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 TC 21 Z9 21 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 Z9 15 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 TC 2 Z9 2 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 TC 14 Z9 14 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 TC 3 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 TC 3 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 TC 16 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 TC 5 Z9 5 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 TC 4 Z9 4 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 TC 13 Z9 13 U1 3 U2 20 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 TC 26 Z9 26 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 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 TC 16 Z9 16 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 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 TC 90 Z9 92 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 TC 13 Z9 13 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD 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 TC 40 Z9 40 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 TC 10 Z9 10 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 TC 42 Z9 42 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 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 TC 94 Z9 94 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 11 Z9 11 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 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 TC 12 Z9 12 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 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 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 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 TC 34 Z9 34 U1 0 U2 2 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 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. NR 116 TC 40 Z9 40 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 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 TC 27 Z9 28 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2009 VL 495 IS 1 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 TC 21 Z9 22 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 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. NR 40 TC 8 Z9 8 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2009 VL 494 IS 3 BP 1031 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 Z9 39 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 TC 20 Z9 20 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 TC 29 Z9 29 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 Z9 49 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 Z9 38 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 TC 35 Z9 35 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 25 Z9 25 U1 0 U2 2 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 TC 83 Z9 84 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD 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 TC 21 Z9 21 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD 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 TC 70 Z9 70 U1 3 U2 10 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 Z9 20 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 TC 1020 Z9 1030 U1 0 U2 26 PU IOP PUBLISHING LTD 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 PY 2009 VL 180 IS 2 BP 225 EP 245 DI 10.1088/0067-0049/180/2/225 PG 21 WC Astronomy & Astrophysics 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 TC 62 Z9 62 U1 0 U2 1 PU IOP PUBLISHING LTD 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 PY 2009 VL 180 IS 2 BP 246 EP 264 DI 10.1088/0067-0049/180/2/246 PG 19 WC Astronomy & Astrophysics 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. NR 51 TC 159 Z9 160 U1 0 U2 3 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 265 EP 282 DI 10.1088/0067-0049/180/2/265 PG 18 WC Astronomy & Astrophysics 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. NR 27 TC 97 Z9 97 U1 0 U2 2 PU IOP PUBLISHING LTD 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 PY 2009 VL 180 IS 2 BP 283 EP 295 DI 10.1088/0067-0049/180/2/283 PG 13 WC Astronomy & Astrophysics 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 NR 30 TC 259 Z9 261 U1 1 U2 7 PU IOP PUBLISHING LTD 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 PY 2009 VL 180 IS 2 BP 296 EP 305 DI 10.1088/0067-0049/180/2/296 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 TC 35 Z9 37 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 TC 38 Z9 39 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 TC 41 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 TC 27 Z9 28 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 TC 26 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 TC 339 Z9 351 U1 14 U2 228 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 NR 33 TC 15 Z9 15 U1 1 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 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. NR 31 TC 41 Z9 42 U1 2 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 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 TC 4 Z9 4 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 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. NR 38 TC 113 Z9 114 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD 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. NR 72 TC 56 Z9 56 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD 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