LAYER; OBSERVING SHIP DATA; NORTH-ATLANTIC; WAVE
CLIMATE; OCEAN WIND; SOUTHERN-HEMISPHERE; REANALYSIS; PACIFIC; TRENDS;
STORMS
AB In this paper a detailed global climatology of wind-sea and swell parameters, based on the 45-yr European Centre for Medium-Range Weather Forecasts Re-Analysis (ERA-40) wave reanalysis is presented. The spatial pattern of the swell dominance of the earth's oceans, in terms of the wave field energy balance and wave field characteristics, is also investigated. Statistical analysis shows that the global ocean is strongly dominated by swell waves. The interannual variability of the wind-sea and swell significant wave heights, and how they are related to the resultant significant wave height, is analyzed over the Pacific, Atlantic, and Indian Oceans. The leading modes of variability of wind sea and swell demonstrate noticeable differences, particularly in the Pacific and Atlantic Oceans. During the Northern Hemisphere winter, a strong north south swell propagation pattern is observed in the Atlantic Ocean. Statistically significant secular increases in the wind-sea and swell significant wave heights are found in the North Pacific and North Atlantic Oceans.
C1 [Semedo, Alvaro; Rutgersson, Anna] Uppsala Univ, Dept Earth Sci, SE-75236 Uppsala, Sweden.
[Semedo, Alvaro] CINAV, Escola Naval, Lisbon, Portugal.
[Suselj, Kay] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Sterl, Andreas] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands.
RP Semedo, A (reprint author), Uppsala Univ, Dept Earth Sci, Villavagen 16, SE-75236 Uppsala, Sweden.
EM alvaro.semedo@met.uu.se
RI Semedo, Alvaro/B-1615-2016;
OI Semedo, Alvaro/0000-0003-1016-5223; Semedo, Alvaro/0000-0002-2434-8517;
Sterl, Andreas/0000-0003-3457-0434
FU European Commission [MRTN-CT-2005-019369]
FX Alvaro Semedo and Kay Suselj were funded by the European Commission's
ModObs project under Contract MRTN-CT-2005-019369. We greatly
appreciated the help of Jean Bidlot from ECMWF (Reading, United Kingdom)
with the many details of the ERA-40 wave data.
NR 62
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U1 2
U2 21
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD MAR 1
PY 2011
VL 24
IS 5
BP 1461
EP 1479
DI 10.1175/2010JCLI3718.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 743NQ
UT WOS:000289025500011
ER
PT J
AU Lewis, A
Challinor, A
Hanson, D
AF Lewis, Antony
Challinor, Anthony
Hanson, Duncan
TI The shape of the CMB lensing bispectrum
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE gravitational lensing; non-gaussianity; integrated Sachs-Wolfe effect;
CMBR theory
ID MICROWAVE BACKGROUND ANISOTROPIES; NON-GAUSSIANITY; POLARIZATION
AB Lensing of the CMB generates a significant bispectrum, which should be detected by the Planck satellite at the 5-sigma level and is potentially a non-negligible source of bias for f(NL) estimators of local non-Gaussianity. We extend current understanding of the lensing bispectrum in several directions: (1) we perform a non-perturbative calculation of the lensing bispectrum which is similar to 10% more accurate than previous, first-order calculations; (2) we demonstrate how to incorporate the signal variance of the lensing bispectrum into estimates of its amplitude, providing a good analytical explanation for previous Monte-Carlo results; and (3) we discover the existence of a significant lensing bispectrum in polarization, due to a previously-unnoticed correlation between the lensing potential and E-polarization as large as 30% at low multipoles. We use this improved understanding of the lensing bispectra to re-evaluate Fisher-matrix predictions, both for Planck and cosmic variance limited data. We confirm that the non-negligible lensing-induced bias for estimation of local non-Gaussianity should be robustly treatable, and will only inflate f(NL) error bars by a few percent over predictions where lensing effects are completely ignored (but note that lensing must still be accounted for to obtain unbiased constraints). We also show that the detection significance for the lensing bispectrum itself is ultimately limited to 9 sigma by cosmic variance. The tools that we develop for non-perturbative calculation of the lensing bispectrum are directly relevant to other calculations, and we give an explicit construction of a simple non-perturbative quadratic estimator for the lensing potential and relate its cross-correlation power spectrum to the bispectrum. Our numerical codes are publicly available as part of CAMB and LensPix.
C1 [Lewis, Antony] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Challinor, Anthony; Hanson, Duncan] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Challinor, Anthony; Hanson, Duncan] Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Challinor, Anthony] Univ Cambridge, Ctr Math Sci, DAMTP, Cambridge CB3 OWA, England.
[Hanson, Duncan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lewis, A (reprint author), Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
EM antony@cosmologist.info; adc1000@ast.cam.ac.uk;
Duncan.Hanson@jpl.nasa.gov
FU Science and Technology Facilities Council [ST/F002858/1, PP/C001214/2];
National Aeronautics and Space Administration
FX AL thanks James Fergusson for help with figure 6 and David Seery for
discussion. AL was supported by the Science and Technology Facilities
Council (grant numbers ST/F002858/1 and PP/C001214/2). Some of the
results in this paper have been derived using HealPix [37]. Part of the
research described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 49
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD MAR
PY 2011
IS 3
AR 018
DI 10.1088/1475-7516/2011/03/018
PG 40
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 772TE
UT WOS:000291258300018
ER
PT J
AU Kahn, RA
Garay, MJ
Nelson, DL
Levy, RC
Bull, MA
Diner, DJ
Martonchik, JV
Hansen, EG
Remer, LA
Tanre, D
AF Kahn, Ralph A.
Garay, Michael J.
Nelson, David L.
Levy, Robert C.
Bull, Michael A.
Diner, David J.
Martonchik, John V.
Hansen, Earl G.
Remer, Lorraine A.
Tanre, Didier
TI Response to "Toward unified satellite climatology of aerosol properties.
3. MODIS versus MISR versus AERONET"
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Aerosol retrieval; Satellite remote sensing; MISR; MODIS
ID MULTIANGLE IMAGING SPECTRORADIOMETER; OPTICAL DEPTH; SIZE DISTRIBUTIONS;
UNITED-STATES; DARK WATER; VALIDATION; OCEANS; SITES; CALIBRATION;
THICKNESS
AB A recent paper by Mishchenko et al. compares near-coincident MISR, MODIS, and AERONET aerosol optical depth (ACID), and gives a much less favorable impression of the utility of the satellite products than that presented by the instrument teams and other groups. We trace the reasons for the differing pictures to whether known and previously documented limitations of the products are taken into account in the assessments. Specifically, the analysis approaches differ primarily in (1) the treatment of outliers, (2) the application of absolute vs. relative criteria for testing agreement, and (3) the ways in which seasonally varying spatial distributions of coincident retrievals are taken into account. Mishchenko et al. also do not distinguish between observational sampling differences and retrieval algorithm error. We assess the implications of the different analysis approaches, and cite examples demonstrating how the MISR and MODIS aerosol products have been applied successfully to a range of scientific investigations. Published by Elsevier Ltd.
C1 [Kahn, Ralph A.; Remer, Lorraine A.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Garay, Michael J.; Nelson, David L.] Raytheon Co, Pasadena, CA 91101 USA.
[Levy, Robert C.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Bull, Michael A.; Diner, David J.; Martonchik, John V.; Hansen, Earl G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tanre, Didier] Univ Sci & Technol Lille, Villeneuve Dascq, France.
RP Kahn, RA (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
EM ralph.kahn@nasa.gov
RI Levy, Robert/M-7764-2013; Kahn, Ralph/D-5371-2012
OI Levy, Robert/0000-0002-8933-5303; Kahn, Ralph/0000-0002-5234-6359
FU NASA; EOS-MISR
FX We thank our colleagues Abhishek Chatterjee, Larry Di Girolamo, Thomas
Holzer-Popp, Alexander Marshak, Lazaros Oreopoulos, Jeffrey Pierce,
Bernard Pinty, and Michel Verstraete for providing reviews of previous
versions of the manuscript, and Jianglong Zhang and Jeff Reid for
helpful discussions and for sending their preprint in advance of
publication. The work of R. Kahn is supported in part by NASA's Climate
and Radiation Research and Analysis Program, under H. Maring, NASA's
Atmospheric Composition Program, and the EOS-MISR project.
NR 57
TC 32
Z9 33
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2011
VL 112
IS 5
BP 901
EP 909
DI 10.1016/j.jqsrt.2010.11.001
PG 9
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 727GS
UT WOS:000287786700015
ER
PT J
AU Ross, AJ
Steele, A
Fries, MD
Kater, L
Downes, H
Jones, AP
Smith, CL
Jenniskens, PM
Zolensky, ME
Shaddad, MH
AF Ross, Aidan J.
Steele, Andrew
Fries, Marc D.
Kater, Lukas
Downes, Hilary
Jones, Adrian P.
Smith, Caroline L.
Jenniskens, Peter M.
Zolensky, Michael E.
Shaddad, Muawia H.
TI MicroRaman spectroscopy of diamond and graphite in Almahata Sitta and
comparison with other ureilites
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID CHEMICAL-VAPOR-DEPOSITION; X-RAY-DIFFRACTION; RAMAN-SPECTROSCOPY;
HEXAGONAL DIAMOND; NOBLE-GAS; GROWTH DIAMONDS; RIES CRATER; THIN-FILMS;
ORIGIN; SHOCK
AB This work is the first detailed study of carbon phases in the ureilite Almahata Sitta (sample #7). We present microRaman data for diamond and graphite in Almahata Sitta, seven unbrecciated ureilites, and two brecciated ureilites. Diamond in Almahata Sitta was found to be distinct from that in unbrecciated and brecciated ureilites, although diamond in unbrecciated and brecciated ureilites is indistinguishable. Almahata Sitta diamond shows a peak center range of 1318.5-1330.2 cm-1 and a full width at half maximum (FWHM) range of 6.6-17.4 cm-1, representing a shock pressure of at least 60 kbar. The actual peak shock pressure may be higher than this due to postshock annealing, if shock synthesis is the source of ureilite diamonds. Diamond in unbrecciated and brecciated ureilites have peak center wave numbers closer to terrestrial kimberlite diamond, but show a wider range of FWHM than Almahata Sitta. The larger peak shift observed in Almahata Sitta may indicate the presence of lonsdaleite. Alternatively, the lower values in brecciated ureilites may be evidence of an annealing step either following the initial diamond-generating shock or as a consequence of heating during reconsolidation of the breccia. Graphite in Almahata Sitta shows a G-band peak center range of 1569.1-1577.1 cm-1 and a G-band FWHM range of 24.3-41.6 cm-1 representing a formation temperature of 990 +/- 120 degrees C. Amorphous carbon was also found. We examine the different theories for diamond formation in ureilites, such as chemical vapor deposition and shock origin from graphite, and explore explanations for the differences between Almahata Sitta and other ureilites.
C1 [Ross, Aidan J.; Downes, Hilary; Jones, Adrian P.] UCL Birkbeck Res Sch Earth Sci, Ctr Planetary Sci, London WC1E 6BT, England.
[Ross, Aidan J.; Downes, Hilary; Smith, Caroline L.] Nat Hist Museum, Dept Mineral, IARC, London SW7 5BD, England.
[Steele, Andrew; Kater, Lukas] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA.
[Fries, Marc D.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Fries, Marc D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Smith, Caroline L.] Univ Glasgow, Dept Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland.
[Jenniskens, Peter M.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Zolensky, Michael E.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Shaddad, Muawia H.] Univ Khartoum, Dept Phys & Astron, Khartoum 11115, Sudan.
RP Ross, AJ (reprint author), UCL Birkbeck Res Sch Earth Sci, Ctr Planetary Sci, Gower St, London WC1E 6BT, England.
EM aidan.ross@ucl.ac.uk
RI Jones, Adrian/D-4896-2013
OI Jones, Adrian/0000-0001-5137-5783
FU CIW; NASA; SRIDLA program; Keck Foundation; NERC (UK) through UCL
FX The authors gratefully acknowledge financial support from CIW, NASA
SRIDLA program, and the Keck Foundation. A. J. R. acknowledges receipt
of a NERC (UK) studentship award through UCL and CASE support from the
NHM. P. J. is supported by a grant from the NASA Planetary Astronomy
program. The sample of Almahata Sitta (sample #7) was provided to CIW by
Peter Jenniskens, and we are indebted to him, Muawia Shaddad, and the
students of the University of Khartoum for their dedication in
recovering this unique meteorite. We are grateful to the Natural History
Museum, London for samples of Dyalpur, Goalpara, and Hajmah (a). We
thank the NASA Meteorite Working Group (Johnson Space Center, Houston,
USA) for the sample of LAR 04315. DaG 319, DaG 868, and DaG 1047 were
purchased from Erich Haiderer, NWA 3140 from the Hupe Collection, and
Sahara 98505 from Planetary Meteorites. We thank A. Beard (Birkbeck) for
his assistance in preparation of thin sections made at UCL and B. Mysen
(CIW) for help with the JASCO. A. J. R. also thanks M. Lakin for proof
reading. We thank D. Hezel, D. Mittlefehldt, K. McNamara, F. Horz, A. El
Goresy, J. Matsuda, and P. De Carli for helpful discussions. M. Miyamoto
and an anonymous reviewer provided constructive reviews.
NR 66
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U1 1
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD MAR
PY 2011
VL 46
IS 3
BP 364
EP 378
DI 10.1111/j.1945-5100.2010.01157.x
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 736NH
UT WOS:000288500900002
ER
PT J
AU Romano, P
Mangano, V
Cusumano, G
Esposito, P
Evans, PA
Kennea, JA
Vercellone, S
La Parola, V
Krimm, HA
Burrows, DN
Gehrels, N
AF Romano, P.
Mangano, V.
Cusumano, G.
Esposito, P.
Evans, P. A.
Kennea, J. A.
Vercellone, S.
La Parola, V.
Krimm, H. A.
Burrows, D. N.
Gehrels, N.
TI Confirmation of the supergiant fast X-ray transient nature of AX
J1841.0-0536 from Swift outburst observations
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE X-rays: binaries; X-rays: individual: AX J1841.0-0536; X-rays:
individual: IGR J17544-2619
AB Swift observed an outburst from the supergiant fast X-ray transient (SFXT) AX J1841.0-0536 on 2010 June 5, and followed it with X-ray Telescope (XRT) for 11 d. The X-ray light curve shows an initial flare followed by a decay and subsequent increase, as often seen in other SFXTs, and a dynamical range of similar to 1600. Our observations allow us to analyse the simultaneous broad-band (0.3-100 keV) spectrum of this source, for the first time down to 0.3 keV, which can be fitted well with models usually adopted to describe the emission from accreting neutron stars in high-mass X-ray binaries, and is characterized by a high absorption (N-H similar to 2 x 10(22) cm(-2)), a flat power law (Gamma similar to 0.2) and a high-energy cut-off. All of these properties resemble those of the prototype of the class, IGR J17544-2619, which underwent an outburst on 2010 March 4, whose observations we also discuss. We show how well AX J1841.0-0536 fits in the SFXT class, based on its observed properties during the 2010 outburst, its large dynamical range in X-ray luminosity, the similarity of the light curve (length and shape) to those of the other SFXTs observed by Swift and the X-ray broad-band spectral properties.
C1 [Romano, P.; Mangano, V.; Cusumano, G.; Vercellone, S.; La Parola, V.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy.
[Esposito, P.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, Italy.
[Evans, P. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Kennea, J. A.; Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krimm, H. A.; Gehrels, N.] Univ Space Res Assoc, Columbia, MD 21044 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
OI La Parola, Valentina/0000-0002-8087-6488; Cusumano,
Giancarlo/0000-0002-8151-1990; Vercellone, Stefano/0000-0003-1163-1396;
Esposito, Paolo/0000-0003-4849-5092
FU ASI-INAF [I/009/10/0]; NASA [NAS5-00136]; PO Sardegna FSE [L.R. 7/2007]
FX We thank the Swift team duty scientists and science planners and the
remainder of the Swift XRT and BAT teams, S. Barthelmy in particular,
for their invaluable help and support. This work was supported in Italy
by contract ASI-INAF I/009/10/0, at PSU by NASA contract NAS5-00136. PE
acknowledges financial support from the Autonomous Region of Sardinia
through a research grant under the programme PO Sardegna FSE 2007-2013,
L.R. 7/2007 'Promoting scientific research and innovation technology in
Sardinia'.
NR 39
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U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2011
VL 412
IS 1
BP L30
EP L34
DI 10.1111/j.1745-3933.2010.00999.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA V41JY
UT WOS:000209543700007
ER
PT J
AU Li, HB
Blundell, R
Hedden, A
Kawamura, J
Paine, S
Tong, E
AF Li, Hua-bai
Blundell, Raymond
Hedden, Abigail
Kawamura, Jonathan
Paine, Scott
Tong, Edward
TI Evidence for dynamically important magnetic fields in molecular clouds
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE MHD; turbulence; stars: formation; ISM: clouds; ISM: kinematics and
dynamics; ISM: magnetic fields
ID TURBULENT AMBIPOLAR DIFFUSION; OH ZEEMAN OBSERVATIONS; STAR-FORMATION;
MAGNETOHYDRODYNAMIC TURBULENCE; DARK CLOUD; INTERSTELLAR TURBULENCE;
ALFVENIC TURBULENCE; IONIZED-GAS; ION SPECTRA; CORES
AB Recent observational evidence that magnetic fields are dynamically important in molecular clouds, compared to self-gravity and turbulence, is reviewed and illustrated with data from the NGC 2024 region. One piece of evidence, turbulence anisotropy, was found in the diffuse envelope of a cloud (A(v) approximate to 1; Heyer et al. 2008); our data further suggest turbulence anisotropy in the cloud (A(v) > 7) and even near the cloud core (A(v) similar to 100). The data also show that magnetic fields can channel gravitational contraction even for a region with supercritical N(H-2)/2B(los) ratio (the ratio between the observed column density and two times the line-of-sight observed field strength), a parameter which has been widely used by observers to estimate core mass-to-flux ratios. Although the mass-to-flux ratio is constant under the flux-freezing condition, we show that N(H-2)/2B(los) grows with time if gravitational contraction is anisotropic due to magnetic fields.
C1 [Li, Hua-bai] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Blundell, Raymond; Hedden, Abigail; Paine, Scott; Tong, Edward] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kawamura, Jonathan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Li, HB (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM li@mpia.de
OI Paine, Scott/0000-0003-4622-5857
FU Harvard-Smithsonian Center for Astrophysics; Smithsonian Institution;
National Aeronautics and Space Administration; Academia Sinica
FX Our deepest appreciation goes to the staff of the SAO Submillimetre
Receiver Lab: Robert Kimberk, Steven Leiker, Cosmo Papa, Patricia Riddle
and Michael Smith. We are grateful for the support of RLT observations
from Jorge May, Leo Bronfman, Claudio Barrientos, Marcos Diaz, Jose
Donoso, Daniel Luhr, Walter Max-Moerbeck, Daniel Marrone and Kevin
Rauch. We thank Zhi-Yun Li, Matthew Kunz and the referee for many
insightful comments. H-bL's research is supported by the post-doctoral
fellowships from Max-Planck-Institut fur Astronomie and from
Harvard-Smithsonian Center for Astrophysics. The RLT was supported in
part by Smithsonian Institution internal research and development funds.
Part of the RLT research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. Operation of the RLT
on Sairecabur has been carried out in collaboration with the Universidad
de Chile. The Submillimetre Array is a joint project between the
Smithsonian Astrophysical Observatory and the Academia Sinica Institute
of Astronomy and Astrophysics and is funded by the Smithsonian
Institution and the Academia Sinica.
NR 68
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U1 0
U2 0
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 MAR
PY 2011
VL 411
IS 3
BP 2067
EP 2075
DI 10.1111/j.1365-2966.2010.17839.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 723DL
UT WOS:000287486400056
ER
PT J
AU Starling, RLC
Wiersema, K
Levan, AJ
Sakamoto, T
Bersier, D
Goldoni, P
Oates, SR
Rowlinson, A
Campana, S
Sollerman, J
Tanvir, NR
Malesani, D
Fynbo, JPU
Covino, S
D'Avanzo, P
O'Brien, PT
Page, KL
Osborne, JP
Vergani, SD
Barthelmy, S
Burrows, DN
Cano, Z
Curran, PA
De Pasquale, M
D'Elia, V
Evans, PA
Flores, H
Fruchter, AS
Garnavich, P
Gehrels, N
Gorosabel, J
Hjorth, J
Holland, ST
van der Horst, AJ
Hurkett, CP
Jakobsson, P
Kamble, AP
Kouveliotou, C
Kuin, NPM
Kaper, L
Mazzali, PA
Nugent, PE
Pian, E
Stamatikos, M
Thone, CC
Woosley, SE
AF Starling, R. L. C.
Wiersema, K.
Levan, A. J.
Sakamoto, T.
Bersier, D.
Goldoni, P.
Oates, S. R.
Rowlinson, A.
Campana, S.
Sollerman, J.
Tanvir, N. R.
Malesani, D.
Fynbo, J. P. U.
Covino, S.
D'Avanzo, P.
O'Brien, P. T.
Page, K. L.
Osborne, J. P.
Vergani, S. D.
Barthelmy, S.
Burrows, D. N.
Cano, Z.
Curran, P. A.
De Pasquale, M.
D'Elia, V.
Evans, P. A.
Flores, H.
Fruchter, A. S.
Garnavich, P.
Gehrels, N.
Gorosabel, J.
Hjorth, J.
Holland, S. T.
van der Horst, A. J.
Hurkett, C. P.
Jakobsson, P.
Kamble, A. P.
Kouveliotou, C.
Kuin, N. P. M.
Kaper, L.
Mazzali, P. A.
Nugent, P. E.
Pian, E.
Stamatikos, M.
Thoene, C. C.
Woosley, S. E.
TI Discovery of the nearby long, soft GRB 100316D with an associated
supernova
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gamma-ray burst: individual: GRB 100316D; supernovae: individual: SN
2010bh
ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; 25 APRIL 1998; HOST
GALAXIES; E-P,E-I-E-ISO CORRELATION; INTERSTELLAR-MEDIUM; AFTERGLOW
EMISSION; SHOCK BREAKOUT; NEUTRON-STAR; LIGHT CURVES
AB We report the Swift discovery of the nearby long, soft gamma-ray burst GRB 100316D, and the subsequent unveiling of its low-redshift host galaxy and associated supernova. We derive the redshift of the event to be z = 0.0591 +/- 0.0001 and provide accurate astrometry for the gamma-ray burst (GRB) supernova (SN). We study the extremely unusual prompt emission with time-resolved gamma-ray to X-ray spectroscopy and find that the spectrum is best modelled with a thermal component in addition to a synchrotron emission component with a low peak energy. The X-ray light curve has a remarkably shallow decay out to at least 800 s. The host is a bright, blue galaxy with a highly disturbed morphology and we use Gemini-South, Very Large Telescope and Hubble Space Telescope observations to measure some of the basic host galaxy properties. We compare and contrast the X-ray emission and host galaxy of GRB 100316D to a subsample of GRB-SNe. GRB 100316D is unlike the majority of GRB-SNe in its X-ray evolution, but resembles rather GRB 060218, and we find that these two events have remarkably similar high energy prompt emission properties. Comparison of the host galaxies of GRB-SNe demonstrates, however, that there is a great diversity in the environments in which GRB-SNe can be found. GRB 100316D is an important addition to the currently sparse sample of spectroscopically confirmed GRB-SNe, from which a better understanding of long GRB progenitors and the GRB-SN connection can be gleaned.
C1 [Starling, R. L. C.; Wiersema, K.; Rowlinson, A.; Tanvir, N. R.; O'Brien, P. T.; Page, K. L.; Osborne, J. P.; Evans, P. A.; Hurkett, C. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Sakamoto, T.; Gehrels, N.; Holland, S. T.; Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sakamoto, T.] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Bersier, D.; Cano, Z.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Goldoni, P.] Lab Astroparticule & Cosmol, F-75205 Paris 13, France.
[Goldoni, P.] CEA Saclay, DSM IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Oates, S. R.; Curran, P. A.; De Pasquale, M.; Kuin, N. P. M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Campana, S.; Covino, S.; D'Avanzo, P.; Thoene, C. C.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Sollerman, J.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Sollerman, J.; Malesani, D.; Fynbo, J. P. U.; Hjorth, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Vergani, S. D.] Univ Paris 07, CNRS, APC, UMR7164, F-75205 Paris 13, France.
[Vergani, S. D.; Flores, H.] CNRS, Observ Paris, GEPI, UMR 8111, F-92195 Meudon, France.
[Barthelmy, S.; Fruchter, A. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[D'Elia, V.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[D'Elia, V.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Garnavich, P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Gorosabel, J.] Inst Astrofis Andalucia IAA CSIC, E-18008 Granada, Spain.
[Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[van der Horst, A. J.; Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland.
[Kamble, A. P.; Kaper, L.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Kaper, L.] Vrije Univ Amsterdam, Ctr Laser, NL-1081 HV Amsterdam, Netherlands.
[Mazzali, P. A.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Mazzali, P. A.; Pian, E.] Scuola Normale Super Pisa, I-56127 Pisa, Italy.
[Mazzali, P. A.] INAF Oss Astron Padova, I-35122 Padua, Italy.
[Nugent, P. E.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Pian, E.] Osserv Astron Trieste, I-34143 Trieste, Italy.
[Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Woosley, S. E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
RP Starling, RLC (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
EM rlcs1@star.le.ac.uk
RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Curran,
Peter/B-5293-2013; Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014;
Jakobsson, Pall/L-9950-2015;
OI Sollerman, Jesper/0000-0003-1546-6615; Curran,
Peter/0000-0003-3003-4626; Fynbo, Johan/0000-0002-8149-8298; Hjorth,
Jens/0000-0002-4571-2306; Jakobsson, Pall/0000-0002-9404-5650; Campana,
Sergio/0000-0001-6278-1576; D'Elia, Valerio/0000-0002-7320-5862; Thone,
Christina/0000-0002-7978-7648; Covino, Stefano/0000-0001-9078-5507;
Pian, Elena/0000-0001-8646-4858
FU ESO Telescopes at the La Silla or Paranal Observatories [084.D-0939,
083.A-0644, 084.A-0260]; NASA [NAS 5-26555, NAS5-00136]; STFC; British
Council and Platform Beta Techniek [PPS WS 005]; Danish National
Research Foundation
FX This work made use of data supplied by the UK Swift Science Data Centre
at the University of Leicester. This work is based on observations made
with ESO Telescopes at the La Silla or Paranal Observatories under
programme IDs 084.D-0939, 083.A-0644 and 084.A-0260(B). This work is
also based on observations made with the NASA/ESA Hubble Space
Telescope, obtained at the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-26555: these observations are associated
with programme 11709. We thank STScI staff for their efforts in
implementing the HST ToO observation, particularly Alison Vick. We
acknowledge the wider Swift team for their many contributions. RLCS, KW,
AR, JPO, KLP and PAE acknowledge financial support from STFC. Financial
support of the British Council and Platform Beta Techniek through the
Partnership Programme in Science (PPS WS 005) is gratefully acknowledged
(KW). The Dark Cosmology Centre is funded by the Danish National
Research Foundation. DNB acknowledges NASA contract NAS5-00136. AJvdH
was supported by an appointment to the NASA Postdoctoral Program at the
MSFC, administered by Oak Ridge Associated Universities through a
contract with NASA.
NR 92
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U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR
PY 2011
VL 411
IS 4
BP 2792
EP 2803
DI 10.1111/j.1365-2966.2010.17879.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 728FF
UT WOS:000287859200042
ER
PT J
AU Halliwell, GR
Shay, LK
Brewster, JK
Teague, WJ
AF Halliwell, G. R., Jr.
Shay, L. K.
Brewster, J. K.
Teague, W. J.
TI Evaluation and Sensitivity Analysis of an Ocean Model Response to
Hurricane Ivan
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID GULF-OF-MEXICO; TROPICAL CYCLONE INTENSITY; SEA-SURFACE TEMPERATURE;
WESTERN NORTH PACIFIC; MIXED-LAYER RESPONSE; VERTICAL DIFFUSIVITIES;
PREDICTION SYSTEM; CLOSURE-MODEL; PART I; HEAT
AB An ocean model response to Hurricane Ivan (2004) over the northwest Caribbean Sea and Gulf of Mexico is evaluated to guide strategies for improving performance during strong forcing events in a region with energetic ocean features with the ultimate goal of improving coupled tropical cyclone forecasts. Based on prior experience, a control experiment is performed using quasi-optimal choices of initial ocean fields, atmospheric forcing fields, air-sea flux parameterizations, vertical mixing parameterizations, and both horizontal and vertical resolutions. Alternate experiments are conducted by altering one single model attribute and comparing the results to SST analyses and moored ADCP current measurements to quantify the sensitivity to that attribute and identify where to concentrate model improvement efforts. Atmospheric forcing that does not resolve the eye and eyewall of the storm (scales > 10 km) substantially degrades the ocean response. Ordering other model attributes from greatest to least sensitivity, ocean model initialization with regard to the accuracy of upper-ocean temperature-salinity profiles along with accurate location of ocean currents and eddies is the most important factor for ensuring good ocean model performance. Ocean dynamics ranks second in this energetic ocean region because a one-dimensional ocean model fails to capture important physical processes that affect SST cooling. Wind stress drag coefficient parameterizations that yield values exceeding 2.5 X 10(-3) at high wind speeds or that remain < 2.0 x 10(-3) over all wind speeds reduce the realism of wind-driven current profiles and have a large impact on both SST cooling and the heat flux from ocean to atmosphere. Turbulent heat flux drag coefficient parameterizations substantially impact the surface heat flux while having little impact on SST cooling, which is primarily controlled by entrainment at the mixed layer base. Vertical mixing parameterizations have a moderate impact on SST cooling but a comparatively larger impact on surface heat flux. The impacts of altering the horizontal and vertical resolutions are small, with horizontal resolution of approximate to 10 km and vertical resolution of approximate to 10 m in the mixed layer being adequate. Optimal choices of all attributes for simulating the ocean response to Ivan are identified.
C1 [Halliwell, G. R., Jr.; Shay, L. K.; Brewster, J. K.] Univ Miami, MPO RSMAS, Miami, FL USA.
[Teague, W. J.] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
RP Halliwell, GR (reprint author), NOAA AOML PhOD, 4301 Rickenbacker Cswy, Miami, FL 33149 USA.
EM george.halliwell@noaa.gov
RI Halliwell, George/B-3046-2011
OI Halliwell, George/0000-0003-4216-070X
FU National Oceanic and Atmospheric Administration [NA17RJ1226]; National
Science Foundation [ATM0444525]; Office of Naval Research [0601153N]
FX This work was sponsored by the National Oceanic and Atmospheric
Administration (Grant NA17RJ1226) and the National Science Foundation
(Grant ATM0444525). The daily Reynolds blended SST maps were obtained
online
(http://www.ncdc.noaa.gov/oa/climate/research/sst/description.php). The
Office of Naval Research supported the Naval Research Laboratory's basic
research project "Slope to Shelf Energetics and Exchange Dynamics"
(SEED) under Program Element 0601153N.
NR 58
TC 27
Z9 27
U1 0
U2 16
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 MAR
PY 2011
VL 139
IS 3
BP 921
EP 945
DI 10.1175/2010MWR3104.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 744UQ
UT WOS:000289120600014
ER
PT J
AU Adeyemo, A
Hunter, G
Dutta, PK
AF Adeyemo, Adedunni
Hunter, Gary
Dutta, Prabir K.
TI Interaction of CO with hydrous ruthenium oxide and development of a
chemoresistive ambient CO sensor
SO SENSORS AND ACTUATORS B-CHEMICAL
LA English
DT Article
DE Infrared spectroscopy; Room temperature gas sensor; CO oxidation; X-ray
photoelectron spectroscopy; Metal oxide sensor; Hydrated ruthenium oxide
ID CARBON-MONOXIDE; ELECTROCHEMICAL CAPACITORS; ELECTRICAL-PROPERTIES;
DRIFT SPECTROSCOPY; CHARGE STORAGE; TAP REACTOR; THIN-FILMS; OXIDATION;
RUO2; DIOXIDE
AB Hydrated ruthenium oxide (RuO(x)(OH)(y)), the material of interest in this study was prepared by reaction of an aqueous solution of ruthenium chloride with base. This material was amorphous, made up of 20-50 nm particles and contains Ru(III) and Ru(IV), as determined by X-ray photoelectron spectroscopy. The conductivity of thick films of RuO(x)(OH)(y) decreased in the presence of CO in a background of air and this change was reversible. Infrared spectroscopy showed the formation of carbonates in the presence of CO, which disappeared upon replacement of CO with O(2). Upon heating RuO(x)(OH)(y), there was a gradual conversion to crystalline RuO(2) beyond 200 degrees C. With these heated materials, the resistance change in the presence of CO at room temperature also gradually diminished. We propose that oxidation of CO on RuO(x)(OH)(y) leads to reduction of the ruthenium and a decrease in conductivity. With the conversion to crystalline RuO(2) upon heating, the material becomes metallic and conductivity changes are diminished. The change in conductivity of RuO(x)(OH)(y) with CO provides a convenient platform for an ambient CO sensor. Such a device also does not show interference from hydrocarbons (2000 ppm), ammonia (150 ppm), CO(2) (2000 ppm), NO (15 ppm) and NO(2) (15 ppm). (C) 2010 Elsevier B.V. All rights reserved.
C1 [Adeyemo, Adedunni; Dutta, Prabir K.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA.
[Hunter, Gary] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Dutta, PK (reprint author), Ohio State Univ, Dept Chem, 100 W 18th Ave, Columbus, OH 43210 USA.
EM dutta.1@osu.edu
FU NASA
FX We acknowledge funding from NASA for this work.
NR 49
TC 20
Z9 21
U1 3
U2 28
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-4005
J9 SENSOR ACTUAT B-CHEM
JI Sens. Actuator B-Chem.
PD MAR 1
PY 2011
VL 152
IS 2
BP 307
EP 315
DI 10.1016/j.snb.2010.12.027
PG 9
WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation
SC Chemistry; Electrochemistry; Instruments & Instrumentation
GA 741QD
UT WOS:000288877700024
ER
PT J
AU Narukage, N
Sakao, T
Kano, R
Hara, H
Shimojo, M
Bando, T
Urayama, F
DeLuca, E
Golub, L
Weber, M
Grigis, P
Cirtain, J
Tsuneta, S
AF Narukage, N.
Sakao, T.
Kano, R.
Hara, H.
Shimojo, M.
Bando, T.
Urayama, F.
DeLuca, E.
Golub, L.
Weber, M.
Grigis, P.
Cirtain, J.
Tsuneta, S.
TI Coronal-Temperature-Diagnostic Capability of the Hinode/X-Ray Telescope
Based on Self-Consistent Calibration
SO SOLAR PHYSICS
LA English
DT Article
DE Corona; Instrumentation and data management
ID SOLAR-A MISSION; EXTREME-ULTRAVIOLET; ATOMIC DATABASE; EMISSION-LINES;
ELEMENTS HYDROGEN; ACTIVE REGIONS; CHIANTI; YOHKOH; XRT; PERFORMANCE
AB The X-Ray Telescope (XRT) onboard the Hinode satellite is an X-ray imager that observes the solar corona with unprecedentedly high angular resolution (consistent with its 1 '' pixel size). XRT has nine X-ray analysis filters with different temperature responses. One of the most significant scientific features of this telescope is its capability of diagnosing coronal temperatures from less than 1 MK to more than 10 MK, which has never been accomplished before. To make full use of this capability, accurate calibration of the coronal temperature response of XRT is indispensable and is presented in this article. The effect of on-orbit contamination is also taken into account in the calibration. On the basis of our calibration results, we review the coronal-temperature-diagnostic capability of XRT.
C1 [Narukage, N.; Kano, R.; Hara, H.; Bando, T.; Tsuneta, S.] Natl Astron Observ Japan NAOJ, Mitaka, Tokyo 1818588, Japan.
[Sakao, T.] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan.
[Shimojo, M.] Natl Astron Observ Japan, Nobeyama Solar Radio Observ, Minamisa Ku, Nagano 3841305, Japan.
[Urayama, F.] Space Engn Dev Co Ltd, Tsukuba, Ibaraki 3050032, Japan.
[DeLuca, E.; Golub, L.; Weber, M.; Grigis, P.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Cirtain, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Narukage, N (reprint author), Natl Astron Observ Japan NAOJ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
EM noriyuki.narukage@nao.ac.jp
RI DeLuca, Edward/L-7534-2013; Shimojo, Masumi/J-2605-2016;
OI DeLuca, Edward/0000-0001-7416-2895; Shimojo, Masumi/0000-0002-2350-3749;
Golub, Leon/0000-0001-9638-3082
FU JAXA and NAOJ (Japan); STFC (UK); NASA; ESA; NSC (Norway)
FX The authors thank the members of the XRT team for useful discussions and
comments. We acknowledge D. Brooks and H. Warren for various pieces of
information on quiet-Sun and active region DEMs. Hinode is a Japanese
mission developed and launched by ISAS/JAXA, collaborating with NAOJ as
a domestic partner, NASA and STFC (UK) as international partners.
Scientific operation of the Hinode mission is conducted by the Hinode
science team organized at ISAS/JAXA. This team mainly consists of
scientists from institutes in the partner countries. Support for the
post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK),
NASA, ESA, and NSC (Norway). CHIANTI is a collaborative project
involving the NRL (USA), the Universities of Florence (Italy) and
Cambridge (UK), and George Mason University (USA). We wish to express
our sincere gratitude to the late Takeo Kosugi, former project manager
of Hinode (Solar-B) at ISAS, who passed away in November 2006. Without
his leadership in the development of Hinode, this mission would never
have been realized. We express our sincere gratitude to those who
participated in, or supported, the XRT end-to-end calibration
measurement at MSFC XRCF that was carried out for two weeks in May June
2005. First of all, we are very much indebted loan extremely-talented
team of people at XRCF led by C. Reily and J. McCracken, including R.
Siler, E. Wright, J. Carpenter, J. Keegley and G. Zirnstein, and also M.
Baker, H. Haight, B. Hale, T. Hill, B. Hoghe, D. Javins, J. Norwood, H.
Rutledge, G. St. John, J. Tucker, and D. Watson. Without their
continuous, enormous support including preparation of the LN2-cooled
cold plate facing XRT radiators in the cryogenic chamber of XRCF, from
an early preparation phase of the XRCF experiment and throughout the
experiment's duration, the filter calibration at XRCF would have been
totally impossible. We are also grateful to people from SAO who
supported the XRCF measurement; G. Austin, W. Podgorski, E. Dennis, J.
Chappel, D. Caldwell, W. Martell, M. Harris, M. Cosmo, D. Weaver, S.
Park and T. Kent who participated in the experiment, and P. Cheimets, J.
Bookbinder, J. Boczenowski. Also A. Sabbag of Naval Research Laboratory
is appreciated for his support during a pre-shipment instrument check
performed at SAO. K. Kumagai and M. Tamura of NAOJ, K. Yaji of Rikkyo
U., and K. Kobayashi of MSFC are greatly appreciated for preparing, and
participating in, the XRCF experiment. Also, people from MSFC, L. Hill,
J. Owens, B. Cobb, D. Coleman, R. Jayroe, T. Perrin, D. Schultz, A.
Sterling and C. Talley are sincerely acknowledged for their various
supportive contributions throughout our stay in Huntsville and also for
our transportation to and from XRCF. Finally, the authors are grateful
to the referees for their detailed and careful reviews.
NR 36
TC 42
Z9 42
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD MAR
PY 2011
VL 269
IS 1
BP 169
EP 236
DI 10.1007/s11207-010-9685-2
PG 68
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 738FZ
UT WOS:000288626700012
ER
PT J
AU Devami, K
Kang, D
Lee, JS
Meyyappan, M
AF Devami, Keivan
Kang, Daegun
Lee, Jeong-Soo
Meyyappan, M.
TI Synthesis of ZnTe nanostructures by vapor-liquid-solid technique
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
ID THERMAL EVAPORATION; GROWTH; NANOWIRES; NANORODS; NANOSAWS; ROUTE
AB We have synthesized nanowires of ZnTe using a vapor-liquid-solid approach and found the morphology to be dependant upon the growth temperature. Widely varying structures ranging from cylindrical and tapered nanowires to nanoribbons are obtained depending on the substrate location, gas flow rate and pressure all of which change the temperature distribution within the reactor. The reactor is also modeled to understand the impact of temperature on growth morphology. (C) 2011 Elsevier B. V. All rights reserved.
C1 [Devami, Keivan; Kang, Daegun; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang, South Korea.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lee, JS (reprint author), Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang, South Korea.
EM ljs6951@postech.ac.kr; m.meyyappan@nasa.gov
RI Davami, Keivan/Q-5283-2016
FU Ministry of Education, Science and Technology [R31-2008-000-10100-0]
FX This work was supported by the World Class University program through
the National Research Foundation of Korea funded by the Ministry of
Education, Science and Technology under Project R31-2008-000-10100-0.
Professor Xuhui Sun is acknowledged for his help with TEM results.
NR 17
TC 11
Z9 11
U1 1
U2 16
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 FEB 28
PY 2011
VL 504
IS 1-3
BP 62
EP 66
DI 10.1016/j.cplett.2011.01.053
PG 5
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 726CF
UT WOS:000287695300013
ER
PT J
AU Lin, II
Hu, CM
Li, YH
Ho, TY
Fischer, TP
Wong, GTF
Wu, JF
Huang, CW
Chu, DA
Ko, DS
Chen, JP
AF Lin, I. -I.
Hu, Chuanmin
Li, Yuan-Hui
Ho, Tung-Yuan
Fischer, Tobias P.
Wong, George T. F.
Wu, Jingfeng
Huang, Chih-Wei
Chu, D. Allen
Ko, Dong S.
Chen, Jen-Ping
TI Fertilization potential of volcanic dust in the low-nutrient
low-chlorophyll western North Pacific subtropical gyre: Satellite
evidence and laboratory study
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
ID SOUTH CHINA SEA; ANATAHAN VOLCANO; MARIANA ISLANDS; 2003 ERUPTION;
NITROGEN-FIXATION; MARINE-PHYTOPLANKTON; PHOSPHATE-DEPLETION; COASTAL
WATERS; ATLANTIC-OCEAN; SURFACE OCEAN
AB In the western North Pacific subtropical ocean, the Anatahan volcano of the Mariana Islands erupted on 10 May 2003 for the first time in recorded history. Based on nine different types of remote sensing data provided by NASA, laboratory experiment of the Anatahan samples, and a 3-D ocean circulation model developed by the U.S. Naval Research Laboratory, the postvolcanic ocean biogeochemical response to the Anatahan eruption was explored. It was observed that soon after the eruption, the aerosol optical depth abruptly increased from the pre-eruption loading of similar to 0.1 to similar to 2. In the week following the eruption, a "bloom-like" patch was observed by NASA's Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) ocean color sensor. Based on the chlorophyll a, fluorescence line height (FLH), at-sensor total radiance, and normalized water-leaving radiance data obtained by MODIS, the cause of the bloom-like patch was diagnosed. The results suggest that the patch was most likely a mixture of suspended volcanic particles and a phytoplankton bloom. FLH was found to be similar to 9-17 x 10(-3) mW cm(-2) mu m(-1) sr(-1) in the patch and similar to 3-5 x 10-3 mW cm(-2) mu m(-1) sr(-1) in the ambient water, indicating that a 2-5-fold increase in biological activity occurred during the week following the eruption. Satellite altimetry indicated that the bloom took place in the presence of downwelling and was not a result of upwelled nutrients in this oligotrophic ocean. Analysis of satellite ocean color spectra of the bloom region found similar spectra as the reference Trichodesmium spectra. Laboratory experiments further substantiate the satellite observations which show elevated concentrations of limiting nutrients provided by the Anatahan samples, and the averaged soluble nitrate, phosphate, and Fe were 42, 3.1, and 2.0 nM, respectively. Though it was not possible to obtain in situ observations of the ocean biogeochemical responses that followed the Anatahan eruption, this study provided evidence based on remote sensing data and laboratory experiment that fertilization of volcanic aerosols occurred following this eruption in one of the most oligotrophic low-nutrient low-chlorophyll ocean deserts on Earth.
C1 [Lin, I. -I.; Huang, Chih-Wei; Chen, Jen-Ping] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 106, Taiwan.
[Hu, Chuanmin] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA.
[Li, Yuan-Hui] Univ Hawaii Manoa, Dept Oceanog, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA.
[Ho, Tung-Yuan; Wong, George T. F.; Huang, Chih-Wei] Acad Sinica, Res Ctr Environm Changes, Taipei 115, Taiwan.
[Fischer, Tobias P.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Wong, George T. F.] Natl Cent Univ, Inst Hydrol & Ocean Sci, Jhongli, Taiwan.
[Wu, Jingfeng] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Chu, D. Allen] NASA, Goddard Space Flight Ctr, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA.
[Ko, Dong S.] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
RP Lin, II (reprint author), Natl Taiwan Univ, Dept Atmospher Sci, 1,Sect 4,Roosevelt Rd, Taipei 106, Taiwan.
EM iilin@as.ntu.edu.tw
RI ChaoMing, Hu/C-3884-2011; Wu, Jingfeng/B-1301-2012; hu,
chuanmin/J-5021-2012; Lin, I-I/J-4695-2013; Chen, Jen-Ping/F-2947-2010;
Ho, Tung-Yuan/F-2323-2017
OI Lin, I-I/0000-0002-8364-8106; Chen, Jen-Ping/0000-0003-4188-6189;
FU National Science Council of Taiwan [NSC97-2111-M-002-014-MY3,
NSC-98-2611-M-002-014-MY3]; U.S. NASA; Academia Sinica, Taiwan
FX We thank the U. S. NASA, Remote Sensing Systems, and the U. S. NOAA for
providing remote sensing data. Thanks to Jennifer A. Wade (Boson
University, USA) for helpful information. This work is primarily
supported by the National Science Council of Taiwan through the
Long-term Observation and Research of the East China Sea grants
NSC97-2111-M-002-014-MY3 (Lin) and NSC-98-2611-M-002-014-MY3 (Lin) and
by the U.S. NASA Ocean Biology and Biogeochemistry program. Additional
support was through NSC 96-2611-M-001-003-MY3 (Wong) and
NSC98-2611-M-001-004-MY3 (Wong) and a thematic research grant entitled
"Atmospheric Forcing on Ocean Biogeochemistry (AFOBi)" by the Academia
Sinica, Taiwan (Wong and Lin).
NR 69
TC 29
Z9 31
U1 0
U2 18
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0886-6236
J9 GLOBAL BIOGEOCHEM CY
JI Glob. Biogeochem. Cycle
PD FEB 26
PY 2011
VL 25
AR GB1006
DI 10.1029/2009GB003758
PG 12
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA 727NP
UT WOS:000287808200001
ER
PT J
AU Welling, DT
Jordanova, VK
Zaharia, SG
Glocer, A
Toth, G
AF Welling, D. T.
Jordanova, V. K.
Zaharia, S. G.
Glocer, A.
Toth, G.
TI The effects of dynamic ionospheric outflow on the ring current
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID WEATHER MODELING FRAMEWORK; SHEET ION COMPOSITION; PLASMA SHEET;
GEOSYNCHRONOUS ORBIT; ELECTRIC-FIELD; TAIL CURRENT; POLAR WIND;
MAGNETOSPHERE; MHD; SPACE
AB The importance of ionospheric O+ on the development of the storm time ring current is recognized but not well understood. The addition of this outflow in global MHD models has the potential to change the magnetic field configuration, particle densities and temperatures, and the convection electric field. This makes including heavy ion outflow in ring current simulations difficult, as this addition cannot be easily decoupled from a host of other changes. This study attempts to overcome this problem by using three coupled models, PWOM, RIM, and BATS-R-US, to drive a ring current model, RAM-SCB. The differences in drivers when outflow is included and is not included are compared to see how outflow changes ring current input. It is found that including this outflow reduces the convection electric field, lowers the plasma sheet number density and temperature, and increases the complexity of the plasma sheet ion composition both temporally and spatially. These changes cause an overall reduction in ring current energy density. Further simulations that attempt to isolate these effects find that the most important change in terms of ring current development is the drop in convection electric field. Local time dependencies of O+ injections are found to be nontrivial as well. Capturing all of these effects requires a whole system, first-principles approach.
C1 [Welling, D. T.; Jordanova, V. K.; Zaharia, S. G.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Glocer, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Toth, G.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Welling, DT (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA.
EM dwelling@lanl.gov; vania@lanl.gov; szaharia@lanl.gov;
alex.glocer-1@nasa.gov; gtoth@umich.edu
RI Glocer, Alex/C-9512-2012; Toth, Gabor/B-7977-2013; Welling,
Daniel/C-1970-2013; feggans, john/F-5370-2012;
OI Glocer, Alex/0000-0001-9843-9094; Toth, Gabor/0000-0002-5654-9823;
Jordanova, Vania/0000-0003-0475-8743
FU U.S. Department of Energy; NASA [NNH09AL06I, NNH07AG24I]; NSF
[ATM0902941, ATM0703210]
FX The authors thank Aaron Ridley for providing the AMIE data used in this
study. Dst data was provided by the World Data Center for Geomagnetism,
Kyoto, and the four Dst observatories (Kakioka, Honolulu, San Juan, and
Hermanus). Solar wind measurements are from the ACE SWEPAM and MAG
instruments and were provided by the NASA GSFC Coordinated Data Analysis
Web. Work at Los Alamos was conducted under the auspices of the U.S.
Department of Energy, with partial support from the IGPP program and
NASA Living With A Star grants NNH09AL06I and NNH07AG24I and NSF
Geospace Environment Modeling grants ATM0902941 and ATM0703210.
NR 67
TC 23
Z9 23
U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB 26
PY 2011
VL 116
AR A00J19
DI 10.1029/2010JA015642
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 727PE
UT WOS:000287812600001
ER
PT J
AU Uchida, H
Tsunemi, H
Tominaga, N
Katsuda, S
Kimura, M
Kosugi, H
Takahashi, H
Takakura, S
AF Uchida, Hiroyuki
Tsunemi, Hiroshi
Tominaga, Nozomu
Katsuda, Satoru
Kimura, Masashi
Kosugi, Hiroko
Takahashi, Hiroaki
Takakura, Satoru
TI First Detection of Ar-K Line Emission from the Cygnus Loop
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE ISM: abundances; ISM: individual (Cygnus Loop); ISM: supernova remnants;
X-rays: ISM
ID METAL-POOR STARS; X-RAY-EMISSION; SUPERNOVA REMNANT; SOUTHWESTERN RIM;
XMM-NEWTON; NUCLEOSYNTHESIS; NORTHEASTERN
AB We observed the Cygnus Loop with XMM-Newton (9 pointings) and Suzaku (32 pointings) between 2002 and 2008. The total effective exposure time is 670.2 ks. By using all of the available data, we intended to improve a signal-to-noise ratio of the spectrum. Accordingly, the accumulated spectra obtained by the XIS and the EPIC show some line features around 3 keV that are attributed to the S He beta and Ar He alpha lines, respectively. Since the Cygnus Loop is an evolved (similar to 10000 yr) supernova remnant whose temperature is relatively low (<1 keV) compared with other young remnants, its spectrum is generally faint above 3.0 keV, no emission lines, such as the Ar-K line, have ever been detected. The detection of the Ar-K line is the first time, and we found that its abundance is significantly higher than that of the solar value: 9.0(-3.8)(+4.0) and 8.4(-2.7)(+2.5) (in units of solar), estimated from the XIS and the EPIC spectra, respectively. We conclude that the Ar-K line originated from the ejecta of the Cygnus Loop. Followup X-ray observations to tightly constrain the abundances of Ar-rich ejecta will be useful to accurately estimate the progenitor's mass.
C1 [Uchida, Hiroyuki; Tsunemi, Hiroshi; Kimura, Masashi; Kosugi, Hiroko; Takahashi, Hiroaki; Takakura, Satoru] Osaka Univ, Dept Earth & Space Sci, Grad Sch Sci, Osaka 5600043, Japan.
[Tominaga, Nozomu] Konan Univ, Dept Phys, Fac Sci & Engn, Kobe, Hyogo 6588501, Japan.
[Tominaga, Nozomu] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778569, Japan.
[Katsuda, Satoru] NASA, Code 662, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Uchida, H (reprint author), Osaka Univ, Dept Earth & Space Sci, Grad Sch Sci, Osaka 5600043, Japan.
EM uchida@ess.sci.osaka-u.ac.jp
RI XRAY, SUZAKU/A-1808-2009
FU JSPS
FX H.U. thanks Professor Jacco Vink and his students for many useful
discussions and their hospitality at Utrecht University. The authors
would like to thank H. Umeda for providing a progenitor model. H.U. and
M.K. are supported by JSPS Research Fellowship for Young Scientists.
S.K. is supported by JSPS Postdoctoral Fellow for Research Abroad.
NR 25
TC 2
Z9 2
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 FEB 25
PY 2011
VL 63
IS 1
BP 199
EP 208
DI 10.1093/pasj/63.1.199
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 733SS
UT WOS:000288283700021
ER
PT J
AU Sakamoto, T
Pal'Shin, V
Yamaoka, K
Ohno, M
Sato, G
Aptekar, R
Barthelmy, SD
Baumgartner, WH
Cummings, JR
Fenimore, EE
Frederiks, D
Gehrels, N
Golenetskii, S
Krimm, HA
Markwardt, CB
Onda, K
Palmer, DM
Parsons, AM
Stamatikos, M
Sugita, S
Tashiro, M
Tueller, J
Ukwatta, TN
AF Sakamoto, Takanori
Pal'Shin, Valentin
Yamaoka, Kazutaka
Ohno, Masarlori
Sato, Goro
Aptekar, Rafail
Barthelmy, Scott D.
Baumgartner, Wayne H.
Cummings, Jay R.
Fenimore, Edward E.
Frederiks, Dmitry
Gehrels, Neil
Golenetskii, Sergey
Krimm, Hans A.
Markwardt, Craig B.
Onda, Kaori
Palmer, David M.
Parsons, Ann M.
Stamatikos, Michael
Sugita, Satoshi
Tashiro, Makoto
Tueller, Jack
Ukwatta, Tilan N.
TI Spectral Cross-Calibration of the Konus-Wind, the Suzaku/WAM, and the
Swift/BAT Data Using Gamma-Ray Bursts
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE gamma rays: burst; gamma rays: observations; instrumentation: detectors
ID ALERT TELESCOPE; ENERGY CORRELATIONS; PEAK ENERGY; CATALOG; AFTERGLOWS;
DISCOVERY; MISSION; BAT
AB We report on the spectral cross-calibration results of the Konus-Wind, the Suzaku/WAM, and the Swift/BAT instruments using simultaneously observed gamma-ray bursts (GRBs). This is the first attempt to use simultaneously observed GRBs as a spectral calibration source to understand systematic problems among the instruments. Based on these joint spectral fits, we find that (1) although a constant factor (a normalization factor) agrees within 20% among the instruments, the BAT constant factor shows a systematically smaller value by 10%-20% compared to that of Konus-Wind, (2) there is a systematic trend that the low-energy photon index becomes steeper by 0.1-0.2 and E-peak becomes systematically higher by 10%-20% when including the BAT data in the joint fits, and (3) the high-energy photon index agrees within 0.2 among the instruments. Our results show that cross-calibration based on joint spectral analysis is an important step to understanding the instrumental effects that could be affecting the scientific results from the GRB prompt emission data.
C1 [Sakamoto, Takanori; Baumgartner, Wayne H.; Cummings, Jay R.; Krimm, Hans A.; Markwardt, Craig B.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Sakamoto, Takanori; Baumgartner, Wayne H.; Cummings, Jay R.] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Pal'Shin, Valentin; Aptekar, Rafail; Frederiks, Dmitry; Golenetskii, Sergey] Ioffe Phys Tech Inst, Expt Astrophys Lab, St Petersburg 194021, Russia.
[Yamaoka, Kazutaka] Aoyama Gakuin Univ, Dept Phys & Math, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan.
[Ohno, Masarlori; Sato, Goro] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, ISAS JAXA, Chuo Ku, Sagamihara, Kanagawa 2298510, Japan.
[Fenimore, Edward E.; Palmer, David M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Krimm, Hans A.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Markwardt, Craig B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Stamatikos, Michael] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Ukwatta, Tilan N.] George Washington Univ, Dept Phys, Ctr Nucl Studies, Washington, DC 20052 USA.
[Onda, Kaori; Tashiro, Makoto] Saitama Univ, Dept Phys, Sakura, Saitama 3388570, Japan.
[Sugita, Satoshi] Nagoya Univ, EcoTopia Sci Inst, Furo, Nagoya 4648603, Japan.
RP Sakamoto, T (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
EM Taka.Sakamoto@nasa.gov
RI Gehrels, Neil/D-2971-2012; Tueller, Jack/D-5334-2012; Barthelmy,
Scott/D-2943-2012; Parsons, Ann/I-6604-2012; Tashiro,
Makoto/J-4562-2012; Frederiks, Dmitry/C-7612-2014; Pal'shin,
Valentin/F-3973-2014; Aptekar, Raphail/B-3456-2015; Golenetskii,
Sergey/B-3818-2015; XRAY, SUZAKU/A-1808-2009;
OI Frederiks, Dmitry/0000-0002-1153-6340
FU Russian Space Agency; RFBR [09-02-00166a]; Ministry of Education,
Culture, Sports, Science and Technology (MEXT) [19047001, 21740214]
FX We would like to thank the anonymous referee for comments and
suggestions that materially improved the paper. The Konus-Wind
experiment is supported by the Russian Space Agency contract and RFBR
grant 09-02-00166a. This research has made use of data obtained from the
Suzaku satellite, a collaborative mission between the space agencies of
Japan (JAXA) and the USA (NASA). It also has been supported in part by a
Grant-in-Aid for Scientific Research (19047001 KY, 21740214 MO) of the
Ministry of Education, Culture, Sports, Science and Technology (MEXT).
NR 33
TC 12
Z9 12
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 FEB 25
PY 2011
VL 63
IS 1
BP 215
EP 277
DI 10.1093/pasj/63.1.215
PG 63
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 733SS
UT WOS:000288283700023
ER
PT J
AU Lamarque, JF
McConnell, JR
Shindell, DT
Orlando, JJ
Tyndall, GS
AF Lamarque, Jean-Francois
McConnell, J. R.
Shindell, D. T.
Orlando, J. J.
Tyndall, G. S.
TI Understanding the drivers for the 20th century change of hydrogen
peroxide in Antarctic ice-cores
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SOUTH-POLE; STRATOSPHERIC OZONE; VOLCANIC-ERUPTIONS; CHEMISTRY; SNOW;
H2O2; AIR; TEMPERATURE; RADICALS; INCREASE
AB Observations and model simulations of an Antarctic ice-core record of hydrogen peroxide during the last similar to 150 years are analyzed. The observations indicate a relative increase in hydrogen peroxide by approximately 50% since 1900, with most of the change since the early 1970s. Using two model simulations spanning 1850 to present, we show that the modeled relative change in annual-mean surface hydrogen peroxide parallels the equivalent signal from the ice core record. In addition, we show that this relative change can be explained by the relative changes in tropospheric ozone concentration and mostly in ozone photolysis rates (J((OD)-D-1)). The simulated signal is therefore intimately related to the changes in stratospheric ozone associated with increases in chlorofluorocarbons; this is further demonstrated using total ozone column observations and the associated observed change in ice-core hydrogen peroxide. Citation: Lamarque, J.-F., J. R. McConnell, D. T. Shindell, J. J. Orlando, and G. S. Tyndall (2011), Understanding the drivers for the 20th century change of hydrogen peroxide in Antarctic ice-cores, Geophys. Res. Lett., 38, L04810, doi:10.1029/2010GL045992.
C1 [Lamarque, Jean-Francois; Orlando, J. J.; Tyndall, G. S.] Natl Ctr Atmospher Res, NCAR Earth Syst Lab, Boulder, CO 80305 USA.
[McConnell, J. R.] Desert Res Inst, Reno, NV 89512 USA.
[Shindell, D. T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Lamarque, JF (reprint author), Natl Ctr Atmospher Res, NCAR Earth Syst Lab, 1850 Table Mesa Dr, Boulder, CO 80305 USA.
EM lamar@ucar.edu
RI Shindell, Drew/D-4636-2012; Lamarque, Jean-Francois/L-2313-2014
OI Lamarque, Jean-Francois/0000-0002-4225-5074
FU NSF [OPP-9904294, OPP-0538427]; National Science Foundation
FX The total ozone column data were obtained from the World Ozone and
Ultraviolet Radiation Data Centre (WOUDC) operated by Environment
Canada, Toronto, Ontario, Canada under the auspices of the World
Meteorological Organization. The authors would like to thank S.
Madronich and D. Kinnison for their constructive feedback on a previous
version of this paper. Development of the ice hydrogen peroxide records
was funded by NSF grants OPP-9904294 and OPP-0538427, and we gratefully
acknowledge the U.S. ITASE and WAIS Divide projects teams for assistance
in obtaining the ice cores. The National Center for Atmospheric Research
is operated by the University Corporation for Atmospheric Research under
sponsorship of the National Science Foundation.
NR 35
TC 11
Z9 11
U1 0
U2 10
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 FEB 25
PY 2011
VL 38
AR L04810
DI 10.1029/2010GL045992
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 727NR
UT WOS:000287808400001
ER
PT J
AU Cumnock, JA
Le, G
Imber, S
Slavin, JA
Zhang, Y
Paxton, LJ
AF Cumnock, J. A.
Le, G.
Imber, S.
Slavin, J. A.
Zhang, Y.
Paxton, L. J.
TI Space Technology 5 multipoint observations of transpolar arc-related
field-aligned currents
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; HIGH-LATITUDE AURORA; POLAR-CAP ARCS; IMF
B-Y; THETA-AURORA; PLASMA; ELECTRODYNAMICS; IONOSPHERE; ROTATION;
EXPLORER
AB We present two transpolar arc events where for the first time we are able to analyze changes in field-aligned currents associated with high-latitude transpolar auroral arcs on time scales of a few minutes. This is accomplished through the use of highly accurate multipoint magnetic field measurements provided by the Space Technology 5 mission, which consists of three microsatellites in low-Earth orbit. In the first event we examine measurements of an arc that is part of a highly dynamic auroral pattern, that of a hook-shaped arc. In the second event, a more stable dusk oval-aligned arc is analyzed. These events illustrate the dynamic nature of arc formation and show the usefulness of high-resolution multipoint measurements. Minimum variance analysis is used to determine the appropriateness of the infinite current sheet approximation and to calculate arc alignment angles which are then compared with those estimated from UV images or precipitating particle data.
C1 [Cumnock, J. A.] Univ Texas Dallas, Ctr Space Sci, Richardson, TX 75083 USA.
[Le, G.; Imber, S.; Slavin, J. A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Zhang, Y.; Paxton, L. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Cumnock, JA (reprint author), Univ Texas Dallas, Ctr Space Sci, MS WT15,POB 830688, Richardson, TX 75083 USA.
EM cumnock@utdallas.edu
RI Le, Guan/C-9524-2012; Slavin, James/H-3170-2012; Paxton,
Larry/D-1934-2015; Zhang, Yongliang/C-2180-2016
OI Le, Guan/0000-0002-9504-5214; Slavin, James/0000-0002-9206-724X; Paxton,
Larry/0000-0002-2597-347X; Zhang, Yongliang/0000-0003-4851-1662
FU NASA [NNX07AC57G]
FX We would like to thank the all the people whose commitment of time and
professional expertise have made the ST5 project a success. The authors
thank the ACE, IMP 8, and Wind instrument teams for providing
magnetometer and plasma data through the GSFC/SPDF OMNIWeb interface at
http://omniweb.gsfc.nasa.gov. We also thank the AFRL, Dave Hardy, and
Fred Rich for providing the DMSP SSJ4 particle data and the William B.
Hanson Center for Space Sciences at the University of Texas at Dallas
for providing the DMSP thermal plasma data. The work at the Johns
Hopkins University Applied Physics Laboratory was supported by NASA
grant NNX07AC57G.
NR 47
TC 5
Z9 5
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB 25
PY 2011
VL 116
AR A02218
DI 10.1029/2010JA015912
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 727PD
UT WOS:000287812500001
ER
PT J
AU Knysh, S
Smelyanskiy, VN
Durkin, GA
AF Knysh, Sergey
Smelyanskiy, Vadim N.
Durkin, Gabriel A.
TI Scaling laws for precision in quantum interferometry and the bifurcation
landscape of the optimal state
SO PHYSICAL REVIEW A
LA English
DT Article
ID LIMIT; NOISE
AB Phase precision in optimal two-channel quantum interferometry is studied in the limit of large photon number N >> 1, for losses occurring in either one or both channels. For losses in one channel an optimal state undergoes an intriguing sequence of local bifurcations as the number of photons (or losses) increase. The optimal state has a continuous form in the Fock state basis for large N. The loss parameter limits any precision improvement over classical light to at most a constant factor independent of N. We determine a crossover value of photon number N(c) beyond which supraclassical precision is progressively lost.
C1 [Knysh, Sergey; Smelyanskiy, Vadim N.; Durkin, Gabriel A.] NASA, Quantum Lab, Appl Phys Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Knysh, S (reprint author), NASA, Quantum Lab, Appl Phys Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Sergey.I.Knysh@nasa.gov; Vadim.N.Smelyanskiy@nasa.gov;
gabriel.durkin@qubit.org
FU Mission Critical Technologies, Inc.
FX G.A.D. contributed to this work while under contract with Mission
Critical Technologies, Inc.
NR 15
TC 81
Z9 82
U1 1
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD FEB 25
PY 2011
VL 83
IS 2
AR 021804
DI 10.1103/PhysRevA.83.021804
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 726MX
UT WOS:000287728100004
ER
PT J
AU Pulkkinen, A
Kuznetsova, M
Ridley, A
Raeder, J
Vapirev, A
Weimer, D
Weigel, RS
Wiltberger, M
Millward, G
Rastatter, L
Hesse, M
Singer, HJ
Chulaki, A
AF Pulkkinen, A.
Kuznetsova, M.
Ridley, A.
Raeder, J.
Vapirev, A.
Weimer, D.
Weigel, R. S.
Wiltberger, M.
Millward, G.
Rastaetter, L.
Hesse, M.
Singer, H. J.
Chulaki, A.
TI Geospace Environment Modeling 2008-2009 Challenge: Ground magnetic field
perturbations
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID IONOSPHERE-THERMOSPHERE MODEL; SPACE WEATHER; SOLAR-WIND; SYSTEMS;
SURFACE; SIMULATION; CODE; LFM
AB Acquiring quantitative metrics-based knowledge about the performance of various space physics modeling approaches is central for the space weather community. Quantification of the performance helps the users of the modeling products to better understand the capabilities of the models and to choose the approach that best suits their specific needs. Further, metrics-based analyses are important for addressing the differences between various modeling approaches and for measuring and guiding the progress in the field. In this paper, the metrics-based results of the ground magnetic field perturbation part of the Geospace Environment Modeling 2008-2009 Challenge are reported. Predictions made by 14 different models, including an ensemble model, are compared to geomagnetic observatory recordings from 12 different northern hemispheric locations. Five different metrics are used to quantify the model performances for four storm events. It is shown that the ranking of the models is strongly dependent on the type of metric used to evaluate the model performance. None of the models rank near or at the top systematically for all used metrics. Consequently, one cannot pick the absolute "winner": the choice for the best model depends on the characteristics of the signal one is interested in. Model performances vary also from event to event. This is particularly clear for root-mean-square difference and utility metric-based analyses. Further, analyses indicate that for some of the models, increasing the global magnetohydrodynamic model spatial resolution and the inclusion of the ring current dynamics improve the models' capability to generate more realistic ground magnetic field fluctuations.
C1 [Pulkkinen, A.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Pulkkinen, A.; Kuznetsova, M.; Rastaetter, L.; Hesse, M.; Chulaki, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Raeder, J.; Vapirev, A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Ridley, A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Weigel, R. S.] George Mason Univ, Dept Computat & Data Sci, Fairfax, VA 22030 USA.
[Weimer, D.] Virginia Polytech Inst & State Univ, Ctr Space Sci & Engn Res, Blacksburg, VA 24061 USA.
[Wiltberger, M.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Singer, H. J.] NOAA, Space Weather Predict Ctr, Boulder, CO USA.
RP Pulkkinen, A (reprint author), Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
EM antti.a.pulkkinen@nasa.gov
RI Ridley, Aaron/F-3943-2011; Hesse, Michael/D-2031-2012; Rastaetter,
Lutz/D-4715-2012; Kuznetsova, Maria/F-6840-2012; Wiltberger,
Michael/B-8781-2008
OI Ridley, Aaron/0000-0001-6933-8534; Rastaetter, Lutz/0000-0002-7343-4147;
Wiltberger, Michael/0000-0002-4844-3148
NR 28
TC 27
Z9 27
U1 1
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD FEB 24
PY 2011
VL 9
AR S02004
DI 10.1029/2010SW000600
PG 13
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 727PR
UT WOS:000287813900001
ER
PT J
AU Amblard, A
Cooray, A
Serra, P
Altieri, B
Arumugam, V
Aussel, H
Blain, A
Bock, J
Boselli, A
Buat, V
Castro-Rodriguez, N
Cava, A
Chanial, P
Chapin, E
Clements, DL
Conley, A
Conversi, L
Dowell, CD
Dwek, E
Eales, S
Elbaz, D
Farrah, D
Franceschini, A
Gear, W
Glenn, J
Griffin, M
Halpern, M
Hatziminaoglou, E
Ibar, E
Isaak, K
Ivison, RJ
Khostovan, AA
Lagache, G
Levenson, L
Lu, N
Madden, S
Maffei, B
Mainetti, G
Marchetti, L
Marsden, G
Mitchell-Wynne, K
Nguyen, HT
O'Halloran, B
Oliver, SJ
Omont, A
Page, MJ
Panuzzo, P
Papageorgiou, A
Pearson, CP
Perez-Fournon, I
Pohlen, M
Rangwala, N
Roseboom, IG
Rowan-Robinson, M
Portal, MS
Schulz, B
Scott, D
Seymour, N
Shupe, DL
Smith, AJ
Stevens, JA
Symeonidis, M
Trichas, M
Tugwell, K
Vaccari, M
Valiante, E
Valtchanov, I
Vieira, JD
Vigroux, L
Wang, L
Ward, R
Wright, G
Xu, CK
Zemcov, M
AF Amblard, Alexandre
Cooray, Asantha
Serra, Paolo
Altieri, B.
Arumugam, V.
Aussel, H.
Blain, A.
Bock, J.
Boselli, A.
Buat, V.
Castro-Rodriguez, N.
Cava, A.
Chanial, P.
Chapin, E.
Clements, D. L.
Conley, A.
Conversi, L.
Dowell, C. D.
Dwek, E.
Eales, S.
Elbaz, D.
Farrah, D.
Franceschini, A.
Gear, W.
Glenn, J.
Griffin, M.
Halpern, M.
Hatziminaoglou, E.
Ibar, E.
Isaak, K.
Ivison, R. J.
Khostovan, A. A.
Lagache, G.
Levenson, L.
Lu, N.
Madden, S.
Maffei, B.
Mainetti, G.
Marchetti, L.
Marsden, G.
Mitchell-Wynne, K.
Nguyen, H. T.
O'Halloran, B.
Oliver, S. J.
Omont, A.
Page, M. J.
Panuzzo, P.
Papageorgiou, A.
Pearson, C. P.
Perez-Fournon, I.
Pohlen, M.
Rangwala, N.
Roseboom, I. G.
Rowan-Robinson, M.
Sanchez Portal, M.
Schulz, B.
Scott, Douglas
Seymour, N.
Shupe, D. L.
Smith, A. J.
Stevens, J. A.
Symeonidis, M.
Trichas, M.
Tugwell, K.
Vaccari, M.
Valiante, E.
Valtchanov, I.
Vieira, J. D.
Vigroux, L.
Wang, L.
Ward, R.
Wright, G.
Xu, C. K.
Zemcov, M.
TI Submillimetre galaxies reside in dark matter haloes with masses greater
than 3 x 10(11) solar masses
SO NATURE
LA English
DT Article
ID HERSCHEL-SPIRE INSTRUMENT; STAR-FORMATION; NUMBER COUNTS; HERMES;
REDSHIFT; SPITZER; ATLAS; BIAS
AB The extragalactic background light at far-infrared wavelengths(1-3) comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year(4). These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes(5,6). Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations(7-10). A previous attempt(11) at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model(12). Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 mu m. From this excess, we find that submillimetre galaxies are located in dark matter haloes with a minimum mass, M-min, such that log(10)[M-min/M-circle dot] = 11.5(-0.2)(+0.7) at 350 mu m, where M-circle dot is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe(13), and is lower than that predicted by semi-analytical models for galaxy formation(14).
C1 [Amblard, Alexandre; Cooray, Asantha; Serra, Paolo; Khostovan, A. A.; Mitchell-Wynne, K.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Altieri, B.; Conversi, L.; Sanchez Portal, M.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain.
[Arumugam, V.; Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Aussel, H.; Elbaz, D.; Madden, S.; Panuzzo, P.] Univ Paris Diderot, CNRS, Lab AIM Paris Saclay, CEA DSM Irfu,CE Saclay, F-91191 Gif Sur Yvette, France.
[Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Boselli, A.; Buat, V.] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain.
[Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Chanial, P.; Clements, D. L.; O'Halloran, B.; Rowan-Robinson, M.; Trichas, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Chapin, E.; Halpern, M.; Marsden, G.; Scott, Douglas; Valiante, E.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Conley, A.; Glenn, J.; Rangwala, N.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA.
[Dwek, E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Eales, S.; Gear, W.; Griffin, M.; Isaak, K.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Farrah, D.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.; Ward, R.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Franceschini, A.; Mainetti, G.; Marchetti, L.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Ibar, E.; Ivison, R. J.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Lagache, G.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France.
[Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Omont, A.; Vigroux, L.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Page, M. J.; Pearson, C. P.; Seymour, N.; Symeonidis, M.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
[Tugwell, K.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada.
[Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
RP Cooray, A (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
EM acooray@uci.edu
RI Dwek, Eli/C-3995-2012; Serra, Paolo/G-9678-2014; amblard,
alexandre/L-7694-2014; Ivison, R./G-4450-2011; Vaccari,
Mattia/R-3431-2016; Cava, Antonio/C-5274-2017
OI Serra, Paolo/0000-0002-7609-3931; amblard,
alexandre/0000-0002-2212-5395; Ivison, R./0000-0001-5118-1313; Vaccari,
Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA)
FX SPIRE has been developed by a consortium of institutes led by Cardiff
University (UK) and including the University of Lethbridge (Canada);
NAOC (China); CEA and LAM (France); IFSI and the University of Padua
(Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College
London, RAL, UCL-MSSL, UKATC and the University of Sussex (UK); and
Caltech/JPL, IPAC and the University of Colorado (USA). This development
has been supported by national funding agencies: CSA (Canada); NAOC
(China); CEA, CNES and CNRS (France); ASI (Italy); MCINN (Spain); SNSB
(Sweden); STFC (UK); and NASA (USA). We thank M. Viero for comments. A.
A., A. Cooray, P. S., A. A. K., K.M.-W. and other US co-authors are
supported by NASA funds for US participants in Herschel through an award
from JPL.
NR 30
TC 72
Z9 72
U1 0
U2 6
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD FEB 24
PY 2011
VL 470
IS 7335
BP 510
EP 512
DI 10.1038/nature09771
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 725NT
UT WOS:000287652900036
PM 21326201
ER
PT J
AU Sullivan, R
Anderson, R
Biesiadecki, J
Bond, T
Stewart, H
AF Sullivan, R.
Anderson, R.
Biesiadecki, J.
Bond, T.
Stewart, H.
TI Cohesions, friction angles, and other physical properties of Martian
regolith from Mars Exploration Rover wheel trenches and wheel scuffs
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GUSEV CRATER; MERIDIANI-PLANUM; SPIRIT ROVER; EXPERIMENTAL ABRASION;
PATHFINDER ROVER; LANDING SITE; SAND GRAINS; DEPOSITS; OPPORTUNITY;
ROUNDNESS
AB The Mars Exploration Rovers Spirit and Opportunity investigated the physical properties of Martian regolith in 7 wheel trenches and 20 wheel scuffs distributed along traverses at Gusev crater and Meridiani Planum. Specialized wheel-trenching sequences allowed analysis of wheel motor and suspension telemetry to determine regolith friction angle phi and cohesion c at trench sites. Friction angles were 30 degrees - 37 degrees, and cohesions were 0-2 kPa. Simpler wheel-scuff maneuvers were analyzed for cohesion by assuming the range of phi determined from trenches; cohesions in wheel-scuffed regoliths were from 0 to 11 kPa. Regolith phi and c can be related to regolith origins. Grain sorting, compaction, shape, size, and angularity influence phi. Impact cratering and aeolian processes have affected grain angularity and sorting of Martian regolith at both Mars Exploration Rover (MER) landing sites and contend in opposing ways to determine grain characteristics in the regolith. Friction angles are consistent with dry, rigid, nonplaty grains with particle size frequencies dominated by very fine sand (as seen by the Microscopic Imager or MI) with at least some grain rounding (unresolved by MI), reflecting physical weathering from aeolian saltation. Friction angle results from MER trenches therefore indicate that regolith states are between fully mature aeolian materials and impact debris. MI and color Pancam views show trench tailings and trench floors are redder, brighter, and have more intermixed extremely fine (unresolved) grains than regolith closer to the surface disturbed and exposed only by rolling tracks.
C1 [Sullivan, R.; Bond, T.; Stewart, H.] Cornell Univ, Ithaca, NY 14853 USA.
[Anderson, R.; Biesiadecki, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sullivan, R (reprint author), Cornell Univ, 308 Space Sci, Ithaca, NY 14853 USA.
EM rjs33@cornell.edu
FU Mars Exploration Rover project; Jet Propulsion Laboratory; Cornell
University; Mars Data Analysis Program; Kennedy Space Center
FX This work was supported by the Mars Exploration Rover project through
contracts with the Jet Propulsion Laboratory and Cornell University, the
Mars Data Analysis Program, and Kennedy Space Center. Lindsey Brock
Hayes, Craig Weinstein, and Daniel Catropa assisted with laboratory
experiments with the direct shear box and MER wheel apparatus at Cornell
University. Insightful comments and suggestions from two anonymous
reviewers improved the quality of the manuscript and are greatly
appreciated. Without support from NASA for the MER extended mission,
most of the data collected and analyzed in this work and the conclusions
we report would not have been possible.
NR 71
TC 23
Z9 25
U1 2
U2 18
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 FEB 23
PY 2011
VL 116
AR E02006
DI 10.1029/2010JE003625
PG 38
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 727OM
UT WOS:000287810700001
ER
PT J
AU Moiseev, A
AF Moiseev, Alexander
CA Fermi LAT Collaboration
TI Fermi gamma-ray space telescope: Science highlights for the first 8
months
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article; Proceedings Paper
CT 2nd Roma International Conference on Astroparticle Physics
CY MAY 13-15, 2009
CL Rome, ITALY
DE Gamma-ray astronomy; Cosmic rays; Gamma-ray burst; Pulsar; Blazar;
Diffuse gamma-radiation
ID LARGE-AREA TELESCOPE; SOURCE LIST; EMISSION; PULSAR; EGRET; DISCOVERY;
MISSION
AB The Fermi Gamma-ray Space Telescope was launched on June 11, 2008 and since August 2008 has successfully been conducting routine science observations of high energy phenomena in the gamma-ray sky. A number of exciting discoveries have been made during its first year of operation, including blazar flares, high-energy gamma-ray bursts, and numerous new gamma-ray sources of different types, among them pulsars and Active Galactic Nuclei (AGN). Fermi-LAT also performed accurate measurement of the diffuse gamma-radiation which clarifies the "GeV excess" reported by EGRET almost 10 years ago, high precision measurement of the high energy electron spectrum, and other observations. An overview of the observatory status and recent results as of April 30, 2009, are presented. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Moiseev, Alexander] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
[Moiseev, Alexander] Univ Maryland, College Pk, MD 20742 USA.
RP Moiseev, A (reprint author), NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
EM alexander.a.moiseev@nasa.gov
NR 25
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD FEB 21
PY 2011
VL 630
IS 1
BP 1
EP 6
DI 10.1016/j.nima.2010.06.016
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 727EQ
UT WOS:000287780800002
ER
PT J
AU Sabatini, S
Tavani, M
Pian, E
Bulgarelli, A
Caraveo, P
Viotti, R
Corcoran, MF
Giuliani, A
Pittori, C
Verrecchia, F
Vercellone, S
Mereghetti, S
Argan, A
Barbiellini, G
Boffelli, F
Cattaneo, PW
Chen, AW
Cocco, V
D'Ammando, F
Costa, E
De Paris, G
Del Monte, E
Di Cocco, G
Donnarumma, I
Evangelista, Y
Ferrari, A
Feroci, M
Fiorini, M
Froysland, T
Fuschino, F
Galli, M
Gianotti, F
Labanti, C
Lapshov, I
Lazzarotto, F
Lipari, P
Longo, F
Marisaldi, M
Mastropietro, M
Morelli, E
Moretti, E
Morselli, A
Pacciani, L
Pellizzoni, A
Perotti, F
Piano, G
Picozza, P
Pilia, M
Porrovecchio, G
Pucella, G
Prest, M
Rapisarda, M
Rappoldi, A
Rubini, A
Soffitta, P
Trifoglio, M
Trois, A
Vallazza, E
Vittorini, V
Zambra, A
Zanello, D
Santolamazza, P
Giommi, P
Colafrancesco, S
Antonelli, LA
Salotti, L
AF Sabatini, S.
Tavani, M.
Pian, E.
Bulgarelli, A.
Caraveo, P.
Viotti, R.
Corcoran, M. F.
Giuliani, A.
Pittori, C.
Verrecchia, F.
Vercellone, S.
Mereghetti, S.
Argan, A.
Barbiellini, G.
Boffelli, F.
Cattaneo, P. W.
Chen, A. W.
Cocco, V.
D'Ammando, F.
Costa, E.
De Paris, G.
Del Monte, E.
Di Cocco, G.
Donnarumma, I.
Evangelista, Y.
Ferrari, A.
Feroci, M.
Fiorini, M.
Froysland, T.
Fuschino, F.
Galli, M.
Gianotti, F.
Labanti, C.
Lapshov, I.
Lazzarotto, F.
Lipari, P.
Longo, F.
Marisaldi, M.
Mastropietro, M.
Morelli, E.
Moretti, E.
Morselli, A.
Pacciani, L.
Pellizzoni, A.
Perotti, F.
Piano, G.
Picozza, P.
Pilia, M.
Porrovecchio, G.
Pucella, G.
Prest, M.
Rapisarda, M.
Rappoldi, A.
Rubini, A.
Soffitta, P.
Trifoglio, M.
Trois, A.
Vallazza, E.
Vittorini, V.
Zambra, A.
Zanello, D.
Santolamazza, P.
Giommi, P.
Colafrancesco, S.
Antonelli, L. A.
Salotti, L.
TI Galactic sources science with AGILE: The case of the Carina Region
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article; Proceedings Paper
CT 2nd Roma International Conference on Astro-particle Physics
CY MAY 13-15, 2009
CL Rome, ITALY
DE Gamma rays: observations; Individual stars (Eta Carinae); Stars: winds;
Outflows; X-rays: bynaries
ID XMM-NEWTON OBSERVATIONS; ETA-CARINAE; COLLIDING WINDS; RAY-EMISSION;
LIGHT-CURVE; BEPPOSAX; BINARIES; MISSION; EVENTS; SPACE
AB During its first 2 years of operation, the gamma-ray AGILE satellite accumulated an extensive dataset for the Galactic plane. The data have been monitored for transient sources and several gamma-ray sources were detected. Their variability and possible association were studied. In this talk we will focus on the results of extensive observations of the Carina Region during the time period 2007 July-2009 January, for a total livetime of similar to 130 days. The region is extremely complex, hosting massive star formation, with the remarkable colliding wind binary Eta Carinae, massive star clusters and HII regions (e.g. NGC 3324, RCW49, Westerlund II) and a giant molecular cloud extending over 150 pc (between I=284.7 and 289). The Carina Nebula itself is the largest and IR highest surface brightness nebula of the Southern emisphere. We monitored several gamma ray sources in the Carina Region. In particular we detect a gamma ray source (1AGLJ1043-5931) consistent with the position of Eta Carinae and report a remarkable 2-days gamma-ray flaring episode from this source on 2008 October 11-13. If 1AGL J1043-5931 is associated with the Eta Car system, our data provide the long sought first detection above 100 MeV of a colliding wind binary. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Sabatini, S.; Tavani, M.; Viotti, R.; Argan, A.; Cocco, V.; D'Ammando, F.; Costa, E.; De Paris, G.; Del Monte, E.; Donnarumma, I.; Evangelista, Y.; Feroci, M.; Lapshov, I.; Lazzarotto, F.; Pacciani, L.; Piano, G.; Porrovecchio, G.; Pucella, G.; Rubini, A.; Soffitta, P.; Trois, A.; Vittorini, V.] INAF IASF Roma, I-00133 Rome, Italy.
[Sabatini, S.; Tavani, M.; D'Ammando, F.; Froysland, T.; Piano, G.; Picozza, P.; Vittorini, V.] Univ Roma Tor Vergata, Dip Fis, I-00133 Rome, Italy.
[Caraveo, P.; Giuliani, A.; Mereghetti, S.; Chen, A. W.; Fiorini, M.; Perotti, F.; Zambra, A.] INAF IASF Milano, I-20133 Milan, Italy.
[Chen, A. W.; Ferrari, A.; Froysland, T.] CIFS Torino, I-10133 Turin, Italy.
[Bulgarelli, A.; Di Cocco, G.; Fuschino, F.; Gianotti, F.; Labanti, C.; Marisaldi, M.; Morelli, E.; Trifoglio, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Barbiellini, G.; Longo, F.; Moretti, E.; Vallazza, E.] Dip Fis, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.; Moretti, E.; Vallazza, E.] INFN Trieste, I-34127 Trieste, Italy.
[Boffelli, F.; Cattaneo, P. W.; Rappoldi, A.] INFN Pavia, I-27100 Pavia, Italy.
[Galli, M.] ENEA Bologna, I-40129 Bologna, Italy.
[Lipari, P.; Zanello, D.] INFN Roma La Sapienza, I-00185 Rome, Italy.
[Mastropietro, M.] CNR IMIP, Rome, Italy.
[Morselli, A.; Piano, G.; Picozza, P.] INFN Roma Tor Vergata, I-00133 Rome, Italy.
[Lazzarotto, F.; Prest, M.; Colafrancesco, S.] Univ Insubria, Dip Fis, I-22100 Como, Italy.
[Rapisarda, M.] ENEA Frascati, I-00044 Rome, Italy.
[Pittori, C.; Verrecchia, F.; Santolamazza, P.; Giommi, P.; Colafrancesco, S.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Salotti, L.] Agenzia Spaziale Italiana, I-00198 Rome, Italy.
[Pian, E.] Osserv Astron Trieste, I-34131 Trieste, Italy.
[Corcoran, M. F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Corcoran, M. F.] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA.
[Ferrari, A.] Univ Turin, Dip Fis, Turin, Italy.
[Antonelli, L. A.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Pellizzoni, A.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, Italy.
[Pilia, M.] Univ Insubria, Dipartimento Fis, I-22100 Como, Italy.
[Vercellone, S.] INAF IASF Palermo, I-90146 Palermo, Italy.
RP Sabatini, S (reprint author), INAF IASF Roma, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
EM sabina.sabatini@iasf-roma.inaf.it
RI Morselli, Aldo/G-6769-2011; Lazzarotto, Francesco/J-4670-2012;
Trifoglio, Massimo/F-5302-2015; Pittori, Carlotta/C-7710-2016;
OI Del Monte, Ettore/0000-0002-3013-6334; trois,
alessio/0000-0002-3180-6002; Marisaldi, Martino/0000-0002-4000-3789;
Labanti, Claudio/0000-0002-5086-3619; Feroci, Marco/0000-0002-7617-3421;
Soffitta, Paolo/0000-0002-7781-4104; Picozza,
Piergiorgio/0000-0002-7986-3321; Fuschino, Fabio/0000-0003-2139-3299;
Caraveo, Patrizia/0000-0003-2478-8018; PREST,
MICHELA/0000-0003-3161-4454; Verrecchia, Francesco/0000-0003-3455-5082;
Gianotti, Fulvio/0000-0003-4666-119X; Lazzarotto,
Francesco/0000-0003-4871-4072; Costa, Enrico/0000-0003-4925-8523;
Donnarumma, Immacolata/0000-0002-4700-4549; Sabatini,
Sabina/0000-0003-2076-5767; Vercellone, Stefano/0000-0003-1163-1396;
MEREGHETTI, SANDRO/0000-0003-3259-7801; Tavani,
Marco/0000-0003-2893-1459; Pian, Elena/0000-0001-8646-4858; Morselli,
Aldo/0000-0002-7704-9553; Trifoglio, Massimo/0000-0002-2505-3630;
Pittori, Carlotta/0000-0001-6661-9779; Pellizzoni, Alberto
Paolo/0000-0002-4590-0040; Bulgarelli, Andrea/0000-0001-6347-0649;
galli, marcello/0000-0002-9135-3228; Pacciani,
Luigi/0000-0001-6897-5996; Fiorini, Mauro/0000-0001-8297-1983; giommi,
paolo/0000-0002-2265-5003
NR 22
TC 0
Z9 0
U1 0
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD FEB 21
PY 2011
VL 630
IS 1
BP 193
EP 197
DI 10.1016/j.nima.2010.06.062
PG 5
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 727EQ
UT WOS:000287780800044
ER
PT J
AU Grasso, D
Profumo, S
Strong, AW
Baldini, L
Bellazzini, R
Bloom, ED
Bregeon, J
Di Bernardo, G
Gaggero, D
Giglietto, N
Kamae, T
Latronico, L
Longo, F
Mazziotta, MN
Moiseev, AA
Morselli, A
Ormes, JF
Pesce-Rollins, M
Pohl, M
Razzano, M
Sgro, C
Spandre, G
Stephens, TE
AF Grasso, D.
Profumo, S.
Strong, A. W.
Baldini, L.
Bellazzini, R.
Bloom, E. D.
Bregeon, J.
Di Bernardo, G.
Gaggero, D.
Giglietto, N.
Kamae, T.
Latronico, L.
Longo, F.
Mazziotta, M. N.
Moiseev, A. A.
Morselli, A.
Ormes, J. F.
Pesce-Rollins, M.
Pohl, M.
Razzano, M.
Sgro, C.
Spandre, G.
Stephens, T. E.
TI Possible interpretations of the high energy cosmic ray electron spectrum
measured with the Fermi space telescope
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article; Proceedings Paper
CT 2nd Roma International Conference on Astro-particle Physics
CY MAY 13-15, 2009
CL Rome, ITALY
DE Fermi-LAT; Cosmic rays electrons; Pulsars; Dark matter
ID SUPERNOVA-REMNANTS; GAMMA-RAYS; POSITRONS; PULSARS
AB The Fermi Large Area Telescope (LAT) recently measured the cosmic ray electrons-plus-positrons (CRE) spectrum between 20 GeV and 1 TeV. In this contribution we discuss several interpretations of those measurements in combination with other experimental data. We show that, as far as concerns the reported Fermi-LAT data alone, a simple interpretation invoking a single class of astrophysical electron sources is possible. If, however, also the CRE spectrum measured by H.E.S.S. and especially the positron fraction reported by PAMELA are accounted, that scenario fails to provide a combined description of those results. Rather, we show that several combinations of parameters, involving e pair emission by pulsars or dark matter annihilation, allow a consistent interpretation of all data sets. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Grasso, D.; Baldini, L.; Bellazzini, R.; Bregeon, J.; Di Bernardo, G.; Gaggero, D.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Profumo, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Profumo, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bloom, E. D.; Kamae, T.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Bloom, E. D.; Kamae, T.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Di Bernardo, G.; Gaggero, D.] Univ Pisa, Dipartimento Fis, I-56127 Pisa, Italy.
[Giglietto, N.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Giglietto, N.] Politecn Bari, I-70126 Bari, Italy.
[Giglietto, N.; Mazziotta, M. N.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Moiseev, A. A.] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Moiseev, A. A.] Univ Maryland, College Pk, MD 20742 USA.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Pohl, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Stephens, T. E.] NASA, Univ Space Res Assoc, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Grasso, D (reprint author), Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
EM dario.grasso@pi.infn.it; profumo@scipp.ucsc.edu; aws@mpe.mpg.de
RI Baldini, Luca/E-5396-2012; Morselli, Aldo/G-6769-2011; Grasso,
Dario/I-2440-2012; giglietto, nicola/I-8951-2012; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016;
OI Pesce-Rollins, Melissa/0000-0003-1790-8018; Morselli,
Aldo/0000-0002-7704-9553; Grasso, Dario/0000-0001-7761-7242; giglietto,
nicola/0000-0002-9021-2888; Mazziotta, Mario /0000-0001-9325-4672;
Baldini, Luca/0000-0002-9785-7726; Stephens, Thomas/0000-0003-3065-6871;
Sgro', Carmelo/0000-0001-5676-6214
NR 28
TC 3
Z9 3
U1 0
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD FEB 21
PY 2011
VL 630
IS 1
BP 48
EP 51
DI 10.1016/j.nima.2010.06.024
PG 4
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 727EQ
UT WOS:000287780800010
ER
PT J
AU Noutsos, A
Abdo, AA
Ackermann, M
Ajello, M
Ballet, J
Barbiellini, G
Baring, MG
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Bonamente, E
Borgland, AW
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Buehler, R
Busetto, G
Caliandro, GA
Cameron, RA
Camilo, F
Caraveo, PA
Casandjian, JM
Cecchi, C
Celik, O
Chaty, S
Chekhtman, A
Chiang, J
Ciprini, S
Claus, R
Cognard, I
Cohen-Tanugi, J
Colafrancesco, S
Cutini, S
Dermer, CD
de Palma, F
Drell, PS
Dumora, D
Ea, CM
Favuzzi, C
Ferrara, EC
Focke, WB
Frailis, M
Freire, PCC
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Godfrey, G
Grandi, P
Grenier, IA
Grove, JE
Guillemot, L
Guiriec, S
Harding, AK
Hughes, RE
Jackson, MS
Johannesson, G
Johnson, AS
Johnson, TJ
Johnson, WN
Johnston, S
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kramer, M
Kuss, M
Lande, J
Lee, SH
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Lyne, AG
Makeev, A
Marelli, M
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Naumann-Godo, M
Nolan, PL
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Panetta, JH
Parent, D
Pelassa, V
Pepe, M
Persic, M
Pesce-Rollins, M
Piron, F
Porter, TA
Raino, S
Ray, PS
Razzano, M
Reimer, A
Reimer, O
Reposeur, T
Romani, RW
Sadrozinski, HFW
Sander, A
Parkinson, PMS
Sgro, C
Siskind, EJ
Smith, DA
Smith, PD
Spandre, G
Spinelli, P
Stappers, BW
Strickman, MS
Suson, DJ
Takahashi, H
Tanaka, T
Theureau, G
Thompson, DJ
Thorsett, SE
Tibolla, O
Torres, DF
Tramacere, A
Usher, TL
Vandenbroucke, J
Vianello, G
Vilchez, N
Villata, M
Vitale, V
von Kienlin, A
Waite, AP
Wang, P
Watters, K
Weltevrede, P
Winer, BL
Wood, KS
Ziegler, M
AF Noutsos, A.
Abdo, A. A.
Ackermann, M.
Ajello, M.
Ballet, J.
Barbiellini, G.
Baring, M. G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Bonamente, E.
Borgland, A. W.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Buehler, R.
Busetto, G.
Caliandro, G. A.
Cameron, R. A.
Camilo, F.
Caraveo, P. A.
Casandjian, J. M.
Cecchi, C.
Celik, Oe
Chaty, S.
Chekhtman, A.
Chiang, J.
Ciprini, S.
Claus, R.
Cognard, I.
Cohen-Tanugi, J.
Colafrancesco, S.
Cutini, S.
Dermer, C. D.
de Palma, F.
Drell, P. S.
Dumora, D.
Ea, C. M.
Favuzzi, C.
Ferrara, E. C.
Focke, W. B.
Frailis, M.
Freire, P. C. C.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Godfrey, G.
Grandi, P.
Grenier, I. A.
Grove, J. E.
Guillemot, L.
Guiriec, S.
Harding, A. K.
Hughes, R. E.
Jackson, M. S.
Johannesson, G.
Johnson, A. S.
Johnson, T. J.
Johnson, W. N.
Johnston, S.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kramer, M.
Kuss, M.
Lande, J.
Lee, S-H.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Lyne, A. G.
Makeev, A.
Marelli, M.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Naumann-Godo, M.
Nolan, P. L.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ormes, J. F.
Panetta, J. H.
Parent, D.
Pelassa, V.
Pepe, M.
Persic, M.
Pesce-Rollins, M.
Piron, F.
Porter, T. A.
Raino, S.
Ray, P. S.
Razzano, M.
Reimer, A.
Reimer, O.
Reposeur, T.
Romani, R. W.
Sadrozinski, H. F-W
Sander, A.
Parkinson, P. M. Saz
Sgro, C.
Siskind, E. J.
Smith, D. A.
Smith, P. D.
Spandre, G.
Spinelli, P.
Stappers, B. W.
Strickman, M. S.
Suson, D. J.
Takahashi, H.
Tanaka, T.
Theureau, G.
Thompson, D. J.
Thorsett, S. E.
Tibolla, O.
Torres, D. F.
Tramacere, A.
Usher, T. L.
Vandenbroucke, J.
Vianello, G.
Vilchez, N.
Villata, M.
Vitale, V.
von Kienlin, A.
Waite, A. P.
Wang, P.
Watters, K.
Weltevrede, P.
Winer, B. L.
Wood, K. S.
Ziegler, M.
TI RADIO AND gamma-RAY CONSTRAINTS ON THE EMISSION GEOMETRY AND BIRTHPLACE
OF PSR J2043+2740
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: stars; pulsars: individual (PSR J2043+2740)
ID LARGE-AREA TELESCOPE; FERMI-LAT OBSERVATIONS; CYGNUS LOOP; SUPERNOVA
REMNANT; SPACE-TELESCOPE; VELOCITY VECTORS; PROPER-MOTION; LIGHT CURVES;
VELA PULSAR; POLARIZATION
AB We report on the first year of Fermi gamma-ray observations of pulsed high-energy emission from the old PSR J2043 + 2740. The study of the gamma-ray efficiency of such old pulsars gives us an insight into the evolution of pulsars' ability to emit in gamma rays as they age. The gamma-ray light curve of this pulsar above 0.1 GeV is clearly defined by two sharp peaks, 0.353 +/- 0.035 periods apart. We have combined the gamma-ray profile characteristics of PSR J2043 + 2740 with the geometrical properties of the pulsar's radio emission, derived from radio-polarization data, and constrained the pulsar-beam geometry in the framework of a two-pole caustic (TPC) and an outer gap (OG) model. The ranges of magnetic inclination and viewing angle were determined to be {alpha, zeta} similar to {52 degrees-57 degrees, 61 degrees-68 degrees} for the TPC model, and {alpha, zeta} similar to {62 degrees-73 degrees, 74 degrees-81 degrees} and {alpha, zeta} similar to {72 degrees-83 degrees, 60 degrees-75 degrees} for the OG model. Based on this geometry, we assess possible birth locations for this pulsar and derive a likely proper motion, sufficiently high to be measurable with VLBI. At a characteristic age of 1.2 Myr, PSR J2043 + 2740 is the third oldest of all discovered, non-recycled, gamma-ray pulsars: it is twice as old as the next oldest, PSR J0357 + 32, and younger only than the recently discovered PSR J1836 + 5925 and PSR J2055 + 25, both of which are at least five and ten times less energetic, respectively.
C1 [Noutsos, A.; Freire, P. C. C.; Guillemot, L.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Noutsos, A.; Ea, C. M.; Kramer, M.; Lyne, A. G.; Stappers, B. W.; Weltevrede, P.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Ray, P. S.; Strickman, M. S.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Abdo, A. A.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Drell, P. S.; Focke, W. B.; Funk, S.; Godfrey, G.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S-H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Smith, P. D.; Tanaka, T.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.; Watters, K.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Drell, P. S.; Focke, W. B.; Funk, S.; Godfrey, G.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S-H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Smith, P. D.; Tanaka, T.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.; Watters, K.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Ballet, J.; Casandjian, J. M.; Chaty, S.; Grenier, I. A.; Naumann-Godo, M.] Univ Paris Diderot, CEA Saclay, Lab AIM,Serv Astrophys, CEA IRFU CNRS, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.; Persic, M.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Bastieri, D.; Busetto, G.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Busetto, G.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France.
[Caliandro, G. A.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Caraveo, P. A.; Marelli, M.] INAF Ist Astrofis Spaziale & Fis, I-20133 Milan, Italy.
[Celik, Oe; Ferrara, E. C.; Harding, A. K.; Johnson, T. J.; McEnery, J. E.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, Oe] CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, Oe] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Cognard, I.; Theureau, G.] CNRS, LPCE, UMR 6115, F-45071 Orleans 02, France.
[Cognard, I.; Theureau, G.] Observ Paris, Stn Radioastron Nancay, CNRS, INSU, F-18330 Nancay, France.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, Montpellier, France.
[Colafrancesco, S.; Cutini, S.] ASI, Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[Dumora, D.; Reposeur, T.; Smith, D. A.] Univ Bordeaux 1, CNRS, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, F-33175 Gradignan, France.
[Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy.
[Frailis, M.; Persic, M.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy.
[Fukazawa, Y.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Hughes, R. E.; Sander, A.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Jackson, M. S.] AlbaNova, Dept Phys, Royal Inst Technol KTH, SE-10691 Stockholm, Sweden.
[Jackson, M. S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Johnson, T. J.; McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Johnson, T. J.; McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Johnston, S.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.; Vilchez, N.] CNRS, Ctr Etud Spatiale Rayonnements, UPS, F-31028 Toulouse 4, France.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Okumura, A.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Orlando, E.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Sadrozinski, H. F-W; Parkinson, P. M. Saz; Thorsett, S. E.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Sadrozinski, H. F-W; Parkinson, P. M. Saz; Thorsett, S. E.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tramacere, A.; Vianello, G.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Villata, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Villata, M (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM anoutsos@mpifr-bonn.mpg.de; guillemo@mpifr-bonn.mpg.de
RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; McEnery,
Julie/D-6612-2012; lubrano, pasquale/F-7269-2012; Morselli,
Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto,
nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Johnson, Neil/G-3309-2014;
Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco,
Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Moskalenko,
Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro,
Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016;
OI Thompson, David/0000-0001-5217-9135; lubrano,
pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553;
giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385;
Funk, Stefan/0000-0002-2012-0080; Johannesson,
Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673;
Gargano, Fabio/0000-0002-5055-6395; Moskalenko,
Igor/0000-0001-6141-458X; Persic, Massimo/0000-0003-1853-4900;
Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Grandi, Paola/0000-0003-1848-6013; Giordano,
Francesco/0000-0002-8651-2394; Thorsett, Stephen/0000-0002-2025-9613;
Frailis, Marco/0000-0002-7400-2135; Villata,
Massimo/0000-0003-1743-6946; Caraveo, Patrizia/0000-0003-2478-8018;
Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864
FU Science and Technology Facilities Council of the United Kingdom
FX The Lovell Telescope is owned and operated by the University of
Manchester as part of the Jodrell Bank Centre for Astrophysics with
support from the Science and Technology Facilities Council of the United
Kingdom.
NR 66
TC 6
Z9 6
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2011
VL 728
IS 2
AR 77
DI 10.1088/0004-637X/728/2/77
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716MP
UT WOS:000286973600004
ER
PT J
AU Salama, F
Galazutdinov, GA
Krelowski, J
Biennier, L
Beletsky, Y
Song, IO
AF Salama, F.
Galazutdinov, G. A.
Krelowski, J.
Biennier, L.
Beletsky, Y.
Song, In-Ok
TI POLYCYCLIC AROMATIC HYDROCARBONS AND THE DIFFUSE INTERSTELLAR BANDS: A
SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: abundances; ISM: lines and bands; ISM: molecules;
molecular data; surveys
ID ANOMALOUS MICROWAVE EMISSION; RING-DOWN SPECTROSCOPY; NAPHTHALENE
CATION; INFRARED-EMISSION; HELIUM DROPLETS; GAS-PHASE; MOLECULES;
PROFILES; REGION; JET
AB We discuss the proposal of relating the origin of some of the diffuse interstellar absorption bands (DIBs) to neutral polycyclic aromatic hydrocarbons (PAHs) present in translucent interstellar clouds. An assessment of ionized PAHs will be examined in a future report. The spectra of several cold, isolated gas-phase PAHs have been measured in the laboratory under experimental conditions that mimic the interstellar conditions and are compared with an extensive set of astronomical spectra of reddened, early-type stars. This comparison provides-for the first time-accurate upper limits for the abundances of specific PAH molecules along specific lines of sight, something not attainable from IR observations alone. The comparison of these unique laboratory data with high-resolution, high signal-to-noise ratio spectra leads to two major findings: (1) a finding specific to the individual molecules that were probed in this study and, which leads to the clear and unambiguous conclusion that the abundance of these specific neutral PAHs must be very low in the individual translucent interstellar clouds that were probed in this survey (PAH features remain below the level of detection) and, (2) a general finding that neutral PAHs exhibit intrinsic band profiles that are similar to the profile of the narrow DIBs indicating that the carriers of the narrow DIBs must have close molecular structure and characteristics. This study is the first quantitative survey of neutral PAHs in the optical range and it opens the way for unambiguous quantitative searches of PAHs in a variety of interstellar and circumstellar environments.
C1 [Salama, F.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Galazutdinov, G. A.] Univ Catolica Norte, Inst Astron, Antofagasta 0610, Chile.
[Krelowski, J.] Nicholas Copernicus Univ, Ctr Astron, PL-87100 Torun, Poland.
[Biennier, L.] Univ Rennes 1, Inst Phys Rennes, CNRS, UMR 6251, F-35042 Rennes, France.
[Beletsky, Y.] European So Observ, Santiago 3107, Chile.
[Song, In-Ok] Korea Adv Inst Sci & Technol KAIST, Korea Sci Acad KSA, Pusan, South Korea.
RP Salama, F (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Mail Stop 245-6, Moffett Field, CA 94035 USA.
EM farid.salama@nasa.gov; runizag@gmail.com; jacek@astri.uni.torun.pl;
ludovic.biennier@univ-rennes1.fr; ybialets@eso.org;
song.inok@kaist.ac.kr
RI Salama, Farid/A-8787-2009; Biennier, Ludovic/O-1618-2014
OI Salama, Farid/0000-0002-6064-4401;
FU NASA Space Mission Directorate; [N203 012 32/1550]
FX F.S. acknowledges the support of the NASA Space Mission Directorate
(APRA Program). J.K. acknowledges the financial support of the Polish
State during the period 2007-2010 (grant N203 012 32/1550). We are
deeply grateful to the ESO archive as well as to the ESO staff members
who assisted us while conducting our own observing runs. We also
acknowledge the outstanding technical support provided by R. Walker at
NASA ARC that made the laboratory measurements possible. Finally, we
acknowledge the constructive and useful comments from the reviewer, G.
Walker.
NR 51
TC 52
Z9 53
U1 3
U2 19
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 FEB 20
PY 2011
VL 728
IS 2
AR 154
DI 10.1088/0004-637X/728/2/154
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716MP
UT WOS:000286973600080
ER
PT J
AU Selwa, M
Solanki, SK
Ofman, L
AF Selwa, M.
Solanki, S. K.
Ofman, L.
TI THE ROLE OF ACTIVE REGION LOOP GEOMETRY. II. SYMMETRY BREAKING IN
THREE-DIMENSIONAL ACTIVE REGION: WHY ARE VERTICAL KINK OSCILLATIONS
OBSERVED SO RARELY?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); Sun: corona; Sun: oscillations
ID CURVED CORONAL LOOPS; FAST MAGNETOHYDRODYNAMIC OSCILLATIONS; FAST
MAGNETOACOUSTIC WAVES; TRANSVERSE OSCILLATIONS; NUMERICAL SIMULATIONS;
MAGNETIC-FIELD; MODE OSCILLATIONS; SOLAR CORONA; TRACE; HOT
AB We present numerical results of simulations of kink oscillations of coronal loops in an idealized active region (AR) that is initialized as a potential dipole magnetic configuration with gravitationally stratified density. We consider loops, with density higher than the surrounding plasma, embedded into the dipolar AR. We study the excitation of kink oscillations of such loops by velocity pulses at different positions, of a given duration and amplitude. The position of the pulse varies in the parametric studies. For a central (symmetric) loop within the AR, we find that the amplitude of vertical kink oscillations is significantly amplified in comparison to horizontal kink oscillations for exciters located centrally (symmetrically) below the loop. For pulses initiated further from such a symmetric loop a combination of vertical and horizontal oscillations is excited. The scenario changes significantly when we study an inclined loop (non-symmetric within a dipole field). In this case, we do not see vertical kink oscillations of any significant amplitude being excited, while horizontal ones can be easily detected. These results indicate that the reason why vertical kink oscillations are observed so rarely is that their excitation requires a set of conditions to occur simultaneously: the exciting pulse must be located roughly below the loop apex and the loop itself must be located symmetrically within the group of loops. The new findings of the present study show the importance of not only the position of the pulse, but mainly of the location of the loop within the set of field lines having the same magnetic connectivity. We find that the slow propagating wave is excited in all the studied loops and its excitation does not depend either on the geometry of the loop or the pulse. We discuss TRACE observations of coronal loop oscillations in view of our findings and find that our results can be used for identifying the polarization of the kink mode based on the location of the loop within the set of field lines of the same connectivity and the position of the flare.
C1 [Selwa, M.; Ofman, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Selwa, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Solanki, S. K.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Solanki, S. K.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi, South Korea.
RP Selwa, M (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
EM mselwa@mcs.st-and.ac.uk; solanki@mps.mpg.de; leon.ofman@nasa.gov
RI Solanki, Sami/E-2487-2013
OI Solanki, Sami/0000-0002-3418-8449
FU NASA [NNG06GI55G, NNX09AG10G]; Korean Ministry of Education, Science and
Technology [R31-10016]
FX M.S.'s and L.O.'s work was financially supported by the NASA SEC Theory
program and NASA grants NNG06GI55G and NNX09AG10G. S.K.S.'s work has
been partially supported by the WCU grant No. R31-10016 funded by the
Korean Ministry of Education, Science and Technology. The
three-dimensional MHD computations were performed at NASA's Advanced
Supercomputing (NAS) center.
NR 43
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2011
VL 728
IS 2
AR 87
DI 10.1088/0004-637X/728/2/87
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716MP
UT WOS:000286973600014
ER
PT J
AU Stephens, IW
Looney, LW
Dowell, CD
Vaillancourt, JE
Tassis, K
AF Stephens, Ian W.
Looney, Leslie W.
Dowell, C. Darren
Vaillancourt, John E.
Tassis, Konstantinos
TI THE GALACTIC MAGNETIC FIELD'S EFFECT IN STAR-FORMING REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: magnetic fields; polarization; stars: formation;
submillimeter: ISM
ID H-II REGIONS; GIANT MOLECULAR CLOUDS; MILKY-WAY; DISTANCE; EMISSION;
POLARIZATION; SCALE; ASSOCIATIONS; INSTABILITY; POLARIMETRY
AB We investigate the effect of the Milky Way's magnetic field in star-forming regions using archived 350 mu m polarization data on 52 Galactic star formation regions from the Hertz polarimeter module. The polarization angles and percentages for individual telescope beams were combined in order to produce a large-scale average for each source and for complexes of sources. In more than 80% of the sources, we find a meaningful mean magnetic field direction, implying the existence of an ordered magnetic field component at the scale of these sources. The average polarization angles were analyzed with respect to the Galactic coordinates in order to test for correlations between polarization percentage, polarization angle, intensity, and Galactic location. No correlation was found, which suggests that the magnetic field in dense molecular clouds is decoupled from the large-scale Galactic magnetic field. Finally, we show that the magnetic field directions in the complexes are consistent with a random distribution on the sky.
C1 [Stephens, Ian W.; Looney, Leslie W.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Dowell, C. Darren; Tassis, Konstantinos] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Vaillancourt, John E.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
RP Stephens, IW (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
EM stephen6@illinois.edu
RI Tassis, Konstantinos/C-3155-2011;
OI Tassis, Konstantinos/0000-0002-8831-2038
FU National Aeronautics and Space Administration; National Science
Foundation [AST-07-09206]
FX Part of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. This research has made use of the
SIMBAD database, operated at CDS, Strasbourg, France. L. W. L.
acknowledges support from the National Science Foundation under grant
no. AST-07-09206. We also acknowledge Richard M. Crutcher for extensive
discussions.
NR 52
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2011
VL 728
IS 2
AR 99
DI 10.1088/0004-637X/728/2/99
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716MP
UT WOS:000286973600025
ER
PT J
AU Tan, LC
Reames, DV
Ng, CK
Shao, X
Wang, LH
AF Tan, Lun C.
Reames, Donald V.
Ng, Chee K.
Shao, Xi
Wang, Linghua
TI WHAT CAUSES SCATTER-FREE TRANSPORT OF NON-RELATIVISTIC SOLAR ELECTRONS?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; magnetohydrodynamics (MHD); Sun: coronal mass
ejections (CMEs); Sun: heliosphere; Sun: particle emission
ID ENERGETIC PARTICLE EVENTS; COSMIC-RAY TRANSPORT; QUASI-LINEAR THEORY;
MAGNETIC-FIELD; INTERPLANETARY TRANSPORT; DISSIPATION RANGE; ALFVEN
WAVES; WIND SPACECRAFT; NEAR-EARTH; TURBULENCE
AB We have examined the cause of the scatter-free transport of non-relativistic solar electrons. Electron scatter-free transport events are compared with the diffusive transport event. The emphasis of our examination is on the energy dependence of electron angular distributions and the steepening of interplanetary magnetic field (IMF) power spectral densities (PSDs). Near and above the proton gyrofrequency, the effects of both R-mode (whistler) and L-mode (electromagnetic ion cyclotron, EMIC) waves need to be taken into account separately. The PSD spectral steepening due to the EMIC wave damping by solar-wind thermal ions becomes essential. In a fast-rise-fast-decay impulsive electron event we have observed such steepening, which significantly reduces PSD levels at frequencies above the proton gyrofrequency. The spectral steepening thus produced favors the occurrence of scatter-free transport of low-energy electrons. Consequently, within the Wind/3D Plasma and Energetic Particle Instrument/Silicon Semiconductor Telescope measured energy range (similar to 25-500 keV), there appears to be an electron energy window, across which the scatter-free transport of lower energy electrons would change to the diffusive transport of higher energy electrons. We have observed such a change and found it is correlated with the occurrence of broken power-law spectra of electrons. Thus the connection between the transition from diffusive to scatter-free electron transport and the concurrent transition from high to low IMF PSD levels with corresponding breaks in the electron power-law energy spectrum and PSD spectrum has been recognized.
C1 [Tan, Lun C.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
[Reames, Donald V.] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA.
[Ng, Chee K.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Tan, Lun C.; Shao, Xi] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Wang, Linghua] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Ng, Chee K.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
RP Tan, LC (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Code 672, Greenbelt, MD 20771 USA.
EM ltan@mail.umd.edu
RI Wang, Linghua/C-4938-2014; Shao, Xi/H-9452-2016
OI Wang, Linghua/0000-0001-7309-4325;
FU NASA [NNX10AE90G, NNX08AQ02G, NNX09AU98G, NNX07AF42G, NNX08AE34G]
FX We gratefully acknowledge data provided by the NASA/Space Physics Data
Facility (SPDF) CDAWeb, ACE Science Center, and Wind/3DP Data Center. We
thank A. Szabo for making the Wind/MFI high-resolution data available to
this work. Also, we thank K. Ogilvie, R. Lin, and A. Szabo for their
support of this work, and the anonymous reviewer for his/her valuable
comments. L.C.T. is supported in part by NASA grant NNX10AE90G, D.V.R.
is supported in part by NASA grant NNX08AQ02G. C.K.N. is supported in
part by NASA grant NNX09AU98G. X.S. is supported in part by NASA grant
NNX07AF42G. L.W. is supported in part by NASA grant NNX08AE34G.
NR 58
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U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2011
VL 728
IS 2
AR 133
DI 10.1088/0004-637X/728/2/133
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716MP
UT WOS:000286973600059
ER
PT J
AU Tedder, SA
Wheeler, JL
Danehy, PM
AF Tedder, Sarah A.
Wheeler, Jeffrey L.
Danehy, Paul M.
TI Characteristics of a broadband dye laser using Pyrromethene and
Rhodamine dyes
SO APPLIED OPTICS
LA English
DT Article
ID CARS TEMPERATURE-MEASUREMENTS; DUAL-PUMP CARS; ENERGY-TRANSFER; LASING
PROPERTIES; PHOTOSTABILITY; COMBUSTION; ABSORPTION; SPECTROSCOPY;
ENHANCEMENT; THERMOMETRY
AB A broadband dye laser pumped by a frequency-doubled Nd:YAG laser with a full width at half-maximum from 592 to 610 nm was created for the use in a dual-pump broadband coherent anti-Stokes Raman spectroscopy (CARS) system called width increased dual-pump enhanced CARS (WIDECARS). The desired broadband dye laser was generated with a mixture of Pyrromethene dyes as an oscillator gain medium and a spectral selective optic in the oscillator cavity. A mixture of Rhodamine dyes was used in the amplifier dye cell. To create this laser, a study was performed to characterize the spectral behavior of broadband dye lasers created with Rhodamine dyes 590, 610, and 640 and Pyrromethene dyes 597 and 650, as well as mixtures of these dyes. (C) 2011 Optical Society of America
C1 [Tedder, Sarah A.; Danehy, Paul M.] NASA Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA.
[Tedder, Sarah A.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Wheeler, Jeffrey L.] Whitworth Univ, Spokane, WA 99251 USA.
RP Tedder, SA (reprint author), NASA Langley Res Ctr, Adv Sensing & Opt Measurement Branch, 18 Langley Blvd, Hampton, VA 23681 USA.
EM sarah.a.tedder@nasa.gov
FU NASA
FX The authors thank Stephen Jones for his support in the laboratory. This
work was funded by NASA's Fundamental Aeronautics Program, Hypersonics
Project, Experimental Capabilities and Propulsion Disciplines.
NR 49
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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 FEB 20
PY 2011
VL 50
IS 6
BP 901
EP 914
DI 10.1364/AO.50.000901
PG 14
WC Optics
SC Optics
GA 724KI
UT WOS:000287574600015
PM 21343970
ER
PT J
AU Glikman, E
Djorgovski, SG
Stern, D
Dey, A
Jannuzi, BT
Lee, KS
AF Glikman, Eilat
Djorgovski, S. G.
Stern, Daniel
Dey, Arjun
Jannuzi, Buell T.
Lee, Kyoung-Soo
TI THE FAINT END OF THE QUASAR LUMINOSITY FUNCTION AT z similar to 4:
IMPLICATIONS FOR IONIZATION OF THE INTERGALACTIC MEDIUM AND COSMIC
DOWNSIZING
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; galaxies: luminosity function; mass function;
large; scale structure of universe; quasars: general; surveys
ID DIGITAL-SKY-SURVEY; LYMAN-BREAK GALAXIES; ORIGINS DEEP SURVEY;
HIGH-REDSHIFT; EVOLUTION; CATALOG; FIELD; REIONIZATION; SWIRE; STARS
AB We present an updated determination of the z similar to 4 QSO luminosity function (QLF), improving the quality of the determination of the faint end of the QLF presented by Glikman et al. (2010). We have observed an additional 43 candidates from our survey sample, yielding one additional QSO at z = 4.23 and increasing the completeness of our spectroscopic follow-up to 48% for candidates brighter than R = 24 over our survey area of 3.76 deg(2). We study the effect of using K-corrections to compute the rest-frame absolute magnitude at 1450 angstrom compared with measuring M-1450 directly from the object spectra. We find a luminosity-dependent bias: template-based K-corrections overestimate the luminosity of low-luminosity QSOs, likely due to their reliance on templates derived from higher luminosity QSOs. Combining our sample with bright quasars from the Sloan Digital Sky Survey and using spectrum-based M1450 for all the quasars, we fit a double power law to the binned QLF. Our best fit has a bright-end slope, alpha = 3.3 +/- 0.2, and faint-end slope, beta = 1.6-0(-0.6)(+0.8). Our new data revise the faint-end slope of the QLF down to flatter values similar to those measured at z similar to 3. The break luminosity, though poorly constrained, is at M-* = -24.1(-1.9)(+0.7), approximately 1-1.5 mag fainter than at z similar to 3. This QLF implies that QSOs account for about half the radiation needed to ionize the intergalactic medium at these redshifts.
C1 [Glikman, Eilat; Lee, Kyoung-Soo] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Glikman, Eilat; Lee, Kyoung-Soo] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Djorgovski, S. G.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dey, Arjun; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Glikman, E (reprint author), Yale Univ, Dept Phys, POB 208121, New Haven, CT 06520 USA.
EM eilat.glikman@yale.edu
FU W. M. Keck Foundation; NSF [AST-0407448, AST-0909182]; Ajax foundation;
NOAO
FX 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.; We
thank Gordon Richards for useful discussions on combining the SDSS and
our QLFs, and Meg Urry for helpful comments. We are grateful to the
staff of W. M. Keck observatory for their assistance during our
observing runs. This work was supported in part by the NSF grants
AST-0407448 and AST-0909182, and by the Ajax foundation. The work of
D.S. was carried out at Jet Propulsion Laboratory, California Institute
of Technology, under a contract with NASA. The research activities of
A.D. and B.T.J. are supported by the NSF through its funding of the
NOAO, which is operated by the Association of Universities for Research
in Astronomy, Inc. under a cooperative agreement with the NSF. This work
makes use of image data from the NDWFS and the DLS as distributed by the
NOAO Science Archive. K.S.L. gratefully acknowledges the generous
support of Gilbert and Jaylee Mead for their namesake fellowship.
NR 31
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 20
PY 2011
VL 728
IS 2
AR L26
DI 10.1088/2041-8205/728/2/L26
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 715YI
UT WOS:000286931200002
ER
PT J
AU Katz, I
Mikellides, IG
AF Katz, Ira
Mikellides, Ioannis G.
TI Neutral gas free molecular flow algorithm including ionization and walls
for use in plasma simulations
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE Plasma simulation; Partially ionized gases
AB Several plasma devices, including Hall and ion thrusters, operate by ionizing a low density neutral gas for which the mean free path between collisions of gas molecules is greater than typical device dimensions. In general, the discrete-particle algorithms used to calculate the neutral gas ignore velocity changes due to collisions between gas molecules. However, particle algorithms are a source of unphysical statistical noise that may detract from the study of the plasma physics, the prime purpose of most simulations. In this paper we present a new neutral gas algorithm for use in plasma simulation codes that exploits the fact that very few collisions change the velocity of neutral gas molecules. The algorithm assumes that the particle velocity distribution function for neutrals emitted from a given surface remains unchanged except for a scale factor that reflects the loss of neutrals to ionization. The sources of neutrals may be gas inlets, and isotropic, thermally accommodated, gas molecules coming off chamber surfaces including recombined ions. The algorithm is implemented in two dimensions (R-Z) with emitting surfaces represented as surfaces of revolution. The advantage of this algorithm over the conventional particle approach is the absence of statistical noise. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Katz, Ira; Mikellides, Ioannis G.] CALTECH, Jet Prop Lab, Elect Prop Grp, Pasadena, CA 91109 USA.
RP Katz, I (reprint author), CALTECH, Jet Prop Lab, Elect Prop Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ira.katz@jpl.nasa.gov; ioannis.g.mikellides@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The authors thank Dr. Richard R. Hofer for providing the HPHall runs.
The research described in this paper was carried out by the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 9
TC 9
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U1 1
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0021-9991
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD FEB 20
PY 2011
VL 230
IS 4
BP 1454
EP 1464
DI 10.1016/j.jcp.2010.11.013
PG 11
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA 714BQ
UT WOS:000286782300035
ER
PT J
AU Borucki, WJ
Koch, DG
Basri, G
Batalha, N
Boss, A
Brown, TM
Caldwell, D
Christensen-Dalsgaard, J
Cochran, WD
DeVore, E
Dunham, EW
Dupree, AK
Gautier, TN
Geary, JC
Gilliland, R
Gould, A
Howell, SB
Jenkins, JM
Kjeldsen, H
Latham, DW
Lissauer, JJ
Marcy, GW
Monet, DG
Sasselov, D
Tarter, J
Charbonneau, D
Doyle, L
Ford, EB
Fortney, J
Holman, MJ
Seager, S
Steffen, JH
Welsh, WF
Allen, C
Bryson, ST
Buchhave, L
Chandrasekaran, H
Christiansen, JL
Ciardi, D
Clarke, BD
Dotson, JL
Endl, M
Fischer, D
Fressin, F
Haas, M
Horch, E
Howard, A
Isaacson, H
Kolodziejczak, J
Li, J
MacQueen, P
Meibom, S
Prsa, A
Quintana, EV
Rowe, J
Sherry, W
Tenenbaum, P
Torres, G
Twicken, JD
Van Cleve, J
Walkowicz, L
Wu, H
AF Borucki, William J.
Koch, David G.
Basri, Gibor
Batalha, Natalie
Boss, Alan
Brown, Timothy M.
Caldwell, Douglas
Christensen-Dalsgaard, Jorgen
Cochran, William D.
DeVore, Edna
Dunham, Edward W.
Dupree, Andrea K.
Gautier, Thomas N., III
Geary, John C.
Gilliland, Ronald
Gould, Alan
Howell, Steve B.
Jenkins, Jon M.
Kjeldsen, Hans
Latham, David W.
Lissauer, Jack J.
Marcy, Geoffrey W.
Monet, David G.
Sasselov, Dimitar
Tarter, Jill
Charbonneau, David
Doyle, Laurance
Ford, Eric B.
Fortney, Jonathan
Holman, Matthew J.
Seager, Sara
Steffen, Jason H.
Welsh, William F.
Allen, Christopher
Bryson, Stephen T.
Buchhave, Lars
Chandrasekaran, Hema
Christiansen, Jessie L.
Ciardi, David
Clarke, Bruce D.
Dotson, Jessie L.
Endl, Michael
Fischer, Debra
Fressin, Francois
Haas, Michael
Horch, Elliott
Howard, Andrew
Isaacson, Howard
Kolodziejczak, Jeffery
Li, Jie
MacQueen, Phillip
Meibom, Soren
Prsa, Andrej
Quintana, Elisa V.
Rowe, Jason
Sherry, William
Tenenbaum, Peter
Torres, Guillermo
Twicken, Joseph D.
Van Cleve, Jeffrey
Walkowicz, Lucianne
Wu, Hayley
TI CHARACTERISTICS OF KEPLER PLANETARY CANDIDATES BASED ON THE FIRST DATA
SET
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: detection; surveys
ID TRANSITING PLANET; INITIAL CHARACTERISTICS; TERRESTRIAL PLANETS; CADENCE
DATA; PERFORMANCE; SCIENCE; STAR
AB In the spring of 2009, the Kepler Mission commenced high-precision photometry on nearly 156,000 stars to determine the frequency and characteristics of small exoplanets, conduct a guest observer program, and obtain asteroseismic data on a wide variety of stars. On 2010 June 15, the Kepler Mission released most of the data from the first quarter of observations. At the time of this data release, 705 stars from this first data set have exoplanet candidates with sizes from as small as that of Earth to larger than that of Jupiter. Here we give the identity and characteristics of 305 released stars with planetary candidates. Data for the remaining 400 stars with planetary candidates will be released in 2011 February. More than half the candidates on the released list have radii less than half that of Jupiter. Five candidates are present in and near the habitable zone; two near super-Earth size, and three bracketing the size of Jupiter. The released stars also include five possible multi-planet systems. One of these has two Neptune-size (2.3 and 2.5 Earth radius) candidates with near-resonant periods.
C1 [Borucki, William J.; Koch, David G.; Lissauer, Jack J.; Bryson, Stephen T.; Dotson, Jessie L.; Haas, Michael; Rowe, Jason] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Basri, Gibor; Marcy, Geoffrey W.; Howard, Andrew; Isaacson, Howard; Walkowicz, Lucianne] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Batalha, Natalie] San Jose State Univ, San Jose, CA 95192 USA.
[Boss, Alan] Carnegie Inst Washington, Washington, DC 20015 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Caldwell, Douglas; DeVore, Edna; Jenkins, Jon M.; Tarter, Jill; Doyle, Laurance; Chandrasekaran, Hema; Christiansen, Jessie L.; Clarke, Bruce D.; Li, Jie; Quintana, Elisa V.; Tenenbaum, Peter; Twicken, Joseph D.; Van Cleve, Jeffrey; Wu, Hayley] SETI Inst, Mountain View, CA 94043 USA.
[Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Aarhus, Denmark.
[Cochran, William D.; Endl, Michael; MacQueen, Phillip] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Dupree, Andrea K.; Geary, John C.; Latham, David W.; Sasselov, Dimitar; Charbonneau, David; Holman, Matthew J.; Buchhave, Lars; Fressin, Francois; Meibom, Soren; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilliland, Ronald] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA.
[Howell, Steve B.; Sherry, William] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Monet, David G.] USN Observ, Flagstaff, AZ 86001 USA.
[Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA.
[Fortney, Jonathan] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Seager, Sara] MIT, Cambridge, MA 02139 USA.
[Steffen, Jason H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA.
[Allen, Christopher] Orbital Sci Corp, Mountain View, CA 94043 USA.
[Ciardi, David] Exoplanet Sci Inst Caltech, Pasadena, CA 91125 USA.
[Fischer, Debra] Yale Univ, New Haven, CT 06520 USA.
[Horch, Elliott] So Connecticut State Univ, New Haven, CT 06515 USA.
[Kolodziejczak, Jeffery] MSFC, Huntsville, AL 35805 USA.
[Prsa, Andrej] Villanova Univ, Villanova, PA 19085 USA.
RP Borucki, WJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM William.J.Borucki@nasa.gov
RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015;
OI Caldwell, Douglas/0000-0003-1963-9616; Howard,
Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354;
Buchhave, Lars A./0000-0003-1605-5666; Ciardi,
David/0000-0002-5741-3047; /0000-0001-6545-639X; Fischer,
Debra/0000-0003-2221-0861
FU NASA's Science Mission Directorate; W. M. Keck Foundation
FX Kepler was competitively selected as the 10th Discovery mission. Funding
for this mission is provided by NASA's Science Mission Directorate. 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. The authors thank the many people who gave so generously of
their time to make this mission a success.
NR 30
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2011
VL 728
IS 2
AR 117
DI 10.1088/0004-637X/728/2/117
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716MP
UT WOS:000286973600043
ER
PT J
AU Gogus, E
Guver, T
Ozel, F
Eichler, D
Kouveliotou, C
AF Gogus, Ersin
Guever, Tolga
Oezel, Feryal
Eichler, David
Kouveliotou, Chryssa
TI LONG-TERM RADIATIVE BEHAVIOR OF SGR 1900+14
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (SGR 1900+14); X-rays: bursts
ID X-RAY PULSAR; SOFT GAMMA REPEATER; MAGNETIZED NEUTRON-STARS; DISCOVERY;
SGR-1900+14; EMISSION; MAGNETARS; OUTBURST; BEPPOSAX
AB The prolific magnetar SGR 1900+14 showed two outbursts in the last decade and has been closely monitored in the X-rays to track the changes in its radiative properties. We use archival Chandra and XMM-Newton observations of SGR 1900+14 to construct a history of its spectrum and persistent X-ray flux spanning a period of about seven years. We show that the decline of its X-ray flux in these two outburst episodes follows the same trend. The flux begins to decline promptly and rapidly subsequent to the flares, then decreases gradually for about 600 days, at which point it resumes a more rapid decline. Utilizing the high-quality spectral data in each epoch, we also study the spectral coevolution of the source with its flux. We find that neither the magnetic field strength nor the magnetospheric properties change over the period spanned by the observations, while the surface temperature as well as the inferred emitting area both decline with time following both outbursts. We also show that the source reached the same minimum flux level in its decline from these two subsequent outbursts, suggesting that this flux level may be its steady quiescent flux.
C1 [Gogus, Ersin] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
[Guever, Tolga; Oezel, Feryal] Univ Arizona, Dept Astron & Steward Observ, Tucson, AZ 85721 USA.
[Eichler, David] Ben Gurion Univ Negev, Dept Phys, IL-84105 Beer Sheva, Israel.
[Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
RP Gogus, E (reprint author), Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
EM ersing@sabanciuniv.edu
RI Guver, Tolga/C-1408-2011; Guver, Tolga/B-1039-2014
OI Guver, Tolga/0000-0002-3531-9842
FU EU [MTKD-CT-2006-042722]; Israel Science Foundation; U. S. Israel
Binational Science Foundation; Joan and Robert Arnow Chair of
Theoretical Astrophysics
FX E.G., T.G., and F.O. acknowledge EU FP6 Transfer of Knowledge Project
Astrophysics of Neutron Stars (MTKD-CT-2006-042722). D.E. acknowledges
support from the Israel Science Foundation, the U. S. Israel Binational
Science Foundation, and the Joan and Robert Arnow Chair of Theoretical
Astrophysics.
NR 33
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2011
VL 728
IS 2
AR 160
DI 10.1088/0004-637X/728/2/160
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716MP
UT WOS:000286973600086
ER
PT J
AU Janson, M
Carson, J
Thalmann, C
McElwain, MW
Goto, M
Crepp, J
Wisniewski, J
Abe, L
Brandner, W
Burrows, A
Egner, S
Feldt, M
Grady, CA
Golota, T
Guyon, O
Hashimoto, J
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Kandori, R
Knapp, GR
Kudo, T
Kusakabe, N
Kuzuhara, M
Matsuo, T
Mayama, S
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suto, H
Suzuki, R
Takami, M
Takato, N
Terada, H
Tofflemire, B
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Janson, M.
Carson, J.
Thalmann, C.
McElwain, M. W.
Goto, M.
Crepp, J.
Wisniewski, J.
Abe, L.
Brandner, W.
Burrows, A.
Egner, S.
Feldt, M.
Grady, C. A.
Golota, T.
Guyon, O.
Hashimoto, J.
Hayano, Y.
Hayashi, M.
Hayashi, S.
Henning, T.
Hodapp, K. W.
Ishii, M.
Iye, M.
Kandori, R.
Knapp, G. R.
Kudo, T.
Kusakabe, N.
Kuzuhara, M.
Matsuo, T.
Mayama, S.
Miyama, S.
Morino, J-I.
Moro-Martin, A.
Nishimura, T.
Pyo, T-S
Serabyn, E.
Suto, H.
Suzuki, R.
Takami, M.
Takato, N.
Terada, H.
Tofflemire, B.
Tomono, D.
Turner, E. L.
Watanabe, M.
Yamada, T.
Takami, H.
Usuda, T.
Tamura, M.
TI NEAR-INFRARED MULTI-BAND PHOTOMETRY OF THE SUBSTELLAR COMPANION GJ 758 B
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; planetary systems; techniques: high angular resolution
ID ADAPTIVE-OPTICS SYSTEM; HR 8799; BROWN DWARFS; COOL STARS; PLANETS;
SPECTROSCOPY; ATMOSPHERES; CATALOG; MODELS; SPOCS
AB GJ 758 B is a cold (similar to 600 K) companion to a Sun-like star at 29 AU projected separation, which was recently detected with high-contrast imaging. Here, we present photometry of the companion in seven photometric bands from Subaru/HiCIAO, Gemini/NIRI, and Keck/NIRC2, providing a rich sampling of the spectral energy distribution in the 1-5 mu m wavelength range. A clear detection at 1.58 mu m combined with an upper limit at 1.69 mu m shows methane absorption in the atmosphere of the companion. The mass of the companion remains uncertain, but an updated age estimate indicates that the most likely mass range is similar to 30-40 M-jup. In addition, we present an updated astrometric analysis that imposes tighter constraints on GJ 758 B's orbit and identifies the proposed second candidate companion, "GJ 758 C," as a background star.
C1 [Janson, M.] Univ Toronto, Toronto, ON M5R 2W9, Canada.
[Carson, J.] Coll Charleston, Charleston, SC 29424 USA.
[Thalmann, C.; Goto, M.; Brandner, W.; Feldt, M.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[McElwain, M. W.; Burrows, A.; Knapp, G. R.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Crepp, J.] CALTECH, Pasadena, CA 91125 USA.
[Wisniewski, J.; Tofflemire, B.] Univ Washington, Seattle, WA 98195 USA.
[Abe, L.] Univ Nica Sophia Antipolis, Lab Hippolyte Fizeau, F-06108 Nice 2, France.
[Egner, S.; Golota, T.; Guyon, O.; Hayano, Y.; Hayashi, M.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T-S; Takato, N.; Terada, H.; Tomono, D.; Takami, H.; Usuda, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Grady, C. A.] Eureka Sci & Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hashimoto, J.; Iye, M.; Kandori, R.; Kudo, T.; Kusakabe, N.; Kuzuhara, M.; Miyama, S.; Morino, J-I.; Suto, H.; Suzuki, R.; Tamura, M.] Natl Astron Observ Japan, Tokyo, Japan.
[Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Kuzuhara, M.] Univ Tokyo, Tokyo 1130033, Japan.
[Matsuo, T.; Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mayama, S.] Grad Univ Adv Studies, Hayama, Kanagawa 2400193, Japan.
[Moro-Martin, A.] CAB CSIC INTA, Dept Astrophys, Madrid, Spain.
[Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Turner, E. L.] Univ Tokyo, Inst Phys & Math Universe, Tokyo, Japan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosciences, Sapporo, Hokkaido, Japan.
[Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 980, Japan.
RP Janson, M (reprint author), Univ Toronto, 50 St George St, Toronto, ON M5R 2W9, Canada.
EM janson@astro.utoronto.ca
RI Turner, Edwin/A-4295-2011; McElwain, Michael/D-3607-2012; MIYAMA,
Shoken/A-3598-2015
OI McElwain, Michael/0000-0003-0241-8956;
FU W.M. Keck foundation; NSF [AST 1009203, AST 0802230, AST 1009314]; AAS
Chretien; Mitsubishi Foundation; JPL; Caltech under NASA
FX We thank David Lafreniere for providing us with the source code for
LOCI, Eric Mamajek for useful discussion, the staff at Subaru, Gemini,
and Keck for their support, and an anonymous referee for useful
suggestions. The Gemini time was allocated by NOAO. The Keck telescope
was funded by the W.M. Keck foundation and time was allocated by NASA
through partnership with Caltech and UC. We acknowledge the cultural
significance that the summit of Mauna Kea has to the indigenous Hawaiian
community. Part of the research was supported by NSF grants AST 1009203,
AST 0802230, AST 1009314, the AAS Chretien grant, a Grant-in-Aid for
Specially Promoted Research, the Mitsubishi Foundation, and JPL, Caltech
under NASA contract.
NR 29
TC 31
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2011
VL 728
IS 2
AR 85
DI 10.1088/0004-637X/728/2/85
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716MP
UT WOS:000286973600012
ER
PT J
AU Miyake, N
Sumi, T
Dong, S
Street, R
Mancini, L
Gould, A
Bennett, DP
Tsapras, Y
Yee, JC
Albrow, MD
Bond, IA
Fouque, P
Browne, P
Han, C
Snodgrass, C
Finet, F
Furusawa, K
Harpsoe, K
Allen, W
Hundertmark, M
Freeman, M
Suzuki, D
Abe, F
Botzler, CS
Douchin, D
Fukui, A
Hayashi, F
Hearnshaw, JB
Hosaka, S
Itow, Y
Kamiya, K
Kilmartin, PM
Korpela, A
Lin, W
Ling, CH
Makita, S
Masuda, K
Matsubara, Y
Muraki, Y
Nagayama, T
Nishimoto, K
Ohnishi, K
Perrott, YC
Rattenbury, N
Saito, T
Skuljan, L
Sullivan, DJ
Sweatman, WL
Tristram, PJ
Wada, K
Yock, PCM
Bolt, G
Bos, M
Christie, GW
Depoy, DL
Drummond, J
Gal-Yam, A
Gaudi, BS
Gorbikov, E
Higgins, D
Hwang, KH
Janczak, J
Kaspi, S
Lee, CU
Koo, JR
Kozlowski, S
Lee, Y
Mallia, F
Maury, A
Maoz, D
McCormick, J
Monard, LAG
Moorhouse, D
Munoz, JA
Natusch, T
Ofek, EO
Pogge, RW
Polishook, D
Santallo, R
Shporer, A
Spector, O
Thornley, G
Allan, A
Bramich, DM
Horne, K
Kains, N
Steele, I
Bozza, V
Burgdorf, MJ
Novati, SC
Dominik, M
Dreizler, S
Glitrup, M
Hessman, FV
Hinse, TC
Jorgensen, UG
Liebig, C
Maier, G
Mathiasen, M
Rahvar, S
Ricci, D
Scarpetta, G
Skottfelt, J
Southworth, J
Surdej, J
Wambsganss, J
Zimmer, F
Batista, V
Beaulieu, JP
Brillant, S
Cassan, A
Cole, A
Corrales, E
Coutures, C
Dieters, S
Greenhill, J
Kubas, D
Menzies, J
AF Miyake, N.
Sumi, T.
Dong, Subo
Street, R.
Mancini, L.
Gould, A.
Bennett, D. P.
Tsapras, Y.
Yee, J. C.
Albrow, M. D.
Bond, I. A.
Fouque, P.
Browne, P.
Han, C.
Snodgrass, C.
Finet, F.
Furusawa, K.
Harpsoe, K.
Allen, W.
Hundertmark, M.
Freeman, M.
Suzuki, D.
Abe, F.
Botzler, C. S.
Douchin, D.
Fukui, A.
Hayashi, F.
Hearnshaw, J. B.
Hosaka, S.
Itow, Y.
Kamiya, K.
Kilmartin, P. M.
Korpela, A.
Lin, W.
Ling, C. H.
Makita, S.
Masuda, K.
Matsubara, Y.
Muraki, Y.
Nagayama, T.
Nishimoto, K.
Ohnishi, K.
Perrott, Y. C.
Rattenbury, N.
Saito, To.
Skuljan, L.
Sullivan, D. J.
Sweatman, W. L.
Tristram, P. J.
Wada, K.
Yock, P. C. M.
Bolt, G.
Bos, M.
Christie, G. W.
DePoy, D. L.
Drummond, J.
Gal-Yam, A.
Gaudi, B. S.
Gorbikov, E.
Higgins, D.
Hwang, K. -H.
Janczak, J.
Kaspi, S.
Lee, C. -U.
Koo, J. -R.
Kozlowski, S.
Lee, Y.
Mallia, F.
Maury, A.
Maoz, D.
McCormick, J.
Monard, L. A. G.
Moorhouse, D.
Munoz, J. A.
Natusch, T.
Ofek, E. O.
Pogge, R. W.
Polishook, D.
Santallo, R.
Shporer, A.
Spector, O.
Thornley, G.
Allan, A.
Bramich, D. M.
Horne, K.
Kains, N.
Steele, I.
Bozza, V.
Burgdorf, M. J.
Novati, S. Calchi
Dominik, M.
Dreizler, S.
Glitrup, M.
Hessman, F. V.
Hinse, T. C.
Jorgensen, U. G.
Liebig, C.
Maier, G.
Mathiasen, M.
Rahvar, S.
Ricci, D.
Scarpetta, G.
Skottfelt, J.
Southworth, J.
Surdej, J.
Wambsganss, J.
Zimmer, F.
Batista, V.
Beaulieu, J. P.
Brillant, S.
Cassan, A.
Cole, A.
Corrales, E.
Coutures, Ch.
Dieters, S.
Greenhill, J.
Kubas, D.
Menzies, J.
CA Moa Collaboration
Fun Collaboration
RoboNet Collaboration
Mindstep Consortium
Planet Collaboration
TI A SUB-SATURN MASS PLANET, MOA-2009-BLG-319Lb
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing: micro; planetary systems
ID DIFFERENCE IMAGE-ANALYSIS; MAGNIFICATION MICROLENSING EVENTS; CLUMP
ABSOLUTE MAGNITUDE; GALACTIC BULGE; SNOW LINE; JUPITER/SATURN ANALOG;
EXTRASOLAR PLANETS; OPTICAL DEPTH; GIANT PLANETS; PARALLAX
AB We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K-or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 +/- 0.02) x 10(-4) and a separation of d = 0.97537 +/- 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t(E), and angular Einstein radius,theta(E), along with a standard Galactic model indicates a host star mass of M-L = 0.38(-0.18)(+0.34) M-circle dot and a planet mass of M-p = 50(-24)(+44)M(circle plus), which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4(-0.6)(+1.2) AU and a distance to the planetary system of D-L = 6.1(-1.2)(+1.1) kpc. This separation is similar to 2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.
C1 [Miyake, N.; Sumi, T.; Furusawa, K.; Suzuki, D.; Abe, F.; Fukui, A.; Hayashi, F.; Hosaka, S.; Itow, Y.; Kamiya, K.; Makita, S.; Masuda, K.; Matsubara, Y.; Nishimoto, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Dong, Subo] Inst Adv Study, Princeton, NJ 08540 USA.
[Street, R.; Tsapras, Y.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Street, R.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Mancini, L.; Bozza, V.; Novati, S. Calchi; Scarpetta, G.] Univ Salerno, Dipartimento Fis E R Caianiello, I-84085 Fisciano, SA, Italy.
[Mancini, L.; Bozza, V.; Novati, S. Calchi; Scarpetta, G.] IIASS, I-84019 Vietri Sul Mare, SA, Italy.
[Mancini, L.] Univ Sannio, Dipartimento Ingn, I-82100 Benevento, Italy.
[Gould, A.; Yee, J. C.; Gaudi, B. S.; Janczak, J.; Kozlowski, S.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Tsapras, Y.] Univ London, Sch Math Sci, Astron Unit, London E1 4NS, England.
[Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Bond, I. A.; Lin, W.; Ling, C. H.; Skuljan, L.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, Auckland, New Zealand.
[Fouque, P.] Univ Toulouse, CNRS, LATT, F-31400 Toulouse, France.
[Browne, P.; Horne, K.; Kains, N.; Dominik, M.; Liebig, C.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Han, C.; Hwang, K. -H.] Chungbuk Natl Univ, Dept Phys, Inst Basic Sci Res, Chonju 361763, South Korea.
[Snodgrass, C.] European So Observ, Santiago 19, Chile.
[Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Finet, F.; Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Harpsoe, K.; Hinse, T. C.; Jorgensen, U. G.; Mathiasen, M.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Kobenhavn O, Denmark.
[Allen, W.] Vintage Lane Observ, Blenheim, New Zealand.
[Hundertmark, M.; Dreizler, S.; Hessman, F. V.] Georg August Univ, Inst Astrophys, D-37077 Gottingen, Germany.
[Freeman, M.; Botzler, C. S.; Douchin, D.; Perrott, Y. C.; Rattenbury, N.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland, New Zealand.
[Hearnshaw, J. B.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Kilmartin, P. M.; Tristram, P. J.] Univ Canterbury, Mt John Univ Observ, Lake Tekapo 8770, New Zealand.
[Korpela, A.; Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
[Muraki, Y.; Wada, K.] Konan Univ, Dept Phys, Kobe, Hyogo 658, Japan.
[Nagayama, T.] Nagoya Univ, Dept Phys & Astrophys, Fac Sci, Nagoya, Aichi 4648602, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan.
[Bolt, G.] Craigie Observ, Perth, WA, Australia.
[Bos, M.] Molehill Astron Observ, Auckland, New Zealand.
[Christie, G. W.] Auckland Observ, Auckland, New Zealand.
[DePoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Drummond, J.] Possum Observ, Patutahi, New Zealand.
[Gal-Yam, A.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Gorbikov, E.; Kaspi, S.; Maoz, D.; Polishook, D.; Shporer, A.; Spector, O.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Gorbikov, E.; Kaspi, S.; Maoz, D.; Polishook, D.; Shporer, A.; Spector, O.] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel.
[Higgins, D.] Hunters Hill Observ, Canberra, ACT, Australia.
[Kaspi, S.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Lee, C. -U.; Koo, J. -R.] Korea Astron & Space Sci Inst, Taejon, South Korea.
[Koo, J. -R.; Lee, Y.] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon, South Korea.
[Mallia, F.; Maury, A.] Campo Catino Austral Observ, San Pedro De Atacama, Chile.
[McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand.
[Monard, L. A. G.] Ctr Backyard Astrophys, Bronberg Observ, Pretoria, South Africa.
[Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand.
[Munoz, J. A.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
[Natusch, T.] AUT Univ, Auckland, New Zealand.
[Ofek, E. O.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Santallo, R.] So Stars Observ, Faaa, Tahiti, Fr Polynesia.
[Allan, A.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Bramich, D. M.] European So Observ, D-85748 Garching, Germany.
[Steele, I.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England.
[Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Grp Collegato Salerno, Sez Napoli, Salerno, Italy.
[Burgdorf, M. J.] Univ Stuttgart, Deutsch SOFIA Inst, Stuttgart, Germany.
[Burgdorf, M. J.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Glitrup, M.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Jorgensen, U. G.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen O, Denmark.
[Liebig, C.; Maier, G.; Wambsganss, J.; Zimmer, F.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
[Rahvar, S.] IPM Inst Studies Theoret Phys & Math, Sch Astron, Tehran, Iran.
[Southworth, J.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Batista, V.; Beaulieu, J. P.; Cassan, A.; Corrales, E.; Coutures, Ch.; Dieters, S.; Kubas, D.] Univ Paris 06, UPMC, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Batista, V.; Beaulieu, J. P.; Cassan, A.; Corrales, E.; Coutures, Ch.; Dieters, S.; Kubas, D.] CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Beaulieu, J. P.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Brillant, S.; Kubas, D.] European So Observ, Santiago 19, Chile.
[Cole, A.; Dieters, S.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, GPO Hobart, Tasmania 7001, Australia.
[Menzies, J.] S African Astron Observ, ZA-7925 Observatory, South Africa.
RP Miyake, N (reprint author), Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
EM nmiyake@stelab.nagoya-u.ac.jp; sumi@stelab.nagoya-u.ac.jp; dong@ias.edu;
gould@astronomy.ohio-state.edu; bennett@nd.edu;
jyee@astronomy.ohio-state.edu; i.a.bond@massey.ac.nz;
cheongho@astroph.chungbuk.ac.kr; furusawa@stelab.nagoya-u.ac.jp;
whallen@xtra.co.nz; dsuke@stelab.nagoya-u.ac.jp;
abe@stelab.nagoya-u.ac.jp; afukui@stelab.nagoya-u.ac.jp;
fhayashi@stelab.nagoya-u.ac.jp; hosaka@stelab.nagoya-u.ac.jp;
itow@stelab.nagoya-u.ac.jp; kkamiya@stelab.nagoya-u.ac.jp;
makita@stelab.nagoya-u.ac.jp; kmasuda@stelab.nagoya-u.ac.jp;
ymatsu@stelab.nagoya-u.ac.jp; nishimo@stelab.nagoya-u.ac.jp;
gbolt@iinet.net.au; molehill@ihug.co.nz; gwchristie@christie.org.nz;
depoy@physics.tamu.edu; john_drummond@xtra.co.nz;
avishay.gal-yam@weizmann.ac.il; gaudi@astronomy.ohio-state.edu;
dhi67540@bigpond.net.au; jyee@astronomy.ohio-state.edu;
simkoz@astronomy.ohio-state.edu; francomallia@campocatinobservatory.org;
alain@spaceobs.com; lagmonar@nmisa.org; acrux@orcon.net.nz;
tim.natusch@aut.ac.nz; pogge@astronomy.ohio-state.edu;
obs930@southernstars-observatory.org; guy.thornley@gmail.com
RI Gaudi, Bernard/I-7732-2012; Dong, Subo/J-7319-2012; Greenhill,
John/C-8367-2013; Kozlowski, Szymon/G-4799-2013; Zimmer,
Fabian/M-4765-2014; Hundertmark, Markus/C-6190-2015; Rahvar,
Sohrab/A-9350-2008;
OI Kozlowski, Szymon/0000-0003-4084-880X; Hundertmark,
Markus/0000-0003-0961-5231; Rahvar, Sohrab/0000-0002-7084-5725; Dominik,
Martin/0000-0002-3202-0343; Cole, Andrew/0000-0003-0303-3855; Ricci,
Davide/0000-0002-9790-0552; Snodgrass, Colin/0000-0001-9328-2905
FU JSPS [JSPS20340052, JSPS18253002, JSPS20740104]; Nagoya University; MEXT
of Japan; Massey University and the University of Auckland; NASA
[NNX07AL71G, NNX10AI81G, NNG04GL51G]; NSF [AST-0708890, AST-0757888];
National Research Foundation of Korea [2009-0081561]; Department of
Culture, Arts, and Leisure (DCAL), Northern Ireland; Communaute
francaise de Belgique-Actions de recherche concertees-Academie
universitaire Wallonie-Europe
FX The MOA project and a part of authors were supported by the Grant-in-Aid
for Scientific Research, the grant JSPS20340052, JSPS18253002, JSPS
Research fellowships, the Global COE Program of Nagoya University "Quest
for Fundamental Principles in the Universe" from JSPS and MEXT of Japan,
the for Research and Technology, and grants-in-aid from Massey
University and the University of Auckland. N.M. was supported by JSPS
Research Fellowships for Young Scientists. T.S. was supported by the
grant JSPS20740104. D.P.B. was supported by grants NNX07AL71G and
NNX10AI81G from NASA and AST-0708890 from the NSF. A.G. and S.D. were
supported in part by NSF AST-0757888. A.G., S.D., S.G., and R.P. were
supported in part by NASA NNG04GL51G. Work by S.D. was performed in part
under contract with the California Institute of Technology (Caltech)
funded by NASA through the Sagan Fellowship Program. J.C.Y. was
supported by an NSF Graduate Research Fellowship. Work by C.H. was
supported by the Creative Research Initiative program (2009-0081561) of
the National Research Foundation of Korea. Astronomical research at
Armagh Observatory was supported by the Department of Culture, Arts, and
Leisure (DCAL), Northern Ireland, UK. F.F., D.R., and J.S. acknowledge
support from the Communaute francaise de Belgique-Actions de recherche
concertees-Academie universitaire Wallonie-Europe.
NR 52
TC 24
Z9 24
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2011
VL 728
IS 2
AR 120
DI 10.1088/0004-637X/728/2/120
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716MP
UT WOS:000286973600046
ER
PT J
AU Pinder, RW
Walker, JT
Bash, JO
Cady-Pereira, KE
Henze, DK
Luo, MZ
Osterman, GB
Shephard, MW
AF Pinder, Robert W.
Walker, John T.
Bash, Jesse O.
Cady-Pereira, Karen E.
Henze, Daven K.
Luo, Mingzhao
Osterman, Gregory B.
Shephard, Mark W.
TI Quantifying spatial and seasonal variability in atmospheric ammonia with
in situ and space-based observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID DEPOSITION; NITROGEN
AB Ammonia plays an important role in many biogeochemical processes, yet atmospheric mixing ratios are not well known. Recently, methods have been developed for retrieving NH(3) from space-based observations, but they have not been compared to in situ measurements. We have conducted a field campaign combining co-located surface measurements and satellite special observations from the Tropospheric Emission Spectrometer (TES). Our study includes 25 surface monitoring sites spanning 350 km across eastern North Carolina, a region with large seasonal and spatial variability in NH3. From the TES spectra, we retrieve a NH3 representative volume mixing ratio (RVMR), and we restrict our analysis to times when the region of the atmosphere observed by TES is representative of the surface measurement. We find that the TES NH3 RVMR qualitatively captures the seasonal and spatial variability found in eastern North Carolina. Both surface measurements and TES NH3 show a strong correspondence with the number of livestock facilities within 10 km of the observation. Furthermore, we find that TES NH3 RVMR captures the month-to-month variability present in the surface observations. The high correspondence with in situ measurements and vast spatial coverage make TES NH3 RVMR a valuable tool for understanding regional and global NH3 fluxes. Citation: Pinder, R. W., J. T. Walker, J. O. Bash, K. E. Cady-Pereira, D. K. Henze, M. Luo, G. B. Osterman, and M. W. Shephard (2011), Quantifying spatial and seasonal variability in atmospheric ammonia with in situ and space-based observations, Geophys. Res. Lett., 38, L04802, doi: 10.1029/2010GL046146.
C1 [Pinder, Robert W.; Walker, John T.; Bash, Jesse O.] US EPA, Off Res & Dev, Res Triangle Pk, NC 27711 USA.
[Cady-Pereira, Karen E.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
[Henze, Daven K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80302 USA.
[Luo, Mingzhao; Osterman, Gregory B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Shephard, Mark W.] Environm Canada, Toronto, ON M3H 5T4, Canada.
RP Pinder, RW (reprint author), US EPA, Off Res & Dev, Mail Drop E243-01, Res Triangle Pk, NC 27711 USA.
EM pinder.rob@epa.gov
RI Henze, Daven/A-1920-2012; Pinder, Robert/F-8252-2011; Bash,
Jesse/E-9688-2013; Walker, John/I-8880-2014
OI Pinder, Robert/0000-0001-6390-7126; Bash, Jesse/0000-0001-8736-0102;
Walker, John/0000-0001-6034-7514
FU NASA [NNX10AG63G]
FX We acknowledge Wayne Fowler and Alf Wall (EPA) for CAMNet field support
and Wayne Robarge and Guillermo Ramirez (Department of Soil Science,
North Carolina State University) for CAMNet analytical support. Research
at Atmospheric and Environmental Research, University of Colorado at
Boulder, and at the Jet Propulsion Laboratory was supported under
contract to NASA project number NNX10AG63G. Although this paper has been
reviewed by the EPA and approved for publication, it does not
necessarily reflect EPA policies or views.
NR 19
TC 26
Z9 26
U1 0
U2 19
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 FEB 18
PY 2011
VL 38
AR L04802
DI 10.1029/2010GL046146
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 723QL
UT WOS:000287521800002
ER
PT J
AU Anderson, CR
Kudela, RM
Benitez-Nelson, C
Sekula-Wood, E
Burrell, CT
Chao, Y
Langlois, G
Goodman, J
Siegel, DA
AF Anderson, Clarissa R.
Kudela, Raphael M.
Benitez-Nelson, Claudia
Sekula-Wood, Emily
Burrell, Christopher T.
Chao, Yi
Langlois, Gregg
Goodman, Jo
Siegel, David A.
TI Detecting toxic diatom blooms from ocean color and a regional ocean
model
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID PSEUDO-NITZSCHIA-AUSTRALIS; DOMOIC ACID PRODUCTION; CENTRAL CALIFORNIA
COAST; HARMFUL ALGAL BLOOMS; SILICATE LIMITATION; KARENIA-BREVIS; SEA
LIONS; BACILLARIOPHYCEAE; SYSTEM; DINOFLAGELLATE
AB An apparent link between upwelling-related physical signatures, macronutrients, and toxic diatom blooms in the various "hotspots" throughout California has motivated attempts to forecast harmful algal blooms (HABs) as a function of select environmental variables. Empirical models for predicting toxic Pseudo-nitzschia blooms in one such region, the Santa Barbara Channel (SBC), are tested in a nowcast mode using predictions based on merging data from MODIS ocean color geophysical products and the Regional Ocean Modeling System (ROMS) applied to the Southern California Bight. Thresholds for each model generate event forecasts. Spatially-explicit, monthly HAB maps are compared to shipboard observations and California monitoring data, demonstrating that the models predict offshore events otherwise undetected by nearshore monitoring. The use of mechanistic hydrodynamic models in concert with empirical, biological models facilitates future process studies on the effects of coastal eutrophication and climate change on regional HAB dynamics. Citation: Anderson, C. R., R. M. Kudela, C. Benitez-Nelson, E. Sekula-Wood, C. T. Burrell, Y. Chao, G. Langlois, J. Goodman, and D. A. Siegel (2011), Detecting toxic diatom blooms from ocean color and a regional ocean model, Geophys. Res. Lett., 38, L04603, doi:10.1029/2010GL045858.
C1 [Anderson, Clarissa R.; Kudela, Raphael M.] Univ Calif Santa Cruz, Ocean Sci Dept, Santa Cruz, CA 95064 USA.
[Anderson, Clarissa R.; Benitez-Nelson, Claudia; Sekula-Wood, Emily; Burrell, Christopher T.] Univ S Carolina, Columbia, SC 29208 USA.
[Chao, Yi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Langlois, Gregg] Dept Hlth Serv, Environm Management Branch, Richmond, CA 94804 USA.
[Goodman, Jo; Siegel, David A.] Univ Calif Santa Barbara, Earth Res Inst, Inst Marine Sci, Santa Barbara, CA 93106 USA.
RP Anderson, CR (reprint author), Univ Calif Santa Cruz, Ocean Sci Dept, 1156 High St, Santa Cruz, CA 95064 USA.
EM clrander@ucsc.edu
RI Siegel, David/C-5587-2008;
OI Benitez-Nelson, Claudia/0000-0002-1004-5048
FU National Oceanic and Atmospheric Administration - Monitoring and Event
Response to Harmful Algal Blooms (NOAA-MERHAB) [NA04NOS4780239];
National Science Foundation Chemical Oceanography; National Aeronautics
and Space Administration; Jet Propulsion Laboratory, California
Institute of Technology under National Aeronautics and Space
Administration (NASA)
FX This research was supported by funding from the National Oceanic and
Atmospheric Administration - Monitoring and Event Response to Harmful
Algal Blooms (NOAA-MERHAB, Award NA04NOS4780239 - PIs: R. Kudela, P.
Miller, and G. Langlois) publication 145, the National Science
Foundation Chemical Oceanography program (PI: C. Benitez-Nelson), and
the National Aeronautics and Space Administration (PI: D. Siegel). The
research described in this paper was carried out, in part, at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration (NASA).
We sincerely thank Nathalie Guillocheau, Bernard Friedman, Raghu
Murtugudde (Chesapeake Bay Forecasting Project), Thomas Ellis, the
Plumes and Blooms staff, and crew of the R.V. Shearwater for significant
contributions to data collection and analysis. We also acknowledge two
anonymous reviewers for comments that greatly improved the paper.
NR 33
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Z9 11
U1 2
U2 28
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 17
PY 2011
VL 38
AR L04603
DI 10.1029/2010GL045858
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 723QK
UT WOS:000287521700001
ER
PT J
AU Pracna, P
Urban, J
Votava, O
Meltzerova, Z
Urban, S
Horneman, VM
Drouin, BJ
AF Pracna, Petr
Urban, Jiri
Votava, Ondrej
Meltzerova, Zuzana
Urban, Stepan
Horneman, Veli-Matti
Drouin, Brian J.
TI Rotational and Rovibrational Spectroscopy of CH3NC of the Ground and
v(4)=1 Vibrational States
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID RESOLUTION INFRARED-SPECTROSCOPY; METHYL ISOCYANIDE; MICROWAVE-SPECTRA;
COLLISIONAL DEACTIVATION; PROPYNE; ISOMERIZATION; PARAMETERS; MOLECULES;
CONSTANTS
AB The parallel vibration-rotation band v(4) of methyl isocyanide (CH3NC), with a band center at 944.9 cm(-1), was studied by FTIR spectroscopy between 890 and 980 cm(-1) in order to improve the ground-state rotational constants. Such improvement is essential for the scheduled studies of excited vibrational levels and their mutual anharmonic resonances occurring at higher values of the K rotational number. Ground-state combination differences generated from this band, spanning values of J/K from 0 to 85/13, were combined with rotational data from the literature and newly measured rotational transitions, extending the J/K range from 3/0 up to 31/14, and fitted simultaneously with a fully quantitative reproduction of the data. The infrared data of the v(4) band were analyzed together with rotational data of the v(4) = 1 level, spanning values of J/K from 4/0 to 14/12. The fit in the approximation of an isolated vibrational state, with the transitions perturbed by weak local resonances excluded, yields reproduction of the data within experimental uncertainties.
C1 [Pracna, Petr; Urban, Jiri; Votava, Ondrej] Acad Sci Czech Republic, Vvi, J Heyrovsky Inst Phys Chem, CR-18223 Prague 8, Czech Republic.
[Meltzerova, Zuzana; Urban, Stepan] Inst Chem Technol, Dept Analyt Chem, CR-16628 Prague 6, Czech Republic.
[Horneman, Veli-Matti] Univ Oulu, Dept Phys, Oulu 90014, Finland.
[Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pracna, P (reprint author), Acad Sci Czech Republic, Vvi, J Heyrovsky Inst Phys Chem, Dolejskova 3, CR-18223 Prague 8, Czech Republic.
EM pracna@jh-inst.cas.cz
RI Urban, Jiri/O-2352-2014
FU Grant Agency of the Academy of Sciences of the Czech Republic
[IAA400400706]; Ministry of Education, Youth and Sports of the Czech
Republic [LC06071]; National Aeronautics and Space Administration
FX This work was supported by the Grant Agency of the Academy of Sciences
of the Czech Republic (project IAA400400706) and the Ministry of
Education, Youth and Sports of the Czech Republic (research program
LC06071). Portions of this research were performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 29
TC 3
Z9 3
U1 1
U2 7
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD FEB 17
PY 2011
VL 115
IS 6
BP 1063
EP 1068
DI 10.1021/jp1090312
PG 6
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 717RV
UT WOS:000287066000014
PM 21268623
ER
PT J
AU Boening, C
Lee, T
Zlotnicki, V
AF Boening, Carmen
Lee, Tong
Zlotnicki, Victor
TI A record-high ocean bottom pressure in the South Pacific observed by
GRACE
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GLOBAL OCEAN; SEA-LEVEL; VARIABILITY; MODEL
AB In late 2009 to early 2010, the Gravity Recovery and Climate Experiment (GRACE) satellite pair observed a record increase in ocean bottom pressure (OBP) over a large mid-latitude region of the South East Pacific. Its magnitude is substantially larger than other oceanic events in the Southern Hemisphere found in the entire GRACE data records (2003-2010) on multi-month time scales. The OBP data help to understand the nature of a similar signal in sea surface height (SSH) anomaly observed by altimetry: the SSH increase is mainly due to mass convergence. Analysis of the barotropic vorticity equation using scatterometer data, atmospheric reanalysis product, and GRACE and altimeter an atmospheric reanalysis product observations suggests that the observed OBP/SSH signal was primarily caused by wind stress curl associated with a strong and persistent anticyclone in late 2009 in combination with effects of planetary vorticity gradient, bottom topography, and friction. Citation: Boening, C., T. Lee, and V. Zlotnicki (2011), A record-high ocean bottom pressure in the South Pacific observed by GRACE, Geophys. Res. Lett., 38, L04602, doi:10.1029/2010GL046013.
C1 [Boening, Carmen; Lee, Tong; Zlotnicki, Victor] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Boening, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Carmen.Boening@jpl.nasa.gov
OI Boening, Claus/0000-0002-6251-5777
FU NASA
FX This work was supported by the NASA Physical Oceanography, Solid Earth,
MEaSUREs and EOSDIS Programs and performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. We thank the German Space Operations Center (GSOC) of the German
Aerospace Center (DLR) for providing continuously and nearly 100% of the
raw telemetry data of the twin GRACE satellites and the processing
centers at University of Texas, JPL, and Geoforschungszentrum Potsdam.
We also thank the two anonymous reviewers for their thorough reviews and
several important suggestions.
NR 21
TC 20
Z9 20
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 17
PY 2011
VL 38
AR L04602
DI 10.1029/2010GL046013
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 723QK
UT WOS:000287521700003
ER
PT J
AU Frankenberg, C
Aben, I
Bergamaschi, P
Dlugokencky, EJ
van Hees, R
Houweling, S
van der Meer, P
Snel, R
Tol, P
AF Frankenberg, C.
Aben, I.
Bergamaschi, P.
Dlugokencky, E. J.
van Hees, R.
Houweling, S.
van der Meer, P.
Snel, R.
Tol, P.
TI Global column-averaged methane mixing ratios from 2003 to 2009 as
derived from SCIAMACHY: Trends and variability
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ATMOSPHERIC METHANE; SATELLITE; SPACE; EMISSIONS
AB After a decade of stable or slightly decreasing global methane concentrations, ground-based in situ data show that CH4 began increasing again in 2007 and that this increase continued through 2009. So far, space-based retrievals sensitive to the lower troposphere in the time period under consideration have not been available. Here we report a long-term data set of column-averaged methane mixing ratios retrieved from spectra of the Scanning Imaging Absorption Spectrometer for Atmospheric Cartography (SCIAMACHY) instrument onboard Envisat. The retrieval quality after 2005 was severely affected by degrading detector pixels within the methane 2v(3) absorption band. We identified the most crucial problems in SCIAMACHY detector degradation and overcame the problem by applying a strict pixel mask as well as a new dark current characterization. Even though retrieval precision after the end of 2005 is invariably degraded, consistent methane retrievals from 2003 through 2009 are now possible. Regional time series in the Sahara, Australia, tropical Africa, South America, and Asia show the methane increase in 2007-2009, but we cannot yet draw a firm conclusion concerning the origin of the increase. Tropical Africa even seems to exhibit a negative anomaly in 2006, but an impact from changes in SCIAMACHY detector degradation cannot be excluded yet. Over Assakrem, Algeria, we observed strong similarities between SCIAMACHY measurements and ground-based data in deseasonalized time series. We further show long-term SCIAMACHY xCH(4) averages at high spatial resolution that provide further insight into methane variations on regional scales. The Red Basin in China exhibits, on average, the highest methane abundance worldwide, while other localized features such as the Sudd wetlands in southern Sudan can also be identified in SCIAMACHY xCH(4) averages.
C1 [Frankenberg, C.; Aben, I.; van Hees, R.; Houweling, S.; van der Meer, P.; Snel, R.; Tol, P.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Bergamaschi, P.] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21020 Ispra, Italy.
[Dlugokencky, E. J.] NOAA, Earth Syst Res Lab, Global Monitoring Div, Boulder, CO 80305 USA.
[Houweling, S.] Inst Marine & Atmospher Res Utrecht, Utrecht, Netherlands.
RP Frankenberg, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM christian.frankenberg@jpl.nasa.gov
RI Frankenberg, Christian/A-2944-2013
OI Frankenberg, Christian/0000-0002-0546-5857
FU Dutch Science Foundation (NWO); European Commission [037048]; GEOMON
[036677]; GEMS-IP [SIP4-CT-2004-516099]; European Union [FP7/2007-2013,
218793]; European Commission; Joint Research Centre (JRC)/Netherlands
Environmental Assessment Agency; Emission Database for Global
Atmospheric Research (EDGAR)
FX CF was mostly supported by the Dutch Science Foundation (NWO) through a
VENI grant. We acknowledge John Burrows, PI of the SCIAMACHY instrument,
for having initiated and realized the SCIAMACHY project. The Netherlands
SCIAMACHY Data Center and ESA are greatly appreciated for providing
data. We thank Wouter Peters for providing CarbonTracker results and A.
Segers, C. Schrijvers, O. Tuinder, and A. Gloudemans for providing ECMWF
data collocated with SCIAMACHY. We acknowledge the European Commission
for supporting the Sixth Framework Programme project HYMN (contract
037048) and GEOMON (contract 036677), GEMS-IP (contract
SIP4-CT-2004-516099). We further acknowledge exchange of information
within the EU 6th FP Network of Excellence ACCENT. The research leading
to these results has received funding from the European Union's Seventh
Framework Programme (FP7/2007-2013) under Grant Agreement 218793. Part
of the research was funded through the EU's Seventh Framework Programme
(FP7/2007-2013) under Grant Agreement 218793 (MACC). We further
acknowledge the source of EDGAR data: European Commission, Joint
Research Centre (JRC)/Netherlands Environmental Assessment Agency (PBL);
Emission Database for Global Atmospheric Research (EDGAR), release
version 4.0 (http://edgar.jrc.ec.europa.eu), 2009. We thank and honor
Annemieke
NR 28
TC 83
Z9 83
U1 2
U2 37
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 FEB 17
PY 2011
VL 116
AR D04302
DI 10.1029/2010JD014849
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 723QA
UT WOS:000287520700003
ER
PT J
AU Li, ZQ
Li, C
Chen, H
Tsay, SC
Holben, B
Huang, J
Li, B
Maring, H
Qian, Y
Shi, G
Xia, X
Yin, Y
Zheng, Y
Zhuang, G
AF Li, Zhanqing
Li, C.
Chen, H.
Tsay, S. -C.
Holben, B.
Huang, J.
Li, B.
Maring, H.
Qian, Y.
Shi, G.
Xia, X.
Yin, Y.
Zheng, Y.
Zhuang, G.
TI East Asian Studies of Tropospheric Aerosols and their Impact on Regional
Climate (EAST-AIRC): An overview
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SOLAR-RADIATION; DUST AEROSOLS; EARTHS SURFACE; CHINA; CLOUD; POLLUTION;
STORM; PRECIPITATION; PACIFIC; DESERT
AB As the most populated region of the world, Asia is a major source of aerosols with potential large impact over vast downstream areas. Papers published in this special section describe the variety of aerosols observed in China and their effects and interactions with the regional climate as part of the East Asian Study of Tropospheric Aerosols and their Impact on Regional Climate (EAST-AIRC). The majority of the papers are based on analyses of observations made under three field projects, namely, the Atmospheric Radiation Measurements ( ARM) Mobile Facility mission in China (AMF-China), the East Asian Study of Tropospheric Aerosols: An International Regional Experiment (EAST-AIRE), and the Atmospheric Aerosols of China and their Climate Effects (AACCE). The former two are U.S.-China collaborative projects, and the latter is a part of the China's National Basic Research program ( or often referred to as "973 project"). Routine meteorological data of China are also employed in some studies. The wealth of general and specialized measurements lead to extensive and close-up investigations of the optical, physical, and chemical properties of anthropogenic, natural, and mixed aerosols; their sources, formation, and transport mechanisms; horizontal, vertical, and temporal variations; direct and indirect effects; and interactions with the East Asian monsoon system. Particular efforts are made to advance our understanding of the mixing and interaction between dust and anthropogenic pollutants during transport. Several modeling studies were carried out to simulate aerosol impact on radiation budget, temperature, precipitation, wind and atmospheric circulation, fog, etc. In addition, impacts of the Asian monsoon system on aerosol loading are also simulated.
C1 [Li, Zhanqing; Li, C.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Li, Zhanqing; Li, C.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20740 USA.
[Li, Zhanqing] Beijing Normal Univ, State Lab Earth Surface Proc & Resource Ecol, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
[Li, Zhanqing; Yin, Y.; Zheng, Y.] Nanjing Univ Informat Sci & Technol, Coll Atmospher Phys, Nanjing 21004, Peoples R China.
[Li, C.; Tsay, S. -C.; Holben, B.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Chen, H.; Shi, G.; Xia, X.] Chinese Acad Sci, Inst Atmospher Phys, Beijing 100029, Peoples R China.
[Huang, J.] Lanzhou Univ, Sch Atmospher Sci, Lanzhou 730000, Peoples R China.
[Li, B.] China Meteorol Adm, Ctr Atmospher Observat, Beijing 100081, Peoples R China.
[Maring, H.] NASA Headquarters, Radiat Sci Program, Washington, DC 20546 USA.
[Qian, Y.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Zhuang, G.] Fudan Univ, Dept Environm Sci & Technol, Shanghai 200433, Peoples R China.
RP Li, ZQ (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
EM zli@atmos.umd.edu
RI qian, yun/E-1845-2011; Li, Can/F-6867-2011; Xia, Xiangao/G-5545-2011;
Yin, Yan/I-8350-2014; Tsay, Si-Chee/J-1147-2014; Li,
Zhanqing/F-4424-2010
OI Xia, Xiangao/0000-0002-4187-6311; Yin, Yan/0000-0002-8391-2712; Li,
Zhanqing/0000-0001-6737-382X
FU MOST [2006CB403706]; DOE [DEFG0208ER64571]; NASA [NNX08AH71G]; U.S. DOE
by Battelle Memorial Institute [DE-AC06-76RLO1830]
FX The study was supported by funding from the MOST (2006CB403706), DOE
(DEFG0208ER64571), and NASA (NNX08AH71G). Figure 1b was created by S.
Colson and J. Marshall. The AMF-China campaign was facilitated by many
DOE scientists and managers, to name a few, M. Alsop, D. Kim Nitschke,
D. Sisterson, W. Ferrell, K. Alapaty, J. Mather, M. Miller, and C.
Flynn. W.-C. Wang of the SUNY Albany played a special role as the chief
scientist for the U.S.China climate change cooperative program under
which the campaign was carried out. Yun Qian's contribution is sponsored
by the U. S. DOE's Office of Science Biological and Environmental
Research under a bilateral agreement with the China Ministry of Science
and Technology on regional climate research. PNNL is operated for the
U.S. DOE by Battelle Memorial Institute under contract
DE-AC06-76RLO1830.
NR 100
TC 86
Z9 89
U1 6
U2 50
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 FEB 17
PY 2011
VL 116
AR D00K34
DI 10.1029/2010JD015257
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 723QA
UT WOS:000287520700005
ER
PT J
AU Lin, Y
Williams, TV
Xu, TB
Cao, W
Elsayed-Ali, HE
Connell, JW
AF Lin, Yi
Williams, Tiffany V.
Xu, Tian-Bing
Cao, Wei
Elsayed-Ali, Hani E.
Connell, John W.
TI Aqueous Dispersions of Few-Layered and Monolayered Hexagonal Boron
Nitride Nanosheets from Sonication-Assisted Hydrolysis: Critical Role of
Water
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Article
ID NANORIBBONS; NANOTUBES; PAPER
AB Hexagonal boron nitride (h-BN) is traditionally considered to be insoluble in water. However, here we demonstrate that water is effective to exfoliate the layered h-BN structures with the assistance of bath sonication, forming "clean" aqueous dispersions of h-BN nanosheets without the use of surfactants or organic functionalization. Besides few layered h-BN nanosheets, there was also evidence on the presence of monolayered nanosheet and nanoribbon species. Most nanosheets were of reduced lateral sizes, which was attributed to the cutting of parent h-BN sheets induced by the sonication-assisted hydrolysis (evidenced by the ammonia test and spectroscopy results). The hydrolysis effect also assisted in the exfoliation of h-BN nanosheets in addition to the solvent polarity effect. The h-BN nanosheets in such "clean" aqueous dispersions were demonstrated to be conveniently processed via solution methods with retained physical properties. The dispersed h-BN nanosheets in water also exhibited strong affinity toward proteins such as ferritin, suggesting that the nanosheet surfaces were available for further bioconjugations. The above findings may pave the way for the applications of these novel 2-dimensional nanomaterials in various fields such as composites, electronics, and biology.
C1 [Lin, Yi; Xu, Tian-Bing] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Williams, Tiffany V.; Connell, John W.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Cao, Wei; Elsayed-Ali, Hani E.] Old Dominion Univ, Appl Res Ctr, Newport News, VA 23606 USA.
RP Lin, Y (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
EM yi.lin-1@nasa.gov
RI Cao, Wei/E-8950-2011;
OI Williams, Tiffany/0000-0003-3463-9200
NR 28
TC 167
Z9 169
U1 23
U2 205
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 FEB 17
PY 2011
VL 115
IS 6
BP 2679
EP 2685
DI 10.1021/jp110985w
PG 7
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA 717RS
UT WOS:000287065700011
ER
PT J
AU Li, RX
He, SJ
Chen, YH
Tang, M
Tang, PB
Di, KC
Matthies, L
Arvidson, RE
Squyres, SW
Crumpler, LS
Parker, T
Sims, M
AF Li, Rongxing
He, Shaojun
Chen, Yunhang
Tang, Min
Tang, Pingbo
Di, Kaichang
Matthies, Larry
Arvidson, Raymond E.
Squyres, Steven W.
Crumpler, Larry S.
Parker, Tim
Sims, Michael
TI MER Spirit rover localization: Comparison of ground image- and orbital
image-based methods and science applications
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GUSEV CRATER; LASER ALTIMETER; LANDING-SITE; MARS; MISSION; ADJUSTMENT
AB During 6 years of continuous operations on the Martian surface, the Mars Exploration Rover (MER) Spirit has covered a traverse of approximately 7 km from the landing point to its current position at "Troy" near Home Plate. Localization of Spirit (and Opportunity) has been performed using two different methods: one that employs an incremental bundle adjustment (IBA) using rover imagery, and one that compares image features common to both a rover orthoimage and an orbital orthoimage. The IBA method continuously yields the desired 3-D rover positions at a very high level of accuracy and provides a simultaneous solution for high-quality topographic mapping of neighborhoods surrounding the rover. On the other hand, high-resolution orbital imagery can verify rover positions wherever the rover track is visible. Rapid rover localization on the orbital orthoimage is often achieved by comparing a rover orthoimage to the orbital orthoimage. In this paper, we present research results from a systematic comparison of these two localization methods over the entire length of the Spirit traverse. Two orbital orthoimages were generated from High Resolution Imaging Science Experiment (HiRISE) imagery. Integration of Mars Orbiter Laser Altimeter (MOLA) data into the HiRISE digital elevation model (DEM) and orthoimage generation was performed and proved to be effective in reducing large inconsistencies between MOLA and HiRISE data. This study found an overall difference of 1.5 percent of the traversed distance between the two sets of traverse positions derived using the two different localization methods. After a geometric transformation from one traverse to the other, the remaining inconsistency then represents the local differences between them and can be reduced to a level of less than 0.15 percent. Discussions of error sources and the strength and weakness of the methods are given. Scientific applications of the localization data are also briefly introduced.
C1 [Li, Rongxing; He, Shaojun; Chen, Yunhang; Tang, Min; Tang, Pingbo; Di, Kaichang] Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Mapping & GIS Lab, Columbus, OH 43210 USA.
[Matthies, Larry; Parker, Tim] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Arvidson, Raymond E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Squyres, Steven W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Crumpler, Larry S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA.
[Sims, Michael] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Li, RX (reprint author), Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Mapping & GIS Lab, Columbus, OH 43210 USA.
EM li.282@osu.edu
RI Tang, Pingbo/I-7649-2012; Tang, Pingbo/I-9534-2012;
OI Tang, Pingbo/0000-0001-9048-1327; Tang, Pingbo/0000-0002-4910-1326
FU NASA; Mars Technology Program; Applied Information Systems Research
Program
FX Funding for this research by NASA through the Mars Exploration Rover
Participating Scientist Program, the Mars Technology Program, and the
Applied Information Systems Research Program is acknowledged. We would
like to thank the USGS for providing their HiRISE DEM and orthoimage for
us to cross-check the results, the University of Arizona for their
HiRISE imagery, and the MER science and engineering teams for
cooperation in rover localization and mapping. Reviewers' constructive
comments are acknowledged.
NR 39
TC 5
Z9 5
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 FEB 16
PY 2011
VL 116
AR E00F16
DI 10.1029/2010JE003773
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 723UP
UT WOS:000287533100001
ER
PT J
AU Yuan, TL
Remer, LA
Pickering, KE
Yu, HB
AF Yuan, Tianle
Remer, Lorraine A.
Pickering, Kenneth E.
Yu, Hongbin
TI Observational evidence of aerosol enhancement of lightning activity and
convective invigoration
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID OPTICAL TRANSIENT DETECTOR; CLOUD ELECTRIFICATION; PART I; MICROPHYSICS;
MODIS; THUNDERSTORMS; ALGORITHM; POLLUTION; PRODUCTS; AMAZON
AB Lightning activity over the West Pacific Ocean east of the Philippines is usually much less frequent than over the nearby maritime continents. However, in 2005 the Lightning Imaging Sensor (LIS) aboard the TRMM satellite observed anomalously high lightning activity in that area. In the same year the Moderate resolution Imaging Spectro-radiometer (MODIS) measured anomalously high aerosol loading. The high aerosol loading was traced to volcanic activity, and not to any factor linked to meteorology, disentangling the usual convolution between aerosols and meteorology. We show that in general lightning activity is tightly correlated with aerosol loadings at both inter-annual and biweekly time scales. We estimate that a similar to 60% increase in aerosol loading leads to more than 150% increase in lightning flashes. Aerosols increase lightning activity through modification of cloud microphysics. Cloud ice particle sizes are reduced and cloud glaciation is delayed to colder temperature when aerosol loading is increased. TRMM precipitation radar measurements indicate that anomalously high aerosol loading is associated with enhanced cloud mixed phase activity and invigorated convection over the maritime ocean. These observed associations between aerosols, cloud microphysics, morphology and lightning activity are not related to meteorological variables or ENSO events. The results have important implications for understanding the variability of lightning and resulting aerosol-chemistry interactions. Citation: Yuan, T., L. A. Remer, K. E. Pickering, and H. Yu (2011), Observational evidence of aerosol enhancement of lightning activity and convective invigoration, Geophys. Res. Lett., 38, L04701, doi:10.1029/2010GL046052.
C1 [Yuan, Tianle] Joint Ctr Environm Technol UMBC, Baltimore, MD USA.
[Yuan, Tianle; Remer, Lorraine A.; Pickering, Kenneth E.; Yu, Hongbin] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Yuan, TL (reprint author), Joint Ctr Environm Technol UMBC, Baltimore, MD USA.
EM tianle.yuan@nasa.gov
RI Yu, Hongbin/C-6485-2008; Yuan, Tianle/D-3323-2011; Pickering,
Kenneth/E-6274-2012
OI Yu, Hongbin/0000-0003-4706-1575;
FU NASA
FX We thank J. V. Martins, I. Koren, C. Wang, M. Chin, Dale Allen, and R.
Albrecht for helpful comments and suggestions. This research is
supported by NASA's Interdisciplinary Research program.
NR 29
TC 67
Z9 69
U1 2
U2 18
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 FEB 16
PY 2011
VL 38
AR L04701
DI 10.1029/2010GL046052
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 723QJ
UT WOS:000287521600003
ER
PT J
AU Nyeo, SL
Ansari, RR
AF Nyeo, Su-Long
Ansari, Rafat R.
TI Sparse Bayesian learning for the Laplace transform inversion in dynamic
light scattering
SO JOURNAL OF COMPUTATIONAL AND APPLIED MATHEMATICS
LA English
DT Article
DE Laplace transform inversion; Regularization method; Sparse Bayesian
learning; Dynamic light scattering; Particle size distribution;
Cataract; Ocular tissues
ID PHOTON-CORRELATION SPECTROSCOPY; MAXIMUM-ENTROPY ANALYSIS; EXPONENTIAL
RELAXATION RATES; RELEVANCE VECTOR MACHINE; ILL-POSED PROBLEMS;
REGULARIZATION PARAMETER; TIKHONOV REGULARIZATION; NUMERICAL INVERSION;
INTEGRAL-EQUATIONS; 1ST KIND
AB A new method is described using the sparse Bayesian learning (SBL) algorithm of Tipping to obtain an optimal and reliable solution to the Laplace transform inversion in dynamic light scattering (DLS).
The linear inverse problem in DLS has numerical solutions that depend on their domains and dimensions. For a given domain and dimension, a sparse solution in an SBL framework is the most-probable solution and can be used for classifying a system of objects by a few relevant values. Recently, we have shown that the SBL algorithm of Tipping is suitable for studying cataract in ocular lenses by describing the opacity of a lens with a few dominant sizes of crystallin proteins in the lens.
However, since the sparseness of SBL solutions cannot reflect a true system, we need to develop a method by using the SBL algorithm to give a true description and, at the same time, a useful classification of the opacity of lenses. We generate a set of sparse solutions of different domains but of the same dimension, and then superimpose them to give a general solution with its dimension treated as a regularization parameter. An optimal solution, which provides a reliable description of a particle system, is determined by the L-curve criterion for selecting the suitable value of the regularization parameter.
The performance of our method is evaluated by analyzing simulated data generated from unimodal and bimodal distributions. From the reconstructed distributions, we see that our method gives high resolution comparable to the sophisticated Bryan's maximum-entropy algorithm, which gives better resolution than CONTIN. Our method is then applied to experimental DLS data of the ocular lenses of a fetal calf and a Rhesus monkey to obtain optimal particle size distributions of crystallins and the crystallin aggregates in the lenses.
We conclude by discussing possible improvements on our method for analyzing DLS data and for solving any linear inverse problem by an SBL algorithm. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Nyeo, Su-Long] Natl Cheng Kung Univ, Dept Phys, Tainan 70101, Taiwan.
[Ansari, Rafat R.] NASA, John H Glenn Res Ctr Lewis Field, Biosci & Technol Branch, Cleveland, OH 44135 USA.
RP Nyeo, SL (reprint author), Natl Cheng Kung Univ, Dept Phys, Tainan 70101, Taiwan.
EM t14269@mail.ncku.edu.tw; Rafat.R.Ansari@nasa.gov
FU National Science Council of the Republic of China [NSC
98-2112-M-006-009]; NASA; Research and Technology Directorate of the
NASA Glenn Research Center
FX Dr. Nyeo would like to acknowledge the financial support from the
National Science Council of the Republic of China under the Contract No.
NSC 98-2112-M-006-009, and Dr. Ansari would like to acknowledge support
from NASA's Human Research Program and the Research and Technology
Directorate of the NASA Glenn Research Center.
NR 39
TC 8
Z9 8
U1 2
U2 15
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0427
J9 J COMPUT APPL MATH
JI J. Comput. Appl. Math.
PD FEB 15
PY 2011
VL 235
IS 8
BP 2861
EP 2872
DI 10.1016/j.cam.2010.12.008
PG 12
WC Mathematics, Applied
SC Mathematics
GA 725JY
UT WOS:000287642200081
ER
PT J
AU Eitzen, ZA
Xu, KM
Wong, T
AF Eitzen, Zachary A.
Xu, Kuan-Man
Wong, Takmeng
TI An Estimate of Low-Cloud Feedbacks from Variations of Cloud Radiative
and Physical Properties with Sea Surface Temperature on Interannual Time
Scales
SO JOURNAL OF CLIMATE
LA English
DT Article
ID ANGULAR-DISTRIBUTION MODELS; ENERGY SYSTEM INSTRUMENT; BOUNDARY-LAYER
CLOUDS; 1998 EL-NINO; STATISTICAL-ANALYSES; OBJECT DATA; PART I;
STRATIFORM CLOUDS; FLUX ESTIMATION; SATELLITE
AB Simulations of climate change have yet to reach a consensus on the sign and magnitude of the changes in physical properties of marine boundary layer clouds. In this study, the authors analyze how cloud and radiative properties vary with SST anomaly in low-cloud regions, based on five years (March 2000-February 2005) of Clouds and the Earth's Radiant Energy System (CERES)-Terra monthly gridded data and matched European Centre for Medium-Range Weather Forecasts (ECMWF) meteorological reanalaysis data. In particular, this study focuses on the changes in cloud radiative effect, cloud fraction, and cloud optical depth with SST anomaly. The major findings are as follows. First, the low-cloud amount (-1.9% to -3.4% K(-1)) and the logarithm of low-cloud optical depth (-0.085 to -0.100 K(-1)) tend to decrease while the net cloud radiative effect (3.86 W m(-2) K(-1)) becomes less negative as SST anomalies increase. These results are broadly consistent with previous observational studies. Second, after the changes in cloud and radiative properties with SST anomaly are separated into dynamic, thermodynamic, and residual components, changes in the dynamic component (taken as the vertical velocity at 700 hPa) have relatively little effect on cloud and radiative properties. However, the estimated inversion strength decreases with increasing SST, accounting for a large portion of the measured decreases in cloud fraction and cloud optical depth. The residual positive change in net cloud radiative effect (1.48W m(-2) K(-1)) and small changes in low-cloud amount (-0.81% 10 0.22% K(-1)) and decrease in the logarithm of optical depth (-0.035 to -0.046 K(-1)) with SST are interpreted as a positive cloud feedback, with cloud optical depth feedback being the dominant contributor. Last, the magnitudes of the residual changes differ greatly among the six low-cloud regions examined in this study, with the largest positive feedbacks (similar to 4 W m(-2) K(-1)) in the southeast and northeast Atlantic regions and a slightly negative feedback (-0.2 W m(-2) K(-1)) in the south-central Pacific region. Because the retrievals of cloud optical depth and/or cloud fraction are difficult in the presence of aerosols, the transport of heavy African continental aerosols may contribute to the large magnitudes of estimated cloud feedback in the two Atlantic regions.
C1 [Eitzen, Zachary A.; Xu, Kuan-Man; Wong, Takmeng] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Eitzen, Zachary A.] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Eitzen, ZA (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM zachary.a.eitzen@nasa.gov
RI Xu, Kuan-Man/B-7557-2013
OI Xu, Kuan-Man/0000-0001-7851-2629
FU NASA EOS; EOS interdisciplinary study program
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 EOS and EOS interdisciplinary study programs managed by Dr. Hal
Maring. The authors thank four anonymous reviewers for their helpful
comments. Helpful discussions with Drs. Norman Loeb, Pat Minnis, Seiji
Kato, and David Doelling are appreciated. The authors thank Prof. Joel
Norris for discussions about the uncertainty analysis. ECMWF-Interim
data were obtained online from http://data.ecmwf.int/data/.
NR 50
TC 17
Z9 17
U1 1
U2 15
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD FEB 15
PY 2011
VL 24
IS 4
BP 1106
EP 1121
DI 10.1175/2010JCLI3670.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 734AD
UT WOS:000288304700008
ER
PT J
AU Slaba, TC
Blattnig, SR
Badavi, FF
Stoffle, NN
Rutledge, RD
Lee, KT
Zapp, EN
Dachev, TP
Tomov, BT
AF Slaba, Tony C.
Blattnig, Steve R.
Badavi, Francis F.
Stoffle, Nicholas N.
Rutledge, Robert D.
Lee, Kerry T.
Zapp, E. Neal
Dachev, Tsvetan P.
Tomov, Borislav T.
