FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Frierson, DMW Kim, D Kang, IS Lee, MI Lin, JL AF Frierson, Dargan M. W. Kim, Daehyun Kang, In-Sik Lee, Myong-In Lin, Jialin TI Structure of AGCM-Simulated Convectively Coupled Kelvin Waves and Sensitivity to Convective Parameterization SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID MADDEN-JULIAN OSCILLATION; TROPICAL INTRASEASONAL VARIABILITY; GENERAL-CIRCULATION MODELS; SIMPLE MULTICLOUD PARAMETERIZATION; CLOUD-RADIATIVE FEEDBACKS; EQUATORIAL WAVES; PART I; STRATIFORM INSTABILITY; WALKER CIRCULATION; VERTICAL STRUCTURE AB A study of the convectively coupled Kelvin wave (CCKW) properties from a series of atmospheric general circulation model experiments over observed sea surface temperatures is presented. The simulations are performed with two different convection schemes (a mass flux scheme and a moisture convergence scheme) using a range of convective triggers, which inhibit convection in different ways. Increasing the strength of the convective trigger leads to significantly slower and more intense CCKW activity in both convection schemes. With the most stringent trigger in the mass flux scheme, the waves have realistic speed and variance and also exhibit clear shallow-to-deep-to-stratiform phase tilts in the vertical, as in observations. While adding a moisture trigger results in vertical phase tilts in the mass flux scheme, the moisture convergence scheme CCKWs show no such phase tilts even with a stringent convective trigger. The changes in phase speed in the simulations are interpreted using the concept of "gross moist stability" (GMS). Inhibition of convection results in a more unstable tropical atmosphere in the time mean, and convection is shallower on average as well. Both of these effects lead to a smaller GMS, which leads to slower propagation of the waves, as expected from theoretical studies. Effects such as changes in radiative heating, atmospheric humidity, and vertical velocity following the wave have a relatively small effect on the GMS as compared with the time mean state determined by the convection scheme. C1 [Frierson, Dargan M. W.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Kim, Daehyun; Kang, In-Sik] Seoul Natl Univ, Seoul, South Korea. [Lee, Myong-In] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lin, Jialin] Ohio State Univ, Columbus, OH 43210 USA. RP Frierson, DMW (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA. EM dargan@atmos.washington.edu RI Frierson, Dargan/F-1763-2010; 안, 민섭/D-9972-2015; OI Frierson, Dargan/0000-0001-8952-5644; Lee, Myong-In/0000-0001-8983-8624 FU NSF [ATM-0846641]; University of Washington; Korean Government (MEST) [NRF-2009-C1AAA001-2009-0093042]; second phase of Brain Korea 21 FX DMWF is supported by NSF Grant ATM-0846641 and a startup grant from the University of Washington. ISK is supported by the National Research Foundation of Korea Grant Funded by Korean Government (MEST) (NRF-2009-C1AAA001-2009-0093042) and the second phase of Brain Korea 21. NR 90 TC 27 Z9 27 U1 0 U2 12 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 JAN PY 2011 VL 68 IS 1 BP 26 EP 45 DI 10.1175/2010JAS3356.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 710WF UT WOS:000286547000003 ER PT J AU Leifer, N Smart, MC Prakash, GKS Gonzalez, L Sanchez, L Smith, KA Bhalla, P Grey, CP Greenbaum, SG AF Leifer, N. Smart, M. C. Prakash, G. K. S. Gonzalez, L. Sanchez, L. Smith, K. A. Bhalla, P. Grey, C. P. Greenbaum, S. G. TI C-13 Solid State NMR Suggests Unusual Breakdown Products in SEI Formation on Lithium Ion Electrodes SO JOURNAL OF THE ELECTROCHEMICAL SOCIETY LA English DT Article ID RAY PHOTOELECTRON-SPECTROSCOPY; GRAPHITE NEGATIVE-ELECTRODE; NUCLEAR-MAGNETIC-RESONANCE; ALKYL CARBONATE SOLUTIONS; PROPYLENE CARBONATE; SURFACE-CHEMISTRY; ELECTROCHEMICAL REDUCTION; DEGRADATION-PRODUCTS; THERMAL-STABILITY; RECHARGEABLE BATTERIES AB This study investigates the organic components of the solid electrolyte interphase (SEI) on the carbonaceous anodic electrode in LiCoO2 batteries using solid-state nuclear magnetic resonance (NMR) techniques. The electrolyte solvents, ethylene carbonate and diethyl carbonate, were enriched on the carbonyl carbon prior to cell assembly and conditioning in an attempt to trace the breakdown pathways of these components. A strong signal was seen, demonstrating that the carbonyl carbons of both electrolytes survive in some reasonable quantity as insoluble breakdown products on the rinsed electrode surface. This confirms that the fate of these carbons as consumed in the formation of CO2 is either not unique, or not as final product. Furthermore the central carbonyl carbon survives, not as an intact carbonyl species, but instead in the form of compounds in which the carbon-oxygen double bond has been disrupted. Formation of this class of species is likely initiated by a nucleophilic attack on the carbonyl carbon by one or more radical, alkoxy, carbanion or fluorine-containing ionic species formed from solvent and/or salt breakdown. These results suggest a new family of electrolyte breakdown products, predominantly consisting of binary, tertiary and/or quaternary ether-type compounds (i.e., orthocarbonates and orthoesters), as well as fluorine-containing alkoxy compounds. (C) 2011 The Electrochemical Society. [DOI: 10.1149/1.3559551] All rights reserved. C1 [Leifer, N.; Gonzalez, L.; Sanchez, L.; Greenbaum, S. G.] CUNY, Hunter Coll, Dept Phys, New York, NY 10065 USA. [Smart, M. C.; Smith, K. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Prakash, G. K. S.; Bhalla, P.] Univ So Calif, Loker Hydrocarbon Res Inst, Los Angeles, CA 90089 USA. [Grey, C. P.] SUNY Stony Brook, Dept Chem, Stony Brook, NY 11794 USA. RP Leifer, N (reprint author), CUNY, Hunter Coll, Dept Phys, New York, NY 10065 USA. EM steve.greenbaum@hunter.cuny.edu FU DCI; National Institutes of Health (NIH) [RR 03037]; National Aeronautics and Space Administration (NASA) FX The authors of this paper would like to acknowledge the help of Dr. Boris Itin at the New York Structural Biology Center, financial support from the DCI Postdoctoral Fellows Program and the National Institutes of Health (NIH) Infrastructure Grant (RR 03037). L. Gonzalez and L. Sanchez acknowledge the NIH funded Minority Access to Research Careers (MARC) and the Minority Biomedical Research Support - Research Initiative for Scientific Enhancement (MBRS-RISE) programs for providing scholarships. Some work described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). CPG thanks Thomas Koester for critical reading of the manuscript. NL thanks Hugo Gottlieb for useful discussions. NR 75 TC 25 Z9 26 U1 4 U2 63 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 0013-4651 J9 J ELECTROCHEM SOC JI J. Electrochem. Soc. PY 2011 VL 158 IS 5 BP A471 EP A480 DI 10.1149/1.3559551 PG 10 WC Electrochemistry; Materials Science, Coatings & Films SC Electrochemistry; Materials Science GA 741ML UT WOS:000288867700006 ER PT J AU Narayanan, SR Haines, B Soler, J Valdez, TI AF Narayanan, S. R. Haines, B. Soler, J. Valdez, T. I. TI Electrochemical Conversion of Carbon Dioxide to Formate in Alkaline Polymer Electrolyte Membrane Cells SO JOURNAL OF THE ELECTROCHEMICAL SOCIETY LA English DT Article ID CONTINUOUS REACTOR; FORMIC-ACID; REDUCTION; ELECTROREDUCTION; PRESSURE; COPPER AB This paper is about the continuous electrochemical conversion of carbon dioxide to formate in a polymer electrolyte membrane cell using an alkaline ion-exchange membrane sandwiched between two catalyzed electrodes. This type of cell configuration allows carbon dioxide conversion to occur at high efficiencies and is particularly attractive for large-scale implementation. Formate was produced at high efficiency, and hydrogen evolution was suppressed with lead and indium as catalysts. The production of formate was monitored by UV-visible spectroscopy. During short experimental runs, the faradaic efficiency of formate production was as high as 80%. The faradaic efficiency was strongly dependent on the concentrations of carbon dioxide, bicarbonate, and carbonate at the surface of the electrodes. Low concentrations of carbon dioxide in the reactant feed led to the mass transport limitations and hence low faradaic efficiencies. The results show that mass transport limitations can be mitigated and high efficiencies can be realized by conducting the electrolysis in a pulsed mode. An alkaline membrane-based flow cell that ensures abundant availability of carbon dioxide to the electrodes can be a cost-effective and efficient approach for the continuous production of fuels from sunlight, storing of renewable energy, and lowering carbon dioxide levels in the atmosphere. (C) 2010 The Electrochemical Society. [DOI: 10.1149/1.3526312] All rights reserved. C1 [Narayanan, S. R.; Haines, B.; Soler, J.; Valdez, T. I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Narayanan, SR (reprint author), Univ So Calif, Loker Hydrocarbon Res Inst, 837 Bloom Walk, Los Angeles, CA 90089 USA. EM sri.narayan@usc.edu FU National Aeronautics and Space Administration FX The work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The authors acknowledge Dr. Julian Blosiu and Dr. S. Surampudi for their guidance and support. NR 25 TC 48 Z9 51 U1 4 U2 47 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 0013-4651 J9 J ELECTROCHEM SOC JI J. Electrochem. Soc. PY 2011 VL 158 IS 2 BP A167 EP A173 DI 10.1149/1.3526312 PG 7 WC Electrochemistry; Materials Science, Coatings & Films SC Electrochemistry; Materials Science GA 700SW UT WOS:000285765600015 ER PT J AU Smart, MC Ratnakumar, BV AF Smart, M. C. Ratnakumar, B. V. TI Effects of Electrolyte Composition on Lithium Plating in Lithium-Ion Cells SO JOURNAL OF THE ELECTROCHEMICAL SOCIETY LA English DT Article ID LOW-TEMPERATURE PERFORMANCE; LI-ION; BATTERIES; INTERCALATION; CARBON; GRAPHITE AB Metallic lithium is typically absent in a lithium-ion (Li-ion) cell under normal conditions of operation. Under strenuous charge conditions of high charge rates and/or low temperatures, however, lithium metal will deposit on the carbon anode in preference to lithium intercalation, especially after considerable cycling and storage, which contribute to the degradation of anode capacity. Such plated lithium will react more readily in the Li-ion battery electrolytes and pose problems related to performance, reliability, and safety of the cell. Factors that affect the anode performance, specifically its polarization and lithium intercalation kinetics, play a crucial role in determining the propensity for lithium deposition. Such factors include the nature of solid electrolyte interphase (SEI), which is in turn governed by the electrolyte constituents, anode/cathode capacity ratios, and the operating conditions. In this paper, the Li intercalation kinetics and their impact on Li plating were studied with two sets of electrolytes containing different proportions of EC and with SEI-stabilizing additives. Electrolytes with low EC-formulations and those without SEI-stabilizing additives are relatively immune to lithium plating. (C) 2011 The Electrochemical Society. [DOI: 10.1149/1.3544439] C1 [Smart, M. C.; Ratnakumar, B. V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Smart, MC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ratnakumar.v.bugga@jpl.nasa.gov FU NASA's Chief Engineer's Office, under National Aeronautics and Space Administration (NASA) FX The work described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, for the Advanced Battery program sponsored by the NASA's Chief Engineer's Office, under contract with the National Aeronautics and Space Administration (NASA). NR 23 TC 44 Z9 45 U1 11 U2 94 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 0013-4651 J9 J ELECTROCHEM SOC JI J. Electrochem. Soc. PY 2011 VL 158 IS 4 BP A379 EP A389 DI 10.1149/1.3544439 PG 11 WC Electrochemistry; Materials Science, Coatings & Films SC Electrochemistry; Materials Science GA 729SX UT WOS:000287972300004 ER PT J AU West, WC Soler, J Smart, MC Ratnakumar, BV Firdosy, S Ravi, V Anderson, MS Hrbacek, J Lee, ES Manthiram, A AF West, W. C. Soler, J. Smart, M. C. Ratnakumar, B. V. Firdosy, S. Ravi, V. Anderson, M. S. Hrbacek, J. Lee, E. S. Manthiram, A. TI Electrochemical Behavior of Layered Solid Solution Li2MnO3-LiMO2 (M = Ni, Mn, Co) Li-Ion Cathodes with and without Alumina Coatings SO JOURNAL OF THE ELECTROCHEMICAL SOCIETY LA English DT Article ID SURFACE MODIFICATION; HIGH-CAPACITY; SECONDARY BATTERIES; ELECTRODES; SPINEL; PERFORMANCE; FTIR AB Thin films of oxides, phosphates, fluorides and other analogous materials on lithium-ion cathode particles are well known to improve cathode performance in terms of cycle life and rate performance. Explanations for this phenomenon abound, but the underlying mechanisms that dictate the nature of these effects are still in question, which motivates the work herein. We have carried out systematic PITT, EIS, Tafel, and cycling experiments as a function of temperature for Al2O3-coated and uncoated layered solid solution Li2MnO3-LiMO2 (M Mn, Co, Ni) cathode materials and shown that we can reproduce the well-documented improvement in performance with surface coatings. In particular the effects are most pronounced at reduced temperatures and after temperature cycling (23 to 0 degrees C to 30 to 0 degrees C). Interestingly, we find the activation energies for the diffusion coefficients estimated from PITT data are nearly identical to the activation energy for exchange current measured from Tafel polarization data. This finding may provide some insight into the relative control of the mass transfer and the charge transfer processes on the overall cathode reaction. Alternately, it may be the due to inadequate correction for the mass transfer effects in the Tafel and PITT analyses. (C) 2011 The Electrochemical Society. [DOI: 10.1149/1.3597319] All rights reserved. C1 [West, W. C.; Soler, J.; Smart, M. C.; Ratnakumar, B. V.; Firdosy, S.; Ravi, V.; Anderson, M. S.; Manthiram, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ravi, V.] Calif State Polytech Univ Pomona, Dept Chem & Mat Engn, Pomona, CA 91768 USA. [Hrbacek, J.; Lee, E. S.; Manthiram, A.] Univ Texas Austin, Electchem Energy Lab, Austin, TX 78712 USA. [Hrbacek, J.; Lee, E. S.; Manthiram, A.] Univ Texas Austin, Mat Sci & Engn Program, Austin, TX 78712 USA. RP West, WC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM william.c.west@jpl.nasa.gov FU National Aeronautics and Space Administration FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors thank J. Kulleck for carrying out the SEM, EDS, and XRD measurements. The authors acknowledge the funding support of NASA's Exploration Technology Development Program. In addition, the authors wish to acknowledge the useful discussions with Prof. S. R. Narayanan of the University of Southern California. NR 26 TC 59 Z9 64 U1 2 U2 106 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 0013-4651 J9 J ELECTROCHEM SOC JI J. Electrochem. Soc. PY 2011 VL 158 IS 8 BP A883 EP A889 DI 10.1149/1.3597319 PG 7 WC Electrochemistry; Materials Science, Coatings & Films SC Electrochemistry; Materials Science GA 784JV UT WOS:000292154300005 ER PT J AU Narayanan, SR Kindler, A Kisor, A Valdez, T Roy, RJ Eldridge, C Murach, B Hoberecht, M Graf, J AF Narayanan, S. R. Kindler, Andrew Kisor, Adam Valdez, Thomas Roy, Robert J. Eldridge, Christopher Murach, Bryan Hoberecht, Mark Graf, John TI Dual-Feed Balanced High-Pressure Electrolysis of Water in a Lightweight Polymer Electrolyte Membrane Stack SO JOURNAL OF THE ELECTROCHEMICAL SOCIETY LA English DT Article ID OXYGEN-EVOLUTION REACTION; DEPENDENCE AB Efficient water electrolyzers that generate high-pressure hydrogen and oxygen are useful for aerospace and civilian applications. A lightweight polymer-electrolyte-membrane electrolyzer capable of producing oxygen and hydrogen at a balanced pressure of 13.8 MPa has been designed and fabricated by Hamilton Sundstrand Space Systems International (HSSSI). This electrolyzer uses a unique metal-laminate cell design that reduces the weight of traditional high-pressure water electrolysis stacks by eliminating the need to place the stack within a pressure vessel. The electrolyzer operates on water fed to the anode and cathode (dual-feed mode). This design simplifies the balance of plant for a regenerative fuel cell system and enhances system safety. The electrolyzer was tested at balanced pressure in the range of 1.72-13.8 MPa using a test system designed and constructed at the Jet Propulsion Laboratory. Current efficiency of 96 to 97% was achieved at a balanced product pressure of 13.8 MPa. The polarization characteristics were governed by the kinetics of oxygen evolution and the ionic resistance of the membrane electrolyte. The electro-osmotic water drag coefficient was determined to be in the range of 2.3-2.4 and this value did not vary with the operating pressure up to 13.8 MPa. The dual-feed electrolyzer is a promising design for achieving high energy efficiencies at high product pressure. (C) 2011 The Electrochemical Society. [DOI: 10.1149/2.038111jes] All rights reserved. C1 [Narayanan, S. R.; Kindler, Andrew; Kisor, Adam; Valdez, Thomas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Roy, Robert J.; Eldridge, Christopher; Murach, Bryan] HSSSI, Windsor Locks, CT 06096 USA. [Hoberecht, Mark] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Graf, John] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Narayanan, SR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sri.narayan@usc.edu FU National Aeronautics and Space Administration; Loker Hydrocarbon Research Institute, University of Southern California FX The work presented here was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract from the National Aeronautics and Space Administration. The Loker Hydrocarbon Research Institute, University of Southern California, supported the costs of preparation of this publication. NR 25 TC 3 Z9 3 U1 2 U2 10 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 0013-4651 J9 J ELECTROCHEM SOC JI J. Electrochem. Soc. PY 2011 VL 158 IS 11 BP B1348 EP B1357 DI 10.1149/2.038111jes PG 10 WC Electrochemistry; Materials Science, Coatings & Films SC Electrochemistry; Materials Science GA 829ZL UT WOS:000295626000018 ER PT J AU Li, L Stone, LS Chen, J AF Li, Li Stone, Leland S. Chen, Jing TI Influence of optic-flow information beyond the velocity field on the active control of heading SO JOURNAL OF VISION LA English DT Article DE heading; optic flow; perception and action; motion perception; visuomotor control; manual control ID VISUAL-CORTEX; EYE-MOVEMENTS; SELF-MOTION; PATH INFORMATION; REACTION-TIME; PERCEPTION; DISCRIMINATION; ORIENTATION; SUFFICIENCY; JUDGMENTS AB We examined both the sufficiency of the optic-flow velocity field and the influence of optic-flow information beyond the velocity field on the active control of heading. The display simulated a vehicle traveling on a circular path through a random-dot 3D cloud under a static or a dynamic scene in which dots were periodically redrawn to remove information beyond the velocity field. Participants used a joystick, under either velocity and acceleration control dynamics, to steer and align the vehicle orientation with their perceived heading while experiencing random perturbations to the vehicle orientation. Frequency-response (Bode) plots show reasonably good performance under both display conditions with a decrease in gain and an increase in phase lag for the dynamic scene for both control dynamics. The performance data were fit by a Crossover Model to identify reaction time and lead time constant to determine how much participants anticipated future heading to generate lead control. Reaction time was longer and lead time constant was smaller for the dynamic than the static scene for both control dynamics. We conclude that the velocity field alone is sufficient to support closed-loop heading control, but optic-flow information beyond the velocity field improves visuomotor performance in self-motion control. C1 [Li, Li; Chen, Jing] Univ Hong Kong, Dept Psychol, Pokfulam, Hong Kong, Peoples R China. [Stone, Leland S.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA. RP Li, L (reprint author), Univ Hong Kong, Dept Psychol, Pokfulam, Hong Kong, Peoples R China. EM lili@hku.hk FU Research Grants Council of Hong Kong [HKU 7478/08H] FX This study was supported by a grant from the Research Grants Council of Hong Kong (HKU 7478/08H) to L. Li. We thank Diederick Niehorster and Joseph Cheng for their assistance in programming and data analysis and two anonymous reviewers for their helpful comments on a previous draft of the article. NR 53 TC 3 Z9 3 U1 0 U2 2 PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC PI ROCKVILLE PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA SN 1534-7362 J9 J VISION JI J. Vision PY 2011 VL 11 IS 4 AR 9 DI 10.1167/11.4.9 PG 16 WC Ophthalmology SC Ophthalmology GA 757MQ UT WOS:000290091000009 PM 21493706 ER PT J AU Watson, AB Ahumada, AJ AF Watson, Andrew B. Ahumada, Albert J. TI Blur clarified: A review and synthesis of blur discrimination SO JOURNAL OF VISION LA English DT Review DE computational modeling; contrast sensitivity; detection/discrimination; masking; spatial vision ID WAVE-FRONT ABERRATIONS; IMAGE QUALITY; VISUAL SENSITIVITY; SPATIAL FILTERS; HUMAN-VISION; CONTRAST; MOTION; MODEL; FOVEAL; ACCOMMODATION AB Blur is an important attribute of human spatial vision, and sensitivity to blur has been the subject of considerable experimental research and theoretical modeling. Often, these models have invoked specialized concepts or mechanisms, such as intrinsic blur, multiple spatial frequency channels, or blur estimation units. In this paper, we review the several experimental studies of blur discrimination and find that they are in broad empirical agreement. However, contrary to previous modeling efforts, we find that specialized mechanisms are not required and that the essential features of blur discrimination are fully accounted for by a visible contrast energy (ViCE) model, in which two spatial patterns are distinguished when the integrated difference between their masked local visible contrast energy responses reaches a threshold value. In the ViCE model, intrinsic blur is represented by the high-frequency limb of the contrast sensitivity function, but the low-frequency limb also contributes to the predictions for large reference blurs, and the model includes masking, which improves predictions for high-contrast stimuli. C1 [Watson, Andrew B.; Ahumada, Albert J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Watson, AB (reprint author), Mail Stop 262-2, Moffett Field, CA 94035 USA. EM andrew.b.watson@nasa.gov FU NASA Space Human Factors Engineering [WBS 466199] FX We thank Roger Watt and an anonymous reviewer for helpful comments. This work was supported by NASA Space Human Factors Engineering (WBS 466199). NR 51 TC 8 Z9 8 U1 1 U2 9 PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC PI ROCKVILLE PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA SN 1534-7362 J9 J VISION JI J. Vision PY 2011 VL 11 IS 5 AR 10 DI 10.1167/11.5.10 PG 23 WC Ophthalmology SC Ophthalmology GA 872OG UT WOS:000298818500008 ER PT J AU Watson, AB AF Watson, Andrew B. TI It seemed like a good idea at the time: A brief history of Journal of Vision SO JOURNAL OF VISION LA English DT Article ID EYE C1 [Watson, Andrew B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Watson, AB (reprint author), NASA, Ames Res Ctr, MS 262-2, Moffett Field, CA 94035 USA. EM andrew.b.watson@nasa.gov FU NASA [WBS 466199] FX This work was supported by NASA Space Human Factors Engineering WBS 466199. I thank Denis Pelli, Jeremy Bluhm, Ted Adelson, Steve Shevell, Suzanne McKee, Joanne Angle, Alice O'Donnell, Cesar Ramirez, and Ellen Salud for helpful comments. NR 11 TC 11 Z9 11 U1 0 U2 1 PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC PI ROCKVILLE PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA SN 1534-7362 J9 J VISION JI J. Vision PY 2011 VL 11 IS 5 AR ii DI 10.1167/11.5.ii PG 21 WC Ophthalmology SC Ophthalmology GA 762YF UT WOS:000290517400002 PM 21551104 ER PT J AU Kapoor, B Pandya, P Sherif, JS AF Kapoor, Bhushan Pandya, Pramod Sherif, Joseph S. TI Cryptography A security pillar of privacy, integrity and authenticity of data communication SO KYBERNETES LA English DT Article DE Cybernetics; Ciphers; Advanced encryption standard (AES); Rijndael; Public-key cryptography; RSA digital signature scheme; Codes AB Purpose - This paper seeks to advance research and strategies that lead to a heightened awareness of the need to protect data from disclosure, to guarantee the authenticity of data and messages, and to protect systems from network-based attacks. Design/methodology/approach - The paper introduces the necessary mathematics of cryptography: integer and modular arithmetic, linear congruence, Euclidean and extended Euclidean algorithm, Fermat's theorem, and Elliptic curve. Findings - The results indicate that encryption has expanded beyond confidentiality concerns to include techniques for message integrity checking, sender/receiver identity authentication, digital signatures, interactive proofs, and secure computation. Practical implications - The results of this research show that all forms of e-commerce activities such as online credit card processing, purchasing stocks, and banking data processing, if compromised, would lead to businesses losing billions of dollars in lost revenues as well as losing confidence in e-commerce. In the last few years, it had been reported that organizations that store and maintain customers' private and confidential records were compromised on many occasions by hackers breaking into the data networks and stealing the records from the storage media. Originality/value - This paper tackles one of the most critical problems of securing data networks. Security problems arise among other things to resource and workload sharing, complexity of interconnected networks; authentication of users; fast expandability of networks; threats to networks such as wiretapping and violations of the seven pillars of security: authentication, authorization, privacy, integrity, non-repudiation, availability, and audit. C1 [Sherif, Joseph S.] Calif State Univ Fullerton, Fullerton, CA 92634 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Sherif, JS (reprint author), Calif State Univ Fullerton, Fullerton, CA 92634 USA. EM jsherif@fullerton.edu NR 11 TC 0 Z9 0 U1 0 U2 8 PU EMERALD GROUP PUBLISHING LIMITED PI BINGLEY PA HOWARD HOUSE, WAGON LANE, BINGLEY BD16 1WA, W YORKSHIRE, ENGLAND SN 0368-492X J9 KYBERNETES JI Kybernetes PY 2011 VL 40 IS 9-10 BP 1422 EP 1439 DI 10.1108/03684921111169468 PG 18 WC Computer Science, Cybernetics SC Computer Science GA 862XP UT WOS:000298127700013 ER PT B AU Ramapriyan, HK Pfister, R Weinstein, B AF Ramapriyan, H. K. Pfister, Robin Weinstein, Beth BE Ramachandran, B Justice, CO Abrams, MJ TI An Overview of the EOS Data Distribution Systems SO LAND REMOTE SENSING AND GLOBAL ENVIRONMENTAL CHANGE: NASA'S EARTH OBSERVING SYSTEM AND THE SCIENCE OF ASTER AND MODIS SE Remote Sensing and Digital Image Processing LA English DT Article; Book Chapter C1 [Ramapriyan, H. K.; Pfister, Robin; Weinstein, Beth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ramapriyan, HK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM hampapuram.k.ramapriyan@nasa.gov NR 7 TC 2 Z9 5 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 978-1-4419-6748-0 J9 REMOTE SENS DIGIT IM PY 2011 VL 11 BP 183 EP 202 DI 10.1007/978-1-4419-6749-7_9 D2 10.1007/978-1-4419-6749-7 PG 20 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Geochemistry & Geophysics; Geology; Remote Sensing; Imaging Science & Photographic Technology GA BSG06 UT WOS:000284351600009 ER PT S AU Campbell, J Prasad, NS Flood, M Harrison, W AF Campbell, Joel Prasad, Narasimha S. Flood, Michael Harrison, Wallace BE Turner, MD Kamerman, GW TI Pseudorandom noise code-based technique for cloud and aerosol discrimination applications SO LASER RADAR TECHNOLOGY AND APPLICATIONS XVI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Laser Radar Technology and Applications XVI CY APR 27-29, 2011 CL Orlando, FL SP SPIE DE ASCENDS; CO2 sensing; O2 sensing; PN codes; CW lidar AB NASA Langley Research Center is working on a continuous wave (CW) laser based remote sensing scheme for the detection of CO2 and O-2 from space based platforms suitable for ACTIVE SENSING OF CO2 EMISSIONS OVER NIGHTS, DAYS, AND SEASONS (ASCENDS) mission. ASCENDS is a future space-based mission to determine the global distribution of sources and sinks of atmospheric carbon dioxide (CO2). A unique, multi-frequency, intensity modulated CW (IMCW) laser absorption spectrometer (LAS) operating at 1.57 micron for CO2 sensing has been developed. Effective aerosol and cloud discrimination techniques are being investigated in order to determine concentration values with accuracies less than 0.3%. In this paper, we discuss the demonstration of a PN code based technique for cloud and aerosol discrimination applications. The possibility of using maximum length (ML)-sequences for range and absorption measurements is investigated. A simple model for accomplishing this objective is formulated, Proof-of-concept experiments carried out using SONAR based LIDAR simulator that was built using simple audio hardware provided promising results for extension into optical wavelengths. C1 [Campbell, Joel; Prasad, Narasimha S.; Flood, Michael; Harrison, Wallace] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Campbell, J (reprint author), NASA, Langley Res Ctr, 5 N Dryden St, Hampton, VA 23681 USA. NR 6 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-611-0 J9 PROC SPIE PY 2011 VL 8037 AR 80370L DI 10.1117/12.888132 PG 11 WC Optics; Physics, Applied SC Optics; Physics GA BWF18 UT WOS:000293783800018 ER PT S AU Yu, AW Krainak, MA Stephen, MA Abshire, JB Harding, DJ Riris, H Li, SX Chen, JR Allan, GR Numata, K Wu, ST Camp, JB AF Yu, Anthony W. Krainak, Michael A. Stephen, Mark A. Abshire, James B. Harding, David J. Riris, Haris Li, Steven X. Chen, Jeffrey R. Allan, Graham R. Numata, Kenji Wu, Stewart T. Camp, Jordan B. BE Singh, UN Pappalardo, G TI Spaceflight laser development for future remote sensing applications SO LIDAR TECHNOLOGIES, TECHNIQUES, AND MEASUREMENTS FOR ATMOSPHERIC REMOTE SENSING VII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Lidar Technologies, Techniques, and Measurements for Atmospheric Remote Sensing VII CY SEP 19-20, 2011 CL Prague, CZECH REPUBLIC SP SPIE DE Space Laser; Lidar; Remote Sensing; Space Instrument ID REFLECTED SUNLIGHT; ATMOSPHERIC CO2; CARBON-DIOXIDE; DIFFERENTIAL ABSORPTION; MESSENGER MISSION; ALTIMETER; COLUMN; TRANSMITTER; SPACE; MERCURY AB At NASA's Goddard Space Flight Center we are developing next generation laser transmitters for future spaceflight, remote instruments including a micropulse altimeter for ice-sheet and sea ice monitoring, laser spectroscopic measurements of atmospheric CO2 and an imaging lidar for high resolution mapping of the Earth's surface. These laser transmitters also have applicability to potential missions to other solar-system bodies for trace gas measurements and surface mapping. In this paper we review NASA spaceflight laser transmitters used to acquire measurements in orbit around Mars, Mercury, Earth and the Moon. We then present an overview of our current spaceflight laser programs and describe their intended uses for remote sensing science and exploration applications. C1 [Yu, Anthony W.; Krainak, Michael A.; Stephen, Mark A.; Abshire, James B.; Harding, David J.; Riris, Haris; Li, Steven X.; Chen, Jeffrey R.; Allan, Graham R.; Numata, Kenji; Wu, Stewart T.; Camp, Jordan B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yu, AW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM anthony.w.yu@nasa.gov RI Riris, Haris/D-1004-2013; Abshire, James/I-2800-2013; Allan, Graham/D-3905-2013; Harding, David/F-5913-2012 NR 41 TC 1 Z9 1 U1 0 U2 6 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-809-1 J9 PROC SPIE PY 2011 VL 8182 AR 818204 DI 10.1117/12.898547 PG 10 WC Remote Sensing; Optics; Physics, Applied SC Remote Sensing; Optics; Physics GA BYC92 UT WOS:000298044100002 ER PT S AU Yu, AW Krainak, MA Harding, DJ Abshire, JB Sun, XL Cavanaugh, J Valett, S Ramos-Izquierdo, L Winkert, T Kirchner, C Plants, M Filemyr, T Kamamia, B Hasselbrack, W Dogoda, P AF Yu, Anthony W. Krainak, Michael A. Harding, David J. Abshire, James B. Sun, Xiaoli Cavanaugh, John Valett, Susan Ramos-Izquierdo, Luis Winkert, Tom Kirchner, Cynthia Plants, Michael Filemyr, Timothy Kamamia, Brian Hasselbrack, William Dogoda, Pete BE Singh, UN Pappalardo, G TI Development Effort of the Airborne Lidar Simulator for the Lidar Surface Topography (LIST) Mission SO LIDAR TECHNOLOGIES, TECHNIQUES, AND MEASUREMENTS FOR ATMOSPHERIC REMOTE SENSING VII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Lidar Technologies, Techniques, and Measurements for Atmospheric Remote Sensing VII CY SEP 19-20, 2011 CL Prague, CZECH REPUBLIC SP SPIE DE Altimetry; lidar; space laser; photo-counting lidar; micropulse lidar AB In this paper we will discuss our development effort of an airborne instrument as a pathfinder for the LIdar Surface Technology (LIST) mission. This paper will discuss the system approach, enabling technologies, instrument concept, final assembly and the preparation for flight with this new multi-beam non-scanning, swath mapping laser altimeter system. C1 [Yu, Anthony W.; Krainak, Michael A.; Harding, David J.; Abshire, James B.; Sun, Xiaoli; Cavanaugh, John; Valett, Susan; Ramos-Izquierdo, Luis; Winkert, Tom; Kirchner, Cynthia; Plants, Michael; Filemyr, Timothy; Kamamia, Brian; Hasselbrack, William; Dogoda, Pete] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yu, AW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Sun, Xiaoli/B-5120-2013; Abshire, James/I-2800-2013; Harding, David/F-5913-2012 NR 9 TC 1 Z9 1 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-809-1 J9 PROC SPIE PY 2011 VL 8182 AR 818207 DI 10.1117/12.898545 PG 6 WC Remote Sensing; Optics; Physics, Applied SC Remote Sensing; Optics; Physics GA BYC92 UT WOS:000298044100004 ER PT S AU Yu, AW Shaw, GB Novo-Gradac, AM Li, SX Cavanaugh, J AF Yu, Anthony W. Shaw, George B. Novo-Gradac, Anne Marie Li, Steven X. Cavanaugh, John BE Singh, UN Pappalardo, G TI In Space Performance of the Lunar Orbiter Laser Altimeter (LOLA) Laser Transmitter SO LIDAR TECHNOLOGIES, TECHNIQUES, AND MEASUREMENTS FOR ATMOSPHERIC REMOTE SENSING VII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Lidar Technologies, Techniques, and Measurements for Atmospheric Remote Sensing VII CY SEP 19-20, 2011 CL Prague, CZECH REPUBLIC SP SPIE DE Space laser; altimetry; topographic mapping ID MISSION AB In this paper we present the final configuration of the space flight laser transmitter as delivered to the Lunar Orbiter Laser Altimeter (LOLA) instrument along with some in-space operation performance data. The LOLA instrument is designed to map the lunar surface and provide unprecedented data products in anticipation of future manned flight missions. The laser transmitter has been operating on orbit at the Moon continuously since July 2009 and accumulated over 1.8 billion laser shots in space. The LOLA laser transmitter design has heritage dated back to the MOLA laser transmitter launched more than 10 years ago and incorporates lessons learned from previous laser altimeter missions at NASA Goddard Space Flight Center. C1 [Yu, Anthony W.; Shaw, George B.; Li, Steven X.; Cavanaugh, John] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yu, AW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 5 TC 1 Z9 1 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-809-1 J9 PROC SPIE PY 2011 VL 8182 AR 818208 DI 10.1117/12.898546 PG 4 WC Remote Sensing; Optics; Physics, Applied SC Remote Sensing; Optics; Physics GA BYC92 UT WOS:000298044100005 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI LIMITING FUTURE COLLISION RISK TO SPACECRAFT AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS Summary SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Editorial Material; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 1 EP 5 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500002 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI LIMITING FUTURE COLLISION RISK TO SPACECRAFT AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS Introduction and Historical Background SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Editorial Material; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 33 TC 0 Z9 0 U1 1 U2 1 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 7 EP 16 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500003 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI LIMITING FUTURE COLLISION RISK TO SPACECRAFT AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS Preface SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Editorial Material; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP VII EP VIII PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500001 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Orbital Debris Environment: Detection and Monitoring SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 17 EP 22 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500004 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Orbital Debris Modeling and Simulation SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 23 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 23 EP 28 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500005 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI The Meteoroid Environment and Its Effects on Spacecraft SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter ID VELOCITY DISTRIBUTION; DEBRIS; MASS C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 32 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 29 EP 39 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500006 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Risk Assessment and Uncertainty SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 25 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 40 EP 46 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500007 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Spacecraft Protection in the MMOD Environment SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter ID BALLISTIC LIMIT CURVES; NONSPHERICAL PROJECTILES; SYSTEMS; SHAPE C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 23 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 47 EP 56 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500008 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Mitigation of Orbital Debris SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter ID ENVIRONMENT; MANAGEMENT C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 57 EP 59 PG 3 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500009 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Hazards Posed by Reentry of Orbital Debris SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 60 EP 64 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500010 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Conjunction Assessment Risk Analysis and Launch Collision Avoidance SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 65 EP 71 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500011 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Spacecraft Anomalies SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter ID DEBRIS C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 72 EP 76 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500012 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Issues External to NASA SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 24 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 77 EP 85 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500013 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Management and Organizational Issues SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 86 EP 90 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500014 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Preparing for the Future SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 91 EP 93 PG 3 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500015 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Compiled List of Findings and Recommendations SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 94 EP 100 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500016 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Statement of Task SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 106 EP 106 PG 1 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500017 ER PT J AU Kessler, DJ Gleghorn, GJ AF Kessler, Donald J. Gleghorn, George J. GP Natl Res Council TI Committee and Staff Biographical Information SO LIMITING FUTURE COLLISION RISK TO SPACECRAFT: AN ASSESSMENT OF NASA'S METEOROID AND ORBITAL DEBRIS PROGRAMS LA English DT Article; Book Chapter C1 [Kessler, Donald J.; Gleghorn, George J.] NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. RP Kessler, DJ (reprint author), NASA, Orbital Debris Programs, Comm Assessment, Washington, DC 20005 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATL ACADEMIES PRESS PI WASHINGTON PA 2101 CONSTITUTION AVE, WASHINGTON, DC 20418 USA BN 978-0-309-21974-7 PY 2011 BP 107 EP 112 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BC4IQ UT WOS:000352549500018 ER PT J AU Rodgveller, CJ Sigler, MF Hanselman, DH Ito, DH AF Rodgveller, Cara J. Sigler, Michael F. Hanselman, Dana H. Ito, Daniel H. TI Sampling Efficiency of Longlines for Shortraker and Rougheye Rockfish Using Observations from a Manned Submersible SO MARINE AND COASTAL FISHERIES LA English DT Article ID SABLEFISH ANOPLOPOMA-FIMBRIA; BEHAVIORAL-RESPONSES; TEMPERATURE; STOCK; TRAWL; BAIT AB Populations of demersal rockfish of the genus Sebastes are challenging to assess because they inhabit rocky areas that are difficult to sample with trawl gear. In contrast, longline gear can sample rocky areas, but several factors besides fish density can affect the relationship between catch rates and density. In this study, longline catch rates of shortraker rockfish Sebastes borealis and rougheye rockfish S. aleutianus were compared with observations of density from a manned submersible to evaluate the species' catchability on longline gear. On separate occasions, rockfish behavior in the presence of longline gear was observed from the submersible. Densities averaged 3.0 shortraker and rougheye rockfish (combined) per 330 m(2) of bottom (the effectively sampled area of a 100-m transect). Longline catch rates averaged 2.7 shortraker and rougheye rockfish per skate of 45 hooks. Longline catch rates were not statistically affected by submersible observations. There was a positive trend between density and longline catch rates, but the relationship was not significant. As observed from the submersible, the proportion of fish free-swimming near the longline increased through the duration of the set, indicating that rockfish were attracted to the line faster than they were caught. The catching process for shortraker and rougheye rockfish lasts longer than for more mobile species such as sablefish Anoplopoma fimbria. C1 [Rodgveller, Cara J.; Sigler, Michael F.; Hanselman, Dana H.] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA. [Ito, Daniel H.] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Resource Ecol & Fisheries Management Div, Seattle, WA 98115 USA. RP Rodgveller, CJ (reprint author), Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA. EM cara.rodgveller@noaa.gov NR 32 TC 0 Z9 0 U1 3 U2 6 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1942-5120 J9 MAR COAST FISH JI Mar. Coast. Fish. PY 2011 VL 3 IS 1 BP 1 EP 9 DI 10.1080/19425120.2011.558447 PG 9 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 873IJ UT WOS:000298874700001 ER PT J AU Weitkamp, LA Orsi, JA Myers, KW Francis, RC AF Weitkamp, L. A. Orsi, J. A. Myers, K. W. Francis, R. C. TI Contrasting Early Marine Ecology of Chinook Salmon and Coho Salmon in Southeast Alaska: Insight into Factors Affecting Marine Survival SO MARINE AND COASTAL FISHERIES LA English DT Article ID JUVENILE PACIFIC SALMON; SIZE-SELECTIVE MORTALITY; NORTHERN CALIFORNIA CURRENT; PRINCE-WILLIAM-SOUND; ONCORHYNCHUS-KISUTCH; PINK SALMON; INTERANNUAL VARIABILITY; ENVIRONMENTAL PROCESSES; VERTICAL-DISTRIBUTION; BRITISH-COLUMBIA AB To identify processes potentially contributing to the differential marine survival rates of Chinook salmon Oncorhynchus tshawytscha and coho salmon O. kisutch originating from Southeast Alaska, we compared the early marine ecology of the two species during the critical first summer in marine waters. We predicted that the higher survival rates for coho salmon relative to Chinook salmon were related to the larger size, faster growth, or different habitat or species associations of coho salmon. Our size and growth expectations were largely substantiated: juvenile coho salmon were larger than juvenile Chinook salmon and had faster length-based growth, although weight-based growth rates were similar. The most obvious difference was in their distributions. Juvenile coho salmon overlapped spatially and temporally with abundant juvenile pink salmon O. gorbuscha and chum salmon O. keta, whereas juvenile Chinook salmon were geographically separated from other salmonids. This suggests that coho salmon benefited from a predation buffer that did not extend to Chinook salmon. Our results indicate that factors influencing marine survival of juvenile Chinook salmon and coho salmon in Southeast Alaska are attributable to species-specific differences in their early marine distribution patterns and species interactions. C1 [Weitkamp, L. A.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Newport Field Stn, Newport, OR 97365 USA. [Weitkamp, L. A.; Myers, K. W.; Francis, R. C.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. [Orsi, J. A.] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Ted Stevens Marine Res Inst, Juneau, AK 99801 USA. RP Weitkamp, LA (reprint author), Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Newport Field Stn, 2032 SE OSU Dr, Newport, OR 97365 USA. EM laurie.weitkamp@noaa.gov FU Northwest Fisheries Science Center (National Oceanic and Atmospheric Administration-Fisheries) FX We thank the Auke Bay Laboratories personnel who participated in the research surveys and conducted initial laboratory analyses. We are grateful to the command and crew of the R/V John N. Cobb (National Oceanic and Atmospheric Administration) for their cooperation and performance throughout the surveys. We also thank the core members of the SECM team-Molly Sturdevant, Emily Fergusson, and Alex Wertheimer-who helped perform the at-sea data collection. Funding for L. Weitkamp was provided by the Northwest Fisheries Science Center (National Oceanic and Atmospheric Administration-Fisheries). This manuscript was greatly improved by comments from J. Scheurer and J. Myers. Reference to trade names does not imply endorsement by the National Marine Fisheries Service. NR 89 TC 3 Z9 3 U1 1 U2 18 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 1942-5120 J9 MAR COAST FISH JI Mar. Coast. Fish. PY 2011 VL 3 IS 1 BP 233 EP 249 DI 10.1080/19425120.2011.588919 PG 17 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 873IJ UT WOS:000298874700016 ER PT J AU Hartman, KJ Phelan, BA Rosendale, JE AF Hartman, Kyle J. Phelan, Beth A. Rosendale, John E. TI Temperature Effects on Bioelectrical Impedance Analysis (BIA) Used to Estimate Dry Weight as a Condition Proxy in Coastal Bluefish SO MARINE AND COASTAL FISHERIES LA English DT Article ID PROXIMATE COMPOSITION; ENERGY DENSITY; BIOENERGETICS MODELS; BODY-COMPOSITION; FISH; GROWTH; WATER AB The highly migratory nature of bluefish Pomatomus saltatrix makes comprehensive study of their populations and their potential responses to factors such as competition, habitat degradation, and climate change difficult. Body composition is an important ecological reference point for fish; however, estimating body composition in fish has been limited by analytical and logistical costs. We applied bioelectrical impedance analysis (BIA) to estimate one body composition component (percent dry weight) as a proxy of condition in bluefish. We used a tetra polar Quantum II BIA analyzer and measured electrical properties in the muscles of bluefish at two locations per fish (dorsal and ventral). In total, 96 bluefish ranging from 193 to 875 mm total length were used in model development and testing. On 59 of these fish BIA measures were taken at both 15 degrees C and 27 degrees C. Temperature had a significant negative effect on resistance and reactance. A subsample of these fish was then analyzed for dry weight as a percentage of their whole body weight (PDW), which is a good indicator of condition because it is highly correlated with fat content in fish. The BIA models predicting PDW inclusive of all lengths of bluefish were highly predictive for 15 degrees C (stepwise regression) and 27 degrees C. Regression (R(pred)(2)) values that estimate future predictive power suggest that both models were robust. Strong relationships between PDW and other body composition components, coupled with the BIA models presented here, provide the tools needed to quantitatively assess bluefish body composition across spatial and temporal scales for which assessment was previously impossible. C1 [Hartman, Kyle J.] W Virginia Univ, Div Forestry & Nat Resources, Morgantown, WV 26506 USA. [Phelan, Beth A.; Rosendale, John E.] Natl Marine Fisheries Serv, NE Fisheries Sci Ctr, Sandy Hook Lab, Highlands, NJ 07732 USA. RP Hartman, KJ (reprint author), W Virginia Univ, Div Forestry & Nat Resources, 322 Percival Hall, Morgantown, WV 26506 USA. EM hartman@wvu.edu FU Bluefish-Striped Bass Dynamics Research Program FX We are grateful to J. Howell, G. Staines, and J. Nye for assistance in field collections and measures and to J. Rosendale for collection and husbandry of bluefish used at Sandy Hook. A. Hafs provided comments that improved this manuscript. Funding for this project was provided by the 2004 Bluefish-Striped Bass Dynamics Research Program to KJH. All procedures involving fish were conducted under guidelines approved by the West Virginia University Animal Care and Use Committee under protocol 05-0201. NR 25 TC 8 Z9 8 U1 0 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1942-5120 J9 MAR COAST FISH JI Mar. Coast. Fish. PY 2011 VL 3 IS 1 BP 307 EP 316 DI 10.1080/19425120.2011.603961 PG 10 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 873IJ UT WOS:000298874700022 ER PT J AU Sturdevant, M Nishimura, G Orsi, J AF Sturdevant, Molly Nishimura, Gary Orsi, Joe TI Sidewinder: Description of a New Block Winch for Deploying Instruments at Sea SO MARINE AND COASTAL FISHERIES LA English DT Article ID CAPTURE EFFICIENCY; TUCKER TRAWL; TECHNOLOGY; NETS AB We describe a new electric winch design and its functionality for conducting research operations off different-sized vessels. Currently, several small oceanographic winches are available for deploying research instruments and nets, but they are typically heavy, noisy, semipermanently mounted to the deck, hydraulically operated, and not readily transferable between vessels. The limitation of winch portability between vessels, in particular, has been exacerbated by the increasing use of a variety of chartered vessels to conduct state and federal agency and university research. To address these challenges, we developed a relatively lightweight (70 kg), portable block-design winch that is spooled with 400 m of plasma line, powered by two 12-V marine batteries, and operated by a remote control box on a pendant equipped with a joystick. The 2.2-kW drive produces 100 kg of line pull at speeds of 0 to 2.0 m/s. The pendant includes digital displays for line speed, scope, and angle as well as an emergency stop. Nicknamed the "Sidewinder," this winch is quiet, can be operated by one person, and is suspended outboard from a davit or crane boom, increasing available deck space and relocating all lines safely away from vessel personnel. On vessels 7 to 50 m in length the Sidewinder has been successfully tested for deploying small gear such as conductivity-temperature-depth profilers and large BONGO plankton nets that require specific deployment and retrieval speeds and line angles. To ensure safe operation, vessel support features such as the power system and davit working load capacity should be considered when the Sidewinder is custom-built. C1 [Sturdevant, Molly; Orsi, Joe] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA. [Nishimura, Gary] Markey Machinery Co Inc, Seattle, WA 98108 USA. RP Sturdevant, M (reprint author), Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA. EM molly.sturdevant@noaa.gov FU Auke Bay Laboratories management FX We thank B. A. Griffin, B. Dempke, P. Hammerschlag, S. Kreis, and J. Davis for contributing invaluable engineering support from the early stages through the duration of the project. Shop expertise provided by A. Wheatley overcame several unexpected challenges during final assembly and shop testing, and support for the electrical controls was provided by S. DeMers and S. Hatvany. We also thank E. A. Fergusson and S. A. Ballard for assistance with field testing, G. Garcia and the captain and crew of the FV Northwest Explorer for vessel assistance, and Auke Bay Laboratories management for supporting this project. Reference to trademarked names does not imply endorsement by the National Marine Fisheries Service. NR 17 TC 0 Z9 0 U1 1 U2 10 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1942-5120 J9 MAR COAST FISH JI Mar. Coast. Fish. PY 2011 VL 3 IS 1 BP 317 EP 323 DI 10.1080/19425120.2011.608582 PG 7 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 873IJ UT WOS:000298874700023 ER PT J AU Tribuzio, CA Kruse, GH AF Tribuzio, Cindy A. Kruse, Gordon H. TI Demographic and risk analyses of spiny dogfish (Squalus suckleyi) in the Gulf of Alaska using age-and stage-based population models SO MARINE AND FRESHWATER RESEARCH LA English DT Article DE elasmobranch; Leslie models; model comparison; shark ID SHARK POPULATIONS; NATURAL MORTALITY; LIFE-HISTORY; MANAGEMENT; ELASMOBRANCHS; CONSERVATION; FISHERIES; ACANTHIAS; PACIFIC AB Demographic models are useful tools for assessing data-limited species and may be an appropriate alternative to cohort analyses for sharks due to their long-lived, slow-growing nature. In this study, age-and stage-based demographic analyses were conducted to examine the intrinsic rebound potential (r) and potential risk of fishing for spiny dogfish (Squalus suckleyi) in the Gulf of Alaska. Monte Carlo simulations were conducted to incorporate input parameter uncertainty. For an unfished population, r was estimated to be 0.02-0.03 year(-1). Fishing mortalities (F) of F = 0.04 and 0.03 (age- and stage-based models respectively), resulted in r 0, indicating that populations fished at higher F are not sustainable. Harvest strategies targeting juveniles (age-based model) and subadults (stage-based model) caused the highest risk of the population falling below defined thresholds (B-MSY, B-40% and B-50%) after 20 years. The age-and stage-based models provided similar estimates of r and sustainable fishing mortality, suggesting that the stage-based model is an appropriate substitute for the age-based model in this case. S. suckleyi and the closely related S. acanthias are often harvested around the world and this modelling approach could be useful to the management of these species and other sharks where data is limited. C1 [Tribuzio, Cindy A.; Kruse, Gordon H.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Div Fisheries, Juneau, AK 99801 USA. RP Tribuzio, CA (reprint author), NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA. EM cindy.tribuzio@noaa.gov FU North Pacific Research Board (NPRB); Rasmuson Fisheries Research Center; Alaska Fisheries Science Center through the Cooperative Institute for Arctic Research FX This report is the result of research sponsored in part by the North Pacific Research Board (NPRB), the Rasmuson Fisheries Research Center and the Alaska Fisheries Science Center Population Dynamics Fellowship through the Cooperative Institute for Arctic Research. We thank V. Gallucci, J. Rice, A. Andrews and W. Strasberger for their involvement in this project, K. Goldman for advice and the Greg Hood of PopTools for software guidance. We thank J. Fujioka, J. Heifetz and the anonymous reviewers for comments on this manuscript. This is NPRB publication number 308. The findings and conclusions in this paper are those of the author(s) and do not necessarily represent the views of the National Marine Fisheries Service, NOAA. Likewise, the use of trade names does not imply endorsement by the National Marine Fisheries Service, NOAA. NR 37 TC 6 Z9 6 U1 2 U2 14 PU CSIRO PUBLISHING PI CLAYTON PA UNIPARK, BLDG 1, LEVEL 1, 195 WELLINGTON RD, LOCKED BAG 10, CLAYTON, VIC 3168, AUSTRALIA SN 1323-1650 EI 1448-6059 J9 MAR FRESHWATER RES JI Mar. Freshw. Res. PY 2011 VL 62 IS 12 BP 1395 EP 1406 DI 10.1071/MF11062 PG 12 WC Fisheries; Limnology; Marine & Freshwater Biology; Oceanography SC Fisheries; Marine & Freshwater Biology; Oceanography GA 854TO UT WOS:000297517600005 ER PT J AU deCarvalho, R Haines, BJ Desai, SD AF deCarvalho, Robert Haines, Bruce J. Desai, Shailen D. TI Sensitivity Analysis Techniques Applied to Jason-1 and Jason-2/OSTM Cross Calibration SO MARINE GEODESY LA English DT Article DE Jason-2; OSTM; Jason-1; altimetry; calibration; validation; sensitivity analysis; error budget; ionospheric correction; scale error; regression dilution ID PRECISION ORBIT DETERMINATION; CLIMATE DATA RECORD; ALTIMETER MISSIONS; TOPEX/POSEIDON; TOPEX; BIAS; HEIGHT; SERIES AB A sensitivity analysis is performed on the level-2 algorithms for the Jason-2/Ocean Surface Topography Mission (OSTM). This analysis quantifies how inaccuracies in the fundamental measurements impact the overall sea-surface-height measurements. The analysis is applied to examine the various biases between OSTM and Jason-1 during their formation-flying phase. We further investigate data from the formation-flying phase by analyzing a statistical artifact that manifests itself as an apparent scale error in differences of the 1-Hz ionospheric corrections from the two missions. C1 [deCarvalho, Robert; Haines, Bruce J.; Desai, Shailen D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP deCarvalho, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 238-600, Pasadena, CA 91109 USA. EM Robert.decarvalho@jpl.nasa.gov FU National Aeronautics and Space Administration 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. NR 22 TC 0 Z9 0 U1 1 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0149-0419 J9 MAR GEOD JI Mar. Geod. PY 2011 VL 34 IS 3-4 SI SI BP 364 EP 381 DI 10.1080/01490419.2011.584836 PG 18 WC Geochemistry & Geophysics; Oceanography; Remote Sensing SC Geochemistry & Geophysics; Oceanography; Remote Sensing GA 855CQ UT WOS:000297541600010 ER PT J AU Sibthorpe, A Brown, S Desai, SD Haines, BJ AF Sibthorpe, Ant Brown, Shannon Desai, Shailen D. Haines, Bruce J. TI Calibration and Validation of the Jason-2/OSTM Advanced Microwave Radiometer Using Terrestrial GPS Stations SO MARINE GEODESY LA English DT Article DE Advanced microwave radiometer; GPS; satellite altimetry; wet troposphere ID PRECISION ORBIT DETERMINATION; WATER-VAPOR; DELAY; TEMPERATURE; PERFORMANCE; ALTIMETRY; MISSIONS; RECEIVER; ANTENNA; MODEL AB We use estimates of zenith tropospheric delay from terrestrial Global Positioning System (GPS) stations to validate the wet path-delay measurements from the Jason-2/Ocean Surface Topography Mission (OSTM) Advanced Microwave Radiometer (AMR). We validate theAMRwet path-delay measurements provided in the version "T" Geophysical Data Records (GDRs) and those generated using a recently developed coastal algorithm that will be applied to the version "C" GDRs. The new coastal algorithm reduces the variance of the GPS-AMR differences by as much as 28% within 25 km of land. This algorithm also facilitates open-ocean measurement accuracies as close to land as 15 km (as opposed to 25 km). We perform AMR/GPS comparisons with three different troposphere-mapping functions for the GPS-based estimates: Niell, Global, and Vienna. The choice of mapping function has minimal impact on our results, although the Vienna mapping function provided the smallest variance in the AMR-GPS differences. C1 [Sibthorpe, Ant; Brown, Shannon; Desai, Shailen D.; Haines, Bruce J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sibthorpe, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 238-600, Pasadena, CA 91109 USA. EM anthony.j.sibthorpe@jpl.nasa.gov RI Sibthorpe, Ant/C-1940-2012 FU National Aeronautics and Space Administration FX The research was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank Rob deCarvalho for various insightful discussions and the three anonymous reviewers for their input, which improved this manuscript. NR 30 TC 2 Z9 3 U1 1 U2 8 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0149-0419 EI 1521-060X J9 MAR GEOD JI Mar. Geod. PY 2011 VL 34 IS 3-4 SI SI BP 420 EP 430 DI 10.1080/01490419.2011.584839 PG 11 WC Geochemistry & Geophysics; Oceanography; Remote Sensing SC Geochemistry & Geophysics; Oceanography; Remote Sensing GA 855CQ UT WOS:000297541600014 ER PT J AU Baker, JD Harting, AL Wurth, TA Johanos, TC AF Baker, Jason D. Harting, Albert L. Wurth, Tracy A. Johanos, Thea C. TI Dramatic shifts in Hawaiian monk seal distribution predicted from divergent regional trends SO MARINE MAMMAL SCIENCE LA English DT Article DE Hawaiian monk seal; Monachus schauinslandi; survival; reproduction; population growth rate ID MONACHUS-SCHAUINSLANDI; SURVIVAL; ISLANDS; ABUNDANCE; SIZE; NORTHWESTERN; MORTALITY; MODEL AB P>Total estimated abundance of Hawaiian monk seals was just 1,161 individuals in 2008 and this number is decreasing. Most monk seals reside in the remote Northwestern Hawaiian Islands (NWHI) where the decline is approximately 4%/yr, whereas relatively fewer seals currently occupy the main Hawaiian Islands (MHI). It is widely accepted that the MHI population is increasing, although there are no formal estimates of total abundance, population growth rate or vital rates. This lack of information has hampered efforts to anticipate future scenarios and plan conservation measures. We present the first estimates of MHI monk seal survival and age-specific reproductive rates. Using these rates, a conservative estimate of current MHI abundance and a previously published stochastic simulation model, we estimate the MHI population growth rate and projected abundance trend. Analogous estimates for the NWHI are derived from a much richer data set. Estimated survival from weaning to age 1 yr is 77% in the MHI, much higher than recent NWHI estimates ranging from 42% to 57%. Moreover, MHI females begin reproducing at a younger age and attain higher birth rates than observed in the NWHI. The estimated MHI intrinsic rate of population growth is 1.07 compared to a 0.89-0.96 range in the NWHI. Assuming an initial abundance of 152 animals in the MHI, projections indicate that if current demographic trends continue, abundance in the NWHI and MHI will equalize in approximately 15 yr. These results underscore the imperative to mitigate the NWHI decline while devoting conservation efforts to foster population growth in the MHI, where documented threats including fishery interactions, direct killing, and disease could rapidly undo the current fragile positive trend. C1 [Baker, Jason D.; Johanos, Thea C.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. [Harting, Albert L.] Harting Biol Consulting, Bozeman, MT 59715 USA. [Wurth, Tracy A.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. RP Baker, JD (reprint author), NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, 2570 Dole St, Honolulu, HI 96822 USA. EM jason.baker@noaa.gov NR 30 TC 25 Z9 26 U1 5 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 EI 1748-7692 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD JAN PY 2011 VL 27 IS 1 BP 78 EP 93 DI 10.1111/j.1748-7692.2010.00395.x PG 16 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 700QU UT WOS:000285760200005 ER PT J AU Schoenfeld, MP Ansari, RR Zakrajsek, JF Billiar, TR Toyoda, Y Wink, DA Nakao, A AF Schoenfeld, Michael P. Ansari, Rafat R. Zakrajsek, June F. Billiar, Timothy R. Toyoda, Yoshiya Wink, David A. Nakao, Atsunori TI Hydrogen therapy may reduce the risks related to radiation-induced oxidative stress in space flight SO MEDICAL HYPOTHESES LA English DT Article ID RICH WATER; ANTIOXIDANT; SPACEFLIGHT; MICE AB Cosmic radiation is known to induce DNA and lipid damage associated with increased oxidative stress and remains a major concern in space travel. Hydrogen, recently discovered as a novel therapeutic medical gas in a variety of biomedical fields, has potent antioxidant and anti-inflammatory activities. It is expected that space mission activities will increase in coming years both in numbers and duration. It is therefore important to estimate and prevent the risks encountered by astronauts due to oxidative stress prior to developing clinical symptoms of disease. We hypothesize that hydrogen administration to the astronauts by either inhalation or drinking hydrogen-rich water may potentially yield a novel and feasible preventative/therapeutic strategy to prevent radiation-induced adverse events. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Nakao, Atsunori] Univ Pittsburgh, Dept Surg, Med Ctr, Pittsburgh, PA 15213 USA. [Schoenfeld, Michael P.] NASA, George C Marshall Space Flight Ctr, Prop Res & Technol Branch, Huntsville, AL 35812 USA. [Ansari, Rafat R.; Zakrajsek, June F.] NASA, John H Glenn Res Ctr Lewis Field, Biosci & Technol Branch, Cleveland, OH USA. [Toyoda, Yoshiya; Nakao, Atsunori] Univ Pittsburgh, Dept Surg, Thomas E Starzl Transplantat Inst, Heart Lung & Esophageal Surg Inst, Pittsburgh, PA 15213 USA. [Wink, David A.] NCI, Radiat Biol Branch, NIH, Bethesda, MD 20892 USA. RP Nakao, A (reprint author), Univ Pittsburgh, Dept Surg, Med Ctr, E1551,Biomed Sci Tower, Pittsburgh, PA 15213 USA. EM anakao@imap.pitt.edu NR 15 TC 15 Z9 18 U1 0 U2 11 PU CHURCHILL LIVINGSTONE PI EDINBURGH PA JOURNAL PRODUCTION DEPT, ROBERT STEVENSON HOUSE, 1-3 BAXTERS PLACE, LEITH WALK, EDINBURGH EH1 3AF, MIDLOTHIAN, SCOTLAND SN 0306-9877 J9 MED HYPOTHESES JI Med. Hypotheses PD JAN PY 2011 VL 76 IS 1 BP 117 EP 118 DI 10.1016/j.mehy.2010.08.046 PG 2 WC Medicine, Research & Experimental SC Research & Experimental Medicine GA 715VP UT WOS:000286918400028 PM 20851533 ER PT J AU Loehr, JA Lee, SMC English, KL Sibonga, J Smith, SM Spiering, BA Hagan, RD AF Loehr, James A. Lee, Stuart M. C. English, Kirk L. Sibonga, Jean Smith, Scott M. Spiering, Barry A. Hagan, R. Donald TI Musculoskeletal Adaptations to Training with the Advanced Resistive Exercise Device SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE LA English DT Article DE RESISTANCE EXERCISE; SPACEFLIGHT; MUSCLE STRENGTH; BONE MINERAL DENSITY; iRED ID INTERNATIONAL-SPACE-STATION; LONG-DURATION SPACEFLIGHT; INDUCED BONE LOSS; RESISTANCE EXERCISE; BED REST; SKELETAL-MUSCLE; FLIGHT; PERFORMANCE; FORCE; HIP AB LOEHR, J. A., S. M. C. LEE, K. L. ENGLISH, J. SIBONGA, S. M. SMITH, B. A. SPIERING, and R. D. HAGAN. Musculoskeletal Adaptations to Training with the Advanced Resistive Exercise Device. Med. Sci. Sports Exerc., Vol. 43, No. 1, pp. 146-156, 2011. Resistance exercise has been used as a means to prevent the musculoskeletal losses associated with spaceflight. Therefore, the National Aeronautics and Space Administration designed the Advanced Resistive Exercise Device (ARED) to replace the initial device flown on the International Space Station. The ARED uses vacuum cylinders and inertial flywheels to simulate, in the absence of gravity, the constant mass and inertia, respectively, of free weight (FW) exercise. Purpose: To compare the musculoskeletal effects of resistance exercise training using the ARED with the effects of training with FW. Methods: Previously untrained, ambulatory subjects exercised using one of two modalities: FW (6 men and 3 women) or ARED (8 men and 3 women). Subjects performed squat, heel raise, and dead lift exercises 3 d.wk(-1) for 16 wk. Squat, heel raise, and dead lift strength (one-repetition maximum; using FW and ARED), bone mineral density (via dual-energy x-ray absorptiometry), and vertical jump were assessed before, during, and after training. Muscle mass (via magnetic resonance imaging) and bone morphology (via quantitative computed tomography) were measured before and after training. Bone biomarkers and circulating hormones were measured before training and after 4, 8, and 16 wk. Results: Muscle strength, muscle volume, vertical jump height, and lumbar spine bone mineral density (via dual-energy x-ray absorptiometry and quantitative computed tomography) significantly increased (P <= 0.05) in both groups. There were no significant differences between groups in any of the dependent variables at any time. Conclusions: After 16 wk of training, ARED exercise resulted in musculoskeletal effects that were not significantly different from the effects of training with FW. Because FW training mitigates bed rest-induced deconditioning, the ARED may be an effective countermeasure for spaceflight-induced deconditioning and should be validated during spaceflight. C1 [Loehr, James A.; Smith, Scott M.; Hagan, R. Donald] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Loehr, James A.; Lee, Stuart M. C.; Spiering, Barry A.] Wyle Integrated Sci & Engn Grp, Houston, TX USA. [English, Kirk L.] JES Tech, Houston, TX USA. [Sibonga, Jean] Univ Space Res Assoc, Houston, TX USA. RP Loehr, JA (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code SK3, Houston, TX 77058 USA. EM james.a.loehr@nasa.gov FU NASA Johnson Space Center FX Funding for this work was provided by the Exercise Counter-measures Project at NASA Johnson Space Center. NR 35 TC 23 Z9 24 U1 0 U2 20 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0195-9131 J9 MED SCI SPORT EXER JI Med. Sci. Sports Exerc. PD JAN PY 2011 VL 43 IS 1 BP 146 EP 156 DI 10.1249/MSS.0b013e3181e4f161 PG 11 WC Sport Sciences SC Sport Sciences GA 695YW UT WOS:000285410000019 PM 20473227 ER PT J AU Barshi, I Healy, AF AF Barshi, Immanuel Healy, Alice F. TI The effects of spatial representation on memory for verbal navigation instructions SO MEMORY & COGNITION LA English DT Article DE Spatial cognition; Memory; Aviation; Communication ID VIEWER ROTATIONS; IMAGINED OBJECT; INFORMATION; COMPREHENSION; PERCEPTION; CAPACITY; MODELS AB Three experiments investigated effects of mental spatial representation on memory for verbal navigation instructions. The navigation instructions referred to a grid of stacked matrices displayed on a computer screen or on paper, with or without depth cues, and presented as two-dimensional diagrams or a three-dimensional physical model. Experimental instructions either did or did not promote a three-dimensional mental representation of the space. Subjects heard navigation instructions, immediately repeated them, and then followed them manually on the grid. In all display and experimental instruction conditions, memory for the navigation instructions was reduced when the task required mentally representing a three-dimensional space, with movements across multiple matrices, as compared with a two-dimensional space, with movements within a single matrix, even though the words in the navigation instructions were identical in all cases. The findings demonstrate that the mental representation of the space influences immediate verbatim memory for navigation instructions. C1 [Healy, Alice F.] Univ Colorado, Dept Psychol & Neurosci, Boulder, CO 80309 USA. [Barshi, Immanuel] NASA, Human Syst Integrat Div, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Healy, AF (reprint author), Univ Colorado, Dept Psychol & Neurosci, Muenzinger Bldg,345 UCB, Boulder, CO 80309 USA. EM Alice.Healy@Colorado.edu NR 30 TC 3 Z9 3 U1 1 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0090-502X J9 MEM COGNITION JI Mem. Cogn. PD JAN PY 2011 VL 39 IS 1 BP 47 EP 62 DI 10.3758/s13421-010-0024-5 PG 16 WC Psychology, Experimental SC Psychology GA 723NO UT WOS:000287513700005 PM 21264616 ER PT J AU Fleischer, I Schroder, C Klingelhofer, G Zipfel, J Morris, RV Ashley, JW Gellert, R Wehrheim, S Ebert, S AF Fleischer, Iris Schroeder, Christian Klingelhoefer, Goestar Zipfel, Jutta Morris, Richard V. Ashley, James W. Gellert, Ralf Wehrheim, Simon Ebert, Sandro TI New insights into the mineralogy and weathering of the Meridiani Planum meteorite, Mars SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID MOSSBAUER-SPECTROSCOPY; IRON-METEORITES; CHONDRITIC METEORITES; PHASES; RESONANCE; SPECTRA AB Meridiani Planum is the first officially recognized meteorite find on the surface of Mars. It was discovered at and named after the landing site of the Mars Exploration Rover Opportunity. Based on its composition, it was classified as a IAB complex iron meteorite. Mossbauer spectra obtained by Opportunity are dominated by kamacite (alpha-Fe-Ni) and exhibit a small contribution of ferric oxide. Several small features in the spectra have been neglected to date. To shed more light on these features, five iron meteorite specimens were investigated as analogs to Meridiani Planum with a laboratory Mossbauer setup. Measurements were performed on (1) their metallic bulk, (2) troilite (FeS) inclusions, (3) cohenite ((Fe,Ni,Co)(3)C) and schreibersite ((Fe,Ni)(3)P), and (4) corroded rims. In addition to these room-temperature measurements, a specimen from the Mundrabilla IAB-ungrouped meteorite was measured at Mars-equivalent temperatures. Based on these measurements, the features in Meridiani Planum spectra can be explained with the presence of small amounts of schreibersite and/or cohenite and iron oxides. The iron oxides can be attributed to a previously reported coating on Meridiani Planum. Their presence indicates weathering through the interaction of the meteorite with small amounts of water. C1 [Fleischer, Iris; Klingelhoefer, Goestar; Wehrheim, Simon; Ebert, Sandro] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55128 Mainz, Germany. [Schroeder, Christian] Univ Bayreuth, D-72076 Tubingen, Germany. [Schroeder, Christian] Univ Tubingen, D-72076 Tubingen, Germany. [Zipfel, Jutta] Senckenberg Forschungsinst, D-60325 Frankfurt, Germany. [Zipfel, Jutta] Nat Museum Frankfurt, Sekt Meteoritenforsch, D-60325 Frankfurt, Germany. [Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, ARES Code KR, Houston, TX 77058 USA. [Ashley, James W.] Arizona State Univ, Mars Space Flight Facil, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Gellert, Ralf] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. RP Fleischer, I (reprint author), Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, Staudinger Weg 9, D-55128 Mainz, Germany. EM fleischi@uni-mainz.de RI Schroder, Christian/B-3870-2009 OI Schroder, Christian/0000-0002-7935-6039 FU German Space Agency (DLR) [50QM9902]; Technical University of Darmstadt; University of Mainz; Russian space agency; JPL engineering; MER Athena Science Team FX Development of the MIMOS II Mossbauer spectrometer was funded by the German Space Agency (DLR) under contract 50QM9902 and supported by the Technical University of Darmstadt and the University of Mainz. We thank Dr. Beda Hofmann (Natural History Museum, Bern, Switzerland), and the Senckenberg-Museum (Frankfurt, Germany) for providing meteorite specimens for this study. The support of the Russian space agency is acknowledged. We acknowledge the unwavering support of JPL engineering and MER operations staff and the MER Athena Science Team. We thank A. Kracher and an anonymous reviewer for thoughtful reviews of the manuscript. NR 63 TC 9 Z9 9 U1 2 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JAN PY 2011 VL 46 IS 1 BP 21 EP 34 DI 10.1111/j.1945-5100.2010.01141.x PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 719YR UT WOS:000287247900002 ER PT S AU Ricco, AJ Parra, M Niesel, D Piccini, M Ly, D McGinnis, M Kudlicki, A Hines, JW Timucin, L Beasley, C Ricks, R McIntyre, M Friedericks, C Henschke, M Leung, R Diaz-Aguado, M Kitts, C Mas, I Rasay, M Agasid, E Luzzi, E Ronzano, K Squires, D Yost, B AF Ricco, Antonio J. Parra, Macarena Niesel, David Piccini, Matthew Ly, Diana McGinnis, Michael Kudlicki, Andrzej Hines, John W. Timucin, Linda Beasley, Chris Ricks, Robert McIntyre, Michael Friedericks, Charlie Henschke, Michael Leung, Ricky Diaz-Aguado, Millan Kitts, Christopher Mas, Ignacio Rasay, Mike Agasid, Elwood Luzzi, Ed Ronzano, Karolyn Squires, David Yost, Bruce BE Becker, H Gray, BL TI PharmaSat: Drug dose response in microgravity from a free-flying integrated biofluidic/optical culture-and-analysis satellite SO MICROFLUIDICS, BIOMEMS, AND MEDICAL MICROSYSTEMS IX SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Microfluidics, BioMEMS, and Medical Microsystems IX CY JAN 23-25, 2011 CL San Francisco, CA SP SPIE, microfluidic ChipShop GmbH, NanoInk, Inc DE PharmaSat; integrated microsystem; yeast; microfluidics; optical absorbance; voriconazole; nanosatellite ID GENE-EXPRESSION; SPACE AB We designed, built, tested, space-qualified, launched, and collected telemetered data from low Earth orbit from PharmaSat, a 5.1-kg free flying "nanosatellite" that supported microbial growth in 48 microfluidic wells, dosed microbes with multiple concentrations of a pharmaceutical agent, and monitored microbial growth and metabolic activity using a dedicated 3-color optical absorbance system at each microwell. The PharmaSat nanosatellite comprised a structure approximately 10 x 10 x 35 cm, including triple-junction solar cells, bidirectional communications, power-generation and energy-storage system, and a sealed payload 1.2-L containment vessel that housed the biological organisms along with the fluidic, optical, thermal, sensor, and electronic subsystems. Growth curves for S. cerevisiae (Brewer's yeast) were obtained for multiple concentrations of the antifungal drug voriconazole in the microgravity conditions of low Earth orbit. Corresponding terrestrial control experiments were conducted for comparison. C1 [Ricco, Antonio J.; Parra, Macarena; Piccini, Matthew; Ly, Diana; Hines, John W.; Timucin, Linda; Beasley, Chris; Ricks, Robert; McIntyre, Michael; Friedericks, Charlie; Henschke, Michael; Leung, Ricky; Diaz-Aguado, Millan; Agasid, Elwood; Luzzi, Ed; Ronzano, Karolyn; Squires, David; Yost, Bruce] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ricco, AJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM ajricco@stanford.edu RI Kudlicki, Andrzej/C-7612-2012; Ricco, Antonio/A-5273-2010; Mavoa, Suzanne/B-5372-2010; OI Ricco, Antonio/0000-0002-2355-4984 NR 9 TC 1 Z9 1 U1 0 U2 9 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-466-6 J9 PROC SPIE PY 2011 VL 7929 AR 79290T DI 10.1117/12.881082 PG 9 WC Nanoscience & Nanotechnology; Optics SC Science & Technology - Other Topics; Optics GA BYC94 UT WOS:000298046300025 ER PT B AU Arnold, SM Wong, TT AF Arnold, Steven M. Wong, Terry T. BE Arnold, SM Wong, TT TI Proceedings of the Symposium Held at Materials Science & Technology 2010 October 18-20, 2010 Houston, Texas, USA INTRODUCTION SO MODELS, DATABASES, AND SIMULATION TOOLS NEEDED FOR THE REALIZATION OF INTEGRATED COMPUTATIONAL MATERIALS ENGINEERING LA English DT Proceedings Paper CT Symposium on Models, Databases, and Simulation Tools Needed for the Realization of Integrated Computational Materials Engineering CY OCT 18-20, 2010 CL Houston, TX SP ASM, Mat Properties Database Comm C1 [Arnold, Steven M.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Wong, Terry T.] Pratt & Whitney Rocketdyne, Canoga Pk, CA USA. RP Arnold, SM (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU ASM INTERNATIONAL PI MATERIALS PARK PA 9503 KINSMAN RD, MATERIALS PARK, OH 44073 USA BN 978-1-61503-831-2 PY 2011 BP 1 EP 5 PG 5 WC Materials Science, Multidisciplinary SC Materials Science GA BH0FQ UT WOS:000394826200001 ER PT B AU Sullivan, RW Arnold, SM AF Sullivan, Rani W. Arnold, Steven M. BE Arnold, SM Wong, TT TI AN ANNOTATIVE REVIEW OF MULTISCALE MODELING AND ITS APPLICATION TO SCALES INHERENT IN THE FIELD OF ICME SO MODELS, DATABASES, AND SIMULATION TOOLS NEEDED FOR THE REALIZATION OF INTEGRATED COMPUTATIONAL MATERIALS ENGINEERING LA English DT Proceedings Paper CT Symposium on Models, Databases, and Simulation Tools Needed for the Realization of Integrated Computational Materials Engineering CY OCT 18-20, 2010 CL Houston, TX SP ASM, Mat Properties Database Comm ID FIBER-REINFORCED COMPOSITES; THIN METAL-FILMS; MATRIX COMPOSITES; POLYMER MATERIALS; FABRIC COMPOSITES; CARBON NANOTUBES; LENGTH SCALES; FAILURE; BEHAVIOR; DAMAGE AB In order to obtain a general understanding of the rich and diverse research being conducted in the area of multiscale modeling (MM), an overview is conducted with a special focus on composite materials. The objective is to glean both qualitative and quantitative information with regards to MM efforts with intentions of revealing some issues that may enable the field of Integrated Computational Materials Engineering (ICME) as well as providing a starting point for specialists and non-specialists in the area of MM with regards to a variety of classifications. C1 [Sullivan, Rani W.] Mississippi State Univ, Mississippi State, MS 39762 USA. [Arnold, Steven M.] NASA Glenn Res Ctr, Cleveland, OH USA. RP Sullivan, RW (reprint author), Mississippi State Univ, Mississippi State, MS 39762 USA. NR 117 TC 1 Z9 1 U1 0 U2 0 PU ASM INTERNATIONAL PI MATERIALS PARK PA 9503 KINSMAN RD, MATERIALS PARK, OH 44073 USA BN 978-1-61503-831-2 PY 2011 BP 6 EP 23 PG 18 WC Materials Science, Multidisciplinary SC Materials Science GA BH0FQ UT WOS:000394826200002 ER PT B AU Bednarcyk, BA Arnold, SM AF Bednarcyk, Brett A. Arnold, Steven M. BE Arnold, SM Wong, TT TI A MULTISCALE, NONLINEAR, MODELING FRAMEWORK ENABLING THE DESIGN AND ANALYSIS OF COMPOSITE MATERIALS AND STRUCTURES SO MODELS, DATABASES, AND SIMULATION TOOLS NEEDED FOR THE REALIZATION OF INTEGRATED COMPUTATIONAL MATERIALS ENGINEERING LA English DT Proceedings Paper CT Symposium on Models, Databases, and Simulation Tools Needed for the Realization of Integrated Computational Materials Engineering CY OCT 18-20, 2010 CL Houston, TX SP ASM, Mat Properties Database Comm ID GENERALIZED-METHOD; CELLS AB A framework for the multiscale design and analysis of composite materials and structures is presented. The ImMAC software suite, developed at NASA Glenn Research Center, embeds efficient, nonlinear micromechanics capabilities within higher scale structural analysis methods such as finite element analysis. The result is an integrated, multiscale tool that relates global loading to the constituent scale, captures nonlinearities at this scale, and homogenizes local nonlinearities to predict their effects at the structural scale. Example applications of the multiscale framework are presented for the stochastic progressive failure of a SiC/Ti composite tensile specimen and the effects of microstructural variations on the nonlinear response of woven polymer matrix composites. C1 [Bednarcyk, Brett A.; Arnold, Steven M.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Bednarcyk, BA (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. NR 19 TC 0 Z9 0 U1 0 U2 0 PU ASM INTERNATIONAL PI MATERIALS PARK PA 9503 KINSMAN RD, MATERIALS PARK, OH 44073 USA BN 978-1-61503-831-2 PY 2011 BP 167 EP 184 PG 18 WC Materials Science, Multidisciplinary SC Materials Science GA BH0FQ UT WOS:000394826200016 ER PT B AU Arnold, SM Wong, TT AF Arnold, Steven M. Wong, Terry T. BE Arnold, SM Wong, TT TI CONCLUSION SO MODELS, DATABASES, AND SIMULATION TOOLS NEEDED FOR THE REALIZATION OF INTEGRATED COMPUTATIONAL MATERIALS ENGINEERING LA English DT Proceedings Paper CT Symposium on Models, Databases, and Simulation Tools Needed for the Realization of Integrated Computational Materials Engineering CY OCT 18-20, 2010 CL Houston, TX SP ASM, Mat Properties Database Comm C1 [Arnold, Steven M.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Wong, Terry T.] Pratt & Whitney Rocketdyne, Canoga Pk, CA USA. RP Arnold, SM (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASM INTERNATIONAL PI MATERIALS PARK PA 9503 KINSMAN RD, MATERIALS PARK, OH 44073 USA BN 978-1-61503-831-2 PY 2011 BP 185 EP 194 PG 10 WC Materials Science, Multidisciplinary SC Materials Science GA BH0FQ UT WOS:000394826200017 ER PT J AU Ma, Q Tipping, RH Lavrentieva, NN AF Ma, Q. Tipping, R. H. Lavrentieva, N. N. TI Pair identity and smooth variation rules applicable for the spectroscopic parameters of H2O transitions involving high-J states SO MOLECULAR PHYSICS LA English DT Article DE energy levels and wavefunctions of H2O states; spectroscopic parameters of H2O lines; half-widths and shifts; HITRAN; HITEMP ID WATER-VAPOR LINES; BROADENING PARAMETERS; HALF-WIDTHS; DATABASE; HITRAN; LIST; BAND AB Two basic rules (i.e. the pair identity and the smooth variation) applicable for H2O transitions involving high-J states have been discovered. The origins of these rules are the properties of the energy levels and wavefunctions of H2O states with the quantum number J above certain boundaries. As a result, for lines involving high-J states in individually defined groups, all their spectroscopic parameters (i.e. the transition wavenumber, intensity, pressure-broadened half-width, pressure-induced shift, and temperature exponent) must follow these rules. One can use these rules to screen spectroscopic data provided by databases and to identify possible errors. In addition, by using extrapolation methods within the individual groups, one is able to predict the spectroscopic parameters for lines in this group involving very high-J states. The latter are required in developing high-temperature molecular spectroscopic databases such as HITEMP. C1 [Ma, Q.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ma, Q.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Tipping, R. H.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Lavrentieva, N. N.] VE Zuev Inst Atmospher Opt SB RAS, Tomsk 634021, Russia. RP Ma, Q (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM qma@giss.nasa.gov RI Lavrentieva, Nina/A-4010-2014 FU NASA [NNG06GB23G, NNX09AB62G, FCCS-547, DE-AI02-93ER61744, NNH08ZDA001N-ACLAB]; Biological and Environmental Research Program (BER), U.S. Department of Energy [DE-AI02-93ER61744]; Office of Science of the U. S. Department of Energy [DE-AC02-05CH11231] FX Two of the authors (Q. Ma and R. H. Tipping) acknowledge financial support from NASA under grants NNG06GB23G, NNX09AB62G, and FCCS-547. Q. Ma wishes to acknowledge financial support from the Biological and Environmental Research Program (BER), U.S. Department of Energy, Interagency Agreement No. DE-AI02-93ER61744, and financial support from NASA under grant NNH08ZDA001N-ACLAB. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U. S. Department of Energy under contract No. DE-AC02-05CH11231. NR 19 TC 8 Z9 8 U1 0 U2 1 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 J9 MOL PHYS JI Mol. Phys. PY 2011 VL 109 IS 15 BP 1925 EP 1941 DI 10.1080/00268976.2011.599343 PG 17 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 827WJ UT WOS:000295459800007 ER PT J AU Balona, LA Cunha, MS Kurtz, DW Brandao, IM Gruberbauer, M Saio, H Ostensen, R Elkin, VG Borucki, WJ Christensen-Dalsgaard, J Kjeldsen, H Koch, DG Bryson, ST AF Balona, L. A. Cunha, M. S. Kurtz, D. W. Brandao, I. M. Gruberbauer, M. Saio, H. Ostensen, R. Elkin, V. G. Borucki, W. J. Christensen-Dalsgaard, J. Kjeldsen, H. Koch, D. G. Bryson, S. T. TI Kepler observations of rapidly oscillating Ap, delta Scuti and gamma Doradus pulsations in Ap stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE asteroseismology; stars: chemically peculiar; stars: individual: BD+44 3063; stars: oscillations; stars: variables: general ID ROAP STARS; MAGNETIC-FIELDS; MODE PULSATIONS; EXCITATION; MECHANISM; DISCOVERY AB Observations of the A5p star KIC 8677585 obtained during the Kepler 10-d commissioning run with 1-min time resolution show that it is a rapidly oscillating Ap (roAp) star with several frequencies with periods near 10 min. In addition, a low frequency at 3.142 d-1 is also clearly present. Multiperiodic gamma Doradus (gamma Dor) and delta Scuti (delta Sct) pulsations, never before seen in any Ap star, are present in Kepler observations of at least three other Ap stars. Since gamma Dor pulsations are seen in Ap stars, it is likely that the low frequency in KIC 8677585 is also a gamma Dor pulsation. The simultaneous presence of both gamma Dor and roAp pulsations and the unexpected detection of delta Sct and gamma Dor pulsations in Ap stars present new opportunities and challenges for the interpretation of these stars. Since it is easy to confuse Am and Ap stars at classification dispersions, the nature of these Ap stars in the Kepler field needs to be confirmed. C1 [Balona, L. A.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Cunha, M. S.; Brandao, I. M.] Univ Porto, Ctr Astrofis, P-4150 Oporto, Portugal. [Cunha, M. S.; Brandao, I. M.] Univ Porto, Fac Ciencias, P-4150 Oporto, Portugal. [Kurtz, D. W.; Elkin, V. G.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England. [Gruberbauer, M.] St Marys Univ, Dept Astron & Phys, Halifax, NS B3H 3C3, Canada. [Saio, H.] Tohoku Univ, Grad Sch Sci, Astron Inst, Sendai, Miyagi 9808578, Japan. [Ostensen, R.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Borucki, W. J.; Koch, D. G.; Bryson, S. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. RP Balona, LA (reprint author), S African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa. EM lab@saao.ac.za RI Brandao, Isa/M-5172-2013 OI Brandao, Isa/0000-0002-1153-0942 FU South African Astronomical Observatory; FCT/MCTES, Portugal [PTDC/CTE-AST/098754/2008, SFRH/BD/41213/2007]; POPH/FSE (EC); NSERC; NASA's Science Mission Directorate FX The authors wish to thank the Kepler team for their generosity in allowing the data to be released to the Kepler Asteroseismic Science Consortium (KASC) ahead of public release and for their outstanding efforts which have made these results possible. Funding for the Kepler Mission is provided by NASA's Science Mission Directorate. We particularly thank Ron Gilliland and Hans Kjeldsen for their tireless work on behalf of KASC.; LAB wishes to thank the South African Astronomical Observatory for financial support.; This work was partially supported by the project PTDC/CTE-AST/098754/2008 and the grant SFRH/BD/41213/2007 funded by FCT/MCTES, Portugal. MSC is supported by a Ciencia 2007 contract, funded by FCT/MCTES(Portugal) and POPH/FSE (EC).; MG has received financial support through D. Guenther's NSERC grant. NR 32 TC 31 Z9 31 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 1 PY 2011 VL 410 IS 1 BP 517 EP 524 DI 10.1111/j.1365-2966.2010.17461.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 693UH UT WOS:000285250400039 ER PT J AU Curran, PA Maccarone, TJ Casella, P Evans, PA Landsman, W Krimm, HA Brocksopp, C Still, M AF Curran, P. A. Maccarone, T. J. Casella, P. Evans, P. A. Landsman, W. Krimm, H. A. Brocksopp, C. Still, M. TI Black hole candidate XTE J1752-223: Swift observations of canonical states during outburst SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; stars: individual: XTE J1752-223; X-rays: binaries; X-rays: bursts ID X-RAY TELESCOPE; ULTRAVIOLET/OPTICAL TELESCOPE; MULTIWAVELENGTH OBSERVATIONS; AQUILA X-1; HARD STATE; VARIABILITY; EMISSION; DISC; CALIBRATION; J1550-564 AB We present Swift broad-band observations of the recently discovered black hole candidate, X-ray transient, XTE J1752-223, obtained over the period of outburst from 2009 October to 2010 June. From Swift-Ultraviolet/Optical Telescope (UVOT) data we confirm the presence of an optical counterpart which displays variability correlated, in the soft state, to the X-ray emission observed by Swift-X-ray Telescope (XRT). The optical counterpart also displays hysteretical behaviour between the states not normally observed in the optical bands, suggesting a possible contribution from a synchrotron-emitting jet to the optical emission in the rising hard state. We offer a purely phenomenological treatment of the spectra as an indication of the canonical spectral state of the source during different periods of the outburst. We find that the high-energy hardness-intensity diagrams over two separate bands follow the canonical behaviour, confirming the spectral states. Our XRT timing analysis shows that in the hard state there is significant variability below 10 Hz which is more pronounced at low energies, while during the soft state the level of variability is consistent with being minimal. These properties of XTE J1752-223 support its candidacy as a black hole in the Galactic Centre region. C1 [Curran, P. A.; Brocksopp, C.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Maccarone, T. J.; Casella, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Evans, P. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Still, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Curran, PA (reprint author), Univ Paris Diderot, CNRS, CEA DSM, AIM,Irfu SAP,Ctr Saclay, Bat 709, FR-91191 Gif Sur Yvette, France. EM peter.curran@cea.fr RI Curran, Peter/B-5293-2013; OI Curran, Peter/0000-0003-3003-4626; Casella, Piergiorgio/0000-0002-0752-3301 FU EU [ITN215212, 2009-237722]; STFC FX We thank the referee for constructive comments and Paul Kuin for useful discussions on UVOT. PAC, PAE and CB acknowledge support from STFC. TJM thanks the EU FP7 for support through grant number ITN215212 'Black Hole Universe'. PC acknowledges funding via a EU Marie Curie Intra-European Fellowship under contract no. 2009-237722. This research has made use of Swift data supplied by the UK Swift Science Data Centre at the University of Leicester and MAXI data provided by RIKEN, JAXA and MAXI teams. NR 41 TC 12 Z9 12 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN 1 PY 2011 VL 410 IS 1 BP 541 EP 547 DI 10.1111/j.1365-2966.2010.17460.