FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Holst, TL
AF Holst, Terry L.
TI Transonic flow potential method development at Ames research center
SO COMPUTERS & FLUIDS
LA English
DT Review
ID NUMERICAL OPTIMIZATION; EQUATION; COMPUTATION; ALGORITHM; AIRFOILS;
DYNAMICS; SCHEMES; DESIGN
AB This paper describes selected developments in transonic flow simulation technology that have utilized nonlinear potential methods for external aerodynamic applications. in particular, the research efforts in this field at Ames Research Center are highlighted. Included are a review of the various potential equation forms, the pertinent characteristics associated with key potential equation numerical algorithms, and a variety of numerical results for various aerodynamic applications to highlight key discussion points. Published by Elsevier Ltd.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Holst, TL (reprint author), NASA, Applicat Branch, Adv Supercomp Div, Moffett Field, CA 94035 USA.
EM Terry.L.Holst@nasa.gov
NR 55
TC 2
Z9 2
U1 0
U2 0
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 MAR
PY 2009
VL 38
IS 3
BP 482
EP 490
DI 10.1016/j.compfluid.2008.06.011
PG 9
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 396DE
UT WOS:000262571600002
ER
PT J
AU Pulliam, TH
AF Pulliam, T. H.
TI Early development of implicit methods for Computational Fluid Dynamics
at NASA Ames
SO COMPUTERS & FLUIDS
LA English
DT Review
ID FLOW; SIMULATION; ALGORITHM; FORM
AB The development of implicit finite-difference methods at the Computational Fluid Dynamics Branch (NASA Ames Research Center) in the 1970 to early 1980s timeframe is presented. The seminal work of Drs. Robert F. Warming and Richard M. Beam is highlighted. Their contribution (along with that of others in the Ames CFD Branch) paved the way for modern large scale application codes. The focus will be on a few of the significant developments (e.g., approximate factorization) and results from those early pioneering days. (C) 2008 Published by Elsevier Ltd.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Pulliam, TH (reprint author), NASA, Ames Res Ctr, MS T27B-1, Moffett Field, CA 94035 USA.
EM Thomas.H.Pulliam@nasa.gov
NR 22
TC 0
Z9 0
U1 1
U2 8
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 MAR
PY 2009
VL 38
IS 3
BP 491
EP 495
DI 10.1016/j.compfluid.2008.06.012
PG 5
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 396DE
UT WOS:000262571600003
ER
PT J
AU Chan, WM
AF Chan, William M.
TI Overset grid technology development at NASA Ames Research Center
SO COMPUTERS & FLUIDS
LA English
DT Review
ID GENERATION; COMPUTATION; FLOW
AB The idea of overset grids arose from the need to model complex multi-component systems where an optimum body-fitted grid is used for each component. One of the main motivations behind the overset grid development work at NASA originated from the requirement to perform simulations involving multiple bodies in relative motion. This article traces the development of overset grid technologies at NASA Ames Research Center, including: data format and visualization software; and algorithms and software tools for surface grid generation, volume grid generation, domain connectivity, forces and moments Calculation. and flow solution computation. Examples of the use of overset grids for NASA aerospace applications are given, and current and future work to improve overset grid technologies are summarized. Published by Elsevier Ltd.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Chan, WM (reprint author), NASA, Ames Res Ctr, Mail Stop T27B-1, Moffett Field, CA 94035 USA.
EM William.M.Chan@nasa.gov
NR 53
TC 25
Z9 27
U1 0
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 MAR
PY 2009
VL 38
IS 3
BP 496
EP 503
DI 10.1016/j.compfluid.2008.06.009
PG 8
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 396DE
UT WOS:000262571600004
ER
PT J
AU Kwak, D
Kiris, C
AF Kwak, Dochan
Kiris, Cetin
TI CFD for incompressible flows at NASA Ames
SO COMPUTERS & FLUIDS
LA English
DT Review
ID NAVIER-STOKES EQUATIONS; NUMERICAL-SIMULATION; SCHEMES
AB Over the past 30 years, numerical methods and simulation tools for incompressible flows have been advanced as a subset of the computational fluid dynamics (CFD) discipline. Although incompressible flows are encountered in many areas of engineering, the simulation of compressible flows has driven most of the development of computational algorithms and tools at NASA Ames Research Center. This is due to the stringent requirements for predicting aerodynamic performances of flight vehicles. Conversely, low-speed incompressible flow through or past flow devices did not require the same numerical accuracy. This practice of tolerating relatively low-fidelity solutions in engineering applications has changed, as the design of low-speed flow devices have become more sophisticated, along with more strict efficiency requirements. Accurate and robust CFD tools have become increasingly important in fluid engineering for incompressible and low-speed flow. This paper reviews advances in computational technologies for incompressible flow simulation developed at Ames, and some engineering successes brought about by these advances made during the same period. Additionally, some of the current challenges faced in computing incompressible flows are presented. Published by Elsevier Ltd.
C1 [Kwak, Dochan; Kiris, Cetin] NASA, Ames Res Ctr, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA.
RP Kwak, D (reprint author), NASA, Ames Res Ctr, NASA Adv Supercomp NAS Div, Mail Stop T27B-1, Moffett Field, CA 94035 USA.
EM Dochan.Kwak@nasa.gov
NR 41
TC 3
Z9 3
U1 1
U2 5
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 MAR
PY 2009
VL 38
IS 3
BP 504
EP 510
DI 10.1016/j.compfluid.2008.06.010
PG 7
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 396DE
UT WOS:000262571600005
ER
PT J
AU Lee-Rausch, EM
Frink, NT
Mavriplis, DJ
Rausch, RD
Milholen, WE
AF Lee-Rausch, E. M.
Frink, N. T.
Mavriplis, D. J.
Rausch, R. D.
Milholen, W. E.
TI Transonic drag prediction on a DLR-F6 transport configuration using
unstructured grid solvers
SO COMPUTERS & FLUIDS
LA English
DT Article
ID TURBULENT FLOWS; WORKSHOP
AB A second international AIAA Drag Prediction Workshop (DPW-II) was organized and held in Orlando Florida on June 21-22, 2003. The primary purpose was to investigate the code-to-code uncertainty, address the sensitivity of the drag prediction to grid size and quantify the uncertainty in predicting nacelle/pylon drag increments at a transonic cruise condition. This paper presents an in-depth analysis of the DPW-11 computational results from three state-of-the-art unstructured grid Navier-Stokes flow solvers exercised on similar families of tetrahedral grids. The flow solvers are USM3D - a tetrahedral cell-centered upwind solver, FUN3D - a tetrahedral node-centered upwind solver, and NSU3D - a general element node-centered central-differenced solver. Overall, grid refinement did not consistently improve the correlation with experimental data for either the wing/body or the wing/body/nacelle pylon configuration. Although. the range in total drag for the wing/body fine grids was only 5 counts, a code-to-code comparison of surface pressures and surface restricted streamlines indicated that the three solvers were not all converging to the same flow solutions-different shock locations and separation patterns were evident. Similarly, the wing/body/nacelle/pylon solutions did not appear to be converging to the same flow solutions. Although the absolute values of total drag predicted by two of the solvers for the medium and fine grids did not compare well with the experiment, the incremental drag predictions were within 3 counts of the experimental data. Although, the sources of code-to-code variation in force and moment predictions for the three unstructured grid codes have not yet been identified, the current study reinforces the necessity of applying multiple codes to the same application to assess uncertainty. Published by Elsevier Ltd.
C1 [Lee-Rausch, E. M.; Frink, N. T.; Rausch, R. D.; Milholen, W. E.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
[Mavriplis, D. J.] Univ Wyoming, Coll Engn, Laramie, WY 82071 USA.
RP Lee-Rausch, EM (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, 100 NASA Rd, Hampton, VA 23681 USA.
EM E.Lee-Rausch@nasa.gov
NR 25
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0045-7930
J9 COMPUT FLUIDS
JI Comput. Fluids
PD MAR
PY 2009
VL 38
IS 3
BP 511
EP 532
DI 10.1016/j.compfluid.2008.02.011
PG 22
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 396DE
UT WOS:000262571600006
ER
PT J
AU Lineberry, QJ
Cao, Y
Lin, Y
Ghose, S
Connell, JW
Pan, WP
AF Lineberry, Quentin J.
Cao, Yan
Lin, Yi
Ghose, Sayata
Connell, John W.
Pan, Wei-Ping
TI Mercury Capture from Flue Gas Using Palladium Nanoparticle-Decorated
Substrates as Injected Sorbent
SO ENERGY & FUELS
LA English
DT Article
ID ACTIVATED CARBON; BITUMINOUS COAL; FUEL GAS; OXIDATION; CATALYST;
REACTOR; STATE
AB Although the Clean Air Mercury Rule (CAMR) was recently vacated by the District of Columbia Court of Appeals, efficient mercury (Hg) capture is still an important topic for the coal-fired power plant industry. Several states have Hg emission regulations that are even more stringent than CAMR guidelines. All coals contain Hg, which is released during combustion. Significant research efforts have been made to capture this toxic element before it is released to the atmosphere where it can stay suspended and travel for great distances. A variety of approaches have been examined, among which the injection of sorbent materials such as powdered activated carbon (PAC) is the current method of choice. The work presented here examined the mercury capture capability of various carbon substrates decorated with metal nanoparticles when injected as sorbents. Sorbent injections were carried out in a Hg in air mixture for laboratory-scale screening and in a real flue gas at a coal-fired power plant. It was found that palladium-decorated carbon substrates showed excellent mercury capture capabilities, with total efficiencies greater than 90% in laboratory-scale tests. In the real flue gas, the total efficiency was on the order of similar to 60%, comparable to the benchmark commercial sorbent Darco Hg-LH, a brominated PAC, although the tested adsorbents had much lower surface areas. The results of this study are presented herein. Novel mercury capture from a coal-fired flue gas was achieved using carbon substrates decorated with palladium nanoparticles.
C1 [Lineberry, Quentin J.; Cao, Yan; Pan, Wei-Ping] Western Kentucky Univ, ICSET, Bowling Green, KY 42101 USA.
[Lin, Yi; Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
[Ghose, Sayata] Natl Inst Aerosp, Hampton, VA 23666 USA.
RP Pan, WP (reprint author), Western Kentucky Univ, ICSET, 2413 Nashville Rd,STE C2, Bowling Green, KY 42101 USA.
EM wei-ping.pan@wku.edu
FU NASA GSRP [NGT1-03012]; NASA [NNH06CC03B]
FX This study was supported by the NASA GSRP through Grant NGT1-03012. Y.L.
was supported by an appointment to the NASA Postdoctoral Program at the
Langley Research Center, administered by Oak Ridge Associated
Universities through NASA contract NNH06CC03B.
NR 13
TC 18
Z9 20
U1 2
U2 19
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0887-0624
J9 ENERG FUEL
JI Energy Fuels
PD MAR-APR
PY 2009
VL 23
BP 1512
EP 1517
DI 10.1021/ef800733h
PG 6
WC Energy & Fuels; Engineering, Chemical
SC Energy & Fuels; Engineering
GA 436TM
UT WOS:000265439000048
ER
PT J
AU Mohamed, OA
AF Mohamed, Osama A.
TI Assessment of progressive collapse potential in corner floor panels of
reinforced concrete buildings
SO ENGINEERING STRUCTURES
LA English
DT Article
DE Progressive failure; Linear analysis; Shear stress; Bending moments;
Framed structures; Bracing; Concrete structures
AB The Department of Defense (DoD) document, UFC 4-023-23, which provides technical guidance for mitigation of progressive collapse, classifies buildings based on the desired level of protection. Medium and high levels of protection categories require the use of the Alternate Path (AP) method to investigate the capability of the structural system to transfer loads safely from a notionally removed column to the remaining structural elements. Certain columns and structural elements at prescribed locations must be investigated to determine the structural bridging capabilities over the removed column. Transfer of loads from a notionally removed corner column to the adjacent structural elements can impose significant stress/deformation demand on structural elements supporting the corner panel. When the panel area exceeds the floor damage limits, the panel and its structural elements must be designed to support the additional load or the loads must be transferred to adjacent columns. This paper investigates the implementation of UFC 4-023-23 to protect against progressive collapse of corner floor panels when their dimensions exceed the damage limits. A case study of a reinforced concrete building is analyzed, designed, and investigated using the AP method. (C) 2008 Elsevier Ltd. All rights reserved.
C1 Univ Hartford, NASA, CT Space Grant Coll Consortium, Hartford, CT 06117 USA.
RP Mohamed, OA (reprint author), Univ Hartford, NASA, CT Space Grant Coll Consortium, Hartford, CT 06117 USA.
EM mohamed@hartford.edu
OI Mohamed, Osama/0000-0003-2278-7548
NR 13
TC 24
Z9 24
U1 1
U2 7
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0141-0296
J9 ENG STRUCT
JI Eng. Struct.
PD MAR
PY 2009
VL 31
IS 3
BP 749
EP 757
DI 10.1016/j.engstruct.2008.11.020
PG 9
WC Engineering, Civil
SC Engineering
GA 411QG
UT WOS:000263664000014
ER
PT J
AU Niederberger, TD
Perreault, NN
Lawrence, JR
Nadeau, JL
Mielke, RE
Greer, CW
Andersen, DT
Whyte, LG
AF Niederberger, Thomas D.
Perreault, Nancy N.
Lawrence, John R.
Nadeau, Jay L.
Mielke, Randall E.
Greer, Charles W.
Andersen, Dale T.
Whyte, Lyle G.
TI Novel sulfur-oxidizing streamers thriving in perennial cold saline
springs of the Canadian high Arctic
SO ENVIRONMENTAL MICROBIOLOGY
LA English
DT Article
ID RIBULOSE-1,5-BISPHOSPHATE CARBOXYLASE/OXYGENASE GENES; IN-SITU
HYBRIDIZATION; AXEL-HEIBERG ISLAND; PROJECT RDP-II; MICROBIAL MATS;
PROKARYOTIC DIVERSITY; OLIGONUCLEOTIDE PROBES; BACTERIAL COMMUNITIES;
HYDROTHERMAL FIELD; EXPEDITION FJORD
AB The perennial springs at Gypsum Hill (GH) and Colour Peak (CP), situated at nearly 80 degrees N on Axel Heiberg Island in the Canadian high Arctic, are one of the few known examples of cold springs in thick permafrost on Earth. The springs emanate from deep saline aquifers and discharge cold anoxic brines rich in both sulfide and sulfate. Grey-coloured microbial streamers form during the winter months in snow-covered regions of the GH spring run-off channels (-1.3 degrees C to 6.9 degrees C, similar to 7.5% NaCl, 0-20 p.p.m. dissolved sulfide, 1 p.p.m. dissolved oxygen) but disappear during the Arctic summer. Culture- and molecular-based analyses of the 16S rRNA gene (FISH, DGGE and clone libraries) indicated that the streamers were uniquely dominated by chemolithoautotrophic sulfur-oxidizing Thiomicrospira species. The streamers oxidized both sulfide and thiosulfate and fixed CO(2) under in situ conditions and a Thiomicrospira strain isolated from the streamers also actively oxidized sulfide and thiosulfate and fixed CO(2) under cold, saline conditions. Overall, the snow-covered spring channels appear to represent a unique polar saline microhabitat that protects and allows Thiomicrospira streamers to form and flourish via chemolithoautrophic, phototrophic-independent metabolism in a high Arctic winter environment characterized by air temperatures commonly below -40 degrees C and with an annual average air temperature of -15 degrees C. These results broaden our knowledge of the physical and chemical boundaries that define life on Earth and have astrobiological implications for the possibility of life existing under similar Martian conditions.
C1 [Niederberger, Thomas D.; Perreault, Nancy N.; Whyte, Lyle G.] McGill Univ, Dept Nat Resource Sci, Ste Anne De Bellevue, PQ H9X 3V9, Canada.
[Perreault, Nancy N.; Greer, Charles W.] Natl Res Council Canada, Biotechnol Res Inst, Montreal, PQ H4P 2R2, Canada.
[Lawrence, John R.] Environm Canada, Saskatoon, SK, Canada.
[Nadeau, Jay L.] McGill Univ, Dept Biomed Engn, Montreal, PQ H3A 2B4, Canada.
[Mielke, Randall E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Andersen, Dale T.] Carl Sagan Ctr, Mountain View, CA USA.
RP Whyte, LG (reprint author), McGill Univ, Dept Nat Resource Sci, 21,111 Lakeshore Rd, Ste Anne De Bellevue, PQ H9X 3V9, Canada.
EM lyle.whyte@mcgill.ca
RI Lawrence, John/D-5758-2011
OI Lawrence, John/0000-0001-5872-1212
FU NASA's Exobiology program [NAG5-12395]; Natural Sciences and Engineering
Research Council of Canada (NSERC) Discovery Program; Northern
Supplements Program; Special Research Opportunities Program; Canadian
Space Agency Canadian Analogue Research Network program; Department of
Indian and Northern Affairs - Northern Scientific Training Program;
Fonds QuEbEcois de la Recherche sur la Nature et les Technologies
(FQRNT); Canadian Space Agency CARN program; NSERC Individual Discovery;
NanoIP programs
FX Logistic support was provided by the Canadian Polar Continental Shelf
Project (PCSP-08, 634-07, 664-06, 66) and McGill University's High
Arctic Research Station. This work was supported by grants from NASA's
Exobiology program (NAG5-12395), the Natural Sciences and Engineering
Research Council of Canada (NSERC) Discovery Program, Northern
Supplements Program, Special Research Opportunities Program, and the
Canadian Space Agency Canadian Analogue Research Network program.
Additional funding for student research was provided by the Department
of Indian and Northern Affairs - Northern Scientific Training Program,
and the Fonds QuEbEcois de la Recherche sur la Nature et les
Technologies (FQRNT). Jay L. Nadeau acknowledges support from the
Canadian Space Agency CARN program and the NSERC Individual Discovery
and NanoIP programs.
NR 72
TC 14
Z9 14
U1 7
U2 14
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1462-2912
J9 ENVIRON MICROBIOL
JI Environ. Microbiol.
PD MAR
PY 2009
VL 11
IS 3
BP 616
EP 629
DI 10.1111/j.1462-2920.2008.01833.x
PG 14
WC Microbiology
SC Microbiology
GA 412WU
UT WOS:000263755700008
PM 19278448
ER
PT J
AU Brooks, R
McKenney-Easterling, M
Brinson, M
Rheinhardt, R
Havens, K
O'Brien, D
Bishop, J
Rubbo, J
Armstrong, B
Hite, J
AF Brooks, R.
McKenney-Easterling, M.
Brinson, M.
Rheinhardt, R.
Havens, K.
O'Brien, D.
Bishop, J.
Rubbo, J.
Armstrong, B.
Hite, J.
TI A Stream-Wetland-Riparian (SWR) index for assessing condition of aquatic
ecosystems in small watersheds along the Atlantic slope of the eastern
US
SO ENVIRONMENTAL MONITORING AND ASSESSMENT
LA English
DT Article
CT 8th Symposium of the Environmental Monitoring and Assessment Program
CY APR 10-11, 2007
CL Washington, DC
DE Assessment; Ecological indicators; Mid-Atlantic; Riparian; Streams;
Wetlands
ID MID-ATLANTIC; LAND-COVER; RIVERINE LANDSCAPES; ECOLOGY; BIODIVERSITY;
PENNSYLVANIA; DISTURBANCE; INTEGRITY; EXAMPLE
AB As part of a regional study by the Atlantic Slope Consortium (ASC) to develop ecological and socioeconomic indicators of aquatic ecosystem condition, we developed and tested a protocol for rapidly assessing condition of the stream, wetland, and riparian components of freshwater aquatic ecosystems. Aspects of hydrology, vegetation, in-stream and wetland characteristics, and on-site stressors were measured in the field. The resulting metrics were used to develop an index of overall condition, termed the Stream Wetland-Riparian (SWR) Index. Values of this Index were compared to existing biotic indices and chemical measures, and to a Landscape Index created using satellite-based land cover data and a geographic information system (GIS). Comparisons were made at several levels of spatial aggregation and resolution, from site to small watershed. The SWR Index and associated Landscape Indices were shown to correlate highly with biological indicators of stream condition at the site level and for small contributing areas. The landscape patterns prevalent throughout the entire watershed do not necessarily match the patterns found adjacent to the stream network. We suggest a top-down approach that managers can use to sequentially apply these methods, to first prioritize watersheds based on a relative condition measure provided by the Landscape Index, and then assess condition and diagnose stressors of aquatic resources at the subwatershed and site level.
C1 [Brooks, R.; McKenney-Easterling, M.; Bishop, J.; Rubbo, J.; Armstrong, B.] Penn State Univ, Dept Geog, Penn State Cooperat Wetlands Ctr, University Pk, PA 16802 USA.
[Brinson, M.; Rheinhardt, R.] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA.
[Havens, K.; O'Brien, D.] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
[O'Brien, D.] Natl Marine Fisheries Serv, Habitat Conservat Div, Natl Ocean & Atmospher Adm, Gloucester Point, VA 23062 USA.
[Rubbo, J.] Hudson River Sloop Clearwater Inc, Poughkeepsie, NY 12601 USA.
[Armstrong, B.] Wallace & Pancher Inc, Hermitage, PA 16148 USA.
[Hite, J.] Rettew, Lancaster, PA 17603 USA.
RP Brooks, R (reprint author), Penn State Univ, Dept Geog, Penn State Cooperat Wetlands Ctr, University Pk, PA 16802 USA.
EM rpb2@psu.edu; O'Brien@noaa.gov; jrubbo@gmail.com;
barmstrong@wallacepancher.com; jhite@rettew.com
NR 33
TC 8
Z9 9
U1 0
U2 20
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-6369
J9 ENVIRON MONIT ASSESS
JI Environ. Monit. Assess.
PD MAR
PY 2009
VL 150
IS 1-4
BP 101
EP 117
DI 10.1007/s10661-008-0673-z
PG 17
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 404NM
UT WOS:000263159900010
PM 19082749
ER
PT J
AU Dick, F
Norbury, JW
AF Dick, Frank
Norbury, John W.
TI Singularity in the laboratory frame angular distribution derived in
two-body scattering theory
SO EUROPEAN JOURNAL OF PHYSICS
LA English
DT Article
AB The laboratory (lab) frame angular distribution derived in two-body scattering theory exhibits a singularity at the maximum lab scattering angle. The singularity appears in the kinematic factor that transforms the centre of momentum (cm) angular distribution to the lab angular distribution. We show that it is caused in the transformation by the funnelling of a range of cm scattering angles into a much smaller range of lab angles. Correct treatment of this singularity is important when transforming angular distributions from the cm or projectile frame to the lab frame.
C1 [Dick, Frank] Worcester Polytech Inst, Worcester, MA 01609 USA.
[Norbury, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Dick, F (reprint author), Worcester Polytech Inst, Worcester, MA 01609 USA.
EM fdick@wpi.edu; john.w.norbury@nasa.gov
NR 32
TC 2
Z9 2
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0143-0807
J9 EUR J PHYS
JI Eur. J. Phys.
PD MAR
PY 2009
VL 30
IS 2
BP 403
EP 416
DI 10.1088/0143-0807/30/2/019
PG 14
WC Education, Scientific Disciplines; Physics, Multidisciplinary
SC Education & Educational Research; Physics
GA 411UF
UT WOS:000263675800019
ER
PT J
AU Galan, SF
Mengshoel, OJ
AF Galan, Severino F.
Mengshoel, Ole J.
TI Constraint Handling Using Tournament Selection: Abductive Inference in
Partly Deterministic Bayesian Networks
SO EVOLUTIONARY COMPUTATION
LA English
DT Article
DE Constraint optimization problem; genetic algorithm; Bayesian network;
approximate abductive inference; most probable explanation
ID NORMATIVE EXPERT SYSTEMS; BELIEF NETWORKS; GENETIC ALGORITHMS; PROBABLE
CONFIGURATIONS; NP-HARD; MAPS
AB Constraints occur in many application areas of interest to evolutionary computation. The area considered here is Bayesian networks (BNs), which is a probability-based method for representing and reasoning with uncertain knowledge. This work deals with constraints in BNs and investigates how tournament selection can be adapted to better process such constraints in the context of abductive inference. Abductive inference in BNs consists of finding the most probable explanation given some evidence. Since exact abductive inference is NP-hard, several approximate approaches to this inference task have been developed. One of them applies evolutionary techniques in order to find optimal or close-to-optimal explanations. A problem with the traditional evolutionary approach is this: As the number of constraints determined by the zeros in the conditional probability tables grows, performance deteriorates because the number of explanations whose probability is greater than zero decreases. To minimize this problem, this paper presents and analyzes a new evolutionary approach to abductive inference in BNs. By considering abductive inference as a constraint optimization problem, the novel approach improves performance dramatically when a BN's conditional probability tables contain a significant number of zeros. Experimental results are presented comparing the performances of the traditional evolutionary approach and the approach introduced in this work. The results show that the new approach significantly outperforms the traditional one.
C1 [Galan, Severino F.] Univ Nacl Educ Distancia, Dept Artificial Intelligence, Madrid 28040, Spain.
[Mengshoel, Ole J.] NASA, Ames Res Ctr, CMU, Moffett Field, CA 94035 USA.
RP Galan, SF (reprint author), Univ Nacl Educ Distancia, Dept Artificial Intelligence, Madrid 28040, Spain.
EM seve@dia.uned.es; ole.j.mengshoel@nasa.gov
FU NASA [NCC2-1426]
FX Ole J. Mengshoel gratefully acknowledges support by NASA under award
NCC2-1426.
NR 50
TC 3
Z9 3
U1 0
U2 0
PU MIT PRESS
PI CAMBRIDGE
PA 55 HAYWARD STREET, CAMBRIDGE, MA 02142 USA
SN 1063-6560
J9 EVOL COMPUT
JI Evol. Comput.
PD SPR
PY 2009
VL 17
IS 1
BP 55
EP 88
DI 10.1162/evco.2009.17.1.55
PG 34
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA 411CS
UT WOS:000263626200004
PM 19207088
ER
PT J
AU Cimatti, A
Robberto, M
Baugh, C
Beckwith, SVW
Content, R
Daddi, E
De Lucia, G
Garilli, B
Guzzo, L
Kauffmann, G
Lehnert, M
Maccagni, D
Martinez-Sansigre, A
Pasian, F
Reid, IN
Rosati, P
Salvaterra, R
Stiavelli, M
Wang, Y
Osorio, MZ
Balcells, M
Bersanelli, M
Bertoldi, F
Blaizot, J
Bottini, D
Bower, R
Bulgarelli, A
Burgasser, A
Burigana, C
Butler, RC
Casertano, S
Ciardi, B
Cirasuolo, M
Clampin, M
Cole, S
Comastri, A
Cristiani, S
Cuby, JG
Cuttaia, F
De Rosa, A
Sanchez, AD
Di Capua, M
Dunlop, J
Fan, X
Ferrara, A
Finelli, F
Franceschini, A
Franx, M
Franzetti, P
Frenk, C
Gardner, JP
Gianotti, F
Grange, R
Gruppioni, C
Gruppuso, A
Hammer, F
Hillenbrand, L
Jacobsen, A
Jarvis, M
Kennicutt, R
Kimble, R
Kriek, M
Kurk, J
Kneib, JP
Le Fevre, O
Macchetto, D
MacKenty, J
Madau, P
Magliocchetti, M
Maino, D
Mandolesi, N
Masetti, N
McLure, R
Mennella, A
Meyer, M
Mignoli, M
Mobasher, B
Molinari, E
Morgante, G
Morris, S
Nicastro, L
Oliva, E
Padovani, P
Palazzi, E
Paresce, F
Garrido, A
Pian, E
Popa, L
Postman, M
Pozzetti, L
Rayner, J
Rebolo, R
Renzini, A
Rottgering, H
Schinnerer, E
Scodeggio, M
Saisse, M
Shanks, T
Shapley, A
Sharples, R
Shea, H
Silk, J
Smail, I
Spano, P
Steinacker, J
Stringhetti, L
Szalay, A
Tresse, L
Trifoglio, M
Urry, M
Valenziano, L
Villa, F
Perez, IV
Walter, F
Ward, M
White, R
White, S
Wright, E
Wyse, R
Zamorani, G
Zacchei, A
Zeilinger, WW
Zerbi, F
AF Cimatti, A.
Robberto, M.
Baugh, C.
Beckwith, S. V. W.
Content, R.
Daddi, E.
De Lucia, G.
Garilli, B.
Guzzo, L.
Kauffmann, G.
Lehnert, M.
Maccagni, D.
Martinez-Sansigre, A.
Pasian, F.
Reid, I. N.
Rosati, P.
Salvaterra, R.
Stiavelli, M.
Wang, Y.
Zapatero Osorio, M.
Balcells, M.
Bersanelli, M.
Bertoldi, F.
Blaizot, J.
Bottini, D.
Bower, R.
Bulgarelli, A.
Burgasser, A.
Burigana, C.
Butler, R. C.
Casertano, S.
Ciardi, B.
Cirasuolo, M.
Clampin, M.
Cole, S.
Comastri, A.
Cristiani, S.
Cuby, J. -G.
Cuttaia, F.
De Rosa, A.
Diaz Sanchez, A.
Di Capua, M.
Dunlop, J.
Fan, X.
Ferrara, A.
Finelli, F.
Franceschini, A.
Franx, M.
Franzetti, P.
Frenk, C.
Gardner, Jonathan P.
Gianotti, F.
Grange, R.
Gruppioni, C.
Gruppuso, A.
Hammer, F.
Hillenbrand, L.
Jacobsen, A.
Jarvis, M.
Kennicutt, R.
Kimble, R.
Kriek, M.
Kurk, J.
Kneib, J. -P.
Le Fevre, O.
Macchetto, D.
MacKenty, J.
Madau, P.
Magliocchetti, M.
Maino, D.
Mandolesi, N.
Masetti, N.
McLure, R.
Mennella, A.
Meyer, M.
Mignoli, M.
Mobasher, B.
Molinari, E.
Morgante, G.
Morris, S.
Nicastro, L.
Oliva, E.
Padovani, P.
Palazzi, E.
Paresce, F.
Perez Garrido, A.
Pian, E.
Popa, L.
Postman, M.
Pozzetti, L.
Rayner, J.
Rebolo, R.
Renzini, A.
Rottgering, H.
Schinnerer, E.
Scodeggio, M.
Saisse, M.
Shanks, T.
Shapley, A.
Sharples, R.
Shea, H.
Silk, J.
Smail, I.
Spano, P.
Steinacker, J.
Stringhetti, L.
Szalay, A.
Tresse, L.
Trifoglio, M.
Urry, M.
Valenziano, L.
Villa, F.
Villo Perez, I.
Walter, F.
Ward, M.
White, R.
White, S.
Wright, E.
Wyse, R.
Zamorani, G.
Zacchei, A.
Zeilinger, W. W.
Zerbi, F.
TI SPACE: the spectroscopic all-sky cosmic explorer
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Observational cosmology; Dark energy; Astronomical and space-research
instrumentation
ID GALAXY REDSHIFT SURVEY; BARYONIC ACOUSTIC-OSCILLATIONS; NEAR-INFRARED
SPECTRA; LUMINOUS RED GALAXIES; PROBING DARK ENERGY; POWER SPECTRUM;
COSMOLOGICAL PARAMETERS; K-CORRECTIONS; DEEP FIELD; 1ST STARS
AB We describe the scientific motivations, the mission concept and the instrumentation of SPACE, a class-M mission proposed for concept study at the first call of the ESA Cosmic-Vision 2015-2025 planning cycle. SPACE aims to produce the largest three-dimensional evolutionary map of the Universe over the past 10 billion years by taking near-IR spectra and measuring redshifts for more than half a billion galaxies at 0 < z < 2 down to AB similar to 23 over 3 pi sr of the sky. In addition, SPACE will also target a smaller sky field, performing a deep spectroscopic survey of millions of galaxies to AB similar to 6 and at 2 < z < 10 +. These goals are unreachable with ground-based observations due to the a parts per thousand 500 times higher sky background (see e.g. Aldering, LBNL report number LBNL-51157, 2001). To achieve the main science objectives, SPACE will use a 1.5 m diameter Ritchey-Chretien telescope equipped with a set of arrays of Digital Micro-mirror Devices covering a total field of view of 0.4 deg(2), and will perform large-multiplexing multi-object spectroscopy (e.g. a parts per thousand 6000 targets per pointing) at a spectral resolution of R similar to 400 as well as diffraction-limited imaging with continuous coverage from 0.8 to 1.8 mu m. Owing to the depth, redshift range, volume coverage and quality of its spectra, SPACE will reveal with unique sensitivity most of the fundamental cosmological signatures, including the power spectrum of density fluctuations and its turnover. SPACE will also place high accuracy constraints on the dark energy equation of state parameter and its evolution by measuring the baryonic acoustic oscillations imprinted when matter and radiation decoupled, the distance-luminosity relation of cosmological supernovae, the evolution of the cosmic expansion rate, the growth rate of cosmic large-scale structure, and high-z galaxy clusters. The datasets from the SPACE mission will represent a long lasting legacy for the whole astronomical community whose data will be mined for many years to come.
C1 [Cimatti, A.] Univ Bologna, Dipartimento Astron, Bologna, Italy.
[Robberto, M.; Beckwith, S. V. W.; Reid, I. N.; Stiavelli, M.; Casertano, S.; MacKenty, J.; Postman, M.; White, R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Daddi, E.] CEA Saclay, F-91191 Gif Sur Yvette, France.
[De Lucia, G.; Kauffmann, G.; Blaizot, J.; Ciardi, B.; White, S.] MPA Garching, Garching, Germany.
[Garilli, B.; Maccagni, D.; Bottini, D.; Franzetti, P.; Scodeggio, M.] INAF, IASFMI, Rome, Italy.
[Lehnert, M.; Hammer, F.] Observ Paris, Paris, France.
[Martinez-Sansigre, A.; Kurk, J.; Schinnerer, E.; Steinacker, J.; Walter, F.] Max Planck Inst Astron, Heidelberg, Germany.
[Pasian, F.; Cristiani, S.; Magliocchetti, M.; Pian, E.; Zacchei, A.] INAF, Osservatorio Astron Trieste, Rome, Italy.
[Rosati, P.; Padovani, P.] ESO Garching, Garching, Germany.
[Salvaterra, R.; Bersanelli, M.; Maino, D.; Mennella, A.] Univ Milan, Milan, Italy.
[Wang, Y.] Univ Oklahoma, Norman, OK 73019 USA.
[Zapatero Osorio, M.; Balcells, M.; Rebolo, R.] IAC, Santa Cruz de Tenerife, Spain.
[Bertoldi, F.] Univ Bonn, D-5300 Bonn, Germany.
[Bulgarelli, A.; Burigana, C.; Butler, R. C.; Cuttaia, F.; De Rosa, A.; Finelli, F.; Gianotti, F.; Gruppuso, A.; Mandolesi, N.; Masetti, N.; Morgante, G.; Nicastro, L.; Palazzi, E.; Paresce, F.; Stringhetti, L.; Trifoglio, M.; Valenziano, L.; Villa, F.] INAF, IASFBO, Rome, Italy.
[Clampin, M.; Gardner, Jonathan P.; Kimble, R.] NASA, GSFC, Washington, DC 20546 USA.
[Comastri, A.; Gruppioni, C.; Mignoli, M.; Pozzetti, L.; Zamorani, G.] INAF, Osservatorio Astron Bologna, Bologna, Italy.
[Diaz Sanchez, A.; Perez Garrido, A.; Villo Perez, I.] U Politecn Cartagena, UPCT, Cartagena, Spain.
[Di Capua, M.] UMD, College Pk, MD USA.
[Dunlop, J.] CRC, Ottawa, ON, Canada.
[Fan, X.] Univ Arizona, Tucson, AZ USA.
[Ferrara, A.] SISSA, I-34014 Trieste, Italy.
[Franceschini, A.] Univ Padua, Padua, Italy.
[Franx, M.; Kriek, M.; Rottgering, H.] Leiden Univ, Leiden, Netherlands.
[Hillenbrand, L.] CALTECH, Pasadena, CA 91125 USA.
[Jacobsen, A.] OpSys Project Consulting, Schoeffengrund, Germany.
[Jarvis, M.] Univ Hertfordshire, Hatfield AL10 9AB, Herts, England.
[Macchetto, D.] ESA, F-75738 Paris 15, France.
[Madau, P.] UCSC, Santa Cruz, CA USA.
[Meyer, M.] Univ Arizona, Steward Observ, Tucson, AZ USA.
[Mobasher, B.] UC Riverside, Riverside, CA USA.
[Oliva, E.] INAF, Osservatorio Astrofis Arcetri, Florence, Italy.
[Oliva, E.] TNG, Rome, Italy.
[Popa, L.] Univ Bucharest, Bucharest, Romania.
[Rayner, J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Renzini, A.] INAF, Osservatorio Astron Padova, Padua, Italy.
[Shea, H.] Ecole Polytech Fed Lausanne, Lausanne, Switzerland.
[Szalay, A.; Wyse, R.] Johns Hopkins Univ, Baltimore, MD USA.
[Urry, M.] Yale Univ, New Haven, CT USA.
[Wright, E.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Zeilinger, W. W.] Univ Vienna, Vienna, Austria.
[Silk, J.] Univ Oxford, Oxford, England.
[Kennicutt, R.] IoA, Cambridge, England.
[Burgasser, A.] MIT, Cambridge, MA 02139 USA.
[Cirasuolo, M.; Dunlop, J.; McLure, R.] ROE, Edinburgh, Midlothian, Scotland.
[Cuby, J. -G.; Grange, R.; Kneib, J. -P.; Le Fevre, O.; Saisse, M.; Tresse, L.] LAM, Marseille, France.
[Content, R.; Sharples, R.] Univ Durham, Ctr Adv Instrumentat, Durham, England.
[Baugh, C.; Bower, R.; Cole, S.; Frenk, C.; Morris, S.; Shanks, T.; Smail, I.; Ward, M.] Univ Durham, Inst Computat Cosmol, Durham, England.
RP Cimatti, A (reprint author), Univ Bologna, Dipartimento Astron, Bologna, Italy.
EM a.cimatti@unibo.it
RI Baugh, Carlton/A-8482-2012; Sharples, Ray/N-7309-2013; Ferrara,
Andrea/A-4357-2011; Smail, Ian/M-5161-2013; Perez-Garrido,
Antonio/L-8507-2014; Trifoglio, Massimo/F-5302-2015; Wang,
Yun/B-5724-2011; Le Fevre, Olivier/G-7389-2011; Morris,
Simon/G-7981-2011; White, Richard/A-8143-2012; Daddi,
Emanuele/D-1649-2012; Clampin, mark/D-2738-2012; Kimble,
Randy/D-5317-2012; Nicastro, Luciano/F-5866-2015; Kneib,
Jean-Paul/A-7919-2015; Palazzi, Eliana/N-4746-2015; Gruppuso,
Alessandro/N-5592-2015; Ciardi, Benedetta/N-7625-2015; Mignoli,
Marco/O-9426-2015; Comastri, Andrea/O-9543-2015; Shea,
Herbert/C-4744-2008; popa, lucia/B-4718-2012; Zapatero Osorio, Maria
Rosa/C-2744-2017; Butler, Reginald/N-4647-2015;
OI Baugh, Carlton/0000-0002-9935-9755; Sharples, Ray/0000-0003-3449-8583;
Smail, Ian/0000-0003-3037-257X; Trifoglio, Massimo/0000-0002-2505-3630;
Wang, Yun/0000-0002-4749-2984; Morris, Simon/0000-0003-4866-110X; Daddi,
Emanuele/0000-0002-3331-9590; Morgante, Gianluca/0000-0001-9234-7412;
Scodeggio, Marco/0000-0002-2282-5850; Molinari,
Emilio/0000-0002-1742-7735; Oliva, Ernesto/0000-0002-9123-0412; bottini,
dario/0000-0001-6917-041X; Pozzetti, Lucia/0000-0001-7085-0412;
Zeilinger, Werner/0000-0001-8507-1403; Nicastro,
Luciano/0000-0001-8534-6788; Kneib, Jean-Paul/0000-0002-4616-4989;
Gruppuso, Alessandro/0000-0001-9272-5292; Mignoli,
Marco/0000-0002-9087-2835; Comastri, Andrea/0000-0003-3451-9970; Shea,
Herbert/0000-0003-3527-3036; Zapatero Osorio, Maria
Rosa/0000-0001-5664-2852; Butler, Reginald/0000-0003-4366-5996;
Magliocchetti, Manuela/0000-0001-9158-4838; Stringhetti,
Luca/0000-0002-3961-9068; Pasian, Fabio/0000-0002-4869-3227; Gruppioni,
Carlotta/0000-0002-5836-4056; Franzetti, Paolo/0000-0002-6986-0127;
Gianotti, Fulvio/0000-0003-4666-119X; Bulgarelli,
Andrea/0000-0001-6347-0649; Cuttaia, Francesco/0000-0001-6608-5017;
Valenziano, Luca/0000-0002-1170-0104; Cristiani,
Stefano/0000-0002-2115-5234; Burigana, Carlo/0000-0002-3005-5796;
Finelli, Fabio/0000-0002-6694-3269; Palazzi, Eliana/0000-0002-8691-7666;
Salvaterra, Ruben/0000-0002-9393-8078; Zerbi, Filippo
Maria/0000-0002-9996-973X; Padovani, Paolo/0000-0002-4707-6841; Villa,
Fabrizio/0000-0003-1798-861X; silk, joe/0000-0002-1566-8148; Garilli,
Bianca/0000-0001-7455-8750; Zamorani, Giovanni/0000-0002-2318-301X;
Masetti, Nicola/0000-0001-9487-7740; Urry, Meg/0000-0002-0745-9792;
Schinnerer, Eva/0000-0002-3933-7677; Zacchei,
Andrea/0000-0003-0396-1192; Pian, Elena/0000-0001-8646-4858
FU University of Bologna; Space Telescope Science Institute
FX The authors acknowledge the support from the University of Bologna and
the Space Telescope Science Institute. Thales Alenia-Milano ( Italy) is
warmly acknowledged for its contributions and support.
NR 67
TC 43
Z9 44
U1 1
U2 13
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 1
BP 39
EP 66
DI 10.1007/s10686-008-9096-7
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KZ
UT WOS:000263505900004
ER
PT J
AU Piro, L
den Herder, J
Ohashi, T
Amati, L
Atteia, JL
Barthelmy, S
Barbera, M
Barret, D
Basso, S
Boer, M
Borgani, S
Boyarskiy, O
Branchini, E
Branduardi-Raymont, G
Briggs, M
Brunetti, G
Budtz-Jorgensen, C
Burrows, D
Campana, S
Caroli, E
Chincarini, G
Christensen, F
Cocchi, M
Comastri, A
Corsi, A
Cotroneo, V
Conconi, P
Colasanti, L
Cusumano, G
de Rosa, A
Del Santo, M
Ettori, S
Ezoe, Y
Ferrari, L
Feroci, M
Finger, M
Fishman, G
Fujimoto, R
Galeazzi, M
Galli, A
Gatti, F
Gehrels, N
Gendre, B
Ghirlanda, G
Ghisellini, G
Giommi, P
Girardi, M
Guzzo, L
Haardt, F
Hepburn, I
Hermsen, W
Hoevers, H
Holland, A
in't Zand, J
Ishisaki, Y
Kawahara, H
Kawai, N
Kaastra, J
Kippen, M
de Korte, PAJ
Kouveliotou, C
Kusenko, A
Labanti, C
Lieu, R
Macculi, C
Makishima, K
Matt, G
Mazzotta, P
McCammon, D
Mendez, M
Mineo, T
Mitchell, S
Mitsuda, K
Molendi, S
Moscardini, L
Mushotzky, R
Natalucci, L
Nicastro, F
O'Brien, P
Osborne, J
Paerels, F
Page, M
Paltani, S
Pareschi, G
Perinati, E
Perola, C
Ponman, T
Rasmussen, A
Roncarelli, M
Rosati, P
Ruchayskiy, O
Quadrini, E
Sakurai, I
Salvaterra, R
Sasaki, S
Sato, G
Schaye, J
Schmitt, J
Sciortino, S
Shaposhnikov, M
Shinozaki, K
Spiga, D
Suto, Y
Tagliaferri, G
Takahashi, T
Takei, Y
Tawara, Y
Tozzi, P
Tsunemi, H
Tsuru, T
Ubertini, P
Ursino, E
Viel, M
Vink, J
White, N
Willingale, R
Wijers, R
Yoshikawa, K
Yamasaki, N
AF Piro, L.
den Herder, J. W.
Ohashi, T.
Amati, L.
Atteia, J. L.
Barthelmy, S.
Barbera, M.
Barret, D.
Basso, S.
Boer, M.
Borgani, S.
Boyarskiy, O.
Branchini, E.
Branduardi-Raymont, G.
Briggs, M.
Brunetti, G.
Budtz-Jorgensen, C.
Burrows, D.
Campana, S.
Caroli, E.
Chincarini, G.
Christensen, F.
Cocchi, M.
Comastri, A.
Corsi, A.
Cotroneo, V.
Conconi, P.
Colasanti, L.
Cusumano, G.
de Rosa, A.
Del Santo, M.
Ettori, S.
Ezoe, Y.
Ferrari, L.
Feroci, M.
Finger, M.
Fishman, G.
Fujimoto, R.
Galeazzi, M.
Galli, A.
Gatti, F.
Gehrels, N.
Gendre, B.
Ghirlanda, G.
Ghisellini, G.
Giommi, P.
Girardi, M.
Guzzo, L.
Haardt, F.
Hepburn, I.
Hermsen, W.
Hoevers, H.
Holland, A.
in't Zand, J.
Ishisaki, Y.
Kawahara, H.
Kawai, N.
Kaastra, J.
Kippen, M.
de Korte, P. A. J.
Kouveliotou, C.
Kusenko, A.
Labanti, C.
Lieu, R.
Macculi, C.
Makishima, K.
Matt, G.
Mazzotta, P.
McCammon, D.
Mendez, M.
Mineo, T.
Mitchell, S.
Mitsuda, K.
Molendi, S.
Moscardini, L.
Mushotzky, R.
Natalucci, L.
Nicastro, F.
O'Brien, P.
Osborne, J.
Paerels, F.
Page, M.
Paltani, S.
Pareschi, G.
Perinati, E.
Perola, C.
Ponman, T.
Rasmussen, A.
Roncarelli, M.
Rosati, P.
Ruchayskiy, O.
Quadrini, E.
Sakurai, I.
Salvaterra, R.
Sasaki, S.
Sato, G.
Schaye, J.
Schmitt, J.
Sciortino, S.
Shaposhnikov, M.
Shinozaki, K.
Spiga, D.
Suto, Y.
Tagliaferri, G.
Takahashi, T.
Takei, Y.
Tawara, Y.
Tozzi, P.
Tsunemi, H.
Tsuru, T.
Ubertini, P.
Ursino, E.
Viel, M.
Vink, J.
White, N.
Willingale, R.
Wijers, R.
Yoshikawa, K.
Yamasaki, N.
TI EDGE: Explorer of diffuse emission and gamma-ray burst explosions
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE X-rays; Cosmology; Clusters; Gamma-ray bursts; Warm-hot intergalactic
medium; Missions
ID GALAXY CLUSTERS; ABSORPTION; TEMPERATURE
AB How structures of various scales formed and evolved from the early Universe up to present time is a fundamental question of astrophysical cosmology. EDGE (Piro et al., 2007) will trace the cosmic history of the baryons from the early generations of massive stars by Gamma-Ray Burst (GRB) explosions, through the period of galaxy cluster formation, down to the very low redshift Universe, when between a third and one half of the baryons are expected to reside in cosmic filaments undergoing gravitational collapse by dark matter (the so-called warm hot intragalactic medium). In addition EDGE, with its unprecedented capabilities, will provide key results in many important fields. These scientific goals are feasible with a medium class mission using existing technology combined with innovative instrumental and observational capabilities by: (a) observing with fast reaction Gamma-Ray Bursts with a high spectral resolution. This enables the study of their star-forming and host galaxy environments and the use of GRBs as back lights of large scale cosmological structures; (b) observing and surveying extended sources (galaxy clusters, WHIM) with high sensitivity using two wide field of view X-ray telescopes (one with a high angular resolution and the other with a high spectral resolution). The mission concept includes four main instruments: a Wide-field Spectrometer (0.1-2.2 eV) with excellent energy resolution (3 eV at 0.6 keV), a Wide-Field Imager (0.3-6 keV) with high angular resolution (HPD = 15") constant over the full 1.4 degree field of view, and a Wide Field Monitor (8-200 keV) with a FOV of A1/4 of the sky, which will trigger the fast repointing to the GRB. Extension of its energy response up to 1 MeV will be achieved with a GRB detector with no imaging capability. This mission is proposed to ESA as part of the Cosmic Vision call. We will outline the science drivers and describe in more detail the payload of this mission.
C1 [Piro, L.; Cocchi, M.; Corsi, A.; Colasanti, L.; de Rosa, A.; Del Santo, M.; Feroci, M.; Galli, A.; Gendre, B.; Macculi, C.; Natalucci, L.; Ubertini, P.] Ist Astrofis Spaziale Fis Cosm, INAF, Rome, Italy.
[den Herder, J. W.; Hermsen, W.; Hoevers, H.; in't Zand, J.; Kaastra, J.; de Korte, P. A. J.; Mendez, M.; Takei, Y.] SRON Netherlands Inst Space Res, SRON, NL-3854 CA Utrecht, Netherlands.
[Ohashi, T.; Sasaki, S.; Shinozaki, K.] Tokyo Metropolitan Univ, Tokyo 158, Japan.
[Amati, L.; Caroli, E.; Labanti, C.] Ist Astrofis Spaziale Fis Cosm, INAF, Bologna, Italy.
[Barthelmy, S.; Gehrels, N.; Mushotzky, R.; Sato, G.; White, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cusumano, G.; Mineo, T.; Perinati, E.] Ist Astrofis Spaziale Fis Cosm, INAF, Palermo, Italy.
[Atteia, J. L.] Observ Midi Pyrenees, LAT, F-31400 Toulouse, France.
[Barret, D.] Ctr Etud Spatiale Rayonnements, Toulouse, France.
[Basso, S.; Campana, S.; Chincarini, G.; Cotroneo, V.; Conconi, P.; Ghirlanda, G.; Ghisellini, G.; Guzzo, L.; Pareschi, G.; Spiga, D.; Tagliaferri, G.] Osserv Astron Brera, INAF, Milan, Italy.
[Borgani, S.; Girardi, M.; Tozzi, P.; Viel, M.] Osserv Astron Trieste, INAF, Trieste, Italy.
[Branchini, E.; Matt, G.; Perola, C.] Univ Roma III, Rome, Italy.
[Briggs, M.; Lieu, R.] Univ Alabama Huntsville, Huntsville, AL USA.
[Budtz-Jorgensen, C.; Christensen, F.] Tech Univ Denmark, DNSC, Copenhagen, Denmark.
[Burrows, D.] Penn State Univ, Philadelphia, PA USA.
[Comastri, A.; Ettori, S.; Roncarelli, M.] Osservatorio Astron Bologna, INAF, Bologna, Italy.
[Ferrari, L.; Gatti, F.] Ist Nazl Fis Nucl, I-16146 Genoa, Italy.
[Finger, M.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
[Fishman, G.; Kouveliotou, C.; Mitchell, S.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Galeazzi, M.; Ursino, E.] Univ Miami, Miami, FL USA.
[Ishisaki, Y.; Sakurai, I.; Tawara, Y.] Nagoya Univ, Nagoya, Aichi 4648601, Japan.
[Kawai, N.] Tokyo Inst Technol, Tokyo 152, Japan.
[Kippen, M.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Ezoe, Y.; Fujimoto, R.; Mitsuda, K.; Takahashi, T.; Yamasaki, N.] JAXA, Inst Space & Aeronaut Sci, Tokyo, Japan.
[Molendi, S.; Quadrini, E.] Ist Astrofis Spaziale Fis Cosm, INAF, Milan, Italy.
[Rasmussen, A.] KIPAC Stand, Palo Alto, CA USA.
[Kawahara, H.; Suto, Y.; Yoshikawa, K.] Univ Tokyo, Tokyo, Japan.
[Paerels, F.] Columbia Univ, New York, NY USA.
[Schaye, J.] Leiden Univ, Leiden, Netherlands.
[Mazzotta, P.] Univ Roma Tor Vergata, Rome, Italy.
[Rosati, P.] ESO, Garching, Germany.
[Boer, M.] Observ Haute Provence, St Michel, Haute Provence, France.
[O'Brien, P.; Osborne, J.; Willingale, R.] Univ Leicester, Leicester, Leics, England.
[Wijers, R.] Univ Amsterdam, Amsterdam, Netherlands.
[Boyarskiy, O.] CERN, Geneva, Switzerland.
[Haardt, F.; Salvaterra, R.] Univ Insubria Como, Como, Italy.
[Kusenko, A.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Paltani, S.] Integral Sci Data Ctr, Versoix, Switzerland.
[Ruchayskiy, O.] Inst Hautes Etud Sci, F-91440 Bures Sur Yvette, France.
[Shaposhnikov, M.] Ecole Polytech Fed Lausanne, Lausanne, Switzerland.
[Schmitt, J.] Univ Hamburg, Hamburg, Germany.
[Tsuru, T.] Kyoto Univ, Kyoto, Japan.
[Vink, J.] Univ Utrecht, Utrecht, Netherlands.
[Giommi, P.] ASI Data Ctr, Rome, Italy.
[Makishima, K.] Tokyo Univ Sci, Tokyo 162, Japan.
[McCammon, D.] Univ Wisconsin, Madison, WI USA.
[Tsunemi, H.] Osaka Univ, Osaka, Japan.
[Brunetti, G.] IRA Bologna, INAF, Bologna, Italy.
[Moscardini, L.] Univ Bologna, Bologna, Italy.
[Barbera, M.] Univ Palermo, Dipartimento Sci Fis & Astron, Palermo, Italy.
[Nicastro, F.] Osserv Astron Roma, INAF, I-00136 Rome, Italy.
[Sciortino, S.] Osserv Astron Palermo, INAF, Palermo, Italy.
[Ponman, T.] Univ Birmingham, Birmingham, W Midlands, England.
[Branduardi-Raymont, G.; Hepburn, I.; Page, M.] UCL, Mullard Space Sci Lab, London, England.
[Holland, A.] Brunel Univ, London, England.
RP Piro, L (reprint author), Ist Astrofis Spaziale Fis Cosm, INAF, Rome, Italy.
EM luigi.piro@iasf-roma.inaf.it
RI Mazzotta, Pasquale/B-1225-2016; Caroli, Ezio/G-1427-2012; Yamasaki,
Noriko/C-2252-2008; White, Nicholas/B-6428-2012; Barthelmy,
Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Mendez,
Mariano/C-8011-2012; Gatti, Flavio/K-4568-2013; gendre,
bruce/O-2923-2013; PIRO, LUIGI/E-4954-2013; Mitsuda,
Kazuhisa/C-2649-2008; Ruchayskiy, Oleg/E-3698-2015; Ettori,
Stefano/N-5004-2015; Amati, Lorenzo/N-5586-2015; Comastri,
Andrea/O-9543-2015
OI Borgani, Stefano/0000-0001-6151-6439; Molendi,
Silvano/0000-0002-2483-278X; Tagliaferri, Gianpiero/0000-0003-0121-0723;
Schaye, Joop/0000-0002-0668-5560; Ghirlanda,
Giancarlo/0000-0001-5876-9259; Ghisellini, Gabriele/0000-0002-0037-1974;
giommi, paolo/0000-0002-2265-5003; Barbera, Marco/0000-0002-3188-7420;
Wijers, Ralph/0000-0002-3101-1808; Nicastro,
Fabrizio/0000-0002-6896-1364; Salvaterra, Ruben/0000-0002-9393-8078;
Pareschi, Giovanni/0000-0003-3967-403X; Macculi,
Claudio/0000-0002-7887-1485; Branchini, Enzo/0000-0002-0808-6908;
Mazzotta, Pasquale/0000-0002-5411-1748; Spiga,
Daniele/0000-0003-1163-7843; Caroli, Ezio/0000-0001-8468-7433; Del
Santo, Melania/0000-0002-1793-1050; Viel, Matteo/0000-0002-2642-5707;
Mineo, Teresa/0000-0002-4931-8445; Labanti, Claudio/0000-0002-5086-3619;
Feroci, Marco/0000-0002-7617-3421; Cusumano,
Giancarlo/0000-0002-8151-1990; Brunetti, Gianfranco/0000-0003-4195-8613;
White, Nicholas/0000-0003-3853-3462; Mendez,
Mariano/0000-0003-2187-2708; gendre, bruce/0000-0002-9077-2025; PIRO,
LUIGI/0000-0003-4159-3984; Ruchayskiy, Oleg/0000-0001-8073-3068; Ettori,
Stefano/0000-0003-4117-8617; Amati, Lorenzo/0000-0001-5355-7388;
Comastri, Andrea/0000-0003-3451-9970
FU Italian space agency (ASI)
FX The EDGE mission has been proposed to ESA as a medium class mission in
the Cosmic Vision program. A large group of scientist from Europe, Japan
and the USA has contributed to this proposal (see
http://projects.iasf-roma.inaf.it/edge for the proposal proper). In
addition the authors like to acknowledge the support of the Italian
space agency (ASI) and the assistance of Thales Alenia Space for
detailed technical assessment.
NR 20
TC 16
Z9 16
U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 1
BP 67
EP 89
DI 10.1007/s10686-008-9092-y
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KZ
UT WOS:000263505900005
ER
PT J
AU Arnaud, M
Barcons, X
Barret, D
Bautz, M
Bellazzini, R
Bleeker, J
Bohringer, H
Boller, T
Brandt, WN
Cappi, M
Carrera, F
Comastri, A
Costa, E
Courvoisier, T
de Korte, P
Dwelly, T
Fabian, A
Flanagan, K
Gilli, R
Griffiths, R
Hasinger, G
Kaastra, J
Kahn, S
Kelley, R
Kunieda, H
Makishima, K
Matt, G
Mendez, M
Mitsuda, K
Nandra, K
Ohashi, T
Page, M
Palumbo, G
Pavlinsky, M
Sciortino, S
Smith, A
Struder, L
Takahashi, T
Turler, M
Turler, M
Ueda, Y
Vignali, C
Vink, J
Warwick, R
Watson, M
Willingale, R
Zhang, SN
AF Arnaud, Monique
Barcons, Xavier
Barret, Didier
Bautz, Marshall
Bellazzini, Ronaldo
Bleeker, Johan
Boehringer, Hans
Boller, Thomas
Brandt, William Nielsen
Cappi, Massimo
Carrera, Francisco
Comastri, Andrea
Costa, Enrico
Courvoisier, Thierry
de Korte, Piet
Dwelly, Tom
Fabian, Andrew
Flanagan, Kathryn
Gilli, Roberto
Griffiths, Richard
Hasinger, Gunther
Kaastra, Jelle
Kahn, Steve
Kelley, Richard
Kunieda, Hideyo
Makishima, Kazuo
Matt, Giorgio
Mendez, Mariano
Mitsuda, Kazuhisa
Nandra, Kirpal
Ohashi, Takaya
Page, Mathew
Palumbo, Giorgio
Pavlinsky, Mikhail
Sciortino, Salvatore
Smith, Alan
Strueder, Lothar
Takahashi, Tadayuki
Tuerler, Marc
Tuerner, Martin
Ueda, Yoshihiro
Vignali, Cristian
Vink, Jacco
Warwick, Robert
Watson, Mike
Willingale, Richard
Zhang, Shuang Nan
TI XEUS: the physics of the hot evolving universe
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE XEUS; Cosmic vision; X-ray astronomy
ID BLACK-HOLES; RAY; SPECTRUM; DETECTOR; OPTICS
AB This paper describes the next generation X-ray observatory XEUS which has been submitted to the European Space Agency in the framework of the Cosmic Vision 2015-2025 competition and has been selected for an assessment study. The paper summarizes the scientific goals and instrumental concepts of the proposed X-ray telescope with 5 m(2) effective area and angular resolution better than 5 arc sec.
C1 [Arnaud, Monique] CEA Saclay, CEA, DSM, DAPNIA,SAP, F-91191 Gif Sur Yvette, France.
[Barcons, Xavier; Carrera, Francisco] CSIC UC, IFCA, Santander, Spain.
[Barret, Didier] UPS, CNRS, CESR, Toulouse, France.
[Bautz, Marshall] MIT, Cambridge, MA 02139 USA.
[Bellazzini, Ronaldo] Ist Nazl Fis Nucl, Pisa, Italy.
[Bleeker, Johan; de Korte, Piet; Kaastra, Jelle] U Utrecht, SRON, Utrecht, Netherlands.
[Boehringer, Hans; Boller, Thomas; Hasinger, Gunther; Strueder, Lothar] MPE, Garching, Germany.
[Brandt, William Nielsen] Penn State Univ, University Pk, PA 16802 USA.
[Cappi, Massimo] IASF, INAF, Bologna, Italy.
[Comastri, Andrea; Gilli, Roberto] Oss Astron Bologna, INAF, Bologna, Italy.
[Costa, Enrico] IASF, INAF, Rome, Italy.
[Courvoisier, Thierry; Tuerler, Marc] ISDC, Geneva, Switzerland.
[Flanagan, Kathryn] STScI, Baltimore, MD USA.
[Griffiths, Richard] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA.
[Kahn, Steve] Stanford Univ, SLAC, KIPAC, Stanford, CA 94305 USA.
[Kelley, Richard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kunieda, Hideyo] Nagoya Univ, Nagoya, Aichi 4648601, Japan.
[Makishima, Kazuo] Univ Tokyo, Tokyo, Japan.
[Matt, Giorgio] U Roma Tre, Rome, Italy.
[Mendez, Mariano] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands.
[Mitsuda, Kazuhisa; Takahashi, Tadayuki] JAXA, ISAS, Sagamihara, Kanagawa, Japan.
[Ohashi, Takaya] Tokyo Metropolitan Univ, Tokyo 158, Japan.
[Page, Mathew; Smith, Alan] UCL, MSSL, Dorking, Surrey, England.
[Palumbo, Giorgio; Vignali, Cristian] Univ Bologna, Bologna, Italy.
[Pavlinsky, Mikhail] IKI, Moscow, Russia.
[Sciortino, Salvatore] Oss Astron, INAF, Palermo, Italy.
[Tuerner, Martin; Warwick, Robert; Watson, Mike; Willingale, Richard] Univ Leicester, Leicester, Leics, England.
[Ueda, Yoshihiro] Kyoto Univ, Kyoto, Japan.
[Vink, Jacco] Univ Utrecht, Utrecht, Netherlands.
[Zhang, Shuang Nan] Tsinghua Univ, IHEP, Beijing 100084, Peoples R China.
[Nandra, Kirpal] Univ London Imperial Coll Sci Technol & Med, London, England.
[Dwelly, Tom] Univ Southampton, Southampton SO9 5NH, Hants, England.
[Fabian, Andrew] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
RP Gilli, R (reprint author), Oss Astron Bologna, INAF, Bologna, Italy.
EM roberto.gilli@oabo.inaf.it
RI Vignali, Cristian/J-4974-2012; Mendez, Mariano/C-8011-2012; Mitsuda,
Kazuhisa/C-2649-2008; Barcons, Xavier/L-3335-2014; Cappi,
Massimo/F-4813-2015; Brandt, William/N-2844-2015; Comastri,
Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015;
OI Vignali, Cristian/0000-0002-8853-9611; Mendez,
Mariano/0000-0003-2187-2708; Barcons, Xavier/0000-0003-1081-8861;
Brandt, William/0000-0002-0167-2453; Comastri,
Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Costa,
Enrico/0000-0003-4925-8523; Cappi, Massimo/0000-0001-6966-8920
FU XEUS Science Advisory Group; ESA International Space Station
FX The authors wish to express their appreciation to all those scientists
who supported XEUS throughout the years and contributed with suggestions
and constructive criticism to the writing of this final proposal. Each
author acknowledges partial financial support from their national
institutions and agencies from the birth of the original idea to the
completion of the proposal, and A. Parmar for acting as a very helpful
secretary of the XEUS Science Advisory Group. G. G. C. P. gratefully
acknowledges the enthusiastic support from ESA International Space
Station department during the early phases of the XEUS concept growth.
Without their help XEUS probably would have never made it to
successfully respond to the Cosmic Vision call.
NR 23
TC 4
Z9 4
U1 1
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 1
BP 139
EP 168
DI 10.1007/s10686-008-9104-y
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KZ
UT WOS:000263505900008
ER
PT J
AU Swinyard, B
Nakagawa, T
Merken, P
Royer, P
Souverijns, T
Vandenbussche, B
Waelkens, C
Davis, P
Di Francesco, J
Halpern, M
Houde, M
Johnstone, D
Joncas, G
Naylor, D
Plume, R
Scott, D
Abergel, A
Bensammar, S
Braine, J
Buat, V
Burgarella, D
Cais, P
Dole, H
Duband, L
Elbaz, D
Gerin, M
Giard, M
Goicoechea, J
Joblin, C
Jones, A
Kneib, JP
Lagache, G
Madden, S
Pons, R
Pajot, F
Rambaud, D
Ravera, L
Ristorcelli, I
Rodriguez, L
Vives, S
Zavagno, A
Geis, N
Krause, O
Lutz, D
Poglitsch, A
Raab, W
Stegmaier, J
Sturm, E
Tuffs, R
Lee, HM
Koo, BC
Im, M
Pak, S
Han, W
Park, JH
Nam, UW
Jin, H
Lee, DH
Yuk, IS
Lee, S
Aikawa, Y
Arimoto, N
Doi, Y
Enya, K
Fukagawa, M
Furusho, R
Hasegawa, S
Hayashi, M
Honda, M
Ida, S
Imanishi, M
Inutsuka, S
Izumiura, H
Kamaya, H
Kaneda, H
Kasuga, T
Kataza, H
Kawabata, K
Kawada, M
Kawakita, H
Kii, T
Koda, J
Kodama, T
Kokubo, E
Komatsu, K
Matsuhara, H
Matsumoto, T
Matsuura, S
Miyata, T
Murakam, H
Nagata, H
Nagata, T
Nakajima, T
Naoto, K
Nishi, R
Noda, A
Okamoto, A
Okamoto, YK
Omukai, K
Onaka, T
Ootsubo, T
Ouchi, M
Saito, H
Sato, Y
Sako, S
Sekiguchi, T
Shibai, H
Sugita, H
Sugitani, K
Susa, H
Tae-soo, P
Tamura, M
Ueda, Y
Ueno, M
Wada, T
Watanabe, J
Yamada, T
Yamamura, I
Yoshida, N
Yoshimi, K
Yui, Y
Benedettini, M
Cerulli, R
Di Giorgio, A
Molinari, S
Orfei, R
Pezzuto, S
Piazzo, L
Saraceno, P
Spinoglio, L
de Graauw, T
de Korte, P
Helmich, F
Hoevers, H
Huisman, R
Shipman, R
van der Tak, F
van der Werf, P
Wild, W
Acosta-Pulido, J
Cernicharo, J
Herreros, J
Martin-Pintado, J
Najarro, F
Perez-Fourmon, I
Pardo, JR
Gomez, F
Rodriguez, NC
Ade, P
Barlow, M
Clements, D
Ferlet, M
Fraser, H
Griffin, D
Griffin, M
Hargrave, P
Isaak, K
Ivison, R
Mansour, M
Laniesse, J
Mauskopf, P
Morozov, D
Oliver, S
Orlando, A
Page, M
Popescu, C
Serjeant, S
Sudiwala, R
Rigopoulou, D
Walker, I
White, G
Viti, S
Winter, B
Bock, J
Bradford, M
Harwit, M
Holmes, W
AF Swinyard, Bruce
Nakagawa, Takao
Merken, Patrick
Royer, Pierre
Souverijns, Tim
Vandenbussche, Bart
Waelkens, Christoffel
Davis, Peter
Di Francesco, James
Halpern, Mark
Houde, Martin
Johnstone, Doug
Joncas, Gilles
Naylor, David
Plume, Rene
Scott, Douglas
Abergel, A.
Bensammar, S.
Braine, J.
Buat, V.
Burgarella, D.
Cais, Ph.
Dole, H.
Duband, L.
Elbaz, D.
Gerin, M.
Giard, M.
Goicoechea, J.
Joblin, C.
Jones, A.
Kneib, J. P.
Lagache, G.
Madden, S.
Pons, R.
Pajot, F.
Rambaud, D.
Ravera, L.
Ristorcelli, I.
Rodriguez, L.
Vives, S.
Zavagno, A.
Geis, Norbert
Krause, Oliver
Lutz, Dieter
Poglitsch, Albrecht
Raab, Walfried
Stegmaier, Jutta
Sturm, Eckhard
Tuffs, Richard
Lee, Hyung Mok
Koo, Bon-Chul
Im, Myungshin
Pak, Soojong
Han, Wonyong
Park, Jang-Hyun
Nam, Uk-Won
Jin, Ho
Lee, Dae-Hee
Yuk, In-Soo
Lee, Sungho
Aikawa, Yuri
Arimoto, Nobuo
Doi, Yasuo
Enya, Keigo
Fukagawa, Misato
Furusho, Reiko
Hasegawa, Sunao
Hayashi, Masahiko
Honda, Mitsuhiko
Ida, Shigeru
Imanishi, Masatoshi
Inutsuka, Shu-ichiro
Izumiura, Hideyuki
Kamaya, Hideyuki
Kaneda, Hidehiro
Kasuga, Toshihiro
Kataza, Hirokazu
Kawabata, Koji
Kawada, Mitsunobu
Kawakita, Hideyo
Kii, Tsuneo
Koda, Jin
Kodama, Tadayuki
Kokubo, Eiichiro
Komatsu, Keiji
Matsuhara, Hideo
Matsumoto, Toshio
Matsuura, Shuji
Miyata, Takashi
Murakam, Hiroshi
Nagata, Hirohisa
Nagata, Tetsuya
Nakajima, Tadashi
Naoto, Kobayashi
Nishi, Ryoichi
Noda, Atsushi
Okamoto, Atsushi
Okamoto, Yoshiko K.
Omukai, Kazuyuki
Onaka, Takashi
Ootsubo, Takafumi
Ouchi, Masami
Saito, Hirobumi
Sato, Yoichi
Sako, Shigeyuki
Sekiguchi, Tomohiko
Shibai, Hiroshi
Sugita, Hiroyuki
Sugitani, Koji
Susa, Hajime
Tae-soo, Pyo
Tamura, Motohide
Ueda, Yoshihiro
Ueno, Munetaka
Wada, Takehiko
Watanabe, Jun'ichi
Yamada, Toru
Yamamura, Issei
Yoshida, Naoki
Yoshimi, Kitamura
Yui, Yukari
Benedettini, Milena
Cerulli, Riccardo
Di Giorgio, Anna
Molinari, Sergio
Orfei, Renato
Pezzuto, Stefano
Piazzo, Lorenzo
Saraceno, Paolo
Spinoglio, Luigi
de Graauw, Thijs
de Korte, Piet
Helmich, Frank
Hoevers, Henk
Huisman, Robert
Shipman, Russell
van der Tak, Floris
van der Werf, Paul
Wild, Wolfgang
Acosta-Pulido, Jose
Cernicharo, Jose
Herreros, Jose
Martin-Pintado, Jesus
Najarro, Francisco
Perez-Fourmon, Ismael
Ramon Pardo, Juan
Gomez, Francisca
Castro Rodriguez, Nieves
Ade, Peter
Barlow, Mike
Clements, David
Ferlet, Marc
Fraser, Helen
Griffin, Douglas
Griffin, Matthew
Hargrave, Peter
Isaak, Kate
Ivison, Robert
Mansour, Malik
Laniesse, Jonathan
Mauskopf, Phillip
Morozov, Dmitry
Oliver, Seb
Orlando, Angiola
Page, Mathew
Popescu, Cristina
Serjeant, Stephen
Sudiwala, Rashmi
Rigopoulou, Dimitra
Walker, Ian
White, Glenn
Viti, Serena
Winter, Berend
Bock, Jamie
Bradford, Matt
Harwit, Martin
Holmes, Warren
CA SPICA Consortium
TI The space infrared telescope for cosmology and astrophysics: SPICA A
joint mission between JAXA and ESA
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Space missions; Infrared
ID POLYCYCLIC AROMATIC-HYDROCARBON; SUBMILLIMETER GALAXIES; STAR-FORMATION;
SPITZER; MODEL; EMISSION; SPECTRUM; UNIVERSE; PAHS; IR
AB The Space Infrared telescope for Cosmology and Astrophysics (SPICA) is planned to be the next space astronomy mission observing in the infrared. The mission is planned to be launched in 2017 and will feature a 3.5 m telescope cooled to < 5 K through the use of mechanical coolers. These coolers will also cool the focal plane instruments thus avoiding the use of consumables and giving the mission a long lifetime. SPICA's large, cold aperture will provide a two order of magnitude sensitivity advantage over current far infrared facilities (> 30 microns wavelength). We describe the scientific advances that will be made possible by this large increase in sensitivity and give details of the mission, spacecraft and focal plane conceptual design.
C1 [Swinyard, Bruce] Rutherford Appleton Lab, Sci & Technol Facil Council, Didcot OX11 0QX, Oxon, England.
[Nakagawa, Takao] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Davis, Peter] BlueSky Spect Inc, Lethbridge, AB, Canada.
[Koda, Jin] CALTECH, Pasadena, CA 91125 USA.
[Ade, Peter; Griffin, Matthew; Hargrave, Peter; Isaak, Kate; Mauskopf, Phillip; Morozov, Dmitry; Orlando, Angiola; Sudiwala, Rashmi; Walker, Ian] Cardiff Univ, Cardiff CF10 3AX, S Glam, Wales.
[Duband, L.] CEA Grenoble, CENG, Serv Basses Temp, F-38054 Grenoble, France.
[Elbaz, D.; Madden, S.; Rodriguez, L.] CEA Saclay, DAPNIA, Serv Astrophys, Saclay, France.
[Giard, M.; Joblin, C.; Pons, R.; Rambaud, D.; Ravera, L.; Ristorcelli, I.] Univ Toulouse 3, CNRS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France.
[Harwit, Martin] Cornell Univ, Ithaca, NY 14853 USA.
[Cernicharo, Jose; Martin-Pintado, Jesus; Najarro, Francisco; Ramon Pardo, Juan; Gomez, Francisca; Castro Rodriguez, Nieves] CSIC, IEM, Dept Astrofas Mol & InfraRoja, Madrid, Spain.
[Bensammar, S.] CNRS, Observ Paris, GEPI, F-75700 Paris, France.
[van der Tak, Floris] Univ Groningen, NL-9700 AB Groningen, Netherlands.
Gunma Astron Observ, Agatsuma, Gunma, Japan.
[Di Francesco, James; Johnstone, Doug] Herzberg Inst Astrophys, Victoria, BC, Canada.
[Kawabata, Koji] Hiroshima Univ, Hiroshima 730, Japan.
[Okamoto, Yoshiko K.] Ibaraki Univ, Mito, Ibaraki, Japan.
[Merken, Patrick; Souverijns, Tim] IMEC RMA, Leuven, Belgium.
[Clements, David] Univ London Imperial Coll Sci Technol & Med, London, England.
CNRS, Inst Astrophys Paris, Paris, France.
[Abergel, A.; Dole, H.; Jones, A.; Lagache, G.; Pajot, F.] CNRS Paris XI, Inst Astrophys Spatiale, Orsay, France.
[Royer, Pierre; Vandenbussche, Bart; Waelkens, Christoffel] Katholieke Univ Leuven, Inst Sterrenkunde, Leuven, Belgium.
[Benedettini, Milena; Cerulli, Riccardo; Di Giorgio, Anna; Molinari, Sergio; Orfei, Renato; Pezzuto, Stefano; Saraceno, Paolo; Spinoglio, Luigi] Ist Fis Spazio Interplanetario, Rome, Italy.
[Enya, Keigo; Hasegawa, Sunao; Kaneda, Hidehiro; Kataza, Hirokazu; Kii, Tsuneo; Komatsu, Keiji; Matsuhara, Hideo; Matsumoto, Toshio; Matsuura, Shuji; Murakam, Hiroshi; Nagata, Hirohisa; Noda, Atsushi; Okamoto, Atsushi; Saito, Hirobumi; Sato, Yoichi; Sugita, Hiroyuki; Wada, Takehiko; Yamamura, Issei; Yoshimi, Kitamura; Yui, Yukari] Japan Aerosp Explorat Agcy, Chofu, Tokyo, Japan.
[Bock, Jamie; Bradford, Matt; Holmes, Warren] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Han, Wonyong; Park, Jang-Hyun; Nam, Uk-Won; Jin, Ho; Lee, Dae-Hee; Yuk, In-Soo; Lee, Sungho] Korea Astron & Space Sci Inst, Daejon, South Korea.
[Aikawa, Yuri] Kobe Univ, Kobe, Hyogo 657, Japan.
[Kawakita, Hideyo] Kyoto Sangyo Univ, Kyoto 603, Japan.
[Inutsuka, Shu-ichiro; Kamaya, Hideyuki; Nagata, Tetsuya; Ueda, Yoshihiro] Kyoto Univ, Kyoto, Japan.
[Pak, Soojong] Kyung Hee Univ, Seoul, South Korea.
[Braine, J.; Cais, Ph.] CNRS, OASU, Lab Astrophys Bordeaux, Bordeaux, France.
CNRS, OAMP, Lab Astrophys Marseille, Marseille, France.
[de Graauw, Thijs; van der Werf, Paul] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Gerin, M.; Goicoechea, J.] CNRS, Observ Paris, LERMA, F-75700 Paris, France.
[Krause, Oliver; Stegmaier, Jutta] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Geis, Norbert; Lutz, Dieter; Poglitsch, Albrecht; Raab, Walfried; Sturm, Eckhard] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Tuffs, Richard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Page, Mathew; Winter, Berend] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
[Fukagawa, Misato; Kawada, Mitsunobu; Ootsubo, Takafumi; Shibai, Hiroshi; Sugitani, Koji; Yoshida, Naoki] Nagoya Univ, Nagoya, Aichi 4648601, Japan.
[Fukagawa, Misato; Kawada, Mitsunobu; Ootsubo, Takafumi; Shibai, Hiroshi; Sugitani, Koji; Yoshida, Naoki] Nagoya City Univ, Nagoya, Aichi, Japan.
[Arimoto, Nobuo; Furusho, Reiko; Hayashi, Masahiko; Imanishi, Masatoshi; Izumiura, Hideyuki; Kasuga, Toshihiro; Kodama, Tadayuki; Kokubo, Eiichiro; Nakajima, Tadashi; Omukai, Kazuyuki; Sekiguchi, Tomohiko; Tae-soo, Pyo; Tamura, Motohide; Watanabe, Jun'ichi; Yamada, Toru] Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo, Japan.
[de Korte, Piet; Helmich, Frank; Hoevers, Henk; Huisman, Robert; Shipman, Russell; van der Tak, Floris; Wild, Wolfgang] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[Nishi, Ryoichi] Niigata Univ, Niigata 95021, Japan.
[Susa, Hajime] Rikkyo Univ, Tokyo 171, Japan.
[Ferlet, Marc; Griffin, Douglas; Mansour, Malik; Laniesse, Jonathan; White, Glenn] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Ouchi, Masami] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Lee, Hyung Mok; Koo, Bon-Chul; Im, Myungshin] Seoul Natl Univ, Seoul, South Korea.
[Fraser, Helen] Strathclyde Univ, Glasgow, Lanark, Scotland.
[Oliver, Seb] Univ Sussex, Brighton BN1 9RH, E Sussex, England.
[Serjeant, Stephen; White, Glenn] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Ida, Shigeru] Tokyo Inst Technol, Tokyo 152, Japan.
[Ivison, Robert] UK Astron Technol Ctr, Edinburgh, Midlothian, Scotland.
Univ Rome, Rome, Italy.
[Halpern, Mark; Scott, Douglas] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada.
[Plume, Rene] Univ Calgary, Calgary, AB T2N 1N4, Canada.
[Barlow, Mike; Viti, Serena] UCL, London, England.
[Popescu, Cristina] Univ Cent Lancashire, Preston PR1 2HE, Lancs, England.
[Joncas, Gilles] Univ Laval, Quebec City, PQ, Canada.
[Naylor, David] Univ Lethbridge, Lethbridge, AB T1K 3M4, Canada.
[Rigopoulou, Dimitra] Univ Oxford, Oxford OX1 2JD, England.
[Doi, Yasuo; Miyata, Takashi; Naoto, Kobayashi; Onaka, Takashi; Sako, Shigeyuki; Ueno, Munetaka] Univ Tokyo, Tokyo 1138654, Japan.
[Houde, Martin] Univ Western Ontario, London, ON N6A 3K7, Canada.
[Acosta-Pulido, Jose; Herreros, Jose; Perez-Fourmon, Ismael] Inst Astrofis Canarias, Tenerife, Spain.
RP Swinyard, B (reprint author), Rutherford Appleton Lab, Sci & Technol Facil Council, Didcot OX11 0QX, Oxon, England.
EM b.m.swinyard@rl.ac.uk
RI Doi, Yasuo/A-3395-2013; Pak, Soojong/E-2360-2013; Doi,
Yasuo/G-2363-2011; Ivison, R./G-4450-2011; Molinari, Sergio/O-4095-2016;
Martin-Pintado, Jesus/H-6107-2015; Najarro, Francisco/G-7288-2015;
OI Doi, Yasuo/0000-0001-8746-6548; Ivison, R./0000-0001-5118-1313;
Molinari, Sergio/0000-0002-9826-7525; Martin-Pintado,
Jesus/0000-0003-4561-3508; Najarro, Francisco/0000-0002-9124-0039;
Johnstone, Doug/0000-0002-6773-459X; Scott, Douglas/0000-0002-6878-9840;
Orlando, Angiola/0000-0001-8004-5054; Barlow,
Michael/0000-0002-3875-1171
NR 33
TC 89
Z9 92
U1 5
U2 15
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 1
BP 193
EP 219
DI 10.1007/s10686-008-9090-0
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KZ
UT WOS:000263505900010
ER
PT J
AU Boulanger, F
Maillard, JP
Appleton, P
Falgarone, E
Lagache, G
Schulz, B
Wakker, BP
Bressan, A
Cernicharo, J
Charmandaris, V
Drissen, L
Helou, G
Henning, T
Lim, TL
Valentjin, E
Abergel, A
Le Bourlot, J
Bouzit, M
Cabrit, S
Combes, F
Deharveng, JM
Desmet, P
Dole, H
Dumesnil, C
Dutrey, A
Fourmond, JJ
Gavila, E
Grange, R
Gry, C
Guillard, P
Guilloteau, S
Habart, E
Huet, B
Joblin, C
Langer, M
Longval, Y
Madden, SC
Martin, C
Miville-Deschenes, MA
des Forets, GP
Pointecouteau, E
Roussel, H
Tresse, L
Verstraete, L
Viallefond, F
Bertoldi, F
Jorgensen, J
Bouwman, J
Carmona, A
Krause, O
Baruffolo, A
Bonoli, C
Bortoletto, F
Danese, L
Granato, GL
Pernechele, C
Rampazzo, R
Silva, L
de Zotti, G
Pardo, J
Spaans, M
van der Tak, FFS
Wild, W
Ferlet, MJ
Howat, SKR
Smith, MD
Swinyard, B
Wright, GS
Joncas, G
Martin, PG
Davis, CJ
Draine, BT
Goldsmith, PF
Mainzer, AK
Ogle, P
Rinehart, SA
Stacey, GJ
Tielens, AGGM
AF Boulanger, F.
Maillard, J. P.
Appleton, P.
Falgarone, E.
Lagache, G.
Schulz, B.
Wakker, B. P.
Bressan, A.
Cernicharo, J.
Charmandaris, V.
Drissen, L.
Helou, G.
Henning, T.
Lim, T. L.
Valentjin, E. A.
Abergel, A.
Le Bourlot, J.
Bouzit, M.
Cabrit, S.
Combes, F.
Deharveng, J. M.
Desmet, P.
Dole, H.
Dumesnil, C.
Dutrey, A.
Fourmond, J. J.
Gavila, E.
Grange, R.
Gry, C.
Guillard, P.
Guilloteau, S.
Habart, E.
Huet, B.
Joblin, C.
Langer, M.
Longval, Y.
Madden, S. C.
Martin, C.
Miville-Deschenes, M. A.
des Forets, G. Pineau
Pointecouteau, E.
Roussel, H.
Tresse, L.
Verstraete, L.
Viallefond, F.
Bertoldi, F.
Jorgensen, J.
Bouwman, J.
Carmona, A.
Krause, O.
Baruffolo, A.
Bonoli, C.
Bortoletto, F.
Danese, L.
Granato, G. L.
Pernechele, C.
Rampazzo, R.
Silva, L.
de Zotti, G.
Pardo, J.
Spaans, M.
van der Tak, F. F. S.
Wild, W.
Ferlet, M. J.
Howat, S. K. Ramsay
Smith, M. D.
Swinyard, B.
Wright, G. S.
Joncas, G.
Martin, P. G.
Davis, C. J.
Draine, B. T.
Goldsmith, P. F.
Mainzer, A. K.
Ogle, P.
Rinehart, S. A.
Stacey, G. J.
Tielens, A. G. G. M.
TI The molecular hydrogen explorer H2EX
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Star formation; Galaxies; ISM; Disks; Astronomical instrumentation
ID HIGH-RESOLUTION; GRATING SPECTROGRAPH; EMISSION-LINES; GALAXIES; TEXES;
H-2
AB The Molecular Hydrogen Explorer, H2EX, was proposed in response to the ESA 2015 - 2025 Cosmic Vision Call as a medium class space mission with NASA and CSA participations. The mission, conceived to understand the formation of galaxies, stars and planets from molecular hydrogen, is designed to observe the first rotational lines of the H(2) molecule (28.2, 17.0, 12.3 and 9.7 mu m) over a wide field, and at high spectral resolution. H2EX can provide an inventory of warm (a parts per thousand yen 100 K) molecular gas in a broad variety of objects, including nearby young star clusters, galactic molecular clouds, active galactic nuclei, local and distant galaxies. The rich array of molecular, atomic and ionic lines, as well as solid state features available in the 8 to 29 mu m spectral range brings additional science dimensions to H2EX. We present the optical and mechanical design of the H2EX payload based on an innovative Imaging Fourier Transform Spectrometer fed by a 1.2 m telescope. The 20'x20' field of view is imaged on two 1024x1024 Si:As detectors. The maximum resolution of 0.032 cm (-aEuro parts per thousand 1) (full width at half maximum) means a velocity resolution of 10 km s (-aEuro parts per thousand 1) for the 0 - 0 S(3) line at 9.7 mu m. This instrument offers the large field of view necessary to survey extended emission in the Galaxy and local Universe galaxies as well as to perform unbiased extragalactic and circumstellar disks surveys. The high spectral resolution makes H2EX uniquely suited to study the dynamics of H(2) in all these environments. The mission plan is made of seven wide-field spectro-imaging legacy programs, from the cosmic web to galactic young star clusters, within a nominal two years mission. The payload has been designed to re-use the Planck platform and passive cooling design.
C1 [Maillard, J. P.; Roussel, H.] CNRS, Inst Astrophys Paris, F-75014 Paris, France.
[Boulanger, F.; Lagache, G.; Abergel, A.; Bouzit, M.; Dole, H.; Dumesnil, C.; Fourmond, J. J.; Guillard, P.; Habart, E.; Langer, M.; Longval, Y.; Miville-Deschenes, M. A.; des Forets, G. Pineau; Verstraete, L.] CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Falgarone, E.; Le Bourlot, J.; Cabrit, S.; Combes, F.; Viallefond, F.] Observ Paris, F-75014 Paris, France.
[Desmet, P.; Gavila, E.; Huet, B.] Thales Alenia Space, F-06322 Cannes La Bocca, France.
[Dutrey, A.; Guilloteau, S.] Observ Bordeaux, F-33270 Floirac, France.
[Joblin, C.; Pointecouteau, E.] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France.
[Deharveng, J. M.; Grange, R.; Gry, C.; Tresse, L.] Lab Astrophys Marseille, F-13376 Marseille, France.
[Bertoldi, F.; Jorgensen, J.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Henning, T.; Bouwman, J.; Carmona, A.; Krause, O.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71003, Greece.
[Bressan, A.; Baruffolo, A.; Bonoli, C.; Bortoletto, F.; Granato, G. L.; Rampazzo, R.; de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Danese, L.] SISSA, I-34014 Trieste, Italy.
[Pernechele, C.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, CA, Italy.
[Silva, L.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
[Cernicharo, J.; Pardo, J.] CSIC, Dep Astrofis Mol & Infrarroja, Inst Estructura Mat, E-28006 Madrid, Spain.
[Valentjin, E. A.; Spaans, M.; van der Tak, F. F. S.; Wild, W.] Netherlands Inst Space Res SRON, Groningen, Netherlands.
[Lim, T. L.; Ferlet, M. J.; Swinyard, B.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Howat, S. K. Ramsay; Wright, G. S.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Drissen, L.; Joncas, G.] Univ Laval, Dept Phys Genie Phys & Opt, Quebec City, PQ G1K 7P4, Canada.
[Martin, P. G.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Appleton, P.; Schulz, B.; Helou, G.; Ogle, P.] CALTECH, IPAC, Pasadena, CA 91125 USA.
[Davis, C. J.] Joint Astron Ctr, Hilo, HI 96720 USA.
[Draine, B. T.] Princeton Univ Observ, Princeton, NJ 08544 USA.
[Goldsmith, P. F.; Mainzer, A. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rinehart, S. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tielens, A. G. G. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Stacey, G. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Wakker, B. P.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Drissen, L.; Joncas, G.] Univ Laval, Observ Mt Megant, Quebec City, PQ G1K 7P4, Canada.
[Smith, M. D.] Univ Kent, Ctr Astrophys & Planet Sci, Sch Phys Sci, Canterbury CT2 7NH, Kent, England.
[Madden, S. C.; Martin, C.] CENS, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Maillard, J. P.; Roussel, H.] Univ Paris 06, F-75014 Paris, France.
[Boulanger, F.; Lagache, G.; Abergel, A.; Bouzit, M.; Dole, H.; Dumesnil, C.; Fourmond, J. J.; Guillard, P.; Habart, E.; Langer, M.; Longval, Y.; Miville-Deschenes, M. A.; des Forets, G. Pineau; Verstraete, L.] Univ Paris 11, F-91405 Orsay, France.
RP Maillard, JP (reprint author), CNRS, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France.
EM francois.boulanger@ias.u-psud.fr; maillard@iap.fr
RI Goldsmith, Paul/H-3159-2016; Charmandaris, Vassilis/A-7196-2008;
Jorgensen, Jes Kristian/L-7936-2014; Langer, Mathieu/C-5100-2013;
OI Granato, Gian Luigi/0000-0002-4480-6909; Rampazzo,
Roberto/0000-0001-5318-9183; Baruffolo, Andrea/0000-0002-1114-4355;
Draine, Bruce/0000-0002-0846-936X; Appleton, Philip/0000-0002-7607-8766;
pernechele, claudio/0000-0002-7752-6268; Charmandaris,
Vassilis/0000-0002-2688-1956; Jorgensen, Jes
Kristian/0000-0001-9133-8047; Langer, Mathieu/0000-0002-9088-2718;
Combes, Francoise/0000-0003-2658-7893
FU Rene Laureijs at ESA; Centre National d'Etudes Spatiales (CNES)
FX The authors gratefully acknowledge help and advices from Rene Laureijs
at ESA who, as former H2EX PI, was the early initiator of the new H2EX
mission. The preparation of the proposal was supported by the Centre
National d'Etudes Spatiales (CNES).
NR 19
TC 3
Z9 3
U1 0
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 1
BP 277
EP 302
DI 10.1007/s10686-008-9108-7
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KZ
UT WOS:000263505900013
ER
PT J
AU Srama, R
Stephan, T
Grun, E
Pailer, N
Kearsley, A
Graps, A
Laufer, R
Ehrenfreund, P
Altobelli, N
Altwegg, K
Auer, S
Baggaley, J
Burchell, MJ
Carpenter, J
Colangeli, L
Esposito, F
Green, SF
Henkel, H
Horanyi, M
Jackel, A
Kempf, S
McBride, N
Moragas-Klostermeyer, G
Kruger, H
Palumbo, P
Srowig, A
Trieloff, M
Tsou, P
Sternovsky, Z
Zeile, O
Roser, HP
AF Srama, Ralf
Stephan, Thomas
Gruen, Eberhard
Pailer, Norbert
Kearsley, Anton
Graps, Amara
Laufer, Rene
Ehrenfreund, Pascale
Altobelli, Nicolas
Altwegg, Kathrin
Auer, Siegfried
Baggaley, Jack
Burchell, Mark J.
Carpenter, James
Colangeli, Luigi
Esposito, Francesca
Green, Simon F.
Henkel, Hartmut
Horanyi, Mihaly
Jaeckel, Annette
Kempf, Sascha
McBride, Neil
Moragas-Klostermeyer, Georg
Krueger, Harald
Palumbo, Pasquale
Srowig, Andre
Trieloff, Mario
Tsou, Peter
Sternovsky, Zoltan
Zeile, Oliver
Roeser, Hans-Peter
TI Sample return of interstellar matter (SARIM)
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Interstellar dust; Interplanetary dust; Collection; Interstellar medium;
Dust collector; Sample return; Chemical composition
ID POLYCYCLIC AROMATIC-HYDROCARBONS; ROSETTA SPACE MISSION; GRAIN IMPACT
ANALYZER; COMET 81P/WILD-2; DUST ACCUMULATOR; GIADA EXPERIMENT; ORBITAL
DEBRIS; EARTH; STARDUST; CASSINI
AB The scientific community has expressed strong interest to re-fly Stardust-like missions with improved instrumentation. We propose a new mission concept, SARIM, that collects interstellar and interplanetary dust particles and returns them to Earth. SARIM is optimised for the collection and discrimination of interstellar dust grains. Improved active dust collectors on-board allow us to perform in-situ determination of individual dust impacts and their impact location. This will provide important constraints for subsequent laboratory analysis.
The SARIM spacecraft will be placed at the L2 libration point of the Sun-Earth system, outside the Earth's debris belts and inside the solar-wind charging environment. SARIM is three-axes stabilised and collects interstellar grains between July and October when the relative encounter speeds with interstellar dust grains are lowest (4 to 20 km/s). During a 3-year dust collection period several hundred interstellar and several thousand interplanetary grains will be collected by a total sensitive area of 1 m(2). At the end of the collection phase seven collector modules are stored and sealed in a MIRKA-type sample return capsule. SARIM will return the capsule containing the stardust to Earth to allow for an extraction and investigation of interstellar samples by latest laboratory technologies.
C1 [Srama, Ralf; Gruen, Eberhard; Kempf, Sascha; Moragas-Klostermeyer, Georg] Max Planck Inst Nucl Phys, Heidelberg, Germany.
[Srama, Ralf; Laufer, Rene; Zeile, Oliver; Roeser, Hans-Peter] Univ Stuttgart, IRS, Stuttgart, Germany.
[Stephan, Thomas] Univ Chicago, Chicago, IL 60637 USA.
[Gruen, Eberhard; Horanyi, Mihaly; Sternovsky, Zoltan] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Pailer, Norbert] Astrium GmbH, Friedrichshafen, Germany.
[Graps, Amara] IFSI, INAF, Rome, Italy.
[Ehrenfreund, Pascale] Leiden Univ, Leiden, Netherlands.
[Altobelli, Nicolas] JPL, Pasadena, CA USA.
[Altwegg, Kathrin; Jaeckel, Annette] Univ Bern, Bern, Switzerland.
[Baggaley, Jack] Univ Canterbury, Christchurch 1, New Zealand.
[Burchell, Mark J.] Univ Kent, Canterbury, Kent, England.
[Carpenter, James] Univ Leicester, Leicester, Leics, England.
[Colangeli, Luigi; Esposito, Francesca] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Green, Simon F.; McBride, Neil] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Henkel, Hartmut] von Hoerner & Sulger GmbH, Schwetzingen, Germany.
[Kempf, Sascha] Tech Univ Carolo Wilhelmina Braunschweig, Braunschweig, Germany.
[Krueger, Harald; Tsou, Peter] MPS, Katlenburg Lindau, Germany.
[Srowig, Andre] KIP, Heidelberg, Germany.
[Trieloff, Mario] Heidelberg Univ, Heidelberg, Germany.
[Palumbo, Pasquale] Univ Parthenope, Naples, Italy.
[Auer, Siegfried] A&M Associates, Basye, VA USA.
[Kearsley, Anton] Nat Hist Museum, London SW7 5BD, England.
RP Srama, R (reprint author), Max Planck Inst Nucl Phys, Heidelberg, Germany.
EM ralf.srama@mpi-hd.mpg.de
RI Green, Simon/C-7408-2009;
OI KEMPF, SASCHA/0000-0001-5236-3004; STERNOVSKY,
ZOLTAN/0000-0002-9658-1350; Esposito, Francesca/0000-0001-9962-1648;
Horanyi, Mihaly/0000-0002-5920-9226; Burchell, Mark/0000-0002-2680-8943
NR 72
TC 7
Z9 7
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 1
BP 303
EP 328
DI 10.1007/s10686-008-9088-7
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KZ
UT WOS:000263505900014
ER
PT J
AU Schneider, J
Boccaletti, A
Mawet, D
Baudoz, P
Beuzit, JL
Doyon, R
Marley, M
Stam, D
Tinetti, G
Traub, W
Trauger, J
Aylward, A
Cho, JYK
Keller, CU
Udry, S
AF Schneider, J.
Boccaletti, A.
Mawet, D.
Baudoz, P.
Beuzit, J. -L.
Doyon, R.
Marley, M.
Stam, D.
Tinetti, G.
Traub, W.
Trauger, J.
Aylward, A.
Cho, J. Y-K.
Keller, C. -U.
Udry, S.
CA SEE-COAST Team
TI Super earth explorer: a coronagraphic off-axis space telescope
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Exoplanets; Coronagraphy
ID PHASE-MASK CORONAGRAPH; TERRESTRIAL PLANETS; EXTRASOLAR PLANETS;
ATMOSPHERE; LIGHT; POLARIZATION
AB The Super-Earth Explorer is an Off-Axis Space Telescope (SEE-COAST) designed for high contrast imaging. Its scientific objective is to make the physico-chemical characterization of exoplanets possibly down to 2 Earth radii. For that purpose it will analyze the spectral and polarimetric properties of the parent starlight reflected by the planets, in the wavelength range 400-1,250 nm.
C1 [Schneider, J.] Observ Paris, LUTH, Meudon, France.
[Boccaletti, A.; Baudoz, P.] Observ Paris, LESIA, Meudon, France.
[Mawet, D.; Marley, M.] NASA Ames, Mountain View, CA USA.
[Beuzit, J. -L.] LAOG, Grenoble, France.
[Doyon, R.] U Montreal, Montreal, PQ, Canada.
[Stam, D.] SRON Utrecht, Utrecht, Netherlands.
[Traub, W.; Trauger, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Keller, C. -U.] U Utrecht, Utrecht, Netherlands.
[Udry, S.] Observ Geneva, Geneva, Switzerland.
[Cho, J. Y-K.] U London, London, England.
[Tinetti, G.; Aylward, A.] UCL, London, England.
RP Schneider, J (reprint author), Observ Paris, LUTH, Meudon, France.
EM jean.schneider@obspm.fr
RI Marley, Mark/I-4704-2013;
OI Tinetti, Giovanna/0000-0001-6058-6654
NR 44
TC 21
Z9 21
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 1
BP 357
EP 377
DI 10.1007/s10686-008-9129-2
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KZ
UT WOS:000263505900016
ER
PT J
AU Cockell, CS
Herbst, T
Leger, A
Absil, O
Beichman, C
Benz, W
Brack, A
Chazelas, B
Chelli, A
Cottin, H
du Foresto, V
Danchi, W
Defrere, D
Den Herder, JW
Eiroa, C
Fridlund, M
Henning, T
Johnston, K
Kaltenegger, L
Labadie, L
Lammer, H
Launhardt, R
Lawson, P
Lay, OP
Liseau, R
Martin, SR
Mawet, D
Mourard, D
Moutou, C
Mugnier, L
Paresce, F
Quirrenbach, A
Rabbia, Y
Rottgering, HJA
Rouan, D
Santos, N
Selsis, F
Serabyn, E
Westall, F
White, G
Ollivier, M
Borde, P
AF Cockell, Charles S.
Herbst, Tom
Leger, Alain
Absil, O.
Beichman, Charles
Benz, Willy
Brack, Andre
Chazelas, Bruno
Chelli, Alain
Cottin, Herve
du Foresto, Vincent Coude
Danchi, William
Defrere, Denis
den Herder, Jan-Willem
Eiroa, Carlos
Fridlund, Malcolm
Henning, Thomas
Johnston, Kenneth
Kaltenegger, Lisa
Labadie, Lucas
Lammer, Helmut
Launhardt, Ralf
Lawson, Peter
Lay, Oliver P.
Liseau, Rene'
Martin, Stefan R.
Mawet, Dimitri
Mourard, Denis
Moutou, Claire
Mugnier, Laurent
Paresce, Francesco
Quirrenbach, Andreas
Rabbia, Yves
Rottgering, Huub J. A.
Rouan, Daniel
Santos, Nuno
Selsis, Franck
Serabyn, Eugene
Westall, Frances
White, Glenn
Ollivier, Marc
Borde, Pascale
TI Darwin-an experimental astronomy mission to search for extrasolar
planets
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Interferometer; Nulling interferometry; Direct imaging of exoplanets;
Exoplanets; Habitable zone
ID NULLING INTERFEROMETERS; SYSTEMATIC-ERRORS
AB As a response to ESA call for mission concepts for its Cosmic Vision 2015-2025 plan, we propose a mission called Darwin. Its primary goal is the study of terrestrial extrasolar planets and the search for life on them. In this paper, we describe different characteristics of the instrument.
C1 [Cockell, Charles S.] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England.
[Herbst, Tom; Henning, Thomas; Labadie, Lucas; Launhardt, Ralf] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Leger, Alain; Chazelas, Bruno; Ollivier, Marc; Borde, Pascale] Univ Paris 11, IAS, F-91405 Orsay, France.
[Absil, O.] Lab Astrophys Observ Grenoble, F-38400 St Martin Dheres, France.
[Beichman, Charles] CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA.
[Benz, Willy] Univ Bern, Inst Phys, Bern, Switzerland.
[Brack, Andre; Westall, Frances] CNRS, Ctr Biophys Mol, F-45071 Orleans 2, France.
[Chelli, Alain] Lab Astrophys Grenoble LAOG, F-38041 Grenoble 9, France.
[Cottin, Herve] Univ Paris 12, CNRS, UMR 7583 91, Lab Interuniv Syst Atmospher, F-94010 Creteil, France.
[du Foresto, Vincent Coude; Rouan, Daniel] Observ Paris, PHASE, LESIA, F-92190 Meudon, France.
[Danchi, William] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Defrere, Denis] Inst Astrophys & Geophys Liege, F-4000 Liege, Belgium.
[den Herder, Jan-Willem] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Eiroa, Carlos] Univ Autonoma Madrid, Fac Ciencias, Dpto Fis Toer CXI, E-28049 Madrid, Spain.
[Fridlund, Malcolm] Estec, European Space Agcy, Astrophys Mission Div, NL-2200 AG Noordwijk, Netherlands.
[Johnston, Kenneth] USN Observ, Washington, DC 20392 USA.
[Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Lawson, Peter; Lay, Oliver P.; Martin, Stefan R.; Mawet, Dimitri; Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Liseau, Rene'] Chalmers, Onsala Space Observ, SE-43992 Onsala, Sweden.
[Rabbia, Yves] CNRS, Dpt GEMINI, UMR 6203, Observ Cote Azur, F-06130 Grasse, France.
[Moutou, Claire] CNRS, LAM, F-13376 Marseille 12, France.
[Mugnier, Laurent] DOTA, ONERA, F-92322 Chatillon, France.
[Paresce, Francesco] INAF, IASF Bologna, Bologna, Italy.
[Quirrenbach, Andreas] Univ Heidelberg, ZAH, D-69117 Heidelberg, Germany.
[Rottgering, Huub J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Santos, Nuno] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Selsis, Franck] Univ Lyon, Ecole Super Lyon, CNRS, CRAL,UMR 5574, F-69007 Lyon, France.
[White, Glenn] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[White, Glenn] Rutherford Appleton Lab, CCLRC, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
RP Cockell, CS (reprint author), Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England.
EM c.s.cockell@open.ac.uk
RI Santos, Nuno/E-9957-2011; Mugnier, Laurent/A-7630-2012; Cottin,
Herve/H-5654-2013;
OI Santos, Nuno/0000-0003-4422-2919; Cottin, Herve/0000-0001-9170-5265;
Mugnier, Laurent/0000-0002-8364-4957; Absil, Olivier/0000-0002-4006-6237
NR 16
TC 29
Z9 29
U1 0
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 1
BP 435
EP 461
DI 10.1007/s10686-008-9121-x
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KZ
UT WOS:000263505900019
ER
PT J
AU Labeyrie, A
Le Coroller, H
Dejonghe, J
Lardiere, O
Aime, C
Dohlen, K
Mourard, D
Lyon, R
Carpenter, KG
AF Labeyrie, Antoine
Le Coroller, Herve
Dejonghe, Julien
Lardiere, Olivier
Aime, Claude
Dohlen, Kjetil
Mourard, Denis
Lyon, Richard
Carpenter, Kenneth G.
TI Luciola hypertelescope space observatory: versatile, upgradable
high-resolution imaging, from stars to deep-field cosmology
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Space interferometer; Hypertelescope; High-resolution; Exo-planet
ID CORONAGRAPHY; TELESCOPES; PLANETS; FUTURE; WAVE
AB Luciola is a large (1 km) "multi-aperture densified-pupil imaging interferometer", or "hypertelescope" employing many small apertures, rather than a few large ones, for obtaining direct snapshot images with a high information content. A diluted collector mirror, deployed in space as a flotilla of small mirrors, focuses a sky image which is exploited by several beam-combiner spaceships. Each contains a "pupil densifier" micro-lens array to avoid the diffractive spread and image attenuation caused by the small sub-apertures. The elucidation of hypertelescope imaging properties during the last decade has shown that many small apertures tend to be far more efficient, regarding the science yield, than a few large ones providing a comparable collecting area. For similar underlying physical reasons, radio-astronomy has also evolved in the direction of many-antenna systems such as the proposed Low Frequency Array having "hundreds of thousands of individual receivers". With its high limiting magnitude, reaching the m (v) = 30 limit of HST when 100 collectors of 25 cm will match its collecting area, high-resolution direct imaging in multiple channels, broad spectral coverage from the 1,200 A... ultra-violet to the 20 mu m infra-red, apodization, coronagraphic and spectroscopic capabilities, the proposed hypertelescope observatory addresses very broad and innovative science covering different areas of ESA's Cosmic Vision program. In the initial phase, a focal spacecraft covering the UV to near IR spectral range of EMCCD photon-counting cameras (currently 200 to 1,000 nm), will image details on the surface of many stars, as well as their environment, including multiple stars and clusters. Spectra will be obtained for each resel. It will also image neutron star, black-hole and micro-quasar candidates, as well as active galactic nuclei, quasars, gravitational lenses, and other Cosmic Vision targets observable with the initial modest crowding limit. With subsequent upgrade missions, the spectral coverage can be extended from 120 nm to 20 mu m, using four detectors carried by two to four focal spacecraft. The number of collector mirrors in the flotilla can also be increased from 12 to 100 and possibly 1,000. The imaging and spectroscopy of habitable exoplanets in the mid infra-red then becomes feasible once the collecting area reaches 6 m(2), using a specialized mid infra-red focal spacecraft. Calculations (Boccaletti et al., Icarus 145, 628-636, 2000) have shown that hypertelescope coronagraphy has unequalled sensitivity for detecting, at mid infra-red wavelengths, faint exoplanets within the exo-zodiacal glare. Later upgrades will enable the more difficult imaging and spectroscopy of these faint objects at visible wavelengths, using refined techniques of adaptive coronagraphy (Labeyrie and Le Coroller 2004). Together, the infra-red and visible spectral data carry rich information on the possible presence of life. The close environment of the central black-hole in the Milky Way will be imageable with unprecedented detail in the near infra-red. Cosmological imaging of remote galaxies at the limit of the known universe is also expected, from the ultra-violet to the near infra-red, following the first upgrade, and with greatly increasing sensitivity through successive upgrades.
These areas will indeed greatly benefit from the upgrades, in terms of dynamic range, limiting complexity of the objects to be imaged, size of the elementary "Direct Imaging Field", and limiting magnitude, approaching that of an 8-m space telescope when 1,000apertures of 25 cm are installed. Similar gains will occur for addressing fundamental problems in physics and cosmology, particularly when observing neutron stars and black holes, single or binary, including the giant black holes, with accretion disks and jets, in active galactic nuclei beyond the Milky Way. Gravitational lensing and micro-lensing patterns, including time-variable patterns and perhaps millisecond lensing flashes which may be beamed by diffraction from sub-stellar masses at sub-parsec distances (Labeyrie, Astron Astrophys 284, 689, 1994), will also be observable initially in the favourable cases, and upgrades will greatly improve the number of observable objects. The observability of gravitational waves emitted by binary lensing masses, in the form of modulated lensing patterns, is a debated issue (Ragazzoni et al., MNRAS 345, 100-110, 2003) but will also become addressable observationally. The technology readiness of Luciola approaches levels where low-orbit testing and stepwise implementation will become feasible in the 2015-2025 time frame. For the following decades beyond 2020, once accurate formation flying techniques will be mastered, much larger hypertelescopes such as the proposed 100 km Exo-Earth Imager and the 100,000 km Neutron Star Imager should also become feasible. Luciola is therefore also seen as a precursor toward such very powerful instruments.
C1 [Labeyrie, Antoine] Coll France, F-75231 Paris, France.
[Labeyrie, Antoine; Mourard, Denis] Observ Cote Azur, Caussols, France.
[Le Coroller, Herve] St Michel Observ, Observ Haute Provence, St Michel, France.
[Dejonghe, Julien] St Michel Observ, Coll France, St Michel, France.
[Lardiere, Olivier] Univ Victoria, Adapt Opt Lab, Greater Victoria, BC, Canada.
[Aime, Claude] Univ Nice Sophia Antipolis, Nice, France.
[Dohlen, Kjetil] Observ Astron Marseille Prov, Marseille, France.
[Lyon, Richard; Carpenter, Kenneth G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Labeyrie, A (reprint author), Coll France, F-75231 Paris, France.
EM antoine.labeyrie@obs-azur.fr
RI Lyon, Richard/D-5022-2012; Carpenter, Kenneth/D-4740-2012
NR 40
TC 15
Z9 15
U1 1
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 1
BP 463
EP 490
DI 10.1007/s10686-008-9123-8
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KZ
UT WOS:000263505900020
ER
PT J
AU Appourchaux, T
Burston, R
Chen, YB
Cruise, M
Dittus, H
Foulon, B
Gill, P
Gizon, L
Klein, H
Klioner, S
Kopeikin, S
Kruger, H
Lammerzahl, C
Lobo, A
Luo, XL
Margolis, H
Ni, WT
Paton, AP
Peng, QH
Peters, A
Rasel, E
Rudiger, A
Samain, E
Selig, H
Shaul, D
Sumner, T
Theil, S
Touboul, P
Turyshev, S
Wang, HT
Wang, L
Wen, LQ
Wicht, A
Wu, J
Zhang, XM
Zhao, C
AF Appourchaux, Thierry
Burston, Raymond
Chen, Yanbei
Cruise, Michael
Dittus, Hansjoerg
Foulon, Bernard
Gill, Patrick
Gizon, Laurent
Klein, Hugh
Klioner, Sergei
Kopeikin, Sergei
Krueger, Hans
Laemmerzahl, Claus
Lobo, Alberto
Luo, Xinlian
Margolis, Helen
Ni, Wei-Tou
Paton, Antonio Pulido
Peng, Qiuhe
Peters, Achim
Rasel, Ernst
Ruediger, Albrecht
Samain, Etienne
Selig, Hanns
Shaul, Diana
Sumner, Timothy
Theil, Stephan
Touboul, Pierre
Turyshev, Slava
Wang, Haitao
Wang, Li
Wen, Linqing
Wicht, Andreas
Wu, Ji
Zhang, Xiaomin
Zhao, Cheng
TI Astrodynamical Space Test of Relativity Using Optical Devices I (ASTROD
I)-A class-M fundamental physics mission proposal for Cosmic Vision
2015-2025
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Probing the fundamental laws of spacetime; Exploring the microscopic
origin of gravity; Testing relativistic gravity; Mapping solar-system
gravity; Solar g-mode detection; Gravitational-wave detection; ASTROD;
ASTROD I
ID ASTROD-I; GENERAL-RELATIVITY; LASER LINK; LISA; GRAVITY; SOLAR;
ACCELERATION; DISTURBANCES
AB ASTROD I is a planned interplanetary space mission with multiple goals. The primary aims are: to test general relativity with an improvement in sensitivity of over three orders of magnitude, improving our understanding of gravity and aiding the development of a new quantum gravity theory; to measure key solar system parameters with increased accuracy, advancing solar physics and our knowledge of the solar system; and to measure the time rate of change of the gravitational constant with an order of magnitude improvement and the anomalous Pioneer acceleration, thereby probing dark matter and dark energy gravitationally. It is an international project, with major contributions from Europe and China and is envisaged as the first in a series of ASTROD missions. ASTROD I will consist of one spacecraft carrying a telescope, four lasers, two event timers and a clock. Two-way, two-wavelength laser pulse ranging will be used between the spacecraft in a solar orbit and deep space laser stations on Earth, to achieve the ASTROD I goals. A second mission, ASTROD (ASTROD II) is envisaged as a three-spacecraft mission which would test General Relativity to 1 ppb, enable detection of solar g-modes, measure the solar Lense-Thirring effect to 10 ppm, and probe gravitational waves at frequencies below the LISA bandwidth. In the third phase (ASTROD III or Super-ASTROD), larger orbits could be implemented to map the outer solar system and to probe primordial gravitational-waves at frequencies below the ASTROD II bandwidth.
C1 [Dittus, Hansjoerg; Laemmerzahl, Claus; Selig, Hanns] Univ Bremen, Ctr Appl Space Technol & Micrograv ZARM, D-28359 Bremen, Germany.
[Appourchaux, Thierry] Ctr Univ Orsay, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Burston, Raymond; Gizon, Laurent] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Chen, Yanbei] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Cruise, Michael] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Dittus, Hansjoerg; Krueger, Hans; Theil, Stephan] German Aerosp Ctr, Inst Space Syst, D-28359 Bremen, Germany.
[Foulon, Bernard; Touboul, Pierre] Off Natl Etud & Rech Aerosp, F-92322 Chatillon, France.
[Gill, Patrick; Klein, Hugh; Margolis, Helen] Natl Phys Lab, Teddington TW11 0LW, Middx, England.
[Klioner, Sergei] Tech Univ Dresden, Inst Planetare Geodasie, Lohrmann Observatorium, D-01062 Dresden, Germany.
[Kopeikin, Sergei] Univ Missouri, Dept Phys & Astron, Columbia, MO 65221 USA.
[Lobo, Alberto] IEEC, Barcelona 08034, Spain.
[Luo, Xinlian; Peng, Qiuhe] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
[Ni, Wei-Tou; Paton, Antonio Pulido; Zhao, Cheng] Chinese Acad Sci, Purple Mt Observ, Ctr Gravitat & Cosmol, Nanjing 210008, Peoples R China.
[Peters, Achim; Wicht, Andreas] Humboldt Univ, Dept Phys, D-10117 Berlin, Germany.
[Rasel, Ernst] Leibniz Univ Hannover, Inst Quantenopt, D-30167 Hannover, Germany.
[Ruediger, Albrecht] Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany.
[Samain, Etienne] R&D Metrol, UMR Gemini, Observ Cote Azur, F-06460 Caussols, France.
[Shaul, Diana; Sumner, Timothy] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, High Energy Phys Grp, London SW7 2BZ, England.
[Turyshev, Slava] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wang, Haitao] Nanjing Univ Aeronaut & Astronaut, Nanjing 210016, Peoples R China.
[Wang, Li] China Acad Space Technol, Ctr Res & Dev, Deep Space Explorat & Space Sci Technol Res Div, Beijing 100094, Peoples R China.
[Wen, Linqing] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia.
[Wu, Ji] Chinese Acad Sci, Ctr Space Sci & Applicat Res, Beijing, Peoples R China.
[Zhang, Xiaomin] DFH Satellite Co Ltd, Beijing 100094, Peoples R China.
RP Dittus, H (reprint author), Univ Bremen, Ctr Appl Space Technol & Micrograv ZARM, D-28359 Bremen, Germany.
EM hansjoerg.dittus@dlr.de; wtni@pmo.ac.cn
RI Gizon, Laurent/B-9457-2008; Peters, Achim/G-3742-2010; Laemmerzahl,
Claus/P-3552-2016; Kopeikin, Sergei/A-8857-2009; Klioner,
Sergei/C-7927-2009; Theil, Stephan/O-2305-2015
OI Laemmerzahl, Claus/0000-0002-8276-5415; Kopeikin,
Sergei/0000-0002-4866-1532; Theil, Stephan/0000-0002-5346-8091
NR 53
TC 23
Z9 23
U1 0
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 2
BP 491
EP 527
DI 10.1007/s10686-008-9131-8
PG 37
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KW
UT WOS:000263505600001
ER
PT J
AU Christophe, B
Andersen, PH
Anderson, JD
Asmar, S
Berio, P
Bertolami, O
Bingham, R
Bondu, F
Bouyer, P
Bremer, S
Courty, JM
Dittus, H
Foulon, B
Gil, P
Johann, U
Jordan, JF
Kent, B
Lammerzahl, C
Levy, A
Metris, G
Olsen, O
Paramos, J
Prestage, JD
Progrebenko, SV
Rasel, E
Rathke, A
Reynaud, S
Rievers, B
Samain, E
Sumner, TJ
Theil, S
Touboul, P
Turyshev, S
Vrancken, P
Wolf, P
Yu, N
AF Christophe, B.
Andersen, P. H.
Anderson, J. D.
Asmar, S.
Berio, Ph.
Bertolami, O.
Bingham, R.
Bondu, F.
Bouyer, Ph.
Bremer, S.
Courty, J. -M.
Dittus, H.
Foulon, B.
Gil, P.
Johann, U.
Jordan, J. F.
Kent, B.
Laemmerzahl, C.
Levy, A.
Metris, G.
Olsen, O.
Paramos, J.
Prestage, J. D.
Progrebenko, S. V.
Rasel, E.
Rathke, A.
Reynaud, S.
Rievers, B.
Samain, E.
Sumner, T. J.
Theil, S.
Touboul, P.
Turyshev, S.
Vrancken, P.
Wolf, P.
Yu, N.
TI Odyssey: a solar system mission
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Gravitation; Relativity; Celestial mechanics; Occultations; Kuiper belt
ID POST-EINSTEINIAN TESTS; GENERAL-RELATIVITY; PIONEER 10/11; GRAVITY;
SUPERNOVAE; ACCELERATION; PRINCIPLE; ENERGY; MATTER
AB The Solar System Odyssey mission uses modern-day high-precision experimental techniques to test the laws of fundamental physics which determine dynamics in the solar system. It could lead to major discoveries by using demonstrated technologies and could be flown within the Cosmic Vision time frame. The mission proposes to perform a set of precision gravitation experiments from the vicinity of Earth to the outer Solar System. Its scientific objectives can be summarized as follows: (1) test of the gravity force law in the Solar System up to and beyond the orbit of Saturn; (2) precise investigation of navigation anomalies at the fly-bys; (3) measurement of Eddington's parameter at occultations; (4) mapping of gravity field in the outer solar system and study of the Kuiper belt. To this aim, the Odyssey mission is built up on a main spacecraft, designed to fly up to 13 AU, with the following components: (a) a high-precision accelerometer, with bias-rejection system, measuring the deviation of the trajectory from the geodesics, that is also giving gravitational forces; (b) Ka-band transponders, as for Cassini, for a precise range and Doppler measurement up to 13 AU, with additional VLBI equipment; (c) optional laser equipment, which would allow one to improve the range and Doppler measurement, resulting in particular in an improved measurement (with respect to Cassini) of the Eddington's parameter. In this baseline concept, the main spacecraft is designed to operate beyond the Saturn orbit, up to 13 AU. It experiences multiple planetary fly-bys at Earth, Mars or Venus, and Jupiter. The cruise and fly-by phases allow the mission to achieve its baseline scientific objectives [(1) to (3) in the above list]. In addition to this baseline concept, the Odyssey mission proposes the release of the Enigma radio-beacon at Saturn, allowing one to extend the deep space gravity test up to at least 50 AU, while achieving the scientific objective of a mapping of gravity field in the outer Solar System [(4) in the above list].
C1 [Christophe, B.; Foulon, B.; Levy, A.; Touboul, P.] Off Natl Etud & Rech Aerosp, F-92322 Chatillon, France.
[Andersen, P. H.; Olsen, O.] Univ Oslo, FFI, Oslo, Norway.
[Anderson, J. D.] Global Aerosp, Los Angeles, CA USA.
[Asmar, S.; Jordan, J. F.; Prestage, J. D.; Turyshev, S.; Yu, N.] JPL, NASA, Pasadena, CA USA.
[Berio, Ph.; Bondu, F.; Metris, G.; Samain, E.; Vrancken, P.] Observ Cote Azur GEMINI, Grasse, France.
[Bertolami, O.; Gil, P.; Paramos, J.] Inst Super Tecn, Lisbon, Portugal.
[Bingham, R.; Kent, B.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Bouyer, Ph.] Inst Opt Grad Sch, Palaiseau, France.
[Bremer, S.; Dittus, H.; Laemmerzahl, C.; Rievers, B.; Theil, S.] Univ Bremen, ZARM, Bremen, Germany.
[Courty, J. -M.; Reynaud, S.] UPMC, CNRS, ENS, Lab Kastler Brossel, Paris, France.
[Johann, U.; Rathke, A.] Astrium, Friedrichshafen, Germany.
[Progrebenko, S. V.] Joint Inst VLBI Europe, Dwingeloo, Netherlands.
[Rasel, E.] Leibniz Univ Hannover, Inst Quantum Opt, Hannover, Germany.
[Sumner, T. J.] Univ London Imperial Coll Sci Technol & Med, London, England.
[Wolf, P.] UPMC, CNRS, Observ Paris, LNE SYRTE, Paris, France.
RP Christophe, B (reprint author), Off Natl Etud & Rech Aerosp, BP 72, F-92322 Chatillon, France.
EM bruno.christophe@onera.fr
RI Rievers, Benny/O-6028-2016; Laemmerzahl, Claus/P-3552-2016; BOUYER,
Philippe/A-9823-2009; Bondu, Francois/A-2071-2012; Gil,
Paulo/B-7272-2012; Paramos, Jorge/J-3440-2013; Reynaud,
Serge/J-8061-2014; Theil, Stephan/O-2305-2015
OI Rievers, Benny/0000-0003-4231-9362; Laemmerzahl,
Claus/0000-0002-8276-5415; Bertolami, Orfeu/0000-0002-7672-0560;
Vrancken, Patrick/0000-0003-2364-5576; BOUYER,
Philippe/0000-0003-4458-0089; Bondu, Francois/0000-0001-6487-5197; Gil,
Paulo/0000-0003-2183-6221; Paramos, Jorge/0000-0001-9853-9431; Reynaud,
Serge/0000-0002-1494-696X; Theil, Stephan/0000-0002-5346-8091
NR 60
TC 31
Z9 31
U1 0
U2 10
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 2
BP 529
EP 547
DI 10.1007/s10686-008-9084-y
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KW
UT WOS:000263505600002
ER
PT J
AU Ertmer, W
Schubert, C
Wendrich, T
Gilowski, M
Zaiser, M
von Zoest, T
Rasel, E
Borde, CJ
Clairon, A
Laurent, P
Lemonde, P
Santarelli, G
Schleich, W
Cataliotti, FS
Inguscio, M
Poli, N
Sorrentino, F
Modugno, C
Tino, GM
Gill, P
Klein, H
Margolis, H
Reynaud, S
Salomon, C
Lambrecht, A
Peik, E
Jentsch, C
Johann, U
Rathke, A
Bouyer, P
Cacciapuoti, L
De Natale, P
Christophe, B
Foulon, B
Touboul, P
Maleki, L
Yu, N
Turyshev, SG
Anderson, JD
Schmidt-Kaler, F
Walser, R
Vigue, J
Buchner, M
Angonin, MC
Delva, P
Tourrenc, P
Bingham, R
Kent, B
Wicht, A
Wang, LJ
Bongs, K
Dittus, H
Lammerzahl, C
Theil, S
Sengstock, K
Peters, A
Muller, T
Arndt, M
Iess, L
Bondu, F
Brillet, A
Samain, E
Chiofalo, ML
Levi, F
Calonico, D
AF Ertmer, W.
Schubert, C.
Wendrich, T.
Gilowski, M.
Zaiser, M.
v. Zoest, T.
Rasel, E.
Borde, Ch. J.
Clairon, A.
Laurent, P.
Lemonde, P.
Santarelli, G.
Schleich, W.
Cataliotti, F. S.
Inguscio, M.
Poli, N.
Sorrentino, F.
Modugno, C.
Tino, G. M.
Gill, P.
Klein, H.
Margolis, H.
Reynaud, S.
Salomon, C.
Lambrecht, A.
Peik, E.
Jentsch, C.
Johann, U.
Rathke, A.
Bouyer, P.
Cacciapuoti, L.
De Natale, P.
Christophe, B.
Foulon, B.
Touboul, P.