TI Statistical validation of HZETRN as a function of vertical cutoff
rigidity using ISS measurements
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE HZETRN; Low Earth Orbit; Space radiation; International Space Station;
Radiation shielding; Transport
ID RADIATION; TRANSPORT; SPECTRA; SHUTTLE; BOARD; MODEL
AB Measurements taken in Low Earth Orbit (LEO) onboard the International Space Station (ISS) and transit vehicles have been extensively used to validate radiation transport models. Primarily, such comparisons were done by integrating measured data over mission or trajectory segments so that individual comparisons to model results could be made. This approach has yielded considerable information but is limited in its ability to rigorously quantify and differentiate specific model errors or uncertainties. Further, as exploration moves beyond LEO and measured data become sparse, the uncertainty estimates derived from these validation cases will no longer be applicable. Recent improvements in the underlying numerical methods used in HZETRN have resulted in significant decreases in code run time. Therefore, the large number of comparisons required to express error as a function of a physical quantity, like cutoff rigidity, are now possible. Validation can be looked at in detail over any portion of a flight trajectory (e.g. minute by minute) such that a statistically significant number of comparisons can be made. This more rigorous approach to code validation will allow the errors caused by uncertainties in the geometry models, environmental models, and nuclear physics models to be differentiated and quantified. It will also give much better guidance for future model development. More importantly, it will allow a quantitative means of extrapolating uncertainties in LEO to free space. In this work, measured data taken onboard the ISS during solar maximum are compared to results obtained with the particle transport code HZETRN. Comparisons are made at a large number (similar to 77,000) of discrete time intervals, allowing error estimates to be given as a function of cutoff rigidity. It is shown that HZETRN systematically underestimates exposure quantities at high cutoff rigidity. The errors are likely associated with increased angular variation in the geomagnetic field near the equator, the lack of pion production in HZETRN, and errors in high energy nuclear physics models, and will be the focus of future work. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Slaba, Tony C.; Blattnig, Steve R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Badavi, Francis F.] Christopher Newport Univ, Newport News, VA 23606 USA.
[Stoffle, Nicholas N.] Lockheed Martin, Houston, TX 77058 USA.
[Rutledge, Robert D.] NOAA Space Weather Predict Ctr, Boulder, CO 80305 USA.
[Lee, Kerry T.; Zapp, E. Neal] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Dachev, Tsvetan P.; Tomov, Borislav T.] Bulgarian Acad Sci, Sofia 1113, Bulgaria.
RP Slaba, TC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM Tony.C.Slaba@nasa.gov
FU NASA [NNX09AR20A]; Advanced Capabilities Division (ACD) under the
Exploration Systems Mission Directorate (ESMD)
FX This research was sponsored by NASA Research grant NNX09AR20A and the
Human Research Program (HRP) in the Advanced Capabilities Division (ACD)
under the Exploration Systems Mission Directorate (ESMD) and performed
by members of the Measurements and Transport Codes project. The authors
would like to thank John Nealy for helpful discussions in this work.
NR 24
TC 15
Z9 15
U1 0
U2 3
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD FEB 15
PY 2011
VL 47
IS 4
BP 600
EP 610
DI 10.1016/j.asr.2010.10.021
PG 11
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 722LG
UT WOS:000287433100005
ER
PT J
AU Norbury, JW
AF Norbury, John W.
TI Perspective on space radiation for space flights in 2020-2040
SO ADVANCES IN SPACE RESEARCH
LA English
DT Review
DE Solar particle events; Solar activity; Galactic cosmic rays; Space
radiation
ID COSMIC-RAY EVENTS; SOLAR-ACTIVITY; SEA SEDIMENTS; SUNS ACTIVITY;
CLIMATE; VARIABILITY; CYCLE; MILLENNIUM; ICE; RECONSTRUCTION
AB The Sun undergoes several well known periodicities in activity, such as the Schwabe 11 year cycle, the Gleissberg 80-90 year cycle, the Suess 200-210 year cycle and the Halstatt 2200-2300 year cycle. In addition, there is evidence that the 20th century levels of solar activity are unusually high. The years 2020-2040 are expected to coincide with increased activity in human space flight beyond low Earth orbit. The solar cycles and the present level of solar activity are reviewed and their activities during the years 2020-2040 are discussed with a perspective on space radiation and the future program of space flight. It is prudent to prepare for continuing levels of high solar activity as well as for the low levels of the current deep minimum, which has corresponded to high galactic cosmic ray flux. Published by Elsevier Ltd. on behalf of COSPAR.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Norbury, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM john.w.norbury@nasa.gov
NR 68
TC 2
Z9 3
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 FEB 15
PY 2011
VL 47
IS 4
BP 611
EP 621
DI 10.1016/j.asr.2010.10.012
PG 11
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 722LG
UT WOS:000287433100006
ER
PT J
AU Song, YT
Colberg, F
AF Song, Y. Tony
Colberg, Frank
TI Deep ocean warming assessed from altimeters, Gravity Recovery and
Climate Experiment, in situ measurements, and a non-Boussinesq ocean
general circulation model
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SEA-LEVEL RISE; BOTTOM PRESSURE; HEAT-CONTENT; SATELLITE ALTIMETRY;
SOUTHERN-OCEAN; GLOBAL OCEAN; GRACE; VARIABILITY; MASS; ABYSSAL
AB Observational surveys have shown significant oceanic bottom water warming, but they are too spatially and temporally sporadic to quantify the deep ocean contribution to the present-day sea level rise (SLR). In this study, altimetry sea surface height (SSH), Gravity Recovery and Climate Experiment (GRACE) ocean mass, and in situ upper ocean (0-700 m) steric height have been assessed for their seasonal variability and trend maps. It is shown that neither the global mean nor the regional trends of altimetry SLR can be explained by the upper ocean steric height plus the GRACE ocean mass. A non-Boussinesq ocean general circulation model (OGCM), allowing the sea level to rise as a direct response to the heat added into the ocean, is then used to diagnose the deep ocean steric height. Constrained by sea surface temperature data and the top of atmosphere (TOA) radiation measurements, the model reproduces the observed upper ocean heat content well. Combining the modeled deep ocean steric height with observational upper ocean data gives the full depth steric height. Adding a GRACE-estimated mass trend, the data-model combination explains not only the altimetry global mean SLR but also its regional trends fairly well. The deep ocean warming is mostly prevalent in the Atlantic and Indian oceans, and along the Antarctic Circumpolar Current, suggesting a strong relation to the oceanic circulation and dynamics. Its comparison with available bottom water measurements shows reasonably good agreement, indicating that deep ocean warming below 700 m might have contributed 1.1 mm/yr to the global mean SLR or one-third of the altimeter-observed rate of 3.11 +/- 0.6 mm/yr over 1993-2008.
C1 [Song, Y. Tony; Colberg, Frank] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Colberg, Frank] CSIRO Marine & Atmospher Res, Aspendale, Vic 3195, Australia.
RP Song, YT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM yuhe.t.song@jpl.nasa.gov
RI Colberg, Frank/F-4360-2014
FU National Aeronautics and Space Administration (NASA)
FX This research is carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration (NASA). Many thanks to C. Y. Kuo
for providing his version of the upper ocean steric height data and S.
G. Purkey and G. C. Johnson for the oceanic bottom water data.
Discussions with V. Zlotnicki, J. Willis, and C. K. Shum are greatly
appreciated.
NR 61
TC 18
Z9 19
U1 3
U2 25
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 FEB 15
PY 2011
VL 116
AR C02020
DI 10.1029/2010JC006601
PG 16
WC Oceanography
SC Oceanography
GA 723QB
UT WOS:000287520800002
ER
PT J
AU De Lannoy, GJM
Ufford, J
Sahoo, AK
Dirmeyer, P
Houser, PR
AF De Lannoy, Gabrielle J. M.
Ufford, Julie
Sahoo, Alok K.
Dirmeyer, Paul
Houser, Paul R.
TI Observed and simulated water and energy budget components at SCAN sites
in the lower Mississippi Basin
SO HYDROLOGICAL PROCESSES
LA English
DT Article
DE water balance; energy balance; SCAN; land surface model; NDVI; MODIS;
actual evapotranspiration; soil moisture
ID SOIL-MOISTURE; UNITED-STATES; RIVER-BASIN; HEAT-FLUX;
EVAPOTRANSPIRATION; MODELS; EVAPORATION; PRECIPITATION; ASSIMILATION;
GRASSLAND
AB Land surface models are typically constrained by one or a few observed variables, while assuming that the internal water and energy partitioning is sensitive to those observed variables and realistic enough to simulate unobserved variables. To verify these assumptions, in situ soil climate analysis network (SCAN) observations in the Lower Mississippi Basin (2002-2008) are analysed to quantify water and energy budget components and they are compared to Community Land Model (CLM3.5) simulations. The local soil texture is identified as a major indicator for water storage characteristics and the Normalized Difference Vegetation Index shows potential as a drought indicator in summer months. Both observations and simulations indicate a regime where, except in some summer months, evapotranspiration controls soil moisture. CLM simulations with different soil texture assignments show discharge sensitivity to soil moisture, but almost no impact on evapotranspiration and other energy balance components. The observed and simulated water budgets show a similar partitioning. However, the SCAN observed water balance does not close because of precipitation measurement errors, unobserved irrigation, lack of specific storage change measurements and errors in the computed actual evapotranspiration. The simulated heat flux partitioning differs from that 'observed', with a larger (resp. smaller) fraction of net radiation being used by latent (resp. sensible) heat flux, and unobserved freeze and thaw events. The comparison between observations and model simulations suggests that a consistent observation collection for multiple variables would be needed to constrain and improve the full set of land surface variable estimates. Copyright (C) 2010 John Wiley & Sons, Ltd.
C1 [Dirmeyer, Paul] Ctr Ocean Land Atmosphere Studies, Calverton, MD 20705 USA.
[De Lannoy, Gabrielle J. M.; Ufford, Julie; Sahoo, Alok K.; Houser, Paul R.] Ctr Res Environm & Water, Calverton, MD 20705 USA.
[De Lannoy, Gabrielle J. M.; Ufford, Julie; Sahoo, Alok K.; Houser, Paul R.] George Mason Univ, Calverton, MD 20705 USA.
[De Lannoy, Gabrielle J. M.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
[Sahoo, Alok K.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
RP De Lannoy, GJM (reprint author), NASA, GSFC, Global Modeling & Assimilat Off, Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Gabrielle.DeLannoy@nasa.gov
RI Dirmeyer, Paul/B-6553-2016; Houser, Paul/J-9515-2013
OI Dirmeyer, Paul/0000-0003-3158-1752; Houser, Paul/0000-0002-2991-0441
NR 54
TC 6
Z9 6
U1 0
U2 10
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0885-6087
EI 1099-1085
J9 HYDROL PROCESS
JI Hydrol. Process.
PD FEB 15
PY 2011
VL 25
IS 4
BP 634
EP 649
DI 10.1002/hyp.7855
PG 16
WC Water Resources
SC Water Resources
GA 721TD
UT WOS:000287377200010
ER
PT J
AU Biancamaria, S
Durand, M
Andreadis, KM
Bates, PD
Boone, A
Mognard, NM
Rodriguez, E
Alsdorf, DE
Lettenmaier, DP
Clark, EA
AF Biancamaria, S.
Durand, M.
Andreadis, K. M.
Bates, P. D.
Boone, A.
Mognard, N. M.
Rodriguez, E.
Alsdorf, D. E.
Lettenmaier, D. P.
Clark, E. A.
TI Assimilation of virtual wide swath altimetry to improve Arctic river
modeling
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE SWOT; Wide swath altimetry; Hydrologic/hydraulic modeling; Data
assimilation; Kalman filter; Kalman smoother; Arctic; Ob River
ID FORECAST ERROR; PRECIPITATION
AB Global surface water variations are still difficult to monitor with current satellite measurements. The future Surface Water and Ocean Topography (SWOT) mission is designed to address this issue. Its main payload will be a wide swath altimeter which will provide maps of water surface elevations between 78 degrees S and 78 degrees N over a 120 km swath. This study aims to combine coupled hydrologic/hydraulic modeling of an Arctic river with virtual SWOT observations using a local ensemble Kalman smoother to characterize river water depth variations. We assumed that modeling errors are only due to uncertainties in atmospheric forcing fields (precipitation and air temperature) and different SWOT orbits were tested. First, we tested orbits that all have a three day repeat period but differ in terms of their spatial coverage of the study reach: these orbits correspond to the first three months of the mission, which will be dedicated to calibration and validation experiments. For these orbits, the mean spatial Root Mean Square Error (RMSE) in modeled channel water depth decreased by between 29% and 79% compared to the modeled RMSE with no assimilation, depending on the spatial coverage. The corresponding mean temporal RMSE decrease was between 54% and 91%. We then tested the nominal orbit with a twenty two day repeat period which will be used during the remaining lifetime of the mission. Unlike the three day repeat orbits, this orbit will observe all continental surfaces (except Antartica and the northern part of Greenland) during one repeat period. The assimilation of SWOT observations computed with this nominal orbit into the hydraulic model leads to a decrease of 59% and 66% in the mean spatial and temporal RMSE in modeled channel water depth, respectively. These results show the huge potential of the future SWOT mission for land surface hydrology, especially at high latitudes which will be very well sampled during one orbit repeat period. Still, further work is needed to reduce current modeling uncertainties and to better characterize SWOT measurement errors. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Biancamaria, S.; Mognard, N. M.] Univ Toulouse, LEGOS, UPS OMP PCA, F-31400 Toulouse, France.
[Biancamaria, S.; Mognard, N. M.] LEGOS, CNES, F-31400 Toulouse, France.
[Biancamaria, S.] LEGOS, CNRS, F-31400 Toulouse, France.
[Durand, M.; Alsdorf, D. E.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
[Durand, M.; Andreadis, K. M.; Alsdorf, D. E.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Bates, P. D.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Boone, A.] Meteo France, CNRS, GAME CNRM, F-31057 Toulouse, France.
[Rodriguez, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Alsdorf, D. E.] Ohio State Univ, Climate Water & Carbon Program, Columbus, OH 43210 USA.
[Lettenmaier, D. P.; Clark, E. A.] Univ Washington, Seattle, WA 98195 USA.
RP Biancamaria, S (reprint author), Univ Toulouse, LEGOS, UPS OMP PCA, 14 Ave Edouard Belin, F-31400 Toulouse, France.
EM sylvain.biancamaria@legos.obs-mip.fr
RI Bates, Paul/C-8026-2012; Durand, Michael/D-2885-2013; lettenmaier,
dennis/F-8780-2011
OI Bates, Paul/0000-0001-9192-9963; lettenmaier, dennis/0000-0003-3317-1327
FU CNES; European Union; NASA; CNES/Noveltis
FX Some authors were funded by the TOSCA SWOT High Resolution Hydrology
project from CNES and the MONARCH-A project from the European Union 7th
Framework Program. Some participants in this project were funded by
NASA's programs in Physical Oceanography and Terrestrial Hydrology. OSU
authors were also funded by their Climate, Water, and Carbon Program.
One of the authors (S. Biancamaria) was supported by a CNES/Noveltis
grant.
NR 29
TC 46
Z9 46
U1 6
U2 35
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 FEB 15
PY 2011
VL 115
IS 2
BP 373
EP 381
DI 10.1016/j.rse.2010.09.008
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 714BS
UT WOS:000286782500010
ER
PT J
AU Sulla-Menashe, D
Friedl, MA
Krankina, ON
Baccini, A
Woodcock, CE
Sibley, A
Sun, GQ
Kharuk, V
Elsakov, V
AF Sulla-Menashe, Damien
Friedl, Mark A.
Krankina, Olga N.
Baccini, Alessandro
Woodcock, Curtis E.
Sibley, Adam
Sun, Guoqing
Kharuk, Viacheslav
Elsakov, Vladimir
TI Hierarchical mapping of Northern Eurasian land cover using MODIS data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Land cover; Classification; MODIS; Decision trees; Biogeography;
Hierarchical classification system
ID REMOTELY-SENSED DATA; ACCURACY ASSESSMENT; CLIMATE-CHANGE; CARBON-CYCLE;
VEGETATION CLASSIFICATION; PRIOR PROBABILITIES; ARCTIC VEGETATION; SNOW
COVER; RESOLUTION; PRODUCTS
AB The Northern Eurasian land mass encompasses a diverse array of land cover types including tundra, boreal forest, wetlands, semi-arid steppe, and agricultural land use. Despite the well-established importance of Northern Eurasia in the global carbon and climate system, the distribution and properties of land cover in this region are not well characterized. To address this knowledge and data gap, a hierarchical mapping approach was developed that encompasses the study area for the Northern Eurasia Earth System Partnership Initiative (NEESPI). The Northern Eurasia Land Cover (NELC) database developed in this study follows the FAO-land Cover Classification System and provides nested groupings of land cover characteristics, with separate layers for land use, wetlands, and tundra. The database implementation is substantially different from other large-scale land cover datasets that provide maps based on a single set of discrete classes. By providing a database consisting of nested maps and complementary layers, the NELC database provides a flexible framework that allows users to tailor maps to suit their needs. The methods used to create the database combine empirically derived climate-vegetation relationships with results from supervised classifications based on Moderate Resolution Imaging Spectroradiometer (MODIS) data. The hierarchical approach provides an effective framework for integrating climate-vegetation relationships with remote sensing-based classifications, and also allows sources of error to be characterized and attributed to specific levels in the hierarchy. The cross-validated accuracy was 73% for the land cover map and 73% and 91% for the agriculture and wetland classifications, respectively. These results support the use of hierarchical classification and climate-vegetation relationships for mapping land cover at continental scales. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Sulla-Menashe, Damien; Friedl, Mark A.; Woodcock, Curtis E.; Sibley, Adam] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Krankina, Olga N.] Oregon State Univ, Coll Forestry, Dept Forest Sci, Corvallis, OR 97331 USA.
[Baccini, Alessandro] Woods Hole Res Ctr, Falmouth, MA 02540 USA.
[Sun, Guoqing] NASA, GSFC, Biospher Sci Branch, Greenbelt, MD 20770 USA.
[Kharuk, Viacheslav] Acad Gorodok Krasnoyarsk, Sukachev Forest Inst, Forest Ecol & Monitoring Branch, Krasnoyarsk 660036, Russia.
[Elsakov, Vladimir] Russian Acad Sci, Inst Biol, Komi Sci Ctr, Syktyvkar 167610, Russia.
RP Sulla-Menashe, D (reprint author), Boston Univ, Dept Geog & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA.
EM dsm@bu.edu
RI Elsakov, Vladimir/P-9630-2015;
OI Sulla-Menashe, Damien/0000-0002-0435-6114
FU NASA [NNG06GF54G, NNX08AE61A]
FX The research was supported by NASA grant numbers NNG06GF54G and
NNX08AE61A. An additional thanks goes to Dr. Bin Tan who was
instrumental in implementing the MODIS classification algorithms, and to
the rest of the NELDA team for helpful input and discussions.
NR 71
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U1 6
U2 40
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 FEB 15
PY 2011
VL 115
IS 2
BP 392
EP 403
DI 10.1016/j.rse.2010.09.010
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 714BS
UT WOS:000286782500012
ER
PT J
AU Spruce, JP
Sader, S
Ryan, RE
Smoot, J
Kuper, P
Ross, K
Prados, D
Russell, J
Gasser, G
McKellip, R
Hargrove, W
AF Spruce, Joseph P.
Sader, Steven
Ryan, Robert E.
Smoot, James
Kuper, Philip
Ross, Kenton
Prados, Donald
Russell, Jeffrey
Gasser, Gerald
McKellip, Rodney
Hargrove, William
TI Assessment of MODIS NDVI time series data products for detecting forest
defoliation by gypsy moth outbreaks
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE MODIS NDVI time series data; Gypsy moth; Regional forest defoliation
detection products; Defoliation classification accuracy; National forest
threat early warning system; Temporal data processing
ID EASTERN-UNITED-STATES; REMOTELY-SENSED DATA; COVER CHANGE; COLOR
COMPOSITES; DISTURBANCES; IMAGERY; WETNESS
AB This paper discusses an assessment of Moderate Resolution Imaging Spectroradiometer (MODIS) time-series data products for detecting forest defoliation from European gypsy moth (Lymantria dispar). This paper describes an effort to aid the United States Department of Agriculture (USDA) Forest Service in developing and assessing MODIS-based gypsy moth defoliation detection products and methods that could be applied in near real time without intensive field survey data collection as a precursor. In our study, MODIS data for 2000-2006 were processed for the mid-Appalachian highland region of the United States. Gypsy moth defoliation maps showing defoliated forests versus non-defoliated areas were produced from temporally filtered and composited MOD02 and MOD13 data using unsupervised classification and image thresholding of maximum value normalized difference vegetation index (NDVI) datasets computed for the defoliation period (June 10-July 27) of 2001 and of the entire time series. These products were validated by comparing stratified random sample locations to relevant Landsat and Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) reference data sets. Composites of 250 m daily MOD02 outperformed 16-day MOD13 data in terms of classifying forest defoliation, showing a lower omission error rate (0.09 versus 0.56), a similar Kappa (0.67 versus 0.79), a comparable commission error rate (0.22 versus 0.14), and higher overall classification agreement (88 versus 79%). Results suggest that temporally processed MODIS time-series data can detect with good agreement to available reference data the extent and location of historical regional gypsy moth defoliation patches of 0.25 km(2) or more for 250-meter products. The temporal processing techniques used in this study enabled effective broad regional, "wall to wall" gypsy moth defoliation detection products for a 6.2 million ha region that were not produced previously with either MODIS or other satellite data. This study provides new, previously unavailable information on the relative agreement of temporally processed, gypsy moth defoliation detection products from MODIS NDVI time series data with respect to higher spatial resolution Landsat and ASTER data. These results also provided needed timely information on the potential of MODIS data for contributing near real time defoliation products to a USDA Forest Service Forest Threat Early Warning System. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Spruce, Joseph P.; Smoot, James; Kuper, Philip; Russell, Jeffrey] Comp Sci Corp, John C Stennis Space Ctr, Stennis Space Ctr, MS USA.
[Spruce, Joseph P.; Ryan, Robert E.; Smoot, James; Kuper, Philip; Prados, Donald] Sci Syst & Applicat Inc, John C Stennis Space Ctr, Stennis Space Ctr, MS USA.
[Sader, Steven] Univ Maine, Orono, ME USA.
[Ryan, Robert E.] Innovat Imaging & Res, John C Stennis Space Ctr, Stennis Space Ctr, MS USA.
[Ross, Kenton] Sci Syst & Applicat Inc, Lanham, MD USA.
[Russell, Jeffrey] USN, Res Lab, John C Stennis Space Ctr, Stennis Space Ctr, MS USA.
[Gasser, Gerald] John C Stennis Space Ctr, Lockheed Martin Mission Serv, Civil Programs, Stennis Space Ctr, MS USA.
[McKellip, Rodney] NASA, John C Stennis Space Ctr, Stennis Space Ctr, MS USA.
[Hargrove, William] US Forest Serv, Eastern Forest Environm Threat Assessment Ctr, Asheville, NC USA.
RP Spruce, JP (reprint author), Comp Sci Corp, John C Stennis Space Ctr, Stennis Space Ctr, MS USA.
EM joseph.p.spruce@nasa.gov
OI Ross, Kenton/0000-0002-6381-5894
FU NASA at the John C. Stennis Space Center, Mississippi [NNS04AB54T]
FX Participation in this research by Science Systems and Applications, Inc.
and Computer Sciences Corporation was supported by NASA at the John C.
Stennis Space Center, Mississippi, under Task Order NNS04AB54T. We thank
Slawomir Blonski and two anonymous reviewers for providing constructive
comments on the manuscript.
NR 53
TC 41
Z9 47
U1 6
U2 37
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 FEB 15
PY 2011
VL 115
IS 2
BP 427
EP 437
DI 10.1016/j.rse.2010.09.013
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 714BS
UT WOS:000286782500015
ER
PT J
AU Wulder, MA
White, JC
Masek, JG
Dwyer, J
Roy, DP
AF Wulder, Michael A.
White, Joanne C.
Masek, Jeffrey G.
Dwyer, John
Roy, David P.
TI Continuity of Landsat observations: Short term considerations
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Landsat; Monitoring; Operational; Research; Continuity; Global; Land
cover; Change detection
ID SPATIAL-RESOLUTION; SATELLITE DATA; FOREST COVER; MODIS; IMAGERY; TM;
CLASSIFICATION; REFLECTANCE; FUSION; PERFORMANCE
AB As of writing in mid-2010, both Landsat-5 and -7 continue to function, with sufficient fuel to enable data collection until the launch of the Landsat Data Continuity Mission (LDCM) scheduled for December of 2012. Failure of one or both of Landsat-5 or -7 may result in a lack of Landsat data for a period of time until the 2012 launch. Although the potential risk of a component failure increases the longer the sensor's design life is exceeded, the possible gap in Landsat data acquisition is reduced with each passing day and the risk of Landsat imagery being unavailable diminishes for all except a handful of applications that are particularly data demanding. Advances in Landsat data compositing and fusion are providing opportunities to address issues associated with Landsat-7 SLC-off imagery and to mitigate a potential acquisition gap through the integration of imagery from different sensors. The latter will likely also provide short-term, regional solutions to application-specific needs for the continuity of Landsat-like observations. Our goal in this communication is not to minimize the community's concerns regarding a gap in Landsat observations, but rather to clarify how the current situation has evolved and provide an up-to-date understanding of the circumstances, implications, and mitigation options related to a potential gap in the Landsat data record. Crown Copyright (C) 2010 Published by Elsevier Inc. All rights reserved.
C1 [Wulder, Michael A.; White, Joanne C.] Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, Victoria, BC V8Z 1M5, Canada.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Dwyer, John] US Geol Survey, Ctr Earth Resources Observat & Sci EROS, Sioux Falls, SD 57198 USA.
[Roy, David P.] S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA.
RP Wulder, MA (reprint author), Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, Victoria, BC V8Z 1M5, Canada.
EM mwulder@nrcan.gc.ca
RI Masek, Jeffrey/D-7673-2012; Wulder, Michael/J-5597-2016;
OI Wulder, Michael/0000-0002-6942-1896; Dwyer, John/0000-0002-8281-0896;
White, Joanne/0000-0003-4674-0373
FU USGS; NASA
FX We gratefully acknowledge USGS and NASA leadership and support of the
Landsat Science Team.
NR 48
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U1 1
U2 22
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 FEB 15
PY 2011
VL 115
IS 2
BP 747
EP 751
DI 10.1016/j.rse.2010.11.002
PG 5
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 714BS
UT WOS:000286782500041
ER
PT J
AU Litvinov, P
Hasekamp, O
Cairns, B
AF Litvinov, Pavel
Hasekamp, Otto
Cairns, Brian
TI Models for surface reflection of radiance and polarized radiance:
Comparison with airborne multi-angle photopolarimetric measurements and
implications for modeling top-of-atmosphere measurements
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Aerosol retrieval over land; Bidirectional reflectance distribution
function (BRDF); Surface total and polarized reflectances; Coupled
atmosphere-surface system; Radiative transfer; Research scanning
polarimeter (RSP)
ID BIDIRECTIONAL REFLECTANCE; AEROSOL PROPERTIES; COHERENT BACKSCATTERING;
SPACEBORNE MEASUREMENTS; LAND SURFACES; RANDOM-MEDIA; RETRIEVAL;
VEGETATION; OCEAN; RADIOMETER
AB In this paper, we investigate the surface-atmosphere radiative interaction in application to the problem of aerosol satellite remote sensing over land. First, we test different models of the Bidirectional Reflectance and Polarization Distribution Function (BRDF and BPDF) for bare soil and vegetation surfaces using multi-angle, multi-spectral photopolarimetric airborne measurements of the Research Scanning Polarimeter (RSP). Then, we investigate the performance of different models of BRDF and BPDF for modeling top-of-atmosphere measurements. We have found that different BRDF models can describe the RSP measurements equally well. However, for soil surfaces, the different BRDF models show a different dependence on illumination geometry (solar zenith and azimuth angles), as well as a different dependence on viewing angle outside the range of RSP measurements. This implies that different models describe the surface-atmosphere interaction differently, leading for soil surfaces to differences in the top-of-atmosphere reflectance up to 4-5%, whereas at surface level the models agree within 2% for RSP illumination and measurement geometry. For vegetation, the different BRDF models show more similar dependence on illumination geometry, meaning that, in general, the differences in top-of-atmosphere reflectances are smaller than the differences in surface total reflectances. For the BPDF. we compare the empirical model of Nadal and Breon (1999) and the model developed by Maignan et al. (2009) with a newly developed model. The latter model compares better with RSP measurements. It was shown that, though all models have essentially different angular profiles at different illumination and viewing geometries, the difference of the top-of-atmosphere degree of linear polarization is less or is of the same order as the degree of linear polarization difference at the surface level taken at RSP illumination and measurement geometry. For the considered models, it can be up to 0.015 but is mostly below 0.005. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Litvinov, Pavel; Hasekamp, Otto] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Cairns, Brian] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Litvinov, P (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
EM P.Litvinov@sron.nl
OI Cairns, Brian/0000-0002-1980-1022
FU Dutch User Support Program (USP) [GO-AO/03]
FX We are grateful to O. Dubovik and K. Knobelspiesse for useful
discussions. We also thank anonymous reviewers for their useful comments
and critical remarks which helped to improve the paper. This research
was supported by the Dutch User Support Program (USP) under project
GO-AO/03.
NR 44
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U1 4
U2 29
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 FEB 15
PY 2011
VL 115
IS 2
BP 781
EP 792
DI 10.1016/j.rse.2010.11.005
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 714BS
UT WOS:000286782500044
ER
PT J
AU Woellert, K
Ehrenfreund, P
Ricco, AJ
Hertzfeld, H
AF Woellert, Kirk
Ehrenfreund, Pascale
Ricco, Antonio J.
Hertzfeld, Henry
TI Cubesats: Cost-effective science and technology platforms for emerging
and developing nations
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Cubesat; Developing countries; Innovation; Capacity building; Space
technology; Nanosatellite
ID SPACE-FLIGHT; AGRICULTURE; VIRULENCE; SATELLITE
AB The development, operation, and analysis of data from cubesats can promote science education and spur technology utilization in emerging and developing nations. This platform offers uniquely low construction and launch costs together with a comparative ubiquity of launch providers; factors that have led more than 80 universities and several emerging nations to develop programs in this field. Their small size and weight enables cubesats to "piggyback" on rocket launches and accompany orbiters travelling to Moon and Mars. It is envisaged that constellations of cubesats will be used for larger science missions. We present a brief history, technology overview, and summary of applications in science and industry for these small satellites. Cubesat technical success stories are offered along with a summary of pitfalls and challenges encountered in both developed and emerging nations. A discussion of economic and public policy issues aims to facilitate the decision-making process for those considering utilization of this unique technology. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Woellert, Kirk; Ehrenfreund, Pascale; Hertzfeld, Henry] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA.
[Ricco, Antonio J.] NASA, Ames Res Ctr, Small Spacecraft Div, Moffett Field, CA 94035 USA.
RP Woellert, K (reprint author), George Washington Univ, Inst Space Policy, 1957 E St NW, Washington, DC 20052 USA.
EM kdwoell@comcast.net
RI Ricco, Antonio/A-5273-2010; Yin, Yimei/G-7749-2012;
OI Ricco, Antonio/0000-0002-2355-4984
FU NASA [NNX09AC08A]
FX K.W. and P.E. acknowledge the support of NASA grant NNX09AC08A. We
gratefully acknowledge helpful discussions with Jordi Puig-Suari, Dino
Lorenzini, Therese Moretto Jorgensen, David Squires, John Hines, and
Bruce Yost.
NR 111
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U1 1
U2 30
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 FEB 15
PY 2011
VL 47
IS 4
BP 663
EP 684
DI 10.1016/j.asr.2010.10.009
PG 22
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 722LG
UT WOS:000287433100012
ER
PT J
AU Lewis, SC
Gagan, MK
Ayliffe, LK
Zhao, JX
Hantoro, WS
Treble, PC
Hellstrom, JC
LeGrande, AN
Kelley, M
Schmidt, GA
Suwargadi, BW
AF Lewis, Sophie C.
Gagan, Michael K.
Ayliffe, Linda K.
Zhao, Jian-xin
Hantoro, Wahyoe S.
Treble, Pauline C.
Hellstrom, John C.
LeGrande, Allegra N.
Kelley, Maxwell
Schmidt, Gavin A.
Suwargadi, Bambang W.
TI High-resolution stalagmite reconstructions of Australian-Indonesian
monsoon rainfall variability during Heinrich stadial 3 and Greenland
interstadial 4
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE speleothem; isotopes; trace elements; Heinrich stadial 3; monsoon;
Intertropical convergence zone (ITCZ)
ID MILLENNIAL-SCALE; LATE PLEISTOCENE; TRACE-ELEMENTS; STABLE-ISOTOPES;
OXYGEN ISOTOPES; SUMMER MONSOON; ASIAN MONSOON; PAST CLIMATE; GISS
MODELE; HULU CAVE
AB Little is known about the possible teleconnections between abrupt climatic changes originating in the North Atlantic and precipitation dynamics in the Australian-Indonesian summer monsoon (AISM) domain. We examine the climatic impacts of Heinrich stadial 3 (HS3) and Greenland interstadials 4 and 3 (GIS4/3) on AISM-associated precipitation through a high-resolution analysis of stable isotope (delta O-18, delta C-13) and trace element (Mg/Ca, P/Ca) ratios in a stalagmite from Liang Luar cave, Flores, Indonesia. Sixteen high precision Th-230 dates indicate that stalagmite LR07-E1 grew rapidly (similar to 0.3-1.0 mm/yr) in two phases between similar to 31.5-30.1 ka and similar to 27.8-25.6 ka, separated by a similar to 2.3 kyr unconformity. Temporally consistent abrupt responses occur in the Flores record during HS3 and GIS4, which are coherent with changes in stalagmite delta O-18 records from China and Brazil. The response of low-latitude precipitation to HS3 cooling and GIS4 warming, as demonstrated by the widely separated sites, comprises three distinct simplified phases: (1) a strong southward migration of the ITCZ during HS3 is associated with a decrease in rainfall at Liang Luar cave and in China, while wetter conditions are reconstructed from Brazil, (2) represents the peak of HS3 impacts and an extended hiatus begins in the Flores record and (3) where suggested dry conditions at Liang Luar throughout GIS4 form part of a coherent north-south anti-phasing in precipitation changes. The reconstructed changes are also broadly consistent with NASA GISS ModelE-R simulations of a Heinrich-like freshwater perturbation in the North Atlantic basin, which produces a southward shift in the ITCZ. The relationship between the palaeoclimate records indicates that atmospheric teleconnections rapidly propagate and synchronise climate change across the hemispheres during periods of abrupt climate change. Our findings augment recent proposals that large-scale atmospheric re-organisations during stadials and interstadials play a key role in driving changes in atmospheric CO2 concentration, air temperature and global climate change. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Lewis, Sophie C.; Gagan, Michael K.; Ayliffe, Linda K.; Treble, Pauline C.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia.
[Zhao, Jian-xin] Univ Queensland, Ctr Microscopy & Microanal, Brisbane, Qld 4072, Australia.
[Hantoro, Wahyoe S.; Suwargadi, Bambang W.] Indonesian Inst Sci, Res & Dev Ctr Geotechnol, Bandung 40135, Indonesia.
[Treble, Pauline C.] Australian Nucl Sci & Technol Org, Lucas Heights, NSW 2234, Australia.
[Hellstrom, John C.] Univ Melbourne, Sch Earth Sci, Parkville, Vic 3010, Australia.
[LeGrande, Allegra N.; Kelley, Maxwell; Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[LeGrande, Allegra N.; Kelley, Maxwell; Schmidt, Gavin A.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
RP Lewis, SC (reprint author), Australian Natl Univ, Res Sch Earth Sci, GPO Box 4, Canberra, ACT 0200, Australia.
EM sophie.lewis@anu.edu.au
RI Ayliffe, Linda/C-3627-2009; Zhao, Jian-xin/A-5938-2008; Hellstrom,
John/B-1770-2008; Schmidt, Gavin/D-4427-2012; LeGrande,
Allegra/D-8920-2012; Lewis, Sophie/H-4968-2011
OI Ayliffe, Linda/0000-0001-7662-5494; Treble, Pauline/0000-0002-1969-8555;
Zhao, Jian-xin/0000-0002-2413-6178; Hellstrom, John/0000-0001-9427-3525;
Schmidt, Gavin/0000-0002-2258-0486; LeGrande,
Allegra/0000-0002-5295-0062; Lewis, Sophie/0000-0001-6416-0634
FU APA/ASS/JAE Scholarships; Paterson Fellowship/ANU Vice-Chancellor;
Australian Research Council [DP0663274]; NSF [ATM 07-53868]
FX We thank H. Scott-Gagan, J. Cali, J. Cowley, S. Eggins and L. Kinsley
for help with isotope and trace element analyses; D. Qu, Y. Feng, G.
Mortimer and M. McCulloch for assistance with the uranium-series
chronology; and N. Anderson, G. Smith, J. Rutledge, R. Drysdale, M.
Griffiths, E. St. Pierre, E. Yulianto and the Indonesian Institute of
Sciences (LIPI) for logistical help and assistance with fieldwork,
carried out under LIPI Research Permit number 2748/SU.3/KS/2007. This
study was funded by APA/ASS/JAE Scholarships and Paterson Fellowship/ANU
Vice-Chancellor travel grants to S.C.L and Australian Research Council
Discovery grant DP0663274 to M.K.G., J.-x. Z. and W. S.H. NSF ATM
07-53868 supports A.N.L and travel for S.C.L We thank RSES and NASA GISS
for institutional support. We gratefully acknowledge the comments of P.
deMenocal and three anonymous reviewers, which greatly improved this
manuscript.
NR 55
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U2 35
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD FEB 15
PY 2011
VL 303
IS 1-2
BP 133
EP 142
DI 10.1016/j.epsl.2010.12.048
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 738JT
UT WOS:000288636800012
ER
PT J
AU Rozas, LP
Minello, TJ
AF Rozas, Lawrence P.
Minello, Thomas J.
TI Variation in penaeid shrimp growth rates along an estuarine salinity
gradient: Implications for managing river diversions
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Farfantepenaeus aztecus; Field experiment; Food addition; Growth
experiments; Litopenaeus setiferus; Restoration
ID JUVENILE BLUE CRABS; CALLINECTES-SAPIDUS RATHBUN; LITOPENAEUS-SETIFERUS;
BROWN SHRIMP; FARFANTEPENAEUS-AZTECUS; SUBTIDAL MACROBENTHOS;
ENVIRONMENTAL-FACTORS; OXYGEN-CONSUMPTION; SOUTH-CAROLINA; HABITAT
CHANGE
AB Freshwater inflows from river diversions may affect nekton populations by altering the salinity and temperature of estuarine waters. To investigate the influence of these environmental variables on the growth and survival rates of brown shrimp Farfantepenaeus aztecus and white shrimp Litopenaeus setiferus, we conducted field experiments in May and September 2007 to expose experimental animals to the range of different combinations of salinity and water temperature that commonly occur in an estuarine environment. Growth rates for shrimp held in mesocosms for approximately 7 days were compared among four locations and three treatments: locations were identified by the dominant marsh vegetation and distance from the Gulf of Mexico (low to high salinity: Intermediate, Brackish, Saline UE=Saline Up Estuary, Saline DE=Saline Down Estuary). At each location, the treatments were replicated four times and included shallow water with additional food, shallow water without food added, and deeper water (an attempt to expose animals to lower temperatures). Our experiments were designed to test the null hypothesis that shrimp growth and survival rates did not differ by location or treatment. Both brown shrimp and white shrimp grew more slowly at the Intermediate than higher salinity locations. Potential prey (benthic infauna) biomass was relatively low at both the Intermediate and Brackish locations in May, and both shrimp species consistently grew faster in mesocosms where food was added. We conclude that reduced growth in low salinity environments is likely due to the combined effects of increased metabolic costs and less food in these areas. River diversions that reduce estuarine salinities over a large portion of available habitat during peak recruitment periods may reduce overall growth rates and shrimp productivity in the affected areas. Published by Elsevier B.V.
C1 [Rozas, Lawrence P.] NOAA, Natl Marine Fisheries Serv, SEFSC, Estuarine Habitats & Coastal Fisheries Ctr, Lafayette, LA 70506 USA.
[Minello, Thomas J.] NOAA, Natl Marine Fisheries Serv, SEFSC, Galveston Lab, Galveston, TX 77551 USA.
RP Rozas, LP (reprint author), NOAA, Natl Marine Fisheries Serv, SEFSC, Estuarine Habitats & Coastal Fisheries Ctr, 646 Cajundome Blvd, Lafayette, LA 70506 USA.
EM lawrence.rozas@noaa.gov
FU Northern Gulf Institute; NOAA Fisheries Service Southeast Fisheries
Science Center
FX This research was conducted through the NOAA Fisheries Service Southeast
Fisheries Science Center by personnel from the Fishery Ecology Branch
(FEB) located at the Galveston Laboratory and the Estuarine Habitats and
Coastal Fisheries Center in Lafayette, Louisiana. The assistance of
everyone in the FEB was essential for the successful completion of this
project. In particular, we thank Merritt Adkins, Jennifer Atchison,
Ronnie Baker, Lauren Flynn, Jim Ditty, Jennifer Doerr, Matt Haverland,
Shawn Hillen, Juan Salas, Zach Smith, and Elizabeth Wilson for helping
to conduct the field experiments and collect and process the samples. We
acknowledge Phil Caldwell for producing Fig. 1 and Matt Kimball for
Figs. 2 and 3. Joy Merino and an anonymous reviewer provided helpful
suggestions that improved the original manuscript. We acknowledge the
Northern Gulf Institute and NOAA Fisheries Service Southeast Fisheries
Science Center for funding this research project. The findings and
conclusions in this report are those of the authors and do not
necessarily represent the views of the NOAA Fisheries Service. [SS]
NR 79
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
EI 1879-1697
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD FEB 15
PY 2011
VL 397
IS 2
BP 196
EP 207
DI 10.1016/j.jembe.2010.12.003
PG 12
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 724BE
UT WOS:000287550300015
ER
PT J
AU Liu, Y
Wang, ZF
Wang, J
Ferrare, RA
Newsom, RK
Welton, EJ
AF Liu, Yang
Wang, Zifeng
Wang, Jun
Ferrare, Richard A.
Newsom, Robert K.
Welton, Ellsworth J.
TI The effect of aerosol vertical profiles on satellite-estimated surface
particle sulfate concentrations
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE MISR; Fractional AOD; SO4; GAM; MPLNET; ARM SGP Raman lidar
ID MATTER COMPONENT CONCENTRATIONS; OPTICAL DEPTH; AIR-POLLUTION;
UNITED-STATES; RAMAN LIDAR; SENSITIVITY; OCEAN
AB The aerosol vertical distribution is an important factor in determining the relationship between satellite retrieved aerosol optical depth (AOD) and ground-level fine particle pollution concentrations. We evaluate how aerosol profiles measured by ground-based lidar and simulated by models can help improve the association between AOD retrieved by the Multi-angle Imaging Spectroradiometer (MISR) and fine particle sulfate (SO4) concentrations using matched data at two lidar sites. At the Goddard Space Flight Center (GSFC) site, both lidar and model aerosol profiles marginally improve the association between SO4 concentrations and MISR fractional AODs, as the correlation coefficient between cross-validation (CV) and observed SO4 concentrations changes from 0.87 for the no-scaling model to 0.88 for models scaled with aerosol vertical profiles. At the GSFC site, a large amount of urban aerosols resides in the well-mixed boundary layer so the column fractional AODs are already excellent indicators of ground-level particle pollution. In contrast, at the Atmospheric Radiation Measurement Program (ARM) site with relatively low aerosol loadings, scaling substantially improves model performance. The correlation coefficient between CV and observed SO4 concentrations is increased from 0.58 for the no-scaling model to 0.76 in the GEOS-Chem scaling model, and the model bias is reduced from 17% to 9%. In summary, despite the inaccuracy due to the coarse horizontal resolution and the challenges of simulating turbulent mixing in the boundary layer, GEOS-Chem simulated aerosol profiles can still improve methods for estimating surface aerosol (504) mass from satellite-based AODs, particularly in rural areas where aerosols in the free troposphere and any long-range transport of aerosols can significantly contribute to the column AOD. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Liu, Yang] Emory Univ, Rollins Sch Publ Hlth, Dept Environm Hlth, Atlanta, GA 30322 USA.
[Wang, Zifeng] Chinese Acad Sci, Inst Remote Sensing Applicat, Beijing, Peoples R China.
[Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA.
[Ferrare, Richard A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Newsom, Robert K.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Liu, Y (reprint author), Emory Univ, Rollins Sch Publ Hlth, Dept Environm Hlth, 1518 Clifton Rd NE, Atlanta, GA 30322 USA.
EM yang.liu@emory.edu
RI Welton, Ellsworth/A-8362-2012; Chem, GEOS/C-5595-2014; Wang,
Jun/A-2977-2008
OI Wang, Jun/0000-0002-7334-0490
FU MISR science team at the Jet Propulsion Laboratory [1363692]; NASA
FX The work of Yang Liu and Zifeng Wang is supported by the MISR science
team at the Jet Propulsion Laboratory led by Dr. David Diner
(subcontract # 1363692). The authors wish to thank Drs. Jeffrey Reid,
John Barnes, and Larry Belcher for their technical support on MPLNET
lidar data. Jun Wang acknowledges the support of NASA Earth Science New
Investigator Program and the computational support provided by the
Holland Computing Center of the University of Nebraska.
NR 25
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U1 4
U2 17
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 FEB 15
PY 2011
VL 115
IS 2
BP 508
EP 513
DI 10.1016/j.rse.2010.09.019
PG 6
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 714BS
UT WOS:000286782500021
ER
PT J
AU Geremia, C
White, PJ
Wallen, RL
Watson, FGR
Treanor, JJ
Borkowski, J
Potter, CS
Crabtree, RL
AF Geremia, Chris
White, P. J.
Wallen, Rick L.
Watson, Fred G. R.
Treanor, John J.
Borkowski, John
Potter, Christopher S.
Crabtree, Robert L.
TI Predicting Bison Migration out of Yellowstone National Park Using
Bayesian Models
SO PLOS ONE
LA English
DT Article
ID POPULATION REGULATION; HERBIVORES; WILDLIFE; MAMMALS; RATES
AB Long distance migrations by ungulate species often surpass the boundaries of preservation areas where conflicts with various publics lead to management actions that can threaten populations. We chose the partially migratory bison ( Bison bison) population in Yellowstone National Park as an example of integrating science into management policies to better conserve migratory ungulates. Approximately 60% of these bison have been exposed to bovine brucellosis and thousands of migrants exiting the park boundary have been culled during the past two decades to reduce the risk of disease transmission to cattle. Data were assimilated using models representing competing hypotheses of bison migration during 1990-2009 in a hierarchal Bayesian framework. Migration differed at the scale of herds, but a single unifying logistic model was useful for predicting migrations by both herds. Migration beyond the northern park boundary was affected by herd size, accumulated snow water equivalent, and aboveground dried biomass. Migration beyond the western park boundary was less influenced by these predictors and process model performance suggested an important control on recent migrations was excluded. Simulations of migrations over the next decade suggest that allowing increased numbers of bison beyond park boundaries during severe climate conditions may be the only means of avoiding episodic, large-scale reductions to the Yellowstone bison population in the foreseeable future. This research is an example of how long distance migration dynamics can be incorporated into improved management policies.
C1 [Geremia, Chris; White, P. J.; Wallen, Rick L.; Treanor, John J.] Natl Pk Serv, Yellowstone Ctr Resources, Yellowstone Natl Pk, WY 82190 USA.
[Geremia, Chris] Colorado State Univ, Nat Resource & Ecol Lab, Ft Collins, CO 80523 USA.
[Watson, Fred G. R.] Calif State Univ Monterey Bay, Watershed Inst, Seaside, CA USA.
[Borkowski, John] Montana State Univ, Dept Math Sci, Bozeman, MT 59717 USA.
[Potter, Christopher S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Crabtree, Robert L.] Yellowstone Ecol Res Ctr, Bozeman, MT USA.
RP Geremia, C (reprint author), Natl Pk Serv, Yellowstone Ctr Resources, Yellowstone Natl Pk, WY 82190 USA.
EM Chris_Geremia@nps.gov
FU National Park Service
FX This research was funded by the National Park Service. The funders had
no role in study design, data collection and analysis, decision to
publish, or preparation of the manuscript.
NR 43
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U1 0
U2 26
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 FEB 14
PY 2011
VL 6
IS 2
AR e16848
DI 10.1371/journal.pone.0016848
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 721PR
UT WOS:000287367600021
PM 21340035
ER
PT J
AU Mckay, CP
AF Mckay, Christopher P.
TI The search for life in our Solar System and the implications for science
and society
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Article
DE life; second genesis; astrobiology; Mars; Europa; Enceladus
ID MARTIAN METEORITE ALH84001; CARBON-DIOXIDE CLOUDS; LIQUID WATER;
SUBSURFACE OCEAN; EARLY MARS; EUROPA; ENCELADUS; TITAN; EARTH;
PERCHLORATE
AB The search for another type of life in the Solar System addresses the fundamental question of life in the Universe. To determine if life forms we discover represent a second genesis, we must find biological material that would allow us to compare that life to the Earth's phylogenetic tree of life. An organism would be alien if, and only if, it did not link to our tree of life. In our Solar System, the worlds of interest for a search for life are Mars, Europa, Enceladus and, for biochemistry based on a liquid other than water, Titan. If we find evidence for a second genesis of life, we will certainly learn from the comparative study of the biochemistry, organismal biology and ecology of the alien life. The discovery of alien life, if alive or revivable, will pose fundamentally new questions in environmental ethics. We should plan our exploration strategy such that we conduct biologically reversible exploration. In the long term we would do well, ethically and scientifically, to strive to support any alien life discovered as part of an overall commitment to enhancing the richness and diversity of life in the Universe.
C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Mckay, CP (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM chris.mckay@nasa.gov
NR 58
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U1 4
U2 56
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-503X
J9 PHILOS T R SOC A
JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci.
PD FEB 13
PY 2011
VL 369
IS 1936
BP 594
EP 606
DI 10.1098/rsta.2010.0247
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 706ML
UT WOS:000286222400008
PM 21220283
ER
PT J
AU Jun, I
Kim, W
Smith, M
Mitrofanov, I
Litvak, M
AF Jun, I.
Kim, W.
Smith, M.
Mitrofanov, I.
Litvak, M.
TI A study of Venus surface elemental composition from 14 MeV neutron
induced gamma ray spectroscopy: Activation analysis
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE Induced radioactivity; Pulsed neutron generator (PNG); Gamma ray
spectrometer (GRS); MCNP
ID EMISSION; MARS
AB The surface elemental composition of Venus can be determined using an artificially pulsed 14 MeV neutron generator (PNG) combined with a gamma ray spectrometer (GRS). The 14 MeV neutrons will interact with the surface materials and generate gamma rays, characteristic of specific elements, whose energy spectrum will be measured by GRS. These characteristic gamma rays are produced mainly through 3 different neutron interaction mechanisms: capture, inelastic, and activation reactions. Each reaction type has a different neutron energy dependency and different time scale for gamma ray production and transport. Certain elements are more easily identified through one reaction type over the others. Thus, careful analysis of the gamma ray spectra during and after the neutron pulse provides a comprehensive understanding of the surface elemental composition. In this paper, we use a well-tested neutron/gamma transport code, called Monte Carlo N-Particles (MCNP), to investigate the measurement capability of a PNG-GRS detection system through the neutron activation reactions. An activation analysis was performed for a representative soil composition of Venus with a notional operational scenario of PNG and GRS. The analysis shows that the proposed instrument concept can identify most of the modeled surface elements at Venus with sufficient accuracy through the activation mode. Specifically, U. Th, K, Si can be measured to within 1%, Fe within 2%, Al within 10%, Ca within 5%, Mg with 15%, Mn with 20%, and Cl within 6%. Although modeled in the analysis, it is shown that the activation mode alone cannot distinguish the S and Ti peaks. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Jun, I.; Kim, W.; Smith, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mitrofanov, I.; Litvak, M.] Space Res Inst, Moscow, Russia.
RP Jun, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM lnsoo.Jun@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 16
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U1 0
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD FEB 11
PY 2011
VL 629
IS 1
BP 140
EP 144
DI 10.1016/j.nima.2010.10.112
PG 5
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 724DK
UT WOS:000287556100022
ER
PT J
AU Dolci, WW
Boldt, MS
Dodson, KE
Pilcher, CB
AF Dolci, Wendy W.
Boldt, Marco S.
Dodson, K. Estelle
Pilcher, Carl B.
TI Leading the Charge to Virtual Meetings
SO SCIENCE
LA English
DT Letter
C1 [Dolci, Wendy W.; Boldt, Marco S.; Dodson, K. Estelle; Pilcher, Carl B.] NASA, Ames Res Ctr, NASA Astrobiol Inst, Moffett Field, CA 94035 USA.
RP Dolci, WW (reprint author), NASA, Ames Res Ctr, NASA Astrobiol Inst, Moffett Field, CA 94035 USA.
EM wendy.w.dolci@nasa.gov
NR 2
TC 3
Z9 3
U1 0
U2 5
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD FEB 11
PY 2011
VL 331
IS 6018
BP 674
EP 674
DI 10.1126/science.331.6018.674-a
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 719LH
UT WOS:000287205700027
PM 21310986
ER
PT J
AU Lyapustin, A
Wang, Y
Laszlo, I
Kahn, R
Korkin, S
Remer, L
Levy, R
Reid, JS
AF Lyapustin, A.
Wang, Y.
Laszlo, I.
Kahn, R.
Korkin, S.
Remer, L.
Levy, R.
Reid, J. S.
TI Multiangle implementation of atmospheric correction (MAIAC): 2. Aerosol
algorithm
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RESOLUTION IMAGING SPECTRORADIOMETER; OPTICAL DEPTH; RETRIEVAL; MODIS;
LAND; VALIDATION; AERONET; PRODUCTS; NETWORK
AB An aerosol component of a new multiangle implementation of atmospheric correction (MAIAC) algorithm is presented. MAIAC is a generic algorithm developed for the Moderate Resolution Imaging Spectroradiometer (MODIS), which performs aerosol retrievals and atmospheric correction over both dark vegetated surfaces and bright deserts based on a time series analysis and image-based processing. The MAIAC look-up tables explicitly include surface bidirectional reflectance. The aerosol algorithm derives the spectral regression coefficient (SRC) relating surface bidirectional reflectance in the blue (0.47 mu m) and shortwave infrared (2.1 mu m) bands; this quantity is prescribed in the MODIS operational Dark Target algorithm based on a parameterized formula. The MAIAC aerosol products include aerosol optical thickness and a fine-mode fraction at resolution of 1 km. This high resolution, required in many applications such as air quality, brings new information about aerosol sources and, potentially, their strength. AERONET validation shows that the MAIAC and MOD04 algorithms have similar accuracy over dark and vegetated surfaces and that MAIAC generally improves accuracy over brighter surfaces due to the SRC retrieval and explicit bidirectional reflectance factor characterization, as demonstrated for several U. S. West Coast AERONET sites. Due to its generic nature and developed angular correction, MAIAC performs aerosol retrievals over bright deserts, as demonstrated for the Solar Village Aerosol Robotic Network (AERONET) site in Saudi Arabia.
C1 [Lyapustin, A.; Kahn, R.; Remer, L.] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Laszlo, I.] NOAA, NESDIS, STAR, Camp Springs, MD 20746 USA.
[Levy, R.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Reid, J. S.] USN, Aerosol & Radiat Sect, Marine Meteorol Div, Res Lab, Monterey, CA 93943 USA.
[Lyapustin, A.; Wang, Y.; Korkin, S.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Lyapustin, A (reprint author), NASA, Atmospheres Lab, Goddard Space Flight Ctr, MC 614-4, Greenbelt, MD 20771 USA.
EM alexei.i.lyapustin@nasa.gov
RI Laszlo, Istvan/F-5603-2010; Levy, Robert/M-7764-2013; Reid,
Jeffrey/B-7633-2014; Lyapustin, Alexei/H-9924-2014; Kahn,
Ralph/D-5371-2012
OI Laszlo, Istvan/0000-0002-5747-9708; Levy, Robert/0000-0002-8933-5303;
Reid, Jeffrey/0000-0002-5147-7955; Lyapustin,
Alexei/0000-0003-1105-5739; Kahn, Ralph/0000-0002-5234-6359
FU NASA; NOAA GOES-R; EOS-MISR; Office of Naval Research [322]
FX The research of A. Lyapustin, Y. Wang, and S. Korkin was funded by the
NASA Terrestrial Ecology Program (D. Wickland) and NASA Applications
Program (L. Friedl and B. Doorn) and in part by the NOAA GOES-R program
(M. Goldberg). The work of R. Kahn is supported in part by NASA's
Climate and Radiation Research and Analysis Program, under H. Maring,
NASA's Atmospheric Composition Program, and the EOS-MISR Project. The
contribution of R. Levy and L. Remer to this work is supported by the
NASA Radiation Science Program (H. Maring). J. Reid's contribution was
supported by the Office of Naval Research Code 322. This work strongly
benefited from multiple discussions with our AERONET and NASA GSFC
colleagues (A. Marshak, B. Holben, A. Sinuyk, A. Smirnov, I. Slutsker,
and M. Sorokin). We are grateful to AERONET team for use of their data.
NR 36
TC 41
Z9 42
U1 3
U2 35
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 FEB 11
PY 2011
VL 116
AR D03211
DI 10.1029/2010JD014986
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 721AA
UT WOS:000287322600005
ER
PT J
AU Lyapustin, A
Martonchik, J
Wang, YJ
Laszlo, I
Korkin, S
AF Lyapustin, Alexei
Martonchik, John
Wang, Yujie
Laszlo, Istvan
Korkin, Sergey
TI Multiangle implementation of atmospheric correction (MAIAC): 1.
Radiative transfer basis and look-up tables
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RETRIEVAL; ALBEDO; ABSORPTION; SURFACE; BRDF
AB This paper describes a radiative transfer basis of the algorithm MAIAC which performs simultaneous retrievals of atmospheric aerosol and bidirectional surface reflectance from the Moderate Resolution Imaging Spectroradiometer (MODIS). The retrievals are based on an accurate semianalytical solution for the top-of-atmosphere reflectance expressed as an explicit function of three parameters of the Ross-Thick Li-Sparse model of surface bidirectional reflectance. This solution depends on certain functions of atmospheric properties and geometry which are precomputed in the look-up table (LUT). This paper further considers correction of the LUT functions for variations of surface pressure/height and of atmospheric water vapor, which is a common task in the operational remote sensing. It introduces a new analytical method for the water vapor correction of the multiple-scattering path radiance. It also summarizes the few basic principles that provide a high efficiency and accuracy of the LUT-based radiative transfer for the aerosol/surface retrievals and optimize the size of LUT. For example, the single-scattering path radiance is calculated analytically for a given surface pressure and atmospheric water vapor. The same is true for the direct surface-reflected radiance, which along with the single-scattering path radiance largely defines the angular dependence of measurements. For these calculations, the aerosol phase functions and kernels of the surface bidirectional reflectance model are precalculated at a high angular resolution. The other radiative transfer functions depend rather smoothly on angles because of multiple scattering and can be calculated at coarser angular resolution to reduce the LUT size. At the same time, this resolution should be high enough to use the nearest neighbor geometry angles to avoid costly three-dimensional interpolation. The pressure correction is implemented via linear interpolation between two LUTs computed for the standard and reduced pressure levels. A linear mixture and a modified linear mixture methods are used to represent different aerosol types in the aerosol/surface retrievals from several base models of the fine and coarse aerosol fractions. In summary, the developed LUT algorithm allows fast high-accuracy simulations of the outgoing radiance with full variability of the atmospheric and surface bidirectional reflectance properties for the aerosol/surface remote sensing.
C1 [Lyapustin, Alexei; Wang, Yujie; Korkin, Sergey] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Laszlo, Istvan] NOAA, NESDIS, STAR, Camp Springs, MD 20746 USA.
[Martonchik, John] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
[Lyapustin, Alexei; Wang, Yujie; Korkin, Sergey] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Lyapustin, A (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 614-4, Greenbelt, MD 20771 USA.
EM alexei.i.lyapustin@nasa.gov
RI Laszlo, Istvan/F-5603-2010; Lyapustin, Alexei/H-9924-2014
OI Laszlo, Istvan/0000-0002-5747-9708; Lyapustin,
Alexei/0000-0003-1105-5739
FU NASA EOS Science; NASA; NOAA GOES-R
FX The work of Alexei Lyapustin, Yujie Wang, and Sergey Korkin was
supported by the NASA EOS Science funding (D. Wickland) and in part by
the NASA Applications Program (L. Friedl and B. Doorn) and NOAA GOES-R
grant (M. Goldberg).
NR 25
TC 67
Z9 67
U1 2
U2 24
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 FEB 11
PY 2011
VL 116
AR D03210
DI 10.1029/2010JD014985
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 721AA
UT WOS:000287322600004
ER
PT J
AU Tavani, M
Bulgarelli, A
Vittorini, V
Pellizzoni, A
Striani, E
Caraveo, P
Weisskopf, MC
Tennant, A
Pucella, G
Trois, A
Costa, E
Evangelista, Y
Pittori, C
Verrecchia, F
Del Monte, E
Campana, R
Pilia, M
De Luca, A
Donnarumma, I
Horns, D
Ferrigno, C
Heinke, CO
Trifoglio, M
Gianotti, F
Vercellone, S
Argan, A
Barbiellini, G
Cattaneo, PW
Chen, AW
Contessi, T
D'Ammando, F
DeParis, G
Di Cocco, G
Di Persio, G
Feroci, M
Ferrari, A
Galli, M
Giuliani, A
Giusti, M
Labanti, C
Lapshov, I
Lazzarotto, F
Lipari, P
Longo, F
Fuschino, F
Marisaldi, M
Mereghetti, S
Morelli, E
Moretti, E
Morselli, A
Pacciani, L
Perotti, F
Piano, G
Picozza, P
Prest, M
Rapisarda, M
Rappoldi, A
Rubini, A
Sabatini, S
Soffitta, P
Vallazza, E
Zambra, A
Zanello, D
Lucarelli, F
Santolamazza, P
Giommi, P
Salotti, L
Bignami, GF
AF Tavani, M.
Bulgarelli, A.
Vittorini, V.
Pellizzoni, A.
Striani, E.
Caraveo, P.
Weisskopf, M. C.
Tennant, A.
Pucella, G.
Trois, A.
Costa, E.
Evangelista, Y.
Pittori, C.
Verrecchia, F.
Del Monte, E.
Campana, R.
Pilia, M.
De Luca, A.
Donnarumma, I.
Horns, D.
Ferrigno, C.
Heinke, C. O.
Trifoglio, M.
Gianotti, F.
Vercellone, S.
Argan, A.
Barbiellini, G.
Cattaneo, P. W.
Chen, A. W.
Contessi, T.
D'Ammando, F.
DeParis, G.
Di Cocco, G.
Di Persio, G.
Feroci, M.
Ferrari, A.
Galli, M.
Giuliani, A.
Giusti, M.
Labanti, C.
Lapshov, I.
Lazzarotto, F.
Lipari, P.
Longo, F.
Fuschino, F.
Marisaldi, M.
Mereghetti, S.
Morelli, E.
Moretti, E.
Morselli, A.
Pacciani, L.
Perotti, F.
Piano, G.
Picozza, P.
Prest, M.
Rapisarda, M.
Rappoldi, A.
Rubini, A.
Sabatini, S.
Soffitta, P.
Vallazza, E.
Zambra, A.
Zanello, D.
Lucarelli, F.
Santolamazza, P.
Giommi, P.
Salotti, L.
Bignami, G. F.
TI Discovery of Powerful Gamma-Ray Flares from the Crab Nebula
SO SCIENCE
LA English
DT Article
ID SYNCHROTRON NEBULA; HIGH-ENERGY; TELESCOPE; PULSARS; EMISSION; SPECTRUM;
SHOCKS; WISPS
AB The well-known Crab Nebula is at the center of the SN1054 supernova remnant. It consists of a rotationally powered pulsar interacting with a surrounding nebula through a relativistic particle wind. The emissions originating from the pulsar and nebula have been considered to be essentially stable. Here, we report the detection of strong gamma-ray (100 mega-electron volts to 10 giga-electron volts) flares observed by the AGILE satellite in September 2010 and October 2007. In both cases, the total gamma-ray flux increased by a factor of three compared with the non-flaring flux. The flare luminosity and short time scale favor an origin near the pulsar, and we discuss Chandra Observatory x-ray and Hubble Space Telescope optical follow-up observations of the nebula. Our observations challenge standard models of nebular emission and require power-law acceleration by shock-driven plasma wave turbulence within an approximately 1-day time scale.
C1 [Tavani, M.; Vittorini, V.; Trois, A.; Costa, E.; Evangelista, Y.; Del Monte, E.; Campana, R.; Donnarumma, I.; Argan, A.; DeParis, G.; Di Persio, G.; Feroci, M.; Giusti, M.; Lazzarotto, F.; Pacciani, L.; Piano, G.; Picozza, P.; Rubini, A.; Sabatini, S.; Soffitta, P.] Ist Astrofis Spaziale & Fis Cosm INAF IASF Roma, Ist Nazl Astrofis, I-00133 Rome, Italy.
[Tavani, M.; Striani, E.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Tavani, M.; Barbiellini, G.; Chen, A. W.; Ferrari, A.; Giusti, M.; Zambra, A.] CIFS, I-10133 Turin, Italy.
[Tavani, M.; Striani, E.; Morselli, A.; Piano, G.; Picozza, P.; Sabatini, S.] Ist Nazl Fis Nucl Roma Tor Vergata, I-00133 Rome, Italy.
[Bulgarelli, A.; Trifoglio, M.; Gianotti, F.; Di Cocco, G.; Labanti, C.; Fuschino, F.; Marisaldi, M.; Morelli, E.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Pucella, G.; Rapisarda, M.] Ente Nuove Tecnol Energia & Ambiente Frascati, I-00044 Frascati, RM, Italy.
[Caraveo, P.; De Luca, A.; Chen, A. W.; Contessi, T.; Giuliani, A.; Mereghetti, S.; Perotti, F.; Zambra, A.] INAF IASF Milano, I-20133 Milan, Italy.
[Barbiellini, G.; Longo, F.; Moretti, E.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.; Moretti, E.; Vallazza, E.] Ist Nazl Fis Nucl, I-34012 Trieste, Italy.
[Cattaneo, P. W.; Rappoldi, A.] Ist Nazl Fis Nucl, I-27100 Pavia, Italy.
[Ferrari, A.] Univ Turin, Dipartimento Fis Gen, I-10125 Turin, Italy.
[Galli, M.] ENEA Bologna, I-40128 Bologna, Italy.
[Lapshov, I.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
[Lipari, P.; Zanello, D.] INFN Roma 1, I-00185 Rome, Italy.
[Lipari, P.; Zanello, D.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Pellizzoni, A.; Pilia, M.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy.
[Pilia, M.; Prest, M.] Univ Insubria, Dipartimento Fis, I-22100 Como, Italy.
[Vercellone, S.; D'Ammando, F.] INAF IASF Palermo, I-90146 Palermo, Italy.
[Pittori, C.; Verrecchia, F.; Lucarelli, F.; Santolamazza, P.; Giommi, P.] European Space Agcy, Earth Observat Ctr ESRIN, Sci Data Ctr, ASI, I-00044 Frascati, Italy.
[Salotti, L.] ASI, Rome, Italy.
[Weisskopf, M. C.; Tennant, A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Horns, D.] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany.
[Ferrigno, C.] Univ Geneva, Integral Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Heinke, C. O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[De Luca, A.; Bignami, G. F.] IUSS, I-27100 Pavia, Italy.
RP Tavani, M (reprint author), Ist Astrofis Spaziale & Fis Cosm INAF IASF Roma, Ist Nazl Astrofis, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
EM pi.agile@iasf-roma.inaf.it
RI Horns, Dieter/C-9727-2011; ferrigno, cassio/D-8230-2012; Morselli,
Aldo/G-6769-2011; Lazzarotto, Francesco/J-4670-2012; Campana,
Riccardo/F-5272-2015; Trifoglio, Massimo/F-5302-2015; Pittori,
Carlotta/C-7710-2016;
OI Tavani, Marco/0000-0003-2893-1459; Lucarelli,
Fabrizio/0000-0002-6311-764X; Verrecchia, Francesco/0000-0003-3455-5082;
Gianotti, Fulvio/0000-0003-4666-119X; Lazzarotto,
Francesco/0000-0003-4871-4072; Costa, Enrico/0000-0003-4925-8523;
Donnarumma, Immacolata/0000-0002-4700-4549; Sabatini,
Sabina/0000-0003-2076-5767; Vercellone, Stefano/0000-0003-1163-1396;
MEREGHETTI, SANDRO/0000-0003-3259-7801; De Luca,
Andrea/0000-0001-6739-687X; Heinke, Craig/0000-0003-3944-6109; Pacciani,
Luigi/0000-0001-6897-5996; giommi, paolo/0000-0002-2265-5003; trois,
alessio/0000-0002-3180-6002; Marisaldi, Martino/0000-0002-4000-3789;
Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Labanti,
Claudio/0000-0002-5086-3619; Feroci, Marco/0000-0002-7617-3421;
Soffitta, Paolo/0000-0002-7781-4104; Picozza,
Piergiorgio/0000-0002-7986-3321; Fuschino, Fabio/0000-0003-2139-3299;
Caraveo, Patrizia/0000-0003-2478-8018; PREST,
MICHELA/0000-0003-3161-4454; galli, marcello/0000-0002-9135-3228;
Cattaneo, Paolo Walter/0000-0001-6877-6882; Morselli,
Aldo/0000-0002-7704-9553; Campana, Riccardo/0000-0002-4794-5453;
Trifoglio, Massimo/0000-0002-2505-3630; Pittori,
Carlotta/0000-0001-6661-9779; Vallazza, Erik Silvio/0000-0002-7465-7430;
Bignami, Giovanni/0000-0001-9582-2450; Bulgarelli,
Andrea/0000-0001-6347-0649
FU ASI [I/089/06/2]
FX We thank the Chandra Observatory Director H. Tananbaum; HST director M.
Mountain; N. Gehrels; and the Swift team for their prompt response in
carrying out the observations reported in this paper. Research partially
supported by ASI grant I/089/06/2.
NR 40
TC 155
Z9 157
U1 1
U2 20
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD FEB 11
PY 2011
VL 331
IS 6018
BP 736
EP 739
DI 10.1126/science.1200083
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 719LH
UT WOS:000287205700061
PM 21212318
ER
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Allafort, A
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bouvier, A
Brandt, TJ
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Cannon, A
Caraveo, PA
Casandjian, JM
Celik, O
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Costamante, L
Cutini, S
D'Ammando, F
Dermer, CD
de Angelis, A
de Luca, A
de Palma, F
Digel, SW
Silva, EDE
Drell, PS
Drlica-Wagner, A
Dubois, R
Dumora, D
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Frailis, M
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grondin, MH
Grove, JE
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashi, K
Hayashida, M
Hays, E
Horan, D
Itoh, R
Johannesson, G
Johnson, AS
Johnson, TJ
Khangulyan, D
Kamae, T
Katagiri, H
Kataoka, J
Kerr, M
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lee, SH
Lemoine-Goumard, M
Longo, F
Loparco, F
Lubrano, P
Madejski, GM
Makeev, A
Marelli, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Naumann-Godo, M
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Ormes, JF
Ozaki, M
Paneque, D
Parent, D
Pelassa, V
Pepe, M
Pesce-Rollins, M
Pierbattista, M
Piron, F
Porter, TA
Raino, S
Rando, R
Ray, PS
Razzano, M
Reimer, A
Reimer, O
Reposeur, T
Ritz, S
Romani, RW
Sadrozinski, HFW
Sanchez, D
Parkinson, PMS
Scargle, JD
Schalk, TL
Sgro, C
Siskind, EJ
Smith, PD
Spandre, G
Spinelli, P
Strickman, MS
Suson, DJ
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JB
Thompson, DJ
Tibaldo, L
Torres, DF
Tosti, G
Tramacere, A
Troja, E
Uchiyama, Y
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Wang, P
Wood, KS
Yang, Z
Ziegler, M
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Allafort, A.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bouvier, A.
Brandt, T. J.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Cannon, A.
Caraveo, P. A.
Casandjian, J. M.
Celik, O.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Costamante, L.
Cutini, S.
D'Ammando, F.
Dermer, C. D.
de Angelis, A.
de Luca, A.
de Palma, F.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Dubois, R.
Dumora, D.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Frailis, M.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grondin, M. -H.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashi, K.
Hayashida, M.
Hays, E.
Horan, D.
Itoh, R.
Johannesson, G.
Johnson, A. S.
Johnson, T. J.
Khangulyan, D.
Kamae, T.
Katagiri, H.
Kataoka, J.
Kerr, M.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lee, S. -H.
Lemoine-Goumard, M.
Longo, F.
Loparco, F.
Lubrano, P.
Madejski, G. M.
Makeev, A.
Marelli, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Moiseev, A. A.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakamori, T.
Naumann-Godo, M.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Parent, D.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Ray, P. S.
Razzano, M.
Reimer, A.
Reimer, O.
Reposeur, T.
Ritz, S.
Romani, R. W.
Sadrozinski, H. F. -W.
Sanchez, D.
Parkinson, P. M. Saz
Scargle, J. D.
Schalk, T. L.
Sgro, C.
Siskind, E. J.
Smith, P. D.
Spandre, G.
Spinelli, P.
Strickman, M. S.
Suson, D. J.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Tramacere, A.
Troja, E.
Uchiyama, Y.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Wang, P.
Wood, K. S.
Yang, Z.
Ziegler, M.
TI Gamma-Ray Flares from the Crab Nebula
SO SCIENCE
LA English
DT Article
ID PULSAR WIND NEBULAE; PARTICLE-ACCELERATION; HIGH-ENERGY; SYNCHROTRON
NEBULA; INVERSE COMPTON; EMISSION; TELESCOPE; POLARIZATION; RADIATION;
SPECTRUM
AB A young and energetic pulsar powers the well-known Crab Nebula. Here, we describe two separate gamma-ray (photon energy greater than 100 mega-electron volts) flares from this source detected by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. The first flare occurred in February 2009 and lasted approximately 16 days. The second flare was detected in September 2010 and lasted approximately 4 days. During these outbursts, the gamma-ray flux from the nebula increased by factors of four and six, respectively. The brevity of the flares implies that the gamma rays were emitted via synchrotron radiation from peta-electron-volt (10(15) electron volts) electrons in a region smaller than 1.4 x 10(-2) parsecs. These are the highest-energy particles that can be associated with a discrete astronomical source, and they pose challenges to particle acceleration theory.
C1 [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Wang, P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Abdo, A. A.; Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Abdo, A. A.; Cheung, C. C.] USN, Res Lab, Washington, DC 20375 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.; Tibaldo, L.] Univ Paris Diderot, CEA Saclay, Inst Res Fundamental Laws Universe, CNRS,CEA,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bonamente, E.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brandt, T. J.; Knoedlseder, J.] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Brandt, T. J.; Smith, P. D.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.; Horan, D.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] CSIC, IEEC, Inst Ciencies Espai, Barcelona 08193, Spain.
[Cannon, A.; Celik, O.; Ferrara, E. C.; Gehrels, N.; Harding, A. K.; Hays, E.; Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.; Thompson, D. J.; Troja, E.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cannon, A.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Caraveo, P. A.; Marelli, M.] Ist Astrofis Spaziale & Fis Cosm, Ist Nazl Astrofis, I-20133 Milan, Italy.
[Celik, O.; Moiseev, A. A.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA.
[Celik, O.; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, O.; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Cohen-Tanugi, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France.
[Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy.
[D'Ammando, F.] INAF IASF, I-00133 Rome, Italy.
[Dermer, C. D.; Grove, J. E.; Ray, P. S.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[de Luca, A.] IUSS, I-27100 Pavia, Italy.
[Dumora, D.; Grondin, M. -H.; Lemoine-Goumard, M.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Itoh, R.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Johnson, T. J.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Kerr, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Khangulyan, D.; Okumura, A.; Ozaki, M.; Takahashi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Siskind, E. J.] NYCB Real Time Comp, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tramacere, A.; Vianello, G.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
RP Blandford, RD (reprint author), Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM rdb3@stanford.edu; buehler@stanford.edu; funk@slac.stanford.edu
RI Hays, Elizabeth/D-3257-2012; Funk, Stefan/B-7629-2015; Loparco,
Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano,
Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Saz
Parkinson, Pablo Miguel/I-7980-2013; Ozaki, Masanobu/K-1165-2013; Rando,
Riccardo/M-7179-2013; Thompson, David/D-2939-2012; Harding,
Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; McEnery,
Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano,
pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss,
Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer,
Olaf/A-3117-2013; Tosti, Gino/E-9976-2013
OI Baldini, Luca/0000-0002-9785-7726; Ray, Paul/0000-0002-5297-5278;
Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577;
Pesce-Rollins, Melissa/0000-0003-1790-8018; De Luca,
Andrea/0000-0001-6739-687X; Giroletti, Marcello/0000-0002-8657-8852;
Cutini, Sara/0000-0002-1271-2924; Gasparrini, Dario/0000-0002-5064-9495;
Tramacere, Andrea/0000-0002-8186-3793; Funk, Stefan/0000-0002-2012-0080;
Loparco, Francesco/0000-0002-1173-5673; Johannesson,
Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395;
Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario
/0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; De Angelis,
Alessandro/0000-0002-3288-2517; Frailis, Marco/0000-0002-7400-2135;
Caraveo, Patrizia/0000-0003-2478-8018; Sgro',
Carmelo/0000-0001-5676-6214; Thompson, David/0000-0001-5217-9135;
lubrano, pasquale/0000-0003-0221-4806; Morselli,
Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer,
Olaf/0000-0001-6953-1385;
FU NASA; U.S. Department of Energy in the United States; CEA/IRFU;
IN2P3/CNRS in France; ASI; INFN in Italy; Ministry of Education,
Culture, Sports, Science and Technology, High Energy Accelerator
Research Organization (KEK); JAXA in Japan; K.A. Wallenberg Foundation;
Swedish Research Council; National Space Board in Sweden; International
Doctorate on Astroparticle Physics
FX The Fermi LAT Collaboration acknowledges support from a number of
agencies and institutes for both development and the operation of the
LAT as well as scientific data analysis. These include NASA and the U.S.
Department of Energy in the United States; CEA/IRFU and IN2P3/CNRS in
France; ASI and INFN in Italy; the Ministry of Education, Culture,
Sports, Science and Technology, High Energy Accelerator Research
Organization (KEK), and JAXA in Japan; and the K.A. Wallenberg
Foundation, the Swedish Research Council, and the National Space Board
in Sweden. Additional support from INAF in Italy and CNES in France for
science analysis during the operations phase is also gratefully
acknowledged. L.T. was partially supported by the International
Doctorate on Astroparticle Physics program.
NR 39
TC 160
Z9 161
U1 0
U2 15
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 FEB 11
PY 2011
VL 331
IS 6018
BP 739
EP 742
DI 10.1126/science.1199705
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 719LH
UT WOS:000287205700062
PM 21212321
ER
PT J
AU Ahmad, Z
Franz, BA
McClain, CR
Kwiatkowska, EJ
Werdell, J
Shettle, EP
Holben, BN
AF Ahmad, Ziauddin
Franz, Bryan A.
McClain, Charles R.
Kwiatkowska, Ewa J.
Werdell, Jeremy
Shettle, Eric P.
Holben, Brent N.
TI New aerosol models for the retrieval of aerosol optical thickness and
normalized water-leaving radiances from the SeaWiFS and MODIS sensors
over coastal regions and open oceans: publisher's note (vol 49, pg 4550,
2010)
SO APPLIED OPTICS
LA English
DT Correction
C1 [Ahmad, Ziauddin; Franz, Bryan A.; McClain, Charles R.; Kwiatkowska, Ewa J.; Werdell, Jeremy; Holben, Brent N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ahmad, Ziauddin] Sci & Data Syst Inc, Silver Spring, MD 20906 USA.
[Kwiatkowska, Ewa J.] Sci Applicat Int Corp, San Diego, CA 92121 USA.
[Werdell, Jeremy] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Shettle, Eric P.] USN, Res Lab, Washington, DC 20375 USA.
RP Ahmad, Z (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Ziauddin.Ahmad@nasa.gov
RI Franz, Bryan/D-6284-2012; Werdell, Jeremy/D-8265-2012
OI Franz, Bryan/0000-0003-0293-2082;
NR 2
TC 1
Z9 1
U1 1
U2 7
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 FEB 10
PY 2011
VL 50
IS 5
BP 626
EP 626
DI 10.1364/AO.50.000626
PG 1
WC Optics
SC Optics
GA 724KC
UT WOS:000287573800003
ER
PT J
AU Sengupta, A
Kulleck, J
Van Norman, J
Mehta, M
AF Sengupta, Anita
Kulleck, James
Van Norman, John
Mehta, Manish
TI Thermal coating erosion in a simulated Martian landing environment
SO WEAR
LA English
DT Article
DE Thermal paint; Coating erosion; Particulate erosion; Plume/ground
interaction
ID SOLID PARTICLE EROSION; COMPOSITES; BEHAVIOR
AB An experimental and computational research program was implemented to quantify the thermal coating erosion that results from supersonic jets impinging on the surface of Mars during landing. Soil entrainment and acceleration in the impinging plume-flows result in high velocity particulate flux that can cause degradation of space-use thermal coatings. Computational fluid dynamics in conjunction with particle tracking simulations were used to determine the range of impact velocities expected during landing. The landing environment was simulated in a subscale particle erosion laboratory experiment with test coupons subjected to representative Martian soil media flux. Direct measurement of Mars rover white paint erosion has been obtained for a range of silica particle sizes (5-300 mu m), impact velocities from 130 to 265 m/s, impingement angles from 30 to 90 degrees, and mass loading of 10-240 mg/cm(2). The post-erosion microstructure, absorptivity, and emissivity of the coating were also measured. (C) 2010 Published by Elsevier B.V.
C1 [Sengupta, Anita; Kulleck, James] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Van Norman, John] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Mehta, Manish] Univ Michigan, Ann Arbor, MI 48109 USA.
RP Sengupta, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 301-365, Pasadena, CA 91109 USA.
EM Anita.Sengupta@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 28
TC 2
Z9 3
U1 2
U2 5
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0043-1648
J9 WEAR
JI Wear
PD FEB 10
PY 2011
VL 270
IS 5-6
BP 335
EP 343
DI 10.1016/j.wear.2010.09.013
PG 9
WC Engineering, Mechanical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 728VP
UT WOS:000287902900001
ER
PT J
AU Colbert, JW
Scarlata, C
Teplitz, H
Francis, P
Palunas, P
Williger, GM
Woodgate, B
AF Colbert, James W.
Scarlata, Claudia
Teplitz, Harry
Francis, Paul
Palunas, Povilas
Williger, Gerard M.
Woodgate, Bruce
TI POLYCYCLIC AROMATIC HYDROCARBON EMISSION WITHIN Ly alpha BLOBS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; infrared: galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; STAR-FORMING
GALAXIES; ACTIVE GALACTIC NUCLEI; PROTO-CLUSTER REGION; HIGH-REDSHIFT;
SUBMILLIMETER GALAXIES; MIDINFRARED SPECTROSCOPY; LUMINOUS GALAXIES;
COLD ACCRETION
AB We present Spitzer observations of Ly alpha blobs (LABs) at z = 2.38-3.09. The mid-infrared ratios (4.5 mu m/8 mu m and 8 mu m/24 mu m) indicate that similar to 60% of LAB infrared counterparts are cool, consistent with their infrared output being dominated by star formation and not active galactic nuclei (AGNs). The rest have a substantial hot dust component that one would expect from an AGN or an extreme starburst. Comparing the mid-infrared to submillimeter fluxes (similar to 850 mu m or rest-frame far-infrared) also indicates that a large percentage (similar to 2/3) of the LAB counterparts have total bolometric energy output dominated by star formation, although the number of sources with submillimeter detections or meaningful upper limits remains small (similar to 10). We obtained Infrared Spectrograph (IRS) spectra of six infrared-bright sources associated with LABs. Four of these sources have measurable polycyclic aromatic hydrocarbon (PAH) emission features, indicative of significant star formation, while the remaining two show a featureless continuum, indicative of infrared energy output completely dominated by an AGN. Two of the counterparts with PAHs are mixed sources, with PAH line-to-continuum ratios and PAH equivalent widths indicative of large energy contributions from both star formation and AGN. Most of the LAB infrared counterparts have large stellar masses, around 10(11)M(circle dot). There is a weak trend of mass upper limit with the Ly alpha luminosity of the host blob, particularly after the most likely AGN contaminants are removed. The range in likely energy sources for the LABs found in this and previous studies suggests that there is no single source of power that is producing all the known LABs.
C1 [Colbert, James W.; Scarlata, Claudia; Teplitz, Harry] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Francis, Paul] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 0200, Australia.
[Palunas, Povilas] Las Campanas Observ, La Serena, Chile.
[Williger, Gerard M.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA.
[Woodgate, Bruce] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Colbert, JW (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RI Woodgate, Bruce/D-2970-2012
NR 68
TC 24
Z9 24
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 59
DI 10.1088/0004-637X/728/1/59
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500059
ER
PT J
AU McAlpine, W
Satyapal, S
Gliozzi, M
Cheung, CC
Sambruna, RM
Eracleous, M
AF McAlpine, W.
Satyapal, S.
Gliozzi, M.
Cheung, C. C.
Sambruna, R. M.
Eracleous, Michael
TI BLACK HOLES IN BULGELESS GALAXIES: AN XMM-NEWTON INVESTIGATION OF NGC
3367 AND NGC 4536
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: starburst; infrared: galaxies; X-rays:
galaxies
ID X-RAY SOURCES; ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; NEARBY
GALAXIES; SPIRAL GALAXIES; HOST GALAXIES; MOLECULAR-HYDROGEN;
STAR-FORMATION; EMISSION; VIEW
AB The vast majority of optically identified active galactic nuclei (AGNs) in the local universe reside in host galaxies with prominent bulges, supporting the hypothesis that black hole formation and growth is fundamentally connected to the buildup of galaxy bulges. However, recent mid-infrared spectroscopic studies with Spitzer of a sample of optically "normal" late-type galaxies reveal, remarkably, the presence of high-ionization [Ne v] lines in several sources, providing strong evidence for AGNs in these galaxies. We present follow-up X-ray observations recently obtained with XMM-Newton of two such sources, the late-type optically normal galaxies NGC 3367 and NGC 4536. Both sources are detected in our observations. Detailed spectral analysis reveals that for both galaxies, the 2-10 keV emission is dominated by a power law with an X-ray luminosity in the L2-10 (keV) similar to 10(39)-10(40) erg s(-1) range, consistent with low-luminosity AGNs. While there is a possibility that X-ray binaries account for some fraction of the observed X-ray luminosity, we argue that this fraction is negligible. These observations therefore add to the growing evidence that the fraction of late-type galaxies hosting AGNs is significantly underestimated using optical observations alone. A comparison of the mid-infrared [Ne v] luminosity and the X-ray luminosities suggests the presence of an additional highly absorbed X-ray source in both galaxies, and that the black hole masses are in the range 10(5)-10(7) M-circle dot for NGC 3367 and 10(4)-10(6) M-circle dot for NGC 4536.
C1 [McAlpine, W.; Satyapal, S.; Gliozzi, M.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Sambruna, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Eracleous, Michael] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Eracleous, Michael] Penn State Univ, Ctr Gravitat Wave Phys, Davey Lab 525, University Pk, PA 16802 USA.
RP McAlpine, W (reprint author), George Mason Univ, Dept Phys & Astron, MS 3F3,4400 Univ Dr, Fairfax, VA 22030 USA.
EM wmcalpine@gmu.edu
FU NASA [NNX08AZ39G, NAG5-1078]
FX It is a pleasure to thank Marla Katz for her invaluable help in the
initial data analysis required for this project. This work would not
have been possible without her dedication and hard work. We are also
very grateful for the helpful comments from the referee, which improved
this paper. 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. S.S. gratefully acknowledges
support by the XMM-Newton Guest Investigator Program under NASA grant
NNX08AZ39G. S.S. and R.M.S. gratefully acknowledge funds from NASA grant
NAG5-1078.
NR 50
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U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 25
DI 10.1088/0004-637X/728/1/25
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500025
ER
PT J
AU Savransky, D
Cady, E
Kasdin, NJ
AF Savransky, Dmitry
Cady, Eric
Kasdin, N. Jeremy
TI PARAMETER DISTRIBUTIONS OF KEPLERIAN ORBITS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE celestial mechanics; methods: analytical; methods: statistical; planets
and satellites: detection
ID OBSCURATIONAL COMPLETENESS; EXTRASOLAR PLANETS; MASS
AB Starting with just the assumption of uniformly distributed orbital orientations, we derive expressions for the distributions of the Keplerian orbital elements as functions of arbitrary distributions of eccentricity and semimajor axis. We present methods for finding the probability density functions of the true anomaly, eccentric anomaly, orbital radius, and other parameters used in describing direct planetary observations. We also demonstrate the independence of the distribution of phase angle, which is highly significant in the study of direct searches, and present examples validating the derived expressions.
C1 [Savransky, Dmitry; Kasdin, N. Jeremy] Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA.
[Cady, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Savransky, D (reprint author), Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA.
EM dsavrans@princeton.edu
RI Savransky, Dmitry/M-1298-2014
OI Savransky, Dmitry/0000-0002-8711-7206
NR 18
TC 4
Z9 4
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 66
DI 10.1088/0004-637X/728/1/66
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500066
ER
PT J
AU Tan, XF
Bernstein, L
Cami, J
Salama, F
AF Tan, Xiaofeng
Bernstein, Lawrence
Cami, Jan
Salama, Farid
TI ON ESTIMATING INTERSTELLAR POLYCYCLIC AROMATIC HYDROCARBON ABUNDANCES
WITH CALCULATED OSCILLATOR STRENGTHS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: abundances; ISM: molecules
ID DENSITY-FUNCTIONAL THEORY; RING-DOWN SPECTROSCOPY; ELECTRONIC
ABSORPTION-SPECTROSCOPY; SUPERSONIC JET; NAPHTHALENE CATION; OPTICAL
CAVITY; PROGRAM RPAC; BASIS-SETS; BANDS; TIME
AB Vibronic bands of polycyclic aromatic hydrocarbons (PAHs) in the UV/visible range are often used to estimate the abundances of PAHs in the interstellar medium by comparing laboratory-measured spectra with astronomical observations. We investigate the errors introduced by associating theoretical electronic oscillator strengths with individual vibronic bands when estimating the abundances of interstellar PAHs. The vibronic oscillator strengths of the 0-0 bands of nine PAHs with two to seven benzene rings, spanning in the 2800-6700 angstrom spectral range, have been calculated using the Franck-Condon approximation and compared to their electronic oscillator strengths. It is found that the use of calculated electronic oscillator strengths rather than the more physically relevant vibronic oscillator strengths underestimates interstellar abundances of the nine PAHs under study, on average by a factor of about 2.4. It is recommended that vibronic oscillator strengths should be systematically used to analyze the vibronic spectra of specific PAHs and to estimate their abundances in the interstellar medium. An empirical correcting factor is suggested for the cases where the vibronic oscillator strengths are unknown for more realistic estimation of interstellar PAH abundances.
C1 [Tan, Xiaofeng; Bernstein, Lawrence] Spectral Sci Inc, Burlington, MA 01803 USA.
[Tan, Xiaofeng; Salama, Farid] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Cami, Jan] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Cami, Jan] SETI Inst, Mountain View, CA 94043 USA.
RP Tan, XF (reprint author), Spectral Sci Inc, 4 4th Ave, Burlington, MA 01803 USA.
EM x.tan@jhu.edu
RI Salama, Farid/A-8787-2009;
OI Salama, Farid/0000-0002-6064-4401; Cami, Jan/0000-0002-2666-9234
FU NASA Ames Research Center; NASA; Spectral Sciences, Inc.
FX This work originates from research conducted by X.T. when he held a
National Research Council Research Associateship Award at NASA Ames
Research Center. F.S. acknowledges the support of the NASA SMD APRA
program. X.T. and L.B. also acknowledge funding under a Spectral
Sciences, Inc., IR&D project.
NR 53
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U1 0
U2 10
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 FEB 10
PY 2011
VL 728
IS 1
AR 62
DI 10.1088/0004-637X/728/1/62
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500062
ER
PT J
AU Wilson, TL
Muders, D
Dumke, M
Henkel, C
Kawamura, JH
AF Wilson, T. L.
Muders, D.
Dumke, M.
Henkel, C.
Kawamura, Jonathan H.
TI THE SUBMILLIMETER J=6-5 LINE OF (CO)-C-13 IN ORION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (Orion BN/KL, Orion Hot Core); ISM: jets and
outflows; ISM: molecules; stars: early-type; submillimeter: stars
ID HEINRICH-HERTZ-TELESCOPE; MOLECULAR CLOUDS; APERTURE SYNTHESIS;
KLEINMANN-LOW; HOT CORE; EMISSION; STAR; KL; NEBULA; OMC-1
AB We present a fully sampled map covering the Orion Hot Core and dense molecular ridge, in the submillimeter J = 6-5 rotational transition of (CO)-C-13, at lambda = 0.45 mm with a resolution of 13 '' and 0.5 km s(-1). The map covers 3' by 2'. The profile centered on the Hot Core peaks at 8.5 km s(-1) and has a peak intensity of 40 K, corrected antenna temperature. It shows line wings from 30 km s(-1) to -20 km s(-1). The map of intensity, integrated from 0 to +18 km s(-1), shows a prominent maximum <5 '' from the center of the Orion Hot Core. The FWHP is 37 '' larger than the regions containing complex molecules. Single dish measurements of lines from the J = 2-1 or J = 1-0 transitions of CO isotopes show no such distinct maximum. Correcting for tau = 1.5 in the J = 6-5 line of (CO)-C-13, and assuming that the level populations are thermalized at 150 K, the beam-averaged column density between 0 to +18 km s(-1) is N((CO)-C-13) = 6.8 x 10(17) cm(-2) and N(CO) = 5.2 x 10(19) cm(-2). When combined with published dust emission data, the CO/H-2 number ratio is 2 x 10(-5), a factor of similar to 5 lower than the canonical value, 10(-4). For the Orion South and Orion Ridge region, the column density of CO is <25% of that found for the Hot Core but CO/H-2 ratios are similar. Models of photon dominated regions, PDRs, predict that CO lines from PDRs are only marginally optically thick. Thus, our map traces warm and dense molecular gas rather than PDRs.
C1 [Wilson, T. L.] USN, Res Lab, Washington, DC 20375 USA.
[Muders, D.; Henkel, C.] Max Planck Inst F Radioastron, D-53121 Bonn, Germany.
[Dumke, M.] European So Observ, Santiago 19, Chile.
[Kawamura, Jonathan H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wilson, TL (reprint author), USN, Res Lab, Code 7210, Washington, DC 20375 USA.
EM tom.wilson@nrl.navy.mil
FU Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration
FX We thank M. Wolfire for advice about the interpretation of PDR emission
in regard to 13CO. We also thank an anonymous referee for a
careful and critical reading of the draft. J.K.'s work was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
NR 54
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 61
DI 10.1088/0004-637X/728/1/61
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500061
ER
PT J
AU Goldstein, ME
Sescu, A
Duck, PW
Choudhari, M
AF Goldstein, M. E.
Sescu, Adrian
Duck, Peter W.
Choudhari, Meelan
TI Algebraic/transcendental disturbance growth behind a row of roughness
elements
SO JOURNAL OF FLUID MECHANICS
LA English
DT Article
DE boundary-layer receptivity; boundary-layer stability; boundary-layer
structure
ID BOUNDARY-LAYER; DILATED PIPES; FLAT-PLATE; FLOW; INSTABILITY; STABILITY;
CHANNELS
AB This paper is a continuation of the work begun in Goldstein et al. (J. Fluid Mech., vol. 644, 2010, P. 123), who constructed an asymptotic high-Reynolds-number solution for the flow over a spanwise periodic array of relatively small roughness elements with (spanwise) separation and plan form dimensions of the order of the local boundary-layer thickness. While that paper concentrated on the linear problem, here the focus is on the case where the flow is nonlinear in the immediate vicinity of the roughness with emphasis on the intermediate wake region corresponding to streamwise distances that are large in comparison with the roughness dimension, but small in comparison with the distance between the roughness array and the leading edge. An analytical O(h(2)) asymptotic solution is obtained for the limiting case of a small roughness height parameter h. These weakly nonlinear results show that the spanwise variable component of the wall-pressure perturbation decays as x(-5/3) ln x when x -> infinity (where x denotes the streamwise distance scaled on the roughness dimension), but the corresponding component of the streamwise velocity perturbation (i.e. the wake velocity) exhibits an O(x(1/3) ln x) algebraic/transcendental growth in the main boundary layer. Numerical solutions for h=O(1) demonstrate that the wake velocity perturbation for the fully nonlinear case grows in the same manner as the weakly nonlinear prediction which is considerably different from the strictly linear result obtained in Goldstein et al. (2010).
C1 [Goldstein, M. E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Sescu, Adrian] Univ Toledo, Dept Mech Ind & Mfg Engn, Toledo, OH 43606 USA.
[Duck, Peter W.] Univ Manchester, Sch Math, Manchester M13 9PL, Lancs, England.
[Choudhari, Meelan] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Goldstein, ME (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Marvin.E.Goldstein@nasa.gov
RI Choudhari, Meelan/F-6080-2017
OI Choudhari, Meelan/0000-0001-9120-7362
FU Aerothermodynamics element of NASA's subsonic fixed wing project;
Aerothermodynamics and Plasma Dynamics element of the hypersonics
project
FX The authors gratefully acknowledge the support of the Aerothermodynamics
element of NASA's subsonic fixed wing project and the Aerothermodynamics
and Plasma Dynamics element of the hypersonics project. A.S. would like
to thank Dr A. Afjeh, Professor and Chair, and Dr R. Hixon, Associate
Professor, MIME Department, University of Toledo.
NR 25
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U1 0
U2 3
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-1120
J9 J FLUID MECH
JI J. Fluid Mech.
PD FEB 10
PY 2011
VL 668
BP 236
EP 266
DI 10.1017/S0022112010004726
PG 31
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 725GZ
UT WOS:000287634500012
ER
PT J
AU Borovikov, SN
Pogorelov, NV
Burlaga, LF
Richardson, JD
AF Borovikov, Sergey N.
Pogorelov, Nikolai V.
Burlaga, Leonard F.
Richardson, John D.
TI PLASMA NEAR THE HELIOSHEATH: OBSERVATIONS AND MODELING
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE interplanetary medium; magnetic fields; solar wind; Sun: heliosphere
ID LOCAL INTERSTELLAR-MEDIUM; SOLAR-WIND; TERMINATION SHOCK; OUTER
HELIOSPHERE; NEUTRAL HYDROGEN; MAGNETIC-FIELDS; 3-DIMENSIONAL FEATURES;
CONSEQUENCES; INTERFACE; VOYAGER-1
AB Sound numerical modeling is capable of providing important predictive information about the solar wind interaction with the local interstellar medium. The results of our three-dimensional simulation show a good agreement with Voyager observations from 2007 to 2010. We analyze the termination shock properties at the Voyager crossing points and juxtapose them with the observed data. The heliospheric current sheet structure in the inner heliosheath is examined.
C1 [Borovikov, Sergey N.; Pogorelov, Nikolai V.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Burlaga, Leonard F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Richardson, John D.] MIT, Kavli Ctr Astrophys & Space Sci, Cambridge, MA 02139 USA.
[Pogorelov, Nikolai V.] Univ Alabama, Dept Phys, Huntsville, AL 35805 USA.
RP Borovikov, SN (reprint author), Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
FU NASA [NNX09AG63G, NNX09AW44G, NNX09AP74A, NNX08AC04G]
FX This work was supported by NASA grants NNX09AG63G, NNX09AW44G,
NNX09AP74A. Calculations were performed on supercomputers from
NASA(SMD-09-1148), NSF (MCA07S033), and DOE (PSS003). J.D.R. was
supported by NASA's Voyager project and NASA grant NNX08AC04G.
NR 30
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 10
PY 2011
VL 728
IS 1
AR L21
DI 10.1088/2041-8205/728/1/L21
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 711WV
UT WOS:000286623000021
ER
PT J
AU Hopwood, R
Wardlow, J
Cooray, A
Khostovan, AA
Kim, S
Negrello, M
da Cunha, E
Burgarella, D
Aretxaga, I
Auld, R
Baes, M
Barton, E
Bertoldi, F
Bonfield, DG
Blundell, R
Buttiglione, S
Cava, A
Clements, DL
Cooke, J
Dannerbauer, H
Dariush, A
de Zotti, G
Dunlop, J
Dunne, L
Dye, S
Eales, S
Fritz, J
Frayer, D
Gurwell, MA
Hughes, DH
Ibar, E
Ivison, RJ
Jarvis, MJ
Lagache, G
Leeuw, L
Maddox, S
Michallowski, MJ
Omont, A
Pascale, E
Pohlen, M
Rigby, E
Rodighiero, G
Scott, D
Serjeant, S
Smail, I
Smith, DJB
Temi, P
Thompson, MA
Valtchanov, I
van der Werf, P
Verma, A
Vieira, JD
AF Hopwood, R.
Wardlow, J.
Cooray, A.
Khostovan, A. A.
Kim, S.
Negrello, M.
da Cunha, E.
Burgarella, D.
Aretxaga, I.
Auld, R.
Baes, M.
Barton, E.
Bertoldi, F.
Bonfield, D. G.
Blundell, R.
Buttiglione, S.
Cava, A.
Clements, D. L.
Cooke, J.
Dannerbauer, H.
Dariush, A.
de Zotti, G.
Dunlop, J.
Dunne, L.
Dye, S.
Eales, S.
Fritz, J.
Frayer, D.
Gurwell, M. A.
Hughes, D. H.
Ibar, E.
Ivison, R. J.
Jarvis, M. J.
Lagache, G.
Leeuw, L.
Maddox, S.
Michallowski, M. J.
Omont, A.
Pascale, E.
Pohlen, M.
Rigby, E.
Rodighiero, G.
Scott, D.
Serjeant, S.
Smail, I.
Smith, D. J. B.
Temi, P.
Thompson, M. A.
Valtchanov, I.
van der Werf, P.
Verma, A.
Vieira, J. D.
TI SPITZER IMAGING OF HERSCHEL-ATLAS GRAVITATIONALLY LENSED SUBMILLIMETER
SOURCES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: individual (SDP.81: H-ATLAS J090311.6+003906, SDP.130: H-ATLAS
J091305.0-005343); galaxies: starburst; gravitational lensing: strong
ID SIMILAR-TO 2; GALAXIES; CO; SPECTROMETER; ULTRAVIOLET; EMISSION;
STELLAR; ULIRGS
AB We present physical properties of two submillimeter selected gravitationally lensed sources, identified in the Herschel Astrophysical Terahertz Large Area Survey. These submillimeter galaxies (SMGs) have flux densities >100 mJy at 500 mu m, but are not visible in existing optical imaging. We fit light profiles to each component of the lensing systems in Spitzer IRAC 3.6 and 4.5 mu m data and successfully disentangle the foreground lens from the background source in each case, providing important constraints on the spectral energy distributions (SEDs) of the background SMG at rest-frame optical-near-infrared wavelengths. The SED fits show that these two SMGs have high dust obscuration with A(V) similar to 4-5 and star formation rates of similar to 100M(circle dot) yr(-1). They have low gas fractions and low dynamical masses compared with 850 mu m selected galaxies.
C1 [Hopwood, R.; Negrello, M.; Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Wardlow, J.; Cooray, A.; Khostovan, A. A.; Kim, S.; Barton, E.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[da Cunha, E.; Cooke, J.] Univ Crete, Dept Phys, Iraklion, Greece.
[Burgarella, D.] Aix Marseille Univ, CNRS, OAMP, Lab Astrophys Marseille, Marseille, France.
[Aretxaga, I.; Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico.
[Auld, R.; Dariush, A.; Dye, S.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Bertoldi, F.] Univ Bonn, Argenlander Inst Astron, D-53121 Bonn, Germany.
[Bonfield, D. G.; Jarvis, M. J.; Thompson, M. A.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Ctr, Hatfield AL10 9AB, Herts, England.
[Blundell, R.; Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Buttiglione, S.; de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Cava, A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Cava, A.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, Astrophys Grp, London SW7 2AZ, England.
[Cooke, J.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Dannerbauer, H.] CEA Saclay, CEA CNRS Univ, Lab AIM Paris Saclay, Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran.
[de Zotti, G.] Scuola Int Super Studi Avanzati, I-34136 Trieste, Italy.
[Dunlop, J.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Dunne, L.; Maddox, S.; Rigby, E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; Michallowski, M. J.; van der Werf, P.] Univ Edinburgh, Royal Observ, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Lagache, G.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France.
[Leeuw, L.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Leeuw, L.] SETI Inst, Mountain View, CA 94043 USA.
[Omont, A.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France.
[Omont, A.] CNRS, F-75014 Paris, France.
[Rodighiero, G.] Univ Padua, Dipartimento Astron, Vicolo Osservatorio, I-35122 Padua, Italy.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Smail, I.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
[Valtchanov, I.] European Space Agcy, Herschel Sci Ctr, Madrid 28691, Spain.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 Leiden, Netherlands.
[Verma, A.] Univ Oxford, Oxford OX1 3RH, England.
RP Hopwood, R (reprint author), Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
RI Baes, Maarten/I-6985-2013; Smail, Ian/M-5161-2013; Wardlow,
Julie/C-9903-2015; Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017;
OI Smith, Daniel/0000-0001-9708-253X; Rodighiero,
Giulia/0000-0002-9415-2296; da Cunha, Elisabete/0000-0001-9759-4797;
Baes, Maarten/0000-0002-3930-2757; Smail, Ian/0000-0003-3037-257X;
Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313;
Cava, Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X;
Scott, Douglas/0000-0002-6878-9840; Dye, Simon/0000-0002-1318-8343
FU Science and Technology Facilities Council [D/002400/1, SF/F005288/1];
NASA; NASA Herschel Science Center through JPL/Caltech; CONACyT [50786,
60878]; NASA through JPL/Caltech
FX Herschel-ATLAS is a project with Herschel, which is an ESA space
observatory with science instruments provided by European-led Principal
Investigator consortia and with important participation from NASA. The
H-ATLAS Web site is http://www.h-atlas.org/ We thank the Science and
Technology Facilities Council, grant D/002400/1 and
studentship/SF/F005288/1. This work is based in part on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. Support for this work was provided by NASA through
an award issued by JPL/Caltech. US participants in H-ATLAS also
acknowledge support from NASA Herschel Science Center through a contract
from JPL/Caltech. I. A. and D. H. H. are partially funded by CONACyT
grants 50786 and 60878.
NR 30
TC 13
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 10
PY 2011
VL 728
IS 1
AR L4
DI 10.1088/2041-8205/728/1/L4
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 711WV
UT WOS:000286623000004
ER
PT J
AU Airapetian, V
Ofman, L
Sittler, EC
Kramar, M
AF Airapetian, V.
Ofman, L.
Sittler, E. C.
Kramar, M.
TI PROBING THE THERMODYNAMICS AND KINEMATICS OF SOLAR CORONAL STREAMERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); solar wind; Sun: corona
ID MAGNETOHYDRODYNAMIC SIMULATIONS; 3-DIMENSIONAL SIMULATION;
HELMET-STREAMER; WIND VELOCITY; MHD MODEL; MINIMUM; WAVES; FLOWS; HOLES;
SUN
AB We present the results of a resistive magnetohydrodynamic (MHD) model of an equatorially confined streamer belt using observational constraints for the heating and acceleration of the solar wind. To initiate the 2.5 dimensional MHD calculations, we used the Potential Field Source Surface model of the coronal magnetic field configuration with the boundary conditions at the photosphere specified by the National Solar Observatory/GONG magnetogram data. Calculations were performed for the fully thermal conductive model with observationally constrained heat flux, q(eff), and the effective temperature, T-eff, derived from the semi-empirical steady-state two-dimensional model of the solar corona. We compared the results of the model to a polytropic solution (polytropic index gamma = 1.05), and demonstrate that our MHD model is in better agreement with reconstructed density and observed flow velocity than the polytropic model for the coronal streamer structure observed during 2008 February 1-13 by the COR1 coronagraph on board the STEREO spacecraft.
C1 [Airapetian, V.; Ofman, L.; Kramar, M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Airapetian, V.; Ofman, L.; Sittler, E. C.; Kramar, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ofman, L (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
FU NASA [NNX08AF85G, NNX08AP88G]
FX The work of V.A. and L.O. was supported by the NASA grant NNX08AF85G.
M.K. and L.O. were also supported by NASA grant NNX08AP88G.
NR 32
TC 8
Z9 8
U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 67
DI 10.1088/0004-637X/728/1/67
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500067
ER
PT J
AU Assef, RJ
Kochanek, CS
Ashby, MLN
Brodwin, M
Brown, MJI
Cool, R
Forman, W
Gonzalez, AH
Hickox, RC
Jannuzi, BT
Jones, C
Le Floc'h, E
Moustakas, J
Murray, SS
Stern, D
AF Assef, R. J.
Kochanek, C. S.
Ashby, M. L. N.
Brodwin, M.
Brown, M. J. I.
Cool, R.
Forman, W.
Gonzalez, A. H.
Hickox, R. C.
Jannuzi, B. T.
Jones, C.
Le Floc'h, E.
Moustakas, J.
Murray, S. S.
Stern, D.
TI THE MID-IR- AND X-RAY-SELECTED QSO LUMINOSITY FUNCTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: distances and redshifts; galaxies:
luminosity function, mass function; quasars: general
ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; WIDE-FIELD SURVEY;
RESOLUTION SPECTRAL TEMPLATES; SPITZER-SPACE-TELESCOPE; GALAXY EVOLUTION
SURVEY; HIGH-REDSHIFT QUASARS; BLACK-HOLES; MIDINFRARED SELECTION; HOST
GALAXIES
AB We present the J-band luminosity function (LF) of 1838 mid-infrared and X-ray-selected active galactic nuclei (AGNs) in the redshift range 0 < z < 5.85. These LFs are constructed by combining the deep multi-wavelength broadband observations from the UV to the mid-IR of the NDWFS Bootes field with the X-ray observations of the XBootes survey and the spectroscopic observations of the same field by AGES. Our sample is primarily composed of IRAC-selected AGNs, targeted using modifications of the Stern et al. criteria, complemented by MIPS 24 mu m and X-ray-selected AGNs to alleviate the biases of IRAC mid-IR selection against z similar to 4.5 quasars and AGNs faint with respect to their hosts. This sample provides an accurate link between low-and high-redshift AGN LFs and does not suffer from the usual incompleteness of optical samples at z similar to 3. We use a set of low-resolution spectral energy distribution templates for AGNs and galaxies presented in a previous paper by Assef et al. to model the selection function of these sources and apply host and reddening corrections. We find that the space density of the brightest quasars strongly decreases from z = 3 to z = 0, while the space density of faint quasars is at least flat, and possibly increasing, over the same redshift range. At z > 3, we observe a decrease in the space density of quasars of all brightnesses. We model the LF by a double power law and find that its evolution cannot be described by either pure luminosity or pure density evolution, but must be a combination of both. We used the bright-end slope determined by Croom et al. (2QZ) as a prior to fit the data in order to minimize the effects of our small survey area. The bright-end power-law index of our best-fit model remains consistent with the prior, while the best-fit faint-end index is consistent with the low-redshift measurements based on the 2QZ and 2SLAQ surveys. Our best-fit model generally agrees with the number of bright quasars predicted by other LFs at all redshifts. If we construct the QSO luminosity function using only the IRAC-selected AGNs, we find that the biases inherent to this selection method significantly modify the behavior of the characteristic density phi(*)(z) only for z < 1 and have no significant impact upon the characteristic magnitude M-*,J(z).
C1 [Assef, R. J.; Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Ashby, M. L. N.; Brodwin, M.; Forman, W.; Hickox, R. C.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Cool, R.] Princeton Univ, Princeton, NJ 08540 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA.
[Hickox, R. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Jannuzi, B. T.] Kitt Peak Natl Observ, Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Le Floc'h, E.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Moustakas, J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Assef, RJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
EM rjassef@astronomy.ohio-state.edu
RI Brown, Michael/B-1181-2015;
OI Brown, Michael/0000-0002-1207-9137; Forman, William/0000-0002-9478-1682
FU W. M. Keck Foundation; Jet Propulsion Laboratory, California Institute
of Technology, under a contract with NASA; National Optical Astronomy
Observatory (NOAO); AURA, Inc., under a cooperative agreement with the
National Science Foundation
FX We thank all the people in the NDWFS, FLAMEX, and SDWFS collaborations
that did not directly participate in this work. We also thank the
anonymous referee for comments and suggestions that helped improve this
work. Support for M. B. was provided by the W. M. Keck Foundation. The
work of D.S. was carried out at Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA. The AGES
observations were obtained at the MMT Observatory, a joint facility of
the Smithsonian Institution and the University of Arizona. This work
made use of images and/or data products provided by the NOAO Deep
Wide-Field Survey (Jannuzi & Dey 1999; B. T. Jannuzi et al. 2011, in
preparation; A. Dey et al. 2011, in preparation), which is supported by
the National Optical Astronomy Observatory (NOAO). This research draws
upon data provided by Dr. Buell Jannuzi and Dr. Arjun Dey as distributed
by the NOAO Science Archive. NOAO is operated by AURA, Inc., under a
cooperative agreement with the National Science Foundation.
NR 61
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 56
DI 10.1088/0004-637X/728/1/56
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500056
ER
PT J
AU Burlon, D
Ajello, M
Greiner, J
Comastri, A
Merloni, A
Gehrels, N
AF Burlon, D.
Ajello, M.
Greiner, J.
Comastri, A.
Merloni, A.
Gehrels, N.
TI THREE-YEAR SWIFT-BAT SURVEY OF ACTIVE GALACTIC NUCLEI: RECONCILING
THEORY AND OBSERVATIONS?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; radiation mechanisms: non-thermal; X-rays: general
ID X-RAY LUMINOSITY; SUPERMASSIVE BLACK-HOLES; ABSORBING COLUMN DENSITIES;
CHANDRA DEEP FIELDS; SEYFERT 2 GALAXIES; ALL-SKY SURVEY; XMM-NEWTON;
STAR-FORMATION; EMISSION-LINE; STATISTICAL PROPERTIES
AB It is well accepted that unabsorbed as well as absorbed active galactic nuclei (AGNs) are needed to explain the nature and shape of the Cosmic X-ray background (CXB), even if the fraction of highly absorbed objects (dubbed Compton-thick sources) still substantially escapes detection. We derive and analyze the absorption distribution using a complete sample of AGNs detected by Swift-BAT in the first three years of the survey. The fraction of Compton-thick AGNs represents only 4.6% of the total AGN population detected by Swift-BAT. However, we show that once corrected for the bias against the detection of very absorbed sources the real intrinsic fraction of Compton-thick AGNs is 20(-6)(+9)%. We proved for the first time (also in the Burst Alert Telescope (BAT) band) that the anti-correlation of the fraction of absorbed AGNs and luminosity is tightly connected to the different behavior of the X-ray luminosity functions (XLFs) of absorbed and unabsorbed AGNs. This points toward a difference between the two subsamples of objects with absorbed AGNs being, on average, intrinsically less luminous than unobscured ones. Moreover, the XLFs show that the fraction of obscured AGNs might also decrease at very low luminosity. This can be successfully interpreted in the framework of a disk cloud outflow scenario as the disappearance of the obscuring region below a critical luminosity. Our results are discussed in the framework of population synthesis models and the origin of the CXB.
C1 [Burlon, D.; Greiner, J.; Merloni, A.] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany.
[Ajello, M.] SLAC Natl Lab, Menlo Pk, CA 94025 USA.
[Ajello, M.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Comastri, A.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Merloni, A.] TUM, D-85748 Garching, Germany.
[Gehrels, N.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Burlon, D (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85740 Garching, Germany.
EM burlon@mpe.mpg.de; majello@slac.stanford.edu
RI Gehrels, Neil/D-2971-2012; Comastri, Andrea/O-9543-2015
OI Comastri, Andrea/0000-0003-3451-9970
FU [DLR50OR0405]; [ASI-INAFI/009/10/0]; [ASI-INAFI/088/06/0]
FX We are in debt to Tahir Yaqoob and Kendrah Murphy for allowing us to use
the results of their model for the transmission of radiation through a
Compton-thick medium before publication. We also acknowledge helpful
comments from the referee. The authors acknowledge the use of NED,
SIMBAD, and HEASARC. We thank the Swift team for the rapid approval of
ToO observations. D.B. is in debt to G. Ghisellini and G. Ghirlanda for
endless discussions, and acknowledges S. Sazonov for stimulating
discussions on the dusty torus and the luminosity function and M.
Bolzonella for help with the Binomial statistics computation of errors.
D.B. also acknowledges R. Gilli, E. Treister, and P. Severgnini for
their kind replies. D.B. is supported through DLR50OR0405. A.C.
acknowledges financial contribution from the agreement
ASI-INAFI/009/10/0 and ASI-INAFI/088/06/0.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 58
DI 10.1088/0004-637X/728/1/58
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500058
ER
PT J
AU Espaillat, C
Furlan, E
D'Alessio, P
Sargent, B
Nagel, E
Calvet, N
Watson, DM
Muzerolle, J
AF Espaillat, C.
Furlan, E.
D'Alessio, P.
Sargent, B.
Nagel, E.
Calvet, N.
Watson, Dan M.
Muzerolle, J.
TI A SPITZER IRS STUDY OF INFRARED VARIABILITY IN TRANSITIONAL AND
PRE-TRANSITIONAL DISKS AROUND T TAURI STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
ID PRE-MAIN-SEQUENCE; PROTOPLANETARY ACCRETION DISKS; INTERSTELLAR SILICATE
MINERALOGY; ECCENTRIC STELLAR BINARIES; HERBIG AE/BE STARS; FORMING
REGION; CHAMELEON-I; CIRCUMSTELLAR DISKS; GRAIN-GROWTH; GM-AURIGAE
AB We present a Spitzer IRS study of variability in 14 T Tauri stars in the Taurus and Chamaeleon star-forming regions. The sample is composed of transitional and pre-transitional objects which contain holes and gaps in their disks. We detect variability between 5 and 38 mu m in all but two of our objects on timescales of 2-3 years. Most of the variability observed can be classified as seesaw behavior, whereby the emission at shorter wavelengths varies inversely with the emission at longer wavelengths. For many of the objects we can reasonably reproduce the observed variability using irradiated disk models, particularly by changing the height of the inner disk wall by similar to 20%. When the inner wall is taller, the emission at the shorter wavelengths is higher since the inner wall dominates the emission at 2-8 mu m. The taller inner wall casts a larger shadow on the outer disk wall, leading to less emission at wavelengths beyond 20 mu m where the outer wall dominates. We discuss how the possible presence of planets in these disks could lead to warps that cause changes in the height of the inner wall. We also find that crystalline silicates are common in the outer disks of our objects and that in the four disks in the sample with the most crystalline silicates, variability on timescales of 1 week is present. In addition to explaining the infrared variability described above, planets can create shocks and collisions which can crystallize the dust and lead to short timescale variability.
C1 [Espaillat, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Furlan, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[D'Alessio, P.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico.
[Sargent, B.; Muzerolle, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Nagel, E.] Univ Guanajuato, Dept Astron, Guanajuato 36240, Gto, Mexico.
[Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Watson, Dan M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
RP Espaillat, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA.
EM cespaillat@cfa.harvard.edu; Elise.Furlan@jpl.nasa.gov;
p.dalessio@crya.unam.mx; sargent@stsci.edu; erick@astro.ugto.mx;
ncalvet@umich.edu; dmw@pas.rochester.edu; muzerol@stsci.edu
OI Furlan, Elise/0000-0001-9800-6248
FU National Science Foundation [0901947]; NASA [NNX08AH94G]; PAPIIT-DGAPA
UNAM; CONACyT
FX We thank the referee for a constructive and thorough report. We thank
Lee Hartmann for providing comments on the manuscript and Steve Lubow
for useful discussions. C.E. was supported by the National Science
Foundation under Award No. 0901947. E.F. was supported by NASA through
the Spitzer Space Telescope Fellowship Program, through a contract
issued by JPL/Caltech under a contract with NASA. P.D. acknowledges a
grant from PAPIIT-DGAPA UNAM. E.N. acknowledges a postdoctoral grant
from CONACyT. N.C. acknowledges support from NASA Origins Grant
NNX08AH94G.
NR 123
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 49
DI 10.1088/0004-637X/728/1/49
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500049
ER
PT J
AU Lee, BL
Ge, JA
Fleming, SW
Stassun, KG
Gaudi, BS
Barnes, R
Mahadevan, S
Eastman, JD
Wright, J
Siverd, RJ
Gary, B
Ghezzi, L
Laws, C
Wisniewski, JP
de Mello, GFP
Ogando, RLC
Maia, MAG
da Costa, LN
Sivarani, T
Pepper, J
Duy, CN
Hebb, L
De Lee, N
Wang, J
Wan, XK
Zhao, B
Chang, LA
Groot, J
Varosi, F
Hearty, F
Hanna, K
van Eyken, JC
Kane, SR
Agol, E
Bizyaev, D
Bochanski, JJ
Brewington, H
Chen, ZP
Costello, E
Dou, LM
Eisenstein, DJ
Fletcher, A
Ford, EB
Guo, PC
Holtzman, JA
Jiang, P
Leger, RF
Liu, JA
Long, DC
Malanushenko, E
Malanushenko, V
Malik, M
Oravetz, D
Pan, KK
Rohan, P
Schneider, DP
Shelden, A
Snedden, SA
Simmons, A
Weaver, BA
Weinberg, DH
Xie, JW
AF Lee, Brian L.
Ge, Jian
Fleming, Scott W.
Stassun, Keivan G.
Gaudi, B. Scott
Barnes, Rory
Mahadevan, Suvrath
Eastman, Jason D.
Wright, Jason
Siverd, Robert J.
Gary, Bruce
Ghezzi, Luan
Laws, Chris
Wisniewski, John P.
Porto de Mello, G. F.
Ogando, Ricardo L. C.
Maia, Marcio A. G.
da Costa, Luiz Nicolaci
Sivarani, Thirupathi
Pepper, Joshua
Duy Cuong Nguyen
Hebb, Leslie
De Lee, Nathan
Wang, Ji
Wan, Xiaoke
Zhao, Bo
Chang, Liang
Groot, John
Varosi, Frank
Hearty, Fred
Hanna, Kevin
van Eyken, J. C.
Kane, Stephen R.
Agol, Eric
Bizyaev, Dmitry
Bochanski, John J.
Brewington, Howard
Chen, Zhiping
Costello, Erin
Dou, Liming
Eisenstein, Daniel J.
Fletcher, Adam
Ford, Eric B.
Guo, Pengcheng
Holtzman, Jon A.
Jiang, Peng
Leger, R. French
Liu, Jian
Long, Daniel C.
Malanushenko, Elena
Malanushenko, Viktor
Malik, Mohit
Oravetz, Daniel
Pan, Kaike
Rohan, Pais
Schneider, Donald P.
Shelden, Alaina
Snedden, Stephanie A.
Simmons, Audrey
Weaver, B. A.
Weinberg, David H.
Xie, Ji-Wei
TI MARVELS-1b: A SHORT-PERIOD, BROWN DWARF DESERT CANDIDATE FROM THE
SDSS-III MARVELS PLANET SEARCH
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; stars: low-mass; techniques: radial velocities
ID HOBBY-EBERLY TELESCOPE; DIGITAL SKY SURVEY; FIXED-DELAY INTERFEROMETRY;
EXTRASOLAR GIANT PLANETS; INITIAL MASS FUNCTION; MAIN-SEQUENCE STARS;
SOLAR-TYPE STARS; F-TYPE STARS; SUBSTELLAR COMPANIONS; STELLAR
COMPANIONS
AB We present a new short-period brown dwarf (BD) candidate around the star TYC 1240-00945-1. This candidate was discovered in the first year of the Multi-object APO Radial Velocity Exoplanets Large-area Survey (MARVELS), which is part of the Sloan Digital Sky Survey (SDSS) III, and we designate the BD as MARVELS-1b. MARVELS uses the technique of dispersed fixed-delay interferometery to simultaneously obtain radial velocity (RV) measurements for 60 objects per field using a single, custom-built instrument that is fiber fed from the SDSS 2.5 m telescope. From our 20 RV measurements spread over a similar to 370 day time baseline, we derive a Keplerian orbital fit with semi-amplitude K = 2.533 +/- 0.025 km s(-1), period P = 5.8953 +/- 0.0004 days, and eccentricity consistent with circular. Independent follow-up RV data confirm the orbit. Adopting a mass of 1.37 +/- 0.11 M-circle dot for the slightly evolved F9 host star, we infer that the companion has a minimum mass of 28.0 +/- 1.5 M-Jup, a semimajor axis 0.071 +/- 0.002 AU assuming an edge-on orbit, and is probably tidally synchronized. We find no evidence for coherent intrinsic variability of the host star at the period of the companion at levels greater than a few millimagnitudes. The companion has an a priori transit probability of similar to 14%. Although we find no evidence for transits, we cannot definitively rule them out for companion radii less than or similar to 1 R-Jup.
C1 [Lee, Brian L.; Ge, Jian; Fleming, Scott W.; Mahadevan, Suvrath; Sivarani, Thirupathi; Duy Cuong Nguyen; De Lee, Nathan; Wang, Ji; Wan, Xiaoke; Zhao, Bo; Chang, Liang; Groot, John; Varosi, Frank; Hearty, Fred; Hanna, Kevin; Chen, Zhiping; Costello, Erin; Dou, Liming; Fletcher, Adam; Ford, Eric B.; Guo, Pengcheng; Jiang, Peng; Liu, Jian; Malik, Mohit; Rohan, Pais; Xie, Ji-Wei] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Stassun, Keivan G.; Gary, Bruce; Pepper, Joshua; Hebb, Leslie] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
[Gaudi, B. Scott; Eastman, Jason D.; Siverd, Robert J.; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Barnes, Rory; Laws, Chris; Wisniewski, John P.; Agol, Eric; Leger, R. French] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Mahadevan, Suvrath; Wright, Jason; Schneider, Donald P.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Mahadevan, Suvrath; Wright, Jason; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Ghezzi, Luan; Ogando, Ricardo L. C.; Maia, Marcio A. G.; da Costa, Luiz Nicolaci] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil.
[Porto de Mello, G. F.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, Brazil.
[Sivarani, Thirupathi] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[van Eyken, J. C.; Kane, Stephen R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Bizyaev, Dmitry; Brewington, Howard; Long, Daniel C.; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Pan, Kaike; Shelden, Alaina; Snedden, Stephanie A.; Simmons, Audrey] Apache Point Observ, Sunspot, NM 88349 USA.
[Bochanski, John J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Eisenstein, Daniel J.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA.
[Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Weaver, B. A.] NYU, Ctr Cosmol & Particle Phys, New York, NY USA.
RP Lee, BL (reprint author), Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
EM lee@astro.ufl.edu
RI Gaudi, Bernard/I-7732-2012; Kane, Stephen/B-4798-2013; Agol,
Eric/B-8775-2013; Tecnologias espaciai, Inct/I-2415-2013; Ogando,
Ricardo/A-1747-2010;
OI Agol, Eric/0000-0002-0802-9145; Ogando, Ricardo/0000-0003-2120-1154;
Eastman, Jason/0000-0003-3773-5142; Fleming, Scott/0000-0003-0556-027X;
Wright, Jason/0000-0001-6160-5888; /0000-0001-6545-639X; Pepper,
Joshua/0000-0002-3827-8417
FU W.M. Keck Foundation; NSF [AST-0705139, AST-0349075, 0645416, AST
08-02230]; SDSS-III consortium; NASA [NNX07AP14G]; University of
Florida; Alfred P. Sloan Foundation; Participating Institutions;
National Science Foundation; US Department of Energy; National
Aeronautics and Space Administration; Center for Exoplanets and
Habitable Worlds; Pennsylvania State University; Eberly College of
Science; Pennsylvania Space Grant Consortium; Vanderbilt Initiative in
Data-Intensive Astrophysics (VIDA); Vanderbilt University; CNPq
[476909/2006-6]; FAPERJ [APQ1/26/170.687/2004]; University of Arizona;
Brazilian Participation Group; University of Cambridge; French
Participation Group; German Participation Group; Michigan State/Notre
Dame/JINA Participation Group; Johns Hopkins University; Lawrence
Berkeley National Laboratory; Max Planck Institute for Astrophysics; New
Mexico State University; New York University; Ohio State University;
University of Portsmouth; Princeton University; University of Tokyo;
University of Utah; University of Virginia; University of Washington;
Yale University; Vanderbilt Initiative in Data-Intensive Astrophysics
(VIDA) from Vanderbilt University
FX Funding for the MARVELS multi-object Doppler instrument was provided by
the W.M. Keck Foundation and NSF with grant AST-0705139. The MARVELS
survey was partially funded by the SDSS-III consortium, NSF Grant
AST-0705139, NASA with grant NNX07AP14G and the University of Florida.
Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, and the US Department of Energy. The SDSS-III Web site is
http://www.sdss3.org/ SDSS-III is managed by the Astrophysical Research
Consortium for the Participating Institutions of the SDSS-III
Collaboration including the University of Arizona, the Brazilian
Participation Group, University of Cambridge, University of Florida, the
French Participation Group, the German Participation Group, the Michigan
State/Notre Dame/JINA Participation Group, Johns Hopkins University,
Lawrence Berkeley National Laboratory, Max Planck Institute for
Astrophysics, New Mexico State University, New York University, the Ohio
State University, University of Portsmouth, Princeton University,
University of Tokyo, the University of Utah, Vanderbilt University,
University of Virginia, University of Washington and Yale University.
The Hobby-Eberly Telescope (HET) is a joint project of the University of
Texas at Austin, the Pennsylvania State University, Stanford University,
Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat
Gottingen. The HET is named in honor of its principal benefactors,
William P. Hobby and Robert E. Eberly. This publication makes use of
data products from the Two Micron All Sky Survey, which is a joint
project of the University of Massachusetts and the Infrared Processing
and Analysis Center/California Institute of Technology, funded by the
National Aeronautics and Space Administration and the National Science
Foundation. The authors thank Debra Fischer for kindly providing a
preliminary version of her precise Doppler pipeline for use with HRS.
FEROS spectra were observed at the ESO 2.2 m telescope under the ESO-ON
agreement. This research is partially supported by funding from the
Center for Exoplanets and Habitable Worlds. The Center for Exoplanets
and Habitable Worlds is supported by the Pennsylvania State University,
the Eberly College of Science, and the Pennsylvania Space Grant
Consortium. K. G. S., L. H., and J.P. acknowledge funding support from
the Vanderbilt Initiative in Data-Intensive Astrophysics (VIDA) from
Vanderbilt University, and from NSF Career award AST-0349075. E. A.
thanks NSF for CAREER Grant 0645416. G. F. P. M. acknowledges financial
support from CNPq grant no. 476909/2006-6 and FAPERJ grant no.
APQ1/26/170.687/2004. J.P.W. acknowledges support from NSF Astronomy &
Astrophysics Postdoctoral Fellowship AST 08-02230.
NR 105
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 32
DI 10.1088/0004-637X/728/1/32
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500032
ER
PT J
AU Mandell, AM
Deming, LD
Blake, GA
Knutson, HA
Mumma, MJ
Villanueva, GL
Salyk, C
AF Mandell, Avi M.
Deming, L. Drake
Blake, Geoffrey A.
Knutson, Heather A.
Mumma, Michael J.
Villanueva, Geronimo L.
Salyk, Colette
TI NON-DETECTION OF L-BAND LINE EMISSION FROM THE EXOPLANET HD189733b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; infrared: planetary systems; planets and satellites:
individual (HD189733b); radiative transfer; techniques: spectroscopic
ID HUBBLE-SPACE-TELESCOPE; MOLECULAR SPECTROSCOPIC DATABASE; HD 189733B;
EXTRASOLAR PLANET; TRANSMISSION SPECTRUM; INFRARED OBSERVATIONS;
SECONDARY ECLIPSE; THERMAL EMISSION; HOT JUPITERS; MU-M
AB We attempt to confirm bright non-local thermodynamic equilibrium (non-LTE) emission from the exoplanet HD 189733b at 3.25 mu m, as recently reported by Swain et al. based on observations at low spectral resolving power (lambda/delta lambda approximate to 30). Non-LTE emission lines from gas in an exoplanet atmosphere will not be significantly broadened by collisions, so the measured emission intensity per resolution element must be substantially brighter when observed at high spectral resolving power. We observed the planet before, during, and after a secondary eclipse event at a resolving power lambda/delta lambda = 27, 000 using the NIRSPEC spectrometer on the Keck II telescope. Our spectra cover a spectral window near the peak found by Swain et al., and we compare emission cases that could account for the magnitude and wavelength dependence of the Swain et al. result with our final spectral residuals. To model the expected line emission, we use a general non-equilibrium formulation to synthesize emission features from all plausible molecules that emit in this spectral region. In every case, we detect no line emission to a high degree of confidence. After considering possible explanations for the Swain et al. results and the disparity with our own data, we conclude that an astrophysical source for the putative non-LTE emission is unlikely. We note that the wavelength dependence of the signal seen by Swain et al. closely matches the 2 nu(2) band of water vapor at 300 K, and we suggest that an imperfect correction for telluric water is the source of the feature claimed by Swain et al.
C1 [Mandell, Avi M.; Deming, L. Drake; Mumma, Michael J.; Villanueva, Geronimo L.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Villanueva, Geronimo L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Salyk, Colette] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Mandell, AM (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM Avi.Mandell@nasa.gov
RI Mandell, Avi/F-9361-2012; mumma, michael/I-2764-2013
FU Goddard Center for Astrobiology; NASA; W. M. Keck Foundation
FX This research was supported by the Goddard Center for Astrobiology and
the NASA Post-doctoral Fellowship Program. 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. The authors 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 also thank the anonymous referee for
constructive comments.
NR 60
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
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DI 10.1088/0004-637X/728/1/18
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500018
ER
PT J
AU Nowak, MA
Hanke, M
Trowbridge, SN
Markoff, SB
Wilms, J
Pottschmidt, K
Coppi, P
Maitra, D
Davis, JE
Tramper, F
AF Nowak, Michael A.
Hanke, Manfred
Trowbridge, Sarah N.
Markoff, Sera B.
Wilms, Joern
Pottschmidt, Katja
Coppi, Paolo
Maitra, Dipankar
Davis, John E.
Tramper, Frank
TI CORONA, JET, AND RELATIVISTIC LINE MODELS FOR SUZAKU/RXTE/CHANDRA-HETG
OBSERVATIONS OF THE CYGNUS X-1 HARD STATE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; radiation mechanisms:
non-thermal; X-rays: binaries
ID LONG-TERM VARIABILITY; X-RAY SPECTROSCOPY; ACCRETING BLACK-HOLES;
BROAD-BAND SPECTRUM; LOW/HARD STATE; GX 339-4; TEMPORAL CORRELATIONS;
INTERSTELLAR-MEDIUM; SEYFERT-GALAXIES; EMITTING REGION
AB Using Suzaku and the Rossi X-ray Timing Explorer (RXTE), we have conducted a series of four simultaneous observations of the galactic black hole candidate Cyg X-1 in what were historically faint and spectrally hard "low states." Additionally, all of these observations occurred near superior conjunction with our line of sight to the X-ray source passing through the dense phases of the "focused wind" from the mass donating secondary. One of our observations was also simultaneous with observations by the Chandra-High Energy Transmission Grating (HETG). These latter spectra are crucial for revealing the ionized absorption due to the secondary's focused wind. Such absorption is present and must be accounted for in all four spectra. These simultaneous data give an unprecedented view of the 0.8-300 keV spectrum of Cyg X-1, and hence bear upon both corona and X-ray emitting jet models of black hole hard states. Three models fit the spectra well: coronae with thermal or mixed thermal/non-thermal electron populations and jets. All three models require a soft component that we fit with a low temperature disk spectrum with an inner radius of only a few tens of GM/c(2). All three models also agree that the known spectral break at 10 keV is not solely due to the presence of reflection, but each gives a different underlying explanation for the augmentation of this break. Thus, whereas all three models require that there is a relativistically broadened Fe line, the strength and inner radius of such a line is dependent upon the specific model, thus making premature line-based estimates of the black hole spin in the Cyg X-1 system. We look at the relativistic line in detail, accounting for the narrow Fe emission and ionized absorption detected by HETG. Although the specific relativistic parameters of the line are continuum dependent, none of the broad line fits allow for an inner disk radius that is >40 GM/c(2).
C1 [Nowak, Michael A.; Trowbridge, Sarah N.; Davis, John E.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA.
[Hanke, Manfred; Wilms, Joern] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany.
[Markoff, Sera B.; Maitra, Dipankar; Tramper, Frank] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1012 WX Amsterdam, Netherlands.
[Pottschmidt, Katja] UMBC, CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Coppi, Paolo] Yale Univ, New Haven, CT USA.
RP Nowak, MA (reprint author), MIT, Kavli Inst Astrophys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM mnowak@space.mit.edu; Manfred.Hanke@sternwarte.uni-erlangen.de;
saraht@mit.edu; s.b.markoff@uva.nl;
joern.wilms@sternwarte.uni-erlangen.de; katja@milkyway.gsfc.nasa.gov;
paolo.coppi@yale.edu; dmaitra@umich.edu; davis@space.mit.edu
RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009
OI Wilms, Joern/0000-0003-2065-5410;
FU Chandra [NNX07AF71G, NNX08AE23G, NNX08AZ66G, GO8-9036X]; NASA
[SV3-73016]; BMWi [50 OR 0701]; European Commission [ITN 215212];
Netherlands Organization for Scientific Research (NWO); Suzaku
FX We thank the RXTE, Suzaku, and Chandra schedulers for making these
simultaneous observations possible. This work was supported by Suzaku
and Chandra guest observer grants, NNX07AF71G, NNX08AE23G, NNX08AZ66G,
GO8-9036X, as well as NASA Grant SV3-73016. M.H. and J.W. acknowledge
the support of the BMWi through DLR Grant 50 OR 0701. The research in
this work has been partially funded by the European Commission under
grant ITN 215212. S.M. and D.M. acknowledge support from a Netherlands
Organization for Scientific Research (NWO) Vidi and OC Fellowship,
respectively.
NR 69
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 13
DI 10.1088/0004-637X/728/1/13
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500013
ER
PT J
AU Yan, RB
Ho, LC
Newman, JA
Coil, AL
Willmer, CNA
Laird, ES
Georgakakis, A
Aird, J
Barmby, P
Bundy, K
Cooper, MC
Davis, M
Faber, SM
Fang, TT
Griffith, RL
Koekemoer, AM
Koo, DC
Nandra, K
Park, SQ
Sarajedini, VL
Weiner, BJ
Willner, SP
AF Yan, Renbin
Ho, Luis C.
Newman, Jeffrey A.
Coil, Alison L.
Willmer, Christopher N. A.
Laird, Elise S.
Georgakakis, Antonis
Aird, James
Barmby, Pauline
Bundy, Kevin
Cooper, Michael C.
Davis, Marc
Faber, S. M.
Fang, Taotao
Griffith, Roger L.
Koekemoer, Anton M.
Koo, David C.
Nandra, Kirpal
Park, Shinae Q.
Sarajedini, Vicki L.
Weiner, Benjamin J.
Willner, S. P.
TI AEGIS: DEMOGRAPHICS OF X-RAY AND OPTICALLY SELECTED ACTIVE GALACTIC
NUCLEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: fundamental parameters; galaxies: nuclei;
galaxies: Seyfert; galaxies: statistics
ID DIGITAL SKY SURVEY; GALAXY REDSHIFT SURVEY; STAR-FORMING GALAXIES;
EMISSION-LINE GALAXIES; SEYFERT 2 GALAXIES; FORMATION RATE INDICATOR;
EXTENDED GROTH STRIP; 2-10 KEV LUMINOSITY; DEEP FIELD-SOUTH; HOST
GALAXIES
AB We develop a new diagnostic method to classify galaxies into active galactic nucleus (AGN) hosts, star-forming galaxies, and absorption-dominated galaxies by combining the [OIII]/H beta ratio with rest-frame U-B color. This can be used to robustly select AGNs in galaxy samples at intermediate redshifts (z < 1). We compare the result of this optical AGN selection with X-ray selection using a sample of 3150 galaxies with 0.3 < z < 0.8 and I-AB < 22, selected from the DEEP2 Galaxy Redshift Survey and the All-wavelength Extended Groth Strip International Survey. Among the 146 X-ray sources in this sample, 58% are classified optically as emission-line AGNs, the rest as star-forming galaxies or absorption-dominated galaxies. The latter are also known as "X-ray bright, optically normal galaxies" (XBONGs). Analysis of the relationship between optical emission lines and X-ray properties shows that the completeness of optical AGN selection suffers from dependence on the star formation rate and the quality of observed spectra. It also shows that XBONGs do not appear to be a physically distinct population from other X-ray detected, emission-line AGNs. On the other hand, X-ray AGN selection also has strong bias. About 2/3 of all emission-line AGNs at L-bol > 10(44) erg s(-1) in our sample are not detected in our 200 ks Chandra images, most likely due to moderate or heavy absorption by gas near the AGN. The 2-7 keV detection rate of Seyfert 2s at z similar to 0.6 suggests that their column density distribution and Compton-thick fraction are similar to that of local Seyferts. Multiple sample selection techniques are needed to obtain as complete a sample as possible.
C1 [Yan, Renbin] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Ho, Luis C.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Coil, Alison L.; Aird, James] Univ Calif San Diego, Dept Phys, San Diego, CA 92093 USA.
[Coil, Alison L.; Aird, James] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA.
[Laird, Elise S.; Nandra, Kirpal] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Georgakakis, Antonis] Natl Observ Athens, V Paulou 11532, Greece.
[Georgakakis, Antonis] Natl Observ Athens, I Metaxa 11532, Greece.
[Barmby, Pauline] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Bundy, Kevin; Davis, Marc] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Cooper, Michael C.] Univ Calif Irvine, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA 92697 USA.
[Davis, Marc] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Faber, S. M.; Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Griffith, Roger L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Park, Shinae Q.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sarajedini, Vicki L.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
RP Yan, RB (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
EM yan@astro.utoronto.ca
RI Georgakakis, Antonis/K-4457-2013; Barmby, Pauline/I-7194-2016;
OI Barmby, Pauline/0000-0003-2767-0090; Weiner,
Benjamin/0000-0001-6065-7483; Georgakakis, Antonis/0000-0002-3514-2442;
Koekemoer, Anton/0000-0002-6610-2048
FU NSF [AST00-71198, AST00-71048, AST05-07483, AST05-07428, AST08-07630,
AST08-08133]; NASA [G05-6141A, GO8-9129A]; STFC; Alfred P. Sloan
Foundation; National Aeronautics and Space Administration; National
Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho;
Max Planck Society; University of Chicago; Fermilab; Institute for
Advanced Study; Japan Participation Group; Johns Hopkins University; Los
Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA);
Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; University of Pittsburgh; Princeton University; United
States Naval Observatory; University of Washington
FX This study makes use of data from AEGIS, a multiwavelength sky survey
conducted with the Chandra, GALEX, Hubble, Keck, CFHT, MMT, Subaru,
Palomar, Spitzer, VLA, and other telescopes and supported in part by the
NSF, NASA, and the STFC. The AEGIS Web site is http://aegis.ucolick.org.
The DEEP2 Web site is http://deep.berkeley.edu/.; The project was
supported in part by the NSF Grants AST00-71198, AST00-71048,
AST05-07483, AST05-07428, AST08-07630, AST08-08133, and NASA Chandra
Grants G05-6141A and GO8-9129A. This research made use of the NASA
Astrophysics Data System, and employed open-source software written and
maintained by David Schlegel, Douglas Finkbeiner, and others.; Funding
for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred
P. Sloan Foundation, the Participating Institutions, the National
Aeronautics and Space Administration, the National Science Foundation,
the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max
Planck Society. The SDSS Web site is http://www.sdss.org/. The SDSS is
managed by the Astrophysical Research Consortium (ARC) for the
Participating Institutions. The Participating Institutions are The
University of Chicago, Fermilab, the Institute for Advanced Study, the
Japan Participation Group, The Johns Hopkins University, Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State
University, the University of Pittsburgh, Princeton University, the
United States Naval Observatory, and the University of Washington.
NR 108
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2011
VL 728
IS 1
AR 38
DI 10.1088/0004-637X/728/1/38
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712GY
UT WOS:000286655500038
ER
PT J
AU Rosen, R
McLaughlin, MA
Thompson, SE
AF Rosen, R.
McLaughlin, M. A.
Thompson, S. E.
TI A NON-RADIAL OSCILLATION MODEL FOR PULSAR STATE SWITCHING
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE pulsars: general; stars: neutron; stars: oscillations (including
pulsations); white dwarfs
ID ZZ-CETI STARS; WHITE-DWARF G29-38; NEUTRON-STARS; GRAVITY MODES; RADIO
PULSARS; PULSATIONS; SPECTROSCOPY; INSTABILITY; IDENTIFICATION;
MECHANISM
AB Pulsars are unique astrophysical laboratories because of their clock-like timing precision, providing new ways to test general relativity and detect gravitational waves. One impediment to high-precision pulsar timing experiments is timing noise. Recently, Lyne et al. showed that the timing noise in a number of pulsars is due to quasi-periodic fluctuations in the pulsars' spin-down rates and that some of the pulsars have associated changes in pulse profile shapes. Here we show that a non-radial oscillation model based on asteroseismological theory can explain these quasi-periodic fluctuations. Application of this model to neutron stars will increase our knowledge of neutron star emission and neutron star interiors and may improve pulsar timing precision.
C1 [Rosen, R.] NRAO, Green Bank, WV 24944 USA.
[McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[Thompson, S. E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Rosen, R (reprint author), NRAO, POB 2, Green Bank, WV 24944 USA.
EM rrosen@nrao.edu
FU WVEPSCOR; Research Corporation; Sloan Foundation; National Science
Foundation
FX M.A.M. is supported by WVEPSCOR, the Research Corporation, the Sloan
Foundation, and the National Science Foundation. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc. We
also thank Duncan Lorimer and Xavier Seimens for helpful comments on the
manuscript.
NR 44
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U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 10
PY 2011
VL 728
IS 1
AR L19
DI 10.1088/2041-8205/728/1/L19
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 711WV
UT WOS:000286623000019
ER
PT J
AU Tsurutani, BT
Lakhina, GS
Verkhoglyadova, OP
Echer, E
Guarnieri, FL
Narita, Y
Constantinescu, DO
AF Tsurutani, Bruce T.
Lakhina, Gurbax S.
Verkhoglyadova, Olga P.
Echer, Ezequiel
Guarnieri, Fernando L.
Narita, Yasuhito
Constantinescu, Dragos O.
TI Magnetosheath and heliosheath mirror mode structures, interplanetary
magnetic decreases, and linear magnetic decreases: Differences and
distinguishing features
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID NONLINEAR ALFVEN WAVES; PLASMA DEPLETION LAYER; TERRESTRIAL BOW SHOCK;
SOLAR-WIND PLASMA; EQUATOR-S; ULYSSES OBSERVATIONS; PONDEROMOTIVE FORCE;
INTERACTION REGIONS; FIELD OBSERVATIONS; GIACOBINI-ZINNER
AB There has been considerable confusion in the literature about what mirror mode (MM), magnetic decrease (MD), and linear magnetic decrease (LMD) structures are and are not. We will reexamine past spacecraft observations to demonstrate the observational similarities and differences between these magnetic and plasma structures. MM structures in planetary magnetosheaths, cometary sheaths, and the heliosheath have the following characteristics: (1) the structures have little or no changes in the magnetic field direction across the magnetic dips; (2) the structures have quasiperiodic spacings, varying from similar to 20 proton gyroradii (r(p)) in the Earth's magnetosheath to similar to 57 r(p) in the heliosheath; and (3) the magnetic dips have smooth edges. Magnetosheath MM structures are generated by the mirror instability where beta(perpendicular to)/beta(parallel to) > 1 + 1/beta(perpendicular to) (beta is the plasma thermal pressure divided by the magnetic pressure). In general, the sources of free energy for the mirror instability are reasonably well understood: shock compression, field line draping, and, in the cases of comets and the heliosheath, also ion pickup. The observational properties of interplanetary MDs are as follows: (1) there is a broad range of magnetic field angular changes across them; (2) their thicknesses can range from as little as 2-3 r(p) to thousands of r(p), with no "characteristic" size; and (3) they typically are bounded by discontinuities. The mechanism(s) for interplanetary MD generation is (are) currently unresolved, although at least five different mechanisms have been proposed in the literature. Tsurutani et al. (2009a) have argued against mirror instability for those MDs generated within interplanetary corotating interaction regions. Interplanetary LMDs are by definition a subset of MDs with small angular changes across them (theta < 10 degrees). Are LMDs generated by the mirror instability or by another mechanism? Is it possible that there are several different types of LMDs involving different generation mechanisms? At the present time, no one knows the answers to these latter questions.
C1 [Tsurutani, Bruce T.; Verkhoglyadova, Olga P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tsurutani, Bruce T.; Narita, Yasuhito; Constantinescu, Dragos O.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Physik, D-38106 Braunschweig, Germany.
[Lakhina, Gurbax S.] Indian Inst Geomagnetism, Navi Mumbai 410218, India.
[Verkhoglyadova, Olga P.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Echer, Ezequiel] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, Brazil.
[Guarnieri, Fernando L.] Univ Vale Paraiba, Dept Phys & Astron, BR-12244000 Sao Jose Dos Campos, Brazil.
RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bruce.tsurutani@jpl.nasa.gov
RI Lakhina, Gurbax /C-9295-2012; Constantinescu, Dragos/A-6007-2013;
OI Lakhina, Gurbax /0000-0002-8956-486X; Verkhoglyadova,
Olga/0000-0002-9295-9539
FU NASA; Indian National Science Academy, New Delhi; Brazilian FAPESP
agency [2007/52533-1]
FX Portions of this work were done at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. G. S. L.
would like to thank the Indian National Science Academy, New Delhi, for
support under the Senior Scientist Scheme. E. E. acknowledges the
Brazilian FAPESP agency contract 2007/52533-1 for support for this work.
B. T. T. thanks the Tech. Un. Braunschweig for the hospitality and
support during his sabbatical stay.
NR 122
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U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB 10
PY 2011
VL 116
AR A02103
DI 10.1029/2010JA015913
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 721BG
UT WOS:000287325800002
ER
PT J
AU Capak, PL
Riechers, D
Scoville, NZ
Carilli, C
Cox, P
Neri, R
Robertson, B
Salvato, M
Schinnerer, E
Yan, L
Wilson, GW
Yun, M
Civano, F
Elvis, M
Karim, A
Mobasher, B
Staguhn, JG
AF Capak, Peter L.
Riechers, Dominik
Scoville, Nick Z.
Carilli, Chris
Cox, Pierre
Neri, Roberto
Robertson, Brant
Salvato, Mara
Schinnerer, Eva
Yan, Lin
Wilson, Grant W.
Yun, Min
Civano, Francesca
Elvis, Martin
Karim, Alexander
Mobasher, Bahram
Staguhn, Johannes G.
TI A massive protocluster of galaxies at a redshift of z approximate to 5.3
SO NATURE
LA English
DT Article
ID LYMAN-BREAK GALAXIES; SOURCE CATALOG; MOLECULAR GAS; SUBMILLIMETER
GALAXIES; COSMOS SURVEY; EVOLUTION; QUASARS; Z-SIMILAR-TO-6; POPULATION;
HISTORY
AB Massive clusters of galaxies have been found that date from as early as 3.9 billion years(1) (3.9 Gyr; z = 1.62) after the Big Bang, containing stars that formed at even earlier epochs(2,3). Cosmological simulations using the current cold dark matter model predict that these systems should descend from 'protoclusters'-early overdensities of massive galaxies that merge hierarchically to form a cluster(4,5). These protocluster regions themselves are built up hierarchically and so are expected to contain extremely massive galaxies that can be observed as luminous quasars and starbursts(4-6). Observational evidence for this picture, however, is sparse because high-redshift protoclusters are rare and difficult to observe(6,7). Here we report a protocluster region that dates from 1 Gyr (z = 55.3) after the Big Bang. This cluster of massive galaxies extends over more than 13 megaparsecs and contains a luminous quasar as well as a system rich in molecular gas(8). These massive galaxies place a lower limit of more than 4 x 10(11) solar masses of dark and luminous matter in this region, consistent with that expected from cosmological simulations for the earliest galaxy clusters(4,5,7).
C1 [Capak, Peter L.; Yan, Lin] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Riechers, Dominik; Scoville, Nick Z.; Robertson, Brant] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Carilli, Chris] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Cox, Pierre; Neri, Roberto] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
[Salvato, Mara] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Schinnerer, Eva; Karim, Alexander] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Wilson, Grant W.; Yun, Min] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Civano, Francesca; Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Staguhn, Johannes G.] Johns Hopkins Univ, Lab Observat Cosmol, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Capak, PL (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM capak@astro.caltech.edu
OI Schinnerer, Eva/0000-0002-3933-7677
FU NASA; NSF
FX These results are based on observations with: the W. M. Keck
Observatory, the IRAM Plateau de Bure Interferometer, the IRAM 30-m
telescope with the GISMO 2-mm camera, the Chandra X-ray Observatory, the
Subaru Telescope, the Hubble Space Telescope, the Canada-France-Hawaii
Telescope with WIRCam and MegaPrime, the United Kingdom Infrared
Telescope, the Spitzer Space Telescope, the Smithsonian Submillimeter
Array Telescope, the James Clerk Maxwell Telescope with the AzTEC 1.1 mm
camera, and the National Radio Astronomy Observatory's Very Large Array.
D. R. and B. R. acknowledge support from NASA through Hubble Fellowship
grants awarded by the Space Telescope Science Institute. P. L. C. and
N.Z.S. acknowledge grant support from NASA. G. W. W., M.Y. and J.G.S.
acknowledge grant support from the NSF.
NR 28
TC 123
Z9 124
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 FEB 10
PY 2011
VL 470
IS 7333
BP 233
EP 235
DI 10.1038/nature09681
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 718RQ
UT WOS:000287144200038
PM 21228776
ER
PT J
AU Marcus, SL
de Viron, O
Dickey, JO
AF Marcus, Steven L.
de Viron, Olivier
Dickey, Jean O.
TI Abrupt atmospheric torque changes and their role in the 1976-1977
climate regime shift
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID PACIFIC DECADAL OSCILLATION; OCEAN RECHARGE MECHANISM; ANGULAR-MOMENTUM;
INTERDECADAL VARIABILITY; EQUATORIAL PACIFIC; MOUNTAIN TORQUE; NORTH
PACIFIC; DATA SET; FLUCTUATIONS; SIMULATIONS
AB During the climate regime/Pacific Decadal Oscillation (PDO) phase shift of 1976-1977, changes of up to several Hadleys occurred in the friction, mountain, and gravity wave torques that maintain the axial angular momentum (AAM) balance of the atmosphere. As required to produce a substantially different but stable climate regime, however, the total torque showed little net change (0.2 Hadley), while the AAM showed a modest increase, between the pretransition and posttransition periods in our data (1968-1975 and 1978-1997). The east-to-west transfer of atmospheric mass that occurs during the cold-to-warm phase shift of the PDO produced positive mountain torque anomalies on the atmosphere resulting from lower (higher) surface pressure to the west (east) of the Andes and Rockies (Himalayas), which were largely compensated by negative friction torque anomalies generated over the equatorial Pacific. The timing of events during the 1976-1977 transition window suggests that changes in low-latitude (Pacific friction and Andes mountains) torques and the PDO index in early to mid-1976 preceded changes in the extratropical torques during 1977, consistent with the poleward propagation of atmospheric zonal flow anomalies documented in previous studies. An increase in the global mean surface temperature and its rate of rise after the regime shift suggest that the negative friction torque anomalies that developed during the transition may have acted to sustain the warmer posttransition regime by suppressing cold-water upwelling in the eastern equatorial Pacific and/or equatorial thermocline heat content recharge processes in the central and western Pacific.
C1 [Marcus, Steven L.; Dickey, Jean O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[de Viron, Olivier] Univ Paris Diderot, F-75005 Paris, France.
[de Viron, Olivier] CNRS, Inst Phys Globe Paris, F-75005 Paris, France.
RP Marcus, SL (reprint author), CALTECH, Jet Prop Lab, Mail Stop 238-600,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM steven.marcus@jpl.nasa.gov
RI de Viron, Olivier/N-6647-2014;
OI de Viron, Olivier/0000-0003-3112-9686; Marcus,
Steven/0000-0002-5763-6961
FU NASA
FX We thank David Thompson (Colorado State University) and colleagues for
generously sharing their corrected global temperature data sets,
Xiaochun Wang and Josh Willis of JPL for useful discussions of oceanic
heat storage variations related to climate change, and two anonymous
reviewers whose comments helped to improve the manuscript. This paper
presents the results of one phase of research performed at the Jet
Propulsion Laboratory, California Institute of Technology, sponsored by
NASA. The contribution of O.d.V. to this study is IPGP contribution
3118.
NR 38
TC 6
Z9 7
U1 0
U2 12
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 FEB 9
PY 2011
VL 116
AR D03107
DI 10.1029/2010JD015032
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 720ZX
UT WOS:000287322300002
ER
PT J
AU Arvidson, RE
Ashley, JW
Bell, JF
Chojnacki, M
Cohen, J
Economou, TE
Farrand, WH
Fergason, R
Fleischer, I
Geissler, P
Gellert, R
Golombek, MP
Grotzinger, JP
Guinness, EA
Haberle, RM
Herkenhoff, KE
Herman, JA
Iagnemma, KD
Jolliff, BL
Johnson, JR
Klingelhofer, G
Knoll, AH
Knudson, AT
Li, R
McLennan, SM
Mittlefehldt, DW
Morris, RV
Parker, TJ
Rice, MS
Schroder, C
Soderblom, LA
Squyres, SW
Sullivan, RJ
Wolff, MJ
AF Arvidson, R. E.
Ashley, J. W.
Bell, J. F., III
Chojnacki, M.
Cohen, J.
Economou, T. E.
Farrand, W. H.
Fergason, R.
Fleischer, I.
Geissler, P.
Gellert, R.
Golombek, M. P.
Grotzinger, J. P.
Guinness, E. A.
Haberle, R. M.
Herkenhoff, K. E.
Herman, J. A.
Iagnemma, K. D.
Jolliff, B. L.
Johnson, J. R.
Klingelhoefer, G.
Knoll, A. H.
Knudson, A. T.
Li, R.
McLennan, S. M.
Mittlefehldt, D. W.
Morris, R. V.
Parker, T. J.
Rice, M. S.
Schroeder, C.
Soderblom, L. A.
Squyres, S. W.
Sullivan, R. J.
Wolff, M. J.
TI Opportunity Mars Rover mission: Overview and selected results from
Purgatory ripple to traverses to Endeavour crater
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MERIDIANI-PLANUM; AEOLIAN PROCESSES; BURNS FORMATION; EREBUS CRATER;
LANDING SITE; EXPLORATION; MINERALOGY; CHEMISTRY; APHELION; DEPOSITS
AB Opportunity has been traversing the Meridiani plains since 25 January 2004 (sol 1), acquiring numerous observations of the atmosphere, soils, and rocks. This paper provides an overview of key discoveries between sols 511 and 2300, complementing earlier papers covering results from the initial phases of the mission. Key new results include (1) atmospheric argon measurements that demonstrate the importance of atmospheric transport to and from the winter carbon dioxide polar ice caps; (2) observations showing that aeolian ripples covering the plains were generated by easterly winds during an epoch with enhanced Hadley cell circulation; (3) the discovery and characterization of cobbles and boulders that include iron and stony-iron meteorites and Martian impact ejecta; (4) measurements of wall rock strata within Erebus and Victoria craters that provide compelling evidence of formation by aeolian sand deposition, with local reworking within ephemeral lakes; (5) determination that the stratigraphy exposed in the walls of Victoria and Endurance craters show an enrichment of chlorine and depletion of magnesium and sulfur with increasing depth. This result implies that regional-scale aqueous alteration took place before formation of these craters. Most recently, Opportunity has been traversing toward the ancient Endeavour crater. Orbital data show that clay minerals are exposed on its rim. Hydrated sulfate minerals are exposed in plains rocks adjacent to the rim, unlike the surfaces of plains outcrops observed thus far by Opportunity. With continued mechanical health, Opportunity will reach terrains on and around Endeavour's rim that will be markedly different from anything examined to date.
C1 [Arvidson, R. E.; Guinness, E. A.; Jolliff, B. L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Ashley, J. W.] Arizona State Univ, Sch Earth & Space Explorat, Mars Space Flight Facil, Tempe, AZ 85287 USA.
[Bell, J. F., III; Rice, M. S.; Squyres, S. W.; Sullivan, R. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Chojnacki, M.] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[Cohen, J.] Honeybee Robot Spacecraft Mech Corp, New York, NY 10001 USA.
[Economou, T. E.] Univ Chicago, Lab Astrophys & Space Res, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Farrand, W. H.; Wolff, M. J.] Space Sci Inst, Boulder, CO 80301 USA.
[Fergason, R.; Geissler, P.; Herkenhoff, K. E.; Johnson, J. R.; Soderblom, L. A.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Fleischer, I.; Klingelhoefer, G.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55099 Mainz, Germany.
[Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada.
[Golombek, M. P.; Herman, J. A.; Parker, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Haberle, R. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Iagnemma, K. D.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA.
[Knoll, A. H.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Knudson, A. T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Li, R.] Ohio State Univ, Dept Civil & Environm Engn, Columbus, OH 43210 USA.
[McLennan, S. M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
[Schroeder, C.] Univ Tubingen, Ctr Appl Geosci, D-72076 Tubingen, Germany.
[Schroeder, C.] Univ Bayreuth, Dept Hydrol, Bayreuth, Germany.
[Mittlefehldt, D. W.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Arvidson, RE (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
EM arvidson@rsmail.wustl.edu
RI Schroder, Christian/B-3870-2009; Chojnacki, Matthew/A-4245-2013;
Johnson, Jeffrey/F-3972-2015
OI Schroder, Christian/0000-0002-7935-6039; Chojnacki,
Matthew/0000-0001-8497-8994;
NR 61
TC 31
Z9 31
U1 1
U2 29
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 FEB 8
PY 2011
VL 116
AR E00F15
DI 10.1029/2010JE003746
PG 33
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 721AS
UT WOS:000287324400001
ER
PT J
AU Farrugia, CJ
Chen, LJ
Torbert, RB
Southwood, DJ
Cowley, SWH
Vrublevskis, A
Mouikis, C
Vaivads, A
Andre, M
Decreau, P
Vaith, H
Owen, CJ
Sibeck, DJ
Lucek, E
Smith, CW
AF Farrugia, C. J.
Chen, Li-Jen
Torbert, R. B.
Southwood, D. J.
Cowley, S. W. H.
Vrublevskis, A.
Mouikis, C.
Vaivads, A.
Andre, M.
Decreau, P.
Vaith, H.
Owen, C. J.
Sibeck, D. J.
Lucek, E.
Smith, C. W.
TI "Crater" flux transfer events: Highroad to the X line?
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID COLLISIONLESS MAGNETIC RECONNECTION; AMPTE-IRM OBSERVATIONS; EARTHS
MAGNETOPAUSE; ELECTRIC-FIELD; CLUSTER; INSTRUMENT; MAGNETOSPHERE;
ENVIRONMENT; SIGNATURE; PLASMA
AB We examine Cluster observations of a so-called magnetosphere "crater FTE," employing data from five instruments (FGM, CIS, EDI, EFW, and WHISPER), some at the highest resolution. The aim of doing this is to deepen our understanding of the reconnection nature of these events by applying recent advances in the theory of collisionless reconnection and in detailed observational work. Our data support the hypothesis of a stratified structure with regions which we show to be spatial structures. We support the bulge-like topology of the core region (R3) made up of plasma jetting transverse to reconnected field lines. We document encounters with a magnetic separatrix as a thin layer embedded in the region (R2) just outside the bulge, where the speed of the protons flowing approximately parallel to the field maximizes: (1) short (fraction of a sec) bursts of enhanced electric field strengths (up to similar to 30 mV/m) and (2) electrons flowing against the field toward the X line at approximately the same time as the bursts of intense electric fields. R2 also contains a density decrease concomitant with an enhanced magnetic field strength. At its interface with the core region, R3, electric field activity ceases abruptly. The accelerated plasma flow profile has a catenary shape consisting of beams parallel to the field in R2 close to the R2/R3 boundary and slower jets moving across the magnetic field within the bulge region. We detail commonalities our observations of crater FTEs have with reconnection structures in other scenarios. We suggest that in view of these properties and their frequency of occurrence, crater FTEs are ideal places to study processes at the separatrices, key regions in magnetic reconnection. This is a good preparation for the MMS mission.
C1 [Farrugia, C. J.; Chen, Li-Jen; Torbert, R. B.; Mouikis, C.; Vaith, H.; Smith, C. W.] Univ New Hampshire, Dept Phys, Ctr Space Sci, Durham, NH 03824 USA.
[Southwood, D. J.] ESA Headquarters, F-75738 Paris, France.
[Cowley, S. W. H.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Vrublevskis, A.] MIT, Plasma Sci & Fus Ctr, Cambridge, MA 02142 USA.
[Vaivads, A.; Andre, M.] Swedish Inst Space Phys, SE-75121 Uppsala, Sweden.
[Decreau, P.] CNRS, LPCE2, F-45071 Orleans, France.
[Lucek, E.] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2BW, England.
[Owen, C. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Sibeck, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Farrugia, CJ (reprint author), Univ New Hampshire, Dept Phys, Ctr Space Sci, 39 Coll Rd,Morse Hall,Rm 414, Durham, NH 03824 USA.
EM charlie.farrugia@unh.edu
RI Owen, Christopher/C-2999-2008; Chen, Li-Jen/C-2106-2012; Sibeck,
David/D-4424-2012
OI Owen, Christopher/0000-0002-5982-4667;
FU NASA [NNX08AD11G, NNG06GD41G]
FX We are very grateful to the referees for their helpful suggestions. Part
of this work was done while A. V. was doing summer work at UNH. This
work is supported by NASA grants NNX08AD11G and NNG06GD41G and by NASA
Cluster grant to UNH.
NR 57
TC 5
Z9 5
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB 8
PY 2011
VL 116
AR A02204
DI 10.1029/2010JA015495
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 721BC
UT WOS:000287325400001
ER
PT J
AU Turtle, EP
Del Genio, AD
Barbara, JM
Perry, JE
Schaller, EL
McEwen, AS
West, RA
Ray, TL
AF Turtle, E. P.
Del Genio, A. D.
Barbara, J. M.
Perry, J. E.
Schaller, E. L.
McEwen, A. S.
West, R. A.
Ray, T. L.
TI Seasonal changes in Titan's meteorology
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GENERAL-CIRCULATION; CLOUDS; ATMOSPHERE; MODEL; WINDS
AB The Cassini Imaging Science Subsystem has observed Titan for similar to 1/4 Titan year, and we report here the first evidence of seasonal shifts in preferred locations of tropospheric methane clouds. South-polar convective cloud activity, common in late southern summer, has become rare. North-polar and northern mid-latitude clouds appeared during the approach to the northern spring equinox in August 2009. Recent observations have shown extensive cloud systems at low latitudes. In contrast, southern mid-latitude and subtropical clouds have appeared sporadically throughout the mission, exhibiting little seasonality to date. These differences in behavior suggest that Titan's clouds, and thus its general circulation, are influenced by both the rapid temperature response of a low-thermal-inertia surface and the much longer radiative timescale of Titan's cold thick troposphere. North-polar clouds are often seen near lakes and seas, suggesting that local increases in methane concentration and/or lifting generated by surface roughness gradients may promote cloud formation. Citation: Turtle, E. P., A. D. Del Genio, J. M. Barbara, J. E. Perry, E. L. Schaller, A. S. McEwen, R. A. West, and T. L. Ray (2011), Seasonal changes in Titan's meteorology, Geophys. Res. Lett., 38, L03203, doi:10.1029/2010GL046266.
C1 [Turtle, E. P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[West, R. A.; Ray, T. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Perry, J. E.; Schaller, E. L.; McEwen, A. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Del Genio, A. D.; Barbara, J. M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Turtle, EP (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM elizabeth.turtle@jhuapl.edu
RI Del Genio, Anthony/D-4663-2012; Turtle, Elizabeth/K-8673-2012
OI Del Genio, Anthony/0000-0001-7450-1359; Turtle,
Elizabeth/0000-0003-1423-5751
FU NASA; ESA; ASI
FX The authors wish to express their sincere gratitude to all who have
worked to make the Cassini-Huygens mission possible and to two anonymous
reviewers for their helpful suggestions. Research was supported by the
Cassini-Huygens mission, a cooperative endeavor of NASA, ESA, and ASI
managed by JPL/Caltech under a contract with NASA.
NR 22
TC 41
Z9 41
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 8
PY 2011
VL 38
AR L03203
DI 10.1029/2010GL046266
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 720ZK
UT WOS:000287321000004
ER
PT J
AU Ivins, ER
Watkins, MM
Yuan, DN
Dietrich, R
Casassa, G
Rulke, A
AF Ivins, Erik R.
Watkins, Michael M.
Yuan, Dah-Ning
Dietrich, Reinhard
Casassa, Gino
Ruelke, Axel
TI On-land ice loss and glacial isostatic adjustment at the Drake Passage:
2003-2009
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID PENINSULA SUMMER TEMPERATURES; HEMISPHERE ANNULAR MODE; TIME-VARIABLE
GRAVITY; ANTARCTIC PENINSULA; CLIMATE-CHANGE; BRANSFIELD STRAIT;
SATELLITE GRAVITY; LATE HOLOCENE; MASS CHANGES; GRACE
AB Land glacier extent and volume at the northern and southern margins of the Drake Passage have been in a state of dramatic demise since the early 1990s. Here time-varying space gravity observations from the Gravity Recovery and Climate Experiment (GRACE) are combined with Global Positioning System (GPS) bedrock uplift data to simultaneously solve for ice loss and for solid Earth glacial isostatic adjustment (GIA) to Little Ice Age (LIA) cryospheric loading. The present-day ice loss rates are determined to be -26 +/- 6 Gt/yr and -41.5 +/- 9 Gt/yr in the Southern and Northern Patagonia Ice Fields (NPI+SPI) and Antarctic Peninsula (AP), respectively. These are consistent with estimates based upon thickness and flux changes. Bounds are recovered for elastic lithosphere thicknesses of 35 <= h <= 70 km and 20 <= h <= 45 km and for upper mantle viscosities of 4-8 x 10(18) Pa s and 3-10 x 10(19) Pa s (using a half-space approximation) for NPI+SPI and AP, respectively, using an iterative forward model strategy. Antarctic Peninsula ice models with a prolonged LIA, extending to A. D. 1930, are favored in all chi(2) fits to the GPS uplift data. This result is largely decoupled from Earth structure assumptions. The GIA corrections account for roughly 20-60% of the space-determined secular gravity change. Collectively, the on-land ice losses correspond to volume increases of the oceans equivalent to 0.19 +/- 0.045 mm/yr of sea level rise for the last 15 years.
C1 [Ivins, Erik R.; Watkins, Michael M.; Yuan, Dah-Ning] CALTECH, Jet Prop Lab, Oceans Climate & Solid Earth Sect, Pasadena, CA 91109 USA.
[Dietrich, Reinhard] Tech Univ Dresden, Inst Planetare Geodasie, D-01069 Dresden, Germany.
[Casassa, Gino] Ctr Estudios Cient, Valdivia 514, Chile.
[Ruelke, Axel] Bundesamt Kartog & Geodasie, D-04105 Leipzig, Germany.
RP Ivins, ER (reprint author), CALTECH, Jet Prop Lab, Oceans Climate & Solid Earth Sect, Mail Stop 300-233,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM erik.r.ivins@jpl.nasa.gov
FU NASA as part of the GRACE Science Team; International Bureau of the BMBF
(Germany); Chilean Government through the Millennium Science Initiative;
Conicyt; Centro de Estudios Cientificos (CECS)
FX This research was supported by NASA's Earth Surface and Interior Focus
Area as part of the GRACE Science Team effort and was performed at the
Jet Propulsion Laboratory, California Institute of Technology. Parts of
this research were supported by the International Bureau of the BMBF
(Germany) and by the Chilean Government through the Millennium Science
Initiative and the Centers of Excellence Base Financing Program of
Conicyt which fund and the Centro de Estudios Cientificos (CECS). We
thank Michael Bentley, David Bromwich, Ben Chao, Eugene Domack, Tom
James, Matt King, Felix Landerer, Eric Rignot, Riccardo Riva,
Christopher Shuman, Alexander Simms, Xiaoping Wu, and Victor Zlotnicki
for their insight and helpful comments. Many of the figures in this
paper were created using GMT open software [Wessel and Smith, 1995].
NR 98
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U1 0
U2 10
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 FEB 8
PY 2011
VL 116
AR B02403
DI 10.1029/2010JB007607
PG 24
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 721AW
UT WOS:000287324800001
ER
PT J
AU Leuko, S
Neilan, BA
Burns, BP
Walter, MR
Rothschild, LJ
AF Leuko, S.
Neilan, B. A.
Burns, B. P.
Walter, M. R.
Rothschild, L. J.
TI Molecular assessment of UVC radiation-induced DNA damage repair in the
stromatolitic halophilic archaeon, Halococcus hamelinensis
SO JOURNAL OF PHOTOCHEMISTRY AND PHOTOBIOLOGY B-BIOLOGY
LA English
DT Article
DE Halophilic archaea; DNA damage; Repair mechanisms; UVC radiation;
Astrobiology
ID HALOBACTERIUM SPECIES NRC-1; NUCLEOTIDE EXCISION-REPAIR;
ULTRAVIOLET-RADIATION; CYANOBACTERIA; PROTEIN; ARCHAEBACTERIA;
DESICCATION; ENVIRONMENT; PHOTOLYASE; AUSTRALIA
AB The halophilic archaeon Halococcus hamelinensis was isolated from living stromatolites in Shark Bay, Western Australia, that are known to be exposed to extreme conditions of salinity, desiccation, and UV radiation. Modern stromatolites are considered analogues of very early life on Earth and thus inhabitants of modern stromatolites, and Hcc. hamelinensis in particular, are excellent candidates to examine responses to high UV radiation. This organism was exposed to high dosages (up to 500 J/m(2)) of standard germicidal UVC (254 nm) radiation and overall responses such as survival, thymine-thymine cyclobutane pyrimidine dimer formation, and DNA repair have been assessed. Results show that Hcc. hamelinensis is able to survive high UVC radiation dosages and that intact cells give an increased level of DNA protection over purified DNA. The organism was screened for the bacterial-like nucleotide excision repair (NER) genes uvrA, uvrB, uvrC, as well as for the photolyase phr2 gene. All four genes were discovered and changes in the expression levels of those genes during repair in either light or dark were investigated by means of quantitative Real-Time (qRT) PCR. The data obtained and presented in this study show that the uvrA, uvrB, and uvrC genes were up-regulated during both repair conditions. The photolyase phr2 was not induced during dark repair, yet showed a 20-fold increase during repair in light conditions. The data presented is the first molecular study of different repair mechanisms in the genus Halococcus following exposure to high UVC radiation levels. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Leuko, S.; Rothschild, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Neilan, B. A.; Burns, B. P.] Univ New S Wales, Sch Biotechnol & Biomol Sci, Sydney, NSW 2052, Australia.
[Neilan, B. A.; Burns, B. P.; Walter, M. R.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia.
RP Leuko, S (reprint author), Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2M7, Canada.
EM leuko@ualberta.ca; b.neilan@unsw.edu.au; brendan.burns@unsw.edu.au;
malcolm.walter@unsw.edu.au; lynn.j.rothschild@nasa.gov
RI BURNS, BRENDAN/B-5093-2009;
OI BURNS, BRENDAN/0000-0002-2962-2597
FU NASA
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the NASA Ames Research Center, administered by Oak Ridge
Associated Universities through a contract with NASA. Parts of funding
were obtained from a NASA Planetary Biology Internship. The authors also
like to thank two anonymous reviewers for their helpful comments and
suggestions to improve this manuscript.
NR 46
TC 5
Z9 6
U1 1
U2 16
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 1011-1344
J9 J PHOTOCH PHOTOBIO B
JI J. Photochem. Photobiol. B-Biol.
PD FEB 7
PY 2011
VL 102
IS 2
BP 140
EP 145
DI 10.1016/j.jphotobiol.2010.10.002
PG 6
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA 717VR
UT WOS:000287076000007
PM 21074452
ER
PT J
AU Keesee, AM
Buzulukova, N
Goldstein, J
McComas, DJ
Scime, EE
Spence, H
Fok, MC
Tallaksen, K
AF Keesee, A. M.
Buzulukova, N.
Goldstein, J.
McComas, D. J.
Scime, E. E.
Spence, H.
Fok, M-C.
Tallaksen, K.
TI Remote observations of ion temperatures in the quiet time magnetosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SOLAR-WIND CONTROL; PLASMA SHEET; RING CURRENT; SPACECRAFT; DENSITY;
IMAGES; MODEL
AB Ion temperature analysis of the first energetic neutral atom images of the quiet-time, extended magnetosphere provides evidence of multiple regions of ion heating. This study confirms the existence of a dawn-dusk asymmetry in ion temperature predicted for quiescent magnetospheric conditions by Spence and Kivelson (1993) and demonstrates that it is an inherent magnetospheric feature. Citation: Keesee, A. M., N. Buzulukova, J. Goldstein, D. J. McComas, E. E. Scime, H. Spence, M.-C. Fok, and K. Tallaksen (2011), Remote observations of ion temperatures in the quiet time magnetosphere, Geophys. Res. Lett., 38, L03104, doi: 10.1029/2010GL045987.
C1 [Keesee, A. M.; Scime, E. E.; Tallaksen, K.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[Buzulukova, N.; Fok, M-C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Goldstein, J.; McComas, D. J.] SW Res Inst, San Antonio, TX 78238 USA.
[Goldstein, J.; McComas, D. J.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA.
[Spence, H.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
RP Keesee, AM (reprint author), W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
EM amy.keesee@mail.wvu.edu; natalia.y.buzulukova@nasa.gov;
jerry.goldstein@swri.edu; dmccomas@swri.edu; escime@wvu.edu;
harlan.spence@unh.edu; mei-ching.h.fok@nasa.gov; ktallaks@mix.wvu.edu
RI Fok, Mei-Ching/D-1626-2012; Spence, Harlan/A-1942-2011; Keesee,
Amy/J-8194-2014;
OI Keesee, Amy/0000-0002-9719-3229; Spence, Harlan/0000-0002-2526-2205
FU WVU
FX This work was carried out as a part of the TWINS NASA Explorer mission;
work at WVU was supported under subcontract to the Southwest Research
Institute.
NR 19
TC 14
Z9 14
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 5
PY 2011
VL 38
AR L03104
DI 10.1029/2010GL045987
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 717JD
UT WOS:000287038600002
ER
PT J
AU Famiglietti, JS
Lo, M
Ho, SL
Bethune, J
Anderson, KJ
Syed, TH
Swenson, SC
de Linage, CR
Rodell, M
AF Famiglietti, J. S.
Lo, M.
Ho, S. L.
Bethune, J.
Anderson, K. J.
Syed, T. H.
Swenson, S. C.
de Linage, C. R.
Rodell, M.
TI Satellites measure recent rates of groundwater depletion in California's
Central Valley
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LAND-SURFACE MODEL; GRACE MEASUREMENTS; ASSIMILATION; STORAGE; SYSTEM;
BASIN
AB In highly-productive agricultural areas such as California's Central Valley, where groundwater often supplies the bulk of the water required for irrigation, quantifying rates of groundwater depletion remains a challenge owing to a lack of monitoring infrastructure and the absence of water use reporting requirements. Here we use 78 months (October, 2003-March, 2010) of data from the Gravity Recovery and Climate Experiment satellite mission to estimate water storage changes in California's Sacramento and San Joaquin River Basins. We find that the basins are losing water at a rate of 31.0 +/- 2.7 mm yr(-1) equivalent water height, equal to a volume of 30.9 km(3) for the study period, or nearly the capacity of Lake Mead, the largest reservoir in the United States. We use additional observations and hydrological model information to determine that the majority of these losses are due to groundwater depletion in the Central Valley. Our results show that the Central Valley lost 20.4 +/- 3.9 mm yr(-1) of groundwater during the 78-month period, or 20.3 km(3) in volume. Continued groundwater depletion at this rate may well be unsustainable, with potentially dire consequences for the economic and food security of the United States. Citation: Famiglietti, J. S., M. Lo, S. L. Ho, J. Bethune, K. J. Anderson, T. H. Syed, S. C. Swenson, C. R. de Linage, and M. Rodell (2011), Satellites measure recent rates of groundwater depletion in California's Central Valley, Geophys. Res. Lett., 38, L03403, doi: 10.1029/2010GL046442.
C1 [Famiglietti, J. S.; Lo, M.] Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA 92697 USA.
[Famiglietti, J. S.; Lo, M.; Ho, S. L.; Anderson, K. J.; Syed, T. H.; de Linage, C. R.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Ho, S. L.] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA.
[Bethune, J.] Carleton Coll, Dept Geol, Northfield, MN 55057 USA.
[Syed, T. H.] Indian Sch Mines, Dept Appl Geol, Dhanbad 826004, Bihar, India.
[Swenson, S. C.] Natl Ctr Atmospher Res, Climate & Global Dynam Div, Boulder, CO 80307 USA.
[Rodell, M.] NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Famiglietti, JS (reprint author), Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA 92697 USA.
EM jfamigli@uci.edu
RI Rodell, Matthew/E-4946-2012; Syed, Tajdarul/G-6731-2014;
OI Rodell, Matthew/0000-0003-0106-7437; LO, MIN-HUI/0000-0002-8653-143X
FU NASA
FX This research was funded by grants from NASA's GRACE Science Team,
Terrestrial Hydrology and Earth and Space Sciences fellowship program.
Claudia Faunt of the U. S. Geological Survey provided critical datasets
used in this work. We thank Q. Tang at the University of Washington for
providing evapotranspiration data.
NR 21
TC 189
Z9 196
U1 8
U2 123
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 FEB 5
PY 2011
VL 38
AR L03403
DI 10.1029/2010GL046442
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 717JD
UT WOS:000287038600008
ER
PT J
AU Cheek, LC
Pieters, CM
Boardman, JW
Clark, RN
Combe, JP
Head, JW
Isaacson, PJ
McCord, TB
Moriarty, D
Nettles, JW
Petro, NE
Sunshine, JM
Taylor, LA
AF Cheek, L. C.
Pieters, C. M.
Boardman, J. W.
Clark, R. N.
Combe, J. P.
Head, J. W.
Isaacson, P. J.
McCord, T. B.
Moriarty, D.
Nettles, J. W.
Petro, N. E.
Sunshine, J. M.
Taylor, L. A.
TI Goldschmidt crater and the Moon's north polar region: Results from the
Moon Mineralogy Mapper (M-3)
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID LUNAR MARE VOLCANISM; REFLECTANCE SPECTRA; SURFACE; SPECTROSCOPY;
PROSPECTOR
AB Soils within the impact crater Goldschmidt have been identified as spectrally distinct from the local highland material. High spatial and spectral resolution data from the Moon Mineralogy Mapper (M-3) on the Chandrayaan-1 orbiter are used to examine the character of Goldschmidt crater in detail. Spectral parameters applied to a north polar mosaic of M-3 data are used to discern large-scale compositional trends at the northern high latitudes, and spectra from three widely separated regions are compared to spectra from Goldschmidt. The results highlight the compositional diversity of the lunar nearside, in particular, where feldspathic soils with a low-Ca pyroxene component are pervasive, but exclusively feldspathic regions and small areas of basaltic composition are also observed. Additionally, we find that the relative strengths of the diagnostic OH/H2O absorption feature near 3000 nm are correlated with the mineralogy of the host material. On both global and local scales, the strongest hydrous absorptions occur on the more feldspathic surfaces. Thus, M-3 data suggest that while the feldspathic soils within Goldschmidt crater are enhanced in OH/H2O compared to the relatively mafic nearside polar highlands, their hydration signatures are similar to those observed in the feldspathic highlands on the farside.
C1 [Cheek, L. C.; Pieters, C. M.; Head, J. W.; Isaacson, P. J.; Moriarty, D.; Nettles, J. W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Boardman, J. W.] Analyt Imaging & Geophys LLC, Boulder, CO 80305 USA.
[Clark, R. N.] US Geol Survey, Fed Ctr, Denver, CO 80225 USA.
[Combe, J. P.; McCord, T. B.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Petro, N. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sunshine, J. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Taylor, L. A.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
RP Cheek, LC (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA.
EM leah_cheek@brown.edu; boardman@aigllc.com; rclark@usgs.gov;
mccordtb@bearfightinstitute.com; noah.e.petro@mail.nasa.gov;
jess@astro.umd.edu; lataylor@utk.edu
RI Petro, Noah/F-5340-2013
FU NASA [NNM05AB26C]; NASA LSI at Brown University [NNA09DB34A]
FX The authors thank B. Ray Hawke and an anonymous reviewer for helpful
comments that improved that quality and clarity of the manuscript.
Support for this analysis was provided through the NASA Discovery
program. M3 science validation is supported through NASA
contract NNM05AB26C. Partial funding for this analysis has also been
provided through NASA LSI at Brown University under contract NNA09DB34A.
Thanks are extended to James Dickson for assistance in figure
preparation. The M3 team is grateful to ISRO for the
opportunity to fly as a guest instrument on Chandrayaan-1.
NR 44
TC 7
Z9 8
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-PLANET
JI J. Geophys. Res.-Planets
PD FEB 4
PY 2011
VL 116
AR E00G02
DI 10.1029/2010JE003702
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 717HB
UT WOS:000287033200001
ER
PT J
AU Dong, XQ
Xi, BK
Kennedy, A
Feng, Z
Entin, JK
Houser, PR
Schiffer, RA
L'Ecuyer, T
Olson, WS
Hsu, KL
Liu, WT
Lin, B
Deng, Y
Jiang, TY
AF Dong, Xiquan
Xi, Baike
Kennedy, Aaron
Feng, Zhe
Entin, Jared K.
Houser, Paul R.
Schiffer, Robert A.
L'Ecuyer, Tristan
Olson, William S.
Hsu, Kuo-lin
Liu, W. Timothy
Lin, Bing
Deng, Yi
Jiang, Tianyu
TI Investigation of the 2006 drought and 2007 flood extremes at the
Southern Great Plains through an integrative analysis of observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MIDLATITUDE CONTINENTAL CLOUDS; NORTHERN-HEMISPHERE WINTER; SGP CENTRAL
FACILITY; TRMM PERSPECTIVE; ENERGY BUDGET; PART II; CLIMATOLOGY;
RADIATION; AMERICA; TEMPERATURE
AB Hydrological years 2006 (HY06; October 2005 to September 2006) and 2007 (HY07; October 2006 to September 2007) provide a unique opportunity to examine hydrological extremes in the central United States because there are no other examples of two such highly contrasting precipitation extremes occurring in consecutive years at the Southern Great Plains (SGP) in recorded history. The HY06 annual precipitation in the state of Oklahoma, as observed by the Oklahoma Mesonet, is around 61% of the normal (92.84 cm, based on the 1921-2008 climatology), which results in HY06 as the second-driest year in the record. In particular, the total precipitation during the winter of 2005-2006 is only 27% of the normal, and this winter ranks as the driest season. On the other hand, the HY07 annual precipitation amount is 121% of the normal, and HY07 ranks as the seventh-wettest year for the entire state and the wettest year for the central region of the state. Summer 2007 is the second-wettest season for the state. Large-scale dynamics play a key role in these extreme events. During the extreme dry period (11/2005-02/2006), a dipole pattern in the 500 hPa geopotential height anomaly existed where an anomalous high was over the southwestern U.S. region and an anomalous low was over the Great Lakes. This pattern is associated with inhibited moisture transport from the Gulf of Mexico and strong sinking motion over the SGP, both contributing to the extreme dryness. The precipitation deficit over the SGP during the extreme dry period is clearly linked to significantly suppressed cyclonic activity over the southwestern United States, which shows a robust relationship with the western Pacific teleconnection pattern. The precipitation events during the extreme wet period (May-July 2007) were initially generated by active synoptic weather patterns, linked with moisture transport from the Gulf of Mexico by the northward low-level jet, and enhanced the frequency of thunderstorms and their associated latent heat release. Although the drought and pluvial conditions are dominated by large-scale dynamic patterns, we have found two possible positive feedback processes during the extreme dry and wet periods in this study that play key certain roles to maintain and reinforce the length and severity of existing drought and flood events. For example, during the extreme dry period, with less clouds, liquid water path, precipitable water vapor, precipitation, and thinner Cu cloud thickness, more net radiation was absorbed and used to evaporate water from the ground. The evaporated moisture, however, was removed by low-level divergence. Thus, with less precipitation and removed atmospheric moisture, more absorbed incoming solar radiation was used to increase surface temperature and to make the ground drier.
C1 [Dong, Xiquan; Xi, Baike; Kennedy, Aaron; Feng, Zhe] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
[Deng, Yi; Jiang, Tianyu] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Entin, Jared K.] NASA Headquarters, Div Earth Sci, Sci Mission Directorate, Washington, DC 20546 USA.
[Houser, Paul R.] George Mason Univ, Dept Geog & Geoinformat Sci, Fairfax, VA 22030 USA.
[Hsu, Kuo-lin] Univ Calif Irvine, Ctr Hydrometeorol & Remote Sensing, Irvine, CA 92697 USA.
[L'Ecuyer, Tristan] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Lin, Bing] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schiffer, Robert A.; Olson, William S.] Univ Maryland Baltimore Cty, GEST Ctr, Baltimore, MD 21250 USA.
[Hsu, Kuo-lin] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA.
RP Dong, XQ (reprint author), Univ N Dakota, Dept Atmospher Sci, 4149 Univ Ave,Stop 9006, Grand Forks, ND 58202 USA.
EM dong@aero.und.edu
RI Deng, Yi/K-6664-2012; Feng, Zhe/D-9531-2013; L'Ecuyer,
Tristan/C-7040-2013; Houser, Paul/J-9515-2013; L'Ecuyer,
Tristan/E-5607-2012; Feng, Zhe/E-1877-2015;
OI Houser, Paul/0000-0002-2991-0441; L'Ecuyer, Tristan/0000-0002-7584-4836;
Feng, Zhe/0000-0002-7540-9017; Dong, Xiquan/0000-0002-3359-6117
FU U.S. Department of Energy Office of Energy Research, Office of Health
and Environmental Research, Environmental Sciences Division; NASA; NEWS
[NNX07AW05G]; NASA CERES [NNL04AA11G]; NASA NEWS [NNX09AJ36G]
FX Surface data and Oklahoma Mesonet precipitation were obtained from the
Atmospheric Radiation Measurement Program sponsored by the U.S.
Department of Energy Office of Energy Research, Office of Health and
Environmental Research, Environmental Sciences Division. This research
was primarily supported by the NASA Energy and Water Cycle Study (NEWS)
project managed by Jared Entin. Authors from the University of North
Dakota were supported by the NEWS project under grant NNX07AW05G and
supported by the NASA CERES project under grant NNL04AA11G. Authors from
the Georgia Institute of Technology were supported by NASA NEWS under
grant NNX09AJ36G.
NR 32
TC 25
Z9 25
U1 2
U2 13
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 FEB 4
PY 2011
VL 116
AR D03204
DI 10.1029/2010JD014776
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 717FW
UT WOS:000287030000001
ER
PT J
AU Lu, YJ
Meyyappan, M
Li, J
AF Lu, Yijiang
Meyyappan, M.
Li, Jing
TI A carbon-nanotube-based sensor array for formaldehyde detection
SO NANOTECHNOLOGY
LA English
DT Article
ID NIO THIN-FILM; CHEMICAL SENSOR; ELECTRONIC NOSE; GAS SENSORS
AB We have fabricated a sensor array consisting of 32 sensor elements with pristine, doped and metal-loaded single-wall carbon nanotubes as sensing materials. The sensor elements consist of interdigitated electrodes with varying finger widths and gaps. The chemiresistor-type sensors provide a significant response to formaldehyde at concentrations down to 10 ppb in air with rapid response and recovery times.
C1 [Lu, Yijiang; Meyyappan, M.; Li, Jing] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Li, J (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Jing.Li-1@nasa.gov
FU NASA Ames UARC
FX YL is with Eloret Corp., supported through a subcontract from NASA Ames
UARC, managed by the University of California Santa Cruz.
NR 20
TC 9
Z9 10
U1 4
U2 37
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD FEB 4
PY 2011
VL 22
IS 5
AR 055502
DI 10.1088/0957-4484/22/5/055502
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 698GI
UT WOS:000285581600013
PM 21178257
ER
PT J
AU Yamada, T
Yamada, H
Lohn, AJ
Kobayashi, NP
AF Yamada, Toshishige
Yamada, Hidenori
Lohn, Andrew J.
Kobayashi, Nobuhiko P.
TI Room-temperature Coulomb staircase in semiconducting InP nanowires
modulated with light illumination
SO NANOTECHNOLOGY
LA English
DT Article
ID QUANTUM-DOT; TRANSISTOR; DIRECTION; EPITAXY; SYSTEM; GROWTH; FILMS
AB Detailed electron transport analysis is performed for an ensemble of conical indium phosphide nanowires bridging two hydrogenated n(+)-silicon electrodes. The current-voltage (I-V) characteristics exhibit a Coulomb staircase in the dark with a period of similar to 1 V at room temperature. The staircase is found to disappear under light illumination. This observation can be explained by assuming the presence of a tiny Coulomb island, and its existence is possible due to the large surface depletion region created within contributing nanowires. Electrons tunnel in and out of the Coulomb island, resulting in the Coulomb staircase I-V. Applying light illumination raises the electron quasi-Fermi level and the tunneling barriers are buried, causing the Coulomb staircase to disappear.
C1 [Yamada, Toshishige] Santa Clara Univ, Ctr Nanostruct, Sch Engn, Santa Clara, CA 95053 USA.
[Yamada, Toshishige; Lohn, Andrew J.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Dept Elect Engn, Santa Cruz, CA 95064 USA.
[Yamada, Hidenori] Univ Calif San Diego, Dept Elect & Comp Engn, San Diego, CA 92092 USA.
[Lohn, Andrew J.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, NECTAR, Adv Studies Labs, Santa Cruz, CA 95064 USA.
[Lohn, Andrew J.; Kobayashi, Nobuhiko P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Yamada, T (reprint author), Santa Clara Univ, Ctr Nanostruct, Sch Engn, Santa Clara, CA 95053 USA.