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 693UH UT WOS:000285250400042 ER PT J AU Clark, DM Eikenberry, SS Brandl, BR Wilson, JC Carson, JC Henderson, CP Hayward, TL Barry, DJ Ptak, AF Colbert, EJM AF Clark, D. M. Eikenberry, S. S. Brandl, B. R. Wilson, J. C. Carson, J. C. Henderson, C. P. Hayward, T. L. Barry, D. J. Ptak, A. F. Colbert, E. J. M. TI Multiwavelength study of Chandra X-ray sources in the Antennae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: starburst; galaxies: star clusters: general; X-rays: binaries ID YOUNG STAR-CLUSTERS; GALAXIES; NGC-4038/4039; COUNTERPARTS; RESOLUTION; DISTANCE; WFPC2 AB We use Wide-field InfraRed Camera (WIRC) infrared (IR) images of the Antennae (NGC 4038/4039) together with the extensive catalogue of 120 X-ray point sources to search for counterpart candidates. Using our proven frame-tie technique, we find 38 X-ray sources with IR counterparts, almost doubling the number of IR counterparts to X-ray sources that we first identified. In our photometric analysis, we consider the 35 IR counterparts that are confirmed star clusters. We show that the clusters with X-ray sources tend to be brighter, K-s approximate to 16 mag, with (J- K-s) = 1.1 mag. We then use archival Hubble Space Telescope (HST) images of the Antennae to search for optical counterparts to the X-ray point sources. We employ our previous IR-to-X-ray frame-tie as an intermediary to establish a precise optical-to-X-ray frame-tie with < 0.6 arcsec rms positional uncertainty. Due to the high optical source density near the X-ray sources, we determine that we cannot reliably identify counterparts. Comparing the HST positions to the 35 identified IR star cluster counterparts, we find optical matches for 27 of these sources. Using Bruzual-Charlot spectral evolutionary models, we find that most clusters associated with an X-ray source are massive, and young, similar to 106 yr. C1 [Clark, D. M.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Clark, D. M.; Eikenberry, S. S.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Brandl, B. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Wilson, J. C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Carson, J. C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Carson, J. C.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Henderson, C. P.; Barry, D. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Hayward, T. L.] AURA, Gemini Observ, La Serena, Chile. [Ptak, A. F.] NASA, GSFC, Greenbelt, MD 20770 USA. [Colbert, E. J. M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Clark, DM (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 877, Ensenada, Baja California, Mexico. EM dmclark@astrosen.unam.mx RI Ptak, Andrew/D-3574-2012 FU NSF [NSF-AST0328522, NSF-9983830, NSF-AST0507547]; Norris Foundation; Cornell University; WIRC FX The authors thank the staff of Palomar Observatory for their excellent assistance in commissioning WIRC and obtaining these data. WIRC was made possible by support from the NSF (NSF-AST0328522), the Norris Foundation and Cornell University. Based on observations made with the NASA/ESA HST, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. DMC is grateful for the many useful discussions with Michelle Edwards and Valerie Mikles. SSE and DMC received support in part by an NSF CAREER award (NSF-9983830) and an NSF grant (NSF-AST0507547). We also thank J. Houck for his support of the WIRC instrument project. NR 23 TC 4 Z9 4 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 JAN PY 2011 VL 410 IS 2 BP 890 EP 898 DI 10.1111/j.1365-2966.2010.17487.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700TA UT WOS:000285766000012 ER PT J AU Rubin, RH Simpson, JP O'Dell, CR McNabb, IA Colgan, SWJ Zhuge, SY Ferland, GJ Hidalgo, SA AF Rubin, Robert H. Simpson, Janet P. O'Dell, C. R. McNabb, Ian A. Colgan, Sean W. J. Zhuge, Scott Y. Ferland, Gary J. Hidalgo, Sergio A. TI Spitzer reveals what is behind Orion's Bar SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: abundances; H ii regions; ISM: individual objects: Orion Nebula ID H-II REGIONS; ELEMENTAL ABUNDANCE RATIOS; ELECTRON-IMPACT EXCITATION; SOLAR MODEL PROBLEM; EMISSION-LINES; PHYSICAL CONDITIONS; SPACE-TELESCOPE; PHOTODISSOCIATION REGION; TRANSITION-PROBABILITIES; INFRARED SPECTROGRAPH AB We present Spitzer Space Telescope observations of 11 regions south-east (SE) of the Bright Bar in the Orion Nebula, along a radial from the exciting star theta 1 Ori C, extending from 2.6 to 12.1 arcmin. Our Cycle 5 programme obtained deep spectra with matching Infrared Spectrograph (IRS) short-high (SH) and long-high (LH) aperture grid patterns. Most previous IR missions observed only the inner few arcmin (the 'Huygens' Region). The extreme sensitivity of Spitzer in the 10-37 mu m spectral range permitted us to measure many lines of interest to much larger distances from theta 1 Ori C. Orion is the benchmark for studies of the interstellar medium, particularly for elemental abundances. Spitzer observations provide a unique perspective on the neon and sulphur abundances by virtue of observing the dominant ionization states of Ne (Ne+, Ne++) and S (S++, S3 +) in Orion and H ii regions in general. The Ne/H abundance ratio is especially well determined, with a value of (1.02 +/- 0.02) x 10-4 or in terms of the conventional expression, 12 + log(Ne/H) = 8.01 +/- 0.01. We obtained corresponding new ground-based spectra at Cerro Tololo Inter-American Observatory (CTIO). These optical data are used to estimate the electron temperature, electron density, optical extinction and the S+/S++ ionization ratio at each of our Spitzer positions. That permits an adjustment for the total gas-phase sulphur abundance because no S+ line is observed by Spitzer. The gas-phase S/H abundance ratio is (7.68 +/- 0.25) x 10-6 or 12 + log(S/H) = 6.89 +/- 0.02. The Ne/S abundance ratio may be determined even when the weaker hydrogen line, H(7-6) here, is not measured. The mean value, adjusted for the optical S+/S++ ratio, is Ne/S = 13.0 +/- 0.2. We derive the electron density (N-e) versus distance from theta 1 Ori C for [S iii] (Spitzer) and [S ii] (CTIO). Both distributions are for the most part decreasing with increasing distance. The values for N-e [S ii] fall below those of N-e [S iii] at a given distance except for the outermost position. This general trend is consistent with the commonly accepted blister model for the Orion Nebula. The natural shape of such a blister is concave with an underlying decrease in density with increasing distance from the source of photoionization. Our spectra are the deepest ever taken in these outer regions of Orion over the 10-37 mu m range. Tracking the changes in ionization structure via the line emission to larger distances provides much more leverage for understanding the far less studied outer regions. A dramatic find is the presence of high-ionization Ne++ all the way to the outer optical boundary similar to 12 arcmin from theta 1 Ori C. This IR result is robust, whereas the optical evidence from observations of high-ionization species (e.g. O++) at the outer optical boundary suffers uncertainty because of scattering of emission from the much brighter inner Huygens Region. The Spitzer spectra are consistent with the Bright Bar being a high-density 'localized escarpment' in the larger Orion Nebula picture. Hard ionizing photons reach most solid angles well SE of the Bright Bar. The so-called Orion foreground 'Veil', seen prominently in projection at our outermost position 12 arcmin from theta 1 Ori C, is likely an H ii region-photo-dissociation region (PDR) interface. The Spitzer spectra show very strong enhancements of PDR lines - [Si ii] 34.8 mu m, [Fe ii] 26.0 mu m and molecular hydrogen - at the outermost position. C1 [Rubin, Robert H.; Simpson, Janet P.; Colgan, Sean W. J.; Zhuge, Scott Y.; Hidalgo, Sergio A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rubin, Robert H.] Orion Enterprises, Moffett Field, CA 94035 USA. [Simpson, Janet P.] SETI Inst, Mountain View, CA 94043 USA. [O'Dell, C. R.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [McNabb, Ian A.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Ferland, Gary J.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Rubin, RH (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM robert.h.rubin@nasa.gov RI Colgan, Sean/M-4742-2014; OI Ferland, Gary/0000-0003-4503-6333 FU NASA [1407, 50082, 07-ATFP07-0124]; HST [10967]; NSF [0607028, 0908877] 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 NASA contract 1407. Support for this work was provided by NASA for this Spitzer programme identification 50082. In addition to the Spitzer support, CRO was supported in part by HST grant AR 10967. GJF gratefully acknowledges support by NSF (0607028 and 0908877) and NASA (07-ATFP07-0124). We thank Don Clayton and Stan Woosley for providing information on the Ne/S ratio from a nucleosynthesis, GCE perspective. We are grateful for the help of our students - David Ng, Tim Craven, Savannah Lodge-Scharff, Evan Gitterman, Chris Lo and Atish Agarwala - at various stages of this work. We thank the referee for valuable comments. NR 64 TC 28 Z9 29 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2011 VL 410 IS 2 BP 1320 EP 1348 DI 10.1111/j.1365-2966.2010.17522.x PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 700TA UT WOS:000285766000044 ER PT S AU Han, JW Lohn, A Kobayashi, NP Meyyappan, M AF Han, Jin-Woo Lohn, Andrew Kobayashi, Nobuhiko P. Meyyappan, M. BE Kobayashi, NP Talin, AA Islam, MS TI Copper oxide thin-flim and nanowire for e-textile applications SO NANOEPITAXY: MATERIALS AND DEVICES III SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Nanoepitaxy - Materials and Devices III CY AUG 24-25, 2011 CL San Diego, CA SP SPIE DE Copper oxide; Nanowire; Thin-film; Interconnect; Resistive memory; Transistor AB Devices fabricated using nanowire structures can provide performance enhancement as well as open new applications. Integration of electronics into textile, referred to as e-textile, offers an opportunity for future electronics. Herein, copper and copper oxide based nanostructures are embedded for e-textile. Metallic copper wire is utilized as a growth substrate, which is simultaneously used as the fiber of mesh textiles. Among various metals, copper is promising as it is non-toxic and relatively abundant on earth. The motivating factor is ease of growth of nanostructures; the nanowire and thin-film forms are synthesized by self-catalytic vapor-solid growth. Simply heating with oxygen gas can form copper oxide nanowires or thin-film depending on the growth conditions. As key building blocks in e-textile, memory, transistor, and interconnect are presented. The resistive memory is comprised of copper oxide thin-film sandwiched within two orthogonal fibers. For a metal semiconductor field effect transistor (MESFET), a Schottky junction is used as the gate to channel barrier. The copper fiber and copper oxide thin-film are devoted to the gate and channel, respectively. For an interconnection, the neighboring fibers are electrically connected by transforming copper oxide nanowires into copper nanowires. Hydrogen thermal reduction of copper oxide is proved to be effective to make conductive nanowires. C1 [Han, Jin-Woo; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM jin-woo.han@nasa.gov RI Kobayashi, Nobuhiko/E-3834-2012 NR 10 TC 0 Z9 0 U1 4 U2 8 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-716-2 J9 PROC SPIE PY 2011 VL 8106 AR 810608 DI 10.1117/12.897454 PG 6 WC Nanoscience & Nanotechnology; Optics; Physics, Applied SC Science & Technology - Other Topics; Optics; Physics GA BXD01 UT WOS:000295777800002 ER PT S AU Ott, MN Thomes, WJ Chuska, RF Switzer, R Blair, DE AF Ott, Melanie N. Thomes, W. Joe, Jr. Chuska, Richard F. Switzer, Robert Blair, Diana E. BE Taylor, EW Cardimona, DA TI Small form factor optical fiber connector evaluation for harsh environments SO NANOPHOTONICS AND MACROPHOTONICS FOR SPACE ENVIRONMENTS V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Nanophotonics and Macrophotonics for Space Environments V (NMSE) CY AUG 22-23, 2011 CL San Diego, CA SP SPIE DE space flight; fiber optic; connector; LIDAR; cable; communication; interconnection; vibration AB For the past decade NASA programs have utilized the Diamond AVIM connector for optical fiber assemblies on space flight instrumentation. These connectors have been used in communications, sensing and LIDAR systems where repeatability and high performance are required. Recently Diamond has released a smaller form factor optical fiber connector called the "Mini-AVIM" which although more compact still includes the tight tolerances and the ratcheting feature of the heritage AVIM. NASA Goddard Space Flight Center Photonics Group in the Parts, Packaging and Assembly Technologies Office has been performing evaluations of this connector to determine how it compares to the performance of the AVIM connector and to assess its feasibility for harsh environmental applications. Vibration and thermal testing were performed on the Mini-AVIM with both multi-mode and single-mode optical fiber using insitu optical transmission monitoring. Random vibration testing was performed using typical launch condition profiles for most NASA missions but extended to 35 Grms, which is much higher than most requirements. Thermal testing was performed incrementally up to a range of -55 degrees C to + 125 degrees C. The test results include both unjacketed fiber and cabled assembly evaluations. The data presented here indicate that the Mini-AVIM provides a viable option for small form factor applications that require a high performance optical fiber connector. C1 [Ott, Melanie N.; Thomes, W. Joe, Jr.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ott, MN (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Melanie.Ott@nasa.gov NR 3 TC 0 Z9 0 U1 1 U2 4 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-774-2 J9 PROC SPIE PY 2011 VL 8164 AR 81640E DI 10.1117/12.895961 PG 14 WC Astronomy & Astrophysics; Nanoscience & Nanotechnology; Optics SC Astronomy & Astrophysics; Science & Technology - Other Topics; Optics GA BXZ24 UT WOS:000297674100013 ER PT S AU Prasad, NS AF Prasad, Narasimha S. BE Taylor, EW Cardimona, DA TI Recent progress made in testing laser diodes and optical materials subjected to exposure in space SO NANOPHOTONICS AND MACROPHOTONICS FOR SPACE ENVIRONMENTS V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Nanophotonics and Macrophotonics for Space Environments V (NMSE) CY AUG 22-23, 2011 CL San Diego, CA SP SPIE DE MISSE 6; MISSE 7; Space Qualification; Laser components; International Space Station; STS-123; STS-128; STS-129; STS-134 AB In this paper, progress made so far in the performance testing of waveguide laser components sent by NASA Langley Research Center on MISSE 6 mission will be discussed. The objective of the Materials International Space Station Experiment (MISSE) is to study the performance of novel materials when subjected to the synergistic effects of the harsh space environment for several months. MISSE missions provide an opportunity for developing space qualifiable materials. The results of post-testing of several optical materials that were recently returned back after more than one year of exposure on the International Space Station (ISS) will be presented. The items were part of the MISSE 6 mission that was transported to the ISS via STS 123 on March 11, 2008 and returned to the Earth via STS 128 that was launched on August 2009. The materials experienced no visible damage during lengthy exposure in space. In the case of laser diode, a comparison of elemental analysis with pre-flight conditions will be presented. Furthermore, the optical components sent on MISSE 7 mission via STS-129 and later retrieved by STS-134 will be briefly discussed. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Prasad, NS (reprint author), NASA, Langley Res Ctr, 5 N Dryden St,MS 468, Hampton, VA 23681 USA. EM narasimha.s.prasad@nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-774-2 J9 PROC SPIE PY 2011 VL 8164 AR 816402 DI 10.1117/12.895411 PG 9 WC Astronomy & Astrophysics; Nanoscience & Nanotechnology; Optics SC Astronomy & Astrophysics; Science & Technology - Other Topics; Optics GA BXZ24 UT WOS:000297674100002 ER PT S AU Slaba, TC McMullen, AM Thibeault, SA Sandridge, CA Clowdsley, MS Blattnig, SR AF Slaba, Tony C. McMullen, Amelia M. Thibeault, Sheila A. Sandridge, Chris A. Clowdsley, Martha S. Blattnig, Steve R. BE Taylor, EW Cardimona, DA TI OLTARIS: An Efficient Web-Based Tool for Analyzing Materials Exposed to Space Radiation SO NANOPHOTONICS AND MACROPHOTONICS FOR SPACE ENVIRONMENTS V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Nanophotonics and Macrophotonics for Space Environments V (NMSE) CY AUG 22-23, 2011 CL San Diego, CA SP SPIE DE OLTARIS; HZETRN; space radiation; particle transport; radiation exposure ID ADULT VOXEL PHANTOM; PROTECTION DOSIMETRY; HZETRN AB The near-Earth space radiation environment includes energetic galactic cosmic rays (GCR), high intensity proton and electron belts, and the potential for solar particle events (SPE). These sources may penetrate shielding materials and deposit significant energy in sensitive electronic devices on board spacecraft and satellites. Material and design optimization methods may be used to reduce the exposure and extend the operational lifetime of individual components and systems. Since laboratory experiments are expensive and may not cover the range of particles and energies relevant for space applications, such optimization may be done computationally with efficient algorithms that include the various constraints placed on the component, system, or mission. In the present work, the web-based tool OLTARIS (On-Line Tool for the Assessment of Radiation in Space) is presented, and the applicability of the tool for rapidly analyzing exposure levels within either complicated shielding geometries or user-defined material slabs exposed to space radiation is demonstrated. An example approach for material optimization is also presented. Slabs of various advanced multifunctional materials are defined and exposed to several space radiation environments. The materials and thicknesses defining each layer in the slab are then systematically adjusted to arrive at an optimal slab configuration. C1 [Slaba, Tony C.; Thibeault, Sheila A.; Sandridge, Chris A.; Clowdsley, Martha S.; Blattnig, Steve R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Slaba, TC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 17 TC 0 Z9 0 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-774-2 J9 PROC SPIE PY 2011 VL 8164 AR 81640G DI 10.1117/12.898960 PG 8 WC Astronomy & Astrophysics; Nanoscience & Nanotechnology; Optics SC Astronomy & Astrophysics; Science & Technology - Other Topics; Optics GA BXZ24 UT WOS:000297674100015 ER PT S AU Thomes, WJ Ott, MN Chuska, RF Switzer, RC Blair, DE AF Thomes, W. Joe, Jr. Ott, Melanie N. Chuska, Richard F. Switzer, Robert C. Blair, Diana E. BE Taylor, EW Cardimona, DA TI Fiber optic cables for transmission of high-power laser pulses SO NANOPHOTONICS AND MACROPHOTONICS FOR SPACE ENVIRONMENTS V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Nanophotonics and Macrophotonics for Space Environments V (NMSE) CY AUG 22-23, 2011 CL San Diego, CA SP SPIE DE Laser polishing; fiber optics; pulsed laser; fiber injection; fiber threshold; optical damage ID BEAM AB High power pulsed lasers are commonly deployed in harsh environments, like space flight and military missions, for a variety of systems such as LIDAR, optical communications over long distances, or optical firing of explosives. Fiber coupling of the laser pulse from the laser to where it is needed can often save size, reduce weight, and lead to a more robust and reliable system. Typical fiber optic termination procedures are not sufficient for injection of these high power laser pulses without catastrophic damage to the fiber endface. In the current study, we will review the causes of fiber damage during high power injection and discuss methods used to avoid these issues to permit fiber use with high reliability in these applications. A brief review of the design considerations for high peak power laser pulse injection will be presented to familiarize the audience with all the areas that need to be considered during the design phase. The majority of this paper focuses on the proper fiber polishing methods for high power use with an emphasis on laser polishing of the fibers. Results from recently build fibers will be shown to demonstrate the techniques. C1 [Thomes, W. Joe, Jr.; Ott, Melanie N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Thomes, WJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Joe.Thomes@nasa.gov NR 10 TC 1 Z9 1 U1 1 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-774-2 J9 PROC SPIE PY 2011 VL 8164 AR 81640F DI 10.1117/12.895964 PG 9 WC Astronomy & Astrophysics; Nanoscience & Nanotechnology; Optics SC Astronomy & Astrophysics; Science & Technology - Other Topics; Optics GA BXZ24 UT WOS:000297674100014 ER PT S AU Thomes, WJ Cavanaugh, JF Ott, MN AF Thomes, W. Joe, Jr. Cavanaugh, John F. Ott, Melanie N. BE Taylor, EW Cardimona, DA TI Proton radiation testing of laser optical components for NASA Jupiter Europa Orbiter Mission SO NANOPHOTONICS AND MACROPHOTONICS FOR SPACE ENVIRONMENTS V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Nanophotonics and Macrophotonics for Space Environments V (NMSE) CY AUG 22-23, 2011 CL San Diego, CA SP SPIE DE Laser optics; optical components; radiation effects; proton; Europa; Jupiter AB The Jupiter Europa Orbiter (JEO) is NASA's element of the joint Europa Jupiter System Mission (EJSM). Based on current trajectories, the spacecraft will spend a significant amount of time in the Jovian radiation belts. Therefore, research endeavors are underway to study the radiation effects on the various parts and components needed to implement the instruments. Data from these studies will be used for component selection and system design to ensure reliable operation throughout the mission duration. The radiation environment en route to Jupiter is nothing new for NASA designed systems, however, the long durations orbiting Jupiter and Europa present new challenges for radiation exposure. High-energy trapped electrons and protons at Jupiter dominate the expected radiation environment. Therefore, most of the initial component level radiation testing is being conducted with proton exposure. In this paper we will present in-situ monitoring of the optical transmission of various laser optical components during proton irradiation. Radiation induced optical attenuation of some components is less than would be expected, based on the authors experiences, and is attributed to the interaction of the protons with the materials. The results are an encouraging first step in screening these optical materials for spaceflight in a high radiation environment. C1 [Thomes, W. Joe, Jr.; Cavanaugh, John F.; Ott, Melanie N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Thomes, WJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Joe.Thomes@nasa.gov NR 3 TC 0 Z9 0 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-774-2 J9 PROC SPIE PY 2011 VL 8164 AR 816403 DI 10.1117/12.895816 PG 10 WC Astronomy & Astrophysics; Nanoscience & Nanotechnology; Optics SC Astronomy & Astrophysics; Science & Technology - Other Topics; Optics GA BXZ24 UT WOS:000297674100003 ER PT J AU Guan, DS Jeevarajan, JA Wang, Y AF Guan, Dongsheng Jeevarajan, Judith A. Wang, Ying TI Enhanced cycleability of LiMn2O4 cathodes by atomic layer deposition of nanosized-thin Al2O3 coatings SO NANOSCALE LA English DT Article ID LITHIUM-ION BATTERIES; SURFACE MODIFICATION; POSITIVE ELECTRODE; CYCLING STABILITY; SPINEL; LICOO2; CHEMISTRY AB This report is the first effort to use atomic layer deposition method for deposition of nanosized-thin and highly conformal Al2O3 coatings onto LiMn2O4 cathodes with precise thickness-control at atomic scale. The coated cathodes exhibit significantly enhanced cycleability than bare cathodes, as the dense ALD coating protects the cathode material from severe dissolution. C1 [Guan, Dongsheng; Wang, Ying] Louisiana State Univ, Dept Mech Engn, Baton Rouge, LA 70803 USA. [Jeevarajan, Judith A.] NASA, Lyndon B Johnson Space Ctr, Battery Grp Lead Safety & Adv Technol, Houston, TX 77058 USA. RP Wang, Y (reprint author), Louisiana State Univ, Dept Mech Engn, Baton Rouge, LA 70803 USA. EM ywang@lsu.edu RI Wang, Ying/J-3286-2012; Guan, Dongsheng/M-5334-2013 OI Guan, Dongsheng/0000-0002-1695-076X FU LSU Junior Faculty; NASA-LABOR; NSF-LABOR; LSU Graduate School FX This work is supported by LSU Junior Faculty Start-up Funds, DART2 Funds sponsored by NASA-LABOR, and PFund sponsored by NSF-LABOR. D.S. Guan acknowledges LSU Graduate School Supplementary Award. The authors would like to thank Dr Shengming Guo's group for their assistance in pressing electrodes. The authors also acknowledge Materials Characterization Center at LSU for using XRD, XPS and SEM. NR 30 TC 78 Z9 78 U1 5 U2 99 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 2040-3364 J9 NANOSCALE JI Nanoscale PY 2011 VL 3 IS 4 BP 1465 EP 1469 DI 10.1039/c0nr00939c PG 5 WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 747FY UT WOS:000289306900015 PM 21327283 ER PT J AU Kar, A Low, KB Oye, M Stroscio, MA Dutta, M Nicholls, A Meyyappan, M AF Kar, Ayan Low, Ke-Bin Oye, Michael Stroscio, Michael A. Dutta, Mitra Nicholls, Alan Meyyappan, M. TI Investigation of Nucleation Mechanism and Tapering Observed in ZnO Nanowire Growth by Carbothermal Reduction Technique SO NANOSCALE RESEARCH LETTERS LA English DT Article ID SILICON NANOWIRES; SURFACES; MODEL; GOLD AB ZnO nanowire nucleation mechanism and initial stages of nanowire growth using the carbothermal reduction technique are studied confirming the involvement of the catalyst at the tip in the growth process. Role of the Au catalyst is further confirmed when the tapering observed in the nanowires can be explained by the change in the shape of the catalyst causing a variation of the contact area at the liquid-solid interface of the nanowires. The rate of decrease in nanowire diameter with length on the average is found to be 0.36 nm/s and this rate is larger near the base. Variation in the ZnO nanowire diameter with length is further explained on the basis of the rate at which Zn atoms are supplied as well as the droplet stability at the high flow rates and temperature. Further, saw-tooth faceting is noticed in tapered nanowires, and the formation is analyzed crystallographically. C1 [Kar, Ayan; Stroscio, Michael A.; Dutta, Mitra] Univ Illinois, Dept Elect & Comp Engn, Chicago, IL 60607 USA. [Stroscio, Michael A.; Dutta, Mitra] Univ Illinois, Dept Phys, Chicago, IL 60607 USA. [Stroscio, Michael A.] Univ Illinois, Dept Bioengn, Chicago, IL 60607 USA. [Low, Ke-Bin; Nicholls, Alan] Univ Illinois, Res Resources Ctr, Chicago, IL 60607 USA. [Oye, Michael; Meyyappan, M.] NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kar, A (reprint author), Univ Illinois, Dept Elect & Comp Engn, Chicago, IL 60607 USA. EM akar2@uic.edu FU Korea Science and Engineering Foundation from the Ministry of Education, Science, and Technology FX A. K would like to thank Dr. Shadi Dayeh and Dr. Ranadeep Bhowmick for helpful discussions and suggestions. We thank Professor Sreeram Vaddiraju for his insightful comments and help with the manuscript. Part of this work was supported by the WCU-ITCE Program at Postech funded by the Korea Science and Engineering Foundation from the Ministry of Education, Science, and Technology. NR 21 TC 10 Z9 10 U1 0 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1931-7573 J9 NANOSCALE RES LETT JI Nanoscale Res. Lett. PY 2011 VL 6 AR 3 DI 10.1007/s11671-010-9738-3 PG 9 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 744OP UT WOS:000289104200003 PM 27502628 ER PT B AU Kaul, AB Coles, JB Megerian, KG Green, RO Pagano, T Bandaru, PR Dokmeci, MR AF Kaul, Anupama B. Coles, James B. Megerian, Krikor G. Green, Robert O. Pagano, Thomas Bandaru, Prabhakar R. Dokmeci, Mehmet R. BE Laudon, M Romanowicz, B TI High-Efficiency Optical Absorbers Derived from Carbon Nanostructures SO NANOTECHNOLOGY 2011: ELECTRONICS, DEVICES, FABRICATION, MEMS, FLUIDICS AND COMPUTATIONAL, NSTI-NANOTECH 2011, VOL 2 LA English DT Proceedings Paper CT NSTI Nanotechnology Conference and Expo CY JUN 13-16, 2011 CL Boston, MA SP Clean Technol & Sustainable Ind Org, European Patent Off, Greenberg Traurig, Innovat & Mat Sci Inst, Jackson Walker LLP, Linde Nanomaterials, Lockheed Martin, Nano Sci & Technol Inst, Nano Tech Japan, NanoEurope Fair & Conf, Nanpolis Suzhou, Suzhou Nanotech Co Ltd, Natl Inst Standards & Technol, Ctr Nanoscale Sci & Technol, Fraunhofer, Res Germany, TechConnect, Technol Innovat Program, Canadian Trade Commiss Serv, Italian Trade Commiss DE carbon nanomaterials; optical absorbers; nanoabsorbers; MWCNTs; PECVD ID PHOTOVOLTAIC APPLICATIONS; NANOWIRE ARRAYS; NANOTUBES AB Optical absorbers based on vertically aligned multi walled carbon nanotubes (MWCNTs), synthesized using electric-field assisted growth, are described here that show an ultra-low reflectance, 100X lower compared to the benchmark, a diffuse metal black - Au-black - from wavelength lambda similar to 350 nm - 2500 mn. The reflectance of the MWCNT arrays was measured to be as low as 0.02 % at 2 gm. The choice of the starting substrate was deemed to be particularly important in order to synthesize a high-areal density of the MWCNTs using the plasma-based chemical vapor deposition (CVD) process which directly impacts the optical absorption efficiency of the nanoabsorbers. Such high efficiency absorbers are particularly attractive for radiometry, as well as energy harnessing applications. C1 [Kaul, Anupama B.; Coles, James B.; Megerian, Krikor G.; Green, Robert O.; Pagano, Thomas] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Bandaru, Prabhakar R.] Univ Calif San Diego, Jacobs Sch Engn, La Jolla, CA 92093 USA. [Dokmeci, Mehmet R.] Northeastern Univ, Dept Elect & Comp Engn, Boston, MA 02115 USA. RP Kaul, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration; internal Research and Technology Development (RTD) program [01STCR, R.10.021.067] FX We would like to thank Robert Kowalczyk for maintenance of the dc PECVD growth chamber. 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 (01STCR, R.10.021.067). NR 16 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-7139-3 PY 2011 BP 104 EP 107 PG 4 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA BG9XB UT WOS:000394060800027 ER PT B AU Kaul, AB Khan, AR Megerian, K Bagge, L Epp, L Dokmeci, MR AF Kaul, Anupama B. Khan, Abdur R. Megerian, Krikor Bagge, Leif Epp, Larry Dokmeci, Mehmet R. BE Laudon, M Romanowicz, B TI AC and DC Applications of Three-Dimensional Nano-electro-Mechanical-Systems SO NANOTECHNOLOGY 2011: ELECTRONICS, DEVICES, FABRICATION, MEMS, FLUIDICS AND COMPUTATIONAL, NSTI-NANOTECH 2011, VOL 2 LA English DT Proceedings Paper CT NSTI Nanotechnology Conference and Expo CY JUN 13-16, 2011 CL Boston, MA SP Clean Technol & Sustainable Ind Org, European Patent Off, Greenberg Traurig, Innovat & Mat Sci Inst, Jackson Walker LLP, Linde Nanomaterials, Lockheed Martin, Nano Sci & Technol Inst, Nano Tech Japan, NanoEurope Fair & Conf, Nanpolis Suzhou, Suzhou Nanotech Co Ltd, Natl Inst Standards & Technol, Ctr Nanoscale Sci & Technol, Fraunhofer, Res Germany, TechConnect, Technol Innovat Program, Canadian Trade Commiss Serv, Italian Trade Commiss DE carbon nanomaterials; CNFs; nanoelectronics; NEMs; resonators; nanorelays ID CARBON; SWITCHES AB In this paper, we describe the implementation of carbon nanofibers (CNFs), synthesized using dc plasma enhanced chemical vapor deposition (PECVD), to three-dimensional (3D) dc nanorelays as well as to AC resonator applications. Such nano-electro-mechanical (NEM) structures are under consideration for NASA's extreme environment electronics applications and the 3D architecture promises to increase integration densities by 10X compared to two-dimensional (2D) planar NEMS. Here we describe the fabrication, electrical characterization and modeling results of these vertically oriented CNFs for such 3D NEMS applications. C1 [Kaul, Anupama B.; Khan, Abdur R.; Megerian, Krikor; Bagge, Leif; Epp, Larry] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Khan, Abdur R.] Univ Southern Calif, Keck Sch Med, Los Angeles, CA 90089 USA. [Bagge, Leif] Univ Texas Austin, Dept Elect & Comp Engn, Austin, TX 78712 USA. [Dokmeci, Mehmet R.] Northeastern Univ, Dept Elect & Comp Engn, Boston, MA 02115 USA. RP Kaul, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU internal Research and Technology Development (RTD) program FX We would like to thank Robert Kowalczyk, Choonsup Lee for technical assistance and 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 9 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-7139-3 PY 2011 BP 290 EP 293 PG 4 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA BG9XB UT WOS:000394060800074 ER PT B AU Wilson, WC Atkinson, GM AF Wilson, W. C. Atkinson, G. M. BE Laudon, M Romanowicz, B TI Space Applications for Wireless Sensors SO NANOTECHNOLOGY 2011: ELECTRONICS, DEVICES, FABRICATION, MEMS, FLUIDICS AND COMPUTATIONAL, NSTI-NANOTECH 2011, VOL 2 LA English DT Proceedings Paper CT NSTI Nanotechnology Conference and Expo CY JUN 13-16, 2011 CL Boston, MA SP Clean Technol & Sustainable Ind Org, European Patent Off, Greenberg Traurig, Innovat & Mat Sci Inst, Jackson Walker LLP, Linde Nanomaterials, Lockheed Martin, Nano Sci & Technol Inst, Nano Tech Japan, NanoEurope Fair & Conf, Nanpolis Suzhou, Suzhou Nanotech Co Ltd, Natl Inst Standards & Technol, Ctr Nanoscale Sci & Technol, Fraunhofer, Res Germany, TechConnect, Technol Innovat Program, Canadian Trade Commiss Serv, Italian Trade Commiss DE wireless sensors; spacecraft; sensors networks AB From ground tests to operations on orbit and on the Moon, many space applications could benefit from small, passive, wireless sensors. Eliminating wires in spacecraft could reduce launch costs through the reduction of mass and lead to reduced fabrication costs. Development of wireless Vehicle Health Monitoring Systems (VHMS) will enable more sensors and increase safety. It is for these reasons that NASA is investigating the use of wireless technology for a variety of spacecraft applications. This paper will present a survey of opportunities for universities, industry, and other governmental agencies to partner in developing new wireless sensors to address the future sensing needs. C1 [Wilson, W. C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Atkinson, G. M.] Virginia Commonwealth Univ, Richmond, VA USA. RP Wilson, WC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM w.c.wilson@larc.nasa.gov; gmatkins@vcu.edu NR 21 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-7139-3 PY 2011 BP 298 EP 301 PG 4 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA BG9XB UT WOS:000394060800076 ER PT S AU Herencia-Zapana, H Hagen, G Narkawicz, A AF Herencia-Zapana, Heber Hagen, George Narkawicz, Anthony BE Bobaru, M Havelund, K Holzmann, GJ Joshi, R TI Formalizing Probabilistic Safety Claims SO NASA FORMAL METHODS SE Lecture Notes in Computer Science LA English DT Proceedings Paper CT 3rd NASA Formal Methods Symposium CY APR 18-20, 2011 CL Pasadena, CA AB A safety claim for a system is a statement that the system, which is subject to hazardous conditions, satisfies a given set of properties. Following work by John Rushby and Bev Littlewood, this paper presents a mathematical framework that can be used to state and formally prove probabilistic safety claims. It also enables hazardous conditions, their uncertainties, and their interactions to be integrated into the safety claim. This framework provides a formal description of the probabilistic composition of an arbitrary number of hazardous conditions and their effects on system behavior. An example is given of a probabilistic safety claim for a conflict detection algorithm for aircraft in a 2D airspace. The motivation for developing this mathematical framework is that it can be used in an automated theorem prover to formally verify safety claims. C1 [Herencia-Zapana, Heber] Natl Inst Aerosp, Hampton, VA 23666 USA. [Hagen, George; Narkawicz, Anthony] NASA, Langley Res Ctr, Hampton, VA USA. RP Herencia-Zapana, H (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. FU National Aeronautics and Space Administration under NASA [NCC-1-02043] FX This work was supported in part by the National Aeronautics and Space Administration under NASA Cooperative Agreement NCC-1-02043 NR 10 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 978-3-642-20397-8 J9 LECT NOTES COMPUT SC PY 2011 VL 6617 BP 162 EP + PG 2 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BZL63 UT WOS:000301947700013 ER PT J AU Bahl, J Lau, MCY Smith, GJD Vijaykrishna, D Cary, SC Lacap, DC Lee, CK Papke, RT Warren-Rhodes, KA Wong, FKY McKay, CP Pointing, SB AF Bahl, Justin Lau, Maggie C. Y. Smith, Gavin J. D. Vijaykrishna, Dhanasekaran Cary, S. Craig Lacap, Donnabella C. Lee, Charles K. Papke, R. Thane Warren-Rhodes, Kimberley A. Wong, Fiona K. Y. McKay, Christopher P. Pointing, Stephen B. TI Ancient origins determine global biogeography of hot and cold desert cyanobacteria SO NATURE COMMUNICATIONS LA English DT Article ID RIBOSOMAL-RNA GENES; MICROBIAL DIVERSITY; SPECIES RICHNESS; AGE; CHROOCOCCIDIOPSIS; AUSTRALIA; LANDFORMS; INFERENCE; ECOLOGY; ARIDITY AB Factors governing large-scale spatio-temporal distribution of microorganisms remain unresolved, yet are pivotal to understanding ecosystem value and function. Molecular genetic analyses have focused on the influence of niche and neutral processes in determining spatial patterns without considering the temporal scale. Here, we use temporal phylogenetic analysis calibrated using microfossil data for a globally sampled desert cyanobacterium, Chroococcidiopsis, to investigate spatio-temporal patterns in microbial biogeography and evolution. Multilocus phylogenetic associations were dependent on contemporary climate with no evidence for distance-related patterns. Massively parallel pyrosequencing of environmental samples confirmed that Chroococcidiopsis variants were specific to either hot or cold deserts. Temporally scaled phylogenetic analyses showed no evidence of recent inter-regional gene flow, indicating populations have not shared common ancestry since before the formation of modern continents. These results indicate that global distribution of desert cyanobacteria has not resulted from widespread contemporary dispersal but is an ancient evolutionary legacy. This highlights the importance of considering temporal scales in microbial biogeography. C1 [Lau, Maggie C. Y.; Lacap, Donnabella C.; Wong, Fiona K. Y.; Pointing, Stephen B.] Univ Hong Kong, Sch Biol Sci, Hong Kong, Hong Kong, Peoples R China. [Bahl, Justin; Smith, Gavin J. D.; Vijaykrishna, Dhanasekaran] Duke NUS Grad Med Sch, Singapore 169857, Singapore. [Cary, S. Craig; Lee, Charles K.] Univ Waikato, Dept Biol Sci, Hamilton, New Zealand. [Papke, R. Thane] Univ Connecticut, Dept Mol & Cell Biol, Storrs, CT 06269 USA. [Warren-Rhodes, Kimberley A.; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Pointing, SB (reprint author), Univ Hong Kong, Sch Biol Sci, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China. EM pointing@hku.hk RI Bahl, Justin/A-4728-2011; Vijaykrishna, Dhanasekaran/D-1011-2010; OI Bahl, Justin/0000-0001-7572-4300; Smith, Gavin JD/0000-0001-5031-468X; Vijaykrishna, Dhanasekaran/0000-0003-3293-6279; Lee, Charles/0000-0002-6562-4733; Cary, Stephen/0000-0002-2876-2387 FU NASA; Hong Kong Research Grants Council [HKU7733/08 HKU7763/10]; Agency for Science, Technology and Research; Ministry of Health, Singapore FX We thank the following for critical discussion on earlier versions of this work: Yuki Chan, Don Cowan, Alfonso Davilla, Alex Heri, Wayne Pollard, Mark Stevens. This research was supported by the NASA Astrobiology Science and Technology for Exploring Planets (ASTEP) Programme and the Hong Kong Research Grants Council (Grant numbers HKU7733/08 HKU7763/10). J.B., G.J.D.S. and D. V. are supported by the Duke-NUS Signature Research Program funded by the Agency for Science, Technology and Research, and the Ministry of Health, Singapore. NR 49 TC 78 Z9 79 U1 3 U2 42 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD JAN PY 2011 VL 2 AR 163 DI 10.1038/ncomms1167 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 732YN UT WOS:000288225700013 ER PT J AU Wojtecki, RJ Meador, MA Rowan, SJ AF Wojtecki, Rudy J. Meador, Michael A. Rowan, Stuart J. TI Using the dynamic bond to access macroscopically responsive structurally dynamic polymers SO NATURE MATERIALS LA English DT Review ID CROSS-LINKED POLYMERS; SEA-CUCUMBER DERMIS; SELF-HEALING MATERIALS; SOL-GEL TRANSITION; STAR-LIKE NANOGELS; COVALENT POLYMERS; COMBINATORIAL CHEMISTRY; SUPRAMOLECULAR POLYMERS; BIOMIMETIC MATERIALS; DISULFIDE EXCHANGE AB New materials that have the ability to reversibly adapt to their environment and possess a wide range of responses ranging from self-healing to mechanical work are continually emerging. These adaptive systems have the potential to revolutionize technologies such as sensors and actuators, as well as numerous biomedical applications. We will describe the emergence of a new trend in the design of adaptive materials that involves the use of reversible chemistry (both non-covalent and covalent) to programme a response that originates at the most fundamental (molecular) level. Materials that make use of this approach - structurally dynamic polymers - produce macroscopic responses from a change in the material's molecular architecture (that is, the rearrangement or reorganization of the polymer components, or polymeric aggregates). This design approach requires careful selection of the reversible/dynamic bond used in the construction of the material to control its environmental responsiveness. C1 [Wojtecki, Rudy J.; Rowan, Stuart J.] Case Western Reserve Univ, Dept Macromol Sci & Engn, Cleveland, OH 44106 USA. [Meador, Michael A.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Wojtecki, RJ (reprint author), Case Western Reserve Univ, Dept Macromol Sci & Engn, 2100 Adelbert Rd, Cleveland, OH 44106 USA. EM stuart.rowan@case.edu FU National Science Foundation [DMR-0602869, CHE-0704026, CBET-0828155]; US Army Research Office [DAAD19-03-1-0208, W911NF-06-1-0414]; Subsonics Fixed Wing Project on the Fundamental Aeronautics Program; NASA [NNX08AY62H] FX The authors thank the National Science Foundation (DMR-0602869, CHE-0704026, and CBET-0828155), the US Army Research Office (DAAD19-03-1-0208 and W911NF-06-1-0414) for funding research in this area. M.A.M. acknowledges support from the Subsonics Fixed Wing Project on the Fundamental Aeronautics Program. R.J.W. acknowledges support through the NASA Graduate Student Research Program (NNX08AY62H). NR 111 TC 456 Z9 462 U1 64 U2 667 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1476-1122 EI 1476-4660 J9 NAT MATER JI Nat. Mater. PD JAN PY 2011 VL 10 IS 1 BP 14 EP 27 DI 10.1038/NMAT2891 PG 14 WC Chemistry, Physical; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA 694YZ UT WOS:000285339100015 PM 21157495 ER PT J AU Werlin, R Priester, JH Mielke, RE Kramer, S Jackson, S Stoimenov, PK Stucky, GD Cherr, GN Orias, E Holden, PA AF Werlin, R. Priester, J. H. Mielke, R. E. Kraemer, S. Jackson, S. Stoimenov, P. K. Stucky, G. D. Cherr, G. N. Orias, E. Holden, P. A. TI Biomagnification of cadmium selenide quantum dots in a simple experimental microbial food chain SO NATURE NANOTECHNOLOGY LA English DT Article ID TROPHIC TRANSFER; FRESH-WATER; PSEUDOMONAS-AERUGINOSA; BACTERIA; NANOPARTICLES; PREDATION; DIGESTION; TOXICITY; PROTOZOA; PROKARYOTES AB Previous studies have shown that engineered nanomaterials can be transferred from prey to predator, but the ecological impacts of this are mostly unknown. In particular, it is not known if these materials can be biomagnified-a process in which higher concentrations of materials accumulate in organisms higher up in the food chain. Here, we show that bare CdSe quantum dots that have accumulated in Pseudomonas aeruginosa bacteria can be transferred to and biomagnified in the Tetrahymena thermophila protozoa that prey on the bacteria. Cadmium concentrations in the protozoa predator were approximately five times higher than their bacterial prey. Quantum-dot-treated bacteria were differentially toxic to the protozoa, in that they inhibited their own digestion in the protozoan food vacuoles. Because the protozoa did not lyse, largely intact quantum dots remain available to higher trophic levels. The observed biomagnification from bacterial prey is significant because bacteria are at the base of environmental food webs. Our findings illustrate the potential for biomagnification as an ecological impact of nanomaterials. C1 [Werlin, R.; Orias, E.] Univ Calif Santa Barbara, Dept Mol Cellular & Dev Biol, Santa Barbara, CA 93106 USA. [Werlin, R.; Priester, J. H.; Mielke, R. E.; Jackson, S.; Stucky, G. D.; Cherr, G. N.; Holden, P. A.] Univ Calif Santa Barbara, UC CEIN, Santa Barbara, CA 93106 USA. [Priester, J. H.; Mielke, R. E.; Holden, P. A.] Univ Calif Santa Barbara, Donald Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA. [Priester, J. H.; Mielke, R. E.; Holden, P. A.] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA. [Mielke, R. E.] NASA, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA. [Kraemer, S.; Stucky, G. D.] Univ Calif Santa Barbara, Dept Mat, Santa Barbara, CA 93106 USA. [Jackson, S.; Cherr, G. N.] Univ Calif Davis, Dept Environm Toxicol, Bodega Marine Lab, Bodega Bay, CA 94923 USA. [Jackson, S.; Cherr, G. N.] Univ Calif Davis, Dept Nutr, Bodega Marine Lab, Bodega Bay, CA 94923 USA. [Stoimenov, P. K.; Stucky, G. D.] Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA. RP Werlin, R (reprint author), Univ Calif Santa Barbara, Dept Mol Cellular & Dev Biol, Santa Barbara, CA 93106 USA. EM holden@bren.ucsb.edu RI Kraemer, Stephan/I-3186-2014 OI Kraemer, Stephan/0000-0003-0577-7444 FU US Environmental Protection Agency [R833323]; National Science Foundation [BES-9977772, DBI-0216480, DMR05-20415]; Environmental Protection Agency [DBI-0830117]; National Center for Research Resources of the National Institutes of Health [R01-RR009231] FX This research was primarily funded by US Environmental Protection Agency Science To Achieve Results (STAR) award no. R833323 (to P.A.H. and G.D.S.), and by the National Science Foundation and the Environmental Protection Agency under cooperative agreement no. DBI-0830117 (to P.A.H., G.N.C. and G.D.S.). Any opinions, findings and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of either the National Science Foundation or the Environmental Protection Agency. This work has not been subjected to Environmental Protection Agency review and no official endorsement should be inferred. Environmental scanning and scanning transmission electron microscopy were partly performed in the Micro-Environmental Imaging and Analysis Facility at University of California Santa Barbara (www.bren.ucsb.edu/facilities/MEIAF/) under National Science Foundation awards nos BES-9977772 and DBI-0216480. Transmission electron microscopy was partly performed in the University of California Santa Barbara Materials Research Laboratory Central Facilities supported by the Materials Research Science and Engineering Centers Program of the National Science Foundation under award no. DMR05-20415. The T. thermophila portion of the work was partially supported by grant no. R01-RR009231 from the National Center for Research Resources of the National Institutes of Health (to E.O.). The authors gratefully acknowledge critical comments on the manuscript by T. Klanjscek. Thanks also go to anonymous reviewers for valuable suggestions that led to significant improvement of the manuscript. NR 45 TC 96 Z9 96 U1 7 U2 77 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1748-3387 J9 NAT NANOTECHNOL JI Nat. Nanotechnol. PD JAN PY 2011 VL 6 IS 1 BP 65 EP 71 DI 10.1038/NNANO.2010.251 PG 7 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA 698EB UT WOS:000285574000015 PM 21170041 ER PT S AU Prasad, NS Roychoudhuri, C AF Prasad, Narasimha S. Roychoudhuri, Chandra BE Roychoudhuri, C Khrennikov, AY Kracklauer, AF TI Visualizing the mode evolution process in passive and active cavities based on the NIW-Principle SO NATURE OF LIGHT: WHAT ARE PHOTONS IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on The Nature of Light - What are Photons IV CY AUG 22-25, 2011 CL San Diego, CA SP SPIE, Gen Resonance, LLC AB This paper will present results of computer models depicting the evolution of diffractive processes through passive and active cavities (traditional stable resonator and single mode fiber) as the number of passes (or the length of propagation) increases. The objective is to visualize how the spatially stable eigen-modes evolve with propagation. Our core assumptions are the validity of the Huygens-Fresnel hypothesis of secondary wavelets and the recently articulated Non-Interaction of Waves (NIW) principle in this conference series. The NIW-principle implies that even the diffracted secondary wavelets propagate conjointly but without re-arranging their spatial energy distribution unless one inserts some interacting material medium within the diffracting beam. Accordingly, we anticipate that the evolution of the measurable energy distribution in the diffraction pattern will be different in the presence of gain medium whose gain profile varies in the direction orthogonal to the cavity axis. We also anticipate that a cavity with high gain profile will generate the stable spatial eigen-mode with a fewer number of passes through the cavity than with lower gain, or no gain. We will also present the mode evolution process when the seed signal is a pulse of length that is shorter than that of the cavity. We believe this paper will provide useful insights to the students who are introduced to the concept of spatially well defined Gaussian laser modes for the first time. C1 [Prasad, Narasimha S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Prasad, NS (reprint author), NASA, Langley Res Ctr, 5 N Dryden St, Hampton, VA 23681 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8731-5 J9 PROC SPIE PY 2011 VL 8121 AR 81211D DI 10.1117/12.895167 PG 7 WC Optics; Physics, Applied SC Optics; Physics GA BBQ57 UT WOS:000307871400045 ER PT S AU Prasad, NS Roychoudhuri, C AF Prasad, Narasimha S. Roychoudhuri, Chandra BE Roychoudhuri, C Khrennikov, AY Kracklauer, AF TI Appreciating the principle of Non-Interaction of waves (NIW-principle) by modeling Talbot diffraction patterns at different planes SO NATURE OF LIGHT: WHAT ARE PHOTONS IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on The Nature of Light - What are Photons IV CY AUG 22-25, 2011 CL San Diego, CA SP SPIE, Gen Resonance, LLC DE Talbot Diffraction; Non-Interaction of Waves (NIW) Principle AB We present an approach to demonstrate the Non-Interaction of Waves (NIW)-principle by showing that dark fringes in the near-field Talbot diffraction patterns are not devoid of energy. We believe that a detector is simply incapable of absorbing any energy at the dark fringe locations simply because the resultant of the induced stimulations on a local detecting dipole due to all the E-vectors is zero. The joint stimulation is strongest at the bright fringe locations. The amplitude (& hence potentially detectable energy) flow through the "dark fringe locations" is demonstrated by obstructing the "bright fringe" locations at the half-Talbot plane with an identical grating that generated this diffraction image. Then, by propagating the transmitted complex amplitudes through the dark fringes, we would like to show that the Talbot plane can still receive more energy than that could have been recorded out of those same dark fringe locations at the half Talbot plane. C1 [Prasad, Narasimha S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Prasad, NS (reprint author), NASA, Langley Res Ctr, 5 N Dryden St, Hampton, VA 23681 USA. NR 3 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8731-5 J9 PROC SPIE PY 2011 VL 8121 AR 81211B DI 10.1117/12.894044 PG 8 WC Optics; Physics, Applied SC Optics; Physics GA BBQ57 UT WOS:000307871400044 ER PT J AU Kateb, B Chiu, K Black, KL Yamamoto, V Khalsa, B Ljubimova, JY Ding, H Patil, R Portilla-Arias, JA Modo, M Moore, DF Farahani, K Okun, MS Prakash, N Neman, J Ahdoot, D Grundfest, W Nikzad, S Heiss, JD AF Kateb, Babak Chiu, Katherine Black, Keith L. Yamamoto, Vicky Khalsa, Bhavraj Ljubimova, Julia Y. Ding, Hui Patil, Rameshwar Portilla-Arias, Jose Antonio Modo, Mike Moore, David F. Farahani, Keyvan Okun, Michael S. Prakash, Neal Neman, Josh Ahdoot, Daniel Grundfest, Warren Nikzad, Shouleh Heiss, John D. TI Nanoplatforms for constructing new approaches to cancer treatment, imaging, and drug delivery: What should be the policy? SO NEUROIMAGE LA English DT Article DE Nanoplatforms; Nanotechnology; Image-guided therapy; Nanomedicine; Nanoneurosurgery; Nanostructures; Contrast agents; Nanoparticles; Nanotechnology policy; Nano-radiology; Nano-neuroscience; Nano-neurology ID NEPHROGENIC SYSTEMIC FIBROSIS; IRON-OXIDE NANOPARTICLES; FUNCTIONALIZED CARBON NANOTUBES; MAGNETIC-RESONANCE TRACKING; BLOOD-BRAIN-BARRIER; MRI CONTRAST AGENTS; PLURONIC((R)) BLOCK-COPOLYMERS; SEMICONDUCTOR QUANTUM DOTS; VX-2 RABBIT TUMORS; SIALYL-LEWIS-X AB Nanotechnology is the design and assembly of submicroscopic devices called nanoparticles, which are 1-100 nm in diameter. Nanomedicine is the application of nanotechnology for the diagnosis and treatment of human disease. Disease-specific receptors on the surface of cells provide useful targets for nanoparticles. Because nanoparticles can be engineered from components that (1) recognize disease at the cellular level, (2) are visible on imaging studies, and (3) deliver therapeutic compounds, nanotechnology is well suited for the diagnosis and treatment of a variety of diseases. Nanotechnology will enable earlier detection and treatment of diseases that are best treated in their initial stages, such as cancer. Advances in nanotechnology will also spur the discovery of new methods for delivery of therapeutic compounds, including genes and proteins, to diseased tissue. A myriad of nanostructured drugs with effective site-targeting can be developed by combining a diverse selection of targeting, diagnostic, and therapeutic components. Incorporating immune target specificity with nanostructures introduces a new type of treatment modality, nano-immunochemotherapy, for patients with cancer. In this review, we will discuss the development and potential applications of nanoscale platforms in medical diagnosis and treatment. To impact the care of patients with neurological diseases, advances in nanotechnology will require accelerated translation to the fields of brain mapping, CNS imaging, and nanoneurosurgery. Advances in nanoplatform, nano-imaging, and nano-drug delivery will drive the future development of nanomedicine, personalized medicine, and targeted therapy. We believe that the formation of a science, technology, medicine law-healthcare policy (STML) hub/center, which encourages collaboration among universities, medical centers, US government, industry, patient advocacy groups, charitable foundations, and philanthropists, could significantly facilitate such advancements and contribute to the translation of nanotechnology across medical disciplines. (C) 2010 Elsevier Inc. All rights reserved. C1 [Kateb, Babak; Moore, David F.; Okun, Michael S.; Prakash, Neal; Grundfest, Warren; Nikzad, Shouleh; Heiss, John D.] IBMISPS, W Hollywood, CA 90046 USA. [Kateb, Babak; Ahdoot, Daniel; Grundfest, Warren; Nikzad, Shouleh] Brain Mapping Fdn, W Hollywood, CA 90046 USA. [Kateb, Babak] Univ So Calif, Viterbi Sch Engn, Los Angeles, CA 90089 USA. [Kateb, Babak; Yamamoto, Vicky; Nikzad, Shouleh] Univ So Calif, Keck Sch Med, Los Angeles, CA 90033 USA. [Kateb, Babak; Black, Keith L.; Ljubimova, Julia Y.; Ding, Hui; Patil, Rameshwar; Portilla-Arias, Jose Antonio] Cedars Sinai Med Ctr, Maxine Dunitz Neurosurg Inst, Los Angeles, CA 90048 USA. [Chiu, Katherine; Khalsa, Bhavraj] Univ Calif Irvine, Sch Med, Irvine, CA 92697 USA. [Moore, David F.] Walter Reed Army Med Ctr, DVBIC, Washington, DC 20307 USA. [Modo, Mike] Kings Coll London, London WC2R 2LS, England. [Neman, Josh; Grundfest, Warren] Univ Calif Los Angeles, David Geffen Sch Med, Los Angeles, CA 90095 USA. [Okun, Michael S.] Univ Florida, Movement Disorders Ctr, Dept Neurol, Gainesville, FL 32610 USA. [Okun, Michael S.] Univ Florida, Movement Disorders Ctr, Dept Neurosurg, Gainesville, FL 32610 USA. [Prakash, Neal] Univ Hawaii, John A Burns Sch Med, Manoa, HI 96813 USA. [Farahani, Keyvan] NCI, Bethesda, MD 20892 USA. [Heiss, John D.] NINDS, Bethesda, MD 20824 USA. [Nikzad, Shouleh] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kateb, B (reprint author), IBMISPS, 8159 Santa Monica Blvd,Suite 200, W Hollywood, CA 90046 USA. EM Bkateb@ibmisps.org RI Modo, Michel/E-5170-2012; Farahani, Keyvan/G-9069-2012; PORTILLA-ARIAS, JOSE/C-3223-2008; OI PORTILLA-ARIAS, JOSE/0000-0003-1105-1842; Khalsa, Bhavraj/0000-0003-0915-931X; Okun, Michael/0000-0002-6247-9358; Heiss, John/0000-0002-3890-0165; Modo, Michel/0000-0003-4436-735X FU NIH/NCI [R01 CA123495]; NIBIB [1 P20 EB007076-01] FX We would like to specially thank Dr. Eggehard Holler for his contribution to the paper. Our thanks and appreciation to Dr. Nakissa Sadrieh for her permission to include the table on FDA-approved drugs in the nanometer scale. We would also like to acknowledge Julia Ljubimova and Mike Modo's grant support from the NIH/NCI R01 CA123495 grant and NIBIB (Quantum Grant-1 P20 EB007076-01), respectively. Dr. Modo's NIBIB Quantum Grant is directed towards tissue engineering and brain research (PEG-based hydrogels, etc.). We acknowledge Dr. Behnam Badie for his editorial contributions and Rohit Majumdar and Adrian Au for their time and help in conducting the literature search. This work is also made possible through a generous contribution of the Brain Mapping Foundation. The contents of this paper are solely the responsibility of the authors and represent the official position of the IBMISP Society. The contents do not represent the official views of NINDS/NIH and NCI/NIH. NR 237 TC 64 Z9 66 U1 13 U2 77 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1053-8119 EI 1095-9572 J9 NEUROIMAGE JI Neuroimage PD JAN PY 2011 VL 54 SU 1 BP S106 EP S124 DI 10.1016/j.neuroimage.2010.01.105 PG 19 WC Neurosciences; Neuroimaging; Radiology, Nuclear Medicine & Medical Imaging SC Neurosciences & Neurology; Radiology, Nuclear Medicine & Medical Imaging GA 813ZF UT WOS:000294408600016 PM 20149882 ER PT J AU Wood, SJ Loehr, JA Guilliams, ME AF Wood, S. J. Loehr, J. A. Guilliams, M. E. TI Sensorimotor reconditioning during and after spaceflight SO NEUROREHABILITATION LA English DT Article DE Vestibular; microgravity; exercise; rehabilitation ID GALVANIC VESTIBULAR STIMULATION; INTERNATIONAL-SPACE-STATION; LONG-DURATION SPACEFLIGHT; MOTION SICKNESS; SPATIAL ORIENTATION; VARIABLE PRACTICE; POSTURAL CONTROL; SKELETAL-MUSCLE; BALANCE CONTROL; MICROGRAVITY AB Exposure to microgravity drives adaptive changes in healthy individuals reconditioned for abnormal gravity states. These changes are maladaptive for return to earth's gravity. The intersubject variability of sensorimotor decrements is striking, although poorly understood. Multisensory integration, which is important for resolving sensory ambiguity on earth, is a critical mechanism for sensorimotor adaptation during and following space flight. The removal of gravitational loading also has profound effects that both negatively impact sensorimotor function and reduce capacity to overcome sensorimotor deficits. Countermeasure strategies include preflight training to facilitate transition to microgravity, pharmaceuticals and restriction of some activities early on orbit, and inflight exercise to minimize deconditioning during longer duration missions. Active motion is important to promote reconditioning upon return to earth's gravity. A supervised reconditioning program utilizes exercises that challenge multisensory integration with an increasing level of difficulty customized to the individual's state of recovery. This program also serves to increase crew self-awareness of fall risk. New resistive and aerobic exercise capabilities onboard the International Space Station contribute to improved postflight mobility. Lessons learned from inflight and postflight reconditioning programs have implications for future exploration crews that will operate more autonomously, as well as rehabilitation in clinical populations on earth. C1 [Wood, S. J.] Univ Space Res Assoc, Houston, TX USA. [Wood, S. J.; Loehr, J. A.; Guilliams, M. E.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Loehr, J. A.; Guilliams, M. E.] Wyle Integrated Sci & Engn Grp, Houston, TX USA. RP Wood, SJ (reprint author), NASA, Johnson Space Ctr SK 272, 2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.j.wood@nasa.gov NR 81 TC 13 Z9 13 U1 0 U2 6 PU IOS PRESS PI AMSTERDAM PA NIEUWE HEMWEG 6B, 1013 BG AMSTERDAM, NETHERLANDS SN 1053-8135 J9 NEUROREHABILITATION JI Neurorehabilitation PY 2011 VL 29 IS 2 BP 185 EP 195 DI 10.3233/NRE-2011-0694 PG 11 WC Clinical Neurology; Rehabilitation SC Neurosciences & Neurology; Rehabilitation GA 842IB UT WOS:000296589600010 PM 22027081 ER PT J AU Samanta, A Ganguly, S Myneni, RB AF Samanta, Arindam Ganguly, Sangram Myneni, Ranga B. TI MODIS Enhanced Vegetation Index data do not show greening of Amazon forests during the 2005 drought SO NEW PHYTOLOGIST LA English DT Letter DE Amazon; drought; rainforests; remote sensing; sensitivity ID BIOMASS; DIEBACK; GROWTH C1 [Samanta, Arindam; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. [Ganguly, Sangram] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. RP Samanta, A (reprint author), Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. EM arindam.sam@gmail.com RI Myneni, Ranga/F-5129-2012 NR 21 TC 23 Z9 23 U1 2 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X J9 NEW PHYTOL JI New Phytol. PY 2011 VL 189 IS 1 BP 11 EP 15 DI 10.1111/j.1469-8137.2010.03516.x PG 5 WC Plant Sciences SC Plant Sciences GA 689AS UT WOS:000284900100005 PM 21039569 ER PT J AU Tsurutani, B Morales, G AF Tsurutani, B. Morales, G. TI "Nonlinear plasma waves in space and laboratories" Preface SO NONLINEAR PROCESSES IN GEOPHYSICS LA English DT Editorial Material C1 [Tsurutani, B.] CALTECH, Jet Prop Lab, Space Plasma Sect, Pasadena, CA 91109 USA. [Morales, G.] Univ Calif Los Angeles, Phys & Astron Dept, Los Angeles, CA 90095 USA. RP Tsurutani, B (reprint author), CALTECH, Jet Prop Lab, Space Plasma Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM bruce.t.tsurutani@jpl.nasa.gov NR 7 TC 0 Z9 0 U1 1 U2 1 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1023-5809 J9 NONLINEAR PROC GEOPH JI Nonlinear Process Geophys. PY 2011 VL 18 IS 5 BP 609 EP 610 DI 10.5194/npg-18-609-2011 PG 2 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 844JK UT WOS:000296743300007 ER PT J AU Stark, J Gorman, J Hennessey, M Reseghetti, F Willis, J Lyman, J Abraham, J Borghini, M AF Stark, J. Gorman, J. Hennessey, M. Reseghetti, F. Willis, J. Lyman, J. Abraham, J. Borghini, M. TI A computational method for determining XBT depths SO OCEAN SCIENCE LA English DT Article ID EXPENDABLE BATHYTHERMOGRAPH XBT; FALL-RATE; PIPE-FLOW; TURBULENCE MODELS; T-7 XBT; TEMPERATURE; LAMINAR; SIPPICAN; EQUATION; TSK AB A new technique for determining the depth of expendable bathythermographs (XBTs) is developed. This new method uses a forward-stepping calculation which incorporates all of the forces on the XBT devices during their descent. Of particular note are drag forces which are calculated using a new drag coefficient expression. That expression, obtained entirely from computational fluid dynamic modeling, accounts for local variations in the ocean environment. Consequently, the method allows for accurate determination of depths for any local temperature environment. The results, which are entirely based on numerical simulation, are compared with the experiments of LM Sippican T-5 XBT probes. It is found that the calculated depths differ by less than 3% from depth estimates using the standard fall-rate equation (FRE). Furthermore, the differences decrease with depth. The computational model allows an investigation of the fluid flow patterns along the outer surface of the probe as well as in the interior channel. The simulations take account of complex flow phenomena such as laminar-turbulent transition and flow separation. C1 [Stark, J.; Gorman, J.; Hennessey, M.; Abraham, J.] Univ St Thomas, Sch Engn, St Paul, MN 55105 USA. [Reseghetti, F.] UTMAR OSS, ENEA, I-19032 Forte S Teresa, Pozzuolo Di Ler, Italy. [Willis, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lyman, J.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Borghini, M.] CNR ISMAR, I-19032 Forte S Teresa, Pozzuolo Di Ler, Italy. RP Abraham, J (reprint author), Univ St Thomas, Sch Engn, St Paul, MN 55105 USA. EM jpabraham@stthomas.edu RI CNR, Ismar/P-1247-2014; OI CNR, Ismar/0000-0001-5351-1486; Gorman, John/0000-0003-4046-7847 NR 37 TC 6 Z9 6 U1 2 U2 4 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1812-0784 J9 OCEAN SCI JI Ocean Sci. PY 2011 VL 7 IS 6 BP 733 EP 743 DI 10.5194/os-7-733-2011 PG 11 WC Meteorology & Atmospheric Sciences; Oceanography SC Meteorology & Atmospheric Sciences; Oceanography GA 867YS UT WOS:000298491300001 ER PT J AU Jones, LW Liang, YY Pituskin, EN Battaglini, CL Scott, JM Hornsby, WE Haykowsky, M AF Jones, Lee W. Liang, Yuanyuan Pituskin, Edith N. Battaglini, Claudio L. Scott, Jessica M. Hornsby, Whitney E. Haykowsky, Mark TI Effect of Exercise Training on Peak Oxygen Consumption in Patients with Cancer: A Meta-Analysis SO ONCOLOGIST LA English DT Article DE Aerobic training; Resistance training; Peak oxygen consumption; Aerobic capacity; Randomized controlled trials ID QUALITY-OF-LIFE; RANDOMIZED CONTROLLED-TRIAL; OPERABLE BREAST-CANCER; CELL LUNG-CANCER; PHYSICAL-FITNESS; AEROBIC EXERCISE; CARDIORESPIRATORY FITNESS; ADJUVANT CHEMOTHERAPY; RISK PROFILE; WOMEN AB Background. We conducted a meta-analysis to determine the effects of supervised exercise training on peak oxygen consumption (VO2peak) in adults with cancer. Methods. A literature review using Ovid MEDLINE (1950-2010), the Cochrane Central Register of Controlled Trials (1991-2010), AMED (1985-2010), Embase (1988-2010), PubMed (1966-2010), Scopus (1950-2010), and Web of Science (1950-2010) was performed to identify randomized controlled trials examining the effects of supervised exercise training on measurement of VO2peak (via gas exchange analysis) in adults with cancer. Studies were selected using predetermined criteria, and two independent reviewers extracted data. Weighted mean differences (WMDs) were calculated using random effect models. Results. Six studies evaluated VO2peak involving a total of 571 adult cancer patients (exercise, n = 344; usual care control, n = 227). Pooled data indicated that exercise training was associated with a statistically significant increase in VO2peak (WMD, 2.90 ml.kg(-1).min(-1); 95% confidence interval [CI], 1.16-4.64); however, significant heterogeneity was evident in this estimate (I-2, 87%). Usual care (control) was associated with a significant decline in VO2peak from baseline to postintervention (WMD, -1.02 ml.kg(-1).min(-1); 95% CI, -1.46 to -0.58; I-2, 22%). Sensitivity analyses indicated superior improvements in VO2peak for studies conducted for a shorter duration (<4 months) and following the completion of adjuvant therapy (p-values < .001). Exercise training was not associated with a higher incidence of adverse events, although safety was not rigorously monitored or reported. Conclusions. Supervised exercise training is associated with significant improvements in VO2peak following a diagnosis of early-stage cancer, with minimal adverse events. The Oncologist 2011; 16: 112-120 C1 [Jones, Lee W.; Hornsby, Whitney E.] Duke Univ, Med Ctr, Dept Radiat Oncol, Durham, NC 27710 USA. [Liang, Yuanyuan] Univ Texas Hlth Sci Ctr San Antonio, San Antonio, TX 78229 USA. [Pituskin, Edith N.; Haykowsky, Mark] Univ Alberta, Edmonton, AB, Canada. [Battaglini, Claudio L.] Univ N Carolina, Chapel Hill, NC USA. [Scott, Jessica M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Jones, LW (reprint author), Duke Univ, Med Ctr, Dept Radiat Oncol, Durham, NC 27710 USA. EM lee.w.jones@duke.edu RI Battaglini, Claudio/D-7247-2013 FU NIH [CA143254, CA142566, CA138634, CA133895, CA125458]; George and Susan Beischer FX L.W.J. is supported by NIH CA143254, CA142566, CA138634, CA133895, CA125458, and George and Susan Beischer. NR 44 TC 78 Z9 79 U1 2 U2 13 PU ALPHAMED PRESS PI DURHAM PA 318 BLACKWELL ST, STE 260, DURHAM, NC 27701-2884 USA SN 1083-7159 EI 1549-490X J9 ONCOLOGIST JI Oncologist PD JAN PY 2011 VL 16 IS 1 BP 112 EP 120 DI 10.1634/theoncologist.2010-0197 PG 9 WC Oncology SC Oncology GA 710JB UT WOS:000286506600013 PM 21212429 ER PT S AU Stahl, HP Barney, R Bauman, J Feinberg, L Mccleese, D Singh, U AF Stahl, H. Philip Barney, Rich Bauman, Jill Feinberg, Lee Mccleese, Dan Singh, Upendra BE Burge, JH Fahnle, OW Williamson, R TI Optical manufacturing and testing requirements identified by the NASA Science Instruments, Observatories and Sensor Systems Technology Assessment SO OPTICAL MANUFACTURING AND TESTING IX SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optical Manufacturing and Testing IX CY AUG 22-24, 2011 CL San Diego, CA SP SPIE DE NASA; Optical Manufacturing Technology; Optical Testing Technology; Technology Development AB Optical manufacturing and testing technologies are critical to enabling NASA's future high priority missions. A technology assessment roadmap for Science Instruments, Observatories and Sensor Systems (SIOSS) was developed for the NASA Office of Chief Technologist. This roadmap identifies a wide range of specific challenges ( including some which require optical manufacturing and testing technology) that require maturation over the next 10 years. C1 [Stahl, H. Philip] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Stahl, HP (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 12 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-736-0 J9 PROC SPIE PY 2011 VL 8126 AR 812603 DI 10.1117/12.898330 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BXY06 UT WOS:000297589300002 ER PT S AU Wallace, JK Rao, S Jensen-Clem, RM Serabyn, G AF Wallace, J. Kent Rao, Shanti Jensen-Clem, Rebecca M. Serabyn, Gene BE Burge, JH Fahnle, OW Williamson, R TI Phase-Shifting Zernike Interferometer Wavefront Sensor SO OPTICAL MANUFACTURING AND TESTING IX SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optical Manufacturing and Testing IX CY AUG 22-24, 2011 CL San Diego, CA SP SPIE DE Wavefront sensing; Zernike phase-contrast; adaptive optics ID TRANSPARENT OBJECTS; CONTRAST AB The canonical Zernike phase-contrast technique(1,2,3,4) transforms a phase object in one plane into an intensity object in the conjugate plane. This is done by applying a static pi/2 phase shift to the central core (similar to lambda/D) of the PSF which is intermediate between the input and output planes. Here we present a new architecture for this sensor. First, the optical system is simple and all reflective. Second, the phase shift in the central core of the PSF is dynamic and or arbitrary size. This common-path, all-reflective design makes it minimally sensitive to vibration, polarization and wavelength. We review the theory of operation, describe the optical system, summarize numerical simulations and sensitivities and review results from a laboratory demonstration of this novel instrument. C1 [Wallace, J. Kent; Rao, Shanti; Serabyn, Gene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wallace, JK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM James.K.Wallace@jpl.nasa.gov NR 11 TC 8 Z9 8 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-736-0 J9 PROC SPIE PY 2011 VL 8126 AR 81260F DI 10.1117/12.892843 PG 11 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BXY06 UT WOS:000297589300012 ER PT S AU Biskach, MP McClelland, RS Saha, T Zhang, WW AF Biskach, Michael P. McClelland, Ryan S. Saha, Timo Zhang, William W. BE ODell, SL Pareschi, G TI Size optimization for mirror segments for X-ray optics SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy V/SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 23-25, 2011 CL San Diego, CA SP SPIE DE Segment Optics; X-ray Optics; Finite Element Modeling; IXO; Mirror Sizing AB Flight Mirror Assemblies (FMAs) for X-ray telescopes similar to that of the International X-ray Observatory (IXO) concept consist of several thousands of individual mirror segments. The size, shape, and location of these mirrors affect many characteristics of the telescope design. Mission requirements among other factors in turn restrict mirror segment parameters such as thickness, axial length, azimuthal span, and mass density. This paper provides an overview of the critical relationships relating to mirror segment size and configuration throughout the design and analysis of an X-ray mirror assembly. A computational analysis is presented in the form of ray tracing pairs of thin X-ray mirror segments of varying sizes aligned in gravity and supported using kinematic constraints with corresponding self weight distortions calculated using finite element analysis (FEA). The work in this paper may be used as a starting point for determining mirror segment sizes for X-ray missions like that of IXO and beyond. C1 [Biskach, Michael P.; McClelland, Ryan S.] SGT Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. [Saha, Timo; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Biskach, MP (reprint author), SGT Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. EM michael.biskach@nasa.gov NR 4 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8757-5 J9 PROC SPIE PY 2011 VL 8147 AR 814711 DI 10.1117/12.892636 PG 9 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BBA80 UT WOS:000306321500035 ER PT S AU Rho, J Andersen, M Tappe, A Reach, WT Bernard, JP Hewitt, J AF Rho, J. Andersen, M. Tappe, A. Reach, W. T. Bernard, J. P. Hewitt, J. BE Joblin, C Tielens, AGGM TI PAH AND DUST PROCESSING IN SUPERNOVA REMNANTS SO PAHS AND THE UNIVERSE: A SYMPOSIUM TO CELEBRATE THE 25TH ANNIVERSARY OF THE PAH HYPOTHESIS SE EAS Publications Series LA English DT Proceedings Paper CT Symposium to Celebrate the 25th Anniversary of the PAH Hypothesis CY MAY 31-JUN 04, 2010 CL Univ Toulouse, Toulouse, FRANCE SP CESR, LCPQ, CNRS, Univ Toulouse, INSU CNRS, Univ Paul Sabatier, CNES, Region Midi Pyrenees, Minist Enseignement Superieur & Rech, ESA, IRSAMC UPS, INC CNRS, Reseau Chimie Theor, INP CNRS, Departement Haute Garonne HO Univ Toulouse ID INTERSTELLAR DUST; EMISSION; GALAXY AB I present observations of shock-processed PAHs and dust in supernova remnants (SNRs). Supernova shocks are one of the primary sites destroying, fragmenting and altering interstellar PAHs and dust. Studies of PAHs through supernova shocks had been limited because of confusion with PAHs in background emission. Spitzer observations with high sensitivity and resolution allow us to separate PAHs associated with the SNRs and unrelated, Galactic PAHs. In the young SNR N132D, PAH features are detected with a higher PAH ratio of 15-20/7.7 mu m than those of other astronomical objects, and we suggest large PAHs have survived behind the shock. We present the spectra of additional 14 SNRs observed with Spitzer IRS and MIPS SED covering the range of 5-90 mu m. Bright PAH features from 6.2 to 15-20 mu m are detected from many of SNRs which emit molecular hydrogen lines, indicating that both large and small PAHs survive in low velocity shocks. We observe a strong correlation between PAH detection and carbonaceous small grains, while a few SNRs with dominant silicate dust lack PAR features. We characterize PAHs depending on the shock velocity, preshock density and temperature of hot gas, and discuss PAH and dust processing in shocks and implication of PAR and dust cycles in ISM. C1 [Rho, J.; Reach, W. T.] NASA, Ames Res Ctr, SOFIA Sci Mission Operat USRA, MS 211-3, Moffett Field, CA 94035 USA. [Andersen, M.] European Space Agcy, ESTEC, Dept Res & Sci Support, NL-2200 AG Noordwijk, Netherlands. [Tappe, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernard, J. P.] CNRS, Ctr Etude Spatiale Rayonnements, F-31028 Toulouse, France. [Hewitt, J.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RP Rho, J (reprint author), NASA, Ames Res Ctr, SOFIA Sci Mission Operat USRA, MS 211-3, Moffett Field, CA 94035 USA. EM jrho@sofia.usra.edu OI Reach, William/0000-0001-8362-4094 NR 10 TC 1 Z9 1 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 978-2-7598-0624-9 J9 EAS PUBLICATIONS PY 2011 VL 46 BP 169 EP + DI 10.1051/eas/1146018 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVJ75 UT WOS:000291672700018 ER PT B AU Dise, NB Shurpali, NJ Weishampel, P Verma, SB Verry, ES Gorham, E Crill, PM Harriss, RC Kelley, CA Yavitt, JB Smemo, KA Kolka, RK Smith, K Kim, J Clement, RJ Arkebauer, TJ Bartlett, KB Billesbach, DP Bridgham, SD Elling, AE Flebbe, PA King, JY Martens, CS Sebacher, DI Williams, CJ Wieder, RK AF Dise, Nancy B. Shurpali, Narasinha J. Weishampel, Peter Verma, Shashi B. Verry, Elon S. Gorham, Eville Crill, Patrick M. Harriss, Robert C. Kelley, Cheryl A. Yavitt, Joseph B. Smemo, Kurt A. Kolka, Randall K. Smith, Kelly Kim, Joon Clement, Robert J. Arkebauer, Timothy J. Bartlett, Karen B. Billesbach, David P. Bridgham, Scott D. Elling, Art E. Flebbe, Patricia A. King, Jennifer Y. Martens, Christopher S. Sebacher, Daniel I. Williams, Christopher J. Wieder, R. Kelman BE Kolka, RK Sebestyen, SD Verry, ES Brooks, KN TI Carbon Emissions from Peatlands SO PEATLAND BIOGEOCHEMISTRY AND WATERSHED HYDROLOGY AT THE MARCELL EXPERIMENTAL FOREST LA English DT Article; Book Chapter ID EDDY-CORRELATION MEASUREMENTS; METHANE EMISSIONS; NORTHERN PEATLANDS; MINNESOTA PEATLAND; ATMOSPHERIC METHANE; DIOXIDE EXCHANGE; NATURAL WETLANDS; BOREAL PEATLAND; GLOBAL CHANGE; FLUX C1 Manchester Metropolitan Univ, Dept Environm & Geog Sci, Manchester M15 6BH, Lancs, England. [Shurpali, Narasinha J.] Univ Eastern Finland, Dept Environm Sci, Kuopio, Finland. [Weishampel, Peter] Northland Coll, Dept Nat Resources, Ashland, WI USA. [Verma, Shashi B.] Univ Nebraska, Sch Nat Resources, Lincoln, NE USA. [Verry, Elon S.; Kolka, Randall K.; Elling, Art E.] US Forest Serv, No Res Stn, USDA, Grand Rapids, MI USA. [Gorham, Eville] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Crill, Patrick M.] Stockholm Univ, Dept Geol & Geochem, S-10691 Stockholm, Sweden. [Harriss, Robert C.] Houston Adv Res Ctr, The Woodlands, TX USA. [Kelley, Cheryl A.] Univ Missouri, Dept Geol Sci, Columbia, MO USA. [Yavitt, Joseph B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [Smemo, Kurt A.] Holden Arboretum, Kirtland, OH USA. [Smith, Kelly] Carlton Cty Soil & Water Conservat Dist, Carlton, MN USA. [Kim, Joon] Yonsei Univ, Global Environm Lab, Seoul 120749, South Korea. [Clement, Robert J.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. [Arkebauer, Timothy J.] Univ Nebraska, Dept Agron & Hort, Lincoln, NE USA. [Bartlett, Karen B.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Billesbach, David P.] Univ Nebraska, Dept Biol Syst Engn, Lincoln, NE USA. [Bridgham, Scott D.] Univ Oregon, Ctr Ecol & Evolutionary Biol, Eugene, OR 97403 USA. [Flebbe, Patricia A.] US Forest Serv, Pacific Southwest Reg, USDA, Vallejo, CA USA. [King, Jennifer Y.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. [Martens, Christopher S.] Univ N Carolina, Dept Marine Sci, Chapel Hill, NC USA. [Sebacher, Daniel I.] NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23665 USA. [Williams, Christopher J.] Franklin & Marshall Coll, Dept Earth & Environm, Lancaster, PA 17604 USA. [Wieder, R. Kelman] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. RP Dise, NB (reprint author), Manchester Metropolitan Univ, Dept Environm & Geog Sci, Manchester M15 6BH, Lancs, England. RI King, Jennifer Y./I-5986-2015; Kelley, Cheryl/K-9392-2015; OI King, Jennifer Y./0000-0003-3433-5952; Williams, Christopher/0000-0002-8819-6786 NR 76 TC 2 Z9 2 U1 1 U2 4 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4398-1425-3; 978-1-4398-1424-6 PY 2011 BP 297 EP 347 PG 51 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA BC9LR UT WOS:000356611000014 ER PT J AU Newman, PA McKenzie, R AF Newman, Paul A. McKenzie, Richard TI UV impacts avoided by he Montreal Protocol SO PHOTOCHEMICAL & PHOTOBIOLOGICAL SCIENCES LA English DT Article ID DISCRETE ORDINATE METHOD; SURFACE ALBEDO; TOTAL OZONE; HUMAN-SKIN; VITAMIN-D; IRRADIANCE; LATITUDE; EXPOSURE; ALTITUDE; CLIMATE AB Temporal and geographical variabilities in the future "world expected" UV environment are compared with the "world avoided", which would have occurred without the Montreal Protocol on Substances That Deplete the Ozone Layer and its subsequent amendments and adjustments. Based on calculations of clear-sky UV irradiances, the effects of the Montreal Protocol have been hugely beneficial to avoid the health risks, such as skin cancer, which are associated with high UV, while there is only a small increase in health risks, such as vitamin D deficiency, that are associated with low UV. However, interactions with climate change may lead to changes in cloud and albedo, and possibly behavioural changes that could also be important. C1 [Newman, Paul A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McKenzie, Richard] Natl Inst Water & Atmospher Res, NIWA Lauder, Omakau 9352, Cent Otago, New Zealand. RP Newman, PA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Newman, Paul/D-6208-2012 OI Newman, Paul/0000-0003-1139-2508 NR 37 TC 12 Z9 13 U1 2 U2 21 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1474-905X J9 PHOTOCH PHOTOBIO SCI JI Photochem. Photobiol. Sci. PY 2011 VL 10 IS 7 BP 1152 EP 1160 DI 10.1039/c0pp00387e PG 9 WC Biochemistry & Molecular Biology; Biophysics; Chemistry, Physical SC Biochemistry & Molecular Biology; Biophysics; Chemistry GA 785CZ UT WOS:000292206300007 PM 21455537 ER PT J AU Sivaraman, B Mebel, AM Mason, NJ Babikov, D Kaiser, RI AF Sivaraman, B. Mebel, A. M. Mason, N. J. Babikov, D. Kaiser, R. I. TI On the electron-induced isotope fractionation in low temperature O-32(2)/O-36(2) ices-ozone as a case study SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS LA English DT Article ID OXYGEN-ISOTOPE; MOLECULAR-OXYGEN; ICY SATELLITES; SOLAR-SYSTEM; MECHANISM; O-3; INTERSTELLAR; SPECTROSCOPY; MATRICES; SPECTRA AB The formation of six ozone isotopomers and isotopologues, (OOO)-O-16-O-16-O-16,(OOO)-O-18-O-18-O-18, (OOO)-O-16-O-16-O-18, (OOO)-O-18-O-18-O-16, (OOO)-O-16-O-18-O-16, and (OOO)-O-18-O-16-O-18, has been studied in electron-irradiated solid oxygen O-16(2) and O-18(2) (1 : 1) ices at 11 K. Significant isotope effects were found to exist which involved enrichment of O-18-bearing ozone molecules. The heavy (OOO)-O-18-O-18-O-18 species is formed with a factor of about six higher than the corresponding (OOO)-O-16-O-16-O-16 isotopologue. Likewise, the heavy (OOO)-O-18-O-18-O-16 species is formed with abundances of a factor of three higher than the lighter (OOO)-O-16-O-16-O-18 counterpart. No isotope effect was observed in the production of (OOO)-O-16-O-18-O-16 versus (OOO)-O-18-O-16-O-18. Such studies on the formation of distinct ozone isotopomers and isotopologues involving non-thermal, non-equilibrium chemistry by irradiation of oxygen ices with high energy electrons, as present in the magnetosphere of the giant planets Jupiter and Saturn, may suggest that similar mechanisms may contribute to the O-18 enrichment on the icy satellites of Jupiter and Saturn such as Ganymede, Rhea, and Dione. In such a Solar System environment, energetic particles from the magnetospheres of the giant planets may induce non-equilibrium reactions of suprathermal and/or electronically excited atoms under conditions, which are quite distinct from isotopic enrichments found in classical, thermal gas phase reactions. C1 [Sivaraman, B.; Mason, N. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Mebel, A. M.] Florida Int Univ, Dept Chem & Biochem, Miami, FL 33199 USA. [Babikov, D.] Marquette Univ, Dept Chem, Milwaukee, WI 53201 USA. [Kaiser, R. I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Kaiser, R. I.] Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. RP Mason, NJ (reprint author), Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. EM n.j.mason@open.ac.uk; ralfk@hawaii.edu RI Mebel, Alexander/A-5234-2009 FU Open University; National Aeronautics Space Administration (NASA) (NASA Astrobiology Institute through the Office of Space Science) [NNA09DA77A] FX One of us (BS) acknowledges receipt of a Postgraduate studentship from the Open University. RIK thanks the National Aeronautics Space Administration (NASA Astrobiology Institute under Cooperative Agreement no. NNA09DA77A issued through the Office of Space Science) for funding. NR 43 TC 8 Z9 8 U1 0 U2 5 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1463-9076 J9 PHYS CHEM CHEM PHYS JI Phys. Chem. Chem. Phys. PY 2011 VL 13 IS 2 BP 421 EP 427 DI 10.1039/c0cp00448k PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 695RN UT WOS:000285390400006 PM 21079822 ER PT J AU Ennis, CP Bennett, CJ Kaiser, RI AF Ennis, Courtney P. Bennett, Chris J. Kaiser, Ralf I. TI On the formation of ozone in oxygen-rich solar system ices via ionizing radiation SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS LA English DT Article ID CRYSTALLINE WATER ICE; GALILEAN SATELLITES; INFRARED INTENSITIES; HYDROGEN-PEROXIDE; INTERSTELLAR ICE; ION IRRADIATION; CARBON-DIOXIDE; SOLID OXYGEN; 10 K; CO2 AB The irradiation of pure molecular oxygen (O(2)) and carbon dioxide (CO(2)) ices with 5 keV H(+) and He(+) ions was investigated experimentally to simulate the chemical processing of oxygen rich planetary and interstellar surfaces by exposure to galactic cosmic ray (GCR), solar wind, and magnetospheric particles. Deposited at 12 K under ultra-high vacuum conditions (UHV), the irradiated condensates were monitored on-line and in situ in the solid-state by Fourier transform infrared spectroscopy (FTIR), revealing the formation of ozone (O(3)) in irradiated oxygen ice; and ozone, carbon monoxide (CO), and cyclic carbon trioxide (c-CO(3)) in irradiated carbon dioxide. In addition to these irradiation products, evolution of gas-phase molecular hydrogen (H(2)), atomic helium (He) and molecular oxygen (O(2)) were identified in the subliming oxygen and carbon dioxide condensates by quadrupole mass spectrometry (QMS). Temporal abundances of the oxygen and carbon dioxide precursors and the observed molecular products were compiled over the irradiation period to develop reaction schemes unfolding in the ices. These reactions were observed to be dependent on the generation of atomic oxygen (O) by the homolytic dissociation of molecular oxygen induced by electronic, S(e), and nuclear, S(n), interaction with the impinging ions. In addition, the destruction of the ozone and carbon trioxide products back to the molecular oxygen and carbon dioxide precursors was promoted over an extended period of ion bombardment. Finally, destruction and formation yields were calculated and compared between irradiation sources (including 5 keV electrons) which showed a surprising correlation between the molecular yields (similar to 10(-3)-10(-4) molecules eV(-1)) created by H(+) and He(+) impacts. However, energy transfer by isoenergetic, fast electrons typically generated ten times more product molecules per electron volt (similar to 10(-2)-10(-3) molecules eV(-1)) than exposure to the ions. Implications of these findings to Solar System chemistry are also discussed. C1 [Ennis, Courtney P.; Bennett, Chris J.; Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Bennett, Chris J.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Kaiser, RI (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. EM ralfk@hawaii.edu RI Ennis, Courtney/M-5050-2015 OI Bennett, Christopher/0000-0002-4181-6976; Ennis, Courtney/0000-0003-1774-8982 FU Air Force Office of Scientific Research [A9550-09-1-0177]; National Aeronautics Space Administration (NASA) Astrobiology Institute through the Office of Space Science [NNA09DA77A] FX CPE and RIK thank the Air Force Office of Scientific Research (A9550-09-1-0177) for support. CJB thanks the National Aeronautics Space Administration (NASA Astrobiology Institute under Cooperative Agreement no. NNA09DA77A issued through the Office of Space Science) for funding. NR 49 TC 14 Z9 14 U1 0 U2 12 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1463-9076 J9 PHYS CHEM CHEM PHYS JI Phys. Chem. Chem. Phys. PY 2011 VL 13 IS 20 BP 9469 EP 9482 DI 10.1039/c1cp20434c PG 14 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 759FA UT WOS:000290224900049 PM 21483931 ER PT J AU Kayi, H Kaiser, RI Head, JD AF Kayi, Hakan Kaiser, Ralf I. Head, John D. TI A computational study on the structures of methylamine-carbon dioxide-water clusters: evidence for the barrier free formation of the methylcarbamic acid zwitterion (CH3NH2+COO-) in interstellar water ices SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS LA English DT Article ID DENSITY-FUNCTIONAL THEORY; MOLECULAR-ORBITAL METHODS; FRAGMENT POTENTIAL METHOD; AMINO-ACIDS; AB-INITIO; VIBRATIONAL-SPECTRA; GASEOUS GLYCINE; LOW-TEMPERATURE; WAVE-FUNCTIONS; SOLAR-SYSTEM AB We investigated theoretically the interaction between methylamine (CH3NH2) and carbon dioxide (CO2) in the presence of water (H2O) molecules thus simulating the geometries of various methylamine-carbon dioxide complexes (CH3NH2/CO2) relevant to the chemical processing of icy grains in the interstellar medium (ISM). Two approaches were followed. In the amorphous water phase approach, structures of methylamine-carbon dioxide-water [CH3NH2/CO2/(H2O)(n)] clusters (n = 0-20) were studied using density functional theory (DFT). In the crystalline water approach, we simulated methylamine and carbon dioxide interactions on a fragment of the crystalline water ice surface in the presence of additional water molecules in the CH3NH2/CO2 environment using DFT and effective fragment potentials (EFP). Both the geometry optimization and vibrational frequency analysis results obtained from these two approaches suggested that the surrounding water molecules which form hydrogen bonds with the CH3NH2/CO2 complex draw the carbon dioxide closer to the methylamine. This enables, when two or more water molecules are present, an electron transfer from methylamine to carbon dioxide to form the methylcarbamic acid zwitterion, CH3NH2+CO2-, in which the carbon dioxide is bent. Our calculations show that the zwitterion is formed without involving any electronic excitation on the ground state surface; this structure is only stable in the presence of water, i.e. in a methyl amine-carbon dioxide-water ice. Notably, in the vibrational frequency calculations on the methylcarbamic acid zwitterion and two water molecules we find the carbon dioxide asymmetric stretch is drastically red shifted by 435 cm(-1) to 1989 cm(-1) and the carbon dioxide symmetric stretch becomes strongly infrared active. We discuss how the methylcarbamic acid zwitterion CH3NH2+CO2- might be experimentally and astronomically identified by its asymmetric CO2 stretching mode using infrared spectroscopy. C1 [Kayi, Hakan; Kaiser, Ralf I.; Head, John D.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Kaiser, Ralf I.] Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. RP Head, JD (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. EM johnh@hawaii.edu RI Kayi, Hakan/C-7300-2009 OI Kayi, Hakan/0000-0001-7300-0325 FU W.M. Keck Foundation; NASA Astrobiology Institute, Office of Space Science [NNA09DA77A] FX This project was supported by the W.M. Keck Foundation and the NASA Astrobiology Institute under Cooperative Agreement no. NNA09DA77A issued through the Office of Space Science. The authors are also grateful for the computing assistance from Mr. M. Belcaid and the generous computing resources provided by the Dell Cluster at the University of Hawaii. NR 77 TC 11 Z9 11 U1 4 U2 31 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1463-9076 J9 PHYS CHEM CHEM PHYS JI Phys. Chem. Chem. Phys. PY 2011 VL 13 IS 23 BP 11083 EP 11098 DI 10.1039/c0cp01962c PG 16 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 770UE UT WOS:000291113200024 PM 21311787 ER PT J AU Zheng, WJ Kim, YS Kaiser, RI AF Zheng, Weijun Kim, Y. Seol Kaiser, Ralf I. TI Formation of nitric oxide and nitrous oxide in electron-irradiated (H2O)-O-18/N-2 ice mixtures-evidence for the existence of free oxygen atoms in interstellar and solar system analog ices SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS LA English DT Article ID CRYSTALLINE WATER ICE; HYDROGEN-PEROXIDE; AMINO-ACIDS; ULTRAVIOLET PHOTOLYSIS; O(D-1) REACTION; SOLID N-2; SURFACE; PLUTO; TEMPERATURE; TRITON AB We investigated the irradiation of low temperature (H2O)-O-18/N-2 ice mixtures with energetic electrons in an ultrahigh vacuum chamber. The newly formed species, such as nitric oxide ((NO)-O-18), nitrous oxide ((NNO)-O-18), hydrogen peroxide ((H2O2)-O-18) and hydrazine (N2H4), were identified in the experiments with infrared absorption spectroscopy and mass spectrometry. The results suggest that the unimolecular decomposition of water molecules within water ices at 10 K can lead to the formation of transient, suprathermal oxygen atoms. These oxygen atoms may play an important role in the formation of oxygen-containing biomolecules such as amino acids and sugar, as well as the decomposition of the biomolecules in the ices. C1 [Zheng, Weijun; Kim, Y. Seol; Kaiser, Ralf I.] Univ Hawaii, Dept Chem, Honolulu, HI 96822 USA. [Zheng, Weijun] Chinese Acad Sci, Inst Chem, Beijing Natl Lab Mol Sci, State Key Lab Mol React Dynam, Beijing 100190, Peoples R China. [Kaiser, Ralf I.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Zheng, WJ (reprint author), Univ Hawaii, Dept Chem, Honolulu, HI 96822 USA. EM zhengwj@iccas.ac.cn; ralfk@hawaii.edu FU NASA Astrobiology Institute at the University of Hawaii-Manoa [NNA04CC08A] FX This work was financed by the NASA Astrobiology Institute under Cooperative Agreement NNA04CC08A at the University of Hawaii-Manoa (WZ, RIK). We are grateful to Ed Kawamura (University of Hawaii at Manoa, Department of Chemistry) for his electrical work. NR 56 TC 3 Z9 3 U1 0 U2 6 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1463-9076 J9 PHYS CHEM CHEM PHYS JI Phys. Chem. Chem. Phys. PY 2011 VL 13 IS 35 BP 15749 EP 15754 DI 10.1039/c1cp20528e PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 810YR UT WOS:000294167700002 PM 21589959 ER PT J AU Kim, YS Zhang, F Kaiser, RI AF Kim, Y. S. Zhang, F. Kaiser, R. I. TI Laboratory simulation of Kuiper belt object volatile ices under ionizing radiation: CO-N-2 ices as a case study SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS LA English DT Article ID ULTRAVIOLET SPECTRA; MATRIX-ISOLATION; INTERSTELLAR; ION; NCN; IRRADIATION; KINETICS; ISOMERS; METHANE; PLUTO AB The exposure of icy Kuiper belt objects (KBOs) by ionizing radiation was simulated in this case of exposing carbon monoxide-nitrogen (CO-N-2) ices by energetic electrons. The radiation-induced chemical processing was monitored on-line and in situ via FTIR spectroscopy and quadrupole mass spectrometry. Besides the array of carbon oxides being reproduced as in neat irradiated carbon monoxide (CO) ices studied previously, the radiation exposure at 10 K resulted in the formation of nitrogen-bearing species of isocyanato radical (OCN), linear (l-NCN), nitric oxide (NO), nitrogen dioxide (NO2), plus diazirinone (N2CO). The infrared assignments of these species were further confirmed by isotopic shifts. The temporal evolution of individual species was found to fit in first-order reaction schemes, prepping up the underlying non-equilibrium chemistry on the formation of OCN, l-NCN, and NO radicals in particular. Also unique to the binary KBO model ices and viable for the future remote detection is diazirinone (N2CO) at 1860 cm(-1) (2v(5)) formed at lower radiation exposure. C1 [Kim, Y. S.; Zhang, F.; Kaiser, R. I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Kaiser, R. I.