Maleki, L.
Yu, N.
Turyshev, S. G.
Anderson, J. D.
Schmidt-Kaler, F.
Walser, R.
Vigue, J.
Buechner, M.
Angonin, M. -C.
Delva, P.
Tourrenc, P.
Bingham, R.
Kent, B.
Wicht, A.
Wang, L. J.
Bongs, K.
Dittus, Hj.
Laemmerzahl, C.
Theil, S.
Sengstock, K.
Peters, A.
Mueller, T.
Arndt, M.
Iess, L.
Bondu, F.
Brillet, A.
Samain, E.
Chiofalo, M. L.
Levi, F.
Calonico, D.
TI Matter wave explorer of gravity (MWXG)
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Test of equivalence principle; Fundamental physics; General relativity;
Atom interferometer; MWXG
ID ATOM INTERFEROMETRY; GRAVITATIONAL MASS; EQUIVALENCE; CONSTANT;
GRADIOMETER; MISSION
AB In response to ESA's Call for proposals of 5 March 2007 of the COSMIC VISION 2015-2025 plan of the ESA science programme, we propose a M-class satellite mission to test of the Equivalence Principle in the quantum domain by investigating the extended free fall of matter waves instead of macroscopic bodies as in the case of GAUGE, MICROSCOPE or STEP. The satellite, called MatterWave Explorer of Gravity, will carry an experiment to test gravity, namely the measurement of the equal rate of free fall with various isotopes of distinct atomic species with precision cold atom interferometry in the vicinity of the earth. This will allow for a first quantum test the Equivalence Principle with spin polarised particles and with pure fermionic and bosonic atomic ensembles. Due to the space conditions, the free fall of Rubidium and Potassium isotopes will be compared with a maximum accelerational sensitivity of 5 center dot 10 (-aEuro parts per thousand 16) m/s(2) corresponding to an accuracy of the test of the Equivalence Principle of 1 part in 10(16). Besides the primary scientific goal, the quantum test of the Equivalence Principle, the mission can be extended to provide additional information about the gravitational field of the earth or for testing theories of fundamental processes of decoherence which are investigated by various theory groups in the context of quantum gravity phenomenology. In this proposal we present in detail the mission objectives and the technical aspects of the proposed mission.
C1 [Ertmer, W.; Schubert, C.; Wendrich, T.; Gilowski, M.; Zaiser, M.; v. Zoest, T.; Rasel, E.] Leibniz Univ Hannover, Inst Quantenopt, D-30167 Hannover, Germany.
[Borde, Ch. J.; Clairon, A.; Laurent, P.; Lemonde, P.; Santarelli, G.] Observ Paris, CNRS, LNE SYRTE, F-75014 Paris, France.
[Schleich, W.; Walser, R.] Univ Ulm, Inst Quantenopt, Ulm, Germany.
[Angonin, M. -C.; Delva, P.; Tourrenc, P.] Univ Paris 06, ERGA, Paris, France.
[Cataliotti, F. S.; Inguscio, M.; Poli, N.; Sorrentino, F.; Modugno, C.; Tino, G. M.] Univ Florence, INFN, LENS, Florence, Italy.
[Gill, P.; Klein, H.; Margolis, H.] Natl Phys Lab, Teddington TW11 0LW, Middx, England.
[Reynaud, S.; Lambrecht, A.] UPMC, ENS, LKB, Paris, France.
[Salomon, C.] Ecole Normale Super, Dept Phys, F-75231 Paris, France.
[Peik, E.] Phys Tech Bundesanstalt, D-3300 Braunschweig, Germany.
[Jentsch, C.; Johann, U.; Rathke, A.] EADS Astrium, Friedrichshafen, Germany.
[Bouyer, P.] Inst Opt Theor & Appl, CNRS, Lab Charles Fabry, Palaiseau, France.
[Cacciapuoti, L.] Estec, ESA, Noordwijk, Netherlands.
[De Natale, P.] INOA CNR, Florence, Italy.
[Christophe, B.; Foulon, B.; Touboul, P.] Off Natl Etud & Rech Aerosp, Chatillon, France.
[Maleki, L.; Yu, N.; Turyshev, S. G.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Anderson, J. D.] Global Aerosp Corp, El Segundo, CA USA.
[Schmidt-Kaler, F.] Univ Ulm, Quanten Informat Verarbeitung, Ulm, Germany.
[Vigue, J.; Buechner, M.] Univ Toulouse 3, LCAR, F-31062 Toulouse, France.
[Vigue, J.; Buechner, M.] CNRS, Toulouse, France.
[Bingham, R.; Kent, B.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Wicht, A.] Univ Dusseldorf, Inst Expt Phys, Dusseldorf, Germany.
[Wang, L. J.; Bongs, K.] Univ Birmingham, Birmingham, W Midlands, England.
[Dittus, Hj.; Laemmerzahl, C.; Theil, S.] Univ Bremen, ZARM, Bremen, Germany.
[Sengstock, K.] Univ Hamburg, Inst Laserphys, Hamburg, Germany.
[Peters, A.] Humboldt Univ, Berlin, Germany.
[Mueller, T.] Natl Univ Singapore, Singapore 117548, Singapore.
[Arndt, M.] Univ Vienna, Vienna, Austria.
[Iess, L.] Univ Roma La Sapienza, Dipartimento Ingn Aerosp & Astronaut, Rome, Italy.
[Bondu, F.; Brillet, A.; Samain, E.] CERGA, OCA, Grasse, France.
[Chiofalo, M. L.] CNISM, Pisa, Italy.
[Chiofalo, M. L.] Scuola Normale Super Pisa, INFN, Pisa, Italy.
[Levi, F.; Calonico, D.] Inst Electtrotecn Nazl Galileo Ferraris, Turin, Italy.
RP Rasel, E (reprint author), Leibniz Univ Hannover, Inst Quantenopt, Welfengarten 1, D-30167 Hannover, Germany.
EM rasel@iqo.uni-hannover.de
RI Sorrentino, Fiodor/M-6662-2016; Peters, Achim/G-3742-2010; BOUYER,
Philippe/A-9823-2009; IESS, Luciano/F-4902-2011; Bondu,
Francois/A-2071-2012; Poli, Nicola/B-2166-2012; Reynaud,
Serge/J-8061-2014; Lambrecht, Astrid/K-1208-2014; Cataliotti,
Francesco/K-4772-2015; Arndt, Markus/A-4571-2012; Buchner,
Matthias/N-5248-2015; Theil, Stephan/O-2305-2015; Laemmerzahl,
Claus/P-3552-2016; Schmidt-Kaler, Ferdinand/E-2151-2017; CALONICO,
Davide/J-9158-2016;
OI Sorrentino, Fiodor/0000-0002-9605-9829; BOUYER,
Philippe/0000-0003-4458-0089; IESS, Luciano/0000-0002-6230-5825; Bondu,
Francois/0000-0001-6487-5197; Poli, Nicola/0000-0003-4225-6832; Reynaud,
Serge/0000-0002-1494-696X; Lambrecht, Astrid/0000-0002-5193-1222;
Cataliotti, Francesco/0000-0003-4458-7977; Arndt,
Markus/0000-0002-9487-4985; Theil, Stephan/0000-0002-5346-8091;
Laemmerzahl, Claus/0000-0002-8276-5415; Peik,
Ekkehard/0000-0001-6309-2975; CALONICO, Davide/0000-0002-0345-859X;
Tino, Guglielmo M./0000-0002-7944-9825
FU DLR [50 WM 0508, 50 WM 0346]
FX The QUANTUS-Team acknowledges support from the DLR under the contract 50
WM 0508 and contract DLR 50 WM 0346.
NR 28
TC 20
Z9 20
U1 2
U2 34
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 2
BP 611
EP 649
DI 10.1007/s10686-008-9125-6
PG 39
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KW
UT WOS:000263505600005
ER
PT J
AU Wolf, P
Borde, CJ
Clairon, A
Duchayne, L
Landragin, A
Lemonde, P
Santarelli, G
Ertmer, W
Rasel, E
Cataliotti, FS
Inguscio, M
Tino, GM
Gill, P
Klein, H
Reynaud, S
Salomon, C
Peik, E
Bertolami, O
Gil, P
Paramos, J
Jentsch, C
Johann, U
Rathke, A
Bouyer, P
Cacciapuoti, L
Izzo, D
De Natale, P
Christophe, B
Touboul, P
Turyshev, SG
Anderson, J
Tobar, ME
Schmidt-Kaler, F
Vigue, J
Madej, AA
Marmet, L
Angonin, MC
Delva, P
Tourrenc, P
Metris, G
Muller, H
Walsworth, R
Lu, ZH
Wang, LJ
Bongs, K
Toncelli, A
Tonelli, M
Dittus, H
Lammerzahl, C
Galzerano, G
Laporta, P
Laskar, J
Fienga, A
Roques, F
Sengstock, K
AF Wolf, P.
Borde, Ch. J.
Clairon, A.
Duchayne, L.
Landragin, A.
Lemonde, P.
Santarelli, G.
Ertmer, W.
Rasel, E.
Cataliotti, F. S.
Inguscio, M.
Tino, G. M.
Gill, P.
Klein, H.
Reynaud, S.
Salomon, C.
Peik, E.
Bertolami, O.
Gil, P.
Paramos, J.
Jentsch, C.
Johann, U.
Rathke, A.
Bouyer, P.
Cacciapuoti, L.
Izzo, D.
De Natale, P.
Christophe, B.
Touboul, P.
Turyshev, S. G.
Anderson, J.
Tobar, M. E.
Schmidt-Kaler, F.
Vigue, J.
Madej, A. A.
Marmet, L.
Angonin, M. -C.
Delva, P.
Tourrenc, P.
Metris, G.
Mueller, H.
Walsworth, R.
Lu, Z. H.
Wang, L. J.
Bongs, K.
Toncelli, A.
Tonelli, M.
Dittus, H.
Laemmerzahl, C.
Galzerano, G.
Laporta, P.
Laskar, J.
Fienga, A.
Roques, F.
Sengstock, K.
TI Quantum physics exploring gravity in the outer solar system: the SAGAS
project
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Fundamental physics; Trans Neptunian objects; Optical link; Atomic
clock; Atomic accelerometer
ID FINE-STRUCTURE CONSTANT; ATOM INTERFEROMETRY; GENERAL-RELATIVITY;
CLOCKS; FREQUENCY; RADIATION; SENSORS; SEARCH; LIMITS; SPACE
AB We summarise the scientific and technological aspects of the Search for Anomalous Gravitation using Atomic Sensors (SAGAS) project, submitted to ESA in June 2007 in response to the Cosmic Vision 2015-2025 call for proposals. The proposed mission aims at flying highly sensitive atomic sensors (optical clock, cold atom accelerometer, optical link) on a Solar System escape trajectory in the 2020 to 2030 time-frame. SAGAS has numerous science objectives in fundamental physics and Solar System science, for example numerous tests of general relativity and the exploration of the Kuiper belt. The combination of highly sensitive atomic sensors and of the laser link well adapted for large distances will allow measurements with unprecedented accuracy and on scales never reached before. We present the proposed mission in some detail, with particular emphasis on the science goals and associated measurements and technologies.
C1 [Wolf, P.; Borde, Ch. J.; Clairon, A.; Duchayne, L.; Landragin, A.; Lemonde, P.; Santarelli, G.] UPMC, CNRS, Observ Paris, SYRTE, F-75014 Paris, France.
[Ertmer, W.; Rasel, E.] Leibniz Univ Hannover, Hannover, Germany.
[Cataliotti, F. S.; Inguscio, M.; Tino, G. M.] Univ Florence, Ist Nazl Fis Nucl, LENS, Florence, Italy.
[Gill, P.; Klein, H.] Natl Phys Lab, London, England.
[Reynaud, S.; Salomon, C.] CNRS, Lab Kastler Brossel, Paris, France.
[Peik, E.] Phys Tech Bundesanstalt, D-3300 Braunschweig, Germany.
[Bertolami, O.; Gil, P.; Paramos, J.] Inst Super Tecn, Lisbon, Portugal.
[Jentsch, C.; Johann, U.; Rathke, A.] EADS Astrium, Friedrichshafen, Germany.
[Bouyer, P.] CNRS, Inst Opt, Lab Charles Fabry, F-75700 Paris, France.
[Cacciapuoti, L.; Izzo, D.] ESA, Estec, Noordwijk, Netherlands.
[De Natale, P.] INOA CNR, Florence, Italy.
[Christophe, B.; Touboul, P.] Off Natl Etud & Rech Aerosp, Chatillon, France.
[Turyshev, S. G.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Anderson, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tobar, M. E.] Univ Western Australia, Perth, WA 6009, Australia.
[Schmidt-Kaler, F.] Univ Ulm, Ulm, Germany.
[Vigue, J.] Univ Toulouse 3, CNRS, LCAR, F-31062 Toulouse, France.
[Madej, A. A.] Natl Res Council Canada, CNRC, Ottawa, ON, Canada.
[Marmet, L.] CNRC, Inst Etalons Nationaux Mesures, Ottawa, ON, Canada.
[Angonin, M. -C.; Delva, P.; Tourrenc, P.] Univ Paris 06, ERGA LERMA, Paris, France.
[Metris, G.] CNRS, Observ Cote Azur, GEMINI, F-06034 Nice, France.
[Mueller, H.] Stanford Univ, Stanford, CA 94305 USA.
[Walsworth, R.] Harvard Univ, Cambridge, MA 02138 USA.
[Lu, Z. H.; Wang, L. J.] Univ Erlangen Nurnberg, Erlangen, Germany.
[Bongs, K.] Univ Birmingham, Birmingham, W Midlands, England.
[Toncelli, A.; Tonelli, M.] Univ Pisa, CNR, INFM, NEST, Pisa, Italy.
[Dittus, H.; Laemmerzahl, C.] Univ Bremen, ZARM, Bremen, Germany.
[Galzerano, G.; Laporta, P.] Politecn Milan, I-20133 Milan, Italy.
[Laskar, J.] CNRS, Observ Paris, IMCCE, Paris, France.
[Fienga, A.] Observ Besancon, Besancon, France.
[Roques, F.] CNRS, Observ Paris, LESIA, Paris, France.
[Sengstock, K.] Univ Hamburg, Hamburg, Germany.
RP Wolf, P (reprint author), UPMC, CNRS, Observ Paris, SYRTE, 61 Av Observ, F-75014 Paris, France.
EM peter.wolf@obspm.fr
RI BOUYER, Philippe/A-9823-2009; Laskar, Jacques/E-1098-2011; Toncelli,
Alessandra/A-5352-2012; Gil, Paulo/B-7272-2012; Paramos,
Jorge/J-3440-2013; Reynaud, Serge/J-8061-2014; Tobar,
Michael/C-9763-2009; Mueller, Holger/E-3194-2015; Cataliotti,
Francesco/K-4772-2015; Laemmerzahl, Claus/P-3552-2016; Schmidt-Kaler,
Ferdinand/E-2151-2017;
OI Peik, Ekkehard/0000-0001-6309-2975; GALZERANO,
GIANLUCA/0000-0002-4388-1421; BOUYER, Philippe/0000-0003-4458-0089;
Laskar, Jacques/0000-0003-2634-789X; Toncelli,
Alessandra/0000-0003-4400-8808; Gil, Paulo/0000-0003-2183-6221; Paramos,
Jorge/0000-0001-9853-9431; Reynaud, Serge/0000-0002-1494-696X; Tobar,
Michael/0000-0002-3139-1994; Cataliotti, Francesco/0000-0003-4458-7977;
Laemmerzahl, Claus/0000-0002-8276-5415; Bertolami,
Orfeu/0000-0002-7672-0560; Tino, Guglielmo M./0000-0002-7944-9825
NR 46
TC 66
Z9 67
U1 1
U2 24
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 2
BP 651
EP 687
DI 10.1007/s10686-008-9118-5
PG 37
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KW
UT WOS:000263505600006
ER
PT J
AU Nobili, AM
Comandi, GL
Doravari, S
Bramanti, D
Kumar, R
Maccarrone, F
Polacco, E
Turyshev, SG
Shao, M
Lipa, J
Dittus, H
Laemmerzhal, C
Peters, A
Mueller, J
Unnikrishnan, CS
Roxburgh, IW
Brillet, A
Marchal, C
Luo, J
van der Ha, J
Milyukov, V
Iafolla, V
Lucchesi, D
Tortora, P
De Bernardis, P
Palmonari, F
Focardi, S
Zanello, D
Monaco, S
Mengali, G
Anselmo, L
Iorio, L
Knezevic, Z
AF Nobili, Anna M.
Comandi, Gian Luca
Doravari, Suresh
Bramanti, Donato
Kumar, Rajeev
Maccarrone, Francesco
Polacco, Erseo
Turyshev, Slava G.
Shao, Michael
Lipa, John
Dittus, Hansjoerg
Laemmerzhal, Claus
Peters, Achim
Mueller, Jurgen
Unnikrishnan, C. S.
Roxburgh, Ian W.
Brillet, Alain
Marchal, Christian
Luo, Jun
van der Ha, Jozef
Milyukov, Vadim
Iafolla, Valerio
Lucchesi, David
Tortora, Paolo
De Bernardis, Paolo
Palmonari, Federico
Focardi, Sergio
Zanello, Dino
Monaco, Salvatore
Mengali, Giovanni
Anselmo, Luciano
Iorio, Lorenzo
Knezevic, Zoran
TI "Galileo Galilei" (GG) a small satellite to test the equivalence
principle of Galileo, Newton and Einstein
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE General relativity; Space physics; Experimental gravity
ID GRAVITATIONAL MASS; FREE-FALL; UNIVERSALITY; GRAVITY
AB "Galileo Galilei" (GG) is a small satellite designed to fly in low Earth orbit with the goal of testing the Equivalence Principle-which is at the basis of the General Theory of Relativity-to 1 part in 10(17). If successful, it would improve current laboratory results by 4 orders of magnitude. A confirmation would strongly constrain theories; proof of violation is believed to lead to a scientific revolution. The experiment design allows it to be carried out at ambient temperature inside a small 1-axis stabilized satellite (250 kg total mass). GG is under investigation at Phase A-2 level by ASI (Agenzia Spaziale Italiana) at Thales Alenia Space in Torino, while a laboratory prototype (known as GGG) is operational at INFN laboratories in Pisa, supported by INFN (Istituto Nazionale di fisica Nucleare) and ASI. A final study report will be published in 2009.
C1 [Nobili, Anna M.; Doravari, Suresh; Bramanti, Donato; Maccarrone, Francesco; Polacco, Erseo; Mengali, Giovanni] Univ Pisa, Pisa, Italy.
[Nobili, Anna M.; Comandi, Gian Luca; Doravari, Suresh; Kumar, Rajeev; Maccarrone, Francesco; Polacco, Erseo; Lucchesi, David; Iorio, Lorenzo] Ist Nazl Fis Nucl, Pisa, Italy.
[Comandi, Gian Luca; Tortora, Paolo; Palmonari, Federico; Focardi, Sergio] Univ Bologna, Bologna, Italy.
[Turyshev, Slava G.; Shao, Michael] JPL, Pasadena, CA USA.
[Lipa, John] Stanford Univ, Stanford, CA 94305 USA.
[Dittus, Hansjoerg; Laemmerzhal, Claus] Univ Bremen, Bremen, Germany.
[Peters, Achim] Humboldt Univ, Berlin, Germany.
[Mueller, Jurgen] Tech Univ Munich, Munich, Germany.
[Unnikrishnan, C. S.] Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India.
[Roxburgh, Ian W.] QMW, London, England.
[Brillet, Alain] CNRS OCA, Nice, France.
[Marchal, Christian] Off Natl Etud & Rech Aerosp, Chatillon, France.
[Luo, Jun] Huazhong Univ, Wuhan, Peoples R China.
[van der Ha, Jozef] Kyushu Univ, Fukuoka 812, Japan.
[Milyukov, Vadim] Moscow MV Lomonosov State Univ, Moscow, Russia.
[Iafolla, Valerio] IFSI INAF, Rome, Italy.
[De Bernardis, Paolo; Monaco, Salvatore] Univ Roma La Sapienza, Rome, Italy.
[Palmonari, Federico; Focardi, Sergio] Ist Nazl Fis Nucl, I-40126 Bologna, Italy.
[Zanello, Dino] Ist Nazl Fis Nucl, Rome La Sapienza, Italy.
[Anselmo, Luciano] CNR CNUCE, Pisa, Italy.
[Knezevic, Zoran] Beograd Observ, Belgrade, Serbia.
RP Nobili, AM (reprint author), Univ Pisa, Pisa, Italy.
EM nobili@dm.unipi.it
RI Peters, Achim/G-3742-2010; Mengali, Giovanni/A-1966-2009; Iorio,
Lorenzo/G-5658-2011; Tortora, Paolo/J-6191-2012; Anselmo,
Luciano/C-4384-2012;
OI Mengali, Giovanni/0000-0002-4277-1765; Iorio,
Lorenzo/0000-0003-4949-2694; Tortora, Paolo/0000-0001-9259-7673;
Anselmo, Luciano/0000-0001-5875-2975; Iafolla, Valerio
Antonio/0000-0001-5297-1157; Monaco, Salvatore/0000-0002-2723-5737
NR 35
TC 16
Z9 17
U1 0
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 2
BP 689
EP 710
DI 10.1007/s10686-008-9128-3
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409KW
UT WOS:000263505600007
ER
PT J
AU Chassefiere, E
Korablev, O
Imamura, T
Baines, KH
Wilson, CF
Titov, DV
Aplin, KL
Balint, T
Blamont, JE
Cochrane, CG
Ferencz, C
Ferri, F
Gerasimov, M
Leitner, JJ
Lopez-Moreno, J
Marty, B
Martynov, M
Pogrebenko, SV
Rodin, A
Whiteway, JA
Zasova, LV
Michaud, J
Bertrand, R
Charbonnier, JM
Carbonne, D
Raizonville, P
AF Chassefiere, E.
Korablev, O.
Imamura, T.
Baines, K. H.
Wilson, C. F.
Titov, D. V.
Aplin, K. L.
Balint, T.
Blamont, J. E.
Cochrane, C. G.
Ferencz, Cs.
Ferri, F.
Gerasimov, M.
Leitner, J. J.
Lopez-Moreno, J.
Marty, B.
Martynov, M.
Pogrebenko, S. V.
Rodin, A.
Whiteway, J. A.
Zasova, L. V.
Michaud, J.
Bertrand, R.
Charbonnier, J. -M.
Carbonne, D.
Raizonville, P.
CA EVE Team
TI European Venus Explorer (EVE): an in-situ mission to Venus
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Planets and satellites; Venus; Planets and satellites; Formation;
Radiative transfer; Hydrodynamics; Balloons; Space vehicles; Instruments
ID ATMOSPHERE; WATER; ALTITUDE; PLANET; MARS
AB The European Venus Explorer (EVE) mission was proposed to the European Space Agency in 2007, as an M-class mission under the Cosmic Vision Programme. Although it has not been chosen in the 2007 selection round for programmatic reasons, the EVE mission may serve as a useful reference point for future missions, so it is described here. It consists of one balloon platform floating at an altitude of 50-60 km, one descent probe provided by Russia, and an orbiter with a polar orbit which will relay data from the balloon and descent probe, and perform science observations. The balloon type preferred for scientific goals is one which oscillates in altitude through the cloud deck. To achieve this flight profile, the balloon envelope contains a phase change fluid, which results in a flight profile which oscillates in height. The nominal balloon lifetime is 7 days-enough for one full circumnavigation of the planet. The descent probe's fall through the atmosphere takes 60 min, followed by 30 min of operation on the surface. The key measurement objectives of EVE are: (1) in situ measurement from the balloon of noble gas abundances and stable isotope ratios, to study the record of the evolution of Venus; (2) in situ balloon-borne measurement of cloud particle and gas composition, and their spatial variation, to understand the complex cloud-level chemistry; (3) in situ measurements of environmental parameters and winds (from tracking of the balloon) for one rotation around the planet, to understand atmospheric dynamics and radiative balance in this crucial region. The portfolio of key measurements is complemented by the Russian descent probe, which enables the investigation of the deep atmosphere and surface.
C1 [Chassefiere, E.] UPMC Univ, CNRS, UVSQ, Serv Aeron,IPSL, Paris, France.
[Korablev, O.; Gerasimov, M.; Zasova, L. V.] Russian Acad Sci, Space Res Inst, Moscow, Russia.
[Imamura, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chofu, Tokyo 1828522, Japan.
[Baines, K. H.; Balint, T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Titov, D. V.] Max Planck Inst Solar Syst Studies, Lindau, Germany.
[Aplin, K. L.] Rutherford Appleton Lab, Didcot, Oxon, England.
[Blamont, J. E.; Michaud, J.; Bertrand, R.; Charbonnier, J. -M.; Carbonne, D.; Raizonville, P.] Ctr Natl Etud Spatiales, Paris, France.
[Ferencz, Cs.] Eotvos Lorand Univ, Budapest, Hungary.
[Ferri, F.] Univ Padua, Padua, Italy.
[Leitner, J. J.] Univ Vienna, Vienna, Austria.
[Lopez-Moreno, J.] Inst Astrofis Andalucia, Andalucia, Spain.
[Marty, B.] Ctr Rech Petrog & Geochim, Nancy, France.
[Martynov, M.] Lavochkin Assoc, Moscow, Russia.
[Pogrebenko, S. V.] Joint Inst VLBI Europe, Dwingeloo, Netherlands.
[Rodin, A.] Moscow Inst Phys & Technol, Moscow, Russia.
[Whiteway, J. A.] York Univ, Toronto, ON M3J 2R7, Canada.
[Wilson, C. F.] Univ Oxford, Oxford, England.
[Cochrane, C. G.] Univ London Imperial Coll Sci Technol & Med, London, England.
RP Chassefiere, E (reprint author), UPMC Univ, CNRS, UVSQ, Serv Aeron,IPSL, Paris, France.
EM Eric.Chassefiere@aero.jussieu.fr
RI Aplin, Karen/B-6078-2008; Korablev, Oleg/L-5083-2013; Rodin,
Alexander/L-1904-2013; Lopez-Moreno, Jose Juan/C-7976-2011;
OI Rodin, Alexander/0000-0002-3601-7790; Lopez-Moreno, Jose
Juan/0000-0002-7946-2624; Korablev, Oleg/0000-0003-1115-0656
NR 47
TC 4
Z9 4
U1 1
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 3
BP 741
EP 760
DI 10.1007/s10686-008-9093-x
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409RP
UT WOS:000263523800002
ER
PT J
AU Kuppers, M
Keller, HU
Kuhrt, E
A'Hearn, MF
Altwegg, K
Bertrand, R
Busemann, H
Capria, MT
Colangeli, L
Davidsson, B
Ehrenfreund, P
Knollenberg, J
Mottola, S
Rathke, A
Weiss, P
Zolensky, M
Akim, E
Basilevsky, A
Galimov, E
Gerasimov, M
Korablev, O
Lomakin, I
Marov, M
Martynov, M
Nazarov, M
Zakharov, A
Zelenyi, L
Aronica, A
Ball, AJ
Barbieri, C
Bar-Nun, A
Benkhoff, J
Biele, J
Biver, N
Blum, J
Bockelee-Morvan, D
Botta, O
Bredehoft, JH
Capaccioni, F
Charnley, S
Cloutis, E
Cottin, H
Cremonese, G
Crovisier, J
Crowther, SA
Epifani, EM
Esposito, F
Ferrari, AC
Ferri, F
Fulle, M
Gilmour, J
Goesmann, F
Gortsas, N
Green, SF
Groussin, O
Grun, E
Gutierrez, PJ
Hartogh, P
Henkel, T
Hilchenbach, M
Ho, TM
Horneck, G
Hviid, SF
Ip, WH
Jackel, A
Jessberger, E
Kallenbach, R
Kargl, G
Komle, NI
Korth, A
Kossacki, K
Krause, C
Kruger, H
Li, ZY
Licandro, J
Lopez-Moreno, JJ
Lowry, SC
Lyon, I
Magni, G
Mall, U
Mann, I
Markiewicz, W
Martins, Z
Maurette, M
Meierhenrich, U
Mennella, V
Ng, TC
Nittler, LR
Palumbo, P
Patzold, M
Prialnik, D
Rengel, M
Rickman, H
Rodriguez, J
Roll, R
Rost, D
Rotundi, A
Sandford, S
Schonbachler, M
Sierks, H
Srama, R
Stroud, RM
Szutowicz, S
Tornow, C
Ulamec, S
Wallis, M
Waniak, W
Weissman, P
Wieler, R
Wurz, P
Yung, KL
Zarnecki, JC
AF Kueppers, Michael
Keller, H. U.
Kuehrt, E.
A'Hearn, M. F.
Altwegg, K.
Bertrand, R.
Busemann, H.
Capria, M. T.
Colangeli, L.
Davidsson, B.
Ehrenfreund, P.
Knollenberg, J.
Mottola, S.
Rathke, A.
Weiss, P.
Zolensky, M.
Akim, E.
Basilevsky, A.
Galimov, E.
Gerasimov, M.
Korablev, O.
Lomakin, I.
Marov, M.
Martynov, M.
Nazarov, M.
Zakharov, A.
Zelenyi, L.
Aronica, A.
Ball, A. J.
Barbieri, C.
Bar-Nun, A.
Benkhoff, J.
Biele, J.
Biver, N.
Blum, J.
Bockelee-Morvan, D.
Botta, O.
Bredehoeft, J. -H.
Capaccioni, F.
Charnley, S.
Cloutis, E.
Cottin, H.
Cremonese, G.
Crovisier, J.
Crowther, S. A.
Epifani, E. M.
Esposito, F.
Ferrari, A. C.
Ferri, F.
Fulle, M.
Gilmour, J.
Goesmann, F.
Gortsas, N.
Green, S. F.
Groussin, O.
Gruen, E.
Gutierrez, P. J.
Hartogh, P.
Henkel, T.
Hilchenbach, M.
Ho, T. -M.
Horneck, G.
Hviid, S. F.
Ip, W. -H.
Jaeckel, A.
Jessberger, E.
Kallenbach, R.
Kargl, G.
Koemle, N. I.
Korth, A.
Kossacki, K.
Krause, C.
Krueger, H.
Li, Z. -Y.
Licandro, J.
Lopez-Moreno, J. J.
Lowry, S. C.
Lyon, I.
Magni, G.
Mall, U.
Mann, I.
Markiewicz, W.
Martins, Z.
Maurette, M.
Meierhenrich, U.
Mennella, V.
Ng, T. C.
Nittler, L. R.
Palumbo, P.
Paetzold, M.
Prialnik, D.
Rengel, M.
Rickman, H.
Rodriguez, J.
Roll, R.
Rost, D.
Rotundi, A.
Sandford, S.
Schoenbaechler, M.
Sierks, H.
Srama, R.
Stroud, R. M.
Szutowicz, S.
Tornow, C.
Ulamec, S.
Wallis, M.
Waniak, W.
Weissman, P.
Wieler, R.
Wurz, P.
Yung, K. L.
Zarnecki, J. C.
TI Triple F-a comet nucleus sample return mission
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Comets; Cosmogony; Sample return; Space mission
ID DEEP IMPACT OBSERVATIONS; TERRESTRIAL PLANETS; MECHANICAL-PROPERTIES;
ROSETTA MISSION; ORGANIC-MATTER; SOLAR-SYSTEM; WATER ICE; ORIGIN;
SURFACE; SPECTROMETER
AB The Triple F (Fresh From the Fridge) mission, a Comet Nucleus Sample Return, has been proposed to ESA's Cosmic Vision program. A sample return from a comet enables us to reach the ultimate goal of cometary research. Since comets are the least processed bodies in the solar system, the proposal goes far beyond cometary science topics (like the explanation of cometary activity) and delivers invaluable information about the formation of the solar system and the interstellar molecular cloud from which it formed. The proposed mission would extract three sample cores of the upper 50 cm from three locations on a cometary nucleus and return them cooled to Earth for analysis in the laboratory. The simple mission concept with a touch-and-go sampling by a single spacecraft was proposed as an M-class mission in collaboration with the Russian space agency ROSCOSMOS.
C1 [Kueppers, Michael; Keller, H. U.; Goesmann, F.; Hartogh, P.; Hilchenbach, M.; Hviid, S. F.; Kallenbach, R.; Korth, A.; Krueger, H.; Mall, U.; Markiewicz, W.; Rengel, M.; Roll, R.; Sierks, H.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Kueppers, Michael; Lyon, I.] European Space Astron Ctr, Madrid 28691, Spain.
[Kuehrt, E.; Knollenberg, J.; Mottola, S.; Benkhoff, J.; Biele, J.; Horneck, G.; Krause, C.; Tornow, C.] DLR, Berlin, Germany.
[A'Hearn, M. F.] Univ Maryland, College Pk, MD 20742 USA.
[Altwegg, K.; Jaeckel, A.; Wurz, P.] Univ Bern, Bern, Switzerland.
[Bertrand, R.] CNES, Toulouse, France.
[Busemann, H.; Ball, A. J.; Green, S. F.; Zarnecki, J. C.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Capria, M. T.; Capaccioni, F.; Magni, G.] IASF INAF, Rome, Italy.
[Colangeli, L.; Epifani, E. M.; Esposito, F.; Mennella, V.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Davidsson, B.; Rickman, H.] Uppsala Univ, Uppsala, Sweden.
[Ehrenfreund, P.] Leiden Univ, Leiden, Netherlands.
[Rathke, A.] EADS Astrium, Friedrichshafen, Germany.
[Weiss, P.; Ng, T. C.; Yung, K. L.] Hong Kong Polytech Univ, Hong Kong, Hong Kong, Peoples R China.
[Zolensky, M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Akim, E.; Marov, M.] Keldysh Inst, Moscow, Russia.
[Basilevsky, A.; Galimov, E.; Nazarov, M.] Vernadskij Inst, Moscow, Russia.
[Gerasimov, M.; Korablev, O.; Zakharov, A.; Zelenyi, L.] Space Res Inst, Moscow, Russia.
[Lomakin, I.; Martynov, M.] Lavochkin Assoc, Moscow, Russia.
[Aronica, A.; Palumbo, P.; Rotundi, A.] Univ Naples Federico 2, Naples, Italy.
[Barbieri, C.; Cremonese, G.; Ferri, F.] Univ Padua, Padua, Italy.
[Bar-Nun, A.; Prialnik, D.] Tel Aviv Univ, IL-69978 Tel Aviv, Israel.
[Blum, J.] Tech Univ Carolo Wilhelmina Braunschweig, Braunschweig, Germany.
[Botta, O.] Int Space Sci Inst, Bern, Switzerland.
[Bredehoeft, J. -H.] Univ Bremen, Bremen, Germany.
[Cloutis, E.] Univ Winnipeg, Winnipeg, MB R3B 2E9, Canada.
[Cottin, H.] Univ Paris, F-75252 Paris, France.
[Gruen, E.; Srama, R.] MPIfK, Heidelberg, Germany.
[Gutierrez, P. J.; Lopez-Moreno, J. J.; Rodriguez, J.] CSIC, IAA, Granada, Spain.
[Ho, T. -M.] ESA, Estec, Noordwijk, Netherlands.
[Ip, W. -H.; Li, Z. -Y.] Natl Cent Univ, Taipei, Taiwan.
[Jessberger, E.] Univ Munster, Munster, Germany.
[Kargl, G.; Koemle, N. I.] IWF, Graz, Austria.
[Kossacki, K.] Univ Warsaw, Warsaw, Poland.
[Licandro, J.] IAC, Tenerife, Spain.
[Lowry, S. C.] Queens Univ Belfast, Belfast, Antrim, North Ireland.
[Mann, I.] Kobe Univ, Kobe, Hyogo 657, Japan.
[Maurette, M.] CNRS, F-91405 Orsay, France.
[Meierhenrich, U.] Univ Nice, Nice, France.
[Nittler, L. R.] Carnegie Inst Washington, Washington, DC 20005 USA.
[Paetzold, M.] Univ Cologne, Cologne, Germany.
[Sandford, S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Stroud, R. M.] USA, Res Lab, Washington, DC 20310 USA.
[Szutowicz, S.] PAS, Space Res Ctr, Warsaw, Poland.
[Ulamec, S.] DLR, Cologne, Germany.
[Wallis, M.] Cardiff Univ, Cardiff, Wales.
[Waniak, W.] Krakow Tech Univ, PL-31155 Krakow, Poland.
[Weissman, P.] JPL, Pasadena, CA USA.
[Wieler, R.] ETH, Zurich, Switzerland.
[Martins, Z.; Schoenbaechler, M.] Univ London Imperial Coll Sci Technol & Med, London, England.
[Groussin, O.] LAM, Marseille, France.
[Fulle, M.] Trieste Observ, Trieste, Italy.
[Ferrari, A. C.] Univ Cambridge, Cambridge, England.
[Crowther, S. A.; Gilmour, J.; Henkel, T.; Lyon, I.; Rost, D.] Univ Manchester, Manchester, Lancs, England.
[Charnley, S.] NASA, Ames Res Ctr, Mountain View, CA USA.
[Biver, N.; Bockelee-Morvan, D.; Crovisier, J.] Observ Paris, Meudon, France.
RP Kuppers, M (reprint author), Max Planck Inst Solar Syst Res, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
EM Michael.Kueppers@sciops.esa.int
RI Green, Simon/C-7408-2009; Wieler, Rainer/A-1355-2010; Blum,
Jurgen/B-5590-2011; Gilmour, Jamie/G-7515-2011; Bredehoft, Jan
Hendrik/E-4221-2012; Cottin, Herve/H-5654-2013; Korablev,
Oleg/L-5083-2013; Gutierrez, Pedro/K-9637-2014; Crowther,
Sarah/P-7082-2014; Lopez-Moreno, Jose Juan/C-7976-2011; Martins,
Zita/H-4860-2015; Meierhenrich, Uwe/A-1643-2008; Ball,
Andrew/B-6747-2009; Stroud, Rhonda/C-5503-2008;
OI Wieler, Rainer/0000-0001-5666-7494; Blum, Jurgen/0000-0003-1531-737X;
Bredehoft, Jan Hendrik/0000-0002-7977-6762; Cottin,
Herve/0000-0001-9170-5265; Gutierrez, Pedro/0000-0002-7332-6269;
Martins, Zita/0000-0002-5420-1081; Meierhenrich,
Uwe/0000-0001-6422-3930; Ball, Andrew/0000-0003-1593-3279; fulle,
marco/0000-0001-8435-5287; Rotundi, Alessandra/0000-0001-5467-157X;
Korablev, Oleg/0000-0003-1115-0656; Stroud, Rhonda/0000-0001-5242-8015;
Busemann, Henner/0000-0002-0867-6908; Aronica,
Alessandro/0000-0003-3205-9472; Cremonese, Gabriele/0000-0001-9021-1140;
Esposito, Francesca/0000-0001-9962-1648; Crowther,
Sarah/0000-0002-5396-1775; Lopez-Moreno, Jose Juan/0000-0002-7946-2624;
Gilmour, Jamie/0000-0003-1990-8636; Capaccioni,
Fabrizio/0000-0003-1631-4314
NR 63
TC 5
Z9 5
U1 1
U2 11
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 3
BP 809
EP 847
DI 10.1007/s10686-008-9115-8
PG 39
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409RP
UT WOS:000263523800005
ER
PT J
AU Blanc, M
Alibert, Y
Andre, N
Atreya, S
Beebe, R
Benz, W
Bolton, SJ
Coradini, A
Coustenis, A
Dehant, V
Dougherty, M
Drossart, P
Fujimoto, M
Grasset, O
Gurvits, L
Hartogh, P
Hussmann, H
Kasaba, Y
Kivelson, M
Khurana, K
Krupp, N
Louarn, P
Lunine, J
McGrath, M
Mimoun, D
Mousis, O
Oberst, J
Okada, T
Pappalardo, R
Prieto-Ballesteros, O
Prieur, D
Regnier, P
Roos-Serote, M
Sasaki, S
Schubert, G
Sotin, C
Spilker, T
Takahashi, Y
Takashima, T
Tosi, F
Turrini, D
Van Hoolst, T
Zelenyi, L
AF Blanc, Michel
Alibert, Yann
Andre, Nicolas
Atreya, Sushil
Beebe, Reta
Benz, Willy
Bolton, Scott J.
Coradini, Angioletta
Coustenis, Athena
Dehant, Veronique
Dougherty, Michele
Drossart, Pierre
Fujimoto, Masaki
Grasset, Olivier
Gurvits, Leonid
Hartogh, Paul
Hussmann, Hauke
Kasaba, Yasumasa
Kivelson, Margaret
Khurana, Krishan
Krupp, Norbert
Louarn, Philippe
Lunine, Jonathan
McGrath, Melissa
Mimoun, David
Mousis, Olivier
Oberst, Juergen
Okada, Tatsuaki
Pappalardo, Robert
Prieto-Ballesteros, Olga
Prieur, Daniel
Regnier, Pascal
Roos-Serote, Maarten
Sasaki, Sho
Schubert, Gerald
Sotin, Christophe
Spilker, Tom
Takahashi, Yukihiro
Takashima, Takeshi
Tosi, Federico
Turrini, Diego
Van Hoolst, Tim
Zelenyi, Lev
TI LAPLACE: A mission to Europa and the Jupiter System for ESA's Cosmic
Vision Programme
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Jupiter; Europa; Jovian system; ESA's Cosmic Vision; Mission
ID ICY GALILEAN SATELLITES; SUBSURFACE OCEAN; JOVIAN SUBNEBULA; PLASMA
TRANSPORT; MAGNETIC-FIELD; TIDAL RESPONSE; GIANT PLANETS; IO; LIFE;
MAGNETOSPHERE
AB The exploration of the Jovian System and its fascinating satellite Europa is one of the priorities presented in ESA's "Cosmic Vision" strategic document. The Jovian System indeed displays many facets. It is a small planetary system in its own right, built-up out of the mixture of gas and icy material that was present in the external region of the solar nebula. Through a complex history of accretion, internal differentiation and dynamic interaction, a very unique satellite system formed, in which three of the four Galilean satellites are locked in the so-called Laplace resonance. The energy and angular momentum they exchange among themselves and with Jupiter contribute to various degrees to the internal heating sources of the satellites. Unique among these satellites, Europa is believed to shelter an ocean between its geodynamically active icy crust and its silicate mantle, one where the main conditions for habitability may be fulfilled. For this very reason, Europa is one of the best candidates for the search for life in our Solar System. So, is Europa really habitable, representing a "habitable zone" in the Jupiter system? To answer this specific question, we need a dedicated mission to Europa. But to understand in a more generic way the habitability conditions around giant planets, we need to go beyond Europa itself and address two more general questions at the scale of the Jupiter system: to what extent is its possible habitability related to the initial conditions and formation scenario of the Jovian satellites? To what extent is it due to the way the Jupiter system works? ESA's Cosmic Vision programme offers an ideal and timely framework to address these three key questions. Building on the in-depth reconnaissance of the Jupiter System by Galileo (and the Voyager, Ulysses, Cassini and New Horizons fly-by's) and on the anticipated accomplishments of NASA's JUNO mission, it is now time to design and fly a new mission which will focus on these three major questions. LAPLACE, as we propose to call it, will deploy in the Jovian system a triad of orbiting platforms to perform coordinated observations of its main components: Europa, our priority target, the Jovian satellites, Jupiter's magnetosphere and its atmosphere and interior. LAPLACE will consolidate Europe's role and visibility in the exploration of the Solar System and will foster the development of technologies for the exploration of deep space in Europe. Its multi-platform and multi-target architecture, combined with its broadly multidisciplinary scientific dimension, will provide an outstanding opportunity to build a broad international collaboration with all interested nations and space agencies.
C1 [Blanc, Michel; Louarn, Philippe] UPS, CNRS, CESR, F-31028 Toulouse 4, France.
[Blanc, Michel] Ecole Polytech, Palaiseau, France.
[Alibert, Yann; Benz, Willy] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Alibert, Yann; Mousis, Olivier] Inst UTINAM, Observ Besancon, F-25010 Besancon, France.
[Andre, Nicolas] European Space Agcy, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands.
[Atreya, Sushil] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Beebe, Reta] New Mexico State Univ, Las Cruces, NM 88003 USA.
[Bolton, Scott J.] SwRI, San Antonio, TX USA.
[Coradini, Angioletta; Tosi, Federico; Turrini, Diego] Ist Fis Spazio Interplanetario, INAF, I-00133 Rome, Italy.
[Coustenis, Athena; Drossart, Pierre] Observ Paris, LESIA, F-92195 Meudon, France.
[Dehant, Veronique; Van Hoolst, Tim] Royal Observ Belgium, Brussels, Belgium.
[Grasset, Olivier] Univ Nantes, Lab Planetol, F-44322 Nantes 03, France.
[Gurvits, Leonid] JIVE, Dwingeloo, Netherlands.
[Hartogh, Paul; Hussmann, Hauke] DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Kasaba, Yasumasa] Tohoku Univ, Dept Geophys, Sendai, Miyagi 9808578, Japan.
[Kivelson, Margaret; Khurana, Krishan] Univ Calif Los Angeles, Los Angeles, CA USA.
[Krupp, Norbert] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Lunine, Jonathan] Univ Arizona, Tucson, AZ USA.
[McGrath, Melissa] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Mimoun, David] Univ Toulouse, ISAE, SUPAERO, F-31055 Toulouse 4, France.
[Oberst, Juergen] DLR, Berlin, Germany.
[Pappalardo, Robert; Spilker, Tom] NASA, JPL, Pasadena, CA USA.
[Prieto-Ballesteros, Olga] CSIC, Ctr Astrobiol, INTA, Lab Geol Planetaria, Madrid, Spain.
[Prieur, Daniel] Univ Bretagne Occidentale, Brest, France.
[Regnier, Pascal] EADS ASTRIUM, Toulouse, France.
[Roos-Serote, Maarten; Sasaki, Sho] Natl Astron Observ, Mizusawa, Iwate, Japan.
[Schubert, Gerald] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zelenyi, Lev] Space Res Inst IKI, Moscow, Russia.
[Dougherty, Michele] Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England.
[Fujimoto, Masaki; Okada, Tatsuaki; Takashima, Takeshi] Japan Aerosp Explorat Agcy, Sagamihara, Kanagawa 2298510, Japan.
RP Blanc, M (reprint author), UPS, CNRS, CESR, 9 Ave Colonel Roche, F-31028 Toulouse 4, France.
EM michel.blanc@cesr.fr
RI Kivelson, Margaret/I-9019-2012; MIMOUN, DAVID/M-7074-2016;
OI Kivelson, Margaret/0000-0003-3859-8581; MIMOUN,
DAVID/0000-0002-3427-2974; Turrini, Diego/0000-0002-1923-7740; Tosi,
Federico/0000-0003-4002-2434
NR 87
TC 26
Z9 26
U1 1
U2 19
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 3
BP 849
EP 892
DI 10.1007/s10686-008-9127-4
PG 44
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409RP
UT WOS:000263523800006
ER
PT J
AU Coustenis, A
Atreya, SK
Balint, T
Brown, RH
Dougherty, MK
Ferri, F
Fulchignoni, M
Gautier, D
Gowen, RA
Griffith, CA
Gurvits, LI
Jaumann, R
Langevin, Y
Leese, MR
Lunine, JI
Mckay, CP
Moussas, X
Muller-Wodarg, I
Neubauer, F
Owen, TC
Raulin, F
Sittler, EC
Sohl, F
Sotin, C
Tobie, G
Tokano, T
Turtle, EP
Wahlund, JE
Waite, JH
Baines, KH
Blamont, J
Coates, AJ
Dandouras, I
Krimigis, T
Lellouch, E
Lorenz, RD
Morse, A
Porco, CC
Hirtzig, M
Saur, J
Spilker, T
Zarnecki, JC
Choi, E
Achilleos, N
Amils, R
Annan, P
Atkinson, DH
Benilan, Y
Bertucci, C
Bezard, B
Bjoraker, GL
Blanc, M
Boireau, L
Bouman, J
Cabane, M
Capria, MT
Chassefiere, E
Coll, P
Combes, M
Cooper, JF
Coradini, A
Crary, F
Cravens, T
Daglis, IA
de Angelis, E
de Bergh, C
de Pater, I
Dunford, C
Durry, G
Dutuit, O
Fairbrother, D
Flasar, FM
Fortes, AD
Frampton, R
Fujimoto, M
Galand, M
Grasset, O
Grott, M
Haltigin, T
Herique, A
Hersant, F
Hussmann, H
Ip, W
Johnson, R
Kallio, E
Kempf, S
Knapmeyer, M
Kofman, W
Koop, R
Kostiuk, T
Krupp, N
Kuppers, M
Lammer, H
Lara, LM
Lavvas, P
Le Mouelic, S
Lebonnois, S
Ledvina, S
Li, J
Livengood, TA
Lopes, RM
Lopez-Moreno, JJ
Luz, D
Mahaffy, PR
Mall, U
Martinez-Frias, J
Marty, B
McCord, T
Salvan, C
Milillo, A
Mitchell, DG
Modolo, R
Mousis, O
Nakamura, M
Neish, CD
Nixon, CA
Mvondo, D
Orton, G
Paetzold, M
Pitman, J
Pogrebenko, S
Pollard, W
Prieto-Ballesteros, O
Rannou, P
Reh, K
Richter, L
Robb, FT
Rodrigo, R
Rodriguez, S
Romani, P
Bermejo, M
Sarris, ET
Schenk, P
Schmitt, B
Schmitz, N
Schulze-Makuch, D
Schwingenschuh, K
Selig, A
Sicardy, B
Soderblom, L
Spilker, LJ
Stam, D
Steele, A
Stephan, K
Strobel, DF
Szego, K
Szopa, C
Thissen, R
Tomasko, MG
Toublanc, D
Vali, H
Vardavas, I
Vuitton, V
West, RA
Yelle, R
Young, EF
AF Coustenis, A.
Atreya, S. K.
Balint, T.
Brown, R. H.
Dougherty, M. K.
Ferri, F.
Fulchignoni, M.
Gautier, D.
Gowen, R. A.
Griffith, C. A.
Gurvits, L. I.
Jaumann, R.
Langevin, Y.
Leese, M. R.
Lunine, J. I.
McKay, C. P.
Moussas, X.
Mueller-Wodarg, I.
Neubauer, F.
Owen, T. C.
Raulin, F.
Sittler, E. C.
Sohl, F.
Sotin, C.
Tobie, G.
Tokano, T.
Turtle, E. P.
Wahlund, J. -E.
Waite, J. H.
Baines, K. H.
Blamont, J.
Coates, A. J.
Dandouras, I.
Krimigis, T.
Lellouch, E.
Lorenz, R. D.
Morse, A.
Porco, C. C.
Hirtzig, M.
Saur, J.
Spilker, T.
Zarnecki, J. C.
Choi, E.
Achilleos, N.
Amils, R.
Annan, P.
Atkinson, D. H.
Benilan, Y.
Bertucci, C.
Bezard, B.
Bjoraker, G. L.
Blanc, M.
Boireau, L.
Bouman, J.
Cabane, M.
Capria, M. T.
Chassefiere, E.
Coll, P.
Combes, M.
Cooper, J. F.
Coradini, A.
Crary, F.
Cravens, T.
Daglis, I. A.
de Angelis, E.
de Bergh, C.
de Pater, I.
Dunford, C.
Durry, G.
Dutuit, O.
Fairbrother, D.
Flasar, F. M.
Fortes, A. D.
Frampton, R.
Fujimoto, M.
Galand, M.
Grasset, O.
Grott, M.
Haltigin, T.
Herique, A.
Hersant, F.
Hussmann, H.
Ip, W.
Johnson, R.
Kallio, E.
Kempf, S.
Knapmeyer, M.
Kofman, W.
Koop, R.
Kostiuk, T.
Krupp, N.
Kueppers, M.
Lammer, H.
Lara, L. -M.
Lavvas, P.
Le Mouelic, S.
Lebonnois, S.
Ledvina, S.
Li, J.
Livengood, T. A.
Lopes, R. M.
Lopez-Moreno, J. -J.
Luz, D.
Mahaffy, P. R.
Mall, U.
Martinez-Frias, J.
Marty, B.
McCord, T.
Menor Salvan, C.
Milillo, A.
Mitchell, D. G.
Modolo, R.
Mousis, O.
Nakamura, M.
Neish, C. D.
Nixon, C. A.
Nna Mvondo, D.
Orton, G.
Paetzold, M.
Pitman, J.
Pogrebenko, S.
Pollard, W.
Prieto-Ballesteros, O.
Rannou, P.
Reh, K.
Richter, L.
Robb, F. T.
Rodrigo, R.
Rodriguez, S.
Romani, P.
Ruiz Bermejo, M.
Sarris, E. T.
Schenk, P.
Schmitt, B.
Schmitz, N.
Schulze-Makuch, D.
Schwingenschuh, K.
Selig, A.
Sicardy, B.
Soderblom, L.
Spilker, L. J.
Stam, D.
Steele, A.
Stephan, K.
Strobel, D. F.
Szego, K.
Szopa, C.
Thissen, R.
Tomasko, M. G.
Toublanc, D.
Vali, H.
Vardavas, I.
Vuitton, V.
West, R. A.
Yelle, R.
Young, E. F.
TI TandEM: Titan and Enceladus mission
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE TandEM; Titan; Enceladus; Saturnian system; Landing probes
ID HUYGENS PROBE; INTERNAL STRUCTURE; LANDING SITE; ATMOSPHERE; METHANE;
ORIGIN; MASS; ENRICHMENT; EVOLUTION; VOLATILES
AB TandEM was proposed as an L-class (large) mission in response to ESA's Cosmic Vision 2015-2025 Call, and accepted for further studies, with the goal of exploring Titan and Enceladus. The mission concept is to perform in situ investigations of two worlds tied together by location and properties, whose remarkable natures have been partly revealed by the ongoing Cassini-Huygens mission. These bodies still hold mysteries requiring a complete exploration using a variety of vehicles and instruments. TandEM is an ambitious mission because its targets are two of the most exciting and challenging bodies in the Solar System. It is designed to build on but exceed the scientific and technological accomplishments of the Cassini-Huygens mission, exploring Titan and Enceladus in ways that are not currently possible (full close-up and in situ coverage over long periods of time). In the current mission architecture, TandEM proposes to deliver two medium-sized spacecraft to the Saturnian system. One spacecraft would be an orbiter with a large host of instruments which would perform several Enceladus flybys and deliver penetrators to its surface before going into a dedicated orbit around Titan alone, while the other spacecraft would carry the Titan in situ investigation components, i.e. a hot-air balloon (MontgolfiSre) and possibly several landing probes to be delivered through the atmosphere.
C1 [Coustenis, A.; Fulchignoni, M.; Gautier, D.; Lellouch, E.; Hirtzig, M.; Bezard, B.; Combes, M.; de Bergh, C.; Luz, D.; Sicardy, B.] Observ Paris, LESIA, F-92195 Meudon, France.
[Atreya, S. K.; Hirtzig, M.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Balint, T.; Baines, K. H.; Spilker, T.; Lopes, R. M.; Orton, G.; Reh, K.; Spilker, L. J.; West, R. A.] CALTECH, JPL, Pasadena, CA 91125 USA.
[Brown, R. H.; Griffith, C. A.; Lunine, J. I.; Lavvas, P.; Neish, C. D.; Tomasko, M. G.; Vuitton, V.; Yelle, R.] Univ Arizona, LPL, Tucson, AZ USA.
[Ferri, F.] Univ Padua, CISAS, Padua, Italy.
[Gurvits, L. I.; Pogrebenko, S.] Joint Inst VLBI Europe, Dwingeloo, Netherlands.
[Jaumann, R.; Sohl, F.; Grott, M.; Hussmann, H.; Knapmeyer, M.; Richter, L.; Schmitz, N.; Stephan, K.] DLR, Inst Planetary Res, Berlin, Germany.
[Langevin, Y.] Univ Paris 11, IAS, Orsay, France.
[Leese, M. R.; Morse, A.; Zarnecki, J. C.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[McKay, C. P.] NASA, AMES, Palo Alto, CA USA.
[Moussas, X.] Univ Athens, Fac Phys, Athens, Greece.
[Neubauer, F.; Tokano, T.; Saur, J.; Paetzold, M.] Univ Cologne, Cologne, Germany.
[Owen, T. C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Raulin, F.; Benilan, Y.; Coll, P.] Univ Paris 12, LISA, Creteil, France.
[Sittler, E. C.; Bjoraker, G. L.; Cooper, J. F.; Fairbrother, D.; Flasar, F. M.; Kostiuk, T.; Mahaffy, P. R.; Nixon, C. A.; Romani, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sotin, C.; Tobie, G.; Grasset, O.; Herique, A.; Le Mouelic, S.] Fac Sci, Lab Planetol & Geodyanm, Nantes, France.
[Turtle, E. P.; Krimigis, T.; Lorenz, R. D.; Mitchell, D. G.; Strobel, D. F.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Wahlund, J. -E.; Modolo, R.] Swedish Inst Space Phys, Uppsala, Sweden.
[Waite, J. H.; Crary, F.; Young, E. F.] SW Res Inst, San Antonio, TX USA.
[Blamont, J.; Boireau, L.] Ctr Natl Etud Spatiales, Paris, France.
[Dandouras, I.; Toublanc, D.] Ctr Etud Spatiale Rayonnements, Toulouse, France.
[Krimigis, T.] Acad Athens, Athens, Greece.
[Porco, C. C.] SSI, CICLOPS, Boulder, CO USA.
[Choi, E.] Bombardier Aerosp, Toronto, ON, Canada.
[Amils, R.; Martinez-Frias, J.; Menor Salvan, C.; Nna Mvondo, D.; Prieto-Ballesteros, O.; Ruiz Bermejo, M.] CSIC, INTA, Ctr Astrobiol, Madrid, Spain.
[Annan, P.] Sensors & Software, Mississauga, ON, Canada.
[Atkinson, D. H.] Univ Idaho, NASA, Moscow, ID 83843 USA.
[Blanc, M.] Ecole Polytech, F-75230 Paris, France.
[Bouman, J.; Koop, R.; Selig, A.; Stam, D.] SRON, Netherlands Inst Space Res, Utrecht, Netherlands.
[Cabane, M.; Chassefiere, E.; Durry, G.; Szopa, C.] Univ Paris 06, Serv Aeron, Paris, France.
[Capria, M. T.; Coradini, A.; de Angelis, E.; Milillo, A.] Ist Nazl Astrofis, Rome, Italy.
[Cravens, T.] Univ Kansas, Lawrence, KS 66045 USA.
[Daglis, I. A.] Natl Observ Athens, Athens, Greece.
[de Pater, I.; Ledvina, S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Dutuit, O.; Kofman, W.; Schmitt, B.; Thissen, R.] Univ Grenoble 1, CNRS, Lab Planetol Grenoble, Grenoble, France.
[Frampton, R.] Boeing Co, Chicago, IL USA.
[Fujimoto, M.; Nakamura, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chofu, Tokyo 1828522, Japan.
[Haltigin, T.; Pollard, W.; Vali, H.] McGill Univ, Montreal, PQ, Canada.
[Hersant, F.] Univ Bordeaux, Bordeaux, France.
[Ip, W.] Natl Cent Univ, Inst Astron, Jhongli, Taiwan.
[Johnson, R.] Univ Virginia, Charlottesville, VA USA.
[Kallio, E.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Kempf, S.; Krupp, N.; Kueppers, M.; Mall, U.] Max Planck Inst, Lindau, Germany.
[Lammer, H.; Schwingenschuh, K.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Lara, L. -M.; Lopez-Moreno, J. -J.; Rodrigo, R.] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Lavvas, P.; Vardavas, I.] Univ Crete, FORTH, Iraklion, Greece.
[Lebonnois, S.] Meteorol Dynam Lab, Paris, France.
[Li, J.] Chinese Acad Sci, IAP, LASG, Taipei, Taiwan.
[Livengood, T. A.] USRA, Natl Ctr Earth & Space Sci Educ, Columbia, MD USA.
[Luz, D.] CAAUL Observatorio Astron Lisboa, P-1349018 Lisbon, Portugal.
[Marty, B.] CRPG, Nancy, France.
[McCord, T.] Bear Fight Ctr, Winthrop, WA USA.
[Mousis, O.] Univ Franche Comte, CNRS, INSU, Inst UTINAM, F-25030 Besancon, France.
[Nixon, C. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Pitman, J.] Lockheed Martin Sensing & Explorat Syst, Denver, CO USA.
[Rannou, P.] Univ Reims, Reims, France.
[Robb, F. T.] Univ Maryland, Inst Biotechnol, Baltimore, MD 21202 USA.
[Rodriguez, S.] CEA, AIM, Saclay, France.
[Sarris, E. T.] Democritus Univ Thrace, GR-67100 Xanthi, Greece.
[Schenk, P.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Schulze-Makuch, D.] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA.
[Soderblom, L.] US Geol Survey, Tucson, AZ USA.
[Steele, A.] Carnegie Inst Sci, Washington, DC 20005 USA.
[Szego, K.] KFKI Res Inst Particle & Nucl Phys, Budapest, Hungary.
[Raulin, F.; Benilan, Y.; Coll, P.] Univ Paris 07, Creteil, France.
[Gowen, R. A.; Coates, A. J.; Achilleos, N.; Fortes, A. D.] Univ Coll London, Mullard Space Sci Lab, Bloomsbury, England.
[Dougherty, M. K.; Mueller-Wodarg, I.; Bertucci, C.; Dunford, C.; Galand, M.] Univ London Imperial Coll Sci Technol & Med, London, England.
RP Coustenis, A (reprint author), Observ Paris, LESIA, F-92195 Meudon, France.
EM athena.coustenis@obspm.fr
RI Vali, Hojatollah/F-3511-2012; Neish, Catherine/G-6321-2012; Vardavas,
Ilias/G-7310-2011; Mahaffy, Paul/E-4609-2012; RANNOU,
Pascal/I-9059-2012; Coates, Andrew/C-2396-2008; Turtle,
Elizabeth/K-8673-2012; Dunford, Charlotte/H-7439-2013; Luz,
David/J-4588-2013; Daglis, Ioannis/L-6100-2013; Kostiuk,
Theodor/A-3077-2014; Mueller-Wodarg, Ingo/M-9945-2014; Ruiz-Bermejo,
Marta/L-1163-2014; Kofman, Wlodek/C-4556-2008; Nixon, Conor/A-8531-2009;
Galand, Marina/C-6804-2009; Fortes, Andrew/C-1349-2011; Schmitt,
Bernard/A-1064-2009; Menor-Salvan, Cesar/H-5961-2011; Knapmeyer,
Martin/A-5783-2012; Livengood, Timothy/C-8512-2012; Flasar, F
Michael/C-8509-2012; Romani, Paul/D-2729-2012; Cooper, John/D-4709-2012;
Bjoraker, Gordon/D-5032-2012; Bouman, Johannes/C-3521-2015; szopa,
cyril/C-6865-2015; Lopez-Moreno, Jose Juan/C-7976-2011; Lorenz,
Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016; Kallio, Esa/F-9410-2014;
Rodriguez, Sebastien/H-5902-2016; Herique, Alain/E-7210-2017;
OI Vali, Hojatollah/0000-0003-3464-9943; Coates,
Andrew/0000-0002-6185-3125; Turtle, Elizabeth/0000-0003-1423-5751;
Dunford, Charlotte/0000-0003-1470-7480; Luz, David/0000-0002-9473-8035;
Daglis, Ioannis/0000-0002-0764-3442; Mueller-Wodarg,
Ingo/0000-0001-6308-7826; Ruiz-Bermejo, Marta/0000-0002-8059-1335;
Nixon, Conor/0000-0001-9540-9121; Fortes, Andrew/0000-0001-5907-2285;
Schmitt, Bernard/0000-0002-1230-6627; Menor-Salvan,
Cesar/0000-0002-1238-190X; Knapmeyer, Martin/0000-0003-0319-2514; szopa,
cyril/0000-0002-0090-4056; Lorenz, Ralph/0000-0001-8528-4644; Lopes,
Rosaly/0000-0002-7928-3167; Kallio, Esa/0000-0002-9791-804X; Rodriguez,
Sebastien/0000-0003-1219-0641; Herique, Alain/0000-0003-3699-883X;
Dandouras, Iannis/0000-0002-7121-1118; capria, maria
teresa/0000-0002-9814-9588; Bertucci, Cesar/0000-0002-2540-5384;
Achilleos, Nicholas/0000-0002-5886-3509; Lopez-Moreno, Jose
Juan/0000-0002-7946-2624; Robb, Frank/0000-0001-5833-6496; Milillo,
Anna/0000-0002-0266-2556; LEBONNOIS, SEBASTIEN/0000-0002-2390-8164; De
Angelis, Elisabetta/0000-0003-0537-6376; KEMPF,
SASCHA/0000-0001-5236-3004
FU Science and Technology Facilities Council [PP/D00084X/1]
NR 51
TC 48
Z9 48
U1 2
U2 46
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 3
BP 893
EP 946
DI 10.1007/s10686-008-9103-z
PG 54
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409RP
UT WOS:000263523800007
ER
PT J
AU Marty, B
Guillot, T
Coustenis, A
Achilleos, N
Alibert, Y
Asmar, S
Atkinson, D
Atreya, S
Babasides, G
Baines, K
Balint, T
Banfield, D
Barber, S
Bezard, B
Bjoraker, GL
Blanc, M
Bolton, S
Chanover, N
Charnoz, S
Chassefiere, E
Colwell, JE
Deangelis, E
Dougherty, M
Drossart, P
Flasar, FM
Fouchet, T
Frampton, R
Franchi, I
Gautier, D
Gurvits, L
Hueso, R
Kazeminejad, B
Krimigis, T
Jambon, A
Jones, G
Langevin, Y
Leese, M
Lellouch, E
Lunine, J
Milillo, A
Mahaffy, P
Mauk, B
Morse, A
Moreira, M
Moussas, X
Murray, C
Mueller-Wodarg, I
Owen, TC
Pogrebenko, S
Prange, R
Read, P
Sanchez-Lavega, A
Sarda, P
Stam, D
Tinetti, G
Zarka, P
Zarnecki, J
AF Marty, B.
Guillot, T.
Coustenis, A.
Achilleos, N.
Alibert, Y.
Asmar, S.
Atkinson, D.
Atreya, S.
Babasides, G.
Baines, K.
Balint, T.
Banfield, D.
Barber, S.
Bezard, B.
Bjoraker, G. L.
Blanc, M.
Bolton, S.
Chanover, N.
Charnoz, S.
Chassefiere, E.
Colwell, J. E.
Deangelis, E.
Dougherty, M.
Drossart, P.
Flasar, F. M.
Fouchet, T.
Frampton, R.
Franchi, I.
Gautier, D.
Gurvits, L.
Hueso, R.
Kazeminejad, B.
Krimigis, T.
Jambon, A.
Jones, G.
Langevin, Y.
Leese, M.
Lellouch, E.
Lunine, J.
Milillo, A.
Mahaffy, P.
Mauk, B.
Morse, A.
Moreira, M.
Moussas, X.
Murray, C.
Mueller-Wodarg, I.
Owen, T. C.
Pogrebenko, S.
Prange, R.
Read, P.
Sanchez-Lavega, A.
Sarda, P.
Stam, D.
Tinetti, G.
Zarka, P.
Zarnecki, J.
CA Kronos Consortium
TI Kronos: exploring the depths of Saturn with probes and remote sensing
through an international mission
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Saturn; Atmosphere; Probes; Cosmic vision
ID CASSINI IMAGING SCIENCE; DEEP ZONAL WINDS; MASS-SPECTROMETER; GIANT
PLANETS; CLOUD LEVEL; JUPITERS ATMOSPHERE; MOIST CONVECTION; EQUATORIAL
JET; INSTRUMENT; ABUNDANCES
AB Kronos is a mission aimed to measure in situ the chemical and isotopic compositions of the Saturnian atmosphere with two probes and also by remote sensing, in order to understand the origin, formation, and evolution of giant planets in general, including extrasolar planets. The abundances of noble gases, hydrogen, carbon, nitrogen, oxygen, sulfur and their compounds, as well as of the D/H, He-4/He-3, Ne-22/Ne-21/Ne-20, Ar-36/Ar-38, C-13/C-12, N-15/N-14, O-18/(O-17)/O-16, Xe-136/Xe-134/Xe-132/Xe-130/Xe-129 isotopic ratios will be measured by mass spectrometry on two probes entering the atmosphere of Saturn at two different locations near mid-latitudes, down to a pressure of 10 Bar. The global composition of Saturn will be investigated through these measurements, together with microwave radiometry determination of H2O and NH3 and their 3D variations. The dynamics of Saturn's atmosphere will be investigated from: (1) measurements of pressure, temperature, vertical distribution of clouds and wind speed along the probes' descent trajectories, and (2) determination of deep winds, differential rotation and convection with combined probe, gravity and radiometric measurements. Besides these primary goals, Kronos will also measure the intensities and characteristics of Saturn's magnetic field inside the D ring as well as Saturn's gravitational field, in order to constrain the abundance of heavy elements in Saturn's interior and in its central core. Depending on the preferred architecture (flyby versus orbiter), Kronos will be in a position to measure the properties of Saturn's innermost magnetosphere and to investigate the ring structure in order to understand how these tiny structures could have formed and survived up to the present times.
C1 [Marty, B.] Nancy Univ, CNRS, CRPG, F-54501 Vandoeuvre Les Nancy, France.
[Guillot, T.] Observ Cote Azur, F-06304 Nice 04, France.
[Coustenis, A.; Bezard, B.; Drossart, P.; Fouchet, T.; Gautier, D.; Lellouch, E.; Prange, R.; Zarka, P.] Observ Paris, LESIA, F-92195 Meudon, France.
[Alibert, Y.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Asmar, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Atkinson, D.] Univ Idaho, Dept Elect & Comp Engn, Moscow, ID 83844 USA.
[Atreya, S.] Univ Michigan, Dept Atmosphere Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Babasides, G.; Moussas, X.] Univ Athens, Fac Phys, Astrophys Lab, Space Grp, Athens 15783, Greece.
[Baines, K.; Balint, T.] Jet Prop Lab, Paadena, CA 91109 USA.
[Banfield, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Barber, S.; Franchi, I.; Leese, M.; Morse, A.; Zarnecki, J.] Open Univ, Milton Keynes MK7 6AA, Bucks, England.
[Bjoraker, G. L.; Flasar, F. M.; Mahaffy, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blanc, M.] Ctr Etud Spatiale Rayonnements, Toulouse, France.
[Bolton, S.] SW Res Inst, San Antonio, TX USA.
[Chanover, N.] New Mexico State Univ, Las Cruces, NM 88003 USA.
[Charnoz, S.] Univ Paris 07, CEA, CNRS, AIM, F-91191 Gif Sur Yvette, France.
[Chassefiere, E.] CNRS, Serv Aeron, IPSL, F-91371 Verrieres Le Buisson, France.
[Colwell, J. E.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Deangelis, E.; Milillo, A.] NAF Inst Fis Spazio Interplanetario, I-00133 Rome, Italy.
[Frampton, R.] Boeing NASA Syst, Huntington Beach, CA 92647 USA.
[Gurvits, L.; Pogrebenko, S.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands.
[Hueso, R.; Sanchez-Lavega, A.] Univ Basque Country, Dept Fis Aplicada 1, ETS Ingenieros, Bilbao 48013, Spain.
[Kazeminejad, B.] GSOC, DLR, D-82234 Wessling, Germany.
[Krimigis, T.; Mauk, B.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Jambon, A.] Univ Paris 07, MAGIE UMR 7047, F-75252 Paris 05, France.
[Jones, G.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, Katlenburg Lindau, Germany.
[Langevin, Y.] Inst Astrophys Spatiale, F-91405 Orsay, France.
[Lunine, J.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Moreira, M.] Univ Paris 07, Inst Phys Globe, CNRS, Lab Geochim & Cosmochim,UMR 7579, F-75252 Paris 05, France.
[Owen, T. C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Sarda, P.] Univ Paris 11, Dept Sci Terre, Grp Geochim Gaz Rares, IDES,CNRS,UMR 8148, F-81405 Orsay, France.
[Tinetti, G.] Univ Paris 06, CNRS, Inst Astrophys, F-75014 Paris, France.
[Stam, D.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
[Read, P.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England.
[Murray, C.] Univ London, Univ London Queen Mary & Westfield Coll, London E1 4NS, England.
[Mueller-Wodarg, I.] Univ London, Univ London Imperial Coll Sci Technol & Med, Space & Atmosphere Phs Grp, London SW7 2BW, England.
[Dougherty, M.] Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England.
[Achilleos, N.] UCL, Dept Phys & Astron, Atmospher Phys Lab, London WC1E 6BT, England.
RP Marty, B (reprint author), Nancy Univ, CNRS, CRPG, BP 20, F-54501 Vandoeuvre Les Nancy, France.
EM bmarty@crpg.cnrs-nancy.fr; guillot@obs-nice.fr;
Athena.Coustenis@obspm.fr
RI Appourchaux, Thierry/F-4692-2010; Flasar, F Michael/C-8509-2012;
Bjoraker, Gordon/D-5032-2012; Mahaffy, Paul/E-4609-2012; Jones,
Geraint/C-1682-2008; Mueller-Wodarg, Ingo/M-9945-2014; Fouchet,
Thierry/C-6374-2017; Mauk, Barry/E-8420-2017
OI Milillo, Anna/0000-0002-0266-2556; Hueso, Ricardo/0000-0003-0169-123X;
Tinetti, Giovanna/0000-0001-6058-6654; Jones,
Geraint/0000-0002-5859-1136; Sanchez-Lavega,
Agustin/0000-0001-7355-1522; Achilleos, Nicholas/0000-0002-5886-3509;
Banfield, Don/0000-0003-2664-0164; Mueller-Wodarg,
Ingo/0000-0001-6308-7826; Fouchet, Thierry/0000-0001-9040-8285; Mauk,
Barry/0000-0001-9789-3797
NR 62
TC 6
Z9 6
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 3
BP 947
EP 976
DI 10.1007/s10686-008-9094-9
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409RP
UT WOS:000263523800008
ER
PT J
AU Turck-Chieze, S
Lamy, P
Carr, C
Carton, PH
Chevalier, A
Dandouras, I
Defise, JM
Dewitte, S
de Wit, TD
Halain, JP
Hasan, S
Hochedez, JF
Horbury, T
Levacher, P
Meissonier, M
Murphy, N
Rochus, P
Ruzmaikin, A
Schmutz, W
Thuillier, G
Vives, S
AF Turck-Chieze, S.
Lamy, P.
Carr, C.
Carton, P. H.
Chevalier, A.
Dandouras, I.
Defise, J. M.
Dewitte, S.
de Wit, T. Dudok
Halain, J. P.
Hasan, S.
Hochedez, J. F.
Horbury, T.
Levacher, P.
Meissonier, M.
Murphy, N.
Rochus, P.
Ruzmaikin, A.
Schmutz, W.
Thuillier, G.
Vives, S.
TI The DynaMICCS perspective A mission for a complete and continuous view
of the Sun dedicated to magnetism, space weather and space climate
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Global solar magnetism; Formation flying; Solar activity; Solar
variability; Solar wind-irradiance; Solar gravity; Acoustic modes
ID ROTATING STARS; RADIATION ZONES; MERIDIONAL CIRCULATION; FIELD
MEASUREMENTS; STELLAR EVOLUTION; QUADRUPOLE-MOMENT; SOLAR TACHOCLINE;
GRAVITY MODES; TRANSPORT; IRRADIANCE
AB The DynaMICCS mission is designed to probe and understand the dynamics of crucial regions of the Sun that determine solar variability, including the previously unexplored inner core, the radiative/convective zone interface layers, the photosphere/chromosphere layers and the low corona. The mission delivers data and knowledge that no other known mission provides for understanding space weather and space climate and for advancing stellar physics (internal dynamics) and fundamental physics (neutrino properties, atomic physics, gravitational moments...). The science objectives are achieved using Doppler and magnetic measurements of the solar surface, helioseismic and coronographic measurements, solar irradiance at different wavelengths and in-situ measurements of plasma/energetic particles/magnetic fields. The DynaMICCS payload uses an original concept studied by ThalSs Alenia Space in the framework of the CNES call for formation flying missions: an external occultation of the solar light is obtained by putting an occulter spacecraft 150 m (or more) in front of a second spacecraft. The occulter spacecraft, a LEO platform of the mini sat class, e.g. PROTEUS, type carries the helioseismic and irradiance instruments and the formation flying technologies. The latter spacecraft of the same type carries a visible and infrared coronagraph for a unique observation of the solar corona and instrumentation for the study of the solar wind and imagers. This mission must guarantee long (one 11-year solar cycle) and continuous observations (duty cycle > 94%) of signals that can be very weak (the gravity mode detection supposes the measurement of velocity smaller than 1 mm/s). This assumes no interruption in observation and very stable thermal conditions. The preferred orbit therefore is the L1 orbit, which fits these requirements very well and is also an attractive environment for the spacecraft due to its low radiation and low perturbation (solar pressure) environment. This mission is secured by instrumental R and D activities during the present and coming years. Some prototypes of different instruments are already built (GOLFNG, SDM) and the performances will be checked before launch on the ground or in space through planned missions of CNES and PROBA ESA missions (PICARD, LYRA, maybe ASPIICS).
C1 [Turck-Chieze, S.; Carton, P. H.] CEA, DSM, IRFU CE Saclay, F-91191 Gif Sur Yvette, France.
[Lamy, P.; Levacher, P.; Vives, S.] Lab Astrophys Marseille, F-13376 Marseille 12, France.
[Chevalier, A.; Dewitte, S.; Hochedez, J. F.] Royal Meteorol Inst Belgium, B-1180 Brussels, Belgium.
[Dandouras, I.] CNRS, CESR, Toulouse, France.
[Defise, J. M.; Halain, J. P.; Rochus, P.] Ctr Spatial Liege, Angleur, Belgium.
[de Wit, T. Dudok] CNRS, LPCE, F-45071 Orleans 2, France.
[Hasan, S.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[Murphy, N.; Ruzmaikin, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Meissonier, M.; Thuillier, G.] CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France.
[Schmutz, W.] PMOD WRC, CH-7260 Davos, Switzerland.
[Carr, C.; Horbury, T.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England.
RP Turck-Chieze, S (reprint author), CEA, DSM, IRFU CE Saclay, F-91191 Gif Sur Yvette, France.
EM cturck@cea.fr
RI Schmutz, Werner/B-4153-2014;
OI Schmutz, Werner/0000-0003-1159-5639; Dandouras,
Iannis/0000-0002-7121-1118
NR 72
TC 15
Z9 15
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 3
BP 1017
EP 1055
DI 10.1007/s10686-008-9111-z
PG 39
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409RP
UT WOS:000263523800012
ER
PT J
AU Maksimovic, M
Velli, M
AF Maksimovic, M.
Velli, M.
TI PHOIBOS: probing heliospheric origins with an inner boundary observing
spacecraft
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Solar corona; Solar wind acceleration; Coronal heating; Space mission
ID SOLAR-WIND; CORONAL HOLE; ALFVEN WAVES; TEMPERATURE; VELOCITY; MODEL;
ION; ACCELERATION; TURBULENCE; UVCS/SOHO
AB The earth is immersed in a hot, rarefied, energetic flow of particles and electromagnetic fields originating from the Sun and engulfing the entire solar system, forming the heliosphere. The existence of the solar wind has been established for almost 50 years now, and abundant data has been accumulated concerning both its average properties and the intermittent, violent energetic manifestations known as Coronal Mass Ejections which often impact the earth's magnetosphere (causing geomagnetic storms and aurorae). The mystery of how the solar corona is heated and the solar wind is accelerated remains unsolved, however, because of the large gap in our knowledge of the inner region of the heliosphere, inside the orbit of mercury. The PHOIBOS mission, with a perihelion at 4 R-s, by accessing the regions where energy in the coronal plasma is channeled from internal, magnetic and turbulent energy into bulk energy of the solar wind flow aims to solve the question of why the Sun has a hot corona and produces a solar wind. The PHOIBOS mission builds on previous Solar Probe studies, but provides an alternative orbit scenario avoiding a Jupiter encounter in favor of multiple Venus encounters and SEP systems to work its way close to the Sun in a gradual manner, providing a much vaster data return.
C1 [Maksimovic, M.] Univ Paris Diderot, CNRS, UPMC, LESIA,Observ Paris, F-92195 Meudon, France.
[Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Velli, M.] Univ Florence, Florence, Italy.
RP Maksimovic, M (reprint author), Univ Paris Diderot, CNRS, UPMC, LESIA,Observ Paris, F-92195 Meudon, France.
EM milan.maksimovic@obspm.fr
FU NASA SEC Advanced Studies; CNES
FX M. Velli would like to thank D. McComas and W. Lewis for many useful
discussions and E. Podlachikova for providing Fig. 11. M Velli was
partially supported by NASA SEC Advanced Studies. Milan Maksimovic would
like to thank the CNES since the overall mission profile presented here
is the outcome of a specific CNES/PASO study conducted by Regis Bertrand
for the trajectory, Emmanuel Hinglais for the system analysis and
Jean-Yves Prado for the overall concept. This study has been performed
in the frame of the CNES support to the French scientific contributors
to the ESA "Cosmic Vision" call. The spacecraft accommodation has been
provided by EADS/Astrium. Finally the authors would like to thank the
PHOIBOS scientific team composed by Thierry Appourchaux, Bruno
Bavassano, Stuart D. Bale, Matthieu Berthomier, Douglas Biesecker, Lars
Blomberg, Peter Bochsler, Volker Bothmer, Jean-Louis Bougeret, Andrew
Breen, Carine Briand, Roberto Bruno, Vincenzo Carbone, Patrick Canu,
Thomas Chust, Jean-Marc Defise, Thierry Dudok de Wit, Luca Del Zanna,
Anders Eriksson, Silvano Fineschi, Lyndsay Fletcher, Keith Goetz, Roland
Grappin, Antonella Greco, Shadia Habbal, Don Hassler, Bernd Heber, Petr
Hellinger, Tim Horbury, Karine Issautier, Justin Kasper, Ludwig Klein,
Craig Kletzing, S m Krucker, Vladimir Krasnoselskikh, William Kurth,
Rosine Lallement, Philippe Lamy, Herve Lamy, Simone Landi, Olivier Le
Contel, Fabio Lepreti, Dominique LeQueau, Robert Lin, Milan Maksimovic,
Francesco Malara, Ian Mann, Ingrid Mann, William Matthaeus, Dave
McComas, Ralph McNutt, Nicole Meyer-Vernet, Zoran Mikic, Michel
Moncuquet, Neil Murphy, Zdenek Nemecek, Emanuele Pace, Filippo
Pantellini, Viviane Pierrard, Jean-Louis Pin on, Elena Podlachikova,
Raymond Pottelette, Lubomir Prech, Ondrej Santolik, Robert Rankin,
Franco Rappazzo, Marco Romoli, Alain Roux, Jana Safrankova, Fouad
Sahraoui, Edward C. Sittler, Luca Sorriso-Valvo, Jan Soucek, Pavel
Travnicek, Andris Vaivads, Andrea Verdini, Nicole Vilmer, Robert
Wimmer-Schweingruber, Gaetano Zimbardo, Thomas Zurbuchen, Ioannis
Zouganelis.
NR 29
TC 3
Z9 3
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 3
BP 1057
EP 1078
DI 10.1007/s10686-008-9113-x
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409RP
UT WOS:000263523800013
ER
PT J
AU Appourchaux, T
Liewer, P
Watt, M
Alexander, D
Andretta, V
Auchere, F
D'Arrigo, P
Ayon, J
Corbard, T
Fineschi, S
Finsterle, W
Floyd, L
Garbe, G
Gizon, L
Hassler, D
Harra, L
Kosovichev, A
Leibacher, J
Leipold, M
Murphy, N
Maksimovic, M
Martinez-Pillet, V
Matthews, BSA
Mewaldt, R
Moses, D
Newmark, J
Regnier, S
Schmutz, W
Socker, D
Spadaro, D
Stuttard, M
Trosseille, C
Ulrich, R
Velli, M
Vourlidas, A
Wimmer-Schweingruber, CR
Zurbuchen, T
AF Appourchaux, T.
Liewer, P.
Watt, M.
Alexander, D.
Andretta, V.
Auchere, F.
D'Arrigo, P.
Ayon, J.
Corbard, T.
Fineschi, S.
Finsterle, W.
Floyd, L.
Garbe, G.
Gizon, L.
Hassler, D.
Harra, L.
Kosovichev, A.
Leibacher, J.
Leipold, M.
Murphy, N.
Maksimovic, M.
Martinez-Pillet, V.
Matthews, B. S. A.
Mewaldt, R.
Moses, D.
Newmark, J.
Regnier, S.
Schmutz, W.
Socker, D.
Spadaro, D.
Stuttard, M.
Trosseille, C.
Ulrich, R.
Velli, M.
Vourlidas, A.
Wimmer-Schweingruber, C. R.
Zurbuchen, T.
TI POLAR investigation of the Sun-POLARIS
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Solar physics; Magnetism; Interior; Corona; Polar observations; Coronal
mass ejections; Dynamo; Solar cycle; Convection; High latitude; Space
weather
ID UPPER CONVECTION ZONE; SOLAR-WIND; ACTIVE-REGION; OSCILLATIONS; ORIGIN
AB The POLAR Investigation of the Sun (POLARIS) mission uses a combination of a gravity assist and solar sail propulsion to place a spacecraft in a 0.48 AU circular orbit around the Sun with an inclination of 75A degrees with respect to solar equator. This challenging orbit is made possible by the challenging development of solar sail propulsion. This first extended view of the high-latitude regions of the Sun will enable crucial observations not possible from the ecliptic viewpoint or from Solar Orbiter. While Solar Orbiter would give the first glimpse of the high latitude magnetic field and flows to probe the solar dynamo, it does not have sufficient viewing of the polar regions to achieve POLARIS's primary objective: determining the relation between the magnetism and dynamics of the Sun's polar regions and the solar cycle.
C1 [Appourchaux, T.; Auchere, F.; Leibacher, J.; Trosseille, C.] Inst Astrophys Spatiale, Orsay, France.
[Liewer, P.; Ayon, J.; Murphy, N.; Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Watt, M.; D'Arrigo, P.; Stuttard, M.] EADS Astrium, Stevenage, Herts, England.
[Alexander, D.] Rice Univ, Houston, TX USA.
[Andretta, V.; Fineschi, S.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Corbard, T.] Observ Cote Azur, F-06003 Nice, France.
[Finsterle, W.; Schmutz, W.] PMOD WRC, Davos, Switzerland.
[Floyd, L.] Interferometrics Inc, Herndon, VA USA.
[Garbe, G.] Natl Space Sci & Technol Ctr, Huntsville, AL USA.
[Gizon, L.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Hassler, D.] SW Res Inst, Boulder, CO USA.
[Kosovichev, A.] Stanford Univ, Stanford, CA 94305 USA.
[Leibacher, J.] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA.
[Leipold, M.] Kayser Threde GmbH, Munich, Germany.
[Maksimovic, M.] Observ Paris, Meudon, France.
[Martinez-Pillet, V.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Moses, D.; Newmark, J.; Socker, D.; Vourlidas, A.] USN, Res Lab, Washington, DC 20375 USA.
[Spadaro, D.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy.
[Ulrich, R.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Wimmer-Schweingruber, C. R.] Univ Kiel, Kiel, Germany.
[Zurbuchen, T.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Regnier, S.] Univ St Andrews, St Andrews, Fife, Scotland.
[Harra, L.; Matthews, B. S. A.] Mullard Space Sci Lab, Holmbury, England.
RP Appourchaux, T (reprint author), Inst Astrophys Spatiale, Orsay, France.
EM Thierry.Appourchaux@ias.u-psud.fr
RI Gizon, Laurent/B-9457-2008; Vourlidas, Angelos/C-8231-2009; Matthews,
Sarah/C-4292-2008; Regnier, Stephane/H-9107-2012; Schmutz,
Werner/B-4153-2014; Regnier, Stephane/K-2423-2015;
OI Leibacher, John/0000-0001-7605-3684; Vourlidas,
Angelos/0000-0002-8164-5948; Regnier, Stephane/0000-0001-8954-4183;
Schmutz, Werner/0000-0003-1159-5639; Regnier,
Stephane/0000-0001-8954-4183; Harra, Louise/0000-0001-9457-6200;
Auchere, Frederic/0000-0003-0972-7022; Spadaro,
Daniele/0000-0003-3517-8688; Andretta, Vincenzo/0000-0003-1962-9741
NR 35
TC 7
Z9 8
U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
J9 EXP ASTRON
JI Exp. Astron.
PD MAR
PY 2009
VL 23
IS 3
BP 1079
EP 1117
DI 10.1007/s10686-008-9107-8
PG 39
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 409RP
UT WOS:000263523800014
ER
PT J
AU Bushnell, D
AF Bushnell, Dennis
TI Algae: A Panacea Crop?
SO FUTURIST
LA English
DT Editorial Material
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Bushnell, D (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WORLD FUTURE SOC
PI BETHESDA
PA 7910 WOODMONT AVE, STE 450, BETHESDA, MD 20814 USA
SN 0016-3317
J9 FUTURIST
JI Futurist
PD MAR-APR
PY 2009
VL 43
IS 2
BP 29
EP 29
PG 1
WC Social Issues
SC Social Issues
GA 404LD
UT WOS:000263152400013
ER
PT J
AU Chen, JH
Papanastassiou, DA
Wasserburg, GJ
AF Chen, J. H.
Papanastassiou, D. A.
Wasserburg, G. J.
TI A search for nickel isotopic anomalies in iron meteorites and chondrites
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID EARLY SOLAR-SYSTEM; REFRACTORY INCLUSIONS; ALLENDE INCLUSIONS; CHROMIUM
ISOTOPES; HYDROCHLORIC ACID; NEARBY SUPERNOVA; CATION EXCHANGE; FE-60;
ELEMENTS; INJECTION
AB We report Ni isotopic data, for (58,60-62)Ni, on (1) FeNi metal and sulfides in different groups of iron meteorites, (2) sulfides and a whole rock sample of the St. Severin chondrite, and (3) chondrules from the Chainpur chondrite. We have developed improved, Multiple-Collector, Positive ion Thermal Ionization Mass Spectrometric (MC-PTIMS) techniques, with Ni(+) ionization efficiency at 1 parts per thousand, and chemical separation techniques for Ni which reduce mass interferences to the I ppm level, so that no mass interference corrections need be applied, except for (64)Ni (from (64)Zn, at the 0.1 parts per thousand level), for which we do not report results. We normalize the data to (62)Ni/(58)Ni to correct for mass dependent isotope fractionation. No evidence was found for resolved radiogenic or general Ni isotope anomalies at the resolution levels of 0.2 and 0.5 epsilon u (epsilon u = 0.01%) for (60)Ni/(58)Ni and (61)Ni/(58)Ni, respectively. From the (56)Fe/(58)Ni ratios and epsilon((60)Ni/(58)Ni) values, we calculate upper limits for the initial value of ((60)Fe/(56)Fe)(0) of (a) <2.7 x 10(-7) for Chainpur chondrules, (b) <10(-8) for the St. Severin sulfide, and (c) <4 x 10(-9) for sulfides from iron meteorites. We measured some of the same meteorites measured by other workers, who reported isotopic anomalies in Ni, using Multiple-Collector, Inductively-Coupled Mass Spectrometry. Our results do not support the previous reports of Ni isotopic anomalies in sulfide samples from Mundrabilla by Cook et al. [Cook D. L., Clayton R. N., Wadhwa, M., Janney P. E., and Davis A. M. (2008). Nickel isotopic anomalies in troilite from iron meteorites. Geophy. Res. Lett. 35, L01203] and in sulfides from Toluca and Odessa by Quitte et al. [Quitte G., Meier M., Latkoczy C., Halliday A. N., and Gunther D., (2006). Nickel isotopes in iron meteorites-nucleosynthetic anomalies in sulfides with no effects in metals and no trace of (60)Fe. Earth Planet. Sci. Lett. 242, 16-25]. Hence, we find no need for specialized physical-chemical planetary processes for the preservation of different Ni isotope compositions, between FeNi metal and sulfides in the same iron meteorites, as proposed by the above reports nor for complex astrophysical scenarios to provide the very peculiar Ni isotope anomalies reported by these workers for sulfides. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Chen, J. H.; Papanastassiou, D. A.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA.
[Papanastassiou, D. A.; Wasserburg, G. J.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Chen, JH (reprint author), CALTECH, Jet Prop Lab, Div Sci, MIS 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM James.H.Chen@jpl.nasa.gov
FU NASA Cosmochemistry [RTOP 344-31-55-01]; JPL RTD [R.03.019.006]
FX We thank D.L. Cook for a careful and fair review. This work was carried
out at the Jet Propulsion Laboratory, California Institute of Technology
and supported by NASA Cosmochemistry (RTOP 344-31-55-01). D.A.
Papanastassiou was supported, in part by JPL RTD (Task R.03.019.006).
NR 41
TC 28
Z9 28
U1 0
U2 15
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD MAR 1
PY 2009
VL 73
IS 5
BP 1461
EP 1471
DI 10.1016/j.gca.2008.11.040
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 412GX
UT WOS:000263714300016
ER
PT J
AU Righter, K
Humayun, M
Campbell, AJ
Danielson, L
Hill, D
Drake, MJ
AF Righter, K.
Humayun, M.
Campbell, A. J.
Danielson, L.
Hill, D.
Drake, M. J.
TI Experimental studies of metal-silicate partitioning of Sb: Implications
for the terrestrial and lunar mantles
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID HIGH PARTIAL PRESSURES; CALCIUM FERRITE SLAG; EUCRITE PARENT BODY; CORE
FORMATION; SIDEROPHILE ELEMENTS; OXIDATION-STATE; MELT COMPOSITION;
OXYGEN FUGACITY; PHASE-EQUILIBRIUM; OCEANIC BASALTS
AB The terrestrial mantle has a well defined Sb depletion of similar to 7 +/- 1 (Jochum and Hofmann, 1997), and the lunar mantle is depleted relative to the Earth by a factor of similar to 50 +/- 5 (Wolf and Anders, 1980). Despite these well defined depletions, there are few data upon which to evaluate their origin-whether due to volatility or core formation. We have carried out a series of experiments to isolate several variables such as oxygen fugacity, temperature, pressure, and silicate and metallic melt compositions, on the magnitude of D(Sb)(met/sil). The activity of Sb in FeNi metal is strongly composition dependent such that solubility of Sb as a function of fO(2) must be corrected for the metal composition. When the correction is applied, Sb solubility is consistent with 3+ valence. Temperature series (at 1.5 GPa) shows that D(Sb)(met/sil) decreases by a factor of 100 over 400 degrees C, and a pressure series exhibits an additional decrease between ambient pressure (100 MPa) and 13 GPa. A strong dependence upon silicate melt composition is evident from a factor of 100 decrease in D(Sb)(met/sil) between nbo/t values of 0.3 and 1.7. Consideration of all these variables indicates that the small Sb depletion for the Earth's mantle can be explained by high PT equilibrium partitioning between metal and silicate melt D(Sb)(met/sil). The relatively large lunar Sb depletion can also be explained by segregation of a small metallic core, at lower pressure conditions where D(Sb)(met/sil) is much higher (2500). Published by Elsevier Ltd.
C1 [Righter, K.; Danielson, L.] NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA.
[Righter, K.; Hill, D.; Drake, M. J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Humayun, M.; Campbell, A. J.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Humayun, M.] Florida State Univ, Natl High Magnet Field Lab, Tallahassee, FL 32310 USA.
[Campbell, A. J.] Univ Maryland, Dept Geol, College Pk, MD 20742 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
OI Humayun, Munir/0000-0001-8516-9435
NR 99
TC 10
Z9 10
U1 1
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD MAR 1
PY 2009
VL 73
IS 5
BP 1487
EP 1504
DI 10.1016/j.gca.2008.11.042
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 412GX
UT WOS:000263714300018
ER
PT J
AU de Linage, C
Rivera, L
Hinderer, J
Boy, JP
Rogister, Y
Lambotte, S
Biancale, R
AF de Linage, Caroline
Rivera, Luis
Hinderer, Jacques
Boy, Jean-Paul
Rogister, Yves
Lambotte, Sophie
Biancale, Richard
TI Separation of coseismic and postseismic gravity changes for the 2004
Sumatra-Andaman earthquake from 4.6 yr of GRACE observations and
modelling of the coseismic change by normal-modes summation
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Satellite geodesy; Seismic cycle; Transient deformation; Time variable
gravity; Subduction zone processes; Dynamics: gravity and tectonics
ID GPS MEASUREMENTS; RUPTURE; DEFORMATION; DECEMBER; SYSTEM
AB This paper is devoted to the simultaneous determination of the coseismic and postseismic gravitational changes caused by the great 2004 December 26 Sumatra-Andaman earthquake from the time-variable global gravity fields recovered by the Gravity Recovery And Climate Experiment (GRACE) mission. Furthermore, a complete modelling of the elasto-gravitational response of a self-gravitating, spherically layered, elastic earth model is carried out using a normal-modes summation for comparison with the observed coseismic gravitational change. Special attention is paid to the ocean mass redistribution. Special care is paid during the inversion of the data to avoid contamination of tectonic gravity changes by ocean tidal model errors, seasonal and interannual signals originating from continental hydrology and oceanic circulation as well as contamination of the coseismic gravity change by the postseismic relaxation. We use a 4.6-yr-long time-series of global gravity solutions including 26 months of postseismic data, provided by the Groupe de Recherche en GEodEsie Spatiale (GRGS). For comparison, the Release-04 solutions of the Center for Space Research (CSR) are also investigated after a spectral windowing or a Gaussian spatial smoothing. Results are shown both in terms of geoid height changes and gravity variations. Coseismic and postseismic gravitational changes estimated from the different gravity solutions are globally similar, although their spatial extent and amplitude depend on the type of filter used in the processing of GRACE fields. The highest signal-to-noise ratio is found with the GRGS solutions. The postseismic signature has a spectral content closer to the GRACE bandwidth than the coseismic signature and is therefore better detected by GRACE. The coseismic signature consists mainly of a strong gravity decrease east of the Sunda trench, in the Andaman Sea. A gravity increase is also detected at a smaller scale, west of the trench. The model for the coseismic gravity changes agrees well with the coseismic signature estimated from GRACE, regarding the overall shape and orientation, location with respect to the trench and order of magnitude. Coseismic gravity changes are followed by a postseismic relaxation that are well fitted by an increasing exponential function with a mean relaxation time of 0.7 yr. The total postseismic gravity change consists of a large-scale positive anomaly centred above the trench and extending over 15 degrees of latitude along the subduction. After 26 months, the coseismic gravity decrease has been partly compensated by the postseismic relaxation, but a negative anomaly still remains south of Phuket. A dominant gravity increase extends over 15 degrees of latitude west of the trench, being maximal south of the epicentre area. By investigating analyses of two global hydrology models and one ocean general circulation model, we show that our GRACE estimates of the coseismic and postseismic gravitational changes are almost not biased by interannual variations originating from continental hydrology and ocean circulation in the subduction area and in the central part of the Andaman Sea, while they are biased by several mu Gal in the Malay Peninsula.
C1 [de Linage, Caroline; Rivera, Luis; Hinderer, Jacques; Boy, Jean-Paul; Rogister, Yves] ULP, CNRS, UMR 7516, EOST,IPGS, F-67084 Strasbourg, France.
[de Linage, Caroline] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Boy, Jean-Paul] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Lambotte, Sophie] Ecole Normale Super, Geol Lab, UMR 8538, F-75231 Paris 5, France.
[Biancale, Richard] GRGS, CNES, F-31401 Toulouse 9, France.
RP de Linage, C (reprint author), ULP, CNRS, UMR 7516, EOST,IPGS, 5 Rue Rene Descartes, F-67084 Strasbourg, France.
EM caroline.delinage@uci.edu
RI Boy, Jean-Paul/E-6677-2017
OI Boy, Jean-Paul/0000-0003-0259-209X
NR 46
TC 44
Z9 44
U1 2
U2 12
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
EI 1365-246X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD MAR
PY 2009
VL 176
IS 3
BP 695
EP 714
DI 10.1111/j.1365-246X.2008.04025.x
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 408RN
UT WOS:000263452600004
ER
PT J
AU Eke, VR
Teodoro, LFA
Elphic, RC
AF Eke, V. R.
Teodoro, L. F. A.
Elphic, R. C.
TI The spatial distribution of polar hydrogen deposits on the Moon
SO ICARUS
LA English
DT Article
DE Data reduction techniques; Image processing; Moon, surface
ID BAYESIAN IMAGE-RECONSTRUCTION; LUNAR SOUTH-POLE; WATER ICE; MERCURY;
FLUXES; PIXON
AB A new analysis of the Lunar Prospector epithermal neutron data is presented, providing an improved map of the distribution of hydrogen near to the lunar poles. This is achieved using a specially developed pixon image reconstruction algorithm to deconvolve the instrumental response of the Lunar Prospector's neutron spectrometer from the observed data, while simultaneously suppressing the statistical noise. The results show that these data alone require the hydrogen to be concentrated into the cold traps at up to 1 wt% water-equivalent hydrogen. This combination of localisation and high concentration suggests that the hydrogen is present either in the form of a volatile compound or as solar wind protons implanted into small regolith grains. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Eke, V. R.] Univ Durham, Dept Phys, Inst Computat Cosmol, Sci Labs, Durham DH1 3LE, England.
[Teodoro, L. F. A.] Univ Glasgow, Astron & Astrophys Grp, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Elphic, R. C.] NASA, Ames Res Ctr, Planetary Syst Branch, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
RP Eke, VR (reprint author), Univ Durham, Dept Phys, Inst Computat Cosmol, Sci Labs, South Rd, Durham DH1 3LE, England.
EM v.r.eke@durham.ac.uk
FU Royal Society University Research Fellowship; Leverhulme Research
Fellowship; NASA Lunar Reconnaissance Orbiter Participating Scientist
Grant
FX We would like to thank Bill Feldman for helpful discussions. V.R.E.
acknowledges the support of a Royal Society University Research
Fellowship. L.F.A.T. acknowledges the support of a Leverhulme Research
Fellowship. R.C.E. acknowledges the support of a NASA Lunar
Reconnaissance Orbiter Participating Scientist Grant.
NR 22
TC 20
Z9 20
U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2009
VL 200
IS 1
BP 12
EP 18
DI 10.1016/j.icarus.2008.10.013
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 419IN
UT WOS:000264213000002
ER
PT J
AU Horne, D
Smith, MD
AF Horne, David
Smith, Michael D.
TI Mars Global Surveyor Thermal Emission Spectrometer (TES) observations of
variations in atmospheric dust optical depth over cold surfaces
SO ICARUS
LA English
DT Article
DE Mars, atmosphere; Mars, surface; Mars, climate; Mars, polar caps
ID ORBITER CAMERA OBSERVATIONS; INTERANNUAL VARIABILITY; MARTIAN
ATMOSPHERE; STORMS; TEMPERATURES; AEROBRAKING
AB The Mars Global Surveyor Thermal Emission Spectrometer (TES) instrument has returned over 200 million thermal infrared spectra of Mars taken between March 1999 and August 2004. This represents one of the most complete records of spatial and temporal changes of the martian atmosphere ever recorded by an orbiting spacecraft. Previous reports of the standard TES retrieval of aerosol optical depth have been limited to those observations taken over surfaces with temperatures above 210 K, limiting the spatiotemporal coverage of Polar Regions with TES. Here, we present an extension to the standard TES retrieval that better models the effects of cold surfaces below 200 K. This modification allows aerosol optical depth to be retrieved from TES spectra over a greater spatiotemporal range than was previously possible, specifically in Polar Regions. This new algorithm is applied to the Polar Regions to show the seasonal variability in dust and ice optical depth for the complete temporal range of the TES database (Mars Year 24, L(s) = 104 degrees, 1 March 1999 to Mars Year 24, L(s) = 82 degrees, 31 August 2004). (C) 2008 Elsevier Inc. All rights reserved.
C1 [Horne, David] Univ Missouri, St Louis, MO 63121 USA.
[Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20071 USA.
RP Horne, D (reprint author), Univ Missouri, 503 Benton Hall, St Louis, MO 63121 USA.
EM horneda@umsl.edu
RI Smith, Michael/C-8875-2012
NR 22
TC 5
Z9 5
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 MAR
PY 2009
VL 200
IS 1
BP 118
EP 128
DI 10.1016/j.icarus.2008.11.007
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 419IN
UT WOS:000264213000009
ER
PT J
AU Lim, LF
Nittler, LR
AF Lim, Lucy F.
Nittler, Larry R.
TI Elemental composition of 433 Eros: New calibration of the NEAR-Shoemaker
XRS data
SO ICARUS
LA English
DT Article
DE Asteroid Eros; Asteroids, composition; Asteroids, surfaces; Asteroids
ID DIFFERENTIAL EMISSION MEASURE; X-RAY SPECTROMETER; CORONAL CALCIUM
ABUNDANCE; ATOMIC DATABASE; FLARE PLASMAS; SOLAR-FLARES; MISSION; IRON;
TEMPERATURE; SPECTRA
AB We present a new calibration of the elemental-abundance data for Asteroid 433 Eros taken by the X-ray spectrometer (XRS) aboard the NEAR-Shoemaker spacecraft. (NEAR is an acronym for "Near-Earth Asteroid Rendezvous.") Quantification of the asteroid Surface elemental abundance ratios depends critically on accurate knowledge of the incident solar X-ray spectrum, which was monitored simultaneously with asteroid observations. Previously published results suffered from incompletely characterized systematic uncertainties due to an imperfect ground calibration of the NEAR gas solar monitor. The solar monitor response function and associated uncertainties have now been characterized by cross-calibration of a large sample of NEAR solar monitor flight data against contemporary broadband solar X-ray data from the Earth-orbiting GOES-8 (Geostationary Operational Environmental Satellite). The results have been used to analyze XRS spectra acquired from Eros during eight major solar flares (including three that have not previously been reported). The end product of this analysis is a revised set of Eros surface elemental abundance ratios with new error estimates that More accurately reflect the remaining uncertainties in the solar flare spectra: Mg/Si = 0.753 + 0.078/-0.055, Al/Si = 0.069 +/- 0.055, S/Si = 0.005 +/- 0.008, Ca/Si = 0.060 + 0.023/-0.024, and Fe/Si = 1.678 + 0.338/-0.320. These revised abundance ratios are consistent within cited uncertainties with the results Of Nittler et al. [Nittler, L.R., and 14 colleagues, 2001. Meteorit. Planet. Sci. 36, 1673-1695] and thus Support the prior conclusions that 433 Eros has a major-element composition similar to ordinary chondrites with the exception of a strong depletion in sulfur, most likely caused by space weathering. Published by Elsevier Inc.
C1 [Lim, Lucy F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nittler, Larry R.] Carnegie Inst Washington, Washington, DC 20015 USA.
RP Lim, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 691, Greenbelt, MD 20771 USA.
EM lucy.f.lim@nasa.gov; Inittler@ciw.edu
RI Lim, Lucy/C-9557-2012
OI Lim, Lucy/0000-0002-9696-9654
NR 57
TC 15
Z9 15
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 MAR
PY 2009
VL 200
IS 1
BP 129
EP 146
DI 10.1016/j.icarus.2008.09.018
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 419IN
UT WOS:000264213000010
ER
PT J
AU Fletcher, LN
Orton, GS
Yanamandra-Fisher, P
Fisher, BM
Parrish, PD
Irwin, PGJ
AF Fletcher, L. N.
Orton, G. S.
Yanamandra-Fisher, P.
Fisher, B. M.
Parrish, P. D.
Irwin, P. G. J.
TI Retrievals of atmospheric variables on the gas giants from ground-based
mid-infrared imaging
SO ICARUS
LA English
DT Article
DE Jupiter; Saturn; Atmospheres, composition; Atmospheres, structure;
Infrared observations; Atmospheres, dynamics
ID MERIDIONAL VARIATIONS; CASSINI CIRS; STRATOSPHERIC TEMPERATURES;
SPATIAL-ORGANIZATION; JUPITERS ATMOSPHERE; UPPER TROPOSPHERE;
TIME-DEPENDENCE; VOYAGER IRIS; SOUTH-POLE; RED-SPOT
AB Thermal-infrared imaging of Jupiter and Saturn using the NASA/IRTF and Subaru observatories are quantitatively analyzed to assess the capabilities for reproducing and extending the zonal mean atmospheric results of the Cassini/CIRS experiment. We describe the development of a robust, systematic and reproducible approach to the acquisition and reduction of planetary images in the mid-infrared (7-25 mu m), and perform an adaptation and validation of the optimal estimation, correlated-k retrieval algorithm described by Irwin et al. [Irwin, R. Teanby, N., de Kok, R., Fletcher, L., Howett, C., Tsang, C., Wilson, C., Calcutt, S., Nixon, C., Parrish, P., 2008. J. Quant. Spectrosc. Radiat. Trans. 109 (6), 1136-1150] for channel-integrated radiances. Synthetic spectral analyses and a comparison to Cassini results are used to verify our abilities to retrieve temperatures, haze opacities and gaseous abundances from filtered imaging. We find that ground-based imaging with a sufficiently high spatial resolution is able to reproduce the three-dimensional temperature and para-H-2 fields measured by spacecraft visiting Jupiter and Saturn, allowing us to investigate vertical wind shear, pressure and, with measured cloud-top winds, Ertel potential vorticity On potential temperature surfaces. Furthermore, by scaling vertical profiles of NH3, PH3, haze opacity and hydrocarbons as free parameters during thermal retrievals, we can produce meridional results comparable with CIRS spectroscopic investigations. This paper demonstrates that mid-IR imaging instruments operating at ground-based observatories have access to several dynamical and chemical diagnostics of the atmospheric state of the gas giants, offering the prospect for quantitative studies over much longer baselines and often covering much wider areas than is possible from spaceborne platforms. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Fletcher, L. N.; Orton, G. S.; Yanamandra-Fisher, P.; Fisher, B. M.; Parrish, P. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Parrish, P. D.] Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3JN, Midlothian, Scotland.
[Irwin, P. G. J.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England.
RP Fletcher, LN (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Leigh.N.Fletcher@jpl.nasa.gov
RI Fletcher, Leigh/D-6093-2011;
OI Fletcher, Leigh/0000-0001-5834-9588; Irwin, Patrick/0000-0002-6772-384X
FU National Aeronautics and Space Administration (NASA); Cassini Project;
UK Science and Technology Facilities Council
FX Fletcher was supported by an appointment to the NASA Post-doctoral
Program at the jet Propulsion Laboratory, California Institute of
Technology, under contract for the National Aeronautics and Space
Administration (NASA), administered by Oak Ridge Associated Universities
through a contract with NASA. Orton acknowledges support from the
Cassini Project and other grants from NASA to the jet Propulsion
Laboratory, California Institute of Technology. Irwin acknowledges the
support of the UK Science and Technology Facilities Council. We are
extremely grateful to Peter Read for his comments regarding the
dynamical implications of these results, and to Thierry Fouchet and one
anonymous reviewer for their constructive criticisms of this manuscript.
We thank Rick Puetter for allowing us to use the PIXON image
reconstruction algorithms. We thank the staff at the NASA/IRTF (operated
by the University of Hawaii under a cooperative agreement with NASA) and
Subaru telescope (operated by the National Astronomical Observatory of
Japan) facilities, without whom these studies Could not have been
undertaken, and we appreciate the support from the Hawaiian community in
allowing us to conduct observations from Mauna Kea.
NR 58
TC 23
Z9 23
U1 1
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR
PY 2009
VL 200
IS 1
BP 154
EP 175
DI 10.1016/j.icarus.2008.11.019
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 419IN
UT WOS:000264213000012
ER
PT J
AU Wahr, J
Selvans, ZA
Mullen, ME
Barr, AC
Collins, GC
Selvans, MM
Pappalardo, RT
AF Wahr, John
Selvans, Zane A.
Mullen, McCall E.
Barr, Amy C.
Collins, Geoffrey C.
Selvans, Michelle M.
Pappalardo, Robert T.
TI Modeling stresses on satellites due to nonsynchronous rotation and
orbital eccentricity using gravitational potential theory
SO ICARUS
LA English
DT Article
DE Europa; Satellites, general; Tides, solid body; Tectonics; Geophysics
ID TIDAL STRESSES; GALILEAN SATELLITES; TECTONIC PATTERNS; SHEAR FAILURE;
EUROPA; ENCELADUS; EVOLUTION; FRACTURE; ORIGIN; PLANET
AB The tidal stress at the surface of a satellite is derived from the gravitational potential of the satellite's parent planet, assuming that the satellite is fully differentiated into a silicate core. a global subsurface ocean, and a decoupled, viscoelastic lithospheric shell. We consider two types of time variability for the tidal force acting on the shell: one caused by the satellite's eccentric orbit within the planet's gravitational field (diurnal tides), and one due to nonsynchronous rotation (NSR) of the shell relative to the satellite's core, which is presumed to be tidally locked. In calculating surface stresses, this method allows the Love numbers h and l, describing the satellite's tidal response, to be specified independently; it allows the use of frequency-dependent viscoelastic rheologies (e.g. a Maxwell solid); and its mathematical form is amenable to the inclusion of stresses due to individual tides. The lithosphere can respond to NSR forcing either viscously or elastically depending on the value of the parameter Delta equivalent to mu/eta omega, where mu and eta are the shear modulus and viscosity of the shell respectively, and omega is the NSR forcing frequency. Delta is proportional to the ratio of the forcing period to the viscous relaxation time. When Delta >> 1 the response is nearly fluid; when Delta << 1 it is nearly elastic. In the elastic case, tensile stresses due to NSR on Europa can be as large as similar to 3.3 MPa, which dominate the similar to 50 kPa stresses predicted to result from Europa's diurnal tides. The faster the viscous relaxation the smaller the NSR stresses, such that diurnal stresses dominate when Delta greater than or similar to 100. Given the uncertainty in current estimates of the NSR period and of the viscosity of Europa's ice shell, it is unclear which tide should be dominant. For Europa, tidal stresses are relatively insensitive both to the theological structure beneath the ice layer and to the thickness of the icy shell. The phase shift between the tidal potential and the resulting stresses increases with Delta. This shift can displace the NSR stresses longitudinally by as much as 45 degrees in the direction opposite of the satellite's rotation. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Wahr, John; Mullen, McCall E.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Selvans, Zane A.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Selvans, Zane A.] Univ Colorado, NASA, Astrobiol Inst, Boulder, CO 80309 USA.
[Barr, Amy C.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Collins, Geoffrey C.] Wheaton Coll, Dept Phys & Astron, Norton, MA 02766 USA.
[Selvans, Michelle M.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Pappalardo, Robert T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wahr, J (reprint author), Univ Colorado, Dept Phys, UCB 390, Boulder, CO 80309 USA.
EM john.wahr@colorado.edu
FU NASA [NNG04GJ19G, NNG06GF44C, CAN-XX-OSS-02]
FX We are grateful to Terry Hurford for providing us with numerical output
from the "flattening" model equivalent to that used in plots from
Greenberg et al. (1998), to Francis Nimmo for thoughtful discussions,
and to Bridget Smith-Konter and Simon Kattenhorn for beta-testing of our
implementation. We thank Isamu Matsuyama and an anonymous reviewer for
helpful comments on the manuscript. Support for this work is provided by
NASA Planetary Geology and Geophysics Grant NNG04GJ19G, and NASA Outer
Planets Research Program Grant NNG06GF44C, and the NASA Astrobiology
Institute under Cooperative Agreement No. CAN-XX-OSS-02 issued through
the Office of Space Science.
NR 60
TC 46
Z9 46
U1 1
U2 18
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 MAR
PY 2009
VL 200
IS 1
BP 188
EP 206
DI 10.1016/j.icarus.2008.11.002
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 419IN
UT WOS:000264213000014
ER
PT J
AU Janssen, MA
Lorenz, RD
West, R
Paganelli, F
Lopes, RM
Kirk, RL
Elachi, C
Wall, SD
Johnson, WTK
Anderson, Y
Boehmer, RA
Callahan, P
Gim, Y
Hamilton, GA
Kelleher, KD
Roth, L
Stiles, B
Le Gall, A
AF Janssen, M. A.
Lorenz, R. D.
West, R.
Paganelli, F.
Lopes, R. M.
Kirk, R. L.
Elachi, C.
Wall, S. D.
Johnson, W. T. K.
Anderson, Y.
Boehmer, R. A.
Callahan, P.
Gim, Y.
Hamilton, G. A.
Kelleher, K. D.
Roth, L.
Stiles, B.
Le Gall, A.
CA Cassini Radar Team
TI Titan's surface at 2.2-cm wavelength imaged by the Cassini RADAR
radiometer: Calibration and first results
SO ICARUS
LA English
DT Article
DE Titan; Satellites, surfaces; Satellites, composition; Radio
observations; Instrumentation
ID PHYSICAL-CHARACTERISTICS; MICROWAVE RADIOMETER; TEMPERATURE; ATMOSPHERE;
RADIATION; MAGELLAN; VENUS
AB The first comprehensive calibration and mapping of the thermal microwave emission from Titan's surface is reported based on radiometric data obtained at 2.2-cm wavelength by the passive radiometer included in the Cassini Radar instrument. The data reported were accumulated from 69 separate observational segments in Titan passes from Ta (October 2004) through T30 (May 2007) and include emission from 94% of Titan's surface. They are diverse in the key observing parameters of emission angle, polarization, and spatial resolution, and their reduction into-calibrated global mosaic maps involved several steps. Analysis of the polarimetry obtained at low to moderate resolution (50+ km) enabled integration of the radiometry into a single mosaic of the equivalent brightness temperature at normal incidence with a relative precision of about 1 K. The Huygens probe measurement of Titan's surface temperature and radiometry obtained on Titan's dune fields allowed us to infer an absolute calibration estimated to be accurate to a level approaching I K. The results provide evidence for a surface that is complex and varied on large scales. The radiometry primarily constrains physical properties of the surface, where we see strong evidence for subsurface (volume) scattering as a dominant mechanism that determines the emissivity, with the possibility of a fluffy or graded-density surface layer in many regions. The results are consistent with, but not necessarily definitive of a surface composition resulting from the slow deposition and processing of organic compounds from the atmosphere. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Janssen, M. A.; West, R.; Lopes, R. M.; Elachi, C.; Wall, S. D.; Johnson, W. T. K.; Anderson, Y.; Boehmer, R. A.; Callahan, P.; Gim, Y.; Hamilton, G. A.; Kelleher, K. D.; Roth, L.; Stiles, B.; Le Gall, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lorenz, R. D.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
[Paganelli, F.] European Ctr Geodynam & Seismol, L-7256 Walferdange, Luxembourg.
[Kirk, R. L.] US Geol Survey, Flagstaff, AZ 86001 USA.
RP Janssen, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM michael.a.janssen@jpl.nasa.gov
RI Lorenz, Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016
OI Lorenz, Ralph/0000-0001-8528-4644; Lopes, Rosaly/0000-0002-7928-3167
NR 41
TC 64
Z9 64
U1 1
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 MAR
PY 2009
VL 200
IS 1
BP 222
EP 239
DI 10.1016/j.icarus.2008.10.017
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 419IN
UT WOS:000264213000016
ER
PT J
AU Zebker, HA
Gim, Y
Callahan, P
Hensley, S
Lorenz, R
AF Zebker, Howard A.
Gim, Yonggyu
Callahan, Philip
Hensley, Scott
Lorenz, Ralph
CA Cassini Radar Team
TI Analysis and interpretation of Cassini Titan radar altimeter echoes
SO ICARUS
LA English
DT Article
DE Titan; Satellites, surfaces; Radar observations; Instrumentation
ID SURFACE; HEIGHT; RETURN
AB The Cassini spacecraft has acquired 25 radar altimeter elevation profiles along Titan's surface as of April 2008, and we have analyzed 18 of these for which there are currently reconstructed ephemeris data. Altimeter measurements were collected at spatial footprint sizes from 6-60 km along ground tracks of length 400-3600 km. The elevation profiles yield topographic information at this resolution with a statistical height accuracy of 35-50 m and kilometer-scale errors several times greater. The data exhibit significant variations in terrain, from flat regions with little topographic expression to very rugged Titanscapes. The bandwidth of the transmitted waveform admits vertical resolution of the terrain height to 35 m at each observed location on the surface. Variations in antenna pointing and changes in surface statistics cause the range-compressed radar echoes to exhibit strong systematic and time-variable biases of hundreds of meters in delay. It is necessary to correct the received echoes for these changes, and we have derived correction algorithms such that the derived echo profiles are accurate at the 100 m level for off-nadir pointing errors of 0.3 degrees and 0.6 degrees, for leading edge and echo centroid estimators, respectively. The leading edge of the echo yields the elevation of the highest points on the surface, which we take to be the peaks of any terrain variation. The mean value of the echo delay is more representative of the mean elevation, so that the difference of these values gives an estimate of any local mountain heights. Finding locations where these values diverge indicates higher-relief terrain. Elevation features are readily seen in the height profiles. Several of the passes show mountains of several hundred m altitude, spread over 10's or even 100's of km in spatial extent, so that slopes are very small. Large expanses of sub-100 m topography are commonplace on Titan, so it is rather smooth in many locations. Other areas exhibit more relief, although the overall observed variation in surface height on any pass is less than about I km. Some elevation features correspond to observed changes in brightness in Cassini infrared images, but many do not. Correspondence between the imaging SAR ground tracks and the altimeter paths is limited, so that identifying elevation changes with higher resolution SAR features is premature at present. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Zebker, Howard A.] Stanford Univ, Dept Geophys, Stanford, CA 94305 USA.
[Zebker, Howard A.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
[Cassini Radar Team] CALTECH, Jet Prop Lab, Cassini Project, Pasadena, CA 91109 USA.
[Lorenz, Ralph] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Zebker, HA (reprint author), Stanford Univ, Dept Geophys, 360 Mitchell Bldg,MC 2215,397 Panama Mall, Stanford, CA 94305 USA.
EM zebker@stanford.edu
RI Lorenz, Ralph/B-8759-2016
OI Lorenz, Ralph/0000-0001-8528-4644
FU Cassini project
FX Measurements such as these could be completed without the combined
efforts of many people associated the Cassini project, and we would like
to acknowledge the project personnel, and especially the Radar team, for
planning and operating the instrument for these acquisitions. We would
also like to acknowledge Giovanni Alberti and his team in Italy for
producing the low-level altimeter data products. We also thank Chuck
Wood and Lauren Wye for thorough reviews and insightful comments that
helped the manuscript. We in addition want to thank Tom Farr and an
anonymous reviewer for many good questions in the review process, which
has greatly improved the paper. This work was supported by the Cassini
project through the Radar team activities.
NR 18
TC 19
Z9 19
U1 0
U2 5
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2009
VL 200
IS 1
BP 240
EP 255
DI 10.1016/j.icarus.2008.10.023
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 419IN
UT WOS:000264213000017
ER
PT J
AU Van Hoolst, T
Rambaux, N
Karatekin, O
Baland, RM
AF Van Hoolst, T.
Rambaux, N.
Karatekin, Oe.
Baland, R. -M.
TI The effect of gravitational and pressure torques on Titan's
length-of-day variations
SO ICARUS
LA English
DT Article
DE Titan; Interiors; Rotational dynamics; Ices
ID ROTATION; STATE
AB Cassini radar observations show that Titan's spin is slightly faster than synchronous spin. Angular momentum exchange between Titan's surface and the atmosphere over seasonal time scales corresponding to Saturn's orbital period of 29.5 year is the most likely cause of the observed non-synchronous rotation. We study the effect of Saturn's gravitational torque and torques between internal layers on the length-of-day (LOD) variations driven by the atmosphere. Because static tides deform Titan into an ellipsoid with the long axis approximately in the direction to Saturn. non-zero gravitational and pressure torques exist that can change the rotation rate of Titan. For the torque calculation, we estimate the flattening of Titan and its interior layers under the assumption of hydrostatic equilibrium. The gravitational forcing by Saturn, due to misalignment of the long axis of Titan with the line joining the mass centers of Titan and Saturn, reduces the LOD variations with respect to those for a spherical Titan by an order of magnitude. Internal gravitational and pressure coupling between the ice shell and the interior beneath a putative ocean tends to reduce any differential rotation between shell and interior and reduces further the LOD variations by a few times. For the current estimate of the atmospheric torque, we obtain LOD variations of a hydrostatic Titan that are more than 100 times smaller than the observations indicate when Titan has no ocean as well as when a subsurface ocean exists. Moreover, Saturn's torque causes the rotation to be slower than synchronous in contrast to the Cassini observations. The calculated LOD variations could be increased if the atmospheric torque is larger than predicted and or if fast viscous relaxation of the ice shell could reduce the gravitational coupling, but it remains to be studied if a two order of magnitude increase is possible and if these effects can explain the phase difference of the predicted rotation variations. Alternatively, the large differences with the observations may suggest that non-hydrostatic effects in Titan are important. In particular, we show that the amplitude and phase of the calculated rotation variations are similar to the observed values if non-hydrostatic effects could strongly reduce the equatorial flattening of the ice shell above an internal ocean. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Van Hoolst, T.; Karatekin, Oe.; Baland, R. -M.] Observ Royal Belgique, B-1180 Brussels, Belgium.
[Rambaux, N.] Univ Paris 06, Observ Paris, IMCCE, F-75014 Paris, France.
[Rambaux, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Van Hoolst, T (reprint author), Observ Royal Belgique, Ringlaan 3, B-1180 Brussels, Belgium.
EM tim.vanhoolst@oma.be
OI Baland, Rose-Marie/0000-0002-5907-0033
FU Belgian PRODEX program
FX We thank T. Tokano for allowing us to use his atmospheric angular
momentum series of Titan. This work was financially supported by the
Belgian PRODEX program managed by the European Space Agency in
collaboration with the Belgian Federal Science Policy Office. N.R.
acknowledges the jet Propulsion Laboratory of the California Institute
of Technology visiting program scientist.