EM tyamada@scu.edu
RI Yamada, Toshishige/E-7834-2012; Yamada, Hidenori/E-8884-2012; Kobayashi,
Nobuhiko/E-3834-2012
OI Yamada, Toshishige/0000-0001-7145-9212;
NR 33
TC 5
Z9 5
U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD FEB 4
PY 2011
VL 22
IS 5
AR 055201
DI 10.1088/0957-4484/22/5/055201
PG 7
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 698GI
UT WOS:000285581600003
PM 21178228
ER
PT J
AU Giacomazzo, B
Rezzolla, L
Baiotti, L
AF Giacomazzo, Bruno
Rezzolla, Luciano
Baiotti, Luca
TI Accurate evolutions of inspiralling and magnetized neutron stars:
Equal-mass binaries
SO PHYSICAL REVIEW D
LA English
DT Article
ID GENERAL-RELATIVISTIC MAGNETOHYDRODYNAMICS; KELVIN-HELMHOLTZ INSTABILITY;
BAR-MODE INSTABILITY; BLACK-HOLE; NUMERICAL RELATIVITY; SIMULATIONS;
PERTURBATIONS; SPACETIMES; SCHEMES
AB By performing new, long and numerically accurate general-relativistic simulations of magnetized, equal-mass neutron-star binaries, we investigate the role that realistic magnetic fields may have in the evolution of these systems. In particular, we study the evolution of the magnetic fields and show that they can influence the survival of the hypermassive neutron star produced at the merger by accelerating its collapse to a black hole. We also provide evidence that, even if purely poloidal initially, the magnetic fields produced in the tori surrounding the black hole have toroidal and poloidal components of equivalent strength. When estimating the possibility that magnetic fields could have an impact on the gravitational-wave signals emitted by these systems either during the inspiral or after the merger, we conclude that for realistic magnetic-field strengths B <= 10(12) G such effects could be detected, but only marginally, by detectors such as advanced LIGO or advanced Virgo. However, magnetically induced modifications could become detectable in the case of small-mass binaries and with the development of gravitational-wave detectors, such as the Einstein Telescope, with much higher sensitivities at frequencies larger than approximate to 2 kHz.
C1 [Giacomazzo, Bruno] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Giacomazzo, Bruno] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Giacomazzo, Bruno; Rezzolla, Luciano] Albert Einstein Inst, Max Planck Inst Gravitat Phy, Potsdam, Germany.
[Rezzolla, Luciano] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Baiotti, Luca] Osaka Univ, Inst Laser Engn, Osaka, Japan.
RP Giacomazzo, B (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RI Giacomazzo, Bruno/I-8088-2012
OI Giacomazzo, Bruno/0000-0002-6947-4023
FU DFG [SFB/Transregio 7]; European Science Foundation; JSPS [19-07803];
MEXT [22740163]; NASA [NNX09AI75G]
FX We thank the developers of LORENE for providing us with initial data,
and those of CACTUS and CARPET for the numerical infrastructures used by
WHISKY. Useful input from J. Read, C. Reisswig, E. Schnetter, A. Tonita,
A. Vicere, and S. Yoshida is also acknowledged. We also thank M. Koppitz
for assisting us in the production of Fig. 1. The computations were
performed on the Damiana Cluster at the AEI, on QueenBee through LONI
(www.loni.org), and at the Texas Advanced Computing Center through
TERAGRID Allocation No. TG-MCA02N014. This work was supported in part by
the DFG Grant SFB/Transregio 7, by "CompStar," a Research Networking
Programme of the European Science Foundation, by the JSPS Grant-in-Aid
for Scientific Research (19-07803), by the MEXT Grant-in-Aid for Young
Scientists (22740163), and by NASA Grant No. NNX09AI75G.
NR 55
TC 70
Z9 70
U1 0
U2 0
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 FEB 4
PY 2011
VL 83
IS 4
AR 044014
DI 10.1103/PhysRevD.83.044014
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 716PC
UT WOS:000286984900002
ER
PT J
AU Carter, JA
Fabrycky, DC
Ragozzine, D
Holman, MJ
Quinn, SN
Latham, DW
Buchhave, LA
Van Cleve, J
Cochran, WD
Cote, MT
Endl, M
Ford, EB
Haas, MR
Jenkins, JM
Koch, DG
Li, J
Lissauer, JJ
MacQueen, PJ
Middour, CK
Orosz, JA
Rowe, JF
Steffen, JH
Welsh, WF
AF Carter, Joshua A.
Fabrycky, Daniel C.
Ragozzine, Darin
Holman, Matthew J.
Quinn, Samuel N.
Latham, David W.
Buchhave, Lars A.
Van Cleve, Jeffrey
Cochran, William D.
Cote, Miles T.
Endl, Michael
Ford, Eric B.
Haas, Michael R.
Jenkins, Jon M.
Koch, David G.
Li, Jie
Lissauer, Jack J.
MacQueen, Phillip J.
Middour, Christopher K.
Orosz, Jerome A.
Rowe, Jason F.
Steffen, Jason H.
Welsh, William F.
TI KOI-126: A Triply Eclipsing Hierarchical Triple with Two Low-Mass Stars
SO SCIENCE
LA English
DT Article
ID BINARY CM DRACONIS; MAGNETIC ACTIVITY; MAIN-SEQUENCE; EVOLUTION; MODELS;
SCIENCE; SYSTEMS; RADII
AB The Kepler spacecraft has been monitoring the light from 150,000 stars in its primary quest to detect transiting exoplanets. Here, we report on the detection of an eclipsing stellar hierarchical triple, identified in the Kepler photometry. KOI-126 [A, (B, C)], is composed of a low-mass binary [masses M(B) = 0.2413 +/- 0.0030 solar mass (M(circle dot)), M(C) = 0.2127 +/- 0.0026 M(circle dot); radii R(B) = 0.2543 +/- 0.0014 solar radius (R(circle dot)), R(C) = 0.2318 +/- 0.0013 R(circle dot); orbital period P(1) = 1.76713 +/- 0.00019 days] on an eccentric orbit about a third star (mass M(A) = 1.347 +/- 0.032 M(circle dot); radius R(A) = 2.0254 +/- 0.0098 R(circle dot); period of orbit around the low-mass binary P(2) = 33.9214 +/- 0.0013 days; eccentricity of that orbit e(2) = 0.3043 +/- 0.0024). The low-mass pair probe the poorly sampled fully convective stellar domain offering a crucial benchmark for theoretical stellar models.
C1 [Carter, Joshua A.; Ragozzine, Darin; Holman, Matthew J.; Quinn, Samuel N.; Latham, David W.; Buchhave, Lars A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Van Cleve, Jeffrey; Cote, Miles T.; Haas, Michael R.; Jenkins, Jon M.; Koch, David G.; Li, Jie; Lissauer, Jack J.; Middour, Christopher K.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, Austin, TX 78712 USA.
[Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA.
[Van Cleve, Jeffrey; Jenkins, Jon M.; Li, Jie; Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA.
[Lissauer, Jack J.] Stanford Univ, Stanford, CA 94305 USA.
[Orosz, Jerome A.; Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Middour, Christopher K.] Orbital Sci Corp, Dulles, VA 20166 USA.
RP Carter, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jacarter@cfa.harvard.edu
RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine,
Darin/C-4926-2013;
OI Buchhave, Lars A./0000-0003-1605-5666; Fabrycky,
Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA [HF-51267.01-A, HF-51272.01-A,
NAS 5-26555]
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. J.A.C. and D. C. F. are Hubble Fellows and acknowledge
support for this work by NASA through Hubble Fellowship grants
HF-51267.01-A and HF-51272.01-A awarded by the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., for NASA under contract NAS 5-26555. J.A.C.
is grateful for helpful discussions with P. Podsiadlowski, S. Rappaport,
G. Torres, A. Levine, J. Winn, S. Seager, and T. Dupuy. J. F. R. is a
NASA Postdoctoral Program Fellow.
NR 26
TC 106
Z9 107
U1 0
U2 2
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD FEB 4
PY 2011
VL 331
IS 6017
BP 562
EP 565
DI 10.1126/science.1201274
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 715ZE
UT WOS:000286933600047
PM 21224439
ER
PT J
AU Hansen, CJ
Bourke, M
Bridges, NT
Byrne, S
Colon, C
Diniega, S
Dundas, C
Herkenhoff, K
McEwen, A
Mellon, M
Portyankina, G
Thomas, N
AF Hansen, C. J.
Bourke, M.
Bridges, N. T.
Byrne, S.
Colon, C.
Diniega, S.
Dundas, C.
Herkenhoff, K.
McEwen, A.
Mellon, M.
Portyankina, G.
Thomas, N.
TI Seasonal Erosion and Restoration of Mars' Northern Polar Dunes
SO SCIENCE
LA English
DT Article
ID SUBLIMATION-DRIVEN ACTIVITY; HIRISE OBSERVATIONS; DEPOSITS
AB Despite radically different environmental conditions, terrestrial and martian dunes bear a strong resemblance, indicating that the basic processes of saltation and grainfall (sand avalanching down the dune slipface) operate on both worlds. Here, we show that martian dunes are subject to an additional modification process not found on Earth: springtime sublimation of Mars' CO2 seasonal polar caps. Numerous dunes in Mars' north polar region have experienced morphological changes within a Mars year, detected in images acquired by the High-Resolution Imaging Science Experiment on the Mars Reconnaissance Orbiter. Dunes show new alcoves, gullies, and dune apron extension. This is followed by remobilization of the fresh deposits by the wind, forming ripples and erasing gullies. The widespread nature of these rapid changes, and the pristine appearance of most dunes in the area, implicates active sand transport in the vast polar erg in Mars' current climate.
C1 [Hansen, C. J.; Bourke, M.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Bourke, M.] Univ Oxford, Sch Geog & Environm, Oxford OX1 3QY, England.
[Bridges, N. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Byrne, S.; Dundas, C.; McEwen, A.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Colon, C.] Rutgers State Univ, Dept Earth & Environm Sci, Newark, NJ 07102 USA.
[Diniega, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Herkenhoff, K.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Mellon, M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Portyankina, G.; Thomas, N.] Univ Bern, Space Res & Planetol Div, CH-0132 Bern, Switzerland.
RP Hansen, CJ (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA.
EM cjhansen@psi.edu
RI Byrne, Shane/B-8104-2012; Bourke, Mary/I-4387-2012; Mellon,
Michael/C-3456-2016; Bridges, Nathan/D-6341-2016;
OI Bourke, Mary/0000-0002-0424-0322; Dundas, Colin/0000-0003-2343-7224
FU Jet Propulsion Laboratory, California Institute of Technology; NASA
FX This work was partially supported by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA.
NR 32
TC 66
Z9 67
U1 6
U2 31
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD FEB 4
PY 2011
VL 331
IS 6017
BP 575
EP 578
DI 10.1126/science.1197636
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 715ZE
UT WOS:000286933600051
PM 21292976
ER
PT J
AU Behrangi, A
Khakbaz, B
Jaw, TC
AghaKouchak, A
Hsu, KL
Sorooshian, S
AF Behrangi, Ali
Khakbaz, Behnaz
Jaw, Tsou Chun
AghaKouchak, Amir
Hsu, Kuolin
Sorooshian, Soroosh
TI Hydrologic evaluation of satellite precipitation products over a
mid-size basin
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Precipitation estimation; Remote sensing; Hydrologic modeling;
Evaluation
ID RAINFALL-RUNOFF MODELS; GLOBAL PRECIPITATION; UNITED-STATES; ANALYSIS
TMPA; OPTIMIZATION; SYSTEM; INFORMATION; CALIBRATION; ALGORITHMS;
RESOLUTION
AB Since the past three decades a great deal of effort is devoted to development of satellite-based precipitation retrieval algorithms. More recently, several satellite-based precipitation products have emerged that provide uninterrupted precipitation time series with quasi-global coverage. These satellite-based precipitation products provide an unprecedented opportunity for hydrometeorological applications and climate studies. Although growing, the application of satellite data for hydrological applications is still very limited. In this study, the effectiveness of using satellite-based precipitation products for streamflow simulation at catchment scale is evaluated. Five satellite-based precipitation products (TMPA-RT, TMPA-V6, CMORPH, PERSIANN, and PERSIANN-adj) are used as forcing data for streamflow simulations at 6-h and monthly time scales during the period of 2003-2008. SACramento Soil Moisture Accounting (SAC-SMA) model is used for streamflow simulation over the mid-size Illinois River basin.
The results show that by employing the satellite-based precipitation forcing the general streamflow pattern is well captured at both 6-h and monthly time scales. However, satellites products, with no bias-adjustment being employed, significantly overestimate both precipitation inputs and simulated streamflows over warm months (spring and summer months). For cold season, on the other hand, the unadjusted precipitation products result in under-estimation of streamflow forecast. It was found that bias-adjustment of precipitation is critical and can yield to substantial improvement in capturing both streamflow pattern and magnitude. The results suggest that along with efforts to improve satellite-based precipitation estimation techniques, it is important to develop more effective near real-time precipitation bias adjustment techniques for hydrologic applications. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Behrangi, Ali] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Behrangi, Ali; Khakbaz, Behnaz; Jaw, Tsou Chun; AghaKouchak, Amir; Hsu, Kuolin; Sorooshian, Soroosh] Univ Calif Irvine, Dept Civil & Environm Engn, Henry Samueli Sch Engn, Ctr Hydrometeorol & Remote Sensing CHRS, Irvine, CA USA.
RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-301, Pasadena, CA 91109 USA.
EM Ali.Behrangi@jpl.nasa.gov
RI sorooshian, soroosh/B-3753-2008
OI sorooshian, soroosh/0000-0001-7774-5113
FU NASA [NNX08AU78H]; NASA-PMM [NNG04GC74G]; NSF STC for Sustainability of
Semi-Arid Hydrology and Riparian Areas (SAHRA) [EAR-9876800];
NOAA/NESDIS/NCDC [NA09NES4400006]; NCSU CICS [2009-1380-01]
FX Partial financial support was provided by NASA Earth and Space Science
Fellowship (NESSF award NNX08AU78H), NASA-PMM (Grant NNG04GC74G), NSF
STC for Sustainability of Semi-Arid Hydrology and Riparian Areas (SAHRA;
Grant EAR-9876800), NOAA/NESDIS/NCDC (prime award number NA09NES4400006,
NCSU CICS sub-award number 2009-1380-01). Part of the research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 42
TC 76
Z9 78
U1 5
U2 42
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
J9 J HYDROL
JI J. Hydrol.
PD FEB 3
PY 2011
VL 397
IS 3-4
BP 225
EP 237
DI 10.1016/j.jhydrol.2010.11.043
PG 13
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA 718IU
UT WOS:000287115300007
ER
PT J
AU Blewett, DT
Coman, EI
Hawke, BR
Gillis-Davis, JJ
Purucker, ME
Hughes, CG
AF Blewett, David T.
Coman, Ecaterina I.
Hawke, B. Ray
Gillis-Davis, Jeffrey J.
Purucker, Michael E.
Hughes, Christopher G.
TI Lunar swirls: Examining crustal magnetic anomalies and space weathering
trends
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID IMPACT BASINS; SOLAR-WIND; TITANIUM ABUNDANCE; MARE SOILS; MOON;
MERCURY; SURFACE; CLEMENTINE; PROSPECTOR; REGOLITH
AB We have used multispectral images from Clementine and data from Lunar Prospector's magnetometer to conduct a survey of lunar crustal magnetic anomalies, prominent lunar swirls, and lesser known swirl markings to provide new information on the nature of swirls and their association with magnetic anomalies. We find that all swirls and swirl-like albedo patterns are associated with areas of magnetized crust, but not all areas of magnetized crust are colocated with swirl-like albedo anomalies. All observed swirls exhibit spectral characteristics similar to immature material and generally have slightly lower FeO values compared with their surroundings as determined with a multispectral iron-mapping method. We discuss these results in relation to the various hypotheses for swirl formation. The comet impact hypothesis for lunar swirls would not predict a difference in the spectrally determined FeO content between swirls and nearby ordinary surfaces. The compositional difference could be explained as a consequence of (1) magnetic shielding of the surface from the solar wind, which could produce anomalous space weathering (little darkening with limited reddening) and potentially alter the predictions of the multispectral iron-mapping algorithm while the compositional contrast could be enhanced by delivery of lower-FeO ejecta from outside the swirl; and (2) accumulation of fine plagioclase-rich dust moving under the influence of electric fields induced by solar wind interactions with a magnetic anomaly. Therefore, we cannot at present clearly distinguish between the solar wind shielding and electrostatic dust accumulation models for swirl formation. We describe future measurements that could contribute to solution of the puzzle of swirl origin.
C1 [Blewett, David T.; Coman, Ecaterina I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Coman, Ecaterina I.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Hawke, B. Ray; Gillis-Davis, Jeffrey J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Purucker, Michael E.] NASA, Goddard Space Flight Ctr, Raytheon Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Hughes, Christopher G.] Univ Pittsburgh, Dept Geol & Planetary Sci, Pittsburgh, PA 15260 USA.
RP Blewett, DT (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM david.blewett@jhuapl.edu
RI Blewett, David/I-4904-2012
OI Blewett, David/0000-0002-9241-6358
FU NASA [NNX08AL53G, NNX09AQ06G]
FX This work made use of the "gridview" data manipulation tool, developed
by Jim Roark at NASA Goddard. We thank Chuck Wood for running the LPOD
website. Apollo and Lunar Orbiter images were obtained from the Lunar
and Planetary Institute web repository. Clementine image cubes were
retrieved from the U.S. Geological Survey's Map-A-Planet website. We
thank Nicola Richmond for contributions to an earlier phase of this
work. Financial support from the NASA Planetary Geology and Geophysics
program is gratefully acknowledged (grants NNX08AL53G and NNX09AQ06G to
D. T. B.). We appreciate the thorough reviews by Lon Hood and Sarah
Noble, which helped us to make major improvements to this paper. This is
HIGP publication 1872 and SOEST contribution 8025.
NR 127
TC 38
Z9 38
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD FEB 3
PY 2011
VL 116
AR E02002
DI 10.1029/2010JE003656
PG 30
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 717GX
UT WOS:000287032800001
ER
PT J
AU Rosenburg, MA
Aharonson, O
Head, JW
Kreslavsky, MA
Mazarico, E
Neumann, GA
Smith, DE
Torrence, MH
Zuber, MT
AF Rosenburg, M. A.
Aharonson, O.
Head, J. W.
Kreslavsky, M. A.
Mazarico, E.
Neumann, G. A.
Smith, D. E.
Torrence, M. H.
Zuber, M. T.
TI Global surface slopes and roughness of the Moon from the Lunar Orbiter
Laser Altimeter
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID KILOMETER-SCALE; MARS; STATISTICS; TOPOGRAPHY
AB The acquisition of new global elevation data from the Lunar Orbiter Laser Altimeter, carried on the Lunar Reconnaissance Orbiter, permits quantification of the surface roughness properties of the Moon at unprecedented scales and resolution. We map lunar surface roughness using a range of parameters: median absolute slope, both directional (along-track) and bidirectional (in two dimensions); median differential slope; and Hurst exponent, over baselines ranging from similar to 17 m to similar to 2.7 km. We find that the lunar highlands and the mare plains show vastly different roughness properties, with subtler variations within mare and highlands. Most of the surface exhibits fractal-like behavior, with a single or two different Hurst exponents over the given baseline range; when a transition exists, it typically occurs near the 1 km baseline, indicating a significant characteristic spatial scale for competing surface processes. The Hurst exponent is high within the lunar highlands, with a median value of 0.95, and lower in the maria (with a median value of 0.76). The median differential slope is a powerful tool for discriminating between roughness units and is useful in characterizing, among other things, the ejecta surrounding large basins, particularly Orientale, as well as the ray systems surrounding young, Copernican-age craters. In addition, it allows a quantitative exploration on mare surfaces of the evolution of surface roughness with age.
C1 [Rosenburg, M. A.; Aharonson, O.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Head, J. W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Kreslavsky, M. A.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Mazarico, E.; Neumann, G. A.; Smith, D. E.; Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Mazarico, E.; Neumann, G. A.; Smith, D. E.; Torrence, M. H.; Zuber, M. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Rosenburg, MA (reprint author), CALTECH, Div Geol & Planetary Sci, MC 150-21, Pasadena, CA 91125 USA.
EM megr@gps.caltech.edu
RI Kreslavsky, Mikhail/J-3425-2013; Neumann, Gregory/I-5591-2013; Mazarico,
Erwan/N-6034-2014;
OI Neumann, Gregory/0000-0003-0644-9944; Mazarico,
Erwan/0000-0003-3456-427X; Kreslavsky, Mikhail/0000-0002-1900-826X
FU NASA [NNX08AZ54G, NNG09EK06C:1]
FX The authors would like to acknowledge the LRO and LOLA engineering
teams, without whom the data presented here would not have been
possible. The research was partially funded by NASA grants NNX08AZ54G
and NNG09EK06C:1.
NR 25
TC 50
Z9 54
U1 0
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD FEB 3
PY 2011
VL 116
AR E02001
DI 10.1029/2010JE003716
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 717GX
UT WOS:000287032800002
ER
PT J
AU Liu, YQ
Brown, J
Demargne, J
Seo, DJ
AF Liu, Yuqiong
Brown, James
Demargne, Julie
Seo, Dong-Jun
TI A wavelet-based approach to assessing timing errors in hydrologic
predictions
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Timing errors; Magnitude errors; Cross wavelet transform; Hydrologic
evaluation; Forecast verification
ID RAINFALL-RUNOFF MODELS; NATIONAL-WEATHER-SERVICE; FORECAST VERIFICATION;
DATA ASSIMILATION; PARAMETER-ESTIMATION; IMPROVED CALIBRATION; CURVE
REGISTRATION; TIME-SERIES; STREAMFLOW; UNCERTAINTY
AB Streamflow predictions typically contain errors in both the timing and the magnitude of peak flows. These two types of error often originate from different sources (e.g. rainfall-runoff modeling vs. routing) and hence may have different implications and ramifications for both model diagnosis and decision support. Thus, where possible and relevant, they should be distinguished and separated in model evaluation and forecast verification applications. Distinct information on timing errors in hydrologic prediction could lead to more targeted model improvements in a diagnostic evaluation context, as well as better-informed decisions in many practical applications, such as flood prediction, water supply forecasting, river regulation, navigation, and engineering design. However, information on timing errors in hydrologic predictions is rarely evaluated or provided. In this paper, we discuss the importance of assessing and quantifying timing error in hydrologic predictions and present a new approach, which is based on the cross wavelet transform (XWT) technique. The XWT technique transforms the time series of predictions and corresponding observations into a two-dimensional time-scale space and provides information on scale- and time-dependent timing differences between the two time series. The results for synthetic timing errors (both constant and time-varying) indicate that the XWT-based approach can estimate timing errors in streamflow predictions with reasonable reliability. The approach is then employed to analyze the timing errors in real streamflow simulations for a number of headwater basins in the US state of Texas. The resulting timing error estimates were consistent with the physiographic and climatic characteristics of these basins. A simple post-factum timing adjustment based on these estimates led to considerably improved agreement between streamflow observations and simulations, further illustrating the potential for using the XWT-based approach for timing error estimation. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Liu, Yuqiong; Brown, James; Demargne, Julie] Natl Ocean & Atmospher Adm, Natl Weather Serv, Off Hydrol Dev, Silver Spring, MD 20910 USA.
[Liu, Yuqiong] Riverside Technol Inc, Ft Collins, CO 80525 USA.
[Brown, James; Demargne, Julie] Univ Corp Atmospher Res, Boulder, CO 80307 USA.
[Seo, Dong-Jun] Univ Texas Arlington, Dept Civil Engn, Arlington, TX 76019 USA.
RP Liu, YQ (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Yuqiong.Liu@nasa.gov
RI Liu, Yuqiong/B-4318-2012
FU National Weather Service (NWS); Climate Program Office (CPO) of the
National Oceanic and Atmospheric Administration (NOAA)
FX This work is supported by the Advanced Hydrologic Prediction Service
(AHPS) program of the National Weather Service (NWS) and the Climate
Predictions Program for the Americas (CPPA) of the Climate Program
Office (CPO) of the National Oceanic and Atmospheric Administration
(NOAA). Core wavelet analysis routines were provided by A. Grinsted and
are available at http://www.pol.ac.uk/home/research/waveletcoherence/.
The authors would like to thank Robert Corby and Paul McKee of the West
Gulf River Forecast Center of the US NWS for providing the basin map and
streamflow datasets. Comments from Pedro Restrepo, Geoff Bonnin, Haksu
Lee, and Gary Carter of the NWS Office of Hydrologic Development helped
to improve an earlier version of this paper. The authors would also like
to thank Alberto Viglione and an anonymous reviewer for their helpful
comments.
NR 65
TC 25
Z9 27
U1 5
U2 17
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
J9 J HYDROL
JI J. Hydrol.
PD FEB 3
PY 2011
VL 397
IS 3-4
BP 210
EP 224
DI 10.1016/j.jhydrol.2010.11.040
PG 15
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA 718IU
UT WOS:000287115300006
ER
PT J
AU Tobiska, WK
Crowley, G
Oh, SJ
Guhathakurta, M
AF Tobiska, W. Kent
Crowley, Geoff
Oh, Seung Jun
Guhathakurta, Madhulika
TI Space weather gets real-on smartphones (vol 9, S02001, 2011)
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Correction
C1 [Tobiska, W. Kent] Utah State Univ, Space Weather Ctr, Logan, UT 84322 USA.
[Crowley, Geoff] ASTRA, Boulder, CO USA.
[Oh, Seung Jun] Space Environm Lab, Seoul, South Korea.
[Guhathakurta, Madhulika] NASA, Sci Mission Directorate, Heliophys Div, Washington, DC 20546 USA.
RP Tobiska, WK (reprint author), Utah State Univ, Space Weather Ctr, Logan, UT 84322 USA.
EM ktobiska@spacenvironment.net
NR 1
TC 1
Z9 1
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD FEB 3
PY 2011
VL 9
AR S02001
DI 10.1029/2010SW000656
PG 1
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 717JK
UT WOS:000287039300001
ER
PT J
AU Lissauer, JJ
Fabrycky, DC
Ford, EB
Borucki, WJ
Fressin, F
Marcy, GW
Orosz, JA
Rowe, JF
Torres, G
Welsh, WF
Batalha, NM
Bryson, ST
Buchhave, LA
Caldwell, DA
Carter, JA
Charbonneau, D
Christiansen, JL
Cochran, W
Desert, JM
Dunham, EW
Fanelli, MN
Fortney, JJ
Gautier, TN
Geary, JC
Gilliland, RL
Haas, MR
Hall, JR
Holman, MJ
Koch, DG
Latham, DW
Lopez, E
McCauliff, S
Miller, N
Morehead, RC
Quintana, EV
Ragozzine, D
Sasselov, D
Short, DR
Steffen, JH
AF Lissauer, Jack J.
Fabrycky, Daniel C.
Ford, Eric B.
Borucki, William J.
Fressin, Francois
Marcy, Geoffrey W.
Orosz, Jerome A.
Rowe, Jason F.
Torres, Guillermo
Welsh, William F.
Batalha, Natalie M.
Bryson, Stephen T.
Buchhave, Lars A.
Caldwell, Douglas A.
Carter, Joshua A.
Charbonneau, David
Christiansen, Jessie L.
Cochran, WilliamD.
Desert, Jean-Michel
Dunham, Edward W.
Fanelli, Michael N.
Fortney, Jonathan J.
Gautier, Thomas N., III
Geary, John C.
Gilliland, Ronald L.
Haas, Michael R.
Hall, Jennifer R.
Holman, Matthew J.
Koch, David G.
Latham, David W.
Lopez, Eric
McCauliff, Sean
Miller, Neil
Morehead, Robert C.
Quintana, Elisa V.
Ragozzine, Darin
Sasselov, Dimitar
Short, Donald R.
Steffen, Jason H.
TI A closely packed system of low-mass, low-density planets transiting
Kepler-11
SO NATURE
LA English
DT Article
ID EXTRASOLAR PLANETS; SUPER-EARTHS; STARS; PERFORMANCE; EVAPORATION;
ISOCHRONES; DYNAMICS; NEPTUNES; JUPITERS; SCIENCE
AB When an extrasolar planet passes in front of (transits) its star, its radius can be measured from the decrease in starlight and its orbital period from the time between transits. Multiple planets transiting the same star reveal much more: period ratios determine stability and dynamics, mutual gravitational interactions reflect planet masses and orbital shapes, and the fraction of transiting planets observed as multiples has implications for the planarity of planetary systems. But few stars have more than one known transiting planet, and none has more than three. Here we report Kepler spacecraft observations of a single Sun-like star, which we call Kepler-11, that reveal six transiting planets, five with orbital periods between 10 and 47 days and a sixth planet with a longer period. The five inner planets are among the smallest for which mass and size have both been measured, and these measurements imply substantial envelopes of light gases. The degree of coplanarity and proximity of the planetary orbits imply energy dissipation near the end of planet formation.
C1 [Lissauer, Jack J.; Rowe, Jason F.; Caldwell, Douglas A.; Christiansen, Jessie L.; Quintana, Elisa V.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Fabrycky, Daniel C.; Fortney, Jonathan J.; Lopez, Eric; Miller, Neil] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Ford, Eric B.; Morehead, Robert C.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Fressin, Francois; Torres, Guillermo; Carter, Joshua A.; Charbonneau, David; Desert, Jean-Michel; Geary, John C.; Holman, Matthew J.; Latham, David W.; Ragozzine, Darin; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Orosz, Jerome A.; Welsh, William F.; Short, Donald R.] San Diego State Univ, San Diego, CA 92182 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Cochran, WilliamD.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Fanelli, Michael N.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hall, Jennifer R.; McCauliff, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
EM jack.lissauer@nasa.gov; fabrycky@ucolick.org
RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine,
Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Fortney,
Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666;
Fabrycky, Daniel/0000-0003-3750-0183
FU NASA [HF-51272.01-A, HF-51267.01-A]; STScl [NAS 5-26555]
FX Kepler was competitively selected as the tenth Discovery mission.
Funding for this mission is provided by NASA's Science Mission
Directorate. We thank the many people who gave so generously of their
time to make the Kepler mission a success. A. Dobrovolskis, T. J. Lee
and D. Queloz provided constructive comments on the manuscript. D.C.F.
and J.A.C. acknowledge NASA support through Hubble Fellowship grants
HF-51272.01-A and HF-51267.01-A, respectively, awarded by STScl,
operated by AURA under contract NAS 5-26555.
NR 35
TC 338
Z9 338
U1 2
U2 20
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD FEB 3
PY 2011
VL 470
IS 7332
BP 53
EP 58
DI 10.1038/nature09760
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 715LQ
UT WOS:000286886400032
PM 21293371
ER
PT J
AU Bunderson, LD
Van de Water, P
Luvall, J
Levetin, E
AF Bunderson, L. D.
Van de Water, P.
Luvall, J.
Levetin, E.
TI Northern New Mexico Spring Pollen Levels
SO JOURNAL OF ALLERGY AND CLINICAL IMMUNOLOGY
LA English
DT Meeting Abstract
CT American-Academy-of-Allergy-Asthma-and-Immunology Annual Meeting
CY MAR 18-22, 2011
CL San Francisco, CA
SP Amer Acad Allergy Asthma & Immunol
C1 [Bunderson, L. D.; Levetin, E.] Univ Tulsa, Tulsa, OK 74104 USA.
[Van de Water, P.] Fresno State Univ, Fresno, CA USA.
[Luvall, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
NR 0
TC 0
Z9 0
U1 0
U2 2
PU MOSBY-ELSEVIER
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0091-6749
J9 J ALLERGY CLIN IMMUN
JI J. Allergy Clin. Immunol.
PD FEB
PY 2011
VL 127
IS 2
SU S
BP AB169
EP AB169
DI 10.1016/j.jaci.2010.12.673
PG 1
WC Allergy; Immunology
SC Allergy; Immunology
GA 832YI
UT WOS:000295846400655
ER
PT J
AU Levetin, E
Bunderson, L
Van de Water, P
Luvall, JC
AF Levetin, E.
Bunderson, L.
Van de Water, P.
Luvall, J. C.
TI Aerobiology of Juniperus ashei Pollen in Texas and Oklahoma
SO JOURNAL OF ALLERGY AND CLINICAL IMMUNOLOGY
LA English
DT Meeting Abstract
CT American-Academy-of-Allergy-Asthma-and-Immunology Annual Meeting
CY MAR 18-22, 2011
CL San Francisco, CA
SP Amer Acad Allergy Asthma & Immunol
C1 [Levetin, E.; Bunderson, L.] Univ Tulsa, Tulsa, OK 74104 USA.
[Van de Water, P.] Calif State Univ Fresno, Fresno, CA 93740 USA.
[Luvall, J. C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
NR 0
TC 0
Z9 0
U1 0
U2 3
PU MOSBY-ELSEVIER
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0091-6749
J9 J ALLERGY CLIN IMMUN
JI J. Allergy Clin. Immunol.
PD FEB
PY 2011
VL 127
IS 2
SU S
BP AB170
EP AB170
DI 10.1016/j.jaci.2010.12.674
PG 1
WC Allergy; Immunology
SC Allergy; Immunology
GA 832YI
UT WOS:000295846400656
ER
PT J
AU Luvall, JC
Sprigg, W
Levetin, E
Huete, A
Nickovic, S
Pejanovic, G
Van de Water, P
Myers, O
Budge, A
Crimmins, T
Krapfl, H
Zelicoff, A
AF Luvall, J. C.
Sprigg, W.
Levetin, E.
Huete, A.
Nickovic, S.
Pejanovic, G.
Van de Water, P.
Myers, O.
Budge, A.
Crimmins, T.
Krapfl, H.
Zelicoff, A.
TI Use of MODIS Satellite Images and an Atmospheric Dust Transport Model To
Evaluate Juniperus Spp. Pollen Phenology and Dispersal to Support Public
Health Alerts
SO JOURNAL OF ALLERGY AND CLINICAL IMMUNOLOGY
LA English
DT Meeting Abstract
CT American-Academy-of-Allergy-Asthma-and-Immunology Annual Meeting
CY MAR 18-22, 2011
CL San Francisco, CA
SP Amer Acad Allergy Asthma & Immunol
C1 [Luvall, J. C.] NASA Marshall Space Flight Ctr, Huntsville, AL USA.
[Sprigg, W.; Huete, A.; Nickovic, S.; Pejanovic, G.] Univ Arizona, Tucson, AZ USA.
[Levetin, E.] Univ Tulsa, Tulsa, OK 74104 USA.
[Van de Water, P.] Calif State Univ Fresno, Fresno, CA 93740 USA.
[Myers, O.; Budge, A.] Univ New Mexico, Albuquerque, NM 87131 USA.
[Crimmins, T.] Univ Arizona, Natl Phenol Network, Tucson, AZ USA.
[Krapfl, H.] New Mexico Dept Hlth, Albuquerque, NM USA.
[Zelicoff, A.] Ares Corp, Albuquerque, NM USA.
NR 0
TC 2
Z9 2
U1 2
U2 10
PU MOSBY-ELSEVIER
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0091-6749
J9 J ALLERGY CLIN IMMUN
JI J. Allergy Clin. Immunol.
PD FEB
PY 2011
VL 127
IS 2
SU S
BP AB19
EP AB19
DI 10.1016/j.jaci.2010.12.086
PG 1
WC Allergy; Immunology
SC Allergy; Immunology
GA 832YI
UT WOS:000295846400070
ER
PT J
AU Kimura, Y
Nuth, JA
Johnson, NM
Farmer, KD
Roberts, KP
Hussaini, SR
AF Kimura, Yuki
Nuth, Joseph A., III
Johnson, Natasha M.
Farmer, Kevin D.
Roberts, Kenneth P.
Hussaini, Syed R.
TI Synthesis of Stacked-Cup Carbon Nanotubes in a Metal Free Low
Temperature System
SO NANOSCIENCE AND NANOTECHNOLOGY LETTERS
LA English
DT Article
DE Nanotube; Electron Microscopes; Fischer-Tropsch Type Reaction
ID SOLAR NEBULA; INTERSTELLAR DIAMONDS; GRAPHITE WHISKERS;
ORGANIC-MOLECULES; VAPOR-PHASE; GROWTH; GRAINS; METEORITES; CATALYST;
ENVIRONMENTS
AB Stacked-cup carbon nanotubes were formed by either Fischer-Tropsch type or Haber-Bosch type reactions in a metal free system. Graphite particles were used as the catalyst. The samples were heated at 600 degrees C in a gas mixture of CO 75 Torr, N-2 75 Torr and H-2 550 Torr for three days. Transmission electron microscope analysis of the catalyst surface at the completion of the experiment recognized the growth of nanotubes. They were 10-50 nm in diameter and similar to 1 mu m in length. They had a hollow channel of 5-20 nm in the center. The nanotubes may have grown on graphite surfaces by the CO disproportionation reaction and the surface tension of the carbon nucleus may have determined the diameter. Although, generally, the diameter of a carbon nanotube depends on the size of the catalytic particles, the diameter of the nanotubes on graphite particles was independent of the particle size and significantly confined within a narrow range compared with that produced using catalytic amorphous iron-silicate nanoparticles. Therefore, they must have an unknown formation process that is different than the generally accepted mechanism.
C1 [Kimura, Yuki] Tohoku Univ, Dept Earth & Planetary Mat Sci, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Kimura, Yuki; Nuth, Joseph A., III; Johnson, Natasha M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Farmer, Kevin D.; Roberts, Kenneth P.; Hussaini, Syed R.] Univ Tulsa, Dept Chem & Biochem, Tulsa, OK 74104 USA.
RP Kimura, Y (reprint author), Tohoku Univ, Dept Earth & Planetary Mat Sci, Grad Sch Sci, Aoba Ku, Aoba 6-3, Sendai, Miyagi 9808578, Japan.
RI Johnson, Natasha/E-3093-2012; Nuth, Joseph/E-7085-2012; Kimura,
Yuki/J-9635-2014
OI Kimura, Yuki/0000-0002-9218-7663
FU Nanotechnology Network of the MEXT, Japan; Tohoku University; Tohoku
University, Japan; NASA EPSCoR
FX Adrian J. Brearley and Ying-Bing Jiang provided technical support for
TEM analysis at the University of New Mexico. The TEM observations were
also performed as part of the Nanotechnology Support Project in Central
Japan (Institute for Molecular Science), supported financially by the
Nanotechnology Network of the MEXT, Japan. This work was also supported
in part by Tohoku University GCOE program for "Global Education and
Research Center for Earth and Planetary Dynamics," Culture and by the
"Program Research" in the Center for Interdisciplinary Research, Tohoku
University, Japan. Formation of the samples was supported by NASA's
Cosmochemistry Research and Analysis Program. We thank Richard Portman
for providing technical support for SEM analysis at the Department of
Biological Sciences, University of Tulsa. Hussaini, Roberts and Farmer
appreciate the financial support provide by the NASA EPSCoR Research
Initiation Grant.
NR 37
TC 1
Z9 1
U1 2
U2 9
PU AMER SCIENTIFIC PUBLISHERS
PI VALENCIA
PA 26650 THE OLD RD, STE 208, VALENCIA, CA 91381-0751 USA
SN 1941-4900
EI 1941-4919
J9 NANOSCI NANOTECH LET
JI Nanosci. Nanotechnol. Lett.
PD FEB
PY 2011
VL 3
IS 1
SI SI
BP 4
EP 10
DI 10.1166/nnl.2011.1111
PG 7
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 798MK
UT WOS:000293211200002
ER
PT J
AU Badavi, FF
Blattnig, SR
Atwell, W
Nealy, JE
Norman, RB
AF Badavi, Francis F.
Blattnig, Steve R.
Atwell, William
Nealy, John E.
Norman, Ryan B.
TI A deterministic electron, photon, proton and heavy ion transport suite
for the study of the Jovian moon Europa
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article
DE CEPTRN; HZETRN; TID; Jupiter; Galileo; Europa
AB A Langley research center (LaRC) developed deterministic suite of radiation transport codes describing the propagation of electron, photon, proton and heavy ion in condensed media is used to simulate the exposure from the spectral distribution of the aforementioned particles in the Jovian radiation environment. Based on the measurements by the Galileo probe (1995-2003) heavy ion counter (HIC), the choice of trapped heavy ions is limited to carbon, oxygen and sulfur (COS). The deterministic particle transport suite consists of a coupled electron photon algorithm (CEPTRN) and a coupled light heavy ion algorithm (HZETRN). The primary purpose for the development of the transport suite is to provide a means to the spacecraft design community to rapidly perform numerous repetitive calculations essential for electron, photon, proton and heavy ion exposure assessment in a complex space structure. In this paper, the reference radiation environment of the Galilean satellite Europa is used as a representative boundary condition to show the capabilities of the transport suite. While the transport suite can directly access the output electron and proton spectra of the Jovian environment as generated by the jet propulsion laboratory (JPL) Galileo interim radiation electron (GIRE) model of 2003; for the sake of relevance to the upcoming Europa Jupiter system mission (EJSM), the JPL provided Europa mission fluence spectrum, is used to produce the corresponding depth dose curve in silicon behind a default aluminum shield of 100 mils (similar to 0.7 g/cm(2)). The transport suite can also accept a geometry describing ray traced thickness file from a computer aided design (CAD) package and calculate the total ionizing dose (TID) at a specific target point within the interior of the vehicle. In that regard, using a low fidelity CAD model of the Galileo probe generated by the authors, the transport suite was verified versus Monte Carlo (MC) simulation for orbits JOI-J35 of the Galileo probe extended mission. For the upcoming EJSM mission with an expected launch date of 2020, the transport suite is used to compute the depth dose profile for the traditional aluminum silicon as a standard shield target combination, as well as simulating the shielding response of a high charge number (Z) material such as tantalum (Ta). Finally, a shield optimization algorithm is discussed which can guide the instrument designers and fabrication personnel with the choice of graded-Z shield selection and analysis. Published by Elsevier B.V.
C1 [Badavi, Francis F.; Norman, Ryan B.] NASA Langley Res Ctr, NASA Postdoctoral Program Fellow, Hampton, VA 23681 USA.
[Badavi, Francis F.] Christopher Newport Univ, OSP, Newport News, VA 23606 USA.
[Atwell, William] Boeing Co, Res & Technol, Space Explorat, Houston, TX 77059 USA.
[Nealy, John E.] Old Dominion Univ, Norfolk, VA 23529 USA.
RP Badavi, FF (reprint author), NASA Langley Res Ctr, NASA Postdoctoral Program Fellow, MS 188E, Hampton, VA 23681 USA.
EM francis.f.badavi@nasa.gov; steve.r.blattnig@nasa.gov;
william.atwell@boeing.com; John.e.nealy@nasa.gov; ryan.b.norman@nasa.gov
RI Norman, Ryan/D-5095-2017
OI Norman, Ryan/0000-0002-9103-7225
NR 18
TC 5
Z9 5
U1 0
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD FEB 1
PY 2011
VL 269
IS 3
BP 232
EP 238
DI 10.1016/j.nimb.2010.12.022
PG 7
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 796FK
UT WOS:000293037000006
ER
PT J
AU St Dennis, JE
Venkataraman, P
He, JB
John, VT
Obrey, SJ
Currier, RP
Lebron-Colon, M
Sola, FJ
Meador, MA
AF St Dennis, J. E.
Venkataraman, Pradeep
He, Jibao
John, Vijay T.
Obrey, Stephen J.
Currier, Robert P.
Lebron-Colon, Marisabel
Sola, Francisco J.
Meador, Michael A.
TI Rod-like carbon nanostructures produced by the direct pyrolysis of
alpha-cyclodextrin
SO CARBON
LA English
DT Article
ID NANOTUBES
AB Carbon nanostructures were produced by the direct pyrolysis of a cyclic glucose oligosaccharide (alpha-cyclodextrin) without the use of a metal catalyst. The nanorods evolve from surfaces of structureless carbon when the precursor is carbonized at 1000 degrees C. The conversion of initially-obtained featureless carbon to the nanostructures can be controlled by the pyrolysis time. The nanorods are of diameters 14-10 nm and consist of multiple disordered curved graphite layers with relatively short persistence lengths. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [St Dennis, J. E.; Venkataraman, Pradeep; John, Vijay T.] Tulane Univ, Dept Chem & Biomol Engn, New Orleans, LA 70118 USA.
[He, Jibao] Tulane Univ, Coordinated Instrument Facil, New Orleans, LA 70118 USA.
[Obrey, Stephen J.; Currier, Robert P.] Los Alamos Natl Lab, Div Chem, Los Alamos, NM 87545 USA.
[Lebron-Colon, Marisabel; Sola, Francisco J.; Meador, Michael A.] NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
RP John, VT (reprint author), Tulane Univ, Dept Chem & Biomol Engn, 6823 St Charles Ave, New Orleans, LA 70118 USA.
EM vj@tulane.edu
RI John, Vijay/G-3747-2010; VENKATARAMAN, PRADEEP/A-8648-2013;
VENKATARAMAN, PRADEEP/P-6058-2014
OI VENKATARAMAN, PRADEEP/0000-0001-9679-229X
FU Department of Energy [DOE-DE-FG02-05ER46243]; Advanced Materials
Research Institute of the University of New Orleans through the PKSFI
program; Louisiana Board of Regents, BoRSF
FX Funding from Department of Energy (DOE-DE-FG02-05ER46243) is gratefully
acknowledged for this work. Additional funding was provided by the
Advanced Materials Research Institute of the University of New Orleans
through the PKSFI program. J. St. Dennis acknowledges a Graduate
Fellowship from the Louisiana Board of Regents, BoRSF, under agreement
NASA/LEQSF(2005-2010)-LaSPACE and NASA/LaSPACE.
NR 12
TC 5
Z9 5
U1 2
U2 25
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0008-6223
J9 CARBON
JI Carbon
PD FEB
PY 2011
VL 49
IS 2
BP 718
EP 722
DI 10.1016/j.carbon.2010.09.027
PG 5
WC Chemistry, Physical; Materials Science, Multidisciplinary
SC Chemistry; Materials Science
GA 699KQ
UT WOS:000285662700044
ER
PT J
AU Billings, L
AF Billings, Linda
TI A call for proactive xenoarchaeological guidelines: A response to Ben
McGee
SO SPACE POLICY
LA English
DT Article
C1 [Billings, Linda] George Washington Univ, Sch Media & Publ Affairs, Washington, DC 20052 USA.
[Billings, Linda] NASA, Astrobiol Program, Washington, DC USA.
RP Billings, L (reprint author), George Washington Univ, Sch Media & Publ Affairs, Washington, DC 20052 USA.
EM libillin@gwu.edu
NR 26
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 0265-9646
J9 SPACE POLICY
JI Space Policy
PD FEB
PY 2011
VL 27
IS 1
BP 53
EP 56
DI 10.1016/j.spacepol.2010.11.001
PG 4
WC International Relations; Social Sciences, Interdisciplinary
SC International Relations; Social Sciences - Other Topics
GA 762VY
UT WOS:000290510800012
ER
PT J
AU Sun, WY
Min, KH
Chern, JD
AF Sun, Wen-Yih
Min, Ki-Hong
Chern, Jiun-Dar
TI Numerical Study of 1998 Late Summer Flood in East Asia
SO ASIA-PACIFIC JOURNAL OF ATMOSPHERIC SCIENCES
LA English
DT Article
DE Regional climate; heavy precipitation; baroclinic wave; East-Asian
summer monsoon
ID REGIONAL CLIMATE MODEL; INTERNAL GRAVITY-WAVES; CUMULUS CONVECTION;
INTEGRATION SCHEME; SURROUNDING AREA; SIMULATION; PARAMETERIZATION;
MONSOON; PRECIPITATION; VERIFICATION
AB The Purdue Regional Model (PRM) is applied to study the evolution of regional climate and weather systems during the heavy precipitation over Korea and China between 30 July and 18 August 1998. The results show that heavy rainfall along the Mei-yu and Changma front was due to the combination of: (1) an anomalous 850 hPa subtropical high, (2) a stronger baroclinicity around 40 degrees N over eastern Asia and a low pressure located to the north of the front, and (3) an excessive evaporation from abnormal wet, warm land. The precipitation ended by 18 August when the subtropical high had retreated and the low pressure in Mongolia moved away from Asia continent. The model reproduced in great detail the observed baroclinic waves to the north, subtropical high and low-level jet to the south, and the front with heavy precipitation extending from southern China, and the Korean peninsula to Japan. High correlations are found for mass, momentum, and moisture fields between model simulation and the European Center for Medium Range Weather Forecast (ECMWF) reanalysis for the 20-day means.
C1 [Sun, Wen-Yih; Min, Ki-Hong] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
[Chern, Jiun-Dar] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Sun, Wen-Yih] Natl Cent Univ, Dept Atmospher Sci, Chungli, Taiwan.
RP Min, KH (reprint author), Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
EM min@purdue.edu
OI Min, Ki-Hong/0000-0001-6133-6040
FU Taiwan Science Council
FX We thank W. R. Hsu, H. H. Hsu, W. S. Kuo, and Y. C. Yu at National
Taiwan University and D.-K. Lee at Seoul National University for useful
discussions, and B. MacCall at Purdue University for proof reading. Part
of this work was supported by Taiwan Science Council when the author
Wen-Yih Sun took a sabbatical leave at the National Taiwan University.
We appreciate two anonymous reviewers and the editor for their valuable
comments and suggestions.
NR 39
TC 11
Z9 11
U1 0
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1976-7633
J9 ASIA-PAC J ATMOS SCI
JI Asia-Pac. J. Atmos. Sci.
PD FEB
PY 2011
VL 47
IS 2
BP 123
EP 135
DI 10.1007/s13143-011-0003-1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 759HS
UT WOS:000290231900003
ER
PT J
AU Nickolaenko, AP
Kudintseva, IG
Pechonaya, O
Hayakawa, M
Nakamura, T
Hobara, Y
Tanaka, Y
AF Nickolaenko, A. P.
Kudintseva, I. G.
Pechonaya, O.
Hayakawa, M.
Nakamura, T.
Hobara, Ya.
Tanaka, Ya.
TI IMPACT OF A GAMMA-RAY BURST ON THE SCHUMANN RESONANCE
SO RADIOPHYSICS AND QUANTUM ELECTRONICS
LA English
DT Article
ID IONOSPHERE; SGR-1806-20; ENERGY; MODELS; FLARE
AB We compare the experimental and simulated data on the impact of an extragalactic gamma-ray burst of December 27, 2004 on the global electromagnetic resonance. It is known from measurements of the signals of ultralong-wave radio stations that the ionizing radiation descended the ionosphere over the dayside hemisphere by 20 km. Such a disturbance should change the eigenfrequencies of the Earth-ionosphere cavity and affect the shape of the observed spectrum of extremely low-frequency Earth's radio noise. The results of observations and modeling of the Schumann-resonance variation under the action of a gamma-ray burst are compared. We employ two models. In the simpler one, the ionospheric disturbance is averaged over the entire globe. The second model allows for the day-night nonuniformity. It is shown that both models yield similar predictions and the effect little depends on the day-night nonuniformity. Since the ionosphere carries the positive electric charge, its vertical displacement causes a current which serves as a "parametric" impulse source of the electromagnetic field. The global size of the source results in that the pulse contains only the lower Schumann-resonance frequency. The extremely low-frequency pulse coincides in time with the gamma-ray burst arrival. The results of observations in the Moshiri observatory (Japan) at the time of a gamma-ray burst, which are compared with the calculation for this observatory are presented. It is shown that both a modification of the Schumann resonance sonogram and a parametric extremely low-frequency radio pulse have been detected in the record.
C1 [Nickolaenko, A. P.] Ukrainean Natl Acad Sci, A Ya Usikov Inst Radiophys & Elect, Kharkov, Ukraine.
[Kudintseva, I. G.] VN Karazin Natl Univ Kharkov, Kharkov, Ukraine.
[Pechonaya, O.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Pechonaya, O.] Columbia Univ, New York, NY USA.
[Hayakawa, M.; Nakamura, T.; Hobara, Ya.] Univ Electrocommun, Tokyo, Japan.
[Tanaka, Ya.] Inst Space & Astronaut Sci, Kanagawa 229, Japan.
RP Nickolaenko, AP (reprint author), Ukrainean Natl Acad Sci, A Ya Usikov Inst Radiophys & Elect, Kharkov, Ukraine.
EM sasha@ire.kharkov.ua
NR 21
TC 3
Z9 3
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0033-8443
J9 RADIOPHYS QUANT EL+
JI Radiophys. Quantum Electron.
PD FEB
PY 2011
VL 53
IS 9-10
BP 542
EP 556
PG 15
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 759UI
UT WOS:000290273600004
ER
PT J
AU Ryan, RE
AF Ryan, Robert E.
TI Flight Operations in the New Millennium
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
AB New approaches are being studied for real-time Interaction, and related supporting processes, with spacecraft and instruments in deep-space. Spacecraft are evolving, improving In many ways, and generally, becoming more robust. Operations are changing also. Operations will be more automated In the future. However, there is a challenge. Deep-space missions are not all alike. The Operations phases of discovery and exploration are an extension of the research that creates the mission; they are the time of obtaining results.
This examines the historical role of flight operations, and Its evolving processes, to develop an understanding of the operational methods that will be effective In the future.
It takes people, equipment, software, space, and connectivity for Operations success. A balance has to be struck between improving technology, gaining knowledge, automation, and realistic expectations.
Finally, the recommended methods to gain efficiency In Operations are system-wide services and shared resources. These common processes will meet the challenge of varied missions.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ryan, RE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU National Aeronautics and Space Administration
FX The research described herein was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 2
TC 0
Z9 0
U1 1
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0885-8985
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD FEB
PY 2011
VL 26
IS 2
BP 42
EP 46
DI 10.1109/MAES.2011.5739489
PG 5
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA 739ZA
UT WOS:000288759600007
ER
PT J
AU Khan-Mayberry, N
James, JT
Tyl, R
Lam, CW
AF Khan-Mayberry, Noreen
James, John T.
Tyl, Rochelle
Lam, Chiu-wing
TI Space Toxicology: Protecting Human Health During Space Operations
SO INTERNATIONAL JOURNAL OF TOXICOLOGY
LA English
DT Article
DE spaceflight operations; space toxicology; human health; pulmonary
toxicity; exposure limits
ID INTRATRACHEAL INSTILLATION; LUNAR; ENVIRONMENT; EXPOSURE; TOXICITY;
DUSTS
AB Space toxicology is a unique and targeted discipline for spaceflight, space habitation, and occupation of celestial bodies including planets, moons, and asteroids. Astronaut explorers face distinctive health challenges and limited resources for rescue and medical care during space operation. A central goal of space toxicology is to protect the health of the astronaut by assessing potential chemical exposures during spaceflight and setting safe limits that will protect the astronaut against chemical exposures while in a physiologically altered state. In order to maintain sustained occupation in space on the International Space Station (ISS), toxicological risks must be assessed and managed within the context of isolation, continuous exposures, reuse of air and water, limited rescue options, and the need to use highly toxic compounds for propulsion and other purposes. As we begin to explore other celestial bodies, in situ toxicological risks, such as inhalation of reactive mineral dusts, must also be managed.
C1 [Khan-Mayberry, Noreen; James, John T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Tyl, Rochelle] RTI Int, Res Triangle Pk, NC USA.
[Lam, Chiu-wing] Wyle Labs, Houston, TX USA.
RP Khan-Mayberry, N (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM noreen.n.khan-mayberry@nasa.gov
FU National Aeronautics and Space Administration
FX The author(s) disclosed receipt of the following financial support for
the research and/or authorship of this article: the National Aeronautics
and Space Administration.
NR 45
TC 2
Z9 2
U1 0
U2 7
PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 1091-5818
J9 INT J TOXICOL
JI Int. J. Toxicol.
PD FEB
PY 2011
VL 30
IS 1
BP 3
EP 18
DI 10.1177/1091581810386389
PG 16
WC Pharmacology & Pharmacy; Toxicology
SC Pharmacology & Pharmacy; Toxicology
GA 733RJ
UT WOS:000288280200001
PM 21266660
ER
PT J
AU Liao, LA
Meneghini, R
AF Liao, Liang
Meneghini, Robert
TI A Study on the Feasibility of Dual-Wavelength Radar for Identification
of Hydrometeor Phases
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID MEASURING MISSION TRMM; POLARIMETRIC RADAR; PRECIPITATION RADAR; MELTING
LAYER; X-BAND; RAIN; SIZE; SNOW; PARAMETERS; PROFILES
AB An important objective for the dual-wavelength Ku-/Ka-band precipitation radar (DPR) that will be on board the Global Precipitation Measurement (GPM) core satellite is to identify the phase state of hydrometeors along the range direction. To assess this, radar signatures are simulated in snow and rain to explore the relation between the differential frequency ratio (DFR), defined as the difference of radar reflectivity factors between Ku and Ka bands, and the radar reflectivity factor at Ku band Z(Ku) for different hydrometeor types. Model simulations indicate that there is clear separation between snow and rain in the Z(Ku)-DFR plane assuming that the snow follows the Gunn Marshall size distribution and rain follows the Marshall-Palmer size distribution. In an effort to verify the simulated results, the data collected by the Airborne Second-Generation Precipitation Radar (APR-2) in the Wakasa Bay Advanced Microwave Scanning Radiometer for Earth Observing System (AMSR-E) campaign are employed. Using the signatures of linear depolarization ratio at Ku band, the APR-2 data can be easily divided into the regions of snow, mixed phase, and rain for stratiform storms. These results are then superimposed onto the theoretical curves computed from the model in the Z(Ku)-DFR plane. For over 90% of the observations from a cold-season stratiform precipitation event, snow and rain can be distinguished if the Ku-band radar reflectivity exceeds 18 dBZ (the minimum detectable level of the GPM DPR at Ku band). This is also the case for snow and mixed-phase hydrometeors. Although snow can be easily distinguished from rain and melting hydrometeors by using Ku- and Ka-band radar, the rain and mixed-phase particles are not always separable. It is concluded that Ku- and Ka-band dual-wavelength radar might provide a potential means to identify the phase state of hydrometeors.
C1 [Liao, Liang] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA.
[Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Liao, LA (reprint author), NASA GSFC, Goddard Earth Sci Technol UMBC, Code 613-1, Greenbelt, MD 20771 USA.
EM liang.liao-1@nasa.gov
RI Measurement, Global/C-4698-2015
FU NASA's Precipitation Measurement Mission (PMM) [NNH06ZDA001N-PMM]
FX The authors thank Dr. Eastwood Im and Dr. Simone Tanelli of the NASA Jet
Propulsion Laboratory for providing the APR-2 radar data and the
processing software. This work is supported by Dr. R. Kakar of NASA
Headquarters under NASA's Precipitation Measurement Mission (PMM) Grant
NNH06ZDA001N-PMM.
NR 32
TC 10
Z9 10
U1 0
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD FEB
PY 2011
VL 50
IS 2
BP 449
EP 456
DI 10.1175/2010JAMC2499.1
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 733ZZ
UT WOS:000288304300013
ER
PT J
AU Wang, CC
Huang, HL
Li, JL
Leou, TM
Chen, GTJ
AF Wang, Chung-Chieh
Huang, Hsiao-Ling
Li, Jui-Lin
Leou, Tzay-Ming
Chen, George Tai-Jen
TI An Evaluation of the Performance of the CWB NFS Model for Warm-Season
Rainfall Distribution and Propagation over the East Asian Continent
SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES
LA English
DT Article
DE Quantitative precipitation forecast; Warm season; Non-hydrostatic
forecast system; Model evaluation
ID BRIGHTNESS TEMPERATURE OBSERVATIONS; TAIWAN AREA; PRECIPITATION
FORECASTS; PREDICTION MODELS; DIURNAL-VARIATION; WESTERN PACIFIC;
EPISODES; GMS; VARIABILITY; CONVECTION
AB This study evaluates the performance of the regional operational model at Central Weather Bureau (CWB), the Non-hydrostatic Forecast System (NFS), in capturing the general distribution and eastward propagation of warm-season rainfall within the diurnal cycle in Hovmoller (longitude-time) space over the East Asian continent. The Tropical Rainfall Measuring Mission (TRMM) 0.25 degrees rain-rates are used to evaluate the NFS coarse domain (45 km) 12 - 36 h QPFs during May - August, 2002 - 2005 both qualitatively and quantitatively.
Our results show that the propagating rainfall signals to the lee of the Tibetan Plateau (TP) in the diurnal cycle, evident in TRMM data, are poorly captured in the NFS QPFs throughout the warm season, similar to earlier results in the United States. The nocturnal rainfall peak near the Sichuan Basin in the NFS is unclear, and the propagation is confined to a smaller region in May - June and almost missing entirely in mid-summer. Overall, the model QPFs exhibit largest disagreement with observations in June, and smallest in May.
There is a tendency for the NFS to over-predict rainfall in eastern TP. However, both the total amount and the diurnal-wave amplitude are under-predicted to the lee, where a lack of propagation signals also leads to increased phase error farther downstream. A persistent phase error (at least 7 h) is also found over 110 - 120 degrees E, with early morning maxima in the model but afternoon in TRMM data. Overall, the 1200 UTC model runs predict less rainfall compared to 0000 UTC runs, while the NFS also showed some improvements from 2002 to 2005 but the leeside propagation is still under-represented.
C1 [Wang, Chung-Chieh] Natl Taiwan Normal Univ, Dept Earth Sci, Taipei, Taiwan.
[Huang, Hsiao-Ling; Chen, George Tai-Jen] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10764, Taiwan.
[Li, Jui-Lin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Leou, Tzay-Ming] Cent Weather Bur, Taipei, Taiwan.
RP Wang, CC (reprint author), Natl Taiwan Normal Univ, Dept Earth Sci, Taipei, Taiwan.
EM cwang@ntnu.edu.tw
FU National Science Council of Taiwan [NSC-96-2111-M-002-010-MY3,
NSC-97-2111-M-003-005-MY2, NSC-99-2111-M-003-004-MY3,
NSC-99-2111-M-002-001]; National Taiwan University (NTU) [99R40044]
FX The authors wish to thank Dr. Mong-Ming Lu of the CWB and another
anonymous reviewer for their helpful comments. The assistance from Ms.
Yi-Wen Wang in the calculation of skill scores and Ms. Yun-Wei Huang in
figure editing is appreciated. This study was jointly supported by the
National Science Council of Taiwan under NSC-96-2111-M-002-010-MY3,
NSC-97-2111-M-003-005-MY2, NSC-99-2111-M-003-004-MY3, and
NSC-99-2111-M-002-001, and by the National Taiwan University (NTU) under
Grant 99R40044.
NR 39
TC 4
Z9 4
U1 2
U2 7
PU CHINESE GEOSCIENCE UNION
PI TAIPEI
PA PO BOX 23-59, TAIPEI 10764, TAIWAN
SN 1017-0839
J9 TERR ATMOS OCEAN SCI
JI Terr. Atmos. Ocean. Sci.
PD FEB
PY 2011
VL 22
IS 1
BP 49
EP 69
DI 10.3319/TAO.2010.07.13.01(A)
PG 21
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Oceanography
SC Geology; Meteorology & Atmospheric Sciences; Oceanography
GA 734UN
UT WOS:000288365200004
ER
PT J
AU Toth, RA
Sung, K
Brown, LR
AF Toth, Robert A.
Sung, Keeyoon
Brown, Linda R.
TI (H2O)-O-16 line strengths revisited: nu(2) and 2 nu(2)-nu(2) at 6 mu m
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Water vapor; H2O; Strengths; Intensities; Hot band; HITRAN; Infrared
ID MOLECULAR SPECTROSCOPIC DATABASE; LYING ROTATIONAL LEVELS; WATER-VAPOR;
VIBRATIONAL-STATES; ENERGY-LEVELS; CM(-1); INTENSITIES; FREQUENCIES;
PARAMETERS; POSITIONS
AB The necessity to revisit water spectroscopy at 6 mu m was prompted by recent work indicating that some prior measurements of (H2O)-O-16 line strengths (ranging through seven orders of magnitude) had larger than expected systematic errors for the stronger transitions. To investigate this, linestrengths of stronger transitions were re-measured (with 14 new H2O spectra recorded with a Bruker 125 HR Fourier transform spectrometer at the Jet Propulsion Laboratory) and combined with re-analyzed prior results (obtained at higher optical densities from 32 spectra recorded with the FTS at Kitt Peak). Systematic differences for some of the older data sets were identified and corrected. In this paper, an internally-consistent sampling of 1243 selected line strengths are reported for (0 1 0)-(0 0 0) and (0 2 0)-(0 1 0) transitions between 783 and 2378 cm(-1). To confirm experimental precisions, observed and calculated line strengths are compared. (c) 2010 Published by Elsevier Inc.
C1 [Toth, Robert A.; Sung, Keeyoon; Brown, Linda R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Brown, LR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mailstop 183-601, Pasadena, CA 91109 USA.
EM ratoth@jpl.nasa.gov
RI Sung, Keeyoon/I-6533-2015
FU National Aeronautics and Space Administration
FX This research was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. The author thanks the National Solar
Observatory at Kitt Peak for the use of the FTS in obtaining the
H2O spectra.
NR 24
TC 3
Z9 3
U1 2
U2 5
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD FEB
PY 2011
VL 265
IS 2
BP 59
EP 68
DI 10.1016/j.jms.2010.10.009
PG 10
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 733SL
UT WOS:000288283000001
ER
PT J
AU Plante, I
Ponomarev, A
Cucinotta, FA
AF Plante, Ianik
Ponomarev, Artem
Cucinotta, Francis A.
TI 3D VISUALISATION OF THE STOCHASTIC PATTERNS OF THE RADIAL DOSE IN
NANO-VOLUMES BY A MONTE CARLO SIMULATION OF HZE ION TRACK STRUCTURE
SO RADIATION PROTECTION DOSIMETRY
LA English
DT Article; Proceedings Paper
CT 15th International Symposium on Microdosimetry
CY OCT 25-30, 2009
CL Verona, ITALY
SP INFN Lab Nazl Legnaro, NASA Johnson Space Ctr, CERN, Univ Oxford, Gray Inst Radiat Oncol & Biol
ID IONIZING-RADIATION; SPATIAL-DISTRIBUTION; SPACE EXPLORATION; CHROMATIN
LOOPS; STRAND BREAKS; IN-VIVO; DISTRIBUTIONS; ELECTRONS; DAMAGE;
PARTICLES
AB The description of energy deposition by high charge and energy (HZE) nuclei is of importance for space radiation risk assessment and due to their use in hadrontherapy. Such ions deposit a large fraction of their energy within the so-called core of the track and a smaller proportion in the penumbra (or track periphery). We study the stochastic patterns of the radial dependence of energy deposition using Monte Carlo track structure codes RITRACKS and RETRACKS, that were used to simulate HZE tracks and calculate energy deposition in voxels of 40 nm. The simulation of a Fe-56(26+) ion of 1 GeV u(-1) revealed zones of high-energy deposition which maybe found as far as a few millimetres away from the track core in some simulations. The calculation also showed that similar to 43% of the energy was deposited in the penumbra. These 3D stochastic simulations combined with a visualisation interface are a powerful tool for biophysicists which may be used to study radiation-induced biological effects such as double strand breaks and oxidative damage and the subsequent cellular and tissue damage processing and signalling.
C1 [Plante, Ianik; Ponomarev, Artem; Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Plante, Ianik; Ponomarev, Artem] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM francis.a.cucinotta@nasa.gov
NR 29
TC 14
Z9 14
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0144-8420
EI 1742-3406
J9 RADIAT PROT DOSIM
JI Radiat. Prot. Dosim.
PD FEB
PY 2011
VL 143
IS 2-4
BP 156
EP 161
DI 10.1093/rpd/ncq526
PG 6
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 730GR
UT WOS:000288022300006
PM 21199826
ER
PT J
AU Hu, SW
Cucinotta, FA
AF Hu, Shaowen
Cucinotta, Francis A.
TI MODELLING THE WAY KU BINDS DNA
SO RADIATION PROTECTION DOSIMETRY
LA English
DT Article; Proceedings Paper
CT 15th International Symposium on Microdosimetry
CY OCT 25-30, 2009
CL Verona, ITALY
SP INFN Lab Nazl Legnaro, NASA Johnson Space Ctr, CERN, Univ Oxford, Gray Inst Radiat Oncol & Biol
ID DEPENDENT PROTEIN-KINASE; STRAND BREAK REPAIR; CATALYTIC SUBUNIT; END;
HETERODIMER; DOCKING; COMPLEX; DOMAIN; PKCS
AB Ku plays a crucial role in the non-homologous end joining pathway to repair DNA double-strand breaks. In this study, we modelled the full-length Ku heterodimer from the truncated crystal structure and NMR structure, and conducted a series of docking and molecular dynamics simulations in an effort to probe the structural, dynamical and energetic features of each domain in free Ku and Ku-DNA complexes.
C1 [Hu, Shaowen] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
[Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Hu, SW (reprint author), Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
EM shaowen.hu-1@nasa.gov; francis.a.cucinotta@nasa.gov
NR 23
TC 1
Z9 1
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0144-8420
J9 RADIAT PROT DOSIM
JI Radiat. Prot. Dosim.
PD FEB
PY 2011
VL 143
IS 2-4
BP 196
EP 201
DI 10.1093/rpd/ncq519
PG 6
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 730GR
UT WOS:000288022300014
PM 21196465
ER
PT J
AU Hu, SW
Cucinotta, FA
AF Hu, Shaowen
Cucinotta, Francis A.
TI A CELL KINETIC MODEL OF GRANULOPOIESIS UNDER RADIATION EXPOSURE:
EXTENSION FROM RODENTS TO CANINES AND HUMANS
SO RADIATION PROTECTION DOSIMETRY
LA English
DT Article; Proceedings Paper
CT 15th International Symposium on Microdosimetry
CY OCT 25-30, 2009
CL Verona, ITALY
SP INFN Lab Nazl Legnaro, NASA Johnson Space Ctr, CERN, Univ Oxford, Gray Inst Radiat Oncol & Biol
ID SPACE; RESPONSES; RISK
AB As significant ionising radiation exposure will occur during prolonged space travel in future, it is essential to understand their adverse effects on the radiosensitive organ systems that are important for immediate survival of humans, e. g. the haematopoietic system. In this paper, a biomathematical model of granulopoiesis is used to analyse the granulocyte changes seen in the blood of mammalians under acute and continuous radiation exposure. This is one of a set of haematopoietic models that have been successfully utilised to simulate and interpret the experimental data of acute and chronic radiation on rodents. Extension to canine and human systems indicates that the results of the model are consistent with the cumulative experimental and empirical data from various sources, implying the potential to integrate them into one united model system to monitor the haematopoietic response of various species under irradiation. The suppression of granulocytes' level of a space traveller under chronic stress of low-dose irradiation as well as the granulopoietic response when encountering a historically large solar particle event is also discussed.
C1 [Hu, Shaowen] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
[Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Hu, SW (reprint author), Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
EM shaowen.hu-1@nasa.gov; francis.a.cucinotta@nasa.gov
NR 22
TC 4
Z9 4
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0144-8420
J9 RADIAT PROT DOSIM
JI Radiat. Prot. Dosim.
PD FEB
PY 2011
VL 143
IS 2-4
BP 207
EP 213
DI 10.1093/rpd/ncq520
PG 7
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 730GR
UT WOS:000288022300016
PM 21196459
ER
PT J
AU Malak, H
Richmond, R
Dicello, JF
AF Malak, Henryk
Richmond, Robert
Dicello, J. F.
TI A NEW NANO-ENHANCED TECHNOLOGY PROPOSED TO QUANTIFY INTRACELLULAR
DETECTION OF RADIATION-INDUCED METABOLIC PROCESSES
SO RADIATION PROTECTION DOSIMETRY
LA English
DT Article; Proceedings Paper
CT 15th International Symposium on Microdosimetry
CY OCT 25-30, 2009
CL Verona, ITALY
SP INFN Lab Nazl Legnaro, NASA Johnson Space Ctr, CERN, Univ Oxford, Gray Inst Radiat Oncol & Biol
ID METALLIC PARTICLES; RAMAN-SPECTROSCOPY; LIVING CELLS; FLUORESCENCE
AB A new approach to intracellular detection and imaging of metabolic processes and pathways is presented that uses surface plasmon resonance to enhance interactions between photon-absorbing metabolites and metal nanoparticles in contact with cells in vitro or in vivo. Photon absorption in the nanoparticles creates plasmon fields, enhancing intrinsic metabolite fluorescence, thereby increasing absorption and emission rates, creating new spectral emission bands, shortening fluorescence lifetimes, becoming more photo-stable and increasing fluorescent resonance energy transfer efficiency. Because the cells remain viable, it is proposed that the method may be used to interrogate cells prior to and after irradiation, with the potential for automated analyses of intracellular interactive pathways associated with radiation exposures at lower doses than existing technologies. The design and concepts of the instrument are presented along with data for unexposed cells.
C1 [Malak, Henryk] Amer Environm Syst Inc, Ellicott City, MD 21043 USA.
[Richmond, Robert] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Dicello, J. F.] Loma Linda Univ, Med Ctr, Dept Radiat Med, Loma Linda, CA 92354 USA.
RP Malak, H (reprint author), Amer Environm Syst Inc, 8444 High Ridge Rd, Ellicott City, MD 21043 USA.
EM photonics@comcast.net
NR 13
TC 0
Z9 0
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0144-8420
J9 RADIAT PROT DOSIM
JI Radiat. Prot. Dosim.
PD FEB
PY 2011
VL 143
IS 2-4
BP 301
EP 304
DI 10.1093/rpd/ncq523
PG 4
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 730GR
UT WOS:000288022300033
PM 21196462
ER
PT J
AU Cucinotta, FA
Plante, I
Ponomarev, AL
Kim, MHY
AF Cucinotta, Francis A.
Plante, Ianik
Ponomarev, Artem L.
Kim, Myung-Hee Y.
TI NUCLEAR INTERACTIONS IN HEAVY ION TRANSPORT AND EVENT-BASED RISK MODELS
SO RADIATION PROTECTION DOSIMETRY
LA English
DT Article; Proceedings Paper
CT 15th International Symposium on Microdosimetry
CY OCT 25-30, 2009
CL Verona, ITALY
SP INFN Lab Nazl Legnaro, NASA Johnson Space Ctr, CERN, Univ Oxford, Gray Inst Radiat Oncol & Biol
ID ABRASION-ABLATION; SPACE EXPLORATION; CROSS-SECTIONS; COLLISIONS;
DISTRIBUTIONS; DEPENDENCE
AB The physical description of the passage of heavy ions in tissue and shielding materials is of interest in radiobiology, cancer therapy and space exploration, including a human mission to Mars. Galactic cosmic rays (GCRs) consist of a large number of ion types and energies. Energy loss processes occur continuously along the path of heavy ions and are well described by the linear energy transfer (LET), straggling and multiple scattering algorithms. Nuclear interactions lead to much larger energy deposition than atomic-molecular collisions and alter the composition of heavy ion beams while producing secondary nuclei often in high multiplicity events. The major nuclear interaction processes of importance for describing heavy ion beams was reviewed, including nuclear fragmentation, elastic scattering and knockout-cascade processes. The quantum multiple scattering fragmentation model is shown to be in excellent agreement with available experimental data for nuclear fragmentation cross sections and is studied for application to thick target experiments. A new computer model, which was developed for the description of biophysical events from heavy ion beams at the NASA Space Radiation Laboratory (NSRL), called the GCR Event Risk-Based Model (GERMcode) is described.
C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Plante, Ianik; Ponomarev, Artem L.; Kim, Myung-Hee Y.] USRA Div Life Sci, Houston, TX 77058 USA.
RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM francis.a.cucinotta@nasa.gov
OI Kim, Myung-Hee/0000-0001-5575-6858
NR 21
TC 16
Z9 16
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0144-8420
EI 1742-3406
J9 RADIAT PROT DOSIM
JI Radiat. Prot. Dosim.
PD FEB
PY 2011
VL 143
IS 2-4
BP 384
EP 390
DI 10.1093/rpd/ncq512
PG 7
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 730GR
UT WOS:000288022300050
PM 21242169
ER
PT J
AU Pisacane, VL
Dolecek, QE
Malak, H
Cucinotta, FA
Zaider, M
Rosenfeld, AB
Rusek, A
Sivertz, M
Dicello, JF
AF Pisacane, V. L.
Dolecek, Q. E.
Malak, H.
Cucinotta, F. A.
Zaider, M.
Rosenfeld, A. B.
Rusek, A.
Sivertz, M.
Dicello, J. F.
TI MICRODOSEMETER INSTRUMENT (MIDN) FOR ASSESSING RISK IN SPACE
SO RADIATION PROTECTION DOSIMETRY
LA English
DT Article; Proceedings Paper
CT 15th International Symposium on Microdosimetry
CY OCT 25-30, 2009
CL Verona, ITALY
SP INFN Lab Nazl Legnaro, NASA Johnson Space Ctr, CERN, Univ Oxford, Gray Inst Radiat Oncol & Biol
AB Radiation in space generally produces higher dose rates than that on the Earth's surface, and contributions from primary galactic and solar events increase with altitude within the magnetosphere. Presently, no personnel monitor is available to astronauts for real-time monitoring of dose, radiation quality and regulatory risk. This group is developing a prototypic instrument for use in an unknown, time-varying radiation field. This microdosemeter-dosemeter nucleon instrument is for use in a spacesuit, spacecraft, remote rover and other applications. It provides absorbed dose, dose rate and dose equivalent in real time so that action can be taken to reduce exposure. Such a system has applications in health physics, anti-terrorism and radiation-hardening of electronics as well. The space system is described and results of ground-based studies are presented and compared with predictions of transport codes. An early prototype in 2007 was successfully launched, the only solid-state microdosemeter to have flown in space.
C1 [Pisacane, V. L.; Dicello, J. F.] USN Acad, Aerosp Engn Dept Mail Stop 11B, Annapolis, MD 21402 USA.
[Dolecek, Q. E.] QED Associates, Georgetown, DE 19947 USA.
[Malak, H.] Amer Environm Syst Inc, Ellicott City, MD 21043 USA.
[Cucinotta, F. A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Zaider, M.] Mem Sloan Kettering Canc Ctr, New York, NY 10021 USA.
[Rosenfeld, A. B.] Univ Wollongong, Ctr Med Radiat Phys, Wollongong, NSW 2522, Australia.
[Rusek, A.; Sivertz, M.] Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Pisacane, VL (reprint author), USN Acad, Aerosp Engn Dept Mail Stop 11B, 590 Holloway Rd, Annapolis, MD 21402 USA.
EM pisacane@usna.edu
RI Rosenfeld, Anatoly/D-1989-2014;
OI Zaider, Marco/0000-0002-5113-7862
NR 4
TC 2
Z9 2
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0144-8420
J9 RADIAT PROT DOSIM
JI Radiat. Prot. Dosim.
PD FEB
PY 2011
VL 143
IS 2-4
BP 398
EP 401
DI 10.1093/rpd/ncq525
PG 4
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 730GR
UT WOS:000288022300053
PM 21199825
ER
PT J
AU Dicello, JF
Gersey, BB
Gridley, DS
Coutrakon, GB
Lesyna, D
Pisacane, VL
Robertson, JB
Schulte, RW
Slater, JD
Wroe, AJ
Slater, JM
AF Dicello, John F.
Gersey, Bradford B.
Gridley, Daila S.
Coutrakon, George B.
Lesyna, David
Pisacane, Vincent L.
Robertson, James B.
Schulte, Reinhard W.
Slater, Jerry D.
Wroe, Andrew J.
Slater, James M.
TI MICRODOSIMETRIC COMPARISON OF SCANNED AND CONVENTIONAL PROTON BEAMS USED
IN RADIATION THERAPY
SO RADIATION PROTECTION DOSIMETRY
LA English
DT Article; Proceedings Paper
CT 15th International Symposium on Microdosimetry
CY OCT 25-30, 2009
CL Verona, ITALY
SP INFN Lab Nazl Legnaro, NASA Johnson Space Ctr, CERN, Univ Oxford, Gray Inst Radiat Oncol & Biol
ID BIOL-PHYS 2006/65/1-7; PROSTATE-CANCER; 2ND CANCERS; FIELD;
RADIOTHERAPY; IMPACT; RISK
AB Multiple groups have hypothesised that the use of scanning beams in proton therapy will reduce the neutron component of secondary radiation in comparison with conventional methods with a corresponding reduction in risks of radiation-induced cancers. Loma Linda University Medical Center (LLUMC) has had FDA marketing clearance for scanning beams since 1988 and an experimental scanning beam has been available at the LLUMC proton facility since 2001. The facility has a dedicated research room with a scanning beam and fast switching that allows its use during patient treatments. Dosimetric measurements and microdosimetric distributions for a scanned beam are presented and compared with beams produced with the conventional methods presently used in proton therapy.
C1 [Dicello, John F.] Loma Linda Univ, Med Ctr, Dept Radiat Med, Lutherville Timonium, MD 21093 USA.
[Gersey, Bradford B.] Prairie View A&M Univ, Ctr Appl Radiat Res, NASA, Prairie View, TX 77446 USA.
[Gridley, Daila S.; Coutrakon, George B.; Schulte, Reinhard W.; Slater, Jerry D.; Wroe, Andrew J.; Slater, James M.] Loma Linda Univ, Med Ctr, Dept Radiat Med, Loma Linda, CA 92354 USA.
[Lesyna, David] Optivus Proton Therapy Inc, Loma Linda, CA 92354 USA.
[Pisacane, Vincent L.] USN Acad, Aerosp Engn Dept Mail Stop 11B, Annapolis, MD 21402 USA.
[Robertson, James B.] E Carolina Univ, Chocowinity, NC 27817 USA.
RP Dicello, JF (reprint author), Loma Linda Univ, Med Ctr, Dept Radiat Med, 25 Westminster Bridge Way, Lutherville Timonium, MD 21093 USA.
EM dicello@usna.edu
RI Gridley, Daila/P-7711-2015
NR 17
TC 5
Z9 5
U1 0
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0144-8420
J9 RADIAT PROT DOSIM
JI Radiat. Prot. Dosim.
PD FEB
PY 2011
VL 143
IS 2-4
BP 513
EP 518
DI 10.1093/rpd/ncq513
PG 6
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA 730GR
UT WOS:000288022300075
PM 21362697
ER
PT J
AU Kaul, UK
AF Kaul, Upender K.
TI Effect of Inflow Boundary Conditions on the Turbulence Solution in
Internal Flows
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 40th AIAA Fluid Dynamics Conference
CY JUN 28-JUL 01, 2010
CL Chicago, IL
ID LOW-REYNOLDS-NUMBER; CHANNEL FLOW; MODEL; EQUATIONS; REGION
C1 [Kaul, Upender K.] NASA, Ames Res Ctr, Fundamental Modeling & Simulat Branch, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA.
RP Kaul, UK (reprint author), NASA, Ames Res Ctr, Fundamental Modeling & Simulat Branch, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA.
NR 24
TC 3
Z9 3
U1 2
U2 4
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD FEB
PY 2011
VL 49
IS 2
BP 426
EP 432
DI 10.2514/1.J050532
PG 7
WC Engineering, Aerospace
SC Engineering
GA 720JO
UT WOS:000287277200015
ER
PT J
AU Scully, ST
Stecker, FW
AF Scully, Sean T.
Stecker, Floyd W.
TI Testing Lorentz invariance with neutrinos from ultrahigh energy cosmic
ray interactions
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Cosmic rays; Neutrinos; Lorentz invariance; Quantum gravity
ID UNIVERSAL RADIATION-FIELD; GAMMA-RAYS; MAGNETIC-FIELDS; STAR-FORMATION;
SPECTRUM; VIOLATION; DETECTOR; PHOTONS; HISTORY; MISSION
AB We have previously shown that a very small amount of Lorentz invariance violation (LIV), which suppresses photomeson interactions of ultrahigh energy cosmic rays (UHECRs) with cosmic background radiation (CBR) photons, can produce a spectrum of cosmic rays that is consistent with that currently observed by the Pierre Auger Observatory (PAD) and HiRes experiments. Here, we calculate the corresponding flux of high energy neutrinos generated by the propagation of UHECR protons through the CBR in the presence of LIV. We find that LIV produces a reduction in the flux of the highest energy neutrinos and a reduction in the energy of the peak of the neutrino energy flux spectrum, both depending on the strength of the LIV. Thus, observations of the UHE neutrino spectrum provide a clear test for the existence and amount of LIV at the highest energies. We further discuss the ability of current and future proposed detectors make such observations. Published by Elsevier B.V.
C1 [Stecker, Floyd W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Scully, Sean T.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA.
RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM scullyst@jmu.edu; Floyd.W.Stecker@nasa.gov
RI Stecker, Floyd/D-3169-2012
NR 48
TC 5
Z9 5
U1 0
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
J9 ASTROPART PHYS
JI Astropart Phys.
PD FEB
PY 2011
VL 34
IS 7
BP 575
EP 580
DI 10.1016/j.astropartphys.2010.11.004
PG 6
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 729MW
UT WOS:000287955500007
ER
PT J
AU Zhang, XA
Chibli, H
Mielke, R
Nadeau, J
AF Zhang, Xuan
Chibli, Hicham
Mielke, Randall
Nadeau, Jay
TI Ultrasmall Gold-Doxorubicin Conjugates Rapidly Kill Apoptosis-Resistant
Cancer Cells
SO BIOCONJUGATE CHEMISTRY
LA English
DT Article
ID CONTRAST AGENT; DNA-DAMAGE; NANOPARTICLES; ADRIAMYCIN; DELIVERY;
THERAPEUTICS; CYTOTOXICITY; SENSITIVITY; TOXICITY; DEATH
AB Ultrasmall (mean diameter, 2.7 nm) gold nanoparticles conjugated to doxorubicin (Au-Dox) are up to 20-fold more cytotoxic to B16 melanoma cells than the equivalent concentration of doxorubicin alone, and act up to six times more quickly. Ultrasmall Au-Dox enters the cell endocytic vesicles and is also seen free in the cytoplasm and nuclei. This is in distinct contrast to larger particles reported in previous studies, which are excluded from the nucleus and which show no increased toxicity over Dox alone. Cell death with Au-Dox is confirmed to be apoptotic by TUNEL staining and ultrastructural examination using transmission electron microscopy. To further explore the mechanism of action, two other cell lines were examined: He La cells which are highly sensitive to Dox, and He La cells overexpressing Bcl-2 which show impaired apoptosis and Dox resistance. Interestingly, the Dox-sensitive cells show a slightly decreased sensitivity to Au-Dox relative to Dox alone, whereas the Dox-resistant cells are not resistant to Au-Dox These results have implications for the design of chemotherapeutic nanoparticles, suggesting that it is possible to selectively target apoptosis-resistant cancer cells while at the same time reducing cytotoxicity to normal cells.
C1 [Zhang, Xuan; Chibli, Hicham; Nadeau, Jay] McGill Univ, Dept Biomed Engn, Montreal, PQ H3A 2B4, Canada.
[Mielke, Randall] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nadeau, J (reprint author), McGill Univ, Dept Biomed Engn, 3775 Univ St, Montreal, PQ H3A 2B4, Canada.
EM jay.nadeau@mcgill.ca
FU U.S. EPA-Science to Achieve Results (STAR) program [R831712]; National
Science and Engineering Research Council of Canada (NSERC); NSERC/CIHR;
NSERC CREATE Canadian Astrobiology Training Program
FX H.C. and J.L.N. acknowledge the U.S. EPA-Science to Achieve Results
(STAR) program Grant #R831712; the National Science and Engineering
Research Council of Canada (NSERC) Individual Discovery program; and the
NSERC/CIHR Collaborative Health Research Program. X.Z. is supported by
the NSERC CREATE Canadian Astrobiology Training Program.
NR 39
TC 39
Z9 42
U1 2
U2 30
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1043-1802
J9 BIOCONJUGATE CHEM
JI Bioconjugate Chem.
PD FEB
PY 2011
VL 22
IS 2
BP 235
EP 243
DI 10.1021/bc100374p
PG 9
WC Biochemical Research Methods; Biochemistry & Molecular Biology;
Chemistry, Multidisciplinary; Chemistry, Organic
SC Biochemistry & Molecular Biology; Chemistry
GA 720RE
UT WOS:000287297000017
PM 21189001
ER
PT J
AU Hafez, M
Kwak, D
AF Hafez, M.
Kwak, D.
TI Implicit Solutions of Navier-Stokes Equations Special Issue Dedicated to
Drs. W.R. Briley and H. McDonald Preface
SO COMPUTERS & FLUIDS
LA English
DT Editorial Material
C1 [Hafez, M.] Univ Calif Davis, Davis, CA 95616 USA.
[Kwak, D.] NASA, Ames Res Ctr, Washington, DC USA.
RP Hafez, M (reprint author), Univ Calif Davis, Davis, CA 95616 USA.
EM mhafez@ucdavis.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0045-7930
J9 COMPUT FLUIDS
JI Comput. Fluids
PD FEB
PY 2011
VL 41
IS 1
SI SI
BP 1
EP 1
DI 10.1016/j.compfluid.2010.09.011
PG 1
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 704UZ
UT WOS:000286082400001
ER
PT J
AU Kwak, D
Kiris, C
Housman, J
AF Kwak, Dochan
Kiris, Cetin
Housman, Jeffrey
TI Implicit methods for viscous incompressible flows
SO COMPUTERS & FLUIDS
LA English
DT Article
DE Computational fluid dynamics; Incompressible flow; Numerical simulation;
Implicit methods
ID NAVIER-STOKES EQUATIONS; SIMULATIONS; ALGORITHM; SCHEME
AB Numerical methods and simulation tools for incompressible flows have been advanced largely as a subset of the computational fluid dynamics (CFD) discipline. Especially within the aerospace community, simulation of compressible flows has driven most of the development of computational algorithms and tools. This is due to the high level of accuracy desired for predicting aerodynamic performance of flight vehicles. Conversely, low-speed incompressible flow encountered in a wide range of fluid engineering problems has not typically required the same level of numerical accuracy. This practice of tolerating relatively low-fidelity solutions in engineering applications for incompressible flow has changed. As the design of flow devices becomes more sophisticated, a narrower margin of error is required. Accurate and robust CFD tools have become increasingly important in fluid engineering for incompressible and low-speed flow. Accuracy depends not only on numerical methods but also on flow physics and geometry modeling. For high-accuracy solutions, geometry modeling has to be very inclusive to capture the elliptic nature of incompressible flow resulting in large grid sizes. Therefore, in this article, implicit schemes or efficient time integration schemes for incompressible flow are reviewed from a CFD tool development point of view. Extension of the efficient solution procedures to arbitrary Mach number flows through a unified time-derivative preconditioning approach is also discussed. The unified implicit solution procedure is capable of solving low-speed compressible flows, transonic, as well as supersonic flows accurately and efficiently. Test cases demonstrating Mach-independent convergence are presented. Published by Elsevier Ltd.
C1 [Kwak, Dochan; Kiris, Cetin; Housman, Jeffrey] NASA, NASA Adv Supercomp NAS Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kwak, D (reprint author), NASA, NASA Adv Supercomp NAS Div, Ames Res Ctr, Mail Stop 258-5, Moffett Field, CA 94035 USA.
EM Dochan.Kwak@nasa.gov
NR 43
TC 6
Z9 6
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0045-7930
J9 COMPUT FLUIDS
JI Comput. Fluids
PD FEB
PY 2011
VL 41
IS 1
SI SI
BP 51
EP 64
DI 10.1016/j.compfluid.2010.09.022
PG 14
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 704UZ
UT WOS:000286082400006
ER
PT J
AU Pulliam, TH
AF Pulliam, T. H.
TI Development of implicit methods in CFD NASA Ames Research Center
1970s-1980s
SO COMPUTERS & FLUIDS
LA English
DT Article
DE Implicit finite differences; CFD; Approximate factorization; Numerical
methods
AB The focus here is on the early development (mid 1970s-1980s) at NASA Ames Research Center of implicit methods in Computational Fluid Dynamics (CFD). A class of implicit finite difference schemes of the Beam and Warming approximate factorization type will be addressed. The emphasis will be on the Euler equations. A review of material pertinent to the solution of the Euler equations within the framework of implicit methods will be presented. The eigensystem of the equations will be used extensively in developing a framework for various methods applied to the Euler equations. The development and analysis of various aspects of this class of schemes will be given along with the motivations behind many of the choices. Various acceleration and efficiency modifications such as matrix reduction, diagonalization and flux split schemes will be presented. Published by Elsevier Ltd.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Pulliam, TH (reprint author), NASA, Ames Res Ctr, MS 258-2, Moffett Field, CA 94035 USA.
EM Thomas.H.Pulliam@nasa.gov
NR 9
TC 1
Z9 2
U1 1
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0045-7930
J9 COMPUT FLUIDS
JI Comput. Fluids
PD FEB
PY 2011
VL 41
IS 1
SI SI
BP 65
EP 71
DI 10.1016/j.compfluid.2010.09.016
PG 7
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 704UZ
UT WOS:000286082400007
ER
PT J
AU Thomas, JL
Diskin, B
Nishikawa, H
AF Thomas, James L.
Diskin, Boris
Nishikawa, Hiroaki
TI A critical study of agglomerated multigrid methods for diffusion on
highly-stretched grids
SO COMPUTERS & FLUIDS
LA English
DT Article
DE Multigrid; Agglomeration; Unstructured; Diffusion; Analysis
ID SOLVERS; EFFICIENCY; ACCURACY
AB Agglomerated multigrid methods for unstructured grids are studied critically for solving a model diffusion equation on highly-stretched grids typical of practical viscous simulations, following a previous work focused on isotropic grids. Different primal elements, including prismatic and tetrahedral elements in three dimensions, are considered. The components of an efficient node-centered full-coarsening multigrid scheme are identified and assessed using quantitative analysis methods. Fast grid-independent convergence is demonstrated for mixed-element grids composed of tetrahedral elements in the isotropic regions and prismatic elements in the highly-stretched regions. Implicit lines natural to advancing-layer/advancing-front grid generation techniques are essential elements of both relaxation and agglomeration. On agglomerated grids, consistent average-least-square discretizations augmented with edge-directional gradients to increase h-ellipticity of the operator are used. Simpler (edge-terms-only) coarse-grid discretizations are also studied and shown to produce grid-dependent convergence only effective on grids with minimal skewing. Published by Elsevier Ltd.
C1 [Thomas, James L.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
[Diskin, Boris; Nishikawa, Hiroaki] 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; hiro@nianet.org
RI Nishikawa, Hiroaki/M-1247-2016
OI Nishikawa, Hiroaki/0000-0003-4472-5313
FU National Institute of Aerospace through NASA [NNL07AA23C, NNL07AA31C]
FX This author was supported by the National Institute of Aerospace under
the NASA Fundamental Aeronautics Program through NASA Contracts
NNL07AA23C and NNL07AA31C.
NR 20
TC 3
Z9 3
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0045-7930
EI 1879-0747
J9 COMPUT FLUIDS
JI Comput. Fluids
PD FEB
PY 2011
VL 41
IS 1
SI SI
BP 82
EP 93
DI 10.1016/j.compfluid.2010.09.023
PG 12
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 704UZ
UT WOS:000286082400009
ER
PT J
AU Fisher, R
Radford, BT
Knowlton, N
Brainard, RE
Michaelis, FB
Caley, MJ
AF Fisher, Rebecca
Radford, Ben T.
Knowlton, Nancy
Brainard, Russell E.
Michaelis, Frances B.
Caley, M. Julian
TI Global mismatch between research effort and conservation needs of
tropical coral reefs
SO CONSERVATION LETTERS
LA English
DT Article
DE Biological conservation; biological knowledge; Coral Triangle; coral
reefs; geocoding; global conservation; global research; Google Maps
(TM); scientific literature; Web of Science
ID CLIMATE-CHANGE; BIODIVERSITY HOTSPOTS; MARINE BIODIVERSITY; ECOSYSTEMS;
RESILIENCE; PRIORITIES; OCEAN
AB Tropical coral reefs are highly diverse and globally threatened. Management to ensure their persistence requires sound biological knowledge in regions where coral reef biodiversity and/or the threats to it are greatest. This paper uses a novel text analysis approach and Google Maps (TM) to examine the spatial coverage of scientific papers on coral reefs listed in Web of Science (R). Results show that research is highly clumped spatially, positively related to per capita gross domestic product, negatively related to coral species richness, and unrelated to threats to coral reefs globally; indicating a serious mismatch between conservation needs and the knowledge required for effective management. Greater research effort alone cannot guarantee better conservation outcomes, but given some regions of the world (e.g., Central Indo-Pacific) remain severely understudied, priority allocation of resources to fill such knowledge gaps should support greater adaptive management capacity through the development of an improved knowledge base for reef managers.
C1 [Fisher, Rebecca; Radford, Ben T.] UWA Oceans Inst M096, Australian Inst Marine Sci, Crawley, WA 6009, Australia.
[Radford, Ben T.] Univ Western Australia M004, Sch Earth & Environm, Crawley, WA 6009, Australia.
[Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20013 USA.
[Knowlton, Nancy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA.
[Brainard, Russell E.] Natl Marine Fisheries Serv, Coral Reef Ecosyst Div, Pacific Islands Fisheries Sci Ctr, NOAA, Honolulu, HI 96814 USA.
[Michaelis, Frances B.; Caley, M. Julian] Australian Inst Marine Sci, Townsville, Qld 4810, Australia.
RP Fisher, R (reprint author), UWA Oceans Inst M096, Australian Inst Marine Sci, 35 Stirling Hwy, Crawley, WA 6009, Australia.
EM r.fisher@aims.gov.au
RI Fisher, Rebecca/C-5459-2011;
OI Fisher, Rebecca/0000-0001-5148-6731
FU BHP Billiton through CReefs Australia (CReefs, Census of Marine Life)
FX Funded by BHP Billiton through CReefs Australia (CReefs, Census of
Marine Life). J. Ruxton assisted with compiling the literature database,
M. Case assisted with geographic analyses and R. O'Leary provided
statistical advice. S. Wilson, S. Kininmonth, M. Case, and M. Puotinen
provided comments on the manuscript. R. F., M. J. C, N.K., and R. B.
conceived the study, F. B. M. provided global context, B. R. assisted
with geocoding and analyses, R. F. and M. J. C. led the writing of the
manuscript; all authors contributed to writing and commenting on drafts.
We thank P. Armsworth and two anonymous reviewers for their comments.
NR 32
TC 29
Z9 29
U1 2
U2 37
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1755-263X
J9 CONSERV LETT
JI Conserv. Lett.
PD FEB
PY 2011
VL 4
IS 1
BP 64
EP 72
DI 10.1111/j.1755-263X.2010.00146.x
PG 9
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA 716PW
UT WOS:000286986900008
ER
PT J
AU Harvey, N
Peres, Y
AF Harvey, Nate
Peres, Yuval
TI An invariant of finitary codes with finite expected square root coding
length
SO ERGODIC THEORY AND DYNAMICAL SYSTEMS
LA English
DT Article
ID BERNOULLI SCHEMES; ENTROPY
AB Let p and q be probability vectors with the same entropy h. Denote by B(p) the Bernoulli shift indexed by Z with marginal distribution p. Suppose that phi is a measure-preserving homomorphism from B(p) to B(q). We prove that if the coding length of phi has a finite 1/2 moment, then delta(2)(p) = delta(2)(p), where delta(2)(p) = Sigma(i) p(i)(-log p(i) - h)(2) is the informational variance of p. In this result, the 1/2 moment cannot be replaced by a lower moment. On the other hand, for any theta < 1, we exhibit probability vectors p and q that are not permutations of each other, such that there exists a finitary isomorphism Phi from B(p) to B(q) where the coding lengths of Phi and of its inverse have a finite theta moment. We also present an extension to ergodic Markov chains.
C1 [Harvey, Nate] UC Berkeley, Dept Math, Berkeley, CA 94720 USA.
[Peres, Yuval] Microsoft Res, Redmond, WA USA.
RP Harvey, N (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM nathaniel.e.harvey@jpl.nasa.gov; peres@microsoft.com
NR 13
TC 0
Z9 0
U1 0
U2 1
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0143-3857
J9 ERGOD THEOR DYN SYST
JI Ergod. Theory Dyn. Syst.
PD FEB
PY 2011
VL 31
BP 77
EP 90
DI 10.1017/S014338570900090X
PN 1
PG 14
WC Mathematics, Applied; Mathematics
SC Mathematics
GA 703WY
UT WOS:000286013200005
ER
PT J
AU Bertacca, D
Bruni, M
Piattella, OF
Pietrobon, D
AF Bertacca, Daniele
Bruni, Marco
Piattella, Oliver F.
Pietrobon, Davide
TI Unified Dark Matter scalar field models with fast transition
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE dark matter theory; dark energy theory
ID PROBE WMAP OBSERVATIONS; DIGITAL SKY SURVEY; COSMOLOGICAL CONSTANT;
K-ESSENCE; IA SUPERNOVAE; LIGHT CURVES; PERTURBATIONS; ENERGY;
QUINTESSENCE; INFLATION
AB We investigate the general properties of Unified Dark Matter (UDM) scalar field models with Lagrangians with a non-canonical kinetic term, looking specifically for models that can produce a fast transition between an early Einstein-de Sitter CDM-like era and a later Dark Energy like phase, similarly to the barotropic fluid UDM models in JCAP 01 (2010) 014. However, while the background evolution can be very similar in the two cases, the perturbations are naturally adiabatic in fluid models, while in the scalar field case they are necessarily non-adiabatic. The new approach to building UDM Lagrangians proposed here allows to escape the common problem of the fine-tuning of the parameters which plague many UDM models. We analyse the properties of perturbations in our model, focusing on the the evolution of the effective speed of sound and that of the Jeans length. With this insight, we can set theoretical constraints on the parameters of the model, predicting sufficient conditions for the model to be viable. An interesting feature of our models is that what can be interpreted as w(DE) can be < -1 without violating the null energy conditions.
C1 [Bertacca, Daniele] Univ Padua, Dipartimento Fis Galileo Galilei, I-35131 Padua, Italy.
[Bertacca, Daniele; Bruni, Marco] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Bertacca, Daniele] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Piattella, Oliver F.] Univ Fed Espirito Santo, Dept Phys, BR-29075910 Vitoria, ES, Brazil.
[Piattella, Oliver F.] Ist Nazl Fis Nucl, Sez Milano, I-20133 Milan, Italy.
[Pietrobon, Davide] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bertacca, D (reprint author), Univ Padua, Dipartimento Fis Galileo Galilei, Via F Marzolo 8, I-35131 Padua, Italy.
EM daniele.bertacca@pd.infn.it; marco.bruni@port.ac.uk;
oliver.piattella@gmail.com; davide.pietrobon@jpl.nasa.gov
RI Piattella, Oliver/J-4373-2013
OI Piattella, Oliver/0000-0003-4558-0574
FU ASI [I/016/07/0]; STFC [ST/H002774/1]; CNPq [150143/2010-9]; National
Aeronautics and Space Administration
FX DB would like to acknowledge the ICG (Portsmouth) for the hospitality
during the development of this project and "Fondazione Ing. Aldo Gini"
for support. DB research has been partly supported by ASI contract
I/016/07/0 "COFIS". MB is supported by STFC grant ST/H002774/1. OFP
research has been supported by the CNPq contract 150143/2010-9. Part of
the research of DP was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. The authors also thank N. Bartolo,
B. R. Crittenden, R. Maartens, S. Matarrese for discussions and
suggestions.
NR 78
TC 11
Z9 11
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD FEB
PY 2011
IS 2
AR 018
DI 10.1088/1475-7516/2011/02/018
PG 25
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 728FK
UT WOS:000287859800019
ER
PT J
AU Ditty, JG
Bremer, JRA
AF Ditty, James G.
Bremer, Jaime R. Alvarado
TI SPECIES DISCRIMINATION OF POSTLARVAE AND EARLY JUVENILE BROWN SHRIMP
(FARFANTEPENAEUS AZTECUS) AND PINK SHRIMP (F. DUORARUM) (DECAPODA:
PENAEIDAE): COUPLING MOLECULAR GENETICS AND COMPARATIVE MORPHOLOGY TO
IDENTIFY EARLY LIFE STAGES
SO JOURNAL OF CRUSTACEAN BIOLOGY
LA English
DT Article
DE Farfantepenaeus; General Discriminant Analysis; Gulf of Mexico;
multiplex PCR assay; spinules
ID GENUS PENAEUS; STOCK IDENTIFICATION; SETIFERUS LINNAEUS; WHITE SHRIMP;
POPULATION; HYBRIDIZATION; TEXAS; DNA; DIFFERENTIATION; BURKENROAD
AB We collected postlarvae (PL) and early juveniles of Farfantepenaeus aztecus and F. duorarum < 7.0 mm CL from the Gulf of Mexico and verified their species identity using a multiplex Polymerase Chain Reaction (PCR) assay, which targeted the 16S rRNA mitochondria! gene. We examined young with >= 5 dorsal teeth (DT) for differences in morphology and used a General Discriminant Analysis approach and 'best' subsets model-building technique to help identify the 'best' characters to discriminate taxa and predict species membership. Farfantepenaeus duorarum with >= 5 DT and F. aztecus with >= 7 DT have spinules on the epigastric and first DT, a character not previously reported for these two species. Differences in antennal scale shape and sixth pleomere length discriminate > 95% of Farfantepenaeus sp. with < 7 - 8 + 2 rostral teeth. Farfantepenaeus duorarum has an antenna! scale with an acutely rounded margin about twice the height of the adjacent lateral spine, and has a sixth pleomere length measurement < 2.5 mm. In F. aztecus, the antennal scale has a more broadly rounded margin with a lateral spine that approaches or exceeds the tip of the scale, and has a sixth pleomere length measurement > 2.5 mm. Species discrimination of Farfantepenaeus sp. with >= 7 - 8 + 2 rostral teeth requires body measurements. Classification models accurately discriminate > 90% of Farfantepenaeus sp. from the western Gulf and increase the reliability of discrimination by > 20% over characters that have been used for species discrimination, some of which are unreliable. The unsatisfactory performance of the models in discriminating Farfantepenaeus sp. from the eastern Gulf is consistent with the possibility of different ecological populations in the eastern and western Gulf that may warrant further study. Integration of molecular taxonomy and comparative morphology, as we did here, can provide insight into the patterns of diversity and ecological and evolutionary principles that encompass fisheries management.
C1 [Ditty, James G.] Natl Marine Fisheries Serv, NOAA, Galveston, TX 77551 USA.
[Bremer, Jaime R. Alvarado] Texas A&M Univ, Dept Marine Biol, Galveston, TX 77553 USA.
RP Ditty, JG (reprint author), Natl Marine Fisheries Serv, NOAA, 4700 Ave U, Galveston, TX 77551 USA.
EM Jim.Ditty@NOAA.gov; alvaradj@tamug.edu
RI Ditty, Jim/B-6686-2009
FU Texas Sea [424013]
FX We thank Texas Sea Grant for funding this study (Project 424013) and the
Southeast Fisheries Science Center, NOAA for additional support. Thanks
to Shawn Hillen, Juan Salas, Jennifer Doerr, Jennifer Atchison, and Dr.
Ronnie Baker of NOAA's Galveston Laboratory who participated in sample
collection. We also thank Dr. Ed Matheson, Nicole Dunham and Bobby
McDonald of the Florida Freshwater Fish Commission; Dr. Jim Tolan of
Texas Parks and Wildlife Department; and, Dr. Maria Criales of the
University of Miami, Florida, for providing shrimp from other areas of
the Gulf of Mexico for comparison. Thanks also to Dr. Darryl Felder of
the University of Louisiana, Lafayette; Dr. Heather Bracken currently of
Brigham Young University, Provo, Utah; and, Brandon Saxton, formerly of
Texas A&M University, Galveston, for assistance with molecular
identification. We also thank two anonymous reviewers for suggested
manuscript improvements. The findings and conclusions of this study are
those of the authors and do not necessarily represent the views of the
funding agency or NOAA.
NR 57
TC 5
Z9 5
U1 2
U2 12
PU CRUSTACEAN SOC
PI SAN ANTONIO
PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA
SN 0278-0372
J9 J CRUSTACEAN BIOL
JI J. Crustac. Biol.
PD FEB
PY 2011
VL 31
IS 1
BP 126
EP 137
DI 10.1651/10-3304.1
PG 12
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 722JA
UT WOS:000287427300014
ER
PT J
AU Zupanski, D
Zhang, SQ
Zupanski, M
Hou, AY
Cheung, SH
AF Zupanski, Dusanka
Zhang, Sara Q.
Zupanski, Milija
Hou, Arthur Y.
Cheung, Samson H.
TI A Prototype WRF-Based Ensemble Data Assimilation System for Dynamically
Downscaling Satellite Precipitation Observations
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID AFFECTED MICROWAVE RADIANCES; RESOLVING MODEL SIMULATIONS; EFFICIENT
DATA ASSIMILATION; TRANSFORM KALMAN FILTER; PART I; 1D+4D-VAR
ASSIMILATION; CLOUD; ECMWF; IMPLEMENTATION; RESOLUTION
AB In the near future, the Global Precipitation Measurement (GPM) mission will provide precipitation observations with unprecedented accuracy and spatial/temporal coverage of the globe. For hydrological applications, the satellite observations need to be downscaled to the required finer-resolution precipitation fields. This paper explores a dynamic downscaling method using ensemble data assimilation techniques and cloud-resolving models. A prototype ensemble data assimilation system using the Weather Research and Forecasting Model (WRF) has been developed. A high-resolution regional WRF with multiple nesting grids is used to provide the first-guess and ensemble forecasts. An ensemble assimilation algorithm based on the maximum likelihood ensemble filter (MLEF) is used to perform the analysis. The forward observation operators from NOAA-NCEP's gridpoint statistical interpolation (GSI) are incorporated for using NOAA-NCEP operational datastream, including conventional data and clear-sky satellite observations. Precipitation observation operators are developed with a combination of the cloud-resolving physics from NASA Goddard cumulus ensemble (GCE) model and the radiance transfer schemes from NASA Satellite Data Simulation Unit (SDSU). The prototype of the system is used as a test bed to optimally combine observations and model information to produce a dynamically downscaled precipitation analysis. A case study on Tropical Storm Erin (2007) is presented to investigate the ability of the prototype of the WRF Ensemble Data Assimilation System (WRF-EDAS) to ingest information from in situ and satellite observations including precipitation-affected radiance. The results show that the analyses and forecasts produced by the WRF-EDAS system are comparable to or better than those obtained with the WRF-GSI analysis scheme using the same set of observations. An experiment was also performed to examine how the analyses and short-term forecasts of microphysical variables and dynamical fields are influenced by the assimilation of precipitation-affected radiances. The results highlight critical issues to be addressed in the next stage of development such as model-predicted hydrometeor control variables and associated background error covariance, bias estimation, and correction in radiance space, as well as the observation error statistics. While further work is needed to optimize the performance of WRF-EDAS, this study establishes the viability of developing a cloud-scale ensemble data assimilation system that has the potential to provide a useful vehicle for downscaling satellite precipitation information to finer scales suitable for hydrological applications.
C1 [Zhang, Sara Q.; Hou, Arthur Y.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zupanski, Dusanka; Zupanski, Milija] Colorado State Univ, CIRA, Ft Collins, CO 80523 USA.
[Cheung, Samson H.] Univ Calif Davis, Davis, CA 95616 USA.
RP Zhang, SQ (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM sara.q.zhang@nasa.gov
RI Hou, Arthur/D-8578-2012; Measurement, Global/C-4698-2015
FU NASA Goddard Space Flight Center; NASA [NNX07AD75G]
FX This research was supported by the GPM Flight Project at NASA Goddard
Space Flight Center, and NASA Precipitation Measurement Mission (PMM)
Science Program under Grant NNX07AD75G to Colorado State University. The
authors of this manuscript would like to thank Toshi Takemura and
William Olson for providing radiative transfer models, and W.-K. Tao and
Roger Shi for providing Goddard microphysics schemes. The AMSR-E
radiance data was provided by National Snow and Ice Data Center, and
computations were carried out at NASA Advanced Supercomputing (NAS).
NR 39
TC 26
Z9 26
U1 2
U2 15
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD FEB
PY 2011
VL 12
IS 1
BP 118
EP 134
DI 10.1175/2010JHM1271.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 729YW
UT WOS:000287991600007
ER
PT J
AU Pueyo, L
Kasdin, NJ
Shaklan, S
AF Pueyo, Laurent
Kasdin, N. Jeremy
Shaklan, Stuart
TI Propagation of aberrations through phase-induced amplitude apodization
coronagraph
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA A-OPTICS IMAGE SCIENCE AND
VISION
LA English
DT Article
ID LYOT CORONAGRAPHS; CONTRAST; SENSITIVITY; SYSTEMS
AB The specification of polishing requirements for the optics in coronagraphs dedicated to exoplanet detection requires careful and accurate optical modeling. Numerical representations of propagated aberrations through the system as well as simulations of the broadband wavefront compensation system using multiple DMs are critical when one devises an error budget for such a class of instruments. In this communication, we introduce an analytical tool that serves this purpose for phase-induced amplitude apodization (PIAA) coronagraphs. We first start by deriving the analytical form of the propagation of a harmonic ripple through a PIAA unit. Using this result, we derive the chromaticity of the field at any plane in the optical train of a telescope equipped with such a coronagraph. Finally, we study the chromatic response of a two-sequential-DM wavefront actuator correcting such a corrugated field and thus quantify the requirements on the manufacturing of PIAA mirrors. (C) 2011 Optical Society of America
C1 [Pueyo, Laurent] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Pueyo, Laurent] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kasdin, N. Jeremy] Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA.
[Shaklan, Stuart] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pueyo, L (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 366 Bloomberg Ctr 3400 N Charles St, Baltimore, MD 21218 USA.
EM lap@pha.jhu.edu
FU NASA
FX The research described in this publication was carried out at the Jet
Propulsion Laboratory (JPL), California Institute of Technology
(Caltech), under a contract with the National Aeronautics and Space
Administration (NASA). The first author was supported by an appointment
to the NASA Post-doctoral Program at the JPL, Caltech, administered by
Oak Ridge Associated Universities through a contract with NASA. This
work was also performed in part under contract with California Institute
of Technology funded by NASA through the Sagan Fellowship Program.
NR 19
TC 7
Z9 7
U1 0
U2 2
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1084-7529
J9 J OPT SOC AM A
JI J. Opt. Soc. Am. A-Opt. Image Sci. Vis.
PD FEB
PY 2011
VL 28
IS 2
BP 189
EP 202
DI 10.1364/JOSAA.28.000189
PG 14
WC Optics
SC Optics
GA 716CG
UT WOS:000286941900011
PM 21293522
ER
PT J
AU Righter, K
Chabot, NL
AF Righter, Kevin
Chabot, Nancy L.
TI Moderately and slightly siderophile element constraints on the depth and
extent of melting in early Mars
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Review
ID TERRESTRIAL MAGMA OCEAN; SHERGOTTITE PARENT BODY; SILICATE
PARTITION-COEFFICIENTS; X-RAY SPECTROMETER; CORE FORMATION;
HIGH-PRESSURE; MARTIAN MANTLE; OXIDATION-STATE; EARLY DIFFERENTIATION;
OXYGEN FUGACITY
AB The thermal history of Mars during accretion and differentiation is important for understanding some fundamental aspects of its evolution such as crust formation, mantle geochemistry, chronology, volatile loss and interior degassing, and atmospheric development. In light of data from new Martian meteorites and exploration rovers, we have made a new estimate of Martian mantle siderophile element depletions. New high pressure and temperature metal-silicate experimental partitioning data and expressions are also available. Using these new constraints, we consider the conditions under which the Martian mantle may have equilibrated with metallic liquid. The resulting conditions that best satisfy six siderophile elements-Ni, Co, W, Mo, P, and Ga-and are consistent with the solidus and liquidus of the Martian mantle phase diagram are a pressure of 14 +/- 3 GPa and temperature of 2100 +/- 200 K. The Martian mantle depletions of Cr and V are also consistent with metal-silicate equilibration in this pressure and temperature range if deep mantle silicate phases are also taken into account. The results are not consistent with either metal-silicate equilibrium at the surface or at the current-day Martian core-mantle boundary. Recent measurements and modeling have concluded that deep (similar to 17 GPa or 1350 km) mantle melting is required to explain isotopic data for Martian meteorites and the nature of differentiation into core, mantle, and crust. This is in general agreement with our estimates of the conditions of Martian core formation based on siderophile elements that result in an intermediate depth magma ocean scenario for metal-silicate equilibrium.
C1 [Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA.
[Chabot, Nancy L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
RI Chabot, Nancy/F-5384-2015
OI Chabot, Nancy/0000-0001-8628-3176
FU Mars Fundamental Research Program; NASA [NNX09AG90G]
FX This research was supported by an award from the Mars Fundamental
Research Program to K. R. and NASA Cosmochemistry grant NNX09AG90G to N.
L. C. The conclusions have benefitted from discussions with V. Debaille,
A. Brandon, J. Jones, E. Medard, and L. Danielson. We appreciate the
helpful and detailed journal reviews of J. Day, R. Fonseca, and N.
Shirai, and editor R. Korotev.
NR 123
TC 23
Z9 23
U1 0
U2 15
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD FEB
PY 2011
VL 46
IS 2
BP 157
EP 176
DI 10.1111/j.1945-5100.2010.01140.x
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 723DU
UT WOS:000287487300001
ER
PT J
AU Herzog, GF
Albrecht, A
Ma, PX
Fink, D
Klein, J
Middleton, R
Bogard, DD
Nyquist, LE
Shih, CY
Garrison, DH
Reese, Y
Masarik, J
Reedy, RC
Rugel, G
Faestermann, T
Korschinek, G
AF Herzog, G. F.
Albrecht, Achim
Ma, Peixue
Fink, David
Klein, Jeffrey
Middleton, Roy
Bogard, Donald D.
Nyquist, L. E.
Shih, C. -Y.
Garrison, D. H.
Reese, Young
Masarik, J.
Reedy, R. C.
Rugel, G.
Faestermann, T.
Korschinek, G.
TI Cosmic-ray exposure history of the Norton County enstatite achondrite
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID PRE-ATMOSPHERIC SIZE; RARE-EARTH ELEMENTS; NEUTRON-CAPTURE;
PRODUCTION-RATES; STONY METEORITES; NOBLE-GASES; HIGH FLUENCES; PARENT
BODY; AUBRITES; CA-41
AB We report measurements of cosmogenic nuclides in up to 11 bulk samples from various depths in Norton County. The activities of 36Cl, 41Ca, 26Al, and 10Be were measured by accelerator mass spectrometry; the concentrations of the stable isotopes of He, Ne, Ar, and Sm were measured by electron and thermal ionization mass spectrometry, respectively. Production rates for the nuclides were modeled using the LAHET and the Monte Carlo N-Particle codes. Assuming a one-stage irradiation of a meteoroid with a pre-atmospheric radius of approximately 50 cm, the model satisfactorily reproduces the depth profiles of 10Be, 26Al, and 53Mn (< 6%) but overestimates the 41Ca concentrations by about 20%. 3He, 21Ne, and 26Al data give a one-stage cosmic-ray exposure (CRE) age of 115 Ma. Argon-36 released at intermediate temperatures, 36Ar(n), is attributed to production by thermal neutrons. From the values of 36Ar(n), an assumed average Cl concentration of 4 ppm, and a CRE age of 115 Ma, we estimate thermal neutron fluences of 1-4 x 1016 neutrons cm-2. We infer comparable values from epsilon 149Sm and epsilon 150Sm. Values calculated from 41Ca and a CRE age of 115 Ma, 0.2-1.4 x 1016 neutrons cm-2, are lower by a factor of approximately 2.5, indicating that nearly half of the 149Sm captures occurred earlier. One possible irradiation history places the center of proto-Norton County at a depth of 88 cm in a large body for 140 Ma prior to its liberation as a meteoroid with a radius of 50 cm and further CRE for 100 Ma.
C1 [Herzog, G. F.; Albrecht, Achim; Ma, Peixue] Rutgers State Univ, Dept Chem & Chem Biol, Piscataway, NJ 08854 USA.
[Fink, David] Australian Nucl Sci & Technol Org, Inst Environm Res, Sydney, NSW 2234, Australia.
[Klein, Jeffrey; Middleton, Roy] Univ Penn, Dept Phys, Philadelphia, PA 19104 USA.
[Bogard, Donald D.; Nyquist, L. E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Shih, C. -Y.; Garrison, D. H.] Jacobs Sverdrup, ESCG, Houston, TX 77058 USA.
[Reese, Young] ESCG Muniz Engn, Houston, TX 77058 USA.
[Masarik, J.] Comenius Univ, Dept Nucl Phys, Bratislava 84215, Slovakia.
[Reedy, R. C.] Planetary Sci Inst, Los Alamos, NM 87544 USA.
[Rugel, G.; Faestermann, T.; Korschinek, G.] Tech Univ Munich, Fak Phys, D-85748 Garching, Germany.
RP Herzog, GF (reprint author), Rutgers State Univ, Dept Chem & Chem Biol, 610 Taylor Rd, Piscataway, NJ 08854 USA.
EM herzog@rutchem.rutgers.edu
RI fink, David/A-9518-2012; Klein, Jeffrey/E-3295-2013;
OI Reedy, Robert/0000-0002-2189-1303; Faestermann,
Thomas/0000-0002-6603-8787
FU NASA [NNG05GF82G]; Slovak Research and Development Agency [APVV-0569-07]
FX We thank Ed Scott for samples and information about them; Devendra Lal
and N. Bhandari for sharing track data; Mitsuru Ebihara for information
concerning rare earth concentrations; Feride Serefiddin for assistance
with the elemental Ca analyses; Paul Field for assistance with ICP-MS
measurements; and Adrian Brearley, Horton Newsom, and Don Burnett for
helpful comments. We benefited from reviews by H. Hidaka and K. Welten.
This work was supported in part by NASA grant NNG05GF82G (G. F. H.), by
NASA's Cosmochemistry Program (D. D. B. and L. E. N.), and by the Slovak
Research and Development Agency under the contract no. APVV-0569-07 (J.
M.).
NR 63
TC 8
Z9 8
U1 1
U2 14
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD FEB
PY 2011
VL 46
IS 2
BP 284
EP 310
DI 10.1111/j.1945-5100.2010.01154.x
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 723DU
UT WOS:000287487300008
ER
PT J
AU Yuan, HB
Liu, XW
Pequignot, D
Rubin, RH
Ercolano, B
Zhang, Y
AF Yuan, H-B
Liu, X-W
Pequignot, D.
Rubin, R. H.
Ercolano, B.
Zhang, Y.
TI Three-dimensional chemically homogeneous and bi-abundance
photoionization models of the 'super-metal-rich' planetary nebula NGC
6153
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM: abundances; planetary nebulae: individual: NGC 6153
ID HE-I LINE; OPTICAL RECOMBINATION LINES; HII-REGIONS; COLLISIONAL
EXCITATION; ELECTRON TEMPERATURES; DENSITY VARIATIONS; GASEOUS NEBULAE;
ORION-NEBULA; SPECTRUM; INTENSITIES
AB Deep spectroscopy of the planetary nebula NGC 6153 shows that its heavy element abundances derived from optical recombination lines (ORLs) are 10 times higher than those derived from collisionally excited lines (CELs), and points to the existence of H-deficient inclusions embedded in the diffuse nebula. In this study, we have constructed chemically homogeneous and bi-abundance three-dimensional photoionization models, using the Monte Carlo photoionization code mocassin. We attempt to reproduce the multiwaveband spectroscopic and imaging observations of NGC 6153, and investigate the nature and origin of the postulated H-deficient inclusions, as well as their impacts on the empirical nebular analyses assuming a uniform chemical composition. Our results show that chemically homogeneous models yield small electron temperature fluctuations and fail to reproduce the strengths of ORLs from C, N, O and Ne ions. In contrast, bi-abundance models incorporating a small amount of metal-rich inclusions (similar to 1.3 per cent of the total nebular mass) are able to match all the observations within the measurement uncertainties. The metal-rich clumps, cooled down to a very low temperature (similar to 800 K) by ionic infrared fine-structure lines, dominate the emission of heavy element ORLs, but contribute almost nil to the emission of most CELs. We find that the abundances of C, N, O and Ne derived empirically from CELs, assuming a uniform chemical composition, are about 30 per cent lower than the corresponding average values of the whole nebula, including the contribution from the H-deficient inclusions. Ironically, in the presence of H-deficient inclusions, the traditional standard analysis of the optical helium recombination lines, assuming a chemically homogeneous nebula, overestimates the helium abundance by 40 per cent.
C1 [Yuan, H-B; Liu, X-W] Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
[Liu, X-W; Rubin, R. H.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Pequignot, D.] CNRS, LUTH, Lab Univers & Ses Theories, FRE 2462, F-92195 Meudon, France.
[Pequignot, D.] Univ Paris 07, Observ Paris Meudon, F-92195 Meudon, France.
[Rubin, R. H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rubin, R. H.] Orion Enterprises, Moffett Field, CA 94035 USA.
[Ercolano, B.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Ercolano, B.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Ercolano, B.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Zhang, Y.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
RP Yuan, HB (reprint author), Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
EM x.liu@pku.edu.cn
FU STFC; HKU [200909159007]; NASA Science Mission Directorate [SMD-08-0633,
SMD-09-1154]
FX We would like to thank the referee for the valuable comments, which
helped improve the quality of the paper. The modelling was carried out
on the SGI Altix330 System at the Department of Astronomy at Peking
University, HP supercomputer operated by the Center for Computational
Science and Engineering at Peking University and the Columbia
supercomputer operated by the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center. We acknowledge our awards, SMD-08-0633
and SMD-09-1154, of High-End Computing (HEC) time on NAS and NCCS
resources by the NASA Science Mission Directorate (SMD). We thank Johnny
Chang for his able and generous support of our research using Columbia.
This research has made use of NASA's Astrophysics Data System
Bibliographic Services. BE is supported by an STFC Advanced Fellowship.
YZ acknowledges financial support from the Seed Funding Programme for
Basic Research in HKU (200909159007).
NR 60
TC 11
Z9 11
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 FEB
PY 2011
VL 411
IS 2
BP 1035
EP 1052
DI 10.1111/j.1365-2966.2010.17732.x
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716QO
UT WOS:000286988800023
ER
PT J
AU Zenitani, S
Miyoshi, T
AF Zenitani, Seiji
Miyoshi, Takahiro
TI Magnetohydrodynamic structure of a plasmoid in fast reconnection in
low-beta plasmas
SO PHYSICS OF PLASMAS
LA English
DT Article
ID FAST MAGNETIC RECONNECTION; ISOLATED CURRENT-SHEET; SOLAR-FLARES; 3
DIMENSIONS; MAGNETOTAIL; MECHANISM; EVOLUTION; COMPUTER; SIMULATIONS;
SHOCKS
AB Plasmoid structures in fast reconnection in low-beta plasmas are investigated by two-dimensional magnetohydrodynamic simulations. A high-resolution shock-capturing code enables us to explore a variety of shock structures: vertical slow shocks behind the plasmoid, another slow shock in the outer-region, and the shock-reflection in the front side. The Kelvin-Helmholtz-like turbulence is also found inside the plasmoid. It is concluded that these shocks are rigorous features in reconnection in low-beta plasmas, where the reconnection jet speed or the upstream Alfven speed exceeds the sound speed. (C) 2011 American Institute of Physics. [doi:10.1063/1.3554655]
C1 [Zenitani, Seiji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Miyoshi, Takahiro] Hiroshima Univ, Grad Sch Sci, Dept Phys Sci, Higashihiroshima 7398526, Japan.
RP Zenitani, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM seiji.zenitani-1@nasa.gov
RI Zenitani, Seiji/D-7988-2013
OI Zenitani, Seiji/0000-0002-0945-1815
FU JSPS [21740399]
FX S.Z. gratefully acknowledges the support from JSPS Fellowship for
Research Abroad. T. M. was partially supported by Grant-in-Aid for Young
Scientists (B) (Grant No. 21740399).
NR 54
TC 16
Z9 16
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-664X
J9 PHYS PLASMAS
JI Phys. Plasmas
PD FEB
PY 2011
VL 18
IS 2
AR 022105
DI 10.1063/1.3554655
PG 9
WC Physics, Fluids & Plasmas
SC Physics
GA 727PH
UT WOS:000287812900006
ER
PT J
AU Tukel, OI
Kremic, T
Rom, WO
Miller, RJ
AF Tukel, Oya I.
Kremic, Tibor
Rom, Walter O.
Miller, Richard J.
TI Knowledge-Salvage Practices for Dormant R&D Projects
SO PROJECT MANAGEMENT JOURNAL
LA English
DT Article
DE R&D projects; knowledge banks; system dynamics
ID OPEN INNOVATION; FIRM; PERFORMANCE; VIEW
AB Most successful firms have an abundance of new and old knowledge in their research and development laboratories, and only a fraction is being put into use in new product development. This knowledge is left over from projects that have been killed at different development stages and may actually carry considerable value. In this article, we propose a knowledge bank as a possible solution to preserve and possibly grow this knowledge. It is a self-sustaining institute with minimal or no ongoing effort from the donor company, yet manages the knowledge in a way that protects proprietary interests and actively fosters communication and interchange among sponsoring companies wherever possible. The framework of this structure, as well as how it works, is described here. Specifically, a system dynamics modeling of the knowledge bank is developed, and a simulation study is conducted using VENSIM (R). The results confirm the viability of creating such a system in a consortium of organizations.
C1 [Tukel, Oya I.; Rom, Walter O.; Miller, Richard J.] Cleveland State Univ, Operat & Supply Chain Management Dept, Cleveland, OH 44115 USA.
[Kremic, Tibor] NASA, John H Glenn Res Ctr, Cleveland, OH USA.
RP Tukel, OI (reprint author), Cleveland State Univ, Operat & Supply Chain Management Dept, Cleveland, OH 44115 USA.
NR 36
TC 4
Z9 4
U1 1
U2 7
PU WILEY PERIODICALS, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN STREET, MALDEN, MA 02148-529 USA
SN 8756-9728
J9 PROJ MANAG J
JI Proj. Manag. J.
PD FEB
PY 2011
VL 42
IS 1
BP 59
EP 72
DI 10.1002/pmj.20207
PG 14
WC Management
SC Business & Economics
GA 713BQ
UT WOS:000286710400006
ER
PT J
AU Stothers, RB
AF Stothers, Richard B.
TI Further Evidence of Convective Cycles in Blazhko RR Lyrae Stars
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID MW LYR
AB The theory of slow convective cycles in the envelopes of RR Lyrae stars showing the Blazhko effect predicts an anticorrelation between the pulsation period and radius for hot members of the group, contrary to what might be expected from the (period, mean density) relation. This negative correlation has actually been observed by Jurcsik et al. for the hot stars MW Lyr, DM Cyg, and (in pail) CZ Lac, the only stars so far measured accurately for radius variations over a Blazhko cycle. Significantly cooler members of the group would be expected to show a normal, positive correlation between pulsation period and radius.
C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Stothers, RB (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM rstothers@giss.nasa.gov
NR 13
TC 5
Z9 5
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD FEB
PY 2011
VL 123
IS 900
BP 127
EP 129
DI 10.1086/658635
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 728WI
UT WOS:000287904800002
ER
PT J
AU Catanzarte, J
Shao, M
AF Catanzarte, Joseph
Shao, Michael
TI Exo-Earth/Super-Earth Yield of JWST Plus a Starshade External Occulter
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID EXTRASOLAR PLANETS; ASTROMETRY; DETECTABILITY; COMPLETENESS; SEARCH;
MASS
AB We estimate the exo-Earth/super-Earth yield of an imaging mission that combines the James Webb Space Telescope (JWST) with a starshade external occulter under a realistic set of astrophysical assumptions. For the purpose of this study, we define "exo-Earth" and "super-Earth" as a planet of mass 1 to 2 M-circle plus and 2 to 10 M-circle plus, respectively, orbiting within the habitable zone (HZ) of a solar-type star. We show that for a survey strategy that relies on a single image as the basis for detection, roughly half of all exo-Eaqh/super-Earth detections will be false alarms for eta(circle plus) of 0.1, 0.2, and 0.3. Here, a false alarm is a mistaken identification of a planet as an exo-Earth/super-Earth, and we define eta(circle plus) as the frequency of exo-Earth/super-Earths orbiting sunlike stars. We then consider two different survey strategies designed to mitigate the false alarm problem. The first is to require that for each candidate exo-Earth/super-Earth, a sufficient number of detections are made to measure the orbit. When the orbit is known we can determine if the planet is in the habitable zone. With this strategy, we find that the number of exo-Earth/super-Earths found is, on average, 0.9, 1.9, and 2.7 for eta(circle plus) = 0.1, 0.2, and 0.3. There is a similar to 40% probability of finding zero exo-Earth/super-Earths for eta(circle plus) = 0.1. A second strategy can be employed if a space-based astrometry mission capable of submicroarcsecond precision has identified and measured the orbits and masses of the planets orbiting nearby stars. In this case, the occulter mission is much more efficient, because it surveys only the stars known to have exo-Earth/super-Earths. We find that with prior knowledge from a space-based astrometric survey of 60 nearby stars, JWST plus an external occulter can obtain spectra, as well as orbital solutions, for the majority (70% to 80%) of the exo-Earth/super-Earths orbiting these 60 stars. The yield of exo-Earth/super-Earths is approximately five times higher than the yield for the JWST plus occulter mission without prior astrometric information. With prior space-based astrometry, the probability that an imaging mission will find zero exo-Earth/super-Earths is reduced to <1% for the case of eta(circle plus) = 0.1.
C1 [Catanzarte, Joseph; Shao, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Catanzarte, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM joseph.catanzarite@jpl.nasa.gov; michael.shao@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research described in this article was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
Copyright (c) 2010 California Institute of Technology. Government
sponsorship acknowledged. We thank Doug Lisman for providing the target
list for the Occulting Ozone Observatory mission. We thank Steve Edberg,
Varoujan Gorjian, Jim Marr, Xiaopei Pan, and especially John Davidson
and Steve Unwin, for critical reading and constructive comments and
suggestions. We wish to thank the referee for a valuable review that
contributed to many improvements in the article.
NR 25
TC 2
Z9 2
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD FEB
PY 2011
VL 123
IS 900
BP 171
EP 178
DI 10.1086/658243
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 728WI
UT WOS:000287904800005
ER
PT J
AU Kitiashvili, IN
Kosovichev, AG
Mansour, NN
Wray, AA
AF Kitiashvili, I. N.
Kosovichev, A. G.
Mansour, N. N.
Wray, A. A.
TI EXCITATION OF ACOUSTIC WAVES BY VORTICES IN THE QUIET SUN
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE hydrodynamics; methods: numerical; Sun: granulation; Sun: oscillations;
turbulence; waves
ID DRIVEN VORTEX FLOWS; SOLAR OSCILLATIONS; NUMERICAL SIMULATIONS;
CONVECTION; PHOTOSPHERE; GRANULATION; ORIGIN; MODEL
AB The five-minute oscillations are one of the basic properties of solar convection. Observations show a mixture of a large number of acoustic wave fronts propagating from their sources. We investigate the process of acoustic waves excitation from the point of view of individual events, by using a realistic three-dimensional radiative hydrodynamic simulation of the quiet Sun. The results show that the excitation events are related to the dynamics of vortex tubes (or swirls) in intergranular lanes of solar convection. These whirlpool-like flows are characterized by very strong horizontal velocities (7-11 km s(-1)) and downflows (approximate to 7 km s(-1)), and are accompanied by strong decreases of temperature, density, and pressure at the surface and 0.5-1 Mm below the surface. High-speed whirlpool flows can attract and capture other vortices. According to our simulation results the processes of vortex interaction, such as vortex annihilation, can cause excitation of acoustic waves on the Sun.
C1 [Kitiashvili, I. N.; Kosovichev, A. G.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Mansour, N. N.; Wray, A. A.] NASA, Ames Res Ctr, Mountain View, CA 94040 USA.
RP Kitiashvili, IN (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM irinasun@stanford.edu
FU International Space Science Institute (ISSI, Bern)
FX The authors thank participants of the ISSI team "Filamentary Structure
and Dynamics of Solar Magnetic Fields," and Drs. G. D. Chagelishvili, J.
G. Lominadze, M. Stix, R. Schichenmaier, and O. Steiner for useful
discussions, and also the International Space Science Institute (ISSI,
Bern) for support.
NR 24
TC 32
Z9 32
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
PY 2011
VL 727
IS 2
AR L50
DI 10.1088/2041-8205/727/2/L50
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706DB
UT WOS:000286196200023
ER
PT J
AU Grainger, S
Frederiksen, CS
Zheng, XG
Fereday, D
Folland, CK
Jin, EK
Kinter, JL
Knight, JR
Schubert, S
Syktus, J
AF Grainger, Simon
Frederiksen, Carsten S.
Zheng, Xiaogu
Fereday, David
Folland, Chris K.
Jin, Emilia K.
Kinter, James L.
Knight, Jeff R.
Schubert, Siegfried
Syktus, Jozef
TI Modes of variability of Southern Hemisphere atmospheric circulation
estimated by AGCMs
SO CLIMATE DYNAMICS
LA English
DT Article
DE Modes of variability; Southern Hemisphere; Atmospheric circulation;
ENSO; Southern Annular Mode
ID LOW-FREQUENCY VARIABILITY; SEA-SURFACE TEMPERATURE; SEASONAL-MEAN
FIELDS; INTRASEASONAL VARIABILITY; STORM TRACKS; ANOMALIES; BLOCKING;
TELECONNECTIONS; REANALYSIS; DISTURBANCES
AB The seasonal mean variability of the atmospheric circulation is affected by processes with time scales from less than seasonal to interannual or longer. Using monthly mean data from an ensemble of Atmospheric General Circulation Model (AGCM) realisations, the interannual variability of the seasonal mean is separated into intraseasonal, and slowly varying components. For the first time, using a recently developed method, the slowly varying component in multiple AGCM ensembles is further separated into internal and externally forced components. This is done for Southern Hemisphere 500 hPa geopotential height from five AGCMs in the CLIVAR International Climate of the Twentieth Century project for the summer and winter seasons. In both seasons, the intraseasonal and slow modes of variability are qualitatively well reproduced by the models when compared with reanalysis data, with a relative metric finding little overall difference between the models. The Southern Annular Mode (SAM) is by far the dominant mode of slowly varying internal atmospheric variability. Two slow-external modes of variability are related to El Nio-Southern Oscillation (ENSO) variability, and a third is the atmospheric response to trends in external forcing. An ENSO-SAM relationship is found in the model slow modes of variability, similar to that found by earlier studies using reanalysis data. There is a greater spread in the representation of model slow-external modes in winter than summer, particularly in the atmospheric response to external forcing trends. This may be attributable to weaker external forcing constraints on SH atmospheric circulation in winter.
C1 [Grainger, Simon; Frederiksen, Carsten S.] Bur Meteorol, Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia.
[Zheng, Xiaogu] Natl Inst Water & Atmospher Res, Wellington, New Zealand.
[Zheng, Xiaogu] Beijing Normal Univ, Coll Global Change & Earth Syst, Beijing 100875, Peoples R China.
[Fereday, David; Folland, Chris K.; Knight, Jeff R.] Hadley Ctr Climate Change, Met Off, Exeter, Devon, England.
[Jin, Emilia K.; Kinter, James L.] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA.
[Jin, Emilia K.; Kinter, James L.] Ctr Ocean Land Atmosphere Studies, Calverton, MD USA.
[Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Syktus, Jozef] Queensland Climate Change Ctr Excellence, Brisbane, Qld, Australia.
RP Grainger, S (reprint author), Bur Meteorol, Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia.
EM S.Grainger@bom.gov.au
RI Syktus, Jozef/E-7173-2011; Folland, Chris/I-2524-2013; Kinter,
James/A-8610-2015
OI Syktus, Jozef/0000-0003-1782-3073; Kinter, James/0000-0002-6277-0559
FU Australian Department of Climate Change; New Zealand Foundation for
Research, Science and Technology [C01X0701]; SRF for ROCS, SEM China;
DECC; MoD-DECC/Defra [GA01101]; MoD [CBC/2B/0417_Annex C5]; National
Science Foundation [ATM-0332910]; National Oceanic and Atmospheric
Administration [NA04OAR4310034]; National Aeronautics and Space
Administration [NNG04GG46G]; Defra
FX This work contributes to the CLIVAR International C20C project. J.
Sisson assisted in the collection of the C20C AGCM data. S. Grainger is
supported by the Australian Climate Change Science Program of the
Australian Department of Climate Change. X. Zheng is supported by the
New Zealand Foundation for Research, Science and Technology (contract
C01X0701) and the SRF for ROCS, SEM China. J. Knight, C. Folland and D.
Fereday were supported by the Joint DECC, Defra and MoD Integrated
Climate Programme-DECC/Defra (GA01101), MoD (CBC/2B/0417_Annex C5). E.
Jin and J. Kinter were supported by grants from the National Science
Foundation (ATM-0332910), National Oceanic and Atmospheric
Administration (NA04OAR4310034), and National Aeronautics and Space
Administration (NNG04GG46G). Comments from M. Zidikheri, H. Zhang and
two anonymous reviewers helped to improve this paper.
NR 49
TC 6
Z9 6
U1 0
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD FEB
PY 2011
VL 36
IS 3-4
BP 473
EP 490
DI 10.1007/s00382-009-0720-7
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 716AL
UT WOS:000286937100006
ER
PT J
AU Ferguson, IM
Duffy, PB
Phillips, TJ
Liang, X
Dracup, JA
Schubert, S
Pegion, P
AF Ferguson, Ian M.
Duffy, Philip B.
Phillips, Thomas J.
Liang, Xu
Dracup, John A.
Schubert, Siegfried
Pegion, Philip
TI Non-stationarity of the signal and noise characteristics of seasonal
precipitation anomalies
SO CLIMATE DYNAMICS
LA English
DT Article
ID WESTERN UNITED-STATES; POTENTIAL PREDICTABILITY; INTERANNUAL
VARIABILITY; CLIMATE PREDICTABILITY; ENSO TELECONNECTIONS; NATURAL
VARIABILITY; BOUNDARY-CONDITIONS; SIMULATION SKILLS; GCM SIMULATIONS;
ENSEMBLE
AB In order to improve seasonal-to-interannual precipitation forecasts and their application by decision makers, there is a clear need to understand when, where, and to what extent seasonal precipitation anomalies are driven by potentially predictable surface-atmosphere interactions versus to chaotic interannual atmospheric dynamics. Using a simple Monte Carlo approach, interannual variability and linear trends in the SST-forced signal and potential predictability of boreal winter precipitation anomalies is examined in an ensemble of twentieth century AGCM simulations. Signal and potential predictability are shown to be non-stationary over more than 80% of the globe, while chaotic noise is shown to be stationary over most of the globe. Correlation analysis with respect to magnitudes of the four leading modes of global SST variability suggests that interannual variability and trends in signal and potential predictability over 35% of the globe is associated with ENSO-related SST variability; signal and potential predictability are not significantly associated with SST modes characterized by a global SST trend, North Atlantic SST variability, and North Pacific SST variability, respectively. Results suggest that mechanisms other than SST variability contribute to the non-stationarity of signal and noise characteristics of hydroclimatic variability over mid- and high-latitude regions.
C1 [Ferguson, Ian M.] Colorado Sch Mines, Dept Geol & Geol Engn, Golden, CO 80401 USA.
[Duffy, Philip B.] Climate Cent Inc, Palo Alto, CA USA.
[Phillips, Thomas J.] Lawrence Livermore Natl Lab, Program Climate Model Diagnost & Intercomparison, Livermore, CA USA.
[Liang, Xu] Univ Pittsburgh, Dept Civil & Environm Engn, Pittsburgh, PA USA.
[Dracup, John A.] Univ Calif Berkeley, Dept Civil & Environm Engn, Berkeley, CA 94720 USA.
[Schubert, Siegfried] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pegion, Philip] NOAA, Earth Syst Res Lab, Boulder, CO USA.
RP Ferguson, IM (reprint author), Colorado Sch Mines, Dept Geol & Geol Engn, Golden, CO 80401 USA.
EM imfergus@mines.edu; pduffy@climatecentral.org; phillips14@llnl.gov;
xuliang@engr.pitt.edu; dracup@ce.berkeley.edu;
siegfried.d.schubert@nasa.gov; Phillip.Pegion@noaa.gov
RI Pegion, Philip/E-5247-2012
NR 61
TC 3
Z9 3
U1 0
U2 3
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD FEB
PY 2011
VL 36
IS 3-4
BP 739
EP 752
DI 10.1007/s00382-010-0850-y
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 716AL
UT WOS:000286937100024
ER
PT J
AU Checa, R
Tapiador, FJ
AF Checa, Ramiro
Tapiador, Francisco J.
TI A Maximum Entropy Modelling of the Rain Drop Size Distribution
SO ENTROPY
LA English
DT Article
DE rain drop size distribution; maximum entropy method
ID MOMENT ESTIMATORS; CONVECTIVE CLOUDS; SPECTRA; GAMMA; PARAMETERS;
DISDROMETER; PRECIPITATION; ALGORITHM; PRINCIPLE; FORMALISM
AB This paper presents a maximum entropy approach to Rain Drop Size Distribution (RDSD) modelling. It is shown that this approach allows (1) to use a physically consistent rationale to select a particular probability density function (pdf) (2) to provide an alternative method for parameter estimation based on expectations of the population instead of sample moments and (3) to develop a progressive method of modelling by updating the pdf as new empirical information becomes available. The method is illustrated with both synthetic and real RDSD data, the latest coming from a laser disdrometer network specifically designed to measure the spatial variability of the RDSD.
C1 [Checa, Ramiro] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Checa, Ramiro; Tapiador, Francisco J.] Univ Castilla La Mancha, Fac Environm Sci, Inst Environm Sci, Toledo, Spain.
RP Checa, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM ramiro.checa@uclm.es; francisco.tapiador@uclm.es
RI Checa-Garcia, Ramiro/P-3426-2014
OI Checa-Garcia, Ramiro/0000-0001-7653-3653
FU JCCM [PPII10-0162-5543]; CENIT [CGL2010-20787]; MiCInn [UNCM08-1E-086];
FEDER
FX Funding from projects PPII10-0162-5543 (JCCM), CENIT project 'PROMETEO',
CGL2010-20787 and UNCM08-1E-086 (MiCInn) and FEDER is gratefully
acknowledged.
NR 42
TC 2
Z9 2
U1 0
U2 4
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 1099-4300
J9 ENTROPY-SWITZ
JI Entropy
PD FEB
PY 2011
VL 13
IS 2
BP 293
EP 315
DI 10.3390/e13020293
PG 23
WC Physics, Multidisciplinary
SC Physics
GA 726ON
UT WOS:000287733800001
ER
PT J
AU Edmonds, LD
AF Edmonds, Larry D.
TI A Proposed Transient Version of the ADC Charge-Collection Model Tested
Against TCAD
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE ADC model; ambipolar diffusion; charge collection; drift-diffusion
AB The ADC model is a charge-collection model mathematically derived for simple p-n junction diodes under steady-state conditions. A transient version of the model is postulated, rather than derived, and tested for correctness by comparisons with TCAD simulation predictions.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Edmonds, LD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM larry.d.edmonds@jpl.nasa.gov
FU U.S. Government or the Jet Propulsion Laboratory, California Institute
of Technology
FX The research in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. Reference herein to
any specific commercial product, process, or service by trade name,
trademark, manufacturer, or otherwise, does not constitute or imply its
endorsement by the U.S. Government or the Jet Propulsion Laboratory,
California Institute of Technology. Government sponsorship acknowledged.
NR 6
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD FEB
PY 2011
VL 58
IS 1
BP 296
EP 304
DI 10.1109/TNS.2010.2087770
PN 2
PG 9
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA 717YW
UT WOS:000287086200017
ER
PT J
AU Nettles, A
Hodge, A
Jackson, J
AF Nettles, Alan
Hodge, Andrew
Jackson, Justin
TI An Examination of the Compressive Cyclic Loading Aspects of Damage
Tolerance for Polymer Matrix Launch Vehicle Hardware
SO JOURNAL OF COMPOSITE MATERIALS
LA English
DT Article
DE fatigue; damage growth; requirements; delamination; impact; compression;
residual strength; load spectrum; launch vehicle
ID COMPOSITE SANDWICH PANELS; CARBON-FIBER; FATIGUE BEHAVIOR; PERFORMANCE;
FAILURE; GROWTH
AB The issue of fatigue loading of structures composed of composite materials is considered in a requirements document that is currently in place for manned launch vehicles. By taking into account the short lives of these parts, coupled with design considerations, it is demonstrated that the necessary coupon level fatigue data collapse to a static case. Data from a literature review of past studies that examined compressive fatigue loading after impact and data generated from this experimental study are presented to support this finding. In other studies from the literature, a stress amplitude of about 60% of the static compression after impact (CAI) strength was found to exist, below which fatigue had no deleterious effects up to one million cycles. In this study, a stress amplitude of about 80% of the static (CAI) strength was found to exist, below which fatigue had no deleterious effects up to 10,000 cycles. A launch vehicle structure should never experience one cycle above 61.4% of static CAI strength, much less 10,000 at 80%. Despite utilizing severe fatigue amplitude loading in impact damaged coupons, residual strength after fatigue was consistently higher than expected. Unrealistically high fatigue stress amplitudes were needed to fail 5 of 15 specimens, before 10,000 cycles was reached. Since a typical launch vehicle structure, such as the ARES I interstage, only experiences a few cycles near limit load, it is concluded that static CAI strength data will suffice for most launch vehicle structures.
C1 [Nettles, Alan; Hodge, Andrew; Jackson, Justin] NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL USA.
RP Nettles, A (reprint author), NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL USA.
EM alan.t.nettles@nasa.gov
FU National Aeronautics and Space Administration, Marshall Space Flight
Center [136905.08.05.12]
FX This study was supported by the National Aeronautics and Space
Administration under the auspices of the Upper Stage Program Office at
Marshall Space Flight Center (136905.08.05.12).
NR 48
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U2 4
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0021-9983
J9 J COMPOS MATER
JI J. Compos Mater.
PD FEB
PY 2011
VL 45
IS 4
BP 437
EP 458
DI 10.1177/0021998310376117
PG 22
WC Materials Science, Composites
SC Materials Science
GA 723UB
UT WOS:000287531600003
ER
PT J
AU Alston, EJ
Sokolik, IN
Doddridge, BG
AF Alston, Erica J.
Sokolik, Irina N.
Doddridge, Bruce G.
TI Investigation into the Use of Satellite Data in Aiding Characterization
of Particulate Air Quality in the Atlanta, Georgia Metropolitan Area
SO JOURNAL OF THE AIR & WASTE MANAGEMENT ASSOCIATION
LA English
DT Article
ID SOUTHEASTERN AEROSOL RESEARCH; OPTICAL DEPTH; UNITED-STATES; MATTER
MASS; POLLUTION; PM2.5; FINE; SURFACE; VISITS
AB Poor air quality episodes occur often in metropolitan Atlanta, GA. The primary focus of this research is to assess the capability of satellites as a tool in characterizing air quality in Atlanta. Results indicate that intracity PM2.5 (particulate matter <= 2.5 mu m in aerodynamic diameter) concentrations show similar patterns as other U.S. urban areas, with the highest concentrations occurring within the city. PM2.5 and MODIS (Moderate Resolution Imaging Spectroradiometer) aerosol optical depth (AOD) have higher values in the summer than spring, yet MODIS AOD doubles in the summer unlike PM2.5. Most (80%) of the Ozone Monitoring Instrument aerosol index (AI) is below 0.5 with little differences between spring and summer. Using this value as a constraint of the carbonaceous aerosol signal in the urban area, aerosol transport events such as wildfire smoke associated with higher positive AI values can be identified. The results indicate that MODIS AOD is well correlated with PM2.5 on a yearly and seasonal basis with correlation coefficients as high as 0.8 for Terra and 0.7 for Aqua. A possible alternative view of the PM2.5 and AOD relationship is seen through the use of AOD thresholds. These probabilistic thresholds provide a means to describe the air quality index (AQI) through the use of multiyear AOD records for a specific area. The National Ambient Air Quality Standards (NAAQS) are used to classify the AOD into different AQI codes and probabilistically determine thresholds of AOD that represent most of a specific AQI category. For example, 80% of cases of moderate AQI days have AOD values between 0.5 and 0.6. The development of AOD thresholds provides a useful tool for evaluating air quality from the use of satellites in regions where there are sparse ground-based measurements of PM2.5.
C1 [Alston, Erica J.; Doddridge, Bruce G.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA.
[Alston, Erica J.; Sokolik, Irina N.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
RP Alston, EJ (reprint author), Chem & Dynam Branch, 21 Langley Blvd MS 401B, Hampton, VA 23681 USA.
EM erica.j.alston@nasa.gov
OI Alston, Erica/0000-0001-6287-7914
FU Science Directorate, NASA Langley Research Center (LaRC); NASA
FX E.J. Alston thanks the Science Directorate, NASA Langley Research Center
(LaRC) for its support. I.N. Sokolik acknowledges support from the NASA
Radiation Sciences Program. All authors thank the anonymous reviewers
whose comments and suggestions improved the quality of this paper.
NR 34
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U1 0
U2 3
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 1096-2247
EI 2162-2906
J9 J AIR WASTE MANAGE
JI J. Air Waste Manage. Assoc.
PD FEB
PY 2011
VL 61
IS 2
BP 211
EP 225
DI 10.3155/1047-3289.61.2.211
PG 15
WC Engineering, Environmental; Environmental Sciences; Meteorology &
Atmospheric Sciences
SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric
Sciences
GA 717UY
UT WOS:000287074100009
PM 21387938
ER
PT J
AU Jacobson, NS
Myers, DL
AF Jacobson, N. S.
Myers, D. L.
TI Active Oxidation of SiC
SO OXIDATION OF METALS
LA English
DT Article
DE Active oxidation; Silicon carbide; Ceramics
ID TO-PASSIVE TRANSITION; DEPOSITED SILICON-CARBIDE; C-O SYSTEM;
HIGH-TEMPERATURE; LOW-PRESSURE; METALLIC SILICON; OXYGEN;
THERMODYNAMICS; NITRIDE; AIR
AB Silicon carbide (SiC) forms a protective condensed-phase oxide (SiO2) in passive oxidation and a volatile sub-oxide (SiO(g)) in active oxidation. The transition between these two modes of oxidation and the rates of active oxidation are critical issues. A literature review indicates that impurity effects, the difference between active-to-passive and passive-to-active transitions, and the effect of total pressure on these transitions remain unexplored for SiC. Measurements were made in a thermogravimetric apparatus (TGA) by changing oxygen potentials either by blending O-2/Ar mixtures or changing total pressures in a pure oxygen gas stream to the point where a transition occurs. Specimens were examined with standard optical and electron-optical techniques. Active-to-passive and passive-to-active transitions were measured and found to be similar for SiC, which is in contrast to pure Si. The similarity in SiC is attributed to SiC/SiO2 interfacial reactions producing the necessary conditions for passive scale formation (active-to-passive) or passive scale breakdown (passive-to-active). Comparable results were obtained in both the O-2/Ar and reduced total O-2 pressure cases for SiC.
C1 [Jacobson, N. S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Myers, D. L.] E Cent Univ, Ada, OK 74820 USA.
RP Jacobson, NS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM nathan.s.jacobson@nasa.gov
NR 29
TC 45
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U1 7
U2 23
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0030-770X
J9 OXID MET
JI Oxid. Met.
PD FEB
PY 2011
VL 75
IS 1-2
BP 1
EP 25
DI 10.1007/s11085-010-9216-4
PG 25
WC Metallurgy & Metallurgical Engineering
SC Metallurgy & Metallurgical Engineering
GA 716QW
UT WOS:000286989600001
ER
PT J
AU Atreya, SK
Witasse, O
Chevrier, VF
Forget, F
Mahaffy, PR
Price, PB
Webster, CR
Zurek, RW
AF Atreya, Sushil K.
Witasse, Olivier
Chevrier, Vincent F.
Forget, Francois
Mahaffy, Paul R.
Price, P. Buford
Webster, Christopher R.
Zurek, Richard W.
TI Methane on Mars: Current observations, interpretation, and future plans
Preface
SO PLANETARY AND SPACE SCIENCE
LA English
DT Editorial Material
C1 [Atreya, Sushil K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Witasse, Olivier] ESTEC ESA, Noordwijk, Netherlands.
[Chevrier, Vincent F.] Univ Arkansas, WM Keck Lab Space & Planetary Simulat, Fayetteville, AR 72701 USA.
[Forget, Francois] Univ Paris 06, Meteorol Dynam Lab, Jussieu, France.
[Mahaffy, Paul R.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Price, P. Buford] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Webster, Christopher R.; Zurek, Richard W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Atreya, SK (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM atreya@umich.edu
RI Mahaffy, Paul/E-4609-2012
NR 0
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U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD FEB
PY 2011
VL 59
IS 2-3
SI SI
BP 133
EP 136
DI 10.1016/j.pss.2010.10.008
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 724AP
UT WOS:000287548800001
ER
PT J
AU Novak, RE
Mumma, MJ
Villanueva, GL
AF Novak, R. E.
Mumma, M. J.
Villanueva, G. L.
TI Measurement of the isotopic signatures of water on Mars; Implications
for studying methane
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Atmosphere; Infrared; Spectroscopy; Isotopologue; Water; Methane
ID MARTIAN ATMOSPHERE; MU-M; CH4; SPECTROMETER; SPECTROGRAPH; GASES; LIFE;
HDO
AB The recent discovery of methane on Mars has led to much discussion concerning its origin. On Earth, the isotopic signatures of methane vary with the nature of its production. Specifically, the ratios among (CH4)-C-12, (CH4)-C-13, and (CH3D)-C-12 differ for biotic and abiotic origins. On Mars, measuring these ratios would provide insights into the origins of methane and measurements of water isotopologues co-released with methane would assist in testing their chemical relationship. Since 1997, we have been measuring HDO and H2O in Mars' atmosphere and comparing their ratio to that in Earth's oceans. We recently incorporated a line-by-line radiative transfer model (LBLRTM) into our analysis. Here, we present a map for [HDO]/[H2O] along the central meridian (154 degrees W) for L-s=50 degrees. From these results, we constructed models to determine the observational conditions needed to quantify the isotopic ratios of methane in Mars' atmosphere. Current ground-based instruments lack the spectral resolution and sensitivity needed to make these measurements. Measurements of the isotopologues of methane will likely require in situ sampling. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Novak, R. E.] Iona Coll, Dept Phys, New Rochelle, NY 10801 USA.
[Mumma, M. J.; Villanueva, G. L.] NASAs, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Villanueva, G. L.] Catholic Univ Amer, Dept Phys, Washington, DC 20008 USA.
RP Novak, RE (reprint author), Iona Coll, Dept Phys, New Rochelle, NY 10801 USA.
EM rnovak@iona.edu; michael.j.mumma@nasa.gov; geronimo.villanueva@nasa.gov
RI mumma, michael/I-2764-2013
FU NSF [AST-0805540]; NASA [344-32-51-96, 344-53-51]; National Aeronautics
and Space Administration, Science Mission Directorate [NNX-08AE38A]
FX REN was supported by NSF RUI Grant AST-0805540. MJM and GLV were
supported by Grants from NASA's Planetary Astronomy Program
(344-32-51-96) and Astrobiology Program (344-53-51). We acknowledge the
Director and Staff of the NASA Infrared Telescope Facility for granting
us the observing time. The NASA-IRTF is operated by the University of
Hawaii under Cooperative Agreement NNX-08AE38A with the National
Aeronautics and Space Administration, Science Mission Directorate,
Planetary Astronomy Program.
NR 30
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD FEB
PY 2011
VL 59
IS 2-3
SI SI
BP 163
EP 168
DI 10.1016/j.pss.2010.06.017
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 724AP
UT WOS:000287548800004
ER
PT J
AU Mischna, MA
Allen, M
Richardson, MI
Newman, CE
Toigo, AD
AF Mischna, Michael A.
Allen, Mark
Richardson, Mark I.
Newman, Claire E.
Toigo, Anthony D.
TI Atmospheric modeling of Mars methane surface releases
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars atmosphere; Methane; Plumes; MarsWRF; General circulation model
ID THERMAL EMISSION SPECTROMETER; GENERAL-CIRCULATION MODELS; MARTIAN
ATMOSPHERE
AB We utilize the MarsWRF general circulation model (GCM) to address the behavior of gas plumes in the Martian atmosphere, with the specific goal of characterizing the source of the recently identified methane detection in the Martian atmosphere. These observations have been interpreted as the release of methane from localized surface sources with spatial and temporal variabilities. Due to the limited temporal coverage of ground-based observations, we use a GCM to simulate the development of passive atmospheric plumes over relevant timescales. The observations can be reproduced best if the release occurred just before the time of observation-no more than 1-2 sols earlier-and if this release were nearly instantaneous rather than a slow, steady emission. Furthermore, it requires a source region spanning a broad latitudinal range rather than a point emission. While the accuracy of our conclusions about this specific methane release scenario is limited by the uncertainties inherent in GCM simulations of the Martian atmosphere, our findings regarding generalized plume behavior are robust, and illustrate the potential power of numerical modeling for constraining plume source conditions. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Mischna, Michael A.; Allen, Mark] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Allen, Mark; Richardson, Mark I.; Newman, Claire E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Toigo, Anthony D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Mischna, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 183-401, Pasadena, CA 91109 USA.
EM michael.a.mischna@jpl.nasa.gov; mark.a.allen@jpl.nasa.gov;
mir@ashimagroup.net; claire@ashimagroup.net; toigo@astro.cornell.edu
FU National Aeronautics and Space Administration
FX The simulations presented in this paper were performed on the
supercomputing clusters at both JPL and the Caltech Division of
Geological and Planetary Sciences. Work by M. Mischna and M. Allen was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. We wish to acknowledge stimulating discussions with Mike
Mumma, Kevin Zahnle and Francois Forget on earlier versions of this
research. Two anonymous reviewers helped to clarify the story and
provided excellent feedback.
NR 16
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD FEB
PY 2011
VL 59
IS 2-3
SI SI
BP 227
EP 237
DI 10.1016/j.pss.2010.07.005
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 724AP
UT WOS:000287548800011
ER
PT J
AU Gough, RV
Turley, JJ
Ferrell, GR
Cordova, KE
Wood, SE
DeHaan, DO
Mckay, CP
Toon, OB
Tolbert, MA
AF Gough, R. V.
Turley, J. J.
Ferrell, G. R.
Cordova, K. E.
Wood, S. E.
DeHaan, D. O.
McKay, C. P.
Toon, O. B.
Tolbert, M. A.
TI Can rapid loss and high variability of Martian methane be explained by
surface H2O2?
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Atmosphere; Surface; Oxidant; Methane; Viking
ID LIFE DETECTION EXPERIMENT; RICH MONTMORILLONITE; ATMOSPHERIC METHANE;
OXIDANT ENHANCEMENT; DUST DEVILS; MARS; SOIL; HABITABILITY; OXIDATION;
PEROXIDE
AB It has been reported by several groups that methane in the Martian atmosphere is both spatially and temporally variable. Gough et al. (2010) suggested that temperature dependent, reversible physical adsorption of methane onto Martian soils could explain this variability. However, it is also useful to consider if there might be chemical destruction of methane (and compensating sources) operating on seasonal time scales. The lifetime of Martian methane due to known chemical loss processes is long (on the order of hundreds of years). However, observations constrain the lifetime to be 4 years or less, and general circulation models suggest methane destruction must occur even faster (< 1 year) to cause the reported variability and rapid disappearance. The Martian surface is known to be highly oxidizing based on the Viking Labeled Release experiments in which organic compounds were quickly oxidized by samples of the regolith. Here we test if simulated Martian soil is also oxidizing towards methane to determine if this is a relevant loss pathway for Martian methane. We find that although two of the analog surfaces studied, TiO2. H2O2 and JSC-Mars-1 with H2O2, were able to oxidize the complex organic compounds (sugars and amino acids) used in the Viking Labeled Release experiments, these analogs were unable to oxidize methane to carbon dioxide within a 72 h experiment. Sodium and magnesium perchlorate, salts that were recently discovered at the Phoenix landing site and are potential strong oxidants, were not observed to directly oxidize either the organic solution or methane. The upper limit reaction coefficient, a, was found to be < 4 x 10(-17) for methane loss on TiO2 center dot H2O2 and < 2 x 10(-17) for methane loss on JSC-Mars-1 with H2O2. Unless the depth of soil on Mars that contains H2O2 is very deep (thicker than 500 m), the lifetime of methane with respect to heterogeneous oxidation by H2O2 is probably greater than 4 years. Therefore, reaction of methane with H2O2 on Martian soils does not appear to be a significant methane sink, and would not destroy methane rapidly enough to cause the reported atmospheric methane variability. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Gough, R. V.; Turley, J. J.; Ferrell, G. R.; Cordova, K. E.; Wood, S. E.; DeHaan, D. O.; Tolbert, M. A.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Gough, R. V.; Turley, J. J.; Ferrell, G. R.; Cordova, K. E.; Wood, S. E.; DeHaan, D. O.; Tolbert, M. A.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[McKay, C. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Toon, O. B.] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Toon, O. B.] Univ Colorado, Dept Atmospher & Ocean Sci ATOC, Boulder, CO 80309 USA.
[Gough, R. V.; Turley, J. J.; Ferrell, G. R.; Cordova, K. E.; Wood, S. E.; DeHaan, D. O.; Tolbert, M. A.] Univ San Diego, Dept Chem & Biochem, San Diego, CA 92110 USA.
RP Gough, RV (reprint author), Univ Colorado, Dept Chem & Biochem, 216 UCB, Boulder, CO 80309 USA.
EM raina.gough@colorado.edu
RI Gough, Raina/F-7574-2013; Cordova, Kyle/I-2556-2014
OI Cordova, Kyle/0000-0002-4988-0497
FU NASA Mars Fundamental Research [NNX09AN19G]
FX This work was supported by NASA Mars Fundamental Research Grant
NNX09AN19G. The authors would like to thank Paul Rice of the
Nanomaterials Characterization Facility at the University of Colorado
for help with the SEM, Tom McCollom for use of his GC and other
equipment, Lisa Mahew for her help with the GC, and Miriam Freedman for
helpful comments.
NR 56
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U2 10
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 FEB
PY 2011
VL 59
IS 2-3
SI SI
BP 238
EP 246
DI 10.1016/j.pss.2010.09.018
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 724AP
UT WOS:000287548800012
ER
PT J
AU Webster, CR
Mahaffy, PR
AF Webster, Christopher R.
Mahaffy, Paul R.
TI Determining the local abundance of Martian methane and its' C-13/C-12
and D/H isotopic ratios for comparison with related gas and soil
analysis on the 2011 Mars Science Laboratory (MSL) mission
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Methane; Isotopes; Atmosphere; Laser; Spectroscopy
ID ATMOSPHERIC METHANE; LASER SPECTROSCOPY; IR SPECTROMETER; LIFE; CARBON;
CH4
AB Understanding the origin of Martian methane will require numerous complementary measurements from both in situ and remote sensing investigations and laboratory work to correlate planetary surface geophysics with atmospheric dynamics and chemistry. Three instruments (Quadrupole Mass Spectrometer (QMS), Gas Chromatograph (GC) and Tunable Laser Spectrometer (TLS)) with sophisticated sample handling and processing capability make up the Sample Analysis at Mars (SAM) analytical chemistry suite on NASA's 2011 Mars Science Laboratory (MSL) Mission. Leveraging off the SAM sample and gas processing capability that includes methane enrichment, TLS has unprecedented sensitivity for measuring absolute methane (parts-per-trillion), water, and carbon dioxide abundances in both the Martian atmosphere and evolved from heated soil samples. In concert with a wide variety of associated trace gases (e.g. SO2, H2S, NH3, higher hydrocarbons, organics, etc.) and other isotope ratios measured by SAM, TLS will focus on determining the absolute abundances of methane, water and carbon dioxide, and their isotope ratios: C-13/C-12 and D/H in methane; C-13/C-12 and O-18/O-17/O-16 in carbon dioxide; and O-18/O-17/O-16 and D/H in water. Measurements near the MSL landing site will be correlated with satellite (Mars Express, Mars 2016) and ground-based observations. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Webster, Christopher R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mahaffy, Paul R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Webster, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Chris.R.Webster@jpl.nasa.gov
RI Mahaffy, Paul/E-4609-2012
FU National Aeronautics and Space Administration (NASA); Goddard Space
Flight Center (GSFC)
FX This research was carried out by the Jet Propulsion Laboratory (JPL),
California Institute of Technology, under contract with the National
Aeronautics and Space Administration (NASA), and by the Goddard Space
Flight Center (GSFC) with support from the Mars Program. The SAM suite
is the responsibility of GSFC (Paul Mahaffy, suite PI), with the GC
provided by CNES, France (Michel Cabane, GC lead) and the TLS provided
by JPL (Chris Webster, TLS lead). The authors acknowledge the huge team
effort from both SAM and TLS teams. (C) 2010, California Institute of
Technology.
NR 38
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD FEB
PY 2011
VL 59
IS 2-3
SI SI
BP 271
EP 283
DI 10.1016/j.pss.2010.08.021
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 724AP
UT WOS:000287548800016
ER
PT J
AU Zurek, RW
Chicarro, A
Allen, MA
Bertaux, JL
Clancy, RT
Daerden, F
Formisano, V
Garvin, JB
Neukum, G
Smith, MD
AF Zurek, Richard W.
Chicarro, Augustin
Allen, Mark A.
Bertaux, Jean-Loup
Clancy, R. Todd
Daerden, Frank
Formisano, Vittorio
Garvin, James B.
Neukum, Gerhard
Smith, Michael D.
TI Assessment of a 2016 mission concept: The search for trace gases in the
atmosphere of Mars
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Atmosphere; Trace gases; Methane; Orbiter
ID METHANE; LIFE
AB The reported detection of methane in the atmosphere of Mars as well as its potentially large seasonal spatial variations challenge our understanding of both the sources and sinks of atmospheric trace gases. The presence of methane suggests ongoing exchange between the subsurface and the atmosphere of potentially biogenic trace gases, while the spatial and temporal variations cannot be accounted for with current knowledge of martian photochemistry. A Joint Instrument Definition Team (JIDT) was asked to assess concepts for a mission that might follow up on these discoveries within the framework of a series of joint missions being considered by ESA and NASA for possible future exploration of Mars. The following is based on the report of the JIDT to the space agencies (Zurek et al., 2009); a synopsis of the report was presented at the Workshop on Mars Methane held in Frascati, Italy, in November 2009. To summarize, the JIDT believed that a scientifically exciting and credible mission could be conducted within the evolving capabilities of the science/telecommunications orbiter being considered by ESA and NASA for possible launch in the 2016 opportunity for Mars. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Zurek, Richard W.; Allen, Mark A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chicarro, Augustin] European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands.
[Bertaux, Jean-Loup] CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France.
[Clancy, R. Todd] Space Sci Inst, Boulder, CO 80301 USA.
[Daerden, Frank] Belgian Inst Space Aeron, B-1180 Brussels, Belgium.
[Formisano, Vittorio] IFSI Roma, Rome, Italy.
[Garvin, James B.; Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Neukum, Gerhard] Free Univ Berlin, D-12249 Berlin, Germany.
RP Zurek, RW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Richard.W.Zurek@jpl.nasa.gov
RI Smith, Michael/C-8875-2012;
OI Daerden, Frank/0000-0001-7433-1839
FU ESA; NASA Headquarters; National Aeronautics and Space Administration
FX The JIDT activity described in this report was supported by ESA and NASA
Headquarters and the ESA ExoMars Project. The Mars Program Office at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration, also
supported the JIDT activity, including the preparation of the final
report and this paper.
NR 10
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD FEB
PY 2011
VL 59
IS 2-3
SI SI
BP 284
EP 291
DI 10.1016/j.pss.2010.07.007
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 724AP
UT WOS:000287548800017
ER
PT J
AU Vance, S
Christensen, LE
Webster, CR
Sung, K
AF Vance, Steve
Christensen, Lance E.
Webster, Christopher R.
Sung, Keeyoon
TI Volatile organic sulfur compounds as biomarkers complementary to
methane: Infrared absorption spectroscopy of CH3SH enables in situ
measurements on Earth and Mars
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Astrobiology; Mars; Methane; Laser absorption spectroscopy; Mars Science
Laboratory; Methyl mercaptan
ID TRANSITION-METAL SULFIDES; LASER SPECTROSCOPY; CARBON FIXATION; LIFE;
ATMOSPHERE; METABOLISM; DEPOSITS
AB As universal products of biological processes, volatile organic sulfur compounds such as methyl mercaptan (CH3SH) may be essential in the search for signs of life on Mars and in exoplanet atmospheres. Methyl mercaptan is implicated in the origin of life at sites of low-temperature hydrothermal activity driven by serpentinization. Serpentinization may occur on Mars, in icy satellite oceans, and in other small wet bodies to a greater extent than on Earth, with important implications for life. We characterized absorption features in pure laboratory sample spectra of CH3SH using the Carbon Isotope Laser Spectrometer (CILS), an infrared (3.27 mu m) tunable diode laser spectrometer with capabilities nearly identical to those of the Tunable Laser Spectrometer (TLS) instrument on the Mars Science Laboratory. The molecular species proves detectable by CILS and TLS at the sensitivities approaching the level of parts per trillion with pre-concentration. These measurements demonstrate the possibility for detection of methyl mercaptan, with implications for its possible use as an in situ biosignature for Earth-based and extraterrestrial exploration. Published by Elsevier Ltd.
C1 [Vance, Steve; Christensen, Lance E.; Webster, Christopher R.; Sung, Keeyoon] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Vance, S (reprint author), CALTECH, Jet Prop Lab, MS 183-401,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Steven.D.Vance@jpl.nasa.gov
RI Sung, Keeyoon/I-6533-2015
FU MSL; Icy Worlds node of NASA's Astrobiology Institute [08-NAI5-0021];
NASA; Caltech; National Aeronautics and Space Administration
FX Linda Brown assisted with the FTIR measurements. Discussions with
Michael Russell provided invaluable direction for this project. The
authors wish to acknowledge support from MSL, the Icy Worlds node of
NASA's Astrobiology Institute (08-NAI5-0021) and the NASA and Caltech
postdoctoral programs. 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. Copyright 2010 California Institute of Technology.
Government sponsorship acknowledged. None of these funding sources
participated directly in the design of this study; in the collection,
analysis and interpretation of data; in the writing of the report; or in
the decision to submit the paper for publication.
NR 30
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD FEB
PY 2011
VL 59
IS 2-3
SI SI
BP 299
EP 303
DI 10.1016/j.pss.2010.08.023
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 724AP
UT WOS:000287548800019
ER
PT J
AU Kraemer, SB
Schmitt, HR
Crenshaw, DM
Melendez, M
Turner, TJ
Guainazzi, M
Mushotzky, RF
AF Kraemer, S. B.
Schmitt, H. R.
Crenshaw, D. M.
Melendez, M.
Turner, T. J.
Guainazzi, M.
Mushotzky, R. F.
TI MULTI-WAVELENGTH PROBES OF OBSCURATION TOWARD THE NARROW-LINE REGION IN
SEYFERT GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: Seyfert
ID ACTIVE GALACTIC NUCLEI; HIGH-RESOLUTION SPECTROSCOPY; INFRARED-SELECTED
SAMPLE; SPACE-TELESCOPE SURVEY; X-RAY-EMISSION; PHYSICAL CONDITIONS;
NEARBY GALAXIES; SPITZER-IRS; MU-M; CIRCUMNUCLEAR DUST
AB We present a study of reddening and absorption toward the narrow line regions (NLRs) in active galactic nuclei (AGNs) selected from the Revised Shapley-Ames, 12 mu m, and Swift/Burst Alert Telescope samples. For the sources in host galaxies with inclinations of b/a > 0.5, we find that the mean ratio of [O III] lambda 5007, from ground-based observations, and [O IV] 28.59 mu m, from Spitzer/Infrared Spectrograph observations, is a factor of two lower in Seyfert 2s than Seyfert 1s. The combination of low [O III]/[O IV] and [O III] lambda 4363/lambda 5007 ratios in Seyfert 2s suggests more extinction of emission from the NLR than in Seyfert 1s. Similar column densities of dusty gas, N-H similar to several x 10(21) cm(-2), can account for the suppression of both [O III] lambda 5007 and [O III] lambda 4363, as compared to those observed in Seyfert 1s. Also, we find that the X-ray line O VII lambda 22.1 angstrom is weaker in Seyfert 2s, consistent with absorption by the same gas that reddens the optical emission. Using a Hubble Space Telescope/Space Telescope Imaging Spectrograph slitless spectrum of the Seyfert 1 galaxy NGC 4151, we estimate that only similar to 30% of the [O III] lambda 5007 comes from within 30 pc of the central source, which is insufficient to account for the low [O III]/[O IV] ratios in Seyfert 2s. If Seyfert 2 galaxies have similar intrinsic [O III] spatial profiles, the external dusty gas must extend further out along the NLR, perhaps in the form of nuclear dust spirals that have been associated with fueling flows toward the AGN.
C1 [Kraemer, S. B.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Kraemer, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Schmitt, H. R.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
[Schmitt, H. R.] Computat Phys Inc, Springfield, VA 22151 USA.
[Crenshaw, D. M.] Georgia State Univ, Astron Off, Dept Phys & Astron, Atlanta, GA 30303 USA.
[Melendez, M.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Guainazzi, M.] European Space Agcy, European Space Astron Ctr, E-28691 Madrid, Spain.
[Mushotzky, R. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Kraemer, SB (reprint author), Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
FU NRL; National Aeronautics and Space Administration
FX Basic research in Astronomy at the NRL is supported by 6.1 base funding.
This research has made use of the NASA/IPAC Extragalactic Database (NED)
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration. We thank Juliette Buet for her assistance with this
project. We thank an anonymous referee for valuable suggestions.
NR 114
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 130
DI 10.1088/0004-637X/727/2/130
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000069
ER
PT J
AU McCabe, C
Duchene, G
Pinte, C
Stapelfeldt, KR
Ghez, AM
Menard, F
AF McCabe, C.
Duchene, G.
Pinte, C.
Stapelfeldt, K. R.
Ghez, A. M.
Menard, F.
TI SPATIALLY RESOLVING THE HK Tau B EDGE-ON DISK FROM 1.2 TO 4.7 mu m: A
UNIQUE SCATTERED LIGHT DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; protoplanetary disks; stars: individual (HK Tau);
stars: pre-main sequence
ID STAR-FORMING REGIONS; SPITZER-IRS SPECTRA; T-TAURI; CIRCUMSTELLAR DISK;
PROTOPLANETARY DISKS; GRAIN-GROWTH; INTERSTELLAR EXTINCTION; INFRARED
EXTINCTION; RADIATIVE-TRANSFER; CIRCUMBINARY RING
AB We present spatially resolved scattered light images of the circumstellar disk around HK Tau B at 3.8 and 4.7 mu m taken with the Keck Telescope Laser Guide Star Adaptive Optics (AO) system, and 1.6-2.12 mu m images taken with the Very Large Telescope/NACO AO system. Combined with previously published optical Hubble Space Telescope data, we investigate the spatially resolved scattered light properties of this edge-on circumstellar disk and probe for the presence of large grains. The 0.6-3.8 mu m scattered light observations reveal strong, and in some cases, unusual, wavelength dependencies in the observed disk morphology. The separation between the two scattered light nebulae, which is directly proportional to the disk-mass-opacity product, decreases by 30% between 0.6 and 3.8 mu m. Over the same wavelength range, the FWHM of the disk nebulosity declines by a factor of two, while the flux ratio between the two nebulae increases by a factor of similar to 8. No other disk known to date shows a flux ratio that increases with wavelength. Both the FWHM and nebula flux ratio are affected by the scattering phase function and the observed behavior can most readily be explained by a phase function that becomes more forward throwing with wavelength. The multi-wavelength scattered light observations also confirm the asymmetric nature of the disk and show that the level of asymmetry is a function of wavelength. We use the MCFOST radiative transfer code to model the disk at four wavelengths, corresponding to the I, H, Ks, and L' bandpasses. A single power-law grain size distribution can recreate the observed disk properties simultaneously at all four wavelengths. Bayesian analysis of the dust parameters finds a 99% probability that the maximum grain size is 5.5 mu m or larger. We also find that the grain size distribution is steep, with a 99% probability of a power-law index of 4.2 or larger, suggesting that these large grains are a small fraction of the overall dust population. The best-fit dust asymmetry parameter for each individual wavelength shows an unusual behavior, increasing with wavelength from the optical through the near-infrared, peaking at similar to 0.8 between 2.2 and 3.8 mu m, then decreasing by a factor of two by similar to 12 mu m. Comparing the wavelength dependence of the asymmetry parameter for HK Tau B with those for the interstellar medium (ISM) and dark cloud dust models, we find considerable evolution from an ISM state and argue for the presence of grain growth within the disk. Further, comparing the wavelength dependence of the asymmetry parameter for GG Tau, HV Tau C, and HK Tau B, the three disks that have been spatially resolved in scattered light between 0.8 and 3.8 mu m, finds a diverse range of dust properties, indicating differing degrees of grain growth for disks at a similar age.
C1 [McCabe, C.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Duchene, G.; Pinte, C.; Menard, F.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, F-38041 Grenoble 9, France.
[Duchene, G.] Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA.
[Pinte, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Stapelfeldt, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
[Ghez, A. M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP McCabe, C (reprint author), Eureka Sci Inc, 2452 Delmer St,Suite 100, Oakland, CA 94602 USA.
EM mccabe@ipac.caltech.edu; Gaspard.Duchene@obs.ujf-grenoble.fr;
Christophe.Pinte@obs.ujf-grenoble.fr; ghez@astro.ucla.edu;
Francois.Menard@obs.ujf-grenoble.fr
RI Stapelfeldt, Karl/D-2721-2012
FU W. M. Keck Foundation; Center for Adaptive Optics; NSF [AST 04-06816];
NSF Science and Technology Center for Adaptive Optics [AST 98-76783];
Agence Nationale de la Recherche [ANR-07-BLAN-0221]; European Commission
[PIEF-GA-2008-220891]
FX We thank the anonymous referee for the thoughtful and constructive
comments on this paper. We also thank the Keck AO team for providing the
K' image of HK Tau taken during engineering time and Elise Furlan for
providing the IRS spectrum of HK Tau. The GEODE team of edge-on disk
modelers have provided many enjoyable discussions on the finer points of
disk modeling and we thank them for reading this manuscript. 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. The
authors recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. This work has
used the http://circumstellardisks.org Web site. This work was supported
by the Center for Adaptive Optics. Support for this work was provided by
NSF grant AST 04-06816 and the NSF Science and Technology Center for
Adaptive Optics, managed by the University of California, Santa Cruz
(AST 98-76783). This work has also been funded in part by the Agence
Nationale de la Recherche through contract ANR-07-BLAN-0221. C. P.
acknowledges funding from the European Commission's Seventh Framework
Program as a Marie Curie Intra-European Fellow (PIEF-GA-2008-220891).
NR 77
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 90
DI 10.1088/0004-637X/727/2/90
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000029
ER
PT J
AU Ricca, A
Bauschlicher, CW
Allamandola, LJ
AF Ricca, Alessandra
Bauschlicher, Charles W., Jr.
Allamandola, Louis J.
TI PROTONATED POLYCYCLIC AROMATIC HYDROCARBONS REVISITED
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; infrared: ISM; ISM: lines and bands; ISM: molecules;
line: identification; methods: numerical; molecular data
ID INFRARED-SPECTRA; EMISSION; PAHS; FREQUENCIES; MOLECULES; EXCHANGE;
POSITION; FEATURES; TRACER; BANDS
AB We reconsider the contribution that singly protonated polycyclic aromatic hydrocarbons (PAHs; HPAH(+)s) might make to the Class A component of the 6.2 mu m interstellar emission feature in light of the recent experimental measurements of protonated naphthalene and coronene. Our calculations on the small HPAH(+)s have a band near 6.2 mu m, as found in experiment. While the larger HPAH(+)s still have emission near 6.2 mu m, the much larger intensity of the band near 6.3 mu m overwhelms the weaker band at 6.2 mu m, so that the 6.2 mu m band is barely visible. Since the large PAHs are more representative of those in the interstellar medium, our work suggests that large HPAH(+)s cannot be major contributors to the observed emission at 6.2 mu m (i.e., Class A species). Saturating large PAH cations with hydrogen atoms retains the 6.2 mu m Class A band position, but the rest of the spectrum is inconsistent with observed spectra.
C1 [Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Entry Syst & Technol Div, Moffett Field, CA 94035 USA.
[Allamandola, Louis J.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Ricca, A (reprint author), SETI Inst, Carl Sagan Ctr, 189 N Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
EM Alessandra.Ricca-1@nasa.gov; Charles.W.Bauschlicher@nasa.gov
FU NASA [NNX09AD18G]; NASA's Astrobiology and Laboratory Astrophysics
Programs
FX A.R. thanks NASA's Astrophysics Theory and Fundamental Physics (ATFP)
(NNX09AD18G) program for its generous support of this work. L.J.A.
gratefully acknowledges support from NASA's Astrobiology and Laboratory
Astrophysics Programs.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 128
DI 10.1088/0004-637X/727/2/128
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000067
ER
PT J
AU Wik, DR
Sarazin, CL
Finoguenov, A
Baumgartner, WH
Mushotzky, RF
Okajima, T
Tueller, J
Clarke, TE
AF Wik, Daniel R.
Sarazin, Craig L.
Finoguenov, Alexis
Baumgartner, Wayne H.
Mushotzky, Richard F.
Okajima, Takashi
Tueller, Jack
Clarke, Tracy E.
TI THE LACK OF DIFFUSE, NON-THERMAL HARD X-RAY EMISSION IN THE COMA
CLUSTER: THE SWIFT BURST ALERT TELESCOPE'S EYE VIEW
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (Coma);
intergalactic medium; magnetic fields; radiation mechanisms:
non-thermal; X-rays: galaxies: clusters
ID OPHIUCHUS GALAXY CLUSTER; MAGNETIC-FIELD; XMM-NEWTON; COSMOLOGICAL
SIMULATIONS; SPATIAL-DISTRIBUTION; INTEGRAL IBIS/ISGRI;
FARADAY-ROTATION; CRAB-NEBULA; ENERGY; SPECTRUM
AB The Coma Cluster of galaxies hosts the brightest radio halo known and has therefore been the target of numerous searches for associated inverse Compton (IC) emission, particularly at hard X-ray energies where the IC signal must eventually dominate over thermal emission. The most recent search with the Suzaku Hard X-ray Detector failed to confirm previous IC detections with RXTE and BeppoSAX, instead setting an upper limit 2.5 times below their non-thermal flux. However, this discrepancy can be resolved if the IC emission is very extended, beyond the scale of the cluster radio halo. Using reconstructed sky images from the 58-month Swift Burst Alert Telescope (BAT) all-sky survey, the feasibility of such a solution is investigated. Building on Renaud et al., we test and implement a method for extracting the fluxes of extended sources, assuming specified spatial distributions. BAT spectra are jointly fit with an XMM-Newton EPIC-pn spectrum derived from mosaic observations. We find no evidence for large-scale IC emission at the level expected from the previously detected non-thermal fluxes. For all non-thermal spatial distributions considered, which span the gamut of physically reasonable IC models, we determine upper limits for which the largest (most conservative) limit is less than or similar to 4.2x10(-12) erg s(-1) cm(-2) (20-80 keV), which corresponds to a lower limit on the magnetic field B > 0.2 mu G. A nominal flux upper limit of <2.7x10(-12) erg s(-1) cm(-2), with corresponding B > 0.25 mu G, is derived for the most probable IC distribution given the size of the radio halo and likely magnetic field radial profile.
C1 [Wik, Daniel R.; Baumgartner, Wayne H.; Okajima, Takashi; Tueller, Jack] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
[Sarazin, Craig L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Finoguenov, Alexis] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Finoguenov, Alexis] Univ Maryland, Baltimore, MD 21250 USA.
[Mushotzky, Richard F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Clarke, Tracy E.] USN, Res Lab, Washington, DC 20375 USA.
RP Wik, DR (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.
EM daniel.r.wik@nasa.gov
RI Tueller, Jack/D-5334-2012; XRAY, SUZAKU/A-1808-2009
FU University of Virginia; NASA [NNX08AZ99G, NNX09AH25G, NNX09AH74G,
NNX08AZ34G, NNX08AW83G]; Basic research in radio astronomy at the NRL
FX We thank W. Reich who kindly provided us with the Deiss et al. (1997)
radio image, C. B. Markwardt who explained to us (and wrote) many of the
BAT software analysis routines used in this work, D. Kushnir and E.
Waxman for helpful comments and pointing out a small error, and the
referee D. Eckert for helpful comments that particularly improved the
clarity of the paper. D. R. W. was supported by a University of Virginia
GSAS Dissertation Year Fellowship and a Virginia Space Grant Consortium
Fellowship. D. R. W. and C. L. S. were supported in part by NASA through
Suzaku grants NNX08AZ99G, NNX09AH25G, and NNX09AH74G, and XMM-Newton
grants NNX08AZ34G and NNX08AW83G. Basic research in radio astronomy at
the NRL is supported by 6.1 Base funding.
NR 52
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 119
DI 10.1088/0004-637X/727/2/119
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000058
ER
PT J
AU Acikmese, B
Blackmore, L
AF Acikmese, Behcet
Blackmore, Lars
TI Lossless convexification of a class of optimal control problems with
non-convex control constraints
SO AUTOMATICA
LA English
DT Article
DE Optimal control theory; Control of constrained systems; Guidance,
navigation and control of vehicles; Convex optimization
ID POWERED-DESCENT GUIDANCE; MODEL-PREDICTIVE CONTROL; TRAJECTORY
OPTIMIZATION; STATE
AB We consider a class of finite time horizon optimal control problems for continuous time linear systems with a convex cost, convex state constraints and non-convex control constraints. We propose a convex relaxation of the non-convex control constraints, and prove that the optimal solution of the relaxed problem is also an optimal solution for the original problem, which is referred to as the lossless convexification of the optimal control problem. The lossless convexification enables the use of interior point methods of convex optimization to obtain globally optimal solutions of the original non-convex optimal control problem. The solution approach is demonstrated on a number of planetary soft landing optimal control problems. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Acikmese, Behcet; Blackmore, Lars] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Acikmese, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM behcet@jpl.nasa.gov; lars@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The authors gratefully acknowledge Mark H. Milman and Daniel P. Scharf
of Jet Propulsion Laboratory for their valuable comments. This research
was performed at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 26
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0005-1098
J9 AUTOMATICA
JI Automatica
PD FEB
PY 2011
VL 47
IS 2
BP 341
EP 347
DI 10.1016/j.automatica.2010.10.037
PG 7
WC Automation & Control Systems; Engineering, Electrical & Electronic
SC Automation & Control Systems; Engineering
GA 720EV
UT WOS:000287264100010
ER
PT J
AU Braman, JMB
Murray, RM
AF Braman, Julia M. B.
Murray, Richard M.
TI Bisimulation conversion and verification procedure for goal-based
control systems
SO FORMAL METHODS IN SYSTEM DESIGN
LA English
DT Article
DE Verification; Hybrid systems; Model checking; Fault-tolerant control
ID FAULT-TOLERANCE; MODEL CHECKING; ROBOTS
AB Fault tolerance and safety verification of control systems are essential for the success of autonomous robotic systems. A control architecture called Mission Data System (MDS), developed at the Jet Propulsion Laboratory, addresses these needs with a goal-based control approach. In this paper, a software algorithm for converting goal network control systems into linear hybrid systems is described. The conversion process is a bisimulation; the resulting linear hybrid system can be verified for safety in the presence of failures using existing symbolic model checkers, and thus the original goal network is verified. A moderately complex example goal network control system is converted to a linear hybrid system using the automatic conversion software that is based on the bisimulation and then is verified.
C1 [Braman, Julia M. B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Murray, Richard M.] CALTECH, Pasadena, CA 91125 USA.
RP Braman, JMB (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM julia.m.braman@nasa.gov
OI Murray, Richard/0000-0002-5785-7481
FU Air Force Office of Scientific Research (AFOSR); Boeing Company
FX The authors would like to gratefully acknowledge Kenneth Meyer, Michel
Ingham, David Wagner, Robert Rasmussen, Kirk Reinholtz, and the rest of
the MDS team at JPL for feedback, suggestions, answered questions, and
MDS and State Analysis instruction. This work was funded in part by the
Air Force Office of Scientific Research (AFOSR) and The Boeing Company.
NR 42
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U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0925-9856
EI 1572-8102
J9 FORM METHOD SYST DES
JI Form. Methods Syst. Des.
PD FEB
PY 2011
VL 38
IS 1
BP 62
EP 95
DI 10.1007/s10703-010-0109-6
PG 34
WC Computer Science, Theory & Methods
SC Computer Science
GA 716QS
UT WOS:000286989200003
ER
PT J
AU Marinova, MM
Aharonson, O
Asphaug, E
AF Marinova, Margarita M.
Aharonson, Oded
Asphaug, Erik
TI Geophysical consequences of planetary-scale impacts into a Mars-like
planet
SO ICARUS
LA English
DT Article
DE Impact processes; Cratering; Mars; Accretion
ID MARTIAN HEMISPHERIC DICHOTOMY; INNER SOLAR-SYSTEM; TERRESTRIAL PLANETS;
OBLIQUE IMPACTS; MAGMA OCEAN; CRUSTAL DICHOTOMY; CRATER DIMENSIONS;
GIANT IMPACTS; ORIGIN; MOON
AB All planetary bodies with old surfaces exhibit planetary-scale impact craters: vast scars caused by the large impacts at the end of Solar System accretion or the late heavy bombardment. Here we investigate the geophysical consequences of planetary-scale impacts into a Mars-like planet, by simulating the events using a smoothed particle hydrodynamics (SPH) model. Our simulations probe impact energies over two orders of magnitude (2 x 10(22)-6 x 10(29) J), impact velocities from the planet's escape velocity to twice Mars' orbital velocity (6-50 km/s), and impact angles from head-on to highly oblique (0-75 degrees). The simulation results confirm that for planetary-scale impacts, surface curvature, radial gravity, the large relative size of the impactor to the planet, and the greater penetration of the impactor, contribute to significant differences in the geophysical expression compared to small craters, which can effectively be treated as acting in a half-space. The results show that the excavated crustal cavity size and the total melt production scale similarly for both small and planetary-scale impacts as a function of impact energy. However, in planetary-scale impacts a significant fraction of the melt is sequestered at depth and thus does not contribute to resetting the planetary surface; complete surface resetting is likely only in the most energetic (6 x 10(29) J), slow, and head-on impacts simulated. A crater rim is not present for planetary-scale impacts with energies >10(29) J and angles <= 45 degrees, but rather the ejecta is more uniformly distributed over the planetary surface. Antipodal crustal removal and melting is present for energetic (>10(29) J), fast (>6 km/s), and low angle (<= 45 degrees) impacts. The most massive impactors (with both high impact energy and low velocity) contribute sufficient angular momentum to increase the rotation period of the Mars-sized target to about a day. Impact velocities of >20 km/s result in net mass erosion from the target, for all simulated energies and angles. The hypothesized impact origin of planetary structures may be tested by the presence and distribution of the geochemically-distinct impactor material. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Marinova, Margarita M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Marinova, Margarita M.; Aharonson, Oded] CALTECH, Pasadena, CA 91125 USA.