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Kaiser, RI (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. EM ralfk@hawaii.edu FU National Aeronautics Space Administration (NASA) Astrobiology Institute through the Office of Space Science [NNA09DA77A] FX This work was supported by the National Aeronautics Space Administration (NASA) Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science. We would like to acknowledge Dr C. S. Jamieson (University of Hawaii) for experimental work. NR 32 TC 9 Z9 9 U1 0 U2 10 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1463-9076 J9 PHYS CHEM CHEM PHYS JI Phys. Chem. Chem. Phys. PY 2011 VL 13 IS 35 BP 15766 EP 15773 DI 10.1039/c1cp20658c PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 810YR UT WOS:000294167700004 PM 21687881 ER PT J AU Kayi, H Kaiser, RI Head, JD AF Kayi, Hakan Kaiser, Ralf I. Head, John D. TI A theoretical investigation of the low energy conformers of the isomers glycine and methylcarbamic acid and their role in the interstellar medium SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS LA English DT Article ID GAUSSIAN-BASIS SETS; MOLECULAR-ORBITAL METHODS; MILLIMETER WAVE SPECTRUM; CRYSTAL-STRUCTURE; ELECTRON-DENSITY; MODEL CHEMISTRY; GASEOUS GLYCINE; CARBON MONOXIDE; CARBAMIC ACID; 1ST-ROW ATOMS AB We have theoretically investigated the low energy conformers of neutral glycine (NH(2)CH(2)COOH) and its isomer methylcarbamic acid (CH(3)NHCOOH) in the gas phase. A total of 16 different levels of the theory, including CCSD(T), MP2 and B3LYP methods with various Pople and Dunning type basis sets with and without polarization and diffuse functions were used. We found eight low energy glycine conformers, where the heavy atoms in three have a planar backbone, and four low energy methylcarbamic acid conformers all with non-planar backbones. Interestingly at all levels of theory, we found that the most stable methylcarbamic acid conformer is significantly lower in energy than the lowest energy glycine conformer. The MP2 level and single point CCSD(T) calculations show the lowest energy methylcarbamic acid conformer to be between 31 to 37 kJ mol(-1) lower in energy than the lowest energy glycine conformer. These calculations suggest that methylcarbamic acid might serve as a precursor to glycine formation in the Interstellar Medium (ISM). We also report the theoretical harmonic vibrational frequencies, infrared intensities, moment of inertia, rotational constants and dipole moments for all of the conformers. In order to understand how glycine or methylcarbamic acid might be formed in the ISM, larger calculations which model glycine or its isomer interacting with several surrounding molecules, such as water, are needed. We demonstrate that B3LYP method should provide a reliable and computationally practical approach to modeling these larger systems. C1 [Kayi, Hakan; Kaiser, Ralf I.; Head, John D.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Kaiser, Ralf I.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. RP Head, JD (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. RI Kayi, Hakan/C-7300-2009 OI Kayi, Hakan/0000-0001-7300-0325 FU W.M. Keck Foundation; NASA Astrobiology Institute through the Office of Space Science [NNA09DA77A]; TeraGrid [TG-CHE100092]; Hawaii Open Supercomputing Center FX This project is supported by the W.M. Keck Foundation and the NASA Astrobiology Institute under Cooperative Agreement no. NNA09DA77A issued through the Office of Space Science. The authors are also grateful for the generous computing resources provided by TeraGrid under grant no. TG-CHE100092 and the Hawaii Open Supercomputing Center. NR 55 TC 10 Z9 10 U1 0 U2 10 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1463-9076 J9 PHYS CHEM CHEM PHYS JI Phys. Chem. Chem. Phys. PY 2011 VL 13 IS 35 BP 15774 EP 15784 DI 10.1039/c1cp20656g PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 810YR UT WOS:000294167700005 PM 21687849 ER PT J AU Thissen, R Witasse, O Dutuit, O Wedlund, CS Gronoff, G Lilensten, J AF Thissen, Roland Witasse, Olivier Dutuit, Odile Wedlund, Cyril Simon Gronoff, Guillaume Lilensten, Jean TI Doubly-charged ions in the planetary ionospheres: a review SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS LA English DT Article ID PHOTOIONIZATION CROSS-SECTIONS; ELECTRON-IMPACT IONIZATION; KINETIC-ENERGY RELEASE; PHOTOELECTRONS COINCIDENCE SPECTROSCOPY; INDUCED DISSOCIATION REACTIONS; BOND-FORMING PROCESSES; THERMAL O++ IONS; HOT PLASMA TORUS; GROUND-STATE N2+; MOLECULAR-IONS AB This paper presents a review of the current knowledge on the doubly-charged atomic and molecular positive ions in the planetary atmospheres of the Solar System. It is focused on the terrestrial planets which have a dense atmosphere of N-2 or CO2, i.e. Venus, the Earth and Mars, but also includes Titan, the largest satellite of Saturn, which has a dense atmosphere composed mainly of N-2 and a few percent of methane. Given the composition of these neutral atmospheres, the following species are considered: C++, N++, O++, CH4++, CO++, N-2(++), NO++, O-2(++), Ar++ and CO2++. We first discuss the status of their detection in the atmospheres of planets. Then, we provide a comprehensive review of their complex and original photochemistry, production and loss processes. Synthesis tables are provided for those ions, while a discussion on individual species is also provided. Methods for detecting doubly-charged ions in planetary atmospheres are presented, namely with mass-spectrometry, remote sensing and fine plasma density measurements. A section covers some original applications, like the possible effect of the presence of doubly-charged ions on the escape of an atmosphere, which is a key topic of ongoing planetary exploration, related to the evolution of a planet. The results of models, displayed in a comparative way for Venus, Earth, Mars and Titan, are discussed, as they can predict the presence of doubly-charged ions and will certainly trigger new investigations. Finally we give our view concerning next steps, challenges and needs for future studies, hoping that new scientific results will be achieved in the coming years and feed the necessary interdisciplinary exchanges amongst different scientific communities. C1 [Thissen, Roland; Dutuit, Odile; Lilensten, Jean] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France. [Witasse, Olivier] European Space Agcy, Estec, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Dutuit, Odile] Austrian Acad Sci IWF OAW, Space Res Inst, A-8042 Graz, Austria. [Wedlund, Cyril Simon] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Gronoff, Guillaume] NASA, Langley Res Ctr, Sci Directorate, Chem & Dynam Branch, Hampton, VA 23665 USA. RP Thissen, R (reprint author), UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France. EM Roland.thissen@obs.ujf-grenoble.fr OI Gronoff, Guillaume/0000-0002-0331-7076 FU French Programme National de Planetologie; NASA; NASA Science Mission Directorate FX Since 10 years, our studies of doubly-charged ions in planetary ionospheres have received constant and precious support from the French Programme National de Planetologic, which is here acknowledged. The work of Guillaume Gronoff was supported by an appointment of the NASA Postdoctoral Program at NASA Langley Research Center, administered by Oak Ridge Associated Univ. through a contract with NASA, and funded by the NASA Science Mission Directorate. NR 206 TC 38 Z9 38 U1 4 U2 31 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1463-9076 EI 1463-9084 J9 PHYS CHEM CHEM PHYS JI Phys. Chem. Chem. Phys. PY 2011 VL 13 IS 41 BP 18264 EP 18287 DI 10.1039/c1cp21957j PG 24 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 831LB UT WOS:000295731100003 PM 21931881 ER PT B AU Tielens, AGGM Allamandola, LJ AF Tielens, Alexander G. G. M. Allamandola, Louis J. BE Khriachtchev, L TI COOL INTERSTELLAR PHYSICS AND CHEMISTRY SO PHYSICS AND CHEMISTRY AT LOW TEMPERATURES LA English DT Article; Book Chapter ID POLYCYCLIC AROMATIC-HYDROCARBONS; INFRARED SPECTRAL PROPERTIES; YOUNG STELLAR OBJECTS; SPITZER SPECTROSCOPIC SURVEY; CHARGE-TRANSFER COMPLEXES; EFFECTIVE RATE CONSTANTS; GRAIN SURFACE-CHEMISTRY; COMETARY ICE ANALOGS; ISO-SWS OBSERVATIONS; AMORPHOUS WATER ICE AB The infrared (IR) spectra of molecular cloud material in the interstellar medium of galaxies are dominated by absorption features due to simple molecules such as H2O, CH3 OH, NH3, CO2, and CO in cryogenic molecular ices. These ices are an important reservoir of material and play an important role in the organic inventory of regions of star and planet formation. Observational studies have revealed the presence of several independent ice components, often along the same line of sight. These interstellar ices are formed by accretion and reaction on grain surfaces and further processed by ultraviolet (UV) photons as well as highly energetic cosmic ray ions. Thermal processing by nearby newly formed stars is also important. In this chapter, we will review the characteristics, formation, and evolution of interstellar ices with the emphasis on relevant laboratory studies in the area of IR spectroscopy of low-temperature molecular mixtures, the surface chemistry of simple species relevant to astrophysical environments, and analog studies of the energetic processing of ices near newly formed stars. C1 [Tielens, Alexander G. G. M.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Allamandola, Louis J.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Tielens, AGGM (reprint author), Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM tielens@strw.leidenuniv.nl; Louis.J.Allamandola@nasa.gov NR 121 TC 7 Z9 7 U1 0 U2 3 PU PAN STANFORD PUBLISHING PTE LTD PI SINGAPORE PA PENTHOUSE LEVEL, SUNTEC TOWER 3, 8 TEMASEK BLVD, SINGAPORE, 038988, SINGAPORE BN 978-9-81426-782-3; 978-9-81426-751-9 PY 2011 BP 341 EP 380 D2 10.4032/9789814267823 PG 40 WC Chemistry, Physical SC Chemistry GA BXW04 UT WOS:000297316000012 ER PT J AU Shafiq, M Wahlund, JE Morooka, MW Kurth, WS Farrell, WM AF Shafiq, Muhammad Wahlund, J. -E. Morooka, M. W. Kurth, W. S. Farrell, W. M. TI Characteristics of the dust-plasma interaction near Enceladus' South Pole SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Saturn magnetosphere; E-ring; Enceladus plume; Dusty plasma; Cassini; RPWS Langmuir probe ID SATURNS E-RING; PLUME; MAGNETOSPHERE; PARTICLES AB We present RPWS Langmuir probe data from the third Enceladus flyby (E3) showing the presence of dusty plasma near Enceladus' South Pole. There is a sharp rise in both the electron and ion number densities when the spacecraft traverses through Enceladus plume. The ion density near Enceladus is found to increase abruptly from about 10(2) cm(-3) before the closest approach to 10(5) cm(-3) just 30 s after the closest approach, an amount two orders of magnitude higher than the electron density. Assuming that the inconsistency between the electron and ion number densities is due to the presence of dust particles that are collecting the missing electron charges, we present dusty plasma characteristics down to sub-micron particle sizes. By assuming a differential dust number density for a range in dust sizes and by making use of Langmuir probe data, the dust densities for certain lower limits in dust size distribution were estimated. In order to achieve the dust densities of micrometer and larger sized grains comparable to the ones reported in the literature, we show that the power law size distribution must hold down to at least 0.03 mu m such that the total differential number density is dominated by the smallest sub-micron sized grains. The total dust number density in Enceladus' plume is of the order of 10(2) cm(-3) reducing to 1 cm(-3) in the E-ring. The dust density for micrometer and larger sized grains is estimated to be about 10(-4) cm(-3) in the plume while it is about 10(-6)-10(-7) cm(-3) in the E-ring. Dust charge for micron sized grains is estimated to be about eight thousand electron charges reducing to below one hundred electron charges for 0.03 mu m sized grains. The effective dusty plasma Debye length is estimated and compared with intergrain distance as well as the electron Debye length. The maximum dust charging time of 1.4 h is found for 0.03 mu m sized grains just 1 min before the closest approach. The charging time decreases substantially in the plume where it is only a fraction of a second for 1 mu m sized grains, 1 s for 0.1 mu m sized grains and about 10 s for 0.03 mu m sized grains. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Shafiq, Muhammad; Wahlund, J. -E.; Morooka, M. W.] Swedish Inst Space Phys, SE-75121 Uppsala, Sweden. [Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Farrell, W. M.] NASA, Planetary Magnetospheres Lab, GSFC, Greenbelt, MD 20771 USA. RP Shafiq, M (reprint author), Swedish Inst Space Phys, Box 537, SE-75121 Uppsala, Sweden. EM mshafiq@irfu.se RI Farrell, William/I-4865-2013; OI Kurth, William/0000-0002-5471-6202 FU Swedish National Space Board (SNSB) FX The support from Swedish National Space Board (SNSB) for the RPWS/LP instrument on board the Cassini spacecraft is acknowledged. NR 40 TC 32 Z9 32 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD JAN PY 2011 VL 59 IS 1 BP 17 EP 25 DI 10.1016/j.pss.2010.10.006 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 710UF UT WOS:000286541800003 ER PT B AU Person, S Yang, GW Rungta, N Khurshid, S AF Person, Suzette Yang, Guowei Rungta, Neha Khurshid, Sarfraz GP ACM SIGPLAN TI Directed Incremental Symbolic Execution SO PLDI 11: PROCEEDINGS OF THE 2011 ACM CONFERENCE ON PROGRAMMING LANGUAGE DESIGN AND IMPLEMENTATION LA English DT Proceedings Paper CT 32nd ACM SIGPLAN Conference on Programming Language Design and Implementation (PLDI 11) CY JUN 04-08, 2011 CL San Jose, CA SP ACM SIGPLAN DE Program Differencing; Symbolic Execution; Software Evolution AB The last few years have seen a resurgence of interest in the use of symbolic execution - a program analysis technique developed more than three decades ago to analyze program execution paths. Scaling symbolic execution and other path-sensitive analysis techniques to large systems remains challenging despite recent algorithmic and technological advances. An alternative to solving the problem of scalability is to reduce the scope of the analysis. One approach that is widely studied in the context of regression analysis is to analyze the differences between two related program versions. While such an approach is intuitive in theory, finding efficient and precise ways to identify program differences, and characterize their effects on how the program executes has proved challenging in practice. In this paper, we present Directed Incremental Symbolic Execution (DiSE), a novel technique for detecting and characterizing the effects of program changes. The novelty of DiSE is to combine the efficiencies of static analysis techniques to compute program difference information with the precision of symbolic execution to explore program execution paths and generate path conditions affected by the differences. DiSE is a complementary technique to other reduction or bounding techniques developed to improve symbolic execution. Furthermore, DiSE does not require analysis results to be carried forward as the software evolves-only the source code for two related program versions is required. A case-study of our implementation of DiSE illustrates its effectiveness at detecting and characterizing the effects of program changes. C1 [Person, Suzette] NASA, Langley Res Ctr, Washington, DC 20546 USA. RP Person, S (reprint author), NASA, Langley Res Ctr, Washington, DC 20546 USA. EM suzette.person@nasa.gov; gyang@ece.utexas.edu; neha.s.rungta@nasa.gov; khurshid@ece.utexas.edu NR 39 TC 19 Z9 20 U1 0 U2 0 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 1515 BROADWAY, NEW YORK, NY 10036-9998 USA BN 978-1-4503-0663-8 PY 2011 BP 504 EP 515 PG 12 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BXZ12 UT WOS:000297656700044 ER PT J AU Shih, CY Nyquist, LE Reese, Y Misawa, K AF Shih, C. -Y. Nyquist, L. E. Reese, Y. Misawa, K. TI Sm-Nd and Rb-Sr studies of lherzolitic shergottite Yamato 984028 SO POLAR SCIENCE LA English DT Article DE Mars; Lherzolitic shergottite; Sm-Nd; Rb-Sr; Crystallization age AB The distribution pattern of the trace elements Rb, Sr, Nd and Sm for Yamato 984028 (Y984028) is consistent with its classification as a lherzolitic shergottite. The Sm-Nd mineral isochron of this lherzolitic shergottite defines its age to be 170 +/- 10 Ma for an initial epsilon(Nd) = +11.6 +/- 0.2. The corresponding Rb-Sr mineral isochron yields an identical age of 170 +/- 9 Ma and an initial Sr-87/Sr-86 = 0.710389 +/- 0.000029. The concordant Sm-Nd and Rb-Sr isochron ages suggest that Y984028 crystallized 170 +/- 7 Ma ago contemporaneously with five other lherzolitic shergottites and ten enriched basaltic and olivine-phyric shergottites. The age, Sr- and Nd- isotopic signatures further suggest that Y984028 and Y-793605, and also probably Y000097 could come from a single magmatic body. Using a two-stage evolution model, the time-averaged Rb-87/Sr-86-ratio for the mantle source of the parent magma of Y984028 is similar to 0.182, within the range of 0.178-0.182 that has been reported for other lherzolitic shergottites. The corresponding time-averaged Sm-147/Nd-144-ratio for the source mantle of its parent magma is super-chondritic at similar to 0.217, implying its source was a depleted mafic part of the Martian mantle similar to that of diabasic shergottite Northwest Africa (NWA) 1460. Rb, Sr, Sm and Nd distributions in Y984028 are likely produced by pyroxene and olivine accumulation, probably from a NWA 1460-like parental melt, in an intrusive magma body. (C) 2010 Elsevier B.V. and NIPR. All rights reserved. C1 [Shih, C. -Y.] ESCG Jacobs Sverdrup, Houston, TX 77258 USA. [Nyquist, L. E.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Reese, Y.] ESCG MEI Technol, Houston, TX 77058 USA. [Misawa, K.] Grad Univ Adv Studies SOKENDAI, Natl Inst Polar Res, Tachikawa, Tokyo 1908518, Japan. RP Shih, CY (reprint author), ESCG Jacobs Sverdrup, Mail Code JE-23,POB 58477, Houston, TX 77258 USA. EM chi-yu.shih-1@nasa.gov; laurence.e.nyquist@nasa.gov; young.reese-1@nasa.gov; misawa@nipr.ac.jp FU National Institute of Polar Research of Japan; NASA Cosmochemistry Program; NIPR Research Project Funds, P8 (Evolution of the Early Solar System Materials); [17540464] FX We appreciate two anonymous referees for their thorough reviews and comments which greatly improve the manuscript. We thank the National Institute of Polar Research of Japan for providing the Y984028 sample for this study and for its financial support for presenting the preliminary results at the 32nd Symposium on Antarctic Meteorites in Tokyo. Financial support for the isotopic studies was provided by funding from the NASA Cosmochemistry Program to L. Nyquist, a Grand-in-Aid for Scientific Research (No. 17540464) to K. Misawa, and by NIPR Research Project Funds, P8 (Evolution of the Early Solar System Materials). NR 49 TC 8 Z9 8 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1873-9652 EI 1876-4428 J9 POLAR SCI JI Polar Sci. PD JAN PY 2011 VL 4 IS 4 BP 515 EP 529 DI 10.1016/j.polar.2010.05.004 PG 15 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA V40AA UT WOS:000209450300002 ER PT J AU Dyar, MD Glotch, TD Lane, MD Wopenka, B Tucker, JM Seaman, SJ Marchand, GJ Klima, R Hiroi, T Bishop, JL Pieters, C Sunshine, J AF Dyar, M. D. Glotch, T. D. Lane, M. D. Wopenka, B. Tucker, J. M. Seaman, S. J. Marchand, G. J. Klima, R. Hiroi, T. Bishop, J. L. Pieters, C. Sunshine, J. TI Spectroscopy of Yamato 984028 SO POLAR SCIENCE LA English DT Article DE Y-984028; Reflectance spectroscopy; Thermal emission spectroscopy; Mossbauer spectroscopy; Raman spectroscopy; Transmission spectroscopy AB Comprehensive spectroscopic characterization of interior and exterior chips of the lherzolitic shergottite Y-984028 has been performed using results from six techniques. Data from UV-visible-near-IR reflectance spectra, thermal (mid-IR) emission spectra, attenuated total reflectance (ATR) spectra, transmission FTIR spectra, Raman microprobe spectra, and Mossbauer spectra of whole rock and mineral separates from this meteorite are integrated and compared. Five of these analytical techniques accurately determined the similar to Fo(65) composition of the olivine within +/- 10 mol%. Both transmission FTIR and ATR spectra show broad features near 3500 cm(-1) indicating the presence of OH/H2O that does not arise from surface water adsorption. The brown color of the Y-984028 olivine is likely due to the presence of nanophase metallic iron particles (npFe(0)) dispersed throughout the olivine during a major shock event on Mars. Y-984028 olivine also contains a significant amount of Fe3+, but this cannot be distinguished from Fe3+ that is present in pyroxene and possibly clay minerals. This meteorite and the nakhlite MIL03346 are the two most oxidized of the SNC meteorites studied to date, with Fe3+ contents consistent with high-temperature equilibration near the QFM oxygen buffer. (C) 2010 Elsevier B.V. and NIPR. All rights reserved. C1 [Dyar, M. D.; Tucker, J. M.; Marchand, G. J.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. [Glotch, T. D.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Lane, M. D.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Wopenka, B.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Wopenka, B.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Seaman, S. J.] Univ Massachusetts, Dept Geosci, Amherst, MA 01003 USA. [Klima, R.; Hiroi, T.; Pieters, C.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Bishop, J. L.] NASA, Ames Res Ctr, SETI Inst, Mountain View, CA 94043 USA. [Sunshine, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Dyar, MD (reprint author), Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA. EM mdyar@mtholyoke.edu FU NASA grant from Mars Fundamental Research Program [NNX07AR66G]; NASA grant [NNG06GJ31G] FX We thank the curators of the Antarctic Meteorite Research Center, National Institute of Polar Research, Japan for the loan of this sample. Helpful suggestions from two anonymous reviewers and the editor greatly improved this manuscript. We are grateful for support from NASA grant NNX07AR66G from the Mars Fundamental Research Program. Reflectance spectra were acquired using the NASA/Keck RELAB, a multi-user facility supported by NASA grant NNG06GJ31G. NR 46 TC 6 Z9 6 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1873-9652 EI 1876-4428 J9 POLAR SCI JI Polar Sci. PD JAN PY 2011 VL 4 IS 4 BP 530 EP 549 DI 10.1016/j.polar.2010.06.001 PG 20 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA V40AA UT WOS:000209450300003 ER PT J AU Hertzfeld, HR AF Hertzfeld, Henry R. BE Sadeh, E TI International Organizations in Civil Space Affairs SO POLITICS OF SPACE: A SURVEY, 1ST EDITION LA English DT Article; Book Chapter C1 [Hertzfeld, Henry R.] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Hertzfeld, Henry R.] NASA, Washington, DC USA. [Hertzfeld, Henry R.] Natl Sci Fdn, Arlington, VA 22230 USA. RP Hertzfeld, HR (reprint author), George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. NR 50 TC 1 Z9 1 U1 0 U2 0 PU ROUTLEDGE PI LONDON PA 11 NEW FETTER LANE, LONDON EC4P 4EE, ENGLAND BN 978-1-85743-419-4 PY 2011 BP 120 EP 142 PG 23 WC International Relations; Political Science SC International Relations; Government & Law GA BWE18 UT WOS:000293731000007 ER PT J AU Brice, CA AF Brice, Craig A. BE Allison, J Collins, P Spanos, G TI UNINTENDED CONSEQUENCES: HOW QUALIFICATION CONSTRAINS INNOVATION SO PROCEEDINGS OF THE 1ST WORLD CONGRESS ON INTEGRATED COMPUTATIONAL MATERIALS ENGINEERING (ICME) LA English DT Proceedings Paper CT 1st World Congress on Integrated Computational Materials Engineering (ICME) CY JUL 10-14, 2011 CL Seven Springs, PA SP The Minerals, Met, & Mat Soc, Met Soc Canadian Inst Min, Met & Petr, Brazilian Met, Mat & Minerals Soc, Mat Australia, Japan Inst Met, Iron & Steel Inst Japan, AF Mat Lab, Army Res Off, Natl Inst Stand & Technol, Natl Sci Fdn, Off Naval Res AB The development and implementation of new materials and manufacturing processes for aerospace application is often hindered by the high cost and long time span associated with current qualification procedures. The data requirements necessary for material and process qualification are extensive and often require millions of dollars and multiple years to complete. Furthermore, these qualification data can become obsolete for even minor changes to the processing route. This burden is a serious impediment to the pursuit of revolutionary new materials and more affordable processing methods for air vehicle structures. The application of integrated computational materials engineering methods to this problem can help to reduce the barriers to rapid insertion of new materials and processes. By establishing predictive capability for the development of microstructural features in relation to processing and relating this to critical property characteristics, a streamlined approach to qualification is possible. This paper critically examines the advantages and challenges to a modeling-assisted qualification approach for aerospace structural materials. An example of how this approach might apply towards the emerging field of additive manufacturing is discussed in detail. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Brice, CA (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 11 TC 2 Z9 2 U1 0 U2 3 PU JOHN WILEY & SONS PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER, W SUSSEX PO 19 8SQ, ENGLAND BN 978-0-47094-319-9 PY 2011 BP 241 EP 246 PG 6 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary SC Engineering; Materials Science GA BHZ84 UT WOS:000327096700034 ER PT B AU Duncan, CB Robison, DE Koelewyn, CL AF Duncan, Courtney B. Robison, David E. Koelewyn, Cynthia Lee GP INST NAVIGATION TI Software Defined GPS Receiver for International Space Station SO PROCEEDINGS OF THE 2011 INTERNATIONAL TECHNICAL MEETING OF THE INSTITUTE OF NAVIGATION LA English DT Proceedings Paper CT International Technical Meeting of the Institute of Navigation CY JAN 24-26, 2011 CL San Diego, CA AB JPL is providing a software defined radio (SDR) that will fly on the International Space Station (ISS) as part of the CoNNeCT project under NASA's SCaN program. The SDR consists of several modules including a Baseband Processor Module (BPM) and a GPS Module (GPSM). The BPM executes applications (waveforms) consisting of software components for the embedded SPARC processor and logic for two Virtex II Field Programmable Gate Arrays (FPGAs) that operate on data received from the GPSM. GPS waveforms on the SDR are enabled by an L-Band antenna, low noise amplifier (LNA), and the GPSM that performs quadrature downconversion at L1, L2, and L5. The GPS waveform for the JPL SDR will acquire and track L1 C/A, L2C, and L5 GPS signals from a CoNNeCT platform on ISS, providing the best GPS-based positioning of ISS achieved to date, the first use of multiple frequency GPS on ISS, and potentially the first L5 signal tracking from space. The system will also enable various radiometric investigations on ISS such as local multipath or ISS dynamic behavior characterization. In following the software-defined model, this work will create a highly portable GPS software and firmware package that can be adapted to another platform with the necessary processor and FPGA capability. This paper also describes ISS applications for the JPL CoNNeCT SDR GPS waveform, possibilities for future global navigation satellite system (GNSS) tracking development, and the applicability of the waveform components to other space navigation applications. C1 [Duncan, Courtney B.; Robison, David E.; Koelewyn, Cynthia Lee] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Duncan, CB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 21 TC 1 Z9 1 U1 0 U2 0 PU INST NAVIGATION PI WASHINGTON PA 815 15TH ST NW, STE 832, WASHINGTON, DC 20005 USA PY 2011 BP 982 EP 988 PG 7 WC Remote Sensing SC Remote Sensing GA BUY90 UT WOS:000290749900090 ER PT S AU Rizzi, SA Przekop, A Turner, T AF Rizzi, Stephen A. Przekop, Adam Turner, Travis BE DeRoeck, G Degrande, G Lombaert, G Muller, G TI On the Response of a Nonlinear Structure to High Kurtosis Non-Gaussian Random Loadings SO PROCEEDINGS OF THE 8TH INTERNATIONAL CONFERENCE ON STRUCTURAL DYNAMICS, EURODYN 2011 SE EURODYN-International Conference on Structural Dynamics LA English DT Proceedings Paper CT 8th International Conference on Structural Dynamics (EURODYN) CY JUL 04-06, 2011 CL Leuven, BELGIUM DE Nonlinear structural dynamics; Non-Gaussian random loading; Damping ID RANDOM VIBRATION AB This paper is a follow-on to recent work by the authors in which the response and high-cycle fatigue of a nonlinear structure subject to non-Gaussian loadings was found to vary markedly depending on the nature of the loading. There it was found that a non-Gaussian loading having a steady rate of short-duration, high-excursion peaks produced essentially the same response as would have been incurred by a Gaussian loading. In contrast, a non-Gaussian loading having the same kurtosis, but with bursts of high-excursion peaks was found to elicit a much greater response. This work is meant to answer the question of when consideration of a loading probability distribution other than Gaussian is important. The approach entailed nonlinear numerical simulation of a beam structure under Gaussian and non-Gaussian random excitations. Whether the structure responded in a Gaussian or non-Gaussian manner was determined by adherence to, or violations of, the Central Limit Theorem. Over a practical range of damping, it was found that the linear response to a non-Gaussian loading was Gaussian when the period of the system impulse response is much greater than the rate of peaks in the loading. Lower damping reduced the kurtosis, but only when the linear response was non-Gaussian. In the nonlinear regime, the response was found to be non-Gaussian for all loadings. The effect of a spring-hardening type of nonlinearity was found to limit extreme values and thereby lower the kurtosis relative to the linear response regime. In this case, lower damping gave rise to greater nonlinearity, resulting in lower kurtosis than a higher level of damping. C1 [Rizzi, Stephen A.; Turner, Travis] NASA, Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA. [Przekop, Adam] Analyt Serv & Mat Inc, Hampton, VA 23666 USA. RP Rizzi, SA (reprint author), NASA, Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA. EM Stephen.A.Rizzi@nasa.gov; Adam.Przekop@nasa.gov; Travis.L.Turner@nasa.gov NR 11 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN ASSOC STRUCTURAL DYNAMICS PI MUNICH PA C/O LEHRSTUHL BAUMECHANIK, TECHNISCHE UNIV MUNCHEN, ARCISSTRASSE 21, MUNICH, D-80290, GERMANY SN 2311-9020 BN 978-90-760-1931-4 J9 EURODYN PY 2011 BP 2697 EP 2704 PG 8 WC Engineering, Civil SC Engineering GA BE0RB UT WOS:000366660802107 ER PT B AU Chatterjee, A Plawsky, JL Wayner, PC Chao, DF Sicker, RJ Lorik, T Chestney, L Eustace, J Zoldak, J AF Chatterjee, Arya Plawsky, Joel L. Wayner, Peter C., Jr. Chao, David F. Sicker, Ronald J. Lorik, Tibor Chestney, Louis Eustace, John Zoldak, John GP ASME TI THE CONSTRAINED VAPOR BUBBLE EXPERIMENT - RESULTS FROM THE INTERNATIONAL SPACE STATION SO PROCEEDINGS OF THE ASME/JSME 8TH THERMAL ENGINEERING JOINT CONFERENCE 2011, VOL 1 PTS A AND B LA English DT Proceedings Paper CT 8th ASME/JSME Thermal Engineering Joint Conference CY MAR 13-17, 2011 CL Honolulu, HI SP Amer Soc Mech Engineers, Japan Soc Mech Engineers ID FIN AB The constrained vapor bubble (CVB) experiment is an experiment in thermal fluid science currently operating on the International Space Station. Flown as the first experiment on the Fluids Integrated Rack on the Destiny module of the US part of the space station, the experiment promises to provide new and exciting insights into the working of a wickless micro heat pipe in the micro-gravity environment. The CVB consists of a relatively simple setup - a quartz cuvette with sharp corners partially filled with pentane as the working fluid. Along with temperature and pressure measurements, the curvature of the pentane menisci formed at the corners of the cuvette can be determined using optical measurements. This is the first time the data collected in space environment is being presented to the public. The data shows that, while the performance of the CVB heat pipe is enhanced due to increased fluid flow, the loss of convection as a heat loss mechanism in the space environment, leads to some interesting consequences. We present some significant differences in the operating characteristics of the heat pipe between the space and Earth's gravity environments and show that this has important ramifications in designing effective radiators for the space environment. C1 [Chatterjee, Arya; Plawsky, Joel L.; Wayner, Peter C., Jr.] Rensselaer Polytech Inst, Troy, NY 12180 USA. [Chao, David F.; Sicker, Ronald J.] NASA Glenn Res Ctr, Cleveland, OH USA. [Lorik, Tibor; Chestney, Louis; Eustace, John; Zoldak, John] Zin Technol, Cleveland, OH USA. RP Chatterjee, A (reprint author), Rensselaer Polytech Inst, Troy, NY 12180 USA. FU NASA Glenn Research; National Aeronautics and Space Administration [NNX09AL98G] FX The authors wish to acknowledge NASA astronaut T J Creamer for contributing his time voluntarily for this project. We also acknowledge people from ZIN Technologies for their efforts. Also NASA Glenn Research supported this project through many years at NASA. We also would like to acknowledge the Lead Increment Scientist for increment 2324, for giving us the extra crew and operations time. This material is based on the work supported by the National Aeronautics and Space Administration under Grant No. NNX09AL98G. Any opinions, findings, and conclusions or recommendations expressed in this publication are those of the authors and do not necessarily reflect the view of NASA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-5454-9 PY 2011 BP 1319 EP + PG 4 WC Engineering, Mechanical SC Engineering GA BFH11 UT WOS:000319843000155 ER PT B AU Raj, R Kim, J McQuillen, J AF Raj, Rishi Kim, Jungho McQuillen, John GP ASME TI ON THE SCALING OF POOL BOILING HEAT FLUX WITH GRAVITY AND HEATER SIZE SO PROCEEDINGS OF THE ASME/JSME 8TH THERMAL ENGINEERING JOINT CONFERENCE 2011, VOL 1 PTS A AND B LA English DT Proceedings Paper CT 8th ASME/JSME Thermal Engineering Joint Conference CY MAR 13-17, 2011 CL Honolulu, HI SP Amer Soc Mech Engineers, Japan Soc Mech Engineers ID REDUCED GRAVITY; DISSOLVED-GAS; MICROGRAVITY; CONVECTION AB A framework for scaling pool boiling heat flux is developed using data from various heater sizes over a range of gravity levels. Boiling is buoyancy dominated for large heaters and/or high gravity conditions and the heat flux is heater size independent. The power law coefficient for gravity is a function of wall temperature. As the heater size or gravity level is reduced, a sharp transition in the heat flux is observed at a threshold value of L-h/L-c=2.1. Below this threshold value, boiling is surface tension dominated and the dependence on gravity is smaller. The gravity scaling parameter for the heat flux in the buoyancy dominated boiling regime developed in the previous work is updated to account for subcooling effect. Based on this scaling parameter and the transition criteria, a methodology for predicting heat flux in the surface tension dominated boiling regime, typically observed under low-gravity conditions, is developed. Given the heat flux at a reference gravity level and heater size, the current framework allows the prediction of heat flux at any other gravity level and/or heater size under similar experimental conditions. The prediction is validated using data at over a range of subcoolings (7 degrees C <= Delta T-sub <= 32.6 degrees C), heater sizes (2.1 mm <= I-h <= 7 mm), and dissolved gas concentrations (3 ppm <= c(g) <= 3500 ppm). The prediction errors are significantly smaller than those from correlations currently available in the literature. C1 [Raj, Rishi; Kim, Jungho] Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA. [McQuillen, John] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Kim, J (reprint author), Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA. EM kimjh@umd.edu NR 32 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-5454-9 PY 2011 BP 1777 EP + PG 4 WC Engineering, Mechanical SC Engineering GA BFH11 UT WOS:000319843000208 ER PT B AU Ashpis, DE Thurman, DR AF Ashpis, David E. Thurman, Douglas R. GP ASME TI TEST CONDITIONS FOR PERFORMANCE CHARACTERIZATION OF DIELECTRIC BARRIER DISCHARGE (DBD) PLASMA ACTUATORS FOR ACTIVE FLOW CONTROL IN JET ENGINES SO PROCEEDINGS OF THE ASME TURBO EXPO 2011, VOL 1 LA English DT Proceedings Paper CT ASME Turbo Expo 2011 CY JUN 06-10, 2011 CL Vancouver, CANADA SP ASME, Int Gas Turbine Inst ID PRESSURE TURBINE-BLADES; ENHANCED AERODYNAMICS; SEPARATION CONTROL AB Dielectric Barrier Discharge (DBD) plasma actuators for active flow control in the jet engine need to be tested in the laboratory to characterize their performance at flight operating conditions. DBD plasma actuators generate a wall-jet electronically by creating weakly ionized plasma, therefore their performance is affected by gas discharge properties, which in turn depend on the pressure and temperature at the actuator placement location. Characterization of actuators is initially performed in a laboratory chamber without external flow. It is usually impractical to simultaneously set engine pressures and temperatures in a chamber, and a simplified approach is desired. It is assumed that the plasma discharge depends only on the gas density. Other temperature effects are assumed to be negligible. Therefore, tests can be performed at room temperature with chamber pressure set to yield the same density as in engine operating flight conditions. Engine data was obtained from four generic engine models; 300-, 150-, and 50-Passenger (PAX) aircraft engines, and a military jet-fighter engine. The static and total pressure, temperature, and density distributions along the engine were calculated for sea-level takeoff and altitude cruise, and the chamber pressures needed to test the actuators were calculated. The results show that testing has to be performed over a wide range of pressures from 12.4 to 0.03 atrn, depending on the application. For example, if a DBD plasma actuator is to be placed at the compressor exit of a 300 PAX engine, it has to be tested at 12.4 atm for takeoff and 6 atm for cruise conditions. If it is to be placed at the low-pressure turbine, it has to be tested at 0.5 and 0.2 atm, respectively. These results have implications for the feasibility and design of DBD plasma actuators for jet engine flow control applications. In addition, the distributions of unit Reynolds number, Mach number, and velocity along the engine are provided. The engine models are non-proprietary and this information can be used for evaluation of other types of actuators and for other purposes. C1 [Ashpis, David E.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Ashpis, DE (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM ashpis@nasa.gov; drthurman@nasa.gov NR 39 TC 1 Z9 1 U1 0 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-5461-7 PY 2011 BP 389 EP 415 PG 27 WC Engineering, Mechanical SC Engineering GA BFO06 UT WOS:000320677300035 ER PT B AU Hendricks, ES AF Hendricks, Eric S. GP ASME TI DEVELOPMENT OF AN OPEN ROTOR CYCLE MODEL IN NPSS USING A MULTI-DESIGN POINT APPROACH SO PROCEEDINGS OF THE ASME TURBO EXPO 2011, VOL 1 LA English DT Proceedings Paper CT ASME Turbo Expo 2011 CY JUN 06-10, 2011 CL Vancouver, CANADA SP ASME, Int Gas Turbine Inst AB NASA's Environmentally Responsible Aviation Project and Subsonic Fixed Wing Project are focused on developing concepts and technologies which may enable dramatic reductions to the environmental impact of future generation subsonic aircraft [1][2]. The open rotor concept (also referred to as the Unducted Fan or advanced turboprop) may allow the achievement of this objective by reducing engine emissions and fuel consumption. To evaluate its potential impact, an open rotor cycle modeling capability is needed. This paper presents the initial development of an open rotor cycle model in the Numerical Propulsion System Simulation (NPSS) computer program which can then be used to evaluate the potential benefit of this engine. The development of this open rotor model necessitated addressing two modeling needs within NPSS. First, a method for evaluating the performance of counter-rotating propellers was needed. Therefore, a new counter-rotating propeller NPSS component was created. This component uses propeller performance maps developed from historic counter-rotating propeller experiments to determine the thrust delivered and power required. Second, several methods for modeling a counter-rotating power turbine within NPSS were explored. These techniques used several combinations of turbine components within NPSS to provide the necessary power to the propellers. Ultimately, a single turbine component with a conventional turbine map was selected. Using these modeling enhancements, an open rotor cycle model was developed in NPSS using a multi-design point approach. The multi-design point (MDP) approach improves the engine cycle analysis process by making it easier to properly size the engine to meet a variety of thrust targets throughout the flight envelope. A number of design points are considered including an aerodynamic design point, sea-level static, takeoff and top of climb. The development of this MDP model was also enabled by the selection of a simple power management scheme which schedules propeller blade angles with the freestream Mach number. Finally, sample open rotor performance results and areas for further model improvements are presented. C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP Hendricks, ES (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-5461-7 PY 2011 BP 441 EP 450 PG 10 WC Engineering, Mechanical SC Engineering GA BFO06 UT WOS:000320677300039 ER PT B AU Mital, SK Goldberg, RK Bonacuse, PJ AF Mital, Subodh K. Goldberg, Robert K. Bonacuse, Peter J. GP ASME TI TWO-DIMENSIONAL NONLINEAR FINITE ELEMENT ANALYSIS OF CMC MICROSTRUCTURES SO PROCEEDINGS OF THE ASME TURBO EXPO 2011, VOL 1 LA English DT Proceedings Paper CT ASME Turbo Expo 2011 CY JUN 06-10, 2011 CL Vancouver, CANADA SP ASME, Int Gas Turbine Inst DE CVI; SiC/SiC Composite; Microstructure; Porosity AB Detailed two-dimensional finite element analyses of the cross-sections of a model CVI (chemical vapor infiltrated) SiC/SiC (silicon carbide fiber in a silicon carbide matrix) ceramic matrix composites are performed. High resolution images of the cross-section of this composite material are generated using serial sectioning of the test specimens. These images are then used to develop very detailed finite element models of the cross-sections using the public domain software OOF2 (Object Oriented Analysis of Material Microstructures). Examination of these images shows that these microstructures have significant variability and irregularity. How these variabilities manifest themselves in the variability in effective properties as well as the stress distribution, damage initiation and damage progression is the overall objective of this work. Results indicate that even though the macroscopic stress-strain behavior of various sections analyzed is very similar, each section has a very distinct damage pattern when subjected to in-plane tensile loads and this damage pattern seems to follow the unique architectural and microstructural details of the analyzed sections. C1 [Mital, Subodh K.] Univ Toledo, NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Mital, SK (reprint author), Univ Toledo, NASA, Glenn Res Ctr, Mail Stop 49-7, Cleveland, OH 44135 USA. EM Subodh.K.Mital@nasa.gov; Robert.K.Goldberg@nasa.gov; Peter.J.Bonacuse@nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-5461-7 PY 2011 BP 491 EP 496 PG 6 WC Engineering, Mechanical SC Engineering GA BFO06 UT WOS:000320677300043 ER PT B AU Muller, H Hohensee, MA Yu, N AF Mueller, H. Hohensee, M. A. Yu, N. BE Kostelecky, VA TI MATTER-WAVE TESTS OF THE GRAVITATIONAL REDSHIFT IN SPACE SO PROCEEDINGS OF THE FIFTH MEETING ON CPT AND LORENTZ SYMMETRY LA English DT Proceedings Paper CT 5th Meeting on CPT and Lorentz Symmetry CY JUN 28-JUL 02, 2010 CL Indiana Univ, Bloomington, IN HO Indiana Univ ID BLOCH OSCILLATIONS; GRAVITY; ATOMS AB A recent measurement of the gravitational redshift was based on interference of matter waves. Operation in microgravity can improve it by a factor of 10(5) and, in some models, even 10(10). C1 [Mueller, H.; Hohensee, M. A.] Univ Calif Berkeley, Dept Phys, 366 Le Conte Hall, Berkeley, CA 94720 USA. [Yu, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Muller, H (reprint author), Univ Calif Berkeley, Dept Phys, 366 Le Conte Hall, Berkeley, CA 94720 USA. EM hm@berkeley.edu RI Mueller, Holger/E-3194-2015 FU David and Lucile Packard Foundation; Alfred P. Sloan Foundation; National Institute of Standards and Technology FX We thank S. Chu, S. Herrmann, J. Kollmeier, S.-Y. Lan, S. Ospelkaus, A. Peters, J. Phillips, and G. Tino for discussions. Support from the David and Lucile Packard Foundation, the Alfred P. Sloan Foundation and the National Institute of Standards and Technology is gratefully acknowledged. NR 9 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-981-4327-67-1 PY 2011 BP 6 EP 10 PG 5 WC Physics, Multidisciplinary; Physics, Particles & Fields SC Physics GA BG9ZT UT WOS:000394395200002 ER PT B AU Vasileiou, V AF Vasileiou, V. CA GBM Collaboration LAT Collaboration BE Kostelecky, VA TI CONSTRAINING LORENTZ INVARIANCE VIOLATION WITH FERMI SO PROCEEDINGS OF THE FIFTH MEETING ON CPT AND LORENTZ SYMMETRY LA English DT Proceedings Paper CT 5th Meeting on CPT and Lorentz Symmetry CY JUN 28-JUL 02, 2010 CL Indiana Univ, Bloomington, IN HO Indiana Univ ID GAMMA-RAY BURSTS; QUANTUM-GRAVITY AB One of the cornerstones of special relativity is the postulate that all observers measure exactly the same photon speeds independently of the photon energies. However, a hypothesized structure of spacetime may alter this conclusion at ultra-small length scales. Even a tiny energy-dependent variation in the speed of light may be revealed, when accumulated over cosmological light travel times, by high temporal-resolution measurements of sharp features in gamma-ray burst (GRB) lightcurves. We report the results of a study of the emission from GRB 090510 as detected by Fermi's LAT and GBM instruments that set unprecedented limits on the dependence of the speed of light on its energy. C1 [Vasileiou, V.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Greenbelt, MD 20771 USA. RP Vasileiou, V (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM vlasios.vasileiou@nasa.gov FU INAF in Italy; CNES in France; NASA in the United States; DRL in Germany FX The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. The Fermi GBM Collaboration acknowledges the support of NASA in the United States and DRL in Germany. NR 8 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-981-4327-67-1 PY 2011 BP 138 EP 142 PG 5 WC Physics, Multidisciplinary; Physics, Particles & Fields SC Physics GA BG9ZT UT WOS:000394395200027 ER PT J AU Nghiem, SV Neumann, G Clemente-Colon, P Rigor, IG Perovich, DK AF Nghiem, Son V. Neumann, Gregory Clemente-Colon, Pablo Rigor, Ignatius G. Perovich, Donald K. BE Chicco, G Nghiem, SV TI Arctic Perennial Sea Ice Crash of the 2000s and its Impacts SO PROCEEDINGS OF THE SECOND INTERNATIONAL CONFERENCE ON BIOENVIRONMENT, BIODIVERSITY AND RENEWABLE ENERGIES (BIONATURE 2011) LA English DT Proceedings Paper CT 2nd International Conference on Bioenvironment, Biodiversity and Renewable Energies (BIONATURE) CY MAY 22-27, 2011 CL Venice, ITALY SP IARIA DE Perennial sea ice loss; Polar Express; albedo; insolation; Arctic passages; tropospheric chemical changes. ID DEPLETION; CHEMISTRY; MERCURY; OZONE; SPRINGTIME; ATMOSPHERE AB Satellite and surface observations show that half of the extent of perennial sea ice in the Arctic Ocean has been lost in the decade of 2000s. Perennial sea ice is the class of old and thick ice important for the stability of the Arctic environment. Perennial ice extent set the record low in 2008 and has remained low as seen in updated satellite scatterometer data and surface drifting buoy measurements in 2011. The drastic decline of Arctic sea ice is far exceeding the worst-case projections from climate models of the Intergovernmental Panel on Climate Change Fourth Assessment Report. The important role of the Polar Express phenomenon has been identified, indicating dynamic and thermodynamic effects are combined to expedite the loss of perennial sea ice. Consequently, major impacts include decreases in Arctic surface albedo, increases in absorbed insolation, facilitation of sea-route opening, and changes in tropospheric chemical processes such as bromine explosion, ozone depletion, and mercury deposition that impact the biosphere. C1 [Nghiem, Son V.; Neumann, Gregory] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Clemente-Colon, Pablo] NOAA, Natl Ice Ctr, Washington, DC USA. [Rigor, Ignatius G.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA. [Perovich, Donald K.] US Army, Corps Engineers, Cold Reg Res & Engn Lab, Hanover, NH USA. RP Nghiem, SV (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Son.V.Nghiem@jpl.nasa.gov; Gregory.Neumann@jpl.nasa.gov; Pablo.Clemente-Colon@noaa.gov; ignatius@apl.washington.edu; Donald.K.Perovich@usace.army.mil FU National Aeronautics and Space Administration (NASA) Cryospheric Sciences Program FX The research carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, was supported by the National Aeronautics and Space Administration (NASA) Cryospheric Sciences Program. The statements, findings, conclusions, and recommendations in this paper are those of the author(s) and do not necessarily reflect the views of the National Oceanic and Atmospheric Administration or the Department of Commerce. NR 36 TC 0 Z9 0 U1 0 U2 0 PU IARIA XPS PRESS PI WILMINGTON PA PO BOX 7827, WILMINGTON, DE 19803 USA BN 978-1-61208-138-0 PY 2011 BP 38 EP 42 PG 5 WC Energy & Fuels; Engineering, Environmental SC Energy & Fuels; Engineering GA BH0GC UT WOS:000394874300008 ER PT J AU Balas, MJ Frost, SA AF Balas, Mark J. Frost, Susan A. BE Galis, A Dillenseger, B TI An Introduction to Evolving Systems: Adaptive Key Component Control with Persistent Disturbance Rejection SO PROCEEDINGS OF THE SEVENTH INTERNATIONAL CONFERENCE ON AUTONOMIC AND AUTONOMOUS SYSTEMS (ICAS 2011) LA English DT Proceedings Paper CT 7th International Conference on Autonomic and Autonomous Systems (ICAS) CY MAY 22-27, 2011 CL Venice, ITALY SP IARIA DE adaptive control; aerospace systems AB This paper presents an introduction to Evolving Systems, which are autonomously controlled subsystems which self-assemble into a new Evolved System with a higher purpose. Evolving Systems of aerospace structures often require additional control when assembling to maintain stability during the entire evolution process. This is the concept of Adaptive Key Component Control which operates through one specific component to maintain stability during the evolution. In addition this control must overcome persistent disturbances that occur while the evolution is in progress. We present theoretical results for the successful operation of Adaptive Key Component control in the presence of such disturbances and an illustrative example. C1 [Balas, Mark J.] Univ Wyoming, Elect & Comp Engn Dept, 1000 E Univ Ave, Laramie, WY 82071 USA. [Frost, Susan A.] NASA Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Balas, MJ (reprint author), Univ Wyoming, Elect & Comp Engn Dept, 1000 E Univ Ave, Laramie, WY 82071 USA. EM mbalas@uwyo.edu; susan.a.frost@nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 0 PU IARIA XPS PRESS PI WILMINGTON PA PO BOX 7827, WILMINGTON, DE 19803 USA BN 978-1-61208-134-2 PY 2011 BP 43 EP 50 PG 8 WC Automation & Control Systems; Computer Science, Cybernetics; Computer Science, Theory & Methods SC Automation & Control Systems; Computer Science GA BH0GG UT WOS:000394889900008 ER PT J AU Lu, T Pham, T Liao, J AF Lu, Thomas Pham, Timothy Liao, Jason BE Laddomada, M Pham, T TI Identification of Abnormal System Noise Temperature Patterns in Deep Space Network Antennas Using Neural Network Trained Fuzzy Logic SO PROCEEDINGS OF THE THIRD INTERNATIONAL CONFERENCE ON ADVANCES IN SATELLITE AND SPACE COMMUNICATIONS (SPACOMM 2011) LA English DT Proceedings Paper CT 3rd International Conference on Advances in Satellite and Space Communications (SPACOMM) CY APR 17-22, 2011 CL Budapest, HUNGARY SP IARIA DE Deep Space Network; Neural network training; Fuzzy logic; Pattern identification; System noise temperature; Link margin. AB This paper presents the development of a fuzzy logic function trained by an artificial neural network to classify the system noise temperature (SNT) of antennas in the NASA Deep Space Network (DSN). The SNT data were classified into normal, marginal, and abnormal classes. The irregular SNT pattern was further correlated with link margin and weather data. A reasonably good correlation is detected among high SNT, low link margin and the effect of bad weather; however we also saw some unexpected non-correlations which merit further study in the future. C1 [Lu, Thomas; Pham, Timothy; Liao, Jason] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Lu, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Thomas.Lu@jpl.nasa.gov; Timothy.Pham@jpl.nasa.gov; Jason.Liao@jpl.nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU IARIA XPS PRESS PI WILMINGTON PA PO BOX 7827, WILMINGTON, DE 19803 USA BN 978-1-61208-128-1 PY 2011 BP 35 EP 40 PG 6 WC Telecommunications SC Telecommunications GA BH0GA UT WOS:000394871800007 ER PT J AU Rapetti, D Allen, SW Mantz, A Ebeling, H AF Rapetti, David Allen, Steven W. Mantz, Adam Ebeling, Harald TI Testing General Relativity on Cosmic Scales with the Observed Abundance of Massive Clusters SO PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT LA English DT Article ID OBSERVATIONS COSMOLOGICAL INTERPRETATION; RELAXED GALAXY CLUSTERS; PROBE WMAP OBSERVATIONS; DARK ENERGY; OBSERVED GROWTH; ACCELERATING UNIVERSE; CONSTRAINTS AB Using observations of the growth of massive, X-ray flux-selected galaxy clusters, we obtain tight constraints on both the growth and expansion histories of the Universe. Our data set consists of 238 cluster detections from the ROSAT All-Sky Survey (RASS), and incorporates follow-up observations of 94 of those clusters from the Chandra X-ray Observatory and/or ROSAT. Using a new statistical framework that self-consistently produces simultaneous constraints on cosmology and X-ray scaling relations we account for survey biases, parameter degeneracies and the impact of systematic uncertainties to obtain improved constraints on departures from General Relativity (GR) on cosmological scales. We parametrize the linear growth rate of cosmic structure with a power law of the mean matter density to the growth index, gamma. Combining the X-ray cluster growth data with cluster gas-mass fraction (f(gas)), Type Ia supernovae (SNIa), baryon acoustic oscillations (BAO), and cosmic microwave background (CMB) data, we find a tight correlation between gamma and the normalization of the matter power spectrum, sigma(8). Allowing gamma and the dark energy equation of state parameter, w, to take any constant values, we find no evidence for departures from the standard paradigm, GR+ACDM (cosmological constant plus cold dark matter). Our results highlight the power of X-ray cluster studies to constrain cosmology. C1 [Rapetti, David] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Rapetti, David; Allen, Steven W.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Rapetti, David; Allen, Steven W.] SLAC Natl Accelerator Lab, Stanford, CA USA. [Mantz, Adam] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Ebeling, Harald] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Rapetti, D (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Blegdamsvej 17, DK-2100 Copenhagen, Denmark. EM drapetti@dark-cosmology.dk RI Rapetti, David/E-6032-2015 OI Rapetti, David/0000-0003-2196-6675 NR 24 TC 1 Z9 1 U1 0 U2 0 PU PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE PI KYOTO PA C/O KYOTO UNIV, YUKAWA HALL, KYOTO, 606-8502, JAPAN SN 0375-9687 J9 PROG THEOR PHYS SUPP JI Prog. Theor. Phys. Suppl. PY 2011 IS 190 BP 179 EP 187 PG 9 GA 853NI UT WOS:000297432600016 ER PT J AU Petrov, L Phillips, C Tzioumis, T Stansby, B Reynolds, C Bignall, HE Gulyaev, S Natusch, T Palmer, N Collett, D Reynolds, JE Amy, SW Wayth, R Tingay, SJ AF Petrov, Leonid Phillips, Chris Tzioumis, Tasso Stansby, Bruce Reynolds, Cormac Bignall, Hayley E. Gulyaev, Sergei Natusch, Tim Palmer, Neville Collett, David Reynolds, John E. Amy, Shaun W. Wayth, Randall Tingay, Steven J. TI First Geodetic Observations Using New VLBI Stations ASKAP-29 and WARK12M SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE instrumentation; interferometers - techniques; interferometric - reference systems ID BASE-LINE INTERFEROMETRY; SCIENCE; ASTROMETRY AB We report the results of a successful 7-hour 1.4 GHz Very Long Baseline Interferometry (VLBI) experiment using two new stations, ASKAP-29 located in Western Australia and WARK12M located on the North Island of New Zealand. This was the first geodetic VLBI observing session with the participation of these new stations. We have determined the positions of ASKAP-29 and WARK12M. Random errors on position estimates are 150-200mm for the vertical component and 40-50mm for the horizontal component. Systematic errors caused by the unmodeled ionosphere path delay may reach 1.3 m for the vertical component. C1 [Petrov, Leonid] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Greenbelt, MD 20771 USA. [Phillips, Chris; Tzioumis, Tasso; Reynolds, John E.; Amy, Shaun W.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Stansby, Bruce; Reynolds, Cormac; Bignall, Hayley E.; Wayth, Randall; Tingay, Steven J.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Gulyaev, Sergei; Natusch, Tim] Auckland Univ Technol, Inst Radio Astron & Space Res, Auckland 1142, New Zealand. [Palmer, Neville] GNS Sci, Lower Hutt 5040, New Zealand. [Collett, David] Land Informat New Zealand, Wellington 6145, New Zealand. RP Petrov, L (reprint author), NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Code 610-2, Greenbelt, MD 20771 USA. EM Leonid.Petrov@lpetrov.net RI Wayth, Randall/B-2444-2013; Bignall, Hayley/B-2867-2013; Tingay, Steven/B-5271-2013; Reynolds, Cormac/B-5635-2013 OI Wayth, Randall/0000-0002-6995-4131; Bignall, Hayley/0000-0001-6247-3071; Reynolds, Cormac/0000-0002-8978-0626 FU Commonwealth Government of Australia; Western Australian State government; Commonwealth of Australia; Western Australian Government; Australian Research Collaboration Service (ARCS) FX This work uses data obtained from the MRO, jointly funded by the Commonwealth Government of Australia and the Western Australian State government. The MRO is managed by the CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. The Long Baseline Array is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The International Centre for Radio Astronomy Research is a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. iVEC is a joint venture between CSIRO, Curtin University, Edith Cowan University, The University of Western Australia and Murdoch University and is supported by the Western Australian Government. SJT is a Western Australian Premier's Research Fellow, funded by the Western Australian government. This project was supported in part by the Australian Research Collaboration Service (ARCS). We used in our work the dataset MAI6NPANA provided by the NASA/Global Modeling and Assimilation Office (GMAO) in the framework of the MERRA atmospheric reanalysis project. NR 37 TC 5 Z9 6 U1 0 U2 1 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1323-3580 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PY 2011 VL 28 IS 2 BP 107 EP 116 DI 10.1071/AS10048 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 780WH UT WOS:000291889600002 ER PT J AU Hinkley, S Oppenheimer, BR Zimmerman, N Brenner, D Parry, IR Crepp, JR Vasisht, G Ligon, E King, D Soummer, R Sivaramakrishnan, A Beichman, C Shao, M Roberts, LC Bouchez, A Dekany, R Pueyo, L Roberts, JE Lockhart, T Zhai, CX Shelton, C Burruss, R AF Hinkley, Sasha Oppenheimer, Ben R. Zimmerman, Neil Brenner, Douglas Parry, Ian R. Crepp, Justin R. Vasisht, Gautam Ligon, Edgar King, David Soummer, Remi Sivaramakrishnan, Anand Beichman, Charles Shao, Michael Roberts, Lewis C., Jr. Bouchez, Antonin Dekany, Richard Pueyo, Laurent Roberts, Jennifer E. Lockhart, Thomas Zhai, Chengxing Shelton, Chris Burruss, Rick TI A New High Contrast Imaging Program at Palomar Observatory SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID INTEGRAL FIELD SPECTROSCOPY; EXTREME ADAPTIVE OPTICS; POINT-SPREAD FUNCTIONS; HIGH STREHL RATIO; EXTRASOLAR PLANET; SPECKLE NOISE; GIANT PLANETS; LYOT CORONAGRAPHS; DYNAMIC-RANGE; HR 8799 AB We describe a new instrument that forms the core of a long-term high contrast imaging program at the 200 inch (5 m) Hale Telescope at Palomar Observatory. The primary scientific thrust is to obtain images and low-resolution spectroscopy of brown dwarfs and young exoplanets of several Jupiter masses in the vicinity of stars within 50 pc of the Sun. The instrument is a microlens-based integral field spectrograph integrated with a diffraction-limited, apodized-pupil Lyot coronagraph. The entire combination is mounted behind the Palomar adaptive optics (AO) system. The spectrograph obtains imaging in 23 channels across the J and H bands (1.06-1.78 mu m). The image plane of our spectrograph is subdivided by a 200 x 200 element microlens array with a plate scale of 19.2 mas per microlens, critically sampling the diffraction-limited point-spread function at 1.06 mu m. In addition to obtaining spectra, this wavelength resolution allows suppression of the chromatically dependent speckle noise, which we describe. In addition, we have recently installed a novel internal wave front calibration system that will provide continuous updates to the AO system every 0.5-1.0 minutes by sensing the wave front within the coronagraph. The Palomar AO system is undergoing an upgrade to a much higher order AO system (PALM-3000): a 3388-actuator tweeter deformable mirror working together with the existing 241-actuator mirror. This system, the highest-resolution AO corrector of its kind, will allow correction with subapertures as small as 8.1 cm at the telescope pupil using natural guide stars. The coronagraph alone has achieved an initial dynamic range in the H band of 2 x 10(-4) at 1 '', without speckle noise suppression. We demonstrate that spectral speckle suppression provides a factor of 10-20 improvement over this, bringing our current contrast at 1 '' to similar to 2 x 10(-5). This system is the first of a new generation of apodized-pupil coronagraphs combined with high-order adaptive optics and integral field spectrographs (e. g., GPI, SPHERE, HiCIAO), and we anticipate that this instrument will make a lasting contribution to high-contrast imaging in the Northern Hemisphere for years. C1 [Hinkley, Sasha; Crepp, Justin R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Oppenheimer, Ben R.; Zimmerman, Neil; Brenner, Douglas; Sivaramakrishnan, Anand] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Zimmerman, Neil] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Parry, Ian R.; King, David] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Vasisht, Gautam; Ligon, Edgar; Shao, Michael; Roberts, Lewis C., Jr.; Pueyo, Laurent; Roberts, Jennifer E.; Lockhart, Thomas; Zhai, Chengxing; Shelton, Chris; Burruss, Rick] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Soummer, Remi; Sivaramakrishnan, Anand] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sivaramakrishnan, Anand] SUNY Stony Brook, Stony Brook, NY USA. [Beichman, Charles] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Bouchez, Antonin; Dekany, Richard] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. RP Hinkley, S (reprint author), CALTECH, Dept Astron, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. OI Zimmerman, Neil/0000-0001-5484-1516 FU NASA; National Science Foundation [AST-0908497, AST-0804417, 0334916, 0215793, 0520822]; National Aeronautics and Space Administration under the Terrestrial Planet Finder Foundation [NNG05GJ86G]; National Science Foundation Science and Technology Center for Adaptive Optics; AST-9876783; internal Research and Technology Development funds FX This work was performed in part under contract with the California Institute of Technology, funded by NASA through the Sagan Fellowship Program. A portion of this work is supported by the National Science Foundation under grant nos. AST-0908497, AST-0804417, 0334916, 0215793, and 0520822, as well as grant NNG05GJ86G from the National Aeronautics and Space Administration under the Terrestrial Planet Finder Foundation Science Program. This work has been partially supported by the National Science Foundation Science and Technology Center for Adaptive Optics, managed by the University of California. Santa Cruz, under cooperative agreement AST-9876783. A portion of the research in this article was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and was funded by internal Research and Technology Development funds. We are grateful to the efforts of Derek Ives, Stewart McLay, Andrew Vick, and the other skilled engineers at the UK Astronomy Technology Centre for their configuration of the detector control software. We also are thankful to Chris Shelton for help in the design of the Atmospheric Dispersion Correcting prisms. Our team is also grateful to the Cordelia Corporation, Hilary and Ethel Lipsitz, the Vincent Astor Fund, Judy Vale, and the Plymouth Hill Foundation. NR 91 TC 98 Z9 98 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JAN PY 2011 VL 123 IS 899 BP 74 EP 86 DI 10.1086/658163 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 711NU UT WOS:000286599500007 ER PT J AU Anderson, BH Haller, HS AF Anderson, Bernhard H. Haller, Harold S. TI Combining Computational Fluid Dynamics Analysis Data with Experimentally Measured Data SO QUALITY ENGINEERING LA English DT Article DE CFD; D-optimal; data scaling; DOE; interlocking DOE; multiple regression; scale-up AB This article presents an approach to reducing the time and cost of experimentation in large wind tunnels, such as the 10 x 10 ft. supersonic wind tunnel at NASA Glenn Research Center, by combining computer simulations of test models from Reynolds averaged Navier-Stokes analysis with small sets of wind tunnel data. To demonstrate the viability of the approach, the impact of microramp flow control on the shock wave boundary layer interaction using paired sets of data from both computational fluid dynamics (CFD) analysis and experimental measurements was compared. By combining the CFD results consisting of 15 central composite face-centered (CCF) simulations with a smaller subset of four/five experimental wind tunnel cases, augmented, interlocking combined data sets were generated from which models were developed that allow the prediction of wind tunnel results. No statistically significant differences were found to exist between the predictions from models generated using the augmented interlocking data sets and the models generated using the complete set of 15 wind tunnel cases based on a paired t-test. From an engineering perspective, the same optimal microramp configuration was obtained using models derived from the combined data set as obtained with the complete set of experimental wind tunnel data. C1 [Haller, Harold S.] Case Western Reserve Univ, Dept Stat, Ctr Stat Consulting, Cleveland, OH 44106 USA. [Anderson, Bernhard H.] NASA, John Glenn Res Ctr, Cleveland, OH USA. [Haller, Harold S.] Real World Qual Syst, Cleveland, OH USA. RP Haller, HS (reprint author), Case Western Reserve Univ, Dept Stat, Ctr Stat Consulting, 10900 Euclid Ave, Cleveland, OH 44106 USA. EM Halhaller@aol.com NR 17 TC 1 Z9 2 U1 0 U2 0 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0898-2112 EI 1532-4222 J9 QUAL ENG JI Qual. Eng. PY 2011 VL 23 IS 1 BP 46 EP 58 DI 10.1080/08982112.2010.505221 PG 13 WC Engineering, Industrial; Statistics & Probability SC Engineering; Mathematics GA 879MY UT WOS:000299335200005 ER PT S AU Erkmen, BI Birnbaum, KM Moision, BE Dolinar, SJ AF Erkmen, Baris I. Birnbaum, Kevin M. Moision, Bruce E. Dolinar, Samuel J. BE Meyers, RE Shih, Y Deacon, KS TI The Dolinar receiver in an information theoretic framework SO QUANTUM COMMUNICATIONS AND QUANTUM IMAGING IX SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Quantum Communications and Quantum Imaging IX CY AUG 24-25, 2011 CL San Diego, CA SP SPIE ID CAPACITY; CHANNEL AB Optical communication at the quantum limit requires that measurements on the optical field be maximally informative, but devising physical measurements that accomplish this objective has proven challenging. The Dolinar receiver exemplifies a rare instance of success in distinguishing between two coherent states: an adaptive local oscillator is mixed with the signal prior to photodetection, which yields an error probability that meets the Helstrom lower bound with equality. Here we apply the same local-oscillator-based architecture with an information-theoretic optimization criterion. We begin with analysis of this receiver in a general framework for an arbitrary coherent-state modulation alphabet, and then we concentrate on two relevant examples. First, we study a binary antipodal alphabet and show that the Dolinar receiver's feedback function not only minimizes the probability of error, but also maximizes the mutual information. Next, we study ternary modulation consisting of antipodal coherent states and the vacuum state. We derive an analytic expression for a near-optimal local-oscillator feedback function, and, via simulation, we determine its photon information efficiency (PIE). We provide the PIE versus dimensional information efficiency (DIE) trade-off curve and show that this modulation and the our receiver combination performs universally better than (generalized) on-off keying plus photon-counting, although, the advantage asymptotically vanishes as the bits-per-photon diverges towards infinity. C1 [Erkmen, Baris I.; Birnbaum, Kevin M.; Moision, Bruce E.; Dolinar, Samuel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Erkmen, BI (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM baris.i.erkmen@jpl.nasa.gov NR 15 TC 1 Z9 1 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-773-5 J9 PROC SPIE PY 2011 VL 8163 AR 81630U DI 10.1117/12.893158 PG 15 WC Optics; Physics, Applied SC Optics; Physics GA BXZ20 UT WOS:000297671600020 ER PT S AU Forouhar, S Frez, C Franz, KJ Ksendzov, A Qiu, Y Soibel, KA Chen, J Hosoda, T Kipshidze, G Shterengas, L Belenky, G AF Forouhar, S. Frez, C. Franz, K. J. Ksendzov, A. Qiu, Y. Soibel, K. A. Chen, J. Hosoda, T. Kipshidze, G. Shterengas, L. Belenky, G. BE Razeghi, M Sudharsanan, R Brown, GJ TI Low power consumption lasers for next generation miniature optical spectrometers for trace gas analysis SO QUANTUM SENSING AND NANOPHOTONIC DEVICES VIII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Quantum Sensing and Nanophotonic Devices VIII CY JAN 23-27, 2011 CL San Francisco, CA SP SPIE AB The air quality of any manned spacecraft needs to be continuously monitored in order to safeguard the health of the crew. Air quality monitoring grows in importance as mission duration increases. Due to the small size, low power draw, and performance reliability, semiconductor laser-based instruments are viable candidates for this purpose. Achieving a minimum instrument size requires lasers with emission wavelength coinciding with the absorption of the fundamental absorption lines of the target gases, which are mostly in the 3.0-5.0 mu m wavelength range. In this paper we report on our progress developing high wall plug efficiency type-I quantum-well GaSb-based diode lasers operating at room temperatures in the spectral region near 3.0-3.5 mu m and quantum cascade (QC) lasers in the 4.0-5.0 mu m range. These lasers will enable the development of miniature, low-power laser spectrometers for environmental monitoring of the spacecraft. C1 [Forouhar, S.; Frez, C.; Franz, K. J.; Ksendzov, A.; Qiu, Y.; Soibel, K. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Forouhar, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 TC 0 Z9 0 U1 0 U2 6 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-482-6 J9 PROC SPIE PY 2011 VL 7945 AR 79450M DI 10.1117/12.871565 PG 4 WC Nanoscience & Nanotechnology; Optics SC Science & Technology - Other Topics; Optics GA BWE00 UT WOS:000293695800017 ER PT S AU Champion, DJ Hobbs, GB Manchester, RN Edwards, RT Backer, DC Bailes, M Bhat, NDR Burke-Spolaor, S Coles, W Demorest, PB Ferdman, RD Folkner, WM Hotan, AW Kramer, M Lommen, AN Nice, DJ Purver, MB Sarkissian, JM Stairs, IH van Straten, W Verbiest, JPW Yardley, DRB AF Champion, D. J. Hobbs, G. B. Manchester, R. N. Edwards, R. T. Backer, D. C. Bailes, M. Bhat, N. D. R. Burke-Spolaor, S. Coles, W. Demorest, P. B. Ferdman, R. D. Folkner, W. M. Hotan, A. W. Kramer, M. Lommen, A. N. Nice, D. J. Purver, M. B. Sarkissian, J. M. Stairs, I. H. van Straten, W. Verbiest, J. P. W. Yardley, D. R. B. BE Burgay, M DAmico, ND Esposito, P Pellizzoni, A Possenti, A TI Measuring the mass of solar system planets using pulsar timing SO RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Radio Pulsars - An Astrophysical Key to Unlock the Secrets of the Universe CY OCT 10-15, 2010 CL Chia, ITALY SP INAF-Osservatorio Astronomico Cagliari, Sardinia Radio Telescope Board, Assoc Cefalu & Astron DE planets and satellites: general; planets and satellites: individual (Jupiter); pulsars: general ID GRAVITY-FIELD; TRACKING DATA; EPHEMERIS; PACKAGE; TEMPO2; MODEL AB High-precision pulsar timing relies on a solar system ephemeris in order to convert times of arrival (TOAs) of pulses measured at an observatory to the solar system barycenter. Any error in the conversion to the barycentric TOAs leads to a systematic variation in the observed timing residuals; specifically, an incorrect planetary mass leads to a predominantly sinusoidal variation having a period and phase associated with the planet's orbital motion about the Sun. By using an array of pulsars (PSRs J0437-4715, J1744-1134, J1857+0943, Jl 909-3744), the masses of the planetary systems from Mercury to Saturn have been determined. These masses are consistent with the best-known masses determined by spacecraft observations, with the mass of the Jovian system, 9.547921(2)x 10(-4) M-circle dot, being significantly more accurate than the mass determined from the Pioneer and Voyager spacecraft, and consistent with but less accurate than the value from the Galileo spacecraft. While spacecraft are likely to produce the most accurate measurements for individual solar system bodies, the pulsar technique is sensitive to planetary system masses and has the potential to provide the most accurate values of these masses for some planets. C1 [Champion, D. J.; Hobbs, G. B.; Manchester, R. N.; Edwards, R. T.; Burke-Spolaor, S.; Nice, D. J.; Sarkissian, J. M.; Yardley, D. R. B.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. [Champion, D. J.; Kramer, M.; Verbiest, J. P. W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Edwards, R. T.] Kilmore Int Sch, Hawthorn, Vic 3764, Australia. [Backer, D. C.] Univ Calif Berkeley, Dept Astron, Radio Astron Lab, Berkeley, CA 94720 USA. [Bailes, M.; Bhat, N. D. R.; Burke-Spolaor, S.] Swinburne Univ Technol, Hawthorn, Vic 3122, Australia. [Coles, W.] Univ Calif San Diego, Dept Elect & Comp Engn, San Diego, CA USA. [Demorest, P. B.] Natl Radio Astron Observ, Charlottesville, VA 22901 USA. [Ferdman, R. D.; Purver, M. B.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Folkner, W. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hotan, A. W.] Curtin Univ, Curie Inst Radio Astron, Bentley, WA 6102, Australia. [Lommen, A. N.] Franklin & Marshall Coll, Lancaster, PA 17604 USA. [Nice, D. J.] Lafayette Coll, Dept Phys, Easton, PA 18042 USA. [Stairs, I. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Yardley, D. R. B.] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia. RP Champion, DJ (reprint author), CSIRO Astron & Space Sci, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. RI Bhat, Ramesh/B-7396-2013; OI Champion, David/0000-0003-1361-7723; Nice, David/0000-0002-6709-2566; van Straten, Willem/0000-0003-2519-7375 FU Australian Research Council Federation Fellowship [FF0348478]; Australian Research Council [DP0878388]; NSF [AST-0647820]; National Science Foundation [AST-0748580]; NSERC Discovery; Commonwealth of Australia FX We thank R. A. Jacobson for useful information about the planetary mass determinations, and F. A. Jenet, S. Oslowski, E. Splaver, K. Xilouris, and X. P. You for assistance with the observations and analysis. We also thank the referee for constructive comments. This work is undertaken as part of the Parkes Pulsar Timing Array project which was supported by R.N.M.s Australian Research Council Federation Fellowship (FF0348478). G.H. is the recipient of an Australian Research Council QEII Fellowship (DP0878388), D.N. is the recipient of an NSF grant (AST-0647820) and A.L. is the recipient of a National Science Foundation CAREER award (AST-0748580). Pulsar research at UBC is funded by an NSERC Discovery Grant. 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 the Commonwealth Scientific and Industrial Research Organisation. NR 18 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0915-6 J9 AIP CONF PROC PY 2011 VL 1357 BP 93 EP + DI 10.1063/1.3615087 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BXF95 UT WOS:000295993400023 ER PT S AU Esposito, P Rea, N Turolla, R Israel, GL Zane, S Stella, L Kouveliotou, C Mereghetti, S Tiengo, A Gotz, D Gogus, E AF Esposito, P. Rea, N. Turolla, R. Israel, G. L. Zane, S. Stella, L. Kouveliotou, C. Mereghetti, S. Tiengo, A. Goetz, D. Gogus, E. BE Burgay, M DAmico, ND Esposito, P Pellizzoni, A Possenti, A TI SGR 0418+5729: a low-magnetic-field magnetar SO RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Radio Pulsars - An Astrophysical Key to Unlock the Secrets of the Universe CY OCT 10-15, 2010 CL Chia, ITALY SP INAF-Osservatorio Astronomico Cagliari, Sardinia Radio Telescope Board, Assoc Cefalu & Astron DE pulsars: individual: SGR 0418+5729; X-rays: stars; stars: neutron ID SOFT GAMMA-REPEATERS; X-RAY; NEUTRON-STARS; RADIATIVE MECHANISM; RADIO PULSAR; EMISSION AB Soft gamma-ray repeaters and anomalous X-ray pulsars are a small (but growing) group of X-ray sources characterized by the emission of short bursts and by a large variability in their persistent flux. They are believed to be magnetars, i.e. neutron stars powered by extreme magnetic fields (10(14)-10(15) G). We found evidence for a magnetar with a low magnetic field, SGR 0418+5729, recently detected after it emitted bursts similar to those of soft gamma-ray repeaters. New X-ray observations show that its dipolar magnetic field cannot be greater than 8 x 10(12) G, well in the range of ordinary radio pulsars, implying that a high surface dipolar magnetic field is not necessarily required for magnetar-like activity. The magnetar population may thus include objects with a wider range of magnetic-field strengths, ages and evolutionary stages than observed so far. C1 [Esposito, P.] INAF Osservatorio Astron Cagliari, Cagliari, Italy. [Rea, N.] Inst Ciences Espai CSIC IEEC, Barcelona, Spain. [Turolla, R.] Univ Padua, Dipartimento Fis Galileo Gali, Padua, Italy. [Turolla, R.; Zane, S.] UCL, Mullard Space Sci Lab, Dorking, Surrey, England. [Israel, G. L.; Stella, L.] INAF Osservatorio Astron Roma, Rome, Italy. [Kouveliotou, C.] NASA Marshall Space Flight Ctr, Huntsville, AL 35811 USA. [Mereghetti, S.; Tiengo, A.] INAF Ist Astrofisica Spaziale Fis Cosmica Mila, Milan, Italy. [Goetz, D.] AIM, CEA DSM, CNRS UPD, Gif Sur Yvette, France. [Gogus, E.] Sabanic Univ, Istanbul, Turkey. RP Esposito, P (reprint author), INAF Osservatorio Astron Cagliari, Cagliari, Italy. OI Israel, GianLuca/0000-0001-5480-6438; Tiengo, Andrea/0000-0002-6038-1090; MEREGHETTI, SANDRO/0000-0003-3259-7801; Esposito, Paolo/0000-0003-4849-5092; Rea, Nanda/0000-0003-2177-6388 NR 19 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0915-6 J9 AIP CONF PROC PY 2011 VL 1357 BP 181 EP + DI 10.1063/1.3615111 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BXF95 UT WOS:000295993400047 ER PT S AU Harding, AK Muslimov, AG AF Harding, Alice K. Muslimov, Alex G. BE Burgay, M DAmico, ND Esposito, P Pellizzoni, A Possenti, A TI Pair Cascades and Deathlines in Magnetic Fields with Offset Polar Caps SO RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Radio Pulsars - An Astrophysical Key to Unlock the Secrets of the Universe CY OCT 10-15, 2010 CL Chia, ITALY SP INAF-Osservatorio Astronomico Cagliari, Sardinia Radio Telescope Board, Assoc Cefalu & Astron DE Neutron stars:pulsars ID LARGE-AREA TELESCOPE; MILLISECOND PULSARS; RAY-EMISSION; CONSTRAINTS; RADIATION; FRONTS; MODELS; RADIO AB We present results of electron-positron pair cascade simulations in a dipole magnetic field whose polar cap is offset from the dipole axis. In such a field geometry, the polar cap is displaced a small fraction of the neutron star radius from the star symmetry axis and the field line radius of curvature is modified. Using the modified parallel electric field near the offset polar cap, we simulate pair cascades to determine the pair deathlines and pair multiplicities as a function of the offset. We find that the pair multiplicity can change dramatically with a modest offset, with a significant increase on one side of the polar cap. Lower pair deathlines allow a larger fraction of the pulsar population, that include old and millisecond pulsars, to produce cascades with high multiplicity. The results have some important implications for pulsar particle production, high-energy emission and cosmic-ray contribution. C1 [Harding, Alice K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Muslimov, Alex G.] Univ Space Res Assoc, CRESST, Columbia, MD 21044 USA. RP Harding, AK (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RI Harding, Alice/D-3160-2012 NR 13 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0915-6 J9 AIP CONF PROC PY 2011 VL 1357 BP 221 EP + DI 10.1063/1.3615121 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BXF95 UT WOS:000295993400057 ER PT S AU Celik, O Johnson, TJ AF Celik, O. Johnson, T. J. CA Fermi LAT Collaboration BE Burgay, M DAmico, ND Esposito, P Pellizzoni, A Possenti, A TI On the Phase-Averaged Spectrum of Pulsars and Shape of Their Cutoffs SO RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Radio Pulsars - An Astrophysical Key to Unlock the Secrets of the Universe CY OCT 10-15, 2010 CL Chia, ITALY SP INAF-Osservatorio Astronomico Cagliari, Sardinia Radio Telescope Board, Assoc Cefalu & Astron DE gamma rays:observations; pulsars ID FERMI-LAT OBSERVATIONS; LARGE-AREA TELESCOPE; VELA PULSAR; SLOT GAPS; EMISSION; RADIATION AB All gamma-ray pulsars exhibit an exponential cutoff in their spectra and for bright pulsars the statistics are sufficiently high to study the detailed shape of the cutoff. The phase-averaged spectra of some pulsars exhibit a sub-exponential cutoff, not predicted by any single physical mechanism. Further studies clarified that this gentler average cutoff is a consequence of having significant variations of the cutoff energy in the phase-resolved spectrum. In conclusion, the phase-averaged spectrum of a pulsar is not a physical quantity to test high-energy emission models. C1 [Celik, O.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celik, O.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Johnson, T. J.] Univ Maryland, Dept Phys & Astron, College Pk, MD 20742 USA. RP Celik, O (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Ozlem.Celik-1@nasa.gov NR 12 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0915-6 J9 AIP CONF PROC PY 2011 VL 1357 BP 225 EP + DI 10.1063/1.3615122 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BXF95 UT WOS:000295993400058 ER PT S AU Guillemot, L Cognard, I Johnson, TJ Venter, C Harding, AK AF Guillemot, L. Cognard, I. Johnson, T. J. Venter, C. Harding, A. K. CA Fermi LAT Collaboration Pulsar Timing Consortium Pulsar Search Consortium BE Burgay, M DAmico, ND Esposito, P Pellizzoni, A Possenti, A TI Multiwavelength analysis of four millisecond pulsars SO RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Radio Pulsars - An Astrophysical Key to Unlock the Secrets of the Universe CY OCT 10-15, 2010 CL Chia, ITALY SP INAF-Osservatorio Astronomico Cagliari, Sardinia Radio Telescope Board, Assoc Cefalu & Astron DE gamma rays: observations; pulsars: millisecond; pulsars: individual (B1937+21 B1957+20, J2017+0603, J2302+4442) ID LARGE-AREA TELESCOPE AB Radio timing observations of millisecond pulsars (MSPs) in support of Fermi LAT observations of the gamma-ray sky enhance the sensitivity of high-energy pulsation searches. With contemporaneous ephemerides we have detected gamma-ray pulsations from PSR B1937+21, the first MSP ever discovered, and B1957+20, the first known black-widow system. The two MSPs share a number of properties: they are energetic and distant compared to other gamma-ray MSPs, and both of them exhibit aligned radio and gamma-ray emission peaks, indicating co-located emission regions in the outer magnetosphere of the pulsars. However, radio observations are also crucial for revealing MSPs in Fermi unassociated sources. In a search for radio pulsations at the position of such unassociated sources, the Nancay Radio Telescope discovered two MSPs, PSRs J2017+0603 and J2302+4442, increasing the sample of known Galactic disk MSPs. Subsequent radio timing observations led to the detection of gamma-ray pulsations from these two MSPs as well. We describe multiwavelength timing and spectral analysis of these four pulsars, and the modeling of their gamma-ray light curves in the context of theoretical models. C1 [Guillemot, L.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Cognard, I.] CNRS, LPCE, UMR, F-45071 Orleans, France. [Johnson, T. J.] Univ Maryland, Dept Phys & Astron, College Pk, MD 20742 USA. [Venter, C.] Northwest Univ, Space Res Ctr, Potchefstroom 2520, South Africa. [Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Guillemot, L (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM guillemo@mpifr-bonn.mpg.de RI Harding, Alice/D-3160-2012; OI Venter, Christo/0000-0002-2666-4812 NR 13 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0915-6 J9 AIP CONF PROC PY 2011 VL 1357 BP 241 EP + DI 10.1063/1.3615125 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BXF95 UT WOS:000295993400061 ER PT S AU Gonthier, PL Billman, C Harding, AK Grenier, IA Pierbattista, M AF Gonthier, Peter L. Billman, Caleb Harding, Alice K. Grenier, Isabelle A. Pierbattista, Marco BE Burgay, M DAmico, ND Esposito, P Pellizzoni, A Possenti, A TI Population Synthesis of Radio and Gamma-ray Pulsars in the Fermi Era SO RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Radio Pulsars - An Astrophysical Key to Unlock the Secrets of the Universe CY OCT 10-15, 2010 CL Chia, ITALY SP INAF-Osservatorio Astronomico Cagliari, Sardinia Radio Telescope Board, Assoc Cefalu & Astron DE Pulsars; non-thermal mechanisms; magnetic fields; neutron stars; gamma-rays; radio AB We present results of our pulsar population synthesis of normal pulsars from the Galactic disk using our previously developed computer code. On the same footing, we use slot gap and outer gap models for gamma-ray emission from normal pulsars to obtain statistics of radio-loud and radio-quiet gamma-ray pulsars. From recently improved understanding of HII and star forming regions in the Galaxy, we develop a new surface density model of the birth location of neutron stars. We explore models of neutron star evolution with magnetic field-decay, and with different initial period and magnetic field distributions. We present preliminary results including simulated population statistics that are compared with recent detections by Fermi of normal, isolated pulsars. C1 [Gonthier, Peter L.; Billman, Caleb] Hope Coll, Dept Phys, Holland, MI 49423 USA. [Harding, Alice K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Grenier, Isabelle A.; Pierbattista, Marco] CEA Saclay, AIM, Ser DOAstrophys, Saclay 91400, France. RP Gonthier, PL (reprint author), Hope Coll, Dept Phys, Holland, MI 49423 USA. RI Harding, Alice/D-3160-2012 FU Michigan Space Grant Consortium,of the National Science Foundation [PHY/DMR-1004811]; NASA Astrophysics Theory and Fundamental Program [NNX09AQ71G]; NASA Fermi Guest Investigator Cycle 3 Program [NNX10AO41G] FX We express our gratitude for the generous support of the Michigan Space Grant Consortium,of the National Science Foundation (REU Grant No. PHY/DMR-1004811), the NASA Astrophysics Theory and Fundamental Program (NNX09AQ71G) and the NASA Fermi Guest Investigator Cycle 3 Program (NNX10AO41G). NR 6 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0915-6 J9 AIP CONF PROC PY 2011 VL 1357 BP 245 EP + DI 10.1063/1.3615126 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BXF95 UT WOS:000295993400062 ER PT S AU Pierbattista, M Grenier, I Harding, A Gonthier, PL AF Pierbattista, M. Grenier, I. Harding, A. Gonthier, P. L. BE Burgay, M DAmico, ND Esposito, P Pellizzoni, A Possenti, A TI Constraining pulsar gap models with the light-curve and flux properties of the gamma-ray pulsar population SO RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Radio Pulsars - An Astrophysical Key to Unlock the Secrets of the Universe CY OCT 10-15, 2010 CL Chia, ITALY SP INAF-Osservatorio Astronomico Cagliari, Sardinia Radio Telescope Board, Assoc Cefalu & Astron DE Pulsars; Neutron star population synthesis; Gamma-ray emission ID SLOT GAPS; ACCELERATION; EMISSION; GEOMETRY AB We compare population synthesis results for inner and outer magnetosphere emission models with the various characteristics measured in the first LAT pulsar catalogue for both the radio-loud and radio-weak or radio-quiet gamma-ray pulsars. We show that all models fail to reproduce the observations: for each model there is a lack of luminous and energetic objects that suggests a non dipolar magnetic field structure or spin-down evolution. The large dispersion that we find in the simulated gamma-ray luminosity versus spin-down power relation does not allow to use the present trend seen in the Fermi data to distinguish among models. For each model and each Fermi detected pulsar, we have generated light curves as a function of obliquity and inclination angles. The theoretical curves were fitted to the observed one, using a maximum-likelihood approach, to derive the best-fit orientations and to compare how well each model can reproduce the data. Including the radio light-curve gives an additional key constraint to restrict the orientation space. C1 [Pierbattista, M.; Grenier, I.] CEA IRFU CNRS Paris Diderot Univ, Lab AIM, Serv Astrophys, CEA Saclay, F-91191 Gif Sur Yvette, France. [Harding, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gonthier, P. L.] Hope Coll, Dept Chem, Holland, MI 49423 USA. RP Pierbattista, M (reprint author), CEA IRFU CNRS Paris Diderot Univ, Lab AIM, Serv Astrophys, CEA Saclay, F-91191 Gif Sur Yvette, France. RI Harding, Alice/D-3160-2012 NR 5 TC 2 Z9 2 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0915-6 J9 AIP CONF PROC PY 2011 VL 1357 BP 249 EP + DI 10.1063/1.3615127 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BXF95 UT WOS:000295993400063 ER PT S AU DeCesar, ME Harding, AK Miller, MC AF DeCesar, Megan E. Harding, Alice K. Miller, M. Coleman BE Burgay, M DAmico, ND Esposito, P Pellizzoni, A Possenti, A TI Likelihood Analysis of High-Energy Pulsar Emission Models SO RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Radio Pulsars - An Astrophysical Key to Unlock the Secrets of the Universe CY OCT 10-15, 2010 CL Chia, ITALY SP INAF-Osservatorio Astronomico Cagliari, Sardinia Radio Telescope Board, Assoc Cefalu & Astron DE gamma-ray: observations; pulsars ID LIGHT CURVES AB The high-quality Fermi LAT observations of gamma-ray pulsars open a new window to understanding the generation mechanisms of high-energy pulsar emission. To explore this, we have simulated high-energy light curves from geometrical representations of the outer gap and slot gap emission models with the vacuum retarded dipole magnetosphere model. These simulated light curves are compared with the LAT light curves of the Vela and Geminga pulsars via maximum likelihood, using a Markov Chain Monte Carlo method to explore the models' phase space. C1 [DeCesar, Megan E.; Miller, M. Coleman] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Harding, Alice K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Miller, M. Coleman] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP DeCesar, ME (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM decesar@astro.umd.edu RI Harding, Alice/D-3160-2012 NR 7 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0915-6 J9 AIP CONF PROC PY 2011 VL 1357 BP 285 EP + DI 10.1063/1.3615136 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BXF95 UT WOS:000295993400072 ER PT S AU Stairs, IH Keith, MJ Arzoumanian, Z Becker, W Bemdsen, A Bouchard, A Bhat, NDR Burgay, M Champion, DJ Chatterjee, S Colegate, T Cordes, JM Crawford, FM Dodson, R Freire, PCC Hobbs, GB Hotan, AW Johnston, S Kaspi, VM Kondratiev, V Kramer, M Lazio, TJW Majid, W Manchester, RN Nice, DJ Pellizzoni, A Possenti, A Ransom, SM Rea, N Shannon, R Smits, R Stappers, BW Torres, DF Van, LAGJ Van, SW Weltevrede, P AF Stairs, I. H. Keith, M. J. Arzoumanian, Z. Becker, W. Bemdsen, A. Bouchard, A. Bhat, N. D. R. Burgay, M. Champion, D. J. Chatterjee, S. Colegate, T. Cordes, J. M. Crawford, F. M. Dodson, R. Freire, P. C. C. Hobbs, G. B. Hotan, A. W. Johnston, S. Kaspi, V. M. Kondratiev, V. Kramer, M. Lazio, T. J. W. Majid, W. Manchester, R. N. Nice, D. J. Pellizzoni, A. Possenti, A. Ransom, S. M. Rea, N. Shannon, R. Smits, R. Stappers, B. W. Torres, D. F. Van Leeuwen, A. G. J. Van Straten, W. Weltevrede, P. BE Burgay, M DAmico, ND Esposito, P Pellizzoni, A Possenti, A TI Pulsars with the Australian Square Kilometre Array Pathfinder SO RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE SE AIP Conference Proceedings LA English DT Proceedings Paper CT Conference on Radio Pulsars - An Astrophysical Key to Unlock the Secrets of the Universe CY OCT 10-15, 2010 CL Chia, ITALY SP INAF-Osservatorio Astronomico Cagliari, Sardinia Radio Telescope Board, Assoc Cefalu & Astron DE pulsars; ASKAP ID FIELD; SCIENCE AB The Australian Square Kilometre Array Pathfinder (ASKAP) is a 36-element array with a 30-square-degree field of view being built at the proposed SKA site in Western Australia. We are conducting a Design Study for pulsar observations with ASKAP, planning both timing and search observations. We provide an overview of the ASKAP telescope and an update on pulsar-related progress. C1 [Stairs, I. H.; Bemdsen, A.