NR 25
TC 25
Z9 25
U1 1
U2 5
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAR
PY 2009
VL 200
IS 1
BP 256
EP 264
DI 10.1016/j.icarus.2008.11.009
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 419IN
UT WOS:000264213000018
ER
PT J
AU Hodyss, R
Johnson, PV
Stern, JV
Goguen, JD
Kanik, I
AF Hodyss, Robert
Johnson, Paul V.
Stern, Julie V.
Goguen, Jay D.
Kanik, Isik
TI Photochemistry of methane-water ices
SO ICARUS
LA English
DT Article
DE Ices; Ices, IR spectroscopy; Satellites, surfaces; Photochemistry
ID OUTER SOLAR-SYSTEM; INFRARED SPECTRAL PROPERTIES; SPECTROSCOPY;
ENCELADUS; ION; IRRADIATION; PHOTOLYSIS; MIXTURES; RELEVANT; BODIES
AB We report a study on the broadband ultraviolet photolysis of methane-water ice mixtures, at low methane concentrations and temperatures relevant to the icy satellites of the outer Solar System. The photochemistry of these mixtures is dominated by the action of hydroxyl radicals on methane and the resulting products. This implies that, given sufficient exposure time, the methane will eventually be completely oxidized to carbon dioxide. The presence of methane inhibits the formation of hydrogen peroxide by serving as a trap for hydroxyl radicals. The distribution of photochemical products is broadly similar to that previously conducted using ion and electron sources, with some differences possibly attributable to the difference in radiation source. The results are applicable to a variety of icy bodies in the Solar System. On Enceladus, where methane mixed with water is measured in the plumes, methane in the surface ices is subject to oxidation and will eventually be converted to CO(2). The C-H stretch feature detected in the VIMS spectra of the Enceladus surface ice suggests that methane is currently being supplied to the surface ice, likely from re-condensation of the plume gas. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Hodyss, Robert; Johnson, Paul V.; Stern, Julie V.; Goguen, Jay D.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hodyss, R (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.p.hodyss@jpl.nasa.gov
RI Johnson, Paul/D-4001-2009
OI Johnson, Paul/0000-0002-0186-8456
FU National Aeronautics and Space Administration (NASA); JPL's Research and
Technology Development program
FX This work was performed at the jet Propulsion Laboratory (JPL),
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration (NASA). Financial support through
JPL's Research and Technology Development program is gratefully
acknowledged. We thank A.L. Lane (JPL) for useful discussions.
NR 33
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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 MAR
PY 2009
VL 200
IS 1
BP 338
EP 342
DI 10.1016/j.icarus.2008.10.024
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 419IN
UT WOS:000264213000025
ER
PT J
AU Lehman, DH
Clark, KB
Cook, BA
Gavit, SA
Kayali, SA
McKinney, JC
Milkovich, DA
Reh, KR
Taylor, RL
Casani, JR
Griebel, T
AF Lehman, David H.
Clark, Karla B.
Cook, Beverly A.
Gavit, Sarah A.
Kayali, Sammy A.
McKinney, John C.
Milkovich, David A.
Reh, Kim R.
Taylor, Randall L.
Casani, John R.
Griebel, Therese
TI Experiences in Managing the Prometheus Project
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
AB Congress authorized NASA's Prometheus Project in February 2003, with the first Prometheus mission slated to explore the icy moons of Jupiter. The project had two major objectives: 1) to develop a nuclear reactor that would provide unprecedented levels of power and show that it could be processed safely and operated reliably in space for long-duration, deep-space exploration; and 2) to explore the three icy moons of Jupiter - Callisto, Ganymede, and Europa - and return science data that would meet the scientific goals as set forth in the Decadal Survey Report of the National Academy of Sciences.
Early in project planning, it was determined that the development of the Prometheus nuclear-powered spaceship would be complex and require the intellectual knowledge residing at numerous organizations across the country. In addition, because of the complex nature of the project and the multiple partners, approaches beyond those successfully used to manage a typical JPL project would be needed. This describes the key experiences in managing Prometheus, which should prove useful for future projects of similar scope and magnitude.
C1 [Lehman, David H.; Clark, Karla B.; Cook, Beverly A.; Gavit, Sarah A.; Kayali, Sammy A.; McKinney, John C.; Milkovich, David A.; Reh, Kim R.; Taylor, Randall L.; Casani, John R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Griebel, Therese] Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Lehman, DH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 2
TC 0
Z9 0
U1 1
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0885-8985
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD MAR
PY 2009
VL 24
IS 3
BP 12
EP 21
PG 10
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA 431VC
UT WOS:000265091300002
ER
PT J
AU Gat, E
AF Gat, Erann
TI Non-Linear Sequencing
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
AB Spacecraft are traditionally commanded using linear sequences of time-based commands. Linear sequences work fairly well, but they are difficult and expensive to generate, and are usually not capable of responding to contingencies. Any anomalous behavior while executing a linear sequence generally results in the spacecraft entering a safe mode. Critical sequences like orbit insertions which must be able to respond to faults without going into safe mode are particularly difficult to design and verify. The effort needed to generate command sequences can be reduced by extending the vocabulary of sequences to include more sophisticated control constructs. The simplest extensions are conditionals and loops. Adding these constructs would make a sequencing language look more or less like a traditional programming language or scripting language, and would come with all the difficulties associated with such a language. In particular, verifying the correctness of a sequence would be tantamount to verifying the correctness of a program, which is undecidable in general. We describe an extended vocabulary for non-linear sequencing based on the architectural notion of cognizant failure. A cognizant failure architecture is divided into components whose contract is to either achieve (or maintain) a certain condition, or report that they have failed to do so. Cognizant failure is an easier condition to verify than correctness, and it can provide high confidence in the safety of the spacecraft. Because cognizant failure inherently implies some kind of representation of the intent of an action, the system can respond to contingencies in more robust and general ways. We will describe an implemented non-linear sequencing system that is being flown on the NASA New Millennium Deep Space 1 Mission as part of the Remote Agent Experiment.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gat, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU National Aeronautics and Space Administration
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 7
TC 0
Z9 0
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0885-8985
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD MAR
PY 2009
VL 24
IS 3
BP 41
EP 46
PG 6
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA 431VC
UT WOS:000265091300007
ER
PT J
AU White, RJ
Peng, GCY
Demir, SS
AF White, Ronald J.
Peng, Grace C. Y.
Demir, Semahat S.
TI Multiscale Modeling of Biomedical, Biological, and Behavioral Systems
(Part 1)
SO IEEE ENGINEERING IN MEDICINE AND BIOLOGY MAGAZINE
LA English
DT Editorial Material
C1 [Peng, Grace C. Y.] Natl Inst Biomed Imaging & Bioengn, Bethesda, MD 20892 USA.
[White, Ronald J.] NASA, Human Res Program, Washington, DC USA.
[White, Ronald J.] Baylor Coll Med, Houston, TX 77030 USA.
[White, Ronald J.] NASA, Div Life Sci, Washington, DC USA.
[White, Ronald J.] Uniformed Serv Univ Hlth Sci, Bethesda, MD 20814 USA.
[White, Ronald J.] Univ Louisiana Lafayette, Lafayette, LA USA.
RP Peng, GCY (reprint author), Natl Inst Biomed Imaging & Bioengn, 6707 Democracy Blvd,Suite 200,MSC 5469, Bethesda, MD 20892 USA.
EM penggr@mail.nih.gov
NR 0
TC 9
Z9 9
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0739-5175
J9 IEEE ENG MED BIOL
JI IEEE Eng. Med. Biol. Mag.
PD MAR-APR
PY 2009
VL 28
IS 2
BP 12
EP 13
DI 10.1109/MEMB.2009.932388
PG 2
WC Engineering, Biomedical; Medical Informatics
SC Engineering; Medical Informatics
GA 431UV
UT WOS:000265090600004
PM 19349247
ER
PT J
AU Baker, CR
Dolan, JM
AF Baker, Christopher R.
Dolan, John M.
TI Street Smarts for Boss Behavioral Subsystem Engineering for the Urban
Challenge
SO IEEE ROBOTICS & AUTOMATION MAGAZINE
LA English
DT Article
DE Software architecture; Tartan Racing; Boss; robot behaviors; Urban
Challenge
C1 [Baker, Christopher R.] Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA.
[Dolan, John M.] NASA, Kennedy Space Ctr, FL 32899 USA.
RP Baker, CR (reprint author), Carnegie Mellon Univ, Inst Robot, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
EM cbaker@andrew.cmu.edu
FU DARPA [HR0011-06-C-0142]
FX This work would not have been possible without the dedicated efforts of
the Tartan Racing team and the generous support of our sponsors
including General Motors, Caterpillar, and Continental. This work was
further supported by DARPA under contract HR0011-06-C-0142.
NR 7
TC 10
Z9 10
U1 1
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1070-9932
J9 IEEE ROBOT AUTOM MAG
JI IEEE Robot. Autom. Mag.
PD MAR
PY 2009
VL 16
IS 1
BP 78
EP 87
DI 10.1109/MRA.2008.931629
PG 10
WC Automation & Control Systems; Robotics
SC Automation & Control Systems; Robotics
GA 416PY
UT WOS:000264019200011
ER
PT J
AU Xu, JC
Hunter, GW
Lukco, D
Liu, CC
Ward, BJ
AF Xu, Jennifer C.
Hunter, Gary W.
Lukco, Dorothy
Liu, Chung-Chiun
Ward, Benjamin J.
TI Novel Carbon Dioxide Microsensor Based on Tin Oxide Nanomaterial Doped
With Copper Oxide
SO IEEE SENSORS JOURNAL
LA English
DT Article
DE Carbon dioxide (CO(2)); copper oxide (CuO); microsensor; nanomaterial;
tin oxide (SnO(2))
ID THIN
AB Carbon dioxide (CO(2)) is one of the major indicators of fire and therefore its measurement is very important for low-false-alarm fire detection and emissions monitoring. However, only a limited number of CO(2) sensing materials exist due to the high chemical stability of CO(2). In this work, a novel CO(2) microsensor based on nanocrystalline tin oxide (SnO(2)) doped with copper oxide (CuO) has been successfully demonstrated. The CuO-SnO(2) based CO(2) microsensors are fabricated by means of microelectromechanical systems technology and sol-gel nanomaterial-synthesis processes. At a doping level of CuO : SnO(2) = 1 : 8 (molar ratio), the resistance of the sensor has a linear response to CO(2) concentrations for the range of 1% to 4 % CO(2) in air at 450 degrees C. This approach has demonstrated the use of SnO(2), typically used for the detection of reducing gases, in the detection of an oxidizing gas.
C1 [Xu, Jennifer C.; Hunter, Gary W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Lukco, Dorothy] ASRC, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Liu, Chung-Chiun; Ward, Benjamin J.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
RP Xu, JC (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Jennifer.C.Xu@nasa.gov; Gary.W.Hunter@nasa.gov;
Dorothy.Lukco@gre.nasa.gov; cxl9@cwru.edu; bward@makelengineering.com
NR 8
TC 19
Z9 19
U1 1
U2 14
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1530-437X
J9 IEEE SENS J
JI IEEE Sens. J.
PD MAR
PY 2009
VL 9
IS 3
BP 235
EP 236
DI 10.1109/JSEN.2008.201195
PG 2
WC Engineering, Electrical & Electronic; Instruments & Instrumentation;
Physics, Applied
SC Engineering; Instruments & Instrumentation; Physics
GA 425JA
UT WOS:000264631600009
ER
PT J
AU Zhou, GQ
Ambrosia, V
Gasiewski, AJ
Bland, G
AF Zhou, Guoqing
Ambrosia, Vince
Gasiewski, Albin J.
Bland, Geoff
TI Foreword to the Special Issue on Unmanned Airborne Vehicle (UAV) Sensing
Systems for Earth Observations
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Editorial Material
C1 [Zhou, Guoqing] Old Dominion Univ, Norfolk, VA 23529 USA.
[Ambrosia, Vince] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gasiewski, Albin J.] Univ Colorado, CU Ctr Environm Technol, NOAA, UCB 0425, Boulder, CO 80309 USA.
[Bland, Geoff] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP Zhou, GQ (reprint author), Old Dominion Univ, Norfolk, VA 23529 USA.
NR 0
TC 15
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U1 1
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2009
VL 47
IS 3
BP 687
EP 689
DI 10.1109/TGRS.2009.2013059
PG 3
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 415JA
UT WOS:000263928900001
ER
PT J
AU Xiong, XX
Wenny, BN
Wu, AS
Barnes, WL
Salomonson, VV
AF Xiong, Xiaoxiong
Wenny, Brian N.
Wu, Aisheng
Barnes, William L.
Salomonson, Vincent V.
TI Aqua MODIS Thermal Emissive Band On-Orbit Calibration, Characterization,
and Performance
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aqua; blackbody (BB); calibration; detector; Moderate Resolution Imaging
Spectroradiometer (MODIS); radiometer; thermal emissive bands (TEBs)
ID REFLECTIVE SOLAR BANDS; RADIOMETRIC CALIBRATION; SURFACE-TEMPERATURE;
TERRA; MISSION; LAND; VALIDATION; CLOUDS; WATER
AB The NASA's Earth Observing System Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) has continued to operate with satisfactory performance since its launch in May 2002, exceeding its nominal six-year design lifetime. Its continuous Earth observations have been used to generate many science data products for studies of the Earth's system. MODIS has 36 spectral bands: 20 reflective solar bands and 16 thermal emissive bands (TEBs). All TEB observations are made at I-km nadir spatial resolution with spectral wavelengths from 3.7 to 14.4 mu m. Primary applications of MODIS TEB include surface, cloud, and atmospheric temperatures, water vapor, and cloud top altitude. MODIS TEB on-orbit calibration uses a quadratic algorithm with its calibration coefficients derived using an on-board blackbody (BB). This paper will present Aqua MODIS TEB on-orbit calibration, characterization, and performance over its six-year mission. Examples of instrument thermal behavior, BB temperature stability, detector short-term stability, and changes in long-term response (or system gain) will be presented. Comparisons will also be made with Terra MODIS, launched in December 1999. On-orbit results show that Aqua MODIS and its focal plane temperatures have behaved normally. BB temperature has remained extremely stable with typical scan-to-scan variations of less than +/- 0.15 mK. Most TEB detectors continue to exceed their specified signal-to-noise ratio requirements, exhibiting excellent short-term stability and calibration accuracy. Excluding a few noisy detectors, either identified prelaunch or occurring postlaunch, on-orbit changes in TEB responses have been less than 0.5% on an annual basis. By comparison, the overall Aqua TEB performance has been better than that of Terra MODIS.
C1 [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Wenny, Brian N.; Wu, Aisheng] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Barnes, William L.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Salomonson, Vincent V.] Univ Utah, Salt Lake City, UT 84112 USA.
RP Xiong, XX (reprint author), NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
EM Xiaoxiong.Xiong-1@nasa.gov; brian_wenny@ssaihq.com;
aisheng_wu@ssaihq.com; William.L.Barnes@nasa.gov;
vincent.v.salomonson@nasa.gov
NR 34
TC 48
Z9 50
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAR
PY 2009
VL 47
IS 3
BP 803
EP 814
DI 10.1109/TGRS.2008.2005109
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 415JA
UT WOS:000263928900011
ER
PT J
AU Sharma, R
Wyatt, CA
Zhang, J
Calle, CI
Mardesich, N
Mazumder, MK
AF Sharma, Rajesh
Wyatt, Christopher A.
Zhang, Jing
Calle, Carlos I.
Mardesich, Nick
Mazumder, Malay K.
TI Experimental Evaluation and Analysis of Electrodynamic Screen as Dust
Mitigation Technology for Future Mars Missions
SO IEEE TRANSACTIONS ON INDUSTRY APPLICATIONS
LA English
DT Article; Proceedings Paper
CT 42nd Annual Meeting of the IEEE-Industry-Applications-Society
CY SEP 23-27, 2007
CL New Orleans, LA
SP IEEE Ind Applicat Soc
DE Dust mitigation technologies; electrodynamics; Mars dust simulant; power
consumption; traveling wave
ID PATHFINDER
AB The electrodynamic screen (EDS) is considered to be one of the feasible dust mitigation technologies for future Mars missions. In this paper, the performance of EDS for surface cleaning was characterized with respect to the following operational parameters: 1) the efficiency or screens under both continuous and intermittent operations with different rates of dust deposition; 2) electrical power requirements for the screen operation with respect to dust removal efficiency (DRE), frequency, and excitation frequency; and 3) the optical transmission efficiency of the transparent EDSs and the corresponding power loss, when these screens were placed on solar panels. The average DRE of EDS during continuous dust loading was over 95%, whereas it was 90% when the screen was activated intermittently. Power consumption by EDS, as well as the size and weight of the power supply, is one of the critical factors for its applicability for dust removal from solar panels during future Mars mission. The power consumption by EDS was measured under several dust loadings and using different frequencies and electrical field intensities for the safe operation of power supplies without Paschen breakdown. Experiments were conducted under simulated Martian atmosphere (5.0 mb CO(2) atmosphere) using a screen with an active surface area of 59 cm(2). The average power consumption of screen varied between 1.02 and 2.87 mW. The optical transmission efficiency for a transparent EDS (PET substrate with indium tin oxide electrodes) was measured for a PET screen with ITO electrodes. It was found that placing the transparent EDS on a typical space-type solar panel resulted in a significant obscuration. The power output of the solar panel decreased by 15%.
C1 [Sharma, Rajesh; Mazumder, Malay K.] Univ Arkansas, Dept Appl Sci, Little Rock, AR 72204 USA.
[Wyatt, Christopher A.] Georgia Inst Technol, Aerosp Syst Design Lab, Sch Aerosp Engn, Atlanta, GA 30332 USA.
[Zhang, Jing] Univ Arkansas, Dept Syst Engn, Little Rock, AR 72204 USA.
[Calle, Carlos I.] NASA, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA.
[Mardesich, Nick] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
RP Sharma, R (reprint author), Univ Arkansas, Dept Appl Sci, Little Rock, AR 72204 USA.
EM rxsharma@ualr.edu; cawyatt@gatech.edu; Jxzhang1@ualr.edu;
Carlos.i.calle@nasa.gov; Nick.Mardesich@jpl.nasa.gov;
mkmazumder@ualr.edu
NR 24
TC 19
Z9 20
U1 0
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0093-9994
J9 IEEE T IND APPL
JI IEEE Trans. Ind. Appl.
PD MAR-APR
PY 2009
VL 45
IS 2
BP 591
EP 596
DI 10.1109/TIA.2009.2013542
PG 6
WC Engineering, Multidisciplinary; Engineering, Electrical & Electronic
SC Engineering
GA 425IJ
UT WOS:000264629900007
ER
PT J
AU Simons, RN
Wintucky, EG
Wilson, JD
Force, DA
AF Simons, Rainee N.
Wintucky, Edwin G.
Wilson, Jeffrey D.
Force, Dale A.
TI Ultra-High Power and Efficiency Space Traveling-Wave Tube Amplifier
Power Combiner With Reduced Size and Mass for NASA Missions
SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES
LA English
DT Article
DE Amplifiers; magic-T; microwave power amplifiers; millimeter wave power
amplifiers; millimeter wave tubes; power combiner; power conditioning;
satellite communication; space technology; traveling-wave tubes (TWTs);
waveguide
AB In the 2008 IEEE Microwave Theory and Techniques Society International Microwave Symposium Digest version of our paper, recent advances in high power and efficiency space traveling-wave tube amplifiers for NASA's space-to-Earth communications are presented. The RF power and efficiency of a new K-band amplifier are 40 W and 50% and that of a new Ka-band amplifier are 200 W and 60%. An important figure-of-merit, which is defined as the ratio of the RF power output to the mass (W/kg) of a traveling-wave tube (TWT), has improved by a factor of 10 over the previous generation Ka-band devices. In this paper, a high power high efficiency Ka-band combiner for multiple TWTs, based on a novel hybrid magic-T waveguide circuit design, is presented. The measured combiner efficiency is as high as 90%. In addition, at the design frequency of 32.05 GHz, error-free uncoded binary phase-shift keying/quadrature phase-shift keying (QPSK) data transmission at 8 Mb/s, which is typical for deep-space communications, is demonstrated. Furthermore, QPSK data transmission at 622 Mb/s is demonstrated with a low bit error rate of 2.4 x 10(-8), which exceeds the deep-space state-of-the-art data rate transmission capability by more than two orders of magnitude. A potential application of the TWT combiner is in deep-space communication systems for planetary exploration requiring transmitter power on the order of a kilowatt or higher.
C1 [Simons, Rainee N.; Wintucky, Edwin G.; Wilson, Jeffrey D.; Force, Dale A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Simons, RN (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Rainee.N.Simons@nasa.gov; Edwin.G.Wintucky@nasa.gov;
Jef-frey.D.Wilson@nasa.gov; Dale.A.Force@nasa.gov
NR 15
TC 8
Z9 8
U1 4
U2 13
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0018-9480
J9 IEEE T MICROW THEORY
JI IEEE Trans. Microw. Theory Tech.
PD MAR
PY 2009
VL 57
IS 3
BP 582
EP 588
DI 10.1109/TMTT.2008.2012298
PG 7
WC Engineering, Electrical & Electronic
SC Engineering
GA 420MZ
UT WOS:000264295200009
ER
PT J
AU Dumas, EM
Ozenne, V
Mielke, RE
Nadeau, JL
AF Dumas, Eve-Marei
Ozenne, Valery
Mielke, Randall E.
Nadeau, Jay L.
TI Toxicity of CdTe Quantum Dots in Bacterial Strains
SO IEEE TRANSACTIONS ON NANOBIOSCIENCE
LA English
DT Article
DE Bacteria; CdTe; quantum dot (QD); reactive oxygen species (ROS)
ID ESCHERICHIA-COLI; IN-VITRO; WATER SUSPENSIONS; HYDROGEN-PEROXIDE; TIO2
PARTICLES; CANCER-CELLS; NANOPARTICLES; CYTOTOXICITY; NANOCRYSTALS;
DERIVATIVES
AB Contradictory results on quantum dot cytotoxicity exist for many types of biological systems, especially microorganisms. In this study, we compare the cytotoxicity of CdTe quantum dots (QDs) to four very different environmental bacterial strains, giving quantitative models of the growth curves for exposed organisms. The mechanisms of toxicity are explored by measuring reactive oxygen species generation by the QDs alone and investigating the oxidative damage to mutant bacteria especially sensitive to ROS. Electron microscopic examination also reveals factors that may contribute to resistance to nanoparticles in some strains.
C1 [Dumas, Eve-Marei; Nadeau, Jay L.] McGill Univ, Dept Biomed Engn, Montreal, PQ H3A 2B4, Canada.
[Mielke, Randall E.] NASA, CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nadeau, JL (reprint author), McGill Univ, Dept Biomed Engn, Montreal, PQ H3A 2B4, Canada.
EM jay.nadeau@mcill.ca
NR 38
TC 40
Z9 40
U1 3
U2 22
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1536-1241
J9 IEEE T NANOBIOSCI
JI IEEE Trans. Nanobiosci.
PD MAR
PY 2009
VL 8
IS 1
BP 58
EP 64
DI 10.1109/TNB.2009.2017313
PG 7
WC Biochemical Research Methods; Nanoscience & Nanotechnology
SC Biochemistry & Molecular Biology; Science & Technology - Other Topics
GA 471FC
UT WOS:000268040200008
PM 19304497
ER
PT J
AU Kaul, AB
Manohara, HM
AF Kaul, Anupama B.
Manohara, Harish M.
TI Carbon Nanotube Vacuum Gauges With Wide Dynamic Range
SO IEEE TRANSACTIONS ON NANOTECHNOLOGY
LA English
DT Article
DE Carbon nanotube (CNT) pressure sensors; low-power vacuum sensors;
microcavity pressure sensors; suspended tubes
ID PRESSURE SENSORS; SILICON
AB Carbon-nanotube-based vacuum gauges have been developed and characterized, which primarily utilize the thermal conductivity principle. The vacuum gauges, comprising 5- to 10-mu m-long single-walled nanotubes contacted on either end with Au/Cr electrodes, have been shown to operate at low power (nanowatts to microwatts) and exhibit a wide dynamic range from 760 to 10(-6). torr. Pressure sensitivity was found to increase rapidly as the bias power was increased. In addition, by etching part of the thermal SiO2 beneath the tubes and minimizing heat conduction through the substrate, pressure sensitivity was extended toward higher vacuums. Results are compared to a conventional thin-film meander resistor, which was fabricated and whose pressure response was also measured for comparative purposes.
C1 [Kaul, Anupama B.; Manohara, Harish M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kaul, AB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM anu.kaul@jpl.nasa.gov; harish.inanohara@jpl.nasa.gov
FU Defense Advanced Research Project Agency seedling fund (Task Order
NMO#715839) [NAS7-03001]; Jet Propulsion Laboratory (JPL) Lew Allen
Award Fund
FX This work was supported by a Defense Advanced Research Project Agency
seedling fund (Task Order NMO#715839) under Contract NAS7-03001 and by
the Jet Propulsion Laboratory (JPL) Lew Allen Award Fund. The review of
this paper was arranged by Associate Editor Dr. K. Matsumoto.
NR 15
TC 8
Z9 8
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1536-125X
J9 IEEE T NANOTECHNOL
JI IEEE Trans. Nanotechnol.
PD MAR
PY 2009
VL 8
IS 2
BP 252
EP 257
DI 10.1109/TNANO.2008.2009534
PG 6
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology;
Materials Science, Multidisciplinary; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Materials Science;
Physics
GA 421FA
UT WOS:000264343600017
ER
PT J
AU Xing, LD
Shrestha, A
Meshkat, L
Wang, WD
AF Xing, Liudong
Shrestha, Akhilesh
Meshkat, Leila
Wang, Wendai
TI Incorporating Common-Cause Failures Into the Modular Hierarchical
Systems Analysis
SO IEEE TRANSACTIONS ON RELIABILITY
LA English
DT Article
DE Common-cause failure; dynamic hierarchical system; modular approach;
phased-mission system
ID PHASED MISSION SYSTEMS; FAULT-TREE ANALYSIS; RELIABILITY-ANALYSIS; MODEL
AB This paper considers the problem of evaluating the reliability of hierarchical systems subject to common-cause failures (CCF); and dynamic failure behavior such as spares, functional dependence, priority dependence, and dependence caused by multi-phased operations. We present a separable solution that has low computational complexity, and which is easy to integrate into existing analytical methods. The resulting approach is applicable to Markov analyses, and combinatorial models for the modular analysis of the system reliability. We illustrate the approach, and the advantages of the proposed approach, through the detailed analyses of two examples of dynamic hierarchical systems subject to CCF.
C1 [Xing, Liudong; Shrestha, Akhilesh] Univ Massachusetts Dartmouth, Dept Elect & Comp Engn, N Dartmouth, MA 02747 USA.
[Meshkat, Leila] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wang, Wendai] Appl Mat Inc, Santa Clara, CA 95054 USA.
RP Xing, LD (reprint author), Univ Massachusetts Dartmouth, Dept Elect & Comp Engn, N Dartmouth, MA 02747 USA.
EM ldxing@ieee.org; g_ashrestha@umassd.edu; leila@mail.jpl.nasa.gov;
wendai_wang@amat.com
FU NSF [CNS-0614652]
FX Manuscript received March 05, 2007; revised November 26, 2007; accepted
September 12, 2008. First published February 10. 2009; current version
published March 04, 2009. This work was supported in part by the NSF
under Grant number CNS-0614652. Associated Editor: R. H. Yeh.
NR 28
TC 19
Z9 20
U1 2
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0018-9529
J9 IEEE T RELIAB
JI IEEE Trans. Reliab.
PD MAR
PY 2009
VL 58
IS 1
BP 10
EP 19
DI 10.1109/TR.2008.2011855
PG 10
WC Computer Science, Hardware & Architecture; Computer Science, Software
Engineering; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA 415WS
UT WOS:000263967800002
ER
PT J
AU Lamar, JE
AF Lamar, John E.
TI Prediction of F-16XL Flight-Flow Physics
SO JOURNAL OF AIRCRAFT
LA English
DT Editorial Material
C1 [Lamar, John E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM johnela-mar@verizon.net
NR 2
TC 4
Z9 4
U1 0
U2 0
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2009
VL 46
IS 2
BP 354
EP 354
DI 10.2514/1.35182
PG 1
WC Engineering, Aerospace
SC Engineering
GA 428OR
UT WOS:000264858800001
ER
PT J
AU Obara, CJ
Lamar, JE
AF Obara, Clifford J.
Lamar, John E.
TI Overview of the Cranked-Arrow Wing Aerodynamics Project International
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA 45th Aerospace Sciences Meeting and Exhibit
CY JAN 08-11, 2007
CL Reno, NV
SP Amer Inst Aeronaut & Astronaut
AB This paper provides a brief history of the F-16XL-1 aircraft, its role in the High-Speed Research Program, and how it was morphed into the Cranked-Arrow Wing Aerodynamics Project. Various flight, wind-tunnel, and computational fluid dynamics data sets were generated as part of the project. These unique and open flight data sets for surface pressures, boundary-layer profiles, and skin-friction distributions, along with surface flow data, are described and sample data comparisons are given. This is followed by a description of how the project became internationally known as Cranked-Arrow Wing Aerodynamics Project International and is concluded by an introduction to the results of a four-year computational predictive study of data collected at flight conditions by participating researchers.
C1 [Obara, Clifford J.] NASA, Langley Res Ctr, Data Acquisit & Test Tech Branch, Hampton, VA 23681 USA.
[Lamar, John E.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
RP Obara, CJ (reprint author), NASA, Langley Res Ctr, Data Acquisit & Test Tech Branch, Mail Stop 237, Hampton, VA 23681 USA.
NR 35
TC 7
Z9 7
U1 0
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2009
VL 46
IS 2
BP 355
EP 368
DI 10.2514/1.34957
PG 14
WC Engineering, Aerospace
SC Engineering
GA 428OR
UT WOS:000264858800002
ER
PT J
AU Boelens, OJ
Badcock, KJ
Gortz, S
Morton, S
Fritz, W
Karman, SL
Michal, T
Lamar, JE
AF Boelens, O. J.
Badcock, K. J.
Gortz, S.
Morton, S.
Fritz, W.
Karman, S. L., Jr.
Michal, T.
Lamar, J. E.
TI F-16XL Geometry and Computational Grids Used in Cranked-Arrow Wing
Aerodynamics Project International
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA 45th Aerospace Sciences Meeting and Exhibit
CY JAN 08-11, 2007
CL Reno, NV
SP Amer Inst Aeronaut & Astronaut
AB The objective of the Cranked-Arrow Wing Aerodynamics Project International was to allow a comprehensive validation of computational fluid dynamics methods against the Cranked-Arrow Wing Aerodynamics Project flight database. A major part of this work involved the generation of high-quality computational grids. Before the grid generation, an airtight geometry of the F-16XL, aircraft was generated by a cooperation of the Cranked-Arrow Wing Aerodynamics Project International partners. Based on this geometry description, both structured and unstructured grids have been generated. The baseline structured (multiblock) grid (and a family of derived grids) has been generated by the National Aerospace Laboratory. Although the algorithms used by the National Aerospace Laboratory had become available just before the Cranked-Arrow Wing Aerodynamics Project International and thus only a limited experience with their application to such a complex configuration had been gained, a grid of good quality was generated well within four weeks. This time compared favorably with that required to produce the unstructured grids in the Cranked-Arrow Wing Aerodynamics Project International. The baseline all-tetrahedral and hybrid unstructured grids have been generated at NASA Langley Research Center and the U.S. Air Force Academy, respectively. To provide more geometrical resolution, trimmed unstructured grids have been generated at the European Aeronautic Defence and Space Company's Military Air Systems, University of Tennessee at Chattanooga SimCenter, Boeing Phantom Works, Royal Institute of Technology, and the Swedish Defence Research Agency. All grids generated within the framework of the Cranked-Arrow Wing Aerodynamics Project International will be discussed in the paper. Both results obtained on the structured grids and the unstructured grids showed a significant improvement in agreement with flight-test data in comparison with those obtained on the structured multiblock grid used during the Cranked-Arrow Wing Aerodynamics Project.
C1 [Boelens, O. J.] NLR, Natl Aerosp Lab, Dept Flight Phys & Loads, Aerosp Vehicles Div, NL-1006 BM Amsterdam, Netherlands.
[Badcock, K. J.] Univ Liverpool, Dept Engn, Computat Fluid Dynam Lab, Liverpool L69 7BZ, Merseyside, England.
[Gortz, S.] Royal Inst Technol, S-10044 Stockholm, Sweden.
[Morton, S.] USAF, Seek Eagle Off, Eglin AFB, FL 32542 USA.
[Fritz, W.] European Aeronaut Def & Space Co, Unit OPEA31, D-81633 Munich, Germany.
[Karman, S. L., Jr.] Univ Tennessee, Grad Sch Computat Engn, Chattanooga, TN 37403 USA.
[Lamar, J. E.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
RP Boelens, OJ (reprint author), NLR, Natl Aerosp Lab, Dept Flight Phys & Loads, Aerosp Vehicles Div, POB 90502, NL-1006 BM Amsterdam, Netherlands.
EM boelens@nlr.nl; K.J.Badcock@liverpool.ac.uk; Stefan.Goertz@dlr.de;
Scott.Morton@eglin.af.mil; willy.fritz@cads.com; Steve-Karman@utc.edu;
todd.r.michal@boeing.com; johnelamar@verizon.net
NR 19
TC 12
Z9 12
U1 0
U2 5
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2009
VL 46
IS 2
BP 369
EP 376
DI 10.2514/1.34852
PG 8
WC Engineering, Aerospace
SC Engineering
GA 428OR
UT WOS:000264858800003
ER
PT J
AU Boelens, OJ
Badcock, KJ
Elmilgui, A
Abdol-Hamid, KS
Massey, SJ
AF Boelens, O. J.
Badcock, K. J.
Elmilgui, A.
Abdol-Hamid, K. S.
Massey, S. J.
TI Comparison of Measured and Block Structured Simulation Results for the
F-16XL Aircraft
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB This paper presents a comparison of the predictions of three Reynolds-averaged Navier-Stokes codes for flight conditions of the F-16XL aircraft that feature vortical How. The three codes, ENSOLV, parallel multiblock, and propulsion aerodynamics branch 3-D unsteady Reynolds-averaged Navier-Stokes, solve on structured multiblock grids. Flight data for comparison were available in the form of surface pressures, skin friction, boundary-layer data, and photographs of tufts. The three codes provided predictions that were consistent with expectations based on the turbulence modelling used, which was kappa-epsilon, kappa-omega with vortex corrections, and an algebraic stress model. The agreement with flight data was good, with the exception of the outer wing primary vortex strength. The confidence in the application of the computational fluid dynamics codes to complex fighter configurations increased significantly through this study.
C1 [Boelens, O. J.] Natl Aerosp Lab, Dept Flight Phys & Loads, Aerosp Vehicles Div, NL-1006 BM Amsterdam, Netherlands.
[Badcock, K. J.] Univ Liverpool, Computat Fluid Dynam Lab, Dept Engn, Liverpool L69 7BZ, Merseyside, England.
[Elmilgui, A.] Analyt Serv & Mat Inc, Hampton, VA 23666 USA.
[Abdol-Hamid, K. S.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
[Massey, S. J.] Eagle Aeronaut, Hampton, VA 23666 USA.
RP Boelens, OJ (reprint author), Natl Aerosp Lab, Dept Flight Phys & Loads, Aerosp Vehicles Div, POB 90502, NL-1006 BM Amsterdam, Netherlands.
EM boelens@nlr.nl; K.J.Badcock@liverpool.ac.uk
FU NLR's programmatic research; Engineering and Physical Sciences Research
Council [GR/S 16485]
FX This ENSOLV study has been conducted under NLR's programmatic research
funding. The Engineering and Physical Sciences Research Council
supported the work at Liverpool through the provision of travel grant
GR/S 16485. The authors would like to thank all the members of the NATO
RTO task group AVT-113, "Understanding and Modeling Vortical Flows to
Improve the Technology Readiness Level for Military Aircraft," and
particularly J.E. Lamar for interesting and fruitful discussions during
the course of this project. The authors would also like to acknowledge
the following papers that have been summarized herein: "Comparison of
Measured and Simulated Flow Features for the Full-Scale F-16XL Aircraft"
by O.J. Boelens, S.P. Spekreijse, H.A. Sytsma, and K.M.J. de Cock
(AIAA-2007-489); "Evaluation of Results from a Reynolds Averaged
Multiblock Code Against F-16XL Flight Data" by K.J. Badcock
(AIAA-2007-490); and "PAB3D Simulations for the CAWAPI F-16XL" by A.
Elmiligui, K.S. Abdol-Hamid, and S.J. Massey (AIAA-2007-491).
NR 16
TC 16
Z9 17
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2009
VL 46
IS 2
BP 377
EP 384
DI 10.2514/1.35064
PG 8
WC Engineering, Aerospace
SC Engineering
GA 428OR
UT WOS:000264858800004
ER
PT J
AU Gortz, S
Jirasek, A
Morton, SA
McDaniel, DR
Cummings, RM
Lamar, JE
Abdol-Hamid, KS
AF Gortz, Stefan
Jirasek, A.
Morton, Scott. A.
McDaniel, David R.
Cummings, Russell M.
Lamar, John E.
Abdol-Hamid, Khaled S.
TI Standard Unstructured Grid Solutions for Cranked Arrow Wing Aerodynamics
Project International F-16XL
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID TURBULENCE MODELS; SIMULATION
AB Steady and unsteady viscous flow simulations of a full-scale, semispan, and full-span model of the F-16XL-1 aircraft are performed with three different computational fluid dynamics codes using a common unstructured grid. Six different flight conditions are considered. They represent Reynolds and Mach number combinations at subsonic speeds, with and without sideslip. The steady computations of the flow at these flight conditions are made with several Reynolds-averaged Navier-Stokes turbulence models of different complexity. Detached-eddy simulation, delayed detached-eddy simulation, and an algebraic hybrid Reynolds-averaged Navier-Stokes/large-eddy simulation model are used to quantify unsteady effects at the same flight conditions. The computed results are compared with flight-test data in the form of surface pressures, skin friction, and boundary-layer velocity profiles. The focus of the comparison is on turbulence modeling effects and effects of unsteadiness. The overall agreement with flight data is good, with no clear trend as to which physical modeling approach is superior for this class of flow. The Reynolds-averaged Navier-Stokes turbulence models perform well in predicting the flow in an average sense. However, some of the flow conditions involve locally unsteady flow over the aircraft, which are held responsible for the scatter between the different turbulence modeling approaches. The detached-eddy simulations are able to quantify the unsteady effects, although they are not consistently better than the Reynolds-averaged Navier-Stokes turbulence models in predicting the flow in an average sense in these flow regions. Detached-eddy simulation fails to predict boundary-layer profiles consistently over a range of flow regimes, with delayed detached-eddy simulation and hybrid Reynolds-averaged Navier-Stokes/large-eddy simulation models offering a remedy to recover some of the predictive capabilities of the underlying Reynolds-averaged Navier-Stokes turbulence model. Nonetheless, the confidence in the predictive capabilities of the computational fluid dynamics codes with regard to complex vortical flowfields around high-performance aircraft of this planform increased significantly during this study.
C1 [Gortz, Stefan] KTH, Royal Inst Technol, S-10044 Stockholm, Sweden.
[Jirasek, A.] FOI, Swedish Def Res Agcy, S-16490 Stockholm, Sweden.
[Morton, Scott. A.] USAF, SEEK EAGLE Off, Eglin AFB, FL 32542 USA.
[McDaniel, David R.; Cummings, Russell M.] USAF Acad, Dept Aeronaut, Colorado Springs, CO 80840 USA.
[Abdol-Hamid, Khaled S.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
RP Gortz, S (reprint author), DLR, German Aerosp Ctr, Lilienthalpl 7, D-38108 Braunschweig, Germany.
NR 36
TC 6
Z9 6
U1 0
U2 3
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2009
VL 46
IS 2
BP 385
EP 408
DI 10.2514/1.35163
PG 24
WC Engineering, Aerospace
SC Engineering
GA 428OR
UT WOS:000264858800005
ER
PT J
AU Rizzi, A
Jirasek, A
Lamar, JE
Crippa, S
Badcock, KJ
Boelens, OJ
AF Rizzi, Arthur
Jirasek, Adam
Lamar, John E.
Crippa, Simone
Badcock, Kenneth J.
Boelens, Okko J.
TI Lessons Learned from Numerical Simulations of the F-16XL Aircraft at
Flight Conditions
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA 45th Aerospace Sciences Meeting and Exhibit
CY JAN 08-11, 2007
CL Reno, NV
SP Amer Inst Aeronaut & Astronaut
AB Nine organizations participated in the Cranked-Arrow Wing Aerodynamics Project International study and have contributed steady and unsteady viscous simulations of a full-scale semispan model of the F-16XL aircraft. Three different categories of flight Reynolds/Mach number combinations are computed and compared with flight-test measurements for the purpose of code validation and improved understanding of the flight physics. Steady-state simulations are done with several turbulence models (of different complexity, with no topology information required) that overcome Boussinesq-assumption problems in vortical flows. Detached-eddy simulation and its successor, delayed detached-eddy simulation, are used to compute the time-accurate flow development. Common structured and unstructured grids as well as individually adapted unstructured grids were used. Although discrepancies are observed in the comparisons, overall reasonable agreement is demonstrated for surface pressure distribution, local skin friction, and boundary velocity profiles at subsonic speeds. The physical modeling, be it steady or unsteady flow, and the grid resolution both contribute to the discrepancies observed in the comparisons with flight data, but at this time, how much each part contributes to the whole cannot be determined. Overall, it can be said that the technology readiness of computational fluid dynamics simulation technology for the study of vehicle performance has matured since 2001, such that it can be used today with a reasonable level of confidence for complex configurations.
C1 [Rizzi, Arthur; Crippa, Simone] Royal Inst Technol, Dept Aeronaut & Vehicle Engn, S-10044 Stockholm, Sweden.
[Jirasek, Adam] Swedish Def Res Agcy, Div Syst Technol, S-16490 Stockholm, Sweden.
[Lamar, John E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Badcock, Kenneth J.] Univ Liverpool, Dept Engn, Liverpool L69 3GH, Merseyside, England.
[Boelens, Okko J.] NLR, Natl Aerosp Lab, Dept Flight Phys & Loads, Aerosp Vehicles Div, NL-1059 CM Amsterdam, Netherlands.
RP Rizzi, A (reprint author), Royal Inst Technol, Dept Aeronaut & Vehicle Engn, S-10044 Stockholm, Sweden.
NR 21
TC 11
Z9 11
U1 1
U2 4
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2009
VL 46
IS 2
BP 423
EP 441
DI 10.2514/1.35698
PG 19
WC Engineering, Aerospace
SC Engineering
GA 428OR
UT WOS:000264858800007
ER
PT J
AU Housman, JA
Kiris, CC
Hafez, MM
AF Housman, Jeffrey A.
Kiris, Cetin C.
Hafez, Mohamed M.
TI Time-Derivative Preconditioning Methods for Multicomponent Flows-Part I:
Riemann Problems
SO JOURNAL OF APPLIED MECHANICS-TRANSACTIONS OF THE ASME
LA English
DT Article; Proceedings Paper
CT Mini-Symposium on Stabilized, Multiscale and Multiphysics Methods held
at the ASME International Mechanical Engineering Congress
CY NOV 05-10, 2006
CL Chicago, IL
SP ASME
DE hybrid conservative/nonconservative method; split coefficient matrix
(SCM) method; time-derivative preconditioning methods; dual time
stepping
ID SCHEMES; ALGORITHM; EQUATIONS; SOLVERS; SYSTEMS; FLUIDS
AB A time-derivative preconditioned system of equations suitable for the numerical simulation of inviscid multicomponent and multiphase flows at all speeds is described. The system is shown to be hyperbolic in time and remains well conditioned in the incompressible limit, allowing time marching numerical methods to remain an efficient solution strategy. It is well known that the application of conservative numerical methods to multicomponent flows containing sharp fluid interfaces will generate nonphysical pressure and velocity oscillations across the component interface. These oscillations may lead to stability problems when the interface separates fluids with large density ratio, such as water and air. The effect of which may lead to the requirement of small physical time steps and slow subiteration convergence for implicit time marching numerical methods. At low speeds the use of nonconservative methods may be considered. In this paper a characteristic-based preconditioned nonconservative method is described. This method preserves pressure and velocity equilibrium across fluid interfaces, obtains density ratio independent stability and convergence, and remains well conditioned in the incompressible limit of the equations. To extend the method to transonic and supersonic flows containing shocks, a hybrid formulation is described, which combines a conservative preconditioned Roe method with the nonconservative preconditioned characteristic-based method. The hybrid method retains the pressure and velocity equilibrium at component interfaces and converges to the physically correct weak solution. To demonstrate the effectiveness of the nonconservative and hybrid approaches, a series of one-dimensional multicomponent Riemann problems is solved with each of the methods. The solutions are compared with the exact solution to the Riemann problem, and stability of the numerical methods are discussed. [DOI: 10.1115/1.3072905]
C1 [Housman, Jeffrey A.; Hafez, Mohamed M.] Univ Calif Davis, Davis, CA 95616 USA.
[Kiris, Cetin C.] NASA, Ames Res Ctr, Adv Supercomp NAS Div, Moffett Field, CA 94035 USA.
RP Housman, JA (reprint author), Univ Calif Davis, 2132 Bainer Hall,1 Shields Ave, Davis, CA 95616 USA.
NR 40
TC 1
Z9 1
U1 0
U2 1
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0021-8936
J9 J APPL MECH-T ASME
JI J. Appl. Mech.-Trans. ASME
PD MAR
PY 2009
VL 76
IS 2
AR 021210
DI 10.1115/1.3072905
PG 13
WC Mechanics
SC Mechanics
GA 442EA
UT WOS:000265821600011
ER
PT J
AU Marks, DA
Wolff, DB
Silberstein, DS
Tokay, A
Pippitt, JL
Wang, JX
AF Marks, David A.
Wolff, David B.
Silberstein, David S.
Tokay, Ali
Pippitt, Jason L.
Wang, Jianxin
TI Availability of High-Quality TRMM Ground Validation Data from Kwajalein,
RMI: A Practical Application of the Relative Calibration Adjustment
Technique
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID MEASURING MISSION TRMM; RADAR OBSERVATIONS; PRECIPITATION RADAR;
RAINFALL PRODUCTS; SATELLITE; CONVECTION; KWAJEX; METEOROLOGY; PROGRAM;
SPACE
AB Since the Tropical Rainfall Measuring Mission (TRMM) satellite launch in November 1997, the TRMM Satellite Validation Office (TSVO) at NASA Goddard Space Flight Center (GSFC) has been performing quality control and estimating rainfall from the KPOL S-band radar at Kwajalein, Republic of the Marshall Islands. Over this period, KPOL has incurred many episodes of calibration and antenna pointing angle uncertainty. To address these issues, the TSVO has applied the relative calibration adjustment (RCA) technique to eight years of KPOL radar data to produce Ground Validation (GV) version 7 products. This application has significantly improved stability in KPOL reflectivity distributions needed for probability matching method (PMM)rain-rate estimation and for comparisons to the TRMM precipitation radar (PR). In years with significant calibration and angle corrections, the statistical improvement in PMM distributions is dramatic. The intent of this paper is to show improved stability in corrected KPOL reflectivity distributions by using the PR as a stable reference. Intermonth fluctuations in mean reflectivity differences between the PR and corrected KPOL are on the order of +/- 1-2 dB, and interyear mean reflectivity differences fluctuate by approximately 61 dB. This represents a marked improvement in stability with confidence comparable to the established calibration and uncertainty boundaries of the PR. The practical application of the RCA method has salvaged eight years of radar data that would have otherwise been unusable and has made possible a high-quality database of tropical ocean-based reflectivity measurements and precipitation estimates for the research community.
C1 [Marks, David A.; Wolff, David B.; Silberstein, David S.; Tokay, Ali; Pippitt, Jason L.; Wang, Jianxin] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Marks, David A.; Wolff, David B.; Silberstein, David S.; Pippitt, Jason L.; Wang, Jianxin] Sci Syst & Applicat Inc, Lanham, MD 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
NR 35
TC 13
Z9 13
U1 1
U2 2
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 2009
VL 26
IS 3
BP 413
EP 429
DI 10.1175/2008JTECHA1174.1
PG 17
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 424PE
UT WOS:000264577800001
ER
PT J
AU Chu, XZ
Yamashita, C
Espy, PJ
Nott, GJ
Jensen, EJ
Liu, HL
Huang, WT
Thayer, JP
AF Chu, Xinzhao
Yamashita, Chihoko
Espy, Patrick J.
Nott, Graeme J.
Jensen, Eric J.
Liu, Han-Li
Huang, Wentao
Thayer, Jeffrey P.
TI Responses of polar mesospheric cloud brightness to stratospheric gravity
waves at the South Pole and Rothera, Antarctica
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article; Proceedings Paper
CT 8th International Workshop on Layered Phenomena in the Mesopause Region
(LPMR-8)
CY AUG 20-23, 2007
CL Univ Alaska Fairbanks, Fairbanks, AK
SP Int Working Grp Layered Phenomena Mesopause Reg, Int Commiss Middle Atmosphere, Int Union Geodesy & Geophys, NASA, Natl Sci Fdn
HO Univ Alaska Fairbanks
DE Polar mesospheric clouds; Gravity waves; Lidar; Antarctica; Stratosphere
ID NOCTILUCENT CLOUDS; LIDAR OBSERVATIONS; RAYLEIGH LIDAR;
DIURNAL-VARIATIONS; MESOPAUSE REGION; GLOBAL CHANGE; GREENLAND;
SONDRESTROM; SATELLITE; URBANA
AB We present the first observational proof that polar mesospheric cloud (PMC) brightness responds to stratospheric gravity waves (GWs) differently at different latitudes by analyzing the Fe Boltzmann lidar data collected from the South Pole and Rothera (67.5 degrees S, 68.0 degrees W), Antarctica. Stratospheric GW strength is characterized by the root-mean-square (RMS) relative density perturbation in the 30-45 km region and PMC brightness is represented by the total backscatter coefficient (TBC) in austral summer from November to February. The linear correlation coefficient (LCC) between GW strength and PMC brightness is found to be +0.09 with a 42% confidence level at the South Pole and -0.49 with a 98% confidence level at Rothera. If a PMC case potentially affected by a space shuttle exhaust plume is removed from the Rothera dataset, the negative correlation coefficient and confidence level increase to -0.61 and 99%, respectively. The Rothera negative correlation increases when shorter-period waves are included while no change is observed in the South Pole correlation. Therefore, observations show statistically that Rothera PMC brightness is negatively correlated with the stratospheric GW strength but no significant correlation exists at the South Pole. A positive correlation of +0.74 with a confidence level of 99.98% is found within a distinct subset of the South Pole data but the rest of the dataset exhibits a random distribution, possibly indicating different populations of ice particles at the South Pole. Our data show that these two locations have similar GW strength and spectrum in the 30-45 km region during summer. The different responses of PMC brightness to GW perturbations are likely caused by the latitudinal differences in background temperatures in the ice crystal growth region between the PMC altitude and the mesopause. At Rothera, where temperatures in this region are relatively warm and supersaturations are not as large, GW-induced temperature perturbations can drive subsaturation in the warm phase. Thus, GWs can destroy growing ice crystals or limit their growth, leading to negative correlation at Rothera. Because the South Pole temperatures in the mesopause region are much colder, GW-perturbed temperature may never be above the frost point and have less of an impact on crystal growth and PMC brightness. The observed phenomena and proposed mechanisms above need to be understood and verified through future modeling of GW effects on PMC microphysics and ray modeling of GW propagation over the South Pole and Rothera. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Chu, Xinzhao; Yamashita, Chihoko; Huang, Wentao; Thayer, Jeffrey P.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Chu, Xinzhao; Yamashita, Chihoko; Huang, Wentao; Thayer, Jeffrey P.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Espy, Patrick J.] Norwegian Univ Sci & Technol, Dept Phys, N-7034 Trondheim, Norway.
[Nott, Graeme J.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Jensen, Eric J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Liu, Han-Li] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Chu, XZ (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
EM Xinzhao.Chu@Colorado.edu
RI Liu, Han-Li/A-9549-2008; Chu, Xinzhao/I-5670-2015; THAYER, JEFFREY
P./B-7264-2016; Cullens, Chihoko/P-2425-2015
OI Liu, Han-Li/0000-0002-6370-0704; Chu, Xinzhao/0000-0001-6147-1963;
THAYER, JEFFREY P./0000-0001-7127-8251; Cullens,
Chihoko/0000-0002-9951-9763
NR 43
TC 9
Z9 10
U1 1
U2 3
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 MAR
PY 2009
VL 71
IS 3-4
SI SI
BP 434
EP 445
DI 10.1016/j.jastp.2008.10.002
PG 12
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 433UQ
UT WOS:000265231700015
ER
PT J
AU Mayr, HG
Mengel, JG
Huang, FT
AF Mayr, Hans G.
Mengel, John G.
Huang, Frank T.
TI Modeling the temperature of the polar mesopause region: Part
I-Inter-annual and long-term variations generated by the stratospheric
QBO
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article; Proceedings Paper
CT 8th International Workshop on Layered Phenomena in the Mesopause Region
(LPMR-8)
CY AUG 20-23, 2007
CL Univ Alaska Fairbanks, Fairbanks, AK
SP Int Working Grp Layered Phenomena Mesopause Reg, Int Commiss Middle Atmosphere, Int Union Geodesy & Geophys, NASA, Natl Sci Fdn
HO Univ Alaska Fairbanks
DE Polar mesospheric clouds (PMC); Quasi-biennial oscillation (QBO);
Inter-annual variations; Middle atmosphere dynamics; Theoretical
modeling; Wave interactions
ID QUASI-BIENNIAL OSCILLATION; DOPPLER-SPREAD PARAMETERIZATION; TROPICAL
MIDDLE ATMOSPHERE; NUMERICAL SPECTRAL MODEL; WAVE MOMENTUM DEPOSITION;
NITRIC-OXIDE EXPLORER; GRAVITY-WAVES; MESOSPHERIC CLOUDS; SEMIANNUAL
OSCILLATION; CIRCULATION MODEL
AB We present results from the Numerical Spectral Model (NSM), which focus on the temperature environment of the mesopause region where polar mesospheric clouds (PMC) form. The PMC occur in summer and are observed varying on time scales from months to years, and the NSM describes the dynamical processes that can generate the temperature variations involved. The NSM simulates the quasi-biennial oscillation (QBO), which dominates the zonal circulation of the lower stratosphere at equatorial latitudes. The modeled QBO extends into the upper mesosphere, due to gravity wave (GW) filtering, consistent with LIARS zonal wind and TIMED temperature measurements. While the QBO zonal winds are confined to equatorial latitudes, the associated temperature variations extend to high latitudes. The meridional circulation redistributes the QBO energy-and the resulting temperature oscillations away from the equator produce inter-annual variations that can exceed 5 K in the polar mesopause region, with considerable differences between the two hemispheres. The NSM shows that the 30-month QBO produces a 5-year or semi-decadal (SD) oscillation, and stratospheric NCEP data provide observational evidence for that. This SD oscillation extends in the temperature to the upper mesosphere, where it Could contribute to the long-term variations of the region. Published by Elsevier Ltd.
C1 [Mayr, Hans G.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Mengel, John G.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Huang, Frank T.] Univ Maryland, Baltimore, MD 21201 USA.
RP Mayr, HG (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-3,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM hans.g.mayr@nasa.gov
NR 66
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 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD MAR
PY 2009
VL 71
IS 3-4
BP 497
EP 507
DI 10.1016/j.jastp.2008.09.033
PG 11
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 433UQ
UT WOS:000265231700022
ER
PT J
AU Mayr, HG
Mengel, JG
Huang, FT
Bailey, SM
AF Mayr, Hans G.
Mengel, John G.
Huang, Frank T.
Bailey, Scott M.
TI Modeling the temperature of the polar mesopause region: Part
II-Intra-seasonal monthly oscillations
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article; Proceedings Paper
CT 8th International Workshop on Layered Phenomena in the Mesopause Region
(LPMR-8)
CY AUG 20-23, 2007
CL Univ Alaska Fairbanks, Fairbanks, AK
SP Int Working Grp Layered Phenomena Mesopause Reg, Int Commiss Middle Atmosphere, Int Union Geodesy & Geophys, NASA, Natl Sci Fdn
HO Univ Alaska Fairbanks
DE Intra-seasonal oscillations (ISO); Polar mesospheric clouds (PMC);
Middle atmosphere dynamics; Theoretical modeling; Wave interactions
ID DOPPLER-SPREAD PARAMETERIZATION; WAVE MOMENTUM DEPOSITION; NITRIC-OXIDE
EXPLORER; MESOSPHERIC CLOUDS; EQUATORIAL MESOSPHERE; LOWER THERMOSPHERE;
MIDDLE ATMOSPHERE; INTRASEASONAL OSCILLATIONS; DIURNAL TIDES;
GRAVITY-WAVES
AB Measurements show that the polar mesospheric clouds (PMC) can vary, in the zonal mean, with periods around I month [Bailey et al., 2005. Observations of polar mesospheric clouds by the Student Nitric Oxide Explorer. J. Geophys. Res. 110, D13203, doi:10.1029/2004JD005422]. This observation has been the impetus for the present paper, where we describe corresponding temperature oscillations generated by the Numerical Spectral Model (NSM). Our numerical results are taken from the 3D and 2D versions of the NSM, which produce inter-annual and long-term variations in the polar mesopause region, as discussed in the accompanying paper (Part I). In the NSM, the intra-seasonal temperature variations with periods around 2 months are generated by the meridional winds that in turn are accelerated by the momentum deposition from small-scale gravity waves (GW) propagating north/south. The wave-driven dynamical process underlying the oscillations is intrinsically non-linear like that generating the quasi-biennial oscillation (QBO). Our analysis demonstrates that the seasonal annual and semi-annual variations excite the oscillation frequencies through non-linear cascading. Published by Elsevier Ltd.
C1 [Mayr, Hans G.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Mengel, John G.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Huang, Frank T.] Univ Maryland, Baltimore, MD 21201 USA.
[Bailey, Scott M.] Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA.
RP Mayr, HG (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-3,8900 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM hans.g.mayr@nasa.gov
NR 25
TC 3
Z9 3
U1 0
U2 0
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 MAR
PY 2009
VL 71
IS 3-4
BP 508
EP 517
DI 10.1016/j.jastp.2008.09.037
PG 10
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 433UQ
UT WOS:000265231700023
ER
PT J
AU Weingartner, T
Eisner, L
Eckert, GL
Danielson, S
AF Weingartner, Thomas
Eisner, Lisa
Eckert, Ginny L.
Danielson, Seth
TI Southeast Alaska: oceanographic habitats and linkages
SO JOURNAL OF BIOGEOGRAPHY
LA English
DT Article; Proceedings Paper
CT Workshop on Southeast Alaska Marine Biology and Oceanography
CY MAR 30-31, 2005
CL Univ Alaska SE, Juneau, AK
SP N Pacific Res Board
HO Univ Alaska SE
DE Geology; marine habitats; meteorology; ocean circulation; ocean mixing;
Southeast Alaska
ID NORTHEAST PACIFIC-OCEAN; CONTINENTAL-SHELF WAVES; VANCOUVER-ISLAND;
SPRING BLOOM; BRITISH-COLUMBIA; HECATE STRAIT; BARRIER JETS; LARVAL
FISH; SEA-LEVEL; AUKE BAY
AB We provide an overview of the physical oceanographic and geological processes that affect marine biological habitats and production in the marine waters throughout the archipelago and continental shelf of Southeast Alaska. Given the paucity of regional data, our overview summarizes work done in adjacent regions of the Gulf of Alaska shelf and basin, and draws on research carried out in similar settings elsewhere. The geological setting, which critically influences the regional meteorology and oceanography, includes a narrow continental shelf, deep channels that permeate the archipelago, fjords, glaciers and a rugged, mountainous coast. The large-scale meteorology is influenced primarily by seasonal variations in the intensity and position of the Aleutian Low. Winds, freshwater runoff, tides and cross-shelf exchange control the regional oceanography. The large-scale flow field advects mass, heat, salt, nutrients and planktonic organisms northward from British Columbia (and even further south) to the northern Gulf of Alaska along the slope, shelf, and within the channels of Southeast Alaska. The deep channels permeating the island archipelago and narrow continental shelf facilitate communication between basin and interior waters. Water properties and flow fields are subject to large annual variations in response to similarly large variations in winds and coastal freshwater discharge. The complex geological setting leads to large spatial heterogeneity in the physical processes controlling the local circulation fields and mixing, thereby creating numerous and diverse marine biological habitats. These various circulation and mixing processes modify substantially Southeast Alaska water masses and thus influence marine ecosystem processes downstream over the northern and western Gulf of Alaska shelf.
C1 [Weingartner, Thomas; Danielson, Seth] Univ Alaska, Inst Marine Sci, Fairbanks, AK 99775 USA.
[Eisner, Lisa] Natl Marine Fisheries Serv, Auke Bay Labs, Juneau, AK USA.
[Eckert, Ginny L.] Univ Alaska, Biol Program, Fairbanks, AK 99775 USA.
[Eckert, Ginny L.] Univ Alaska, Div Fisheries, Juneau, AK 99775 USA.
RP Weingartner, T (reprint author), Univ Alaska, Inst Marine Sci, Fairbanks, AK 99775 USA.
EM weingart@ims.uaf.edu
NR 74
TC 26
Z9 26
U1 3
U2 14
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0305-0270
EI 1365-2699
J9 J BIOGEOGR
JI J. Biogeogr.
PD MAR
PY 2009
VL 36
IS 3
BP 387
EP 400
DI 10.1111/j.1365-2699.2008.01994.x
PG 14
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 407CD
UT WOS:000263340300002
ER
PT J
AU Gonzalez, P
Borrajo, JP
Serra, J
Chiussi, S
Leon, B
Martinez-Fernandez, J
Varela-Feria, FM
de Arellano-Lopez, AR
de Carlos, A
Munoz, FM
Lopez, M
Singh, M
AF Gonzalez, P.
Borrajo, J. P.
Serra, J.
Chiussi, S.
Leon, B.
Martinez-Fernandez, J.
Varela-Feria, F. M.
de Arellano-Lopez, A. R.
de Carlos, A.
Munoz, F. M.
Lopez, M.
Singh, M.
TI A new generation of bio-derived ceramic materials for medical
applications
SO JOURNAL OF BIOMEDICAL MATERIALS RESEARCH PART A
LA English
DT Article
DE silicon carbide; biomineralization; porosity; in vitro test; in vivo
test; cell proliferation; bone ingrowth; osteointegration
ID SILICON-CARBIDE; MECHANICAL-BEHAVIOR
AB A new generation of bio-derived ceramics can be developed as a base material for medical implants. Specific plant species are used as templates on which innovative transformation processes can modify the chemical composition maintaining the original biostructure. Building on the outstanding mechanical properties of the starting lignocellulosic templates, it is possible to develop lightweight and high-strength scaffolds for bone substitution. In vitro and in vivo experiments demonstrate the excellent biocompatibility of this new silicon carbide material (bioSiC) and how it gets colonized by the hosting bone tissue because of its unique interconnected hierarchic porosity, which opens the door to new biomedical applications. (C) 2008 Wiley Periodicals, Inc. J Biomed Mater Res 88A: 807-813, 2009
C1 [Gonzalez, P.; Borrajo, J. P.; Serra, J.; Chiussi, S.; Leon, B.] Univ Vigo, Dept Fis Aplicada, Vigo 36310, Spain.
[Martinez-Fernandez, J.; Varela-Feria, F. M.; de Arellano-Lopez, A. R.] Univ Seville, Dept Fis Mat Condensada, ICMSE, Seville, Spain.
[de Carlos, A.] Univ Vigo, Dept Bioquim Genet & Inmunol, Vigo 36310, Spain.
[Munoz, F. M.; Lopez, M.] Univ Santiago Compostela, Dept Ciencias Clin Vet, Fac Vet, Lugo, Spain.
[Singh, M.] NASA, Ohio Aerosp Inst, Glenn Res Ctr, Cleveland, OH USA.
RP Gonzalez, P (reprint author), Univ Vigo, Dept Fis Aplicada, Campus Lagoas Marcosende, Vigo 36310, Spain.
EM pglez@uvigo.es
RI Chiussi, Stefano/D-6218-2014; New Materials Group, FA3/D-6799-2014; de
Carlos, Alejandro/L-5819-2014; MARTINEZ FERNANDEZ, JULIAN/K-1826-2012;
Lopez Pena, Monica/L-2121-2014; Munoz, Fernando/I-1858-2015;
OI GONZALEZ, PIO/0000-0002-7353-712X; R. de Arellano Lopez,
Antonio/0000-0002-7443-0244; Chiussi, Stefano/0000-0002-3933-8725; New
Materials Group, FA3/0000-0003-4286-2015; de Carlos,
Alejandro/0000-0003-0138-4918; MARTINEZ FERNANDEZ,
JULIAN/0000-0002-1199-6638; Lopez Pena, Monica/0000-0001-6387-4790;
Munoz, Fernando/0000-0002-4130-1526; Serra, Julia/0000-0001-6187-4025
FU University of Vigo [MAT2004-02791, PGID1T03TMT30101PR,
PGIDT05PXIC30301PN]; Seville [MAT2006-13005-C03]
FX The authors thank E. Solla, V. Castano, J. Rodino, and N. Mino. The
University of Vigo acknowledges the financial support of projects
MAT2004-02791, PGID1T03TMT30101PR and PGIDT05PXIC30301PN. The research
in Seville was funded by project MAT2006-13005-C03.
NR 24
TC 21
Z9 21
U1 0
U2 15
PU WILEY-LISS
PI HOBOKEN
PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 1549-3296
J9 J BIOMED MATER RES A
JI J. Biomed. Mater. Res. Part A
PD MAR 1
PY 2009
VL 88A
IS 3
BP 807
EP 813
DI 10.1002/jbm.a.31951
PG 7
WC Engineering, Biomedical; Materials Science, Biomaterials
SC Engineering; Materials Science
GA 404BP
UT WOS:000263126000029
PM 18384165
ER
PT J
AU Kurtoglu, T
Campbell, MI
Arnold, CB
Stone, RB
Mcadams, DA
AF Kurtoglu, Tolga
Campbell, Matthew I.
Arnold, Cari Bryant
Stone, Robert B.
Mcadams, Daniel A.
TI A Component Taxonomy as a Framework for Computational Design Synthesis
SO JOURNAL OF COMPUTING AND INFORMATION SCIENCE IN ENGINEERING
LA English
DT Article
ID CONCEPTUAL DESIGN; KNOWLEDGE; ONTOLOGY; SYSTEMS
AB In this paper we present our findings on the development of a taxonomy for electromechanical components. In building this taxonomy, we have two main objectives: First, we strive to establish a framework for future computational tools that archive, search, or reuse component knowledge during the conceptual phase of design. Second, we aim to define a standard vocabulary that derives uniformity and consistency in the representation of electromechanical component space. Through both empirically dissecting existing products and defining categories based on functional analysis, we defined 135 generic component types. The use and necessity of the resulting taxonomy by a suite of computational design tools are illustrated in two applications of conceptual design. [DOI:10.1115/1.3086032]
C1 [Kurtoglu, Tolga] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Campbell, Matthew I.] Univ Texas Austin, Dept Mech Engn, Austin, TX 78712 USA.
[Arnold, Cari Bryant] Penn State Univ, Engn Design Program, University Pk, PA 16802 USA.
[Stone, Robert B.] Missouri Univ Sci & Technol, Dept Interdisciplinary Engn, Rolla, MO 65409 USA.
[Mcadams, Daniel A.] Texas A&M Univ, Dept Mech Engn, College Stn, TX USA.
RP Kurtoglu, T (reprint author), NASA, Ames Res Ctr, MS 269-3 Moffett Field, Moffett Field, CA 94035 USA.
EM tolga.kurtoglu@nasa.gov; mc1@mail.utexas.edu; cari.arnold@psu.edu;
rstone@mst.edu; dmcadams@tamu.edu
FU National Science Foundation [IIS-0307665]
FX The authors would like to thank the National Science Foundation for
supporting this work under Grant No.IIS-0307665.
NR 36
TC 20
Z9 20
U1 1
U2 3
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 1530-9827
J9 J COMPUT INF SCI ENG
JI J. Comput. Inf. Sci. Eng.
PD MAR
PY 2009
VL 9
IS 1
AR 011007
DI 10.1115/1.3086032
PG 10
WC Computer Science, Interdisciplinary Applications; Engineering,
Manufacturing
SC Computer Science; Engineering
GA 442LE
UT WOS:000265841900008
ER
PT J
AU Delgado, IR
Steinetz, BM
Rimnac, CM
Lewandowski, JJ
AF Delgado, Irebert R.
Steinetz, Bruce M.
Rimnac, Clare M.
Lewandowski, John J.
TI Fatigue Crack Growth Behavior Evaluation of Grainex Mar-M 247 for NASA's
High Temperature High Speed Turbine Seal Test Rig
SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE
ASME
LA English
DT Article; Proceedings Paper
CT 52nd ASME Turbo Expo 2007
CY MAY 14-17, 2007
CL Montreal, CANADA
SP Amer Soc Mech Engineers, Int Gas Turbine Inst
DE aerospace industry; aerospace test facilities; eddy current testing;
fatigue cracks; gas turbines; jet engines; seals (stoppers)
ID LIFE
AB The fatigue crack growth behavior of Grainex Mar-M 247 is evaluated for NASA's turbine seal test facility. The facility is used to test air-to-air seals primarily for use in advanced jet engine applications. Because of extreme seal test conditions of temperature, pressure, and surface speeds, surface cracks may develop over time in the disk bolt holes. An inspection interval is developed to preclude catastrophic disk failure by using experimental fatigue crack growth data. By combining current fatigue crack growth results with previous fatigue strain-life experimental work, an inspection interval is determined for the test disk. The fatigue crack growth life of NASA disk bolt holes is found to be 367 cycles at a crack depth of 0.501 mm using a factor of 2 on life at maximum operating conditions. Combining this result with previous fatigue strain-life experimental work gives a total fatigue life of 1032 cycles at a crack depth of 0.501 mm. Eddy-current inspections are suggested starting at 665 cycles since eddy current detection thresholds are currently at 0.381 mm. Inspection intervals are recommended every 50 cycles when operated at maximum operating conditions.
C1 [Delgado, Irebert R.; Steinetz, Bruce M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Rimnac, Clare M.; Lewandowski, John J.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
RP Delgado, IR (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM irebert.r.delgado@nasa.gov
NR 31
TC 0
Z9 0
U1 1
U2 9
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0742-4795
J9 J ENG GAS TURB POWER
JI J. Eng. Gas. Turbines Power-Trans. ASME
PD MAR
PY 2009
VL 131
IS 2
AR 022504
DI 10.1115/1.2980058
PG 12
WC Engineering, Mechanical
SC Engineering
GA 393KN
UT WOS:000262372300014
ER
PT J
AU Howard, SA
AF Howard, Samuel A.
TI Misalignment in Gas Foil Journal Bearings: An Experimental Study
SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE
ASME
LA English
DT Article; Proceedings Paper
CT 53rd ASME Turbo Expo 2008
CY JUN 09-13, 2008
CL Berlin, GERMANY
SP Int Gas Turbine Inst, ASME
DE dynamic response; machine bearings; monitoring; production equipment;
rotors
AB As gas foil journal bearings become more prevalent in production machines, such as small gas turbine propulsion systems and microturbines, system level performance issues must be identified and quantified in order to provide for successful design practices. Several examples of system level design parameters that are not fully understood in foil bearing systems are thermal management schemes, alignment requirements, balance requirements, thrust load balancing, and others. In order to address some of these deficiencies and begin to develop guidelines, this paper presents a preliminary experimental investigation of the misalignment tolerance of gas foil journal bearing systems. Using a notional gas foil bearing supported rotor and a laser-based shaft alignment system, increasing levels of misalignment are imparted to the bearing supports while monitoring temperature at the bearing edges. The amount of misalignment that induces bearing failure is identified and compared with other conventional bearing types such as cylindrical roller bearings and angular contact ball bearings. Additionally, the dynamic response of the rotor indicates that the gas foil bearing force coefficients may be affected by misalignment.
C1 NASA, Glenn Res Ctr, Brookpark, OH 44135 USA.
RP Howard, SA (reprint author), NASA, Glenn Res Ctr, Brookpark, OH 44135 USA.
EM samuel.a.howard@nasa.gov
NR 13
TC 15
Z9 15
U1 0
U2 13
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0742-4795
J9 J ENG GAS TURB POWER
JI J. Eng. Gas. Turbines Power-Trans. ASME
PD MAR
PY 2009
VL 131
IS 2
AR 022501
DI 10.1115/1.2966392
PG 7
WC Engineering, Mechanical
SC Engineering
GA 393KN
UT WOS:000262372300011
ER
PT J
AU Fong, T
Nagatani, K
Wettergreen, D
AF Fong, Terrence
Nagatani, Keiji
Wettergreen, David
TI Space Robotics, Part I
SO JOURNAL OF FIELD ROBOTICS
LA English
DT Editorial Material
C1 [Fong, Terrence] NASA, Ames Res Ctr, Washington, DC USA.
[Nagatani, Keiji] Tohoku Univ, Sendai, Miyagi 980, Japan.
[Wettergreen, David] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA.
RP Fong, T (reprint author), NASA, Ames Res Ctr, Washington, DC USA.
NR 0
TC 0
Z9 0
U1 0
U2 3
PU JOHN WILEY & SONS INC
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 1556-4959
J9 J FIELD ROBOT
JI J. Field Robot.
PD MAR
PY 2009
VL 26
IS 3
BP 241
EP 242
DI 10.1002/rob.20290
PG 2
WC Robotics
SC Robotics
GA 414SB
UT WOS:000263884400001
ER
PT J
AU Kim, WS
Nesnas, IA
Bajracharya, M
Madison, R
Ansar, AI
Steele, RD
Biesiadecki, JJ
Ali, KS
AF Kim, Won S.
Nesnas, Issa A.
Bajracharya, Max
Madison, Richard
Ansar, Adnan I.
Steele, Robert D.
Biesiadecki, Jeffrey J.
Ali, Khaled S.
TI Targeted Driving Using Visual Tracking on Mars: From Research to Flight
SO JOURNAL OF FIELD ROBOTICS
LA English
DT Article
ID IMAGE REGISTRATION
AB This paper presents the development, validation, and deployment of the visual target tracking capability onto the Mars Exploration Rover (MER) mission. Visual target tracking enables targeted driving, in which the rover approaches a designated target in a closed visual feedback loop, increasing the target position accuracy by an order of magnitude and resulting in fewer ground-in-the-loop cycles. As a result of an extensive validation, we developed a reliable normalized cross-correlation visual tracker. To enable tracking with the limited computational resources of a planetary rover, the tracker uses the vehicle motion estimation to scale and roll the template image, compensating for large image changes between rover steps. The validation showed that a designated target can be reliably tracked within several pixels or a few centimeters of accuracy over a 10-m traverse using a rover step size of 10% of the target distance in any direction. It also showed that the target is not required to have conspicuous features and can be selected anywhere on natural rock surfaces excluding rock boundary and shadowed regions. The tracker was successfully executed on the Opportunity rover near Victoria Crater on four distinct runs, including a single-sol instrument placement. We present the flight experiment data of the tracking performance and execution time. (c) 2009 whey Periodicals, Inc.
C1 [Kim, Won S.; Nesnas, Issa A.; Bajracharya, Max; Ansar, Adnan I.; Steele, Robert D.; Biesiadecki, Jeffrey J.; Ali, Khaled S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Madison, Richard] Charles Stark Draper Lab, Cambridge, MA 02139 USA.
RP Kim, WS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Won.S.Kim@jpl.nasa.gov; Issa.A.Nesnas@jpl.nasa.gov;
Max.Bajracharya@jpl.nasa.gov; rmadison@draper.com;
Adnan.I.Ansar@jpl.nasa.gov; Robert.D.Steele@jpl.nasa.gov;
Jeffrey.J.Biesiadecki@jpl.nasa.gov; Khaled.S.Ali@jpl.nasa.gov
FU NASA Mars Technology Program; Mars Science Laboratory Focused Technology
Program, and Mars Exploration Program
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. This work is supported by the NASA Mars
Technology Program, Mars Science Laboratory Focused Technology Program,
and Mars Exploration Program. The authors would like to acknowledge
contributions by Clayton Kunz, Esfandiar Bandari, Maria Bualat, Matt
Deans, and Liam Pedersen at NASA Ames Research Center. The authors also
would like to thank Mark Maimone for valuable suggestions during the VTT
integration into MER, Richard Volpe for suggesting the template image
roll, and Sarnad Hayati and Gabriel Udomkesmalee for their support.
Reviewers' cornments greatly enhanced the quality of this paper.
NR 39
TC 6
Z9 6
U1 1
U2 3
PU JOHN WILEY & SONS INC
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 1556-4959
J9 J FIELD ROBOT
JI J. Field Robot.
PD MAR
PY 2009
VL 26
IS 3
BP 243
EP 263
DI 10.1002/rob.20283
PG 21
WC Robotics
SC Robotics
GA 414SB
UT WOS:000263884400002
ER
PT J
AU Hernandez-Pajares, M
Juan, JM
Sanz, J
Orus, R
Garcia-Rigo, A
Feltens, J
Komjathy, A
Schaer, SC
Krankowski, A
AF Hernandez-Pajares, M.
Juan, J. M.
Sanz, J.
Orus, R.
Garcia-Rigo, A.
Feltens, J.
Komjathy, A.
Schaer, S. C.
Krankowski, A.
TI The IGS VTEC maps: a reliable source of ionospheric information since
1998
SO JOURNAL OF GEODESY
LA English
DT Article
DE GPS; Ionospheric VTEC maps; IGS; GNSS
ID TOTAL ELECTRON-CONTENT; LUNAR TIDE
AB The International GNSS Service (IGS) Working Group on Ionosphere was created in 1998. Since then, the Scientific community behind IGS, in particular CODE, ESA, JPL and UPC, have been continuosly contributing to reliable IGS combined vertical total electron content (VTEC) maps in both rapid and final schedules. The details on how these products are being generated, performance numbers, proposed improvement as far as VTEC evolution trends during near one Solar Cycle, are summarized in this paper. The confirmation of (1) the good performance of the IGS combined VTEC maps, and (2) the characteristic VTEC variability periods, are two main results of this work.
C1 [Orus, R.] ESTEC ESA, Propagat Sect, Noordwijk, Netherlands.
[Feltens, J.] ESOC ESA, Darmstadt, Germany.
[Komjathy, A.] JPL NASA, Pasadena, CA USA.
[Schaer, S. C.] CODE Swisstopo, Bern, Switzerland.
[Krankowski, A.] UWM Olsztyn, Olsztyn, Poland.
RP Hernandez-Pajares, M (reprint author), gAGE UPC Mod C3 Campus Nord,Jordi Girona 1-3, Barcelona 08034, Spain.
EM manuel@mat.upc.es
RI Juan Zornoza, Jose Miguel/S-6224-2016; Sanz Subirana, Jaume/C-1265-2014
OI Juan Zornoza, Jose Miguel/0000-0003-1126-2367; Sanz Subirana,
Jaume/0000-0001-8880-7084
FU IGS [ESP2007-62676]
FX The authors are grateful to the IGS community support in general and to
different sponsors partially supporting their work for IGS, such as the
Spanish project ESP2007-62676 for UPC authors.
NR 27
TC 206
Z9 225
U1 7
U2 31
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0949-7714
J9 J GEODESY
JI J. Geodesy
PD MAR
PY 2009
VL 83
IS 3-4
BP 263
EP 275
DI 10.1007/s00190-008-0266-1
PG 13
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA 409RX
UT WOS:000263524600009
ER
PT J
AU Beutler, G
Moore, AW
Mueller, II
AF Beutler, Gerhard
Moore, Angelyn W.
Mueller, Ivan I.
TI The international global navigation satellite systems service (IGS):
development and achievements
SO JOURNAL OF GEODESY
LA English
DT Article
DE Global positioning system (GPS); Global navigation satellite systems
(GNSS); Orbit determination; International GNSS service
AB Since 21 June 1992 the International GPS Service (IGS), renamed International GNSS Service in 2005, produces and makes available uninterrupted time series of its products, in particular GPS observations from the IGS Global Network, GPS orbits, Earth orientation parameters (components x and y of polar motion, length of day) with daily time resolution, satellite and receiver clock information for each day with different latencies and accuracies, and station coordinates and velocities in weekly batches for further analysis by the IERS (International Earth Rotation and Reference Systems Service). At a later stage the IGS started exploiting its network for atmosphere monitoring, in particular for ionosphere mapping, for troposphere monitoring, and time and frequency transfer. This is why new IGS products encompass ionosphere maps and tropospheric zenith delays. This development became even more important when more and more space-missions carrying space-borne GPS for various purposes were launched. This article offers an overview for the broader scientific community of the development of the IGS and of the spectrum of topics addressed today with IGS data and products.
C1 [Beutler, Gerhard] Univ Bern, Inst Astron, CH-3012 Bern, Switzerland.
[Moore, Angelyn W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mueller, Ivan I.] Ohio State Univ, Dept Geodet Sci, Hilliard, OH 43026 USA.
RP Beutler, G (reprint author), Univ Bern, Inst Astron, Sidlerstr 5, CH-3012 Bern, Switzerland.
EM gerhard.beutler@aiub.unibe.ch; awmoore@mail.jpl.nasa.gov;
mueller.3@osu.edu
FU National Aeronautics and Space Administration
FX The contributions of the IGS network to the scientific community are
fundamentally due to the diligent effort of the many site operators
worldwide. Likewise, the development of IGS' geodetic products is thanks
to personnel at each analysis center. The long-term success of the IGS
is a credit to the Governing Board members, product coordinators, and
Central Bureau management past and present. A. Moore'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 24
TC 15
Z9 16
U1 1
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0949-7714
J9 J GEODESY
JI J. Geodesy
PD MAR
PY 2009
VL 83
IS 3-4
BP 297
EP 307
DI 10.1007/s00190-008-0268-z
PG 11
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA 409RX
UT WOS:000263524600012
ER
PT J
AU Noll, C
Bock, Y
Habrich, H
Moore, A
AF Noll, C.
Bock, Y.
Habrich, H.
Moore, A.
TI Development of data infrastructure to support scientific analysis for
the International GNSS Service
SO JOURNAL OF GEODESY
LA English
DT Article
DE GNSS; GPS; GLONASS; IGS; IAG; Space geodesy; GGOS; Reference frames;
Tracking networks; Precise orbit determination; Earth orientation
parameters
ID ACHIEVEMENTS; SYSTEMS
AB The International GNSS Service provides data and products to support a wide range of global, multidisciplinary scientific research. The service has established a hierarchy of components to facilitate its mission: a globally distributed network of Tracking Stations, Data Centers, Analysis Centers, a Central Bureau, and a Governing Board. The Data Centers, in conjunction with the Central Bureau, serve as the primary means of distributing GNSS data, products, and general information to the user community through ftp and Web servers and email services. The requirements of analysis centers and the scientific community have evolved over the lifetime of the IGS, requiring enhancement and extension of the supporting data center infrastructure. The diversity of IGS data and products extends today from the realm of the real-time and near real-time to the long-term archive and thus forms a basis for multidisciplinary research spanning decades. Reliability of all components is a key requirement within the IGS and is accomplished through the geographic distribution of data centers and the creation of independent, redundant, parallel channels for the transmission of data and products. We discuss the development of the IGS data infrastructure, current status, and plans for future enhancements. Descriptions of IGS data and products and associated metadata are also included.
C1 [Noll, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bock, Y.] Univ Calif San Diego, Cecil H & Ida M Green Inst Geophys & Planetary Ph, La Jolla, CA 92093 USA.
[Habrich, H.] Bundesamt Kartographie & Geodasie, D-60598 Frankfurt, Germany.
[Moore, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Noll, C (reprint author), NASA, Goddard Space Flight Ctr, Code 690-1, Greenbelt, MD 20771 USA.
EM Carey.Noll@nasa.gov; ybock@ucsd.edu; heinz.habrich@bkg.bund.de;
Angelyn.W.Moore@jpl.nasa.gov
RI Noll, Carey/D-8884-2012
FU National Aeronautics and Space Administration; NASA/REASoN through JPL;
NASA/ACCESS/; System Research Laboratory through the Joint Institute of
Marine Sciences
FX The authors would like to acknowledge the support of the organizations
contributing to the International GNSS Service. The work of A. Moore is
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. The work at SOPAC is funded by a NASA/REASoN grant
through JPL, a NASA/ACCESS/grant, and a NOAA grant from the Earth System
Research Laboratory through the Joint Institute of Marine Sciences.
Thanks to Frank Webb, Sharon Kedar and Paul Jamason for their input.
NR 22
TC 6
Z9 6
U1 0
U2 4
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0949-7714
J9 J GEODESY
JI J. Geodesy
PD MAR
PY 2009
VL 83
IS 3-4
BP 309
EP 325
DI 10.1007/s00190-008-0245-6
PG 17
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA 409RX
UT WOS:000263524600013
ER
PT J
AU Byun, SH
Bar-Sever, YE
AF Byun, Sung H.
Bar-Sever, Yoaz E.
TI A new type of troposphere zenith path delay product of the international
GNSS service
SO JOURNAL OF GEODESY
LA English
DT Article
DE Zenith path delay; ZPD; IGS; Troposphere; GPS antenna phase map;
Analysis centers (ACs)
ID ATMOSPHERIC WATER-VAPOR; MAPPING FUNCTIONS; GPS RECEIVER; METEOROLOGY
AB The International GNSS Service (IGS) has been producing the total troposphere zenith path delay (ZPD) product that is based on combined ZPD contributions from several IGS Analysis Centers (AC) since GPS week 890 in 1997. A new approach to the production of the IGS ZPD has been proposed that replaces the direct combination of diverse ZPD products with point positioning estimates using the IGS Combined Final orbit and clock products. The new product was formally adopted in 2007 after several years of concurrent production with the legacy product. We describe here the advantages of the new approach for the IGS ZPD product, which enhance the value of the new ZPD product for climate studies. We also address the impact the IGS adoption in November 2006 of new GPS antenna phase center standards has had on the new ZPD product. Finally we describe plans to further enhance the ZPD products.
C1 [Byun, Sung H.; Bar-Sever, Yoaz E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bar-Sever, YE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM byun@jpl.nasa.gov; yoaz.e.bar-sever@jpl.nasa.gov
FU Jet Propulsion Laboratory; California Institute of Technology; National
Aeronautics and Space Administration
FX The research described in this publication was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 11
TC 62
Z9 66
U1 5
U2 23
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0949-7714
J9 J GEODESY
JI J. Geodesy
PD MAR
PY 2009
VL 83
IS 3-4
BP 367
EP 373
DI 10.1007/s00190-008-0288-8
PG 7
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA 409RX
UT WOS:000263524600018
ER
PT J
AU Sridhar, B
Chen, NY
AF Sridhar, Banavar
Chen, Neil Y.
TI Short-Term National Airspace System Delay Prediction Using Weather
Impacted Traffic Index
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID IDENTIFICATION
C1 [Sridhar, Banavar] NASA, Ames Res Ctr, Aviat Syst Div, Moffett Field, CA 94035 USA.
RP Sridhar, B (reprint author), NASA, Ames Res Ctr, Aviat Syst Div, Moffett Field, CA 94035 USA.
NR 16
TC 3
Z9 3
U1 0
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD MAR-APR
PY 2009
VL 32
IS 2
BP 657
EP 662
DI 10.2514/1.38798
PG 6
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 422FP
UT WOS:000264413200031
ER
PT J
AU Capo-Lugo, PA
Bainum, PM
AF Capo-Lugo, Pedro A.
Bainum, Peter M.
TI Solar Pressure Effects for a Constellation in Highly Elliptical Orbit
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
C1 [Bainum, Peter M.] Howard Univ, Dept Mech Engn, Washington, DC 20059 USA.
[Capo-Lugo, Pedro A.] NASA, George C Marshall Space Flight Ctr, Navigat & Control Syst Design & Anal Branch, Huntsville, AL 35812 USA.
RP Bainum, PM (reprint author), Howard Univ, Dept Mech Engn, Washington, DC 20059 USA.
EM Pedro.A.Capo-Lugo@nasa.gov; pbainum@fac.howard.edu
FU National Science Foundation (NSF); Alliances for Graduate Education and
Professoriate (AGEP)
FX This research has been supported by the National Science Foundation
(NSF) Alliances for Graduate Education and Professoriate (AGEP) Program
at Howard University
NR 16
TC 3
Z9 3
U1 1
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD MAR-APR
PY 2009
VL 32
IS 2
BP 675
EP 679
DI 10.2514/1.37484
PG 5
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 422FP
UT WOS:000264413200035
ER
PT J
AU Bayard, DS
AF Bayard, David S.
TI Reduced-Order Kalman Filtering with Relative Measurements
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bayard, DS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM david.bayard@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Inslitute of Technology; National
Aeronautics and Space Administration
FX This research was performed at the Jet Propulsion Laboratory, California
Inslitute of Technology, under a contract with the National Aeronautics
and Space Administration, and funded through the internal Research and
Technology Development program.
NR 16
TC 6
Z9 6
U1 0
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD MAR-APR
PY 2009
VL 32
IS 2
BP 679
EP 686
DI 10.2514/1.37217
PG 8
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 422FP
UT WOS:000264413200036
ER
PT J
AU Sengupta, A
Goebel, DM
Owens, AG
AF Sengupta, Anita
Goebel, Dan M.
Owens, Allison G.
TI Langmuir Probe Studies of Magnetic Confinement in an Ion Thruster
Discharge Plasma
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article; Proceedings Paper
CT AIAA/ASME/SAE/ASEE 41st Joint Propulsion Conference
CY JUL 10-13, 2005
CL Tucson, AZ
SP AIAA, ASME, SAE, ASEE
ID DIAGNOSTICS
AB Magnetic confinement studies on a 30-cm-diameter ion thruster were performed to determine the dependence of plasma confinement and uniformity on the ring-cusp magnetic field. Tour primary cases were investigated to determine the effects of an additional magnetic cusp, increasing the strength of the highest value closed magnetic contour line, and varying the magnetic field free volume. A laboratory model NASA Solar Electric Propulsion Technology Application Readiness engine was modified to investigate three- and four-ring-cusp geometries. Electrical parameters and langmuir probe sweeps in the discharge chamber were used to measure the performance of each configuration. Increasing the strength of the closed magnetic contour line reduces ion loss to the anode, resulting in a reduction fit discharge power for a given beam current. Similarly, increasing the magnetic field free volume in the near-grid region improves plasma uniformity, removing the on-axis current density peak responsible for accelerator grid erosion. The enhanced magnetic circuit geometries investigated resulted in a 20% reduction in discharge loss and discharge current at the TH15 (2.3 kW) throttle point, with similar gains over the full throttle range. The reduction in discharge power and peak current density can significantly increase the total throughout per engine by limiting wear mechanisms that limit thruster life.
C1 [Sengupta, Anita; Goebel, Dan M.; Owens, Allison G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sengupta, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 125-109, Pasadena, CA 91109 USA.
NR 21
TC 3
Z9 4
U1 1
U2 6
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
J9 J PROPUL POWER
JI J. Propul. Power
PD MAR-APR
PY 2009
VL 25
IS 2
BP 387
EP 396
DI 10.2514/1.36547
PG 10
WC Engineering, Aerospace
SC Engineering
GA 423JP
UT WOS:000264492900015
ER
PT J
AU Panzarella, CH
Kassemi, M
AF Panzarella, Charles H.
Kassemi, Mohammad
TI Comparison of Several Zero-Boil-Off Pressure Control Strategies for
Cryogenic Fluid Storage in Microgravity
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
ID SPACE; TANKS
AB Four different tank pressure control strategies based on various combinations of active cooling and/or forced mixing are investigated numerically. The first, and most effective, strategy uses a subcooled liquid,jet to simultaneously mix and cool the bulk liquid. The second strategy is based on separate mixing and cooling via a forced uncooled liquid jet and an independent cold finger. The third strategy uses a cold finger alone with no forced mixing. Finally, the fourth strategy examines the effect of mixing alone without any active cooling. Detailed numerical solutions are obtained for each case by solving the Navier-Stokes and energy equations in the liquid region coupled to a lumped heat and mass treatment of the vapor region. It is shown that the most rapid and effective means of countering self-pressurization is achieved with a subcooled liquid jet. In the case of separate mixing and cooling, the pressure can still be reduced, but over a much longer period of time. Finally, cooling without any forced mixing is able to limit the pressure rise, but not very effectively, although for long-duration storage in which rapid pressure control is not required, this may still constitute a viable approach. While presenting the results of the various simulation case studies, an in-depth comparative analysis of transport phenomena associated with each case is also performed from which salient engineering recommendations are derived for optimization of the zero-boil-off design.
C1 [Panzarella, Charles H.] Equ Engn Grp, Shaker Hts, OH 44122 USA.
[Kassemi, Mohammad] NASA, Lewis Field, John H Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH 44135 USA.
RP Panzarella, CH (reprint author), Equ Engn Grp, 20600 Chagrin Blvd, Shaker Hts, OH 44122 USA.
EM chpanzarella@equityeng.com; mohammad.kassemi@nasa.gov
FU Cryogenic Fluid Management (CFM)
FX This work has been supported by the Cryogenic Fluid Management (CFM)
Project under NASA's Exploration Technology Development Program, The
valuable technical discussions and suggestions provided by David
Plachta, David Chato, and Jeffery Moder it NASA John H. Glenn Research
Center at Lewis Field are,list) gratefully acknowledged.
NR 28
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U1 1
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
J9 J PROPUL POWER
JI J. Propul. Power
PD MAR-APR
PY 2009
VL 25
IS 2
BP 424
EP 434
DI 10.2514/1.35611
PG 11
WC Engineering, Aerospace
SC Engineering
GA 423JP
UT WOS:000264492900019
ER
PT J
AU Mishchenko, MI
Berg, MJ
Sorensen, CM
van der Mee, CVM
AF Mishchenko, Michael I.
Berg, Matthew J.
Sorensen, Christopher M.
van der Mee, Cornelis V. M.
TI On definition and measurement of extinction cross section
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Electromagnetic scattering; Extinction
ID ABSORBING MEDIUM; LIGHT-SCATTERING; OPTICAL THEOREM; PARTICLES; MEDIA
AB Following the recent analyses of extinction by Berg et al. [J Opt Soc Am A 2008,25:1504-1513, J Opt Soc. Am A 2008;25:1514-1520], we show that although it is possible to define and measure the extinction cross section for a single particle using a detector of light facing the incident beam, this requires certain theoretical assumptions and experimental precautions. Published by Elsevier Ltd.
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Berg, Matthew J.; Sorensen, Christopher M.] Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA.
[van der Mee, Cornelis V. M.] Univ Cagliari, Dipartimento Matemat & Informat, I-09123 Cagliari, Italy.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM mmishchenko@giss.nasa.gov
RI Sorensen, Christopher/G-4900-2013; Mishchenko, Michael/D-4426-2012
OI Sorensen, Christopher/0000-0002-1980-3394;
FU NASA
FX We thank two anonymous reviewers for useful comments on a preliminary
version of this paper. This research was partially sponsored by the NASA
Radiation Sciences Program managed by Hal Maring.
NR 13
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U1 2
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAR
PY 2009
VL 110
IS 4-5
BP 323
EP 327
DI 10.1016/j.jqsrt.2008.11.010
PG 5
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 427KQ
UT WOS:000264778600009
ER
PT J
AU Mazaheri, A
Wood, WA
AF Mazaheri, Alireza
Wood, William A.
TI Heating Augmentation for Short Hypersonic Protuberances
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB Computational aeroheating analyses of the Space Shuttle Orbiter plug-repair models are validated against data collected in the Calspan-University of Buffalo Research Center 48 in. shock tunnel. The comparison shows that the average difference between computed heat transfer results and the data is about 9.5%. Using computational fluid dynamics and wind-tunnel data, an empirical correlation for estimating heating augmentation oil short hypersonic protuberances (k/delta < 0.3) is proposed. This proposed correlation is compared with several computed flight simulation cases and good agreement is achieved. Accordingly, this correlation is proposed for further investigation (on other short hypersonic protuberances For estimating heating augmentation.
C1 [Mazaheri, Alireza] Analyt Mech Associates Inc, Aerothermodynam Branch, Hampton, VA 23666 USA.
[Mazaheri, Alireza; Wood, William A.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
RP Mazaheri, A (reprint author), Analyt Mech Associates Inc, Aerothermodynam Branch, Hampton, VA 23666 USA.
EM Ali.R.Mazaheri@nasa.gov; William.A.Wood@nasa.gov
FU NASA Langley Research Center [NNL06AC49T]
FX The work of the first author is funded by NASA Langley Research Center
through contact number NNL06AC49T.
NR 12
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Z9 4
U1 0
U2 0
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2009
VL 46
IS 2
BP 284
EP 291
DI 10.2514/1.39992
PG 8
WC Engineering, Aerospace
SC Engineering
GA 429EI
UT WOS:000264903200009
ER
PT J
AU Prince, JL
Dec, JA
Tolson, RH
AF Prince, Jill L.
Dec, John A.
Tolson, Robert H.
TI Autonomous Aerobraking Using Thermal Response Surface Analysis
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID MARS ODYSSEY AEROBRAKING; ACCELEROMETER DATA; GLOBAL SURVEYOR
AB Aerobraking is a proven method of significantly increasing fire science payload that can be placed into low Mars orbits when compared to an all propulsive capture. However the aerobraking phase is long and has mission cost and risk implications. The main cost benefit is that aerobraking permits the use of a smaller and cheaper launch vehicle, but additional operational costs are incurred during the long aerobraking phase. Risk is increased due to the repeated thermal loading of spacecraft components and the multiple attitude kind propulsive maneuvers required for successful aerobraking. Both the cost and risk burdens can be significantly reduced by automating the aerobraking operations phase. All of the previous Mars orbiter missions that have used aerobraking have increasingly relied on onboard calculations during aerobraking. Even though the tempearature of spacecraft components has been the limiting factor, operational methods have relied on using a surrogate variable for mission control. This paper describes several methods, based directly on space craft component maximum temperature, tor autonomously predicting the subsequent aerobraking, orbits and prescribing apoapsis propulsive maneuvers to maintain the spacecraft within specified temperature limits. Specifically, this paper describes the rise of thermal response surface analysis in predicting the temperature of the spacecraft components and the corresponding uncertainty in this temperature prediction.
C1 [Prince, Jill L.] NASA, Langley Res Ctr, Explorat Syst Engn Branch, Hampton, VA 23681 USA.
[Dec, John A.] NASA, Langley Res Ctr, Struct & Thermal Syst Branch, Hampton, VA 23681 USA.
[Tolson, Robert H.] N Carolina State Univ, Dept Mech & Aerosp Engn, Hampton, VA 23666 USA.
RP Prince, JL (reprint author), NASA, Langley Res Ctr, Explorat Syst Engn Branch, Mail Stop 489, Hampton, VA 23681 USA.
NR 14
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Z9 4
U1 0
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2009
VL 46
IS 2
BP 292
EP 298
DI 10.2514/1.32793
PG 7
WC Engineering, Aerospace
SC Engineering
GA 429EI
UT WOS:000264903200010
ER
PT J
AU Yam, CH
Davis, DC
Longuski, JM
Howell, KC
Buffington, B
AF Yam, Chit Hong
Davis, Diane Craig
Longuski, James M.
Howell, Kathleen C.
Buffington, Brent
TI Saturn Impact Trajectories for Cassini End-of-Mission
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID SMALL SATELLITES
AB Potential end-of-mission scenarios to be considered for the Cassini spacecraft must satisfy planetary quarantine requirements designed to prevent contamination of a pristine environment, which could include Titan and the other Saturnian moons. One assumed acceptable option for safe,disposal of the spacecraft includes Saturn impact trajectories. Two classes of impact trajectories are investigated: short-period orbits characterized by periods of 610 days and long-period orbits with period, greater than 850 days. To impact Saturn with short-period orbits, a series of successive Titan flybys is required to increase inclination and decrease periapsis to within Saturn's atmosphere, while simultaneously avoiding the rings and mitigating Delta V expenditures. To ensure that the spacecraft is not prematurely damaged by material in the rings, Tisser and graphs are employed to determine when the ring-plane crossing distance is within the F-G ring gap: the necessary geometry for the penultimate transfer. For long-period Impact trajectories, solar gravity is exploited to significantly lower periapsis. Depending on the size and orientation or the long-period orbit, a maneuver (<50 m/s) at apoapsis must be added to ensure impact. For sufficiently large orbits with favorable characteristics, solar gravity alone drops the spacecraft's periapsis into Saturn's atmosphere. No maneuver is necessary after the final Titan flyby, providing an attractive "flyby-and-forget" option.
C1 [Yam, Chit Hong; Davis, Diane Craig; Longuski, James M.; Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
[Buffington, Brent] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yam, CH (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, 701 W Stadium Ave, W Lafayette, IN 47907 USA.
EM chithongyam@gmail.com; decraig@purdue.edu; longuski@purdue.edu;
howell@purdue.edu; Brent.Buffington@jpl.nasa.gov
NR 7
TC 8
Z9 10
U1 0
U2 0
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2009
VL 46
IS 2
BP 353
EP 364
DI 10.2514/1.38760
PG 12
WC Engineering, Aerospace
SC Engineering
GA 429EI
UT WOS:000264903200016
ER
PT J
AU Mobrem, M
Adams, DS
AF Mobrem, Mehran
Adams, Douglas S.
TI Deployment Analysis of Lenticular Jointed Antennas Onboard the Mars
Express Spacecraft
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB Extensive analytical and experimental activities were carried out that culminated in successful deployments in May and June of 2005 of three lenticular, jointed booms that formed a first of its kind of ground penetrating radar antenna onboard the Mars Express spacecraft. These activities went well beyond the normal required tasks due to a postlaunch realization that the stowed booms retained at high level of stored energy. This high level of stored energy resulted in an uncontrolled boom deployment rather than predictable boom deployment. Experimentally measured straight section properties and hinge properties were incorporated into specialized modeling techniques that were then used to simulate the boom lenticular joints. System level models were exercised to understand the boom deployment dynamics and spacecraft level implications including spacecraft attitude control and possible entanglement. Discussion includes a comparison of deployment simulation results to measured flight data taken during the three boom deployments. Important parameters that govern lenticular joint behavior are outlined and a short summary of lessons learned and recommendations is included to better understand future applications of this technology.
C1 [Mobrem, Mehran] Northrop Grumman Space Technol Astro Aerosp, Carpinteria, CA 93013 USA.
[Adams, Douglas S.] CALTECH, Jet Prop Lab, Spacecraft Struct & Dynam Grp, Pasadena, CA 91109 USA.
RP Mobrem, M (reprint author), Northrop Grumman Space Technol Astro Aerosp, Carpinteria, CA 93013 USA.
NR 6
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Z9 16
U1 0
U2 3
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2009
VL 46
IS 2
BP 394
EP 402
DI 10.2514/1.36890
PG 9
WC Engineering, Aerospace
SC Engineering
GA 429EI
UT WOS:000264903200020
ER
PT J
AU Adams, DS
Mobrem, M
AF Adams, Douglas S.
Mobrem, Mehran
TI Lenticular Jointed Antenna Deployment Anomaly and Resolution Onboard the
Mars Express Spacecraft
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB During the summer of 2005, ESA deployed a series of three lenticular jointed antenna booms that formed a first-of-its-kind ground-penetrating radar antenna onboard the Mars Express spacecraft. The booms were cacti released from their cradles with a high level of stored energy and allowed to deploy in a chaotic manner with no direct control over their speed or range of motion until their final geometries were achieved. Despite careful preparations, all unforeseen anomaly occurred during the release of the first boom that resulted in a partially deployed state. The flight team was able to determine the boom's intermediate geometry with a high degree of accuracy and to recommend a corrective spacecraft maneuver. This determination, the measured boom properties, and the on-orbit environment that led to the irregularity are discussed, along with file subsequent resolution-of the situation and the ultimately successful deployment. Experience gained from the first boom was used to develop a new spacecraft maneuver that was designed to mitigate the chances of another anomaly occurring during the deployment of the second boom, which took place successfully several week later. These activities are summarized and the resulting flight data are presented for both dipole booms, which demonstrate a fully deployed and healthy antenna.
C1 [Adams, Douglas S.] CALTECH, Jet Prop Lab, Spacecraft Struct & Dynam Grp, Pasadena, CA 91109 USA.
[Mobrem, Mehran] Northrop Grumman Space Technol Astro Aerosp, Carpinteria, CA 93013 USA.
RP Adams, DS (reprint author), CALTECH, Jet Prop Lab, Spacecraft Struct & Dynam Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 5
TC 9
Z9 11
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2009
VL 46
IS 2
BP 403
EP 410
DI 10.2514/1.36891
PG 8
WC Engineering, Aerospace
SC Engineering
GA 429EI
UT WOS:000264903200021
ER
PT J
AU Sullivan, RM
Ghosn, LJ
Lerch, BA
AF Sullivan, Roy M.
Ghosn, Louis J.
Lerch, Bradley A.
TI Application of an Elongated Kelvin Model to Space Shuttle Foams
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID CELLS
AB The space shuttle foams are rigid closed-cell polyurethane foams. The two foams used most extensively on the space shuttle external tank are BX-265 and NCF124-124. Because of-the foaming and rising process, the foam microstructures are elongated In the rise direction. As a result, these two foams exhibit a nonisotropic mechanical behavior. A detailed microstructural characterization of the two foams is presented. Key features of the foam cells are described and the average cell dimensions in the two foams are summarized. Experimental studies are also conducted to measure the room temperature mechanical response of the two foams in the two principal material directions (parallel to the rise and perpendicular to the rise). The measured elastic modulus, proportional limit stress, ultimate tensile strength, and Poisson's ratios are reported. The generalized elongated Kelvin foam model previously developed by the authors is reviewed and the equations which result from this model are summarized. Using the measured microstructural dimensions and the measured stiffness,ratio, the foam tensile strength ratio and Poisson's ratios are predicted for both foams and are compared with the experimental data. The predicted tensile strength ratio is in close agreement with the measured strength ratio for both BX-265 and NCFI124-124. The comparison between the predicted Poisson's ratios and the measured values is not as favorable.
C1 [Sullivan, Roy M.; Lerch, Bradley A.] NASA, John H Glenn Res Ctr, Struct & Mat Div, Mech & Life Predict Branch, Cleveland, OH 44135 USA.
[Ghosn, Louis J.] NASA, John H Glenn Res Ctr, Struct & Mat Div, Ohio Aerosp Inst, Cleveland, OH 44135 USA.
RP Sullivan, RM (reprint author), NASA, John H Glenn Res Ctr, Struct & Mat Div, Mech & Life Predict Branch, 21000 Brookpk Rd,Mail Stop 49-7, Cleveland, OH 44135 USA.
NR 6
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U1 0
U2 1
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2009
VL 46
IS 2
BP 411
EP 418
DI 10.2514/1.37555
PG 8
WC Engineering, Aerospace
SC Engineering
GA 429EI
UT WOS:000264903200022
ER
PT J
AU Oliveira, J
Kirk, DR
Schallhorn, PA
AF Oliveira, Justin
Kirk, Daniel R.
Schallhorn, Paul A.
TI Analytical Model for Cryogenic Stratification in a Rotating and
Reduced-Gravity Environment
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID PROPELLANT STRATIFICATION
AB Modeling the thermal behavior of cryogenic propellants within the upper stages of a launch vehicle is necessary for successful mission planning. During orbital transfer the upper stage may coast for several hours, during which the propellants are heated by solar radiation and undergo thermal stratification. At the end of a coast, the propellant temperature and pressure must he within it narrowly defined range to ensure engine restart. This work develops a thermal stratification model that-includes the thermal conditioning spin of the stage. The model may be used to assess the impact of thermal stratification within propellant tanks over a range of axial accelerations, spin rates, heat fluxes, and tank geometries. The parabolic dishing effect front spinning the tank results In an increased stratum thickness, title to the larger length of the free-convection boundary layer along the tank wall. However, due to the balance between the increased wall-heating area and Increased free-surface area, stratum temperatures may be cooler or warmer, depending oil the spin rate.
C1 [Oliveira, Justin; Kirk, Daniel R.] Florida Inst Technol, Dept Mech & Aerosp Engn, Melbourne, FL 32901 USA.
[Schallhorn, Paul A.] NASA, Environm & Launch Approval Branch, Kennedy Space Ctr, FL 32899 USA.
RP Oliveira, J (reprint author), Florida Inst Technol, Dept Mech & Aerosp Engn, Melbourne, FL 32901 USA.
FU Analex [05001, 06-001]
FX This work was made possible by Analex agreement numbers 05001, and
06-001. The authors also wish to thank Mike Campbell, Sukhdeep Chase,
Martin Margulies, Cindy Fortenberry, and Xiaoyi Li of the NASA John F.
Kennedy Space Center Launch Services Program and Analex Corporation for
their technical input, advice, and highly beneficial suggestions for
improvement to this work.
NR 9
TC 5
Z9 7
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2009
VL 46
IS 2
BP 459
EP 465
PG 7
WC Engineering, Aerospace
SC Engineering
GA 429EI
UT WOS:000264903200027
ER
PT J
AU Berger, KT
Greene, FA
Kimmel, R
Alba, C
Johnson, H
AF Berger, Karen T.
Greene, Frank A.
Kimmel, Roger
Alba, Christopher
Johnson, Heath
TI Aerothermodynamic Testing and Boundary-Layer Trip Sizing of the HIFiRE
Flight 1 Vehicle (vol 45, pg 1117, 2008)
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Correction
ID ROUGHNESS
AB An experimental wind-tunnel test was conducted in the NASA Langley Research Center's 20 in. Mach 6 air tunnel in support of the Hypersonic International Flight Research Experimentation Program. The information in this paper focuses on the flight 1 configuration, the first in a series of flight experiments. The paper documents the experimental measurements made over Reynolds numbers ranging from 2.1 to 5.6 x 10(6)/ft and angles of attack from -5 to +5 deg on several scaled ceramic heat-transfer models of the flight 1 configuration. Global heat transfer was measured using phosphor thermography, and the resulting images and heat-transfer distributions were used to infer the state of the boundary layer (in the vehicle wind- and lee-side surfaces. Boundary-layer trips were used to obtain turbulent heating information, and the experimental data highlighted in this paper were used to size and place the boundary-layer trip for the flight vehicle. The required height of the-flight boundary-layer trip was determined to he 0.079 in., and the trip was moved from the design location of 7.87 to 20.47 in. to ensure that augmented heating would not impact the laminar side of the vehicle. The allowable roughness was selected to be 3.2 x 10(-3) in.
C1 [Berger, Karen T.; Greene, Frank A.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Kimmel, Roger] USAF, Res Lab, Air Vehicles Directorate, Wright Patterson AFB, OH 45433 USA.
[Alba, Christopher; Johnson, Heath] Univ Minnesota, Minneapolis, MN 55455 USA.
RP Berger, KT (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Mail Stop 408A, Hampton, VA 23681 USA.
NR 21
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U1 2
U2 5
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR-APR
PY 2009
VL 46
IS 2
BP 473
EP 480
PG 8
WC Engineering, Aerospace
SC Engineering
GA 429EI
UT WOS:000264903200030
ER
PT J
AU Burnett, J
Smith, SM
Aung, K
Dyer, CB
AF Burnett, J.
Smith, S. M.
Aung, K.
Dyer, C. B.
TI Homocysteine and Cognitive Performance in Elders with Self-Neglect.
SO JOURNAL OF THE AMERICAN GERIATRICS SOCIETY
LA English
DT Meeting Abstract
CT Annual Meeting of the American-Geriatrics-Society
CY APR 29-MAY 02, 2009
CL Chicago, IL
SP Amer Geriatr Soc
C1 [Burnett, J.; Dyer, C. B.] Univ Texas Houston, Hlth Sci Ctr, Div Geriatr & Palliat Med, Houston, TX USA.
[Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasure Div, Houston, TX 77058 USA.
[Aung, K.] Univ Texas Hlth Sci Ctr San Antonio, San Antonio, TX 78229 USA.
[Burnett, J.; Smith, S. M.; Aung, K.; Dyer, C. B.] Consortium Res Elder Self Neglect Texas, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0002-8614
J9 J AM GERIATR SOC
JI J. Am. Geriatr. Soc.
PD MAR
PY 2009
VL 57
SU 1
BP S140
EP S140
PG 1
WC Geriatrics & Gerontology; Gerontology
SC Geriatrics & Gerontology
GA 425BL
UT WOS:000264611900399
ER
PT J
AU Burnett, J
Smith, SM
Aung, K
Dyer, CB
AF Burnett, J.
Smith, S. M.
Aung, K.
Dyer, C. B.
TI Parathyroid Hormone Levels and Cognition.
SO JOURNAL OF THE AMERICAN GERIATRICS SOCIETY
LA English
DT Meeting Abstract
CT Annual Meeting of the American-Geriatrics-Society
CY APR 29-MAY 02, 2009
CL Chicago, IL
SP Amer Geriatr Soc
C1 [Burnett, J.; Dyer, C. B.] Univ Texas Houston, Hlth Sci Ctr, Div Geriatr & Palliat Med, Houston, TX USA.
[Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Human Adaptat & Countermeasure Div, Houston, TX 77058 USA.
[Aung, K.; Dyer, C. B.] Univ Texas Hlth Sci Ctr San Antonio, San Antonio, TX 78229 USA.
[Burnett, J.; Smith, S. M.; Aung, K.] Consortium Res Elder Self Neglect Texas, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0002-8614
J9 J AM GERIATR SOC
JI J. Am. Geriatr. Soc.
PD MAR
PY 2009
VL 57
BP S139
EP S139
PG 1
WC Geriatrics & Gerontology; Gerontology
SC Geriatrics & Gerontology
GA 425BL
UT WOS:000264611900398
ER
PT J
AU Ott, LE
Bacmeister, J
Pawson, S
Pickering, K
Stenchikov, G
Suarez, M
Huntrieser, H
Loewenstein, M
Lopez, J
Xueref-Remy, I
AF Ott, L. E.
Bacmeister, J.
Pawson, S.
Pickering, K.
Stenchikov, G.
Suarez, M.
Huntrieser, H.
Loewenstein, M.
Lopez, J.
Xueref-Remy, I.
TI Analysis of Convective Transport and Parameter Sensitivity in a Single
Column Version of the Goddard Earth Observation System, Version 5,
General Circulation Model
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID STRATOSPHERIC-TROPOSPHERIC EXPERIMENT; CLOUD-RESOLVING MODEL;
LARGE-SCALE MODELS; NUMERICAL SIMULATIONS; ARAKAWA-SCHUBERT; CUMULUS
ENSEMBLE; DEEP CONVECTION; GCSS MODEL; TOGA-COARE; JULY 10
AB Convection strongly influences the distribution of atmospheric trace gases. General circulation models (GCMs) use convective mass fluxes calculated by parameterizations to transport gases, but the results are difficult to compare with trace gas observations because of differences in scale. The high resolution of cloud-resolving models (CRMs) facilitates direct comparison with aircraft observations. Averaged over a sufficient area, CRM results yield a validated product directly comparable to output from a single global model grid column. This study presents comparisons of vertical profiles of convective mass flux and trace gas mixing ratios derived from CRM and single column model (SCM) simulations of storms observed during three field campaigns. In all three cases, SCM simulations underpredicted convective mass flux relative to CRM simulations. As a result, the SCM simulations produced lower trace gas mixing ratios in the upper troposphere in two of the three storms than did the CRM simulations.
The impact of parameter sensitivity in the moist physics schemes employed in the SCM has also been examined. Statistical techniques identified the most significant parameters influencing convective transport. Convective mass fluxes are shown to be strongly dependent on chosen parameter values. Results show that altered parameter settings can substantially improve the comparison between SCM and CRM convective mass flux. Upper tropospheric trace gas mixing ratios were also improved in two storms. In the remaining storm, the SCM representation of CO2 was not improved because of differences in entrainment and detrainment levels in the CRM and SCM simulations.
C1 [Ott, L. E.; Pawson, S.; Suarez, M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Bacmeister, J.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Stenchikov, G.] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA.
[Huntrieser, H.] Deutsch Zentrum Luft & Raumfahrt, Inst Phys Atmosphare, Oberpfaffenhofen, Germany.
[Loewenstein, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lopez, J.] Bay Area Environm Res Inst, Sonoma, CA USA.
[Xueref-Remy, I.] CEA, CNRS, UMR 1572, Inst Pierre Simon Laplace,Lab Sci Climat & Enviro, F-91198 Gif Sur Yvette, France.
RP Ott, LE (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA.
EM lesley.e.ott@nasa.gov
RI Ott, Lesley/E-2250-2012; Pickering, Kenneth/E-6274-2012; Georgiy,
Stenchikov/J-8569-2013; Pawson, Steven/I-1865-2014
OI Pawson, Steven/0000-0003-0200-717X
FU ORAU; NASA's MAP program [NAG5-11276]; National Science Foundation
[ATM9912336, ATM0004120]; European Commission (Research DG)
[ENV4-CT97-0409]
FX Lesley Ott was supported through an ORAU postdoctoral fellowship. SCM
research was funded by NASA's MAP program as part of a study to
understand the distribution and transport of carbon species in the
environment using GEOS-5. We thank Michele Rienecker for her support and
encouragement to perform this research in the GMAO. CRM studies were
supported under National Science Foundation Grants ATM9912336 and
ATM0004120 and NASA Grant NAG5-11276. We thank Wei-Kuo Tao of NASA GSFC
for supplying the 3D GCE model and Alex DeCaria of Millersville
University for assistance with the CSCTM. The EULINOX project was funded
by the European Commission (Research DG) through the Environment and
Climate program (Contract ENV4-CT97-0409). We thank the EULINOX team
that carried out the airborne measurements (Schlager et al., DLR). We
would also like to thank Karsten Baumann for providing observational
data from the STERAO campaign and Yansen Wang, formerly of UMBC/JCET and
currently at the US Army Research Center in Adelphi, MD, for providing
the MM5 simulation of the 3 July CRYSTAL-FACE storm.
NR 54
TC 15
Z9 15
U1 0
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD MAR
PY 2009
VL 66
IS 3
BP 627
EP 646
DI 10.1175/2008JAS2694.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 426BB
UT WOS:000264681300004
ER
PT J
AU Paoli, R
Shariff, K
AF Paoli, Roberto
Shariff, Karim
TI Turbulent Condensation of Droplets: Direct Simulation and a Stochastic
Model
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID DIRECT NUMERICAL SIMULATIONS; ISOTROPIC TURBULENCE; MICROSCOPIC
APPROACH; PART II; GROWTH; CLOUDS; SCALAR
AB The effect of turbulent mixing on droplet condensation is studied via direct numerical simulations of a population of droplets in a periodic box of homogeneous isotropic turbulence. Each droplet is tracked as a fluid particle whose radius grows by condensation of water vapor. Forcing of the small wavenumbers is used to sustain velocity, vapor, and temperature fluctuations. Temperature and vapor fluctuations lead to supersaturation fluctuations, which are responsible for broadening the droplet size distribution in qualitative agreement with in situ measurements. A model for the condensation of a population of cloud droplets in a homogeneous turbulent flow is presented. The model consists of a set of Langevin (stochastic) equations for the droplet area, supersaturation, and temperature surrounding the droplets. These equations yield corresponding ordinary differential equations for various moments and correlations. The statistics predicted by the model, for instance, the droplet area-supersaturation correlation, reproduce the simulations well.
C1 [Paoli, Roberto] European Ctr Res & Adv Training Sci Computat, Toulouse, France.
[Paoli, Roberto] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA.
[Shariff, Karim] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Paoli, R (reprint author), CERFACS, 42 Ave Gaspard Coriolis, F-31057 Toulouse 1, France.
EM paoli@cerfacs.fr
OI Shariff, Karim/0000-0002-7256-2497
NR 30
TC 8
Z9 8
U1 0
U2 4
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 MAR
PY 2009
VL 66
IS 3
BP 723
EP 740
DI 10.1175/2008JAS2734.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 426BB
UT WOS:000264681300009
ER
PT J
AU Iguchi, T
Kozu, T
Kwiatkowski, J
Meneghini, R
Awaka, J
Okamoto, K
AF Iguchi, Toshio
Kozu, Toshiaki
Kwiatkowski, John
Meneghini, Robert
Awaka, Jun
Okamoto, Ken'ichi
TI Uncertainties in the Rain Profiling Algorithm for the TRMM Precipitation
Radar
SO JOURNAL OF THE METEOROLOGICAL SOCIETY OF JAPAN
LA English
DT Article
ID SURFACE REFERENCE TECHNIQUE; ATTENUATION; AIRBORNE
AB This paper describes the basic structure and flow of the rain profiling algorithm for the TRMM Precipitation Radar, and discusses the major assumptions and sources of error in the algorithm. In particular, it describes how the uncertainties in individual parameters affect the attenuation correction and rain estimates. Major parameters involved are the drop size distribution, the phase state of precipitating particles, their density and shape, inhomogeneity of precipitation distribution within the footprint, attenuation due to cloud liquid water and water vapor, freezing height, uncertainty of the surface scattering cross section, and fluctuation of the radar echo signal. Among these parameters that affect the rain estimates, the effect of inhomogeneity of rain distribution is summarized in detail. The paper also describes how these parameters are taken into account in different versions of the standard algorithm 2A25.
C1 [Iguchi, Toshio] Natl Inst Informat & Commun Technol, Appl Electromagnet Res Ctr, Koganei, Tokyo 1848795, Japan.
[Kozu, Toshiaki] Shimane Univ, Matsue, Shimane, Japan.
[Kwiatkowski, John] George Mason Univ, Fairfax, VA 22030 USA.
[Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Awaka, Jun] Tokai Univ, Dept Marine Biol & Sci, Sapporo, Hokkaido, Japan.
[Okamoto, Ken'ichi] Tottori Univ Environm Studies, Tottori, Japan.
RP Iguchi, T (reprint author), Natl Inst Informat & Commun Technol, Appl Electromagnet Res Ctr, 4-2-1 Nukui Kitamachi, Koganei, Tokyo 1848795, Japan.
EM iguchi@nict.go.jp
RI PMM, JAXA/K-8537-2016
NR 17
TC 141
Z9 144
U1 2
U2 17
PU METEOROLOGICAL SOC JAPAN
PI TOKYO
PA C/O JAPAN METEOROLOGICAL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO,
100-0004, JAPAN
SN 0026-1165
EI 2186-9057
J9 J METEOROL SOC JPN
JI J. Meteorol. Soc. Jpn.
PD MAR
PY 2009
VL 87A
SI SI
BP 1
EP 30
DI 10.2151/jmsj.87A.1
PG 30
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 467CK
UT WOS:000267713900002
ER
PT J
AU Liao, L
Meneghini, R
AF Liao, Liang
Meneghini, Robert
TI Changes in the TRMM Version-5 and Version-6 Precipitation Radar Products
Due to Orbit Boost
SO JOURNAL OF THE METEOROLOGICAL SOCIETY OF JAPAN
LA English
DT Article
ID MEASURING MISSION TRMM; GROUND-BASED RADAR; RAINFALL; VALIDATION;
SATELLITE; WSR-88D; SIZE; ATTENUATION; KWAJALEIN; SHAPE
AB The performance of the version-5 and version-6 Tropical Rainfall Measuring Mission (TRMM) Precipitation Radar (PR) products before and after the satellite orbit boost is assessed through a series of comparisons with Weather Surveillance Radar (WSR)-88D ground-based radar in Melbourne, Florida. Analysis of the comparisons of radar reflectivity near the storm top from the ground radar and both versions of the PR indicates that the PR bias relative to the WSR radar at Melbourne is on the order of I dB for both pre- and post-boost periods, indicating that the PR products maintain accurate calibration after the orbit boost. Comparisons with the WSR-88D near-surface reflectivity factors indicate that both versions of the PR products accurately correct for attenuation in stratiform rain. However, in convective rain, both versions exhibit negative biases in the near-surface radar reflectivity with version-6 products having larger negative biases than version-5. Rain rate comparisons between the ground and space radars show similar characteristics.
C1 [Liao, Liang] Goddard Earth Sci & Technol Ctr UMBC, Greenbelt, MD USA.
[Meneghini, Robert] NASA, GSFC, Greenbelt, MD 20771 USA.
RP Liao, L (reprint author), NASA, Goddard Space Flight Ctr, Goddard Earth Sci & Technol UMBC, Code 613-1, Greenbelt, MD 20771 USA.
EM Liang.Liao-1@nasa.gov
FU NASA!s Precipitation Measurement Mission (PMM) [NNH06ZDA001N-PMM]
FX We wish to thank David Wolff, David Marks, and the Goddard Space Flight
Center TRMM office for providing ground-based WSR data. This work is
supported by Dr. R. Kakar of NASA Headquarters under NASA!s
Precipitation Measurement Mission (PMM) grant NNH06ZDA001N-PMM.
NR 30
TC 16
Z9 19
U1 0
U2 2
PU METEOROLOGICAL SOC JAPAN
PI TOKYO
PA C/O JAPAN METEOROLOGICAL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO,
100-0004, JAPAN
SN 0026-1165
EI 2186-9057
J9 J METEOROL SOC JPN
JI J. Meteorol. Soc. Jpn.
PD MAR
PY 2009
VL 87A
SI SI
BP 93
EP 107
DI 10.2151/jmsj.87A.93
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 467CK
UT WOS:000267713900007
ER
PT J
AU Amitai, E
Llort, X
Sempere-Torres, D
AF Amitai, E.
Llort, X.