[Asphaug, Erik] Univ Calif Santa Cruz, Dept Earth Sci, Santa Cruz, CA 95064 USA.
RP Marinova, MM (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
EM Margarita.M.Marinova@gmail.com; oa@gps.-caltech.edu; easphaug@ucsc.edu
FU Henshaw Fellowship; NSERC; Canadian Space Agency
FX We thank Robin Canup, Paul Asimow, Andy Ingersoll, and Dave Stevenson
for insightful discussions and dedicated help. This work was supported
by a Henshaw Fellowship, an NSERC post-graduate fellowship, and a
Canadian Space Agency supplement.
NR 79
TC 26
Z9 26
U1 2
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2011
VL 211
IS 2
BP 960
EP 985
DI 10.1016/j.icarus.2010.10.032
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 715TE
UT WOS:000286909700004
ER
PT J
AU Li, JY
Kuchner, MJ
Allen, RJ
Sheppard, SS
AF Li, Jian-Yang
Kuchner, Marc J.
Allen, Ronald J.
Sheppard, Scott S.
TI Measuring the sizes, shapes, surface features and rotations of Solar
System objects with interferometry
SO ICARUS
LA English
DT Article
DE Asteroids; Centaurs
ID HUBBLE-SPACE-TELESCOPE; KUIPER-BELT OBJECTS; DIFFERENT PHASE ANGLES;
NEAR-EARTH ASTEROIDS; CENTAUR 1999 UG(5); PHOTOMETRIC ANALYSIS; 50000
QUAOAR; WATER ICE; 2003 EL61; 1 CERES
AB We consider the application of interferometry to measuring the sizes and shapes of small bodies in the Solar System that cannot be spatially resolved by today's single-dish telescopes. Assuming ellipsoidal shapes, we provide a formalism to derive the shape parameters from visibility measurements along three different baseline orientations. Our results indicate that interferometers can measure the size of an object to better than 15% uncertainty if the limb-darkening is unknown. Assuming a Minnaert scattering model, one can theoretically derive the limb-darkening parameters from simultaneous measurements of visibilities at several different projected baseline lengths to improve the size and shape determination to an accuracy of a few percent. The best size measurement can be reached when one axis of the object's projected disk is aligned with one baseline orientation, and the measurement of cross-sectional area is independent of baseline orientation. We construct a 3-D shape model for the dwarf planet Haumea and use it to synthesize interferometric data sets. Using the Haumea model, we demonstrate that when photometric light curve, visibility light curve, and visibility phase center displacement are combined, the rotational period and sense of rotation can all be derived, and the rotational pole can be estimated. Because of its elongated shape and the dark red spot, the rotation of Haumea causes its optical photocenter to move in a loop on the sky. Our simulations show that this loop has an extend of about 80 mu as without the dark red spot, and about 200 mu as with it. Such movements are easily detectable by space-based astrometric interferometer designed e.g. for planet detection. As an example, we consider the possible contributions to the study of small bodies in the Solar System by the Space Interferometry Mission. We show that such a mission could make substantial contributions in characterizing the fundamental physical properties of the brightest Kuiper Belt Objects and Centaurs as well as a large number of main belt asteroids. We compile a list of Kuiper Belt Objects and Centaurs that are potentially scientifically interesting and observable by such missions. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Li, Jian-Yang] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Allen, Ronald J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Sheppard, Scott S.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Li, JY (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM jyli@astro.umd.edu
RI Kuchner, Marc/E-2288-2012
FU NASA Exoplanet Science Institute
FX We thank the NASA Exoplanet Science Institute for support of this
research via a SIM Science Studies grant. The authors are extremely
grateful to the reviewers, who provided reviews that have helped improve
this manuscript substantially.
NR 99
TC 4
Z9 4
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2011
VL 211
IS 2
BP 1007
EP 1021
DI 10.1016/j.icarus.2010.11.017
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 715TE
UT WOS:000286909700007
ER
PT J
AU Johnson, AP
Pratt, LM
Vishnivetskaya, T
Pfiffner, S
Bryan, RA
Dadachova, E
Whyte, L
Radtke, K
Chan, E
Tronick, S
Borgonie, G
Mancinelli, RL
Rothschild, LJ
Rogoff, DA
Horikawa, DD
Onstott, TC
AF Johnson, A. P.
Pratt, L. M.
Vishnivetskaya, T.
Pfiffner, S.
Bryan, R. A.
Dadachova, E.
Whyte, L.
Radtke, K.
Chan, E.
Tronick, S.
Borgonie, G.
Mancinelli, R. L.
Rothschild, L. J.
Rogoff, D. A.
Horikawa, D. D.
Onstott, T. C.
TI Extended survival of several organisms and amino acids under simulated
martian surface conditions
SO ICARUS
LA English
DT Article
DE Exobiology; Mars; Regoliths; Search for extraterrestrial life;
Photochemistry
ID X-RAY SPECTROMETER; SIBERIAN PERMAFROST; ULTRAVIOLET-RADIATION;
MERIDIANI-PLANUM; EARLY MARS; METHANOGENIC ARCHAEA; SPACECRAFT SURFACES;
BACILLUS-SUBTILIS; LOW-TEMPERATURE; UV-IRRADIATION
AB Recent orbital and landed missions have provided substantial evidence for ancient liquid water on the martian surface as well as evidence of more recent sedimentary deposits formed by water and/or ice. These observations raise serious questions regarding an independent origin and evolution of life on Mars. Future missions seek to identify signs of extinct martian biota in the form of biomarkers or morphological characteristics, but the inherent danger of spacecraft-borne terrestrial life makes the possibility of forward contamination a serious threat not only to the life detection experiments, but also to any extant martian ecosystem. A variety of cold and desiccation-tolerant organisms were exposed to 40 days of simulated martian surface conditions while embedded within several centimeters of regolith simulant in order to ascertain the plausibility of such organisms survival as a function of environmental parameters and burial depth. Relevant amino acid biomarkers associated with terrestrial life were also analyzed in order to understand the feasibility of detecting chemical evidence for previous biological activity. Results indicate that stresses due to desiccation and oxidation were the primary deterrent to organism survival, and that the effects of UV-associated damage, diurnal temperature variations, and reactive atmospheric species were minimal. Organisms with resistance to desiccation and radiation environments showed increased levels of survival after the experiment compared to organisms characterized as psychrotolerant. Amino acid analysis indicated the presence of an oxidation mechanism that migrated downward through the samples during the course of the experiment and likely represents the formation of various oxidizing species at mineral surfaces as water vapor diffused through the regolith. Current sterilization protocols may specifically select for organisms best adapted to survival at the martian surface, namely species that show tolerance to radical-induced oxidative damage and low water activity environments. Additionally, any hypothetical martian ecosystems may have evolved similar physiological traits that allow sporadic metabolism during periods of increased water activity. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Johnson, A. P.] Indiana Univ, Dept Mol & Cellular Biochem, Bloomington, IN 47405 USA.
[Pratt, L. M.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Vishnivetskaya, T.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA.
[Pfiffner, S.] Univ Tennessee, Ctr Environm Biotechnol, Dept Microbiol, Knoxville, TN 37932 USA.
[Dadachova, E.] Albert Einstein Coll Med, Dept Nucl Med, Dept Microbiol & Immunol, Bronx, NY 10461 USA.
[Whyte, L.; Radtke, K.] McGill Univ, Dept Nat Resource Sci, Quebec City, PQ H9X 3V9, Canada.
[Chan, E.; Tronick, S.; Onstott, T. C.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA.
[Borgonie, G.] Univ Ghent, Dept Biol, Nematol Sect, B-9000 Ghent, Belgium.
[Mancinelli, R. L.] SETI Inst, Mountain View, CA 94043 USA.
[Rogoff, D. A.] NASA, Ames Res Ctr, BAER Inst, Moffett Field, CA 94035 USA.
RP Johnson, AP (reprint author), Indiana Univ, Dept Mol & Cellular Biochem, 1001 E 10th St, Bloomington, IN 47405 USA.
EM adpjohns@indiana.edu; prattl@indiana.edu; vishnivetsta@ornl.gov;
pfiffner@utk.edu; rbryan@aecom.yu.edu;
ekaterina.dadachova@einstein.yu.edu; lyle.whyte@mcgill.ca;
kristin.radtke@mail.mcgill.ca; eric.chan@tamu.edu;
shannon.tronick@gmail.com; GBorgonie@gmail.com;
rocco.l.mancinelli@nasa.gov; lynn.j.rothschild@nasa.gov;
Dana.A.Rogoff@nasa.gov; horikawadd@gmail.com; tullis@princeton.edu
RI Dadachova, Ekaterina/I-7838-2013; Vishnivetskaya, Tatiana/A-4488-2008;
Mancinelli, Rocco/L-8971-2016
OI Vishnivetskaya, Tatiana/0000-0002-0660-023X;
FU NASA Astrobiology Institute [NNA04CC03A S000018]; Indiana University
[2004 2058-000]
FX Special thanks to Dr. Paul Todd and Mr. Michael (Andy) Kurk of Tech Shot
Laboratories, Greenville, IN, for their help in setup, running and
sampling within the Mars Environmental Chamber. Additional thanks go to
Dr. Christine Shriner, Indiana University Department of Geological
Sciences, for her help in determining particle size distribution of the
I-MAR regolith. A large thank you goes to Dr. James Brophy, Indiana
University Department of Geological Sciences, for his help in obtaining
samples of the Collier Cone basalt and electron microprobe analysis of
the final elemental composition of the I-MAR regolith. Thanks to Dr.
Daniel P. Glavin and an unknown reviewer for their valuable insight and
comments on this manuscript while in review. This work was funded by the
NASA Astrobiology Institute Grant NNA04CC03A S000018. Tuition, fees, and
stipend support for Adam Johnson was provided by the Indiana University
Lily Metacyt Endowment Grant #2004 2058-000.
NR 116
TC 13
Z9 13
U1 4
U2 31
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2011
VL 211
IS 2
BP 1162
EP 1178
DI 10.1016/j.icarus.2010.11.011
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 715TE
UT WOS:000286909700018
ER
PT J
AU Smith, EJ
AF Smith, E. J.
TI Solar cycle evolution of the heliospheric magnetic field: The Ulysses
legacy
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Heliosphere; Magnetic field; Solar wind; Solar cycle
ID NORTH-SOUTH ASYMMETRY; RAPID LATITUDE SCAN; CURRENT SHEET; HELIOGRAPHIC
LATITUDES; WIND SPEED; GEOMAGNETIC-ACTIVITY; SECTOR STRUCTURE;
INTERPLANETARY; FLUX; SUN
AB Important contributions of Ulysses to understanding the solar cycle evolution of the heliospheric magnetic field (HMF) and solar wind are reviewed: a dramatic reorientation of the HMF as the solar dipole rotates between axial and equatorial orientations; solar cycle variation of the total heliospheric magnetic flux and its response to changes in solar magnetic fields; the unusual on-going solar minimum and its effects; a connection between magnetic flux and solar wind mass flux in the heliosphere and at the source; a recurrent north-south heliospheric asymmetry at solar minimum and the equatorial offset of the solar magnetic dipole. (C) 2010 Published by Elsevier Ltd.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Smith, EJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM edward.j.smith@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The results reported here represent one aspect of research carried out
by the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
Access to, and use of solar wind data (D.J. McComas, PI) is greatly
appreciated. I am grateful to Kevli Mursula for the invitation to
present this review. The comments of the reviewers were helpful
especially the one who demanded a reorganization of the manuscript so
the Ulysses legacy and context would be clearer.
NR 82
TC 18
Z9 18
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD FEB
PY 2011
VL 73
IS 2-3
SI SI
BP 277
EP 289
DI 10.1016/j.jastp.2010.03.019
PG 13
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 717NS
UT WOS:000287055300014
ER
PT J
AU Ruzmaikin, A
Feynman, J
Jun, I
AF Ruzmaikin, Alexander
Feynman, Joan
Jun, Insoo
TI Distribution of extreme solar energetic proton fluxes
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Energetic particles; Solar variability; Time series analysis; Stochastic
processes
ID EVENTS; MODEL
AB The knowledge of the high intensity tails of probability distributions that determine the rate of occurrence of extreme events of solar energetic particles is a critical element in the evaluation of hazards for human and robotic space missions. Here instead of the standard approach based on fitting a selected distribution function to the observed data we investigate a different approach, which is based on a study of the scaling properties of the maximum particle flux in time intervals of increasing length. To find the tail of the probability distributions we apply the "Max-Spectrum" method (Stoev, S.A., Michailidis, G., 2006. On the estimation of the heavy-tail exponent in time series using the Max-Spectrum. Technical Report 447, Department of Statistics, University of Michigan) to 1973-1997 IMP-8 proton data and the 1987-2008 GOES data, which cover a wide range of proton energies. We find that both data sets indicate a power-law tail with the power exponents close to 0.6 at least in the energy range 9-60 MeV. The underlying probability distribution is consistent with the Frechet type (power-law behavior) extreme value distribution. Since the production of high fluxes of energetic particles is caused by fast Coronal Mass Ejections (CMEs) this heavy-tailed distribution also means that the Sun generates more fast CMEs than would be expected from a Poissonian-type process. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Ruzmaikin, Alexander; Feynman, Joan; Jun, Insoo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Alexander.Ruzmaikin@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. We are grateful to Stilian Stoev for providing
us with his codes and discussions of the Max-Spectrum method. We thank
Alan Tylka for the processed IMP data. We thank two reviewers for
helpful comments. The GOES data are from the NOAA web site
http://www.ngdc.noaa.gov/stp/GOES/.
NR 20
TC 2
Z9 2
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD FEB
PY 2011
VL 73
IS 2-3
SI SI
BP 300
EP 307
DI 10.1016/j.jastp.2009.12.016
PG 8
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 717NS
UT WOS:000287055300017
ER
PT J
AU Townsend, LJ
Coe, MJ
Corbet, RHD
McBride, VA
Hill, AB
Bird, AJ
Schurch, MPE
Haberl, F
Sturm, R
Pathak, D
van Soelen, B
Bartlett, ES
Drave, SP
Udalski, A
AF Townsend, L. J.
Coe, M. J.
Corbet, R. H. D.
McBride, V. A.
Hill, A. B.
Bird, A. J.
Schurch, M. P. E.
Haberl, F.
Sturm, R.
Pathak, D.
van Soelen, B.
Bartlett, E. S.
Drave, S. P.
Udalski, A.
TI The orbital solution and spectral classification of the high-mass X-ray
binary IGR J01054-7253 in the Small Magellanic Cloud
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ephemerides; Magellanic Clouds; X-rays: binaries; stars: emission; line;
Be
ID II OUTBURST; ACCRETION; STARS; SPECTROSCOPY; VARIABILITY; UNDERGOES;
CATALOG; SXP6.85; PULSARS; LONG
AB We present X-ray and optical data on the Be/X-ray binary (BeXRB) pulsar IGR J 01054-7253 = SXP11.5 in the Small Magellanic Cloud (SMC). Rossi X-ray Timing Explorer (RXTE) observations of this source in a large X-ray outburst reveal an 11.483 +/- 0.002 s pulse period and show both the accretion-driven spin-up of the neutron star and the motion of the neutron star around the companion through Doppler shifting of the spin period. Model fits to these data suggest an orbital period of 36.3 +/- 0.4 d and of (4.7 +/- 0.3) x 10-10 seconds s-1. We present an orbital solution for this system, making it one of the best-described BeXRB systems in the SMC. The observed pulse period, spin-up and X-ray luminosity of SXP11.5 in this outburst are found to agree with the predictions of neutron star accretion theory. Timing analysis of the long-term optical light curve reveals a periodicity of 36.70 +/- 0.03 d, in agreement with the orbital period found from the model fit to the X-ray data. Using blue-end spectroscopic observations we determine the spectral type of the counterpart to be O9.5-B0 IV-V. This luminosity class is supported by the observed V-band magnitude. Using optical and near-infrared photometry and spectroscopy, we study the circumstellar environment of the counterpart in the months after the X-ray outburst.
C1 [Townsend, L. J.; Coe, M. J.; McBride, V. A.; Bird, A. J.; Bartlett, E. S.; Drave, S. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Corbet, R. H. D.] Univ Maryland Baltimore Cty, Xray Astrophys Lab, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hill, A. B.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble LAOG, UMR 5571, F-38041 Grenoble 09, France.
[Schurch, M. P. E.] Univ Cape Town, Dept Astron, ACGC, ZA-7701 Rondebosch, South Africa.
[Haberl, F.; Sturm, R.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Pathak, D.] Cardiff Univ, Sch Phys & Astron, Faulkes Telescopes Project, Cardiff CF24 3AA, S Glam, Wales.
[van Soelen, B.] Univ Free State, Dept Phys, ZA-9300 Bloemfontein, South Africa.
[Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Townsend, LJ (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
EM ljt203@soton.ac.uk
OI Haberl, Frank/0000-0002-0107-5237; Hill, Adam/0000-0003-3470-4834;
Pathak, Devanka/0000-0002-1768-8353; Bartlett,
Elizabeth/0000-0003-0634-4405
FU University of Southampton; European Community [ERC-StG-200911]; Dorothy
Hodgkin Postgraduate Award; South African Square Kilometre Array
Project; Polish MNiSW [N20303032/4275]
FX LJT is supported by a Mayflower scholarship from the University of
Southampton. ABH is funded by contract ERC-StG-200911 from the European
Community. DP acknowledges support from a Dorothy Hodgkin Postgraduate
Award. BvS is funded by the South African Square Kilometre Array
Project. This paper uses observations made at the South African
Astronomical Observatory (SAAO). The authors are grateful for the
assistance of D. J. Wium with the photometric observations performed on
the SAAO 1.9-m telescope. The OGLE project is partially supported by the
Polish MNiSW grant N20303032/4275. LJT would like to thank the X-shooter
team at ESO for providing a good beta-version pipeline and several
helpful suggestions during the reduction of the SV1 data presented in
this paper. We would like to thank the anonymous referee for their
positive and swift feedback and constructive comments.
NR 51
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U1 0
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 FEB
PY 2011
VL 410
IS 3
BP 1813
EP 1824
DI 10.1111/j.1365-2966.2010.17563.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703TN
UT WOS:000286004300034
ER
PT J
AU Mishchenko, MI
Dlugach, JM
Mackowski, DW
AF Mishchenko, Michael I.
Dlugach, Janna M.
Mackowski, Daniel W.
TI Light scattering by wavelength-sized particles "dusted" with
subwavelength-sized grains
SO OPTICS LETTERS
LA English
DT Article
ID SURFACE-ROUGHNESS; AEROSOLS
AB The numerically exact superposition T-matrix method is used to compute the scattering cross sections and the Stokes scattering matrix for polydisperse spherical particles covered with a large number of much smaller grains. We show that the optical effect of the presence of microscopic dust on the surfaces of wavelength-sized, weakly absorbing particles is much less significant than that of a major overall asphericity of the particle shape. (C) 2011 Optical Society of America
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
[Mackowski, Daniel W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM mmishchenko@giss.nasa.gov
RI Mackowski, Daniel/K-1917-2013; Mishchenko, Michael/D-4426-2012
FU National Aeronautics and Space Administration (NASA)
FX We are grateful to Timo Nousiainen for a useful discussion and anonymous
reviewers for constructive comments and suggestions. This research was
supported by the National Aeronautics and Space Administration (NASA)
Radiation Sciences Program managed by Hal Maring and by the NASA Glory
Mission Project.
NR 22
TC 12
Z9 12
U1 0
U2 5
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
EI 1539-4794
J9 OPT LETT
JI Opt. Lett.
PD FEB 1
PY 2011
VL 36
IS 3
BP 337
EP 339
DI 10.1364/OL.36.000337
PG 3
WC Optics
SC Optics
GA 713HO
UT WOS:000286726900010
PM 21283182
ER
PT J
AU Jones, CE
Davis, BA
AF Jones, Cathleen E.
Davis, Bruce A.
TI HIGH RESOLUTION RADAR FOR RESPONSE AND RECOVERY MONITORING CONTAINMENT
BOOMS IN BARATARIA BAY
SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING
LA English
DT Editorial Material
ID SAR IMAGES
C1 [Jones, Cathleen E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jones, CE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM cathleen.jones@ipl.nasa.gov; Bruce.A.Davis@dhs.gov
NR 5
TC 5
Z9 5
U1 0
U2 3
PU AMER SOC PHOTOGRAMMETRY
PI BETHESDA
PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA
SN 0099-1112
J9 PHOTOGRAMM ENG REM S
JI Photogramm. Eng. Remote Sens.
PD FEB
PY 2011
VL 77
IS 2
BP 102
EP 105
PG 4
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA 722VR
UT WOS:000287463900001
ER
PT J
AU Chrysoulakis, N
Abrams, M
Kamarianakis, Y
Stanislawski, M
AF Chrysoulakis, N.
Abrams, M.
Kamarianakis, Y.
Stanislawski, M.
TI Validation of ASTER GDEM for the Area of Greece
SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING
LA English
DT Article
ID DIGITAL ELEVATION MODELS; SPACEBORNE THERMAL EMISSION; REFLECTION
RADIOMETER ASTER; PRODUCTS; PLATFORM; IMAGES; SRTM; DEM
AB The ASTER (Advanced Spaceborne Thermal Emission and Reflection Radiometer) Global Digital Elevation Model (GDEM), which was released in June 2009, provides elevation data for over 99 percent of Earth's land area. GDEM was found to contain significant anomalies mainly caused by residual clouds in the ASTER scenes, or by the algorithm used to generate the final GDEM from the variable number of individual DEMs. In this paper, the GDEM, for the whole area of Greece was validated by comparing it with reference DEMs with higher resolution derived either from aerial stereo imagery, or from ASTER raw data analysis; as well as with elevation values provided by a number of Geodetic Control Points (GCP) and GPS measurements. The vertical accuracy (at 95 percent confidence) was calculated to be more than 30 m (RMSE = 16.01 m) when compared to the GCPs, whereas the vertical accuracy was calculated around 20 in (RMSE = 11.08 m) when compared with the GPS derived elevations. It can be therefore stated that the current version of ASTER GDEM overall does not meet its pre-production estimated vertical accuracy of 20 in at 95 percent confidence over Greece, however, it can be used in several applications, such as topographic analysis, hydrological and geomorphological modeling, landscape visualization, and energy balance studies.
C1 [Chrysoulakis, N.; Stanislawski, M.] Fdn Res & Technol Hellas, Inst Appl & Computat Math, Iraklion 71110, Crete, Greece.
[Abrams, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kamarianakis, Y.] Cornell Univ, Sch Civil & Environm Engn, Ithaca, NY 14853 USA.
RP Chrysoulakis, N (reprint author), Fdn Res & Technol Hellas, Inst Appl & Computat Math, N Plastira 100,POB 1385, Iraklion 71110, Crete, Greece.
EM zedd2@iacm.forth.gr
FU European Community [FP7/2007-2013, 211345]; National Aeronautics and
Space Administration
FX The research leading to these results has received funding from the
European Community's Seventh Framework Programme (FP7/2007-2013) under
Grant Agreement No. 211345 (BRIDGE Project). Work by Abrams was
performed at the Jet Propulsion Laboratory, California Institute of
Technology under contract with the National Aeronautics and Space
Administration.
NR 36
TC 10
Z9 11
U1 0
U2 6
PU AMER SOC PHOTOGRAMMETRY
PI BETHESDA
PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA
SN 0099-1112
J9 PHOTOGRAMM ENG REM S
JI Photogramm. Eng. Remote Sens.
PD FEB
PY 2011
VL 77
IS 2
BP 157
EP 165
PG 9
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA 722VR
UT WOS:000287463900007
ER
PT J
AU Devasthale, A
Tjernstrom, M
Karlsson, KG
Thomas, MA
Jones, C
Sedlar, J
Omar, AH
AF Devasthale, Abhay
Tjernstrom, Michael
Karlsson, Karl-Goran
Thomas, Manu Anna
Jones, Colin
Sedlar, Joseph
Omar, Ali H.
TI The vertical distribution of thin features over the Arctic analysed from
CALIPSO observations
SO TELLUS SERIES B-CHEMICAL AND PHYSICAL METEOROLOGY
LA English
DT Article
ID CLOUD PROPERTIES; SURFACE; RADIATION; OCEAN; ALGORITHM; EMISSIVITY;
RETRIEVAL
AB Clouds play a crucial role in the Arctic climate system. Therefore, it is essential to accurately and reliably quantify and understand cloud properties over the Arctic. It is also important to monitor and attribute changes in Arctic clouds. Here, we exploit the capability of the CALIPSO-CALIOP instrument and provide comprehensive statistics of tropospheric thin clouds, otherwise extremely difficult to monitor from passive satellite sensors. We use 4 yr of data (June 2006-May 2010) over the circumpolar Arctic, here defined as 67-82 degrees N, and characterize probability density functions of cloud base and top heights, geometrical thickness and zonal distribution of such cloud layers, separately for water and ice phases, and discuss seasonal variability of these properties. When computed for the entire study area, probability density functions of cloud base and top heights and geometrical thickness peak at 200-400, 1000-2000 and 400-800 m, respectively, for thin water clouds, while for ice clouds they peak at 6-8, 7-9 and 400-1000 m, respectively. In general, liquid clouds were often identified below 2 km during all seasons, whereas ice clouds were sensed throughout the majority of the upper troposphere and also, but to a smaller extent, below 2 km for all seasons.
C1 [Devasthale, Abhay; Karlsson, Karl-Goran] Swedish Meteorol & Hydrol Inst, Remote Sensing Div, S-60176 Norrkoping, Sweden.
[Tjernstrom, Michael; Sedlar, Joseph] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden.
[Thomas, Manu Anna] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England.
[Jones, Colin] Swedish Meteorol & Hydrol Inst, Rossby Ctr, S-60176 Norrkoping, Sweden.
[Omar, Ali H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA.
RP Devasthale, A (reprint author), Swedish Meteorol & Hydrol Inst, Remote Sensing Div, Folkborgsvagen 1, S-60176 Norrkoping, Sweden.
EM Abhay.Devasthale@smhi.se
RI Omar, Ali/D-7102-2017;
OI Omar, Ali/0000-0003-1871-9235; Devasthale, Abhay/0000-0002-6717-8343
FU Swedish National Space Board
FX The authors gratefully acknowledge the CALIPSO Science Team and NASA
Langley Atmospheric Science Data Center (ASDC) for making data freely
available for research. This work was supported by the Swedish National
Space Board.
NR 37
TC 13
Z9 13
U1 1
U2 11
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0280-6509
J9 TELLUS B
JI Tellus Ser. B-Chem. Phys. Meteorol.
PD FEB
PY 2011
VL 63
IS 1
BP 77
EP 85
DI 10.1111/j.1600-0889.2010.00516.x
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 703SP
UT WOS:000286001900006
ER
PT J
AU Devasthale, A
Tjernstrom, M
Omar, AH
AF Devasthale, Abhay
Tjernstrom, Michael
Omar, Ali H.
TI The vertical distribution of thin features over the Arctic analysed from
CALIPSO observations
SO TELLUS SERIES B-CHEMICAL AND PHYSICAL METEOROLOGY
LA English
DT Article
ID POLLUTION TRANSPORT; AIR-POLLUTION; AEROSOL; CLOUD; CLIMATE; SUMMER;
TROPOSPHERE; EMISSIVITY; ALGORITHM; PROFILES
AB Influx of aerosols from the mid-latitudes has a wide range of impacts on the Arctic atmosphere. In this study, the capability of the CALIPSO-CALIOP instrument to provide accurate observations of aerosol layers is exploited to characterize their vertical distribution, probability density functions (PDFs) of aerosol layer thickness, base and top heights, and optical depths over the Arctic for the 4-yr period from June 2006 to May 2010. It is shown that the bulk of aerosols, from about 65% in winter to 45% in summer, are confined below the lowermost kilometer of the troposphere. In the middle troposphere (3-5 km), spring and autumn seasons show slightly higher aerosol amounts compared to other two seasons. The relative vertical distribution of aerosols shows that clean continental aerosol is the largest contributor in all seasons except in summer, when layers of polluted continental aerosols are almost as large. In winter and spring, polluted continental aerosols are the second largest contributor to the total number of observed aerosol layers, whereas clean marine aerosol is the second largest contributor in summer and autumn. The PDFs of the geometrical thickness of the observed aerosol layers peak about 400-700 m. Polluted continental and smoke aerosols, which are associated with the intrusions from mid-latitudes, have much broader distributions of optical and geometrical thicknesses, suggesting that they appear more often optically thicker and higher up in the troposphere.
C1 [Devasthale, Abhay] Swedish Meteorol & Hydrol Inst, Remote Sensing Div, S-60176 Norrkoping, Sweden.
[Tjernstrom, Michael] Univ Stockholm, Dept Meteorol, S-10691 Stockholm, Sweden.
[Tjernstrom, Michael] Univ Stockholm, Bert Bolin Ctr Climate Res, Stockholm, Sweden.
[Omar, Ali H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA.
RP Devasthale, A (reprint author), Swedish Meteorol & Hydrol Inst, Remote Sensing Div, Folkborgsvagen 1, S-60176 Norrkoping, Sweden.
EM Abhay.Devasthale@smhi.se
RI Omar, Ali/D-7102-2017;
OI Omar, Ali/0000-0003-1871-9235; Devasthale, Abhay/0000-0002-6717-8343
FU Swedish National Space Board
FX The authors gratefully acknowledge the CALIPSO Science Team and the NASA
Langley Atmospheric Science Data Center (ASDC) for making CALIPSO data
freely available for research. This work is supported by the Swedish
National Space Board.
NR 36
TC 8
Z9 10
U1 1
U2 8
PU CO-ACTION PUBLISHING
PI JARFALLA
PA RIPVAGEN 7, JARFALLA, SE-175 64, SWEDEN
SN 0280-6509
EI 1600-0889
J9 TELLUS B
JI Tellus Ser. B-Chem. Phys. Meteorol.
PD FEB
PY 2011
VL 63
IS 1
BP 86
EP 95
DI 10.1111/j.1600-0889.2010.00517.x
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 703SP
UT WOS:000286001900007
ER
PT J
AU Yaitskova, N
Troy, M
AF Yaitskova, Natalia
Troy, Mitchell
TI Rolled edges and phasing of segmented telescopes
SO APPLIED OPTICS
LA English
DT Article
ID MIRROR SEGMENTS; KECK TELESCOPES; ALGORITHM
AB To achieve the diffraction limit, the segments in a segmented telescope must be correctly aligned to a fraction of a wavelength. This alignment is performed via optical measurements using starlight. We investigate the piston degree of freedom or phasing of the segments and the impact of rolled segment edges on the accuracy of the optical alignment. Three models for edge profiles are developed and fit to data from optic manufacturers. These profiles are then used, along with a simplified model of a Shack-Hartmann optical sensor, to determine their impact on phasing accuracy. The results can help estimate the residual phasing error and set requirements on segment polishing. (c) 2011 Optical Society of America
C1 [Yaitskova, Natalia] European Org Astron Res So Hemisphere, D-85748 Garching, Germany.
[Troy, Mitchell] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yaitskova, N (reprint author), European Org Astron Res So Hemisphere, Karl Schwarzschildstr 2, D-85748 Garching, Germany.
EM nyaitsko@eso.org
FU California Institute of Technology; National Aeronautics and Space
Administration (NASA); Association of Canadian Universities for Research
in Astronomy; University of California; Gordon and Betty Moore
Foundation; Canada Foundation for Innovation; Ontario Ministry of
Research and Innovation; National Research Council of Canada (NRC);
Natural Sciences and Engineering Research Council of Canada; British
Columbia Knowledge Development Fund; Association of Universities for
Research in Astronomy; United States National Science Foundation (NSF)
FX This research was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, and was sponsored by the California
Institute of Technology and the National Aeronautics and Space
Administration (NASA). The TMT Project gratefully acknowledges the
support of the TMT partner institutions. They are the Association of
Canadian Universities for Research in Astronomy, the California
Institute of Technology, and the University of California. This work was
supported as well by the Gordon and Betty Moore Foundation, the Canada
Foundation for Innovation, the Ontario Ministry of Research and
Innovation, the National Research Council of Canada (NRC), the Natural
Sciences and Engineering Research Council of Canada, the British
Columbia Knowledge Development Fund, the Association of Universities for
Research in Astronomy, and the United States National Science Foundation
(NSF).
NR 17
TC 1
Z9 1
U1 0
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD FEB 1
PY 2011
VL 50
IS 4
BP 542
EP 553
DI 10.1364/AO.50.000542
PG 12
WC Optics
SC Optics
GA 714JJ
UT WOS:000286805600033
PM 21283246
ER
PT J
AU Jones, DL
Fomalont, E
Dhawan, V
Romney, J
Folkner, WM
Lanyi, G
Border, J
Jacobson, RA
AF Jones, Dayton L.
Fomalont, Ed
Dhawan, Vivek
Romney, Jon
Folkner, William M.
Lanyi, Gabor
Border, James
Jacobson, Robert A.
TI VERY LONG BASELINE ARRAY ASTROMETRIC OBSERVATIONS OF THE CASSINI
SPACECRAFT AT SATURN
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE astrometry; planets and satellites: individual (Saturn); techniques:
interferometric
ID CELESTIAL REFERENCE FRAME; RADIO INTERFEROMETRY; POSITION; JUPITER;
SYSTEM; MASS
AB The planetary ephemeris is an essential tool for interplanetary spacecraft navigation, studies of solar system dynamics (including, for example, barycenter corrections for pulsar timing ephemerides), the prediction of occultations, and tests of general relativity. We are carrying out a series of astrometric very long baseline interferometry observations of the Cassini spacecraft currently in orbit around Saturn, using the Very Long Baseline Array (VLBA). These observations provide positions for the center of mass of Saturn in the International Celestial Reference Frame (ICRF) with accuracies similar to 0.3 mas (1.5 nrad) or about 2 km at the average distance of Saturn. This paper reports results from eight observing epochs between 2006 October and 2009 April. These data are combined with two VLBA observations by other investigators in 2004 and a Cassini-based gravitational deflection measurement by Fomalont et al. in 2009 to constrain a new ephemeris (DE 422). The DE 422 post-fit residuals for Saturn with respect to the VLBA data are generally 0.2 mas, but additional observations are needed to improve the positions of all of our phase reference sources to this level. Over time we expect to be able to improve the accuracy of all three coordinates in the Saturn ephemeris (latitude, longitude, and range) by a factor of at least three. This will represent a significant improvement not just in the Saturn ephemeris but also in the link between the inner and outer solar system ephemerides and in the link to the inertial ICRF.
C1 [Jones, Dayton L.; Folkner, William M.; Lanyi, Gabor; Border, James; Jacobson, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fomalont, Ed] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Dhawan, Vivek; Romney, Jon] Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Jones, DL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dayton.jones@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX We are grateful to Larry Teitelbaum for support of this project through
the Advanced Tracking and Observational Techniques office of JPL's
Interplanetary Network Directorate, and to John Benson and the VLBA
operations staff at NRAO for their excellent support of these
observations. We also thank Peter Antreasian and Fred Pelletier at JPL
for providing the reconstructed Cassini orbit files used for data
correlation at NRAO. The anonymous referee's comments led to significant
improvements in the paper. The VLBA is a facility of the National Radio
Astronomy Observatory, which is operated by Associated Universities,
Inc., under a cooperative agreement with the National Science
Foundation. Part of this research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 35
TC 19
Z9 21
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2011
VL 141
IS 2
AR 29
DI 10.1088/0004-6256/141/2/29
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706AW
UT WOS:000286186100001
ER
PT J
AU Urzay, J
Nayagam, V
Williams, FA
AF Urzay, Javier
Nayagam, Vedha
Williams, Forman A.
TI Theory of the propagation dynamics of spiral edges of diffusion flames
in von Karman swirling flows
SO COMBUSTION AND FLAME
LA English
DT Article
DE Edge flames; Triple flames; Non-premixed combustion; Spiral waves; Flame
extinction; Swirling flows
ID MIXING LAYERS; EXCITABLE MEDIA; LAMINAR FLAMES; WAVE DYNAMICS; TRIPLE
FLAME; COUNTERFLOW; EXTINCTION; COMBUSTION; FRONTS; BURNER
AB This analysis addresses the propagation of spiral edge flames found in von Karman swirling flows induced in rotating porous-disk burners. In this configuration, a porous disk 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. Among other flame patterns experimentally found, a stable, rotating spiral flame is observed for sufficiently large rotation velocities and small fuel flow rates as a result of partial extinction of the underlying diffusion flame. The tip of the spiral can undergo a steady rotation for sufficiently large rotational velocities or small fuel flow rates, whereas a meandering tip in an epicycloidal trajectory is observed for smaller rotational velocities and larger fuel flow rates. A formulation of this problem is presented in the equidiffusional and thermodiffusive limits within the framework of one-step chemistry with large activation energies. Edge-flame propagation regimes are obtained by scaling analyses of the conservation equations and exemplified by numerical simulations of straight two-dimensional edge flames near a cold porous wall, for which lateral heat losses to the disk and large strains induce extinction of the trailing diffusion flame but are relatively unimportant in the front region, consistent with the existence of the cooling tail found in the experiments. The propagation dynamics of a steadily rotating spiral edge is studied in the large-core limit, for which the characteristic Markstein length is much smaller than the distance from the center at which the spiral tip is anchored. An asymptotic description of the edge tangential structure is obtained, spiral edge shapes are calculated, and an expression is found that relates the spiral rotational velocity to the rest of the parameters. A quasiestatic stability analysis of the edge shows that the edge curvature at extinction in the tip region is responsible for the stable tip anchoring at the core radius. Finally, experimental results are analyzed, and theoretical predictions are tested. (C) 2010 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.
[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, La Jolla, CA 92093 USA.
EM jurzay@ucsd.edu; vedha.nayagam@grc.nasa.gov; faw@ucsd.edu
RI Urzay, Javier /H-6029-2013
FU NASA
FX The authors are indebted to Professor A. Linan for instructive
conversations about this problem. The first author is also grateful to
Professor P.A. Libby, Professor E. Fernandez-Tarrazo, Dr. V. Kurdyumov,
Professor J. Daou and Professor J.C. Prince for thoughtful suggestions
on the numerical calculations, and to Professor J.C. Del Alamo's lab for
the computational time. This work was partially supported by the NASA
Microgravity Combustion Science Program.
NR 46
TC 2
Z9 2
U1 3
U2 12
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
J9 COMBUST FLAME
JI Combust. Flame
PD FEB
PY 2011
VL 158
IS 2
BP 255
EP 272
DI 10.1016/j.combustflame.2010.08.015
PG 18
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA 710ZU
UT WOS:000286556300006
ER
PT J
AU Pfeffer, J
Boucher, M
Hinderer, J
Favreau, G
Boy, JP
de Linage, C
Cappelaere, B
Luck, B
Oi, M
Le Moigne, N
AF Pfeffer, Julia
Boucher, Marie
Hinderer, Jacques
Favreau, Guillaume
Boy, Jean-Paul
de Linage, Caroline
Cappelaere, Bernard
Luck, Bernard
Oi, Monique
Le Moigne, Nicolas
TI Local and global hydrological contributions to time-variable gravity in
Southwest Niger
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Satellite geodesy; Time variable gravity; Hydrology; Permeability and
porosity; Africa
ID WATER STORAGE; MAGNETIC-RESONANCE; SUPERCONDUCTING GRAVIMETER; AQUIFER
CHARACTERIZATION; SEMIARID NIGER; SURFACE LOADS; WEST NIGER; LONG-TERM;
SYSTEM; GRACE
AB P>Advances in methods of observation are essential to ensure a better understanding of changes in water resources considering climate variability and human activities. The GHYRAF (Gravity and Hydrology in Africa) experiments aim to combine gravimetric measurements with dense hydrological surveys to better characterize the annual water storage variability in tropical West Africa. The first absolute gravimetric measurements were performed in Southwest Niger, near a temporary pond where rapid infiltration to an unconfined aquifer occurs. As gravity is sensitive both to local and global variations of water mass distribution, the large-scale hydrological contribution to time-variable gravity has been removed using either GRACE satellite data or global hydrology models. The effect of the local water storage changes was modelled using in situ measurements of the water table, soil moisture and pond water level. The adjustment of these simulations to residual ground gravity observations helped to constrain the specific yield to a value ranging between 1.8 and 6.2 per cent. This range of value is consistent, albeit on the low side, with the aquifer water content (6-12 per cent) estimated by magnetic resonance soundings, which are known to slightly overestimate the specific yield in this geological context. The comparison of these two independent geophysical methods shows their potential to constrain the local hydrogeological parameters. Besides, this study evidences the worth of correcting the gravity signal for large-scale hydrology before recovering local water storage parameters.
C1 [Pfeffer, Julia; Hinderer, Jacques; Boy, Jean-Paul; Luck, Bernard] CNRS UdS, IPGS EOST, UMR 7516, F-67084 Strasbourg, France.
[Boucher, Marie; Favreau, Guillaume; Cappelaere, Bernard; Oi, Monique] Inst Rech Dev, Niamey, Niger.
[Boucher, Marie; Favreau, Guillaume; Cappelaere, Bernard; Oi, Monique] Univ Montpellier 2, F-34095 Montpellier 5, France.
[Boy, Jean-Paul] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[de Linage, Caroline] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Le Moigne, Nicolas] Univ Montpellier 2, UMR CNRS UM2 5243, Montpellier, France.
RP Pfeffer, J (reprint author), CNRS UdS, IPGS EOST, UMR 7516, 5 Rue Rene Descartes, F-67084 Strasbourg, France.
EM Julia.Pfeffer@unistra.fr
RI Favreau, guillaume/A-7573-2008; Boucher, Marie/M-7393-2016; Boy,
Jean-Paul/E-6677-2017
OI Favreau, guillaume/0000-0001-7358-9301; Boucher,
Marie/0000-0003-4994-2448; Boy, Jean-Paul/0000-0003-0259-209X
FU French Agence Nationale de la Recherche (ANR); Centre National d' Etudes
Spatiales (CNES); French ministry of research
FX This project is funded by the French Agence Nationale de la Recherche
(ANR) during 4 yr (2008-2011). It is also partly granted by the Centre
National d' Etudes Spatiales (CNES). Jean-Paul Boy is currently visiting
NASA Goddard Space Flight Center, with a Marie Curie International
Outgoing Fellowship (No. PIOF-GA-2008-221753). The GLDAS data used in
this study were acquired as part of the mission of NASA's Earth Science
Division and archived and distributed by the Goddard Earth Sciences
(GES) Data and Information Services Center (DISC). Hydrological surveys
are part of the regional AMMA-CATCH hydrological and meteorological
observatory on West Africa, funded by French ministry of research
(http://www.amma-catch.org). We thank the Institut de Recherche pour le
Developpement (IRD) in Niger for the strong logistic and manpower
support. We also warmly acknowledge the Ministry of Hydraulics and the
Department of Geology of the University Abdou Moumouni in Niamey (Niger)
for their assistance.
NR 67
TC 19
Z9 20
U1 3
U2 19
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0956-540X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD FEB
PY 2011
VL 184
IS 2
BP 661
EP 672
DI 10.1111/j.1365-246X.2010.04894.x
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 706NO
UT WOS:000286225300010
ER
PT J
AU Moller, D
Hensley, S
Sadowy, GA
Fisher, CD
Michel, T
Zawadzki, M
Rignot, E
AF Moller, Delwyn
Hensley, Scott
Sadowy, Gregory A.
Fisher, Charles D.
Michel, Thierry
Zawadzki, Mark
Rignot, Eric
TI The Glacier and Land Ice Surface Topography Interferometer: An Airborne
Proof-of-Concept Demonstration of High-Precision Ka-Band Single-Pass
Elevation Mapping
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Ice; interferometry; radar
ID GREENLAND; ALTIMETRY; SHEETS; DESIGN; SYSTEM; RADAR
AB As part of the NASA International Polar Year activities, a Ka-band cross-track interferometric synthetic aperture radar (SAR) recently demonstrated high-precision elevation swath mapping capability. This proof-of-concept instrument was achieved by interfacing two Ka-band slotted-waveguide antennas in a cross-track geometry and Ka-band electronics with the Jet Propulsion Laboratory's L-band uninhabited aerial vehicle SAR. Deployed on the NASA Gulfstream III, initial engineering flights in March and April 2009 marked the first airborne demonstration of single-pass cross-track interferometry at Ka-band. Results of a preliminary interferometric assessment indicate height precisions that, for a 3 m x 3 m posting, range from 30 cm in the near range to 3 m in the far range and greater than 5 km of swath over the urban areas imaged. The engineering flights were followed by a comprehensive campaign to Greenland in May 2009 for ice-surface topography mapping assessment. Toward that end, coordinated flights with the NASA Wallops Airborne Topographic Mapper lidar were conducted in addition to establishing ground calibration sites at both the Summit Station of the National Science Foundation and the Swiss Camp of the Cooperative Institute for Research in the Environmental Sciences. Comparisons of the radar-derived elevation measurements with both in situ and lidar data are planned for a subsequent paper; however, at this stage, a single data example over rugged ice cover produced a swath up to 7 km with the desired height precision as estimated from interferometric correlation data. While a systematic calibration, including assessment and modeling of biases, due to penetration of the electromagnetic waves into the snow cover has not yet been addressed, these initial results indicate that we will exceed our system requirements.
C1 [Moller, Delwyn] Remote Sensing Solut Inc, Barnstable, MA 02630 USA.
[Hensley, Scott; Sadowy, Gregory A.; Fisher, Charles D.; Michel, Thierry; Zawadzki, Mark; Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
RP Moller, D (reprint author), Remote Sensing Solut Inc, Barnstable, MA 02630 USA.
EM dkmoller@remotesensingsolutions.com
RI Rignot, Eric/A-4560-2014
OI Rignot, Eric/0000-0002-3366-0481
FU National Aeronautics and Space Administration
FX Manuscript received February 8, 2010; revised May 12, 2010; accepted
June 26, 2010. Date of publication September 2, 2010; date of current
version January 21, 2011. The research described in this paper was
conducted at the Jet Propulsion Laboratory under a contract with the
National Aeronautics and Space Administration.
NR 19
TC 12
Z9 13
U1 3
U2 15
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD FEB
PY 2011
VL 49
IS 2
BP 827
EP 842
DI 10.1109/TGRS.2010.2057254
PG 16
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 710LY
UT WOS:000286514400021
ER
PT J
AU Bala, G
Gopalakrishnan, R
Jayaraman, M
Nemani, R
Ravindranath, NH
AF Bala, Govindasamy
Gopalakrishnan, Ranjith
Jayaraman, Mathangi
Nemani, Ramakrishna
Ravindranath, N. H.
TI CO2-fertilization and potential future terrestrial carbon uptake in
India
SO MITIGATION AND ADAPTATION STRATEGIES FOR GLOBAL CHANGE
LA English
DT Article
DE Carbon sequestration; Climate change; CO2 fertilization; Forests;
Potential vegetation; Terrestrial carbon cycle model
ID CLIMATE-CHANGE; GLOBAL CLIMATE; COUPLED CLIMATE; VEGETATION DYNAMICS;
CO2 CONCENTRATIONS; CYCLE FEEDBACK; MODEL; ECOSYSTEM; BALANCE;
TEMPERATURE
AB There is huge knowledge gap in our understanding of many terrestrial carbon cycle processes. In this paper, we investigate the bounds on terrestrial carbon uptake over India that arises solely due to CO (2) -fertilization. For this purpose, we use a terrestrial carbon cycle model and consider two extreme scenarios: unlimited CO2-fertilization is allowed for the terrestrial vegetation with CO2 concentration level at 735 ppm in one case, and CO2-fertilization is capped at year 1975 levels for another simulation. Our simulations show that, under equilibrium conditions, modeled carbon stocks in natural potential vegetation increase by 17 Gt-C with unlimited fertilization for CO2 levels and climate change corresponding to the end of 21st century but they decline by 5.5 Gt-C if fertilization is limited at 1975 levels of CO2 concentration. The carbon stock changes are dominated by forests. The area covered by natural potential forests increases by about 36% in the unlimited fertilization case but decreases by 15% in the fertilization-capped case. Thus, the assumption regarding CO2-fertilization has the potential to alter the sign of terrestrial carbon uptake over India. Our model simulations also imply that the maximum potential terrestrial sequestration over India, under equilibrium conditions and best case scenario of unlimited CO2-fertilization, is only 18% of the 21st century SRES A2 scenarios emissions from India. The limited uptake potential of the natural potential vegetation suggests that reduction of CO2 emissions and afforestation programs should be top priorities.
C1 [Bala, Govindasamy] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
[Gopalakrishnan, Ranjith; Jayaraman, Mathangi; Ravindranath, N. H.] Indian Inst Sci, Ctr Sustainable Technol, Bangalore 560012, Karnataka, India.
[Nemani, Ramakrishna] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bala, Govindasamy] Indian Inst Sci, Divecha Ctr Climate Change, Bangalore 560012, Karnataka, India.
RP Bala, G (reprint author), Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
EM gbala@caos.iisc.ernet.in
FU Royal Norwegian Embassy; CICERO, Oslo
FX Research for this publication was conducted under the project "Impact of
climate change on tropical forest ecosystems and biodiversity in India",
funded by the Royal Norwegian Embassy, in collaboration with CICERO,
Oslo. We thank the Royal Norwegian Embassy and CICERO for their support.
We thank Dr. Devaraju for his help in making the schematic diagram for
this paper.
NR 35
TC 2
Z9 2
U1 1
U2 10
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1381-2386
J9 MITIG ADAPT STRAT GL
JI Mitig. Adapt. Strateg. Glob. Chang.
PD FEB
PY 2011
VL 16
IS 2
SI SI
BP 143
EP 160
DI 10.1007/s11027-010-9260-z
PG 18
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 712OG
UT WOS:000286675500003
ER
PT J
AU Mikellides, IG
Tassis, K
Yorke, HW
AF Mikellides, I. G.
Tassis, K.
Yorke, H. W.
TI 2D Magnetohydrodynamics simulations of induced plasma dynamics in the
near-core region of a galaxy cluster
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE MHD; galaxies: clusters: intracluster medium
ID ACTIVE GALACTIC NUCLEI; ANISOTROPIC THERMAL CONDUCTION; FUSION
PROPULSION SYSTEM; TANGLED MAGNETIC-FIELDS; HEATING-COOLING FLOWS;
FLUX-LIMITED SAMPLE; X-RAY-EMISSION; INTRACLUSTER MEDIUM; AGN FEEDBACK;
FARADAY-ROTATION
AB The mechanisms that maintain thermal balance in the intracluster medium (ICM) and produce the observed spatial distribution of the plasma density and temperature in galaxy clusters remain a subject of debate. We present results from numerical simulations of the cooling-core cluster A2199 produced by the 2D resistive magnetohydrodynamics (MHD) code MACH2. In our simulations we explore the effect of anisotropic thermal conduction on the energy balance of the system. The results from idealized cases in 2D axisymmetric geometry underscore the importance of the initial plasma density in ICM simulations, especially the near-core values since the radiation cooling rate is proportional to ne 2. Heat conduction is found to be non-effective in preventing catastrophic cooling in this cluster. In addition we performed 2D planar MHD simulations starting from initial conditions deliberately violating both thermal balance and hydrostatic equilibrium in the ICM, to assess contributions of the convective terms in the energy balance of the system against anisotropic thermal conduction. We find that in this case work done by the pressure on the plasma can dominate the early evolution of the internal energy over anisotropic thermal conduction in the presence of subsonic flows, thereby reducing the impact of the magnetic field. Deviations from hydrostatic equilibrium near the cluster core may be associated with transient activity of a central active galactic nucleus and/or remnant dynamical activity in the ICM and warrant further study in three dimensions.
C1 [Mikellides, I. G.; Tassis, K.; Yorke, H. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mikellides, IG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ioannis.G.Mikellides@jpl.nasa.gov
RI Tassis, Konstantinos/C-3155-2011;
OI Tassis, Konstantinos/0000-0002-8831-2038
FU National Aeronautics and Space Administration
FX The authors wish to thank Jeremiah Ostriker and Matt Kunz for their
useful comments. We are also grateful to Moustafa T. Chahine for his
support through the Innovative Spontaneous Concepts Research and
Technology Program. This work was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration, and made extensive
use of the NASA Astrophysics Data System and arXiv.org preprint server.
NR 121
TC 5
Z9 5
U1 1
U2 2
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 FEB
PY 2011
VL 410
IS 4
BP 2602
EP 2616
DI 10.1111/j.1365-2966.2010.17635.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706IG
UT WOS:000286211000044
ER
PT J
AU Bautista, MA
Melendez, M
Hartman, H
Gull, TR
Lodders, K
AF Bautista, M. A.
Melendez, M.
Hartman, H.
Gull, T. R.
Lodders, K.
TI The abundance of iron-peak elements and the dust composition in eta
Carinae: manganese
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE atomic data; atomic processes; line: formation; stars: abundances;
stars: individual: eta Carinae; ISM: atoms
ID STRONTIUM FILAMENT; MN-II; NI-II; LIFETIME MEASUREMENTS; HOMUNCULUS
NEBULA; GASEOUS NEBULAE; ULTRAVIOLET; LINES; EXCITATION; EMISSION
AB We study the chemical abundances of the strontium filament found in the ejecta of eta Carinae. In particular, we derive the abundances of iron-peak elements from the spectra of their singly ionized ions present in the optical/infrared (IR) spectra. In this paper we analyse the spectrum of Mn II using a new non-local thermodynamic equilibrium (non-LTE) model for this system. In constructing this models we carried out theoretical calculations of radiative transition rates and electron impact excitation rate coefficients. We find that relative to Ni the gas-phase abundance ratio of Mn is roughly solar, similar to the Cr abundance but in contrast to the large enhancements in the abundances of Sc and Ti. We interpret this result as an indication of non-equilibrium condensation in the ejecta of eta Carinae.
C1 [Bautista, M. A.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Melendez, M.; Gull, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Melendez, M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hartman, H.] Lund Univ, Lund Observ, SE-22100 Lund, Sweden.
[Lodders, K.] Washington Univ, Dept Earth & Planetary Sci, Planetary Chem Lab, St Louis, MO 63130 USA.
[Lodders, K.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
RP Bautista, MA (reprint author), Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
EM manuel.bautista@wmich.edu
RI Gull, Theodore/D-2753-2012; Hartman, Henrik/K-3113-2013
OI Gull, Theodore/0000-0002-6851-5380;
FU NASA [NNX09AB99G, NAS 5-26555]; Space Telescope Science Institute
[GO-11745]; Swedish Research Council (VR); National Science Foundation
[AST 0807356]
FX MAB acknowledges financial support from grants from the NASA Astronomy
and Physics Research and Analysis Programme (award NNX09AB99G) and the
Space Telescope Science Institute (project GO-11745). HH acknowledge
support from the Swedish Research Council (VR). Based on observations
made with the NASA/ESA Hubble Space Telescope, obtained (from the Data
Archive) at the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-26555. These observations are associated with
programmes 8036, 8327, 8483, 8619 and 9420. Work by KL was supported by
the National Science Foundation grant AST 0807356 and while working at
the Foundation.
NR 38
TC 2
Z9 2
U1 0
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 FEB
PY 2011
VL 410
IS 4
BP 2643
EP 2652
DI 10.1111/j.1365-2966.2010.17642.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706IG
UT WOS:000286211000047
ER
PT J
AU Adamczak, AD
Spriggs, AA
Fitch, DM
Burke, C
Shin, EE
Grunlan, JC
AF Adamczak, Andrea D.
Spriggs, Adam A.
Fitch, Danielle M.
Burke, Chris
Shin, Eugene E.
Grunlan, Jaime C.
TI Blistering in Carbon-Fiber-Filled Fluorinated Polyimide
SO POLYMER COMPOSITES
LA English
DT Article
ID IMIDE OLIGOMER; COMPOSITES; AFR-PEPA-4; STABILITY; MODEL
AB A blistering study was performed on a fluorinated polyimide resin and its carbon-fiber composite in an effort to determine the blister-formation temperature and the influence of blisters on composite performance. The fluorinated resin and carbon-fiber composite exhibit higher glass-transition (435-455 degrees C) and decomposition temperatures (above 520 degrees C) than similar polyimide resins and their carbon-fiber composites currently used. Two techniques were used to determine moisture-induced blister formation. A transverse extensometer with quartz lamps as a heating source measured thickness expansion, as did a thermomechanical analyzer as a function of temperature. Both methods successfully measured the onset of blister formation with varying amounts of absorbed moisture (up to 3 wt%) in the samples. The polyimide resin exhibited blister temperatures ranging from 225 to 362 degrees C, with 1.7-3.0 wt% absorbed moisture, and the polyimide composite had blister temperatures from 246 to 294 degrees C with 0.5-1.5 wt% moisture. The blistering effects of the polyimide composites were found to have little correlation with modulus. POLYM. COMPOS., 32:185-192, 2011. (C) 2010 Society of Plastics Engineers
C1 [Adamczak, Andrea D.; Spriggs, Adam A.; Fitch, Danielle M.; Grunlan, Jaime C.] Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA.
[Burke, Chris; Shin, Eugene E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Grunlan, JC (reprint author), Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA.
EM jgrunlan@tamu.edu
RI Grunlan, Jaime/K-3242-2016
OI Grunlan, Jaime/0000-0001-5241-9741
FU Air Force Office of Scientific Research [FA 9550-04-1-0137]
FX Contract grant sponsor: Air Force Office of Scientific Research;
contract grant number: FA 9550-04-1-0137.
NR 24
TC 0
Z9 5
U1 1
U2 9
PU JOHN WILEY & SONS INC
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0272-8397
J9 POLYM COMPOSITE
JI Polym. Compos.
PD FEB
PY 2011
VL 32
IS 2
BP 185
EP 192
DI 10.1002/pc.21029
PG 8
WC Materials Science, Composites; Polymer Science
SC Materials Science; Polymer Science
GA 711BW
UT WOS:000286561700004
ER
PT J
AU Bhaduri, K
Stefanski, MD
Srivastava, AN
AF Bhaduri, Kanishka
Stefanski, Mark D.
Srivastava, Ashok N.
TI Privacy-Preserving Outlier Detection Through Random Nonlinear Data
Distortion
SO IEEE TRANSACTIONS ON SYSTEMS MAN AND CYBERNETICS PART B-CYBERNETICS
LA English
DT Article
DE Data mining; non-linear; perturbation; privacy-preserving
ID ALGORITHMS
AB Consider a scenario in which the data owner has some private or sensitive data and wants a data miner to access them for studying important patterns without revealing the sensitive information. Privacy-preserving data mining aims to solve this problem by randomly transforming the data prior to their release to the data miners. Previous works only considered the case of linear data perturbations-additive, multiplicative, or a combination of both-for studying the usefulness of the perturbed output. In this paper, we discuss nonlinear data distortion using potentially nonlinear random data transformation and show how it can be useful for privacy-preserving anomaly detection from sensitive data sets. We develop bounds on the expected accuracy of the nonlinear distortion and also quantify privacy by using standard definitions. The highlight of this approach is to allow a user to control the amount of privacy by varying the degree of nonlinearity. We show how our general transformation can be used for anomaly detection in practice for two specific problem instances: a linear model and a popular nonlinear model using the sigmoid function. We also analyze the proposed nonlinear transformation in full generality and then show that, for specific cases, it is distance preserving. A main contribution of this paper is the discussion between the invertibility of a transformation and privacy preservation and the application of these techniques to outlier detection. The experiments conducted on real-life data sets demonstrate the effectiveness of the approach.
C1 [Bhaduri, Kanishka] NASA, Miss Crit Technol Inc, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Stefanski, Mark D.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
RP Bhaduri, K (reprint author), NASA, Miss Crit Technol Inc, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Kanishka.Bhaduri-1@nasa.gov; mark.d.stefanski@gmail.com;
Ashok.N.Srivastava@nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX Manuscript received July 8, 2009; revised March 10, 2010; accepted May
22, 2010. Date of publication June 28, 2010; date of current version
January 14, 2011. This work was supported by the National Aeronautics
and Space Administration (NASA) Aviation Safety Program, Integrated
Vehicle Health Management Project. This paper was recommended by
Associate Editor B. Sick.
NR 33
TC 2
Z9 2
U1 1
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1083-4419
J9 IEEE T SYST MAN CY B
JI IEEE Trans. Syst. Man Cybern. Part B-Cybern.
PD FEB
PY 2011
VL 41
IS 1
BP 260
EP 272
DI 10.1109/TSMCB.2010.2051540
PG 13
WC Automation & Control Systems; Computer Science, Artificial Intelligence;
Computer Science, Cybernetics
SC Automation & Control Systems; Computer Science
GA 708TX
UT WOS:000286388300021
PM 20595089
ER
PT J
AU Guo, HQ
Meador, MAB
McCorkle, L
Quade, DJ
Guo, JA
Hamilton, B
Cakmak, M
Sprowl, G
AF Guo, Haiquan
Meador, Mary Ann B.
McCorkle, Linda
Quade, Derek J.
Guo, Jiao
Hamilton, Bart
Cakmak, Miko
Sprowl, Guilherme
TI Polyimide Aerogels Cross-Linked through Amine Functionalized
Polyoligomeric Silsesquioxane
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE aerogels; polyimides; polyoligomeric silsesquioxane; mesoporous
ID STRUCTURE-PROPERTY RELATIONSHIPS; POROUS 3D NANOSTRUCTURES; SILICA
AEROGELS; MECHANICAL-PROPERTIES; THERMAL-CONDUCTIVITY; IMIDE OLIGOMERS;
POSS; NANOCOMPOSITES; POLYSTYRENE
AB We report the first synthesis of polyimide aerogels cross-linked through a polyhedral oligomeric silsesquioxane, octa(aminophenyl)silsesquioxane (OAPS). Gels formed from polyamic acid solutions of 3,3',4,4'-biphenyltetracarboxylic dianhydride (BPDA), bisaniline-p-xylidene (BAX) and OAPS were chemically imidized and dried using supercritical CO(2) extraction to give aerogels having density around 0.1 g/cm(3). The aerogels are greater than 90 % porous, have high surface areas (230 to 280 m(2)/g) and low thermal conductivity (14 mW/m-K at room temperature). Notably, the polyimide aerogels cross-linked with OAPS have higher modulus than polymer reinforced silica aerogels of similar density and can be fabricated as both monoliths and thin films. Thin films of the aerogel are flexible and foldable making them an ideal insulation for space suits, and inflatable structures for habitats or decelerators for planetary re-entry, as well as more down to earth applications.
C1 [Guo, Haiquan; McCorkle, Linda] Ohio Aerosp Inst, Cleveland, OH USA.
[Meador, Mary Ann B.; Quade, Derek J.; Sprowl, Guilherme] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Guo, Jiao; Hamilton, Bart; Cakmak, Miko] Univ Akron, Natl Polymer Innovat Ctr, Akron, OH 44325 USA.
RP Guo, HQ (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH USA.
EM haiquan.n.guo@nasa.gov; maryann.meador@nasa.gov
OI Meador, Mary Ann/0000-0003-2513-7372
FU Fundamental Aeronautics Program (Hypersonics); Interdisciplinary
National Science Program Incorporating Research and Education Experience
(INSPIRE)
FX We gratefully acknowledge support from the Fundamental Aeronautics
Program (Hypersonics). G.S. thanks the Interdisciplinary National
Science Program Incorporating Research and Education Experience
(INSPIRE) Project for support through a summer internship. We also thank
Jozef Gembarovic from the Thermophysical Properties Research Lab, Inc.
(TPRL), for measurement of thermal conductivity; Daniel Scheiman, ASRC,
for carrying out porosimetry and thermal analysis; and Anna Palczer for
nitrogen sorption experiments.
NR 38
TC 84
Z9 93
U1 30
U2 231
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD FEB
PY 2011
VL 3
IS 2
BP 546
EP 552
DI 10.1021/am101123h
PG 7
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA 725IW
UT WOS:000287639400062
PM 21294517
ER
PT J
AU Nissen, JA
Lipa, JA
Wang, S
Avaloff, D
Stricker, DA
AF Nissen, J. A.
Lipa, J. A.
Wang, S.
Avaloff, D.
Stricker, D. A.
TI Testing relativity with orbiting clocks
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Relativity; Time; Standard Model Extension
ID GENERAL-RELATIVITY
AB We describe the background and status of a superconducting microwave clock suitable for relativity experiments in earth orbit. The project has the capability of performing improved tests of Lorentz invariance via a Michelson-Morley type experiment, and setting new limits on nine parameters in the Standard Model Extension. If flown with a high stability atomic clock, a Kennedy-Thorndike experiment along with additional tests in general relativity could be performed.
In orbit, unwanted cavity frequency variations are expected to be caused mainly by acceleration effects due to residual drag and vibration, temperature variations, and fluctuations in the energy stored in the cavity. A cavity support system has been designed to reduce acceleration effects and a high resolution thermometer has been implemented to improve temperature control. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Nissen, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lipa, J. A.; Wang, S.; Avaloff, D.; Stricker, D. A.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
RP Nissen, JA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 171-331, Pasadena, CA 91109 USA.
EM joel.a.nissen@jpl.nasa.gov
NR 15
TC 1
Z9 1
U1 4
U2 9
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 FEB 1
PY 2011
VL 47
IS 3
BP 525
EP 527
DI 10.1016/j.asr.2010.08.001
PG 3
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 722HA
UT WOS:000287422000014
ER
PT J
AU Walker, SA
Tweed, J
Tripathi, RK
Badavi, FF
Miller, J
Zeitlin, C
Heilbronn, LH
AF Walker, S. A.
Tweed, J.
Tripathi, R. K.
Badavi, F. F.
Miller, J.
Zeitlin, C.
Heilbronn, L. H.
TI Validation of a multi-layer Green's function code for ion beam transport
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Radiation transport; Botlzmann equation; HZE ion transport; Green's
function solution
ID INTERNATIONAL-SPACE-STATION; MEV/NUCLEON FE-56; HZE PROPAGATION; TARGETS
AB To meet the challenge of future deep space programs, an accurate and efficient engineering code for analyzing the shielding requirements against high-energy galactic heavy ion radiation is needed. In consequence, a new version of the HZETRN code capable of simulating high charge and energy (HZE) ions with either laboratory or space boundary conditions is currently under development. This code, GRNTRN, is based on a Green's function approach to the solution of the one-dimensional Boltzmann transport equation and like its predecessor is deterministic in nature. The computational model consists of the lowest order asymptotic approximation followed by a Neumann series expansion with non-perturbative corrections. The physical description includes energy loss with straggling, nuclear attenuation, nuclear fragmentation with energy dispersion and down shift. Code validation in the laboratory environment is addressed by showing that GRNTRN accurately predicts energy loss spectra as measured by solid-state detectors in ion beam experiments with multi-layer targets. In order to verify and benchmark the code with space boundary conditions, measured particle fluxes are propagated through several thicknesses of shielding using both GRNTRN and the current version of HZETRN. The favorable agreement obtained indicates that GRNTRN accurately models the propagation of HZE ions in laboratory settings. It also compares very well with the extensively validated space environment HZETRN code and thus provides verification of the HZETRN propagator. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Walker, S. A.; Tweed, J.] Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA.
[Tripathi, R. K.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Badavi, F. F.] Christopher Newport Univ, Newport News, VA 23606 USA.
[Miller, J.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Zeitlin, C.] SW Res Inst, Boulder, CO 80302 USA.
[Heilbronn, L. H.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA.
RP Tweed, J (reprint author), Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA.
EM jtweed@odu.edu
RI Heilbronn, Lawrence/J-6998-2013
OI Heilbronn, Lawrence/0000-0002-8226-1057
NR 27
TC 1
Z9 1
U1 0
U2 3
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD FEB 1
PY 2011
VL 47
IS 3
BP 533
EP 544
DI 10.1016/j.asr.2010.09.012
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 722HA
UT WOS:000287422000016
ER
PT J
AU Crabbe, A
Schurr, MJ
Monsieurs, P
Morici, L
Schurr, J
Wilson, JW
Ott, CM
Tsaprailis, G
Pierson, DL
Stefanyshyn-Piper, H
Nickerson, CA
AF Crabbe, Aurelie
Schurr, Michael J.
Monsieurs, Pieter
Morici, Lisa
Schurr, Jill
Wilson, James W.
Ott, C. Mark
Tsaprailis, George
Pierson, Duane L.
Stefanyshyn-Piper, Heidi
Nickerson, Cheryl A.
TI Transcriptional and Proteomic Responses of Pseudomonas aeruginosa PAO1
to Spaceflight Conditions Involve Hfq Regulation and Reveal a Role for
Oxygen
SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY
LA English
DT Article
ID SHEAR MODELED MICROGRAVITY; BACTERIAL GENE-EXPRESSION; MICROARRAY
ANALYSIS; MASS-SPECTROMETRY; PROTEIN DATABASE; EPITHELIAL-CELLS;
VIRULENCE; TYPHIMURIUM; RESISTANCE; TANDEM
AB Assessing bacterial behavior in microgravity is important for risk assessment and prevention of infectious diseases during spaceflight missions. Furthermore, this research field allows the unveiling of novel connections between low-fluid-shear regions encountered by pathogens during their natural infection process and bacterial virulence. This study is the first to characterize the spaceflight-induced global transcriptional and proteomic responses of Pseudomonas aeruginosa, an opportunistic pathogen that is present in the space habitat. P. aeruginosa responded to spaceflight conditions through differential regulation of 167 genes and 28 proteins, with Hfq as a global transcriptional regulator. Since Hfq was also differentially regulated in spaceflight-grown Salmonella enterica serovar Typhimurium, Hfq represents the first spaceflight-induced regulator acting across bacterial species. The major P. aeruginosa virulence-related genes induced in spaceflight were the lecA and lecB lectin genes and the gene for rhamnosyltransferase (rhlA), which is involved in rhamnolipid production. The transcriptional response of spaceflight-grown P. aeruginosa was compared with our previous data for this organism grown in microgravity analogue conditions using the rotating wall vessel (RWV) bioreactor. Interesting similarities were observed, including, among others, similarities with regard to Hfq regulation and oxygen metabolism. While RWV-grown P. aeruginosa mainly induced genes involved in microaerophilic metabolism, P. aeruginosa cultured in spaceflight presumably adopted an anaerobic mode of growth, in which denitrification was most prominent. Whether the observed changes in pathogenesis-related gene expression in response to spaceflight culture could lead to an alteration of virulence in P. aeruginosa remains to be determined and will be important for infectious disease risk assessment and prevention, both during spaceflight missions and for the general public.
C1 [Crabbe, Aurelie; Nickerson, Cheryl A.] Arizona State Univ, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ 85287 USA.
[Schurr, Michael J.] Univ Colorado, Sch Med, Aurora, CO USA.
[Monsieurs, Pieter] CEN SCK, Belgian Nucl Res Ctr, B-2400 Mol, Belgium.
[Wilson, James W.] Villanova Univ, Dept Biol, Villanova, PA 19085 USA.
[Ott, C. Mark; Pierson, Duane L.] NASA, Lyndon B Johnson Space Ctr, Habitabil & Environm Factors Div, Houston, TX 77058 USA.
[Stefanyshyn-Piper, Heidi] NASA, Lyndon B Johnson Space Ctr, Astronaut Off, Houston, TX 77058 USA.
[Morici, Lisa] Tulane Univ, Hlth Sci Ctr, New Orleans, LA 70118 USA.
[Tsaprailis, George] Univ Arizona, Ctr Toxicol, Tucson, AZ USA.
[Schurr, Jill] Affymetrix Inc, Santa Clara, CA USA.
RP Nickerson, CA (reprint author), Arizona State Univ, Biodesign Inst, Ctr Infect Dis & Vaccinol, 1001 S McAllister Ave, Tempe, AZ 85287 USA.
EM cheryl.nickerson@asu.edu
RI Monsieurs, Pieter/A-2917-2009
FU NASA [NCC2-1362]; Arizona Proteomics Consortium [ES06694]; NIH/NCI
[CA023074]; Institute of the University of Arizona [BIO5]
FX This work was supported by NASA grant NCC2-1362 to C.A.N., the Arizona
Proteomics Consortium (supported by NIEHS grant ES06694 to the SWEHSC),
NIH/NCI grant CA023074 to the AZCC, and the BIO5 Institute of the
University of Arizona.
NR 50
TC 38
Z9 41
U1 7
U2 31
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 FEB
PY 2011
VL 77
IS 4
BP 1221
EP 1230
DI 10.1128/AEM.01582-10
PG 10
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA 717WM
UT WOS:000287078100009
PM 21169425
ER
PT J
AU Jiang, NB
Webster, M
Lempert, WR
Miller, JD
Meyer, TR
Ivey, CB
Danehy, PM
AF Jiang, Naibo
Webster, Matthew
Lempert, Walter R.
Miller, Joseph D.
Meyer, Terrence R.
Ivey, Christopher B.
Danehy, Paul M.
TI MHz-rate nitric oxide planar laser-induced fluorescence imaging in a
Mach 10 hypersonic wind tunnel
SO APPLIED OPTICS
LA English
DT Article
ID STIMULATED BRILLOUIN-SCATTERING; OPTICAL PARAMETRIC OSCILLATOR;
PULSE-BURST LASER; HIGH-SPEED FLOW; REPETITION-RATE; TURBULENT FLAMES;
VISUALIZATION; OH; DIAGNOSTICS; MODES
AB Nitric oxide planar laser-induced fluorescence (NO PLIF) imaging at repetition rates as high as 1 MHz is demonstrated in the NASA Langley 31 in. Mach 10 hypersonic wind tunnel. Approximately 200 time-correlated image sequences of between 10 and 20 individual frames were obtained over eight days of wind tunnel testing spanning two entries in March and September of 2009. The image sequences presented were obtained from the boundary layer of a 20 degrees flat plate model, in which transition was induced using a variety of different shaped protuberances, including a cylinder and a triangle. The high-speed image sequences captured a variety of laminar and transitional flow phenomena, ranging from mostly laminar flow, typically at a lower Reynolds number and/or in the near wall region of the model, to highly transitional flow in which the temporal evolution and progression of characteristic streak instabilities and/or corkscrew-shaped vortices could be clearly identified. (C) 2010 Optical Society of America
C1 [Jiang, Naibo; Webster, Matthew; Lempert, Walter R.] Ohio State Univ, Dept Mech Engn, Columbus, OH 43201 USA.
[Jiang, Naibo; Webster, Matthew; Lempert, Walter R.] Ohio State Univ, Dept Chem, Columbus, OH 43201 USA.
[Miller, Joseph D.; Meyer, Terrence R.] Iowa State Univ, Dept Mech Engn, Ames, IA 50011 USA.
[Ivey, Christopher B.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Danehy, Paul M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Lempert, WR (reprint author), Ohio State Univ, Dept Mech Engn, 201 W 19th Ave, Columbus, OH 43201 USA.
EM lempert.1@osu.edu
RI Meyer, Terrence/F-1556-2011; Ivey, Christopher/I-8642-2012
OI Ivey, Christopher/0000-0003-0008-7532
NR 29
TC 34
Z9 34
U1 1
U2 14
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 FEB 1
PY 2011
VL 50
IS 4
BP A20
EP A28
DI 10.1364/AO.50.000A20
PG 9
WC Optics
SC Optics
GA 714JJ
UT WOS:000286805600004
PM 21283217
ER
PT J
AU Dumas, G
Schinnerer, E
Tabatabaei, FS
Beck, R
Velusamy, T
Murphy, E
AF Dumas, G.
Schinnerer, E.
Tabatabaei, F. S.
Beck, R.
Velusamy, T.
Murphy, E.
TI THE LOCAL RADIO-IR RELATION IN M51
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M51a, NGC5194); galaxies: ISM; infrared: galaxies;
radio continuum: galaxies
ID SPECTRAL ENERGY-DISTRIBUTION; SPITZER-SPACE-TELESCOPE; FAR-INFRARED
EMISSION; STAR-FORMING GALAXIES; SPIRAL GALAXIES; NEARBY GALAXIES; DISK
GALAXIES; STARBURST GALAXIES; CONTINUUM SURVEY; NGC-5194 M51A
AB We observed M51 at three frequencies, 1.4 GHz (20 cm), 4.9 GHz (6 cm), and 8.4 GHz (3.6 cm), with the Very Large Array and the Effelsberg 100 m telescope to obtain the highest quality radio continuum images of a nearby spiral galaxy. These radio data were combined with deconvolved Spitzer IRAC 8 mu m and MIPS 24 mu m images to search for and investigate local changes in the radio-IR correlation. Utilizing wavelet decomposition, we compare the distribution of the radio and IR emission on spatial scales between 200 pc and 30 kpc. We show that the radio-IR correlation is not uniform across the galactic disk. It presents a complex behavior with local extrema corresponding to various galactic structures, such as complexes of H II regions, spiral arms, and interarm filaments, indicating that the contribution of the thermal and non-thermal radio emission is a strong function of environment. In particular, the relation of the 24 mu m and 20 cm emission presents a linear relation within the spiral arms and globally over the galaxy, while it deviates from linearity in the interarm and outer regions as well in the inner region, with two different behaviors: it is sublinear in the interarm and outer region and overlinear in the central 3.5 kpc. Our analysis suggests that the changes in the radio/IR correlation reflect variations of interstellar medium properties between spiral arms and interarm region. The good correlation in the spiral arms implies that 24 mu m and 20 cm are tracing recent star formation, while a change in the dust opacity, "Cirrus" contribution to the IR emission and/or the relation between the magnetic field strength and the gas density can explain the different relations found in the interarm, outer, and inner regions.
C1 [Dumas, G.; Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Tabatabaei, F. S.; Beck, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Velusamy, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Murphy, E.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Dumas, G (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
OI Schinnerer, Eva/0000-0002-3933-7677
FU National Aeronautics and Space Administration; DFG [SCH 53614-1, SCH
53614-2, SPP 1177]
FX The authors thank Daniela Calzetti for providing the H alpha image. We
are also thankful to A. Fletcher, R. Kennicutt, and U. Lisenfeld for
very fruitful discussions and to the anonymous referee for useful
comments and suggestions that helped to improve this paper. This work is
partly based on observations made with the Spitzer Space Telescope,
which is operated by NASA/JPL/Caltech, on observations with the 100 m
telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at
Effelsberg and on observations made with the NRAO Very Large Array. The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. Part of this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. G. D.
was supported by DFG grants SCH 53614-1 and SCH 53614-2 as part of SPP
1177.
NR 53
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2011
VL 141
IS 2
AR 41
DI 10.1088/0004-6256/141/2/41
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706AW
UT WOS:000286186100013
ER
PT J
AU Snell, RL
Narayanan, G
Yun, MS
Heyer, M
Chung, A
Irvine, WM
Erickson, NR
Liu, GL
AF Snell, Ronald L.
Narayanan, Gopal
Yun, Min S.
Heyer, Mark
Chung, Aeree
Irvine, William M.
Erickson, Neal R.
Liu, Guilin
TI THE REDSHIFT SEARCH RECEIVER 3 mm WAVELENGTH SPECTRA OF 10 GALAXIES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: ISM; ISM: abundances; ISM: molecules; radio lines: galaxies
ID DENSE MOLECULAR GAS; ULTRALUMINOUS INFRARED GALAXIES; GALACTIC-CENTER;
INTERSTELLAR-MEDIUM; NEARBY GALAXIES; SAGITTARIUS B2; STAR-FORMATION;
LINE SURVEY; CHEMISTRY; CLOUDS
AB The 3 mm wavelength spectra of 10 galaxies have been obtained at the Five College Radio Astronomy Observatory using a new, very broadband receiver and spectrometer, called the Redshift Search Receiver (RSR). The RSR has an instantaneous bandwidth of 37 GHz covering frequencies from 74 to 111 GHz and has a spectral resolution of 31 MHz (similar to 100 km s(-1)). During tests of the RSR on the FCRAO 14 m telescope the complete 3 mm spectra of the central regions of NGC 253, Maffei 2, NGC 1068, IC 342, M82, NGC 3079, NGC 3690, NGC 4258, Arp 220, and NGC 6240 were obtained. Within the wavelength band covered by the RSR, 20 spectral lines from 14 different atomic and molecular species were detected. Based on simultaneous fits to the spectrum of each galaxy, a number of key molecular line ratios are derived. A simple model which assumes the emission arises from an ensemble of Milky Way like Giant Molecular Cloud cores can adequately fit the observed line ratios using molecular abundances based on Galactic molecular cloud cores. Variations seen in some line ratios, such as (CO)-C-13/HCN and HCO+/HCN, can be explained if the mean density of the molecular gas varies from galaxy to galaxy. However, NGC 3690, NGC 4258, and NGC 6240 show very large HCO+/HCN ratios and require significant abundance enhancement of HCO+ over HCN, possible due to the proximity to active galactic nucleus activity. Finally, the mass of dense molecular gas is estimated and we infer that 25%-85% of the total molecular gas in the central regions of these galaxies must have densities greater than 10(4) cm(-3).
C1 [Snell, Ronald L.; Narayanan, Gopal; Yun, Min S.; Heyer, Mark; Chung, Aeree; Irvine, William M.; Erickson, Neal R.; Liu, Guilin] Univ Massachusetts, Dept Astron, LGRT 619, Amherst, MA 01003 USA.
[Chung, Aeree] Harvard Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Irvine, William M.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
RP Snell, RL (reprint author), Univ Massachusetts, Dept Astron, LGRT 619, 710 N Pleasant St, Amherst, MA 01003 USA.
EM snell@astro.umass.edu; gopal@astro.umass.edu; myun@astro.umass.edu;
heyer@astro.umass.edu; achung@cfa.harvard.edu; irvine@astro.umass.edu;
neal@astro.umass.edu; gliu@astro.umass.edu
FU NSF [AST 0096854, AST 0704966, AST 0838222]; NASA [NNX09AH33A]
FX This work was supported by NSF grants AST 0096854, AST 0704966 and AST
0838222, and by NASA grant NNX09AH33A. We thank Hugh Crowl and Bing
Jiang who assisted in data collection and Lauren Harley who assisted in
some of the data reduction and spectral line fitting.
NR 57
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2011
VL 141
IS 2
AR 38
DI 10.1088/0004-6256/141/2/38
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706AW
UT WOS:000286186100010
ER
PT J
AU Walkowicz, LM
Basri, G
Batalha, N
Gilliland, RL
Jenkins, J
Borucki, WJ
Koch, D
Caldwell, D
Dupree, AK
Latham, DW
Meibom, S
Howell, S
Brown, TM
Bryson, S
AF Walkowicz, Lucianne M.
Basri, Gibor
Batalha, Natalie
Gilliland, Ronald L.
Jenkins, Jon
Borucki, William J.
Koch, David
Caldwell, Doug
Dupree, Andrea K.
Latham, David W.
Meibom, Soeren
Howell, Steve
Brown, Timothy M.
Bryson, Steve
TI WHITE-LIGHT FLARES ON COOL STARS IN THE KEPLER QUARTER 1 DATA
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE stars: emission-line, Be; stars: flare; stars: low-mass
ID M-DWARFS; AD LEONIS; PHOTOMETRIC VARIABILITY; STELLAR FLARE;
SOLAR-FLARES; YZ-CMI; X-RAY; SUN; 1ST; PERFORMANCE
AB We present the results of a search for white-light flares on similar to 23,000 cool dwarfs in the Kepler Quarter 1 long cadence data. We have identified 373 flaring stars, some of which flare multiple times during the observation period. We calculate relative flare energies, flare rates, and durations and compare these with the quiescent photometric variability of our sample. We find that M dwarfs tend to flare more frequently but for shorter durations than K dwarfs and that they emit more energy relative to their quiescent luminosity in a given flare than K dwarfs. Stars that are more photometrically variable in quiescence tend to emit relatively more energy during flares, but variability is only weakly correlated with flare frequency. We estimate distances for our sample of flare stars and find that the flaring fraction agrees well with other observations of flare statistics for stars within 300 pc above the Galactic plane. These observations provide a more rounded view of stellar flares by sampling stars that have not been pre-selected by their activity, and are informative for understanding the influence of these flares on planetary habitability.
C1 [Walkowicz, Lucianne M.; Basri, Gibor] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Batalha, Natalie; Jenkins, Jon; Borucki, William J.; Koch, David; Caldwell, Doug; Bryson, Steve] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Dupree, Andrea K.; Latham, David W.; Meibom, Soeren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Howell, Steve] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
RP Walkowicz, LM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
RI Caldwell, Douglas/L-7911-2014
OI Caldwell, Douglas/0000-0003-1963-9616
FU Kepler Fellowship for the Study of Planet-Bearing Stars; NASA's Science
Mission Directorate
FX L.M.W. is grateful for the support of the Kepler Fellowship for the
Study of Planet-Bearing Stars. Funding for this Discovery mission is
provided by NASA's Science Mission Directorate.
NR 35
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2011
VL 141
IS 2
AR 50
DI 10.1088/0004-6256/141/2/50
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706AW
UT WOS:000286186100022
ER
PT J
AU Xia, LF
Malhotra, S
Rhoads, J
Pirzkal, N
Zheng, ZY
Meurer, G
Straughn, A
Grogin, N
Floyd, D
AF Xia, Lifang
Malhotra, Sangeeta
Rhoads, James
Pirzkal, Norbert
Zheng, Zhenya
Meurer, Gerhardt
Straughn, Amber
Grogin, Norman
Floyd, David
TI SPECTROSCOPIC STUDY OF THE HST/ACS PEARS EMISSION-LINE GALAXIES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: star formation; quasars: emission lines; techniques:
spectroscopic
ID ORIGINS DEEP SURVEY; GOODS-SOUTH FIELD; VLT/FORS2 SPECTROSCOPY;
EVOLUTION; OBJECTS
AB We present spectroscopy of 76 emission-line galaxies (ELGs) in Chandra Deep Field South taken with the LDSS3 spectrograph on the Magellan Telescope. These galaxies are selected because they have emission lines with the Advanced Camera for Surveys (ACS) grism data in the Hubble Space Telescope Probing Evolution and Reionization Spectroscopically (PEARS) grism Survey. The ACS grism spectra cover the wavelength range 6000-9700 angstrom and most PEARS grism redshifts are based on a single emission line + photometric redshifts from broadband colors; the Magellan spectra cover a wavelength range from 4000 angstrom to 9000 angstrom and provide a check on redshifts derived from PEARS data. We find an accuracy of sigma(z) = 0.006 for the ACS grism redshifts with only one catastrophic outlier. We probe for active galactic nuclei (AGNs) in our sample via several different methods. In total, we find 7 AGNs and AGN candidates out of 76 galaxies. Two AGNs are identified from the X-ray full-band luminosity, L-X-ray,L- FB > 10(43) erg s(-1), the line widths, and the power-law continuum spectra. Two unobscured faint AGN candidates are identified from the X-ray full-band luminosity L-X-ray,L-FB similar to 10(41) erg s(-1), the hardness ratio and the column density, and the emission-line and X-ray derived SFRs. Two candidates are classified based on the line ratio of [N II]lambda 6584/H alpha versus [O III]lambda 5007/H beta(BPT diagram), which are between the empirical and theoretical demarcation curves, i.e., the transition region from star-forming galaxies to AGNs. One AGN candidate is identified from the high-ionization emission line He II angstrom 4686.
C1 [Xia, Lifang; Malhotra, Sangeeta; Rhoads, James; Zheng, Zhenya] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Pirzkal, Norbert; Grogin, Norman] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Zheng, Zhenya] Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Peoples R China.
[Meurer, Gerhardt] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Straughn, Amber] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Floyd, David] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia.
RP Xia, LF (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM lifang.xia@asu.edu; npirzkal@stsci.edu; zhengzy@mail.ustc.edu.cn;
meurer@pha.jhu.edu; amber.straughn@asu.edu; nagrogin@stsci.edu;
dfloyd@unimel.edu.au
FU NASA through Space Telescope Science Institute [NASA5-26555]; HST
[10530]
FX This paper includes data gathered with the 6.5 m Magellan Telescopes
located at Las Campanas Observatory, Chile. PEARS is an HST Treasury
Program 10530 (PI: S. Malhotra). Support for program was provided by
NASA through a grant from the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NASA5-26555 and is supported by HST
grant 10530.
NR 13
TC 13
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2011
VL 141
IS 2
AR 64
DI 10.1088/0004-6256/141/2/64
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706AW
UT WOS:000286186100036
ER
PT J
AU Butters, OW
Norton, AJ
Mukai, K
Tomsick, JA
AF Butters, O. W.
Norton, A. J.
Mukai, K.
Tomsick, J. A.
TI RXTE and XMM observations of intermediate polar candidates
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE binaries: general; X-rays: binaries; novae, cataclysmic variables
ID FAINT CATACLYSMIC VARIABLES; PHOTON IMAGING CAMERA; HIGH-SPEED
PHOTOMETRY; CHANDRA LOCALIZATIONS; INTEGRAL SOURCES; GALACTIC PLANE;
SPECTROSCOPY; NOVA; CONFIRMATION; OPHIUCHI
AB Aims. We aim to determine the credentials of nine candidate intermediate polars in order to confirm whether or not they are magnetic cataclysmic variables.
Methods. Frequency analysis of RXTE and XMM data was used to search for temporal variations that could be associated with the spin period of the magnetic white dwarf. X-ray spectral analysis was carried out to characterize the emission and absorption properties of each target.
Results. The hard X-ray light curve of V2069 Cyg shows a pulse period of 743.2 s, and its spectrum is fit by an absorbed bremsstrahlung model with an iron line, confirming this to be a genuine intermediate polar. The hard X-ray light curve of the previously confirmed intermediate polar IGR J00234+6141 is shown to be consistent with the previous low-energy X-ray detection of a 563.5 s pulse period. The likely polar IGR J14536-5522 shows no coherent modulation at the previously identified period of 3.1 h, but does exhibit a clear signal at periods likely to be harmonically related to it. Whilst our RXTE observations of RX J0153.3+7447, Swift J061223.0+701243.9, V436 Car, and DD Cir are largely too faint to give any definitive results, the observations of IGR J16167-4957 and V2487 Oph show some characteristics of intermediate polars, and these objects remain good candidates.
Conclusions. We confirmed one new hard X-ray selected intermediate polar from our sample, V2069 Cyg.
C1 [Butters, O. W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Norton, A. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Mukai, K.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
[Mukai, K.] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA.
[Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Butters, OW (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM oliver.butters@star.le.ac.uk
OI Norton, Andrew/0000-0001-7619-8269; Butters, Olly/0000-0003-0354-8461
NR 41
TC 4
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U1 0
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2011
VL 526
AR A77
DI 10.1051/0004-6361/201015848
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 709RF
UT WOS:000286458400089
ER
PT J
AU Del Zanna, G
Mitra-Kraev, U
Bradshaw, SJ
Mason, HE
Asai, A
AF Del Zanna, G.
Mitra-Kraev, U.
Bradshaw, S. J.
Mason, H. E.
Asai, A.
TI The 22 May 2007 B-class flare: new insights from Hinode observations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: spectroscopic; Sun: flares
ID BENCHMARKING ATOMIC DATA; ELECTRON-IMPACT EXCITATION; LOOP RADIATIVE
HYDRODYNAMICS; X-RAY TELESCOPE; SOLAR-FLARES; CHROMOSPHERIC EVAPORATION;
IMAGING SPECTROMETER; IRON PROJECT; NUMERICAL SIMULATIONS; TRANSITION
REGION
AB We present multi-wavelength observations of a small B-class flare which occurred on the Sun on 2007 May 22. The observations include data from Hinode, GOES, TRACE and the Nobeyama Radioheliograph. We obtained spatially and spectrally-resolved information from the Hinode EUV Imaging Spectrometer (EIS) during this event. The temporal and temperature coverage of the EIS observations provides new insights into our understanding of chromospheric evaporation and cooling. The flare showed many "typical" features, such as brightenings in the ribbons, hot (10 MK) loop emission and subsequent cooling. We also observed a new feature, strong (up to 170 km s(-1)) blue-shifted emission in lines formed around 2-3 MK, located at the footpoints of the 10 MK coronal emission and within the ribbons. Electron densities at 2 MK in the kernels are high, of the order of 10(11) cm(-3), suggesting a very narrow layer where the chromospheric evaporation occurs. We have run a non-equilibrium hydrodynamic numerical simulation using the HYDRAD code to study the cooling of the 10 MK plasma, finding good agreement between the predicted and observed temperatures, densities and ion populations. Line blending for some potentially useful diagnostic lines for flares, which are observed with Hinode/EIS, is also discussed.
C1 [Del Zanna, G.; Mitra-Kraev, U.; Mason, H. E.] DAMTP, 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 Computat & Data Sci, Fairfax, VA 22030 USA.
[Bradshaw, S. J.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
[Asai, A.] Natl Astron Observ Japan, Nobeyama Solar Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan.
[Asai, A.] Kyoto Univ, Unit Synerget Studies Space, Kyoto 6078471, Japan.
RP Del Zanna, G (reprint author), DAMTP, Ctr Math Sci, Wilberforce Rd, Cambridge CB3 0WA, England.
EM g.del-zanna@damtp.cam.ac.uk
FU STFC
FX Support from STFC is acknowledged. 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). We acknowledge
making extensive use of the Hinode data Centre Europe (Norway), and
using NoRH and TRACE data. We warmly thank C. Chifor. She was Hinode/EIS
Chief Observer between 21 May and 1 June 2007 when she visited the
JAXA/ISAS facilities in Japan. She coordinated the EIS observing plan
with the XRT and SOT observing plans and with other instruments. We
thank the anonymous referee for detailed and useful comments which
helped to improve the manuscript.
NR 61
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2011
VL 526
AR A1
DI 10.1051/0004-6361/201014906
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 709RF
UT WOS:000286458400013
ER
PT J
AU Malespin, C
Ballance, CP
Pindzola, MS
Witthoeft, MC
Kallman, TR
Loch, SD
AF Malespin, C.
Ballance, C. P.
Pindzola, M. S.
Witthoeft, M. C.
Kallman, T. R.
Loch, S. D.
TI Electron-impact excitation of H-like Cr, Mn, Fe, Co, and Ni for
applications in modeling X-ray astrophysical sources
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE atomic data; atomic processes; supernovae: general
ID SUPERNOVA REMNANT W49B; R-MATRIX APPROACH; ATOMIC IONS; COLLISION
STRENGTHS; RATE COEFFICIENTS; IA SUPERNOVAE; IRON PROJECT; EMISSION;
IONIZATION; XXVI
AB Context. Accurate atomic data for the less abundance Fe-peak elements are required for use in X-ray astrophysical studies.
Aims. We calculate high quality electron-impact excitation collision strengths and effective collision strengths for hydrogenic Cr, Mn, Fe, Co, and Ni.
Methods. We use the Dirac R-matrix method, the intermediate coupling frame transformation R-matrix method, the semi-relativistic distorted-wave method and the fully-relativistic distorted-wave method to calculate collision strengths for each of the ions. The ADAS collisional-radiative codes are used to produce photon emissivity coefficients for each ion.
Results. Results are presented for atomic energy levels, spontaneous emission coefficients, electron-impact excitation collision strengths and associated effective collision strengths for each of the five species under consideration. We find relativistic effects can contribute an approximate 10% increase to the background cross section in relation to semi-relativistic collision calculations. We also confirm that radiation damping plays a prominent role for certain near threshold resonances. In order check the integration of our results within collisional-radiative modeling codes, we have used the ADAS package for some preliminary modeling of photon emissivities. The atomic data shall be made available online through the OPEN-ADAS site and the CFADC database
C1 [Malespin, C.; Witthoeft, M. C.; Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ballance, C. P.; Pindzola, M. S.; Loch, S. D.] Auburn Univ, Auburn, AL 36849 USA.
RP Malespin, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Charles.A.Malespin@nasa.gov
RI Malespin, Charles/F-3445-2012
FU NASA ROSES ADAP [NNX10AD46G]
FX This work was supported by NASA ROSES ADAP grant NNX10AD46G. The
computational work was carried out on the Alabama supercomputer and on
the NERSC facilities in California. We would like to thank Una Hwang for
the many useful discussions and help that she provided throughout the
project.
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2011
VL 526
AR A115
DI 10.1051/0004-6361/201016132
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 709RF
UT WOS:000286458400127
ER
PT J
AU Micelotta, ER
Jones, AP
Tielens, AGGM
AF Micelotta, E. R.
Jones, A. P.
Tielens, A. G. G. M.
TI Polycyclic aromatic hydrocarbon processing by cosmic rays
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE dust, extinction; cosmic rays; galaxies: halos; galaxies: starburst;
ISM: jets and outflows; intergalactic medium
ID HYDROGENATED AMORPHOUS-CARBON; MOVING ELECTRIFIED PARTICLES; STARBURST
GALAXY M82; INTERSTELLAR-MEDIUM; GALACTIC WINDS; INTRACLUSTER MEDIUM;
SUPERNOVA-REMNANTS; RADIO OBSERVATIONS; IONIZATION RATE; STOPPING POWER
AB Context. Cosmic rays are present in almost all phases of the ISM. Polycyclic aromatic hydrocarbons (PAHs) and cosmic rays represent an abundant and ubiquitous component of the interstellar medium. However, the interaction between them has never before been fully investigated.
Aims. To study the effects of cosmic ray ion (H, He, CNO and Fe-Co-Ni) and electron bombardment of PAHs in galactic and extragalactic environments.
Methods. We calculate the nuclear and electronic interactions for collisions between PAHs and cosmic ray ions and electrons with energies between 5 MeV/nucleon and 10 GeV, above the threshold for carbon atom loss, in normal galaxies, starburst galaxies and cooling flow galaxy clusters.
Results. The timescale for PAH destruction by cosmic ray ions depends on the electronic excitation energy E-0 and on the amount of energy available for dissociation. Small PAHs are destroyed faster, with He and the CNO group being the more effective projectiles. For electron collisions, the lifetime is independent of the PAH size and varies with the threshold energy T-0.
Conclusions. Cosmic rays process the PAHs in diffuse clouds, where the destruction due to interstellar shocks is less efficient. In the hot gas filling galactic halos, outflows of starburst galaxies and intra-cluster medium, PAH destruction is dominated by collisions with thermal ions and electrons, but this mechanism is ineffective if the molecules are in denser cloudlets and isolated from the hot gas. Cosmic rays can access the denser clouds and together with X-rays will set the lifetime of those protected PAHs. This limits the use of PAHs as a "dye" for tracing the presence of cold entrained material.
C1 [Micelotta, E. R.; Tielens, A. G. G. M.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[Micelotta, E. R.; Jones, A. P.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Micelotta, E. R.; Jones, A. P.] CNRS, UMR 8617, F-91405 Orsay, France.
[Micelotta, E. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Micelotta, E. R.] CRESST, Greenbelt, MD 20771 USA.
[Micelotta, E. R.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Tielens, A. G. G. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Micelotta, ER (reprint author), Leiden Univ, Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands.
EM elisabetta.micelotta@nasa.gov
OI Micelotta, Elisabetta/0000-0002-6555-5109
FU EARA Training Network (EU) [MEST-CT-2004-504604]; ERC [246876]
FX We would like to thank the referee for careful reading and valuable
comments. We are grateful to F. Galliano for providing us with the
values of G0 in NGC 891 and to H. Leroux for useful
discussions on the physics of radiation damage in carbon materials.
E.R.M. thanks G. Lavaux for support and technical assistance and
acknowledges financial support by the EARA Training Network (EU grant
MEST-CT-2004-504604). Studies of interstellar PAHs at Leiden Observatory
are supported by the advanced-ERC grant 246876 on "The role of large
Polycyclic Aromatic Hydrocarbon molecules in the Universe".
NR 116
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2011
VL 526
AR A52
DI 10.1051/0004-6361/201015741
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 709RF
UT WOS:000286458400064
ER
PT J
AU Moehler, S
Dreizler, S
Lanz, T
Bono, G
Sweigart, AV
Calamida, A
Nonino, M
AF Moehler, S.
Dreizler, S.
Lanz, T.
Bono, G.
Sweigart, A. V.
Calamida, A.
Nonino, M.
TI The hot horizontal-branch stars in omega Centauri
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: horizontal-branch; stars: evolution; techniques: spectroscopic;
globular clusters: individual: NGC 5139
ID BLUE HOOK STARS; BLANKETED MODEL ATMOSPHERES; SPACE-TELESCOPE
OBSERVATIONS; DWARF COOLING CURVE; RED GIANT BRANCH; GLOBULAR-CLUSTERS;
MAIN-SEQUENCE; FLASHER SCENARIO; SPECTROSCOPIC ANALYSES; 2ND-GENERATION
STARS
AB Context. UV observations of some massive globular clusters have revealed a significant population of stars hotter and fainter than the hot end of the horizontal branch (HB), the so-called blue hook stars. This feature might be explained either by the late hot flasher scenario where stars experience the helium flash while on the white dwarf cooling curve or by the progeny of the helium-enriched sub-population postulated to exist in some clusters. Previous spectroscopic analyses of blue hook stars in omega Cen and NGC2808 support the late hot flasher scenario, but the stars contain much less helium than expected and the predicted C and N enrichment cannot be verified.
Aims. We compare the observed effective temperatures, surface gravities, helium abundances, and carbon line strengths (where detectable) of our targets stars with the predictions of the two aforementioned scenarios.
Methods. Moderately high resolution spectra of hot HB stars in the globular cluster omega Cen were analysed for radial velocity variations, atmospheric parameters, and abundances using LTE and non-LTE model atmospheres.
Results. We find no evidence of close binaries among our target stars. All stars below 30 000 K are helium-poor and very similar to HB stars observed in that temperature range in other globular clusters. In the temperature range 30 000 K to 50 000 K, we find that 28% of our stars are helium-poor (log He-n/H-n < -1.6), while 72% have roughly solar or super-solar helium abundance (log He-n/H-n >= -1.5). We also find that carbon enrichment is strongly correlated with helium enrichment, with a maximum carbon enrichment of 3% by mass.
Conclusions. A strong carbon enrichment in tandem with helium enrichment is predicted by the late hot flasher scenario, but not by the helium-enrichment scenario. We conclude that the helium-rich HB stars in omega Cen cannot be explained solely by the helium-enrichment scenario invoked to explain the blue main sequence.
C1 [Moehler, S.; Calamida, A.] European So Observ, D-85748 Garching, Germany.
[Dreizler, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Lanz, T.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bono, G.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Bono, G.; Calamida, A.] Rome Astron Observ, INAF, I-00040 Monte Porzio Catone, Italy.
[Sweigart, A. V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nonino, M.] Trieste Astron Observ, INAF, I-40131 Trieste, Italy.
RP Moehler, S (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM smoehler@eso.org; dreizler@astro.physik.uni-goettingen.de;
lanz@astro.umd.edu; bono@roma2.infn.it; Allen.V.Sweigart@nasa.gov;
acalamid@eso.org; nonino@ts.astro.it
FU Monte dei Paschi di Siena; PRIN-MIUR2007
FX We thank the staff at the Paranal observatory and at ESO Garching for
their excellent work, which made this paper possible. Two of us (GB, AC)
were partially supported by Monte dei Paschi di Siena (P.I.: S.
Degl'Innocenti) and by PRIN-MIUR2007 (P.I.: G. Piotto). This research
has made use of NASA's Astrophysics Data System. We thank the anonymous
referee for helpful comments.
NR 57
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2011
VL 526
AR A136
DI 10.1051/0004-6361/201015020
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 709RF
UT WOS:000286458400148
ER
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Allafort, A
Baldini, L
Ballet, J
Barbiellini, G
Baring, MG
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bouvier, A
Brandt, TJ
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Cannon, A
Caraveo, PA
Carrigan, S
Casandjian, JM
Cavazzuti, E
Cecchi, C
Celik, O
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cutini, S
Dermer, CD
de Palma, F
Silva, EDE
Drell, PS
Dubois, R
Dumora, D
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Frailis, M
Fuhrmann, L
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Guillemot, L
Guiriec, S
Hayashida, M
Hays, E
Horan, D
Hughes, RE
Johannesson, G
Johnson, AS
Johnson, WN
Kadler, M
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lee, SH
Lemoine-Goumard, M
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Makeev, A
Max-Moerbeck, W
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Naumann-Godo, M
Nishino, S
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Paneque, D
Panetta, JH
Parent, D
Pavlidou, V
Pearson, TJ
Pelassa, V
Pepe, M
Pesce-Rollins, M
Piron, F
Porter, TA
Raino, S
Rando, R
Razzano, M
Readhead, A
Reimer, A
Reimer, O
Richards, JL
Ripken, J
Ritz, S
Roth, M
Sadrozinski, HFW
Sanchez, D
Sander, A
Scargle, JD
Sgro, C
Siskind, EJ
Smith, PD
Spandre, G
Spinelli, P
Stawarz, L
Stevenson, M
Strickman, MS
Sokolovsky, KV
Suson, DJ
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JB
Thayer, JG
Thompson, DJ
Tibaldo, L
Torres, F
Tosti, G
Tramacere, A
Uchiyama, Y
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vilchez, N
Vitale, V
Waite, AP
Wang, P
Wehrle, AE
Winer, BL
Wood, KS
Yang, Z
Ylinen, T
Zensus, JA
Ziegler, M
Aleksic, J
Antonelli, LA
Antoranz, P
Backes, M
Barrio, JA
Gonzalez, JB
Bednarek, W
Berdyugin, A
Berger, K
Bernardini, E
Biland, A
Blanch, O
Bock, RK
Boller, A
Bonnoli, G
Bordas, P
Tridon, DB
Bosch-Ramon, V
Bose, D
Braun, I
Bretz, T
Camara, M
Carmona, E
Carosi, A
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Covino, S
Dazzi, F
de Angelis, A
del Pozo, ED
De Lotto, B
De Maria, M
De Sabata, F
Mendez, CD
Ortega, AD
Doert, M
Dominguez, A
Prester, DD
Dorner, D
Doro, M
Elsaesser, D
Ferenc, D
Fonseca, MV
Font, L
Lopen, RJG
Garczarczyk, M
Gaug, M
Giavitto, G
Godinovi, N
Hadasch, D
Herrero, A
Hildebrand, D
Hohne-Monch, D
Hose, J
Hrupec, D
Jogler, T
Klepser, S
Krahenbuhl, T
Kranich, D
Krause, J
La Barbera, A
Leonardo, E
Lindfors, E
Lombardi, S
Lopez, M
Lorenz, E
Majumdar, P
Makariev, E
Maneva, G
Mankuzhiyil, N
Mannheim, K
Maraschi, L
Mariotti, M
Martinez, M
Mazin, D
Meucci, M
Miranda, JM
Mirzoyan, R
Miyamoto, H
Moldon, J
Moralejo, A
Nieto, D
Nilsson, K
Orito, R
Oya, I
Paoletti, R
Paredes, JM
Partini, S
Pasanen, M
Pauss, F
Pegna, RG
Perez-Torres, MA
Persic, M
Peruzzo, J
Pochon, J
Moroni, PGP
Prada, F
Prandini, E
Puchades, N
Puljak, I
Reichardt, T
Reinthal, R
Rhode, W
Ribo, M
Rico, J
Rissi, M
Rugamer, S
Saggion, A
Saito, K
Saito, TY
Salvati, M
Sanchez-Conde, M
Satalecka, K
Scalzotto, V
Scapin, V
Schultz, C
Schweizer, T
Shayduk, M
Shore, SN
Sierpowska-Bartosik, A
Sillanpaa, A
Sitarek, J
Sobczynska, D
Spanier, F
Spiro, S
Stamerra, A
Steinke, B
Storz, J
Strah, N
Struebig, JC
Suric, T
Takalo, LO
Tavecchio, F
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Vankov, H
Wagner, RM
Weitzel, Q
Zabalza, V
Zandanel, F
Zanin, R
Acciari, VA
Arlen, T
Aune, T
Benbow, W
Boltuch, D
Bradbury, SM
Buckley, JH
Bugaev, V
Cannon, A
Cesarini, A
Ciupik, L
Cui, W
Dickherber, R
Errando, M
Falcone, A
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gillanders, GH
Godambe, S
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Holder, J
Huang, D
Hui, CM
Humensky, TB
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Konopelko, A
Krawczynski, H
Krennrich, F
Lang, MJ
Maier, G
McArthur, S
McCann, A
McCutcheon, M
Moriarty, P
Mukherjee, R
Ong, R
Otte, N
Pandel, D
Perkins, JS
Pichel, A
Pohl, M
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Rovero, AC
Schroedter, M
Sembroski, GH
Senturk, GD
Steele, D
Swordy, SP
Tesic, G
Theiling, M
Thibadeau, S
Varlotta, A
Vincent, S
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Weisgarber, T
Williams, DA
Wood, M
Zitzer, B
Villata, M
Raiteri, CM
Aller, HD
Aller, MF
Arkharov, AA
Blinov, DA
Calcidese, P
Chen, WP
Efimova, NV
Kimeridze, G
Konstantinova, TS
Kopatskaya, EN
Koptelova, E
Kurtanidze, OM
Kurtanidze, SO
Lahteenmaki, A
Larionov, VM
Larionova, EG
Larionova, LV
Ligustri, R
Morozova, DA
Nikolashvili, MG
Sigua, LA
Troitsky, IS
Angelakis, E
Capalbi, M
Carraminana, A
Carrasco, L
Cassaro, P
de la Fuente, E
Gurwell, MA
Kovalev, YY
Kovalev, YA
Krichbaum, TP
Krimm, HA
Leto, P
Lister, ML
Maccaferri, G
Moody, JW
Mori, Y
Nestoras, I
Orlati, A
Pagani, C
Pace, C
Pearson, R
Perri, M
Piner, BG
Pushkarev, AB
Ros, E
Sadun, AC
Sakamoto, T
Tornikoski, M
Yatsu, Y
Zook, A
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Allafort, A.
Baldini, L.
Ballet, J.
Barbiellini, G.
Baring, M. G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bouvier, A.
Brandt, T. J.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Cannon, A.
Caraveo, P. A.
Carrigan, S.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Celik, O. .
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
Dermer, C. D.
de Palma, F.
do Couto e Silva, E.
Drell, P. S.
Dubois, R.
Dumora, D.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Frailis, M.
Fuhrmann, L.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
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Kovalev, Yu. A.
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Krimm, H. A.
Leto, P.
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Maccaferri, G.
Moody, J. W.
Mori, Y.
Nestoras, I.
Orlati, A.
Pagani, C.
Pace, C.
Pearson, R., III
Perri, M.
Piner, B. G.
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CA Fermi-LAT Collaboration
MAGIC Collaboration
VERITAS Collaboration
TI INSIGHTS INTO THE HIGH-ENERGY gamma-RAY EMISSION OF MARKARIAN 501 FROM
EXTENSIVE MULTIFREQUENCY OBSERVATIONS IN THE FERMI ERA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; BL Lacertae objects: general; BL Lacertae
objects: individual (Mrk 501); galaxies: active; gamma rays: general;
radiation mechanisms: non-thermal
ID BL LACERTAE OBJECTS; CHERENKOV TELESCOPE SYSTEM; MAGNETOSONIC
SHOCK-WAVES; ACTIVE GALACTIC NUCLEI; LOG-PARABOLIC SPECTRA; LARGE-AREA
TELESCOPE; EARLY-TYPE GALAXIES; X-RAY; PARTICLE-ACCELERATION; TEV
VARIABILITY
AB We report on the gamma-ray activity of the blazar Mrk 501 during the first 480 days of Fermi operation. We find that the average Large Area Telescope (LAT) gamma-ray spectrum of Mrk 501 can be well described by a single power-law function with a photon index of 1.78 +/- 0.03. While we observe relatively mild flux variations with the Fermi-LAT (within less than a factor of two), we detect remarkable spectral variability where the hardest observed spectral index within the LAT energy range is 1.52 +/- 0.14, and the softest one is 2.51 +/- 0.20. These unexpected spectral changes do not correlate with the measured flux variations above 0.3 GeV. In this paper, we also present the first results from the 4.5 month long multifrequency campaign (2009 March 15-August 1) on Mrk 501, which included the Very Long Baseline Array (VLBA), Swift, RXTE, MAGIC, and VERITAS, the F-GAMMA, GASP-WEBT, and other collaborations and instruments which provided excellent temporal and energy coverage of the source throughout the entire campaign. The extensive radio to TeV data set from this campaign provides us with the most detailed spectral energy distribution yet collected for this source during its relatively low activity. The average spectral energy distribution of Mrk 501 is well described by the standard one-zone synchrotron self-Compton (SSC) model. In the framework of this model, we find that the dominant emission region is characterized by a size less than or similar to 0.1 pc (comparable within a factor of few to the size of the partially resolved VLBA core at 15-43 GHz), and that the total jet power (similar or equal to 10(44) erg s(-1)) constitutes only a small fraction (similar to 10(-3)) of the Eddington luminosity. The energy distribution of the freshly accelerated radiating electrons required to fit the time-averaged data has a broken power-law form in the energy range 0.3 GeV-10 TeV, with spectral indices 2.2 and 2.7 below and above the break energy of 20 GeV. We argue that such a form is consistent with a scenario in which the bulk of the energy dissipation within the dominant emission zone of Mrk 501 is due to relativistic, proton-mediated shocks. We find that the ultrarelativistic electrons and mildly relativistic protons within the blazar zone, if comparable in number, are in approximate energy equipartition, with their energy dominating the jet magnetic field energy by about two orders of magnitude.
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[Antoranz, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Pegna, R. G.; Moroni, P. G. Prada; Stamerra, A.] Univ Siena, I-53100 Siena, Italy.
[Antoranz, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Pegna, R. G.; Moroni, P. G. Prada; Stamerra, A.] INFN Pisa, I-53100 Siena, Italy.
[Backes, M.; Doert, M.; Rhode, W.; Strah, N.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Barrio, J. A.; Bose, D.; Camara, M.; Contreras, J. L.; Fonseca, M. V.; Nieto, D.; Oya, I.] Univ Complutense, E-28040 Madrid, Spain.
[Gonzalez, J. Becerra; Berger, K.; Ortega, A. Diago; Lopen, R. J. Garcia; Herrero, A.; Sanchez-Conde, M.] Univ La Laguna, Dept Astrophys, E-38205 San Cristobal la Laguna, Tenerife, Spain.
[Bednarek, W.; Sierpowska-Bartosik, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Berdyugin, A.; Lindfors, E.; Nilsson, K.; Pasanen, M.; Reinthal, R.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Tuorla Observ, FIN-21500 Piikkio, Finland.
[Bernardini, E.; Satalecka, K.; Maier, G.; Pohl, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Biland, A.; Boller, A.; Braun, I.; Dorner, D.; Hildebrand, D.; Kraehenbuehl, T.; Kranich, D.; Lorenz, E.; Pauss, F.; Rissi, M.; Weitzel, Q.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
[Bordas, P.; Bosch-Ramon, V.; Paredes, J. M.; Ribo, M.; Zabalza, V.] Univ Barcelona ICC IEED, E-08028 Barcelona, Spain.
[Bretz, T.; Elsaesser, D.; Hoehne-Moench, D.; Mannheim, K.; Ruegamer, S.; Spanier, F.; Storz, J.; Struebig, J. C.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[De Lotto, B.; De Maria, M.; De Sabata, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[De Lotto, B.; De Maria, M.; De Sabata, F.] Univ Trieste, I-34127 Trieste, Italy.
[Mendez, C. Delgado] Ctr Invest Energet Medioambientales & Tecnol CIE, Madrid, Spain.
[Dominguez, A.; Perez-Torres, M. A.; Prada, F.; Zandanel, F.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Prester, D. Dominis; Ferenc, D.; Godinovi, N.; Hrupec, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Rijeka, Rudjer Boskovic Inst, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia.
[Font, L.] Univ Autonoma Barcelona, E-08193 Barcelona, Spain.
[Makariev, E.; Maneva, G.; Temnikov, P.; Vankov, H.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria.
[Maraschi, L.; Tavecchio, F.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Persic, M.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; La Barbera, A.; Salvati, M.; Spiro, S.] INAF Natl Inst Astrophys, I-00136 Rome, Italy.
[Shore, S. N.] Univ Pisa, Dipartimento Fis Enrico Fermi, I-56127 Pisa, Italy.
[Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Arlen, T.; Ong, R.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Cesarini, A.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Galway, Ireland.
[Ciupik, L.; Fortson, L.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Chicago, IL 60605 USA.
[Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.; Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Huang, D.; Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA.
[Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Krennrich, F.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Pichel, A.; Rovero, A. C.] Parbellon IAFE, Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina.
[Pohl, M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Senturk, G. D.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Steele, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Villata, M.; Raiteri, C. M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy.
[Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Arkharov, A. A.; Blinov, D. A.; Efimova, N. V.; Larionov, V. M.; Pushkarev, A. B.] Pulkovo Observ, St Petersburg 196140, Russia.
[Chen, W. P.; Koptelova, E.] Natl Cent Univ, Grad Inst Astron, Jhongli 32054, Taiwan.
[Efimova, N. V.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Nikolashvili, M. G.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia.
[Kimeridze, G.; Kurtanidze, O. M.; Kurtanidze, S. O.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia.
[Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland.
[Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia.
[Ligustri, R.] Circolo Astrofili Talmassons, I-33030 Campoformido, UD, Italy.
[Carraminana, A.; Carrasco, L.] Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico.
[Cassaro, P.] Ist Radioastron, Sez Noto, INAF, I-96017 Noto, SR, Italy.
[de la Fuente, E.] Univ Guadalajara, CUCEI, Dpto Fis, Inst Astron & Meteorol, Jalisco, Mexico.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Leto, P.] Osserv Astrofis Catania, I-95123 Catania, Italy.
[Maccaferri, G.; Orlati, A.] Ist Radioastron, INAF, Staz Radioastron Med, I-40059 Bologna, Italy.
[Moody, J. W.; Pace, C.; Pearson, R., III] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA.
[Mori, Y.; Yatsu, Y.] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan.
[Pagani, C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Piner, B. G.] Whittier Coll, Dept Phys & Astron, Whittier, CA USA.
[Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine.
[Ros, E.] Univ Valencia, Valencia 46010, Spain.
[Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80220 USA.
[Zook, A.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA.
[Conrad, J.] Royal Swedish Acad Sci, Stockholm, Sweden.
RP Paneque, D (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
EM dpaneque@mppmu.mpg.de; stawarz@astro.isas.jaxa.jp
RI Sgro, Carmelo/K-3395-2016; Maneva, Galina/L-7120-2016; Backes,
Michael/N-5126-2016; Torres, Diego/O-9422-2016; Temnikov,
Petar/L-6999-2016; Orlando, E/R-5594-2016; Barrio, Juan/L-3227-2014;
Cortina, Juan/C-2783-2017; Morozova, Daria/H-1298-2013; Troitskiy,
Ivan/K-7979-2013; Grishina, Tatiana/H-6873-2013; Loparco,
Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano,
Fabio/O-8934-2015; Pushkarev, Alexander/M-9997-2015; Miranda, Jose
Miguel/F-2913-2013; Font, Lluis/L-4197-2014; Moskalenko,
Igor/A-1301-2007; Contreras Gonzalez, Jose Luis/K-7255-2014; Mazziotta,
Mario /O-8867-2015; Lopez Moya, Marcos/L-2304-2014; GAug,
Markus/L-2340-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Ribo,
Marc/B-3579-2015; Kovalev, Yuri/J-5671-2013; Funk, Stefan/B-7629-2015;
Pavlidou, Vasiliki/C-2944-2011; Sokolovsky, Kirill/D-2246-2015;
Antoranz, Pedro/H-5095-2015; Delgado, Carlos/K-7587-2014; Nieto,
Daniel/J-7250-2015; Kovalev, Yuri/N-1053-2015; Pearson,
Timothy/N-2376-2015; Tosti, Gino/E-9976-2013; Larionov,
Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Larionova,
Elena/H-7287-2013; Efimova, Natalia/I-2196-2013; Blinov,
Dmitry/G-9925-2013; Rando, Riccardo/M-7179-2013; Lahteenmaki,
Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Johnson,
Neil/G-3309-2014; Kurtanidze, Omar/J-6237-2014; Rico,
Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Prada Moroni, Pier
Giorgio/G-5565-2011; Braun, Isabel/C-9373-2012; Thompson,
David/D-2939-2012; Gehrels, Neil/D-2971-2012; McEnery,
Julie/D-6612-2012; Baldini, Luca/E-5396-2012; Mannheim,
Karl/F-6705-2012; lubrano, pasquale/F-7269-2012; Morselli,
Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; Doro, Michele/F-9458-2012;
giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Fonseca
Gonzalez, Maria Victoria/I-2004-2015;
OI Backes, Michael/0000-0002-9326-6400; Torres, Diego/0000-0002-1522-9065;
Temnikov, Petar/0000-0002-9559-3384; Barrio, Juan/0000-0002-0965-0259;
Cortina, Juan/0000-0003-4576-0452; Villata, Massimo/0000-0003-1743-6946;
Larionova, Liudmila/0000-0002-0274-1481; Leto,
Paolo/0000-0003-4864-2806; Morozova, Daria/0000-0002-9407-7804;
Troitskiy, Ivan/0000-0002-4218-0148; Grishina,
Tatiana/0000-0002-3953-6676; Loparco, Francesco/0000-0002-1173-5673;
Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano,
Fabio/0000-0002-5055-6395; Miranda, Jose Miguel/0000-0002-1472-9690;
Font, Lluis/0000-0003-2109-5961; Moskalenko, Igor/0000-0001-6141-458X;
Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Mazziotta, Mario
/0000-0001-9325-4672; Lopez Moya, Marcos/0000-0002-8791-7908; GAug,
Markus/0000-0001-8442-7877; Moralejo Olaizola,
Abelardo/0000-0002-1344-9080; Kovalev, Yuri/0000-0001-9303-3263; Funk,
Stefan/0000-0002-2012-0080; Pavlidou, Vasiliki/0000-0002-0870-1368;
Sokolovsky, Kirill/0000-0001-5991-6863; Antoranz,
Pedro/0000-0002-3015-3601; Delgado, Carlos/0000-0002-7014-4101; Nieto,
Daniel/0000-0003-3343-0755; Pearson, Timothy/0000-0001-5213-6231;
Larionov, Valeri/0000-0002-4640-4356; Kopatskaya,
Evgenia/0000-0001-9518-337X; Larionova, Elena/0000-0002-2471-6500;
Efimova, Natalia/0000-0002-8071-4753; Blinov,
Dmitry/0000-0003-0611-5784; Rico, Javier/0000-0003-4137-1134; Braun,
Isabel/0000-0002-9389-0502; Thompson, David/0000-0001-5217-9135;
lubrano, pasquale/0000-0003-0221-4806; Morselli,
Aldo/0000-0002-7704-9553; Doro, Michele/0000-0001-9104-3214; giglietto,
nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Frailis,
Marco/0000-0002-7400-2135; Cesarini, Andrea/0000-0002-8611-8610;
leonardo, elvira/0000-0003-0271-7673; Fonseca Gonzalez, Maria
Victoria/0000-0003-2235-0725; Caraveo, Patrizia/0000-0003-2478-8018; De
Lotto, Barbara/0000-0003-3624-4480; Sgro', Carmelo/0000-0001-5676-6214;
SPINELLI, Paolo/0000-0001-6688-8864; Rando,
Riccardo/0000-0001-6992-818X; Persic, Massimo/0000-0003-1853-4900; Ward,
John E/0000-0003-1973-0794; Cassaro, Pietro/0000-0001-5139-9662;
Giordano, Francesco/0000-0002-8651-2394; Orlati,
Andrea/0000-0001-8737-255X; Prada Moroni, Pier
Giorgio/0000-0001-9712-9916; De Angelis, Alessandro/0000-0002-3288-2517;
LA BARBERA, ANTONINO/0000-0002-5880-8913; Cui, Wei/0000-0002-6324-5772
FU K. A. Wallenberg Foundation; International Doctorate on Astroparticle
Physics (IDAPP) program; INFN Padova; Academy of Finland [212656,
210338]; National Radio Astronomy Observatory's Very Long Baseline Array
(VLBA) [BK150, BP143, MOJAVE]; Russian RFBR foundation [09-02-00092];
Georgian National Science Foundation [GNSF/ST07/4-180]; NASA
[NNX08AW31G]; NSF [AST-0808050]
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; Partially supported by the
International Doctorate on Astroparticle Physics (IDAPP) program.;
Supported by INFN Padova.; We acknowledge the use of public data from
the Swift and RXTE data archive. The Metsahovi team acknowledges the
support from the Academy of Finland to the observing projects (numbers
212656, 210338, among others). This research has made use of data
obtained from the National Radio Astronomy Observatory's Very Long
Baseline Array (VLBA), projects BK150, BP143, and MOJAVE. The National
Radio Astronomy Observatory is a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc. St. Petersburg University team acknowledges support
from Russian RFBR foundation via grant 09-02-00092. AZT-24 observations
are made within an agreement between Pulkovo, Rome and Teramo
observatories. This research is partly based on observations with the
100-m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie)
at Effelsberg, as well as with the Medicina and Noto telescopes operated
by INAF-Istituto di Radioastronomia. The Submillimeter Array is a joint
project between the Smithsonian Astrophysical Observatory and the
Academia Sinica Institute of Astronomy and Astrophysics and is funded by
the Smithsonian Institution and the Academia Sinica. M. Villata
organized the optical-to-radio observations by GASP-WEBT as the
president of the collaboration. Abastumani Observatory team acknowledges
financial support by the Georgian National Science Foundation through
grant GNSF/ST07/4-180. The OVRO 40 m program was funded in part by NASA
(NNX08AW31G) and the NSF (AST-0808050).
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 129
DI 10.1088/0004-637X/727/2/129
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000068
ER
PT J
AU Campo, CJ
Harrington, J
Hardy, RA
Stevenson, KB
Nymeyer, S
Ragozzine, D
Lust, NB
Anderson, DR
Collier-Cameron, A
Blecic, J
Britt, CBT
Bowman, WC
Wheatley, PJ
Loredo, TJ
Deming, D
Hebb, L
Hellier, C
Maxted, PFL
Pollaco, D
West, RG
AF Campo, Christopher J.
Harrington, Joseph
Hardy, Ryan A.
Stevenson, Kevin B.
Nymeyer, Sarah
Ragozzine, Darin
Lust, Nate B.
Anderson, David R.
Collier-Cameron, Andrew
Blecic, Jasmina
Britt, Christopher B. T.
Bowman, William C.
Wheatley, Peter J.
Loredo, Thomas J.
Deming, Drake
Hebb, Leslie
Hellier, Coel
Maxted, Pierre F. L.
Pollaco, Don
West, Richard G.
TI ON THE ORBIT OF EXOPLANET WASP-12b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (WASP-12); techniques: photometric
ID SPITZER-SPACE-TELESCOPE; EXTRASOLAR GIANT PLANETS; INFRARED ARRAY
CAMERA; THERMAL EMISSION; TIDAL EVOLUTION; BAND EMISSION; LIGHT CURVES;
ATMOSPHERE; INVERSION; SYSTEMS
AB We observed two secondary eclipses of the exoplanet WASP-12b using the Infrared Array Camera on the Spitzer Space Telescope. The close proximity of WASP-12b to its G-type star results in extreme tidal forces capable of inducing apsidal precession with a period as short as a few decades. This precession would be measurable if the orbit had a significant eccentricity, leading to an estimate of the tidal Love number and an assessment of the degree of central concentration in the planetary interior. An initial ground-based secondary-eclipse phase reported by Lopez-Morales et al. (0.510 +/- 0.002) implied eccentricity at the 4.5 sigma level. The spectroscopic orbit of Hebb et al. has eccentricity 0.049 +/- 0.015, a 3 sigma result, implying an eclipse phase of 0.509 +/- 0.007. However, there is a well-documented tendency of spectroscopic data to overestimate small eccentricities. Our eclipse phases are 0.5010 +/- 0.0006 (3.6 and 5.8 mu m) and 0.5006 +/- 0.0007 (4.5 and 8.0 mu m). An unlikely orbital precession scenario invoking an alignment of the orbit during the Spitzer observations could have explained this apparent discrepancy, but the final eclipse phase of Lopez-Morales et al. (0.510 +/-(+0.007)(-0.006)) is consistent with a circular orbit at better than 2 sigma. An orbit fit to all the available transit, eclipse, and radial-velocity data indicates precession at < 1 sigma; a non-precessing solution fits better. We also comment on analysis and reporting for Spitzer exoplanet data in light of recent re-analyses.
C1 [Campo, Christopher J.; Harrington, Joseph; Hardy, Ryan A.; Stevenson, Kevin B.; Nymeyer, Sarah; Lust, Nate B.; Blecic, Jasmina; Britt, Christopher B. T.; Bowman, William C.] Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL 32816 USA.
[Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Anderson, David R.; Hellier, Coel; Maxted, Pierre F. L.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Collier-Cameron, Andrew] Univ St Andrews, Sch Phys & Astron, Haugh KY16 9SS, Fife, Scotland.
[Wheatley, Peter J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Loredo, Thomas J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hebb, Leslie] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Pollaco, Don] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[West, Richard G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Campo, CJ (reprint author), Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL 32816 USA.
EM ccampo@knights.ucf.edu
RI Harrington, Joseph/E-6250-2011; Ragozzine, Darin/C-4926-2013;
OI Blecic, Jasmina/0000-0002-0769-9614; Stevenson,
Kevin/0000-0002-7352-7941; Cameron, Andrew/0000-0002-8863-7828; Hardy,
Ryan/0000-0002-3849-9551; Harrington, Joseph/0000-0002-8955-8531;
Wheatley, Peter/0000-0003-1452-2240
FU NASA; NASA through JPL/Caltech
FX We thank the observers listed in Table 2 for allowing us to use their
results and the organizers of the Exoplanet Transit Database for
coordinating the collection and uniform analysis of these data. The IRAC
data are based on observations made with the Spitzer Space Telescope,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology under a contract with NASA. Support for this work was
provided by NASA through an award issued by JPL/Caltech. The point of M.
Ingemyr is based on observations made with the Nordic Optical Telescope
(NOT), operated on the island of La Palma jointly by Denmark, Finland,
Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de
los Muchachos Instituto Astrofisica de Canarias, and ALFOSC, which is
owned by the Instituto Astrofisica de Andalucia (IAA) and operated at
the NOT under agreement between IAA and NBlfAFG of the Astronomical
Observatory of Copenhagen. We thank contributors to SciPy, Matplotlib,
and the Python Programming Language, W. Landsman and other contributors
to the Interactive Data Language Astronomy Library, the free- and
open-source community, the NASA Astrophysics Data System, and the JPL
Solar System Dynamics group for free software and services.
NR 40
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
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AR 125
DI 10.1088/0004-637X/727/2/125
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000064
ER
PT J
AU Crockett, RM
Kaviraj, S
Silk, JI
Whitmore, BC
O'Connell, RW
Mutchler, M
Balick, B
Bond, HE
Calzetti, D
Carollo, CM
Disney, MJ
Dopita, MA
Frogel, JA
Hall, DNB
Holtzman, JA
Kimble, RA
McCarthy, PJ
Paresce, F
Saha, A
Trauger, JT
Walker, AR
Windhorst, RA
Young, ET
Jeong, H
Yi, SK
AF Crockett, R. Mark
Kaviraj, Sugata
Silk, Joseph I.
Whitmore, Bradley C.
O'Connell, Robert W.
Mutchler, Max
Balick, Bruce
Bond, Howard E.
Calzetti, Daniela
Carollo, C. Marcella
Disney, Michael J.
Dopita, Michael A.
Frogel, Jay A.
Hall, Donald N. B.
Holtzman, Jon A.
Kimble, Randy A.
McCarthy, Patrick J.
Paresce, Francesco
Saha, Abhijit
Trauger, John T.
Walker, Alistair R.
Windhorst, Rogier A.
Young, Erick T.
Jeong, Hyunjin
Yi, Sukyoung K.
TI ANATOMY OF A POST-STARBURST MINOR MERGER: A MULTI-WAVELENGTH WFC3 STUDY
OF NGC 4150
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: evolution;
ultraviolet: galaxies
ID EARLY-TYPE GALAXIES; COLOR-MAGNITUDE RELATION; DIGITAL SKY SURVEY;
MASS-METALLICITY RELATION; HUBBLE-SPACE-TELESCOPE; STAR-FORMATION
HISTORIES; LARGE-MAGELLANIC-CLOUD; ELLIPTIC GALAXIES; SAURON PROJECT;
STELLAR POPULATION
AB We present a spatially resolved near-UV/optical study, using the Wide Field Camera 3 (WFC3) on board the Hubble Space Telescope, of NGC 4150, a sub-L-*, early-type galaxy (ETG) of around 6 x 10(9) M-circle dot, which has been observed as part of the WFC3 Early-Release Science Programme. Previous work indicates that this galaxy has a large reservoir of molecular hydrogen gas, exhibits a kinematically decoupled core (a likely indication of recent merging) and strong, central H beta absorption (indicative of young stars). While relatively uninspiring in its optical image, the core of NGC 4150 shows ubiquitous near-UV emission and remarkable dusty substructure. Our analysis shows this galaxy to lie in the near-UV green valley, and its pixel-by-pixel photometry exhibits a narrow range of near-UV/optical colors that are similar to those of nearby E+A (post-starburst) galaxies and lie between those of M83 (an actively star-forming spiral) and the local quiescent ETG population. We parameterize the properties of the recent star formation (RSF; age, mass fraction, metallicity, and internal dust content) in the NGC 4150 pixels by comparing the observed near-UV/optical photometry to stellar models. The typical age of the RSF is around 0.9 Gyr, consistent with the similarity of the near-UV colors to post-starburst systems, while the morphological structure of the young component supports the proposed merger scenario. The typical RSF metallicity, representative of the metallicity of the gas fuelling star formation, is similar to 0.3-0.5 Z(circle dot). Assuming that this galaxy is a merger and that the gas is sourced mainly from the infalling companion, these metallicities plausibly indicate the gas-phase metallicity (GPM) of the accreted satellite. Comparison to the local mass-GPM relation suggests (crudely) that the mass of the accreted system is similar to 3 x 10(8) M-circle dot, making NGC 4150 a 1: 20 minor merger. A summation of the pixel RSF mass fractions indicates that the RSF contributes similar to 2%-3% of the stellar mass. This work reaffirms our hypothesis that minor mergers play a significant role in the evolution of ETGs at late epochs.
C1 [Crockett, R. Mark; Kaviraj, Sugata; Silk, Joseph I.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Kaviraj, Sugata] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, London SW7 2AZ, England.
[Whitmore, Bradley C.; Mutchler, Max; Bond, Howard E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Balick, Bruce] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Calzetti, Daniela] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Carollo, C. Marcella] Swiss Fed Inst Technol, Dept Phys, CH-8093 Zurich, Switzerland.
[Disney, Michael J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Frogel, Jay A.] Assoc Univ Res Astron, Washington, DC 20005 USA.
[Hall, Donald N. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Kimble, Randy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McCarthy, Patrick J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Paresce, Francesco] INAF, Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy.
[Saha, Abhijit] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Trauger, John T.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Walker, Alistair R.] Cerro Tololo Interamer Observ, La Serena, Chile.
[Windhorst, Rogier A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Young, Erick T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Jeong, Hyunjin; Yi, Sukyoung K.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea.
RP Crockett, RM (reprint author), Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
EM mark.crockett@astro.ox.ac.uk
RI Dopita, Michael/P-5413-2014;
OI Dopita, Michael/0000-0003-0922-4986; silk, joe/0000-0002-1566-8148
FU NASA [NAS5-26555]; Space Telescope Science Institute; NASA through Space
Telescope Science Institute [11359/60]; STFC [DBRPDV0]; Royal Commission
for the Exhibition; Worcester College Oxford; BIPAC Institute at the
University of Oxford; Korean government through the Korea Research
Foundation [KRF-C00156]; Korea Science and Engineering Foundation
[20090078756]
FX We thank an anonymous referee for helpful comments and suggestions. This
paper is based on Early Release Science observations made by the WFC3
Scientific Oversight Committee. We are grateful to the Director of the
Space Telescope Science Institute for awarding Director's Discretionary
time for this program. Finally, we are deeply indebted to the brave
astronauts of STS-125 for rejuvenating HST. Support for Program numbers
11359/60 as provided by NASA through a grant from the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.
R. M. C. acknowledges funding from STFC through research grant DBRPDV0.
S. K. acknowledges a Research Fellowship from the Royal Commission for
the Exhibition of 1851, an Imperial College Research Fellowship, a
Senior Research Fellowship from Worcester College Oxford and support
from the BIPAC Institute at the University of Oxford. S.K.Y. was
supported by the Korean government through the Korea Research Foundation
Grant (KRF-C00156) and the Korea Science and Engineering Foundation
Grant (No. 20090078756).
NR 78
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 115
DI 10.1088/0004-637X/727/2/115
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000054
ER
PT J
AU Dwek, E
Cherchneff, I
AF Dwek, Eli
Cherchneff, Isabelle
TI THE ORIGIN OF DUST IN THE EARLY UNIVERSE: PROBING THE STAR FORMATION
HISTORY OF GALAXIES BY THEIR DUST CONTENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst;
infrared: galaxies; quasars: individual (SDSS J114816.64+525150.3)
ID ORGANIC REFRACTORY COMPONENT; DIGITAL SKY SURVEY; INTERSTELLAR DUST;
SUPERNOVA REMNANT; CHEMICAL EVOLUTION; HIGH-REDSHIFT; Z-SIMILAR-TO-6
QUASARS; SOLAR NEIGHBORHOOD; RADIATIVE-TRANSFER; SPACE-TELESCOPE
AB Two distinct scenarios for the origin of the similar to 4 x 10(8) M-circle dot of dust observed in the high-redshift (z = 6.4) quasar J1148+5251 have been proposed. The first assumes that this galaxy is much younger than the age of the universe at that epoch so that only supernovae (SNe) could have produced this dust. The second scenario assumes a significantly older galactic age, so that the dust could have formed in lower-mass asymptotic giant branch (AGB) stars. Presenting new integral solutions for the chemical evolution of metals and dust in galaxies, we offer a critical evaluation of these two scenarios and observational consequences that can discriminate between the two. We show that AGB stars can produce the inferred mass of dust in this object, however, the final mass of surviving dust depends on the galaxy's star formation history (SFH). In general, SNe cannot produce the observed amount of dust unless the average SN event creates over similar to 2 M-circle dot of dust in its ejecta. However, special SFHs can be constructed in which SNe can produce the inferred dust mass with a reasonable average dust yield of similar to 0.15 M-circle dot. The two scenarios propose different origins for the galaxy's spectral energy distribution, different star formation efficiencies and stellar masses, and consequently different comoving number densities of J1148+5251-type hyperluminous infrared (IR) objects. The detection of diagnostic mid-IR fine structure lines and more complete surveys determining the comoving number density of these objects can discriminate between the two scenarios.
C1 [Dwek, Eli] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Cherchneff, Isabelle] Univ Basel, Dept Phys, CH-4056 Basel, Switzerland.
RP Dwek, E (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM eli.dwek@nasa.gov; isabelle.cherchneff@unibas.ch
RI Dwek, Eli/C-3995-2012
NR 69
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 63
DI 10.1088/0004-637X/727/2/63
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000002
ER
PT J
AU Kawakita, H
Mumma, MJ
AF Kawakita, Hideyo
Mumma, Michael J.
TI FLUORESCENCE EXCITATION MODELS OF AMMONIA AND AMIDOGEN RADICAL (NH2) IN
COMETS: APPLICATION TO COMET C/2004 Q2 (MACHHOLZ)
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; comets: individual (C/2004 Q2 (Machholz)); line:
formation; line: identification
ID OH PROMPT EMISSION; SELECTIVE PHOTODISSOCIATION DYNAMICS; JUPITER-FAMILY
COMETS; C/1999 H1 LEE; SPIN TEMPERATURE; ORGANIC VOLATILES; STATE
AMMONIA; ICY MATERIALS; HALE-BOPP; 193.3 NM
AB Ammonia is a major reservoir of nitrogen atoms in cometary materials. However, detections of ammonia in comets are rare, with several achieved at radio wavelengths. A few more detections were obtained through near-infrared observations (around the 3 mu m wavelength region), but moderate relative velocity shifts are required to separate emission lines of cometary ammonia from telluric absorption lines in the 3 mu m wavelength region. On the other hand, the amidogen radical (NH2-a photodissociation product of ammonia in the coma) also shows rovibrational emission lines in the 3 mu m wavelength region. Thus, gas production rates for ammonia can be determined from the rovibrational emission lines of ammonia (directly) and amidogen radical (indirectly) simultaneously in the near-infrared. In this article, we present new fluorescence excitation models for cometary ammonia and amidogen radical in the near-infrared, and we apply these models to the near-infrared high-dispersion spectra of comet C/2004 Q2 (Machholz) to determine the mixing ratio of ammonia to water in the comet. Based on direct detection of NH3 lines, the mixing ratio of NH3/H2O is 0.46% +/- 0.03% in C/2004 Q2 (Machholz), in agreement with other results. The mixing ratio of ammonia determined from the NH2 observations (0.31%-0.79%) is consistent but has relatively larger error, owing to uncertainty in the photodissociation rates of ammonia. At the present level of accuracy, we confirm that NH3 could be the sole parent of NH2 in this comet.
C1 [Kawakita, Hideyo] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kita Ku, Kyoto 6038555, Japan.
[Mumma, Michael J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Kawakita, H (reprint author), Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kita Ku, Kyoto 6038555, Japan.
EM kawakthd@cc.kyoto-su.ac.jp
RI mumma, michael/I-2764-2013
FU MEXT [22540257]; NASA [RTOP 196-41-54]
FX Data presented herein were obtained at the W. M. Keck Observatory. This
work was financially supported by MEXT under Grant-in-Aid for Scientific
Research 22540257 (H. K.) and by the NASA Planetary Astronomy Program
under RTOP 196-41-54 (M.J.M.). The authors would like to thank Hitomi
Kobayashi for her great effort on the data reduction.
NR 62
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
DI 10.1088/0004-637X/727/2/91
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000030
ER
PT J
AU Marshall, FE
Antonelli, LA
Burrows, DN
Covino, S
de Pasquale, M
Evans, PA
Fugazza, D
Holland, ST
Liang, EW
O'Brien, PT
Oates, SR
Osborne, JP
Pagani, C
Sakamoto, T
Siegel, MH
Wu, XF
Zhang, B
AF Marshall, F. E.
Antonelli, L. A.
Burrows, D. N.
Covino, S.
de Pasquale, M.
Evans, P. A.
Fugazza, D.
Holland, S. T.
Liang, E. W.
O'Brien, P. T.
Oates, S. R.
Osborne, J. P.
Pagani, C.
Sakamoto, T.
Siegel, M. H.
Wu, X. F.
Zhang, B.
TI THE LATE PEAKING AFTERGLOW OF GRB 100418A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: individual (GRB 100418A)
ID GAMMA-RAY BURST; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; LIGHT CURVES;
ALERT TELESCOPE; CENTRAL ENGINE; REM; IDENTIFICATION; CALIBRATION;
GRB-060206; SUPERNOVA
AB GRB 100418A is a long gamma-ray burst (GRB) at redshift z = 0.6235 discovered with the Swift Gamma-ray Burst Explorer with unusual optical and X-ray light curves. After an initial short-lived, rapid decline in X-rays, the optical and X-ray light curves observed with Swift are approximately flat or rising slightly out to at least similar to 7 x 10(3) s after the trigger, peak at similar to 5 x 10(4) s, and then follow an approximately power-law decay. Such a long optical plateau and late peaking is rarely seen in GRB afterglows. Observations with Rapid Eye Mount during a gap in the Swift coverage indicate a bright optical flare at similar to 2.5 x 10(4) s. The long plateau phase of the afterglow is interpreted using either a model with continuous injection of energy into the forward shock of the burst or a model in which the jet of the burst is viewed off-axis. In both models the isotropic kinetic energy in the late afterglow after the plateau phase is >= 10(2) times the 10(51) erg of the prompt isotropic gamma-ray energy release. The energy injection model is favored because the off-axis jet model would require the intrinsic T-90 for the GRB jet viewed on-axis to be very short, similar to 10 ms, and the intrinsic isotropic gamma-ray energy release and the true jet energy to be much higher than the typical values of known short GRBs. The non-detection of a jet break up to t similar to 2 x 10(6) s indicates a jet half-opening angle of at least similar to 14 degrees, and a relatively high-collimation-corrected jet energy of E-jet >= 10(52) erg.
C1 [Marshall, F. E.; Sakamoto, T.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Antonelli, L. A.] INAF Astron Observ Rome, I-00040 Rome, Italy.
[Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Covino, S.; Fugazza, D.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Covino, S.] INAF TNG Fdn Galileo Galilei, Brena Baja 38712, TF, Spain.
[de Pasquale, M.; Oates, S. R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Evans, P. A.; O'Brien, P. T.; Osborne, J. P.; Pagani, C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Holland, S. T.; Sakamoto, T.] NASA, Ctr Res & Explorat Space Sci & Technol, GSFC, Greenbelt, MD 20771 USA.
[Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Liang, E. W.; Wu, X. F.; Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
[Liang, E. W.] Guangxi Univ, Dept Phys, Guangxi 530004, Peoples R China.
[Sakamoto, T.] Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Wu, X. F.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
RP Marshall, FE (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
EM frank.marshall@nasa.gov
RI Wu, Xuefeng/G-5316-2015;
OI Wu, Xuefeng/0000-0002-6299-1263; Covino, Stefano/0000-0001-9078-5507
FU NASA [NNX09AT66G, NNX10AD48G]; NSF [AST-0908362]; National Basic
Research Program of China (973 Program) [2009CB824800]; STFC
FX This work made use of data supplied by the UK Swift Science Data Centre
at the University of Leicester and the High Energy Astrophysics Science
Archive Research Center, provided by NASA's Goddard Space Flight Center.
B.Z., X. F. W., and E. W. L. acknowledge NASA NNX09AT66G, NNX10AD48G,
and NSF AST-0908362 for support. X. F. W. and E. W. L. are also
supported by National Basic Research Program of China (973 Program
2009CB824800). P. A. E., J.P.O., and C. P. acknowledge STFC support.
NR 65
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 132
DI 10.1088/0004-637X/727/2/132
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000071
ER
PT J
AU Meschiari, S
Laughlin, G
Vogt, SS
Butler, RP
Rivera, EJ
Haghighipour, N
Jalowiczor, P
AF Meschiari, Stefano
Laughlin, Gregory
Vogt, Steven S.
Butler, R. Paul
Rivera, Eugenio J.
Haghighipour, Nader
Jalowiczor, Peter
TI THE LICK-CARNEGIE SURVEY: FOUR NEW EXOPLANET CANDIDATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: numerical; planets and satellites: detection
ID SUN-LIKE STAR; EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS; VELOCITY JITTER;
NEARBY STARS; DEBRIS DISKS; SUPER-EARTH; HOST STARS; COOL STARS; F-DWARF
AB We present new precise HIRES radial velocity (RV) data sets of five nearby stars obtained at Keck Observatory. HD 31253, HD 218566, HD 177830, HD 99492, and HD 74156 are host stars of spectral classes F through K and show RV variations consistent with new or additional planetary companions in Keplerian motion. The orbital parameters of the candidate planets in the five planetary systems span minimum masses of M sin i = 27.43 M-empty set to 8.28 M-J, periods of 17.05-4696.95 days and eccentricities ranging from circular to extremely eccentric (e approximate to 0.63). The fifth star, HD 74156, was known to have both a 52 day and a 2500 day planet, and was claimed to also harbor a third planet at 336 days, in apparent support of the "Packed Planetary System" hypothesis. Our greatly expanded data set for HD 74156 provides strong confirmation of both the 52 day and 2500 day planets, but strongly contradicts the existence of a 336 day planet, and offers no significant evidence for any other planets in the system.
C1 [Meschiari, Stefano; Laughlin, Gregory; Vogt, Steven S.; Rivera, Eugenio J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO, Lick Observ, Santa Cruz, CA 95064 USA.
[Butler, R. Paul] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
RP Meschiari, S (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO, Lick Observ, Santa Cruz, CA 95064 USA.
RI Butler, Robert/B-1125-2009;
OI Meschiari, Stefano/0000-0002-2930-0416
FU NASA Astrobiology Institute at NASA Ames Research Center; NSF
[AST-0449986, AST-0307493, AST-0908870]; NASA OSS [NNX07AR40G]; NASA;
Carnegie Institution of Washington; NASA Astrobiology Institute at the
Institute for Astronomy, University of Hawaii [NNA04CC08A]; NASA/EXOB
[NNX09AN05G]; UC-Keck; UH-Keck; NASA-Keck Time Assignment Committees
FX G. L. acknowledges support from the NASA Astrobiology Institute at NASA
Ames Research Center, and from the NSF CAREER Program through NSF Grant
AST-0449986. S. S. V. gratefully acknowledges support from NSF grants
AST-0307493 and AST-0908870. R. P. B. gratefully acknowledges support
from NASA OSS Grant NNX07AR40G, the NASA Keck PI program, and from the
Carnegie Institution of Washington. N.H. acknowledges support from the
NASA Astrobiology Institute under Cooperative Agreement NNA04CC08A at
the Institute for Astronomy, University of Hawaii, and the NASA/EXOB
grant NNX09AN05G. The work herein is based on observations obtained at
the W. M. Keck Observatory, which is operated jointly by the University
of California and the California Institute of Technology, and we thank
the UC-Keck, UH-Keck, and NASA-Keck Time Assignment Committees for their
support. We also wish to extend our special thanks to those of Hawaiian
ancestry on whose sacred mountain of Mauna Kea we are privileged to be
guests. Without their generous hospitality, the Keck observations
presented herein would not have been possible. This research has made
use of the NStEd database operated by NASA and the SIMBAD database,
operated at CDS, Strasbourg, France. This paper was produced using
BAM.
NR 44
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
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AR 117
DI 10.1088/0004-637X/727/2/117
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000056
ER
PT J
AU Mousis, O
Lunine, JI
Petit, JM
Zahnle, K
Biennier, L
Picaud, S
Johnson, TV
Mitchell, JBA
Boudon, V
Cordier, D
Devel, M
Georges, R
Griffith, C
Iro, N
Marley, MS
Marboeuf, U
AF Mousis, O.
Lunine, J. I.
Petit, J. -M.
Zahnle, K.
Biennier, L.
Picaud, S.
Johnson, T. V.
Mitchell, J. B. A.
Boudon, V.
Cordier, D.
Devel, M.
Georges, R.
Griffith, C.
Iro, N.
Marley, M. S.
Marboeuf, U.
TI ON THE VOLATILE ENRICHMENTS AND HEAVY ELEMENT CONTENT IN HD189733b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: composition; planets and satellites: formation;
planets and satellites: general; planets and satellites: individual
(HD189733b); protoplanetary disks; stars: abundances
ID GIANT PLANET FORMATION; SOLAR NEBULA; GRAVITATIONAL-INSTABILITY;
CARBONACEOUS DUST; HOT JUPITERS; MU-M; EVOLUTION; MIGRATION; SATURN;
ACCRETION
AB Favored theories of giant planet formation center around two main paradigms, namely the core accretion model and the gravitational instability model. These two formation scenarios support the hypothesis that the giant planet metallicities should be higher or equal to that of the parent star. Meanwhile, spectra of the transiting hot Jupiter HD189733b suggest that carbon and oxygen abundances range from depleted to enriched with respect to the star. Here, using a model describing the formation sequence and composition of planetesimals in the protoplanetary disk, we determine the range of volatile abundances in the envelope of HD189733b that is consistent with the 20-80 M-circle plus of heavy elements estimated to be present in the planet's envelope. We then compare the inferred carbon and oxygen abundances to those retrieved from spectroscopy, and we find a range of supersolar values that directly fit both spectra and internal structure models. In some cases, we find that the apparent contradiction between the subsolar elemental abundances and the mass of heavy elements predicted in HD189733b by internal structure models can be explained by the presence of large amounts of carbon molecules in the form of polycyclic aromatic hydrocarbons and soots in the upper layers of the envelope, as suggested by recent photochemical models. A diagnostic test that would confirm the presence of these compounds in the envelope is the detection of acetylene. Several alternative hypotheses that could also explain the subsolar metallicity of HD189733b are formulated: the possibility of differential settling in its envelope, the presence of a larger core that did not erode with time, a mass of heavy elements lower than the one predicted by interior models, a heavy element budget resulting from the accretion of volatile-poor planetesimals in specific circumstances, or the combination of all these mechanisms.
C1 [Mousis, O.; Petit, J. -M.; Picaud, S.] Univ Franche Comte, Observ Besancon, CNRS UMR 6213, Inst UTINAM, F-25010 Besancon, France.
[Lunine, J. I.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy.
[Zahnle, K.; Marley, M. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Biennier, L.; Mitchell, J. B. A.; Cordier, D.; Georges, R.] Univ Europeenne Bretagne, Rennes, France.
[Biennier, L.; Mitchell, J. B. A.; Cordier, D.; Georges, R.] Univ Rennes 1, CNRS, Inst Phys Rennes, UMR 6251, F-35042 Rennes, France.
[Johnson, T. V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Boudon, V.] Univ Bourgogne, CNRS, UMR 5209, Lab Interdisciplinaire Carnot Bourgogne, F-21078 Dijon, France.
[Cordier, D.] Ecole Natl Super Chim Rennes, CNRS, UMR 6226, F-35708 Rennes 7, France.
[Devel, M.] ENSMM, UTBM, UFC, CNRS,FEMTO ST, Besancon, France.
[Griffith, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Iro, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Marboeuf, U.] Univ Grenoble 1, CNRS, INSU, Lab Planetol Grenoble, F-38041 Grenoble, France.
RP Mousis, O (reprint author), Univ Franche Comte, Observ Besancon, CNRS UMR 6213, Inst UTINAM, BP 1615, F-25010 Besancon, France.
EM olivier.mousis@obs-besancon.fr
RI BOUDON, Vincent/A-4504-2010; DEVEL, Michel/A-5677-2009; Marley,
Mark/I-4704-2013; Biennier, Ludovic/O-1618-2014;
OI DEVEL, Michel/0000-0001-8785-6896; Marley, Mark/0000-0002-5251-2943
FU CNES; "Incentivazione alla mobilita" di studiosi straineri e italiani
residenti all'estero
FX We thank J.-P. Beaulieu and G. Tinetti for their valuable comments on
the manuscript. O.M. acknowledges support from CNES. J.I.L.'s work was
supported within the scope of the program "Incentivazione alla mobilita"
di studiosi straineri e italiani residenti all'estero. We acknowledge T.
Guillot for enlightening discussions and information on his work. We
thank an anonymous reviewer for his constructive comments which helped
us improve our manuscript.
NR 50
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
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AR 77
DI 10.1088/0004-637X/727/2/77
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000016
ER
PT J
AU Osborne, JP
Page, KL
Beardmore, AP
Bode, MF
Goad, MR
O'Brien, TJ
Starrfield, S
Rauch, T
Ness, JU
Krautter, J
Schwarz, G
Burrows, DN
Gehrels, N
Drake, JJ
Evans, A
Eyres, SPS
AF Osborne, J. P.
Page, K. L.
Beardmore, A. P.
Bode, M. F.
Goad, M. R.
O'Brien, T. J.
Starrfield, S.
Rauch, T.
Ness, J. -U.
Krautter, J.
Schwarz, G.
Burrows, D. N.
Gehrels, N.
Drake, J. J.
Evans, A.
Eyres, S. P. S.
TI THE SUPERSOFT X-RAY PHASE OF NOVA RS OPHIUCHI 2006
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: symbiotic; novae, cataclysmic variables; stars: oscillations;
X-rays: individual (RS Oph)
ID SWIFT OBSERVATIONS; LIGHT-CURVE; BLAST WAVE; INTERFEROMETRIC
OBSERVATIONS; CATACLYSMIC VARIABLES; INFRARED OBSERVATIONS; SPECTRAL
EVOLUTION; MODEL ATMOSPHERES; RECURRENT NOVAE; CLASSICAL NOVAE
AB Swift X-ray observations of the similar to 60 day supersoft phase of the recurrent nova RS Ophiuchi (RS Oph) 2006 show the progress of nuclear burning on the white dwarf (WD) in exquisite detail. First seen 26 days after the optical outburst, this phase started with extreme variability likely due to variable absorption, although intrinsic WD variations are not excluded. About 32 days later, a steady decline in count rate set in. NLTE model atmosphere spectral fits during the supersoft phase show that the effective temperature of the WD increases from similar to 65 eV to similar to 90 eV during the extreme variability phase, falling slowly after about day 60 and more rapidly after day 80. The bolometric luminosity is seen to be approximately constant and close to Eddington from day 45 up to day 60, the subsequent decline possibly signaling the end of extensive nuclear burning. Before the decline, a multiply-periodic similar to 35 s modulation of the soft X-rays was present and may be the signature of a nuclear fusion driven instability. Our measurements are consistent with a WD mass near the Chandrasekhar limit; combined with a deduced accumulation of mass transferred from its binary companion, this leads us to suggest that RS Oph is a strong candidate for a future supernova explosion. The main uncertainty now is whether the WD is the CO type necessary for a Type Ia supernova. This may be confirmed by detailed abundance analyses of spectroscopic data from the outbursts.
C1 [Osborne, J. P.; Page, K. L.; Beardmore, A. P.; Goad, M. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Bode, M. F.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[O'Brien, T. J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England.
[Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Ness, J. -U.] ESAC, XMM Newton Sci Operat Ctr, Madrid 28691, Spain.
[Krautter, J.] Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany.
[Schwarz, G.] Amer Astron Soc, Washington, DC 20009 USA.
[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.
[Drake, J. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Evans, A.] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
[Eyres, S. P. S.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
RP Osborne, JP (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM julo@star.le.ac.uk
RI Gehrels, Neil/D-2971-2012
FU STFC; NSF; NASA; German Aerospace Center (DLR) [05 OR 0806]
FX We thank the Swift Science Team and the Swift Mission Operations Team
for their excellent support of this observing campaign. J.O., K. P., M.
G., A. B., and M. F. B. acknowledge the support of STFC. S. S.
acknowledges partial support to ASU from NSF and NASA. T. R. is
supported by the German Aerospace Center (DLR) under grant 05 OR 0806.
The authors are grateful to John Nousek for his helpful comments on an
initial draft of this paper and to Simon Vaughan for providing the TCL
"shakefit" procedure.
NR 79
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 124
DI 10.1088/0004-637X/727/2/124
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000063
ER
PT J
AU Roy, A
Ade, PAR
Bock, JJ
Chapin, EL
Devlin, MJ
Dicker, SR
France, K
Gibb, AG
Griffin, M
Gundersen, JO
Halpern, M
Hargrave, PC
Hughes, DH
Klein, J
Marsden, G
Martin, PG
Mauskopf, P
Ortiz, JLM
Netterfield, CB
Noriega-Crespo, A
Olmi, L
Patanchon, G
Rex, M
Scott, D
Semisch, C
Truch, MDP
Tucker, C
Tucker, GS
Viero, MP
Wiebe, DV
AF Roy, Arabindo
Ade, Peter A. R.
Bock, James J.
Chapin, Edward L.
Devlin, Mark J.
Dicker, Simon R.
France, Kevin
Gibb, Andrew G.
Griffin, Matthew
Gundersen, Joshua O.
Halpern, Mark
Hargrave, Peter C.
Hughes, David H.
Klein, Jeff
Marsden, Gaelen
Martin, Peter G.
Mauskopf, Philip
Ortiz, Jorge L. Morales
Netterfield, Calvin B.
Noriega-Crespo, Alberto
Olmi, Luca
Patanchon, Guillaume
Rex, Marie
Scott, Douglas
Semisch, Christopher
Truch, Matthew D. P.
Tucker, Carole
Tucker, Gregory S.
Viero, Marco P.
Wiebe, Donald V.
TI THE BALLOON-BORNE LARGE APERTURE SUBMILLIMETER TELESCOPE (BLAST) 2005: A
10 deg(2) SURVEY OF STAR FORMATION IN CYGNUS X
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE balloons; ISM: clouds; stars: formation; stars: massive; submillimeter:
general
ID YOUNG STELLAR OBJECTS; GALACTIC PLANE SURVEY; COMPACT HII-REGIONS; H-II
REGIONS; MASSIVE STARS; MOLECULAR CLOUDS; FORMING REGION; MILKY-WAY;
MILLIMETER CONTINUUM; INTERSTELLAR-MEDIUM
AB We present Cygnus X in a new multi-wavelength perspective based on an unbiased BLAST survey at 250, 350, and 500 mu m, combined with rich data sets for this well-studied region. Our primary goal is to investigate the early stages of high-mass star formation. We have detected 184 compact sources in various stages of evolution across all three BLAST bands. From their well-constrained spectral energy distributions, we obtain the physical properties mass, surface density, bolometric luminosity, and dust temperature. Some of the bright sources reaching 40 K contain well-known compact H II regions. We relate these to other sources at earlier stages of evolution via the energetics as deduced from their position in the luminosity-mass (L-M) diagram. The BLAST spectral coverage, near the peak of the spectral energy distribution of the dust, reveals fainter sources too cool (similar to 10 K) to be seen by earlier shorter-wavelength surveys like IRAS. We detect thermal emission from infrared dark clouds and investigate the phenomenon of cold "starless cores" more generally. Spitzer images of these cold sources often show stellar nurseries, but these potential sites for massive star formation are "starless" in the sense that to date there is no massive protostar in a vigorous accretion phase. We discuss evolution in the context of the L-M diagram. Theory raises some interesting possibilities: some cold massive compact sources might never form a cluster containing massive stars, and clusters with massive stars might not have an identifiable compact cold massive precursor.
C1 [Roy, Arabindo; Netterfield, Calvin B.; Viero, Marco P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Ade, Peter A. R.; Griffin, Matthew; Hargrave, Peter C.; Mauskopf, Philip; Tucker, Carole] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Bock, James J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, James J.; Viero, Marco P.] CALTECH, Pasadena, CA 91125 USA.
[Chapin, Edward L.; Gibb, Andrew G.; Halpern, Mark; Marsden, Gaelen; Scott, Douglas; Wiebe, Donald V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Devlin, Mark J.; Dicker, Simon R.; Klein, Jeff; Semisch, Christopher; Truch, Matthew D. P.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[France, Kevin] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO USA.
[Gundersen, Joshua O.] Univ Miami, Dept Phys, Carol Gables, FL 33146 USA.
[Hughes, David H.] INAOE, Puebla, Mexico.
[Martin, Peter G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto M58 3H8, ON, Canada.
[Ortiz, Jorge L. Morales; Olmi, Luca] Univ Puerto Rico, Dept Phys, San Juan, PR 00936 USA.
[Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Noriega-Crespo, Alberto] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Olmi, Luca] Ist Radioastron, I-50125 Florence, Italy.
[Patanchon, Guillaume] Lab APC, F-75205 Paris, France.
[Rex, Marie] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Tucker, Gregory S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
RP Roy, A (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
EM aroy@cita.utoronto.ca
RI Klein, Jeffrey/E-3295-2013;
OI Olmi, Luca/0000-0002-1162-7947
FU NASA [NAG5-12785, NAG5-13301, NNGO-6GI11G]; Canadian Space Agency (CSA);
UK Particle Physics & Astronomy Research Council (PPARC); Canada's
Natural Sciences and Engineering Research Council (NSERC)
FX The BLAST collaboration acknowledges the support of NASA through grant
numbers NAG5-12785, NAG5-13301, and NNGO-6GI11G, the Canadian Space
Agency (CSA), the UK Particle Physics & Astronomy Research Council
(PPARC), and Canada's Natural Sciences and Engineering Research Council
(NSERC). We would also thank the Columbia Scientific Balloon Facility
(CSBF) staff for their outstanding work.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 114
DI 10.1088/0004-637X/727/2/114
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000053
ER
PT J
AU Shabram, M
Fortney, JJ
Greene, TP
Freedman, RS
AF Shabram, Megan
Fortney, Jonathan J.
Greene, Thomas P.
Freedman, Richard S.
TI TRANSMISSION SPECTRA OF TRANSITING PLANET ATMOSPHERES: MODEL VALIDATION
AND SIMULATIONS OF THE HOT NEPTUNE GJ 436b FOR THE JAMES WEBB SPACE
TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; radiative transfer; stars: individual (GJ 436, HD
209458)
ID EXTRASOLAR GIANT PLANETS; MASS DWARF STARS; HD 189733B; MU-M; BROWN
DWARFS; SYNTHETIC SPECTRA; SUPER-EARTHS; T-DWARFS; WATER; SPITZER
AB We explore the transmission spectrum of the Neptune-class exoplanet GJ 436b, including the possibility that its atmospheric opacity is dominated by a variety of nonequilibrium chemical products. We also validate our transmission code by demonstrating close agreement with analytic models that use only Rayleigh scattering or water vapor opacity. We find broad disagreement with radius variations predicted by another published model. For GJ 436b, the relative coolness of the planet's atmosphere, along with its implied high metallicity, may make it dissimilar in character compared to "hot Jupiters." Some recent observational and modeling efforts suggest low relative abundances of H2O and CH4 present in GJ 436b's atmosphere, compared to calculations from equilibrium chemistry. We include these characteristics in our models and examine the effects of absorption from methane-derived higher-order hydrocarbons. To our knowledge, the effects of these nonequilibrium chemical products on the spectra of close-in giant planets have not previously been investigated. Significant absorption from HCN and C2H2 is found throughout the infrared, while C2H4 and C2H6 are less easily seen. We perform detailed simulations of James Webb Space Telescope observations, including all likely noise sources, and find that we will be able to constrain chemical abundance regimes from this planet's transmission spectrum. For instance, the width of the features at 1.5, 3.3, and 7 mu m indicates the amount of HCN versus C2H2 present. The NIRSpec prism mode will be useful due to its large spectral range and the relatively large number of photo-electrons recorded per spectral resolution element. However, extremely bright host stars like GJ 436 may be better observed with a higher spectroscopic resolution mode in order to avoid detector saturation. We find that observations with the MIRI low-resolution spectrograph should also have high signal-to-noise in the 5-10 mu m range due to the brightness of the star and the relatively low spectral resolution (R similar to 100) of this mode.
C1 [Shabram, Megan] Univ Florida, Dept Astron, Bryant Space Ctr 211, Gainesville, FL 32611 USA.
[Shabram, Megan; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Greene, Thomas P.; Freedman, Richard S.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Freedman, Richard S.] SETI Inst, Mountain View, CA 94043 USA.
RP Shabram, M (reprint author), Univ Florida, Dept Astron, Bryant Space Ctr 211, Gainesville, FL 32611 USA.
OI Fortney, Jonathan/0000-0002-9843-4354
FU Spitzer Theory Program; University Affiliated Research Center (UARC);
JWST NIRCam instrument [NASA WBS 411672.05.05.02.02]
FX We thank Jean-Michel Desert, David Sing, David Spiegel, Alain Lecavelier
des Etangs, Mark Marley, Heather Knutson, and Adam Burrows for useful
discussions, and Eliza Kempton, Travis Barman, and Nikku Madhusudhan for
discussions and the sharing of model results. J.J.F. and M.S.
acknowledge the support of the Spitzer Theory Program and a University
Affiliated Research Center (UARC) Aligned Research Program (ARP) grant.
UARC is a partnership between University of California, Santa Cruz and
NASA Ames Research Center. T.P.G. acknowledges support from the JWST
NIRCam instrument, NASA WBS 411672.05.05.02.02.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 65
DI 10.1088/0004-637X/727/2/65
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000004
ER
PT J
AU Usmanov, AV
Matthaeus, WH
Breech, BA
Goldstein, ML
AF Usmanov, Arcadi V.
Matthaeus, William H.
Breech, Benjamin A.
Goldstein, Melvyn L.
TI SOLAR WIND MODELING WITH TURBULENCE TRANSPORT AND HEATING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); methods: numerical; solar wind; turbulence
ID INTERSTELLAR PICKUP PROTONS; WHOLE SUN MONTH; ALFVEN WAVES;
MAGNETIC-FIELD; MHD TURBULENCE; MAGNETOHYDRODYNAMIC SIMULATIONS; PLASMA
OBSERVATIONS; SPATIAL TRANSPORT; OUTER HELIOSPHERE; CONSERVATION-LAWS
AB We have developed 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 equations coupled with a set of small-scale transport equations for the turbulence energy, normalized cross helicity, and correlation scale. The combined set of time-dependent equations is solved in the frame of reference corotating with the Sun using a time-relaxation method. We use the model to study the self-consistent interaction between the large-scale solar wind and smaller-scale turbulence and the role of the turbulence in the large-scale structure and temperature distribution in the solar wind. To illuminate the roles of the turbulent cascade and the pickup protons in heating the solar wind depending on the heliocentric distance, we compare the model results with and without turbulence/pickup protons. The variations of plasma temperature in the outer heliosphere are compared with Ulysses and Voyager 2 observations.
C1 [Usmanov, Arcadi V.; Breech, Benjamin A.] NASA, Goddard Space Flight Ctr, Postdoctoral Program, Greenbelt, MD 20771 USA.
[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.
RP Usmanov, AV (reprint author), NASA, Goddard Space Flight Ctr, Postdoctoral Program, Code 673, Greenbelt, MD 20771 USA.
EM arcadi.usmanov@nasa.gov
RI Goldstein, Melvyn/B-1724-2008; Usmanov, Arcadi/A-9860-2013
FU NASA [NNG06GE65G, NNX09AH79G, NNX08AI47G]; NSF [ATM-0539995]; NASA
Advanced Supercomputing (NAS) Division at the Ames Research Center; NASA
Center for Computational Sciences (NCCS) at the Goddard Space Flight
Center
FX We acknowledge the use of Ulysses and Voyager 2 data supplied by the
National Space Science Data Center. The work of A.V.U. was supported by
NASA grants NNG06GE65G and NNX09AH79G to the University of Delaware.
W.H.M. was partially supported by the NASA Heliophysics Theory Program
NNX08AI47G and by the NSF Solar Terrestrial Program ATM-0539995.
B.A.B.'s research was supported by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center. Resources
supporting this work were provided by the NASA High-End Computing (HEC)
Program through the NASA Advanced Supercomputing (NAS) Division at the
Ames Research Center and the NASA Center for Computational Sciences
(NCCS) at the Goddard Space Flight Center.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 84
DI 10.1088/0004-637X/727/2/84
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000023
ER
PT J
AU Virgili, FJ
Zhang, B
O'Brien, P
Troja, E
AF Virgili, Francisco J.
Zhang, Bing
O'Brien, Paul
Troja, Eleonora
TI ARE ALL SHORT-HARD GAMMA-RAY BURSTS PRODUCED FROM MERGERS OF COMPACT
STELLAR OBJECTS?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: miscellaneous; gamma-ray burst: general; methods: statistical
ID NEUTRON-STAR MERGERS; SHORT-DURATION GRBS; HOST GALAXIES; REDSHIFT
DISTRIBUTIONS; BLACK-HOLES; LOCAL-RATE; AFTERGLOW; LUMINOSITY; BINARY;
ORIGIN
AB The origin and progenitors of short-hard gamma-ray bursts (GRBs) remain a puzzle and a highly debated topic. Recent Swift observations suggest that these GRBs may be related to catastrophic explosions in degenerate compact stars, denoted as "Type I" GRBs. The most popular models include the merger of two compact stellar objects (NS-NS or NS-BH). We utilize a Monte Carlo approach to determine whether a merger progenitor model can self-consistently account for all the observations of short-hard GRBs, including a sample with redshift measurements in the Swift era (z-known sample) and the CGRO/BATSE sample. We apply various merger time delay distributions invoked in compact star merger models to derive the redshift distributions of these Type I GRBs, and then constrain the unknown luminosity function of Type I GRBs using the observed luminosity-redshift (L-z) distributions of the z-known sample. The best luminosity function model, together with the adopted merger delay model, is then applied to confront the peak flux distribution (log N-log P distribution) of the BATSE and Swift samples. We find that for all the merger models invoking a range of merger delay timescales (including those invoking a large fraction of "prompt mergers"), it is difficult to reconcile the models with all the data. The data are instead statistically consistent with the following two possible scenarios. First, that short/hard GRBs are a superposition of compact-star-merger-origin (Type I) GRBs and a population of GRBs that track the star formation history, which are probably related to the deaths of massive stars (Type II GRBs). Second, the entire short/hard GRB population is consistent with a typical delay of 2 Gyr with respect to the star formation history with modest scatter. This may point toward a different Type I progenitor than the traditional compact star merger models.
C1 [Virgili, Francisco J.; Zhang, Bing] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
[O'Brien, Paul] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Troja, Eleonora] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Virgili, FJ (reprint author), Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
EM virgilif@physics.unlv.edu; zhang@physics.unlv.edu
FU NSF [AST-0908362]; NASA [NNG05GB67G, NNX09AO94G, NNX08AE57A,
NNX09AT66G]; Nevada EPSCoR; NASA at the GSFC
FX This work was partially supported by NSF under grant AST-0908362, and by
NASA under grants NNG05GB67G, NNX09AO94G, NNX08AE57A, NNX09AT66G, and
through the Nevada EPSCoR program (Nevada Space Grant). E. T. was
supported by an appointment to the NASA Postdoctoral Program at the
GSFC, administered by Oak Ridge Associated Universities through a
contract with NASA. We also thank Chris Belczynski for providing the
redshift distribution data of NS-NS and NS-BH merger events from his
population synthesis code, and Rob Preece, Josh Bloom, Rachid Ouyed, and
Amei Amei for helpful discussions and comments.
NR 95
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2011
VL 727
IS 2
AR 109
DI 10.1088/0004-637X/727/2/109
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 712JE
UT WOS:000286662000048
ER
PT J
AU de Marcellus, P
Meinert, C
Nuevo, M
Filippi, JJ
Danger, G
Deboffle, D
Nahon, L
d'Hendecourt, LLS
Meierhenrich, UJ
AF de Marcellus, Pierre
Meinert, Cornelia
Nuevo, Michel
Filippi, Jean-Jacques
Danger, Gregoire
Deboffle, Dominique
Nahon, Laurent
d'Hendecourt, Louis Le Sergeant
Meierhenrich, Uwe J.
TI NON-RACEMIC AMINO ACID PRODUCTION BY ULTRAVIOLET IRRADIATION OF ACHIRAL
INTERSTELLAR ICE ANALOGS WITH CIRCULARLY POLARIZED LIGHT
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrobiology; astrochemistry; comets: general; ISM: molecules;
meteorites, meteors, meteoroids; Online-only material: color figures
ID STAR-FORMATION REGIONS; EARLY SOLAR-SYSTEM; MURCHISON METEORITE;
UV-IRRADIATION; ORIGIN; HOMOCHIRALITY; PHOTOLYSIS; DISCOVERY; ISOVALINE;
CHIRALITY
AB The delivery of organic matter to the primitive Earth via comets and meteorites has long been hypothesized to be an important source for prebiotic compounds such as amino acids or their chemical precursors that contributed to the development of prebiotic chemistry leading, on Earth, to the emergence of life. Photochemistry of inter/circumstellar ices around protostellar objects is a potential process leading to complex organic species, although difficult to establish from limited infrared observations only. Here we report the first abiotic cosmic ice simulation experiments that produce species with enantiomeric excesses (e.e.'s). Circularly polarized ultraviolet light (UV-CPL) from a synchrotron source induces asymmetric photochemistry on initially achiral inter/circumstellar ice analogs. Enantioselective multidimensional gas chromatography measurements show significant e.e.'s of up to 1.34% for (C-13)-alanine, for which the signs and absolute values are related to the helicity and number of CPL photons per deposited molecule. This result, directly comparable with some L excesses measured in meteorites, supports a scenario in which exogenous delivery of organics displaying a slight L excess, produced in an extraterrestrial environment by an asymmetric astrophysical process, is at the origin of biomolecular asymmetry on Earth. As a consequence, a fraction of the meteoritic organic material consisting of non-racemic compounds may well have been formed outside the solar system. Finally, following this hypothesis, we support the idea that the protosolar nebula has indeed been formed in a region of massive star formation, regions where UV-CPL of the same helicity is actually observed over large spatial areas.
C1 [de Marcellus, Pierre; Nuevo, Michel; Danger, Gregoire; Deboffle, Dominique; d'Hendecourt, Louis Le Sergeant] Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France.
[Meinert, Cornelia; Filippi, Jean-Jacques; Meierhenrich, Uwe J.] Univ Nice Sophia Antipolis, Lab Chim Mol Bioact & Aromes, UMR 6001, F-06108 Nice, France.
[Nuevo, Michel] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Danger, Gregoire] Univ Aix Marseille 1, Lab Phys Interact Ion & Mol, UMR 6633, F-13393 Marseille, France.
[Nahon, Laurent] Synchrotron SOLEIL, F-91192 Gif Sur Yvette, France.
[d'Hendecourt, Louis Le Sergeant] CNRS, F-91405 Orsay, France.
RP d'Hendecourt, LLS (reprint author), Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France.
EM laurent.nahon@synchrotron-soleil.fr; ldh@ias.u-psud.fr
RI Meierhenrich, Uwe/A-1643-2008
OI Meierhenrich, Uwe/0000-0001-6422-3930
FU French CNES; Agence Nationale de la Recherche [ANR-07-BLAN-0293]
FX This experimental study was initially proposed in 2001 by the late
Professor Dr. J.M. Greenberg. L.L.S.H. thanks the French CNES for
support to the Chiral-MICMOC experiment. We gratefully acknowledge Dr.
L.J. Allamandola for significant improvements on this manuscript. We are
indebted to the general technical staff of the SOLEIL facility as well
as to G. Garcia and N. De Oliveira, beamline scientists on DESIRS. We
are grateful to J.-F. Gil for technical help in implementing the MICMOC
chamber on the DESIRS beamline. This work was also supported by the
Agence Nationale de la Recherche (ANR-07-BLAN-0293).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
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AR L27
DI 10.1088/2041-8205/727/2/L27
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706DB
UT WOS:000286196200027
ER
PT J
AU Guiriec, S
Connaughton, V
Briggs, MS
Burgess, M
Ryde, F
Daigne, F
Meszaros, P
Goldstein, A
McEnery, J
Omodei, N
Bhat, PN
Bissaldi, E
Camero-Arranz, A
Chaplin, V
Diehl, R
Fishman, G
Foley, S
Gibby, M
Giles, MM
Greiner, J
Gruber, D
von Kienlin, A
Kippen, M
Kouveliotou, C
McBreen, S
Meegan, CA
Paciesas, W
Preece, R
Rau, A
Tierney, D
van der Horst, AJ
Wilson-Hodge, C
AF Guiriec, Sylvain
Connaughton, Valerie
Briggs, Michael S.
Burgess, Michael
Ryde, Felix
Daigne, Frederic
Meszaros, Peter
Goldstein, Adam
McEnery, Julie
Omodei, Nicola
Bhat, P. N.
Bissaldi, Elisabetta
Camero-Arranz, Ascension
Chaplin, Vandiver
Diehl, Roland
Fishman, Gerald
Foley, Suzanne
Gibby, Melissa
Giles, Misty M.
Greiner, Jochen
Gruber, David
von Kienlin, Andreas
Kippen, Marc
Kouveliotou, Chryssa
McBreen, Sheila
Meegan, Charles A.
Paciesas, William
Preece, Robert
Rau, Arne
Tierney, Dave
van der Horst, Alexander J.
Wilson-Hodge, Colleen
TI DETECTION OF A THERMAL SPECTRAL COMPONENT IN THE PROMPT EMISSION OF GRB
100724B
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; gamma-ray burst: individual (GRB 1000724B);
gamma rays: stars; radiation mechanisms: non-thermal; radiation
mechanisms: thermal
ID GAMMA-RAY-BURSTS; FERMI OBSERVATIONS; BATSE OBSERVATIONS; SHOCK MODEL;
BRIGHT; SPECTROSCOPY; EVOLUTION; CATALOG; MONITOR
AB Observations of GRB 100724B with the Fermi Gamma-Ray Burst Monitor find that the spectrum is dominated by the typical Band functional form, which is usually taken to represent a non-thermal emission component, but also includes a statistically highly significant thermal spectral contribution. The simultaneous observation of the thermal and non-thermal components allows us to confidently identify the two emission components. The fact that these seem to vary independently favors the idea that the thermal component is of photospheric origin while the dominant non-thermal emission occurs at larger radii. Our results imply either a very high efficiency for the non-thermal process or a very small size of the region at the base of the flow, both quite challenging for the standard fireball model. These problems are resolved if the jet is initially highly magnetized and has a substantial Poynting flux.
C1 [Guiriec, Sylvain; Connaughton, Valerie; Briggs, Michael S.; Burgess, Michael; Goldstein, Adam; Bhat, P. N.; Chaplin, Vandiver; Paciesas, William; Preece, Robert] Univ Alabama, NSSTC, Huntsville, AL 35805 USA.
[Ryde, Felix] Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden.
[Ryde, Felix] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden.
[Daigne, Frederic] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France.
[Meszaros, Peter] Penn State Univ, Dept Astron & Astrophys, Dept Phys, University Pk, PA 16802 USA.
[Meszaros, Peter] Penn State Univ, Ctr Particle Astrophys, University Pk, PA 16802 USA.
[McEnery, Julie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McEnery, Julie] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, Julie] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Omodei, Nicola] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bissaldi, Elisabetta; Diehl, Roland; Foley, Suzanne; Greiner, Jochen; Gruber, David; von Kienlin, Andreas; Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Camero-Arranz, Ascension] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Fishman, Gerald; Kouveliotou, Chryssa; Wilson-Hodge, Colleen] NASA, George C Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA.
[Gibby, Melissa; Giles, Misty M.] Jacobs Technol Inc, Huntsville, AL USA.
[Kippen, Marc] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[McBreen, Sheila; Tierney, Dave] Univ Coll Dublin, Dublin 4, Ireland.
[Meegan, Charles A.] NSSTC, Univ Space Res Assoc, Huntsville, AL 35805 USA.
[van der Horst, Alexander J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
RP Guiriec, S (reprint author), Univ Alabama, NSSTC, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM sylvain.guiriec@nasa.gov
RI McEnery, Julie/D-6612-2012; Bissaldi, Elisabetta/K-7911-2016;
OI Bissaldi, Elisabetta/0000-0001-9935-8106; Preece,
Robert/0000-0003-1626-7335; Omodei, Nicola/0000-0002-5448-7577
FU German Bundesministerium fur Wirtschaft und Technologie (BMWi) via the
Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [50 QV 0301, 50 OG
0502]; NASA [NNX08AL40G]; Irish Research Council for Science,
Engineering and Technology; Marie Curie Actions; Swedish National Space
Board
FX The GBM project is supported by the German Bundesministerium fur
Wirtschaft und Technologie (BMWi) via the Deutsches Zentrum fur Luft-
und Raumfahrt (DLR) under the contract numbers 50 QV 0301 and 50 OG
0502. A. J. v. d. H. was supported by an appointment to the NASA
Postdoctoral Program at the MSFC, administered by Oak Ridge Associated
Universities through a contract with NASA. S. F. acknowledges the
support of the Irish Research Council for Science, Engineering and
Technology, cofunded by Marie Curie Actions under FP7. P. M.
acknowledges the support of NASA NNX08AL40G. F. R. acknowledges the
support of the Swedish National Space Board.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
PY 2011
VL 727
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AR L33
DI 10.1088/2041-8205/727/2/L33
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706DB
UT WOS:000286196200006
ER
PT J
AU Wilson-Hodge, CA
Cherry, ML
Case, GL
Baumgartner, WH
Beklen, E
Bhat, PN
Briggs, MS
Camero-Arranz, A
Chaplin, V
Connaughton, V
Finger, MH
Gehrels, N
Greiner, J
Jahoda, K
Jenke, P
Kippen, RM
Kouveliotou, C
Krimm, HA
Kuulkers, E
Lund, N
Meegan, CA
Natalucci, L
Paciesas, WS
Preece, R
Rodi, JC
Shaposhnikov, N
Skinner, GK
Swartz, D
von Kienlin, A
Diehl, R
Zhang, XL
AF Wilson-Hodge, Colleen A.
Cherry, Michael L.
Case, Gary L.
Baumgartner, Wayne H.
Beklen, Elif
Bhat, P. Narayana
Briggs, Michael S.
Camero-Arranz, Ascension
Chaplin, Vandiver
Connaughton, Valerie
Finger, Mark H.
Gehrels, Neil
Greiner, Jochen
Jahoda, Keith
Jenke, Peter
Kippen, R. Marc
Kouveliotou, Chryssa
Krimm, Hans A.
Kuulkers, Erik
Lund, Niels
Meegan, Charles A.
Natalucci, Lorenzo
Paciesas, William S.
Preece, Robert
Rodi, James C.
Shaposhnikov, Nikolai
Skinner, Gerald K.
Swartz, Doug
von Kienlin, Andreas
Diehl, Roland
Zhang, Xiao-Ling
TI WHEN A STANDARD CANDLE FLICKERS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE pulsars: individual (Crab Pulsar); X-rays: individual (Crab Nebula)
ID X-RAY-EMISSION; CRAB-NEBULA; BURST MONITOR; SYNCHROTRON NEBULA;
TIMING-EXPLORER; PULSAR; TELESCOPE; CALIBRATION; WISPS; VARIABILITY
AB The Crab Nebula is the only hard X-ray source in the sky that is both bright enough and steady enough to be easily used as a standard candle. As a result, it has been used as a normalization standard by most X-ray/gamma-ray telescopes. Although small-scale variations in the nebula are well known, since the start of science operations of the Fermi Gamma-ray Burst Monitor (GBM) in 2008 August, a similar to 7% (70 mCrab) decline has been observed in the overall Crab Nebula flux in the 15-50 keV band, measured with the Earth occultation technique. This decline is independently confirmed in the similar to 15-50 keV band with three other instruments: the Swift Burst Alert Telescope (Swift/BAT), the Rossi X-ray Timing Explorer Proportional Counter Array (RXTE/PCA), and the Imager on-Board the INTEGRAL Satellite (IBIS). A similar decline is also observed in the similar to 3-15 keV data from the RXTE/PCA and in the 50-100 keV band with GBM, Swift/BAT, and INTEGRAL/IBIS. The pulsed flux measured with RXTE/PCA since 1999 is consistent with the pulsar spin-down, indicating that the observed changes are nebular. Correlated variations in the Crab Nebula flux on a similar to 3 year timescale are also seen independently with the PCA, BAT, and IBIS from 2005 to 2008, with a flux minimum in 2007 April. As of 2010 August, the current flux has declined below the 2007 minimum.
C1 [Wilson-Hodge, Colleen A.; Jenke, Peter; Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, VP Space Sci Off 62, Huntsville, AL 35812 USA.
[Cherry, Michael L.; Case, Gary L.; Rodi, James C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Baumgartner, Wayne H.; Krimm, Hans A.; Shaposhnikov, Nikolai; Skinner, Gerald K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, CRESST, Greenbelt, MD 20771 USA.
[Beklen, Elif] Middle E Tech Univ, Dept Phys, TR-06531 Ankara, Turkey.
[Beklen, Elif] Suleyman Demirel Univ, Dept Phys, TR-32260 Isparta, Turkey.
[Bhat, P. Narayana; Briggs, Michael S.; Chaplin, Vandiver; Connaughton, Valerie; Paciesas, William S.; Preece, Robert] Univ Alabama, Huntsville, AL 35899 USA.
[Camero-Arranz, Ascension] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Finger, Mark H.; Meegan, Charles A.; Swartz, Doug] Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Greiner, Jochen; von Kienlin, Andreas; Diehl, Roland; Zhang, Xiao-Ling] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kippen, R. Marc] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Krimm, Hans A.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Kuulkers, Erik] ESAC, ESA, ISOC, Villanueva De La Canada 28691, Madrid, Spain.
[Lund, Niels] Tech Univ Denmark, Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark.
[Natalucci, Lorenzo] INAF IASF Roma, I-00133 Rome, Italy.
[Shaposhnikov, Nikolai; Skinner, Gerald K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Wilson-Hodge, CA (reprint author), NASA, George C Marshall Space Flight Ctr, VP Space Sci Off 62, Huntsville, AL 35812 USA.
EM colleen.wilson@nasa.gov
RI Gehrels, Neil/D-2971-2012; Jahoda, Keith/D-5616-2012;
OI Preece, Robert/0000-0003-1626-7335
FU NASA [NNX07AT62A]; Louisiana Board of Regents Graduate Fellowship
Program; Spanish Ministerio de Ciencia e Innovacion [2008-0116]; ESA
FX This work is supported by the NASA Fermi Guest Investigator program,
NASA/Louisiana Board of Regents Cooperative Agreement NNX07AT62A (LSU),
the Louisiana Board of Regents Graduate Fellowship Program (J.C.R.), and
the Spanish Ministerio de Ciencia e Innovacion through the 2008
postdoctoral program MICINN/Fulbright under grant 2008-0116 (A.C.-A.).
This research has made use of data obtained through the High Energy
Astrophysics Science Archive Research Center Online Service, provided by
the NASA/Goddard Space Flight Center; public Swift/BAT results made
available by the Swift/BAT team; and observations with INTEGRAL, an ESA
project funded by ESA member states (especially the PI countries:
Denmark, France, Germany, Italy, Switzerland, Spain) and Poland, and
with the participation of Russia and the USA.
NR 50
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
PY 2011
VL 727
IS 2
AR L40
DI 10.1088/2041-8205/727/2/L40
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706DB
UT WOS:000286196200013
ER
PT J
AU Jarosik, N
Bennett, CL
Dunkley, J
Gold, B
Greason, MR
Halpern, M
Hill, RS
Hinshaw, G
Kogut, A
Komatsu, E
Larson, D
Limon, M
Meyer, SS
Nolta, MR
Odegard, N
Page, L
Smith, KM
Spergel, DN
Tucker, GS
Weiland, JL
Wollack, E
Wright, EL
AF Jarosik, N.
Bennett, C. L.
Dunkley, J.
Gold, B.
Greason, M. R.
Halpern, M.
Hill, R. S.
Hinshaw, G.
Kogut, A.
Komatsu, E.
Larson, D.
Limon, M.
Meyer, S. S.
Nolta, M. R.
Odegard, N.
Page, L.
Smith, K. M.
Spergel, D. N.
Tucker, G. S.
Weiland, J. L.
Wollack, E.
Wright, E. L.
TI SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: SKY
MAPS, SYSTEMATIC ERRORS, AND BASIC RESULTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic background radiation; space vehicles: instruments
ID WINDOW FUNCTIONS; POWER SPECTRUM; BEAM PROFILES; DESIGN; POLARIZATION;
LIMITS
AB New full-sky temperature and polarization maps based on seven years of data from WMAP are presented. The new results are consistent with previous results, but have improved due to reduced noise from the additional integration time, improved knowledge of the instrument performance, and improved data analysis procedures. The improvements are described in detail. The seven-year data set is well fit by a minimal six-parameter flat Lambda CDM model. The parameters for this model, using the WMAP data in conjunction with baryon acoustic oscillation data from the Sloan Digital Sky Survey and priors on H-0 from Hubble Space Telescope observations, are Omega(b)h(2) = 0.02260 +/- 0.00053, Omega(c)h(2) = 0.1123 +/- 0.0035, Omega(Lambda) = 0.728(-0.016)(+0.015), n(s) = 0.963 +/- 0.012, tau = 0.087 +/- 0.014, and sigma(8) = 0.809 +/- 0.024 (68% CL uncertainties). The temperature power spectrum signal-to-noise ratio per multipole is greater that unity for multipoles l less than or similar to 919, allowing a robust measurement of the third acoustic peak. This measurement results in improved constraints on the matter density, Omega(m)h(2) = 0.1334(-0.0055)(+0.0056), and the epoch of matter-radiation equality, z(eq) = 3196(-133)(+134), using WMAP data alone. The new WMAP data, when combined with smaller angular scale microwave background anisotropy data, result in a 3 sigma detection of the abundance of primordial helium, Y-He = 0.326 +/- 0.075. When combined with additional external data sets, the WMAP data also yield better determinations of the total mass of neutrinos, Sigma m(nu) <= 0.58 eV (95% CL), and the effective number of neutrino species, N-eff = 4.34(-0.88)(+0.86). The power-law index of the primordial power spectrum is now determined to be n(s) = 0.963 +/- 0.012, excluding the Harrison-Zel'dovich-Peebles spectrum by >3 sigma. These new WMAP measurements provide important tests of big bang cosmology.
C1 [Jarosik, N.; Page, L.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Bennett, C. L.; Gold, B.; Larson, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Dunkley, J.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Greason, M. R.; Hill, R. S.; Odegard, N.; Weiland, J. L.] ADNET Syst Inc, Lanham, MD 20706 USA.
[Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hinshaw, G.; Kogut, A.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Meyer, S. S.] Univ Chicago, Dept Astrophys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, Dept Phys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, EFI, Chicago, IL 60637 USA.
[Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Smith, K. M.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Spergel, D. N.] Princeton Univ, Princeton Ctr Theoret Phys, Princeton, NJ 08544 USA.
[Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Wright, E. L.] UCLA Phys & Astron, Los Angeles, CA 90095 USA.
RP Jarosik, N (reprint author), Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA.
RI Komatsu, Eiichiro/A-4361-2011; Spergel, David/A-4410-2011; Wollack,
Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698
FU Science Mission Directorate Office at NASA Headquarters
FX WMAP is funded by the Science Mission Directorate Office at NASA
Headquarters. We acknowledge the use of the HEALPix (Gorski et al. 2005)
software package. The numerous data products described in this document
are available from the Legacy Archive for Microwave Background Data
Analysis (LAMBDA): http://lambda.gsfc.nasa.gov.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD FEB
PY 2011
VL 192
IS 2
BP 1
EP 15
AR 14
DI 10.1088/0067-0049/192/2/14
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706BL
UT WOS:000286189700001
ER
PT J
AU Bennett, CL
Hill, RS
Hinshaw, G
Larson, D
Smith, KM
Dunkley, J
Gold, B
Halpern, M
Jarosik, N
Kogut, A
Komatsu, E
Limon, M
Meyer, SS
Nolta, MR
Odegard, N
Page, L
Spergel, DN
Tucker, GS
Weiland, JL
Wollack, E
Wright, EL
AF Bennett, C. L.
Hill, R. S.
Hinshaw, G.
Larson, D.
Smith, K. M.
Dunkley, J.
Gold, B.
Halpern, M.
Jarosik, N.
Kogut, A.
Komatsu, E.