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. [Keith, M. J.; Hobbs, G. B.; Johnston, S.; Manchester, R. N.; Shannon, R.] CSIRO, Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Arzoumanian, Z.] NASA, USRA, CRESST, Greenbelt, MD 20771 USA. [Becker, W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bouchard, A.; Kaspi, V. M.] McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. [Van Straten, W.] Swinburne Univ Technol, CTR Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Burgay, M.; Pellizzoni, A.; Possenti, A.] INAF, Osservatorio Astron Cagliari, I-09012 Capoterra, Italy. [Champion, D. J.; Freire, P. C. C.; Kramer, M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Chatterjee, S.; Cordes, J. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Colegate, T.; Hotan, A. W.] ICRAR, Curtin Inst Radioastron, Perth, WA 6845, Australia. [Crawford, F. M.] Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA. [Dodson, R.] Univ Western Australia, ICRAR, Perth, WA 6000, Australia. [Kondratiev, V.; Smits, R.; Van Leeuwen, A. G. J.] ASTRON, NL-7990 Dwingeloo, Netherlands. [Kramer, M.; Smits, R.; Stappers, B. W.; Weltevrede, P.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Lazio, T. J. W.; Majid, W.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Nice, D. J.] Lafayette Coll, Dept Phys, Easton, PA 18042 USA. [Ransom, S. M.] Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. [Rea, N.] UAB, Fac Sci, IEEE CSIC, E-08193 Barcelona, Spain. [Torres, D. F.] UAB, Fac Sci, ICREA & IEEE CSIC, E-08193 Barcelona, Spain. [Van Leeuwen, A. G. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 Amsterdam, Netherlands. RP Stairs, IH (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. RI Colegate, Tim/B-5286-2013; Bhat, Ramesh/B-7396-2013; Kondratiev, Vladislav/N-1105-2015; OI Rea, Nanda/0000-0003-2177-6388; van Straten, Willem/0000-0003-2519-7375; Kondratiev, Vladislav/0000-0001-8864-7471; Champion, David/0000-0003-1361-7723; Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Shannon, Ryan/0000-0002-7285-6348; Burgay, Marta/0000-0002-8265-4344; Nice, David/0000-0002-6709-2566 FU Commonwealth Government of Australia; State Government of Western Australia; CSIRO; NSERC Discovery; SRO FX The Murchison Radio-astronomy Observatory (MRO) is jointly funded by the Commonwealth Government of Australia and State Government of Western Australia and managed by the CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Pulsar and ASKAP research at UBC is supported by NSERC Discovery and SRO grants. NR 11 TC 1 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0915-6 J9 AIP CONF PROC PY 2011 VL 1357 BP 335 EP + DI 10.1063/1.3615151 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BXF95 UT WOS:000295993400087 ER PT S AU Ramesham, R AF Ramesham, Rajeshuni BE GarciaBlanco, S Ramesham, R TI Reliability of Sn/Pb and Lead-free (SnAgCu) Solders of Surface Mounted Miniaturized Passive Components for Extreme Temperature (-185 degrees C to+125 degrees C) Space Missions SO RELIABILITY, PACKAGING, TESTING, AND CHARACTERIZATION OF MEMS/MOEMS AND NANODEVICES X SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Reliability, Packaging, Testing, and Characterization of MEMS/MOEMS and Nanodevices X CY JAN 24-25, 2011 CL San Francisco, CA SP SPIE, INO, DALSA, Smart Equipment Technol (SET) DE Reliability; extreme temperatures; baking; thermal cycling; Mars environments; Jupiter environments; intermittent failures; passive components; passive chip resistors; lead-free; tin-lead solders ID JOINTS AB Surface mount electronic package test boards have been assembled using tin/lead (Sn/Pb) and lead-free (Pb-free or SnAgCu or SAC305) solders. The soldered surface mount packages include ball grid arrays (BGA), flat packs, various sizes of passive chip components, etc. They have been optically inspected after assembly and subsequently subjected to extreme temperature thermal cycling to assess their reliability for future deep space, long-term, extreme temperature environmental missions. In this study, the employed temperature range (-185 degrees C to +125 degrees C) covers military specifications (-55 degrees C to +100 degrees C), extreme cold Martian (-120 degrees C to +115 degrees C), asteroid Nereus (-180 degrees C to +25 degrees C) and JUNO (-150 degrees C to +120 degrees C) environments. The boards were inspected at room temperature and at various intervals as a function of extreme temperature thermal cycling and bake duration. Electrical resistance measurements made at room temperature are reported and the tests to date have shown some change in resistance as a function of extreme temperature thermal cycling and some showed increase in resistance. However, the change in interconnect resistance becomes more noticeable with increasing number of thermal cycles. Further research work will be carried out to understand the reliability of packages under extreme temperature applications (-185 degrees C to +125 degrees C) via continuously monitoring the daisy chain resistance for BGA, Flat-packs, lead less chip packages, etc. This paper will describe the experimental reliability results of miniaturized passive components (01005, 0201, 0402, 0603, 0805, and 1206) assembled using surface mounting processes with tin-lead and lead-free solder alloys under extreme temperature environments. C1 CALTECH, Jet Prop Lab, NASA,Off Safety & Mission Success, Reliabil Engn & Mission Environm Assurance Off, Pasadena, CA 91109 USA. RP Ramesham, R (reprint author), CALTECH, Jet Prop Lab, NASA,Off Safety & Mission Success, Reliabil Engn & Mission Environm Assurance Off, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Rajeshuni.Ramesham@jpl.nasa.gov NR 10 TC 0 Z9 0 U1 1 U2 7 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-465-9 J9 PROC SPIE PY 2011 VL 7928 AR 79280F DI 10.1117/12.873466 PG 17 WC Nanoscience & Nanotechnology; Optics SC Science & Technology - Other Topics; Optics GA BYC60 UT WOS:000297982500014 ER PT S AU Kalashnikova, OV Garay, MJ Sokolik, IN Diner, DJ Kahn, RA Martonchik, JV Lee, JN Torres, O Yang, WD Marshak, A Kassabian, S Chodas, M AF Kalashnikova, Olga V. Garay, Michael J. Sokolik, Irina N. Diner, David J. Kahn, Ralph A. Martonchik, John V. Lee, Jae N. Torres, Omar Yang, Weidong Marshak, Alexander Kassabian, Sero Chodas, Mark BE Kassianov, EI Comeron, A Picard, RH Schafer, K TI Capabilities and limitations of MISR aerosol products in dust-laden regions SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XVI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Remote Sensing of Clouds and the Atmosphere XVI CY SEP 21-22, 2011 CL Prague, CZECH REPUBLIC SP SPIE DE MISR; Terra; mineral dust; multiangle; remote sensing ID REMOTE-SENSING OBSERVATIONS; OPTICAL DEPTHS; CLIMATE; DESERT; VARIABILITY; TRANSPORT; IDENTIFY; ABILITY; MODEL AB Atmospheric mineral dust particles have significant effects on climate and the environment, and despite notable advances in modeling and satellite and ground-based measurements, remain one of the major factors contributing to large uncertainty in aerosol radiative forcing. We examine the Multi-angle Imaging SpectroRadiometer (MISR) 11+ year aerosol data record to demonstrate MISR's unique strengths and assess potential biases of MISR products for dust study applications. In particular, we examine MISR's unique capabilities to 1) distinguish dust aerosol from spherical aerosol types, 2) provide aerosol optical depths over bright desert source regions, and 3) provide high-resolution retrievals of dust plume heights and associated winds. We show examples of regional and global MISR data products in dusty regions together with quantitative evaluations of product accuracies through comparisons with independent data sources, and demonstrate applications of MISR data to dust regional and climatological studies, such as dust property evolution during transport, dust source climatology in relation to climatic factors, and dust source dynamics. The potential use of MISR radiance data to study dust properties is also discussed. C1 [Kalashnikova, Olga V.; Diner, David J.; Martonchik, John V.; Lee, Jae N.; Kassabian, Sero; Chodas, Mark] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Kalashnikova, OV (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA. EM Olga.Kalashnikova@jpl.nasa.gov RI Kahn, Ralph/D-5371-2012; Torres, Omar/G-4929-2013 OI Kahn, Ralph/0000-0002-5234-6359; NR 33 TC 2 Z9 2 U1 0 U2 6 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-804-6 J9 PROC SPIE PY 2011 VL 8177 AR 81770O DI 10.1117/12.897773 PG 11 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BYA81 UT WOS:000297789000023 ER PT S AU Rault, DF Xu, PQ AF Rault, Didier F. Xu, Philippe Q. BE Kassianov, EI Comeron, A Picard, RH Schafer, K TI Expected data quality from the upcoming OMPS/LP mission SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XVI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Remote Sensing of Clouds and the Atmosphere XVI CY SEP 21-22, 2011 CL Prague, CZECH REPUBLIC SP SPIE DE Remote sensing; limb scatter; atmospheric ozone vertical distribution ID LIMB SCATTER MEASUREMENTS; STRATOSPHERIC AEROSOL; RETRIEVAL; OZONE AB The performance of the OMPS/LP retrieval algorithm is assessed by conducting a series of numerical experiments and evaluating the quality of the primary (ozone profile) and secondary products (aerosol profiles, NO2, cloud height, surface reflectance) as well as height registration under a set of realistic atmospheric conditions selected randomly. The study considers a number of orbits corresponding to Winter/Summer solstice and Spring/Autumn Equinox. It is shown that the quality of the OMPS/LP retrieval products (accuracy, precision, vertical resolution, height registration) varies along the orbit, as the single scattering angle transitions from backscatter to forward scatter and zenith angles vary from sunrise to sunset. Instrument effects (straylight, gain consolidation, instrument noise) are also investigated. It is shown that ozone profiles can be retrieved with an accuracy of 5% or better from the tropopause up to 50 km, a precision of about 3-5% from 18 to 50 km, and a vertical resolution of 1.5-2 km. Stratospheric aerosol extinction profile can be retrieved with an accuracy/precision of about 30%. The scene-based tangent height registration algorithm is shown to yield height information with an RMS error of 250-300m. C1 [Rault, Didier F.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Rault, DF (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 23 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-804-6 J9 PROC SPIE PY 2011 VL 8177 AR 817709 DI 10.1117/12.897848 PG 12 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BYA81 UT WOS:000297789000009 ER PT S AU Zhou, DK Larar, AM Liu, X Smith, WL Strow, LL Yang, P AF Zhou, Daniel K. Larar, Allen M. Liu, Xu Smith, William L. Strow, L. Larrabee Yang, Ping BE Kassianov, EI Comeron, A Picard, RH Schafer, K TI Ultraspectral sounding retrieval error budget and estimation SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE XVI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Remote Sensing of Clouds and the Atmosphere XVI CY SEP 21-22, 2011 CL Prague, CZECH REPUBLIC SP SPIE DE Atmospheric composition; error; radiative transfer; remote sensing; satellite ID RADIATIVE-TRANSFER; VALIDATION AB The ultraspectral infrared radiances obtained from satellite observations provide atmospheric, surface, and/or cloud information. The intent of the measurement of the thermodynamic state is the initialization of weather and climate models. Great effort has been given to retrieving and validating these atmospheric, surface, and/or cloud properties. Error Consistency Analysis Scheme (ECAS), through fast radiative transfer model (RTM) forward and inverse calculations, has been developed to estimate the error budget in terms of absolute and standard deviation of differences in both spectral radiance and retrieved geophysical parameter domains. The retrieval error is assessed through ECAS without assistance of other independent measurements such as radiosonde data. ECAS re-evaluates instrument random noise, and establishes the link between radiometric accuracy and retrieved geophysical parameter accuracy. ECAS can be applied to measurements of any ultraspectral instrument and any retrieval scheme with associated RTM. In this paper, ECAS is described and demonstration is made with the measurements of the METOP-A satellite Infrared Atmospheric Sounding Interferometer (IASI). C1 [Zhou, Daniel K.; Larar, Allen M.; Liu, Xu] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Zhou, DK (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM daniel.k.zhou@nasa.gov NR 10 TC 0 Z9 0 U1 1 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-804-6 J9 PROC SPIE PY 2011 VL 8177 AR 81770C DI 10.1117/12.897559 PG 6 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BYA81 UT WOS:000297789000012 ER PT B AU Katsaros, KB Bentamy, A Bourassa, M Ebuchi, N Gower, J Liu, WT Vignudelli, S AF Katsaros, Kristina B. Bentamy, Abderrahim Bourassa, Mark Ebuchi, Naoto Gower, James (Jim) Liu, W. Timothy Vignudelli, Stefano BE Tang, DL TI Climate Data Issues from an Oceanographic Remote Sensing Perspective SO REMOTE SENSING OF THE CHANGING OCEANS LA English DT Proceedings Paper CT 9th Pan Ocean Remote Sensing Conference, PORSEC2008 CY DEC 02-06, 2008 CL S China Sea Inst Oceanog, Guangzhou, PEOPLES R CHINA SP Natl Nat Sci Fdn China, Chinese Acad Sci, Guangzhou Assoc Sci & Technol, Guangdong Nat Sci Fdn HO S China Sea Inst Oceanog DE Oceanographic satellite sensors; Scatterometers; Altimeters; Microwave radiometers; Infrared and ocean color sensors; Winds; Sea surface temperature; Air-sea fluxes; International cooperation for climate quality data; Sampling; Consistency; Archiving and distribution ID SEA-SURFACE TEMPERATURE; MEASURING MISSION TRMM; WIND VECTORS; PASSIVE MICROWAVE; BOUNDARY-LAYER; SATELLITE DATA; OCEAN; PRECIPITATION; SCATTEROMETER; RESOLUTION AB In this chapter we review several climatologically. important variables with a history of observation from spaceborne platforms. These include sea surface temperature and wind vectors, altimetric estimates of sea surface height, energy and water vapor fluxes at the sea surface, precipitation over the ocean, and ocean color. We then discuss possible improvements in sampling for climate and climate change definition. Issues of consistency of different data sources, archiving and distribution of these types of data are discussed. The practical prospect of immediate international coordination through the concept of virtual constellations is discussed and applauded. C1 [Katsaros, Kristina B.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. [Katsaros, Kristina B.] Northwest Res Associates, Bellevue, WA USA. [Bentamy, Abderrahim] IFREMER, Plouzane, France. [Bourassa, Mark] COAPS, Tallahassee, FL USA. [Bourassa, Mark] Florida State Univ, Tallahassee, FL 32306 USA. [Ebuchi, Naoto] Hokkaido Univ, Inst Low Temp Sci, Sapporo, Hokkaido, Japan. [Gower, James (Jim)] Fisheries & Oceans Canada, Inst Ocean Sci, Sidney, BC, Canada. [Liu, W. Timothy] Jet Prop Lab, Pasadena, CA USA. [Vignudelli, Stefano] CNR, Pisa, Italy. RP Katsaros, KB (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM katsaros@whidbey.net; Abderrahim.Bentamy@ifremer.fr; bourassa@coaps.fsu.edu; ebuchi@lowtem.hokudai.ac.jp; Jim.gower@dfo-mpo.gc.ca; W.Timothy.Liu@jpl.nasa.gov; vignudelli@pi.ibf.cnr.it FU U.S. National Science Foundation, NSF; NASA; ESA; South China Sea Institute of Oceanology, Chinese Academy of Sciences FX We appreciate the contribution of: Figure 2.2 by Dr. Stanley Wilson. We are grateful for support by the U.S. National Science Foundation, NSF, by NASA and ESA for the PORSEC 2008 meeting and by the Chinese hosts, especially The South China Sea Institute of Oceanology, Chinese Academy of Sciences and the chair of the Local Organizing committee, Dr. Danling (Lingzis) Tang, who made arrangements for the Workshop on Climate Data possible on the last day of the conference in Guangzhou, China, December 6, 2008. K. Katsaros gratefully acknowledges support from an NSF research grant to University of Miami, Rosenstiel School, ATM 0631685. NR 65 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-642-16540-5 PY 2011 BP 7 EP 32 DI 10.1007/978-3-642-16541-2_2 PG 26 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BH0HQ UT WOS:000395049400002 ER PT B AU Liu, AK AF Liu, Antony K. BE Tang, DL TI Coastal Monitoring by Satellite-Based SAR SO REMOTE SENSING OF THE CHANGING OCEANS LA English DT Proceedings Paper CT 9th Pan Ocean Remote Sensing Conference, PORSEC2008 CY DEC 02-06, 2008 CL S China Sea Inst Oceanog, Guangzhou, PEOPLES R CHINA SP Natl Nat Sci Fdn China, Chinese Acad Sci, Guangzhou Assoc Sci & Technol, Guangdong Nat Sci Fdn HO S China Sea Inst Oceanog DE Synthetic Aperture Radar; Fisheries-oceanography; Vessel monitoring system; Sea-ice motion; Pollution and hazard protection ID SYNTHETIC-APERTURE RADAR; SEA-ICE MOTION; WAVELET ANALYSIS; DRIFT; IMAGERY; SSM/I; ZONE AB The ability of Synthetic Aperture Radar (SAR) for monitoring surface signatures of swells, wind fronts, bottom features, oil slicks, and eddies has been amply demonstrated. The combined use of IR (AVHRR), ocean color (SeaWiFS, MODIS), and SAR (ERS-1/2, ENVISAT, RADARSAT) data can provide frequent high resolution coverage of the coastal area for the evolution study of oceanic processes. This chapter presents examples of these applications. During the Bering Sea Fisheries-Oceanography Coordinated Investigation (FOCI) field test, simultaneous satellite SAR data and in-situ measurements from moorings and ships were collected. Ships and their wakes are commonly observable in high-resolution satellite SAR imagery. This can be useful in national defense intelligence, shipping traffic, and fishing enforcement, especially when combined with the Vessel Monitoring System (VMS). SAR images can track the movement of the ice edge and floes in the marginal ice zone (MIZ). Results are relevant to climate change and fishery management. Sea-ice motion derived by satellite data can be used to interpret the Arctic ice retreat in the summer of 2007. Underwater bathymetry has been mapped by satellite remote sensing (SAR, SPOT, and LANDSAT) in the Spratly Islands of South China Sea (SCS) for ship navigation. As presented by these case studies, the use of SAR-derived observations can supply valuable information for the protection of the environment. C1 [Liu, Antony K.] Natl Taiwan Ocean Univ, Keelung, Taiwan. [Liu, Antony K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Liu, AK (reprint author), Natl Taiwan Ocean Univ, Keelung, Taiwan. EM akliu@ntou.edu.tw FU U.S. Office of Naval Research (ONR); National Aeronautics and Space Administration (NASA); Taiwan's National Science Council (NSC) FX The author would like to thank Prof. Ming-Kuang Hsu and Dr. Yunhe Zhao for providing assistance to this study, and Prof. Ming-An Lee of the National Taiwan Ocean University (NTOU) for providing Fig. 10.8. This work was supported by the U.S. Office of Naval Research (ONR) and National Aeronautics and Space Administration (NASA). The author is a Principal Investigator on ESA and CSA projects; all ERS-2 SAR and ENVISAT ASAR data are copyrighted by ESA, and RADARSAT data is copyrighted by CSA. The author is now a Visiting Professor of NTOU, and the support from Taiwan's National Science Council (NSC) is also highly appreciated. NR 32 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-642-16540-5 PY 2011 BP 195 EP 215 DI 10.1007/978-3-642-16541-2_10 PG 21 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BH0HQ UT WOS:000395049400010 ER PT B AU Song, YT Han, SC AF Song, Y. Tony Han, Shin-Chan BE Tang, DL TI Satellite Observations Defying the Long-Held Tsunami Genesis Theory SO REMOTE SENSING OF THE CHANGING OCEANS LA English DT Proceedings Paper CT 9th Pan Ocean Remote Sensing Conference, PORSEC2008 CY DEC 02-06, 2008 CL S China Sea Inst Oceanog, Guangzhou, PEOPLES R CHINA SP Natl Nat Sci Fdn China, Chinese Acad Sci, Guangzhou Assoc Sci & Technol, Guangdong Nat Sci Fdn HO S China Sea Inst Oceanog DE Tsunami genesis theory; GRACE; Vertical uplift; Horizontal displacement; Seismograph; GPS data ID SUMATRA-ANDAMAN EARTHQUAKE; INDIAN-OCEAN TSUNAMI; DECEMBER 26; GENERATION; ALTIMETRY; AFTERSLIP; BOTTOM AB Using seismographs and GPS displacement measurements, we have estimated the seafloor deformation history of the December 2004 Sumatra-Andaman earthquake and the March 2005 Nias earthquake by separating their deformation period into intervals of 800-s, 1-h, and 6-months. We have then calculated their corresponding gravity changes (induced by the seafloor deformation), which are 11.3, 12.5, and 14.9 microgalileo, respectively. We show that the seismographs and GPS-derived values are consistent with the known postseismic to coseismic moment ratio of 30% and the Gravity Recovery and Climate Experiment (GRACE) satellites measurements of 15 microgalileo for the same period of 6 months. However, the vertical component of the accumulated seafloor deformation during the tsunami formation period (similar to 30 min) could only generate a potential energy of 1.2 x 10(15) Joules and account for only one third of the actual tsunami height. The evidence is overwhelmingly contrary to the long-held theory that the vertical deformation of seafloor is the primary source of tsunamis. Furthermore, we have carefully examined the pioneering wave-maker experiment that initially conceived the ubiquitous tsunami genesis theory. Surprisingly, we found that the experimental ratio of the horizontal slip distance to the water depth the non-dimensional parameter that allows comparing the experiment with reality on an apple-to-apple basis was - 200 times of realistic earthquake parameters. The experimental conclusion is problematic in conceiving the tsunami theory. By including the horizontal momentum energy transferred by the faulting continental slope in a three-dimensional tsunami model, we have re-examined the December 2004 tsunami using both seismographs and GPS measurements. Our results show that the new theory is more consistent with altimetry and tide data than the conventional theory of using the vertical force alone, suggesting that the tsunami formation mechanism is not as simple as previously thought. C1 [Song, Y. Tony] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Han, Shin-Chan] NOAA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Song, YT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Tony.Song@jpl.nasa.gov; Shin-Chan.Han@nasa.gov NR 29 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-642-16540-5 PY 2011 BP 327 EP 342 DI 10.1007/978-3-642-16541-2_17 PG 16 WC Oceanography; Remote Sensing SC Oceanography; Remote Sensing GA BH0HQ UT WOS:000395049400017 ER PT S AU Kokhanovsky, AA Platnick, S King, MD AF Kokhanovsky, Alexander A. Platnick, Steven King, Michael D. BE Burrows, JP Platt, U Borrell, P TI Remote Sensing of Terrestrial Clouds from Space using Backscattering and Thermal Emission Techniques SO REMOTE SENSING OF TROPOSPHERIC COMPOSITION FROM SPACE SE Physics of Earth and Space Environments LA English DT Article; Book Chapter ID SOLAR-RADIATION MEASUREMENTS; ROTATIONAL RAMAN-SCATTERING; LIQUID WATER CLOUDS; OPTICAL-THICKNESS; THERMODYNAMIC-PHASE; EFFECTIVE RADIUS; TOP HEIGHT; SATELLITE; MODIS; ATMOSPHERE C1 [Kokhanovsky, Alexander A.] Univ Bremen, Inst Environm Phys, D-2800 Bremen 33, Germany. [Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [King, Michael D.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Kokhanovsky, AA (reprint author), Univ Bremen, Inst Environm Phys, D-2800 Bremen 33, Germany. RI King, Michael/C-7153-2011 OI King, Michael/0000-0003-2645-7298 NR 65 TC 11 Z9 11 U1 0 U2 3 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 1610-1677 BN 978-3-642-14790-6 J9 PHYS EARTH SPACE ENV PY 2011 BP 231 EP 257 DI 10.1007/978-3-642-14791-3_5 D2 10.1007/978-3-642-14791-3 PG 27 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BUR01 UT WOS:000290127000005 ER PT S AU Boccaletti, A Baudoz, P Mawet, D Schneider, J Tinetti, G Galicher, R Stam, D Cavarroc, C Hough, J Doel, P Pinfield, D Keller, CU Beuzit, JL Udry, S Ferrari, A Martin, E Menard, F Sein, E AF Boccaletti, A. Baudoz, P. Mawet, D. Schneider, J. Tinetti, G. Galicher, R. Stam, D. Cavarroc, C. Hough, J. Doel, P. Pinfield, D. Keller, C. -U. Beuzit, J. -L. Udry, S. Ferrari, A. Martin, E. Menard, F. Sein, E. BE Martin, EL Ge, J Lin, W TI Spectral and polarimetric characterization of gazeous and telluric planets with SEE COAST SO RESEARCH, SCIENCE AND TECHNOLOGY OF BROWN DWARFS AND EXOPLANETS SE EPJ Web of Conferences LA English DT Proceedings Paper CT International Conference on Occasion of a Total Eclipse of the Sun CY JUL 20-24, 2009 CL Shanghai, PEOPLES R CHINA SP US Natl Sci Fdn, Shanghai Astronom Observ, Chinese Acad Sci, Natl Sci Fdn China, Nanjing Inst Astronom Opt & Technol, Univ Sci & Technol China, Purple Mt Observ ID LABORATORY DEMONSTRATION; EXTRASOLAR PLANETS; EARTH; CORONAGRAPH AB SEE COAST stands for Super Earth Explorer - Coronagraphic Off-Axis Space Telescope. The concept was initially proposed to ESA for Cosmic Vision. None of the direct detection exoplanet proposals were selected in 2007 and we are now pursuing our efforts to consolidate the astrophysical program and the technical developments for the next call for proposal. The prime objective of SEE COAST is to contribute to the understanding of the formation and evolution of planetary systems. Exploring the diversity of these objects is therefore the main driver to define the instrumentation. In the next decade the improvement of radial velocity instruments and obviously temporal coverage will provide us with a large numbers of long period giants as well as telluric planets, namely Super Earths. Obtaining the spectral and polarimetric signatures of these objects in the visible range to measure atmospheric parameters (molecular composition, clouds, soils,...) will be unique and with important scientific returns. A space mission complementary to near IR instruments like SPHERE, GPI, JWST and later ELTs for the full characterization of giants and Super Earths is a first secure step towards the longer term goal that is the characterization of telluric planets with mass and atmosphere comparable to that of the Earth. An overview of the astrophysical motivation and the trade-off that lead to a simple integrated concept of a space-based high contrast imaging instrument are given here. C1 [Boccaletti, A.; Baudoz, P.; Schneider, J.; Galicher, R.] Observ Paris, Meudon, France. [Mawet, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tinetti, G.; Doel, P.] UCL, Dept Phys & Astron, London, England. [Stam, D.] SRON, Utrecht, Netherlands. [Cavarroc, C.] CEA SAp, Saclay, France. [Hough, J.; Pinfield, D.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield, Herts, England. [Keller, C. -U.] Univ Utrecht, Utrecht, Netherlands. [Beuzit, J. -L.] Lab Astrophys Grenoble, Grenoble, France. [Udry, S.; Menard, F.] Observ Geneva, Versoix, Switzerland. [Ferrari, A.] Astrophys Lab Marseille, Marseille, France. [Martin, E.] Ctr Astrobiol, Madrid, Spain. [Sein, E.] Astrium, Paris, France. RP Boccaletti, A (reprint author), Observ Paris, Meudon, France. EM anthony.boccaletti@obspm.fr OI Tinetti, Giovanna/0000-0001-6058-6654 NR 30 TC 0 Z9 0 U1 0 U2 1 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 2100-014X BN 978-2-7598-0664-5 J9 EPJ WEB CONF PY 2011 VL 16 AR UNSP 07002 DI 10.1051/epjconf/20111607002 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBO05 UT WOS:000307650700049 ER PT S AU Leggett, SK Burningham, B Saumon, D Marley, MS Warren, SJ Jones, HRA Pinfield, DJ Smart, RL AF Leggett, S. K. Burningham, B. Saumon, D. Marley, M. S. Warren, S. J. Jones, H. R. A. Pinfield, D. J. Smart, R. L. BE Martin, EL Ge, J Lin, W TI Mid-infrared followup of cold brown dwarfs: Diversity in age, mass and metallicity SO RESEARCH, SCIENCE AND TECHNOLOGY OF BROWN DWARFS AND EXOPLANETS SE EPJ Web of Conferences LA English DT Proceedings Paper CT International Conference on Occasion of a Total Eclipse of the Sun CY JUL 20-24, 2009 CL Shanghai, PEOPLES R CHINA SP US Natl Sci Fdn, Shanghai Astronom Observ, Chinese Acad Sci, Natl Sci Fdn China, Nanjing Inst Astronom Opt & Technol, Univ Sci & Technol China, Purple Mt Observ ID SPITZER-SPACE-TELESCOPE; EXOPLANET HOST STAR; T-DWARFS; SKY SURVEY; 2MASS; SPECTRA; DISCOVERY; COMPANION; UKIDSS; TEMPERATURE AB We use Spitzer IRAC 3.6-8.0 mu m photometry of late-type T dwarfs to investigate various trends which can aid the planning and interpretation of infrared (IR) surveys for the coldest T or Y dwarfs. Brown dwarfs with effective temperature (T-eff) < 700K emit > 50% of their flux at lambda > 3 mu m, and the ratio of the mid-IR to the near-IR flux becomes very sensitive to T-eff. The color H - [4.5] is a good indicator of T-eff with a weak dependence on metallicity ([m/H]) and gravity (g) while H - K and [4.5] - [5.8] are sensitive to [m/H] and g. Thus T-eff and g can be constrained and mass and age can then be determined from evolutionary models. There are 12 dwarfs known with H - [4.5] > 3.0 and 500 less than or similar to T-eff K less than or similar to 800, which we examine in detail. The ages of these dwarfs range from very young (0.1-1.0 Gyr) to old (3-12 Gyr). The mass range is possibly as low as 5 M-Jup to 70 M-Jup, and [m/H] also spans a large range of similar to -0.3 to similar to +0.3. The T8-T9 dwarfs found so far in the UKIRT IR Deep Sky Survey are unexpectedly young and low-mass. Extensions to the warm Spitzer and WISE space missions are needed to obtain mid-IR data for cold brown dwarfs, and to discover more of these rare objects. C1 [Leggett, S. K.] Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA. [Burningham, B.; Jones, H. R. A.; Pinfield, D. J.] Hertfordshire U, Three Rivers, England. [Saumon, D.] LANL, Los Alamos, NM 87545 USA. [Marley, M. S.] NASA Ames, Mountain View, CA 94040 USA. [Warren, S. J.] Imperial Coll London, London, England. [Smart, R. L.] Astron Obs Torino, Turin, Italy. RP Leggett, SK (reprint author), Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA. EM sleggett@gemini.edu OI Leggett, Sandy/0000-0002-3681-2989 NR 28 TC 1 Z9 1 U1 0 U2 1 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 2100-014X BN 978-2-7598-0664-5 J9 EPJ WEB CONF PY 2011 VL 16 AR UNSP 06007 DI 10.1051/epjconf/20111606007 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBO05 UT WOS:000307650700040 ER PT J AU Antcliff, R AF Antcliff, Rich TI INDUSTRIAL RESEARCH INSTITUTE'S R&D TRENDS FORECAST FOR 2011 SO RESEARCH-TECHNOLOGY MANAGEMENT LA English DT Article C1 [Antcliff, Rich] NASA, Langley Res Ctr, Washington, DC USA. EM richard.r.antcliff@nasa.gov NR 0 TC 1 Z9 1 U1 0 U2 0 PU INDUSTRIAL RESEARCH INST, INC PI ARLINGTON PA 2200 CLARENDON BLVD, STE 1102, ARLINGTON, VA 22201 USA SN 0895-6308 J9 RES TECHNOL MANAGE JI Res.-Technol. Manage. PD JAN-FEB PY 2011 VL 54 IS 1 BP 18 EP 23 PG 6 WC Business; Engineering, Industrial; Management SC Business & Economics; Engineering GA 705RK UT WOS:000286155400006 ER PT S AU Wincheski, B Simpson, J AF Wincheski, Buzz Simpson, John BE Thompson, DO Chimenti, DE TI DEVELOPMENT AND APPLICATION OF WIDE BANDWIDTH MAGNETO-RESISTIVE SENSOR BASED EDDY CURRENT PROBE SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 30A AND 30B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 37th Annual Review of Progress in Quantitative Nondestructive Evaluation (QNDE) CY JUL 18-23, 2010 CL San Diego, CA SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE DE Eddy Current; Magneto-resistive; high frequency; high resolution AB The integration of magneto-resistive sensors into eddy current probes can significantly expand the capabilities of conventional eddy current nondestructive evaluation techniques. The room temperature solid-state sensors have typical bandwidths in the megahertz range and resolutions of tens of microgauss. The low frequency sensitivity of magneto-resistive sensors has been capitalized upon in previous research to fabricate very low frequency eddy current sensors for deep flaw detection in multilayer conductors. In this work a modified probe design is presented to expand the capabilities of the device. The new probe design incorporates a dual induction source enabling operation from low frequency deep flaw detection to high frequency high resolution near surface material characterization. Applications of the probe for the detection of localized near surface conductivity anomalies are presented. Finite element modeling of the probe is shown to be in good agreement with experimental measurements. C1 [Wincheski, Buzz] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Simpson, John] Lockheed Martin Space Operat, Hampton, VA 23681 USA. RP Wincheski, B (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 6 TC 2 Z9 2 U1 1 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0888-3 J9 AIP CONF PROC PY 2011 VL 1335 BP 388 EP 395 DI 10.1063/1.3591879 PG 8 WC Physics, Applied SC Physics GA BYH04 UT WOS:000298674300046 ER PT S AU Zalameda, JN Winfree, WP Seebo, JP Johnston, PH AF Zalameda, J. N. Winfree, W. P. Seebo, J. P. Johnston, P. H. BE Thompson, DO Chimenti, DE TI THERMOGRAPHY INSPECTION FOR DETECTION AND TRACKING OF COMPOSITE CYLINDER DAMAGE DURING LOAD TESTING SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 30A AND 30B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 37th Annual Review of Progress in Quantitative Nondestructive Evaluation (QNDE) CY JUL 18-23, 2010 CL San Diego, CA SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE DE Thermal NDE; Thermal Diffusivity; Composite Matrix Cracks; Delamination ID THERMAL-DIFFUSIVITY AB Two thermography techniques, passive and active, are used to detect damage initiation and progression in a cyclically loaded composite cylinder. The passive thermography tracks damage progression in real time during cyclic loading. Active flash thermography, using a flash tube enclosed within the cylinder, images delaminations. A differential thermography processing technique eliminates normal material variations and improves sensitivity to and sizing of delaminations. The thermography results were compared to non-immersion ultrasonic results. C1 [Zalameda, J. N.; Winfree, W. P.; Johnston, P. H.] NASA, Langley Res Ctr, MS231, Hampton, VA 23681 USA. [Seebo, J. P.] Lockheed Martin Corp, NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Zalameda, JN (reprint author), NASA, Langley Res Ctr, MS231, Hampton, VA 23681 USA. NR 9 TC 3 Z9 3 U1 0 U2 7 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0888-3 J9 AIP CONF PROC PY 2011 VL 1335 BP 450 EP 457 DI 10.1063/1.3591887 PG 8 WC Physics, Applied SC Physics GA BYH04 UT WOS:000298674300054 ER PT S AU Waller, JM Nichols, CT Wentzel, DJ Saulsberry, RL AF Waller, J. M. Nichols, C. T. Wentzel, D. J. Saulsberry, R. L. BE Thompson, DO Chimenti, DE TI USE OF MODAL ACOUSTIC EMISSION TO MONITOR DAMAGE PROGRESSION IN CARBON FIBER/EPOXY COMPOSITES SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 30A AND 30B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 37th Annual Review of Progress in Quantitative Nondestructive Evaluation (QNDE) CY JUL 18-23, 2010 CL San Diego, CA SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE DE Modal Acoustic Emission; Felicity Ratio; Fast Fourier Transform; COPV AB Broad-band modal acoustic emission (AE) was used to characterize micromechanical damage progression in uniaxial IM7 and T1000 carbon fiber-epoxy (C/Ep) tows, and a helical and hoop-wrapped IM7 composite overwrapped pressure vessel (COPV). To expedite analysis, tows and the COPV were subjected to an intermittent load hold tensile stress profile. Damage progression in tow specimens was followed by analyzing the Fast Fourier Transforms (FFTs) associated with AE events. FFT analysis showed that damage was usually cooperative, consisting of several failure modes occurring at once, and was dominated by fiber breakage throughout the duration of the stress profile. Evidence was found for the existence of a universal damage parameter, referred to here as the critical Felicity ratio, or Felicity ratio at rupture (FR*), which had a value close to 0.96 for the tows and the COPV tested. The use of FR* to predict the burst pressure of the COPV is demonstrated. C1 [Waller, J. M.; Saulsberry, R. L.] NASA, Dept Lab, Labs Dept, Johnson Space Ctr,White Sands Test Facil, Las Cruces, NM 88011 USA. [Nichols, C. T.] New Mexico State Univ, Dept Mech & Aerosp Engn, Las Cruces, NM 88003 USA. [Wentzel, D. J.] Miami Univ, Dept Phys, Oxford, OH 45056 USA. RP Waller, JM (reprint author), NASA, Dept Lab, Labs Dept, Johnson Space Ctr,White Sands Test Facil, Las Cruces, NM 88011 USA. FU Office of Safety and Mission Assurance Office; NASA FX Ongoing efforts at WSTF to develop AE methods specific to C/Ep COPVs have been sponsored by the Office of Safety and Mission Assurance Office, NASA, Washington, DC. NR 11 TC 1 Z9 1 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0888-3 J9 AIP CONF PROC PY 2011 VL 1335 BP 919 EP 926 DI 10.1063/1.3592036 PG 8 WC Physics, Applied SC Physics GA BYH04 UT WOS:000298674300111 ER PT S AU Wang, N Lobkis, OI Rokhlin, SI Cantrell, JH AF Wang, N. Lobkis, O. I. Rokhlin, S. I. Cantrell, J. H. BE Thompson, DO Chimenti, DE TI ULTRASONIC CHARACTERIZATION OF INTERFACES IN COMPOSITE BONDS SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 30A AND 30B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 37th Annual Review of Progress in Quantitative Nondestructive Evaluation (QNDE) CY JUL 18-23, 2010 CL San Diego, CA SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE DE Ultrasonic; Composite Bonds; Interface; Molecular Bonds ID ENVIRONMENTAL DEGRADATION; IMPERFECT INTERFACES; ADHESIVE BONDS; SPECTROSCOPY; LAYER AB The inverse determination of imperfect interfaces from reflection spectra of normal and oblique incident ultrasonic waves in adhesive bonds of multidirectional composites is investigated. The oblique measurements are complicated by the highly dispersed nature of oblique wave spectra at frequencies above 3MHz. Different strategies for bond property reconstruction, including a modulation method, are discussed. The relation of measured interfacial spring density to the physico-chemical model of a composite interface described by polymer molecular bonds to emulate loss of molecular strength on an adhesive composite interface is discussed. This potentially relates the interfacial (adhesion) strength (number of bonds at the adhesive substrate interface) to the spring constant (stiffness) area density (flux), which is an ultrasonically measurable parameter. C1 [Wang, N.; Lobkis, O. I.; Rokhlin, S. I.] Ohio State Univ, Edison Joining Technol Ctr, 1248 Arthur E Adams Dr, Columbus, OH 43221 USA. [Cantrell, J. H.] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Wang, N (reprint author), Ohio State Univ, Edison Joining Technol Ctr, 1248 Arthur E Adams Dr, Columbus, OH 43221 USA. FU NASA [NNX08BA37A] FX This work is sponsored by NASA Grant No. NNX08BA37A. NR 13 TC 3 Z9 3 U1 0 U2 7 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0888-3 J9 AIP CONF PROC PY 2011 VL 1335 BP 1079 EP 1086 DI 10.1063/1.3592056 PG 8 WC Physics, Applied SC Physics GA BYH04 UT WOS:000298674300131 ER PT S AU Johnston, PH AF Johnston, P. H. BE Thompson, DO Chimenti, DE TI PULSE-ECHO PHASED ARRAY ULTRASONIC INSPECTION OF PULTRUDED ROD STITCHED EFFICIENT UNITIZED STRUCTURE (PRSEUS) SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 30A AND 30B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 37th Annual Review of Progress in Quantitative Nondestructive Evaluation (QNDE) CY JUL 18-23, 2010 CL San Diego, CA SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE DE Phased Array; Ultrasonics; Composites; Out-of-Autoclave AB A PRSEUS test article was subjected to controlled impact on the skin face followed by static and cyclic axial compressions. Phased array ultrasonic inspection was conducted before impact, and after each of the test conditions. A linear phased array probe with a manual X-Y scanner was used for interrogation. Ultrasound showed a delamination between the skin and stringer flange adjacent to the impact. As designed, the stitching in the flange arrested the lateral flaw formation. Subsequent ultrasonic data showed no delamination growth due to continued loading. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Johnston, PH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 2 TC 0 Z9 0 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0888-3 J9 AIP CONF PROC PY 2011 VL 1335 BP 1432 EP 1439 DI 10.1063/1.3592100 PG 8 WC Physics, Applied SC Physics GA BYH04 UT WOS:000298674300175 ER PT S AU Roth, DJ Rauser, RW Abdul-Aziz, A Cotton, R Burke, E Zhang, S Marsh, M Davis, BA Studor, GF AF Roth, D. J. Rauser, R. W. Abdul-Aziz, A. Cotton, R. Burke, E. Zhang, S. Marsh, M. Davis, B. A. Studor, G. F. BE Thompson, DO Chimenti, DE TI RECENT IMPROVEMENTS IN DISPLAY AND ANALYSIS OF NDE DATA AT NASA SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 30A AND 30B SE AIP Conference Proceedings LA English DT Proceedings Paper CT 37th Annual Review of Progress in Quantitative Nondestructive Evaluation (QNDE) CY JUL 18-23, 2010 CL San Diego, CA SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE DE Nondestructive Evaluation; NDE; Data Visualization; Waveforms; Imaging AB This talk reviews several recent NDE data visualization and analysis improvements implemented at NASA Glenn Research Center. Examples will be shown in the areas of X-ray computed tomography and waveform-based NDE. Emphasis is on methods that are most useful not only for the NDE professional analyzing the data but also for sharing of the data with customers such as material processors, testers, and modelers who need to use the data for various engineering decisions. C1 [Roth, D. J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Rauser, R. W.] Univ Toledo, Toledo, OH 43606 USA. [Abdul-Aziz, A.] Cleveland State Univ, Cleveland, OH 44115 USA. [Cotton, R.] Simpleware, Exeter EX4 4RN, England. [Burke, E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Zhang, S.; Marsh, M.] Visualizat Sci Grp, Burlington, MA 01803 USA. [Davis, B. A.; Studor, G. F.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Roth, DJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 4 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0888-3 J9 AIP CONF PROC PY 2011 VL 1335 BP 1605 EP 1612 DI 10.1063/1.3592121 PG 8 WC Physics, Applied SC Physics GA BYH04 UT WOS:000298674300196 ER PT B AU Jain, A AF Jain, Abhinandan TI Robot and Multibody Dynamics: Analysis and Algorithms SO ROBOT AND MULTIBODY DYNAMICS: ANALYSIS AND ALGORITHMS LA English DT Article; Book ID MECHANICAL SYSTEM DYNAMICS; PARALLEL O(LOG(N)) CALCULATION; ARTICULATED-BODY ALGORITHM; SPATIAL OPERATOR ALGEBRA; ORDER-N-FORMULATION; OPEN-LOOP-SYSTEMS; RECURSIVE FORMULATION; QUASI-VELOCITIES; INVERSE DYNAMICS; MANIPULATOR DYNAMICS C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM abhi.jain@jpl.nasa.gov NR 186 TC 35 Z9 35 U1 1 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-1-4419-7266-8 PY 2011 BP 3 EP 482 DI 10.1007/978-1-4419-7267-5 PG 480 WC Engineering, Electrical & Electronic; Mathematics, Applied; Robotics SC Engineering; Mathematics; Robotics GA BSU19 UT WOS:000285803000001 ER PT B AU Boy, G AF Boy, Guy BE Barnard, Y Risser, R Krems, J TI Design for Safety: A Cognitive Engineering Approach SO SAFETY OF INTELLIGENT DRIVER SUPPORT SYSTEMS: DESIGN, EVALUATION AND SOCIAL PERSPECTIVES SE Human Factors in Road and Rail Transport LA English DT Article; Book Chapter C1 [Boy, Guy] Florida Inst Technol, Human Ctr Design Inst, Melbourne, FL 32901 USA. [Boy, Guy] Florida Inst Human & Machine Cognit, Ocala, FL USA. [Boy, Guy] NASA, Kennedy Space Ctr, Miami, FL USA. RP Boy, G (reprint author), Florida Inst Technol, Human Ctr Design Inst, Melbourne, FL 32901 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASHGATE PUBLISHING LTD PI ALDERSHOT PA GOWER HOUSE, CROFT ROAD, ALDERSHOT GU11 3HR, ENGLAND BN 978-0-7546-9525-7; 978-0-7546-7776-5 J9 HUM FACT ROAD RAIL PY 2011 BP 43 EP 63 PG 21 WC Transportation SC Transportation GA BC6ML UT WOS:000354117800005 ER PT J AU de Sherbinin, A Warner, K Ehrhart, C AF de Sherbinin, Alex Warner, Koko Ehrhart, Charles TI Casualties of Climate Change SO SCIENTIFIC AMERICAN LA English DT Article C1 [de Sherbinin, Alex] Columbia Univ, Earth Inst, New York, NY 10027 USA. [de Sherbinin, Alex] NASA, Socioecon Data & Applicat Ctr, Washington, DC 20546 USA. RP de Sherbinin, A (reprint author), Columbia Univ, Earth Inst, New York, NY 10027 USA. OI de Sherbinin, Alex/0000-0002-8875-4864 NR 0 TC 8 Z9 9 U1 2 U2 9 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 0036-8733 J9 SCI AM JI Sci.Am. PD JAN PY 2011 VL 304 IS 1 BP 64 EP 71 DI 10.1038/scientificamerican0111-64 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 697WE UT WOS:000285549700033 PM 21265329 ER PT S AU Yao, HB Hruska, Z Kincaid, R Ononye, A Brown, RL Bhatnagar, D Cleveland, TE AF Yao, Haibo Hruska, Zuzana Kincaid, Russell Ononye, Ambrose Brown, Robert L. Bhatnagar, Deepak Cleveland, Thomas E. BE Kim, MS Tu, SI Chao, K TI Development of Narrow-band Fluorescence Index for the Detection of Aflatoxin Contaminated Corn SO SENSING FOR AGRICULTURE AND FOOD QUALITY AND SAFETY III SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on the Sensing for Agriculture and Food Quality and Safety III CY APR 26-27, 2011 CL Orlando, FL SP SPIE DE aflatoxin; fluorescence hyperspectral image; corn; fluorescence index ID REFLECTANCE SPECTROSCOPY; KERNELS AB Aflatoxin is produced by the fungus Aspergillus flavus when the fungus invades developing corn kernels. Because of its potent toxicity, the levels of aflatoxin are regulated by the Food and Drug Administration (FDA) in the US, allowing 20 ppb (parts per billion) limits in food, and feed intended for interstate commerce. Currently, aflatoxin detection and quantification methods are based on analytical tests. These tests require the destruction of samples, can be costly and time consuming, and often rely on less than desirable sampling techniques. Thus, the ability to detect aflatoxin in a rapid, non-invasive way is crucial to the corn industry in particular. This paper described how narrow-band fluorescence indices were developed for aflatoxin contamination detection based on single corn kernel samples. The indices were based on two bands extracted from full wavelength fluorescence hyperspectral imagery. The two band results were later applied to two large sample experiments with 25 g and 1 kg of corn per sample. The detection accuracies were 85% and 95% when 100 ppb threshold was used. Since the data acquisition period is significantly lower for several image bands than for full wavelength hyperspectral data, this study would be helpful in the development of real-time detection instrumentation for the corn industry. C1 [Yao, Haibo; Hruska, Zuzana; Kincaid, Russell; Ononye, Ambrose] Mississippi State Univ, Geosyst Res Inst, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. RP Yao, HB (reprint author), Mississippi State Univ, Geosyst Res Inst, Stennis Space Ctr, Bldg 1103,Suite 118, Stennis Space Ctr, MS 39529 USA. EM haibo@gri.msstate.edu NR 13 TC 1 Z9 1 U1 0 U2 8 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-601-1 J9 PROC SPIE PY 2011 VL 8027 AR 80270D DI 10.1117/12.884400 PG 9 WC Agriculture, Multidisciplinary; Food Science & Technology; Optics SC Agriculture; Food Science & Technology; Optics GA BVP10 UT WOS:000292147300011 ER PT S AU Tian, J Smith, WL AF Tian, Jialin Smith, William L., Sr. BE Meynart, R Neeck, SP Shimoda, H TI Principal Component Noise Filtering for NAST-I Radiometric Calibration SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES XV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites XV CY SEP 19-22, 2011 CL Prague, CZECH REPUBLIC SP SPIE DE NAST-I; radiometric calibration; principal component (PC) noise filtering; Fourier transform spectrometer (FTS); remote sensing AB The National Polar-orbiting Operational Environmental Satellite System (NPOESS) Airborne Sounder Testbed-Interferometer (NAST-I) instrument is a high-resolution scanning interferometer that measures emitted thermal radiation between 3.3 and 18 microns. The NAST-I radiometric calibration is achieved using internal blackbody calibration references at ambient and hot temperatures. In this paper, we introduce a refined calibration technique that utilizes a principal component (PC) noise filter to minimize the impact of measurement noise on the calibration of Earth scene radiance spectra. To test the procedure and estimate the PC filter noise performance, we form dependent and independent test samples using odd and even sets of blackbody spectra. To determine the optimal number of eigenvectors, the PC filter algorithm is applied to both dependent and independent blackbody spectra with a varying number of eigenvectors. The optimal number of PCs is selected so that the total root-mean-square (RMS) error of the calibrated reference scene blackbody data is minimized. To estimate the filter noise performance, we examine four different scenarios: apply PC filtering to both dependent and independent datasets, apply PC filtering to dependent calibration data only, apply PC filtering to independent data only, and no PC filtering. The independent blackbody radiances are predicted for each case and comparisons are made. The results show significant reduction in noise in the final calibrated scene radiances with the implementation of the PC filtering algorithm. C1 [Tian, Jialin] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Tian, J (reprint author), NASA, Langley Res Ctr, MS 472, Hampton, VA 23681 USA. EM Jialin.Tian-1@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-803-9 J9 PROC SPIE PY 2011 VL 8176 AR 81760V DI 10.1117/12.898407 PG 10 WC Engineering, Aerospace; Optics; Imaging Science & Photographic Technology SC Engineering; Optics; Imaging Science & Photographic Technology GA BXL74 UT WOS:000296319800024 ER PT B AU Cardace, D Hoehler, TM AF Cardace, Dawn Hoehler, Tori M. BE Harrison, S Rajakaruna, N TI Microbes in Extreme Environments Implications for Life on the Early Earth and Other Planets SO SERPENTINE: THE EVOLUTION AND ECOLOGY OF A MODEL SYSTEM LA English DT Article; Book Chapter ID PRESENT-DAY SERPENTINIZATION; DEEP SUBSEAFLOOR SEDIMENTS; SOUTH CHAMORRO SEAMOUNT; CITY HYDROTHERMAL FIELD; LOST CITY; SP NOV.; BACTERIAL DIVERSITY; SUBSURFACE LIFE; SEA SEDIMENTS; NEW-CALEDONIA C1 [Cardace, Dawn] Univ Rhode Isl, Kingston, RI 02881 USA. [Hoehler, Tori M.] NASA, Ames Res Ctr, Moffett Field, CA USA. RP Cardace, D (reprint author), Univ Rhode Isl, Kingston, RI 02881 USA. EM cardace@uri.edu; Tori.M.Hoehler@nasa.gov NR 70 TC 0 Z9 0 U1 5 U2 8 PU UNIV CALIFORNIA PRESS PI BERKELEY PA 2120 BERKELEY WAY, BERKELEY, CA 94720 USA BN 978-0-520-94845-7; 978-0-520-26835-7 PY 2011 BP 29 EP 48 D2 10.1525/california/9780520268357.001.0001 PG 20 WC Plant Sciences; Ecology; Environmental Sciences SC Plant Sciences; Environmental Sciences & Ecology GA BXK28 UT WOS:000296243200004 ER PT S AU Neudeck, PG Prokop, NF Greer, LC Chen, LY Krasowski, MJ AF Neudeck, Philip G. Prokop, Norman F. Greer, Lawrence C., III Chen, Liang-Yu Krasowski, Michael J. BE Monakhov, EV Hornos, T Svensson, BG TI Low Earth Orbit Space Environment Testing of Extreme Temperature 6H-SiC JFETs on the International Space Station SO SILICON CARBIDE AND RELATED MATERIALS 2010 SE Materials Science Forum LA English DT Proceedings Paper CT 8th European Conference on Silicon Carbide and Related Materials CY AUG 29-SEP 02, 2010 CL Sundvolden Conf Ctr, Oslo, NORWAY SP Aixtron, Dow Corning, Birkeland Innovation, Centrotherm, CREE Inc, Gen Elect, LPE, Norden NordForsk, SiCED, SiCrystal AG, Res Council Norway, Univ Oslo HO Sundvolden Conf Ctr DE 6H-SiC; JFET; International Space Station; Low-Earth Orbit AB This paper reports long-term electrical results from two 6H-SiC junction field effect transistors (JFETs) presently being tested in Low Earth Orbit (LEO) space environment on the outside of the International Space Station (ISS). The JFETs have demonstrated excellent functionality and stability through 4600 hours of LEO space deployment. Observed changes in measured device characteristics tracked changes in measured temperature, consistent with well-known JFET temperature-dependent device physics. C1 [Neudeck, Philip G.; Prokop, Norman F.; Greer, Lawrence C., III; Krasowski, Michael J.] NASA, Glenn Res Ctr, MS 77-1,21000 Brookpk Rd, Cleveland, OH 44135 USA. [Chen, Liang-Yu] NASA, Glenn Res Ctr, OAI, Cleveland, OH 44135 USA. RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr, MS 77-1,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Neudeck@nasa.gov; Norman.F.Prokop@nasa.gov; liangyu.chen-1@nasa.gov FU US Naval Research Laboratory; NASA Aviation Safety; NASA Fundamental Aeronautics; NASA Electronic Parts FX MISSE-7 funding and implementation by US Naval Research Laboratory under the direction of Dr. Phillip Jenkins. The authors are also grateful for the assistance of Robert Buttler, Joe Flatico, Dan Spina, and Ed Sechkar. Device fabrication was funded by NASA Aviation Safety, NASA Fundamental Aeronautics, and NASA Electronic Parts and Packaging programs. NR 9 TC 2 Z9 2 U1 0 U2 1 PU TRANS TECH PUBLICATIONS LTD PI DURNTEN-ZURICH PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2011 VL 679-680 BP 579 EP + DI 10.4028/www.scientific.net/MSF.679-680.579 PG 2 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA BVJ83 UT WOS:000291673500139 ER PT S AU Speer, KM Neudeck, PG Mehregany, M AF Speer, Kevin M. Neudeck, Philip G. Mehregany, Mehran BE Monakhov, EV Hornos, T Svensson, BG TI Use of vacuum as a gate dielectric: the SiC VacFET SO SILICON CARBIDE AND RELATED MATERIALS 2010 SE Materials Science Forum LA English DT Proceedings Paper CT 8th European Conference on Silicon Carbide and Related Materials CY AUG 29-SEP 02, 2010 CL Sundvolden Conf Ctr, Oslo, NORWAY SP Aixtron, Dow Corning, Birkeland Innovation, Centrotherm, CREE Inc, Gen Elect, LPE, Norden NordForsk, SiCED, SiCrystal AG, Res Council Norway, Univ Oslo HO Sundvolden Conf Ctr DE Silicon carbide; field-effect transistor; vacuum dielectric; semiconductor interfaces ID SIC/SIO2 INTERFACES; PASSIVATION; RELIABILITY; NITROGEN AB We introduce the vacuum field-effect transistor (VacFET), the first SiC FET to use a vacuum-sealed cavity in place of the traditional, solid gate dielectric. This device architecture eliminates the need to thermally oxidize the SiC surface, a practice which has been widely reported to inhibit the performance and reliability of SiC MOSFETs. Using a combination of batch-compatible electronics and micromachining processing techniques, a polycrystalline SiC bridge is suspended above a 4H-SiC substrate, and the underlying cavity is sealed under vacuum. The fundamental studies made possible by such a device could shed much-needed light on the basic electronic properties of an inverted SiC surface. In this introductory report, we detail the analytical design and fabrication necessary to manufacture the VacFET, and we also demonstrate proof of the concept using turn-on and output characteristics of the first functional SiC device. C1 [Speer, Kevin M.; Mehregany, Mehran] Case Western Reserve Univ, Dept Elect Engn & Comp Sci, 10900 Euclid Ave, Cleveland, OH 44106 USA. [Neudeck, Philip G.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Speer, KM (reprint author), Case Western Reserve Univ, Dept Elect Engn & Comp Sci, 10900 Euclid Ave, Cleveland, OH 44106 USA. EM kevin.m.speer@ieee.org; Neudeck@nasa.gov; mehran@case.edu FU DARPA [N66001-07-12031] FX This work was funded by DARPA grant #N66001-07-12031. The authors are grateful for valuable technical discussions with Dr. Kevin Matocha (GE), Dr. Ty McNutt (APEI), Prof. Christian Zorman (CWRU), and Mr. David Spry (NASA Glenn), and help from Dr. Glenn Beheim and Mr. Charles Blaha of NASA Glenn. NR 13 TC 1 Z9 1 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI DURNTEN-ZURICH PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2011 VL 679-680 BP 657 EP + DI 10.4028/www.scientific.net/MSF.679-680.657 PG 2 WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA BVJ83 UT WOS:000291673500158 ER PT J AU Pasachoff, JM Tingle, ED Dammasch, IE Sterling, AC AF Pasachoff, Jay M. Tingle, Evan D. Dammasch, Ingolf E. Sterling, Alphonse C. TI Simultaneous Observations of the Chromosphere with TRACE and SUMER SO SOLAR PHYSICS LA English DT Article DE Chromosphere; Corona; Transition zone; SUMER; TRACE ID X-RAY TELESCOPE; CORONAL JETS; HINODE XRT; SOLAR; YOHKOH AB Using mainly the 1600 continuum channel and also the 1216 Lyman-alpha channel (which includes some UV continuum and C iv emission) aboard the TRACE satellite, we observed the complete lifetime of a transient, bright chromospheric loop. Simultaneous observations with the SUMER instrument aboard the SOHO spacecraft revealed interesting material velocities through the Doppler effect existing above the chromospheric loop imaged with TRACE, possibly corresponding to extended nonvisible loops, or the base of an X-ray jet. C1 [Pasachoff, Jay M.] Williams Coll, Hopkins Observ, Williamstown, MA 01267 USA. [Pasachoff, Jay M.] CALTECH, Pasadena, CA 91125 USA. [Tingle, Evan D.] Harvard Smithsonian Ctr Astrophys, Middletown, CT 06459 USA. [Dammasch, Ingolf E.] Solar Influences Data Anal Ctr SIDC, Royal Observ Belgium, B-1180 Brussels, Belgium. [Sterling, Alphonse C.] NASA, MSFC, Space Sci Off VP62, Huntsville, AL 35805 USA. RP Pasachoff, JM (reprint author), Williams Coll, Hopkins Observ, Williamstown, MA 01267 USA. EM jay.m.pasachoff@williams.edu FU NASA [NNG04GF99G, NNG04GK44G]; NASA's Marshall Space Flight Center [NNM07AA01G, NNX10AK47A]; National Science Foundation; Keck Foundation; NASA's Office of Space Science FX Our work was funded in part by NASA grants NNG04GF99G and NNG04GK44G from the Solar Terrestrial Program and grants NNM07AA01G and NNX10AK47A from NASA's Marshall Space Flight Center. E.D.T.'s participation was sponsored by a grant from the Research Experiences for Undergraduate Program of the National Science Foundation to the Keck Northeast Astronomy Consortium, formerly sponsored by the Keck Foundation. A. C. S. was supported by funding from NASA's Office of Space Science through the Living with a Star, the Solar Physics Supporting Research and Technology, and the Sun-Earth Connection Guest Investigator Programs. SOHO is a joint project of the European Space Agency and NASA. TRACE is a project of NASA, with its telescope from the Smithsonian Astrophysical Observatory and overall direction from the Lockheed Martin Solar and Astrophysics Laboratory. NR 19 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JAN PY 2011 VL 268 IS 1 BP 151 EP 163 DI 10.1007/s11207-010-9673-6 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 695IS UT WOS:000285364400006 ER PT S AU Davila, JM AF Davila, Joseph M. BE Fineschi, S Fennelly, J TI High-resolution solar imaging with a photon sieve SO SOLAR PHYSICS AND SPACE WEATHER INSTRUMENTATION IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Solar Physics and Space Weather Instrumentation IV CY AUG 21-24, 2011 CL San Diego, CA SP SPIE DE sun; corona; coronal heating ID TELESCOPES AB Dissipation in the solar corona is expected to occur in extremely thin current sheets of order 1-100 km. Emission from these current sheets should be visible in coronal EUV emission lines. However, this spatial scale is far below the resolution of existing imaging instruments. Conventional optics cannot be easily manufactured with sufficient surface figure accuracy to obtain the required < 0.1 arcsec resolution. A photon sieve, a diffractive imaging element similar to a Fresnel zone plate, can be manufactured to provide a few 0.001 arcsec resolution, with much more relaxed tolerances than conventional imaging technology. A simple design for a sounding rocket payload is presented that obtains 80 mas (0.080 arcsec) imaging with a 100 mm diameter photon sieve to image Fe XIV 334 and Fe XVI 335. These images will not only show the structure of the corona at a resolution never before obtained, they will also allow a study of the temperature structure in the dissipation region. C1 NASA, Goddard Space Flight Ctr, Senior Scientist Heliophys Div, Greenbelt, MD 20771 USA. RP Davila, JM (reprint author), NASA, Goddard Space Flight Ctr, Senior Scientist Heliophys Div, Code 670, Greenbelt, MD 20771 USA. NR 12 TC 3 Z9 4 U1 3 U2 5 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-758-2 J9 PROC SPIE PY 2011 VL 8148 AR 81480O DI 10.1117/12.898956 PG 11 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BXZ21 UT WOS:000297671900022 ER PT S AU Gopalswamy, N Davila, JM Auchere, F Schou, J Korendyke, C Shih, A Johnston, JC MacDowall, RJ Maksimovic, M Sittler, E Szabo, A Wesenberg, R Vennerstrom, S Heber, B AF Gopalswamy, Nat Davila, Joseph M. Auchere, Frederic Schou, Jesper Korendyke, Clarence Shih, Albert Johnston, Janet C. MacDowall, Robert J. Maksimovic, Milan Sittler, Edward Szabo, Adam Wesenberg, Richard Vennerstrom, Suzanne Heber, Bernd BE Fineschi, S Fennelly, J TI Earth-Affecting Solar Causes Observatory (EASCO): A mission at the Sun-Earth L5 SO SOLAR PHYSICS AND SPACE WEATHER INSTRUMENTATION IV SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Solar Physics and Space Weather Instrumentation IV CY AUG 21-24, 2011 CL San Diego, CA SP SPIE DE Coronal mass ejections; corotating interaction regions; Sun-Earth L5; solar electric propulsion; helioseismology; coronagraph; heliospheric imager; EASCO mission design AB Coronal mass ejections (CMEs) and corotating interaction regions (CIRs) as well as their source regions are important because of their space weather consequences. The current understanding of CMEs primarily comes from the Solar and Heliospheric Observatory (SOHO) and the Solar Terrestrial Relations Observatory (STEREO) missions, but these missions lacked some key measurements: STEREO did not have a magnetograph; SOHO did not have in-situ magnetometer. SOHO and other imagers such as the Solar Mass Ejection Imager (SMEI) located on the Sun-Earth line are also not well-suited to measure Earth-directed CMEs. The Earth-Affecting Solar Causes Observatory (EASCO) is a proposed mission to be located at the Sun-Earth L5 that overcomes these deficiencies. The mission concept was recently studied at the Mission Design Laboratory (MDL), NASA Goddard Space Flight Center, to see how the mission can be implemented. The study found that the scientific payload (seven remote-sensing and three in-situ instruments) can be readily accommodated and can be launched using an intermediate size vehicle; a hybrid propulsion system consisting of a Xenon ion thruster and hydrazine has been found to be adequate to place the payload at L5. Following a 2-year transfer time, a 4-year operation is considered around the next solar maximum in 2025. C1 [Gopalswamy, Nat; Davila, Joseph M.; Shih, Albert; MacDowall, Robert J.; Sittler, Edward; Szabo, Adam; Wesenberg, Richard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM nat.gopalswamy@nasa.gov RI MacDowall, Robert/D-2773-2012; Gopalswamy, Nat/D-3659-2012; Shih, Albert/D-4714-2012; OI Auchere, Frederic/0000-0003-0972-7022 NR 6 TC 3 Z9 3 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-81948-758-2 J9 PROC SPIE PY 2011 VL 8148 AR 81480Z DI 10.1117/12.901538 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BXZ21 UT WOS:000297671900030 ER PT S AU Prasad, NS Rosiewicz, A Coleman, SM AF Prasad, Narasimha S. Rosiewicz, Alex Coleman, Steven M. BE Clarkson, WA Hodgson, N Shori, R TI Development of a low SWaP laser transmitter for atmospheric lidar applications SO SOLID STATE LASERS XX: TECHNOLOGY AND DEVICES SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Solid State Lasers XX - Technology and Devices CY JAN 23-27, 2011 CL San Francisco, CA SP SPIE DE ASCENDS; CO(2); O(2); DFB laser diode AB NASA Langley Research Center (LaRC) is working on a prototype laser system for simultaneous measurement of CO(2) and O(2) for planned Active Sensing of CO(2) Emissions over Nights, Days, and Seasons (ASCENDS) mission application. For this purpose, 1571 nm spectral band for CO(2) sensing and 1262 nm spectral band for oxygen sensing have been selected. In this paper, we discuss recent progress made in the development of single mode, compact and stable, seed laser technologies for CO(2) and O(2) transmitters. In particular, the development of an advanced distributed feedback laser (DFB) module master oscillator operating at 1571 nm, that is efficiently coupled to drive electronics and nano-cooling scheme in a single hermetically sealed package of volume less than 2 '' x 2 '' x 0.5 '', is presented. C1 [Prasad, Narasimha S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Prasad, NS (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8449-9 J9 PROC SPIE PY 2011 VL 7912 AR 791206 DI 10.1117/12.878856 PG 8 WC Optics; Physics, Applied SC Optics; Physics GA BXZ84 UT WOS:000297726600003 ER PT S AU Clark, PE Curtis, SA Rilee, ML AF Clark, P. E. Curtis, S. A. Rilee, M. L. BE Robertson, GA TI A New Paradigm for Robotic Rovers SO SPACE, PROPULSION AND ENERGY SCIENCES INTERNATIONAL FORUM SE Physics Procedia LA English DT Proceedings Paper CT Space, Propulsion and Energy Sciences International Forum CY MAR 15-17, 2011 CL Univ Maryland, Coll Park, MD SP Inst Adv Studies Space, Prop & Energy Sci (IASSPES), Integr Res Inst (IRI), Amer Astronaut Soc, Astrosociol Res Inst, Nucl Plasma Soc HO Univ Maryland DE Robotics; Rovers; Extreme Mobility; Space Exploration ID TETRAHEDRAL ROVERS AB We are in the process of developing rovers with extreme mobility needed to explore remote, rugged terrain. We call these systems Tetrahedral Explorer Technologies (TETs). Architecture is based on conformable tetrahedra, the simplest space-filling form, as building blocks, single or networked, where apices act as nodes from which struts reversibly deploy. The tetrahedral framework acts as a simple skeletal muscular structure. We have already prototyped a simple robotic walker from a single reconfigurable tetrahedron capable of tumbling and a more evolved 12Tetrahedral Walker, the Autonomous Landed Investigator (ALI), which has interior nodes for payload, more continuous motion, and is commandable through a user friendly interface. ALI is an EMS level mission concept which would allow autonomous in situ exploration of the lunar poles within the next decade. ALI would consist of one or more 12tetrahedral walkers capable of rapid locomotion with the many degrees of freedom and equipped for navigation in the unilluminated, inaccessible and thus largely unexplored rugged terrains where lunar resources are likely to be found: the Polar Regions. ALI walkers would act as roving reconnaissance teams for unexplored regions, analyzing samples along the way. (C) 2011 Published by Elsevier B.V. Selection and/or peer-review under responsibility of Institute for Advanced studies in Space, Propulsion and Energy Sciences C1 [Clark, P. E.; Curtis, S. A.; Rilee, M. L.] NASA GSFC, Greenbelt, MD 20771 USA. RP Clark, PE (reprint author), NASA GSFC, Code 695, Greenbelt, MD 20771 USA. EM pamela.clark@gsfc.nasa.gov NR 12 TC 6 Z9 7 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1875-3892 J9 PHYSCS PROC PY 2011 VL 20 DI 10.1016/j.phpro.2011.08.028 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BYP01 UT WOS:000299526500027 ER PT S AU Clark, PE Millar, PS Yeh, PS Feng, S Brigham, D Beaman, B AF Clark, P. E. Millar, P. S. Yeh, P. S. Feng, S. Brigham, D. Beaman, B. BE Robertson, GA TI Small Cold Temperature Instrument Packages SO SPACE, PROPULSION AND ENERGY SCIENCES INTERNATIONAL FORUM SE Physics Procedia LA English DT Proceedings Paper CT Space, Propulsion and Energy Sciences International Forum CY MAR 15-17, 2011 CL Univ Maryland, Coll Park, MD SP Inst Adv Studies Space, Prop & Energy Sci (IASSPES), Integr Res Inst (IRI), Amer Astronaut Soc, Astrosociol Res Inst, Nucl Plasma Soc HO Univ Maryland DE Space Instruments; Mechanical; Thermal; Electronic Design; Power System; Surface Measurements AB We are developing a small cold temperature instrument package concept that integrates a cold temperature power system with ultra low temperature ultra low power electronics components and power supplies now under development into a 'cold temperature surface operational' version of a planetary surface instrument package. We are already in the process of developing a lower power lower temperature version for an instrument of mutual interest to SMD and ESMD to support the search for volatiles (the mass spectrometer VAPoR, Volatile Analysis by Pyrolysis of Regolith) both as a stand alone instrument and as part of an environmental monitoring package. We build on our previous work to develop strategies for incorporating Ultra Low Temperature/Ultra Low Power (ULT/ULP) electronics, lower voltage power supplies, as well as innovative thermal design concepts for instrument packages. Cryotesting has indicated that our small Si RHBD CMOS chips can deliver >80% of room temperature performance at 40K (nominal minimum lunar surface temperature). We leverage collaborations, past and current, with the JPL battery development program to increase power system efficiency in extreme environments. We harness advances in MOSFET technology that provide lower voltage thresholds for power switching circuits incorporated into our low voltage power supply concept. Conventional power conversion has a lower efficiency. Our low power circuit concept based on 'synchronous rectification' could produce stable voltages as low as 0.6V with 85% efficiency. Our distributed micro-battery-based power supply concept incorporates cold temperature power supplies operating with a 4V or 8V battery. This work will allow us to provide guidelines for applying the low temperature, low power system approaches generically to the widest range of surface instruments. (C) 2011 Published by Elsevier B.V. Selection and/or peer-review under responsibility of Institute for Advanced studies in Space, Propulsion and Energy Sciences C1 [Clark, P. E.; Millar, P. S.; Yeh, P. S.; Feng, S.; Brigham, D.; Beaman, B.] NASA GSFC, Greenbelt, MD 20770 USA. RP Clark, PE (reprint author), NASA GSFC, Greenbelt, MD 20770 USA. EM Pamela.E.Clark@NASA.gov NR 7 TC 0 Z9 1 U1 1 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1875-3892 J9 PHYSCS PROC PY 2011 VL 20 DI 10.1016/j.phpro.2011.08.027 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics SC Engineering; Astronomy & Astrophysics GA BYP01 UT WOS:000299526500026 ER PT J AU Gonzalez, WD Echer, E Tsurutani, BT de Gonzalez, ALC Dal Lago, A AF Gonzalez, Walter D. Echer, Ezequiel Tsurutani, Bruce T. Clua de Gonzalez, Alicia L. Dal Lago, Alisson TI Interplanetary Origin of Intense, Superintense and Extreme Geomagnetic Storms SO SPACE SCIENCE REVIEWS LA English DT Review DE Intense geomagnetic storms; Geomagnetic activity; Extreme geomagnetic storms ID COROTATING INTERACTION REGIONS; SOLAR-WIND; MAGNETIC STORMS; NOVEMBER 2003; MAXIMUM; FIELD; DST; GEOEFFECTIVENESS; CLOUDS; SATURATION AB We present a review on the interplanetary causes of intense geomagnetic storms (Dsta parts per thousand currency signa'100 nT), that occurred during solar cycle 23 (1997-2005). It was reported that the most common interplanetary structures leading to the development of intense storms were: magnetic clouds, sheath fields, sheath fields followed by a magnetic cloud and corotating interaction regions at the leading fronts of high speed streams. However, the relative importance of each of those driving structures has been shown to vary with the solar cycle phase. Superintense storms (Dsta parts per thousand currency signa'250 nT) have been also studied in more detail for solar cycle 23, confirming initial studies done about their main interplanetary causes. The storms are associated with magnetic clouds and sheath fields following interplanetary shocks, although they frequently involve consecutive and complex ICME structures. Concerning extreme storms (Dsta parts per thousand currency signa'400 nT), due to the poor statistics of their occurrence during the space era, only some indications about their main interplanetary causes are known. For the most extreme events, we review the Carrington event and also discuss the distribution of historical and space era extreme events in the context of the sunspot and Gleissberg solar activity cycles, highlighting a discussion about the eventual occurrence of more Carrington-type storms. C1 [Gonzalez, Walter D.; Echer, Ezequiel; Clua de Gonzalez, Alicia L.; Dal Lago, Alisson] Natl Inst Space Res, Sao Jose Dos Campos, SP, Brazil. [Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Gonzalez, WD (reprint author), Natl Inst Space Res, Sao Jose Dos Campos, SP, Brazil. EM gonzalez@dge.inpe.br RI Tecnologias espaciai, Inct/I-2415-2013 FU "Fundacao de Amparo a Pesquisa do Estado de Sao Paulo", FAPESP [2008/06650-9, 2007/52533-1]; "Conselho Nacional de Pesquisas", CNPq [PQ-300321/2005-8, PQ-300211/2008-2, PQ-342734/2008-2]; NASA FX W. D. G. would like to thank the "Fundacao de Amparo a Pesquisa do Estado de Sao Paulo", FAPESP (2008/06650-9) and the "Conselho Nacional de Pesquisas", CNPq (PQ-300321/2005-8). E. E. would like to thank the FAPESP (2007/52533-1) and CNPq (PQ-300211/2008-2) and A. L. C. G. would like to thank CNPq (PQ-342734/2008-2). Portions of this work were done at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. NR 57 TC 22 Z9 23 U1 2 U2 5 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 JAN PY 2011 VL 158 IS 1 BP 69 EP 89 DI 10.1007/s11214-010-9715-2 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 763FH UT WOS:000290540100004 ER PT J AU Scott, JM Warburton, DER Williams, D Whelan, S Krassioukov, A AF Scott, J. M. Warburton, D. E. R. Williams, D. Whelan, S. Krassioukov, A. TI Challenges, concerns and common problems: physiological consequences of spinal cord injury and microgravity SO SPINAL CORD LA English DT Review DE SCI; spaceflight; muscle atrophy; orthostatic hypotension ID SHORT-DURATION SPACEFLIGHT; MULTIPLE SYSTEM ATROPHY; PURE AUTONOMIC FAILURE; BODY NEGATIVE-PRESSURE; BONE-MINERAL CONTENT; DOWN BED REST; HEAD-UP TILT; ORTHOSTATIC HYPOTENSION; SKELETAL-MUSCLE; SPACE-FLIGHT AB Introduction: Similarities between the clinical presentation of individuals living with spinal cord injury (SCI) and astronauts are remarkable, and may be of great interest to clinicians and scientists alike. Objectives: The primary purpose of this review is to outline the manner in which cardiovascular, musculoskeletal, renal, immune and sensory motor systems are affected by microgravity and SCI. Methods: A comprehensive review of the literature was conducted (using PubMed) to evaluate the hallmark symptoms seen after spaceflight and SCI. This literature was then examined critically to determine symptoms common to both populations. Results: Both SCI and prolonged microgravity exposure are associated with marked deteriorations in various physiological functions. Atrophy in muscle and bone, cardiovascular disturbances, and alterations in renal, immune and sensory motor systems are conditions commonly observed not only in individuals with SCI, but also in those who experience prolonged gravity unloading. Conclusion: The preponderance of data indicates that similar physiological changes occur in both SCI and prolonged space flight. These findings have important implications for future research in SCI and prolonged space flight. Spinal Cord (2011) 49, 4-16; doi: 10.1038/sc.2010.53; published online 25 May 2010 C1 [Scott, J. M.; Warburton, D. E. R.] Univ British Columbia, Dept Educ, Cardiovasc Physiol & Rehabil Lab, Vancouver, BC V5Z 1M9, Canada. [Warburton, D. E. R.] Univ British Columbia, Dept Med, Fac Expt Med, Vancouver, BC, Canada. [Warburton, D. E. R.; Krassioukov, A.] Int Collaborat Repair Discoveries, Vancouver, BC, Canada. [Williams, D.; Whelan, S.; Krassioukov, A.] McMaster Univ, Dept Surg, Hamilton, ON L8S 4L8, Canada. [Krassioukov, A.] Univ British Columbia, Dept Med, Fac Phys Med & Rehabil, Vancouver, BC, Canada. [Krassioukov, A.] Vancouver Coastal Hlth, GF Strong Rehabil Ctr, Spinal Cord Program, Vancouver, BC, Canada. RP Scott, JM (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM jessica.m.scott@nasa.gov FU Canadian Institutes of Health Research; International Collaboration on Repair Discoveries; Heart and Stroke Foundation; Christopher and Dana Reeve Foundation; Natural Sciences and Engineering Research Council of Canada; MSFHR FX Dr Warburton is supported by a career award from the Canadian Institutes of Health Research and is a Michael Smith Foundation for Health Research (MSFHR) Clinical Scholar. Dr Krassioukov is supported by International Collaboration on Repair Discoveries, the Heart and Stroke Foundation, and Christopher and Dana Reeve Foundation. Jessica Scott was supported by doctoral graduate scholarships from the Natural Sciences and Engineering Research Council of Canada and the MSFHR. NR 120 TC 13 Z9 13 U1 1 U2 14 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1362-4393 J9 SPINAL CORD JI Spinal Cord PD JAN PY 2011 VL 49 IS 1 BP 4 EP 16 DI 10.1038/sc.2010.53 PG 13 WC Clinical Neurology; Rehabilitation SC Neurosciences & Neurology; Rehabilitation GA 703QU UT WOS:000285996800003 PM 20498665 ER PT J AU Hafiychuk, V Luchinsky, DG Smelyanskiy, VN Tyson, R Miller, J Banks, C AF Hafiychuk, V. Luchinsky, D. G. Smelyanskiy, V. N. Tyson, R. Miller, J. Banks, C. BE Chang, FK TI Comparisons of SHM Sensor Models with Empirical Test Data for Sandwich Composite Structures SO STRUCTURAL HEALTH MONITORING 2011: CONDITION-BASED MAINTENANCE AND INTELLIGENT STRUCTURES, VOL 1 SE Structural Health Monitoring LA English DT Proceedings Paper CT 8th International Workshop on Structural Health Monitoring CY SEP 13-15, 2011 CL Stanford Univ, Stanford, CA SP AF Off Sci Res, Army Res Off, Natl Sci Fdn, Off Naval Res HO Stanford Univ ID SCATTERING; WAVES; PLATE AB This paper reports on analytical work, as well as experimental testing, that were accomplished at the Ames Research Center and at the Marshall Space Flight Center to examine acoustic wave propagating and the ability to detect intrinsic faults in sandwich type composite structures. Sandwich type composites are being studied for use in NASAs new heavy lift launch vehicle and flaw detection is crucial for safety and for failure prognostics. The work reported on in this paper involved both the theoretical modeling as well as comparison with empirical testing needed to answer the question of feasibility for reliable, and accurate, structural health monitoring (SHM) in the composite structure of interest. The analytical model of the transient wave propagation and scattering based on the Mindlin plate theory was developed. A scattered transient field properties are calculated theoretically using this model and numerically using the finite element model for acoustic waves generated by an acoustic-patch actuator. It is shown that theoretical results are in agreement with the results of numerical simulations and with experimental results. C1 [Hafiychuk, V.; Luchinsky, D. G.; Smelyanskiy, V. N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Hafiychuk, V (reprint author), NASA, Ames Res Ctr, Mail Stop 269-3, Moffett Field, CA 94035 USA. RI Luchinsky, Dmitry/N-4177-2014 NR 8 TC 0 Z9 0 U1 0 U2 1 PU DESTECH PUBLICATIONS, INC PI LANCASTER PA 439 DUKE STREET, LANCASTER, PA 17602-4967 USA BN 978-1-60595-053-2 J9 STRUCT HLTH MONIT PY 2011 BP 413 EP 420 PG 8 WC Endocrinology & Metabolism; Instruments & Instrumentation SC Endocrinology & Metabolism; Instruments & Instrumentation GA BXY69 UT WOS:000297634100049 ER PT J AU Tessler, A Spangler, JL Mattone, M Gherlone, M Di Sciuva, M AF Tessler, A. Spangler, J. L. Mattone, M. Gherlone, M. Di Sciuva, M. BE Chang, FK TI Real-Time Characterization of Aerospace Structures Using Onboard Strain Measurement Technologies and Inverse Finite Element Method SO STRUCTURAL HEALTH MONITORING 2011: CONDITION-BASED MAINTENANCE AND INTELLIGENT STRUCTURES, VOL 1 SE Structural Health Monitoring LA English DT Proceedings Paper CT 8th International Workshop on Structural Health Monitoring CY SEP 13-15, 2011 CL Stanford Univ, Stanford, CA SP AF Off Sci Res, Army Res Off, Natl Sci Fdn, Off Naval Res HO Stanford Univ ID SHEAR AB The inverse problem of real-time reconstruction of full-field structural displacements, strains, and stresses is addressed using an inverse finite element method based on shear deformable shell finite element technology. Utilizing surface strain measurements from strain sensors mounted on load-carrying structural components, the methodology enables accurate computations of the three-dimensional displacement field for a general built-up shell structure undergoing multi-axial deformations. The strain and stress computations are then carried out at the element level using strain-displacement and constitutive relations. This high fidelity computational technology is essential for providing feedback to the actuation and control systems of the next generation of aerospace vehicles, and for assessing real-time internal loads and structural integrity. C1 [Tessler, A.] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. RP Tessler, A (reprint author), NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Mail Stop 190, Hampton, VA 23681 USA. OI Gherlone, Marco/0000-0002-5711-0046 NR 9 TC 2 Z9 2 U1 0 U2 1 PU DESTECH PUBLICATIONS, INC PI LANCASTER PA 439 DUKE STREET, LANCASTER, PA 17602-4967 USA BN 978-1-60595-053-2 J9 STRUCT HLTH MONIT PY 2011 BP 981 EP 988 PG 8 WC Endocrinology & Metabolism; Instruments & Instrumentation SC Endocrinology & Metabolism; Instruments & Instrumentation GA BXY69 UT WOS:000297634100119 ER PT S AU Ma, WP Jacobs, G Keogh, R Yen, CH Klettlinger, JLS Davis, BH AF Ma, Wenping Jacobs, Gary Keogh, Robert Yen, Chia H. Klettlinger, Jennifer L. S. Davis, Burtron H. BE DeKlerk, A King, DL TI Fischer-Tropsch Synthesis: Effect of Pt Promoter on Activity, Selectivities to Hydrocarbons and Oxygenates, and Kinetic Parameters over 15%Co/Al2O3 SO SYNTHETIC LIQUIDS PRODUCTION AND REFINING SE ACS Symposium Series LA English DT Proceedings Paper CT Symposium on Coal, Gas, Biomass and Waste-to-Liquids Conversion CY AUG, 2010 CL Boston, MA SP ACS, Div Fuel Chem DE Fischer-Tropsch synthesis; Pt-Co/Al2O3; Co metal; CoO; Pt; hydrocarbon selectivity; oxygenate selectivity; kinetics ID SUPPORTED COBALT CATALYSTS; CO HYDROGENATION; IRON CATALYSTS; RU; REDUCTION; CO/AL2O3; PERFORMANCE; ADSORPTION; REACTOR; DESIGN AB The effect of Pt promoter on the catalytic performance of 15%Co/Al2O3 catalyst was studied in a 1-L continuously stirred tank reactor (CSTR). Catalytic performance parameters investigated include catalyst activity, CH4 and C5+ selectivities, olefin and paraffin contents, 1-olefin and 2-olefin selectivities, oxygenate selectivity, and kinetic behavior. The addition of 0.5% Pt increased the CO hydrogenation rate constant by 140%, consistent with the finding that the Pt promoter significantly increased Co reduction and thus the number of surface Co-0 sites. However, Pt did not alter Co site time yield (STY). Both the unpromoted and Pt promoted 15%Co/Al2O3 catalysts displayed the same Co STY value at 220 degrees C, 5.5x10(-3) s(-1). A comparison of selectivities of the unpromoted and Pt promoted 15%Co/Al2O3 was made at similar CO conversion levels. The Pt promoter increased light hydrocarbon (C-2-C-4) formation and simultaneously decreased heavier hydrocarbon formation, probably due to hydrogen dissociation on Pt metal and spillover onto Co metal, leading to an increase in the chain termination rate. Pt promoter did not apparently change the overall olefin and paraffin contents, but CO conversion was found to be a primary factor in influencing secondary reactions of olefins on the 15%Co/Al2O3 catalyst. Furthermore, 0.3-1.0% water soluble oxygenates were found to be formed on the Co catalyst. At similar CO conversion levels, Pt slightly improved the oxygenates selectivity. Effects of CO conversion and H-2/CO ratio on hydrocarbon and oxygenate selectivities are also discussed in this paper. Finally, the kinetic behavior of both unpromoted and Pt promoted 15%Co/Al2O3 catalysts was studied using the CAER kinetic model, -r(CO) = kP(CO)(a)P(H2)(b)/(1 + mP(H2O)/P-H2). Kinetic parameters for both catalysts were assessed and are reported in this study. C1 [Ma, Wenping; Jacobs, Gary; Keogh, Robert; Davis, Burtron H.] Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA. [Yen, Chia H.; Klettlinger, Jennifer L. S.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Ma, WP (reprint author), Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA. EM davis@caer.uky.edu RI Jacobs, Gary/M-5349-2015 OI Jacobs, Gary/0000-0003-0691-6717 NR 47 TC 1 Z9 1 U1 0 U2 7 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 SIXTEENTH ST NW, WASHINGTON, DC 20036 USA SN 0097-6156 BN 978-0-8412-2681-4 J9 ACS SYM SER JI ACS Symp. Ser. PY 2011 VL 1084 BP 127 EP + PG 4 WC Energy & Fuels SC Energy & Fuels GA BDE77 UT WOS:000312966300006 ER PT B AU Johnson, SB AF Johnson, Stephen B. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI The Theory of System Health Management SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 [Johnson, Stephen B.] NASA, Marshall Space Flight Ctr, Colorado Springs, CO 80919 USA. [Johnson, Stephen B.] Univ Colorado, Colorado Springs, CO 80907 USA. RP Johnson, SB (reprint author), NASA, Marshall Space Flight Ctr, Colorado Springs, CO 80919 USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 3 EP 27 D2 10.1002/9781119994053 PG 25 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800004 ER PT B AU Sauer, BA AF Sauer, Beverly A. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Multimodal Communication SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter ID GESTURE; SPEECH; RISK; NEGOTIATION; SYSTEMS; REVEAL C1 [Sauer, Beverly A.] BAS Consultants Inc, Mclean, VA 22101 USA. [Sauer, Beverly A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Sauer, BA (reprint author), BAS Consultants Inc, Mclean, VA 22101 USA. NR 97 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 29 EP 47 D2 10.1002/9781119994053 PG 19 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800005 ER PT B AU Johnson, SB AF Johnson, Stephen B. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI SYSTEM HEALTH MANAGEMENT WITH AEROSPACE APPLICATIONS Preface SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Editorial Material; Book Chapter C1 [Johnson, Stephen B.] NASA, Marshall Space Flight Ctr, Colorado Springs, CO 80904 USA. [Johnson, Stephen B.] Univ Colorado, Colorado Springs, CO 80907 USA. RP Johnson, SB (reprint author), NASA, Marshall Space Flight Ctr, Colorado Springs, CO 80904 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP XXXIII EP XXXIII D2 10.1002/9781119994053 PG 1 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800002 ER PT B AU Rogers, EW AF Rogers, Edward W. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Knowledge Management SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rogers, EW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 24 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 65 EP 76 D2 10.1002/9781119994053 PG 12 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800007 ER PT B AU Deal, RW Kessler, SS AF Deal, Ryan W. Kessler, Seth S. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Architecture SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 [Deal, Ryan W.] NASA, Marshall Space Flight Ctr, Greenbelt, MD 20771 USA. [Kessler, Seth S.] Metis Design Corp, Boston, MA USA. RP Deal, RW (reprint author), NASA, Marshall Space Flight Ctr, Greenbelt, MD 20771 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 115 EP 127 D2 10.1002/9781119994053 PG 13 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800011 ER PT B AU Mackey, RM AF Mackey, Ryan M. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Assessing and Maturing Technology Readiness Levels SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Mackey, RM (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. NR 11 TC 0 Z9 0 U1 0 U2 3 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 145 EP 157 D2 10.1002/9781119994053 PG 13 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800013 ER PT B AU Markosian, LZ Feather, MS Brinza, DE AF Markosian, Lawrence Z. Feather, Martin S. Brinza, David E. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Verification and Validation SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter ID SOFTWARE; TOOLS C1 [Markosian, Lawrence Z.] NASA, Stinger Ghaffarian Technol, Ames Res Ctr, Washington, DC 20546 USA. [Feather, Martin S.; Brinza, David E.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Markosian, LZ (reprint author), NASA, Stinger Ghaffarian Technol, Ames Res Ctr, Washington, DC 20546 USA. NR 39 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 159 EP 183 D2 10.1002/9781119994053 PG 25 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800014 ER PT B AU Patterson-Hine, A AF Patterson-Hine, Ann BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Analytical Methods SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Editorial Material; Book Chapter C1 NASA, Ames Res Ctr, Washington, DC 20546 USA. RP Patterson-Hine, A (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 197 EP 198 D2 10.1002/9781119994053 PG 2 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800016 ER PT B AU Lutz, R Nikora, A AF Lutz, Robyn Nikora, Allen BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Failure Assessment SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter ID SOFTWARE-RELIABILITY; TAXONOMY; SYSTEM C1 [Lutz, Robyn; Nikora, Allen] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. [Lutz, Robyn] Iowa State Univ, Ames, IA USA. RP Lutz, R (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. NR 52 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 219 EP 232 D2 10.1002/9781119994053 PG 14 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800018 ER PT B AU Vesely, WE AF Vesely, William E. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Probabilistic Risk Assessment SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 NASA Headquarters, Washington, DC 20546 USA. RP Vesely, WE (reprint author), NASA Headquarters, Washington, DC 20546 USA. NR 10 TC 2 Z9 2 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 253 EP 263 D2 10.1002/9781119994053 PG 11 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800020 ER PT B AU Patterson-Hine, A Aaseng, GB Biswas, G Narashimhan, S Pattipati, K AF Patterson-Hine, Ann Aaseng, Gordon B. Biswas, Gautam Narashimhan, Sriram Pattipati, Krishna BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Diagnosis SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter ID MODEL-BASED DIAGNOSIS; FAULT-DIAGNOSIS; SYSTEMS C1 [Patterson-Hine, Ann; Aaseng, Gordon B.] NASA, Ames Res Ctr, Washington, DC 20546 USA. [Biswas, Gautam] Vanderbilt Univ, Nashville, TN USA. [Pattipati, Krishna] Univ Connecticut, Storrs, CT USA. RP Patterson-Hine, A (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA. NR 65 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 265 EP 280 D2 10.1002/9781119994053 PG 16 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800021 ER PT B AU Roemer, MJ Byington, CS Kacprzynski, GJ Vachtsevanos, G Goebel, K AF Roemer, Michael J. Byington, Carl S. Kacprzynski, Gregory J. Vachtsevanos, George Goebel, Kai BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Prognostics SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter ID NEURAL NETWORK; SYSTEMS; MODEL C1 [Goebel, Kai] NASA, Ames Res Ctr, Washington, DC USA. NR 46 TC 1 Z9 1 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 281 EP 295 D2 10.1002/9781119994053 PG 15 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800022 ER PT B AU Hughitt, BK AF Hughitt, Brian K. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Quality Assurance SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 NASA Headquarters, Washington, DC 20546 USA. RP Hughitt, BK (reprint author), NASA Headquarters, Washington, DC 20546 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 299 EP 308 D2 10.1002/9781119994053 PG 10 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800024 ER PT B AU McCann, RS Spirkovska, L AF McCann, Robert S. Spirkovska, Lilly BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Human Factors SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 [McCann, Robert S.; Spirkovska, Lilly] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP McCann, RS (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA. NR 29 TC 1 Z9 1 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 319 EP 337 D2 10.1002/9781119994053 PG 19 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800026 ER PT B AU Waterman, RD Nicoli, PE Zide, AJ Waterman, SJ Perotti, JM Ferrell, RA Brown, BL AF Waterman, Robert D. Nicoli, Patricia E. Zide, Alan J. Waterman, Susan J. Perotti, Jose M. Ferrell, Robert A. Brown, Barbara L. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Launch Operations SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 [Waterman, Robert D.; Nicoli, Patricia E.; Zide, Alan J.; Waterman, Susan J.; Perotti, Jose M.; Ferrell, Robert A.] NASA, Kennedy Space Ctr, Merritt Isl, FL 32899 USA. [Brown, Barbara L.] NASA, Ames Res Ctr, Mountain View, CA USA. RP Waterman, RD (reprint author), NASA, Kennedy Space Ctr, Merritt Isl, FL 32899 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 339 EP 350 D2 10.1002/9781119994053 PG 12 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800027 ER PT B AU O'Hagan, B Crocker, A AF O'Hagan, Brian Crocker, Alan BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Fault Management Techniques in Human Spaceflight Operations SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 [O'Hagan, Brian; Crocker, Alan] NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP O'Hagan, B (reprint author), NASA, Johnson Space Ctr, Houston, TX 77058 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 351 EP 367 D2 10.1002/9781119994053 PG 17 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800028 ER PT B AU Hunter, GW Oberle, LG Baaklini, GY Perotti, JM Hong, T AF Hunter, Gary W. Oberle, Lawrence G. Baaklini, George Y. Perotti, Jose M. Hong, Todd BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Intelligent Sensors for Health Management SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 [Hunter, Gary W.; Oberle, Lawrence G.; Baaklini, George Y.