Sempere-Torres, D.
TI Comparison of TRMM Radar Rainfall Estimates with NOAA Next-Generation
QPE
SO JOURNAL OF THE METEOROLOGICAL SOCIETY OF JAPAN
LA English
DT Article
ID PRECIPITATION RADAR; ALGORITHM; WSR-88D
AB Rainfall rate fields based on TRMM spaceborne radar observations are compared to those based on the new NOAA Next-Generation Quantitative Precipitation Estimation (QPE) high-resolution national mosaic product (Q2). These rainfall fields can be considered as radar products with the largest coverage currently available from space and ground-based radar observations. They probably can also be considered as the most advanced radar rainfall rate products covering a large area. How well do these two products agree? While the accumulated rain rates from all overpasses combined differ by less than 10%, a comparison between the satellite and ground radar probability distribution functions (pdfs) of the instantaneous rain rate shows very large discrepancies. In general, systematic anomalies over the continental U.S. in TRMM radar pdfs compared to the ground-radar pdfs can be recognized. The pdfs of the TRMM radar are generally shifted towards lower rain rates. Moreover, double peaks occur more frequently in the Q2 than in the TRMM radar pdf. Initial results from the comparisons between these two advanced products are presented.
C1 [Amitai, E.] Chapman Univ, Schmid Coll Sci, Orange, CA 92866 USA.
[Amitai, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Llort, X.; Sempere-Torres, D.] Univ Politecn Cataluna, GRAHI, Barcelona, Spain.
RP Amitai, E (reprint author), Chapman Univ, Schmid Coll Sci, 1 Univ Dr, Orange, CA 92866 USA.
EM amitai@chapman.edu
OI Sempere-Torres, Daniel/0000-0002-6378-0337
FU NASXs Precipitation Measurement Missions Project [NNX07AK47G]; Spanish
MICINN [ESP2007-62417]
FX Funding for the first author is from NASXs Precipitation Measurement
Missions Project through grant #NNX07AK47G. Funding for the second and
third authors comes from the Spanish MICINN-Project ESP2007-62417. TRMM
data were provided by NASA Precipitation Processing System (PPS/TSDIS),
headed by Erich Stocker of the Goddard Space Flight Center. Q2 data were
provided by NOAA NSSL's Hydrometeorological Research Group (HMRG).
Special thanks to HMRG leader Kenneth Howard, Steven Vasiloff, and Jian
Zhang. The authors wish to thank Robert Meneghini of the NASA Goddard
Space Flight Center for his helpful comments.
NR 9
TC 24
Z9 24
U1 0
U2 2
PU METEOROLOGICAL SOC JAPAN
PI TOKYO
PA C/O JAPAN METEOROLOGICAL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO,
100-0004, JAPAN
SN 0026-1165
EI 2186-9057
J9 J METEOROL SOC JPN
JI J. Meteorol. Soc. Jpn.
PD MAR
PY 2009
VL 87A
SI SI
BP 109
EP 118
DI 10.2151/jmsj.87A.109
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 467CK
UT WOS:000267713900008
ER
PT J
AU Wang, NY
Liu, CT
Ferraro, R
Wolff, D
Zipser, E
Kummerow, C
AF Wang, Nai-Yu
Liu, Chuntao
Ferraro, Ralph
Wolff, Dave
Zipser, Ed
Kummerow, Chris
TI TRMM 2A12 Land Precipitation Product - Status and Future Plans
SO JOURNAL OF THE METEOROLOGICAL SOCIETY OF JAPAN
LA English
DT Article
ID RAIN-PROFILING ALGORITHM; SENSOR MICROWAVE IMAGER; MEASURING MISSION
TRMM; PASSIVE MICROWAVE; BRIGHTNESS TEMPERATURES; RETRIEVAL ALGORITHMS;
GROUND VALIDATION; COMBINED RADAR; SATELLITE; ICE
AB The Tropical Rainfall Measuring Mission (TRMM) Microwave Imager (TMI) 2A12 product consists of unique components configured for land and oceanic precipitation retrievals. This design was based on the vastly different physical characteristics of the retrieval, involving primarily emission over ocean and entirely scattering over land. This paper describes the current status of the TRMM Version 6 (V6) 2A12 product over land and envisioned improvements for TRMM TMI V7 and GPM GMI VI.
On a global scale, the 2A12 land algorithm exhibits biases when compared with the TRMM 2A25 (Precipitation Radar (PR) based) and rain gauges. These range from 6 percent for GPCC to 20 percent for 2A25. Closer comparison also reveals regional and seasonal biases, with the largest positive biases found in warm-season convective zones and over semi-arid regions. Some negative biases are found in warm-rain precipitation regimes where scattering at 85 GHz is unable to detect a precipitation signal. On an instantaneous time scale, 2A12 land also produces a positive bias when compared with high-quality radar data from Melbourne, Florida, a TRMM ground validation site. The largest discrepancies occur for rain rates of less than 2 mm h(-1).
A number of known "anomalies" are highlighted, including overestimation of rainfall in deep convective systems, underestimation in warm-rain regimes, and a number of features associated with the screening component of the algorithm (e.g., snow cover, deserts, etc.).
Future improvements for TRMM TMI V7 are described and include the use of ancillary data to determine the underlying surface characteristics and the development of improved brightness-temperature to rain-rate relationships with a more robust data set of TMI and PR matchups, stratified by atmospheric parameters (i.e., surface temperature, atmospheric moisture, etc.) obtained from Numerical Weather Prediction (NWP) model fields. Finally, the promise of an improved land algorithm through the use of high-frequency microwave measurements is described. This will form the basis for the Global Precipitation Measurement (GPM) Global Microwave Imager (GMI) VI algorithm.
C1 [Wang, Nai-Yu] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Liu, Chuntao; Zipser, Ed] Univ Utah, Dept Meteorol, Salt Lake City, UT 84112 USA.
[Ferraro, Ralph] NOAA NESDIS, College Pk, MD USA.
[Wolff, Dave] NASA GSFC, Greenbelt, MD USA.
[Kummerow, Chris] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
RP Wang, NY (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM Nai-Yu.Wang@noaa.gov
RI Ferraro, Ralph/F-5587-2010; Wang, Nai-Yu/E-5303-2016; Measurement,
Global/C-4698-2015
OI Ferraro, Ralph/0000-0002-8393-7135;
FU NASA; NOAA
FX The authors would like to thank our colleagues on the National
Aeronautics and Space Administration (NASA) Precipitation Measurement
Missions' Science Team for their collaboration over the past several
years. We are also grateful for the support we received from NASA (R.
Kakar) and NOAA (G. Dittberner and C. Miller). In addition, we would
like to thank the Climate Rainfall Data Center at Colorado State
University for the use of the data provided in Figs. 2 and 3. This work
was partially supported through a grant between NOAA and the University
of Maryland/ Cooperative Institute for Climate Studies.
NR 51
TC 50
Z9 50
U1 0
U2 7
PU METEOROLOGICAL SOC JAPAN
PI TOKYO
PA C/O JAPAN METEOROLOGICAL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO,
100-0004, JAPAN
SN 0026-1165
EI 2186-9057
J9 J METEOROL SOC JPN
JI J. Meteorol. Soc. Jpn.
PD MAR
PY 2009
VL 87A
SI SI
BP 237
EP 253
DI 10.2151/jmsj.87A.237
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 467CK
UT WOS:000267713900016
ER
PT J
AU Adler, RF
Wang, JJ
Gu, GJ
Huffman, GJ
AF Adler, Robert F.
Wang, Jian-Jian
Gu, Guojun
Huffman, George J.
TI A Ten-Year Tropical Rainfall Climatology Based on a Composite of TRMM
Products
SO JOURNAL OF THE METEOROLOGICAL SOCIETY OF JAPAN
LA English
DT Article
ID MEASURING MISSION TRMM; GLOBAL PRECIPITATION; PROFILING ALGORITHM;
MICROWAVE IMAGER; RADAR
AB A new climatology of tropical surface rain is described based on a composite of ten years of precipitation retrievals and analyses from the Tropical Rainfall Measuring Mission (TRMM). This TRMM Composite Climatology (TCC) consists of a combination of selected TRMM rainfall products over both land and ocean. This new climatology will be useful as a summary of surface rain estimates from TRMM (not replacing the individual products) and should be useful as a ready comparison with other non-TRMM estimates and for comparison with calculated precipitation from general circulation models.
The TCC mean precipitation for each calendar month and for the annual total is determined by a simple mean of the three chosen products (slightly different combination of products over land and ocean). Over ocean areas, the three TRMM products are those based on the passive microwave (2A12), radar (2A25) and combined retrievals (2B31). Over land, the multi-satellite product (3B43) is substituted for the passive microwave product. The standard deviation (sigma) at each point among the three estimates gives a measure of dispersion, which can be used as an indicator of confidence and as an estimate of error. The mean annual precipitation over the TRMM domain of 35 degrees N to 35 degrees S in the new climatology is 2.68 mm d(-1) (ocean and land combined) with a sigma of .05 mm d(-1), or 2.0%. The ocean (land) value is 2.74 mm d(-1) (2.54) with a sigma/mean of 2.1% (5.4%). The larger dispersion (and assumed error) over land is due to the greater difficulty of satellite rain retrieval over land, especially with passive microwave techniques and especially in mountains and along coasts. The maps of sigma and sigma/mean indicate these regions of less confidence, including areas over the ocean such as the eastern Pacific Ocean.
Examples of values for different latitude bands, seasonal variations, and relations of the individual inputs to the composite mean are given. Comparison with analyses from the Global Precipitation Climatology Project (GPCP) indicates lower values than GPCP for the TRMM composite in middle latitudes over the ocean and over northern Australia and India during their respective summer monsoons.
C1 [Adler, Robert F.; Wang, Jian-Jian; Gu, Guojun; Huffman, George J.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Adler, Robert F.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Wang, Jian-Jian; Gu, Guojun] Univ Maryland, Goddard Ctr Earth Sci & Technol, Baltimore, MD USA.
[Huffman, George J.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Adler, RF (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 661, Greenbelt, MD 20771 USA.
EM Robert.F.Adler@nasa.gov
RI Huffman, George/F-4494-2014
OI Huffman, George/0000-0003-3858-8308
FU NASA's Precipitation Measurement Missions (PMM) program
FX The authors wish to thank all the TRMM science investigators who have
developed the TRMM algorithms and all the people who have so capably
processed the TRMM data to produce the products used in this study. This
research has been supported by funding from NASA's Precipitation
Measurement Missions (PMM) program, headed by Dr. Ramesh Kakar.
NR 21
TC 21
Z9 21
U1 0
U2 10
PU METEOROLOGICAL SOC JAPAN
PI TOKYO
PA C/O JAPAN METEOROLOGICAL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO,
100-0004, JAPAN
SN 0026-1165
EI 2186-9057
J9 J METEOROL SOC JPN
JI J. Meteorol. Soc. Jpn.
PD MAR
PY 2009
VL 87A
SI SI
BP 281
EP 293
DI 10.2151/jmsj.87A.281
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 467CK
UT WOS:000267713900019
ER
PT J
AU Weisberg, MK
Smith, C
Benedix, G
Folco, L
Righter, K
Zipfel, J
Yamaguchi, A
Aoudjehane, HC
AF Weisberg, Michael K.
Smith, Caroline
Benedix, Gretchen
Folco, Luigi
Righter, Kevin
Zipfel, Jutta
Yamaguchi, Akira
Aoudjehane, Hasnaa Chennaoui
TI The Meteoritical Bulletin, No. 95
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
AB The Meteoritical Bulletin No. 95 reports 1093 (282 non-Antarctic and 801 Antarctic) newly approved meteorite names and their recovery histories. macroscopic descriptions, petrography mineral compositions and geochemistry. Meteorites reported include lunar meteorites, eucrites, mesosiderites, angrites, ureilites, an acapulcoite, and H, L, LL, R, CO, CM, CK and CV chondrites. Three new falls, the Bunburra Rockhole (Australia) eucrite and the recent (Nov., 2008) Buzzard Coulee (Canada) H4 chondrite, and Tamdakht (Morocco) H5 chondrite are reported.
C1 [Weisberg, Michael K.] Kingsborough Community Coll, Dept Phys Sci, Brooklyn, NY 11235 USA.
[Weisberg, Michael K.] CUNY, Grad Sch, Brooklyn, NY 11235 USA.
[Weisberg, Michael K.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA.
[Smith, Caroline; Benedix, Gretchen] Nat Hist Museum, Dept Mineral, London SW7 5BD, England.
[Smith, Caroline] Univ Glasgow, Sch Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland.
[Folco, Luigi] Univ Siena, Museo Nazl Antartide, I-53100 Siena, Italy.
[Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Zipfel, Jutta] Forschungsinst & Nat Museum Senckenberg, Sekt Meteoritenforsch, D-60325 Frankfurt, Germany.
[Yamaguchi, Akira] Natl Inst Polar Res, Antarctic Meteorite Res Ctr, Itabashi Ku, Tokyo 1738515, Japan.
[Aoudjehane, Hasnaa Chennaoui] Univ Hassan II Casablanca, Fac Sci, Dept Geol, Casablanca, Morocco.
RP Weisberg, MK (reprint author), Kingsborough Community Coll, Dept Phys Sci, 2001 Orienta Blvd, Brooklyn, NY 11235 USA.
EM meteorite@kingsborough.edu
OI Benedix, Gretchen/0000-0003-0990-8878
NR 3
TC 14
Z9 14
U1 3
U2 13
PU METEORITICAL SOC
PI FAYETTEVILLE
PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD MAR
PY 2009
VL 44
IS 3
BP 429
EP 462
PG 34
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 445EM
UT WOS:000266032600007
ER
PT J
AU Carvalho, P
Rocha, G
Hobson, MP
AF Carvalho, Pedro
Rocha, Graca
Hobson, M. P.
TI A fast Bayesian approach to discrete object detection in astronomical
data sets - PowellSnakes I
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; cosmic microwave background; cosmology:
observations
ID SOURCE EXTRACTION; CLUSTERS; MAPS
AB A new fast Bayesian approach is introduced for the detection of discrete objects immersed in a diffuse background. This new method, called PowellSnakes, speeds up traditional Bayesian techniques by (i) replacing the standard form of the likelihood for the parameters characterizing the discrete objects by an alternative exact form that is much quicker to evaluate; (ii) using a simultaneous multiple minimization code based on Powell's direction set algorithm to locate rapidly the local maxima in the posterior and (iii) deciding whether each located posterior peak corresponds to a real object by performing a Bayesian model selection using an approximate evidence value based on a local Gaussian approximation to the peak. The construction of this Gaussian approximation also provides the covariance matrix of the uncertainties in the derived parameter values for the object in question. This new approach provides a speed up in performance by a factor of '100' as compared to existing Bayesian source extraction methods that use Monte Carlo Markov chain to explore the parameter space, such as that presented by Hobson & McLachlan. The method can be implemented in either real or Fourier space. In the case of objects embedded in a homogeneous random field, working in Fourier space provides a further speed up that takes advantage of the fact that the correlation matrix of the background is circulant. We illustrate the capabilities of the method by applying to some simplified toy models. Furthermore, PowellSnakes has the advantage of consistently defining the threshold for acceptance/rejection based on priors which cannot be said of the frequentist methods. We present here the first implementation of this technique (version I). Further improvements to this implementation are currently under investigation and will be published shortly. The application of the method to realistic simulated Planck observations will be presented in a forthcoming publication.
C1 [Carvalho, Pedro; Hobson, M. P.] Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
[Rocha, Graca] IPAC, Pasadena, CA 91125 USA.
[Rocha, Graca] JPL, Pasadena, CA 91109 USA.
RP Carvalho, P (reprint author), Cavendish Lab, Astrophys Grp, J J Thomson Ave, Cambridge CB3 0HE, England.
EM carvalho@mrao.cam.ac.uk; graca@caltech.edu; mph@mrao.cam.ac.uk
FU Cavendish Astrophysics Group of the University of Cambridge; NASA
Science Mission Directorate
FX PC thanks the Cavendish Astrophysics Group of the University of
Cambridge for support and hospitality during the progression of this
work. GR acknowledges support from the US Planck Project, which is
funded by the NASA Science Mission Directorate. GR would like to
acknowledge useful discussions with Krzystof Gorsky and Charles
Lawrence.
NR 18
TC 52
Z9 52
U1 0
U2 0
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2009
VL 393
IS 3
BP 681
EP 702
DI 10.1111/j.1365-2966.2008.14016.x
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 407JL
UT WOS:000263359300001
ER
PT J
AU Hardcastle, MJ
Cheung, CC
Feain, IJ
Stawarz, L
AF Hardcastle, M. J.
Cheung, C. C.
Feain, I. J.
Stawarz, L.
TI High-energy particle acceleration and production of ultra-high-energy
cosmic rays in the giant lobes of Centaurus A
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE acceleration of particles; cosmic rays; galaxies: jets; radio continuum:
galaxies
ID ACTIVE GALACTIC NUCLEI; RADIO GALAXY CENTAURUS; EXTRAGALACTIC BACKGROUND
LIGHT; MAGNETIC-FIELD STRENGTHS; PROBE WMAP OBSERVATIONS; X-RAY;
CONTINUUM SPECTRUM; DYNAMICAL MODELS; GAMMA-RAYS; BLACK-HOLE
AB The nearby radio galaxy Centaurus A is poorly studied at high frequencies with conventionals radio telescope because of its very large angular size, but is one of a very few extragalactic objects to be detected and resolved by the Wilkinson Microwave Anisotropy Probe (WMAP). We have used the five-year WMAP data for Cen A to constrain the high-frequency radio spectra of the 10 degrees giant lobes and to search for spectral changes as a function of position along the lobes. We show that the high-frequency radio spectra of the northern and southern giant lobes are significantly different: the spectrum of the southern lobe steepens monotonically (and is steeper further from the active nucleus) whereas the spectrum of the northern lobe remains consistent with a power law. The inferred differences in the northern and southern giant lobes may be the result of real differences in their high-energy particle acceleration histories, perhaps due to the influence of the northern middle lobe, an intermediate-scale feature which has no detectable southern counterpart. In light of these results, we discuss the prospects for Fermi Gamma-ray Space Telescope detections of inverse-Compton emission from the giant lobes and the lobes' possible role in the production of the ultra-high-energy cosmic rays (UHECR) detected by the Pierre Auger Observatory. We show that the possibility of a Fermi detection depends sensitively on the physical conditions in the giant lobes, with the northern lobe more likely to be detected, and that any emission observed by Fermi is likely to be dominated by photons at the soft end of the Fermi energy band. On the other hand, we argue that the estimated conditions in the giant lobes imply that UHECRs can be accelerated there, with a potentially detectable. gamma-ray signature at TeV energies.
C1 [Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England.
[Cheung, C. C.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Feain, I. J.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Stawarz, L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Stawarz, L.] Uniwersytet Jagiellonski, Obserwatorium Astron, PL-30244 Krakow, Poland.
RP Hardcastle, MJ (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England.
EM m.j.hardcastle@herts.ac.uk
RI Hardcastle, Martin/E-2264-2012
OI Hardcastle, Martin/0000-0003-4223-1117
FU Royal Society; NASA Postdoctoral Program at Goddard Space Flight Center;
NASA; MEiN [1-P03D-003-29]
FX MJH thanks the Royal Society for a research fellowship. CCC is supported
by an appointment to the NASA Postdoctoral Program at Goddard Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA. LS acknowledges support by MEiN grant
1-P03D-003-29. We thank Nils Odegard for providing the WMAP data,
Norbert Junkes for providing us with radio data from ground-based
observations of CenA, Matthieu Renard for helpful discussions of the
detectability of the Cen A lobes with coded-mask high-energy
instruments, Gustavo Romero and Sergey Troitsky for helpful comments on
the initial version of the paper, Daniel Mazin and Martin Raue for
providing us with data on the EBL spectral energy density, and an
anonymous referee for valuable comments which have allowed us to make
significant improvements to the paper. This research has made use of the
NASA/IPAC Extragalactic Data base (NED) which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
NR 82
TC 73
Z9 73
U1 0
U2 5
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2009
VL 393
IS 3
BP 1041
EP 1053
DI 10.1111/j.1365-2966.2008.14265.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 407JL
UT WOS:000263359300027
ER
PT J
AU Han, M
Braun, SA
Persson, POG
Bao, JW
AF Han, Mei
Braun, Scott A.
Persson, P. Ola G.
Bao, Jian-Wen
TI Alongfront Variability of Precipitation Associated with a Midlatitude
Frontal Zone: TRMM Observations and MM5 Simulation
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID MOIST SYMMETRIC STABILITY; PART I; LIGHTNING CHARACTERISTICS;
EXTRATROPICAL CYCLONES; MESOSCALE RAINBANDS; HURRICANE EYEWALLS; WINTER
CYCLONES; ICE SCATTERING; UNITED-STATES; CLOUD MODEL
AB On 19 February 2001, the Tropical Rainfall Measuring Mission (TRMM) satellite observed complex alongfront variability in the precipitation structure of an intense cold-frontal rainband. The TRMM Microwave Imager brightness temperatures suggested that, compared to the northern and southern ends of the rainband, a greater amount of precipitation ice was concentrated in the middle portion of the rainband where the front bowed out. A model simulation conducted using the fifth-generation Pennsylvania State University-National Center for Atmospheric Research (PSU-NCAR) Mesoscale Model (MM5) is examined to explain the distribution of precipitation associated with the cold-frontal rainband. The simulation reveals that the enhanced precipitation ice production and the implied mean ascent along the central part of the front were associated with a synergistic interaction between a low-level front and an upper-level front associated with an intrusion of high-PV stratospheric air. The low-level front contributed to an intense bow-shaped narrow cold-frontal rainband (NCFR). The upper-level front was dynamically active only along the central to northern portion of the NCFR, where the upper-level PV advection and Q-vector convergence were most prominent. The enhanced mean ascent associated with the upper-level front contributed to a wide cold-frontal rainband (WCFR) that trailed or overlapped with the NCFR along its central to northern segments. Because of the combination of the forcing from both lower- and upper-level fronts, the ascent was deepest and most intense along the central portion of the front. Thus, a large concentration of precipitation ice, attributed to both the NCFR and WCFR, was produced.
C1 [Han, Mei; Braun, Scott A.] NASA, Mesoscale Atmospher Proc Branch, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Han, Mei] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Persson, P. Ola G.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Persson, P. Ola G.; Bao, Jian-Wen] NOAA, Environm Technol Lab, Boulder, CO USA.
RP Han, M (reprint author), NASA, Mesoscale Atmospher Proc Branch, Atmospheres Lab, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD 20771 USA.
EM mei.han-1@nasa.gov
RI Han, Mei/H-2344-2012
FU NASA Headquarters
FX The authors gratefully thank two anonymous reviewers and the editor, Dr.
James D. Doyle, for their valuable comments, which led to significant
improvements of the paper. This work was supported by Dr. Ramesh Kakar
at NASA Headquarters with funds from the NASA Precipitation Measurement
Mission science program.
NR 46
TC 4
Z9 4
U1 0
U2 1
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD MAR
PY 2009
VL 137
IS 3
BP 1008
EP 1028
DI 10.1175/2008MWR2465.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 435TS
UT WOS:000265366800013
ER
PT J
AU Ackerman, AS
Vanzanten, MC
Stevens, B
Savic-Jovcic, V
Bretherton, CS
Chlond, A
Golaz, JC
Jiang, HL
Khairoutdinov, M
Krueger, SK
Lewellen, DC
Lock, A
Moeng, CH
Nakamura, K
Petters, MD
Snider, JR
Weinbrecht, S
Zulauf, M
AF Ackerman, Andrew S.
vanZanten, Margreet C.
Stevens, Bjorn
Savic-Jovcic, Verica
Bretherton, Christopher S.
Chlond, Andreas
Golaz, Jean-Christophe
Jiang, Hongli
Khairoutdinov, Marat
Krueger, Steven K.
Lewellen, David C.
Lock, Adrian
Moeng, Chin-Hoh
Nakamura, Kozo
Petters, Markus D.
Snider, Jefferson R.
Weinbrecht, Sonja
Zulauf, Mike
TI Large-Eddy Simulations of a Drizzling, Stratocumulus-Topped Marine
Boundary Layer
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID ICE-PHASE MICROPHYSICS; CLOUD MICROPHYSICS; SHIP TRACKS; STOCHASTIC
BACKSCATTER; NUMERICAL-SIMULATION; STRATIFORM CLOUDS; MODEL DESCRIPTION;
PART I; PARAMETERIZATION; ENTRAINMENT
AB Cloud water sedimentation and drizzle in a stratocumulus-topped boundary layer are the focus of an intercomparison of large-eddy simulations. The context is an idealized case study of nocturnal stratocumulus under a dry inversion, with embedded pockets of heavily drizzling open cellular convection. Results from 11 groups are used. Two models resolve the size distributions of cloud particles, and the others parameterize cloud water sedimentation and drizzle. For the ensemble of simulations with drizzle and cloud water sedimentation, the mean liquid water path (LWP) is remarkably steady and consistent with the measurements, the mean entrainment rate is at the low end of the measured range, and the ensemble-average maximum vertical wind variance is roughly half that measured. On average, precipitation at the surface and at cloud base is smaller, and the rate of precipitation evaporation greater, than measured. Including drizzle in the simulations reduces convective intensity, increases boundary layer stratification, and decreases LWP for nearly all models. Including cloud water sedimentation substantially decreases entrainment, decreases convective intensity, and increases LWP for most models. In nearly all cases, LWP responds more strongly to cloud water sedimentation than to drizzle. The omission of cloud water sedimentation in simulations is strongly discouraged, regardless of whether or not precipitation is present below cloud base.
C1 [Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[vanZanten, Margreet C.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
[Stevens, Bjorn; Savic-Jovcic, Verica] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Bretherton, Christopher S.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Chlond, Andreas] Max Planck Inst Meteorol, Hamburg, Germany.
[Golaz, Jean-Christophe] NOAA, Geophys Fluid Dynam Lab, UCAR Visiting Scientist Program, Princeton, NJ USA.
[Jiang, Hongli] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Khairoutdinov, Marat] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
[Krueger, Steven K.; Zulauf, Mike] Univ Utah, Dept Meteorol, Salt Lake City, UT 84112 USA.
[Lewellen, David C.] W Virginia Univ, MAE Dept, Morgantown, WV 26506 USA.
[Lock, Adrian] Met Off, Exeter, Devon, England.
[Moeng, Chin-Hoh] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Nakamura, Kozo] Japan Agcy Marine Earth Sci & Technol, Frontier Res Ctr Global Change, Yokohama, Japan.
[Petters, Markus D.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Snider, Jefferson R.] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
[Weinbrecht, Sonja] Univ Reading, Dept Meteorol, Reading, Berks, England.
RP Ackerman, AS (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM andrew.ackerman@nasa.gov
RI Petters, Markus/D-2144-2009; Ackerman, Andrew/D-4433-2012; Stevens,
Bjorn/A-1757-2013; Golaz, Jean-Christophe/D-5007-2014; Jiang,
Hongli/N-3281-2014; Snider, Jefferson/F-9175-2016
OI Petters, Markus/0000-0002-4082-1693; Ackerman,
Andrew/0000-0003-0254-6253; Stevens, Bjorn/0000-0003-3795-0475; Golaz,
Jean-Christophe/0000-0003-1616-5435; Snider,
Jefferson/0000-0002-9318-1343
NR 75
TC 95
Z9 95
U1 1
U2 21
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD MAR
PY 2009
VL 137
IS 3
BP 1083
EP 1110
DI 10.1175/2008MWR2582.1
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 435TS
UT WOS:000265366800017
ER
PT J
AU Remer, LA
AF Remer, Lorraine A.
TI ATMOSPHERIC SCIENCE Smoke above clouds
SO NATURE GEOSCIENCE
LA English
DT News Item
ID AEROSOLS
C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
RP Remer, LA (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-2, Greenbelt, MD 20771 USA.
EM Lorraine.a.remer@nasa.gov
NR 10
TC 2
Z9 2
U1 2
U2 4
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD MAR
PY 2009
VL 2
IS 3
BP 167
EP 168
DI 10.1038/ngeo456
PG 2
WC Geosciences, Multidisciplinary
SC Geology
GA 420KY
UT WOS:000264289900010
ER
PT J
AU Chand, D
Wood, R
Anderson, TL
Satheesh, SK
Charlson, RJ
AF Chand, D.
Wood, R.
Anderson, T. L.
Satheesh, S. K.
Charlson, R. J.
TI Satellite-derived direct radiative effect of aerosols dependent on cloud
cover
SO NATURE GEOSCIENCE
LA English
DT Article
ID ATMOSPHERIC CHEMISTRY; OPTICAL-PROPERTIES; BLACK CARBON; SAFARI 2000;
CLIMATE; MODIS; OCEAN; SMOKE
AB Aerosols from biomass burning can alter the radiative balance of the Earth by reflecting and absorbing solar radiation(1). Whether aerosols exert a net cooling or a net warming effect will depend on the aerosol type and the albedo of the underlying surface(2). Here, we use a satellite-based approach to quantify the direct, top-of-atmosphere radiative effect of aerosol layers advected over the partly cloudy boundary layer of the southeastern Atlantic Ocean during July-October of 2006 and 2007. We show that the warming effect of aerosols increases with underlying cloud coverage. This relationship is nearly linear, making it possible to define a critical cloud fraction at which the aerosols switch from exerting a net cooling to a net warming effect. For this region and time period, the critical cloud fraction is about 0.4, and is strongly sensitive to the amount of solar radiation the aerosols absorb and the albedo of the underlying clouds. We estimate that the regional-mean warming effect of aerosols is three times higher when large-scale spatial covariation between cloud cover and aerosols is taken into account. These results demonstrate the importance of cloud prediction for the accurate quantification of aerosol direct effects.
C1 [Chand, D.; Wood, R.; Anderson, T. L.; Charlson, R. J.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Satheesh, S. K.] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
[Satheesh, S. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chand, D (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA.
EM duli@atmos.washington.edu
RI Wood, Robert/A-2989-2008
OI Wood, Robert/0000-0002-1401-3828
FU NASA's CALIPSO Mission [NAS1-99105]; National Science Foundation
[ATM-0601177, ATM-0205198]; National Oceanographic and Atmospheric
Administration [NA070AR4310282]
FX This work was supported by University of Washington startup funds,
NASA's CALIPSO Mission ( contract NAS1-99105), National Science
Foundation ( grants ATM-0601177 and ATM-0205198) and the National
Oceanographic and Atmospheric Administration ( grant NA070AR4310282). S.
K. S. would like to thank NPP administered by Oak Ridge Associated
Universities (ORAU) for an NPP fellowship.
NR 31
TC 117
Z9 119
U1 7
U2 30
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD MAR
PY 2009
VL 2
IS 3
BP 181
EP 184
DI 10.1038/NGEO437
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 420KY
UT WOS:000264289900016
ER
PT J
AU Niles, PB
Michalski, J
AF Niles, Paul B.
Michalski, Joseph
TI Meridiani Planum sediments on Mars formed through weathering in massive
ice deposits
SO NATURE GEOSCIENCE
LA English
DT Article
ID LAYERED DEPOSITS; OMEGA/MARS EXPRESS; MARTIAN SURFACE; BURNS FORMATION;
EQUATORIAL ICE; DIAGENESIS; SULFATES; ORIGIN; STRATIGRAPHY; LATITUDES
AB The sulphate-rich deposits at Meridiani Planum, Mars, discovered by the rover Opportunity, were proposed to be playa evaporites that had been reworked by eolian processes. Alternative hypotheses include volcanic or impact-driven formation of the sediments. Here we argue that the cation chemistry, scale, mineralogy and structure of the Meridiani sedimentary deposits are best explained by eolian or impact-driven reworking of the sublimation residue from a large-scale deposit consisting of dust and ice. We suggest that silicate material underwent significant acid weathering inside the ice deposit when thin films of water, formed through radiant heating, enabled the reaction between silicate material and sulphate-rich aerosols deposited from the atmosphere. The massive ice deposit could have formed during a period of high obliquity or polar wander, and subsequently sublimed away when obliquity changed or the pole moved to a new location. We propose acid weathering inside massive ice deposits as an explanation for the formation of many of the sulphate-rich layered deposits on Mars, which share many characteristics, including mineralogy, structure, erosional characteristics and size, with the sediments found at Meridiani Planum.
C1 [Niles, Paul B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Michalski, Joseph] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
RP Niles, PB (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM paul.b.niles@nasa.gov
NR 44
TC 81
Z9 82
U1 2
U2 20
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD MAR
PY 2009
VL 2
IS 3
BP 215
EP 220
DI 10.1038/NGEO438
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 420KY
UT WOS:000264289900024
ER
PT J
AU Czaja, AD
Kudryavtsev, AB
Cody, GD
Schopf, JW
AF Czaja, Andrew D.
Kudryavtsev, Anatoliy B.
Cody, George D.
Schopf, J. William
TI Characterization of permineralized kerogen from an Eocene fossil fern
SO ORGANIC GEOCHEMISTRY
LA English
DT Review
ID SOLID-STATE NMR; CHROMATOGRAPHY MASS-SPECTROMETRY; POLYCYCLIC
AROMATIC-HYDROCARBONS; RESONANCE RAMAN-SPECTROSCOPY; PLANT-CELL WALLS;
PYROLYSIS-GC-MS; ORGANIC-MATTER; MOLECULAR TAPHONOMY; WESTERN-AUSTRALIA;
COKE FORMATION
AB The processes of organic Maturation that occur during the permineralization of fossils and the detailed chemistry of the resulting products are incompletely understood. Primary among Such processes is the geochemical alteration of biological matter to produce kerogen, such as that which comprises the cell walls of the fossils studied here: essentially unmetamorphosed, Eocene plant axes (specimens of the fossil fern Dennstaedtiopsis aerenchymata cellularly permineralized in cherts of the Clarno Formation of Oregon and the Allenby Formation of British Columbia). The composition and molecular Structure of the kerogen that comprises the cell walls of such axes were analyzed using ultraviolet Raman spectroscopy (UV-Raman), solid state C-13 nuclear magnetic resonance spectroscopy (C-13 NMR) and pyrolysis-gas chromatography-mass spectrometry (py-GC-MS).
Cellularly well-preserved fern axes from both geologic units exhibit similar overall molecular structure, being composed primarily of networks of aromatic rings and polyene chains that, unlike more mature kerogens, lack large polycyclic aromatic hydrocarbon (PAH) constituents. The cell walls of the Allenby Formation specimens are, however, less altered than those of the Clarno chert, exhibiting more prevalent oxygen-containing and alkyl functional groups and comprising a greater fraction of rock mass.
The study represents the first demonstration of the effectiveness (and limitations) of the combined use of UV-Raman, C-13 NMR and py-GC-MS for the analysis of the kerogenous cell walls of chert-permineralized vascular plants. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Schopf, J. William] Univ Calif Los Angeles, Dept Earth & Space Sci, Inst Geophys & Planetary Phys, Ctr Study Evolut & Origin Life,Mol Biol Inst, Los Angeles, CA 90095 USA.
[Kudryavtsev, Anatoliy B.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Ctr Study Evolut & Origin Life, Los Angeles, CA 90095 USA.
[Kudryavtsev, Anatoliy B.; Schopf, J. William] Univ Calif Los Angeles, NASA, Astrobiol Inst, Los Angeles, CA 90095 USA.
[Cody, George D.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
RP Czaja, AD (reprint author), Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA.
EM aczaja@geology.wisc.edu
FU NASA Exobiology Grant [NAG5-12357]; NSF Pre-doctoral Fellowship; CSEOL
Fellowship; Sigma Xi; Geological Society of America Student Research
Grant
FX The research was supported by NASA Exobiology Grant NAG5-12357 to
J.W.S., the IGPP Center for the Study of Evolution and the Origin of
Life (CSEOL), and an NSF Pre-doctoral Fellowship, a CSEOL Fellowship,
Sigma Xi Grants-in-Aid of Research and a Geological Society of America
Student Research Grant to A.D.C. Samples of the Princeton chert were
provided by R. Stockey, University of Alberta, Edmonton. For technical
assistance, we thank R. Alkaly and E. Ruth. We also thank N. Gupta and
D. Curry for helpful comments and suggestions.
NR 112
TC 16
Z9 16
U1 2
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0146-6380
J9 ORG GEOCHEM
JI Org. Geochem.
PD MAR
PY 2009
VL 40
IS 3
BP 353
EP 364
DI 10.1016/j.orggeochem.2008.12.002
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 422ZD
UT WOS:000264465300007
ER
PT J
AU Biswas, R
Oliker, L
Vetter, J
AF Biswas, Rupak
Oliker, Leonid
Vetter, Jeffrey
TI Revolutionary technologies for acceleration of emerging petascale
applications
SO PARALLEL COMPUTING
LA English
DT Editorial Material
C1 [Biswas, Rupak] NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA.
[Oliker, Leonid] Univ Calif Berkeley, Lawrence Berkeley Lab, NERSC, CRD, Berkeley, CA 94720 USA.
[Vetter, Jeffrey] Oak Ridge Natl Lab, CSM Div, Oak Ridge, TN 37831 USA.
RP Biswas, R (reprint author), NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA.
EM rupak.biswas@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-8191
J9 PARALLEL COMPUT
JI Parallel Comput.
PD MAR
PY 2009
VL 35
IS 3
BP 117
EP 118
DI 10.1016/j.parco.2009.01.002
PG 2
WC Computer Science, Theory & Methods
SC Computer Science
GA 425SA
UT WOS:000264656200001
ER
PT J
AU Gurell, J
Wahlgren, GM
Nave, G
Wyart, JF
AF Gurell, J.
Wahlgren, G. M.
Nave, G.
Wyart, J-F
TI Wavelengths, energy levels and hyperfine structure constants in Ho II
SO PHYSICA SCRIPTA
LA English
DT Article
ID HOLLOW-CATHODE; METAL-POOR; HOLMIUM; SPECTRA; CONFIGURATIONS; ABUNDANCE;
LIFETIMES; SUN; 6P
AB We recorded spectra of Ho II emitted by hollow-cathode lamps, using the ultraviolet Fourier transform spectrometer (FTS) at Lund Observatory and the 2-m FTS at the National Institute of Standards and Technology. The combined wavenumber coverage spans the interval from 8000 to 49 600 cm(-1) (12 500 to 2016 angstrom). We measured 303 lines in these spectra and used them to determine energies and hyperfine structure constants of 100 levels. Of these, 41 energy levels have not been reported previously and hyperfine structure constants have not been reported previously for 83 levels. Comparisons between the hyperfine structure constants and energy levels presented in this article and those previously determined from other studies are included and discrepancies are discussed. A theoretical study of the odd-parity levels leads to hyperfine structure parameters and to predictions for unknown excited levels of the ground-state configuration.
C1 [Gurell, J.] Stockholm Univ, AlbaNova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden.
[Gurell, J.; Wahlgren, G. M.] Lund Observ, SE-22100 Lund, Sweden.
[Wahlgren, G. M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wahlgren, G. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nave, G.] NIST, Atom Phys Div, Gaithersburg, MD 20899 USA.
[Wyart, J-F] CNRS, UPR3321, Aime Cotton Lab, F-91405 Orsay, France.
[Wyart, J-F] CNRS, LERMA, UMR 8112, Observ Paris, F-92195 Meudon, France.
RP Gurell, J (reprint author), Stockholm Univ, AlbaNova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden.
EM jonas.gurell@physto.se
FU NASA [NNG06GJ29G]
FX GMW acknowledges financial support from NASA grant NNG06GJ29G. We
acknowledge the help of U Litzen, H Nilsson and K Oberg.
NR 28
TC 2
Z9 3
U1 2
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0031-8949
J9 PHYS SCRIPTA
JI Phys. Scr.
PD MAR
PY 2009
VL 79
IS 3
AR 035306
DI 10.1088/0031-8949/79/03/035306
PG 14
WC Physics, Multidisciplinary
SC Physics
GA 414UP
UT WOS:000263891000013
ER
PT J
AU Malone, CP
Johnson, PV
Kanik, I
Ajdari, B
Rahman, SS
Bata, SS
Emigh, A
Khakoo, MA
AF Malone, C. P.
Johnson, P. V.
Kanik, I.
Ajdari, B.
Rahman, S. S.
Bata, S. S.
Emigh, A.
Khakoo, M. A.
TI Electron-impact excitation of molecular nitrogen. II. Vibrationally
resolved excitation of the C (3)Pi(u)(v(')) state
SO PHYSICAL REVIEW A
LA English
DT Article
DE electron impact excitation; ground states; molecule-electron collisions;
nitrogen; ultraviolet spectra; vibrational states
ID DIFFERENTIAL CROSS-SECTIONS; N-2; COLLISIONS; N2; ENERGIES
AB Vibrationally resolved differential cross sections (DCSs) for electron impact from the X (1)Sigma(+)(g)(v(')=0) ground-state level in N-2 are presented for excitation of the C (3)Pi(u)(v(')) state, where v(')=0, 1, 2, 3, and 4. DCSs for the full C (3)Pi(u)(v(')) state, where v(')=0-4, are also presented. The vibrationally resolved DCSs were obtained from energy-loss spectra in the region of 10.75 to 12.75 eV measured at incident energies of 13, 15, 17.5, 20, 25, 30, 50, and 100 eV and for scattering angles ranging from 5 degrees to 130 degrees. Relative excitation probabilities for the vibrational levels of the C (3)Pi(u) state are shown to demonstrate non-Franck-Condon behavior for excitation energies less than approximately 50 eV. These results are compared with existing measurements.
C1 [Malone, C. P.; Johnson, P. V.; Kanik, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Malone, C. P.; Ajdari, B.; Khakoo, M. A.] Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92834 USA.
[Rahman, S. S.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90024 USA.
[Bata, S. S.] Brea Olinda High Sch, Brea, CA 92821 USA.
[Emigh, A.] Fullerton Union High Sch, Fullerton, CA 92832 USA.
RP Malone, CP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Johnson, Paul/D-4001-2009; Malone, Charles/A-6294-2010
OI Johnson, Paul/0000-0002-0186-8456; Malone, Charles/0000-0001-8418-1539
FU California State University, Fullerton; Jet Propulsion Laboratory,
California Institute of Technology; National Aeronautics and Space
Administration (NASA); National Science Foundation
[NSF-PHY-RUI-0653452]; NASA's Outer Planets and Planetary Atmospheres
Research programs
FX This work was performed at the California State University, Fullerton
and at the Jet Propulsion Laboratory, California Institute of Technology
under a contract with the National Aeronautics and Space Administration
(NASA). We gratefully acknowledge financial support through the National
Science Foundation under Grant No. NSF-PHY-RUI-0653452, and NASA's Outer
Planets and Planetary Atmospheres Research programs.
NR 23
TC 8
Z9 8
U1 0
U2 8
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD MAR
PY 2009
VL 79
IS 3
AR 032705
DI 10.1103/PhysRevA.79.032705
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 427HK
UT WOS:000264770200096
ER
PT J
AU Malone, CP
Johnson, PV
Kanik, I
Ajdari, B
Khakoo, MA
AF Malone, C. P.
Johnson, P. V.
Kanik, I.
Ajdari, B.
Khakoo, M. A.
TI Electron-impact excitation of molecular nitrogen. I. Excitation of the C
(3)Pi(u), E (3)Sigma(+)(g), and a(') (1)Sigma(+)(g) states
SO PHYSICAL REVIEW A
LA English
DT Article
DE electron energy loss spectra; electron impact excitation; excited
states; ground states; molecule-electron collisions; nitrogen
ID SCATTERING CROSS-SECTIONS; INTERMEDIATE ENERGY REGION;
DIATOMIC-MOLECULES; INCIDENT ENERGIES; N-2; N2; COLLISIONS; HE
AB Differential cross sections (DCSs) are presented for electron-impact excitation of the C (3)Pi(u), E (3)Sigma(+)(g), and a(') (1)Sigma(+)(g) states in N-2 from the X (1)Sigma(+)(g)(v(')=0) ground-state level. The DCSs were obtained from measurements of energy-loss spectra in the region of 10.75 to 12.75 eV measured at incident energies of 13, 15, 17.5, 20, 25, 30, 50, and 100 eV, and for scattering angles ranging from 5 degrees to 130 degrees. The results are compared with existing measurements.
C1 [Malone, C. P.; Johnson, P. V.; Kanik, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Malone, C. P.; Ajdari, B.; Khakoo, M. A.] Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92834 USA.
RP Malone, CP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Johnson, Paul/D-4001-2009; Malone, Charles/A-6294-2010
OI Johnson, Paul/0000-0002-0186-8456; Malone, Charles/0000-0001-8418-1539
NR 38
TC 9
Z9 9
U1 0
U2 11
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 MAR
PY 2009
VL 79
IS 3
AR 032704
DI 10.1103/PhysRevA.79.032704
PG 16
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 427HK
UT WOS:000264770200095
ER
PT J
AU Noya, EG
Srivastava, D
Menon, M
AF Gonzalez Noya, Eva
Srivastava, Deepak
Menon, Madhu
TI Heat-pulse rectification in carbon nanotube Y junctions
SO PHYSICAL REVIEW B
LA English
DT Article
DE carbon nanotubes; molecular dynamics method; phonons; rectification;
thermal conductivity
ID THERMAL-CONDUCTIVITY
AB Using molecular-dynamics simulations we demonstrate the existence of heat-pulse rectification in carbon nanotube Y junctions. The heat pulse is found to propagate unimpeded from stem to branches, while in the reverse direction there is a substantial reflection back into the branches with significantly reduced transmission. Based on this we discuss the implications for phonon rectification applications for these junctions.
C1 [Gonzalez Noya, Eva] Univ Complutense Madrid, Fac Ciencias Quim, Dept Quim Fis, E-28040 Madrid, Spain.
[Srivastava, Deepak] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA.
[Menon, Madhu] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA.
[Menon, Madhu] Univ Kentucky, Ctr Computat Sci, Lexington, KY 40506 USA.
RP Noya, EG (reprint author), Univ Complutense Madrid, Fac Ciencias Quim, Dept Quim Fis, E-28040 Madrid, Spain.
EM eva.noya@gmail.com; dsrivastava@mail.arc.nasa.gov; super250@pop.uky.edu
RI Noya, Eva/F-4958-2010
OI Noya, Eva/0000-0002-6359-1026
FU NASA Ames; NASA [NAS2-03144]; DOE [DE-FG02-00ER45817,
DE-FG02-07ER46375]; U.S.- ARO [W911NF-05-1-0372]
FX E. G. N. gratefully acknowledges useful discussions with L. J. Gallego.
Part of this work (E.G.N.) was supported by NASA Ames in 2003-4, and
(D.S.) is supported by NASA Contract No. NAS2-03144. D. S. thanks G.
Deardorff for useful discussions on visualization of results. M. M.
gratefully acknowledges support from grants by DOE (Grants No.
DE-FG02-00ER45817 and No. DE-FG02-07ER46375) and U.S.- ARO (Contract No.
W911NF-05-1-0372).
NR 15
TC 27
Z9 28
U1 0
U2 8
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1098-0121
J9 PHYS REV B
JI Phys. Rev. B
PD MAR
PY 2009
VL 79
IS 11
AR 115432
DI 10.1103/PhysRevB.79.115432
PG 5
WC Physics, Condensed Matter
SC Physics
GA 427GX
UT WOS:000264768900139
ER
PT J
AU Hao, SG
Kramer, MJ
Wang, CZ
Ho, KM
Nandi, S
Kreyssig, A
Goldman, AI
Wessels, V
Sahu, KK
Kelton, KF
Hyers, RW
Canepari, SM
Rogers, JR
AF Hao, S. G.
Kramer, M. J.
Wang, C. Z.
Ho, K. M.
Nandi, S.
Kreyssig, A.
Goldman, A. I.
Wessels, V.
Sahu, K. K.
Kelton, K. F.
Hyers, R. W.
Canepari, S. M.
Rogers, J. R.
TI Experimental and ab initio structural studies of liquid Zr2Ni
SO PHYSICAL REVIEW B
LA English
DT Article
DE ab initio calculations; liquid alloys; liquid structure; liquid theory;
molecular dynamics method; nickel alloys; nucleation; rapid
solidification; supercooling; undercooling; vitrification; X-ray
diffraction; zirconium alloys
ID SHORT-RANGE ORDER; LOCAL ATOMIC ARRANGEMENTS; TOTAL-ENERGY CALCULATIONS;
FORMING QUASI-CRYSTALS; WAVE BASIS-SET; NI-ZR ALLOY; UNDERCOOLED MELTS;
AMORPHOUS BINARY; POLYTETRAHEDRAL MATERIALS; MOLECULAR-DYNAMICS
AB High-energy x-ray diffraction and ab initio molecular-dynamics simulations demonstrate that the short-range order in the deeply undercooled Zr2Ni liquid is quite nuanced. The second diffuse scattering peak in the total structure factory sharpens with supercooling, revealing a shoulder on the high-Q side that is often taken to be a hallmark of increasing icosahedral order. However, a Voronoi tessellation indicates that only approximately 3.5% of all the atoms are in an icosahedral or icosahedral-like environment. In contrast, a Honeycutt-Andersen analysis indicates that a much higher fraction of the atoms is in icosahedral (15%-18%) or distorted icosahedral (25%-28%) bond-pair environments. These results indicate that the liquid contains a large population of fragmented clusters with pentagonal and distorted pentagonal faces, but the fully developed icosahedral fragments are rare. Interestingly, in both cases, the ordering changes little over the 500 K of cooling. All metrics show that the nearest-neighbor atomic configurations of the most deeply supercooled simulated liquid (1173 K) differ topologically and chemically from those in the stable C16 compound, even though the partial pair distributions are similar. The most significant structural change upon decreasing the temperature from 1673 to 1173 K is an increase in the population of Zr in Ni-centered clusters. The structural differences between the liquid and the C16 increase the nucleation barrier, explaining glass formation in the rapidly quenched alloys.
C1 [Hao, S. G.; Kramer, M. J.; Wang, C. Z.; Ho, K. M.; Nandi, S.; Kreyssig, A.; Goldman, A. I.] US DOE, Ames Lab, Ames, IA 50011 USA.
[Hao, S. G.; Kramer, M. J.; Wang, C. Z.; Ho, K. M.; Nandi, S.; Kreyssig, A.; Goldman, A. I.] Iowa State Univ, Ames, IA 50011 USA.
[Wessels, V.; Sahu, K. K.; Kelton, K. F.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Hyers, R. W.; Canepari, S. M.] Univ Massachusetts, Amherst, MA 01003 USA.
[Rogers, J. R.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Hao, SG (reprint author), US DOE, Ames Lab, Ames, IA 50011 USA.
RI Hyers, Robert/G-3755-2010; Hao, Shaogang/E-3527-2010
FU U. S. Department of Energy [DE-AC02-07CH11358]; Director for Energy
Research, Office of Basic Energy Sciences; Office of Science, Basic
Energy Sciences, U. S. Department of Energy [DE-AC02-06CH11357];
National Science Foundation [DMR-0606065]; NASA [NNM04AA016]
FX Ames Laboratory is operated for the U. S. Department of Energy by Iowa
State University under Contract No. DE-AC02-07CH11358. This work was
supported by the Director for Energy Research, Office of Basic Energy
Sciences, including a grant of computer time at the National Energy
Research Supercomputing Center (NERSC) in Berkeley. The high-energy
x-ray work at the MUCAT sector of the APS was supported by the Office of
Science, Basic Energy Sciences, U. S. Department of Energy under
Contract No. DE-AC02-06CH11357. The work at Washington University was
partially supported by the National Science Foundation under Grant No.
DMR-0606065 and by NASA under Contract No. NNM04AA016.
NR 53
TC 24
Z9 24
U1 4
U2 14
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1098-0121
EI 1550-235X
J9 PHYS REV B
JI Phys. Rev. B
PD MAR
PY 2009
VL 79
IS 10
AR 104206
DI 10.1103/PhysRevB.79.104206
PG 7
WC Physics, Condensed Matter
SC Physics
GA 427GU
UT WOS:000264768600049
ER
PT J
AU Norbury, JW
AF Norbury, John W.
TI Pion cross section parametrizations for intermediate energy,
nucleus-nucleus collisions
SO PHYSICAL REVIEW C
LA English
DT Article
ID HEAVY-ION COLLISIONS; GEV/C BEAM MOMENTUM; GAMMA-RAYS; MICROSCOPIC
CALCULATIONS; INCLUSIVE PRODUCTION; PARTICLE-PRODUCTION;
MOLECULAR-DYNAMICS; PROTON-PROTON; CHARGED PIONS; LARGE ANGLES
AB Space radiation and cosmic ray transport codes require simple and accurate models for hadron production in intermediate energy, nucleus-nucleus collisions. Several arithmetic parametrization models for pion production are compared to laboratory frame data. It is found that models based on high energy parametrizations are unable to describe intermediate energy, differential cross section data. However, simple thermal model parametrizations, when appropriately transformed from the center of momentum to the laboratory frame, are able to account for the data. Heavy ion transport codes that require algebraic cross section formulas can therefore use arithmetic parametrizations at high energy, but should use thermal model parametrizations at intermediate energy.
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 63
TC 3
Z9 3
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9985
EI 2469-9993
J9 PHYS REV C
JI Phys. Rev. C
PD MAR
PY 2009
VL 79
IS 3
AR 037901
DI 10.1103/PhysRevC.79.037901
PG 4
WC Physics, Nuclear
SC Physics
GA 427FV
UT WOS:000264766100075
ER
PT J
AU Cardoso, V
Miranda, AS
Berti, E
Witek, H
Zanchin, VT
AF Cardoso, Vitor
Miranda, Alex S.
Berti, Emanuele
Witek, Helvi
Zanchin, Vilson T.
TI Geodesic stability, Lyapunov exponents, and quasinormal modes
SO PHYSICAL REVIEW D
LA English
DT Article
ID HOLE NORMAL-MODES; SCHWARZSCHILD BLACK-HOLES; HIGHER DIMENSIONS; WKB
APPROACH; PERTURBATIONS; BINARIES; EQUATION; ORBITS; ENERGY; STAR
AB Geodesic motion determines important features of spacetimes. Null unstable geodesics are closely related to the appearance of compact objects to external observers and have been associated with the characteristic modes of black holes. By computing the Lyapunov exponent, which is the inverse of the instability time scale associated with this geodesic motion, we show that, in the eikonal limit, quasinormal modes of black holes in any dimensions are determined by the parameters of the circular null geodesics. This result is independent of the field equations and only assumes a stationary, spherically symmetric and asymptotically flat line element, but it does not seem to be easily extendable to anti-de Sitter spacetimes. We further show that (i) in spacetime dimensions greater than four, equatorial circular timelike geodesics in a Myers-Perry black-hole background are unstable, and (ii) the instability time scale of equatorial null geodesics in Myers-Perry spacetimes has a local minimum for spacetimes of dimension d >= 6.
C1 [Cardoso, Vitor; Witek, Helvi] Inst Super Tecn, Dept Fis, Ctr Multidisciplinar Astrofis CENTRA, P-1049001 Lisbon, Portugal.
[Miranda, Alex S.] Univ Fed Rio de Janeiro, Inst Fis, BR-21941972 Rio De Janeiro, RJ, Brazil.
[Witek, Helvi] Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany.
[Zanchin, Vilson T.] Univ Fed ABC, Ctr Ciencias Nat & Humanas, BR-09210170 Santo Andre, SP, Brazil.
[Cardoso, Vitor; Berti, Emanuele] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA.
[Berti, Emanuele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cardoso, V (reprint author), Inst Super Tecn, Dept Fis, Ctr Multidisciplinar Astrofis CENTRA, Ave Rovisco Pais 1, P-1049001 Lisbon, Portugal.
EM vcardoso@fisica.ist.utl.pt; astmiranda@if.ufrj.br;
berti@wugrav.wustl.edu; xhelvi.witek@ist.utl.pt; zanchin@ufabc.edu.br
RI Miranda, Alex/D-2502-2013; Zanchin, Vilson/J-3025-2012; Berti,
Emanuele/C-9331-2016; Cardoso, Vitor/K-1877-2015
OI Zanchin, Vilson/0000-0001-8499-1515; Berti,
Emanuele/0000-0003-0751-5130; Cardoso, Vitor/0000-0003-0553-0433
NR 63
TC 119
Z9 119
U1 0
U2 7
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 MAR
PY 2009
VL 79
IS 6
AR 064016
DI 10.1103/PhysRevD.79.064016
PG 13
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 427EL
UT WOS:000264762500063
ER
PT J
AU Zuckerwar, AJ
Ash, RL
AF Zuckerwar, Allan J.
Ash, Robert L.
TI Volume viscosity in fluids with multiple dissipative processes
SO PHYSICS OF FLUIDS
LA English
DT Article
DE entropy; equations of state; Navier-Stokes equations; shock waves;
viscosity
ID RELAXATION-TIMES
AB The variational principle of Hamilton is applied to derive the volume viscosity coefficients of a reacting fluid with multiple dissipative processes. The procedure, as in the case of a single dissipative process, yields two dissipative terms in the Navier-Stokes equation: The first is the traditional volume viscosity term, proportional to the dilatational component of the velocity; the second term is proportional to the material time derivative of the pressure gradient. Each dissipative process is assumed to be independent of the others. In a fluid comprising a single constituent with multiple relaxation processes, the relaxation times of the multiple processes are additive in the respective volume viscosity terms. If the fluid comprises several relaxing constituents (each with a single relaxation process), the relaxation times are again additive but weighted by the mole fractions of the fluid constituents. A generalized equation of state is derived, for which two special cases are considered: The case of "low-entropy production," where entropy variation is neglected, and that of "high entropy production," where the progress variables of the internal molecular processes are neglected. Applications include acoustical wave propagation, Stokes flow around a sphere, and the structure and thickness of a normal shock. Finally, it is shown that the analysis presented here resolves several misconceptions concerning the volume viscosity of fluids.
C1 [Zuckerwar, Allan J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Ash, Robert L.] Old Dominion Univ, Dept Aerosp Engn, Norfolk, VA 23508 USA.
RP Zuckerwar, AJ (reprint author), NASA, Langley Res Ctr, Mail Stop 238 Hampton, Hampton, VA 23681 USA.
EM ajzuckerwar@yahoo.com; rash@odu.edu
NR 29
TC 6
Z9 6
U1 0
U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-6631
EI 1089-7666
J9 PHYS FLUIDS
JI Phys. Fluids
PD MAR
PY 2009
VL 21
IS 3
AR 033105
DI 10.1063/1.3085814
PG 12
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 427LZ
UT WOS:000264782100016
ER
PT J
AU Deline, CA
Bengtson, RD
Breizman, BN
Tushentsov, MR
Jones, JE
Chavers, DG
Dobson, CC
Schuettpelz, BM
AF Deline, Christopher A.
Bengtson, Roger D.
Breizman, Boris N.
Tushentsov, Mikhail R.
Jones, Jonathan E.
Chavers, D. Greg
Dobson, Chris C.
Schuettpelz, Branwen M.
TI Plume detachment from a magnetic nozzle
SO PHYSICS OF PLASMAS
LA English
DT Article
DE aerospace propulsion; nozzles; plasma applications; plasma
magnetohydrodynamics; plasma probes
ID TRIPLE PROBE; PLASMA DETACHMENT; LAYER; SYSTEM; FIELDS
AB High-powered electric propulsion thrusters utilizing a magnetized plasma require that plasma exhaust detach from the applied magnetic field in order to produce thrust. This paper presents experimental results demonstrating that a sufficiently energetic and flowing plasma can indeed detach from a magnetic nozzle. Microwave interferometer and probe measurements provide plume density, electron temperature, and ion flux measurements in the nozzle region. Measurements of ion flux show a low-beta plasma plume which follows applied magnetic field lines until the plasma kinetic pressure reaches the magnetic pressure and a high-beta plume expanding ballistically afterward. Several magnetic configurations were tested including a reversed field nozzle configuration. Despite the dramatic change in magnetic field profile, the reversed field configuration yielded little measurable change in plume trajectory, demonstrating the plume is detached. Numerical simulations yield density profiles in agreement with the experimental results.
C1 [Deline, Christopher A.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Bengtson, Roger D.; Breizman, Boris N.; Tushentsov, Mikhail R.] Univ Texas Austin, Inst Fus Studies, Austin, TX 78712 USA.
[Jones, Jonathan E.; Chavers, D. Greg; Dobson, Chris C.] George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Schuettpelz, Branwen M.] Univ Alabama, Huntsville, AL 35899 USA.
RP Deline, CA (reprint author), Natl Renewable Energy Lab, Golden, CO 80401 USA.
EM cdeline@umich.edu
RI Deline, Christopher/K-5998-2013
OI Deline, Christopher/0000-0002-9867-8930
FU NASA [NNJ05HB77C]
FX This work was supported in part by a NASA Graduate Student Researchers
Program fellowship and financial support of the Ad Astra Rocket Co. to
C. A. Deline. Dissertation and technical support was provided to Deline
by his thesis advisor, B. Gilchrist, at the University of Michigan. The
work at The University of Texas at Austin, University of Alabama at
Huntsville and Marshall Space Flight Center was supported by NASA under
Contract No. NNJ05HB77C. Special thanks go to A. Arefiev and J. Meyer at
the University of Texas for technical and analytical support. The
authors would also like to thank M. LaPointe for numerous helpful
comments.
NR 28
TC 15
Z9 15
U1 1
U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD MAR
PY 2009
VL 16
IS 3
AR 033502
DI 10.1063/1.3080206
PG 9
WC Physics, Fluids & Plasmas
SC Physics
GA 427LW
UT WOS:000264781800053
ER
PT J
AU Fairen, AG
Schulze-Makuch, D
Rodriguez, AP
Fink, W
Davila, AF
Uceda, ER
Furfaro, R
Amils, R
McKay, CP
AF Fairen, Alberto G.
Schulze-Makuch, Dirk
Rodriguez, Alexis P.
Fink, Wolfgang
Davila, Alfonso F.
Uceda, Esther R.
Furfaro, Roberto
Amils, Ricardo
McKay, Christopher P.
TI Evidence for Amazonian acidic liquid water on Mars-A reinterpretation of
MER mission results
SO PLANETARY AND SPACE SCIENCE
LA English
DT Review
DE Mars; Liquid water; Amazonian; Mars Exploration Rovers; Meridiani
Planum; Gusev crater
ID ROVER LANDING SITE; MERIDIANI-PLANUM; GUSEV CRATER; SPIRIT ROVER;
OPPORTUNITY ROVER; NORTHERN PLAINS; MOSSBAUER SPECTROMETER; WEATHERING
PRODUCTS; SEDIMENTARY-ROCKS; TERRA-MERIDIANI
AB The Mars Exploration Rover (MER) missions have confirmed aqueous activity on Mars. Here we review the analyses of the field-based MER data, and conclude that some weathering processes in Meridiani Planum and Gusev crater are better explained by late diagenetic water-rock interactions than by early diagenesis only. At Meridiani, the discovery of jarosite by MER-1 Opportunity indicates acidic aqueous activity, evaporation, and desiccation of rock materials. MER-based information, placed into the context of published data, point to local and limited aqueous activity during geologically recent times in Meridiani. Pre-Amazonian environmental changes (including important variations in the near-surface groundwater reservoirs, impact cratering, and global dust storms and other pervasive wind-related erosion) are too extreme for pulverulent jarosite to survive over extended time periods, and therefore we argue instead that jarosite deposits must have formed in a climatically more stable period. Any deposits of pre-existent concretionary jarosite surviving up to the Amazonian would not have reached completion in the highly saline and acidic brines occurring at Meridiani. MER-2 Spirit has also revealed evidence for local and limited Amazonian aqueous environmental conditions in Gusev crater, including chemical weathering leading to goethite and hematite precipitation, rock layering, and chemical enhancement of Cl, S, Br, and oxidized iron in rocks and soils. The estimated relative age of the impact crater materials in Gusev indicates that these processes have taken place during the last 2 billion years. We conclude that minor amounts of shallow acidic liquid water have been present on the surface of Mars at local scales during the Amazonian Period. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Fairen, Alberto G.; Davila, Alfonso F.; McKay, Christopher P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Schulze-Makuch, Dirk] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA.
[Rodriguez, Alexis P.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Fink, Wolfgang] CALTECH, Visual & Autonomous Explorat Syst Res Lab, Pasadena, CA 91125 USA.
[Uceda, Esther R.] NASA, Ames Res Ctr, Biosci Div, Moffett Field, CA 94035 USA.
[Furfaro, Roberto] Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA.
[Amils, Ricardo] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain.
RP Fairen, AG (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
EM afairen@arc.nasa.gov
RI Davila, Alfonso/A-2198-2013;
OI Davila, Alfonso/0000-0002-0977-9909; Schulze-Makuch,
Dirk/0000-0002-1923-9746
NR 112
TC 17
Z9 17
U1 0
U2 12
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 MAR
PY 2009
VL 57
IS 3
BP 276
EP 287
DI 10.1016/j.pss.2008.11.008
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 426EI
UT WOS:000264690400002
ER
PT J
AU Zhang, ZF
Nielsen, E
Plaut, JJ
Orosei, R
Picardi, G
AF Zhang, Zhenfei
Nielsen, Erling
Plaut, Jeffrey J.
Orosei, Roberto
Picardi, Giovanni
TI Ionospheric corrections of MARSIS subsurface sounding signals with
filters including collision frequency
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Ionosphere; Sounding radar; Collision frequency
ID MARTIAN IONOSPHERE; RADAR SOUNDINGS; DISTORTION; WAVES; VENUS
AB Ionospheric corrections of Mars advanced radar for subsurface and ionosphere sounding (MARSIS) Subsurface sounding signals are necessary before they can be further analyzed. Usually the ionosphere correction only considers the phase dispersion owing to the electron densities. In this paper we show that if the electron-neutral collision frequency is included in the correction filter, the signal-to-noise ratio of the processed signal can be further maximized and the spatial resolution of the signal be improved. Three different models of the ionosphere profile have been studied, and it is shown that a uniform slab model, of both densities and collisions, is feasible and probably the best choice when implementing the correction filter including collisions. The physical significance of the parameters obtained with the uniform model (equivalent parameters) is discussed, and it is shown that they are useful for the estimation of the real physical parameters of the ionosphere. We developed a recursive, random search algorithim to facilitate the realization of the correction process with the filter including collision frequency. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Zhang, Zhenfei] China Univ Geosci, Inst Math Geol & Remote Sensing, Dept Resources, Wuhan 430074, Peoples R China.
[Zhang, Zhenfei] China Univ Geosci, Ctr Space Sci, Wuhan 430074, Peoples R China.
[Zhang, Zhenfei; Nielsen, Erling] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Plaut, Jeffrey J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Orosei, Roberto] Ist Nazl Astrofis, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy.
[Picardi, Giovanni] Univ Roma La Sapienza, Infocom Dept, I-00184 Rome, Italy.
RP Zhang, ZF (reprint author), China Univ Geosci, Inst Math Geol & Remote Sensing, Dept Resources, 388 Lumo Rd, Wuhan 430074, Peoples R China.
EM zfzhang@cug.edu.cn
NR 32
TC 7
Z9 7
U1 0
U2 0
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 MAR
PY 2009
VL 57
IS 3
BP 393
EP 403
DI 10.1016/j.pss.2008.11.016
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 426EI
UT WOS:000264690400012
ER
PT J
AU Lipatov, AS
Rankin, R
AF Lipatov, A. S.
Rankin, R.
TI Nonlinear field line resonances. Effect of Hall term on plasma
compression: 1D Hall-MHD modeling
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Magnetospheric physics; Magnetosphere-ionosphere interactions; MHD waves
and instabilities; Space plasma physics; Nonlinear phenomena
ID SOLAR CORONAL LOOPS; ALFVEN WAVES; FLUID SIMULATIONS; WIND;
MAGNETOSPHERE; MAGNETOPAUSE; ABSORPTION; MIRROR; FREJA; CODE
AB A model is presented that describes the excitation of small-scale density perturbations and electromagnetic fields by standing shear Alfven waves in a Cartesian geometry. The model includes the effects of plasma betas and the Hall term effects. The characteristics of magnetospheric density cavities and the formation of the significant peak in density are discussed in the paper. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Lipatov, A. S.; Rankin, R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada.
[Lipatov, A. S.] Moscow Inst Phys & Technol, Dept Problems Phys & Energet, Moscow, Russia.
[Lipatov, A. S.] Russian Acad Sci, AA Dorodnitsyn Comp Ctr, Moscow 119991, Russia.
RP Lipatov, AS (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 673,Bld 21,Rm 025,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Alexander.Lipatov-1@nasa.gov
RI Rankin, Robert/C-5435-2013
OI Rankin, Robert/0000-0003-0151-6343
FU Canadian Space Agency; Department of Physics at the University of
Alberta, Edmonton; GEST Center UMBC/NASA GSFC [900-37-172, 670-90-315]
FX A.S.L. was supported in part by grant of the Canadian Space Agency
during his work (December 2004-March 2006) in the Department of Physics
at the University of Alberta, Edmonton and by the tasks 900-37-172 and
670-90-315 from the GEST Center UMBC/NASA GSFC. Computational resources
were provided by the University of Alberta (Western Canada Research
Grid) and the Max-Planck Institute for Solar System Research.
NR 38
TC 1
Z9 1
U1 0
U2 4
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 MAR
PY 2009
VL 57
IS 3
BP 404
EP 414
DI 10.1016/j.pss.2008.12.012
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 426EI
UT WOS:000264690400013
ER
PT J
AU Stothers, RB
AF Stothers, Richard B.
TI A Comparison of Stellar Extinction and Space-Based Measurements of
Stratospheric Aerosol Optical Depth
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID MOUNT-PINATUBO ERUPTION; SAN-PEDRO-MARTIR; ATMOSPHERIC EXTINCTION;
LA-SILLA; EVOLUTION; PHOTOMETRY
AB Observed increases of stellar extinction after the two largest recent volcanic eruptions (El Chichon 1982 and Pinatubo 1991) are compiled here from published sources and compared with space-based measurements of stratospheric aerosol optical depth. Hemispheric and global annual mean optical depths following the two eruptions show close agreement between the two methods, if allowance is made for the fact that the stellar extinction data refer only to midlatitudes.
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 30
TC 1
Z9 1
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD MAR
PY 2009
VL 121
IS 877
BP 303
EP 306
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 427XP
UT WOS:000264812700010
ER
PT J
AU Kondo, H
Searby, ND
Mojarrab, R
Phillips, J
Alwood, J
Yumoto, K
Almeida, EAC
Limoli, CL
Globus, RK
AF Kondo, Hisataka
Searby, Nancy D.
Mojarrab, Rose
Phillips, Jonathan
Alwood, Joshua
Yumoto, Kenji
Almeida, Eduardo A. C.
Limoli, Charles L.
Globus, Ruth K.
TI Total-Body Irradiation of Postpubertal Mice with Cs-137 Acutely
Compromises the Microarchitecture of Cancellous Bone and Increases
Osteoclasts
SO RADIATION RESEARCH
LA English
DT Article
ID LONG-DURATION SPACEFLIGHT; HIGH-DOSE IRRADIATION; TRABECULAR BONE;
MINERAL DENSITY; MOUSE; RADIATION; SPACE; CELLS; RESORPTION; INVITRO
AB Ionizing radiation can cause substantial tissue degeneration, which may threaten the long-term health of astronauts and radiotherapy patients. To determine whether a single dose of radiation acutely compromises structural integrity in the postpubertal skeleton, 18-week-old male mice were exposed to Cs-137 gamma radiation (1 or 2 Gy). The structure of high-turnover, cancellous bone was analyzed by microcomputed tomography (microCT) 3 or 10 days after irradiation and in basal controls (tissues harvested at the time of irradiation) and age-matched controls. Irradiation (2 Gy) caused a 20% decline in tibial cancellous bone volume fraction (BV/TV) within 3 days and a 43% decline within 10 days, while 1 Gy caused a 28% reduction 10 days later. The BV/TV decrement was due to increased spacing and decreased thickness of trabeculae. Radiation also increased (similar to 150%) cancellous surfaces lined with tartrate-resistant, acid phosphatase-positive osteoclasts, an index of increased bone resorption. Radiation decreased lumbar vertebral BV/TV 1 month after irradiation, showing the persistence of cancellous bone loss, although mechanical properties in compression were unaffected. In sum, a single dose of gamma radiation rapidly increased osteoclast surface in cancellous tissue and compromised cancellous microarchitecture in the remodeling appendicular and axial skeleton of postpubertal mice. (C) 2009 by Radiation Research Society
C1 [Kondo, Hisataka; Searby, Nancy D.; Mojarrab, Rose; Phillips, Jonathan; Alwood, Joshua; Yumoto, Kenji; Almeida, Eduardo A. C.; Globus, Ruth K.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
[Kondo, Hisataka; Yumoto, Kenji; Limoli, Charles L.] Univ Calif Irvine, Dept Radiat Oncol, Irvine, CA USA.
[Alwood, Joshua] Stanford Univ, Dept Aeronaut & Space Engn, Palo Alto, CA 94304 USA.
RP Globus, RK (reprint author), NASA, Ames Res Ctr, Space Biosci Div, MS 236-7, Moffett Field, CA 94035 USA.
EM Ruth.K.Globus@NASA.gov
FU NASA [NNH04ZUU005N/RAD2004-0000-0110]
FX This work was supported by NASA grant NNH04ZUU005N/RAD2004-0000-0110. We
thank Dr. Christopher Jacobs and Derek Lindsey for the microCT and Derek
Lindsay and Gary Beaupre for advising on compression testing at the Bone
and Joint Center, Veteran's Administration Palo Alto Health Care System.
We also are grateful to Marjolein van der Meulen at Cornell for expert
advice and Emily Morey-Holton at Ames Research Center for helpful advice
in the course of these studies and for critically reviewing the
manuscript.
NR 38
TC 40
Z9 43
U1 0
U2 5
PU RADIATION RESEARCH SOC
PI LAWRENCE
PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA
SN 0033-7587
J9 RADIAT RES
JI Radiat. Res.
PD MAR
PY 2009
VL 171
IS 3
BP 283
EP 289
DI 10.1667/RR1463.1
PG 7
WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology,
Nuclear Medicine & Medical Imaging
GA 412MD
UT WOS:000263728000003
PM 19267555
ER
PT J
AU Kurtoglu, T
Campbell, MI
AF Kurtoglu, Tolga
Campbell, Matthew I.
TI An evaluation scheme for assessing the worth of automatically generated
design alternatives
SO RESEARCH IN ENGINEERING DESIGN
LA English
DT Article
DE Concept generation; Design automation; Design selection
AB This paper introduces a tool called the designer preference modeler (DPM) that analyzes the designer's decision making during concept evaluation, and constructs a designer preference model to be used for evaluation of automatically generated design alternatives. The method is based on establishing an interaction between a designer and a computational synthesis tool during conceptual design. The synthesis software generates design alternatives using a catalog of design knowledge formulated as grammar rules which describe how electromechanical designs are built. DPM carefully selects a set from these alternatives and presents it to the designer for evaluation. The designer's evaluations are translated into a preference model that is subsequently used to search the solution space for best designs. Application of the method to the design of a consumer product shows DPM's range of capabilities.
C1 [Kurtoglu, Tolga] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Campbell, Matthew I.] Univ Texas Austin, Dept Mech Engn, Automated Design Lab, Austin, TX 78712 USA.
RP Kurtoglu, T (reprint author), NASA, Ames Res Ctr, MS 269-3, Moffett Field, CA 94035 USA.
EM Tolga.Kurtoglu@nasa.gov; mc1@mail.utexas.edu
RI Campbell, Matthew/B-5334-2009
OI Campbell, Matthew/0000-0003-1296-6542
NR 29
TC 12
Z9 12
U1 1
U2 3
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0934-9839
J9 RES ENG DES
JI Res. Eng. Design
PD MAR
PY 2009
VL 20
IS 1
BP 59
EP 76
DI 10.1007/s00163-008-0062-1
PG 18
WC Engineering, Multidisciplinary; Engineering, Industrial; Engineering,
Manufacturing
SC Engineering
GA 413GR
UT WOS:000263781400005
ER
PT J
AU Wang, TY
Kuang, WJ
Ma, SZ
AF Wang TianYuan
Kuang WeiJia
Ma ShiZhuang
TI Numerical simulation of Martian historical dynamo: Impact of the
Rayleigh number on the dynamo state
SO SCIENCE IN CHINA SERIES D-EARTH SCIENCES
LA English
DT Article
DE Mars; magnetic field; Rayleigh number; dynamo
ID MAGNETIC-FIELD; SNC METEORITES; CORE FORMATION; MARS; MANTLE;
CONVECTION; MODEL; FLUID; MAP
AB The observed Mars remnant magnetism suggests that there was an active dynamo in the Martian core. We use the MoSST core dynamics model to simulate the Martian historical dynamo, focusing on the variation of the dynamo states with the Rayleigh number Ra (a non-dimensional parameter describing the buoyancy force in the core). Our numerical results show that the mean field length scale does not vary monotonically with the Rayleigh number, and the field morphology at the core mantle boundary changes with Rayleigh number. In particular, it drifts westward with a speed decreasing with Rayleigh number.
C1 [Wang TianYuan; Ma ShiZhuang] Chinese Acad Sci, Grad Univ, Lab Computat Geodynam, Beijing 100049, Peoples R China.
[Kuang WeiJia] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Wang, TY (reprint author), Chinese Acad Sci, Grad Univ, Lab Computat Geodynam, Beijing 100049, Peoples R China.
EM tywang@mails.gucas.ac.cn
RI Kuang, Weijia/K-5141-2012
OI Kuang, Weijia/0000-0001-7786-6425
FU National Natural Science Foundation of China [40328006]
FX Supported by National Natural Science Foundation of China (Grant No.
40328006)
NR 44
TC 2
Z9 2
U1 0
U2 2
PU SCIENCE PRESS
PI BEIJING
PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA
SN 1006-9313
J9 SCI CHINA SER D
JI Sci. China Ser. D-Earth Sci.
PD MAR
PY 2009
VL 52
IS 3
BP 402
EP 410
DI 10.1007/s11430-009-0034-y
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA 417VH
UT WOS:000264106100012
ER
PT J
AU Potts, C
AF Potts, Christopher
TI How do spacecraft orient themselves in the absence of magnetic poles? Is
there any truth to the system they use on Star Trek?
SO SCIENTIFIC AMERICAN
LA English
DT Letter
C1 NASA, Jet Prop Lab, Pasadena, CA USA.
RP Potts, C (reprint author), NASA, Jet Prop Lab, Pasadena, CA USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SCI AMERICAN INC
PI NEW YORK
PA 415 MADISON AVE, NEW YORK, NY 10017 USA
SN 0036-8733
J9 SCI AM
JI Sci.Am.
PD MAR
PY 2009
VL 300
IS 3
BP 84
EP 84
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 409GW
UT WOS:000263495200035
ER
PT J
AU Carnell, LS
Siochi, EJ
Wincheski, RA
Holloway, NM
Clark, RL
AF Carnell, Lisa S.
Siochi, Emilie J.
Wincheski, Russell A.
Holloway, Nancy M.
Clark, Robert L.
TI Electric field effects on fiber alignment using an auxiliary electrode
during electrospinning
SO SCRIPTA MATERIALIA
LA English
DT Article
DE Modeling; Electrospinning; Fibers; Polymer processing; Theory
ID BENDING INSTABILITY; POLYMER-SOLUTIONS; JETS; NANOFIBERS
AB Control of electrospun fiber placement and distribution was investigated by examining the effect of electric field parameters on the electrospinning of fibers. The experimental set-up in this study eliminated the bending instability and whipping, allowing the jet to be modeled as a stable trajectory. Coupling of experimental and computational results suggests the potential for predicting aligned fiber distribution in electrospun mats. (C) 2008 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Carnell, Lisa S.; Siochi, Emilie J.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
[Wincheski, Russell A.] NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23681 USA.
[Holloway, Nancy M.] NASA, Langley Res Ctr, Fabricat Technol Dev Branch, Hampton, VA 23681 USA.
[Clark, Robert L.] Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA.
RP Carnell, LS (reprint author), NASA, Langley Res Ctr, Adv Mat & Proc Branch, MS 226, Hampton, VA 23681 USA.
EM lisa.a.scottcarnell@nasa.gov
NR 12
TC 27
Z9 30
U1 3
U2 28
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 MAR
PY 2009
VL 60
IS 6
BP 359
EP 361
DI 10.1016/j.scriptamat.2008.09.035
PG 3
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 407XR
UT WOS:000263398100001
ER
PT J
AU Swanson, A
Huang, SL
Crabtree, R
AF Swanson, Alan
Huang, Shengli
Crabtree, Robert
TI Using a LIDAR Vegetation Model to Predict UHF SAR Attenuation in
Coniferous Forests
SO SENSORS
LA English
DT Article
DE SAR; Lidar; Forest; Attenuation
ID L-BAND; IMAGERY; PARAMETERS
AB Attenuation of radar signals by vegetation can be a problem for target detection and GPS reception, and is an important parameter in models describing vegetation backscatter. Here we first present a model describing the 3D distribution of stem and foliage structure based on small footprint scanning LIDAR data. Secondly we present a model that uses ray-tracing methodology to record detailed interactions between simulated radar beams and vegetation components. These interactions are combined over the SAR aperture and used to predict two-way attenuation of the SAR signal. Accuracy of the model is demonstrated using UHF SAR observations of large trihedral corner reflectors in coniferous forest stands. Our study showed that the model explains between 66% and 81% of the variability in observed attenuation.
C1 [Swanson, Alan; Huang, Shengli; Crabtree, Robert] Yellowstone Ecol Res Ctr, Bozeman, MT 59718 USA.
[Huang, Shengli] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Swanson, A (reprint author), Yellowstone Ecol Res Ctr, 2048 Anal Dr,Suite B, Bozeman, MT 59718 USA.
EM swanson@yellowstoneresearch.org; huang@yellowstoneresearch.org;
crabtree@yellowstoneresearch.org
FU Air Force Research Lab [F33615-03-C-1432]
FX This work was done under the financial support from Air Force Research
Lab (No F33615-03-C-1432). We would like to thank Mike Bakich and Jim
Leonard for their support with the reflector model.
NR 16
TC 3
Z9 3
U1 0
U2 0
PU MOLECULAR DIVERSITY PRESERVATION INTERNATIONAL-MDPI
PI BASEL
PA KANDERERSTRASSE 25, CH-4057 BASEL, SWITZERLAND
SN 1424-8220
J9 SENSORS-BASEL
JI Sensors
PD MAR
PY 2009
VL 9
IS 3
BP 1559
EP 1573
DI 10.3390/s90301559
PG 15
WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation
SC Chemistry; Electrochemistry; Instruments & Instrumentation
GA 424NF
UT WOS:000264572700019
PM 22573972
ER
PT J
AU Snowden, S
AF Snowden, S. L.
TI What Can Be Learned from X-ray Spectroscopy Concerning Hot Gas in the
Local Bubble and Charge Exchange Processes?
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE X-rays; Solar system; Interstellar medium
ID SOLAR-WIND; INTERSTELLAR GAS; ROSAT SURVEY; EMISSION; PLASMA; IONS;
MAPS; SKY
AB Both solar wind charge exchange emission and diffuse thermal emission from the Local Bubble are strongly dominated in the soft X-ray band by lines from highly ionized elements. While both processes share many of the same lines, the spectra should differ significantly due to the different production mechanisms, abundances, and ionization states. Despite their distinct spectral signatures, current and past observatories have lacked the spectral resolution to adequately distinguish between the two sources. High-resolution X-ray spectroscopy instrumentation proposed for future missions has the potential to answer fundamental questions such as whether there is any hot plasma in the Local Hot Bubble, and if so what are the abundances of the emitting plasma and whether the plasma is in equilibrium. Such instrumentation will provide dynamic information about the solar wind including data on ion species which are currently difficult to track. It will also make possible remote sensing of the solar wind.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Snowden, S (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
EM steven.l.snowden@nasa.gov
RI Snowden, Steven/D-5292-2012
NR 26
TC 11
Z9 11
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2009
VL 143
IS 1-4
BP 253
EP 262
DI 10.1007/s11214-008-9343-2
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 413NH
UT WOS:000263799300020
ER
PT J
AU Hodis, HN
Mack, WJ
Dustin, L
Mahrer, PR
Azen, SP
Detrano, R
Selhub, J
Alaupovic, P
Liu, CR
Liu, CH
Hwang, J
Wilcox, AG
Selzer, RH
AF Hodis, Howard N.
Mack, Wendy J.
Dustin, Laurie
Mahrer, Peter R.
Azen, Stanley P.
Detrano, Robert
Selhub, Jacob
Alaupovic, Petar
Liu, Chao-ran
Liu, Ci-hua
Hwang, Juliana
Wilcox, Alison G.
Selzer, Robert H.
CA BVAIT Res Grp
TI High-Dose B Vitamin Supplementation and Progression of Subclinical
Atherosclerosis A Randomized Controlled Trial
SO STROKE
LA English
DT Article
DE atherosclerosis; computed tomography; folate; homocysteine; intima media
thickness; randomized controlled trials; vitamin B(12); vitamin B(6);
folic acid
ID INTIMA-MEDIA THICKNESS; CORONARY-HEART-DISEASE; ULTRAFAST
COMPUTED-TOMOGRAPHY; PLASMA HOMOCYSTEINE; FOLIC-ACID; VASCULAR-DISEASE;
ARTERY-DISEASE; RISK-FACTOR; FOLATE; HOMOCYST(E)INE
AB Background and Purpose-Although plasma total homocysteine (tHcy) levels are associated with cardiovascular disease, it remains unclear whether homocysteine is a cause or a marker of atherosclerotic vascular disease. We determined whether reduction of tHcy levels with B vitamin supplementation reduces subclinical atherosclerosis progression.
Methods-In this double-blind clinical trial, 506 participants 40 to 89 years of age with an initial tHcy >8.5 mu mol/L without diabetes and cardiovascular disease were randomized to high-dose B vitamin supplementation (5 mg folic acid+0.4 mg vitamin B(12) + 50 mg vitamin B(6)) or matching placebo for 3.1 years. Subclinical atherosclerosis progression across 3 vascular beds was assessed using high-resolution B-mode ultrasonography to measure carotid artery intima media thickness (primary outcome) and multidetector spiral CT to measure aortic and coronary artery calcium (secondary outcome).
Results-Although the overall carotid artery intima media thickness progression rate was lower with B vitamin supplementation than with placebo, statistically significant between-group differences were not found (P=0.31). However, among subjects with baseline tHcy >= 9.1 mu mol/L, those randomized to B vitamin supplementation had a statistically significant lower average rate of carotid artery intima media thickness progression compared with placebo (P = 0.02); among subjects with a baseline tHcy <9.1 mu mol/L, there was no significant treatment effect (probability value for treatment interaction=0.02). B vitamin supplementation had no effect on progression of aortic or coronary artery calcification overall or within subgroups.
Conclusion-High-dose B vitamin supplementation significantly reduces progression of early-stage subclinical atherosclerosis (carotid artery intima media thickness) in well-nourished healthy B vitamin "replete" individuals at low risk for cardiovascular disease with a fasting tHcy >= 9.1 mu mol/L. (Stroke. 2009; 40: 730-736.)
C1 [Hodis, Howard N.; Mack, Wendy J.; Dustin, Laurie; Azen, Stanley P.; Liu, Chao-ran; Liu, Ci-hua; Hwang, Juliana; Selzer, Robert H.] Univ So Calif, Keck Sch Med, Atherosclerosis Res Unit, Los Angeles, CA 90033 USA.
[Hodis, Howard N.; Mack, Wendy J.; Dustin, Laurie; Azen, Stanley P.] Univ So Calif, Keck Sch Med, Dept Prevent Med, Los Angeles, CA 90033 USA.
[Hodis, Howard N.; Liu, Chao-ran; Liu, Ci-hua] Univ So Calif, Keck Sch Med, Dept Med, Los Angeles, CA 90033 USA.
[Hodis, Howard N.; Hwang, Juliana] Univ So Calif, Keck Sch Med, Dept Radiol, Los Angeles, CA 90033 USA.
[Hodis, Howard N.; Hwang, Juliana] Univ So Calif, Sch Pharm, Dept Mol Pharmacol & Toxicol, Los Angeles, CA 90033 USA.
[Mahrer, Peter R.] Kaiser Permanente Med Ctr, Los Angeles, CA 90034 USA.
[Detrano, Robert] Harbor Univ Calif Los Angeles, Med Ctr, Los Angeles, CA USA.
[Selhub, Jacob] Tufts Univ, USDA, Human Nutr Res Ctr Aging, Boston, MA 02111 USA.
[Selhub, Jacob] Tufts Univ, Dept Vitamin Metab & Aging, Boston, MA 02111 USA.
[Alaupovic, Petar] Oklahoma Med Res Fdn, Oklahoma City, OK 73104 USA.
[Selzer, Robert H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Hodis, HN (reprint author), Univ So Calif, Keck Sch Med, Atherosclerosis Res Unit, 2250 Alcazar St,CSC132, Los Angeles, CA 90033 USA.
EM athero@usc.edu
FU National Institute on Aging [R01AG-17160]; National Institutes of Health
FX This study was supported by grant R01AG-17160 from the National
Institute on Aging, National Institutes of Health. Leiner Health
Products provided the B vitamin supplements and placebo.
NR 31
TC 57
Z9 59
U1 2
U2 5
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0039-2499
J9 STROKE
JI Stroke
PD MAR
PY 2009
VL 40
IS 3
BP 730
EP 736
DI 10.1161/STROKEAHA.108.526798
PG 7
WC Clinical Neurology; Peripheral Vascular Disease
SC Neurosciences & Neurology; Cardiovascular System & Cardiology
GA 410PN
UT WOS:000263590200025
PM 19118243
ER
PT J
AU Gelaro, R
Zhu, YQ
AF Gelaro, Ronald
Zhu, Yanqiu
TI Examination of observation impacts derived from observing system
experiments (OSEs) and adjoint models
SO TELLUS SERIES A-DYNAMIC METEOROLOGY AND OCEANOGRAPHY
LA English
DT Article
ID VARIATIONAL DATA ASSIMILATION; OBSERVATION SENSITIVITY; ERROR
AB With the adjoint of a data assimilation system, the impact of any or all assimilated observations on measures of forecast skill can be estimated accurately and efficiently. The approach allows aggregation of results in terms of individual data types, channels or locations, all computed simultaneously. In this study, adjoint-based estimates of observation impact are compared with results from standard observing system experiments (OSEs) using forward and adjoint versions of the NASA GEOS-5 atmospheric data assimilation system. Despite important underlying differences in the way observation impacts are measured in the two approaches, the results show that they provide consistent estimates of the overall impact of most of the major observing systems in reducing a dry total-energy metric of 24-h forecast error over the globe and extratropics and, to a lesser extent, over the tropics. Just as importantly, however, it is argued that the two approaches provide unique, but complementary, information about the impact of observations on numerical weather forecasts. Moreover, when used together, they reveal both redundancies and dependencies between observing system impacts as observations are added or removed from the data assimilation system. Understanding these dependencies appears to pose an important challenge in making optimal use of the global observing system for numerical weather prediction.
C1 [Gelaro, Ronald] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Zhu, Yanqiu] Sci Applicat Int Corp, Beltsville, MD 20705 USA.
RP Gelaro, R (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
EM ron.gelaro@nasa.gov
FU NASA [MAP/04-0000-0080]
FX The authors thank Ricardo Todling for his development of key components
of the GEOS-5 system and related tools used in this study, and Ron
Errico for his guidance and insightful discussions of this work. We also
acknowledge the efforts of two anonymous reviewers whose comments helped
improve the paper. This work was supported by the Atmospheric Data
Assimilation Development component of the NASA Modeling, Analysis and
Prediction program (MAP/04-0000-0080).
NR 21
TC 44
Z9 44
U1 3
U2 9
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0280-6495
J9 TELLUS A
JI Tellus Ser. A-Dyn. Meteorol. Oceanol.
PD MAR
PY 2009
VL 61
IS 2
BP 179
EP 193
DI 10.1111/j.1600-0870.2008.00388.x
PG 15
WC Meteorology & Atmospheric Sciences; Oceanography
SC Meteorology & Atmospheric Sciences; Oceanography
GA 405XU
UT WOS:000263258300001
ER
PT J
AU Frank, DN
Wysocki, A
Specht-Glick, DD
Rooney, A
Feldman, RA
St Amand, AL
Pace, NR
Trent, JD
AF Frank, Daniel N.
Wysocki, Annette
Specht-Glick, Dee Dee
Rooney, Alejandro
Feldman, Robert A.
St Amand, Allison L.
Pace, Norman R.
Trent, Jonathan D.
TI Microbial diversity in chronic open wounds
SO WOUND REPAIR AND REGENERATION
LA English
DT Article
ID LEG ULCERS; MOLECULAR ANALYSIS; IDENTIFICATION; AMPLIFICATION;
INFECTIONS; ULCERATION; DIAGNOSIS; BIOFILMS; VALIDITY; DISEASE
AB Chronic wounds expose the dermal matrix and underlying tissue to a diversity of microbes from the body and surrounding environment. We determined the microbial diversity of 19 chronic wounds using both molecular methods ( sequence analysis of rRNA genes) and routine clinical culturing methods using swab samples. We identified 93 phylotypes in 2,653 rRNA clone sequences and found that compared with other environments, the microbial diversity of chronic wounds is relatively well characterized, i.e., 95% of sequences have >97% identity with known human commensals. In total, 75% of sequences belonged to four well-known wound-associated phylotypes: Staphylococcus (25%), Corynebacterium (20%), Clostridiales (18%), and Pseudomonas (12%). Approximately 0.5% of sequences ( seven phylotypes) belonged to potentially new species. Individual wound samples contained four to 22 phylotypes, but in all wounds only a few ( one to three) phylotypes were dominant. In more than half the wound specimens, polymerase chain reaction and culturing methods gave different diversity and dominance information about the microbes present. This exploratory study suggests that combining molecular and culturing methods provides a more complete characterization of the microbial diversity of chronic wounds, and can thereby expand our understanding of how microbiology impacts chronic wound pathology and healing.
C1 [Trent, Jonathan D.] NASA, Ames Res Ctr, Bioengn Branch, Moffett Field, CA 94035 USA.
[Frank, Daniel N.; St Amand, Allison L.; Pace, Norman R.] Univ Colorado, Dept Mol Cellular & Dev Biol, Boulder, CO 80309 USA.
[Frank, Daniel N.] Univ Mississippi, Med Ctr, Mucosal & Vaccine Res Program Colorado, Jackson, MS 39216 USA.
[Wysocki, Annette] Univ Mississippi, Med Ctr, Sch Nursing, Jackson, MS 39216 USA.
[Wysocki, Annette] Univ Mississippi, Med Ctr, Div Plast Surg, Dept Surg, Jackson, MS 39216 USA.
[Specht-Glick, Dee Dee] St Patricks Hosp, Wound Care Ctr, Missoula, MT USA.
[Rooney, Alejandro] USDA, Microbial Genom & Bioproc Res Unit, Peoria, IL USA.
[Feldman, Robert A.] SymBio Corp, Menlo Pk, CA USA.
RP Trent, JD (reprint author), NASA, Ames Res Ctr, Bioengn Branch, MS 239-15, Moffett Field, CA 94035 USA.
EM jtrent@mail.arc.nasa.gov
FU DARPA; NIH
FX We dedicate this paper to M. Averner, who provided inspiration for all
aspects of this research. We thank C. Chao, H. Kagawa, and N. Pei for
editorial assistance. We acknowledge J. Bielitzki from DARPA for support
to the Trent lab and NIH for support to the Pace lab.
NR 37
TC 49
Z9 51
U1 0
U2 12
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1067-1927
J9 WOUND REPAIR REGEN
JI Wound Repair Regen.
PD MAR-APR
PY 2009
VL 17
IS 2
BP 163
EP 172
DI 10.1111/j.1524-475X.2009.00472.x
PG 10
WC Cell Biology; Dermatology; Medicine, Research & Experimental; Surgery
SC Cell Biology; Dermatology; Research & Experimental Medicine; Surgery
GA 418ZJ
UT WOS:000264188600003
PM 19320883
ER
PT J
AU Campbell, J
AF Campbell, Joel
TI The Dispersion Relation for the 1/sinh(2) Potential in the Classical
Limit
SO ZEITSCHRIFT FUR NATURFORSCHUNG SECTION A-A JOURNAL OF PHYSICAL SCIENCES
LA English
DT Article
DE Dispersion Relation; Solitons; Sutherland Model
ID MANY-BODY SYSTEM
AB The dispersion relation for the inverse hyperbolic potential is calculated in the classical limit. This is shown for both the low amplitude phonon branch and the high amplitude soliton branch. It is shown that these results qualitatively follow the previously found ones for the inverse squared potential where explicit analytic solutions are known.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Campbell, J (reprint author), NASA, Langley Res Ctr, MS 488, Hampton, VA 23681 USA.
EM joel.f.campbell@nasa.gov
NR 9
TC 0
Z9 0
U1 0
U2 0
PU VERLAG Z NATURFORSCH
PI TUBINGEN
PA POSTFACH 2645, 72016 TUBINGEN, GERMANY
SN 0932-0784
J9 Z NATURFORSCH A
JI Z. Naturfors. Sect. A-J. Phys. Sci.
PD MAR-APR
PY 2009
VL 64
IS 3-4
BP 153
EP 156
PG 4
WC Chemistry, Physical; Physics, Multidisciplinary
SC Chemistry; Physics
GA 455VP
UT WOS:000266795800001
ER
PT J
AU Horikawa, DD
Iwata, KI
Kawai, K
Koseki, S
Okuda, T
Yamamoto, K
AF Horikawa, Daiki D.
Iwata, Ken-Ichi
Kawai, Kiyoshi
Koseki, Shigenobu
Okuda, Takashi
Yamamoto, Kazutaka
TI High Hydrostatic Pressure Tolerance of Four Different Anhydrobiotic
Animal Species
SO ZOOLOGICAL SCIENCE
LA English
DT Article
DE anhydrobiosis; Tardigrada; Nematoda; Chironomidae; Anostraca
ID EUTARDIGRADE RICHTERSIUS-CORONIFER; RADIATION TOLERANCE;
POLYPEDILUM-VANDERPLANKI; TARDIGRADES; TEMPERATURES; TREHALOSE; WATER;
CRYPTOBIOSIS; DEHYDRATION; INSECT
AB High hydrostatic pressure (HHP) can induce physical changes in DNA, proteins, and lipids, causing lethal or sublethal damage to organisms. However, HHP tolerance of animals has not been studied sufficiently. In this study, HHP tolerance of four species of invertebrate anhydrobiotes (the tardigrade Milnesium tardigradum, a nematode species in the family Plectidae, larvae of Polypedilum vanderplanki, and cysts of Artemia franciscana), which have the potential to enter anhydrobiosis upon desiccation, were investigated by exposing them to 1.2 GPa for 20 minutes. This exposure killed the anhydrobiotes in their ordinary hydrated state, but did not affect their survival in the anhydrobiotic state. The results indicated that the hydrated anhydrobiotes were vulnerable to HHP, but that HHP of 1.2 GPa was not sufficient to kill them in anhyrdobiosis.
C1 [Horikawa, Daiki D.] Univ Tokyo, Grad Sch Sci, Bunkyo Ku, Tokyo 1130033, Japan.
[Horikawa, Daiki D.; Iwata, Ken-Ichi; Okuda, Takashi] Natl Inst Agrobiol Sci, Tsukuba, Ibaraki 3058634, Japan.
[Kawai, Kiyoshi; Koseki, Shigenobu; Yamamoto, Kazutaka] Natl Food Res Inst, Tsukuba, Ibaraki 3058642, Japan.
RP Horikawa, DD (reprint author), NASA, Ames Res Ctr, Mail Stop 239-20, Moffett Field, CA 94035 USA.
EM daiki.horikawa-1@nasa.gov
RI Koseki, Shigenobu/J-8317-2012
NR 43
TC 15
Z9 16
U1 2
U2 16
PU ZOOLOGICAL SOC JAPAN
PI TOKYO
PA TOSHIN-BUILDING, HONGO 2-27-2, BUNKYO-KU, TOKYO, 113-0033, JAPAN
SN 0289-0003
J9 ZOOL SCI
JI Zool. Sci.
PD MAR
PY 2009
VL 26
IS 3
BP 238
EP 242
DI 10.2108/zsj.26.238
PG 5
WC Zoology
SC Zoology
GA 434HL
UT WOS:000265265700010
PM 19341346
ER
PT J
AU Benna, M
Acuna, MH
Anderson, BJ
Barabash, S
Boardsen, SA
Gloeckler, G
Gold, RE
Ho, GC
Korth, H
Krimigis, SM
McNutt, RL
Raines, JM
Sarantos, M
Slavin, JA
Solomon, SC
Zhang, TLL
Zurbuchen, TH
AF Benna, Mehdi
Acuna, Mario H.
Anderson, Brian J.
Barabash, Stanislav
Boardsen, Scott A.
Gloeckler, George
Gold, Robert E.
Ho, George C.
Korth, Haje
Krimigis, Stamatios M.
McNutt, Ralph L., Jr.
Raines, Jim M.
Sarantos, Menelaos
Slavin, James A.
Solomon, Sean C.
Zhang, Tielong L.
Zurbuchen, Thomas H.
TI Modeling the response of the induced magnetosphere of Venus to changing
IMF direction using MESSENGER and Venus Express observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ESCAPE
AB The second MESSENGER flyby of Venus on 5 June 2007 provided a new opportunity to study the response of the induced magnetosphere of the planet to changes in the direction of the interplanetary magnetic field (IMF). At the time of the MESSENGER flyby, the European Space Agency's Venus Express spacecraft was located outside the magnetosphere and provided a monitor of solar wind conditions. Measurements by the Venus Express magnetometer show that the IMF underwent four major changes in direction and magnitude while MESSENGER was traveling through the inner magnetosphere of Venus. The response of the magnetosphere to each of these IMF changes was determined with a semi-time-dependant global magnetohydrodynamic (MHD) model, and the results were compared with magnetic and compositional measurements by the Magnetometer (MAG) and the Energetic Particle and Plasma Spectrometer (EPPS) on MESSENGER. Our modeling results show that this semi-time-dependant MHD technique produces magnetic field profiles that can account for both of the field reversals seen by MAG and the peak in the pick-up ion density measured by EPPS. Moreover, these results reveal that the plasma sheet that confines most of the pick-up ions has a barred disk shape and continuously rotates along the Sun-planet axis to align its smallest dimension with the transverse direction of the IMF. Citation: Benna, M., et al. (2009), Modeling the response of the induced magnetosphere of Venus to changing IMF direction using MESSENGER and Venus Express observations, Geophys. Res. Lett., 36, L04109, doi:10.1029/2008GL036718.
C1 [Benna, Mehdi; Acuna, Mario H.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Anderson, Brian J.; Gold, Robert E.; Ho, George C.; Korth, Haje; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Barabash, Stanislav] Swedish Inst Space Phys, SE-98128 Kiruna, Sweden.
[Boardsen, Scott A.; Sarantos, Menelaos; Slavin, James A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Gloeckler, George; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Slavin, James A.; Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Zhang, Tielong L.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
RP Benna, M (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM mehdi.benna@nasa.gov
RI Anderson, Brian/I-8615-2012; Slavin, James/H-3170-2012; Sarantos,
Menelaos/H-8136-2013; McNutt, Ralph/E-8006-2010; Ho, George/G-3650-2015;
Benna, Mehdi/F-3489-2012
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166;
Ho, George/0000-0003-1093-2066;
FU NASA [NNX07AR61G]; NASA Discovery Program [NASW-00002]; Carnegie
Institution of Washington [NAS5-97271]
FX This work has been supported by NASA under MESSENGER Participating
Scientist grant NNX07AR61G. The MESSENGER project is supported by the
NASA Discovery Program under contracts NASW-00002 to the Carnegie
Institution of Washington and NAS5-97271 to the Johns Hopkins University
Applied Physics Laboratory. Calculations were carried out on the
high-performance computing resources of the NASA Center for
Computational Sciences. The authors thank the teams of both MESSENGER
and Venus Express for making this rendezvous at Venus a success.
NR 13
TC 3
Z9 3
U1 1
U2 2
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 28
PY 2009
VL 36
AR L04109
DI 10.1029/2008GL036718
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 412NN
UT WOS:000263731600002
ER
PT J
AU Limpasuvan, V
Wu, DL
AF Limpasuvan, Varavut
Wu, Dong L.
TI Anomalous two-day wave behavior during the 2006 austral summer
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID RESOLUTION DOPPLER IMAGER; BAROCLINIC INSTABILITY; QUASI-2-DAY WAVE;
TEMPERATURE; MESOSPHERE; UARS; STRATOPAUSE; MLS
AB An anomalous behavior of the two-day wave is observed during the 2006 Austral Summer in the mesospheric temperature and line-of-sight wind, retrieved from the Microwave Limb Sounder (MLS) aboard NASA's Earth Observing System (EOS) Aura mission. During January 2006, the wave appears to exist in an unusually strong summer easterly jet, and its spectral signature spreads over a broader range of zonal wavenumber and frequency. In addition to the typical wavenumber 3 component, a wavenumber 2 disturbance with a near 2-day period is also evident, traveling westward at similar phase speed. The wavenumber 3 component exhibits the previously observed dual characteristics of both a normal and an instability mode, while the wavenumber 2 feature appears to be an instability mode, in agreement with recent theoretical calculations. Citation: Limpasuvan, V., and D. L. Wu (2009), Anomalous two-day wave behavior during the 2006 austral summer, Geophys. Res. Lett., 36, L04807, doi:10.1029/2008GL036387.
C1 [Limpasuvan, Varavut] Coastal Carolina Univ, Dept Chem & Phys, Conway, SC 29528 USA.
[Wu, Dong L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Limpasuvan, V (reprint author), Coastal Carolina Univ, Dept Chem & Phys, POB 251954, Conway, SC 29528 USA.
EM var@coastal.edu
RI Limpasuvan, Varavut/K-6266-2013; Wu, Dong/D-5375-2012
NR 22
TC 31
Z9 31
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 FEB 28
PY 2009
VL 36
AR L04807
DI 10.1029/2008GL036387
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 412NN
UT WOS:000263731600001
ER
PT J
AU Owen, T
Niemann, HB
AF Owen, Tobias
Niemann, H. B.
TI The origin of Titan's atmosphere: some recent advances
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Review
DE origin; atmosphere; composition; noble gases; deuterium
ID HUYGENS PROBE; NOBLE-GASES; NITROGEN; JUPITER; ABUNDANCES;
PLANETESIMALS; CONSTRAINTS; VOLATILES; DEUTERIUM; EVOLUTION
AB It is possible to make a consistent story for the origin of Titan's atmosphere starting with the birth of Titan in the Saturn subnebula. If we use comet nuclei as a model, Titan's nitrogen and methane could have easily been delivered by the ice that makes up approximately 50 per cent of its mass. If Titan's atmospheric hydrogen is derived from that ice, it is possible that Titan and comet nuclei are in fact made of the same protosolar ice. The noble gas abundances are consistent with relative abundances found in the atmospheres of Mars and Earth, the Sun, and the meteorites.
C1 [Owen, Tobias] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Niemann, H. B.] Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
RP Owen, T (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM owen@ifa.hawaii.edu
NR 37
TC 12
Z9 12
U1 1
U2 12
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 28
PY 2009
VL 367
IS 1889
BP 607
EP 615
DI 10.1098/rsta.2008.0247
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 396MH
UT WOS:000262595300002
PM 19019783
ER
PT J
AU Flasar, FM
Achterberg, RK
AF Flasar, F. M.
Achterberg, R. K.
TI The structure and dynamics of Titan's middle atmosphere
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Review
DE Titan; middle atmosphere; dynamics; temperatures
ID COMPOSITE INFRARED SPECTROMETER; LATITUDINAL VARIATIONS;
GENERAL-CIRCULATION; SEASONAL-VARIATIONS; THERMAL STRUCTURE; SATURN
SYSTEM; STRATOSPHERE; SPECTRA; TEMPERATURE; VORTEX
AB Titan's middle atmosphere is characterized by cyclostrophic winds and strong seasonal modulation. Cassini CIRS observations, obtained in northern winter, indicate that the stratosphere near 1 mbar is warmest at low latitudes, with the South Pole a few degrees colder and the North Pole approximately 20 K colder. Associated with the cold northern temperatures are strong circumpolar winds with speeds as high as 190 m s(-1). Within this vortex, the mixing ratios of several organic gases are enhanced relative to those at low latitudes. Comparison with Voyager thermal infrared measurements, obtained 25 years ago in northern spring, suggests that the enhancement currently observed will increase as the winter progresses. The stratopause height increases from 0.1 mbar near the equator to 0.01 mbar near the North Pole, where it is the warmest part of the atmosphere, greater than 200 K. This implies subsidence at the pole, which is consistent with the enhanced organics observed. Condensate features, several still not identified, are also apparent in the infrared spectra at high northern latitudes. In many ways, the winter vortex observed on Titan, with cyclostrophic winds, resembles the polar winter vortices on the Earth, where the mean winds are geostrophic.
C1 [Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Achterberg, R. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Flasar, FM (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA.
EM f.m.flasar@nasa.gov
RI Flasar, F Michael/C-8509-2012
NR 60
TC 15
Z9 15
U1 1
U2 7
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 28
PY 2009
VL 367
IS 1889
BP 649
EP 664
DI 10.1098/rsta.2008.0242
PG 16
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 396MH
UT WOS:000262595300005
PM 19073460
ER
PT J
AU Chaubell, J
Bruno, OP
Ao, CO
AF Chaubell, Julian
Bruno, Oscar P.
Ao, Chi O.
TI Evaluation of EM-wave propagation in fully three-dimensional atmospheric
refractive index distributions
SO RADIO SCIENCE
LA English
DT Article
ID RADIO OCCULTATION SIGNALS; RANDOM-MEDIA; NUMERICAL-SIMULATION;
HETEROGENEOUS MEDIA; RYTOV APPROXIMATION; LOWER TROPOSPHERE; VALIDITY;
EQUATION
AB We present a novel numerical method, based on high-frequency localization, for evaluation of electromagnetic-wave propagation through atmospheres exhibiting fully three-dimensional (height, range and cross-range) refractive index variations. This methodology, which is based on localization of Rytov-integration domains to small tubes around geometrical optics paths, can accurately solve three-dimensional propagation problems in orders-of-magnitude shorter computing times than other algorithms available presently. For example, the proposed approach can accurately produce solutions for propagation of approximate to 20 cm GPS signals across hundreds of kilometers of realistic, three-dimensional atmospheres in computing times on the order of 1 hour in a present-day single-processor workstation, a task for which other algorithms would require, in such single-processor computers, computing times on the order of several months.
C1 [Chaubell, Julian; Ao, Chi O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Chaubell, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM julian@jpl.nasa.gov
FU Air Force Office of Scientific Research; National Science Foundation;
National Aeronautics and Space Administration; Julian Chaubell held a
National Research Council Research Associateship; Jet Propulsion
Laboratory
FX This work was supported in part by the Air Force Office of Scientific
Research, the National Science Foundation and the National Aeronautics
and Space Administration. This research was performed, in part, while
Julian Chaubell held a National Research Council Research Associateship
Award at Jet Propulsion Laboratory.
NR 28
TC 0
Z9 0
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
J9 RADIO SCI
JI Radio Sci.
PD FEB 28
PY 2009
VL 44
AR RS1012
DI 10.1029/2008RS003882
PG 19
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA 412QQ
UT WOS:000263739700002
ER
PT J
AU Rinsland, CP
Mahieu, E
Chiou, L
Herbin, H
AF Rinsland, Curtis P.
Mahieu, Emmanuel
Chiou, Linda
Herbin, Herve
TI First ground-based infrared solar absorption measurements of free
tropospheric methanol (CH3OH): Multidecade infrared time series from
Kitt Peak (31.9 degrees N 111.6 degrees W): Trend, seasonal cycle, and
comparison with previous measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ORGANIC PEROXY-RADICALS; NONMETHANE HYDROCARBONS; CARBON-MONOXIDE; ERROR
ANALYSIS; OZONE; MODEL; EMISSIONS; NORTHERN; CO
AB Atmospheric CH3OH (methanol) free tropospheric (2.09-14-km altitude) time series spanning 22 years has been analyzed on the basis of high-spectral resolution infrared solar absorption spectra of the strong nu(8) band recorded from the U. S. National Solar Observatory on Kitt Peak (latitude 31.9 degrees N, 111.6 degrees W, 2.09-km altitude) with a 1-m Fourier transform spectrometer (FTS). The measurements span October 1981 to December 2003 and are the first long time series of CH3OH measurements obtained from the ground. The results were analyzed with SFIT2 version 3.93 and show a factor of three variations with season, a maximum at the beginning of July, a winter minimum, and no statistically significant long-term trend over the measurement time span.
C1 [Rinsland, Curtis P.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Mahieu, Emmanuel] Univ Liege, Inst Astrophys & Geophys, B-4000 Cointe Ougree, Belgium.
[Herbin, Herve] Univ Sci & Technol Lille, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France.
[Chiou, Linda] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, Mail Stop 401A, Hampton, VA 23681 USA.
EM c.p.rinsland@larc.nasa.gov; emmanuel.mahieu@ulg.ac.be;
linda.s.chiou@nasa.gov; herve.herbin@univ-lille1.fr
FU NASA's Upper Atmospheric Chemistry and Modeling Program (ACMAP); Upper
Atmosphere Research Program (UARP); "Actions de Recherche Concertees"
(Communaute Francaise de Belgique)
FX The infrared solar absorption spectra were recorded with the U. S.
National Solar Observatory (NSO) Fourier transform spectrometer.
Analysis of the ACE spectra at the NASA Langley Research Center was
supported by NASA's Upper Atmospheric Chemistry and Modeling Program
(ACMAP) and Upper Atmosphere Research Program (UARP). Emmanuel Mahieu
was primarily supported by the Belgian Federal Science Policy Office
(PRODEX and SSD Programmes), Brussels. Financial support by the "Actions
de Recherche Concertees" (Communaute Francaise de Belgique) is also
acknowledged. We thank Gaelle Dufour of the Laboratoire de Meteorologie
Dynamique/Institut Pierre Simon Laplace, Palaiseau, France, for
suggestions that improve our manuscript.
NR 41
TC 7
Z9 7
U1 1
U2 3
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 27
PY 2009
VL 114
AR D04309
DI 10.1029/2008JD011003
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 412OC
UT WOS:000263733100006
ER
PT J
AU Wu, JB
Del Genio, AD
Yao, MS
Wolf, AB
AF Wu, Jingbo
Del Genio, Anthony D.
Yao, Mao-Sung
Wolf, Audrey B.
TI WRF and GISS SCM simulations of convective updraft properties during
TWP-ICE
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID INTERNATIONAL CLOUD EXPERIMENT; HIGH-RESOLUTION SIMULATION; CUMULUS
CONVECTION; BULK PARAMETERIZATION; TROPICAL CONVECTION; DEEP CONVECTION;
PART I; MODEL; SENSITIVITY; MICROPHYSICS
AB The Weather Research and Forecasting (WRF) model, running at cloud-resolving model resolution (1.3 km and 0.6 km), is used to simulate cumulus updraft speeds associated with three distinct convective regimes sampled during the intensive observing period of the Tropical Warm Pool-International Cloud Experiment (TWP-ICE) near Darwin, Australia. The WRF model produces strong updrafts during a monsoon break period and weaker updrafts during an active monsoon period, consistent with observational proxies of convective strength. It also captures the observed feature of midlevel convection during a suppressed monsoon period. The ability of the WRF model to differentiate the updraft speeds among three subperiods is robust to changes in its microphysics and turbulence schemes, resolution, and forcing procedure. For comparison to the parameterized diagnostic updraft speeds in the Goddard Institute for Space Studies Single Column Model (GISS SCM), we define an equivalent mean updraft speed for deep convection in the WRF simulation as the ratio of the domain average upward flux of hydrometeors to the domain average hydrometeor water content. Parameterized convective updraft speeds diagnosed from the thermodynamic structure in the SCM can reproduce the WRF difference between the active and break period updraft strength and the shallower suppressed monsoon convection, but only if a free parameter that regulates entrainment strength is allowed to vary. SCM updraft speeds are consistently too strong in the upper troposphere compared with the WRF. Hydrometeor profiles in both the WRF and the SCM are sensitive to assumptions about the ice phase microphysics.
C1 [Wu, Jingbo] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
[Del Genio, Anthony D.; Yao, Mao-Sung] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Wolf, Audrey B.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA.
RP Wu, JB (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
EM jwu@giss.nasa.gov
RI Del Genio, Anthony/D-4663-2012
OI Del Genio, Anthony/0000-0001-7450-1359
FU DOE Atmospheric Radiation Measurement Program; NASA
FX This work was supported by the DOE Atmospheric Radiation Measurement
Program, NASA Precipitation Measurement Missions Program, and NASA
Modeling and Analysis Program. We thank Ann Fridlind, Jay Mace, Peter
May, and Shaocheng Xie for helpful discussions about the TWP-ICE data
and three reviewers for constructive comments.
NR 53
TC 31
Z9 31
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 27
PY 2009
VL 114
AR D04206
DI 10.1029/2008JD010851
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 412OC
UT WOS:000263733100004
ER
PT J
AU Kellogg, PJ
Goetz, K
Monson, SJ
Bale, SD
Reiner, MJ
Maksimovic, M
AF Kellogg, P. J.
Goetz, K.
Monson, S. J.
Bale, S. D.
Reiner, M. J.
Maksimovic, Milan
TI Plasma wave measurements with STEREO S/WAVES: Calibration, potential
model, and preliminary results
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND FLUCTUATIONS; ION RESONANT WAVES; PHOTOELECTRON SHEATH;
CASSINI OBSERVATIONS; DENSITY PROFILE; ELECTRIC-FIELD; SPACECRAFT;
CONVERSION; ISOTROPY; PHOTOEMISSION
AB The S/WAVES experiments on the two STEREO spacecraft measure waves, both in situ plasma waves and remotely generated waves such as Type II and Type III solar bursts. A part of the experiment is aimed at understanding the generation of electromagnetic waves from electrostatic Langmuir waves. For this, rapid measurements of plasma density, sufficiently rapid to be on the time scale of Langmuir wave fluctuations, are deemed necessary. Measurements of the potential of the antennas relative to the spacecraft can supply these rapid measurements. The antennas were not provided with a bias current, and so this unbiased technique has not been used previously. However, the cylindrical antennas of S/WAVES respond to temperature as well as the density of the ambient plasma, giving five quantities, n(e), T-e, and 3 components of E, to be determined from the three measurements of antenna potential. The work presented here discusses the analysis and interpretation of these measurements from the early part of the mission, when there were frequent observations of foreshock Langmuir waves to use for calibration. A model of the photoemission-plasma equilibrium has been constructed, using these and other measurements. It is shown that the response to one or a few of the five quantities may be negligible, depending on the phenomenon observed, so that useful measurements are obtained of the others. Application to observation and analysis of various plasma wave phenomena will be discussed.
C1 [Kellogg, P. J.; Goetz, K.; Monson, S. J.] Univ Minnesota Twin Cities, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Reiner, M. J.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Reiner, M. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Maksimovic, Milan] Observ Paris, Sect Meudon, LESIA, F-92195 Meudon, France.
RP Kellogg, PJ (reprint author), Univ Minnesota Twin Cities, Sch Phys & Astron, Minneapolis, MN 55455 USA.
EM kellogg@waves.space.umn.edu
RI Bale, Stuart/E-7533-2011
OI Bale, Stuart/0000-0002-1989-3596
FU National Aeronautics and Space Administration [NNX07AF23G]; University
of California [NXX06AF25G]; CNES; CNRS
FX Work at the University of Minnesota was supported by the National
Aeronautics and Space Administration under grant NNX07AF23G and at the
University of California under grant NXX06AF25G. The work at
Observatoire Paris-Meudon was supported by the French agencies CNES and
CNRS. The authors thank K.O. Ogilvie at GSFC Code 692 and R. Lin at UC
Berkeley and CDAWeb for Wind data used in determining photoemission
spectra, C. T. Russell and J. G. Luhmann for promptly making STEREO
IMPACT magnetic field data available, and the editors of The
Astrophysical Journal for permission to use Figure 14.
NR 44
TC 27
Z9 27
U1 0
U2 1
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 27
PY 2009
VL 114
AR A02107
DI 10.1029/2008JA013566
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 412QA
UT WOS:000263738100002
ER
PT J
AU Soibel, A
Wright, MW
Farr, W
Keo, S
Hill, C
Yang, RQ
Liu, HC
AF Soibel, A.
Wright, M. W.
Farr, W.
Keo, S.
Hill, C.
Yang, R. Q.
Liu, H. C.
TI High-speed operation of interband cascade lasers
SO ELECTRONICS LETTERS
LA English
DT Article
AB High-speed interband cascade lasers have been fabricated and the. first experimental evidence that these devices can be directly modulated at a frequency of 3.2 GHz and above is reported.
C1 [Soibel, A.; Wright, M. W.; Farr, W.; Keo, S.; Hill, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Yang, R. Q.] Univ Oklahoma, Sch Elect & Comp Engn, Norman, OK 73019 USA.
[Liu, H. C.] Natl Res Council Canada, Inst Microstruct Sci, Ottawa, ON K1A 0R6, Canada.
RP Soibel, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM asoibel@jpl.nasa.gov
RI Soibel, Alexander/A-1313-2007
FU Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration ( NASA).
FX The authors are grateful to M. Shaw, J. Bueno and P. M. Echternach for
their help with RF measurements, to A. Ksendzov for assistance with
oxide deposition and to H. Hemmati, S. Forouhar, S. D. Gunapala, J. A.
North, L. G. Gref and R. T. Odle for their support and encouragement.
The research described in this Letter was performed at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration ( NASA).
NR 10
TC 4
Z9 5
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 FEB 26
PY 2009
VL 45
IS 5
BP 264
EP U40
DI 10.1049/el:20090079
PG 2
WC Engineering, Electrical & Electronic
SC Engineering
GA 413IA
UT WOS:000263785600017
ER
PT J
AU Sarantos, M
Slavin, JA
AF Sarantos, Menelaos
Slavin, James A.
TI On the possible formation of Alfven wings at Mercury during encounters
with coronal mass ejections
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MAGNETOSPHERE; SURFACE; EXOSPHERE; CONDUCTIVITY; SATELLITES; PLASMA
AB The solar wind conditions near Mercury's perihelion, especially during Interplanetary Coronal Mass Ejection (ICME) events, will often be characterized by very low Alfven Mach number (<= 3). We suggest that the low Mach numbers and large north-south magnetic fields during ICMEs will lead to the formation of "Alfven wings'' that will affect the configuration of the Hermean magnetosphere. It is shown that an electrical conductance threshold of about 5 S, comparable to the Alfven conductance in the solar wind, is required for generation of Alfven wings at Mercury. Assuming crustal conductances above this value it is demonstrated that currents in the Alfven wings and closing across the planetary surface will produce significant perturbations (>= 10 nT) of the magnetospheric magnetic field. Citation: Sarantos, M., and J. A. Slavin (2009), On the possible formation of Alfven wings at Mercury during encounters with coronal mass ejections, Geophys. Res. Lett., 36, L04107, doi: 10.1029/2008GL036747.
C1 [Sarantos, Menelaos; Slavin, James A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Sarantos, M (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
EM menelaos.sarantos-1@nasa.gov
RI Slavin, James/H-3170-2012; Sarantos, Menelaos/H-8136-2013
OI Slavin, James/0000-0002-9206-724X;
FU NASA Postdoctoral Program (NPP) Fellowship
FX M.S. was supported by the NASA Postdoctoral Program (NPP) Fellowship.
NR 19
TC 5
Z9 5
U1 1
U2 3
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 26
PY 2009
VL 36
AR L04107
DI 10.1029/2008GL036747
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 412NC
UT WOS:000263730500003
ER
PT J
AU Omidi, N
Phan, T
Sibeck, DG
AF Omidi, N.
Phan, T.
Sibeck, D. G.
TI Hybrid simulations of magnetic reconnection initiated in the
magnetosheath
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EARTHS BOW SHOCK; SOLAR-WIND; DISCONTINUITIES; FIELD
AB Interaction of solar wind tangential discontinuities (TDs) with the bow shock may initiate reconnection in the magnetosheath. We employ 2.5-D electromagnetic, hybrid simulations that treat the ions kinetically via particle-in-cell methods and the electrons as a massless fluid to study this interaction. We present results from eight runs corresponding to TD thicknesses ranging from 10 to 260 ion skin depths and shear angles ranging from 120 degrees to 180 degrees. Our results indicate a transition from time-dependent to steady state reconnection as the thickness of the solar wind TD increases above 30 ion skin depths. As the shear angle in the magnetic field decreases, it takes longer to initiate reconnection, and reconnection jet speeds diminish, suggesting a lower reconnection rate. Implications of these results for magnetic reconnection at currents sheets in general and at the magnetopause in particular are also discussed.
C1 [Omidi, N.] Solana Sci Inc, Solana Beach, CA 92075 USA.
[Phan, T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Omidi, N (reprint author), Solana Sci Inc, 777 S Pacific Coast Highway,208, Solana Beach, CA 92075 USA.
EM omidi@solanasci.com
RI Sibeck, David/D-4424-2012
FU NSF [ATM-0502992]; RTOP [955518.02.01.02.29]; Dynamics of the Bow Shock
FX Work for this project was supported by NSF grant ATM-0502992 to Solana
Scientific Inc. Work by D. G. Sibeck was funded by RTOP
955518.02.01.02.29, Dynamics of the Bow Shock.