Limon, M.
Meyer, S. S.
Nolta, M. R.
Odegard, N.
Page, L.
Spergel, D. N.
Tucker, G. S.
Weiland, J. L.
Wollack, E.
Wright, E. L.
TI SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: ARE
THERE COSMIC MICROWAVE BACKGROUND ANOMALIES?
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic background radiation; cosmological parameters; cosmology:
observations; dark matter; early universe; instrumentation: detectors;
large-scale structure of universe; space vehicles; space vehicles:
instruments; telescopes
ID OBSERVATIONS COSMOLOGICAL INTERPRETATION; HEMISPHERICAL POWER ASYMMETRY;
LARGE-ANGLE CORRELATIONS; SYSTEMATIC-ERROR LIMITS; GAUSSIAN COLD SPOT;
STATISTICAL ISOTROPY; SKY MAPS; RADIOMETER CHARACTERIZATION;
BAYESIAN-ANALYSIS; SPECTRUM ANALYSIS
AB A simple six-parameter Lambda CDM model provides a successful fit to WMAP data. This holds both when the WMAP data are analyzed alone or in combination with other cosmological data. Even so, it is appropriate to examine the data carefully to search for hints of deviations from the now standard model of cosmology, which includes inflation, dark energy, dark matter, baryons, and neutrinos. The cosmological community has subjected the WMAP data to extensive and varied analyses. While there is widespread agreement as to the overall success of the six-parameter Lambda CDM model, various "anomalies" have been reported relative to that model. In this paper we examine potential anomalies and present analyses and assessments of their significance. In most cases we find that claimed anomalies depend on posterior selection of some aspect or subset of the data. Compared with sky simulations based on the best-fit model, one can select for low probability features of the WMAP data. Low probability features are expected, but it is not usually straightforward to determine whether any particular low probability feature is the result of the a posteriori selection or non-standard cosmology. Hypothesis testing could, of course, always reveal an alternative model that is statistically favored, but there is currently no model that is more compelling. We find that two cold spots in the map are statistically consistent with random cosmic microwave background (CMB) fluctuations. We also find that the amplitude of the quadrupole is well within the expected 95% confidence range and therefore is not anomalously low. We find no significant anomaly with a lack of large angular scale CMB power for the best-fit Lambda CDM model. We examine in detail the properties of the power spectrum data with respect to the Lambda CDM model and find no significant anomalies. The quadrupole and octupole components of the CMB sky are remarkably aligned, but we find that this is not due to any single map feature; it results from the statistical combination of the full-sky anisotropy fluctuations. It may be due, in part, to chance alignments between the primary and secondary anisotropy, but this only shifts the coincidence from within the last scattering surface to between it and the local matter density distribution. While this alignment appears to be remarkable, there was no model that predicted it, nor has there been a model that provides a compelling retrodiction. We examine claims of a hemispherical or dipole power asymmetry across the sky and find that the evidence for these claims is not statistically significant. We confirm the claim of a strong quadrupolar power asymmetry effect, but there is considerable evidence that the effect is not cosmological. The likely explanation is an insufficient handling of beam asymmetries. We conclude that there is no compelling evidence for deviations from the Lambda CDM model, which is generally an acceptable statistical fit to WMAP and other cosmological data.
C1 [Bennett, C. L.; Larson, D.; Gold, B.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hill, R. S.; Odegard, N.; Weiland, J. L.] ADNET Syst Inc, Lanham, MD 20706 USA.
[Hinshaw, G.; Kogut, A.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smith, K. M.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Dunkley, J.] Univ Oxford, Oxford OX1 3RH, England.
[Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Jarosik, N.; Page, L.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Meyer, S. S.] Univ Chicago, Dept Astrophys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, Dept Phys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, EFI, Chicago, IL 60637 USA.
[Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Spergel, D. N.] Princeton Univ, Princeton Ctr Theoret Phys, Princeton, NJ 08544 USA.
[Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Wright, E. L.] UCLA Phys & Astron, Los Angeles, CA 90095 USA.
RP Bennett, CL (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
RI Komatsu, Eiichiro/A-4361-2011; Spergel, David/A-4410-2011; Wollack,
Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698
FU NASA Science Mission Directorate
FX The WMAP mission is made possible by the support of the NASA Science
Mission Directorate. This research has made use of NASA's Astrophysics
Data System Bibliographic Services. We thank Jon Urrestilla for sharing
the texture power spectrum with us. We also acknowledge use of the
HEALPix (Gorski et al. 2005), CAMB (Lewis et al. 2000), and CMBFAST
(Seljak & Zaldarriaga 1996) packages. We are very grateful to Duncan
Hanson for useful discussions.
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JI Astrophys. J. Suppl. Ser.
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SC Astronomy & Astrophysics
GA 706BL
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ER
PT J
AU Gold, B
Odegard, N
Weiland, JL
Hill, RS
Kogut, A
Bennett, CL
Hinshaw, G
Chen, X
Dunkley, J
Halpern, M
Jarosik, N
Komatsu, E
Larson, D
Limon, M
Meyer, SS
Nolta, MR
Page, L
Smith, KM
Spergel, DN
Tucker, GS
Wollack, E
Wright, EL
AF Gold, B.
Odegard, N.
Weiland, J. L.
Hill, R. S.
Kogut, A.
Bennett, C. L.
Hinshaw, G.
Chen, X.
Dunkley, J.
Halpern, M.
Jarosik, N.
Komatsu, E.
Larson, D.
Limon, M.
Meyer, S. S.
Nolta, M. R.
Page, L.
Smith, K. M.
Spergel, D. N.
Tucker, G. S.
Wollack, E.
Wright, E. L.
TI SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS:
GALACTIC FOREGROUND EMISSION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic background radiation; cosmology: observations; diffuse radiation;
Galaxy: halo; Galaxy: structure; ISM: structure
ID NRAO PMN SURVEYS; SPINNING DUST GRAINS; POINT-SOURCE SEARCH; SOURCE
CATALOG; MAPS; SKY; RADIATION; PARAMETERS; PROSPECTS; REGION
AB We present updated estimates of Galactic foreground emission using seven years of WMAP data. Using the power spectrum of differences between multi-frequency template-cleaned maps, we find no evidence for foreground contamination outside of the updated (KQ85y7) foreground mask. We place a 15 mu K upper bound on rms foreground contamination in the cleaned maps used for cosmological analysis. Further, the cleaning process requires only three power-law foregrounds outside of the mask. We find no evidence for polarized foregrounds beyond those from soft (steep-spectrum) synchrotron and thermal dust emission; in particular we find no indication in the polarization data of an extra "haze" of hard synchrotron emission from energetic electrons near the Galactic center. We provide an updated map of the cosmic microwave background (CMB) using the internal linear combination method, updated foreground masks, and updates to point source catalogs using two different techniques. With additional years of data, we now detect 471 point sources using a five-band technique and 417 sources using a three-band CMB-free technique. In total there are 62 newly detected point sources, a 12% increase over the five-year release. Also new are tests of the Markov chain Monte Carlo foreground fitting procedure against systematics in the time-stream data, and tests against the observed beam asymmetry. Within a few degrees of the Galactic plane, the behavior in total intensity of low-frequency foregrounds is complicated and not completely understood. WMAP data show a rapidly steepening spectrum from 20 to 40 GHz, which may be due to emission from spinning dust grains, steepening synchrotron, or other effects. Comparisons are made to a 1 deg 408 MHz map (Haslam et al.) and the 11 deg ARCADE 2 data (Singal et al.). We find that spinning dust or steepening synchrotron models fit the combination of WMAP and 408 MHz data equally well. ARCADE data appear inconsistent with the steepening synchrotron model and consistent with the spinning dust model, though some discrepancies remain regarding the relative strength of spinning dust emission. More high-resolution data in the 10-40 GHz range would shed much light on these issues.
C1 [Gold, B.; Bennett, C. L.; Larson, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Odegard, N.; Weiland, J. L.; Hill, R. S.] Adnet Syst Inc, Lanham, MD 20706 USA.
[Kogut, A.; Hinshaw, G.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Chen, X.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Dunkley, J.] Univ Oxford, Oxford OX1 3RH, England.
[Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Jarosik, N.; Page, L.; Spergel, D. N.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Meyer, S. S.] Univ Chicago, Dept Astrophys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, Dept Phys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, EFI, Chicago, IL 60637 USA.
[Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Smith, K. M.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Wright, E. L.] UCLA Phys & Astron, Los Angeles, CA 90095 USA.
RP Gold, B (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
EM bgold@pha.jhu.edu
RI Spergel, David/A-4410-2011; Wollack, Edward/D-4467-2012; Komatsu,
Eiichiro/A-4361-2011
OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698;
FU Science Mission Directorate Office at NASA Headquarters; NASA
[NNG05GE76G, NNX07AL75G S01, LTSA03-000-0090, ATPNNG04GK55G,
ADP03-0000-092]
FX The WMAP mission is made possible by the support of the Science Mission
Directorate Office at NASA Headquarters. This research was additionally
supported by NASA grants NNG05GE76G, NNX07AL75G S01, LTSA03-000-0090,
ATPNNG04GK55G, and ADP03-0000-092. This research has made use of NASA's
Astrophysics Data System Bibliographic Services. We acknowledge use of
the HEALPix, CAMB, and CMBFAST packages.
NR 51
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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JI Astrophys. J. Suppl. Ser.
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SC Astronomy & Astrophysics
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ER
PT J
AU Komatsu, E
Smith, KM
Dunkley, J
Bennett, CL
Gold, B
Hinshaw, G
Jarosik, N
Larson, D
Nolta, MR
Page, L
Spergel, DN
Halpern, M
Hill, RS
Kogut, A
Limon, M
Meyer, SS
Odegard, N
Tucker, GS
Weiland, JL
Wollack, E
Wright, EL
AF Komatsu, E.
Smith, K. M.
Dunkley, J.
Bennett, C. L.
Gold, B.
Hinshaw, G.
Jarosik, N.
Larson, D.
Nolta, M. R.
Page, L.
Spergel, D. N.
Halpern, M.
Hill, R. S.
Kogut, A.
Limon, M.
Meyer, S. S.
Odegard, N.
Tucker, G. S.
Weiland, J. L.
Wollack, E.
Wright, E. L.
TI SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS:
COSMOLOGICAL INTERPRETATION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic background radiation; cosmology: observations; dark matter; early
universe; space vehicles
ID DIGITAL SKY SURVEY; PRIMORDIAL NON-GAUSSIANITY; COSMIC
BACKGROUND-RADIATION; RELAXED GALAXY CLUSTERS; EQUATION-OF-STATE;
DARK-MATTER HALO; ISOTHERMAL DENSITY PERTURBATIONS; INFLATIONARY
UNIVERSE SCENARIO; GRAVITATIONAL LENSING SYSTEMS; GALACTIC FOREGROUND
EMISSION
AB The combination of seven-year data from WMAP and improved astrophysical data rigorously tests the standard cosmological model and places new constraints on its basic parameters and extensions. By combining the WMAP data with the latest distance measurements from the baryon acoustic oscillations (BAO) in the distribution of galaxies and the Hubble constant (H-0) measurement, we determine the parameters of the simplest six-parameter Lambda CDM model. The power-law index of the primordial power spectrum is n(s) = 0.968 +/- 0.012 (68% CL) for this data combination, a measurement that excludes the Harrison-Zel'dovich-Peebles spectrum by 99.5% CL. The other parameters, including those beyond the minimal set, are also consistent with, and improved from, the five-year results. We find no convincing deviations from the minimal model. The seven-year temperature power spectrum gives a better determination of the third acoustic peak, which results in a better determination of the redshift of the matter-radiation equality epoch. Notable examples of improved parameters are the total mass of neutrinos, Sigma m(nu) < 0.58 eV (95% CL), and the effective number of neutrino species, N-eff = 4.34(-0.88)(+0.86) (68% CL), which benefit from better determinations of the third peak and H-0. The limit on a constant dark energy equation of state parameter from WMAP+BAO+H-0, without high-redshift Type Ia supernovae, is w = -1.10 +/- 0.14 (68% CL). We detect the effect of primordial helium on the temperature power spectrum and provide a new test of big bang nucleosynthesis by measuring Y-p = 0.326 +/- 0.075 (68% CL). We detect, and show on the map for the first time, the tangential and radial polarization patterns around hot and cold spots of temperature fluctuations, an important test of physical processes at z = 1090 and the dominance of adiabatic scalar fluctuations. The seven-year polarization data have significantly improved: we now detect the temperature-E-mode polarization cross power spectrum at 21 sigma, compared with 13 sigma from the five-year data. With the seven-year temperature-B-mode cross power spectrum, the limit on a rotation of the polarization plane due to potential parity-violating effects has improved by 38% to Delta a = -1 degrees.1 +/- 1 degrees.4(statistical) +/- 1 degrees.5(systematic) (68% CL). We report significant detections of the Sunyaev-Zel'dovich (SZ) effect at the locations of known clusters of galaxies. The measured SZ signal agrees well with the expected signal from the X-ray data on a cluster-by-cluster basis. However, it is a factor of 0.5-0.7 times the predictions from "universal profile" of Arnaud et al., analytical models, and hydrodynamical simulations. We find, for the first time in the SZ effect, a significant difference between the cooling-flow and non-cooling-flow clusters (or relaxed and non-relaxed clusters), which can explain some of the discrepancy. This lower amplitude is consistent with the lower-than-theoretically expected SZ power spectrum recently measured by the South Pole Telescope Collaboration.
C1 [Komatsu, E.] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA.
[Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Smith, K. M.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Dunkley, J.] Univ Oxford, Oxford OX1 3RH, England.
[Bennett, C. L.; Gold, B.; Larson, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hinshaw, G.; Kogut, A.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jarosik, N.; Page, L.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Spergel, D. N.] Princeton Univ, Princeton Ctr Theoret Phys, Princeton, NJ 08544 USA.
[Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hill, R. S.; Odegard, N.; Weiland, J. L.] ADNET Syst Inc, Lanham, MD 20706 USA.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Meyer, S. S.] Univ Chicago, Dept Phys & Astrophys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, EFI, Chicago, IL 60637 USA.
[Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Wright, E. L.] UCLA Phys & Astron, Los Angeles, CA 90095 USA.
RP Komatsu, E (reprint author), Univ Texas Austin, Texas Cosmol Ctr, 2511 Speedway,RLM 15-306, Austin, TX 78712 USA.
EM komatsu@astro.as.utexas.edu
RI Komatsu, Eiichiro/A-4361-2011; Spergel, David/A-4410-2011; Wollack,
Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698
FU NASA [NNG05GE76G, NNX07AL75G S01, LTSA03-000-0090, ATPNNG04GK55G,
ADP03-0000-092, NNX08AL43G]; NSF [AST-0807649, PHY-0758153]; Alfred P.
Sloan Research Fellowship; Research Councils UK (RCUK)
FX The WMAP mission is made possible by the support of the Science Mission
Directorate Office at NASA Headquarters. This research was additionally
supported by NASA grants NNG05GE76G, NNX07AL75G S01, LTSA03-000-0090,
ATPNNG04GK55G, ADP03-0000-092, and NNX08AL43G, and NSF grants
AST-0807649 and PHY-0758153. E.K. acknowledges support from an Alfred P.
Sloan Research Fellowship. J.D. is partly supported by an Research
Councils UK (RCUK) fellowship. We thank Mike Greason for his help on the
analysis of the WMAP data, and T. B. Griswold for the artwork. We thank
D. Jeong for his help on calculating the peak bias presented in Section
2, B. A. Reid for discussion on the treatment of massive neutrinos in
the expansion rate which has led to our exact treatment in Section 3.3,
A. G. Riess for discussion on the Type Ia supernova data set and the
H0 measurement, M. Sullivan for discussion on the Type Ia
supernova data set, S. H. Suyu and P. J. Marshall for providing us with
the likelihood function for the time-delay distance and discussion on
strong lensing measurements, A. Vikhlinin for the X-ray data on his
nearby cluster samples (used in Section 7.3), N. Afshordi, P. Bode, R.
Lieu, Y.-T. Lin, D. Nagai, N. Sehgal, L. Shaw, and H. Trac for
discussion and feedback on Section 7 (SZ effect), and F. Takahashi for
his help on refining the results on axion dark matter presented in
Section 4.4. Computations for the analysis of non-Gaussianity in Section
6 were carried out by the Terascale Infrastructure for Groundbreaking
Research in Engineering and Science (TIGRESS) at the Princeton Institute
for Computational Science and Engineering (PICSciE). This research has
made use of NASA's Astrophysics Data System Bibliographic Services. We
acknowledge use of the HEALPix (Gorski et al. 2005), CAMB (Lewis et al.
2000), and CMBFAST (Seljak & Zaldarriaga 1996) packages.
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SC Astronomy & Astrophysics
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ER
PT J
AU Larson, D
Dunkley, J
Hinshaw, G
Komatsu, E
Nolta, MR
Bennett, CL
Gold, B
Halpern, M
Hill, RS
Jarosik, N
Kogut, A
Limon, M
Meyer, SS
Odegard, N
Page, L
Smith, KM
Spergel, DN
Tucker, GS
Weiland, JL
Wollack, E
Wright, EL
AF Larson, D.
Dunkley, J.
Hinshaw, G.
Komatsu, E.
Nolta, M. R.
Bennett, C. L.
Gold, B.
Halpern, M.
Hill, R. S.
Jarosik, N.
Kogut, A.
Limon, M.
Meyer, S. S.
Odegard, N.
Page, L.
Smith, K. M.
Spergel, D. N.
Tucker, G. S.
Weiland, J. L.
Wollack, E.
Wright, E. L.
TI SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS:
POWER SPECTRA AND WMAP-DERIVED PARAMETERS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic background radiation; cosmological parameters; cosmology:
observations; dark matter; early universe; space vehicles: instruments
ID PRIMORDIAL HELIUM ABUNDANCE; OBSERVATIONS COSMOLOGICAL INTERPRETATION;
GALACTIC FOREGROUND EMISSION; BACKGROUND ANISOTROPIES; POLARIZATION;
TEMPERATURE; RECOMBINATION; MAPS; REANALYSIS; LIKELIHOOD
AB The WMAP mission has produced sky maps from seven years of observations at L2. We present the angular power spectra derived from the seven-year maps and discuss the cosmological conclusions that can be inferred from WMAP data alone. With the seven-year data, the temperature (TT) spectrum measurement has a signal-to-noise ratio per multipole that exceeds unity for l < 919; and in band powers of width Delta l = 10, the signal-to-noise ratio exceeds unity up to l = 1060. The third acoustic peak in the TT spectrum is now well measured by WMAP. In the context of a flat Lambda CDM model, this improvement allows us to place tighter constraints on the matter density from WMAP data alone, Omega(m)h(2) = 0.1334(-0.0055)(+0.0056), and on the epoch of matter-radiation equality, z(eq) = 3196(-133)(+134). The temperature-polarization (TE) spectrum is detected in the seven-year data with a significance of 20 sigma, compared to 13 sigma with the five-year data. We now detect the second dip in the TE spectrum near l similar to 450 with high confidence. The TB and EB spectra remain consistent with zero, thus demonstrating low systematic errors and foreground residuals in the data. The low-l EE spectrum, a measure of the optical depth due to reionization, is detected at 5.5 sigma significance when averaged over l = 2-7: l(l+ 1)C-l(EE)/(2 pi) = 0.074(-0.025)(+0.034) mu K-2 (68% CL). We now detect the high-l, 24 <= l <= 800, EE spectrum at over 8 sigma. The BB spectrum, an important probe of gravitational waves from inflation, remains consistent with zero; when averaged over l = 2-7, l(l + 1)C-l(BB)/(2 pi) < 0.055 mu K-2 (95% CL). The upper limit on tensor modes from polarization data alone is a factor of two lower with the seven-year data than it was using the five-year data. The data remain consistent with the simple Lambda CDM model: the best-fit TT spectrum has an effective chi(2) of 1227 for 1170 degrees of freedom, with a probability to exceed of 9.6%. The allowable volume in the six-dimensional space of Lambda CDM parameters has been reduced by a factor of 1.5 relative to the five-year volume, while the Lambda CDM model that allows for tensor modes and a running scalar spectral index has a factor of three lower volume when fit to the seven-year data. We test the parameter recovery process for bias and find that the scalar spectral index, n(s), is biased high, but only by 0.09 sigma, while the remaining parameters are biased by <0.15 sigma. The improvement in the third peak measurement leads to tighter lower limits from WMAP on the number of relativistic degrees of freedom (e.g., neutrinos) in the early universe: N-eff > 2.7 (95% CL). Also, using WMAP data alone, the primordial helium mass fraction is found to be Y-He = 0.28(-0.15)(+0.14), and with data from higher-resolution cosmic microwave background experiments included, we now establish the existence of pre-stellar helium at >3 sigma. These new WMAP measurements provide important tests of big bang cosmology.
C1 [Larson, D.; Bennett, C. L.; Gold, B.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Dunkley, J.] Univ Oxford, Oxford OX1 3RH, England.
[Hinshaw, G.; Kogut, A.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hill, R. S.; Odegard, N.; Weiland, J. L.] ADNET Syst Inc, Lanham, MD 20706 USA.
[Jarosik, N.; Page, L.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Meyer, S. S.] Univ Chicago, Dept Astrophys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, Dept Phys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, EFI, Chicago, IL 60637 USA.
[Smith, K. M.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Spergel, D. N.] Princeton Univ, Princeton Ctr Theoret Phys, Princeton, NJ 08544 USA.
[Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Wright, E. L.] UCLA Phys & Astron, Los Angeles, CA 90095 USA.
RP Larson, D (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
EM dlarson@pha.jhu.edu
RI Komatsu, Eiichiro/A-4361-2011; Spergel, David/A-4410-2011; Wollack,
Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698
FU NASA Science Mission Directorate
FX The WMAP mission is made possible by the support of the NASA Science
Mission Directorate. This research has made use of NASA's Astrophysics
Data System Bibliographic Services. Some of the results in this paper
have been derived using the HEALPix (Gorski et al. 2005) package. We
acknowledge use of the CAMB (Lewis et al. 2000) and CMBFAST (Seljak &
Zaldarriaga 1996) packages.
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J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
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PY 2011
VL 192
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AR 16
DI 10.1088/0067-0049/192/2/16
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706BL
UT WOS:000286189700003
ER
PT J
AU Weiland, JL
Odegard, N
Hill, RS
Wollack, E
Hinshaw, G
Greason, MR
Jarosik, N
Page, L
Bennett, CL
Dunkley, J
Gold, B
Halpern, M
Kogut, A
Komatsu, E
Larson, D
Limon, M
Meyer, SS
Nolta, MR
Smith, KM
Spergel, DN
Tucker, GS
Wright, EL
AF Weiland, J. L.
Odegard, N.
Hill, R. S.
Wollack, E.
Hinshaw, G.
Greason, M. R.
Jarosik, N.
Page, L.
Bennett, C. L.
Dunkley, J.
Gold, B.
Halpern, M.
Kogut, A.
Komatsu, E.
Larson, D.
Limon, M.
Meyer, S. S.
Nolta, M. R.
Smith, K. M.
Spergel, D. N.
Tucker, G. S.
Wright, E. L.
TI SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS:
PLANETS AND CELESTIAL CALIBRATION SOURCES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: individual (Cygnus A, 3C274); ISM: supernova remnants; planets
and satellites: general; radio continuum: general; space vehicles:
instruments
ID SUPERNOVA REMNANT CASSIOPEIA; RADIO FLUX-DENSITY; BRIGHTNESS TEMPERATURE
SPECTRA; CRAB-NEBULA; SATURNS RINGS; CYGNUS-A; CONTINUUM OBSERVATIONS;
SYNCHROTRON-RADIATION; MILLIMETER-WAVELENGTH; FOREGROUND EMISSION
AB We present WMAP seven-year observations of bright sources which are often used as calibrators at microwave frequencies. Ten objects are studied in five frequency bands (23-94 GHz): the outer planets (Mars, Jupiter, Saturn, Uranus, and Neptune) and five fixed celestial sources (Cas A, Tau A, Cyg A, 3C274, and 3C58). The seven-year analysis of Jupiter provides temperatures which are within 1 sigma of the previously published WMAP five-year values, with slightly tighter constraints on variability with orbital phase (0.2% +/- 0.4%), and limits (but no detections) on linear polarization. Observed temperatures for both Mars and Saturn vary significantly with viewing geometry. Scaling factors are provided which, when multiplied by the Wright Mars thermal model predictions at 350 mu m, reproduce WMAP seasonally averaged observations of Mars within similar to 2%. An empirical model is described which fits brightness variations of Saturn due to geometrical effects and can be used to predict the WMAP observations to within 3%. Seven-year mean temperatures for Uranus and Neptune are also tabulated. Uncertainties in Uranus temperatures are 3%-4% in the 41, 61, and 94 GHz bands; the smallest uncertainty for Neptune is 8% for the 94 GHz band. Intriguingly, the spectrum of Uranus appears to show a dip at similar to 30 GHz of unidentified origin, although the feature is not of high statistical significance. Flux densities for the five selected fixed celestial sources are derived from the seven-year WMAP sky maps and are tabulated for Stokes I, Q, and U, along with polarization fraction and position angle. Fractional uncertainties for the Stokes I fluxes are typically 1% to 3%. Source variability over the seven-year baseline is also estimated. Significant secular decrease is seen for Cas A and Tau A: our results are consistent with a frequency-independent decrease of about 0.53% per year for Cas A and 0.22% per year for Tau A. We present WMAP polarization data with uncertainties of a few percent for Tau A. Where appropriate, WMAP results are compared against previous findings in the literature. With an absolute calibration uncertainty of 0.2%, WMAP data are a valuable asset for calibration work.
C1 [Weiland, J. L.; Odegard, N.; Hill, R. S.; Greason, M. R.] ADNET Syst Inc, Lanham, MD 20706 USA.
[Wollack, E.; Hinshaw, G.; Kogut, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jarosik, N.; Page, L.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Bennett, C. L.; Gold, B.; Larson, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Dunkley, J.] Univ Oxford, Oxford OX1 3RH, England.
[Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Meyer, S. S.] Univ Chicago, Dept Astrophys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, Dept Phys, KICP, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, EFI, Chicago, IL 60637 USA.
[Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Smith, K. M.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Spergel, D. N.] Princeton Univ, Princeton Ctr Theoret Phys, Princeton, NJ 08544 USA.
[Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Wright, E. L.] UCLA Phys & Astron, Los Angeles, CA 90095 USA.
RP Weiland, JL (reprint author), ADNET Syst Inc, 7515 Mission Dr,Suite A100, Lanham, MD 20706 USA.
EM jweiland@sesda2.com
RI Komatsu, Eiichiro/A-4361-2011; Spergel, David/A-4410-2011; Wollack,
Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698
FU Science Mission Directorate Office at NASA Headquarters
FX The WMAP mission is made possible by the support of the Science Mission
Directorate Office at NASA Headquarters. This research has made use of
NASA's Astrophysics Data System Bibliographic Services. We acknowledge
the use of the HEALPix package (Gorski et al. 2005).
NR 124
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U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD FEB
PY 2011
VL 192
IS 2
AR 19
DI 10.1088/0067-0049/192/2/19
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706BL
UT WOS:000286189700006
ER
PT J
AU Kumar, A
Chen, F
Niyogi, D
Alfieri, JG
Ek, M
Mitchell, K
AF Kumar, Anil
Chen, Fei
Niyogi, Dev
Alfieri, Joseph G.
Ek, Michael
Mitchell, Kenneth
TI Evaluation of a Photosynthesis-Based Canopy Resistance Formulation in
the Noah Land-Surface Model
SO BOUNDARY-LAYER METEOROLOGY
LA English
DT Article
DE Canopy resistance; Evapotranspiration; Land data assimilation system;
Noah land-surface model; Photosynthesis; Surface energy flux
ID INTERNATIONAL H2O PROJECT; DATA ASSIMILATION SYSTEM; MESOSCALE
ETA-MODEL; SENSIBLE HEAT-FLUX; BOUNDARY-LAYER; STOMATAL CONDUCTANCE;
SOIL-MOISTURE; FIFE OBSERVATIONS; WARM-SEASON; PART II
AB Accurately representing complex land-surface processes balancing complexity and realism remains one challenge that the weather modelling community is facing nowadays. In this study, a photosynthesis-based Gas-exchange Evapotranspiration Model (GEM) is integrated into the Noah land-surface model replacing the traditional Jarvis scheme for estimating the canopy resistance and transpiration. Using 18-month simulations from the High Resolution Land Data Assimilation System (HRLDAS), the impact of the photosynthesis-based approach on the simulated canopy resistance, surface heat fluxes, soil moisture, and soil temperature over different vegetation types is evaluated using data from the Atmospheric Radiation Measurement (ARM) site, Oklahoma Mesonet, 2002 International H2O Project (IHOP_2002), and three Ameriflux sites. Incorporation of GEM into Noah improves the surface energy fluxes as well as the associated diurnal cycle of soil moisture and soil temperature during both wet and dry periods. An analysis of midday, average canopy resistance shows similar day-to-day trends in the model fields as seen in observed patterns. Bias and standard deviation analyses for soil temperature and surface fluxes show that GEM responds somewhat better than the Jarvis scheme, mainly because the Jarvis approach relies on a parametrised minimum canopy resistance and meteorological variables such as air temperature and incident radiation. The analyses suggest that adding a photosynthesis-based transpiration scheme such as GEM improves the ability of the land-data assimilation system to simulate evaporation and transpiration under a range of soil and vegetation conditions.
C1 [Kumar, Anil] NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kumar, Anil; Chen, Fei] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Kumar, Anil; Niyogi, Dev; Alfieri, Joseph G.] Purdue Univ, W Lafayette, IN 47907 USA.
[Ek, Michael; Mitchell, Kenneth] Natl Ctr Environm Predict, Camp Springs, MD USA.
RP Kumar, A (reprint author), NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Code 614-3, Greenbelt, MD 20771 USA.
EM anil.kumar@nasa.gov
RI Chen, Fei/B-1747-2009
FU DOE ARM [08ER64674]; NOAA JCSDA [NA06NES4400013]; NASA THP [NNX08AV80G,
NNX08AU67]; NCAR USWRP STEP; NCAR Water System [NSF 01]; NSF
[ATM-0296159, ATM-0236885, OCI-0753116]; NASA GWEC [NNG05GB41G]; NASA
Headquarters through the NASA [NNX07AN67H]
FX The authors would like to acknowledge the support from the DOE ARM
Program (08ER64674), NOAA JCSDA (NA06NES4400013), NASA THP (NNX08AV80G,
NNX08AU67), NCAR USWRP STEP, the NCAR Water System (Grant NSF 01) and
STEP programs, NSF (ATM-0296159, ATM-0236885, and OCI-0753116), NASA
GWEC (NNG05GB41G), and NASA Headquarters through the NASA Earth and
Space Science Fellowship (NNX07AN67H).
NR 58
TC 17
Z9 17
U1 1
U2 16
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0006-8314
J9 BOUND-LAY METEOROL
JI Bound.-Layer Meteor.
PD FEB
PY 2011
VL 138
IS 2
BP 263
EP 284
DI 10.1007/s10546-010-9559-z
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 705AT
UT WOS:000286100800005
ER
PT J
AU Solomon, A
Goddard, L
Kumar, A
Carton, J
Deser, C
Fukumori, I
Greene, AM
Hegerl, G
Kirtman, B
Kushnir, Y
Newman, M
Smith, D
Vimont, D
Delworth, T
Meehl, GA
Stockdale, T
AF Solomon, Amy
Goddard, Lisa
Kumar, Arun
Carton, James
Deser, Clara
Fukumori, Ichiro
Greene, Arthur M.
Hegerl, Gabriele
Kirtman, Ben
Kushnir, Yochanan
Newman, Matthew
Smith, Doug
Vimont, Dan
Delworth, Tom
Meehl, Gerald A.
Stockdale, Timothy
CA US CLIVAR Decadal Predictability W
TI DISTINGUISHING THE ROLES OF NATURAL AND ANTHROPOGENICALLY FORCED DECADAL
CLIMATE VARIABILITY Implications for Prediction
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; EQUATORIAL PACIFIC-OCEAN; ATLANTIC MULTIDECADAL
OSCILLATION; EL-NINO-LIKE; NORTH-ATLANTIC; ATMOSPHERIC CIRCULATION;
COUPLED MODEL; WIND STRESSES; PART I; ENSO
AB DISTINGUISHING THE ROLES OF NATURAL AND ANTHROPOGENICALLY FORCED DECADAL CLIMATE VARIABILITY: IMPLICATIONS FOR PREDICTION
Given that over the course of the next 10-30 years the magnitude of natural decalial variations may rival that of anthropogenically forced climate change on regional scales, it is envisioned that initialized decadal predictions will provide important information for climate-related management and adaptation decisions. Such predictions are presently one of the grand challenges for the climate community. This requires identifying those physical phenomena and their model equivalents that May provide additional predictability on decadal time scales, including an assessment of the physical processes through which anthropogenic forcing may interact with or project upon natural variability. Such a physical framework is necessary to provide a consistent assessment (and insight into potential improvement) of the decadal prediction experiments planned to be assessed as part of the IPCC's Fifth Assessment Report.
C1 [Solomon, Amy] NOAA, ESRL, PSD, Boulder, CO 80305 USA.
[Solomon, Amy; Newman, Matthew] Univ Colorado, Boulder, CO 80309 USA.
[Goddard, Lisa; Greene, Arthur M.] NOAA, Int Res Inst Climate & Soc, Palisades, NY USA.
[Kumar, Arun] NOAA, Climate Predict Ctr, Camp Springs, MD USA.
[Carton, James] Univ Maryland, College Pk, MD 20742 USA.
[Deser, Clara; Meehl, Gerald A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Fukumori, Ichiro] NASA, Jet Prop Lab, Pasadena, CA USA.
[Hegerl, Gabriele] Univ Edinburgh, Edinburgh, Midlothian, Scotland.
[Kirtman, Ben] Univ Miami, Miami, FL USA.
[Kirtman, Ben] Ctr Ocean Land Atmosphere Studies, Calverton, MD USA.
[Kushnir, Yochanan] Columbia Univ, Lamont Doherty Earth Observ, New York, NY USA.
[Smith, Doug] Met Off Hadley Ctr, Exeter, Devon, England.
[Vimont, Dan] Univ Wisconsin, Madison, WI USA.
[Delworth, Tom] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Stockdale, Timothy] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
RP Solomon, A (reprint author), NOAA, ESRL, PSD, 325 Broadway, Boulder, CO 80305 USA.
RI Kushnir, Yochanan/B-4472-2013; carton, james/C-4807-2009; Newman,
Matthew /F-8336-2010; Solomon, Amy/L-8988-2013; Delworth,
Thomas/C-5191-2014
OI carton, james/0000-0003-0598-5198; Newman, Matthew /0000-0001-5348-2312;
FU U.S. CLIVAR; U.S. CLIVAR office
FX The authors of this paper are members of the Decadal Predictability
Working Group, sponsored by U.S. CLIVAR. We appreciate the support from
the U.S. CLIVAR office. We thank two anonymous reviewers for their
helpful and thoughtful suggestions.
NR 93
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Z9 83
U1 2
U2 45
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD FEB
PY 2011
VL 92
IS 2
BP 141
EP 156
DI 10.1175/2010BAMS2962.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 743LT
UT WOS:000289020500008
ER
PT J
AU Atlas, R
Hoffman, RN
Ardizzone, J
Leidner, SM
Jusem, JC
Smith, DK
Gombos, D
AF Atlas, Robert
Hoffman, Ross N.
Ardizzone, Joseph
Leidner, S. Mark
Jusem, Juan Carlos
Smith, Deborah K.
Gombos, Daniel
TI A CROSS-CALIBRATED MULTIPLATFORM OCEAN SURFACE WIND VELOCITY PRODUCT FOR
METEOROLOGICAL AND OCEANOGRAPHIC APPLICATIONS
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID VARIATIONAL ANALYSIS METHOD; NSCAT AMBIGUITY REMOVAL;
SATELLITE-OBSERVATIONS; DIRECT MINIMIZATION; DATA ASSIMILATION;
CENTRAL-AMERICA; PACIFIC COAST; ALGORITHM; HEAT; SEA
AB A CROSS-CALIBRATED, MULTI PLATFORM OCEAN SURFACE WIND VELOCITY PRODUCT FOR METEOROLOGICAL AND OCEANOGRAPHIC APPLICATIONS
The ocean surface wind mediates exchanges between the ocean and the atmosphere. These air-sea exchange processes are critical for understanding and predicting atmosphere, ocean, and wave phenomena on many time and space scales. A cross-calibrated multiplatform (CCMP) long-term data record of satellite ocean surface winds is available from 1987 to 2008 with planned extensions through 2012. A variational analysis method (VAM) is used to combine surface wind data derived from conventional and in situ sources and multiple satellites into a. consistent near-global analysis at 25-km resolution, every 6 h. The input data are cross-calibrated wind speeds derived from the Special Sensor Microwave: Imager (SSM/I; F08-F15), the Tropical Rainfall Measuring Mission Microwave Imager (TMI), and the Advanced Microwave Scanning Radiometer for Earth Observing System (AMSR-E), and wind vectors from SeaWinds on the NASA Quick Scatterometer (QuikSCAT) and on the second Japanese Advanced Earth Observing Satellite (AD-EOS-2; i.e., the Midori-2 satellite). These are combined with ECMWF: reanalyses and operational analyses by the VAM. VAM analyses and derived data are currently available for interested investigators through the Jet Propulsion Laboratory (JPL) Physical Oceanography Distributed Active Archive Center (PO.DAAC). This paper describes the methodology used to assimilate the input data along with the validation and evaluation of the derived CCMP products.
C1 [Atlas, Robert] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
[Hoffman, Ross N.; Gombos, Daniel] Atmospher & Environm Res Inc, Lexington, MA USA.
[Ardizzone, Joseph; Jusem, Juan Carlos] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smith, Deborah K.] Remote Sensing Syst, Santa Rosa, CA USA.
RP Atlas, R (reprint author), NOAA, Atlantic Oceanog & Meteorol Lab, 4301 Rickenbacker Causeway, Miami, FL 33149 USA.
EM robert.atlas@noaa.gov
RI Atlas, Robert/A-5963-2011
OI Atlas, Robert/0000-0002-0706-3560
FU NASA's Research, Education and Applications Solution Network (REASON);
Making Earth Science Data Records for Use in Research Environments
(MEASURES) programs
FX Remote Sensing Systems (RSS; Santa Rosa, California; available online at
www.remss.com/) provided the satellite data. We thank F. Wentz, of RSS
for help in acquiring and understanding these datasets. The conventional
data used in our analyses were obtained from the Scientific Division of
the National Center for Atmospheric Research (NCAR). Additional buoy
data were obtained from the Pacific Marine and Environmental Laboratory
(PMEL). ERA-40 Re-Analysis and ECMWF operational analysis datasets were
obtained from the Computation and Information Systems Laboratory (CISL)
at NCAR. The cross-calibrated multiplatform (CCMP) ocean surface wind
product is hosted at the Physical Oceanography Distributed Active
Archive Center (PO.DAAC; available online at
http://podaac.jpl.nasa.gov/DATA_CATALOG/compinfo.html). We thank a
Moroni (Jet Propulsion Laboratory, California Institute of Technology,
Pasadena, California) for help in preparing the CCMP winds for public
release. NASA's Research, Education and Applications Solution Network
(REASON) and Making Earth Science Data Records for Use in Research
Environments (MEASURES) programs funded this work. All of the RSS data
described here were produced through another component of the MEASURES
program, named the Distributed Information Services: Climate/Ocean
Products and Visualizations for Earth Research (DISCOVER) project. The
work represents a continuation and expansion of the SSMI Derived Global
Ocean Surface Wind Components project that began under the NASA
Pathfinder Program. We thank the reviewers and the editor for their
useful suggestions that helped to improve this paper.
NR 39
TC 228
Z9 235
U1 5
U2 33
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD FEB
PY 2011
VL 92
IS 2
BP 157
EP +
DI 10.1175/2010BAMS2946.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 743LT
UT WOS:000289020500009
ER
PT J
AU Archinal, BA
A'Hearn, MF
Bowell, E
Conrad, A
Consolmagno, GJ
Courtin, R
Fukushima, T
Hestroffer, D
Hilton, JL
Krasinsky, GA
Neumann, G
Oberst, J
Seidelmann, PK
Stooke, P
Tholen, DJ
Thomas, PC
Williams, IP
AF Archinal, B. A.
A'Hearn, M. F.
Bowell, E.
Conrad, A.
Consolmagno, G. J.
Courtin, R.
Fukushima, T.
Hestroffer, D.
Hilton, J. L.
Krasinsky, G. A.
Neumann, G.
Oberst, J.
Seidelmann, P. K.
Stooke, P.
Tholen, D. J.
Thomas, P. C.
Williams, I. P.
TI Report of the IAU Working Group on Cartographic Coordinates and
Rotational Elements: 2009
SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY
LA English
DT Article
DE Cartographic coordinates; Longitude; Latitude; Rotation axes; Rotation
periods; Sizes; Shapes; Planets; Satellites; Dwarf planets; Minor
planets; Comets
ID CASSINI-ISS IMAGES; INTERIOR STRUCTURE; GLOBAL SHAPE; SATELLITES;
PLANETS; GRAVITY; TOPOGRAPHY; PERIOD; CERES; STATE
AB Every three years the IAU Working Group on Cartographic Coordinates and Rotational Elements revises tables giving the directions of the poles of rotation and the prime meridians of the planets, satellites, minor planets, and comets. This report takes into account the IAU Working Group for Planetary System Nomenclature (WGPSN) and the IAU Committee on Small Body Nomenclature (CSBN) definition of dwarf planets, introduces improved values for the pole and rotation rate of Mercury, returns the rotation rate of Jupiter to a previous value, introduces improved values for the rotation of five satellites of Saturn, and adds the equatorial radius of the Sun for comparison. It also adds or updates size and shape information for the Earth, Mars' satellites Deimos and Phobos, the four Galilean satellites of Jupiter, and 22 satellites of Saturn. Pole, rotation, and size information has been added for the asteroids (21) Lutetia, (511) Davida, and (2867) teins. Pole and rotation information has been added for (2) Pallas and (21) Lutetia. Pole and rotation and mean radius information has been added for (1) Ceres. Pole information has been updated for (4) Vesta. The high precision realization for the pole and rotation rate of the Moon is updated. Alternative orientation models for Mars, Jupiter, and Saturn are noted. The Working Group also reaffirms that once an observable feature at a defined longitude is chosen, a longitude definition origin should not change except under unusual circumstances. It is also noted that alternative coordinate systems may exist for various (e.g. dynamical) purposes, but specific cartographic coordinate system information continues to be recommended for each body. The Working Group elaborates on its purpose, and also announces its plans to occasionally provide limited updates to its recommendations via its website, in order to address community needs for some updates more often than every 3 years. Brief recommendations are also made to the general planetary community regarding the need for controlled products, and improved or consensus rotation models for Mars, Jupiter, and Saturn.
C1 [Archinal, B. A.] US Geol Survey, Flagstaff, AZ 86001 USA.
[A'Hearn, M. F.] Univ Maryland, College Pk, MD 20742 USA.
[Bowell, E.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Conrad, A.] WM Keck Observ, Kamuela, HI USA.
[Consolmagno, G. J.] Vatican Observ, Vatican City, Vatican.
[Courtin, R.] Observ Paris, CNRS, LESIA, F-75014 Paris, France.
[Fukushima, T.] Natl Astron Observ Japan, Tokyo, Japan.
[Hestroffer, D.] Observ Paris, CNRS, IMCCE, F-75014 Paris, France.
[Hilton, J. L.] US Naval Observ, Washington, DC USA.
[Krasinsky, G. A.] Inst Appl Astron, St Petersburg, Russia.
[Neumann, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Oberst, J.] DLR Berlin Adlershof, Berlin, Germany.
[Seidelmann, P. K.] Univ Virginia, Charlottesville, VA USA.
[Stooke, P.] Univ Western Ontario, London, ON, Canada.
[Tholen, D. J.] Univ Hawaii, Honolulu, HI 96822 USA.
[Thomas, P. C.] Cornell Univ, Ithaca, NY USA.
[Williams, I. P.] Queen Mary Univ London, London, England.
RP Archinal, BA (reprint author), US Geol Survey, Flagstaff, AZ 86001 USA.
EM barchinal@usgs.gov
RI Neumann, Gregory/I-5591-2013;
OI Neumann, Gregory/0000-0003-0644-9944; Williams, Iwan
Prys/0000-0002-8069-1344
NR 74
TC 106
Z9 116
U1 0
U2 12
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0923-2958
J9 CELEST MECH DYN ASTR
JI Celest. Mech. Dyn. Astron.
PD FEB
PY 2011
VL 109
IS 2
BP 101
EP 135
DI 10.1007/s10569-010-9320-4
PG 35
WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications
SC Astronomy & Astrophysics; Mathematics
GA 712JH
UT WOS:000286662300001
ER
PT J
AU Breaker, LC
Ruzmaikin, A
AF Breaker, Laurence C.
Ruzmaikin, Alexander
TI The 154-year record of sea level at San Francisco: extracting the
long-term trend, recent changes, and other tidbits
SO CLIMATE DYNAMICS
LA English
DT Article
DE Sea level; Empirical mode decomposition; Inverse barometer correction;
Long-term trend; Recent changes in sea level; ENSO; Pacific decadal
oscillation
ID EMPIRICAL MODE DECOMPOSITION; PACIFIC COAST; NORTH-AMERICA; VARIABILITY;
OSCILLATIONS; MODULATION; CALIFORNIA; NOISE; RISE
AB A data adaptive method called ensemble empirical mode decomposition (EEMD) is used to examine the 154-year record of monthly sea level at San Francisco. The mode that is lowest in frequency corresponds to the long-term trend. The next highest mode corresponds to an oscillation with a period of similar to 100 years and may be related to solar variability. When this mode is combined with the long-term trend, the rate of increase in sea level starts to decrease by similar to 1980. The next lower mode corresponds to interdecadal time scales and thus includes the Pacific Decadal Oscillation. When combined with the two lower modes, sea level itself starts to decrease by the mid-1990s. These results are consistent with the most recent results from the intergovernmental panel on climate change (IPCC), and may be the first obtained from a tidal record. Prior to conducting EEMD, corrections for glacial isostatic adjustment (GIA) and the inverse barometer (IB) effect were applied. The effect of applying the GIA correction was relatively small, but the IB correction reduced the slope of the long-term trend in sea level by almost 15%. This reduction is due to a long-term increase in the variance of sea level pressure. To determine if the 10-15 year ENSO modulation cycle could be detected from the decomposition we first compared the envelope from the mode associated with ENSO, with the two adjacent modes that were lower in frequency. Spectral analysis revealed no significant maxima in the ENSO mode envelope, but a major peak in the spectrum for the two adjacent modes, with a period of 12.8 years. This is consistent with a local response to El Nio warming for the ENSO mode, but a non-local response for the two adjacent modes. A similar analysis was performed for the Southern Oscillation Index and a spectral maximum was found between 12 and 16 years, consistent with our non-local interpretation of the previous two modes.
C1 [Breaker, Laurence C.] Moss Landing Marine Labs, Moss Landing, CA 92923 USA.
[Ruzmaikin, Alexander] Jet Prop Lab, Pasadena, CA 91009 USA.
RP Breaker, LC (reprint author), Moss Landing Marine Labs, Moss Landing, CA 92923 USA.
EM Lbreaker@mlml.calstate.edu
NR 46
TC 20
Z9 21
U1 2
U2 14
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
J9 CLIM DYNAM
JI Clim. Dyn.
PD FEB
PY 2011
VL 36
IS 3-4
BP 545
EP 559
DI 10.1007/s00382-010-0865-4
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 716AL
UT WOS:000286937100011
ER
PT J
AU Kessell, A
Tversky, B
AF Kessell, Angela
Tversky, Barbara
TI Visualizing space, time, and agents: production, performance, and
preference
SO COGNITIVE PROCESSING
LA English
DT Article
DE Diagram; Production; Comprehension; Preference; Space; Time
ID SPATIAL DIAGRAM REPRESENTATIONS; MEMORY; KNOWLEDGE
AB Visualizations of space, time, and agents (or objects) are ubiquitous in science, business, and everyday life, from weather maps to scheduling meetings. Effective communications, including visual ones, emerge from use in the field, but no conventional visualization form has yet emerged for this confluence of information. The real-world spiral of production, comprehension, and use that fine-tunes communications can be accelerated in the laboratory. Here, we do so in search of effective visualizations of space, time, and agents. Users' production, preference, and performance aligned to favor matrix representations with time as rows or columns and space and agents as entries. Overall, performance and preference were greater for matrices with discrete dots representing cell entries than for matrices with lines, but lines connecting cells may provide an advantage when evaluating temporal sequence. Both the diagram type and the technique have broader applications.
C1 [Kessell, Angela] Stanford Univ, Stanford, CA 94305 USA.
[Tversky, Barbara] Columbia Teachers Coll, New York, NY USA.
RP Kessell, A (reprint author), San Jose State Univ, NASA, Ames Res Ctr, Mail Stop 262-4, San Jose, CA 94035 USA.
EM angela.kessell@nasa.gov
NR 19
TC 8
Z9 8
U1 0
U2 4
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1612-4782
J9 COGN PROCESS
JI Cogn. Process.
PD FEB
PY 2011
VL 12
IS 1
BP 43
EP 52
DI 10.1007/s10339-010-0379-3
PG 10
WC Psychology, Experimental
SC Psychology
GA 711TE
UT WOS:000286613500006
PM 21082213
ER
PT J
AU Schultz, JK
Baker, JD
Toonen, RJ
Harting, AL
Bowen, BW
AF Schultz, Jennifer K.
Baker, Jason D.
Toonen, Robert J.
Harting, Albert L.
Bowen, Brian W.
TI Range-Wide Genetic Connectivity of the Hawaiian Monk Seal and
Implications for Translocation
SO CONSERVATION BIOLOGY
LA English
DT Article
DE pinniped; population connectivity; stock structure; translocation
ID POPULATION-STRUCTURE; MICROSATELLITE MARKERS; MONACHUS-SCHAUINSLANDI;
MIGRATION RATES; DIFFERENTIATION; CONSERVATION; MANAGEMENT; INFERENCE;
SOFTWARE; PATTERNS
AB The Hawaiian monk seal (Monachus schauinslandi) is one of the most critically endangered marine mammals. Less than 1200 individuals remain, and the species is declining at a rate of approximately 4% per year as a result of juvenile starvation, shark predation, and entanglement in marine debris. Some of these problems may be alleviated by translocation; however, if island breeding aggregates are effectively isolated subpopulations, moving individuals may disrupt local adaptations. In these circumstances, managers must balance the pragmatic need of increasing survival with theoretical concerns about genetic viability. To assess range-wide population structure of the Hawaiian monk seal, we examined an unprecedented, near-complete genetic inventory of the species (n = 1897 seals, sampled over 14 years) at 18 microsatellite loci. Genetic variation was not spatially partitioned ((theta) over cap (w) = -0.03, p = 1.0), and a Bayesian clustering method provided evidence of one panmictic population (K = 1). Pairwise F-ST comparisons (among 7 island aggregates over 14 annual cohorts) did not reveal temporally stable, spatial reproductive isolation. Our results coupled with long-term tag-resight data confirm seal movement and gene flow throughout the Hawaiian Archipelago. Thus, human-mediated translocation of seals among locations is not likely to result in genetic incompatibilities.
C1 [Schultz, Jennifer K.; Toonen, Robert J.; Bowen, Brian W.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA.
[Baker, Jason D.] Natl Marine Fisheries Serv, Pacific Islands Fisheries Sci Ctr, Honolulu, HI 96822 USA.
[Harting, Albert L.] Harting Biol Consulting, Bozeman, MT 59715 USA.
RP Schultz, JK (reprint author), Univ Hawaii, Sch Ocean & Earth Sci & Technol, Hawaii Inst Marine Biol, POB 1346, Kaneohe, HI 96744 USA.
EM jschultz@hawaii.edu
RI Toonen, Rob/K-2891-2012
OI Toonen, Rob/0000-0001-6339-4340
FU Papahanaumokuakea Marine National Monument; Marine Conservation Biology
Institute; National Marine Fisheries Service; Environmental Protection
Agency; National Science Foundation Integrative Graduate Education and
Research [OCE-0453167]; School of Ocean and Earth Science and Technology
Young Investigator Program
FX We thank the numerous seasonal field crews for their efforts in the
collection of data and tissue plugs. Thanks to T. Johanos for
unpublished National Marine Fisheries Service data. C. Littnan and F.
Parrish provided helpful comments on this manuscript. Funding for this
project was provided by the Papahanaumokuakea Marine National Monument,
the Marine Conservation Biology Institute, and the National Marine
Fisheries Service. J.K.S. was supported by an Environmental Protection
Agency Science to Achieve Results Fellowship, a National Science
Foundation Integrative Graduate Education and Research Traineeship
Program Fellowship awarded to B. Wilcox (OCE-0453167), and the School of
Ocean and Earth Science and Technology Young Investigator Program. We
thank editors G. Meffe and R. Waples and three anonymous reviewers who
provided insightful recommendations that greatly improved this
manuscript. This is contribution 1414 from the Hawaii Institute of
Marine Biology and contribution 7988 from the School of Ocean and Earth
Science and Technology at the University of Hawaii.
NR 56
TC 8
Z9 8
U1 4
U2 43
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0888-8892
EI 1523-1739
J9 CONSERV BIOL
JI Conserv. Biol.
PD FEB
PY 2011
VL 25
IS 1
BP 124
EP 132
DI 10.1111/j.1523-1739.2010.01615.x
PG 9
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 708QX
UT WOS:000286380500015
PM 21166713
ER
PT J
AU Nguyen, AN
Messenger, S
AF Nguyen, Ann N.
Messenger, Scott
TI Presolar History Recorded in Extraterrestrial Materials
SO ELEMENTS
LA English
DT Article
DE circumstellar and interstellar dust; stellar evolution and
nucleosynthesis; galactic evolution; Solar System formation; nanoscale
analytical techniques
ID GIANT BRANCH STARS; SILICON-CARBIDE; INTERPLANETARY DUST; MURCHISON
METEORITE; SOLAR-SYSTEM; AGB STARS; GRAINS; ISOTOPES; NUCLEOSYNTHESIS;
MOLYBDENUM
AB Extraterrestrial samples include a rich variety of materials with different histories. Among the array of Solar System materials are tiny grains with extremely anomalous isotopic compositions-records of nucleosynthetic processes that occurred deep within their now extinct parent stars. The isotopic and mineralogical characterization of these presolar grains in the laboratory provides unprecedented insight into stellar and galactic evolution, nucleosynthesis, and dust formation and processing. The discovery of presolar grains has opened up a pivotal new dimension in the field of astrophysics. Coupled with astronomical observations and astrophysical studies, stardust analyses bring nanometer-scale detail to the history of our immense Galaxy.
C1 [Nguyen, Ann N.; Messenger, Scott] NASA, Lyndon B Johnson Space Ctr, ARES, Robert M Walker Lab Space Sci, Houston, TX 77058 USA.
[Nguyen, Ann N.] ESCG Jacobs Technol, Houston, TX 77058 USA.
RP Nguyen, AN (reprint author), NASA, Lyndon B Johnson Space Ctr, ARES, Robert M Walker Lab Space Sci, Houston, TX 77058 USA.
EM lan-anh.n.nguyen@nasa.gov; scott.r.messenger@nasa.gov
NR 32
TC 9
Z9 9
U1 0
U2 3
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 1811-5209
J9 ELEMENTS
JI Elements
PD FEB
PY 2011
VL 7
IS 1
BP 17
EP 22
DI 10.2113/gselements.7.1.17
PG 6
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 730OL
UT WOS:000288043200005
ER
PT J
AU Brodeur, RD
Daly, EA
Benkwitt, CE
Morgan, CA
Emmett, RL
AF Brodeur, Richard D.
Daly, Elizabeth A.
Benkwitt, Cassandra E.
Morgan, Cheryl A.
Emmett, Robert L.
TI Catching the prey: Sampling juvenile fish and invertebrate prey fields
of juvenile coho and Chinook salmon during their early marine residence
SO FISHERIES RESEARCH
LA English
DT Article
DE Prey fields; Sampling gears; Catchability; Micronekton; Salmon diets;
California Current
ID COLUMBIA RIVER PLUME; DIEL FEEDING CHRONOLOGY; ONCORHYNCHUS-KISUTCH;
PACIFIC SALMON; GASTRIC EVACUATION; CONTINENTAL-SHELF; FOOD-CONSUMPTION;
NORTH-AMERICA; OREGON; WATERS
AB Marine diets of juvenile coho (Oncorhynchus kisutch) and Chinook salmon (Oncorhynchus tshawytscha) in the northern California Current are made up primarily of micronekton prey including juvenile fish, adult euphausiids, and large crab megalopae. However, these animals are seldom caught in the conventional plankton gears used to define juvenile salmon prey fields in ocean salmon programs. Four types of sampling gears with various mouth openings and configurations were examined for the ability to catch known juvenile salmon prey. Samples were examined for differences in species composition, relative biomass, length distribution, and taxonomic overlap with prey in the diets of salmon sampled concurrently. The herring, Marinovich, and Methot trawl nets generally caught juvenile prey fish such as hexagrammids, rockfish, cottids, and osmerids. These prey were in the 15-95 mm fork-length range, consistent with the type and size eaten by juvenile salmon. The bongo net sampled smaller invertebrate prey, which are rarely eaten by juvenile salmon, but instead are common prey of the juvenile fish that salmon consume. Overlap between prey fields and salmon diets was moderate for samples from the larger gear types but low for those from bongo nets towed in the same area. The fact that no gear matched exactly with coho and Chinook salmon diets was related to differences in catchability of the prey in different gears but may also in part be probably due to the high mobility of juvenile salmon, which enables these fish to consume food in locations distant from where they are sampled, and also to selectively feed in areas of high prey concentration. Based on our analysis, we recommend the use of micronekton gears with larger mouth openings and mesh sizes for better filtration rather than standard plankton gears (i.e., bongo nets) for direct estimates of available prey resources for juvenile coho or Chinook salmon. Sampling the abundance, size, and distribution of prey fields for juvenile salmon during their first summer in the ocean, a period of high natural mortality, may help us to better understand the mechanisms of bottom-up forcing on interannual changes in salmon mortality. Published by Elsevier B.V.
C1 [Brodeur, Richard D.; Emmett, Robert L.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Hatfield Marine Sci Ctr, Newport, OR 97365 USA.
[Daly, Elizabeth A.; Morgan, Cheryl A.] Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA.
[Benkwitt, Cassandra E.] Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA.
RP Brodeur, RD (reprint author), Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Hatfield Marine Sci Ctr, Newport, OR 97365 USA.
EM rick.brodeur@noaa.gov
OI Benkwitt, Cassandra/0000-0001-6756-7958
FU Bonneville Power Administration; NOAA Northwest Fisheries Science Center
FX We are grateful to those who helped collect the data including Chris
Toole, Lanaya Fitzgerald, Scott Heppell, Toby Auth, and the captain and
crews of the RV Miller Freeman, FV Piky, and FV Frosti. Mike Halstead of
Eastside Nets modified a previous version of the herring trawl to make
it suitable for use in the ocean environment. We thank Ed Casillas, Bill
Pearcy, and two anonymous reviewers for helpful comments on earlier
versions of the manuscript. This research was supported by the
Bonneville Power Administration and the NOAA Northwest Fisheries Science
Center.
NR 38
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Z9 12
U1 0
U2 15
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-7836
J9 FISH RES
JI Fish Res.
PD FEB
PY 2011
VL 108
IS 1
BP 65
EP 73
DI 10.1016/j.fishres.2010.11.023
PG 9
WC Fisheries
SC Fisheries
GA 722JM
UT WOS:000287428500009
ER
PT J
AU Ma, WP
Jacobs, G
Sparks, DE
Gnanamani, MK
Pendyala, VRR
Yen, CH
Klettlinger, JLS
Tomsik, TM
Davis, BH
AF Ma, Wenping
Jacobs, Gary
Sparks, Dennis E.
Gnanamani, Muthu K.
Pendyala, Venkat Ramana Rao
Yen, Chia H.
Klettlinger, Jennifer L. S.
Tomsik, Thomas M.
Davis, Burtron H.
TI Fischer-Tropsch synthesis: Support and cobalt cluster size effects on
kinetics over Co/Al2O3 and Co/SiO2 catalysts
SO FUEL
LA English
DT Article
DE Fischer-Tropsch synthesis; Water effect; Cobalt catalyst; Co cluster
size effect; Support effect
ID PARTICLE-SIZE; CO HYDROGENATION; STEADY-STATE; DEACTIVATION MECHANISM;
HYDROCARBON SYNTHESIS; INTRINSIC KINETICS; IRON CATALYSTS; SLURRY-PHASE;
WATER; SELECTIVITY
AB The influence of support type and cobalt cluster size (i.e., with average diameters falling within the range of 8-40 nm) on the kinetics of Fischer-Tropsch synthesis (FT) were investigated by kinetic tests employing a CSTR and two Co/gamma-Al2O3 catalysts having different average pore sizes, and two Co/SiO2 catalysts prepared on the same support but having different loadings. A kinetic model -r(CO) = kP(CO)(a)P(H2)(b)/(1 + mP(H2O)/P-H2) that contains a water effect constant "m" was used to fit the experimental data obtained with all four catalysts. Kinetic parameters suggest that both support type and average Co particle size impact FT behavior. Cobalt cluster size influenced kinetic parameters such as reaction order, rate constant, and the water effect parameter. In the cluster size range studied, decreasing the average Co cluster diameter by about 30% led to an increase in the intrinsic reaction rate constant k, defined on a per g of catalyst basis, by 62-102% for the gamma-Al2O3 and SiO2-supported cobalt catalysts. This increase was due to the higher active Co-0 surface site density as measured by hydrogen chemisorption. Moreover, less inhibition by adsorbed CO and greater H-2 dissociation on catalysts having smaller Co particles was suggested by the higher a and lower b values obtained for the measured reaction orders. Interestingly, irrespective of support type, the catalysts having smaller average Co particles were more sensitive to water. Comparing the catalysts having strong interactions between cobalt and support (Co/Al2O3) to the ones with weak interactions (Co/SiO2), the water effect parameters were found to be positive (indicating a negative influence on CO conversion) and negative (denoting a positive effect on CO conversion), respectively. No clear trend was observed for b values among the different supports, but greater a and a/b values were observed for both Al2O3-supported Co catalysts, implying greater inhibition of the FT rate by strongly adsorbed CO on Co/Al2O3 relative to Co/SiO2. For both supports, the order on P-CO was always found to be negative (i.e., suggesting an inhibiting effect) and positive for P-H2 for all four catalysts. The order of the reaction on P-H2 was close to 0.5, suggesting that dissociated H-2 is likely involved in the catalytic cycle. Finally, in the limited range of average pore diameters studied (13.5 and 18.2 nm), the average pore size of the Al2O3-supported Co catalysts displayed no observable impact on the reaction rate or water effect, suggesting either that the reaction is kinetically controlled, or that the pore size difference was not significant enough to elicit a measurable response. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Ma, Wenping; Jacobs, Gary; Sparks, Dennis E.; Gnanamani, Muthu K.; Pendyala, Venkat Ramana Rao; Davis, Burtron H.] Univ Kentucky, Ctr Appl Energy Res, Lexington, KY 40511 USA.
[Yen, Chia H.; Klettlinger, Jennifer L. S.; Tomsik, Thomas M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Davis, BH (reprint author), Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA.
EM davis@caer.uky.edu
RI Gnanamani, Muthu Kumaran/M-7736-2015; Jacobs, Gary/M-5349-2015
OI Gnanamani, Muthu Kumaran/0000-0003-1274-2645; Jacobs,
Gary/0000-0003-0691-6717
FU NASA [NNX07AB93A]; Commonwealth of Kentucky
FX This work was supported by NASA contract, #NNX07AB93A and the
Commonwealth of Kentucky.
NR 78
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Z9 36
U1 0
U2 63
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0016-2361
J9 FUEL
JI Fuel
PD FEB
PY 2011
VL 90
IS 2
BP 756
EP 765
DI 10.1016/j.fuel.2010.10.029
PG 10
WC Energy & Fuels; Engineering, Chemical
SC Energy & Fuels; Engineering
GA 683FZ
UT WOS:000284458900040
ER
PT J
AU Frankenberg, C
Butz, A
Toon, GC
AF Frankenberg, C.
Butz, A.
Toon, G. C.
TI Disentangling chlorophyll fluorescence from atmospheric scattering
effects in O-2 A-band spectra of reflected sun-light
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID FOURIER-TRANSFORM SPECTROMETER; ROTATIONAL RAMAN-SCATTERING; GASES
OBSERVING SATELLITE; VECTOR RADIATIVE-TRANSFER; PLANT FLUORESCENCE;
MODEL-CALCULATIONS; CO2 RETRIEVAL; INSTRUMENT; AEROSOL; PHOTOSYNTHESIS
AB Global retrieval of solar induced fluorescence emitted by terrestrial vegetation can provide an unprecedented measure for photosynthetic efficiency. The GOSAT (JAXA, launched Feb. 2009) and OCO-2 (NASA, to be launched 2013) satellites record high-resolution spectra in the O-2 A-band region, overlapping part of the chlorophyll fluorescence spectrum. We show that fluorescence cannot be unambiguously discriminated from atmospheric scattering effects using O-2 absorption lines. This can cause systematic biases in retrieved scattering parameters (aerosol optical thickness, aerosol height, surface pressure, surface albedo) if fluorescence is neglected. Hence, we demonstrate an efficient alternative fluorescence least-squares retrieval method based solely on strong Fraunhofer lines in the vicinity of the O-2 A-band, disentangling fluorescence from scattering effects. Not only does the Fraunhofer line fit produce a more accurate estimate of fluorescence emission, but it also allows improved retrievals of atmospheric aerosols from the O-2 A-band. Citation: Frankenberg, C., A. Butz, and G. C. Toon (2011), Disentangling chlorophyll fluorescence from atmospheric scattering effects in O-2 A-band spectra of reflected sun-light, Geophys. Res. Lett., 38, L03801, doi:10.1029/2010GL045896.
C1 [Frankenberg, C.; Toon, G. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Butz, A.] SRON Netherlands Inst Space Res, NL-3584 Utrecht, Netherlands.
RP Frankenberg, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM christian.frankenberg@jpl.nasa.gov
RI Butz, Andre/A-7024-2013; Frankenberg, Christian/A-2944-2013
OI Butz, Andre/0000-0003-0593-1608; Frankenberg,
Christian/0000-0002-0546-5857
FU Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration
FX We thank O. Hasekamp and J. Landgraf from the SRON-Netherlands Institute
for Space Research for kindly providing their radiative transfer code
used in this study. The research described in this paper was carried out
by the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
NR 38
TC 57
Z9 57
U1 5
U2 40
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 FEB 1
PY 2011
VL 38
AR L03801
DI 10.1029/2010GL045896
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 717IY
UT WOS:000287038100002
ER
PT J
AU Mazarico, E
Neumann, GA
Smith, DE
Zuber, MT
Torrence, MH
AF Mazarico, E.
Neumann, G. A.
Smith, D. E.
Zuber, M. T.
Torrence, M. H.
TI Illumination conditions of the lunar polar regions using LOLA topography
SO ICARUS
LA English
DT Article
DE Moon
ID RECONNAISSANCE ORBITER MISSION; PLANETARY SCIENCE; NEUTRON DETECTOR;
MOON; CLEMENTINE; DEPOSITS; SURFACE; POLES; SHAPE; ICE
AB We use high-resolution altimetry data obtained by the Lunar Orbiter Laser Altimeter instrument onboard the Lunar Reconnaissance Orbiter to characterize present illumination conditions in the polar regions of the Moon. Compared to previous studies, both the spatial and temporal extent of the simulations are increased significantly, as well as the coverage (fill ratio) of the topographic maps used, thanks to the 28 Hz firing rate of the five-beam instrument. We determine the horizon elevation in a number of directions based on 240 m-resolution polar digital elevation models reaching down to similar to 75 degrees latitude. The illumination of both polar regions extending to similar to 80 degrees can be calculated for any geometry from those horizon longitudinal profiles. We validated our modeling with recent Lunar Reconnaissance Orbiter Wide-Angle Camera images. We assessed the extent of permanently shadowed regions (PSRs, defined as areas that never receive direct solar illumination), and obtained total areas generally larger than previous studies (12,866 and 16,055 km(2), in the north and south respectively). We extended our direct illumination model to account for singly-scattered light, and found that every PSR does receive some amount of scattered light during the year. We conducted simulations over long periods (several 18.6-years lunar precession cycles) with a high temporal resolution (6 h), and identified the most illuminated locations in the vicinity of both poles. Because of the importance of those sites for exploration and engineering considerations, we characterized their illumination more precisely over the near future. Every year, a location near the Shackleton crater rim in the south polar region is sunlit continuously for 240 days, and its longest continuous period in total darkness is about 1.5 days. For some locations small height gains (similar to 10 m) can dramatically improve their average illumination and reduce the night duration, rendering some of those particularly attractive energy-wise as possible sites for near-continuous sources of solar power. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Mazarico, E.; Neumann, G. A.; Smith, D. E.; Torrence, M. H.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Mazarico, E.; Smith, D. E.; Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Torrence, M. H.] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA.
RP Mazarico, E (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698,B34 W271, Greenbelt, MD 20771 USA.
EM erwan.m.mazarico@nasa.gov
RI Neumann, Gregory/I-5591-2013; Mazarico, Erwan/N-6034-2014
OI Neumann, Gregory/0000-0003-0644-9944; Mazarico,
Erwan/0000-0003-3456-427X
FU NASA
FX EM wishes to acknowledge support from the NASA Postdoctoral Program,
administered by the Oak Ridge Associated Universities, under a contract
with NASA. We would like to thank the LRO Project and the LOLA
Instrument Team. We also acknowledge Jurgen Oberst and Frank Scholten
(DLR) who provided the LROC WAC images used in Fig. 5; Timothy Stubbs
and Yongli Wang for comparisons with their ray-tracing model; and
Emerson Spereyer and Mark Robinson (ASU) who provided more recent LROC
WAC images used in Fig. S1.
NR 44
TC 45
Z9 48
U1 0
U2 8
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2011
VL 211
IS 2
BP 1066
EP 1081
DI 10.1016/j.icarus.2010.10.030
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 715TE
UT WOS:000286909700011
ER
PT J
AU Immer, C
Metzger, P
Hintze, PE
Nick, A
Horan, R
AF Immer, Christopher
Metzger, Philip
Hintze, Paul E.
Nick, Andrew
Horan, Ryan
TI Apollo 12 Lunar Module exhaust plume impingement on Lunar Surveyor III
SO ICARUS
LA English
DT Article
DE Moon, Surface; Experimental techniques; Cratering; Impact processes
ID DESCENT ENGINE; SOIL
AB Understanding plume impingement by retrorockets on the surface of the Moon is paramount for safe lunar outpost design in NASA's planned return to the Moon for the Constellation Program. Visual inspection, Scanning Electron Microscopy, and surface scanned topology have been used to investigate the damage to the Lunar Surveyor Ill spacecraft that was caused by the Apollo 12 Lunar Module's close proximity landing. Two parts of the Surveyor Ill craft returned by the Apollo 12 astronauts, Coupons 2050 and 2051, which faced the Apollo 12 landing site, show that a fine layer of lunar regolith coated the materials and was subsequently removed by the Apollo 12 Lunar Module landing rocket. The coupons were also pitted by the impact of larger soil particles with an average of 103 pits/cm(2). The average entry size of the pits was 83.7 mu m (major diameter) x 74.5 mu m (minor diameter) and the average estimated penetration depth was 88.4 mu m. Pitting in the surface of the coupons correlates to removal of lunar fines and is likely a signature of lunar material imparting localized momentum/energy sufficient to cause cracking of the paint. Comparison with the lunar soil particle size distribution and the optical density of blowing soil during lunar landings indicates that the Surveyor III spacecraft was not exposed to the direct spray of the landing Lunar Module, but instead experienced only the fringes of the spray of soil. Had Surveyor Ill been exposed to the direct spray, the damage would have been orders of magnitude higher. Published by Elsevier Inc.
C1 [Metzger, Philip] NASA, Granular Mech & Regolith Operat Lab, Kennedy Space Ctr, FL 32899 USA.
[Immer, Christopher; Nick, Andrew; Horan, Ryan] ASRC Aerosp, Appl Phys Lab, Kennedy Space Ctr, FL 32899 USA.
[Hintze, Paul E.] NASA, Corros Technol Lab, Kennedy Space Ctr, FL 32899 USA.
RP Metzger, P (reprint author), NASA, Granular Mech & Regolith Operat Lab, NE-S-1, Kennedy Space Ctr, FL 32899 USA.
EM christopher.d.immer@nasa.gov; Philip.T.Metzger@nasa.gov;
Paul.E.Hintze@nasa.gov; andrew.j.nick@nasa.gov; ryan.j.horan@nasa.gov
RI Metzger, Philip/R-3136-2016;
OI Metzger, Philip/0000-0002-6871-5358; Hintze, Paul/0000-0002-9962-2955
FU Kennedy Space Center
FX We would like to thank Kennedy Space Center's Core Technical
Capabilities program and the program manager, Linda Shayknian for
funding to pursue this study. We would like to thank Gary Lofgren and
Judith Alton at the Curatorial facility at Johnson Space center for help
selecting the parts to study and making them available to us for loan
and also for access to the Lunar Material Archives. We would like to
thank United Space Alliance and Chris Martin for help using the
Cyberscan and Veeco Instruments.
NR 41
TC 21
Z9 23
U1 0
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2011
VL 211
IS 2
BP 1089
EP 1102
DI 10.1016/j.icarus.2010.11.013
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 715TE
UT WOS:000286909700013
ER
PT J
AU Abu-Surra, S
Divsalar, D
Ryan, WE
AF Abu-Surra, Shadi
Divsalar, Dariush
Ryan, William E.
TI Enumerators for Protograph-Based Ensembles of LDPC and Generalized LDPC
Codes
SO IEEE TRANSACTIONS ON INFORMATION THEORY
LA English
DT Article
DE Asymptotic enumerators; finite-length enumerators; IDPC codes;
protograph; pseudoweight enumerators; stopping set enumerators; trapping
set enumerators; weight enumerators
ID PARITY-CHECK CODES; FLOOR TANNER CODES; DISTANCE DISTRIBUTIONS; GRAPHS;
SETS
AB Protograph-based LDPC and generalized LDPC (G-LDPC) codes have the advantages of a simple design procedure and highly structured encoders and decoders. The design of such "protograph-based codes" relies on what is effectively a computer-based search. As such, following Gallager, it is prudent to restrict the search to a "good ensemble," for example, an ensemble whose minimum distance grows linearly with codeword length. A good ensemble can also mean one with good stopping set, trapping set, or pseudocodeword properties. In this paper, ensemble codeword weight enumerators for finite-length LDPC and G-LDPC codes based on protographs were derived, and then the asymptotic case was considered. The asymptotic results allow us to determine whether or not the typical relative minimum distance in the ensemble grows linearly with codeword length. Then, the codeword weight enumerator technique is adapted to yield ensemble stopping set, trapping set, and pseudocodeword enumerators for protograph LDPC and G-LDPC codes. In this case, the asymptotic results allow us to determine whether or not the typical relative smallest stopping set size, trapping set size, and pseudoweight grows linearly with codeword length. Trapping set enumerators for G-LDPC code ensembles represent a more complex problem which we do not consider here.
C1 [Abu-Surra, Shadi; Ryan, William E.] Univ Arizona, Dept Elect & Comp Engn, Tucson, AZ 85721 USA.
[Divsalar, Dariush] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Abu-Surra, S (reprint author), Samsung Telecommun Amer, Richardson, TX 75082 USA.
EM sasurra@sta.samsung.com; Dariush.Divsalar@jpl.nasa.gov;
ryan@ece.arizona.edu
NR 54
TC 30
Z9 33
U1 1
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9448
EI 1557-9654
J9 IEEE T INFORM THEORY
JI IEEE Trans. Inf. Theory
PD FEB
PY 2011
VL 57
IS 2
BP 858
EP 886
DI 10.1109/TIT.2010.2094819
PG 29
WC Computer Science, Information Systems; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA 710LW
UT WOS:000286514200018
ER
PT J
AU Mengshoel, OJ
Wilkins, DC
Roth, D
AF Mengshoel, Ole J.
Wilkins, David C.
Roth, Dan
TI Initialization and Restart in Stochastic Local Search: Computing a Most
Probable Explanation in Bayesian Networks
SO IEEE TRANSACTIONS ON KNOWLEDGE AND DATA ENGINEERING
LA English
DT Article
DE Stochastic local search; Bayesian networks; initialization; restart;
finite mixture models
ID BELIEF NETWORKS; ALGORITHMS; INFERENCE; HARD; SAT; FRAMEWORK; PRODUCT
AB For hard computational problems, stochastic local search has proven to be a competitive approach to finding optimal or approximately optimal problem solutions. Two key research questions for stochastic local search algorithms are: Which algorithms are effective for initialization? When should the search process be restarted? In the present work, we investigate these research questions in the context of approximate computation of most probable explanations (MPEs) in Bayesian networks (BNs). We introduce a novel approach, based on the Viterbi algorithm, to explanation initialization in BNs. While the Viterbi algorithm works on sequences and trees, our approach works on BNs with arbitrary topologies. We also give a novel formalization of stochastic local search, with focus on initialization and restart, using probability theory and mixture models. Experimentally, we apply our methods to the problem of MPE computation, using a stochastic local search algorithm known as Stochastic Greedy Search. By carefully optimizing both initialization and restart, we reduce the MPE search time for application BNs by several orders of magnitude compared to using uniform at random initialization without restart. On several BNs from applications, the performance of Stochastic Greedy Search is competitive with clique tree clustering, a state-of-the-art exact algorithm used for MPE computation in BNs.
C1 [Mengshoel, Ole J.] Carnegie Mellon Univ, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wilkins, David C.] Stanford Univ, Symbol Syst Program, Stanford, CA 94305 USA.
[Roth, Dan] Univ Illinois, Dept Comp Sci, Urbana, IL 61801 USA.
RP Mengshoel, OJ (reprint author), Carnegie Mellon Univ, NASA, Ames Res Ctr, Mail Stop 269-3,Bldg T35-B,Rm 107,POB 1, Moffett Field, CA 94035 USA.
EM ole.mengshoel@sv.cmu.edu; dwilkins@stanford.edu; danr@cs.uiuc.edu
FU NASA [NCC2-1426]; US National Science Foundation (NSF) [CCF-0937044,
ECCS-0931978]; ONR [N00014-95-1-0749]; ARL [DAAL01-96-2-0003]; NRL
[N00014-97-C-2061]; NSF [IIS-9801638, SBR-987345]
FX This material is based, in part, upon work by Ole J. Mengshoel supported
by NASA award NCC2-1426 as well as the US National Science Foundation
(NSF) grants CCF-0937044 and ECCS-0931978. Ole J. Mengshoel and David C.
Wilkins gratefully acknowledge support in part by ONR grant
N00014-95-1-0749, ARL grant DAAL01-96-2-0003, and NRL grant
N00014-97-C-2061. Dan Roth gratefully acknowledges the support of NSF
grants IIS-9801638 and SBR-987345. David Fried and Song Han are
acknowledged for their codevelopment of the Raven software, used in
experimental work reported here. Comments from the anonymous reviewers,
which helped improve the paper, are also acknowledged.
NR 46
TC 5
Z9 5
U1 0
U2 2
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1041-4347
EI 1558-2191
J9 IEEE T KNOWL DATA EN
JI IEEE Trans. Knowl. Data Eng.
PD FEB
PY 2011
VL 23
IS 2
BP 235
EP 247
DI 10.1109/TKDE.2010.98
PG 13
WC Computer Science, Artificial Intelligence; Computer Science, Information
Systems; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA 695SA
UT WOS:000285391700006
ER
PT J
AU Platt, CMR
Vaughan, MA
Austin, RT
AF Platt, C. M. R.
Vaughan, M. A.
Austin, R. T.
TI Characteristics of CALIPSO and CloudSat Backscatter at the Top Center
Layers of Mesoscale Convective Systems and Relation to Cloud
Microphysics
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID CIRRUS CLOUDS; ICE CRYSTALS; OPTICAL-PROPERTIES; RADIATIVE-TRANSFER;
SINGLE-SCATTERING; LIGHT-SCATTERING; PARTICLE SHAPES; LIDAR; EXTINCTION;
LITE
AB Following the discovery of anomalously high values of lidar integrated attenuated backscatter near the top center layers of mesoscale convective systems (MCSs) observed by the NASA Lidar In-Space Technology Experiment (LITE), a search of Cloud Aerosol Lidar with Orthogonal Polarization (CALIOP) data on board the Cloud Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) platform revealed the same phenomena in a sample of eight MCSs investigated. The backscatter depolarization ratio also showed changes concurrent with the high integrated backscatter and either increased or decreased concurrently with the anomalous backscatter. Simultaneous CloudSat data in the A-Train formation showed a cloud-top altitude similar to that measured by CALIOP, indicating fairly large ice crystals were reaching cloud top. Based on previous work, the CALIOP and CloudSat returns were likely due to a mix of small ice droxtals or frozen drops extending in a continuous spectrum to large crystals composed of well-formed hexagonal columns, thick hexagonal plates, spheroids, and irregular particles. The CALIOP lidar would detect the whole spectrum whereas CloudSat would detect ice crystals greater than similar to 30 mu m in effective radius; there were apparently enough of such crystals to allow CloudSat to detect a cloud-top height similar to that found by CALIOP. Using such a model, it was estimated that the measured backscatter phase function in the most active part of the cloud could be reconciled approximately with theoretical values of the various crystal habits. However, it was harder to reconcile the changes in depolarization ratio given the absence of values of this parameter for small droxtal crystals.
C1 [Platt, C. M. R.] CSIRO Marine & Atmospher Res, Aspendale, Vic, Australia.
[Vaughan, M. A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Austin, R. T.] Colorado State Univ, Ft Collins, CO 80523 USA.
RP Platt, CMR (reprint author), 47 Koetong Parade, Mt Eliza, Vic, Australia.
EM mplatt@net2000.com.au
FU NASA Langley Research Center; Colorado State University
FX Author C. M. Platt thanks NASA Langley Research Center and Colorado
State University for financial support; Dr. Stuart Young, Dr. Yongxiang
Hu, Dr. Ken Sassen, and the paper reviewers made useful comments and
suggestions that have improved the paper substantially.
NR 24
TC 3
Z9 3
U1 0
U2 1
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD FEB
PY 2011
VL 50
IS 2
BP 368
EP 378
DI 10.1175/2010JAMC2537.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 733ZZ
UT WOS:000288304300008
ER
PT J
AU Marks, DA
Wolff, DB
Carey, LD
Tokay, A
AF Marks, David A.
Wolff, David B.
Carey, Lawrence D.
Tokay, Ali
TI Quality Control and Calibration of the Dual-Polarization Radar at
Kwajalein, RMI
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID DIFFERENTIAL PROPAGATION PHASE; POLARIMETRIC RADAR; REFLECTIVITY
CALIBRATION; RAINFALL ESTIMATION; TRMM; VALIDATION; SHAPE; SATELLITE;
RAINDROPS; CLOUD
AB The dual-polarization weather radar on the Kwajalein Atoll in the Republic of the Marshall Islands (KPOL)is one of the only full-time (24/7) operational S-band dual-polarimetric (DP) radars in the tropics. Through the use of KPOL DP and disdrometer measurements from Kwajalein, quality control (QC) and reflectivity calibration techniques were developed and adapted for use. Data studies in light rain show that KPOL DP measurements are of sufficient quality for these applications. While the methodology for the development of such applications is well documented, the tuning of specific algorithms to the particular regime and observed raindrop size distributions requires a comprehensive testing and adjustment period. Presented are algorithm descriptions and results from five case studies in which QC and absolute reflectivity calibration were performed and assessed. Also described is a unique approach for calibrating the differential reflectivity field when vertically pointing observations are not available. Results show the following: 1) DP-based QC provides superior results compared to the legacy Tropical Rainfall Measuring Mission (TRMM) QC algorithm (based on height and reflectivity thresholds), and 2) absolute reflectivity calibration can be performed using observations of light rain via a published differential phase based integration technique; results are within +/- 1 dB compared to independent measurements. Future extension of these algorithms to upgraded Weather Surveillance Radar-1988 Doppler (WSR-88D) polarization diverse radars will benefit National Aeronautics and Space Administration's (NASA's) Precipitation Measurement Missions (PMM) validation programs.
C1 [Marks, David A.; Wolff, David B.; Tokay, Ali] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Marks, David A.; Wolff, David B.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Carey, Lawrence D.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA.
[Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP Marks, DA (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-1, Greenbelt, MD 20771 USA.
EM david.a.marks@nasa.gov
RI Wolff, David/H-5502-2012; Measurement, Global/C-4698-2015
FU NASA [NNG07EJ50C]
FX This research is supported by NASA Grant NNG07EJ50C. The authors thank
Dr. Ramesh Kakar (NASA Headquarters), Dr. Arthur Hou (GPM Project
Scientist, NASA/GSFC), Dr. Scott Braun (TRMM Project Scientist,
NASA/GSFC), and Dr. Mathew Schwaller (GPM GV Program Manager, NASA/GSFC)
for their support of this effort. Appreciation is extended to David
Silberstein for numerous helpful discussions, and to the TRMM Satellite
Validation Office staff, including Bail Kelley, Jason Pippitt, David
Makofski, and Jianxin Wang. CSU-CHILL data were provided by Patrick
Kennedy of Colorado State University. NCAR S-Pol data were provided by
the NCAR ATD. We thank the staff of Atmospheric Technology Services
Company for providing KPOL data.
NR 45
TC 12
Z9 12
U1 1
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD FEB
PY 2011
VL 28
IS 2
BP 181
EP 196
DI 10.1175/2010JTECHA1462.1
PG 16
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 736VG
UT WOS:000288522500005
ER
PT J
AU Tselioudis, G
Rossow, WB
AF Tselioudis, George
Rossow, William B.
TI Time Scales of Variability of the Tropical Atmosphere Derived from
Cloud-Defined Weather States
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SURFACE; ISCCP; OCEAN; ENSO
AB The recent analysis of Rossow et al. used a clustering technique to derive six tropical weather states (WS) based on mesoscale cloud-type patterns and documented the spatial distribution of those WS and the modes of variability of the convective WS in the tropical western Pacific. In this study, the global tropics are separated into 30 degrees X 30 degrees regions, and a clustering algorithm is applied to the regional WS frequency distributions to derive the dominant modes of weather state variability (or the climate state variability) in each region. The results show that the whole tropical atmosphere oscillates between a convectively active and a convectively suppressed regime with the exception of the eastern parts of the two ocean basins, where the oscillation is between a stratocumulus and a trade cumulus regime. The dominant mode of both those oscillations is the seasonal cycle with the exception of the eastern Indian and western-central Pacific region, where El Nino frequencies dominate. The transitions between the convectively active and suppressed regimes produce longwave (LW) and shortwave (SW) top-of-atmosphere (TOA) radiative differences that are of opposite sign and of similar magnitude, being of order 20-30 W m(-2) over ocean and 10-20 W m(-2) over land and thus producing an overall balance in the TOA radiative budget. The precipitation differences between the convectively active and suppressed regimes are found to be of order 2.5-3 mm day(-1) ocean and 1-2.4 mm day(-1) over land. Finally, the transitions between the stratocumulus and shallow cumulus regimes produce noticeable TOA SW differences of order 10-20 W m(-2) and very small TOA LW and precipitation differences. The potential climate feedback implications of the regime radiation and precipitation differences are discussed.
C1 [Tselioudis, George] Columbia Univ, NASA GISS, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Tselioudis, George] Acad Athens, Res Ctr Atmospher Phys & Climatol, Athens, Greece.
[Rossow, William B.] CUNY City Coll, NOAA CREST Ctr, New York, NY 10031 USA.
RP Tselioudis, G (reprint author), Columbia Univ, NASA GISS, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA.
EM gt9@columbia.edu
RI Rossow, William/F-3138-2015
FU NASA [08MAP0004, NNXD7AN04G]
FX We thank Alison Sheffield for her valuable contribution in implementing
the clustering diagnostics. We also thank an anonymous reviewer for
thorough and constructive comments. Work by G. T and W. B. R was
supported by the NASA Modeling and Analysis Program (managed by Dr.
David Considine) under Grants 08MAP0004 and NNXD7AN04G.
NR 13
TC 9
Z9 9
U1 0
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD FEB 1
PY 2011
VL 24
IS 3
BP 602
EP 608
DI 10.1175/2010JCLI3574.1
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 734AB
UT WOS:000288304500002
ER
PT J
AU Pinty, B
Taberner, M
Haemmerle, VR
Paradise, SR
Vermote, E
Verstraete, MM
Gobron, N
Widlowski, JL
AF Pinty, Bernard
Taberner, Malcolm
Haemmerle, Vance R.
Paradise, Susan R.
Vermote, Eric
Verstraete, Michel M.
Gobron, Nadine
Widlowski, Jean-Luc
TI Global-Scale Comparison of MISR and MODIS Land Surface Albedos
SO JOURNAL OF CLIMATE
LA English
DT Article
ID RADIATIVE-TRANSFER CODE; BIDIRECTIONAL REFLECTANCE; ATMOSPHERIC
CORRECTION; VECTOR VERSION; SATELLITE DATA; AERONET SITES; VALIDATION;
RETRIEVAL; PRODUCTS; ENERGY
AB The Moderate Resolution Imaging Spectroradiometer (MODIS) white-sky surface albedos are compared with similar products generated on the basis of the Multiangle Imaging SpectroRadiometer (MISR) surface bidirectional reflectance factor (BRF) model parameters available for the year 2005. The analysis is achieved using global-scale statistics to characterize the broad patterns of these two independent albedo datasets. The results obtained in M. Taberner et al. have shown that robust statistics can be established and that both datasets are highly correlated. As a result, the slight but consistent biases and trends identified in this paper, derived from statistics obtained on a global basis, should be considered sufficiently reliable to merit further investigation. The present paper reports on the zonal- and seasonal-mean differences retrieved from the analysis of the MODIS and MISR surface albedo broadband products. The MISR - MODIS differences exhibit a systematic positive bias or offset in the range of 0.01-0.03 depending on the spectral domain of interest. Results obtained in the visible domain exhibit a well-marked and very consistent meridional trend featuring a "smile effect" such that the MISR - MODIS differences reach maxima at the highest latitudes in both hemispheres. The analysis of seasonal variations observed in MISR and MODIS albedo products reveals that, in the visible domain, the MODIS albedos generate weaker seasonal changes than MISR and that the differences increase poleward from the equatorial regions. A detailed investigation of MODIS and MISR aerosol optical depth retrievals suggests that this large-scale meridional trend is probably not caused by differences in the aerosol load estimated by each instrument. The scale and regularity of the meridional trend suggests that this may be due to the particular sampling regime of each instrument in the viewing azimuthal planes and/or approximations in the atmospheric correction processes. If this is the case, then either MODIS is underestimating, or MISR overestimating, the surface anisotropy or both.
C1 [Pinty, Bernard; Verstraete, Michel M.; Gobron, Nadine; Widlowski, Jean-Luc] Commiss European Communities, DG Joint Res Ctr, Inst Environm & Sustainabil, Global Environm Monitoring Unit, I-21027 Ispra, VA, Italy.
[Pinty, Bernard] ESA, ESRIN, Earth Observat Directorate, Frascati, Italy.
[Taberner, Malcolm] Plymouth Marine Lab, Remote Sensing Grp, Plymouth, Devon, England.
[Haemmerle, Vance R.; Paradise, Susan R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Vermote, Eric] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
RP Pinty, B (reprint author), Commiss European Communities, DG Joint Res Ctr, Inst Environm & Sustainabil, Global Environm Monitoring Unit, TP 272,Via Enrico Fermi 2749, I-21027 Ispra, VA, Italy.
EM bernard.pinty@jrc.ec.europa.eu
RI Vermote, Eric/K-3733-2012;
OI Verstraete, Michel/0000-0003-0968-8721
NR 35
TC 17
Z9 18
U1 1
U2 14
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD FEB 1
PY 2011
VL 24
IS 3
BP 732
EP 749
DI 10.1175/2010JCLI3709.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 734AB
UT WOS:000288304500011
ER
PT J
AU Imber, SM
Slavin, JA
Auster, HU
Angelopoulos, V
AF Imber, S. M.
Slavin, J. A.
Auster, H. U.
Angelopoulos, V.
TI A THEMIS survey of flux ropes and traveling compression regions:
Location of the near-Earth reconnection site during solar minimum
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MAGNETIC RECONNECTION; GEOTAIL OBSERVATIONS; AURORAL BRIGHTENINGS;
PLASMOID EJECTION; FLOW BURSTS; BULK FLOWS; MAGNETOTAIL; ISEE-3; IMP-8;
FIELD
AB A statistical study of flux ropes and traveling compression regions (TCRs) during the Time History of Events and Macroscale Interactions during Substorms second tail season has been performed. A combined total of 135 flux ropes and TCRs in the range GSM X similar to -14 to -31 R-E were identified, many of these occurring in series of two or more events separated by a few tens of seconds. Those occurring within 10 min of each other were combined into aggregated reconnection events. For the purposes of this survey, these are most likely the products of reconnection occurring simultaneously at multiple, closely spaced x-lines as opposed to statistically independent episodes of reconnection. The 135 flux ropes and TCRs were grouped into 87 reconnection events; of these, 28 were moving tailward and 59 were moving Earthward. The average location of the near-Earth x-line determined from statistical analysis of these reconnection events is (XGSM, Y*GSM) = (-30R(E), 5R(E)), where Y* includes a correction for the solar aberration angle. A strong east-west asymmetry is present in the tailward events, with >80% being observed at GSM Y* > 0. Our results indicate that the Earthward flows are similarly asymmetric in the midtail region, becoming more symmetric inside -18 R-E. Superposed epoch analyses indicate that the occurrence of reconnection closer to the Earth, i.e., X > -20 R-E, is associated with elevated solar wind velocity and enhanced negative interplanetary magnetic field B-Z. Reconnection events taking place closer to the Earth are also far more effective in producing geomagnetic activity, judged by the AL index, than reconnection initiated beyond X similar to -25 R-E.
C1 [Imber, S. M.; Slavin, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Auster, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterrestr Phys, D-38106 Braunschweig, Germany.
[Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
RP Imber, SM (reprint author), NASA, Goddard Space Flight Ctr, Code 670-0,Bldg 21,Greenbelt Rd, Greenbelt, MD 20771 USA.
EM suzanne.imber@nasa.gov
RI Slavin, James/H-3170-2012
OI Slavin, James/0000-0002-9206-724X
FU NASA [NAS5-02099]; DLR [50 OC 0302]
FX We acknowledge NASA contract NAS5-02099, DLR contract 50 OC 0302, and C.
W. Carlson and J. P. McFadden for use of ESA data.
NR 47
TC 47
Z9 47
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB 1
PY 2011
VL 116
AR A02201
DI 10.1029/2010JA016026
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 717IB
UT WOS:000287035800001
ER
PT J
AU Rosero, E
Gulden, LE
Yang, ZL
De Goncalves, LG
Niu, GY
Kaheil, YH
AF Rosero, Enrique
Gulden, Lindsey E.
Yang, Zong-Liang
De Goncalves, Luis G.
Niu, Guo-Yue
Kaheil, Yasir H.
TI Ensemble Evaluation of Hydrologically Enhanced Noah-LSM: Partitioning of
the Water Balance in High-Resolution Simulations over the Little Washita
River Experimental Watershed
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID LAND-SURFACE MODEL; PARAMETERIZATION SCHEMES; BASIN EXPERIMENT; DOWNWARD
APPROACH; TEMPORAL ANALYSIS; PART I; RUNOFF; PROJECT; CLIMATE; FLUXES
AB The ability of two versions of the Noah land surface model (LSM) to simulate the water cycle of the Little Washita River experimental watershed is evaluated. One version that uses the standard hydrological parameterizations of Noah 2.7 (STD) is compared another version that replaces STD's subsurface hydrology with a simple aquifer model and topography-related surface and subsurface runoff parameterizations (GW). Simulations on a distributed grid at fine resolution are compared to the long-term distribution of observed daily-mean runoff, the spatial statistics of observed soil moisture, and locally observed latent heat flux. The evaluation targets the typical behavior of ensembles of models that use realistic, near-optimal sets of parameters important to runoff. STD and GW overestimate the ratio of runoff to evapotranspiration. In the subset of STD and GW runs that best reproduce the timing and the volume of streamflow, the surface-to-subsurface runoff ratio is overestimated and simulated streamflow is much flashier than observations. Both models' soil columns wet and dry too quickly, implying that there are structural shortcomings in the formulation of STD that cannot be overcome by adding GW's increased complexity to the model. In its current formulation, GW extremely underestimates baseflow's contribution to total runoff and requires a shallow water table to function realistically. In the catchment (depth to water table > 10m), GW functions as a simple bucket model. Because model parameters are likely scale and site dependent, the need for even "physically based" models to be extensively calibrated for all domains on which they are applied is underscored.
C1 [Rosero, Enrique; Gulden, Lindsey E.; Yang, Zong-Liang] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX 78712 USA.
[De Goncalves, Luis G.] Univ Maryland, Maryland Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[De Goncalves, Luis G.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[Niu, Guo-Yue] Univ Arizona, Tucson, AZ USA.
[Kaheil, Yasir H.] Columbia Univ, Int Res Inst Climate & Soc, Palisades, NY USA.
RP Rosero, E (reprint author), Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, 1 Univ Stn C1100, Austin, TX 78712 USA.
EM liang@jsg.utexas.edu
RI Yang, Zong-Liang/B-4916-2011; de Goncalves, Luis Gustavo/G-2522-2012;
Niu, Guo-Yue/B-8317-2011;
OI de Goncalves, Luis Gustavo/0000-0002-1571-0916
FU OHD/NWS; NOAA [NA07OAR4310216]; NOAA-CPPA [GC08-521]; NSF; Jackson
School of Geosciences
FX The first author was supported by the Graduate Fellowship of the
Hydrology Training Program of the OHD/NWS. The project was also funded
by the NOAA Grant NA07OAR4310216, the NOAA-CPPA Proposal GC08-521, NSF,
and the Jackson School of Geosciences. Bailing Li, at NASA/GSFC,
provided us with 1 km-LIS land-cover, monthly vegetation fraction and
albedo climatology data. The NEXRAD stage IV was prepared by Seungbum
Hong at UT Austin. We acknowledge the USGS, ARS micronet and AmeriFlux
for the validation datasets. We thank D. J. Gochis at NCAR and K.
Mitchell at NCEP for their insight. We benefited from the computational
resources at the Texas Advanced Computing Center (TACC).
NR 83
TC 8
Z9 9
U1 2
U2 17
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD FEB
PY 2011
VL 12
IS 1
BP 45
EP 64
DI 10.1175/2010JHM1228.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 729YW
UT WOS:000287991600003
ER
PT J
AU Schneider, M
Hase, F
Blavier, JF
Toon, GC
Leblanc, T
AF Schneider, M.
Hase, F.
Blavier, J. -F.
Toon, G. C.
Leblanc, T.
TI An empirical study on the importance of a speed-dependent Voigt line
shape model for tropospheric water vapor profile remote sensing
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Water vapor; Molecular spectroscopy; High spectral resolution; Line
shape models; Speed-dependent Voigt line shape; Spectroscopic databases;
Hitran; Atmospheric remote sensing
ID SPECTROSCOPIC DATABASE; QUALITY ASSESSMENT; HIGH-RESOLUTION; FTIR;
RETRIEVAL; VALIDATION; PARAMETERS
AB We use high quality ground-based solar absorption spectra measured in close coincidence with Vaisala RS92 radiosonde in situ water vapor profiles to demonstrate that a Voigt line shape model yields systematic errors in the remotely sensed tropospheric water vapor profiles. We analyse absorption signatures of 4 (H2O)-O-16 and 2 (HDO)-O-16 bands situated between 790 and 4710 cm(-1). We find that applying a speed-dependent Voigt line shape model instead of a Voigt line shape model significantly improves the agreement between the water vapor profiles obtained by the radiosondes and by infrared remote-sensing in the different bands. An optimal agreement is obtained for a Gamma(2) (relaxation rate for speed-dependence) of 6-21% of Gamma(0) (Voigt relaxation rate), which is consistent to the values derived from laboratory experiments. Our study suggests that further extensive laboratory investigations of line shape models are a key for improving the quality of modern water vapor remote sensing products. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Schneider, M.; Hase, F.] KIT, IMK ASF, Karlsruhe, Germany.
[Schneider, M.] CIAI, Agencia Estatal Meteorol AEMET, Santa Cruz De Tenerife, Spain.
[Blavier, J. -F.; Toon, G. C.] CALTECH, JPL, Pasadena, CA USA.
[Leblanc, T.] CALTECH, JPL, Wrightwood, CA USA.
RP Schneider, M (reprint author), KIT, IMK ASF, Karlsruhe, Germany.
EM matthias.schneider@kit.edu
RI Hase, Frank/A-7497-2013; Schneider, Matthias/B-1441-2013
FU Deutsche Forschungsgemeinschaft [SCHN 1126/1-1, 1-2]; Spanish Ministry
of Science and Innovation; NASA
FX M. Schneider has been supported by the Deutsche Forschungsgemeinschaft
via the project RISOTO (Geschaftszeichen SCHN 1126/1-1 and 1-2) and
since May 2010 he enjoys a Ramon y Cajal Grant from the Spanish Ministry
of Science and Innovation. We are grateful to the Goddard Space Flight
Center for providing the temperature and pressure profiles of the
National Centers for Environmental Prediction via the automailer system.
Part of this work was performed at the Jet Propulsion Laboratory,
California Institute of Technology under contract with NASA. We thank K.
Yoshimura (U. Tokyo) for providing the IsoGSM
HD16O/H216O simulations.
NR 23
TC 22
Z9 22
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD FEB
PY 2011
VL 112
IS 3
BP 465
EP 474
DI 10.1016/j.jqsrt.2010.09.008
PG 10
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 716HP
UT WOS:000286960000009
ER
PT J
AU Spiering, BA
Lee, SMC
Mulavara, AP
Bentley, JR
Buxton, RE
Lawrence, EL
Sinka, J
Guilliams, ME
Ploutz-Snyder, LL
Bloomberg, JJ
AF Spiering, Barry A.
Lee, Stuart M. C.
Mulavara, Ajitkumar P.
Bentley, Jason R.
Buxton, Roxanne E.
Lawrence, Emily L.
Sinka, Joseph
Guilliams, Mark E.
Ploutz-Snyder, Lori L.
Bloomberg, Jacob J.
TI TEST BATTERY DESIGNED TO QUICKLY AND SAFELY ASSESS DIVERSE INDICES OF
NEUROMUSCULAR FUNCTION AFTER UNWEIGHTING
SO JOURNAL OF STRENGTH AND CONDITIONING RESEARCH
LA English
DT Article
DE aging; muscle; power; rehabilitation; spaceflight
ID STATISTICAL-METHODS; MOTOR-PERFORMANCE; BED REST; RELIABILITY;
ACTIVATION; MECHANISMS; STRENGTH; ADULTS
AB Spiering, BA, Lee, SMC, Mulavara, AP, Bentley, JR, Buxton, RE, Lawrence, EL, Sinka, J, Guilliams, ME, Ploutz-Snyder, LL, and Bloomberg, JJ. Test battery designed to quickly and safely assess diverse indices of neuromuscular function after unweighting. J Strength Cond Res 25(2): 545-555, 2011-Adequately describing the functional consequences of unweighting (e.g., bed rest, immobilization, spaceflight) requires assessing diverse indices of neuromuscular function (i.e., strength, power, endurance, central activation, force steadiness). Additionally, because unweighting increases the susceptibility of muscle to damage, testing should consider supplementary safety features. The purpose of this study was to develop a test battery for quickly assessing diverse indices of neuromuscular function. Commercially available exercise equipment was modified to include data acquisition hardware (e. g., force plates, position transducers) and auxiliary safety hardware (e. g., magnetic brakes). Ten healthy, ambulatory subjects (31 +/- 5 years, 173 +/- 11 cm, 73 +/- 14 kg) completed a battery of lower-and upper-body neuromuscular function tests on 3 occasions separated by at least 48 hours. The battery consisted of the following tests, in order: (1) knee extension central activation, (2) knee extension force steadiness, (3) leg press maximal strength, (4) leg press maximal power, (5) leg press power endurance, (6) bench press maximal strength, (7) bench press force steadiness, (8) bench press maximal power, and (9) bench press power endurance. Central activation, strength, rate of force development, maximal power, and power endurance (total work) demonstrated good-to-excellent measurement reliability (SEM = 3-14%; intraclass correlation coefficient [ICC] = 0.87-0.99). The SEM of the force steadiness variables was 20-35% (ICC = 0.20-0.60). After familiarization, the test battery required 49 +/- 6 minutes to complete. In conclusion, we successfully developed a test battery that could be used to quickly and reliably assess diverse indices of neuromuscular function. Because the test battery involves minimal eccentric muscle actions and impact forces, the potential for muscle injury has likely been reduced.
C1 [Spiering, Barry A.; Lee, Stuart M. C.; Bentley, Jason R.; Lawrence, Emily L.; Sinka, Joseph; Guilliams, Mark E.] Wyle Integrated Sci & Engn Grp, Houston, TX USA.
[Mulavara, Ajitkumar P.; Ploutz-Snyder, Lori L.] Univ Space Res Assoc, Houston, TX USA.
[Buxton, Roxanne E.] Univ Houston, Houston, TX USA.
[Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Spiering, BA (reprint author), Wyle Integrated Sci & Engn Grp, Houston, TX USA.
EM bspiering@fullerton.edu
FU National Aeronautics and Space Administration
FX We thank Brent Crowell, Kirk English, Jamie Guined, Mark Leach, Peggy
Lynn, and Leah Stroud for invaluable assistance during data collection;
Drs. Marcus Bamman, John McCarthy, and Gordon Warren, for constructive
input during the conception of this project; Dr. Mitzi Laughlin for
advice on the statistical approach; and an enthusiastic group of
volunteers for participation in the study. Present address for author
BAS is Department of Kinesiology, California State University,
Fullerton, CA 92831. This work was supported by the National Aeronautics
and Space Administration. The authors report no conflict of interest.
Results of the present study do not constitute endorsement by the
National Strength and Conditioning Association.
NR 18
TC 5
Z9 5
U1 0
U2 3
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 1064-8011
J9 J STRENGTH COND RES
JI J. Strength Cond. Res.
PD FEB
PY 2011
VL 25
IS 2
BP 545
EP 555
DI 10.1519/JSC.0b013e3181f56780
PG 11
WC Sport Sciences
SC Sport Sciences
GA 709SI
UT WOS:000286461300036
PM 21217531
ER
PT J
AU Schreck, CJ
Molinari, J
Mohr, KI
AF Schreck, Carl J., III
Molinari, John
Mohr, Karen I.
TI Attributing Tropical Cyclogenesis to Equatorial Waves in the Western
North Pacific
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; SYNOPTIC-SCALE DISTURBANCES; ROSSBY-GRAVITY
WAVES; CYCLONE ACTIVITY; PART I; NUMBER-FREQUENCY; EASTERLY WAVES;
RAINFALL; VARIABILITY; MODULATION
AB Tropical cyclogenesis is attributed to an equatorial wave when the filtered rainfall anomaly exceeds a threshold value at the genesis location. It is argued that 0 mm day(-1) (simply requiring a positive anomaly) is too small a threshold because unrelated noise can produce a positive anomaly. A threshold of 6 mm day(-1) is too large because two-thirds of storms would have no precursor disturbance. Between these extremes, consistent results are found for a range of thresholds from 2 to 4 mm day(-1). Roughly twice as many tropical cyclones are attributed to tropical depression (TD)-type disturbances as to equatorial
Rossby waves, mixed Rossby-gravity waves, or Kelvin waves. The influence of the Madden-Julian oscillation (MJO) is even smaller. The use of variables such as vorticity and vertical wind shear in other studies gives a larger contribution for the MJO. It is suggested that its direct influence on the rainfall in forming tropical cyclones is less than for other variables.
The impacts of tropical cyclone-related precipitation anomalies are also presented. Tropical cyclones can contribute more than 20% of the warm-season rainfall and 50% of its total variance. The influence of tropical cyclones on the equatorial wave spectrum is generally small. The exception occurs in shorter-wavelength westward-propagating waves, for which tropical cyclones represent up to 27% of the variance. Tropical cyclones also significantly contaminate wave-filtered rainfall anomalies in their immediate vicinity. To mitigate this effect, the tropical cyclone-related anomalies were removed before filtering in this study.
C1 [Molinari, John] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY USA.
[Mohr, Karen I.] NASA Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD USA.
[Schreck, Carl J., III] N Carolina State Univ, Cooperat Inst Climate & Satellites, Asheville, NC USA.
[Schreck, Carl J., III] Natl Climat Ctr, Asheville, NC USA.
RP Schreck, CJ (reprint author), Natl Climat Ctr, Cooperat Inst Climate & Satellites NC, 151 Patton Ave, Asheville, NC 28801 USA.
EM carl.schreck@noaa.gov
RI Schreck, Carl/B-8711-2011; Mohr, Karen/E-4331-2012
OI Schreck, Carl/0000-0001-9331-5754;
FU NSF [ATM0839991]; NASA Precipitation Measuring Mission [NNX07AD45G.]
FX This research has benefited greatly from conversations with Anantha
Aiyyer, Paul Roundy, and Adam Sobel. We also thank the three anonymous
reviewers whose insightful comments significantly improved this paper.
We obtained the TMPA data from the NASA Goddard Distributed Active
Archive Center (online at
http://disc.sci.gsfc.nasa.gov/data/datapool/TRMM/). We are grateful to
Dave Vollaro for his assistance in obtaining and interpolating this
data. This work was supported by NSF Grant ATM0839991 and NASA
Precipitation Measuring Mission Grant NNX07AD45G.
NR 46
TC 25
Z9 25
U1 1
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD FEB
PY 2011
VL 68
IS 2
BP 195
EP 209
DI 10.1175/2010JAS3396.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 731XQ
UT WOS:000288144300002
ER
PT J
AU Petitat, M
Marrocchi, Y
McKeegan, KD
Mostefaoui, S
Meibom, A
Zolensky, ME
Gounelle, M
AF Petitat, M.
Marrocchi, Y.
McKeegan, K. D.
Mostefaoui, S.
Meibom, A.
Zolensky, M. E.
Gounelle, M.
TI 53Mn-53Cr ages of Kaidun carbonates
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID EARLY SOLAR-SYSTEM; CHROMIUM ISOTOPE SYSTEMATICS; AQUEOUS ACTIVITY;
IRON-METEORITES; CI CHONDRITES; PARENT BODIES; CHRONOLOGY; MN-53; BODY
AB We report the 53Mn-53Cr systematics of three dolomite grains from two different CI1 clasts contained within the Kaidun meteorite breccia. Three internal isochrones result in initial 53Mn/55Mn ratios of (4.2 +/- 0.4) x 10-6, (4.6 +/- 1.3) x 10-6, and (5.2 +/- 1.1) x 10-6. These initial values are consistent with those measured for dolomite in the Orgueil CI1 chondrite (Hoppe et al. 2007; Petitat et al. 2009) but significantly lower than the initial ratio determined by Hutcheon et al. (1999) from a combination of different carbonate types within various lithologies of the Kaidun meteorite. We construct an accretion scenario for the Kaidun breccia by comparing the mineralogy and formation time scales of carbonates in the Kaidun CI1 lithologies to the analogous ones of the CI1 chondrite Orgueil. In Orgueil, dolomite precipitation precedes the formation of the first bruennerite grains by a few million years (Hoppe et al. 2007; Petitat et al. 2009). As the CI1 clasts in Kaidun lack breunnerite grains, and considering that aqueous alteration occurred prior to reaccretion of the various clasts onto the Kaidun parent body (e.g., MacPherson et al. 2009), we hypothesize that after rapid accretion and early aqueous alteration occurring within the first approximately 4 Myr after solar system formation, impact disruption of several asteroids and their reassembly into the Kaidun parent asteroid was complete within an additional approximately 2 Myr. This confirms that aqueous alteration, impact, and reaccretion of material in the asteroid belt were early processes that began contemporaneously with chondrule formation.
C1 [Petitat, M.; Marrocchi, Y.; Mostefaoui, S.; Meibom, A.; Gounelle, M.] CNRS, Lab Mineral & Cosmochim Museum, F-75005 Paris, France.
[Petitat, M.; Marrocchi, Y.; Mostefaoui, S.; Meibom, A.; Gounelle, M.] Museum Natl Hist Nat, UMR 7202, F-75005 Paris, France.
[McKeegan, K. D.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Zolensky, M. E.] KT NASA Johnson Space Ctr, Houston, TX 77058 USA.
RP Petitat, M (reprint author), CNRS, Lab Mineral & Cosmochim Museum, 57 Rue Cuvier, F-75005 Paris, France.
EM mpetitat@gmail.com
RI McKeegan, Kevin/A-4107-2008; UCLA, SIMS/A-1459-2011
OI McKeegan, Kevin/0000-0002-1827-729X;
FU Origin network
FX We wish to thank the associate editor G. Srinivasan and two anonymous
reviewers for their comments and discussions. This work is based on the
PhD thesis of Manuel Petitat at the Laboratoire de Mineralogie et de
Cosmochimie du Museum, Museum National d'Histoire Naturelle, Paris and
was supported by the Origin network (Marie Curie European Fellowship).
NR 33
TC 21
Z9 21
U1 0
U2 3
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD FEB
PY 2011
VL 46
IS 2
BP 275
EP 283
DI 10.1111/j.1945-5100.2010.01150.x
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 723DU
UT WOS:000287487300007
ER
PT J
AU Kolenberg, K
Bryson, S
Szabo, R
Kurtz, DW
Smolec, R
Nemec, JM
Guggenberger, E
Moskalik, P
Benko, JM
Chadid, M
Jeon, YB
Kiss, LL
Kopacki, G
Nuspl, J
Still, M
Christensen-Dalsgaard, J
Kjeldsen, H
Borucki, WJ
Caldwell, DA
Jenkins, JM
Koch, D
AF Kolenberg, K.
Bryson, S.
Szabo, R.
Kurtz, D. W.
Smolec, R.
Nemec, J. M.
Guggenberger, E.
Moskalik, P.
Benko, J. M.
Chadid, M.
Jeon, Y-B
Kiss, L. L.
Kopacki, G.
Nuspl, J.
Still, M.
Christensen-Dalsgaard, J.
Kjeldsen, H.
Borucki, W. J.
Caldwell, D. A.
Jenkins, J. M.
Koch, D.
TI Kepler photometry of the prototypical Blazhko star RR Lyr: an old friend
seen in a new light
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: photometric; stars: horizontal branch; stars: individual: RR
Lyr; stars: individual: KIC7198959; stars: oscillations; stars:
variables: RR Lyrae
ID STELLAR MODELS; MW LYR; SCIENCE; BEHAVIOR; CEPHEID
AB We present our analysis of the long-cadence Kepler data for the well-studied Blazhko star RR Lyr, gathered during the first two quarters of the satellite's observations and covering a total of 127 d. Besides being of great importance for our understanding of RR Lyrae stars in general, these RR Lyr data can be regarded as a case study for observations of bright stars with Kepler. Kepler can perform high-precision photometry on targets like RR Lyr, as the saturated flux is conserved to a very high degree. The Kepler data on RR Lyr are revolutionary in several respects. Even with long-cadence sampling (one measurement per 29.4 min), the unprecedented precision (< mmag) of the Kepler photometry allows the study of the star's extreme light-curve variations in detail. The multiplet structures at the main frequency and its harmonics, typical for Blazhko stars, are clearly detected up to the quintuplets. For the first time, photometric data of RR Lyr reveal the presence of half-integer frequencies, linked to a period-doubling effect. This phenomenon may be connected to the still unexplained Blazhko modulation. Moreover, with three observed Blazhko cycles at our disposal, we observe that there is no exact repetition in the light-curve changes from one modulation cycle to the next for RR Lyr. This may be due to additional periodicities in the star, or to transient or quasi-periodic changes.
C1 [Kolenberg, K.; Smolec, R.; Guggenberger, E.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Bryson, S.; Still, M.; Borucki, W. J.; Koch, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Szabo, R.; Benko, J. M.; Kiss, L. L.; Nuspl, J.] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England.
[Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada.
[Moskalik, P.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Chadid, M.] Univ Nice Sophia Antipolis, Observ Cote Azur, UMR 6525, F-06108 Nice 02, France.
[Jeon, Y-B] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Kiss, L. L.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia.
[Kopacki, G.] Uniwersytetu Wroclawskiego, Inst Astron, PL-51622 Wroclaw, Poland.
[Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Caldwell, D. A.; Jenkins, J. M.] SETI Inst, Mountain View, CA 94043 USA.
RP Kolenberg, K (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM katrien.kolenberg@univie.ac.at
RI Smolec, Radoslaw/F-1435-2013; Caldwell, Douglas/L-7911-2014;
OI Smolec, Radoslaw/0000-0001-7217-4884; Caldwell,
Douglas/0000-0003-1963-9616; Szabo, Robert/0000-0002-3258-1909; Benko,
Jozsef/0000-0003-3851-6603
FU NASA's Science Mission Directorate; Austrian Fonds zur Forderung der
wissenschaftlichen Forschung [T359-N16, P19962]; National Office for
Research and Technology through the Hungarian Space Office [URK09350];
Hungarian Academy of Sciences; OTKA [K76816, MB08C 81013]; FWF
FX The authors kindly thank the anonymous referee for constructive
comments. Funding for this Discovery mission is provided by NASA's
Science Mission Directorate. The authors gratefully acknowledge the
entire Kepler team, whose outstanding efforts have made these results
possible.; KK and EG acknowledge support from the Austrian Fonds zur
Forderung der wissenschaftlichen Forschung, project number T359-N16 and
P19962. RSz, JB and LLK are supported by the National Office for
Research and Technology through the Hungarian Space Office Grant No.
URK09350, the Lendulet program of the Hungarian Academy of Sciences, and
OTKA Grants K76816 and MB08C 81013. RS is supported by FWF project
AP2120521.
NR 52
TC 38
Z9 39
U1 0
U2 2
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 FEB
PY 2011
VL 411
IS 2
BP 878
EP 890
DI 10.1111/j.1365-2966.2010.17728.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716QO
UT WOS:000286988800011
ER
PT J
AU Ghisellini, G
Tagliaferri, G
Foschini, L
Ghirlanda, G
Tavecchio, F
Della Ceca, R
Haardt, F
Volonteri, M
Gehrels, N
AF Ghisellini, G.
Tagliaferri, G.
Foschini, L.
Ghirlanda, G.
Tavecchio, F.
Della Ceca, R.
Haardt, F.
Volonteri, M.
Gehrels, N.
TI High-redshift Fermi blazars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; BL Lacertae objects: general;
quasars: general; gamma-rays: general; X-rays: general
ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; 3C 454.3; BLACK-HOLES;
POWER; VARIABILITY; OUTBURST; CATALOG; JETS
AB With the release of the first-year Fermi catalogue, the number of blazars detected above 100 MeV lying at high redshift has been largely increased. There are 28 blazars at z > 2 in the 'clean' sample. All of them are flat spectrum radio quasars. We study and model their overall spectral energy distribution in order to find the physical parameters of the jet-emitting region, and for all of them, we estimate their black hole masses and accretion rates. We then compare the jet with the accretion disc properties, setting these sources in the broader context of all the other bright gamma-ray or hard X-ray blazars. We confirm that the jet power correlates with the accretion luminosity. We find that the high-energy emission peak shifts to smaller frequencies as the observed luminosity increases, according to the blazar sequence, making the hard X-ray band the most suitable for searching the most-luminous and distant blazars.
C1 [Ghisellini, G.; Tagliaferri, G.; Foschini, L.; Ghirlanda, G.; Tavecchio, F.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Della Ceca, R.] INAF Osservatorio Astron Brera, I-20100 Milan, Italy.
[Haardt, F.] Univ Insubria, Dipartimento Fis & Matemat, I-22100 Como, Italy.
[Haardt, F.] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan, Italy.
[Volonteri, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MA USA.
RP Ghisellini, G (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, Italy.
EM gabriele.ghisellini@brera.inaf.it
RI Gehrels, Neil/D-2971-2012; Foschini, Luigi/H-3833-2012;
OI Foschini, Luigi/0000-0001-8678-0324; Ghirlanda,
Giancarlo/0000-0001-5876-9259; Della Ceca, Roberto/0000-0001-7551-2252;
Ghisellini, Gabriele/0000-0002-0037-1974; Tagliaferri,
Gianpiero/0000-0003-0121-0723
FU ASI [I/088/06/0]; NASA
FX This work was partly financially supported by an ASI I/088/06/0) grant.
This research made use of the NASA/IPAC Extragalactic Data base (NED),
which is operated by the Jet Propulsion Laboratory, Caltech, under
contract with the NASA, and of the Swift public data made available by
the HEASARC archive system. We also thank the Swift team for quickly
approving and performing the requested ToO observations.
NR 37
TC 32
Z9 32
U1 1
U2 4
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 FEB
PY 2011
VL 411
IS 2
BP 901
EP 914
DI 10.1111/j.1365-2966.2010.17723.x
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716QO
UT WOS:000286988800013
ER
PT J
AU Catanzaro, G
Ripepi, V
Bernabei, S
Marconi, M
Balona, L
Kurtz, DW
Smalley, B
Borucki, WJ
Bruntt, H
Christensen-Dalsgaard, J
Grigahcene, A
Kjeldsen, H
Koch, DG
Monteiro, MJPFG
Suarez, JC
Szabo, R
Uytterhoeven, K
AF Catanzaro, G.
Ripepi, V.
Bernabei, S.
Marconi, M.
Balona, L.
Kurtz, D. W.
Smalley, B.
Borucki, W. J.
Bruntt, H.
Christensen-Dalsgaard, J.
Grigahcene, A.
Kjeldsen, H.
Koch, D. G.
Monteiro, M. J. P. F. G.
Suarez, J. C.
Szabo, R.
Uytterhoeven, K.
TI Atmospheric parameters and pulsational properties for a sample of delta
Sct, gamma Dor and hybrid Kepler targets star
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: early-type; stars: fundamental parameters; stars: oscillations
ID CLUSTER NGC 6811; SCUTI STARS; RADIAL-VELOCITIES; DORADUS STARS;
EFFECTIVE TEMPERATURE; STELLAR EVOLUTION; BETA PHOTOMETRY; HIPPARCOS;
PULSATORS; ISOCHRONES
AB We report spectroscopic observations for 19 delta Sct candidates observed by the Kepler satellite both in long and short cadence mode. For all these stars, by using spectral synthesis, we derive the effective temperature, the surface gravity and the projected rotational velocity. An equivalent spectral-type classification has been also performed for all stars in the sample. These determinations are fundamental for modelling the frequency spectra that will be extracted from the Kepler data for asteroseismic inference. For all the 19 stars, we also present periodograms obtained from Kepler data. We find that all stars show peaks in both low- (gamma Dor; g-mode) and high-frequency (delta Sct; p-mode) regions. Using the amplitudes and considering 5 cycles d-1 as a boundary frequency, we classified three stars as pure gamma Dor, four as gamma Dor-delta hybrid Sct, five as delta Sct-gamma Dor hybrid and six as pure delta Sct. The only exception is the star KIC 05296877, which we suggest could be a binary.
C1 [Catanzaro, G.] INAF, Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Ripepi, V.; Marconi, M.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Bernabei, S.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Balona, L.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England.
[Smalley, B.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Borucki, W. J.; Koch, D. G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bruntt, H.] Observ Paris, LESIA, F-92195 Meudon, France.
[Bruntt, H.; Christensen-Dalsgaard, J.; Kjeldsen, H.] Univ Aarhus, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Grigahcene, A.; Monteiro, M. J. P. F. G.] Univ Porto, Fac Ciencias, P-410762 Oporto, Portugal.
Univ Porto, Ctr Astrofis, P-410762 Oporto, Portugal.
[Suarez, J. C.] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Szabo, R.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary.
[Uytterhoeven, K.] Univ Paris Diderot, Lab AIM, CEA DSM, CNRS, F-91191 Gif Sur Yvette, France.
Univ Paris Diderot, CEA, IRFU,SAp, Ctr Saclay, F-91191 Gif Sur Yvette, France.
RP Catanzaro, G (reprint author), INAF, Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy.
EM gca@oact.inaf.it
RI Monteiro, Mario J.P.F.G./B-4715-2008; Suarez, Juan Carlos/C-1015-2009;
OI Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Suarez, Juan
Carlos/0000-0003-3649-8384; Catanzaro, Giovanni/0000-0003-4337-8612
FU Italian ESS project [ASI/INAF I/015/07/0, WP 03170]; European Helio- and
Asteroseismology Network (HELAS); European Commission; NASA's Science
Mission Directorate; National Science Foundation; National Office for
Reseach and Technology through the Hungarian Space Office [URK09350];
Hungarian Academy of Sciences; FCT-Portugal [PTDC/CTE-AST/098754/2008];
NASA
FX This work was supported by the Italian ESS project, contract ASI/INAF
I/015/07/0, WP 03170 and by the European Helio- and Asteroseismology
Network (HELAS), a major international collaboration funded by the
European Commission's Sixth Framework Programme.; Funding for the Kepler
mission is provided by NASA's Science Mission Directorate. We thank the
entire Kepler team for the development and operations of this
outstanding mission.; This research has made use of the SIMBAD data
base, operated at CDS, Strasbourg, France. This publication makes use of
data products from the 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 NASA and the
National Science Foundation. This work has made use of BaSTI web tools.
RS has been supported by the National Office for Reseach and Technology
through the Hungarian Space Office Grant No. URK09350 and the LENDULET
program of the Hungarian Academy of Sciences. MJPFGM and AG are
co-supported by project PTDC/CTE-AST/098754/2008 from FCT-Portugal.
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JI Mon. Not. Roy. Astron. Soc.
PD FEB
PY 2011
VL 411
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BP 1167
EP 1176
DI 10.1111/j.1365-2966.2010.17749.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 716QO
UT WOS:000286988800033
ER
PT J
AU Campana, S
Salvaterra, R
Tagliaferri, G
Kouveliotou, C
Grindlay, J
AF Campana, S.
Salvaterra, R.
Tagliaferri, G.
Kouveliotou, C.
Grindlay, J.
TI Probing the very high redshift Universe with gamma-ray bursts: prospects
for observations with future X-ray instruments
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gamma-ray burst: general; X-rays: general
ID DISTANT COSMIC EXPLOSION; CORE-COLLAPSE SUPERNOVAE; EARLY
STAR-FORMATION; POPULATION-III; COLUMN DENSITIES; ALPHA SYSTEMS;
BLACK-HOLES; HII REGION; 1ST STARS; AFTERGLOW
AB Gamma-ray bursts (GRBs) are the most violent explosions in the Universe. Long-duration GRBs are associated with the collapse of massive stars, rivalling their host galaxies in luminosity. The discovery of the most distant spectroscopically confirmed object in the Universe, GRB090423, opened a new window on the high-redshift Universe, making it possible to study the cosmic reionization epoch and the preceding dark ages, as well as the generation of the first stars (Population III) using GRBs. Obviously this enables a wealth of new studies using the near-infrared (NIR) characteristics of GRB afterglows. Here we explore a different path, focusing on the next generation of X-ray missions with large-area-focusing telescopes and fast-repointing capabilities. We found that X-ray data can complement NIR observations and for the brightest GRBs can provide an accurate and independent redshift determination. Metallicity studies can also be carried out profitably once the redshift is known. Finally we discuss observational signatures of GRBs arising from Population III stars in the X-ray band.
C1 [Campana, S.; Tagliaferri, G.] Osserv Astron Brera, INAF, I-23807 Merate, Lc, Italy.
[Salvaterra, R.] Univ Insubria, I-22100 Como, Italy.
[Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Grindlay, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Campana, S (reprint author), Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, Lc, Italy.
EM sergio.campana@brera.inaf.it
OI Campana, Sergio/0000-0001-6278-1576; Salvaterra,
Ruben/0000-0002-9393-8078; Tagliaferri, Gianpiero/0000-0003-0121-0723
FU ASI [I/011/07/0]
FX This work has been partially supported by ASI grant I/011/07/0. This
work made use of data supplied by the UK Swift Science Data Centre at
the University of Leicester.
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JI Mon. Not. Roy. Astron. Soc.
PD FEB
PY 2011
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DI 10.1111/j.1365-2966.2010.17540.x
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SC Astronomy & Astrophysics
GA 703TN
UT WOS:000286004300018
ER
PT J
AU Bloemen, S
Marsh, TR
Ostensen, RH
Charpinet, S
Fontaine, G
Degroote, P
Heber, U
Kawaler, SD
Aerts, C
Green, EM
Telting, J
Brassard, P
Gansicke, BT
Handler, G
Kurtz, DW
Silvotti, R
Van Grootel, V
Lindberg, JE
Pursimo, T
Wilson, PA
Gilliland, RL
Kjeldsen, H
Christensen-Dalsgaard, J
Borucki, WJ
Koch, D
Jenkins, JM
Klaus, TC
AF Bloemen, S.
Marsh, T. R.
Ostensen, R. H.
Charpinet, S.
Fontaine, G.
Degroote, P.
Heber, U.
Kawaler, S. D.
Aerts, C.
Green, E. M.
Telting, J.
Brassard, P.
Gaensicke, B. T.
Handler, G.
Kurtz, D. W.
Silvotti, R.
Van Grootel, V.
Lindberg, J. E.
Pursimo, T.
Wilson, P. A.
Gilliland, R. L.
Kjeldsen, H.
Christensen-Dalsgaard, J.
Borucki, W. J.
Koch, D.
Jenkins, J. M.
Klaus, T. C.
TI Kepler observations of the beaming binary KPD 1946+4340
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: close; binaries: eclipsing; stars: individual: KPD 1946+4340;
subdwarfs
ID SUBDWARF-B-STARS; LIGHT CURVES; WHITE-DWARF; INITIAL CHARACTERISTICS;
PALOMAR-GREEN; CADENCE DATA; SDB STARS; HOT; PHOTOMETRY; HYDROGEN
AB The Kepler Mission has acquired 33.5 d of continuous 1-min photometry of KPD 1946+4340, a short-period binary system that consists of a subdwarf B star (sdB) and a white dwarf. In the light curve, eclipses are clearly seen, with the deepest occurring when the compact white dwarf crosses the disc of the sdB (0.4 per cent) and the more shallow ones (0.1 per cent) when the sdB eclipses the white dwarf. As expected, the sdB is deformed by the gravitational field of the white dwarf, which produces an ellipsoidal modulation of the light curve. Spectacularly, a very strong Doppler beaming (also known as Doppler boosting) effect is also clearly evident at the 0.1 per cent level. This originates from the sdB's orbital velocity, which we measure to be 164.0 +/- 1.9 km s-1 from supporting spectroscopy. We present light-curve models that account for all these effects, as well as gravitational lensing, which decreases the apparent radius of the white dwarf by about 6 per cent, when it eclipses the sdB. We derive system parameters and uncertainties from the light curve using Markov chain Monte Carlo simulations. Adopting a theoretical white dwarf mass-radius relation, the mass of the subdwarf is found to be 0.47 +/- 0.03 M-circle dot and the mass of the white dwarf 0.59 +/- 0.02 M-circle dot. The effective temperature of the white dwarf is 15 900 +/- 300 K. With a spectroscopic effective temperature of T-eff = 34 730 +/- 250 K and a surface gravity of log g = 5.43 +/- 0.04, the subdwarf has most likely exhausted its core helium, and is in a shell He burning stage.
The detection of Doppler beaming in Kepler light curves potentially allows one to measure radial velocities without the need of spectroscopic data. For the first time, a photometrically observed Doppler beaming amplitude is compared to a spectroscopically established value. The sdB's radial velocity amplitude derived from the photometry (168 +/- 4 km s-1) is in perfect agreement with the spectroscopic value. After subtracting our best model for the orbital effects, we searched the residuals for stellar oscillations but did not find any significant pulsation frequencies.
C1 [Bloemen, S.; Ostensen, R. H.; Degroote, P.; Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Marsh, T. R.; Gaensicke, B. T.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Charpinet, S.; Van Grootel, V.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France.
Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Heber, U.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP Astron Inst, D-96049 Bamberg, Germany.
[Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Aerts, C.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Green, E. M.; Lindberg, J. E.; Pursimo, T.; Wilson, P. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Telting, J.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain.
[Handler, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England.
[Silvotti, R.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy.
[Lindberg, J. E.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Wilson, P. A.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kjeldsen, H.; Christensen-Dalsgaard, J.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Jenkins, J. M.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Klaus, T. C.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bloemen, S (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium.
EM steven.bloemen@ster.kuleuven.be
RI Gaensicke, Boris/A-9421-2012; Heber, Ulrich/G-3306-2013;
OI Gaensicke, Boris/0000-0002-2761-3005; Heber, Ulrich/0000-0001-7798-6769;
Silvotti, Roberto/0000-0002-1295-8174; Lindberg,
Johan/0000-0003-3811-4591; Charpinet, Stephane/0000-0002-6018-6180;
Kawaler, Steven/0000-0002-6536-6367
FU NASA; European Research Council under the European Community
[FP7/2007-2013, 227224 (PROSPERITY)]; Research Council of K.U. Leuven
[GOA/2008/04]; UK's Science and Technology Facilities Council (STFC)
[ST/F002599/1, PP/D005914/1]
FX We thank the referee Martin van Kerkwijk for his helpful suggestions.
The authors gratefully acknowledge everybody, who has contributed to
make the Kepler Mission possible. Funding for the Kepler Mission is
provided by NASA's Science Mission Directorate. Part of the data
presented here have been taken using ALFOSC, which is owned by the
Instituto de Astrofisica de Andalucia (IAA) and operated at the Nordic
Optical Telescope (Observatorio del Roque de los Muchachos, La Palma)
under agreement between IAA and the NBIfAFG of the Astronomical
Observatory of Copenhagen. This research also made use of data taken
with the Bok telescope (Steward Observatory, Kitt Peak). The research
leading to these results has received funding from the European Research
Council under the European Community's Seventh Framework Programme
(FP7/2007-2013)/ERC grant agreement no. 227224 (PROSPERITY), as well as
from the Research Council of K.U. Leuven grant agreement GOA/2008/04.
During this research, TRM was supported under grants from the UK's
Science and Technology Facilities Council (STFC, ST/F002599/1 and
PP/D005914/1).
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JI Mon. Not. Roy. Astron. Soc.
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SC Astronomy & Astrophysics
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UT WOS:000286004300032
ER
PT J
AU Romano, P
La Parola, V
Vercellone, S
Cusumano, G
Sidoli, L
Krimm, HA
Pagani, C
Esposito, P
Hoversten, EA
Kennea, JA
Page, KL
Burrows, DN
Gehrels, N
AF Romano, P.
La Parola, V.
Vercellone, S.
Cusumano, G.
Sidoli, L.
Krimm, H. A.
Pagani, C.
Esposito, P.
Hoversten, E. A.
Kennea, J. A.
Page, K. L.
Burrows, D. N.
Gehrels, N.
TI Two years of monitoring supergiant fast X-ray transients with Swift
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE X-rays: binaries; X-rays: individual: IGR J16479-4514; X-rays:
individual: XTE J1739-302; X-rays: individual: IGR J17544-2619
ID IGR J16479-4514; XTE J1739-302; INTEGRAL OBSERVATIONS; ORBITAL PERIOD;
NEUTRON-STAR; OUTBURST; TELESCOPE; J11215-5952; J17544-2619; DISCOVERY
AB We present results based on 2 yr of intense Swift monitoring of three supergiant fast X-ray transients (SFXTs), IGR J16479-4514, XTE J1739-302 and IGR J17544-2619, which we started in 2007 October. Our out-of-outburst intensity-based X-ray (0.3-10 keV) spectroscopy yields absorbed power laws characterized by hard photon indices (Gamma similar to 1 -2). The broad-band (0.3-150 keV) spectra of these sources, obtained while they were undergoing new outbursts observed during the second year of monitoring, can be fitted well with models typically used to describe the X-ray emission from accreting neutron stars in high-mass X-ray binaries. We obtain an assessment of how long each source spends in each state using a systematic monitoring with a sensitive instrument. By considering our monitoring as a casual sampling of the X-ray light curves, we can infer that the time these sources spend in bright outbursts is between 3 and 5 per cent of the total. The most probable X-ray flux for these sources is similar to(1 -2) x 10-11 erg cm-2 s-1 (2-10 keV, unabsorbed), corresponding to luminosities of the order of a few 1033 to a few 1034 erg s-1 (two orders of magnitude lower than the bright outbursts). In particular, the duty-cycle of inactivity is similar to 19, 39 and 55 per cent (similar to 5 per cent uncertainty) for IGR J16479-4514, XTE J1739-302 and IGR J17544-2619, respectively. We present a complete list of BAT onboard detections, which further confirm the continued activity of these sources. This demonstrates that true quiescence is a rare state and that these transients accrete matter throughout their life at different rates. Variability in the X-ray flux is observed at all time-scales and intensity ranges we can probe. Superimposed on the day-to-day variability is intraday flaring, which involves flux variations up to one order of magnitude that can occur down to time-scales as short as similar to 1 ks, and which can be naturally explained by the accretion of single clumps composing the donor wind with masses M-cl similar to (0.3 -2) x 1019 g. Thanks to the Swift observations, the general picture we obtain is that, despite individual differences, common X-ray characteristics of this class are now well defined, such as outburst lengths well in excess of hours, with a multiple peaked structure, and a high dynamic range (including bright outbursts), up to approximately four orders of magnitude.
C1 [Romano, P.; La Parola, V.; Vercellone, S.; Cusumano, G.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy.
[Sidoli, L.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy.
[Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krimm, H. A.; Gehrels, N.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Pagani, C.; Hoversten, E. A.; Kennea, J. A.; Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Pagani, C.; Page, K. L.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Esposito, P.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, Italy.
[Esposito, P.] Ist Nazl Fis Nucl, Sez Pavia, I-27100 Pavia, Italy.
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 Sidoli, Lara/0000-0001-9705-2883; Cusumano,
Giancarlo/0000-0002-8151-1990; Vercellone, Stefano/0000-0003-1163-1396;
La Parola, Valentina/0000-0002-8087-6488; Esposito,
Paolo/0000-0003-4849-5092
FU NASA at PSU [NAS5-00136]; Swift project
FX PR dedicates this effort to her grandmother G. Ghedin; she could not
follow her aspiration, yet worked hard so that others could. We
acknowledge the input from our colleagues along the way during this
large project, in particular A. Beardmore, M. M. Chester, L. Ducci, C.
Guidorzi, T. Mineo and M. Perri. We thank the Swift team duty scientists
and science planners. We also thank the remainder of the Swift XRT, BAT
and UVOT teams, S. Barthelmy and J.A. Nousek in particular, for their
invaluable help and support with the planning and execution of the
observing strategy. We also thank the anonymous referee for comments
that helped improve this paper. This work was supported at PSU by NASA
contract NAS5-00136. HAK was supported by the Swift project.
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SC Astronomy & Astrophysics
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PT J
AU Abadie, J
Abbott, BP
Abbott, R
Adhikari, R
Ajith, P
Allen, B
Allen, G
Ceron, EA
Amin, RS
Anderson, SB
Anderson, WG
Arain, MA
Araya, M
Aso, Y
Aston, S
Aufmuth, P
Aulbert, C
Babak, S
Baker, P
Ballmer, S
Barker, D
Barr, B
Barriga, P
Barsotti, L
Barton, MA
Bartos, I
Bassiri, R
Bastarrika, M
Behnke, B
Benacquista, M
Bennett, MF
Betzwieser, J
Beyersdorf, PT
Bilenko, IA
Billingsley, G
Biswas, R
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Bland, B
Bock, O
Bodiya, TP
Bondarescu, R
Bork, R
Born, M
Bose, S
Brady, PR
Braginsky, VB
Brau, JE
Breyer, J
Bridges, DO
Brinkmann, M
Britzger, M
Brooks, AF
Brown, DA
Bullington, A
Buonanno, A
Burmeister, O
Byer, RL
Cadonati, L
Cain, J
Camp, JB
Cannizzo, J
Cannon, KC
Cao, J
Capano, C
Cardenas, L
Caudill, S
Cavaglia, M
Cepeda, C
Chalermsongsak, T
Chalkley, E
Charlton, P
Chatterji, S
Chelkowski, S
Chen, Y
Christensen, N
Chua, SSY
Chung, CTY
Clark, D
Clark, J
Clayton, JH
Conte, R
Cook, D
Corbitt, TRC
Cornish, N
Coward, D
Coyne, DC
Creighton, JDE
Creighton, TD
Cruise, AM
Culter, RM
Cumming, A
Cunningham, L
Dahl, K
Danilishin, SL
Danzmann, K
Daudert, B
Davies, G
Daw, EJ
Dayanga, T
Debra, D
Degallaix, J
Dergachev, V
DeSalvo, R
Dhurandhar, S
Diaz, M
Donovan, F
Dooley, KL
Doomes, EE
Drever, RWP
Driggers, J
Dueck, J
Duke, I
Dumas, JC
Edgar, M
Edwards, M
Effler, A
Ehrens, P
Etzel, T
Evans, M
Evans, T
Fairhurst, S
Faltas, Y
Fan, Y
Fazi, D
Fehrmann, H
Finn, LS
Flasch, K
Foley, S
Forrest, C
Fotopoulos, N
Frede, M
Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Friedrich, D
Fritschel, P
Frolov, VV
Fulda, P
Fyffe, M
Garofoli, JA
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Goetz, E
Goggin, LM
Gonzalez, G
Gossler, S
Grant, A
Gras, S
Gray, C
Greenhalgh, RJS
Gretarsson, AM
Grosso, R
Grote, H
Grunewald, S
Gustafson, EK
Gustafson, R
Hage, B
Hallam, JM
Hammer, D
Hammond, GD
Hanna, C
Hanson, J
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Haughian, K
Hayama, K
Hayler, T
Heefner, J
Heng, IS
Heptonstall, A
Hewitson, M
Hild, S
Hirose, E
Hoak, D
Hodge, KA
Holt, K
Hosken, DJ
Hough, J
Howell, E
Hoyland, D
Hughey, B
Husa, S
Huttner, SH
Ingram, DR
Isogai, T
Ivanov, A
Johnson, WW
Jones, DI
Jones, G
Jones, R
Ju, L
Kalmus, P
Kalogera, V
Kandhasamy, S
Kanner, J
Katsavounidis, E
Kawabe, K
Kawamura, S
Kawazoe, F
Kells, W
Keppel, DG
Khalaidovski, A
Khalili, FY
Khan, R
Khazanov, E
Kim, H
King, PJ
Kissel, JS
Klimenko, S
Kokeyama, K
Kondrashov, V
Kopparapu, R
Koranda, S
Kozak, D
Kringel, V
Krishnan, B
Kuehn, G
Kullman, J
Kumar, R
Kwee, P
Lam, PK
Landry, M
Lang, M
Lantz, B
Lastzka, N
Lazzarini, A
Leaci, P
Lei, M
Leindecker, N
Leonor, I
Lin, H
Lindquist, PE
Littenberg, TB
Lockerbie, NA
Lodhia, D
Lormand, M
Lu, P
Lubinski, M
Lucianetti, A
Luck, H
Lundgren, A
Machenschalk, B
MacInnis, M
Mageswaran, M
Mailand, K
Mak, C
Mandel, I
Mandic, V
Marka, S
Marka, Z
Markosyan, A
Markowitz, J
Maros, E
Martin, IW
Martin, RM
Marx, JN
Mason, K
Matichard, F
Matone, L
Matzner, RA
Mavalvala, N
McCarthy, R
McClelland, DE
McGuire, SC
McIntyre, G
McKechan, DJA
Mehmet, M
Melatos, A
Melissinos, AC
Mendell, G
Menendez, DF
Mercer, RA
Merrill, L
Meshkov, S
Messenger, C
Meyer, MS
Miao, H
Miller, J
Mino, Y
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Miyakawa, O
Moe, B
Mohanty, SD
Mohapatra, SRP
Moreno, G
Mors, K
Mossavi, K
MowLowry, C
Mueller, G
Muller-Ebhardt, H
Mukherjee, S
Mullavey, A
Munch, J
Murray, PG
Nash, T
Nawrodt, R
Nelson, J
Newton, G
Nishida, E
Nishizawa, A
O'Dell, J
O'Reilly, B
O'Shaughnessy, R
Ochsner, E
Ogin, GH
Oldenburg, R
Ottaway, DJ
Ottens, RS
Overmier, H
Owen, BJ
Page, A
Pan, Y
Pankow, C
Papa, MA
Patel, P
Pathak, D
Pedraza, M
Pekowsky, L
Penn, S
Peralta, C
Perreca, A
Pickenpack, M
Pinto, IM
Pitkin, M
Pletsch, HJ
Plissi, MV
Postiglione, F
Principe, M
Prix, R
Prokhorov, L
Puncken, O
Quetschke, V
Raab, FJ
Rabeling, DS
Radkins, H
Raffai, P
Raics, Z
Rakhmanov, M
Raymond, V
Reed, CM
Reed, T
Rehbein, H
Reid, S
Reitze, DH
Riesen, R
Riles, K
Roberts, P
Robertson, NA
Robinson, C
Robinson, EL
Roddy, S
Rover, C
Rollins, J
Romano, JD
Romie, JH
Rowan, S
Rudiger, A
Ryan, K
Sakata, S
Sammut, L
de la Jordana, LS
Sandberg, V
Sannibale, V
Santamaria, L
Santostasi, G
Saraf, S
Sarin, P
Sathyaprakash, BS
Sato, S
Satterthwaite, M
Saulson, PR
Savage, R
Schilling, R
Schnabel, R
Schofield, R
Schulz, B
Schutz, BF
Schwinberg, P
Scott, J
Scott, SM
Searle, AC
Seifert, F
Sellers, D
Sengupta, AS
Sergeev, A
Shapiro, B
Shawhan, P
Shoemaker, DH
Sibley, A
Siemens, X
Sigg, D
Sintes, AM
Skelton, G
Slagmolen, BJJ
Slutsky, J
Smith, JR
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Bondarescu, R.
Bork, R.
Born, M.
Bose, S.
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Braginsky, V. B.
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Brinkmann, M.
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Doomes, E. E.
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Driggers, J.
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Dumas, J-C
Edgar, M.
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Mukherjee, S.
Mullavey, A.
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Nash, T.
Nawrodt, R.
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Nishizawa, A.
O'Dell, J.
O'Reilly, B.
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Pickenpack, M.
Pinto, I. M.
Pitkin, M.
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Postiglione, F.
Principe, M.
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Stuver, A. L.
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Sung, M.
Susmithan, S.
Sutton, P. J.
Szokoly, G. P.
Talukder, D.
Tanner, D. B.
Tarabrin, S. P.
Taylor, J. R.
Taylor, R.
Thorne, K. A.
Thorne, K. S.
Thuering, A.
Titsler, C.
Tokmakov, K. V.
Torres, C.
Torrie, C. I.
Traylor, G.
Trias, M.
Turner, L.
Ugolini, D.
Urbanek, K.
Vahlbruch, H.
Vallisneri, M.
Van Den Broeck, C.
Van der Sluys, M. V.
van Veggel, A. A.
Vass, S.
Vaulin, R.
Vecchio, A.
Veitch, J.
Veitch, P. J.
Veltkamp, C.
Villar, A.
Vorvick, C.
Vyachanin, S. P.
Waldman, S. J.
Wallace, L.
Wanner, A.
Ward, R. L.
Wei, P.
Weinert, M.
Weinstein, A. J.
Weiss, R.
Wen, L.
Wen, S.
Wessels, P.
West, M.
Westphal, T.
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.
Winkelmann, L.
Winkler, W.
Wipf, C. C.
Wiseman, A. G.
Woan, G.
Wooley, R.
Worden, J.
Yakushin, I.
Yamamoto, H.
Yamamoto, K.
Yeaton-Massey, D.
Yoshida, S.
Zanolin, M.
Zhang, L.
Zhang, Z.
Zhao, C.
Zotov, N.
Zucker, M. E.
Zweizig, J.
Buchner, S.
CA LIGO Sci Collaboration
TI Search for gravitational waves associated with the August 2006 timing
glitch of the Vela pulsar
SO PHYSICAL REVIEW D
LA English
DT Article
ID RELATIVISTIC STELLAR MODELS; NON-RADIAL PULSATION; NONRADIAL PULSATION;
SCIENCE RUN; NEUTRON STARQUAKES; ANALYTIC ANALYSIS; WIND TORI; DYNAMICS;
STARS; 5TH
AB The physical mechanisms responsible for pulsar timing glitches are thought to excite quasinormal mode oscillations in their parent neutron star that couple to gravitational-wave emission. In August 2006, a timing glitch was observed in the radio emission of PSR B0833-45, the Vela pulsar. At the time of the glitch, the two colocated Hanford gravitational-wave detectors of the Laser Interferometer Gravitational-wave observatory (LIGO) were operational and taking data as part of the fifth LIGO science run (S5). We present the first direct search for the gravitational-wave emission associated with oscillations of the fundamental quadrupole mode excited by a pulsar timing glitch. No gravitational-wave detection candidate was found. We place Bayesian 90% confidence upper limits of 6.3 x 10(-21) to 1.4 x 10(-20) on the peak intrinsic strain amplitude of gravitational-wave ring-down signals, depending on which spherical harmonic mode is excited. The corresponding range of energy upper limits is 5.0 x 10(44) to 1.3 x 10(45) erg.
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[Allen, B.; Aulbert, C.; Bock, O.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Burmeister, O.; Dahl, K.; Danzmann, K.; Degallaix, J.; Dueck, J.; Fehrmann, H.; Frede, M.; Friedrich, D.; Giampanis, S.; Gossler, S.; Grote, H.; Hayama, K.; Hewitson, M.; Kawazoe, F.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Kullman, J.; Lastzka, N.; Leaci, P.; Lueck, H.; Machenschalk, B.; Mehmet, M.; Messenger, C.; Mors, K.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Prix, R.; Puncken, O.; Rehbein, H.; Roever, C.; Ruediger, A.; Schilling, R.; Schnabel, R.; Schulz, B.; Seifert, F.; Taylor, J. R.; Veltkamp, C.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Willke, B.; Winkelmann, L.; Winkler, W.; Yamamoto, K.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Roberts, P.; Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
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[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Husa, S.; Sancho de la Jordana, L.; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma De Mallorca, Spain.
[Hosken, D. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Aston, S.; Chelkowski, S.; Cruise, A. M.; Culter, R. M.; Freise, A.; Fulda, P.; Hallam, J. M.; Hild, S.; Hoyland, D.; Lodhia, D.; Page, A.; Perreca, A.; Vecchio, A.; Veitch, J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Arain, M. A.; Dooley, K. L.; Faltas, Y.; Klimenko, S.; Lin, H.; Lucianetti, A.; Martin, R. M.; Mitselmakher, G.; Mueller, G.; Ottens, R. S.; Pankow, C.; Reitze, D. H.; Tanner, D. B.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA.
[Barr, B.; Bassiri, R.; Bastarrika, M.; Chalkley, E.; Cumming, A.; Cunningham, L.; Edgar, M.; Grant, A.; Hammond, G. D.; Haughian, K.; Heng, I. S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Martin, I. W.; Miller, J.; Murray, P. G.; Nawrodt, R.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Scott, J.; Sorazu, B.; Speirits, F.; Strain, K. A.; Tokmakov, K. V.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland.
[Buonanno, A.; Kanner, J.; Ochsner, E.; Pan, Y.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA.
[Cadonati, L.; Mohapatra, S. R. P.] Univ Massachusetts, Amherst, MA 01003 USA.
[Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Harms, J.; Kandhasamy, S.; Mandic, V.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Brau, J. E.; Frey, R.; Harstad, E. D.; Leonor, I.; Schofield, R.] Univ Oregon, Eugene, OR 97403 USA.
[Forrest, C.; Melissinos, A. C.] Univ Rochester, Rochester, NY 14627 USA.
[Conte, R.] Univ Salerno, I-84084 Salerno, Italy.
[Pinto, I. M.; Postiglione, F.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland.
[Allen, B.; Ceron, E. Amador; Anderson, W. G.; Biswas, R.; Brady, P. R.; Clayton, J. H.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Goggin, L. M.; Hammer, D.; Koranda, S.; Mercer, R. A.; Moe, B.; Oldenburg, R.; Papa, M. A.; Siemens, X.; Skelton, G.; Vaulin, R.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Bose, S.; Dayanga, T.; Ghosh, S.; Steplewski, S.; Talukder, D.] Washington State Univ, Pullman, WA 99164 USA.
[Buchner, S.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
[Buchner, S.] Univ Witwatersrand, Sch Phys, ZA-2040 Wits, South Africa.
[Barriga, P.; Blair, D.; Coward, D.; Dumas, J-C; Fan, Y.; Gras, S.; Howell, E.; Ju, L.; Merrill, L.; Miao, H.; Susmithan, S.; Wen, L.; Zhang, Z.; Zhao, C.] Univ Western Australia, Crawley 6009, Australia.
RP Abadie, J (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
RI Sergeev, Alexander/F-3027-2017; Ward, Robert/I-8032-2014; Howell,
Eric/H-5072-2014; Lam, Ping Koy/A-5276-2008; Danilishin,
Stefan/K-7262-2012; Vecchio, Alberto/F-8310-2015; Mow-Lowry,
Conor/F-8843-2015; Khan, Rubab/F-9455-2015; Finn, Lee
Samuel/A-3452-2009; 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; Bartos, Imre/A-2592-2017;
Frey, Raymond/E-2830-2016; Strigin, Sergey/I-8337-2012; 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; Zhao,
Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Pitkin, Matthew/I-3802-2013;
Vyatchanin, Sergey/J-2238-2012; Miao, Haixing/O-1300-2013; Khazanov,
Efim/B-6643-2014; Lucianetti, Antonio/G-7383-2014; Hammond,
Giles/B-7861-2009; Khalili, Farit/D-8113-2012; Hild, Stefan/A-3864-2010;
Santamaria, Lucia/A-7269-2012; Prokhorov, Leonid/I-2953-2012;
McClelland, David/E-6765-2010; Strain, Kenneth/D-5236-2011; Raab,
Frederick/E-2222-2011; Martin, Iain/A-2445-2010; Lueck,
Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Freise,
Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Hammond,
Giles/A-8168-2012
OI Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946;
Whiting, Bernard F/0000-0002-8501-8669; Principe,
Maria/0000-0002-6327-0628; Kanner, Jonah/0000-0001-8115-0577;
Santamaria, Lucia/0000-0002-5986-0449; Hallam, Jonathan
Mark/0000-0002-7087-0461; Nishizawa, Atsushi/0000-0003-3562-0990;
Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735;
Zweizig, John/0000-0002-1521-3397; O'Shaughnessy,
Richard/0000-0001-5832-8517; Pathak, Devanka/0000-0002-1768-8353; Stein,
Leo/0000-0001-7559-9597; Ward, Robert/0000-0001-5503-5241; Whelan,
John/0000-0001-5710-6576; Howell, Eric/0000-0001-7891-2817; Fairhurst,
Stephen/0000-0001-8480-1961; Matichard, Fabrice/0000-0001-8982-8418;
Husa, Sascha/0000-0002-0445-1971; Pinto, Innocenzo
M./0000-0002-2679-4457; Lam, Ping Koy/0000-0002-4421-601X; Danilishin,
Stefan/0000-0001-7758-7493; Vecchio, Alberto/0000-0002-6254-1617; Khan,
Rubab/0000-0001-5100-5168; Finn, Lee Samuel/0000-0002-3937-0688;
Postiglione, Fabio/0000-0003-0628-3796; Sigg,
Daniel/0000-0003-4606-6526; Frey, Raymond/0000-0003-0341-2636; Allen,
Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Pitkin,
Matthew/0000-0003-4548-526X; Miao, Haixing/0000-0003-4101-9958;
McClelland, David/0000-0001-6210-5842; Strain,
Kenneth/0000-0002-2066-5355; Lueck, Harald/0000-0001-9350-4846;
FU 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
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 paper has been
assigned LIGO Document No. P1000030-v11.
NR 48
TC 31
Z9 31
U1 2
U2 10
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 FEB 1
PY 2011
VL 83
IS 4
AR 042001
DI 10.1103/PhysRevD.83.042001
PG 13
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 716OS
UT WOS:000286983900001
ER
PT J
AU Etiope, G
Oehler, DZ
Allen, CC
AF Etiope, G.
Oehler, D. Z.
Allen, C. C.
TI Methane emissions from Earth's degassing: Implications for Mars
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Methane; Earth's degassing; Seepage
ID ATMOSPHERIC METHANE; MARTIAN ATMOSPHERE; GAS SEEPS; GEOLOGIC EMISSIONS;
SEDIMENTARY BASINS; MUD VOLCANOS; ORIGIN; LIFE; SERPENTINIZATION;
DIVERSITY
AB The presence of methane on Mars is of great interest, since one possibility for its origin is that it derives from living microbes. However, CH4 in the martian atmosphere also could be attributable to geologic emissions released through pathways similar to those occurring on Earth. Using recent data on methane degassing of the Earth, we have estimated the relative terrestrial contributions of fossil geologic methane vs. modern methane from living methanogens, and have examined the significance that various geologic sources might have for Mars.
Geologic degassing includes microbial methane (produced by ancient methanogens), thermogenic methane (from maturation of sedimentary organic matter), and subordinately geothermal and volcanic methane (mainly produced abiogenically). Our analysis suggests that similar to 80% of the "natural" emission to the terrestrial atmosphere originates from modern microbial activity and similar to 20% originates from geologic degassing, for a total CH4 emission of similar to 28.0 x 10(7) tonnes year(-1).
Estimates of methane emission on Mars range from 12.6 x 10(1) to 57.0 x 10(4) tonnes year(-1) and are 3-6 orders of magnitude lower than that estimated for Earth. Nevertheless, the recently detected martian, Northern-Summer-2003 CH4 plume could be compared with methane expulsion from large mud volcanoes or from the integrated emission of a few hundred gas seeps, such as many of those located in Europe, USA, Mid-East or Asia. Methane could also be released by diffuse microseepage from martian soil, even if macro-seeps or mud volcanoes were lacking or inactive. We calculated that a weak microseepage spread over a few tens of km(2), as frequently occurs on Earth, may be sufficient to generate the lower estimate of methane emission in the martian atmosphere.
At least 65% of Earth's degassing is provided by kerogen thermogenesis. A similar process may exist on Mars, where kerogen might include abiogenic organics (delivered by meteorites and comets) and remnants of possible, past martian life. The remainder of terrestrial degassed methane is attributed to fossil microbial gas (similar to 25%) and geothermal-volcanic emissions (similar to 10%). Global abiogenic emissions from serpentinization are negligible on Earth, but, on Mars, individual seeps from serpentinization could be significant. Gas discharge from clathrate-permafrost destabilization should also be considered.
Finally, we have shown examples of potential degassing pathways on Mars, including mud volcano-like structures, fault and fracture systems, and major volcanic edifices. All these types of structures could provide avenues for extensive gas expulsion, as on Earth. Future investigations of martian methane should be focused on such potential pathways. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Etiope, G.] Ist Nazl Geofis & Vulcanol, Sez Roma 2, I-00143 Rome, Italy.
[Oehler, D. Z.; Allen, C. C.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
RP Etiope, G (reprint author), Ist Nazl Geofis & Vulcanol, Sez Roma 2, Via V Murata 605, I-00143 Rome, Italy.
EM etiope@ingv.it
RI Etiope, Giuseppe/H-3343-2011
OI Etiope, Giuseppe/0000-0001-8614-4221
FU NASA Astromaterials Research and Exploration Science (ARES) Directorate
at Johnson Space Center; ARES; NASA
FX This study was developed in the framework of the INGV Specific Objective
"Degassing and petroliferous gases". D.Z. Oehler and C.C. Allen are
supported by the NASA Astromaterials Research and Exploration Science
(ARES) Directorate at Johnson Space Center and an ARES Mission Enabling
Grant for Planetary Mapping. D.Z. Oehler is additionally supported by a
NASA Grant from the Exobiology and Evolutionary Biology Program.
NR 108
TC 10
Z9 10
U1 4
U2 31
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 FEB
PY 2011
VL 59
IS 2-3
SI SI
BP 182
EP 195
DI 10.1016/j.pss.2010.06.003
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 724AP
UT WOS:000287548800006
ER
PT J
AU Coustenis, A
Atkinson, D
Balint, T
Beauchamp, P
Atreya, S
Lebreton, JP
Lunine, J
Matson, D
Erd, C
Reh, K
Spilker, TR
Elliott, J
Hall, J
Strange, N
AF Coustenis, A.
Atkinson, D.
Balint, T.
Beauchamp, P.
Atreya, S.
Lebreton, J-P
Lunine, J.
Matson, D.
Erd, C.
Reh, K.
Spilker, T. R.
Elliott, J.
Hall, J.
Strange, N.
TI Atmospheric planetary probes and balloons in the solar system
SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART G-JOURNAL OF
AEROSPACE ENGINEERING
LA English
DT Article
DE probes; balloons; robotic exploration; Venus; Titan; giant planets
ID GIANT PLANETS; VENUS; EVOLUTION; JUPITER; EXPLORATION; CHEMISTRY;
CLIMATE; SATURN; ORIGIN
AB A primary motivation for in situ probe and balloon missions in the solar system is to progressively constrain models of its origin and evolution. Specifically, understanding the origin and evolution of multiple planetary atmospheres within our solar system would provide a basis for comparative studies that lead to a better understanding of the origin and evolution of our own solar system as well as extra-solar planetary systems. Hereafter, the authors discuss in situ exploration science drivers, mission architectures, and technologies associated with probes at Venus, the giant planets and Titan.
C1 [Coustenis, A.] Observ Paris, LESIA, F-92195 Meudon, France.
[Atkinson, D.] Univ Idaho, Dept Elect & Comp Engn, Moscow, ID 83843 USA.
[Balint, T.; Beauchamp, P.; Matson, D.; Reh, K.; Spilker, T. R.; Elliott, J.; Hall, J.; Strange, N.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Atreya, S.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Lebreton, J-P; Erd, C.] ESA ESTEC, Noordwijk, Netherlands.
[Lunine, J.] Univ Rome, Dipartimento Fis, Rome, Italy.
RP Coustenis, A (reprint author), Observ Paris, LESIA, 5 Pl Jules Janssen, F-92195 Meudon, France.
EM Athena.coustenis@obspm.fr
NR 45
TC 0
Z9 0
U1 1
U2 3
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0954-4100
J9 P I MECH ENG G-J AER
JI Proc. Inst. Mech. Eng. Part G-J. Aerosp. Eng.
PD FEB
PY 2011
VL 225
IS G2
SI SI
BP 154
EP 180
DI 10.1177/2041302510393099
PG 27
WC Engineering, Aerospace; Engineering, Mechanical
SC Engineering
GA 729WZ
UT WOS:000287986200004
ER
PT J
AU van Dishoeck, EF
Kristensen, LE
Benz, AO
Bergin, EA
Caselli, P
Cernicharo, J
Herpin, F
Hogerheijde, MR
Johnstone, D
Liseau, R
Nisini, B
Shipman, R
Tafalla, M
van der Tak, F
Wyrowski, F
Aikawa, Y
Bachiller, R
Baudry, A
Benedettini, M
Bjerkeli, P
Blake, GA
Bontemps, S
Braine, J
Brinch, C
Bruderer, S
Chavarria, L
Codella, C
Daniel, F
de Graauw, T
Deul, E
di Giorgio, AM
Dominik, C
Doty, SD
Dubernet, ML
Encrenaz, P
Feuchtgruber, H
Fich, M
Frieswijk, W
Fuente, A
Giannini, T
Goicoechea, JR
Helmich, FP
Herczeg, GJ
Jacq, T
Jorgensen, JK
Karska, A
Kaufman, MJ
Keto, E
Larsson, B
Lefloch, B
Lis, D
Marseille, M
McCoey, C
Melnick, G
Neufeld, D
Olberg, M
Pagani, L
Panic, O
Parise, B
Pearson, JC
Plume, R
Risacher, C
Salter, D
Santiago-Garcia, J
Saraceno, P
Stauber, P
van Kempen, TA
Visser, R
Viti, S
Walmsley, M
Wampfler, SF
Yildiz, UA
AF van Dishoeck, E. F.
Kristensen, L. E.
Benz, A. O.
Bergin, E. A.
Caselli, P.
Cernicharo, J.
Herpin, F.
Hogerheijde, M. R.
Johnstone, D.
Liseau, R.
Nisini, B.
Shipman, R.
Tafalla, M.
van der Tak, F.
Wyrowski, F.
Aikawa, Y.
Bachiller, R.
Baudry, A.
Benedettini, M.
Bjerkeli, P.
Blake, G. A.
Bontemps, S.
Braine, J.
Brinch, C.
Bruderer, S.
Chavarria, L.
Codella, C.
Daniel, F.
de Graauw, Th.
Deul, E.
di Giorgio, A. M.
Dominik, C.
Doty, S. D.
Dubernet, M. L.
Encrenaz, P.
Feuchtgruber, H.
Fich, M.
Frieswijk, W.
Fuente, A.
Giannini, T.
Goicoechea, J. R.
Helmich, F. P.
Herczeg, G. J.
Jacq, T.
Jorgensen, J. K.
Karska, A.
Kaufman, M. J.
Keto, E.
Larsson, B.
Lefloch, B.
Lis, D.
Marseille, M.
McCoey, C.
Melnick, G.
Neufeld, D.
Olberg, M.
Pagani, L.
Panic, O.
Parise, B.
Pearson, J. C.
Plume, R.
Risacher, C.
Salter, D.
Santiago-Garcia, J.
Saraceno, P.
Staeuber, P.
van Kempen, T. A.
Visser, R.
Viti, S.
Walmsley, M.
Wampfler, S. F.
Yildiz, U. A.
TI Water in Star-forming Regions with the Herschel Space Observatory
(WISH). I. Overview of Key Program and First Results
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; PROTOSTELLAR SHOCK L1157-B1;
FAR-INFRARED OBSERVATIONS; WAVE-ASTRONOMY-SATELLITE; VELA MOLECULAR
CLOUDS; CHESS SPECTRAL SURVEY; NGC-7129 FIRS 2; GAS-PHASE H2O; HOT CORES
AB Water In Star-forming regions with Herschel (WISH) is a key program on the Herschel Space Observatory designed to probe the physical and chemical structures of young stellar objects using water and related molecules and to follow the water abundance from collapsing clouds to planet-forming disks. About 80 sources are targeted, covering a wide ranee of luminosities-from low (< 1 L-circle dot) to high (> 10(5) L-circle dot)-and a wide range of evolutionary stages-from cold prestellar cores to warm protostellar envelopes and outflows to disks around young stars. Both the HIFI and PACS instruments are used to observe a variety of lines of H2O, (H2O)-O-18 and chemically related species at the source position and in small maps around the protostars and selected outflow positions. In addition, high-frequency lines of CO, (CO)-C-13, and (CO)-O-18 are obtained with Herschel and are complemented by ground-based observations of dust continuum, HDO, CO and its isotopologs, and other molecules to ensure a self-consistent data set for analysis. An overview of the scientific motivation and observational strategy of the program is given, together with the modeling approach and analysis tools that have been developed. Initial science results are presented. These include a lack of water in cold gas at abundances that are lower than most predictions, strong water emission from shocks in protostellar environments, the importance of UV radiation in heating the gas along outflow walls across the full range of luminosities, and surprisingly widespread detection of the chemically related hydrides OH+ and H2O+ in outflows and foreground gas. Quantitative estimates of the energy budget indicate that H2O is generally not the dominant coolant in the warm dense gas associated with protostars. Very deep limits on the cold gaseous water reservoir in the outer regions of protoplanetary disks are obtained that have profound implications for our understanding of grain growth and mixing in disks.
C1 [van Dishoeck, E. F.; Kristensen, L. E.; Hogerheijde, M. R.; Brinch, C.; Deul, E.; Salter, D.; van Kempen, T. A.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[van Dishoeck, E. F.; Feuchtgruber, H.; Herczeg, G. J.; Karska, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Benz, A. O.; Bruderer, S.; Staeuber, P.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Caselli, P.; Codella, C.; Walmsley, M.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain.
[Herpin, F.; Baudry, A.; Bontemps, S.; Braine, J.; Chavarria, L.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France.
[Herpin, F.; Baudry, A.; Bontemps, S.; Braine, J.; Chavarria, L.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France.
[Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada.
[Liseau, R.; Bjerkeli, P.; Olberg, M.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden.
[Nisini, B.; Giannini, T.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Shipman, R.; van der Tak, F.; de Graauw, Th.; Helmich, F. P.; Marseille, M.; Risacher, C.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
[Tafalla, M.; Bachiller, R.] Observ Astron Nacl IGN, Madrid 28014, Spain.
[van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Aikawa, Y.] Kobe Univ, Dept Earth & Planetary Sci, Kobe, Hyogo 6578501, Japan.
[Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] Area Ric Tor Vergata, INAF Inst Fis Spazio Interplanetario, I-00133 Rome, Italy.
[Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
[Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA.
[Dubernet, M. L.] Univ Paris 06, LPMAA UMR CNRS 7092, F-75252 Paris 05, France.
[Dubernet, M. L.] Observ Paris, LUTH UMR CNRS 8102, F-92195 Meudon, France.
[Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France.
[Encrenaz, P.; Pagani, L.] Observ Paris, UMR 8112, CNRS, F-75014 Paris, France.
[Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain.
[Jorgensen, J. K.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark.
[Kaufman, M. J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Keto, E.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden.
[Lefloch, B.] Univ Grenoble 1, Lab Astrophys Grenoble, CNRS, UMR5571, F-38041 Grenoble 9, France.
[Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Panic, O.] European So Observ, D-85748 Garching, Germany.
[Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Santiago-Garcia, J.] Inst RadioAstron Milimetr, E-18012 Granada, Spain.
[Viti, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
RP van Dishoeck, EF (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM ewine@strw.leidenuniv.nl
RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser,
Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler,
Susanne/D-2270-2015; Brinch, Christian/G-5157-2015; Fuente,
Asuncion/G-1468-2016; Karska, Agata/O-5311-2016;
OI , Brunella Nisini/0000-0002-9190-0113; Codella,
Claudio/0000-0003-1514-3074; Yildiz, Umut/0000-0001-6197-2864;
Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes
Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657;
Brinch, Christian/0000-0002-5074-7183; Fuente,
Asuncion/0000-0001-6317-6343; Karska, Agata/0000-0001-8913-925X;
Bjerkeli, Per/0000-0002-7993-4118; Giannini, Teresa/0000-0002-0224-096X
NR 280
TC 139
Z9 139
U1 2
U2 14
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD FEB
PY 2011
VL 123
IS 900
BP 138
EP 170
DI 10.1086/658676
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 728WI
UT WOS:000287904800004
ER
PT J
AU Barghouty, AF
AF Barghouty, A. F.
TI The radiation quality factor as an Ornstein-Uhlenbeck process
SO RADIATION MEASUREMENTS
LA English
DT Article
DE Space radiation; Radiation quality factor; Monte-Carlo simulations;
Stochastic processes; Ornstein-Uhlenbeck process
AB Radiation protection strategies for extended or deep space missions rely on accurate and robust estimates of exposure dose and corresponding risk to crew health, systems functions, and mission safety in general. Simulation and modeling of dose and risk associated with such exposures are, to various degrees, made difficult by the inherent complexity and variability in characterizing the radiation environment, its passage and interaction with matter, and its biological effects. One of the more important contributors to the overall uncertainty in dose or risk assessment is the empirical variability in the radiation quality factor, Q which is typically used to differentiate such effects. Motivated in part by recent Monte-Carlo based simulations of this variability, we propose and demonstrate a stochastic dynamic model for Q based on the Ornstein-Uhlenbeck process. The proposed model's probability density function is a Gaussian in Q and with a linearly (in the logarithm of the LET variable) growing variance, but with rather complex scaling properties. The model's density function is shown to be quite sensitive to any functional parameterization of the mean (deterministic) behavior of the quality factor with a discontinuous first derivative in LET. The proposed linear stochastic model is also shown to be insensitive, however, to the precise functional form of the deterministic Q. Published by Elsevier Ltd.
C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Barghouty, AF (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM abdulnasser.f.barghouty@nasa.gov
NR 33
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1350-4487
J9 RADIAT MEAS
JI Radiat. Meas.
PD FEB
PY 2011
VL 46
IS 2
BP 224
EP 231
DI 10.1016/j.radmeas.2010.11.018
PG 8
WC Nuclear Science & Technology
SC Nuclear Science & Technology
GA 725DS
UT WOS:000287626000010
ER
PT J
AU Kiefer, RL
Gabler, WJ
Hovey, MT
Thibeault, SA
AF Kiefer, Richard L.
Gabler, William J.
Hovey, Michael T.
Thibeault, Sheila A.
TI The effects of exposure in space on two high-performance polymers
SO RADIATION PHYSICS AND CHEMISTRY
LA English
DT Article
DE Polyimide; Poly(etherimide); MISSE; Atomic oxygen
ID ATOMIC OXYGEN
AB Films of a polyimide, poly(pyromellitimide-1,4-diphenyl ether), and a poly(etherimide), commercial Ultem (R), both pure and with additives were exposed to the low earth orbit (LEO) space environment on several missions of the Materials on the International Space Station Experiment (MISSE). The additives, which contained aluminum or boron, were designed to interact with atomic oxygen to form a protective metal oxide coating. A polyimide film containing 10% aluminum acetylacetonate (Al(acac)(3)) survived an exposure of nearly four year while an adjacent pure film was completely eroded.
After exposure in space, films containing aluminum showed an enhanced amount of the element on the surface along with an enhanced amount of oxygen. Boron-containing films showed no enhancement of the element after exposure. The temperature of 10% mass loss increased with space exposure for films containing aluminum but decreased for those containing boron. The glass transition temperature (T(g)) increased after space exposure for polyimide films containing Al(acac)(3). (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Kiefer, Richard L.; Gabler, William J.; Hovey, Michael T.] Coll William & Mary, Dept Chem, Williamsburg, VA 23185 USA.
[Thibeault, Sheila A.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Kiefer, RL (reprint author), Coll William & Mary, Dept Chem, POB 8795, Williamsburg, VA 23185 USA.
EM rlkief@wm.edu
FU National Aeronautics and Space Administration [NNL06AA18A]; NASA Langley
Research Center
FX This research was supported by the National Aeronautics and Space
Administration through cooperative agreement NNL06AA18A with the NASA
Langley Research Center.
NR 7
TC 7
Z9 10
U1 2
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0969-806X
J9 RADIAT PHYS CHEM
JI Radiat. Phys. Chem.
PD FEB
PY 2011
VL 80
IS 2
BP 126
EP 129
DI 10.1016/j.radphyschem.2010.07.019
PG 4
WC Chemistry, Physical; Nuclear Science & Technology; Physics, Atomic,
Molecular & Chemical
SC Chemistry; Nuclear Science & Technology; Physics
GA 692QJ
UT WOS:000285169900002
ER
PT J
AU Boesch, H
Baker, D
Connor, B
Crisp, D
Miller, C
AF Boesch, Hartmut
Baker, David
Connor, Brian
Crisp, David
Miller, Charles
TI Global Characterization of CO2 Column Retrievals from Shortwave-Infrared
Satellite Observations of the Orbiting Carbon Observatory-2 Mission
SO REMOTE SENSING
LA English
DT Article
DE trace gases; remote sensing; inverse theory
ID FSI WFM-DOAS; ATMOSPHERIC CO2; MIDTROPOSPHERIC CO2; DATA ASSIMILATION;
SURFACE; SCIAMACHY; DIOXIDE; SINKS; SPECTROMETER; GASES
AB The global characteristics of retrievals of the column-averaged CO2 dry air mole fraction, X-CO2, from shortwave infrared observations has been studied using the expected measurement performance of the NASA Orbiting Carbon Observatory-2 (OCO-2) mission. This study focuses on X-CO2 retrieval precision and averaging kernels and their sensitivity to key parameters such as solar zenith angle (SZA), surface pressure, surface type and aerosol optical depth (AOD), for both nadir and sunglint observing modes. Realistic simulations have been carried out and the single sounding retrieval errors for X-CO2 have been derived from the formal retrieval error covariance matrix under the assumption that the retrieval has converged to the correct answer and that the forward model can adequately describe the measurement. Thus, the retrieval errors presented in this study represent an estimate of the retrieval precision. For nadir observations, we find single-sounding retrieval errors with values typically less than 1 part per million (ppm) over most land surfaces for SZAs less than 70 degrees and up to 2.5 ppm for larger SZAs. Larger errors are found over snow/ice and ocean surfaces due to their low albedo in the spectral regions of the CO2 absorption bands and, for ocean, also in the O-2 A band. For sunglint observations, errors over the ocean are significantly smaller than in nadir mode with values in the range of 0.3 to 0.6 ppm for small SZAs which can decrease to values as small as 0.15 for the largest SZAs. The vertical sensitivity of the retrieval that is represented by the column averaging kernel peaks near the surface and exhibits values near unity throughout most of the troposphere for most anticipated scenes. Nadir observations over dark ocean or snow/ice surfaces and observations with large AOD and large SZA show a decreased sensitivity to near-surface CO2. All simulations are carried out for a mid-latitude summer atmospheric profile, a given aerosol type and vertical distribution, a constant windspeed for ocean sunglint and by excluding the presence of thin cirrus clouds. The impact of these parameters on averaging kernels and X-CO2 retrieval errors are studied with sensitivity studies. Systematic biases in retrieved X-CO2, as can be introduced by uncertainties in the spectroscopic parameters, instrument calibration or deficiencies in the retrieval algorithm itself, are not included in this study. The presented error estimates will therefore only describe the true retrieval errors once systematic biases are eliminated. It is expected that it will be possible to retrieve X-CO2 for cloud free observations and for low AOD (here less than 0.3 for the wavelength region of the O-2 A band) with sufficient accuracy for improving CO2 surface flux estimates and we find that on average 18% to 21% of all observations are sufficiently cloud-free with only few areas suffering from the presence of persistent clouds or high AOD. This results typically in tens of useful observations per 16 day ground track repeat cycle at a 1 degrees x 1 degrees resolution. Averaging observations acquired along similar to 1 degrees intervals for individual ground tracks will significantly reduce the random component of the errors of the X-CO2 average product for ingestion into data assimilation/inverse models.
If biases in the X-CO2 retrieval of the order of a few tenth ppm can be successfully removed by validation or by bias-correction in the flux inversion, then it can be expected that OCO-2 X-CO2 data can lead to tremendous improvements in estimates of CO2 surface-atmosphere fluxes.
C1 [Boesch, Hartmut] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Baker, David] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Connor, Brian] BC Consulting Ltd, Alexandra 9320, New Zealand.
[Crisp, David; Miller, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Boesch, H (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
EM hartmut.boesch@le.ac.uk; baker@cira.colostate.edu;
bcconsulting@xtra.co.nz; david.crisp@jpl.nasa.gov;
charles.e.miller@jpl.nasa.gov
RI Boesch, Hartmut/G-6021-2012
FU Research Council UK
FX This work was partly performed by the Jet Propulsion Laboratory of the
California Institute of Technology, under contract to the National
Aeronautics and Space Administration. We gratefully acknowledge Denis
O'Brien for use of his orbit simulator and we would like to thank Robert
Parker and Austin Cogan for proof-reading. HB is funded by the Research
Council UK.
NR 57
TC 79
Z9 80
U1 5
U2 35
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD FEB
PY 2011
VL 3
IS 2
BP 270
EP 304
DI 10.3390/rs3020270
PG 35
WC Remote Sensing
SC Remote Sensing
GA 978MK
UT WOS:000306745600004
ER
PT J
AU Atli, KC
Karaman, I
Noebe, RD
Maier, HJ
AF Atli, K. C.
Karaman, I.
Noebe, R. D.
Maier, H. J.
TI Comparative analysis of the effects of severe plastic deformation and
thermomechanical training on the functional stability of
Ti50.5Ni24.5Pd25 high-temperature shape memory alloy
SO SCRIPTA MATERIALIA
LA English
DT Article
DE Equal channel angular extrusion/equal channel angular pressing; TiNiPd;
High-temperature shape memory alloys; Training; Actuator
ID ZN-AL ALLOY; NITI; TRANSFORMATION; PHASE
AB We compare the effectiveness of a conventional thermomechanical training procedure and severe plastic deformation via equal channel angular extrusion to achieve improved functional stability in a Ti50.5Ni24.5Pd25 high-temperature shape memory alloy. Thermomechanical testing indicates that both methods result in enhanced shape memory characteristics, such as reduced irrecoverable strain and thermal hysteresis The mechanisms responsible for the improvements are discussed in light of microstructural findings from transmission electron microscopy. (C) 2010 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Atli, K. C.; Karaman, I.] Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA.
[Karaman, I.] Texas A&M Univ, Mat Sci & Engn Grad Program, College Stn, TX 77843 USA.
[Noebe, R. D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Maier, H. J.] Univ Gesamthsch Paderborn, Lehrstuhl Werkstoffkunde Mat Sci, D-33098 Paderborn, Germany.
RP Atli, KC (reprint author), Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA.
EM ikaraman@tamu.edu
RI Karaman, Ibrahim/E-7450-2010; Atli, Kadri/D-6978-2013
OI Karaman, Ibrahim/0000-0001-6461-4958; Atli, Kadri/0000-0002-4807-2113
FU NASA [NNX07A-B56A]; National Science Foundation, Division of Industrial
Innovation and Partnerships [IIP-0832545]
FX This work was supported by the NASA Fundamental Aeronautics Program,
Subsonic Fixed Wing Project through Cooperative Agreement No.
NNX07A-B56A, Janet Hurst, API. Additional support was provided by the
National Science Foundation, Division of Industrial Innovation and
Partnerships, Grant No. IIP-0832545.
NR 18
TC 24
Z9 24
U1 3
U2 13
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6462
J9 SCRIPTA MATER
JI Scr. Mater.
PD FEB
PY 2011
VL 64
IS 4
BP 315
EP 318
DI 10.1016/j.scriptamat.2010.10.022
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 703CL
UT WOS:000285951600003
ER
PT J
AU Shreiber, D
Gupta, M
Cravey, R
AF Shreiber, D.
Gupta, M.
Cravey, R.
TI Comparative study of 1-D and 2-D metamaterial lens for microwave
nondestructive evaluation of dielectric materials
SO SENSORS AND ACTUATORS A-PHYSICAL
LA English
DT Article
DE Metamaterials lens; NDE; Microwave; Metamaterial sensor
ID REFRACTION
AB A novel microwave nondestructive evaluation (NDE) sensor was developed in an attempt to increase the sensitivity of the microwave NDE method for detection of material defects small relative to a wavelength. The sensor was designed on the basis of a negative index material (NIM) lens. Transmission at the resonant frequency through the 1-D lens was determined to be about 10 times higher than that with the 2-D lens. However, the focusing ability of the 1-D lens was found to be slightly lower to the 2-D lens (focus spot size for the 1-D lens was determined to be 0.7 lambda vs. 0.48 lambda for the 2-D lens). A fiberglass material sample with a 3 mm (0.037 lambda) diameter through hole (perpendicular to the propagation direction of the wave) was tested with both lenses. The hole was successfully detected with an 8.2 cm wavelength electromagnetic wave with both lenses, but the image obtained with a 2-D lens was much sharper. Therefore, the choice of the lens to be used in a sensor is prescribed by the specific requirements of the testing system. For example, a 1-D lens should be considered when the simplicity of the testing system is deemed more important than the quality of the image obtained from a defect. A 1-D lens also allows for a longer sample standoff distance and higher transmission. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Shreiber, D.; Gupta, M.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
[Cravey, R.] NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Hampton, VA 23681 USA.
RP Gupta, M (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
EM mgupta@virginia.edu
OI Shreiber, David/0000-0001-8248-419X
FU NASA Langley Research Center
FX The authors would like to thank Terry Mack, Kenneth Dudley and Bob Young
of the NASA Langley Research Center for their help in the design of the
experimental setup and valuable advice through the duration of the
experiments. We thank NASA Langley Research Center for their support of
this work and Langley Professor grant.
NR 9
TC 16
Z9 16
U1 1
U2 12
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0924-4247
J9 SENSOR ACTUAT A-PHYS
JI Sens. Actuator A-Phys.
PD FEB
PY 2011
VL 165
IS 2
BP 256
EP 260
DI 10.1016/j.sna.2010.12.004
PG 5
WC Engineering, Electrical & Electronic; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 731LO
UT WOS:000288108500017
ER
PT J
AU Kitiashvili, IN
Kosovichev, AG
Mansour, NN
Wray, AA
AF Kitiashvili, I. N.
Kosovichev, A. G.
Mansour, N. N.
Wray, A. A.
TI Numerical MHD Simulations of Solar Magnetoconvection and Oscillations in
Inclined Magnetic Field Regions
SO SOLAR PHYSICS
LA English
DT Article
DE Sunspots: penumbra, magnetic fields; Granulation; Oscillations: solar
ID SUNSPOT UMBRAL DOTS; REALISTIC SIMULATIONS; RADIAL OSCILLATIONS;
P-MODES; CONVECTION; EXCITATION; HELIOSEISMOLOGY; WAVES; SUN
AB The sunspot penumbra is a transition zone between the strong vertical magnetic field area (sunspot umbra) and the quiet Sun. The penumbra has a fine filamentary structure that is characterized by magnetic field lines inclined toward the surface. Numerical simulations of solar convection in inclined magnetic field regions have provided an explanation of the filamentary structure and the Evershed outflow in the penumbra. In this article, we use radiative MHD simulations to investigate the influence of the magnetic field inclination on the power spectrum of vertical velocity oscillations. The results reveal a strong shift of the resonance mode peaks to higher frequencies in the case of a highly inclined magnetic field. The frequency shift for the inclined field is significantly greater than that in vertical-field regions of similar strength. This is consistent with the behavior of fast MHD waves.
C1 [Kitiashvili, I. N.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA.
[Kitiashvili, I. N.; Kosovichev, A. G.] Stanford Univ, Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Mansour, N. N.; Wray, A. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kitiashvili, IN (reprint author), Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA.
EM irinasun@stanford.edu; sasha@sun.stanford.edu
NR 20
TC 11
Z9 11
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD FEB
PY 2011
VL 268
IS 2
BP 283
EP 291
DI 10.1007/s11207-010-9679-0
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735HB
UT WOS:000288403500004
ER
PT J
AU Hartlep, T
Kosovichev, AG
Zhao, J
Mansour, NN
AF Hartlep, T.
Kosovichev, A. G.
Zhao, J.
Mansour, N. N.
TI Signatures of Emerging Subsurface Structures in Acoustic Power Maps of
the Sun
SO SOLAR PHYSICS
LA English
DT Article
DE Emerging active regions; Wave propagation simulation; SOHO/MDI
observations; Helioseismology
ID HELIOSEISMOLOGY
AB We show that under certain conditions, subsurface structures in the solar interior can alter the average acoustic power observed at the photosphere above them. By using numerical simulations of wave propagation, we show that this effect is large enough for it to be potentially used for detecting emerging active regions before they appear on the surface. In our simulations, simplified subsurface structures are modeled as regions with enhanced or reduced acoustic wave speed. We investigate the dependence of the acoustic power above a subsurface region on the sign, depth, and strength of the wave-speed perturbation. Observations from the Solar and Heliospheric Observatory/Michelson Doppler Imager (SOHO/MDI) prior and during the emergence of NOAA active region 10488 are used to test the use of acoustic power as a potential precursor of the emergence of magnetic flux.
C1 [Hartlep, T.; Kosovichev, A. G.; Zhao, J.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Mansour, N. N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Hartlep, T (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM thartlep@sun.stanford.edu
RI Zhao, Junwei/A-1177-2007;
OI Hartlep, Thomas/0000-0002-5062-9507
NR 9
TC 22
Z9 22
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD FEB
PY 2011
VL 268
IS 2
BP 321
EP 327
DI 10.1007/s11207-010-9544-1
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 735HB
UT WOS:000288403500007
ER
PT J
AU Russo, RE
Bol'shakov, AA
Mao, XL
McKay, CP
Perry, DL
Sorkhabi, O
AF Russo, Richard E.
Bol'shakov, Alexander A.
Mao, Xianglei
McKay, Christopher P.
Perry, Dale L.
Sorkhabi, Osman
TI Laser Ablation Molecular Isotopic Spectrometry
SO SPECTROCHIMICA ACTA PART B-ATOMIC SPECTROSCOPY
LA English
DT Article
DE Optical isotopic measurements; Laser ablation plasma; Molecular emission
spectra; Real-time chemical analysis; Chemical analysis; LAMIS
ID INDUCED BREAKDOWN SPECTROSCOPY; MASS-SPECTROMETRY; SOLID SAMPLES;
EMISSION-SPECTROSCOPY; ICP-MS; PLASMA; URANIUM; RATIO; FEMTOSECOND;
NANOSECOND
AB A new method of performing optical isotopic analysis of condensed samples in ambient air and at ambient pressure has been developed: Laser Ablation Molecular Isotopic Spectrometry (LAMIS). The technique uses radiative transitions from molecular species either directly vaporized from a sample or formed by associative mechanisms of atoms or ions in a laser ablation plume. This method is an advanced modification of a known atomic emission technique called laser-induced breakdown spectroscopy (LIBS). The new method - LAMIS - can determine not only chemical composition but also isotopic ratios of elements in the sample. Isotopic measurements are enabled by significantly larger isotopic shifts found in molecular spectra relative to atomic spectra. Analysis can be performed from a distance and in real time. No sample preparation or pre-treatment is required. Detection of the isotopes of hydrogen, boron, carbon, and oxygen are discussed to illustrate the technique. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Russo, Richard E.; Mao, Xianglei; Perry, Dale L.; Sorkhabi, Osman] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Russo, Richard E.; Bol'shakov, Alexander A.] Appl Spectra Inc, Fremont, CA 94538 USA.
[McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Russo, RE (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
EM rerusso@lbl.gov
RI Bol'shakov, Alexander/A-9258-2015
OI Bol'shakov, Alexander/0000-0002-6034-7079
FU Defense Threat Reduction Administration (DTRA) of the U. S. Department
of Defense [LB09005541, LB09005541A]; U.S. Department of Energy through
the National Nuclear Security Administration (NNSA) [DE-AC02-05CH11231];
NASA [NNX10CA07C]
FX This work was supported by the Defense Threat Reduction Administration
(DTRA) of the U. S. Department of Defense under federal award nos.
LB09005541 and LB09005541A; and contract no. DE-AC02-05CH11231 awarded
by the U.S. Department of Energy through the National Nuclear Security
Administration (NNSA); and NASA contract no. NNX10CA07C awarded to
Applied Spectra Inc.
NR 43
TC 64
Z9 64
U1 2
U2 56
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0584-8547
J9 SPECTROCHIM ACTA B
JI Spectroc. Acta Pt. B-Atom. Spectr.
PD FEB
PY 2011
VL 66
IS 2
BP 99
EP 104
DI 10.1016/j.sab.2011.01.007
PG 6
WC Spectroscopy
SC Spectroscopy
GA 747OI
UT WOS:000289328900001
ER
PT J
AU Howard, SA
San Andres, L
AF Howard, Samuel A.
San Andres, Luis
TI A New Analysis Tool Assessment for Rotordynamic Modeling of Gas Foil
Bearings
SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE
ASME
LA English
DT Article
ID COUPLED FINITE-ELEMENT; JOURNAL BEARINGS; STRUCTURAL STIFFNESS;
THRUST-BEARINGS; COEFFICIENTS; PERFORMANCE; PREDICTION; FLOW; LOAD
AB Gas foil bearings offer several advantages over traditional bearing types that make them attractive for use in high-speed turbomachinery. They can operate at very high temperatures, require no lubrication supply (oil pumps, seals, etc.), exhibit very long life with no maintenance, and once operating airborne, have very low power loss. The use of gas foil bearings in high-speed turbomachinery has been accelerating in recent years although the pace has been slow. One of the contributing factors to the slow growth has been a lack of analysis tools, benchmarked to measurements, to predict gas foil bearing behavior in rotating machinery. To address this shortcoming, NASA Glenn Research Center (GRC) has supported the development of analytical tools to predict gas foil bearing performance. One of the codes has the capability to predict rotordynamic coefficients, power loss, film thickness, structural deformation, and more. The current paper presents an assessment of the predictive capability of the code named XLGFBTH c. A test rig at GRC is used as a simulated case study to compare rotordynamic analysis using output from the code to actual rotor response as measured in the test rig. The test rig rotor is supported on two gas foil journal bearings manufactured at GRC with all pertinent geometry disclosed. The resulting comparison shows that the rotordynamic coefficients calculated using XLGFBTH c represent the dynamics of the system reasonably well especially as they pertain to predicting critical speeds. [DOI: 10.1115/1.4001997]
C1 [Howard, Samuel A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[San Andres, Luis] Texas A&M Univ, Turbomachinery Lab, College Stn, TX 77843 USA.
RP Howard, SA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM samuel.a.howard@nasa.gov; lsanandres@tamu.edu
RI San Andres, Luis /C-6662-2014
OI San Andres, Luis /0000-0002-9619-3817
NR 34
TC 2
Z9 2
U1 0
U2 7
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0742-4795
EI 1528-8919
J9 J ENG GAS TURB POWER
JI J. Eng. Gas. Turbines Power-Trans. ASME
PD FEB
PY 2011
VL 133
IS 2
AR 022505
DI 10.1115/1.4001997
PG 9
WC Engineering, Mechanical
SC Engineering
GA 674KM
UT WOS:000283741200015
ER
PT J
AU Mishchenko, MI
Mackowski, DW
AF Mishchenko, Michael I.
Mackowski, Daniel W.
TI Coherent backscattering in the cross-polarized channel
SO PHYSICAL REVIEW A
LA English
DT Article
ID WEAK-LOCALIZATION; MULTIPLE-SCATTERING; RANDOM-MEDIA; COLD ATOMS;
T-MATRIX; LIGHT; PHOTONS; SPHERES
AB We analyze the asymptotic behavior of the cross-polarized enhancement factor in the framework of the standard low-packing-density theory of coherent backscattering by discrete random media composed of spherically symmetric particles. It is shown that if the particles are strongly absorbing or if the smallest optical dimension of the particulate medium (i.e., the optical thickness of a plane-parallel slab or the optical diameter of a spherically symmetric volume) approaches zero, then the cross-polarized enhancement factor tends to its upper-limit value 2. This theoretical prediction is illustrated using direct computer solutions of the Maxwell equations for spherical volumes of discrete random medium.