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Perotti, Jose M.] NASA, Kennedy Space Ctr, Merritt Isl, FL USA. [Hong, Todd] NASA, Johnson Space Ctr, Houston, TX USA. RP Hunter, GW (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 13 TC 2 Z9 2 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 405 EP 418 D2 10.1002/9781119994053 PG 14 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800032 ER PT B AU Button, RM Chicatelli, A AF Button, Robert M. Chicatelli, Amy BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Electrical Power Health Management SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 [Button, Robert M.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Chicatelli, Amy] Qinetiq North Amer NASA Glenn Res Ctr, Cleveland, OH USA. RP Button, RM (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. NR 15 TC 1 Z9 1 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 429 EP 443 D2 10.1002/9781119994053 PG 15 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800034 ER PT B AU Watson, MD Varnavas, K Patrick, C Hodge, R Byington, CS Chau, S Baroth, EC AF Watson, Michael D. Varnavas, Kosta Patrick, Clint Hodge, Ron Byington, Carl S. Chau, Savio Baroth, Edmund C. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Avionics Health Management SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 [Watson, Michael D.; Varnavas, Kosta; Hodge, Ron] NASA, Marshall Space Flight Ctr, Huntsville, AL 35811 USA. [Patrick, Clint] US Army Integrated Air & Missile Def, Huntsville, AL USA. [Byington, Carl S.; Baroth, Edmund C.] Impact Technol, San Diego, CA USA. [Chau, Savio] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Watson, MD (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35811 USA. NR 25 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 445 EP 465 D2 10.1002/9781119994053 PG 21 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800035 ER PT B AU Brown, EN Kelley, AR Gormley, TJ AF Brown, Edward N. Kelley, Anthony R. Gormley, Thomas J. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Launch Vehicle Health Management SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 [Brown, Edward N.] Boeing Co, Chicago, IL 60606 USA. [Kelley, Anthony R.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA. [Gormley, Thomas J.] Gormley & Associates, Norwalk, CT USA. RP Brown, EN (reprint author), Boeing Co, Chicago, IL 60606 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 523 EP 541 D2 10.1002/9781119994053 PG 19 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800041 ER PT B AU Morgan, PS AF Morgan, Paula S. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Robotic Spacecraft Health Management SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter C1 CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Morgan, PS (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 543 EP 554 D2 10.1002/9781119994053 PG 12 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800042 ER PT B AU Dempsey, PJ Zakrajsek, JJ AF Dempsey, Paula J. Zakrajsek, James J. BE Johnson, SB Gormley, TJ Kessler, SS Mott, CD PattersonHine, A Reichard, KM Scandura, PA TI Rotorcraft Health Management SO SYSTEM HEALTH MANAGEMENT: WITH AEROSPACE APPLICATIONS LA English DT Article; Book Chapter ID VIBRATION; GEAR C1 [Dempsey, Paula J.; Zakrajsek, James J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Dempsey, PJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 40 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-1-119-99404-6; 978-0-470-74133-7 PY 2011 BP 577 EP 587 D2 10.1002/9781119994053 PG 11 WC Engineering, Aerospace; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BA6FH UT WOS:000337126800045 ER PT J AU Su, Z Roebeling, RA Schulz, J Holleman, I Levizzani, V Timmermans, WJ Rott, H Mognard-Campbell, N de Jeu, R Wagner, W Rodell, M Salama, MS Parodi, GN Wang, L AF Su, Z. Roebeling, R. A. Schulz, J. Holleman, I. Levizzani, V. Timmermans, W. J. Rott, H. Mognard-Campbell, N. de Jeu, R. Wagner, W. Rodell, M. Salama, M. S. Parodi, G. N. Wang, L. BE Wilderer, P TI Observation of Hydrological Processes Using Remote Sensing SO TREATISE ON WATER SCIENCE, VOL 2: THE SCIENCE OF HYDROLOGY LA English DT Article; Book Chapter ID SURFACE-ENERGY BALANCE; SOIL-MOISTURE RETRIEVAL; SNOW WATER EQUIVALENT; INHERENT OPTICAL-PROPERTIES; RESOLUTION IMAGING SPECTROMETER; SOUTHERN GREAT-PLAINS; TOPEX/POSEIDON SATELLITE ALTIMETRY; SPARSELY VEGETATED SURFACES; UPPER-TROPOSPHERIC HUMIDITY; SYNTHETIC-APERTURE RADAR C1 [Su, Z.; Timmermans, W. J.; Salama, M. S.; Parodi, G. N.; Wang, L.] Univ Twente, NL-7500 AE Enschede, Netherlands. [Roebeling, R. A.; Holleman, I.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Schulz, J.] Deutsch Wetterdienst, Offenbach, Germany. [Levizzani, V.] ISAC CNR, Bologna, Italy. [Rott, H.] Univ Innsbruck, A-6020 Innsbruck, Austria. [Mognard-Campbell, N.] OMP LEGOS, Toulouse, France. [de Jeu, R.] Vrije Univ Amsterdam, Amsterdam, Netherlands. [Wagner, W.] Vienna Univ Technol, A-1040 Vienna, Austria. [Rodell, M.] NASA GSFC, Greenbelt, MD USA. RP Su, Z (reprint author), Univ Twente, POB 217, NL-7500 AE Enschede, Netherlands. NR 451 TC 3 Z9 3 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS BN 978-0-444-53199-5 PY 2011 BP 351 EP 399 PG 49 WC Geosciences, Multidisciplinary; Water Resources SC Geology; Water Resources GA BA2FH UT WOS:000333356000015 ER PT J AU Oswald, FB Zaretsky, EV Poplawski, JV AF Oswald, Fred B. Zaretsky, Erwin V. Poplawski, Joseph V. TI Interference-Fit Life Factors for Ball Bearings SO TRIBOLOGY TRANSACTIONS LA English DT Article DE Interference Fit; Ball Bearings; Rolling Bearings; Fatigue Analysis; Contacts; Life Prediction Methods; Maintenance; Rolling Bearings; Rolling-Element Fatigue; Wear; Stress Analysis; Contacts ID ELASTOHYDRODYNAMIC CONTACT ZONE; STRESS FIELD; PREDICTION; FATIGUE AB The effect of hoop stresses on the rolling-element fatigue life of angular-contact and deep-groove ball bearings was determined for common inner-ring interference fits at the ABEC-5 tolerance level. The analysis was applied to over 1,150 bearing configurations and load cases. Hoop stresses were superimposed on the Hertzian principal stresses created by the applied bearing load to calculate the inner-race maximum shearing stress. The resulting fatigue life of the bearing was recalculated through a series of equations. The reduction in the fatigue life is presented as life factors that are applied to the unfactored bearing life. The life factors found in this study ranged from 1.00 (no life reduction)where there was no net interface pressureto a worst case of 0.38 (a 62% life reduction). For a given interference fit, the reduction in life is different for angular-contact and deep-groove ball bearings. Interference fits also affect the maximum Hertz stress-life relation. Experimental data of Czyzewski, showing the effect of interference fit on rolling-element fatigue life, were reanalyzed to determine the shear stress-life exponent. The Czyzewski data shear stress-life exponent c equals 8.77, compared with the assumed value of 9. Results are presented as tables and charts of life factors for angular-contact and deep-groove ball bearings with light, normal, and heavy loads and interference fits ranging from extremely light to extremely heavy. C1 [Oswald, Fred B.; Zaretsky, Erwin V.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Poplawski, Joseph V.] JV Poplawski & Associates, Bethlehem, PA 18018 USA. RP Oswald, FB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA. NR 27 TC 7 Z9 9 U1 0 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-2004 J9 TRIBOL T JI Tribol. Trans. PY 2011 VL 54 IS 1 BP 1 EP 20 AR PII 930099427 DI 10.1080/10402004.2010.512428 PG 20 WC Engineering, Mechanical SC Engineering GA 733RP UT WOS:000288280800001 ER PT J AU Vlcek, BL Zaretsky, EV AF Vlcek, Brian L. Zaretsky, Erwin V. TI Rolling-Element Fatigue Testing and Data Analysis-A Tutorial SO TRIBOLOGY TRANSACTIONS LA English DT Article DE Rolling-Element Fatigue; Bearing Fatigue Testing; Bench-Type Testing; Probabilistic Analysis of Fatigue Data; Weibull Analysis ID BEARING LIFE PREDICTION; CONTACT FATIGUE; ROLLER PROFILE AB In order to rank bearing materials, lubricants and other design variables using rolling-element bench-type fatigue testing of bearing components and full-scale rolling-element bearing tests, the investigator needs to be cognizant of the variables that affect rolling-element fatigue life and be able to maintain and control them within an acceptable experimental tolerance. Once these variables are controlled, the number of tests and the test conditions must be specified to assure reasonable statistical certainty of the final results. There is a reasonable correlation between the results from elemental test rigs with those results obtained with full-scale bearings. Using the statistical methods of Weibull and Johnson, the minimum number of tests required can be determined. This article brings together and discusses the technical aspects of rolling-element fatigue testing and data analysis and makes recommendations to assure quality and reliable testing of rolling-element specimens and full-scale rolling-element bearings. C1 [Vlcek, Brian L.] Georgia So Univ, Statesboro, GA 30460 USA. [Zaretsky, Erwin V.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Vlcek, BL (reprint author), Georgia So Univ, Statesboro, GA 30460 USA. NR 39 TC 10 Z9 10 U1 1 U2 9 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-2004 J9 TRIBOL T JI Tribol. Trans. PY 2011 VL 54 IS 4 BP 523 EP 541 DI 10.1080/10402004.2011.568673 PG 19 WC Engineering, Mechanical SC Engineering GA 890VC UT WOS:000300172700004 ER PT J AU Radil, K Batcho, Z AF Radil, Kevin Batcho, Zach TI Air Injection as a Thermal Management Technique for Radial Foil Air Bearings SO TRIBOLOGY TRANSACTIONS LA English DT Article DE Foil Air Bearings; Gas Bearings; Turbomachinery ID JOURNAL BEARINGS AB A thermal management technique for radial foil air bearings was experimentally evaluated. The technique is based on injecting air directly into the internal circulating fluid-film to reduce bulk temperatures and axial thermal gradients. The tests were performed on a single top foil, Generation III, radial foil bearing instrumented with three thermocouples to monitor internal temperatures. A through hole in the bearing shell coincident with the gap between the top foil's fixed and free ends provided entry for the injection air. The tests were conducted at room temperature with the bearing operating at speeds from 20 to 40 krpm while supporting 222 N. Two different mass flow rates of injection air were evaluated for this method, 0.017 and 0.051 kg/min. Test results suggest that the air injection approach is a viable thermal management technique capable of controlling bulk temperatures and axial thermal gradients in radial foil air bearings. C1 [Radil, Kevin] NASA, RDRL VTP, Glenn Res Ctr, Cleveland, OH USA. [Batcho, Zach] US Mil Acad, West Point, NY 10996 USA. RP Radil, K (reprint author), NASA, RDRL VTP, Glenn Res Ctr, Cleveland, OH USA. NR 20 TC 6 Z9 6 U1 0 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-2004 J9 TRIBOL T JI Tribol. Trans. PY 2011 VL 54 IS 4 BP 666 EP 673 DI 10.1080/10402004.2011.589964 PG 8 WC Engineering, Mechanical SC Engineering GA 890VC UT WOS:000300172700014 ER PT J AU Dellacorte, C AF Dellacorte, Christopher TI Stiffness and Damping Coefficient Estimation of Compliant Surface Gas Bearings for Oil-Free Turbomachinery SO TRIBOLOGY TRANSACTIONS LA English DT Article DE Mechanical Engineering; Bearings; Stiffness Damping; Rotordynamics ID FOIL JOURNAL BEARINGS; BUMP FOILS AB Gas foil bearings are a key technology in many commercial and emerging oil-free turbomachinery systems. These bearings are nonlinear and have been difficult to analytically model in terms of performance characteristics such as load capacity, power loss, stiffness, and damping. Previous investigations led to an empirically derived method, a rule-of-thumb, to estimate load capacity. This method has been a valuable tool in system development. The current article extends this concept to include rules for stiffness and damping coefficient estimation. It is expected that these rules will further accelerate the development and deployment of advanced oil-free machines operating on gas foil bearings. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Dellacorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 37 TC 11 Z9 11 U1 0 U2 5 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-2004 J9 TRIBOL T JI Tribol. Trans. PY 2011 VL 54 IS 4 BP 674 EP 684 DI 10.1080/10402004.2011.589966 PG 11 WC Engineering, Mechanical SC Engineering GA 890VC UT WOS:000300172700015 ER PT J AU Street, KW Morales, W Koch, VR Valco, DJ Richard, RM Hanks, N AF Street, Kenneth W., Jr. Morales, Wilfredo Koch, Victor R. Valco, Daniel J. Richard, Ryan M. Hanks, Nicole TI Evaluation of Vapor Pressure and Ultra-High Vacuum Tribological Properties of Ionic Liquids SO TRIBOLOGY TRANSACTIONS LA English DT Article DE Ionic Liquids; Space Tribology; Vapor Pressure; Spiral Orbit Tribometry ID SPIRAL ORBIT TRIBOMETRY; LUBRICANTS AB Ionic liquids are a class of salts that incorporate polyatomic anions and cations. These materials are typically viscous fluids at room temperature. The fluids are generally characterized as possessing negligible vapor pressures under ambient conditions. These beneficial properties have led us to study the effectiveness of ionic liquids containing both organic cations and anions for use as lubricants with space applications. This article presents vapor pressure measurements for four ionic liquids as well as friction coefficient data from a spiral orbit tribometer in the boundary lubrication regime under simulated space conditions using stainless steel tribocouples. In addition, we present the first tribological data on mixed ionic liquids and an ionic liquid additive. Postmortem infrared and Raman analyses of the balls and races indicates that the major degradation pathway for these organic ionic liquids is similar to those of other carbon-based liquid lubricants; that is, deterioration of the organic structure into amorphous graphitic carbon. The coefficients of friction and lifetimes of these lubricants are comparable to or better than those of several commonly used space oils. C1 [Street, Kenneth W., Jr.; Morales, Wilfredo] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Koch, Victor R.] Covalent Associates Inc, Corvallis, OR 97330 USA. [Valco, Daniel J.] Ohio State Univ, Dept Chem & Biomol Engn, Columbus, OH 43210 USA. [Richard, Ryan M.] Cleveland State Univ, Dept Chem, Cleveland, OH 44115 USA. [Hanks, Nicole] Mercyhurst Coll, Dept Chem, Erie, PA 16546 USA. RP Street, KW (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 18 TC 22 Z9 22 U1 7 U2 38 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-2004 J9 TRIBOL T JI Tribol. Trans. PY 2011 VL 54 IS 6 BP 911 EP 919 DI 10.1080/10402004.2011.606963 PG 9 WC Engineering, Mechanical SC Engineering GA 890VL UT WOS:000300173800011 ER PT J AU de la Pena, F Berger, MH Hochepied, JF Dynys, F Stephan, O Walls, M AF de la Pena, F. Berger, M. -H. Hochepied, J. -F. Dynys, F. Stephan, O. Walls, M. TI Mapping titanium and tin oxide phases using EELS: An application of independent component analysis SO ULTRAMICROSCOPY LA English DT Article DE Electron energy-loss spectroscopy (EELS); Independent component analysis; Blind separation of sources; Multivariate statistical analysis; Quantification; TiO(2); SnO(2); Spinodal decomposition ID MULTIVARIATE-ANALYSIS; SPECTRUM IMAGES; TIO2-SNO2 AB We study materials that present challenges for conventional elemental mapping techniques and can in some cases be treated successfully using independent component analysis (ICA). In this case the material in question is obtained from a TiO(2)-SiO(2) solid solution that is spinodally decomposed into TiO(2) rich-SnO(2) rich multilayers. Conventional elemental mapping is difficult because the edges most easily mapped for these elements (Ti-L, Sn-M and O-K) all have onsets within the same 80 eV range. ICA is used to separate entire spectral signals corresponding to particular material phases or molecular units rather than particular elements and is thus able to distinguish between TiO(2) and SnO(2). We show that quantification of oxide species can be performed by different methods that require extra assumptions, but nevertheless should be feasible in many cases. (C) 2010 Elsevier B.V. All rights reserved. C1 [de la Pena, F.; Stephan, O.; Walls, M.] Univ Paris 11, Phys Solides Lab, F-91405 Orsay, France. [Berger, M. -H.] MINES ParisTech, Ctr Mat, CNRS, UMR 7633, F-91003 Evry, France. [Hochepied, J. -F.] MINES ParisTech, CEP SCPI, F-75272 Paris 06, France. [Dynys, F.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Walls, M (reprint author), Univ Paris 11, Phys Solides Lab, Bat 510, F-91405 Orsay, France. EM walls@lps.u-psud.fr RI Berger, Marie-Helene/B-9785-2013; de la Pena, Francisco/B-3955-2017 OI de la Pena, Francisco/0000-0002-1121-6099 FU European Commission; French TEM and Atom-probe network (METSA); European Community [MEST-CT-2004-514307]; European Office for Air Force Research and Development (EOARD) [073031]; Carnot M.I.N.E.S. Institute FX This work was supported by the ESTEEM IP3 project within the 6th Framework Programme of the European Commission, the French TEM and Atom-probe network (METSA) F. de la Pena acknowledges support by the European Community Marie Curie Action (no.MEST-CT-2004-514307) and M.H. Berger and the support by European Office for Air Force Research and Development (EOARD Grant no. 073031) and the Carnot M.I.N.E.S. Institute. NR 29 TC 37 Z9 37 U1 12 U2 77 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3991 J9 ULTRAMICROSCOPY JI Ultramicroscopy PD JAN PY 2011 VL 111 IS 2 BP 169 EP 176 DI 10.1016/j.ultramic.2010.10.001 PG 8 WC Microscopy SC Microscopy GA 710YF UT WOS:000286552200012 PM 21185462 ER PT S AU Jenkins, JM Dunnuck, J AF Jenkins, Jon M. Dunnuck, Jeb BE MacEwen, HA Breckinridge, JB TI The Little Photometer That Could: Technical Challenges and Science Results from the Kepler Mission SO UV/OPTICAL/IR SPACE TELESCOPES AND INSTRUMENTS: INNOVATIVE TECHNOLOGIES AND CONCEPTS V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on UV/Optical/IR Space Telescopes and Instruments - Innovative Technologies and Concepts V CY AUG 21-24, 2011 CL San Diego, CA SP SPIE DE Kepler Mission; exoplanet; transit; photometry; data compression; systematic error correction ID PLANETS; CANDIDATES; HAT-P-7B; SYSTEM; STARS AB The Kepler spacecraft launched on March 7, 2009, initiating NASA's first search for Earth-size planets orbiting Sun-like stars. Since launch, Kepler has announced the discovery of 17 exoplanets, including a system of six transiting a Sun-like star, Kepler-11, and the first confirmed rocky planet, Kepler-10b, with a radius of 1.4 that of Earth. Kepler is proving to be a cornucopia of discoveries: it has identified over 1200 candidate planets based on the first 120 days of observations, including 54 that are in or near the habitable zone of their stars, and 68 that are 1.2 Earth radii or smaller. An astounding 408 of these planetary candidates are found in 170 multiple systems, demonstrating the compactness and flatness of planetary systems composed of small planets. Never before has there been a photometer capable of reaching a precision near 20 ppm in 6.5 hours and capable of conducting nearly continuous and uninterrupted observations for months to years. In addition to exoplanets, Kepler is providing a wealth of astrophysics, and is revolutionizing the field of asteroseismology. Designing and building the Kepler photometer and the software systems that process and analyze the resulting data to make the discoveries presented a daunting set of challenges, including how to manage the large data volume. The challenges continue into flight operations, as the photometer is sensitive to its thermal environment, complicating the task of detecting 84 ppm drops in brightness corresponding to Earth-size planets transiting Sun-like stars. C1 [Jenkins, Jon M.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94305 USA. RP Jenkins, JM (reprint author), NASA, SETI Inst, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94305 USA. EM Jon.Jenkins@nasa.gov NR 45 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8756-8 J9 PROC SPIE PY 2011 VL 8146 AR 814602 DI 10.1117/12.897767 PG 12 WC Astronomy & Astrophysics; Optics; Imaging Science & Photographic Technology SC Astronomy & Astrophysics; Optics; Imaging Science & Photographic Technology GA BBA82 UT WOS:000306323000002 ER PT J AU Stansbery, G AF Stansbery, Gene BE Letcher, TM Vallero, DA TI Space Waste SO WASTE: A HANDBOOK FOR MANAGEMENT LA English DT Article; Book Chapter ID DEBRIS C1 NASA, Orbital Debris Program Off, Johnson Space Ctr, KX2, Washington, DC 20546 USA. RP Stansbery, G (reprint author), NASA, Orbital Debris Program Off, Johnson Space Ctr, KX2, Washington, DC 20546 USA. NR 22 TC 1 Z9 1 U1 0 U2 1 PU ELSEVIER ACADEMIC PRESS INC PI SAN DIEGO PA 525 B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 USA BN 978-0-12-381476-0 PY 2011 BP 377 EP 391 DI 10.1016/B978-0-12-381475-3.10026-9 PG 15 WC Engineering, Environmental SC Engineering GA BET35 UT WOS:000318016300028 ER PT J AU Moreno, MJ AF Moreno, Max J. TI Analysis of the Relationship Between Submerged Aquatic Vegetation (SAV) and Water Trophic Status of Lakes Clustered in Northwestern Hillsborough County, Florida SO WATER AIR AND SOIL POLLUTION LA English DT Article DE Total phosphorus; Total nitrogen; Chlorophyll-alpha; Phytoplankton; Relationship; Water quality; PVI; PAC; Macrophytes ID CHLOROPHYLL-A CONCENTRATIONS; PHOSPHORUS REMOVAL; MACROPHYTES; PREDICTION; BIOMASS; RUNOFF AB This study examined the relationship between abundance of submerged aquatic vegetation (SAV) and the water trophic status of a group of lakes located in northwestern Hillsborough county. SAV abundance was expressed by the percent of lake volume infested with SAV (PVI) and the percent of lake area covered with SAV (PAC). The group of lakes was divided into two subgroups based on SAV abundance less than 20 PVI (PVI < 20) and lakes with more than 20 PVI (PVI > 20). Mean concentrations of total phosphorus (TP), total nitrogen (TN), and chlorophyll-alpha in lake water were used as indicators of trophic status, with the concentration of each nutrient in one group of lakes compared to its corresponding concentration in the other group. Lakes with PVI < 20 had a mean concentration of TP and chlorophyll-alpha of 28 and 11 A mu g/l, respectively, while those with a PVI > 20 had a mean concentration of 18 and 4 A mu g/l for the same parameters, respectively. The results of a t test and one-way ANOVA performed at the 95% confidence level indicated that the differences were significant for the concentrations of TP and chlorophyll-alpha but not for TN, the last of which had a mean lake water concentration of 0.8 and 0.7 mg/l for the PVI < 20 and PVI > 20 subgroups, respectively. C1 [Moreno, Max J.] Univ S Florida, Coll Publ Hlth, Dept Environm & Occupat Hlth, Tampa, FL 33612 USA. RP Moreno, MJ (reprint author), Oak Ridge Associated Univ, NASA Postdoctoral Program, Natl Space Sci & Technol Ctr, NASA, 320 Sparkman Dr, Huntsville, AL 35806 USA. EM mmoreno@health.usf.edu FU Department of Environmental and Occupational Health at the College of Public Health at the University of South Florida FX The author would like to express his appreciation for the financial support provided by the Department of Environmental and Occupational Health at the College of Public Health at the University of South Florida. He also thanks Dr. Jim Griffin and Mr. David Eilers for their assistance in data management, the Water Atlas for making the data available, the Hillsborough County Environmental Protection Commission laboratory for the information on water analysis, Dr. Alfred Mbah for his help with statistics, and Ms. Greta Klungness and Mr. Haofei Yu for their assistance with geographical information systems. Last but not the least, the author wants to express his great appreciation for the support, teaching, and guidance received from his major advisor Dr. Noreen Poor. NR 27 TC 8 Z9 8 U1 4 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0049-6979 J9 WATER AIR SOIL POLL JI Water Air Soil Pollut. PD JAN PY 2011 VL 214 IS 1-4 BP 539 EP 546 DI 10.1007/s11270-010-0444-7 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences; Water Resources SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences; Water Resources GA 696VF UT WOS:000285468800043 ER PT B AU Debes, JH AF Debes, John H. BE Hoard, DW TI The Origin and Evolution of White Dwarf Dust Disks SO WHITE DWARF ATMOSPHERES AND CIRCUMSTELLAR ENVIRONMENTS LA English DT Article; Book Chapter ID GASEOUS DEBRIS DISC; INTERSTELLAR-MEDIUM; STELLAR EVOLUTION; METAL-RICH; CIRCUMSTELLAR DISKS; PLANETARY SYSTEMS; ASTEROID BELT; SOLAR-SYSTEM; WARM DUST; ACCRETION C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Debes, JH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 75 TC 3 Z9 3 U1 0 U2 0 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PAPPELALLEE 3, W-69469 WEINHEIM, GERMANY BN 978-3-527-63659-4; 978-3-527-41031-6 PY 2011 BP 173 EP 201 D2 10.1002/9783527636570 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BA6WO UT WOS:000337295500007 ER PT B AU Soto Toro, FA Vu, BT Hamilton, MS AF Soto Toro, Felix A. Vu, Bruce T. Hamilton, Mark S. BE Baralt, J Callaos, N Ham, C Lace, N Lesso, W Zinn, CD TI Qualification of Electrical Ground Support Equipment for New Space Programs SO WMSCI 2011: 15TH WORLD MULTI-CONFERENCE ON SYSTEMICS, CYBERNETICS AND INFORMATICS, VOL I LA English DT Proceedings Paper CT 15th World Multi-Conference on Systematics, Cybernetics and Informatics (WMSCI 2011) CY JUL 19-22, 2011 CL Orlando, FL SP Int Inst Informat & Syst DE Qualification; Testing; Ground Support Equipment; Electromagnetic Interference Testing; Vibration Testing; Acoustic Testing; Power Spectral Density AB With the Space Shuttle program coming to an end, the National Aeronautics and Space Administration (NASA) is moving to a new space flight program that will allow expeditions beyond low earth orbit. The space vehicles required to comply with these missions will be carrying heavy payloads. This implies that the Earth departure stage capabilities most be of higher magnitudes, given the current propulsion technology. The engineering design of the new flight hardware comes with some structural, thermal, propulsion and other subsystems' challenges. Meanwhile, the necessary ground support equipment (GSE) used to test, validate, verify and process the flight hardware must withstand the new program specifications. This paper intends to provide the qualification considerations during implementation of new electrical GSE for space programs. A team of engineers was formed to embark on this task, and facilitate the logistics process and ensure that the electrical, mechanical and fluids subsystems conduct the proper level of testing. Ultimately, each subsystem must certify that each piece of ground support equipment used in the field is capable of withstanding the strenuous vibration, acoustics, environmental, thermal and Electromagnetic Interference (EMI) levels experienced during pre-launch, launch and post-launch activities. The benefits of capturing and sharing these findings will provide technical, cost savings and schedule impacts information to both the technical and management community. C1 [Soto Toro, Felix A.] NASA, Elect Engn Div, Kennedy Space Ctr, FL 32899 USA. [Vu, Bruce T.] NASA, Mech Engn Div, Kennedy Space Ctr, FL 32899 USA. [Hamilton, Mark S.] NASA, Div Mat Sci, Kennedy Space Ctr, FL 32899 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU INT INST INFORMATICS & SYSTEMICS PI ORLANDO PA 14269 LORD BARCLAY DR, ORLANDO, FL 32837 USA BN 978-1-936338-29-0 PY 2011 BP 49 EP 52 PG 4 WC Computer Science, Cybernetics; Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BG8OX UT WOS:000392561800010 ER PT B AU Vazquez Ramos, G Yuan, JS AF Vazquez Ramos, Gabriel Yuan, Jiann-Shiun BE Baralt, J Callaos, N Ham, C Lace, N Lesso, W Zinn, CD TI Development of a Novel Wireless Electric Power Transfer System for Space Applications SO WMSCI 2011: 15TH WORLD MULTI-CONFERENCE ON SYSTEMICS, CYBERNETICS AND INFORMATICS, VOL I LA English DT Proceedings Paper CT 15th World Multi-Conference on Systematics, Cybernetics and Informatics (WMSCI 2011) CY JUL 19-22, 2011 CL Orlando, FL SP Int Inst Informat & Syst DE Magnetic Resonance; Wireless Power Transfer; Magnetic Coupling; Space Systems; Power Amplifier AB This paper will introduce a new implementation for wireless electric power transfer systems: space applications. Due to the risks that constitute the use of electrical connector for some space missions/applications, a simple wireless power system design approach will be evaluated as an alternative for the use of electrical connectors. This approach takes into consideration the overall system performance by designing the magnetic resonance elements and by verifying the overall system electrical behavior. System characterization is accomplished by executing circuit and analytical simulations using Matlab and LTSpicelV (R) software packages. The design methodology was validated by two different experiments: frequency consideration (design of three magnetic elements) and a small scale proof-of concept prototype. Experiment results shows successful wireless power transfer for all the cases studied. The proof-of concept prototype provided similar to 4 W of wireless power to the load (light bulb) at a separation of 3 cm from the source. In addition, a resonant circuit was designed and installed to the battery terminals of a handheld radio without batteries, making it turn on at a separation of similar to 5 cm or less from the source. It was also demonstrated by prototype experimentation that multiple loads can be powered wirelessly at the same time with a single electric power source. C1 [Vazquez Ramos, Gabriel] NASA, Launch Serv Program, Mail Code VA H3, Kennedy Space Ctr, FL 32899 USA. [Yuan, Jiann-Shiun] Univ Cent Florida, Dept Elect Engn & Comp Sci, Orlando, FL 32816 USA. EM Gabriel.VazquezRamos-1@nasa.gov; yuanj@mail.ucf.edu NR 15 TC 0 Z9 0 U1 0 U2 0 PU INT INST INFORMATICS & SYSTEMICS PI ORLANDO PA 14269 LORD BARCLAY DR, ORLANDO, FL 32837 USA BN 978-1-936338-29-0 PY 2011 BP 53 EP 58 PG 6 WC Computer Science, Cybernetics; Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BG8OX UT WOS:000392561800011 ER PT J AU Wargan, K Pawson, S Stajner, I Thouret, V AF Wargan, Krzysztof Pawson, Steven Stajner, Ivanka Thouret, Valerie TI Spatial structure of assimilated ozone in the upper troposphere and lower stratosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; MOZAIC AIRBORNE PROGRAM; EOS MLS; MONITORING INSTRUMENT; AURA SATELLITE; SYSTEM; AIRCRAFT; VARIABILITY AB Ozone distributions display a rich spatial structure in the upper troposphere and lower stratosphere (UTLS). This study uses in situ aircraft observations to examine how accurately such spatial distributions of ozone are represented in an assimilation of NASA's EOS-Aura ozone data using meteorological fields from the Goddard Earth Observing System, Version 4. Total ozone columns from the Ozone Monitoring Instrument (OMI) and stratospheric profiles from the Microwave Limb Sounder (MLS) are assimilated. The results demonstrate that the dominant large-scale ozone distribution is well-constrained (to realistic concentrations) near 250 hPa in the UTLS. Spatial patterns and the spectral power of variations are similar in the model simulations and the assimilation. The spectral power of the analysis increments is concentrated at large scales. Thus transport, rather than direct assimilation of small-scale features, is responsible for the spatial ozone structure in the UTLS. Consistent with the documented behavior of the Lin-Rood transport scheme, we demonstrate that the assimilated ozone represents realistic features on spatial scales of about four-to-six model grid boxes (500-800 km) and that smaller scales present in the aircraft observations are represented too weakly in the modeled and assimilated ozone fields. For the assimilated ozone, this result is robust over a range of realistic model-error-covariance length scales. The results indicate that observations of ozone on spatial scales that constrain the large-scale gradients are suited to producing global analyses of UTLS ozone that represent features at higher spatial resolution. C1 [Wargan, Krzysztof; Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20770 USA. [Wargan, Krzysztof] Sci Applicat Int Corp, Beltsville, MD USA. [Stajner, Ivanka] Noblis Inc, Falls Church, VA 22042 USA. [Thouret, Valerie] Univ Toulouse, UPS, Lab Aerol, F-31400 Toulouse, France. [Thouret, Valerie] CNRS, Lab Aerol, Toulouse, France. RP Wargan, K (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Phys, S Kensington Campus, London SW7 2AZ, England. EM steven.pawson@nasa.gov RI Stajner, Ivanka/B-5228-2009; Pawson, Steven/I-1865-2014; OI Stajner, Ivanka/0000-0001-6103-3939; Pawson, Steven/0000-0003-0200-717X; Wargan, Krzysztof/0000-0002-3795-2983 FU NASA; INSU-CNRS (France); Meteo-France; Forschungszentrum Julich (FZJ) Germany FX We appreciate the support from and discussions with our colleagues Eric Nielsen and Andrew Tangborn. We are grateful to Nathaniel Livesey and Lucien Froidevaux of the MLS Scence Team at NASA's JPL and to Pieternel Levelt at KNMI for discussions about the MLS and the Dutch-Finnish OMI data. Comments by three anonymous reviewers and the Associate Editor substantially improved the presentation of our results. The research was funded by NASA's Atmospheric Chemistry Modeling and Analysis Program (ACMAP). Computing resources were provided by NASA's High-Performance Computing pro-gram. We acknowledge the strong support of the European Commission, Airbus, and the airlines (Lufthansa, Austrian, Air France), who have carried and maintained the MOZAIC equipment, free of charge, since 1994. MOZAIC is presently funded by INSU-CNRS (France), Meteo-France, and Forschungszentrum Julich (FZJ) Germany. The MOZAIC database is supported by ETHER (CNES and INSU-CNRS). NR 39 TC 9 Z9 10 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 31 PY 2010 VL 115 AR D24316 DI 10.1029/2010JD013941 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 701QP UT WOS:000285837600002 ER PT J AU Tian, YD Peters-Lidard, CD AF Tian, Yudong Peters-Lidard, Christa D. TI A global map of uncertainties in satellite-based precipitation measurements SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TEMPORAL RESOLUTION; PASSIVE MICROWAVE; RAINFALL; PRODUCTS; VALIDATION; PROJECT; CMORPH AB A global map of measurement uncertainties in satellite-based precipitation estimates has been produced by computing the variance from an ensemble of six different TRMM-era data sets at daily, 0.25 degrees resolution. This analysis yields a lower-bound estimate of the uncertainties, and a consistent global view of the error characteristics and their regional and seasonal variations, and reveals many undocumented error features over areas with no validation data available. The uncertainties are relatively small (40-60%) over the oceans, especially in the tropics, and over southern South America. There are large uncertainties (100-140%) over high latitudes (poleward of 40 degrees latitude), especially during the cold season. High relative uncertainties are also evident through the seasons over complex terrain areas, including the Tibetan Plateau, the Rockies and the Andes. Coastlines and water bodies also indicate high measurement uncertainty. The estimated global uncertainties also exhibit systematic seasonal, regional as well as rain-rate dependencies, with lowest uncertainties over tropical oceanic regions with strong, convective precipitation, and highest ones over wintery, complex land surfaces with light precipitation. Citation: Tian, Y., and C. D. Peters-Lidard (2010), A global map of uncertainties in satellite-based precipitation measurements, Geophys. Res. Lett., 37, L24407, doi:10.1029/2010GL046008. C1 [Tian, Yudong; Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Tian, YD (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Mail Code 614-3, Greenbelt, MD 20771 USA. EM yudong.tian@nasa.gov RI Measurement, Global/C-4698-2015; Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 FU Air Force Weather Agency (AFWA) [MIPR F3HRA19027G001] FX This research is partially supported by the Air Force Weather Agency (AFWA) MIPR F3HRA19027G001 (PI: C. Peters-Lidard). The authors wish to thank John Eylander at AFWA for program support, and George Huffman, Robert Adler, Robert Joyce, John Janowiak, Takuji Kubota, Tomoo Ushio, F. Joseph Turk, and Kuo-lin Hsu for their efforts in producing and providing the respective data sets. Helpful comments from George Huffman and an anonymous reviewer are greatly appreciated. NR 18 TC 89 Z9 90 U1 3 U2 34 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 31 PY 2010 VL 37 AR L24407 DI 10.1029/2010GL046008 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 701RQ UT WOS:000285840700004 ER PT J AU Omar, A Liu, ZY Vaughan, M Thornhill, K Kittaka, C Ismail, S Hu, YX Chen, G Powell, K Winker, D Trepte, C Winstead, E Anderson, B AF Omar, Ali Liu, Zhaoyan Vaughan, Mark Thornhill, Kenneth Kittaka, Chieko Ismail, Syed Hu, Yongxiang Chen, Gao Powell, Kathleen Winker, David Trepte, Charles Winstead, Edward Anderson, Bruce TI Extinction-to-backscatter ratios of Saharan dust layers derived from in situ measurements and CALIPSO overflights during NAMMA SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID AXIALLY-SYMMETRICAL PARTICLES; SIZE SHAPE DISTRIBUTIONS; LIGHT-SCATTERING; MINERAL DUST; ATLANTIC-OCEAN; OPTICAL-PROPERTIES; SAMUM 2006; NONSPHERICAL PARTICLES; RADIATIVE PROPERTIES; MATRIX COMPUTATIONS AB We determine the extinction-to-backscatter (S-a) ratios of dust using (1) airborne in situ measurements of microphysical properties, (2) modeling studies, and (3) the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) observations recorded during the NASA African Monsoon Multidisciplinary Analyses (NAMMA) field experiment conducted from Sal, Cape Verde during August to September 2006. Using CALIPSO measurements of the attenuated backscatter of lofted Saharan dust layers, we apply the transmittance technique to estimate dust S-a ratios at 532 nm and a two-color method to determine the corresponding 1064 nm S-a. This method yielded dust S-a ratios of 39.8 +/- 1.4 and 51.8 +/- 3.6 sr at 532 and 1064 nm, respectively. Second, S-a at both wavelengths is independently calculated using size distributions measured aboard the NASA DC-8 and estimates of Saharan dust complex refractive indices applied in a T-Matrix scheme. We found S-a ratios of 39.1 +/- 3.5 and 50.0 +/- 4 sr at 532 and 1064 nm, respectively, using the T-Matrix calculations applied to measured size spectra. Finally, in situ measurements of the total scattering (550 nm) and absorption coefficients (532 nm) are used to generate an extinction profile that is used to constrain the CALIPSO 532 nm extinction profile and thus generate a stratified 532 nm S-a. This method yielded an S-a ratio at 532 nm of 35.7 sr in the dust layer and 25 sr in the marine boundary layer consistent with a predominantly sea-salt aerosol near the ocean surface. Combinatorial simulations using noisy size spectra and refractive indices were used to estimate the mean and uncertainty (one standard deviation) of these S-a ratios. These simulations produced a mean (+/- uncertainty) of 39.4 (+/- 5.9) and 56.5 (+/- 16.5) sr at 532 and 1064 nm, respectively, corresponding to percentage uncertainties of 15% and 29%. These results will provide a measurements-based estimate of the dust S-a for use in backscatter lidar inversion algorithms such as CALIOP (Cloud-Aerosol Lidar With Orthogonal Polarization). C1 [Omar, Ali; Liu, Zhaoyan] NASA, Langley Res Ctr, Sci Directorate, Natl Inst Aerosp, Hampton, VA 23681 USA. [Thornhill, Kenneth; Winstead, Edward] NASA, Langley Res Ctr, Sci Applicat Int Corp, Hampton, VA 23681 USA. RP Omar, A (reprint author), NASA, Langley Res Ctr, Sci Directorate, Natl Inst Aerosp, MS 475, Hampton, VA 23681 USA. EM ali.h.omar@nasa.gov RI Liu, Zhaoyan/B-1783-2010; Hu, Yongxiang/K-4426-2012; Omar, Ali/D-7102-2017 OI Liu, Zhaoyan/0000-0003-4996-5738; Omar, Ali/0000-0003-1871-9235 FU NASA FX We thank the relevant DC-8 instrument PIs for the NAMMA data, the MODIS and MOPPITT teams for their data, and the CALIPSO team for data, guidance, and many useful discussions. We acknowledge the use of the public-domain T-matrix code by Michael Mishchenko and thank Kam Pui Lee, Susan Kooi, and Sharon Burton for the CALIPSO and LASE images. We gratefully acknowledge funding support from the NASA Radiation Sciences and Atmospheric Composition Programs, respectively, managed by Hal Maring and Bruce Doddridge. NR 72 TC 21 Z9 21 U1 2 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 31 PY 2010 VL 115 AR D24217 DI 10.1029/2010JD014223 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 701QP UT WOS:000285837600004 ER PT J AU Jian, LK Russell, CT Luhmann, JG Anderson, BJ Boardsen, SA Strangeway, RJ Cowee, MM Wennmacher, A AF Jian, L. K. Russell, C. T. Luhmann, J. G. Anderson, B. J. Boardsen, S. A. Strangeway, R. J. Cowee, M. M. Wennmacher, A. TI Observations of ion cyclotron waves in the solar wind near 0.3 AU SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID PICK-UP; INTERSTELLAR HYDROGEN; HELIUM AB Using 2 Hz magnetic field data from the MESSENGER mission, we have investigated more than 300 strong narrowband ion cyclotron wave (ICW) events at a heliocentric distance of about 0.3 AU during 31 May to 9 June 2008. These nearly circularly polarized transverse waves are observed extensively and discretely in the solar wind, with a median duration of 21 s. They are preferentially observed when the magnetic field is more radial than the ambient solar wind. The waves appear both left-handed and right-handed in the spacecraft frame. Their wave frequencies in the spacecraft frame are generally larger than the local proton cyclotron frequency (f(pc)), with a median of 1.44 f(pc). The wave power spectra do not cutoff at the local f(pc). On the basis of their wave characteristics, we conclude that they are intrinsically left-handed in the solar wind frame and they are generated closer to the Sun and carried out to the spacecraft by the super Alfvenic solar wind. After removing the Doppler shift, the wave frequencies in the solar wind frame are all below the local f(pc), with a median of 0.35 f(pc). The ICWs propagate nearly parallel to the magnetic field, and the median wave amplitude is about 0.73 nT, 3% of the background magnetic field. We compare these observations with earlier Helios observations at 0.3 AU in 1976 and contemporary 1 AU observations. C1 [Jian, L. K.; Russell, C. T.; Strangeway, R. J.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Anderson, B. J.] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 20723 USA. [Boardsen, S. A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Boardsen, S. A.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Cowee, M. M.] Los Alamos Natl Lab, Space Sci & Applicat ISR 1, Los Alamos, NM 87545 USA. [Wennmacher, A.] Univ Cologne, Inst Geophys & Meteorol, D-50923 Cologne, Germany. RP Jian, LK (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. EM jlan@igpp.ucla.edu RI Anderson, Brian/I-8615-2012; Russell, Christopher/E-7745-2012; Jian, Lan/B-4053-2010 OI Russell, Christopher/0000-0003-1639-8298; Jian, Lan/0000-0002-6849-5527 FU NASA [NAS5-03131] FX This work is supported by NASA's STEREO program through grant NAS5-03131 administered by University of California-Berkeley. We thank all the PIs for making the data available. We appreciate Fritz Neubauer, Peter Gary, and Philip Isenberg for their useful discussions. NR 30 TC 25 Z9 25 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 31 PY 2010 VL 115 AR A12115 DI 10.1029/2010JA015737 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 701RJ UT WOS:000285839900003 ER PT J AU Bell, JM Bougher, SW Waite, JH Ridley, AJ Magee, BA Mandt, KE Westlake, J DeJong, AD De La Haye, V Bar-Nun, A Jacovi, R Toth, G Gell, D Fletcher, G AF Bell, Jared M. Bougher, Stephen W. Waite, J. Hunter, Jr. Ridley, Aaron J. Magee, Brian A. Mandt, Kathleen E. Westlake, Joseph DeJong, Anna D. De La Haye, Virginie Bar-Nun, Akiva Jacovi, Ronen Toth, Gabor Gell, David Fletcher, Gregory TI Simulating the one-dimensional structure of Titan's upper atmosphere: 2. Alternative scenarios for methane escape SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID COUPLING PHOTOCHEMISTRY; HETEROGENEOUS REACTION; HYDROGEN BUDGET; HAZE FORMATION; ORGANIC HAZE; AEROSOLS; MODEL; CHEMISTRY; TEMPERATURES; SPECTROMETER AB In Bell et al. (2010) (paper 1), we provide a series of benchmark simulations that validate a newly developed Titan Global Ionosphere-Thermosphere Model (T-GITM) and calibrate its estimates of topside escape rates with recent work by Cui et al. (2008), Strobel (2009), and Yelle et al. (2008). Presently, large uncertainties exist in our knowledge of the density and thermal structure of Titan's upper atmosphere between the altitudes of 500 km and 1000 km. In this manuscript, we explore a spectrum of possible model configurations of Titan's upper atmosphere that are consistent with observations made by the Cassini Ion-Neutral Mass Spectrometer (INMS), Composite Infrared Spectrometer, Cassini Plasma Spectrometer, Magnetospheric Imaging Instrument, and by the Huygens Gas Chromatograph Mass Spectrometer and Atmospheric Science Instrument. In particular, we explore the ramifications of multiplying the INMS densities of Magee et al. (2009) by a factor of 3.0, which significantly alters the overall density, thermal, and dynamical structures simulated by T-GITM between 500 km and 1500 km. Our results indicate that an entire range of topside CH4 escape fluxes can equivalently reproduce the INMS measurements, ranging from similar to 10(8) - 1.86 x 10(13) molecules m(-2) s(-1) (referred to the surface). The lowest topside methane escape rates are achieved by scaling the INMS densities by a factor of 3.0 and either (1) increasing the methane homopause altitude to similar to 1000 km or (2) including a physicochemical loss referred to as aerosol trapping. Additionally, when scaling the INMS densities by a factor of 3.0, we find that only Jeans escape velocities are required to reproduce the H-2 measurements of INMS. C1 [Bell, Jared M.; Waite, J. Hunter, Jr.; Magee, Brian A.; DeJong, Anna D.; De La Haye, Virginie; Gell, David; Fletcher, Gregory] SW Res Inst, Div Space Sci & Engn, San Antonio, TX 78228 USA. [Bar-Nun, Akiva] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. [Bougher, Stephen W.; Ridley, Aaron J.; Toth, Gabor] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Jacovi, Ronen] CALTECH, Jet Prop Lab, Ice Spect Lab, Pasadena, CA 91109 USA. [Mandt, Kathleen E.; Westlake, Joseph] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. RP Bell, JM (reprint author), SW Res Inst, Div Space Sci & Engn, 6220 Culebra Rd,POB 28510, San Antonio, TX 78228 USA. RI Bougher, Stephen/C-1913-2013; Toth, Gabor/B-7977-2013; Mandt, Kathleen/M-9812-2013; Westlake, Joseph/G-2732-2015; Ridley, Aaron/F-3943-2011 OI Bougher, Stephen/0000-0002-4178-2729; Toth, Gabor/0000-0002-5654-9823; Mandt, Kathleen/0000-0001-8397-3315; Westlake, Joseph/0000-0003-0472-8640; Ridley, Aaron/0000-0001-6933-8534 FU NASA through the Jet Propulsion Laboratory [NAS703001NM0710023] FX x The authors would like to acknowledge funding from NASA grant NAS703001NM0710023, subcontracted through the Jet Propulsion Laboratory (JPL). NR 54 TC 20 Z9 20 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 30 PY 2010 VL 115 AR E12018 DI 10.1029/2010JE003638 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 701QF UT WOS:000285836400001 ER PT J AU Haider, SA Sheel, V Smith, MD Maguire, WC Molina-Cuberos, GJ AF Haider, S. A. Sheel, V. Smith, M. D. Maguire, W. C. Molina-Cuberos, G. J. TI Effect of dust storms on the D region of the Martian ionosphere: Atmospheric electricity SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID RADIO OCCULTATION MEASUREMENTS; METEORIC IONS; MARS; MODEL; RECOMBINATION; CHEMISTRY AB We have used dust opacity values observed by the Thermal Emission Imaging System onboard Mars Odyssey to estimate the effect of dust aerosols in the D region of the Martian ionosphere. An ion-dust aerosol model has been developed to calculate ion concentrations and conductivity at midlatitudes during a dust storm in the Southern Hemisphere. We report that the concentration of the water cluster ions H+(H2O)(n), NO2-(H2O)(n), and CO3-(H2O)(n) are reduced by 2 orders of magnitude in the presence of dust aerosols. This indicates that during a dust storm, when the optical depth changes considerably, a large hole in the ion concentrations may appear until this anomalous condition returns to the normal condition after a period of about a few days. During such dust storms, the total ion conductivity is reduced by an order of magnitude. C1 [Haider, S. A.; Sheel, V.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Maguire, W. C.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Molina-Cuberos, G. J.] Univ Murcia, Grp Electromagnetismo, E-30100 Murcia, Spain. [Smith, M. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Haider, SA (reprint author), Phys Res Lab, Ahmadabad 380009, Gujarat, India. EM haider@prl.res.in RI Molina-Cuberos, Gregorio /K-7522-2014; Smith, Michael/C-8875-2012 OI Molina-Cuberos, Gregorio /0000-0002-5664-7028; NR 40 TC 13 Z9 13 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 30 PY 2010 VL 115 AR A12336 DI 10.1029/2010JA016125 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 701RF UT WOS:000285839400007 ER PT J AU Huang, XC Valeev, EF Lee, TJ AF Huang, Xinchuan Valeev, Edward F. Lee, Timothy J. TI Comparison of one-particle basis set extrapolation to explicitly correlated methods for the calculation of accurate quartic force fields, vibrational frequencies, and spectroscopic constants: Application to H2O, N2H+, NO2+, and C2H2 SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ELECTRONIC-STRUCTURE CALCULATIONS; RESOLUTION THRESHOLD PHOTOIONIZATION; LASER-ABSORPTION-SPECTROSCOPY; COUPLED-CLUSTER METHODS; GAUSSIAN-BASIS SETS; WAVE-FUNCTIONS; MOLECULAR CALCULATIONS; PROJECTION OPERATORS; PROTONATED NITROGEN; MICROWAVE-SPECTRUM AB One-particle basis set extrapolation is compared with one of the new R12 methods for computing highly accurate quartic force fields (QFFs) and spectroscopic data, including molecular structures, rotational constants, and vibrational frequencies for the H2O, N2H+, NO2+, and C2H2 molecules. In general, agreement between the spectroscopic data computed from the best R12 and basis set extrapolation methods is very good with the exception of a few parameters for N2H+ where it is concluded that basis set extrapolation is still preferred. The differences for H2O and NO2+ are small and it is concluded that the QFFs from both approaches are more or less equivalent in accuracy. For C2H2, however, a known one-particle basis set deficiency for C-C multiple bonds significantly degrades the quality of results obtained from basis set extrapolation and in this case the R12 approach is clearly preferred over one-particle basis set extrapolation. The R12 approach used in the present study was modified in order to obtain high precision electronic energies, which are needed when computing a QFF. We also investigated including core-correlation explicitly in the R12 calculations, but conclude that current approaches are lacking. Hence core-correlation is computed as a correction using conventional methods. Considering the results for all four molecules, it is concluded that R12 methods will soon replace basis set extrapolation approaches for high accuracy electronic structure applications such as computing QFFs and spectroscopic data for comparison to high-resolution laboratory or astronomical observations, provided one uses a robust R12 method as we have done here. The specific R12 method used in the present study, CCSD(T)(R12), incorporated a reformulation of one intermediate matrix in order to attain machine precision in the electronic energies. Final QFFs for N2H+ and NO2+ were computed, including basis set extrapolation, core-correlation, scalar relativity, and higher-order correlation and then used to compute highly accurate spectroscopic data for all isotopologues. Agreement with high-resolution experiment for (N2H+)-N-14 and (N2D+)-N-14 was excellent, but for (NO2+)-N-14-O-16 agreement for the two stretching fundamentals is outside the expected residual uncertainty in the theoretical values, and it is concluded that there is an error in the experimental quantities. It is hoped that the highly accurate spectroscopic data presented for the minor isotopologues of N2H+ and NO2+ will be useful in the interpretation of future laboratory or astronomical observations. (C) 2010 American Institute of Physics. [doi:10.1063/1.3506341] C1 [Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Valeev, Edward F.] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA. RP Lee, TJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Timothy.J.Lee@nasa.gov RI Valeyev, Eduard/A-5313-2009; HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012 OI Valeyev, Eduard/0000-0001-9923-6256; FU NASA [0 TR/LA PID 1022, 08-APRA08-0050]; NASA/SETI Institute [NNX09AI49A]; American Chemical Society [46811-G6]; U.S. National Science Foundation [CHE-0847295, CHE-0741927]; Alfred P. Sloan Foundation; Camille & Henry Dreyfus Foundation FX The authors gratefully acknowledge support from the NASA Herschel GO Program, Cycle 0 TR/LA PID 1022, and the NASA Grant No. 08-APRA08-0050. Dr. David Schwenke is gratefully acknowledged for helpful discussions. X. H. acknowledges the financial support by NASA/SETI Institute Cooperative Agreement NNX09AI49A. E. F. V. gratefully acknowledges the support of the American Chemical Society Petroleum Research Fund (Grant No. 46811-G6), the U.S. National Science Foundation (CAREER Award No. CHE-0847295 and CRIF:MU Award No. CHE-0741927), the Alfred P. Sloan Foundation, and the Camille & Henry Dreyfus Foundation. NR 83 TC 20 Z9 20 U1 1 U2 11 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 28 PY 2010 VL 133 IS 24 AR 244108 DI 10.1063/1.3506341 PG 15 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 700UG UT WOS:000285769200012 PM 21197977 ER PT J AU McCleese, DJ Heavens, NG Schofield, JT Abdou, WA Bandfield, JL Calcutt, SB Irwin, PGJ Kass, DM Kleinbohl, A Lewis, SR Paige, DA Read, PL Richardson, MI Shirley, JH Taylor, FW Teanby, N Zurek, RW AF McCleese, D. J. Heavens, N. G. Schofield, J. T. Abdou, W. A. Bandfield, J. L. Calcutt, S. B. Irwin, P. G. J. Kass, D. M. Kleinbohl, A. Lewis, S. R. Paige, D. A. Read, P. L. Richardson, M. I. Shirley, J. H. Taylor, F. W. Teanby, N. Zurek, R. W. TI Structure and dynamics of the Martian lower and middle atmosphere as observed by the Mars Climate Sounder: Seasonal variations in zonal mean temperature, dust, and water ice aerosols SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMAL STRUCTURE; GLOBAL SURVEYOR; TES AB The first Martian year and a half of observations by the Mars Climate Sounder aboard the Mars Reconnaissance Orbiter has revealed new details of the thermal structure and distributions of dust and water ice in the atmosphere. The Martian atmosphere is shown in the observations by the Mars Climate Sounder to vary seasonally between two modes: a symmetrical equinoctial structure with middle atmosphere polar warming and a solstitial structure with an intense middle atmosphere polar warming overlying a deep winter polar vortex. The dust distribution, in particular, is more complex than appreciated before the advent of these high (similar to 5 km) vertical resolution observations, which extend from near the surface to above 80 km and yield 13 dayside and 13 nightside pole-to-pole cross sections each day. Among the new features noted is a persistent maximum in dust mass mixing ratio at 15-25 km above the surface (at least on the nightside) during northern spring and summer. The water ice distribution is very sensitive to the diurnal and seasonal variation of temperature and is a good tracer of the vertically propagating tide. C1 [McCleese, D. J.; Schofield, J. T.; Abdou, W. A.; Kass, D. M.; Kleinbohl, A.; Shirley, J. H.; Zurek, R. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bandfield, J. L.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Calcutt, S. B.; Irwin, P. G. J.; Read, P. L.; Taylor, F. W.; Teanby, N.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England. [Heavens, N. G.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Lewis, S. R.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Paige, D. A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Richardson, M. I.] Ashima Res, Pasadena, CA 91106 USA. RP McCleese, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Calcutt, Simon/0000-0002-0102-3170; Teanby, Nicholas/0000-0003-3108-5775; Heavens, Nicholas/0000-0001-7654-503X; Irwin, Patrick/0000-0002-6772-384X; Lewis, Stephen/0000-0001-7237-6494 FU NASA FX We would like to thank Tina Pavlicek for her contributions to MCS instrument operations and Mark Apolinski for his work on processing the MCS data. We also wish to thank Wayne Hartford and Mark Foote for their contributions to the design and fabrication of the instrument and the MRO spacecraft operations teams who make this investigation possible. Work at the Jet Propulsion Laboratory, California Institute of Technology, was performed under a contract with NASA. NR 26 TC 61 Z9 62 U1 1 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 28 PY 2010 VL 115 AR E12016 DI 10.1029/2010JE003677 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 701QE UT WOS:000285836300001 ER PT J AU Mantry, S Ramsey-Musolf, MJ Sacco, GF AF Mantry, Sonny Ramsey-Musolf, Michael J. Sacco, Gian Franco TI Examination of higher-order twist contributions in parity-violating deep-inelastic electron-deuteron scattering SO PHYSICAL REVIEW C LA English DT Article ID NEUTRAL-CURRENT; MODEL AB We show that parity-violating deep-inelastic scattering (PVDIS) of longitudinally polarized electrons from deuterium can in principle be a relatively clean probe of higher twist quark-quark correlations beyond the parton model. As first observed by Bjorken and Wolfenstein, the dominant contribution to the electron polarization asymmetry, proportional to the axial vector electron coupling, receives corrections at twist four from the matrix element of a single four-quark operator. We reformulate the Bjorken-Wolfenstein argument in a matter suitable for the interpretation of experiments planned at the Thomas Jefferson National Accelerator Facility (JLab). In particular, we observe that because the contribution of the relevant twist-four operator satisfies the Callan-Gross relation, the ratio of parity-violating longitudinal and transverse cross sections, R(gamma Z), is identical to that for purely electromagnetic scattering, R(gamma), up to perturbative and power-suppressed contributions. This result simplifies the interpretation of the asymmetry in terms of other possible novel hadronic and electroweak contributions. We use the results of MIT Bag Model calculations to estimate contributions of the relevant twist-four operator to the leading term in the asymmetry as a function of Bjorken x and Q(2). We compare these estimates with possible leading twist corrections from violation of charge symmetry in the parton distribution functions. C1 [Mantry, Sonny; Ramsey-Musolf, Michael J.] Univ Wisconsin, Madison, WI 53706 USA. [Ramsey-Musolf, Michael J.] CALTECH, Pasadena, CA 91125 USA. [Sacco, Gian Franco] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mantry, S (reprint author), Univ Wisconsin, Madison, WI 53706 USA. EM mantry147@gmail.com; mjrm@physics.wisc.edu; gianfranco.sacco@jpl.nasa.gov FU US Department of Energy [DE-FG02-08ER4153]; Wisconsin Alumni Research Foundation; Alfred P. Sloan Foundation FX We thank A. Belitsky, C. Keppel, K. Kumar, T. Hobbs, T. Longergan, W. Melnitchouk, P. Mulders, P. Reimer, P. Souder, and C. Weiss for helpful exchanges and references to the literature. This work was supported in part under US Department of Energy Contract No. DE-FG02-08ER4153, the Wisconsin Alumni Research Foundation, and the Alfred P. Sloan Foundation. NR 18 TC 21 Z9 21 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2813 J9 PHYS REV C JI Phys. Rev. C PD DEC 27 PY 2010 VL 82 IS 6 AR 065205 DI 10.1103/PhysRevC.82.065205 PG 13 WC Physics, Nuclear SC Physics GA 713MZ UT WOS:000286743400006 ER PT J AU Furst, JU Strekalov, DV Elser, D Aiello, A Andersen, UL Marquardt, C Leuchs, G AF Fuerst, J. U. Strekalov, D. V. Elser, D. Aiello, A. Andersen, U. L. Marquardt, Ch. Leuchs, G. TI Low-Threshold Optical Parametric Oscillations in a Whispering Gallery Mode Resonator SO PHYSICAL REVIEW LETTERS LA English DT Article ID MONOLITHIC MICRORESONATOR; LITHIUM-NIOBATE; MICROCAVITIES; GENERATION AB In whispering gallery mode (WGM) resonator light is guided by continuous total internal reflection along a curved surface. Fabricating such resonators from an optically nonlinear material one takes advantage of their exceptionally high quality factors and small mode volumes to achieve extremely efficient optical frequency conversion. Our analysis of the phase-matching conditions for optical parametric down-conversion (PDC) in a spherical WGM resonator shows their direct relation to the sum rules for photons' angular momenta and predicts a very low parametric oscillation threshold. We realized such an optical parametric oscillator (OPO) based on naturally phase-matched PDC in lithium niobate. We demonstrated a single-mode, strongly nondegenerate OPO with a threshold of 6: 7 mu W and linewidth under 10 MHz. This work demonstrates the remarkable capabilities of WGM-based OPOs. C1 [Fuerst, J. U.; Strekalov, D. V.; Elser, D.; Aiello, A.; Andersen, U. L.; Marquardt, Ch.; Leuchs, G.] Max Planck Inst Sci Light, Erlangen, Germany. [Fuerst, J. U.; Elser, D.; Aiello, A.; Marquardt, Ch.; Leuchs, G.] Univ Erlangen Nurnberg, Dept Phys, Erlangen, Germany. [Strekalov, D. V.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Andersen, U. L.] Tech Univ Denmark, Dept Phys, DK-2800 Lyngby, Denmark. RP Furst, JU (reprint author), Max Planck Inst Sci Light, Erlangen, Germany. RI Andersen, Ulrik/A-5965-2011; Marquardt, Christoph/E-5332-2011; Leuchs, Gerd/G-6178-2012; Aiello, Andrea/A-7518-2012; Elser, Dominique/F-2750-2010; OI Andersen, Ulrik/0000-0002-1990-7687; Marquardt, Christoph/0000-0002-5045-513X; Leuchs, Gerd/0000-0003-1967-2766; Aiello, Andrea/0000-0003-1647-0448; Elser, Dominique/0000-0003-4852-5036 FU EU; Alexander von Humboldt foundation FX The authors would like to acknowledge funding from EU project COMPAS. D. V. S. acknowledges funding from the Alexander von Humboldt foundation, and J. U. F. from IMPRS. J. U. F. and Ch. M. thank Alessandro Villar for helpful discussions. NR 25 TC 64 Z9 64 U1 4 U2 31 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 27 PY 2010 VL 105 IS 26 AR 263904 DI 10.1103/PhysRevLett.105.263904 PG 4 WC Physics, Multidisciplinary SC Physics GA 713UQ UT WOS:000286763300003 PM 21231666 ER PT J AU Sato, K Kelley, RL Takei, Y Tamura, T Yamasaki, NY Ohashi, T Gupta, A Galeazzi, M AF Sato, Kosuke Kelley, Richard L. Takei, Yoh Tamura, Takayuki Yamasaki, Noriko Y. Ohashi, Takaya Gupta, Anjali Galeazzi, Massimiliano TI Study of the Intracluster and Intergalactic Medium in the Sculptor Supercluster with Suzaku SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies: clusters: individual (A 2801, A 2804, and A 2811); intergalactic medium; X-rays: diffuse background ID X-RAY-ABSORPTION; XMM-NEWTON; MISSING BARYONS; DARK-MATTER; HOT GAS; CLUSTER; TEMPERATURE; EMISSION; GALAXIES; ASCA AB We studied the high-temperature plasma in the direction of the Sculptor supercluster at z = 0.108 with Suzaku. Suzaku carried out four observations in the supercluster: namely, A 281 I, A 2811 offset, A 2804, A 2801 regions in 2005 November-December, including the regions beyond the virial radii of these clusters. The spectra taken in regions outside of the virial radii of the member clusters were used as background that included both of the Galactic and Cosmic X-ray Background (CXB) components. Temperature and metal abundance profiles were determined to the virial radii of the member clusters, and we then searched for oxygen line emission in the region outside of the virial radii of the clusters. As a result, the temperature of the clusters decreased toward the virial radii, and the spectral fits for the filament region did not require any extra component other than the Galactic and CXB components. We constrained the intensities of the O VII and O VIII lines to be less than 8.1 and 5.1 x 10(-8) photons cm(-2) s(-1) arcmin-2, respectively, as 2 sigma upper limits in the filament region. The intensity of O VII indicates n(H) < 1.6 x 10(-5) cm(-3) (Z/0.1 Z(circle dot))(-1/2)(L/25 Mpc)(-1/2), which corresponds to an over density of delta < 60(Z/0.1 Z(circle dot))(-1/2)(L/25 Mpc)(-1/2). C1 [Sato, Kosuke] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kelley, Richard L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Takei, Yoh; Tamura, Takayuki; Yamasaki, Noriko Y.] Japan Aerosp Explorat Agcy, ISAS, Chuo Ku, Kanagawa 2525210, Japan. [Ohashi, Takaya] Tokyo Metropolitan Univ, Dept Phys, Tokyo 1920397, Japan. [Gupta, Anjali; Galeazzi, Massimiliano] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. RP Sato, K (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM k_sato@mit.edu RI Yamasaki, Noriko/C-2252-2008; Kelley, Richard/K-4474-2012; Tamura, Takayuki/K-8236-2012; XRAY, SUZAKU/A-1808-2009 FU JSPS; Ministry of Education, Culture, Sports, Science and Technology [20340068, 20340041, 20840051, 21224003, 21740134] FX The authors are grateful to Noel Bermann for supporting the data analysis. We also thank the referee for providing valuable comments. K.S. is supported by a JSPS Postdoctral fellowship for research abroad. Part of this work was financially supported by the Ministry of Education, Culture, Sports, Science and Technology, Grant-in-Aid for Scientific Research Nos. 20340068, 20340041, 20840051, 21224003, 21740134. NR 47 TC 7 Z9 7 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD DEC 25 PY 2010 VL 62 IS 6 BP 1423 EP 1433 DI 10.1093/pasj/62.6.1423 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 708KG UT WOS:000286360100010 ER PT J AU Siegel, PH Pikov, V AF Siegel, P. H. Pikov, V. TI Impact of low intensity millimetre waves on cell functions SO ELECTRONICS LETTERS LA English DT Article ID INDUCED HYPOALGESIA; WATER DYNAMICS; SPECTROSCOPY; DEPENDENCE; RADIATION; FIELDS AB Investigations on the biological impact of low levels of millimetre-wave energy date back to the first experiments on the generation and detection of these high-frequency signals by Sir Jagadis Chunder Bose at the end of the 19th century. Slightly more than a hundred years later, millimetre-wave transmission has become a ubiquitous commercial reality. Despite the widespread use of millimetre-wave transmitters for communications, radar and even non-lethal weapons systems, only a handful of researchers have funded programmes focusing on millimetre-wave interactions with biological systems. As such, there is a growing need for a better understanding of the mechanisms of these interactions and their possible adverse and therapeutic implications. Independent of the health impact of long-term exposure to high doses of millimetre-wave energy on whole organisms, there exists the potential for subtle effects on specific tissues or organs which can best be quantified in studies which examine real-time changes in cellular function as energy is applied. In this Letter, a series of experiments are presented which show changes in cell membrane potential and the action potential firing rate of cortical neurons under short (1 min) exposures to continuous-wave 60 GHz radiation at mu W/cm(2) power levels, more than 1000 times below the US government maximum permissible exposure. The findings have implications for non-contact stimulation and control of neurologic function, and might prove useful in a variety of health applications from suppression of peripheral neuropathic pain to the treatment of central neurological disorders. C1 [Siegel, P. H.] CALTECH, Pasadena, CA 91125 USA. [Siegel, P. H.] Jet Prop Lab, Pasadena, CA 91125 USA. [Pikov, V.] Huntington Med Res Inst, Pasadena, CA 91105 USA. RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA. EM phs@caltech.edu NR 27 TC 6 Z9 6 U1 1 U2 25 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 DEC 23 PY 2010 VL 46 IS 26 SU S BP S70 EP S72 DI 10.1049/el.2010.8442 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 704KX UT WOS:000286053000026 ER PT J AU Siegel, P AF Siegel, Peter TI Dr Peter Siegel SO ELECTRONICS LETTERS LA English DT Editorial Material C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Siegel, P (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU INST ENGINEERING TECHNOLOGY-IET PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND SN 0013-5194 J9 ELECTRON LETT JI Electron. Lett. PD DEC 23 PY 2010 VL 46 IS 26 SU S BP S69 EP S69 DI 10.1049/el.2010.8455 PG 1 WC Engineering, Electrical & Electronic SC Engineering GA 704KX UT WOS:000286053000025 ER PT J AU Burton, ME Dougherty, MK Russell, CT AF Burton, M. E. Dougherty, M. K. Russell, C. T. TI Saturn's internal planetary magnetic field SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ROTATION PERIOD; MODEL; MAGNETOSPHERE; INTERIOR; JUPITER; DYNAMO AB A model of Saturn's internal planetary magnetic field based on data from the Cassini prime mission has been derived. In the absence of a determination of the rotation rate, the model is constrained to be axisymmetric. Non-axisymmetric models for a range of plausible planetary rotation periods have also been derived and we evaluate upper limits on the asymmetry of the internal magnetic field based on those models. We investigate whether a maximum in the non-axisymmetric magnetic field can be identified at a particular rotation rate thus providing insight into the rotation rate of the planet's interior. No such peak can unambiguously be identified. An axisymmetric octupole model is adequate to fit the data and addition of higher order terms does not improve the goodness of fit. The largest value of the dipole tilt obtained from non-axisymmetric models (<0.1 degrees) confirm the high degree of symmetry of Saturn's magnetic field. Citation: Burton, M. E., M. K. Dougherty, and C. T. Russell (2010), Saturn's internal planetary magnetic field, Geophys. Res. Lett., 37, L24105, doi:10.1029/2010GL045148. C1 [Burton, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dougherty, M. K.] Univ London Imperial Coll Sci Technol & Med, London SW7 5BZ, England. [Russell, C. T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Burton, ME (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM marcia.burton@jpl.nasa.gov RI Russell, Christopher/E-7745-2012 OI Russell, Christopher/0000-0003-1639-8298 NR 24 TC 37 Z9 37 U1 3 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 23 PY 2010 VL 37 AR L24105 DI 10.1029/2010GL045148 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 699BO UT WOS:000285639100001 ER PT J AU Risi, C Bony, S Vimeux, F Frankenberg, C Noone, D Worden, J AF Risi, Camille Bony, Sandrine Vimeux, Francoise Frankenberg, Christian Noone, David Worden, John TI Understanding the Sahelian water budget through the isotopic composition of water vapor and precipitation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; WEST-AFRICAN MONSOON; LARGE-SCALE ADVECTION; PART I; ANTARCTIC PRECIPITATION; INTERANNUAL VARIABILITY; GLOBAL PRECIPITATION; SUBTROPICAL HUMIDITY; CLIMATE VARIABILITY; RELATIVE-HUMIDITY AB The goal of this paper is to investigate the added value of water isotopic measurements to estimate the relative influence of large-scale dynamics, convection, and land surface recycling on the Sahelian water budget. To this aim, we use isotope data in the lower tropospheric water vapor measured by the SCIAMACHY and TES satellite instruments and in situ precipitation data from the Global Network for Isotopes in Precipitation and collected during the African Monsoon Multidisciplinary Analysis field campaign, together with water-tagging experiments with the Laboratoire de Meteorologie Dynamique general circulation model (LMDZ) fitted with isotopes. We show that some isotopic biases in LMDZ reveal the misrepresentation of dehydrating processes that would be undetected without isotopic measurements. In dry regions, the vapor isotopic composition is primarily controlled by the intensity of the air dehydration. In addition, it may also keep some memory of dehydration pathways that is erased in the humidity distribution, namely the relative contribution of dehydration in the tropical upper troposphere versus midlatitudes. In wet regions, vapor and rain isotope compositions are primarily controlled by changes in convection, through rain reevaporation and through the progressive depletion of the vapor by convective mixing along air mass trajectories. Gradients in vapor isotope composition along air mass trajectories may help estimate continental recycling intensity, provided that we could quantify the effect of convection on the isotopic composition of water vapor. C1 [Risi, Camille; Noone, David] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Risi, Camille; Bony, Sandrine] Meteorol Dynam Lab, F-75252 Paris 05, France. [Frankenberg, Christian; Worden, John] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vimeux, Francoise] UMR CEA CNRS UVSQ, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. [Vimeux, Francoise] CNRS, IRD, UM1, UM2,Lab HydroSci Montpellier, Gif Sur Yvette, France. RP Risi, C (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Bldg 318,216 UCB, Boulder, CO 80309 USA. EM camille.risi@lmd.jussieu.fr RI Frankenberg, Christian/A-2944-2013; OI Frankenberg, Christian/0000-0002-0546-5857; Bony, Sandrine/0000-0002-4791-4438 FU European Community; IPSL project; AMMA API; LEFE/MISTERRE national programme FX We gratefully thank Luc Descroix, Boubacar Ibrahim, Eric Lebreton, and Ibrahim Mamadou for the rain sampling in the Niamey region; S. Falourd and B. Minster for helping with the isotopic measurements. Based on a French initiative, AMMA was built by an international scientific group and is currently funded by a large number of agencies, especially from France, the United Kingdom, the United States and Africa. It has been the beneficiary of a major financial contribution from the European Community's Sixth Framework Research Programme. Detailed information on scientific coordination and funding is available on the AMMA International web site http://www.amma-international.org. This work was funded by the IPSL project, AMMA API and LEFE/MISTERRE national programme. We thank three anonymous reviewers for their constructive comments. NR 107 TC 43 Z9 45 U1 0 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 23 PY 2010 VL 115 AR D24110 DI 10.1029/2010JD014690 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 699CT UT WOS:000285642200009 ER PT J AU Benson, JL Kass, DM Kleinbohl, A McCleese, DJ Schofield, JT Taylor, FW AF Benson, Jennifer L. Kass, David M. Kleinboehl, Armin McCleese, Daniel J. Schofield, John T. Taylor, Fredric W. TI Mars' south polar hood as observed by the Mars Climate Sounder SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMAL EMISSION SPECTROMETER; ORBITER CAMERA; ICE CLOUDS AB We have used observations from the Mars Climate Sounder to investigate south polar hood water ice clouds (at 12 mu mm), including the first systematic examination of the vertical (5 km resolution) and nighttime structure. We find that the structure and evolution of the polar hood is controlled more strongly by atmospheric temperature variations than by intrinsic fluctuations in water vapor abundance. The clouds form as a belt during L-S = 10 degrees-70 degrees (phase 1) and L-S = 100 degrees-200 degrees (phase 2). During phase 1, the cloud belt extends over a wide latitude range, between 30 degrees S and 75 degrees S with a visible column optical depth between 0.075 and 0.15. The cloud belt then evaporates as temperatures warm. During phase 2, the cloud belt reappears due to an increase in water vapor as a partial band of low-opacity clouds south of the Tharsis region and eventually becomes continuous in longitude, with a visible column opacity between 0.125 and 0.25. As the southern spring equinox approaches, the cloud belt shifts southward, following the seasonal cap edge. From L-S = 140 degrees to L-S = 200 degrees, the daytime belt lies about 15 degrees farther south than the nighttime belt, due to tidally driven diurnal temperature differences. The vertical structure of the cloud belt is consistent within and between the two seasonal phases and is characterized by a thick lower cloud deck and an upper layer whose altitude shifts between the nighttime and daytime because of thermal tidal control of the condensation altitudes. Overall, the southern polar hood is observed to rapidly form and dissipate as the temperature crosses the saturation point of water vapor. C1 [Benson, Jennifer L.; Kass, David M.; Kleinboehl, Armin; McCleese, Daniel J.; Schofield, John T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Taylor, Fredric W.] Univ Oxford, Oxford OX1 3PU, England. RP Benson, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-237, Pasadena, CA 91109 USA. EM jennifer.benson@jpl.nasa.gov FU National Aeronautics and Space Administration FX We would like to thank the MCS instrument operations team. We also wish to thank Stephen Lewis, Peter Read, James Shirley, Nicholas Heavens, and two anonymous reviewers for their helpful comments on this paper. Work at the Jet Propulsion Laboratory, California Institute of Technology, was performed under a contract with the National Aeronautics and Space Administration. Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. NR 24 TC 19 Z9 19 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 23 PY 2010 VL 115 AR E12015 DI 10.1029/2009JE003554 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 699AX UT WOS:000285637400001 ER PT J AU Cruikshank, DP AF Cruikshank, Dale P. TI Generating an Atmosphere SO SCIENCE LA English DT Editorial Material ID OXYGEN; WATER C1 NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. RP Cruikshank, DP (reprint author), NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. EM dale.p.cruikshank@nasa.gov NR 7 TC 3 Z9 3 U1 0 U2 3 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 DEC 23 PY 2010 VL 330 IS 6012 BP 1755 EP 1756 DI 10.1126/science.1200473 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 698OS UT WOS:000285603700022 PM 21205657 ER PT J AU Cull, S Arvidson, RE Mellon, MT Skemer, P Shaw, A Morris, RV AF Cull, Selby Arvidson, Raymond E. Mellon, Michael T. Skemer, Philip Shaw, Amy Morris, Richard V. TI Compositions of subsurface ices at the Mars Phoenix landing site SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ULTRAVIOLET; WATER; MODEL AB NASA's Phoenix Lander uncovered two types of ice at its 2008 landing site on the northern plains of Mars: a brighter, slab-like ice that broke during Robotic Arm operations; and a darker icy deposit. Spectra from the Phoenix Surface Stereo Imager (SSI) are used to demonstrate that the brighter material consists of nearly pure water ice, which probably formed by migration and freezing of liquid water. The darker icy material consists of similar to 30 +/- 20 wt% ice, with the remainder composed of fine-grained soil, indicating that it probably formed as pore ice. These two types of ice represent two different emplacement mechanisms and periods of deposition. Citation: Cull, S., R. E. Arvidson, M. T. Mellon, P. Skemer, A. Shaw, and R. V. Morris (2010), Compositions of subsurface ices at the Mars Phoenix landing site, Geophys. Res. Lett., 37, L24203, doi: 10.1029/2010GL045372. C1 [Cull, Selby; Arvidson, Raymond E.; Skemer, Philip; Shaw, Amy] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Mellon, Michael T.] Univ Colorado, DEPT XXX, Boulder, CO 80309 USA. [Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Cull, S (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. RI Mellon, Michael/C-3456-2016 NR 22 TC 10 Z9 10 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 22 PY 2010 VL 37 AR L24203 DI 10.1029/2010GL045372 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 699BM UT WOS:000285638900004 ER PT J AU Martins, JPA Teixeira, J Soares, PMM Miranda, PMA Kahn, BH Dang, VT Irion, FW Fetzer, EJ Fishbein, E AF Martins, Joao P. A. Teixeira, Joao Soares, Pedro M. M. Miranda, Pedro M. A. Kahn, Brian H. Dang, Van T. Irion, Frederick W. Fetzer, Eric J. Fishbein, Evan TI Infrared sounding of the trade-wind boundary layer: AIRS and the RICO experiment SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SHALLOW CUMULUS CONVECTION; RETRIEVALS; VALIDATION; PRODUCTS; DEPTH AB The new generation of remote sensors on board NASA's A-Train constellation offers the possibility of observing the atmospheric boundary layer in different regimes, with or without clouds. In this study we use data from the Atmospheric InfraRed Sounder (AIRS) and of the Rain In Cumulus over the Ocean (RICO) campaign, to verify the accuracy and precision of the AIRS Version 5 Level 2 support product. This AIRS product has an improved vertical sampling that is necessary for the estimation of boundary layer properties. Good agreement is found between AIRS and RICO data, in a regime of oceanic shallow cumulus that is known to be difficult to analyze with other remote sensing data, and also shows a low sensitivity to cloud or land fraction. This suggests that AIRS data may be used for global boundary layer studies to support parameterization development in regions of difficult in-situ observation. Citation: Martins, J. P. A., J. Teixeira, P. M. M. Soares, P. M. A. Miranda, B. H. Kahn, V. T. Dang, F. W. Irion, E. J. Fetzer, and E. Fishbein (2010), Infrared sounding of the trade-wind boundary layer: AIRS and the RICO experiment, Geophys. Res. Lett., 37, L24806, doi: 10.1029/2010GL045902. C1 [Martins, Joao P. A.; Soares, Pedro M. M.; Miranda, Pedro M. A.] Univ Lisbon, CGUL, IDL, P-1749016 Lisbon, Portugal. [Teixeira, Joao; Kahn, Brian H.; Dang, Van T.; Irion, Frederick W.; Fetzer, Eric J.; Fishbein, Evan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Martins, JPA (reprint author), Univ Lisbon, CGUL, IDL, Edificio C8,Piso 3,Sala 8-8-32, P-1749016 Lisbon, Portugal. EM joaopam@gmail.com RI Martins, Joao/C-1713-2009; Miranda, Pedro/B-6971-2008; Soares, Pedro /K-6239-2012 OI Martins, Joao/0000-0003-4117-0754; Miranda, Pedro/0000-0002-4288-9456; Soares, Pedro /0000-0002-9155-5874 FU Portuguese Science Foundation (FCT) [SFRH/BD/37800/2007, PTDC/CLI/73814/2006]; European Union; NASA MAP program; Office of Naval Research; National Aeronautics and Space Administration FX JM is thankful to L. Nuijens, I. Trigo and C. Liang for discussions and comments on earlier versions of this paper. We would also like to thank P. Zuidema and an anonymous reviewer for their comments that greatly improved this manuscript. This work was partially funded by the Portuguese Science Foundation (FCT) under the grant SFRH/BD/37800/2007 and under Project REWRITE - PTDC/CLI/73814/2006, co-financed by the European Union under Program FEDER. JT acknowledges the support of the NASA MAP program and the Office of Naval Research. Part of 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 25 TC 11 Z9 11 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 22 PY 2010 VL 37 AR L24806 DI 10.1029/2010GL045902 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 699BM UT WOS:000285638900007 ER PT J AU Moorthy, KK Beegum, SN Babu, SS Smirnov, A John, SR Kumar, KR Narasimhulu, K Dutt, CBS Nair, VS AF Moorthy, K. Krishna Beegum, S. Naseema Babu, S. Suresh Smirnov, Alexander John, Sherine Rachel Kumar, K. Raghavendra Narasimhulu, K. Dutt, C. B. S. Nair, Vijayakumar S. TI Optical and physical characteristics of Bay of Bengal aerosols during W-ICARB: Spatial and vertical heterogeneities in the marine atmospheric boundary layer and in the vertical column SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID INDO-GANGETIC BASIN; PENINSULAR INDIA; SIZE DISTRIBUTIONS; SUN PHOTOMETER; MONSOON SEASON; ATLANTIC-OCEAN; BLACK CARBON; ART.; DEPTHS; ASIA AB Analysis of the continuous and collocated measurements of columnar spectral aerosol optical depths (AODs) and mass size distributions in the marine atmospheric boundary layer (MABL) over the Bay of Bengal (BoB), carried out from 27 December 2008 to 29 January 2009 during the Winter Integrated Campaign for Aerosols, Gases and Radiation Budget (W-ICARB), revealed distinct regional features in the spatial variations of the aerosol properties in the MABL and column. In general, AODs were high over the northern and northwestern parts of the BoB, with pockets of very high values, within which the AODs were as high as similar to 0.8 while the smallest values (similar to 0.1) were observed over the northeastern BoB, off the Myanmar and Bangladesh coasts. Interestingly, though, this region had the highest Angstrom wavelength exponent alpha (similar to 1.5), notwithstanding the generally high values that prevailed over the eastern as well as northern coastal regions of India. Back trajectory analyses revealed the significant role of the advected aerosols in the observed spatial pattern. Within the MABL, high accumulation mode mass concentrations (M-A) prevailed over the entire BoB with the accumulation fraction ranging from 0.6 to 0.95, whereas very high fine-mode (r < 0.1 mu m) aerosol mass fractions (similar to 0.8) were observed over the northeastern and western coastal BoB adjoining the Indian mainland (where alpha was high to very high). The vertical distributions, inferred from the columnar and MABL properties as well as from the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations data, revealed better homogeneity in the northeastern and eastern BoB, whereas significant heterogeneity was seen over other regions. C1 [Moorthy, K. Krishna; Beegum, S. Naseema; Babu, S. Suresh; John, Sherine Rachel; Nair, Vijayakumar S.] Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum 695022, Kerala, India. [Dutt, C. B. S.] ISRO Head Quarters, Bangalore 560094, Karnataka, India. [Kumar, K. Raghavendra; Narasimhulu, K.] Sri Krishnadevaraya Univ, Dept Phys, Anantapur 515005, Andhra Pradesh, India. [Smirnov, Alexander] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20770 USA. RP Moorthy, KK (reprint author), Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum 695022, Kerala, India. RI Smirnov, Alexander/C-2121-2009; OI Smirnov, Alexander/0000-0002-8208-1304; Moorthy, K. Krishna/0000-0002-7234-3868 NR 54 TC 36 Z9 36 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 22 PY 2010 VL 115 AR D24213 DI 10.1029/2010JD014094 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 699CS UT WOS:000285642100002 ER PT J AU Baiotti, L Damour, T Giacomazzo, B Nagar, A Rezzolla, L AF Baiotti, Luca Damour, Thibault Giacomazzo, Bruno Nagar, Alessandro Rezzolla, Luciano TI Analytic Modeling of Tidal Effects in the Relativistic Inspiral of Binary Neutron Stars SO PHYSICAL REVIEW LETTERS LA English DT Article AB To detect the gravitational-wave (GW) signal from binary neutron stars and extract information about the equation of state of matter at nuclear density, it is necessary to match the signal with a bank of accurate templates. We present the two longest (to date) general-relativistic simulations of equal-mass binary neutron stars with different compactnesses, C = 0.12 and C = 0.14, and compare them with a tidal extension of the effective-one-body (EOB) model. The typical numerical phasing errors over the similar or equal to 22 GW cycles are Delta phi similar or equal to +/- 0.24 rad. By calibrating only one parameter (representing a higher-order amplification of tidal effects), the EOB model can reproduce, within the numerical error, the two numerical waveforms essentially up to the merger. By contrast, the third post-Newtonian Taylor-T4 approximant with leading-order tidal corrections dephases with respect to the numerical waveforms by several radians. C1 [Baiotti, Luca] Osaka Univ, Inst Laser Engn, Suita, Osaka, Japan. [Baiotti, Luca] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 606, Japan. [Damour, Thibault; Nagar, Alessandro] Inst Hautes Etud Sci, F-91440 Bures Sur Yvette, France. [Damour, Thibault] ICRANet, Pescara, Italy. [Giacomazzo, Bruno] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacomazzo, Bruno] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. [Giacomazzo, Bruno; Rezzolla, Luciano] Albert Einstein Inst, Max Planck Inst Gravitat Phys, Potsdam, Germany. [Rezzolla, Luciano] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. RP Baiotti, L (reprint author), Osaka Univ, Inst Laser Engn, Suita, Osaka, Japan. RI Giacomazzo, Bruno/I-8088-2012 OI Giacomazzo, Bruno/0000-0002-6947-4023 FU DFG [SFB/Transregio 7]; CompStar; JSPS [19-07803]; MEXT [22740163]; NASA [NNX09AI75G] FX We thank the developers of CACTUS and CARPET for their continuous improvements. The simulations were performed on Ranger (TACC/TG-MCA02N014) and Damiana (AEI). This work was supported by the DFG grant SFB/Transregio 7, by "CompStar,'' a Research Networking Programme of the ESF, by the JSPS Grant-in-Aid for Scientific Research (19-07803), by the MEXT Grant-in-Aid for Young Scientists (22740163), and by NASA (NNX09AI75G). NR 33 TC 80 Z9 81 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 22 PY 2010 VL 105 IS 26 AR 261101 DI 10.1103/PhysRevLett.105.261101 PG 4 WC Physics, Multidisciplinary SC Physics GA 713SD UT WOS:000286756800004 PM 21231639 ER PT J AU Scollo, S Folch, A Coltelli, M Realmuto, VJ AF Scollo, S. Folch, A. Coltelli, M. Realmuto, V. J. TI Three-dimensional volcanic aerosol dispersal: A comparison between Multiangle Imaging Spectroradiometer (MISR) data and numerical simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TEPHRA-FALL DEPOSITS; CLOUD-TOP HEIGHTS; MT.-ETNA VOLCANO; OPTICAL-THICKNESS; SIZE DISTRIBUTION; SATELLITE DATA; PLUME; ERUPTION; ASH; RETRIEVAL AB The three-dimensional reconstruction of volcanic plumes is a central goal to enhance our understanding on dispersal processes. In this paper we use data from the Multiangle Imaging Spectroradiometer (MISR) on board NASA's Terra spacecraft combined with a stereo matching retrieval procedure. We show the potential of MISR in capturing important features of volcanic plumes like column height, optical depth, type, and shape of the finest particles of two highly explosive eruptions occurring on Mount Etna in 2001 and 2002. This work tests how tephra dispersal models reconstruct the 3-D shape of volcanic clouds. We compare MISR data with FALL3D, an Eulerian model for the transport and deposition of volcanic ash and aerosols coupled with the Weather Research and Forecasting mesoscale meteorological model. Agreement between simulations and MISR data is good regarding both events, although it could be improved by increasing the accuracy of the meteorological data, a better constraint on volcanological input parameters like the height of the eruptive column and improving our understanding of processes such as aggregation phenomena and volcanic cloud microphysics. C1 [Scollo, S.; Coltelli, M.] Ist Nazl Geofis & Vulcanol Sez Catania, I-95123 Catania, Italy. [Folch, A.] Barcelona Supercomp Ctr, Barcelona 08034, Spain. [Realmuto, V. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Scollo, S (reprint author), Ist Nazl Geofis & Vulcanol Sez Catania, Piazza Roma 2, I-95123 Catania, Italy. EM scollo@ct.ingv.it; arnau.folch@bsc.es; coltelli@ct.ingv.it; vincent.j.realmuto@jpl.nasa.gov RI Coltelli, Mauro/F-1676-2015; Folch, Arnau/G-2996-2015 OI Coltelli, Mauro/0000-0001-7868-3946; Folch, Arnau/0000-0002-0677-6366 FU Ministry of Universities and Research; Barcelona Supercomputing Center (BSC); National Aeronautics and Space Administration FX The authors are grateful to D. Andronico and G. Bluth for their preliminary review of the paper. We thank M. Prestifilippo and M. Palano for providing plot base maps. The authors greatly thank the native speaker Stephen Conwey; Maria Carreras, and J.M. Baldasano, head of the BSC Earth Science Department, for supporting this work; David L. Nelson for his assistance in the analysis of the MISR data obtained by MINX and a review of the paper; the principal investigator David Diner and all the MISR team of NASA at Jet Propulsion Laboratory, California Institute of Technology, are sincerely thanked for their useful suggestions, encouragement to pursue this research, and support during the stay of one of the authors (Simona Scollo) at JPL. The MISR data used in this study were obtained from the NASA Langley Research Center Atmospheric Science Data Center. We greatly thank the editor Yinon Rudich, the reviewer Adam Durant, and two anonymous reviewers that improved the quality of the paper with their constructive suggestions. This work was funded by the FIRB project "Sviluppo Nuove Tecnologie per la Protezione e Difesa del Territorio dai Rischi Naturali" of Ministry of Universities and Research for one of the authors (S. Scollo), and by the HPC-Europa Transnational Access programme at the Barcelona Supercomputing Center (BSC). "Part of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration". NR 89 TC 11 Z9 11 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 21 PY 2010 VL 115 AR D24210 DI 10.1029/2009JD013162 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 699CR UT WOS:000285642000001 ER PT J AU Moore, TE Fok, MC Delcourt, DC Slinker, SP Fedder, JA AF Moore, T. E. Fok, M. -C. Delcourt, D. C. Slinker, S. P. Fedder, J. A. TI Global response to local ionospheric mass ejection SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND; PLASMA SHEET; RING CURRENT; ION OUTFLOW; POLAR-CAP; DENSITY; EVENTS AB We revisit a reported "Ionospheric Mass Ejection" using prior event observations to guide a global simulation of local ionospheric outflows, global magnetospheric circulation, and plasma sheet pressurization, and comparing our results with the observed global response. Our simulation framework is based on test particle motions in the Lyon-Fedder-Mobarry (LFM) global circulation model electromagnetic fields. The inner magnetosphere is simulated with the Comprehensive Ring Current Model (CRCM) of Fok and Wolf, driven by the transpolar potential developed by the LFM magnetosphere, and includes an embedded plasmaspheric simulation. Global circulation is stimulated using the observed solar wind conditions for the period 24-25 September 1998. This period begins with the arrival of a Coronal Mass Ejection, initially with northward, but later with southward interplanetary magnetic field. Test particles are launched from the ionosphere with fluxes specified by local empirical relationships of outflow to electrodynamic and particle precipitation imposed by the MHD simulation. Particles are tracked until they are lost from the system downstream or into the atmosphere, using the full equations of motion. Results are compared with the observed ring current and a simulation of polar and auroral wind outflows driven globally by solar wind dynamic pressure. We find good quantitative agreement with the observed ring current, and reasonable qualitative agreement with earlier simulation results, suggesting that the solar wind driven global simulation generates realistic energy dissipation in the ionosphere and that the Strangeway relations provide a realistic local outflow description. C1 [Moore, T. E.; Fok, M. -C.