NR 20
TC 9
Z9 10
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB 26
PY 2009
VL 114
AR A02222
DI 10.1029/2008JA013647
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 412PZ
UT WOS:000263738000001
ER
PT J
AU Pieters, CM
Boardman, J
Buratti, B
Chatterjee, A
Clark, R
Glavich, T
Green, R
Head, J
Isaacson, P
Malaret, E
McCord, T
Mustard, J
Petro, N
Runyon, C
Staid, M
Sunshine, J
Taylor, L
Tompkins, S
Varanasi, P
White, M
AF Pieters, Carle M.
Boardman, Joseph
Buratti, Bonnie
Chatterjee, Alok
Clark, Roger
Glavich, Tom
Green, Robert
Head, James, III
Isaacson, Peter
Malaret, Erick
McCord, Thomas
Mustard, John
Petro, Noah
Runyon, Cassandra
Staid, Matthew
Sunshine, Jessica
Taylor, Lawrence
Tompkins, Stefanie
Varanasi, Padma
White, Mary
TI The Moon Mineralogy Mapper (M-3) on Chandrayaan-1
SO CURRENT SCIENCE
LA English
DT Article
DE Imaging spectrometer; lunar composition; mineralogy
AB The Moon Mineralogy Mapper (M-3) is a NASA-supported guest instrument on ISRO's remote sensing mission to Moon, Chandrayaan-1. The M-3 is an imaging spectrometer that operates from the visible into the near-infrared (0.42-3.0 mu m) where highly diagnostic mineral absorption bands occur. Over the course of the mission M-3 will provide low resolution spectroscopic data for the entire lunar surface at 140 m/pixel (86 spectral channels) to be used as a base-map and high spectral resolution science data (80 m/pixel; 260 spectral channels) for 25-50% of the surface. The detailed mineral assessment of different lunar terrains provided by M-3 is principal information needed for understanding the geologic evolution of the lunar crust and lays the foundation for focused future in-depth exploration of the Moon.
C1 [Pieters, Carle M.; Head, James, III; Isaacson, Peter; Mustard, John] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Boardman, Joseph] Analyt Imaging & Geophys LLC, Boulder, CO USA.
[Buratti, Bonnie; Chatterjee, Alok; Glavich, Tom; Green, Robert; Varanasi, Padma; White, Mary] Jet Prop Lab, Pasadena, CA 91109 USA.
[Clark, Roger] US Geol Survey, Denver, CO 80225 USA.
[McCord, Thomas] Bear Fight Ctr, Winthrop, WA 98862 USA.
[Petro, Noah] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Runyon, Cassandra] Coll Charleston, Charleston, SC 29424 USA.
[Staid, Matthew] PSI, Tucson, AZ 85719 USA.
[Sunshine, Jessica] Univ Maryland, Baltimore, MD 21201 USA.
[Taylor, Lawrence] Univ Tennessee, Knoxville, TN 37996 USA.
RP Pieters, CM (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
EM Carle_Pieters@brown.edu
NR 9
TC 86
Z9 95
U1 1
U2 18
PU INDIAN ACAD SCIENCES
PI BANGALORE
PA C V RAMAN AVENUE, SADASHIVANAGAR, P B #8005, BANGALORE 560 080, INDIA
SN 0011-3891
J9 CURR SCI INDIA
JI Curr. Sci.
PD FEB 25
PY 2009
VL 96
IS 4
BP 500
EP 505
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 416PS
UT WOS:000264018600028
ER
PT J
AU Spudis, P
Nozette, S
Bussey, B
Raney, K
Winters, H
Lichtenberg, CL
Marinelli, W
Crusan, JC
Gates, MM
AF Spudis, Paul
Nozette, Stewart
Bussey, Ben
Raney, Keith
Winters, Helene
Lichtenberg, Christopher L.
Marinelli, William
Crusan, Jason C.
Gates, Michele M.
TI Mini-SAR: an imaging radar experiment for the Chandrayaan-1 mission to
the Moon
SO CURRENT SCIENCE
LA English
DT Article
DE Ice; Moon; poles; radar; SAR
ID LUNAR SOUTH-POLE; ICE; DEPOSITS
AB Mini-SAR is a single frequency (S-band; 13-cm wave-length) Synthetic Aperture Radar (SAR) in a lightweight (similar to 9 kg) package. Previous Earth- and space-based radar observations of the permanently shadowed regions of the lunar poles have measured areas of high circular polarization ratio consistent with volume scattering from water ice buried at shallow (0.1-1 m) depths. This detection is not definitive because of poor viewing geometry and a limited number of observations. Mini-SAR utilizes a unique hybrid polarization architecture, which allows determination of the Stokes parameters of the reflected signal, intended to distinguish volume scattering (caused by the presence of ice) from other scattering mechanisms (e. g. sub-wavelength scale surface roughness).
C1 [Spudis, Paul; Nozette, Stewart] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Bussey, Ben; Raney, Keith; Winters, Helene] Appl Phys Lab, Laurel, MD 20723 USA.
[Lichtenberg, Christopher L.] USN, Air Warfare Ctr, China Lake, CA 93555 USA.
[Marinelli, William; Crusan, Jason C.; Gates, Michele M.] NASA, Washington, DC 20546 USA.
RP Spudis, P (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
EM spudis@lpi.usra.edu
FU Lunar and Planetary Institute Contribution [1444]
FX We thank NASA's Spaceflight Operations Mission Directorate and the
Exploration Systems Mission Directorate, and the Department of Defense
for supporting the Mini-SAR project. This paper is Lunar and Planetary
Institute Contribution Number 1444.
NR 14
TC 19
Z9 23
U1 0
U2 5
PU INDIAN ACAD SCIENCES
PI BANGALORE
PA C V RAMAN AVENUE, SADASHIVANAGAR, P B #8005, BANGALORE 560 080, INDIA
SN 0011-3891
J9 CURR SCI INDIA
JI Curr. Sci.
PD FEB 25
PY 2009
VL 96
IS 4
BP 533
EP 539
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 416PS
UT WOS:000264018600034
ER
PT J
AU von Frese, RRB
Potts, LV
Wells, SB
Leftwich, TE
Kim, HR
Kim, JW
Golynsky, AV
Hernandez, O
Gaya-Pique, LR
AF von Frese, Ralph R. B.
Potts, Laramie V.
Wells, Stuart B.
Leftwich, Timothy E.
Kim, Hyung Rae
Kim, Jeong Woo
Golynsky, Alexander V.
Hernandez, Orlando
Gaya-Pique, Luis R.
TI GRACE gravity evidence for an impact basin in Wilkes Land, Antarctica
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
DE megaimpact; GRACE; Antarctica
ID PERMIAN-TRIASSIC BOUNDARY; CORRELATED FREE-AIR; DOUBLE MASS EXTINCTION;
MARS GLOBAL SURVEYOR; NORTHWESTERN AUSTRALIA; CRUSTAL THICKNESS; TERRAIN
GRAVITY; FLOOD BASALTS; CRATER; ANOMALIES
AB New details on the east Antarctic gravity field from the Gravity Recovery and Climate Experiment (GRACE) mission reveal a prominent positive free-air gravity anomaly over a roughly 500-km diameter subglacial basin centered on (70 degrees S, 120 degrees E) in north central Wilkes Land. This regional inverse correlation between topography and gravity is quantitatively consistent with thinned crust from a giant meteorite impact underlain by an isostatically disturbed mantle plug. The inferred impact crater is nearly three times the size of the Chicxulub crater and presumably formed before the Cretaceous formation of the east Antarctic coast that cuts the projected ring faults. It extensively thinned and disrupted the Wilkes Land crust where the Kerguelen hot spot and Gondwana rifting developed but left the adjacent Australian block relatively undisturbed. The micrometeorite and fossil evidence suggests that the impact may have occurred at the beginning of the greatest extinction of life on Earth at similar to 260 Ma when the Siberian Traps were effectively antipodal to it. Antipodal volcanism is common to large impact craters of the Moon and Mars and may also account for the antipodal relationships of essentially half of the Earth's large igneous provinces and hot spots. Thus, the impact may have triggered the "Great Dying'' at the end of the Permian and contributed to the development of the hot spot that produced the Siberian Traps and now may underlie Iceland. The glacial ice up to a few kilometers thick that has covered the crater for the past 30-40 Ma poses formidable difficulties to sampling the subglacial geology. Thus, the most expedient and viable test of the prospective crater is to survey it for relevant airborne gravity and magnetic anomalies.
C1 [von Frese, Ralph R. B.; Kim, Jeong Woo; Hernandez, Orlando; Gaya-Pique, Luis R.] Ohio State Univ, Byrd Polar Res Ctr, Sch Earth Sci, Columbus, OH 43210 USA.
[von Frese, Ralph R. B.; Potts, Laramie V.] Ohio State Univ, Lab Space Geodesy & Remote Sensing Res, Columbus, OH 43210 USA.
[Potts, Laramie V.] New Jersey Inst Technol, Dept Engn Technol, Newark, NJ 07102 USA.
[Kim, Hyung Rae] Kongju Natl Univ, Dept Geoenvironm Sci, Kong Ju 314701, Chungnam Do, South Korea.
[Kim, Hyung Rae] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Kim, Jeong Woo] Univ Calgary, Dept Geomat Engn, Calgary, AB T2N 1N4, Canada.
[Golynsky, Alexander V.] VNIIOkeangeol, Dept Antarctic Geol, St Petersburg 190121, Russia.
[Hernandez, Orlando] Univ Nacl Colombia, Dept Geosci, Bogota, Colombia.
[Gaya-Pique, Luis R.] CNRS, IPGS, Equipe Geomagnetisme, F-75005 Paris, France.
RP von Frese, RRB (reprint author), Ohio State Univ, Byrd Polar Res Ctr, Sch Earth Sci, Columbus, OH 43210 USA.
EM vonfrese@geology.ohio-state.edu
FU U.S. National Science Foundation(NSF) [OPP 0338005]; Ohio Supercomputer
Center at Ohio State University; Goddard Earth Sciences and Technology
Center Research Fellowship
FX The Office of Polar Programs of the U.S. National Science Foundation
under research grant NSF-OPP 0338005, the Ohio Supercomputer Center at
Ohio State University, and the Goddard Earth Sciences and Technology
Center Research Fellowship awarded to HRK supported elements of this
research. We thank two anonymous reviewers for their constructive
comments.
NR 68
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD FEB 25
PY 2009
VL 10
AR Q02014
DI 10.1029/2008GC002149
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 412MQ
UT WOS:000263729300001
ER
PT J
AU Parrington, M
Jones, DBA
Bowman, KW
Thompson, AM
Tarasick, DW
Merrill, J
Oltmans, SJ
Leblanc, T
Witte, JC
Millet, DB
AF Parrington, M.
Jones, D. B. A.
Bowman, K. W.
Thompson, A. M.
Tarasick, D. W.
Merrill, J.
Oltmans, S. J.
Leblanc, T.
Witte, J. C.
Millet, D. B.
TI Impact of the assimilation of ozone from the Tropospheric Emission
Spectrometer on surface ozone across North America
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID UNITED-STATES
AB We examine the impact of assimilating ozone observations from the Tropospheric Emission Spectrometer (TES) on North American surface ozone abundances in the GEOS-Chem model in August 2006. The assimilation reduces the negative bias in the modeled free tropospheric ozone, which enhances the ozone flux into the boundary layer. Surface ozone abundances increased by as much as 9 ppb in western North America and by less than 2 ppb in the southeast, resulting in a total background source of ozone of 20-40 ppb. The enhanced ozone in the model reduced the model bias with respect to surface ozone observations in the western USA, but exacerbated it in the east. This increase in the bias in the boundary layer in the east, despite the agreement between the assimilation and ozonesonde measurements in the free troposphere, suggests errors in the ozone sources or sinks or in boundary layer mixing in the model. Citation: Parrington, M., D. B. A. Jones, K. W. Bowman, A. M. Thompson, D. W. Tarasick, J. Merrill, S. J. Oltmans, T. Leblanc, J. C. Witte, and D. B. Millet ( 2009), Impact of the assimilation of ozone from the Tropospheric Emission Spectrometer on surface ozone across North America, Geophys. Res. Lett., 36, L04802, doi: 10.1029/2008GL036935.
C1 [Parrington, M.; Jones, D. B. A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Bowman, K. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Thompson, A. M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Tarasick, D. W.] Meteorol Serv Ctr, Downsview, ON, Canada.
[Merrill, J.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02881 USA.
[Oltmans, S. J.] NOAA, Climate Monitoring & Diagnost Lab, Boulder, CO 80303 USA.
[Leblanc, T.] CALTECH, Table Mt Facil, Jet Prop Lab, Wrightwood, CA 92397 USA.
[Witte, J. C.] Sci Syst & Applicat Inc, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Millet, D. B.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA.
RP Parrington, M (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada.
EM mark.parrington@utoronto.ca
RI Millet, Dylan/G-5832-2012; Parrington, Mark/E-7148-2013; Jones,
Dylan/O-2475-2014; Chem, GEOS/C-5595-2014; Thompson, Anne /C-3649-2014;
OI Parrington, Mark/0000-0003-4313-6218; Jones, Dylan/0000-0002-1935-3725;
Thompson, Anne /0000-0002-7829-0920; Tarasick, David/0000-0001-9869-0692
FU Canadian Foundation for Climate and Atmospheric Sciences; Natural
Sciences and Engineering Research Council; NASA
FX This work was supported by funding from the Canadian Foundation for
Climate and Atmospheric Sciences and the Natural Sciences and
Engineering Research Council. We thank an anonymous reviewer for helpful
comments. The GEOS-Chem model is maintained at Harvard University with
support from the NASA Atmospheric Chemistry Modeling and Analysis
Program. The IONS-06 ozonesondes were sponsored by NASA ( Tropospheric
Chemistry Program), NOAA/ESRL Global Monitoring Division, and
Environment Canada/MSC Ozone group.
NR 17
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 25
PY 2009
VL 36
AR L04802
DI 10.1029/2008GL036935
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 412MY
UT WOS:000263730100006
ER
PT J
AU Sarantos, M
Slavin, JA
Benna, M
Boardsen, SA
Killen, RM
Schriver, D
Travnicek, P
AF Sarantos, Menelaos
Slavin, James A.
Benna, Mehdi
Boardsen, Scott A.
Killen, Rosemary M.
Schriver, David
Travnicek, Pavel
TI Sodium-ion pickup observed above the magnetopause during MESSENGER's
first Mercury flyby: Constraints on neutral exospheric models
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MAGNETOSPHERE; SURFACE
AB Single-particle tracings of sodium pickup ions launched upstream of Mercury's magnetopause are used to investigate the access of these ions to the magnetosphere and set limits on the distribution of neutral sodium about the planet during the first MESSENGER flyby. The transport of pickup ions is modeled using flow velocity and magnetic fields from a three-dimensional magnetohydrodynamic simulation. Extensive penetration of pickup ions into the magnetosphere is found in the post-noon and dusk local time sectors due to the northward interplanetary magnetic field at the time of MESSENGER's first flyby. It is concluded that: (1) pickup of magnetosheath photoions may be an important source of hot planetary ions within the magnetosphere; and (2) the sodium ions in the magnetosheath observed by MESSENGER must originate from an extended neutral exosphere due to ion sputtering and/or to a partially escaping distribution generated by photonstimulated desorption with yields modified by regolith trapping. Citation: Sarantos, M., J. A. Slavin, M. Benna, S. A. Boardsen, R. M. Killen, D. Schriver, and P. Travnicek (2009), Sodium-ion pickup observed above the magnetopause during MESSENGER's first Mercury flyby: Constraints on neutral exospheric models, Geophys. Res. Lett., 36, L04106, doi: 10.1029/2008GL036207.
C1 [Sarantos, Menelaos; Slavin, James A.; Boardsen, Scott A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Benna, Mehdi] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD USA.
[Boardsen, Scott A.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD USA.
[Killen, Rosemary M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Schriver, David; Travnicek, Pavel] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
RP Sarantos, M (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM menelaos.sarantos-1@nasa.gov
RI Slavin, James/H-3170-2012; Sarantos, Menelaos/H-8136-2013; Travnicek,
Pavel/G-8608-2014; Benna, Mehdi/F-3489-2012
OI Slavin, James/0000-0002-9206-724X;
FU NASA [NAS5-97271]; Carnegie Institution of Washington [NASW-00002]
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to the Johns Hopkins University Applied Physics
Laboratory and NASW-00002 to the Carnegie Institution of Washington.
NR 19
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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 FEB 25
PY 2009
VL 36
AR L04106
DI 10.1029/2008GL036207
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 412MY
UT WOS:000263730100003
ER
PT J
AU Holmes, TRH
De Jeu, RAM
Owe, M
Dolman, AJ
AF Holmes, T. R. H.
De Jeu, R. A. M.
Owe, M.
Dolman, A. J.
TI Land surface temperature from Ka band (37 GHz) passive microwave
observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID VEGETATION OPTICAL DEPTH; SOIL-MOISTURE RETRIEVAL; POLARIZATION
DIFFERENCE; CARBON-DIOXIDE; WATER-CONTENT; FOREST; METHODOLOGY;
VALIDATION; FREQUENCY; ECOSYSTEM
AB An alternative to thermal infrared satellite sensors for measuring land surface temperature (T-s) is presented. The 37 GHz vertical polarized brightness temperature is used to derive T-s because it is considered the most appropriate microwave frequency for temperature retrieval. This channel balances a reduced sensitivity to soil surface characteristics with a relatively high atmospheric transmissivity. It is shown that with a simple linear relationship, accurate values for Ts can be obtained from this frequency, with a theoretical bias of within 1 K for 70% of vegetated land areas of the globe. Barren, sparsely vegetated, and open shrublands cannot be accurately described with this single channel approach because variable surface conditions become important. The precision of the retrieved land surface temperature is expected to be better than 2.5 K for forests and 3.5 K for low vegetation. This method can be used to complement existing infrared derived temperature products, especially during clouded conditions. With several microwave radiometers currently in orbit, this method can be used to observe the diurnal temperature cycles with surprising accuracy.
C1 [Holmes, T. R. H.; De Jeu, R. A. M.; Dolman, A. J.] Vrije Univ Amsterdam, Dept Hydrol & Geoenvironm Sci, NL-1081 HV Amsterdam, Netherlands.
[Owe, M.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP Holmes, TRH (reprint author), Vrije Univ Amsterdam, Dept Hydrol & Geoenvironm Sci, NL-1081 HV Amsterdam, Netherlands.
EM thomas.holmes@falw.vu.nl
RI Holmes, Thomas/F-4512-2010;
OI Holmes, Thomas/0000-0002-4651-0079; Dolman, A.J./0000-0003-0099-0457
FU EU [036946-2]
FX This work was partly funded by the EU 6th Framework program WATCH
(project 036946-2). We appreciate the help from Michiel van der Molen
with the longwave emissivity derivation and the helpful comments of John
Gash. We thank the organizations who support the FLUXNETsites (Illinois
StateWater Survey, INRA, Max Planck Institute Jena, NOAA/ARL,
Universidade Tecnica de Lisboa, University of Tuscia Viterbo, Wageningen
University, and Weisman Institute of Science) for making the data
available to us.
NR 37
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U1 1
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 25
PY 2009
VL 114
AR D04113
DI 10.1029/2008JD010257
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 412NZ
UT WOS:000263732800001
ER
PT J
AU Fogt, RL
Perlwitz, J
Pawson, S
Olsen, MA
AF Fogt, Ryan L.
Perlwitz, Judith
Pawson, Steven
Olsen, Mark A.
TI Intra-annual relationships between polar ozone and the SAM
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID TRENDS
AB Observed co-variations between polar total column ozone and the Southern Hemisphere Annular Mode (SAM) during 1962-2004 are presented and evaluated in a chemistry-climate model (CCM). Results show that austral spring total column ozone variability at South Pole is significantly related to the SAM, perhaps up to four months later; this relationship is only seen in simulations that include ozone depletion. The austral spring SAM also is linked to following late spring - early summer total column ozone over the polar cap, since both respond to the wave-driving of the stratosphere. Overall, the CCM captures many of the observed ozone-SAM links, but over-predicts the relationship between spring ozone and austral summer SAM, as a consequence of the delayed breakdown of the polar vortex in the CCM. Citation: Fogt, R. L., J. Perlwitz, S. Pawson, and M. A. Olsen (2009), Intra-annual relationships between polar ozone and the SAM, Geophys. Res. Lett., 36, L04707, doi: 10.1029/2008GL036627.
C1 [Fogt, Ryan L.; Perlwitz, Judith] NOAA, Div Phys Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Olsen, Mark A.] NASA, Goddard Earth Sci & Technol Ctr, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pawson, Steven] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Perlwitz, Judith] Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
RP Fogt, RL (reprint author), NOAA, Div Phys Sci, Earth Syst Res Lab, 325 Broadway R PSD1, Boulder, CO 80305 USA.
EM ryan.fogt@noaa.gov
RI Perlwitz, Judith/B-7201-2008; Fogt, Ryan/B-6989-2008; Pawson,
Steven/I-1865-2014
OI Perlwitz, Judith/0000-0003-4061-2442; Fogt, Ryan/0000-0002-5398-3990;
Pawson, Steven/0000-0003-0200-717X
FU NASA; National Research Council
FX This work was supported by the NASA Modeling and Analysis Program and
used high-end computational resources provided by NASA's Columbia
Project. R. Fogt's contribution was supported by the National Research
Council Research Associateship Programs. We thank Sam Oltmans of NOAA's
Global Monitoring Division for kindly providing the total column ozone
data for the South Pole. Ozone data for Syowa were obtained through the
World Ozone and Ultraviolet Radiation Data Centre. Discussions with
Susan Solomon and the comments from two anonymous reviewers helped to
improve the manuscript in several places and are greatly appreciated.
NR 15
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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 24
PY 2009
VL 36
AR L04707
DI 10.1029/2008GL036627
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 412MV
UT WOS:000263729800004
ER
PT J
AU Wall, SD
Lopes, RM
Stofan, ER
Wood, CA
Radebaugh, JL
Horst, SM
Stiles, BW
Nelson, RM
Kamp, LW
Janssen, MA
Lorenz, RD
Lunine, JI
Farr, TG
Mitri, G
Paillou, P
Paganelli, F
Mitchell, KL
AF Wall, S. D.
Lopes, R. M.
Stofan, E. R.
Wood, C. A.
Radebaugh, J. L.
Horst, S. M.
Stiles, B. W.
Nelson, R. M.
Kamp, L. W.
Janssen, M. A.
Lorenz, R. D.
Lunine, J. I.
Farr, T. G.
Mitri, G.
Paillou, P.
Paganelli, F.
Mitchell, K. L.
TI Cassini RADAR images at Hotei Arcus and western Xanadu, Titan: Evidence
for geologically recent cryovolcanic activity
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ICY SATELLITES; HUYGENS PROBE; SURFACE; VOLCANISM; MAPPER; VENUS
AB Images obtained by the Cassini Titan Radar Mapper (RADAR) reveal lobate, flowlike features in the Hotei Arcus region that embay and cover surrounding terrains and channels. We conclude that they are cryovolcanic lava flows younger than surrounding terrain, although we cannot reject the sedimentary alternative. Their appearance is grossly similar to another region in western Xanadu and unlike most of the other volcanic regions on Titan. Both regions correspond to those identified by Cassini's Visual and Infrared Mapping Spectrometer (VIMS) as having variable infrared brightness, strengthening the case that these are recent cryovolcanoes. Citation: Wall, S. D., et al. (2009), Cassini RADAR images at Hotei Arcus and western Xanadu, Titan: Evidence for geologically recent cryovolcanic activity, Geophys. Res. Lett., 36, L04203, doi: 10.1029/2008GL036415.
C1 [Wall, S. D.; Lopes, R. M.; Stiles, B. W.; Nelson, R. M.; Kamp, L. W.; Janssen, M. A.; Farr, T. G.; Mitri, G.; Mitchell, K. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Horst, S. M.; Lunine, J. I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Lorenz, R. D.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
[Stofan, E. R.; Paganelli, F.] Proxemy Res, Bowie, MD 20715 USA.
[Paillou, P.] Univ Bordeaux, UMR5804, Observ Aquitain Sci Univers, F-33270 Floirac, France.
[Radebaugh, J. L.] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA.
[Wood, C. A.] Wheeling Jesuit Univ, Ctr Educ Technol, Wheeling, WV 26003 USA.
RP Wall, SD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM stephen.d.wall@jpl.nasa.gov
RI Horst, Sarah/A-9906-2010; Lorenz, Ralph/B-8759-2016; Lopes,
Rosaly/D-1608-2016
OI Horst, Sarah/0000-0003-4596-0702; Lorenz, Ralph/0000-0001-8528-4644;
Lopes, Rosaly/0000-0002-7928-3167
NR 37
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U1 3
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 24
PY 2009
VL 36
AR L04203
DI 10.1029/2008GL036415
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 412MV
UT WOS:000263729800002
ER
PT J
AU David, RLA
Wei, MH
Liu, D
Bathel, BF
Plog, JP
Ratner, A
Kornfield, JA
AF David, R. L. Ameri
Wei, Ming-Hsin
Liu, David
Bathel, Brett F.
Plog, Jan P.
Ratner, Albert
Kornfield, Julia A.
TI Effects of Pairwise, Self-Associating Functional Side Groups on Polymer
Solubility, Solution Viscosity, and Mist Control
SO MACROMOLECULES
LA English
DT Article
ID THERMOREVERSIBLE GELATION; RHEOLOGICAL BEHAVIOR; RADICAL-ADDITION; DRAG
REDUCTION; DYNAMICS; FLOW; COPOLYMERS; MERCAPTANS; BREAKUP
AB Solution properties are reported for homologous series of narrowly distributed polymers with systematically varied content of self-associating groups. Anionically polymerized polybutadienes of two lengths (510 and 1250 kg/mol) serve as prepolymers that are modified by incorporation of carboxylic acid side groups using thiol-ene coupling to pendant vinyl groups. Carboxylic acid groups strongly reduce polymer solubility in hydrocarbon solvents, restricting the extent of functionalization that can be examined in single-phase solutions (e.g., in chlorododecane, functionalization must be kept < 1.8 mol% even for the shorter of the two backbones). In the single-phase regime, addition of hydrogen bond "stickers" weakly affects solution viscosity. Even at concentrations that produce overlap at the scale of strand length between stickers, viscosity increases are less than 1 order of magnitude. These controlled studies (Using functionalized and unmodified polymer homologues of matched, well-defined length) challenge the pre-existing understanding of the rheology of self-associating polymers. The results indicate that effects of intrachain pairing are important beyond the dilute regime-behavior unaccounted for in earlier experimental and theoretical studies. The implications for mist control of aviation fuel are that self-associating polymers of acceptable solubility in the fuel are not superior to nonassociating polymers even at concentrations several times above overlap.
C1 [David, R. L. Ameri; Wei, Ming-Hsin; Liu, David; Kornfield, Julia A.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
[Ratner, Albert] Univ Iowa, Dept Mech & Ind Engn, Iowa City, IA 52242 USA.
[Plog, Jan P.] Themo Fisher Sci, D-76227 Karlsruhe, Germany.
[Bathel, Brett F.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Kornfield, JA (reprint author), CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
EM jak@cheme.caltech.edu
FU FAA; NASA; Caltech Milliken Foundation; Caltech Gates Grubstake Fund
FX Funding for this research was provided by the FAA and NASA, the Caltech
Milliken Foundation, and the Caltech Gates Grubstake Fund. We thank Dr.
Steven Smith of Procter and Gamble Company for supplying the 1,2-PB
precursor materials and Dr. Suneel Kunamaneni for contributing the ideas
that initiated the direction of this work.
NR 32
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U1 1
U2 13
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0024-9297
J9 MACROMOLECULES
JI Macromolecules
PD FEB 24
PY 2009
VL 42
IS 4
BP 1380
EP 1391
DI 10.1021/ma802058s
PG 12
WC Polymer Science
SC Polymer Science
GA 408IW
UT WOS:000263429700067
ER
PT J
AU Martin, JW
Godwin, S
Moffitt, R
AF Martin, Joel W.
Godwin, Scott
Moffitt, Robert
TI Additions to the decapod crustacean fauna of the Hawaiian Islands, I. A
review of the genus Sakaila Manning and Holthuis, 1981 (Decapoda,
Brachyura, Aethridae), with the description of a new species from the
Northwestern Hawaiian Islands
SO ZOOTAXA
LA English
DT Review
DE Sakaila; Brachyura; Aethridae; Hawaii; French Frigate Shoals
ID CALAPPIDAE; CRABS; PARTHENOPIDAE; LEUCOSIIDAE; FAMILY
AB The brachyuran crab genus Sakaila, currently considered a member of the family Aethridae, is reviewed and revised. Illustrations are provided for all of the known species, and a new species, the fourth in the genus, is described based on one female from French Frigate Shoals, one male from Maro Reef, both in the Northwestern Hawaiian Islands, and a second male from Johnston Atoll. Previous species are known only from the eastern Atlantic off the west coast of Africa (S. africana Manning and Holthuis, 1981) and from the far western Pacific off Japan (S. japonica Sakai, 1963, and S. imperialis Sakai, 1963). The new species differs from its congeners mostly in the overall spination of the carapace and legs, which is more pronounced in the new species. A key to the known species is provided and the current status of each species is discussed.
C1 [Martin, Joel W.] Nat Hist Museum Los Angeles Cty, Res & Collect Branch, Los Angeles, CA 90007 USA.
[Godwin, Scott] Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA.
[Moffitt, Robert] NOAA, Natl Marine Fisheries Serv, Honolulu, HI 96822 USA.
RP Martin, JW (reprint author), Nat Hist Museum Los Angeles Cty, Res & Collect Branch, 900 Exposit Blvd, Los Angeles, CA 90007 USA.
EM jmartin@nhm.org; lgodwin@hawaii.edu; Robert.Moffitt@noaa.gov
NR 18
TC 4
Z9 4
U1 0
U2 1
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD FEB 23
PY 2009
IS 2018
BP 25
EP 44
PG 20
WC Zoology
SC Zoology
GA 412IO
UT WOS:000263718700002
ER
PT J
AU Brown, BA
Lindesay, J
AF Brown, Beth A.
Lindesay, James
TI Construction of a Penrose diagram for an accreting black hole
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
AB A Penrose diagram is constructed for a spatially coherent black hole that accretes at stepwise steady rates as measured by a distant observer from an initial state described by a metric of Minkowski form. Coordinate lines are computationally derived, and radial lightlike trajectories verify the viability of the diagram. Coordinate dependences of significant features, such as the horizon and radial mass scale, are clearly demonstrated on the diagram. The onset of a singularity at the origin is shown to open a new region in space time that contains the interior of the black hole.
C1 [Brown, Beth A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lindesay, James] Howard Univ, Computat Phys Lab, Washington, DC 20059 USA.
RP Brown, BA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jlslac@slac.stanford.edu
FU NASA Administrator's Fellowship Program
FX BAB would like to acknowledge the support of the NASA Administrator's
Fellowship Program. JL must regretfully inform the reader that his
colleague Dr. Beth A Brown, the co-author, unexpectedly passed during
the preparation of the final draft of this manuscript.
NR 7
TC 3
Z9 3
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD FEB 21
PY 2009
VL 26
IS 4
AR 045010
DI 10.1088/0264-9381/26/4/045010
PG 5
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 403DD
UT WOS:000263061600010
ER
PT J
AU Jiang, XN
Waliser, DE
AF Jiang, Xianan
Waliser, Duane E.
TI Two dominant subseasonal variability modes of the eastern Pacific ITCZ
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID WEST-AFRICAN MONSOON; GULF-OF-CALIFORNIA; INTRASEASONAL VARIABILITY;
BOREAL SUMMER; OSCILLATION; PRECIPITATION; MODULATION; NORTHWARD;
AMERICAN; SURGES
AB Two subseasonal variability (SSV) modes over the eastern Pacific (EPAC) have been identified based on rainfall observations. The first SSV mode with a dominant period of 40 days has been documented in detail in previous studies. The second SSV mode associated with the EPAC intertropical convergence zone (ITCZ) rainfall, to the best of our knowledge, is documented for the first time, exhibiting a prevailing period of 18 days (hereafter, a 20-d SSV mode). This 20-d SSV mode is largely characterized by northward propagation. While its strongest signals are present over the EPAC, the impacts of this 20-d SSV mode are also discerned over the North American Monsoon, the Gulf of Mexico, and Caribbean Sea. Analysis of the low-frequency variability of these two SSV modes shows that they are anti-correlated on the interannual time scales. The physics responsible for the origins of the two SSV modes over the EPAC are still elusive. Citation: Jiang, X., and D. E. Waliser (2009), Two dominant subseasonal variability modes of the eastern Pacific ITCZ, Geophys. Res. Lett., 36, L04704, doi:10.1029/2008GL036820.
C1 [Jiang, Xianan; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jiang, Xianan; Waliser, Duane E.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
RP Jiang, XN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM xianan@jifresse.ucla.edu
RI Jiang, Xianan/A-2283-2012
NR 30
TC 20
Z9 23
U1 0
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 FEB 21
PY 2009
VL 36
AR L04704
DI 10.1029/2008GL036820
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 410XL
UT WOS:000263611500005
ER
PT J
AU Rong, PP
Russell, JM
Mlynczak, MG
Remsberg, EE
Marshall, BT
Gordley, LL
Lopez-Puertas, M
AF Rong, P. P.
Russell, J. M., III
Mlynczak, M. G.
Remsberg, E. E.
Marshall, B. T.
Gordley, L. L.
Lopez-Puertas, M.
TI Validation of Thermosphere Ionosphere Mesosphere Energetics and
Dynamics/Sounding of the Atmosphere using Broadband Emission Radiometry
(TIMED/SABER) v1.07 ozone at 9.6 mu m in altitude range 15-70 km
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TERRESTRIAL MIDDLE ATMOSPHERE; INFRARED LIMB EMISSION; ALGORITHM;
INSTRUMENT; SATELLITE; INVERSION; PROFILES; RADIANCE; QUALITY
AB The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument operating onboard the Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) satellite since 2002 has provided day and nighttime measurements of ozone on a daily basis in the middle to upper atmosphere (15-100 km) using limb scanning in the 9.6-mu m band. The focus of this paper is on validation of v1.07 O-3 in the stratosphere and mesosphere region below 70 km. SABER v1.07 O-3 measurements have a precision of similar to 1-2% in the stratosphere and similar to 3-5% in the lower mesosphere. A SABER positive bias exists in all regions other than the lower stratosphere. The positive biases in the stratosphere are within similar to 5-12% in most cases except in the equatorial to middle latitudes in the altitude range similar to 30-50 km, where they reach similar to 15-17% and exceed the combined systematic error by similar to 5-6%. The comparisons in the lower mesosphere indicate that SABER O-3 captures the diurnal variability very well. The best agreement of similar to 5-7% occurs for daytime comparisons with solar occultation measurements in the lower mesosphere. As with most large satellite data sets, a small portion of the O-3 profiles show unrealistically large values. The occurrences of these profiles were revealed using a probability approach, which enabled the identification of the time frames and spatial regions where these anomalies occur.
C1 [Rong, P. P.; Russell, J. M., III] Hampton Univ, Hampton, VA 23668 USA.
[Marshall, B. T.; Gordley, L. L.] GATS Inc, Newport News, VA 23606 USA.
[Lopez-Puertas, M.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Mlynczak, M. G.; Remsberg, E. E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Rong, PP (reprint author), Hampton Univ, Hampton, VA 23668 USA.
RI Mlynczak, Martin/K-3396-2012; Lopez Puertas, Manuel/M-8219-2013
OI Lopez Puertas, Manuel/0000-0003-2941-7734
NR 35
TC 22
Z9 22
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 21
PY 2009
VL 114
AR D04306
DI 10.1029/2008JD010073
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 410XV
UT WOS:000263612500001
ER
PT J
AU Lundgren, P
Hetland, EA
Liu, Z
Fielding, EJ
AF Lundgren, Paul
Hetland, Eric A.
Liu, Zhen
Fielding, Eric J.
TI Southern San Andreas-San Jacinto fault system slip rates estimated from
earthquake cycle models constrained by GPS and interferometric synthetic
aperture radar observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID NORTH AMERICA MOTION; UPPER-MANTLE; STRIKE-SLIP; CRUSTAL DEFORMATION;
ELSINORE FAULT; SALTON TROUGH; SHEAR ZONE; CALIFORNIA; RHEOLOGY; PLATE
AB We use ground geodetic and interferometric synthetic aperture radar satellite observations across the southern San Andreas ( SAF)-San Jacinto ( SJF) fault systems to constrain their slip rates and the viscosity structure of the lower crust and upper mantle on the basis of periodic earthquake cycle, Maxwell viscoelastic, finite element models. Key questions for this system are the SAF and SJF slip rates, the slip partitioning between the two main branches of the SJF, and the dip of the SAF. The best-fitting models generally have a high-viscosity lower crust (eta= 10(21) Pa s) overlying a lower-viscosity upper mantle (eta = 10(19) Pa s). We find considerable trade-offs between the relative time into the current earthquake cycle of the San Jacinto fault and the upper mantle viscosity. With reasonable assumptions for the relative time in the earthquake cycle, the partition of slip is fairly robust at around 24-26 mm/a for the San Jacinto fault system and 16-18 mm/a for the San Andreas fault. Models for two subprofiles across the SAF-SJF systems suggest that slip may transfer from the western ( Coyote Creek) branch to the eastern ( Clark-Superstition hills) branch of the SJF from NW to SE. Across the entire system our best-fitting model gives slip rates of 2 +/- 3, 12 +/- 9, 12 +/- 9, and 17 +/- 3 mm/a for the Elsinore, Coyote Creek, Clark, and San Andreas faults, respectively, where the large uncertainties in the slip rates for the SJF branches reflect the large uncertainty in the slip rate partitioning within the SJF system.
C1 [Lundgren, Paul; Liu, Zhen; Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hetland, Eric A.] CALTECH, Seismol Lab, Pasadena, CA 91125 USA.
RP Lundgren, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM paul.r.lundgren@jpl.nasa.gov; ehetland@alum.mit.edu
RI Hetland, Eric/D-4297-2012; Fielding, Eric/A-1288-2007; Liu,
Zhen/D-8334-2017
OI Fielding, Eric/0000-0002-6648-8067;
FU Tectonics Observatory; Seismological Laboratory, Caltech; internal
Research and Technology Development
FX We thank the European Space Agency for ERS data provided through the
WInSAR archive. CMM3 data were provided through the Southern California
Earthquake Center. Maps and profiles in this paper were generated using
the public domain Generic Mapping Tools ( GMT) software [ Wessel and
Smith, 1995]. We greatly appreciate thorough and insightful reviews by
Noah Fay, one anonymous reviewer, and associate editor Tim Dixon. E. A.
H. thanks the Tectonics Observatory and the Seismological Laboratory,
Caltech, for postdoctoral support. This research was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration and
funded through the internal Research and Technology Development program.
NR 78
TC 42
Z9 42
U1 2
U2 9
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 21
PY 2009
VL 114
AR B02403
DI 10.1029/2008JB005996
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 410YP
UT WOS:000263614500006
ER
PT J
AU Asai, A
Shibata, K
Ishii, TT
Oka, M
Kataoka, R
Fujiki, K
Gopalswamy, N
AF Asai, Ayumi
Shibata, Kazunari
Ishii, Takako T.
Oka, Mitsuo
Kataoka, Ryuho
Fujiki, Ken'ichi
Gopalswamy, Nat
TI Evolution of the anemone AR NOAA 10798 and the related geo-effective
flares and CMEs
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTIONS; X-RAY JETS; MAGNETIC-FIELDS; ACTIVE REGIONS;
WIND OBSERVATIONS; SOLAR CORONA; SOHO MISSION; RECONNECTION; RADIO; SUN
AB We present a detailed examination of the features of the active region (AR) NOAA 10798. This AR generated coronal mass ejections (CMEs) that caused a large geomagnetic storm on 24 August 2005 with the minimum Dst index of -216 nT. We examined the evolution of the AR and the features on/near the solar surface and in the interplanetary space. The AR emerged in the middle of a small coronal hole, and formed a sea anemone like configuration. Ha filaments were formed in the AR, which have southward axial field. Three M class flares were generated, and the first two that occurred on 22 August 2005 were followed by Halo-type CMEs. The speeds of the CMEs were fast, and recorded about 1200 and 2400 km s(-1), respectively. The second CME was especially fast, and caught up and interacted with the first (slower) CME during their travelings toward Earth. These acted synergically to generate an interplanetary disturbance with strong southward magnetic field of about -50 nT, which was followed by the large geomagnetic storm.
C1 [Asai, Ayumi] Natl Astron Observ Japan, Nobeyama Solar Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan.
[Asai, Ayumi] Natl Astron Observ Japan, Mitaka, Tokyo, Japan.
[Asai, Ayumi] Grad Univ Adv Studies, Hayama, Japan.
[Shibata, Kazunari; Ishii, Takako T.; Oka, Mitsuo] Kyoto Univ, Kwasan & Hida Observ, Kyoto 6078471, Japan.
[Oka, Mitsuo] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35807 USA.
[Kataoka, Ryuho] RIKEN, Wako, Saitama 3510198, Japan.
[Fujiki, Ken'ichi] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Asai, A (reprint author), Natl Astron Observ Japan, Nobeyama Solar Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan.
EM asai@nro.nao.ac.jp
RI Gopalswamy, Nat/D-3659-2012
FU Ministry of Education, Culture, Sports, Science and Technology (MEXT) of
Japan; Ministry of Education, Science, Sports, Technology, and Culture
of Japan [17GS0208]; Solar-Terrestrial Environment Laboratory, Nagoya
University; JSPS Postdoctoral Fellows for Research Abroad
FX We first acknowledge anonymous referees for their useful comments and
suggestions. We wish to thank J. Kozyra, K. Hayashi, N. V. Nitta, V.
Yurchyshyn, and B. J. Thompson for fruitful discussions and their
helpful comments. This work was supported by the Grant-in-Aid for the
Global COE Program "The Next Generation of Physics, Spun from
Universality and Emergence" from the Ministry of Education, Culture,
Sports, Science and Technology (MEXT) of Japan. This work was also
supported by the Grant-in-Aid for Creative Scientific Research "The
Basic Study of Space Weather Prediction" (17GS0208, Head Investigator:
K. Shibata) from the Ministry of Education, Science, Sports, Technology,
and Culture of Japan. This work was partially carried out by the joint
research program of the Solar-Terrestrial Environment Laboratory, Nagoya
University. We would like to acknowletge all the members of the
Geotail/PWI, LEP, and MGF for providing the data. We would like to thank
WDC for Geomagnetism, Kyoto Dst index service. Our thanks also go to the
SMART teams of Hida Observatory, Kyoto University, Big Bear Solar
Observatory, and Meudon Observatoire de Paris, Section de Meudon, for
letting us use the Ha data. We made extensive use of SOHO, and ACE Data
Center. M. O. was supported by the Grant-in-Aid for JSPS Postdoctoral
Fellows for Research Abroad.
NR 58
TC 10
Z9 10
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB 21
PY 2009
VL 114
AR A00A21
DI 10.1029/2008JA013291
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410YU
UT WOS:000263615000003
ER
PT J
AU Hwang, KJ
Lynch, KA
Newman, DL
Carlson, CW
AF Hwang, K. -J.
Lynch, K. A.
Newman, D. L.
Carlson, C. W.
TI FAST observations of downward current regions: Effect of ionospheric
constraints on parallel signatures
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ELECTRIC-FIELDS; ION CONICS; AURORA; ACCELERATION
AB Downward current region auroral crossings by the FAST (Fast Auroral Snapshot) spacecraft show that divergent electric fields which are perpendicular to the geomagnetic field (E-perpendicular to) have two types of structures: those whose potential contours close below the spacecraft but above the ionosphere (U-shaped), and those that are not completely closed but partially couple to the low-altitude ionosphere (composite). Using FAST data from above 3000 km altitude, we investigate parallel signatures of particle motions in these downward current regions, focusing on the distinctions between U-shaped and composite potential structures. We analyze probability density functions of electron velocity moments and ion energies, and power spectral density scaling laws of wave turbulence above the potential drop. Results indicate that U-shaped potential structures show aspects of fully developed turbulence. Composite structures are often characterized by intermittent signatures, possibly because of lower ionospheric constraints. These results support a picture of an evolutionary process from composite to U-shaped potential structures in downward current regions.
C1 [Hwang, K. -J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Carlson, C. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Lynch, K. A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03747 USA.
[Newman, D. L.] Univ Colorado, Ctr Integrated Plasma Studies, Boulder, CO 80309 USA.
RP Hwang, KJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM joohwang@umbc.edu; kristina.lynch@dartmouth.edu;
david.newman@colorado.edu; cwc@ssl.berkeley.edu
FU NASA [NAG5-10472]; Dartmouth College
FX This work was supported by NASA grant NAG5-10472 and by Dartmouth
College. We appreciate a helpful discussion with Christopher C. Chaston
about our BBELF PSD results.
NR 19
TC 1
Z9 1
U1 0
U2 0
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 21
PY 2009
VL 114
AR A02219
DI 10.1029/2008JA013080
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410YU
UT WOS:000263615000002
ER
PT J
AU Hwang, KJ
Lynch, KA
Newman, DL
Carlson, CW
AF Hwang, K. -J.
Lynch, K. A.
Newman, D. L.
Carlson, C. W.
TI FAST observations of downward current regions: Effect of magnetospheric
conditions on the parallel potential drop
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID AURORAL CURRENT REGION; BEAMS; ION
AB The effects of background plasma sheet boundary conditions on the downward current region potential structures are investigated using FAST observations of both ionospheric and plasma sheet populations. Precipitating plasma sheet electrons are observed to partially control the magnitude of the potential drop consistent with theories of charge-neutrality requirements throughout ionospheric and magnetospheric regions. This leads to a new empirical model of a downward current region (DCR) current-voltage relation for U-shaped events. Hot plasma sheet ions are observed to play an important role in reducing the variability of the potential drop, possibly by acting as a sink or buffer for free energy caused by the resulting energetic upward electron beams. The statistical studies of boundary conditions in the auroral downward current region in this and our companion paper show that both ionospheric and magnetospheric conditions appear to regulate the DCR potential structures observed at FAST altitudes. The initiation of downward current region potentials seems to be influenced mainly by low-altitude ionospheric conditions. Once the U-shaped potential structure is formed, the effects of the ionospheric influences may be relaxed and modulated by effects from magnetospheric conditions.
C1 [Hwang, K. -J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lynch, K. A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03747 USA.
[Newman, D. L.] Univ Colorado, Ctr Integrated Plasma Studies, Boulder, CO 80309 USA.
[Carlson, C. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Hwang, KJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM joohwang@umbc.edu; kristina.lynch@dartmouth.edu;
david.newman@colorado.edu; cwc@ssl.berkeley.edu
FU NASA [NAG5-10472]; Dartmouth College
FX This work was supported by NASA grant NAG5-10472 and by Dartmouth
College.
NR 11
TC 2
Z9 2
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB 21
PY 2009
VL 114
AR A02218
DI 10.1029/2008JA013079
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410YU
UT WOS:000263615000001
ER
PT J
AU Waquet, F
Leon, JF
Cairns, B
Goloub, P
Deuze, JL
Auriol, F
AF Waquet, F.
Leon, J. -F.
Cairns, B.
Goloub, P.
Deuze, J. -L.
Auriol, F.
TI Analysis of the spectral and angular response of the vegetated surface
polarization for the purpose of aerosol remote sensing over land
SO APPLIED OPTICS
LA English
DT Article
ID RESEARCH SCANNING POLARIMETER; OPTICAL-PROPERTIES; URBAN AREA;
REFLECTANCE; SATELLITE; RETRIEVAL; ALGORITHM; VALIDATION; SPACEBORNE;
SCATTERING
AB A precise estimate of the polarization induced by the surface in reflected radiation is crucial for remote sensing applications dedicated to monitoring the atmosphere. Here we present airborne observations acquired during a field campaign in the North of France over vegetated surfaces. Polarized reflectances were measured in four spectral bands in the range between 0.67 and 2.2 mu m and for scattering angles between 75 degrees and 145 degrees. Our results confirm that the polarization generated by the reflection of vegetated surfaces can be understood as being primarily a specular reflection process. It is not possible from our measurements to see any spectral dependence of the surface polarization in the given spectral channels. The surface polarization is well fitted by existing surface models which have two degrees of freedom that allow the magnitude and angular behavior of the surface-polarized reflectance to be adjusted. (C) 2009 Optical Society of America
C1 [Waquet, F.; Leon, J. -F.; Goloub, P.; Deuze, J. -L.; Auriol, F.] Univ Sci & Tech Lille Flandres Artois, Opt Atmospher Lab, UMR 8518, CNRS, F-59655 Villeneuve Dascq, France.
[Cairns, B.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Waquet, F (reprint author), Univ Sci & Tech Lille Flandres Artois, Opt Atmospher Lab, UMR 8518, CNRS, F-59655 Villeneuve Dascq, France.
EM waquet@loa.univ-lille1.fr
OI Cairns, Brian/0000-0002-1980-1022
NR 40
TC 25
Z9 33
U1 2
U2 19
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 2009
VL 48
IS 6
BP 1228
EP 1236
DI 10.1364/AO.48.001228
PG 9
WC Optics
SC Optics
GA 421VV
UT WOS:000264387300026
PM 23567585
ER
PT J
AU Burlaga, LF
Ness, NF
Acuna, MH
Richardson, JD
Stone, E
McDonald, FB
AF Burlaga, L. F.
Ness, N. F.
Acuna, M. H.
Richardson, J. D.
Stone, E.
McDonald, F. B.
TI OBSERVATIONS OF THE HELIOSHEATH AND SOLAR WIND NEAR THE TERMINATION
SHOCK BY VOYAGER 2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; MHD; shock waves; solar wind
ID HELIOSPHERIC MAGNETIC-FIELD; MERGED INTERACTION REGIONS; LOCAL
INTERSTELLAR-MEDIUM; NEUTRAL HYDROGEN; PICKUP PROTONS; PLASMA;
ABSORPTION; IONS; AU
AB This paper describes the principal features of 24 hr averages of the magnetic field strength variations B(t) and their relationships to the plasma and energetic particles observed prior to and after the crossing of the termination shock (TS) by Voyager 2 (V2). The solar wind (pre-TS crossing) and heliosheath (post-TS crossing) data extend from day of year (DOY) 1 through 241, 2007 and from 2007 DOY 245 through 2008 DOY 80, respectively. In the solar wind, two merged interaction regions (MIRs) were observed in which the ratio of plasma pressure to magnetic pressure in the solar wind was relatively low. Strong magnetic fields and low values of beta were also observed just prior to its crossing of the TS. The predicted correlation between peaks in the intensity of energetic particles in the solar wind when V2 crossed the heliospheric current sheet from positive to negative magnetic polarity in the solar wind was not observed. In the heliosheath, V2 observed a feature characterized by large enhancements of the density N and the proton temperature T, a small increase in speed V, and a depression in B. The distributions of 24 hr averages of B and beta were approximately log-normal in both the solar wind and the heliosheath. A unipolar region was observed for 73 days in the heliosheath, as the heliospheric current sheet moved toward the equatorial plane to latitudes lower than V2.
C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Acuna, M. H.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Richardson, J. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Stone, E.] CALTECH, Pasadena, CA 91109 USA.
[McDonald, F. B.] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA.
RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Code 673, Greenbelt, MD 20771 USA.
EM leonard.f.burlaga@nasa.gov; nfnudel@yahoo.com; mario.acuna@nasa.gov;
jdr@space.mit.edu; ecs@srl.caltech.edu; fmcdonal@umd.edu
NR 34
TC 31
Z9 32
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 FEB 20
PY 2009
VL 692
IS 2
BP 1125
EP 1130
DI 10.1088/0004-637X/692/2/1125
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 411TW
UT WOS:000263674700012
ER
PT J
AU Hinderks, JR
Ade, P
Bock, J
Bowden, M
Brown, ML
Cahill, G
Carlstrom, JE
Castro, PG
Church, S
Culverhouse, T
Friedman, R
Ganga, K
Gear, WK
Gupta, S
Harris, J
Haynes, V
Keating, G
Kovac, J
Kirby, E
Lange, AE
Leitch, E
Mallie, OE
Melhuish, S
Memari, Y
Murphy, A
Orlando, A
Schwarz, R
Sullivan, CO
Piccirillo, L
Pryke, C
Rajguru, N
Rusholme, B
Taylor, AN
Thompson, KL
Tucker, C
Turner, AH
Wu, EYS
Zemcov, M
AF Hinderks, J. R.
Ade, P.
Bock, J.
Bowden, M.
Brown, M. L.
Cahill, G.
Carlstrom, J. E.
Castro, P. G.
Church, S.
Culverhouse, T.
Friedman, R.
Ganga, K.
Gear, W. K.
Gupta, S.
Harris, J.
Haynes, V.
Keating, G.
Kovac, J.
Kirby, E.
Lange, A. E.
Leitch, E.
Mallie, O. E.
Melhuish, S.
Memari, Y.
Murphy, A.
Orlando, A.
Schwarz, R.
Sullivan, C. O'
Piccirillo, L.
Pryke, C.
Rajguru, N.
Rusholme, B.
Taylor, A. N.
Thompson, K. L.
Tucker, C.
Turner, A. H.
Wu, E. Y. S.
Zemcov, M.
TI QUaD: A HIGH-RESOLUTION COSMIC MICROWAVE BACKGROUND POLARIMETER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic microwave background; instrumentation: polarimeters
ID ANGULAR SCALE INTERFEROMETER; POLARIZATION POWER SPECTRA; PROBE WMAP
OBSERVATIONS; OPTICAL DESIGN; 2003 FLIGHT; SOUTH-POLE; RECEIVER;
BRIGHTNESS; ANISOTROPY; BOLOMETER
AB We describe the QUaD experiment, a millimeter-wavelength polarimeter designed to observe the cosmic microwave background (CMB) from a site at the South Pole. The experiment comprises a 2.64 m Cassegrain telescope equipped with a cryogenically cooled receiver containing an array of 62 polarization-sensitive bolometers. The focal plane contains pixels at two different frequency bands, 100 GHz and 150 GHz, with angular resolutions of 5' and 3'.5, respectively. The high angular resolution allows observation of CMB temperature and polarization anisotropies over a wide range of scales. The instrument commenced operation in early 2005 and collected science data during three successive Austral winter seasons of observation.
C1 [Hinderks, J. R.; Bowden, M.; Church, S.; Kirby, E.; Rusholme, B.; Thompson, K. L.; Wu, E. Y. S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Ade, P.; Gear, W. K.; Gupta, S.; Harris, J.; Haynes, V.; Melhuish, S.; Orlando, A.; Piccirillo, L.; Tucker, C.; Turner, A. H.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Bock, J.; Kovac, J.; Leitch, E.; Rusholme, B.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, J.; Lange, A. E.; Leitch, E.; Orlando, A.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
[Brown, M. L.; Castro, P. G.; Memari, Y.; Taylor, A. N.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Cahill, G.; Sullivan, C. O'] Natl Univ Ireland, Maynooth, Kildare, Ireland.
[Carlstrom, J. E.; Culverhouse, T.; Friedman, R.; Murphy, A.; Schwarz, R.; Pryke, C.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Ganga, K.] CNRS, Lab APC, F-75205 Paris 13, France.
[Keating, G.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Hinderks, J. R.; Bowden, M.; Church, S.; Kirby, E.; Rusholme, B.; Thompson, K. L.; Wu, E. Y. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
RP Hinderks, JR (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RI Melhuish, Simon/B-1299-2016;
OI Melhuish, Simon/0000-0001-8725-4991; Orlando,
Angiola/0000-0001-8004-5054
FU National Science Foundation in the USA [AST-0096778, ANT-0338138,
ANT-0338335, ANT-0338238, NSF PHY-0114422]; UK Science and technology
Facilities Council (STFC); NSF Graduate Research Fellowship; Stanford
Graduate Fellowship; NASA Postdoctoral Fellowship; PPARC fellowships;
Fundacao para a Ciencia e a Tecnologia; Stanford Terman Fellowship; John
B. and Nelly L. Kilory Foundation Fellowship; Kavli Inst for
Cosmological Physics; NDSEG fellowship; NASA Postdoctoral Program at the
Goddard Space Flight Center; Jet Propulsion Laboratory
FX We acknowledge the staff of the Amundsen-Scott South Pole Station and
all involved in the United States Antarctic Program for their superb
support during the construction and operation of experiment. Special
thanks go to our bave winter-over scientist Robert Schwarz who has spent
three consecutive winter seasons with the QUaD. We also acknowledge the
tremendous efforts of the Stanford University Physics Department machine
shop in the construction of the focal plane assembly. J.R.H. thanks
David Chuss for useful comments on this draft and Simon Radford for
providing the 350 m tipper data. QUaD is funded by the National Science
Foundation in the USA, through grants
AST-0096778,ANT-0338138,ANT-0338335, and ANT-0338238, by the UK Science
and technology Facilities Council (STFC) and its predecessor the
Particle Physics and Astronomy Research Council (PPARC), and by the
Science Foundation Ireland.; J.R.H. acknowledges the support of an NSF
Graduate Research Fellowship, a Stanford Graduate Fellowship, and a NASA
Postdoctoral Fellowship. M.L.B. and A.O. acknowledge the award of PPARC
fellowships. P.G.C. is funded by the Fundacao para a Ciencia e a
Tecnologia. S.E.C. acknowledge support from a Stanford Terman
Fellowship. J.M.K. acknowledges support from a John B. and Nelly L.
Kilory Foundation Fellowship. C.P. and J.E.C. acknowledge partial
support from the Kavli Inst for Cosmological Physics through the grant
NSF PHY-0114422. E.Y.W. acknowledges receipt of an NDSEG fellowship.
M.Z. acknowledges the support of a NASA Postdoctoral Fellowship. This
research was supported in part by appointments to the NASA Postdoctoral
Program at the Goddard Space Flight Center (J.R.H.) and the Jet
Propulsion Laboratory (M.Z.), administered by Oak Ridge Associated
Universities through a contract with NASA.
NR 40
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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 20
PY 2009
VL 692
IS 2
BP 1221
EP 1246
DI 10.1088/0004-637X/692/2/1221
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 411TW
UT WOS:000263674700019
ER
PT J
AU Pryke, C
Ade, P
Bock, J
Bowden, M
Brown, ML
Cahill, G
Castro, PG
Church, S
Culverhouse, T
Friedman, R
Ganga, K
Gear, WK
Gupta, S
Hinderks, J
Kovac, J
Lange, AE
Leitch, E
Melhuish, SJ
Memari, Y
Murphy, JA
Orlando, A
Schwarz, R
Sullivan, CO
Piccirillo, L
Rajguru, N
Rusholme, B
Taylor, AN
Thompson, KL
Turner, AH
Wu, EYS
Zemcov, M
AF Pryke, C.
Ade, P.
Bock, J.
Bowden, M.
Brown, M. L.
Cahill, G.
Castro, P. G.
Church, S.
Culverhouse, T.
Friedman, R.
Ganga, K.
Gear, W. K.
Gupta, S.
Hinderks, J.
Kovac, J.
Lange, A. E.
Leitch, E.
Melhuish, S. J.
Memari, Y.
Murphy, J. A.
Orlando, A.
Schwarz, R.
Sullivan, C. O'
Piccirillo, L.
Rajguru, N.
Rusholme, B.
Taylor, A. N.
Thompson, K. L.
Turner, A. H.
Wu, E. Y. S.
Zemcov, M.
CA QUaD Collaboration
TI SECOND AND THIRD SEASON QUaD COSMIC MICROWAVE BACKGROUND TEMPERATURE AND
POLARIZATION POWER SPECTRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic microwave background; cosmology: observations; polarization
ID PROBE WMAP OBSERVATIONS; ANGULAR SCALE INTERFEROMETER; 2003 FLIGHT; CMB
TEMPERATURE; ANISOTROPY; BOOMERANG; RADIATION; DESIGN; IMAGER; CAPMAP
AB We report results from the second and third seasons of observation with the QUaD experiment. Angular power spectra of the cosmic microwave background are derived for both temperature and polarization at both 100 GHz and 150 GHz, and as cross-frequency spectra. All spectra are subjected to an extensive set of jackknife tests to probe for possible systematic contamination. For the implemented data cuts and processing technique such contamination is undetectable. We analyze the difference map formed between the 100 and 150 GHz bands and find no evidence of foreground contamination in polarization. The spectra are then combined to form a single set of results which are shown to be consistent with the prevailing LCDM model. The sensitivity of the polarization results is considerably better than that of any previous experiment for the first time multiple acoustic peaks are detected in the E-mode power spectrum at high significance.
C1 [Pryke, C.; Culverhouse, T.; Friedman, R.; Schwarz, R.] Univ Chicago, Dept Astron & Astrophys, Enrico Fermi Inst, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Ade, P.; Bowden, M.; Gear, W. K.; Gupta, S.; Melhuish, S. J.; Orlando, A.; Piccirillo, L.; Rajguru, N.; Turner, A. H.; Zemcov, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Bock, J.; Leitch, E.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, J.; Kovac, J.; Lange, A. E.; Leitch, E.; Orlando, A.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
[Bowden, M.; Church, S.; Hinderks, J.; Rusholme, B.; Thompson, K. L.; Wu, E. Y. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Bowden, M.; Church, S.; Hinderks, J.; Rusholme, B.; Thompson, K. L.; Wu, E. Y. S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Brown, M. L.; Castro, P. G.; Memari, Y.; Taylor, A. N.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Cahill, G.; Murphy, J. A.; Sullivan, C. O'] Natl Univ Ireland Maynooth, Dept Expt Phys, Maynooth, Kildare, Ireland.
[Ganga, K.] CNRS, Lab APC, F-75205 Paris 13, France.
RP Pryke, C (reprint author), Univ Chicago, Dept Astron & Astrophys, Enrico Fermi Inst, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
RI Melhuish, Simon/B-1299-2016;
OI Melhuish, Simon/0000-0001-8725-4991; Orlando,
Angiola/0000-0001-8004-5054
FU National Science Foundation in the USA [AST-0096778, ANT-0338138,
ANT0338335, ANT-0338238]; Particle Physics and Astronomy Research
Council in the UK; Science Foundation Ireland; NSF [PHY-0114422]; John
B. and Nelly L. Kilroy Foundation Fellowship
FX QUaD is funded by the National Science Foundation in the USA, through
grants AST-0096778, ANT-0338138, ANT0338335, and ANT-0338238, by the
Particle Physics and Astronomy Research Council in the UK, and by the
Science Foundation Ireland. We would like to thank the staff of the
Amundsen-Scott South Pole Station and all involved in the United States
Antarctic Program for the superb support operation which makes the
science presented here possible. Special thanks go to our intrepid
winter over scientist Robert Schwarz who spent three consecutive winter
seasons tending the QUaD experiment. The BOOMERanG Collaboration kindly
allowed the use of their CMB maps for our calibration purposes. M. L. B.
acknowledges the award of a PPARC fellowship. S. E. C. acknowledges
support from a Stanford Terman Fellowship. J. R. H. acknowledges the
support of an NSF Graduate Research Fellowship and a Stanford Graduate
Fellowship. C. P. and J. E. C. acknowledge partial support from the
Kavli Institute for Cosmological Physics through the grant NSF
PHY-0114422. E. Y. W. acknowledges receipt of an NDSEG fellowship. J. M.
K acknowledges support from a John B. and Nelly L. Kilroy Foundation
Fellowship.
NR 33
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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 2009
VL 692
IS 2
BP 1247
EP 1270
DI 10.1088/0004-637X/692/2/1247
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 411TW
UT WOS:000263674700020
ER
PT J
AU Montanari, E
Titarchuk, L
Frontera, F
AF Montanari, Enrico
Titarchuk, Lev
Frontera, Filippo
TI BeppoSAX OBSERVATIONS OF THE POWER AND ENERGY SPECTRAL EVOLUTION IN THE
BLACK HOLE CANDIDATE XTE J1650-500
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; radiation mechanisms:
non-thermal; stars: individual (XTE J1650-500)
ID X-RAY BINARIES; QUASI-PERIODIC OSCILLATION; ASTRONOMY SATELLITE;
FREQUENCY CORRELATION; NEUTRON-STAR; ON-BOARD; CONCENTRATOR
SPECTROMETER; MONTE-CARLO; XTE-J1650-500; CYGNUS-X-1
AB We study the time variability and spectral evolution of the black hole candidate source XTE J1650-500 using the BeppoSAX wide energy range (0.12-200 keV) observations performed during the 2001 X-ray outburst. The source evolves from a low/hard state (LHS) toward a high/soft state (HSS). In all states, the emergent photon spectrum is described by the sum of Comptonization and soft (disk) blackbody components. In the LHS, the Comptonization component dominates in the resulting spectrum. On the other hand, during the HSS observed by BeppoSAX the soft (disk) component is already dominant. In this state, the Comptonization part of the spectrum is much softer than that in the LHS (photon index Gamma is similar to 2.4 in the HSS vs. Gamma similar to 1.7 in the LHS). In the BeppoSAX data, we find a strong signature of the index saturation with the mass accretion rate, which can be considered as an observational evidence of the converging flow (black hole) in XTE J1650-500. We derive power spectra (PSs) of the source time variability in different spectral states as a function of energy band. When the source undergoes a transition to softer states, the PS as a whole is shifted to higher frequencies, which can be interpreted as a contraction of the Compton cloud during hard-soft spectral evolution. It is worthwhile to emphasize a detection of a strong low-frequency red noise component in the HSS PS, which can be considered a signature of the presence of the strong extended disk in the HSS. Also as a result of our data analysis, we find a very weak sign of K(alpha) line appearance in this BeppoSAX data set. This finding does not confirm previous claims by Miniutti et al. on the presence of a broad and strongly relativistic iron emission line in this particular set of BeppoSAX data.
C1 [Montanari, Enrico; Titarchuk, Lev; Frontera, Filippo] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy.
[Montanari, Enrico; Titarchuk, Lev] IIS Calvi, Finale Emilia, MO, Italy.
[Titarchuk, Lev] George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Titarchuk, Lev] USN, Res Lab, Washington, DC 20375 USA.
[Titarchuk, Lev] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Frontera, Filippo] INAF IASF, I-40129 Bologna, Italy.
RP Montanari, E (reprint author), Univ Ferrara, Dipartimento Fis, Via Saragat 1, I-44100 Ferrara, Italy.
EM montana@fe.infn.it; lev.titarchuk@nrl.navy.mil; frontera@fe.infn.it
NR 50
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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 FEB 20
PY 2009
VL 692
IS 2
BP 1597
EP 1608
DI 10.1088/0004-637X/692/2/1597
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 411TW
UT WOS:000263674700049
ER
PT J
AU Rudjord, O
Groeneboom, NE
Eriksen, HK
Huey, G
Gorski, KM
Jewell, JB
AF Rudjord, O.
Groeneboom, N. E.
Eriksen, H. K.
Huey, Greg
Gorski, K. M.
Jewell, J. B.
TI COSMIC MICROWAVE BACKGROUND LIKELIHOOD APPROXIMATION BY A GAUSSIANIZED
BLACKWELL-RAO ESTIMATOR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic microwave background; cosmology: observations; methods:
statistical
ID PROBE WMAP OBSERVATIONS; POWER SPECTRUM ESTIMATION; BAYESIAN-ANALYSIS;
MAPS; DISTRIBUTIONS
AB We introduce a new cosmic microwave background (CMB) temperature likelihood approximation called the Gaussianized Blackwell-Rao estimator. This estimator is derived by transforming the observed marginal power spectrum distributions obtained by the CMB Gibbs sampler into standard univariate Gaussians, and then approximating their joint transformed distribution by a multivariate Gaussian. The method is exact for full-sky coverage and uniform noise and an excellent approximation for sky cuts and scanning patterns relevant for modern satellite experiments such as the Wilkinson Microwave Anisotropy Probe (WMAP) and Planck. The result is a stable, accurate, and computationally very efficient CMB temperature likelihood representation that allows the user to exploit the unique error propagation capabilities of the Gibbs sampler to high ls. A single evaluation of this estimator between l = 2 and 200 takes similar to 0.2 CPU milliseconds, while for comparison, a singe pixel space likelihood evaluation between l = 2 and 30 for a map with similar to 2500 pixels requires similar to 20 s. We apply this tool to the five-year WMAP temperature data, and re-estimate the angular temperature power spectrum, C-l, and likelihood, L(C-l), for l <= 200, and derive new cosmological parameters for the standard six-parameter Lambda CDM model. Our spectrum is in excellent agreement with the official WMAP spectrum, but we find slight differences in the derived cosmological parameters. Most importantly, the spectral index of scalar perturbations is n(s) = 0.973 +/- 0.014, 1.9 sigma away from unity and 0.6 sigma higher than the official WMAP result, n(s) = 0.965 +/- 0.014. This suggests that an exact likelihood treatment is required to higher ls than previously believed, reinforcing and extending our conclusions from the three-year WMAP analysis. In that case, we found that the suboptimal likelihood approximation adopted between l = 12 and 30 by the WMAP team biased n(s) low by 0.4 sigma, while here we find that the same approximation between l = 30 and 200 introduces a bias of 0.6 sigma in n(s).
C1 [Rudjord, O.; Groeneboom, N. E.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Eriksen, H. K.] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway.
[Huey, Greg; Gorski, K. M.; Jewell, J. B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Rudjord, O (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway.
EM oystein.rudjord@astro.uio.no; leuat@irio.co.uk; k.k.eriksen@astro.uio.no
FU Jet Propulsion Laboratory; California Institute of Technology; National
Aeronautics and Space Administration; Research Council of Norway
FX We thank Tony Banday, Ben Wandelt, and Graca Rocha for useful and
interesting discussions. We acknowledge use of the HEALPix software
(Gorski et al. 2005) and analysis package for deriving the results in
this paper. We acknowledge use of the LAMBDA. This work was partially
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. O.R., N.E.G., and H. K. E. acknowledge financial support
from the Research Council of Norway.
NR 31
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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 20
PY 2009
VL 692
IS 2
BP 1669
EP 1677
DI 10.1088/0004-637X/692/2/1669
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 411TW
UT WOS:000263674700053
ER
PT J
AU Treu, T
Gavazzi, R
Gorecki, A
Marshall, PJ
Koopmans, LVE
Bolton, AS
Moustakas, LA
Burles, S
AF Treu, Tommaso
Gavazzi, Raphael
Gorecki, Alexia
Marshall, Philip J.
Koopmans, Leon V. E.
Bolton, Adam S.
Moustakas, Leonidas A.
Burles, Scott
TI THE SLACS SURVEY. VIII. THE RELATION BETWEEN ENVIRONMENT AND INTERNAL
STRUCTURE OF EARLY-TYPE GALAXIES (vol 690, pg 670, 2009)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Treu, Tommaso; Gavazzi, Raphael; Gorecki, Alexia; Marshall, Philip J.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Gavazzi, Raphael] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France.
[Koopmans, Leon V. E.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Bolton, Adam S.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Moustakas, Leonidas A.; Burles, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
MIT, Dept Phys, Cambridge, MA 02139 USA.
MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Treu, T (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
EM tt@physics.ucsb.edu; gavazzi@iap.fr; pjm@physics.ucsb.edu;
koopmans@astro.rug.nl; bolton@ifa.hawaii.edu; leonidas@jpl.nasa.gov;
burles@mit.edu
NR 1
TC 4
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 20
PY 2009
VL 692
IS 2
BP 1690
EP 1690
DI 10.1088/0004-637X/692/2/1690
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 411TW
UT WOS:000263674700055
ER
PT J
AU Katsuda, S
Petre, R
Long, KS
Reynolds, SP
Winkler, PF
Mori, K
Tsunemi, H
AF Katsuda, Satoru
Petre, Robert
Long, Knox S.
Reynolds, Stephen P.
Winkler, P. Frank
Mori, Koji
Tsunemi, Hiroshi
TI THE FIRST X-RAY PROPER-MOTION MEASUREMENTS OF THE FORWARD SHOCK IN THE
NORTHEASTERN LIMB OF SN 1006
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual (SN 1006); shock waves; supernova remnants; X-rays: ISM
ID TYCHOS SUPERNOVA REMNANT; RADIO-EMISSION; SN-1006; EXPANSION;
CASSIOPEIA; IMAGERY; SN1006; GAS
AB We report on the first X-ray proper-motion measurements of the nonthermally dominated forward shock in the northeastern limb of SN 1006, based on two Chandra observations taken in 2000 and 2008. We find that the proper motion of the forward shock is about 0 ''.48 yr(-1) and does not vary around the rim within the similar to 10% measurement uncertainties. The proper motion measured is consistent with that determined by previous radio observations. The mean expansion index of the forward shock is calculated to be similar to 0.54 which matches the value expected based on an evolutionary model of a Type Ia supernova with either a power-law or an exponential ejecta density profile. Assuming pressure equilibrium around the periphery from the thermally dominated northwestern rim to the nonthermally dominated northeastern rim, we estimate the ambient density to the northeast of SN 1006 to be similar to 0.085 cm(-3).
C1 [Katsuda, Satoru; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Katsuda, Satoru; Tsunemi, Hiroshi] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
[Mori, Koji] Miyazaki Univ, Dept Appl Phys, Fac Engn, Miyazaki 8892192, Japan.
RP Katsuda, S (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
EM Satoru.Katsuda@nasa.gov; Robert.Petre-1@nasa.gov; long@stsci.edu;
reynolds@ncsu.edu; winkler@middlebury.edu; mori@astro.miyazaki-u.ac.jp;
tsunemi@ess.sci.osaka-u.ac.jp
FU JSPS; NASA [NNG06EO90A]; NSF [AST 03-07613]
FX We acknowledge helpful scientific discussions with Una Hwang and Hiroya
Yamaguchi. S.K. is supported by a JSPS Research Fellowship for Young
Scientists. S.K. is also supported in part by the NASA grant under the
contract NNG06EO90A. P.F.W. acknowledges the support of the NSF through
grant AST 03-07613.
NR 29
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PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 20
PY 2009
VL 692
IS 2
BP L105
EP L108
DI 10.1088/0004-637X/692/2/L105
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 404JZ
UT WOS:000263149100010
ER
PT J
AU Taguchi, S
Hosokawa, K
Nakao, A
Collier, MR
Moore, TE
Sato, N
Yukimatu, AS
AF Taguchi, S.
Hosokawa, K.
Nakao, A.
Collier, M. R.
Moore, T. E.
Sato, N.
Yukimatu, A. S.
TI HF radar polar patch and its relation with the cusp during B-Y-dominated
IMF: Simultaneous observations at two altitudes
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; NEAR-EARTH MAGNETOSPHERE; CAP F-REGION;
SOLAR-WIND; MAGNETOPAUSE RECONNECTION; DAYSIDE MAGNETOPAUSE; IONOSPHERIC
CONVECTION; PARTICLE-PRECIPITATION; ION PRECIPITATION; DE-2 OBSERVATIONS
AB Recent studies have shown that the motion of the cusp can be deduced from the energetic neutral atom signals detected in the magnetosphere by the Low Energy Neutral Atom (LENA) imager on the IMAGE spacecraft. We use this approach to understand the characteristics of the formation of a polar patch seen in the dayside ionosphere. During a period of the 28 March 2001 LENA cusp signal event, the SuperDARN radars at Syowa East, Syowa South, and Kerguelen Island identified large-scale features of a polar patch. A region of high backscatter power observed by the radars separates into two parts around 77 degrees, and its high-latitude part moves in the poleward and duskward direction. The separation latitude is about 5 degrees higher than the equatorward boundary of the cusp, which is deduced from the LENA cusp signal. We interpret these observations, including features obtained with other SuperDARN radars in the northern hemisphere, as being due to the IMF B-Y-controlled zonal jet flow that occurred during a period of increase in vertical bar B-Y/B-Z vertical bar, without requiring the change in B-Y polarity that has been often invoked in previous studies. The sharp equatorward boundary of the radar signatures of the polar patch would be an interface between the preexisting flow generally in the antisunward direction and the enhanced zonal flow. The flow enhancement appears to be a fundamental process that forms the large-scale polar patch at latitudes several degrees higher than the cusp.
C1 [Taguchi, S.; Hosokawa, K.; Nakao, A.] Univ Electrocommun, Dept Informat & Commun Engn, Tokyo 1828585, Japan.
[Collier, M. R.; Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sato, N.; Yukimatu, A. S.] Natl Inst Polar Res, Tokyo 1738515, Japan.
RP Taguchi, S (reprint author), Univ Electrocommun, Dept Informat & Commun Engn, Tokyo 1828585, Japan.
EM taguchi@ice.uec.ac.jp
RI Moore, Thomas/D-4675-2012; Collier, Michael/I-4864-2013
OI Moore, Thomas/0000-0002-3150-1137; Collier, Michael/0000-0001-9658-6605
FU Japan Society for the Promotion of Science [18540443]; IMAGE Project
[UPN 370-28-20]
FX This research was supported by Grant-in-Aid for Scientific Research (C)
18540443 under Japan Society for the Promotion of Science and by the
IMAGE Project under UPN 370-28-20 at Goddard Space Flight Center. The
authors would like to acknowledge valuable discussion with Yozo Murata
and Shin Suzuki. The authors are indebted to the PIs of the various
SuperDARN radars, without whose efforts this study would not have been
possible. The 41th Japanese Antarctic Research Expedition (JARE) has
carried out the HF radar operation at Syowa station. CUTLASS (Hankasalmi
and Pykkvybaer radar pair) is supported by an award from STFC. The
authors also thank C. T. Russell (PI of Polar magnetic field data), D.
McComas (PI of ACE plasma data), N. Ness (PI of ACE magnetic field
data), J. H. King, and N. Papatashvilli (OMNI data) for providing data
through the NASA CDAWeb.
NR 79
TC 5
Z9 5
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD FEB 20
PY 2009
VL 114
AR A02311
DI 10.1029/2008JA013624
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410YT
UT WOS:000263614900003
ER
PT J
AU Stow, CA
Jolliff, J
McGillicuddy, DJ
Doney, SC
Allen, JI
Friedrichs, MAM
Rose, KA
Wallheadg, P
AF Stow, Craig A.
Jolliff, Jason
McGillicuddy, Dennis J., Jr.
Doney, Scott C.
Allen, J. Icarus
Friedrichs, Marjorie A. M.
Rose, Kenneth A.
Wallheadg, Philip
TI Skill assessment for coupled biological/physical models of marine
systems
SO JOURNAL OF MARINE SYSTEMS
LA English
DT Article
DE Goodness-of-fit; Skill metric; Skill assessment; Model uncertainty
ID WATER-QUALITY MODELS; ECOSYSTEM MODEL; DATA ASSIMILATION;
DECISION-MAKING; CURRENT STATE; OCEAN MODEL; NORTH-SEA; UNCERTAINTY;
QUANTIFICATION; VARIABILITY
AB Coupled biological/physical models of marine systems serve many purposes including the synthesis of information, hypothesis generation, and as a tool for numerical experimentation. However, marine system models are increasingly used for prediction to support high-stakes decision-making. In such applications it is imperative that a rigorous model skill assessment is conducted so that the model's capabilities are tested and understood. Herein, we review several metrics and approaches useful to evaluate model skill. The definition of skill and the determination of the skill level necessary for a given application is context specific and no single metric is likely to reveal all aspects of model skill. Thus, we recommend the use of several metrics, in concert, to provide a more thorough appraisal. The routine application and presentation of rigorous skill assessment metrics will also serve the broader interests of the modeling community, ultimately resulting in improved forecasting abilities as well as helping us recognize our limitations. Published by Elsevier B.V.
C1 [Stow, Craig A.] NOAA, Great Lakes Environm Res Lab, Ann Arbor, MI 48105 USA.
[Jolliff, Jason] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS USA.
[McGillicuddy, Dennis J., Jr.; Doney, Scott C.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Allen, J. Icarus] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England.
[Friedrichs, Marjorie A. M.] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA.
[Rose, Kenneth A.] Louisiana State Univ, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA.
[Wallheadg, Philip] Natl Oceanog Ctr, Southampton, Hants, England.
RP Stow, CA (reprint author), NOAA, Great Lakes Environm Res Lab, 2205 Commonwealth Blvd, Ann Arbor, MI 48105 USA.
EM craig.stow@noaa.gov; jolliff@nrissc.navy.mil; dmcgillicuddy@whoi.edu;
sdoney@whoi.edu; jia@pml.ac.uk; marjy@vims.edu; karose@lsu.edu;
pjw5@noc.soton.ac.uk
RI Doney, Scott/F-9247-2010;
OI Doney, Scott/0000-0002-3683-2437; Stow, Craig/0000-0001-6171-7855;
Friedrichs, Marjorie/0000-0003-2828-7595
FU NERC core strategic Oceans2025 program; NOAA; NSF; NIEHS; ECOHAB
FX JIA was funded by theme 9 of the NERC core strategic Oceans2025 program.
This manuscript is GLERL contribution number 1464. DJM gratefully
acknowledges support from NOAA, NSF, and NIEHS; this is ECOHAB
contribution number 281.
NR 59
TC 159
Z9 161
U1 3
U2 43
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0924-7963
EI 1879-1573
J9 J MARINE SYST
JI J. Mar. Syst.
PD FEB 20
PY 2009
VL 76
IS 1-2
SI SI
BP 4
EP 15
DI 10.1016/j.jmarsys.2008.03.011
PG 12
WC Geosciences, Multidisciplinary; Marine & Freshwater Biology;
Oceanography
SC Geology; Marine & Freshwater Biology; Oceanography
GA 414GD
UT WOS:000263851000002
PM 28366997
ER
PT J
AU Gregg, WW
Friedrichs, MAM
Robinson, AR
Rose, KA
Schlitzer, R
Thompson, KR
Doney, SC
AF Gregg, Watson W.
Friedrichs, Marjorie A. M.
Robinson, Allan R.
Rose, Kenneth A.
Schlitzer, Reiner
Thompson, Keith R.
Doney, Scott C.
TI Skill assessment in ocean biological data assimilation
SO JOURNAL OF MARINE SYSTEMS
LA English
DT Article
DE Data assimilation; Ocean biology models; Ocean biogeochemistry models;
Skill assessment; Fisheries data assimilation; Fisheries models
ID MARINE ECOSYSTEM MODEL; PHYSICAL-BIOGEOCHEMICAL MODEL; CONSTRAINT
PARAMETER-ESTIMATION; EFFICIENT DATA ASSIMILATION; SALMON
ONCORHYNCHUS-NERKA; ENSEMBLE KALMAN FILTER; ATLANTIC TIME-SERIES;
1997-98 EL-NINO; IN-SITU DATA; NORTH-ATLANTIC
AB There is growing recognition that rigorous skill assessment is required to understand the ability of ocean biological models to represent ocean processes and distributions. Statistical analysis of model results with observations represents the most quantitative form of skill assessment, and this principle serves as well for data assimilation models. However, skill assessment for data assimilation requires special consideration. This is because there are three sets of information in data assimilation: the free-run model, data, and the assimilation model, which uses information from both the free-run model and the data. Intercomparison of results among the three sets of information is important and useful for assessment, but is not conclusive since the three information sets are intertwined. An independent data set is necessary for an objective determination. Other useful measures of ocean biological data assimilation assessment include responses of unassimilated variables to the data assimilation, performance outside the prescribed region/time of interest, forecasting, and trend analysis. Examples of each approach from the literature are provided. A comprehensive list of ocean biological data assimilation and their applications of skill assessment, in both ecosystem/biogeochernical and fisheries efforts, is summarized. Published by Elsevier B.V.
C1 [Gregg, Watson W.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Friedrichs, Marjorie A. M.] Coll William & Mary, Virginia Inst Marine Sci, Williamsburg, VA 23187 USA.
[Robinson, Allan R.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Rose, Kenneth A.] Louisiana State Univ, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA.
[Thompson, Keith R.] Dalhousie Univ, Halifax, NS B3H 3J5, Canada.
RP Gregg, WW (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
EM watson.gregg@nasa.gov
RI Doney, Scott/F-9247-2010;
OI Doney, Scott/0000-0002-3683-2437; Friedrichs,
Marjorie/0000-0003-2828-7595
FU NASA/GMAO; NASA Modeling, Analysis and Prediction Program; NASA Ocean
Biology and Biogeochemistry Program
FX We thank Steven Pawson, NASA/GMAO, and 3 anonymous reviewers for review
and commentary of the manuscript. We also thank members of the Skill
Assessment Worldng Team (Skill Assessment for Coupled
Biological/Physical Models of Marine Systems held July 11-13, 2006 and
March 6-8, 2007 at Chapel RdI, NC) for insightful discussions on data
assimilation and its evaluation, especially Icarus Allen, Geoffrey
Evans, Dale Haidvoget, John Kindle, Daniel Lynch, Dennis McGillicuddy,
Roger Proctor, and Dougie Speirs. The two workshops were sponsored by
the NOAA Center for Sponsored Coastal Ocean Research. We thank Andreas
Oschlies, Caroline Raick, and Ricardo Torres for permission to use
figures. This work was partially supported by the NASA Modeling,
Analysis and Prediction Program (to WWG and SCD) and NASA Ocean Biology
and Biogeochemistry Program (to MAMF).
NR 85
TC 38
Z9 39
U1 0
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0924-7963
J9 J MARINE SYST
JI J. Mar. Syst.
PD FEB 20
PY 2009
VL 76
IS 1-2
BP 16
EP 33
DI 10.1016/j.jmarsys.2008.05.006
PG 18
WC Geosciences, Multidisciplinary; Marine & Freshwater Biology;
Oceanography
SC Geology; Marine & Freshwater Biology; Oceanography
GA 414GD
UT WOS:000263851000003
ER
PT J
AU Gregg, WW
Casey, NW
AF Gregg, Watson W.
Casey, Nancy W.
TI Skill assessment of a spectral ocean-atmosphere radiative model
SO JOURNAL OF MARINE SYSTEMS
LA English
DT Article
DE Radiative transfer; Ocean ecosystems; Surface irradiance; Spectral
irradiance; Shortwave radiation; Primary production
ID OPTICAL-PROPERTIES; SOLAR IRRADIANCE; WATER CLOUDS; PHYTOPLANKTON;
ABSORPTION; REFLECTANCE; VALIDATION; EFFICIENCY; SURFACE; ISCCP
AB Ocean phytoplankton, cletrital material, and water absorb and scatter light spectrally. The Ocean-Atmosphere Spectral Irradiance Model (OASIM) is intended to provide surface irradiance over the oceans with sufficient spectral resolution to support ocean ecology, biogeochemistry, and heat exchange investigations, and of sufficient duration to support inter-annual and decadal investigations. OASIM total surface irradiance (integrated 200 nm to 4 pm) was compared to in situ data and three publicly available global data products at monthly 1-degree resolution. OASIM spectrally-integrated surface irradiance had root mean square (RMS) difference= 20.1 W m(-2) (about 11%), bias= 1.6 W m(-2) (about 0.8%), regression slope= 1.01 and correlation coefficient=0.89, when compared to 2322 in situ observations. OASIM had the lowest bias of any of the global data products evaluated (ISCCP-FD, NCEP, and ISLSCP 11), and the best slope (nearest to unity). It had the second best RMS, and the third best correlation coefficient. OASIM total surface irradiance compared well with ISCCP-FD (RMS = 20.7 Wm(-2); bias-11.4 Wm(-2) r=0.98) and ISLSCP II(RMS=25.2 Wm(-2); bias =-13.8 Wm(-2) : r = 0.97), but less well with NCEP (RMS = 43.0 W m(-2); bias =-22.6W m(-2); r=0.91). Comparisons of OASIM photosynthetically available radiation (PAR) with PAR derived from SeaWiFS showed low bias (-1.8 mol photons m(-2) d(-1), or about 5%), RMS (4.25 mol photons m-2 d(-1), or about 12%), near unity slope (1.03) and high correlation coefficient (0.97). Coupled with previous estimates of clear sky spectral irradiance in OASIM (6.6% RMS at 1 nm resolution), these results suggest that OASIM provides reasonable estimates of surface broadband and spectral irradiance in the oceans, and can support studies on ocean ecosystems, carbon cycling, and heat exchange. Published by Elsevier B.V.
C1 [Gregg, Watson W.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Casey, Nancy W.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Gregg, WW (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
EM watson.gregg@nasa.gov; ncasey@gmao.gsfc.nasa.gov
NR 38
TC 9
Z9 9
U1 0
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0924-7963
EI 1879-1573
J9 J MARINE SYST
JI J. Mar. Syst.
PD FEB 20
PY 2009
VL 76
IS 1-2
SI SI
BP 49
EP 63
DI 10.1016/j.jmarsys.2008.05.007
PG 15
WC Geosciences, Multidisciplinary; Marine & Freshwater Biology;
Oceanography
SC Geology; Marine & Freshwater Biology; Oceanography
GA 414GD
UT WOS:000263851000005
ER
PT J
AU Friedrichs, MAM
Carr, ME
Barber, RT
Scardi, M
Antoine, D
Armstrong, RA
Asanuma, I
Behrenfeld, MJ
Buitenhuis, ET
Chai, F
Christian, JR
Ciotti, AM
Doney, SC
Dowell, M
Dunne, J
Gentili, B
Gregg, W
Hoepffner, N
Ishizaka, J
Kameda, T
Lima, I
Marra, J
Melin, F
Moore, JK
Morel, A
O'Malley, RT
O'Reilly, J
Saba, VS
Schmeltz, M
Smyth, TJ
Tjiputra, J
Waters, K
Westberry, TK
Winguth, A
AF Friedrichs, Marjorie A. M.
Carr, Mary-Elena
Barber, Richard T.
Scardi, Michele
Antoine, David
Armstrong, Robert A.
Asanuma, Ichio
Behrenfeld, Michael J.
Buitenhuis, Erik T.
Chai, Fei
Christian, James R.
Ciotti, Aurea M.
Doney, Scott C.
Dowell, Mark
Dunne, John
Gentili, Bernard
Gregg, Watson
Hoepffner, Nicolas
Ishizaka, Joji
Kameda, Takahiko
Lima, Ivan
Marra, John
Melin, Frederic
Moore, J. Keith
Morel, Andre
O'Malley, Robert T.
O'Reilly, Jay
Saba, Vincent S.
Schmeltz, Marjorie
Smyth, Tim J.
Tjiputra, Jerry
Waters, Kirk
Westberry, Toby K.
Winguth, Arne
TI Assessing the uncertainties of model estimates of primary productivity
in the tropical Pacific Ocean
SO JOURNAL OF MARINE SYSTEMS
LA English
DT Article
DE Primary production; Modeling; Remote sensing; Satellite ocean color;
Statistical analysis; Tropical Pacific Ocean (15 degrees N to 15 degrees
S and 125 degrees E; to 95 degrees W)
ID CENTRAL EQUATORIAL PACIFIC; GENERAL-CIRCULATION MODEL; MARINE ECOSYSTEM
MODEL; SKILL ASSESSMENT; INTERANNUAL VARIABILITY; SATELLITE CHLOROPHYLL;
METAL CONTAMINATION; REGIONAL SCALES; ARABIAN SEA; COLOR
AB Depth-integrated primary productivity (PP) estimates obtained from satellite ocean color-based models (SatPPMs) and those generated from biogeochemical ocean general circulation models (BCGCMs) represent a key resource for biogeochemical and ecological studies at global as well as regional scales. Calibration and validation of these PP models are not straightforward, however, and comparative studies show large differences between model estimates. The goal of this paper is to compare PP estimates obtained from 30 different models (21 SatPPMs and 9 BOGCMs) to a tropical Pacific PP database consisting of similar to 1000 C-14 measurements spanning more than a decade (1983-1996). Primary findings include: skill varied significantly between models, but performance was not a function of model complexity or type (i.e. SatPPM vs. BOGCM); nearly all models underestimated the observed variance of PR specifically yielding too few low PP (< 0.2 g Cm-2 d(-1)) values; more than half of the total root-mean-squared model-data differences associated with the satellite-based PP models might be accounted for by uncertainties in the input variables and/or the PP data; and the tropical Pacific database captures a broad scale shift from low biomassnormalized productivity in the 1980s to higher biomass-normalized productivity in the 1990s, which was not successfully captured by any of the models. This latter result suggests that interdecadal and global changes will be a significant challenge for both SatPPMs and BOGCMs. Finally, average root-mean-squared differences between in situ PP data on the equator at 140 degrees W and PP estimates from the satellite-based productivity models were 58% lower than analogous values computed in a previous PP model comparison 6 years ago. The success of these types of comparison exercises is illustrated by the continual modification and improvement of the participating models and the resulting increase in model skill. (C) 2008 Elsevier BY. All rights reserved.
C1 [Friedrichs, Marjorie A. M.; Saba, Vincent S.] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA.
[Carr, Mary-Elena; Schmeltz, Marjorie] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
[Barber, Richard T.] Duke Univ, Marine Lab, Beaufort, NC 28516 USA.
[Scardi, Michele] Univ Roma Tor Vergata, Dept Biol, I-00133 Rome, Italy.
[Antoine, David; Gentili, Bernard; Morel, Andre] Univ Paris 06, Paris 6, France.
[Antoine, David; Gentili, Bernard; Morel, Andre] CNRS, Lab Oceanog Villefranche, Paris, France.
[Armstrong, Robert A.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
[Asanuma, Ichio] Tokyo Univ Informat Sci, Wakaba Ku, Chiba 2658501, Japan.
[Behrenfeld, Michael J.; O'Malley, Robert T.; Westberry, Toby K.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA.
[Buitenhuis, Erik T.] Univ E Anglia, Lab Global Marine & Atmospher Chem, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England.
[Chai, Fei] Univ Maine, Sch Marine Sci, Orono, ME 04469 USA.
[Christian, James R.] Fisheries & Oceans Canada, Sidney, BC V8L 4B2, Canada.
[Ciotti, Aurea M.] Univ Estadual Paulista, BR-11330900 Sao Paulo, Brazil.
[Doney, Scott C.; Lima, Ivan] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA.
[Dowell, Mark; Hoepffner, Nicolas; Melin, Frederic] Commiss European Communities, Joint Res Ctr, I-21020 Ispra, Italy.
[Dunne, John] Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
[Gregg, Watson] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Ishizaka, Joji] Nagasaki Univ, Fac Fisheries, Nagasaki 8528521, Japan.
[Kameda, Takahiko] Natl Res Inst Far Seas Fisheries, Grp Oceanog, Shizuoka 4248633, Japan.
[Marra, John] CUNY Brooklyn Coll, Dept Geol, Brooklyn, NY 11210 USA.
[Moore, J. Keith] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[O'Reilly, Jay] NOAA NMFS Narragansett Lab, Narragansett, RI 02887 USA.
[Smyth, Tim J.] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England.
[Tjiputra, Jerry] Bjerknes Ctr Climate Res, N-5007 Bergen, Norway.
[Waters, Kirk] NOAA Coastal Serv Ctr, Charleston, SC 29405 USA.
[Winguth, Arne] Univ Texas Arlington, Dept Earth & Environm Sci, Arlington, TX 76019 USA.
RP Friedrichs, MAM (reprint author), Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA.
EM mady@vims.edu; mcarr@ei.columbia.edu; rbarber@duke.edu;
mscardi@mclink.it; antoine@obs-vlfr.fr; rarmstrong@notes.cc.sunysb.edu;
asanuma@rsch.tuis.ac.jp; mjb@science.oregonstate.edu;
martinburo@email.com; fchai@umaine.edu; Jim.Christian@ec.gc.ca;
ciotti@csv.unesp.br; sdoney@whoi.edu; mark.dowell@jrc.it;
jpd@gfdl.noaa.gov; gentili@obs-vlfr.fr; watson.gregg@nasa.gov;
nicolas.hoepffner@jrc.it; ishizaka@nagasaki-u.ac.jp;
takukame@affrc.go.jp; ilima@whoi.edu; jfm7780@brooklyn.cuny.edu;
frederic.melin@jrc.it; jkmoore@uci.edu; morel@obs-vifr.fr;
omalleyr@science.oregonstate.edu; jay.oreiliy@noaa.gov; vssaba@vims.edu;
tjsm@pml.ac.uk; jtj061@bjerknes.uib.no; kirk.waters@noaa.gov;
toby.westberry@sdence.oregonstate.edu; awinguth@uta.edu
RI Armstrong, Robert/C-9086-2009; Ciotti, Aurea Maria/B-7188-2011;
Buitenhuis, Erik/A-7692-2012; Smyth, Tim/D-2008-2012; Doney,
Scott/F-9247-2010; Dunne, John/F-8086-2012; Westberry, Toby/A-9871-2013;
Antoine, David/C-3817-2013; Lima, Ivan/A-6823-2016;
OI Friedrichs, Marjorie/0000-0003-2828-7595; Ciotti, Aurea
Maria/0000-0001-7163-8819; Buitenhuis, Erik/0000-0001-6274-5583; Doney,
Scott/0000-0002-3683-2437; Dunne, John/0000-0002-8794-0489; Antoine,
David/0000-0002-9082-2395; Lima, Ivan/0000-0001-5345-0652; Tjiputra,
Jerry/0000-0002-4600-2453
NR 99
TC 109
Z9 111
U1 4
U2 56
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0924-7963
J9 J MARINE SYST
JI J. Mar. Syst.
PD FEB 20
PY 2009
VL 76
IS 1-2
SI SI
BP 113
EP 133
DI 10.1016/j.jmarsys.2008.05.010
PG 21
WC Geosciences, Multidisciplinary; Marine & Freshwater Biology;
Oceanography
SC Geology; Marine & Freshwater Biology; Oceanography
GA 414GD
UT WOS:000263851000009
ER
PT J
AU Tansel, B
Sager, J
Garland, J
Xu, SH
AF Tansel, Berrin
Sager, John
Garland, Jay
Xu, Shaohua
TI Effect of transmembrane pressure on overall membrane resistance during
cross-flow filtration of solutions with high-ionic content
SO JOURNAL OF MEMBRANE SCIENCE
LA English
DT Article
DE Membrane flux; Membrane resistance; Mass transfer limitation; Limiting
flux; Ionic crowding
ID CRITICAL FLUX; NANOFILTRATION; NF
AB The purpose of the study was to investigate the change in membrane resistance in relation to operating pressure for clean RO and NF membranes during filtration of a bioreactor effluent. Experiments were conducted using a SEPA CFII membrane element cell and effluent from a bioreactor with high-ionic content. Flux-pressure profiles of two RO and one NF membranes were analyzed and compared with those for filtration of deionized water. The flux-pressure profile increased linearly with increasing pressure for all three membranes during filtration of deionized water. However, during filtration of the bioreactor effluent, the rate of increase in flux decreased after the pressure reached a critical level with both RO membranes. The changes in flux and membrane resistance were analyzed in relation to the operating pressure which was correlated to transmembrane pressure using logarithmic and second order polynomial correlations. Experimental results showed that a second order polynomial function described the flux-pressure profile more adequately than the linear correlation. The use of the flux ratio (i.e., flux with bioreactor effluent to flux with deionized water) allowed a basis for comparison of change in membrane resistance with transmembrane pressure for different membranes. The critical pressure which resulted in the minimum membrane resistance was determined by the change in the membrane resistance expressed in dimension-less form as the ratio of the observed membrane resistance with bioreactor effluent and deionized water. (c) 2008 Elsevier B.V. All rights reserved.
C1 [Tansel, Berrin] Florida Int Univ, Dept Civil & Environm Engn, Miami, FL 33146 USA.
[Sager, John] NASA, Cape Canaveral, FL 32899 USA.
[Garland, Jay] Gen Dynam Corp, Cape Canaveral, FL 32899 USA.
[Xu, Shaohua] Florida Space Res Inst, Cape Canaveral, FL 32899 USA.
RP Tansel, B (reprint author), Florida Int Univ, Dept Civil & Environm Engn, Miami, FL 33146 USA.
EM tanselb@fiu.edu
NR 11
TC 5
Z9 5
U1 1
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0376-7388
J9 J MEMBRANE SCI
JI J. Membr. Sci.
PD FEB 20
PY 2009
VL 328
IS 1-2
BP 205
EP 210
DI 10.1016/j.memsci.2008.12.003
PG 6
WC Engineering, Chemical; Polymer Science
SC Engineering; Polymer Science
GA 414UV
UT WOS:000263891600024
ER
PT J
AU Mumma, MJ
Villanueva, GL
Novak, RE
Hewagama, T
Bonev, BP
DiSanti, MA
Mandell, AM
Smith, MD
AF Mumma, Michael J.
Villanueva, Geronimo L.
Novak, Robert E.
Hewagama, Tilak
Bonev, Boncho P.
DiSanti, Michael A.
Mandell, Avi M.
Smith, Michael D.
TI Strong Release of Methane on Mars in Northern Summer 2003
SO SCIENCE
LA English
DT Article
ID MARTIAN DUST DEVILS; MU-M; OXIDANT ENHANCEMENT; ATMOSPHERE; LIFE;
ORIGIN; CH4; HABITABILITY; SPECTROSCOPY; SPECTRUM
AB Living systems produce more than 90% of Earth's atmospheric methane; the balance is of geochemical origin. On Mars, methane could be a signature of either origin. Using high- dispersion infrared spectrometers at three ground- based telescopes, we measured methane and water vapor simultaneously on Mars over several longitude intervals in northern early and late summer in 2003 and near the vernal equinox in 2006. When present, methane occurred in extended plumes, and the maxima of latitudinal profiles imply that the methane was released from discrete regions. In northern midsummer, the principal plume contained similar to 19,000 metric tons of methane, and the estimated source strength (>= 0.6 kilogram per second) was comparable to that of the massive hydrocarbon seep at Coal Oil Point in Santa Barbara, California.
C1 [Mumma, Michael J.; Villanueva, Geronimo L.; Hewagama, Tilak; Bonev, Boncho P.; DiSanti, Michael A.; Mandell, Avi M.; Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Villanueva, Geronimo L.; Bonev, Boncho P.] Univ Amer, Dept Phys, Washington, DC 20008 USA.
[Novak, Robert E.] Iona Coll, Dept Phys, New Rochelle, NY 10801 USA.
[Hewagama, Tilak] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Mumma, MJ (reprint author), NASA, Goddard Space Flight Ctr, Mailstop 690-3, Greenbelt, MD 20771 USA.
EM michael.j.mumma@nasa.gov
RI Hewagama, T/C-8488-2012; Smith, Michael/C-8875-2012; Mandell,
Avi/F-9361-2012; mumma, michael/I-2764-2013
FU NASA the Planetary Astronomy Program [RTOP 344-32-07]; Astrobiology
Institute [RTOP 344-53-51]; NSF Research at Undergraduate Institutions
Program [AST-0505765]
FX We thank T. C. Onstott and L. M. Pratt for helpful comments and two
anonymous referees for their comments and suggestions. This work was
supported by NASA [the Planetary Astronomy Program (RTOP 344-32-07 to
M.J.M), Astrobiology Institute (RTOP 344-53-51, to M.J.M), and
Postdoctoral Program (G.L.V.)] by NSF (Research at Undergraduate
Institutions Program AST-0505765 to R.E.N.). We thank the director and
staff of NASA's InfraRed Telescope Facility (operated for NASA by the
University of Hawaii) for exceptional support throughout our long Mars
observing program. Data were also obtained at the W. M. Keck
Observatory, operated as a scientific partnership by CalTech, the
University of California Los Angeles, and NASA.
NR 42
TC 267
Z9 277
U1 12
U2 83
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 20
PY 2009
VL 323
IS 5917
BP 1041
EP 1045
DI 10.1126/science.1165243
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 409AK
UT WOS:000263478400036
PM 19150811
ER
PT J
AU Gruber, N
Gloor, M
Fletcher, SEM
Doney, SC
Dutkiewicz, S
Follows, MJ
Gerber, M
Jacobson, AR
Joos, F
Lindsay, K
Menemenlis, D
Mouchet, A
Muller, SA
Sarmiento, JL
Takahashi, T
AF Gruber, Nicolas
Gloor, Manuel
Fletcher, Sara E. Mikaloff
Doney, Scott C.
Dutkiewicz, Stephanie
Follows, Michael J.
Gerber, Markus
Jacobson, Andrew R.
Joos, Fortunat
Lindsay, Keith
Menemenlis, Dimitris
Mouchet, Anne
Mueller, Simon A.
Sarmiento, Jorge L.
Takahashi, Taro
TI Oceanic sources, sinks, and transport of atmospheric CO2
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Review
ID ANTHROPOGENIC CARBON-DIOXIDE; AIR-SEA FLUX; ATLANTIC-OCEAN; INORGANIC
CARBON; WIND-SPEED; INTERHEMISPHERIC TRANSPORT; THERMOHALINE
CIRCULATION; INTERANNUAL VARIABILITY; EQUATORIAL PACIFIC; CYCLE
FEEDBACKS
AB We synthesize estimates of the contemporary net air-sea CO2 flux on the basis of an inversion of interior ocean carbon observations using a suite of 10 ocean general circulation models (Mikaloff Fletcher et al., 2006, 2007) and compare them to estimates based on a new climatology of the air-sea difference of the partial pressure of CO2 (pCO(2)) (Takahashi et al., 2008). These two independent flux estimates reveal a consistent description of the regional distribution of annual mean sources and sinks of atmospheric CO2 for the decade of the 1990s and the early 2000s with differences at the regional level of generally less than 0.1 Pg C a(-1). This distribution is characterized by outgassing in the tropics, uptake in midlatitudes, and comparatively small fluxes in the high latitudes. Both estimates point toward a small(similar to -0.3 Pg C a(-1)) contemporary CO2 sink in the Southern Ocean (south of 44 degrees S), a result of the near cancellation between a substantial outgassing of natural CO2 and a strong uptake of anthropogenic CO2. A notable exception in the generally good agreement between the two estimates exists within the Southern Ocean: the ocean inversion suggests a relatively uniform uptake, while the pCO(2)-based estimate suggests strong uptake in the region between 58 degrees S and 44 degrees S, and a source in the region south of 58 degrees S. Globally and for a nominal period between 1995 and 2000, the contemporary net air-sea flux of CO2 is estimated to be -1.7 +/- 0.4 Pg C a(-1) (inversion) and -1.4 +/- 0.7 Pg C a(-1) (pCO(2)-climatology), respectively, consisting of an outgassing flux of river-derived carbon of similar to+0.5 Pg C a(-1), and an uptake flux of anthropogenic carbon of -2.2 +/- 0.3 Pg C a(-1) (inversion) and -1.9 +/- 0.7 Pg C a(-1) (pCO(2)-climatology). The two flux estimates also imply a consistent description of the contemporary meridional transport of carbon with southward ocean transport throughout most of the Atlantic basin, and strong equatorward convergence in the Indo-Pacific basins. Both transport estimates suggest a small hemispheric asymmetry with a southward transport of between -0.2 and -0.3 Pg C a(-1) across the equator. While the convergence of these two independent estimates is encouraging and suggests that it is now possible to provide relatively tight constraints for the net air-sea CO2 fluxes at the regional basis, both studies are limited by their lack of consideration of long-term changes in the ocean carbon cycle, such as the recent possible stalling in the expected growth of the Southern Ocean carbon sink.
C1 [Gruber, Nicolas] ETH, Inst Biogeochem & Pollutant Dynam, CH-8092 Zurich, Switzerland.
[Gloor, Manuel] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
[Gloor, Manuel] Univ Leeds, Inst Earth & Biosphere, Leeds LS2 9JT, W Yorkshire, England.
[Gloor, Manuel] Univ Leeds, Inst Earth Energy & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Fletcher, Sara E. Mikaloff] Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA.
[Doney, Scott C.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Dutkiewicz, Stephanie; Follows, Michael J.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Gerber, Markus; Joos, Fortunat; Mueller, Simon A.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Jacobson, Andrew R.] NOAA, Earth Syst Res Lab, Global Monitoring Div, Boulder, CO 80305 USA.
[Lindsay, Keith] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Menemenlis, Dimitris] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mouchet, Anne] Univ Liege, Astrophys & Geophys Inst, B-4000 Liege, Belgium.
[Takahashi, Taro] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
RP Gruber, N (reprint author), ETH, Inst Biogeochem & Pollutant Dynam, CHN E31-2,Univ Str 16, CH-8092 Zurich, Switzerland.
EM nicolas.gruber@env.ethz.ch; e.gloor@leeds.ac.uk; mikaloff@princeton.edu;
sdoney@whoi.edu; stephd@ocean.mit.edu; mick@ocean.mit.edu;
mgerber@climate.unibe.ch; andy.jacobson@noaa.gov; joos@climate.unibe.ch;
klindsay@ucar.edu; menemenlis@jpl.nasa.gov; a.mouchet@ulg.ac.be;
s.a.mueller@open.ac.uk; jls@princeton.edu; taka@ldeo.columbia.edu
RI Gruber, Nicolas/B-7013-2009; Follows, Michael/G-9824-2011; Doney,
Scott/F-9247-2010; Mouchet, Anne/K-1911-2014;
OI Gruber, Nicolas/0000-0002-2085-2310; Doney, Scott/0000-0002-3683-2437;
Mouchet, Anne/0000-0002-8846-3063; Mikaloff Fletcher,
Sara/0000-0003-0741-0320; Joos, Fortunat/0000-0002-9483-6030
NR 111
TC 209
Z9 217
U1 10
U2 143
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0886-6236
EI 1944-9224
J9 GLOBAL BIOGEOCHEM CY
JI Glob. Biogeochem. Cycle
PD FEB 18
PY 2009
VL 23
AR GB1005
DI 10.1029/2008GB003349
PG 21
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA 410XM
UT WOS:000263611600003
ER
PT J
AU Ao, CO
Hajj, GA
Meehan, TK
Dong, D
Iijima, BA
Mannucci, AJ
Kursinski, ER
AF Ao, C. O.
Hajj, G. A.
Meehan, T. K.
Dong, D.
Iijima, B. A.
Mannucci, A. J.
Kursinski, E. R.
TI Rising and setting GPS occultations by use of open-loop tracking
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GLOBAL POSITIONING SYSTEM; LOW-EARTH-ORBIT; RADIO OCCULTATION; LOWER
TROPOSPHERE; ATMOSPHERE; SIGNALS; SUPERREFRACTION; REFRACTIVITY;
INVERSION; CHAMP
AB The success of GPS occultations has been demonstrated by several missions including GPS/MET, CHAMP, SAC-C, GRACE, and COSMIC. However, tracking the GPS signal in the lower troposphere or obtaining accurate refractivity there has proven particularly challenging. The first receiver software with open-loop (OL) tracking capability was recently tested and successfully implemented on SAC-C. Besides improving the ability to probe deeper into the lower troposphere and planetary boundary layer, OL tracking also enables the acquisition of rising GPS signals for the first time, thereby doubling the number of occultations from the same instrument. In this paper, we describe the atmospheric Doppler and delay models used in the SAC-C and COSMIC OL tracking software. We discuss the testing carried out on SAC-C and present some examples of OL processing. We show that OL data give vast improvements in sampling the lowest part of the atmosphere. Over 80% of the SAC-C OL profiles now reach below 2 km altitude in the tropics, compared to only 50% achieved under closed-loop tracking.
C1 [Ao, C. O.; Hajj, G. A.; Meehan, T. K.; Dong, D.; Iijima, B. A.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kursinski, E. R.] Univ Arizona, Dept Atmospher Sci, Tucson, AZ 85721 USA.
RP Ao, CO (reprint author), CALTECH, Jet Prop Lab, M-S 138-308,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM chi.o.ao@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. We wish to thank Da Kuang and Marc Pestana for
assistance in data processing. We would like to thank Michael Armatys
for the 50-bps GPS navigation data collected with the NASA Global
Differential GPS system.
NR 33
TC 24
Z9 24
U1 2
U2 6
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 18
PY 2009
VL 114
AR D04101
DI 10.1029/2008JD010483
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 410XS
UT WOS:000263612200003
ER
PT J
AU Kaul, AB
Megerian, KG
von Allmen, P
Baron, RL
AF Kaul, Anupama B.
Megerian, Krikor G.
von Allmen, Paul
Baron, Richard L.
TI Single, aligned carbon nanotubes in 3D nanoscale architectures enabled
by top-down and bottom-up manufacturable processes
SO NANOTECHNOLOGY
LA English
DT Article
ID CHEMICAL-VAPOR-DEPOSITION; GROWTH; ARRAYS
AB We have developed manufacturable approaches for forming single, vertically aligned carbon nanotubes, where the tubes are centered precisely, and placed within a few hundred nm of 1-1.5 mu m deep trenches. These wafer-scale approaches were enabled by using chemically amplified resists and high density, low pressure plasma etching techniques to form the 3D nanoscale architectures. The tube growth was performed using dc plasma-enhanced chemical vapor deposition (PECVD), and the materials used in the pre-fabricated 3D architectures were chemically and structurally compatible with the high temperature (700 degrees C) PECVD synthesis of our tubes, in an ammonia and acetylene ambient. Such scalable, high throughput top-down fabrication processes, when integrated with the bottom-up tube synthesis techniques, should accelerate the development of plasma grown tubes for a wide variety of applications in electronics, such as nanoelectromechanical systems, interconnects, field emitters and sensors. Tube characteristics were also engineered to some extent, by adjusting the Ni catalyst thickness, as well as the pressure and plasma power during growth.
C1 [Kaul, Anupama B.; Megerian, Krikor G.; von Allmen, Paul; Baron, Richard L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kaul, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM anupama.b.kaul@jpl.nasa.gov
FU National Aeronautics and Space Administration; internal Research and
Technology Development (RTD) program
FX We would like to thank Mr Robert Kowalczyk for making system
modifications to the dc PECVD growth chamber, Dr Eric Wong for thermal
CVD growth (figure 3(d)), Mr Anthony Turner for assistance with layout
software, Dr Henry LeDuc for the use of deposition equipment, and Dr
Choonsup Lee for useful discussions. This research was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration and
was funded through the internal Research and Technology Development
(R&TD) program.
NR 23
TC 9
Z9 9
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD FEB 18
PY 2009
VL 20
IS 7
AR 075303
DI 10.1088/0957-4484/20/7/075303
PG 10
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 399FP
UT WOS:000262786100010
PM 19417414
ER
PT J
AU Sharma, R
Das, PP
Misra, M
Mahajan, V
Bock, JP
Trigwell, S
Biris, AS
Mazumder, MK
AF Sharma, Rajesh
Das, Prajna P.
Misra, Mano
Mahajan, Vishal
Bock, Jacob P.
Trigwell, Steve
Biris, Alexandru S.
Mazumder, Malay K.
TI Enhancement of the photoelectrochemical conversion efficiency of
nanotubular TiO2 photoanodes using nitrogen plasma assisted surface
modification
SO NANOTECHNOLOGY
LA English
DT Article
ID VISIBLE-LIGHT IRRADIATION; METAL ION-IMPLANTATION; PHOTOCATALYTIC
ACTIVITY; DOPED TIO2; THIN-FILM; OXYGEN; WATER; ARRAYS; PHOTOREACTIVITY;
ADSORPTION
AB A synergistic combination of nanostructure synthesis and plasma surface modification was used to enhance the photoelectrochemical activity of titania (TiO2) anodes. Titania nanotubular photoanodes were synthesized by electrochemical anodization of Ti thin foils. Nitrogen plasma was used to dope N at the surface of the photoanodes while removing chemisorbed species. X-ray photoelectron spectroscopy analysis showed an increase in the surface concentration of nitrogen. The photocurrent density of plasma treated samples was approximately 80% higher than that of the control. The open circuit potential of the plasma treated samples was more negative compared to that of the control, implying a favorable energetics for water splitting. This increase in photoactivity could be ascribed to: (1) increased absorption of visible light due to bandgap reduction, (2) minimization of charge carrier traps, (3) optimal oxygen vacancies, and (4) increased surface area for enhanced optical absorption and improved charge carrier generation.
C1 [Sharma, Rajesh; Bock, Jacob P.; Biris, Alexandru S.; Mazumder, Malay K.] Univ Arkansas, Dept Appl Sci, Little Rock, AR 72204 USA.
[Das, Prajna P.; Misra, Mano; Mahajan, Vishal] Univ Nevada, Dept Chem & Met Engn, Reno, NV 89557 USA.
[Trigwell, Steve] NASA, ASRC Aerosp, Kennedy Space Ctr, FL 32899 USA.
RP Sharma, R (reprint author), Univ Arkansas, Dept Appl Sci, Little Rock, AR 72204 USA.
EM rxsharma@ualr.edu
RI Biris, Alexandru/A-8507-2010
FU United States Department of Energy [GO86054]; Arkansas Science and
Technology Authority
FX The authors gratefully acknowledge financial support from the United
States Department of Energy Grant # GO86054 and Arkansas Science and
Technology Authority. The authors also acknowledge Hidetaka Ishihara and
Jeremy Stark for their assistance in preparation of this manuscript.
NR 34
TC 21
Z9 21
U1 1
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD FEB 18
PY 2009
VL 20
IS 7
AR 075704
DI 10.1088/0957-4484/20/7/075704
PG 7
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 399FP
UT WOS:000262786100028
PM 19417432
ER
PT J
AU Albert, S
Bauerecker, S
Boudon, V
Brown, LR
Champion, JP
Loete, M
Nikitin, A
Quack, M
AF Albert, S.
Bauerecker, S.
Boudon, V.
Brown, L. R.
Champion, J. -P.
Loete, M.
Nikitin, A.
Quack, M.
TI Global analysis of the high resolution infrared spectrum of methane
(CH4)-C-12 in the region from 0 to 4800 cm(-1)
SO CHEMICAL PHYSICS
LA English
DT Review
DE Methane; High resolution infrared spectra; Line intensities; Vibrational
states; Rovibrational analysis
ID MONTE-CARLO CALCULATIONS; ELECTRIC-DIPOLE MOMENT; 9-DIMENSIONAL
POTENTIAL SURFACE; ABSOLUTE FREQUENCY MEASUREMENTS; FOURIER-TRANSFORM
SPECTROSCOPY; AMPLITUDE NUCLEAR MOTION; MU-M; ENERGY-LEVELS; LINE
PARAMETERS; MOLECULAR-SPECTROSCOPY
AB We report the global analysis of methane ((CH4)-C-12) lines from high resolution rovibrational spectra including accurate line positions and intensities in the region 0-4800 cm(-1). This covers four polyads: The Ground State Monad (rotational levels), the Dyad (940-1850 cm(-1), 2 vibrational levels, 2 sublevels), the Pentad (2150-3350 cm(-1), 5 vibrational levels, 9 sublevels) and the Octad (3550-4800 cm(-1), 8 vibrational levels, 24 sublevels) and some of the associated hot bands (Pentad-Dyad and Octad-Dyad). New Fourier transform infrared (FTIR) spectra of the Pentad and Octad regions have been recorded with a very high resolution (better than 0.001 cm(-1) instrumental bandwidth, unapodized) at 78 K using the Bruker IFS 125 HR Zurich prototype (ZP2001) spectrometer in combination with a long optical path collisional cooling system [S. Albert, S. Bauerecker, M. Quack, A. Steinlin, Mol. Phys. 105 (2007) 541]. Existing spectra previously recorded with the FTIR spectrometer at the National Solar Observatory on Kitt Peak in Arizona were remeasured selectively to provide new intensities and positions of weaker lines above 4400 cm(-1). These were combined with previously reported absorption data from MR and laser absorption, as well as high-resolution stimulated Raman and microwave spectra. The effective hamiltonian was expanded up to order 6 for the Ground State, order 6 for the Dyad, order 5 for the Pentad and order 5 for the Octad. A total of 16,738 line positions were used in the least squares adjustment characterized by the following global root mean square deviations d(RMS) for line positions: 1.3 x 10(-4) cm(-1) for the Dyad, 6.0 x 10(-4) cm(-1) for the Pentad, and 3.5 x 10(-3) cm(-1) for the Octad. Absolute intensities were also analyzed for all the cold bands and some of the hot bands in the region under consideration and we obtained d(RMS) = 9.6% including 3262 experimental line intensities for the Octad. This analysis represents a large improvement over the previous one [J.-C. Hilico, O. Robert, M. Loete, S. Toumi, A.S. Pine. L.R. Brown, J. Mol. Spectrosc. 208 (2001) 1] with d(RMS) = 0.041 cm(-1) for positions and 15.6% for intensities in the Octad for a smaller data set. The new results are discussed as benchmarks in relation to accurate potential energy hypersurfaces and for atmospheric and planetary spectra. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Boudon, V.; Champion, J. -P.; Loete, M.] Univ Bourgogne, Inst Carnot Bourgogne, CNRS, UMR 5209, F-21078 Dijon, France.
[Albert, S.; Bauerecker, S.; Quack, M.] ETH, CH-8093 Zurich, Switzerland.
[Bauerecker, S.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Phys & Theoret Chem, D-38106 Braunschweig, Germany.
[Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nikitin, A.] Russian Acad Sci, Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634055, Russia.
RP Boudon, V (reprint author), Univ Bourgogne, Inst Carnot Bourgogne, CNRS, UMR 5209, 9 Av A Savory,BP 47870, F-21078 Dijon, France.
EM Vincent.Boudon@u-bourgogne.fr
RI BOUDON, Vincent/A-4504-2010; Champion, Jean-Paul/C-3963-2009; Nikitin,
Andrei/K-2624-2013; Quack, Martin/H-4457-2016
OI Nikitin, Andrei/0000-0002-4280-4096;
FU ETH Zurich, Schweizererischer Nationalfonds; Conseil Regional de
Bourgogne; LEFE-CHAT National Program of the CNRS; RFBR (Russia)
[06-05-650100]; SpecMo Research Group (CNRS) [GDR 3152]; Jet Propulsion
Laboratory (JPL), California Institute of Technology
FX This work was supported financially by ETH Zurich, Schweizererischer
Nationalfonds, the Conseil Regional de Bourgogne, the LEFE-CHAT National
Program of the CNRS and by RFBR (Russia) through Grant 06-05-650100. We
also wish to thank the SpecMo Research Group (CNRS GDR 3152). Part of
the research at the Jet Propulsion Laboratory (JPL), California
Institute of Technology was performed under contracts with the National
Aeronautics and Space Administration. We enjoyed discussions with Hans
Hollenstein and Hans-Martin Niederer, who also reproduced the entire fit
of data in the paper independently for a check.
NR 116
TC 113
Z9 113
U1 3
U2 32
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0301-0104
J9 CHEM PHYS
JI Chem. Phys.
PD FEB 17
PY 2009
VL 356
IS 1-3
SI SI
BP 131
EP 146
DI 10.1016/j.chemphys.2008.10.019
PG 16
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 416HX
UT WOS:000263997700017
ER
PT J
AU Herbin, H
Hurtmans, D
Clarisse, L
Turquety, S
Clerbaux, C
Rinsland, CP
Boone, C
Bernath, PF
Coheur, PF
AF Herbin, H.
Hurtmans, D.
Clarisse, L.
Turquety, S.
Clerbaux, C.
Rinsland, C. P.
Boone, C.
Bernath, P. F.
Coheur, P. -F.
TI Distributions and seasonal variations of tropospheric ethene (C2H4) from
Atmospheric Chemistry Experiment (ACE-FTS) solar occultation spectra
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; BIOMASS BURNING EMISSIONS; NONMETHANE
HYDROCARBONS; TRANSPORT; SPACE; EVOLUTION; METHANOL; IMPACT; GASES;
TRACE
AB This work reports the first measurements of ethene (C2H4)distributions in the upper troposphere. These are obtained by retrieving vertical profiles from 5 to 20 km from infrared solar occultation spectra recorded in 2005 and 2006 by the Atmospheric Chemistry Experiment-Fourier Transform Spectrometer (ACE-FTS). Background volume mixing ratios (vmrs) ranging from a few to about 50 pptv (10(-12)) are measured at the different altitudes, while for certain occultations, vmrs as high as 200 pptv are observed. Zonal distributions and vertically resolved latitudinal distributions are derived for the two year period analyzed, highlighting spatial -including a North-South gradient- as well as seasonal variations. We show the latter to be more pronounced at the highest latitudes, presumably as a result of less active photochemistry during winter. The observation of C2H4 enhancements in remote Arctic regions at high latitudes is consistent with the occurrence of fast transport processes of gaseous pollution from the continents leading to Arctic haze. Citation: Herbin, H., D. Hurtmans, L. Clarisse, S. Turquety, C. Clerbaux, C. P. Rinsland, C. Boone, P. F. Bernath, and P.-F. Coheur (2009), Distributions and seasonal variations of tropospheric ethene (C2H4) from Atmospheric Chemistry Experiment (ACE-FTS) solar occultation spectra, Geophys. Res. Lett., 36, L04801, doi:10.1029/2008GL036338.
C1 [Herbin, H.; Hurtmans, D.; Clarisse, L.; Clerbaux, C.; Coheur, P. -F.] Univ Libre Bruxelles, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium.
[Boone, C.; Bernath, P. F.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Turquety, S.; Clerbaux, C.] UPMC Paris 06, CNRS, IPSL, UMR 7620,Serv Aeron, Paris, France.
[Rinsland, C. P.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Herbin, H (reprint author), Univ Libre Bruxelles, Serv Chim Quant & Photophys, 50 Ave FD Roosevelt, B-1050 Brussels, Belgium.
EM pfcoheur@ulb.ac.be
RI Clarisse, Lieven/C-3933-2011; Bernath, Peter/B-6567-2012; clerbaux,
cathy/I-5478-2013
OI Clarisse, Lieven/0000-0002-8805-2141; Bernath,
Peter/0000-0002-1255-396X;
FU Fonds de la Recherche Scientifique; Belgian State Federal Office for
Scientific, Technical and Cultural Affairs; European Space Agency;
Actions de Recherche Concertees; Centre National d'Etudes Spatiales; UK
Natural Environment Research Council (NERC); NASA's Atmospheric
Chemistry and Modeling Program (ACMAP); F.N.R.S (Belgium)
FX The research in Belgium was funded by the Fonds de la Recherche
Scientifique (FRS-FNRS, M.I.S. n degrees F.4511.08), the Belgian State
Federal Office for Scientific, Technical and Cultural Affairs and the
European Space Agency (ESA-Prodex arrangement C90-327). Financial
support by the "Actions de Recherche Concertees" (Communaute Francaise
de Belgique) is also acknowledged. C. Clerbaux and S. Turquety are
grateful to CNES (Centre National d'Etudes Spatiales) for financial
support. The ACE mission is supported primarily by the Canadian Space
Agency (CSA) and some support was also provided by the UK Natural
Environment Research Council (NERC). NASA Langley Research Center was
supported by NASA's Atmospheric Chemistry and Modeling Program (ACMAP).