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Mackowski, Daniel W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM mmishchenko@giss.nasa.gov
RI Mackowski, Daniel/K-1917-2013; Mishchenko, Michael/D-4426-2012
FU NASA
FX We thank the anonymous reviewer for an instructive suggestion. This
research was supported in part by the NASA Radiation Sciences Program
managed by Hal Maring.
NR 32
TC 9
Z9 9
U1 1
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD JAN 31
PY 2011
VL 83
IS 1
AR 013829
DI 10.1103/PhysRevA.83.013829
PG 5
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 713OL
UT WOS:000286747200038
ER
PT J
AU Ricketts, CL
Contreras, CS
Walker, RL
Salama, F
AF Ricketts, Claire L.
Contreras, Cesar S.
Walker, Robert L.
Salama, Farid
TI The coupling of a reflectron time-of-flight mass spectrometer with a
cosmic simulation chamber: A powerful new tool for laboratory
astrophysics
SO INTERNATIONAL JOURNAL OF MASS SPECTROMETRY
LA English
DT Article
DE Reflectron time-of-flight mass spectrometry (ReTOF-MS); Pulsed discharge
nozzle (PDN) source; Cavity ringdown spectroscopy (CRDS); Polycyclic
aromatic hydrocarbon (PAH); Planetary atmospheres; Interstellar medium
(ISM)
ID RING-DOWN SPECTROSCOPY; INTERSTELLAR; EXPANSION; PLASMA
AB The addition of an orthogonal reflectron time-of-flight mass spectrometer (ReTOF-MS) to the NASA Ames cosmic simulation chamber (CSC) experiment is described. The simulation chamber contains the elements that produce the molecular species under astrophysically relevant conditions. A pulsed discharge nozzle (PDN) produces ions, neutrals and radicals in a plasma discharge, which are then expanded and supersonically cooled into the chamber. The coupling of the ReTOF-MS to the CSC provides real-time identification of the species, including cations and neutrals, formed in the plasma, an insight into the chemical pathways of the species reacting in the plasma, and an efficient method for the quick determination of the species present in the plasma, which can then be probed spectroscopically with the cavity ring-down spectrometer (CRDS). The combination of the ReTOF-MS, CRDS and PDN components into a single instrument offers a powerful tool, which can be used to probe a variety of different astrophysical environments such as interstellar clouds and planetary atmospheres. The experimental details and representative mass spectra are presented for plasmas generated in combinations of argon and methane samples. These mass spectra show the unambiguous detection of externally generated ions from the plasma in the simulation chamber. In addition, the various spectra show evidence of fragmentation and bond forming reactivity, illustrating the impact of the composition of the plasma. Published by Elsevier B.V.
C1 [Ricketts, Claire L.; Contreras, Cesar S.; Walker, Robert L.; Salama, Farid] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Astrophys Branch, Moffett Field, CA 94035 USA.
RP Salama, F (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Astrophys Branch, Mail Stop 245-6, Moffett Field, CA 94035 USA.
EM Claire.L.Ricketts@nasa.gov; Cesar.Contreras@nasa.gov;
Robert.L.Walker@nasa.gov; Farid.Salama@nasa.gov
RI Salama, Farid/A-8787-2009
OI Salama, Farid/0000-0002-6064-4401
FU NASA
FX This work is supported by NASA. We acknowledge the support provided by
the NASA Science Mission Directorate Planetary Atmospheres,
Cosmochemistry and Astronomy and Physics Research and Analysis (APRA)
Programs. C.L.R. and C.S.C. acknowledge the support of the NASA
Postdoctoral Program (NPP). The authors acknowledge fruitful discussions
with Paul Jordan, Ludovic Biennier, Hassan Sabbah, Joseph Roser, Jerome
Remy, Oscar Martinez, Veronica Bierbaum and Nigel Adams.
NR 21
TC 8
Z9 8
U1 0
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1387-3806
J9 INT J MASS SPECTROM
JI Int. J. Mass Spectrom.
PD JAN 30
PY 2011
VL 300
IS 1
BP 26
EP 30
DI 10.1016/j.ijms.2010.11.017
PG 5
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 727HP
UT WOS:000287789200004
ER
PT J
AU Skofronick-Jackson, G
Johnson, BT
AF Skofronick-Jackson, Gail
Johnson, Benjamin T.
TI Surface and atmospheric contributions to passive microwave brightness
temperatures for falling snow events
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MILLIMETER WAVELENGTHS; INFORMATION-CONTENT; CLOUD; ICE; RETRIEVALS;
RADIOMETER; ASSIMILATION; EMISSIVITY; MISSION; SYSTEM
AB Physically based passive microwave precipitation retrieval algorithms require a set of relationships between satellite-observed brightness temperatures (TBs) and the physical state of the underlying atmosphere and surface. These relationships are nonlinear, such that inversions are ill-posed especially over variable land surfaces. In order to elucidate these relationships, this work presents a theoretical analysis using TB weighting functions to quantify the percentage influence of the TB resulting from absorption, emission, and/or reflection from the surface, as well as from frozen hydrometeors in clouds, from atmospheric water vapor, and from other contributors. The percentage analysis was also compared to Jacobians. The results are presented for frequencies from 10 to 874 GHz, for individual snow profiles, and for averages over three cloud-resolving model simulations of falling snow. The bulk structure (e. g., ice water path and cloud depth) of the underlying cloud scene was found to affect the resultant TB and percentages, producing different values for blizzard, lake effect, and synoptic snow events. The slant path at a 53 degrees viewing angle increases the hydrometeor contributions relative to nadir viewing channels. Jacobians provide the magnitude and direction of change in the TB values due to a change in the underlying scene; however, the percentage analysis provides detailed information on how that change affected contributions to the TB from the surface, hydrometeors, and water vapor. The TB percentage information presented in this paper provides information about the relative contributions to the TB and supplies key pieces of information required to develop and improve precipitation retrievals over land surfaces.
C1 [Skofronick-Jackson, Gail] NASA, Goddard Space Flight Ctr, Mesoscale Proc Branch, Greenbelt, MD 20771 USA.
[Johnson, Benjamin T.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP Skofronick-Jackson, G (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Proc Branch, Code 613-1,Bldg 33,Room A416, Greenbelt, MD 20771 USA.
EM Gail.S.Jackson@nasa.gov; Benjamin.T.Johnson@nasa.gov
RI Skofronick-Jackson, Gail/D-5354-2012; Johnson, Benjamin/E-8557-2015
OI Johnson, Benjamin/0000-0003-3444-9669
FU NASA Headquarters
FX W.-K. Tao and his team are thanked for generating and providing the WRF
model simulation and Dong-Eon Chang is thanked for the MM5 simulation.
We thank Gousheng Liu for providing the nonspherical ice particle
scattering database. We also thank our anonymous reviewers for
constructive comments that greatly improved this paper. This work was
supported by Ramesh Kakar at NASA Headquarters through Precipitation
Measurement Mission funding.
NR 31
TC 18
Z9 18
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 29
PY 2011
VL 116
AR D02213
DI 10.1029/2010JD014438
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 713SN
UT WOS:000286757800002
ER
PT J
AU van Sebille, E
Kamenkovich, I
Willis, JK
AF van Sebille, Erik
Kamenkovich, Igor
Willis, Josh K.
TI Quasi-zonal jets in 3-D Argo data of the northeast Atlantic
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID WORLD OCEAN; CIRCULATION; MODEL; TURBULENCE
AB Time-mean zonal velocities, estimated from Argo float trajectories and density profiles, are systematically examined for quasi-zonal jets, or striations, with the use of a simple search algorithm. A comparison to altimeter data combined with an independent estimate of the mean dynamic topography shows that the jets in the 2004-2006 period examined are persistent and stationary. The jets have a typical meridional width of 100 to 200 km and a median transport of 4 Sverdrups. The jets tilt at approximately 6 from southwest to northeast in the horizontal plane, but show no significant tilt in the vertical plane. Velocities and the cross-stream width are similar for the westward and eastward jets. Citation: van Sebille, E., I. Kamenkovich, and J. K. Willis (2011), Quasi-zonal jets in 3-D Argo data of the northeast Atlantic, Geophys. Res. Lett., 38, L02606, doi:10.1029/2010GL046267.
C1 [van Sebille, Erik; Kamenkovich, Igor] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Willis, Josh K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP van Sebille, E (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
EM EvanSebille@rsmas.miami.edu
RI van Sebille, Erik/F-6781-2010
OI van Sebille, Erik/0000-0003-2041-0704
FU U.S. National Science Foundation [OCE0241438]; National Science
foundation [OCE0842834]; Jet Propulsion Laboratory, California Institute
of Technology, under NASA
FX E.vS. was supported by the U.S. National Science Foundation grant
OCE0241438. I. K. was supported by the National Science foundation grant
OCE0842834. J.W. was partly supported the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. The
AVISO data set was produced by Ssalto/Duacs, with support from CNES. We
would like to thank Pavel Berloff, Tom Farrar, and two reviewers for
their suggestions.
NR 20
TC 12
Z9 12
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2011
VL 38
AR L02606
DI 10.1029/2010GL046267
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 713TL
UT WOS:000286760200003
ER
PT J
AU Poppe, A
Halekas, JS
Horanyi, M
AF Poppe, Andrew
Halekas, Jasper S.
Horanyi, Mihaly
TI Negative potentials above the day-side lunar surface in the terrestrial
plasma sheet: Evidence of non-monotonic potentials
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID DUST TRANSPORT; PROSPECTOR; LEVITATION; SHADOW; PLATE
AB The Lunar Prospector (LP) Electron Reflectometer (ER) instrument conducted a series of measurements of the lunar surface potential in a variety of conditions. Occasionally, when the Moon was exposed to the terrestrial plasma sheet and in daylight, large, unexpected negative potentials (similar to-500 V) were measured. In this paper, we compare LP ER measurements with one-dimensional particle-in-cell simulations of the potential above the lunar surface when the Moon is exposed to both solar UV radiation and the terrestrial plasma sheet. The simulations show that large negative potentials will be measured by LP ER due to the presence of stable, non-monotonic potentials. Implications of these measurements to other airless bodies in the solar system are also discussed. Citation: Poppe, A., J. S. Halekas, and M. Horanyi (2011), Negative potentials above the day-side lunar surface in the terrestrial plasma sheet: Evidence of non-monotonic potentials, Geophys. Res. Lett., 38, L02103, doi:10.1029/2010GL046119.
C1 [Poppe, Andrew; Horanyi, Mihaly] Univ Colorado, Dept Phys, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Poppe, Andrew; Horanyi, Mihaly] Univ Colorado, Colorado Ctr Lunar Dust & Atmospher Studies, Boulder, CO 80309 USA.
[Poppe, Andrew; Halekas, Jasper S.; Horanyi, Mihaly] NASA, Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA 94035 USA.
[Halekas, Jasper S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Poppe, A (reprint author), Univ Colorado, Dept Phys, Atmospher & Space Phys Lab, UCB 392, Boulder, CO 80309 USA.
EM poppe@lasp.colorado.edu; jazzman@ssl.berkeley.edu; horanyi@colorado.edu
OI Poppe, Andrew/0000-0001-8137-8176; Horanyi, Mihaly/0000-0002-5920-9226;
Halekas, Jasper/0000-0001-5258-6128
FU NASA [NNX08BA17H, NNX08AY77G]; Colorado Center for Lunar Dust and
Atmospheric Studies of NASA's Lunar Science Institute; NASA Lunar
Science Institute
FX The authors thank G. T. Delory for helpful conversations on this
subject. A. P. was supported by the NASA Earth and Space Science
Fellowship program, grant NNX08BA17H. M. H. was supported by the
Colorado Center for Lunar Dust and Atmospheric Studies of NASA's Lunar
Science Institute and by NASA's LASER program, grant NNX08AY77G. J. S.
H. was supported by the NASA Lunar Science Institute.
NR 25
TC 26
Z9 26
U1 0
U2 0
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 JAN 28
PY 2011
VL 38
AR L02103
DI 10.1029/2010GL046119
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 713TL
UT WOS:000286760200002
ER
PT J
AU Huang, XC
Schwenke, DW
Lee, TJ
AF Huang, Xinchuan
Schwenke, David W.
Lee, Timothy J.
TI Rovibrational spectra of ammonia. II. Detailed analysis, comparison, and
prediction of spectroscopic assignments for (NH3)-N-14, (NH3)-N-15, and
(ND3)-N-14
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID POTENTIAL-ENERGY SURFACE; MU-M REGION; BANDS; INTENSITIES; NH3
AB Several aspects of ammonia rovibrational spectra have been investigated using the new HSL-2 potential energy surface that includes an approximate correction for nonadiabatic effects. The unprecedented accuracy of rovibrational energy levels and transition energies computed using HSL-2 was demonstrated in Part I of this study. For (NH3)-N-14, new assignments for a few nu(3) + nu(4) band transitions and energy levels are suggested, and discrepancies between computed and HITRAN energy levels in the 2 nu(4) band are analyzed (2 nu(4) is the most difficult band below 5000 cm (1)). New assignments are suggested for existing or missing 2 nu(4) levels. Several new vibrational bands are identified from existing, unassigned HITRAN data, including 2 nu(2) + nu(4), (nu(3) + nu(4)) -A'/A '', nu(1) + 2 nu(2), and 2 nu(2) + 2 nu(4). The strong mixing between the 2 nu(4) and 2 nu(2) + nu(4) bands is carefully examined and found to be the source of the difficulties in the experimental modeling of 2 nu(4). Discussion is presented for preliminary J = 10 results, where the overall root-mean-square error is estimated to be less than 0.039 cm(-1). The analysis of the 4 nu(2) band demonstrates both the reliability and the accuracy of predictions from HSL-2. The full list of computed J = 0 band origins (with assignments) and the inversion splittings up to 7000-8000 cm(-1) above the zero-point energy are presented. J = 0-2 levels are reported for those bands below 5100 cm(-1) that are missing from the HITRAN database. For (NH3)-N-15, excellent agreement is found for the available nu(2) and nu(3) + nu(4)(E) transition energies, but significant deficiencies are shown for HITRAN levels and several corrections are suggested. The N-15 isotopic effects are presented for the J = 0-6 levels of 13 HITRAN bands. For (ND3)-N-14, we reproduce the pure rotational inversion spectra line frequencies with an accuracy similar to that for (NH3)-N-14. However, it is not possible to reproduce simultaneously all four pairs of inversion-split vibrational fundamentals to better than 0.05 cm(-1) uncertainty. It is suggested that a reanalysis of some suspicious (ND3)-N-14 fundamental bands is required. The analyses presented here and in Part I show that rovibrational energy levels and transition frequencies computed with HSL-2 (with nonadiabatic corrections) remain highly accurate well beyond the experimental data used in the refinement procedure. Calculations using HSL-2 are capable of revealing many deficiencies in experimental analyses of ammonia spectra and provide reliable predictions with similar accuracy. It is expected that the results of this study will be useful in the future interpretation of high-resolution spectra from laboratory experiments or from astronomical observations. The present work represents a very significant advance in the state of our knowledge of the spectroscopy of ammonia and its isotopologues. (C) 2011 American Institute of Physics. [doi:10.1063/1.3541352]
C1 [Schwenke, David W.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
RP Lee, TJ (reprint author), NASA, Ames Res Ctr, MS 245-1, Moffett Field, CA 94035 USA.
EM Xinchuan.Huang-1@nasa.gov; David.W.Schwenke@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 [Cycle 0 TR/LA PID 1022, 08-APRA08-0050]; NASA/SETI Institute
[NNX09AI49A]
FX The authors gratefully acknowledge support from the NASA Herschel GO
Program, Cycle 0 TR/LA PID 1022, and the NASA Grant No. 08-APRA08-0050.
X.H. acknowledges the financial support by NASA/SETI Institute
Cooperative Agreement NNX09AI49A. We would like to thank Dr. Holger S.P.
Muller for fruitful communications on 15NH3
modeling. We thank Dr. Isabelle Kleiner and Dr. Linda R. Brown for
stimulating discussions.
NR 19
TC 43
Z9 44
U1 1
U2 21
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 JAN 28
PY 2011
VL 134
IS 4
AR 044321
DI 10.1063/1.3541352
PG 18
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 715PY
UT WOS:000286897600064
PM 21280739
ER
PT J
AU Huang, XC
Schwenke, DW
Lee, TJ
AF Huang, Xinchuan
Schwenke, David W.
Lee, Timothy J.
TI Rovibrational spectra of ammonia. I. Unprecedented accuracy of a
potential energy surface used with nonadiabatic corrections
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID ELECTRONIC GROUND-STATE; MU-M REGION; (NH3)-N-14; NH3; SPECTROSCOPY;
TRANSITIONS; INTENSITIES; TERAHERTZ; BANDS; WATER
AB In this work, we build upon our previous work on the theoretical spectroscopy of ammonia, NH(3). Compared to our 2008 study, we include more physics in our rovibrational calculations and more experimental data in the refinement procedure, and these enable us to produce a potential energy surface (PES) of unprecedented accuracy. We call this the HSL-2 PES. The additional physics we include is a second-order correction for the breakdown of the Born-Oppenheimer approximation, and we find it to be critical for improved results. By including experimental data for higher rotational levels in the refinement procedure, we were able to greatly reduce our systematic errors for the rotational dependence of our predictions. These additions together lead to a significantly improved total angular momentum (J) dependence in our computed rovibrational energies. The root-mean-square error between our predictions using the HSL-2 PES and the reliable energy levels from the HITRAN database for J = 0-6 and J = 7/8 for (14)NH(3) is only 0.015 cm(-1) and 0.020/0.023 cm(-1), respectively. The root-mean-square errors for the characteristic inversion splittings are approximately 1/3 smaller than those for energy levels. The root-mean-square error for the 6002 J = 0-8 transition energies is 0.020 cm(-1). Overall, for J = 0-8, the spectroscopic data computed with HSL-2 is roughly an order of magnitude more accurate relative to our previous best ammonia PES (denoted HSL-1). These impressive numbers are eclipsed only by the root-mean-square error between our predictions for purely rotational transition energies of (15)NH(3) and the highly accurate Cologne database (CDMS): 0.00034 cm(-1) (10 MHz), in other words, 2 orders of magnitude smaller. In addition, we identify a deficiency in the (15)NH(3) energy levels determined from a model of the experimental data. (C) 2011 American Institute of Physics. [doi:10.1063/1.3541351]
C1 [Schwenke, David W.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
RP Lee, TJ (reprint author), NASA, Ames Res Ctr, MS 245-1, Moffett Field, CA 94035 USA.
EM Xinchuan.Huang-1@nasa.gov; David.W.Schwenke@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 [Cycle 0 TR/LA PID 1022, 08-APRA08-0050]; NASA/SETI Institute
[NNX09AI49A]
FX The authors gratefully acknowledge support from the NASA Herschel GO
Program, Cycle 0 TR/LA PID 1022, and the NASA Grant 08-APRA08-0050. X.H
acknowledges the financial support by NASA/SETI Institute Cooperative
Agreement NNX09AI49A.
NR 29
TC 56
Z9 58
U1 1
U2 37
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 JAN 28
PY 2011
VL 134
IS 4
AR 044320
DI 10.1063/1.3541351
PG 15
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 715PY
UT WOS:000286897600063
PM 21280738
ER
PT J
AU Glaze, LS
Baloga, SM
Wimert, J
AF Glaze, Lori S.
Baloga, Stephen M.
Wimert, Jesse
TI Explosive volcanic eruptions from linear vents on Earth, Venus, and
Mars: Comparisons with circular vent eruptions
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID BASALTIC FISSURE ERUPTIONS; PLUME HEIGHTS; TYRRHENA PATERA; LAVA FLOW;
TRANSPORT; COLUMNS; MODEL; MONS; CONVECTION; DISPERSAL
AB Conditions required to support buoyant convective plumes are investigated for explosive volcanic eruptions from circular and linear vents on Earth, Venus, and Mars. Vent geometry (linear versus circular) plays a significant role in the ability of an explosive eruption to sustain a buoyant plume. On Earth, linear and circular vent eruptions are both capable of driving buoyant plumes to equivalent maximum rise heights; however, linear vent plumes are more sensitive to vent size. For analogous mass eruption rates, linear vent plumes surpass circular vent plumes in entrainment efficiency approximately when L(o) >= 3r(o) owing to the larger entrainment area relative to the control volume. Relative to circular vents, linear vents on Venus favor column collapse and the formation of pyroclastic flows because the range of conditions required to establish and sustain buoyancy is narrow. When buoyancy can be sustained, however, maximum plume heights exceed those from circular vents. For current atmospheric conditions on Mars, linear vent eruptions are capable of injecting volcanic material slightly higher than analogous circular vent eruptions. However, both geometries are more likely to produce pyroclastic fountains, as opposed to convective plumes, owing to the low-density atmosphere. Because of the atmospheric density profile and water content on Earth, explosive eruptions enjoy favorable conditions for producing sustained buoyant columns, while pyroclastic flows would be relatively more prevalent on Venus and Mars. These results have implications for the injection and dispersal of particulates into the planetary atmosphere and the ability to interpret the geologic record of planetary volcanism.
C1 [Glaze, Lori S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baloga, Stephen M.] Proxemy Res, Gaithersburg, MD 20882 USA.
[Wimert, Jesse] Univ Maryland, Dept Geol, College Pk, MD 20742 USA.
RP Glaze, LS (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Lori.S.Glaze@nasa.gov; Steve@Proxemy.com; jwimert@umd.edu
RI Glaze, Lori/D-1314-2012
FU NASA [WBS 811073.02.01.04.44, NNX08AF16G]; University of Maryland
FX This work was funded by the NASA Planetary Geology and Geophysics
Program (WBS 811073.02.01.04.44 for L. Glaze, and grant NNX08AF16G for
S. Baloga). J. Wimert was supported by L. Glaze (Planetary Geology and
Geophysics WBS) through the University of Maryland CRESST program. The
authors would like to thank Steve Self for a very constructive review of
this manuscript.
NR 56
TC 6
Z9 6
U1 1
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JAN 28
PY 2011
VL 116
AR E01011
DI 10.1029/2010JE003577
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 713VF
UT WOS:000286764800001
ER
PT J
AU Heavens, NG
McCleese, DJ
Richardson, MI
Kass, DM
Kleinbohl, A
Schofield, JT
AF Heavens, N. G.
McCleese, D. J.
Richardson, M. I.
Kass, D. M.
Kleinboehl, A.
Schofield, J. T.
TI Structure and dynamics of the Martian lower and middle atmosphere as
observed by the Mars Climate Sounder: 2. Implications of the thermal
structure and aerosol distributions for the mean meridional circulation
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GLOBAL SURVEYOR AEROBRAKING; DUST STORMS; NUMERICAL SIMULATIONS; MODEL
SIMULATION; POLAR WARMINGS; WAVES; DISTURBANCES; ASSIMILATION;
ASYMMETRY; TIDES
AB Retrievals of temperature, dust, and water ice from data collected by the Mars Climate Sounder (MCS) on Mars Reconnaissance Orbiter (MRO) illustrate for the first time the seasonal and diurnal variability of both the thermal structure of the middle atmosphere (above 40 km) and also the vertical distribution of aerosols. These retrievals reveal clear signatures of significant mean meridional cells in the middle and lower atmosphere at both the solstices and equinoxes. We investigate the degree to which the lower and middle atmospheric circulations are kinematically coupled and conclude that kinematic coupling is strong in the tropics throughout the year but weak near the pole except during the "polar warming" events associated with dust storm activity.
C1 [McCleese, D. J.; Kass, D. M.; Kleinboehl, A.; Schofield, J. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Richardson, M. I.] Ashima Res, Pasadena, CA 91106 USA.
[Heavens, N. G.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA.
RP Heavens, NG (reprint author), Cornell Univ, Dept Earth & Atmospher Sci, 1118 Bradfield Hall, Ithaca, NY 14853 USA.
EM heavens@cornell.edu
OI Heavens, Nicholas/0000-0001-7654-503X
FU Jet Propulsion Laboratory, California Institute of Technology; NASA
FX We thank two anonymous reviewers for their helpful comments on this
manuscript. We would also like to thank Tina Pavlicek for her
contributions to MCS instrument operations and Mark Apolinski for his
work on processing the MCS data. We also wish to thank Wayne Hartford
and Mark Foote for their contributions to the design and fabrication of
the instrument and the MRO spacecraft operations teams who make this
investigation possible. This work was performed in part at and funded by
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with NASA.
NR 60
TC 19
Z9 19
U1 0
U2 7
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 JAN 28
PY 2011
VL 116
AR E01010
DI 10.1029/2010JE003713
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 713VF
UT WOS:000286764800002
ER
PT J
AU Nedoluha, GE
Connor, BJ
Barrett, J
Mooney, T
Parrish, A
Boyd, I
Wrotny, JE
Gomez, RM
Koda, J
Santee, ML
Froidevaux, L
AF Nedoluha, Gerald E.
Connor, Brian J.
Barrett, James
Mooney, Thomas
Parrish, Alan
Boyd, Ian
Wrotny, Jonathan E.
Gomez, R. Michael
Koda, Jin
Santee, Michelle L.
Froidevaux, Lucien
TI Ground-based measurements of ClO from Mauna Kea and intercomparisons
with Aura and UARS MLS
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CHLORINE MONOXIDE; STRATOSPHERE; VALIDATION; CHEMISTRY; OZONE;
ANTARCTICA; MESOSPHERE; SATELLITE; HALOE; MODEL
AB The ground-based measurements of upper stratospheric ClO, made with a ground-based millimeter wave instrument at Mauna Kea, Hawaii (19.8 degrees N, 204.5 degrees E) starting in 1992, are compared with UARS (Upper Atmosphere Research Satellite) MLS ClO measurements (1991-1998) and the Aura MLS ClO measurements (2004-2009). The ground-based measurements are made as part of the Network for the Detection of Atmospheric Composition Change (NDACC). Intercomparisons between the ground-based measurements and the Aura MLS measurements show that both instruments retrieve similar seasonal variations over Mauna Kea. The seasonal variation in ClO is also compared with measurements of variations in stratospheric CH4, which affects the partitioning of total inorganic chlorine. Using the ground-based instruments as a transfer standard, we find that the agreement between UARS and Aura MLS ClO measurements near the peak of the mixing ratio profile is within similar to 1%. Combining the uncertainties in the biases calculated from the coincident ground-based and satellite measurements, we find that using the ground-based data as a transfer standard allows us to provide a 2 sigma limit to the bias between the UARS and Aura measurements of 3%-4% near the peak of the ClO profile. Given agreement between UARS and Aura MLS of similar to 1%+/- 4%, there is no reason to apply any bias correction in order to use the UARS and Aura MLS ClO measurements as a single data set.
C1 [Nedoluha, Gerald E.; Gomez, R. Michael] USN, Res Lab, Washington, DC 20375 USA.
[Connor, Brian J.] BC Consulting, Alexandra, New Zealand.
[Barrett, James; Mooney, Thomas; Koda, Jin] SUNY Stony Brook, Stony Brook, NY 11794 USA.
[Parrish, Alan] Univ Massachusetts, Amherst, MA 01003 USA.
[Santee, Michelle L.; Froidevaux, Lucien] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Boyd, Ian] Natl Inst Water & Atmospher Res, Auckland 1149, New Zealand.
[Wrotny, Jonathan E.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
RP Nedoluha, GE (reprint author), USN, Res Lab, 4555 Overlook Ave, Washington, DC 20375 USA.
EM nedoluha@nrl.navy.mil
FU National Aeronautics and Space Administration; NASA [NNX09AF40G]
FX We are deeply indebted to Prof. Philip Solomon of Stony Brook
University, who was one of the first to envision that stratospheric ClO
could be monitored by ground-based remote measurements. Subsequently, he
led this program from its inception in the 1980s until his death in
April 2008. Work at the Jet Propulsion Laboratory, California Institute
of Technology, was done under contract with the National Aeronautics and
Space Administration. The ground-based measurement program is funded by
NASA grant NNX09AF40G.
NR 22
TC 6
Z9 6
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 JAN 27
PY 2011
VL 116
AR D02307
DI 10.1029/2010JD014732
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 713SI
UT WOS:000286757300010
ER
PT J
AU Quinto-Hernandez, A
Wodtke, AM
Bennett, CJ
Kim, YS
Kaiser, RI
AF Quinto-Hernandez, Alfredo
Wodtke, Alec M.
Bennett, Chris J.
Kim, Y. Seol
Kaiser, Ralf I.
TI On the Interaction of Methyl Azide (CH3N3) Ices with Ionizing Radiation:
Formation of Methanimine (CH2NH), Hydrogen Cyanide (HCN), and Hydrogen
Isocyanide (HNC)
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID ICY GRAIN MANTLES; O1 HALE-BOPP; INFRARED-SPECTRUM; TITANS ATMOSPHERE;
ULTRAVIOLET PHOTOLYSIS; INTERSTELLAR-MEDIUM; MATRIX-ISOLATION;
CARBON-DIOXIDE; SURFACE; SPECTROSCOPY
AB Methyl azide (CH3N3) might be a potential precursor in the synthesis of prebiotic molecules via nonequilibrium reactions on interstellar ices initiated by energetic galactic cosmic rays (GCR) and photons. Here, we investigate the effects of energetic electrons as formed in the track of cosmic ray particles and 193 nm photons with solid methyl azide at 10 K and the inherent formation of methanimine (CH2NH), hydrogen cyanide (HCN), and hydrogen isocyanide (HNC). We present a systematic kinetic study and outline feasible reaction pathways to these molecules. These processes might be also important in solar system analogue ices.
C1 [Bennett, Chris J.; Kim, Y. Seol; Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
[Quinto-Hernandez, Alfredo; Wodtke, Alec M.] Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA.
[Bennett, Chris J.] Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
RP Kaiser, RI (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
EM ralfk@hawaii.edu
RI Wodtke, Alec/I-4848-2012;
OI Bennett, Christopher/0000-0002-4181-6976; Wodtke,
Alec/0000-0002-6509-2183
FU Chemistry Division of the U.S. National Science Foundation [NSF-CRC
CHE-0627854]; National Council for Science and Technology
(CONACYT-Mexico); University of California Institute for Mexico; United
States (UC-MEXUS)
FX This project was supported by the Chemistry Division of the U.S.
National Science Foundation within the Collaborative Research in
Chemistry Program (NSF-CRC CHE-0627854). A.Q.H. is indebted to the
National Council for Science and Technology (CONACYT-Mexico) and the
University of California Institute for Mexico and the United States
(UC-MEXUS) for the continuing financial support. A.Q.H. further thanks
the UH NASA Astrobiology Institute for support of his accommodations at
the University of Hawaii at Manoa. C.J.B. and A.Q.H. thank the National
Aeronautics Space Administration (NASA-Astrobiology Institute under
Cooperative Agreement no. NNA09DA77A issued through the Office of Space
Science). We are also grateful to Dr. Gu (Department of Chemistry,
University of Hawaii at Mama) for his technical assistance.
NR 76
TC 8
Z9 8
U1 1
U2 21
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD JAN 27
PY 2011
VL 115
IS 3
BP 250
EP 264
DI 10.1021/jp103028v
PG 15
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 707SO
UT WOS:000286306500004
PM 21162584
ER
PT J
AU Nedoluha, GE
Gomez, RM
Hicks, BC
Helmboldt, J
Bevilacqua, RM
Lambert, A
AF Nedoluha, Gerald E.
Gomez, R. Michael
Hicks, Brian C.
Helmboldt, Joe
Bevilacqua, Richard M.
Lambert, Alyn
TI Ground-based microwave measurements of water vapor from the
midstratosphere to the mesosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TEMPERATURE; ATMOSPHERE
AB We present 5 months of retrievals from a new Water Vapor Millimeter-wave Spectrometer (WVMS) instrument that has been deployed at Table Mountain, California (34.4 degrees N, 242.3 degrees E). The single most important improvement over previous WVMS instruments is that instead of a set of 90 filters, this instrument has a fast Fourier transform spectrometer that provides 16,384 channels across 500 MHz, with a channel bandwidth of similar to 30 kHz. The additional information provided by this spectrometer makes it possible to extend the altitude range of the WVMS measurements from the current similar to 40-80 km range to similar to 26-80 km. We present details of the retrieval scheme and study the effects on the retrieved profiles of fitting instrumental baseline components. We compare the retrievals to coincident measurements from the NASA Aura Microwave Limb Sounder (MLS) instrument with a particular emphasis on understanding the stability of the 26 km retrievals. While the retrieval is sensitive to variations at this altitude, neither the MLS-retrieved water vapor mixing ratios nor those retrieved by WVMS show much variation over the 5 month period: a good indication of the stability of both instruments.
C1 [Nedoluha, Gerald E.; Gomez, R. Michael; Hicks, Brian C.; Helmboldt, Joe; Bevilacqua, Richard M.] USN, Res Lab, Washington, DC 20375 USA.
[Lambert, Alyn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nedoluha, GE (reprint author), USN, Res Lab, 4555 Overlook Ave,Code 7227, Washington, DC 20375 USA.
EM nedoluha@nrl.navy.mil
RI Helmboldt, Joseph/C-8105-2012
FU National Aeronautics and Space Administration; NASA; Naval Research
Laboratory
FX We wish to thank S. McDermid, D. Walsh, and T. LeBlanc at Mauna Loa for
their technical assistance. Work at the Jet Propulsion Laboratory,
California Institute of Technology, was carried out under a contract
with the National Aeronautics and Space Administration. This project was
funded by NASA under the Upper Atmosphere Research Program and by the
Naval Research Laboratory.
NR 17
TC 12
Z9 12
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 JAN 27
PY 2011
VL 116
AR D02309
DI 10.1029/2010JD014728
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 713SI
UT WOS:000286757300009
ER
PT J
AU Yasunari, TJ
Koster, RD
Lau, KM
Aoki, T
Sud, YC
Yamazaki, T
Motoyoshi, H
Kodama, Y
AF Yasunari, Teppei J.
Koster, Randal D.
Lau, K. -M.
Aoki, Teruo
Sud, Yogesh C.
Yamazaki, Takeshi
Motoyoshi, Hiroki
Kodama, Yuji
TI Influence of dust and black carbon on the snow albedo in the NASA
Goddard Earth Observing System version 5 land surface model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CATCHMENT-BASED APPROACH; ASIAN SUMMER MONSOON; TIBETAN PLATEAU;
SPECTRAL ALBEDO; PHYSICAL PARAMETERS; SOLAR-RADIATION; GOCART MODEL;
DIRTY SNOW; ICE CORE; CLIMATE
AB Present-day land surface models rarely account for the influence of both black carbon and dust in the snow on the snow albedo. Snow impurities increase the absorption of incoming shortwave radiation (particularly in the visible bands), whereby they have major consequences for the evolution of snowmelt and life cycles of snowpack. A new parameterization of these snow impurities was included in the catchment-based land surface model used in the National Aeronautics and Space Administration Goddard Earth Observing System version 5. Validation tests against in situ observed data were performed for the winter of 2003-2004 in Sapporo, Japan, for both the new snow albedo parameterization (which explicitly accounts for snow impurities) and the preexisting baseline albedo parameterization (which does not). Validation tests reveal that daily variations of snow depth and snow surface albedo are more realistically simulated with the new parameterization. Reasonable perturbations in the assigned snow impurity concentrations, as inferred from the observational data, produce significant changes in snowpack depth and radiative flux interactions. These findings illustrate the importance of parameterizing the influence of snow impurities on the snow surface albedo for proper simulation of the life cycle of snow cover.
C1 [Yasunari, Teppei J.; Koster, Randal D.; Lau, K. -M.; Sud, Yogesh C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yasunari, Teppei J.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Aoki, Teruo] Meteorol Res Inst, Tsukuba, Ibaraki 3050052, Japan.
[Yamazaki, Takeshi] Tohoku Univ, Grad Sch Sci, Dept Geophys, Sendai, Miyagi 9808578, Japan.
[Motoyoshi, Hiroki] Natl Res Inst Earth Sci & Disaster Prevent, Snow & Ice Res Ctr, Nagaoka, Niigata 9400821, Japan.
[Kodama, Yuji] Hokkaido Univ, Inst Low Temp Sci, Sapporo, Hokkaido 0600819, Japan.
RP Yasunari, TJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM teppei.j.yasunari@nasa.gov
RI Koster, Randal/F-5881-2012; Yasunari, Teppei/E-5374-2010; Lau, William
/E-1510-2012
OI Koster, Randal/0000-0001-6418-6383; Yasunari,
Teppei/0000-0002-9896-9404; Lau, William /0000-0002-3587-3691
FU NASA [NCC5-494]
FX This research was conducted as a part of the Joint Aerosol Monsoon
Experiment (JAMEX), supported by the NASA Interdisciplinary
Investigation Program. The first author is on a visiting fellowship to
the Goddard Earth Science and Technology Center at the University of
Maryland at Baltimore County (NASA Grant and Cooperative Agreement
NCC5-494). Meteorological data at AWS/JMA were observed and maintained
by the Japan Meteorological Agency. Mass absorption coefficient data
were provided by Mark Flanner at the University of Michigan and Charlie
Zender at the University of California. The online snow albedo model
based on that of Mark Flanner and others was used. Tomonori Tanikawa at
Earth Observation Research Center (EORC), Japan Aerospace Exploration
Agency (JAXA) offered useful comments on formulations of the snow albedo
model. We appreciate useful comments from two anonymous reviewers.
NR 77
TC 24
Z9 26
U1 4
U2 20
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 JAN 27
PY 2011
VL 116
AR D02210
DI 10.1029/2010JD014861
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 713SI
UT WOS:000286757300011
ER
PT J
AU Kwok, R
Morison, J
AF Kwok, R.
Morison, J.
TI Dynamic topography of the ice-covered Arctic Ocean from ICESat
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SEA-ICE
AB We construct the dynamic ocean topography (DOT) of the Arctic Ocean, for five ICESat campaigns (winter of 2004-2008), using sea surface height estimates in open leads. Results show that the mean winter DOT over the Arctic Ocean varies by similar to 1 m and features a distinct dome of similar to 40 cm over the Beaufort Sea. Standard deviation of the mean field is similar to 20 cm. Spatial coherence between the five winter DOTs is consistently high (>0.9), whereas the coherence between the DOTs and the winter (DJFM) sea-level pressure fields over the Arctic Basin is variable. This suggests persistence of the underlying hydrodynamic processes at interannual time-scales compared to seasonal atmospheric forcing. Comparison of dynamic heights (DH) from hydrographic surveys and the DOT in 2008 shows a remarkable correlation of 0.92. The geostrophic velocity fields computed from the DOT and interpolated DH fields highlight the smaller scale oceanographic features in the satellite estimates. Citation: Kwok, R., and J. Morison (2011), Dynamic topography of the ice-covered Arctic Ocean from ICESat, Geophys. Res. Lett., 38, L02501, doi: 10.1029/2010GL046063.
C1 [Kwok, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morison, J.] Univ Washington, Polar Sci Ctr, Seattle, WA 98105 USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
FU NASA [NNX08AH62G]; NSF [OPP 0352754, ARC-0634226, ARC-0856330]
FX The authors also wish to thank Matt Alkire, Miles McPhee, Roger
Andersen, Glenn Cunningham, Cecilia Peralta-Ferriz, Andrey Proshutinsky,
Ignatius Rigor, Mike Steele, and John Toole. R.K. performed this work at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA. J.M. performed this work under NSF grants OPP
0352754, ARC-0634226, ARC-0856330, and NASA grant NNX08AH62G.
NR 17
TC 24
Z9 26
U1 2
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 26
PY 2011
VL 38
AR L02501
DI 10.1029/2010GL046063
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 713TE
UT WOS:000286759500004
ER
PT J
AU AghaKouchak, A
Behrangi, A
Sorooshian, S
Hsu, K
Amitai, E
AF AghaKouchak, A.
Behrangi, A.
Sorooshian, S.
Hsu, K.
Amitai, E.
TI Evaluation of satellite-retrieved extreme precipitation rates across the
central United States
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RAINFALL PRODUCTS; RESOLUTION; RADAR; VALIDATION; GAUGE; ALGORITHM;
COPULA; MODEL; BASIN
AB Water resources management, forecasting, and decision making require reliable estimates of precipitation. Extreme precipitation events are of particular importance because of their severe impact on the economy, the environment, and the society. In recent years, the emergence of various satellite-retrieved precipitation products with high spatial resolutions and global coverage have resulted in new sources of uninterrupted precipitation estimates. However, satellite-based estimates are not well integrated into operational and decision-making applications because of a lack of information regarding the associated uncertainties and reliability of these products. In this study, four satellite-derived precipitation products (CMORPH, PERSIANN, TMPA-RT, and TMPA-V6) are evaluated with respect to their performance in capturing precipitation extremes. The Stage IV (radar-based, gauge-adjusted) precipitation estimates are used as reference data. The results show that with respect to the probability of detecting extremes and the volume of correctly identified precipitation, CMORPH and PERSIANN data sets lead to better estimates. However, their false alarm ratio and volume are higher than those of TMPA-RT and TMPA-V6. Overall, no single precipitation product can be considered ideal for detecting extreme events. In fact, all precipitation products tend to miss a significant volume of rainfall. With respect to verification metrics used in this study, the performance of all satellite products tended to worsen as the choice of extreme precipitation threshold increased. The analyses suggest that extensive efforts are necessary to develop algorithms that can capture extremes more reliably.
C1 [AghaKouchak, A.; Sorooshian, S.; Hsu, K.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA.
[Behrangi, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Amitai, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Amitai, E.] Chapman Univ, Sch Earth & Environm Sci, Orange, CA USA.
RP AghaKouchak, A (reprint author), Univ Calif Irvine, Dept Civil & Environm Engn, E4130 Engn Gateway, Irvine, CA 92697 USA.
EM amir.a@uci.edu
RI sorooshian, soroosh/B-3753-2008
OI sorooshian, soroosh/0000-0001-7774-5113
FU NOAA/NESDIS/NCDC [NA09NES4400006, 2009-1380-01]
FX The financial support for this study was made available by
NOAA/NESDIS/NCDC (prime award NA09NES4400006, NCSU CICS sub-award
2009-1380-01).
NR 40
TC 59
Z9 59
U1 6
U2 28
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 26
PY 2011
VL 116
AR D02115
DI 10.1029/2010JD014741
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 713SF
UT WOS:000286757000003
ER
PT J
AU Nair, US
McNider, R
Patadia, F
Christopher, SA
Fuller, K
AF Nair, Udaysankar S.
McNider, Richard
Patadia, Falguni
Christopher, Sundar A.
Fuller, Kirk
TI Sensitivity of nocturnal boundary layer temperature to tropospheric
aerosol surface radiative forcing under clear-sky conditions
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GLOBAL CLIMATE-CHANGE; AIR-POLLUTION; UNITED-STATES; PART II; RANGE;
TRENDS; MODEL; CLOUDS; PARAMETERIZATION; 20TH-CENTURY
AB Since the middle of the last century, global surface air temperature exhibits an increasing trend, with nocturnal temperatures increasing at a much higher rate. Proposed causative mechanisms include the radiative impact of atmospheric aerosols on the nocturnal boundary layer (NBL) where the temperature response is amplified due to shallow depth and its sensitivity to potential destabilization. A 1-D version of the Regional Atmospheric Modeling System is used to examine the sensitivity of the nocturnal boundary layer temperature to the surface longwave radiative forcing (SLWRF) from urban aerosol loading and doubled atmospheric carbon dioxide concentrations. The analysis is conducted for typical midlatitude nocturnal boundary layer case days from the CASES-99 field experiment and is further extended to urban sites in Pune and New Delhi, India. For the cases studied, locally, the nocturnal SLWRF from urban atmospheric aerosols (2.7-47 W m(-2)) is comparable or exceeds that caused by doubled atmospheric carbon dioxide (3 W m(-2)), with the surface temperature response ranging from a compensation for daytime cooling to an increase in the nocturnal minimum temperature. The sensitivity of the NBL to radiative forcing is approximately 4 times higher compared to the daytime boundary layer. Nighttime warming or cooling may occur depending on the nature of diurnal variations in aerosol optical depth. Soil moisture also modulates the magnitude of SLWRF, decreasing from 3 to 1 W m(-2) when soil saturation increases from 37% to 70%. These results show the importance of aerosols on the radiative balance of the climate system.
C1 [Nair, Udaysankar S.; Christopher, Sundar A.; Fuller, Kirk] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35805 USA.
[McNider, Richard] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA.
[Patadia, Falguni] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Nair, US (reprint author), Univ Alabama, Ctr Earth Syst Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM nair@nsstc.uah.edu
RI Christopher, Sundar/E-6781-2011
FU DOE [DE-FG02-05ER45187]; NSF [ATM-0417774]; NASA
FX This research was supported by DOE grant DE-FG02-05ER45187 and NSF grant
ATM-0417774. Sundar Christopher was supported by NASA Radiation Sciences
Program. We would also like to thank Jonathan G. Fairman Jr. for
assistance with the preparation of the figures.
NR 51
TC 6
Z9 6
U1 4
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 22
PY 2011
VL 116
AR D02205
DI 10.1029/2010JD014068
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 710OC
UT WOS:000286520100002
ER
PT J
AU Birn, J
Nakamura, R
Panov, EV
Hesse, M
AF Birn, J.
Nakamura, R.
Panov, E. V.
Hesse, M.
TI Bursty bulk flows and dipolarization in MHD simulations of magnetotail
reconnection
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EARTH PLASMA SHEET; RAPID FLUX TRANSPORT; THIN CURRENT SHEETS;
HIGH-SPEED FLOWS; BALLOONING INSTABILITY; AURORAL STREAMERS; SUBSTORM
ONSET; 3-DIMENSIONAL RECONNECTION; MAGNETOSPHERIC SUBSTORMS; MAGNETIC
RECONNECTION
AB Using three-dimensional MHD simulations of magnetic reconnection in the magnetotail, we investigate the fate of earthward bursty bulk flows (BBFs). The flow bursts are identified as entropy-depleted magnetic flux tubes ("bubbles") generated by the severance of a plasmoid via magnetic reconnection. The onset of fast reconnection coincides closely with a drastic entropy reduction at the onset of lobe reconnection. The fact that, in the simulation, the Alfven speed does not change significantly at this time suggests that the destabilization of ballooning/interchange modes is important in driving faster reconnection as well as in providing cross-tail structure. In the initial phase, the BBFs are associated with earthward propagating dipolarization fronts. When the flow is stopped nearer to Earth, the region of dipolarization expands both azimuthally and tailward. Tailward flows are found to be associated with a rebound of the earthward flow and with reversed vortices on the outside of the flow. Earthward and tailward flows are also associated with expansion and contraction of the near plasma sheet. All of these features are consistent with recent satellite observations by Cluster and the Time History of Events and their Macroscopic Interactions during Substorms (THEMIS) mission.
C1 [Birn, J.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM 87545 USA.
[Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nakamura, R.; Panov, E. V.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
RP Birn, J (reprint author), Los Alamos Natl Lab, Space Sci & Applicat Grp, POB 1663, Los Alamos, NM 87545 USA.
EM jbirn@lanl.gov
RI Hesse, Michael/D-2031-2012; Nakamura, Rumi/I-7712-2013; NASA MMS,
Science Team/J-5393-2013
OI Nakamura, Rumi/0000-0002-2620-9211; NASA MMS, Science
Team/0000-0002-9504-5214
FU U.S. Department of Energy; NASA; SRT Programs
FX This work was performed under the auspices of the U.S. Department of
Energy, supported by NASA's MMS/SMART Theory and Modeling, Heliophysics
Theory, and SR&T Programs.
NR 69
TC 100
Z9 100
U1 2
U2 15
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 JAN 22
PY 2011
VL 116
AR A01210
DI 10.1029/2010JA016083
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 710PG
UT WOS:000286523100005
ER
PT J
AU Olgin, JG
Smith-Konter, BR
Pappalardo, RT
AF Olgin, John G.
Smith-Konter, Bridget R.
Pappalardo, Robert T.
TI Limits of Enceladus's ice shell thickness from tidally driven tiger
stripe shear failure
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LIQUID WATER; SOUTH-POLE; RESERVOIR; FRICTION; EUROPA; ORIGIN; OCEAN;
PLUME
AB Enceladus's south polar thermal anomaly and water-rich plumes suggest the existence of a subsurface ocean, which is overlain by an ice shell of uncertain thickness. Our objective is to constrain Enceladus's ice shell thickness, through assessment of tidally driven Coulomb failure of Enceladus's tiger stripe faults. We find that thin to moderate ice shell thicknesses (<40 km) support shear failure along the tiger stripes, assuming low ice coefficients of friction (0.1-0.3) and shallow fault depths (<3 km). These results are marginally consistent with the minimum ice shell thickness which can permit convection within Enceladus's ice shell. A plausible scenario is one in which the heat loss and tectonic style of Enceladus has changed through time, with convection initiating in a thick ice shell, and tiger stripe activity commencing as the ice shell thinned. Citation: Olgin, J. G., B. R. Smith-Konter, and R. T. Pappalardo (2011), Limits of Enceladus's ice shell thickness from tidally driven tiger stripe shear failure, Geophys. Res. Lett., 38, L02201, doi: 10.1029/2010GL044950.
C1 [Olgin, John G.; Smith-Konter, Bridget R.] Univ Texas El Paso, Dept Geol Sci, El Paso, TX 79968 USA.
[Pappalardo, Robert T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Olgin, JG (reprint author), Univ Texas El Paso, Dept Geol Sci, 500 W Univ Ave, El Paso, TX 79968 USA.
RI Smith-Konter, Bridget/D-2823-2011
OI Smith-Konter, Bridget/0000-0001-6004-1005
FU NASA [NNG06GF44G]
FX This research was supported by the NASA Outer Planets Research Program
(NNG06GF44G). The portion of this work performed by RTP was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with NASA. We thank Simon Kattenhorn, Francis Nimmo,
and an anonymous reviewer for their help with improving this manuscript.
NR 28
TC 11
Z9 11
U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 21
PY 2011
VL 38
AR L02201
DI 10.1029/2010GL044950
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 710MY
UT WOS:000286517100001
ER
PT J
AU Chiacchio, M
Ewen, T
Wild, M
Chin, MA
Diehl, T
AF Chiacchio, Marc
Ewen, Tracy
Wild, Martin
Chin, Mian
Diehl, Thomas
TI Decadal variability of aerosol optical depth in Europe and its
relationship to the temporal shift of the North Atlantic Oscillation in
the realm of dimming and brightening
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SURFACE SOLAR-RADIATION; CLIMATE; TRENDS; MODEL; IMPACT; FUTURE;
TEMPERATURE; REDUCTION; SATELLITE; ENERGY
AB Long-term aerosol optical depth (AOD) over Europe was analyzed from the Goddard Chemistry Aerosol Radiation and Transport (GOCART) model from 1979-2007. In particular, we studied the decadal sulfate AOD variability caused by large sulfur emissions from anthropogenic sources in Europe with a peak in 1988-1989. Simulated annual means from 1985-2007 over the continent showed statistically significant declines of 69% and a maximum of 75% in eastern Europe. Seasonally, greatest variations occurred during winter and spring followed by summer and autumn. The decrease in AOD agrees with the increase in the annual, spring, and summer mean solar radiation in Europe after the mid-1980s as well as surface-based AOD measurements. However, the long-term AOD variability does not explain the trends found in solar radiation during winter and autumn, which may be due to the contribution from the North Atlantic Oscillation (NAO) and associated cloud cover. We also investigated a possible link between sulfate AOD and NAO and found a statistically significant correlation of -0.77 in winter for Europe. Wavelet coherence analysis revealed a strong and significant antiphase relationship around 1 year that was most pronounced in the late 1980s. Cross-correlation analysis showed a seasonal dependence of sulfate AOD and NAO with negative correlation during winter and positive during summer. This analysis may help explain the seasonal decadal variability of surface solar radiation and whether sulfate aerosols have contributed to the large positive trend of the NAO during the 1980s. However, the cause and effect relationship between sulfate aerosols and NAO remains unclear.
C1 [Chiacchio, Marc; Ewen, Tracy; Wild, Martin] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland.
[Chin, Mian; Diehl, Thomas] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ewen, Tracy] Univ Zurich, Dept Geog, Zurich, Switzerland.
RP Chiacchio, M (reprint author), ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland.
EM marc.chiacchio@env.ethz.ch
RI Wild, Martin/J-8977-2012; Chin, Mian/J-8354-2012
FU National Centre of Competence in Climate Research (NCCR Climate), Swiss
National Science Foundation
FX The authors would like to express their gratitude to Christoph Schar and
Atsumu Ohmura for their support. We thank Doris Folini for her
assistance. We thank the reviewers for their helpful comments and
suggestions to improve this paper. Wavelet analysis was performed from a
MatLab software package at
http://www.pol.ac.uk/home/research/waveletcoherence/. This research is
financially supported by the National Centre of Competence in Climate
Research (NCCR Climate) sponsored by the Swiss National Science
Foundation.
NR 65
TC 10
Z9 10
U1 1
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 21
PY 2011
VL 116
AR D02108
DI 10.1029/2010JD014471
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 710NX
UT WOS:000286519600003
ER
PT J
AU Desai, TG
Lawson, JW
Keblinski, P
AF Desai, Tapan G.
Lawson, John W.
Keblinski, Pawel
TI Modeling initial stage of phenolic pyrolysis: Graphitic precursor
formation and interfacial effects
SO POLYMER
LA English
DT Article
DE Reactive molecular dynamics simulation; Polymer pyrolysis; Carbonization
ID REACTIVE FORCE-FIELD; THERMAL-DECOMPOSITION; MOLECULAR-DYNAMICS; REAXFF;
RESIN; COMPOSITES; SIMULATION
AB Reactive molecular dynamics simulations are used to study the initial stage of pyrolysis of phenolic polymers with carbon nanotube and carbon fiber. The products formed are characterized and water is found to be the primary product in all cases. The water formation mechanisms are analyzed and the value of the activation energy for water formation is estimated. A detailed study of graphitic precursor formation reveals the presence of two temperature zones. In the lower temperature zone (<2000 K) polymerization occurs resulting in the formation of large, stable graphitic precursors, while in the high temperature zone (>2000 K) polymer scission results in formation of short polymer chains/molecules. Simulations performed in the high temperature zone of the phenolic resin (with carbon nanotubes and carbon fibers) show that the presence of interfaces does not have a substantial effect on the chain scission rate or the activation energy value for water formation. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Desai, Tapan G.] Adv Cooling Technol Inc, Lancaster, PA 17601 USA.
[Lawson, John W.] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
[Keblinski, Pawel] Rensselaer Polytech Inst, Dept Mat Sci & Engn, Troy, NY 12180 USA.
RP Desai, TG (reprint author), Adv Cooling Technol Inc, Lancaster, PA 17601 USA.
EM tapandesai06@gmail.com
FU NASA [NNX10CC69P]
FX The work was supported by the NASA Small Business Innovation Research
Grant (SBIR), under Contract No. NNX10CC69P. We thank Dr. Howard
Pearlman from Advanced Cooling Technologies, Inc. for his input during
the project.
NR 17
TC 29
Z9 29
U1 5
U2 55
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0032-3861
J9 POLYMER
JI Polymer
PD JAN 21
PY 2011
VL 52
IS 2
BP 577
EP 585
DI 10.1016/j.polymer.2010.11.018
PG 9
WC Polymer Science
SC Polymer Science
GA 709ZM
UT WOS:000286480100044
ER
PT J
AU Favata, M
AF Favata, Marc
TI Conservative corrections to the innermost stable circular orbit (ISCO)
of a Kerr black hole: A new gauge-invariant post-Newtonian ISCO
condition, and the ISCO shift due to test-particle spin and the
gravitational self-force
SO PHYSICAL REVIEW D
LA English
DT Article
ID COALESCING BINARY-SYSTEMS; INSPIRALING COMPACT BINARIES;
GENERAL-RELATIVITY; EXTENDED BODIES; DYNAMICS; MOTION; WAVES; EQUATIONS;
OBJECTS; ORDER
AB The innermost stable circular orbit (ISCO) delimits the transition from circular orbits to those that plunge into a black hole. In the test-mass limit, well-defined ISCO conditions exist for the Kerr and Schwarzschild spacetimes. In the finite-mass case, there are a large variety of ways to define an ISCO in a post-Newtonian (PN) context. Here I generalize the gauge-invariant ISCO condition of Blanchet and Iyer [Classical Quantum Gravity 20, 755 (2003)] to the case of spinning (nonprecessing) binaries. The Blanchet-Iyer ISCO condition has two desirable and unexpected properties: (1) it exactly reproduces the Schwarzschild ISCO in the test-mass limit, and (2) it accurately approximates the recently calculated shift in the Schwarzschild ISCO frequency due to the conservative-piece of the gravitational self-force [L. Barack and N. Sago, Phys. Rev. Lett. 102, 191101 (2009)]. The generalization of this ISCO condition to spinning binaries has the property that it also exactly reproduces the Kerr ISCO in the test-mass limit (up to the order at which PN spin corrections are currently known). The shift in the ISCO due to the spin of the test-particle is also calculated. Remarkably, the gauge-invariant PN ISCO condition exactly reproduces the ISCO shift predicted by the Papapetrou equations for a fully relativistic spinning particle. It is surprising that an analysis of the stability of the standard PN equations of motion is able (without any form of "resummation'') to accurately describe strong-field effects of the Kerr spacetime. The ISCO frequency shift due to the conservative self-force in Kerr is also calculated from this new ISCO condition, as well as from the effective-one-body Hamiltonian of Barausse and Buonanno [Phys. Rev. D 81, 084024 (2010)]. These results serve as a useful point of comparison for future gravitational self-force calculations in the Kerr spacetime.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Favata, Marc] CALTECH, Pasadena, CA 91125 USA.
RP Favata, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM favata@tapir.caltech.edu
FU NASA
FX I gratefully acknowledge Luc Blanchet and Alessandra Buonanno for their
helpful comments on this manuscript. For several useful discussions I
also thank the members of the relativity groups at JPL and Caltech, as
well as the participants of a Perimeter Institute conference in June
2010. This research was supported through an appointment to the NASA
Postdoctoral Program at the Jet Propulsion Laboratory, administered by
Oak Ridge Associated Universities through a contract with NASA.
NR 71
TC 29
Z9 29
U1 0
U2 2
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 21
PY 2011
VL 83
IS 2
AR 024028
DI 10.1103/PhysRevD.83.024028
PG 17
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 714IR
UT WOS:000286803700003
ER
PT J
AU Favata, M
AF Favata, Marc
TI Conservative self-force correction to the innermost stable circular
orbit: Comparison with multiple post-Newtonian-based methods
SO PHYSICAL REVIEW D
LA English
DT Article
ID COALESCING BINARY-SYSTEMS; BLACK-HOLE ABSORPTION; GRAVITATIONAL-WAVES;
GENERAL-RELATIVITY; COMPACT BINARIES; EXTENDED BODIES; RADIATION;
DYNAMICS; PARTICLE; EXPANSION
AB Barack and Sago [Phys. Rev. Lett. 102, 191101 (2009)] have recently computed the shift of the innermost stable circular orbit (ISCO) of the Schwarzschild spacetime due to the conservative self-force that arises from the finite-mass of an orbiting test-particle. This calculation of the ISCO shift is one of the first concrete results of the self-force program, and provides an exact (fully relativistic) point of comparison with approximate post-Newtonian (PN) computations of the ISCO. Here this exact ISCO shift is compared with nearly all known PN-based methods. These include both "nonresummed'' and "resummed'' approaches (the latter reproduce the test-particle limit by construction). The best agreement with the exact (Barack-Sago) result is found when the pseudo-4PN coefficient of the effective-one-body (EOB) metric is fit to numerical relativity simulations. However, if one considers uncalibrated methods based only on the currently known 3PN-order conservative dynamics, the best agreement is found from the gauge-invariant ISCO condition of Blanchet and Iyer [Classical Quantum Gravity 20, 755 (2003)], which relies only on the (nonresummed) 3PN equations of motion. This method reproduces the exact test-particle limit without any resummation. A comparison of PN methods with the ISCO in the equal-mass case (computed via sequences of numerical relativity initial-data sets) is also performed. Here a (different) nonresummed method also performs very well (as was previously shown). These results suggest that the EOB approach-while exactly incorporating the conservative test-particle dynamics and having several other important advantages-does not (in the absence of calibration) incorporate conservative self-force effects more accurately than standard PN methods. I also consider how the conservative self-force ISCO shift, combined in some cases with numerical relativity computations of the ISCO, can be used to constrain our knowledge of (1) the EOB effective metric, (2) phenomenological inspiral-merger-ringdown templates, and (3) 4PN- and 5PN-order terms in the PN orbital energy. These constraints could help in constructing better gravitational-wave templates. Lastly, I suggest a new method to calibrate unknown PN terms in inspiral templates using numerical-relativity calculations.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Favata, Marc] CALTECH, Pasadena, CA 91125 USA.
RP Favata, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM favata@tapir.caltech.edu
FU NASA
FX This research was supported through an appointment to the NASA
Postdoctoral Program at the Jet Propulsion Laboratory, administered by
Oak Ridge Associated Universities through a contract with NASA. I
gratefully acknowledge Emanuele Berti, Luc Blanchet, Alessandra
Buonanno, and Alexandre Le Tiec for detailed comments on this
manuscript. For helpful discussions I thank Parameswaran Ajith, Curt
Cutler, Harald Pfeiffer, Mark Scheel, Michele Vallisneri, Bernard
Whiting, and participants at a Perimeter Institute conference in June
2010. I also thank the anonymous referee for helpful comments that
improved this manuscript.
NR 149
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U1 0
U2 1
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 21
PY 2011
VL 83
IS 2
AR 024027
DI 10.1103/PhysRevD.83.024027
PG 26
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 714IR
UT WOS:000286803700002
ER
PT J
AU Kahler, SW
Krucker, S
Szabo, A
AF Kahler, S. W.
Krucker, S.
Szabo, A.
TI Solar energetic electron probes of magnetic cloud field line lengths
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTIONS; FLUX-ROPE GEOMETRY; WIND; TOPOLOGY; PARAMETERS;
SIGNATURES; EVENTS; STEREO; PARTICLES; HELICITY
AB Magnetic clouds (MCs) are large interplanetary coronal mass ejections of enhanced and low-variance fields with rotations indicative of magnetic flux ropes originally connected to the Sun. The MC flux rope models require field lines with larger pitch angles and longer lengths with increasing distance from the MC axis. While the models can provide good fits to the in situ solar wind observations, there have not been definitive observational tests of the global magnetic field geometry, particularly for the field line lengths. However, impulsive solar energetic (E > 10 keV) electron events occasionally occur within an MC, and the electron onsets can be used to infer Le, the magnetic field line lengths traveled by the electrons from the Sun to the points in the MC where the electron onsets occur. We selected 8 MCs in and near which 30 solar electron events were observed by the 3DP instrument on the Wind spacecraft. We compared the corresponding Le values with calculated model field line lengths to test two MC models. Some limitations on the technique are imposed by variations of the models and uncertainly about MC boundary locations. We found generally poor correlations between the computed electron path lengths and the model field line lengths. Only one value of Le inside an MC, that of 18 October 1995, exceeded 3.2 AU, indicating an absence of the long path lengths expected in the highly wound outer regions of MC models. We briefly consider the implications for MC models.
C1 [Kahler, S. W.] USAF, Space Vehicles Directorate, Res Lab, 29 Randolph Rd, Hanscom AFB, MA 01731 USA.
[Krucker, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Szabo, A.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
RP Kahler, SW (reprint author), USAF, Space Vehicles Directorate, Res Lab, 29 Randolph Rd, Hanscom AFB, MA 01731 USA.
EM AFRL.RVB.PA@hanscom.af.mil
FU NASA [NNG 05GH18G]; AFOSR work unit [2301RDZ4]
FX We acknowledge the Wind MFI and 3DP instrument teams for the use of
their data. The work at UC Berkeley was supported through NASA grant NNG
05GH18G for Wind. The work at AFRL was supported by AFOSR work unit
2301RDZ4. The work benefited considerably from comments of the reviewers
and of colleagues at Caltech.
NR 52
TC 22
Z9 22
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JAN 21
PY 2011
VL 116
AR A01104
DI 10.1029/2010JA015328
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 710PE
UT WOS:000286522900001
ER
PT J
AU Weber, RC
Lin, PY
Garnero, EJ
Williams, Q
Lognonne, P
AF Weber, Renee C.
Lin, Pei-Ying
Garnero, Edward J.
Williams, Quentin
Lognonne, Philippe
TI Seismic Detection of the Lunar Core
SO SCIENCE
LA English
DT Article
ID MELTING RELATIONS; PLANETARY BODIES; METALLIC CORES; HIGH-PRESSURE;
PROSPECTOR; MANTLE; MOON; CONSTRAINTS; EVOLUTION; STATE
AB Despite recent insight regarding the history and current state of the Moon from satellite sensing and analyses of limited Apollo-era seismic data, deficiencies remain in our understanding of the deep lunar interior. We reanalyzed Apollo lunar seismograms using array-processing methods to search for the presence of reflected and converted seismic energy from the core. Our results suggest the presence of a solid inner and fluid outer core, overlain by a partially molten boundary layer. The relative sizes of the inner and outer core suggest that the core is similar to 60% liquid by volume. Based on phase diagrams of iron alloys and the presence of partial melt, the core probably contains less than 6 weight % of lighter alloying components, which is consistent with a volatile-depleted interior.
C1 [Weber, Renee C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Lin, Pei-Ying; Garnero, Edward J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Williams, Quentin] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Lognonne, Philippe] Univ Paris Diderot, Inst Phys Globe, Sorbonne Paris Cite, St Maur Des Fosses, France.
RP Weber, RC (reprint author), NASA, George C Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM renee.c.weber@nasa.gov
RI Lognonne, Philippe/F-8846-2010
FU NASA [NNH09AK41I]
FX This work was funded by NASA Planetary Geology and Geophysics grant
NNH09AK41I to R.C.W. The authors thank four reviewers, and Y. Nakamura
for helpful comments and discussions.
NR 29
TC 146
Z9 150
U1 7
U2 47
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD JAN 21
PY 2011
VL 331
IS 6015
BP 309
EP 312
DI 10.1126/science.1199375
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 712BF
UT WOS:000286636300030
PM 21212323
ER
PT J
AU Beerer, IM
Knutson, HA
Burrows, A
Fortney, JJ
Agol, E
Charbonneau, D
Cowan, NB
Deming, D
Desert, JM
Langton, J
Laughlin, G
Lewis, NK
Showman, AP
AF Beerer, Ingrid M.
Knutson, Heather A.
Burrows, Adam
Fortney, Jonathan J.
Agol, Eric
Charbonneau, David
Cowan, Nicolas B.
Deming, Drake
Desert, Jean-Michel
Langton, Jonathan
Laughlin, Gregory
Lewis, Nikole K.
Showman, Adam P.
TI SECONDARY ECLIPSE PHOTOMETRY OF WASP-4b WITH WARM SPITZER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; stars: individual (WASP-4b); techniques:
photometric
ID INFRARED-EMISSION SPECTRUM; PLANET HD 189733B; TRANSITING GIANT PLANETS;
GROUND-BASED DETECTION; THERMAL EMISSION; EXTRASOLAR PLANET; HOT
JUPITERS; TEMPERATURE INVERSION; MODEL ATMOSPHERES; BAND EMISSION
AB We present photometry of the giant extrasolar planet WASP-4b at 3.6 and 4.5 mu m taken with the Infrared Array Camera on board the Spitzer Space Telescope as part of Spitzer's extended warm mission. We find secondary eclipse depths of 0.319% +/- 0.031% and 0.343% +/- 0.027% for the 3.6 and 4.5 mu m bands, respectively, and show model emission spectra and pressure-temperature profiles for the planetary atmosphere. These eclipse depths are well fit by model emission spectra with water and other molecules in absorption, similar to those used for TrES-3 and HD 189733b. Depending on our choice of model, these results indicate that this planet has either a weak dayside temperature inversion or no inversion at all. The absence of a strong thermal inversion on this highly irradiated planet is contrary to the idea that highly irradiated planets are expected to have inversions, perhaps due the presence of an unknown absorber in the upper atmosphere. This result might be explained by the modestly enhanced activity level of WASP-4b's G7V host star, which could increase the amount of UV flux received by the planet, therefore reducing the abundance of the unknown stratospheric absorber in the planetary atmosphere as suggested in Knutson et al. We also find no evidence for an offset in the timing of the secondary eclipse and place a 2 sigma upper limit on vertical bar e cos omega vertical bar of 0.0024, which constrains the range of tidal heating models that could explain this planet's inflated radius.
C1 [Beerer, Ingrid M.; Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Fortney, Jonathan J.; Laughlin, Gregory] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Agol, Eric; Cowan, Nicolas B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Charbonneau, David; Desert, Jean-Michel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.
[Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA.
[Lewis, Nikole K.; Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Beerer, IM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
RI Agol, Eric/B-8775-2013;
OI Agol, Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354;
Charbonneau, David/0000-0002-9003-484X
FU NASA; Miller Institute for Basic Research Science; NSF [0645416]
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. Support
for this work was provided by NASA. Heather A. Knutson is supported by a
fellowship from the Miller Institute for Basic Research Science. Eric
Agol acknowledges the support of NSF CAREER grant No. 0645416.
NR 60
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U1 2
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 23
DI 10.1088/0004-637X/727/1/23
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000023
ER
PT J
AU Bodaghee, A
Tomsick, JA
Rodriguez, J
Chaty, S
Pottschmidt, K
Walter, R
Romano, P
AF Bodaghee, A.
Tomsick, J. A.
Rodriguez, J.
Chaty, S.
Pottschmidt, K.
Walter, R.
Romano, P.
TI SUZAKU OBSERVES WEAK FLARES FROM IGR J17391-3021 REPRESENTING A COMMON
LOW-ACTIVITY STATE IN THIS SUPERGIANT FAST X-RAY TRANSIENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; gamma rays: general; stars: neutron;
supergiants; X-rays: binaries; X-rays: individual (IGR J17391-3021=XTE
J1739-302)
ID GALACTIC-CENTER REGION; XTE J1739-302; MULTIWAVELENGTH OBSERVATIONS;
INTEGRAL OBSERVATIONS; INTERSTELLAR-MEDIUM; COMPANION STAR;
NEUTRON-STAR; BINARIES; J17544-2619; ACCRETION
AB We present an analysis of a 37 ks observation of the supergiant fast X-ray transient IGR J17391-3021 (= XTE J1739-302) gathered with Suzaku. The source evolved from quiescence to a low-activity level culminating in three weak flares lasting similar to 3 ks each in which the peak luminosity is only a factor of five times that of the pre-flare luminosity. The minimum observed luminosity was 1.3 x 10(33) erg s(-1)(d/2.7 kpc)(2) in the 0.5-10 keV range. The weak flares are accompanied by significant changes in the spectral parameters including a column density (N-H = (4.1(-0.5)(+0.4)) x 10(22) cm(-2)) that is similar to 2-9 times the absorption measured during quiescence. Accretion of obscuring clumps of stellar wind material can explain both the small flares and the increase in N-H. Placing this observation in the context of the recent Swift monitoring campaign, we find that weak-flaring episodes, or at least epochs of enhanced activity just above the quiescent level but well below the moderately bright or high-luminosity outbursts, represent more than 60% +/- 5% of all observations in the 0.5-10 keV energy range making this the most common state in the emission behavior of IGR J17391-3021.
C1 [Bodaghee, A.; Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Rodriguez, J.; Chaty, S.] Univ Paris Diderot, Lab AIM, CEA IRFU,CNRS INSU, CEA DSM IRFU SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Walter, R.] Univ Geneva, INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Walter, R.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland.
[Romano, P.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy.
RP Bodaghee, A (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM bodaghee@ssl.berkeley.edu
RI XRAY, SUZAKU/A-1808-2009;
OI Rodriguez, Jerome/0000-0002-4151-4468; Chaty,
Sylvain/0000-0002-5769-8601
FU Suzaku Guest Observer Grant [NNX08AB88G]; Chandra Grant [G089055X]
FX The authors thank the anonymous referee whose revision of the draft led
to significant improvements in the quality of the manuscript. A.B. and
J.T. acknowledge Suzaku Guest Observer Grant NNX08AB88G and Chandra
Grant G089055X. 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; the SIMBAD database
operated at CDS, Strasbourg, France; NASA's Astrophysics Data System
Bibliographic Services.
NR 50
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 59
DI 10.1088/0004-637X/727/1/59
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000059
ER
PT J
AU Fox, OD
Chevalier, RA
Dwek, E
Skrutskie, MF
Sugerman, BEK
Leisenring, JM
AF Fox, Ori D.
Chevalier, Roger A.
Dwek, Eli
Skrutskie, Michael F.
Sugerman, Ben E. K.
Leisenring, Jarron M.
TI DISENTANGLING THE ORIGIN AND HEATING MECHANISM OF SUPERNOVA DUST:
LATE-TIME SPITZER SPECTROSCOPY OF THE TYPE IIn SN 2005ip (vol 725, pg
1768, 2010)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Fox, Ori D.; Chevalier, Roger A.; Skrutskie, Michael F.; Leisenring, Jarron M.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Fox, Ori D.; Dwek, Eli] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sugerman, Ben E. K.] Goucher Coll, Dept Phys & Astron, Baltimore, MD 21204 USA.
RP Fox, OD (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
EM ofox@virginia.edu
RI Dwek, Eli/C-3995-2012
NR 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 JAN 20
PY 2011
VL 727
IS 1
AR 61
DI 10.1088/0004-637X/727/1/61
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000061
ER
PT J
AU Gilbert, H
Kilper, G
Alexander, D
Kucera, T
AF Gilbert, Holly
Kilper, Gary
Alexander, David
Kucera, Therese
TI COMPARING SPATIAL DISTRIBUTIONS OF SOLAR PROMINENCE MASS DERIVED FROM
CORONAL ABSORPTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: abundances; Sun: chromosphere; Sun: filaments, prominences
ID GROUND-BASED OBSERVATIONS; TRANSITION REGION; NEUTRAL HYDROGEN;
ACTIVE-REGION; H-ALPHA; SOHO; FILAMENTS; TRACE; EXPLORER; FEATURES
AB In a previous study, Gilbert et al. derived the column density and total mass of solar prominences using a new technique, which measures how much coronal radiation in the Fe XII (195 angstrom) spectral band is absorbed by prominence material, while considering the effects of both foreground and background radiation. In the present work, we apply this method to a sample of prominence observations in three different wavelength regimes: one in which only H(0) is ionized (504 angstrom < lambda < 911 angstrom), a second where both H(0) and He(0) are ionized (228 angstrom < lambda < 504 angstrom), and finally at wavelengths where H(0), He(0), and He(+) are all ionized (lambda < 228 angstrom). This approach, first suggested by Kucera et al., permits the separation of the contributions of neutral hydrogen and helium to the total column density in prominences. Additionally, an enhancement of the technique allowed the calculation of the two-dimensional (2D) spatial distribution of the column density from the continuum absorption in each extreme-ultraviolet observation. We find the total prominence mass is consistently lower in the 625 angstrom observations compared to lines in the other wavelength regimes. There is a significant difference in total mass between the 625 angstrom and 195 angstrom lines, indicating the much higher opacity at 625 angstrom is causing a saturation of the continuum absorption and thus, a potentially large underestimation of mass.
C1 [Gilbert, Holly; Kilper, Gary; Kucera, Therese] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Alexander, David] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
RP Gilbert, H (reprint author), NASA, Goddard Space Flight Ctr, Code 670, Greenbelt, MD 20771 USA.
EM holly.r.gilbert@nasa.gov
RI Gilbert, Holly/C-7215-2012; Kucera, Therese/C-9558-2012;
OI Kucera, Therese/0000-0001-9632-447X
FU NASA [NNX07AI10G]
FX We thank Joe Gurman for sharing his knowledge of the EIT observations
and his help in revising the manuscript, and Petr Heinzel and Nicolas
Labrosse for their insightful comments and help with understanding the
saturation issues. We also thank Tom Holzer for helping make sure the
derivation in Appendix A is correct. This work was partially supported
by NASA grant NNX07AI10G. SOHO is a mission of international cooperation
between ESA and NASA.
NR 23
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PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 25
DI 10.1088/0004-637X/727/1/25
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000025
ER
PT J
AU Kilcik, A
Yurchyshyn, VB
Abramenko, V
Goode, PR
Gopalswamy, N
Ozguc, A
Rozelot, JP
AF Kilcik, A.
Yurchyshyn, V. B.
Abramenko, V.
Goode, P. R.
Gopalswamy, N.
Ozguc, A.
Rozelot, J. P.
TI MAXIMUM CORONAL MASS EJECTION SPEED AS AN INDICATOR OF SOLAR AND
GEOMAGNETIC ACTIVITIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; solar-terrestrial relations; Sun: activity; Sun:
coronal mass ejections (CMEs)
ID MAGNETIC CLOUDS; CYCLE; SOLAR-CYCLE-23; MINIMUM; RECONSTRUCTION;
SUNSPOTS; INDEXES; EVENTS; STORMS; SHOCK
AB We investigate the relationship between the monthly averaged maximal speeds of coronal mass ejections (CMEs), international sunspot number (ISSN), and the geomagnetic Dst and Ap indices covering the 1996-2008 time interval (solar cycle 23). Our new findings are as follows. (1) There is a noteworthy relationship between monthly averaged maximum CME speeds and sunspot numbers, Ap and Dst indices. Various peculiarities in the monthly Dst index are correlated better with the fine structures in the CME speed profile than that in the ISSN data. (2) Unlike the sunspot numbers, the CME speed index does not exhibit a double peak maximum. Instead, the CME speed profile peaks during the declining phase of solar cycle 23. Similar to the Ap index, both CME speed and the Dst indices lag behind the sunspot numbers by several months. (3) The CME number shows a double peak similar to that seen in the sunspot numbers. The CME occurrence rate remained very high even near the minimum of the solar cycle 23, when both the sunspot number and the CME average maximum speed were reaching their minimum values. (4) A well-defined peak of the Ap index between 2002 May and 2004 August was co-temporal with the excess of the mid-latitude coronal holes during solar cycle 23. The above findings suggest that the CME speed index may be a useful indicator of both solar and geomagnetic activities. It may have advantages over the sunspot numbers, because it better reflects the intensity of Earth-directed solar eruptions.
C1 [Kilcik, A.; Yurchyshyn, V. B.; Abramenko, V.; Goode, P. R.] Big Bear Solar Observ, Big Bear City, CA 92314 USA.
[Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ozguc, A.] Bogazici Univ, Kandilli Observ, TR-34684 Istanbul, Turkey.
[Ozguc, A.] Bogazici Univ, Earthquake Res Inst, TR-34684 Istanbul, Turkey.
[Rozelot, J. P.] Univ Nice, OCA Fizeau Dpt, F-06130 Grasse, France.
RP Kilcik, A (reprint author), Big Bear Solar Observ, Big Bear City, CA 92314 USA.
RI Gopalswamy, Nat/D-3659-2012; Kilcik, Ali/C-5452-2016
OI Kilcik, Ali/0000-0002-0094-1762
FU NASA [GI NNX08AJ20G, LWS NNX08AQ89G]; NSF [ATM0716512]
FX We thank the referees for their valuable comments and suggestions, which
led to a significant improvement of the paper. We acknowledge usage of
ISSN and Ap index from the National Geophysical Data Center. The Dst
index data were provided by the World Data Center for Geomagnetism at
Kyoto University. The CME catalog is generated and maintained by the
Center for Solar Physics and Space Weather, 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. We thank
W. Cao for help during the manuscript preparation. This research was
supported by NASA grants GI NNX08AJ20G and LWS NNX08AQ89G as well as NSF
ATM0716512 grant.
NR 48
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U1 0
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 44
DI 10.1088/0004-637X/727/1/44
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000044
ER
PT J
AU Laurent, P
Titarchuk, L
AF Laurent, Philippe
Titarchuk, Lev
TI SPECTRAL INDEX AS A FUNCTION OF MASS ACCRETION RATE IN BLACK HOLE
SOURCES: MONTE CARLO SIMULATIONS AND AN ANALYTICAL DESCRIPTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; radiation mechanisms:
non-thermal; X-rays: general
ID OSCILLATION FREQUENCY CORRELATION; X-RAY BINARIES; NEUTRON-STAR;
OBSERVATIONAL EVIDENCE; INTRINSIC SIGNATURE; POWER-LAW; COMPTONIZATION;
VARIABILITY; CYGNUS-X-1; STATES
AB We present herein a theoretical study of correlations between spectral indexes of X-ray emergent spectra and mass accretion rate (m) over dot in black hole (BH) sources, which provide a definitive signature for BHs. It has been firmly established, using the Rossi X-ray Timing Explorer (RXTE) in numerous BH observations during hard-soft state spectral evolution, that the photon index of X-ray spectra increases when (m) over dot increases and, moreover, the index saturates at high values of (m) over dot. In this paper, we present theoretical arguments that the observationally established index saturation effect versus mass accretion rate is a signature of the bulk (converging) flow onto the BH. Also, we demonstrate that the index saturation value depends on the plasma temperature of converging flow. We self-consistently calculate the Compton cloud (CC) plasma temperature as a function of mass accretion rate using the energy balance between energy dissipation and Compton cooling. We explain the observable phenomenon, index-(m) over dot correlations using a Monte Carlo simulation of radiative processes in the innermost part (CC) of a BH source and we account for the Comptonization processes in the presence of thermal and bulk motions, as basic types of plasma motion. We show that, when (m) over dot increases, BH sources evolve to high and very soft states (HSS and VSS, respectively), in which the strong blackbody(BB)-like and steep power-law components are formed in the resulting X-ray spectrum. The simultaneous detections of these two components strongly depends on sensitivity of high-energy instruments, given that the relative contribution of the hard power-law tail in the resulting VSS spectrum can be very low, which is why, to date RXTE observations of the VSS X-ray spectrum have been characterized by the presence of the strong BB-like component only. We also predict specific patterns for high-energy e-fold (cutoff) energy (E(fold)) evolution with m. for thermal and dynamical (bulk) Comptonization cases. For the former case, E(fold) monotonically decreases with (m) over dot, in the latter case, the E(fold) decrease is followed by its increase at high values of (m) over dot. The observational evolution of E(fold) versus m. can be another test for the presence of a converging flow effect in the formation of the resulting spectra in the close vicinity of BHs.
C1 [Laurent, Philippe] CEA Saclay, CEA DSM IRFU APC, F-91191 Gif Sur Yvette, France.
[Titarchuk, Lev] Univ Ferrara, Dept Phys, I-44100 Ferrara, Italy.
[Titarchuk, Lev] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20770 USA.
[Titarchuk, Lev] George Mason Univ, Dept Computat & Data Sci, Fairfax, VA 22030 USA.
RP Laurent, P (reprint author), CEA Saclay, CEA DSM IRFU APC, F-91191 Gif Sur Yvette, France.
EM plaurent@cea.fr; titarchuk@fe.infn.fe
RI laurent, philippe/E-6211-2013
NR 32
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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 JAN 20
PY 2011
VL 727
IS 1
AR 34
DI 10.1088/0004-637X/727/1/34
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000034
ER
PT J
AU Melnick, GJ
Tolls, V
Snell, RL
Bergin, EA
Hollenbach, DJ
Kaufman, MJ
Li, D
Neufeld, DA
AF Melnick, Gary J.
Tolls, Volker
Snell, Ronald L.
Bergin, Edwin A.
Hollenbach, David J.
Kaufman, Michael J.
Li, Di
Neufeld, David A.
TI DISTRIBUTION OF WATER VAPOR IN MOLECULAR CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: clouds; ISM: molecules; radio
lines: ISM
ID WAVE-ASTRONOMY-SATELLITE; DENSE INTERSTELLAR CLOUDS; C-12/C-13 ISOTOPE
RATIO; SPITZER-SPACE-TELESCOPE; MASS STAR-FORMATION; CHEMICAL-MODELS;
DARK CLOUD; IC 5146; ORION; EMISSION
AB We report the results of a large-area study of water vapor along the Orion Molecular Cloud ridge, the purpose of which was to determine the depth-dependent distribution of gas-phase water in dense molecular clouds. We find that the water vapor measured toward 77 spatial positions along the face-on Orion ridge, excluding positions surrounding the outflow associated with BN/KL and IRc2, display integrated intensities that correlate strongly with known cloud surface tracers such as CN, C2H, (CO)-C-13 J = 5-4, and HCN, and less well with the volume tracer N2H+. Moreover, at total column densities corresponding to A(V) < 15 mag, the ratio of H2O to (CO)-O-18 integrated intensities shows a clear rise approaching the cloud surface. We show that this behavior cannot be accounted for by either optical depth or excitation effects, but suggests that gas-phase water abundances fall at large AV. These results are important as they affect measures of the true water-vapor abundance in molecular clouds by highlighting the limitations of comparing measured water-vapor column densities with such traditional cloud tracers as (CO)-C-13 or (CO)-O-18. These results also support cloud models that incorporate freeze out of molecules as a critical component in determining the depth-dependent abundance of water vapor.
C1 [Melnick, Gary J.; Tolls, Volker] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Snell, Ronald L.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Hollenbach, David J.] SETI Inst, Mountain View, CA 94043 USA.
[Kaufman, Michael J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Li, Di] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Melnick, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM gmelnick@cfa.harvard.edu; vtolls@cfa.harvard.edu; snell@astro.umass.edu;
ebergin@umich.edu; dhollenbach@seti.org; mkaufman@email.sjsu.edu;
dili@jpl.nasa.gov; neufeld@pha.jhu.edu
FU Long Term Space Astrophysics (LTSA) [NNG06GB30G]; NSF [AST 08-38222]
FX G.J.M., R.L.S., E.A.B., D.J.H., and M.J.K. gratefully acknowledge the
financial support of NASA grant NNG06GB30G from the Long Term Space
Astrophysics (LTSA) Research Program. The Five College Radio Astronomy
Observatory was operated with support from the NSF through grant AST
08-38222.
NR 71
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 13
DI 10.1088/0004-637X/727/1/13
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000013
ER
PT J
AU Sandell, G
Weintraub, DA
Hamidouche, M
AF Sandell, Goeran
Weintraub, David A.
Hamidouche, Murad
TI A SUBMILLIMETER MAPPING SURVEY OF HERBIG AeBe STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; ISM: clouds; stars: formation; stars: pre-main
sequence; stars: variables: T Tauri, Herbig Ae/Be; submillimeter: stars
ID INTERMEDIATE-MASS STARS; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS;
EMISSION-LINE STARS; R-CORONAE-AUSTRALIS; FU-ORIONIS STARS; T-TAURI
STARS; SPECTRAL ENERGY-DISTRIBUTIONS; FAR-INFRARED OBSERVATIONS;
RADIO-CONTINUUM EMISSION
AB We have acquired submillimeter observations of 33 fields containing 37 Herbig Ae/Be (HAEBE) stars or potential HAEBE stars, including SCUBA maps of all but two of these stars. Nine target stars show extended dust emission. The other 18 are unresolved, suggesting that the dust envelopes or disks around these stars are less than a few arcseconds in angular size. In several cases, we find that the strongest submillimeter emission originates from younger, heavily embedded sources rather than from the HAEBE star, which means that previous models must be viewed with caution. These new data, in combination with far-infrared flux measurements available in the literature, yield spectral energy distributions (SEDs) from far-infrared to millimeter wavelengths for all the observed objects. Isothermal fits to these SEDs demonstrate excellent fits, in most cases, to the flux densities longward of 100 mu m. We find that a smaller proportion of B-type stars than A-and F-type stars are surrounded by circumstellar disks, suggesting that disks around B stars dissipate on shorter timescales than those around later spectral types. Our models also reveal that the mass of the circumstellar material and the value of beta are correlated, with low masses corresponding to low values of beta. Since low values of beta imply large grain sizes, our results suggest that a large fraction of the mass in low-beta sources is locked up in very large grains. Several of the isolated HAEBE stars have disks with very flat submillimeter SEDs. These disks may be on the verge of forming planetary systems.
C1 [Sandell, Goeran; Hamidouche, Murad] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Weintraub, David A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
RP Sandell, G (reprint author), NASA, Ames Res Ctr, SOFIA USRA, Mail Stop N211-3,Bldg N21,Rm 249, Moffett Field, CA 94035 USA.
EM Goran.H.Sandell@nasa.gov; david.a.weintraub@vanderbilt.edu;
mhamidouche@sofia.usra.edu
FU Canadian Space Agency
FX This work made extensive use of the SIMBAD Astronomical Database at the
Centre de Donnees astronomiques deStrasbourg, France, and NASA's
Astrophysics Data System Abstract Service. This research used the
facilities of the Canadian Astronomy Data Centre operated by the
National Research Council of Canada with the support of the Canadian
Space Agency. 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. We thank Meredith Hughes for giving us flux densities she observed
with the SMA and we also acknowledge useful discussions and help from
William Vacca and Bhaswati Mookerjea. Comments and suggestions by the
referee were also appreciated.
NR 243
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U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 26
DI 10.1088/0004-637X/727/1/26
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000026
ER
PT J
AU Zhu, Z
Kathuria, A
Krishna, SG
Mojarradi, M
Jalali-Farahani, B
Barnaby, H
Wu, W
Gildenblat, G
AF Zhu, Z.
Kathuria, A.
Krishna, S. G.
Mojarradi, M.
Jalali-Farahani, B.
Barnaby, H.
Wu, W.
Gildenblat, G.
TI Design applications of compact MOSFET model for extended temperature
range (60-400K)
SO ELECTRONICS LETTERS
LA English
DT Article
AB An advanced MOSFET model for the 60-400 K temperature range is developed starting with the industry standard PSP model. The new model is experimentally verified, implemented in a commonly used circuit simulator and tested for convergence. This provides a robust and accurate description of low temperature MOSFET characteristics, including analogue performance. Simulations on a switched-capacitor integrator design are performed to illustrate the capabilities of the new model and to justify a new design methodology for the extended temperature range.
C1 [Zhu, Z.; Kathuria, A.; Krishna, S. G.; Jalali-Farahani, B.; Barnaby, H.; Wu, W.; Gildenblat, G.] Arizona State Univ, Ira A Fulton Sch Engn, Tempe, AZ 85281 USA.
[Mojarradi, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zhu, Z (reprint author), Arizona State Univ, Ira A Fulton Sch Engn, Tempe, AZ 85281 USA.
EM zeqin.zhu@asu.edu
FU Jet Propulsion Lab [1340201]
FX This work is supported in part by the Jet Propulsion Lab under grant no.
1340201. We are grateful to TowerJazz for providing the test structures
used in this study. Special thanks are extended to G. Dessai for reading
the manuscript.
NR 8
TC 2
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U1 0
U2 2
PU INST ENGINEERING TECHNOLOGY-IET
PI HERTFORD
PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND
SN 0013-5194
J9 ELECTRON LETT
JI Electron. Lett.
PD JAN 20
PY 2011
VL 47
IS 2
BP 141
EP +
DI 10.1049/el.2010.3468
PG 2
WC Engineering, Electrical & Electronic
SC Engineering
GA 708OX
UT WOS:000286374600047
ER
PT J
AU Bennett, CJ
Hama, T
Kim, YS
Kawasaki, M
Kaiser, RI
AF Bennett, Chris J.
Hama, Tetsuya
Kim, Yong Seol
Kawasaki, Masahiro
Kaiser, Ralf I.
TI LABORATORY STUDIES ON THE FORMATION OF FORMIC ACID (HCOOH) IN
INTERSTELLAR AND COMETARY ICES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; comets: general; cosmic rays; infrared: ISM; ISM:
molecules; methods: laboratory; molecular processes
ID HOT MOLECULAR CORES; SOLAR-SYSTEM ICES; CARBON-MONOXIDE; WATER ICE;
SOLID CO; ORGANIC-MOLECULES; INFRARED-SPECTRA; DARK CLOUD; ABSORPTION
FEATURES; LOW-TEMPERATURES
AB Mixtures of water (H2O) and carbon monoxide (CO) ices were irradiated at 10 K with energetic electrons to simulate the energy transfer processes that occur in the track of galactic cosmic-ray particles penetrating interstellar ices. We identified formic acid (HCOOH) through new absorption bands in the infrared spectra at 1690 and 1224 cm(-1) (5.92 and 8.17 mu m, respectively). During the subsequent warm-up of the irradiated samples, formic acid is evident from the mass spectrometer signal at the mass-to-charge ratio, m/z = 46 (HCOOH+) as the ice sublimates. The detection of formic acid was confirmed using isotopically labeled water-d2 with carbon monoxide, leading to formic acid-d2 (DCOOD). The temporal fits of the reactants, reaction intermediates, and products elucidate two reaction pathways to formic acid in carbon monoxide-water ices. The reaction is induced by unimolecular decomposition of water forming atomic hydrogen (H) and the hydroxyl radical (OH). The dominating pathway to formic acid (HCOOH) was found to involve addition of suprathermal hydrogen atoms to carbon monoxide forming the formyl radical (HCO); the latter recombined with neighboring hydroxyl radicals to yield formic acid (HCOOH). To a lesser extent, hydroxyl radicals react with carbon monoxide to yield the hydroxyformyl radical (HOCO), which recombined with atomic hydrogen to produce formic acid. Similar processes are expected to produce formic acid within interstellar ices, cometary ices, and icy satellites, thus providing alternative processes for the generation of formic acid whose abundance in hot cores such as Sgr-B2 cannot be accounted for solely by gas-phase chemistry.
C1 [Bennett, Chris J.; Kim, Yong Seol; Kaiser, Ralf I.] Univ Hawaii, Dept Chem, Honolulu, HI 96822 USA.
[Bennett, Chris J.; Kaiser, Ralf I.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Hama, Tetsuya; Kawasaki, Masahiro] Kyoto Univ, Dept Mol Engn, Kyoto 6158510, Japan.
RP Kaiser, RI (reprint author), Univ Hawaii, Dept Chem, Honolulu, HI 96822 USA.
EM ralfk@hawaii.edu
RI HAMA, Tetsuya/A-9766-2012;
OI HAMA, Tetsuya/0000-0002-4991-4044; Bennett,
Christopher/0000-0002-4181-6976
FU National Aeronautics Space Administration (NASA Astrobiology Institute)
[NNA09DA77]
FX This material is based upon work supported by the National Aeronautics
Space Administration (NASA Astrobiology Institute under Cooperative
Agreement No. NNA09DA77 A issued by the Office of Space Science).
NR 91
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 27
DI 10.1088/0004-637X/727/1/27
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000027
ER
PT J
AU McIntosh, SW
Leamon, RJ
De Pontieu, B
AF McIntosh, Scott W.
Leamon, Robert J.
De Pontieu, Bart
TI THE SPECTROSCOPIC FOOTPRINT OF THE FAST SOLAR WIND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar wind; Sun: corona; Sun: surface magnetism; Sun: transition region
ID EQUATORIAL CORONAL HOLE; TRANSITION REGION; MAGNETIC-FIELDS; QUIET-SUN;
ALFVEN WAVES; SPECTRAL ATLAS; NETWORK; CHROMOSPHERE; SUMER; SPICULES
AB We analyze a large, complex equatorial coronal hole (ECH) and its immediate surroundings with a focus on the roots of the fast solar wind. We start by demonstrating that our ECH is indeed a source of the fast solar wind at 1 AU by examining in situ plasma measurements in conjunction with recently developed measures of magnetic conditions of the photosphere, inner heliosphere, and the mapping of the solar wind source region. We focus the bulk of our analysis on interpreting the thermal and spatial dependence of the non-thermal line widths in the ECH as measured by SOHO/SUMER by placing the measurements in context with recent studies of ubiquitous Alfven waves in the solar atmosphere and line profile asymmetries (indicative of episodic heating and mass loading of the coronal plasma) that originate in the strong, unipolar magnetic flux concentrations that comprise the supergranular network. The results presented in this paper are consistent with a picture where a significant portion of the energy responsible for the transport of heated mass into the fast solar wind is provided by episodically occurring small-scale events (likely driven by magnetic reconnection) in the upper chromosphere and transition region of the strong magnetic flux regions that comprise the supergranular network.
C1 [McIntosh, Scott W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Leamon, Robert J.] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA.
[De Pontieu, Bart] Lockheed Martin Solar & Astrophys Lab, Org ADBS, Palo Alto, CA 94304 USA.
RP McIntosh, SW (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA.
EM mscott@ucar.edu; robert.j.leamon@nasa.gov; bdp@lmsal.com
FU National Aeronautics and Space Administration [NNX08AU30G, NNH08CC02C,
NNX08AL22G, NNX08BA99G, NNX08AH45G]; National Science Foundation
FX S.W.M. thanks Marco Velli, Egil Leer, and Tom Holzer for very
illuminating discussions about this, and related, work. We are indebted
to Klaus Wilhelm for comments on the manuscript and discussions
regarding the work of the SUMER team with respect to the Si blend impact
on the Ne VIII line profiles presented. The material presented was
supported by the National Aeronautics and Space Administration under
grants to S.W.M. and R.J.L. issued from the Living with a Star Targeted
Research & Technology Program (NNX08AU30G, NNH08CC02C, respectively). In
addition, part of the work presented here is supported by grants
NNX08AL22G, NNX08BA99G, and NNX08AH45G to S.W.M. and B.D.P. SOHO is a
mission of international cooperation between ESA and NASA. Finally, we
acknowledge the (anonymous) referee whose comments strengthened the
argument presented in this manuscript. The National Center for
Atmospheric Research is sponsored by the National Science Foundation.
NR 70
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 7
DI 10.1088/0004-637X/727/1/7
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000007
ER
PT J
AU Neill, JD
Sullivan, M
Gal-Yam, A
Quimby, R
Ofek, E
Wyder, TK
Howell, DA
Nugent, P
Seibert, M
Martin, DC
Overzier, R
Barlow, TA
Foster, K
Friedman, PG
Morrissey, P
Neff, SG
Schiminovich, D
Bianchi, L
Donas, J
Heckman, TM
Lee, YW
Madore, BF
Milliard, B
Rich, RM
Szalay, AS
AF Neill, James D.
Sullivan, Mark
Gal-Yam, Avishay
Quimby, Robert
Ofek, Eran
Wyder, Ted K.
Howell, D. Andrew
Nugent, Peter
Seibert, Mark
Martin, D. Christopher
Overzier, Roderik
Barlow, Tom A.
Foster, Karl
Friedman, Peter G.
Morrissey, Patrick
Neff, Susan G.
Schiminovich, David
Bianchi, Luciana
Donas, Jose
Heckman, Timothy M.
Lee, Young-Wook
Madore, Barry F.
Milliard, Bruno
Rich, R. Michael
Szalay, Alex S.
TI THE EXTREME HOSTS OF EXTREME SUPERNOVAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; stars: luminosity function, mass function; stars:
massive; supernovae: general
ID STAR-FORMING GALAXIES; CORE-COLLAPSE SUPERNOVAE; DIGITAL SKY SURVEY;
LUMINOUS SUPERNOVA; FORMATION RATES; MASSIVE STAR; IIN SUPERNOVAE; IA
SUPERNOVAE; UV; ULTRAVIOLET
AB We use GALEX ultraviolet (UV) and optical integrated photometry of the hosts of 17 luminous supernovae (LSNe, having peak M-V < -21) and compare them to a sample of 26,000 galaxies from a cross-match between the SDSS DR4 spectral catalog and GALEX interim release 1.1. We place the LSN hosts on the galaxy NUV - r versus M-r color-magnitude diagram (CMD) with the larger sample to illustrate how extreme they are. The LSN hosts appear to favor low-density regions of the galaxy CMD falling on the blue edge of the blue cloud toward the low-luminosity end. From the UV-optical photometry, we estimate the star formation history of the LSN hosts. The hosts have moderately low star formation rates (SFRs) and low stellar masses (M-*) resulting in high specific star formation rates (sSFR). Compared with the larger sample, the LSN hosts occupy low-density regions of a diagram plotting sSFR versus M-* in the area having higher sSFR and lower M-*. This preference for low M-*, high sSFR hosts implies that the LSNe are produced by an effect having to do with their local environment. The correlation of mass with metallicity suggests that perhaps wind-driven mass loss is the factor that prevents LSNe from arising in higher-mass, higher-metallicity hosts. The massive progenitors of the LSNe (> 100 M-circle dot), by appearing in low-SFR hosts, are potential tests for theories of the initial mass function that limit the maximum mass of a star based on the SFR.
C1 [Neill, James D.; Quimby, Robert; Ofek, Eran; Wyder, Ted K.; Martin, D. Christopher; Barlow, Tom A.; Foster, Karl; Friedman, Peter G.; Morrissey, Patrick] CALTECH, Pasadena, CA 91125 USA.
[Sullivan, Mark] Univ Oxford, Oxford OX1 3RH, England.
[Gal-Yam, Avishay] Weizmann Inst Sci, Fac Phys, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Howell, D. Andrew] Global Telescope Network, Las Cumbres Observ, Goleta, CA 93117 USA.
[Nugent, Peter] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Seibert, Mark; Madore, Barry F.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Overzier, Roderik] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Neff, Susan G.] NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA.
[Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Bianchi, Luciana] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Donas, Jose; Milliard, Bruno] Lab Astrophys Marseille, F-13376 Marseille 12, France.
[Heckman, Timothy M.; Szalay, Alex S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lee, Young-Wook] Yonsei Univ, Ctr Space Astrophys, Seoul 120749, South Korea.
[Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Neill, JD (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
OI Sullivan, Mark/0000-0001-9053-4820
FU Office of Science of the US Department of Energy [DE-AC02-05CH11231]
FX The National Energy Research Scientific Computing Center, which is
supported by the Office of Science of the US Department of Energy under
Contract No. DE-AC02-05CH11231, provided staff, computational resources
and data storage for this project.
NR 64
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 15
DI 10.1088/0004-637X/727/1/15
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000015
ER
PT J
AU Torres, G
Fressin, F
Batalha, NM
Borucki, WJ
Brown, TM
Bryson, ST
Buchhave, LA
Charbonneau, D
Ciardi, DR
Dunham, EW
Fabrycky, DC
Ford, EB
Gautier, TN
Gilliland, RL
Holman, MJ
Howell, SB
Isaacson, H
Jenkins, JM
Koch, DG
Latham, DW
Lissauer, JJ
Marcy, GW
Monet, DG
Prsa, A
Quinn, SN
Ragozzine, D
Rowe, JF
Sasselov, DD
Steffen, JH
Welsh, WF
AF Torres, Guillermo
Fressin, Francois
Batalha, Natalie M.
Borucki, William J.
Brown, Timothy M.
Bryson, Stephen T.
Buchhave, Lars A.
Charbonneau, David
Ciardi, David R.
Dunham, Edward W.
Fabrycky, Daniel C.
Ford, Eric B.
Gautier, Thomas N., III
Gilliland, Ronald L.
Holman, Matthew J.
Howell, Steve B.
Isaacson, Howard
Jenkins, Jon M.
Koch, David G.
Latham, David W.
Lissauer, Jack J.
Marcy, Geoffrey W.
Monet, David G.
Prsa, Andrej
Quinn, Samuel N.
Ragozzine, Darin
Rowe, Jason F.
Sasselov, Dimitar D.
Steffen, Jason H.
Welsh, William F.
TI MODELING KEPLER TRANSIT LIGHT CURVES AS FALSE POSITIVES: REJECTION OF
BLEND SCENARIOS FOR KEPLER-9, AND VALIDATION OF KEPLER-9 d, A
SUPER-EARTH-SIZE PLANET IN A MULTIPLE SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; planetary systems; stars: individual (Kepler-9, KIC
3323887, KOI-377); stars: statistics
ID STAR; CANDIDATES; MASS; PARAMETERS; EVOLUTION
AB Light curves from the Kepler Mission contain valuable information on the nature of the phenomena producing the transit-like signals. To assist in exploring the possibility that they are due to an astrophysical false positive, we describe a procedure (BLENDER) to model the photometry in terms of a "blend" rather than a planet orbiting a star. A blend may consist of a background or foreground eclipsing binary (or star-planet pair) whose eclipses are attenuated by the light of the candidate and possibly other stars within the photometric aperture. We apply BLENDER to the case of Kepler-9 (KIC 3323887), a target harboring two previously confirmed Saturn-size planets (Kepler-9 b and Kepler-9 c) showing transit timing variations, and an additional shallower signal with a 1.59 day period suggesting the presence of a super-Earth-size planet. Using BLENDER together with constraints from other follow-up observations we are able to rule out all blends for the two deeper signals and provide independent validation of their planetary nature. For the shallower signal, we rule out a large fraction of the false positives that might mimic the transits. The false alarm rate for remaining blends depends in part (and inversely) on the unknown frequency of small-size planets. Based on several realistic estimates of this frequency, we conclude with very high confidence that this small signal is due to a super-Earth-size planet (Kepler-9 d) in a multiple system, rather than a false positive. The radius is determined to be 1.64(-0.14)(+0.19) R-circle plus, and current spectroscopic observations are as yet insufficient to establish its mass.
C1 [Torres, Guillermo; Fressin, Francois; Charbonneau, David; Fabrycky, Daniel C.; Holman, Matthew J.; Latham, David W.; Quinn, Samuel N.; Ragozzine, Darin; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA.
[Borucki, William J.; Bryson, Stephen T.; Koch, David G.; Lissauer, Jack J.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Isaacson, Howard] San Francisco State Univ, San Francisco, CA 94132 USA.
[Jenkins, Jon M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Monet, David G.] USN, Observ, Flagstaff, AZ 86001 USA.
[Prsa, Andrej] Villanova Univ, Villanova, PA 19085 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA.
RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM gtorres@cfa.harvard.edu
RI Ragozzine, Darin/C-4926-2013;
OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi,
David/0000-0002-5741-3047; Charbonneau, David/0000-0002-9003-484X;
Fabrycky, Daniel/0000-0003-3750-0183
FU NASA
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. We are grateful to Leo Girardi for computing isochrones for
this work in the Kepler passband, to Frederic Pont for very helpful
discussions on false alarm probabilities, and to David Sing for advice
on limb-darkening coefficients. We also thank the anonymous referee for
insightful comments on the original version of this paper.
NR 44
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 24
DI 10.1088/0004-637X/727/1/24
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000024
ER
PT J
AU Way, MJ
Gazis, PR
Scargle, JD
AF Way, M. J.
Gazis, P. R.
Scargle, Jeffrey D.
TI STRUCTURE IN THE THREE-DIMENSIONAL GALAXY DISTRIBUTION. I. METHODS AND
EXAMPLE RESULTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: clusters: general; large-scale
structure of universe; methods: data analysis
ID LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; CAMPANAS REDSHIFT SURVEY;
N-BODY SIMULATIONS; DARK-MATTER HALOES; DATA RELEASE; VORONOI
TESSELLATION; TOPOLOGY PRESERVATION; EXTRAGALACTIC OBJECTS;
STATISTICAL-ANALYSIS
AB Three methods for detecting and characterizing structure in point data, such as that generated by redshift surveys, are described: classification using self-organizing maps, segmentation using Bayesian blocks, and density estimation using adaptive kernels. The first two methods are new, and allow detection and characterization of structures of arbitrary shape and at a wide range of spatial scales. These methods should elucidate not only clusters, but also the more distributed, wide-ranging filaments and sheets, and further allow the possibility of detecting and characterizing an even broader class of shapes. The methods are demonstrated and compared in application to three data sets: a carefully selected volume-limited sample from the Sloan Digital Sky Survey redshift data, a similarly selected sample from the Millennium Simulation, and a set of points independently drawn from a uniform probability distribution-a so-called Poisson distribution. We demonstrate a few of the many ways in which these methods elucidate large-scale structure in the distribution of galaxies in the nearby universe.
C1 [Way, M. J.; Gazis, P. R.; Scargle, Jeffrey D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Way, M. J.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Way, M. J.] Dept Space Phys & Astron, Uppsala, Sweden.
RP Way, MJ (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM Michael.J.Way@nasa.gov; PGazis@sbcglobal.net; Jeffrey.D.Scargle@nasa.gov
RI Way, Michael/D-5254-2012;
OI Way, Michael/0000-0003-3728-0475
FU Alfred P. Sloan Foundation; National Aeronautics and Space
Administration; National Science Foundation; U.S. Department of Energy;
Japanese Monbukagakusho; Max Planck Society; NASA-Ames Director;
University of Chicago, Fermilab; Institute for Advanced Study; Japan
Participation Group; Johns Hopkins University, Los Alamos National
Laboratory; Max-Planck-Institute for Astronomy; Max-Planck-Institute for
Astrophysics; New Mexico State University; University of Pittsburgh;
Princeton University; United States Naval Observatory; University of
Washington
FX We are grateful to the NASA-Ames Director's Discretionary Fund and to
Joe Bredekamp and the NASA Applied Information Systems Research Program
for support and encouragement. We thank the Institute for Pure and
Applied Mathematics at UCLA and the Banff International Research Station
for hospitality over times where some of this work was carried out.
Helpful discussions and suggestions over the years came from Chris
Henze, Creon Levit, and Ashok Srivastava.; Funding for the SDSS has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Aeronautics and Space Administration, the
National Science Foundation, the U.S. Department of Energy, the Japanese
Monbukagakusho, and the Max Planck Society. The SDSS Web site is
http://www.sdss.org/.; The SDS is managed by the Astrophysical Research
Consortium for the Participating Institutions. The Participating
Institutions are The University of Chicago, Fermilab, the Institute for
Advanced Study, the Japan Participation Group, The Johns Hopkins
University, Los Alamos National Laboratory, the Max-Planck-Institute for
Astronomy, the Max-Planck-Institute for Astrophysics, New Mexico State
University, University of Pittsburgh, Princeton University, the United
States Naval Observatory, and the University of Washington.
NR 182
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2011
VL 727
IS 1
AR 48
DI 10.1088/0004-637X/727/1/48
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703PT
UT WOS:000285992000048
ER
PT J
AU Ransom, SM
Ray, PS
Camilo, F
Roberts, MSE
Celik, O
Wolff, MT
Cheung, CC
Kerr, M
Pennucci, T
DeCesar, ME
Cognard, I
Lyne, AG
Stappers, BW
Freire, PCC
Grove, JE
Abdo, AA
Desvignes, G
Donato, D
Ferrara, EC
Gehrels, N
Guillemot, L
Gwon, C
Harding, AK
Johnston, S
Keith, M
Kramer, M
Michelson, PF
Parent, D
Parkinson, PMS
Romani, RW
Smith, DA
Theureau, G
Thompson, DJ
Weltevrede, P
Wood, KS
Ziegler, M
AF Ransom, S. M.
Ray, P. S.
Camilo, F.
Roberts, M. S. E.
Celik, Oe.
Wolff, M. T.
Cheung, C. C.
Kerr, M.
Pennucci, T.
DeCesar, M. E.
Cognard, I.
Lyne, A. G.
Stappers, B. W.
Freire, P. C. C.
Grove, J. E.
Abdo, A. A.
Desvignes, G.
Donato, D.
Ferrara, E. C.
Gehrels, N.
Guillemot, L.
Gwon, C.
Harding, A. K.
Johnston, S.
Keith, M.
Kramer, M.
Michelson, P. F.
Parent, D.
Parkinson, P. M. Saz
Romani, R. W.
Smith, D. A.
Theureau, G.
Thompson, D. J.
Weltevrede, P.
Wood, K. S.
Ziegler, M.
TI THREE MILLISECOND PULSARS IN FERMI LAT UNASSOCIATED BRIGHT SOURCES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE pulsars: general; pulsars: individual (J0614-3329, J1231-1411,
J2214+3000)
ID LARGE-AREA TELESCOPE; DATA-ANALYSIS SYSTEMS; RAY-SPACE-TELESCOPE; X-RAY;
POPULATION; EMISSION; BINARY; DISCOVERY; RADIO
AB We searched for radio pulsars in 25 of the non-variable, unassociated sources in the Fermi LAT Bright Source List with the Green Bank Telescope at 820 MHz. We report the discovery of three radio and gamma-ray millisecond pulsars (MSPs) from a high Galactic latitude subset of these sources. All of the pulsars are in binary systems, which would have made them virtually impossible to detect in blind gamma-ray pulsation searches. They seem to be relatively normal, nearby (<= 2 kpc) MSPs. These observations, in combination with the Fermi detection of gamma-ray from other known radio MSPs, imply that most, if not all, radio MSPs are efficient gamma-ray producers. The gamma-ray spectra of the pulsars are power law in nature with exponential cutoffs at a few GeV, as has been found with most other pulsars. The MSPs have all been detected as X-ray point sources. Their soft X-ray luminosities of similar to 10(30)-10(31) erg s(-1) are typical of the rare radio MSPs seen in X-rays.
C1 [Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Ray, P. S.; Wolff, M. T.; Grove, J. E.; Gwon, C.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Roberts, M. S. E.] Eureka Sci, Oakland, CA 94602 USA.
[Celik, Oe.; DeCesar, M. E.; Donato, D.; Ferrara, E. C.; Gehrels, N.; Harding, A. K.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, Oe.; Donato, D.] CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, Oe.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Cheung, C. C.; Abdo, A. A.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Kerr, M.; Michelson, P. F.; Romani, R. W.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Kerr, M.; Michelson, P. F.; Romani, R. W.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Pennucci, T.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[DeCesar, M. E.; Donato, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[DeCesar, M. E.; Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cognard, I.; Theureau, G.] CNRS, UMR 6115, LPCE, F-45071 Orleans 02, France.
[Cognard, I.; Theureau, G.] CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France.
[Lyne, A. G.; Stappers, B. W.; Kramer, M.; Weltevrede, P.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Freire, P. C. C.; Guillemot, L.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Desvignes, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Desvignes, G.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
[Johnston, S.; Keith, M.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Parent, D.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Smith, D. A.] Univ Bordeaux 1, CNRS IN2p3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
RP Ransom, SM (reprint author), Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA.
EM sransom@nrao.edu; Paul.Ray@nrl.navy.mil
RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Gehrels,
Neil/D-2971-2012;
OI Thompson, David/0000-0001-5217-9135; Roberts,
Mallory/0000-0002-9396-9720; Ransom, Scott/0000-0001-5799-9714; Ray,
Paul/0000-0002-5297-5278
FU NASA [NNG09EE57I]
FX We acknowledge helpful discussions with Natalie Webb and Lynne Valencic.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. This work was partially supported by NASA Grant No.
NNG09EE57I. The Fermi LAT Collaboration acknowledges support from a
number of agencies and institutes for both development and the operation
of the LAT as well as scientific data analysis. These include NASA and
DOE in the US, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy,
MEXT, KEK, and JAXA in Japan, and the K.A. Wallenberg Foundation, the
Swedish Research Council and the National Space Board in Sweden.
Additional support from INAF in Italy and CNES in France for science
analysis during the operations phase is also gratefully acknowledged.
NR 33
TC 77
Z9 77
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 20
PY 2011
VL 727
IS 1
AR L16
DI 10.1088/2041-8205/727/1/L16
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 703QG
UT WOS:000285993800016
ER
PT J
AU Briggs, MS
Connaughton, V
Wilson-Hodge, C
Preece, RD
Fishman, GJ
Kippen, RM
Bhat, PN
Paciesas, WS
Chaplin, VL
Meegan, CA
von Kienlin, A
Greiner, J
Dwyer, JR
Smith, DM
AF Briggs, Michael S.
Connaughton, Valerie
Wilson-Hodge, Colleen
Preece, Robert D.
Fishman, Gerald J.
Kippen, R. Marc
Bhat, P. N.
Paciesas, William S.
Chaplin, Vandiver L.
Meegan, Charles A.
von Kienlin, Andreas
Greiner, Jochen
Dwyer, Joesph R.
Smith, David M.
TI Electron-positron beams from terrestrial lightning observed with Fermi
GBM
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GAMMA-RAY FLASHES; RUNAWAY ELECTRONS; BURST MONITOR; THUNDERSTORM; AIR
AB Terrestrial Gamma-ray Flashes (TGFs) are brief pulses of energetic radiation observed in low-earth orbit. They are associated with thunderstorms and lightning and have been observed both as gamma-ray and electron flashes depending on the position of the spacecraft with respect to the source. While gamma-ray TGFs are detected as short pulses lasting less than 1 ms, most TGFs seen by the Fermi Gamma-ray Burst Monitor (GBM) with durations greater than 1 ms are, instead, the result of electrons traveling from the sources along geomagnetic field lines. We perform spectral analysis of the three brightest electron TGFs detected by GBM and discover strong 511 keV positron annihilation lines, demonstrating that these electron TGFs also contain substantial positron components. This shows that pair production occurs in conjunction with some terrestrial lightning and that most likely all TGFs are injecting electron-positron beams into the near Earth environment. Citation: Briggs, M. S., et al. (2011), Electron-positron beams from terrestrial lightning observed with Fermi GBM, Geophys. Res. Lett., 38, L02808, doi:10.1029/2010GL046259.
C1 [Briggs, Michael S.; Connaughton, Valerie; Preece, Robert D.; Bhat, P. N.; Paciesas, William S.; Chaplin, Vandiver L.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Wilson-Hodge, Colleen; Fishman, Gerald J.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Dwyer, Joesph R.] Florida Inst Technol, Melbourne, FL 32901 USA.
[von Kienlin, Andreas; Greiner, Jochen] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Kippen, R. Marc] Los Alamos Natl Lab, ISR 1, Los Alamos, NM 87545 USA.
[Meegan, Charles A.] USRA, Huntsville, AL 35805 USA.
[Smith, David M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Preece, Robert D.] Univ Alabama, Dept Phys, Huntsville, AL 35805 USA.
RP Briggs, MS (reprint author), Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM michael.briggs@uah.edu; jerry.fishman@nasa.gov; mkippen@lanl.gov;
chip.meegan@nasa.gov; azk@mpe.mpg.de; jdwyer@fit.edu;
dsmith@scipp.ucsc.edu
OI Preece, Robert/0000-0003-1626-7335
NR 19
TC 66
Z9 66
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 JAN 20
PY 2011
VL 38
AR L02808
DI 10.1029/2010GL046259
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 710MX
UT WOS:000286517000004
ER
PT J
AU Jeong, SJ
Ho, CH
Brown, ME
Kug, JS
Piao, SL
AF Jeong, Su-Jong
Ho, Chang-Hoi
Brown, Molly E.
Kug, Jong-Seong
Piao, Shilong
TI Browning in desert boundaries in Asia in recent decades
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SAHARA DESERT; NDVI DATA; VEGETATION; DATASET; CLIMATE; INDEX
AB In this study, the changes in desert boundaries in Asia (Gobi, Karakum, Lut, Taklimakan, and Thar deserts) during the growing season (April-October) in the years 1982-2008 were investigated by analyzing the normalized difference vegetation index (NDVI), precipitation, and temperature. In the desert boundary regions, the domain mean NDVI values increased by 7.2% per decade in 1982-1998 but decreased by 6.8% per decade thereafter. Accordingly, the bare soil areas (or nonvegetated areas) of the inside of the desert boundaries contracted by 9.8% per decade in the 1990s and expanded by 8.7% per decade in the 2000s. It is noted that the five deserts experience nearly simultaneous NDVI changes although they cover a very diverse area of Asia. In contrast, changes in temperature and precipitation in the deserts show rather diverse results. In desert boundaries located along 40 degrees N (Gobi, Taklimakan, and Karakum), the decadal changes in vegetation greenness were mainly related to regional climate during the entire analysis period. Precipitation increased in the 1990s, providing favorable conditions for vegetation growth (i.e., greening), but precipitation reduced (19 mm per decade) and warming intensified (0.7 degrees C per decade) in the 2000s, causing less moisture to be available for vegetation growth (i.e., browning). In desert boundaries below 40 degrees N (Lut and Thar), although an increase in precipitation (8 mm per decade) led to greening in the 1990s, local changes in precipitation and temperature did not necessarily cause browning in the 2000s. Observed multidecadal changes in vegetation greenness in the present study suggest that under significant global and/or regional warming, changes in moisture availability for vegetation growth in desert boundaries are an important factor when understanding decadal changes in areas vulnerable to desertification over Asia.
C1 [Jeong, Su-Jong; Ho, Chang-Hoi] Seoul Natl Univ, Sch Earth & Environm Sci, KR-151742 Seoul, South Korea.
[Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Kug, Jong-Seong] Korea Ocean Res & Dev Inst, KR-726744 Ansan, South Korea.
[Piao, Shilong] Peking Univ, Dept Ecol, Beijing 100871, Peoples R China.
RP Jeong, SJ (reprint author), Seoul Natl Univ, Sch Earth & Environm Sci, KR-151742 Seoul, South Korea.
EM hoch@cpl.snu.ac.kr
RI KUG, JONG-SEONG/A-8053-2013; Brown, Molly/M-5146-2013; Jeong,
Su-Jong/J-4110-2014; Ho, Chang-Hoi/H-8354-2015; Brown, Molly/E-2724-2010
OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314
FU Korea Meteorological Administration Research and Development Program
[CATER 2006-4204]
FX This research was funded by the Korea Meteorological Administration
Research and Development Program under grant CATER 2006-4204.
NR 22
TC 21
Z9 22
U1 0
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 20
PY 2011
VL 116
AR D02103
DI 10.1029/2010JD014633
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 710NV
UT WOS:000286519400004
ER
PT J
AU Jimenez, C
Prigent, C
Mueller, B
Seneviratne, SI
McCabe, MF
Wood, EF
Rossow, WB
Balsamo, G
Betts, AK
Dirmeyer, PA
Fisher, JB
Jung, M
Kanamitsu, M
Reichle, RH
Reichstein, M
Rodell, M
Sheffield, J
Tu, K
Wang, K
AF Jimenez, C.
Prigent, C.
Mueller, B.
Seneviratne, S. I.
McCabe, M. F.
Wood, E. F.
Rossow, W. B.
Balsamo, G.
Betts, A. K.
Dirmeyer, P. A.
Fisher, J. B.
Jung, M.
Kanamitsu, M.
Reichle, R. H.
Reichstein, M.
Rodell, M.
Sheffield, J.
Tu, K.
Wang, K.
TI Global intercomparison of 12 land surface heat flux estimates
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID NET ECOSYSTEM EXCHANGE; ATMOSPHERE WATER FLUX; SPACE-TIME CLIMATE;
ISLSCP-II DATA; SOIL-MOISTURE; SATELLITE-OBSERVATIONS; ECMWF MODEL; DATA
SETS; EVAPOTRANSPIRATION; VEGETATION
AB A global intercomparison of 12 monthly mean land surface heat flux products for the period 1993-1995 is presented. The intercomparison includes some of the first emerging global satellite-based products (developed at Paris Observatory, Max Planck Institute for Biogeochemistry, University of California Berkeley, University of Maryland, and Princeton University) and examples of fluxes produced by reanalyses (ERA-Interim, MERRA, NCEP-DOE) and off-line land surface models (GSWP-2, GLDAS CLM/Mosaic/Noah). An intercomparison of the global latent heat flux (Q(le)) annual means shows a spread of similar to 20 W m(-2) (all-product global average of similar to 45 W m(-2)). A similar spread is observed for the sensible (Q(h)) and net radiative (R-n) fluxes. In general, the products correlate well with each other, helped by the large seasonal variability and common forcing data for some of the products. Expected spatial distributions related to the major climatic regimes and geographical features are reproduced by all products. Nevertheless, large Q(le) and Q(h) absolute differences are also observed. The fluxes were spatially averaged for 10 vegetation classes. The larger Q(le) differences were observed for the rain forest but, when normalized by mean fluxes, the differences were comparable to other classes. In general, the correlations between Q(le) and R-n were higher for the satellite-based products compared with the reanalyses and off-line models. The fluxes were also averaged for 10 selected basins. The seasonality was generally well captured by all products, but large differences in the flux partitioning were observed for some products and basins.
C1 [Jimenez, C.; Prigent, C.] Observ Paris, CNRS, Lab Etud Rayonnement & Matiere Astrophys, F-75014 Paris, France.
[Balsamo, G.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Betts, A. K.] Atmospher Res, Pittsford, VT 05763 USA.
[Dirmeyer, P. A.] Ctr Ocean Land Atmosphere Studies, Calverton, MD 20705 USA.
[Fisher, J. B.] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QI, England.
[Jung, M.; Reichstein, M.] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
[Kanamitsu, M.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92037 USA.
[McCabe, M. F.] Univ New S Wales, Sch Civil & Environm Engn, Sydney, NSW 2052, Australia.
[Mueller, B.; Seneviratne, S. I.] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland.
[Reichle, R. H.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Rodell, M.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[Rossow, W. B.] CUNY City Coll, NOAA Cooperat Remote Sensing Sci & Technol Ctr, New York, NY 10031 USA.
[Wood, E. F.; Sheffield, J.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[Tu, K.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Wang, K.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA.
RP Jimenez, C (reprint author), Observ Paris, CNRS, Lab Etud Rayonnement & Matiere Astrophys, F-75014 Paris, France.
EM carlos.jimenez@obspm.fr
RI Mueller, Brigitte/E-2594-2011; McCabe, Matthew/G-5194-2011; Seneviratne,
Sonia/G-8761-2011; Reichle, Rolf/E-1419-2012; Reichstein,
Markus/A-7494-2011; Balsamo, Gianpaolo/I-3362-2013; Rossow,
William/F-3138-2015; Dirmeyer, Paul/B-6553-2016; Rodell,
Matthew/E-4946-2012; Wang, Kaicun/F-7813-2012
OI Fisher, Joshua/0000-0003-4734-9085; Mueller,
Brigitte/0000-0003-1876-4722; McCabe, Matthew/0000-0002-1279-5272;
Seneviratne, Sonia/0000-0001-9528-2917; Reichstein,
Markus/0000-0001-5736-1112; Balsamo, Gianpaolo/0000-0002-1745-3634;
Dirmeyer, Paul/0000-0003-3158-1752; Rodell, Matthew/0000-0003-0106-7437;
Wang, Kaicun/0000-0002-7414-5400
FU GEWEX
FX The LandFlux-Eval initiative acknowledges support by GEWEX. C. D.
Kummerow, as chair of the GEWEX Radiation Panel, is acknowledged for
encouraging the LandFlux activity, and contributing to the scientific
discussions. The GLDAS data were acquired as part of the mission of
NASA's Earth Science Division and archived and distributed by the
Goddard Earth Sciences (GES) Data and Information Services Center (DISC)
are acknowledged by disseminating the GLDAS data. The Global Modeling
and Assimilation Office (GMAO) and the GES DISC are acknowledged for
disseminating the MERRA data.
NR 92
TC 133
Z9 133
U1 9
U2 63
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 JAN 20
PY 2011
VL 116
AR D02102
DI 10.1029/2010JD014545
PG 27
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 710NV
UT WOS:000286519400002
ER
PT J
AU Heavens, NG
Richardson, MI
Kleinbohl, A
Kass, DM
McCleese, DJ
Abdou, W
Benson, JL
Schofield, JT
Shirley, JH
Wolkenberg, PM
AF Heavens, N. G.
Richardson, M. I.
Kleinboehl, A.
Kass, D. M.
McCleese, D. J.
Abdou, W.
Benson, J. L.
Schofield, J. T.
Shirley, J. H.
Wolkenberg, P. M.
TI Vertical distribution of dust in the Martian atmosphere during northern
spring and summer: High-altitude tropical dust maximum at northern
summer solstice
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MARS ORBITER CAMERA; WATER-ICE CLOUDS; INTERANNUAL VARIABILITY; PARTICLE
SIZES; CIRCULATION; PATHFINDER; STORMS; MODELS; SIMULATIONS; AEROSOL
AB The vertical distribution of dust in Mars' atmosphere is a critical unknown in the simulation of its general circulation and a source of insight into the lifting and transport of dust. Zonal average vertical profiles of dust opacity retrieved by Mars Climate Sounder show that the vertical dust distribution is mostly consistent with Mars general circulation model (GCM) simulations in southern spring and summer but not in northern spring and summer. Unlike the GCM simulations, the mass mixing ratio of dust has a maximum at 1525 km over the tropics during much of northern spring and summer: the high-altitude tropical dust maximum (HATDM). The HATDM has significant and characteristic longitudinal variability, which it maintains for time scales on the order of or greater than those on which advection, sedimentation, and vertical eddy diffusion would act to eliminate both the longitudinal and vertical inhomogeneity of the distribution. While outflow from dust storms is able to produce enriched layers of dust at altitudes much greater than 25 km, tropical dust storm activity during the period in which the HATDM occurs is likely too rare to support the HATDM. Instead, the lifting of dust by mesoscale circulations over topography, pseudomoist convection due to the solar heating of dust, and scavenging of dust by water ice are all possible drivers of the HATDM.
C1 [Heavens, N. G.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA.
[Richardson, M. I.] Ashima Res, Pasadena, CA 91106 USA.
[Kleinboehl, A.; Kass, D. M.; McCleese, D. J.; Abdou, W.; Benson, J. L.; Schofield, J. T.; Shirley, J. H.; Wolkenberg, P. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Heavens, NG (reprint author), Cornell Univ, Dept Earth & Atmospher Sci, 1118 Bradfield Hall, Ithaca, NY 14853 USA.
EM heavens@cornell.edu
OI Heavens, Nicholas/0000-0001-7654-503X
FU Jet Propulsion Laboratory, California Institute of Technology under NASA
FX The authors would like to thank two anonymous reviewers for their
comments on this manuscript and Scot Rafkin, John Wilson, Francois
Forget, Aymeric Spiga, Stephen Fuerstenau, and Dan Tyler for useful
discussions. This work was funded by and performed in part at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA as part of the Mars Reconnaissance Orbiter project.
NR 50
TC 33
Z9 33
U1 0
U2 13
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 JAN 20
PY 2011
VL 116
AR E01007
DI 10.1029/2010JE003692
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 710OE
UT WOS:000286520300001
ER
PT J
AU Davis, CJ
de Koning, CA
Davies, JA
Biesecker, D
Millward, G
Dryer, M
Deehr, C
Webb, DF
Schenk, K
Freeland, SL
Mostl, C
Farrugia, CJ
Odstrcil, D
AF Davis, C. J.
de Koning, C. A.
Davies, J. A.
Biesecker, D.
Millward, G.
Dryer, M.
Deehr, C.
Webb, D. F.
Schenk, K.
Freeland, S. L.
Moestl, C.
Farrugia, C. J.
Odstrcil, D.
TI A comparison of space weather analysis techniques used to predict the
arrival of the Earth-directed CME and its shockwave launched on 8 April
2010
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID CORONAL MASS EJECTIONS; INTERPLANETARY MAGNETIC-FIELD; ADVANCED
COMPOSITION EXPLORER; STRUCTURED SOLAR-WIND; 3-DIMENSIONAL PROPAGATION;
GEOMETRIC LOCALIZATION; PROTON TEMPERATURE; MODEL; FILAMENTS; CLOUDS
AB The Earth-directed coronal mass ejection (CME) of 8 April 2010 provided an opportunity for space weather predictions from both established and developmental techniques to be made from near-real time data received from the SOHO and STEREO spacecraft; the STEREO spacecraft provide a unique view of Earth-directed events from outside the Sun-Earth line. Although the near-real time data transmitted by the STEREO Space Weather Beacon are significantly poorer in quality than the subsequently downlinked science data, the use of these data has the advantage that near-real time analysis is possible, allowing actual forecasts to be made. The fact that such forecasts cannot be biased by any prior knowledge of the actual arrival time at Earth provides an opportunity for an unbiased comparison between several established and developmental forecasting techniques. We conclude that for forecasts based on the STEREO coronagraph data, it is important to take account of the subsequent acceleration/deceleration of each CME through interaction with the solar wind, while predictions based on measurements of CMEs made by the STEREO Heliospheric Imagers would benefit from higher temporal and spatial resolution. Space weather forecasting tools must work with near-real time data; such data, when provided by science missions, is usually highly compressed and/or reduced in temporal/spatial resolution and may also have significant gaps in coverage, making such forecasts more challenging.
C1 [Davis, C. J.; Davies, J. A.] STFC, Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[de Koning, C. A.; Biesecker, D.; Millward, G.; Dryer, M.] NOAA SWPC, Boulder, CO 80305 USA.
[Deehr, C.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Webb, D. F.] Boston Coll, ISR, Chestnut Hill, MA 02467 USA.
[Schenk, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Freeland, S. L.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Moestl, C.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Farrugia, C. J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Odstrcil, D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
RP Davis, CJ (reprint author), STFC, Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
EM chris.davis@stfc.ac.uk
RI Scott, Christopher/H-8664-2012;
OI Scott, Christopher/0000-0001-6411-5649; Moestl,
Christian/0000-0001-6868-4152
FU U.S. Navy [N00173-10-1-G-001]; NASA [NNX10AQ29G, NNX09AJ84G]
FX The authors would like to thank N. Ness at the Bartol Research Institute
for supplying the ACE magnetic field data and D. J. MComas at the
Southwest Research Institute for the ACE/SWEPAM data. Both data sets
were accessed from the CDAWeb interface supported by the Goddard Space
Flight Center via their website at http://cdaweb.gsfc.nasa.gov. D.W. was
supported by U.S. Navy contract N00173-10-1-G-001. C.J.F. was supported
by NASA grant NNX10AQ29G. C.A. de Koning was supported by NASA grant
NNX09AJ84G.
NR 54
TC 19
Z9 19
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD JAN 20
PY 2011
VL 9
AR S01005
DI 10.1029/2010SW000620
PG 16
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 710PC
UT WOS:000286522700001
ER
PT J
AU da Costa, AA
Diver, DA
Laing, EW
Stark, CR
Teodoro, LFA
AF da Costa, A. A.
Diver, D. A.
Laing, E. W.
Stark, C. R.
Teodoro, L. F. A.
TI Pulsar electrodynamics: Relativistic kinetic theory of radiative
plasmas-collective phenomena and their radiation
SO PHYSICAL REVIEW D
LA English
DT Article
ID GAMMA-RAY PULSAR; CRAB PULSAR; NUMERICAL SIMULATIONS; MODEL;
MAGNETOSPHERES; ELECTRONS; EMISSION; SPECTRA
AB The classical modeling of radiation by accelerated charged particles in pulsars predicts a cutoff in photon energy at around 25 GeV. While this is broadly consistent with observations, the classical treatment is not self-consistent, and cannot be extended to explain the rare high-energy detections of photons in the 100s of GeV range. In this paper we revisit the theoretical modeling of high-energy radiation processes in very strong electromagnetic fields, in the context of both single particles and collective plasmas. There are no classical constraints on this description. We find that there is indeed a critical energy of around 50 GeV that arises naturally in this self-consistent treatment, but rather than being a cutoff, this critical energy signals a transition from radiation that is classical to a quasiquantum description, in which the particle is able to radiate almost its total energy in a single event. This new modeling therefore places pulsar radiation processes on a more secure physical basis, and admits the possibility of the production of TeV photons in a self-consistent way.
C1 [da Costa, A. A.] Inst Super Tecn UTL, Dept Engn Electroten & Comp, Seccao Telecomunicacoes, P-1049001 Lisbon, Portugal.
[da Costa, A. A.; Diver, D. A.; Laing, E. W.; Stark, C. R.; Teodoro, L. F. A.] Univ Glasgow, Sch Phys Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Stark, C. R.] Univ St Andrews, Sch Math Stat, Math Inst, St Andrews KY16 9SS, Fife, Scotland.
[Teodoro, L. F. A.] NASA, BAER, Space Sci Astrobiol Div, Ames Res Ctr, Moffett, CA 94935 USA.
RP da Costa, AA (reprint author), Inst Super Tecn UTL, Dept Engn Electroten & Comp, Seccao Telecomunicacoes, P-1049001 Lisbon, Portugal.
RI Diver, Declan/E-6672-2010; Stark, Craig /A-7667-2016
OI Diver, Declan/0000-0001-6478-6020;
FU UK Science and Technology Funding Council [STFC/F002149/I,
PP/E001122/1]; Fundacao para a Ciencia e Tecnologia, Portugal
[SFRH/BSAB/771/2007]; Glasgow University
FX D. A. D. gratefully acknowledges funding from the UK Science and
Technology Funding Council (STFC/F002149/I), as does C. R. S.
(PP/E001122/1). A. A. daC. is grateful to the Fundacao para a Ciencia e
Tecnologia, Portugal, who sponsored his sabbatical leave, under Grant
No. SFRH/BSAB/771/2007; thanks are due equally to the Instituto Superior
Tecnico and to the Department of Physics and Astronomy, University of
Glasgow, for, respectively, granting and hosting A. A. daC.'s sabbatical
leave. L. F. A. T. is grateful to the Leverhulme Trust for funding at
Glasgow University. Finally, thanks are due to H. E. Potts, C. S.
Maclachlan, and E. Bennet for their helpful comments and stimulating
discussion, and to an anonymous referee whose helpful comments helped to
shape this paper. The School of Physics and Astronomy at the University
of Glasgow is a member of the Scottish Universities Physics Alliance.
NR 42
TC 1
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U1 0
U2 6
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 19
PY 2011
VL 83
IS 2
AR 023013
DI 10.1103/PhysRevD.83.023013
PG 16
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 714IO
UT WOS:000286803300004
ER
PT J
AU Detrixhe, M
Besson, D
Gorham, PW
Allison, P
Baughmann, B
Beatty, JJ
Belov, K
Bevan, S
Binns, WR
Chen, C
Chen, P
Clem, JM
Connolly, A
De Marco, D
Dowkontt, PF
DuVernois, MA
Frankenfeld, C
Grashorn, EW
Hogan, DP
Griffith, N
Hill, B
Hoover, S
Israel, MH
Javaid, A
Liewer, KM
Matsuno, S
Mercurio, BC
Miki, C
Mottram, M
Nam, J
Nichol, RJ
Palladino, K
Romero-Wolf, A
Ruckman, L
Saltzberg, D
Seckel, D
Varner, GS
Vieregg, AG
Wang, Y
AF Detrixhe, M.
Besson, D.
Gorham, P. W.
Allison, P.
Baughmann, B.
Beatty, J. J.
Belov, K.
Bevan, S.
Binns, W. R.
Chen, C.
Chen, P.
Clem, J. M.
Connolly, A.
De Marco, D.
Dowkontt, P. F.
DuVernois, M. A.
Frankenfeld, C.
Grashorn, E. W.
Hogan, D. P.
Griffith, N.
Hill, B.
Hoover, S.
Israel, M. H.
Javaid, A.
Liewer, K. M.
Matsuno, S.
Mercurio, B. C.
Miki, C.
Mottram, M.
Nam, J.
Nichol, R. J.
Palladino, K.
Romero-Wolf, A.
Ruckman, L.
Saltzberg, D.
Seckel, D.
Varner, G. S.
Vieregg, A. G.
Wang, Y.
CA ANITA Collaboration
TI Ultrarelativistic magnetic monopole search with the ANITA-II
balloon-borne radio interferometer
SO PHYSICAL REVIEW D
LA English
DT Article
ID DETECTOR; FLUX
AB We have conducted a search for extended energy deposition trails left by ultrarelativistic magnetic monopoles interacting in Antarctic ice. The nonobservation of any satisfactory candidates in the 31 days of accumulated ANITA-II (Antarctic Impulsive Transient Antenna) flight data results in an upper limit on the diffuse flux of relativistic monopoles. We obtain a 90% C.L. limit of order 10(-19) (cm(2) s sr)(-1) for values of Lorentz factor, gamma, 10(10) <= at the anticipated energy E(tot) = 10(16) GeV. This bound is stronger than all previously published experimental limits for this kinematic range.
C1 [Detrixhe, M.; Besson, D.; Frankenfeld, C.; Hogan, D. P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gorham, P. W.; Allison, P.; DuVernois, M. A.; Hill, B.; Matsuno, S.; Miki, C.; Romero-Wolf, A.; Ruckman, L.; Varner, G. S.; Wang, Y.] Univ Hawaii, Dept Phys & Astron, Manoa, HI 96822 USA.
[Wang, Y.] Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA.
[Baughmann, B.; Beatty, J. J.; Grashorn, E. W.; Griffith, N.; Mercurio, B. C.; Palladino, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Binns, W. R.; Dowkontt, P. F.; Israel, M. H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Chen, C.; Chen, P.] Natl Taiwan Univ, Dept Phys, Taipei, Taiwan.
[Clem, J. M.; De Marco, D.; Javaid, A.; Seckel, D.] Univ Delaware, Dept Phys, Newark, DE 19716 USA.
[Bevan, S.; Connolly, A.; Mottram, M.; Nichol, R. J.] UCL, Dept Phys, London, England.
[Belov, K.; Hoover, S.; Saltzberg, D.; Vieregg, A. G.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Liewer, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nam, J.] Ewha Womans Univ, Seoul, South Korea.
RP Detrixhe, M (reprint author), Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
RI Nichol, Ryan/C-1645-2008; Vieregg, Abigail/D-2287-2012; Belov,
Konstantin/D-2520-2013; Connolly, Amy/J-3958-2013; Beatty,
James/D-9310-2011
OI Beatty, James/0000-0003-0481-4952
NR 34
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U1 0
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD JAN 19
PY 2011
VL 83
IS 2
AR 023513
DI 10.1103/PhysRevD.83.023513
PG 11
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 714IO
UT WOS:000286803300006
ER
PT J
AU Kent, ST
Howard, G
Crosson, WL
Prineas, RJ
McClure, LA
AF Kent, Shia T.
Howard, George
Crosson, William L.
Prineas, Ronald J.
McClure, Leslie A.
TI The association of remotely-sensed outdoor temperature with blood
pressure levels in REGARDS: a cross-sectional study of a large, national
cohort of African-American and white participants
SO ENVIRONMENTAL HEALTH
LA English
DT Article
ID SEASONAL-VARIATION; RACIAL-DIFFERENCES; COLD; HYPERTENSION; WEATHER;
STRESS; HEALTH; MOOD; INFLAMMATION; MORTALITY
AB Background: Evidence is mounting regarding the clinically significant effect of temperature on blood pressure.
Methods: In this cross-sectional study the authors obtained minimum and maximum temperatures and their respective previous week variances at the geographic locations of the self-reported residences of 26,018 participants from a national cohort of blacks and whites, aged 45+. Linear regression of data from 20,623 participants was used in final multivariable models to determine if these temperature measures were associated with levels of systolic or diastolic blood pressure, and whether these relations were modified by stroke-risk region, race, education, income, sex hypertensive medication status, or age.
Results: After adjustment for confounders, same-day maximum temperatures 20 degrees F lower had significant associations with 1.4 mmHg (95% CI: 1.0, 1.9) higher systolic and 0.5 mmHg (95% CI: 0.3, 0.8) higher diastolic blood pressures. Same-day minimum temperatures 20 degrees F lower had a significant association with 0.7 mmHg (95% CI: 0.3, 1.0) higher systolic blood pressures but no significant association with diastolic blood pressure differences. Maximum and minimum previous-week temperature variabilities showed significant but weak relationships with blood pressures. Parameter estimates showed effect modification of negligible magnitude.
Conclusions: This study found significant associations between outdoor temperature and blood pressure levels, which remained after adjustment for various confounders including season. This relationship showed negligible effect modification.
C1 [Kent, Shia T.] Univ Alabama Birmingham, Sch Publ Hlth, Dept Epidemiol, Birmingham, AL 35294 USA.
[Kent, Shia T.; Howard, George; McClure, Leslie A.] Univ Alabama Birmingham, Sch Publ Hlth, Dept Biostat, Birmingham, AL 35294 USA.
[Crosson, William L.] NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA.
[Prineas, Ronald J.] Wake Forest Univ, Bowman Gray Sch Med, Div Publ Hlth Sci, Winston Salem, NC USA.
RP Kent, ST (reprint author), Univ Alabama Birmingham, Sch Publ Hlth, Dept Epidemiol, Birmingham, AL 35294 USA.
EM shia@uab.edu
RI McClure, Leslie/P-2929-2015
FU National Institute of Neurological Disorders and Stroke, National
Institutes of Health, Department of Health and Human Services [U01
NS041588]; NASA
FX This research project is supported by a cooperative agreement U01
NS041588 from the National Institute of Neurological Disorders and
Stroke, National Institutes of Health, Department of Health and Human
Services. The content is solely the responsibility of the authors and
does not necessarily represent the official views of the National
Institute of Neurological Disorders and Stroke or the National
Institutes of Health. Representatives of the funding agency have been
involved in the review of the manuscript but not directly involved in
the collection, management, analysis or interpretation of the data. The
authors acknowledge the participating investigators and institutions for
their valuable contributions: The University of Alabama at Birmingham,
Birmingham, Alabama (Study PI, Statistical and Data Coordinating Center,
Survey Research Unit): George Howard DrPH, Leslie McClure PhD, Virginia
Howard PhD, Libby Wagner MA, Virginia Wadley PhD, Rodney Go PhD, Monika
Safford MD, Ella Temple PhD, Margaret Stewart MSPH, J. David Rhodes BSN;
University of Vermont (Central Laboratory): Mary Cushman MD; Wake Forest
University (ECG Reading Center): Ron Prineas MD, PhD; Alabama
Neurological Institute (Stroke Validation Center, Medical Monitoring):
Camilo Gomez MD, Susana Bowling MD; University of Arkansas for Medical
Sciences (Survey Methodology): LeaVonne Pulley PhD; University of
Cincinnati (Clinical Neuroepidemiology): Brett Kissela MD, Dawn
Kleindorfer MD; Examination Management Services, Incorporated (In-Person
Visits): Andra Graham; Medical University of South Carolina (Migration
Analysis Center): Daniel Lackland DrPH; Indiana University School of
Medicine (Neuropsychology Center): Frederick Unverzagt PhD; National
Institute of Neurological Disorders and Stroke, National Institutes of
Health (funding agency): Claudia Moy PhD. Additional funding, data, data
processing, and consultation were provided by an investigator-initiated
grant-in-aid from NASA. NASA did not have any role in the design and
conduct of the study, the collection, management, analysis, and
interpretation of the data or the preparation or approval of the
manuscript. The manuscript was sent to NASA Marshall Space Flight Center
for review prior to submission for publication.
NR 40
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U2 5
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1476-069X
J9 ENVIRON HEALTH-GLOB
JI Environ. Health
PD JAN 19
PY 2011
VL 10
AR 7
DI 10.1186/1476-069X-10-7
PG 12
WC Environmental Sciences; Public, Environmental & Occupational Health
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health
GA 714RJ
UT WOS:000286826400001
PM 21247466
ER
PT J
AU Thompson, TW
Ustinov, EA
Heggy, E
AF Thompson, Thomas W.
Ustinov, Eugene A.
Heggy, Essam
TI Modeling radar scattering from icy lunar regoliths at 13 cm and 4 cm
wavelengths
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID SOUTH-POLE; GALILEAN SATELLITES; 70-CM WAVELENGTH; WATER ICE; MOON;
IMAGES; ANOMALIES; MERCURY; SURFACE; MARS
AB Two orbital synthetic aperture radars (SARs), the Chandrayaan-1 Mini-SAR (13 cm wavelength) and the Lunar Reconnaissance Orbiter (LRO) Mini-RF (13 and 4.2 cm wavelengths), have been imaging the lunar surface searching for ice deposits in the polar permanently shadowed areas. To understand the radar signatures of lunar polar ices, an empirical two-component model with parametric variations of the specular and diffuse components was developed and validated. This model estimates scattering differences associated with slopes, surface roughness, thin regolith over ice, and patches of ice. Lunar radar backscatter cross sections for the average surface for the Chandrayaan-1 and LRO instruments are estimated from the radar cross sections from the Moon at 3.8, 23, and 68 cm wavelengths measured in the 1960s at the Massachusetts Institute of Technology. This modeling predicts that enhanced diffuse scattering from near-surface ice can be separated from rocks if the scattering is characterized by both the high reflectivity and circular polarization ratios (CPRs) like those observed on Mercury, Mars, and the Galilean satellites. Scattering from near-surface ices covered by a thin regolith can be separated from rocks if the enhancement is twice the average or more. If, however, the lunar ice is dispersed throughout the regolith as ice-filling pores, then scattering differences might be too small to detect. Preliminary validation using LRO radar data for a few polar and midlatitude craters indicate that the observed CPRs are consistent with our models for different regolith ice and roughness conditions.
C1 [Thompson, Thomas W.; Ustinov, Eugene A.; Heggy, Essam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Thompson, TW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM thomas.w.thompson@jpl.nasa.gov
RI Heggy, Essam/E-8250-2013; Ustinov, Eugene/D-1350-2015
OI Heggy, Essam/0000-0001-7476-2735; Ustinov, Eugene/0000-0003-0227-4286
FU NASA
FX The authors thank the Chandrayaan-1 and LRO Mini-SAR teams at Johns
Hopkins Applied Physics Laboratory for superb operation and science
support of the instruments. Comments by two anonymous reviewers were
invaluable in the preparation of a revised manuscript. The authors also
thank the Lunar and Planetary Institute and the Astromaterials Group at
the NASA Johnson Space Center for their support of the dielectric
constant measurements of basalt dust mixtures. Research by one of us
(EH) was carried out at the Lunar and Planetary Institute and at the
Institut de Physique du Globe de Paris and was sponsored by NASA
Planetary Geology and Geophysics Program. This research was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
NR 42
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U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JAN 19
PY 2011
VL 116
AR E01006
DI 10.1029/2009JE003368
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 710OA
UT WOS:000286519900001
ER
PT J
AU Kassi, S
Leshchishina, O
Gordon, IE
Yu, SS
Campargue, A
AF Kassi, Samir
Leshchishina, Olga
Gordon, Iouli E.
Yu, Shanshan
Campargue, Alain
TI Hyperfine structure of the a(1)Delta(g) - X-3 Sigma(-)(g) transitions of
(OO)-O-16-O-17, (OO)-O-17-O-18 and O-17(2) by CRDS at 80 K
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
ID CAVITY RINGDOWN SPECTROSCOPY; 1.5 MU-M; RESONANCE-SPECTRUM;
ISOTOPOLOGUES; OXYGEN
AB The high sensitivity absorption spectrum of the a(1)Delta(g) - X-3 Sigma(-)(g) band of O-16(17), (OO)-O-17-O-18 and O-17(2) has been recorded by CW-Cavity Ring Down Spectroscopy near 1.27 mu m. The spectra were obtained between 7640 and 7917 cm (1) with a O-17-enriched sample at room temperature and at 80 K. Due to the I = 5/2 nuclear spin of the O-17 atom, the nuclear hyperfine structure of the transitions could be partly resolved at low temperature. The parameter coupling of the nuclear spin to the electronic angular momentum in the a(1)Delta(g) state has been derived for the three studied isotopologues of oxygen. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Kassi, Samir; Leshchishina, Olga; Campargue, Alain] Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France.
[Leshchishina, Olga] Zuev Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634021, Russia.
[Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Yu, Shanshan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Campargue, A (reprint author), Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France.
EM Alain.CAMPARGUE@ujf-grenoble.fr
RI Yu, Shanshan/D-8733-2016
FU ANR [NT09_436466]; National Aeronautics and Space Administration
FX Part of this work was performed at Grenoble University under the ANR
project 'IDEO' (NT09_436466). A portion of this research was performed
at Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
NR 21
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U1 0
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2614
EI 1873-4448
J9 CHEM PHYS LETT
JI Chem. Phys. Lett.
PD JAN 18
PY 2011
VL 502
IS 1-3
BP 37
EP 41
DI 10.1016/j.cplett.2010.12.017
PG 5
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 703PY
UT WOS:000285992600005
ER
PT J
AU Roberts, LC
Bradford, LW
AF Roberts, Lewis C., Jr.
Bradford, L. William
TI Improved models of upper-level wind for several astronomical
observatories
SO OPTICS EXPRESS
LA English
DT Article
ID STATISTICS; TURBULENCE; TELESCOPE; SYSTEMS
AB An understanding of wind speed and direction as a function of height are critical to the proper modeling of atmospheric turbulence. We have used radiosonde data from launch sites near significant astronomical observatories and created mean profiles of wind speed and direction and have also computed Richardson number profiles. Using data from the last 30 years, we extend the 1977 Greenwood wind profile to include parameters that show seasonal variations and differences in location. The added information from our models is useful for the design of adaptive optics systems and other imaging systems. Our analysis of the Richardson number suggests that persistent turbulent layers may be inferred when low values are present in our long term averaged data. Knowledge of the presence of these layers may help with planning for adaptive optics and laser communications. (C) 2011 Optical Society of America
C1 [Roberts, Lewis C., Jr.] CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA.
[Bradford, L. William] Pacific Def Solut, Kihei, HI 96753 USA.
RP Roberts, LC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91009 USA.
EM lewis.c.roberts@jpl.nasa.gov
FU Air Force Office of Scientific Research; Air Force Research Laboratory's
Directed Energy Directorate; National Aeronautics and Space
Administration
FX This research was funded by the Air Force Office of Scientific Research
and by the Air Force Research Laboratory's Directed Energy Directorate.
A portion of the research in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
Radiosonde data were obtained from the Wyoming Weather Web, maintained
by the Department of Atmospheric Science of the University of Wyoming.
NR 24
TC 2
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U1 0
U2 2
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD JAN 17
PY 2011
VL 19
IS 2
BP 820
EP 837
DI 10.1364/OE.19.000820
PG 18
WC Optics
SC Optics
GA 707US
UT WOS:000286314600043
PM 21263622
ER
PT J
AU Xu, F
Davis, AB
West, RA
Esposito, LW
AF Xu, Feng
Davis, Anthony B.
West, Robert A.
Esposito, Larry W.
TI Markov chain formalism for polarized light transfer in plane-parallel
atmospheres, with numerical comparison to the Monte Carlo method
SO OPTICS EXPRESS
LA English
DT Article
ID VECTOR RADIATIVE-TRANSFER; DISCRETE-ORDINATE METHOD; SUCCESSIVE ORDER;
SCATTERING MODEL; TRANSFER CODE; MISSION; INTENSITY; RETRIEVAL;
AEROSOLS; MEDIA
AB Building on the Markov chain formalism for scalar (intensity only) radiative transfer, this paper formulates the solution to polarized diffuse reflection from and transmission through a vertically inhomogeneous atmosphere. For verification, numerical results are compared to those obtained by the Monte Carlo method, showing deviations less than 1% when 90 streams are used to compute the radiation from two types of atmospheres, pure Rayleigh and Rayleigh plus aerosol, when they are divided into sublayers of optical thicknesses of less than 0.03. (C) 2011 Optical Society of America
C1 [Xu, Feng; Davis, Anthony B.; West, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Esposito, Larry W.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
RP Xu, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM feng.xu@jpl.nasa.gov
RI Xu, Feng/G-3673-2013
FU National Aeronautics and Space Administration; Jet Propulsion Laboratory
(JPL)
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. F. Xu
is supported by an appointment to the NASA Postdoctoral Program (NPP) at
the Jet Propulsion Laboratory (JPL); the NPP is administered by Oak
Ridge Associated Universities under contract with NASA. We thank Michael
Garay for providing some successive orders of scattering results for
benchmarking in the early stage of this project. The whole "(Vector)
Radiative Transfer" task force at JPL is also acknowledged for lively
discussions on a weekly basis. Copyright 2010. All rights reserved.
NR 26
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U1 0
U2 1
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD JAN 17
PY 2011
VL 19
IS 2
BP 946
EP 967
DI 10.1364/OE.19.000946
PG 22
WC Optics
SC Optics
GA 707US
UT WOS:000286314600055
PM 21263634
ER
PT J
AU Dolan, KA
Hurtt, GC
Chambers, JQ
Dubayah, RO
Frolking, S
Masek, JG
AF Dolan, Katelyn A.
Hurtt, George C.
Chambers, Jeffrey Q.
Dubayah, Ralph O.
Frolking, Steve
Masek, Jeffrey G.
TI Using ICESat's Geoscience Laser Altimeter System (GLAS) to assess
large-scale forest disturbance caused by hurricane Katrina
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE GLAS; Hurricane Katrina; Lidar; ICESat; Forest disturbance
ID US CARBON SINK; ABOVEGROUND BIOMASS; VERTICAL STRUCTURE; TEMPERATE
FOREST; LIDAR DATA; HEIGHT; VEGETATION; FOOTPRINT; IMPACTS; MODELS
AB In 2005, hurricane Katrina resulted in a large disturbance to U.S. forests. Recent estimates of damage from hurricane Katrina have relied primarily on optical remote sensing and field data. This paper is the first large-scale study to use satellite-based lidar data to quantify changes in forest structure from that event. GLAS data for the years prior to and following hurricane Katrina were compared to wind speed, forest cover, and damage data to assess the adequacy of sensor sampling, and to estimate changes in Mean Canopy Height (MCH) over all areas that experienced tropical force winds and greater. Statistically significant decreases in MCH post-Katrina were found to increase with wind intensity: Tropical Storm Delta MCH = -0.5 m, Category 1 Delta MCH = -2 m, and Category 2 Delta MCH = -4 m. A strong relationship was also found between changes in non-photosynthetic vegetation (Delta NPV), a metric previously shown to be related to storm damage, and post-storm MCH. The season of data acquisition was shown to influence calculations of MCH and MCH loss, but did not preclude the detection of major large-scale patterns of damage. Results from this study show promise for using space-borne lidar for large-scale assessments of forest disturbance, and highlight the need for future data on vegetation structure from space. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Dolan, Katelyn A.; Hurtt, George C.] Univ New Hampshire, Inst Study Earth Oceans, Durham, NH 03824 USA.
[Chambers, Jeffrey Q.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA.
[Hurtt, George C.; Dubayah, Ralph O.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Frolking, Steve] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Dolan, KA (reprint author), Univ New Hampshire, Inst Study Earth Oceans, Durham, NH 03824 USA.
EM kdolan@unh.edu
RI Hurtt, George/A-8450-2012; Masek, Jeffrey/D-7673-2012; Chambers,
Jeffrey/J-9021-2014
OI Chambers, Jeffrey/0000-0003-3983-7847
FU NASA-UNH Research and Discover; NASA
FX We thank M. A. Lefsky and J.P. Fisk for their time and help on this
research. KAD was supported by graduate fellowships from the NASA-UNH
Research and Discover and NASA Earth and Space Science Fellowship
programs. GCH, SF, and RD were supported by NASA Terrestrial Ecology and
Interdisciplinary Science Programs.
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U1 1
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD JAN 17
PY 2011
VL 115
IS 1
BP 86
EP 96
DI 10.1016/j.rse.2010.08.007
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 685YH
UT WOS:000284663500008
ER
PT J
AU Kulikov, I
Mannucci, AJ
Pi, XQ
Raymond, C
Hajj, GA
AF Kulikov, Igor
Mannucci, Anthony J.
Pi, Xiaoqing
Raymond, Carol
Hajj, George A.
TI Electron density retrieval from occulting GNSS signals using a
gradient-aided inversion technique
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Radio occultation; Electron density data retrieval
ID RADIO OCCULTATION MEASUREMENTS; GLOBAL-POSITIONING-SYSTEM; GPS;
IONOSPHERE; PROFILES; MAPS; PERFORMANCE; RECEIVER; CHAMP; MODEL
AB In the coming years, opportunities for remote sensing of electron density in the Earth's ionosphere will expand with the advent of Galileo, which will become part of the global navigation satellite system (GNSS). Methods for accurate electron density retrieval from radio occultation data continue to improve. We describe a new method of electron density retrieval using total electron content measurements obtained in low Earth orbit. This method can be applied to data from dual-frequency receivers tracking the GPS or Galileo transmitters. This simulation study demonstrates that the method significantly improves retrieval accuracy compared to the standard Abel inversion approach that assumes a spherically symmetric ionosphere. Our method incorporates horizontal gradient information available from global maps of Total Electron Content (TEC), which are available from the International GNSS Service (IGS) on a routine basis. The combination of ground and space measurements allows us to improve the accuracy of electron density profiles near the occultation tangent point in the E and F regions of the ionosphere. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Kulikov, Igor; Mannucci, Anthony J.; Pi, Xiaoqing; Raymond, Carol] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hajj, George A.] RBS Sempra Commod, Stamford, CT USA.
RP Kulikov, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Igor.K.Kulikov@jpl.nasa.gov
FU National Aeronautics and Space Administration [101248 700 R
622.74.10.24]
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Sponsorship of NASA Earth Surface
and Interior Focus Area program (Grant No. 101248 700 R 622.74.10.24) is
gratefully acknowledged.
NR 43
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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 JAN 15
PY 2011
VL 47
IS 2
BP 289
EP 295
DI 10.1016/j.asr.2010.07.002
PG 7
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 718ET
UT WOS:000287104600013
ER
PT J
AU Vernieres, G
Jones, CKRT
Ide, K
AF Vernieres, Guillaume
Jones, Christopher K. R. T.
Ide, Kayo
TI Capturing eddy shedding in the Gulf of Mexico from Lagrangian
observations
SO PHYSICA D-NONLINEAR PHENOMENA
LA English
DT Article
DE Lagrangian data assimilation; Inverse method; Ensemble Kalman filter
ID ENSEMBLE KALMAN FILTER; DATA ASSIMILATION; LOOP CURRENT; MODEL;
INVERSION; FORECAST
AB The nonlinear process of eddy shedding is studied in the context of the Gulf of Mexico. We show that model runs which do not include eddy detachment can reproduce such an event with the assimilation of suitable data obtained from a control run with eddy detachment. This works surprisingly well and with small amounts of data provided the data originates from instruments that are carried by the flow, i.e. Lagrangian. This is compared with analogous assimilation of data from fixed stations which capture the eddy poorly. The remarkable efficacy of Lagrangian data assimilation in this context is explained by considering the structure of the correlation functions and their associated regions of influence. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Vernieres, Guillaume] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Vernieres, Guillaume] Sci Applicat Int Corp, Beltsville, MD 20705 USA.
[Jones, Christopher K. R. T.] Univ N Carolina, Dept Math, Chapel Hill, NC 27599 USA.
[Ide, Kayo] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
RP Vernieres, G (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Mail Code 610-1, Greenbelt, MD 20771 USA.
EM guillaume.vernieres-1@nasa.gov
RI Ide, Kayo/F-8443-2010
FU Office of Naval Research [N000140910418, N000140910986, N000140910235]
FX The research of Kayo Ide was supported by the Office of Naval Research
under grant number N000140910418. The research of Guillame Vernieres and
Christopher Jones was supported by the Office of Naval research under
grants N000140910986 and N000140910235.
NR 28
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U1 0
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-2789
J9 PHYSICA D
JI Physica D
PD JAN 15
PY 2011
VL 240
IS 2
BP 166
EP 179
DI 10.1016/j.physd.2010.06.008
PG 14
WC Mathematics, Applied; Physics, Multidisciplinary; Physics, Mathematical
SC Mathematics; Physics
GA 709BA
UT WOS:000286409000007
ER
PT J
AU Smialek, JL
AF Smialek, James L.
TI Hydrogen and moisture-induced scale spallation: Cathodic descaling of a
single crystal superalloy
SO ELECTROCHIMICA ACTA
LA English
DT Article; Proceedings Paper
CT 8th International-Society-of-Electrochemistry Spring Meeting
CY MAY 02-05, 2010
CL Ohio State Univ, Columbus, OH
SP Int Soc Electrochem
HO Ohio State Univ
DE Superalloys; Alumina scales; Moisture; Hydrogen embrittlement; Sulfur
segregation
ID WATER-VAPOR; FRACTURE-RESISTANCE; OXIDATION BEHAVIOR; SULFUR
SEGREGATION; CRACK-PROPAGATION; ALUMINA; INTERFACES; STRENGTH; FATIGUE;
ALPHA-AL2O3
AB Moisture-induced delayed spallation (MIDS) of protective alumina scales at room temperature is a well known phenomenon. One mechanism proposes that water and Al-alloy react, produce hydrogen at the scale-metal interface, and enable spallation. To test this mechanism, preoxidized samples of a single crystal superalloy, Rene'N5 + Y, were subjected to standard cathodic hydrogen charging treatments known to produce hydrogen embrittlement in bulk Ni and Ni3Al alloys. Cathodic hydrogen charging, at < 1 mA and an estimated -0.45V SCE, stripped the scales at the oxide-metal interface, resulting in an initial loss of similar to 3 mg/cm(2) and little additional change with time. This was supported by macro-photos and SEM of the spalled surface. On the other hand. anodic polarization at < 1 mA produced less, but steady, linear weight loss (0.3 mg/cm(2)), primarily by anodic dissolution of the metal. Hydrogen charging was thus shown to be detrimental to the alumina scale-metal bond, supporting the hydrogen factor in MIDS. These and other MIDS results show remarkable similarities to embrittlement of Ni subject to hydrogen charging at similar potentials and varying amounts of interfacial (grain boundary) sulfur segregation. The MIDS phenomenon is also discussed in terms of comparative static corrosion fatigue characteristics. It is not necessarily related to other diverse moisture effects occurring at high temperature. Published by Elsevier Ltd.
C1 NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Smialek, JL (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
EM james.l.smialek@nasa.gov
NR 48
TC 6
Z9 6
U1 1
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0013-4686
J9 ELECTROCHIM ACTA
JI Electrochim. Acta
PD JAN 15
PY 2011
VL 56
IS 4
SI SI
BP 1823
EP 1834
DI 10.1016/j.electacta.2010.09.072
PG 12
WC Electrochemistry
SC Electrochemistry
GA 729LP
UT WOS:000287951600018
ER
PT J
AU Du, K
Rood, MJ
Welton, EJ
Varma, RM
Hashmonay, RA
Kim, BJ
Kemme, MR
AF Du, Ke
Rood, Mark J.
Welton, Ellsworth J.
Varma, Ravi M.
Hashmonay, Ram A.
Kim, Byung J.
Kemme, Michael R.
TI Optical Remote Sensing To Quantify Fugitive Particulate Mass Emissions
from Stationary Short-Term and Mobile Continuous Sources: Part I. Method
and Examples
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID DUST; VISIBILITY
AB The emissions of particulate matter (PM) from anthropogenic sources raise public concern. A new method is described here that was developed to complete in situ rapid response measurements of PM mass emissions from fugitive dust sources by use of optical remote sensing (ORS) and an anemometer. The ORS system consists of one ground-based micropulse light detection and ranging (MPL) device that was mounted on a positioner, two open path-Fourier transform infrared (OP-FTIR) spectrometers, and two open path-laser transmissometers (OP-LT). An algorithm was formulated to compute PM light extinction profiles along each of the plume's cross sections that were determined with the MPL Size-specific PM mass emission factors were then calculated by integrating the light extinction profiles with particle mass extinction efficiencies (determined with the OP-FTIRs/OP-LTs) and the wind's speed and direction. This method also quantifies the spatial and temporal variability of the plume's PM mass concentrations across each of the plume's cross sections. Example results from three field studies are also described to demonstrate how this new method is used to determine mass emission factors as well as characterize the dust plumes' horizontal and vertical dimensions
C1 [Du, Ke] Chinese Acad Sci, Inst Urban Environm, Xiamen, Peoples R China.
[Rood, Mark J.] Univ Illinois, Dept Civil & Environm Engn, Urbana, IL 61801 USA.
[Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Varma, Ravi M.] Natl Inst Technol Calicut, Dept Phys, Calicut 673601, Kerala, India.
[Hashmonay, Ram A.] Environ, Chapel Hill, NC 27514 USA.
[Kim, Byung J.; Kemme, Michael R.] US Army, Construct Engn Res Lab, Engn Res & Dev Ctr, Champaign, IL 61826 USA.
RP Du, K (reprint author), Chinese Acad Sci, Inst Urban Environm, Xiamen, Peoples R China.
EM kdu@iue.ac.cn
RI Du, Ke/A-6649-2012; Welton, Ellsworth/A-8362-2012; Varma,
Ravi/A-9640-2009
FU Strategic Environmental Research and Development Program [SI-1400];
Fujian Science and Technology Commission [2010Y0056]; Xiamen
Distinguished Young Scholar Award [3502Z20105008]; NSFC [41005081]
FX The authors thank the supporting staff from Yuma Proving Ground and
Yakima Training Center for coordinating the field campaigns, and the
following agencies that provided funds/support for this research:
Strategic Environmental Research and Development Program (Project
SI-1400), Fujian Science and Technology Commission (No. 2010Y0056),
Xiamen Distinguished Young Scholar Award (No. 3502Z20105008), and the
NSFC (No. 41005081).
NR 19
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U1 1
U2 21
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD JAN 15
PY 2011
VL 45
IS 2
BP 658
EP 665
DI 10.1021/es101904q
PG 8
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 704YB
UT WOS:000286090500050
PM 21142142
ER
PT J
AU Duraj, SA
Hepp, AF
Woloszynek, R
Protasiewicz, JD
Dequeant, M
Ren, T
AF Duraj, Stan A.
Hepp, Aloysius F.
Woloszynek, Robert
Protasiewicz, John D.
Dequeant, Michael
Ren, Tong
TI Synthesis of two new group 13 benzoato-chloro complexes: A structural
study of gallium and indium chelating carboxylates
SO INORGANICA CHIMICA ACTA
LA English
DT Article
DE Gallium; Indium; Structure; Benzoate; Carboxylate; Chelate
ID METAL-ORGANIC FRAMEWORKS; COORDINATION CHEMISTRY; CRYSTAL-STRUCTURE;
MOLECULAR-STRUCTURES; LIGAND; TOPOLOGY; ADDUCT;
PYRIDINE-2,6-BIS(ACETYLOXIME); DECOMPOSITION; DEPOSITION
AB Two new heteroleptic chelated-benzoato gallium (III) and indium (III) complexes have been prepared and structurally characterized. The molecular structures of [GaCl(2)(4-Mepy)(2)(O(2)CPh)]center dot 4-Mepy (1) and [InCl(4-Mepy) (2)(O(2)CPh)(2)]center dot 4-Mepy (2) have been determined by single-crystal X-ray diffraction. The gallium compound (1) is a distorted octahedron with cis-chloride ligands co-planar with the chelating benzoate and the 4-methylpyridines trans to each other. This is the first example of a Ga(III) structure with a chelating benzoate. The indium compound (2) is a distorted pentagonal bipyramid with two chelating benzoates, one 4-methylpyridine in the plane and a chloride trans to the other 4-methylpyridine. The indium bis-benzoate is an unusual example of a seven-coordinate structure with classical ligands. Both complexes, which due to the chelates, could also be described as pseudo-trigonal bipyramidal, include a three-bladed motif with three roughly parallel aromatic rings that along with a solvent of crystallization and electron-withdrawing chloride ligand(s) stabilize the solid-state structures. Published by Elsevier B.V.
C1 [Duraj, Stan A.] Cleveland State Univ, Dept Chem, Cleveland, OH 44115 USA.
[Hepp, Aloysius F.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Woloszynek, Robert; Protasiewicz, John D.] Case Western Reserve Univ, Dept Chem, Cleveland, OH 44106 USA.
[Dequeant, Michael] Hendrix Coll, Dept Chem, Conway, AR 72032 USA.
[Ren, Tong] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
RP Duraj, SA (reprint author), Cleveland State Univ, Dept Chem, Cleveland, OH 44115 USA.
EM duraj@csuohio.edu; Aloysius.F.Hepp@nasa.gov; protasiewicz@case.edu;
dequeant@hendrix.edu
RI Protasiewicz, John/C-3484-2008
FU Cleveland State University; NASA Glenn Research Center; Department of
Chemistry, Case Western Reserve University; Department of Chemistry at
University of Miami Coral Gables
FX S.A. Duraj thanks Cleveland State University for support during a
sabbatical at Case Western Reserve University. A.F. Hepp acknowledges
support from the NASA Glenn Research Center's Internal Research and
Development Fund. S.A. Duraj, R.A. Woloszynek, and J.D. Protasiewicz
acknowledge support from the Department of Chemistry, Case Western
Reserve University. M. Dequeant and T. Ren acknowledge support from the
Department of Chemistry at University of Miami Coral Gables, FL where
the structural data were collected and solved.
NR 62
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U1 0
U2 14
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0020-1693
J9 INORG CHIM ACTA
JI Inorg. Chim. Acta
PD JAN 15
PY 2011
VL 365
IS 1
BP 54
EP 60
DI 10.1016/j.ica.2010.08.026
PG 7
WC Chemistry, Inorganic & Nuclear
SC Chemistry
GA 698WF
UT WOS:000285624200008
ER
PT J
AU Dickey, JO
Marcus, SL
de Viron, O
AF Dickey, Jean O.
Marcus, Steven L.
de Viron, Olivier
TI Air Temperature and Anthropogenic Forcing: Insights from the Solid Earth
SO JOURNAL OF CLIMATE
LA English
DT Article
ID ANGULAR-MOMENTUM; TORSIONAL OSCILLATIONS; CLIMATE SIMULATIONS;
SURFACE-TEMPERATURE; CORE; ROTATION; MODELS; LENGTH; SERIES; SYSTEM
AB Earth's rotation rate [i.e., length of day (LOD)], the angular momentum of the core (CAM), and surface air temperature (SAT) all have decadal variability. Previous investigators have found that the LOD fluctuations are largely attributed to core mantle interactions and that the SAT is strongly anticorrelated with the decadal LOD. It is shown here that 1) the correlation among these three quantities exists until 1930, at which time anthropogenic forcing becomes highly significant; 2) correcting for anthropogenic effects, the correlation is present for the full span with a broadband variability centered at 78 yr; and 3) this result underscores the reality of anthropogenic temperature change, its size, and its temporal growth. The cause of this common variability needs to be further investigated and studied. Since temperature cannot affect the CAM or LOD to a sufficient extent, the results favor either a direct effect of Earth's core-generated magnetic field (e.g., through the modulation of charged-particle fluxes, which may impact cloud formation) or a more indirect effect of some other core process on the climate-or yet another process that affects both. In all three cases, their signals would be much smaller than the anthropogenic greenhouse gas effect on Earth's radiation budget during the coming century.
C1 [Dickey, Jean O.; Marcus, Steven L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[de Viron, Olivier] Univ Paris Diderot, Paris, France.
[de Viron, Olivier] Inst Phys Globe, Paris, France.
RP Dickey, JO (reprint author), CALTECH, Jet Prop Lab, MS 238-600,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jean.dickey@jpl.nasa.gov
RI de Viron, Olivier/N-6647-2014;
OI de Viron, Olivier/0000-0003-3112-9686; Marcus,
Steven/0000-0002-5763-6961
FU National Aeronautics and Space Administration (NASA)
FX This paper is dedicated to Professor Raymond Hide on the occasion of his
80th birthday; we thank Ray for his mentoring and advice and for
igniting our interest in Earth's core. We gratefully acknowledge
Professor George Philander for insightful discussions, Jim Hansen and
colleagues for the GISS data set, Tim Johns for providing the HadCM3
data set, and Peter Stott and Gareth Jones for providing the HadGEM1
data set. The authors also thank the editor Anthony J. Broccoli and
three anonymous reviewers whose comments greatly improved this paper.
This paper presents the results of one phase of research carried out at
the Jet Propulsion Laboratory, California Institute of Technology,
sponsored by the National Aeronautics and Space Administration (NASA).
The contribution of author OdV to this work is IPGP contribution 3063.
NR 30
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U1 0
U2 0
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD JAN 15
PY 2011
VL 24
IS 2
BP 569
EP 574
DI 10.1175/2010JCLI3500.1
PG 6
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 716VR
UT WOS:000287002100016
ER
PT J
AU Stefszky, M
Mow-Lowry, CM
McKenzie, K
Chua, S
Buchler, B
Symul, T
McClelland, DE
Lam, PK
AF Stefszky, Michael
Mow-Lowry, Conor M.
McKenzie, Kirk
Chua, Sheon
Buchler, Ben C.
Symul, Thomas
McClelland, David E.
Lam, Ping Koy
TI An investigation of doubly-resonant optical parametric oscillators and
nonlinear crystals for squeezing
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
ID 2ND-HARMONIC GENERATION; QUANTUM CRYPTOGRAPHY; WEDGED CRYSTAL; LIGHT;
KTIOPO4; SYSTEMS; NOISE
AB A squeezed light source requires properties such as high squeezing amplitude, high bandwidth and stability over time, ideally using as few resources, such as laser power, as possible. We compare three nonlinear materials, two of which have not been well characterized for squeezed state production, and also investigate the viability of doubly-resonant optical parametric oscillator cavities in achieving these requirements. A model is produced that provides a new way of looking at the construction of an optical parametric oscillator/optical parametric amplifier setup where second harmonic power is treated as a limited resource. The well-characterized periodically poled potassium titanyl phosphate (PPKTP) is compared in an essentially identical setup to two relatively new materials, periodically poled stoichiometric lithium tantalate (PPSLT) and 1.7% magnesium oxide doped periodically poled stoichiometric lithium niobate (PPSLN). Although from the literature PPSLT and PPSLN present advantages such as a higher damage threshold and a higher nonlinearity, respectively, PPKTP was still found to have the most desirable properties. With PPKTP, 5.8 dB of squeezing below the shot noise limit was achieved. With PPSLT, 5.0 dB of squeezing was observed but the power required to see this squeezing was much higher than expected. A technical problem with the PPSLN limited the observed squeezing to around 1.0 dB. This problem is discussed.
C1 [Stefszky, Michael; Buchler, Ben C.; Symul, Thomas; Lam, Ping Koy] Australian Natl Univ, Quantum Opt Grp, Dept Quantum Sci, Canberra, ACT 0200, Australia.
[Stefszky, Michael; Mow-Lowry, Conor M.; McKenzie, Kirk; Chua, Sheon; McClelland, David E.] Australian Natl Univ, Dept Quantum Sci, Ctr Gravitat Phys, Canberra, ACT 0200, Australia.
[McKenzie, Kirk] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Stefszky, M (reprint author), Australian Natl Univ, Quantum Opt Grp, Dept Quantum Sci, GPO Box 4, Canberra, ACT 0200, Australia.
EM michael.stefszky@anu.edu.au
RI McClelland, David/E-6765-2010; Symul, Thomas/G-3764-2010; Lam, Ping
Koy/A-5276-2008; Mow-Lowry, Conor/F-8843-2015; Buchler, Ben/D-4581-2009
OI McClelland, David/0000-0001-6210-5842; Lam, Ping
Koy/0000-0002-4421-601X; Buchler, Ben/0000-0002-2852-7483
FU Australian Research Council
FX We acknowledge financial support from the Australian Research Council.
NR 43
TC 9
Z9 9
U1 2
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD JAN 14
PY 2011
VL 44
IS 1
AR 015502
DI 10.1088/0953-4075/44/1/015502
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 696PT
UT WOS:000285454600013
ER
PT J
AU Aghedo, AM
Bowman, KW
Worden, HM
Kulawik, SS
Shindell, DT
Lamarque, JF
Faluvegi, G
Parrington, M
Jones, DBA
Rast, S
AF Aghedo, A. M.
Bowman, K. W.
Worden, H. M.
Kulawik, S. S.
Shindell, D. T.
Lamarque, J. F.
Faluvegi, G.
Parrington, M.
Jones, D. B. A.
Rast, S.
TI The vertical distribution of ozone instantaneous radiative forcing from
satellite and chemistry climate models
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPOSPHERIC EMISSION SPECTROMETER; LOWER STRATOSPHERE; ZONAL STRUCTURE;
LIGHTNING NOX; TROPICAL O-3; PREINDUSTRIAL; SIMULATIONS; IMPACT;
TEMPERATURE; VARIABILITY
AB We evaluate the instantaneous radiative forcing (IRF) of tropospheric ozone predicted by four state-of-the-art global chemistry climate models (AM2-Chem, CAM-Chem, ECHAM5-MOZ, and GISS-PUCCINI) against ozone distribution observed from the NASA Tropospheric Emission Spectrometer (TES) during August 2006. The IRF is computed through the application of an observationally constrained instantaneous radiative forcing kernels (IRFK) to the difference between TES and model-predicted ozone. The IRFK represent the sensitivity of outgoing longwave radiation to the vertical and spatial distribution of ozone under all-sky condition. Through this technique, we find total tropospheric IRF biases from -0.4 to + 0.7 W/m(2) over large regions within the tropics and midlatitudes, due to ozone differences over the region in the lower and middle troposphere, enhanced by persistent bias in the upper troposphere-lower stratospheric region. The zonal mean biases also range from -30 to + 50 mW/m(2) for the models. However, the ensemble mean total tropospheric IRF bias is less than 0.2 W/m(2) within the entire troposphere.
C1 [Aghedo, A. M.; Bowman, K. W.; Kulawik, S. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Worden, H. M.; Lamarque, J. F.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Shindell, D. T.; Faluvegi, G.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Parrington, M.; Jones, D. B. A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Rast, S.] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
RP Aghedo, AM (reprint author), CALTECH, Jet Prop Lab, MS 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM adetutu.m.aghedo@jpl.nasa.gov
RI Shindell, Drew/D-4636-2012; Pfister, Gabriele/A-9349-2008; Parrington,
Mark/E-7148-2013; Lamarque, Jean-Francois/L-2313-2014; Jones,
Dylan/O-2475-2014
OI Parrington, Mark/0000-0003-4313-6218; Lamarque,
Jean-Francois/0000-0002-4225-5074; Jones, Dylan/0000-0002-1935-3725
FU NASA ROSES; United States government
FX We appreciate comments from Luca Pozzoli at the Joint Research Centre,
Italy; Martin G. Schultz at ICG-2, Research Centre, Julich, Germany;
Larry Horowitz at NOAA Geophysical Fluid Dynamics Laboratory, Princeton,
New Jersey, United States; and colleagues in the Tropospheric Emission
Spectrometer group, Jet Propulsion Laboratory, California Institute of
Technology, Pasadena, California, United States. A. M. A. thanks Heidi
Lorenz-Wirzba of the supercomputing group at JPL and also Louis
Kornblueh, Johann Feichter, Uwe Schulzweida, Erich Roeckner, and Monika
Esch of Max Planck Institute for Meteorology, Hamburg, Germany, for
their support at different stages of porting, compiling, and running
ECHAM5-MOZ on the JPL supercomputer. The research described in this
paper was partially carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a NASA ROSES contract received
by K. W. B. and H. M. W. United States government sponsorship
acknowledged.
NR 84
TC 17
Z9 17
U1 1
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 JAN 13
PY 2011
VL 116
AR D01305
DI 10.1029/2010JD014243
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 707XP
UT WOS:000286324900001
ER
PT J
AU Neish, CD
Bussey, DBJ
Spudis, P
Marshall, W
Thomson, BJ
Patterson, GW
Carter, LM
AF Neish, C. D.
Bussey, D. B. J.
Spudis, P.
Marshall, W.
Thomson, B. J.
Patterson, G. W.
Carter, L. M.
TI The nature of lunar volatiles as revealed by Mini-RF observations of the
LCROSS impact site
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID COHERENT-BACKSCATTER; POLAR-REGIONS; RADAR IMAGES; WATER ICE; DEPOSITS;
ARECIBO; POLES; POLARIZATION; SURFACES; MOON
AB On 9 October 2009 the Lunar Crater Observation and Sensing Satellite (LCROSS) impacted Cabeus crater, located near the south pole of the Moon. Prior to that impact, the Mini-RF instruments on ISRO's Chandrayaan-1 and NASA's Lunar Reconnaissance Orbiter (LRO) obtained S band (12.6 cm) synthetic aperture radar images of the impact site at 150 and 30 m resolution, respectively. These observations show that the floor of Cabeus has a circular polarization ratio (CPR) comparable to or less than the average of nearby terrain in the southern lunar highlands. Furthermore, <2% of the pixels in Cabeus crater have CPR values greater than unity. This observation is not consistent with the presence of thick deposits of nearly pure water ice within a few meters of the lunar surface, but it does not rule out the presence of small ( C(6)H(6) + H, under single collision conditions. This reaction portrays the simplest representative of a reaction class in which aromatic molecules with a benzene core can be formed from acyclic precursors via barrierless reactions of ethynyl radicals with substituted 1,3-butadiene molecules. Unique gas-grain astrochemical models imply that this low-temperature route controls the synthesis of the very first aromatic ring from acyclic precursors in cold molecular clouds, such as in the Taurus Molecular Cloud. Rapid, subsequent barrierless reactions of benzene with ethynyl radicals can lead to naphthalene-like structures thus effectively propagating the ethynyl-radical mediated formation of aromatic molecules in the interstellar medium.
C1 [Jones, Brant M.; Zhang, Fangtong; Kaiser, Ralf I.] Univ Hawaii, Dept Chem, Honolulu, HI 96822 USA.
[Jones, Brant M.; Kaiser, Ralf I.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Jamal, Adeel; Mebel, Alexander M.] Florida Int Univ, Dept Chem & Biochem, Miami, FL 33199 USA.
[Cordiner, Martin A.; Charnley, Steven B.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Lanham, MD 20706 USA.
RP Kaiser, RI (reprint author), Univ Hawaii, Dept Chem, Honolulu, HI 96822 USA.
EM ralfk@hawaii.edu
RI Charnley, Steven/C-9538-2012; Mebel, Alexander/A-5234-2009
FU NASA Astrobiology Institute; Goddard Center for Astrobiology; NASA
FX The experimental work and electronic structure calculations were
supported by the chemistry division of the US National Science
Foundation (National Science Foundation Collaborative Research in
Chemistry CHE-0627854). The experiments were supported in part by an
appointment to the National Aeronautics and Space Administration (NASA)
Postdoctoral Program at the NASA Astrobiology Institute, administered by
Oak Ridge Associated Universities (B.M.J.). The chemical modeling work
was supported by the Goddard Center for Astrobiology and the NASA
Exobiology Program.
NR 47
TC 39
Z9 39
U1 7
U2 45
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 JAN 11
PY 2011
VL 108
IS 2
BP 452
EP 457
DI 10.1073/pnas.1012468108
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 704ZU
UT WOS:000286097700008
PM 21187430
ER
PT J
AU Koutroumpa, D
Smith, RK
Edgar, RJ
Kuntz, KD
Plucinsky, PP
Snowden, SL
AF Koutroumpa, Dimitra
Smith, Randall K.
Edgar, Richard J.
Kuntz, Kip D.
Plucinsky, Paul P.
Snowden, Steven L.
TI XMM-NEWTON OBSERVATIONS OF MBM 12: MORE CONSTRAINTS ON THE SOLAR WIND
CHARGE EXCHANGE AND LOCAL BUBBLE EMISSIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: bubbles; ISM: supernova remnants; solar wind; Sun: heliosphere;
X-rays: diffuse background; X-rays: ISM
ID X-RAY-EMISSION; EXTREME-ULTRAVIOLET EMISSION; INTERSTELLAR-MEDIUM;
MOLECULAR CLOUD; HOT BUBBLE; GAS; NEUTRALS; SUZAKU; MAPS; SPECTRA
AB We present the first analysis of an XMM-Newton observation of the nearby molecular cloud MBM 12. We find that in the direction of MBM 12 the total OVII (0.57 keV) triplet emission is 1.8(-0.6)(+0.5) photons cm(-2) s(-1) sr(-1) (or line units, LU) while for the OVIII (0.65 keV) line emission we find a 3 sigma upper limit of < 1 LU. We use a heliospheric model to calculate the OVII and OVIII emission generated by Solar Wind Charge-eXchange (SWCX) which we compare to the XMM-Newton observations. This comparison provides new constraints on the relative heliospheric and Local Bubble contributions to the local diffuse X-ray background. The heliospheric SWCX model predicts 0.82 LU for OVII, which accounts for similar to 46% +/- 15% of the observed value, and 0.33 LU for the OVIII line emission consistent with the XMM-Newton observed value. We discuss our results in combination with previous observations of MBM 12 with Chandra and Suzaku.
C1 [Koutroumpa, Dimitra; Snowden, Steven L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smith, Randall K.; Edgar, Richard J.; Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kuntz, Kip D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Koutroumpa, D (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
RI XRAY, SUZAKU/A-1808-2009
FU NASA [NAS5-00132]; Goddard Space Flight Center
FX We thank the MIT Space Plasma Group (K.W. Ogilvie and A.J. Lazarus) for
the WIND data, and the STEREO/PLASTIC Investigation (A.B. Galvin, PI)
and NASA Contract NAS5-00132 for the PLASTIC Level 2 data used in this
study. We also thank the ACE/SWICS-SWIMS instrument teams (J. Raines, S.
Lepri, and T. Zurbuchen) and the ACE Science Center for providing the
ACE data, and the Ulysses/SWICS team (G. Gloeckler, T. Zurbuchen, and R.
von Steiger) for the Ulysses/SWICS data. Finally, we are grateful to our
referee, Jeffrey Linsky, for his constructive remarks that considerably
improved the manuscript.; This research was supported by an appointment
to the NASA Postdoctoral Program at the Goddard Space Flight Center,
administered by Oak Ridge Associated Universities through a contract
with NASA.
NR 45
TC 22
Z9 22
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2011
VL 726
IS 2
AR 91
DI 10.1088/0004-637X/726/2/91
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698WB
UT WOS:000285623600035
ER
PT J
AU Eplee, RE
Sun, JQ
Meister, G
Patt, FS
Xiong, XX
McClain, CR
AF Eplee, Robert E., Jr.
Sun, Jun-Qiang
Meister, Gerhard
Patt, Frederick S.
Xiong, Xiaoxiong
McClain, Charles R.
TI Cross calibration of SeaWiFS and MODIS using on-orbit observations of
the Moon
SO APPLIED OPTICS
LA English
DT Article
ID VICARIOUS CALIBRATION; LUNAR CALIBRATION; SOLAR; TERRA; AQUA
AB Observations of the Moon provide a primary technique for the on-orbit cross calibration of Earth remote sensing instruments. Monthly lunar observations are major components of the on-orbit calibration strategies of SeaWiFS and MODIS. SeaWiFS has collected more than 132 low phase angle and 59 high phase angle lunar observations over 12 years, Terra MODIS has collected more than 82 scheduled and 297 unscheduled lunar observations over nine years, and AquaMODIS has collected more than 61 scheduled and 171 unscheduled lunar observations over seven years. The NASA Ocean Biology Processing Group Calibration and Validation Team and the NASA MODIS Characterization Support Team use the USGS RObotic Lunar Observatory (ROLO) photometric model of the Moon to compare these time series of lunar observations over time and varying observing geometries. The cross-calibration results show that Terra MODIS and Aqua MODIS agree, band to band, at the 1%-3% level, while SeaWiFS and either MODIS instrument agree at the 3%-8% level. The combined uncertainties of these comparisons are 1.3% for Terra and Aqua MODIS, 1.4% for SeaWiFS and Terra MODIS, and 1.3% for SeaWiFS and Aqua MODIS. Any residual phase dependence in the ROLO model, based on these observations, is less than 1.7% over the phase angle range of -80 degrees to -6 degrees and +5 degrees to +82 degrees. The lunar cross calibration of SeaWiFS, Terra MODIS, and AquaMODIS is consistent with the vicarious calibration of ocean color products for these instruments, with the vicarious gains mitigating the calibration biases for the ocean color bands. (C) 2011 Optical Society of America
C1 [Eplee, Robert E., Jr.; Patt, Frederick S.] Sci Applicat Int Corp, Beltsville, MD 20705 USA.
[Sun, Jun-Qiang] Sigma Space Corp, Lanham, MD 20706 USA.
[Meister, Gerhard; Xiong, Xiaoxiong; McClain, Charles R.] NASA, Hydrospher & Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Eplee, RE (reprint author), Sci Applicat Int Corp, 4600 Powdermill Rd,Suite 400, Beltsville, MD 20705 USA.
EM Robert.E.Eplee@nasa.gov
RI Meister, Gerhard/F-7159-2012
NR 20
TC 28
Z9 29
U1 3
U2 8
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 JAN 10
PY 2011
VL 50
IS 2
BP 120
EP 133
DI 10.1364/AO.50.000120
PG 14
WC Optics
SC Optics
GA 704JT
UT WOS:000286049200001
PM 21221136
ER
PT J
AU Ackermann, M
Ajello, M
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Bloom, ED
Bonamente, E
Borgland, AW
Brandt, TJ
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cecchi, C
Charles, E
Chekhtman, A
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Dermer, CD
de Palma, F
Digel, SW
Drell, PS
Dubois, R
Favuzzi, C
Ferrara, EC
Focke, WB
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashi, K
Hayashida, M
Hughes, RE
Itoh, R
Johannesson, G
Johnson, AS
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lee, SH
Garde, ML
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Makeev, A
Martin, P
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Naumann-Godo, M
Nishino, S
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Parent, D
Pelassa, V
Pepe, M
Pesce-Rollins, M
Piron, F
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Ripken, J
Sada, T
Sadrozinski, HFW
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Strickman, MS
Strong, AW
Suson, DJ
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JB
Thompson, DJ
Tibaldo, L
Torres, DF
Tramacere, A
Uchiyama, Y
Uehara, T
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vilchez, N
Vitale, V
Vladimirov, AE
Waite, AP
Wang, P
Wood, KS
Yang, Z
Ziegler, M
AF Ackermann, M.
Ajello, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Brandt, T. J.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Dermer, C. D.
de Palma, F.
Digel, S. W.
Drell, P. S.
Dubois, R.
Favuzzi, C.
Ferrara, E. C.
Focke, W. B.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashi, K.
Hayashida, M.
Hughes, R. E.
Itoh, R.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lee, S. -H.
Garde, M. Llena
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Makeev, A.
Martin, P.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Naumann-Godo, M.
Nishino, S.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Parent, D.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Ripken, J.
Sada, T.
Sadrozinski, H. F. -W.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Strickman, M. S.
Strong, A. W.
Suson, D. J.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tramacere, A.
Uchiyama, Y.
Uehara, T.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vilchez, N.
Vitale, V.
Vladimirov, A. E.
Waite, A. P.
Wang, P.
Wood, K. S.
Yang, Z.
Ziegler, M.
TI CONSTRAINTS ON THE COSMIC-RAY DENSITY GRADIENT BEYOND THE SOLAR CIRCLE
FROM FERMI gamma-RAY OBSERVATIONS OF THE THIRD GALACTIC QUADRANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; gamma rays: ISM; ISM: general
ID LARGE-AREA TELESCOPE; RADIAL-DISTRIBUTION; MOLECULAR CLOUDS; MILKY-WAY;
CO SURVEY; EGRET OBSERVATIONS; OUTER GALAXY; EMISSION; MONOCEROS; GAS
AB We report an analysis of the interstellar gamma-ray emission in the third Galactic quadrant measured by the Fermi Large Area Telescope. The window encompassing the Galactic plane from longitude 210 degrees to 250 degrees has kinematically well-defined segments of the Local and the Perseus arms, suitable to study the cosmic-ray (CR) densities across the outer Galaxy. We measure no large gradient with Galactocentric distance of the gamma-ray emissivities per interstellar H atom over the regions sampled in this study. The gradient depends, however, on the optical depth correction applied to derive the H I column densities. No significant variations are found in the interstellar spectra in the outer Galaxy, indicating similar shapes of the CR spectrum up to the Perseus arm for particles with GeV to tens of GeV energies. The emissivity as a function of Galactocentric radius does not show a large enhancement in the spiral arms with respect to the interarm region. The measured emissivity gradient is flatter than expectations based on a CR propagation model using the radial distribution of supernova remnants and uniform diffusion properties. In this context, observations require a larger halo size and/or a flatter CR source distribution than usually assumed. The molecular mass calibrating ratio, X-CO = N(H-2)/W-CO, is found to be (2.08 +/- 0.11) x 10(20) cm(-2)(K km s(-1))(-1) in the Local arm clouds and is not significantly sensitive to the choice of Hi spin temperature. No significant variations are found for clouds in the interarm region.