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Delcourt, D. C.] Ctr Etud Environm Terrestre & Planetaires, F-94107 St Maur, France. [Fedder, J. A.] Leading Edge Technol Inc, Alexandria, VA 22301 USA. [Slinker, S. P.] USN, Res Lab, Washington, DC 20375 USA. RP Moore, TE (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Code 670, Greenbelt, MD 20771 USA. EM t.e.moore@nasa.gov RI Moore, Thomas/D-4675-2012; Fok, Mei-Ching/D-1626-2012 OI Moore, Thomas/0000-0002-3150-1137; FU NASA Heliophysics Division [WBS 936723.02.01.03.82]; NASA FX We thank Manuel Buenfil and Robert Wiegand, who through their mastery of mathematics, programming, database, and visualization, made this work possible. We acknowledge support from the NASA Heliophysics Division through the ROSES program under WBS 936723.02.01.03.82, and NASA's High Performance Computing Program. NR 24 TC 4 Z9 4 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 21 PY 2010 VL 115 AR A00J14 DI 10.1029/2010JA015640 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 699BQ UT WOS:000285639300004 ER PT J AU Huang, FT Mayr, HG Russell, JM Mlynczak, MG AF Huang, Frank T. Mayr, Hans G. Russell, James M., III Mlynczak, Martin G. TI Ozone diurnal variations in the stratosphere and lower mesosphere, based on measurements from SABER on TIMED SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID QUASI-BIENNIAL OSCILLATION; RESEARCH SATELLITE UARS; LIMB SOUNDER INSTRUMENT; TEMPERATURE CORRELATIONS; LOWER THERMOSPHERE; DIMENSIONAL MODEL; ATMOSPHERE; MLS; VARIABILITY; VALIDATION AB We report on derived results of global zonal mean ozone diurnal variations over 24 h of local solar time, based on satellite measurements from SABER on the Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) satellite, with focus on the stratosphere and lower mesosphere. On a global scale, results in this altitude range are new. We had previously reported on ozone diurnal variations, but the focus was at higher altitudes, where the variations can be relatively large. In the stratosphere, there can be systematic diurnal variations on the order of a few percent, with multiple local maxima over a day, and these can exist down to altitudes of similar to 31 hPa (similar to 24 km) and lower. At these altitudes, photochemistry is expected to be less effective, and dynamics (e. g., tides) can be more important. The diurnal variations also depend on latitude and season. As a function of altitude, for low latitudes at least, the ozone diurnal variations show a pattern of local-time phase progression such that beginning at similar to 31 hPa the mixing ratios are smaller in the afternoon (compared to values at midnight), then (as the altitude increases) become mostly larger in the afternoon beginning from similar to 10 to 4.6 hPa, revert back to intermediate afternoon values near 2.2, 1.5 hPa, and again return to lower daytime values at about 1 hPa, with this last trend continuing to higher altitudes in the mesosphere. This pattern of variation is generally supported by previous results by us and by others, based on data from MLS UARS, MLS Aura, rocket-borne, and ground-based measurements. C1 [Huang, Frank T.] Univ Maryland Baltimore Cty, GEST, Baltimore, MD 21228 USA. [Mayr, Hans G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Huang, FT (reprint author), Univ Maryland Baltimore Cty, GEST, Baltimore, MD 21228 USA. EM fthuang@comcast.net RI Mlynczak, Martin/K-3396-2012 FU NASA FX We thank Editor Joost de Gouw, and three reviewers for insightful comments that improved this paper. F. T. Huang was supported under a NASA contract to the Goddard Earth Sciences and Technology Center (GEST), University of Maryland Baltimore County. NR 46 TC 15 Z9 15 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 21 PY 2010 VL 115 AR D24308 DI 10.1029/2010JD014484 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 699CR UT WOS:000285642000007 ER PT J AU Krotkov, NA Schoeberl, MR Morris, GA Carn, S Yang, K AF Krotkov, N. A. Schoeberl, M. R. Morris, G. A. Carn, S. Yang, K. TI Dispersion and lifetime of the SO2 cloud from the August 2008 Kasatochi eruption SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING INSTRUMENT; SULFUR-DIOXIDE; VOLCANIC-ERUPTIONS; MODEL; SATELLITE; EMISSIONS; CLIMATE; SULFATE; TOMS; ULTRAVIOLET AB Hemispherical dispersion of the SO2 cloud from the August 2008 Kasatochi eruption is analyzed using satellite data from the Ozone Monitoring Instrument (OMI) and the Goddard Trajectory Model (GTM). The operational OMI retrievals underestimate the total SO2 mass by 20-30% on 8-11 August, as compared with more accurate offline Extended Iterative Spectral Fit (EISF) retrievals, but the error decreases with time due to plume dispersion and a drop in peak SO2 column densities. The GTM runs were initialized with and compared to the operational OMI SO2 data during early plume dispersion to constrain SO2 plume heights and eruption times. The most probable SO2 heights during initial dispersion are estimated to be 10-12 km, in agreement with direct height retrievals using EISF algorithm and IR measurements. Using these height constraints a forward GTM run was initialized on 11 August to compare with the month-long Kasatochi SO2 cloud dispersion patterns. Predicted volcanic cloud locations generally agree with OMI observations, although some discrepancies were observed. Operational OMI SO2 burdens were refined using GTM-predicted mass-weighted probability density height distributions. The total refined SO2 mass was integrated over the Northern Hemisphere to place empirical constraints on the SO2 chemical decay rate. The resulting lower limit of the Kasatochi SO2 e-folding time is similar to 8-9 days. Extrapolation of the exponential decay back in time yields an initial erupted SO2 mass of similar to 2.2 Tg on 8 August, twice as much as the measured mass on that day. C1 [Krotkov, N. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schoeberl, M. R.] Sci & Technol Corp, Columbia, MD 21046 USA. [Morris, G. A.] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA. [Carn, S.] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA. [Yang, K.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Krotkov, NA (reprint author), NASA, Goddard Space Flight Ctr, MS 613-3, Greenbelt, MD 20771 USA. EM nickolay.a.krotkov@nasa.gov RI Krotkov, Nickolay/E-1541-2012 OI Krotkov, Nickolay/0000-0001-6170-6750 FU NASA [NNG06GI00G, NNH04ZYS004N, NNS06AA05G]; Fulbright Scholar program; NASA Earth Science Division FX Funding for this work was provided by the NASA awards NNG06GI00G (Mapping SO2 emissions with NASA Ozone Monitoring Instrument (OMI) and GOCART model for air quality and climate science), NNH04ZYS004N (Validation of OMI L2 Sulfur Dioxide retrievals over volcanic and anthropogenic sources), and CAN NNS06AA05G (Volcanic Cloud Data for Aviation Hazards). The Dutch-Finnish-built OMI instrument is part of the NASA EOS Aura satellite payload. The OMI project is managed by NIVR and KNMI in the Netherlands. The authors would like to thank the KNMI OMI team for producing L1B radiance data and the U. S. OMI Science and Operations teams for continuing support. G. A. Morris thanks the Fulbright Scholar program and the NASA Earth Science Division for financial support while conducting this research and thanks colleagues J. Hirokawa, M. Fujiwara, and F. Hasebe in the department of Environmental Earth Science at Hokkaido University, Sapporo, Japan, where G. A. Morris conducted his research. The authors would like to thank anonymous reviewers for their important suggestions that helped improving the manuscript. NR 66 TC 43 Z9 43 U1 1 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 21 PY 2010 VL 115 AR D00L20 DI 10.1029/2010JD013984 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 699CR UT WOS:000285642000003 ER PT J AU Oman, LD Plummer, DA Waugh, DW Austin, J Scinocca, JF Douglass, AR Salawitch, RJ Canty, T Akiyoshi, H Bekki, S Braesicke, P Butchart, N Chipperfield, MP Cugnet, D Dhomse, S Eyring, V Frith, S Hardiman, SC Kinnison, DE Lamarque, JF Mancini, E Marchand, M Michou, M Morgenstern, O Nakamura, T Nielsen, JE Olivie, D Pitari, G Pyle, J Rozanov, E Shepherd, TG Shibata, K Stolarski, RS Teyssedre, H Tian, W Yamashita, Y Ziemke, JR AF Oman, L. D. Plummer, D. A. Waugh, D. W. Austin, J. Scinocca, J. F. Douglass, A. R. Salawitch, R. J. Canty, T. Akiyoshi, H. Bekki, S. Braesicke, P. Butchart, N. Chipperfield, M. P. Cugnet, D. Dhomse, S. Eyring, V. Frith, S. Hardiman, S. C. Kinnison, D. E. Lamarque, J. -F. Mancini, E. Marchand, M. Michou, M. Morgenstern, O. Nakamura, T. Nielsen, J. E. Olivie, D. Pitari, G. Pyle, J. Rozanov, E. Shepherd, T. G. Shibata, K. Stolarski, R. S. Teyssedre, H. Tian, W. Yamashita, Y. Ziemke, J. R. TI Multimodel assessment of the factors driving stratospheric ozone evolution over the 21st century SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID CHEMISTRY-CLIMATE MODEL; MIDDLE ATMOSPHERE; GREENHOUSE GASES; DOUBLED CO2; CARBON-DIOXIDE; TECHNICAL NOTE; NITROUS-OXIDE; DATA RECORD; TEMPERATURE; TRENDS AB The evolution of stratospheric ozone from 1960 to 2100 is examined in simulations from 14 chemistry-climate models, driven by prescribed levels of halogens and greenhouse gases. There is general agreement among the models that total column ozone reached a minimum around year 2000 at all latitudes, projected to be followed by an increase over the first half of the 21st century. In the second half of the 21st century, ozone is projected to continue increasing, level off, or even decrease depending on the latitude. Separation into partial columns above and below 20 hPa reveals that these latitudinal differences are almost completely caused by differences in the model projections of ozone in the lower stratosphere. At all latitudes, upper stratospheric ozone increases throughout the 21st century and is projected to return to 1960 levels well before the end of the century, although there is a spread among models in the dates that ozone returns to specific historical values. We find decreasing halogens and declining upper atmospheric temperatures, driven by increasing greenhouse gases, contribute almost equally to increases in upper stratospheric ozone. In the tropical lower stratosphere, an increase in upwelling causes a steady decrease in ozone through the 21st century, and total column ozone does not return to 1960 levels in most of the models. In contrast, lower stratospheric and total column ozone in middle and high latitudes increases during the 21st century, returning to 1960 levels well before the end of the century in most models. C1 [Oman, L. D.; Douglass, A. R.; Frith, S.; Nielsen, J. E.; Stolarski, R. S.; Ziemke, J. R.] NASA, Atmospher Chem & Dynam Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Akiyoshi, H.; Nakamura, T.; Yamashita, Y.] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan. [Austin, J.] NOAA Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA. [Bekki, S.; Cugnet, D.; Marchand, M.] UPMC, LATMOS IPSL, F-75252 Paris, France. [Braesicke, P.; Pyle, J.] Univ Cambridge, Dept Chem, Ctr Atmospher Sci, NCAS Climate Chem, Cambridge CB2 1EW, England. [Butchart, N.; Hardiman, S. C.] Met Off Hadley Ctr, Exeter EX1 3PB, Devon, England. [Salawitch, R. J.; Canty, T.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Chipperfield, M. P.; Dhomse, S.; Tian, W.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Eyring, V.] Deutsch Zentrum Luft & Raumfahrt, Inst Atmospher Phys, D-82234 Oberpfaffenhofen, Germany. [Kinnison, D. E.; Lamarque, J. -F.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Mancini, E.; Pitari, G.] Univ Aquila, Dipartimento Fis, I-67010 Laquila, Italy. [Michou, M.; Olivie, D.; Teyssedre, H.] CNRS, GAME CNRM, F-31057 Toulouse, France. [Morgenstern, O.] Natl Inst Water & Atmospher Res, Lauder 9352, New Zealand. [Plummer, D. A.; Scinocca, J. F.] Canadian Ctr Climate Modelling & Anal, Victoria, BC V8W 3V6, Canada. [Rozanov, E.] World Radiat Ctr, Phys Meteorol Observ Davos, CH-7260 Davos, Switzerland. [Shepherd, T. G.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Shibata, K.] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki 3050052, Japan. [Waugh, D. W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Ziemke, J. R.] Univ Maryland, Goddard Earth Sci & Technol Ctr, Catonsville, MD 21228 USA. [Rozanov, E.] ETHZ, IAC, Zurich, Switzerland. [Frith, S.; Nielsen, J. E.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Oman, LD (reprint author), NASA, Atmospher Chem & Dynam Branch, Goddard Space Flight Ctr, Code 613-3, Greenbelt, MD 20771 USA. EM luke.d.oman@nasa.gov RI Pitari, Giovanni/O-7458-2016; Eyring, Veronika/O-9999-2016; Waugh, Darryn/K-3688-2016; Canty, Timothy/F-2631-2010; Dhomse, Sandip/C-8198-2011; Salawitch, Ross/B-4605-2009; Rozanov, Eugene/A-9857-2012; Douglass, Anne/D-4655-2012; Oman, Luke/C-2778-2009; Stolarski, Richard/B-8499-2013; Chipperfield, Martyn/H-6359-2013; Lamarque, Jean-Francois/L-2313-2014; bekki, slimane/J-7221-2015; Nakamura, Tetsu/M-7914-2015; Braesicke, Peter/D-8330-2016 OI Pitari, Giovanni/0000-0001-7051-9578; Eyring, Veronika/0000-0002-6887-4885; Mancini, Eva/0000-0001-7071-0292; Morgenstern, Olaf/0000-0002-9967-9740; Waugh, Darryn/0000-0001-7692-2798; Canty, Timothy/0000-0003-0618-056X; Dhomse, Sandip/0000-0003-3854-5383; Salawitch, Ross/0000-0001-8597-5832; Rozanov, Eugene/0000-0003-0479-4488; Oman, Luke/0000-0002-5487-2598; Stolarski, Richard/0000-0001-8722-4012; Chipperfield, Martyn/0000-0002-6803-4149; Lamarque, Jean-Francois/0000-0002-4225-5074; bekki, slimane/0000-0002-5538-0800; Nakamura, Tetsu/0000-0002-2056-7392; Braesicke, Peter/0000-0003-1423-0619 FU NASA MAP; ACMAP; Aura programs; NSF; Ministry of the Environment of Japan [A-071, A-0903]; DECC/Defra [GA01101]; European Commission FX This research was supported by the NASA MAP, ACMAP, and Aura programs and the NSF Large-scale Climate Dynamics program. We thank Susan Strahan for very helpful comments on this manuscript, and we thank three anonymous reviewers for thoughtful, constructive reviews of the submitted paper. We acknowledge the Chemistry-Climate Model Validation (CCMVal) Activity of the WCRP SPARC project for organizing and coordinating the model data analysis activity and the British Atmospheric Data Centre for collecting and archiving the CCMVal model outputs. CCSRNIES research was supported by the Global Environmental Research Fund of the Ministry of the Environment of Japan (A-071 and A-0903), and simulations were completed with the supercomputer at CGER, NIES. The MRI simulation was made with the supercomputer at the National Institute for Environmental Studies, Japan. The contribution from the Met Office Hadley Centre was supported by the Joint DECC and Defra Integrated Climate Programme-DECC/Defra (GA01101). The contribution from the LATMOS-IPSL was supported by the European Commission through the funding of the RECONCILE and GEOMON projects. The National Center for Atmospheric Research is operated by the University Corporation for Atmospheric Research under sponsorship of the National Science Foundation. Any opinions, findings, and conclusions or recommendations expressed in the publication are those of the authors and do not necessarily reflect the views of the National Science Foundation. NR 69 TC 30 Z9 30 U1 1 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 21 PY 2010 VL 115 AR D24306 DI 10.1029/2010JD014362 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 699CR UT WOS:000285642000006 ER PT J AU Wang, WC Huang, JP Minnis, P Hu, YX Li, JM Huang, ZW Ayers, JK Wang, TH AF Wang, Wencai Huang, Jianping Minnis, Patrick Hu, Yongxiang Li, Jiming Huang, Zhongwei Ayers, J. Kirk Wang, Tianhe TI Dusty cloud properties and radiative forcing over dust source and downwind regions derived from A-Train data during the Pacific Dust Experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ANGULAR-DISTRIBUTION MODELS; ENERGY SYSTEM INSTRUMENT; APRIL 1998; TERRA SATELLITE; FLUX ESTIMATION; MODIS DATA; PRECIPITATION; TRANSPORT; CLIMATE; CERES AB Dusty cloud properties and radiative forcing over northwestern China (source region) are compared to the same quantities over the northwestern Pacific (downwind region) during the Pacific Dust Experiment (PACDEX; April 2007 to May 2007) using collocated data from three satellites in the A-Train constellation: CALIPSO (Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations), the Clouds and Earth Radiant Energy System on Aqua, and CloudSat. Dusty clouds are defined as clouds extant in a dust plume environment (i.e., dust aerosols observed within 50 m of the cloud), while pure clouds are those in dust-free conditions. CALIPSO lidar and CloudSat radar measurements are used to discriminate between dusty and pure clouds in both study regions. It was found that dust aerosols change the microphysical characteristics of clouds, reducing the cloud optical depth, liquid and ice water path, and effective droplet size. The decreased cloud optical depths and water paths diminish the cloud cooling effect, leading to a greater warming effect. The dust aerosols cause an instantaneous net cloud cooling effect of 43.4% and 16.7% in the source and downwind regions, respectively. The dust aerosol effects appear to be greater for ice clouds than for liquid water clouds in the downwind region. These results are consistent with PACDEX aircraft observations. C1 [Wang, Wencai; Huang, Jianping; Li, Jiming; Huang, Zhongwei; Wang, Tianhe] Lanzhou Univ, Coll Atmospher Sci, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China. [Ayers, J. Kirk] SSAI, Hampton, VA 23666 USA. [Minnis, Patrick; Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23666 USA. RP Wang, WC (reprint author), Lanzhou Univ, Coll Atmospher Sci, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China. EM hjp@lzu.edu.cn RI Hu, Yongxiang/K-4426-2012; Wang, Tianhe/F-8236-2012; Huang, Zhongwei/K-5484-2013; Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 FU National Science Foundation of China [40725015, 40633017]; Chinese Academy of Sciences [IAP09311]; NASA; Radiation Sciences Program FX This research was supported by the National Science Foundation of China under grants 40725015 and 40633017, by the Knowledge Innovation Program of the Chinese Academy of Sciences under grant IAP09311, by the NASA Science Mission through the CALIPSO Project, and by the Radiation Sciences Program through the CERES Project. The CALIPSO, CERES Single Scanner Footprint, and CloudSat data were obtained from the NASA Earth Observing System Data and Information System, Atmospheric Sciences Data Center (ASDC), at Langley Research Center. NR 47 TC 28 Z9 28 U1 3 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 21 PY 2010 VL 115 AR D00H35 DI 10.1029/2010JD014109 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 699CR UT WOS:000285642000004 ER PT J AU Moore, TE Khazanov, GV AF Moore, T. E. Khazanov, G. V. TI Mechanisms of ionospheric mass escape SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LATITUDE F-REGION; VELOCITY DISTRIBUTION FUNCTION; MONTE-CARLO CALCULATIONS; POLAR WIND; SOLAR-WIND; CENTRIFUGAL ACCELERATION; AURORAL IONOSPHERE; ION ENERGIZATION; PLASMA; UPFLOWS AB The dependence of ionospheric O(+) escape flux on electromagnetic energy flux and electron precipitation into the ionosphere is derived for a hypothetical ambipolar pickup process, powered the relative motion of plasmas and neutral upper atmosphere, and by electron precipitation, at heights where the ions are magnetized but influenced by photo-ionization, collisions with gas atoms, ambipolar and centrifugal acceleration. Ion pickup by the convection electric field produces "ring-beam" or toroidal velocity distributions, as inferred from direct plasma measurements, from observations of the associated waves, and from the spectra of incoherent radar echoes. Ring beams are unstable to plasma wave growth, resulting in rapid relaxation via transverse velocity diffusion, into transversely accelerated ion populations. Ion escape is substantially facilitated by the ambipolar potential, but is only weakly affected by centrifugal acceleration. If, as cited simulations suggest, ion ring beams relax into nonthermal velocity distributions with characteristic speed equal to the local ion-neutral flow speed, a generalized "Jeans escape" calculation shows that the escape flux of ionospheric O(+) increases with Poynting flux and with precipitating electron density in rough agreement with observations. C1 [Moore, T. E.; Khazanov, G. V.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Moore, TE (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Code 670, Greenbelt, MD 20771 USA. EM t.e.moore@nasa.gov RI Moore, Thomas/D-4675-2012; feggans, john/F-5370-2012 OI Moore, Thomas/0000-0002-3150-1137; FU NASA LWS TRT program [WBS 936723.02.01.03.82] FX The NASA LWS TRT program supported this work under WBS 936723.02.01.03.82. This work was inspired by the ideas of J.-P. St.-Maurice and discussions with Rickard Lundin. The authors thank Thomas Cravens, Pamela Puhl-Quinn, and Peter Gary for helpful discussions. Philip Isenberg and Martin Lee were especially helpful in understanding Alfven wave and ion cyclotron heating. The authors thank the reviewers of this and an earlier version of this paper submitted to Geophysical Research Letters, Mei-Ching Fok and Alex Glocer for critical readings of the manuscript. NR 49 TC 15 Z9 16 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 21 PY 2010 VL 115 AR A00J13 DI 10.1029/2009JA014905 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 699BQ UT WOS:000285639300001 ER PT J AU Pfaff, R Rowland, D Freudenreich, H Bromund, K Le, G Acuna, M Klenzing, J Liebrecht, C Martin, S Burke, WJ Maynard, NC Hunton, DE Roddy, PA Ballenthin, JO Wilson, GR AF Pfaff, R. Rowland, D. Freudenreich, H. Bromund, K. Le, G. Acuna, M. Klenzing, J. Liebrecht, C. Martin, S. Burke, W. J. Maynard, N. C. Hunton, D. E. Roddy, P. A. Ballenthin, J. O. Wilson, G. R. TI Observations of DC electric fields in the low-latitude ionosphere and their variations with local time, longitude, and plasma density during extreme solar minimum SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EQUATORIAL-SPREAD-F; VERTICAL ION DRIFTS; PREREVERSAL ENHANCEMENT; DISTURBANCE DYNAMO; ELECTRODYNAMICS; REGION; DEPENDENCE; SATELLITE; BUBBLES; DE-2 AB DC electric fields and associated E x B plasma drifts detected with the double-probe experiment on the C/NOFS satellite during extreme solar minimum conditions near the June 2008 solstice are shown to be highly variable, with weak to moderate ambient amplitudes of similar to 1-2 mV/m (similar to 25-50 m/s). Average field or drift patterns show similarities to those reported for more active solar conditions, i.e., eastward and outward during day and westward and inward at night. However, these patterns vary significantly with longitude and are not always present. Daytime vertical drifts near the magnetic equator are largest in the prenoon sector. Observations of weak to nonexistent prereversal enhancements in the vertical drifts near sunset are attributable to reduced dynamo activity during solar minimum as well as seasonal effects. Enhanced meridional drifts are observed near sunrise in certain longitude regions, precisely where the enhanced eastward flow that persisted from earlier local times terminates. The nightside ionosphere is characterized by larger-amplitude, structured electric fields dominated by horizontal scales of 500-1500 km even where local plasma densities appear relatively undisturbed. Data acquired during successive orbits indicate that plasma drifts and densities are persistently organized by longitude. The high duty cycle of the C/NOFS observations and its unique orbit promise to expose new physics of the low-latitude ionosphere. C1 [Pfaff, R.; Rowland, D.; Freudenreich, H.; Bromund, K.; Le, G.; Acuna, M.; Klenzing, J.; Liebrecht, C.; Martin, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hunton, D. E.; Roddy, P. A.; Ballenthin, J. O.; Wilson, G. R.] USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, Lincoln, MA 01731 USA. [Burke, W. J.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. [Maynard, N. C.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RP Pfaff, R (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM robert.f.pfaff@nasa.gov RI Le, Guan/C-9524-2012; Klenzing, Jeff/E-2406-2011; Rowland, Douglas/F-5589-2012; Pfaff, Robert/F-5703-2012 OI Le, Guan/0000-0002-9504-5214; Klenzing, Jeff/0000-0001-8321-6074; Rowland, Douglas/0000-0003-0948-6257; Pfaff, Robert/0000-0002-4881-9715 FU USAF Space Test Program FX The Communication/Navigation Outage Forecast System (C/NOFS) mission, conceived and developed by the Air Force Research Laboratory, is sponsored and executed by the USAF Space Test Program. NR 41 TC 44 Z9 44 U1 1 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 21 PY 2010 VL 115 AR A12324 DI 10.1029/2010JA016023 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 699BQ UT WOS:000285639300016 ER PT J AU Ostensen, RH Silvotti, R Charpinet, S Oreiro, R Handler, G Green, EM Bloemen, S Heber, U Gansicke, BT Marsh, TR Kurtz, DW Telting, JH Reed, MD Kawaler, SD Aerts, C Rodriguez-Lopez, C Vuckovic, M Ottosen, TA Liimets, T Quint, AC Van Grootel, V Randall, SK Gilliland, RL Kjeldsen, H Christensen-Dalsgaard, J Borucki, WJ Koch, D Quintana, EV AF Ostensen, R. H. Silvotti, R. Charpinet, S. Oreiro, R. Handler, G. Green, E. M. Bloemen, S. Heber, U. Gaensicke, B. T. Marsh, T. R. Kurtz, D. W. Telting, J. H. Reed, M. D. Kawaler, S. D. Aerts, C. Rodriguez-Lopez, C. Vuckovic, M. Ottosen, T. A. Liimets, T. Quint, A. C. Van Grootel, V. Randall, S. K. Gilliland, R. L. Kjeldsen, H. Christensen-Dalsgaard, J. Borucki, W. J. Koch, D. Quintana, E. V. TI First Kepler results on compact pulsators - I. Survey target selection and the first pulsators SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; binaries: close; stars: oscillations; subdwarfs; white dwarfs ID SUBDWARF-B-STARS; WHITE-DWARF STARS; ALL-SKY SURVEY; HUBBLE-SPACE-TELESCOPE; G-MODE OSCILLATIONS; SDB STARS; CATACLYSMIC VARIABLES; DRIVING MECHANISM; SPECTRAL-ANALYSIS; DATA RELEASE AB We present results from the first two quarters of a survey to search for pulsations in compact stellar objects with the Kepler spacecraft. The survey sample and the various methods applied in its compilation are described, and spectroscopic observations are presented to separate the objects into accurate classes. From the Kepler photometry we clearly identify nine compact pulsators and a number of interesting binary stars. Of the pulsators, one shows the strong, rapid pulsations typical of a V361 Hya-type sdB variable (sdBV); seven show long-period pulsation characteristics of V1093 Her-type sdBVs; and one shows low-amplitude pulsations with both short and long periods. We derive effective temperatures and surface gravities for all the subdwarf B stars in the sample and demonstrate that below the boundary region where hybrid sdB pulsators are found, all our targets are pulsating. For the stars hotter than this boundary temperature a low fraction of strong pulsators (< 10 per cent) is confirmed. Interestingly, the short-period pulsator also shows a low-amplitude mode in the long-period region, and several of the V1093 Her pulsators show low-amplitude modes in the short-period region, indicating that hybrid behaviour may be common in these stars, also outside the boundary temperature region where hybrid pulsators have hitherto been found. C1 [Ostensen, R. H.; Oreiro, R.; Bloemen, S.; Aerts, C.; Vuckovic, M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Silvotti, R.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Charpinet, S.; Rodriguez-Lopez, C.; Van Grootel, V.] Univ Toulouse, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Oreiro, R.] Inst Astrofis Andalucia, Granada 18008, Spain. [Handler, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Green, E. M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Heber, U.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Heber, U.] FAU Erlangen Nurnberg, Astron Inst, ECAP, D-96049 Bamberg, Germany. [Gaensicke, B. T.; Marsh, T. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England. [Telting, J. H.; Ottosen, T. A.; Liimets, T.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain. [Reed, M. D.; Quint, A. C.] Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA. [Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Aerts, C.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Rodriguez-Lopez, C.] Univ Vigo, Dept Fis Aplicada, Vigo 36310, Spain. [Vuckovic, M.; Kjeldsen, H.; Christensen-Dalsgaard, J.] European So Observ, Santiago 19, Chile. [Ottosen, T. A.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Liimets, T.] Tartu Observ, EE-61602 Toravere, Estonia. [Randall, S. K.] ESO, D-85748 Garching, Germany. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Quintana, E. V.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Ostensen, RH (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium. EM roy@ster.kuleuven.be RI Gaensicke, Boris/A-9421-2012; Heber, Ulrich/G-3306-2013; OI Gaensicke, Boris/0000-0002-2761-3005; Heber, Ulrich/0000-0001-7798-6769; Amby, Thomas Mellergaard/0000-0002-8116-1097; Silvotti, Roberto/0000-0002-1295-8174; Oreiro Rey, Raquel/0000-0002-4899-6199; Rodriguez-Lopez, Cristina/0000-0001-5559-7850; Charpinet, Stephane/0000-0002-6018-6180; Kawaler, Steven/0000-0002-6536-6367 FU NASA's Science Mission Directorate; European Research Council under the European Community [227224]; Research Council of K.U.Leuven [GOA/2008/04]; NASA FX The authors gratefully acknowledge the Kepler team and everybody who has contributed to making this mission possible. Funding for the Kepler Mission is provided by NASA's Science Mission Directorate.; The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No 227224 (PROSPERITY), as well as from the Research Council of K.U.Leuven grant agreement GOA/2008/04. ACQ is supported by the Missouri Space Grant Consortium, funded by NASA. NR 67 TC 72 Z9 72 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 21 PY 2010 VL 409 IS 4 BP 1470 EP 1486 DI 10.1111/j.1365-2966.2010.17366.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 689XI UT WOS:000284963800012 ER PT J AU Kawaler, SD Reed, MD Quint, AC Ostensen, RH Silvotti, R Baran, AS Charpinet, S Bloemen, S Kurtz, DW Telting, J Handler, G Kjeldsen, H Christensen-Dalsgaard, J Borucki, WJ Koch, DG AF Kawaler, S. D. Reed, M. D. Quint, A. C. Ostensen, R. H. Silvotti, R. Baran, A. S. Charpinet, S. Bloemen, S. Kurtz, D. W. Telting, J. Handler, G. Kjeldsen, H. Christensen-Dalsgaard, J. Borucki, W. J. Koch, D. G. TI First Kepler results on compact pulsators - II. KIC 010139564, a new pulsating subdwarf B (V361 Hya) star with an additional low-frequency mode SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: oscillations; subdwarfs; stars: variables: general ID STRUCTURAL PARAMETERS; FORMATION CHANNELS; SPECTRAL-ANALYSIS; SDB STARS; ASTEROSEISMOLOGY; HOT; FEIGE-48; OSCILLATIONS; PG-1219+534; PG-1325+101 AB We present the discovery of non-radial pulsations in a hot subdwarf B star based on 30.5 d of nearly continuous time series photometry using the Kepler spacecraft. KIC 010139564 is found to be a short-period pulsator of the V361 Hya (EC 14026) class with more than 10 independent pulsation modes whose periods range from 130 to 190 s. It also shows one periodicity at a period of 3165 s. If this periodicity is a high-order g-mode, then this star may be the hottest member of the hybrid DW Lyn stars. In addition to the resolved pulsation frequencies, additional periodic variations in the light curve suggest that a significant number of additional pulsation frequencies may be present. The long duration of the run, the extremely high duty cycle and the well-behaved noise properties allow us to explore the stability of the periodic variations, and to place strong constraints on how many of them are independent stellar oscillation modes. We find that most of the identified periodicities are indeed stable in phase and amplitude, suggesting a rotation period of 2-3 weeks for this star, but further observations are needed to confirm this suspicion. C1 [Kawaler, S. D.; Baran, A. S.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Reed, M. D.; Quint, A. C.] Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA. [Ostensen, R. H.; Bloemen, S.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Silvotti, R.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Baran, A. S.] Krakow Pedag Univ, PL-30084 Krakow, Poland. [Charpinet, S.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England. [Telting, J.] Nord Opt Telescope, Santa Cruze De La Palma 38700, Spain. [Handler, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kjeldsen, H.; Christensen-Dalsgaard, J.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark. [Borucki, W. J.; Koch, D. G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kawaler, SD (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. EM sdk@iastate.edu OI Silvotti, Roberto/0000-0002-1295-8174; Charpinet, Stephane/0000-0002-6018-6180; Kawaler, Steven/0000-0002-6536-6367 FU European Research Council under the European Community [227224]; Research Council of K.U. Leuven [GOA/2008/04]; NASA; Polish Ministry of Science [554/MOB/2009/0]; NASA's Science Mission Directorate FX For RHO and SB, the research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no227224 (PROSPERITY) and from the Research Council of K.U. Leuven (GOA/2008/04). ACQ is supported by the Missouri Space Grant Consortium, funded by NASA. AB acknowledges support from the Polish Ministry of Science (554/MOB/2009/0). Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The authors gratefully acknowledge the entire Kepler team, whose efforts have made these results possible. NR 48 TC 27 Z9 27 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 21 PY 2010 VL 409 IS 4 BP 1487 EP 1495 DI 10.1111/j.1365-2966.2010.17528.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 689XI UT WOS:000284963800013 ER PT J AU Reed, MD Kawaler, SD Ostensen, RH Bloemen, S Baran, A Telting, JH Silvotti, R Charpinet, S Quint, AC Handler, G Gilliland, RL Borucki, WJ Koch, DG Kjeldsen, H Christensen-Dalsgaard, J AF Reed, M. D. Kawaler, S. D. Ostensen, R. H. Bloemen, S. Baran, A. Telting, J. H. Silvotti, R. Charpinet, S. Quint, A. C. Handler, G. Gilliland, R. L. Borucki, W. J. Koch, D. G. Kjeldsen, H. Christensen-Dalsgaard, J. TI First Kepler results on compact pulsators - III. Subdwarf B stars with V1093 Her and hybrid (DW Lyn) type pulsations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: oscillations; subdwarfs ID G-MODE OSCILLATIONS; CLASS PROTOTYPE; HOT; ASTEROSEISMOLOGY; PARAMETERS; TELESCOPE; STABILITY AB We present the discovery of non-radial pulsations in five hot subdwarf B (sdB) stars based on 27 d of nearly continuous time series photometry using the Kepler spacecraft. We find that every sdB star cooler than approximate to 27 500 K that Kepler has observed (seven so far) is a long-period pulsator of the V1093 Her (PG 1716) class or a hybrid star with both short and long periods. The apparently non-binary long-period and hybrid pulsators are described here. The V1093 Her periods range from 1 to 4.5 h and are associated with g-mode pulsations. Three stars also exhibit short periods indicative of p-modes with periods of 2-5 min and in addition, these stars exhibit periodicities between both classes from 15 to 45 min. We detect the coolest and longest-period V1093 Her-type pulsator to date, KIC010670103 (T-eff approximate to 20 900 K, P-max approximate to 4.5 h) as well as a suspected hybrid pulsator, KIC002697388, which is extremely cool (T-eff approximate to 23 900 K) and for the first time hybrid pulsators which have larger g-mode amplitudes than p-mode ones. All of these pulsators are quite rich with many frequencies and we are able to apply asymptotic relationships to associate periodicities with modes for KIC010670103. Kepler data are particularly well suited for these studies as they are long duration, extremely high duty cycle observations with well-behaved noise properties. C1 [Reed, M. D.; Quint, A. C.] Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA. [Kawaler, S. D.; Baran, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Ostensen, R. H.; Bloemen, S.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Baran, A.] Krakow Pedag Univ, PL-30084 Krakow, Poland. [Telting, J. H.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain. [Silvotti, R.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Charpinet, S.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Handler, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Borucki, W. J.; Koch, D. G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kjeldsen, H.; Christensen-Dalsgaard, J.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. RP Reed, MD (reprint author), Missouri State Univ, Dept Phys Astron & Mat Sci, 901 S Natl, Springfield, MO 65897 USA. EM MikeReed@missouristate.edu OI Silvotti, Roberto/0000-0002-1295-8174; Charpinet, Stephane/0000-0002-6018-6180; Kawaler, Steven/0000-0002-6536-6367 FU NASA's Science Mission Directorate; NASA; European Research Council under the European Community [227224]; Research Council of K.U. Leuven [GOA/2008/04]; Polish Ministry [554/MOB/2009/0] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The authors gratefully acknowledge the entire Kepler team, whose efforts have made these results possible. ACQ is supported by the Missouri Space Grant Consortium, funded by NASA. The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no227224 (PROSPERITY) and from the Research Council of K.U. Leuven (GOA/2008/04). AB gratefully acknowledges support from the Polish Ministry under grant No. 554/MOB/2009/0. NR 35 TC 31 Z9 31 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 21 PY 2010 VL 409 IS 4 BP 1496 EP 1508 DI 10.1111/j.1365-2966.2010.17423.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 689XI UT WOS:000284963800014 ER PT J AU Kawaler, SD Reed, MD Ostensen, RH Bloemen, S Kurtz, DW Quint, AC Silvotti, R Baran, AS Green, EM Charpinet, S Telting, J Aerts, C Handler, G Kjeldsen, H Christensen-Dalsgaard, J Borucki, WJ Koch, DG AF Kawaler, S. D. Reed, M. D. Ostensen, R. H. Bloemen, S. Kurtz, D. W. Quint, A. C. Silvotti, R. Baran, A. S. Green, E. M. Charpinet, S. Telting, J. Aerts, C. Handler, G. Kjeldsen, H. Christensen-Dalsgaard, J. Borucki, W. J. Koch, D. G. TI First Kepler results on compact pulsators - V. Slowly pulsating subdwarf B stars in short-period binaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: binaries: close; stars: oscillations; subdwarfs; stars: variables: general ID WHOLE EARTH TELESCOPE; G-MODE OSCILLATIONS; ECLIPSING BINARY; ADIABATIC SURVEY; CLASS PROTOTYPE; TIDAL FRICTION; CLOSE BINARIES; PG 1336-018; ASTEROSEISMOLOGY; PARAMETERS AB The survey phase of the Kepler Mission includes a number of hot subdwarf B (sdB) stars to search for non-radial pulsations. We present our analysis of two sdB stars that are found to be g-mode pulsators of the V1093 Her class. These two stars also display the distinct irradiation effect typical of sdB stars with a close M-dwarf companion with orbital periods of less than half a day. Because the orbital period is so short, the stars should be in synchronous rotation, and if so, the rotation period should imprint itself on the multiplet structure of the pulsations. However, we do not find clear evidence for such rotational splitting. Though the stars do show some frequency spacings that are consistent with synchronous rotation, they also display multiplets with splittings that are much smaller. Longer-duration time series photometry will be needed to determine if those small splittings are in fact rotational splitting, or caused by slow amplitude or phase modulation. Further data should also improve the signal-to-noise ratio, perhaps revealing lower-amplitude periodicities that could confirm the expectation of synchronous rotation. The pulsation periods seen in these stars show period spacings that are suggestive of high-overtone g-mode pulsations. C1 [Kawaler, S. D.; Baran, A. S.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Reed, M. D.; Quint, A. C.] Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65897 USA. [Ostensen, R. H.; Bloemen, S.; Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England. [Silvotti, R.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Baran, A. S.] Krakow Pedag Univ, PL-30084 Krakow, Poland. [Green, E. M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Charpinet, S.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Telting, J.] Nord Opt Telescope, Santa Cruze De La Palma 38700, Spain. [Handler, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kjeldsen, H.; Christensen-Dalsgaard, J.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Borucki, W. J.; Koch, D. G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kawaler, SD (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. EM sdk@iastate.edu OI Silvotti, Roberto/0000-0002-1295-8174; Charpinet, Stephane/0000-0002-6018-6180; Kawaler, Steven/0000-0002-6536-6367 FU European Research Council under the European Community [227224]; Research Council of K.U. Leuven [GOA/2008/04]; NASA; Polish Ministry of Science [554/MOB/2009/0]; NASA's Science Mission Directorate FX For RO, CA, and SB, the research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no227224 (PROSPERITY) and from the Research Council of K.U. Leuven (GOA/2008/04). ACQ is supported by the Missouri Space Grant Consortium, funded by NASA. AB acknowledges support from the Polish Ministry of Science (554/MOB/2009/0). Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The authors gratefully acknowledge the entire Kepler team, whose efforts have made these results possible. NR 52 TC 28 Z9 28 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 21 PY 2010 VL 409 IS 4 BP 1509 EP 1517 DI 10.1111/j.1365-2966.2010.17475.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 689XI UT WOS:000284963800015 ER PT J AU Benko, JM Kolenberg, K Szabo, R Kurtz, DW Bryson, S Bregman, J Still, M Smolec, R Nuspl, J Nemec, JM Moskalik, P Kopacki, G Kollath, Z Guggenberger, E Di Criscienzo, M Christensen-Dalsgaard, J Kjeldsen, H Borucki, WJ Koch, D Jenkins, JM Van Cleve, JE AF Benko, J. M. Kolenberg, K. Szabo, R. Kurtz, D. W. Bryson, S. Bregman, J. Still, M. Smolec, R. Nuspl, J. Nemec, J. M. Moskalik, P. Kopacki, G. Kollath, Z. Guggenberger, E. Di Criscienzo, M. Christensen-Dalsgaard, J. Kjeldsen, H. Borucki, W. J. Koch, D. Jenkins, J. M. Van Cleve, J. E. TI Flavours of variability: 29 RR Lyrae stars observed with Kepler SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: oscillations; stars: variables: RR Lyrae ID NONRADIAL PULSATION; MODELS; KINEMATICS; CEPHEID; CATALOG; SCIENCE AB We present our analysis of Kepler observations of 29 RR Lyrae stars, based on 138 d of observation. We report precise pulsation periods for all stars. Nine of these stars had incorrect or unknown periods in the literature. 14 of the stars exhibit both amplitude and phase Blazhko modulations, with Blazhko periods ranging from 27.7 to more than 200 d. For V445 Lyr, a longer secondary variation is also observed in addition to its 53.2-d Blazhko period. The unprecedented precision of the Kepler photometry has led to the discovery of the the smallest modulations detected so far. Moreover, additional frequencies beyond the well-known harmonics and Blazhko multiplets have been found. These frequencies are located around the half-integer multiples of the main pulsation frequency for at least three stars. In four stars, these frequencies are close to the first and/or second overtone modes. The amplitudes of these periodicities seem to vary over the Blazhko cycle. V350 Lyr, a non-Blazhko star in our sample, is the first example of a double-mode RR Lyrae star that pulsates in its fundamental and second overtone modes. C1 [Benko, J. M.; Szabo, R.; Nuspl, J.; Kollath, Z.] Konkoly Observ Budapest, H-1525 Budapest, Hungary. [Kolenberg, K.; Smolec, R.; Guggenberger, E.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England. [Jenkins, J. M.; Van Cleve, J. E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada. [Moskalik, P.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Kopacki, G.] Uniwersytetu Wroclawskiego, Inst Astron, PL-51622 Wroclaw, Poland. [Di Criscienzo, M.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. RP Benko, JM (reprint author), Konkoly Observ Budapest, POB 67, H-1525 Budapest, Hungary. EM benko@konkoly.hu RI Smolec, Radoslaw/F-1435-2013; OI Smolec, Radoslaw/0000-0001-7217-4884; Szabo, Robert/0000-0002-3258-1909; Benko, Jozsef/0000-0003-3851-6603 FU NASA's Science Mission Directorate; National Office for Research and Technology through the Hungarian Space Office [URK09350]; Hungarian Academy of Sciences; Austrian FWF [T359, P19962] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. This project has been supported by the National Office for Research and Technology through the Hungarian Space Office Grant No. URK09350 and the 'Lendulet' programme of the Hungarian Academy of Sciences. KK acknowledges the support of Austrian FWF projects T359 and P19962. The authors gratefully acknowledge the entire Kepler team, whose outstanding efforts have made these results possible. NR 40 TC 56 Z9 57 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 21 PY 2010 VL 409 IS 4 BP 1585 EP 1593 DI 10.1111/j.1365-2966.2010.17401.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 689XI UT WOS:000284963800023 ER PT J AU Jones, T Ellis, R Jullo, E Richard, J AF Jones, Tucker Ellis, Richard Jullo, Eric Richard, Johan TI MEASUREMENT OF A METALLICITY GRADIENT IN A z=2 GALAXY: IMPLICATIONS FOR INSIDE-OUT ASSEMBLY HISTORIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: evolution; galaxies: high-redshift; gravitational lensing: strong ID STAR-FORMING GALAXIES; SIMILAR-TO 2; HIGH-REDSHIFT; LENSED GALAXIES; HII-REGIONS; MASS; GAS; ABUNDANCES; SPECTRA; SPECTROSCOPY AB We present near-infrared imaging spectroscopy of the strongly lensed z = 2.00 galaxy SDSS J120601.69+514227.8 ("the Clone arc"). Using OSIRIS on the Keck 2 telescope with laser guide star adaptive optics, we achieve resolved spectroscopy with 0.20 arcsec FWHM resolution in the diagnostic emission lines [O III], H alpha, and [N II]. The lensing magnification allows us to map the velocity and star formation from Ha emission at a physical resolution of similar or equal to 300 pc in the galaxy source plane. With an integrated star formation rate of similar or equal to 50 M-circle dot yr(-1), the galaxy is typical of sources similarly studied at this epoch. It is dispersion dominated with a velocity gradient of similar or equal to +/- 80 km s(-1) and average dispersion (sigma) over bar = 85 km s(-1); the dynamical mass is 2.4 x 10(10) M-circle dot within a half-light radius of 2.9 kpc. Robust detection of [N II] emission across the entire OSIRIS field of view enables us to trace the gas phase metallicity distribution with 500 pc resolution. We find a strong radial gradient in both the [N II]/H alpha and [O III]/H alpha ratios indicating a metallicity gradient of -0.27 +/- 0.05 dex kpc(-1) with central metallicity close to solar. We demonstrate that the gradient is seen independently in two multiple images. While the physical gradient is considerably steeper than that observed in local galaxies, in terms of the effective radius at that epoch, the gradient is similar. This suggests that subsequent growth occurs in an inside-out manner with the inner metallicity gradient diminished over time due to radial mixing and enrichment from star formation. C1 [Jones, Tucker; Ellis, Richard] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Jullo, Eric] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Richard, Johan] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England. RP Jones, T (reprint author), CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA. FU NPP; NASA; EU FX E.J. is supported by the NPP, administered by Oak Ridge Associated Universities through a contract with NASA. Part of this work was carried out at Jet Propulsion Laboratories, California Institute of Technology under a contract with NASA. J.R. acknowledges support from an EU-Marie Curie fellowship. We thank the referee for useful comments which improved this Letter. T.A.J. thanks Wal Sargent and Judy Cohen for helpful discussions. We thank the Keck Observatory staff for their assistance in obtaining these observations. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 36 TC 54 Z9 54 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 20 PY 2010 VL 725 IS 2 BP L176 EP L180 DI 10.1088/2041-8205/725/2/L176 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691AD UT WOS:000285051400014 ER PT J AU Tinto, M Alves, MED AF Tinto, Massimo da Silva Alves, Marcio Eduardo TI LISA sensitivities to gravitational waves from relativistic metric theories of gravity SO PHYSICAL REVIEW D LA English DT Article ID POLARIZATIONS AB The direct observation of gravitational waves will provide a unique tool for probing the dynamical properties of highly compact astrophysical objects, mapping ultrarelativistic regions of space-time, and testing Einstein's general theory of relativity. LISA (Laser Interferometer Space Antenna), a joint National Aeronautics and Space Administration and European Space Agency mission to be launched in the next decade, will perform these scientific tasks by detecting and studying low-frequency cosmic gravitational waves through their influence on the phases of six modulated laser beams exchanged between three remote spacecraft. By directly measuring the polarization components of the waves LISA will detect, we will be able to test Einstein's theory of relativity with good sensitivity. Since a gravitational wave signal predicted by the most general relativistic metric theory of gravity accounts for six polarization modes (the usual two Einstein's tensor polarizations as well as two vector and two scalar wave components), we have derived the LISA time-delay interferometric responses and estimated their sensitivities to vector- and scalar-type waves. We find that (i) at frequencies larger than roughly the inverse of the one-way light time (approximate to 6 x 10(-2) Hz), LISA is more than ten times sensitive to scalar-longitudinal and vector signals than to tensor and scalar-transverse waves, and (ii) in the low part of its frequency band is equally sensitive to tensor and vector waves and somewhat less sensitive to scalar signals. C1 [Tinto, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [da Silva Alves, Marcio Eduardo] Inst Nacl Pesquisas Espaciais, Div Astrofis, BR-12227010 Sao Jose Dos Campos, SP, Brazil. RP Tinto, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Massimo.Tinto@jpl.nasa.gov; alvesmes@unifei.edu.br FU PCI/CNPq/MCT [680.006/2009-5]; FAPESP [2006/56041-3]; National Aeronautics and Space Administration FX We would like to thank Odylio Aguiar and Mario Novello for their kind hospitality at their institutions while this research was first formulated, and for financial support. We also thank Frank B. Estabrook and John W. Armstrong for their constant encouragement during the development of this work. MESA would like to thank Jose C. N. de Araujo for his encouragement, and PCI/CNPq/MCT (Grant No. 680.006/2009-5) and FAPESP (Grant No. 2006/56041-3) for financial support. This research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 27 TC 17 Z9 17 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD DEC 20 PY 2010 VL 82 IS 12 AR 122003 DI 10.1103/PhysRevD.82.122003 PG 8 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 713NB UT WOS:000286743600002 ER PT J AU Hoegy, WR Grebowsky, JM AF Hoegy, Walter R. Grebowsky, Joseph M. TI Venus nightside ionospheric holes SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LOCATION; FIELD; FLOW AB Pioneer Venus Orbiter (PVO) measured the ionosphere and atmosphere of Venus for 13 years 10 months yielding a rich data set of archived data from a complement of instruments. One particularly striking feature seen was the occurrence of deep localized nightside ionization depletions commonly called holes. A number of theories have been put forth to explain their observed characteristics, but there is still no consensus on their source. A possibly related phenomenon in the Venus nightside ionosphere is the occurrence of "disappearing" or severely disturbed ionospheres characterized by deep, widespread plasma depletions in almost the entire nightside. This paper reexamines the holes and "disappearing ionospheres" and other characteristics of the nightside ionosphere during solar maximum using a more extensive database than earlier studies. The hole locations, occurrences, and dependencies on solar wind dynamic pressure (Psw) are analyzed, and a comparison is made with earlier studies. It is shown that there is no Psw threshold for holes to occur and at Psw values greater than similar to 9 nPa, hole occurrence decreases while the occurrence of severely disturbed orbits increases, suggesting that holes may evolve into severely disturbed orbits. Other characteristics of the nightside are shown to be influenced by solar wind pressure to varying degrees; for example, the density integrated along the orbit path below the ionopause, and the median density at low altitudes exhibit strong inverse correlation with Psw, while the peak density is nearly independent of Psw. C1 [Hoegy, Walter R.] Leelanau Res, Empire, MI 49630 USA. [Grebowsky, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hoegy, WR (reprint author), Leelanau Res, 13601 S Beaver Pond, Empire, MI 49630 USA. EM wrhoegy@gmail.com RI Grebowsky, Joseph/I-7185-2013 FU NASA GSFC [NNX09AH51G] FX The authors would like to thank the referees for helpful comments. This study was supported by grant NNX09AH51G from NASA GSFC. NR 20 TC 3 Z9 3 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 18 PY 2010 VL 115 AR A12322 DI 10.1029/2010JA015675 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696VQ UT WOS:000285469900003 ER PT J AU Meyer, K Platnick, S AF Meyer, Kerry Platnick, Steven TI Utilizing the MODIS 1.38 mu m channel for cirrus cloud optical thickness retrievals: Algorithm and retrieval uncertainties SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL THIN CIRRUS; BULK SCATTERING PROPERTIES; ICE CRYSTALS; PART II; MODELS; WATER; BAND; REFLECTANCE; TERRA AB The cloud products from the Moderate Resolution Imaging Spectroradiometers (MODIS) on Terra and Aqua have been widely used within the atmospheric research community. The retrieval algorithms, however, oftentimes have difficulty detecting and retrieving thin cirrus, due to sensitivities to surface reflectance. Conversely, the 1.38 mu m channel, located within a strong water vapor absorption band, is quite useful for detecting thin cirrus clouds since the signal from the surface can be blocked or substantially attenuated by the absorption of atmospheric water vapor below cirrus. This channel, however, suffers from nonnegligible attenuation due to the water vapor located above and within the cloud layer. Here we provide details of a new technique pairing the 1.38 mu m and 1.24 mu m channels to estimate the above/in-cloud water vapor attenuation and to subsequently retrieve thin cirrus optical thickness (tau) from attenuation-corrected 1.38 mu m reflectance measurements. In selected oceanic cases, this approach is found to increase cirrus retrievals by up to 38% over MOD06. For these cases, baseline 1.38 mu m retrieval uncertainties are estimated to be between 15 and 20% for moderately thick cirrus (tau > 1), with the largest error source being the unknown cloud effective particle radius, which is not retrieved with the described technique. Uncertainties increase to around 90% for the thinnest clouds (tau < 0.5) where instrument and surface uncertainties dominate. C1 [Meyer, Kerry; Platnick, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Meyer, Kerry] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Meyer, Kerry] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Meyer, K (reprint author), NASA, Goddard Space Flight Ctr, Code 613-2, Greenbelt, MD 20771 USA. EM kerry.meyer@nasa.gov RI Platnick, Steven/J-9982-2014; Meyer, Kerry/E-8095-2016 OI Platnick, Steven/0000-0003-3964-3567; Meyer, Kerry/0000-0001-5361-9200 FU NASA FX This research was supported by an appointment to the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA, at the Goddard Space Flight Center, and by MODIS science team funding from NASA. In addition, the authors wish to thank Zhibo Zhang for his generous assistance and many helpful suggestions during the course of this work and Tom Arnold for his development of and assistance with the MODIS imaging software. NR 41 TC 11 Z9 11 U1 2 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 DEC 18 PY 2010 VL 115 AR D24209 DI 10.1029/2010JD014872 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 696TC UT WOS:000285463300008 ER PT J AU Ohtani, S Korth, H Keika, K Zheng, Y Brandt, PC Mende, SB AF Ohtani, S. Korth, H. Keika, K. Zheng, Y. Brandt, P. C. Mende, S. B. TI Inductive electric fields in the inner magnetosphere during geomagnetically active periods SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID RING CURRENT; PLASMA SHEET; NEUTRAL ATOM; TAIL CURRENT; SOLAR-WIND; STORM; SUBSTORMS; PHASE; MAGNETOTAIL; DEPENDENCE AB The present study examines the characteristics of electric fields in the nightside inner magnetosphere during geomagnetically active periods. Electric field and magnetic field measurements made by the Cluster spacecraft on their perigee passes are used. The results are summarized as follows: (1) The duskward electric field component E-Y tends to be larger in the premidnight sector and off the equator, presumably corresponding to the more frequent occurrence of substorms and boundary layer crossings, respectively. (2) The occurrence distribution of E-Y is biased positively with an average of 0.6-0.8 mV/m, which reflects enhanced convection at active time. (3) The occurrence distribution of E-Y is also characterized by extending tails with a standard deviation larger than the twice the average. Although the occurrence ratio decreases sharply with increasing magnitude of E-Y, vertical bar E-Y vertical bar occasionally exceeds 5 mV/m. (4) The sign of E-Y is well organized by the change of magnetic field. When the local magnetic configuration becomes more dipolar, E-Y tends to be positive (duskward), whereas it tends to be negative (dawnward) when the configuration becomes more stretched. (5) As for strong electric fields, E-Y tends to be proportional to the change of the H magnetic component, and from the induction equation, the typical spatial scale of E-Y is estimated at 4.2 R-E. Results 4 and 5 strongly suggests that those strong electric fields are inductive. However, the corresponding process/phenomenon can be different from event to event. It is also suggested that substorm(-like) processes inside the ring current effectively intensify the ring current. C1 [Ohtani, S.; Korth, H.; Zheng, Y.; Brandt, P. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Keika, K.] New Jersey Inst Technol, Ctr Solar Terr Res, Newark, NJ 07102 USA. [Mende, S. B.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Zheng, Y.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ohtani, S (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM ohtani@jhuapl.edu RI Zheng, Yihua/D-7368-2012; Ohtani, Shinichi/E-3914-2016; Brandt, Pontus/N-1218-2016 OI Ohtani, Shinichi/0000-0002-9565-6840; Brandt, Pontus/0000-0002-4644-0306 FU NASA [NNX07AG07G, NNX09AF46G] FX The Cluster EFW data were provided by M. Andre through the Cluster Active Archive (CAA). We are most grateful to C. Cully for his kind advice for using the EFW data. The Cluster fluxgate magnetometer data were provided by E. Lucek through CAA. The Sym-H index was provided by T. Iyemori through the World Data Center for Geomagnetism, Kyoto. The ACE/MFI and Solar Wind Electron Proton Alpha Monitor data sets were provided by C. W. Smith and D. J. McComas, respectively, through NASA/CDAWeb. Work at Johns Hopkins University Applied Physics Laboratory was supported by NASA grants NNX07AG07G and NNX09AF46G. NR 40 TC 9 Z9 9 U1 1 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 DEC 18 PY 2010 VL 115 AR A00I14 DI 10.1029/2010JA015745 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696VQ UT WOS:000285469900004 ER PT J AU Peterson, H Bailey, M Hallett, J Beasley, W AF Peterson, Harold Bailey, Matthew Hallett, John Beasley, William TI Reply to comment by J. de Urquijo and F. J. Gordillo-Vazquez on "NOx production in laboratory discharges simulating blue jets and red sprites" SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Editorial Material C1 [Peterson, Harold] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Beasley, William] Univ Oklahoma, Sch Meteorol, Norman, OK 73072 USA. [Bailey, Matthew; Hallett, John] Desert Res Inst, Div Atmospher Sci, Reno, NV 89512 USA. RP Peterson, H (reprint author), NASA, George C Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM harold.peterson@nasa.gov NR 4 TC 2 Z9 2 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 DEC 17 PY 2010 VL 115 AR A12320 DI 10.1029/2010JA016040 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696VN UT WOS:000285469600005 ER PT J AU Andersen, MPS Andersen, VF Nielsen, OJ Sander, SP Wallington, TJ AF Andersen, Mads P. Sulbaek Andersen, Vibeke F. Nielsen, Ole J. Sander, Stanley P. Wallington, Timothy J. TI Atmospheric Chemistry of HCF2O(CF2CF2O)(x)CF2H (x=2-4): Kinetics and Mechanisms of the Chlorine-Atom-Initiated Oxidation SO CHEMPHYSCHEM LA English DT Article DE atmospheric chemistry; chlorine; kinetics; radical reactions; reaction mechanisms ID DEGRADATION MECHANISM; THERMAL-DECOMPOSITION; SELF-REACTION; OH RADICALS; GAS-PHASE; CL ATOMS; PRODUCTS; HCF2OCF2OCF2CF2OCF2H; PEROXYNITRATES; SPECTRUM AB Smog chamber/FTIR techniques were used to measure k(Cl+HCF2O(CF2CF2O)(x)CF2H)=(5.3 +/- 1.5) x 10(-17) cm(3) molecule(-1) s(-1) in 700 Torr of N-2/O-2 diluent at 296 +/- 1 K. The Cl-initiated atmospheric oxidation of HCF2O(CF2CF2O)(x)CF2H, x = 2,3 and 4, gave COF2 in molar yields of (593 +/- 41) %, (758 +/- 71)% and (939 +/- 73) %, respectively, with no other observable carbon-containing products (i.e., essentially complete conversion of the hydrofluoropolyethers into COF2). Quantitative infrared spectra for HCF2O(CF2CF2O)(x)CF2H (x=2-4) were recorded and used to estimate the radiative efficiencies of the title compounds (1.07, 1.33, and 1.36 Wm(-2)ppb(-1)). Global warming potentials (100 year time horizon) of 3870, 4730 and 5060 were estimated for HCF2O(CF2CF2O)(x)CF2H, x = 2, 3 and 4, respectively. The results are discussed with respect to the atmospheric chemistry and environmental impact of hydrofluoropolyethers. C1 [Andersen, Mads P. Sulbaek; Sander, Stanley P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wallington, Timothy J.] Ford Motor Co, Syst Analyt & Environm Sci Dept, Dearborn, MI 48121 USA. [Andersen, Vibeke F.; Nielsen, Ole J.] Univ Copenhagen, Dept Chem, DK-2100 Copenhagen, Denmark. RP Andersen, MPS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Stop 183-901, Pasadena, CA 91109 USA. EM mads@sulbaek.dk; twalling@ford.com RI Sulbaek Andersen, Mads/C-4708-2008; Nielsen, Ole/B-9988-2011 OI Sulbaek Andersen, Mads/0000-0002-7976-5852; Nielsen, Ole/0000-0002-0088-3937 FU Danish Natural Science Research Council; Villum Kann Rasmussen Foundation for the Copenhagen Center for Atmospheric Research (CCAR); National Aeronautics and Space Administration FX We thank John Owens (3M EMMD Fluids Laboratory) for providing high-purity samples of the HFPEs. O.J.N. and V. F. A. acknowledge financial support from the Danish Natural Science Research Council and the Villum Kann Rasmussen Foundation for the Copenhagen Center for Atmospheric Research (CCAR). This work was performed partly at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. M.P.S.A. is supported by an appointment to the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. NR 23 TC 1 Z9 1 U1 0 U2 13 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1439-4235 J9 CHEMPHYSCHEM JI ChemPhysChem PD DEC 17 PY 2010 VL 11 IS 18 SI SI BP 4035 EP 4041 DI 10.1002/cphc.201000438 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 693XG UT WOS:000285258100025 ER PT J AU Gurnett, DA Groene, JB Persoon, AM Menietti, JD Ye, SY Kurth, WS MacDowall, RJ Lecacheux, A AF Gurnett, D. A. Groene, J. B. Persoon, A. M. Menietti, J. D. Ye, S. -Y. Kurth, W. S. MacDowall, R. J. Lecacheux, A. TI The reversal of the rotational modulation rates of the north and south components of Saturn kilometric radiation near equinox SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID PLANETARY MAGNETIC-FIELDS; RADIO-EMISSION; PERIOD AB It has been known for many years that Saturn emits intense radio emissions at kilometer wavelengths and that this radiation is modulated by the rotation of the planet at a rate that varies slowly on time scales of years. Recently it has been shown that the radio emission consists of two components that have different rotational modulation rates, one emitted from the northern auroral region and the other emitted from the southern auroral region. In this paper we show using radio measurements from the Cassini spacecraft that the rotational modulation rates of the northern and southern components reversed near Saturn's recent equinox, which occurred on 11 August 2009. We show that a similar reversal was also observed by the Ulysses spacecraft near the previous equinox, which occurred on 19 November 1995. The solar control implied by these reversals has important implications on how Saturn's rotation is coupled into the magnetosphere. Citation: Gurnett, D. A., J. B. Groene, A. M. Persoon, J. D. Menietti, S.-Y. Ye, W. S. Kurth, R. J. MacDowall, and A. Lecacheux (2010), The reversal of the rotational modulation rates of the north and south components of Saturn kilometric radiation near equinox, Geophys. Res. Lett., 37, L24101, doi:10.1029/2010GL045796. C1 [Gurnett, D. A.; Groene, J. B.; Persoon, A. M.; Menietti, J. D.; Ye, S. -Y.; Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lecacheux, A.] Observ Paris, CNRS, UMR 8109, LEISA, F-92195 Meudon, France. RP Gurnett, DA (reprint author), Univ Iowa, Dept Phys & Astron, 203 Van Allen Hall, Iowa City, IA 52242 USA. EM donald-gurnett@uiowa.edu RI MacDowall, Robert/D-2773-2012; OI Kurth, William/0000-0002-5471-6202 FU NASA [1356500, 959515]; Centre National d'Studies Spatiale at Observatoire de Paris; Jet Propulsion Laboratory FX The research at the University of Iowa was supported by NASA through contracts 1356500 and 959515 with the Jet Propulsion Laboratory, and the research at Observatoire de Paris was supported by the Centre National d'Studies Spatiale. NR 24 TC 38 Z9 38 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 17 PY 2010 VL 37 AR L24101 DI 10.1029/2010GL045796 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 696SP UT WOS:000285462000005 ER PT J AU Field, RD Jones, DBA Brown, DP AF Field, Robert D. Jones, Dylan B. A. Brown, Derek P. TI Effects of postcondensation exchange on the isotopic composition of water in the atmosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; ASIAN MONSOON REGION; STABLE-ISOTOPES; TIBETAN PLATEAU; INTERANNUAL VARIABILITY; QUANTITATIVE-ANALYSIS; AIR-TEMPERATURE; CLOUD PROCESSES; SUMMER MONSOON; ICE CORES AB We conducted experiments with an atmospheric general circulation model to determine the effects of non-Rayleigh, postcondensation exchange (PCE) on the isotopic composition of water in the atmosphere. PCE was found to universally deplete vapor of heavy isotopes but had differential effects on the isotopic composition of precipitation. At low latitudes, local PCE with fresh vapor at the surface enriches precipitation in heavy isotopes, particularly during light rainfall. When rainfall is heavy, PCE tends to deplete vapor and precipitation of heavy isotopes via atmospheric moisture recycling, supporting recent interpretations of vapor isotope measurements from satellites, particularly over the Asian Monsoon region. In the extratropics, PCE causes local enrichment of precipitation, which is often entirely offset by upstream PCE depletion of the source vapor, resulting in a net depletion in local precipitation. The transition from net enrichment to net depletion is controlled by the transition from rain to snow-dominated precipitation. Surprisingly, this transition was also found to influence the temperature effect. In regions with a strong seasonal mix of rain and snow, such as Europe, the temperature effect appears to be controlled by PCE rather than Rayleigh depletion. C1 [Brown, Derek P.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Brown, Derek P.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Field, Robert D.; Jones, Dylan B. A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Field, RD (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM rf2426@columbia.edu RI Jones, Dylan/O-2475-2014 OI Jones, Dylan/0000-0002-1935-3725 FU Canadian Foundation for Climate and Atmospheric Sciences through the Polar Climate Stability Network; Natural Sciences and Engineering Research Council of Canada FX The authors thank Joe Galewsky for the vapor delta D measurements over Mauna Kea, John Worden for helpful comments, and Gavin Schmidt for guidance in using ModelE. This work was supported by the Canadian Foundation for Climate and Atmospheric Sciences through the Polar Climate Stability Network and by a graduate scholarship from the Natural Sciences and Engineering Research Council of Canada for R.F. NR 83 TC 35 Z9 35 U1 1 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 DEC 17 PY 2010 VL 115 AR D24305 DI 10.1029/2010JD014334 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 696TB UT WOS:000285463200003 ER PT J AU Jeong, MJ Li, ZQ AF Jeong, Myeong-Jae Li, Zhanqing TI Separating real and apparent effects of cloud, humidity, and dynamics on aerosol optical thickness near cloud edges SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPERATIONAL RAMAN LIDAR; MARINE BOUNDARY-LAYER; SOUTHERN GREAT-PLAINS; WATER-VAPOR; SIZE DISTRIBUTIONS; IN-SITU; OCEAN; RETRIEVALS; SCATTERING; PROFILES AB Aerosol optical thickness (AOT) is one of aerosol parameters that can be measured on a routine basis with reasonable accuracy from Sun-photometric observations at the surface. However, AOT-derived near clouds is fraught with various real effects and artifacts, posing a big challenge for studying aerosol and cloud interactions. Recently, several studies have reported correlations between AOT and cloud cover, pointing to potential cloud contamination and the aerosol humidification effect; however, not many quantitative assessments have been made. In this study, various potential causes of apparent correlations are investigated in order to separate the real effects from the artifacts, using well-maintained observations from the Aerosol Robotic Network, Total Sky Imager, airborne nephelometer, etc., over the Southern Great Plains site operated by the U.S. Department of Energy's Atmospheric Radiation Measurement Program. It was found that aerosol humidification effects can explain about one fourth of the correlation between the cloud cover and AOT. New particle genesis, cloud-processed particles, atmospheric dynamics, and aerosol indirect effects are likely to be contributing to as much as the remaining three fourth of the relationship between cloud cover and AOT. C1 [Jeong, Myeong-Jae] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Jeong, Myeong-Jae] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Li, Zhanqing] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Li, Zhanqing] Univ Maryland, ESSIC, College Pk, MD 20742 USA. [Li, Zhanqing] Nanjing Univ Informat Sci & Technol, Sch Atmospher Phys, Nanjing, Jiangsu, Peoples R China. RP Jeong, MJ (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM myeong-jae.jeong@nasa.gov RI Jeong, Myeong/B-8803-2008; Li, Zhanqing/F-4424-2010 OI Li, Zhanqing/0000-0001-6737-382X FU U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Climate Change Research Division; U.S. DOE [DE-FG02-01ER63166]; DOE/ARM [DEFG0208ER64571]; NASA [NNX08AH71G]; MOST [2008CB403706] FX The data used in this study were obtained from the Atmospheric Radiation Measurement (ARM) Program sponsored by the U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Climate Change Research Division. We thank Dr. Rick Wagener and Dr. Brent Holben for their effort in establishing and maintaining the "Cart_Site" and "CART_SITE" for the AERONET. We are also grateful to the National Oceanic and Atmospheric Administration (NOAA), Climate Monitoring and Diagnostics Laboratory (CMDL), Aerosols Group for providing In Situ Aerosol Profiles (IAP) data sets. We sincerely thank the anonymous reviewers for their careful and constructive comments. This work is supported by the U.S. DOE ARM program grant DE-FG02-01ER63166 managed by Dr. Wanda Ferrell. The study was funded by the DOE/ARM Program (DEFG0208ER64571), NASA Radiation Science Program (NNX08AH71G), and MOST's National Basic Research Program (2008CB403706). NR 47 TC 22 Z9 22 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 16 PY 2010 VL 115 AR D00K32 DI 10.1029/2009JD013547 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 696TA UT WOS:000285463100001 ER PT J AU El-Alaoui, M Ashour-Abdalla, M Richard, RL Goldstein, ML Weygand, JM Walker, RJ AF El-Alaoui, Mostafa Ashour-Abdalla, Maha Richard, Robert L. Goldstein, Melvyn L. Weygand, James M. Walker, Raymond J. TI Global magnetohydrodynamic simulation of reconnection and turbulence in the plasma sheet SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SELF-ORGANIZED CRITICALITY; KELVIN-HELMHOLTZ INSTABILITY; SOLAR-WIND TURBULENCE; LOCALIZED RECONNECTION; MAGNETIC RECONNECTION; ISOTROPIC TURBULENCE; SUBSTORM ONSET; MHD; FLUCTUATIONS; MAGNETOTAIL AB Plasma sheet turbulence is examined by using a global MHD simulation. The simulation used idealized purely southward interplanetary magnetic field (IMF) driving conditions to eliminate the effect of solar wind and IMF variations. The results were compared with spacecraft observations of turbulence by computing power spectral densities and probability distribution functions. The fluctuations in the simulation were found to have properties characteristic of turbulence. The MHD simulation exhibited nested vortices on multiple scales, with the largest scales associated with reconnection outflows and the diversion of high-speed flows in the near-Earth region. The importance of strong localized reconnection regions in the simulation for driving the largest scale fluctuations supports the idea it is the main process driving turbulence in the plasma sheet. Interplay between turbulence and the reconnection process is probably present. Scaling arguments show that the scale at which turbulence is dissipated is consistent with the resistivity in the model. C1 [El-Alaoui, Mostafa; Ashour-Abdalla, Maha; Richard, Robert L.; Weygand, James M.; Walker, Raymond J.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Ashour-Abdalla, Maha] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Lab Geospace Sci, Greenbelt, MD 20771 USA. [Walker, Raymond J.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP El-Alaoui, M (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, 405 Hilgard Ave, Los Angeles, CA 90095 USA. EM mostafa@igpp.ucla.edu RI Goldstein, Melvyn/B-1724-2008 FU NASA [NNX10AQ47G, NNX08AO48G, NNG06GI95G] FX Research at UCLA was supported by NASA grants NNX10AQ47G, NNX08AO48G, and NNG06GI95G. The computations were performed on NASA's Columbia supercomputer and on Kraken (a Cray XT5) at the National Institute for Computational Sciences. UCLA-IGPP publication 6479. NR 74 TC 15 Z9 15 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 16 PY 2010 VL 115 AR A12236 DI 10.1029/2010JA015653 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696VL UT WOS:000285469400002 ER PT J AU Cucinotta, FA Hu, SW Schwadron, NA Kozarev, K Townsend, LW Kim, MHY AF Cucinotta, Francis A. Hu, Shaowen Schwadron, Nathan A. Kozarev, K. Townsend, Lawrence W. Kim, Myung-Hee Y. TI Space radiation risk limits and Earth-Moon-Mars environmental models SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID SOLAR PARTICLE EVENTS; GALACTIC COSMIC-RAYS; CANCER-RISKS; EXPOSURE; ASTRONAUTS; EXPLORATION; MISSIONS AB We review NASA's short-term and career radiation limits for astronauts and methods for their application to future exploration missions outside of low Earth orbit. Career limits are intended to restrict late occurring health effects and include a 3% risk of exposure-induced death from cancer and new limits for central nervous system and heart disease risks. Short-term dose limits are used to prevent in-flight radiation sickness or death through restriction of the doses to the blood forming organs and to prevent clinically significant cataracts or skin damage through lens and skin dose limits, respectively. Large uncertainties exist in estimating the health risks of space radiation, chiefly the understanding of the radiobiology of heavy ions and dose rate and dose protraction effects, and the limitations in human epidemiology data. To protect against these uncertainties NASA estimates the 95% confidence in the cancer risk projection intervals as part of astronaut flight readiness assessments and mission design. Accurate organ dose and particle spectra models are needed to ensure astronauts stay below radiation limits and to support the goal of narrowing the uncertainties in risk projections. Methodologies for evaluation of space environments, radiation quality, and organ doses to evaluate limits are discussed, and current projections for lunar and Mars missions are described. C1 [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Hu, Shaowen; Kim, Myung-Hee Y.] USRA, Div Space Life Sci, Houston, TX 77058 USA. [Schwadron, Nathan A.; Kozarev, K.] Boston Univ, Dept Astron, Boston, MA 01760 USA. [Townsend, Lawrence W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM francis.a.cucinotta@nasa.gov; shaowen.hu-1@nasa.gov; nathanas@bu.edu; kamen@bu.edu; ltownsen@tennessee.edu; myung-hee.y.kim@nasa.gov OI Kim, Myung-Hee/0000-0001-5575-6858 FU NASA FX This work was supported by the NASA LWS EMMREM project and the NASA Space Radiation Program. We appreciate useful discussions with Walter Schimmerling related to this work. NR 36 TC 20 Z9 21 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD DEC 16 PY 2010 VL 8 AR S00E09 DI 10.1029/2010SW000572 PG 12 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 696XR UT WOS:000285475200001 ER PT J AU Zhang, H Sibeck, DG Zong, QG Gary, SP McFadden, JP Larson, D Glassmeier, KH Angelopoulos, V AF Zhang, H. Sibeck, D. G. Zong, Q. -G. Gary, S. P. McFadden, J. P. Larson, D. Glassmeier, K. -H. Angelopoulos, V. TI Time History of Events and Macroscale Interactions during Substorms observations of a series of hot flow anomaly events SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS BOW SHOCK; DIAMAGNETIC CAVITIES; HYBRID SIMULATION; SOLAR-WIND; ION-BEAM; UPSTREAM; PLASMA; INSTABILITIES; MAGNETOSHEATH; EVOLUTION AB A series of seven hot flow anomaly (HFA) events has been observed by the Time History of Events and Macroscale Interactions during Substorms (THEMIS) C spacecraft just upstream from the subsolar bow shock from 0100 to 1300 UT on 19 August 2008. Both young (no shocks at edges, two distinct ion populations) and mature (strong shocks at edges, a single hot ion population) HFAs have been observed. Further upstream, THEMIS B observed four proto-HFAs (density and magnetic field strength depletions, plasma heating but no flow deflections) which later developed into HFAs observed by THEMIS C. We present evidence indicating that electromagnetic right-hand resonant ion beam instabilities heat ions inside HFAs. Observations of small-amplitude perturbations (Delta B/B < 50%) consistent with the resonant ion beam instability in a proto-HFA, 30 s electromagnetic waves (Delta B/B similar to 1) in a young HFA, and magnetic pulsations in a mature HFA (Delta B/B similar to 4) indicate that they are at early, middle, and late (nonlinear) stages of the electromagnetic right-hand resonant ion beam instabilities. Both young and mature HFAs are associated with strong electromagnetic waves near the lower hybrid frequency (0.1-1 Hz). The lower hybrid waves are the likely source of the electron heating inside HFAs. THEMIS B observations of four proto-HFAs which later developed into HFAs observed by THEMIS C indicate that these four HFAs might extend beyond 14 R(E) upstream from the bow shock, while the other three HFAs may extend between 5 and 14 R(E) upstream from the bow shock. We present an example of an HFA that lies displaced toward the side of the tangential discontinuity with a quasi-parallel bow shock configuration rather than lying centered on the driving interplanetary magnetic field discontinuity. C1 [Zhang, H.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Zhang, H.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zong, Q. -G.] Univ Massachusetts, Ctr Atmospher Sci, Lowell, MA 01854 USA. [Gary, S. P.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [McFadden, J. P.; Larson, D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Glassmeier, K. -H.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany. [Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Dept Earth & Space Sci, Los Angeles, CA 90065 USA. RP Zhang, H (reprint author), Univ Alaska Fairbanks, Inst Geophys, 903 Koyukuk Dr,POB 757320, Fairbanks, AK 99775 USA. EM hzhang@gi.alaska.edu RI Sibeck, David/D-4424-2012 FU NSF [AGS-0963111] FX The first author thanks Nick Omidi for helpful discussions. This work is partly supported by NSF grant AGS-0963111. NR 37 TC 24 Z9 25 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 15 PY 2010 VL 115 AR A12235 DI 10.1029/2009JA015180 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696VK UT WOS:000285469300001 ER PT J AU Rossow, WB Zhang, YC AF Rossow, William B. Zhang, Yuanchong TI Evaluation of a Statistical Model of Cloud Vertical Structure Using Combined CloudSat and CALIPSO Cloud Layer Profiles SO JOURNAL OF CLIMATE LA English DT Article ID HIGH-LEVEL CLOUDS; UPPER-AIR OBSERVATIONS; DATA PRODUCTS; SAGE-II; ISCCP; SATELLITE; SURFACE; CIRCULATION; COMBINATION; RAWINSONDE AB A model of the three-dimensional distribution of clouds was developed from the statistics of cloud layer occurrence from the International Satellite Cloud Climatology Project (ISCCP) and the statistics of cloud vertical structure (CVS) from an analysis of radiosonde humidity profiles. The CVS model associates each cloud type, defined by cloud-top pressure of the topmost cloud layer and total column optical thickness, with a particular CVS. The advent of satellite cloud radar (CloudSat) and lidar [Cloud Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO)] measurements (together C&C) of CVS allows for a quantitative evaluation of this statistical model. The zonal monthly-mean cloud layer distribution from the ISCCP CVS agrees with that from C&C to within 10% (when normalized to the same total cloud amount). The largest differences are an overestimate of middle-level cloudiness in winter polar regions, an overestimate of cloud-top pressures of the highest-level clouds, especially in the tropics, and an underestimate of low-level cloud amounts over southern midlatitude oceans. A more severe test of the hypothesized relationship is made by comparing CVS for individual satellite pixels. The agreement of CVS is good for isolated low-level clouds and reasonably good when the uppermost cloud layer is a high-level cloud; however, the agreement is not good when the uppermost cloud layer is a middle-level cloud, even when ISCCP correctly locates cloud top. An improved CVS model combining C&C and ISCCP may require classification at spatial scales larger than individual satellite pixels. C1 [Rossow, William B.] CUNY City Coll, CREST, New York, NY 10031 USA. [Zhang, Yuanchong] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Zhang, Yuanchong] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. RP Rossow, WB (reprint author), CUNY City Coll, CREST, Steinman Hall T-107,140th St & Convent Ave, New York, NY 10031 USA. EM wbrossow@ccny.cuny.edu RI Rossow, William/F-3138-2015 FU NASA [NNXD7AT10G, NNDXD8AL79A] FX We thank Hajime Okamoto and Yuichiro Hagihara for their discussion of these results and their lidar analysis. We also acknowledge useful conversations with Kaori Sato, Jay Mace, and Dave Winker. This work was supported by the NASA CloudSat/CALIPSO program (H. Maring), NASA Grant NNXD7AT10G; and the NASA MEASURES program (M. Maiden), NASA Grant NNDXD8AL79A. NR 38 TC 15 Z9 15 U1 1 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD DEC 15 PY 2010 VL 23 IS 24 BP 6641 EP 6653 DI 10.1175/2010JCLI3734.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 710YS UT WOS:000286553500012 ER PT J AU Lemoine, FG Zelensky, NP Chinn, DS Pavlis, DE Rowlands, DD Beckley, BD Luthcke, SB Willis, P Ziebart, M Sibthorpe, A Boy, JP Luceri, V AF Lemoine, F. G. Zelensky, N. P. Chinn, D. S. Pavlis, D. E. Rowlands, D. D. Beckley, B. D. Luthcke, S. B. Willis, P. Ziebart, M. Sibthorpe, A. Boy, J. P. Luceri, V. TI Towards development of a consistent orbit series for TOPEX, Jason-1, and Jason-2 SO ADVANCES IN SPACE RESEARCH LA English DT Article DE SLR; DORIS; Precision orbit determination; Mean sea level; TOPEX; Jason ID TERRESTRIAL REFERENCE FRAME; GRAVITY-FIELD MODELS; RADIATION PRESSURE; GLOBAL OCEAN; TOPEX/POSEIDON; DORIS; GRACE; SERVICE; ASSIMILATION; SYSTEM AB The TOPEX/Poseidon, Jason-1 and Jason-2 set of altimeter data now provide a time series of synoptic observations of the ocean that span nearly 17 years from the launch of TOPEX in 1992. The analysis of the altimeter data including the use of altimetry to monitor the global change in mean sea level requires a stable, accurate, and consistent orbit reference over the entire time span. In this paper, we describe the recomputation of a time series of orbits that rely on a consistent set of reference frames and geophysical models. The recomputed orbits adhere to the IERS 2003 standards for ocean and earth tides, use updates to the ITRF2005 reference frame for both the SLR and DORIS stations, apply GRACE-derived models for modeling of the static and time-variable gravity, implement the University College London (UCL) radiation pressure model for Jason-1, use improved troposphere modeling for the DORIS data, and apply the GOT4.7 ocean tide model for both dynamical ocean tide modeling and for ocean loading. The new TOPEX orbits have a mean SLR fit of 1.79 cm compared to 2.21 cm for the MGDR-B orbits. These new TOPEX orbits agree radially with independent SLR/crossover orbits at 0.70 cm RMS, and the orbit accuracy is estimated at 1.5-2.0 cm RMS over the entire TOPEX time series. The recomputed Jason-1 orbits agree radially with the Jason-1 GDR-C orbits at 1.08 cm RMS. The GSFC SLR/DORIS dynamic and reduced-dynamic orbits for Jason-2 agree radially with independent orbits from the CNES and JPL at 0.70-1.06 cm RMS. Applying these new orbits, and using the latest altimeter corrections for TOPEX, Jason-1, and Jason-2 from September 1992 to May 2009, we find a global rate in mean sea level of 3.0 +/- 0.4 mm/yr. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Lemoine, F. G.; Zelensky, N. P.; Chinn, D. S.; Pavlis, D. E.; Rowlands, D. D.; Beckley, B. D.; Luthcke, S. B.; Boy, J. P.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Zelensky, N. P.; Chinn, D. S.; Pavlis, D. E.; Beckley, B. D.] SGT Inc, Greenbelt, MD 20770 USA. [Willis, P.] Inst Geog Natl, Direct Tech, F-94165 St Mande, France. [Willis, P.] Univ Paris 07, CNRS, IPGP, F-75013 Paris, France. [Ziebart, M.] UCL, Dept Civil Environm & Geomat Engn, London WC1E 6BT, England. [Sibthorpe, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boy, J. P.] CNRS UdS, EOST IPGS, UMR 7516, F-67084 Strasbourg, France. [Luceri, V.] Ctr Geodesia Spaziale G Colombo, E GEOS SPA, ASI CGS, I-75100 Matera, Italy. RP Lemoine, FG (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. EM Frank.G.Lemoine@nasa.gov RI Willis, Pascal/A-8046-2008; Rowlands, David/D-2751-2012; Luthcke, Scott/D-6283-2012; Lemoine, Frank/D-1215-2013; Sibthorpe, Ant/C-1940-2012; Boy, Jean-Paul/E-6677-2017 OI Willis, Pascal/0000-0002-3257-0679; Boy, Jean-Paul/0000-0003-0259-209X FU CNES (Centre National d'Etudes Spatiales); NERC (Natural Environment Research Council) [NE/C519138/1]; European Union [221753]; Ocean Surface Topography Science Team; IDS Program in Mean Sea Level FX We acknowledge the geodetic services, including the International Laser Ranging Service (ILRS) the International GNSS Service (IGS), and the International DORIS Service (IDS), without whose data, precise orbit determination for TOPEX, Jason-1 and Jason-2 would not be possible. Part of this work was supported by the CNES (Centre National d'Etudes Spatiales) using DORIS data. This is IPGP contribution 2645. A. Sibthorpe's contribution, supported by NERC (Natural Environment Research Council) Grant #NE/C519138/1, was performed while at University College London, UK. J.P. Boy was supported while in residence at the NASA Goddard Space Flight Center under a Marie-Curie International Fellowship (Contract 221753) from the European Union. The US National Aeronautics and Space Administration supported this work under the auspices of the Ocean Surface Topography Science Team and the IDS Program in Mean Sea Level. NR 79 TC 57 Z9 61 U1 1 U2 8 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 15 PY 2010 VL 46 IS 12 BP 1513 EP 1540 DI 10.1016/j.asr.2010.05.007 PG 28 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 692BB UT WOS:000285125400004 ER PT J AU Zelensky, NP Lemoine, FG Ziebart, M Sibthorpe, A Willis, P Beckley, BD Klosko, SM Chinn, DS Rowlands, DD Luthcke, SB Pavlis, DE Luceri, V AF Zelensky, Nikita P. Lemoine, Frank G. Ziebart, Marek Sibthorpe, Ant Willis, Pascal Beckley, Brian D. Klosko, Steven M. Chinn, Douglas S. Rowlands, David D. Luthcke, Scott B. Pavlis, Despina E. Luceri, Vincenza TI DORIS/SLR POD modeling improvements for Jason-1 and Jason-2 SO ADVANCES IN SPACE RESEARCH LA English DT Article DE SLR; DORIS; Precision orbit determination; Jason-1; Jason-2 ID PRECISION ORBIT DETERMINATION; TOPEX POSEIDON; TOPEX/POSEIDON; SPACECRAFT; PRESSURE; ASSIMILATION; PREDICTION; ITRF2005; SERVICE; FORCES AB The long-term stability and the precision of the satellite orbit is a critical component of the Jason-1 and Jason-2 (OSTM) Missions, providing the reference frame for ocean mapping using altimeter data. DORIS tracking in combination with SLR has provided orbits, which are both highly accurate and consistent across missions using the latest and most accurate POD models. These models include GRACE-derived static and time varying gravity fields and a refined Terrestrial Reference Frame based on SLR and DORIS data yielding a uniform station complement. Additional improvements have been achieved based on advances in modeling the satellite surface forces and the tropospheric path delay for DORIS measurements. This paper presents these model improvements for Jason-1 and Jason-2, including a description of DORIS sensitivity to error in tropospheric path delay. We show that the detailed University College London (UCL) radiation pressure model for Jason-1, which includes self-shadowing and thermal re-radiation, is superior to the use of a macromodel for radiation pressure surface force modeling. Improvements in SLR residuals are seen over all Beta-prime angles for both Jason-1 and Jason-2 using the UCL model, with the greatest improvement found over regimes of low Beta-prime where orbit Earth shadowing is maximum. The overall radial orbit improvement for Jason-1 using the UCL model is 3 mm RMS, as corroborated by the improvement in the independent altimeter crossover data. Special attention is paid to Jason-2 POD to assess improvements gained with the latest advances in DORIS receiver technology. Tests using SLR and altimeter crossover residuals suggest the Jason-2 reduced-dynamic DORIS-only, SLR/DORIS, and GPS orbits have all achieved 1-cm radial accuracy. Tests using independent SLR data acquired at high elevation show an average fit value of 1.02 cm for the DORIS-only and 0.94 cm for the GPS reduced-dynamic orbits. Orbit differences suggest that the largest remaining errors in the Jason-2 dynamic orbit solutions are due to radiation pressure mis-modeling and variations in the geopotential not captured in the GRACE-derived annual terms. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Zelensky, Nikita P.; Lemoine, Frank G.; Beckley, Brian D.; Klosko, Steven M.; Chinn, Douglas S.; Rowlands, David D.; Luthcke, Scott B.; Pavlis, Despina E.