P.F. Coheur and L. Clarisse are Research Associate and Scientific
Collaborator with the F.N.R.S (Belgium).
NR 27
TC 8
Z9 8
U1 1
U2 3
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 2009
VL 36
AR L04801
DI 10.1029/2008GL036338
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 410XG
UT WOS:000263611000002
ER
PT J
AU Nelson, RM
Kamp, LW
Lopes, RMC
Matson, DL
Kirk, RL
Hapke, BW
Wall, SD
Boryta, MD
Leader, FE
Smythe, WD
Mitchell, KL
Baines, KH
Jaumann, R
Sotin, C
Clark, RN
Cruikshank, DP
Drossart, P
Lunine, JI
Combes, M
Bellucci, G
Bibring, JP
Capaccioni, F
Cerroni, P
Coradini, A
Formisano, V
Filacchione, G
Langevin, Y
McCord, TB
Mennella, V
Nicholson, PD
Sicardy, B
Irwin, PGJ
Pearl, JC
AF Nelson, Robert M.
Kamp, Lucas W.
Lopes, Rosaly M. C.
Matson, Dennis L.
Kirk, Randolph L.
Hapke, Bruce W.
Wall, Stephen D.
Boryta, Mark D.
Leader, Frank E.
Smythe, William D.
Mitchell, Karl L.
Baines, Kevin H.
Jaumann, Ralf
Sotin, Christophe
Clark, Roger N.
Cruikshank, Dale P.
Drossart, Pierre
Lunine, Jonathan I.
Combes, Michel
Bellucci, Giancarlo
Bibring, Jean-Pierre
Capaccioni, Fabrizio
Cerroni, Pricilla
Coradini, Angioletta
Formisano, Vittorio
Filacchione, Gianrico
Langevin, Yves
McCord, Thomas B.
Mennella, Vito
Nicholson, Phillip D.
Sicardy, Bruno
Irwin, Patrick G. J.
Pearl, John C.
TI Photometric changes on Saturn's Titan: Evidence for active cryovolcanism
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SURFACE
AB We report infrared spectrophotometric variability on the surface of Saturn's moon Titan detected in images returned by the Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini Saturn Orbiter. The changes were observed at 7 degrees S, 138 degrees W and occurred between October 27, 2005 and January 15, 2006. After that date the surface was unchanged until the most recent observation, March 18, 2006. We previously reported spectrophotometric variability at another location (26 degrees S, 78 degrees W). Cassini Synthetic Aperture RADAR (SAR) images find that the surface morphology at both locations is consistent with surface flows possibly resulting from cryovolcanic activity (Wall et al., companion paper, this issue). The VIMS-reported time variability and SAR morphology results suggest that Titan currently exhibits intermittent surface changes consistent with present ongoing surface processes. We suggest that these processes involve material from Titan's interior being extruded or effused and deposited on the surface, as might be expected from cryovolcanism. Citation: Nelson, R. M., et al. (2009), Photometric changes on Saturn's Titan: Evidence for active cryovolcanism, Geophys. Res. Lett., 36, L04202, doi:10.1029/2008GL036206.
C1 [Nelson, Robert M.; Kamp, Lucas W.; Lopes, Rosaly M. C.; Matson, Dennis L.; Wall, Stephen D.; Leader, Frank E.; Smythe, William D.; Mitchell, Karl L.; Baines, Kevin H.; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bibring, Jean-Pierre; Langevin, Yves] Univ Paris Sud Orsay, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA.
[Boryta, Mark D.] Mt San Antonio Coll, Dept Earth Sci & Astron, Walnut, CA 91789 USA.
[Combes, Michel] Observ Paris, Dept Rech Spatiale, F-92195 Meudon, France.
[Cruikshank, Dale P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Drossart, Pierre; Sicardy, Bruno] Observ Paris, LESIA, F-92195 Meudon, France.
[Hapke, Bruce W.] Univ Pittsburgh, Dept Geol & Planetary Sci, Pittsburgh, PA 15260 USA.
[Irwin, Patrick G. J.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England.
[Jaumann, Ralf] DLR, Inst Space Sensor Technol & Planetary Explorat, D-12489 Berlin, Germany.
[Kirk, Randolph L.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Lunine, Jonathan I.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[McCord, Thomas B.] Space Sci Inst, Bear Fight Ctr, Winthrop, WA 98862 USA.
[Mennella, Vito] Osserv Astron Capodimonte, Inst Nazl Astrofis, I-80131 Naples, Italy.
[Nicholson, Phillip D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Pearl, John C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Nelson, RM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.m.nelson@jpl.nasa.gov
RI Lopes, Rosaly/D-1608-2016;
OI Lopes, Rosaly/0000-0002-7928-3167; Bellucci,
Giancarlo/0000-0003-0867-8679; Cerroni, Priscilla/0000-0003-0239-2741;
Capaccioni, Fabrizio/0000-0003-1631-4314; Filacchione,
Gianrico/0000-0001-9567-0055; Irwin, Patrick/0000-0002-6772-384X
FU NASA
FX This work done at JPL, California Institute of Technology, under
contract with NASA.
NR 14
TC 25
Z9 25
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 17
PY 2009
VL 36
AR L04202
DI 10.1029/2008GL036206
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 410XG
UT WOS:000263611000001
ER
PT J
AU Fiore, AM
Dentener, FJ
Wild, O
Cuvelier, C
Schultz, MG
Hess, P
Textor, C
Schulz, M
Doherty, RM
Horowitz, LW
MacKenzie, IA
Sanderson, MG
Shindell, DT
Stevenson, DS
Szopa, S
Van Dingenen, R
Zeng, G
Atherton, C
Bergmann, D
Bey, I
Carmichael, G
Collins, WJ
Duncan, BN
Faluvegi, G
Folberth, G
Gauss, M
Gong, S
Hauglustaine, D
Holloway, T
Isaksen, ISA
Jacob, DJ
Jonson, JE
Kaminski, JW
Keating, TJ
Lupu, A
Marmer, E
Montanaro, V
Park, RJ
Pitari, G
Pringle, KJ
Pyle, JA
Schroeder, S
Vivanco, MG
Wind, P
Wojcik, G
Wu, S
Zuber, A
AF Fiore, A. M.
Dentener, F. J.
Wild, O.
Cuvelier, C.
Schultz, M. G.
Hess, P.
Textor, C.
Schulz, M.
Doherty, R. M.
Horowitz, L. W.
MacKenzie, I. A.
Sanderson, M. G.
Shindell, D. T.
Stevenson, D. S.
Szopa, S.
Van Dingenen, R.
Zeng, G.
Atherton, C.
Bergmann, D.
Bey, I.
Carmichael, G.
Collins, W. J.
Duncan, B. N.
Faluvegi, G.
Folberth, G.
Gauss, M.
Gong, S.
Hauglustaine, D.
Holloway, T.
Isaksen, I. S. A.
Jacob, D. J.
Jonson, J. E.
Kaminski, J. W.
Keating, T. J.
Lupu, A.
Marmer, E.
Montanaro, V.
Park, R. J.
Pitari, G.
Pringle, K. J.
Pyle, J. A.
Schroeder, S.
Vivanco, M. G.
Wind, P.
Wojcik, G.
Wu, S.
Zuber, A.
TI Multimodel estimates of intercontinental source-receptor relationships
for ozone pollution
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Review
ID EASTERN UNITED-STATES; REGIONAL AIR-QUALITY; MICS-ASIA-II; TROPOSPHERIC
OZONE; SURFACE OZONE; CARBON-MONOXIDE; NORTH-AMERICA; MACE-HEAD;
BACKGROUND OZONE; TRANSATLANTIC TRANSPORT
AB Understanding the surface O-3 response over a "receptor" region to emission changes over a foreign "source" region is key to evaluating the potential gains from an international approach to abate ozone (O-3) pollution. We apply an ensemble of 21 global and hemispheric chemical transport models to estimate the spatial average surface O-3 response over east Asia (EA), Europe (EU), North America (NA), and south Asia (SA) to 20% decreases in anthropogenic emissions of the O-3 precursors, NOx, NMVOC, and CO (individually and combined), from each of these regions. We find that the ensemble mean surface O-3 concentrations in the base case (year 2001) simulation matches available observations throughout the year over EU but overestimates them by > 10 ppb during summer and early fall over the eastern United States and Japan. The sum of the O-3 responses to NOx, CO, and NMVOC decreases separately is approximately equal to that from a simultaneous reduction of all precursors. We define a continental-scale "import sensitivity" as the ratio of the O-3 response to the 20% reductions in foreign versus "domestic" (i.e., over the source region itself) emissions. For example, the combined reduction of emissions from the three foreign regions produces an ensemble spatial mean decrease of 0.6 ppb over EU (0.4 ppb from NA), less than the 0.8 ppb from the reduction of EU emissions, leading to an import sensitivity ratio of 0.7. The ensemble mean surface O-3 response to foreign emissions is largest in spring and late fall (0.7-0.9 ppb decrease in all regions from the combined precursor reductions in the three foreign regions), with import sensitivities ranging from 0.5 to 1.1 (responses to domestic emission reductions are 0.8-1.6 ppb). High O-3 values are much more sensitive to domestic emissions than to foreign emissions, as indicated by lower import sensitivities of 0.2 to 0.3 during July in EA, EU, and NA when O-3 levels are typically highest and by the weaker relative response of annual incidences of daily maximum 8-h average O-3 above 60 ppb to emission reductions in a foreign region(< 10-20% of that to domestic) as compared to the annual mean response (up to 50% of that to domestic). Applying the ensemble annual mean results to changes in anthropogenic emissions from 1996 to 2002, we estimate a Northern Hemispheric increase in background surface O-3 of about 0.1 ppb a(-1), at the low end of the 0.1-0.5 ppb a(-1) derived from observations. From an additional simulation in which global atmospheric methane was reduced, we infer that 20% reductions in anthropogenic methane emissions from a foreign source region would yield an O-3 response in a receptor region that roughly equals that produced by combined 20% reductions of anthropogenic NOx, NMVOC, and CO emissions from the foreign source
C1 [Fiore, A. M.; Horowitz, L. W.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA.
[Dentener, F. J.; Cuvelier, C.; Van Dingenen, R.; Marmer, E.] Commiss European Communities, Inst Environm & Sustainabil, DG Joint Res Ctr, I-21020 Ispra, Italy.
[Wild, O.] Univ Lancaster, Dept Environm Sci, Lancester Environm Ctr, Lancaster LA1 4YQ, England.
[Schultz, M. G.; Schroeder, S.] Forschungszentrum Julich, ICG 2, D-52425 Julich, Germany.
[Hess, P.] Cornell Univ, Ithaca, NY 14853 USA.
[Textor, C.] Univ Paris 06, GMES France Atmosphere, Serv Aeron, INSU,CNRS, F-75252 Paris, France.
[Textor, C.; Schulz, M.; Szopa, S.; Hauglustaine, D.] CNRS, UVSQ, IPSL, CEA,Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France.
[Doherty, R. M.; MacKenzie, I. A.; Stevenson, D. S.] Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3JN, Midlothian, Scotland.
[Sanderson, M. G.; Collins, W. J.; Pringle, K. J.] Hadley Ctr, Met Off, Exeter EX1 3PB, Devon, England.
[Shindell, D. T.; Faluvegi, G.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Zeng, G.; Pyle, J. A.] Univ Cambridge, Dept Chem, Natl Ctr Atmospher Sci, Cambridge CB2 1EW, England.
[Atherton, C.; Bergmann, D.] Lawrence Livermore Natl Lab, Atmospher Earth & Energy Div, Livermore, CA 94551 USA.
[Bey, I.; Folberth, G.] Ecole Polytech Fed Lausanne, Lab Modelisat Chim Atmospher, CH-1015 Lausanne, Switzerland.
[Carmichael, G.] Univ Iowa, Coll Engn, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA.
[Duncan, B. N.] NASA, Goddard Space Flight Ctr, UMBC Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA.
[Gauss, M.; Isaksen, I. S. A.] Univ Oslo, Dept Geosci, N-0315 Oslo, Norway.
[Gong, S.] Environm Canada, Air Qual Res Div, Sci & Technol Branch, Toronto, ON, Canada.
[Hauglustaine, D.] European Sci Fdn, Life Earth & Environm Sci, F-67080 Strasbourg, France.
[Holloway, T.] Univ Wisconsin, Ctr Sustainabil & Global Environm, Nelson Inst Environm Studies, Madison, WI 53726 USA.
[Park, R. J.] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151742, South Korea.
[Jonson, J. E.; Wind, P.] Norwegian Meteorol Inst, Oslo, Norway.
[Kaminski, J. W.; Lupu, A.] York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 1P3, Canada.
[Keating, T. J.] US EPA, Off Air & Radiat, Washington, DC 20460 USA.
[Montanaro, V.; Pitari, G.] Univ Aquila, Dept Phys, I-67100 Laquila, Italy.
[Vivanco, M. G.] CIEMAT, Atmospher Pollut Unit, E-28040 Madrid, Spain.
[Wojcik, G.] Northrop Grumman Corp, Atmospher Effects Grp, Chantilly, VA 20151 USA.
[Zuber, A.] Commiss European Communities, Environm Directorate Gen, B-1049 Brussels, Belgium.
[Jacob, D. J.; Park, R. J.; Wu, S.] Harvard Univ, Atmospher Chem Modeling Grp, Cambridge, MA 02138 USA.
RP Fiore, AM (reprint author), NOAA, Geophys Fluid Dynam Lab, 201 Forrestal Rd, Princeton, NJ 08542 USA.
EM Arlene.Fiore@noaa.gov; frank.dentener@jrc.it; O.Wild@lancaster.ac.uk;
kees.cuvelier@jrc.it; m.schultz@fz-juelich.de; hess@ucar.edu;
christiane.textor@aero.jussieu.fr; michael.schulz@isce.ipsl.fr;
ruth.doherty@ed.ac.uk; Larry.Horowitz@noaa.gov;
iamack@staffmail.ed.ac.uk; Michael.sanderson@metoffice.gov.uk;
dshindell@giss.nasa.gov; dstevens@staffmail.ed.ac.uk;
sophie.szopa@Isce.ipsl.fr; rita.van-dingenen@jrc.it;
Cynthia.Atherton@moore.org; dbergmann@llnl.gov; isabelle.bey@epfl.ch;
gcarmich@engineering.uiowa.edu; bill.collins@metoffice.gov.uk;
Bryan.N.Duncan@nasa.gov; greg.faluvegi@gmail.com;
gerd.folberth@metoffice.gov.uk; Michael.gauss@geo.uio.no;
Sunling.Gong@ec.gc.ca; dhauglustaine@esf.org; taholloway@wisc.edu;
ivar.isaksen@geofysikk.uio.no; djacob@fas.harvard.edu;
jan.eiof.jonson@met.no; jacek@yorku.ca; Keating.Terry@epamail.epa.gov;
alexlupu@yorku.ca; elina.marmer@jrc.it;
veronica.montanaro@aquila.infn.it; rjpark@snu.ac.kr;
gianni.pitari@aquila.infn.it; pringle@mpch-mainz.mpg.de;
John.Pyle@atm.ch.cam.ac.uk; s.schroeder@fz-juelich.de;
m.garcia@ciemat.es; peter.wind@met.no; gary.wojcik@ngc.com;
slwu@mtu.edu; Andre.ZUBER@ec.europa.eu
RI Horowitz, Larry/D-8048-2014; Vivanco, Marta/L-9816-2014; Park,
Rokjin/I-5055-2012; Hess, Peter/M-3145-2015; Schulz,
Michael/A-6930-2011; Pitari, Giovanni/O-7458-2016; Pringle, Kirsty
/A-4697-2013; Pfister, Gabriele/A-9349-2008; Wild, Oliver/A-4909-2009;
Collins, William/A-5895-2010; Folberth, Gerd/F-7376-2010; Szopa,
Sophie/F-8984-2010; mackenzie, ian/E-9320-2013; Lupu,
Alexandru/D-3689-2009; Bergmann, Daniel/F-9801-2011; Stevenson,
David/C-8089-2012; Shindell, Drew/D-4636-2012; Duncan,
Bryan/A-5962-2011; Schultz, Martin/I-9512-2012
OI Horowitz, Larry/0000-0002-5886-3314; Vivanco, Marta/0000-0002-5828-1859;
Park, Rokjin/0000-0001-8922-0234; Hess, Peter/0000-0003-2439-3796;
Schulz, Michael/0000-0003-4493-4158; Pitari,
Giovanni/0000-0001-7051-9578; Folberth, Gerd/0000-0002-1075-440X; Wild,
Oliver/0000-0002-6227-7035; Collins, William/0000-0002-7419-0850; Szopa,
Sophie/0000-0002-8641-1737; Lupu, Alexandru/0000-0002-4520-5523;
Bergmann, Daniel/0000-0003-4357-6301; Stevenson,
David/0000-0002-4745-5673; Schultz, Martin/0000-0003-3455-774X
FU U.S. DOE Atmospheric Science Program (Office of Science, BER) at LLNL
[DE-AC52-07NA27344]; NERC [NE/D012538/1]; NASA; UK Defra [AQ902]; DECC
[GA01101]; MoD [CBC/2B/0417_Annex C5]; Canadian Foundation for Climate
and Atmospheric Sciences; Ontario Ministry of the Environment; Canadian
Foundation for Innovation; Ontario Innovation Trust; Spanish Ministry of
the Environment; Korea Meteorological Administration Research and
Development Program [CATER 2007-3205]
FX We are grateful to D. Jaffe and D. Reidmiller (University of
Washington), and to A. Gnanadesikan and R. Stouffer (GFDL) and three
anonymous reviewers for insightful comments on previous versions of the
manuscript. C. A. and D. B. were supported primarily by the U.S. DOE
Atmospheric Science Program (Office of Science, BER) at LLNL under
contract DE-AC52-07NA27344. R. M. D., I. A. M., and D. S. S. acknowledge
funding from NERC (NE/D012538/1); B.N.D. from NASA MAP; M. G. S.,
K.J.P., and W.J.C. from the UK Defra under contract AQ902 and the Joint
DECC and MoD Programme, (DECC) GA01101 (MoD) CBC/2B/0417_Annex C5; A. L.
and J. W. K. from the Canadian Foundation for Climate and Atmospheric
Sciences, the Ontario Ministry of the Environment, the Canadian
Foundation for Innovation and the Ontario Innovation Trust; and M. G. V.
from the Spanish Ministry of the Environment. R. J. P. was partly
supported by the Korea Meteorological Administration Research and
Development Program under grant CATER 2007-3205.
NR 103
TC 183
Z9 187
U1 50
U2 173
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 2009
VL 114
AR D04301
DI 10.1029/2008JD010816
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 410XQ
UT WOS:000263612000001
ER
PT J
AU Halkides, DJ
Lee, T
AF Halkides, D. J.
Lee, Tong
TI Mechanisms controlling seasonal-to-interannual mixed layer temperature
variability in the southeastern tropical Indian Ocean
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; SEA-SURFACE TEMPERATURE; DIPOLE MODE; ZONAL
MODE; INDONESIAN THROUGHFLOW; COUPLED GCM; DYNAMICS; ENSO; MONSOON;
EVENTS
AB We use an Estimating the Circulation and Climate of the Ocean assimilation product to investigate seasonal-interannual mixed layer temperature (MLT) budgets in the southeastern tropical Indian Ocean (SETIO) during 1993-2006. We examine spatial inhomogeneity of the SETIO MLT budget, contrasting three subregions with different forcing/circulation characteristics to better understand the area mean budget over the full SETIO. The subregions are the equatorial zone (box 1), the Sumatra-Java upwelling zone (box 2), and east of the thermocline ridge (box 3). Seasonally, surface heat flux dominates MLT in all regions; advection and subsurface processes generally play secondary roles. On interannual scales, surface heat flux makes major contributions in all three boxes to termination of SETIO cooling associated with the Indian Ocean Zonal/Dipole Mode. Ocean dynamics show vital differences between regions: Subsurface processes cool box 1 and 2 but warm box 3. Horizontal advection warms box 1 but cools box 2 and 3. Averaging the MLT budget over the SETIO obscures regional physics. We explain spatial variations of the SETIO MLT budget in terms of differences in forcing, circulation, MLT distribution, and mixed layer and barrier layer thicknesses. We also examine SETIO MLT budget differences during 1994, 1997, and 2006, years exhibiting notable SETIO cooling events. In box 1, horizontal advection dominates warming after the 1994 and 2006 coolings, while in 1997, surface heat flux dominates warming. In box 2, cooling peaks earlier in 1994 than in 1997 and 2006 because of subsurface processes. Last, we show that the MLT budget is very different from heat budgets for fixed depth layers (e. g., the top 50-60 m).
C1 [Halkides, D. J.; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Halkides, DJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM halkides@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology; NASA
FX We thank the JPL ECCO team for their Kalman filter assimilation product,
Josh Willis for providing XBT data, and Akiko Hayashi for producing
gridded SSH maps from the level 2 TOPEX/Poseidon and JASON-1 data. The
latter data are distributed by the Physical Oceanography Distributed
Active Archive Center (PO.DAAC) at the NASA Jet Propulsion Laboratory,
Pasadena, California (http://podaac.jpl.nasa.gov). This research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA.
NR 72
TC 24
Z9 24
U1 0
U2 11
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 17
PY 2009
VL 114
AR C02012
DI 10.1029/2008JC004949
PG 23
WC Oceanography
SC Oceanography
GA 410YD
UT WOS:000263613300002
ER
PT J
AU Zhai, PW
Hu, YX
Trepte, CR
Lucker, PL
AF Zhai, Peng-Wang
Hu, Yongxiang
Trepte, Charles R.
Lucker, Patricia L.
TI A vector radiative transfer model for coupled atmosphere and ocean
systems based on successive order of scattering method
SO OPTICS EXPRESS
LA English
DT Article
ID DISCRETE-ORDINATE-METHOD; IMPULSE-RESPONSE SOLUTION; MONTE-CARLO
CALCULATIONS; MATRIX OPERATOR THEORY; POLARIZED-LIGHT; TRANSFER
EQUATION; MULTIPLE-SCATTERING; PHASE FUNCTIONS; MUELLER MATRIX;
SATELLITE DATA
AB A vector radiative transfer model has been developed for coupled atmosphere and ocean systems based on the Successive Order of Scattering ( SOS) Method. The emphasis of this study is to make the model easy-to-use and computationally efficient. This model provides the full Stokes vector at arbitrary locations which can be conveniently specified by users. The model is capable of tracking and labeling different sources of the photons that are measured, e. g. water leaving radiances and reflected sky lights. This model also has the capability to separate florescence from multi-scattered sunlight. The delta - fit technique has been adopted to reduce computational time associated with the strongly forward-peaked scattering phase matrices. The exponential - linear approximation has been used to reduce the number of discretized vertical layers while maintaining the accuracy. This model is developed to serve the remote sensing community in harvesting physical parameters from multi-platform, multi-sensor measurements that target different components of the atmosphere-oceanic system. (C) 2009 Optical Society of America
C1 [Lucker, Patricia L.] NASA, Langley Res Ctr, MS 475, SSAI, Hampton, VA 23681 USA.
RP Zhai, PW (reprint author), SSAI 1 Enterprise Pkwy Suite 200, Hampton, VA 23666 USA.
EM Pengwang.zhai-1@nasa.gov
RI Hu, Yongxiang/K-4426-2012
FU NASA Postdoctoral Program; NASA Langley Research Center; NASA Radiation
Science program; NASA Biogeochemistry program
FX This research was supported by Peng-Wang Zhai's appointment to the NASA
Postdoctoral Program at the NASA Langley Research Center administered by
Oak Ridge Associated Universities through a contract with NASA. He also
thanks the Science Systems & Applications, Inc. (SSAI) in Hampton, VA
for providing the office space and computer support. This study is also
supported by Dr. Hal Maring of NASA Radiation Science program and Dr.
Paula Bontempi of NASA Biogeochemistry program.
NR 90
TC 46
Z9 48
U1 0
U2 8
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 FEB 16
PY 2009
VL 17
IS 4
BP 2057
EP 2079
DI 10.1364/OE.17.002057
PG 23
WC Optics
SC Optics
GA 408JY
UT WOS:000263432500002
PM 19219111
ER
PT J
AU Foster, JL
Hall, DK
Kelly, REJ
Chiu, L
AF Foster, J. L.
Hall, D. K.
Kelly, R. E. J.
Chiu, L.
TI Seasonal snow extent and snow mass in South America using SMMR and SSM/I
passive microwave data (1979-2006)
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE South America; Snow cover; Snow mass; Passive microwave; Satellite
ID ALGORITHM; COVER
AB Seasonal snow cover in South America was examined in this study using passive microwave satellite data from the Scanning Multichannel Microwave Radiometer (SMMR) on board the Nimbus-7 satellite and the Special Sensor Microwave Imagers (SSM/I) on board Defense Meteorological Satellite Program (DMSP) satellites. For the period from 1979-2006, both snow cover extent and snow water equivalent (snow mass) were investigated during the coldest months (May-September), primarily in the Patagonia area of Argentina and in the Andes of Chile, Argentina and Bolivia, where most of the seasonal snow is found. Since winter temperatures in this region are often above freezing, the coldest winter month was found to be the month having the most extensive snow cover and usually the month having the deepest snow cover as well. Sharp year-to-year differences were recorded using the passive microwave observations. The average snow cover extent for July, the month with the greatest average extent during the 28-year period of record, is 321,674 km(2). In July of 1984, the average monthly snow cover extent was 701,250 km(2) - the most extensive coverage observed between 1979 and 2006. However, in July of 1989, snow cover extent was only 120,000 km2. The 28-year period of record shows a sinusoidal like pattern for both snow cover and snow mass, though neither trend is significant at the 95% level. Published by Elsevier Inc.
C1 [Foster, J. L.; Hall, D. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kelly, R. E. J.] Univ Waterloo, Dept Geog, Waterloo, ON N2L 3G1, Canada.
[Chiu, L.] George Mason Univ, Geoinformat Dept, Fairfax, VA 22030 USA.
RP Foster, JL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM james.l.foster@nasa.gov
RI Hall, Dorothy/D-5562-2012
NR 27
TC 22
Z9 28
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 16
PY 2009
VL 113
IS 2
BP 291
EP 305
DI 10.1016/j.rse.2008.09.010
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 400VH
UT WOS:000262897000001
ER
PT J
AU Nagol, JR
Vermote, EF
Prince, SD
AF Nagol, Jyoteshwar R.
Vermote, Eric F.
Prince, Stephen D.
TI Effects of atmospheric variation on AVHRR NDVI data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE AVHRR; NDVI; Global change; Error; Uncertainty; PAL; GIMMS; GVI; LTDR;
AERONET; Accuracy; Precision
ID HIGH-RESOLUTION RADIOMETER; VEGETATION INDEX DATA; GLOBAL-SCALE;
TIME-SERIES; LAND; MODIS; TEMPERATURE; PRODUCTS; NETWORK; IMAGES
AB The AVHRR (Advanced Very High Resolution Radiometer) series of instruments has frequently been used for vegetation studies. The 25+ year record has enabled important time-series studies. Many applications use NDVI (Normalized Difference Vegetation Index), or derivatives of it, as their operational variable. However, most AVHRR datasets have incomplete atmospheric correction, because of which there is considerable, but largely unknown, uncertainty in the significance of differences in NDVI and other short wave observations from AVHRR instruments.
The purpose of this study was to gain better understanding of the impact of incomplete or lack of atmospheric correction in widely-used, publicly available processed AVHRR-NDVI long-term datasets. This was accomplished by comparison with atmospherically corrected AVHRR data at AERONET (AErosol RObotic NETwork) sunphotometer sites in 1999. The datasets included in this study are: TOA (Top Of Atmosphere) that is with no atmospheric correction; PAL (Pathfinder AVHRR Land); and an early version of the new LTDR (Long Term Data Record) NOW The other publicly available clatasets like GIMMS (Global Inventory Modeling and Mapping studies) and GVI (Global Vegetation Index) have atmospheric error budget similar to that of TOA, because no atmospheric correction is used in either processing stream. Of the three clatasets, LTDR was found to have least errors (accuracy = 0.0064 to -0.024, precision = 0.02 to 0.037 for clear and average atmospheric conditions) followed by PAL (accuracy = -0.145 to -0.035, precision = 0.0606 to 0.0418), and TOA (accuracy = -0.0791 to -0.112, precision = 0.0613 to 0.0684). It was also observed that temporal maximum value compositing technique does not cause significant improvement of precision in regions experiencing persistently high AOT (Aerosol Optical Thickness). (C) 2008 Elsevier Inc. All rights reserved.
C1 [Nagol, Jyoteshwar R.; Prince, Stephen D.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Vermote, Eric F.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Vermote, Eric F.] NASA, GSFC Code 614 5, Washington, DC USA.
RP Nagol, JR (reprint author), Univ Maryland, Dept Geog, 2181 LeFrak Hall, College Pk, MD 20742 USA.
EM jnagol@umd.edu
RI Vermote, Eric/K-3733-2012; Nagol, Jyoteshwar/P-2026-2015
OI Nagol, Jyoteshwar/0000-0003-0497-7874
NR 42
TC 51
Z9 52
U1 2
U2 15
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 16
PY 2009
VL 113
IS 2
BP 392
EP 397
DI 10.1016/j.rse.2008.10.007
PG 6
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 400VH
UT WOS:000262897000010
ER
PT J
AU Panciera, R
Walker, JP
Kalma, JD
Kim, EJ
Saleh, K
Wigneron, JP
AF Panciera, Rocco
Walker, Jeffrey P.
Kalma, Jetse D.
Kim, Edward J.
Saleh, Kauzar
Wigneron, Jean-Pierre
TI Evaluation of the SMOS L-MEB passive microwave soil moisture retrieval
algorithm
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Soil moisture; Microwave radiometry; SMOS; NAFE
ID L-BAND; CROP FIELDS; VEGETATION; EMISSION; RADIOMETRY; FREQUENCY; MODEL;
GRASS; POLARIZATION; BEHAVIOR
AB Soil moisture will be mapped globally by the European Soil Moisture and Ocean Salinity (SMOS) mission to be launched in 2009. The expected soil moisture accuracy will be 4.0 %v/v. The core component of the SMOS soil moisture retrieval algorithm is the L-band Microwave Emission of the Biosphere (L-MEB) model which simulates the microwave emission at L-band from the soil-vegetation layer. The model parameters have been calibrated with data acquired by tower mounted radiometer studies in Europe and the United States, with a typical footprint size of approximately 10 m. In this study. aircraft L-band data acquired during the National Airborne Field Experiment (NAFE) intensive campaign held in South-eastern Australia in 2005 are used to perform the first evaluation of the L-MEB model and its proposed parameterization when applied to coarser footprints (62.5 m), The model could be evaluated across large areas including a wide range of land surface conditions, typical of the Australian environment. Soil moisture was retrieved from the aircraft brightness temperatures using L-MEB and ground measured ancillary data (soil temperature, soil texture, vegetation water content and surface roughness) and subsequently evaluated against ground measurements of soil moisture. The retrieval accuracy when using the L-MEB 'default' set of model parameters was found to be better than 4.0 %v/v only over grassland covered sites. Over crops the model was found to underestimate soil moisture by up to 32 %v/v. After site specific calibration of the vegetation and roughness parameters, the retrieval accuracy was found to be equal or better than 4.8 %v/v for crops and grasslands at 62.5-m resolution. it is suggested that the proposed value of roughness parameter H(R) for crops is too low, and that variability of HR With Soil moisture must be taken into consideration to obtain accurate retrievals at these scales. The analysis presented here is a crucial step towards validating the application of L-MEB for soil moisture retrieval from satellite observations in an operational context. (C) 2008 Elsevier Inc. All rights reserved.
C1 [Panciera, Rocco; Walker, Jeffrey P.] Univ Melbourne, Dept Civil & Environm Engn, Parkville, Vic 3010, Australia.
[Kalma, Jetse D.] Univ Newcastle, Sch Engn, Callaghan, NSW 2308, Australia.
[Kim, Edward J.] NASA, Goddard Space Flight Ctr, Washington, DC USA.
[Saleh, Kauzar] Univ Cambridge, Dept Geog, Cambridge CB2 1TN, England.
[Wigneron, Jean-Pierre] EPHYSE, INRA, Bordeaux, France.
RP Panciera, R (reprint author), Univ Melbourne, Dept Civil & Environm Engn, Parkville, Vic 3010, Australia.
EM rocco@civenv.unimelb.edu.au
RI Walker, Jeffrey/D-2624-2009;
OI wigneron, jean-pierre/0000-0001-5345-3618
FU Australian Research Council [LE0453434, DP0557543]
FX The authors would like to thank the NAFE'05 participants. The National
Airborne Field Experiment 2005 has been made possible through recent
infrastructure (LE0453434) and research (DP0557543) funding from the
Australian Research Council, and the collaboration of a large number of
scientists from throughout Australia, United States and Europe. The
authors also wish to thank Cristina Martinez for providing the laser
mastersizer soil particle analysis data.
NR 34
TC 65
Z9 68
U1 0
U2 26
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD FEB 16
PY 2009
VL 113
IS 2
BP 435
EP 444
DI 10.1016/j.rse.2008.10.010
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 400VH
UT WOS:000262897000014
ER
PT J
AU Vertrees, RA
McCarthy, M
Solley, T
Popov, VL
Roaten, J
Pauley, M
Wen, XD
Goodwin, TJ
AF Vertrees, Roger A.
McCarthy, Maureen
Solley, Travis
Popov, Vselovod L.
Roaten, John
Pauley, Matthew
Wen, Xiaodong
Goodwin, Thomas J.
TI Development of a three-dimensional model of lung cancer using cultured
transformed lung cells
SO CANCER BIOLOGY & THERAPY
LA English
DT Article
DE tissue engineering; lung cells; three-dimensional culture
ID EPITHELIAL MEMBRANE ANTIGEN; MUCIN GENE-EXPRESSION; III BETA-TUBULIN;
IN-VITRO; MONOCLONAL-ANTIBODIES; CARCINOMA CELLS; SQUAMOUS
DIFFERENTIATION; VONWILLEBRAND-FACTOR; MESENCHYMAL CELLS;
BASEMENT-MEMBRANE
AB Despite great strides in understanding cancer biology, the role cellular differentiation and three-dimensional (3-D) structural organization play in metastasis and malignancy remains unclear. Development of 3-D cultures may ultimately provide a model facilitating discovery and interpretation of more relevant information for the expression and role of antibodies in lung cellular pathobiology. The purpose was to develop traditional monolayer (ML) and 3-D cultures of a known transformed metastatic lung cell line and then determine similarities and differences between cultures in terms of differentiation, molecular marker expression and metastasis. A transformed lung cell line (BZR-T33) was initially transfected with green fluorescent protein (GFP) in ML culture. Nude mice were inoculated with BZR-T33 and observed for metastasis. BZR-T33 was grown as ML and 3-D cultures under identical conditions. Immunohistochemical comparison for degree of antibody expression between cultures and control tissue were studied. Electron microscopy (EM) for identification of ultra structures was done and compared between cultures. A 3-D co-culture containing GFP-transformed cells over an immortalized lung-cell line was developed. The GFP-transfected cell line formed tumors and metastasized in mice. EM identified significant mitochondrial and granular endoplasmic reticular pathology in ML not seen in 3-D. Degree of differentiation shows ultra structures and antibody expressions were more representative of control tissue in 3-D than ML. The co-culture experiment in 3-D demonstrates the ability of transformed cells to penetrate the sub-layer of immortalized cells. Development of 3-D cultures will provide a new and powerful tool to study lung biology and pathobiology.
C1 [Vertrees, Roger A.; Solley, Travis; Wen, Xiaodong] Univ Texas Med Branch, Dept Surg, Galveston, TX 77555 USA.
[Popov, Vselovod L.] Univ Texas Med Branch, Dept Pathol, Galveston, TX 77555 USA.
[Roaten, John; Pauley, Matthew] Univ Texas Med Branch, Sch Med, Galveston, TX 77555 USA.
[Goodwin, Thomas J.] NASA, Lyndon B Johnson Space Ctr, Dis Modeling Tissue Analogues Lab, Houston, TX 77058 USA.
RP Vertrees, RA (reprint author), Univ Texas Med Branch, Dept Surg, 301 Univ Blvd, Galveston, TX 77555 USA.
EM rvertree@utmb.edu
FU NASA's Biological Sciences and Applications Division [NAS9-17720];
Thermasoltions Inc., of Melbourne, FL UTMB [58699]
FX The authors would like to acknowledge the efforts of Eileen Figueroa and
Steve Schuenke for their assistance in preparing this manuscript.
NR 67
TC 5
Z9 5
U1 2
U2 2
PU LANDES BIOSCIENCE
PI AUSTIN
PA 1002 WEST AVENUE, 2ND FLOOR, AUSTIN, TX 78701 USA
SN 1538-4047
J9 CANCER BIOL THER
JI Cancer Biol. Ther.
PD FEB 15
PY 2009
VL 8
IS 4
BP 356
EP 365
DI 10.4161/cbt.8.4.7432
PG 10
WC Oncology
SC Oncology
GA 426KH
UT WOS:000264706700010
PM 19305159
ER
PT J
AU Kato, Y
Suzuki, K
Nakamura, K
Hickman, AH
Nedachi, M
Kusakabe, M
Bevacqua, DC
Ohmoto, H
AF Kato, Yasuhiro
Suzuki, Katsuhiko
Nakamura, Kentaro
Hickman, Arthur H.
Nedachi, Munetomo
Kusakabe, Minoru
Bevacqua, David C.
Ohmoto, Hiroshi
TI Hematite formation by oxygenated groundwater more than 2.76 billion
years ago
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE hematite; pyrite; Re-Os age; oxygenated groundwater; Archean; Archean
Biosphere Drilling Project
ID NORTH PILBARA TERRAIN; WESTERN-AUSTRALIA; RE-OS; ATMOSPHERIC OXYGEN;
ARCHEAN ATMOSPHERE; ISOTOPIC EVIDENCE; SULFUR ISOTOPES; EVOLUTION;
CRATON; FRACTIONATION
AB Geoscientific drilling in the Marble Bar area of the Pilbara Craton, Western Australia, resulted in the discovery of locally abundant hematite in Archean basalts similar to 200 m below the present land surface. The hematized basalts occurring along a bedding-parallel shear zone are cross-cut by pyrite veinlets (<3 mm in width) and contain euhedral pyrite grains (10-500 mu m in diameter) with sharp crystal edges, indicating that the hematite formed before the pyrite. We have dated the pyrite in the veinlets at 2.763 +/- 0.016 Ga using the Re-Os method. Therefore, the hematite formed prior to 2.763 Ga.
The basalts containing the hematite belong to the Apex Basalt of the Warrawoona Group, and were erupted onto the Archean seafloor at 3.46 Ga. Due to 2.9 Ga orogenic deformation and subsequent deep erosion, the Apex Basalt was exposed at the surface of a continental landmass prior to 2.77 Ga. Sometime in the period between similar to 2.9 Ga and 2.77 Ga, the basalt section we describe was less than 200 m below the Late Archean land surface, and within range of groundwater percolation through the shear zone in the basalts. Geological, mineralogical and geochemical lines of evidence strongly suggest that the infiltration of O-2-rich groundwater through the bedding-parallel shear in the basalts formed hematite prior to 2.76 Ga, and hence oxygenated surface environments, at least localized and/or short-lived, emerged more than 300 million years before the widely accepted Great Oxidation Event during 2.45 and 2.32 Ga. (c) 2008 Elsevier B.V. All rights reserved.
C1 [Kato, Yasuhiro] Univ Tokyo, Dept Syst Innovat, Bunkyo Ku, Tokyo 1138656, Japan.
[Suzuki, Katsuhiko] Japan Agcy Marine Earth Sci & Technol, Inst Res Earth Evolut IFREE, Yokosuka, Kanagawa 2370061, Japan.
[Nakamura, Kentaro] Univ Tokyo, FRCER, Tokyo 1138656, Japan.
[Hickman, Arthur H.] Geol Survey Western Australia, Perth, WA 6004, Australia.
[Nedachi, Munetomo] Kagoshima Univ, Dept Phys, Kagoshima 8900065, Japan.
[Kusakabe, Minoru] Okayama Univ, Inst Study Earths Interior, Tottori 6820193, Japan.
[Bevacqua, David C.; Ohmoto, Hiroshi] Penn State Univ, NASA, Astrobiol Inst, University Pk, PA 16802 USA.
[Bevacqua, David C.; Ohmoto, Hiroshi] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
RP Kato, Y (reprint author), Univ Tokyo, Dept Syst Innovat, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1138656, Japan.
EM ykato@sys.t.u-tokyo.ac.jp
FU Japanese Ministry of Science, Education and Sports; Geological Survey of
Western Australia; NASA Astrobiology Institute
FX The ABDP drilling and research for this study were funded by the
Japanese Ministry of Science, Education and Sports (to Y.K., K.S., K.N.,
M.N. and MX), the Geological Survey of Western Australia (to A.H.) and
the NASA Astrobiology Institute (to H.O.). H.O. also acknowledges
support from the NASA Exobiology Program and the National Science
Foundation. A.H. publishes with permission of the Executive Director of
the Geological Survey of Western Australia. We thank S. Awaji and M.
Ohtsuki for assistance with chemical analyses, and M. Handier, Y.
Watanabe and K. Spangler for valuable comments and suggestions on an
earlier manuscript. Thorough review by R.W. Carlson, H. Elderfield, H.
Stein, and three anonymous reviewers has greatly improved our
manuscript.
NR 48
TC 24
Z9 25
U1 1
U2 21
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 FEB 15
PY 2009
VL 278
IS 1-2
BP 40
EP 49
DI 10.1016/j.epsl.2008.11.021
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 412FC
UT WOS:000263708400004
ER
PT J
AU Millet, DB
Atlas, EL
Blake, DR
Blake, NJ
Diskin, GS
Holloway, JS
Hudman, RC
Meinardi, S
Ryerson, TB
Sachse, GW
AF Millet, Dylan B.
Atlas, Elliot L.
Blake, Donald R.
Blake, Nicola J.
Diskin, Glenn S.
Holloway, John S.
Hudman, Rynda C.
Meinardi, Simone
Ryerson, Thomas B.
Sachse, Glen W.
TI Halocarbon Emissions from the United States and Mexico and Their Global
Warming Potential
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID ATMOSPHERIC HYDROXYL; METHYL CHLOROFORM; TROPOSPHERIC OH; ART.;
INVENTORY; CHEMISTRY; RADICALS; CH3CN; OCEAN; CITY
AB We use recent aircraft measurements of a comprehensive suite of anthropogenic halocarbons, carbon monoxide (CO), and related tracers to place new constraints on North American halocarbon emissions and quantify their global warming potential. Using a chemical transport model (GEOS-Chem) we find that the ensemble of observations are consistent with our prior best estimate of the U.S. anthropogenic CO source, but suggest a 30% underestimate of Mexican emissions. We develop an optimized CO emission inventory on this basis and quantify halocarbon emissions from their measured enhancements relative to CO. Emissions continue for many compounds restricted under the Montreal Protocol, and we show that halocarbons make up an important fraction of the total greenhouse gas source for both countries: our best estimate is 9% (uncertainty range 6-12%) and 32% (21-52%) of equivalent CO2 emissions for the U.S. and Mexico, respectively, on a 20 year time scale. Performance of bottom-up emission inventories is variable, with underestimates for some compounds and overestimates for others. Ongoing methylchloroform emissions are significant in the U.S. (2.8 Gg/y in 2004-2006), in contrast to bottom-up estimates (< 0.05 Gg), with implications for tropospheric OH calculations. Mexican methylchloroform emissions are minor.
C1 [Millet, Dylan B.] Univ Minnesota, St Paul, MN 55108 USA.
[Atlas, Elliot L.] Univ Miami, Miami, FL 33149 USA.
[Blake, Donald R.; Blake, Nicola J.; Meinardi, Simone] Univ Calif Irvine, Irvine, CA 92697 USA.
[Diskin, Glenn S.; Sachse, Glen W.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Holloway, John S.; Ryerson, Thomas B.] NOAA CSD, Boulder, CO 80305 USA.
[Hudman, Rynda C.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
RP Millet, DB (reprint author), Univ Minnesota, St Paul, MN 55108 USA.
EM dbm@umn.edu
RI Hudman, Rynda/C-6118-2009; Millet, Dylan/G-5832-2012; Holloway,
John/F-9911-2012; Ryerson, Tom/C-9611-2009; Chem, GEOS/C-5595-2014;
Atlas, Elliot/J-8171-2015
OI Holloway, John/0000-0002-4585-9594;
NR 46
TC 30
Z9 32
U1 2
U2 14
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD FEB 15
PY 2009
VL 43
IS 4
BP 1055
EP 1060
DI 10.1021/es802146j
PG 6
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 406MC
UT WOS:000263298600017
PM 19320157
ER
PT J
AU Cantrell, JH
AF Cantrell, John H.
TI Nonlinear dislocation dynamics at ultrasonic frequencies
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
DE Bessel functions; dislocation loops; shear modulus; stress effects;
ultrasonic effects
ID HARMONIC-GENERATION
AB An analytical model of the effects of the Peierls-Nabarro barrier stress on the nonlinear dynamics of dislocation motion in crystalline solids resulting from a perturbative ultrasonic wave is derived. The nonlinearity is quantified by a material nonlinearity parameter beta extracted from measurements of the amplitudes of the fundamental and harmonically generated ultrasonic waveforms. The beta parameter is found to be functionally dependent on the magnitude of the Peierls-Nabarro barrier stress, the dislocation loop length, the shear modulus, and the Burgers vector of the crystal. The parameter is shown to exhibit a Bessel function oscillatory dependence on the stress amplitude of the fundamental ultrasonic wave resulting directly from the Peierls-Nabarro barrier stress. A sharp increase in the magnitude of beta is shown to occur at low ultrasonic amplitudes where the dislocation motion is confined between adjacent lattice planes bounding the unperturbed dislocation. The generalization of the model to polycrystalline solids predicts a significant reduction in the beta oscillations that results in a dramatic hooklike shape of the beta versus stress amplitude curve at small values of the ultrasonic stress amplitude. Experimental observations of the hooklike shape (known as the Buck hook) have been reported in literature but the phenomenon has been previously unexplained. The present model shows that the Buck hook is a consequence of dislocation dynamics at low ultrasonic drive amplitudes.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Cantrell, JH (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA.
EM john.h.cantrell@nasa.gov
NR 14
TC 19
Z9 19
U1 0
U2 13
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD FEB 15
PY 2009
VL 105
IS 4
AR 043520
DI 10.1063/1.3081972
PG 7
WC Physics, Applied
SC Physics
GA 413OV
UT WOS:000263803300033
ER
PT J
AU Chow, S
Suzuki, N
Brodeur, RD
Ueno, Y
AF Chow, Seinen
Suzuki, Nobuaki
Brodeur, Richard D.
Ueno, Yasuhiro
TI Little population structuring and recent evolution of the Pacific saury
(Cololabis saira) as indicated by mitochondrial and nuclear DNA sequence
data
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Marine fish; Mitochondrial DNA; Nuclear DNA; Pacific saury; Population
structure; Recent evolution
ID NORTH PACIFIC; EPIPELAGIC NEKTON; CONTROL REGION; MARINE FISHES; GROWTH;
OCEAN; POLYMORPHISM; SARDINES
AB Genetic population structure of the Pacific saury (Cololabis saira) was investigated using nucleotide sequence analysis on the mitochondrial DNA control region (355-361 bp). Although the left domain of the control region is known to be highly variable in many species, extremely low nucleotide and haplotype diversities (pi-0.17% and h=0.418, respectively) were observed in a total of 141 individuals collected from five distant locales (East China Sea, Sea of Okhotsk, northwest Pacific, central North Pacific and northeast Pacific). No significant haplotype frequency differences were detected among widely separated samples, therefore we were unable to reject the null hypothesis of no genetic structuring in the Pacific saury population. Moderate levels of nucleotide substitution (p-distance) were observed between the Pacific saury and its Atlantic counterpart (Scomberesox saurus) in the control region (7.44%), cytochrome b gene (4.64%), and internal transcribed spacer (ITS1) (11.49%), indicating that the low sequence diversity of the control region in the Pacific saury is not due to the slow mutation rate. The molecular data suggest the Pacific saury may be a relatively recent offshoot among the extant members in the family Scomberesocidae. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Chow, Seinen] Natl Res Inst Fisheries Sci, Kanagawa 2360386, Japan.
[Suzuki, Nobuaki] Seikai Natl Fisheries Res Inst, Okinawa 9070451, Japan.
[Brodeur, Richard D.] NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
[Ueno, Yasuhiro] Tohoku Natl Fisheries Res Inst, Aomori 0310841, Japan.
RP Chow, S (reprint author), Natl Res Inst Fisheries Sci, Nagai 6-31-1, Kanagawa 2360386, Japan.
EM chow@affrc.go.jp
FU Ministry of Education, Science, Sports, and Culture of Japan [17380126];
Ministry of Agriculture, Forestry and Fisheries of Japan
FX We are grateful to Professor K. Numachi for kindly providing us his
original research article, H. Sato, Hokkaido Fisheries Experimental
Station, for supporting sample collection, and to H. Hasegawa, M.
Michibayashi and K. Saito for their technical help for molecular
analysis. We wish to thank P. Bentzen, S. Clifford and B. B. Collette
for kindly providing the Atlantic saury samples. We thank S. Grant, M.
Canino, and R. Baldwin for helpful comments on previous versions of this
manuscript. This work was supported in part by a Grant-in-Aid for
Scientific Research on Priority Areas (B) (No. 17380126) from the
Ministry of Education, Science, Sports, and Culture of Japan and the
Ministry of Agriculture, Forestry and Fisheries of Japan.
NR 44
TC 3
Z9 3
U1 1
U2 9
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD FEB 14
PY 2009
VL 369
IS 1
BP 17
EP 21
DI 10.1016/j.jembe.2008.10.023
PG 5
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 411DL
UT WOS:000263628100003
ER
PT J
AU Balikhin, MA
Sagdeev, RZ
Walker, SN
Pokhotelov, OA
Sibeck, DG
Beloff, N
Dudnikova, G
AF Balikhin, M. A.
Sagdeev, R. Z.
Walker, S. N.
Pokhotelov, O. A.
Sibeck, D. G.
Beloff, N.
Dudnikova, G.
TI THEMIS observations of mirror structures: Magnetic holes and instability
threshold
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID PLASMAS
AB Nonpropagating mirror-mode structures are commonly observed in many regions of natural plasma such as solar wind, planetary magnetosheaths, in cometary plasma, Io wake, terrestrial ring current and even on the outskirts of solar system. Mirror structures are typically observed in the shape of magnetic holes or peaks. Fast survey mode plasma data from the THEMIS satellites are used to solve the puzzle of how mirror structures in the form of dips can be observed in the regions of mirror stable plasma. THEMIS data also show that for mirror structures with spatial scales that considerably exceed ion Larmor radius the perpendicular temperature anticorrelates with the strength of the magnetic field. This contradiction with the conservation of adiabatic invariants is explained by the role of trapped particles. Citation: Balikhin, M. A., R. Z. Sagdeev, S. N. Walker, O. A. Pokhotelov, D. G. Sibeck, N. Beloff, and G. Dudnikova (2009), THEMIS observations of mirror structures: Magnetic holes and instability threshold, Geophys. Res. Lett., 36, L03105, doi: 10.1029/2008GL036923.
C1 [Balikhin, M. A.; Walker, S. N.; Pokhotelov, O. A.] Univ Sheffield, Dept Automat Control & Syst Engn, Sheffield S1 3JD, S Yorkshire, England.
[Beloff, N.] Univ Sussex, Dept Informat, Falmer BN1 9QJ, England.
[Sagdeev, R. Z.; Dudnikova, G.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Balikhin, MA (reprint author), Univ Sheffield, Dept Automat Control & Syst Engn, Mappin St, Sheffield S1 3JD, S Yorkshire, England.
EM balikhin@acse.shef.ac.uk; rs124@umd.edu; simon.walker@shef.ac.uk;
o.a.pokhotelov@shef.ac.uk; david.g.sibeck@nasa.gov;
n.beloff@sussex.ac.uk; gdudniko@umd.edu
RI Sibeck, David/D-4424-2012
FU STFC [3520]
FX The authors wish to thank the THEMIS team for providing the observations
reported in this paper. M. A. B., O. A. P. and S. N. W. would like to
acknowledge financial support from STFC. R. Z. S. acknowledges support
by ISTC project 3520.
NR 15
TC 21
Z9 21
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 13
PY 2009
VL 36
AR L03105
DI 10.1029/2008GL036923
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 406XR
UT WOS:000263328700005
ER
PT J
AU Winberry, JP
Anandakrishnan, S
Alley, RB
Bindschadler, RA
King, MA
AF Winberry, J. Paul
Anandakrishnan, Sridhar
Alley, Richard B.
Bindschadler, Robert A.
King, Matt A.
TI Basal mechanics of ice streams: Insights from the stick-slip motion of
Whillans Ice Stream, West Antarctica
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
ID TILL DEFORMATION; GLACIER BEDS; GPS DATA; BENEATH; FRICTION
AB The downstream portion of Whillans Ice Stream, West Antarctica, moves primarily by stick-slip motion. The observation of stick-slip motion suggests that the bed is governed by velocity-weakening physics and that the basal physics is more unstable than suggested by laboratory studies. The stick-slip cycle of Whillans Ice Plain exhibits substantial variability in both the duration of sticky periods and in slip magnitude. To understand this variability, we modeled the forces acting on the ice stream during the stick phase of the stick-slip cycle. The ocean tides introduce changes in the rate at which stress is applied to the ice plain. Increased loading rates promote earlier failure and vice versa. Results show that the bed of Whillans Ice Stream strengthens over time (healing) during the quiescent intervals in the stick-slip cycle, with the bed weakening during slip events. The time-dependent strengthening of the ice plain bed following termination of slip events indicates that the strength of the bed may vary by up to 0.35 kPa during the course of a single day.
C1 [Winberry, J. Paul] Cent Washington Univ, Dept Geol Sci, Ellensburg, WA 98926 USA.
[Winberry, J. Paul; Anandakrishnan, Sridhar; Alley, Richard B.] Penn State Univ, Dept Geosci, Ctr Remote Sensing Ice Sheets, University Pk, PA 16802 USA.
[Bindschadler, Robert A.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20770 USA.
[King, Matt A.] Univ Newcastle, Sch Civil Engn & Geosci, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
RP Winberry, JP (reprint author), Cent Washington Univ, Dept Geol Sci, 400 E Univ Way, Ellensburg, WA 98926 USA.
EM winberry@geology.cwu.edu
RI Winberry, Paul/E-5557-2011; King, Matt/B-4622-2008
OI King, Matt/0000-0001-5611-9498
FU US National Science Foundation [NSF-OPP-0229659]; New York Air National
Guard; UNAVCO
FX This work was funded by the US National Science Foundation
(NSF-OPP-0229659). M. A. K. was partly funded by a NERC fellowship. We
thank Raytheon Polar Services, the New York Air National Guard, and Ken
Borek Air for logistical support; UNAVCO for providing GPS receivers; as
well as Don Voigt, Huw Horgan, Ian Joughin, and Leo Peters for help with
the field deployment. Comments by Gordon Hamilton, Kelly Brunt, and an
anonymous reviewer improved the manuscript.
NR 33
TC 47
Z9 47
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-EARTH
JI J. Geophys. Res.-Earth Surf.
PD FEB 13
PY 2009
VL 114
AR F01016
DI 10.1029/2008JF001035
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA 406YE
UT WOS:000263330000002
ER
PT J
AU Neumann, GA
Mazarico, E
AF Neumann, Gregory A.
Mazarico, Erwan
TI PLANETARY SCIENCE Seeing the Missing Half
SO SCIENCE
LA English
DT Editorial Material
ID LUNAR; MASCONS; BASINS
C1 [Neumann, Gregory A.; Mazarico, Erwan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Neumann, GA (reprint author), NASA, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA.
EM gregory.a.neumann@nasa.gov; 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
NR 16
TC 3
Z9 3
U1 1
U2 1
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 13
PY 2009
VL 323
IS 5916
BP 885
EP 887
DI 10.1126/science.1170655
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 406KW
UT WOS:000263295400026
PM 19213904
ER
PT J
AU Fischer, EV
Hsu, NC
Jaffe, DA
Jeong, MJ
Gong, SL
AF Fischer, E. V.
Hsu, N. C.
Jaffe, D. A.
Jeong, M. -J.
Gong, S. L.
TI A decade of dust: Asian dust and springtime aerosol load in the US
Pacific Northwest
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID UNITED-STATES; SIMULATED CLIMATOLOGY; TRANSPORT; REGIONS
AB We integrate SeaWiFS aerosol optical thickness (AOT) over the Taklamakan and Gobi Deserts with U. S. aerosol observations to study surface aerosol variability in the Northwest U. S. in relation to Asian dust emissions. The results indicate that similar to 50% of the interannual variability in springtime average PM(2.5) and PM(10) can be explained by changes in Asian dust emissions. On a seasonal timescale, variations in dust emissions appear to be more important in determining the total material crossing the Pacific than the variations in meteorology represented by the PNA or the LRT3 indices. We are able to explain similar to 80% of the interannual variability using three variables: AOT, a transport index, and regional precipitation. This suggests that a strong source, favorable transport and sufficient residence time are needed for Asian dust to have a maximum seasonal impact in the Northwest. The results contextualize case studies and demonstrate the utility of the Deep Blue algorithm. Citation: Fischer, E. V., N. C. Hsu, D. A. Jaffe, M.-J. Jeong, and S. L. Gong (2009), A decade of dust: Asian dust and springtime aerosol load in the U. S. Pacific Northwest, Geophys. Res. Lett., 36, L03821, doi: 10.1029/2008GL036467.
C1 [Fischer, E. V.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Hsu, N. C.; Jeong, M. -J.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
[Jaffe, D. A.] Univ Washington, Bothell, WA 98011 USA.
[Jeong, M. -J.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Gong, S. L.] Environm Canada, Air Qual Res Div, Sci & Technol Branch, Toronto, ON M3H 5T4, Canada.
RP Fischer, EV (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA.
EM evf@u.washington.edu
RI Jeong, Myeong/B-8803-2008; Hsu, N. Christina/H-3420-2013; Fischer,
Emily/G-9478-2012; Fischer, Emily/K-7330-2015
OI Fischer, Emily/0000-0001-8298-3669
NR 17
TC 31
Z9 31
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 12
PY 2009
VL 36
AR L03821
DI 10.1029/2008GL036467
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 406XQ
UT WOS:000263328600005
ER
PT J
AU Shao, H
Zou, XL
Hajj, GA
AF Shao, Hui
Zou, Xiaolei
Hajj, George A.
TI Test of a non-local excess phase delay operator for GPS radio
occultation data assimilation
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE GPS radio occultation technique; excess phase delay; refractivity;
atmospheric data assimilation; non-local GPS observation operator
ID GPS/MET BENDING ANGLE; NUMERICAL WEATHER PREDICTION; ESTIMATION INVERSE
METHOD; TEMPERATURE; ATMOSPHERE; PROFILES; HUMIDITY; ADJOINT; IMPACT
AB A physically-sound, non-local excess phase delay observation operator is developed for simulating excess phase delay measurements from GPS radio occultation (RO) missions. By approximating an observed ray by a straight line, the refractivity gradient information along an observed ray path is included in the simulated excess phase delay. This observation operator is used to simulate observations from the German CHAllenging Minisatellite Payload (CHAMP) RO mission based on large-scale analysis. The need to use such an observation operator for GPS RO data assimilation in spherically asymmetric regions is shown by results from a set of forward simulation and data assimilation experiments. A modification that renders the non-local excess phase delay observation operator more suitable for parallel implementation of GPS RO data assimilation is proposed.
C1 [Shao, Hui; Zou, Xiaolei] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA.
[Shao, Hui] Natl Ctr Atmospher Res, MMM, Boulder, CO 80307 USA.
[Hajj, George A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Shao, H (reprint author), Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA.
EM zou@met.fsu.edu; george.hajj@jpl.nasa.gov
FU National Science Foundation [ATM-0101036]
FX This study is supported by the National Science Foundation under the
project ATM-0101036.
NR 27
TC 2
Z9 3
U1 1
U2 4
PU SPIE-SOC PHOTOPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1931-3195
J9 J APPL REMOTE SENS
JI J. Appl. Remote Sens.
PD FEB 12
PY 2009
VL 3
AR 033508
DI 10.1117/1.3094060
PG 16
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 520SL
UT WOS:000271868100001
ER
PT J
AU Popp, PJ
Marcy, TP
Gao, RS
Watts, LA
Fahey, DW
Richard, EC
Oltmans, SJ
Santee, ML
Livesey, NJ
Froidevaux, L
Sen, B
Toon, GC
Walker, KA
Boone, CD
Bernath, PF
AF Popp, P. J.
Marcy, T. P.
Gao, R. S.
Watts, L. A.
Fahey, D. W.
Richard, E. C.
Oltmans, S. J.
Santee, M. L.
Livesey, N. J.
Froidevaux, L.
Sen, B.
Toon, G. C.
Walker, K. A.
Boone, C. D.
Bernath, P. F.
TI Stratospheric correlation between nitric acid and ozone
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID IN-SITU MEASUREMENTS; FOURIER-TRANSFORM SPECTROMETER; ARCTIC LOWER
STRATOSPHERE; UPPER TROPOSPHERE; UNITED-STATES; ACE-FTS; HNO3;
CHEMISTRY; O-3; DENITRIFICATION
AB An extensive data set of nitric acid (HNO3) and ozone (O-3) measurements has been collected in the lower and middle stratosphere with in situ instruments onboard the NASA WB-57F aircraft and remote sounding instruments that include the JPL MkIV Interferometer, the Aura Microwave Limb Sounder, and the Atmospheric Chemistry Experiment Fourier Transform Spectrometer. The measurements utilized in this study span a broad latitudinal range between the deep tropics and northern high latitudes. The data are used to establish the robustness of the HNO3-O-3 correlation in the stratosphere and the latitudinal dependence in the correlation. Good agreement is found among the HNO3-O-3 correlations observed with the various instruments. Comparing HNO3-O-3 correlations relaxes the coincidence criteria necessary when making direct comparisons of HNO3 measurements and allows meaningful comparisons between data sets that are not closely matched in time or space. The utility of this correlation is further demonstrated by establishing vertical profiles of proxy HNO3 mixing ratios using the observed correlation and widely available ozonesonde data. These profiles expand the range of data available for validating remote measurements of HNO3. The HNO3-O-3 correlation is also demonstrated as a diagnostic for identifying locally enhanced HNO3 in the upper troposphere. In situ measurements of HNO3 near the tropical tropopause during the Aura validation campaigns are consistent with ACE-FTS observations, with both revealing extremely low mixing ratios (< 125 ppt) and a HNO3 minimum in this region.
C1 [Boone, C. D.; Bernath, P. F.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England.
[Popp, P. J.; Marcy, T. P.; Gao, R. S.; Watts, L. A.; Fahey, D. W.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Santee, M. L.; Livesey, N. J.; Froidevaux, L.; Sen, B.; Toon, G. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Oltmans, S. J.] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Richard, E. C.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
[Walker, K. A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A1, Canada.
RP Popp, PJ (reprint author), Univ Colorado, Leeds Sch Business, Boulder, CO 80309 USA.
EM peter.popp@colorado.edu
RI Bernath, Peter/B-6567-2012; Gao, Ru-Shan/H-7455-2013; Watts,
Laurel/G-4532-2013; Fahey, David/G-4499-2013; Manager, CSD
Publications/B-2789-2015
OI Bernath, Peter/0000-0002-1255-396X; Watts, Laurel/0000-0002-0834-3329;
Fahey, David/0000-0003-1720-0634;
FU NASA; NOAA; Canadian Space Agency; Natural Sciences and Engineering
Research Council of Canada
FX The authors wish to thank the air and ground crews of the NASA WB-57F
aircraft. This work was partially supported by the NASA Upper
Atmospheric Research Program and NOAA Atmospheric Chemistry and Climate
Program. Work performed at the Jet Propulsion Laboratory, California
Institute of Technology, was done under contract with NASA. The
Atmospheric Chemistry Experiment (ACE), also known as SCISAT-1, is a
Canadian-led mission mainly supported by the Canadian Space Agency and
the Natural Sciences and Engineering Research Council of Canada.
NR 44
TC 9
Z9 9
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 12
PY 2009
VL 114
AR D03305
DI 10.1029/2008JD010875
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 406XY
UT WOS:000263329400004
ER
PT J
AU Kounaves, SP
Hecht, MH
West, SJ
Morookian, JM
Young, SMM
Quinn, R
Grunthaner, P
Wen, XW
Weilert, M
Cable, CA
Fisher, A
Gospodinova, K
Kapit, J
Stroble, S
Hsu, PC
Clark, BC
Ming, DW
Smith, PH
AF Kounaves, Samuel P.
Hecht, Michael H.
West, Steven J.
Morookian, John-Michael
Young, Suzanne M. M.
Quinn, Richard
Grunthaner, Paula
Wen, Xiaowen
Weilert, Mark
Cable, Casey A.
Fisher, Anita
Gospodinova, Kalina
Kapit, Jason
Stroble, Shannon
Hsu, Po-Chang
Clark, Benton C.
Ming, Douglas W.
Smith, Peter H.
TI The MECA Wet Chemistry Laboratory on the 2007 Phoenix Mars Scout Lander
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID X-RAY SPECTROMETER; ION-SELECTIVE ELECTRODES; MERIDIANI-PLANUM;
CHEMICAL-COMPOSITION; BURNS FORMATION; MARTIAN SOIL; GUSEV CRATER;
ROCKS; ARRAY; GROUNDWATER
AB To analyze and interpret the chemical record, the 2007 Phoenix Mars Lander includes four wet chemistry cells. These Wet Chemistry Laboratories (WCLs), part of the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) package, each consist of a lower "beaker'' containing sensors designed to analyze the chemical properties of the regolith and an upper "actuator assembly'' for adding soil, water, reagents, and stirring. The beaker contains an array of sensors and electrodes that include six membrane-based ion selective electrodes (ISE) to measure Ca2+, Mg2+, K+, Na+, NO3-/ClO4-, and NH4+; two ISEs for H+ (pH); a Ba2+ ISE for titrimetric determination of SO42-; two Li+ ISEs as reference electrodes; three solid crystal pellet ISEs for Cl-, Br-, and I-; an iridium oxide electrode for pH; a carbon ring electrode for conductivity; a Pt electrode for oxidation reduction potential (Eh); a Pt and two Ag electrodes for determination of Cl-, Br-, and I- using chronopotentiometry (CP); a Au electrode for identifying redox couples using cyclic voltammetry (CV); and a Au microelectrode array that could be used for either CV or to indicate the presence of several heavy metals, including Cu2+, Cd2+, Pb2+, Fe2/3+, and Hg2+ using anodic stripping voltammetry (ASV). The WCL sensors and analytical procedures have been calibrated and characterized using standard solutions, geological Earth samples, Mars simulants, and cuttings from a Martian meteorite. Sensor characteristics such as limits of detection, interferences, and implications of the Martian environment are also being studied. A sensor response library is being developed to aid in the interpretation of the data.
C1 [Kounaves, Samuel P.; Young, Suzanne M. M.; Cable, Casey A.; Gospodinova, Kalina; Kapit, Jason; Stroble, Shannon; Hsu, Po-Chang] Tufts Univ, Dept Chem, Medford, MA 02155 USA.
[Hecht, Michael H.; Morookian, John-Michael; Grunthaner, Paula; Weilert, Mark; Fisher, Anita] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[West, Steven J.] Invensys Corp, Foxboro Field Devices Div, Foxboro, MA 02035 USA.
[West, Steven J.; Wen, Xiaowen] Thermo Fisher Sci, Beverly, MA 01915 USA.
[Quinn, Richard] SETI Inst, Mountain View, CA 94043 USA.
[Clark, Benton C.] Lockheed Martin Corp, Littleton, CO 80127 USA.
[Ming, Douglas W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Smith, Peter H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Kounaves, SP (reprint author), Tufts Univ, Dept Chem, 62 Talbot Ave, Medford, MA 02155 USA.
EM samuel.kounaves@tufts.edu
OI Kounaves, Samuel/0000-0002-2629-4831
NR 33
TC 26
Z9 26
U1 2
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 12
PY 2009
VL 114
AR E00A19
DI 10.1029/2008JE003084
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 406YL
UT WOS:000263330700001
ER
PT J
AU Lin, II
Chen, CH
Pun, IF
Liu, WT
Wu, CC
AF Lin, I. -I.
Chen, Chi-Hong
Pun, Iam-Fei
Liu, W. Timothy
Wu, Chun-Chieh
TI Warm ocean anomaly, air sea fluxes, and the rapid intensification of
tropical cyclone Nargis (2008)
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID HURRICANE INTENSITY; THERMAL STRUCTURE; EDDY
AB On 2 May 2008, category-4 tropical cyclone Nargis devastated Myanmar. It was observed that just prior to its landfall, Nargis rapidly intensified from a weak category-1 ;storm to an intense category-4 storm within only 24 h. Using in situ ocean depth-temperature measurements and satellite altimetry, it is found that Nargis' rapid intensification took place on a pre-existing warm ocean anomaly in the Bay of Bengal. In the anomaly, the subsurface ocean is evidently warmer than climatology, as characterized by the depth of the 26 degrees C isotherm of 73-101 m and the tropical cyclone heat potential of 77 105 kj cm(-2). This pre-existing deep, warm subsurface layer leads to reduction in the cyclone-induced ocean cooling, as shown from the ocean mixed layer numerical experiments. As a result, there was a near 300% increase in the air-sea enthalpy flux to support Nargis' rapid intensification. Citation: Lin, I.-I., C.-H. Chen, I.-F. Pun, W. T. Liu, and C.-C. Wu(2009), Warm ocean anomaly, air sea fluxes, and the rapid intensification of tropical cyclone Nargis (2008), Geophys. Res. Lett., 36, L03817, doi: 10.1029/2008GL035815.
C1 [Lin, I. -I.; Chen, Chi-Hong; Pun, Iam-Fei; Wu, Chun-Chieh] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 106, Taiwan.
[Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA 91011 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 Lin, I-I/J-4695-2013;
OI Lin, I-I/0000-0002-8364-8106; Wu, Chun-Chieh/0000-0002-3612-4537
FU National Science Council [97-2111-M-002-014-MY3, 95-2611-M-002-024-MY3];
National Aeronautics and Space Administration
FX The authors wish to thank Dong-Ping Wang for providing the mixed layer
model, and to Sau Ni Hui for data processing. Thanks also to the NCEP,
the AVISO altimetry team, and the Argo float team for data provision.
This work is supported by the National Science Council, Taiwan through
NSC 97-2111-M-002-014-MY3 and NSC 95-2611-M-002-024-MY3. This work is
also under Taiwan National Science Council's Integrated Typhoon-Ocean
Program (ITOP). The work of W. T. Liu was supported by the National
Aeronautics and Space Administration.
NR 18
TC 69
Z9 72
U1 5
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 11
PY 2009
VL 36
AR L03817
DI 10.1029/2008GL035815
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 406XO
UT WOS:000263328400001
ER
PT J
AU Farrell, SA
Barret, D
Skinner, GK
AF Farrell, S. A.
Barret, D.
Skinner, G. K.
TI Superorbital variability in hard X-rays
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: neutron; X-rays: binaries
ID WARPED ACCRETION DISCS; LONG-TERM PROPERTIES; UNEVENLY SPACED DATA;
TIME-SERIES ANALYSIS; CLUSTER NGC 6624; RXTE ASM DATA; SCORPIUS X-1; 4U
1820-30; CYGNUS X-2; NEUTRON-STAR
AB We present the results of a study with the Swift Burst Alert Telescope in the 14-195 keV range of the long-term variability of five low-mass X-ray binaries with reported or suspected superorbital periods - 4U 1636-536, 4U 1820-303, 4U 1916-053, Cyg X-2 and Sco X-1. No significant persistent periodic modulation was detected around the previously reported periods in the 4U 1916-053, Cyg X-2 or Sco X-1 light curves. The similar to 170-d period of 4U 1820-303 was detected up to 24 keV, consistent with variable accretion due to the previously proposed triple system model. The similar to 46-d period in 4U 1636-536 was detected up to 100 keV, with the modulation in the low- and high-energy bands found to be phase shifted by similar to 180 degrees with respect to each other. This phase shift, when taken together with the near-coincident onset of the similar to 46-d modulation and the low/hard X-ray state, leads us to speculate that the modulation could herald transient jet formation.
C1 [Farrell, S. A.; Barret, D.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Skinner, G. K.] NASA, Goddard Space Flight Ctr, CRESST & Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Skinner, G. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Farrell, SA (reprint author), CNRS UPS, Ctr Etud Spatiale Rayonnements, 9 Ave Colonel Roche, F-31028 Toulouse 4, France.
EM sean.farrell@cesr.fr
NR 85
TC 12
Z9 12
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 FEB 11
PY 2009
VL 393
IS 1
BP 139
EP 156
DI 10.1111/j.1365-2966.2008.14167.x
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 399EF
UT WOS:000262782500027
ER
PT J
AU Kar, A
Yang, JY
Dutta, M
Stroscio, MA
Kumari, J
Meyyappan, M
AF Kar, Ayan
Yang, Jianyong
Dutta, Mitra
Stroscio, Michael A.
Kumari, Jyoti
Meyyappan, M.
TI Rapid thermal annealing effects on tin oxide nanowires prepared by
vapor-liquid-solid technique
SO NANOTECHNOLOGY
LA English
DT Article
ID GROWTH; SNO2
AB Tin oxide nanowires have been grown on p-type silicon substrates using a gold-catalyst-assisted vapor-liquid-solid growth process. The nanowires were annealed in the presence of oxygen at 700 degrees C for different time intervals. The changes in material properties of the nanowires after annealing were investigated using various characterization techniques. Annealing improves the crystal quality of the nanowires as seen from Raman spectroscopy analysis. Photoluminescence (PL) data indicates a decrease in the oxygen vacancies and defects after annealing, affecting the luminescence from the nanowires. In addition, x-ray photoelectron spectroscopy (XPS) was used to obtain the changes in the tin and oxygen atomic concentrations before and after annealing, from which the stoichiometry was calculated.
C1 [Kar, Ayan; Yang, Jianyong; Dutta, Mitra; Stroscio, Michael A.] Univ Illinois, Dept Elect & Comp Engn, Chicago, IL 60607 USA.
[Dutta, Mitra; Stroscio, Michael A.] Univ Illinois, Dept Phys, Chicago, IL 60607 USA.
[Stroscio, Michael A.] Univ Illinois, Dept Bioengn, Chicago, IL 60607 USA.
[Kumari, Jyoti; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
RP Kar, A (reprint author), Univ Illinois, Dept Elect & Comp Engn, Chicago, IL 60607 USA.
EM dutta@ece.uic.edu
NR 14
TC 24
Z9 25
U1 2
U2 16
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD FEB 11
PY 2009
VL 20
IS 6
AR 065704
DI 10.1088/0957-4484/20/6/065704
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 395AK
UT WOS:000262494200030
PM 19417398
ER
PT J
AU Zhai, CX
Yu, J
Shao, M
Goullioud, R
Milman, M
Shen, TP
AF Zhai, Chengxing
Yu, Jeffrey
Shao, Mike
Goullioud, Renaud
Milman, Mark
Shen, Tsae-Pyng
TI SIM PlanetQuest white-light fringe modeling: picometer accuracy
calibration and estimation algorithms
SO APPLIED OPTICS
LA English
DT Article
ID ASTROMETRY
AB SIM PlanetQuest will perform narrow-angle astrometry with microarcsecond accuracy using starlight interferometry requiring tens of picometers accuracy in estimating the optical path difference change between observing two stars. One challenge is to accurately model the white-light fringes and calibrate the required model parameters. Previous studies have developed algorithms based on a CCD-pixel-level calibration scheme assuming slowly varying phase-dispersion functions. However, recent measurements from the SIM PlanetQuest Spectral Calibration Development Unit (SCDU) showed that wavefront aberrations caused the phase-dispersion functions to vary by tens of nanometers across the bandwidth of a CCD pixel, making the previous CCD-pixel-based calibration scheme inadequate. We present a white-light fringe model including the extra phase dispersions caused by the wavefront aberrations together with a calibration and estimation scheme using long-stroke fringe measurements to resolve the bandwidth of pixels. Using simulated data, we show that the total systematic errors in the calibration and estimation scheme are less than a picometer. With SCDU experimental data, we demonstrate that the end-to-end accuracy of the calibration and estimation algorithm is better than 20 pro, achieving the SIM PlanetQuest Engineering Milestone 4. (C) 2009 Optical Society of America
C1 [Zhai, Chengxing; Yu, Jeffrey; Shao, Mike; Goullioud, Renaud; Milman, Mark; Shen, Tsae-Pyng] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zhai, CX (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Chengxing.Zhai@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX We thank the SCDU working team members Rick Demers (SCDU lead), Hong
Tang, Xin An, and George Sun for providing the SCDU experimental data
and many useful discussions. This work was prepared at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration (NASA).
NR 13
TC 4
Z9 4
U1 0
U2 1
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD FEB 10
PY 2009
VL 48
IS 5
BP 847
EP 861
DI 10.1364/AO.48.000847
PG 15
WC Optics
SC Optics
GA 419HS
UT WOS:000264210900006
PM 19209195
ER
PT J
AU Gappinger, RO
Diaz, RT
Ksendzov, A
Lawson, PR
Lay, OP
Liewer, KM
Loya, FM
Martin, SR
Serabyn, E
Wallace, JK
AF Gappinger, Robert O.
Diaz, Rosemary T.
Ksendzov, Alexander
Lawson, Peter R.
Lay, Oliver P.
Liewer, Kurt M.
Loya, Frank M.
Martin, Stefan R.
Serabyn, Eugene
Wallace, James K.
TI Experimental evaluation of achromatic phase shifters for mid-infrared
starlight suppression
SO APPLIED OPTICS
LA English
DT Article
ID NULLING INTERFEROMETRY; SPACE INTERFEROMETER; NEARBY STARS; PLANETS;
NULLER; PROGRESS; SYSTEM
AB Phase shifters are a key component of nulling interferometry, one of the potential routes to enabling the measurement of faint exoplanet spectra. Here, three different achromatic phase shifters are evaluated experimentally in the mid-infrared, where such nulling interferometers may someday operate. The methods evaluated include the use of dispersive glasses, a through-focus field inversion, and field reversals on reflection from antisymmetric flat-mirror periscopes. All three approaches yielded deep, broadband, mid-infrared nulls, but the deepest broadband nulls were obtained with the periscope architecture. In the periscope system, average null depths of 4 x 10(-5) were obtained with a 25% bandwidth, and 2 x 10(-5) with a 20% bandwidth, at a central wavelength of 9.5 mu m. The best short term nulls at 20% bandwidth were approximately 9 x 10(-6), in line with error budget predictions and the limits of the current generation of hardware. (C) 2009 Optical Society of America
C1 [Gappinger, Robert O.; Diaz, Rosemary T.; Ksendzov, Alexander; Lawson, Peter R.; Lay, Oliver P.; Liewer, Kurt M.; Loya, Frank M.; Martin, Stefan R.; Serabyn, Eugene; Wallace, James K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gappinger, RO (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Robert.O.Gappinger@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX The work described in this paper was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration (NASA).
NR 37
TC 21
Z9 21
U1 0
U2 1
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD FEB 10
PY 2009
VL 48
IS 5
BP 868
EP 880
DI 10.1364/AO.48.000868
PG 13
WC Optics
SC Optics
GA 419HS
UT WOS:000264210900008
PM 19209197
ER
PT J
AU Muslimov, AG
Harding, AK
AF Muslimov, Alex G.
Harding, Alice K.
TI PAIR-STARVED PULSAR MAGNETOSPHERES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: general; stars: neutron
ID X-RAY-EMISSION; ROTATING MAGNETOSPHERES; APPROXIMATION; ACCELERATION;
SIMULATIONS; FRONTS; PLASMA
AB We propose a simple analytic model for the innermost (within the light cylinder (LC) of canonical radius similar to c/Omega) structure of open-magnetic-field lines of a rotating neutron star (NS) with relativistic outflow of charged particles (electrons/ positrons) and an arbitrary angle between the NS spin and magnetic axes. We present the self-consistent solution of Maxwell's equations for the magnetic field and electric current in the pair-starved regime where the density of electron-positron plasma generated above the pulsar polar cap is not sufficient to completely screen the accelerating electric field and thus establish the E center dot B = 0 condition above the pair-formation front up to the very high altitudes within the LC. The proposed model may provide a theoretical framework for developing the refined model of the global pair-starved pulsar magnetosphere.
C1 [Muslimov, Alex G.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Muslimov, Alex G.; Harding, Alice K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Muslimov, AG (reprint author), Univ Space Res Assoc, Columbia, MD 21044 USA.
RI Harding, Alice/D-3160-2012
NR 31
TC 12
Z9 12
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2009
VL 692
IS 1
BP 140
EP 148
DI 10.1088/0004-637X/692/1/140
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410CG
UT WOS:000263553000012
ER
PT J
AU Kane, SR
Mahadevan, S
Cochran, WD
Street, RA
Sivarani, T
Henry, GW
Williamson, MH
AF Kane, Stephen R.
Mahadevan, Suvrath
Cochran, William D.
Street, Rachel A.
Sivarani, Thirupathi
Henry, Gregory W.
Williamson, Michael H.
TI DISCOVERY OF A LOW-MASS COMPANION TO THE SOLAR-TYPE STAR TYC 2534-698-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: low-mass, brown dwarfs
ID HOBBY-EBERLY TELESCOPE; BROWN-DWARF; PLANET; SPECTROGRAPH; PHOTOMETRY;
SYSTEM
AB Brown dwarfs and low-mass stellar companions are interesting objects to study since they occupy the mass region between deuterium and hydrogen burning. We report here the serendipitous discovery of a low-mass companion in an eccentric orbit around a solar-type main-sequence star. The stellar primary, TYC 2534-698-1, is a G2V star that was monitored both spectroscopically and photometrically over the course of several months. Radial velocity observations indicate a minimum mass of 0.037 M(circle dot) and an orbital period of similar to 103 days for the companion. Photometry outside of the transit window shows the star to be stable to within similar to 6 millimags. The semimajor axis of the orbit places the companion in the "brown dwarf desert" and we discuss potential follow-up observations that could constrain the mass of the companion.
C1 [Kane, Stephen R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Mahadevan, Suvrath; Sivarani, Thirupathi] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Street, Rachel A.] Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Henry, Gregory W.; Williamson, Michael H.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
RP Kane, SR (reprint author), CALTECH, NASA, Exoplanet Sci Inst, MS 100-22,770 S Wilson Ave, Pasadena, CA 91125 USA.
EM skane@ipac.caltech.edu
RI Kane, Stephen/B-4798-2013
NR 25
TC 5
Z9 5
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 FEB 10
PY 2009
VL 692
IS 1
BP 290
EP 297
DI 10.1088/0004-637X/692/1/290
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410CG
UT WOS:000263553000027
ER
PT J
AU Blair, WP
Sankrit, R
Torres, SI
Chayer, P
Danforth, CW
AF Blair, William P.
Sankrit, Ravi
Torres, Sharon I.
Chayer, Pierre
Danforth, Charles W.
TI FAR ULTRAVIOLET SPECTROSCOPIC EXPLORER OBSERVATIONS OF KPD 2055+3111, A
STAR BEHIND THE CYGNUS LOOP
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual (Cygnus Loop); stars: individual (KPD 2055+3111);
supernova remnants
ID VELA SUPERNOVA REMNANT; ON-ORBIT PERFORMANCE; PRIMARY SHOCK FRONT;
MOLECULAR-HYDROGEN; RADIATIVE SHOCKS; INTERSTELLAR-MEDIUM; NONRADIATIVE
SHOCK; FUSE OBSERVATIONS; ADIABATIC SURVEY; BAND SYSTEM
AB We have observed a star behind the Cygnus Loop supernova remnant using the Far Ultraviolet Spectroscopic Explorer (FUSE) satellite to study the line-of-sight interstellar medium structures toward and through this prototypical remnant. An sdOB star, KPD 2055+3111, was identified from Ultraviolet Imaging Telescope UV images and lies in projection within the bright northeast Cygnus Loop filaments (NGC 6992). This is the first known UV background source for the Cygnus Loop. We have observed this star as well as the directly adjacent emission-line filaments. Although the intrinsic spectrum of the star is complex, a broad OVI lambda 1032 absorption line due the Cygnus Loop is present in the stellar spectrum, confirming that the star lies beyond the Cygnus Loop. Optical spectroscopy of the star and model fits permits a distance estimate to the star of 576 +/- 61 pc, thus providing an independent upper limit on the distance to the Cygnus Loop. Numerous absorption transitions of molecular hydrogen are present in the FUSE spectrum of KPD 2055+3111. Assessment of the properties of the H(2) indicates a column density of (3.3 +/- 0.6) x 10(16) cm(-2) and a two-temperature J-level population T (J = 0-1) = 106 +/- 40 K and T (J = 2-5) = 850 +/- 230 K. There is no direct evidence from linewidths, component structure, or velocity displacements that the detected H(2) is associated with the Cygnus Loop as opposed to the interstellar gas along the sight line, so either source remains viable. The OVI emission line profiles directly adjacent to line of sight to the star show dramatic variability on small (20 '') spatial scales, highlighting how differently the UV-emitting gas can be distributed compared with optical and other wave bands. This impacts the ability to directly compare the emission and absorption components along the sight line.
C1 [Blair, William P.; Torres, Sharon I.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Sankrit, Ravi] SOFIA USRA, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Chayer, Pierre] NRC, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Danforth, Charles W.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Chayer, Pierre] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Blair, WP (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
EM wpb@pha.jhu.edu; rsankrit@sofia.usra.edu; torres.sharon@gmail.com;
chayer@stsci.edu; danforth@casa.colorado.edu
FU NASA [NAG5-12423, NNG04GJ25G, NNG05GD75G]
FX It is a pleasure to thank the FUSE operations team at JHU for their
efforts in obtaining these data. We also thank Robert Fesen for
obtaining the new optical data on KPD 2055+3111. This work has been
supported by NASA grants NAG5-12423, NNG04GJ25G, and NNG05GD75G, all to
the Johns Hopkins University.
NR 53
TC 17
Z9 17
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2009
VL 692
IS 1
BP 335
EP 345
DI 10.1088/0004-637X/692/1/335
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410CG
UT WOS:000263553000031
ER
PT J
AU Brosius, JW
Holman, GD
AF Brosius, Jeffrey W.
Holman, Gordon D.
TI OBSERVATIONS OF THE THERMAL AND DYNAMIC EVOLUTION OF A SOLAR MICROFLARE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: flares; Sun: transition region; Sun: UV
radiation; Sun: X-rays, gamma rays
ID CORONAL DIAGNOSTIC SPECTROMETER; HIGH TIME RESOLUTION; HARD X-RAY; LOOP
RADIATIVE HYDRODYNAMICS; CHROMOSPHERIC EVAPORATION; RHESSI MICROFLARES;
ULTRAVIOLET BRIGHTENINGS; EXTREME-ULTRAVIOLET; ATOMIC DATABASE;
EMISSION-LINES
AB We observed a solar microflare over a wide temperature range with three instruments aboard the SOHO spacecraft (Coronal Diagnostic Spectrometer (CDS), Extreme-ultraviolet Imaging Telescope (EIT), and Michelson Doppler Imager (MDI)), TRACE (1600 angstrom), GOES, and RHESSI. The microflare's properties and behavior are those of a miniature flare undergoing gentle chromospheric evaporation, likely driven by nonthermal electrons. Extremeultraviolet spectra were obtained at a rapid cadence (9.8 s) with CDS in stare mode that included emission lines originating from the chromosphere (temperature of formation T(m) approximate to 1 x 104 K) and transition region (TR), to coronal and flare (T(m) approximate to 8 x 10(6) K) temperatures. Light curves derived from the CDS spectra and TRACE images (obtained with a variable cadence approximate to 34 s) reveal two precursor brightenings before the microflare. After the precursors, chromospheric and TR emission are the first to increase, consistent with energy deposition by nonthermal electrons. The initial slow rise is followed by a brief (20 s) impulsive EUV burst in the chromospheric and TR lines, during which the coronal and hot flare emission gradually begin to increase. Relative Doppler velocities measured with CDS are directed upward with maximum values approximate to 20 km s(-1) during the second precursor and shortly before the impulsive peak, indicating gentle chromospheric evaporation. Electron densities derived from an O IV line intensity ratio (T(m) approximate to 1.6 x 10(5) K) increased from 2.6 x 10(10) cm(-3) during quiescent times to 5.2 x 10(11) cm(-3) at the impulsive peak. The X-ray emission observed by RHESSI peaked after the impulsive peak at chromospheric and TR temperatures and revealed no evidence of emission from nonthermal electrons. Spectral fits to the RHESSI data indicate a maximum temperature of approximate to 13 MK, consistent with a slightly lower temperature deduced from the GOES data. Magnetograms fromMDI show that the microflare occurred in and around a growing island of negative magnetic polarity embedded in a large area of positive magnetic field. The microflare was compact, covering an area of 4 x 10(7) km(2) in the EIT image at 195 angstrom, and appearing as a point source located 7 '' west of the EIT source in the RHESSI image. TRACE images suggest that the microflare filled small loops.
C1 [Brosius, Jeffrey W.; Holman, Gordon D.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Brosius, JW (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA.
EM Jeffrey.W.Brosius@nasa.gov; Gordon.D.Holman@nasa.gov
RI Holman, Gordon/C-9548-2012
FU NASA [NNX07AI09G]; RHESSI
FX J.W.B. acknowledges NASA support through SR&T grant NNX07AI09G. G. D. H.
acknowledges partial support through SR&T grant NNX07AI09G and the
RHESSI project.
NR 48
TC 29
Z9 30
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2009
VL 692
IS 1
BP 492
EP 501
DI 10.1088/0004-637X/692/1/492
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410CG
UT WOS:000263553000042
ER
PT J
AU Valencic, LA
Smith, RK
Dwek, E
Graessle, D
Dame, TM
AF Valencic, Lynne A.
Smith, Randall K.
Dwek, Eli
Graessle, Dale
Dame, T. M.
TI EXAMINING DUST GRAIN MODELS USING THE REDDENING AND X-RAY DUST HALO OF
TERZAN 2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; globular clusters: individual (Terzan 2); X-rays: ISM
ID GLOBULAR-CLUSTER TERZAN-2; INTERSTELLAR DUST; INFRARED-EMISSION;
GALACTIC-CENTER; MILKY-WAY; H-I; SCATTERING; EXTINCTION; ABSORPTION;
PHOTOMETRY
AB We use the X-ray dust halo of the low-mass X-ray binary 4U 1724-307, located in the globular cluster Terzan 2, to probe the interstellar medium along this line of sight (LOS). The X-ray dust halo arises from X-rays scattering off of interstellar dust grains. Using a low optical depth sight line to determine the Chandra ACIS point-spread function, we extracted the radial profile as a function of energy and used it to determine the H column density (N(H)) and cloud location along the LOS for several dust grain models, including the commonly-used models of MRN and WD. The resulting N(H) values were used to determine the reddening E(B-V), which was then compared with the average E(B-V) for this sight line found by other workers. We found that for this LOS, only the ZDA BARE-AC-S, BARE-GR-FG, and BARE-GR-S models yield reddenings within 1 sigma of the literature average.
C1 [Valencic, Lynne A.; Dwek, Eli] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Valencic, Lynne A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Smith, Randall K.; Graessle, Dale; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Valencic, LA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM valencic@milkyway.gsfc.nasa.gov
RI Dwek, Eli/C-3995-2012
FU NASA
FX The authors thank an anonymous referee for many helpful and insightful
comments. 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 50
TC 6
Z9 6
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2009
VL 692
IS 1
BP 502
EP 510
DI 10.1088/0004-637X/692/1/502
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410CG
UT WOS:000263553000043
ER
PT J
AU Ghosh, KK
Narasimha, D
AF Ghosh, Kajal K.
Narasimha, D.
TI A QUASI-STELLAR OBJECT PLUS HOST SYSTEM LENSED INTO A 6 '' EINSTEIN RING
BY A LOW-REDSHIFT GALAXY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (SDSS J091949.16+342304.0); galaxies: structure;
galaxies: evolution; galaxies: elliptical and lenticular, cD;
gravitational lensing
ID DIGITAL-SKY-SURVEY; GRAVITATIONAL LENSES; BINARY QUASARS; TRIPLE QUASAR;
DISCOVERY; CLUSTERS; EMISSION
AB We report the serendipitous discovery of an Einstein Ring in the optical band from the Sloan Digital Sky Survey (SDSS) data and four associated images of a background source. The lens galaxy appears to be a nearby dwarf spheroid at a redshift of 0.0375 +/- 0.002. The lensed quasar is at a redshift of 0.6842 +/- 0.0014, and its multiple images are distributed almost 360. around the lens nearly along a ring of radius similar to 6."0. Single-component lens models require a mass of the galaxy of almost 10(12) M circle dot within 6."0 from the lens center. With the available data, we are unable to determine the exact positions, orientations, and fluxes of the quasar and the galaxy, though there appears to be evidence for a double- or multiple-merging image of the quasar. We have also detected strong radio and X-ray emissions from this system. It is indicative that this ring system may be embedded in a group or cluster of galaxies. This unique ring, by virtue of the closeness of the lens galaxy, offers a possible probe of some key issues such as the mass-to-light ratio of intrinsically faint galaxies and the existence of large-scalemagnetic fields in elliptical galaxies.
C1 [Ghosh, Kajal K.] NASA, USRA NSSTC MSFC, Huntsville, AL 35805 USA.
[Narasimha, D.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
RP Ghosh, KK (reprint author), NASA, USRA NSSTC MSFC, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM kajal.k.ghosh@nasa.gov; dna@tifr.res.in
FU Alfred P. Sloan Foundation; Participating Institutions; National
Aeronautics and Space Administration; National Science Foundation; U.S.
Department of Energy; Japanese Monbuka-gakusho; Max Planck Society
FX Our sincere thanks to the referee for valuable comments and suggestions
that helped to improve the paper. We thank Carlos M. Gutierrez de la
Cruz and Martin Lopez-Corredoira, who obtained the optical and
near-infrared spectra of the quasar and its images, presented in this
paper, during their observations. In this paper, we have extensively
used data from the Sloan Digital Sky Survey (SDSS). 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
Monbuka-gakusho, and the Max Planck Society. The SDSS website is
http://www.sdss.org/. This research has made use of the NASA/IPAC
Extragalactic Database (NED), which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with NASA
of data products from the Two Micron All Sky Survey, VLA/FIRST, NVSS,
and ROSAT/PSPC.
NR 31
TC 4
Z9 4
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2009
VL 692
IS 1
BP 694
EP 701
DI 10.1088/0004-637X/692/1/694
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410CG
UT WOS:000263553000059
ER
PT J
AU Sayers, J
Golwala, SR
Rossinot, P
Ade, PAR
Aguirre, JE
Bock, JJ
Edgington, SF
Glenn, J
Goldin, A
Haig, D
Lange, AE
Laurent, GT
Mauskopf, PD
Nguyen, HT
AF Sayers, J.
Golwala, S. R.
Rossinot, P.
Ade, P. A. R.
Aguirre, J. E.
Bock, J. J.
Edgington, S. F.
Glenn, J.
Goldin, A.
Haig, D.
Lange, A. E.
Laurent, G. T.
Mauskopf, P. D.
Nguyen, H. T.
TI A SEARCH FOR COSMIC MICROWAVE BACKGROUND ANISOTROPIES ON ARCMINUTE
SCALES WITH BOLOCAM (vol 690, pg 1597, 2009)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Sayers, J.; Golwala, S. R.; Rossinot, P.; Edgington, S. F.; Lange, A. E.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Ade, P. A. R.; Haig, D.; Mauskopf, P. D.] Cardiff Univ, Cardiff CF24 3YB, S Glam, Wales.
[Aguirre, J. E.; Glenn, J.; Laurent, G. T.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Aguirre, J. E.; Glenn, J.; Laurent, G. T.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Bock, J. J.; Goldin, A.; Nguyen, H. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sayers, J (reprint author), CALTECH, Div Phys Math & Astron, Mail Code 59-33, Pasadena, CA 91125 USA.
EM jack@caltech.edu
NR 1
TC 0
Z9 0
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2009
VL 692
IS 1
BP 942
EP 942
DI 10.1088/0004-637X/692/1/942
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410CG
UT WOS:000263553000079
ER
PT J
AU Link, J
Col, L
Guida, V
Dow, D
O'Reilly, J
Green, J
Overholtz, W
Palka, D
Legault, C
Vitaliano, J
Griswold, C
Fogarty, M
Friedland, K
AF Link, Jason
Col, Laurel
Guida, Vincent
Dow, David
O'Reilly, John
Green, Jack
Overholtz, William
Palka, Debra
Legault, Chris
Vitaliano, Joseph
Griswold, Carolyn
Fogarty, Michael
Friedland, Kevin
TI Response of balanced network models to large-scale perturbation:
Implications for evaluating the role of small pelagics in the Gulf of
Maine
SO ECOLOGICAL MODELLING
LA English
DT Article
DE Network analysis; Energy budget; Food web; Trophodynamics; Ecosystem
approaches to fisheries management; Tradeoffs
ID NORTHERN BENGUELA ECOSYSTEM; HERRING CLUPEA-HARENGUS; GEORGES-BANK;
ZOOPLANKTON ABUNDANCE; MANAGEMENT; FISHERY; COLLAPSE; ECOPATH; SEA;
GROUNDFISH
AB Exploring the response of an ecosystem, and subsequent tradeoffs among its biological community, to human perturbations remains a key challenge for the implementation of an ecosystem approaches to fisheries (EAF). To address this and related issues, we developed two network (or energy budget) models, Ecopath and Econetwrk, for the Gulf of Maine ecosystem. These models included 31 network "nodes" or biomass state variables across a broad range of trophic levels, with the present emphasis to particularly elucidate the role of small pelagics. After initial network balancing, various perturbation scenarios were evaluated to explore how potential changes to different fish, fisheries and lower trophic levels can affect model outputs. Categorically across all scenarios and interpretations thereof, there was minimal change at the second trophic levels and most of the "rebalancing" after a perturbation occur-red via alteration of the diet matrix. Yet the model results from perturbations to a balanced energy budget fall into one of three categories. First, some model results were intuitive and in obvious agreement with established ecological and fishing theory. Second, some model results were counter-intuitive upon initial observation, seemingly contradictory to known ecological and fishing theory; but upon further examination the results were explainable given the constraints of an equilibrium energy budget. Finally, some results were counter-intuitive and difficult to reconcile with theory or further examination of equilibrium constraints. A detailed accounting of biomass flows for example scenarios explores some of the non-intuitive results more rigorously. Collectively these results imply a need to carefully track biomass flows and results of any given perturbation and to critically evaluate the conditions under which a new equilibrium is obtained for these types of models, which has implications for dynamic simulations based off of them. Given these caveats, the role of small pelagics as a prominent component of this ecosystem remains a robust conclusion. We discuss how one might use this approach in the context of further developing an EAF, recognizing that a more holistic, integrated perspective will be required as we continue to evaluate tradeoffs among marine biological communities. Published by Elsevier B.V.
C1 [Link, Jason; Col, Laurel; Dow, David; Overholtz, William; Palka, Debra; Legault, Chris; Fogarty, Michael] Woods Hole Lab, NE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Woods Hole, MA 02543 USA.
[O'Reilly, John; Green, Jack; Griswold, Carolyn; Friedland, Kevin] Narragansett Lab, NE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Narragansett, RI 02882 USA.
[Guida, Vincent; Vitaliano, Joseph] James J Howard Marine Sci Lab, NE Fisheries Sci Ctr, Natl Marine Fisheries Serv, Highlands, NJ 07732 USA.
RP Link, J (reprint author), Woods Hole Lab, NE Fisheries Sci Ctr, Natl Marine Fisheries Serv, 166 Water St, Woods Hole, MA 02543 USA.
EM jlink@mercury.wh.whoi.edu
NR 43
TC 15
Z9 15
U1 2
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-3800
J9 ECOL MODEL
JI Ecol. Model.
PD FEB 10
PY 2009
VL 220
IS 3
BP 351
EP 369
DI 10.1016/j.ecolmodel.2008.10.009
PG 19
WC Ecology
SC Environmental Sciences & Ecology
GA 405FX
UT WOS:000263209400008
ER
PT J
AU Sexton, JO
Bax, T
Siqueira, P
Swenson, JJ
Hensley, S
AF Sexton, Joseph O.
Bax, Tyler
Siqueira, Paul
Swenson, Jennifer J.
Hensley, Scott
TI A comparison of lidar, radar, and field measurements of canopy height in
pine and hardwood forests of southeastern North America
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE Forest structure; Canopy height; Radar interferometry; InSAR; Lidar;
GeoSAR; SRTM
ID BAND SRTM DEM; C-BAND; TOPOGRAPHY MISSION; SHUTTLE RADAR; SAR
INTERFEROMETRY; CARBON ESTIMATION; TREE HEIGHT; VEGETATION; BIOMASS;
MODEL
AB Forest canopy height is essential information for many forest management activities and is a critical parameter in models of ecosystem processes. Several methods are available to measure canopy height from single-tree to regional and global scales, but the methods vary widely in their sensitivities, leading to different height estimates even for identical stands. We compare four technologies for estimating canopy height in pine and hardwood forests of the Piedmont region of North Carolina, USA: (1) digital elevation data from the global Shuttle Radar Topography Mission (SRTM) C-band radar interferometry, (2) X- and P-band radar interferometry from the recently developed airborne Geographic Synthetic Aperture Radar (GeoSAR) sensor, (3) small footprint lidar measurements (in pine only), and (4) field measurements acquired by in situ forest mensuration. Differences between measurements were smaller in pine than in hardwood forests, with biases ranging from 5.13 to 12.17 m in pine (1.60-13.77 m for lidar) compared to 6.60-15.28 m in hardwoods and RMSE from 8.40 to 14.21 m in pine (4.73-14.92 m for lidar) compared to 9.54-16.84 in hardwood. GeoSAR measurements of canopy height were among the most comparable measurements overall and showed potential for successful calibration, with R(2) = 0.87 in pine canopies and R(2) = 0.38 in hardwood canopies from simple linear regression. An improved calibration based on differential canopy penetration is presented and applied to SRTM measurements, resulting in canopy height estimates in pine forests with RMSE and standard error <4.00 m. Each of the remotely sensed methods studied produces reasonable and consistent depictions of canopy height that can be compared with data of similar provenance, but due to differences in underlying sensitivities between the methods, comparisons between measurements from various sources require cross-calibration and will be most useful at broad scales. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Sexton, Joseph O.; Bax, Tyler; Swenson, Jennifer J.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Siqueira, Paul] Univ Massachusetts, Dept Elect & Comp Engn, Microwave Remote Sensing Lab, Amherst, MA 01003 USA.
[Hensley, Scott] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sexton, JO (reprint author), Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
EM joseph.sexton@duke.edu; tyler.bax@duke.edu
RI Siqueira, Paul/D-9760-2016;
OI Siqueira, Paul/0000-0001-5781-8282; Swenson,
Jennifer/0000-0002-2069-667X
FU NASA
FX Lidar data were provided by the North Carolina Floodplain Mapping
Program. Forest inventory measurements were provided by the Office of
the Duke Forest, Duke University. John Kerkering performed and reported
analyses of a pilot study, and John P. Fay assisted lidar data
processing. Analyses were performed in the Duke University Landscape
Ecology Laboratory, with technical assistance from Dean Urban, Ben Best
and Ibrahim Alameddine. This research was supported by a NASA Earth
System Science Fellowship, "Suburban forest dynamics: fusing remote
sensing and ecological models" (J.O. Sexton, 2005-2008). Two anonymous
reviewers provided suggestions that improved the manusctript greatly.
NR 47
TC 53
Z9 53
U1 1
U2 25
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD FEB 10
PY 2009
VL 257
IS 3
BP 1136
EP 1147
DI 10.1016/j.foreco.2008.11.022
PG 12
WC Forestry
SC Forestry
GA 405IE
UT WOS:000263215700042
ER
PT J
AU Schuster, GL
Lin, B
Dubovik, O
AF Schuster, Gregory L.
Lin, Bing
Dubovik, Oleg
TI Remote sensing of aerosol water uptake
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SKY RADIANCE MEASUREMENTS; OPTICAL-PROPERTIES; ATMOSPHERIC AEROSOL;
RELATIVE-HUMIDITY; LIGHT-SCATTERING; REFRACTIVE-INDEX; PARTICLES;
ABSORPTION; VISIBILITY; RETRIEVAL
AB Aerosol water content is an important component of aerosol radiative forcing, but the effect of water uptake on aerosols throughout the atmospheric column is not monitored at the present time. We present a technique for retrieving the volume fraction of water in atmospheric aerosols, and apply the technique to the AERONET database. We estimate that the volume fraction of water and the geometric hygroscopic growth factor (gHGF) can be retrieved to within 0.3 using this retrieval. The growth factors we obtain are consistent with published measurements, and indicate that aerosol water uptake is high in humid continental regions (gHGF similar to 1.3 along the U. S. East Coast in August) and low in regions dominated by desert dust (gHGF similar to 1.04 in Saudi Arabia). Citation: Schuster, G. L., B. Lin, and O. Dubovik (2009), Remote sensing of aerosol water uptake, Geophys. Res. Lett., 36, L03814, doi: 10.1029/2008GL036576.
C1 [Schuster, Gregory L.; Lin, Bing] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Dubovik, Oleg] Univ Lille 1, Opt Atmospher Lab, CNRS, F-59655 Villeneuve Dascq, France.
RP Schuster, GL (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM gregory.l.schuster@nasa.gov
RI Dubovik, Oleg/A-8235-2009
OI Dubovik, Oleg/0000-0003-3482-6460
FU NASA
FX We appreciate the efforts of the 53 AERONET and PHOTONS (Service
d'Observation from LOA/USTL/CNRS) principal investigators and the entire
AERONET/PHOTONS teams. Relative humidity data are funded by the NASA
Earth Observing System project at the COVE site and by NOAA Global
Monitoring Division for the Bondville and Boulder sites. This work was
funded by NASA SMD/ESD and the CERES project.
NR 25
TC 22
Z9 24
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 FEB 10
PY 2009
VL 36
AR L03814
DI 10.1029/2008GL036576
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 406XM
UT WOS:000263328200006
ER
PT J
AU Martin, PJ
Book, JW
Burrage, DM
Rowley, CD
Tudor, M
AF Martin, P. J.
Book, J. W.
Burrage, D. M.
Rowley, C. D.
Tudor, M.
TI Comparison of model-simulated and observed currents in the central
Adriatic during DART
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SEA GENERAL-CIRCULATION; COASTAL OCEAN MODEL; WINTER; WATER
AB Numerical simulations of the Adriatic Sea were performed with the Navy Coastal Ocean Model (NCOM) during the Dynamics of the Adriatic in Real Time (DART) Experiments conducted between October 2005 and September 2006. Grid resolution was 1 km. Model forcing included tides, surface fluxes from the Aire Limitee Adaptation Dynamique Developpement International (ALADIN) atmospheric model, relaxation to a daily satellite sea surface temperature analysis, extensive river and runoff discharges, and open boundary conditions south of Otranto specified from a global model. Currents predicted by the model were compared with currents from 12 Acoustic Doppler Current Profiler (ADCP) moorings located along a line between the Gargano Peninsula, Italy, and Split, Croatia. The nontidal comparisons were performed with detided currents. Correlations between the model and ADCP currents were highest in the Western Adriatic Current (WAC), which flows southeastward along the Italian coast. Lowest correlations were in the interior of the Adriatic, likely because of instability processes. Correlations between the ALADIN winds and the model and ADCP currents at the mooring locations were also highest in the WAC. For November 2005 through August 2006, the model and ADCP mean WAC transports were 0.321 and 0.304 Sv, respectively, with a temporal correlation of 0.79. Comparison of current variance showed best agreement near the Italian and Croatian coasts. In the interior, the NCOM current variance compared fairly well with that of the ADCPs for November-January but decreased significantly relative to the ADCPs for February-August. Spectral analyses indicate most of the difference in variance to be at periods exceeding 2 days.
C1 [Martin, P. J.; Rowley, C. D.] USN, Stennis Space Ctr, Res Lab, Ocean Dynam & Predict Branch,Oceanog Div, Stennis Space Ctr, MS 39529 USA.
[Tudor, M.] Croatian Meteorol & Hydrol Serv, HR-10000 Zagreb, Croatia.
RP Martin, PJ (reprint author), USN, Stennis Space Ctr, Res Lab, Ocean Dynam & Predict Branch,Oceanog Div, Stennis Space Ctr, MS 39529 USA.
EM paul.martin@nrlssc.navy.mil; book@nrlssc.navy.mil;
derek.burrage@nrlssc.navy.mil; clark.rowley@nrlssc.navy.mil;
tudor@cirus.dhz.hr
OI Rowley, Clark/0000-0003-3496-6404; Tudor, Martina/0000-0002-2683-2652
FU Office of Naval Research; "Global Remote Littoral Forcing via Deep Water
Pathways'' research programs [0602435N, 0601153N];
[NRL/JA/7320-08-8149]
FX Thanks to the captains, crews, and scientists of the R/V G. Dallaporta,
R/V Alliance, and R/V Universitatis for the successful deployments and
recoveries of all the moorings. The success of the mooring effort was in
large part due to the dedicated efforts of Mark Hulbert, Andrew Quaid,
and Wesley Goode of the NRL technical team. We thank Elio Pachini of
CNR-ISMAR-Ancona and Giuseppe Siena of CoNISMa for their respective help
during the first deployment and final recovery cruises. Also, thanks to
Elio Pachini, Mira Morovic, Mirko Orlic, Gordana Beg Paklar, Aniello
Russo, and Sandro Carniel for their help with cruise logistics and
planning. Michel Rixen of the NATO Undersea Research Centre (NURC) led
and organized the larger international DART collaborative project and
contributed in many ways to this work. The NRL DART project greatly
benefited from being part of a NURC/NRL Joint Research Project and from
the larger collaborative effort. Thanks to the reviewers for their
useful suggestions. This work was supported by the Office of Naval
Research as part of the "Dynamics of the Adriatic in RealTime'' and
"Global Remote Littoral Forcing via Deep Water Pathways'' research
programs (Program Elements 0602435N and 0601153N, respectively). This is
NRL contribution NRL/JA/7320-08-8149.
NR 46
TC 17
Z9 17
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-OCEANS
JI J. Geophys. Res.-Oceans
PD FEB 10
PY 2009
VL 114
AR C01S05
DI 10.1029/2008JC004842
PG 18
WC Oceanography
SC Oceanography
GA 406YG
UT WOS:000263330200001
ER
PT J
AU Meyer-Vernet, N
Lecacheux, A
Kaiser, ML
Gurnett, DA
AF Meyer-Vernet, N.
Lecacheux, A.
Kaiser, M. L.
Gurnett, D. A.
TI Detecting nanoparticles at radio frequencies: Jovian dust stream impacts
on Cassini/RPWS
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID JUPITERS MAGNETOSPHERE; THERMAL NOISE; PLASMA; IONIZATION; VOYAGER-2;
SATURN; RING; IO
AB We analyse wave observations by the Cassini/RPWS instrument performed during the Jovian fly-by, when the on-board dust analyser recorded dust streams which were interpreted as nanoparticles moving at about the solar wind speed. The observed wave pulses are produced by ionisation of dust grains impacting the spacecraft. Nanoparticles are detected because they move fast and the voltage produced by impact ionisation increases very fast with speed, so that they produce wave pulses as high as do much larger grains of smaller speeds. The observed wave level and spectral shape are compatible with those expected for the streams deduced from the dust analyser observations, and the impact rates observed on both instruments appear to vary similarly. The present result is the first wave detection simultaneous with a conventional detection by a dust analyser attributed to nanoparticles. Citation: Meyer-Vernet, N., A. Lecacheux, M. L. Kaiser, and D. A. Gurnett (2009), Detecting nanoparticles at radio frequencies: Jovian dust stream impacts on Cassini/RPWS, Geophys. Res. Lett., 36, L03103, doi:10.1029/2008GL036752.
C1 [Meyer-Vernet, N.; Lecacheux, A.] Univ Paris Diderot, CNRS, LESIA, Observ Paris, F-92190 Meudon, France.
[Kaiser, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gurnett, D. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
RP Meyer-Vernet, N (reprint author), Univ Paris Diderot, CNRS, LESIA, Observ Paris, 5 Pl Jules Janssen, F-92190 Meudon, France.
EM nicole.meyer@obspm.fr
FU Centre National d'Etudes Spatiales
FX We acknowledge support by the Centre National d'Etudes Spatiales.
NR 24
TC 29
Z9 29
U1 0
U2 3
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 7
PY 2009
VL 36
AR L03103
DI 10.1029/2008GL036752
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 404TA
UT WOS:000263174700005
ER
PT J
AU Oman, L
Waugh, DW
Pawson, S
Stolarski, RS
Newman, PA
AF Oman, Luke
Waugh, Darryn W.
Pawson, Steven
Stolarski, Richard S.
Newman, Paul A.
TI On the influence of anthropogenic forcings on changes in the
stratospheric mean age
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID BREWER-DOBSON CIRCULATION; CLIMATE MODEL SIMULATIONS; SEA-SURFACE
TEMPERATURE; AIR; TROPOSPHERE; TRANSPORT; OZONE
AB A common feature of stratospheric simulations of the past or future is an increase in tropical upwelling and a decrease in mean age. Possible causes of these changes include ( 1) increases in tropical sea surface temperatures (SSTs) driven by increases in well-mixed greenhouse gases (WMGHGs), ( 2) the direct radiative effect of increases in WMGHGs, and ( 3) changes in ozone. Here we examine a suite of simulations from the Goddard Earth Observing System chemistry-climate model (GEOS CCM) to isolate the relative role of these three factors. Our analysis indicates that all three factors cause changes in the mean age, but the relative impact of each factor depends on the time period analyzed. Over the past 30-40 years ozone depletion is the major factor causing the decrease in mean age, with negligible changes due to direct radiative impact of WMGHGs. However, ozone is predicted to recover back to 1970 levels during the next 50-60 years, and this causes an increase in the mean age, whereas the continued increase in SSTs from increased levels of WMGHGs and the direct radiative impact of WMGHGs will still cause a decrease in the mean age. The net impact of these factors will still result in a decreasing mean age although the rate will be smaller than that of the past. The decreases in mean age are primarily caused by increases in upwelling in the tropical lower stratosphere. The increased upwelling from both increased tropical SSTs and polar ozone loss appears to be related to changes in zonal winds and increases in wave activity propagating into the stratosphere. The different contributions of changes in SSTs, WMGHGs, and ozone to the circulation of the stratosphere may help explain the large spread in the rate of change of tropical upwelling seen in previous studies.
C1 [Oman, Luke; Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Stolarski, Richard S.; Newman, Paul A.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA.
RP Oman, L (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, 301 Olin Bldg,3400 N Charles St, Baltimore, MD 21218 USA.
EM oman@jhu.edu
RI Oman, Luke/C-2778-2009; Newman, Paul/D-6208-2012; Stolarski,
Richard/B-8499-2013; Pawson, Steven/I-1865-2014; Waugh,
Darryn/K-3688-2016
OI Oman, Luke/0000-0002-5487-2598; Newman, Paul/0000-0003-1139-2508;
Stolarski, Richard/0000-0001-8722-4012; Pawson,
Steven/0000-0003-0200-717X; Waugh, Darryn/0000-0001-7692-2798
NR 29
TC 49
Z9 49
U1 0
U2 10
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 7
PY 2009
VL 114
AR D03105
DI 10.1029/2008JD010378
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 404TJ
UT WOS:000263175600001
ER
PT J
AU Winick, JR
Wintersteiner, PP
Picard, RH
Esplin, D
Mlynczak, MG
Russell, JM
Gordley, LL
AF Winick, J. R.
Wintersteiner, P. P.
Picard, R. H.
Esplin, D.
Mlynczak, M. G.
Russell, J. M., III
Gordley, L. L.
TI OH layer characteristics during unusual boreal winters of 2004 and 2006
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID WIND IMAGING INTERFEROMETER; ROCKET MEASUREMENTS; CIRCULATION;
ATMOSPHERE; NIGHTGLOW; ALOHA-93; AIRGLOW
AB We report observations of unusual mesospheric OH airglow made by the SABER instrument on the TIMED satellite. During portions of the boreal winters of 2004 and 2006, and over much of the region poleward of 60 degrees N, the OH layer was similar to 5-8 km lower than normal and twice as bright. Using retrieved volume emission rates (VERs) in two SABER channels, we document the characteristics, spatial extent, and temporal variability of the anomalous behavior. We show that it is correlated with unusual mesospheric and upper stratospheric temperature patterns that have been reported, and other observations. The unusual layer properties are likely produced by enhanced downward transport of atomic oxygen, a circumstance consistent with the planetary wave dynamics thought to be responsible for the other changes. These observations raise the possibility of using easily observed OH airglow as a proxy for perturbed meteorological conditions.
C1 [Winick, J. R.] RVBYM, AF Res Lab, Hanscom AFB, MA 01730 USA.
[Wintersteiner, P. P.] Arcon Corp, Waltham, MA USA.
[Esplin, D.] Utah State Univ, Dept Elect & Comp Engn, Logan, UT 84322 USA.
[Mlynczak, M. G.] NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23665 USA.
[Russell, J. M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Gordley, L. L.] Gordley Analyt & Tech Software, Newport News, VA USA.
RP Winick, JR (reprint author), RVBYM, AF Res Lab, 29 Randolph Rd, Hanscom AFB, MA 01730 USA.
EM AFRL.RVB.PA@hanscom.af.mil
RI Mlynczak, Martin/K-3396-2012
FU Air Force Office of Scientific Research; NASA TIMED; NASA HQ Space
FX This work was supported by the Air Force Office of Scientific Research (
Kent Miller, Program Manager) and by the NASA TIMED mission under the
SABER project. D. E. also acknowledges support from NASA HQ Space Grant.
J. R. W. wishes to thank Doran Baker of Utah State University for
supporting D. E. under the NASA Space Grant program.
NR 32
TC 33
Z9 33
U1 0
U2 0
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 7
PY 2009
VL 114
AR A02303
DI 10.1029/2008JA013688
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 404UX
UT WOS:000263179600002
ER
PT J
AU Koren, I
Remer, LA
Longo, K
Brown, F
Lindsey, R
AF Koren, Ilan
Remer, Lorraine A.
Longo, Karla
Brown, Foster
Lindsey, Rebecca
TI Reply to comment by W. Schroeder et al. on "Reversal of trend of biomass
burning in the Amazon''
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Editorial Material
ID DEFORESTATION
C1 [Koren, Ilan] Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel.
[Brown, Foster] Univ Fed Acre, BR-69915900 Rio Branco, Acre, Brazil.
[Lindsey, Rebecca] NASA, Earth Observ, Lanham, MD 20706 USA.
[Longo, Karla] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Remer, Lorraine A.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613 2, Greenbelt, MD 20771 USA.
[Brown, Foster] Woods Hole Res Ctr, Falmouth, MA USA.
RP Koren, I (reprint author), Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel.
EM ilan.koren@weizmann.ac.il; Lorraine.A.Remer@nasa.gov;
karla.longo@dge.inpe.br; fbrown@uol.com.br; eoeditor@yahoo.com
RI Koren, Ilan/K-1417-2012
OI Koren, Ilan/0000-0001-6759-6265
NR 9
TC 3
Z9 3
U1 0
U2 3
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 6
PY 2009
VL 36
AR L03807
DI 10.1029/2008GL036063
PG 3
WC Geosciences, Multidisciplinary
SC Geology
GA 404SY
UT WOS:000263174500002
ER
PT J
AU McKay, CP
AF McKay, Christopher P.
TI PLANETARY SCIENCE Biologically Reversible Exploration
SO SCIENCE
LA English
DT Editorial Material
ID MARS; EARTH
C1 [McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP McKay, CP (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM christopher.mckay@nasa.gov
NR 12
TC 7
Z9 8
U1 0
U2 1
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 6
PY 2009
VL 323
IS 5915
BP 718
EP 718
DI 10.1126/science.1167987
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 403EV
UT WOS:000263066800024
PM 19197043
ER
PT J
AU Waugh, DW
Oman, L
Kawa, SR
Stolarski, RS
Pawson, S
Douglass, AR
Newman, PA
Nielsen, JE
AF Waugh, D. W.
Oman, L.
Kawa, S. R.
Stolarski, R. S.
Pawson, S.
Douglass, A. R.
Newman, P. A.
Nielsen, J. E.
TI Impacts of climate change on stratospheric ozone recovery
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GREENHOUSE GASES; MODEL SIMULATIONS; CARBON-DIOXIDE; WATER-VAPOR;
TEMPERATURE; DEPLETION; AIR
AB The impact of increasing greenhouse gases (GHGs) on the ``recovery'' of stratospheric ozone is examined using simulations of the Goddard Earth Observing System Chemistry-Climate Model. In this model, GHG-induced climate change has a large impact on the ozone evolution and when O-3 recovery milestones are reached. The two distinct milestones of "O-3 returning to historical values'' and "O-3 being no longer significantly influenced by ozone depleting substances (ODSs)'' can be reached at very different dates, and which occurs first varies between regions. GHG-induced cooling in the upper stratosphere causes O-3 to increase, and O-3 returns to 1980 or 1960 values several decades before O-3 is no longer significantly influenced by ODSs. In contrast, transport changes in the tropical and southern mid-latitude lower stratosphere cause O-3 to decrease. Here O-3 never returns to 1980 values, even when anthropogenic ODSs have been removed from the atmosphere. O-3 returning to 1960 ( or 1980) values should not necessarily be interpreted as O-3 recovery from the effects of ODSs. Citation: Waugh, D. W., L. Oman, S. R. Kawa, R. S. Stolarski, S. Pawson, A. R. Douglass, P. A. Newman, and J. E. Nielsen ( 2009), Impacts of climate change on stratospheric ozone recovery, Geophys. Res. Lett., 36, L03805, doi: 10.1029/2008GL036223.
C1 [Waugh, D. W.; Oman, L.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Nielsen, J. E.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Kawa, S. R.; Stolarski, R. S.; Pawson, S.; Douglass, A. R.; Newman, P. A.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA.
RP Waugh, DW (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, 329 Olin Hall,3400 N Charles St, Baltimore, MD 21218 USA.
EM waugh@jhu.edu
RI Oman, Luke/C-2778-2009; Newman, Paul/D-6208-2012; Douglass,
Anne/D-4655-2012; Kawa, Stephan/E-9040-2012; Stolarski,
Richard/B-8499-2013; Pawson, Steven/I-1865-2014; Waugh,
Darryn/K-3688-2016
OI Oman, Luke/0000-0002-5487-2598; Newman, Paul/0000-0003-1139-2508;
Stolarski, Richard/0000-0001-8722-4012; Pawson,
Steven/0000-0003-0200-717X; Waugh, Darryn/0000-0001-7692-2798
FU NASA MAP; NSF Large-scale Climate Dynamics programs
FX We thank David Fahey for very helpful comments on the manuscript. This
research was supported by the NASA MAP and NSF Large-scale Climate
Dynamics programs. Computational resources were provided through NASA's
High-End Computing program.
NR 24
TC 63
Z9 65
U1 2
U2 18
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 5
PY 2009
VL 36
AR L03805
DI 10.1029/2008GL036223
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 404SV
UT WOS:000263174200003
ER
PT J
AU Yang, K
Krotkov, NA
Krueger, AJ
Carn, SA
Bhartia, PK
Levelt, PF
AF Yang, Kai
Krotkov, Nickolay A.
Krueger, Arlin J.
Carn, Simon A.
Bhartia, Pawan K.
Levelt, Pieternel F.
TI Improving retrieval of volcanic sulfur dioxide from backscattered UV
satellite observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; ROTATIONAL RAMAN-SCATTERING; OBJECTIVES;
ALGORITHM; ERUPTION; OMI
AB Existing algorithms that use satellite measurements of solar backscattered ultraviolet (BUV) radiances to retrieve sulfur dioxide (SO(2)) vertical columns underestimate the large SO(2) amounts encountered in fresh volcanic eruption clouds. To eliminate this underestimation we have developed a new technique, named the Iterative Spectral Fitting (ISF) algorithm, for accurate retrieval of SO2 vertical columns in the full range of volcanic emissions. The ISF algorithm is applied to Ozone Monitoring Instrument (OMI) BUV measurements of the Sierra Negra eruption (Galapagos Islands, Ecuador) in October 2005. The results represent major improvements over the operational OMI SO(2) products. Based on the ISF data, we report the largest SO(2) vertical column amount (> 1000 Dobson Units (DU), where 1 DU = 2.69 x 10(16) molecules/cm(2)) ever observed by a space borne instrument, implying that very high concentrations of SO2 can occur in the lower troposphere during effusive eruptions. Citation: Yang, K., N. A. Krotkov, A. J. Krueger, S. A. Carn, P. K. Bhartia, and P. F. Levelt (2009), Improving retrieval of volcanic sulfur dioxide from backscattered UV satellite observations, Geophys. Res. Lett., 36, L03102, doi: 10.1029/2008GL036036.