C1 [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vladimirov, A. E.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vladimirov, A. E.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Tibaldo, L.] Univ Paris Diderot, Lab AIM, CEA IRFU, CEA Saclay,CNRS,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brandt, T. J.; Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Brandt, T. J.; Hughes, R. E.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] IEEC CSIC, Inst Ciencies Espai, Barcelona 08193, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Chekhtman, A.; Dermer, C. D.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France.
[Conrad, J.; Garde, M. Llena; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Garde, M. Llena; Ripken, J.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Ferrara, E. C.; Harding, A. K.; McEnery, J. E.; Thompson, D. J.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Itoh, R.; Katagiri, H.; Mizuno, T.; Nishino, S.; Sada, T.; Uehara, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Martin, P.; Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tramacere, A.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA.
[Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Ackermann, M (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
EM isabelle.grenier@cea.fr; mizuno@hep01.hepl.hiroshima-u.ac.jp;
luigi.tibaldo@pd.infn.it
RI Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015;
Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro,
Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016;
Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; McEnery,
Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano,
pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss,
Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer,
Olaf/A-3117-2013; Ozaki, Masanobu/K-1165-2013; Rando,
Riccardo/M-7179-2013; Johnson, Neil/G-3309-2014; Funk,
Stefan/B-7629-2015; Gargano, Fabio/O-8934-2015
OI Loparco, Francesco/0000-0002-1173-5673; Johannesson,
Gudlaugur/0000-0003-1458-7036; Moskalenko, Igor/0000-0001-6141-458X;
Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Giordano, Francesco/0000-0002-8651-2394;
Caraveo, Patrizia/0000-0003-2478-8018; Sgro',
Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X;
Thompson, David/0000-0001-5217-9135; lubrano,
pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553;
giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385;
Funk, Stefan/0000-0002-2012-0080; Gargano, Fabio/0000-0002-5055-6395
FU K. A. Wallenberg Foundation; International Doctorate on Astroparticle
Physics (IDAPP) program; NASA [NNX09AC15G]
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; Partially supported by the
International Doctorate on Astroparticle Physics (IDAPP) program.; This
paper makes use of a development version of GALPROP provided by the
GALPROP team to the LAT collaboration solely for interpretation of the
LAT data. GALPROP development is supported by NASA Grant NNX09AC15G.
NR 51
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2011
VL 726
IS 2
AR 81
DI 10.1088/0004-637X/726/2/81
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698WB
UT WOS:000285623600025
ER
PT J
AU Christiansen, JL
Ballard, S
Charbonneau, D
Deming, D
Holman, MJ
Madhusudhan, N
Seager, S
Wellnitz, DD
Barry, RK
Livengood, TA
Hewagama, T
Hampton, DL
Lisse, CM
A'Hearn, MF
AF Christiansen, Jessie L.
Ballard, Sarah
Charbonneau, David
Deming, Drake
Holman, Matthew J.
Madhusudhan, Nikku
Seager, Sara
Wellnitz, Dennis D.
Barry, Richard K.
Livengood, Timothy A.
Hewagama, Tilak
Hampton, Don L.
Lisse, Carey M.
A'Hearn, Michael F.
TI SYSTEM PARAMETERS, TRANSIT TIMES, AND SECONDARY ECLIPSE CONSTRAINTS OF
THE EXOPLANET SYSTEMS HAT-P-4, TrES-2, TrES-3, and WASP-3 FROM THE NASA
EPOXI MISSION OF OPPORTUNITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; stars: individual (HAT-P-4, WASP-3, TrES-2,
TrES-3)
ID PLANET SYSTEMS; LIGHT CURVES; HOT JUPITER; DEEP IMPACT; ATMOSPHERES;
EMISSION; STELLAR; PROJECT; KEPLER; ORBIT
AB As part of the NASA EPOXI Mission of Opportunity, we observed seven known transiting extrasolar planet systems in order to construct time series photometry of extremely high phase coverage and precision. Here we present the results for four "hot-Jupiter systems" with near-solar stars-HAT-P-4, TrES-3, TrES-2, and WASP-3. We observe 10 transits of HAT-P-4, estimating the planet radius R-p = 1.332 +/- 0.052 R-Jup, the stellar radius R-* = 1.602 +/- 0.061 R-circle dot, the inclination i = 89.67 +/- 0.30 deg, and the transit duration from first to fourth contact tau = 255.6 +/- 1.9 minutes. For TrES-3, we observe seven transits and find R-p = 1.320 +/- 0.057 R-Jup, R-* = 0.817 +/- 0.022 R-circle dot, i = 81.99 +/- 0.30 deg, and tau = 81.9 +/- 1.1 minutes. We also note a long-term variability in the TrES-3 light curve, which may be due to star spots. We observe nine transits of TrES-2 and find R-p = 1.169 +/- 0.034 R-Jup, R-* = 0.940 +/- 0.026 R-circle dot, i = 84.15 +/- 0.16 deg, and tau = 107.3 +/- 1.1 minutes. Finally, we observe eight transits of WASP-3, finding R-p = 1.385 +/- 0.060 R-Jup, R-* = 1.354 +/- 0.056 R-circle dot, i = 84.22 +/- 0.81 deg, and tau = 167.3 +/- 1.3 minutes. We present refined orbital periods and times of transit for each target. We state 95% confidence upper limits on the secondary eclipse depths in our broadband visible bandpass centered on 650 nm. These limits are 0.073% for HAT-P-4, 0.062% for TrES-3, 0.16% for TrES-2, and 0.11% for WASP-3. We combine the TrES-3 secondary eclipse information with the existing published data and confirm that the atmosphere likely does not have a temperature inversion.
C1 [Christiansen, Jessie L.; Ballard, Sarah; Charbonneau, David; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Deming, Drake; Barry, Richard K.; Livengood, Timothy A.; Hewagama, Tilak] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Madhusudhan, Nikku; Seager, Sara] MIT, Cambridge, MA 02159 USA.
[Wellnitz, Dennis D.; Hewagama, Tilak] Univ Maryland, College Pk, MD 20742 USA.
[Hampton, Don L.] Univ Alaska Fairbanks, Fairbanks, AK 99775 USA.
[Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Christiansen, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jchristi@cfa.harvard.edu
RI Wellnitz, Dennis/B-4080-2012; Hewagama, T/C-8488-2012; Livengood,
Timothy/C-8512-2012; Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Charbonneau, David/0000-0002-9003-484X
FU National Aeronautics and Space Administration [NNX08AB64A, NNX08AD05A]
FX Support for this work was provided by the EPOXI Project of the National
Aeronautics and Space Administration's Discovery Program via funding to
the Goddard Space Flight Center, and to Harvard University via
Co-operative Agreement NNX08AB64A, and to the Smithsonian Astrophysical
Observatory via Co-operative Agreement NNX08AD05A. The authors
acknowledge and are grateful for the use of publicly available transit
modeling routines by Eric Agol and Kaisey Mandel, and also the
Levenberg-Marquardt least-squares minimization routine MPFITFUN by Craig
Markwardt. This work has used data obtained by various observers
collected in the Exoplanet Transit Database, http://var.astro.cz/ETD.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2011
VL 726
IS 2
AR 94
DI 10.1088/0004-637X/726/2/94
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698WB
UT WOS:000285623600038
ER
PT J
AU Deming, D
Knutson, H
Agol, E
Desert, JM
Burrows, A
Fortney, JJ
Charbonneau, D
Cowan, NB
Laughlin, G
Langton, J
Showman, AP
Lewis, NK
AF Deming, Drake
Knutson, Heather
Agol, Eric
Desert, Jean-Michel
Burrows, Adam
Fortney, Jonathan J.
Charbonneau, David
Cowan, Nicolas B.
Laughlin, Gregory
Langton, Jonathan
Showman, Adam P.
Lewis, Nikole K.
TI WARM SPITZER PHOTOMETRY OF THE TRANSITING EXOPLANETS CoRoT-1 AND CoRoT-2
AT SECONDARY ECLIPSE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; techniques: photometric
ID PLANET HD 189733B; INFRARED-EMISSION SPECTRUM; IRRADIATED GIANT PLANETS;
EXTRASOLAR PLANET; THERMAL EMISSION; TEMPERATURE INVERSION;
SPACE-TELESCOPE; HOT JUPITERS; LIGHT CURVES; MU-M
AB We measure secondary eclipses of the hot giant exoplanets CoRoT-1 at 3.6 and 4.5 mu m, and CoRoT-2 at 3.6 mu m, both using Warm Spitzer. We find that the Warm Spitzer mission is working very well for exoplanet science. For consistency of our analysis we also re-analyze archival cryogenic Spitzer data for secondary eclipses of CoRoT-2 at 4.5 and 8 mu m. We compare the total data for both planets, including optical eclipse measurements by the CoRoT mission, and ground-based eclipse measurements at 2 mu m, to existing models. Both planets exhibit stronger eclipses at 4.5 than at 3.6 mu m, which is often indicative of an atmospheric temperature inversion. The spectrum of CoRoT-1 is best reproduced by a 2460 K blackbody, due either to a high altitude layer that strongly absorbs stellar irradiance, or an isothermal region in the planetary atmosphere. The spectrum of CoRoT-2 is unusual because the 8 mu m contrast is anomalously low. Non-inverted atmospheres could potentially produce the CoRoT-2 spectrum if the planet exhibits line emission from CO at 4.5 mu m, caused by tidal-induced mass loss. However, the viability of that hypothesis is questionable because the emitting region cannot be more than about 30% larger than the planet's transit radius, based on the ingress and egress times at eclipse. An alternative possibility to account for the spectrum of CoRoT-2 is an additional opacity source that acts strongly at wavelengths less than 5 mu m, heating the upper atmosphere while allowing the deeper atmosphere seen at 8 mu m to remain cooler. We obtain a similar result as Gillon et al. for the phase of the secondary eclipse of CoRoT-2, implying an eccentric orbit with e cos(omega) = -0.0030 +/- 0.0004.
C1 [Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.
[Knutson, Heather] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Agol, Eric; Cowan, Nicolas B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Desert, Jean-Michel; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Cowan, Nicolas B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA.
[Showman, Adam P.; Lewis, Nikole K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Deming, D (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.
RI Agol, Eric/B-8775-2013;
OI Charbonneau, David/0000-0002-9003-484X; Agol, Eric/0000-0002-0802-9145;
Fortney, Jonathan/0000-0002-9843-4354
FU NASA [NNX07AG80G]; Miller Institute for Basic Research in Science; NSF
[0645416, PHY05-51164]; JPL/Spitzer [1328092, 1348668, 1312647]
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. Support
for this work was provided by NASA. H.K. is supported by a fellowship
from the Miller Institute for Basic Research in Science. E.A.
acknowledges support under NSF CAREER grant no. 0645416. A.B. was
supported by NASA grant NNX07AG80G and under JPL/Spitzer Agreements
1328092, 1348668, and 1312647. He is also pleased to note that part of
this work was performed while in residence at the Kavli Institute for
Theoretical Physics, funded by the NSF through grant no. PHY05-51164. We
thank Dr. Rory Barnes for informative conversations regarding the tidal
evolution of CoRoT-2, and an anonymous referee for a very thorough
review that improved this paper significantly.
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J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2011
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DI 10.1088/0004-637X/726/2/95
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698WB
UT WOS:000285623600039
ER
PT J
AU Hinkley, S
Monnier, JD
Oppenheimer, BR
Roberts, LC
Ireland, M
Zimmerman, N
Brenner, D
Parry, IR
Martinache, F
Lai, O
Soummer, R
Sivaramakrishnan, A
Beichman, C
Hillenbrand, L
Zhao, M
Lloyd, JP
Bernat, D
Vasisht, G
Crepp, JR
Pueyo, L
Shao, M
Perrin, MD
King, DL
Bouchez, A
Roberts, JE
Dekany, R
Burruss, R
AF Hinkley, Sasha
Monnier, John D.
Oppenheimer, Ben R.
Roberts, Lewis C., Jr.
Ireland, Michael
Zimmerman, Neil
Brenner, Douglas
Parry, Ian R.
Martinache, Frantz
Lai, Olivier
Soummer, Remi
Sivaramakrishnan, Anand
Beichman, Charles
Hillenbrand, Lynne
Zhao, Ming
Lloyd, James P.
Bernat, David
Vasisht, Gautam
Crepp, Justin R.
Pueyo, Laurent
Shao, Michael
Perrin, Marshall D.
King, David L.
Bouchez, Antonin
Roberts, Jennifer E.
Dekany, Richard
Burruss, Rick
TI ESTABLISHING alpha Oph AS A PROTOTYPE ROTATOR: IMPROVED ASTROMETRIC
ORBIT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: adaptive optics; methods: data analysis; stars:
individual (HIP86032); techniques: image processing
ID ADAPTIVE OPTICS SYSTEM; BINARY STARS; LYOT PROJECT; M-DWARFS; OPHIUCHI;
COMPANIONS; SEQUENCE; MULTIPLICITY; CONSTRAINTS; PERFORMANCE
AB The nearby star alpha Oph (Ras Alhague) is a rapidly rotating A5IV star spinning at similar to 89% of its breakup velocity. This system has been imaged extensively by interferometric techniques, giving a precise geometric model of the star's oblateness and the resulting temperature variation on the stellar surface. Fortuitously, alpha Oph has a previously known stellar companion, and characterization of the orbit provides an independent, dynamically based check of both the host star and the companion mass. Such measurements are crucial to constrain models of such rapidly rotating stars. In this study, we combine eight years of adaptive optics imaging data from the Palomar, AEOS, and CFHT telescopes to derive an improved, astrometric characterization of the companion orbit. We also use photometry from these observations to derive a model-based estimate of the companion mass. A fit was performed on the photocenter motion of this system to extract a component mass ratio. We find masses of 2.40(-0.37)(+0.23) M-circle dot and 0.85(-0.04)(+0.06) M-circle dot for alpha Oph A and alpha Oph B, respectively. Previous orbital studies of this system found a mass too high for this system, inconsistent with stellar evolutionary calculations. Our measurements of the host star mass are more consistent with these evolutionary calculations, but with slightly higher uncertainties. In addition to the dynamically derived masses, we use IJHK photometry to derive a model-based mass for a Oph B, of 0.77 +/- 0.05 M-circle dot marginally consistent with the dynamical masses derived from our orbit. Our model fits predict a periastron passage on 2012 April 19, with the two components having a 50 mas separation from 2012 March to May. A modest amount of interferometric and radial velocity data during this period could provide a mass determination of this star at the few percent level.
C1 [Hinkley, Sasha; Hillenbrand, Lynne; Crepp, Justin R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Monnier, John D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Oppenheimer, Ben R.; Zimmerman, Neil; Brenner, Douglas; Sivaramakrishnan, Anand] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
[Roberts, Lewis C., Jr.; Zhao, Ming; Vasisht, Gautam; Pueyo, Laurent; Shao, Michael; Roberts, Jennifer E.; Burruss, Rick] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ireland, Michael] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Zimmerman, Neil] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Parry, Ian R.; King, David L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Martinache, Frantz] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Lai, Olivier] CFHT Corp, Kamuela, HI 96743 USA.
[Soummer, Remi; Sivaramakrishnan, Anand] STScI, Baltimore, MD 21218 USA.
[Sivaramakrishnan, Anand] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Sivaramakrishnan, Anand] Univ Calif Santa Cruz, Ctr Adapt Opt, Santa Cruz, CA 95064 USA.
[Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Lloyd, James P.; Bernat, David] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Perrin, Marshall D.] Univ Calif Los Angeles, Div Astron, Los Angeles, CA 90095 USA.
[Bouchez, Antonin; Dekany, Richard] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA.
RP Hinkley, S (reprint author), CALTECH, Dept Astron, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA.
RI Lloyd, James/B-3769-2011;
OI Zimmerman, Neil/0000-0001-5484-1516
FU NASA; National Science Foundation [AST-0804417, 0334916, 0215793,
0520822, AST-0707927]; US Air Force; Cordelia Corporation, Hilary and
Ethel Lipsitz, the Vincent Astor Fund; National Aeronautics and Space
Administration
FX This work was performed in part under contract with the California
Institute of Technology (Caltech) funded by NASA through the Sagan
Fellowship Program. The Lyot Project is based upon work supported by the
National Science Foundation under Grant Nos. AST-0804417, 0334916,
0215793, and 0520822. The Lyot Project gratefully acknowledges the
support of the US Air Force and NSF in creating the special Advanced
Technologies and Instrumentation opportunity that provides access to the
AEOS telescope. The Lyot Project is also grateful to the Cordelia
Corporation, Hilary and Ethel Lipsitz, the Vincent Astor Fund, Judy
Vale, and an anonymous donor who initiated the project. A portion of the
research in this paper was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Thanks also to Anthony Boccaletti
for clarification of his epoch of the alpha Oph astrometry. We thank
Willie Torres for help checking the notation of our orbital elements,
and also to the anonymous referee for several helpful comments. J.D.M.
gratefully acknowledges support from the National Science Foundation
under Grant AST-0707927.
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JI Astrophys. J.
PD JAN 10
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SC Astronomy & Astrophysics
GA 698WB
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ER
PT J
AU Kazantzidis, S
Lokas, EL
Callegari, S
Mayer, L
Moustakas, LA
AF Kazantzidis, Stelios
Lokas, Ewa L.
Callegari, Simone
Mayer, Lucio
Moustakas, Leonidas A.
TI ON THE EFFICIENCY OF THE TIDAL STIRRING MECHANISM FOR THE ORIGIN OF
DWARF SPHEROIDALS: DEPENDENCE ON THE ORBITAL AND STRUCTURAL PARAMETERS
OF THE PROGENITOR DISKY DWARFS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: interactions; galaxies:
kinematics and dynamics; galaxies: structure; Local Group
ID COLD DARK-MATTER; MILKY-WAY SATELLITES; STAR-FORMATION HISTORIES;
DIGITAL SKY SURVEY; EXPLORING HALO SUBSTRUCTURE; LAMBDA-CDM UNIVERSE;
GALAXY LEO I; LOCAL GROUP; STELLAR POPULATIONS; GALACTIC HALOS
AB The tidal stirring model posits the formation of dwarf spheroidal galaxies (dSphs) via the tidal interactions between late-type, rotationally supported dwarfs and Milky-Way-sized host galaxies. Using a comprehensive set of collisionless N-body simulations, we investigate the efficiency of the tidal stirring mechanism for the origin of dSphs. In particular, we examine the degree to which the tidal field of the primary galaxy affects the sizes, masses, shapes, and kinematics of the disky dwarfs for a range of dwarf orbital and structural parameters. Our study is the first to employ self-consistent, equilibrium models for the progenitor dwarf galaxies constructed from a composite distribution function and consisting of exponential stellar disks embedded in massive, cosmologically motivated dark matter halos. Exploring a wide variety of dwarf orbital configurations and initial structures, we demonstrate that in the majority of cases the disky dwarfs experience significant mass loss and their stellar distributions undergo a dramatic morphological, as well as dynamical, transformation. Specifically, the stellar components evolve from disks to bars and finally to pressure-supported, spheroidal systems with kinematic and structural properties akin to those of the classic dSphs in the Local Group (LG) and similar environments. The self-consistency of the adopted dwarf models is crucial for confirming this complex transformation process via tidally induced dynamical instabilities and impulsive tidal heating of the stellar distribution. Our results suggest that such tidal transformations should be common occurrences within the currently favored cosmological paradigm and highlight the key factor responsible for an effective metamorphosis to be the strength of the tidal shocks at the pericenters of the orbit. We also demonstrate that the combination of short orbital times and small pericentric distances, characteristic of dwarfs being accreted by their hosts at high redshift, induces the strongest and most complete transformations. Our models also indicate that the efficiency of the transformation via tidal stirring is affected significantly by the structure of the progenitor disky dwarfs. While the mass-to-light ratios, M/L, of the dwarf galaxies typically decrease monotonically with time as the extended dark matter halos are efficiently tidally stripped, we identify a few cases where this trend is reversed later in the evolution when stellar mass loss becomes more effective. We also find that the dwarf remnants satisfy the relation V-max = root 3 sigma(*), where sigma(*) is the one-dimensional, central stellar velocity dispersion and V-max is the maximum halo circular velocity, which has intriguing implications for the missing satellites problem. Assuming that the distant dSphs in the LG, such as Leo I, Tucana, and Cetus, are the products of tidal stirring, our findings suggest that these galaxies should have only been partially stirred by the tidal field of their hosts. We thus predict that these remote dwarfs should exhibit higher values of V-rot/sigma(*), where V-rot is the stellar rotational velocity, compared with those of dSphs located closer to the primary galaxies. Overall, we conclude that the action of tidal forces from the hosts constitutes a crucial evolutionary mechanism for shaping the nature of dwarf galaxies in environments such as that of the LG.
Environmental mechanisms of this type should thus be included as ingredients in models of dwarf galaxy formatio and evolution.
C1 [Kazantzidis, Stelios] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA.
[Kazantzidis, Stelios] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Kazantzidis, Stelios] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Lokas, Ewa L.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Callegari, Simone; Mayer, Lucio] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland.
[Mayer, Lucio] Swiss Fed Inst Technol, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
[Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kazantzidis, S (reprint author), Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA.
EM stelios@mps.ohio-state.edu; lokas@camk.edu.pl; callegar@physik.uzh.ch;
lucio@phys.ethz.ch; leonidas@jpl.nasa.gov
OI Moustakas, Leonidas/0000-0003-3030-2360
FU Center for Cosmology and Astro-Particle Physics (CCAPP) at The Ohio
State University; Polish Ministry of Science and Higher Education
[NN203025333]; NASA; JPL Office of the Chief Information Officer
FX The authors acknowledge useful discussions with James Bullock, Mandeep
Gill, Andrey Kravtsov, Andrea Maccio, Chiara Mastropietro, Mario Mateo,
Chris Orban, Michael Stamatikos, Justin Read, and David Weinberg. S.K.
thanks Victor Debattista for valuable conversations on bar instabilities
and related issues which significantly informed this work. S.K. also
acknowledges the hospitality of the Nicolaus Copernicus Astronomical
Center during a visit when the final stages of this work were completed.
S.K. is funded by the Center for Cosmology and Astro-Particle Physics
(CCAPP) at The Ohio State University. E.L.L. is grateful for the
hospitality of CCAPP during her visit. This research was partially
supported by the Polish Ministry of Science and Higher Education under
grant NN203025333. The work of L.A.M. was carried out at the Jet
Propulsion Laboratory (JPL), California Institute of Technology, under a
contract with NASA. L.A.M. acknowledges support from the NASA ATFP
program. The numerical simulations were performed on the Cosmos cluster
at JPL. Cosmos was provided by funding from the JPL Office of the Chief
Information Officer. This work was also supported by an allocation of
computing time from the Ohio Supercomputer Center (http://www.osc.edu).
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PY 2011
VL 726
IS 2
AR 98
DI 10.1088/0004-637X/726/2/98
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698WB
UT WOS:000285623600042
ER
PT J
AU Parkin, ER
Pittard, JM
Corcoran, MF
Hamaguchi, K
AF Parkin, E. R.
Pittard, J. M.
Corcoran, M. F.
Hamaguchi, K.
TI SPIRALING OUT OF CONTROL: THREE-DIMENSIONAL HYDRODYNAMICAL MODELING OF
THE COLLIDING WINDS IN eta CARINAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE hydrodynamics; stars: early-type; stars: individual (eta Carinae);
stars: massive; stars: winds, outflows; X-rays: stars
ID X-RAY-EMISSION; ADAPTIVE MESH REFINEMENT; RADIATION-DRIVEN WINDS; O STAR
BINARIES; HOMUNCULUS NEBULA; SPECTROSCOPIC EVENT; STELLAR WINDS;
LIGHT-CURVE; MASS-LOSS; 2003.5 MINIMUM
AB Three-dimensional adaptive mesh refinement hydrodynamical simulations of the wind-wind collision between the enigmatic supermassive star eta Car and its mysterious companion star are presented which include radiative driving of the stellar winds, gravity, optically thin radiative cooling, and orbital motion. Simulations with static stars with a periastron passage separation reveal that the preshock companion star's wind speed is sufficiently reduced so that radiative cooling in the postshock gas becomes important, permitting the runaway growth of nonlinear thin-shell instabilities (NTSIs) which massively distort the wind-wind collision region (WCR). However, large-scale simulations, which include the orbital motion of the stars, show that orbital motion reduces the impact of radiative inhibition and thus increases the acquired preshock velocities. As such, the postshock gas temperature and cooling time see a commensurate increase, and sufficient gas pressure is preserved to stabilize the WCR against catastrophic instability growth. We then compute synthetic X-ray spectra and light curves and find that, compared to previous models, the X-ray spectra agree much better with XMM-Newton observations just prior to periastron. The narrow width of the 2009 X-ray minimum can also be reproduced. However, the models fail to reproduce the extended X-ray minimum from previous cycles. We conclude that the key to explaining the extended X-ray minimum is the rate of cooling of the companion star's postshock wind. If cooling is rapid then powerful NTSIs will heavily disrupt the WCR. Radiative inhibition of the companion star's preshock wind, albeit with a stronger radiation-wind coupling than explored in this work, could be an effective trigger.
C1 [Parkin, E. R.] Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium.
[Parkin, E. R.; Pittard, J. M.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Corcoran, M. F.; Hamaguchi, K.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA.
[Corcoran, M. F.; Hamaguchi, K.] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Hamaguchi, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
RP Parkin, ER (reprint author), Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia.
EM parkin@mso.anu.edu.au
FU University of Leeds; PRODEX XMM/Integral contract (Belspo); Royal
Society; University of Chicago
FX We thank Ian Stevens and Sven van Loo for helpful discussions, and the
referee for useful suggestions which improved the presentation of this
work. This work was supported in part by a Henry Ellison Scholarship
from the University of Leeds, and by a PRODEX XMM/Integral contract
(Belspo). J.M.P. thanks the Royal Society for funding. This research has
made use of NASA's Astrophysics Data System. This research has made use
of data obtained from the High Energy Astrophysics Science Archive
Research Centre (HEASARC) provided by NASA's Goddard Space Flight
Center. Some of the software used in this work was in part developed by
the DOE-supported ASC/Alliance Center for Astrophysical Thermonuclear
Flashes at the University of Chicago. We thank the White Rose Grid and
the UK National Grid Service (NGS) for use of their computer facilities.
NR 102
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2011
VL 726
IS 2
AR 105
DI 10.1088/0004-637X/726/2/105
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698WB
UT WOS:000285623600049
ER
PT J
AU van der Horst, AJ
Kamble, AP
Paragi, Z
Sage, LJ
Pal, S
Taylor, GB
Kouveliotou, C
Granot, J
Ramirez-Ruiz, E
Ishwara-Chandra, CH
Oosterloo, TA
Wijers, RAMJ
Wiersema, K
Strom, RG
Bhattacharya, D
Rol, E
Starling, RLC
Curran, PA
Garrett, MA
AF van der Horst, A. J.
Kamble, A. P.
Paragi, Z.
Sage, L. J.
Pal, S.
Taylor, G. B.
Kouveliotou, C.
Granot, J.
Ramirez-Ruiz, E.
Ishwara-Chandra, C. H.
Oosterloo, T. A.
Wijers, R. A. M. J.
Wiersema, K.
Strom, R. G.
Bhattacharya, D.
Rol, E.
Starling, R. L. C.
Curran, P. A.
Garrett, M. A.
TI DETAILED RADIO VIEW ON TWO STELLAR EXPLOSIONS AND THEIR HOST GALAXY: XRF
080109/SN 2008D AND SN 2007uy in NGC 2770
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC2770); supernovae: individual (SN2008D,
SN2007uy)
ID GAMMA-RAY BURSTS; SHOCK BREAKOUT; RELATIVISTIC JETS; HI OBSERVATIONS;
MOLECULAR GAS; IBC SUPERNOVA; EMISSION; AFTERGLOW; IDENTIFICATION; RATES
AB The galaxy NGC 2770 hosted two core-collapse supernova (SN) explosions, SN 2008D and SN 2007uy, within 10 days of each other and 9 years after the first SN of the same type, SN 1999eh, was found in that galaxy. In particular, SN 2008D attracted a lot of attention due to the detection of an X-ray outburst, which has been hypothesized to be caused by either a (mildly) relativistic jet or the SN shock breakout. We present an extensive study of the radio emission from SN 2008D and SN 2007uy: flux measurements with the Westerbork Synthesis Radio Telescope and the Giant Metrewave Radio Telescope, covering similar to 600 days with observing frequencies ranging from 325 MHz to 8.4 GHz. The results of two epochs of global Very Long Baseline Interferometry observations are also discussed. We have examined the molecular gas in the host galaxy NGC 2770 with the Arizona Radio Observatory 12 m telescope, and present the implications of our observations for the star formation and seemingly high SN rate in this galaxy. Furthermore, we discuss the near-future observing possibilities of the two SNe and their host galaxy at low radio frequencies with the Low Frequency Array.
C1 [van der Horst, A. J.; Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Kamble, A. P.; Wijers, R. A. M. J.; Strom, R. G.; Rol, E.] Univ Amsterdam, Astron Inst, Amsterdam, Netherlands.
[Paragi, Z.] Joint Inst VLBI Europe JIVE, NL-7990 AA Dwingeloo, Netherlands.
[Paragi, Z.] MTA Res Grp Phys Geodesy & Geodynam, H-1585 Budapest, Hungary.
[Sage, L. J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Pal, S.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley 6009, Australia.
[Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Ne Albuquerque, NM 87131 USA.
[Granot, J.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Ramirez-Ruiz, E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ishwara-Chandra, C. H.] Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
[Oosterloo, T. A.; Strom, R. G.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Oosterloo, T. A.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Wiersema, K.; Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Bhattacharya, D.] Inter Univ Ctr Astron & Astrophys, Pune, Maharashtra, India.
[Curran, P. A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Garrett, M. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Garrett, M. A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
RP van der Horst, AJ (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
EM Alexander.J.VanDerHorst@nasa.gov
RI Curran, Peter/B-5293-2013; Bhattacharya, Dipankar/J-6927-2015;
OI Curran, Peter/0000-0003-3003-4626; Bhattacharya,
Dipankar/0000-0003-3352-3142; Wijers, Ralph/0000-0002-3101-1808
FU Netherlands Foundation for Scientific Research; national research
councils; National Science Foundation; MSFC; NWO-Vici [C.2320.0017];
OTKA [K72515]; Royal Society
FX We greatly appreciate the support from the WSRT, GMRT, EVN, and ARO
staff in their help with scheduling and obtaining these observations. We
thank Bob Campbell and Andreas Brunthaler for useful comments regarding
astrometric accuracy of the VLBI data. The WSRT is operated by ASTRON
(Netherlands Institute for Radio Astronomy) with support from the
Netherlands Foundation for Scientific Research. The GMRT is operated by
the National Center for Radio Astrophysics of the Tata Institute of
Fundamental Research. The EVN is a joint facility of European, Chinese,
South African and other radio astronomy institutes funded by their
national research councils. The National Radio Astronomy Observatory is
operated by Associated Universities, Inc., under cooperative agreement
with the National Science Foundation. The ARO 12 m Telescope is operated
by the Arizona Radio Observatory, Steward Observatory, University of
Arizona. A.J.v.d.H. was supported by an appointment to the NASA
Postdoctoral Program at the MSFC, administered by Oak Ridge Associated
Universities through a contract with NASA. A.P.K. was supported by
NWO-Vici grant C.2320.0017 and also gratefully acknowledges hospitality
in 2009 January provided by the IUCAA where part of this work was
carried out. Z.P. acknowledges support from the Hungarian Scientific
Research Fund (OTKA, grant K72515). J.G. acknowledges a Royal Society
Wolfson Research Merit Award.
NR 76
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2011
VL 726
IS 2
AR 99
DI 10.1088/0004-637X/726/2/99
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698WB
UT WOS:000285623600043
ER
PT J
AU Frayer, DT
Harris, AI
Baker, AJ
Ivison, RJ
Smail, I
Negrello, M
Maddalena, R
Aretxaga, I
Baes, M
Birkinshaw, M
Bonfield, DG
Burgarella, D
Buttiglione, S
Cava, A
Clements, DL
Cooray, A
Dannerbauer, H
Dariush, A
De Zotti, G
Dunlop, JS
Dunne, L
Dye, S
Eales, S
Fritz, J
Gonzalez-Nuevo, J
Herranz, D
Hopwood, R
Hughes, DH
Ibar, E
Jarvis, MJ
Lagache, G
Leeuw, LL
Lopez-Caniego, M
Maddox, S
Michallowski, MJ
Omont, A
Pohlen, M
Rigby, E
Rodighiero, G
Scott, D
Serjeant, S
Smith, DJB
Swinbank, AM
Temi, P
Thompson, MA
Valtchanov, I
van der Werf, PP
Verma, A
AF Frayer, D. T.
Harris, A. I.
Baker, A. J.
Ivison, R. J.
Smail, Ian
Negrello, M.
Maddalena, R.
Aretxaga, I.
Baes, M.
Birkinshaw, M.
Bonfield, D. G.
Burgarella, D.
Buttiglione, S.
Cava, A.
Clements, D. L.
Cooray, A.
Dannerbauer, H.
Dariush, A.
De Zotti, G.
Dunlop, J. S.
Dunne, L.
Dye, S.
Eales, S.
Fritz, J.
Gonzalez-Nuevo, J.
Herranz, D.
Hopwood, R.
Hughes, D. H.
Ibar, E.
Jarvis, M. J.
Lagache, G.
Leeuw, L. L.
Lopez-Caniego, M.
Maddox, S.
Michallowski, M. J.
Omont, A.
Pohlen, M.
Rigby, E.
Rodighiero, G.
Scott, D.
Serjeant, S.
Smith, D. J. B.
Swinbank, A. M.
Temi, P.
Thompson, M. A.
Valtchanov, I.
van der Werf, P. P.
Verma, A.
TI GREEN BANK TELESCOPE ZPECTROMETER CO(1-0) OBSERVATIONS OF THE STRONGLY
LENSED SUBMILLIMETER GALAXIES FROM THE HERSCHEL ATLAS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: individual (SDP.81:
H-ATLAS J090311.6+003906, SDP.130: H-ATLAS J091305.0-005343); galaxies:
starburst
ID LUMINOUS INFRARED GALAXIES; MOLECULAR GAS; REDSHIFT DISTRIBUTION; DISK
GALAXIES; POPULATION; EMISSION; LINE; CONSTRAINTS; CLUSTERS; REGIONS
AB The Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) has uncovered a population of strongly lensed submillimeter galaxies (SMGs). The Zpectrometer instrument on the Green Bank Telescope (GBT) was used to measure the redshifts and constrain the masses of the cold molecular gas reservoirs for two candidate high-redshift lensed sources. We derive CO(1-0) redshifts of z = 3.042 +/- 0.001 and z = 2.625 +/- 0.001, and measure molecular gas masses of (1-3) x10(10) M-circle dot, corrected for lens amplification and assuming a conversion factor of alpha = 0.8M(circle dot) (Kkm s-(1) pc(2))(-1). We find typical L(IR)/L'(CO) ratios of 120 +/- 40 and 140 +/- 50L(circle dot) (Kkm s(-1) pc(2))(-1), which are consistent with those found for local ultraluminous infrared galaxies (ULIRGs) and other high-redshift SMGs. From analysis of published data, we find no evidence for enhanced L(IR)/L'(CO(1-0)) ratios for the SMG population in comparison to local ULIRGs. The GBT results highlight the power of using the CO lines to derive blind redshifts, which is challenging for the SMGs at optical wavelengths given their high obscuration.
C1 [Frayer, D. T.; Maddalena, R.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; van der Werf, P. P.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Smail, Ian; Swinbank, A. M.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Negrello, M.; Hopwood, R.; Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Aretxaga, I.; Hughes, D. H.] Inst Nacl Astrofis Opt & Elect Luis Enrique Erro, Puebla 72840, Mexico.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Birkinshaw, M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England.
[Bonfield, D. G.; Jarvis, M. J.; Thompson, M. A.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[Burgarella, D.] CNRS, Lab Astrophys Marseille, UMR6110, F-13388 Marseille, France.
[Buttiglione, S.; De Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[Cooray, A.] Univ Calif Irvine, Ctr Cosmol, Irvine, CA 92697 USA.
[Dannerbauer, H.] Univ Paris Diderot, AIM, CEA DSM CNRS, DAPNIA Serv Astrophy,SEA Saclay, F-91191 Gif Sur Yvette, France.
[Dariush, A.; Dye, S.; Eales, S.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[De Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Dunlop, J. S.; Michallowski, M. J.] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Dunne, L.; Maddox, S.; Rigby, E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Gonzalez-Nuevo, J.] Scuola Int Super Avanzati, I-34151 Trieste, Italy.
[Herranz, D.; Lopez-Caniego, M.] Inst Fis Cantabria CSIC UC, Santander 39005, Spain.
[Lagache, G.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France.
[Leeuw, L. L.] SETI Inst, Mountain View, CA 94043 USA.
[Leeuw, L. L.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Omont, A.] CNRS, Inst Astrophys Paris, F-75014 Paris, France.
[Omont, A.] Univ Paris 06, F-75014 Paris, France.
[Rodighiero, G.] Univ Padua, Dept Astron, I-35122 Padua, Italy.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Valtchanov, I.] ESA, Herschel Sci Ctr, ESAC, Madrid 28691, Spain.
[van der Werf, P. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Verma, A.] Univ Oxford, Oxford OX1 3RH, England.
RP Frayer, DT (reprint author), Natl Radio Astron Observ, POB 2, Green Bank, WV 24944 USA.
RI Baes, Maarten/I-6985-2013; Lopez-Caniego, Marcos/M-4695-2013; Smail,
Ian/M-5161-2013; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo,
Joaquin/I-3562-2014; Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017;
OI Baes, Maarten/0000-0002-3930-2757; Smail, Ian/0000-0003-3037-257X;
Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo,
Joaquin/0000-0003-1354-6822; Ivison, R./0000-0001-5118-1313; Cava,
Antonio/0000-0002-4821-1275; Lopez-Caniego, Marcos/0000-0003-1016-9283;
Maddox, Stephen/0000-0001-5549-195X; Scott, Douglas/0000-0002-6878-9840;
Dye, Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X;
Rodighiero, Giulia/0000-0002-9415-2296
FU National Science Foundation [AST-0708653]
FX We acknowledge the staff at Green Bank who have made these observations
possible. We are indebted to the late Senator Robert C. Byrd for his
strong support of the Green Bank Telescope. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. A.J.B.
acknowledges support from the National Science Foundation through grant
AST-0708653.
NR 50
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 10
PY 2011
VL 726
IS 2
AR L22
DI 10.1088/2041-8205/726/2/L22
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 700CP
UT WOS:000285710700008
ER
PT J
AU Fok, MC
Moore, TE
Slinker, SP
Fedder, JA
Delcourt, DC
Nose, M
Chen, SH
AF Fok, Mei-Ching
Moore, Thomas E.
Slinker, Steve P.
Fedder, Joel A.
Delcourt, Dominique C.
Nose, Masahito
Chen, Sheng-Hsien
TI Modeling the superstorm in November 2003
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID GLOBAL MHD SIMULATION; ION-CYCLOTRON WAVES; RING CURRENT IONS; INNER
MAGNETOSPHERE; GEOMAGNETIC STORMS; ELECTRIC-FIELDS; MAGNETIC-FIELD;
IONOSPHERE; PARTICLES; ENERGY
AB The superstorm on 20-21 November 2003 was the largest geomagnetic storm in solar cycle 23 as measured by Dst, which attained a minimum value of -422 nT. We have simulated this storm to understand how particles originating from the solar wind and ionosphere get access to the magnetosphere and how the subsequent transport and energization processes contribute to the buildup of the ring current. The global electromagnetic configuration and the solar wind H+ distribution are specified by the Lyon-Fedder-Mobarry (LFM) magnetohydrodynamics model. The outflow of H+ and O+ ions from the ionosphere are also considered. Their trajectories in the magnetosphere are followed by a test-particle code. The particle distributions at the inner plasma sheet established by the LFM model and test-particle calculations are then used as boundary conditions for a ring current model. Our simulations reproduce the rapid decrease of Dst during the storm main phase and the fast initial phase of recovery. Shielding in the inner magnetosphere is established at early main phase. This shielding field lasts several hours and then breaks down at late main phase. At the peak of the storm, strong penetration of ions earthward to L shell of 1.5 is revealed in the simulation. It is surprising that O+ is significant but not the dominant species in the ring current in our calculation for this major storm. It is very likely that substorm effects are not well represented in the models and O+ energization is underestimated. Ring current simulation with O+ energy density at the boundary set comparable to Geotail observations produces excellent agreement with the observed symH. As expected in superstorms, ring current O+ is the dominant species over H+ during the main to midrecovery phase of the storm.
C1 [Fok, Mei-Ching; Moore, Thomas E.; Chen, Sheng-Hsien] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Delcourt, Dominique C.] Ecole Polytech, CNRS, UMR 7648, Lab Phys Plasmas, F-94107 St Maur Des Fosses, France.
[Fedder, Joel A.] Leading Edge Technol Inc, Alexandria, VA 22308 USA.
[Nose, Masahito] Kyoto Univ, Grad Sch Sci, Data Anal Ctr Geomagnetism & Space Magnetism, Sakyo Ku, Kyoto 6068502, Japan.
[Slinker, Steve P.] USN, Res Lab, Washington, DC 20375 USA.
RP Fok, MC (reprint author), NASA, Goddard Space Flight Ctr, Code 673,Bldg 21,Rm 248, Greenbelt, MD 20771 USA.
EM mei-ching.h.fok@nasa.gov
RI Moore, Thomas/D-4675-2012; Fok, Mei-Ching/D-1626-2012; Nose,
Masahito/B-1900-2015
OI Moore, Thomas/0000-0002-3150-1137; Nose, Masahito/0000-0002-2789-3588
FU NASA Heliophysics Division [936723.02.01.03.82, 955518.02.01.02.57];
NASA [R0608]
FX We gratefully acknowledge use of the ACE solar wind data provided
through OMNI and Geotail data from http://sd-www.jhuapl.edu/Geotail/.
The Dst and symH data are provided by the World Data Center for
Geomagnetism, Kyoto, Japan. We would like to thank Natalia Buzulukova
for valuable comments. We also thank Manuel Buenfil and Robert Wiegand
for performing the test-particle and bulk parameter calculations. We
acknowledge support from the NASA Heliophysics Division through the
ROSES program under Work Breakdown Structures 936723.02.01.03.82 and
955518.02.01.02.57, and NASA's High Performance Computing Program under
task R0608.
NR 55
TC 12
Z9 12
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JAN 7
PY 2011
VL 116
AR A00J17
DI 10.1029/2010JA015720
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 704NS
UT WOS:000286060300001
ER
PT J
AU Lawrence, DJ
Hurley, DM
Feldman, WC
Elphic, RC
Maurice, S
Miller, RS
Prettyman, TH
AF Lawrence, D. J.
Hurley, D. M.
Feldman, W. C.
Elphic, R. C.
Maurice, S.
Miller, R. S.
Prettyman, T. H.
TI Sensitivity of orbital neutron measurements to the thickness and
abundance of surficial lunar water
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID EPITHERMAL NEUTRONS; SURFACE MATURITY; PROSPECTOR; MOON; ICE; POLES;
TIO2; MARS
AB Recent near-infrared spectral data have shown that surficial water (H2O/OH) exists over large expanses of the lunar surface. These results have led to a reexamination of the hydrogen abundance sensitivity limits of orbital neutron data to detect surficial hydrogen on the lunar surface. A wet-over-dry, two-layer stratigraphy is modeled for the first time using neutron transport codes. For thin layers (<30 g/cm(2)), the epithermal neutron flux increases with increasing hydrogen concentration. This behavior is in contrast to the standard behavior for a single layer or dry-over-wet stratigraphy where the epithermal neutron counting rate decreases with increasing hydrogen concentration. These neutron transport results are applied to a H2O/OH enhancement at Goldschmidt crater. The neutron behavior at Goldschmidt is mostly controlled by spatial variations in neutron absorbing elements. After accounting for variations from neutron absorbing elements, there remain residual neutron enhancements at Goldschmidt crater with marginal statistical significance. If these residual enhancements are due to hydrogen, then their magnitude implies the presence of an upper layer with thickness of similar to 3-30 g/cm(2) (or 1.7-17 cm for an assumed density of 1.8 g/cm(3)) having an enhanced hydrogen abundance of 0.1-1 wt % water equivalent hydrogen. However, more work needs to be done to understand systematic variations of neutron counting rates at the 1-3% signal contrast level before a definitive conclusion can be made that the residual neutron enhancement at Goldschmidt crater is due to enhanced hydrogen abundances.
C1 [Lawrence, D. J.; Hurley, D. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20733 USA.
[Feldman, W. C.; Prettyman, T. H.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Elphic, R. C.] NASA, Ames Res Ctr, Planetary Syst Branch, Moffett Field, CA 94035 USA.
[Maurice, S.] Ctr Etud Spatiale Rayonnements, Observ Midi Pyrenees, F-31400 Toulouse, France.
[Miller, R. S.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
RP Lawrence, DJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Dr,MP3-E169, Laurel, MD 20733 USA.
EM david.j.lawrence@jhuapl.edu
RI Maurice, Sylvestre/B-3575-2015; Hurley, Dana/F-4488-2015; Lawrence,
David/E-7463-2015;
OI Hurley, Dana/0000-0003-1052-1494; Lawrence, David/0000-0002-7696-6667;
Prettyman, Thomas/0000-0003-0072-2831
FU NASA Lunar Science Institute
FX D. Lawrence (SDG), D. Hurley, and R. Miller conducted this work with the
support of NASA Lunar Science Institute.
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JAN 7
PY 2011
VL 116
AR E01002
DI 10.1029/2010JE003678
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 704NM
UT WOS:000286059700001
ER
PT J
AU Mackowski, DW
Mishchenko, MI
AF Mackowski, Daniel W.
Mishchenko, Michael I.
TI Direct simulation of multiple scattering by discrete random media
illuminated by Gaussian beams
SO PHYSICAL REVIEW A
LA English
DT Article
ID SOLAR-SYSTEM BODIES; LIGHT-SCATTERING; COHERENT BACKSCATTERING; T
MATRIX; SPHERES; ABSORPTION; VOLUME
AB The conventional orientation-averaging procedure developed in the framework of the superposition T-matrix approach is generalized to include the case of illumination by a Gaussian beam (GB). The resulting computer code is parallelized and used to perform extensive numerically exact calculations of electromagnetic scattering by volumes of discrete random medium consisting of monodisperse spherical particles. The size parameters of the scattering volumes are 40, 50, and 60, while their packing density is fixed at 5%. We demonstrate that all scattering patterns observed in the far-field zone of a random multisphere target and their evolution with decreasing width of the incident GB can be interpreted in terms of idealized theoretical concepts such as forward-scattering interference, coherent backscattering (CB), and diffuse multiple scattering. It is shown that the increasing violation of electromagnetic reciprocity with decreasing GB width suppresses and eventually eradicates all observable manifestations of CB. This result supplements the previous demonstration of the effects of broken reciprocity in the case of magneto-optically active particles subjected to an external magnetic field.
C1 [Mackowski, Daniel W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
[Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Mackowski, DW (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
EM dmckwski@eng.auburn.edu
RI Mackowski, Daniel/K-1917-2013; Mishchenko, Michael/D-4426-2012
FU NASA
FX This research was supported in part by the NASA Radiation Sciences.
NR 48
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U2 9
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD JAN 7
PY 2011
VL 83
IS 1
AR 013804
DI 10.1103/PhysRevA.83.013804
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 713IY
UT WOS:000286732900011
ER
PT J
AU Frissell, NA
Baker, JBH
Ruohoniemi, JM
Clausen, LBN
Kale, ZC
Rae, IJ
Kepko, L
Oksavik, K
Greenwald, RA
West, ML
AF Frissell, N. A.
Baker, J. B. H.
Ruohoniemi, J. M.
Clausen, L. B. N.
Kale, Z. C.
Rae, I. J.
Kepko, L.
Oksavik, K.
Greenwald, R. A.
West, M. L.
TI First radar observations in the vicinity of the plasmapause of pulsed
ionospheric flows generated by bursty bulk flows
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SUBSTORM CURRENT WEDGE; PI2 PULSATIONS; INSTRUMENT; LATITUDES; BRAKING;
EVENTS
AB Recent expansion of the SuperDARN network to mid-latitudes and the addition of a new high-time resolution mode provides new opportunities to observe mid-latitude ultra-low frequency waves and other ionospheric sub-auroral features at high temporal resolution. On 22 February 2008, the Blackstone SuperDARN radar and THEMIS ground magnetometers simultaneously observed substorm Pi2 pulsations. Similarities in measurements from the Blackstone radar and a magnetometer at Remus suggest a common generating mechanism. Cross-phase analysis of magnetometer data places these measurements at the ionospheric projection of the plasmapause, while fine spatial and temporal details of the radar data show evidence of field line compressions. About 1 min prior to ground Pi2 observation, 2 Earthward-moving Bursty Bulk Flows (BBFs) were observed by THEMIS probes D and E in the near-Earth plasma sheet. We conclude that the first 2 pulses of the Pi2s observed at Blackstone and Remus result from compressional energy generated by BBFs braking against the magnetospheric dipolar region. Citation: Frissell, N. A., J. B. H. Baker, J. M. Ruohoniemi, L. B. N. Clausen, Z. C. Kale, I. J. Rae, L. Kepko, K. Oksavik, R. A. Greenwald, and M. L. West (2011), First radar observations in the vicinity of the plasmapause of pulsed ionospheric flows generated by bursty bulk flows, Geophys. Res. Lett., 38, L01103, doi:10.1029/2010GL045857.
C1 [Frissell, N. A.; Baker, J. B. H.; Ruohoniemi, J. M.; Clausen, L. B. N.; Greenwald, R. A.] Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24060 USA.
[Kale, Z. C.; Rae, I. J.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada.
[Kepko, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Oksavik, K.] Univ Ctr Svalbard, Dept Arctic Geophys, N-9171 Longyearbyen, Norway.
[West, M. L.] Montclair State Univ, Dept Math Sci, Montclair, NJ 07043 USA.
RP Frissell, NA (reprint author), Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, 1991 Kraft Dr,Ste 2019, Blacksburg, VA 24060 USA.
EM nafrissell@vt.edu
RI Kepko, Larry/D-7747-2012; Rae, Jonathan/D-8132-2013;
OI Kepko, Larry/0000-0002-4911-8208; Oksavik, Kjellmar/0000-0003-4312-6992;
Greenwald, Raymond/0000-0002-7421-5536
FU NSF [ATM-0849031, ATM-0946900]; Research Council of Norway; NASA
[NAS5-02099]; CSA
FX Support for this research and funding for the construction of the
Blackstone SuperDARN radar is provided by NSF grants ATM-0849031 and
ATM-0946900. K. Oksavik thanks the Research Council of Norway for
financial support. Kp and AE indices were obtained from the
WDC in Kyoto. We acknowledge NASA contract NAS5-02099 and V.
Angelopoulos for use of data from the THEMIS Mission. Specifically C. W.
Carlson and J. P. McFadden for use of ESA data, S. Mende, C. T. Russell,
and I. Mann for use of GMAG data, and the CSA for support of the CARISMA
network. We thank J. Green for providing data from the NOAA/POES TED
instrument, and E. Zesta for SAMBA GMAG data. STEP 210 GMAG data was
copied from the Solar-Terrestrial Environment Laboratory, Nagoya
University. SW and IMF data was obtained from the CDAWeb OMNI database
by J. H. King and N. Papitashvili. Satellite positions and magnetic
footprints were obtained with the TIPSOD program by NASA GSFC SSC.
NR 28
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 6
PY 2011
VL 38
AR L01103
DI 10.1029/2010GL045857
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 704OB
UT WOS:000286061200002
ER
PT J
AU Madhusudhan, N
Harrington, J
Stevenson, KB
Nymeyer, S
Campo, CJ
Wheatley, PJ
Deming, D
Blecic, J
Hardy, RA
Lust, NB
Anderson, DR
Collier-Cameron, A
Britt, CBT
Bowman, WC
Hebb, L
Hellier, C
Maxted, PFL
Pollacco, D
West, RG
AF Madhusudhan, Nikku
Harrington, Joseph
Stevenson, Kevin B.
Nymeyer, Sarah
Campo, Christopher J.
Wheatley, Peter J.
Deming, Drake
Blecic, Jasmina
Hardy, Ryan A.
Lust, Nate B.
Anderson, David R.
Collier-Cameron, Andrew
Britt, Christopher B. T.
Bowman, William C.
Hebb, Leslie
Hellier, Coel
Maxted, Pierre F. L.
Pollacco, Don
West, Richard G.
TI A high C/O ratio and weak thermal inversion in the atmosphere of
exoplanet WASP-12b
SO NATURE
LA English
DT Article
ID GIANT PLANETS; HOT JUPITERS; HD 189733B; TEMPERATURE; EMISSION;
PHOTOCHEMISTRY; CHEMISTRY; SPECTRA; DWARFS; STARS
AB The carbon-to-oxygen ratio (C/O) in a planet provides critical information about its primordial origins and subsequent evolution. A primordial C/O greater than 0.8 causes a carbide-dominated interior, as opposed to the silicate-dominated composition found on Earth(1); the atmosphere can also differ from those in the Solar System(1,2). The solar C/O is 0.54 (ref. 3). Here we report an analysis of dayside multi-wavelength photometry(4,5) of the transiting hot Jupiter WASP-12b (ref. 6) that reveals C/O >= 1 in its atmosphere. The atmosphere is abundant in CO. It is depleted in water vapour and enhanced in methane, each by more than two orders of magnitude compared to a solar-abundance chemical-equilibrium model at the expected temperatures. We also find that the extremely irradiated atmosphere (T > 2,500 K) of WASP-12b lacks a prominent thermal inversion (or stratosphere) and has very efficient day-night energy circulation. The absence of a strong thermal inversion is in stark contrast to theoretical predictions for the most highly irradiated hot-Jupiter atmospheres(7-9).
C1 [Madhusudhan, Nikku] MIT, Cambridge, MA 02139 USA.
[Harrington, Joseph; Stevenson, Kevin B.; Nymeyer, Sarah; Campo, Christopher J.; Blecic, Jasmina; Hardy, Ryan A.; Lust, Nate B.; Britt, Christopher B. T.; Bowman, William C.] Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL 32816 USA.
[Wheatley, Peter J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Anderson, David R.; Hellier, Coel; Maxted, Pierre F. L.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Collier-Cameron, Andrew] Univ St Andrews, Sch Phys & Astron, Haugh KY16 9SS, Fife, Scotland.
[Hebb, Leslie] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Pollacco, Don] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[West, Richard G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Madhusudhan, N (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
EM nmadhu@mit.edu
RI Harrington, Joseph/E-6250-2011;
OI Blecic, Jasmina/0000-0002-0769-9614; Cameron,
Andrew/0000-0002-8863-7828; Hardy, Ryan/0000-0002-3849-9551; Harrington,
Joseph/0000-0002-8955-8531; Wheatley, Peter/0000-0003-1452-2240
FU NASA; JPL/Caltech
FX We thank the authors of ref. 5 for sharing their ground-based
observations before publication, and Thomas J. Loredo for discussions.
N.M. thanks S. Seager for financial support during his stay at MIT,
where most of the modelling work was carried out. This work is based on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with NASA. Support for this work was provided by NASA through
an award issued by JPL/Caltech.
NR 30
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PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JAN 6
PY 2011
VL 469
IS 7328
BP 64
EP 67
DI 10.1038/nature09602
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 702UO
UT WOS:000285921600031
PM 21150901
ER
PT J
AU Jezek, K
Wu, XQ
Gogineni, P
Rodriguez, E
Freeman, A
Rodriguez-Morales, F
Clark, CD
AF Jezek, Kenneth
Wu, Xiaoqing
Gogineni, Prasad
Rodriguez, Ernesto
Freeman, Anthony
Rodriguez-Morales, Fernando
Clark, Chris D.
TI Radar images of the bed of the Greenland Ice Sheet
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID NW SCOTLAND; TOMOGRAPHY; BEDROCK; MEGAGROOVES; GLACIERS; MISSION
AB In this paper, we apply radar tomography methods to very-high-frequency, airborne synthetic-aperture radar data to measure the ice thickness field and to construct three-dimensional basal image maps of a 5 x 20 km study area located along the southern flank of the Jakobshavn Glacier, Greenland. Unlike ice radar measurements typically made at nadir, our approach uses radar-echo phase and amplitude measured across an antenna array to determine the propagation angle and signal strength of pixel elements distributed on each side of the aircraft flight path. That information, combined with knowledge of aircraft position and the assumed dielectric properties of the glacier, can be used to measure ice thickness and radar reflectivity across a 3-km wide swath. Combining ice thickness and surface topography data, we estimate basal topography and basal drag. We conclude that the glacier is sliding over the bed. We use the three-dimensional image maps of the bed to inspect the modern subglacial geomorphology and find for the first time beneath the Greenland Ice Sheet assemblages of long ridge-groove landforms that are oriented in the direction of the ice flow. Spatial dimensions (10 to 30 m depths, 150 to 500 m spacing and lengths of 10 km or more) and correlation with the current ice flow direction suggest that these are glacial erosional features similar to mega-grooves observed on deglaciated terrain. Citation: Jezek, K., X. Wu, P. Gogineni, E. Rodriguez, A. Freeman, F. Rodriguez-Morales, and C. D. Clark (2011), Radar images of the bed of the Greenland Ice Sheet, Geophys. Res. Lett., 38, L01501, doi: 10.1029/2010GL045519.
C1 [Jezek, Kenneth] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Wu, Xiaoqing; Rodriguez, Ernesto; Freeman, Anthony] Jet Prop Lab, Pasadena, CA 91109 USA.
[Gogineni, Prasad; Rodriguez-Morales, Fernando] Univ Kansas, Ctr Remote Sensing Ice Sheets, Lawrence, KS 66045 USA.
[Clark, Chris D.] Univ Sheffield, Dept Geog, Sheffield S10 2TN, S Yorkshire, England.
RP Jezek, K (reprint author), Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
RI Clark, Chris/C-3830-2009;
OI clark, chris/0000-0002-1021-6679
FU NASA Earth Science and Technology Office; NASA; National Science
Foundation
FX This research was supported by grants from the NASA Earth Science and
Technology Office, the NASA Cryosphere Program, and by the Office of
Polar Programs of the National Science Foundation.
NR 28
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U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 5
PY 2011
VL 38
AR L01501
DI 10.1029/2010GL045519
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 704NU
UT WOS:000286060500001
ER
PT J
AU Wray, JJ
Milliken, RE
Dundas, CM
Swayze, GA
Andrews-Hanna, JC
Baldridge, AM
Chojnacki, M
Bishop, JL
Ehlmann, BL
Murchie, SL
Clark, RN
Seelos, FP
Tornabene, LL
Squyres, SW
AF Wray, J. J.
Milliken, R. E.
Dundas, C. M.
Swayze, G. A.
Andrews-Hanna, J. C.
Baldridge, A. M.
Chojnacki, M.
Bishop, J. L.
Ehlmann, B. L.
Murchie, S. L.
Clark, R. N.
Seelos, F. P.
Tornabene, L. L.
Squyres, S. W.
TI Columbus crater and other possible groundwater-fed paleolakes of Terra
Sirenum, Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID THERMAL EMISSION SPECTROMETER; YELLOWSTONE-NATIONAL-PARK; SCIENCE
EXPERIMENT HIRISE; MERIDIANI-PLANUM; CLAY-MINERALS; REFLECTANCE
SPECTROSCOPY; OMEGA/MARS EXPRESS; MARTIAN HIGHLANDS;
INFRARED-SPECTROSCOPY; SOUTHERN HIGHLANDS
AB Columbus crater in the Terra Sirenum region of the Martian southern highlands contains light-toned layered deposits with interbedded sulfate and phyllosilicate minerals, a rare occurrence on Mars. Here we investigate in detail the morphology, thermophysical properties, mineralogy, and stratigraphy of these deposits; explore their regional context; and interpret the crater's aqueous history. Hydrated mineral-bearing deposits occupy a discrete ring around the walls of Columbus crater and are also exposed beneath younger materials, possibly lava flows, on its floor. Widespread minerals identified in the crater include gypsum, polyhydrated and monohydrated Mg/Fe-sulfates, and kaolinite; localized deposits consistent with montmorillonite, Fe/Mg-phyllosilicates, jarosite, alunite, and crystalline ferric oxide or hydroxide are also detected. Thermal emission spectra suggest abundances of these minerals in the tens of percent range. Other craters in northwest Terra Sirenum also contain layered deposits and Al/Fe/Mg-phyllosilicates, but sulfates have so far been found only in Columbus and Cross craters. The region's intercrater plains contain scattered exposures of Al-phyllosilicates and one isolated mound with opaline silica, in addition to more common Fe/Mg-phyllosilicates with chlorides. A Late Noachian age is estimated for the aqueous deposits in Columbus, coinciding with a period of inferred groundwater upwelling and evaporation, which (according to model results reported here) could have formed evaporites in Columbus and other craters in Terra Sirenum. Hypotheses for the origin of these deposits include groundwater cementation of crater-filling sediments and/or direct precipitation from subaerial springs or in a deep (similar to 900 m) paleolake. Especially under the deep lake scenario, which we prefer, chemical gradients in Columbus crater may have created a habitable environment at this location on early Mars. Citation: Wray, J. J., et al. (2011), Columbus crater and other possible groundwater-fed paleolakes of Terra Sirenum, Mars, J. Geophys. Res., 116, E01001, doi:10.1029/2010JE003694.
C1 [Wray, J. J.; Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Milliken, R. E.] Univ Notre Dame, Dept Civil Engn & Geol Sci, Notre Dame, IN 46556 USA.
[Dundas, C. M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Swayze, G. A.; Clark, R. N.] US Geol Survey, Denver, CO 80225 USA.
[Andrews-Hanna, J. C.] Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA.
[Baldridge, A. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chojnacki, M.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Bishop, J. L.] SETI Inst, Mountain View, CA 94043 USA.
[Ehlmann, B. L.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Murchie, S. L.; Seelos, F. P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Tornabene, L. L.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20024 USA.
RP Wray, JJ (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM jwray@astro.cornell.edu
RI Wray, James/B-8457-2008; Chojnacki, Matthew/A-4245-2013; Murchie,
Scott/E-8030-2015; Seelos, Frank/C-7875-2016
OI Wray, James/0000-0001-5559-2179; Dundas, Colin/0000-0003-2343-7224;
Chojnacki, Matthew/0000-0001-8497-8994; Murchie,
Scott/0000-0002-1616-8751; Seelos, Frank/0000-0001-9721-941X
FU Fannie & John Hertz Foundation; NSF
FX We thank S. Mattson and A. Dumke for their efforts producing HiRISE and
HRSC DEMs, respectively. Early reviews by J. K. Crowley, G. A.
Desborough, and S. A. Wilson Purdy as well as discussions with J. F.
Mustard, M. P. Golombek, N. A. Cabrol, J. A. Grant, D. J. Des Marais, V.
F. Chevrier, T. S. Altheide, and S. Karunatillake improved the paper. We
thank R. P. Irwin III and an anonymous reviewer for their thorough
attention to the manuscript. J.J.W. thanks the Fannie & John Hertz
Foundation and the NSF Graduate Research Fellowship for support. We
thank the HiRISE and CRISM science and operations teams for acquiring
the data most critical to our observations and interpretations.
NR 223
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U1 5
U2 31
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 JAN 5
PY 2011
VL 116
AR E01001
DI 10.1029/2010JE003694
PG 41
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 704NI
UT WOS:000286059300001
ER
PT J
AU Abbasi, R
Abdou, Y
Abu-Zayyad, T
Adams, J
Aguilar, JA
Ahlers, M
Andeen, K
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Bay, R
Alba, JLB
Beattie, K
Beatty, JJ
Bechet, S
Becker, JK
Becker, KH
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bose, D
Boser, S
Botner, O
Braun, J
Buitink, S
Carson, M
Chirkin, D
Christy, B
Clem, J
Clevermann, F
Cohen, S
Colnard, C
Cowen, DF
D'Agostino, MV
Danninger, M
Davis, JC
De Clercq, C
Demirors, L
Depaepe, O
Descamps, F
Desiati, P
de Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dierckxsens, M
Dreyer, J
Dumm, JP
Duvoort, MR
Ehrlich, R
Eisch, J
Ellsworth, RW
Engdegard, O
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feusels, T
Filimonov, K
Finley, C
Foerster, MM
Fox, BD
Franckowiak, A
Franke, R
Gaisser, TK
Gallagher, J
Geisler, M
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Goodman, JA
Grant, D
Griesel, T
Gross, A
Grullon, S
Gurtner, M
Ha, C
Hallgren, A
Halzen, F
Han, K
Hanson, K
Helbing, K
Herquet, P
Hickford, S
Hill, GC
Hoffman, KD
Homeier, A
Hoshina, K
Hubert, D
Huelsnitz, W
Hulss, JP
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobsen, J
Japaridze, GS
Johansson, H
Joseph, JM
Kampert, KH
Kappes, A
Karg, T
Karle, A
Kelley, JL
Kemming, N
Kenny, P
Kiryluk, J
Kislat, F
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Koskinen, DJ
Kowalski, M
Kowarik, T
Krasberg, M
Krings, T
Kroll, G
Kuehn, K
Kuwabara, T
Labare, M
Lafebre, S
Laihem, K
Landsman, H
Larson, MJ
Lauer, R
Lehmann, R
Lunemann, J
Madsen, J
Majumdar, P
Marotta, A
Maruyama, R
Mase, K
Matis, HS
Matusik, M
Meagher, K
Merck, M
Meszaros, P
Meures, T
Middell, E
Milke, N
Miller, J
Montaruli, T
Morse, R
Movit, SM
Nahnhauer, R
Nam, JW
Naumann, U
Niessen, P
Nygren, DR
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Ono, M
Panknin, S
Paul, L
de los Heros, CP
Petrovic, J
Piegsa, A
Pieloth, D
Porrata, R
Posselt, J
Price, PB
Prikockis, M
Przybylski, GT
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Rizzo, A
Rodrigues, JP
Roth, P
Rothmaier, F
Rott, C
Ruhe, T
Rutledge, D
Ruzybayev, B
Ryckbosch, D
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Schlenstedt, S
Schmidt, T
Schukraft, A
Schultes, A
Schulz, O
Schunck, M
Seckel, D
Semburg, B
Seo, SH
Sestayo, Y
Seunarine, S
Silvestri, A
Singh, K
Slipak, A
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stephens, G
Stezelberger, T
Stokstad, RG
Stoyanov, S
Strahler, EA
Straszheim, T
Sullivan, GW
Swillens, Q
Taavola, H
Taboada, I
Tamburro, A
Tarasova, O
Tepe, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Tosi, D
Turcan, D
van Eijndhoven, N
Vandenbroucke, J
Van Overloop, A
van Santen, J
Voge, M
Voigt, B
Walck, C
Waldenmaier, T
Wallraff, M
Walter, M
Weaver, C
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Wikstrom, G
Williams, DR
Wischnewski, R
Wissing, H
Wolf, M
Woschnagg, K
Xu, C
Xu, XW
Yodh, G
Yoshida, S
Zarzhitsky, P
AF Abbasi, R.
Abdou, Y.
Abu-Zayyad, T.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Andeen, K.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Bay, R.
Alba, J. L. Bazo
Beattie, K.
Beatty, J. J.
Bechet, S.
Becker, J. K.
Becker, K. -H.
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Buitink, S.
Carson, M.
Chirkin, D.
Christy, B.
Clem, J.
Clevermann, F.
Cohen, S.
Colnard, C.
Cowen, D. F.
D'Agostino, M. V.
Danninger, M.
Davis, J. C.
De Clercq, C.
Demiroers, L.
Depaepe, O.
Descamps, F.
Desiati, P.
de Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dierckxsens, M.
Dreyer, J.
Dumm, J. P.
Duvoort, M. R.
Ehrlich, R.
Eisch, J.
Ellsworth, R. W.
Engdegard, O.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feusels, T.
Filimonov, K.
Finley, C.
Foerster, M. M.
Fox, B. D.
Franckowiak, A.
Franke, R.
Gaisser, T. K.
Gallagher, J.
Geisler, M.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Goodman, J. A.
Grant, D.
Griesel, T.
Gross, A.
Grullon, S.
Gurtner, M.
Ha, C.
Hallgren, A.
Halzen, F.
Han, K.
Hanson, K.
Helbing, K.
Herquet, P.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Homeier, A.
Hoshina, K.
Hubert, D.
Huelsnitz, W.
Huelss, J. -P.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobsen, J.
Japaridze, G. S.
Johansson, H.
Joseph, J. M.
Kampert, K. -H.
Kappes, A.
Karg, T.
Karle, A.
Kelley, J. L.
Kemming, N.
Kenny, P.
Kiryluk, J.
Kislat, F.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Koskinen, D. J.
Kowalski, M.
Kowarik, T.
Krasberg, M.
Krings, T.
Kroll, G.
Kuehn, K.
Kuwabara, T.
Labare, M.
Lafebre, S.
Laihem, K.
Landsman, H.
Larson, M. J.
Lauer, R.
Lehmann, R.
Luenemann, J.
Madsen, J.
Majumdar, P.
Marotta, A.
Maruyama, R.
Mase, K.
Matis, H. S.
Matusik, M.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Middell, E.
Milke, N.
Miller, J.
Montaruli, T.
Morse, R.
Movit, S. M.
Nahnhauer, R.
Nam, J. W.
Naumann, U.
Niessen, P.
Nygren, D. R.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Ono, M.
Panknin, S.
Paul, L.
Perez de los Heros, C.
Petrovic, J.
Piegsa, A.
Pieloth, D.
Porrata, R.
Posselt, J.
Price, P. B.
Prikockis, M.
Przybylski, G. T.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Rizzo, A.
Rodrigues, J. P.
Roth, P.
Rothmaier, F.
Rott, C.
Ruhe, T.
Rutledge, D.
Ruzybayev, B.
Ryckbosch, D.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Schlenstedt, S.
Schmidt, T.
Schukraft, A.
Schultes, A.
Schulz, O.
Schunck, M.
Seckel, D.
Semburg, B.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Silvestri, A.
Singh, K.
Slipak, A.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stephens, G.
Stezelberger, T.
Stokstad, R. G.
Stoyanov, S.
Strahler, E. A.
Straszheim, T.
Sullivan, G. W.
Swillens, Q.
Taavola, H.
Taboada, I.
Tamburro, A.
Tarasova, O.
Tepe, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Tosi, D.
Turcan, D.
van Eijndhoven, N.
Vandenbroucke, J.
Van Overloop, A.
van Santen, J.
Voge, M.
Voigt, B.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Walter, M.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Wikstrom, G.
Williams, D. R.
Wischnewski, R.
Wissing, H.
Wolf, M.
Woschnagg, K.
Xu, C.
Xu, X. W.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
TI Measurement of the atmospheric neutrino energy spectrum from 100 GeV to
400 TeV with IceCube
SO PHYSICAL REVIEW D
LA English
DT Article
ID SOUTH-POLE; TRACK RECONSTRUCTION; OPTICAL-PROPERTIES; DEEP ICE;
TELESCOPES; ABSORPTION; SCATTERING; DETECTOR; AMANDA; FLUX
AB A measurement of the atmospheric muon neutrino energy spectrum from 100 GeV to 400 TeV was performed using a data sample of about 18 000 up-going atmospheric muon neutrino events in IceCube. Boosted decision trees were used for event selection to reject misreconstructed atmospheric muons and obtain a sample of up-going muon neutrino events. Background contamination in the final event sample is less than 1%. This is the first measurement of atmospheric neutrinos up to 400 TeV, and is fundamental to understanding the impact of this neutrino background on astrophysical neutrino observations with IceCube. The measured spectrum is consistent with predictions for the atmospheric nu(mu) + (nu) over bar (mu) flux.
C1 [Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Geisler, M.; Gluesenkamp, T.; Huelss, J. -P.; Krings, T.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Kappes, A.; Kemming, N.; Kolanoski, H.; Lehmann, R.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
[Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium.
[Bose, D.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Singh, K.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Gross, A.; Han, K.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Grant, D.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subatom & Radiat Phys, B-9000 Ghent, Belgium.
[Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Voge, M.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
[Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Berghaus, P.; Braun, J.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kelley, J. L.; Krasberg, M.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wikstrom, G.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wikstrom, G.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Prikockis, M.; Rutledge, D.; Slipak, A.; Stephens, G.; Toale, P. A.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; Olivo, M.; Perez de los Heros, C.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Duvoort, M. R.] Univ Utrecht, Dept Phys & Astron, SRON, NL-3584 CC Utrecht, Netherlands.
[Auffenberg, J.; Becker, K. -H.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Matusik, M.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schlenstedt, S.; Spiering, C.; Tarasova, O.; Tosi, D.; Voigt, B.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany.
[Montaruli, T.] Univ Bari, Dipartmento Fis, Sez INFN, I-70126 Bari, Italy.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Huelsnitz, W (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
EM whuelsnitz@icecube.umd.edu
RI Przybylski, Grzegorz/F-7474-2015; Aguilar Sanchez, Juan
Antonio/H-4467-2015; Taavola, Henric/B-4497-2011; Wiebusch,
Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012; Tamburro,
Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Hallgren,
Allan/A-8963-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014;
Koskinen, David/G-3236-2014; Maruyama, Reina/A-1064-2013; Sarkar,
Subir/G-5978-2011; Beatty, James/D-9310-2011;
OI Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Taavola,
Henric/0000-0002-2604-2810; Wiebusch, Christopher/0000-0002-6418-3008;
Auffenberg, Jan/0000-0002-1185-9094; Koskinen,
David/0000-0002-0514-5917; Maruyama, Reina/0000-0003-2794-512X; Sarkar,
Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Actis,
Oxana/0000-0001-8851-3983; Ter-Antonyan, Samvel/0000-0002-5788-1369;
Schukraft, Anne/0000-0002-9112-5479; Perez de los Heros,
Carlos/0000-0002-2084-5866; Carson, Michael/0000-0003-0400-7819; Hubert,
Daan/0000-0002-4365-865X; Benabderrahmane, Mohamed
Lotfi/0000-0003-4410-5886
FU U.S. National Science Foundation; Office of Polar Programs; Physics
Division, University of Wisconsin Alumni Research Foundation; Grid
Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of
Wisconsin-Madison; Open Science Grid (OSG) grid infrastructure;
U.S.Department of Energy; National Energy Research Scientific Computing
Center; Louisiana Optical Network Initiative (LONI) grid computing
resources; National Science and Engineering Research Council of Canada;
Swedish Research Council; Swedish Polar Research Secretariat; Swedish
National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg
Foundation, Sweden; German Ministry for Education and Research (BMBF);
Deutsche Forschungsgemeinschaft (DFG); Research Department of Plasmas
with Complex Interactions (Bochum), Germany; Fund for Scientific
Research (FNRS-FWO); FWO; Flanders Institute to encourage scientific and
technological research in industry (IWT); Belgian Federal Science Policy
Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New
Zealand; Japan Society for Promotion of Science (JSPS); Swiss National
Science Foundation (SNSF), Switzerland; EU; Capes Foundation; Ministry
of Education of Brazil
FX We acknowledge support from the following agencies: U.S. National
Science Foundation, Office of Polar Programs, U.S. National Science
Foundation, Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid
infrastructure; U.S.Department of Energy, and National Energy Research
Scientific Computing Center, the Louisiana Optical Network Initiative
(LONI) grid computing resources; National Science and Engineering
Research Council of Canada; Swedish Research Council, Swedish Polar
Research Secretariat, Swedish National Infrastructure for Computing
(SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF), Deutsche
Forschungsgemeinschaft (DFG), Research Department of Plasmas with
Complex Interactions (Bochum), Germany; Fund for Scientific Research
(FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage
scientific and technological research in industry (IWT), Belgian Federal
Science Policy Office (Belspo); University of Oxford, United Kingdom;
Marsden Fund, New Zealand; Japan Society for Promotion of Science
(JSPS); the Swiss National Science Foundation (SNSF), Switzerland. A.
Gro beta acknowledges support by the EU Marie Curie OIF Program. J.P.
Rodrigues acknowledges support by the Capes Foundation, Ministry of
Education of Brazil.
NR 45
TC 127
Z9 128
U1 2
U2 12
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD JAN 5
PY 2011
VL 83
IS 1
AR 012001
DI 10.1103/PhysRevD.83.012001
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 713TA
UT WOS:000286759100001
ER
PT J
AU Sanders, GB
Larson, WE
AF Sanders, Gerald B.
Larson, William E.
TI Integration of In-Situ Resource Utilization into lunar/Mars exploration
through field analogs
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE In-Situ Resource Utilization; ISRU; Analogs; Analogues; Field testing
AB The ability to extract and process resources at the site of exploration into useful products such as propellants, life support and power system consumables, and radiation and rocket exhaust plume debris shielding, known as In-Situ Resource Utilization or ISRU, has the potential to significantly reduce the launch mass, risk, and cost of robotic and human exploration of space. The incorporation of ISRU into missions can also significantly influence technology selection and system development in other areas such as power, life support, and propulsion. For example, the ability to extract or produce large amounts of oxygen and/or water in-situ could minimize the need to completely close life support air and water processing system cycles, change thermal and radiation protection of habitats, and influence propellant selection for ascent vehicles and surface propulsive hoppers. While concepts and even laboratory work on evaluating and developing ISRU techniques such as oxygen extraction from lunar regolith have been going on since before the Apollo 11 Moon landing, no ISRU system has ever flown in space, and only recently have ISRU technologies been developed at a scale and at a system level that is relevant to actual robotic and human mission applications. Because ISRU hardware and systems have never been demonstrated or utilized before on robotic or human missions, architecture and mission planners and surface system hardware developers are hesitant to rely on ISRU products and services that are critical to mission and system implementation success. To build confidence in ISRU systems for future missions and assess how ISRU systems can best influence and integrate with other surface system elements, NASA, with international partners, are performing analog field tests to understand how to take advantage of ISRU capabilities and benefits with the minimum of risk associated with introducing this game-changing approach to exploration. This paper will describe and review the results of four analog field tests (Moses Lake in 6/08, Mauna Kea in 11/08, Flagstaff in 9/09, and Mauna Kea in 1/10) that have begun the process of integrating ISRU into robotic and human exploration systems and missions, and propose future ISRU-related analog field test activities that can be performed in collaboration with non-US space agencies.
C1 [Sanders, Gerald B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Larson, William E.] NASA Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA.
RP Sanders, GB (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM gerald.b.sanders@nasa.gov; william.e.larson@nasa.gov
NR 14
TC 7
Z9 8
U1 2
U2 19
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 JAN 4
PY 2011
VL 47
IS 1
BP 20
EP 29
DI 10.1016/j.asr.2010.08.020
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 718ES
UT WOS:000287104500002
ER
PT J
AU Ponomarev, AL
Sundaresan, A
Vazquez, ME
Guida, P
Kim, A
Cucinotta, FA
AF Ponomarev, Artem L.
Sundaresan, Alamelu
Vazquez, Marcelo E.
Guida, Peter
Kim, Angela
Cucinotta, Francis A.
TI A model of the effects of heavy ion radiation on human tissue
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Heavy ions; Tissue irradiation; Tissue damage; Tissue toxicity; Cellular
apoptosis; Image segmentation
ID NEURONAL PROGENITOR CELLS; HIGH-LET RADIATION; DEPENDENCE; APOPTOSIS;
INDUCTION; DNA
AB In heavy ion radiotherapy and space travel humans are exposed to energetic heavy ions (C, Si, Fe and others). This type of irradiation often produces more severe biological effects per unit dose than more common X-rays. A new Monte Carlo model generates a physical space with the complex geometry of human tissue or a cell culture based model of tissue, which is affected by the passage of ionizing radiation. For irradiation, the model relies on a physical code for the ion track structure; for tissues, cellular maps are derived from two- or three-dimensional confocal microscopy images using image segmentation algorithm, which defines cells as pixilated volumes. The model is used to study tissue-specific statistics of direct ion hits and the remote ion action on cells. As an application of the technique, we considered the spatial pattern of apoptotic cells after heavy ion irradiation. The pattern of apoptosis is modeled as a stochastic process, which is defined by the action cross section taken from available experimental data. To characterize the degree of apoptosis, an autocorrelation function that describes the spatial correlation of apoptotic cells is introduced. The values of the autocorrelation function demonstrate the effect of the directionality of the radiation track on the spatial arrangements of inactivated cells in tissue. This effect is intrinsic only to high linear-energy-transfer radiation. (c) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Ponomarev, Artem L.] USRA, Houston, TX 77058 USA.
[Ponomarev, Artem L.; Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA.
[Sundaresan, Alamelu] Texas So Univ, Dept Biol, Houston, TX 77004 USA.
[Vazquez, Marcelo E.] Baylor Coll Med, Natl Space Biomed Res Inst, Houston, TX 77030 USA.
[Guida, Peter; Kim, Angela] Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Ponomarev, AL (reprint author), USRA, 3600 Space Ctr Blvd, Houston, TX 77058 USA.
EM artem.l.ponomarev@nasa.gov
FU NASA; office of science (BER) US DOE [OE-AI03-05ER64088]; US DOE
[DE-A103-05ER64088]; NSBRI [MCC 9-58-98, RE00202]
FX Funding was through the NASA Risk Assessment Project. Funding was
through NASA under the Risk Assessment Project (AP), and by the office
of science (BER) US DOE, Interagency Agreement No. OE-AI03-05ER64088
(FC). Support was provided by the US DOE (DE-A103-05ER64088) and the
NASA Space Radiation Program Risk Assessment Project. Support was
provided by NSBRI grant MCC 9-58-98, project RE00202 (MV, PG, AK).
NR 18
TC 1
Z9 1
U1 1
U2 6
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD JAN 4
PY 2011
VL 47
IS 1
BP 37
EP 48
DI 10.1016/j.asr.2010.08.014
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 718ES
UT WOS:000287104500004
ER
PT J
AU Weiss, NG
Hayes, MA
Garcia, AA
Ansari, RR
AF Weiss, Noah G.
Hayes, Mark A.
Garcia, Antonio A.
Ansari, Rafat R.
TI Isoelectric Focusing in a Drop
SO LANGMUIR
LA English
DT Article
ID NATURAL PH GRADIENTS; ON-A-CHIP; DIGITAL MICROFLUIDICS; SUPERHYDROPHOBIC
SURFACE; SEPARATION; CRYSTALLIZATION; AMPHOLYTES; PARTICLES; DNA
AB A novel approach to molecular separations is investigated using a technique termed droplet-based isoelectric focusing. Drops are manipulated discretely on a superhydrophobic surface, subjected to low voltages for isoelectric focusing, and split-resulting in a preparative separation. A universal indicator dye demonstrates the generation of stable, reversible pH gradients (3-10) in ampholyte buffers, and these gradients lead to protein focusing within the drop length. Focusing was visually characterized, spectroscopically verified, and assessed quantitatively by noninvasive light scattering measurements. It was found to correlate with a quantitative model based on 1D steady-state theory. This work illustrates that molecular separations can be deployed within a single open drop, and the differential fractions can be separated into new discrete liquid elements.
C1 [Garcia, Antonio A.] Arizona State Univ, Sch Biol & Hlth Syst Engn, Tempe, AZ 85287 USA.
[Weiss, Noah G.; Hayes, Mark A.] Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85287 USA.
[Ansari, Rafat R.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Garcia, AA (reprint author), Arizona State Univ, Sch Biol & Hlth Syst Engn, Tempe, AZ 85287 USA.
EM tony.garcia@asu.edu
FU NSF [CBET0925100]; NIH [2RO1EB004761-06, R21EB010191-01A1]
FX R.R.A. and A.A.G. acknowledge funding support provided by NSF
CBET0925100. M.A.H. acknowledges support in part with NIH grants
2RO1EB004761-06 and R21EB010191-01A1. Mr. Jim King's help at the NASA
John H. Glenn Research Center in setting up the light scattering
experiment is very much appreciated. R.R.A. thanks the Research and
Technology Division of NASA Glenn Research Center for laboratory
support.
NR 39
TC 5
Z9 7
U1 3
U2 13
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0743-7463
J9 LANGMUIR
JI Langmuir
PD JAN 4
PY 2011
VL 27
IS 1
BP 494
EP 498
DI 10.1021/la104085t
PG 5
WC Chemistry, Multidisciplinary; Chemistry, Physical; Materials Science,
Multidisciplinary
SC Chemistry; Materials Science
GA 697ZP
UT WOS:000285560400067
PM 21117663
ER
PT J
AU Lacelle, D
Davila, AF
Pollard, WH
Andersen, D
Heldmann, J
Marinova, M
McKay, CP
AF Lacelle, Denis
Davila, Alfonso F.
Pollard, Wayne H.
Andersen, Dale
Heldmann, Jennifer
Marinova, Margarita
McKay, Christopher P.
TI Stability of massive ground ice bodies in University Valley, McMurdo Dry
Valleys of Antarctica: Using stable O-H isotope as tracers of
sublimation in hyper-arid regions
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE massive ground ice; sublimation; permafrost; stable O-H isotopes;
McMurdo Dry Valleys
ID LAST GLACIAL MAXIMUM; BEACON VALLEY; EAST ANTARCTICA; CLIMATE; OXYGEN;
WATER; DEUTERIUM; HYDROGEN; CANADA; CORE
AB To date, studies of the stability of subsurface ice in the McMurdo Dry Valleys of Antarctica have been mainly based on climate-based vapor diffusion models. In University Valley (1800 m), a small glacier is found at the base of the head of the valley, and adjacent to the glacier, a buried body of massive ice was uncovered beneath 20-40 cm of loose cryotic sediments and sandstone boulders, This study assesses the origin and stability of the buried body of massive ice by measuring the geochemistry and stable O-H isotope composition of the ice and applies a sublimation and molecular diffusion model that accounts for the observed trends. The results indicate that the buried massive ice body represents an extension of the adjacent glacier that was buried by a rock avalanche during a cold climate period. The contrasting delta O-18 profiles and regression slope values between the uppermost 6 cm of the buried massive ice (upward convex delta O-18 profile and SD-18O = 5.1) and that below it (progressive increase in delta O-18 and SD-18O = 6.4) suggest independent post-depositional processes affected the isotope composition of the ice. The upward convex delta O-18 profile in the uppermost 6 cm is consistent with the ice undergoing sublimation. Using a sublimation and molecular diffusion model, and assuming that diffusion occurred through solid ice, the sublimation rate needed to fit the measured delta O-18 profile is 0.2 . 10(-3) mm yr(-1), a value that is more similar to net ice removal rates derived from He-3 data from cobbles in Beacon Valley till (7.0 . 10(-3) mm yr(-1)) than sublimation rates computed based on current climate (0.1-0.2 mm yr(-1)). We suggest that the climate-based sublimation rates are offset due to potential ice recharge mechanisms or to missing parameters, particularly the nature and thermo-physical properties of the overlying sediments (i.e., temperature, humidity, pore structure and ice content, grain size). (C) 2010 Elsevier B.V. All rights reserved.
C1 [Lacelle, Denis] Univ Ottawa, Dept Earth Sci, Ottawa, ON, Canada.
[Davila, Alfonso F.; Andersen, Dale] Carl Sagan Ctr Study Life Universe, SETI Inst, Mountain View, CA USA.
[Davila, Alfonso F.; Heldmann, Jennifer; Marinova, Margarita; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Pollard, Wayne H.] McGill Univ, Dept Geog, Montreal, PQ, Canada.
RP Lacelle, D (reprint author), Univ Ottawa, Dept Earth Sci, Ottawa, ON, Canada.
EM denis.lacelle@gmail.com
RI Davila, Alfonso/A-2198-2013;
OI Davila, Alfonso/0000-0002-0977-9909; Lacelle, Denis/0000-0002-6691-8717
FU NASA via NSF/OPP [B-302-M]
FX This work was supported by NASA's ASTEP program and with field support
via NSF/OPP (project B-302-M). We would like to thank the two reviewers
for their constructive comments on the manuscript.
NR 50
TC 13
Z9 13
U1 0
U2 16
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD JAN 3
PY 2011
VL 301
IS 1-2
BP 403
EP 411
DI 10.1016/j.epsl.2010.11.028
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 712CM
UT WOS:000286640400041
ER
PT S
AU Harvey, F
Raskin, RG
AF Harvey, Francis
Raskin, Robert G.
BE Ashish, N
Sheth, AP
TI Spatial Cyberinfrastructure: Building New Pathways for Geospatial
Semantics on Existing Infrastructures
SO GEOSPATIAL SEMANTICS AND THE SEMANIC WEB: FOUNDATIONS, ALGORITHMS, AND
APPLICATIONS
SE Semantic Web and Beyond-Computing for Human Experience
LA English
DT Article; Book Chapter
ID AUTOMATED GEOGRAPHY; GIS
AB Spatial data infrastructures (SDI), with technological and conceptual roots stretching back multiple decades, are moving into a new era through the development of spatial cyberinfrastructures (spatial CI) that account for geospatial semantics. While the technology and concepts share many similarities, spatial cyberinfrastructures distinctly focus on the provision of information to support scientific knowledge sharing. These cyberinfrastructures are increasingly connected into an ecology of scientific knowledge sharing based on the formalization of geospatial semantics and support for shared knowledge and collective intelligence. We trace the development of cyberinfrastructures from spatial data infrastructures as the potential framework for geospatial semantical interoperability. The chapter also points to substantial semantic research challenges and the potential of spatial cyberinfrastructures.
C1 [Harvey, Francis] Univ Minnesota, Dept Geog, Minneapolis, MN 55455 USA.
[Raskin, Robert G.] NASA, Sci Data Syst Sect, Jet Prop Lab, Pasadena, CA USA.
RP Harvey, F (reprint author), Univ Minnesota, Dept Geog, Minneapolis, MN 55455 USA.
EM fharvey@umn.edu; robert.g.raskin@jpl.nasa.gov
NR 39
TC 2
Z9 2
U1 2
U2 3
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 1559-7474
BN 978-1-4419-9445-5
J9 SEMAT WEB BEYOND-COM
PY 2011
VL 12
BP 87
EP 96
DI 10.1007/978-1-4419-9446-2_4
D2 10.1007/978-1-4419-9446-2
PG 10
WC Computer Science, Artificial Intelligence; Computer Science, Information
Systems; Computer Science, Theory & Methods
SC Computer Science
GA BVX98
UT WOS:000293120600004
ER
PT S
AU Yeom, K
AF Yeom, Kiwon
BE Kim, TH
Adeli, H
Fang, WC
Vasilakos, T
Stoica, A
Patrikakis, CZ
Zhao, G
Villalba, JG
Xiao, Y
TI Building Self-organizing Autonomic Agent Based on a Mobile Cell
SO COMMUNICATION AND NETWORKING, PT I
SE Communications in Computer and Information Science
LA English
DT Proceedings Paper
CT International Conference on Future Generation Communication and
Networking (FGCN 2011)
CY DEC 08-10, 2011-2012
CL Jeju Island, SOUTH KOREA
DE self-organization; federation of agents; modular agents
AB This paper proposes and evaluates a biologically inspired autonomous system that makes networked agents or applications to be autonomous, scalable. adaptive. With the proposed system. a network application consisting of an associate of agents is designed by decentralized agents, which are analogous to mobile cells that have ability to migrate in biological systems. Each agent has a unique functionality for network systems, and implements biological behaviors such as migration, replication, reproduction, and death. The proposed system allows agents to autonomously sense its surrounding environments to evaluate whether they adapts well to the sensed environment conditions. Empirical measurement results show that the agent adapts well to the dynamic environments.
C1 San Jose State Univ, Res Fdn, NASA Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
RP Yeom, K (reprint author), San Jose State Univ, Res Fdn, NASA Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
EM kiwon.yeom@nasa.gov
NR 22
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 1865-0929
BN 978-3-642-27191-5
J9 COMM COM INF SC
PY 2011
VL 265
BP 156
EP 165
PG 10
WC Computer Science, Artificial Intelligence; Computer Science, Information
Systems; Computer Science, Theory & Methods; Telecommunications
SC Computer Science; Telecommunications
GA BCO32
UT WOS:000310819300020
ER
PT J
AU Thomas, HE
Watson, IM
Carn, SA
Prata, AJ
Realmuto, VJ
AF Thomas, Helen E.
Watson, I. Matthew
Carn, Simon A.
Prata, Alfredo J.
Realmuto, Vincent J.
TI A comparison of AIRS, MODIS and OMI sulphur dioxide retrievals in
volcanic clouds
SO GEOMATICS NATURAL HAZARDS & RISK
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; MASAYA VOLCANO; 2007 ERUPTION; EMISSIONS;
NICARAGUA; ETNA
AB Volcanic degassing is a major contributor to the global sulphur dioxide (SO2) budget, characterized by quiescent emissions in the lower troposphere with sporadic, spatially variable explosive eruptions into the upper troposphere and lower stratosphere (UTLS). The volcanic input of SO2 to the atmosphere can be quantified using a suite of satellite-based instruments with a range of orbits and resolutions, resulting in differing estimates of SO2 extent and concentration from eruptions. We compare near-coincident retrievals of SO2 from the Moderate Resolution Imaging Spectroradiometer (MODIS), Atmospheric Infrared Radiation Sounder (AIRS) and Ozone Monitoring Instrument (OMI) at four eruptive settings. The OMI instrument is the most sensitive, with the ability to detect both low and high altitude clouds, but as an ultraviolet sensor, retrievals are limited to daytime, unlike the infrared sensors. AIRS retrievals are up to an order of magnitude less sensitive than OMI, restricted to water-free clouds in the upper troposphere. MODIS has the lowest sensitivity and is therefore constrained to the largest eruptions. Total tonnages from each sensor reflect these varying sensitivities along with potential calibration discrepancies. Results suggest that by using a number of instruments in synergy a more complete method of eruption detection is achieved.
C1 [Thomas, Helen E.; Watson, I. Matthew; Carn, Simon A.] Michigan Technol Univ, Dept Geol Min Engn & Sci, Houghton, MI 49931 USA.
[Watson, I. Matthew] Univ Bristol, Sch Earth Sci, Bristol BS8 IRJ, Avon, England.
[Prata, Alfredo J.] NILU, Dept Atmospher & Climate Res, N-2027 Kjeller, Norway.
[Realmuto, Vincent J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Thomas, HE (reprint author), Michigan Technol Univ, Dept Geol Min Engn & Sci, 630 Dow Environm Sci & Engn Bldg, Houghton, MI 49931 USA.
EM hethomas@mtu.edu
FU NASA [NNX 08AF80G]
FX The authors thank three anonymous reviewers whose detailed reviews have
greatly improved the content of this article. Helen Thomas acknowledges
funding from NASA grant NNX 08AF80G.
NR 37
TC 14
Z9 14
U1 1
U2 15
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 1947-5705
J9 GEOMAT NAT HAZ RISK
JI Geomat. Nat. Hazards Risk
PY 2011
VL 2
IS 3
SI SI
BP 217
EP 232
DI 10.1080/19475705.2011.564212
PG 16
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Water Resources
SC Geology; Meteorology & Atmospheric Sciences; Water Resources
GA 982QL
UT WOS:000307060400004
ER
PT S
AU Yeom, K
AF Yeom, Kiwon
BE Kim, TH
Adeli, H
Grosky, WI
Pissinou, N
Shih, TK
Rothwell, EJ
Kang, BH
Shin, SJ
TI Distributed Formation Control for Communication Relay with Position less
Flying Agents
SO MULTIMEDIA, COMPUTER GRAPHICS AND BROADCASTING, PT I
SE Communications in Computer and Information Science
LA English
DT Proceedings Paper
CT International Conference on Multimedia, Computer Graphics and
Broadcasting (MulGraB 2011)
CY DEC 08-10, 2011
CL Jeju Isl, SOUTH KOREA
DE distributed formation; swarm; flying agent; self-organization
ID ROBOTICS
AB Distributed formation of swarming with no coordinated agreement or positioning information is an interesting research area. This principle is applied to the development of ad-hoc wireless communication networks based on flying agent for finding ground users in disaster areas. We describe a decentralized self-control algorithm for coordinating a swarm of identical flying agents to spatially self-organize into arbitrary shapes using local communication maintaining a certain level of density. The proposed approach generates a shared coordinate system by flying agents which are continuously performing local trilateration, and achieves pre-defined shape formation by allowing agents to scatter within the defined 2D shape using virtual pheromones to maintain their communication pathways.
C1 San Jose State Univ, NASA, Human Syst Integrat Div, Ames Res Ctr,Res Fdn, Moffett Field, CA 94035 USA.
RP Yeom, K (reprint author), San Jose State Univ, NASA, Human Syst Integrat Div, Ames Res Ctr,Res Fdn, Moffett Field, CA 94035 USA.
EM kiwon.yeom@nasa.gov
NR 15
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 1865-0929
BN 978-3-642-27203-5
J9 COMM COM INF SC
PY 2011
VL 262
BP 18
EP 27
PG 10
WC Computer Science, Hardware & Architecture; Computer Science, Theory &
Methods
SC Computer Science
GA BCL22
UT WOS:000310546400003
ER
PT S
AU Pineda, JL
Goldsmith, PF
Chapman, NL
Snell, R
Li, D
Cambresy, L
Brunt, C
AF Pineda, J. L.
Goldsmith, P. F.
Chapman, N. L.
Snell, R.
Li, D.
Cambresy, L.
Brunt, C.
BE Rollig, M
Simon, R
Ossenkopf, V
Stutzki, J
TI THE RELATION BETWEEN DUST AND GAS IN THE TAURUS MOLECULAR CLOUD
SO CONDITIONS AND IMPACT OF STAR FORMATION: NEW RESULTS WITH HERSCHEL AND
BEYOND
SE EAS Publications Series
LA English
DT Proceedings Paper
CT 5th Zermatt ISM Symposium Conditions and Impact of Star Formation: New
Results with Herschel and Beyond
CY SEP 19-24, 2010
CL Zermatt, SWITZERLAND
SP Deutsch Forschungsgemeinschaft, Int Stiftung Hochalpine Forschungstationen Jungfraujoch & Gornergrat, Burgergemeinde Zermatt, Gornergrat Monte Rosa Bahn
ID DARK CLOUD
AB We report a study of the relation between dust and gas over a 100 deg(2) area in the Taurus molecular cloud. We compare the H-2 column density derived from dust extinction with the CO column density derived from the (CO)-C-12 and (CO)-C-13 J = 1 -> 0 lines. We derive the visual extinction from reddening determined from 2MASS data. The comparison is done at an angular size of 200 '', corresponding to 0.14 pc at a distance of 140 pc. We find that the relation between visual extinction A(V) and N(CO) is linear between A(V) similar or equal to 3 and 10 mag in the region associated with the B213-L1495 filament. In other regions the linear relation flattens for A(V) greater than or similar to 4 mag. Accounting for the observed relation between the column density of CO and CO2 ices and A(V), we find a linear relationship between the column of carbon monoxide and dust for observed visual extinctions up to the maximum value in our data similar or equal to 23 mag.
C1 [Pineda, J. L.; Goldsmith, P. F.; Chapman, N. L.; Li, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Pineda, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Jorge.Pineda@jpl.nasa.gov; Paul.F.Goldsmith@jpl.nasa.gov;
dili@jpl.nasa.gov; cambresy@astro.unistra.fr
NR 4
TC 0
Z9 0
U1 0
U2 2
PU E D P SCIENCES
PI CEDEX A
PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A,
FRANCE
SN 1633-4760
BN 978-2-7598-0696-6
J9 EAS PUBLICATIONS
PY 2011
VL 52
BP 157
EP +
DI 10.1051/eas/1152025
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BCA60
UT WOS:000309482300025
ER
PT S
AU Vaillancourt, JE
Dowell, CD
Jones, TJ
Novak, G
Chuss, DT
Crutcher, RM
Dotson, JL
Harper, DA
Hildebrand, RH
Houde, M
Krejny, MM
Lazarian, A
Looney, L
Stephens, IM
Tassis, K
Werner, MW
AF Vaillancourt, J. E.
Dowell, C. D.
Jones, T. J.
Novak, G.
Chuss, D. T.
Crutcher, R. M.
Dotson, J. L.
Harper, D. A.
Hildebrand, R. H.
Houde, M.
Krejny, M. M.
Lazarian, A.
Looney, L.
Stephens, I. M.
Tassis, K.
Werner, M. W.
BE Rollig, M
Simon, R
Ossenkopf, V
Stutzki, J
TI FAR-INFRARED POLARIMETRY OF THE INTERSTELLAR MEDIUM
SO CONDITIONS AND IMPACT OF STAR FORMATION: NEW RESULTS WITH HERSCHEL AND
BEYOND
SE EAS Publications Series
LA English
DT Proceedings Paper
CT 5th Zermatt ISM Symposium Conditions and Impact of Star Formation: New
Results with Herschel and Beyond
CY SEP 19-24, 2010
CL Zermatt, SWITZERLAND
SP Deutsch Forschungsgemeinschaft, Int Stiftung Hochalpine Forschungstationen Jungfraujoch & Gornergrat, Burgergemeinde Zermatt, Gornergrat Monte Rosa Bahn
ID MAGNETIC-FIELDS; POLARIZATION SPECTRUM; MOLECULAR CLOUDS; GRAIN
ALIGNMENT; STAR-FORMATION; EMISSION
AB Polarimetry at far-infrared wavelengths is a key tool for studying physical processes on size scales ranging from interstellar dust grains to entire galaxies. A multi-wavelength continuum polarimeter at these wavelengths will allow studies of thermal dust polarization in an effort to constrain the grains' physical properties and test grain alignment theory. High spatial resolution (5-30 arcsec) and sensitive observations will measure the influence of magnetic fields on infrared cirrus clouds, the envelopes and disks of YSOs, outflows from both low- and high-mass star forming regions, and the relative strength of magnetic, gravitational, and turbulent effects in star- and cloud-formation.
C1 [Vaillancourt, J. E.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Univ Space Res Assoc, Moffett Field, CA 94035 USA.
RP Vaillancourt, JE (reprint author), NASA, Ames Res Ctr, SOFIA Sci Ctr, Univ Space Res Assoc, Moffett Field, CA 94035 USA.
EM jvaillancourt@sofia.usra.edu
OI Vaillancourt, John/0000-0001-8916-1828
NR 25
TC 0
Z9 0
U1 0
U2 0
PU E D P SCIENCES
PI CEDEX A
PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A,
FRANCE
SN 1633-4760
BN 978-2-7598-0696-6
J9 EAS PUBLICATIONS
PY 2011
VL 52
BP 259
EP 262
DI 10.1051/eas/1152042
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BCA60
UT WOS:000309482300042
ER
PT S
AU Neudeck, PG
Krasowski, MJ
Prokop, NF
AF Neudeck, P. G.
Krasowski, M. J.
Prokop, N. F.
BE Shenai, K
Garg, R
Ma, R
Dudley, M
Khan, A
TI Assessment of Durable SiC JFET Technology for+600 degrees C to-125
degrees C Integrated Circuit Operation
SO GALLIUM NITRIDE AND SILICON CARBIDE POWER TECHNOLOGIES
SE ECS Transactions
LA English
DT Proceedings Paper
CT Symposium on GaN and SiC Power Technologies held during the 220th
Meeting of the Electrochemical-Society
CY OCT 09-14, 2011
CL Boston, MA
SP Electrochem Soc, Dielect Sci & Technol, Elect & Photon
ID SILICON-CARBIDE; TEMPERATURE; IMPLANTATION; ALUMINUM; DEFECTS
AB Electrical characteristics and circuit design considerations for prototype 6H-SiC JFET integrated circuits (ICs) operating over the broad temperature range of -125 degrees C to +600 degrees C are described. Strategic implementation of circuits with transistors and resistors in the same 6H-SiC n-channel layer enabled ICs with nearly temperature-independent functionality to be achieved. The frequency performance of the circuits declined at temperatures increasingly below or above room temperature, roughly corresponding to the change in 6H-SiC n-channel resistance arising from incomplete carrier ionization at low temperature and decreased electron mobility at high temperature. In addition to very broad temperature functionality, these simple digital and analog demonstration integrated circuits successfully operated with little change in functional characteristics over the course of thousands of hours at 500 degrees C before experiencing interconnect-related failures. With appropriate further development, these initial results establish a new technology foundation for realizing durable 500 degrees C ICs for combustion engine sensing and control, deep-well drilling, and other harsh-environment applications.
C1 [Neudeck, P. G.; Krasowski, M. J.; Prokop, N. F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 46
TC 8
Z9 9
U1 0
U2 2
PU ELECTROCHEMICAL SOC INC
PI PENNINGTON
PA 65 S MAIN ST, PENNINGTON, NJ 08534-2839 USA
SN 1938-5862
BN 978-1-60768-262-2
J9 ECS TRANSACTIONS
PY 2011
VL 41
IS 8
BP 163
EP 176
DI 10.1149/1.3631494
PG 14
WC Electrochemistry; Engineering, Electrical & Electronic; Physics, Applied
SC Electrochemistry; Engineering; Physics
GA BCB39
UT WOS:000309600300015
ER
PT B
AU Del Zanna, L
Landi, S
Matteini, L
Velli, M
AF Del Zanna, L.
Landi, S.
Matteini, L.
Velli, M.
BE Pogorelov, NV
Font, JA
Audit, E
Zank, GP
TI The Expanding Box Model in ECHO: Application to the Parametric Decay of
Alfven Waves in the Fast Solar Wind
SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2011
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 6th Annual International Conference on Numerical Modeling of Space
Plasma Flows
CY JUN 13-17, 2011
CL Valencia, SPAIN
SP Univ Alabama, Ctr Space Plasma & Aeronom Res, French Commissariat Atom Energy, Inst Investigat Fundamental Laws Universe
ID NONLINEAR EVOLUTION; SIMULATIONS; INSTABILITY; FLUCTUATIONS
AB The nonlinear evolution and the decay instability of monochromatic Alfven waves in the fast solar wind is studied through MHD numerical simulations taking into account the effects of the radial expansion of the background plasma. This is achieved by means of the expanding box model, a local approach which allows to maintain Cartesian coordinates and periodical boundary conditions. In this contribution we discuss the implementation of the model in the ECHO code and we present preliminary results of the decay instability in the presence of radial expansion effects.
C1 [Del Zanna, L.; Landi, S.; Matteini, L.] Univ Florence, Dipartimento Fis & Astron, I-50121 Florence, Italy.
[Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Del Zanna, L (reprint author), Univ Florence, Dipartimento Fis & Astron, I-50121 Florence, Italy.
EM ldz@arcetri.astro.it
RI Del Zanna, Luca/N-5598-2015
OI Del Zanna, Luca/0000-0001-5200-882X
FU NASA; Italian Space Agency (ASI); National Institute of Astrophysics
(INAF)
FX This work was carried out in part at the Jet Propulsion Laboratory under
a contract with NASA. We also acknowledge support from the Italian Space
Agency (ASI contract) and the National Institute of Astrophysics (INAF).
NR 22
TC 3
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U1 0
U2 2
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-800-8
J9 ASTR SOC P
PY 2011
VL 459
BP 196
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BCC77
UT WOS:000309737100031
ER
PT B
AU Yee, HC
Kotov, DV
Sjogreen, B
AF Yee, H. C.
Kotov, D. V.
Sjoegreen, B.
BE Pogorelov, NV
Font, JA
Audit, E
Zank, GP
TI Numerical Dissipation and Wrong Propagation Speed of Discontinuities For
Stiff Source Terms
SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2011
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 6th Annual International Conference on Numerical Modeling of Space
Plasma Flows
CY JUN 13-17, 2011
CL Valencia, SPAIN
SP Univ Alabama, Ctr Space Plasma & Aeronom Res, French Commissariat Atom Energy, Inst Investigat Fundamental Laws Universe
AB In compressible turbulent combustion/nonequilibrium flows, the constructions of numerical schemes for (a) stable and accurate simulation of turbulence with strong shocks, and (b) obtaining correct propagation speed of discontinuities for stiff reacting terms on "coarse grids" share one important ingredient - minimization of numerical dissipation while maintaining numerical stability. This dual requirement to achieve both numerical stability and accuracy with zero or minimal use of numerical dissipation is most often conflicting for existing schemes that were designed for non-reacting flows. The goal of this paper is to relate numerical dissipations that are inherited in a selected set of high order shock-capturing schemes with the onset of wrong propagation speed of discontinuities for two representative stiff detonation wave problems.
C1 [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kotov, D. V.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA.
[Sjoegreen, B.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
RP Yee, HC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU DOE/SciDAC SAP [DE-AI02-06ER25796]; Center for Turbulence Research,
Stanford University; NASA Fundamental Aeronautics (Hypersonic); U.S.
Department of Energy; Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]
FX The support of the DOE/SciDAC SAP grant DE-AI02-06ER25796 is
acknowledged. The work was performed by the second author as a postdoc
fellow at the Center for Turbulence Research, Stanford University. The
financial support from the NASA Fundamental Aeronautics (Hypersonic)
program for the first author is gratefully acknowledged. The work by the
third author was performed under the auspices of the U.S. Department of
Energy by Lawrence Livermore National Laboratory under Contract
DE-AC52-07NA27344.
NR 23
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PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-800-8
J9 ASTR SOC P
PY 2011
VL 459
BP 359
EP +
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BCC77
UT WOS:000309737100056
ER
PT S
AU DeKock, B
Sanders, D
VanZwieten, T
Capo-Lugo, P
AF DeKock, Brandon
Sanders, Devon
VanZwieten, Tannen
Capo-Lugo, Pedro
BE Miller, KB
TI DESIGN AND INTEGRATION OF AN ALL-MAGNETIC ATTITUDE CONTROL SYSTEM FOR
FASTSAT-HSV01'S MULTIPLE POINTING OBJECTIVES
SO GUIDANCE AND CONTROL 2011
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 34th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 04-09, 2011
CL Breckenridge, CO
SP Amer Astronaut Soc
AB The FASTSAT-HSV01 spacecraft is a microsatellite with magnetic torque rods as its sole attitude control actuator. FASTSAT's multiple payloads and mission functions require the Attitude Control System (ACS) to maintain Local Vertical Local Horizontal (LVLH)-referenced attitudes without spin-stabilization, while the pointing errors for some attitudes be significantly smaller than the previous best-demonstrated for this type of control system. The mission requires the ACS to hold multiple stable, unstable, and non-equilibrium attitudes, as well as eject a 3U Cube Sat from an onboard P-POD and recover from the ensuing tumble. This paper describes the ACS, the reasons for design choices, how the ACS integrates with the rest of the spacecraft, and gives recommendations for potential future applications of the work.
C1 [DeKock, Brandon] BdSystems, Space Engn Technol Div, Huntsville, AL USA.
RP Sanders, D (reprint author), NASA, George C Marshall Space Flight Ctr, EV41, Huntsville, AL 35812 USA.
EM devon.s.sanders@nasa.gov
NR 5
TC 0
Z9 0
U1 1
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-571-8
J9 ADV ASTRONAUT SCI
PY 2011
VL 141
BP 127
EP 145
PG 19
WC Automation & Control Systems; Engineering, Aerospace
SC Automation & Control Systems; Engineering
GA BBY65
UT WOS:000308840900008
ER
PT S
AU Holt, GN
Getchius, J
Tracy, WH
AF Holt, Greg N.
Getchius, Joel
Tracy, William H.
BE Miller, KB
TI INITIAL CONSIDERATIONS FOR NAVIGATION AND FLIGHT DYNAMICS OF A CREWED
NEAR-EARTH OBJECT MISSION
SO GUIDANCE AND CONTROL 2011
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 34th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 04-09, 2011
CL Breckenridge, CO
SP Amer Astronaut Soc
ID TRAJECTORY DESIGN
AB A crewed mission to a Near-Earth Object (NEO) was recently identified as a NASA Space Policy goal and priority. In support of this goal, a study was conducted to identify the initial considerations for performing the navigation and flight dynamics tasks of this mission class. Although missions to a NEO are not new, the unique factors involved in human spaceflight present challenges that warrant special examination. During the cruise phase of the mission, one of the most challenging factors is the noisy acceleration environment associated with a crewed vehicle. Additionally, the presence of a human crew necessitates a timely return trip, which may need to be expedited in an emergency situation where the mission is aborted. Tracking, navigation, and targeting results are shown for sample human-class trajectories to NEOs. Additionally, the benefit of in-situ navigation beacons on robotic precursor missions is presented. This mission class will require a longer duration flight than Apollo and, unlike previous human missions, there will likely be limited communication and tracking availability. This will necessitate the use of more onboard navigation and targeting capabilities. Finally, the rendezvous and proximity operations near an asteroid will be unlike anything previously attempted in a crewed spaceflight. The unknown gravitational environment and physical surface properties of the NEO may cause the rendezvous to behave differently than expected. Symbiosis of the human pilot and onboard navigation/targeting are presented which give additional robustness to unforeseen perturbations.
C1 [Holt, Greg N.] NASA, Flight Dynam Nav, Mission Operat, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Holt, GN (reprint author), NASA, Flight Dynam Nav, Mission Operat, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 10
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 978-0-87703-571-8
J9 ADV ASTRONAUT SCI
PY 2011
VL 141
BP 285
EP 301
PG 17
WC Automation & Control Systems; Engineering, Aerospace
SC Automation & Control Systems; Engineering
GA BBY65
UT WOS:000308840900016
ER
PT S
AU Cangahuala, LA
Broschart, S
Acikmese, B
Mandic, M
Blackmore, L
Riedel, E
Bayard, D
Wallace, M
AF Cangahuala, L. Alberto
Broschart, Stephen
Acikmese, Behcet
Mandic, Milan
Blackmore, Lars
Riedel, Ed
Bayard, David
Wallace, Mark
BE Miller, KB
TI GN&C TRADES FOR TOUCH-AND-GO SAMPLING AT SMALL BODIES
SO GUIDANCE AND CONTROL 2011
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 34th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 04-09, 2011
CL Breckenridge, CO
SP Amer Astronaut Soc
ID MARTIAN SATELLITES; GRAVITY
AB Touch-And-Go (TAG) is an approach for asteroid/comet sample collection different from any other robotic mission phase. At a high level, the primary engineering trade is to optimize (a) the maximum integral of sample collection rate vs. operating duration of the hardware against (b) safety considerations for the spacecraft while preserving sample integrity and quality. There are several design choices that need to be made for a given sample collection approach, including required GN&C autonomy (beyond baseline capabilities), thruster suite capabilities, fault detection augmentations, control strategy, etc. This paper describes two TAG design examples (at comet Tempel 1 and Deimos) and shows how the target body and science goals force differences in the two designs. The paper documents (a) TAG functions and concept of operations, (b) design constraints and assumptions, (c) contact considerations such as position, velocity, orientation, and duration, and (d) forecasted safety margins and sample collection performance based on high fidelity simulations. In addition, the paper describes GN&C considerations and capabilities for sample verification.
C1 [Cangahuala, L. Alberto; Broschart, Stephen; Acikmese, Behcet; Mandic, Milan; Blackmore, Lars; Riedel, Ed; Bayard, David; Wallace, Mark] CALTECH, Jet Prop Lab, Autonomous Syst Div, Pasadena, CA 91109 USA.
RP Cangahuala, LA (reprint author), CALTECH, Jet Prop Lab, Autonomous Syst Div, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 25
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 978-0-87703-571-8
J9 ADV ASTRONAUT SCI
PY 2011
VL 141
BP 385
EP 401
PG 17
WC Automation & Control Systems; Engineering, Aerospace
SC Automation & Control Systems; Engineering
GA BBY65
UT WOS:000308840900022
ER
PT S
AU Naasz, BJ
Strube, M
Van Eepoel, J
Barbee, BW
Getzandanner, KM
AF Naasz, Bo J.
Strube, Matthew
Van Eepoel, John
Barbee, Brent W.
Getzandanner, Kenneth M.
BE Miller, KB
TI SATELLITE SERVICING'S AUTONOMOUS RENDEZVOUS AND DOCKING TESTBED ON THE
INTERNATIONAL SPACE STATION
SO GUIDANCE AND CONTROL 2011
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 34th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 04-09, 2011
CL Breckenridge, CO
SP Amer Astronaut Soc
AB The Space Servicing Capabilities Project (SSCP) at NASA's Goddard Space Flight Center (GSFC) has been tasked with developing systems for servicing space assets. Starting in 2009, the SSCP completed a study documenting potential customers and the business case for servicing, as well as defining several notional missions and required technologies. In 2010, SSCP moved to the implementation stage by completing several ground demonstrations and commencing development of two International Space Station (ISS) payloads-the Robotic Refueling Mission (RRM) and the Dextre Pointing Package (DPP)-to mitigate new technology risks for a robotic mission to service existing assets in geosynchronous orbit. This paper introduces the DPP, scheduled to fly in July of 2012 on the third operational SpaceX Dragon mission, and its Autonomous Rendezvous and Docking (AR&D) instruments. The combination of sensors and advanced avionics provide valuable on-orbit demonstrations of essential technologies for servicing existing vehicles, both cooperative and non-cooperative.
C1 [Naasz, Bo J.; Strube, Matthew; Van Eepoel, John; Barbee, Brent W.; Getzandanner, Kenneth M.] NASA GSFC, Greenbelt, MD 20771 USA.
RP Naasz, BJ (reprint author), NASA GSFC, Code 595,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
NR 17
TC 0
Z9 0
U1 1
U2 6
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-571-8
J9 ADV ASTRONAUT SCI
PY 2011
VL 141
BP 483
EP 503
PG 21
WC Automation & Control Systems; Engineering, Aerospace
SC Automation & Control Systems; Engineering
GA BBY65
UT WOS:000308840900028
ER
PT S
AU O'Donnell, JR
Bourkland, KL
Hsu, OC
Liu, KC
Mason, PAC
Morgenstern, WM
Russo, AM
Starin, SR
Vess, MF
AF O'Donnell, James R., Jr.
Bourkland, Kristin L.
Hsu, Oscar C.
Liu, Kuo-Chia (Alice)
Mason, Paul A. C.
Morgenstern, Wendy M.
Russo, Angela M.
Starin, Scott R.
Vess, Melissa F.
BE Miller, KB
TI SOLAR DYNAMICS OBSERVATORY LAUNCH AND COMMISSIONING
SO GUIDANCE AND CONTROL 2011
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 34th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 04-09, 2011
CL Breckenridge, CO
SP Amer Astronaut Soc
AB The Solar Dynamics Observatory (SDO) was launched on February 11, 2010. Over the next three months, the spacecraft was raised from its launch orbit into its final geosynchronous orbit and its systems and instruments were tested and calibrated in preparation for its desired ten year science mission studying the Sun. A great deal of activity during this time involved the spacecraft attitude control system (ACS); testing control modes, calibrating sensors and actuators, and using the ACS to help commission the spacecraft instruments and to control the propulsion system as the spacecraft was maneuvered into its final orbit.
This paper will discuss the chronology of the SDO launch and commissioning, showing the ACS analysis work performed to diagnose propellant slosh transient and attitude oscillation anomalies that were seen during commissioning, and to determine how to overcome them. The simulations and tests devised to demonstrate correct operation of all onboard ACS modes and the activities in support of instrument calibration will be discussed and the final maneuver plan performed to bring SDO on station will be shown. In addition to detailing these commissioning and anomaly resolution activities, the unique set of tests performed to characterize SDO's on-orbit jitter performance will be discussed.
C1 [O'Donnell, James R., Jr.; Bourkland, Kristin L.; Hsu, Oscar C.; Liu, Kuo-Chia (Alice); Mason, Paul A. C.; Morgenstern, Wendy M.; Russo, Angela M.; Starin, Scott R.; Vess, Melissa F.] NASA, Goddard Space Flight Ctr, Attitude Control Syst Engn Branch, Greenbelt, MD 20771 USA.
RP O'Donnell, JR (reprint author), NASA, Goddard Space Flight Ctr, Attitude Control Syst Engn Branch, Mail Code 591, Greenbelt, MD 20771 USA.
NR 10
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 978-0-87703-571-8
J9 ADV ASTRONAUT SCI
PY 2011
VL 141
BP 565
EP 590
PG 26
WC Automation & Control Systems; Engineering, Aerospace
SC Automation & Control Systems; Engineering
GA BBY65
UT WOS:000308840900033
ER
PT S
AU Blackmore, L
Murray, E
Scharf, DP
Aung, M
Bayard, D
Brugarolas, P
Hadaegh, F
Kang, B
Lee, A
Milman, M
Sirlin, S
AF Blackmore, Lars
Murray, Emmanuel
Scharf, Daniel P.
Aung, MiMi
Bayard, David
Brugarolas, Paul
Hadaegh, Fred
Kang, Bryan
Lee, Allan
Milman, Mark
Sirlin, Sam
BE Miller, KB
TI INSTRUMENT POINTING CAPABILITIES: PAST, PRESENT AND FUTURE
SO GUIDANCE AND CONTROL 2011
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 34th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 04-09, 2011
CL Breckenridge, CO
SP Amer Astronaut Soc
AB This paper surveys the instrument pointing capabilities of past, present and future space telescopes and interferometers. As an important aspect of this survey, we present a taxonomy for "apples-to-apples" comparisons of pointing performances. First, pointing errors are defined relative to either an inertial frame or a celestial target. Pointing error can then be further sub-divided into DC, that is, steady state, and AC components. We refer to the magnitude of the DC error relative to the inertial frame as absolute pointing accuracy, and we refer to the magnitude of the DC error relative to a celestial target as relative pointing accuracy. The magnitude of the AC error is referred to as pointing stability. While an AC/DC partition is not new, we leverage previous work by some of the authors to quantitatively clarify and compare varying definitions of jitter and time window averages. With this taxonomy and for sixteen past, present, and future missions, pointing accuracies and stabilities, both required and achieved, are presented. In addition, we describe the attitude control technologies used to and, for future missions, planned to achieve these pointing performances.
C1 [Blackmore, Lars; Murray, Emmanuel; Scharf, Daniel P.; Bayard, David; Brugarolas, Paul; Hadaegh, Fred; Kang, Bryan; Milman, Mark; Sirlin, Sam] CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, Pasadena, CA 91109 USA.
RP Blackmore, L (reprint author), CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, 4800 Oak Grove Dr,M-S 198-326, Pasadena, CA 91109 USA.
NR 34
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 978-0-87703-571-8
J9 ADV ASTRONAUT SCI
PY 2011
VL 141
BP 675
EP 692
PG 18
WC Automation & Control Systems; Engineering, Aerospace
SC Automation & Control Systems; Engineering
GA BBY65
UT WOS:000308840900039
ER
PT S
AU Carpenter, JR
Markley, FL
AF Carpenter, J. Russell
Markley, F. Landis
BE Coffey, SL
Junkins, JL
Luu, KK
Ross, IM
Sabol, C
Schumacher, PW
TI SEQUENTIAL PROBABILITY RATIO TEST FOR COLLISION AVOIDANCE MANEUVER
DECISIONS
SO KYLE T. ALFRIEND ASTRODYNAMICS SYMPOSIUM
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT American-Astronautical-Society Kyle T Alfriend Astrodynamics Symposium
CY MAY 17-19, 2010
CL Monterey, CA
SP Amer Astronaut Soc, Space Flight Mech Comm
AB When facing a conjunction between space objects, decision makers must choose whether to maneuver for collision avoidance or not. We apply a well-known decision procedure, the sequential probability ratio test, to this problem. We propose two approaches to the problem solution, one based on a frequentist method, and the other on a Bayesian method. The frequentist method does not require any prior knowledge concerning the conjunction, while the Bayesian method assumes knowledge of prior probability densities. Our results show that both methods achieve desired missed detection rates, but the frequentist method's false alarm performance is inferior to the Bayesian method's.
C1 [Carpenter, J. Russell] NASA, Nav & Mission Design Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Carpenter, JR (reprint author), NASA, Nav & Mission Design Branch, Goddard Space Flight Ctr, Code 595, Greenbelt, MD 20771 USA.
NR 9
TC 0
Z9 0
U1 0
U2 2
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-565-7
J9 ADV ASTRONAUT SCI
PY 2011
VL 139
BP 267
EP 280
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BCA64
UT WOS:000309482700017
ER
PT S
AU Gaebler, J
Hur-Diaz, S
Carpenter, R
AF Gaebler, John
Hur-Diaz, Sun
Carpenter, Russell
BE Coffey, SL
Junkins, JL
Luu, KK
Ross, IM
Sabol, C
Schumacher, PW
TI COMPARISON OF SIGMA-POINT AND EXTENDED KALMAN FILTERS ON A REALISTIC
ORBIT DETERMINATION SCENARIO
SO KYLE T. ALFRIEND ASTRODYNAMICS SYMPOSIUM
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT American-Astronautical-Society Kyle T Alfriend Astrodynamics Symposium
CY MAY 17-19, 2010
CL Monterey, CA
SP Amer Astronaut Soc, Space Flight Mech Comm
AB Sigma-point filters have received a lot of attention in recent years as a better alternative to extended Kalman filters for highly nonlinear problems. In this paper, we compare the performance of the additive divided difference sigma-point filter to the extended Kalman filter when applied to orbit determination of a realistic operational scenario based on the Interstellar Boundary Explorer mission. For the scenario studied, both filters provided equivalent results. The performance of each is discussed in detail.
C1 [Gaebler, John; Carpenter, Russell] NASA, Nav & Mission Design Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gaebler, J (reprint author), NASA, Nav & Mission Design Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 8
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 978-0-87703-565-7
J9 ADV ASTRONAUT SCI
PY 2011
VL 139
BP 319
EP 325
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BCA64
UT WOS:000309482700020
ER
PT B
AU Chuss, DT
Voellmer, G
Wollack, EJ
Moseley, SH
Novak, G
Krejny, M
Walker, CK
Kulesa, C
D'Aubigny, CYD
Golish, D
Loewenstein, RF
Bennett, CL
Zeng, LZ
Eimer, J
AF Chuss, David T.
Voellmer, George
Wollack, Edward J.
Moseley, S. Harvey
Novak, Giles
Krejny, Megan
Walker, Christopher K.
Kulesa, Craig
D'Aubigny, Christian Y. Drouet
Golish, Dathon
Loewenstein, Robert F.
Bennett, Charles L.
Zeng, Lingzhen
Eimer, Joseph
BE Bastien, P
Manset, N
Clemens, DP
StLouis, N
TI Variable-delay Polarization Modulators (VPMs) for Far-infrared through
Millimeter Astronomy
SO ASTRONOMICAL POLARIMETRY 2008: SCIENCE FROM SMALL TO LARGE TELESCOPES
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Astronomical Polarimetry 2008 - Science from Small to
Large Telescopes
CY JUL 06-11, 2008
CL La Malbaie, CANADA
SP Canadian Inst Theoret Astrophys, Univ Montreal, Fac Arts & Sci, Ctr Rech Astrophys Quebec
ID POLARIMETER
AB We describe a novel means of polarization modulation with potential applications for the far-infrared through millimeter. A Variable-delay Polarization Modulator (VPM) modulates polarization via introduction of a variable phase between two fixed linear orthogonal polarizations. Our implementation does so by employing a grid-mirror pair in which the mirror is translated, thereby changing the relative phase between the two polarizations and systematically modulating the polarization state. For the Hertz/VPM project, we have implemented a pair of VPMs in a submillimeter polarimeter at the University of Arizonas SMTO. Promising initial results have shown the instrumental polarization in this system to be below 1%. In this presentation, we describe this polarimeter, its initial results, and prospects for VPMs including use in measuring the polarization of the cosmic microwave background to search for the polarized signature of cosmic inflation.
C1 [Chuss, David T.; Voellmer, George; Wollack, Edward J.; Moseley, S. Harvey] NASA, Goddard Space Flight Ctr, Obs Cosmol Lab, Code 665,Bldg 34,Rm E342, Greenbelt, MD 20771 USA.
RP Chuss, DT (reprint author), NASA, Goddard Space Flight Ctr, Obs Cosmol Lab, Code 665,Bldg 34,Rm E342, Greenbelt, MD 20771 USA.
EM David.T.Chuss@nasa.gov; g-novak@northwestern.edu;
megan@lennon.astro.northwestern.edu
RI Wollack, Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Zeng, Lingzhen/0000-0001-6924-9072
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 978-1-58381-780-3
J9 ASTR SOC P
PY 2011
VL 449
BP 9
EP +
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BBY34
UT WOS:000308674100002
ER
PT B
AU Chuss, DT
Cao, N
Denis, K
Hsieh, WT
Moseley, SH
Schneider, G
Stevenson, T
Travers, D
U-Yen, K
Wollack, EJ
AF Chuss, D. T.
Cao, N.
Denis, K.
Hsieh, W. -T.
Moseley, S. H.
Schneider, G.
Stevenson, T.
Travers, D.
U-Yen, K.
Wollack, E. J.
BE Bastien, P
Manset, N
Clemens, DP
StLouis, N
TI A Detector for Cosmic Microwave Background Polarimetry
SO ASTRONOMICAL POLARIMETRY 2008: SCIENCE FROM SMALL TO LARGE TELESCOPES
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Astronomical Polarimetry 2008 - Science from Small to
Large Telescopes
CY JUL 06-11, 2008
CL La Malbaie, CANADA
SP Canadian Inst Theoret Astrophys, Univ Montreal, Fac Arts & Sci, Ctr Rech Astrophys Quebec
AB We present preliminary design and development work on polarized detectors intended to enable Cosmic Microwave Background polarization measurements that will probe the first moments of the universe. The ultimate measurement will be challenging, requiring background-limited detectors and good control of systematic errors. A large collection of single-mode polarized detectors will eventually be required for the reliable detection of the weak polarized signature that is expected to result from gravitational waves produced by cosmic inflation. Toward this end, we are integrating the beam control of HE11 feedhorns with the sensitivity of transition-edge sensors. The coupling between these two devices is achieved via waveguide probe antennas and superconducting microstrip lines. This implementation allows band-pass filters to be incorporated on the detector chip. This focal plane prototype is an important step along the path to this detection, resulting in a capability that will enable various future high-performance instrument concepts.
C1 [Chuss, D. T.; Cao, N.; Denis, K.; Hsieh, W. -T.; Moseley, S. H.; Schneider, G.; Stevenson, T.; Travers, D.; U-Yen, K.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Obs Cosmol Lab, Greenbelt, MD 20771 USA.
RP Chuss, DT (reprint author), NASA, Goddard Space Flight Ctr, Obs Cosmol Lab, Code 665,Bldg 34,Rm E342, Greenbelt, MD 20771 USA.
EM David.T.Chuss@nasa.gov
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
NR 3
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 978-1-58381-780-3
J9 ASTR SOC P
PY 2011
VL 449
BP 81
EP 82
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BBY34
UT WOS:000308674100015
ER
PT B
AU Andersson, BG
Potter, SB
AF Andersson, B-G
Potter, S. B.
BE Bastien, P
Manset, N
Clemens, DP
StLouis, N
TI Observational Evidence for Radiative Interstellar Grain Alignment
SO ASTRONOMICAL POLARIMETRY 2008: SCIENCE FROM SMALL TO LARGE TELESCOPES
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Astronomical Polarimetry 2008 - Science from Small to
Large Telescopes
CY JUL 06-11, 2008
CL La Malbaie, CANADA
SP Canadian Inst Theoret Astrophys, Univ Montreal, Fac Arts & Sci, Ctr Rech Astrophys Quebec
ID MAGNETIC-FIELD; TORQUES; DUST; POLARIZATION; CLOUDS
AB The alignment mechanisms of interstellar dust grains is a long standing astrophysical problem. Interstellar polarization was first discovered in 1949 and soon thereafter attributed to dichroic extinction caused by asymmetric dust grains aligned with the magnetic field. For a long time the alignment mechanism was thought to involve paramagnetic relaxation in rapidly spinning dust grains. Modern theory indicates that the classical alignment mechanisms are likely not efficient, but rather favor alignment through direct radiative torques. We have used multi-band polarimetry towards stars probing six nearby clouds to show that the wavelength of maximum polarization is linearly correlated with the visual extinction (Andersson & Potter 2007; AP07; where further details can be found). We find a universal relation with a common positive slope between the clouds and a DC offset correlated with the average of the total-to-selective extinction < R-V >. These results provide strong observational support for radiatively driven grain alignment. Recent observations of an additional set of approximate to 60 sightlines in the Taurus cloud confirm and strengthen these results.
C1 [Andersson, B-G] NASA, Ames Res Ctr, SOFIA Sci Ctr USRA, MS N211-3, Moffett Field, CA 94035 USA.
[Potter, S. B.] South African Astronom Observatory, Cape Town, South Africa.
RP Andersson, BG (reprint author), NASA, Ames Res Ctr, SOFIA Sci Ctr USRA, MS N211-3, Moffett Field, CA 94035 USA.
EM bg@sofia.usra.edu; sbp@saao.ac.za
NR 20
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 978-1-58381-780-3
J9 ASTR SOC P
PY 2011
VL 449
BP 134
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BBY34
UT WOS:000308674100022
ER
PT B
AU Andersson, BG
Piirola, V
AF Andersson, B. -G.
Piirola, V.
BE Bastien, P
Manset, N
Clemens, DP
StLouis, N
TI Does Purcell Alignment Work, After All?: Multi-Band Polarimetry of Stars
Behind IC 63
SO ASTRONOMICAL POLARIMETRY 2008: SCIENCE FROM SMALL TO LARGE TELESCOPES
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Astronomical Polarimetry 2008 - Science from Small to
Large Telescopes
CY JUL 06-11, 2008
CL La Malbaie, CANADA
SP Canadian Inst Theoret Astrophys, Univ Montreal, Fac Arts & Sci, Ctr Rech Astrophys Quebec
ID GRAIN ALIGNMENT; RADIATIVE TORQUES; POLARIZATION; CONSTRAINTS
AB Grain alignment was for a long time thought to be driven by grain spin-up caused by the ejection of newly formed H-2 molecules from their surfaces. Modern theory has downplayed the likely contribution from such "Purcell Alignment", instead favoring direct radiative torques on the grains (Lazarian Hoang 200, and references therein), while leaving the possibility open for a role for Purcell-like ("pin-wheel") alignment in some special circumstances (Draine & Weingartner 1997; Hoang & Lazarian 2008). To observationally address the contribution of such pin-wheel alignment, we are studying the wavelength dependent polarization induced by dust in the reflection nebula IC 63. We find a tantalizing indication of active pin-wheel alignment. One sight line, probing an area of NIR fluorescent emission, shows both a higher level of polarization and a smaller wavelength of maximum polarization - both tracers of enhanced grain alignment - than other sight lines through the nebula.
C1 [Andersson, B. -G.] NASA, Ames Res Ctr, SOFIA Sci Ctr USRA, Moffett Field, CA 94035 USA.
RP Andersson, BG (reprint author), NASA, Ames Res Ctr, SOFIA Sci Ctr USRA, MS N211-3, Moffett Field, CA 94035 USA.
EM bg@sofia.usra.edu
NR 7
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 978-1-58381-780-3
J9 ASTR SOC P
PY 2011
VL 449
BP 154
EP 156
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BBY34
UT WOS:000308674100026
ER
PT S
AU Simpson, DG
AF Simpson, David G.
BE Seago, JH
Seaman, RL
Allen, SL
TI UTC AND THE HUBBLE SPACE TELESCOPE FLIGHT SOFTWARE
SO DECOUPLING CIVIL TIMEKEEPING FROM EARTH ROTATION
SE Science and Technology Series
LA English
DT Proceedings Paper
CT Colloquium Exploring Implications of Redefining Coordinated Universal
Time (UTC)
CY OCT 05-07, 2011
CL Analyt Graph Inc, Exton, PA
SP Amer Astronaut Soc, Amer Inst Aeronaut & Astronaut, Natl Opt Astron Observ, Virtual Astronom Observ
HO Analyt Graph Inc
AB Many scientific spacecraft include on-board computers whose flight software implicitly assumes a correspondence between the UT1 and UTC time scales. Using the Hubble Space Telescope flight software as an example, we examine the aspects of on-board computer flight software that may make use of these time scales, and consider how the software may be impacted by allowing the two time scales to diverge.
C1 NASA, Sci Data Proc Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Simpson, DG (reprint author), NASA, Sci Data Proc Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 8
TC 0
Z9 0
U1 0
U2 0
PU AMER ASTRONAUTICAL SOC
PI SAN DIEGO
PA PUBLICATIONS OFFICE PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 0278-4017
BN 978-0-87703-575-6
J9 SCI TECH
PY 2011
VL 113
BP 237
EP 248
PG 12
WC Astronomy & Astrophysics; Instruments & Instrumentation
SC Astronomy & Astrophysics; Instruments & Instrumentation
GA BBY78
UT WOS:000308895700015
ER
PT S
AU Prasad, NS
Roychoudhuri, C
AF Prasad, Narasimha S.
Roychoudhuri, Chandra
BE Roychoudhuri, C
Khrennikov, AY
Kracklauer, AF
TI Microscope and spectroscope results are not limited by Heisenberg's
Uncertainty Principle!
SO NATURE OF LIGHT: WHAT ARE PHOTONS IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on The Nature of Light - What are Photons IV
CY AUG 22-25, 2011
CL San Diego, CA
SP SPIE, Gen Resonance, LLC
DE Uncertainty principle; validity of uncertainty principle; overcoming
uncertainty principle; overcoming time-frequency bandwidth limit
AB A reviewing of many published experimental and theoretical papers demonstrate that the resolving powers of microscopes, spectroscopes and telescopes can be enhanced by orders of magnitude better than old classical limits by various advanced techniques including de-convolution of the CW-response function of these instruments. Heisenberg's original analogy of limited resolution of a microscope, to support his mathematical uncertainty relation, is no longer justifiable today. Modern techniques of detecting single isolated atoms through fluorescence also over-ride this generalized uncertainty principle. Various nano-technology techniques are also making atoms observable and location precisely measurable. Even the traditional time-frequency uncertainty relation or bandwidth limit delta nu delta t >= 1 can be circumvented while doing spectrometry with short pulses by deriving and de-convolving the pulse-response function of the spectrometer just as we do for CW input.
C1 [Prasad, Narasimha S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Prasad, NS (reprint author), NASA, Langley Res Ctr, 5 N Dryden St, Hampton, VA 23681 USA.
NR 5
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 978-0-8194-8731-5
J9 PROC SPIE
PY 2011
VL 8121
AR 81210F
DI 10.1117/12.895207
PG 7
WC Optics; Physics, Applied
SC Optics; Physics
GA BBQ57
UT WOS:000307871400015
ER
PT J
AU Griffiths, JM
King, DW
AF Griffiths, Jose-Marie
King, Donald W.
BE Baker, D
Evans, W
TI The future of librarians in the workforce: a US perspective
SO LIBRARIES AND SOCIETY: ROLE, RESPONSIBILITY AND FUTURE IN AN AGE OF
CHANGE
SE Chandos Information Professional Series
LA English
DT Article; Book Chapter
C1 [Griffiths, Jose-Marie; King, Donald W.] Bryant Univ, Smithfield, RI 02917 USA.
[Griffiths, Jose-Marie] Natl Sci Board, Arlington, VA USA.
[Griffiths, Jose-Marie] Presidents Informat Technol Advisory Comm, Arlington, VA USA.
[Griffiths, Jose-Marie] US Natl Commiss Lib & Informat Sci, Washington, DC USA.
[Griffiths, Jose-Marie] Natl Acad Sci, Washington, DC USA.
[Griffiths, Jose-Marie] NASA, Washington, DC USA.
[Griffiths, Jose-Marie] US DOE, Washington, DC 20560 USA.
[Griffiths, Jose-Marie] US Dept Commerce, Washington, DC 20230 USA.
[Griffiths, Jose-Marie] US Geol Survey, Reston, VA USA.
[Griffiths, Jose-Marie] USN, Washington, DC USA.
[Griffiths, Jose-Marie] Amer Assoc Advancement Sci, Washington, DC USA.
[King, Donald W.] Westat Corp, Gaithersburg, MD USA.
[King, Donald W.] Amer Stat Assoc, Alexandria, VA 22314 USA.
RP Griffiths, JM (reprint author), Bryant Univ, Smithfield, RI 02917 USA.
NR 28
TC 0
Z9 0
U1 0
U2 1
PU CHANDOS PUBL
PI SAWSTON
PA 80 HIGH ST, SAWSTON, CAMBRIDGE CB22 3HJ, ENGLAND
BN 978-1-84334-131-4
J9 CHANDOS INF PROF SER
PY 2011
BP 279
EP 302
D2 10.1533/9781780632636
PG 24
WC Information Science & Library Science
SC Information Science & Library Science
GA BYR59
UT WOS:000299894500021
ER
PT S
AU Lawson, PR
Lay, OP
Martin, SR
Peters, RD
Booth, AJ
Gappinger, RO
Ksendzov, A
Scharf, DP
AF Lawson, P. R.
Lay, O. P.
Martin, S. R.
Peters, R. D.
Booth, A. J.
Gappinger, R. O.
Ksendzov, A.
Scharf, D. P.
BE Martin, EL
Ge, J
Lin, W
TI New technologies for exoplanet detection with mid-IR interferometers
SO RESEARCH, SCIENCE AND TECHNOLOGY OF BROWN DWARFS AND EXOPLANETS
SE EPJ Web of Conferences
LA English
DT Proceedings Paper
CT International Conference on Occasion of a Total Eclipse of the Sun
CY JUL 20-24, 2009
CL Shangai, PEOPLES R CHINA
SP US Natl Sci Fdn, Shanghai Astronom Observ, Chinese Acad Sci, Natl Sci Fdn China, Nanjing Inst Astronom Opt & Technol, Univ Sci & Technol China, Purple Mt Observ
ID FIBERS; PHASE
AB This paper provides an overview of technology development for the Terrestrial Planet Finder Interferometer (TPF-I). TPF-I is a mid-infrared space interferometer being designed with the capability of detecting Earth-like planets in the habitable zones around nearby stars.
C1 [Lawson, P. R.; Lay, O. P.; Martin, S. R.; Peters, R. D.; Booth, A. J.; Gappinger, R. O.; Ksendzov, A.; Scharf, D. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lawson, PR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Peter.R.Lawson@jpl.nasa.gov
NR 16
TC 1
Z9 1
U1 0
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
SN 2100-014X
BN 978-2-7598-0664-5
J9 EPJ WEB CONF
PY 2011
VL 16
AR 07001
DI 10.1051/epjconf/20111607001
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BBO05
UT WOS:000307650700048
ER
PT S
AU Serabyn, E
Mawet, D
AF Serabyn, E.
Mawet, D.
BE Martin, EL
Ge, J
Lin, W
TI Phase mask coronagraphy at JPL and Palomar
SO RESEARCH, SCIENCE AND TECHNOLOGY OF BROWN DWARFS AND EXOPLANETS
SE EPJ Web of Conferences
LA English
DT Proceedings Paper
CT International Conference on Occasion of a Total Eclipse of the Sun
CY JUL 20-24, 2009
CL Shangai, PEOPLES R CHINA
SP US Natl Sci Fdn, Shanghai Astronom Observ, Chinese Acad Sci, Natl Sci Fdn China, Nanjing Inst Astronom Opt & Technol, Univ Sci & Technol China, Purple Mt Observ
AB For the imaging of faint companions, phase mask coronagraphy has the dual advantages of a small inner working angle and high throughput. This paper summarizes our recent work in developing phase masks and in demonstrating their capabilities at JPL. Four-quadrant phase masks have been manufactured at JPL by means of both evaporation and etching, and we have been developing liquid crystal vortex phase masks in partnership with a commercial vendor. Both types of mask have been used with our extreme adaptive optics well-corrected subaperture at Palomar to detect known brown dwarf companions as close as similar to 2.5 lambda/D to stars. Moreover, our recent vortex masks perform very well in laboratory tests, with a demonstrated infrared contrast of about 10(-6) at 3 lambda/D, and contrasts of a few 10(-7) with an initial optical wavelength device. The demonstrated performance already meets the needs of ground-based extreme adaptive optics coronagraphy, and further planned improvements are aimed at reaching the 10(-10) contrast needed for terrestrial exoplanet detection with a space-based coronagraph.
C1 [Serabyn, E.; Mawet, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Serabyn, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM gene.serabyn@jpl.nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 0
PU E D P SCIENCES
PI CEDEX A
PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A,
FRANCE
SN 2100-014X
BN 978-2-7598-0664-5
J9 EPJ WEB CONF
PY 2011
VL 16
AR 03004
DI 10.1051/epjconf/20111603004
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BBO05
UT WOS:000307650700017
ER
PT S
AU Blake, PN
Saha, T
Zhang, WW
O'Dell, S
Kester, T
Jones, W
AF Blake, Peter N.
Saha, Timo
Zhang, William W.
O'Dell, Stephen
Kester, Thomas
Jones, William
BE ODell, SL
Pareschi, G
TI Forming Mandrels for Making Lightweight X-Ray Mirrors
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE
Optics + Photonics International Symposium on Optical Engineering +
Applications
CY AUG 23-25, 2011
CL San Diego, CA
SP SPIE
DE x-ray mirrors; deterministic microgrinding; polishing
AB Future x-ray astronomical misisons, similar to the proposed International X-ray Observatory (IXO), will utilize replicated mirrors to reduce both mass and production costs. Accurately figured and measured molds (called mandrels) - on which the mirror substrates are thermally formed, replicating the surface of the mandrels - are essential to enable these missions. The Optics Branches of the Goddard Space Flight Center (GSFC) and Marshall Space Flight Center (MSFC) have developed fabrication processes along with metrologies that yield high-precision mandrels; and through the SBIR program, they encourage small businesses to attack parts of the remaining problems. The Goddard full-aperture mandrel polisher (the MPM-500) has been developed to a level where mandrel surfaces match the 1.5 arcsec HPD level allocation in a 5 arcsec telescope program. This paper reviews this current technology and describe a pilot program to design a suite of machine tools and process parameters capable of producing many hundreds of these precision objects. A major challenge is to keep mid-spatial frequency errors below 2 nm rms - a severe specification; but we must also note the factors which work to our advantage: e.g., how the figure departs from a pure cone by only one micron, and how the demanding figure specifications which apply in the axial direction are relaxed by an order of magnitude in the azimuthal. Careful study of other large optical fabrication programs in the light of these challenges and advantages has yielded a realistic plan for the economical production of mandrels that meet program requirements in both surface and quantity.
C1 [Blake, Peter N.; Saha, Timo; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[O'Dell, Stephen; Kester, Thomas; Jones, William] Marshall Space Flight Ctr, Huntsville, AL 35811 USA.
RP Blake, PN (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM peter.n.blake@nasa.gov
OI O'Dell, Stephen/0000-0002-1868-8056
NR 6
TC 1
Z9 1
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 978-0-8194-8757-5
J9 PROC SPIE
PY 2011
VL 8147
AR 814713
DI 10.1117/12.895118
PG 8
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BBA80
UT WOS:000306321500037
ER
PT S
AU Chan, KW
Hong, MD
Saha, T
Zhang, W
AF Chan, Kai-Wing
Hong, Melinda
Saha, Timo
Zhang, William
BE ODell, SL
Pareschi, G
TI Metrology of IXO Mirror Segments
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE
Optics + Photonics International Symposium on Optical Engineering +
Applications
CY AUG 23-25, 2011
CL San Diego, CA
SP SPIE
DE X-ray optics; Lightweight mirror; Metrology; Normal incidence metrology
ID OPTICS
AB For future x-ray astrophysics mission that demands optics with large throughput and excellent angular resolution, many telescope concepts build around assembling thin mirror segments in a Wolter I geometry, such as that originally proposed for the International X-ray Observatory. The arc-second resolution requirement posts unique challenges not just for fabrication, mounting but also for metrology of these mirror segments. In this paper, we shall discuss the metrology of these segments using normal incidence metrological method with interferometers and null lenses. We present results of the calibration of the metrology systems we are currently using, discuss their accuracy and address the precision in measuring near-cylindrical mirror segments and the stability of the measurements.
C1 [Chan, Kai-Wing] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA.
[Hong, Melinda] SGT Inc, Greenbelt, MD 20770 USA.
[Saha, Timo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zhang, William] NASA, Goddard Space Flight Ctr, X Ray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Chan, KW (reprint author), Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA.
NR 12
TC 5
Z9 5
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 978-0-8194-8757-5
J9 PROC SPIE
PY 2011
VL 8147
AR 814716
DI 10.1117/12.894347
PG 12
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BBA80
UT WOS:000306321500040
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 ODell, SL
Pareschi, G
TI Mathematical formalism for designing wide-field x-ray telescopes: mirror
nodal positions and detector tilts
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE
Optics + Photonics International Symposium on Optical Engineering +
Applications
CY AUG 23-25, 2011
CL San Diego, CA
SP SPIE
DE X-ray astronomy; X-ray optics; ray trace; wide field-of-view
optimization
ID GRAZING-INCIDENCE OPTICS
AB We describe a mathematical formalism for determining the mirror shell nodal positions and detector tilts that optimize the spatial resolution averaged over a field-of-view for a nested x-ray telescope, assuming known mirror segment surface prescriptions and known detector focal surface. The results are expressed in terms of ensemble averages over variable combinations of the ray positions and wavevectors in the flat focal plane intersecting the optical axis at the nominal on-axis focus, which can be determined by Monte-Carlo ray traces of the individual mirror shells. This work is part of our continuing efforts to provide analytical tools to aid in the design process for wide-field survey x-ray astronomy missions.
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
OI O'Dell, Stephen/0000-0002-1868-8056
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 978-0-8194-8757-5
J9 PROC SPIE
PY 2011
VL 8147
AR 814712
DI 10.1117/12.895227
PG 15
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BBA80
UT WOS:000306321500036
ER
PT S
AU Gubarev, MV
Khaykovich, B
Ramsey, B
Moncton, D
Zavlin, VE
Kilaru, K
Romaine, S
Rosati, RE
Bruni, R
Robertson, L
Crow, L
Ambaye, H
Lauter, V
AF Gubarev, Mikhail V.
Khaykovich, Boris
Ramsey, Brian
Moncton, David
Zavlin, Vyacheslav E.
Kilaru, Kiranmayee
Romaine, Suzanne
Rosati, Richard E.
Bruni, Ricardo
Robertson, Lee
Crow, Lowell
Ambaye, Haile
Lauter, Valeria
BE ODell, SL
Pareschi, G
TI From x-ray telescopes to neutron focusing
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE
Optics + Photonics International Symposium on Optical Engineering +
Applications
CY AUG 23-25, 2011
CL San Diego, CA
SP SPIE
DE neutron optics; grazing incidence optics; neutron microscope
ID OPTICS
AB In the case of neutrons the refractive index is slightly less than unity for most elements and their isotopes [1]. Consequently, thermal and cold neutrons can be reflected from smooth surfaces at grazing-incidence angles. Hence, the optical technologies developed for x-ray astronomy can be applied for neutron focusing. The focusing capabilities of grazing incidence neutron imaging optics have been successfully demonstrated using nickel mirrors. The mirrors were fabricated using an electroformed nickel replication process at Marshall Space Flight Center. Results of the neutron optics experiments and current status of the multilayer coating replication technique development are presented.
C1 [Gubarev, Mikhail V.; Ramsey, Brian] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
RP Gubarev, MV (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
EM MikhailV.Gubarev@nasa.gov
RI Khaykovich, Boris/A-7376-2012; Ambaye, Haile/D-1503-2016
OI Khaykovich, Boris/0000-0002-9490-2771; Ambaye, Haile/0000-0002-8122-9952
NR 18
TC 2
Z9 2
U1 0
U2 5
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-8757-5
J9 PROC SPIE
PY 2011
VL 8147
AR 81470B
DI 10.1117/12.897325
PG 8
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BBA80
UT WOS:000306321500011
ER
PT S
AU Kilaru, K
Merthe, DJ
Ali, Z
Gubarev, MV
Kester, T
Benson, CM
McKinney, WR
Takacs, PZ
Yashchuk, VV
AF Kilaru, Kiranmayee
Merthe, Daniel J.
Ali, Zulfiqar
Gubarev, Mikhail V.
Kester, Thomas
Benson, Carl M.
McKinney, Wayne R.
Takacs, Peter Z.
Yashchuk, Valeriy V.
BE ODell, SL
Pareschi, G
TI Development of a multi-beam long trace profiler
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE
Optics + Photonics International Symposium on Optical Engineering +
Applications
CY AUG 23-25, 2011
CL San Diego, CA
SP SPIE
DE Long Trace Profiler; optical metrology; x-ray optics metrology;
multi-beam profiler
ID MIRRORS
AB In order to fulfill the angular resolution requirements and make the performance goals for future NASA missions feasible, it is crucial to develop instruments capable of fast and precise figure metrology of x-ray optical elements for further correction of the surface errors. The Long Trace Profilometer (LTP) is an instrument widely used for measuring the surface figure of grazing incidence X-ray mirrors. In the case of replicated optics designed for x-ray astronomy applications, such as mirrors and the corresponding mandrels have a cylindrical shape and their tangential profile is parabolic or hyperbolic. Modern LTPs have sub-micro radian accuracy, but the measuring speed is very low, because the profilometer measures surface figure point by point using a single laser beam. The measurement rate can be significantly improved by replacing the single optical beam with multiple beams. The goal of this study is to demonstrate the viability of multi-beam metrology as a way of significantly improving the quality and affordability of replicated x-ray optics. The multi-beam LTP would allow one- and two-dimensional scanning with sub-micro radian resolution and a measurement rate of about ten times faster compared to the current LTP. The design details of the instrument's optical layout and the status of optical tests will be presented.
C1 [Kilaru, Kiranmayee; Gubarev, Mikhail V.; Kester, Thomas; Benson, Carl M.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Merthe, Daniel J.; Ali, Zulfiqar; McKinney, Wayne R.; Yashchuk, Valeriy V.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Takacs, Peter Z.] Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Kilaru, K (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM kiranmayee.kilaru-1@nasa.gov
RI McKinney, Wayne/F-2027-2014
OI McKinney, Wayne/0000-0003-2586-3139
FU Brookhaven Science Associates; LLC [DE-AC02-98CH10886]; U.S. Department
of Energy [DE-AC02-05CH11231]; Lawrence Berkeley National Laboratory
FX We would like to acknowledge the partial funding available for this work
from MSFCs technology investment program.Also, our acknowledgements to
Lawrence Berkeley National Laboratory for providing the LTP control
software code in order to speed up the development process. This
manuscript has been authored, in part, by Brookhaven Science Associates,
LLC under Contract No. DE-AC02-98CH10886 with the U.S. Department of
Energy. The Advanced Light Source is supported by the Director, Office
of Science, Office of Basic Energy Sciences, Material Science Division,
of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231 at
Lawrence Berkeley National Laboratory.One author, Zulfiqar Ali, wishes
to thank the HEC, Pakistan for providing Post-doctoral scholarship.
NR 12
TC 4
Z9 4
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 978-0-8194-8757-5
J9 PROC SPIE
PY 2011
VL 8147
AR 814719
DI 10.1117/12.895532
PG 8
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BBA80
UT WOS:000306321500043
ER
PT S
AU Kilaru, K
Ramsey, BD
Gubarev, MV
Gaskin, JA
O'Dell, SL
Zhang, W
AF Kilaru, Kiranmayee
Ramsey, Brian D.
Gubarev, Mikhail V.
Gaskin, Jessica A.
O'Dell, Stephen L.
Zhang, William
BE ODell, SL
Pareschi, G
TI Differential deposition to correct surface figure deviations in
astronomical grazing-incidence X-ray optics
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE
Optics + Photonics International Symposium on Optical Engineering +
Applications
CY AUG 23-25, 2011
CL San Diego, CA
SP SPIE
DE Grazing incidence X-ray optics; Differential deposition; Surface figure
deviations in X-ray optics; Reflective X-ray optics; Focusing X-ray
optics; Coatings on X-ray optics
AB A coating technique is being developed to correct the surface figure deviations in grazing-incidence X-ray optics. These optics are typically designed to have precise conic profiles, and any deviation in this profile, as a result of fabrication, results in a degradation of the imaging performance. To correct the mirror profiles, physical vapor deposition has been utilized to selectively deposit a filler material inside the mirror shell. The technique, termed differential deposition, has been implemented as a proof of concept on miniature X-ray optics developed at MSFC for medical-imaging applications. The technique is now being transferred to larger grazing-incidence optics suitable for astronomy.
C1 [Kilaru, Kiranmayee] NASA, Postdoctoral Program, Huntsville, AL 35812 USA.
[Ramsey, Brian D.; Gubarev, Mikhail V.; Gaskin, Jessica A.; O'Dell, Stephen L.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Zhang, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Kilaru, K (reprint author), NASA, Postdoctoral Program, Huntsville, AL 35812 USA.
OI O'Dell, Stephen/0000-0002-1868-8056
NR 11
TC 4
Z9 4
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 978-0-8194-8757-5
J9 PROC SPIE
PY 2011
VL 8147
AR 81470X
DI 10.1117/12.895939
PG 8
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BBA80
UT WOS:000306321500031
ER
PT S
AU O'Dell, SL
Atkins, C
Button, TW
Cotroneo, V
Davis, WN
Doel, P
Feldman, CH
Freeman, MD
Gubarev, MV
Kolodziejczak, JJ
Michette, AG
Ramsey, BD
Reid, PB
Sanmartin, DR
Saha, TT
Schwartz, DA
Trolier-McKinstry, S
Wilke, RHT
Willingale, R
Zhang, WW
AF O'Dell, Stephen L.
Atkins, Carolyn
Button, Timothy W.
Cotroneo, Vincenzo
Davis, William N.
Doel, Peter
Feldman, Charlotte H.
Freeman, Mark D.
Gubarev, Mikhail V.
Kolodziejczak, Jeffery J.
Michette, Alan G.
Ramsey, Brian D.
Reid, Paul B.
Sanmartin, Daniel Rodriguez
Saha, Timo T.
Schwartz, Daniel A.
Trolier-McKinstry, Susan
Wilke, Rudeger H. T.
Willingale, Richard
Zhang, William W.
BE ODell, SL
Pareschi, G
TI Toward active x-ray telescopes
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE
Optics + Photonics International Symposium on Optical Engineering +
Applications
CY AUG 23-25, 2011
CL San Diego, CA
SP SPIE
DE X-ray telescopes; x-ray optics; active optics; adjustable optics;
piezoelectric devices
ID MIRRORS
AB Future x-ray observatories will require high-resolution (< 1 '') optics with very-large-aperture (> 25 m(2)) areas. Even with the next generation of heavy-lift launch vehicles, launch-mass constraints and aperture-area requirements will limit the areal density of the grazing-incidence mirrors to about 1 kg/m(2) or less. Achieving sub-arcsecond x-ray imaging with such lightweight mirrors will require excellent mirror surfaces, precise and stable alignment, and exceptional stiffness or deformation compensation. Attaining and maintaining alignment and figure control will likely involve active (in-space adjustable) x-ray optics. In contrast with infrared and visible astronomy, active optics for x-ray astronomy is in its infancy. In the middle of the past decade, two efforts began to advance technologies for adaptive x-ray telescopes: The Smart X-ray Optics (SXO) Basic Technology project in the United Kingdom (UK) and the Generation-X (Gen-X) concept studies in the United States (US). This paper discusses relevant technological issues and summarizes progress toward active x-ray telescopes.
C1 [O'Dell, Stephen L.; Gubarev, Mikhail V.; Kolodziejczak, Jeffery J.; Ramsey, Brian D.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
RP O'Dell, SL (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
RI Button, Tim/I-6803-2012;
OI O'Dell, Stephen/0000-0002-1868-8056; Trolier-McKinstry,
Susan/0000-0002-7267-9281
NR 44
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 978-0-8194-8757-5
J9 PROC SPIE
PY 2011
VL 8147
AR 81471Q
DI 10.1117/12.896458
PG 18
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BBA80
UT WOS:000306321500059
ER
PT S
AU Saha, TT
Rohrbach, S
Zhang, WW
Evans, TC
Hong, M
AF Saha, Timo T.
Rohrbach, Scott
Zhang, William W.
Evans, Tyler C.
Hong, Melinda
BE ODell, SL
Pareschi, G
TI Grazing incidence wavefront sensing and verification of x-ray optics
performance
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE
Optics + Photonics International Symposium on Optical Engineering +
Applications
CY AUG 23-25, 2011
CL San Diego, CA
SP SPIE
DE X-ray optics; x-ray mirrors; mirror alignment; wavefront sensing
ID INCIDENCE TELESCOPES; SURFACE
AB Evaluation of interferometric mirror metrology data and characterization of a telescope wavefront can be powerful tools in understanding image characteristics of an x-ray optical system. In the development of soft x-ray telescope for the International X-Ray Observatory (IXO), we have developed new approaches to support the telescope development process.
Interferometrically measuring the optical components over all relevant spatial frequencies can be used to evaluate and predict the performance of an x-ray telescope. Typically, the mirrors are measured using a mount that minimizes the mount and gravity induced errors. In the assembly and mounting process the shape of the mirror segments can dramatically change. We have developed wavefront sensing techniques suitable for the x-ray optical components to aid us in the characterization and evaluation of these changes.
Hartmann sensing of a telescope and its components is a simple method that can be used to evaluate low order mirror surface errors and alignment errors. Phase retrieval techniques can also be used to assess and estimate the low order axial errors of the primary and secondary mirror segments.
In this paper we describe the mathematical foundation of our Hartmann and phase retrieval sensing techniques. We show how these techniques can be used in the evaluation and performance prediction process of x-ray telescopes.
C1 [Saha, Timo T.; Rohrbach, Scott; Zhang, William W.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Evans, Tyler C.; Hong, Melinda] SGT Inc, Greenbelt, MD 20770 USA.
RP Saha, TT (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
FU Goddard Space Flight Center; NASA Astronomy and Physics Research and
Analysis (APRA) [07-APRA07-0142]
FX This work has been financially supported in part by the International
X-Ray Observatory Project office at Goddard Space Flight Center and NASA
Astronomy and Physics Research and Analysis (APRA) grant 07-APRA07-0142.
NR 15
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 978-0-8194-8757-5
J9 PROC SPIE
PY 2011
VL 8147
AR 814717
DI 10.1117/12.893404
PG 12
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BBA80
UT WOS:000306321500041
ER
PT S
AU West, E
Pavelitz, S
Kobayashi, K
Robinson, B
Cirtain, J
Gaskin, J
Winebarger, A
Krause, L
McGuirk, M
Darnel, J
AF West, Edward
Pavelitz, Steve
Kobayashi, Ken
Robinson, Brian
Cirtain, Jonathan
Gaskin, Jessica
Winebarger, Amy
Krause, Linda
McGuirk, Michael
Darnel, Jonathan
BE ODell, SL
Pareschi, G
TI Development of an EUV test facility at the Marshall Space Flight Center
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE
Optics + Photonics International Symposium on Optical Engineering +
Applications
CY AUG 23-25, 2011
CL San Diego, CA
SP SPIE
DE Extreme Ultraviolet; EUV; X-Ray test facilities; Hi-C; SUVI; EUV
telescopes; EUV source
AB This paper will describe a new Extreme Ultraviolet (EUV) test facility that is being developed at the Marshall Space Flight Center (MSFC) to test EUV telescopes. Two flight programs, Hi-C, the high resolution coronal imager (a sounding rocket program), and SUVI, the Solar Ultraviolet Imager (GOES-R), set the requirements for this new facility. This paper will discuss those requirements, the EUV source characteristics, the wavelength resolution that is expected and the vacuum chambers (Stray Light Facility, Xray Calibration Facility and the NSSTC EUV test chamber) where this facility will be used.
C1 [West, Edward; Pavelitz, Steve; Cirtain, Jonathan; Gaskin, Jessica; Winebarger, Amy; Krause, Linda] NASA, Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
[Kobayashi, Ken; Robinson, Brian] Univ Alabama, Huntsville, AL USA.
[McGuirk, Michael] MIT, Lincoln Lab, Lexington, MA 02420 USA.
[Darnel, Jonathan] IM Syst Grp, Rockville, MD 20852 USA.
RP West, E (reprint author), NASA, Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
NR 3
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 978-0-8194-8757-5
J9 PROC SPIE
PY 2011
VL 8147
AR 81471A
DI 10.1117/12.904922
PG 11
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BBA80
UT WOS:000306321500044
ER
PT S
AU Zhang, WW
Biskach, MP
Blake, PN
Chan, KW
Evans, TC
Hong, ML
Jones, WD
Kolos, LD
Mazzarella, JM
McClelland, RS
O'Dell, SL
Saha, TT
Sharpe, MV
AF Zhang, W. W.
Biskach, M. P.
Blake, P. N.
Chan, K. W.
Evans, T. C.
Hong, M. L.
Jones, W. D.
Kolos, L. D.
Mazzarella, J. M.
McClelland, R. S.
O'Dell, S. L.
Saha, T. T.
Sharpe, M. V.
BE ODell, SL
Pareschi, G
TI Lightweight and high angular resolution x-ray optics for astronomical
missions
SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE
Optics + Photonics International Symposium on Optical Engineering +
Applications
CY AUG 23-25, 2011
CL San Diego, CA
SP SPIE
DE X-ray optics; lightweight optics; glass slumping; mirror alignment;
mirror bonding
ID GENERATION-X
AB X-ray optics of both high angular resolution and light weight are essential for advancing x-ray astrophysics. High angular resolution is important for avoiding source confusion and reducing background, thus allowing observation of the most distant objects in the early Universe. It is also important in enabling gratings to achieve high spectral resolution, to study the myriad plasmas in planetary, stellar, and galactic environments, as well as inter-planetary, inter-stellar, and inter-galactic media. Light weight is essential for further increasing photon collection area: X-ray observations must be performed from space, where mass available for a telescope has always been and is expected to continue to be quite limited. This paper reports on a program to develop x-ray optics satisfying these two requirements. The objective of this technology program is to enable Explorer-class missions in the near term and facility-class missions in the long term.
C1 [Zhang, W. W.; Blake, P. N.; Kolos, L. D.; Saha, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhang, WW (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
NR 9
TC 4
Z9 4
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 978-0-8194-8757-5
J9 PROC SPIE
PY 2011
VL 8147
AR 81470K
DI 10.1117/12.893697
PG 12
WC Astronomy & Astrophysics; Optics
SC Astronomy & Astrophysics; Optics
GA BBA80
UT WOS:000306321500019
ER
PT S
AU Clampin, M
AF Clampin, Mark
BE MacEwen, HA
Breckinridge, JB
TI Overview of the James Webb Space Telescope Observatory
SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES
AND CONCEPTS V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on UV/Optical/IR Space Telescopes and Instruments -
Innovative Technologies and Concepts V
CY AUG 21-24, 2011
CL San Diego, CA
SP SPIE
AB The James Webb Space Telescope (JWST) is a large aperture, space telescope designed to provide imaging and spectroscopy over the near and mid-infrared from 1.0 mu m to 28 mu m. JWST is a passively cooled infrared telescope, employing a five layer sunshield to achieve an operating temperature of similar to 40 K. JWST will be launched to an orbit at L2 aboard an Ariane 5 launcher in 2013. The Goddard Space Flight Center (GSFC) is the lead center for the JWST program and manages the project for NASA. The prime contractor for JWST is Northrop Grumman Aerospace Systems (NGST). JWST is an international partnership with the European Space Agency (ESA), and the Canadian Space Agency (CSA). ESA will contribute the Ariane 5 launch, and a multi-object infrared spectrograph. CSA will contribute the Fine Guidance Sensor (FGS), which includes the Tunable Filter Imager (TFI). A European consortium, in collaboration with the Jet Propulsion Laboratory (JPL), builds the mid-infrared imager (MIRI). In this paper we present an overview of the JWST science program, and discuss recent progress in the development of the observatory. In this paper we will discuss the scientific motivations for JWST, and discuss recent progress in the construction of the observatory, focusing on the telescope and its optics, which have recently completed polishing.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Clampin, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 8
TC 4
Z9 4
U1 7
U2 12
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-8756-8
J9 PROC SPIE
PY 2011
VL 8146
AR 814605
DI 10.1117/12.897446
PG 10
WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
GA BBA82
UT WOS:000306323000005
ER
PT S
AU Clark, N
Breckinridge, JB
AF Clark, Natalie
Breckinridge, James B.
BE MacEwen, HA
Breckinridge, JB
TI Polarization compensation of Fresnel aberrations in telescopes
SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES
AND CONCEPTS V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on UV/Optical/IR Space Telescopes and Instruments -
Innovative Technologies and Concepts V
CY AUG 21-24, 2011
CL San Diego, CA
SP SPIE
DE Polarization; exoplanet; telescope; birefringence; polyimide; wavefront;
adaptive optics; and phase
ID STRATIFIED MEDIA; CORONAGRAPHS; PROPAGATION; OPTICS
AB Large aperture space telescopes are built with low F#'s to accommodate the mechanical constraints of launch vehicles and to reduce resonance frequencies of the on-orbit system. Inherent with these low F# is Fresnel polarization which effects image quality. We present the design and modeling of a nano-structure consisting of birefringent layers. Analysis shows a device that functions across a 400nm bandwidth tunable from 300nm to 1200nm. This Fresnel compensator device has a cross leakage of less than 0.001 retardance.
C1 [Clark, Natalie] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Clark, N (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 18
TC 4
Z9 4
U1 0
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 978-0-8194-8756-8
J9 PROC SPIE
PY 2011
VL 8146
AR 81460O
DI 10.1117/12.896638
PG 12
WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
GA BBA82
UT WOS:000306323000024
ER
PT S
AU Content, DA
Goullioud, R
Lehan, JP
Mentzell, JE
AF Content, D. A.
Goullioud, R.
Lehan, J. P.
Mentzell, J. E.
BE MacEwen, HA
Breckinridge, JB
TI Optical design trade study for the Wide Field Infrared Survey Telescope
[WFIRST]
SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES
AND CONCEPTS V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on UV/Optical/IR Space Telescopes and Instruments -
Innovative Technologies and Concepts V
CY AUG 21-24, 2011
CL San Diego, CA
SP SPIE
DE Space astrophysics; exoplanet microlensing; Dark Energy; wide field
imaging; three mirror anastigmat
ID SUPERNOVAE
AB The Wide Field Infrared Survey Telescope (WFIRST) mission concept was ranked first in new space astrophysics mission by the Astro2010 Decadal Survey incorporating the Joint Dark Energy Mission (JDEM)-Omega payload concept and multiple science white papers. This mission is based on a space telescope at L2 studying exoplanets [via gravitational microlensing], probing dark energy, and surveying the near infrared sky. Since the release of NWNH, the WFIRST project has been working with the WFIRST science definition team (SDT) to refine mission and payload concepts. We present the driving requirements. The current interim reference mission point design, based on the use of a 1.3m unobscured aperture three mirror anastigmat form, with focal imaging and slitless spectroscopy science channels, is consistent with the requirements, requires no technology development, and out performs the JDEM-Omega design.
C1 [Content, D. A.; Mentzell, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Content, DA (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
NR 20
TC 4
Z9 4
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 978-0-8194-8756-8
J9 PROC SPIE
PY 2011
VL 8146
AR 81460Y
DI 10.1117/12.898528
PG 12
WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
GA BBA82
UT WOS:000306323000033
ER
PT S
AU Greenhouse, MA
Balzano, V
Davila, P
Drury, MP
Dunn, JL
Glazer, SD
Greville, E
Henegar, G
Johnson, EL
Lundquist, R
McCloskey, JC
Ohl, RG
Rashford, RA
Voyton, MF
AF Greenhouse, Matthew A.
Balzano, Vicki
Davila, Pam
Drury, Michael P.
Dunn, Jamie L.
Glazer, Stuart D.
Greville, Ed
Henegar, Gregory
Johnson, Eric L.
Lundquist, Ray
McCloskey, John C.
Ohl, Raymond G.
Rashford, Robert A.
Voyton, Mark F.
BE MacEwen, HA
Breckinridge, JB
TI Status of the James Webb Space Telescope Integrated Science Instrument
Module System
SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES
AND CONCEPTS V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on UV/Optical/IR Space Telescopes and Instruments -
Innovative Technologies and Concepts V
CY AUG 21-24, 2011
CL San Diego, CA
SP SPIE
DE JWST; Instrumentation
AB The Integrated Science Instrument Module (ISIM) of the James Webb Space Telescope (JWST) is discussed from a systems perspective with emphasis on development status and advanced technology aspects. The ISIM is one of three elements that comprise the JWST space vehicle and is the science instrument payload of the JWST. The major subsystems of this flight element and their build status are described.
C1 [Greenhouse, Matthew A.; Davila, Pam; Drury, Michael P.; Dunn, Jamie L.; Glazer, Stuart D.; Greville, Ed; Henegar, Gregory; Johnson, Eric L.; Lundquist, Ray; McCloskey, John C.; Ohl, Raymond G.; Rashford, Robert A.; Voyton, Mark F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Greenhouse, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM matt.greenhouse@nasa.gov
NR 22
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 978-0-8194-8756-8
J9 PROC SPIE
PY 2011
VL 8146
AR 814606
DI 10.1117/12.895228
PG 23
WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
GA BBA82
UT WOS:000306323000006
ER
PT S
AU Kogut, A
Chuss, DT
Dotson, J
Fixsen, DJ
Halpern, M
Hinshaw, GF
Meyer, S
Moseley, SH
Seiffert, MD
Spergel, DN
Wollack, EJ
AF Kogut, Alan
Chuss, David T.
Dotson, Jessie
Fixsen, Dale J.
Halpern, Mark
Hinshaw, Gary F.
Meyer, Stephan
Moseley, S. Harvey
Seiffert, Michael D.
Spergel, David N.
Wollack, Edward J.
BE MacEwen, HA
Breckinridge, JB
TI The Primordial Inflation Explorer (PIXIE)
SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES
AND CONCEPTS V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on UV/Optical/IR Space Telescopes and Instruments -
Innovative Technologies and Concepts V
CY AUG 21-24, 2011
CL San Diego, CA
SP SPIE
DE polarimeter; cosmic microwave background; Fourier transform
spectrometer; bolometer
ID MICROWAVE BACKGROUND-RADIATION; POLARIZATION; ANISOTROPY; EMISSION;
SCALE; WAVES; COBE
AB The Primordial Inflation Explorer is an Explorer-class mission to measure the gravity-wave signature of primordial inflation through its distinctive imprint on the linear polarization of the cosmic microwave background. PIXIE uses an innovative optical design to achieve background-limited sensitivity in 400 spectral channels spanning 2.5 decades in frequency from 30 GHz to 6 THz (1 cm to 50 mu m wavelength). Multi-moded non-imaging optics feed a polarizing Fourier Transform Spectrometer to produce a set of interference fringes, proportional to the difference spectrum between orthogonal linear polarizations from the two input beams. The differential design and multiple signal modulations spanning 11 orders of magnitude in time combine to reduce the instrumental signature and confusion from unpolarized sources to negligible levels. PIXIE will map the full sky in Stokes I, Q, and U parameters with angular resolution 2 degrees.6 and sensitivity 0.2 mu K per 1 degrees square pixel. The principal science goal is the detection and characterization of linear polarization from an inflationary epoch in the early universe, with tensor-to-scalar ratio r < 10(-3) at 5 standard deviations. We describe the PIXIE instrument and mission architecture needed to detect the signature of an inflationary epoch in the early universe using only 4 semiconductor bolometers.
C1 [Kogut, Alan; Fixsen, Dale J.; Moseley, S. Harvey; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kogut, A (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
EM Alan.J.Kogut@nasa.gov
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
NR 30
TC 3
Z9 3
U1 2
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 978-0-8194-8756-8
J9 PROC SPIE
PY 2011
VL 8146
AR 81460T
DI 10.1117/12.892558
PG 17
WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
GA BBA82
UT WOS:000306323000029
ER
PT S
AU Martin, SR
Liewer, KM
Ksendzov, A
Serabyn, E
AF Martin, Stefan R.
Liewer, Kurt M.
Ksendzov, Alexander
Serabyn, Eugene
BE MacEwen, HA
Breckinridge, JB
TI An optical fiber-based high contrast imager
SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES
AND CONCEPTS V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on UV/Optical/IR Space Telescopes and Instruments -
Innovative Technologies and Concepts V
CY AUG 21-24, 2011
CL San Diego, CA
SP SPIE
DE High contrast imaging; optical fiber arrays; exoplanet imaging
ID INTERFEROMETRIC ARRAYS; CONSTRAINTS; COMPANIONS; TELESCOPE; PLANETS;
SYSTEM; AU
AB Arrays of single mode fibers can be used to form segmented pupils of almost arbitrary geometry. Such pupil arrays can be used both for interferometric imaging, for example by non-redundant aperture masking or in direct imaging systems such as the phased array coronagraph. Achieving control over the optical coupling, phase and dispersion for fiber arrays of reasonable size is a technological challenge. Progress has been made using a monolithic block of single mode fibers, lens arrays and masks, and mirror arrays. On one testbed, arrays of up to 37 beamlets are being combined to form a single image. On a second testbed, control of dispersion between fibers of slightly different length is being evaluated. The combination of the techniques being demonstrated has a range of potential uses in astronomy. In this paper we discuss the initial testbed results.
C1 [Martin, Stefan R.; Liewer, Kurt M.; Ksendzov, Alexander; Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Martin, SR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 19
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 978-0-8194-8756-8
J9 PROC SPIE
PY 2011
VL 8146
AR 81460J
DI 10.1117/12.895517
PG 13
WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
GA BBA82
UT WOS:000306323000019
ER
PT S
AU Serabyn, E
Mawet, D
Wallace, JK
Liewer, K
Trauger, J
Moody, D
Kern, B
AF Serabyn, E.
Mawet, D.
Wallace, J. K.
Liewer, K.
Trauger, J.
Moody, D.
Kern, B.
BE MacEwen, HA
Breckinridge, JB
TI Recent Progress in Vector Vortex Coronagraphy
SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES
AND CONCEPTS V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on UV/Optical/IR Space Telescopes and Instruments -
Innovative Technologies and Concepts V
CY AUG 21-24, 2011
CL San Diego, CA
SP SPIE
DE vortex; coronagraphy; exoplanets
ID TELESCOPES
AB The optical vortex coronagraph has great potential for enabling high-contrast observations very close to bright stars, and thus for reducing the size of space telescopes needed for exoplanet characterization missions. Here we discuss several recent developments in optical vortex coronagraphy. In particular, we describe multi-stage vortex configurations that allow the use of on-axis telescopes for high-contrast coronagraphy, and also enable the direct measurement of the amplitudes and phases of focal plane speckles. We also briefly describe recent laboratory demonstrations of the optical properties of the dual-stage vortex, and of the broadband performance of single stage vortex masks. Indeed, the demonstrated performance of the vector vortex phase masks already in hand, approximate to 10(-8), is approximately that needed for an initial coronagraphic mission, such as an exoplanet explorer, aimed at detecting exozodiacal light and jovian exoplanets.
C1 [Serabyn, E.; Wallace, J. K.; Liewer, K.; Trauger, J.; Moody, D.; Kern, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Serabyn, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 9
TC 3
Z9 3
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 978-0-8194-8756-8
J9 PROC SPIE
PY 2011
VL 8146
AR 81460L
DI 10.1117/12.895267
PG 8
WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
GA BBA82
UT WOS:000306323000021
ER
PT S
AU Serabyn, E
Liewer, K
Martin, SR
Mawet, D
Ksendzov, A
AF Serabyn, E.
Liewer, K.
Martin, S. R.
Mawet, D.
Ksendzov, A.
BE MacEwen, HA
Breckinridge, JB
TI Fiber-Based Interferometry and Imaging
SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES
AND CONCEPTS V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on UV/Optical/IR Space Telescopes and Instruments -
Innovative Technologies and Concepts V
CY AUG 21-24, 2011
CL San Diego, CA
SP SPIE
DE optical fibers; nulling interferometry; coronagraphy; pupil remapping
ID BEAM COMBINER; HIGH-CONTRAST; TELESCOPE
AB Single-mode optical fibers are playing an increasing role in astronomical interferometry, e.g., in high-accuracy visibility measurements and in nulling interferometry. However, such observing modes typically involve only small numbers of fibers. On the other hand, some recently proposed observing techniques call for arrays of single mode fibers coupled to arrays of sub-apertures within a large telescope pupil. The concepts include pupil-masked visibility measurements (non-redundant masking), pupil-sheared nulling interferometry, and coronagraphic imaging using a fiber-linked phased-array of small optical telescopes. The latter arrangement may also be relevant to optical communications. Here we provide an overview of a number of recent novel applications of single-mode fibers and single-mode fiber arrays.
C1 [Serabyn, E.; Liewer, K.; Martin, S. R.; Ksendzov, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Serabyn, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 21
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 978-0-8194-8756-8
J9 PROC SPIE
PY 2011
VL 8146
AR 81460I
DI 10.1117/12.895268
PG 7
WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
GA BBA82
UT WOS:000306323000018
ER
PT S
AU Stahl, HP
Henrichs, T
Luedtke, A
West, M
AF Stahl, H. Philip
Henrichs, Todd
Luedtke, Alexander
West, Miranda
BE MacEwen, HA
Breckinridge, JB
TI Update on parametric cost models for space telescopes
SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES
AND CONCEPTS V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on UV/Optical/IR Space Telescopes and Instruments -
Innovative Technologies and Concepts V
CY AUG 21-24, 2011
CL San Diego, CA
SP SPIE
DE Space Telescope Cost Model; Parametric Cost Model
AB Parametric cost models are used to plan missions, compare concepts and justify technology investments. This paper updates an ongoing effort to develop cost modes for space telescopes and summarizes how recent database changes have changed previously published preliminary results. While the models are evolving, the previously published findings are valid: telescope cost increases with aperture diameter; it costs less per square meter of collecting aperture to build a large telescope than a small telescope; lower areal density telescopes cost more than more massive telescopes.
C1 [Stahl, H. Philip] NASA, MSFC, Huntsville, AL 35821 USA.
RP Stahl, HP (reprint author), NASA, MSFC, Huntsville, AL 35821 USA.
NR 2
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 978-0-8194-8756-8
J9 PROC SPIE
PY 2011
VL 8146
AR 81460F
DI 10.1117/12.894085
PG 7
WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
GA BBA82
UT WOS:000306323000015
ER
PT S
AU Stahl, HP
Barney, R
Bauman, J
Feinberg, L
Mccleese, D
Singh, U
AF Stahl, H. Philip
Barney, Rich
Bauman, Jill
Feinberg, Lee
Mccleese, Dan
Singh, Upendra
BE MacEwen, HA
Breckinridge, JB
TI Summary of the NASA Science Instrument, Observatory and Sensor System
(SIOSS) Technology Assessment
SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES
AND CONCEPTS V
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on UV/Optical/IR Space Telescopes and Instruments -
Innovative Technologies and Concepts V
CY AUG 21-24, 2011
CL San Diego, CA
SP SPIE
DE NASA; Space Technology; Technology Development
AB In July 2010, NASA's Office of Chief Technologist initiated a study to identify where substantial enhancements in mission capabilities are needed to enable and enhance future missions, and to provide strategic guidance for the agency's budget formulation and prioritization process. This paper summarizes the Science Instruments, Observatories and Sensor Systems technology assessment with an emphasis on the needs of NASA's Astrophysics Division.
C1 [Stahl, H. Philip] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Stahl, HP (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
NR 11
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 978-0-8194-8756-8
J9 PROC SPIE
PY 2011
VL 8146
AR 81460C
DI 10.1117/12.894077
PG 15
WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic
Technology
GA BBA82
UT WOS:000306323000012
ER
PT S
AU Parsons, A
Bodnarik, J
Burger, D
Evans, L
Floyd, S
Lim, L
McClanahan, T
Namkung, M
Suzanne, N
Schweitzer, J
Starr, R
Trombka, J
AF Parsons, Ann
Bodnarik, Julia
Burger, Dan
Evans, Larry
Floyd, Samuel
Lim, Lucy
McClanahan, Timothy
Namkung, Min
Suzanne, Nowicki
Schweitzer, Jeffrey
Starr, Richard
Trombka, Jacob
GP IEEE
TI Development of the Probing In-Situ With Neutron And Gamma Rays (PING)
Instrument for Planetary Science Applications
SO 2011 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE
(NSS/MIC)
SE IEEE Nuclear Science Symposium Conference Record
LA English
DT Proceedings Paper
CT IEEE Nuclear Science Symposium/Medical Imaging Conference (NSS/MIC)/18th
International Workshop on Room-Temperature Semiconductor X-Ray and
Gamma-Ray Detectors
CY OCT 23-29, 2011
CL Valencia, SPAIN
SP IEEE, Inst Elect & Elect Engineers Nucl & Plasma Sci Soc (IEEE NPSS)
AB This paper describes the testing of a prototype active neutron/ gamma ray instrument for use in planetary science space applications. The Probing In situ with Neutrons and Gamma rays (PING) instrument can measure the full bulk elemental composition of a planet's surface over a 1 m(2) area and down to 30 - 50 cm depth without the need to drill into the surface material. PING consists of three components: a pulsed neutron generator that emits 14 MeV neutrons that penetrate the surface and excite the nuclei of the planetary material; a gamma ray spectrometer that measures the energy and intensity of the gamma rays emitted by these nuclear reactions; and neutron detectors to measure the neutron moderation properties of the material. PING is tested on Earth at a unique facility near NASA/Goddard Space Flight Center where PING can be safely operated outdoors and unshielded sitting atop large (1.8m x 1.8m x .9m), well-characterized granite and basalt monuments. We will describe both this test facility and our experiments, and present gamma ray spectroscopy results that demonstrate PING's capabilities.
C1 [Parsons, Ann; Bodnarik, Julia; Evans, Larry; Floyd, Samuel; Lim, Lucy; McClanahan, Timothy; Namkung, Min; Suzanne, Nowicki; Starr, Richard; Trombka, Jacob] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Evans, Larry] Comp Sci Corp, Lanham, MD USA.
[Starr, Richard] Catholic Univ Amer, Washington, DC 20064 USA.
[Bodnarik, Julia] Vanderbilt Univ, 221 Kirkland Hall, Nashville, TN 37235 USA.
[Suzanne, Nowicki] Univ Michigan, Grad Studennt, Ann Arbor, MI USA.
[Trombka, Jacob] Univ Maryland, College Pk, MD USA.
[Schweitzer, Jeffrey] Univ Connecticut, Storrs, CT USA.
[Burger, Dan] Vanderbilt Univ, 221 Kirkland Hall, Nashville, TN 37235 USA.
RP Parsons, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Ann.M.Parsons@nasa.gov
RI Parsons, Ann/I-6604-2012
FU NASN Goddard Space Flight Center
FX This work was supported in partby NASN Goddard Space Flight Center.
NR 1
TC 0
Z9 0
U1 0
U2 4
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1082-3654
BN 978-1-4673-0120-6
J9 IEEE NUCL SCI CONF R
PY 2011
BP 1234
EP 1238
PG 5
WC Engineering, Electrical & Electronic; Physics, Applied; Imaging Science
& Photographic Technology; Radiology, Nuclear Medicine & Medical Imaging
SC Engineering; Physics; Imaging Science & Photographic Technology;
Radiology, Nuclear Medicine & Medical Imaging
GA BAM64
UT WOS:000304755601091
ER
PT S
AU Chen, W
Carini, GA
De Geronimo, G
Gaskin, JA
Keister, JW
Li, S
Li, Z
Ramsey, BD
Siddons, DP
Smith, GC
Verbitskaya, E
AF Chen, W.
Carini, G. A.
De Geronimo, G.
Gaskin, J. A.
Keister, J. W.
Li, S.
Li, Z.
Ramsey, B. D.
Siddons, D. P.
Smith, G. C.
Verbitskaya, E.
GP IEEE
TI Radiation effects of n-type, low resistivity, spiral Silicon Drift
Detector hybrid systems
SO 2011 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE
(NSS/MIC)
SE IEEE Nuclear Science Symposium Conference Record
LA English
DT Proceedings Paper
CT IEEE Nuclear Science Symposium/Medical Imaging Conference (NSS/MIC)/18th
International Workshop on Room-Temperature Semiconductor X-Ray and
Gamma-Ray Detectors
CY OCT 23-29, 2011
CL Valencia, SPAIN
SP IEEE, Inst Elect & Elect Engineers Nucl & Plasma Sci Soc (IEEE NPSS)
ID X-RAY SPECTROMETERS; CMOS TECHNOLOGIES
AB We have developed a new thin-window, n-type, low-resistivity, spiral silicon drift detector (SDD) array - to be used as an extraterrestrial X-ray spectrometer (in varying environments) for NASA. To achieve low-energy response, a thin SDD entrance window was produced using a previously developed method. These thin-window devices were also produced on lower resistivity, thinner, n-type, silicon material, effectively ensuring their radiation hardness in anticipation of operation in potentially harsh radiation environments (such as found around the Jupiter system). Using the Indiana University Cyclotron Facility beam line RERS1, we irradiated a set of suitable diodes up to 5 Mrad and the latest iteration of our ASICs up to 12 Mrad. Then we irradiated two hybrid detectors consisting of newly, such-produced in-house (BNL) SDD chips bonded with ASICs with doses of 0.25 Mrad and 1 Mrad. Also we irradiated another hybrid detector consisting of previously produced (by KETEK) on n-type, high-resistivity SDD chip bonded with BNL's ASICs with a dose of 1 Mrad. The measurement results of radiated diodes (up to 5 Mrad), ASICs (up to 12 Mrad) and hybrid detectors (up to 1 Mrad) are presented here.
C1 [Chen, W.; Carini, G. A.; De Geronimo, G.; Keister, J. W.; Li, S.; Li, Z.; Siddons, D. P.; Smith, G. C.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Carini, G. A.] SLAC Natl Accelerator Lab, Brookhaven Natl Lab, Menlo Pk, CA USA.
[Gaskin, J. A.; Ramsey, B. D.] NASA, MSFC, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Verbitskaya, E.] Inst Russian Acad Sci, Phys Tech, St Petersburg, Russia.
RP Chen, W (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA.
EM weichen@bnl.gov
RI Verbitskaya, Elena/D-1521-2014
FU U.S. Department of Energy [DE-AC02-98CHI0886]; NASA Research
Opportunities in Space and Earth Science; Planetary Instrument
Definition and Development Program
FX This work was supported in part by the U.S. Department of Energy under
Contract No. DE-AC02-98CHI0886. This work was also funded in-part by the
NASA Research Opportunities in Space and Earth Science, Planetary
Instrument Definition and Development Program.
NR 11
TC 1
Z9 1
U1 0
U2 2
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1082-3654
BN 978-1-4673-0120-6
J9 IEEE NUCL SCI CONF R
PY 2011
BP 1697
EP 1701
PG 5
WC Engineering, Electrical & Electronic; Physics, Applied; Imaging Science
& Photographic Technology; Radiology, Nuclear Medicine & Medical Imaging
SC Engineering; Physics; Imaging Science & Photographic Technology;
Radiology, Nuclear Medicine & Medical Imaging
GA BAM64
UT WOS:000304755601189
ER
PT S
AU Bodnarik, JG
Schweitzer, JS
Parsons, AM
Evans, LG
Starr, RD
AF Bodnarik, Julia G.
Schweitzer, Jeffrey S.
Parsons, Ann M.
Evans, Larry G.
Starr, Richard D.
GP IEEE
TI PING Gamma Ray and Neutron Measurements of a Meter-Sized Carbonaceous
Asteroid Analog
SO 2011 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE
(NSS/MIC)
SE IEEE Nuclear Science Symposium Conference Record
LA English
DT Proceedings Paper
CT IEEE Nuclear Science Symposium/Medical Imaging Conference (NSS/MIC)/18th
International Workshop on Room-Temperature Semiconductor X-Ray and
Gamma-Ray Detectors
CY OCT 23-29, 2011
CL Valencia, SPAIN
SP IEEE, Inst Elect & Elect Engineers Nucl & Plasma Sci Soc (IEEE NPSS)
AB The only main source of elemental composition information for carbonaceous (spectral type C or C-type) asteroids is from their optical, near-infrared and infrared properties, which include their spectral reflectance characteristics, albedo, polarization, and the comparison of optical spectroscopy with meteorite groups corresponding to asteroids of every spectral type. However, these sources reflect observations from widely contrasting spatial scales presently yielding a void in the continuum of microscopic and macroscopic evidence, a lack of in situ measurement confirmation, and require deeper sensing techniques to discern the nature of carbonaceous asteroids. The Probing In situ with Neutrons and Gamma rays (PING) instrument is ideally suited to address these issues because it can be used to determine the bulk elemental composition of asteroids. One aspect of the current work includes experimentally testing and optimizing PING on a known meter-sized basalt and polyethylene layered C-type asteroid analog sample that has the same neutron response as that of a C-type asteroid. To insure that the neutron response for the asteroid analog sample is like that of a C-type asteroid, the key elements are that the thermal and epithermal neutron fluxes, as a function of depth beneath the surface, need to closely approximate those of a C-type asteroid. In this paper, we will present the PING basalt layering experimental data and Monte Carlo computer simulations.
C1 [Bodnarik, Julia G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Schweitzer, Jeffrey S.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Parsons, Ann M.; Evans, Larry G.; Starr, Richard D.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
RP Bodnarik, JG (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
EM Julia.G.Bodnarik@nasa.gov
RI Parsons, Ann/I-6604-2012
FU Fisk University; Vanderbilt University; NASA Planetary Instrumentation
Definition and Development Program; NASA Goddard Space Flight Center
Internal Research And Development; NASA Goddard Space Flight Center
Solar System Exploration Division
FX This work was supported in part by Fisk University, Vanderbilt
University, the NASA Planetary Instrumentation Definition and
Development Program, the NASA Goddard Space Flight Center Internal
Research And Development, and the NASA Goddard Space Flight Center Solar
System Exploration Division.