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Zelensky, Nikita P.; Beckley, Brian D.; Klosko, Steven M.; Chinn, Douglas S.; Pavlis, Despina E.] SGT Inc, Greenbelt, MD 20770 USA. [Ziebart, Marek] UCL, Dept Civil Environm & Geomat Engn, London WC1E 6BT, England. [Sibthorpe, Ant] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Willis, Pascal] Inst Geog Natl, Direct Tech, F-94165 St Mande, France. [Willis, Pascal] Univ Paris 07, CNRS, IPGP, F-75013 Paris, France. [Luceri, Vincenza] Ctr Geodesia Spaziale G Colombo, E GEOS SPA, ASI CGS, I-75100 Matera, Italy. RP Zelensky, NP (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. EM nzelensky@sgt-inc.com RI Willis, Pascal/A-8046-2008; Rowlands, David/D-2751-2012; Luthcke, Scott/D-6283-2012; NCEO, COMET+`/A-3443-2013; Lemoine, Frank/D-1215-2013; Sibthorpe, Ant/C-1940-2012 OI Willis, Pascal/0000-0002-3257-0679; FU US National Aeronautics and Space Administration under Ocean Surface Topography Science Team; IDS Program in Mean Sea Level; Centre National d'Etudes Spatiales (CNES); NERC (Natural Environment Research Council) [NE/C519138/1] FX This work is based on SLR, DORIS, and GPS observations of the Jason-1 and Jason-2 satellites. We acknowledge the International Laser Ranging Service (ILRS) the International GNSS Service (IGS), and the International DORIS Service (IDS), for providing such data. This work was supported by the US National Aeronautics and Space Administration under the auspices of the Ocean Surface Topography Science Team and the IDS Program in Mean Sea Level. Part of this work was supported by the Centre National d'Etudes Spatiales (CNES) using DORIS data. A. Sibthorpe's contribution, supported by NERC (Natural Environment Research Council) Grant #NE/C519138/1, was performed while at University College London, UK. This paper is IPGP contribution number 2565. The authors are grateful for the long standing collaboration with the OSTST POD Team members, CNES, JPL, and UT CSR. NR 73 TC 25 Z9 27 U1 1 U2 7 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 15 PY 2010 VL 46 IS 12 BP 1541 EP 1558 DI 10.1016/j.asr.2010.05.008 PG 18 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 692BB UT WOS:000285125400005 ER PT J AU Govind, R Lemoine, FG Valette, JJ Chinn, D Zelensky, N AF Govind, R. Lemoine, F. G. Valette, J. J. Chinn, D. Zelensky, N. TI DORIS geodesy: A dynamic determination of geocentre location SO ADVANCES IN SPACE RESEARCH LA English DT Article DE DORIS; Geodesy; Geocentre; SLR; Precise orbit determination ID SATELLITE; EARTH; SERVICE; MODEL; PRESSURE; ORBITS; MOTION; RANGE; GRACE; SLR AB Geoscience Australia contributed a multi-satellite, multi-year weekly time series to the International DORIS Service combined submission for the construction of International Terrestrial Reference Frame 2008 (ITRF2008). This contributing solution was extended to a study of the capability of DORIS to dynamically estimate the variation in the geocentre location. Two solutions, comprising different constraint configurations of the tracking network, were undertaken. The respective DORIS satellite orbit solutions (SPOT-2, SPOT-4, SPOT-5 and Envisat) were verified and validated by comparison with those produced at the Goddard Space Flight Center (GSFC), DORIS Analysis Centre, for computational consistency and standards. In addition, in the case of Envisat, the trajectories from the GA determined SLR and DORIS orbits were compared. The results for weekly dynamic geocentre estimates from the two constraint configurations were bench-marked against the geometric geocentre estimates from the IDS-2 combined solution. This established that DORIS is capable of determining the dynamic geocentre variation by estimating the degree one spherical harmonic coefficients of the Earth's gravity potential. It was established that constrained configurations produced similar results for the geocentre location and consequently similar annual amplitudes. For the minimally constrained configuration Greenbelt-Kitab, the mean of the uncertainties of the geocentre location were 2.3, 2.3 and 7.6 mm and RMS of the mean uncertainties were 1.9, 1.2 and 3.5 mm for the X, Y and Z components, respectively. For GA_IDS-2_Datum constrained configuration, the mean of the uncertainties of the geocentre location were 1.7, 1.7 and 6.2 mm and RMS of the mean uncertainties were 0.9, 0.7 and 2.9 mm for the X, Y and Z components, respectively. The mean of the differences of the two DORIS dynamic geocentre solutions with respect to the IDS-2 combination were 1.6, 4.0 and 5.1 mm with an RMS of the mean 21.2, 14.0 and 31.5 mm for the Greenbelt-Kitab configuration and 4.1, 3.9 and 4.3 mm with an RMS 8.1, 9.0 and 28.6 mm for the GA_IDS-2_Datum constraint configuration. The annual amplitudes for each component were estimated to be 5.3, 10.8 and 11.0 mm for the Greenbelt-Kitab configuration and 5.3, 9.3 and 9.4 mm for the GA_IDS-2_Datum constraint configuration. The two DORIS determined dynamic geocentre solutions were compared to the SLR determined dynamic solution (which was determined from the same process of the GA contribution to the ITRF2008 ILRS combination) gave mean differences of 3.3, -4.7 and 2.5 mm with an RMS of 20.7, 17.5 and 28.0 mm for the X, Y and Z components, respectively for the Greenbelt-Kitab configuration and 1.1, -5.4 and 4.4 mm with an RMS of 9.7, 13.3 and 24.9 mm for the GA_IDS-2_Datum configuration. The larger variability is reflected in the respective amplitudes. As a comparison, the annual amplitudes of the SLR determined dynamic geocentre are 0.9, 1.0 and 6.8 mm in the X, Y and Z components. The results from this study indicate that there is potential to achieve precise dynamically determined geocentre from DORIS. Crown copyright (C) 2010 Published by Elsevier Ltd. on behalf of COSPAR. All rights reserved. C1 [Govind, R.] Geosci Australia, Geospatial & Earth Monitoring Div, Canberra, ACT 2601, Australia. [Lemoine, F. G.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Valette, J. J.] Collecte Localisat Satellites, F-31520 Ramonville St Agne, France. [Chinn, D.; Zelensky, N.] SGT Inc, Greenbelt, MD 20770 USA. [Govind, R.] Univ New S Wales, Sch Surveying & Spatial Informat Syst, Sydney, NSW, Australia. RP Govind, R (reprint author), Geosci Australia, Geospatial & Earth Monitoring Div, GPO Box 378, Canberra, ACT 2601, Australia. EM Ramesh.Govind@ga.gov.au; Frank.Lemoine@gsfc.nasa.gov; Jean-Jacques.Valette@cls.fr RI Lemoine, Frank/D-1215-2013 NR 45 TC 1 Z9 1 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 DEC 15 PY 2010 VL 46 IS 12 BP 1593 EP 1605 DI 10.1016/j.asr.2010.08.025 PG 13 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 692BB UT WOS:000285125400009 ER PT J AU Valette, JJ Lemoine, FG Ferrage, P Yaya, P Altamimi, Z Willis, P Soudarin, L AF Valette, Jean-Jacques Lemoine, Frank G. Ferrage, Pascale Yaya, Philippe Altamimi, Zuheir Willis, Pascal Soudarin, Laurent TI IDS contribution to ITRF2008 SO ADVANCES IN SPACE RESEARCH LA English DT Article DE DORIS; Intra-technique combination; Terrestrial reference frame; Polar motion ID TERRESTRIAL REFERENCE FRAME; INTERNATIONAL DORIS SERVICE; PRECISE ORBIT DETERMINATION; GEODETIC OBSERVATORY PECNY; THERMOSPHERIC MODEL; JASON-1; SATELLITE; PRESSURE; NETWORK; ENVISAT AB For the first time, the International DORIS Service (IDS) has produced a technique level combination based on the contributions of seven analysis centers (ACs), including the European Space Operations Center (ESOC), Geodetic Observatory Pecny (GOP), Geoscience Australia (GAU), the NASA Goddard Space Flight Center (GSFC), the Institut Geographique National (IGN), the Institute of Astronomy, Russian Academy of Sciences (INASAN, named as INA), and CNES/CLS (named as LCA). The ACs used five different software packages to process the DORIS data from 1992 to 2008, including NAPEOS (ESA), Bernese (GOP), GEODYN (GAU, GSC), GIPSY/OASIS (INA), and GINS (LCA). The data from seven DORIS satellites, TOPEX/Poseidon, SPOT-2, SPOT-3, SPOT-4, SPOT-5, Envisat and Jason-1 were processed and all the analysis centers produced weekly SINEX files in either variance covariance or normal equation format. The processing by the analysis centers used the latest GRACE-derived gravity models, forward modelling of atmospheric gravity, updates to the radiation pressure modelling to improve the DORIS geocenter solutions, denser parameterization of empirically determined drag coefficients to improve station and EOP solutions, especially near the solar maximum in 2001-2002, updated troposphere mapping functions, and an ITRF2005-derived station set for orbit determination, DPOD2005. The CATREF software was used to process the weekly AC solutions, and produce three iterations of an IDS global weekly combination. Between the development of the initial solution IDS-1, and the final solution, IDS-3, the ACs improved their analysis strategies and submitted updated solutions to eliminate troposphere-derived biases in the solution scale, to reduce drag-related degradations in station positioning, and to refine the estimation strategy to improve the combination geocenter solution. An analysis of the frequency content of the individual AC geocenter and scale solutions was used as the basis to define the scale and geocenter of the IDS-3 combination. The final IDS-3 combination has an internal position consistency (WRMS) that is 15 to 20 mm before 2002 and 8 to 10 mm after 2002, when 4 or 5 satellites contribute to the weekly solutions. The final IDS-3 combination includes solutions for 130 DORIS stations on 67 different sites of which 35 have occupations over 16 years (1993.0-2009.0). The EOPs from the IDS-3 combination were compared with the IERS 05 C04 time series and the RMS agreement was 0.24 mas and 0.35 mas for the X and Y components of polar motion. The comparison to ITRF2005 in station position shows an agreement of 6 to 8 mm RMS in horizontal and 10.3 mm in height. The RMS comparison to ITRF2005 in station velocity is at 1.8 mm/year on the East component, to 1.2 mm/year in North component and 1.6 mm/year in height. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Valette, Jean-Jacques; Yaya, Philippe; Soudarin, Laurent] Collecte Localisat Satellites, F-31520 Ramonville St Agne, France. [Lemoine, Frank G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ferrage, Pascale] Ctr Natl Etud Spatiales, F-31401 Toulouse 9, France. [Altamimi, Zuheir] Inst Geog Natl, LAREG, F-77455 Champs Sur Marne, France. [Willis, Pascal] Inst Geog Natl, Direct Tech, F-94165 St Mande, France. [Willis, Pascal] Inst Phys Globe Paris, UFR STEP, F-75013 Paris, France. RP Valette, JJ (reprint author), Collecte Localisat Satellites, 8-10 Rue Hermes,Parc Technol Canal, F-31520 Ramonville St Agne, France. EM jvalette@cls.fr RI Altamimi, Zuheir/A-4168-2009; Willis, Pascal/A-8046-2008; Lemoine, Frank/D-1215-2013 OI Willis, Pascal/0000-0002-3257-0679; FU Centre National d'Etudes Spatiales (CNES); National Aeronautics and Space Administration FX We would like to thank all the Agencies who host a DORIS beacon around the world and all the IDS Analysis Centers for generating products for the International DORIS Service. Part of this work was supported by the Centre National d'Etudes Spatiales (CNES). It is based on observations with DORIS receivers carried on the TOPEX/Poseidon, SPOT-2, SPOT-3, SPOT-4, SPOT-5, Envisat, and Jason-1 satellites. Frank Lemoine, was supported by the National Aeronautics and Space Administration, under the program, "Interdisciplinary Studies in Mean Sea Level". This paper is IPGP contribution number 2615. NR 56 TC 28 Z9 28 U1 0 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 15 PY 2010 VL 46 IS 12 BP 1614 EP 1632 DI 10.1016/j.asr.2010.05.029 PG 19 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 692BB UT WOS:000285125400011 ER PT J AU Yu, ZH Liscinsky, DS Winstead, EL True, BS Timko, MT Bhargava, A Herndon, SC Miake-Lye, RC Anderson, BE AF Yu, Zhenhong Liscinsky, David S. Winstead, Edward L. True, Bruce S. Timko, Michael T. Bhargava, Anuj Herndon, Scott C. Miake-Lye, Richard C. Anderson, Bruce E. TI Characterization of Lubrication Oil Emissions from Aircraft Engines SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID AEROSOL MASS-SPECTROMETER; AIR-QUALITY; FIELD; PARTICLES; STABILITY; FUEL AB In this first ever study, particulate matter (PM) emitted from the lubrication system overboard breather vent for two different models of aircraft engines has been systematically characterized. Lubrication oil was confirmed as the predominant component of the emitted particulate matter based upon the characteristic mass spectrum of the pure oil. Total particulate mass and size distributions of the emitted oil are also investigated by several high-sensitivity aerosol characterization instruments. The emission index (El) of lubrication oil at engine idle is in the range of 2-12 mg kg(-1) and increases with engine power. The chemical composition of the oil droplets is essentially independent of engine thrust, suggesting that engine oil does not undergo thermally driven chemical transformations during the similar to 4 h test window. Volumetric mean diameter is around 250-350 nm for all engine power conditions with a slight power dependence. C1 [Yu, Zhenhong; Timko, Michael T.; Herndon, Scott C.; Miake-Lye, Richard C.] Aerodyne Res Inc, Billerica, MA 01821 USA. [Liscinsky, David S.; True, Bruce S.] United Technol Res Ctr, E Hartford, CT 06108 USA. [Winstead, Edward L.] Sci Syst & Applicat Inc, Hampton, VA 23681 USA. [Bhargava, Anuj] Pratt & Whitney, E Hartford, CT 06108 USA. [Anderson, Bruce E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Yu, ZH (reprint author), Aerodyne Res Inc, Billerica, MA 01821 USA. FU Department of Defense [W912HQ-08-C-0052 (WP-1625)] FX This study was financially supported by the Strategic Environmental Research and Development Program (SERDP) of Department of Defense Contract W912HQ-08-C-0052 (WP-1625). We thank Pratt & Whitney for providing engine test opportunities and invaluable information on engine performance. In particular the assistance of Eric Hoy, Phil Santoro, Steve Hunt, Larry Underwood, and Wayne Jordan at P&W is gratefully acknowledged. NR 24 TC 13 Z9 13 U1 1 U2 7 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD DEC 15 PY 2010 VL 44 IS 24 BP 9530 EP 9534 DI 10.1021/es102145z PG 5 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 694AK UT WOS:000285266900046 PM 21090602 ER PT J AU Usui, T Sanborn, M Wadhwa, M McSween, HY AF Usui, Tomohiro Sanborn, Matthew Wadhwa, Meenakshi McSween, Harry Y., Jr. TI Petrology and trace element geochemistry of Robert Massif 04261 and 04262 meteorites, the first examples of geochemically enriched lherzolitic shergottites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID RARE-EARTH-ELEMENTS; PHYRIC MARTIAN BASALTS; OXYGEN FUGACITY; MINERAL CHEMISTRY; ION MICROPROBE; UPPER-MANTLE; RB-SR; OLIVINE; PETROGENESIS; MARS AB Shergottites sampled two distinct geochemical reservoirs on Mars. Basaltic and olivine-phyric shergottites individually sampled both geochemically enriched and depleted reservoirs, whereas lherzolitic shergottites are previously known only to exhibit a relatively limited intermediate geochemical signature that may have resulted from the mixing of the two geochemical end-member reservoirs. Here we show that recently discovered shergottites Robert Massif (RBT) 04261 and RBT 04262 are the first examples of lherzolitic shergottites originating from the enriched reservoir. RBT 04261 and RBT 04262, initially identified as olivine-phyric shergottites, are actually lherzolitic shergottites. Both meteorites exhibit nearly identical textures and mineral compositions, suggesting that they should be paired. Each consists of two distinct textures: poikilitic and non-poikilitic. The poikilitic areas are composed of pyroxene oikocrysts enclosing olivine grains; all pyroxene oikocrysts have pigeonite cores mantled by augite. The non-poikilitic areas are composed of olivine, pyroxene, maskelynite and minor amounts of merrillite, chromite and ilmenite. Olivine and pyroxene show the lowest Mg-number, and maskelynite has the lowest anorthite component among the lherzolitic shergottites. Moreover, the modal abundances of maskelynite in these two meteorites are distinctly higher than the other lherzolitic shergottites. The rare earth element (REE) budgets of RBT 04261 and RBT 04262 are dominated by merrillite. The slightly light rare earth element (LREE)-enriched pattern of this mineral is similar to that of merrillite in the geochemically enriched basaltic shergottites Shergotty and Zagami, and unlike the LREE-depleted pattern of merrillite in the other lherzolitic shergottites. The REE patterns of both high- and low-Ca pyroxenes are also similar to those in Shergotty and Zagami. The REE pattern of a melt calculated to be in equilibrium with the core of a pyroxene oikocryst is parallel to that of the RBT 04262 whole-rock as well as whole-rock compositions of other geochemically enriched basaltic shergottites. These observations imply that RBT 04262 sampled an enriched and oxidized reservoir similar to that sampled by some of the basaltic shergottites and are consistent with an oxidizing condition for the formation of RBT 04262 (logfO(2) = QFM-1.6). The petrographic and geochemical observations presented here suggest that RBT 04261 and RBT 04262 represent the most evolved magma among the lherzolitic shergottites and that this magma originated from a geochemically enriched reservoir on Mars. Based on an evaluation of the relationship between petrographic, geochemical and chronological signatures for shergottites including RBT 04261 and RBT 04262, we propose that both geochemically enriched and depleted shergottites were ejected from the same launch site on Mars. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Usui, Tomohiro; McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA. [Sanborn, Matthew; Wadhwa, Meenakshi] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Usui, T (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code KR,2101 NASA Pkwy, Houston, TX 77058 USA. EM tomohiro.usui@nasa.gov RI Usui, Tomohiro/G-1204-2010; OI Usui, Tomohiro/0000-0002-4653-293X; Sanborn, Matthew/0000-0003-3218-1195 FU NASA [NNG06GG36G, NNX08AH22G] FX We thank A. Patchen for assistance with electron microprobe analyses. We are grateful to T. Mikouchi, J.A. Barrat and an anonymous reviewer for constructive reviews, and H. Nagahara for editorial handling. This research was supported in part by NASA Cosmochemistry Grants NNG06GG36G to H.Y.M. and NNX08AH22G to M.W. NR 60 TC 24 Z9 24 U1 1 U2 13 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 DEC 15 PY 2010 VL 74 IS 24 BP 7283 EP 7306 DI 10.1016/j.gca.2010.09.010 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 691JR UT WOS:000285076600021 ER PT J AU Shafer, JT Brandon, AD Lapen, TJ Righter, M Peslier, AH Beard, BL AF Shafer, J. T. Brandon, A. D. Lapen, T. J. Righter, M. Peslier, A. H. Beard, B. L. TI Trace element systematics and Sm-147-Nd-143 and Lu-176-Hf-176 ages of Larkman Nunatak 06319: Closed-system fractional crystallization of an enriched shergottite magma SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID HF ISOTOPE GEOCHEMISTRY; MANTLE-CRUST SYSTEM; MARTIAN METEORITE; SM-ND; DIFFERENTIATION HISTORY; SNC METEORITES; RB-SR; MARS; EVOLUTION; DAR-AL-GANI-476 AB Combined Sm-147-Nd-143 and Lu-176-Hf-176 chronology of the martian meteorite Larkman Nunatak (LAR) 06319 indicates an igneous crystallization age of 193 +/- 20 Ma (2 sigma weighted mean). The individual Sm-147-Nd-143 and Lu-176-Hf-176 internal isochron ages are 183 +/- 12 Ma and 197 +/- 29 Ma, respectively, and are concordant with two previously determined Sm-147-Nd-143 and Rb-87-Sr-87 internal isochron ages of 190 +/- 26 Ma and 207 +/- 14 Ma, respectively (Shih et al., 2009). With respect to the Sm-147-Nd-143 isotope systematics, maskelynite lies above the isochron defined by primary igneous phases and is therefore not in isotopic equilibrium with the other phases in the rock. Non-isochronous maskelynite is interpreted to result from shock-induced reaction between plagioclase and partial melts of pyroxene and phosphate during transformation to maskelynite, which resulted in it having unsupported Nd-143 relative to its measured Sm-147/Nd-144 ratio. The rare earth element (REE) and high field strength element (HFSE) compositions of major constituent minerals can be modeled as the result of progressive crystallization of a single magma with no addition of secondary components. The concordant ages, combined with igneous textures, mineralogy, and trace clement systematics indicate that the weighted average of the radiometric ages records the true crystallization age of this rock. The young igneous age for LAR 06319 and other shergottites are in conflict with models that advocate for circa 4.1 Ga crystallization ages of shergottites from Pb isotope compositions, however, they are consistent with updated crater counting statistics indicating that young volcanic activity on Mars is more widespread than previously realized (Neukum et al., 2010). (C) 2010 Elsevier Ltd. All rights reserved. C1 [Shafer, J. T.; Brandon, A. D.; Lapen, T. J.; Righter, M.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. [Shafer, J. T.] Lunar & Planetary Inst, Houston, TX 77059 USA. [Brandon, A. D.] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Peslier, A. H.] Jacobs Technol, ESCG, Houston, TX 77058 USA. [Beard, B. L.] NASA, Astrobiol Inst, Houston, TX 77058 USA. RP Shafer, JT (reprint author), Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. EM jtshafer@uh.edu RI Peslier, Anne/F-3956-2010 FU Lunar and Planetary Institute; NASA; University of Houston Institute for Space System Operations FX J.S. was supported on a Lunar and Planetary Institute post-doctoral fellowship during the analytical phase of this work. A.D.B. and T.L.J. acknowledge support for their respective NASA Cosmochemistry awards. T.J.L. also acknowledges the University of Houston Institute for Space System Operations for partially supporting the analytical campaign at UW-Madison. NASA and the Antarctic Meteorite Working Group are thanked for providing the sample of LAR 06319 examined in this study. We thank reviewers James Day, Audrey Bouvier, and an anonymous reviewer for constructive and helpful reviews and editor Richard Walker for his efficient editorial handling of the manuscript. NR 60 TC 30 Z9 30 U1 1 U2 20 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 DEC 15 PY 2010 VL 74 IS 24 BP 7307 EP 7328 DI 10.1016/j.gca.2010.09.009 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 691JR UT WOS:000285076600022 ER PT J AU Gunapala, SD Ting, DZ Hill, CJ Nguyen, J Soibel, A Rafol, SB Keo, SA Mumolo, JM Lee, MC Liu, JK Yang, B AF Gunapala, S. D. Ting, D. Z. Hill, C. J. Nguyen, J. Soibel, A. Rafol, S. B. Keo, S. A. Mumolo, J. M. Lee, M. C. Liu, J. K. Yang, B. TI Demonstration of a 1024 x 1024 Pixel InAs-GaSb Superlattice Focal Plane Array SO IEEE PHOTONICS TECHNOLOGY LETTERS LA English DT Article DE Infrared detectors; infrared imaging; quantum-well devices AB We describe the demonstration of a 1024 x 1024 pixel long-wavelength infrared focal plane array based on an InAs-GaSb superlattice absorber surrounded by an electron-blocking and a hole-blocking unipolar barrier. An 11.5-mu m cutoff focal plane without antireflection coating based on this complementary barrier infrared detector design has yielded noise equivalent differential temperature of 53 mK at operating temperature of 80 K, with 300 K background and f/2 cold-stop. C1 [Gunapala, S. D.; Ting, D. Z.; Hill, C. J.; Nguyen, J.; Soibel, A.; Rafol, S. B.; Keo, S. A.; Mumolo, J. M.; Lee, M. C.; Liu, J. K.; Yang, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gunapala, SD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Soibel, Alexander/A-1313-2007 FU National Aeronautics and Space Administration; Missile Defense Agency FX The research described in this letter was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work was supported by the Missile Defense Agency. NR 6 TC 27 Z9 27 U1 2 U2 16 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1041-1135 J9 IEEE PHOTONIC TECH L JI IEEE Photonics Technol. Lett. PD DEC 15 PY 2010 VL 22 IS 24 BP 1856 EP 1858 DI 10.1109/LPT.2010.2089677 PG 3 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 691AG UT WOS:000285051700010 ER PT J AU Oleson, TA Sahai, N AF Oleson, Timothy A. Sahai, Nita TI Interaction energies between oxide surfaces and multiple phosphatidylcholine bilayers from extended-DLVO theory SO JOURNAL OF COLLOID AND INTERFACE SCIENCE LA English DT Article DE Supported phospholipid bilayer; Dipalmitoylphosphatidylcholine; Oxide; Silica; Alumina; Multiple bilayers; Interaction energy; Kinetics ID SUPPORTED LIPID-BILAYERS; ATOMIC-FORCE MICROSCOPY; VESICLE ADSORPTION; NEUTRON REFLECTIVITY; HAMAKER CONSTANTS; DISPERSION FORCES; WAALS INTERACTION; WATER-STRUCTURE; MEMBRANES; TEMPERATURE AB Interaction energies between dipalmitoylphosphandylcholine (DPPC) Mayers and corundum (alpha-Al(2)O(3)) or quartz (alpha-SiO(2)) are calculated according to extended Derjaguin-Landau-Verwey-Overbeek (DLVO) theory in order to examine oxide dependent multiple bilayer adsorption Energies are investigated at two ionic strengths (I=17 or 217 mM) and compared to corresponding DPPC adsorption experiments on corundum and quartz particles The repulsive hydration interaction diminishes sharply with separation distance and beyond similar to 3 nm the interaction energy is determined by the electrostatic and van der Waals contributions only We revise the electrostatic interaction to account for solution exclusion by the Mayers extending the distance over which this interaction occurs Calculated oxide-bilayer interaction energies explain our experimentally-observed adsorption of three bilayers on corundum compared to two on quartz at low I and only two bilayers on both oxides at high I The results are consistent with our hypothesis that electric double layer extension at low I allows oxide-bilayer electrostatic interactions to contribute to deposition of DPPC bilayers at large (similar to 14 nm) separations Theoretically predicted pseudo infinite supported bilayer stacks formed from vesicles are not observed experimentally due to kinetic considerations Potential relevance to biomedical applications and to the role of mineral surfaces in proto cell membrane self assembly is discussed (C) 2010 Elsevier Inc All rights reserved C1 [Oleson, Timothy A.; Sahai, Nita] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Sahai, Nita] Univ Wisconsin, Environm Chem & Technol Program, Madison, WI 53706 USA. [Sahai, Nita] Univ Wisconsin, Mat Sci Program, Madison, WI 53706 USA. [Sahai, Nita] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA. RP Sahai, N (reprint author), Univ Wisconsin, Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA. FU NS NSF [EAR 0346889]; American Chemical Society [41777-AC2]; NASA Astrobiology Institute (NAI); Wisconsin Alumni Research Foundation (WARF); Department of Geoscience University of Wisconsin - Madison; American Association of Petroleum Geologists (AAPG) FX The authors thank Qiang Cui (University of Wisconsin - Madison) for helpful discussion of this work This work was funded by the following grants to NS NSF Career Award (EAR 0346889) American Chemical Society Petroleum Research Fund (41777-AC2) NASA Astrobiology Institute (NAI) and a Wisconsin Alumni Research Foundation (WARF) Award TAO was supported by the Van Hise Graduate Fellowship through the Department of Geoscience University of Wisconsin - Madison as well as a Graduate Grant-In-Aid of Research from the American Association of Petroleum Geologists (AAPG) NR 68 TC 15 Z9 15 U1 2 U2 24 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9797 J9 J COLLOID INTERF SCI JI J. Colloid Interface Sci. PD DEC 15 PY 2010 VL 352 IS 2 BP 316 EP 326 DI 10.1016/j.jcis.2010.08.056 PG 11 WC Chemistry, Physical SC Chemistry GA 679SC UT WOS:000284180100014 PM 20869066 ER PT J AU Oleson, TA Sahai, N Pedersen, JA AF Oleson, Timothy A. Sahai, Nita Pedersen, Joel A. TI Electrostatic effects on deposition of multiple phospholipid bilayers at oxide surfaces SO JOURNAL OF COLLOID AND INTERFACE SCIENCE LA English DT Article DE Supported phospholipid bilayer; Dipalmitoylphosphatidylcholine; Oxide; Silica; Alumina; Multiple bilayers; Adsorption; Isotherm ID SUPPORTED LIPID-BILAYERS; MOLECULAR-DYNAMICS SIMULATION; ATOMIC-FORCE MICROSCOPE; VESICLE ADSORPTION; TITANIUM-DIOXIDE; DIVALENT-CATIONS; ELECTRIC-FIELD; ASYMMETRIC DISTRIBUTION; PHOSPHATIDYL SERINE; MEDICAL MINERALOGY AB We investigated electrostatic effects on the formation of multiple supported phospholipid bilayers (SPB) by varying the oxide substrate ionic strength the presence of divalent Ca-2 and phospholipid (PL) headgroup charge Whereas the current understanding of processes and forces controlling SPB formation is based primarily on studies involving planar substrates we report results from experiments using aqueous suspensions of quartz (alpha-SiO2) and corundum (alpha-Al2O3) particles Using fluorescent dye-loaded dipalmitoylphosphatidylcholine (DPPC) vesicles we determined that the vesicles underwent oxide particle-induced rupture and formed supported planar Mayers rather than a supported vesicle layer Adsorption Isotherms of DPPC at pH 7 2 in solutions of varying ionic strength set by NaCl and with or with out 2 mM Ca2+ support our hypotheses that van der Waals forces predominantly account for two DPPC Mayers and that adsorption beyond the second bilayer occurs at low ionic strength due to extension of the electric double-layer near the oxide surface In contrast adsorption isotherms of anionic dipalmitoylphosphatidylserine (DPPS) and cationic dipalmitoylethylphosphatidylcholine (DPEPC) show that adsorption of highly charged bilayers is decreased or prevented altogether due to bilayer-oxide and/or bilayer-bilayer repulsion Results have potential implications for biomedical industrial and environmental remediation applications involving SPBs and for proto-cell stability in origin of-life hypotheses (C) 2010 Elsevier Inc All rights reserved C1 [Oleson, Timothy A.; Sahai, Nita] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Sahai, Nita; Pedersen, Joel A.] Univ Wisconsin, Environm Chem & Technol Program, Madison, WI 53706 USA. [Sahai, Nita] Univ Wisconsin, Mat Sci Program, Madison, WI 53706 USA. [Sahai, Nita] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA. [Pedersen, Joel A.] Univ Wisconsin, Dept Soil Sci, Madison, WI 53706 USA. RP Sahai, N (reprint author), Univ Wisconsin, Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA. FU NS NSF [EAR 0346889]; American Chemical Society [41777-AC2]; Wisconsin Alumni Research Foundation (WARF); Department of Geoscience University of Wisconsin-Madison; American Association of Petroleum Geologists (AAPG) FX We acknowledge and thank Profs Judith Burstyn and Eric Roden (University of Wisconsin-Madison) for use of the spectrofluorimeter and UV-vis spectrophotometer respectively We also thank Professor Jim Weisshaar Tingting Wang and Jamie Ellis (University of Wisconsin-Madison) for helpful consultation regarding planning and execution of our fluorescence experiments Min-U-Sil 5 quartz particles were generously donated by U S Silica This work was funded by the following grants to NS NSF Career Award (EAR 0346889) American Chemical Society Petroleum Research Fund (41777-AC2) and a Wisconsin Alumni Research Foundation (WARF) Award TAO was supported by the Van Hise Graduate Fellowship through the Department of Geoscience University of Wisconsin-Madison as well as a Graduate Grant-in-Aid of Research from the American Association of Petroleum Geologists (AAPG) NR 123 TC 15 Z9 15 U1 5 U2 31 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9797 J9 J COLLOID INTERF SCI JI J. Colloid Interface Sci. PD DEC 15 PY 2010 VL 352 IS 2 BP 327 EP 336 DI 10.1016/j.jcis.2010.08.057 PG 10 WC Chemistry, Physical SC Chemistry GA 679SC UT WOS:000284180100015 PM 20869065 ER PT J AU Navarro-Gonzalez, R Vargas, E de la Rosa, J Raga, AC McKay, CP AF Navarro-Gonzalez, Rafael Vargas, Edgar de la Rosa, Jose Raga, Alejandro C. McKay, Christopher P. TI Reanalysis of the Viking results suggests perchlorate and organics at midlatitudes on Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID X-RAY SPECTROMETER; CHEMICAL-COMPOSITION; GAS CHROMATOGRAPHY; HYDROGEN-PEROXIDE; PATHFINDER SITE; SURFACE SAMPLES; ATACAMA DESERT; SOILS; ROCKS; CHEMISTRY AB The most comprehensive search for organics in the Martian soil was performed by the Viking Landers. Martian soil was subjected to a thermal volatilization process to vaporize and break organic molecules, and the resultant gases and volatiles were analyzed by gas chromatography-mass spectrometry. Only water at 0.1-1.0 wt% was detected, with traces of chloromethane at 15 ppb, at Viking landing site 1, and water at 0.05-1.0 wt% and carbon dioxide at 50-700 ppm, with traces of dichloromethane at 0.04-40 ppb, at Viking landing site 2. These chlorohydrocarbons were considered to be terrestrial contaminants, although they had not been detected at those levels in the blank runs. Recently, perchlorate was discovered in the Martian Arctic soil by the Phoenix Lander. Here we show that when Mars-like soils from the Atacama Desert containing 32 +/- 6 ppm of organic carbon are mixed with 1 wt% magnesium perchlorate and heated, nearly all the organics present are decomposed to water and carbon dioxide, but a small amount is chlorinated, forming 1.6 ppm of chloromethane and 0.02 ppm of dichloromethane at 500 C. A chemical kinetics model was developed to predict the degree of oxidation and chlorination of organics in the Viking oven. Reinterpretation of the Viking results therefore suggests <= 0.1% perchlorate and 1.5-6.5 ppm organic carbon at landing site 1 and <= 0.1% perchlorate and 0.7-2.6 ppm organic carbon at landing site 2. The detection of organics on Mars is important to assess locations for future experiments to detect life itself. C1 [Navarro-Gonzalez, Rafael; Vargas, Edgar; de la Rosa, Jose; Raga, Alejandro C.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Mexico City 04510, DF, Mexico. [McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Navarro-Gonzalez, R (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Lab Quim Plasmas & Estudios Planetarios, Ciudad Univ,Apartado Postal 70-543, Mexico City 04510, DF, Mexico. EM navarro@nucleares.unam.mx RI Gonzalez, Rafael/D-1748-2009 FU National Autonomous University of Mexico (DGAPA) [IN-107107, IN-109110]; National Council of Science and Technology of Mexico (CONACyT) [45810-F, 98466]; National Aeronautics and Space Administration FX This research was supported by grants from the National Autonomous University of Mexico (DGAPA IN-107107 and IN-109110) and the National Council of Science and Technology of Mexico (CONACyT 45810-F and 98466) and by the National Aeronautics and Space Administration ASTEP program. NR 46 TC 100 Z9 101 U1 6 U2 62 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 15 PY 2010 VL 115 AR E12010 DI 10.1029/2010JE003599 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 696UF UT WOS:000285466200001 ER PT J AU Buzulukova, N Fok, MC Goldstein, J Valek, P McComas, DJ Brandt, PC AF Buzulukova, N. Fok, M. -C. Goldstein, J. Valek, P. McComas, D. J. Brandt, P. C. TI Ring current dynamics in moderate and strong storms: Comparative analysis of TWINS and IMAGE/HENA data with the Comprehensive Ring Current Model SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID RICE CONVECTION MODEL; MAGNETIC-FIELD; ELECTRIC-FIELDS; INNER MAGNETOSPHERE; LARGE-SCALE; JUNE 4-6; ART.; SHEET; IONOSPHERE; ELECTRODYNAMICS AB We present a comparative study of ring current dynamics during strong and moderate storms. The ring current during the strong storm is studied with IMAGE/HENA data near the solar cycle maximum in 2000. The ring current during the moderate storm is studied using energetic neutral atom (ENA) data from the Two Wide-Angle Imaging Neutral-Atom Spectrometers (TWINS) mission during the solar minimum in 2008. For both storms, the local time distributions of ENA emissions show signatures of postmidnight enhancement (PME) during the main phases. To model the ring current and ENA emissions, we use the Comprehensive Ring Current Model (CRCM). CRCM results show that the main-phase ring current pressure peaks in the premidnight-dusk sector, while the most intense CRCM-simulated ENA emissions show PME signatures. We analyze two factors to explain this difference: the dependence of charge-exchange cross section on energy and pitch angle distributions of ring current. We find that the IMF B-y effect (twisting of the convection pattern due to B-y) is not needed to form the PME. Additionally, the PME is more pronounced for the strong storm, although relative shielding and hence electric field skewing is well developed for both events. C1 [Buzulukova, N.; Fok, M. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Goldstein, J.; Valek, P.; McComas, D. J.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78228 USA. [Goldstein, J.; Valek, P.; McComas, D. J.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA. [Brandt, P. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Buzulukova, N (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 673,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM nbuzulukova@gmail.com RI Fok, Mei-Ching/D-1626-2012; Brandt, Pontus/N-1218-2016; OI Brandt, Pontus/0000-0002-4644-0306; Valek, Philip/0000-0002-2318-8750 FU NASA [955518.02.01.02.57]; ORAU FX We thank the TWINS team for a lot of discussions and fruitful comments. The computer programs to calculate ionospheric conductivities and solve for the electrostatic potential were written by R. Spiro and S. Sazykin. Dst, AU/AL, and SYMH indices were provided by the World Data Center for Geomagnetism, Kyoto. ACE SW and IMF data were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. This work was supported by the TWINS mission, which is a part of NASA's Explorers Program, and NASA Heliophysics Guest Investigators Program, under Work Breakdown Structure 955518.02.01.02.57. For N.B., this work was supported by an appointment to the NPP at the NASA Goddard Space Flight Center administered by ORAU through a contract with NASA and by an appointment at the NASA Goddard Space Flight Center administered by CRESST/UMD through a contract with NASA. N.B. thanks A. Glocer and E. Mitchell for proofreading of the manuscript. NR 55 TC 19 Z9 19 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 15 PY 2010 VL 115 AR A12234 DI 10.1029/2010JA015292 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696VK UT WOS:000285469300002 ER PT J AU Luo, MZ Boxe, C Jiang, J Nassar, R Livesey, N AF Luo, Mingzhao Boxe, Christopher Jiang, Jonathan Nassar, Ray Livesey, Nathaniel TI Interpretation of Aura satellite observations of CO and aerosol index related to the December 2006 Australia fires SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Remote sensing; Satellite observations; TES; OMI; MLS; GEOS-Chem; HYSPLIT ID CARBON-MONOXIDE CONCENTRATION; PRECURSOR EMISSION CONTROLS; RANGE OZONE TRANSPORT; EARTHS ATMOSPHERE; FOREST-FIRES; AIR-QUALITY; PLUME-RISE; CHEMISTRY; MODEL AB Enhanced carbon monoxide (CO) in the upper troposphere (UT) is shown by nearly collocated Tropospheric Emission Spectrometer (TES) and Microwave Limb Sounder (MLS) measurements near and down-wind from the known wildfire region of SE Australia from December 12th-19th, 2006. Enhanced ultraviolet (UV) aerosol index (Al) derived from the Ozone Monitoring Instrument (ON) measurements correlates with these high CO concentrations. The Hybrid Single Particle Langrangian Integrated Trajectory (HYSPLIT) model back trajectories trace selected air parcels, where TES observes enhanced CO in the upper and lower troposphere, to the SE Australia fire region as their initial location. Simultaneously, they show a lack of vertical advection along their tracks. TES retrieved CO vertical profiles in the higher and lower southern latitudes are examined together with the averaging kernels and show that TES CO retrievals are most sensitive at approximately 300-400 hPa. The enhanced CO observed by TES in the upper (215 hPa) and lower (681 hPa) troposphere are, therefore, influenced by mid-tropospheric CO. CEOS-Chem model simulations with an 8-day emission inventory, as the wildfire source over Australia, are sampled to the TES/MLS observation times and locations. These simulations only show CO enhancements in the lower troposphere near and down-wind from the wildfire region of SE Australia with drastic underestimates of UT CO plumes. Although CloudSat along-track ice-water content curtains are examined to see whether possible vertical convection events can explain the high UT CO values, sparse observations of collocated Aura CO and CloudSat along-track ice-water content measurements for the single event precludes any conclusive correlation. Vertical convection that uplifts the fire-induced CO (i.e., most notably referred to as pyro-cumulonimbus (pyroCb)) may provide an explanation for the incongruence between these simulations and the TES/MLS observations of enhanced CO in the UT. (C) 2010 Elsevier Inc. All rights reserved. C1 [Luo, Mingzhao; Boxe, Christopher; Jiang, Jonathan; Livesey, Nathaniel] CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. [Nassar, Ray] Univ Toronto, Dept Phys, Ctr Global Change Sci, Toronto, ON M5S 1A7, Canada. [Nassar, Ray] Univ Toronto, Dept Geog, Ctr Global Change Sci, Toronto, ON M5S 1A7, Canada. RP Boxe, C (reprint author), CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. EM christopher.boxe@jpl.nasa.gov RI Chem, GEOS/C-5595-2014; OI Nassar, Ray/0000-0001-6282-1611 FU NASA; National Aeronautics and Space Administration; Natural Sciences and Engineering Research Council (NSERC) of Canada FX We would like to thank the helpful discussions on this work with Drs. Jennifer Logan, Jimmie Lopez, Line Jourdain, Lenny Pfister and O. Torres. J. H. Jiang acknowledges the support from the NASA ACMAP program. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Funding at the University of Toronto was provided by the Natural Sciences and Engineering Research Council (NSERC) of Canada. NR 54 TC 7 Z9 7 U1 0 U2 9 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2010 VL 114 IS 12 BP 2853 EP 2862 DI 10.1016/j.rse.2010.07.003 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 670CZ UT WOS:000283400100003 ER PT J AU Hilker, T Hall, FG Coops, NC Lyapustin, A Wang, YJ Nesic, Z Grant, N Black, TA Wulder, MA Kljun, N Hopkinson, C Chasmer, L AF Hilker, Thomas Hall, Forrest G. Coops, Nicholas C. Lyapustin, Alexei Wang, Yujie Nesic, Zoran Grant, Nick Black, T. Andrew Wulder, Michael A. Kljun, Natascha Hopkinson, Chris Chasmer, Laura TI Remote sensing of photosynthetic light-use efficiency across two forested biomes: Spatial scaling SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE PRI; LUE; Light-use efficiency; AMSPEC; Eddy covariance; Shadow fraction; GPP; SOA; DF49; Douglas-fir; Aspen; MODIS; MAIAC; Spatial scaling; Carbon cycle; Terrestrial carbon cycle; LiDAR; Canopy height model ID PHOTOCHEMICAL REFLECTANCE INDEX; RADIATION-USE EFFICIENCY; DOUGLAS-FIR FOREST; DISCRETE-RETURN LIDAR; CARBON-DIOXIDE FLUXES; BOREAL ASPEN FOREST; LEAF-AREA INDEX; SPECTRAL REFLECTANCE; ECOSYSTEM RESPIRATION; MEDITERRANEAN FOREST AB Eddy covariance (EC) measurements have greatly advanced our knowledge of carbon exchange in terrestrial ecosystems. However, appropriate techniques are required to upscale these spatially discrete findings globally. Satellite remote sensing provides unique opportunities in this respect, but remote sensing of the photosynthetic light-use efficiency (epsilon), one of the key components of Gross Primary Production, is challenging. Some progress has been made in recent years using the photochemical reflectance index, a narrow waveband index centered at 531 and 570 nm. The high sensitivity of this index to various extraneous effects such as canopy structure, and the view observer geometry has so far prevented its use at landscape and global scales. One critical aspect of upscaling PRI is the development of generic algorithms to account for structural differences in vegetation. Building on previous work, this study compares the differences in the PRI: epsilon relationship between a coastal Douglas-fir forest located on Vancouver Island, British Columbia, and a mature Aspen stand located in central Saskatchewan, Canada. Using continuous, tower-based observations acquired from an automated multi-angular spectro-radiometer (AMSPEC II) installed at each site, we demonstrate that PRI can be used to measure epsilon throughout the vegetation season at the DF-49 stand (r(2)= 0.91, p<0.00) as well as the deciduous site (r(2) = 0.88, p <0.00). It is further shown that this PRI signal can be also observed from space at both sites using daily observations from the Moderate Resolution Imaging Spectro-radiometer (MODIS) and a multi-angular implementation of atmospheric correction (MAIAC) (r(2) = 0.54 DF-49; r(2) = 0.63 SOA; p<0.00). By implementing a simple hillshade model derived from airborne light detection and ranging (LiDAR) to approximate canopy shadow fractions (alpha(s)), it is further demonstrated that the differences observed in the relationship between PRI and epsilon at DF-49 and SOA can be attributed largely to differences in alpha(s). The findings of this study suggest that algorithms used to separate physiological from extraneous effects in PRI reflectance may be more broadly applicable and portable across these two climatically and structurally different biome types, when the differences in canopy structure are known. (C) 2010 Elsevier Inc. All rights reserved. C1 [Hilker, Thomas; Coops, Nicholas C.] Univ British Columbia, Fac Forest Resources Management, Vancouver, BC V6T 1Z4, Canada. [Hall, Forrest G.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Hall, Forrest G.; Lyapustin, Alexei; Wang, Yujie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nesic, Zoran; Grant, Nick; Black, T. Andrew] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada. [Wulder, Michael A.] Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, Victoria, BC V8Z 1M5, Canada. [Kljun, Natascha] Swansea Univ, Sch Environm & Soc, Dept Geog, Swansea SA2 8PP, W Glam, Wales. [Hopkinson, Chris] NSCC Annapolis Valley Campus, Appl Geomat Res Grp, Middleton, NS B0S 1P0, Canada. [Chasmer, Laura] Wilfrid Laurier Univ, Cold Reg Res Ctr, CRRC, Waterloo, ON N2L 3C5, Canada. RP Hilker, T (reprint author), Univ British Columbia, Fac Forest Resources Management, 2424 Main Mall, Vancouver, BC V6T 1Z4, Canada. EM thomas.hilker@ubc.ca RI Coops, Nicholas/J-1543-2012; Lyapustin, Alexei/H-9924-2014; Kljun, Natascha/B-8467-2008; Wulder, Michael/J-5597-2016; Nesic, Zoran/C-9655-2015 OI Coops, Nicholas/0000-0002-0151-9037; Lyapustin, Alexei/0000-0003-1105-5739; Kljun, Natascha/0000-0001-9650-2184; Wulder, Michael/0000-0002-6942-1896; FU Natural Sciences and Engineering Research Council of Canada (NSERC); BIOCAP; NASA; NERC (Natural Environment Research Council, UK) [NE/G000360/1] FX We would like to thank Dominic Lessard, Andrew Hum and Rick Ketler from UBC Faculty of Land and Food Systems (LFS) for their assistance in technical design, installation, and maintenance of AMSPEC II. This research is partially funded by the Canadian Carbon Program, the Natural Sciences and Engineering Research Council of Canada (NSERC) and BIOCAP, and an NSERC-Accelerator grant to Dr. Coops. The work of Drs. Lyapustin and Wang was supported by the NASA Terrestrial Ecology Program (Dr. Wickland). Acquisition of the LiDAR data at SOA was supported by NERC (Natural Environment Research Council, UK) grant number NE/G000360/1. NR 61 TC 68 Z9 71 U1 9 U2 64 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2010 VL 114 IS 12 BP 2863 EP 2874 DI 10.1016/j.rse.2010.07.004 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 670CZ UT WOS:000283400100004 ER PT J AU Barahona, D Rodriguez, J Nenes, A AF Barahona, D. Rodriguez, J. Nenes, A. TI Sensitivity of the global distribution of cirrus ice crystal concentration to heterogeneous freezing SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; UPPER-TROPOSPHERIC CLOUDS; TROPICAL TROPOPAUSE; RELATIVE-HUMIDITY; LOWER STRATOSPHERE; AQUEOUS-SOLUTIONS; WATER ACTIVITY; GRAVITY-WAVES; MINERAL DUST; NUCLEATION AB This study presents the sensitivity of global ice crystal number concentration, N-c, to the parameterization of heterogeneous ice nuclei (IN). Simulations are carried out with the NASA Global Modeling Initiative chemical and transport model coupled to an analytical ice microphysics parameterization. Heterogeneous freezing is described using nucleation spectra derived from theoretical considerations and empirical data for dust, black carbon, ammonium sulfate, and glassy aerosol as IN precursors. When competition between homogeneous and heterogeneous freezing is considered, global mean N-c vary by up to a factor of twenty depending on the heterogeneous freezing spectrum used. IN effects on N-c strongly depend on dust and black carbon concentrations and are strongest under conditions of weak updraft and high temperature. Regardless of the heterogeneous spectrum used, dust is an important contributor of IN over large regions of the Northern Hemisphere. Black carbon however exhibits appreciable effects on N-c when the freezing fraction is greater than 1%. Compared to in situ observations, N-c is overpredicted at temperatures below 205 K, even if a fraction of liquid aerosol is allowed to act as glassy IN. Assuming that cirrus formation is forced by weak updraft addressed this overprediction but promoted heterogeneous freezing effects to the point where homogeneous freezing is inhibited for IN concentrations as low as 1 L-1. Chemistry and dynamics must be considered to explain cirrus characteristics at low temperature. Only cloud formation scenarios where competition between homogeneous and heterogeneous freezing is the dominant feature would result in maximum supersaturation levels consistent with observations. C1 [Barahona, D.; Nenes, A.] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA. [Nenes, A.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Rodriguez, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP Barahona, D (reprint author), Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA. EM athanasios.nenes@gatech.edu RI Barahona, Donifan/G-4157-2011 FU NASA ACMAP FX This study was supported by NASA ACMAP. NR 93 TC 23 Z9 24 U1 1 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 14 PY 2010 VL 115 AR D23213 DI 10.1029/2010JD014273 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 696SW UT WOS:000285462700003 ER PT J AU Fok, MC Buzulukova, N Chen, SH Valek, PW Goldstein, J McComas, DJ AF Fok, M. -C. Buzulukova, N. Chen, S. -H. Valek, P. W. Goldstein, J. McComas, D. J. TI Simulation and TWINS observations of the 22 July 2009 storm SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ENERGETIC NEUTRAL ATOM; PITCH ANGLE DISTRIBUTIONS; TIME RING CURRENT; INNER MAGNETOSPHERE; PLASMA SHEET; MAGNETIC-FIELD; ION COMPOSITION; NOSE STRUCTURES; RADIATION BELT; IMAGE MISSION AB TWINS is the first mission to perform stereo imaging of the Earth's ring current. The magnetic storm on 22 July 2009 was at the time the largest storm observed since TWINS began routine stereo imaging in June 2008. On 22 July 2009, the Dst dropped to nearly -80 nT at 0700 and 1000 UT. During the main phase, and at the peak of the storm, TWINS 1 and 2 were near apogee and moving between predawn and postdawn local time. The energetic neutral atom (ENA) imagers on the two spacecraft captured the storm intensification and the formation of the partial ring current. The peak of the high-altitude ENA emissions was seen in the midnight-to-dawn local time sector. The development of this storm has been simulated using the comprehensive ring current model (CRCM) to understand and interpret the observed signatures. We perform CRCM runs with constant and time-varying magnetic field. The model calculations are validated by comparing the simulated ENA and ion flux intensities with TWINS ENA images and in situ ion data from a THEMIS satellite. Simulation with a static magnetic field produces a strong shielding electric field that skews the ion drift trajectories toward dawn. The model's corresponding peak ENA emissions are always more eastward than those in the observed TWINS images. On the other hand, the simulation with a dynamic magnetic field gives better spatial agreement with both ENA and in situ particle data, suggesting that temporal variations of the geomagnetic field exert a significant influence upon global ring current ion dynamics. C1 [Fok, M. -C.; Buzulukova, N.; Chen, S. -H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Valek, P. W.; Goldstein, J.; McComas, D. J.] SW Res Inst, San Antonio, TX 78228 USA. [Valek, P. W.; Goldstein, J.; McComas, D. J.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA. RP Fok, MC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mei-ching.h.fok@nasa.gov RI Fok, Mei-Ching/D-1626-2012; OI Valek, Philip/0000-0002-2318-8750 FU NASA at the Goddard Space Flight Center; NASA [955518.02.01.02.57] FX We gratefully acknowledge use of the ACE solar wind data provided through OMNI and THEMIS data from http://themis.ssl.berkeley.edu/. The Dst and symH data are provided by the World Data Center for Geomagnetism at Kyoto University, Japan. We thank Vassilis Angelopoulos for comments on the THEMIS data and providing software to remove background of the data. For Natalia Buzulukova, this work 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. We are indebted to all of the dedicated work of the TWINS team bringing these great stereo ENA images of the magnetosphere to reality. This work was supported by the TWINS mission as a part of NASA's Explorer Program, and by NASA Heliophysics Guest Investigators Program under Work Breakdown Structure 955518.02.01.02.57. NR 78 TC 17 Z9 17 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 DEC 14 PY 2010 VL 115 AR A12231 DI 10.1029/2010JA015443 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696VG UT WOS:000285468900004 ER PT J AU Kim, RS Cho, KS Moon, YJ Dryer, M Lee, J Yi, Y Kim, KH Wang, H Park, YD Kim, YH AF Kim, R. -S. Cho, K. -S. Moon, Y. -J. Dryer, M. Lee, J. Yi, Y. Kim, K. -H. Wang, H. Park, Y. -D. Kim, Yong Ha TI An empirical model for prediction of geomagnetic storms using initially observed CME parameters at the Sun SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; SOLAR-WIND; INTERPLANETARY SHOCK; EARTHWARD DIRECTION; HALO CMES; GEOEFFECTIVENESS; FIELD AB In this study, we discuss the general behaviors of geomagnetic storm strength associated with observed parameters of coronal mass ejection (CME) such as speed (V) and earthward direction (D) of CMEs as well as the longitude (L) and magnetic field orientation (M) of overlaying potential fields of the CME source region, and we develop an empirical model to predict geomagnetic storm occurrence with its strength (gauged by the Dst index) in terms of these CME parameters. For this we select 66 halo or partial halo CMEs associated with M-class and X-class solar flares, which have clearly identifiable source regions, from 1997 to 2003. After examining how each of these CME parameters correlates with the geoeffectiveness of the CMEs, we find several properties as follows: (1) Parameter D best correlates with storm strength Dst; (2) the majority of geoeffective CMEs have been originated from solar longitude 15 W, and CMEs originated away from this longitude tend to produce weaker storms; (3) correlations between Dst and the CME parameters improve if CMEs are separated into two groups depending on whether their magnetic fields are oriented southward or northward in their source regions. Based on these observations, we present two empirical expressions for Dst in terms of L, V, and D for two groups of CMEs, respectively. This is a new attempt to predict not only the occurrence of geomagnetic storms, but also the storm strength (Dst) solely based on the CME parameters. C1 [Kim, R. -S.; Yi, Y.; Kim, Yong Ha] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305754, KR, South Korea. [Kim, R. -S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cho, K. -S.; Park, Y. -D.] Korea Astron & Space Sci Inst, Solar & Space Weather Res Grp, Taejon 305348, KR, South Korea. [Moon, Y. -J.; Kim, K. -H.] Kyung Hee Univ, Sch Space Res, Yongin 446701, KR, South Korea. [Dryer, M.] Natl Ocean & Atmospher Adm, Boulder, CO 80305 USA. [Lee, J.; Wang, H.] New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA. RP Kim, RS (reprint author), Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305754, KR, South Korea. EM rskim@cnu.ac.kr RI Moon, Yong-Jae/E-1711-2013; Kim , Khan-Hyuk/E-2361-2013 FU Korean Government (MOEHRD) [KRF-2006-612-C00014, KRF-2005-202-C00158, KRF-2008-314-C00158, 20090071744]; KASI; Korean Ministry of Education, Science and Technology [R31-10016]; NASA [NAG5-12527, NAS5-01072, NNX08-8AQ90G]; NSF [AST-0908344, ANT-083995, ATM-0839216] FX This work was supported by the Korea Research Foundation grant funded by the Korean Government (MOEHRD) (KRF-2006-612-C00014, KRF-2005-202-C00158) and by the "Development of Korean Space Weather Center," the project of KASI, and the KASI basic research fund. Y.J.M. has been supported by the WCU grant (R31-10016) funded by the Korean Ministry of Education, Science and Technology and by the Korea Research Foundation grant funded by the Korean Government (MOEHRD, Basic Research Promotion Fund) (KRF-2008-314-C00158, 20090071744). M.D. was supported by NASA's Living With a Star prograrm via grant NAG5-12527 to Exploration Physics International, Inc. M.D. also thanks NOAA's Space Weather Prediction Center for their hospitality during his emeritus status. J.L. was supported NSF grants AST-0908344 and ANT-083995 and NASA grant NAS5-01072. H.W. was supported by NASA grant NNX08-8AQ90G and NSF grant ATM-0839216. The CME catalog used here is generated and maintained by NASA and the Catholic University of America in cooperation with the Naval Research Laboratory. The Dst index is provided by the World Data Center for Geomagnetism at Kyoto University. NR 42 TC 8 Z9 8 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 14 PY 2010 VL 115 AR A12108 DI 10.1029/2010JA015322 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696VG UT WOS:000285468900003 ER PT J AU Hansen, J Ruedy, R Sato, M Lo, K AF Hansen, J. Ruedy, R. Sato, M. Lo, K. TI GLOBAL SURFACE TEMPERATURE CHANGE SO REVIEWS OF GEOPHYSICS LA English DT Review ID IN-SITU; TIME-SERIES; AIR-TEMPERATURE; UNITED-STATES; NORTHERN-HEMISPHERE; CLIMATE; URBAN; NETWORK; UNCERTAINTIES; TRENDS AB We update the Goddard Institute for Space Studies (GISS) analysis of global surface temperature change, compare alternative analyses, and address questions about perception and reality of global warming. Satellite-observed night lights are used to identify measurement stations located in extreme darkness and adjust temperature trends of urban and periurban stations for nonclimatic factors, verifying that urban effects on analyzed global change are small. Because the GISS analysis combines available sea surface temperature records with meteorological station measurements, we test alternative choices for the ocean data, showing that global temperature change is sensitive to estimated temperature change in polar regions where observations are limited. We use simple 12 month (and n x 12) running means to improve the information content in our temperature graphs. Contrary to a popular misconception, the rate of warming has not declined. Global temperature is rising as fast in the past decade as in the prior 2 decades, despite year-to-year fluctuations associated with the El Nino-La Nina cycle of tropical ocean temperature. Record high global 12 month running mean temperature for the period with instrumental data was reached in 2010. C1 [Hansen, J.; Ruedy, R.; Sato, M.; Lo, K.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Hansen, J (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM jhansen@giss.nasa.gov NR 62 TC 684 Z9 715 U1 45 U2 354 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 8755-1209 EI 1944-9208 J9 REV GEOPHYS JI Rev. Geophys. PD DEC 14 PY 2010 VL 48 AR RG4004 DI 10.1029/2010RG000345 PG 29 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 696XO UT WOS:000285474900001 ER PT J AU Schramm, JP Hofmann, DC Demetriou, MD Johnson, WL AF Schramm, Joseph P. Hofmann, Douglas C. Demetriou, Marios D. Johnson, William L. TI Metallic-glass-matrix composite structures with benchmark mechanical performance SO APPLIED PHYSICS LETTERS LA English DT Article ID CELLULAR METALS; TOUGHNESS; PANELS AB Metallic-glass-matrix composites demonstrating unusual combination of high strength, high toughness, and excellent processability are utilized to fabricate cellular structures of egg-box topology. Under compressive loading, the egg-box panels are capable of undergoing extensive plastic collapse at very high plateau stresses enabling absorption of large amounts of mechanical energy. In terms of specific mechanical energy absorbed, the present panels far outperform panels of similar topology made of aluminum or fiber-reinforced polymer composites, and even surpass steel structures of highly buckling-resistant topologies, thus emerging among the highest performance structures of any kind. (C) 2010 American Institute of Physics. [doi:10.1063/1.3521412] C1 [Schramm, Joseph P.; Hofmann, Douglas C.; Demetriou, Marios D.; Johnson, William L.] CALTECH, Keck Lab, Pasadena, CA 91125 USA. [Hofmann, Douglas C.] CALTECH, Jet Prop Lab, Enterprise Engn Div, Engn & Sci Directorate, Pasadena, CA 91109 USA. RP Hofmann, DC (reprint author), CALTECH, Keck Lab, Pasadena, CA 91125 USA. EM dch@jpl.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration (NASA); Office of Naval Research [N00014-07-1-1115] FX D.C.H. acknowledges support from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). The work was supported by the Office of Naval Research under Award No. N00014-07-1-1115. NR 14 TC 10 Z9 10 U1 0 U2 24 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 13 PY 2010 VL 97 IS 24 AR 241910 DI 10.1063/1.3521412 PG 3 WC Physics, Applied SC Physics GA 696ZX UT WOS:000285481000022 ER PT J AU Marcus, SL de Viron, O Dickey, JO AF Marcus, Steven L. de Viron, Olivier Dickey, Jean O. TI Interannual atmospheric torque and El Nino-Southern Oscillation: Where is the polar motion signal? SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID ANGULAR-MOMENTUM; EARTH; FLUCTUATIONS; EXCITATION; LATITUDE; ENSO AB In this paper, we investigate the atmospheric excitation of polar motion (PM) associated with the El Nino-Southern Oscillation (ENSO) phenomenon. ENSO effects on length-of-day due to changes in the axial component of atmospheric angular momentum (AAM) have long been recognized, but identification of PM excitation with ENSO-induced equatorial AAM anomalies has proved more elusive. Here we use an appropriately modified form of the inverted barometer (IB) assumption to study ENSO-related atmospheric torques arising from pressure loading on the Earth's ellipsoidal bulge and mountains and from frictional wind stress over the Earth's land-and ocean-covered surface. The resulting dissipation torques, which accommodate adjustment of the oceanic mass distribution to time-variable atmospheric loading, are found to be small. The ellipsoidal torques have the largest amplitude, reflecting the order-of-magnitude discrepancy between the height departures of the Earth's bulge (similar to 20 km) and its surface orography (similar to 2 km). Because of relatively uniform pressure covariances with the Southern Oscillation Index over the continents for the largely land-based X component and the uniform IB response for the largely ocean-based Y component; however, the ENSO-related PM excitation arising from the ellipsoidal torques is reduced to an amplitude comparable with the sum of regional mountain torques from the individual continents. The largest of these are generated over Asia and Antarctica, arising from efficient coupling of ENSO-related surface pressure anomalies with large-scale orographic features. The geometrical mitigation of the ellipsoidal torques, classically expected to dominate equatorial AAM forcing, accounts for the lack of a detectable atmosphere-driven polar motion response to ENSO. C1 [Marcus, Steven L.; Dickey, Jean O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [de Viron, Olivier] Univ Paris Diderot, F-75005 Paris, France. [de Viron, Olivier] Inst Phys Globe, CNRS, F-75005 Paris, France. RP Marcus, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI de Viron, Olivier/N-6647-2014; OI de Viron, Olivier/0000-0003-3112-9686; Marcus, Steven/0000-0002-5763-6961 FU National Aeronautics and Space Administration FX This paper presents the results of one phase of research carried out at the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the National Aeronautics and Space Administration. The contribution of OdV to this study is IPGP contribution 3062. NR 25 TC 2 Z9 2 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-SOL EA JI J. Geophys. Res.-Solid Earth PD DEC 11 PY 2010 VL 115 AR B12409 DI 10.1029/2010JB007524 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 693WA UT WOS:000285254900001 ER PT J AU Beaulieu, JP Kipping, DM Batista, V Tinetti, G Ribas, I Carey, S Noriega-Crespo, JA Griffith, CA Campanella, G Dong, S Tennyson, J Barber, RJ Deroo, P Fossey, SJ Liang, D Swain, MR Yung, Y Allard, N AF Beaulieu, J. P. Kipping, D. M. Batista, V. Tinetti, G. Ribas, I. Carey, S. Noriega-Crespo, J. A. Griffith, C. A. Campanella, G. Dong, S. Tennyson, J. Barber, R. J. Deroo, P. Fossey, S. J. Liang, D. Swain, M. R. Yung, Y. Allard, N. TI Water in the atmosphere of HD 209458b from 3.6-8 mu m IRAC photometric observations in primary transit SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; occultations; planets and satellites: general; planetary systems ID EXTRASOLAR PLANET ATMOSPHERE; TRANSMISSION SPECTRA; EMISSION-SPECTRUM; DAYSIDE SPECTRUM; GIANT PLANETS; 189733B; TEMPERATURE; METHANE; SEARCH; STAR AB The hot Jupiter HD 209458b was observed during primary transit at 3.6, 4.5, 5.8 and 8.0 mu m using the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. We describe the procedures we adopted to correct for the systematic effects present in the IRAC data and the subsequent analysis. The light curves were fitted including limb-darkening effects and fitted using Markov Chain Monte Carlo and prayer-bead Monte Carlo techniques, obtaining almost identical results. The final depth measurements obtained by a combined Markov Chain Monte Carlo fit are at 3.6 mu m, 1.469 +/- 0.013 and 1.448 +/- 0.013 per cent; at 4.5 mu m, 1.478 +/- 0.017 per cent; at 5.8 mu m, 1.549 +/- 0.015 per cent; and at 8.0 mu m, 1.535 +/- 0.011 per cent. Our results clearly indicate the presence of water in the planetary atmosphere. Our broad-band photometric measurements with IRAC prevent us from determining the additional presence of other molecules such as CO, CO2 and methane for which spectroscopy is needed. While water vapour with a mixing ratio of 10(-4) to 10(-3) combined with thermal profiles retrieved from the day side may provide a very good fit to our observations, this data set alone is unable to resolve completely the degeneracy between water abundance and atmospheric thermal profile. C1 [Beaulieu, J. P.; Batista, V.; Allard, N.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, Paris, France. [Beaulieu, J. P.; Kipping, D. M.; Tinetti, G.; Campanella, G.; Tennyson, J.; Barber, R. J.; Fossey, S. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Ribas, I.] CSIC, Inst Ciencies Espai, IEEC, Bellaterra 08193, Spain. [Carey, S.; Noriega-Crespo, J. A.] CALTECH, IPAC Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Griffith, C. A.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Campanella, G.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Dong, S.] Ohio State Univ, Columbus, OH 43210 USA. [Deroo, P.; Swain, M. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Liang, D.] Acad Sinica, Res Ctr Environm Changes, Taipei 115, Taiwan. [Liang, D.; Yung, Y.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Allard, N.] Observ Paris, GEPI, F-75014 Paris, France. RP Beaulieu, JP (reprint author), Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, 98Bis Blvd Arago, Paris, France. EM beaulieu@iap.fr RI Tennyson, Jonathan/I-2222-2012; Dong, Subo/J-7319-2012; Ribas, Ignasi/M-2134-2014 OI Tennyson, Jonathan/0000-0002-4994-5238; Ribas, Ignasi/0000-0002-6689-0312 FU Royal Society University Research Fellowship; STFC; Leverhulme Trust; Ateneo Federato della Scienza e della Tecnologia - Universita di Roma 'La Sapienza', Collegio univ; Programme Origine des Planetes et de la Vie; NASA; [ANR-06-BLAN-0416] FX We are very grateful to Tommi Koskinen, Alan Aylward Steve Miller, Jean-Pierre Maillard and Giusi Micela for their insightful comments. GT is supported by a Royal Society University Research Fellowship; DMK by STFC; RJB by the Leverhulme Trust; GC by Ateneo Federato della Scienza e della Tecnologia - Universita di Roma 'La Sapienza', Collegio univ. 'Don N. Mazza' and LLP-Erasmus Student Placement. We acknowledge the support by ANR-06-BLAN-0416 and the 'Programme Origine des Planetes et de la Vie'. This paper 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. NR 57 TC 67 Z9 67 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 11 PY 2010 VL 409 IS 3 BP 963 EP 974 DI 10.1111/j.1365-2966.2010.16516.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 688MU UT WOS:000284854300006 ER PT J AU Altamirano, D Watts, A Linares, M Markwardt, CB Strohmayer, T Patruno, A AF Altamirano, D. Watts, A. Linares, M. Markwardt, C. B. Strohmayer, T. Patruno, A. TI Type I X-ray bursts and burst oscillations in the accreting millisecond X-ray pulsar IGR J17511-3057 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; binaries: close; stars: individual: IGR J17511-3057; stars: neutron; pulsars: general; X-rays: stars ID PROPORTIONAL COUNTER ARRAY; ATOLL SOURCE STATES; NEUTRON-STARS; HETE J1900.1-2455; TIMING-EXPLORER; XTE J1814-338; ENERGY-DEPENDENCE; HARMONIC CONTENT; AQUILA X-1; DISCOVERY AB We report the discovery of burst oscillations at the spin frequency in ten thermonuclear bursts from the accreting millisecond X-ray pulsar (AMXP) IGR J17511-3057. The burst oscillation properties are, like those from the persistent AMXPs SAX J1808.4-3658 and XTE J1814-338, anomalous compared to burst oscillations from intermittent pulsars or non-pulsing low-mass X-ray binaries. Like SAX J1808.4-3658 they show frequency drifts in the rising phase rather than the tail. There is also evidence for harmonic content. Where IGR J17511-3057 is unusual compared to the other two persistent pulsars is that oscillations are not detected throughout all bursts. As accretion rate drops the bursts get brighter and their rise/decay time-scales become shorter, while the oscillation amplitude falls below the detection threshold: first in the burst peak and then also in the rise. None of the bursts from IGR J17511-3057 shows evidence for photospheric radius expansion (which might be expected to suppress oscillation amplitude) which allow us to set an upper limit to the distance of 6.9 kpc. We discuss the implications of our results for models of the burst oscillation mechanism. C1 [Altamirano, D.; Watts, A.; Patruno, A.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Linares, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Markwardt, C. B.; Strohmayer, T.] NASA, Astroparticle Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Altamirano, D (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM d.altamirano@uva.nl FU Netherlands Organization for Scientific Research (NWO) FX We thank M. Nowak for sharing the X-ray burst time of occurrence in their Chandra data, respectively. AP acknowledges support from the Netherlands Organization for Scientific Research (NWO) Veni Fellowship. ML acknowledges support from the Netherlands Organization for Scientific Research (NWO) Rubicon Fellowship. NR 54 TC 18 Z9 18 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 11 PY 2010 VL 409 IS 3 BP 1136 EP 1145 DI 10.1111/j.1365-2966.2010.17369.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 688MU UT WOS:000284854300022 ER PT J AU Szabo, R Kollath, Z Molnar, L Kolenberg, K Kurtz, DW Bryson, ST Benko, JM Christensen-Dalsgaard, J Kjeldsen, H Borucki, WJ Koch, D Twicken, JD Chadid, M Di Criscienzo, M Jeon, YB Moskalik, P Nemec, JM Nuspl, J AF Szabo, R. Kollath, Z. Molnar, L. Kolenberg, K. Kurtz, D. W. Bryson, S. T. Benko, J. M. Christensen-Dalsgaard, J. Kjeldsen, H. Borucki, W. J. Koch, D. Twicken, J. D. Chadid, M. Di Criscienzo, M. Jeon, Y-B. Moskalik, P. Nemec, J. M. Nuspl, J. TI Does Kepler unveil the mystery of the Blazhko effect? First detection of period doubling in Kepler Blazhko RR Lyrae stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: RR Lyrae; stars: individual: V808 Cyg; stars individual: V355 Lyr; stars: oscillations; stars: variables: RR Lyrae ID INITIAL CHARACTERISTICS; CADENCE DATA; MODELS; PULSATIONS; CEPHEIDS AB The first detection of the period doubling phenomenon is reported in the Kepler RR Lyrae stars RR Lyr, V808 Cyg and V355 Lyr. Interestingly, all these pulsating stars show Blazhko modulation. The period doubling manifests itself as alternating maxima and minima of the pulsational cycles in the light curve, as well as through the appearance of half-integer frequencies located halfway between the main pulsation period and its harmonics in the frequency spectrum. The effect was found to be stronger during certain phases of the modulation cycle. We were able to reproduce the period-doubling bifurcation in our non-linear RR Lyrae models computed by the Florida-Budapest hydrocode. This enabled us to trace the origin of this instability in RR Lyrae stars to a resonance, namely a 9:2 resonance between the fundamental mode and a high-order (ninth) radial overtone showing strange-mode characteristics. We discuss the connection of this new type of variation to the mysterious Blazhko effect and argue that it may give us fresh insights into solving this century-old enigma. C1 [Szabo, R.; Kollath, Z.; Molnar, L.; Benko, J. M.; Nuspl, J.] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary. [Kolenberg, K.] Univ Vienna, Astron Inst, A-1180 Vienna, Austria. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England. [Twicken, J. D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Chadid, M.] Univ Nice, Observ Cote Azur, UMR 6525, F-06108 Nice 02, France. [Di Criscienzo, M.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Jeon, Y-B.] Korea Astron & Space Inst, Taejon 305346, South Korea. [Moskalik, P.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada. RP Szabo, R (reprint author), Hungarian Acad Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary. EM rszabo@konkoly.hu OI Szabo, Robert/0000-0002-3258-1909; Benko, Jozsef/0000-0003-3851-6603; Molnar, Laszlo/0000-0002-8159-1599 FU NASA's Science Mission Directorate; National Office for Research and Technology through the Hungarian Space Office [URK09350]; Hungarian Academy of Sciences; Austrian FWF [T359, P19962] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. This project has been supported by the National Office for Research and Technology through the Hungarian Space Office Grant No. URK09350 and the 'Lendulet' programme of the Hungarian Academy of Sciences. KK acknowledges the support of Austrian FWF projects T359 and P19962. The authors gratefully acknowledge the entire Kepler team, whose outstanding efforts have made these results possible. NR 29 TC 68 Z9 69 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 11 PY 2010 VL 409 IS 3 BP 1244 EP 1252 DI 10.1111/j.1365-2966.2010.17386.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 688MU UT WOS:000284854300032 ER PT J AU Rehak, P Carini, G Chen, W De Geronimo, G Fried, J Li, Z Pinelli, DA Siddons, DP Vernon, E Gaskin, JA Ramsey, BD AF Rehak, Pavel Carini, Gabriella Chen, Wei De Geronimo, Gianluigi Fried, Jack Li, Zheng Pinelli, Donald A. Siddons, D. Peter Vernon, Emerson Gaskin, Jessica A. Ramsey, Brian D. TI Arrays of silicon drift detectors for an extraterrestrial X-ray spectrometer SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 11th European Symposium on Semiconductor Detectors CY JUN 07-11, 2009 CL Wildbad Kreuth, GERMANY SP PNSensor GmbH, PNDetector GmbH, XIA LLC DE SDD; Spectrometer; Detector; Hexagonal; Spiral; ASIC; Array; X-ray; Junction; Field; Silicon; Drift AB Arrays of Silicon Drift Detectors (SDD) were designed produced and tested These arrays are the central part of an X-Ray Spectrometer (XRS) for measuring the abundances of light surface elements (C-Fe) fluoresced by ambient radiation on the investigated celestial object The basic building element (or cell) of the arrays consists of a single hexagonal SDD Signal electrons drift toward the center of the hexagon where a very low capacitance anode is located The hexagonal shape of an individual SOD allows for a continuous covering of large detection areas of various shapes To match the number of SOD cells with the external Application Specific Integrated Circuit (ASIC) two arrays one with 16 and another with 64 cells were developed One side of SDDs called the window side is a continuous thin rectifying junction through which the X-ray radiation enters the detector The opposite side called the device side contains electron collecting anodes as well as all other electrodes needed to generate the drift field and to sink leakage current produced on Si-SiO2 interface On both sides of the detector array there is a system of guard rings which smoothly adjusts the voltage of the boundary cells to the ground potential of the silicon outside the sensitive volume The drift voltage inside the detector is generated by an implanted rectifying contact which forms a hexagonal spiral This spiral produces the main valley where signal electrons drift as well as the voltage divider to produce the drift field System performance is shown by a spectrum of Mn X-rays produced by the decay of Fe-55 (C) 2010 Elsevier B V All rights reserved C1 [Rehak, Pavel; Carini, Gabriella; Chen, Wei; De Geronimo, Gianluigi; Fried, Jack; Li, Zheng; Pinelli, Donald A.; Siddons, D. Peter; Vernon, Emerson] Brookhaven Natl Lab, Upton, NY 11973 USA. [Gaskin, Jessica A.; Ramsey, Brian D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Chen, W (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA. NR 5 TC 12 Z9 12 U1 1 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD DEC 11 PY 2010 VL 624 IS 2 BP 260 EP 264 DI 10.1016/j.nima.2010.05.058 PG 5 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 695LA UT WOS:000285370400005 ER PT J AU Abdo, AA Ackermann, M Ajello, M Allafort, A Baldini, L Ballet, J Barbiellini, G Baring, MG Bastieri, D Bellazzini, R Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bouvier, A Bregeon, J Brigida, M Bruel, P Burnett, TH Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Celik, O Chaty, S Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Conrad, J den Hartog, PR Dermer, CD de Angelis, A de Palma, F Dib, R Dormody, M Silva, EDE Drell, PS Dubois, R Dumora, D Enoto, T Favuzzi, C Frailis, M Fusco, P Gargano, F Gehrels, N Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grondin, MH Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hays, E Israel, GL Johannesson, G Johnson, AS Kaspi, VM Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Lee, SH Lemoine-Goumard, M Longo, F Loparco, F Lovellette, MN Lubrano, P Makeev, A Marelli, M Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Nolan, PL Nuss, E Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Parent, D Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Rea, N Reimer, A Reimer, O Reposeur, T Ritz, S Sadrozinski, HFW Parkinson, PMS Sgro, C Siskind, EJ Smith, DA Spandre, G Spinelli, P Strickman, MS Takahashi, H Tanaka, T Thayer, JB Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Troja, E Uchiyama, Y Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Winer, BL Wood, KS Yang, Z Ziegler, M AF Abdo, A. A. Ackermann, M. Ajello, M. Allafort, A. Baldini, L. Ballet, J. Barbiellini, G. Baring, M. G. Bastieri, D. Bellazzini, R. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bouvier, A. Bregeon, J. Brigida, M. Bruel, P. Burnett, T. H. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Celik, Oe. Chaty, S. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Conrad, J. den Hartog, P. R. Dermer, C. D. de Angelis, A. de Palma, F. Dib, R. Dormody, M. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Enoto, T. Favuzzi, C. Frailis, M. Fusco, P. Gargano, F. Gehrels, N. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grondin, M. -H. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hays, E. Israel, G. L. Johannesson, G. Johnson, A. S. Kaspi, V. M. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Lee, S. -H. Lemoine-Goumard, M. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Makeev, A. Marelli, M. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Nolan, P. L. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Parent, D. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Rea, N. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Sadrozinski, H. F. -W. Parkinson, P. M. Saz Sgro, C. Siskind, E. J. Smith, D. A. Spandre, G. Spinelli, P. Strickman, M. S. Takahashi, H. Tanaka, T. Thayer, J. B. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Troja, E. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Winer, B. L. Wood, K. S. Yang, Z. Ziegler, M. TI SEARCH FOR GAMMA-RAY EMISSION FROM MAGNETARS WITH THE FERMI LARGE AREA TELESCOPE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: stars; magnetic fields; pulsars: individual (4U 0142+614, 1E 1048.1-5937, 1E 1841-045, 1E 1547-5408, 1RXS J1708-4009, XTE J1810-197, CXOU J1647-4552, 1E 2259+586, SGR 1900+14, SGR 1806-20, SGR 1627-41, SGR 0501+4516, SGR 0418+5729); stars: magnetars ID RESONANT CYCLOTRON SCATTERING; HARD X-RAYS; 4U 0142+61; AXP 4U-0142+61; 1E 1547.0-5408; SGR 0501+4516; CRAB PULSAR; DISCOVERY; REPEATER; OUTBURST AB We report on the search for 0.1-10 GeV emission from magnetars in 17 months of Fermi Large Area Telescope (LAT) observations. No significant evidence for gamma-ray emission from any of the currently known magnetars is found. The most stringent upper limits to date on their persistent emission in the Fermi energy range are estimated between similar to 10(-12) and 10(-10) erg s(-1) cm(-2), depending on the source. We also searched for gamma-ray pulsations and possible outbursts, also with no significant detection. The upper limits derived support the presence of a cutoff at an energy below a few MeV in the persistent emission of magnetars. They also show the likely need for a revision of current models of outer-gap emission from strongly magnetized pulsars, which, in some realizations, predict detectable GeV emission from magnetars at flux levels exceeding the upper limits identified here using the Fermi-LAT observations. C1 [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.; Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Allafort, A.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Chiang, J.; Claus, R.; den Hartog, P. R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Enoto, T.; Glanzman, T.; Godfrey, G.; Johnson, A. S.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Allafort, A.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Chiang, J.; Claus, R.; den Hartog, P. R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Enoto, T.; Glanzman, T.; Godfrey, G.; Johnson, A. S.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Chaty, S.; Grenier, I. A.; Naumann-Godo, M.; Tibaldo, L.] CEA IRFU CNRS Univ Paris Diderot, Lab AIM, Serv Astrophys, CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Bastieri, D.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caliandro, G. A.; Hadasch, D.; Rea, N.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain. [Caraveo, P. A.; Marelli, M.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Celik, Oe.; Gehrels, N.; Harding, A. K.; Hays, E.; McEnery, J. E.; Moiseev, A. A.; Thompson, D. J.; Troja, E.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celik, Oe.; Moiseev, A. A.; Vasileiou, V.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA. [Celik, Oe.; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Celik, Oe.; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA. [Conrad, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dib, R.; Kaspi, V. M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Dormody, M.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Dormody, M.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Dumora, D.; Grondin, M. -H.; Lemoine-Goumard, M.; Reposeur, T.; Smith, D. A.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res CSPAR, Huntsville, AL 35899 USA. [Hanabata, Y.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Israel, G. L.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Roma, Italy. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mehault, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.; Vianello, G.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Chavannes Des Bois, Switzerland. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM tburnett@u.washington.edu; andrea.caliandro@ieec.uab.es; daniela.hadasch@gmail.com; rea@ieec.uab.es RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Saz Parkinson, Pablo Miguel/I-7980-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Rea, Nanda/I-2853-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Marelli, Martino/0000-0002-8017-0338; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Chaty, Sylvain/0000-0002-5769-8601; Pesce-Rollins, Melissa/0000-0003-1790-8018; Israel, GianLuca/0000-0001-5480-6438; Giroletti, Marcello/0000-0002-8657-8852; Rea, Nanda/0000-0003-2177-6388; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Sgro', Carmelo/0000-0001-5676-6214; Giordano, Francesco/0000-0002-8651-2394; Rando, Riccardo/0000-0001-6992-818X FU K. A. Wallenberg Foundation; International Doctorate on Astroparticle Physics (IDAPP); NASA, United States; DOE, United States; CEA/Irfu, France; IN2P3/CNRS, France; ASI, Italy; INFN, Italy; MEXT, Japan; KEK, Japan; JAXA, Japan; Swedish Research Council; National Space Board in Sweden; INAF in Italy; CNES in France FX Partially supported by the International Doctorate on Astroparticle Physics (IDAPP) program.; The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. NR 43 TC 25 Z9 25 U1 0 U2 1 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 DEC 10 PY 2010 VL 725 IS 1 BP L73 EP L78 DI 10.1088/2041-8205/725/1/L73 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UE UT WOS:000284575400016 ER PT J AU Duvall, TL Birch, AC AF Duvall, T. L., Jr. Birch, A. C. TI THE VERTICAL COMPONENT OF THE SUPERGRANULAR MOTION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE convection; methods: data analysis; Sun: helioseismology; Sun: photosphere; Sun: surface magnetism ID WAVE-LIKE PROPERTIES; SOLAR SUPERGRANULATION; HELIOSEISMOLOGY; GRANULATION; INTENSITY; FLOWS AB Supergranules are observed at the solar photosphere as a cellular horizontal flow pattern with flow diverging from cell centers and converging on cell boundaries. Clark & Johnson calculated that mass conservation leads to an expected vertical flow of only 10 ms(-1), which has been difficult to observe. In the present work, Doppler images near the disk center from Michelson Doppler Imager are averaged about locations of cell centers to obtain the necessary signal-to-noise ratio to see the vertical flow. It is found that, for an average over 1100 cell centers, there is a 10 ms(-1) upflow at cell center and a 5 ms(-1) downflow at the cell boundaries, confirming the previous estimate. The rms vertical flow is 4 ms(-1), smaller than Giovanelli's upper limit of 10 ms(-1). C1 [Duvall, T. L., Jr.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. [Birch, A. C.] NW Res Associates Inc, Colorado Res Associates Div, Boulder, CO 80301 USA. RP Duvall, TL (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 661, Greenbelt, MD 20771 USA. EM Thomas.L.Duvall@nasa.gov RI Duvall, Thomas/C-9998-2012 FU NASA [NAG5-13261, NNH04CC05C] FX The MDI project is supported by NASA contract NAG5-13261 to Stanford University. SOHO is a project of international cooperation between ESA and NASA. The work of A.C.B. was supported by NASA contract NNH04CC05C. NR 20 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2010 VL 725 IS 1 BP L47 EP L51 DI 10.1088/2041-8205/725/1/L47 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UE UT WOS:000284575400011 ER PT J AU Slaba, TC Blattnig, SR Badavi, FF AF Slaba, T. C. Blattnig, S. R. Badavi, F. F. TI Faster and more accurate transport procedures for HZETRN SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Space radiation; Particle transport; Radiation exposure; Radiation transport; HZETRN ID ONE-DIMENSION AB The deterministic transport code HZETRN was developed for research scientists and design engineers studying the effects of space radiation on astronauts and instrumentation protected by various shielding materials and structures. In this work, several aspects of code verification are examined. First, a detailed derivation of the light particle (A <= 4) and heavy ion (A > 4) numerical marching algorithms used in HZETRN is given. References are given for components of the derivation that already exist in the literature, and discussions are given for details that may have been absent in the past. The present paper provides a complete description of the numerical methods currently used in the code and is identified as a key component of the verification process. Next, a new numerical method for light particle transport is presented, and improvements to the heavy ion transport algorithm are discussed. A summary of round-off error is also given, and the impact of this error on previously predicted exposure quantities is shown. Finally, a coupled convergence study is conducted by refining the discretization parameters (step-size and energy grid-size). From this study, it is shown that past efforts in quantifying the numerical error in HZETRN were hindered by single precision calculations and computational resources. It is determined that almost all of the discretization error in HZETRN is caused by the use of discretization parameters that violate a numerical convergence criterion related to charged target fragments below 50 AMeV. Total discretization errors are given for the old and new algorithms to 100 g/cm(2) in aluminum and water, and the improved accuracy of the new numerical methods is demonstrated. Run time comparisons between the old and new algorithms are given for one, two, and three layer slabs of 100 g/cm2 of aluminum, polyethylene, and water. The new algorithms are found to be almost 100 times faster for solar particle event simulations and almost 10 times faster for galactic cosmic ray simulations. Published by Elsevier Inc. C1 [Slaba, T. C.; Blattnig, S. R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Badavi, F. F.] Christopher Newport Univ, Newport News, VA 23607 USA. RP Slaba, TC (reprint author), NASA, Langley Res Ctr, Mail Stop 188E,2 W Reid St,Rm 281, Hampton, VA 23681 USA. EM Tony.C.Slaba@nasa.gov; Steve.R.Blattnig@nasa.gov; Francis.F.Badavi@nasa.gov FU NASA [NNL06AA14A, NNX09AR20A] FX This research was sponsored by NASA Research Grant NNL06AA14A and NNX09AR20A. The authors thank William Oberkampf for his guidance and helpful discussion. NR 30 TC 39 Z9 39 U1 2 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD DEC 10 PY 2010 VL 229 IS 24 BP 9397 EP 9417 DI 10.1016/j.jcp.2010.09.010 PG 21 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 676HN UT WOS:000283901700023 ER PT J AU Niemann, HB Atreya, SK Demick, JE Gautier, D Haberman, JA Harpold, DN Kasprzak, WT Lunine, JI Owen, TC Raulin, F AF Niemann, H. B. Atreya, S. K. Demick, J. E. Gautier, D. Haberman, J. A. Harpold, D. N. Kasprzak, W. T. Lunine, J. I. Owen, T. C. Raulin, F. TI Composition of Titan's lower atmosphere and simple surface volatiles as measured by the Cassini-Huygens probe gas chromatograph mass spectrometer experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID VOYAGER INFRARED OBSERVATIONS; AMORPHOUS WATER ICE; HETEROGENEOUS REACTION; CHEMICAL-COMPOSITION; ORGANIC HAZE; NOBLE-GASES; METHANE; ABUNDANCES; ORIGIN; NITROGEN AB The Cassini-Huygens probe gas chromatograph mass spectrometer (GCMS) determined the composition of the Titan atmosphere from similar to 140 km altitude to the surface. After landing, it returned composition data of gases evaporated from the surface. Height profiles of molecular nitrogen (N-2), methane (CH4), and molecular hydrogen (H-2) were determined. Traces were detected on the surface of evaporating methane, ethane (C2H6), acetylene (C2H2), cyanogen (C2N2), and carbon dioxide (CO2). The methane data showed evidence that methane precipitation occurred recently. The methane mole fraction was (1.48 +/- 0.09) x 10(-2) in the lower stratosphere (139.8-75.5 km) and (5.65 +/- 0.18) x 10(-2) near the surface (6.7 km to the surface). The molecular hydrogen mole fraction was (1.01 +/- 0.16) x 10(-3) in the atmosphere and (9.90 +/- 0.17) x 10(-4) on the surface. Isotope ratios were 167.7 +/- 0.6 for N-14/N-15 in molecular nitrogen, 91.1 +/- 1.4 for C-12/C-13 in methane, and (1.35 +/- 0.30) x 10(-4) for D/H in molecular hydrogen. The mole fractions of Ar-36 and radiogenic Ar-40 are (2.1 +/- 0.8) x 10(-7) and (3.39 +/- 0.12) x 10(-5), respectively. Ne-22 has been tentatively identified at a mole fraction of (2.8 +/- 2.1) x 10(-7). Krypton and xenon were below the detection threshold of 1 x 10(-8) mole fraction. Science data were not retrieved from the gas chromatograph subsystem as the abundance of the organic trace gases in the atmosphere and on the ground did not reach the detection threshold. Results previously published from the GCMS experiment are superseded by this publication. C1 [Niemann, H. B.; Haberman, J. A.; Harpold, D. N.; Kasprzak, W. T.] NASA, Greenbelt, MD 20771 USA. [Atreya, S. K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Demick, J. E.] Huntington Coll, Dept Phys & Phys Sci, Montgomery, AL 36106 USA. [Gautier, D.] Observ Paris, LESIA, F-92195 Meudon, France. [Lunine, J. I.