C1 [Yang, Kai; Krotkov, Nickolay A.; Bhartia, Pawan K.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Krueger, Arlin J.; Carn, Simon A.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Levelt, Pieternel F.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
[Yang, Kai; Krotkov, Nickolay A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Yang, K (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Mail Code 613-3, Greenbelt, MD 20771 USA.
EM kai.yang-1@nasa.gov
RI Krotkov, Nickolay/E-1541-2012; Bhartia, Pawan/A-4209-2016
OI Krotkov, Nickolay/0000-0001-6170-6750; Bhartia,
Pawan/0000-0001-8307-9137
FU NASA [NNS06AA05G]; U.S. OMI Science Team
FX This work was supported in part by NASA under grant NNS06AA05G (NASA
volcanic cloud data for aviation hazards) and by the U.S. OMI Science
Team.
NR 23
TC 28
Z9 29
U1 1
U2 13
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 4
PY 2009
VL 36
AR L03102
DI 10.1029/2008GL036036
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 404ST
UT WOS:000263174000002
ER
PT J
AU Haynes, JM
L'Ecuyer, TS
Stephens, GL
Miller, SD
Mitrescu, C
Wood, NB
Tanelli, S
AF Haynes, John M.
L'Ecuyer, Tristan S.
Stephens, Graeme L.
Miller, Steven D.
Mitrescu, Cristian
Wood, Norman B.
Tanelli, Simone
TI Rainfall retrieval over the ocean with spaceborne W-band radar
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MICROWAVE BRIGHTNESS TEMPERATURES; RADIATIVE-TRANSFER EQUATION;
MONTE-CARLO INTEGRATION; MILLIMETER-WAVE RADAR; MELTING-LAYER; SIZE
DISTRIBUTIONS; PRECIPITATION; MODEL; SCATTERING; ALGORITHM
AB A method for retrieving precipitation over the ocean using spaceborne W-band (94 GHz) radar is introduced and applied to the CloudSat Cloud Profiling Radar. The method is most applicable to stratiform-type precipitation. Measurements of radar backscatter from the ocean surface are combined with information about surface wind speed and sea surface temperature to derive the path-integrated attenuation through precipitating cloud systems. The scattering and extinction characteristics of raindrops are modeled using a combination of Mie theory (for raindrops) and the discrete dipole approximation (for ice crystals and melting snow), and a model of the melting layer is implemented to represent the transition between ice and liquid water. Backward Monte Carlo modeling is used to model multiple scattering from precipitating hydrometeors between the radar and ocean surface, which is shown to be significant for precipitation rates exceeding 3-5 mm h(-1), particularly when precipitating ice is present. An uncertainty analysis is presented and the algorithm is applied to near-global CloudSat observations and compared with other near-global precipitation sources. In the tropics, CloudSat tends to underestimate the heaviest precipitation. It is found that in the middle latitudes, however, CloudSat observes precipitation more often and with greater resulting accumulation than other spaceborne sensors.
C1 [Haynes, John M.; L'Ecuyer, Tristan S.; Stephens, Graeme L.; Wood, Norman B.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Miller, Steven D.] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Mitrescu, Cristian] USN, Res Lab, Monterey, CA 93943 USA.
[Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Haynes, JM (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
EM haynes@atmos.colostate.edu; tristan@atmos.colostate.edu;
stephens@atmos.colostate.edu; miller@cira.colostate.edu;
norm@atmos.colostate.edu; simone.tanelli@jpl.nasa.gov
RI L'Ecuyer, Tristan/C-7040-2013; L'Ecuyer, Tristan/E-5607-2012
OI L'Ecuyer, Tristan/0000-0002-7584-4836
FU NASA [NNX07AR97G]; Jet Propulsion Laboratory, California Institute of
technology; National Aeronautics and Space Administration
FX This study was supported partially by NASA grant NNX07AR97G. We wish to
thank Denis O' Brien of Colorado State University for providing the
backward Monte Carlo model used in this study and for his assistance
adapting it for use in the CloudSat configuration. Simone Tanelli's
contribution was performed at the Jet Propulsion Laboratory, California
Institute of technology, under contract with the National Aeronautics
and Space Administration.
NR 45
TC 120
Z9 121
U1 0
U2 23
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 2009
VL 114
AR D00A22
DI 10.1029/2008JD009973
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 404TE
UT WOS:000263175100001
ER
PT J
AU Hegglin, MI
Boone, CD
Manney, GL
Walker, KA
AF Hegglin, M. I.
Boone, C. D.
Manney, G. L.
Walker, K. A.
TI A global view of the extratropical tropopause transition layer from
Atmospheric Chemistry Experiment Fourier Transform Spectrometer O-3,
H2O, and CO
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LOWERMOST STRATOSPHERE; MIDDLE ATMOSPHERE; UPPER TROPOSPHERE; TRANSPORT;
SPURT; CLIMATOLOGY; VALIDATION; AIRBORNE; EXCHANGE; OZONE
AB The global behavior of the extratropical tropopause transition layer (ExTL) is investigated using O-3, H2O, and CO measurements from the Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS) on Canada's SCISAT-1 satellite obtained between February 2004 and May 2007. The ExTL depth is derived using H2O-O-3 and CO-O-3 correlations. The ExTL top derived from H2O-O-3 shows an increase from roughly 1-1.5 km above the thermal tropopause in the subtropics to 3-4 km (2.5-3.5 km) in the north (south) polar region, implying somewhat weaker troposphere-stratosphere-transport in the Southern Hemisphere. The ExTL bottom extends similar to 1 km below the thermal tropopause, indicating a persistent stratospheric influence on the troposphere at all latitudes. The ExTL top derived from the CO-O-3 correlation is lower, at 2 km or similar to 345 K (1.5 km or similar to 335 K) in the Northern (Southern) Hemisphere. Its annual mean coincides with the relative temperature maximum just above the thermal tropopause. The vertical CO gradient maximizes at the thermal tropopause, indicating a local minimum in mixing within the tropopause region. The seasonal changes in and the scales of the vertical H2O gradients show a similar pattern as the static stability structure of the tropopause inversion layer (TIL), which provides observational support for the hypothesis that H2O plays a radiative role in forcing and maintaining the structure of the TIL.
C1 [Hegglin, M. I.; Walker, K. A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Boone, C. D.; Walker, K. A.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Manney, G. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Manney, G. L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
RP Hegglin, MI (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada.
EM michaela@atmosp.physics.utoronto.ca; cboone@acebox.uwaterloo.ca;
Gloria.L.Manney@jpl.nasa.gov; kwalker@atmosp.physics.utoronto.ca
RI Hegglin, Michaela/D-7528-2017
OI Hegglin, Michaela/0000-0003-2820-9044
FU Canadian Space Agency (CSA); Canadian Foundation for Climate and
Atmospheric Sciences; CSA through the C-SPARC network; National
Aeronautics and Space Administration
FX ACE is funded primarily by the Canadian Space Agency (CSA). We thank the
CSA for access to the data. This research has been supported by the
Canadian Foundation for Climate and Atmospheric Sciences and the CSA
through the C-SPARC network. Many thanks go to Bill Randel and Fei Wu
for providing the GPS data, and to William Daffer for his work in
providing the derived meteorological products. Work at the Jet
Propulsion Laboratory, California Institute of Technology, was done
under contract with the National Aeronautics and Space Administration.
Thanks go to Ted Shepherd for assistance with Appendix A, and to Matt
Hitchman and Peter Hoor for helpful comments on an earlier version of
the manuscript.
NR 52
TC 65
Z9 65
U1 0
U2 19
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 4
PY 2009
VL 114
AR D00B11
DI 10.1029/2008JD009984
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 404TE
UT WOS:000263175100002
ER
PT J
AU Pumphrey, HC
Cofield, RE
Filipiak, MJ
Livesey, NJ
AF Pumphrey, Hugh C.
Cofield, Richard E.
Filipiak, Mark J.
Livesey, Nathaniel J.
TI An all-sky survey at 230 GHz by MLS on Aura
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Galaxy; CO; Radio-astronomy; MLS; Limb-sounding; Stratosphere
ID MILKY-WAY; CO SURVEY; SATELLITE
AB The Microwave Limb Sounder (MLS) instrument is a small satellite-borne radio telescope. Its purpose is to make limb-scanning measurements of atmospheric composition. One of the gases to which it is sensitive is carbon monoxide (CO), detected via the J = 2 -> 1 rotational transition at 230 GHz. CO is present in molecular gas clouds in the Milky Way. Although it was not designed for the purpose, MLS can detect emissions from galactic CO, allowing a map of the 230 GHz radio sky to be constructed. We report the MLS measurements of galactic radio emission and discuss their effect on the atmospheric mission of MLS. The region of the Milky Way with emissions strong enough to significantly affect MLS observations of atmospheric CO is identified. Ground-based radio astronomers have been mapping the sky using CO emission for many years. However, the MLS data are the first such survey to be carried out from space. The MLS survey covers a larger area of the sky than any other 230 GHz survey, but no previously unknown gas clouds are observed. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Pumphrey, Hugh C.; Filipiak, Mark J.] Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JN, Midlothian, Scotland.
[Cofield, Richard E.; Livesey, Nathaniel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pumphrey, HC (reprint author), Univ Edinburgh, Sch Geosci, W Mains Rd, Edinburgh EH9 3JN, Midlothian, Scotland.
EM H.C.Pumphrey@ed.ac.uk; Richard.E.Cofield@jpl.nasa.gov;
M.J.Filipiak@ed.ac.uk; Nathaniel.J.Livesey@jpl.nasa.gov
NR 7
TC 4
Z9 4
U1 0
U2 0
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD FEB 2
PY 2009
VL 43
IS 3
BP 342
EP 348
DI 10.1016/j.asr.2008.11.010
PG 7
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 407TX
UT WOS:000263388300002
ER
PT J
AU Oswald, TH
Macher, W
Rucker, HO
Fischer, G
Taubenschuss, U
Bougeret, JL
Lecacheux, A
Kaiser, ML
Goetz, K
AF Oswald, T. H.
Macher, W.
Rucker, H. O.
Fischer, G.
Taubenschuss, U.
Bougeret, J. L.
Lecacheux, A.
Kaiser, M. L.
Goetz, K.
TI Various methods of calibration of the STEREO/WAVES antennas
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE STEREO; S/WAVES; Antennas; Antenna calibration; Solar radio waves
ID RHEOMETRY
AB On October 25th, 2006, NASA's two STEREO spacecraft were launched which are designed to increase our knowledge of the physics of the solar system. On board they carry a sophisticated radio experiment, called S/WAVES. The key technology, used by S/WAVES is the direction finding capability in addition to the use of two spacecraft which makes it possible to triangulate radio sources. Direction finding requires the reception properties of the antennas to be known very accurately. We applied several different methods to calibrate the S/WAVES antennas. In this paper the methods are described and compared and the results are presented and discussed with respect to advantages and disadvantages of the different methods. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Oswald, T. H.; Macher, W.; Rucker, H. O.; Taubenschuss, U.] Austrian Acad Sci, Space Res Inst, Dept Near Earth Space Phys, A-8042 Graz, Austria.
[Fischer, G.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Bougeret, J. L.; Lecacheux, A.] CNRS, UMR 8109, LESIA, Observ Paris, F-92195 Meudon, France.
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Goetz, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
RP Oswald, TH (reprint author), Austrian Acad Sci, Space Res Inst, Dept Near Earth Space Phys, Schmiedlstr 6, A-8042 Graz, Austria.
EM thomas.oswald@oeaw.ac.at
RI Taubenschuss, Ulrich/E-3739-2015
FU Austrian Research Promotion Agency [ASAP-CO-001-05]
FX The research leading to this paper was made possible by a project within
the framework of the Austrian Space Applications Programme
(ASAP-CO-001-05) of the Austrian Research Promotion Agency.
NR 13
TC 10
Z9 10
U1 0
U2 2
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD FEB 2
PY 2009
VL 43
IS 3
BP 355
EP 364
DI 10.1016/j.asr.2008.07.017
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 407TX
UT WOS:000263388300004
ER
PT J
AU Xiong, X
Chiang, K
Sun, J
Barnes, WL
Guenther, B
Salomonson, VV
AF Xiong, X.
Chiang, K.
Sun, J.
Barnes, W. L.
Guenther, B.
Salomonson, V. V.
TI NASA EOS Terra and Aqua MODIS on-orbit performance
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE MODIS; NASA EOS; Terra; Aqua; Remote sensing; Calibration
ID RESOLUTION IMAGING SPECTRORADIOMETER; CALIBRATION
AB MODIS is a major instrument for NASA's Earth Observing System (EOS) missions. It is currently operating on-board the EOS Terra and Aqua spacecraft, launched in December 1999 and May 2002, respectively. The MODIS instrument was developed with improvements over heritage sensors in terms of its spectral, spatial, and temporal resolutions, and with more stringent calibration requirements. It makes observations in 36 spectral bands covering wavelengths from 0.41 to 14.4 mu m and at three nadir spatial resolutions: 250 m, 500 m, and I km. Together Terra and Aqua MODIS have produced more than 10 years of global data sets that have significantly helped scientists worldwide to better understand the Earth as an interacting system and the impacts on this system due to human related activities. In order to maintain on-orbit calibration and data product quality, MODIS was built with a complete set of on-board calibrators (OBCs), including a solar diffuser (SD), a solar diffuser stability monitor (SDSM), a blackbody (BB), a deep space view (SV) port, and a spectro-radiometric calibration assembly (SRCA). In this paper, we provide a brief description of both Terra and Aqua MODIS on-orbit operation and calibration activities and present results of on-orbit radiometric, spatial, and spectral characterization. Examples of short-term stability and long-term response changes are illustrated using observations made with the on-board calibrators. On-orbit performance parameters, including detectors noise characterization, are also compared to pre-launch design specifications. (C) 2008 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Chiang, K.; Sun, J.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Xiong, X.; Barnes, W. L.; Guenther, B.; Salomonson, V. V.] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Barnes, W. L.; Guenther, B.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Salomonson, V. V.] Univ Utah, Salt Lake City, UT 84112 USA.
RP Chiang, K (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd, Lanham, MD 20706 USA.
EM vincent_chiang@ssaihq.com
NR 15
TC 51
Z9 53
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 2
PY 2009
VL 43
IS 3
BP 413
EP 422
DI 10.1016/j.asr.2008.04.008
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 407TX
UT WOS:000263388300011
ER
PT J
AU Wang, CC
Trivedi, S
Jin, F
Swaminathan, V
Rodriguez, P
Prasad, NS
AF Wang, Chen-Chia
Trivedi, Sudhir
Jin, Feng
Swaminathan, V.
Rodriguez, Ponciano
Prasad, Narasimha S.
TI High sensitivity pulsed laser vibrometer and its application as a laser
microphone
SO APPLIED PHYSICS LETTERS
LA English
DT Article
DE diaphragms; measurement by laser beam; microphones; rough surfaces;
vibration measurement
AB We experimentally demonstrate a high sensitivity pulsed laser vibrometer that is capable of detecting optically rough surfaces vibrating with the displacement value of 75 pm as well as its application as a laser microphone. By directing the probe light beam repeatedly onto the vibrating diaphragm and/or pressure sensing interface, the sensitivity of the pulsed laser vibrometer in detecting the displacement of the vibrating diaphragm is significantly improved down to an estimated value of less than 4 pm In this paper, we present the principles of operation of this new kind of laser microphone together with experimental validations.
C1 [Wang, Chen-Chia; Trivedi, Sudhir; Jin, Feng] Brimrose Corp Amer, Baltimore, MD 21236 USA.
[Swaminathan, V.] USA, RDECOM ARDEC, Picatinny Arsenal, NJ 07806 USA.
[Rodriguez, Ponciano] INAOE, Puebla 7200, Mexico.
[Prasad, Narasimha S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Wang, CC (reprint author), Brimrose Corp Amer, 7720 Belair Rd, Baltimore, MD 21236 USA.
EM ccwang@brimrose.com
FU U. S. Army ARDEC [W15QKN-07-P0546]; U. S. Army RDECOM CERDEC NVESD
[W15P7T-O6-CF004]
FX The authors acknowledge the partial financial support by U. S. Army
ARDEC under Contract No. W15QKN-07-P0546 and U. S. Army RDECOM CERDEC
NVESD through a SBIR Phase II contract (Contract No. W15P7T-O6-CF004).
We also thank Brad Libbey and James Habersat of U. S. Army Nightvision
Laboratory for their insightful guidance and comments that contributed
to the foundation of our work.
NR 9
TC 8
Z9 8
U1 0
U2 5
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD FEB 2
PY 2009
VL 94
IS 5
AR 051112
DI 10.1063/1.3078520
PG 3
WC Physics, Applied
SC Physics
GA 404QB
UT WOS:000263167000012
ER
PT J
AU Mawet, D
Serabyn, E
Liewer, K
Hanot, C
McEldowney, S
Shemo, D
O'Brien, N
AF Mawet, D.
Serabyn, E.
Liewer, K.
Hanot, Ch.
McEldowney, S.
Shemo, D.
O'Brien, N.
TI Optical Vectorial Vortex Coronagraphs using Liquid Crystal Polymers:
theory, manufacturing and laboratory demonstration
SO OPTICS EXPRESS
LA English
DT Article
ID PHASE-MASK CORONAGRAPH; SUBWAVELENGTH DIELECTRIC GRATINGS; PANCHARATNAM
PHASE; ADAPTIVE OPTICS; MANIPULATION; PLANET; POLARIMETRY; VORTICES;
IMAGE; LIGHT
AB In this paper, after briefly reviewing the theory of vectorial vortices, we describe our technological approach to generating the necessary phase helix, and report results obtained with the first optical vectorial vortex coronagraph (OVVC) in the laboratory. To implement the geometrical phase ramp, we make use of Liquid Crystal Polymers (LCP), which we believe to be the most efficient technological path to quickly synthesize optical vectorial vortices of virtually any topological charge. With the first prototype device of topological charge 2, a maximum peak-to-peak attenuation of 1.4 x 10(-2) and a residual light level of 3 x 10(-5) at an angular separation of 3.5 lambda/d (at which point our current noise floor is reached) have been obtained at a wavelength of 1.55 mu m. These results demonstrate the validity of using space-variant birefringence distributions to generate a new family of coronagraphs usable in natural unpolarized light, opening a path to high performance coronagraphs that are achromatic and have low-sensitivity to low-order wavefront aberrations. (C) 2008 Optical Society of America
C1 [Mawet, D.; Serabyn, E.; Liewer, K.; Hanot, Ch.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McEldowney, S.; Shemo, D.; O'Brien, N.] JDSU, Santa Rosa, CA 95407 USA.
[Hanot, Ch.] Univ Liege, Inst Astrophys & Geophys Liege, B-4000 Liege, Belgium.
RP Mawet, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Dimitri.Mawet@jpl.nasa.gov
FU NASA Postdoctoral Program at the JPL; Caltech
FX This work was carried out at the Jet Propulsion Laboratory (JPL),
California Institute of Technology (Caltech), under contract with the
National Aeronautics and Space Administration (NASA). The first author
was supported by an appointment to the NASA Postdoctoral Program at the
JPL, Caltech, administered by Oak Ridge Associated Universities through
a contract with NASA.
NR 31
TC 81
Z9 82
U1 0
U2 9
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 FEB 2
PY 2009
VL 17
IS 3
BP 1902
EP 1918
DI 10.1364/OE.17.001902
PG 17
WC Optics
SC Optics
GA 408JX
UT WOS:000263432400080
PM 19189021
ER
PT J
AU Li, L
Adelstein, BD
Ellis, SR
AF Li, Li
Adelstein, Bernard D.
Ellis, Stephen R.
TI Perception of Image Motion During Head Movement
SO ACM TRANSACTIONS ON APPLIED PERCEPTION
LA English
DT Article
DE Human Factors; Design; Measurement; Performance; Head movement; image
motion; object motion; motion perception; VE latency
ID SELF-MOTION; OBJECT; ENVIRONMENT; SPEED
AB We examined human perception of head-referenced image motion during concurrent head movement. The visual stimulus was a checkerboard image in a head mounted display that moved from side-to-side. Observers rated the magnitude of the checkerboard motion while either rotating their head about a vertical axis (yaw), about a horizontal axis (pitch), or holding it still. In Experiment 1, we tested four image oscillation frequencies (0.25, 0.5, 1, and 2 Hz) while holding the head motion frequency constant at 0.5 Hz. In Experiment 2, we tested three head motion frequencies (0.25, 0.5, and 1 Hz) while holding the image oscillation frequency constant at 1 Hz. Across all image and head motion frequencies, perceptual sensitivity to image motion was reduced by about 45% during horizontal head movement. During vertical head movement, perceptual sensitivity was reduced by about 25% when head and image motion were of the same frequency. Compared with when the head was still, horizontal and vertical head movements produced a downward shift of about 10% in overall motion magnitude estimation response. Findings from this study provide virtual environment developers with a quantitative description of the influence of concurrent head movement on the perception of frontoparallel image motion.
C1 [Li, Li] Univ Hong Kong, Dept Psychol, Hong Kong, Hong Kong, Peoples R China.
[Adelstein, Bernard D.; Ellis, Stephen R.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
RP Li, L (reprint author), Univ Hong Kong, Dept Psychol, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China.
EM lili@hku.hk; Bernard.D.Adelstein@nasa.gov; sellis@mail.arc.nasa.gov
RI Li, Li/D-4924-2009
FU NASA's Space Human Factors Engineering Program; University of Hong Kong
FX This research was supported by NASA's Space Human Factors Engineering
Program and the University of Hong Kong Seed Funding Program for Basic
Research.
NR 23
TC 3
Z9 3
U1 0
U2 0
PU ASSOC COMPUTING MACHINERY
PI NEW YORK
PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA
SN 1544-3558
J9 ACM T APPL PERCEPT
JI ACM Trans. Appl. Percept.
PD FEB
PY 2009
VL 6
IS 1
AR 5
DI 10.1145/1462055.1462060
PG 15
WC Computer Science, Software Engineering
SC Computer Science
GA 450YM
UT WOS:000266437900005
ER
PT J
AU Zhou, D
Semones, E
Gaza, R
Johnson, S
Zapp, N
Weyland, M
Rutledge, R
Lin, T
AF Zhou, D.
Semones, E.
Gaza, R.
Johnson, S.
Zapp, N.
Weyland, M.
Rutledge, R.
Lin, T.
TI Radiation measured with different dosimeters during STS-121 space
mission
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Cosmic rays; Space radiation; Passive and active dosimeters; LET spectra
ID LOW-EARTH-ORBIT; CR-39 DETECTORS; SPECTRA; FIELD
AB Radiation impact to astronauts depends on the particles' linear energy transfer (LET) and is dominated by high LET radiation. Radiation risk experienced by astronauts can be determined with the radiation LET spectrum measured and the risk response function obtained from radiobiology. Systematical measurement of the space radiation is an important part for the research on the impact of radiation to astronauts and to make the radiation ALARA (is low as reasonably achievable). For NASA space missions at low Earth orbit (LEO), the active dosimeter used for all LET is the tissue equivalent proportional counter (TEPC) and the passive dosimeters used for the astronauts and for the monitored areas are the combination of CR-39 plastic nuclear trick detectors (PNTDs) for high LET and thermoluminescence dosimeters (TLDs) and optically Stimulated luminescence dosimeter (OSLDs) for low LET TEPC, CR-39 PNTDs and TLDs/OSLDs were used to measure the radiation during STS-121 space mission. LET spectra and radiation quantities were obtained with active and passive dosimeters, This paper will introduce the physical principles for TEPC and CR-39 detectors, the LET spectrum method for radiation measurement using CR-39 detectors and TEPC, and will present and compare the radiation LET spectra and quantities measured with TEPC, CR-39 PNTDs and TLDs/OSLDs. Published by Elsevier Ltd.
C1 [Zhou, D.; Semones, E.; Gaza, R.; Johnson, S.; Zapp, N.; Weyland, M.; Rutledge, R.; Lin, T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Zhou, D.; Gaza, R.] Univ Space Res Assoc, Houston, TX 77058 USA.
RP Zhou, D (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 Nasa Pkwy, Houston, TX 77058 USA.
EM dazhuang.zhou-1@nasa.gov
FU NSRL; BNL; TAMU; HIMAC; STS-114; STS-121
FX The authors wish to thank all those who assisted them in their work at
NSRL, BNL, TAMU, HIMAC, STS-114, and STS-121 mission.
NR 26
TC 6
Z9 7
U1 1
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD FEB
PY 2009
VL 64
IS 4
BP 437
EP 447
DI 10.1016/j.actaastro.2008.10.001
PG 11
WC Engineering, Aerospace
SC Engineering
GA 400LE
UT WOS:000262868700006
ER
PT J
AU Booth-Morrison, C
Noebe, RD
Seidman, DN
AF Booth-Morrison, Christopher
Noebe, Ronald D.
Seidman, David N.
TI Effects of tantalum on the temporal evolution of a model Ni-Al-Cr
superalloy during phase decomposition
SO ACTA MATERIALIA
LA English
DT Article
DE Nickel-based superalloys; Tantalum; Atom-probe tomography;
Nanostructures
ID 3-DIMENSIONAL ATOM-PROBE; NICKEL-BASE SUPERALLOYS;
MONTE-CARLO-SIMULATION; ALLOYING ELEMENTS; SITE SUBSTITUTION; RHENIUM
ADDITION; NI3AL; NANOSTRUCTURE; PRECIPITATION; TUNGSTEN
AB The effects of a 2.0 at.% addition of Ta to a model Ni-10.0Al-8.5Cr (at.%) superalloy aged at 1073 K are assessed using scanning electron microscopy and atom-probe tomography. The gamma'(LI(2))-precipitate morphology that develops as a result of gamma-(fcc)matrix phase decomposition is found to evolve from a bimodal distribution of spheroidal precipitates, to {001}-faceted cuboids and parallelepipeds aligned along the elastically soft < 001 >-type directions. The phase compositions and the widths of the gamma'-precipitate/gamma-matrix heterophase interfaces evolve temporally as the Ni-Al-Cr-Ta alloy undergoes quasi-stationary state coarsening after 1 h of aging. Tantalum is observed to partition preferentially to the gamma'-precipitate phase, and Suppresses the mobility of Ni in the gamma-matrix sufficiently to cause accumulation of Ni on the gamma-matrix side of the gamma'/gamma interface. Additionally, Computational modeling, employing Thermo-Calc, Dictra, and and PrecipiCalc, is employed to elucidate the kinetic pathways that lead to phase decomposition in this concentrated Ni-Al-Cr-Ta alloy. (C) 2008 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Booth-Morrison, Christopher; Seidman, David N.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA.
[Noebe, Ronald D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Seidman, David N.] Northwestern Univ, Ctr Atom Probe Tomog NUCAPT, Evanston, IL 60208 USA.
RP Seidman, DN (reprint author), Northwestern Univ, Dept Mat Sci & Engn, 2220 Campus Dr, Evanston, IL 60208 USA.
EM d-seidman@northwestern.edu
RI Seidman, David/B-6697-2009
FU National Science Foundation (NSF) [DMR-080461]; Northwestern University;
NSF-NSEC; NSF-MRSEC; Keck Foundation; State of Illinois and Northwestern
University; Northwestern University Center for Atom-Probe Tomography
(NUCAPT); NSF-MRI [DMR 0420532]; ONR-DURIP [N00014-0400798,
N00014-0610539]
FX This research was sponsored by the National Science Foundation (NSF)
under grant DMR-080461. The SEM and TEM studies were performed in the
EPIC facility of the NUANCE Center at Northwestern University. The
NUANCE Center is supported by NSF-NSEC, NSF-MRSEC, the Keck Foundation,
the State of Illinois and Northwestern University. Atom-probe
tomographic measurements were performed at the Northwestern University
Center for Atom-Probe Tomography (NUCAPT). Research Assistant Professor
D. Isheim is kindly thanked for managing NUCAPT. The
LEAP(kappa) tomograph was purchased and upgraded with funding
from the NSF-MRI (DMR 0420532) and ONR-DURIP (N00014-0400798 and
N00014-0610539). We extend our gratitude to Dr. C. Campbell of the
National Institute of Standards and Technology, Metallurgy Division
(Gaithersburg, MD), for diffusivity calculations, to Dr. C.K. Sudbrack,
Dr. K.E. Yoon and Dr. M. Nathal for discussions, and to Mr. Y. Zhou, Mr.
M. Anderson and Dr. Y. Amouyal for their assistance with the APT, SEM
and TEM work, respectively. We thank Prof. G.B. Olson and Dr. H.-J. Jou
of QuesTek LLC (Evanston, I L) for use of PrecipiCalc.
NR 78
TC 14
Z9 14
U1 2
U2 22
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6454
J9 ACTA MATER
JI Acta Mater.
PD FEB
PY 2009
VL 57
IS 3
BP 909
EP 920
DI 10.1016/j.actamat.2008.10.029
PG 12
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 402PJ
UT WOS:000263025300030
ER
PT J
AU Collins, SW
Westra, BW
Lin, JC
Jones, GS
AF Collins, S. W.
Westra, B. W.
Lin, J. C.
Jones, G. S.
TI Wind tunnel testing of powered lift, all-wing STOL model
SO AERONAUTICAL JOURNAL
LA English
DT Article
AB Short take-off and landing (STOL) systems can offer significant capabilities to warfighters and, for civil operators thriving on maximising efficiencies they can improve airspace use while containing noise within airport environments. In order to provide data for next generation systems, a wind tunnel test of an all-wing cruise efficient, short take-off and landing (CE STOL) configuration was conducted in the National Aeronautics and Space Administration (NASA) Langley Research Center (LaRC) 14ft by 22ft Subsonic Wind Tunnel. The test's purpose was to mature the aerodynamic aspects of an integrated powered lift system within an advanced mobility configuration capable of CE STOL. The full-span model made use of steady flap blowing and a lifting centerbody to achieve high lift coefficients. The test occurred during April through June of 2007 and included objectives for advancing the state-of-the-art of powered lift testing through gathering force and moment data, on-body pressure data, and off-body flow field measurements during automatically controlled blowing conditions. Data were obtained for variations in model configuration, angles of attack and sideslip, blowing coefficient.. and height above ground. The database produced by this effort is being used to advance design techniques and computational tools for developing systems with integrated powered lift technologies.
C1 [Collins, S. W.; Westra, B. W.] Northrop Grumman Corp, El Segundo, CA USA.
[Lin, J. C.; Jones, G. S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Collins, SW (reprint author), Northrop Grumman Corp, El Segundo, CA USA.
EM scott.collins@ngc.com
NR 9
TC 0
Z9 1
U1 1
U2 3
PU ROYAL AERONAUTICAL SOC
PI LONDON
PA 4 HAMILTON PL, LONDON W1J 7BQ, ENGLAND
SN 0001-9240
J9 AERONAUT J
JI Aeronaut. J.
PD FEB
PY 2009
VL 113
IS 1140
BP 129
EP 137
PG 9
WC Engineering, Aerospace
SC Engineering
GA 412OH
UT WOS:000263733600008
ER
PT J
AU Wu, YH
Walker, J
Schwede, D
Peters-Lidard, C
Dennis, R
Robarge, W
AF Wu, Yihua
Walker, John
Schwede, Donna
Peters-Lidard, Christa
Dennis, Robin
Robarge, Wayne
TI A new model of bi-directional ammonia exchange between the atmosphere
and biosphere: Ammonia stomatal compensation point
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Ammonia; Deposition; Emission; Compensation point; Modeling;
Bi-directional flux; Soybean
ID DRY DEPOSITION MODEL; OILSEED RAPE; APOPLASTIC NH4+; GRADIENT
MEASUREMENTS; GLUTAMINE-SYNTHETASE; BARLEY PLANTS; NH3 EXCHANGE; BARE
SOIL; LEAVES; NITROGEN
AB A new multi-layer canopy resistance model of bi-directional NH(3) exchange is presented. This new model, which is based on the Multi-Layer BioChemical deposition (MLBC) model [Wu, Y., Brashers, B., Finkelstein, P.L., Pleim, J.E., 2003a. A multiplayer biochemical dry deposition model. I. model formulation. J. Geophys. Res. 108, D1; Wu, Y., Brashers, B., Finkelstein, P.L., Pleim, J.E., 2003b. A multiplayer biochemical dry deposition model. II. Model evaluation. J. Geophys. Res. 108, D1], incorporates a parameterization for the ammonia stomatal compensation point that is theoretically derived to consider the effects of leaf temperature and apoplastic concentrations of NH(4)(+) and H(+). The new ammonia stomatal compensation point scheme accounts for the effects of deposition, emission and leaf temperature on the dynamics of apoplast [NH(4)(+)] and [H(+)]. The new model is evaluated against bidirectional NH(3) fluxes measured over fertilized soybean. The general patterns of observed deposition and emission are successfully reproduced when the ammonia stomatal compensation point is included. Driven by the effects of deposition, emission and leaf temperature, modeled apoplastic [NH(4)(+)] and [H(+)] display significant diurnal variation when the buffer effect of the underlying metabolic processes generating or consuming NH(4)(+) were ignored. Model predictive capability is improved slightly by incorporating the feedback into a dynamic stomatal compensation point. A simple implementation of the feedback mechanism in the current model provides opportunities for improvement. While the stomatal flux is shown to be an important process in the regulation of canopy-scale fluxes, it appears that exchange with leaf surface water and soil may also be important. Published by Elsevier B.V.
C1 [Wu, Yihua] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA.
[Walker, John] US EPA, Natl Risk Management Res Lab, Res Triangle Pk, NC 27711 USA.
[Schwede, Donna; Dennis, Robin] US EPA, Natl Exposure Res Lab, Res Triangle Pk, NC 27711 USA.
[Peters-Lidard, Christa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Robarge, Wayne] N Carolina State Univ, Dept Soil Sci, Raleigh, NC 27695 USA.
RP Wu, YH (reprint author), NOAA, NCEP, EMC, 5200 Auth Rd, Camp Springs, MD 20746 USA.
EM Yihua.Wu@noaa.gov
RI Peters-Lidard, Christa/E-1429-2012; Walker, John/I-8880-2014
OI Peters-Lidard, Christa/0000-0003-1255-2876; Walker,
John/0000-0001-6034-7514
NR 68
TC 20
Z9 20
U1 2
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD FEB
PY 2009
VL 149
IS 2
BP 263
EP 280
DI 10.1016/j.agrformet.2008.08.012
PG 18
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA 397TH
UT WOS:000262684500006
ER
PT J
AU Borak, JS
Jasinski, MF
AF Borak, Jordan S.
Jasinski, Michael F.
TI Effective interpolation of incomplete satellite-derived leaf-area index
time series for the continental United States
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Interpolation; Leaf-area index; MODIS; Time series
ID MODIS; PRODUCTS
AB Many earth science modeling applications employ continuous input data fields derived from satellite data. Environmental factors, sensor limitations and algorithmic constraints lead to data products of inherently variable quality. This necessitates interpolation of one form or another in order to produce high quality input fields free of missing data. The present research tests several interpolation techniques as applied to satellite-derived leaf-area index (LAI), an important quantity in many global climate and ecological models. The study evaluates and applies a variety of interpolation techniques for the Moderate Resolution Imaging Spectroradiometer (MODIS) LAI product over the time period of 2001-2006 for a region containing the conterminous United States. Results indicate that the accuracy of an individual interpolation technique depends upon the underlying land cover. Spatial interpolation provides better results in forested areas, while temporal interpolation performs more effectively over non-forest cover types. Combination of spatial and temporal approaches offers superior interpolative capabilities to any single method, and in fact, generation of continuous data fields requires a hybrid approach such as this. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Borak, Jordan S.] Wyle Informat Syst, Lanham, MD 20706 USA.
[Jasinski, Michael F.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP Borak, JS (reprint author), Wyle Informat Syst, 7515 Mission Dr,Suite A100, Lanham, MD 20706 USA.
EM Jordan.S.Borak@nasa.gov; Michael.F.Jasinski@nasa.gov
FU NASA
FX This research was funded by the NASA Earth Science Division Applied
Sciences Homeland Security Program and the Terrestrial Hydrology
Program. The authors are grateful to two anonymous reviewers for their
comments that greatly enhanced the quality of the manuscript.
NR 18
TC 19
Z9 21
U1 1
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD FEB
PY 2009
VL 149
IS 2
BP 320
EP 332
DI 10.1016/j.agrformet.2008.08.017
PG 13
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA 397TH
UT WOS:000262684500010
ER
PT J
AU Mckay, CP
AF Mckay, Christopher P.
TI Snow recurrence sets the depth of dry permafrost at high elevations in
the McMurdo Dry Valleys of Antarctica
SO ANTARCTIC SCIENCE
LA English
DT Article
DE Beacon Valley; ice-cemented ground; Mars; snow; University Valley
ID BEACON VALLEY; GLACIER ICE; GROUND ICE; MARS; STABILITY; SUBLIMATION
AB Dry permafrost oil Earth is unique to the Antarctic and is found in the upper elevations of the McMurdo Dry Valleys. Despite its widespread presence in the Dry Valleys, the factors that control the distribution of dry permafrost and the ice-cemented ground below it are poorly understood. Here I show, by a combination of theoretical analysis and field observations, that the recurrence of snow can explain the depth of dry permafrost and the location of ice-cemented ground in Antarctica. For data from Linnaeus Terrace at 1600-1650 m elevation in Upper Wright Valley a recurrence intervals of about two years explains the presence of ground ice at 25 cm depth, under 12.5 cm of dry permafrost. Snow recurrence periods longer than 10 years Would create only dry permafrost at this site. The snow gradient in University Valley resulting from the windblown snow from the polar plateau creates a corresponding gradient in the depth to ice-cemented ground. On the floor of Beacon Valley, the presence of dry permafrost without underlying ice-cemented ground indicates snow recurrence intervals of more than 10 years and implies that the ancient massive ice in this valley is not stable. Snow recurrence may also set the depth to ground ice on Mars.
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 cmckay@mail.arc.nasa.gov
FU NASA IPY program
FX This work was supported by the NASA IPY program. The able assistance of
the other members of the field team and the excellent logistics support
from the NSF Office of Polar Programs allowed the field work to be
completed. 1 thank the editor and two reviewers for comments that
greatly improved the paper.
NR 19
TC 30
Z9 31
U1 0
U2 2
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0954-1020
J9 ANTARCT SCI
JI Antarct. Sci.
PD FEB
PY 2009
VL 21
IS 1
BP 89
EP 94
DI 10.1017/S0954102008001508
PG 6
WC Environmental Sciences; Geography, Physical; Geosciences,
Multidisciplinary
SC Environmental Sciences & Ecology; Physical Geography; Geology
GA 407UF
UT WOS:000263389100007
ER
PT J
AU Aspin, C
Greene, TP
Reipurth, B
AF Aspin, Colin
Greene, Thomas P.
Reipurth, Bo
TI V1647 ORIONIS: KECK/NIRSPEC 2 mu m ECHELLE OBSERVATIONS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; reflection nebulae; stars: individual (V1647
Ori)
ID NEAR-INFRARED SPECTROSCOPY; PROTOSTELLAR DISK MODELS; YOUNG STELLAR
OBJECTS; MCNEILS NEBULA OBJECT; HERBIG-HARO FLOWS; MOLECULAR OUTFLOWS;
CLASS-I; OUTBURST; STARS; SUBMILLIMETER
AB We present new Keck II NIRSPEC high-spectral resolution 2 mu m echelle observations of the young eruptive variable star V1647 Orionis. This star went into outburst in late 2003 and faded to its pre-outburst brightness after approximately 26 months. V1647 Orionis is the illuminating star of McNeil's Nebula and is located near M 78 in the Lynds 1630 dark cloud. Our spectra have a resolving power of approximately 18,000 and allow us to study in detail the weak absorption features present on the strong near-IR veiled continuum. An analysis of the echelle orders containing Mg I (2.1066 mu m) and Al I (2.1099 mu m), Br gamma (2.1661 mu m), the Na I doublet (2.206 and 2.209 mu m), and the CO overtone bandhead (2.2935 mu m) gives us considerable information on the physical and geometric characteristics of the regions producing these spectral features. We find that, at high spectral resolution, V1647 Orionis in quiescence resembles a significant number of FU Orionis type eruptive variables and does not appear similar to the quiescent EX Lupi variables observed. This correspondence is discussed and implications for the evolutionary state of the star are considered.
C1 [Aspin, Colin; Reipurth, Bo] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Greene, Thomas P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Aspin, C (reprint author), Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA.
EM caa@ifa.hawaii.edu; thomas.p.greene@nasa.gov; reipurth@ifa.hawaii.edu
FU NASA; NASA Origins of Solar Systems program [WBS 411672.04.01.02];
National Aeronautics and Space Administration [NNA04CC08A]
FX The data presented herein were obtained at the W. M. Keck Observatory
from telescope time allocated by the University of Hawaii Time
Allocation Committee. 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 sacred mountain. C. A. acknowledges supported by
NASA through the American Astronomical Society's Small Research Grant
Program. T. P. G. acknowledges grant support from the NASA Origins of
Solar Systems program WBS 411672.04.01.02 for this work. B. R.
acknowledges supported from the National Aeronautics and Space
Administration through the NASA Astrobiology Institute under Cooperative
Agreement No. NNA04CC08A issued through the Office of Space Science.
NR 49
TC 7
Z9 7
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2009
VL 137
IS 2
BP 2968
EP 2980
DI 10.1088/0004-6256/137/2/2968
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 400WV
UT WOS:000262901000003
ER
PT J
AU Ghosh, KK
Saripalli, L
Gandhi, P
Foellmi, C
Gutierrez, CM
Lopez-Corredoira, M
AF Ghosh, Kajal K.
Saripalli, Lakshmi
Gandhi, Poshak
Foellmi, Cedric
Gutierrez, Carlos M.
Lopez-Corredoira, Martin
TI MULTIWAVELENGTH STUDY OF THE BRIGHT X-RAY SOURCE POPULATION IN THE
INTERACTING GALAXIES NGC5774/NGC5775
SO ASTRONOMICAL JOURNAL
LA English
DT Review
DE binaries: general; black hole physics; galaxies: interactions; X-rays:
individual (NGC 5774 and NGC5775)
ID MASS BLACK-HOLES; XMM-NEWTON OBSERVATIONS; RADIAL-VELOCITY FIELD;
RING-SHAPED NEBULAE; YOUNG STAR-CLUSTERS; CHANDRA OBSERVATIONS; NEARBY
GALAXIES; ACCRETION DISKS; OPTICAL COUNTERPARTS; GLOBULAR-CLUSTER
AB A few nearby interacting galaxies are known that host elevated numbers of ultraluminous X-ray sources. Here we report the results of a multiwavelength study of the X-ray source population in the field of the interacting pair of galaxies NGC5774/5775. A total of 49 discrete sources are detected, including 12 ultraluminous X-ray source candidates with luminosities above 10(39) erg s(-1) in the 0.5-8.0 keV X-ray band. X-ray source positions are mapped onto optical and radio images to search for potential counterparts. Twelve sources in the field have optical counterparts. Optical colors are used to differentiate these sources, which are mostly located outside the optical extent of the interacting galaxies, as potential globular clusters (2), one compact blue dwarf galaxy, and quasars (5). We obtained optical spectra of two of the latter, which confirm that they are background quasars. We expect three background sources in the field of these two galaxies. These results are used to determine the true X-ray population of these two interacting galaxies, which are connected with two bridges. Two high-mass X-ray binaries are detected on these two bridges, suggesting their formation through the interaction-induced star formation episode. NGC5774 is an extremely low star forming galaxy with five X-ray sources plus three ultraluminous X-ray source candidates. Observed X-ray population of this galaxy does not scale with the star formation rate (SFR) alone but it may scale jointly with the mass of the galaxy and the SFR. Twenty-four X-ray sources (excluding the active galactic nucleus, AGN) are detected in NGC5775. and its X-ray luminosity function is consistent with that of other interacting galaxies, suggesting that these galaxies have comparable numbers of luminous sources. No X-ray point source was detected at the center of this galaxy to a limiting luminosity of 3 x 1037 erg s(-1). Wind/outflow is detected from the central region of NGC5775. Subsolar diffuse gas with temperature similar to 0.31 +/- 0.04 keV is present in this galaxy, which suggest that NGC5775 is in the beginning of the evolutionary process. Twelve ultraluminous X-ray source candidates are detected within the D(25) isophotes of NGC5774/5775. Several of them are highly variable X-ray sources that fall below the detection levels in one of two X-ray observations spaced 15 months apart. Two ultraluminous X-ray sources are located in the halo of NGC5775 and one of them is hosted in a globular star cluster. Four of the remaining 10 candidates have powerlaw X-ray spectra with photon indices around 1.8 and are extremely luminous with no optical counterparts. One of these four objects is the brightest (similar to 10(41) erg s(-1)) with a possible 6.2 hr period and it varied by more than a factor of 500. Two of the rest six ultraluminous X-ray source candidates are having steep-powerlaw X-ray spectra and are embedded in diffuse Ha emission, which are probably ionized nebulae. These nebulae could be due to energetic supernova explosions or to continuous inflation by jets. Rest four ultraluminous X-ray source candidates are flat-powerlaw X-ray sources hosted in either young star clusters or bright star forming complexes. Two of them are radio sources.
Finally, we find that the number of ultraluminous X-ray source candidates in interacting/merging galaxies are correlated with the far-infrared, K-band, and UV luminosities of their host galaxies, suggesting that the formation and evolution of ultraluminous X-ray sources depend not only on the SF but also on the mass of their host galaxies.
C1 [Ghosh, Kajal K.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
[Saripalli, Lakshmi] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Gandhi, Poshak] RIKEN, Inst Phys & Chem Sci, Wako, Saitama 3510198, Japan.
[Foellmi, Cedric] Univ Grenoble 1, Astrophys Lab, F-38400 St Martin Dheres, France.
[Gutierrez, Carlos M.; Lopez-Corredoira, Martin] IAC, E-38205 Tenerife, Spain.
RP Ghosh, KK (reprint author), NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, VP62, Huntsville, AL 35812 USA.
RI Saripalli, Lakshmi/D-4878-2012; Astronomy & Astrophysics Group, Raman
Res Institute/D-4046-2012; M, Manjunath/N-4000-2014
OI M, Manjunath/0000-0001-8710-0730
NR 170
TC 8
Z9 8
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD FEB
PY 2009
VL 137
IS 2
BP 3263
EP 3285
DI 10.1088/0004-6256/137/2/3263
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 400WV
UT WOS:000262901000025
ER
PT J
AU Masetti, N
Parisi, P
Palazzi, E
Jimenez-Bailon, E
Morelli, L
Chavushyan, V
Mason, E
McBride, VA
Bassani, L
Bazzano, A
Bird, AJ
Dean, AJ
Galaz, G
Gehrels, N
Landi, R
Malizia, A
Minniti, D
Schiavone, F
Stephen, JB
Ubertini, P
AF Masetti, N.
Parisi, P.
Palazzi, E.
Jimenez-Bailon, E.
Morelli, L.
Chavushyan, V.
Mason, E.
McBride, V. A.
Bassani, L.
Bazzano, A.
Bird, A. J.
Dean, A. J.
Galaz, G.
Gehrels, N.
Landi, R.
Malizia, A.
Minniti, D.
Schiavone, F.
Stephen, J. B.
Ubertini, P.
TI Unveiling the nature of INTEGRAL objects through optical spectroscopy
VII. Identification of 20 Galactic and extragalactic hard X-ray sources
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Review
DE galaxies: Seyfert; quasars: emission lines; X-rays: binaries; stars:
novae, cataclysmic variables; techniques: spectroscopic; X-rays: general
ID ALL-SKY SURVEY; SLEW SURVEY CATALOG; 6DF GALAXY SURVEY; MULTIWAVELENGTH
OBSERVATIONS; CI CAMELOPARDALIS; HOST GALAXIES; DATA RELEASE;
XMM-NEWTON; EMISSION; NUCLEI
AB Within the framework of our program of assessment of the nature of unidentified or poorly known INTEGRAL sources, we present here spectroscopy of optical objects, selected through positional cross-correlation with soft X-ray detections (afforded with satellites such as Swift, ROSAT, Chandra and/or XMM-Newton) as putative counterparts of hard X-ray sources detected with the IBIS instrument onboard INTEGRAL. Using 6 telescopes of various sizes and archival data from two on-line spectroscopic surveys we are able to identify, either for the first time or independent of other groups, the nature of 20 INTEGRAL hard X-ray sources. Our results indicate that: 11 of these objects are active galactic nuclei (AGNs) at redshifts between 0.014 and 0.978, 7 of which display broad emission lines, 2 show narrow emission lines only, and 2 have unremarkable or no emission lines (thus are likely Compton thick AGNs); 5 are cataclysmic variables (CVs), 4 of which are (possibly magnetic) dwarf novae and one is a symbiotic star; and 4 are Galactic X-ray binaries (3 with high-mass companions and one with a low-mass secondary). It is thus again found that the majority of these sources are AGNs or magnetic CVs, confirming our previous findings. When possible, the main physical parameters for these hard X-ray sources are also computed using the multiwavelength information available in the literature. These identifications support the importance of INTEGRAL in the study of the hard X-ray spectrum of all classes of X-ray emitting objects, and the effectiveness of a strategy of multi-catalogue cross-correlation plus optical spectroscopy to securely pinpoint the actual nature of unidentified hard X-ray sources.
C1 [Masetti, N.; Parisi, P.; Palazzi, E.; Bassani, L.; Landi, R.; Malizia, A.; Schiavone, F.; Stephen, J. B.] Ist Astrofis Spaziale Fis Cosm, INAF, I-40129 Bologna, Italy.
[Parisi, P.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Jimenez-Bailon, E.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Morelli, L.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Chavushyan, V.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico.
[Mason, E.] European So Observ, Santiago 19, Chile.
[McBride, V. A.; Bird, A. J.; Dean, A. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Bazzano, A.; Ubertini, P.] Ist Astrofis Spaziale Fis Cosm, INAF, I-00133 Rome, Italy.
[Galaz, G.; Minniti, D.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Masetti, N (reprint author), Ist Astrofis Spaziale Fis Cosm, INAF, Via Gobetti 101, I-40129 Bologna, Italy.
EM masetti@iasfbo.inaf.it
RI Gehrels, Neil/D-2971-2012; Palazzi, Eliana/N-4746-2015;
OI Palazzi, Eliana/0000-0002-8691-7666; Bassani,
Loredana/0000-0003-4858-6963; Masetti, Nicola/0000-0001-9487-7740;
mason, elena/0000-0003-3877-0484; Malizia, Angela/0000-0002-6558-1163
FU ASI; INAF [I/023/05/0]; ASI-INTEGRAL [I/008/07]; University of Padua
[CPDR061795/06]; CONACYT [54480-F]; Basal CATA [PFB 06/09]; FONDAP
Center for Astrophysics [15010003]
FX We thank Silvia Galleti for Service Mode observations at the Loiano
telescope; Pablo Rodr guez-Gil and Andrew Cardwell for Service Mode
observations at the WHT; Francesca Ghinassi for Service Mode
observations at the TNG; Antonio De Blasi and Ivan Bruni for night
assistance at the Loiano telescope; Edgardo Cosgrove, Manuel Hernandez
and Jose Velasquez for day and night assistance at the CTIO telescope;
Alessandro Ederoclite for support at the ESO 3.6 m telescope; Ariel
Sanchez for night assistance at the ESO 3.6 m telescope; Mauro Orlandini
for comments and suggestions. We also thank the anonymous referee for
useful remarks which helped us to improve the quality of this paper.
This research has made use of the ASI Science Data Center Multimission
Archive; it also used the NASA Astrophysics Data System Abstract
Service, the NASA/IPAC Extragalactic Database (NED), and the NASA/IPAC
Infrared Science Archive, which are operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. This publication made use
of data products from the Two Micron All Sky Survey (2MASS), which is a
joint project of the University of Massachusetts and the Infrared
Processing and Analysis Center/California Institute of Technology,
funded by the National Aeronautics and Space Administration and the
National Science Foundation. This research has also made use of data
extracted from the 6dF Galaxy Survey and the Sloan Digitized Sky Survey
archives; it has also made use of the ESO Science Archive operated at
Garching bei Munchen, Germany, of the SIMBAD database operated at CDS,
Strasbourg, France, and of the HyperLeda catalogue operated at the
Observatoire de Lyon, France. The authors acknowledge the ASI and INAF
financial support via grant No. I/023/05/0. P. P. is supported by the
ASI-INTEGRAL grant No. I/008/07. L. M. is supported by the University of
Padua through grant No. CPDR061795/06. V. C. is supported by the CONACYT
research grant 54480-F (Mexico). D. M. is supported by the Basal CATA
PFB 06/09, and FONDAP Center for Astrophysics grant No. 15010003. N. M.
and L. M. thank the Pontificia Universidad Catolica de Chile for the
pleasant hospitality in Santiago de Chile during the preparation of this
paper.
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FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2009
VL 495
IS 1
BP 121
EP 135
DI 10.1051/0004-6361:200811322
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410BL
UT WOS:000263550000011
ER
PT J
AU Byrne, JP
Gallagher, PT
McAteer, RTJ
Young, CA
AF Byrne, J. P.
Gallagher, P. T.
McAteer, R. T. J.
Young, C. A.
TI The kinematics of coronal mass ejections using multiscale methods
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: coronal mass ejections (CMEs); Sun: activity; techniques: image
processing; methods: data analysis
ID FLUX-ROPE; BREAKOUT MODEL; ACCELERATION; EVOLUTION; LASCO; PROPAGATION;
INITIATION; TRACKING; FEATURES; ERUPTION
AB Aims. The diffuse morphology and transient nature of coronal mass ejections (CMEs) make them difficult to identify and track using traditional image processing techniques. We apply multiscale methods to enhance the visibility of the faint CME front. This enables an ellipse characterisation to objectively study the changing morphology and kinematics of a sample of events imaged by the Large Angle Spectrometric Coronagraph (LASCO) onboard the Solar and Heliospheric Observatory (SOHO) and the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) onboard the Solar Terrestrial Relations Observatory (STEREO). The accuracy of these methods allows us to test the CMEs for non-constant acceleration and expansion.
Methods. We exploit the multiscale nature of CMEs to extract structure with a multiscale decomposition, akin to a Canny edge detector. Spatio-temporal filtering highlights the CME front as it propagates in time. We apply an ellipse parameterisation of the front to extract the kinematics (height, velocity, acceleration) and changing morphology ( width, orientation).
Results. The kinematic evolution of the CMEs discussed in this paper have been shown to differ from existing catalogues. These catalogues are based upon running-difference techniques that can lead to over-estimating CME heights. Our resulting kinematic curves are not well-fitted with the constant acceleration model. It is shown that some events have high acceleration below similar to 5 R(circle dot). Furthermore, we find that the CME angular widths measured by these catalogues are over-estimated, and indeed for some events our analysis shows non-constant CME expansion across the plane-of-sky.
C1 [Byrne, J. P.; Gallagher, P. T.; McAteer, R. T. J.] Univ Dublin Trinity Coll, Sch Phys, Astrophys Res Grp, Dublin 2, Ireland.
[Young, C. A.] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA.
RP Byrne, JP (reprint author), Univ Dublin Trinity Coll, Sch Phys, Astrophys Res Grp, Dublin 2, Ireland.
EM jbyrne6@gmail.com
RI McAteer, R. T. James/D-3736-2011; Byrne, Jason/K-4827-2013; Gallagher,
Peter/C-7717-2011
OI Byrne, Jason/0000-0002-9412-8878; Gallagher, Peter/0000-0001-9745-0400
FU Science Foundation Ireland's Research Frontiers Programme; NASA's Living
With A Star Program; Marie Curie Fellowshi
FX This work is supported by grants from Science Foundation Ireland's
Research Frontiers Programme and NASA's Living With A Star Program. JMA
is grateful to the STEREO/COR1 team at NASA/GSFC and is currently funded
by a Marie Curie Fellowship. We would also like to thank the anonymous
referee for their very helpful comments. SOHO is a project of
international collaboration between ESA and NASA. The STEREO/SECCHI
project is an international consortium of the Naval Research Laboratory
( USA), Lockheed Martin Solar and Astrophysics Lab ( USA), NASA Goddard
Space Flight Center ( USA), Rutherford Appleton Laboratory (UK),
University of Birmingham ( UK), Max-Planck-Institut fur
Sonnen-systemforschung ( Germany), Centre Spatial de Liege ( Belgium),
Institut d'Optique Theorique et Appliquee ( France), and Institut
d'Astrophysique Spatiale ( France).
NR 42
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2009
VL 495
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BP 325
EP 334
DI 10.1051/0004-6361:200809811
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 410BL
UT WOS:000263550000030
ER
PT J
AU Papadakis, IE
Sobolewska, M
Arevalo, P
Markowitz, A
McHardy, IM
Miller, L
Reeves, JN
Turner, TJ
AF Papadakis, I. E.
Sobolewska, M.
Arevalo, P.
Markowitz, A.
McHardy, I. M.
Miller, L.
Reeves, J. N.
Turner, T. J.
TI A correlation between the spectral and timing properties of AGN
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; X-rays: galaxies
ID X-RAY VARIABILITY; ACTIVE GALACTIC NUCLEI; NARROW-LINE SEYFERT-1;
BLACK-HOLE MASS; XMM-NEWTON; POWER SPECTRUM; CYGNUS X-1; RXTE; LONG;
LUMINOSITY
AB Context. We present the results from a combined study of the average X-ray spectral and timing properties of 14 nearby AGN.
Aims. We investigate whether a "spectral-timing" AGN correlation exists, similar to the one observed in Cyg X-1, compare the two correlations, and constrain possible physical mechanisms responsible for the X-ray emission in compact, accreting objects.
Methods. For 11 of the sources in the sample, we used all the available data from the RXTE archive, which were taken until the end of 2006. There are 7795 RXTE observations in total for these AGN, obtained over a period of similar to 7-11 years. We extracted their 3-20 keV spectra and fitted them with a simple power-law model, modified by the presence of a Gaussian line (at 6.4 keV) and cold absorption, when necessary. We used the best-fit slopes to construct their sample distribution function, and we used the median of the distribution, and the mean of the best-fit slopes, which are above the 80th percentile of the distributions, to estimate the mean spectral slope of the objects. The latter estimate is more appropriate in the case when the energy spectra of the sources are significantly affected by absorption and/or reflection effects. We also used results from the literature to estimate the average spectral slope of the three remaining objects.
Results. The AGN average spectral slopes are not correlated either with the black hole mass or the characteristic frequencies that were detected in the power spectra. They are positively correlated, though, with the characteristic frequency when normalised to the sources black hole mass. This correlation is similar to the spectral-timing correlation that has been observed in Cyg X-1, but not the same.
Conclusions. The AGN spectral-timing correlation can be explained if we assume that the accretion rate determines both the average spectral slope and the characteristic time scales in these systems. The spectrum should steepen and the characteristic frequency should increase, proportionally, with increasing accretion rate. We also provide a quantitative expression between spectral slope and accretion rate. Thermal Comptonisation models are broadly consistent with our result, and can also explain the difference between the spectral-timing correlations in Cyg X-1 and AGN, but only if the ratio of the soft photons' luminosity to the power injected to the hot corona is proportionally related to the accretion rate.
C1 [Papadakis, I. E.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece.
[Papadakis, I. E.; Sobolewska, M.] Fdn Res & Technol, IESL, Iraklion 71110, Greece.
[Arevalo, P.; McHardy, I. M.] Univ Southampton, Sch Phys & Astron, Southampton S017 1BJ, Hants, England.
[Markowitz, A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Miller, L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Reeves, J. N.] Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Turner, T. J.] NASA, Goddard Space Flight Ctr, Explorat Univ Div, Greenbelt, MD 20771 USA.
RP Papadakis, IE (reprint author), Univ Crete, Dept Phys, POB 2208, Iraklion 71003, Crete, Greece.
EM jhep@physics.uoc.gr
RI Papadakis, Iossif/C-3235-2011
FU EU [MTKD-CT-2006-039965]; Ministry of Science and Higher Education
[N20301132/1518]
FX We would like to thank the referee, P.O. Petrucci, for valuable comments
which helped us to improve the paper significantly. I. E. P. and M. S.
acknowledge support by the EU grant MTKD-CT-2006-039965. M. S. also
acknowledges support by the the Polish grant N20301132/1518 from
Ministry of Science and Higher Education.
NR 57
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2009
VL 494
IS 3
BP 905
EP 913
DI 10.1051/0004-6361:200811005
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406SP
UT WOS:000263315500011
ER
PT J
AU Zwintz, K
Kallinger, T
Guenther, DB
Gruberbauer, M
Huber, D
Rowe, J
Kuschnig, R
Weiss, WW
Matthews, JM
Moffat, AFJ
Rucinski, SM
Sasselov, D
Walker, GAH
Casey, MP
AF Zwintz, K.
Kallinger, T.
Guenther, D. B.
Gruberbauer, M.
Huber, D.
Rowe, J.
Kuschnig, R.
Weiss, W. W.
Matthews, J. M.
Moffat, A. F. J.
Rucinski, S. M.
Sasselov, D.
Walker, G. A. H.
Casey, M. P.
TI MOST photometry of the enigmatic PMS pulsator HD 142666
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: pre-main sequence; stars: variables: delta Sct; stars:
individual: HD 142666; techniques: photometric
ID PRE-MAIN-SEQUENCE; STANDARD SOLAR MODEL; TIME-SERIES DATA; INSTABILITY
STRIP; FOURIER SPACE; STARS; OPACITIES; SEISMOLOGY; REDUCTION; EVOLUTION
AB Context. Modeling of pre-main sequence (PMS) stars through asteroseismology of PMS p-mode pulsators has only recently become possible, and spacebased photometry is one of the important sources of data for these efforts. We present precise photometry of the pulsating Herbig Ae star HD 142666 obtained in two consecutive years with the MOST (Microvariability & Oscilations of STars) satellite.
Aims. Previously, only a single pulsation period was known for HD 142666. The MOST photometry reveals that HD 142666 is multiperiodic. However, the unique identification of pulsation frequencies is complicated by the presence of irregular variability caused by the star's circumstellar dust disk. The two light curves obtained with MOST in 2006 and 2007 provided data of unprecedented quality to study the pulsations in HD 142666 and also to monitor the circumstellar variability.
Methods. Frequency analysis was performed using the routine SIGSPEC and the results from the 2006 and 2007 campaigns were then compared to each other with the software CINDERELLA to identify frequencies common to both light curves. The correlated frequencies were then submitted to an asteroseismic analysis.
Results. We attribute 12 frequencies to pulsation. Model fits to the three frequencies with the highest amplitudes lie well outside the uncertainty box for the star's position in the HR diagram based on published values. Some of the frequencies appear to be rotationally split modes.
Conclusions. The models suggest that either (1) the published estimate of the luminosity of HD 142666, based on a relation between circumstellar disk radius and stellar luminosity, is too high and/or (2) additional physics such as mass accretion may be needed in our models to accurately fit both the observed frequencies and HD 142666's position in the HR diagram.
C1 [Zwintz, K.; Kallinger, T.; Gruberbauer, M.; Huber, D.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Guenther, D. B.; Casey, M. P.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Rowe, J.; Kuschnig, R.; Matthews, J. M.; Walker, G. A. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Rowe, J.] NASA, Moffett Field, CA 94035 USA.
[Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Rucinski, S. M.] Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada.
[Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Huber, D.] Univ Sydney, Sch Phys, Inst Astron, Sydney, NSW 2006, Australia.
RP Zwintz, K (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM zwintz@astro.univie.ac.at; kallinger@astro.univie.ac.at;
guenther@ap.smu.ca; Gruberbauer@astro.univie.ac.at;
dhuber@physics.usyd.edu.au; rowe@phas.ubc.ca; kuschnig@astro.ubc.ca;
Weiss@astro.univie.ac.at; matthews@astro.ubc.ca;
moffat@astro.umontreal.ca; rucinski@astro.utoronto.ca;
sasselov@cfa.harvard.edu; gordonwa@uvic.ca; mcasey@astro.univie.ac.at
OI Kallinger, Thomas/0000-0003-3627-2561; Zwintz,
Konstanze/0000-0001-9229-8315
FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung
[T335-N16P17580]; The Natural Sciences and Engineering Research Council
of Canada; FQRT (Quebec); Canadian Space Agency
FX K. Z., T. K., M. G., R. K. and W. W. W. acknowledge support by the
Austrian Fonds zur Forderung der wissenschaftlichen Forschung (KZ:
project T335-N16; TK, MG, RK and WWW: project P17580). The Natural
Sciences and Engineering Research Council of Canada supports the
research of D. B. G., J. M. M., A. F. J. M., S. M. R. and M. P. C; A. F.
J. M. is also supported by FQRT (Quebec), and R. K. is also supported by
the Canadian Space Agency. Special thanks goes to Gregg Wade and Jason
Grunhunt who provided the newest values for Teff.
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J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
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EP 1040
DI 10.1051/0004-6361:200811116
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406SP
UT WOS:000263315500022
ER
PT J
AU Raftery, CL
Gallagher, PT
Milligan, RO
Klimchuk, JA
AF Raftery, C. L.
Gallagher, P. T.
Milligan, R. O.
Klimchuk, J. A.
TI Multi-wavelength observations and modelling of a canonical solar flare
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: flares; hydrodynamics
ID CORONAL DIAGNOSTIC SPECTROMETER; CHROMOSPHERIC EVAPORATION; X-RAY;
TRANSITION REGION; ATOMIC DATABASE; IMPULSIVE PHASE; EMISSION-LINES;
ACTIVE-REGION; LOOPS; RHESSI
AB Aims. We investigate the temporal evolution of temperature, emission measure, energy loss, and velocity in a C-class solar flare from both observational and theoretical perspectives.
Methods. The properties of the flare were derived by following the systematic cooling of the plasma through the response functions of a number of instruments - the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI; > 5 MK), GOES-12 (5-30 MK), the Transition Region and Coronal Explorer (TRACE 171 angstrom; 1 MK), and the Coronal Diagnostic Spectrometer (CDS; similar to 0.03-8 MK). These measurements were studied in combination with simulations from the 0-D enthalpy based thermal evolution of loops (EBTEL) model.
Results. At the flare onset, upflows of similar to 90 km s(-1) and low-level emission were observed in Fe XIX, consistent with pre-flare heating and gentle chromospheric evaporation. During the impulsive phase, upflows of similar to 80 km s(-1) in Fe XIX and simultaneous downflows of similar to 20 km s(-1) in He I and O V were observed, indicating explosive chromospheric evaporation. The plasma was subsequently found to reach a peak temperature of greater than or similar to 13 MK in approximately 10 min. Using EBTEL, conduction was found to be the dominant loss mechanism during the initial similar to 300 s of the decay phase. It was also found to be responsible for driving gentle chromospheric evaporation during this period. As the temperature fell below similar to 8 MK, and for the next similar to 4000 s, radiative losses were determined to dominate over conductive losses. The radiative loss phase was accompanied by significant downflows of <= 40 km s(-1) in O V.
Conclusions. This is the first extensive study of the evolution of a canonical solar flare using both spectroscopic and broad-band instruments in conjunction with a 0-D hydrodynamic model. While our results are in broad agreement with the standard flare model, the simulations suggest that both conductive and non-thermal beam heating play important roles in heating the flare plasma during the impulsive phase of at least this event.
C1 [Raftery, C. L.; Gallagher, P. T.] Univ Dublin Trinity Coll, Sch Phys, Astrophys Res Grp, Dublin 2, Ireland.
[Raftery, C. L.; Milligan, R. O.; Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Solar Phys Lab Code 671, Greenbelt, MD 20771 USA.
RP Raftery, CL (reprint author), Univ Dublin Trinity Coll, Sch Phys, Astrophys Res Grp, Dublin 2, Ireland.
EM rafteryc@tcd.ie
RI Klimchuk, James/D-1041-2012; Gallagher, Peter/C-7717-2011
OI Klimchuk, James/0000-0003-2255-0305; Gallagher,
Peter/0000-0001-9745-0400
FU ESA/Prodex; NASA
FX C. L. R. is supported by an ESA/ Prodex grant administered by Enterprise
Ireland. R. O. M. would like to thank the NASA Postdoctoral Program for
the Fellowship award to conduct research at the NASA Goddard Space
Flight Center. The work of J. A. K. is also supported by NASA. We would
like to thank Brian Dennis, Dominic Zarro and the RHESSI team at NASA
Goddard Space Flight Center for their advice and continued support. We
would also like to thank the referee for their constructive advice in
improving the overall quality of this paper.
NR 54
TC 37
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U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2009
VL 494
IS 3
BP 1127
EP 1136
DI 10.1051/0004-6361:200810437
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406SP
UT WOS:000263315500031
ER
PT J
AU Markowitz, A
Reeves, JN
George, IM
Braito, V
Smith, R
Vaughan, S
Arevalo, P
Tombesi, F
AF Markowitz, A.
Reeves, J. N.
George, I. M.
Braito, V.
Smith, R.
Vaughan, S.
Arevalo, P.
Tombesi, F.
TI A COMPREHENSIVE X-RAY SPECTRAL ANALYSIS OF THE SEYFERT 1.5 NGC 3227
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE galaxies: active; galaxies: individual (NGC 3227); galaxies: Seyfert;
X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; LINE REGION SIZES; ADVECTION-DOMINATED
ACCRETION; XMM-NEWTON OBSERVATION; PHOTON IMAGING CAMERA; DUSTY WARM
ABSORBER; BLACK-HOLE MASS; GALAXY NGC-3227; PLASMA DIAGNOSTICS;
CONTINUUM EMISSION
AB We present results of a 100 ks XMM-Newton observation of the Seyfert 1.5 AGN NGC 3227. Our best-fit broadband model to the European Photon Imaging Camera (EPIC)-pn spectrum consists of a moderately flat (photon index of 1.57) hard X-ray power law absorbed by cold gas with a column density of 3 x 10(21) cm(2), plus a strong soft excess, modeled as a steep power law with a photon index of 3.35, absorbed by cold gas with a column density of 9 x 10(20) cm(-2). The soft excess increases in normalization by similar to 20% in similar to 20 ks, independently of the hard X-ray emission component, and the UV continuum, tracked via the Optical Monitor, also shows a strong increasing trend over the observation, consistent with reprocessing of soft X-ray emission. Warm absorber signatures are evident in both the EPIC and the Reflection Grating Spectrometer spectra; we model two absorbing layers, with ionization parameters log xi = 1.2 and 2.9 erg cm s(-1), and with similar column densities (similar to 10(21) to 2 x 10(21) cm(-2)). The outflow velocities relative to systemic of the high- and low-ionization absorbers are estimated to be -(2060(-170)(+240) ) km s(-1) and -(420(-190)(+430) ) km s(-1), respectively. The Fe K alpha line FWHM width is 7000 +/- 1500 km s(-1); its inferred distance from the black hole is consistent with the broad-line region and with the inner radius of the dust reverberation mapped by Suganuma et al. An emission feature near 6.0 keV is modeled equally well as a narrow redshifted Fe K line, possibly associated with a disk "hot spot," or as the red wing to a relativistically broadened Fe line profile. Swift Burst Alert Telescope and archival Rossi X-Ray Timing Explorer (RXTE) data suggest at most a weak Compton reflection hump (R less than or similar to 0.5), and a high- energy cutoff near 100 keV. From RXTE monitoring, we find tentative evidence for a significant fraction of the Fe line flux to track variations in the continuum on timescales < 700 days.
C1 [Markowitz, A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Reeves, J. N.] Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[George, I. M.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[George, I. M.; Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.
[Braito, V.; Smith, R.; Vaughan, S.] Univ Leicester, Xray Astron Grp, Leicester LE1 7RH, Leics, England.
[Arevalo, P.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Tombesi, F.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Tombesi, F.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Tombesi, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
RP Markowitz, A (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, MC 0424, La Jolla, CA 92093 USA.
OI Braito, Valentina/0000-0002-2629-4989
FU NASA/GSFC; NASA/IPAC Extragalactic Database; NASA; NIST Atomic Spectra
Database
FX A.M. thanks M. Elvis, A. Marscher, and D. Evans for helpful suggestions.
This work is based on an observation obtained with XMM-Newton, an ESA
science mission, and has made use of HEASARC online services, supported
by NASA/GSFC, the NASA/IPAC Extragalactic Database, operated by
JPL/California Institute of Technology under contract with NASA, and the
NIST Atomic Spectra Database.
NR 120
TC 27
Z9 27
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2009
VL 691
IS 2
BP 922
EP 945
DI 10.1088/0004-637X/691/2/922
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406OH
UT WOS:000263304300003
ER
PT J
AU Reynolds, CS
Nowak, MA
Markoff, S
Tueller, J
Wilms, J
Young, AJ
AF Reynolds, Christopher S.
Nowak, Michael A.
Markoff, Sera
Tueller, Jack
Wilms, Joern
Young, Andrew J.
TI PROBING THE ACCRETION DISK AND CENTRAL ENGINE STRUCTURE OF NGC 4258 WITH
SUZAKU AND XMM-NEWTON OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: individual (NGC 4258); galaxies: Seyfert;
X-rays: galaxies
ID X-RAY SPECTROSCOPY; BLACK-HOLE; ACTIVE NUCLEUS; GALAXY NGC-4258;
SEYFERT-GALAXIES; LUMINOSITY; M81; REFLECTION; EMISSION; BEPPOSAX
AB We present an X-ray study of the low-luminosity active galactic nucleus (AGN) in NGC 4258 using data from Suzaku, XMM-Newton, and the Swift/Burst Alert Telescope survey. We find that signatures of X-ray reprocessing by cold gas are very weak in the spectrum of this Seyfert-2 galaxy; a weak, narrow fluorescent K alpha emission line of cold iron is robustly detected in both the Suzaku and XMM-Newton spectra but at a level much below that of most other Seyfert-2 galaxies. We conclude that the circumnuclear environment of this AGN is very "clean" and lacks the Compton-thick obscuring torus of unified Seyfert schemes. From the narrowness of the iron line, together with evidence of line flux variability between the Suzaku and XMM-Newton observations, we constrain the line emitting region to be between 3 x 10(3)r(g) and 4 x 10(4)r(g) from the black hole. We show that the observed properties of the iron line can be explained if the line originates from the surface layers of a warped accretion disk. In particular, we present explicit calculations of the expected iron line from a disk warped by Lens-Thirring precession from a misaligned central black hole. Finally, the Suzaku data reveal clear evidence of large amplitude 2-10 keV variability on timescales of 50 ksec and smaller amplitude flares on timescales as short as 5-10 ksec. If associated with accretion disk processes, such rapid variability requires an origin in the innermost regions of the disk (r approximate to 10r(g) or less). Analysis of the difference spectrum between a high-and low-flux states suggests that the variable component of the X-ray emission is steeper and more absorbed than the average AGN emission, suggesting that the primary X-ray source and absorbing screen have a spatial structure on comparable scales. We note the remarkable similarity between the circumnuclear environment of NGC 4258 and another well studied low-luminosity AGN, M81*.
C1 [Reynolds, Christopher S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Reynolds, Christopher S.] Univ Maryland, Maryland Astron Ctr Theory & Computat, College Pk, MD 20742 USA.
[Nowak, Michael A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Markoff, Sera] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
[Tueller, Jack] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Wilms, Joern] Univ Erlangen Nurnberg, Astron Inst, Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
[Young, Andrew J.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England.
RP Reynolds, CS (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RI Tueller, Jack/D-5334-2012; Wilms, Joern/C-8116-2013; XRAY,
SUZAKU/A-1808-2009
OI Wilms, Joern/0000-0003-2065-5410;
FU NASA [NNX06A135G, NNX07AE97G]
FX We thank R. Mushotzky for stimulating conversations throughout this
work. C.S.R. thanks the NASA Suzaku and XMM-Newton Guest Observer
Programs for support under grants NNX06A135G and NNX07AE97G.
NR 41
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2009
VL 691
IS 2
BP 1159
EP 1167
DI 10.1088/0004-637X/691/2/1159
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406OH
UT WOS:000263304300021
ER
PT J
AU Woodruff, HC
Ireland, MJ
Tuthill, PG
Monnier, JD
Bedding, TR
Danchi, WC
Scholz, M
Townes, CH
Wood, PR
AF Woodruff, H. C.
Ireland, M. J.
Tuthill, P. G.
Monnier, J. D.
Bedding, T. R.
Danchi, W. C.
Scholz, M.
Townes, C. H.
Wood, P. R.
TI THE KECK APERTURE MASKING EXPERIMENT: SPECTRO-INTERFEROMETRY OF THREE
MIRA VARIABLES FROM 1.1 TO 3.8 mu m
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: interferometers; stars: AGB and post-AGB; stars:
individual (Mira, W Hya, R Leo); techniques: interferometric
ID M GIANTS; DUST SHELLS; R-LEONIS; EFFECTIVE TEMPERATURES; ANGULAR
DIAMETERS; K-BAND; PULSATION; STARS; TELESCOPE; IMAGES
AB We present results from a spectro-interferometric study of the Miras o Cet, R Leo, and W Hya obtained with the Keck Aperture Masking Experiment from 1998 September to 2002 July. The spectrally dispersed visibility data permit fitting with circularly symmetric brightness profiles such as a simple uniform disk (UD). The stellar angular diameter obtained over up to similar to 450 spectral channels spanning the region 1.1-3.8 mu m is presented. Use of a simple UD brightness model facilitates comparison between epochs and with existing data and theoretical models. Strong size variations with wavelength were recorded for all stars, probing zones of H(2)O, CO, OH, and dust formation. Comparison with contemporaneous spectra extracted from our data shows a strong anticorrelation between the observed angular diameter and flux. These variations consolidate the notion of a complex stellar atmosphere consisting of molecular shells with time-dependent densities and temperatures. Our findings are compared with existing data and pulsation models. The models were found to reproduce the functional form of the wavelength versus angular diameter curve well, although some departures are noted in the 2.8-3.5 mu m range.
C1 [Woodruff, H. C.; Ireland, M. J.; Tuthill, P. G.; Bedding, T. R.; Scholz, M.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Monnier, J. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Scholz, M.] Univ Heidelberg, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Townes, C. H.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94725 USA.
[Wood, P. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
RP Woodruff, HC (reprint author), Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
FU National Science Foundation; Australian Research Council; Deutsche
Forschungsgemeinschaft (MS); Keck Foundation
FX This work has been supported by grants from the National Science
Foundation, the Australian Research Council, and the Deutsche
Forschungsgemeinschaft (MS). 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 acknowledge with thanks the variable star
observations from the American Association of Variable Star Observers
(AAVSO) International Database contributed by observers worldwide and
used in this research. We also thank Albert Jones and Peter Williams for
the W Hya light curve data.
NR 42
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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 FEB 1
PY 2009
VL 691
IS 2
BP 1328
EP 1336
DI 10.1088/0004-637X/691/2/1328
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406OH
UT WOS:000263304300035
ER
PT J
AU Kashlinsky, A
Atrio-Barandela, F
Kocevski, D
Ebeling, H
AF Kashlinsky, A.
Atrio-Barandela, F.
Kocevski, D.
Ebeling, H.
TI A MEASUREMENT OF LARGE-SCALE PECULIAR VELOCITIES OF CLUSTERS OF
GALAXIES: TECHNICAL DETAILS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; cosmic microwave background; early universe;
large-scale structure of universe; methods: numerical; methods:
statistical
ID ELLIPTIC GALAXIES; LOCAL GROUP; HOT PLASMA; ANISOTROPY; UNIVERSE; FLOWS;
COSMOLOGY; SAMPLE; SPECTROSCOPY; PHOTOMETRY
AB This paper presents detailed analysis of large-scale peculiar motions derived from a sample of similar to 700 X-ray clusters and cosmic microwave background (CMB) data obtained with WMAP. We use the kinematic Sunyaev-Zeldovich (KSZ) effect combining it into a cumulative statistic that preserves the bulk motion component with the noise integrated down. Such statistic is the dipole of CMB temperature fluctuations evaluated over the pixels of the cluster catalog. To remove the cosmological CMB fluctuations the maps are filtered with a Wiener-type filter in each of the eight WMAP channels (Q, V, W) that have negligible foreground component. Our findings are as follows. The thermal SZ (TSZ) component of the clusters is described well by the Navarro-Frenk-White profile expected if the hot gas traces the dark matter in the cluster potential wells. Such gas has X-ray temperature decreasing rapidly toward the cluster outskirts, which we demonstrate results in the decrease of the TSZ component as the aperture is increased to encompass the cluster outskirts. We then detect a statistically significant dipole in the CMB pixels at cluster positions. Arising exclusively at the cluster pixels, this dipole cannot originate from the foreground or instrument noise emissions and must be produced by the CMB photons that interacted with the hot intracluster gas via the SZ effect. The dipole remains as the monopole component, due to the TSZ effect, vanishes within the small statistical noise out to the maximal aperture where we still detect the TSZ component. We demonstrate with simulations that the mask and cross-talk effects are small for our catalog and contribute negligibly to the measurements. The measured dipole thus arises from the KSZ effect produced by the coherent large-scale bulk flow motion. The cosmological implications of the measurements are discussed by us in the 2008 work of Kashlinsky et al.
C1 [Kashlinsky, A.] SSAI, Greenbelt, MD 20771 USA.
[Kashlinsky, A.] Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Atrio-Barandela, F.] Univ Salamanca, Salamanca 37008, Spain.
[Kocevski, D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Kashlinsky, A (reprint author), SSAI, Code 665, Greenbelt, MD 20771 USA.
EM alexander.kashlinsky@nasa.gov
RI Atrio-Barandela, Fernando/A-7379-2017
OI Atrio-Barandela, Fernando/0000-0002-2130-2513
NR 47
TC 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 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2009
VL 691
IS 2
BP 1479
EP 1493
DI 10.1088/0004-637X/691/2/1479
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406OH
UT WOS:000263304300046
ER
PT J
AU Dudik, RP
Satyapal, S
Marcu, D
AF Dudik, R. P.
Satyapal, S.
Marcu, D.
TI A SPITZER SPECTROSCOPIC SURVEY OF LOW-IONIZATION NUCLEAR EMISSION-LINE
REGIONS: CHARACTERIZATION OF THE CENTRAL SOURCE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: fundamental parameters; galaxies: nuclei;
infrared: galaxies; techniques: spectroscopic
ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; DWARF SEYFERT
NUCLEI; X-RAY; SPACE-TELESCOPE; NEARBY GALAXIES; OPTICAL SPECTROSCOPY;
LUMINOSITY FUNCTION; SPECTROGRAPH IRS; RADIO PROPERTIES
AB We have conducted a comprehensive mid-infrared (IR) spectroscopic investigation of 67 low-ionization nuclear emission line regions (LINERs) using archival observations from the high-resolution modules of the Infrared Spectrograph on board the Spitzer Space Telescope. Using the [Ne V] 14 and 24 mu m lines as active galactic nuclei (AGNs) diagnostics, we detect active black holes in 39% of the galaxies in our sample, many of which show no signs of activity in either the optical or X-ray bands. In particular, a detailed comparison of multiwavelength diagnostics shows that optical studies fail to detect AGNs in galaxies with large far-IR luminosities. These observations emphasize that the nuclear power source in a large percentage of LINERs is obscured in the optical. Indeed, the majority of LINERs show mid-IR [Ne V] 14/[Ne V] 24 mu m flux ratios well below the theoretical low-density limit, suggesting that there is substantial extinction toward even the [Ne V]-emitting region. Combining optical, X-ray, and mid-IR diagnostics, we find an AGN detection rate in LINERs of 74%, higher than previously reported statistics of the fraction of LINERs hosting AGNs. The [Ne V] 24 mu m /[O IV] 26 mu m mid-IR line flux ratio in AGN-LINERs is similar to that of standard AGNs, suggesting that the spectral energy distribution of the intrinsic optical/UV continuum is similar in the two. This result is in contrast to previous suggestions of a UV deficit in the intrinsic broadband continuum emission in AGN-LINERs. Consistent with our finding of extinction to the [Ne V]-emitting region, we propose that extinction may also be responsible for the observed optical/UV deficit seen in at least some AGN-LINERs.
C1 [Dudik, R. P.; Satyapal, S.; Marcu, D.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA.
[Dudik, R. P.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD USA.
[Dudik, R. P.] USN Observ, Washington, DC 20392 USA.
[Dudik, R. P.] Res Support Instruments, Lanham, MD 20706 USA.
RP Dudik, RP (reprint author), George Mason Univ, Dept Phys & Astron, MS 3F3,4400 Univ Dr, Fairfax, VA 22030 USA.
EM rpdudik@usno.navy.mil
FU NASA [NAG5-11432, NAG03-4134X]; NASA Graduate Student Research Program
FX S.S. gratefully acknowledges financial support from NASA grant
NAG5-11432 and NAG03-4134X. R.P.D gratefully acknowledges financial
support from the NASA Graduate Student Research Program.
NR 65
TC 38
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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 FEB 1
PY 2009
VL 691
IS 2
BP 1501
EP 1524
DI 10.1088/0004-637X/691/2/1501
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406OH
UT WOS:000263304300048
ER
PT J
AU Pellizzoni, A
Pilia, M
Possenti, A
Fornari, F
Caraveo, P
Del Monte, E
Mereghetti, S
Tavani, M
Argan, A
Trois, A
Burgay, M
Chen, A
Cognard, I
Costa, E
D'Amico, N
Esposito, P
Evangelista, Y
Feroci, M
Fuschino, F
Giuliani, A
Halpern, J
Hobbs, G
Hotan, A
Johnston, S
Kramer, M
Longo, F
Manchester, RN
Marisaldi, M
Palfreyman, J
Weltevrede, P
Barbiellini, G
Boffelli, F
Bulgarelli, A
Cattaneo, PW
Cocco, V
D'Ammando, F
De Paris, G
Di Cocco, G
Donnarumma, I
Fiorini, M
Froysland, T
Galli, M
Gianotti, F
Harding, A
Labanti, C
Lapshov, I
Lazzarotto, F
Lipari, P
Mauri, F
Morselli, A
Pacciani, L
Perotti, F
Picozza, P
Prest, M
Pucella, G
Rapisarda, M
Rappoldi, A
Soffitta, P
Trifoglio, M
Vallazza, E
Vercellone, S
Vittorini, V
Zambra, A
Zanello, D
Pittori, C
Verrecchia, F
Preger, B
Santolamazza, P
Giommi, P
Salotti, L
AF Pellizzoni, A.
Pilia, M.
Possenti, A.
Fornari, F.
Caraveo, P.
Del Monte, E.
Mereghetti, S.
Tavani, M.
Argan, A.
Trois, A.
Burgay, M.
Chen, A.
Cognard, I.
Costa, E.
D'Amico, N.
Esposito, P.
Evangelista, Y.
Feroci, M.
Fuschino, F.
Giuliani, A.
Halpern, J.
Hobbs, G.
Hotan, A.
Johnston, S.
Kramer, M.
Longo, F.
Manchester, R. N.
Marisaldi, M.
Palfreyman, J.
Weltevrede, P.
Barbiellini, G.
Boffelli, F.
Bulgarelli, A.
Cattaneo, P. W.
Cocco, V.
D'Ammando, F.
De Paris, G.
Di Cocco, G.
Donnarumma, I.
Fiorini, M.
Froysland, T.
Galli, M.
Gianotti, F.
Harding, A.
Labanti, C.
Lapshov, I.
Lazzarotto, F.
Lipari, P.
Mauri, F.
Morselli, A.
Pacciani, L.
Perotti, F.
Picozza, P.
Prest, M.
Pucella, G.
Rapisarda, M.
Rappoldi, A.
Soffitta, P.
Trifoglio, M.
Vallazza, E.
Vercellone, S.
Vittorini, V.
Zambra, A.
Zanello, D.
Pittori, C.
Verrecchia, F.
Preger, B.
Santolamazza, P.
Giommi, P.
Salotti, L.
TI HIGH-RESOLUTION TIMING OBSERVATIONS OF SPIN-POWERED PULSARS WITH THE
AGILE GAMMA-RAY TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: observations; pulsars: general; pulsars: individual (Vela,
Crab, Geminga, PSR B 1706-44); stars: neutron
ID CRAB-LIKE PULSARS; HIGH-ENERGY; X-RAY; VELA PULSAR; SLOT GAPS; INTERNAL
TEMPERATURE; OUTER MAGNETOSPHERE; EGRET OBSERVATIONS; PSR J0218+4232;
NEUTRON STARS
AB Astro-rivelatore Gamma ad Immagini LEggero (AGILE) is a small gamma-ray astronomy satellite mission of the Italian Space Agency dedicated to high-energy astrophysics launched in 2007 April. Its similar to 1 mu s absolute time tagging capability coupled with a good sensitivity in the 30MeV-30 GeV range, with simultaneous X-ray monitoring in the 18-60 keV band, makes it perfectly suited for the study of gamma-ray pulsars following up on the Compton Gamma RayObservatory/EGRET heritage. In this paper, we present the first AGILE timing results on the known gamma-ray pulsars Vela, Crab, Geminga, and B1706-44. The data were collected from 2007 July to 2008 April, exploiting the mission Science Verification Phase, the Instrument Timing Calibration, and the early Observing Pointing Program. Thanks to its large field of view, AGILE collected a large number of gamma-ray photons from these pulsars (similar to 10,000 pulsed counts for Vela) in only few months of observations. The coupling of AGILE timing capabilities, simultaneous radio/X-ray monitoring, and new tools aimed at precise photon phasing, also exploiting timing noise correction, unveiled new interesting features at the submillisecond level in the pulsars' high-energy light curves.
C1 [Pellizzoni, A.; Pilia, M.; Fornari, F.; Caraveo, P.; Mereghetti, S.; Chen, A.; Esposito, P.; Giuliani, A.; Fiorini, M.; Perotti, F.; Vercellone, S.; Zambra, A.] INAF IASF Milano, I-20133 Milan, Italy.
[Pilia, M.; Possenti, A.; Burgay, M.; D'Amico, N.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, Italy.
[Del Monte, E.; Tavani, M.; Argan, A.; Trois, A.; Costa, E.; Evangelista, Y.; Feroci, M.; Cocco, V.; D'Ammando, F.; De Paris, G.; Di Cocco, G.; Donnarumma, I.; Lapshov, I.; Lazzarotto, F.; Pacciani, L.; Pucella, G.; Soffitta, P.] INAF IASF Roma, I-00133 Rome, Italy.
[Tavani, M.; D'Ammando, F.; Froysland, T.; Vittorini, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Chen, A.; Froysland, T.] CIFS Torino, I-10133 Turin, Italy.
[Cognard, I.] CNRS, Lab Phys & Chim Environm, F-45071 Orleans, France.
[D'Amico, N.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, Italy.
[Esposito, P.; Boffelli, F.; Cattaneo, P. W.; Mauri, F.; Rappoldi, A.] Ist Nazl Fis Nucl, I-27100 Pavia, Italy.
[Esposito, P.; Boffelli, F.] Univ Pavia, Dipartimento Fis Nucl & Teor, I-27100 Pavia, Italy.
[Fuschino, F.; Marisaldi, M.; Bulgarelli, A.; Gianotti, F.; Labanti, C.; Trifoglio, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Halpern, J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Hobbs, G.; Johnston, S.; Manchester, R. N.; Weltevrede, P.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Hotan, A.] Curtin Univ Technol, Perth, WA 6000, Australia.
[Kramer, M.] Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England.
[Longo, F.; Barbiellini, G.; Vallazza, E.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Longo, F.; Barbiellini, G.; Vallazza, E.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy.
[Palfreyman, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Galli, M.] ENEA Bologna, I-40059 Medicina, BO, Italy.
[Harding, A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Lipari, P.; Zanello, D.] INFN Roma La Sapienza, I-00185 Rome, Italy.
[Morselli, A.; Picozza, P.] INFN Roma Tor Vergata, I-00133 Rome, Italy.
[Prest, M.] Univ Insubria, Dipartimento Fis, I-22100 Como, Italy.
[Rapisarda, M.] ENEA Roma, I-00044 Frascati, Roma, Italy.
[Pittori, C.; Verrecchia, F.; Preger, B.; Santolamazza, P.; Giommi, P.] ASI ASDC, I-00044 Frascati, Roma, Italy.
[Salotti, L.] ASI, I-00198 Rome, Italy.
RP Pellizzoni, A (reprint author), INAF IASF Milano, Via E Bassini 15, I-20133 Milan, Italy.
EM alberto@iasf-milano.inaf.it
RI D'Amico, Nichi/A-5715-2009; Harding, Alice/D-3160-2012; Morselli,
Aldo/G-6769-2011; Lazzarotto, Francesco/J-4670-2012; Trifoglio,
Massimo/F-5302-2015; Pittori, Carlotta/C-7710-2016;
OI trois, alessio/0000-0002-3180-6002; Donnarumma,
Immacolata/0000-0002-4700-4549; Pellizzoni, Alberto
Paolo/0000-0002-4590-0040; Caraveo, Patrizia/0000-0003-2478-8018; PREST,
MICHELA/0000-0003-3161-4454; Verrecchia, Francesco/0000-0003-3455-5082;
Marisaldi, Martino/0000-0002-4000-3789; Vercellone,
Stefano/0000-0003-1163-1396; MEREGHETTI, SANDRO/0000-0003-3259-7801;
Esposito, Paolo/0000-0003-4849-5092; Tavani, Marco/0000-0003-2893-1459;
Soffitta, Paolo/0000-0002-7781-4104; Picozza,
Piergiorgio/0000-0002-7986-3321; Burgay, Marta/0000-0002-8265-4344;
Fuschino, Fabio/0000-0003-2139-3299; Gianotti,
Fulvio/0000-0003-4666-119X; Lazzarotto, Francesco/0000-0003-4871-4072;
Costa, Enrico/0000-0003-4925-8523; Fiorini, Mauro/0000-0001-8297-1983;
Bulgarelli, Andrea/0000-0001-6347-0649; giommi,
paolo/0000-0002-2265-5003; Morselli, Aldo/0000-0002-7704-9553;
Trifoglio, Massimo/0000-0002-2505-3630; Pittori,
Carlotta/0000-0001-6661-9779; Palfreyman, Jim/0000-0001-8691-8039;
galli, marcello/0000-0002-9135-3228; Cattaneo, Paolo
Walter/0000-0001-6877-6882; Pacciani, Luigi/0000-0001-6897-5996;
Labanti, Claudio/0000-0002-5086-3619; Feroci, Marco/0000-0002-7617-3421
FU NASA XMM-Newton [NNX06AH58G, NNX07AU65]; Italian Minister of Research
(MIUR) [PRIN-MIUR 2005]; ESA Member States and NASA
FX We acknowledge D. A. Smith, D. J. Thompson, and G. Tosti of GLAST Team
for useful discussions on multiwavelength observations of pulsars and
for their comments on the paper draft. J. P. H. was supported by NASA
XMM-Newton grants NNX06AH58G and NNX07AU65G. A. P. and M. B. received
financial support from the Italian Minister of Research (MIUR) under
national program PRIN-MIUR 2005. The Parkes radio telescope is part of
the Australia Telescope, which is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO.
XMM-Newton is an ESA science mission with instruments and contributions
directly funded by ESA Member States and NASA.
NR 64
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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 2009
VL 691
IS 2
BP 1618
EP 1633
DI 10.1088/0004-637X/691/2/1618
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406OH
UT WOS:000263304300056
ER
PT J
AU Burlaga, LF
Ness, NF
Acuna, MH
AF Burlaga, L. F.
Ness, N. F.
Acuna, M. H.
TI MAGNETIC FIELD STRENGTH FLUCTUATIONS AND TEMPERATURE IN THE HELIOSHEATH
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; interplanetary medium; solar wind; Sun: magnetic
fields
ID WIND TERMINATION SHOCK; VOYAGER 2 OBSERVATIONS; SOLAR-WIND; PLASMA; AU;
STATISTICS; UPSTREAM
AB We analyze high-resolution observations of the magnetic field strength B made by Voyager 2 (V2) in the heliosheath behind the termination shock from 2007 day of year 245-301. The magnetic field strength is highly variable during intervals of several hours, with large jumps in B on scales of minutes to a few hours. The distributions of increments of B are kurtotic on scales from 48 s to 1.7 hr owing to large tails produced by the jumps in B, and they are approximately Gaussian on the scale of 6.8 hr. The distributions of increments of B are described accurately by the q-Gaussian distribution of nonextensive statistical mechanics on scales of 48 s to 6.8 hr. The entropic index q is a function of scale, and it has a broad peak between 192 and 3072 s centered at approximate to 770 s. The characteristic width of the jumps in B(t) in four intervals is L approximate to 150,000 km, consistent with the scale of the maximum value of the entropic index. The characteristic width L is a multiple n of the pickup proton gyroradius, where 1 <= n <= 17, approximately. From L we estimate that the pickup proton temperature T in the post-shock flow is of the order of 2.5 x 10(6) K if n = 9 or 1.3 x 10(7) K if n = 4. Given more accurate estimates of n, it will be possible to use this method to estimate T in the heliosheath as a function of time and distance.
C1 [Burlaga, L. F.] NASA, Geophys Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Acuna, M. H.] NASA, Planetary Magnetospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Burlaga, LF (reprint author), NASA, Geophys Phys Lab, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA.
EM Leonard.F.Burlaga@NASA.gov; nfnudel@yahoo.com; Mario.H.Acuna@NASA.gov
FU Catholic University of America [NNX07AW09G]
FX The data in this Letter are from the magnetic field experiment on
Voyager 2. N. F. N. was partially supported by grant NNX07AW09G to the
Catholic University of America. T. McClanahan and S. Kramer carried out
the processing of the data. The "zero-offset tables" were computed by D.
Berdichevsky.
NR 34
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PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
PY 2009
VL 691
IS 2
BP L82
EP L86
DI 10.1088/0004-637X/691/2/L82
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 404JW
UT WOS:000263148800005
ER
PT J
AU Gopalswamy, N
Yashiro, S
Temmer, M
Davila, J
Thompson, WT
Jones, S
McAteer, RTJ
Wuelser, JP
Freeland, S
Howard, RA
AF Gopalswamy, N.
Yashiro, S.
Temmer, M.
Davila, J.
Thompson, W. T.
Jones, S.
McAteer, R. T. J.
Wuelser, J-P
Freeland, S.
Howard, R. A.
TI EUV WAVE REFLECTION FROM A CORONAL HOLE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun:
magnetic fields; Sun: UV radiation
ID EIT WAVES; PROPAGATING DISTURBANCE; MORETON/EIT WAVE; MASS EJECTION;
SOLAR CORONA; MHD WAVES; EMISSION; ALPHA; FLARE; SUN
AB We report on the detection of EUV wave reflection from a coronal hole, as observed by the Solar Terrestrial Relations Observatory mission. The EUV wave was associated with a coronal mass ejection (CME) erupting near the disk center. It was possible to measure the kinematics of the reflected waves for the first time. The reflected waves were generally slower than the direct wave. One of the important implications of the wave reflection is that the EUV transients are truly a wave phenomenon. The EUV wave reflection has implications for CME propagation, especially during the declining phase of the solar cycle when there are many low-latitude coronal holes.
C1 [Gopalswamy, N.; Yashiro, S.; Davila, J.; Thompson, W. T.; Jones, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Temmer, M.] Graz Univ, IGAM Inst Phys, A-8010 Graz, Austria.
[McAteer, R. T. J.] Trinity Coll Dublin, Astrophys Res Grp, Dublin 2, Ireland.
[Howard, R. A.] USN, Res Lab, Washington, DC 20375 USA.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA.
EM nat.gopalswamy@nasa.gov
RI McAteer, R. T. James/D-3736-2011; Gopalswamy, Nat/D-3659-2012; Thompson,
William/D-7376-2012;
OI Temmer, Manuela/0000-0003-4867-7558
FU NASA [NNX08AD60A]; Austrian Academy of Sciences [APART 11262]; Marie
Curie Intra-European
FX S. Y. acknowledges support by NASA (NNX08AD60A). M. T. acknowledges
support by the project APART 11262 of the Austrian Academy of Sciences.
R. T. J. Mc. A. is a Marie Curie Intra-European Fellow. The SECCHI
instrument was constructed by a consortium of international
institutions: the Naval Research Laboratory (USA), the Lockheed Martin
Solar and Astrophysical Laboratory (USA), the NASA Goddard Space Flight
Center (USA), the Max-Planck-Institut fur Sonnensystemforschung
(Germany), the Centre Spatial de Liege (Belgium), the University of
Birmingham (UK), the Rutherford Appleton Laboratory (UK), the Institut
d'Optique (France), and the Institute d' Astrophysique Spatiale
(France).
NR 31
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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 1
PY 2009
VL 691
IS 2
BP L123
EP L127
DI 10.1088/0004-637X/691/2/L123
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 404JW
UT WOS:000263148800015
ER
PT J
AU Harra, LK
Williams, DR
Wallace, AJ
Magara, T
Hara, H
Tsuneta, S
Sterling, AC
Doschek, GA
AF Harra, L. K.
Williams, D. R.
Wallace, A. J.
Magara, T.
Hara, H.
Tsuneta, S.
Sterling, A. C.
Doschek, G. A.
TI CORONAL NONTHERMAL VELOCITY FOLLOWING HELICITY INJECTION BEFORE AN
X-CLASS FLARE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona; Sun: flares
ID EUV IMAGING SPECTROMETER; MAGNETIC-FIELDS; SOLAR-FLARES; HINODE;
EVOLUTION; MISSION; PHASE
AB We explore the "pre-flare" behavior of the corona in a three-day period building up to an X-class flare on 2006 December 13 by analyzing EUV spectral profiles from the Hinode EUV Imaging Spectrometer (EIS) instrument. We found an increase in the coronal spectral line widths, beginning after the time of saturation of the injected helicity as measured by Magara & Tsuneta. In addition, this increase in line widths (indicating nonthermal motions) starts before any eruptive activity occurs. The Hinode EIS has the sensitivity to measure changes in the buildup to a flare many hours before the flare begins.
C1 [Harra, L. K.; Williams, D. R.; Wallace, A. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Magara, T.; Hara, H.; Tsuneta, S.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Sterling, A. C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Doschek, G. A.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
RP Harra, LK (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM lkh@mssl.ucl.ac.uk
RI Williams, David/E-6676-2011; Magara, Tetsuya/E-2406-2013;
OI Williams, David/0000-0001-9922-8117; Harra, Louise/0000-0001-9457-6200
FU JAXA; NAOJ; STFC; NASA; ESA; NSC
FX 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 (USA), ESA, and NSC (Norway). G. A. D. is
supported by funds from the NASA Hinode program and the NRL 6.1 basic
research program.
NR 18
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
PY 2009
VL 691
IS 2
BP L99
EP L102
DI 10.1088/0004-637X/691/2/L99
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 404JW
UT WOS:000263148800009
ER
PT J
AU Jennings, DE
Flasar, FM
Kunde, VG
Samuelson, RE
Pearl, JC
Nixon, CA
Carlson, RC
Mamoutkine, AA
Brasunas, JC
Guandique, E
Achterberg, RK
Bjoraker, GL
Romani, PN
Segura, ME
Albright, SA
Elliott, MH
Tingley, JS
Calcutt, S
Coustenis, A
Courtin, R
AF Jennings, D. E.
Flasar, F. M.
Kunde, V. G.
Samuelson, R. E.
Pearl, J. C.
Nixon, C. A.
Carlson, R. C.
Mamoutkine, A. A.
Brasunas, J. C.
Guandique, E.
Achterberg, R. K.
Bjoraker, G. L.
Romani, P. N.
Segura, M. E.
Albright, S. A.
Elliott, M. H.
Tingley, J. S.
Calcutt, S.
Coustenis, A.
Courtin, R.
TI TITAN'S SURFACE BRIGHTNESS TEMPERATURES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE infrared: solar system; planets and satellites: individual (Titan);
radiation mechanisms: thermal; radiative transfer
ID COMPOSITE INFRARED SPECTROMETER; GENERAL-CIRCULATION MODEL; ATMOSPHERIC
TEMPERATURES; SATURN SYSTEM; SPECTRA; WINDS; ABUNDANCES; VOYAGER-1;
DYNAMICS; METHANE
AB Radiance from the surface of Titan can be detected from space through a spectral window of low opacity in the thermal infrared at 19 mu m (530 cm-1). By combining Composite Infrared Spectrometer observations from Cassini's first four years, we have mapped the latitude distribution of zonally averaged surface brightness temperatures. The measurements are corrected for atmospheric opacity as derived from the dependence of radiance on the emission angle. At equatorial latitudes near the Huygens landing site, the surface brightness temperature is found to be 93.7 +/- 0.6K, in excellent agreement with the in situ measurement. Temperature decreases toward the poles, reaching 90.5 +/- 0.8K at 87 degrees N and 91.7 +/- 0.7K at 88 degrees S. The meridional distribution of temperature has a maximum near 10 degrees S, consistent with Titan's late northern winter.
C1 [Jennings, D. E.; Flasar, F. M.; Kunde, V. G.; Samuelson, R. E.; Pearl, J. C.; Nixon, C. A.; Carlson, R. C.; Mamoutkine, A. A.; Brasunas, J. C.; Guandique, E.; Achterberg, R. K.; Bjoraker, G. L.; Romani, P. N.; Segura, M. E.; Albright, S. A.; Elliott, M. H.; Tingley, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kunde, V. G.; Samuelson, R. E.; Nixon, C. A.; Achterberg, R. K.] Univ Maryland, College Pk, MD 20742 USA.
[Carlson, R. C.] Catholic Univ Amer, Washington, DC 20064 USA.
[Mamoutkine, A. A.; Guandique, E.; Elliott, M. H.; Tingley, J. S.] Adnet Syst Inc, Rockville, MD 20852 USA.
[Segura, M. E.] Perotsystems, Fairfax, VA 22031 USA.
[Albright, S. A.] Syst & Software Designers Inc, Clarksville, MD 21029 USA.
[Calcutt, S.] Univ Oxford, Oxford OX1 3PU, England.
[Coustenis, A.; Courtin, R.] Observ Meudon, LESIA, F-92195 Meudon, France.
RP Jennings, DE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM donald.e.jennings@nasa.gov
RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Romani,
Paul/D-2729-2012; Bjoraker, Gordon/D-5032-2012; Jennings,
Donald/D-7978-2012; brasunas, john/I-2798-2013;
OI Nixon, Conor/0000-0001-9540-9121; Calcutt, Simon/0000-0002-0102-3170
FU NASA
FX We acknowledge support from NASA's Cassini mission and Cassini Data
Analysis Program. We appreciate helpful discussions with R. Lorenz, M.
Janssen, and B. Bezard relating their work to our observations.
NR 40
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PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
PY 2009
VL 691
IS 2
BP L103
EP L105
DI 10.1088/0004-637X/691/2/L103
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 404JW
UT WOS:000263148800010
ER
PT J
AU Stecker, FW
Scully, ST
AF Stecker, Floyd W.
Scully, Sean T.
TI IS THE UNIVERSE MORE TRANSPARENT TO GAMMA RAYS THAN PREVIOUSLY THOUGHT?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE diffuse radiation; galaxies: individual (3C279); gamma rays: theory
ID BROAD-LINE REGION; GALAXY COUNTS; 3C 279; ABSORPTION; RADIATION;
SPECTRA; ENERGY; BLAZARS; ISOCAM; 3C-279
AB The MAGIC collaboration has recently reported the detection of the strong gamma-ray blazar 3C279 during a 1-2 day flare. They have used their spectral observations to draw conclusions regarding upper limits on the opacity of the universe to high-energy gamma-rays and, by implication, upper limits on the extragalactic mid-infrared background radiation. In this Letter, we examine the effect of gamma-ray absorption by the extragalactic infrared radiation on intrinsic spectra for this blazar and compare our results with the observational data on 3C279. We find agreement with our previous results, contrary to the recent assertion of the MAGIC group that the universe is more transparent to gamma-rays than our calculations indicate. Our analysis indicates that in the energy range between similar to 80 and similar to 500 GeV, 3C279 has a best-fit intrinsic spectrum with a spectral index of similar to 1.78 using our fast evolution model and similar to 2.19 using our baseline model. However, we also find that spectral indices in the range of 1.0-3.0 are almost as equally acceptable as the best-fit spectral indices. Assuming the same intrinsic spectral index for this flare as for the 1991 flare from 3C279 observed by EGRET, viz., 2.02, which lies between our best-fit indices, we estimate that the MAGIC flare was similar to 3 times brighter than the EGRET flare observed 15 years earlier.
C1 [Stecker, Floyd W.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Scully, Sean T.] James Madison Univ, Dept Phys, Harrisonburg, VA 22807 USA.
RP Stecker, FW (reprint author), NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Floyd.W.Stecker@nasa.gov; scullyst@jmu.edu
RI Stecker, Floyd/D-3169-2012
FU Thomas F.& KateMiller Jeffress Memorial Trust [J-805]
FX We thank Rudolf Bock for sending us a list of data on the spectrum of
3C279 observed by MAGIC. S. T. S. gratefully acknowledges partial
support from the Thomas F.& KateMiller Jeffress Memorial Trust grant
J-805.
NR 25
TC 20
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 1
PY 2009
VL 691
IS 2
BP L91
EP L94
DI 10.1088/0004-637X/691/2/L91
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 404JW
UT WOS:000263148800007
ER
PT J
AU Hinshaw, G
Weiland, JL
Hill, RS
Odegard, N
Larson, D
Bennett, CL
Dunkley, J
Gold, B
Greason, MR
Jarosik, N
Komatsu, E
Nolta, MR
Page, L
Spergel, DN
Wollack, E
Halpern, M
Kogut, A
Limon, M
Meyer, SS
Tucker, GS
Wright, EL
AF Hinshaw, G.
Weiland, J. L.
Hill, R. S.
Odegard, N.
Larson, D.
Bennett, C. L.
Dunkley, J.
Gold, B.
Greason, M. R.
Jarosik, N.
Komatsu, E.
Nolta, M. R.
Page, L.
Spergel, D. N.
Wollack, E.
Halpern, M.
Kogut, A.
Limon, M.
Meyer, S. S.
Tucker, G. S.
Wright, E. L.
TI FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: DATA
PROCESSING, SKY MAPS, AND BASIC RESULTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic microwave background; cosmology: observations; early universe;
dark matter; space vehicles; space vehicles: instruments;
instrumentation: detectors; telescopes
ID ANGULAR POWER SPECTRUM; GALAXY REDSHIFT SURVEY; SYSTEMATIC-ERROR LIMITS;
WMAP OBSERVATIONS; DARK ENERGY; DATA SET; CONSTRAINTS; DESIGN
AB We present new full-sky temperature and polarization maps in five frequency bands from 23 to 94 GHz, based on data from the first five years of the Wilkinson Microwave Anisotropy Probe (WMAP) sky survey. The new maps are consistent with previous maps and are more sensitive. The five-year maps incorporate several improvements in data processing made possible by the additional years of data and by a more complete analysis of the instrument calibration and in-flight beam response. We present several new tests for systematic errors in the polarization data and conclude that W-band polarization data is not yet suitable for cosmological studies, but we suggest directions for further study. We do find that Ka-band data is suitable for use; in conjunction with the additional years of data, the addition of Ka band to the previously used Q- and V-band channels significantly reduces the uncertainty in the optical depth parameter, tau. Further scientific results from the five-year data analysis are presented in six companion papers and are summarized in Section 7 of this paper. With the five-year WMAP data, we detect no convincing deviations from the minimal six-parameter Lambda CDM model: a flat universe dominated by a cosmological constant, with adiabatic and nearly scale-invariant Gaussian fluctuations. Using WMAP data combined with measurements of Type Ia supernovae and Baryon Acoustic Oscillations in the galaxy distribution, we find (68% CL uncertainties): Omega(b)h(2) = 0.02267(-0.00059)(+0.00058), Omega(c)h(2) = 0.1131 +/- 0.0034, Omega(Lambda) = 0.726 +/- 0.015, n(s) = 0.960 +/- 0.013, tau = 0.084 +/- 0.016, and Delta(2)(R) = (2.445 +/- 0.096) x 10(-9) at k = 0.002 Mpc(-1). From these we derive sigma(8) = 0.812 +/- 0.026, H(0) = 70.5 +/- 1.3 km s(-1) Mpc(-1), Omega(b) = 0.0456 +/- 0.0015, Omega(c) = 0.228 +/- 0.013, Omega(m)h(2) = 0.1358(-0.0036)(+0.0037), z(reion) = 10.9 +/- 1.4, and t(0) = 13.72 +/- 0.12 Gyr. The new limit on the tensor-to-scalar ratio is r < 0.22 (95% CL), while the evidence for a running spectral index is insignificant, dn(s)/d ln k = - 0.028 +/- 0.020 (68% CL). We obtain tight, simultaneous limits on the (constant) dark energy equation of state and the spatial curvature of the universe: - 0.14 < 1 + w < 0.12 (95% CL) and -0.0179 < Omega(k) < 0.0081 (95% CL). The number of relativistic degrees of freedom, expressed in units of the effective number of neutrino species, is found to be N(eff) = 4.4 +/- 1.5 (68% CL), consistent with the standard value of 3.04. Models with N(eff) = 0 are disfavored at >99.5% confidence. Finally, new limits on physically motivated primordial non-Gaussianity parameters are -9 < f(NL)(local) < 111 (95% CL) and -151 < f(NL)(equil) < 253 (95% CL) for the local and equilateral models, respectively.
C1 [Hinshaw, G.; Wollack, E.; Kogut, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Weiland, J. L.; Hill, R. S.; Odegard, N.; Greason, M. R.] Adnet Syst Inc, Lanham, MD 20706 USA.
[Larson, D.; Bennett, C. L.; Gold, B.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Dunkley, J.; Jarosik, N.; Page, L.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Dunkley, J.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Dunkley, J.] Univ Oxford, Oxford OX1 3RH, England.
[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.
[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.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Astrophys, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Phys, 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 Hinshaw, G (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
EM Gary.F.Hinshaw@nasa.gov
RI Wollack, Edward/D-4467-2012; Kogut, Alan/D-6293-2012; Komatsu,
Eiichiro/A-4361-2011; Spergel, David/A-4410-2011
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]; Alfred P. Sloan Research Fellowship
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. EK acknowledges support from an
Alfred P. Sloan Research Fellowship. This research has made use of
NASA's Astrophysics Data System Bibliographic Services. We acknowledge
use of the HEALPix, CAMB, CMBFAST, and CosmoMC packages.
NR 49
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JI Astrophys. J. Suppl. Ser.
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SC Astronomy & Astrophysics
GA 406EI
UT WOS:000263277400001
ER
PT J
AU Hill, RS
Weiland, JL
Odegard, N
Wollack, E
Hinshaw, G
Larson, D
Bennett, CL
Halpern, M
Page, L
Dunkley, J
Gold, B
Jarosik, N
Kogut, A
Limon, M
Nolta, MR
Spergel, DN
Tucker, GS
Wright, EL
AF Hill, R. S.
Weiland, J. L.
Odegard, N.
Wollack, E.
Hinshaw, G.
Larson, D.
Bennett, C. L.
Halpern, M.
Page, L.
Dunkley, J.
Gold, B.
Jarosik, N.
Kogut, A.
Limon, M.
Nolta, M. R.
Spergel, D. N.
Tucker, G. S.
Wright, E. L.
TI FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: BEAM MAPS
AND WINDOW FUNCTIONS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic microwave background; planets and satellites: individual
(Jupiter, Mars, Saturn); space vehicles: instruments; telescopes
ID BRIGHTNESS TEMPERATURES; WMAP OBSERVATIONS; SUBMILLIMETER; PROFILES;
PLANETS
AB Cosmology and other scientific results from the Wilkinson Microwave Anisotropy Probe (WMAP) mission require an accurate knowledge of the beam patterns in flight. While the degree of beam knowledge for the WMAP one-year and three-year results was unprecedented for a CMB experiment, we have significantly improved the beam determination as part of the five-year data release. Physical optics fits are done on both the A and the B sides for the first time. The cutoff scale of the fitted distortions on the primary mirror is reduced by a factor of similar to 2 from previous analyses. These changes enable an improvement in the hybridization of Jupiter data with beam models, which is optimized with respect to error in the main beam solid angle. An increase in main-beam solid angle of similar to 1% is found for the V2 and W1-W4 differencing assemblies. Although the five-year results are statistically consistent with previous ones, the errors in the five-year beam transfer functions are reduced by a factor of similar to 2 as compared to the three-year analysis. We present radiometry of the planet Jupiter as a test of the beam consistency and as a calibration standard; for an individual differencing assembly, errors in the measured disk temperature are similar to 0.5%.
C1 [Hill, R. S.; Weiland, J. L.; Odegard, N.] Adnet Syst Inc, Lanham, MD 20706 USA.
[Wollack, E.; Hinshaw, G.; Kogut, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Larson, D.; Bennett, C. L.; Gold, B.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Page, L.; Dunkley, J.; Jarosik, N.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Dunkley, J.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Dunkley, J.] Univ Oxford, Oxford OX1 3RH, England.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 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 Hill, RS (reprint author), Adnet Syst Inc, 7515 Mission Dr,Suite A100, Lanham, MD 20706 USA.
EM Robert.S.Hill@nasa.gov
RI Kogut, Alan/D-6293-2012; 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]
FX We thank Chris Barnes for his many contributions to the study of WMAP
beams, and especially for his development of the physical optics
model-fitting procedure. We acknowledge use of the HEALPix package
(Gorski et al. 2005). 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.
NR 20
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PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD FEB
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SC Astronomy & Astrophysics
GA 406EI
UT WOS:000263277400002
ER
PT J
AU Gold, B
Bennett, CL
Hill, RS
Hinshaw, G
Odegard, N
Page, L
Spergel, DN
Weiland, JL
Dunkley, J
Halpern, M
Jarosik, N
Kogut, A
Komatsu, E
Larson, D
Meyer, SS
Nolta, MR
Wollack, E
Wright, EL
AF Gold, B.
Bennett, C. L.
Hill, R. S.
Hinshaw, G.
Odegard, N.
Page, L.
Spergel, D. N.
Weiland, J. L.
Dunkley, J.
Halpern, M.
Jarosik, N.
Kogut, A.
Komatsu, E.
Larson, D.
Meyer, S. S.
Nolta, M. R.
Wollack, E.
Wright, E. L.
TI FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: GALACTIC
FOREGROUND EMISSION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic microwave background; cosmology: observations; diffuse radiation;
Galaxy: halo; Galaxy: structure; ISM: structure
ID RADIO-CONTINUUM EMISSION; WMAP OBSERVATIONS; SPINNING DUST; TENTATIVE
DETECTION; 408 MHZ; RADIATION; POLARIZATION; GRAINS; SKY; ABSORPTION
AB We present a new estimate of foreground emission in the Wilkinson Microwave Anisotropy Probe (WMAP) data, using a Markov chain Monte Carlo method. The new technique delivers maps of each foreground component for a variety of foreground models with estimates of the uncertainty of each foreground component, and it provides an overall goodness-of-fit estimate. The resulting foreground maps are in broad agreement with those from previous techniques used both within the collaboration and by other authors. We find that for WMAP data, a simple model with power-law synchrotron, free-free, and thermal dust components fits 90% of the sky with a reduced chi(2)(v) of 1.14. However, the model does not work well inside the Galactic plane. The addition of either synchrotron steepening or a modified spinning dust model improves the fit. This component may account for up to 14% of the total flux at the Ka band (33 GHz). We find no evidence for foreground contamination of the cosmic microwave background temperature map in the 85% of the sky used for cosmological analysis.
C1 [Gold, B.; Bennett, C. L.; Larson, D.] 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.
[Page, L.; Dunkley, J.; Jarosik, N.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Spergel, D. N.; Dunkley, J.] Princeton Univ, Princeton Ctr Theoret Phys, 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.
[Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Astrophys, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Phys, 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.
[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 Kogut, Alan/D-6293-2012; Komatsu, Eiichiro/A-4361-2011; Spergel,
David/A-4410-2011; Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD FEB
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SC Astronomy & Astrophysics
GA 406EI
UT WOS:000263277400003
ER
PT J
AU Wright, EL
Chen, X
Odegard, N
Bennett, CL
Hill, RS
Hinshaw, G
Jarosik, N
Komatsu, E
Nolta, MR
Page, L
Spergel, DN
Weiland, JL
Wollack, E
Dunkley, J
Gold, B
Halpern, M
Kogut, A
Larson, D
Limon, M
Meyer, SS
Tucker, GS
AF Wright, E. L.
Chen, X.
Odegard, N.
Bennett, C. L.
Hill, R. S.
Hinshaw, G.
Jarosik, N.
Komatsu, E.
Nolta, M. R.
Page, L.
Spergel, D. N.
Weiland, J. L.
Wollack, E.
Dunkley, J.
Gold, B.
Halpern, M.
Kogut, A.
Larson, D.
Limon, M.
Meyer, S. S.
Tucker, G. S.
TI FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: SOURCE
CATALOG
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; cosmic microwave background; quasars: general; radio
continuum: galaxies; surveys
ID WMAP OBSERVATIONS; POINT SOURCES; BEAM PROFILES; RADIO-SOURCES; MISSION;
PREDICTIONS
AB We present the list of point sources found in the Wilkinson Microwave Anisotropy Probe (WMAP) five-year maps. The technique used in the first-year and three-year analyses now finds 390 point sources, and the five-year source catalog is complete for regions of the sky away from the Galactic plane to a 2 Jy limit, with SNR > 4.7 in all bands in the least covered parts of the sky. The noise at high frequencies is still mainly radiometer noise, but at low frequencies the cosmic microwave background (CMB) anisotropy is the largest uncertainty. A separate search of CMB-free V-W maps finds 99 sources of which all but one can be identified with known radio sources. The sources seen by WMAP are not strongly polarized. Many of the WMAP sources show significant variability from year to year, with more than a 2: 1 range between the minimum and maximum fluxes.
C1 [Wright, E. L.; Chen, X.] UCLA Phys & Astron, Los Angeles, CA 90095 USA.
[Odegard, N.; Hill, R. S.; Weiland, J. L.] Adnet Syst Inc, Lanham, MD 20706 USA.
[Bennett, C. L.; Gold, B.; Larson, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hinshaw, G.; Wollack, E.; Kogut, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jarosik, N.; Page, L.; Dunkley, J.] Princeton Univ, Dept Phys, Princeton, NJ 08544 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.
[Spergel, D. N.; Dunkley, J.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Spergel, D. N.] Princeton Univ, Princeton Ctr Theoret Phys, 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.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Astrophys, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Phys, 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.
RP Wright, EL (reprint author), UCLA Phys & Astron, POB 951547, Los Angeles, CA 90095 USA.
EM wright@astro.ucla.edu
RI Kogut, Alan/D-6293-2012; 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]
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. E. K. acknowledges support from an
Alfred P. Sloan Research Fellowship. This research has made use of
NASA's Astrophysics Data System Bibliographic Services. We acknowledge
use of the HEALPix, CAMB, and CMBFAST packages.
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SC Astronomy & Astrophysics
GA 406EI
UT WOS:000263277400004
ER
PT J
AU Nolta, MR
Dunkley, J
Hill, RS
Hinshaw, G
Komatsu, E
Larson, D
Page, L
Spergel, DN
Bennett, CL
Gold, B
Jarosik, N
Odegard, N
Weiland, JL
Wollack, E
Halpern, M
Kogut, A
Limon, M
Meyer, SS
Tucker, GS
Wright, EL
AF Nolta, M. R.
Dunkley, J.
Hill, R. S.
Hinshaw, G.
Komatsu, E.
Larson, D.
Page, L.
Spergel, D. N.
Bennett, C. L.
Gold, B.
Jarosik, N.
Odegard, N.
Weiland, J. L.
Wollack, E.
Halpern, M.
Kogut, A.
Limon, M.
Meyer, S. S.
Tucker, G. S.
Wright, E. L.
TI FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: ANGULAR
POWER SPECTRA
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmic microwave background; cosmological parameters; cosmology:
observations; early universe; large-scale structure of universe; space
vehicles: instruments
ID COSMIC BACKGROUND IMAGER; WMAP OBSERVATIONS; CMB TEMPERATURE; 2003
FLIGHT; POLARIZATION; PREDICTIONS; BOOMERANG; MISSION
AB We present the temperature and polarization angular power spectra of the cosmic microwave background derived from the first five years of Wilkinson Microwave Anisotropy Probe data. The five-year temperature spectrum is cosmic variance limited up to multipole l = 530, and individual l-modes have signal-to-noise ratio S/N > 1 for l < 920. The best-fitting six-parameter Lambda CDM model has a reduced chi(2) for l = 33-1000 of chi(2)/nu = 1.06, with a probability to exceed of 9.3%. There is now significantly improved data near the third peak which leads to improved cosmological constraints. The temperature-polarization correlation is seen with high significance. After accounting for foreground emission, the low-l reionization feature in the EE power spectrum is preferred by Delta chi(2) = 19.6 for optical depth tau = 0.089 by the EE data alone, and is now largely cosmic variance limited for l = 2-6. There is no evidence for cosmic signal in the BB, TB, or EB spectra after accounting for foreground emission. We find that, when averaged over l = 2-6, l(l + 1)CBB(l)(BB)/(2 pi) < 0.15 mu K(2) (95% CL).
C1 [Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Dunkley, J.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Dunkley, J.; Page, L.; Jarosik, N.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Dunkley, J.] Univ Oxford, Oxford OX1 3RH, England.
[Hill, R. S.; Odegard, N.; Weiland, J. L.] Adnet Syst Inc, Lanham, MD 20706 USA.
[Hinshaw, G.; Wollack, E.; Kogut, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Larson, D.; Bennett, C. L.; Gold, B.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[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.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Astrophys, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Phys, 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 Nolta, MR (reprint author), Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada.
EM nolta@cita.utoronto.ca
RI Kogut, Alan/D-6293-2012; 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
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JI Astrophys. J. Suppl. Ser.
PD FEB
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PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406EI
UT WOS:000263277400005
ER
PT J
AU Dunkley, J
Komatsu, E
Nolta, MR
Spergel, DN
Larson, D
Hinshaw, G
Page, L
Bennett, CL
Gold, B
Jarosik, N
Weiland, JL
Halpern, M
Hill, RS
Kogut, A
Limon, M
Meyer, SS
Tucker, GS
Wollack, E
Wright, EL
AF Dunkley, J.