NR 4
TC 0
Z9 0
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1082-3654
BN 978-1-4673-0120-6
J9 IEEE NUCL SCI CONF R
PY 2011
BP 1861
EP 1865
PG 5
WC Engineering, Electrical & Electronic; Physics, Applied; Imaging Science
& Photographic Technology; Radiology, Nuclear Medicine & Medical Imaging
SC Engineering; Physics; Imaging Science & Photographic Technology;
Radiology, Nuclear Medicine & Medical Imaging
GA BAM64
UT WOS:000304755602017
ER
PT S
AU Allen, B
Hong, J
Grindlay, J
Burke, M
Barthelmy, S
Baker, R
Harrison, F
Mao, P
Cook, W
AF Allen, Branden
Hong, Jaesub
Grindlay, Jonathan
Burke, Michael
Barthelmy, Scott
Baker, Robert
Harrison, Fiona
Mao, Peter
Cook, William
GP IEEE
TI Development of the ProtoEXIST2 Advanced CZT Detector Plane
SO 2011 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE
(NSS/MIC)
SE IEEE Nuclear Science Symposium Conference Record
LA English
DT Proceedings Paper
CT IEEE Nuclear Science Symposium/Medical Imaging Conference (NSS/MIC)/18th
International Workshop on Room-Temperature Semiconductor X-Ray and
Gamma-Ray Detectors
CY OCT 23-29, 2011
CL Valencia, SPAIN
SP IEEE, Inst Elect & Elect Engineers Nucl & Plasma Sci Soc (IEEE NPSS)
DE CdZnTe; Astronomy; X-ray; Gamma-ray; Radiation Detection; Pixel
Distortion; Distortion Mapping
ID MISSION; ISGRI; BAT
AB The ProtoEXIST program was conceived for the development of a highly scalable detector plane architecture utilizing pixilated CdZnTe (CZT) detectors for eventual deployment in a large scale (1-4 m(2) active area) coded aperture X-ray telescope. Development is now underway for ProtoEXIST2, which ultimately will be comprised of a closely tiled 8x8 array of 19.9 mm x 19.9 mm, 5 mm thick Redlen CZT crystals, analogous to ProtoEXIST1, but will now utilize the NuASIC which accommodates the direct bonding of CZT detectors with a 32x32 pixilated anode with a 604.8 mu m pixel pitch and a guard ring surrounding the perimeter of the anode pattern. Currently 6 prototype detectors have been fabricated and tested. An energy threshold of approximately 6 keV and energy resolutions of 2.5 keV FWHM at 122.0 keV and 2.1 keV at 59.6 keV have been achieved with individual detectors. The performance and energy resolution of the individual prototype detectors is discussed in detail. In addition, during preliminary testing of the prototype ProtoEXIST2 detectors reduced photopeak efficiency and pixel distortions were observed for pixels within approximately 3 mm of the CZT edge. These distortions have been largely corrected with two independent techniques: the application of an 73 mm x 73 mm extended cathode centered directly above the detector and the use of a grounded, 6mm tall, electrostatic side shield surrounding the perimeter of the detector. The effects of the side shield and extended cathode are covered in detail.
C1 [Allen, Branden; Hong, Jaesub; Grindlay, Jonathan; Burke, Michael] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Barthelmy, Scott; Baker, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Harrison, Fiona; Mao, Peter; Cook, William] CALTECH, Pasadena, CA 91125 USA.
RP Allen, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ballen@cfa.harvard.edu
FU NASA grants to Harvard [NNX09A076G, NNX11AF35G]
FX We thank Alexi Bolitinokov for discussion in the early phases of
testing. This work was supported by NASA grants to Harvard, NNX09A076G
and NNX11AF35G.
NR 21
TC 5
Z9 5
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1082-3654
BN 978-1-4673-0120-6
J9 IEEE NUCL SCI CONF R
PY 2011
BP 4470
EP 4480
PG 11
WC Engineering, Electrical & Electronic; Physics, Applied; Imaging Science
& Photographic Technology; Radiology, Nuclear Medicine & Medical Imaging
SC Engineering; Physics; Imaging Science & Photographic Technology;
Radiology, Nuclear Medicine & Medical Imaging
GA BAM64
UT WOS:000304755604149
ER
PT S
AU Nowicki, SF
Anderson, SE
Parsons, AM
AF Nowicki, Suzanne F.
Anderson, Stephen E.
Parsons, Ann M.
GP IEEE
TI 6 MeV Energy Calibration and Reconstruction with Pixelated CZT Detectors
using Digital Methods
SO 2011 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE
(NSS/MIC)
SE IEEE Nuclear Science Symposium Conference Record
LA English
DT Proceedings Paper
CT IEEE Nuclear Science Symposium/Medical Imaging Conference (NSS/MIC)/18th
International Workshop on Room-Temperature Semiconductor X-Ray and
Gamma-Ray Detectors
CY OCT 23-29, 2011
CL Valencia, SPAIN
SP IEEE, Inst Elect & Elect Engineers Nucl & Plasma Sci Soc (IEEE NPSS)
DE CZT; gamma-ray spectroscopy; high energy
ID CDZNTE DETECTORS
AB CZT is an attractive material for gamma-ray spectroscopy due to its high resolution, high efficiency and ability to operate at room temperature. It has shown better than 1 % FWHM energy resolution at 662 keV. However, at higher energies, the electron cloud gets bigger than the size of a single pixel. This effect is known as charge sharing and contributes to energy resolution degradation. It is important for planetary science and astrophysics applications to broaden the energy range of pixelated CZT detectors. A digitizer system was used to study the response of a 2 cm x 2 cm x 1.5 cm pixelated CZT detector manufactured by Redlen Technology Inc., to a source of 6.129 MeV from the de-excitation of the second excited state of O-16. The 5.107 MeV double escape peak was identified and has shown that the response of the system is linear at high energy.
C1 [Nowicki, Suzanne F.; Parsons, Ann M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Anderson, Stephen E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Nowicki, SF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM suzanne.f.nowicki@nasa.gov
RI Parsons, Ann/I-6604-2012
FU NASA Goddard Space Flight Center
FX This work was supported by the NASA Goddard Space Flight Center.
NR 8
TC 1
Z9 1
U1 0
U2 3
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1082-3654
BN 978-1-4673-0120-6
J9 IEEE NUCL SCI CONF R
PY 2011
BP 4697
EP 4700
PG 4
WC Engineering, Electrical & Electronic; Physics, Applied; Imaging Science
& Photographic Technology; Radiology, Nuclear Medicine & Medical Imaging
SC Engineering; Physics; Imaging Science & Photographic Technology;
Radiology, Nuclear Medicine & Medical Imaging
GA BAM64
UT WOS:000304755604192
ER
PT S
AU Rocha, C
Munoz, C
AF Rocha, Camilo
Munoz, Cesar
BE Simao, A
Morgan, C
TI Simulation and Verification of Synchronous Set Relations in Rewriting
Logic
SO FORMAL METHODS: FOUNDATIONS AND APPLICATIONS: SBMF 2011
SE Lecture Notes in Computer Science
LA English
DT Proceedings Paper
CT 14th Brazilian Symposium on Formal Methods (SBMF)
CY SEP 26-30, 2011
CL Sao Paulo, BRAZIL
SP CNPq, Brazilian Sci & Technol Res Council, CAPES, Brazilian Higher Educ Fund Council, FAPESP, Sao Paulo Res Fdn, Google Inc, Univ Sao Paulo, Univ Presbiteriana Mackenzie
ID P SYSTEMS
AB This paper presents a mathematical foundation and a rewriting logic infrastructure for the execution and property verification of synchronous set relations. The mathematical foundation is given in the language of abstract set relations. The infrastructure consists of an order-sorted rewrite theory in Maude, a rewriting logic system, that enables the synchronous execution of a set relation provided by the user. By using the infrastructure, existing algorithm verification techniques already available in Maude for traditional asynchronous rewriting, such as reachability analysis and model checking, are automatically available to synchronous set rewriting. The use of the infrastructure is illustrated with an executable operational semantics of a simple synchronous language and the verification of temporal properties of a synchronous system.
C1 [Rocha, Camilo] Univ Illinois, Urbana, IL USA.
[Munoz, Cesar] NASA, Langley Res Ctr, Washington, DC USA.
RP Rocha, C (reprint author), Univ Illinois, Urbana, IL USA.
FU NASA's Autonomous Systems and Avionics Project, Software Verification
Algorithms.; NSF [CCF 09-05584]; National Aeronautics and Space
Administration at Langley Research Center under Research Cooperative
Agreement [NNL09AA00A]
FX The authors would like to thank the anonymous referees for their
comments, which helped to improve the paper. This work is supported by
NASA's Autonomous Systems and Avionics Project, Software Verification
Algorithms. The first author has been partially supported by NSF grant
CCF 09-05584 and by the National Aeronautics and Space Administration at
Langley Research Center under Research Cooperative Agreement No.
NNL09AA00A awarded to the National Institute of Aerospace.
NR 16
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0302-9743
BN 978-3-642-25031-6
J9 LECT NOTES COMPUT SC
PY 2011
VL 7021
BP 60
EP +
PG 3
WC Computer Science, Theory & Methods
SC Computer Science
GA BBB82
UT WOS:000306388800005
ER
PT B
AU Szabat, KA
O'Connor, A
Tavana, M
AF Szabat, Kathryn A.
O'Connor, Aidan
Tavana, Madjid
BA Tavana, M
BF Tavana, M
TI Managing Adaptability, Intervention, and People in Enterprise
Information Systems Preface
SO MANAGING ADAPTABILITY, INTERVENTION, AND PEOPLE IN ENTERPRISE
INFORMATION SYSTEMS
LA English
DT Editorial Material; Book Chapter
C1 [Szabat, Kathryn A.; Tavana, Madjid] La Salle Univ, Dept Management, Philadelphia, PA 19141 USA.
[O'Connor, Aidan] Ecole Super Commerce & Management, Paris, France.
[Tavana, Madjid] Management Informat Syst & Decis Sci, Philadelphia, PA USA.
[Tavana, Madjid] La Salle Univ, Ctr Technol & Management, Philadelphia, PA USA.
[Tavana, Madjid] Kennedy Space Ctr, Kennedy Space Ctr, FL USA.
[Tavana, Madjid] Johnson Space Ctr, Houston, TX USA.
[Tavana, Madjid] Naval Res Lab, Washington, DC USA.
[Tavana, Madjid] Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
[Tavana, Madjid] AF Res Lab, Wright Patterson AFB, OH USA.
RP Szabat, KA (reprint author), La Salle Univ, Dept Management, Philadelphia, PA 19141 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IGI GLOBAL
PI HERSEY
PA 701 E CHOCOLATE AVE, STE 200, HERSEY, PA 17033-1240 USA
BN 978-1-60960-530-8; 978-1-60960-529-2
PY 2011
BP XII
EP +
D2 10.4018/978-1-60960-529-2
PG 39
WC Business; Management
SC Business & Economics
GA BZV42
UT WOS:000303059500001
ER
PT S
AU Greer, F
Hoenk, ME
Jacquot, BC
Jones, TJ
Dickie, MR
Monacos, SP
Nikzad, S
Hamden, E
Schmonivich, D
Day, P
Leduc, H
AF Greer, F.
Hoenk, M. E.
Jacquot, B. C.
Jones, T. J.
Dickie, M. R.
Monacos, S. P.
Nikzad, S.
Hamden, E.
Schmonivich, D.
Day, P.
Leduc, H.
BE Elam, JW
Londergan, A
VanDerStraten, O
Roozeboom, F
DeGendt, S
Bent, SF
Delabie, A
TI Enabling High Performance Instruments for Astronomy and Space
Exploration with ALD
SO ATOMIC LAYER DEPOSITION APPLICATIONS 7
SE ECS Transactions
LA English
DT Proceedings Paper
CT 7th Symposium on Atomic Layer Deposition Applications/220th Meeting of
the Electrochemical-Society (ECS)
CY OCT 10-12, 2011
CL Boston, MA
SP Electrochem Soc (ECS), Air Liquide, Appl Mat, Cambridge NanoTech, Gelest, Tokyo Electron, Dielect Sci & Technol, Elect & Photon
ID SILICON
AB Future UV, X-ray, and sub-millimeter telescopes and spectrometers have the potential to revolutionize our understanding of the formation and habitability of the modern universe.(1-4) Star formation, dark energy, and the composition of the intergalactic medium are only some of the key scientific topics that can be addressed by UV astronomy and astrophysics. Sub-millimeter astronomy can probe the fine structure of the cosmic microwave background, giving glimpses into the early universe immediately following the Big Bang.(5) Various surface engineering techniques including molecular beam epitaxy and atomic layer deposition have been utilized here to significantly boost the performance of key components of instruments for astronomy and astrophysics investigation, taking advantage of the atomic level precision that these techniques provide.
C1 [Greer, F.; Hoenk, M. E.; Jacquot, B. C.; Jones, T. J.; Dickie, M. R.; Monacos, S. P.; Nikzad, S.; Day, P.; Leduc, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Greer, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU ELECTROCHEMICAL SOC INC
PI PENNINGTON
PA 65 S MAIN ST, PENNINGTON, NJ 08534-2839 USA
SN 1938-5862
BN 978-1-60768-256-1
J9 ECS TRANSACTIONS
PY 2011
VL 41
IS 2
BP 263
EP 268
DI 10.1149/1.3633676
PG 6
WC Electrochemistry; Physics, Applied
SC Electrochemistry; Physics
GA BAX20
UT WOS:000305937200028
ER
PT S
AU DeBonis, JR
AF DeBonis, James R.
BE Salvetti, MV
Geurts, B
Meyers, J
Sagaut, P
TI An Examination of the Spatial Resolution Requirements for LES of a
Compressible Jet
SO QUALITY AND RELIABILITY OF LARGE-EDDY SIMULATIONS II
SE ERCOFTAC Series
LA English
DT Proceedings Paper
CT 2nd Workshop on Quality and Reliability of Large-Eddy Simulations
CY SEP 09-11, 2009
CL Univ Pisa, Pisa, ITALY
HO Univ Pisa
DE spatial discretization; grid resolution; jet flow
ID SCHEMES
AB This work examines the grid requirements necessary for a properly resolved large-eddy simulation (LES) of a compressible jet. The numerical scheme used for the analysis and its corresponding computational grid are used to estimate, a priori, the resolution of the simulation. This estimated resolution, expressed in terms of wave number, is compared to the resolution in the turbulent spectra obtained from the simulation. Two levels of grid resolution are examined. The solution yields good agreement with experimental data for mean flow and first-order turbulent statistics. The estimated resolution of the analysis properly predicts the trends with respect to the computed turbulent spectra.
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP DeBonis, JR (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM james.r.debonis@nasa.gov
RI sagaut, pierre/M-3880-2014
OI sagaut, pierre/0000-0002-3785-120X
NR 10
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 1382-4309
BN 978-94-007-0231-8
J9 ERCOFTAC SER
PY 2011
VL 16
BP 329
EP 338
DI 10.1007/978-94-007-0231-8_30
PG 10
WC Mechanics
SC Mechanics
GA BAZ65
UT WOS:000306194400030
ER
PT J
AU Finkelstein, H
Blaber, E
Dvorochkin, N
Globus, RK
Burns, BP
Almeida, EA
AF Finkelstein, H.
Blaber, E.
Dvorochkin, N.
Globus, R. K.
Burns, B. P.
Almeida, E. A.
TI Spaceflight alters the migratory ability of stem cell derived
keratinocytes resulting in decreased wound healing potential
SO MOLECULAR BIOLOGY OF THE CELL
LA English
DT Meeting Abstract
CT Annual Meeting of the American-Society-for-Cell-Biology (ASCB)
CY DEC 03-07, 2011
CL Denver, CO
SP Amer Soc Cell Biol (ASCB)
C1 [Finkelstein, H.; Blaber, E.; Dvorochkin, N.; Globus, R. K.; Almeida, E. A.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
[Blaber, E.; Burns, B. P.] UNSW, Sch Biotechnol & Biomol Sci, Sydney, NSW, Australia.
[Almeida, E. A.] UCSF, Dept Cell Tissue Biol, San Francisco, CA USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC CELL BIOLOGY
PI BETHESDA
PA 8120 WOODMONT AVE, STE 750, BETHESDA, MD 20814-2755 USA
SN 1059-1524
J9 MOL BIOL CELL
JI Mol. Biol. Cell
PY 2011
VL 22
MA 1533
PG 2
WC Cell Biology
SC Cell Biology
GA 961YM
UT WOS:000305505503120
ER
PT S
AU Sandford, SA
AF Sandford, Scott A.
BE Cernicharo, J
Bachiller, R
TI The Power of Sample Return Missions - Stardust and Hayabusa
SO MOLECULAR UNIVERSE
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 280th Symposium of the International Astronomical Union
CY MAY 30-JUN 03, 2011
CL Toledo, SPAIN
SP Int Astronom Union, Minist Ciencia & Technologia, Consejo Superior Investigac Cientificas, Inst Nacl Tecnica Aeroespacial (INTA), Inst Geograf Nacl, Univ Castilla Mancha
DE Stardust Mission; Hayabusa Mission; comets: general; comets: individual
(Wild 2); asteroids; sample return
ID COMET 81P/WILD 2; X-RAY-FLUORESCENCE; ASTEROID ITOKAWA; ISOTOPIC
COMPOSITIONS; PARTICLES; WILD-2; SPACECRAFT; MATTER; DUST; MICROSCOPE
AB Sample return missions offer opportunities to learn things about other objects in our Solar System (and beyond) that cannot be determined by observations using in situ spacecraft. This is largely because the returned samples can be studied in terrestrial laboratories where the analyses are not limited by the constraints - power, mass, time, precision, etc. - imposed by normal spacecraft operations. In addition, the returned samples serve as a scientific resource that is available far into the future; the study of the samples can continue long after the original spacecraft mission is finished. This means the samples can be continually revisited as both our scientific understanding and analytical techniques improve with time.
These advantages come with some additional difficulties, however. In particular, sample return missions must deal with the additional difficulties of proximity operations near the objects they are to sample, and they must be capable of successfully making a round trip between the Earth and the sampled object. Such missions therefore need to take special precautions against unique hazards and be designed to successfully complete relatively extended mission durations.
Despite these difficulties, several recent missions have managed to successfully complete sample returns from a number of Solar System objects. These include the Stardust mission (samples from Comet 81P/Wild 2), the Hayabusa mission (samples from asteroid 25143 Itokawa), and the Genesis mission (samples of solar wind). This paper will review the advantages and difficulties of sample return missions in general and will summarize some key findings of the recent Stardust and Hayabusa missions.
C1 NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Sandford, SA (reprint author), NASA, Astrophys Branch, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA.
EM Scott.A.Sandford@nasa.gov
NR 36
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 978-1-107-01980-5
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2011
IS 280
BP 275
EP 287
DI 10.1017/S174392131102504X
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAT30
UT WOS:000305449300024
ER
PT J
AU Malekpour, MR
AF Malekpour, Mahyar R.
GP IEEE
TI A Self-Stabilizing Synchronization Protocol For Arbitrary Digraphs
SO 2011 IEEE 17TH PACIFIC RIM INTERNATIONAL SYMPOSIUM ON DEPENDABLE
COMPUTING (PRDC)
LA English
DT Proceedings Paper
CT 17th IEEE Pacific Rim International Symposium on Dependable Computing
(PRDC)
CY DEC 12-14, 2011
CL Pasadena, CA
SP IEEE, IEEE Comp Soc, IFIP, Jet Prop Lab (JPL)
DE self-stabilizing; arbitrary; digraph; emergent system; distributed;
clock; synchronization
ID SMALL-WORLD NETWORKS; CLOCK SYNCHRONIZATION; OSCILLATORS; SYSTEMS;
FAULTS
AB This paper presents a self-stabilizing distributed clock synchronization protocol in the absence of faults in the system. It is focused on the distributed clock synchronization of an arbitrary, non-partitioned digraph ranging from fully connected to 1-connected networks of nodes while allowing for differences in the network elements. This protocol does not rely on assumptions about the initial state of the system, other than the presence of at least one node, and no central clock or a centrally generated signal, pulse, or message is used. Nodes are anonymous, i.e., they do not have unique identities. There is no theoretical limit on the maximum number of participating nodes. The only constraint on the behavior of the node is that the interactions with other nodes are restricted to defined links and interfaces. This protocol deterministically converges within a time bound that is a linear function of the self-stabilization period. We present an outline of a deductive proof of the correctness of the protocol. A bounded model of the protocol was mechanically verified for a variety of topologies. Results of the mechanical proof of the correctness of the protocol are provided. The model checking results have verified the correctness of the protocol as they apply to the networks with unidirectional and bidirectional links. In addition, the results confirm the claims of determinism and linear convergence. As a result, we conjecture that the protocol solves the general case of this problem. We also present several variations of the protocol and discuss that this synchronization protocol is indeed an emergent system.
C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Malekpour, MR (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM mahyar.r.malekpour@nasa.gov
NR 37
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-0-7695-4590-5
PY 2011
BP 254
EP 263
DI 10.1109/PRDC.2011.37
PG 10
WC Computer Science, Hardware & Architecture; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA BAP65
UT WOS:000305062200028
ER
PT J
AU McKelvin, ML
Gamble, EB
Holzmann, GJ
AF McKelvin, Mark L., Jr.
Gamble, Edward B., Jr.
Holzmann, Gerard J.
GP IEEE
TI Model Checking Multitask Applications for OSEK Compliant Real-Time
Operating Systems
SO 2011 IEEE 17TH PACIFIC RIM INTERNATIONAL SYMPOSIUM ON DEPENDABLE
COMPUTING (PRDC)
LA English
DT Proceedings Paper
CT 17th IEEE Pacific Rim International Symposium on Dependable Computing
(PRDC)
CY DEC 12-14, 2011
CL Pasadena, CA
SP IEEE, IEEE Comp Soc, IFIP, Jet Prop Lab (JPL)
ID SPIN
AB In the verification of multitask software in real-time embedded systems, general purpose model checkers do not inherently consider characteristics of the real-time operating system, such as priority-based scheduling, priority inversion, and protocols for protecting shared memory resources. Since explicit state model checkers generally explore all possible execution paths and task interleaving, this could potentially lead to exploring execution paths that are redundant, unnecessarily increasing verification complexity and hampering tractability. Based on this premise, in this work we investigate how one can improve the performance of explicit state model checkers, such as SPIN, for the verification of multitask applications that target real-time operating systems.
C1 [McKelvin, Mark L., Jr.; Gamble, Edward B., Jr.; Holzmann, Gerard J.] CALTECH, Jet Prop Lab, Lab Reliable Software, Pasadena, CA 91109 USA.
RP McKelvin, ML (reprint author), CALTECH, Jet Prop Lab, Lab Reliable Software, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mark.mckelvin@jpl.nasa.gov; ed.gamble@jpl.nasa.gov;
gerard.j.holzmann@jpl.nasa.gov
NR 16
TC 0
Z9 0
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-0-7695-4590-5
PY 2011
BP 280
EP 281
DI 10.1109/PRDC.2011.49
PG 2
WC Computer Science, Hardware & Architecture; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA BAP65
UT WOS:000305062200034
ER
PT J
AU Tso, KS
Pajevski, MJ
Johnson, B
AF Tso, Kam S.
Pajevski, Michael J.
Johnson, Bryan
GP IEEE
TI Access Control of Web and Java Based Applications
SO 2011 IEEE 17TH PACIFIC RIM INTERNATIONAL SYMPOSIUM ON DEPENDABLE
COMPUTING (PRDC)
LA English
DT Proceedings Paper
CT 17th IEEE Pacific Rim International Symposium on Dependable Computing
(PRDC)
CY DEC 12-14, 2011
CL Pasadena, CA
SP IEEE, IEEE Comp Soc, IFIP, Jet Prop Lab (JPL)
AB Cyber security has gained national and international attention as a result of near continuous headlines from financial institutions, retail stores, government offices and universities reporting compromised systems and stolen data. Concerns continue to rise as threats of service interruption, unauthorized access, stealing and altering of information, and spreading of viruses become ever more prevalent and serious. Controlling access to application layer resources is a critical component in a layered security solution that includes encryption, firewalls, virtual private networks, antivirus, and intrusion detection. In this paper we discuss the development of an application-level access control solution, based on an open-source access manager augmented with custom software components, to provide protection to both Web-based and Java-based client and server applications.
C1 [Tso, Kam S.; Pajevski, Michael J.; Johnson, Bryan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tso, KS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 9
TC 0
Z9 0
U1 0
U2 6
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-0-7695-4590-5
PY 2011
BP 320
EP 325
DI 10.1109/PRDC.2011.54
PG 6
WC Computer Science, Hardware & Architecture; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA BAP65
UT WOS:000305062200046
ER
PT B
AU Mattmann, CA
Crichton, DJ
Hart, AF
Goodale, C
Hughes, JS
Kelly, S
Cinquini, L
Painter, TH
Lazio, J
Waliser, D
Medvidovic, N
Kim, J
Lean, P
AF Mattmann, Chris A.
Crichton, Daniel J.
Hart, Andrew F.
Goodale, Cameron
Hughes, J. Steven
Kelly, Sean
Cinquini, Luca
Painter, Thomas H.
Lazio, Joseph
Waliser, Duane
Medvidovic, Nenad
Kim, Jinwon
Lean, Peter
BE Furht, B
Escalante, A
TI Architecting Data-Intensive Software Systems
SO HANDBOOK OF DATA INTENSIVE COMPUTING
LA English
DT Article; Book Chapter
ID WESTERN UNITED-STATES; SNOWPACK; IMPACTS; CLIMATE; WINTER
C1 [Mattmann, Chris A.; Crichton, Daniel J.; Hart, Andrew F.; Goodale, Cameron; Hughes, J. Steven; Kelly, Sean; Cinquini, Luca; Painter, Thomas H.; Lazio, Joseph; Waliser, Duane] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA.
[Medvidovic, Nenad] Univ So Calif, Dept Comp Sci, Viterbi Sch Engn, Los Angeles, CA 90089 USA.
[Kim, Jinwon] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA USA.
[Lean, Peter] Univ Reading, Dept Meteorol, Reading, Berks, England.
RP Mattmann, CA (reprint author), CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA.
EM chris.a.mattmann@nasa.gov; daniel.j.crichton@jpl.nasa.gov;
andrew.f.hart@jpl.nasa.gov; cameron.e.goodale@jpl.nasa.gov;
john.s.hughes@jpl.nasa.gov; sean.kelly@jpl.nasa.gov;
luca.cinquini@jpl.nasa.gov; thomas.painter@jpl.nasa.gov;
joseph.lazio@jpl.nasa.gov; duane.e.waliser@jpl.nasa.gov; neno@usc.edu;
jkim@atmos.ucla.edu; p.w.lean@reading.ac.uk
NR 37
TC 3
Z9 3
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
BN 978-1-4614-1414-8
PY 2011
BP 25
EP 57
DI 10.1007/978-1-4614-1415-5_2
D2 10.1007/978-1-4614-1415-5
PG 33
WC Computer Science, Theory & Methods
SC Computer Science
GA BZZ54
UT WOS:000303419100002
ER
PT S
AU Hossain, MS
Atiquzzaman, M
Ivancic, W
AF Hossain, Md Shohrab
Atiquzzaman, Mohammed
Ivancic, William
GP IEEE
TI Scalability Analysis of a Multihomed Network Mobility Protocol
SO 2011 IEEE GLOBECOM WORKSHOPS (GC WKSHPS)
SE IEEE Globecom Workshops
LA English
DT Proceedings Paper
CT IEEE GLOBECOM Workshops (GC Wkshps)
CY DEC 05-09, 2011
CL Houston, TX
SP IEEE
DE Mobility Protocols; Scalability analysis; Network Mobility; Mathematical
Modeling; Multihoming
AB Previous studies have analyzed cost and performance of multihomed network mobility management protocols, such as, Seamless IP diversity-based Network Mobility management scheme (SINEMO). However, increase in the number of mobile nodes raises scalability issues which can result in its performance degradation. In this paper, we have developed analytical models for scalability analysis of SINEMO in terms of network size, mobility rate, and traffic rate. We have used numerical results to validate the analytical model and compared scalability with basic Network Mobility (NEMO) protocol. Results show that the network-mobility protocols exhibit asymptotically identical scalability for the network though the mobility agent of SINEMO scales better than NEMO. This scalability model can help in quantitative scalability analysis of other mobility protocols, thereby visualizing the effects of future network expansion on the performance of the mobility protocols.
C1 [Hossain, Md Shohrab; Atiquzzaman, Mohammed] Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA.
[Ivancic, William] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Hossain, MS (reprint author), Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA.
EM shohrab@ou.edu; atiq@ou.edu; wivancic@grc.nasa.gov
FU NASA [NNX06AE44G]
FX The research work reported in this paper was supported by NASA Grant
NNX06AE44G.
NR 10
TC 3
Z9 3
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 2166-0069
BN 978-1-4673-0040-7
J9 IEEE GLOBE WORK
PY 2011
BP 513
EP 517
PG 5
WC Computer Science, Information Systems; Engineering, Electrical &
Electronic; Telecommunications
SC Computer Science; Engineering; Telecommunications
GA BAG61
UT WOS:000304097200096
ER
PT S
AU Hossain, MS
Atiquzzaman, M
Ivancic, WD
AF Hossain, Md. Shohrab
Atiquzzaman, Mohammed
Ivancic, William D.
GP IEEE
TI Survivability Evaluation of NEMO with Multiple Mobile Routers
SO 2011 IEEE GLOBECOM WORKSHOPS (GC WKSHPS)
SE IEEE Globecom Workshops
LA English
DT Proceedings Paper
CT IEEE GLOBECOM Workshops (GC Wkshps)
CY DEC 05-09, 2011
CL Houston, TX
SP IEEE
DE Network mobility; survivability evaluation; CTMC modeling; DDoS attack;
Mobile Router
ID IP
AB Mobile networks (NEMO) can be formed with IP-enabled devices in motion. Mobile Router (MR) acts as the gateway for all the nodes inside a mobile network. As the MR is the key entity in NEMO, the load on MR can be very high and can become the performance bottleneck. Increase in number of MRs can improve the reliability, as a single MR can be single point of failure. There have no survivability analysis of NEMO based on multiple MRs. In this paper, we have performed quantitative survivability analysis of NEMO with multiple MRs, taking into consideration possible node and link failures along with denial of service attacks. We have presented numerical results which reveals that increase in number of mobile routers improves the performance of the mobile network by reducing the mean delay and drop probability while withstanding attack packets.
C1 [Hossain, Md. Shohrab; Atiquzzaman, Mohammed] Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA.
[Ivancic, William D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Hossain, MS (reprint author), Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA.
EM shohrab@ou.edu; atiq@ou.edu; wivancic@grc.nasa.gov
FU NASA [NNX06AE44G]
FX The research work reported in this paper was supported by NASA Grant
NNX06AE44G.
NR 11
TC 0
Z9 0
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 2166-0069
BN 978-1-4673-0040-7
J9 IEEE GLOBE WORK
PY 2011
BP 524
EP 528
PG 5
WC Computer Science, Information Systems; Engineering, Electrical &
Electronic; Telecommunications
SC Computer Science; Engineering; Telecommunications
GA BAG61
UT WOS:000304097200098
ER
PT S
AU Swain, MR
Deroo, P
Vasisht, G
AF Swain, Mark R.
Deroo, Pieter
Vasisht, Gautam
BE Sozzetti, A
Lattanzi, MG
Boss, AP
TI NICMOS spectroscopy of HD 189733b
SO ASTROPHYSICS OF PLANETARY SYSTEMS: FORMATION, STRUCTURE, AND DYNAMICAL
EVOLUTION
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 276th Symposium of the International-Astronomical-Union on Astrophysics
of Planetary Systems: Formation, Structure, and Dynamical Evolution
CY OCT 10-15, 2010
CL Torino, ITALY
SP Int Astronom Union Div 3, Int Astronom Union Commiss 51, Int Astronom Union Commiss 53, Ist Nazl Astrofis, Osservatorio Astronom Torino
DE techniques: spectroscopic; infrared: stars; planetary systems
ID EXTRASOLAR PLANET; EMISSION-SPECTRUM; ATMOSPHERE; 209458B; METHANE;
WATER
AB Spectral features corresponding to methane and water opacity were reported based on transmission spectroscopy of HD 189733b with Hubble/NICMOS. Recently, these data, and a similar data set for XO-1b, have been reexamined in Gibson et al. (2010), who claim they cannot reliably reproduce prior results. We examine the methods used by the Gibson team and identify two specific issues that could act to increase the formal uncertainties and to create instability in the minimization process. This would also be consistent with the GPA10 finding that they could not identify a way to select among the several instrument models they constructed. In the case of XO-1b, the Gibson team significantly changed the way in which the instrument model is defined (both with respect to the three approaches they used for HD 189733b, and the approach used by previous authors); this change, which omits the effect of the spectrum position on the detector, makes direct intercomparison of results difficult. In the experience of our group, the position of the spectrum on the detector is an important element of the instrument model because of the significant residual structure in the NICMOS spectral flat field. The approach of changing instrument models significantly complicates understanding the data reduction process and interpreting the results. Our team favors establishing a consistent method of handling NICMOS instrument systematic errors and applying it uniformly to data sets.
C1 [Deroo, Pieter; Vasisht, Gautam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Swain, MR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove, Pasadena, CA 91109 USA.
EM Mark.R.Swain@jpl.nasa.gov
NR 16
TC 3
Z9 3
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 978-0-521-19652-9
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2011
VL 276
BP 148
EP 153
DI 10.1017/S1743921311020096
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAN65
UT WOS:000304838200024
ER
PT S
AU Clampin, M
AF Clampin, Mark
BE Sozzetti, A
Lattanzi, MG
Boss, AP
TI The James Webb Space Telescope and its capabilities for exoplanet
science
SO ASTROPHYSICS OF PLANETARY SYSTEMS: FORMATION, STRUCTURE, AND DYNAMICAL
EVOLUTION
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 276th Symposium of the International-Astronomical-Union on Astrophysics
of Planetary Systems: Formation, Structure, and Dynamical Evolution
CY OCT 10-15, 2010
CL Torino, ITALY
SP Int Astronom Union Div 3, Int Astronom Union Commiss 51, Int Astronom Union Commiss 53, Ist Nazl Astrofis, Osservatorio Astronom Torino
DE planetary systems; instrumentation: high angular resolution;
instrumentation: miscellaneous; telescopes; space vehicles
ID EXTRASOLAR PLANET; ATMOSPHERE; METHANE
AB The James Webb Space Telescope is a large aperture (6.5 meter), cryogenic space telescope with a suite of near and mid-infrared instruments covering the wavelength range of 0.6 ?m to 28 ?m. JWSTs primary science goal is to detect and characterize the first galaxies. It will also study the assembly of galaxies, star formation, and the formation of evolution of planetary systems. JWSTs instrument complement offers numerous capabilities to study the formation and evolution of exoplanets via direct imaging, high contrast coronagraphic imaging and photometric and spectroscopic observations of transiting exoplanets.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Clampin, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM mark.clampin@nasa.gov
NR 21
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 978-0-521-19652-9
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2011
VL 276
BP 335
EP 342
DI 10.1017/S1743921311020400
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAN65
UT WOS:000304838200055
ER
PT S
AU Barry, RK
Deming, LD
AF Barry, Richard K.
Deming, L. Drake
BE Sozzetti, A
Lattanzi, MG
Boss, AP
TI Alien Earth: Glint observations of a remote planet
SO ASTROPHYSICS OF PLANETARY SYSTEMS: FORMATION, STRUCTURE, AND DYNAMICAL
EVOLUTION
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 276th Symposium of the International-Astronomical-Union on Astrophysics
of Planetary Systems: Formation, Structure, and Dynamical Evolution
CY OCT 10-15, 2010
CL Torino, ITALY
SP Int Astronom Union Div 3, Int Astronom Union Commiss 51, Int Astronom Union Commiss 53, Ist Nazl Astrofis, Osservatorio Astronom Torino
DE infrared: planetary systems; astrobiology; astrochemistry; planetary
systems; Earth
AB We give a preliminary report on a multi-wavelength study of specular reflections from the oceans and clouds of Earth. We use space-borne observations from a distance sufficient to ensure that light rays reflected from all parts of Earth are closely parallel, as they will be when studying exoplanets. We find that the glint properties of Earth in this far-field vantage point are surprising - in the sense that some of the brightest reflections are not from conventional ocean-glints, but appear to arise from cirrus cloud crystals. The Earth observations discussed here were acquired with the High Resolution Instrument (HRI) - a 0.3 m f/35 telescope on the Deep Impact (DI) spacecraft during the Extrasolar Planet Observation and Characterization (EPOCh) investigation.
C1 [Barry, Richard K.; Deming, L. Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Barry, RK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Richard.K.Barry@NASA.gov
NR 1
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 978-0-521-19652-9
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2011
VL 276
BP 471
EP 472
DI 10.1017/S1743921311020849
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAN65
UT WOS:000304838200099
ER
PT S
AU Serabyn, E
Mawet, D
Burruss, R
AF Serabyn, Eugene
Mawet, Dimitri
Burruss, Rick
BE Sozzetti, A
Lattanzi, MG
Boss, AP
TI Imaging faint companions very close to stars
SO ASTROPHYSICS OF PLANETARY SYSTEMS: FORMATION, STRUCTURE, AND DYNAMICAL
EVOLUTION
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 276th Symposium of the International-Astronomical-Union on Astrophysics
of Planetary Systems: Formation, Structure, and Dynamical Evolution
CY OCT 10-15, 2010
CL Torino, ITALY
SP Int Astronom Union Div 3, Int Astronom Union Commiss 51, Int Astronom Union Commiss 53, Ist Nazl Astrofis, Osservatorio Astronom Torino
DE instrumentation: adaptive optics; planetary systems; binaries (including
multiple): close
AB A vortex coronagraph on our extreme adaptive optics "well-corrected subaperture" on the Hale telescope has recently allowed the imaging of the triple-planet HR8799 system with a 1.5 in subaperture. Moreover, a faint, low-mass companion to a second star was imaged only one diffraction beam width away from the primary. These results illustrate the potential of the vortex coronagraph, which can enable exoplanet imaging and characterization with smaller telescopes than previously thought.
C1 [Serabyn, Eugene; Mawet, Dimitri; Burruss, Rick] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Serabyn, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM gene.serabyn@jpl.nasa.gov
NR 4
TC 1
Z9 1
U1 0
U2 3
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND
SN 1743-9213
BN 978-0-521-19652-9
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2011
VL 276
BP 551
EP 552
DI 10.1017/S1743921311021181
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAN65
UT WOS:000304838200133
ER
PT S
AU Meier, DL
AF Meier, David L.
BE Romero, GE
Sunyaev, RA
Belloni, TM
TI The formation of relativistic cosmic jets
SO JETS AT ALL SCALES
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 275th Symposium of the International-Astronomical-Union on Jets at All
Scales
CY SEP 13-17, 2010
CL Buenos Aires, ARGENTINA
SP IAU Div 10, IAU Div 11, Inst Argentino Radioastronomia
DE black hole physics; accretion; MHD; galaxies: jets; X-ray binaries: jets
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE; NUMERICAL SIMULATIONS; ACCRETION
DISKS; MAGNETIZED JETS; RADIO-LOUD; MODEL; MAGNETOSPHERE; INSTABILITY;
EVOLUTION
AB I review current ideas on the launching, acceleration, collimation and propagation of relativistic jets and the influence of strong magnetic fields in the process. Recently, several important elements of the entire jet "engine" structure have been shown to play key roles in the production of an astrophysical jet. Depending on the type of system, these include the spin of the central black hole, the thermal and/or magnetic state of the accretion flow, the presence of a re-collimation point in the jet outflow far away from the central object, and the behavior of MHD shocks and kink instabilities in the final jet. While these physical processes probably are at work in all types of relativistic jets (and many even in more benign stellar outflows), I shall concentrate on ones produced by lower luminosity black hole sources, both in active galactic nuclei and in X-ray binaries. I also will discuss the connection between the theoretical concepts and the large body of observational data, now available on these systems.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Meier, DL (reprint author), CALTECH, Jet Prop Lab, MS 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM David.L.Meier@jpl.nasa.gov
NR 47
TC 1
Z9 1
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 978-0-52176-607-4
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2011
VL 275
BP 13
EP 23
DI 10.1017/S1743921310015590
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAP08
UT WOS:000304974800002
ER
PT B
AU Deroo, P
Swain, M
Vasisht, G
Chen, P
Tinetti, G
Bouwman, J
Angerhausen, D
Yung, Y
AF Deroo, Pieter
Swain, Mark
Vasisht, Gautam
Chen, Pin
Tinetti, Giovanna
Bouwman, Jeroen
Angerhausen, Daniel
Yung, Yuk
BE Beaulieu, JP
Dieters, S
Tinetti, G
TI Exoplanet Spectroscopy: The Hubble Case
SO MOLECULES IN THE ATMOSPHERES OF EXTRASOLAR PLANETS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Molecules in the Atmospheres of Extrasolar Planets
CY NOV 19-21, 2008
CL Observ Paris, Paris, FRANCE
HO Observ Paris
AB The Hubble Space Telescope has recently emerged as the first telescope to detect molecular signatures in an exoplanet via infrared spectroscopy. Molecular spectroscopy of exoplanets is demanding and requires an accurate determination and removal of the instrument systematics. Here we report on our effort to extract accurate exoplanet spectra from NICMOS spectrophotometry. We developed a standardized and highly automated pipeline to remove instrument systematics based on our previous results. We tested the pipeline and find excellent agreement with observation specific implementations. The process of decorrelating instrument parameters from the measured time series is well understood, stable and guarantees reproducible results.
C1 [Deroo, Pieter; Swain, Mark; Vasisht, Gautam; Chen, Pin] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Tinetti, Giovanna] UCL, London WC1E 6BT, England.
[Bouwman, Jeroen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Angerhausen, Daniel] Univ Stuttgart, Inst Space Syst, German SOFIA Ins, D-70569 Stuttgart, Germany.
[Yung, Yuk] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Deroo, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM pieter.d.deroo@jpl.nasa.gov; mark.r.swain@jpl.nasa.gov;
gautam.vasisht@jpl.nasa.gov; pin.chen@jpl.nasa.gov; g.tinetti@ucl.ac.uk;
anger@phl.uni-koeln.de; yly@gps.caltech.edu
NR 2
TC 1
Z9 1
U1 0
U2 1
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-782-7
J9 ASTR SOC P
PY 2011
VL 450
BP 63
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAP07
UT WOS:000304974700007
ER
PT B
AU Lewis, NK
Showman, AP
Fortney, JJ
Marley, MS
Freedman, RS
AF Lewis, N. K.
Showman, A. P.
Fortney, J. J.
Marley, M. S.
Freedman, R. S.
BE Beaulieu, JP
Dieters, S
Tinetti, G
TI Atmospheric Dynamics of Two Eccentric Transiting Planets: GJ 436b and HD
17156b
SO MOLECULES IN THE ATMOSPHERES OF EXTRASOLAR PLANETS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Molecules in the Atmospheres of Extrasolar Planets
CY NOV 19-21, 2008
CL Observ Paris, Paris, FRANCE
HO Observ Paris
ID EXTRASOLAR PLANETS; TIDAL EVOLUTION; HOT JUPITERS; SPITZER
AB Extrasolar planets on eccentric orbits present a unique opportunity to study the effects of variable heating and non-synchronous rotation on the atmospheric dynamics of hot Jupiters and hot Neptunes. We present three-dimensional atmospheric circulation models that include realistic radiative transfer for two such extrasolar planets: GJ 436b (e=0.15) and HD17156b (e=0.67). GJ436b is one of the smallest transiting extrasolar planet known to date. Because of its size, it is likely to have an atmospheric composition more similar to Neptune (similar to 30x Solar), which has an effect on the radiative transfer and hence dynamics of the planet's atmosphere. HD17156b is a fairly massive Jupiter sized planet on a highly elliptical orbit. During its orbit, HD17156b passes through the radiative regime of both pM and pL Class planets as defined by Fortney et al. (2008), which makes it an ideal candidate to test the effects of TiO and VO in the atmospheres of extrasolar planets. We contrast the global circulation patterns and vertical thermal structures of these planets to those of HD189733b and HD209458b and postulate possible observational implications.
C1 [Lewis, N. K.; Showman, A. P.] Univ Arizona, Dept Planetary Sci, 1629 Univ Blvd, Tucson, AZ 85721 USA.
[Fortney, J. J.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marley, M. S.; Freedman, R. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lewis, NK (reprint author), Univ Arizona, Dept Planetary Sci, 1629 Univ Blvd, Tucson, AZ 85721 USA.
EM nlewis@lpl.arizona.edu; showman@lpl.arizona.edu;
freedman@darkstar.arc.nasa.gov
FU NASA Origins [NNX08AF27G]; NASA NESSF [NNX08AX02H]
FX This study was supported by NASA Origins grant NNX08AF27G and NASA NESSF
grant NNX08AX02H.
NR 19
TC 1
Z9 1
U1 1
U2 1
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-782-7
J9 ASTR SOC P
PY 2011
VL 450
BP 71
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAP07
UT WOS:000304974700008
ER
PT B
AU Serabyn, E
AF Serabyn, E.
BE Beaulieu, JP
Dieters, S
Tinetti, G
TI The Potential of High Contrast Coronagraphy
SO MOLECULES IN THE ATMOSPHERES OF EXTRASOLAR PLANETS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Molecules in the Atmospheres of Extrasolar Planets
CY NOV 19-21, 2008
CL Observ Paris, Paris, FRANCE
HO Observ Paris
ID PHASE-MASK CORONAGRAPH; EARTH-LIKE PLANETS; LABORATORY DEMONSTRATION;
EXTRASOLAR PLANET; ADAPTIVE OPTICS; APODIZATION; TELESCOPE
AB The direct detection of faint companions near much brighter stars requires the development of very high-contrast, small field-of-view detection techniques, and the past decade has seen remarkable conceptual and instrumental progress in this area. New coronagraphic techniques are being developed and deployed, as are extreme adaptive optics (ExAO) systems that will enable the advantageous exploitation of these new techniques. This paper provides a short overview of promising high contrast coronagraphic techniques, as well as recent examples of ExAO coronagraphy and transit measurements obtained with the ExAO-level "well-corrected subaperture" at Palomar.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Serabyn, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM gene.serabyn@jpl.nasa.gov
NR 26
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 978-1-58381-782-7
J9 ASTR SOC P
PY 2011
VL 450
BP 173
EP 180
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAP07
UT WOS:000304974700020
ER
PT B
AU Clampin, M
Kalas, P
Graham, J
Chiang, E
AF Clampin, Mark
Kalas, Paul
Graham, James
Chiang, Eugene
BE Beaulieu, JP
Dieters, S
Tinetti, G
TI Follow the Dust: Discovery of an Exosolar Planet in Fomalhaut's Debris
Disk
SO MOLECULES IN THE ATMOSPHERES OF EXTRASOLAR PLANETS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Molecules in the Atmospheres of Extrasolar Planets
CY NOV 19-21, 2008
CL Observ Paris, Paris, FRANCE
HO Observ Paris
ID CIRCUMSTELLAR DISK; SPECTRA; IMAGES; DYNAMICS; COLORS; BELT
AB Fomalhaut is one of the IRAS "big four" infrared excess stars. The debris disk is associated with the IR excess is resolved in the visible to sub-mm. It is an attractive target for an exoplanet search because the debris disk morphology is consistent with dynamical sculpting by one or more planets; it is a nearby (7.69 pc) star; and is relatively young (100 - 300 Myr) offering the possibility that any planets would still be radiating heat from their formation. We report here on an optical detection of an exoplanet candidate, Fomalhaut b. Fomalhaut b lies about 119 astronomical units (AU) from the star, and our observations separated by 1.73 years reveal counterclockwise orbital motion. Dynamical models of the interaction between the planet and the belt indicate that the planetos mass is at most three times that of Jupiter. The flux detected at 0.8 mu m is also consistent with that of a planet with mass no greater than a few times that of Jupiter. The brightness at 0.6 mu m and the lack of detection at longer wavelengths suggest that the detected flux may include starlight reflected off a circumplanetary disk, with dimension comparable to the orbits of the Galilean satellites.
C1 [Clampin, Mark] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
[Kalas, Paul; Graham, James; Chiang, Eugene] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Chiang, Eugene] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
RP Clampin, M (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
EM mark.clampin@nasa.gov
NR 21
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 978-1-58381-782-7
J9 ASTR SOC P
PY 2011
VL 450
BP 191
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAP07
UT WOS:000304974700022
ER
PT J
AU Galvan, DA
Komjathy, A
Song, YT
Stephens, P
Hickey, MP
Foster, J
AF Galvan, D. A.
Komjathy, A.
Song, Y. Tony
Stephens, P.
Hickey, M. P.
Foster, J.
GP ION
TI Observing Tsunamis in the Ionosphere Using Ground-Based GPS Measurements
SO PROCEEDINGS OF THE 24TH INTERNATIONAL TECHNICAL MEETING OF THE SATELLITE
DIVISION OF THE INSTITUTE OF NAVIGATION (ION GNSS 2011)
LA English
DT Proceedings Paper
CT 24th International Technical Meeting of the Satellite Division of the
Institute of Navigation (ION GNSS)
CY SEP 20-23, 2010
CL Portland, OR
SP Inst Navigat, Satellite Div
ID GRAVITY-WAVES; OSCILLATIONS; EARTHQUAKE
AB Ground-based Global Positioning System (GPS) measurements of ionospheric Total Electron Content (TEC) show variations consistent with atmospheric internal gravity waves caused by ocean tsunamis. We have observed such traveling ionospheric disturbances (TIDs) following recent seismic events, including the Tohoku tsunami of March 11, 2011. We analyze fluctuations correlated in time, space, and wave properties with this tsunami in TEC estimates processed using JPL's Global Ionospheric Mapping Software. The TEC estimates were band-pass filtered to remove ionospheric TEC variations with periods outside the typical range of internal gravity waves caused by tsunamis. Observable variations in TEC appear correlated with the Tohoku tsunami near the epicenter, at Hawaii, and near the west coast of North America. Disturbance magnitudes are 1-10% of the background TEC value. Observations near the epicenter are compared to estimates of expected tsunami-driven TEC variations produced by Embry Riddle Aeronautical University's Spectral Full Wave Model, an atmosphere-ionosphere coupling model, and found to be in good agreement. The potential exists to apply these detection techniques to real-time GPS TEC data, providing estimates of tsunami speed and amplitude that may be useful for future early warning systems.
C1 [Galvan, D. A.; Komjathy, A.; Song, Y. Tony; Stephens, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Galvan, DA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 24
TC 0
Z9 0
U1 0
U2 0
PU INST NAVIGATION
PI WASHINGTON
PA 815 15TH ST NW, STE 832, WASHINGTON, DC 20005 USA
PY 2011
BP 3172
EP 3182
PG 11
WC Computer Science, Hardware & Architecture; Telecommunications
SC Computer Science; Telecommunications
GA BAF73
UT WOS:000304032003024
ER
PT S
AU Blumberg, BS
AF Blumberg, Baruch S.
BE VallsGabaud, D
Boksenberg, A
TI Astronomical exploration and the public imagination
SO ROLE OF ASTRONOMY IN SOCIETY AND CULTURE
SE IAU Symposium Proceedings Series
LA English
DT Proceedings Paper
CT 260th Symposium of the International-Astronomical-Union
CY JAN 19-23, 2009
CL UNESCO, Paris, FRANCE
SP Observ Paris, Int Astronom Union, Acad Sci Paris, Inst Natl Sci Univ, Region Ile France
HO UNESCO
C1 [Blumberg, Baruch S.] NASA Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA 94035 USA.
EM Baruch.Blumberg@fccc.edu
NR 0
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 978-0-521-76477-3
J9 IAU SYMP P SERIES
JI IAU Symposium Proc. Series
PY 2011
IS 260
BP 9
EP 15
DI 10.1017/S1743921311002080
PG 7
WC Astronomy & Astrophysics; History & Philosophy Of Science; Social
Sciences, Interdisciplinary
SC Astronomy & Astrophysics; History & Philosophy of Science; Social
Sciences - Other Topics
GA BAM51
UT WOS:000304684000003
ER
PT B
AU Wahlgren, GM
Lebzelter, T
Wolff, B
AF Wahlgren, G. M.
Lebzelter, T.
Wolff, B.
BE Kerschbaum, F
Lebzelter, T
Wing, RF
TI The Carbon Isotope Ratio and Metallicity of YY Psc
SO WHY GALAXIES CARE ABOUT AGB STARS II: SHINING EXAMPLES AND COMMON
INHABITANTS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Why Galaxies Care About AGB Stars II: Shining Examples and
Common Inhabitants
CY AUG 16-20, 2010
CL Univ Campus, Vienna, AUSTRIA
HO Univ Campus
ID GIANTS
AB The chemical composition and carbon isotope ratio of the bright, giant star YY Psc (M3 III) are investigated from high resolution, high signal-to-noise spectra obtained with the ESO VLT/CRIRES instrument. The high-quality, sharp-lined spectrum was obtained as part of the ongoing CRIRES-POP observing program. The spectrum was analyzed using synthetic spectrum techniques, and a preliminary analysis shows that the C-12/C-13 ratio is similar to 10 and the iron abundance is consistent with the solar value.
C1 [Wahlgren, G. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wahlgren, G. M.] Catholic Univ Amer, Washington, DC 20064 USA.
[Lebzelter, T.] Univ Vienna, Vienna, Austria.
[Wolff, B.] European So Observ, Garching, Germany.
RP Wahlgren, GM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
FU NASA [NNG06GJ29G]
FX GMW acknowledge support from NASA grant NNG06GJ29G.
NR 4
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 978-1-58381-770-4
J9 ASTR SOC P
PY 2011
VL 445
BP 181
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAH05
UT WOS:000304132300036
ER
PT B
AU Gielen, C
Van Winckel, H
Min, M
Waters, R
Dominik, C
Evans, TL
Matsuura, M
Deroo, P
Cami, J
AF Gielen, C.
Van Winckel, H.
Min, M.
Waters, R.
Dominik, C.
Evans, T. Lloyd
Matsuura, M.
Deroo, P.
Cami, J.
CA SAGE-Spec Team
BE Kerschbaum, F
Lebzelter, T
Wing, RF
TI Stable Discs around Galactic and LMC Post-AGB Binaries
SO WHY GALAXIES CARE ABOUT AGB STARS II: SHINING EXAMPLES AND COMMON
INHABITANTS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Why Galaxies Care About AGB Stars II: Shining Examples and
Common Inhabitants
CY AUG 16-20, 2010
CL Univ Campus, Vienna, AUSTRIA
HO Univ Campus
ID LARGE-MAGELLANIC-CLOUD; CIRCUMBINARY DISC; SPITZER SURVEY; STARS; DUST;
DEPLETION; SAGE
AB The results of our study of a particular class of Galactic and extragalactic evolved stars, which are part of a binary system and surrounded by a stable dusty disc, are discussed. By combining spectroscopic, photometric and interferometric observations with detailed models describing dust properties and disc structure, we investigate the exact disc composition and structure.
C1 [Gielen, C.; Van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, Louvain, Belgium.
[Min, M.] Univ Utrecht, Astron Inst Utrecht, NL-3508 TC Utrecht, Netherlands.
[Waters, R.; Dominik, C.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1012 WX Amsterdam, Netherlands.
[Dominik, C.] Radbound Univ Nijmegen, Dept Astrophys, Nijmegen, Netherlands.
[Evans, T. Lloyd] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews, Fife, Scotland.
[Matsuura, M.] UCL, UCL Inst Origins, Dept Phys & Astron, London WC1E 6BT, England.
[Deroo, P.] Jet Propuls Lab, Pasadena, CA USA.
[Cami, J.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
RP Gielen, C (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Louvain, Belgium.
RI Van Winckel, Hans/I-7863-2013
OI Van Winckel, Hans/0000-0001-5158-9327
NR 17
TC 3
Z9 3
U1 0
U2 1
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-770-4
J9 ASTR SOC P
PY 2011
VL 445
BP 281
EP +
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAH05
UT WOS:000304132300053
ER
PT B
AU Norris, RP
Wahlgren, GM
Bruhweiler, FC
McCollum, B
AF Norris, R. P.
Wahlgren, G. M.
Bruhweiler, F. C.
McCollum, B.
BE Kerschbaum, F
Lebzelter, T
Wing, RF
TI The Infrared Variation of the Symbiotic Star BI Cru
SO WHY GALAXIES CARE ABOUT AGB STARS II: SHINING EXAMPLES AND COMMON
INHABITANTS
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Why Galaxies Care About AGB Stars II: Shining Examples and
Common Inhabitants
CY AUG 16-20, 2010
CL Univ Campus, Vienna, AUSTRIA
HO Univ Campus
ID SPITZER-SPACE-TELESCOPE; MISSION
AB We have obtained observations of six symbiotic stars with Spitzer MIPS (photometery at 24 mu m and 70 mu m) and IRS (spectroscopic range 9.9-37.2 mu m). Here we report the presence of 10 mu m and 18 mu m dust features in one of these stars, BI Cru, which were not observed in ISO spectra of the same system.
C1 [Norris, R. P.; Wahlgren, G. M.; Bruhweiler, F. C.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wahlgren, G. M.; Bruhweiler, F. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[McCollum, B.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Norris, RP (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
NR 7
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 978-1-58381-770-4
J9 ASTR SOC P
PY 2011
VL 445
BP 359
EP +
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAH05
UT WOS:000304132300080
ER
PT B
AU Barnes, R
Meadows, VS
Domagal-Goldman, SD
Heller, R
Jackson, B
Lopez-Morales, M
Tanner, A
Gomez-Perez, N
Ruedas, T
AF Barnes, Rory
Meadows, Victoria S.
Domagal-Goldman, Shawn D.
Heller, Rene
Jackson, Brian
Lopez-Morales, Mercedes
Tanner, Angelle
Gomez-Perez, Natalia
Ruedas, Thomas
BE JohnsKrull, CMJ
Browning, MK
West, AA
TI Habitability of Planets Orbiting Cool Stars
SO 16TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 16th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun
CY AUG 28-SEP 03, 2010
CL Univ Washington, Seattle, WA
SP Natl Sci Fdn, NASA Astrobiol Inst, European Space Agcy, Astrophys Res Consortium/Apache Point Observ, Univ Washington Coll Arts & Sci, Univ Washington Dept Astron
HO Univ Washington
ID EARTH-LIKE PLANETS; LOW-MASS STARS; GIANT PLANETS; TERRESTRIAL PLANETS;
TIDAL EVOLUTION; MAIN-SEQUENCE; M-DWARFS; ATMOSPHERE; BIOSIGNATURES;
EVAPORATION
AB Terrestrial planets are more likely to be detected if they orbit M dwarfs due to the favorable planet/star size and mass ratios. However, M dwarf habitable zones are significantly closer to the star than the one around our Sun, which leads to different requirements for planetary habitability and its detection. We review 1) the current limits to detection, 2) the role of M dwarf spectral energy distributions on atmospheric chemistry, 3) tidal effects, stressing that tidal locking is not synonymous with synchronous rotation, 4) the role of atmospheric mass loss and propose that some habitable worlds may be the volatile-rich, evaporated cores of giant planets, and 5) the role of planetary rotation and magnetic field generation, emphasizing that slow rotation does not preclude strong magnetic fields and their shielding of the surface from stellar activity. Finally we present preliminary findings of the NASA Astrobiology Institute's workshop "Revisiting the Habitable Zone." We assess the recently-announced planet G1 581 g and find no obvious barriers to habitability. We conclude that no known phenomenon completely precludes the habitability of terrestrial planets orbiting cool stars.
C1 [Barnes, Rory; Meadows, Victoria S.] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
[Barnes, Rory; Meadows, Victoria S.; Domagal-Goldman, Shawn D.] Virtual Planetary Lab, Seattle, WA 98195 USA.
[Domagal-Goldman, Shawn D.] NASA Headquarters, Planetary Sci Div, Washington, DC USA.
[Domagal-Goldman, Shawn D.] NASA, Washington, DC USA.
[Heller, Rene] Astrophys Inst Postdam AIP, D-14482 Potsdam, Germany.
[Jackson, Brian] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lopez-Morales, Mercedes] CSIC, IEEC, Inst Ciencies Lespai, Fac Ciencies, E-08193 Barcelona, Spain.
[Lopez-Morales, Mercedes; Gomez-Perez, Natalia; Ruedas, Thomas] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Tanner, Angelle] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
[Gomez-Perez, Natalia] Univ Los Andes, Dept Fis, Bogota, Colombia.
RP Barnes, R (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
RI Domagal-Goldman, Shawn/F-3521-2012
OI Domagal-Goldman, Shawn/0000-0003-0354-9325
NR 53
TC 2
Z9 2
U1 1
U2 2
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-776-6
J9 ASTR SOC P
PY 2011
VL 448
BP 391
EP +
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAK14
UT WOS:000304381600040
ER
PT B
AU Covey, KR
Plavchan, P
Bastien, F
Flaccomio, E
Flaherty, K
Marsden, S
Morales-Calderon, M
Muzerolle, J
Turner, NJ
AF Covey, Kevin R.
Plavchan, Peter
Bastien, Fabienne
Flaccomio, Ettore
Flaherty, Kevin
Marsden, Stephen
Morales-Calderon, Maria
Muzerolle, James
Turner, Neal J.
BE JohnsKrull, CMJ
Browning, MK
West, AA
TI Young Stars in the Time Domain: A CS16 Splinter Summary
SO 16TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 16th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun
CY AUG 28-SEP 03, 2010
CL Univ Washington, Seattle, WA
SP Natl Sci Fdn, NASA Astrobiol Inst, European Space Agcy, Astrophys Res Consortium/Apache Point Observ, Univ Washington Coll Arts & Sci, Univ Washington Dept Astron
HO Univ Washington
ID T-TAURI STARS; ORION NEBULA CLUSTER; X-RAY VARIABILITY; LOW-MASS STARS;
SURFACE DIFFERENTIAL ROTATION; SEQUENCE ECLIPSING BINARY; MIDINFRARED
VARIABILITY; ACTIVE STARS; BROWN DWARFS; ACCRETION
AB Variability is a defining characteristic of young stellar systems, and optical variability has been heavily studied to select and characterize the photospheric properties of young stars. In recent years, multi-epoch observations sampling a wider range of wavelengths and time-scales have revealed a wealth of time-variable phenomena at work during the star formation process. This splinter session was convened to summarize recent progress in providing improved coverage and understanding of time-variable processes in young stars and circumstellar disks. We begin by summarizing results from several multi-epoch Spitzer campaigns, which have demonstrated that many young stellar objects evidence significant mid-IR variability. While some of these variations can be attributed to processes in the stellar photosphere, others appear to trace short time-scale changes in the circumstellar disk which can be successfully modeled with axisymmetric or non-axisymmetric structures. We also review recent studies probing variability at shorter wavelengths that provide evidence for high frequency pulsations associated with accretion outbursts, correlated optical/X-ray variability in Classical T Tauri stars, and magnetic reversals in young solar analogs.
C1 [Covey, Kevin R.] Cornell Univ, Dept Astron, 226 Space Sci Bldg, Ithaca, NY 14853 USA.
[Covey, Kevin R.] Boston Univ, Dept Astron, Visiting Res, Boston, MA 02215 USA.
[Plavchan, Peter] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Bastien, Fabienne] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Flaccomio, Ettore] Inaf, Observ Astron Palermo, Piazza Paralamento, I-90134 Palermo, Italy.
[Flaherty, Kevin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Marsden, Stephen] James Cook Univ, Sch Engn & Phys Sci, Ctr Astron, Townsville, Qld 4811, Australia.
[Morales-Calderon, Maria] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Muzerolle, James] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Covey, KR (reprint author), Cornell Univ, Dept Astron, 226 Space Sci Bldg, Ithaca, NY 14853 USA.
RI Morales-Calderon, Maria/C-8384-2017
OI Morales-Calderon, Maria/0000-0001-9526-9499
NR 58
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 978-1-58381-776-6
J9 ASTR SOC P
PY 2011
VL 448
BP 415
EP +
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAK14
UT WOS:000304381600042
ER
PT B
AU Deacon, NR
Pinfield, DJ
Lucas, PW
Liu, MC
Bessell, MS
Burningham, B
Cushing, MC
Day-Jones, AC
Dhital, S
Law, NM
Mainzer, AK
Zhang, ZH
AF Deacon, N. R.
Pinfield, D. J.
Lucas, P. W.
Liu, Michael C.
Bessell, M. S.
Burningham, B.
Cushing, M. C.
Day-Jones, A. C.
Dhital, S.
Law, N. M.
Mainzer, A. K.
Zhang, Z. H.
BE JohnsKrull, CMJ
Browning, MK
West, AA
TI Ultracool Dwarf Science from Widefield Multi-Epoch Surveys
SO 16TH CAMBRIDGE WORKSHOP ON COOL STARS, STELLAR SYSTEMS AND THE SUN
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 16th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun
CY AUG 28-SEP 03, 2010
CL Univ Washington, Seattle, WA
SP Natl Sci Fdn, NASA Astrobiol Inst, European Space Agcy, Astrophys Res Consortium/Apache Point Observ, Univ Washington Coll Arts & Sci, Univ Washington Dept Astron
HO Univ Washington
ID DIGITAL SKY SURVEY; INITIAL MASS FUNCTION; PROPER MOTION SURVEY;
T-DWARFS; BROWN DWARF; SURVEY 2MASS; USNO-B; UKIDSS; DISCOVERIES;
CATALOG
AB Widefield surveys have always provided a rich hunting ground for the coolest stars and brown dwarfs. The single epoch surveys at the beginning of this century greatly expanded the parameter space for ultracool dwarfs. Here we outline the science possible from new multi-epoch surveys which add extra depth and open the time domain to study.
C1 [Deacon, N. R.; Liu, Michael C.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Pinfield, D. J.; Lucas, P. W.; Burningham, B.; Zhang, Z. H.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Bessell, M. S.] Res Sch Astron & Astrophys, Mount Stromlo Observ, Weston, ACT 2611, Australia.
[Cushing, M. C.; Mainzer, A. K.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Day-Jones, A. C.] Univ Chile, Camino Observ, Santiago 1515, Chile.
[Dhital, S.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Law, N. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Deacon, NR (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
NR 39
TC 1
Z9 1
U1 0
U2 1
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-776-6
J9 ASTR SOC P
PY 2011
VL 448
BP 429
EP +
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BAK14
UT WOS:000304381600043
ER
PT B
AU Kletetschka, G
AF Kletetschka, Gunther
BE Petrovsky, E
HerreroBervera, E
Harinarayana, T
Ivers, D
TI Magnetic Measurements on Maple and Sequoia Trees
SO EARTH'S MAGNETIC INTERIOR
SE IAGA Special Sopron Book Series
LA English
DT Article; Book Chapter
ID PINE PINUS-LONGAEVA; TELOMERASE ACTIVITY; FOREST SOILS; POWER-PLANT;
LIFE-SPANS; FLY-ASH; CONTAMINATION; ANOMALIES; POLLUTION; RECORD
AB Magnetic measurements of soil and tree bark adjacent to a busy highway revealed a significant variation in the concentration of magnetic particles with distance from the highway. Furthermore, forest-facing tree-bark contains significantly more magnetic particles than road-facing tree-bark. Magnetic particles were detected both on the bark of the maple trees and in the first centimeter of the soil cover (O/A horizon). Stability of the Saturation Isothermal Magnetization (SIRM) and the hysteresis parameters of the soil indicates the presence of Single-Domain/Pseudo-Single-Domain (SD/PSD) magnetic carriers. Measurements of the tree bark hysteresis parameters and SIRM detect a significantly lower coercivity component that we interpret to be an indication of more abundant PSD-type magnetic grains. Magnetic measurements around the perimeters of eight tree trunks reveal magnetic carriers whose distribution is antipodal to the source direction (highway). We interpret our observation by adopting an air circulation model, where suspended PSD/SD particles are carried in the air stream. The air stream from the heavy traffic lowers the amount of moisture on the tree trunk surfaces facing the highway and thus reduces an adhesive potential on this side. Therefore, more particles can stay on the moist side of the trunk protected from the direct airflow. A magnetic signature of tree rings was tested as a potential paleo-climatic indicator. We have examined wood from sequoia tree, located in Mountain Home State Forest, California, whose tree ring record spans over the period 600-1700 A.D. We have measured low and high-field magnetic susceptibility, the Natural Remanent Magnetization (NRM), Saturation Isothermal Remanent Magnetization (SIRM), and stability against thermal and Alternating Field (AF) demagnetization. Magnetic investigation of the 200 mm long sequoia material suggests that the magnetic efficiency of natural remanence (=natural remanent magnetization normalized by saturation remanence) may be a sensitive paleoclimate indicator because it is substantially higher (in average >0.01 = 1%) during the Medieval Warm Epoch (700-1300 A.D.) than during the Little Ice Age (1300-1850 A.D.) where it is <0.01 = 1%. Diamagnetic behavior has been noted to be prevalent in regions with higher tree ring density. The mineralogical nature of the remanence carrier was not directly detected but maghemite is suggested due to low coercivity and absence of Verwey transition. Tree ring density, along with the wood's magnetic remanence efficiency, records the Little Ice Age (LIA), which is well documented in Europe and elsewhere. Magnetic analysis of the thermal stability reveals the blocking temperatures near 200 degrees C. This phenomenon suggests that the remanent component in this tree may be thermal in origin and was controlled by local thermal conditions.
C1 [Kletetschka, Gunther] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Kletetschka, Gunther] Catholic Univ Amer, Washington, DC 20064 USA.
[Kletetschka, Gunther] Acad Sci Czech Republic, Inst Geol, Prague, Czech Republic.
RP Kletetschka, G (reprint author), NASA, Goddard Space Flight Ctr, Code 691, Greenbelt, MD USA.
EM gunther.kletetschka@gsfc.nasa.gov
RI Kletetschka, Gunther/C-9996-2011
OI Kletetschka, Gunther/0000-0002-0645-9037
NR 32
TC 0
Z9 0
U1 0
U2 12
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
BN 978-94-007-0322-3
J9 IAGA SPEC SOPRON
PY 2011
VL 1
BP 427
EP 441
DI 10.1007/978-94-007-0323-0_28
D2 10.1007/978-94-007-0323-0
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA BYW50
UT WOS:000300642800028
ER
PT S
AU Ambrosia, VG
Sullivan, DV
Buechel, SW
AF Ambrosia, Vincent G.
Sullivan, Donald V.
Buechel, Sally W.
BE Sinha, AK
Arctur, D
Jackson, I
Gundersen, LC
TI Integrating sensor data and geospatial tools to enhance real-time
disaster management capabilities: Wildfire observations
SO SOCIETAL CHALLENGES AND GEOINFORMATICS
SE Geological Society of America Special Papers
LA English
DT Article; Book Chapter
ID BOREAL FOREST-FIRES; ALGORITHM
AB The primary factors needed to manage disaster events are time-critical geospatial information on the event occurrence and presentation of that information in an easily manageable, collaborative/interactive geospatial decision-support and visualization environment. In this chapter, we describe the development, integration, and use of an unmanned airborne system (UAS), a multispectral sensor with autonomous onboard processing capabilities, a data distribution system, and geospatial processes to deliver real-time information to emergency incident management teams facing wildland fires. The unique integration of the described tools has contributed to an order of magnitude decrease in the delivery time of critical geospatial information to disaster managers. The UAS wildfire imaging campaigns in the western United States in 2007 and 2008 are briefly described in the context of real-world adaptation and utility of the resultant information improvements. These capabilities have far-reaching applications to other time-critical, disaster event management scenarios, and they are being expanded to further utilize various UAS platforms and other airborne sensor system data. This chapter will also describe the resultant integration issues faced and the solutions for ubiquitous adaptation of many of these processes in future UAS missions.
C1 [Ambrosia, Vincent G.] Calif State Univ Monterey Bay, Seaside, CA 93955 USA.
[Ambrosia, Vincent G.; Sullivan, Donald V.; Buechel, Sally W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ambrosia, VG (reprint author), Calif State Univ Monterey Bay, Seaside, CA 93955 USA.
NR 6
TC 2
Z9 2
U1 0
U2 1
PU GEOLOGICAL SOC AMER INC
PI BOULDER
PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA
SN 0072-1077
BN 978-0-8137-2482-9
J9 GEOL SOC AM SPEC PAP
PY 2011
VL 482
BP 1
EP 12
DI 10.1130/2011.2482(01)
D2 10.1130/9780813724829
PG 12
WC Geology
SC Geology
GA BYW18
UT WOS:000300632500002
ER
PT B
AU Barbier, SB
Bartolone, L
Christian, E
Thieman, J
Eastman, T
Lewis, E
AF Barbier, S. Beth
Bartolone, Lindsay
Christian, Eric
Thieman, James
Eastman, Timothy
Lewis, Elaine
BE Jensen, JB
Manning, JG
Gibbs, MG
TI Extraordinary Matter: Visualizing Space Plasmas and Particles
SO EARTH AND SPACE SCIENCE: MAKING CONNECTIONS IN EDUCATION AND PUBLIC
OUTREACH
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 122nd Annual Meeting of the Astronomical Society of the Pacific (ASP)
CY JUL 31-AUG 04, 2010
CL Geolog Soc Amer, Boulder, CO
SP NASA Lunar Sci Inst, IPAC, NASA Herschel Sci Ctr, Spitzer Sci Ctr, WH Freeman & Co, Collaborat Astron Teach Scholars, Ctr Astron Educ, Sky Skan, NASA, NRAO, Stratopher Observ Infrared Astron, Planck, Univ Chicago Press, I Clicker, Aerospace, Capitol Coll, CAPER Team, AAS, Windows Universe, Seiler, Celestron, Explore Sci, MWT Assoc Inc, Boulder Beer
HO Geolog Soc Amer
AB Atoms and sub-atomic particles play a crucial role in the dynamics of our universe, but these particles and the space plasmas comprised of them are often overlooked in popular scientific and educational resources. Although the concepts are pertinent to a wide range of topics, even the most basic particle and plasma physics principles axe generally unfamiliar to non-scientists. Educators and public communicators need assistance in explaining these concepts that cannot be easily demonstrated in the everyday world. Active visuals are a highly effective aid to understanding, but resources of this type are currently few in number and difficult to find, and most do not provide suitable context for audience comprehension. To address this need, our team is developing an online multimedia reference library of animations, visualizations, interactivities, and videos resources Extraordinary Matter: Visualizing Space Plasmas and Particles. The site targets grades 9-14 and the equivalent in informal education and public outreach. Each ready-to-use product will be accompanied by a supporting explanation at a reading level matching the educational level of the concept. It will also have information on relevant science, technology, engineering, and mathematics (STEM) educational standards, activities, lesson plans, related products, links, and suggested uses. These products are intended to stand alone, making them adaptable to the widest range of uses, including scientist presentations, museum displays, educational websites and CDs, teacher professional development, and classroom use. This project is funded by a NASA Education and Public Outreach in Earth and Space Science (EPOESS) grant.
C1 [Barbier, S. Beth] SP Syst Inc, Greenbelt, MD 20770 USA.
[Bartolone, Lindsay] Adler Planetarium, Chicago, IL USA.
[Christian, Eric; Thieman, James] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Eastman, Timothy] Wyle Informat Syst LLC, Mclean, VA USA.
[Lewis, Elaine] Honeywell Technol Solut Inc, Columbia, MD USA.
RP Barbier, SB (reprint author), SP Syst Inc, Greenbelt, MD 20770 USA.
RI Christian, Eric/D-4974-2012
OI Christian, Eric/0000-0003-2134-3937
NR 2
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 978-1-58381-766-7
J9 ASTR SOC P
PY 2011
VL 443
BP 211
EP +
PG 2
WC Astronomy & Astrophysics; Education, Scientific Disciplines
SC Astronomy & Astrophysics; Education & Educational Research
GA BAH68
UT WOS:000304180400039
ER
PT B
AU Sharma, M
Mendoza, D
Smith, D
Hasan, H
AF Sharma, Mangala
Mendoza, Darlene
Smith, Denise
Hasan, Hashima
CA NASA SMD Astrophys EPO Community
BE Jensen, JB
Manning, JG
Gibbs, MG
TI NASA Astrophysics EPO Resources For Engaging Girls in Science
SO EARTH AND SPACE SCIENCE: MAKING CONNECTIONS IN EDUCATION AND PUBLIC
OUTREACH
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 122nd Annual Meeting of the Astronomical Society of the Pacific (ASP)
CY JUL 31-AUG 04, 2010
CL Geolog Soc Amer, Boulder, CO
SP NASA Lunar Sci Inst, IPAC, NASA Herschel Sci Ctr, Spitzer Sci Ctr, WH Freeman & Co, Collaborat Astron Teach Scholars, Ctr Astron Educ, Sky Skan, NASA, NRAO, Stratopher Observ Infrared Astron, Planck, Univ Chicago Press, I Clicker, Aerospace, Capitol Coll, CAPER Team, AAS, Windows Universe, Seiler, Celestron, Explore Sci, MWT Assoc Inc, Boulder Beer
HO Geolog Soc Amer
AB A new collaboration among the NASA Science Mission Directorate (SMD) Astrophysics EPO community is to engage girls in science who do not self-select as being interested in science, through the library setting. The collaboration seeks to (i) improve how girls view themselves as someone who knows about, uses, and sometimes contributes to science, and (ii) increase the capacity of EPO practitioners and librarians (both school and public) to engage girls in science. As part of this collaboration, we are collating the research on audience needs and best practices, and SMD EPO resources, activities and projects that focus on or can be recast toward engaging girls in science. This ASP article highlights several available resources and individual projects, such as: (i) Afterschool Universe, an out-of-school hands-on astronomy curriculum targeted at middle school students and an approved Great Science for Girls curriculum; (ii) Big Explosions and Strong Gravity, a Girl Scout patch-earning event for middle school aged girls to learn astronomy through hands-on activities and interaction with actual astronomers; and (iii) the JWST-NIRCAM Train the Trainer workshops and activities for Girl Scouts of USA leaders; etc.
The NASA Astrophysics EPO community welcomes the broader EPO community to discuss with us how best to engage non-science-attentive girls in science, technology, engineering, and mathematics (STEM), and to explore further collaborations on this theme.
C1 [Sharma, Mangala; Smith, Denise] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Mendoza, Darlene] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hasan, Hashima] NASA, Washington, DC 20546 USA.
RP Sharma, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
NR 2
TC 0
Z9 0
U1 0
U2 2
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-766-7
J9 ASTR SOC P
PY 2011
VL 443
BP 320
EP 322
PG 3
WC Astronomy & Astrophysics; Education, Scientific Disciplines
SC Astronomy & Astrophysics; Education & Educational Research
GA BAH68
UT WOS:000304180400065
ER
PT B
AU Littleton, A
Wolt, A
Glass, M
AF Littleton, Aleya
Wolt, Andrew
Glass, Margaret
BE Jensen, JB
Manning, JG
Gibbs, MG
TI SDOisGO: Using Social Media to Create Community
SO EARTH AND SPACE SCIENCE: MAKING CONNECTIONS IN EDUCATION AND PUBLIC
OUTREACH
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 122nd Annual Meeting of the Astronomical Society of the Pacific (ASP)
CY JUL 31-AUG 04, 2010
CL Geolog Soc Amer, Boulder, CO
SP NASA Lunar Sci Inst, IPAC, NASA Herschel Sci Ctr, Spitzer Sci Ctr, WH Freeman & Co, Collaborat Astron Teach Scholars, Ctr Astron Educ, Sky Skan, NASA, NRAO, Stratopher Observ Infrared Astron, Planck, Univ Chicago Press, I Clicker, Aerospace, Capitol Coll, CAPER Team, AAS, Windows Universe, Seiler, Celestron, Explore Sci, MWT Assoc Inc, Boulder Beer
HO Geolog Soc Amer
AB Twitter, the newest wave in social media, redefines our understanding of community. No longer are people confined by geography, but rather communities are formed through individuals seeking out others of like mind, creating groups with common beliefs and interests without the constraints of distance. NASA has begun hosting "tweetups," or meet-ups of twitter followers interested in NASA and space. The initial tweetups were based purely on gathering in a single location and sharing a unique experience. By taking the approach that tweetups should not be limited by location, the SDO team was able to include and inspire a larger community of space enthusiasts and newcomers than were able to be present at the launch and first light events.
C1 [Littleton, Aleya; Glass, Margaret] NASA, ADNET Syst Inc, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Wolt, Andrew] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20117 USA.
RP Littleton, A (reprint author), NASA, ADNET Syst Inc, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM Aleya.vandoren@nasa.gov; Andrew.wolt@nasa.gov; Emilie.Drobnes@nasa.gov
NR 0
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 978-1-58381-766-7
J9 ASTR SOC P
PY 2011
VL 443
BP 336
EP +
PG 3
WC Astronomy & Astrophysics; Education, Scientific Disciplines
SC Astronomy & Astrophysics; Education & Educational Research
GA BAH68
UT WOS:000304180400069
ER
PT B
AU Lochner, JC
Mattson, BJ
AF Lochner, James C.
Mattson, Barbara J.
BE Jensen, JB
Manning, JG
Gibbs, MG
TI Uncovering the Stories Behind the Science: Infusing Astro 101 with the
History of Modern Cosmology
SO EARTH AND SPACE SCIENCE: MAKING CONNECTIONS IN EDUCATION AND PUBLIC
OUTREACH
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 122nd Annual Meeting of the Astronomical Society of the Pacific (ASP)
CY JUL 31-AUG 04, 2010
CL Geolog Soc Amer, Boulder, CO
SP NASA Lunar Sci Inst, IPAC, NASA Herschel Sci Ctr, Spitzer Sci Ctr, WH Freeman & Co, Collaborat Astron Teach Scholars, Ctr Astron Educ, Sky Skan, NASA, NRAO, Stratopher Observ Infrared Astron, Planck, UnivChicago Press, I Clicker, Aerospace, Capitol Coll, CAPER Team, AAS, Windows Universe, Seiler, Celestron, Explore Sci, MWT Assoc Inc, Boulder Beer
HO Geolog Soc Amer
AB Utilizing the history of discoveries enhances students' understanding of science and the nature of science. We have incorporated the history of modern cosmology into the context of a variety of topics taught in upper-level high school and Astro 101 courses through Cosmic Times, a suite of curriculum support materials. We describe here these materials and their applications to two specific examples of topics taught in Astro 101.
C1 [Lochner, James C.; Mattson, Barbara J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Lochner, JC (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
NR 2
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 978-1-58381-766-7
J9 ASTR SOC P
PY 2011
VL 443
BP 458
EP 461
PG 4
WC Astronomy & Astrophysics; Education, Scientific Disciplines
SC Astronomy & Astrophysics; Education & Educational Research
GA BAH68
UT WOS:000304180400091
ER
PT B
AU Yee, HC
Sjogreen, B
Hadjadj, A
AF Yee, H. C.
Sjoegreen, B.
Hadjadj, A.
BE Pogorelov, NV
Audit, E
Zank, GP
TI LES of Temporally Evolving Mixing Layers by Three High Order Schemes
SO NUMERICAL MODELING OF SPACE PLASMA FLOWS - ASTRONUM 2010
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT 5th Annual International Conference on Numerical Modeling of Space
Plasma Flows (ASTRONUM 2010)
CY JUN 13-18, 2010
CL San Diego, CA
ID COMPRESSIBLE TURBULENCE; NUMERICAL DISSIPATION; DIRECT SIMULATION
AB The performance of three high order shock-capturing schemes is compared for large eddy simulations (LES) of temporally evolving mixing layers for different convective Mach number (M-e) ranging from the quasi-incompressible regime to highly compressible supersonic regime. The considered high order schemes are fifth-order WENO (WENO5), seventh-order WENO (WENO7), and the associated eighth-order central spatial base scheme with the dissipative portion of WENO7 as a nonlinear post-processing filter step (WENO7fi). This high order nonlinear filter method (Yee & Sjogreen 2009) is designed for accurate and efficient simulations of shock-free compressible turbulence, turbulence with shocklets and turbulence with strong shocks with minimum tuning of scheme parameters. The LES results by WENO7fi using the same scheme parameter agree well with experimental results of Barone et al. (2006), and published direct numerical simulations (DNS) by Rogers & Moser (1994) and Pantano & Sarkar (2002), whereas results by WENO5 and WENO7 compare poorly with experimental data and DNS computations.
C1 [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sjoegreen, B.] Lawrence Livemore Natl Lab, Livermore, CA 94551 USA.
[Hadjadj, A.] CORIA, UMR 6614, INSA Rouen, F-76800 St Etienne, France.
RP Yee, HC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
NR 27
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 978-1-58381-768-1
J9 ASTR SOC P
PY 2011
VL 444
BP 266
EP +
PG 3
WC Astronomy & Astrophysics; Mathematics, Applied
SC Astronomy & Astrophysics; Mathematics
GA BAH66
UT WOS:000304180200041
ER
PT J
AU Treleaven, K
Pavone, M
Frazzoli, E
AF Treleaven, Kyle
Pavone, Marco
Frazzoli, Emilio
GP IEEE
TI An Asymptotically Optimal Algorithm for Pickup and Delivery Problems
SO 2011 50TH IEEE CONFERENCE ON DECISION AND CONTROL AND EUROPEAN CONTROL
CONFERENCE (CDC-ECC)
LA English
DT Proceedings Paper
CT 50th IEEE Conference of Decision and Control (CDC)/European Control
Conference (ECC)
CY DEC 12-15, 2011
CL Orlando, FL
SP Honeywell, MathWorks, United Technol Res Ctr, HYCON2, IEEE, Contrl Syst Soc (CSS), EUCA
ID TREE
AB Pickup and delivery problems (PDPs), in which objects or people have to be transported between specific locations, are among the most common combinatorial problems in real-world operations. One particular PDP is the Stacker Crane problem (SCP), where each commodity/customer is associated with a pickup location and a delivery location, and the objective is to find a minimum-length tour visiting all locations with the constraint that each pickup location and its associated delivery location are visited in consecutive order. The SCP is a route optimization problem behind several transportation systems, e.g., Transportation-On-Demand (TOD) systems. The SCP is NP-Hard and the best know approximation algorithm only provides a 9/5 approximation ratio. We present an algorithm for the stochastic SCP which: (i) is asymptotically optimal, i. e., it produces a solution approaching the optimal one as the number of pickups/deliveries goes to infinity; and (ii) has computational complexity O(n(2+epsilon)), where n is the number of pickup/delivery pairs and epsilon is an arbitrarily small positive constant. Our results leverage a novel connection between the Euclidean Bipartite Matching Problem and the theory of random permutations.
C1 [Treleaven, Kyle; Frazzoli, Emilio] MIT, Dept Aeronaut & Astronaut, Lab Informat & Decis Syst, Cambridge, MA 02139 USA.
[Pavone, Marco] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Treleaven, K (reprint author), MIT, Dept Aeronaut & Astronaut, Lab Informat & Decis Syst, Cambridge, MA 02139 USA.
EM ktreleav@mit.edu; marco.pavone@jpl.nasa.gov; frazzoli@mit.edu
FU Future Urban Mobility project of the Singapore-MIT Alliance for Research
and Technology (SMART) Center; Singapores National Research Foundation
FX This research was supported in part by the Future Urban Mobility project
of the Singapore-MIT Alliance for Research and Technology (SMART)
Center, with funding from Singapores National Research Foundation.
NR 12
TC 1
Z9 1
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-61284-801-3
PY 2011
BP 584
EP 590
PG 7
WC Automation & Control Systems
SC Automation & Control Systems
GA BAA55
UT WOS:000303506201029
ER
PT J
AU Morozov, AV
Ali, AA
D'Amato, AM
Ridley, AJ
Kukreja, SL
Bernstein, DS
AF Morozov, Alexey V.
Ali, Asad A.
D'Amato, Anthony M.
Ridley, Aaron J.
Kukreja, Sunil L.
Bernstein, Dennis S.
GP IEEE
TI Retrospective-Cost-Based Model Refinement for System Emulation and
Subsystem Identification
SO 2011 50TH IEEE CONFERENCE ON DECISION AND CONTROL AND EUROPEAN CONTROL
CONFERENCE (CDC-ECC)
LA English
DT Proceedings Paper
CT 50th IEEE Conference of Decision and Control (CDC)/European Control
Conference (ECC)
CY DEC 12-15, 2011
CL Orlando, FL
SP Honeywell, MathWorks, United Technol Res Ctr, HYCON2, IEEE, Contrl Syst Soc (CSS), EUCA
AB We consider the problem of data-based model refinement, where we assume the availability of an initial model, which may incorporate both physical laws and empirical observations. With this initial model as a starting point, our goal is to use additional measurements to refine the model. In particular, components of the model that are poorly modeled can be updated, thereby resulting in a higher fidelity model. We consider two special cases, namely, system emulation and subsystem identification. In the former case, the main system is assumed to be uncertain and we seek an estimate of the unknown subsystem that allows the overall model to approximate the true system. In this case, there is no expectation that the constructed subsystem model approximates the unknown subsystem. In the latter case, we assume that the main system is accurately modeled and we seek an estimate of the unknown subsystem that approximates the unknown subsystem.
C1 [Morozov, Alexey V.; Ali, Asad A.; D'Amato, Anthony M.; Bernstein, Dennis S.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
[Ridley, Aaron J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI USA.
[Kukreja, Sunil L.] NASA Dryden Flight Res Ctr, Struct Dynam Grp, Edwards AFB, CA USA.
RP Morozov, AV (reprint author), Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
EM morozova@umich.edu; asadali@umich.edu; amdamato@umich.edu;
ridley@umich.edu; sunil.l.kukreja@nasa.gov; dsbaero@umich.edu
RI Ridley, Aaron/F-3943-2011
OI Ridley, Aaron/0000-0001-6933-8534
FU NASA GSRP; NASA [NNX09AO55H, NNX0BA57A]; NSF [CDI-1027192, CNS-103523]
FX This work was supported in part by NASA GSRP, NASA grants NNX09AO55H and
NNX0BA57A, and NSF grants CDI-1027192 and CNS-103523
NR 10
TC 4
Z9 4
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-61284-801-3
PY 2011
BP 2142
EP 2147
PG 6
WC Automation & Control Systems
SC Automation & Control Systems
GA BAA55
UT WOS:000303506202122
ER
PT J
AU Bloem, M
Bambos, N
AF Bloem, Michael
Bambos, Nicholas
GP IEEE
TI Coordinated Tactical Air Traffic and Airspace Management
SO 2011 50TH IEEE CONFERENCE ON DECISION AND CONTROL AND EUROPEAN CONTROL
CONFERENCE (CDC-ECC)
LA English
DT Proceedings Paper
CT 50th IEEE Conference of Decision and Control (CDC)/European Control
Conference (ECC)
CY DEC 12-15, 2011
CL Orlando, FL
SP Honeywell, MathWorks, United Technol Res Ctr, HYCON2, IEEE, Contrl Syst Soc (CSS), EUCA
AB Air traffic management and airspace management reduce air traffic congestion to maintain safety. Managing traffic induces costs on airspace users and managing airspace causes additional work for air traffic controllers. This paper proposes and simulates algorithms for tactically reducing airspace congestion with coordinated air traffic and airspace management. A modified version of the Projective Cone Scheduling algorithm performs tactical air traffic management. An algorithm based on approximate dynamic programming accomplishes tactical airspace management. Three types of coordination between these air traffic and airspace management algorithms are investigated. Monte Carlo simulations of a simple problem instance involving severe congestion indicate that increased coordination between air traffic and airspace management can lead to lower costs with no increase in algorithm computation time.
C1 [Bloem, Michael] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bambos, Nicholas] Stanford Univ, Stanford, CA 94305 USA.
RP Bloem, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM michael.bloem@nasa.gov; bambos@stanford.edu
NR 20
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-61284-801-3
PY 2011
BP 5287
EP 5292
PG 6
WC Automation & Control Systems
SC Automation & Control Systems
GA BAA55
UT WOS:000303506205147
ER
PT J
AU Stepanyan, V
Krishnakumar, K
AF Stepanyan, Vahram
Krishnakumar, Kalmanje
GP IEEE
TI M-MRAC for Nonlinear Systems with Bounded Disturbances
SO 2011 50TH IEEE CONFERENCE ON DECISION AND CONTROL AND EUROPEAN CONTROL
CONFERENCE (CDC-ECC)
LA English
DT Proceedings Paper
CT 50th IEEE Conference of Decision and Control (CDC)/European Control
Conference (ECC)
CY DEC 12-15, 2011
CL Orlando, FL
SP Honeywell, MathWorks, United Technol Res Ctr, HYCON2, IEEE, Contrl Syst Soc (CSS), EUCA
ID REFERENCE ADAPTIVE-CONTROL; TRANSIENT PERFORMANCE; IMPROVEMENT
AB This paper presents design and performance analysis of a modified reference model MRAC (M-MRAC) architecture for a class of multi-input multi-output uncertain nonlinear systems in the presence of bounded disturbances. M-MRAC incorporates an error feedback in the reference model definition, which allows for fast adaptation without generating high frequency oscillations in the control signal, which closely follows the certainty equivalent control signal. The benefits of the method are demonstrated via a simulation example of an aircraft's wing rock motion.
C1 [Stepanyan, Vahram] NASA, Mission Crit Technol Inc, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Krishnakumar, Kalmanje] NASA, Intelligent Syst Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Stepanyan, V (reprint author), NASA, Mission Crit Technol Inc, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM vahram.stepanyan@nasa.gov; kalmanje.krishnakumar@nasa.gov
NR 18
TC 5
Z9 5
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-61284-801-3
PY 2011
BP 5419
EP 5424
PG 6
WC Automation & Control Systems
SC Automation & Control Systems
GA BAA55
UT WOS:000303506206007
ER
PT S
AU Landau, D
Strange, N
AF Landau, Damon
Strange, Nathan
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI HUMAN EXPLORATION OF NEAR-EARTH ASTEROIDS VIA SOLAR ELECTRIC PROPULSION
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
ID MISSION ARCHITECTURES; OBJECTS
AB There have been many proposed technologies and architectures to extend a human presence beyond the Moon. Solar electric propulsion (SEP) provides the capability to implement a wide variety of missions with relatively low injected mass to low-Earth orbit. Because of its broad applicability this technology can enable progressively ambitious steps towards Mars by incrementally increasing power. The benefits of SEP are addressed for cis-lunar excursions, near-Earth asteroid exploration, and missions to Phobos and Deimos, and compared to chemical propulsion and nuclear thermal technologies. In particular, SEP expands the range of near-Earth asteroids accessible with a constrained launch capability (IMLEO).
C1 [Landau, Damon] CALTECH, Jet Prop Lab, Outer Planet Mission Anal Grp, Pasadena, CA 91125 USA.
RP Landau, D (reprint author), CALTECH, Jet Prop Lab, Outer Planet Mission Anal Grp, M-S 301-121, Pasadena, CA 91125 USA.
NR 39
TC 0
Z9 0
U1 0
U2 2
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 21
EP 37
PN 1-3
PG 17
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600002
ER
PT S
AU Witzberger, KE
Zeiler, T
AF Witzberger, Kevin E.
Zeiler, Tom
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI DIRECT METHOD TRANSCRIPTION FOR A HUMAN-CLASS TRANSLUNAR INJECTION
TRAJECTORY OPTIMIZATION
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB This paper presents a new trajectory optimization software package developed in the framework of a low-to-high fidelity three degree-of-freedom (3-DOF)/ 6-DOF vehicle simulation program named Mission Analysis Simulation Tool in Fortran (MASTIF) and its application to a translunar trajectory optimization problem. The functionality of the developed optimization package is implemented as a new "mode" in generalized settings to make it applicable for a general trajectory optimization problem. In doing so, a direct optimization method using collocation is employed for solving the problem. Trajectory optimization problems in MASTIF are transcribed to a constrained nonlinear programming (NLP) problem and solved with SNOPT, a commercially available NLP solver. A detailed description of the optimization software developed is provided as well as the transcription specifics for the translunar injection (TLI) problem. The analysis includes a 3-DOF trajectory TLI optimization and a 3-DOF vehicle TLI simulation using closed-loop guidance.
C1 [Witzberger, Kevin E.] NASA, Glenn Res Ctr, Mission Design & Anal Branch, Cleveland, OH 44135 USA.
RP Witzberger, KE (reprint author), NASA, Glenn Res Ctr, Mission Design & Anal Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
NR 17
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 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 303
EP 320
PN 1-3
PG 18
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600020
ER
PT S
AU Wallace, MS
Broschart, S
Bonfiglio, E
Bhaskharan, S
Cangahuala, A
AF Wallace, Mark S.
Broschart, Stephen
Bonfiglio, Eugene
Bhaskharan, Shyam
Cangahuala, Alberto
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI TRAJECTORY DESIGN CONSIDERATIONS FOR SMALL-BODY TOUCH-AND-GO
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
ID ORBITAL STABILITY ZONES; SATELLITE DYNAMICS; SOLAR-RADIATION; 1996
FG(3); ASTEROIDS; SPACECRAFT; COMET; MODEL
AB "Touch-and-Go," or TAG, is an approach to small-body surface interrogation missions in which the spacecraft descends to the surface, remains in contact for a short time, and then ascends without coming to rest. Appropriate trajectory design solutions to support TAG missions vary widely based on the spacecraft dynamics, small-body environment, spacecraft and ground systems capabilities, and mission objectives. This paper discusses various factors that are considered during the process of developing a TAG mission trajectory and presents a few case study examples to demonstrate how TAG trajectories may vary from mission to mission.
C1 [Wallace, Mark S.; Broschart, Stephen; Bonfiglio, Eugene; Bhaskharan, Shyam; Cangahuala, Alberto] CALTECH, Jet Prop Lab, Autonomous Syst Div, Pasadena, CA 91109 USA.
RP Wallace, MS (reprint author), CALTECH, Jet Prop Lab, Autonomous Syst Div, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 44
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 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 625
EP 642
PN 1-3
PG 18
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600039
ER
PT S
AU Whiffen, GJ
AF Whiffen, Gregory J.
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI LOW ALTITUDE MAPPING ORBIT DESIGN AND MAINTENANCE FOR THE DAWN DISCOVERY
MISSION AT VESTA
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB NASA's Dawn discovery mission will orbit the giant asteroid Vesta beginning in the summer of 2011. Four different near polar science orbits are planned. The lowest planned orbit at Vesta is called the Low Altitude Mapping Orbit or LAMO and is by far the most challenging to design and maintain due to the strong, nonspherical gravity expected there. This paper describes the orbit selection process. The true gravity field of Vesta remains highly uncertain. The proposed orbit selection process will be applied once sufficient gravity knowledge is obtained at higher orbits. The orbit selection process is applied here to a fictitious gravity field based on a Hubble space telescope shape model for Vesta assuming uniform density. The outcome of the process described here is a variety of stable orbits. However, initially stable orbits at the LAMO altitude are not expected to remain stable operationally due to the unpredictable impulses resulting from the Dawn spacecraft thruster firings to de-saturate its momentum wheels. As a result, orbital maintenance maneuvers will probably be necessary. This paper also briefly describes the statistical maneuver design process that resulted in the orbit maintenance plan.
C1 CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Pasadena, CA 91109 USA.
RP Whiffen, GJ (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 6
TC 0
Z9 0
U1 0
U2 2
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1193
EP 1211
PN 1-3
PG 19
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600071
ER
PT S
AU Whiffen, GJ
AF Whiffen, Gregory J.
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI THE STABILITY OF POWERED FLIGHT AROUND ASTEROIDS WITH APPLICATION TO
VESTA
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB The reliability of low-thrust trajectories between science orbits around large asteroids must be evaluated subject to the unavoidable uncertainties of orbit determination, asteroid physical parameters, momentum de-saturation maneuvers, and transfer maneuver execution error. This paper presents a computationally inexpensive way to extend the concept or orbital stability to trajectories undergoing continuously powered low-thrust flight. Trajectories that are stable using this measure are shown to be stable under the combined uncertainties expected during operations. The measure is general and relatively simple to implement. The method was applied to maneuvers planed around the asteroid Vesta in support of NASA's Dawn Discovery mission.
C1 CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Pasadena, CA 91109 USA.
RP Whiffen, GJ (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 6
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 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1233
EP 1241
PN 1-3
PG 9
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600073
ER
PT S
AU Dankanich, JW
Oleson, SR
AF Dankanich, John W.
Oleson, Steven R.
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI INTERPLANETARY ELECTRIC PROPULSION CHIRON MISSION TRADES SUPPORTING THE
DECADAL SURVEY
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB The decadal survey committee was tasked to develop a comprehensive science and mission strategy for planetary science that updates and extends the National Academies Space Studies Board's current solar system exploration decadal survey. A Chiron orbiter mission has been evaluated as a part of this 2015-2025 Planetary Science Decadal Survey. A comprehensive Chiron orbiter mission design was completed, including a broad search of interplanetary transfer options. The scope of interplanetary trades was originally limited to chemical ballistic solutions due to the power constraint of two Advanced Stirling Radioisotope Generators. All ballistic solutions with no more than 13 year transit times were found non-viable. Solar electric propulsion can increase delivered mass, but does not allow for practical insertion velocities. Based on the propulsion limitations, the scope was increased to include radioisotope powered electric propulsion options. Based on those analyses, it is expected that the science mission can be closed with six standard ASRGs with a 13 year transfer or an 11 year transfer using the next generation ASRGs combined with radioisotope electric propulsion. Interplanetary electric propulsion trajectory trades and sensitivity analyses are presented herein.
C1 [Dankanich, John W.] NASA, ISPT Program, Cleveland, OH 44135 USA.
RP Dankanich, JW (reprint author), NASA, ISPT Program, 21000 Brookpk Rd,M-S 77-4, Cleveland, OH 44135 USA.
NR 9
TC 0
Z9 0
U1 2
U2 2
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1245
EP 1255
PN 1-3
PG 11
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600074
ER
PT S
AU Dankanich, JW
McAdams, J
AF Dankanich, John W.
McAdams, James
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI INTERPLANETARY ELECTRIC PROPULSION URANUS MISSION TRADES SUPPORTING THE
DECADAL SURVEY
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB The Decadal Survey Committee was tasked to develop a comprehensive science and mission strategy for planetary science that updates and extends the National Academies Space Studies Board's current solar system exploration decadal survey. A Uranus orbiter mission has been evaluated as a part of this 2013-2022 Planetary Science Decadal Survey. A comprehensive Uranus orbiter mission design was completed, including a broad search of interplanetary electric propulsion transfer options. The scope of interplanetary trades was limited to electric propulsion concepts, both solar and radioisotope powered. Solar electric propulsion offers significant payloads to Uranus. Inserted mass into the initial science orbit due is highly sensitive to transfer time due to arrival velocities. The recommended baseline trajectory is a 13 year transfer with an Atlas 551, a 1+1 NEXT stage with 15 kW of power using an EEJU trajectory and a 1,000 km EGA flyby altitude constraint. This baseline delivers over 2,000 kg into the initial science orbit. Interplanetary trajectory trades and sensitivity analyses are presented herein.
C1 [Dankanich, John W.] NASA, In Space Prop Technol Project, Cleveland, OH 44135 USA.
RP Dankanich, JW (reprint author), NASA, In Space Prop Technol Project, 21000 Brookpk Rd,M-S 77-4, Cleveland, OH 44135 USA.
NR 8
TC 0
Z9 0
U1 2
U2 3
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1271
EP 1289
PN 1-3
PG 19
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600076
ER
PT S
AU Park, RS
Asmar, SW
Fahnestock, EG
Konopliv, AS
Lu, WW
Watkins, MM
AF Park, Ryan S.
Asmar, Sami W.
Fahnestock, Eugene G.
Konopliv, Alex S.
Lu, Wenwen
Watkins, Mike M.
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI ESTIMATING A HIGH-RESOLUTION LUNAR GRAVITY FIELD AND TIME-VARYING CORE
SIGNATURE
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB This paper presents the expected results of estimating a high-resolution lunar gravity field and time-varying tide and lunar core signatures using the measurements from the Gravity Recovery And Interior Laboratory (GRAIL) mission. An overall GRAIL mission capability is presented based on detailed error analysis of spacecraft dynamics and kinematics models, realistic DSN and inter-spacecraft tracking measurement uncertainties, and length of the data arcs. The largest source of dynamics un-modeled error comes from the spacecraft thermal radiation force, and in order to characterize its error contribution, an a priori error constraint model is derived based on orbit geometry and expected force magnitude. The result shows that estimating a lunar gravity field is robust against both dynamics and kinematics errors and a nominal field of degree 300 or better can be determined assuming a 2.5x10(-4)/n(2) power law. The resolution of the gravity field is most sensitive to the inter-spacecraft Ka-band tracking accuracy. The core signature, however, is more sensitive to dynamic modeling errors and satisfying the latter science requirements depends on how accurately the spacecraft dynamics can be modeled.
C1 [Park, Ryan S.] CALTECH, Jet Prop Lab, Outer Planet Nav Grp, Pasadena, CA 91125 USA.
RP Park, RS (reprint author), CALTECH, Jet Prop Lab, Outer Planet Nav Grp, Pasadena, CA 91125 USA.
NR 13
TC 1
Z9 1
U1 0
U2 2
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1459
EP 1478
PN 1-3
PG 20
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600088
ER
PT S
AU Owen, WM
AF Owen, William M., Jr.
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI METHODS OF OPTICAL NAVIGATION
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
ID CATALOG
AB Optical navigation is the use of onboard imaging to aid in the determination of the spacecraft trajectory and of the targets' ephemerides. Opnav techniques provide a direct measurement of the direction from a spacecraft to target bodies. Opnav data thus complement both radiometric tracking data (for instance, Doppler and range) and the groundbased astrometry which is used to determine the a priori ephemeris of the targets.
We present the geometry and camera models which form the mathematical basis for optical navigation and some of the image processing techniques by which one can extract the optical observables-that is, the sample and line coordinates of images from pictures.
C1 CALTECH, Jet Prop Lab, Opt Nav Grp, Pasadena, CA 91109 USA.
RP Owen, WM (reprint author), CALTECH, Jet Prop Lab, Opt Nav Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 18
TC 2
Z9 2
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1635
EP 1653
PN 1-3
PG 19
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600098
ER
PT S
AU Nolet, S
Gillam, SD
Jones, JB
AF Nolet, Simon
Gillam, Stephen D.
Jones, Jeremy B.
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI OPTICAL NAVIGATION PLANNING PROCESS FOR THE CASSINI SOLSTICE MISSION
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB During the Cassini Equinox Mission, the Optical Navigation strategy has gradually evolved toward maintenance of an acceptable level of uncertainty on the positions of the bodies to be observed. By counteracting the runoff of the uncertainty over time, this strategy helps satisfy the spacecraft pointing requirements throughout the Solstice Mission, while considerably reducing the required imaging frequency. Requirements for planning observations were established, and the planning process itself was largely automated to facilitate re-planning if it becomes necessary. This paper summarizes the process leading to the optical navigation schedule for the seven years of the Solstice Mission.
C1 [Nolet, Simon; Gillam, Stephen D.; Jones, Jeremy B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nolet, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 230-205, Pasadena, CA 91109 USA.
NR 6
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 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1655
EP 1668
PN 1-3
PG 14
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600099
ER
PT S
AU Rush, BP
Owen, WM
Bhaskaran, S
Synnott, SP
AF Rush, Brian P.
Owen, William M., Jr.
Bhaskaran, Shyam
Synnott, Stephen P.
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI OPTICAL NAVIGATION FOR THE EPOXI MISSION
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB The Deep Impact spacecraft flew by comet Hartley 2 on November 4, 2010 as part of its extended mission called EPOXI. Successful navigation depended critically on the quality and timing of optical navigation data processing, because pictures of the comet provided the most precise comet-relative position of the spacecraft. This paper describes the planning, including the picture timing and pointing; the methods used to determine the center of the comet image in each picture; and the optical navigation results, which provided the necessary information to allow the cameras to accurately target the comet for science imaging at encounter.
C1 [Rush, Brian P.; Owen, William M., Jr.; Bhaskaran, Shyam; Synnott, Stephen P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rush, BP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 5
TC 1
Z9 1
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1669
EP 1676
PN 1-3
PG 8
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600100
ER
PT S
AU Riedel, JE
Vaughan, A
Wang, MK
Mastrodemos, N
AF Riedel, J. Ed
Vaughan, Andrew
Wang, Mike
Mastrodemos, Nickolaos
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI POST-FLIGHT LUNAR LANDING-SITE LOCALIZATION AND RECONSTRUCTION USING
DESCENT CAMERA IMAGERY
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB This paper describes a process for reconstruction of the surface position of a landed lunar spacecraft by use of descent imagery. Reconstruction of the landed location is necessary to provide both scientific context of the science obtained from a lander, and to compute the ascent and Earth return trajectory for a mission that would return samples, such as the Moonrise proposal. The method was developed using two system models 1) LCROSS descent (pre-impact) images, comparing with the radio-metric ground truth, and 2) Simulations of the potential Moonrise landing trajectory and lunar terrain, utilizing camera simulations of the Moonrise imager as it would be used during descent. Two methods are used for computing the trajectory, and resultant landing site, the AutoNav onboard navigator, which forms the "N" component of AutoGNC, and the Optical Navigation Program (ONP), which forms the core of JPL's ground-based optical navigation system. This paper describes the methodology of the estimation process, and gives LCROSS results from real data, and results based on the simulations for the Moonrise proposal.
C1 [Riedel, J. Ed; Vaughan, Andrew; Wang, Mike; Mastrodemos, Nickolaos] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Riedel, JE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM joseph.e.riedel@jpl.nasa.gov
NR 9
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 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1687
EP 1703
PN 1-3
PG 17
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600102
ER
PT S
AU Cheng, Y
Clouse, D
Johnson, A
Owen, W
Vaughan, A
AF Cheng, Yang
Clouse, Daniel
Johnson, Andrew
Owen, William
Vaughan, Andrew
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI EVALUATION AND IMPROVEMENT OF PASSIVE OPTICAL TERRAIN RELATIVE
NAVIGATION ALGORITHMS FOR PINPOINT LANDING
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
ID POSE ESTIMATION; DESCENT; ENTRY
AB Future solar system in situ exploration will deploy a pin-point landing (PPL) capability, which is defined as the capability of landing a spacecraft within 100 meters of a targeted site. PPL provides safe and affordable access to high scientific targets, allows the highest science returns, and reduces risk to the spacecraft. PPL relies on computer vision based terrain relative navigation (TRN) technology. This technology recognizes the local terrain and locates the spacecraft within the local terrain frame. Currently, both active sensing (radar or lidar) and passive sensing technologies are actively pursued. In this paper we will focus on passive optical TRN, which compares a descent image with an on-board reference map to locate the spacecraft during descending. First, we present the findings from evaluating two algorithms: MAIA and OBIRON using imagery collected during a field test campaign in 2008. Then we point out the strengths and weaknesses of both algorithms and then suggest some modifications to the algorithms to improve performance. Finally, we give a brief report of the performance of the modified TRN algorithm that is based on a modular TRN toolkit that merges the algorithm components from MAIA and OBIRON.
C1 [Cheng, Yang; Clouse, Daniel; Johnson, Andrew; Owen, William; Vaughan, Andrew] CALTECH, JPL, Pasadena, CA 91125 USA.
RP Cheng, Y (reprint author), CALTECH, JPL, Pasadena, CA 91125 USA.
EM yang.cheng@jpl.nasa.gov; Daniel.S.Clouse@jpl.nasa.gov; aej@jpl.nasa.gov;
William.M.Owen@jpl.nasa.gov; Andrew.T.Vanghan@jpl.nasa.gov
NR 24
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 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1719
EP 1738
PN 1-3
PG 20
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600104
ER
PT S
AU Mastrodemos, N
Rush, B
Vaughan, D
Owen, B
AF Mastrodemos, Nickolaos
Rush, Brian
Vaughan, Drew
Owen, Bill
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI OPTICAL NAVIGATION FOR DAWN AT VESTA
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB The Dawn S/C, launched in September 2007, towards Vesta and Ceres, will enter into orbit about asteroid Vesta in July 2011 and will conduct science remote sensing operations for approximately one year at various orbital altitudes. Vesta navigation operations begin with early approach in May 2011 until departure to Ceres in July 2012. A key navigation aspect is optical navigation, which will be conducted at all mission phases. Here we review the optical navigation plan, imaging, methodology, data types, as well as expected performance in the context of the overall mission navigation. A key aspect of optical navigation at Dawn that will receive particular attention is the extensive use of landmark navigation during most of mission phases. In addition to supporting real-time navigation operations, optical navigation will be used to determine some key physical characteristics of Vesta, such as the asteroid's pole & shape, to assist mission design & science operations.
C1 [Mastrodemos, Nickolaos; Rush, Brian; Vaughan, Drew; Owen, Bill] CALTECH, Jet Prop Lab, Opt Nav Grp, Pasadena, CA 91109 USA.
RP Mastrodemos, N (reprint author), CALTECH, Jet Prop Lab, Opt Nav Grp, Sec343, Pasadena, CA 91109 USA.
NR 11
TC 1
Z9 1
U1 0
U2 3
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 1739
EP 1754
PN 1-3
PG 16
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779600105
ER
PT S
AU Liou, JC
AF Liou, J. -C.
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI ACTIVE DEBRIS REMOVAL - A GRAND ENGINEERING CHALLENGE FOR THE
TWENTY-FIRST CENTURY
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
AB The collision between Iridium 33 and Cosmos 2251 in 2009 has reignited interest in using active debris removal to remediate the near-Earth orbital debris environment. A recent NASA study shows that, in order to stabilize the environment in the low Earth orbit (LEO) region for the next 200 years, active debris removal of about five large and massive (1 to more than 8 metric tons) objects per year is needed. To develop the capability to remove five of those objects per year in a cost-effective manner truly represents a grand challenge in engineering and technology development.
C1 NASA, Orbital Debris Program Off, Johnson Space Ctr, Houston, TX 77058 USA.
RP Liou, JC (reprint author), NASA, Orbital Debris Program Off, Johnson Space Ctr, Mail Code KX,2101 NASA Pkwy, Houston, TX 77058 USA.
NR 6
TC 1
Z9 1
U1 0
U2 3
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 2185
EP 2190
PN 1-3
PG 6
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779601026
ER
PT S
AU Parker, JS
Anderson, RL
Peterson, A
AF Parker, Jeffrey S.
Anderson, Rodney L.
Peterson, Andrew
BE Jah, MK
Guo, YP
Bowes, AL
Lai, PC
TI A SURVEY OF BALLISTIC TRANSFERS TO LOW LUNAR ORBIT
SO SPACEFLIGHT MECHANICS 2011, PTS I-III
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 21st AAS/AIAA Space Flight Mechanics Meeting
CY FEB 13-17, 2011
CL New Orleans, LA
SP AAS, AIAA
ID MOON
AB A simple strategy is identified to generate ballistic transfers between the Earth and Moon, i.e., transfers that perform two maneuvers: a trans-lunar injection maneuver to depart the Earth and a Lunar Orbit Insertion maneuver to insert into orbit at the Moon. This strategy is used to survey the performance of numerous transfers between varying Earth parking orbits and varying low lunar target orbits. The transfers surveyed include short 3-6 day direct transfers, longer 3-4 month low-energy transfers, and variants that include Earth phasing orbits and/or lunar flybys.
C1 [Parker, Jeffrey S.; Anderson, Rodney L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Parker, JS (reprint author), CALTECH, Jet Prop Lab, M-S 301-121,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
OI Anderson, Rodney/0000-0001-5336-2775
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 978-0-87703-569-5
J9 ADV ASTRONAUT SCI
PY 2011
VL 140
BP 2461
EP 2480
PN 1-3
PG 20
WC Engineering, Aerospace
SC Engineering
GA BAC15
UT WOS:000303779601043
ER
PT S
AU Calle, CI
AF Calle, C. I.
BE Taylor, DM
TI The electrostatic environments of Mars and the Moon
SO PROCEEDINGS OF THE 13TH INTERNATIONAL CONFERENCE ON ELECTROSTATICS:
ELECTROSTATICS 2011
SE Journal of Physics Conference Series
LA English
DT Proceedings Paper
CT 13th International Conference on Electrostatics
CY APR 10-14, 2011
CL Bangor Univ, Bangor, WALES
SP CST, JCI Chilworth
HO Bangor Univ
ID DUST; DISCHARGES; GLOW
AB The electrical activity present in the environment near the surfaces of Mars and the moon has very different origins and presents a challenge to manned and robotic planetary exploration missions. Mars is covered with a layer of dust that has been redistributed throughout the entire planet by global dust storms. Dust, levitated by these storms as well as by the frequent dust devils, is expected to be electrostatically charged due to the multiple grain collisions in the dust-laden atmosphere. Dust covering the surface of the moon is expected to be electrostatically charged due to the solar wind, cosmic rays, and the solar radiation itself through the photoelectric effect. Electrostatically charged dust has a large tendency to adhere to surfaces. NASA's Mars exploration rovers have shown that atmospheric dust falling on solar panels can decrease their efficiency to the point of rendering the rover unusable. And as. the Apollo missions to the moon showed, lunar dust adhesion can hinder manned and unmanned lunar exploration activities. Taking advantage of the electrical activity on both planetary system bodies, dust removal technologies are now being developed that use electrostatic and dielectrophoretic forces to produce controlled dust motion. This paper presents a short review of the theoretical and semiempirical models that have been developed for the lunar and Martian electrical environments.
C1 NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA.
RP Calle, CI (reprint author), NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA.
EM carlos.i.calle@nasa.gov
NR 27
TC 1
Z9 1
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 1742-6588
J9 J PHYS CONF SER
PY 2011
VL 301
AR 012006
DI 10.1088/1742-6596/301/1/012006
PG 6
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA BAB66
UT WOS:000303702800006
ER
PT S
AU Breeveld, AA
Landsman, W
Holland, ST
Roming, P
Kuin, NPM
Page, MJ
AF Breeveld, A. A.
Landsman, W.
Holland, S. T.
Roming, P.
Kuin, N. P. M.
Page, M. J.
BE McEnery, JE
Racusin, JL
Gehrels, N
TI An Updated Ultraviolet Calibration for the Swift/UVOT
SO GAMMA RAY BURSTS 2010
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference of the Gamma Ray Bursts
CY NOV 01-04, 2010
CL Annapolis, MD
DE instrumentation: detectors; photometers; astrometry; ultraviolet
ID TELESCOPE; MISSION
AB We present an updated calibration of the Swift/UVOT broadband ultraviolet (uvw1, uvm2, and uvw2) filters. The new calibration accounts for the similar to 1% per year decline in the UVOT sensitivity observed in all filters, and makes use of additional calibration sources with a wider range of colours and with HST spectrophotometry. In this paper we present the new effective area curves and instrumental photometric zeropoints and compare with the previous calibration.
C1 [Breeveld, A. A.; Kuin, N. P. M.; Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
[Landsman, W.; Holland, S. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Holland, S. T.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Roming, P.] Southwest Res Inst, Dept Space Sci, San Antonio, TX 78238 USA.
RP Breeveld, AA (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
FU STFC; PSU by NASA's Office of Space Science [AG5-8401, NAS5-00136]
FX This work is supported at MSSL by funding from STFC and at PSU by NASAs
Office of Space Science through grant NAG5-8401 and NAS5-00136. We
acknowledge the use of public data from the Swift archive. We would like
to thank Tracey Poole for her IDL routines.
NR 6
TC 110
Z9 110
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 978-0-7354-0916-3
J9 AIP CONF PROC
PY 2011
VL 1358
DI 10.1063/1.3621807
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BZU09
UT WOS:000302963100082
ER
PT S
AU Chiang, J
Racusin, JL
AF Chiang, J.
Racusin, J. L.
CA Fermi-LAT Collaboration
BE McEnery, JE
Racusin, JL
Gehrels, N
TI The Search for High Energy Extended Emission by Fermi-LAT from
Swift-localized Gamma-ray Bursts
SO GAMMA RAY BURSTS 2010
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference of the Gamma Ray Bursts
CY NOV 01-04, 2010
CL Annapolis, MD
DE gamma-ray sources; gamma-ray bursts
ID AFTERGLOWS; COMPONENT
AB The brighter Fermi-LAT bursts have exhibited emission at energies > 0.1 GeV that persists as late as similar to 2 ks after the prompt phase has nominally ended. This so-called "extended emission" could arise from continued activity of the prompt burst mechanism or it could be the start of a high energy afterglow component. The high energy extended emission seen by the LAT has typically followed a t(-gamma) power-law temporal decay where gamma approximate to 1.2-1.7 and has shown no strong indication of spectral evolution. In contrast, the prompt burst emission generally displays strong spectral variability and more complex temporal changes in the LAT band. This differing behavior suggests that the extended emission likely corresponds to an early afterglow phase produced by an external shock. In this study, we look for evidence of high energy extended emission from 145 Swift-localized GRBs that have occurred since the launch of Fermi. A majority of these bursts were either outside of the LAT field-of-view or were otherwise not detected by the LAT during the prompt phase. However, because of the scanning operation of the Fermi satellite, the long-lived extended emission of these bursts may be detectable in the LAT data on the similar to few ks time scale. We will look for emission from individual bursts and will perform a stacking analysis in order to set bounds on this emission for the sample as a whole. The detection of such emission would have implications for afterglow models and for the overall energy budget of GRBs.
C1 [Chiang, J.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Racusin, J. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chiang, J (reprint author), Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
FU INAF in Italy; CNES in France
FX The Fermi LAT Collaboration acknowledges support from a number
of agencies and institutes for both development and the operation of the
LAT as well as scientific data analysis. These include NASA and DOE in
the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in
Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg
Foundation, the Swedish Research Council and the National Space Board in
Sweden. Additional support from INAF in Italy and CNES in France for
science analysis during the operations phase is also gratefully
acknowledged.
NR 9
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 978-0-7354-0916-3
J9 AIP CONF PROC
PY 2011
VL 1358
DI 10.1063/1.3621772
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BZU09
UT WOS:000302963100048
ER
PT S
AU Giacomazzo, B
Rezzolla, L
Baiotti, L
Link, D
Font, JA
AF Giacomazzo, Bruno
Rezzolla, Luciano
Baiotti, Luca
Link, David
Font, Jose A.
BE McEnery, JE
Racusin, JL
Gehrels, N
TI General Relativistic Simulations of Binary Neutron Star Mergers
SO GAMMA RAY BURSTS 2010
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference of the Gamma Ray Bursts
CY NOV 01-04, 2010
CL Annapolis, MD
DE neutron stars; gravitational waves; gamma-ray bursts; numerical
relativity
ID GAMMA-RAY BURSTS
AB Binary neutron star mergers are one of the possible candidates for the central engine of short gamma-ray bursts (GRBs) and they are also powerful sources of gravitational waves. We have used our fully general relativistic hydrodynamical code Whisky to investigate the merger of binary neutron star systems and we have in particular studied the properties of the tori that can be formed by these systems, their possible connection with the engine of short GRBs and the gravitational wave signals that detectors such as advanced LIGO will be able to detect. We have also shown how the mass of the torus varies as a function of the total mass of the neutron stars composing the binary and of their mass ratio and we have found that tori sufficiently massive to power short GRBs can indeed be formed.
C1 [Giacomazzo, Bruno] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Giacomazzo, Bruno] NASA Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD USA.
[Rezzolla, Luciano; Link, David] Albert Einstein Inst, Max Planck Inst Gravitationsphys, Potsdam, Germany.
[Baiotti, Luca] Osaka Univ, Inst Laser Engn, Suita, Osaka, Japan.
[Link, David] Humboldt Univ, Inst Phys, Berlin, Germany.
[Font, Jose A.] Univ Valencia, Dept Astron & Astrophys, Valencia, Spain.
RP Giacomazzo, B (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RI Giacomazzo, Bruno/I-8088-2012
OI Giacomazzo, Bruno/0000-0002-6947-4023
FU DFG [SFB/Transregio 7]; "CompStar"; Research Networking Programme of the
European Science Foundation; JSPS Postdoctoral Fellowship For Foreign
Researchers; Spanish Ministerio de Educacion y Ciencia [AYA
2007-67626-C03-01]; NASA [NNX09AI75G]; [19-07803]
FX This work was supported in part by the DFG grant SFB/Transregio 7, by
CompStar, a Research Networking Programme of the European Science
Foundation, by the JSPS Postdoctoral Fellowship For Foreign Researchers,
Grant-in-Aid for Scientific Research (19-07803), by the Spanish
Ministerio de Educacion y Ciencia (AYA 2007-67626-C03-01), and by NASA
grant number NNX09AI75G
NR 17
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 978-0-7354-0916-3
J9 AIP CONF PROC
PY 2011
VL 1358
DI 10.1063/1.3621768
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BZU09
UT WOS:000302963100044
ER
PT S
AU Holland, ST
De Pasquale, M
Mao, J
Sakamoto, T
Schady, P
Covino, S
D'Avanzo, P
Antonelli, A
D'Elia, V
Chincarini, G
Fiore, F
Pandey, SB
AF Holland, S. T.
De Pasquale, M.
Mao, J.
Sakamoto, T.
Schady, P.
Covino, S.
D'Avanzo, P.
Antonelli, A.
D'Elia, V.
Chincarini, G.
Fiore, F.
Pandey, S. B.
BE McEnery, JE
Racusin, JL
Gehrels, N
TI GRB 081029: Understanding Multiple Afterglow Components
SO GAMMA RAY BURSTS 2010
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference of the Gamma Ray Bursts
CY NOV 01-04, 2010
CL Annapolis, MD
DE gamma-ray burst: individual: GRB 081029
AB We present an analysis of the unusual optical light curve of the gamma-ray burst GRB 081029, which occurred at a redshift of z = 3.8479. We combine X-ray and optical observations from the Swift X-Ray Telescope and the Swift UltraViolet Optical Telescope with optical and infrared data obtained using the REM and ROTSE telescopes to construct a detailed data set extending from 86 s to similar to 100 000 s after the BAT trigger. Our data also cover a wide energy range, from 10 keV to 0.77 eV (1.24 angstrom to 16 000 angstrom). The X-ray afterglow shows a shallow initial decay followed by a rapid decay starting at about 18 000 s. The optical and infrared afterglow, however, shows an uncharacteristic rise at about 5000 s that does not correspond to any feature in the X-ray light curve. Our data are not consistent with synchrotron radiation from a single-component jet interacting with an external medium. We do, however, find that the observed light curve can be explained using multi-component model for the jet.
C1 [Holland, S. T.; Sakamoto, T.] NASA GSFC, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
RP Holland, ST (reprint author), NASA GSFC, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
OI D'Elia, Valerio/0000-0002-7320-5862; Covino,
Stefano/0000-0001-9078-5507; Fiore, Fabrizio/0000-0002-4031-4157
NR 10
TC 2
Z9 2
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 978-0-7354-0916-3
J9 AIP CONF PROC
PY 2011
VL 1358
DI 10.1063/1.3621754
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BZU09
UT WOS:000302963100030
ER
PT S
AU Hurley, K
Golenetskii, S
Aptekar, R
Mazets, E
Pal'shin, V
Frederiks, D
Mitrofanov, IG
Golovin, D
Kozyrev, A
Litvak, M
Sanin, AB
Boynton, W
Fellows, C
Harshman, K
Starr, R
von Kienlin, A
Rau, A
Yamaoka, K
Ohno, M
Fukazawa, Y
Takahashi, T
Tashiro, M
Terada, Y
Murakami, T
Makishima, K
Barthelmy, S
Cummings, J
Gehrels, N
Krimm, H
Cline, T
Goldsten, J
Del Monte, E
Feroci, M
Marisaldi, M
Briggs, M
Connaughton, V
Meegan, C
Smith, DM
Wigger, C
Hajdas, W
AF Hurley, K.
Golenetskii, S.
Aptekar, R.
Mazets, E.
Pal'shin, V.
Frederiks, D.
Mitrofanov, I. G.
Golovin, D.
Kozyrev, A.
Litvak, M.
Sanin, A. B.
Boynton, W.
Fellows, C.
Harshman, K.
Starr, R.
von Kienlin, A.
Rau, A.
Yamaoka, K.
Ohno, M.
Fukazawa, Y.
Takahashi, T.
Tashiro, M.
Terada, Y.
Murakami, T.
Makishima, K.
Barthelmy, S.
Cummings, J.
Gehrels, N.
Krimm, H.
Cline, T.
Goldsten, J.
Del Monte, E.
Feroci, M.
Marisaldi, M.
Briggs, M.
Connaughton, V.
Meegan, C.
Smith, D. M.
Wigger, C.
Hajdas, W.
BE McEnery, JE
Racusin, JL
Gehrels, N
TI The Third Interplanetary Network
SO GAMMA RAY BURSTS 2010
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference of the Gamma Ray Bursts
CY NOV 01-04, 2010
CL Annapolis, MD
DE gamma-rays: bursts; instrumentation
ID GAMMA-RAY BURSTS; HIGH-ENERGY EMISSION; MUON NEUTRINOS; SEARCH;
CONSTRAINTS
AB The 3rd interplanetary network (IPN), which has been in operation since 1990, presently consists of 9 spacecraft: AGILE, Fermi, RHESSI, Suzaku, and Swift, in low Earth orbit; INTEGRAL, in eccentric Earth orbit with apogee 0.5 light-seconds; Wind, up to similar to 7 light-seconds from Earth; MESSENGER, en route to Mercury; and Mars Odyssey, in orbit around Mars. The IPN operates as a full-time, all-sky monitor for transients down to a threshold of about 6x10(-7) erg cm(-2) or 1 photon cm(-2) s(-1). It detects similar to 335 cosmic gamma-ray bursts per year. These events are generally not the same ones detected by narrower field of view instruments such as Swift, INTEGRAL IBIS, SuperAGILE, and MAXI; the localization accuracy is in the several arcminute and above range. The data are publicly available and can be utilized for a wide variety of studies.
C1 [Hurley, K.] UC Berkeley Space Sci Lab, Berkeley, CA 94720 USA.
[Golenetskii, S.; Aptekar, R.; Mazets, E.; Pal'shin, V.; Frederiks, D.] Russian Acad Sci, Ioffe Phys Tech Inst, St Petersburg, Russia.
[Mitrofanov, I. G.; Golovin, D.; Kozyrev, A.; Litvak, M.] Inst Space Res, Moscow, Russia.
[Fellows, C.; Harshman, K.; Starr, R.] Univ Arizona, Dept Plant Sci, Tucson, AZ USA.
[Smith, D. M.] Univ Calif, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA USA.
[Wigger, C.; Hajdas, W.] Paul Scherrer Inst, CH-5232 Villigen, Switzerland.
[von Kienlin, A.; Rau, A.] Max Planck Inst Extraterr Phys, Garching, Germany.
[Yamaoka, K.] Aoyama Gakuin Univ, Dept Phys & Math, Kanagawa, Japan.
[Ohno, M.; Takahashi, T.] JAXA, ISAS, Kanagawa, Japan.
[Fukazawa, Y.] Hiroshima Univ, Dept Phys, Hiroshima, Japan.
[Tashiro, M.; Terada, Y.] Saitama Univ, Dept Phys, Saitama, Japan.
[Murakami, T.] Kanazawa Univ, Dept Phys, Kanazawa, Ishikawa 9201192, Japan.
[Makishima, K.] RIKEN, Inst Phys & Chem Res, Makishima Cosm Radiat Lab, Saitama, Japan.
[Barthelmy, S.; Cummings, J.; Gehrels, N.; Krimm, H.; Cline, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Goldsten, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Del Monte, E.; Feroci, M.] INAF, IASF, Rome, Italy.
[Marisaldi, M.] INAF, IASF, Bologna, Italy.
[Smith, D. M.; Wigger, C.] Univ Alabama, Huntsville, AL USA.
[Hajdas, W.] Univ Space Res Assoc, Huntsville, AL USA.
RP Hurley, K (reprint author), UC Berkeley Space Sci Lab, Berkeley, CA 94720 USA.
EM khurley@ssl.berkeley.edu
RI Frederiks, Dmitry/C-7612-2014; Pal'shin, Valentin/F-3973-2014; Aptekar,
Raphail/B-3456-2015; Golenetskii, Sergey/B-3818-2015;
OI Frederiks, Dmitry/0000-0002-1153-6340; Feroci,
Marco/0000-0002-7617-3421; Marisaldi, Martino/0000-0002-4000-3789
FU NASA [NNX09AV61G, NNX08AZ85G]; Russian Space Agency; RFBR
[09-02-12080-ofi_m]
FX KH is grateful for support under the Suzaku Guest Investigator program
through NASA grants NNX09AV61G and NNX08AZ85G. The Konus-Wind experiment
is supported by a Russian Space Agency contract and RFBR grant
09-02-12080-ofi_m.
NR 10
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 978-0-7354-0916-3
J9 AIP CONF PROC
PY 2011
VL 1358
DI 10.1063/1.3621810
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BZU09
UT WOS:000302963100085
ER
PT S
AU Lin, L
Kouveliotou, C
van der Horst, AJ
AF Lin, Lin
Kouveliotou, Chryssa
van der Horst, Alexander J.
BE McEnery, JE
Racusin, JL
Gehrels, N
TI Fermi/GBM Observations of SGR J0501+4516
SO GAMMA RAY BURSTS 2010
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference of the Gamma Ray Bursts
CY NOV 01-04, 2010
CL Annapolis, MD
DE soft gamma repeater; duration; spectra
ID RAY BURST MONITOR; SOFT-GAMMA-REPEATER-1806-20; EMISSION
AB The magnetar candidate SGR J0501+4516 was discovered when it became active for about 13 days from August 22 to September 3, 2008. During this period, the Gamma-ray Burst Monitor (GBM) onboard Fermi detected over 30 bursts. We present here our results on the temporal and spectral analysis of the 29 bursts for which high spectral and time resolution data is available. We find that the T-90 durations of the bursts follow a log-normal distribution with a mean value of similar to 123 ms. We fit the time-integrated spectrum of each burst with several models: a black body function, optically thin thermal brehmsstrahlung, a power law with an exponential cut-off, two black body functions, and the combination of a black body and a power law. We discuss our results in the context of the spectral properties of other magnetar bursts and we also present some correlations between the spectral parameters of the best fit models for all bursts. Finally, we present the results of our time-resolved spectral analysis of the five brightest bursts and discuss how they compare with our time-integrated results.
C1 [Lin, Lin] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Lin, Lin] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Kouveliotou, Chryssa] NASA Marshall Space Flight Ctr, Space Sci Off, VP62, Huntsville, AL 35812 USA.
[van der Horst, Alexander J.] Univ Space Res Associat, NSSTC, Huntsville, AL 35812 USA.
RP Lin, L (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
FU NASA [NNH07ZDA001-GLAST]
FX We thank Ersin Gocgus, Sylvain Guiriec and Yuki Kaneko for their input
and useful discussions. This publication is part of the GBM/Magnetar Key
Project (NASA grant NNH07ZDA001-GLAST, PI: C. Kouveliotou)
NR 15
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 978-0-7354-0916-3
J9 AIP CONF PROC
PY 2011
VL 1358
DI 10.1063/1.3621796
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BZU09
UT WOS:000302963100071
ER
PT S
AU Racusin, JL
AF Racusin, Judith L.
BE McEnery, JE
Racusin, JL
Gehrels, N
TI Fermi and Swift Gamma-ray Burst Afterglow Populations Studies
SO GAMMA RAY BURSTS 2010
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference of the Gamma Ray Bursts
CY NOV 01-04, 2010
CL Annapolis, MD
DE gamma-ray sources; gamma-ray bursts
ID TELESCOPE; EMISSION; SAMPLE; GRBS
AB The new and extreme population of GRBs detected by Fermi-LAT shows several new features in high energy gamma-rays that are providing interesting and unexpected clues into GRB prompt and afterglow emission mechanisms. Over the last 6 years, it has been Swift that has provided the robust data set of UV/optical and X-ray afterglow observations that opened many windows into components of GRB emission structure. The relationship between the LAT GRBs and the well studied, fainter, less energetic GRBs detected by Swift-BAT is only beginning to be explored by multi-wavelength studies. We explore the large sample of GRBs detected by BAT only, BAT and Fermi-GBM, and GBM and LAT, focusing on these samples separately in order to search for statistically significant differences between the populations, using only those GRBs with measured redshifts in order to physically characterize these objects. We disentangle which differences are instrumental selection effects versus intrinsic properties, in order to better understand the nature of the special characteristics of the LAT bursts.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Racusin, JL (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 661, Greenbelt, MD USA.
NR 15
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 978-0-7354-0916-3
J9 AIP CONF PROC
PY 2011
VL 1358
DI 10.1063/1.3621781
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BZU09
UT WOS:000302963100056
ER
PT S
AU Ukwatta, TN
Linnemann, J
Dhuga, KS
Gehrels, N
AF Ukwatta, T. N.
Linnemann, J.
Dhuga, K. S.
Gehrels, N.
BE McEnery, JE
Racusin, JL
Gehrels, N
TI Follow the BAT: Monitoring Swift BAT FoV for Prompt Optical Emission
from Gamma-ray Bursts
SO GAMMA RAY BURSTS 2010
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference of the Gamma Ray Bursts
CY NOV 01-04, 2010
CL Annapolis, MD
DE Gamma-Ray Bursts
ID PRECURSOR ACTIVITY; TELESCOPES; AFTERGLOW; BRIGHT
AB We investigate the feasibility of implementing a system called 'Follow the BAT' that will coordinate ground-based robotic optical and near infrared (NIR) telescopes to monitor the Swift BAT field-of-view (FoV). The system will optimize the monitoring locations in the BAT FoV based on individual robotic telescopes' location, FoV, sensitivity and local weather conditions. The aim is to perform coordinated BAT FoV monitoring by professional as well as amateur astronomers around the world. The scientific goal of the proposed system is to facilitate detection of prompt optical and NIR emission from GRBs, especially from short duration GRBs. We have performed a Monte Carlo simulation to investigate the feasibility of the project.
C1 [Ukwatta, T. N.; Linnemann, J.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Dhuga, K. S.] George Washington Univ, Washington, DC 20052 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ukwatta, TN (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
NR 15
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 978-0-7354-0916-3
J9 AIP CONF PROC
PY 2011
VL 1358
DI 10.1063/1.3621814
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BZU09
UT WOS:000302963100089
ER
PT S
AU Lall, P
Harsha, M
Kumar, K
Goebel, K
Jones, J
Suhling, J
AF Lall, Pradeep
Harsha, Mahendra
Kumar, Krishan
Goebel, Kai
Jones, Jim
Suhling, Jeff
GP IEEE
TI Interrogation of Accrued Damage and Remaining Life in Field-Deployed
Electronics Subjected to Multiple Thermal Environments of Thermal Aging
and Thermal Cycling
SO 2011 IEEE 61ST ELECTRONIC COMPONENTS AND TECHNOLOGY CONFERENCE (ECTC)
SE Electronic Components and Technology Conference
LA English
DT Proceedings Paper
CT IEEE 61st Electronic Components and Technology Conference (ECTC)
CY MAY 31-JUN 03, 2011
CL Lake Buena Vista, FL
SP IEEE, IEEE Components, Packaging & Mfg Technol Soc (CPMT)
ID BOUNDARY-SCAN; RELIABILITY; SHOCK; VIBRATION; MODELS; IMPACT; BIST
AB Field deployed electronics may accrue damage due to environmental exposure and usage after finite period of service but may not often have any macro-indicators of failure such as cracks or delamination. A method to interrogate the damage state of field deployed electronics in the pre-failure space may allow insight into the damage initiation, progression, and remaining useful life of the deployed system. Aging has been previously shown to effect the reliability and constitutive behavior of second-level leadfree interconnects. Prognostication of accrued damage and assessment of residual life can provide valuable insight into impending failure. In this paper, field deployed parts have been extracted and prognosticated for accrued damage and remaining useful life in an anticipated future deployment environment. A subset of the field deployed parts have been tested to failure in the anticipated field deployed environment to validate the assessment of remaining useful life. In addition, some parts have been subjected to additional know thermo-mechanical stresses and the incremental damage accrued validated with respect to the amount of additional damage imposed on the assemblies. The presented methodology uses leading indicators of failure based on micro-structural evolution of damage to identify accrued damage in electronic systems subjected to sequential stresses of thermal aging and thermal cycling. Damage equivalency methodologies have been developed to map damage accrued in thermal aging to the reduction in thermo-mechanical cyclic life based on damage proxies. The expected error with interrogation of system state and assessment of residual life has been quantified. Prognostic metrics including alpha-lambda metric, sample standard deviation, mean square error, mean absolute percentage error, average bias, relative accuracy, and cumulative relative accuracy have been used to compare the performance of the damage proxies.
C1 [Lall, Pradeep; Harsha, Mahendra; Kumar, Krishan; Suhling, Jeff] Auburn Univ, Dept Mech Engn, NSF Ctr Adv Vehicle & Extreme Environm Elect CAVE, Auburn, AL 36849 USA.
[Goebel, Kai] NASA Ames Res Ctr, Moffett Field, CA USA.
[Jones, Jim] Oracle Corp, Sunnyvale, CA USA.
RP Lall, P (reprint author), Auburn Univ, Dept Mech Engn, NSF Ctr Adv Vehicle & Extreme Environm Elect CAVE, Auburn, AL 36849 USA.
EM lall@auburn.edu
FU NASA-IVHM [NNA08BA21C]
FX The research presented in this paper has been supported by NASA-IVHM
Program Grant NNA08BA21C from the National Aeronautics and Space
Administration.
NR 45
TC 4
Z9 4
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0569-5503
BN 978-1-61284-498-5
J9 ELEC COMP C
PY 2011
BP 775
EP 789
PG 15
WC Engineering, Electrical & Electronic
SC Engineering
GA BZP73
UT WOS:000302341400118
ER
PT S
AU Scardelletti, MC
Ponchak, GE
Jordan, JL
Varaljay, NC
McQuaid, EA
Zorman, CA
AF Scardelletti, Maximilian C.
Ponchak, George E.
Jordan, Jennifer L.
Varaljay, Nicholas C.
McQuaid, Elizabeth A.
Zorman, Christian A.
GP IEEE
TI Temperature Dependence of SiC Thin Film Metal-Insulator-Metal (MIM)
Capacitors on Alumina over a Temperature Range from 25 to 500 degrees C
SO 2011 IEEE 61ST ELECTRONIC COMPONENTS AND TECHNOLOGY CONFERENCE (ECTC)
SE Electronic Components and Technology Conference
LA English
DT Proceedings Paper
CT IEEE 61st Electronic Components and Technology Conference (ECTC)
CY MAY 31-JUN 03, 2011
CL Lake Buena Vista, FL
SP IEEE, IEEE Components, Packaging & Mfg Technol Soc (CPMT)
AB In this paper, we present the design, fabrication and characterization of thin film, silicon carbide (SiC) metal-insulator-metal capacitors over a temperature range of 25 to 500 degrees C. The 600 nm thick silicon carbide insulating film was grown with a plasma enhanced chemical vapor deposition unit at 300 and 450 degrees C. Two bottom electrode metal alloys were investigated to determine their effects at higher temperatures on the capacitor reliability. Five capacitor geometries with areas of 0.029, 0.144, 0.292, 0.436 and 0.593 mm(2) were measured on a high temperature probe station over a frequency range from 10 MHz to 10 GHz. The S-parameters were measured on a vector network analyzer and the lumped circuit model was extracted using Agilent's Advanced Design System (TM) software suite. The dielectric constant was extracted from the measured capacitance values. A C-V meter was also used to determine the capacitance and conductance.
C1 [Scardelletti, Maximilian C.; Ponchak, George E.; Jordan, Jennifer L.; Varaljay, Nicholas C.; McQuaid, Elizabeth A.] NASA, Glenn Res Ctr, 21000 Brookpk RD, Cleveland, OH 44135 USA.
[Zorman, Christian A.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
RP Scardelletti, MC (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk RD, Cleveland, OH 44135 USA.
EM Maximilian.C.Scardelletti@nasa.gov
FU Vehicle Health Management High Temperature Wireless Sensors program at
NASA
FX This work was supported by the Vehicle Health Management High
Temperature Wireless Sensors program at NASA.
NR 12
TC 0
Z9 0
U1 0
U2 3
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0569-5503
BN 978-1-61284-498-5
J9 ELEC COMP C
PY 2011
BP 1058
EP 1063
PG 6
WC Engineering, Electrical & Electronic
SC Engineering
GA BZP73
UT WOS:000302341400159
ER
PT S
AU Lall, P
Lowe, R
Goebel, K
AF Lall, Pradeep
Lowe, Ryan
Goebel, Kai
GP IEEE
TI Particle Filter Models and Phase Sensitive Detection for Prognostication
and Health Monitoring of Leadfree Electronics under Shock and Vibration
SO 2011 IEEE 61ST ELECTRONIC COMPONENTS AND TECHNOLOGY CONFERENCE (ECTC)
SE Electronic Components and Technology Conference
LA English
DT Proceedings Paper
CT IEEE 61st Electronic Components and Technology Conference (ECTC)
CY MAY 31-JUN 03, 2011
CL Lake Buena Vista, FL
SP IEEE, IEEE Components, Packaging & Mfg Technol Soc (CPMT)
ID RELIABILITY; RESISTANCE; TRACKING; FATIGUE; IMPACT
AB In this paper, a prognostication health management (PHM) methodology has been presented for electronic components subjected to mechanical shock and vibration. Electronic assemblies have been monitored using state-space vectors from resistance spectroscopy, phase-sensitive detection and particle filtering (PF) to quantify damage initiation, progression and remaining useful life of the electronic assembly. The presented methodology is an advancement of the state-of-art, which presently focuses on reactive failure detection and provides limited or no insight into the system reliability and residual life. Previously damage initiation, damage progression, and residual life in the pre-failure space has been correlated with micro-structural damage based proxies, feature vectors based on time, spectral and joint time-frequency characteristics of electronics [Lall2004(a-d), 2005(a-b), 2006(a-f), 2007(a-e), 2008(a-f)]. Precise resistance measurements based on the resistance spectroscopy method have been used to monitor interconnects for damage and prognosticate failure [Lall 2009(a,b), 2010(a,b), Constable 1992, 2001]. In this paper, the effectiveness of the proposed particle filter and resistance spectroscopy based approach in a prognostic health management (PHM) framework has been demonstrated for electronics. The measured state variable has been related to the underlying damage state using non-linear finite element analysis. The particle filter has been used to estimate the state variable, rate of change of the state variable, acceleration of the state variable and construct a feature vector. The estimated state-space parameters have been used to extrapolate the feature vector into the future and predict the time-to-failure at which the feature vector will cross the failure threshold. Remaining useful life has been calculated based on the evolution of the state space feature vector. Standard prognostic health management metrics were used to quantify the performance of the algorithm against the actual remaining useful life. Application to part replacement decisions for ultra-high reliability system has been demonstrated. Using the technique described in the paper the appropriate time to re-order a replacement part could be monitored, and defended statistically. Robustness of the prognostication algorithm has been quantified using standard performance evaluation metrics.
C1 [Lall, Pradeep; Lowe, Ryan] Auburn Univ, Dept Mech Engn, NSF Ctr Adv Vehicle & Extreme Environm Elect CAVE, Auburn, AL 36849 USA.
[Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lall, P (reprint author), Auburn Univ, Dept Mech Engn, NSF Ctr Adv Vehicle & Extreme Environm Elect CAVE, Auburn, AL 36849 USA.
EM lall@auburn.edu
FU NASA-IVHM Program from the National Aeronautics and Space Administration
[NNA08BA21C]
FX The research presented in this paper has been supported by NASA-IVHM
Program Grant NNA08BA21C from the National Aeronautics and Space
Administration.
NR 61
TC 4
Z9 4
U1 0
U2 4
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0569-5503
BN 978-1-61284-498-5
J9 ELEC COMP C
PY 2011
BP 1097
EP 1109
PG 13
WC Engineering, Electrical & Electronic
SC Engineering
GA BZP73
UT WOS:000302341400165
ER
PT S
AU Lall, P
Gupta, P
Goebel, K
AF Lall, Pradeep
Gupta, Prashant
Goebel, Kai
GP IEEE
TI Identification of Failure Modes in Portable Electronics Subjected to
Mechanical-Shock using Supervised Learning of Damage Progression
SO 2011 IEEE 61ST ELECTRONIC COMPONENTS AND TECHNOLOGY CONFERENCE (ECTC)
SE Electronic Components and Technology Conference
LA English
DT Proceedings Paper
CT IEEE 61st Electronic Components and Technology Conference (ECTC)
CY MAY 31-JUN 03, 2011
CL Lake Buena Vista, FL
SP IEEE, IEEE Components, Packaging & Mfg Technol Soc (CPMT)
ID ARTIFICIAL NEURAL-NETWORKS; TIME-FREQUENCY-DISTRIBUTIONS; CLASSIFICATION
AB An anomaly detection and failure mode classification method has been developed for electronic assemblies with multiple failure modes. The presented prognostic health management method targets the pre-failure space of the electronic assembly life to trigger repair or replacement of impending failures. Presently, health monitoring systems focus on reactive diagnostic detection of failure modes. Examples of diagnostic detection include the built in self test and on-board diagnostics. In this paper, damage pre-cursors from time-spectral measurements of the electronic assemblies has been measured under applied vibration and shock stimulus. The time-evolution of spectral content of the damage pre-cursors has been studied using joint time frequency analysis in a full-field manner on the printed circuit assembly. Frequency moments have been used to build a feature vector. Evolution of the feature vector with damage initiation and progression has been studied under shock and vibration. The feature vector from multiple locations in the board assemblies has been mapped into a de-correlated feature space using Sammon's mapping. Several chip-scale packages have been studied, with SAC305 and SAC405 leadfree second-level interconnects. Transient strain has been measured during the drop-event using digital image correlation and high-speed cameras operating at 100,000 fps. Continuity has been monitored simultaneously for failure identification. In addition, explicit finite element models have been developed and various kinds of failure modes have been simulated such as solder ball cracking, trace fracture, package falloff and solder ball failure. The neural net has been trained using simulated data-sets created from error-seeded models with specific failure modes. The neural net has then been used to identify and classify the failure modes in board assemblies experimentally. Supervised learning of multilayer neural net in conjunction with parity has been used to identify the hard-separation boundaries between failure mode clusters in the de-correlated feature space. The assemblies have been cross-sectioned to verify the identified failure modes. Cross-sections indicate that the experimentally measured failures modes correlate well with the position of the cluster in the de-correlated feature space.
C1 [Lall, Pradeep; Gupta, Prashant] Auburn Univ, Dept Mech Engn, NSF Ctr Adv Vehicle & Extreme Environm Elect CAVE, Auburn, AL 36849 USA.
[Goebel, Kai] NASA Ames Res Ctr, Moffett Field, CA USA.
RP Lall, P (reprint author), Auburn Univ, Dept Mech Engn, NSF Ctr Adv Vehicle & Extreme Environm Elect CAVE, Auburn, AL 36849 USA.
EM lall@auburn.edu
FU NASA-IVHM Program [NNA08BA21C]; National Aeronautics and Space
Administration
FX The research presented in this paper has been supported by NASA-IVHM
Program Grant NNA08BA21C from the National Aeronautics and Space
Administration.
NR 43
TC 0
Z9 0
U1 1
U2 2
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0569-5503
BN 978-1-61284-498-5
J9 ELEC COMP C
PY 2011
BP 1944
EP 1957
PG 14
WC Engineering, Electrical & Electronic
SC Engineering
GA BZP73
UT WOS:000302341400301
ER
PT S
AU MacAskill, JA
Madzunkov, SM
Chutjian, A
AF MacAskill, J. A.
Madzunkov, S. M.
Chutjian, A.
BE McDaniel, FD
Doyle, BL
TI Dipole Excitation with a Paul Ion Trap Mass Spectrometer
SO APPLICATION OF ACCELERATORS IN RESEARCH AND INDUSTRY: TWENTY-FIRST
INTERNATIONAL CONFERENCE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 21st International Conference on Application of Accelerators in Research
and Industry (CAARI)
CY AUG 08-13, 2010
CL Ft Worth, TX
SP Univ N Texas, Sandia Natl Lab, Los Alamos Natl Labs, AccSys Technol Inc, High Voltage Engn Europa BV, Natl Electrostat Corp, TDK-Lambda Amer
DE Paul ion trap; dipole excitation; mass spectrometry
ID RESONANCES
AB Preliminary results are presented for the use of an auxiliary radiofrequency (rf) excitation voltage in combination with a high purity, high voltage rf generator to perform dipole excitation within a high precision Paul ion trap. These results show the effects of the auxiliary excitation frequency over a continuous frequency range on the resultant mass spectra from the Paul trap with particular emphasis on ion ejection times, ion signal intensity, and peak shapes. Ion ejection times are found to decrease continuously with variations in dipole frequency about several resonant values and show remarkable symmetries. Signal intensities vary in a complex fashion with numerous resonant features and are driven to zero at specific frequency values. Observed intensity variations depict dipole excitations that target ions of all masses as well as individual masses. Substantial increases in mass resolution are obtained with resolving powers for nitrogen increasing from 114 to 325.
C1 [MacAskill, J. A.; Madzunkov, S. M.; Chutjian, A.] CALTECH, Jet Prop Lab, Atom & Mol Phys Grp, Pasadena, CA 91109 USA.
RP MacAskill, JA (reprint author), CALTECH, Jet Prop Lab, Atom & Mol Phys Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 6
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 978-0-7354-0891-3
J9 AIP CONF PROC
PY 2011
VL 1336
BP 127
EP 131
DI 10.1063/1.3586072
PG 5
WC Physics, Applied
SC Physics
GA BZT55
UT WOS:000302912900026
ER
PT S
AU Dioszegi, I
Rusek, A
Dane, BR
Chiang, IH
Meek, AG
Dilmanian, FA
AF Dioszegi, I.
Rusek, A.
Dane, B. R.
Chiang, I. H.
Meek, A. G.
Dilmanian, F. A.
BE McDaniel, FD
Doyle, BL
TI Monte Carlo Simulations Of The Dose Distributions From Carbon Microbeams
Used In An Experimental Radiation Therapy Method
SO APPLICATION OF ACCELERATORS IN RESEARCH AND INDUSTRY: TWENTY-FIRST
INTERNATIONAL CONFERENCE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 21st International Conference on Application of Accelerators in Research
and Industry (CAARI)
CY AUG 08-13, 2010
CL Ft Worth, TX
SP Univ N Texas, Sandia Natl Labs, Los Alamos Natl Lab, AccSys Technol Inc, High Voltage Engn Europa BV, Natl Electrostat Corp, TDK-Lambda Amer
DE Monte Carlo simulation; MCNPX; Carbon radiotherapy; microbeam
ID ION RADIOTHERAPY; BEAM
AB Recent upgrades of the MCNPX Monte Carlo code include transport of heavy ions. We employed the new code to simulate the energy and dose distributions produced by carbon beams in rabbit's head in and around a brain tumor. The work was within our experimental technique of interlaced carbon microbeams, which uses two 90 degrees arrays of parallel, thin planes of carbon beams (microbeams) interlacing to produce a solid beam at the target. A similar version of the method was earlier developed with synchrotron-generated x-ray microbeams. We first simulated the Bragg peak in high density polyethylene and other materials, where we could compare the calculated carbon energy deposition to the measured data produced at the NASA Space Radiation Laboratory (NSRL) at Brookhaven National Laboratory (BNL). The results showed that new MCNPX code gives a reasonable account of the carbon beam's dose up to similar to 200 MeV/nucleon beam energy. At higher energies, which were not relevant to our project, the model failed to reproduce the Bragg-peak's extent of increasing nuclear breakup tail. In our model calculations we determined the dose distribution along the beam path, including the angular straggling of the microbeams, and used the data for determining the optimal values of beam spacing in the array for producing adequate beam interlacing at the target. We also determined, for the purpose of Bragg-peak spreading at the target, the relative beam intensities of the consecutive exposures with stepwise lower beam energies, and simulated the resulting dose distribution in the spread out Bragg-peak. The details of the simulation methods used and the results obtained are presented.
C1 [Dioszegi, I.] Brookhaven Natl Lab, Nonproliferat & Natl Secur Dept, Upton, NY 11973 USA.
[Rusek, A.; Chiang, I. H.] NASA, Brookhaven Natl Lab, Space Radiat Lab, Upton, NY 11973 USA.
[Dane, B. R.] SUNY Stony Brook, Sch Med, Stony Brook, NY 11794 USA.
[Meek, A. G.; Dilmanian, F. A.] SUNY Stony Brook, Dept Radiat Oncol, Stony Brook, NY 11794 USA.
[Dilmanian, F. A.] Brookhaven Natl Lab, Med Dept, Upton, NY 11973 USA.
RP Dioszegi, I (reprint author), Brookhaven Natl Lab, Nonproliferat & Natl Secur Dept, Upton, NY 11973 USA.
FU Musella Brain Tumor Foundation; SB's Targeted Research Opportunities
program; SB's Office of the Dean of School of Medicine; SB's Research
Foundation funds; Voices against Brain Cancer
FX We thank Joseph Gatz III, Charles Pearson, and Michael Sivertz for
assistance. Funding for this work was provided by Musella Brain Tumor
Foundation, SBs Targeted Research Opportunities program, SBs Office of
the Dean of School of Medicine, SBs Research Foundation funds (Allen G.
Meek, MD, PI), and Voices against Brain Cancer.
NR 8
TC 1
Z9 1
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 978-0-7354-0891-3
J9 AIP CONF PROC
PY 2011
VL 1336
BP 406
EP 409
DI 10.1063/1.3586130
PG 4
WC Physics, Applied
SC Physics
GA BZT55
UT WOS:000302912900084
ER
PT S
AU Tripathi, RK
AF Tripathi, Ram K.
BE McDaniel, FD
Doyle, BL
TI Radiation Effects In Space
SO APPLICATION OF ACCELERATORS IN RESEARCH AND INDUSTRY: TWENTY-FIRST
INTERNATIONAL CONFERENCE
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 21st International Conference on Application of Accelerators in Research
and Industry (CAARI)
CY AUG 08-13, 2010
CL Ft Worth, TX
SP Univ N Texas, Sandia Natl Lab, Los Alamos Natl Labs, AccSys Technol Inc, High Voltage Engn Europa BV, Natl Electrostat Corp, TDK-Lambda Amer
DE Space Radiation; Cosmic Rays; Solar Particle Events; Radiation Effects
on Space Missions; astronauts; materials and Electronics
AB Protecting space missions from severe exposures from radiation, in general, and long duration/deep space human missions, in particular, is a critical design driver, and could be a limiting factor. The space radiation environment consists of galactic cosmic rays (GCR), solar particle events (SPE), trapped radiation, and includes ions of all the known elements over a very broad energy range. These ions penetrate spacecraft materials producing nuclear fragments and secondary particles that damage biological tissues and microelectronic devices. One is required to know how every element (and all isotopes of each element) in the periodic table interacts and fragments on every other element in the same table as a function of kinetic energy ranging over many decades. In addition, the accuracy of the input information and database, in general and nuclear data in particular, impacts radiation exposure health assessments and payload penalty. After a brief review of effects of space radiation on materials and electronics, human space missions to Mars is discussed.
C1 NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Tripathi, RK (reprint author), NASA Langley Res Ctr, MS 188 E, Hampton, VA 23681 USA.
NR 6
TC 2
Z9 2
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 978-0-7354-0891-3
J9 AIP CONF PROC
PY 2011
VL 1336
BP 649
EP 654
DI 10.1063/1.3586182
PG 6
WC Physics, Applied
SC Physics
GA BZT55
UT WOS:000302912900136
ER
PT J
AU Morrison, H
Zuidema, P
Ackerman, AS
Avramov, A
de Boer, G
Fan, JW
Fridlind, AM
Hashino, T
Harrington, JY
Luo, YL
Ovchinnikov, M
Shipway, B
AF Morrison, Hugh
Zuidema, Paquita
Ackerman, Andrew S.
Avramov, Alexander
de Boer, Gijs
Fan, Jiwen
Fridlind, Ann M.
Hashino, Tempei
Harrington, Jerry Y.
Luo, Yali
Ovchinnikov, Mikhail
Shipway, Ben
TI Intercomparison of cloud model simulations of Arctic mixed-phase
boundary layer clouds observed during SHEBA/FIRE-ACE
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
ID PREDICTION-SYSTEM SHIPS; STRATIFORM CLOUDS; MICROPHYSICS
PARAMETERIZATION; ICE CRYSTALS; PART II; RESOLVING SIMULATIONS; MARINE
STRATOCUMULUS; CONDENSATION NUCLEI; VAPOR-DEPOSITION; M-PACE
AB An intercomparison of six cloud-resolving and large-eddy simulation models is presented. This case study is based on observations of a persistent mixed-phase boundary layer cloud gathered on 7 May, 1998 from the Surface Heat Budget of Arctic Ocean (SHEBA) and First ISCCP Regional Experiment -Arctic Cloud Experiment (FIRE-ACE). Ice nucleation is constrained in the simulations in a way that holds the ice crystal concentration approximately fixed, with two sets of sensitivity runs in addition to the baseline simulations utilizing different specified ice nucleus (IN) concentrations. All of the baseline and sensitivity simulations group into two distinct quasi-steady states associated with either persistent mixed-phase clouds or all-ice clouds after the first few hours of integration, implying the existence of multiple states for this case. These two states are associated with distinctly different microphysical, thermodynamic, and radiative characteristics. Most but not all of the models produce a persistent mixed-phase cloud qualitatively similar to observations using the baseline IN/crystal concentration, while small increases in the IN/crystal concentration generally lead to rapid glaciation and conversion to the all-ice state. Budget analysis indicates that larger ice deposition rates associated with increased IN/crystal concentrations have a limited direct impact on dissipation of liquid in these simulations. However, the impact of increased ice deposition is greatly enhanced by several interaction pathways that lead to an increased surface precipitation flux, weaker cloud top radiative cooling and cloud dynamics, and reduced vertical mixing, promoting rapid glaciation of the mixed-phase cloud for deposition rates in the cloud layer greater than about 1-2 x 10(-5) g kg(-1) s(-1) for this case. These results indicate the critical importance of precipitation-radiative-dynamical interactions in simulating cloud phase, which have been neglected in previous fixed-dynamical parcel studies of the cloud phase parameter space. Large sensitivity to the IN/crystal concentration also suggests the need for improved understanding of ice nucleation and its parameterization in models.
C1 [Morrison, Hugh] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Zuidema, Paquita] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Ackerman, Andrew S.; Avramov, Alexander; Fridlind, Ann M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Avramov, Alexander] Columbia Univ, Earth Inst, New York, NY USA.
[de Boer, Gijs] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Fan, Jiwen; Ovchinnikov, Mikhail] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Hashino, Tempei] Univ Wisconsin, Madison, WI USA.
[Harrington, Jerry Y.] Penn State Univ, State Coll, PA USA.
[Luo, Yali] Chinese Acad Meteorol Sci, Beijing, Peoples R China.
[Shipway, Ben] UK Met Off, Exeter, Devon, England.
RP Morrison, H (reprint author), Natl Ctr Atmospher Res, 3450 Mitchell Lane, Boulder, CO 80307 USA.
EM morrison@ucar.edu
RI Fridlind, Ann/E-1495-2012; Fan, Jiwen/E-9138-2011; Ackerman,
Andrew/D-4433-2012; Zuidema, Paquita/C-9659-2013; Shipway,
Ben/E-1375-2011; de Boer, Gijs/F-3949-2011
OI Ackerman, Andrew/0000-0003-0254-6253; Zuidema,
Paquita/0000-0003-4719-372X; Shipway, Ben/0000-0002-7419-0789; de Boer,
Gijs/0000-0003-4652-7150
FU U. S. DOE ARM [DE-FG02-08ER64574]; NSF Science and Technology Center for
Multiscale Modeling of Atmospheric Processes (CMMAP) [ATM-0425247]; NASA
[NNX07AQ81G, NNG04G171G]; US DOE [ER64187-1027586-0011923,
DE-AC02-05CH11231]; U. S. DOE Atmospheric System Research, an Office of
Science, Office of Biological and Environmental Research (OBER); DOE
Office of Science, OBER [DE-AI02-06ER64173, DE-AI02-08ER64527]; DOE
National Energy Research Scientific Computing Center; NASA Radiation
Sciences Program and Advanced Supercomputing Division; National Science
Foundation [ATM-0639542, AGS-0951807]; Department of Energy
[DE-FG02-05ER64058, DE-FG02-08ER4570]; National Natural Science
Foundation of China [40875064, 40921003]; Chinese Academy of
Meteorological Sciences [2007R001]; Special Fund for Research in
Meteorology [GYHY200806020]; [DE-AC05-76RLO-1830]
FX We thank our colleagues in the SHEBA Atmospheric Surface Flux Group, E.
Andreas, C. Fairall, P. Guest, and P. O. Persson, for collecting and
processing the SHEBA surface data, and R. Moritz for the SHEBA sonde
data. We also thank M. Shupe and B. van Deidenhoven for helpful
discussions. HM was supported by U. S. DOE ARM DE-FG02-08ER64574 and the
NSF Science and Technology Center for Multiscale Modeling of Atmospheric
Processes (CMMAP), managed by Colorado State University under
cooperative agreement ATM-0425247. GB acknowledges NASA (NNX07AQ81G) and
the US DOE (ER64187-1027586-0011923) for funding support. Lawrence
Berkeley National Laboratory is managed by the University of California
under US DOE grant DE-AC02-05CH11231. JF and MO were supported primarily
by the U. S. DOE Atmospheric System Research, an Office of Science,
Office of Biological and Environmental Research (OBER) program; the
Pacific Northwest National Laboratory is operated for the DOE by
Battelle under contract DE-AC05-76RLO-1830. ASA and AMF were supported
by the DOE Office of Science, OBER, through Interagency Agreements
DE-AI02-06ER64173 and DE-AI02-08ER64527, the DOE National Energy
Research Scientific Computing Center, and the NASA Radiation Sciences
Program and Advanced Supercomputing Division. PZ was supported by NASA
Interdisciplinary Studies grant NNG04G171G. JYH would like to thank the
National Science Foundation for support under Grants ATM-0639542 and
AGS-0951807 and The Department of Energy Atmospheric Systems Research
Program for support under Grants DE-FG02-05ER64058 and DE-FG02-08ER4570.
YL was supported by the National Natural Science Foundation of China
(projects 40875064 and 40921003), the Basic Research Fund of the Chinese
Academy of Meteorological Sciences (2007R001), and the Special Fund for
Research in Meteorology (GYHY200806020). TH was supported by NASA
(NNX07AQ81G).
NR 79
TC 39
Z9 39
U1 2
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PY 2011
VL 3
AR M06003
DI 10.1029/2011MS000066
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 931EM
UT WOS:000303198400009
ER
PT J
AU vanZanten, MC
Stevens, B
Nuijens, L
Siebesma, AP
Ackerman, AS
Burnet, F
Cheng, A
Couvreux, F
Jiang, H
Khairoutdinov, M
Kogan, Y
Lewellen, DC
Mechem, D
Nakamura, K
Noda, A
Shipway, BJ
Slawinska, J
Wang, S
Wyszogrodzki, A
AF vanZanten, Margreet C.
Stevens, Bjorn
Nuijens, Louise
Siebesma, A. Pier
Ackerman, A. S.
Burnet, F.
Cheng, A.
Couvreux, F.
Jiang, H.
Khairoutdinov, M.
Kogan, Y.
Lewellen, D. C.
Mechem, D.
Nakamura, K.
Noda, A.
Shipway, B. J.
Slawinska, J.
Wang, S.
Wyszogrodzki, A.
TI Controls on precipitation and cloudiness in simulations of trade-wind
cumulus as observed during RICO
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
ID LARGE-EDDY SIMULATIONS; MARINE BOUNDARY-LAYER; SHALLOW CUMULUS; CLOUDS;
PARAMETERIZATION; CONVECTION; STRATOCUMULUS; MODEL; MICROPHYSICS; RADAR
AB Twelve large-eddy simulations, with a wide range of microphysical representations, are compared to each other and to independent measurements. The measurements and the initial and forcing data for the simulations are taken from the undisturbed period of the Rain in Cumulus over the Ocean (RICO) field study. A regional downscaling of meteorological analyses is performed so as to provide forcing data consistent with the measurements. The ensemble average of the simulations plausibly reproduces many features of the observed clouds, including the vertical structure of cloud fraction, profiles of cloud and rain water, and to a lesser degree the population density of rain drops. The simulations do show considerable departures from one another in the representation of the cloud microphysical structure and the ensuant surface precipitation rates, increasingly so for the more simplified microphysical models. There is a robust tendency for simulations that develop rain to produce a shallower, somewhat more stable cloud layer. Relations between cloud cover and precipitation are ambiguous.
C1 [Stevens, Bjorn; Nuijens, Louise] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
[vanZanten, Margreet C.; Siebesma, A. Pier] Royal Netherlands Meteorol Inst KNMI De Bilt, De Bilt, Netherlands.
[Stevens, Bjorn; Nuijens, Louise] Univ Calif Los Angeles, Dept Atmos & Ocean Sci, Los Angeles, CA USA.
[Siebesma, A. Pier] Delft Univ Technol, Dept Multiscale Phys, Delft, Netherlands.
[Ackerman, A. S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Burnet, F.; Couvreux, F.] Meteo France, CNRS, GAME, Toulouse, France.
[Cheng, A.] SSAI Inc, Langley Res Ctr, Washington, DC USA.
[Jiang, H.] Colorado State Univ, CIRA, Ft Collins, CO 80523 USA.
[Khairoutdinov, M.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY USA.
[Kogan, Y.] Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Norman, OK 73019 USA.
[Lewellen, D. C.] W Virginia Univ, Dept Mech & Aero Engn, Morgantown, WV 26506 USA.
[Mechem, D.] Univ Kansas, Dept Geog, Lawrence, KS 66045 USA.
[Shipway, B. J.] Met Off, Exeter, Devon, England.
[Slawinska, J.] Univ Warsaw, Inst Geophys, Warsaw, Poland.
[Wang, S.] USN, Res Lab, Monterey, CA USA.
[Wyszogrodzki, A.] Res Applicat Lab, NCAR, Boulder, CO USA.
RP Stevens, B (reprint author), Max Planck Inst Meteorol, Bundesstr 53, D-20146 Hamburg, Germany.
EM bjorn.stevens@zmaw.de
RI Couvreux, Fleur/B-3996-2010; Ackerman, Andrew/D-4433-2012; Stevens,
Bjorn/A-1757-2013; Shipway, Ben/E-1375-2011; Jiang, Hongli/N-3281-2014
OI Ackerman, Andrew/0000-0003-0254-6253; Stevens,
Bjorn/0000-0003-3795-0475; Shipway, Ben/0000-0002-7419-0789;
FU Netherlands Organisation for Scientific Research (NWO) [857.00.007]
FX We thank all of those who participated in RICO and helped collect and
prepare the data that made this study possible, in particular Robert
Rauber and Larry Di Girolamo are thanked for the discussions that helped
frame the present study. The Goddard Institute for Space Studies is
thanked for hosting an initial workshop to help organize the
intercomparison. Computing resources for ASA were provided by the NASA
High-End Computing Program through the NASA Advanced Supercomputing
Division at Ames Research Center. MvZ would like to acknowledge the
financial support of Grant 857.00.007 of the Netherlands Organisation
for Scientific Research (NWO). Brian Medeiros and Chiara Antoniazzi are
thanked for help in preparing some of the analysis of lidar data. Peter
Bogenschutz, Christopher S. Bretherton, Wojciech Grabowski and Steve
Krueger are thanked for their contributions to the discussion of the
case study, Irina Sandu and Wojciech Grabowski are thanked for comments
on a draft version of this manuscript. Three constructive and thoughtful
reviews greatly improved the manuscript.
NR 46
TC 96
Z9 96
U1 3
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PY 2011
VL 3
AR M06001
DI 10.1029/2011MS000056
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 931EM
UT WOS:000303198400003
ER
PT S
AU Foster, JL
Hall, D
Riggs, G
AF Foster, James L.
Hall, Dorothy
Riggs, George
BE Neale, CMU
Maltese, A
Richter, K
TI Remote sensing of snow cover and snow water equivalent for the historic
February snowstorms in the Baltimore/Washington DC area during February
2010
SO REMOTE SENSING FOR AGRICULTURE, ECOSYSTEMS, AND HYDROLOGY XIII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Remote Sensing for Agriculture, Ecosystems, and Hydrology
XIII/18th International Symposium on Remote Sensing
CY SEP 19-21, 2011
CL Prague, CZECH REPUBLIC
SP SPIE - Int Soc Opt Engn
DE snowfall; snowpack; passive microwave; AMSR-E
ID DEPTH; ALGORITHM
AB The unprecedented snowfall during early February 2010 in the Baltimore/Washington area provided a unique opportunity to map, monitor and measure snowfall, snow cover extent, snow water equivalent (SWE), and snow melt using a suite of remote sensing instruments. Because snow cover in the Middle Atlantic area of the United States is in most years patchy and a true multi-layered snow pack is rarely established, utilizing a remote sensing approach to observe snow parameters is more challenging than in regions where falling snow and snow packs are more reliable. The Advanced Microwave Scanning Radiometer for EOS (AMSR-E) was used to assess SWE and the onset of melt. Although the passive microwave signatures illustrated in this study are clearly related to snow, it is not straightforward whether or not the signatures are due to variations in SWE or to snowpack metamorphism or to a combination of both.
This study shows that the SWE algorithm was affected by the high variability of snowfall intensity and accumulation as well as by the complex surface features in the Baltimore/Washington area. On the two days when intense snowfalls occurred, February 6 and 10, 2010, retrievals of SWE were compromised. This was likely a result of thermal emission from water droplets in low-level clouds within portions of the storm, which acted to increase AMSR-E Tbs, thereby rendering minimal or zero values for SWE. The presence of such clouds strongly impacts the sensitivity of estimating SWE using radiometric measurements near 19 and 37 GHz. Glaze or icy layers within and on the surface of the snowpack served to increase scattering, thus lowering Tb and boosting the retrieved SWE values, resulting in an overestimation of SWE, first in southern portions of the study area and then farther north as the month of February progressed.
C1 [Foster, James L.; Hall, Dorothy; Riggs, George] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Proc Lab, Greenbelt, MD USA.
RP Foster, JL (reprint author), NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Proc Lab, Greenbelt, MD USA.
NR 13
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 978-0-81948-801-5
J9 PROC SPIE
PY 2011
VL 8174
AR 817402
DI 10.1117/12.896002
PG 8
WC Remote Sensing; Optics; Imaging Science & Photographic Technology
SC Remote Sensing; Optics; Imaging Science & Photographic Technology
GA BZS28
UT WOS:000302735700002
ER
PT S
AU Centrella, J
AF Centrella, Joan
BE Aharonian, FA
Hofmann, W
Rieger, FM
TI Gravitational Wave Astrophysics: Opening the New Frontier
SO 25TH TEXAS SYMPOSIUM ON RELATIVISTIC ASTROPHYSICS (TEXAS 2010)
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT 25th Texas Symposium on Relativistic Astrophysics (TEXAS)
CY DEC 06-10, 2010
CL Heidelberg, GERMANY
SP Max Planck Soc (MPG), Max-Planck-Inst Kernphysik (MPIK), German Fed Minist Educ & Res (BMBF), Int Union Pure & Appl Phys (IUPAP), Struck Innovat Syst, Springer Verlag, Cambridge Univ Press
DE Gravitational wave astrophysics; gravitational radiation; gravitational
wave detectors; black holes
ID PULSAR TIMING ARRAYS; HOLE BINARY-SYSTEMS; MILLISECOND PULSARS; LIGO
AB The gravitational wave window onto the universe is expected to open in similar to 5 years, when ground-based detectors make the first detections in the high-frequency regime. Gravitational waves are ripples in spacetime produced by the motions of massive objects such as black holes and neutron stars. Since the universe is nearly transparent to gravitational waves, these signals carry direct information about their sources - such as masses, spins, luminosity distances, and orbital parameters - through dense, obscured regions across cosmic time. This article explores gravitational waves as cosmic messengers, highlighting key sources, detection methods, and the astrophysical payoffs across the gravitational wave spectrum.
C1 NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Centrella, J (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
NR 36
TC 3
Z9 3
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 978-0-7354-0941-5
J9 AIP CONF PROC
PY 2011
VL 1381
DI 10.1063/1.3635827
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BZT89
UT WOS:000302943200007
ER
PT S
AU Jenke, PA
Finger, MH
Wilson-Hodge, CA
Camero-Arranz, A
AF Jenke, P. A.
Finger, M. H.
Wilson-Hodge, C. A.
Camero-Arranz, A.
BE Gogus, E
Belloni, T
Ertan, U
TI New Timing Results of the X-ray Binary Pulsar OAO 1657-415
SO ASTROPHYSICS OF NEUTRON STARS 2010: A CONFERENCE IN HONOR OF M. ALI
ALPAR
SE AIP Conference Proceedings
LA English
DT Proceedings Paper
CT Conference on Astrophysics of Neutron Stars in Honor of M Ali Alpar
(ASTRONS)
CY AUG 02-06, 2010
CL Cesme, TURKEY
SP Sabanci Univ, European Commiss FP6 Marie Curie Act
DE X-rays; Pulsars; Timing
ID ORBIT
AB OAO 1657-415 is an eclipsing X-ray binary pulsar that has undergone several torque reversals throughout its long history of observation. We present a frequency history spanning nearly 19 years of observations from the Burst and Transient Source Experiment (BATSE) and from the Gamma-Ray Burst Monitor (GBM). Orbital ephemerides of the pulsar system is obtained at several intervals throughout this history. With these ephemerides, statistically significant orbital decay is established.
C1 [Jenke, P. A.; Wilson-Hodge, C. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Finger, M. H.] Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Camero-Arranz, A.] Natl Space & Sci Technol Ctr, Huntsville, AL 35805 USA.
RP Jenke, PA (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 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 978-0-7354-0939-2
J9 AIP CONF PROC
PY 2011
VL 1379
DI 10.1063/1.3629520
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA BZT86
UT WOS:000302936600045
ER
PT S
AU Gore, BF
Hooey, BL
Haan, N
Bakowski, DL
Mahlstedt, E
AF Gore, Brian F.
Hooey, Becky L.
Haan, Nancy
Bakowski, Deborah L.
Mahlstedt, Eric
BE Kurosu, M
TI A Methodical Approach for Developing Valid Human Performance Models of
Flight Deck Operations
SO HUMAN CENTERED DESIGN (HCD)
SE Lecture Notes in Computer Science
LA English
DT Proceedings Paper
CT 2nd International Conference on Human Centered Design (HCD)/14th
International Conference on Human-Computer Interaction (HCI)
CY JUL 09-14, 2011
CL Orlando, FL
ID SYSTEM; MEMORY
AB Validation is critically important when human performance models are used to predict the effect of future system designs on human performance. A model of flight deck operations was validated using a rigorous, iterative, model validation process. The process included the validation of model inputs (task trace and model input parameters), process models (workload, perception, and visual attention) and model outputs of human performance measures (including workload and visual attention). This model will be used to evaluate proposed changes to flight deck technologies and pilot procedures in the NextGen Closely Spaced Parallel Operations concept.
C1 [Gore, Brian F.; Hooey, Becky L.; Bakowski, Deborah L.; Mahlstedt, Eric] San Jose State Univ, NASA, Ames Res Ctr, MS 262-4,POB 1, Moffett Field, CA 94035 USA.
[Haan, Nancy] Dell Services Federal Govt, Moffett Field, CA USA.
RP Gore, BF (reprint author), San Jose State Univ, NASA, Ames Res Ctr, MS 262-4,POB 1, Moffett Field, CA 94035 USA.
EM Brian.F.Gore@nasa.gov; Becky.L.Hooey@nasa.gov; Nancy.Johnson@NASA.gov;
Debi.Bakowski@nasa.gov; Eric.Mahlstedt@nasa.gov
FU Federal Aviation Administration (FAA)/NASA Inter Agency
[DTFAWA-10-X-80005]
FX The composition of this work was supported by the Federal Aviation
Administration (FAA)/NASA Inter Agency Agreement DTFAWA-10-X-80005 Annex
5 (FAA POCs Dr. Tom McCloy, Mr. Dan Hershler; NASA POC Dr. David C.
Foyle). The authors would like to thank Connie Socash, Dr. Christopher
Wickens, Dr. Andrew M. Gacy, and Mala Gosakan from Alion Science and
Technology (MAAD Operations) for their invaluable model development
support and all reviewers for their insightful comments.
NR 20
TC 1
Z9 1
U1 0
U2 1
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0302-9743
BN 978-3-642-21752-4; 978-3-642-21753-1
J9 LECT NOTES COMPUT SC
PY 2011
VL 6776
BP 379
EP 388
PG 10
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA BZS57
UT WOS:000302795300043
ER
PT S
AU Battiste, V
Lachter, J
Ligda, SV
Nguyen, JH
Bacon, LP
Koteskey, RW
Johnson, WW
AF Battiste, Vernol
Lachter, Joel
Ligda, Sarah V.
Nguyen, Jimmy H.
Bacon, L. Paige
Koteskey, Robert W.
Johnson, Walter W.
BE Salvendy, G
Smith, MJ
TI Is ACARS and FANS-1A Just Another Data Link to the Controller?
SO HUMAN INTERFACE AND THE MANAGEMENT OF INFORMATION: INTERACTING WITH
INFORMATION, PT 2
SE Lecture Notes in Computer Science
LA English
DT Proceedings Paper
CT Symposium on Human Interface/14th International Conference on
Human-Computer Interaction (HCI)
CY JUL 09-14, 2011
CL Orlando, FL
AB This report investigates issues surrounding TBO procedures for the current aircraft fleet when requesting deviations around weather. Air and ground procedures were developed to stringently follow TBO principles using three types of communication: Voice, ACARS, and FANS. ACARS and FANS are both text-based communication systems, but FANS allows uplinked flight plans to be automatically loaded into the FMS, while ACARS does not. From the controller perspective, though, all flight plan modifications were completed using a trial planner and delivered via voice or data comm, making FANS and ACARS similar. The controller processed pilots' request and approved or modified them based on traffic management constraints. In this context, the rate of non-conformance across all conditions was higher than anticipated, with off path errors being in excess of 20%. Controllers did not differentiate between the ACARS and FANS data comm, and showed mixed preferences for Voice vs data comm (ACARS and FANS).
C1 [Battiste, Vernol; Lachter, Joel; Ligda, Sarah V.; Koteskey, Robert W.] San Jose State Univ, Flight Deck Display Res Lab, San Jose, CA 95192 USA.
[Johnson, Walter W.] NASA Ames Res Ctr, Flight Deck Display Res Lab, Moffett Field, CA USA.
[Nguyen, Jimmy H.; Bacon, L. Paige] Calif State Univ Long Beach, Long Beach, CA USA.
RP Battiste, V (reprint author), San Jose State Univ, Flight Deck Display Res Lab, San Jose, CA 95192 USA.
EM vernol.battiste-1@nasa.gov; joel.lachter@nasa.gov;
sarah.v.ligda@nasa.gov; mrjimnguyen@gmail.com; paigebacon86@gmail.com;
rob.koteskey@gmail.com; walter.johnson@nasa.gov
FU NASA
FX This study was supported by the NASA Airspace Program, Concepts and
Development Project. We would like to thank George Lawton, Dominic Wong,
Riva Canton, Tom Quinonez and John Luk for software programming support.
We would particularly like to thank Dr. Kim Vu and Dr. Tom Strybel of
California State University, Long Beach, as well as their students for
their aid and support in running this study.
NR 12
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0302-9743
BN 978-3-642-21668-8; 978-3-642-21669-5
J9 LECT NOTES COMPUT SC
PY 2011
VL 6772
BP 453
EP 462
PN 2
PG 10
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA BZS56
UT WOS:000302792800054
ER
PT S
AU Brandt, SL
Lachter, J
Dao, AQV
Battiste, V
Johnson, WW
AF Brandt, Summer L.
Lachter, Joel
Dao, Arik-Quang V.
Battiste, Vernol
Johnson, Walter W.
BE Salvendy, G
Smith, MJ
TI Flight Deck Workload and Acceptability of Verbal and Digital
Communication Protocols
SO HUMAN INTERFACE AND THE MANAGEMENT OF INFORMATION: INTERACTING WITH
INFORMATION, PT 2
SE Lecture Notes in Computer Science
LA English
DT Proceedings Paper
CT Symposium on Human Interface/14th International Conference on
Human-Computer Interaction (HCI)
CY JUL 09-14, 2011
CL Orlando, FL
DE Trajectory Based Operations (TBO); Datacom; NextGen; Human-in-the-Loop
simulation
AB The Federal Aviation Administration hopes to convert air traffic management to Trajectory Based Operations (TBO), under which aircraft flight plans are known to computer systems which aid in scheduling and separation. However, few aircraft flying today have equipment designed to support TBO. We conducted a human-in-the-loop simulation of TBO using current fleet equipage. Three aircraft equipage levels were explored: Voice (the equipment currently used), FANS (the Future Aircraft Navigation System datacom designed for use in TBO), and ACARS (a datacom system widely used for communication with Airline Operation Centers). FANS uplinked flight plans can be automatically loaded into the Flight Management System, while ACARS delivers text that must be entered manually. Pilots rated various aspects of the procedures. Voice was preferred to FANS, with ACARS rated worst, apparently because of slow response times for requests with datacom. Using a mixture of Voice and datacom may provide the benefits of both.
C1 [Brandt, Summer L.; Lachter, Joel; Dao, Arik-Quang V.; Battiste, Vernol] San Jose State Univ, Moffett Field, CA 94035 USA.
[Johnson, Walter W.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Brandt, SL (reprint author), San Jose State Univ, Moffett Field, CA 94035 USA.
EM summer.l.brandt@nasa.gov; joel.lachter@nasa.gov; quang.v.dao@nasa.gov;
vernol.battiste-1@nasa.gov; walter.w.johnson@nasa.gov
FU NASA
FX This study was supported by the NASA Airspace Program, Concepts and
Development Project. We would like to thank George Lawton, Dominic Wong,
Riva Canton, Tom Quinonez and John Luk for software programming support,
and Sarah Ligda and Patrick Cravalho for assistance with recruiting
participants. We would particularly like to thank Dr. Kim Vu and Dr. Tom
Strybel of California State University, Long Beach, as well for their
aid and support in running this study.
NR 11
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0302-9743
BN 978-3-642-21668-8; 978-3-642-21669-5
J9 LECT NOTES COMPUT SC
PY 2011
VL 6772
BP 463
EP 472
PN 2
PG 10
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA BZS56
UT WOS:000302792800055
ER
PT S
AU Dao, AQV
Brandt, SL
Bacon, LP
Kraut, JM
Nguyen, J
Minakata, K
Raza, H
Johnson, WW
AF Dao, Arik-Quang V.
Brandt, Summer L.
Bacon, L. Paige
Kraut, Joshua M.
Nguyen, Jimmy
Minakata, Katsumi
Raza, Hamzah
Johnson, Walter W.
BE Salvendy, G
Smith, MJ
TI Conflict Resolution Automation and Pilot Situation Awareness
SO HUMAN INTERFACE AND THE MANAGEMENT OF INFORMATION: INTERACTING WITH
INFORMATION, PT 2
SE Lecture Notes in Computer Science
LA English
DT Proceedings Paper
CT Symposium on Human Interface/14th International Conference on
Human-Computer Interaction (HCI)
CY JUL 09-14, 2011
CL Orlando, FL
DE situation awareness; flight deck; automation; NextGen; SAGAT; SPAM
AB This study compared pilot situation awareness across three traffic management concepts that varied traffic separation responsibility between the pilots, air-traffic controllers, and an automation system. In Concept 1, the flight deck was equipped with conflict resolution tools that enable them to perform the tasks of weather avoidance and self-separation from surrounding traffic. In Concept 2, air-traffic controllers were responsible for traffic separation, but pilots were provided tools for weather and traffic avoidance. In Concept 3, a ground based automation was used for conflict detection and resolution, and the flight deck tools allowed pilots to deviate for weather, but not detect conflicts. Results showed that pilot situation awareness was highest in Concept 1, where the pilots were most engaged, and lowest in Concept 3, where automation was heavily used. These findings suggest that pilot situation awareness on conflict resolution tasks can be improved by keeping them in the decision-making loop.
C1 [Dao, Arik-Quang V.; Brandt, Summer L.] San Jose State Univ, Moffett Field, CA 94035 USA.
[Bacon, L. Paige; Kraut, Joshua M.; Nguyen, Jimmy; Minakata, Katsumi; Raza, Hamzah] Calif State Univ Long Beach, Dept Psychol, Long Beach, CA 90840 USA.
[Johnson, Walter W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Dao, AQV (reprint author), San Jose State Univ, Moffett Field, CA 94035 USA.
EM quang.v.dao@nasa.gov; summer.l.brandt@nasa.gov;
lauren.bacon@student.csulb.edu; josh.kraut@student.csulb.edu;
jimmy.nguyen@student.csulb.edu; kminakata@gmail.com;
hamzah.raza@student.csulb.edu; walter.w.johnson@nasa.gov
FU NASA [NNA06CN30A]
FX This study was supported by the NASA Concepts and Technology Development
Project, and in collaboration with NASA cooperative agreement
(NNA06CN30A) researchers. These researchers, located at Cal State
University Long Beach, Cal State University Northridge, and Purdue
University, provided pseudopilots and controllers as part of a
distributed simulation network. All participant pilots were tested at
NASA Ames FDDRL. We thank Kim-Phuong Vu, Vernol Battiste, and Tom
Strybel for their comments on prior versions of this paper
NR 16
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 978-3-642-21668-8; 978-3-642-21669-5
J9 LECT NOTES COMPUT SC
PY 2011
VL 6772
BP 473
EP 482
PN 2
PG 10
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA BZS56
UT WOS:000302792800056
ER
PT S
AU Kiken, A
Rorie, RC
Bacon, LP
Billinghurst, S
Kraut, JM
Strybel, TZ
Vu, KPL
Battiste, V
AF Kiken, Ariana
Rorie, R. Conrad
Bacon, L. Paige
Billinghurst, Sabrina
Kraut, Joshua M.
Strybel, Thomas Z.
Vu, Kim-Phuong L.
Battiste, Vernol
BE Salvendy, G
Smith, MJ
TI Effect of ATC Training with NextGen Tools and Online Situation Awareness
and Workload Probes on Operator Performance
SO HUMAN INTERFACE AND THE MANAGEMENT OF INFORMATION: INTERACTING WITH
INFORMATION, PT 2
SE Lecture Notes in Computer Science
LA English
DT Proceedings Paper
CT Symposium on Human Interface/14th International Conference on
Human-Computer Interaction (HCI)
CY JUL 09-14, 2011
CL Orlando, FL
DE Training; NextGen; Air Traffic Control
AB The purpose of the present study was to examine (a) how controller performance changes with the introduction of NextGen tools and (b) how much training is needed for controllers to achieve a performance criterion after the tools have been introduced. Seven retired controllers were trained on an enroute sector in three phases: voice, Data Comm, and online probe. The voice phase trained current-day air traffic management techniques, the Data Comm phase trained NextGen tools, including Data Comm, conflict alerting, and conflict probes, and the probe phase trained controllers on an online probing technique. Although safety was not affected by the introduction of NextGen tools, the tools disrupted operator sector efficiency performance.
C1 [Kiken, Ariana; Rorie, R. Conrad; Bacon, L. Paige; Billinghurst, Sabrina; Kraut, Joshua M.; Strybel, Thomas Z.; Vu, Kim-Phuong L.] Calif State Univ Long Beach, Ctr Human Factors Adv Aeronaut Technol, 1250 N Bellflower Blvd, Long Beach, CA 90840 USA.
[Battiste, Vernol] San Jose State Univ Fdn, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kiken, A (reprint author), Calif State Univ Long Beach, Ctr Human Factors Adv Aeronaut Technol, 1250 N Bellflower Blvd, Long Beach, CA 90840 USA.
EM aegkiken@gmail.com; robert_rorie@yahoo.com; paigebacon86@gmail.com;
sabrinabillinghurst@gmail.com; krautjosh@gmail.com; tstrybel@csulb.edu;
kvu8@csulb.edu; vernol.battiste-1@nasa.gov
NR 15
TC 3
Z9 3
U1 0
U2 0
PU SPRINGER-VERLAG BERLIN
PI BERLIN
PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY
SN 0302-9743
BN 978-3-642-21668-8; 978-3-642-21669-5
J9 LECT NOTES COMPUT SC
PY 2011
VL 6772
BP 483
EP 492
PN 2
PG 10
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA BZS56
UT WOS:000302792800057
ER
PT S
AU Nguyen, JH
Bacon, LP
Rorie, RC
Herron, M
Vu, KPL
Strybel, TZ
Battiste, V
AF Nguyen, Jimmy H.
Bacon, L. Paige
Rorie, R. Conrad
Herron, Meghann
Vu, Kim-Phuong L.
Strybel, Thomas Z.
Battiste, Vernol
BE Salvendy, G
Smith, MJ
TI How Data Comm Methods and Multi-dimensional Traffic Displays Influence
Pilot Workload under Trajectory Based Operations
SO HUMAN INTERFACE AND THE MANAGEMENT OF INFORMATION: INTERACTING WITH
INFORMATION, PT 2
SE Lecture Notes in Computer Science
LA English
DT Proceedings Paper
CT Symposium on Human Interface/14th International Conference on
Human-Computer Interaction (HCI)
CY JUL 09-14, 2011
CL Orlando, FL
DE Data Comm; 2-D displays; 3-D display; ACARS; FANS-1A; Trajectory Based
Operations; Workload; NASA CSD
AB The goal of the present study was to examine the impact of different data-communication (Data Comm) methods and use of multi-dimensional displays (2-D or 3-D) on pilot workload when Trajectory Based Operations (TBO) are employed. Eight pilots flew simulated enroute flights using an integrated (FANS-1A) or non-integrated (ACARS) Data Comm method. Pilots were also asked to rate the workload and acceptability of a route modification with the different Data Comm methods. Online assessments during the flight simulation showed no difference in pilot ratings of workload and route acceptability. However, in post trial questionnaires, pilots reported an overall preference for FANS as a Data Comm method compared to ACARS. The display type did not change pilots' positive ratings for the FANS method, but 3-D displays increase the operator's ability to understand the proposed flight plan changes when they used ACARS.
C1 [Nguyen, Jimmy H.; Bacon, L. Paige; Rorie, R. Conrad; Herron, Meghann; Vu, Kim-Phuong L.; Strybel, Thomas Z.] Calif State Univ Long Beach, 1250 Bellflower Blvd, Long Beach, CA 90840 USA.
[Battiste, Vernol] NASA, Ames Res Ctr, FDDRL, Moffett Field, CA USA.
RP Nguyen, JH (reprint author), Calif State Univ Long Beach, 1250 Bellflower Blvd, Long Beach, CA 90840 USA.
EM Jimmy.Nguyen@student.csulb.com; Lauren.Bacon@student.csulb.com;
Robert.Rorie@student.csulb.com; MeghannBrowne@gmail.com; kvu8@csulb.edu;
tstrybel@csulb.edu; Vernol.Battiste-1@nasa.gov
FU NASA [NNX09AU66A]
FX This study was supported in part by NASA cooperative agreement
NNX09AU66A
NR 9
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 978-3-642-21668-8; 978-3-642-21669-5
J9 LECT NOTES COMPUT SC
PY 2011
VL 6772
BP 507
EP 515
PN 2
PG 9
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA BZS56
UT WOS:000302792800060
ER
EF