Komatsu, E.
Nolta, M. R.
Spergel, D. N.
Larson, D.
Hinshaw, G.
Page, L.
Bennett, C. L.
Gold, B.
Jarosik, N.
Weiland, J. L.
Halpern, M.
Hill, R. S.
Kogut, A.
Limon, M.
Meyer, S. S.
Tucker, G. S.
Wollack, E.
Wright, E. L.
TI FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: LIKELIHOODS
AND PARAMETERS FROM THE WMAP DATA
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Review
DE cosmic microwave background; cosmology: observations; early universe;
polarization
ID DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; COSMIC BACKGROUND IMAGER;
GALAXY REDSHIFT SURVEY; LY-ALPHA FOREST; SEQUENCE CLUSTER SURVEY;
PRIMORDIAL HELIUM ABUNDANCE; LUMINOUS RED GALAXIES; LARGE-SCALE
STRUCTURE; IMPROVED COSMOLOGICAL CONSTRAINTS
AB This paper focuses on cosmological constraints derived from analysis of WMAP data alone. A simple Lambda CDM cosmological model fits the five-year WMAP temperature and polarization data. The basic parameters of the model are consistent with the three-year data and now better constrained: Omega(b)h(2) = 0.02273 +/- 0.00062, Omega(c)h(2) = 0.1099 +/- 0.0062, Omega(Lambda) = 0.742 +/- 0.030, n(s) = 0.963(-0.015)(+0.014), tau = 0.087 +/- 0.017, and sigma(8) = 0.796 +/- 0.036, with h = 0.719(-0.027)(+0.026). With five years of polarization data, we have measured the optical depth to reionization, tau > 0, at 5 sigma significance. The redshift of an instantaneous reionization is constrained to be z(reion) = 11.0 +/- 1.4 with 68% confidence. The 2 sigma lower limit is zreion > 8.2, and the 3 sigma limit is z(reion) > 6.7. This excludes a sudden reionization of the universe at z = 6 atmore than 3.5 sigma significance, suggesting that reionization was an extended process. Using two methods for polarized foreground cleaning we get consistent estimates for the optical depth, indicating an error due to the foreground treatment of tau similar to 0.01. This cosmological model also fits small-scale cosmic microwave background (CMB) data, and a range of astronomical data measuring the expansion rate and clustering of matter in the universe. We find evidence for the first time in the CMB power spectrum for a nonzero cosmic neutrino background, or a background of relativistic species, with the standard three light neutrino species preferred over the best-fit Lambda CDM model with N-eff = 0 at > 99.5% confidence, and N-eff > 2.3 (95% confidence limit (CL)) when varied. The five-year WMAP data improve the upper limit on the tensor-to-scalar ratio, r < 0.43 (95% CL), for power-law models, and halve the limit on r for models with a running index, r < 0.58 (95% CL). With longer integration we find no evidence for a running spectral index, with dn(s)/d ln k = -0.037 +/- 0.028, and find improved limits on isocurvature fluctuations. The current WMAP-only limit on the sum of the neutrino masses is Sigma m(v) < 1.3 eV (95% CL), which is robust, to within 10%, to a varying tensor amplitude, running spectral index, or dark energy equation of state.
C1 [Dunkley, J.; Page, L.; Jarosik, N.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Dunkley, J.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Dunkley, J.] Univ Oxford, Oxford OX1 3RH, England.
[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.
[Spergel, D. N.] Princeton Univ, Princeton Ctr Theoret Phys, Princeton, NJ 08544 USA.
[Larson, D.; Bennett, C. L.; Gold, B.] 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.
[Weiland, J. L.; Hill, R. S.] Adnet Syst Inc, Lanham, MD 20706 USA.
[Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Tucker, G. S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Astrophys, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Phys, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, EFI, Chicago, IL 60637 USA.
[Wright, E. L.] UCLA Phys & Astron, Los Angeles, CA 90095 USA.
RP Dunkley, J (reprint author), Princeton Univ, Dept Phys, Jadwin Hall, Princeton, NJ 08544 USA.
EM j.dunkley@physics.ox.ac.uk
RI Wollack, Edward/D-4467-2012; Kogut, Alan/D-6293-2012; Komatsu,
Eiichiro/A-4361-2011; Spergel, David/A-4410-2011
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. E. K. acknowledges support from an
Alfred P. Sloan Research Fellowship. We thank Antony Lewis for
discussion about lensing in CAMB, Will Percival for discussion and
provision of BAO data, Catherine Heymans, Jonathan Benjamin, and Richard
Massey for discussion of weak lensing data, Michael Wood-Vasey for
discussion of ESSENCE supernova data, Eric Aubourg for discussion of
SNLS supernova data, Gary Steigman for discussion of BBN constraints,
Bruce Draine and Todd Thompson for discussion of dust and synchrotron
emission. This research has made use of NASA's Astrophysics Data System
Bibliographic Services. We acknowledge the use of the HEALPix, CAMB,
CMBFAST, and CosmoMC packages.
NR 318
TC 1153
Z9 1155
U1 4
U2 20
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD FEB
PY 2009
VL 180
IS 2
BP 306
EP 329
DI 10.1088/0067-0049/180/2/306
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406EI
UT WOS:000263277400006
ER
PT J
AU Komatsu, E
Dunkley, J
Nolta, MR
Bennett, CL
Gold, B
Hinshaw, G
Jarosik, N
Larson, D
Limon, M
Page, L
Spergel, DN
Halpern, M
Hill, RS
Kogut, A
Meyer, SS
Tucker, GS
Weiland, JL
Wollack, E
Wright, EL
AF Komatsu, E.
Dunkley, J.
Nolta, M. R.
Bennett, C. L.
Gold, B.
Hinshaw, G.
Jarosik, N.
Larson, D.
Limon, M.
Page, L.
Spergel, D. N.
Halpern, M.
Hill, R. S.
Kogut, A.
Meyer, S. S.
Tucker, G. S.
Weiland, J. L.
Wollack, E.
Wright, E. L.
TI FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS:
COSMOLOGICAL INTERPRETATION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Review
DE cosmic microwave background; cosmology: observations; dark matter; early
universe; instrumentation: detectors; space vehicles: instruments;
telescopes
ID LARGE-SCALE STRUCTURE; PRIMORDIAL POWER SPECTRUM; COSMIC BACKGROUND
IMAGER; HUBBLE-SPACE-TELESCOPE; 3-POINT CORRELATION-FUNCTION;
HIGH-REDSHIFT SUPERNOVAE; EQUATION-OF-STATE; ISOTHERMAL DENSITY
PERTURBATIONS; INFLATIONARY UNIVERSE SCENARIO; LUMINOUS RED GALAXIES
AB The Wilkinson Microwave Anisotropy Probe (WMAP) 5-year data provide stringent limits on deviations from the minimal, six-parameter. cold dark matter model. We report these limits and use them to constrain the physics of cosmic inflation via Gaussianity, adiabaticity, the power spectrum of primordial fluctuations, gravitational waves, and spatial curvature. We also constrain models of dark energy via its equation of state, parity-violating interaction, and neutrino properties, such as mass and the number of species. We detect no convincing deviations from the minimal model. The six parameters and the corresponding 68% uncertainties, derived from the WMAP data combined with the distance measurements from the Type Ia supernovae (SN) and the Baryon Acoustic Oscillations (BAO) in the distribution of galaxies, are: Omega(b)h(2) = 0.02267(-0.00059)(+0.00058), Omega(c)h(2) = 0.1131 +/- 0.0034, Omega(Lambda) = 0.726 +/- 0.015, n(s) = 0.960 +/- 0.013, tau = 0.084 +/- 0.016, and Delta(2)(R) = (2.445 +/- 0.096) x 10(-9) at k = 0.002 Mpc(-1). From these, we derive sigma(8) = 0.812 +/- 0.026, H-0 = 70.5 +/- 1.3 kms(-1) Mpc(-1), Omega(b) = 0.0456 +/- 0.0015, Omega(c) = 0.228 +/- 0.013, Omega(m)h(2) = 0.1358(-0.0036)(+0.0037), z(reion) = 10.9 +/- 1.4, and t(0) = 13.72 +/- 0.12 Gyr. With the WMAP data combined with BAO and SN, we find the limit on the tensor-to-scalar ratio of r < 0.22 (95% CL), and that n(s) > 1 is disfavored even when gravitational waves are included, which constrains the models of inflation that can produce significant gravitational waves, such as chaotic or power-law inflation models, or a blue spectrum, such as hybrid inflation models. We obtain tight, simultaneous limits on the (constant) equation of state of dark energy and the spatial curvature of the universe: -0.14 < 1 + w(0) < 0.12 (95% CL) and -0.0179 < Omega(k) < 0.0081 (95% CL). We provide a set of "WMAP distance priors," to test a variety of dark energy models with spatial curvature. We test a time-dependent w with a present value constrained as -0.33 < 1 + w(0) < 0.21 (95% CL). Temperature and dark matter fluctuations are found to obey the adiabatic relation to within 8.9% and 2.1% for the axion-type and curvaton-type dark matter, respectively. The power spectra of TB and EB correlations constrain a parity-violating interaction, which rotates the polarization angle and converts E to B. The polarization angle could not be rotated more than -5 degrees.9 < Delta alpha < 2 degrees.4 (95% CL) between the decoupling and the present epoch. We find the limit on the total mass of massive neutrinos of Sigma m(v) < 0.67 eV (95% CL), which is free from the uncertainty in the normalization of the large-scale structure data. The number of relativistic degrees of freedom (dof), expressed in units of the effective number of neutrino species, is constrained as N-eff = 4.4 +/- 1.5 (68%), consistent with the standard value of 3.04. Finally, quantitative limits on physically-motivated primordial non-Gaussianity parameters are -9 < f(NL)(local) < 111 (95% CL) and -151 < f(NL)(equil) < 253 (95% CL) for the local and equilateral models, respectively.
C1 [Komatsu, E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Dunkley, J.; Jarosik, N.; Page, L.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Dunkley, J.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Dunkley, J.] Univ Oxford, Oxford OX1 3RH, England.
[Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[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.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Spergel, D. N.] Princeton Univ, Princeton Ctr Theoret Sci, Princeton, NJ 08544 USA.
[Halpern, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hill, R. S.; Weiland, J. L.] Adnet Syst Inc, Lanham, MD 20706 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Astrophys, Chicago, IL 60637 USA.
[Meyer, S. S.] Univ Chicago, KICP, Dept Phys, 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, Dept Astron, 2511 Speedway,RLM 15-306, Austin, TX 78712 USA.
EM komatsu@astro.as.utexas.edu
RI Kogut, Alan/D-6293-2012; 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
NR 509
TC 3338
Z9 3352
U1 38
U2 154
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD FEB
PY 2009
VL 180
IS 2
BP 330
EP 376
DI 10.1088/0067-0049/180/2/330
PG 47
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 406EI
UT WOS:000263277400007
ER
PT J
AU Folk, CL
Remington, RW
Wu, SC
AF Folk, Charles L.
Remington, Roger W.
Wu, Shu-Chieh
TI Additivity of abrupt onset effects supports nonspatial distraction, not
the capture of spatial attention
SO ATTENTION PERCEPTION & PSYCHOPHYSICS
LA English
DT Article
ID SELECTIVE ATTENTION; PERCEPTUAL LOAD; CONTROL SETTINGS; VISUAL-SEARCH;
SINGLETONS
AB In a recent article, Schreij, Owens, and Theeuwes (2008) reported that abruptly onsetting distractors produce costs in performance even when spatial-cuing effects confirm the presence of a top-down set for color. The authors argued that these results show that abruptly onsetting new objects capture attention independent of a top-down set and, thus, provide conclusive evidence against the theory that attentional capture is contingent on top-down attentional control settings (Folk, Remington, & Johnston, 1992). In the following article, we argue that, contrary to the conclusion drawn by Schreij et al., their own data (1) disconfirm the claim that their abrupt onsets captured spatial attention and (2) are consistent with nonspatial interference accounts of singleton-distractor effects. In support of the nonspatial account, we show that in a paradigm similar to Schreij et al.'s, distractors that do not capture attention can nonetheless influence responses to a target. We conclude that the results of Schreij et al. do not represent a challenge to contingent capture theory.
C1 [Folk, Charles L.] Villanova Univ, Dept Psychol, Villanova, PA 19085 USA.
[Remington, Roger W.] Univ Queensland, Brisbane, Qld, Australia.
[Wu, Shu-Chieh] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Folk, CL (reprint author), Villanova Univ, Dept Psychol, Villanova, PA 19085 USA.
EM charles.folk@villanova.edu
NR 13
TC 25
Z9 26
U1 2
U2 9
PU PSYCHONOMIC SOC INC
PI AUSTIN
PA 1710 FORTVIEW RD, AUSTIN, TX 78704 USA
SN 1943-3921
J9 ATTEN PERCEPT PSYCHO
JI Atten. Percept. Psychophys.
PD FEB
PY 2009
VL 71
IS 2
BP 308
EP 313
DI 10.3758/APP.71.2.308
PG 6
WC Psychology; Psychology, Experimental
SC Psychology
GA 402XP
UT WOS:000263046700008
PM 19304620
ER
PT J
AU Scheuring, RA
Mathers, CH
Jones, JA
Wear, ML
AF Scheuring, Richard A.
Mathers, Charles H.
Jones, Jeffrey A.
Wear, Mary L.
TI Musculoskeletal Injuries and Minor Trauma in Space: Incidence and Injury
Mechanisms in US Astronauts
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE astronaut; NASA; strain; sprain; abrasion; contusion; laceration;
dislocation; EVA; injury
ID BACK-PAIN; MICROGRAVITY; PROGRAM; HEALTH
AB Introduction: Astronauts have sustained musculoskeletal injuries and minor trauma in space, but our knowledge of these injuries is based mainly on anecdotal reports. The purpose of our study was to catalog and analyze all in-flight musculoskeletal injuries occurring throughout the U.S. space program to date. Methods: A database on in-flight musculoskeletal injuries among U.S. astronauts was generated from records at the Johnson Space Center. Results: A total of 219 in-flight musculoskeletal injuries were identified. 198 occurring in men and 21 in women. Incidence over the course of the space program was 0.021 per flight day for men and 0.015 for women. Hand injuries represented the most common location of injuries, with abrasions and small lacerations representing common manifestations of these injuries. Crew activity in the spacecraft cabin such as translating between modules, aerobic and resistive exercise, and injuries caused by the extravehicular activity (EVA) suit components were the leading causes of musculoskeletal injuries. Exercise-related injuries accounted for an incidence of 0.003 per day and exercise is the most frequent source of injuries in astronauts living aboard the International Space Station (ISS). Interaction with EVA suit components accounted for an incidence of 0.26 injuries per EVA. Discussion: Hand injuries were among the most common events occurring in U.S. astronauts during spaceilight. Identifying the incidence and mechanism of in-flight injuries will allow flight surgeons to quantify the amount of medical supplies needed in the design of next-generation spacecraft. Engineers can use in-flight injury data to further refine the EVA suit and vehicle components.
C1 [Scheuring, Richard A.; Jones, Jeffrey A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Mathers, Charles H.] Univ Texas Galveston, Med Branch, Galveston, TX 77550 USA.
[Wear, Mary L.] Wyle Labs, Houston, TX USA.
RP Scheuring, RA (reprint author), NASA, Lyndon B Johnson Space Ctr, SD4,2101 NASA Pkwy, Houston, TX 77058 USA.
EM richard.a.scheuring@nasa.gov
NR 15
TC 29
Z9 29
U1 2
U2 5
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD FEB
PY 2009
VL 80
IS 2
BP 117
EP 124
DI 10.3357/ASEM.2270.2009
PG 8
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 399RX
UT WOS:000262818100008
PM 19198198
ER
PT J
AU Whitcomb, J
Moghaddam, M
McDonald, K
Kellndorfer, J
Podest, E
AF Whitcomb, Jane
Moghaddam, Mahta
McDonald, Kyle
Kellndorfer, Josef
Podest, Erika
TI Mapping vegetated wetlands of Alaska using L-band radar satellite
imagery
SO CANADIAN JOURNAL OF REMOTE SENSING
LA English
DT Article
ID SYNTHETIC-APERTURE RADAR; ERS-1 SAR DATA; CARBON BALANCE; METHANE
EMISSIONS; THEMATIC MAPPER; INVENTORY MAPS; NORTHERN; MODEL; AREA;
CLASSIFICATION
AB Wetlands act as major sinks and sources of important atmospheric greenhouse gases and can switch between atmospheric sink and source in response to climatic and anthropogenic forces in ways that are poorly understood. Despite their importance in the carbon cycle, the locations, types, and extents of northern wetlands are not accurately known. We have used two seasons of L-band synthetic aperture radar (SAR) imagery to produce a thematic map of wetlands throughout Alaska. The classification is developed using the Random Forests decision tree algorithm with training and testing data compiled from the National Wetlands Inventory (NWI) and the Alaska Geospatial Data Clearinghouse (AGDC). Mosaics of summer and winter Japanese Earth Resources Satellite 1 (JERS-1) SAR imagery were employed together with other inputs and ancillary datasets, including the SAR backscatter texture map, slope and elevation maps from a digital elevation model (DEM), an open-water map, a map of proximity to water, data collection dates, and geographic latitude. The accuracy of the resulting thematic map was quantified using extensive ground reference data. This approach distinguished as many as nine different wetlands classes, which were aggregated into four vegetated wetland classes. The per-class average error rate for aggregate wetlands classes ranged between 5.0% and 30.5%, and the total aggregate accuracy calculated based on all classified pixels was 89.5%. As the first high-resolution large-scale synoptic wetlands map of Alaska, this product provides an initial basis for improved characterization of land-atmosphere CH(4) and CO(2) fluxes and climate change impacts associated with thawing soils and changes in extent and drying of wetland ecosystems.
C1 [McDonald, Kyle; Podest, Erika] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Whitcomb, Jane; Moghaddam, Mahta] Univ Michigan, Dept Elect Engn & Comp Sci, Ann Arbor, MI 48109 USA.
[Kellndorfer, Josef] Woods Hole Res Ctr, Falmouth, MA 02536 USA.
RP McDonald, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kyle.mcdonald@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX The North America JERS-1 SAR mosaics were generated by the Jet
Propulsion Laboratory (JPL), California Institute of Technology, within
the framework of the JAXA Global Boreal Forest Mapping (GBFM) project.
Image copyright JAXA/METI North America mosaic products are available on
DVD ROM and can be ordered from
www.asf.alaska.edu/dataproducts/unrestricted.html. This work was carried
out at the University of Michigan, Ann Arbor, and JPL under contract
with the National Aeronautics and Space Administration (NASA).
NR 83
TC 44
Z9 44
U1 1
U2 15
PU CANADIAN AERONAUTICS SPACE INST
PI KANATA
PA 350 TERRY FOX DR, STE 104, KANATA, ON K2K 2W5, CANADA
SN 1712-7971
J9 CAN J REMOTE SENS
JI Can. J. Remote Sens.
PD FEB
PY 2009
VL 35
IS 1
BP 54
EP 72
PG 19
WC Remote Sensing
SC Remote Sensing
GA 449GT
UT WOS:000266319500004
ER
PT J
AU Chen, YH
Del Genio, AD
AF Chen, Yonghua
Del Genio, Anthony D.
TI Evaluation of tropical cloud regimes in observations and a general
circulation model
SO CLIMATE DYNAMICS
LA English
DT Article
DE Cluster analysis; Tropical cloud regimes; GISS Model E; ARSCL; ISCCP D1;
MJO
ID MADDEN-JULIAN OSCILLATION; VERTICAL STRUCTURE; WESTERN PACIFIC;
SATELLITE; ECMWF; IDENTIFICATION; SIMULATIONS; VARIABILITY; COMBINATION;
CONVECTION
AB Tropical cloud regimes defined by cluster analysis of International Satellite Cloud Climatology Project (ISCCP) cloud top pressure (CTP)-optical thickness distributions and ISCCP-like Goddard Institute for Space Studies (GISS) general circulation model (GCM) output are analyzed in this study. The observations are evaluated against radar-lidar cloud-top profiles from the atmospheric radiation measurement (ARM) Program active remote sensing of cloud layers (ARSCL) product at two tropical locations and by placing them in the dynamical context of the Madden-Julian oscillation (MJO). ARSCL highest cloud-top profiles indicate that differences among some of the six ISCCP regimes may not be as prominent as suggested by ISCCP at the ARM tropical sites. An experimental adjustment of the ISCCP CTPs to produce cloud-top height profiles consistent with ARSCL eliminates the independence between those regimes. Despite these ambiguities, the ISCCP regime evolution over different phases of the MJO is consistent with existing MJO mechanisms, but with a greater mix of cloud types in each phase than is usually envisioned. The GISS Model E GCM produces two disturbed and two suppressed regimes when vertical convective condensate transport is included in the model's cumulus parameterization. The primary model deficiencies are the absence of an isolated cirrus regime, a lack of mid-level cloud relative to ARSCL, and a tendency for occurrences of specific parameterized processes such as deep and shallow convection and stratiform low cloud formation to not be associated preferentially with any single cloud regime.
C1 Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Chen, Yonghua; Del Genio, Anthony D.] Inst Space Studies, New York, NY 10025 USA.
[Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Chen, YH (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA.
EM ychen@giss.nasa.gov
RI Del Genio, Anthony/D-4663-2012
OI Del Genio, Anthony/0000-0001-7450-1359
FU Cloud Modeling and Analysis Initiative of the NASA Modeling and Analysis
Program; DOE Atmospheric Radiation Measurement Program
FX This study was supported by the Cloud Modeling and Analysis Initiative
of the NASA Modeling and Analysis Program and by the DOE Atmospheric
Radiation Measurement Program. The authors thank Keith Williams, Allyson
Sheffield, and George Tselioudis for helpful discussions of cluster
analysis. The ISCCP data were obtained from Allyson Sheffield, and the
ARSCL data from the ARM archive at Oak Ridge National Laboratory. The
k-means clustering algorithm code was downloaded from
http://isccp.giss.nasa.gov/tcluster.html. The authors are also thankful
for the two anonymous reviewers who provided helpful suggestions that
improved the original manuscript.
NR 40
TC 44
Z9 45
U1 3
U2 8
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 2009
VL 32
IS 2-3
BP 355
EP 369
DI 10.1007/s00382-008-0386-6
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 389IO
UT WOS:000262086300014
ER
PT J
AU Lynn, BH
Healy, R
Druyan, LM
AF Lynn, Barry H.
Healy, Richard
Druyan, Leonard M.
TI Quantifying the sensitivity of simulated climate change to model
configuration
SO CLIMATIC CHANGE
LA English
DT Article
ID WESTERN UNITED-STATES; CONVECTIVE ADJUSTMENT SCHEME; SURFACE-HYDROLOGY
MODEL; REGIONAL CLIMATE; BOUNDARY-LAYER; PART I; PARAMETERIZATION
SCHEMES; RADIATIVE-TRANSFER; CHANGE SCENARIOS; MESOSCALE MODEL
AB This study used "factor separation" to quantify the sensitivity of simulated present and future surface temperatures and precipitation to alternative regional climate model physics components. The method enables a quantitative isolation of the effects of using each physical component as well as the combined effect of two or more components. Simulation results are presented from eight versions of the Mesoscale Modeling System Version 5 (MM5), one-way nested within one version of the Goddard Institute for Space Studies Atmosphere-Ocean Global Climate Model (GISS AOGCM). The MM5 simulations were made at 108 km grid spacing over the continental United States for five summers in the 1990s and 2050s. Results show that the choice of cumulus convection parameterization is the most important "factor" in the simulation of contemporary surface summer temperatures and precipitation over both the western and eastern USA. The choice of boundary layer scheme and radiation package also increases the range of model simulation results. Moreover, the alternative configurations give quite different results for surface temperature and precipitation in the 2050s. For example, simulated 2050s surface temperatures by the scheme with the coolest 1990s surface temperatures are comparable to 1990s temperatures produced by other schemes. The study analyzes the spatial distribution of 1990s to 2050s projected changes in the surface temperature for the eight MM5 versions. The predicted surface temperature change at a given grid point, averaged over all eight model configurations, is generally about twice the standard deviation of the eight predicted changes, indicating relative consensus among the different model projections. Factor separation analysis indicates that the choice of cumulus parameterization is the most important modeling factor amongst the three tested contributing to the computed 1990s to 2050s surface temperature change, although enhanced warming over many areas is also attributable to synergistic effects of changing all three model components. Simulated ensemble mean precipitation changes, however, are very small and generally smaller than the inter-model standard deviations. The MM5 versions therefore offer little consensus regarding 1990s to 2050s changes in precipitation rates.
C1 [Druyan, Leonard M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Lynn, Barry H.] Hebrew Univ Jerusalem, Dept Earth Sci, Efrat, Israel.
[Lynn, Barry H.] Weather It Is Ltd, Efrat, Israel.
[Healy, Richard] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Druyan, Leonard M.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
RP Druyan, LM (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM LDruyan@giss.nasa.gov
RI Healy, Richard/J-9214-2015
OI Healy, Richard/0000-0002-5098-8921
FU U.S. Environmental Protection Agency's Science to Achieve Results (STAR)
program [R828733]; NSF [ATM-0652518]; NASA [NNX07AI93G]; NASA Goddard
Institute for Space Studies
FX This research was supported by Grant R828733 from the U.S. Environmental
Protection Agency's Science to Achieve Results (STAR) program, NSF Grant
ATM-0652518, NASA Grant NNX07AI93G and the NASA Climate Variability and
Climate Change Programs. It was part of a broader program within the
Climate Impacts Group of the NASA Goddard Institute for Space Studies.
We thank Drs. Filippo Giorgi, Hann- Ming Henry Juang, Mike Iacono and
three anonymous reviewers for their helpful comments.
NR 56
TC 11
Z9 11
U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0165-0009
J9 CLIMATIC CHANGE
JI Clim. Change
PD FEB
PY 2009
VL 92
IS 3-4
BP 275
EP 298
DI 10.1007/s10584-008-9494-x
PG 24
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 397GC
UT WOS:000262649900003
ER
PT J
AU Sjogreen, B
Yee, HC
AF Sjogreen, Bjorn
Yee, H. C.
TI Variable High Order Multiblock Overlapping Grid Methods for Mixed Steady
and Unsteady Multiscale Viscous Flows
SO COMMUNICATIONS IN COMPUTATIONAL PHYSICS
LA English
DT Article
CT 7th International Conference on Spectral and High Order Methods
CY JUN 18-22, 2007
CL Chinese Acad Sci, Beijing, PEOPLES R CHINA
HO Chinese Acad Sci
DE Multiblock grid; overset grids; high order numerical methods; blunt body
hypersonic flows; mixed steady and unsteady flows
ID SCHEMES
AB Flows containing steady or nearly steady strong shocks on parts of the flow field, and unsteady turbulence with shocklets on other parts of the flow field are difficult to capture accurately and efficiently employing the same numerical scheme, even under the multiblock grid or adaptive grid refinement framework. While sixth-order or higher-order shock-capturing methods are appropriate for unsteady turbulence with shocklets, third-order or lower shock-capturing methods are more effective for strong steady or nearly steady shocks in terms of convergence. In order to minimize the short comings of low order and high order shock-capturing schemes for the subject flows, a multiblock overlapping grid with different types of spatial schemes and orders of accuracy on different blocks is proposed. The recently developed single block high order filter scheme in generalized geometries for Navier Stokes and magnetohydrodynamics systems is extended to multiblock overlapping grid geometries. The first stage in validating the high order overlapping approach with several test cases is included.
C1 [Sjogreen, Bjorn] Lawrence Livermore Natl Lab, Ctr Appl Sci Comp, Livermore, CA 94551 USA.
[Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Sjogreen, B (reprint author), Lawrence Livermore Natl Lab, Ctr Appl Sci Comp, Livermore, CA 94551 USA.
EM sjogreen2@llnl.gov; helen.m.yee@nasa.gov
NR 11
TC 8
Z9 8
U1 0
U2 0
PU GLOBAL SCIENCE PRESS
PI WANCHAI
PA ROOM 2303, OFFICER TOWER, CONVENTION PLAZA, 1 HARBOUR ROAD, WANCHAI,
HONG KONG 00000, PEOPLES R CHINA
SN 1815-2406
J9 COMMUN COMPUT PHYS
JI Commun. Comput. Phys.
PD FEB
PY 2009
VL 5
IS 2-4
BP 730
EP 744
PG 15
WC Physics, Mathematical
SC Physics
GA 410FT
UT WOS:000263563600030
ER
PT J
AU Sun, YZ
Wang, ZJ
Liu, Y
AF Sun, Yuzhi
Wang, Z. J.
Liu, Yen
TI Efficient Implicit Non-linear LU-SGS Approach for Compressible Flow
Computation Using High-Order Spectral Difference Method
SO COMMUNICATIONS IN COMPUTATIONAL PHYSICS
LA English
DT Article
CT 7th International Conference on Spectral and High Order Methods
CY JUN 18-22, 2007
CL Chinese Acad Sci, Beijing, PEOPLES R CHINA
HO Chinese Acad Sci
DE High order; unstructured grids; spectral difference; Navier-Stokes;
implicit
ID FINITE VOLUME METHOD; NAVIER-STOKES EQUATIONS; UNSTRUCTURED GRIDS;
CONSERVATION-LAWS; TRIANGULAR MESHES; BASIC FORMULATION; EULER
EQUATIONS; ELEMENT METHOD; SCHEMES; SYSTEMS
AB An implicit non-linear lower-upper symmetric Gauss-Seidel (LU-SGS) solution algorithm has been developed for a high-order spectral difference Navier-Stokes solver on unstructured hexahedral grids. The non-linear LU-SGS solver is preconditioned by a block element matrix, and the system of equations is then solved with the LU decomposition approach. The large sparse Jacobian matrix is computed numerically, resulting in extremely simple operations for arbitrarily complex residual operators. Several inviscid and viscous test cases were performed to evaluate the performance. The implicit solver has shown speedup of 1 to 2 orders of magnitude over the multi-stage Runge-Kutta time integration scheme.
C1 [Sun, Yuzhi; Wang, Z. J.] Iowa State Univ, Dept Aerosp Engn, Ames, IA 50011 USA.
[Liu, Yen] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Wang, ZJ (reprint author), Iowa State Univ, Dept Aerosp Engn, Ames, IA 50011 USA.
EM sunyuzhi@iastate.edu; zjw@iastate.edu; Yen.Liu@nasa.gov
RI Wang, Z.J./A-9628-2010
OI Wang, Z.J./0000-0002-6203-6303
NR 44
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U1 0
U2 4
PU GLOBAL SCIENCE PRESS
PI WANCHAI
PA ROOM 2303, OFFICER TOWER, CONVENTION PLAZA, 1 HARBOUR ROAD, WANCHAI,
HONG KONG 00000, PEOPLES R CHINA
SN 1815-2406
J9 COMMUN COMPUT PHYS
JI Commun. Comput. Phys.
PD FEB
PY 2009
VL 5
IS 2-4
BP 760
EP 778
PG 19
WC Physics, Mathematical
SC Physics
GA 410FT
UT WOS:000263563600032
ER
PT J
AU Nair, RD
Choi, HW
Tufo, HM
AF Nair, R. D.
Choi, H. -W.
Tufo, H. M.
TI Computational aspects of a scalable high-order discontinuous Galerkin
atmospheric dynamical core
SO COMPUTERS & FLUIDS
LA English
DT Article
ID PRIMITIVE EQUATIONS; SPHERICAL GRIDS; ELEMENT METHOD; CUBED-SPHERE;
MODEL; SCHEME
AB A new atmospheric general circulation model (dynamical core) based on the discontinuous Galerkin (DG) method is developed. This model is conservative, high-order accurate and has been integrated into the NCAR's high-order method modeling environment (HOMME) to leverage scalable parallel computing capability to thousands of processors. The computational domain for this 3-D hydrostatic model is a cubed-sphere with curvilinear coordinates; the governing equations are cast in flux-form. The horizontal DG discretization employs a high-order nodal basis set of orthogonal Lagrange-Legendre polynomials and fluxes of inter-element boundaries are approximated with Lax-Friedrichs numerical flux. The vertical discretization follows the 1-D vertical Lagrangian coordinates approach combined with the cell-integrated semi-Lagrangian conservative remapping procedure. Time integration follows the third-order strong stability preserving explicit Runge-Kutta scheme. The domain decomposition is applied through space-filling curve approach. To validate the 3-D DG model in HOMME framework, a baroclinic instability test is used and the results are compared with those from the established models. Parallel performance is evaluated on IBM Blue Gene/L Supercomputers. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Nair, R. D.; Tufo, H. M.] NCAR, Computat & Informat Syst Lab, IMAGe, Boulder, CO 80305 USA.
[Tufo, H. M.] Univ Colorado, Dept Comp Sci, Boulder, CO 80309 USA.
[Choi, H. -W.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Nair, RD (reprint author), NCAR, Computat & Informat Syst Lab, IMAGe, 1850 Table Mesa Dr, Boulder, CO 80305 USA.
EM rnair@ucar.edu; Hae-Won.Choi@nasa.gov; tufo@ucar.edu
FU NSF [DE-FG02-04ER63870, DE-FG02-07ER64464]; NSF MRI [CNS-0421498,
CNS-0420873, CNS-0420985]; IBM Shared University Research Program
FX The Authors would like to thank Prof Christiane Jablonowski for the
baroclinic instability test comparison data, Dr. John Dennis for the
performance study support and Dr. Peter Lauritzen for the internal
review of the manuscript. This project is supported by the NSF
sponsorship of the NCAR and DOE awards #DE-FG02-04ER63870 and
#DE-FG02-07ER64464. Computer time is provided through the NSF MRI Grants
CNS-0421498, CNS-0420873, and CNS-0420985, and through the IBM Shared
University Research Program.
NR 34
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U1 0
U2 3
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 2009
VL 38
IS 2
BP 309
EP 319
DI 10.1016/j.compfluid.2008.04.006
PG 11
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA 406GA
UT WOS:000263281800012
ER
PT J
AU Chen, AJ
Leptoukh, G
Kempler, S
Lynnes, C
Savtchenko, A
Nadeau, D
Farley, J
AF Chen, Aijun
Leptoukh, Gregory
Kempler, Steven
Lynnes, Christopher
Savtchenko, Andery
Nadeau, Denis
Farley, John
TI Visualization of A-Train vertical profiles using Google Earth
SO COMPUTERS & GEOSCIENCES
LA English
DT Article
DE Vertical geospatial data; A-Train; Giovanni; CloudSat; Earth remote
sensing; KML; KMZ; COLLADA; Google earth
AB Online tools, such as those pioneered by Google Earth (GE), are changing the way in which scientists and the general public interact with three-dimensional geospatial data in a virtual environment. However, while GE provides a number of features to facilitate geospatial data visualization, there is currently no readily available method for rendering vertical geospatial data derived from Earth-viewing remote sensing satellites as an orbit curtain seen from above. Here, a solution (one of many possible) is demonstrated to render vertical profiles of atmospheric data from the A-Train satellite formation in GE, using as a proof-of-concept data from one of the instruments-the NASA CloudSat satellite. CloudSat carries a nadir-viewing Cloud Profiling Radar that produces data revealing the vertical distribution of cloud characteristics along the satellite track. These data are first rendered into a long vertical image for a user-selected spatial range through the NASA Goddard Interactive Online Visualization ANd aNalysis Infrastructure (GIOVANNI) system (http://giovanni.gsfc.nasa.gov/). The vertical image is then chopped into small slices representing 15 s of satellite time (similar to 103 km long ground distance). Each small piece, as a texture, is fed into a generalized COLLAborative Design Activity (COLLADA) three-dimensional (3-D) model. Using the satellite orbit coordinates, the repeated 15 s "3-D model slices" are spliced together to form a vertical "curtain" image in Keyhole Markup Language (KML) format. Each model slice is geolocated along the CloudSat orbit path based on its size, scale and angle with the longitude line that are precisely calculated on the fly. The resulting vertical cloud data can be viewed in GE, either transparently or opaquely, superimposed above the Earth's surface with an exaggerated vertical scale. Since CloudSat is just a part of the A-Train formation, the full utility of this tool can be explored within the context of the A-Train Data Depot (ATDD, http://disc.gsfc.nasa.gov/atdd/) and the corresponding Giovanni instance (http://disc1.sci.gsfc.nasa.gov/daac-bin/G3/gui.cgi?instance_id=atrain). The latter portal allows scientists and the general public to access and visualize complex A-Train datasets without having to delve into data formats specific to a given mission. (c) 2008 Elsevier Ltd. All rights reserved.
C1 [Chen, Aijun] George Mason Univ, CSISS, Greenbelt, MD 20770 USA.
[Chen, Aijun; Leptoukh, Gregory; Kempler, Steven; Lynnes, Christopher; Savtchenko, Andery; Nadeau, Denis; Farley, John] NASA, Goddard Space Flight Ctr, GES DISC, Greenbelt, MD 20771 USA.
[Nadeau, Denis] Wyle Informat Syst, Mclean, VA 22102 USA.
[Savtchenko, Andery; Farley, John] ADNET Inc, Rockville, MD 20852 USA.
RP Chen, AJ (reprint author), George Mason Univ, CSISS, 6301 Ivy Lane,Suite 620, Greenbelt, MD 20770 USA.
EM aijunchen@gmail.com
RI Lynnes, Christopher/B-4506-2010
OI Lynnes, Christopher/0000-0001-6744-3349
NR 7
TC 31
Z9 33
U1 1
U2 17
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0098-3004
J9 COMPUT GEOSCI-UK
JI Comput. Geosci.
PD FEB
PY 2009
VL 35
IS 2
BP 419
EP 427
DI 10.1016/j.cageo.2008.08.006
PG 9
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 407XS
UT WOS:000263398200023
ER
PT J
AU Peterson, SD
Axholt, M
Ellis, SR
AF Peterson, Stephen D.
Axholt, Magnus
Ellis, Stephen R.
TI Objective and subjective assessment of stereoscopically separated labels
in augmented reality
SO COMPUTERS & GRAPHICS-UK
LA English
DT Article; Proceedings Paper
CT IEEE Virtual Reality 2008 Conference
CY MAR 08-12, 2008
CL Reno, NV
SP IEEE, Desert Res Inst, Natl Sci Fdn, Intersense, Visbox, Mechdyne, World Viz, Sensics, Virtools
DE Label placement; User interfaces; Visual clutter; Augmented reality; Air
traffic control
ID STEREOMOTION; PLACEMENT; SEARCH
AB We present a new technique for managing visual clutter caused by overlapping labels in complex information displays. This technique, label layering, utilizes stereoscopic disparity as a means to segregate labels in depth for increased legibility and clarity. By distributing overlapping labels in depth, we have found that selection time during a visual search task in situations with high levels of visual overlap is reduced by 4s or 24%. Our data show that the stereoscopically based depth order of the labels must be correlated with the distance order of their corresponding objects, for practical benefits. An algorithm using our label layering technique accordingly could be an alternative to traditional label placement algorithms that avoid label overlap at the cost of distracting view plane motion, symbology dimming or label size reduction. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Peterson, Stephen D.; Axholt, Magnus] Linkoping Univ, Dept Sci & Technol, SE-60174 Norrkoping, Sweden.
[Ellis, Stephen R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Peterson, SD (reprint author), Linkoping Univ, Dept Sci & Technol, SE-60174 Norrkoping, Sweden.
EM stepe@itn.liu.se; magax@itn.liu.se; sellis@mail.arc.nasa.gov
NR 38
TC 8
Z9 9
U1 0
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0097-8493
EI 1873-7684
J9 COMPUT GRAPH-UK
JI Comput. Graph.-UK
PD FEB
PY 2009
VL 33
IS 1
BP 23
EP 33
DI 10.1016/j.cag.2008.11.006
PG 11
WC Computer Science, Software Engineering
SC Computer Science
GA 416IQ
UT WOS:000263999800005
ER
PT J
AU Ramp, SR
Davis, RE
Leonard, NE
Shulman, I
Chao, Y
Robinson, AR
Marsden, J
Lermusiaux, PFJ
Fratantoni, DM
Paduan, JD
Chavez, FP
Bahr, FL
Liang, S
Leslie, W
Li, Z
AF Ramp, S. R.
Davis, R. E.
Leonard, N. E.
Shulman, I.
Chao, Y.
Robinson, A. R.
Marsden, J.
Lermusiaux, P. F. J.
Fratantoni, D. M.
Paduan, J. D.
Chavez, F. P.
Bahr, F. L.
Liang, S.
Leslie, W.
Li, Z.
TI Preparing to predict: The Second Autonomous Ocean Sampling Network
(AOSN-II) experiment in the Monterey Bay
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Ocean circulation; Ocean heat budget; Ocean winds; Ocean temperature;
Salinity; Density
ID LAGRANGIAN COHERENT STRUCTURES; LOCALIZED MULTISCALE ENERGY; DATA-DRIVEN
SIMULATIONS; CENTRAL CALIFORNIA; DATA ASSIMILATION; VORTICITY ANALYSIS;
MASSACHUSETTS BAY; CONTINENTAL-SHELF; POINT SUR; VARIABILITY
AB The Autonomous Ocean Sampling Network Phase Two (AOSN-II) experiment was conducted in and offshore from the Monterey Bay on the central California coast during July 23-September 6, 2003. The objective of the experiment was to learn how to apply new tools, technologies, and analysis techniques to adaptively sample the coastal ocean in a manner demonstrably superior to traditional methodologies, and to use the information gathered to improve predictive skill for quantities of interest to end-users. The scientific goal was to study the upwelling/relaxation cycle near an open coastal bay in an eastern boundary current region, particularly as it developed and spread from a coastal headland. The suite of observational tools used included a low-flying aircraft, a fleet of underwater gliders, including several under adaptive autonomous control, and propeller-driven AUVs in addition to moorings, ships, and other more traditional hardware. The data were delivered in real time and assimilated into the Harvard Ocean Prediction System (HOPS), the Navy Coastal Ocean Model (NCOM), and the jet Propulsion Laboratory implementation of the Regional Ocean Modeling System (JPL/ROMS).
Two upwelling events and one relaxation event were sampled during the experiment. The upwelling in both cases began when a pool of cold water less than 13 degrees C appeared near Cape Ano Nuevo and subsequently spread offshore and southward across the bay as the equatorward wind stress continued. The primary difference between the events was that the first event spread offshore and southward, while the second event spread only southward and not offshore. The difference is attributed to the position and strength of meanders and eddies of the California Current System offshore, which blocked or steered the cold upwelled water. The space and time scales of the mesoscale variability were much shorter than have been previously observed in deep-water eddies offshore. Additional process studies are needed to elucidate the dynamics of the flow. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Ramp, S. R.; Chavez, F. P.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA.
[Davis, R. E.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Leonard, N. E.] Princeton Univ, Dept Mech Engn, Princeton, NJ 08544 USA.
[Shulman, I.] USN, Res Lab, Stennis Space Ctr, MS 39529 USA.
[Chao, Y.; Li, Z.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Robinson, A. R.; Liang, S.; Leslie, W.] Harvard Univ, Cambridge, MA 02138 USA.
[Marsden, J.] CALTECH, Pasadena, CA 91125 USA.
[Lermusiaux, P. F. J.] MIT, Cambridge, MA 02139 USA.
[Paduan, J. D.; Bahr, F. L.] USN, Postgrad Sch, Monterey, CA USA.
[Fratantoni, D. M.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
RP Ramp, SR (reprint author), Monterey Bay Aquarium Res Inst, 7700 Sandholdt Rd, Moss Landing, CA 95039 USA.
EM sramp@mbari.org
RI Fratantoni, David/C-7121-2011; Lermusiaux, Pierre/H-6003-2011;
OI Davis, Russ/0000-0003-1903-6313
FU Office of Naval Research, Ocean, Atmosphere, and Space Department;
Monterey Bay Aquarium Research Institute
FX The authors are indebted to the Office of Naval Research, Ocean,
Atmosphere, and Space Department, for funding the AOSN program. Dr. Tom
Curtin of ONR provided direction and leadership for the AOSN program
over a period of many years to make it a reality. Additional support,
especially for shore-side logistics, was provided by the Monterey Bay
Aquarium Research Institute. Aircraft support was provided by the NPS
Center for Interdisciplinary Remotely Piloted Aircraft Studies (CIRPAS),
especially by Bob Bluth, Haf Jonsson, and Gintas Buzorius. Countless
technical staff and graduate students worked long hours during the field
program to collect and process real-time data, implement models and
assimilate the data, and to disseminate and discuss the results.
NR 73
TC 52
Z9 55
U1 4
U2 16
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD FEB
PY 2009
VL 56
IS 3-5
BP 68
EP 86
DI 10.1016/j.dsr2.2008.08.013
PG 19
WC Oceanography
SC Oceanography
GA 452MH
UT WOS:000266543600003
ER
PT J
AU Doyle, JD
Jiang, QF
Chao, Y
Farrara, J
AF Doyle, James D.
Jiang, Qingfang
Chao, Yi
Farrara, John
TI High-resolution real-time modeling of the marine atmospheric boundary
layer in support of the AOSN-II field campaign
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Air-sea interaction; AOSN-II; High-resolution atmospheric modeling; Sea
breeze circulation; Coastal low-level jet
ID WIND STRESS CURL; NORTHERN CALIFORNIA; SEA-BREEZE; SUPERCRITICAL-FLOW;
DOPPLER LIDAR; COASTAL OCEAN; MONTEREY BAY; SIMULATIONS; DYNAMICS;
REANALYSIS
AB The Navy's COAMPS atmospheric model has been used to provide twice-daily, real-time forecasts of 72-h duration in support of the AOSN-II field campaign during August 2003. The model was configured with four grid meshes with a minimum horizontal grid increment of 3 km. A statistical analysis of the model forecasts using available buoy observations demonstrates the skill of the atmospheric model predictions with characteristic wind speed RMS and bias errors of 1-3 m s(-1) and less than 0.5-1.0 m s(-1), respectively, and temperature RMS errors of 1-2 degrees C and biases typically less than 1.0 degrees C. The highest-resolution mesh provides more accurate wind-speed variances during the upwelling periods in the nearshore region, where the wind-speed gradients and diurnal variations are the largest. Persistent and strong low-level winds from a northwesterly direction were associated with a mid-tropospheric trough and jet stream that was substantially stronger than the overall mean monthly conditions. During the relaxation periods, which were relatively infrequent during August 2003, the trough was weaker than the mean conditions with a closed low west of the coast that resulted in southerlies near the coast. During upwelling-favorable conditions, the mean marine inversion was substantially stronger than during the relaxation periods with the surface-stress field exhibiting maxima in the lee of prominent coastal capes and topography, particularly during the periods of strong larger-scale low-level flow. The persistent mean stress pattern that is topographically locked, yields maxima in the stress curl pattern that induce favorable regions of coastal upwelling near and downwind of the coastal promontories and headlands. Published by Elsevier Ltd.
C1 [Doyle, James D.] USN, Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA.
[Jiang, Qingfang] UCAR, Monterey, CA USA.
[Chao, Yi; Farrara, John] CALTECH, JPL, Pasadena, CA 91125 USA.
RP Doyle, JD (reprint author), USN, Res Lab, Marine Meteorol Div, 7 Grace Hopper Ave, Monterey, CA 93943 USA.
EM james.doyle@nrlmry.navy.mil
FU Office of Naval Research's Program Element [0601153N]; National
Aeronautics and Space Administration (NASA); Fleet Numerical Meteorology
and Oceanography Command
FX The first two authors acknowledge support through the Office of Naval
Research's Program Element 0601153N. The research for Y. Chao and J.
Farrara was carried out, in part, at the jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration (NASA). Computational resources
were supported in part by the Fleet Numerical Meteorology and
Oceanography Command. COAMPS (R) is a registered trademark of the Naval
Research Laboratory. We acknowledge Richard Lind of the Naval
Postgraduate School for providing the Fort Ord shortwave radiation data.
We are grateful for helpful comments from three anonymous reviewers and
as well as suggestions and comments from Tracy Haack.
NR 35
TC 40
Z9 40
U1 0
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD FEB
PY 2009
VL 56
IS 3-5
BP 87
EP 99
DI 10.1016/j.dsr2.2008.08.009
PG 13
WC Oceanography
SC Oceanography
GA 452MH
UT WOS:000266543600004
ER
PT J
AU Chao, Y
Li, ZJ
Farrara, J
McWilliams, JC
Bellingham, J
Capet, X
Chavez, F
Choi, JK
Davis, R
Doyle, J
Fratantoni, DM
Li, P
Marchesiello, P
Moline, MA
Paduan, J
Ramp, S
AF Chao, Yi
Li, Zhijin
Farrara, John
McWilliams, James C.
Bellingham, James
Capet, Xavier
Chavez, Francisco
Choi, Jei-Kook
Davis, Russ
Doyle, Jim
Fratantoni, David M.
Li, Peggy
Marchesiello, Patrick
Moline, Mark A.
Paduan, Jeff
Ramp, Steve
TI Development, implementation and evaluation of a data-assimilative ocean
forecasting system off the central California coast
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Data assimilation; Ocean modeling; Ocean forecast; Coastal ocean;
Adaptive sampling; Reanalysis
ID MONTEREY BAY; MODELING SYSTEM; SURFACE; FLOW; TOPOGRAPHY; DYNAMICS; ROMS
AB The development and implementation of a real-time ocean forecast system based on the Regional Ocean Modeling System (ROMS) off the coast of central California are described. The ROMS configuration consists of three nested modeling domains with increasing spatial resolutions: the US West coastal ocean at 15-km resolution, the central California coastal ocean at 5 km, and the Monterey Bay region at 1.5 km. All three nested models have 32 vertical sigma (or terrain-following) layers and were integrated in conj. unction with a three-dimensional variational data assimilation algorithm (3DVAR) to produce snapshots of the ocean state every 6 h (the reanalysis) and 48-h forecasts once a day. This ROMS forecast system was operated in real time during the field experiment known as the Autonomous Ocean Sampling Network (AOSN-II) in August 2003. After the field experiment, a number of improvements were made to the ROMS forecast system: more data were added in the reanalysis with more careful quality control procedures, improvements were made in the data assimilation scheme, as well as model surface and side boundary conditions.
The results from the ROMS reanalysis are presented here. The ROMS reanalysis is first compared with the assimilated data as a consistency check. An evaluation of the ROMS reanalysis against the independent measurements that are not assimilated into the model is then presented. This evaluation shows the mean differences in temperature and salinity between reanalysis and observations to be less than 1 degrees C and 0.2 psu (practical salinity unit), respectively, with root-mean-square (RMS) differences of less than 1.5 degrees C and 0.25 psu. Qualitative agreement is found between independent current measurements and the ROMS reanalysis. The agreement is particularly good for the vertically integrated current along the offshore glider tracks: the ROMS reanalysis can realistically reproduce the poleward California Undercurrent. Reasonably good agreement is found in the spatial patterns of the surface current as measured by high-frequency (HF) radars. Preliminary results concerning the ROMS forecast skill and predictability are also presented. Future plans to improve the ROMS forecast system with a particular focus on assimilation of HF radar current measurements are discussed. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Chao, Yi; Li, Zhijin; Li, Peggy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Farrara, John] Raytheon ITSS, Pasadena, CA USA.
[McWilliams, James C.; Capet, Xavier] Univ Calif Los Angeles, Los Angeles, CA USA.
[Bellingham, James; Chavez, Francisco] Monterey Bay Aquarium Res Inst, Moss Landing, CA USA.
[Choi, Jei-Kook] USN, Oceanog Off, Stennis Space Ctr, MS 39529 USA.
[Davis, Russ] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92103 USA.
[Doyle, Jim] USN, Res Lab, Monterey, CA USA.
[Fratantoni, David M.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Marchesiello, Patrick] IRD, Noumea, New Caledonia.
[Moline, Mark A.] Calif Polytech State Univ San Luis Obispo, San Luis Obispo, CA 93407 USA.
[Paduan, Jeff; Ramp, Steve] USN, Postgrad Sch, Monterey, CA USA.
RP Chao, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 183-601, Pasadena, CA 91109 USA.
EM Yi.Chao@jpl.nasa.gov
RI Fratantoni, David/C-7121-2011;
OI Davis, Russ/0000-0003-1903-6313
FU National Aeronautics and Space Administration (NASA); Office of Naval
Research (ONR) [0601153N]
FX 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).
Support from the Office of Naval Research (ONR) through a subcontract
from MBARI to Raytheon is acknowledged. Additional support is
acknowledged through ONR's program element 0601153N for J. Doyle.
Computational resources for COAMPS were supported in part by the FNMOC.
COAMPS (R) is a registered trademark of the NRL. Thanks also go to the
rest of the JPL ROMS team (KJ Park, Xiaochun Wang, Quoc Vu, Carrie
Zhang) and Dr. Kayo Ide at UCLA who have provided advice and technical
help throughout the field experiment and post-experiment reanalysis
phase.
NR 32
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Z9 42
U1 0
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD FEB
PY 2009
VL 56
IS 3-5
BP 100
EP 126
DI 10.1016/j.dsr2.2008.08.011
PG 27
WC Oceanography
SC Oceanography
GA 452MH
UT WOS:000266543600005
ER
PT J
AU Wang, XC
Chao, Y
Dong, CM
Farrara, J
Li, ZJ
McWilliams, JC
Paduan, JD
Rosenfeld, LK
AF Wang, Xiaochun
Chao, Yi
Dong, Changming
Farrara, John
Li, Zhijin
McWilliams, James C.
Paduan, Jeffrey D.
Rosenfeld, Leslie K.
TI Modeling tides in Monterey Bay, California
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Monterey Bay; Barotropic tides; Baroclinic tides; Modeling; Energy flux;
High-frequency radar
ID INTERNAL TIDE; BOUNDARY-CONDITION; SUBMARINE-CANYON; BRITISH-COLUMBIA;
OCEAN; SYSTEM; WAVES; SIMULATION; GENERATION; RADIATION
AB In the process of developing a tide-permitting coastal ocean forecasting system, tidal signals are added to an oceanic general circulation model for Monterey Bay, California. The model, which is configured from the regional ocean modeling system (ROMS), has three one-way nested domains with the finest resolution of 1.6 km in the horizontal direction and 32 levels in the vertical direction. In present research, the tidal simulation of the system is validated against tide gauges, ADCP current observations, high-frequency radar surface-current observations, and compared with the output from two barotropic tidal models. The results indicate that the barotropic tides from the model compare well with observations in terms of sea-surface height, with discrepancies in amplitude of less than 10% of the amplitude of the most energetic M(2) constituent. However, the discrepancy for the barotropic tidal currents can reach 30% among models with similar accuracy in sea-surface height. The generation and propagation of baroclinic tides associated with the Monterey Submarine Canyon are qualitatively reproduced by the model with weaker strength. The surface tidal current simulation is improved, especially in terms of magnitude, when the model has a more realistic stratification through changes in both barotropic and baroclinic tidal Currents. (C) 2008 Elsevier Ltd. All rights reserved.
C1 [Wang, Xiaochun; Chao, Yi; Farrara, John; Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wang, Xiaochun; Farrara, John] Raytheon ITSS, Pasadena, CA 91101 USA.
[Dong, Changming; McWilliams, James C.] Univ Calif Los Angeles, IGPP, Los Angeles, CA 90095 USA.
[Paduan, Jeffrey D.; Rosenfeld, Leslie K.] USN, Postgrad Sch, Dept Oceanog, Monterey, CA 93943 USA.
RP Chao, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 300-323, Pasadena, CA 91109 USA.
EM ychao@jpl.nasa.gov
FU National Aeronautics and Space Administration; Office of Naval Research;
NOAA COTS; California Coastal Conservancy; NOAA [NA160C2936]
FX The research was carried out, in part, by the jet Propulsion Laboratory
(JPL), California Institute of Technology, under contract with the
National Aeronautics and Space Administration. The financial support was
provided by the Office of Naval Research through a subcontract from
Monterey Bay Aquarium Research Institute to Raytheon, and NOAA COTS
funding and California Coastal Conservancy through the COCMP program
(both through subcontracts from Scripps Institution of Oceanography/UCSD
to Raytheon). The long-term support from Drs. Emily Greene and Michael
Lampel at the Pasadena office of Raytheon is acknowledged. Computations
were performed on computers provided by the JPL Supercomputer Project
and the NASA Advanced Supercomputing Division at Ames Research Center.
High-frequency radar data were supported during this period by NOAA
award No. NA160C2936 to the Center for Integrated Marine Technologies
(CIMT). The authors would like to thank three anonymous reviewers for
their insightful and detailed comments. XCW would like to thank Dr.
Peggy Li, Mr. Quoc Vu, and Mrs. Hongchun Zhang for their technical help
and Drs. C. K. Shum, Eric Kunze, Gary Egbert, and Mike Foreman for
discussions.
NR 53
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U1 3
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD FEB
PY 2009
VL 56
IS 3-5
BP 219
EP 231
DI 10.1016/j.dsr2.2008.08.012
PG 13
WC Oceanography
SC Oceanography
GA 452MH
UT WOS:000266543600012
ER
PT J
AU Ramette, A
Boetius, A
Danchin, A
Eloe, E
Celussi, M
Croal, L
Gifford, S
Gomez-Consarnau, L
Hahn, MW
Hoehler, TM
Jorgensen, BB
Karl, DM
Kolter, R
Moran, MA
Muller, V
Ollivier, B
Guyot, F
Oremland, RS
Stolz, JF
Pearson, A
Stahl, DA
Teusink, B
Bruggeman, FJ
Molenaar, D
Stoeck, T
Epstein, S
Tummler, B
Wommack, KE
Zehr, JP
AF Ramette, Alban
Boetius, Antje
Danchin, Antoine
Eloe, Emiley
Celussi, Mauro
Croal, Laura
Gifford, Scott
Gomez-Consarnau, Laura
Hahn, Martin W.
Hoehler, Tori M.
Jorgensen, Bo B.
Karl, David M.
Kolter, Roberto
Moran, Mary Ann
Mueller, Volker
Ollivier, Bernard
Guyot, Francois
Oremland, Ronald S.
Stolz, John F.
Pearson, Ann
Stahl, David A.
Teusink, Bas
Bruggeman, Frank J.
Molenaar, Douwe
Stoeck, Thorsten
Epstein, Slava
Tuemmler, Burkhard
Wommack, K. Eric
Zehr, Jonathan P.
TI Crystal ball-2009
SO ENVIRONMENTAL MICROBIOLOGY REPORTS
LA English
DT Editorial Material
ID MICROBIAL COMMUNITY; PHOTOSYNTHESIS GENES; ENERGY-CONSERVATION; RARE
BIOSPHERE; MARINE VIRUSES; DEEP-SEA; BACTERIA; DIVERSITY; OCEAN;
MICROORGANISMS
C1 [Ramette, Alban; Boetius, Antje; Jorgensen, Bo B.] Max Planck Inst Marine Microbiol, Bremen, Germany.
[Danchin, Antoine] Inst Pasteur, Genet Bacterial Genomes CNRS, URA2171, Paris, France.
[Eloe, Emiley] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Celussi, Mauro] Ist Nazl Oceanog & Geofis Sperimentale, Dipartimento Oceanog Biol, Trieste, Italy.
[Croal, Laura] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA.
[Gifford, Scott; Moran, Mary Ann] Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA.
[Gomez-Consarnau, Laura] Univ Kalmar, Sch Pure & Appl Nat Sci, Kalmar, Sweden.
[Hahn, Martin W.] Austrian Acad Sci, Inst Limnol, A-5310 Mondsee, Austria.
[Hoehler, Tori M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Jorgensen, Bo B.] Univ Aarhus, Inst Biol, DK-8000 Aarhus C, Denmark.
[Karl, David M.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA.
[Kolter, Roberto] Harvard Univ, Sch Med, Boston, MA USA.
[Mueller, Volker] Goethe Univ Frankfurt, Frankfurt, Germany.
[Ollivier, Bernard] Univ Aix Marseille 1, Lab Microbiol IRD, UMR IFR BAIM 180, Marseille, France.
[Ollivier, Bernard] Univ Aix Marseille 2, Marseille, France.
[Guyot, Francois] Univ Paris 06, IMPMC, Lab Mineral, Paris, France.
[Guyot, Francois] Univ Paris 06, CNRS, IPGP, Paris, France.
[Oremland, Ronald S.] US Geol Survey, Menlo Pk, CA 94025 USA.
[Stolz, John F.] Duquesne Univ, Dept Biol Sci, Pittsburgh, PA 15219 USA.
[Pearson, Ann] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Stahl, David A.] Univ Washington, Seattle, WA 98195 USA.
[Teusink, Bas; Bruggeman, Frank J.; Molenaar, Douwe] Vrije Univ Amsterdam, NISB, Ctr Integrat Bioinformat IBIVU, Amsterdam, Netherlands.
[Stoeck, Thorsten] Univ Kaiserslautern, Dept Ecol, Kaiserslautern, Germany.
[Epstein, Slava] Northeastern Univ, Dept Biol, Boston, MA 02115 USA.
[Tuemmler, Burkhard] Hannover Med Sch, D-30623 Hannover, Germany.
[Wommack, K. Eric] Univ Delaware, Dept Plant & Soil Sci, Delaware Biotechnol Inst, Delaware, OH USA.
[Wommack, K. Eric] Univ Delaware, Grad Coll Marine & Earth Studies, Delaware Biotechnol Inst, Delaware, OH USA.
[Zehr, Jonathan P.] Univ Calif Santa Cruz, Dept Ocean Sci, Santa Cruz, CA 95064 USA.
RP Ramette, A (reprint author), Max Planck Inst Marine Microbiol, Bremen, Germany.
RI IMPMC, Geobio/F-8819-2016; Boetius, Antje/D-5459-2013; Hahn,
Martin/B-9998-2008; Molenaar, Douwe/D-2017-2010; Moran, Mary
Ann/B-6939-2012; Jorgensen, Bo/C-2214-2013; Zehr, Jonathan/B-3513-2014;
Bruggeman, Frank/C-4356-2015; Ramette, Alban/E-9197-2016; Ollivier,
Bernard/I-6150-2016; GUYOT, Francois/C-3824-2016
OI Boetius, Antje/0000-0003-2117-4176; Hahn, Martin/0000-0003-0501-2556;
Molenaar, Douwe/0000-0001-7108-4545; Jorgensen, Bo/0000-0001-9398-8027;
Zehr, Jonathan/0000-0002-5691-5408; Bruggeman,
Frank/0000-0002-0255-4766; Ramette, Alban/0000-0002-3437-4639; GUYOT,
Francois/0000-0003-4622-2218
NR 66
TC 2
Z9 2
U1 3
U2 31
PU WILEY-BLACKWELL PUBLISHING, INC
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1758-2229
J9 ENV MICROBIOL REP
JI Environ. Microbiol. Rep.
PD FEB
PY 2009
VL 1
IS 1
BP 3
EP 26
DI 10.1111/j.1758-2229.2008.00010.x
PG 24
WC Environmental Sciences; Microbiology
SC Environmental Sciences & Ecology; Microbiology
GA 606PB
UT WOS:000278438000002
ER
PT J
AU Vishwanath, V
Burns, R
Leigh, J
Seablom, M
AF Vishwanath, Venkatrarn
Burns, Robert
Leigh, Jason
Seablom, Michael
TI Accelerating tropical cyclone analysis using LambdaRAM, a distributed
data cache over wide-area ultra-fast networks
SO FUTURE GENERATION COMPUTER SYSTEMS-THE INTERNATIONAL JOURNAL OF ESCIENCE
LA English
DT Article
DE Data-intensive computing; Multi-dimensional remote data striding;
Climate modeling and analysis; Distributed data caches; LambdaGrids;
Tropical cyclone analysis; Hurricane analysis
ID MEMORY
AB Data-intensive scientific applications require rapid access to local and geographically distributed data, however, there are significant I/O latency bottlenecks associated with storage systems and wide-area networking. LambdaRAM is a high-performance, multi-dimensional, distributed cache, that takes advantage of memory from multiple clusters interconnected by ultra-high-speed networking, to provide applications with rapid access to both local and remote data. It mitigates latency bottlenecks by employing proactive latency-mitigation heuristics based on an application's access patterns. We present results using LambdaRAM to rapidly stride through remote multi-dimensional NASA Modeling, Analysis and Prediction (MAP) 2006 project datasets, based on time and geographical coordinates, to compute wind shear for cyclone and hurricane and tropical cyclone analysis. Our current experiments have demonstrated up to a 20-fold speedup in the computation of wind shear with LambdaRAM. (C) 2008 Elsevier B.V. All rights reserved.
C1 [Vishwanath, Venkatrarn; Leigh, Jason] Univ Illinois, EVL, Chicago, IL 60607 USA.
[Burns, Robert; Seablom, Michael] NASA, GSFC, SIVO, Greenbelt, MD 20771 USA.
RP Vishwanath, V (reprint author), Univ Illinois, EVL, Room 1120 SEO, Chicago, IL 60607 USA.
EM venkat@evl.uic.edu; robert.w.burns@nasa.gov; spiff@uic.edu;
michael.s.seablom@nasa.gov
FU National Science Foundation (NSF) [CNS-0420477, OCI-0441094,
OCI-0225642]; State of Illinois, Sharp Laboratories of America, Pacific
Interface; Northrop Grumman Corporation
FX We would like to thank Bill Putnam (NASA, GSFC), Carlos Cruz (NASA,
GSFC), Pat Gary (NASA GSFC), Bill Fink (NASA, GSFC), Paul Lang (NASA,
GSFC), Alan Verlo (EVL, UIC), Lance Long (EVL, UIC), Maxine Brown (EVL,
UIC), Luc Renambot (EVL, UIC), Larry Smarr (CalIT2, UCSD), Tom DeFanti
(CalIT2, UCSD), Joseph Greenseid (NGC), Anand Patwardhan (UMBC) and Milt
Halem (UMBC). This material is based upon work supported by the National
Science Foundation (NSF), awards CNS-0420477, OCI-0441094, and
OCI-0225642, as well as funding from the State of Illinois, Sharp
Laboratories of America, Pacific Interface on behalf of NTT Network
Innovation Laboratories in Japan, and Northrop Grumman Corporation on
behalf of NASA. Any opinions, findings, and conclusions or
recommendations expressed in this publication are those of the authors
and do not necessarily reflect the views of the funding agencies and
companies.
NR 32
TC 1
Z9 1
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-739X
EI 1872-7115
J9 FUTURE GENER COMP SY
JI Futur. Gener. Comp. Syst.
PD FEB
PY 2009
VL 25
IS 2
BP 184
EP 191
DI 10.1016/j.future.2008.07.005
PG 8
WC Computer Science, Theory & Methods
SC Computer Science
GA 364DJ
UT WOS:000260316100012
ER
PT J
AU Mulavara, AP
Cohen, HS
Bloomberg, JJ
AF Mulavara, Ajitkumar P.
Cohen, Helen S.
Bloomberg, Jacob J.
TI Critical features of training that facilitate adaptive generalization of
over ground locomotion
SO GAIT & POSTURE
LA English
DT Article
DE Balance therapy; Motor learning; Plasticity; Locomotion; Rehabilitation
ID VARIABLE PRACTICE; SENSORIMOTOR ADAPTATION; VESTIBULOOCULAR REFLEX;
TREADMILL LOCOMOTION; VIRTUAL ENVIRONMENT; OBSTACLE AVOIDANCE; MOTOR
SKILL; WALKING; TASK; INTERFERENCE
AB When subjects learn motor tasks under novel visumotor conditions variations in sensory input during training facilitate adaptive generalization. We tested the hypotheses that training with multiple sensory input variations is more effective than a single or no variation and that training Must include critical features of the criterion task. Normal adults were pre- and post-tested on an obstacle avoidance task while wearing visual distortion lenses after treadmill walking (Experiment 1), or balance training (Experiment 2). Subjects were randomized to training groups in which they wore either: (1) three different visual distortion lenses, (2) a single pair of visual distortion lenses, or (3) sham lenses. Post-tests were done while wearing novel lenses. In Experiment 1 subjects who trained with multiple lenses adapted better than single or sham lens groups. The single lens-training group with magnifying lenses adapted better than the other single lens groups. In Experiment 2, training for dynamic balance, alone, did not increase training efficacy. Thus, training for an obstacle avoidance task in a novel visual environment required a critical feature of the criterion task: locomotion. Constant practice with a single lens was successful only if the best lens was selected, but the best lens could not be known ahead of time. Therefore variable practice with multiple lenses on a task that included a critical feature of the criterion task was the best training strategy to enhance adaptive generalization. (c) 2008 Elsevier B.V. All rights reserved.
C1 [Cohen, Helen S.] Baylor Coll Med, Bobby R Alford Dept Otolaryngol Head & Neck Surg, Houston, TX 77030 USA.
[Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Washington, DC 20546 USA.
RP Cohen, HS (reprint author), Baylor Coll Med, Bobby R Alford Dept Otolaryngol Head & Neck Surg, 1 Baylor Plaza, Houston, TX 77030 USA.
EM hcohen@bcm.tmc.edu
FU NIH [DC04167]; National Space Biomedical Research Institute; NASA [NCC
9-58]
FX Supported by NIH grant DC04167 and the National Space Biomedical
Research Institute through NASA NCC 9-58. We thank the staff of the
Center for Balance Disorders, Baylor College of Medicine, for technical
assistance and Dr. Deborah Harm of NASA Johnson Space Center for
assistance with statistical analysis.
NR 31
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Z9 26
U1 1
U2 5
PU ELSEVIER IRELAND LTD
PI CLARE
PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000,
IRELAND
SN 0966-6362
J9 GAIT POSTURE
JI Gait Posture
PD FEB
PY 2009
VL 29
IS 2
BP 242
EP 248
DI 10.1016/j.gaitpost.2008.08.012
PG 7
WC Neurosciences; Orthopedics; Sport Sciences
SC Neurosciences & Neurology; Orthopedics; Sport Sciences
GA 409LJ
UT WOS:000263506900013
PM 18838271
ER
PT J
AU Milazzo, MP
Keszthelyi, LP
Jaeger, WL
Rosiek, M
Mattson, S
Verba, C
Beyer, RA
Geissler, PE
McEwen, AS
AF Milazzo, M. P.
Keszthelyi, L. P.
Jaeger, W. L.
Rosiek, M.
Mattson, S.
Verba, C.
Beyer, R. A.
Geissler, P. E.
McEwen, A. S.
CA HiRISE Team
TI Discovery of columnar jointing on Mars
SO GEOLOGY
LA English
DT Article
ID CERBERUS FOSSAE; LAVA; BASALT; GROUNDWATER; GROWTH; FLOWS; WATER
AB We report on the discovery of columnar jointing in Marte Valles, Mars. These columnar lavas were discovered in the wall of a pristine, 16-km-diameter impact crater and exhibit the features of terrestrial columnar basalts. There are discontinuous outcrops along the entire crater wall, suggesting that the columnar rocks covered a surface area of at least 200 km(2), assuming that the rocks obliterated by the impact event were similarly jointed. We also see columns in the walls of other fresh craters in the nearby volcanic plains of Elysium Planitia-Amazonis Planitia, which include Marte Vallis, and in a well-preserved crater in northeast Hellas.
C1 [Milazzo, M. P.; Keszthelyi, L. P.; Jaeger, W. L.; Rosiek, M.; Verba, C.; Geissler, P. E.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA.
[Mattson, S.; McEwen, A. S.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Beyer, R. A.] SETI Search Extraterrestrial Intelligence Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Beyer, R. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Milazzo, MP (reprint author), US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA.
EM moses@usgs.gov
OI Beyer, Ross/0000-0003-4503-3335
FU National Aeronautics and Space Administration (NASA)
FX We thank everyone at the HiRISE (High Resolution Imaging Science
Experiment) Operations Center (HiROC) at the University of Arizona for
their tremendous efforts in requiring and processing the HiRISE images
this study used. This work was funded by the National Aeronautics and
Space Administration (NASA) through the Mars Reconnaissance Orbiter
project, and has made use of NASA's Astrophysics Data System. The data
were processed with the U.S. Geological Survey Integrated Software for
Imagers and Spectrometers (ISIS). We thank Scott Rowland and John Wolff,
who provided in-depth reviews that significantly improved the quality of
the paper.
NR 24
TC 23
Z9 23
U1 2
U2 8
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD FEB
PY 2009
VL 37
IS 2
BP 171
EP 174
DI 10.1130/G25187A.1
PG 4
WC Geology
SC Geology
GA 403QK
UT WOS:000263096900019
ER
PT J
AU Jones, PD
Briffa, KR
Osborn, TJ
Lough, JM
van Ommen, TD
Vinther, BM
Luterbacher, J
Wahl, ER
Zwiers, FW
Mann, ME
Schmidt, GA
Ammann, CM
Buckley, BM
Cobb, KM
Esper, J
Goosse, H
Graham, N
Jansen, E
Kiefer, T
Kull, C
Kuttel, M
Mosley-Thompson, E
Overpeck, JT
Riedwyl, N
Schulz, M
Tudhope, AW
Villalba, R
Wanner, H
Wolff, E
Xoplaki, E
AF Jones, P. D.
Briffa, K. R.
Osborn, T. J.
Lough, J. M.
van Ommen, T. D.
Vinther, B. M.
Luterbacher, J.
Wahl, E. R.
Zwiers, F. W.
Mann, M. E.
Schmidt, G. A.
Ammann, C. M.
Buckley, B. M.
Cobb, K. M.
Esper, J.
Goosse, H.
Graham, N.
Jansen, E.
Kiefer, T.
Kull, C.
Kuettel, M.
Mosley-Thompson, E.
Overpeck, J. T.
Riedwyl, N.
Schulz, M.
Tudhope, A. W.
Villalba, R.
Wanner, H.
Wolff, E.
Xoplaki, E.
TI High-resolution palaeoclimatology of the last millennium: a review of
current status and future prospects
SO HOLOCENE
LA English
DT Review
DE Palaeoclimatology; high-resolution; last millennium; tree rings;
dendroclimatology; chronology; uncertainty; corals; ice-cores;
speleothems; documentary evidence; instrumental records; varves;
borehole temperature; marine sediments; composite plus scaling; CPS;
climate field reconstruction; CFR; pseudo-proxy approach; time series;
climate forcing
ID SEA-SURFACE TEMPERATURE; TREE-RING-WIDTH; NORTH-ATLANTIC OSCILLATION;
STABLE-ISOTOPE RECORDS; LATE-HOLOCENE CLIMATE; MEDIEVAL WARM PERIOD;
INTERTROPICAL CONVERGENCE ZONE; PROXY-BASED RECONSTRUCTIONS; CORAL-BASED
RECONSTRUCTION; GENERAL-CIRCULATION MODEL
AB This review of late-Holocene palaeoclimatology represents the results from a PAGES/CLIVAR Intersection Panel meeting that took place in June 2006. The review is in three parts: the principal high-resolution proxy disciplines (trees, corals, ice cores and documentary evidence), emphasizing current issues in their e for climate reconstruction; the various approaches that have been adopted to combine multiple climate us proxy records to provide estimates of past annual-to-decadal timescale Northern Hemisphere surface temperatures and other climate variables, such as large-scale circulation indices; and the forcing histories used in climate model simulations of the past millennium. We discuss the need to develop a framework through which current and new approaches to interpreting these proxy data may be rigorously assessed using pseudo-proxies derived from climate model runs, where the 'answer' is known. The article concludes with a list of recommendations. First, more raw proxy data are required from the diverse disciplines and from more locations, as well as replication, for all proxy sources, of the basic raw measurements to improve absolute dating, and to better distinguish the proxy climate signal from noise. Second, more effort is required to improve the understanding of what individual proxies respond to, supported by more site measurements and process studies. These activities should also be mindful of the correlation structure of instrumental data, indicating which adjacent proxy records ought to be in agreement and which not. Third, large-scale climate reconstructions should be attempted using a wide variety of techniques, emphasizing those for which quantified errors can be estimated at specified timescales. Fourth, a greater use of climate model simulations is needed to guide the choice of reconstruction techniques (the pseudo-proxy concept) and possibly help determine where, given limited resources, future sampling should be concentrated.
C1 [Jones, P. D.; Briffa, K. R.; Osborn, T. J.] Univ E Anglia, Sch Environm Sci, Climat Res Unit, Norwich NR4 7TJ, Norfolk, England.
[Lough, J. M.] Australian Inst Marine Sci, Townsville, Qld 4810, Australia.
[van Ommen, T. D.] Australian Antarctic Div, Hobart Tasmania 7001, Australia.
[van Ommen, T. D.] ACE CRC, Hobart Tasmania 7001, Australia.
[Vinther, B. M.] Univ Copenhagen, Niels Bohr Inst, Ctr Ice & Climate, DK-2100 Copenhagen, Denmark.
[Luterbacher, J.; Kuettel, M.; Riedwyl, N.; Wanner, H.; Xoplaki, E.] Univ Bern, Oeschger Ctr Climate Change Res, CH-3012 Bern, Switzerland.
[Luterbacher, J.; Kuettel, M.; Riedwyl, N.; Wanner, H.; Xoplaki, E.] Univ Bern, NCCR Climate, CH-3012 Bern, Switzerland.
[Luterbacher, J.; Kuettel, M.; Riedwyl, N.; Wanner, H.; Xoplaki, E.] Univ Bern, Inst Geog Climatol & Meteorol, CH-3012 Bern, Switzerland.
[Wahl, E. R.] Alfred Univ, Div Environm Studies & Geol, NOAA Paleoclimatol, Boulder, CO 80305 USA.
[Zwiers, F. W.] Environm Canada, Div Climate Res, Toronto, ON M3H 5T4, Canada.
[Mann, M. E.] Penn State Univ, Dept Meteorol, Ctr Earth Syst Sci, University Pk, PA 16802 USA.
[Schmidt, G. A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Ammann, C. M.] Natl Ctr Atmospher Res, Climate & Global Dynam Div, Boulder, CO 80307 USA.
[Buckley, B. M.] Lamont Doherty Earth Observ, Tree Ring Lab, Palisades, NY 10964 USA.
[Cobb, K. M.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Esper, J.] Swiss Fed Res Inst WSL, CH-8903 Birmensdorf, Switzerland.
[Goosse, H.] Catholic Univ Louvain, Inst Astron & Geophys G Lemaitre, B-1348 Louvain, Belgium.
[Graham, N.] Hydrol Res Ctr, La Jolla, CA 92130 USA.
[Jansen, E.] Univ Bergen, Dept Geol, Bjerknes Ctr Climate Res, NO-5007 Bergen, Norway.
[Kiefer, T.] PAGES Int Project Off, CH-3007 Bern, Switzerland.
[Kull, C.] Advisory Body Climate Change, CH-3007 Bern, Switzerland.
[Mosley-Thompson, E.] Ohio State Univ, Dept Geog, Columbus, OH 43210 USA.
[Mosley-Thompson, E.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Overpeck, J. T.] Univ Arizona, Inst Study Planet Earth, Tucson, AZ 85721 USA.
[Schulz, M.] Univ Bremen, MARUM Ctr Marine Environm Sci, D-28334 Bremen, Germany.
[Schulz, M.] Univ Bremen, Fac Geosci, D-28334 Bremen, Germany.
[Tudhope, A. W.] Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JW, Midlothian, Scotland.
[Villalba, R.] IANIGLA CRICYT, Argentinean Inst Snow Ice & Environm Sci, RA-5500 Mendoza, Argentina.
[Wolff, E.] British Antarctic Survey, Div Phys Sci, Cambridge CB3 0ET, England.
RP Jones, PD (reprint author), Univ E Anglia, Sch Environm Sci, Climat Res Unit, Norwich NR4 7TJ, Norfolk, England.
EM p.jones@uea.ac.uk
RI Briffa, Keith/C-8834-2009; Jones, Philip/C-8718-2009; Schmidt,
Gavin/D-4427-2012; van Ommen, Tas/B-5020-2012; Lough,
Janice/L-1682-2013; Wolff, Eric/D-7925-2014; Schulz,
Michael/P-7276-2016; Osborn, Timothy/E-9740-2011; Mann,
Michael/B-8472-2017;
OI Jones, Philip/0000-0001-5032-5493; Schmidt, Gavin/0000-0002-2258-0486;
van Ommen, Tas/0000-0002-2463-1718; Wolff, Eric/0000-0002-5914-8531;
Schulz, Michael/0000-0001-6500-2697; Osborn,
Timothy/0000-0001-8425-6799; Mann, Michael/0000-0003-3067-296X; Briffa,
Keith/0000-0003-3323-3639
FU Office of Science (BER); US Department of Energy [DE-FG0298ER62601]; UK
Natural Environment Research Council [NER/T/S/2002/00440]; EC project
Millennium [017008]; Australian Government's Cooperative Research
Centres Programme; Antarctic Ecosystems and Climate CRC; US National
Science Foundation [0542356]; National Center for Atmospheric Research
FX The workshop that was the genesis of this paper, entitled 'Past
Millennia Climate Variability - Synthesis and Outlook' was held in
Wengen, Switzerland from 7 to 10 June 2006 and was organized by the
international joint PAGES (Past Global Changes)/CLIVAR (Climate
Variability and Predictability) intersection working group in concert
with the PAGES office in Bern, Switzerland. The workshop, which was
funded by EPRI (Electric Power Research Institute), PAGES, the Swiss
NCCR-Climate Programme and CLIVAR, represented the continued efforts of
the international PAGES/CLIVAR intersection to identify the key priority
areas for future international collaborative research to advance
understanding of the nature of natural climate variability and the
extent to which human activities are causing change. The authors thank
Henry Diaz, Frank Oldfield and an anonymous reviewer for thorough
reviews. PDJ has been supported by the Office of Science (BER), US
Department of Energy, Grant No. DE-FG0298ER62601). KRB and TJO also
acknowledge funding from UK Natural Environment Research Council
(NER/T/S/2002/00440). JE acknowledges funding from EC project Millennium
(Grant No. 017008). TDvO acknowledges the support of the Australian
Government's Cooperative Research Centres Programme, through the
Antarctic Ecosystems and Climate CRC. HG is a research associate with
Fonds National de la Recherche Scientific, Belgium. MEM acknowledges
support from the US National Science Foundation (Grant No. 0542356). ERW
acknowledges support for new research included in this paper from the
National Center for Atmospheric Research (funded by the National Science
Foundation) and Alfred University, USA.
NR 513
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PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0959-6836
EI 1477-0911
J9 HOLOCENE
JI Holocene
PD FEB
PY 2009
VL 19
IS 1
BP 3
EP 49
DI 10.1177/0959683608098952
PG 47
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 399PU
UT WOS:000262812600001
ER
PT J
AU Manning, CV
Zahnle, KJ
Mckay, CP
AF Manning, Curtis V.
Zahnle, Kevin J.
Mckay, Christopher P.
TI Impact processing of nitrogen on early Mars
SO ICARUS
LA English
DT Article
DE Mars; Mars, atmosphere; Mars, surface; Atmospheres, evolution; Impact
processes
ID MARTIAN ATMOSPHERE; PLANETARY-ATMOSPHERES; TERRESTRIAL PLANETS; ABIOTIC
FIXATION; EROSION; EARTH; DECOMPOSITION; NITRATE; ORIGIN; VENUS
AB An intense impact flux upon a planet having a CO(2) + N(2) atmosphere, such as Mars, provides energy to synthesize nitric oxide, NO, which is likely converted into nitrate minerals. The same impact flux can decompose nitrate minerals if present in the crust. We build a numerical model to study the effects of early impact processes on the evolution of nitrogen in a dominantly CO(2) atmosphere. We model the period of intense post-accretionary bombardment, the roughly 500 Myr period after crustal stabilization that locks in previously accreted volatiles. A best-guess, "fiducial" set of parameters is chosen, with a fixed "veneer" of post-accretionary impactors (delta R = 950 m thick), assumed to contain carbon at 1 wt% (f(g) = 0.01), with a molar C/N ratio of 18, an initial atmospheric pressure of I bar (with CO(2)/N(2) = 36), and a power law impactor mass distribution slope b = 0.75. This model produces a nitrate reservoir RNO(3) similar or equal to 0.5 x 10(19) moles, equivalent to similar to 30 mbars of N(2), during the intense impact phase. Starting with I bar, the atmosphere grows to 2.75 bars. Results of models with variations of parameter values show that R(NO3) responds sluggishly to changes in parameter values. To significantly limit the size of this reservoir, one is required to limit the initial total atmospheric pressure be less than about 0.5 bars, and the impactor volatile content fg to be less than 0.003. The value of fg substantially determines whether the atmosphere grows or not; when f(g) = 0.01, the atmosphere gains about 1.7 bars, while for f(g) = 0.003, the atmosphere gains less than 200 mbars, and for f(g) = 0.001, it loses about 400 mbars. Impact erosion is a minor sink of N, constituting generally less than 10% of the total supply. The loss of impactor volatile plumes can take almost 50% of incoming N and C under fiducial parameters, when atmospheric pressures are low. This nitrogen does not significantly interact with Mars, and hence is not properly delivered. When the initial N is greater than the delivered N, most of the nitrogen ends up as nitrates; when delivered N is larger, most nitrogen ends up in the atmosphere. The reason for this dichotomy seems to be that initial nitrogen is present during the whole bombardment, while delivered N,oil average, only experiences half the bombardment. The operating caveat here is that the above results are all conditioned oil the assumption that impact processes dominate this period of Mars atmospheric evolution. (c) 2008 Elsevier Inc. All rights reserved.
C1 [Manning, Curtis V.; Zahnle, Kevin J.; Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Manning, CV (reprint author), NASA, Ames Res Ctr, Bldg 245,Room 212,MS 245-3, Moffett Field, CA 94035 USA.
EM cmanning@arc.nasa.gov
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2009
VL 199
IS 2
BP 273
EP 285
DI 10.1016/j.icarus.2008.10.015
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 405UV
UT WOS:000263250600005
ER
PT J
AU Carter, LM
Campbell, BA
Watters, TR
Phillips, RJ
Putzig, NE
Safaeinili, A
Plaut, JJ
Okubo, CH
Egan, AF
Seu, R
Biccari, D
Orosei, R
AF Carter, Lynn M.
Campbell, Bruce A.
Watters, Thomas R.
Phillips, Roger J.
Putzig, Nathaniel E.
Safaeinili, Ali
Plaut, Jeffrey J.
Okubo, Chris H.
Egan, Anthony F.
Seu, Roberto
Biccari, Daniela
Orosei, Roberto
TI Shallow radar (SHARAD) sounding observations of the Medusae Fossae
Formation, Mars
SO ICARUS
LA English
DT Article
DE Mars; Mars, surface; Radar observations; Volcanism
ID MARTIAN GEOLOGIC RECORD; VOLCANIC GEOLOGY; DEPOSITS; PATERA; REGION;
DISPERSAL; ERUPTIONS; THARSIS; ICE
AB The SHARAD (shallow radar) sounding radar on the Mars Reconnaissance Orbiter detects subsurface reflections in the eastern and western parts of the Medusae Fossae Formation (MFF). The radar waves penetrate up to 580 in of the MFF and detect clear subsurface interfaces in two locations: west MFF between 150 and 155 degrees E and east MFF between 209 and 213 degrees E. Analysis of SHARAD radargrams suggests that the real part of the permittivity is similar to 3.0, which falls within the range of permittivity values inferred from MARSIS data for thicker parts of the MFF. The SHARAD data cannot uniquely determine the composition of the MFF material, but the low permittivity implies that the upper few hundred meters of the MFF material has a high porosity. One possibility is that the MFF is comprised of low-density welded or interlocked pyroclastic deposits that are capable Of Sustaining the steep-sided yardangs and ridges seen in imagery. The SHARAD surface echo power across the MFF is low relative to typical martian plains, and completely disappears in parts of the east MFF that correspond to the radar-dark Stealth region. These areas are extremely rough at centimeter to meter scales, and the lack of echo power is most likely due to a combination of surface roughness and a low near-surface permittivity that reduces the echo strength from any locally flat regions, There is also no radar evidence for internal layering in any of the SHARAD data for the MFF, despite the fact that tens-of-meters scale layering is apparent in infrared and visible wavelength images of nearby areas. These interfaces may not be detected in SHARAD data if their permittivity contrasts are low, or if the layers are discontinuous. The lack of closely spaced internal radar reflectors suggests that the MFF is not an equatorial analog to the current martian polar deposits, which show clear evidence of multiple internal layers in SHARAD data. (c) 2008 Elsevier Inc. All rights reserved.
C1 [Carter, Lynn M.; Campbell, Bruce A.; Watters, Thomas R.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
[Phillips, Roger J.; Putzig, Nathaniel E.; Egan, Anthony F.] SW Res Inst, Boulder, CO 80302 USA.
[Safaeinili, Ali; Plaut, Jeffrey J.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Okubo, Chris H.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Seu, Roberto; Biccari, Daniela] Univ Roma La Sapienza, Dipartimento INFOCOM, I-00184 Rome, Italy.
[Orosei, Roberto] Inst Nazl Astrofis, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
RP Carter, LM (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 135,POB 37012, Washington, DC 20013 USA.
EM carterl@si.edu
RI Carter, Lynn/D-2937-2012
FU NASA MRO
FX We thank the SHARAD Operations Center team, including Emanuele
Gjacomoni, Federica Russo, Marco Cutigni, Oreste Fuga, and Riccardo
Mecozzi for their assistance with targeting, calibration, and data
processing. We thank the HIRISE and MRO engineering and operations teams
for their work in designing, building, and operating the equipment. We
are grateful to Fabrizio Bernardini for assistance with SHARAD data
processing. Lionel Wilson and an anonymous reviewer provided helpful
comments. The Shallow Subsurface Radar (SHARAD) was provided by the
Italian Space Agency through a contract with Thales Alenia Space Italia,
and it is operated by the INFOCOM Department, University of Rome "La
Sapienza." This work was partially supported through a NASA MRO
Participating Scientist grant to L.M. Carter.
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD FEB
PY 2009
VL 199
IS 2
BP 295
EP 302
DI 10.1016/j.icarus.2008.10.007
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 405UV
UT WOS:000263250600007
ER
PT J
AU Sizemore, HG
Mellon, MT
Golombek, MR
AF Sizemore, Hanna G.
Mellon, Michael T.
Golombek, Matthew R.
TI Ice table depth variability near small rocks at the Phoenix landing
site, Mars: A pre-landing assessment
SO ICARUS
LA English
DT Article
DE Mars; Mars, surface; Ices; Regoliths
ID THERMAL INERTIA; GROUND-ICE; TRANSPORT; STABILITY; SOIL
AB We combine thermal simulations of ground ice stability near small rocks with extrapolations of the abundance of rocks at the Phoenix landing site based oil HiRISE rock Counts to estimate the degree of ice table depth variability within the 3.8 m(2) workspace that can be excavated during the mission. Detailed predictions of this kind are important both to test Current ground-ice theory and to optimize soil investigations after landing. We find that Phoenix will very likely have access to at least one rock in the diameter range 5 cm to I m. Our simulations, which assume the ice to be in diffusive equilibrium with atmospheric water vapor, indicate that all rocks in this size range are associated with an annulus of deep ice-free soil. Ice table depth variability of 1-5 cm is very likely at the landing site clue to the presence of small rocks. Further, there are scenarios in which Phoenix might exploit the presence of individual large rocks and/or the arrangement of small rocks to sample soils at depths > 10 cm below the average depth predicted from orbit (similar to 4 cm). Scale analysis to constrain uncertainties in simulation results indicates that estimates of maximum depths may be somewhat conservative and that ice table depressions associated with individual rocks Could be deeper and laterally more extended than indicated by formal predictions by mm to cm. (c) 2008 Elsevier Inc. All rights reserved.
C1 [Sizemore, Hanna G.; Mellon, Michael T.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Golombek, Matthew R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sizemore, HG (reprint author), Univ Colorado, Atmospher & Space Phys Lab, UCB 392, Boulder, CO 80309 USA.
EM hanna.sizemore@colorado.edu
RI Mellon, Michael/C-3456-2016
NR 19
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2009
VL 199
IS 2
BP 303
EP 309
DI 10.1016/j.icarus.2008.10.008
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 405UV
UT WOS:000263250600008
ER
PT J
AU Lissauer, JJ
Hubickyj, O
D'Angelo, G
Bodenheimer, P
AF Lissauer, Jack J.
Hubickyj, Olenka
D'Angelo, Gennaro
Bodenheimer, Peter
TI Models of Jupiter's growth incorporating thermal and hydrodynamic
constraints
SO ICARUS
LA English
DT Article
DE Jovian planets; Jupiter, interior; Accretion; Planetary formation;
Planet-disk interaction
ID GIANT PLANET FORMATION; OLIGARCHIC GROWTH; GAS DRAG; ACCRETION;
EVOLUTION; PROTOPLANETS; MIGRATION; CAPTURE; MASS; DISK
AB We model the growth Of Jupiter via core nucleated accretion, applying constraints from hydrodynamical processes that result from the disk-planet interaction. We compute the planet's internal structure using a well tested planetary formation code that is based upon a Henyey-type stellar evolution code. The planet's interactions with the protoplanetary disk are calculated using 3-D hydrodynamic simulations. Previous models of Jupiter's growth have taken the radius of the planet to be approximately one Hill sphere radius, RH. However, 3-D hydrodynamic simulations show that only gas within similar to 0.25R(H) remains bound to the planet, with the more distant gas eventually participating in the shear flow of the protoplanetary disk. Therefore in our new simulations, the planet's Outer boundary is placed at the location where gas has the thermal energy to reach the portion of the flow not bound to the planet. We find that the smaller radius increases the time required for planetary growth by similar to 5%. Thermal pressure limits the rate at which a planet less than a few dozen times as massive as Earth can accumulate gas from the protoplanetary disk, whereas hydrodynamics regulates the growth rate for more massive planets. Within a moderately viscous disk, the accretion rate peaks when the planet's mass is about equal to the Mass Of Saturn. In a less viscous disk hydrodynamical limits to accretion are smaller, and the accretion rate peaks at lower mass. Observations suggest that the typical lifetime of massive disks around young stellar objects is similar to 3 Myr. To account for the dissipation of such disks, we perform some of our simulations of Jupiter's growth within a disk whose surface gas density decreases on this timescale. In all of the cases that we simulate, the planet's effective radiating temperature rises to well above 1000 K soon after hydrodynamic limits begin to control the rate of gas accretion and the planet's distended envelope begins to contract. According to Our simulations, proto-Jupiter's distended and thermally-supported envelope was too small to capture the planet's current retinue of irregular satellites as advocated by Pollack et a]. [Pollack,.I.B., Burns, J.A., Tauber, M.E., 1979. Icarus 37, 587-611). Published by Elsevier Inc.
C1 [Lissauer, Jack J.; Hubickyj, Olenka; D'Angelo, Gennaro] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Hubickyj, Olenka; Bodenheimer, Peter] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA.
EM jack.lissauer@nasa.gov
RI D'Angelo, Gennaro/L-7676-2014
OI D'Angelo, Gennaro/0000-0002-2064-0801
FU NASA's Outer Planets Research Program [344-30-99-02]; NASA Origins of
Solar Systems [NNX08AH82G]; NASA High-End Computing Program Systems
[SMD-06-0181, SMD-07-0372]
FX We thank Jeff Cuzzi and two anonymous referees for providing valuable
comments. Primary support for this study was provided by NASA's Outer
Planets Research Program Grant 344-30-99-02; additional support came
from NASA Origins of Solar Systems Grant NNX08AH82G. G.D. is supported
through the NASA Postdoctoral Program. Computational resources for the 3
-D hydrodynamic calculations were provided by the NASA High-End
Computing Program Systems Under Grants SMD-06-0181 and SMD-07-0372.
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2009
VL 199
IS 2
BP 338
EP 350
DI 10.1016/j.icarus.2008.10.004
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 405UV
UT WOS:000263250600012
ER
PT J
AU Fletcher, LN
Orton, GS
Teanby, NA
Irwin, PGJ
Bjoraker, GL
AF Fletcher, L. N.
Orton, G. S.
Teanby, N. A.
Irwin, P. G. J.
Bjoraker, G. L.
TI Methane and its isotopologues on Saturn from Cassini/CIRS observations
SO ICARUS
LA English
DT Article
DE Saturn; Atmospheres, composition; Atmospheres, structure
ID PROBE MASS-SPECTROMETER; GIANT PLANET FORMATION; ISO-SWS OBSERVATIONS;
D/H ISOTOPIC RATIO; RADIATIVE-TRANSFER; UPPER TROPOSPHERE; CLOUD
STRUCTURE; SOLAR-SYSTEM; ATMOSPHERE; JUPITER
AB High spectral resolution observations from the Cassini Composite Infrared Spectrometer [Flasar, F.M., and 44 colleagues, 2004. Space Sci. Rev. 115, 169-297] are analysed to derive new estimates for the mole fractions of CH(4), CH(3)D and (13)CH(4) of (4.7 +/- 0.2) x 10(-3), (3.0 +/- 0.2) x 10(-7) and (5.1 +/- 0.2) x 10-5 respectively, The mole fractions show no hemispherical asymmetries or latitudinal variability. The analysis combines data from the far-IR methane rotational lines and the mid-IR features of methane and its isotopologues, using both the correlated-k retrieval algorithm of [Irwin et a]. [Irwin, P., and 9 colleagues, 2008. J. Quant. Spectrosc. Radiat. Trans. 109, 1136-1150] and a line-by-line approach to evaluate the reliability of the retrieved quantities. C/H was found to be enhanced by 10.9 +/- 0.5 times the solar composition of Grevesse et al. [Grevesse, N., Asplund, M., Sauval, A., 2007. Space Sci. Rev. 130 (1), 105-114], 2.25 +/- 0.55 times larger than the enrichment on Jupiter, and supporting the increasing fractional core mass with distance from the Sun predicted by the core accretion model of planetary formation. A comparison of the jovian and saturnian C/N, C/S and C/P ratios suggests different reservoirs of the trapped volatiles in a primordial solar nebula whose composition varies with distance from the Sun. This is supported by our derived D/H ratio in methane of (1.6 +/- 0.2) x 10(-5), which appears to be smaller than the jovian value of Lellouch et al. [Lellouch, E., Bezard, B., Fouchet, T., Feuchtgruber, H., Encrenaz, T., de Graauw, T., 2001. Astron. Astrophys. 370, 610-622]. Mid-IR emission features provided an estimate of (12)C/(13)C = 91.8(7.8)(+8.4), which is consistent with both the terrestrial ratio and jovian ratio, suggesting that carbon was accreted from a shared reservoir for all of the planets. (c) 2008 Elsevier Inc. All rights reserved.
C1 [Fletcher, L. N.; Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Teanby, N. A.; Irwin, P. G. J.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England.
[Bjoraker, G. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fletcher, LN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM leigh.n.fletcher@jpl.nasa.gov
RI Fletcher, Leigh/D-6093-2011; Bjoraker, Gordon/D-5032-2012;
OI Fletcher, Leigh/0000-0001-5834-9588; Teanby,
Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X
FU NASA Postdoctoral Program at the jet Propulsion Laboratory,
FX Fletcher was supported by an appointment to the NASA Postdoctoral
Program at the jet Propulsion Laboratory, administered by Oak Ridge
Associated Universities through a contract with NASA. Irwin and Teanby
acknowledge the support of the Science and Technology Facilities
Council. Orton and Bjoraker acknowledge support from the Cassini
Project. Some of the radiative-transfer calculations were performed on
JPL supercomputing facilities which were provided by funding from the
JPL Office of the Chief Information Officer. We thank Daniel Gautier and
Thierry Fouchet for useful discussions concerning the implications of
these results, and Emmanuel Lellouch and one anonymous reviewer for
their thorough and constructive criticisms of this manuscript. We
acknowledge the members of the CIRS investigation team who have assisted
in the design of the imaging sequences, instrument commands and other
vital operational tasks, and the Ground Systems Operations for the
Cassini Project.
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2009
VL 199
IS 2
BP 351
EP 367
DI 10.1016/j.icarus.2008.09.019
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 405UV
UT WOS:000263250600013
ER
PT J
AU Helled, R
Schubert, G
Anderson, JD
AF Helled, Ravit
Schubert, Gerald
Anderson, John D.
TI Empirical models of pressure and density in Saturn's interior:
Implications for the helium concentration, its depth dependence, and
Saturn's precession rate
SO ICARUS
LA English
DT Article
DE Saturn; Saturn, interior; Abundances, interiors
ID GIANT PLANETS; PHASE-SEPARATION; VOYAGER MEASUREMENTS; FLUID PLANETS;
JUPITER; OCCULTATION; EVOLUTION; SYSTEM; ATMOSPHERE; EXOPLANETS
AB We present 'empirical' models (pressure vs. density) of Saturn's interior constrained by the gravitational coefficients J(2), J(4), and J(6) for different assumed rotation rates of the planet. The empirical pressure-density profile is interpreted in terms of a hydrogen and helium physical equation of state to deduce the hydrogen to helium ratio in Saturn and to constrain the depth dependence of helium and heavy element abundances. The planet's internal structure (pressure vs. density) and composition are found to be insensitive to the assumed rotation rate for periods between 10h:32m:35s and 10h:41m:35s. We find that helium is depleted in the upper envelope, while in the high pressure region (P greater than or similar to 1 Mbar) either the helium abundance or the concentration of heavier elements is significantly enhance Taking the ratio of hydrogen to helium in Saturn to be solar, we find that the maximum mass of heavy elements in Saturn's interior ranges from similar to 6 to 20 M-circle plus. The empirical models of Saturn's interior yield a moment of inertia factor varying from 0.22271 to 0.22599 for rotation periods between 10h:32m:35s and 10h:41m:35s, respectively. A long-term precession rate of about 0.754 '' yr(-1) is found to be consistent with the derived moment of inertia values and assumed rotation rates over the entire range of investigated rotation rates. This suggests that the long-term precession period of Saturn is somewhat shorter than the generally assumed value of 1.77 x 10(6) years inferred from modeling and observations. (c) 2008 Elsevier Inc. All rights reserved.
C1 [Helled, Ravit; Schubert, Gerald] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Helled, Ravit; Schubert, Gerald] Univ Calif Los Angeles, Inst Geophys & Planetary Sci, Los Angeles, CA 90095 USA.
[Anderson, John D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Helled, R (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
EM rhelled@ess.ucla.edu
NR 43
TC 16
Z9 16
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 2009
VL 199
IS 2
BP 368
EP 377
DI 10.1016/j.icarus.2008.10.005
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 405UV
UT WOS:000263250600014
ER
PT J
AU Nelson, RM
Kamp, LW
Matson, DL
Irwin, PGJ
Baines, KH
Boryta, MD
Leader, FE
Jaumann, R
Smythe, WD
Sotin, C
Clark, RN
Cruikshank, DP
Drossart, P
Pearl, JC
Hapke, BW
Lunine, J
Combes, M
Bellucci, G
Bibring, JP
Capaccioni, F
Cerroni, P
Coradini, A
Formisano, V
Filacchione, G
Langevin, RY
McCord, TB
Mennella, V
Nicholson, PD
Sicardy, B
AF Nelson, R. M.
Kamp, L. W.
Matson, D. L.
Irwin, P. G. J.
Baines, K. H.
Boryta, M. D.
Leader, F. E.
Jaumann, R.
Smythe, W. D.
Sotin, C.
Clark, R. N.
Cruikshank, D. P.
Drossart, P.
Pearl, J. C.
Hapke, B. W.
Lunine, J.
Combes, M.
Bellucci, G.
Bibring, J. -P.
Capaccioni, F.
Cerroni, P.
Coradini, A.
Formisano, V.
Filacchione, G.
Langevin, R. Y.
McCord, T. B.
Mennella, V.
Nicholson, P. D.
Sicardy, B.
TI Saturn's Titan: Surface change, ammonia, and implications for
atmospheric and tectonic activity
SO ICARUS
LA English
DT Article
DE Titan; Spectrophotometry; Infrared observations; Ices; Spectroscopy
ID TROPOSPHERIC CLOUDS; MIDLATITUDE CLOUDS; INTERNAL STRUCTURE; ADAPTIVE
OPTICS; 9500 CM(-1); MU-M; HAZE; ABSORPTION; SCATTERING; ALBEDO
AB Titan is known to have a Young Surface. Here we present evidence from the Cassini Visual and Infrared Mapping spectrometer that it is currently geologically active. We report that changes in the near-infrared reflectance of a 73,000 km 2 area on Titan (latitude 26 degrees S, longitude 78 degrees W) occurred between July 2004 and March of 2006. The reflectance of the area increased by a factor of two between July 2004 and March-April 2005; it then returned to the July 2004 level by November 2005. By late December 2005 the reflectance had surged upward again, establishing a new maximum. Thereafter, it trended downward for the next three months. Detailed spectrophotometric analyses suggest these changes happen at or very near the surface. The spectral differences between the region and its surroundings rule out changes in the distribution of the ices of reasonably expected materials such as H(2)O, CO(2), and CH(4) as possible causes. Remarkably, the change is spectrally consistent with the deposition and removal of NH(3) frost over a water ice substrate. NH3 has been proposed as a constituent of Titan's interior and has never been reported on the surface. The detection of NH3 frost on the surface might possibly be explained by episodic effusive events occur which bring juvenile ammonia from the interior to the surface. If so. its decomposition would feed nitrogen to the atmosphere now and in the future. The lateral extent of the region exceeds that of active areas on the Earth (Hawaii) or to (Loki). (c) 2008 Elsevier Inc. All rights reserved.
C1 [Nelson, R. M.; Kamp, L. W.; Matson, D. L.; Baines, K. H.; Leader, F. E.; Smythe, W. D.] NASA, Div Earth & Space Sci, JPL, Pasadena, CA 91109 USA.
[Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England.
[Boryta, M. D.] Mt San Antonio Coll, Dept Geol, Walnut, CA 91789 USA.
[Jaumann, R.] DLR, Inst Planetaty Explorat, Berlin, Germany.
[Sotin, C.] Univ Nantes, Lab Planetol & Geodynam, Nantes, France.
[Clark, R. N.] US Geol Survey, Fed Ctr, Lakewood, CO 80225 USA.
[Cruikshank, D. P.] NASA AMES, Moffett Field, CA 94035 USA.
[Drossart, P.; Sicardy, B.] Observ Paris, F-92195 Meudon, France.
[Pearl, J. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hapke, B. W.] Univ Pittsburgh, Pittsburgh, PA 15260 USA.
[Lunine, J.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Combes, M.] Observ Paris, Off Director, F-75014 Paris, France.
[Bellucci, G.; Capaccioni, F.; Cerroni, P.; Coradini, A.; Formisano, V.; Filacchione, G.] Ist Astrofis Spaziale Fis Cosm, I-00133 Rome, Italy.
[Bibring, J. -P.; Langevin, R. Y.] Univ Paris 11, Fac Sci, F-91405 Orsay, France.
[McCord, T. B.] Univ Washington, Winthrop, WA 98862 USA.
[Mennella, V.] Osserv Astron Capodimonte, I-80131 Naples, Italy.
[Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Nelson, RM (reprint author), NASA, Div Earth & Space Sci, JPL, Mail Stop 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.m.nelson@jpl.nasa.gov
OI Cerroni, Priscilla/0000-0003-0239-2741; Bellucci,
Giancarlo/0000-0003-0867-8679; Capaccioni, Fabrizio/0000-0003-1631-4314;
Filacchione, Gianrico/0000-0001-9567-0055; Irwin,
Patrick/0000-0002-6772-384X
NR 42
TC 43
Z9 43
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 2009
VL 199
IS 2
BP 429
EP 441
DI 10.1016/j.icarus.2008.08.013
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 405UV
UT WOS:000263250600018
ER
PT J
AU Seo, H
Kim, SJ
Kim, JH
Geballe, TR
Courtin, R
Brown, LR
AF Seo, Haingja
Kim, Sang Joon
Kim, Joo Hyeon
Geballe, Thomas R.
Courtin, Regis
Brown, Linda R.
TI Titan at 3 microns: Newly identified spectral features and an improved
analysis of haze opacity
SO ICARUS
LA English
DT Article
DE Titan; Atmospheres, composition; Spectroscopy; Infrared observations;
Saturn; satellites
ID HIGH-RESOLUTION SPECTROSCOPY; JOVIAN TEMPERATURE STRUCTURE; NEAR-IR
SPECTROPHOTOMETRY; NORTH POLAR STRATOSPHERE; ATMOSPHERIC TEMPERATURES;
MIDLATITUDE CLOUDS; CONDENSATE CLOUDS; EMISSION-SPECTRUM; THERMAL
EMISSION; INFRARED-SPECTRA
AB We have reanalyzed the high-resolution spectrum of Titan between 2.87 and 3.12 mu m observed with NIRSPEC/Keck II on 2001 Nov. 21 in southern summer, using updated CH(3)D and C(2)H(6) line-by-line models. From new synthetic spectra, we identify all but a few of the previously unidentified significant absorption spectral features in this wavelength range as due to these two species, both of which had been previously detected by Voyager and ground-based observations at other wavelengths. We also derive opacities and reflectivities of haze particles as functions of altitude for the 2.87-2.92 mu m wavelength range, where Titan's atmosphere is partially transparent down to the surface. The extinction per unit altitude is observed to increase from 100 km (similar to 8 mbar) toward lower altitude. The derived total optical depth is approximately 1.1 for the 2.97-2.92 mu m range. At wavelengths increasing beyond 2.92 mu m the haze layers become much more optically thick, and the surface is rapidly hidden from view. These conclusions apply to equatorial and southern-temperate regions on Titan, excluding polar regions. We also find it unlikely that there is a large enhancement of the tropospheric CH(4) mole fraction over the Value reported from analysis of the Huygens/GCMS observations. (c) 2008 Elsevier Inc. All rights reserved.
C1 [Seo, Haingja; Kim, Sang Joon; Kim, Joo Hyeon] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, South Korea.
[Geballe, Thomas R.] Gemini Observ, Hilo, HI 96720 USA.
[Courtin, Regis] Observ Paris, CNRS, LESIA, F-92195 Meudon, France.
[Brown, Linda R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kim, SJ (reprint author), Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, South Korea.
EM sjkim1@khu.ac.kr
RI Kim, Sang Joon/E-2383-2013
FU Korea Science and Engineering Foundation [R01-2008-00020002-0]
FX The observational data on which this paper is based were obtained on the
W.M. Keck Observatory by Gemini staff, supported by the Gemini
Observatory, which is operated by the Association of Universities for
Research in Astronomy on behalf of the International Gemini partnership
of Argentina, Australia, Brazil, Canada Chile, the United Kingdom, and
the United States of America' The W.M. Keck Observatory is operated as a
scientific partnership among the California Institute of Technology, the
University of California, and the National Aeronuatics and Space
Administration. T.R.G.'s research is supported by the Gemini
Observatory. Part of the research described in this paper was performed
at the jet Propulsion Laboratory, California Institute of Technology,
under contract with The National Aeronautics and Space Administration.
We thank two anonymous referees, whose detailed comments improved the
paper significantly. SJX acknowledges a support from the Korea Science
and Engineering Foundation (R01-2008-00020002-0).
NR 61
TC 13
Z9 13
U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2009
VL 199
IS 2
BP 449
EP 457
DI 10.1016/j.icarus.2008.09.017
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 405UV
UT WOS:000263250600020
ER
PT J
AU Groussin, O
Lamy, R
Toth, I
Kelley, M
Fernandez, Y
A'Hearn, M
Campins, H
Licandro, J
Lisse, C
Lowry, S
Meech, K
Snodgrass, C
AF Groussin, O.
Lamy, R.
Toth, I.
Kelley, M.
Fernandez, Y.
A'Hearn, M.
Campins, H.
Licandro, J.
Lisse, C.
Lowry, S.
Meech, K.
Snodgrass, C.
TI The size and thermal properties of the nucleus of Comet 22P/Kopff
SO ICARUS
LA English
DT Article
DE Comets; Comets, nucleus
ID SPITZER-SPACE-TELESCOPE; JUPITER FAMILY COMETS; DISTANT COMETS;
9P/TEMPEL-1; MAGNITUDES; PHOTOMETRY; ASTEROIDS
AB We detected the nucleus of Comet 22P/Kopff at 4.87 AU from the Sun with the two IRS peak-up cameras of the Spitzer Space Telescope on April 19, 2007. Using the thermal model of [Groussin, O., and 15 colleagues, 2007. Icarus 187, 16-25], we derive a nucleus size of 1.89 +/- 0.16 km, in agreement with [Lamy, P., Toth. I., Jorda, L., Groussin, 0., A'Hearn, M.F, Weaver, H.A., 2002. Icarus 156, 442-455], and a thermal inertia 1 <= 30 J K(-1) m(-2) S(-1/2). (C) 2008 Elsevier Inc. All rights reserved.
C1 [Groussin, O.; Lamy, R.] Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Toth, I.] Konkoly Observ Budapest, H-1525 Budapest, Hungary.
[Kelley, M.; Fernandez, Y.; Campins, H.] Univ Cent Florida, Dept Phys, Orlando, FL 32828 USA.
[A'Hearn, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Licandro, J.] Inst Astrofis Canarias, Tenerife 38205, Spain.
[Lisse, C.] Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Dept Space, Laurel, MD 20723 USA.
[Lowry, S.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
[Meech, K.] Univ Hawaii, Honolulu, HI 96822 USA.
[Snodgrass, C.] European So Observ, Santiago 19, Chile.
RP Groussin, O (reprint author), Lab Astrophys Marseille, Technopole Marseille Etoile,38 Rue Frederic Jolio, F-13388 Marseille 13, France.
EM olivier.groussin@oamp.fr
RI Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Kelley, Michael/0000-0002-6702-7676;
Fernandez, Yanga/0000-0003-1156-9721; Snodgrass,
Colin/0000-0001-9328-2905
FU NASA
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 through an award issued by
JPL/Caltech.
NR 18
TC 10
Z9 10
U1 0
U2 0
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 2009
VL 199
IS 2
BP 568
EP 570
DI 10.1016/j.icarus.2008.07.015
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 405UV
UT WOS:000263250600031
ER
PT J
AU Riggan, PJ
Hoffman, JW
Brass, JA
AF Riggan, Philip J.
Hoffman, James W.
Brass, James A.
TI Estimating Fire Properties by Remote Sensing
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
AB Contemporary knowledge of the role of fire in the global environment is limited by inadequate measurements of the extent and impact of individual fires. Observations by operational polar-orbiting and geostationary satellites provide an indication of fire occurrence but are ill-suited for estimating the temperature, area, or radiant emissions of active wildland and agricultural fires. Simulations here of synthetic remote sensing pixels comprised of observed high-resolution fire data together with ash or vegetation background demonstrate that fire properties including flame temperature, fractional area, and radiant-energy flux can best be estimated from concurrent radiance measurements at wavelengths near 1.6, 3.9, and 12 mu m. Successful observations at night may be made at scales to at least I km for the cluster of fire data simulated herein. During the daytime, uncertainty in the composition of the background and its reflection of solar radiation would limit successful observations to a scale of approximately 100 m or less. Measurements at three wavelengths in the long-wave infrared would be unaffected by reflected solar radiation and could be applied to separate flame properties in a binary system of flame and background. However, likely variation in the composition of the background and its temperature limit the approach to measurements that are of high resolution in relation to the scale of the flaming front. Alternative approaches using radiances at wavelengths near 4 and 12 mu m alone must fail absent a correction for the background, yet the correction is made imprecise by uncertainty in composition of the background where it comprises more than one-third of a pixel.
C1 [Riggan, Philip J.] US Forest Serv, USDA, Pacific SW Res Stn, Riverside, CA 92507 USA.
[Hoffman, James W.] Space Instruments Inc, Encinitas, CA 92024 USA.
[Brass, James A.] NASA, Ames Res Ctr, Moffett Federal Airfield, CA 94035 USA.
RP Riggan, PJ (reprint author), US Forest Serv, USDA, Pacific SW Res Stn, 4955 Canyon Crest Dr, Riverside, CA 92507 USA.
FU Research Joint Venture Agreement; USDA Forest Service, International
Programs; US Agency for International Development
FX This research was supported by a Research Joint Venture Agreement
between Space Instruments, Inc., and the Pacific Southwest Research
Station, USDA Forest Service; by the USDA Forest Service, International
Programs; and by the US Agency for International Development. Trade
names, commercial products, and enterprises are mentioned solely for
information. No endorsement by the US Department of Agriculture is
implied.
NR 5
TC 1
Z9 1
U1 1
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0885-8985
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD FEB
PY 2009
VL 24
IS 2
BP 13
EP 19
PG 7
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA 411VL
UT WOS:000263681000002
ER
PT J
AU Morelli, G
AF Morelli, Gene
TI Fit to Fly
SO IEEE CONTROL SYSTEMS MAGAZINE
LA English
DT Editorial Material
C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Morelli, G (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 2
TC 0
Z9 0
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1066-033X
J9 IEEE CONTR SYST MAG
JI IEEE Control Syst. Mag.
PD FEB
PY 2009
VL 29
IS 1
BP 14
EP 18
DI 10.1109/MCS.2008.930833
PG 5
WC Automation & Control Systems
SC Automation & Control Systems
GA 395SE
UT WOS:000262543000004
ER
PT J
AU Thomas, B
Rea, S
Moyna, B
Alderman, B
Matheson, D
AF Thomas, Bertrand
Rea, Simon
Moyna, Brian
Alderman, Byron
Matheson, Dave
TI A 320-360 GHz Subharmonically Pumped Image Rejection. Mixer Using Planar
Schottky Diodes
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE Image rejection; sideband separation; submillimeter wave; subharmonic
mixer; planar Schottky diodes
ID MILLIMETER; DESIGN
AB This letter presents the design, fabrication and test of an integrated 320-360 GHz subharmonic image rejection mixer using planar Schottky diodes. The integrated circuit uses two sepearate anti-parallel pairs of diodes mounted onto a single quartz.. based circuit. Measurement results give best single sideband (SSB receiver noise temperatures of approximately 34110 K at 340 GHz, with an image rejection from 7.2 to 24.1 dB over the 320-360 GHz frequency band. This work represents the first demonstration of a Schottky based SSB mixer at submillimeter wavelengths.
C1 [Thomas, Bertrand; Alderman, Byron; Matheson, Dave] Rutherford Appleton Lab, STFC, Didcot OX11 0QX, Oxon, England.
[Rea, Simon] EADS ASTRIUM Ltd, Portsmouth PO3 5PU, Hants, England.
RP Thomas, B (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM d.matheson@rl.ac.uk
NR 19
TC 12
Z9 16
U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1531-1309
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD FEB
PY 2009
VL 19
IS 2
BP 101
EP 103
DI 10.1109/LMWC.2009.2011332
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA 409AR
UT WOS:000263479100017
ER
PT J
AU Ponchak, GE
Jordan, JL
Scardelletti, MC
AF Ponchak, George E.
Jordan, Jennifer L.
Scardelletti, Maximilian C.
TI High Temperature Characteristics of Coplanar Waveguide on R-Plane
Sapphire and Alumina
SO IEEE TRANSACTIONS ON ADVANCED PACKAGING
LA English
DT Article
DE Alumina; attenuation; coplanar waveguide; effective permittivity; high
temperature; sapphire
ID MICROWAVE MEASUREMENT; PERMITTIVITY; ATTENUATION; PROBE
AB This paper presents the characteristics of coplanar waveguide transmission lines on R-plane sapphire and alumina over the temperature range of 25 degrees C-400 degrees C and the frequency range of 45 MHz-50 GHz. A thru-reflect-line calibration technique and open circuited terminated stubs are used to extract the attenuation and effective permittivity. It is shown that the effective permittivity of the transmission lines and, therefore, the relative dielectric constant of the two substrates increase linearly with temperature. The attenuation of the coplanar waveguide varies linearly with temperature through 200 degrees C, and increases at a greater rate above 200 degrees C.
C1 [Ponchak, George E.; Jordan, Jennifer L.; Scardelletti, Maximilian C.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Ponchak, GE (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM george.ponchak@ieee.org; jennifer.l.jordan@nasa.gov;
maxim-ilian.c.scardelletti@nasa.gov
FU NASA Integrated Vehicle Health Management (IVHM) program
FX Manuscript received August 28, 2007; revised December 11, 2007. Current
version published February 13, 2009. This work was supported by the NASA
Integrated Vehicle Health Management (IVHM) program. This work was
recommended for publication by Associate Editor O. Ramahi upon
evaluation of the reviewers comments.
NR 28
TC 5
Z9 5
U1 1
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1521-3323
J9 IEEE T ADV PACKAGING
JI IEEE Trans. Adv. Packag.
PD FEB
PY 2009
VL 32
IS 1
BP 146
EP 151
DI 10.1109/TADVP.2008.2009123
PG 6
WC Engineering, Manufacturing; Engineering, Electrical & Electronic;
Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 413BN
UT WOS:000263768000018
ER
PT J
AU Xu, SH
Rahmat-Samii, Y
Imbriale, WA
AF Xu, Shenheng
Rahmat-Samii, Yahya
Imbriale, William A.
TI Subreflectarrays for Reflector Surface Distortion Compensation
SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION
LA English
DT Article
DE Distortion compensation; reflectarray; reflector antenna
ID VARIABLE SIZE; ANTENNAS; DESIGN; REFLECTARRAYS; PATCHES
AB With the increasing interest in the applications of large deployable reflector antennas operating at high frequencies, the requirement on the reflector surface accuracy becomes more demanding. Thermal effects inevitably cause certain reflector surface distortions, thus degrading the overall antenna performance. This paper introduces a novel reflector surface distortion compensation technique using a subreflectarray and presents detailed discussions. A microstrip reflectarray is used as a subreflector, illuminated by a primary feed. By properly adjusting the additional phase shift provided by the subreflectarray, the aperture phase errors caused by the main reflector surface distortions are compensated, resulting in a considerably improved antenna performance. As an example, a distorted 20-m offset parabolic reflector antenna operating at X-band is successfully compensated by a subreflectarray, and the simulation results are compared with those obtained by array feed and shaped subreflector compensation techniques. The microstrip subreflectarray is low-profile, lightweight, and cost-effective. Only one primary feed is required, and a reconfigurable design can be achieved if electronically reconfigurable reflectarray elements are adopted.
C1 [Xu, Shenheng; Rahmat-Samii, Yahya] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
[Imbriale, William A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Xu, SH (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
EM shxu@ee.ucla.edu; rahmat@ee.ucla.edu; imbriale@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration
FX This work was supported in part by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 25
TC 18
Z9 21
U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-926X
EI 1558-2221
J9 IEEE T ANTENN PROPAG
JI IEEE Trans. Antennas Propag.
PD FEB
PY 2009
VL 57
IS 2
BP 364
EP 372
DI 10.1109/TAP.2008.2011250
PG 9
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 444MI
UT WOS:000265984700008
ER
PT J
AU Inan, OT
Etemadi, M
Sanchez, ME
Marcu, O
Bhattacharya, S
Kovacs, GTA
AF Inan, Omer T.
Etemadi, Mozziyar
Sanchez, Max E.
Marcu, Oana
Bhattacharya, Sharmila
Kovacs, Gregory T. A.
TI A Miniaturized Video System for Monitoring the Locomotor Activity of
Walking Drosophila Melanogaster in Space and Terrestrial Settings
SO IEEE TRANSACTIONS ON BIOMEDICAL ENGINEERING
LA English
DT Article
DE Activity monitor; Drosophila melanogaster; locomotor behavior; space
biology
ID MICROGRAVITY; TEMPERATURE; BEHAVIOR
AB A novel method is presented for monitoring movement of Drosophila melanogaster (the fruit fly) in space. Transient fly movements were captured by a $60,2.5-cm-cubed monochrome video camera imaging flies illuminated by a uniform light source. The video signal from this camera was bandpass filtered (0.3-10 Hz) and amplified by an analog circuit to extract the average light changes as a function of time. The raw activity signal output of this circuit was recorded on a computer and digitally processed to extract the fly movement "events" from the waveform. These events corresponded to flies entering and leaving the image and were used for extracting activity parameters such as interevent duration. The efficacy of the system in quantifying locomotor activity was evaluated by varying environmental temperature and measuring the activity level of the flies. The results of this experiment matched those reported in the literature.
C1 [Inan, Omer T.; Etemadi, Mozziyar; Kovacs, Gregory T. A.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
[Sanchez, Max E.; Marcu, Oana] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Kovacs, Gregory T. A.] Stanford Univ, Dept Med, Stanford, CA 94305 USA.
RP Inan, OT (reprint author), Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
EM omeri@stanford.edu
FU National Aeronautics and Space Administration's (NASA) National Center
for Space Biological Technologies [NNA04CC32A]
FX Manuscript received December 19, 2007 revised June 16. 2008. First
published October 3, 2008: current version published March 25, 2009.
This work was supported by the National Aeronautics and Space
Administration's (NASA) National Center for Space Biological
Technologies under Cooperative Agreement NNA04CC32A. Asterisk indicates
corresponding authol:
NR 15
TC 3
Z9 3
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 0018-9294
J9 IEEE T BIO-MED ENG
JI IEEE Trans. Biomed. Eng.
PD FEB
PY 2009
VL 56
IS 2
BP 522
EP 524
DI 10.1109/TBME.2008.2006018
PG 3
WC Engineering, Biomedical
SC Engineering
GA 435VZ
UT WOS:000265372700039
PM 19272912
ER
PT J
AU Colliander, A
Torres, F
Corbella, I
AF Colliander, Andreas
Torres, Francesc
Corbella, Ignasi
TI Correlation Denormalization in Interferometric or Polarimetric
Radiometers: A Unified Approach
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Denormalization; interferometric radiometry; Microwave Imaging
Radiometer using Aperture Synthesis (MIRAS); polarimetric radiometer;
synthetic aperture radiometry
ID SYNTHETIC-APERTURE RADIOMETER; MICROWAVE RADIOMETER; SMOS CALIBRATION;
SOIL-MOISTURE; MIRAS; SALINITY; MISSION; SPACE; EARTH
AB This paper presents a general analysis of correlation measurements in an interferometer or a