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. [Owen, T. C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Raulin, F.] Univ Paris 12, Univ Paris 07, CNRS, LISA, F-94000 Creteil, France. RP Niemann, HB (reprint author), NASA, Mail Code 699, Greenbelt, MD 20771 USA. EM hasso.b.niemann@nasa.gov RI Harpold, Dan/I-3345-2013 FU NASA; ESA; CNES FX We acknowledge the Huygens Atmospheric Structure Instrument (HASI) team for providing the atmospheric pressure-temperature-altitude data to the GCMS team. We thank D. Strobel for his discussion on atmospheric loss and for providing a preprint of his paper on molecular hydrogen in Titan's atmosphere. The contributions of personnel at NASA Goddard Space Flight Center (GSFC), University of Michigan, University of Paris, and Ohio State University are acknowledged. We are indebted to Eric Raaen of GSFC for his continued support in instrument testing, data analysis, and development of laboratory software. We thank Kiran Patel of GSFC for the assistance he provided for the postlaunch instrument calibration. We also thank the personnel at the European Space Research and Technology Centre (ESTEC) and the European Space Operations Center (ESOC) for their technical support and guidance during this mission. We acknowledge NASA, ESA, and CNES for support of the mission. NR 84 TC 136 Z9 137 U1 0 U2 43 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 10 PY 2010 VL 115 AR E12006 DI 10.1029/2010JE003659 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 693YH UT WOS:000285260800002 ER PT J AU Purucker, ME Nicholas, JB AF Purucker, Michael E. Nicholas, Joseph B. TI Global spherical harmonic models of the internal magnetic field of the Moon based on sequential and coestimation approaches SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LUNAR-PROSPECTOR; CALIBRATION; ANOMALIES AB Three new models of the global internal magnetic field of the Moon based on Lunar Prospector (LP) fluxgate magnetometer observations are developed for use in understanding the origin of the Moon's crustal magnetic field and for modeling its interaction with the solar wind. The models are at spherical harmonic degree 170, corresponding to 64 km wavelength resolution, from 30 km mean altitude LP observations. Coverage is complete except for a few areas near each pole. Original signal amplitudes are best preserved in the sequential approach map, whereas feature recognition is superior in the coestimation and harmonic wave number correlation maps. Spherical harmonic degrees less than 15, corresponding to 666 km wavelength, are largely absent from the Moon's internal magnetic field. We interpret this bound in terms of the Moon's impact history. A derived magnetization map suggests magnetizations may locally exceed 0.2 A/m in the lunar crust at the survey resolution if the magnetic crust is as thick as 40 km. C1 [Purucker, Michael E.; Nicholas, Joseph B.] NASA, Goddard Space Flight Ctr, Raytheon Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Purucker, ME (reprint author), NASA, Goddard Space Flight Ctr, Raytheon Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. FU NASA FX We would like to acknowledge the Lunar Prospector team and especially the late Mario Acuna for the collection of this data set. M. Wieczorek, J. Head, N. Olsen, J. Halekas, D. Clark, V. Lesur, T. Sabaka, H. Tsunakawa, I. Garrick-Bethell, C. Russell, K. Whaler, and L. Hood provided valuable comments, data sets, or codes. We thank H. Tsunakawa for the Selene global magnetic model. M. Mandea provided an uninterrupted time for writing at Boiscommun, and B. Langlais, R. Lillis, D. Blewett, J. Slavin, and H. Frey were a source of stimulating discussions on related topics. A. Isac provided assistance with the figures. M. Purucker and J. Nicholas were supported by a NASA Discovery Data Analysis Program (DDAP) contract. GMT [Wessel and Smith, 1998] was used for the graphics and some analysis. SHTOOLS, by M. Wieczorek (IPGP), was used to implement the Driscoll and Healy sampling theorem [Driscoll and Healy, 1994]. We thank an anonymous reviewer and the Editor for improvements to the manuscript. NR 26 TC 35 Z9 37 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 10 PY 2010 VL 115 AR E12007 DI 10.1029/2010JE003650 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 693YH UT WOS:000285260800001 ER PT J AU Koval, A Szabo, A AF Koval, A. Szabo, A. TI Multispacecraft observations of interplanetary shock shapes on the scales of the Earth's magnetosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MULTIPLE SPACECRAFT OBSERVATIONS; RANKINE-HUGONIOT PROBLEM; SOLAR-WIND; 3-DIMENSIONAL PLASMA; NORMALS; MONITOR AB We are presenting a study of interplanetary shock shapes as observed by multiple spacecraft in the solar wind. The analysis of the 1 May 1998 shock observed by six spacecraft is presented in detail as an example to demonstrate possible complex shock shapes with small- and large-scale curvatures of the shock surface. To systematically estimate the shock front deviation from planarity on different scales, we are presenting an analysis of 62 shocks observed by Wind and at least one other spacecraft. Our results show the presence of local (on scales up to similar to 30 R(E)) shock curvatures with radii of less than similar to 50 to similar to 200 R(E) for the majority of analyzed shocks. On larger scales, the shock curvature decreases and reaches the limit of the strongest possible curvature with radius of similar to 400 R(E) on scales greater than similar to 100 R(E) for all analyzed shocks. C1 [Koval, A.; Szabo, A.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. [Koval, A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Koval, A (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Mail Code 672,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM andriy.koval@nasa.gov; adam.szabo@nasa.gov NR 32 TC 5 Z9 5 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 10 PY 2010 VL 115 AR A12105 DI 10.1029/2010JA015373 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 693WQ UT WOS:000285256500002 ER PT J AU Wilson, LB Cattell, CA Kellogg, PJ Goetz, K Kersten, K Kasper, JC Szabo, A Wilber, M AF Wilson, L. B., III Cattell, C. A. Kellogg, P. J. Goetz, K. Kersten, K. Kasper, J. C. Szabo, A. Wilber, M. TI Large-amplitude electrostatic waves observed at a supercritical interplanetary shock SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS BOW SHOCK; CYCLOTRON HARMONIC-WAVES; QUASI-PERPENDICULAR SHOCK; CRITICAL MACH NUMBER; ISEE-2 OBSERVATIONS; COLLISIONLESS SHOCKS; DRIFT INSTABILITY; WIND SPACECRAFT; INTENSE BURSTS; UPSTREAM AB We present the first observations at an interplanetary shock of large-amplitude (> 100 mV/m pk-pk) solitary waves and large-amplitude (similar to 30 mV/m pk-pk) waves exhibiting characteristics consistent with electron Bernstein waves. The Bernstein-like waves show enhanced power at integer and half-integer harmonics of the cyclotron frequency with a broadened power spectrum at higher frequencies, consistent with the electron cyclotron drift instability. The Bernstein-like waves are obliquely polarized with respect to the magnetic field but parallel to the shock normal direction. Strong particle heating is observed in both the electrons and ions. The observed heating and waveforms are likely due to instabilities driven by the free energy provided by reflected ions at this supercritical interplanetary shock. These results offer new insights into collisionless shock dissipation and wave-particle interactions in the solar wind. C1 [Wilson, L. B., III; Cattell, C. A.; Kellogg, P. J.; Goetz, K.; Kersten, K.] Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. [Kasper, J. C.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Szabo, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wilber, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Wilson, LB (reprint author), Univ Minnesota, Dept Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA. EM wilson@physics.umn.edu; cattell@fields.space.umn.edu; pauljkellogg@gmail.com; goetz@waves.space.umn.edu; kkersten@physics.umn.edu; jkasper@cfa.harvard.edu; adam.szabo-1@nasa.gov; wilber@ssl.berkeley.edu RI Kasper, Justin/D-1152-2010; Wilson III, Lynn/D-4425-2012; OI Kasper, Justin/0000-0002-7077-930X; Wilson III, Lynn/0000-0002-4313-1970; Cattell, Cynthia/0000-0002-3805-320X FU NESSF [NNX07AU72H, NNX07AI05G] FX We thank R. Lin (3DP), K. Ogilvie (SWE), and R. Lepping (MFI) for the use of data from their instruments. We would also like to thank M. Pulupa, S. D. Bale, and P. Schroeder for technical help with the 3DP software and analysis. We thank Linghua Wang for help in calibration of the SST Foil data. This research was supported by NESSF grant NNX07AU72H and grant NNX07AI05G. NR 51 TC 18 Z9 18 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 10 PY 2010 VL 115 AR A12104 DI 10.1029/2010JA015332 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 693WQ UT WOS:000285256500001 ER PT J AU Bottke, WF Walker, RJ Day, JMD Nesvorny, D Elkins-Tanton, L AF Bottke, William F. Walker, Richard J. Day, James M. D. Nesvorny, David Elkins-Tanton, Linda TI Stochastic Late Accretion to Earth, the Moon, and Mars SO SCIENCE LA English DT Article ID SIDEROPHILE ELEMENT SYSTEMATICS; CORE FORMATION; OSMIUM ISOTOPE; ASTEROID BELT; MANTLE; ORIGIN; DIFFERENTIATION; CONSTRAINTS; METEORITES; SILICATE AB Core formation should have stripped the terrestrial, lunar, and martian mantles of highly siderophile elements (HSEs). Instead, each world has disparate, yet elevated HSE abundances. Late accretion may offer a solution, provided that >= 0.5% Earth masses of broadly chondritic planetesimals reach Earth's mantle and that similar to 10 and similar to 1200 times less mass goes to Mars and the Moon, respectively. We show that leftover planetesimal populations dominated by massive projectiles can explain these additions, with our inferred size distribution matching those derived from the inner asteroid belt, ancient martian impact basins, and planetary accretion models. The largest late terrestrial impactors, at 2500 to 3000 kilometers in diameter, potentially modified Earth's obliquity by similar to 10 degrees, whereas those for the Moon, at similar to 250 to 300 kilometers, may have delivered water to its mantle. C1 [Bottke, William F.; Nesvorny, David] SW Res Inst, Boulder, CO 80302 USA. [Bottke, William F.; Nesvorny, David] NASA, Lunar Sci Inst, Boulder, CO 80302 USA. [Walker, Richard J.; Day, James M. D.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Day, James M. D.] Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA. [Elkins-Tanton, Linda] MIT, Cambridge, MA 02139 USA. RP Bottke, WF (reprint author), SW Res Inst, 1050 Walnut St,Suite 400, Boulder, CO 80302 USA. EM bottke@boulder.swri.edu RI Day, James/A-5099-2010; Elkins-Tanton, Linda/C-5508-2008; Walker, Richard/K-6869-2016 OI Day, James/0000-0001-9520-3465; Elkins-Tanton, Linda/0000-0003-4008-1098; Walker, Richard/0000-0003-0348-2407 FU NASA's Lunar Science Institute [NNA09DB33A]; NASA [NNG04GJ49A] FX We thank A. Barr, R. Canup, R. Citron, L. Dones, H. Levison, J. Jones, H. Nekvasil, A. Morbidelli, D. Minton, S. Mojzsis, G. J. Taylor, and D. Vokouhlicky for many useful discussions and two anonymous reviewers for constructive reviews. W.F.B's and D.N.'s participation was supported by NASA's Lunar Science Institute through a grant to the Center for Lunar Origin and Evolution at the Southwest Research Institute in Boulder, Colorado. R.J.W.'s and J.M.D.D.'s work was supported by NASA's Lunar Science Institute through contract NNA09DB33A to the Center for Lunar Science and Exploration at the Lunar and Planetary Institute in Houston, Texas, and the NASA Astrobiology Program through grant NNG04GJ49A to the Goddard Center for Astrobiology in Greenbelt, Maryland. NR 39 TC 76 Z9 77 U1 0 U2 27 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 DEC 10 PY 2010 VL 330 IS 6010 BP 1527 EP 1530 DI 10.1126/science.1196874 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 692LE UT WOS:000285153500061 PM 21148387 ER PT J AU Treuhaft, RN Goncalves, FG Drake, JB Chapman, BD dos Santos, JR Dutra, LV Graca, PMLA Purcell, GH AF Treuhaft, R. N. Goncalves, F. G. Drake, J. B. Chapman, B. D. dos Santos, J. R. Dutra, L. V. Graca, P. M. L. A. Purcell, G. H. TI Biomass estimation in a tropical wet forest using Fourier transforms of profiles from lidar or interferometric SAR SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RADAR AB Tropical forest biomass estimation based on the structure of the canopy is a burgeoning and crucial remote sensing capability for balancing terrestrial carbon budgets. This paper introduces a new approach to structural biomass estimation based on the Fourier transform of vertical profiles from lidar or interferometric SAR (InSAR). Airborne and field data were used from 28 tropical wet forest stands at La Selva Biological Station, Costa Rica, with average biomass of 229 Mg-ha(-1). RMS scatters of remote sensing biomass estimates about field measurements were 58.3 Mg-ha(-1), 21%, and 76.1 Mg-ha(-1), 26%, for lidar and InSAR, respectively. Using mean forest height, the RMS scatter was 97 Mg-ha(-1), approximate to 34% for both lidar and InSAR. The confidence that Fourier transforms are a significant improvement over height was >99% for lidar and approximate to 90% for InSAR. Lidar Fourier transforms determined the useful range of vertical wavelengths to be 14 m to 100 m. Citation: Treuhaft, R. N., F. G. Goncalves, J. B. Drake, B. D. Chapman, J. R. dos Santos, L. V. Dutra, P. M. L. A. Graca, and G. H. Purcell (2010), Biomass estimation in a tropical wet forest using Fourier transforms of profiles from lidar or interferometric SAR, Geophys. Res. Lett., 37, L23403, doi:10.1029/2010GL045608. C1 [Treuhaft, R. N.; Goncalves, F. G.; Chapman, B. D.; Purcell, G. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Goncalves, F. G.] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. [Drake, J. B.] US Forest Serv, USDA, Tallahassee, FL 32303 USA. [dos Santos, J. R.; Dutra, L. V.] Inst Nacl Pesquisas Espaciais, BR-12227 Sao Jose Dos Campos, SP, Brazil. [Graca, P. M. L. A.] Inst Nacl de Pesquisas da Amazonia, BR-69060 Manaus, Amazonas, Brazil. RP Treuhaft, RN (reprint author), CALTECH, Jet Prop Lab, MS 138-212, Pasadena, CA 91109 USA. EM robert.treuhaft@jpl.nasa.gov; fabio.goncalves@jpl.nasa.gov; jasondrake@fs.fed.us; bruce.chapman@jpl.nasa.gov; jroberto@dsr.inpe.br; dutra@dpi.inpe.br; pmlag@inpa.govbr; george.purcell@jpl.nasa.gov RI de Alencastro Graca, Paulo Mauricio/B-3375-2013; Dutra, Luciano/C-6582-2009 OI Dutra, Luciano/0000-0002-7757-039X FU National Aeronautics and Space Administration FX The research described in this paper was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 16 TC 20 Z9 20 U1 0 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 DEC 9 PY 2010 VL 37 AR L23403 DI 10.1029/2010GL045608 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 693WE UT WOS:000285255300005 ER PT J AU Han, SC Sauber, J Luthcke, S AF Han, Shin-Chan Sauber, Jeanne Luthcke, Scott TI Regional gravity decrease after the 2010 Maule (Chile) earthquake indicates large-scale mass redistribution SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SUMATRA-ANDAMAN EARTHQUAKE; LAYERED SPHERICAL EARTH; GRACE AB We report small but detectable changes in the GRACE satellites' relative trajectory after the M8.8 Maule, Chile earthquake on 27 February 2010 that can be used to delineate the shift in the gravity field. A gravity anomaly of -5 mu Gal with a spatial scale of 500 km was found east of the epicenter after the earthquake. Based on coseismic models, the long-wavelength negative gravity change is primarily the result of crustal dilatation as well as surface subsidence in the onland region. The offshore positive gravity anomaly predicted from finite fault coseismic models is considerably smaller because the gravity changes due to surface uplift and interior deformation are opposite in polarity. Our study suggests a role for large-scale gravity observations in deciphering changes of the Earth's interior during great earthquakes by filling in the seldom-observed long-wavelength spectrum of earthquake deformations as a complement to surface geodetic measurements and seismic data. Citation: Han, S.-C., J. Sauber, and S. Luthcke (2010), Regional gravity decrease after the 2010 Maule (Chile) earthquake indicates large-scale mass redistribution, Geophys. Res. Lett., 37, L23307, doi:10.1029/2010GL045449. C1 [Han, Shin-Chan; Sauber, Jeanne; Luthcke, Scott] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Han, Shin-Chan] Univ Maryland Baltimore Cty, GEST, Baltimore, MD 21228 USA. RP Han, SC (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. EM shin-chan.han@nasa.gov RI Luthcke, Scott/D-6283-2012; Sauber, Jeanne/D-7684-2012; Han, Shin-Chan/A-2022-2009 FU NASA FX This work was supported by NASA GRACE projects and Earth Surface and Interior program. We thank DLR for providing the GRACE telemetry data and JPL for producing the high-quality Level-1B products. David Rowlands is acknowledged for explanation on two GRACE satellites. We thank Chen Ji, Thorne Lay, Charles Ammon, and Anthony Sladen for coseismic finite fault models and Fred Pollitz for numerical codes to compute coseismic displacement and gravity change. The constructive comments from reviewers helped to improve the paper. NR 13 TC 27 Z9 33 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 9 PY 2010 VL 37 AR L23307 DI 10.1029/2010GL045449 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 693WE UT WOS:000285255300003 ER PT J AU Herman, JR AF Herman, Jay R. TI Use of an improved radiation amplification factor to estimate the effect of total ozone changes on action spectrum weighted irradiances and an instrument response function SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ULTRAVIOLET-B RADIATION; VITAMIN-D PRODUCTION; DEPLETION; SKIN; SUNLIGHT; UVB; WAVELENGTHS; INDUCTION; HUMANS; CANCER AB Multiple scattering radiative transfer results are used to calculate action spectrum weighted irradiances and fractional irradiance changes in terms of a power law in ozone Omega, U(Omega/200)(-RAF), where the new radiation amplification factor (RAF) is just a function of solar zenith angle. Including Rayleigh scattering caused small differences in the estimated 30 year changes in action spectrum-weighted irradiances compared to estimates that neglect multiple scattering. The radiative transfer results are applied to several action spectra and to an instrument response function corresponding to the Solar Light 501 meter. The effect of changing ozone on two plant damage action spectra are shown for plants with high sensitivity to UVB (280-315 nm) and those with lower sensitivity, showing that the probability for plant damage for the latter has increased since 1979, especially at middle to high latitudes in the Southern Hemisphere. Similarly, there has been an increase in rates of erythemal skin damage and pre-vitamin D-3 production corresponding to measured ozone decreases. An example conversion function is derived to obtain erythemal irradiances and the UV index from measurements with the Solar Light 501 instrument response function. An analytic expressions is given to convert changes in erythemal irradiances to changes in CIE vitamin-D action spectrum weighted irradiances. C1 [Herman, Jay R.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD USA. RP Herman, JR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jay.r.herman@nasa.gov OI Herman, Jay/0000-0002-9146-1632 NR 49 TC 8 Z9 8 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 9 PY 2010 VL 115 AR D23119 DI 10.1029/2010JD014317 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 693XC UT WOS:000285257700003 ER PT J AU Abbasi, R Abdou, Y Abu-Zayyad, T Adams, J Aguilar, JA Ahlers, M Andeen, K Auffenberg, J Bai, X Baker, M Barwick, SW Bay, R Alba, JLB Beattie, K Beatty, JJ Bechet, S Becker, JK Becker, KH Benabderrahmane, ML BenZvi, S Berdermann, J Berghaus, P Berley, D Bernardini, E Bertrand, D Besson, DZ Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Braun, J Buitink, S Carson, M Chirkin, D Christy, B Clem, J Clevermann, F Cohen, S Colnard, C Cowen, DF D'Agostino, MV Danninger, M Davis, JC De Clercq, C Demirors, L Depaepe, O Descamps, F Desiati, P de Vries-Uiterweerd, G DeYoung, T Diaz-Velez, JC Dierckxsens, M Dreyer, J Dumm, JP Duvoort, MR Ehrlich, R Eisch, J Ellsworth, RW Engdegard, O Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feusels, T Filimonov, K Finley, C Foerster, MM Fox, BD Franckowiak, A Franke, R Gaisser, TK Gallagher, J Geisler, M Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Goodman, JA Grant, D Griesel, T Gross, A Grullon, S Gurtner, M Ha, C Hallgren, A Halzen, F Han, K Hanson, K Helbing, K Herquet, P Hickford, S Hill, GC Hoffman, KD Homeier, A Hoshina, K Hubert, D Huelsnitz, W Hulss, JP Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobsen, J Japaridze, GS Johansson, H Joseph, JM Kampert, KH Kappes, A Karg, T Karle, A Kelley, JL Kemming, N Kenny, P Kiryluk, J Kislat, F Klein, SR Koehne, JH Kohnen, G Kolanoski, H Kopke, L Koskinen, DJ Kowalski, M Kowarik, T Krasberg, M Krings, T Kroll, G Kuehn, K Kuwabara, T Labare, M Lafebre, S Laihem, K Landsman, H Larson, MJ Lauer, R Lehmann, R Lunemann, J Madsen, J Majumdar, P Marotta, A Maruyama, R Mase, K Matis, HS Matusik, M Meagher, K Merck, M Meszaros, P Meures, T Middell, E Milke, N Miller, J Montaruli, T Morse, R Movit, SM Nahnhauer, R Nam, JW Naumann, U Niessen, P Nygren, DR Odrowski, S Olivas, A Olivo, M O'Murchadha, A Ono, M Panknin, S Paul, L de los Heros, CP Petrovic, J Piegsa, A Pieloth, D Porrata, R Posselt, J Price, PB Prikockis, M Przybylski, GT Rawlins, K Redl, P Resconi, E Rhode, W Ribordy, M Rizzo, A Rodrigues, JP Roth, P Rothmaier, F Rott, C Ruhe, T Rutledge, D Ruzybayev, B Ryckbosch, D Sander, HG Santander, M Sarkar, S Schatto, K Schlenstedt, S Schmidt, T Schukraft, A Schultes, A Schulz, O Schunck, M Seckel, D Semburg, B Seo, SH Sestayo, Y Seunarine, S Silvestri, A Singh, K Slipak, A Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stephens, G Stezelberger, T Stokstad, RG Stoyanov, S Strahler, EA Straszheim, T Sullivan, GW Swillens, Q Taavola, H Taboada, I Tamburro, A Tarasova, O Tepe, A Ter-Antonyan, S Tilav, S Toale, PA Toscano, S Tosi, D Turcan, D van Eijndhoven, N Vandenbroucke, J Van Overloop, A van Santen, J Voge, M Voigt, B Walck, C Waldenmaier, T Wallraff, M Walter, M Weaver, C Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Wikstrom, G Williams, DR Wischnewski, R Wissing, H Wolf, M Woschnagg, K Xu, C Xu, XW Yodh, G Yoshida, S Zarzhitsky, P AF Abbasi, R. Abdou, Y. Abu-Zayyad, T. Adams, J. Aguilar, J. A. Ahlers, M. Andeen, K. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Bay, R. Alba, J. L. Bazo Beattie, K. Beatty, J. J. Bechet, S. Becker, J. K. Becker, K. -H. Benabderrahmane, M. L. BenZvi, S. Berdermann, J. Berghaus, P. Berley, D. Bernardini, E. Bertrand, D. Besson, D. Z. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Braun, J. Buitink, S. Carson, M. Chirkin, D. Christy, B. Clem, J. Clevermann, F. Cohen, S. Colnard, C. Cowen, D. F. D'Agostino, M. V. Danninger, M. Davis, J. C. De Clercq, C. Demiroers, L. Depaepe, O. Descamps, F. Desiati, P. de Vries-Uiterweerd, G. DeYoung, T. Diaz-Velez, J. C. Dierckxsens, M. Dreyer, J. Dumm, J. P. Duvoort, M. R. Ehrlich, R. Eisch, J. Ellsworth, R. W. Engdegard, O. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feusels, T. Filimonov, K. Finley, C. Foerster, M. M. Fox, B. D. Franckowiak, A. Franke, R. Gaisser, T. K. Gallagher, J. Geisler, M. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Goodman, J. A. Grant, D. Griesel, T. Gross, A. Grullon, S. Gurtner, M. Ha, C. Hallgren, A. Halzen, F. Han, K. Hanson, K. Helbing, K. Herquet, P. Hickford, S. Hill, G. C. Hoffman, K. D. Homeier, A. Hoshina, K. Hubert, D. Huelsnitz, W. Huelss, J. -P. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobsen, J. Japaridze, G. S. Johansson, H. Joseph, J. M. Kampert, K. -H. Kappes, A. Karg, T. Karle, A. Kelley, J. L. Kemming, N. Kenny, P. Kiryluk, J. Kislat, F. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Koskinen, D. J. Kowalski, M. Kowarik, T. Krasberg, M. Krings, T. Kroll, G. Kuehn, K. Kuwabara, T. Labare, M. Lafebre, S. Laihem, K. Landsman, H. Larson, M. J. Lauer, R. Lehmann, R. Luenemann, J. Madsen, J. Majumdar, P. Marotta, A. Maruyama, R. Mase, K. Matis, H. S. Matusik, M. Meagher, K. Merck, M. Meszaros, P. Meures, T. Middell, E. Milke, N. Miller, J. Montaruli, T. Morse, R. Movit, S. M. Nahnhauer, R. Nam, J. W. Naumann, U. Niessen, P. Nygren, D. R. Odrowski, S. Olivas, A. Olivo, M. O'Murchadha, A. Ono, M. Panknin, S. Paul, L. de los Heros, C. Perez Petrovic, J. Piegsa, A. Pieloth, D. Porrata, R. Posselt, J. Price, P. B. Prikockis, M. Przybylski, G. T. Rawlins, K. Redl, P. Resconi, E. Rhode, W. Ribordy, M. Rizzo, A. Rodrigues, J. P. Roth, P. Rothmaier, F. Rott, C. Ruhe, T. Rutledge, D. Ruzybayev, B. Ryckbosch, D. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Schlenstedt, S. Schmidt, T. Schukraft, A. Schultes, A. Schulz, O. Schunck, M. Seckel, D. Semburg, B. Seo, S. H. Sestayo, Y. Seunarine, S. Silvestri, A. Singh, K. Slipak, A. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stephens, G. Stezelberger, T. Stokstad, R. G. Stoyanov, S. Strahler, E. A. Straszheim, T. Sullivan, G. W. Swillens, Q. Taavola, H. Taboada, I. Tamburro, A. Tarasova, O. Tepe, A. Ter-Antonyan, S. Tilav, S. Toale, P. A. Toscano, S. Tosi, D. Turcan, D. van Eijndhoven, N. Vandenbroucke, J. Van Overloop, A. van Santen, J. Voge, M. Voigt, B. Walck, C. Waldenmaier, T. Wallraff, M. Walter, M. Weaver, Ch. Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Wikstroem, G. Williams, D. R. Wischnewski, R. Wissing, H. Wolf, M. Woschnagg, K. Xu, C. Xu, X. W. Yodh, G. Yoshida, S. Zarzhitsky, P. CA IceCube Collaboration TI Search for a Lorentz-violating sidereal signal with atmospheric neutrinos in IceCube SO PHYSICAL REVIEW D LA English DT Article AB A search for sidereal modulation in the flux of atmospheric muon neutrinos in IceCube was performed. Such a signal could be an indication of Lorentz-violating physics. Neutrino oscillation models, derivable from extensions to the standard model, allow for neutrino oscillations that depend on the neutrino's direction of propagation. No such direction-dependent variation was found. A discrete Fourier transform method was used to constrain the Lorentz and CPT-violating coefficients in one of these models. Because of the unique high energy reach of IceCube, it was possible to improve constraints on certain Lorentz-violating oscillations by 3 orders of magnitude with respect to limits set by other experiments. C1 [Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Geisler, M.; Gluesenkamp, T.; Huelss, J. -P.; Krings, T.; Laihem, K.; Meures, T.; Paul, L.; Schukraft, A.; Schunck, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Williams, D. R.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Beattie, K.; Buitink, S.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Kappes, A.; Kemming, N.; Kolanoski, H.; Lehmann, R.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Becker, J. K.; Dreyer, J.; Fedynitch, A.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados. [Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Petrovic, J.; Swillens, Q.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium. [Bose, D.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Singh, K.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Adams, J.; Gross, A.; Han, K.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Kuehn, K.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Grant, D.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Subat & Radiat Phys, B-9000 Ghent, Belgium. [Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Voge, M.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany. [Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Besson, D. Z.; Kenny, P.; Koskinen, D. J.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Berghaus, P.; Braun, J.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Kelley, J. L.; Krasberg, M.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wikstroem, G.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Wikstroem, G.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; Olivo, M.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Duvoort, M. R.] Univ Utrecht, Dept Phys & Astron, SRON, NL-3584 CC Utrecht, Netherlands. [Auffenberg, J.; Becker, K. -H.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Matusik, M.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schlenstedt, S.; Spiering, C.; Tarasova, O.; Tosi, D.; Voigt, B.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany. [Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Huelsnitz, W (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA. EM whuelsnitz@icecube.umd.edu RI Taavola, Henric/B-4497-2011; Wiebusch, Christopher/G-6490-2012; Kowalski, Marek/G-5546-2012; Tamburro, Alessio/A-5703-2013; Botner, Olga/A-9110-2013; Hallgren, Allan/A-8963-2013; Tjus, Julia/G-8145-2012; Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; OI Taavola, Henric/0000-0002-2604-2810; Wiebusch, Christopher/0000-0002-6418-3008; Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Actis, Oxana/0000-0001-8851-3983; Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft, Anne/0000-0002-9112-5479; Perez de los Heros, Carlos/0000-0002-2084-5866; Buitink, Stijn/0000-0002-6177-497X; Carson, Michael/0000-0003-0400-7819; Hubert, Daan/0000-0002-4365-865X; Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886 FU U.S. National Science Foundation-Office of Polar Programs; U.S. National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW) at the University of Wisconsin-Madison; Open Science Grid (OSG); U.S. Department of Energy, and National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI); National Science and Engineering Research Council of Canada; Swedish Research Council; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; EU; Capes Foundation, Ministry of Education of Brazil; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden FX We acknowledge support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; National Science and Engineering Research Council of Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; A. Gross acknowledges support by the EU Marie Curie OIF Program; J. P. Rodrigues acknowledges support by the Capes Foundation, Ministry of Education of Brazil. NR 29 TC 44 Z9 44 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD DEC 9 PY 2010 VL 82 IS 11 AR 112003 DI 10.1103/PhysRevD.82.112003 PG 6 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 711DC UT WOS:000286566200001 ER PT J AU Bounoua, L Hall, FG Sellers, PJ Kumar, A Collatz, GJ Tucker, CJ Imhoff, ML AF Bounoua, L. Hall, F. G. Sellers, P. J. Kumar, A. Collatz, G. J. Tucker, C. J. Imhoff, M. L. TI Quantifying the negative feedback of vegetation to greenhouse warming: A modeling approach SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID DOUBLED ATMOSPHERIC CO2; CLIMATE-CHANGE; CARBON-DIOXIDE; NDVI DATA; NITROGEN; RUNOFF; WATER AB Several climate models indicate that in a 2 x CO(2) environment, temperature and precipitation would increase and runoff would increase faster than precipitation. These models, however, did not allow the vegetation to increase its leaf density as a response to the physiological effects of increased CO2 and consequent changes in climate. Other assessments included these interactions but did not account for the vegetation down-regulation to reduce plant's photosynthetic activity and as such resulted in a weak vegetation negative response. When we combine these interactions in climate simulations with 2 x CO(2), the associated increase in precipitation contributes primarily to increase evapotranspiration rather than surface runoff, consistent with observations, and results in an additional cooling effect not fully accounted for in previous simulations with elevated CO(2). By accelerating the water cycle, this feedback slows but does not alleviate the projected warming, reducing the land surface warming by 0.6 degrees C. Compared to previous studies, these results imply that long term negative feedback from CO(2)-induced increases in vegetation density could reduce temperature following a stabilization of CO(2) concentration. Citation: Bounoua, L., F. G. Hall, P. J. Sellers, A. Kumar, G. J. Collatz, C. J. Tucker, and M. L. Imhoff (2010), Quantifying the negative feedback of vegetation to greenhouse warming: A modeling approach, Geophys. Res. Lett., 37, L23701, doi: 10.1029/2010GL045338. C1 [Bounoua, L.; Hall, F. G.; Collatz, G. J.; Tucker, C. J.; Imhoff, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kumar, A.] NOAA, Climate Predict Ctr, Camp Springs, MD 20746 USA. [Sellers, P. J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Hall, F. G.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Bounoua, L (reprint author), NASA, Goddard Space Flight Ctr, Code 614-4, Greenbelt, MD 20771 USA. EM lahouari.bounoua@nasa.gov; forrest.g.hall@nasa.gov; piers.j.sellers@nasa.gov; arun.kumar@noaa.gov; george.j.collatz@nasa.gov; compton.j.tucker@nasa.gov; marc.l.imhoff@nasa.gov RI collatz, george/D-5381-2012 FU NASA FX We thank R. Betts for his insightful remarks. The work was partially supported by the NASA's LCLUC-program. NR 22 TC 25 Z9 25 U1 0 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 DEC 7 PY 2010 VL 37 AR L23701 DI 10.1029/2010GL045338 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 693WC UT WOS:000285255100001 ER PT J AU Loeffler, MJ Baragiola, RA AF Loeffler, M. J. Baragiola, R. A. TI Photolysis of solid NH3 and NH3-H2O mixtures at 193 nm SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MU-M BAND; ICY SATELLITES; WATER ICE; TRAILING HEMISPHERES; INFRARED-SPECTRUM; SOLAR-SYSTEM; AMMONIA; ENCELADUS; SPECTROSCOPY; ULTRAVIOLET AB We have studied UV photolysis of solid ammonia and ammonia-dihydrate samples at 40 K, using infrared spectroscopy, mass spectrometry, and microgravimetry. We have shown that in the pure NH3 sample, the main species ejected are NH3, H-2, and N-2, where the hydrogen and nitrogen increase with laser fluence. This increase in N-2 ejection with laser fluence explains the increase in mass loss rate detected by a microbalance. In contrast, for the ammonia-water mixture, we see very weak signals of H-2 and N-2 in the mass spectrometer, consistent with the very small mass loss during the experiment and with a <5% decrease in the NH3 infrared absorption bands spectroscopy after a fluence of similar to 3 x 10(19) photons/cm(2). The results imply that ammonia-ice mixtures in the outer solar system are relatively stable under solar irradiation. (C) 2010 American Institute of Physics. [doi:10.1063/1.3506577] C1 [Loeffler, M. J.; Baragiola, R. A.] Univ Virginia, Lab Atom & Surface Phys Engn Phys, Charlottesville, VA 22904 USA. [Loeffler, M. J.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. RP Baragiola, RA (reprint author), Univ Virginia, Lab Atom & Surface Phys Engn Phys, Charlottesville, VA 22904 USA. EM raul@virginia.edu RI Loeffler, Mark/C-9477-2012 FU NASA [NNX07AL48G, NNX08AMB6G] FX This work was supported by NASA Grant Nos. NNX07AL48G (Outer Planet Research) and NNX08AMB6G (Planetary Geology and Geophysics). NR 47 TC 7 Z9 7 U1 2 U2 19 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 7 PY 2010 VL 133 IS 21 AR 214506 DI 10.1063/1.3506577 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 692NL UT WOS:000285159400013 PM 21142307 ER PT J AU Kahn, RA Gaitley, BJ Garay, MJ Diner, DJ Eck, TF Smirnov, A Holben, BN AF Kahn, Ralph A. Gaitley, Barbara J. Garay, Michael J. Diner, David J. Eck, Thomas F. Smirnov, Alexander Holben, Brent N. TI Multiangle Imaging SpectroRadiometer global aerosol product assessment by comparison with the Aerosol Robotic Network SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MATTER COMPONENT CONCENTRATIONS; REMOTE-SENSING OBSERVATIONS; SKY RADIANCE MEASUREMENTS; OPTICAL-PROPERTIES; SIZE DISTRIBUTIONS; RADIOMETRIC CALIBRATION; SOUTHERN AFRICA; DUST AEROSOLS; DRY SEASON; IN-SITU AB A statistical approach is used to assess the quality of the Multiangle Imaging SpectroRadiometer (MISR) version 22 (V22) aerosol products. Aerosol optical depth (AOD) retrieval results are improved relative to the early postlaunch values reported by [Kahn et al. (2005)], which varied with particle type category. Overall, about 70% to 75% of MISR AOD retrievals fall within 0.05 or 20% x AOD of the paired validation data from the Aerosol Robotic Network (AERONET), and about 50% to 55% are within 0.03 or 10% x AERONET AOD, except at sites where dust or mixed dust and smoke are commonly found. Retrieved particle microphysical properties amount to categorical values, such as three size groupings: "small," "medium," and "large." For particle size, ground-based AERONET sun photometer Angstrom exponents are used to assess statistically the corresponding MISR values, which are interpreted in terms of retrieved size categories. Coincident single-scattering albedo (SSA) and fraction AOD spherical data are too limited for statistical validation. V22 distinguishes two or three size bins, depending on aerosol type, and about two bins in SSA (absorbing vs. nonabsorbing), as well as spherical vs. nonspherical particles, under good retrieval conditions. Particle type sensitivity varies considerably with conditions and is diminished for midvisible AODs below about 0.15 or 0.2. On the basis of these results, specific algorithm upgrades are proposed and are being investigated by the MISR team for possible implementation in future versions of the product. C1 [Kahn, Ralph A.; Holben, Brent N.] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gaitley, Barbara J.; Diner, David J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eck, Thomas F.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Garay, Michael J.] Raytheon Co, Pasadena, CA 91101 USA. [Smirnov, Alexander] Sigma Space Corp, Lanham, MD 20706 USA. RP Kahn, RA (reprint author), NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ralph.kahn@nasa.gov RI Smirnov, Alexander/C-2121-2009; ECK, THOMAS/D-7407-2012; Kahn, Ralph/D-5371-2012 OI Smirnov, Alexander/0000-0002-8208-1304; Kahn, Ralph/0000-0002-5234-6359 FU NASA; EOS-MISR project FX We thank our colleagues on the Jet Propulsion Laboratory's MISR instrument team and at the NASA Langley Research Center's Atmospheric Sciences Data Center for their roles in producing the MISR data sets and Susan Paradise for contributions to Figure 4 and related discussion of over-water retrievals. We also thank the AERONET principal investigators for contributing to the global aerosol database, as well as Lorraine Remer and two anonymous reviewers for helpful comments on the manuscript. The work of R. Kahn is supported in part by NASA's Climate and Radiation Research and Analysis Program, under H. Maring, NASA's Atmospheric Composition Program, and the EOS-MISR project. NR 66 TC 168 Z9 168 U1 5 U2 33 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 7 PY 2010 VL 115 AR D23209 DI 10.1029/2010JD014601 PG 28 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 693WX UT WOS:000285257200006 ER PT J AU Barry, MA Boudreau, BP Johnson, BD Reed, AH AF Barry, M. A. Boudreau, B. P. Johnson, B. D. Reed, A. H. TI First-order description of the mechanical fracture behavior of fine-grained surficial marine sediments during gas bubble growth SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID ECKERNFORDE BAY; MUDDY SEDIMENTS; METHANE; POCKMARKS; GELATIN; ASCENT; CRACK; SOIL AB Bubbles in sediments, imaged via Computed Tomography (CT) scanning, and in surrogate transparent material (gelatin), are well-described geometrically as eccentric oblate spheroids. While sediments are undoubtedly visco-elasto-plastic solids, only part of that complex behavior appears to influence significantly the formation and shape of gas bubbles. Specifically, the shape of these bubbles can be explained if the mechanical response of fine-grained sediment is approximated by Linear Elastic Fracture Mechanics (LEFM). To determine the adequacy of the LEFM approximation for gas bubble growth in fine-grained sediments, a number of gas bubbles were injected and grown in natural sediments, while monitoring the size and shape using an industrial CT scanner. A comparison of measured inverse aspect ratios (IARs) of the injected bubbles with calculated IARs from pressure records provides support for the LEFM theory. Deviations from LEFM are observable in the data, but as bubbles grow larger they trend more closely toward the theory. The use of LEFM has been shown to describe gas bubble growth in shallow coastal sediments to first order. C1 [Barry, M. A.; Boudreau, B. P.; Johnson, B. D.] Dalhousie Univ, Dept Oceanog, Halifax, NS B3H 4J1, Canada. [Reed, A. H.] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. RP Barry, MA (reprint author), Dalhousie Univ, Dept Oceanog, 1355 Oxford St, Halifax, NS B3H 4J1, Canada. EM barrym@dal.ca FU US Office of Naval Research [N00014-05-1-175, N00014-08-1-0818]; NSERC; NRL [0601153N] FX We gratefully acknowledge support for this work by the US Office of Naval Research under Grants N00014-05-1-175 and N00014-08-1-0818 and a NSERC Discovery Grant to BPB. The CT-scanning work was also supported by NRL Base Funding, PE#0601153N. We thank the anonymous reviewers for their critical, but enlightening comments. NR 33 TC 16 Z9 16 U1 2 U2 12 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 DEC 7 PY 2010 VL 115 AR F04029 DI 10.1029/2010JF001833 PG 10 WC Geosciences, Multidisciplinary SC Geology GA 693XL UT WOS:000285258600001 ER PT J AU Garcia-Garcia, D Chao, BF Boy, JP AF Garcia-Garcia, D. Chao, B. F. Boy, J. -P. TI Steric and mass-induced sea level variations in the Mediterranean Sea revisited SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID TIME-VARIABLE GRAVITY; GRACE MEASUREMENTS; VARIABILITY; SYSTEM; REANALYSIS; ALTIMETRY; FIELD AB The total sea level variation (SLV) is the combination of steric and mass-induced SLV, whose exact shares are key to understanding the oceanic response to climate system changes. Total SLV can be observed by radar altimetry satellites such as TOPEX/POSEIDON and Jason 1/2. The steric SLV can be computed through temperature and salinity profiles from in situ measurements or from ocean general circulation models (OGCM), which can assimilate the said observations. The mass-induced SLV can be estimated from its time-variable gravity (TVG) signals. We revisit this problem in the Mediterranean Sea estimating the observed, steric, and mass-induced SLV, for the latter we analyze the latest TVG data set from the GRACE (Gravity Recovery and Climate Experiment) satellite mission launched in 2002, which is 3.5 times longer than in previous studies, with the application of a two-stage anisotropic filter to reduce the noise in high-degree and -order spherical harmonic coefficients. We confirm that the intra-annual total SLV are only produced by water mass changes, a fact explained in the literature as a result of the wind field around the Gibraltar Strait. The steric SLV estimated from the residual of "altimetry minus GRACE" agrees in phase with that estimated from OGCMs and in situ measurements, although showing a higher amplitude. The net water fluxes through both the straits of Gibraltar and Sicily have also been estimated accordingly. C1 [Garcia-Garcia, D.] Univ Alicante, Space Geodesy Lab, Dept Appl Math, EPS, E-03080 Alicante, Spain. [Chao, B. F.] Acad Sinica, Inst Earth Sci, Taipei 11529, Taiwan. [Boy, J. -P.] Univ Strasbourg, CNRS, IPGS, EOST,UMR 7516, F-67084 Strasbourg, France. [Boy, J. -P.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Garcia-Garcia, D (reprint author), Univ Alicante, Space Geodesy Lab, Dept Appl Math, EPS, POB 99, E-03080 Alicante, Spain. EM d.garcia@ua.es RI Garcia-Garcia, David/L-7535-2014; Chao, Benjamin Fong/N-6156-2013; Boy, Jean-Paul/E-6677-2017 OI Garcia-Garcia, David/0000-0002-7273-9037; Boy, Jean-Paul/0000-0003-0259-209X FU Marie Curie International Outgoing Fellowship [PIOF-GA-2008-221753]; MICIN [ESP2006-11357, AYA2009-07981]; Generalitat Valenciana [ACOMP2009/031] FX We thank the organizations providing the data used in this study and the very helpful comments of two anonymous reviewers. This work was elaborated during the stay of the first author at the National Central University of Taiwan, thanks to a grant from the Generalitat Valenciana, Spain. Jean-Paul Boy is currently visiting NASA Goddard Space Flight Center, with a Marie Curie International Outgoing Fellowship (PIOF-GA-2008-221753). This work was partly funded by two Spanish projects from MICIN, ESP2006-11357, and AYA2009-07981 and one from Generalitat Valenciana (ACOMP2009/031). NR 53 TC 10 Z9 10 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC 7 PY 2010 VL 115 AR C12016 DI 10.1029/2009JC005928 PG 14 WC Oceanography SC Oceanography GA 693XP UT WOS:000285259000001 ER PT J AU Connaughton, V Briggs, MS Holzworth, RH Hutchins, ML Fishman, GJ Wilson-Hodge, CA Chaplin, VL Bhat, PN Greiner, J von Kienlin, A Kippen, RM Meegan, CA Paciesas, WS Preece, RD Cramer, E Dwyer, JR Smith, DM AF Connaughton, V. Briggs, M. S. Holzworth, R. H. Hutchins, M. L. Fishman, G. J. Wilson-Hodge, C. A. Chaplin, V. L. Bhat, P. N. Greiner, J. von Kienlin, A. Kippen, R. M. Meegan, C. A. Paciesas, W. S. Preece, R. D. Cramer, E. Dwyer, J. R. Smith, D. M. TI Associations between Fermi Gamma-ray Burst Monitor terrestrial gamma ray flashes and sferics from the World Wide Lightning Location Network SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ELECTRONS; SPRITES AB We report on a search for correlations between terrestrial gamma ray flashes (TGFs) detected by the Fermi Gamma-ray Burst Monitor (GBM) and lightning strokes measured using the World Wide Lightning Location Network (WWLLN). We associate 15 of a total 50 GBM-detected TGFs with individual discharges. We establish the relative timing between the TGF and the lightning stroke to an accuracy of <50 mu s, and find that in 13 of these 15 lightning-TGF associations, the lightning stroke and the peak of the TGF are simultaneous to similar to 40 mu s. This suggests that a large fraction of TGFs are coincident with lightning discharges. The two nonsimultaneous associations do not show a consistent TGF-lightning stroke temporal sequence. All 15 associations are with sferics within 300 km of the subspacecraft position. For those TGFs not correlated with a particular lightning stroke, we find storm activity within 300 km of the subspacecraft position in all but four of the TGFs. For three of these four TGFs, we find storm activity very close to one of the magnetic footprints of the spacecraft position. We associate the subspacecraft TGFs with gamma ray events and the footprint events with electrons traveling along magnetic field lines before hitting the Fermi spacecraft. C1 [Connaughton, V.; Briggs, M. S.; Chaplin, V. L.; Bhat, P. N.; Paciesas, W. S.; Preece, R. D.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA. [Cramer, E.; Dwyer, J. R.] Florida Inst Technol, Melbourne, FL 32901 USA. [Fishman, G. J.; Wilson-Hodge, C. A.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Greiner, J.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Holzworth, R. H.; Hutchins, M. L.] Univ Washington, Seattle, WA 98195 USA. [Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Smith, D. M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Paciesas, W. S.; Preece, R. D.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Meegan, C. A.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. RP Connaughton, V (reprint author), Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM bobholz@ess.washington.edu; jerry.fishman@nasa.gov; valerie@nasa.gov; azk@mpe.mpg.de; mkippen@lanl.gov; jdwyer@fit.edu; dsmith@scipp.ucsc.edu OI Preece, Robert/0000-0003-1626-7335 NR 27 TC 46 Z9 46 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 7 PY 2010 VL 115 AR A12307 DI 10.1029/2010JA015681 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 693WJ UT WOS:000285255800003 ER PT J AU Verkhoglyadova, OP Li, G Zank, GP Hu, Q Cohen, CMS Mewaldt, RA Mason, GM Haggerty, DK von Rosenvinge, TT Looper, MD AF Verkhoglyadova, O. P. Li, G. Zank, G. P. Hu, Q. Cohen, C. M. S. Mewaldt, R. A. Mason, G. M. Haggerty, D. K. von Rosenvinge, T. T. Looper, M. D. TI Understanding large SEP events with the PATH code: Modeling of the 13 December 2006 SEP event SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ENERGETIC PARTICLE EVENTS; EJECTION-DRIVEN SHOCKS; INTERPLANETARY TRAVELING SHOCKS; HYDROMAGNETIC WAVE EXCITATION; RANKINE-HUGONIOT PROBLEM; ADIABATIC DECELERATION; ISOTOPE SPECTROMETER; STRUCTURES RELEVANT; ION-ACCELERATION; SPACE WEATHER AB The Particle Acceleration and Transport in the Heliosphere (PATH) numerical code was developed to understand solar energetic particle (SEP) events in the near-Earth environment. We discuss simulation results for the 13 December 2006 SEP event. The PATH code includes modeling a background solar wind through which a CME-driven oblique shock propagates. The code incorporates a mixed population of both flare and shock-accelerated solar wind suprathermal particles. The shock parameters derived from ACE measurements at 1 AU and observational flare characteristics are used as input into the numerical model. We assume that the diffusive shock acceleration mechanism is responsible for particle energization. We model the subsequent transport of particles originated at the flare site and particles escaping from the shock and propagating in the equatorial plane through the interplanetary medium. We derive spectra for protons, oxygen, and iron ions, together with their time-intensity profiles at 1 AU. Our modeling results show reasonable agreement with in situ measurements by ACE, STEREO, GOES, and SAMPEX for this event. We numerically estimate the Fe/O abundance ratio and discuss the physics underlying a mixed SEP event. We point out that the flare population is as important as shock geometry changes during shock propagation for modeling time-intensity profiles and spectra at 1 AU. The combined effects of seed population and shock geometry will be examined in the framework of an extended PATH code in future modeling efforts. C1 [Verkhoglyadova, O. P.; Li, G.; Zank, G. P.; Hu, Q.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Cohen, C. M. S.; Mewaldt, R. A.] CALTECH, Pasadena, CA 91125 USA. [Mason, G. M.; Haggerty, D. K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Li, G.; Zank, G. P.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Looper, M. D.] Aerosp Corp, Los Angeles, CA 90009 USA. [von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Verkhoglyadova, OP (reprint author), Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. EM olga.verkhoglyadova@jpl.nasa.gov RI Li, Gang/B-4977-2012; OI Li, Gang/0000-0003-4695-8866; Verkhoglyadova, Olga/0000-0002-9295-9539 FU NASA [NNX06AC21G, NNG04GF83G, NNG05GH38G, NNG05GM62G, NNX07AN45G]; NSF [ATM0317509, ATM0428880] FX This work is supported in part by NASA grants NNX06AC21G, NNG04GF83G, NNG05GH38G, NNG05GM62G, and NNX07AN45G (for the EPAM and ULEIS work at APL) and NSF grants ATM0317509 and ATM0428880. NR 52 TC 37 Z9 38 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 DEC 7 PY 2010 VL 115 AR A12103 DI 10.1029/2010JA015615 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 693WJ UT WOS:000285255800002 ER PT J AU Killen, RM Potter, AE Hurley, DM Plymate, C Naidu, S AF Killen, R. M. Potter, A. E. Hurley, D. M. Plymate, C. Naidu, S. TI Observations of the lunar impact plume from the LCROSS event SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SODIUM; VAPOR AB We observed emission from sodium (Na) ejected from the Lunar Crater Observing and Sensing Satellite (LCROSS) impact into Cabeus Crater on October 9, 2009, using the McMath-Pierce telescope. In our 88 km(2) field of view, we saw on the order of 2 g of Na in the first 9 minutes after the LCROSS impact. A comparison of our observed Na above the limb with simulations that assume a gas temperature of 1000 K indicates that 0.5 - 2.6 (1.5 +/- 1) kg of Na were released during the LCROSS impact. Lower temperatures would result in a lower total sodium release. The model of an isotropic expanding cloud best reproduces the observations. Citation: Killen, R. M., A. E. Potter, D. M. Hurley, C. Plymate, and S. Naidu (2010), Observations of the lunar impact plume from the LCROSS event, Geophys. Res. Lett., 37, L23201, doi:10.1029/2010GL045508. C1 [Killen, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hurley, D. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Naidu, S.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Potter, A. E.; Plymate, C.] Natl Solar Observ, Tucson, AZ 85719 USA. RP Killen, RM (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA. EM rosemary.killen@nasa.gov RI Killen, Rosemary/E-7127-2012 FU NASA FX This research was supported by NASA under a grant to the DREAM Team of the NASA Lunar Science Institute. Observations were obtained at the McMath Pierce Solar Telescope on Kitt Peak, Arizona, operated by the National Solar Observatory under agreement with the National Science Foundation. NR 13 TC 13 Z9 13 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 4 PY 2010 VL 37 AR L23201 DI 10.1029/2010GL045508 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 690OY UT WOS:000285015300003 ER PT J AU Landerer, FW Dickey, JO Guntner, A AF Landerer, Felix W. Dickey, Jean O. Guentner, Andreas TI Terrestrial water budget of the Eurasian pan-Arctic from GRACE satellite measurements during 2003-2009 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GLOBAL HYDROLOGICAL MODEL; TIME-VARIABLE GRAVITY; EASTERN SIBERIA; FRESH-WATER; PRECIPITATION; VARIABILITY; STORAGE; SYSTEM; TEMPERATURES; PERMAFROST AB We assess the controls of the terrestrial water budget over the Eurasian pan-Arctic drainage region from 2003 to 2009 by combining observations from the Gravity Recovery and Climate Experiment (GRACE) with reanalysis estimates of net precipitation and observations of river discharge from gauges. Of particular interest are the expansive permafrost regions. Thawing permafrost has been implicated to contribute to the observed discharge increases through the melting of excess ground ice. We show that terrestrial water storage (TWS) over large areas of the Eurasian pan-Arctic region has increased during 2003-2009. However, significant interannual TWS variability is present and most TWS increases occur over nonpermafrost regions in the Ob and Yenisei basins. Over the central Lena basin, which is mostly underlain by permafrost, TWS steadily increased until 2007 but has slightly declined since. By combining GRACE observations of TWS anomalies with discharge and net precipitation, we show that the terrestrial water budget is at least qualitatively closed over the Eurasian Arctic basins. The observed TWS and discharge increases over the study time period were driven by increased atmospheric moisture fluxes. Therefore, we conclude that melting of excess ground ice in permafrost regions did not act as a source to observed changes in discharge. Nonetheless, the signature of significant TWS increases points to ongoing thickening of the active layer in particular over the discontinuous permafrost regions in the central Lena basin. C1 [Landerer, Felix W.; Dickey, Jean O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Guentner, Andreas] GFZ German Res Ctr Geosci, Helmholtz Ctr Potsdam, D-14473 Potsdam, Germany. RP Landerer, FW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 238-600, Pasadena, CA 91109 USA. EM landerer@jpl.nasa.gov RI Guntner, Andreas/C-9892-2011; OI Guntner, Andreas/0000-0001-6233-8478; Landerer, Felix/0000-0003-2678-095X FU NASA at Jet Propulsion Laboratory; National Aeronautics and Space Administration (NASA) FX We acknowledge many productive conversations with D. Bromwich and M. Serreze. We thank three reviewers for their constructive comments that helped us to improve the paper and V. Zlotnicki and M. Watkins for support with the GRACE data and discussions. Permafrost data come from NSIDC (http://nsidc.org/data/ggd318. html [Brown et al., 1998]), discharge observations come from the ArcticRIMS project (http://rims.unh.edu/data.shtml), and J. Alcamo and P. Doll are acknowledged for providing the WGHM model. F. W. L. was supported through the NASA Postdoctoral Program at Jet Propulsion Laboratory. This paper presents the results of one phase of research carried out at the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the National Aeronautics and Space Administration (NASA). NR 60 TC 29 Z9 32 U1 2 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 4 PY 2010 VL 115 AR D23115 DI 10.1029/2010JD014584 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 690PU UT WOS:000285017500009 ER PT J AU Huang, SY Zhou, M Sahraoui, F Deng, XH Pang, Y Yuan, ZG Wei, Q Wang, JF Zhou, XM AF Huang, S. Y. Zhou, M. Sahraoui, F. Deng, X. H. Pang, Y. Yuan, Z. G. Wei, Q. Wang, J. F. Zhou, X. M. TI Wave properties in the magnetic reconnection diffusion region with high beta: Application of the k-filtering method to Cluster multispacecraft data SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS MAGNETOSPHERE; PLASMA-WAVES; MAGNETOPAUSE; IDENTIFICATION; TURBULENCE; CHALLENGE; ELECTRON AB Magnetic reconnection is a crucial physical process in laboratory and astrophysical plasmas. Plasma waves are believed to provide the dissipation mechanism in magnetic reconnection. In this paper we analyze the properties of low-frequency waves in a magnetotail reconnection diffusion region with a small guide field and high beta. Using the k-filtering method on the magnetic field data measured by Cluster spacecraft, we found that low-frequency waves in the diffusion region were highly oblique propagating mode. We compared the measured dispersion relation with theoretical ones calculated using the linear (hot) two-fluid and Vlasov-Maxwell theory. It is found that the observed waves in the diffusion region (with high plasma beta) follow the dispersion relation of the Alfven-Whistler wave mode. Comparisons with previous simulations and observational results are also discussed. C1 [Huang, S. Y.; Zhou, M.; Deng, X. H.; Pang, Y.; Yuan, Z. G.; Wei, Q.; Wang, J. F.; Zhou, X. M.] Wuhan Univ, Sch Elect Informat, Wuhan 430072, Peoples R China. [Sahraoui, F.] Observ St Maur, Ecole Polytech, CNRS, Lab Phys Plasmas, St Maur, France. [Zhou, M.; Deng, X. H.; Pang, Y.] Nanchang Univ, Inst Space Sci & Technol, Nanjing, Peoples R China. [Sahraoui, F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Huang, SY (reprint author), Wuhan Univ, Sch Elect Informat, Wuhan 430072, Peoples R China. EM monmentum82@hotmail.com RI Yuan, Zhigang/F-9114-2012 FU National natural Science Foundation of China (NSFC) [40890163, 40574073, 40574074, 40640420563, 40325012]; Ministry of Education of China [307019] FX We thank the Cluster teams (FGM, CIS, EFW, and PEACE) and Cluster Active Archive for the high-quality data and successful operation. This work is supported by the National natural Science Foundation of China (NSFC) under grants 40890163, 40574073, 40574074, 40640420563, 40325012, and by the key project of Ministry of Education of China under grant 307019. Philippa Browning thanks the reviewers for their assistance in evaluating the manuscript. NR 40 TC 21 Z9 25 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 4 PY 2010 VL 115 AR A12211 DI 10.1029/2010JA015335 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 690QT UT WOS:000285020000003 ER PT J AU Peterson, H Bailey, M Hallett, J Beasley, W AF Peterson, Harold Bailey, Matthew Hallett, John Beasley, William TI Reply to comment by S. Nijdam et al. on "NOx production in laboratory discharges simulating blue jets and red sprites" SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Editorial Material ID ENERGY C1 [Peterson, Harold] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Bailey, Matthew; Hallett, John] Desert Res Inst, Div Atmospher Sci, Reno, NV 89512 USA. [Beasley, William] Univ Oklahoma, Sch Meteorol, Norman, OK 73072 USA. RP Peterson, H (reprint author), NASA, George C Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM harold.peterson@nasa.gov NR 22 TC 6 Z9 6 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 4 PY 2010 VL 115 AR A12306 DI 10.1029/2010JA015946 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 690QT UT WOS:000285020000017 ER PT J AU Roberts, DA AF Roberts, D. Aaron TI Evolution of the spectrum of solar wind velocity fluctuations from 0.3 to 5 AU SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETOHYDRODYNAMIC TURBULENCE; HELIOS OBSERVATIONS; RADIAL EVOLUTION; MHD TURBULENCE; ULYSSES; ENERGY; ORIGIN; SPEED; WAVES AB Recent work has shown that at 1 AU from the Sun, the power spectrum of the solar wind magnetic field has the -5/3 spectral slope expected for Kolmogorov turbulence but that the velocity has closer to a -3/2 spectrum. This paper traces the changes in solar wind velocity spectra from 0.3 to 5 AU using data from the Helios and Ulysses spacecraft to show that this is a transient stage in solar wind evolution. The spectrum of the velocity is found to be flatter than that of the magnetic field for the higher frequencies examined for all cases until the slopes become equal (at -5/3) well past 1 AU when the wind is relatively non-Alfvenic. In some respects, in particular in the evolution of the frequency at which the spectrum changes from flatter at larger scales to a "turbulent" spectrum at smaller scales, the velocity field evolves more rapidly than the magnetic, and this is associated with the dominance of the magnetic energy over the kinetic at "inertial range" scales. The speed of the flow is argued to be largely unrelated to the spectral slopes, consistent with previous work, whereas high Alfvenicity appears to slow the spectral evolution, as expected from theory. This study shows that, for the solar wind, the idea of a simple "inertial range" with uniform spectral properties is not realistic, and new phenomenologies will be needed to capture the true situation. It is also noted that a flattening of the velocity spectrum often occurs at small scales. C1 NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Roberts, DA (reprint author), NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Code 672, Greenbelt, MD 20771 USA. EM aaron.roberts@nasa.gov RI Roberts, Dana/D-4625-2012 FU NASA FX This work was supported, in part, by NASA Supporting Research and Technology grants to the Goddard Space Flight Center. The data for this work were retrieved from NASA's Space Physics Data Facility, and we acknowledge the many people responsible for the provision, reduction, and preparation of those data sets. The referees were very helpful in clarifying the arguments. NR 24 TC 24 Z9 24 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 4 PY 2010 VL 115 AR A12101 DI 10.1029/2009JA015120 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 690QT UT WOS:000285020000001 ER PT J AU Sharma, RP Goldstein, ML Dwivedi, NK Chauhan, PK AF Sharma, R. P. Goldstein, M. L. Dwivedi, Navin Kumar Chauhan, Prashant K. TI Whistler propagation and modulation in the presence of nonlinear Alfven waves SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ELECTRON MAGNETOHYDRODYNAMIC TURBULENCE; SOLAR-WIND; PLASMA; IDENTIFICATION; MAGNETOSPHERE; DISSIPATION; CAVITATION; GENERATION; CORONA AB This paper presents the modulation of whistler waves due to linear interactions between a weak whistler signal and a pump kinetic Alfven wave (KAW) in intermediate-beta (m(e)/m(i) << beta << 1) plasmas (where beta is the ratio of the ion sound speed to the Alfven speed). As a consequence of ponderomotive nonlinearity, the pump KAW becomes filamented when its power exceeds the threshold for the filamentation instability. The periodic enhancements of the whistler amplitude occur in the locations where the beam width is narrower and are thus produced by the focusing of the whistler beam. Our results reveal that KAW has a (magnetic) power spectrum with an approximate scaling of k (5/3)(where k is vertical bar k vertical bar). The amplified whistler has electric field power spectra that are steeper than k (8/3) (where k is vertical bar k vertical bar). These results are consistent with recent observations by the Cluster spacecraft in the magnetotail region of the Earth's magnetosphere. C1 [Sharma, R. P.; Dwivedi, Navin Kumar] Indian Inst Technol, Ctr Energy Studies, New Delhi 110016, India. [Chauhan, Prashant K.] Inst Super Tecn, Grp Laser & Plasmas, P-1049001 Lisbon, Portugal. [Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sharma, RP (reprint author), Indian Inst Technol, Ctr Energy Studies, Hauz Khas, New Delhi 110016, India. EM navin.dwivedi@gmail.com RI Goldstein, Melvyn/B-1724-2008 FU DST (India); ISRO (India) FX This work is partially supported by DST (India) and ISRO (India) under RESPOND program. One of the authors (N.K.D.) is grateful for valuable conversations with H. D. Pandey,. Karuna Batra and H. D. Singh. NR 36 TC 5 Z9 5 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 4 PY 2010 VL 115 AR A12207 DI 10.1029/2009JA015123 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 690QT UT WOS:000285020000002 ER PT J AU Wang, SH Lin, NH Chou, MD Tsay, SC Welton, EJ Hsu, NC Giles, DM Liu, GR Holben, BN AF Wang, Sheng-Hsiang Lin, Neng-Huei Chou, Ming-Dah Tsay, Si-Chee Welton, Ellsworth J. Hsu, N. Christina Giles, David M. Liu, Gin-Rong Holben, Brent N. TI Profiling transboundary aerosols over Taiwan and assessing their radiative effects SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL-PROPERTIES; TROPOSPHERIC AEROSOLS; LIDAR; ASIA; PACIFIC; AERONET; ABSORPTION; RETRIEVAL; TRANSPORT; PATHWAYS AB A synergistic process was developed to study the vertical distributions of aerosol optical properties and their effects on solar heating using data retrieved from ground-based radiation measurements and radiative transfer simulations. Continuous MPLNET and AERONET observations were made at a rural site in northern Taiwan from 2005 to 2007. The aerosol vertical extinction profiles retrieved from ground-based lidar measurements were categorized into near-surface, mixed, and two-layer transport types, representing 76% of all cases. Fine-mode (Angstrom exponent, alpha, similar to 1.4) and moderately absorbing aerosols (columnar single-scattering albedo similar to 0.93, asymmetry factor similar to 0.73 at 440 nm wavelength) dominated in this region. The column-integrated aerosol optical thickness at 500 nm (tau(500nm)) ranges from 0.1 to 0.6 for the near-surface transport type but can be doubled in the presence of upper layer aerosol transport. We utilize aerosol radiative efficiency (ARE, the impact on solar radiation per unit change of tau(500nm)) to quantify the radiative effects due to different vertical distributions of aerosols. Our results show that the ARE at the top of atmosphere (-23 W m(-2)) is weakly sensitive to aerosol vertical distributions confined in the lower troposphere. On the other hand, values of the ARE at the surface are -44.3, -40.6, and -39.7 W m(-2) for near-surface, mixed, and two-layer transport types, respectively. Further analyses show that the impact of aerosols on the vertical profile of solar heating is larger for the near-surface transport type than for the two-layer transport type. The impacts of aerosol on the surface radiation and the solar heating profiles have implications for the stability and convection in the lower troposphere. C1 [Wang, Sheng-Hsiang; Lin, Neng-Huei; Chou, Ming-Dah; Liu, Gin-Rong] Natl Cent Univ, Dept Atmospher Sci, Chungli 320, Taiwan. [Wang, Sheng-Hsiang] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Wang, Sheng-Hsiang; Tsay, Si-Chee; Welton, Ellsworth J.; Hsu, N. Christina; Giles, David M.; Holben, Brent N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Giles, David M.] Sigma Space Corp, Lanham, MD 20703 USA. [Liu, Gin-Rong] Natl Cent Univ, Ctr Space & Remote Sensing Res, Chungli 320, Taiwan. RP Wang, SH (reprint author), Natl Cent Univ, Dept Atmospher Sci, 300 Chung Da Rd, Chungli 320, Taiwan. EM nhlin@cc.ncu.edu.tw RI Welton, Ellsworth/A-8362-2012; Hsu, N. Christina/H-3420-2013; Tsay, Si-Chee/J-1147-2014; Wang, Sheng-Hsiang/F-4532-2010 OI Wang, Sheng-Hsiang/0000-0001-9675-3135 FU National Science Council of Taiwan [97-2752-M-008-011-PAE, 96-2752-M-008-007-PAE, 97-2745-M-008-010, 96-2745-M-008-005]; Taiwan Environmental Protection Administration [EPA-97-U1L1-02-101, EPA-98-FA11-03-A015]; NASA Earth Observing System and Radiation Sciences Program FX This work was supported by the National Science Council of Taiwan under contracts 97-2752-M-008-011-PAE, 96-2752-M-008-007-PAE, 97-2745-M-008-010, and 96-2745-M-008-005 and by the Taiwan Environmental Protection Administration under contracts EPA-97-U1L1-02-101 and EPA-98-FA11-03-A015. The NASA MPLNET and AERONET are funded by the NASA Earth Observing System and Radiation Sciences Program. The authors gratefully acknowledge the NOAA Air Resources Laboratory for the provision of the HYSPLIT transport and dispersion model used in this publication. Special thanks go to the scientists (NASA/GSFC) and technicians (NCU) responsible for consulting, operating, and maintaining the instrumentation that generated this high-quality data set and ultimately enabled this paper to be written; these colleagues include Tom Eck, Timothy Berkoff, James Campbell, Larry Belcher, Ferret Kuo, and Eric Chia. NR 45 TC 12 Z9 12 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 3 PY 2010 VL 115 AR D00K31 DI 10.1029/2009JD013798 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 690PQ UT WOS:000285017100004 ER PT J AU Bell, JM Bougher, SW Waite, JH Ridley, AJ Magee, BA Mandt, KE Westlake, J DeJong, AD Bar-Nun, A Jacovi, R Toth, G De La Haye, V AF Bell, Jared M. Bougher, Stephen W. Waite, J. Hunter, Jr. Ridley, Aaron J. Magee, Brian A. Mandt, Kathleen E. Westlake, Joseph DeJong, Anna D. Bar-Nun, Akiva Jacovi, Ronen Toth, Gabor De La Haye, Virginie TI Simulating the one-dimensional structure of Titan's upper atmosphere: 1. Formulation of the Titan Global Ionosphere-Thermosphere Model and benchmark simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID NEUTRAL MASS-SPECTROMETER; RANGE MOMENT METHODS; HYDRODYNAMICALLY ESCAPING ATMOSPHERE; MOLECULAR SPECTROSCOPIC DATABASE; GENERAL-CIRCULATION MODEL; TIME-DEPENDENT MODEL; SPHERICAL GEOMETRY; RADIATIVE-TRANSFER; CASSINI ION; VOIGT FUNCTION AB We employ a newly developed Navier-Stokes model, the Titan Global Ionosphere-Thermosphere Model (T-GITM) to address the one dimensional (1-D) coupled composition, dynamics, and energetics of Titan's upper atmosphere. Our main goals are to delineate the details of this new theoretical tool and to present benchmark calibration simulations compared against the Ion-Neutral Mass Spectrometer (INMS) neutral density measurements. First, we outline the key physical routines contained in T-GITM and their computational formulation. Then, we compare a series of model simulations against recent 1-D work by Cui et al. (2008), Strobel (2008, 2009), and Yelle et al. (2008) in order to provide a fiducial for calibrating this new model. In paper 2 and a future paper, we explore the uncertainties in our knowledge of Titan's atmosphere between similar to 500 km and 1000 km in order to determine how the present measurements constrain our theoretical understanding of atmospheric structures and processes. C1 [Bell, Jared M.; Waite, J. Hunter, Jr.; Magee, Brian A.; Mandt, Kathleen E.; DeJong, Anna D.; De La Haye, Virginie] SW Res Inst, Div Space Sci & Engn, San Antonio, TX 78228 USA. [Bar-Nun, Akiva] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. [Westlake, Joseph] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. [Bougher, Stephen W.; Ridley, Aaron J.; Toth, Gabor] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Jacovi, Ronen] CALTECH, Jet Prop Lab, Ice Spect Lab, Pasadena, CA 91109 USA. RP Bell, JM (reprint author), SW Res Inst, Div Space Sci & Engn, 6220 Culebra Rd,POB 28510, San Antonio, TX 78228 USA. RI Toth, Gabor/B-7977-2013; Bougher, Stephen/C-1913-2013; Mandt, Kathleen/M-9812-2013; Ridley, Aaron/F-3943-2011; Westlake, Joseph/G-2732-2015 OI Toth, Gabor/0000-0002-5654-9823; Bougher, Stephen/0000-0002-4178-2729; Mandt, Kathleen/0000-0001-8397-3315; Ridley, Aaron/0000-0001-6933-8534; Westlake, Joseph/0000-0003-0472-8640 FU NASA; NASA through the Jet Propulsion Laboratory (JPL) [NAS703001NM0710023] FX J. Bell would like to thank Darrel Strobel for his help in refining the formulation for the turbulent velocities now employed in Titan GITM. This research was partially funded by the NASA Graduate Student Research Program (NASA GSRP) as part of J. Bell's thesis work. The authors also acknowledge support from NASA grant NAS703001NM0710023, subcontracted through the Jet Propulsion Laboratory (JPL). NR 102 TC 24 Z9 24 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 2 PY 2010 VL 115 AR E12002 DI 10.1029/2010JE003636 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 690QR UT WOS:000285019800003 ER PT J AU Deming, D AF Deming, Drake TI PLANETARY SCIENCE A cloudy view of exoplanets SO NATURE LA English DT Editorial Material ID TRANSMISSION SPECTRUM; EXTRASOLAR PLANET; HD 189733B; ATMOSPHERE C1 NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Deming, D (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. EM leo.d.deming@nasa.gov NR 8 TC 1 Z9 1 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 2 PY 2010 VL 468 IS 7324 BP 636 EP 637 DI 10.1038/468636a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 688GB UT WOS:000284836700023 PM 21124440 ER PT J AU Chatfield, RB Ren, XR Brune, W Schwab, J AF Chatfield, Robert B. Ren, Xinrong Brune, William Schwab, James CA Queens Coll PMTACS Measurement Teams TI Controls on urban ozone production rate as indicated by formaldehyde oxidation rate and nitric oxide SO ATMOSPHERIC ENVIRONMENT LA English DT Article; Proceedings Paper CT 2nd Biennial Conference on Atmospheric Chemistry Mechanisms CY DEC, 2008 CL Air Quality Res Ctr, Davis, CA HO Air Quality Res Ctr DE Tropospheric ozone; Smog; Ozone abatement; Atmospheric chemical mechanisms; New York City ID VOLATILE ORGANIC-COMPOUNDS; OH REACTIVITY; PHOTOCHEMISTRY; TROPOSPHERE; CHEMISTRY AB Several strong statistical relationships quantifying local ozone generation are found which use only easily measured variables nitrogen oxides (NOx) formaldehyde (HCHO) its photolysis i e UV) and temperature (T) A parameterized regression developed for rural air was adapted to central Queens New York City i e considerable fresh emissions Measurements of the radicals [HO2] and [OH] were available These provided explicit reference estimates of the predominant terms for chemical ozone production P-o(O-3) = k [HO2][NO] of the predominant chemical loss of nitrogen oxides L(NO2) = k[OH][NO2] and also their ratio (This is termed a production efficiency for O-3) Chemical modeling supports a robust extension from P-o(O-3) to total chemical production P(O-3) The two regression variables [NO] and (JHCHO double right arrow rads) [HCHO] which best explain Po(O-3) have low correlation R similar to 02 (variable interacting urban plumelets?) In our analysis R-2 for Po(O-3) (and an estimate for its rate-determining [HO2]) was in the range 0 48-0 81 Signally the method suggests a quantitative and very local application of descriptions of VOC limitation or NOx limitation to P(O-3) and L(NO2) expressed as dimensionless sensitivity variables Unexpected sources transport or chemistry may be highlighted using only HCHO NOx and UV radiation More complex relationships are needed in a focused analysis of intermediate polluted situations where timescales or individual sources may give trouble Here we find that T is informative and cooperates with j x [HCHO] in defining [HO2] Sensitivities for radicals and NO for P-o(O-3) are similar similar to 0 4 but sensitivities for radicals and NO2 for L(NO2) emphasize NO2 Remaining variability in the statistical estimates of P-o(O-3) and L(NO2) is modulated by incompletely understood slowly varying gain factors Understanding of these gain factors promises a better empirical indicator for P-o(O-3)/L(NO2) Complete 3-d simulations are not replaced but this view helps separate sub-problems in the estimation of HO2 and P(O-3) (c) 2010 Elsevier Ltd All rights reserved C1 [Chatfield, Robert B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ren, Xinrong] Univ Miami, Rosenstiel Sch Marine & Atmos Sci, Miami, FL 33149 USA. [Brune, William] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. [Schwab, James] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12203 USA. RP Chatfield, RB (reprint author), NASA, Ames Res Ctr, MS 245 5, Moffett Field, CA 94035 USA. RI Ren, Xinrong/B-2229-2010; Ren, Xinrong/E-7838-2015 OI Ren, Xinrong/0000-0001-9974-1666 NR 27 TC 3 Z9 3 U1 1 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2010 VL 44 IS 40 SI SI BP 5395 EP 5406 DI 10.1016/j.atmosenv.2010.08.056 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 696PA UT WOS:000285452100009 ER PT J AU Cottin, H Guan, YY Stalport, F Macari, F Jerome, M Philippon, C Coll, P Fray, N Szopa, C Raulin, F AF Cottin, H. Guan, Y. Y. Stalport, F. Macari, F. Jerome, M. Philippon, C. Coll, P. Fray, N. Szopa, C. Raulin, F. TI UV-olution Investigation of Photochemistry of Organic Compounds in Low Earth Orbit-A Review of the Main Results SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Meeting Abstract C1 [Cottin, H.; Guan, Y. Y.; Stalport, F.; Macari, F.; Jerome, M.; Philippon, C.; Coll, P.; Fray, N.; Raulin, F.] Univ Paris 7 & Paris 12, LISA, CNRS, UMR 7583, Creteil, France. [Stalport, F.] NASA, GSFC, Atmospher Expt Lab, Greenbelt, MD USA. [Szopa, C.] Univ Paris 6 & Versailles, LATMOS, CNRS, UMR 8190, Verrieres Le Buisson, France. RI Cottin, Herve/H-5654-2013; szopa, cyril/C-6865-2015 OI Cottin, Herve/0000-0001-9170-5265; szopa, cyril/0000-0002-0090-4056 NR 0 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2010 VL 40 IS 6 SI SI BP 585 EP 585 PG 1 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 691GX UT WOS:000285069400090 ER PT J AU Irom, F Nguyen, DN Underwood, ML Virtanen, A AF Irom, Farokh Nguyen, Duc N. Underwood, Mark L. Virtanen, Ari TI Effects of Scaling in SEE and TID Response of High Density NAND Flash Memories SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Floating gate; nonvolatile memory; single event effect; single event upset; single level; total ionizing ID COMMERCIAL NAND; RADIATION; DEVICES AB Heavy ion single-event effect (SEE) measurements and total ionizing dose (TID) response for Micron Technology single-level cell 1, 2, 4, 8 Gb commercial NAND flash memory and multi-level cell 8, 16, 32 Gb are reported. The heavy ion measurements were extended down to LET 0.1 MeV-cm(2)/mg. Scaling effects in SEE and TID response are discussed. Floating gate bit error upset cross section does not scale with feature size at high LETs, except for single-level cell 8 Gb device which is built with 51 nm processes. The threshold LET does not change with scaling. Charge pump TID degradation and standby current improves with scaling. In general, the effect of radiation is either unchanged or is less severe for highly scaled NAND flash memories. C1 [Irom, Farokh; Nguyen, Duc N.; Underwood, Mark L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Virtanen, Ari] Univ Jyvaskyla, Dept Phys, Accelerator Lab, Jyvaskyla, Finland. RP Irom, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM farokh.irom@jpl.nasa.gov; duc.n.nguyen@jpl.nasa.gov; mark.l.under-wood@jpl.nasa.gov; ari.virtanen@phys.jyu.fi OI Virtanen, Ari/0000-0002-6591-6787 FU National Aeronautics and Space Administration (NASA) FX Manuscript received July 15, 2010; revised September 08, 2010 and September 17, 2010; accepted September 27, 2010. Date of current version December 15, 2010. The research in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA), under the NASA Electronic Parts and Packaging Program. NR 18 TC 14 Z9 14 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3329 EP 3335 DI 10.1109/TNS.2010.2084102 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200048 ER PT J AU Des Marais, DJ AF Des Marais, David J. TI Exploring Mars for Evidence of Habitable Environments and Life SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Article ID MERIDIANI-PLANUM; OPPORTUNITY ROVER; MARTIAN CHANNELS; TERRA-MERIDIANI; VALLEY NETWORKS; BURNS FORMATION; GUSEV CRATER; DRAINAGE; HEMATITE; DEPOSITS C1 NASA, Ames Res Ctr, Washington, DC 20546 USA. RP Des Marais, DJ (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA. NR 79 TC 4 Z9 4 U1 2 U2 5 PU AMER PHILOSOPHICAL SOC PI PHILADELPHIA PA 104 SOUTH FIFTH ST, PHILADELPHIA, PA 19106-3387 USA SN 0003-049X EI 2326-9243 J9 P AM PHILOS SOC JI Proc. Amer. Philos. Soc. PD DEC PY 2010 VL 154 IS 4 BP 402 EP 421 PG 20 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 764OT UT WOS:000290642100002 ER PT J AU Finger, HB AF Finger, Harold B. TI ROBERT C. SEAMANS JR. 30 OCTOBER 1918 . 28 JUNE 2008 SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Biographical-Item C1 NASA, Washington, DC 20546 USA. RP Finger, HB (reprint author), NASA, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER PHILOSOPHICAL SOC PI PHILADELPHIA PA 104 SOUTH FIFTH ST, PHILADELPHIA, PA 19106-3387 USA SN 0003-049X J9 P AM PHILOS SOC JI Proc. Amer. Philos. Soc. PD DEC PY 2010 VL 154 IS 4 BP 503 EP 506 PG 4 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 764OT UT WOS:000290642100012 ER PT J AU Basilevsky, AT Neukum, G Nyquist, L AF Basilevsky, A. T. Neukum, G. Nyquist, L. TI The spatial and temporal distribution of lunar mare basalts as deduced from analysis of data for lunar meteorites SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Moon; Lunar meteorites; Cryptomare; Mare basalt ages ID URANIUM-LEAD SYSTEMATICS; U-TH-PB; SM-ND; ISOTOPIC SYSTEMATICS; RB-SR; LAPAZ ICEFIELD-02205; ASUKA 881757; LOW U/PB; MOON; AGES AB In this work we analyze data for lunar meteorites with emphasis on the spatial and temporal distribution of lunar mare basalts. The data are mostly from the Lunar Meteorite Compendium (http://www-curator.jsc.nasa.gov/antmet/Imc/contents.cfm cited hereafter as Compendium) compiled by Kevin Righter, NASA Johnson Space Center, and from the associated literature. Analysis of the data showed that (i) a significant part of the lunar meteorite source craters are not larger than hundreds of meters in diameter; (ii) cryptomaria seem to be rather abundant in lunar highlands; (iii) the ratios of lunar meteorites belonging to three broad petrologic groups (mare basalt/gabbro, feldspatic highland breccias, and mingled breccias which are a mixture of mare and highland components) seem to be roughly proportional to the areal distribution of these rocks on the lunar surface; and (iv) the meteorite mare basalt ages show a range from similar to 2.5 to 4.3 Ga and fill the gaps in the Apollo/Luna basalt age distribution. The ages of mare basalt clasts from mingled breccias seem to be systematically higher than those of "normal" mare basalts, which supports the suggestion that mingled breccias originated mostly from cryptomaria. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Basilevsky, A. T.] RAS, Vernadsky Inst Geochem & Analyt Chem, Moscow 117901, Russia. [Basilevsky, A. T.; Neukum, G.] Free Univ Berlin, D-1000 Berlin, Germany. [Nyquist, L.] KR NASA Johnson Space Ctr, Houston, TX 77058 USA. RP Basilevsky, AT (reprint author), RAS, Vernadsky Inst Geochem & Analyt Chem, Moscow 117901, Russia. EM atbas@geokhi.ru NR 66 TC 10 Z9 10 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD DEC PY 2010 VL 58 IS 14-15 BP 1900 EP 1905 DI 10.1016/j.pss.2010.08.020 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 696HT UT WOS:000285433200015 ER PT J AU Gordon, KL Thompson, CM Lyon, RE AF Gordon, K. L. Thompson, C. M. Lyon, R. E. TI Flame Retardant Epoxy Resins containing Aromatic Poly(phosphonamides) SO HIGH PERFORMANCE POLYMERS LA English DT Article DE Flame retardant; polyphosphonamides; epoxy resins ID PHOSPHORUS-CONTAINING EPOXY; COMBUSTION; POLYMERS; CONDENSATION; FLAMMABILITY AB As part of a program to develop more survivable aircraft, flame-retardant epoxy resins were investigated for their potential as fire-resistant exterior composite structures for future subsonic commercial and general aviation aircraft. Four different poly(phosphonamide)s were prepared by low temperature NMR condensation and characterized by Fourier transform infrared spectroscopy, (1)H-NMR spectroscopy, (31)P-NMR, differential scanning calorimetry, viscometry and gel-permeation chromatography. The poly(phosphonamides) were used as toughening agents (with 4,4'-diaminodiphenyl sulfone) to partially cure a commercially available unmodified liquid epoxy resin. The resulting cured epoxy formulations were evaluated for water uptake, flame retardance and fracture toughness. The formulations show good flame retardation with phosphorus content as low as 1.6% by weight, but exhibited high moisture uptake compared to the baseline epoxy. The fracture toughness of the cured formulations showed no detrimental effect due to phosphorus content (similar to 1.5% P). The heat of combustion of the pyrolysis gases, h(c) = 23.5 +/- 1.3 kJ g(-1) for the poly(phosphonamide) formulations were essentially the same as the N,N,N,N'-tetraglycidylether of -4,4'-methylene dianiline/4,4'-diaminodiphenyl sulfone epoxy formulation, h(c) = 24 kJ g(-1). C1 [Gordon, K. L.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. [Thompson, C. M.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Lyon, R. E.] Atlantic City Int Airport, William J Hughes Tech Ctr, Fed Aviat Adm, Atlantic City, NJ 08405 USA. RP Gordon, KL (reprint author), NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. EM k.l.gordon@larc.nasa.gov NR 27 TC 8 Z9 8 U1 3 U2 28 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0954-0083 J9 HIGH PERFORM POLYM JI High Perform. Polym. PD DEC PY 2010 VL 22 IS 8 BP 945 EP 958 DI 10.1177/0954008310363164 PG 14 WC Polymer Science SC Polymer Science GA 737UY UT WOS:000288595200005 ER PT J AU Di, LP Moe, K van Zyl, TL AF Di, Liping Moe, Karen van Zyl, Terence L. TI Earth Observation Sensor Web: An Overview SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Editorial Material C1 [Di, Liping] George Mason Univ, CSISS, Fairfax, VA 22030 USA. [Di, Liping] George Mason Univ, Dept Geog & Geoinformat Sci, Fairfax, VA 22030 USA. [Moe, Karen] NASA, Goddard Space Flight Ctr, Earth Sci Technol Off, Greenbelt, MD 20771 USA. [Moe, Karen] NASA, Earth Sci Data Syst Working Grp Technol Infus, Greenbelt, MD USA. [van Zyl, Terence L.] Meraka Inst, Pretoria, South Africa. RI van Zyl, Terence/B-9841-2008 NR 7 TC 21 Z9 21 U1 1 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD DEC PY 2010 VL 3 IS 4 BP 415 EP 417 DI 10.1109/JSTARS.2010.2089575 PN 1 PG 3 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 695GN UT WOS:000285358700001 ER PT J AU Rengarajan, SR Zawadzkr, MS Hodges, RE AF Rengarajan, Sembiam R. Zawadzkr, Mark S. Hodges, Richard E. TI Waveguide-Slot Array Antenna Designs for Low-Average-Sidelobe Specifications SO IEEE ANTENNAS AND PROPAGATION MAGAZINE LA English DT Article DE Slot arrays; antenna arrays; waveguide antennas; moment methods; array design; waveguide arrays AB This paper discusses the design, analysis, and development of waveguide-fed planar slot arrays to achieve low-average-sidelobe specifications, as may arise in radiometer applications. Such antennas may be required to meet strict average sidelobe levels in different angular regions, and low average return loss over a specified bandwidth. In addition to Elliott's design technique, we used a Moment-Method analysis program, Ansoft's HFSS code, and results of tolerance studies using Monte Carlo simulations to meet the design objectives. Comparisons of simulated results and experimental results are also presented. C1 [Rengarajan, Sembiam R.] Calif State Univ Northridge, Dept Elect & Comp Engn, Northridge, CA 91330 USA. [Zawadzkr, Mark S.; Hodges, Richard E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rengarajan, SR (reprint author), Calif State Univ Northridge, Dept Elect & Comp Engn, Northridge, CA 91330 USA. EM srengarajan@csun.edu; Mark.S.Zawadzki@jpl.nasa.gov; Richard.E.Hodges@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was conducted at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, under a contract with the National Aeronautics and Space Administration. The authors wish to thank Dr. Ronald J. Pogorzelski for reviewing this paper. We also acknowledge Jackie Chen and Dr. Behrouz Khayatian for their support. Dr. Jeff Harrell at JPL, and Near Field Systems Inc., Torrance, CA, helped with the measurements. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise does not constitute or imply its endorsement by the United States Government or the Jet Propulsion Laboratory, California Institute of Technology. NR 14 TC 14 Z9 15 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1045-9243 EI 1558-4143 J9 IEEE ANTENN PROPAG M JI IEEE Antennas Propag. Mag. PD DEC PY 2010 VL 52 IS 6 BP 89 EP 98 DI 10.1109/MAP.2010.5723227 PG 10 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 731DG UT WOS:000288085900009 ER PT J AU Siegel, PH Pikov, V AF Siegel, P. H. Pikov, V. TI Impact of low intensity millimetre waves on cell functions SO ELECTRONICS LETTERS LA English DT Editorial Material ID INDUCED HYPOALGESIA; WATER DYNAMICS; SPECTROSCOPY; DEPENDENCE; RADIATION AB Investigations on the biological impact of low levels of millimetre-wave energy date back to the first experiments on the generation and detection of these high-frequency signals by Sir Jagadis Chunder Bose at the end of the 19th century. Slightly more than a hundred years later, millimetre-wave transmission has become a ubiquitous commercial reality. Despite the widespread use of millimetre-wave transmitters for communications, radar and even non-lethal weapons systems, only a handful of researchers have funded programmes focusing on millimetre-wave interactions with biological systems. As such, there is a growing need for a better understanding of the mechanisms of these interactions and their possible adverse and therapeutic implications. Independent of the health impact of long-term exposure to high doses of millimetre-wave energy on whole organisms, there exists the potential for subtle effects on specific tissues or organs which can best be quantified in studies which examine real-time changes in cellular function as energy is applied. In this Letter, a series of experiments are presented which show changes in cell membrane potential and the action potential firing rate of cortical neurons under short (1 mm) exposures to continuous-wave 60 GHz radiation at mu W/cm(2) power levels, more than 1000 times below the US government maximum permissible exposure. The findings have implications for non-contact stimulation and control of neurologic function, and might prove useful in a variety of health applications from suppression of peripheral neuropathic pain to the treatment of central neurological disorders. C1 [Siegel, P. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Pikov, V.] Huntington Med Res Inst, Pasadena, CA 91105 USA. RP Siegel, PH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM phs@caltech.edu NR 27 TC 0 Z9 0 U1 2 U2 6 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 DEC PY 2010 SU S BP S70 EP S72 DI 10.1049/el.2010.8442 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 728QN UT WOS:000287888900025 ER PT J AU Trippe, ML Crenshaw, DM Deo, RP Dietrich, M Kraemer, SB Rafter, SE Turner, TJ AF Trippe, M. L. Crenshaw, D. M. Deo, R. P. Dietrich, M. Kraemer, S. B. Rafter, S. E. Turner, T. J. TI A MULTI-WAVELENGTH STUDY OF THE NATURE OF TYPE 1.8/1.9 SEYFERT GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert; infrared: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; NARROW-LINE SEYFERT-1; H-ALPHA-EMISSION; LONG-SLIT SPECTROSCOPY; X-RAY-PROPERTIES; NGC 1365; LOW-LUMINOSITY; OPTICAL SPECTROSCOPY; NEARBY GALAXIES; SPECTRAL ATLAS AB We focus on determining the underlying physical cause of a Seyfert galaxy's appearance as type 1.8 or 1.9. Are these "intermediate" Seyfert types typical Seyfert 1 nuclei with reddened broad-line regions? Or are they objects with intrinsically weak continua and broad emission lines? We compare measurements of the optical reddening of the narrow and broad-line regions with each other and with the X-ray column derived from XMM-Newton 0.5-10 keV spectra to determine the presence and location of dust in the line of sight. We also searched the literature to see if the objects showed evidence for broad-line variability, and determined if the changes were consistent with a change in reddening or a change in the intrinsic ionizing continuum flux. We find that 10 of 19 objects previously classified as Seyfert 1.8/1.9s received this designation due to their low continuum flux. In four objects, the classification was due to broad emission-line region reddening, either by the torus or dust structures in the vicinity of the narrow emission-line region; in the remaining five objects there is not sufficient evidence to favor one scenario over the other. These findings imply that, in general, samples of 1.8/1.9s are not suitable for use in studies of gas and dust in the central torus. C1 [Trippe, M. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Crenshaw, D. M.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Deo, R. P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Dietrich, M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kraemer, S. B.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Kraemer, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Rafter, S. E.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. RP Trippe, ML (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; ESA Member States; NASA FX Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.; Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. NR 87 TC 23 Z9 23 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 2 BP 1749 EP 1767 DI 10.1088/0004-637X/725/2/1749 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300033 ER PT J AU Fox, OD Chevalier, RA Dwek, E Skrutskie, MF Sugerman, BEK Leisenring, JM AF Fox, Ori D. Chevalier, Roger A. Dwek, Eli Skrutskie, Michael F. Sugerman, Ben E. K. Leisenring, Jarron M. TI DISENTANGLING THE ORIGIN AND HEATING MECHANISM OF SUPERNOVA DUST: LATE-TIME SPITZER SPECTROSCOPY OF THE TYPE IIn SN 2005ip SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; infrared: stars; supernovae: general; supernovae: individual (SN 2005ip) ID LUMINOUS BLUE VARIABLES; INFRARED-EMISSION; SPACE-TELESCOPE; CIRCUMSTELLAR MEDIUM; MASSIVE STARS; SPECTROGRAPH; EJECTA; PROGENITORS; OUTBURST; 1987A AB This paper presents late-time near-infrared and Spitzer mid-infrared photometric and spectroscopic observations of warm dust in the Type IIn SN 2005ip in NGC 2906. The spectra show evidence for two dust components with different temperatures. Spanning the peak of the thermal emission, these observations provide strong constraints on the dust mass, temperature, and luminosity, which serve as critical diagnostics for disentangling the origin and heating mechanism of each component. The results suggest that the warmer dust has a mass of similar to 5 x 10(-4) M-circle dot, originates from newly formed dust in the ejecta, or possibly the cool, dense shell, and is continuously heated by the circumstellar interaction. By contrast, the cooler component likely originates from a circumstellar shock echo that forms from the heating of a large, pre-existing dust shell similar to 0.01-0.05 M-circle dot by the late-time circumstellar interaction. The progenitor wind velocity derived from the blue edge of the He I 1.083 mu m P Cygni profile indicates a progenitor eruption likely formed this dust shell similar to 100 years prior to the supernova explosion, which is consistent with a Luminous Blue Variable progenitor star. C1 [Fox, Ori D.; Chevalier, Roger A.; Skrutskie, Michael F.; Leisenring, Jarron M.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Fox, Ori D.; Dwek, Eli] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sugerman, Ben E. K.] Goucher Coll, Dept Phys & Astron, Baltimore, MD 21204 USA. RP Fox, OD (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. EM ofox@virginia.edu RI Dwek, Eli/C-3995-2012 FU NASA [PID 50256]; NASA through JPL/Caltech; NASA GSRP; ARCS; VSGC; NSF [AST-0807727] FX This work is based on observations made with the Spitzer Space Telescope (PID 50256), 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. O.D.F. is grateful for support from NASA GSRP, ARCS, and VSGC. R.A.C. was supported by NSF grant AST-0807727. The authors thank Genevieve de Messieres, JD Smith, and the entire Spitzer Science Help Desk for their extensive help with the Spitzer data reduction. We are also grateful to Joel Sop for his help with the data reduction in the early stages. We are also thankful to Sarah Doverspike and the anonymous referee for their helpful edits. NR 61 TC 30 Z9 30 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 2 BP 1768 EP 1778 DI 10.1088/0004-637X/725/2/1768 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300034 ER PT J AU Brassington, NJ Fabbiano, G Blake, S Zezas, A Angelini, L Davies, RL Gallagher, J Kalogera, V Kim, DW King, AR Kundu, A Trinchieri, G Zepf, S AF Brassington, N. J. Fabbiano, G. Blake, S. Zezas, A. Angelini, L. Davies, R. L. Gallagher, J. Kalogera, V. Kim, D. -W. King, A. R. Kundu, A. Trinchieri, G. Zepf, S. TI THE X-RAY SPECTRA OF THE LUMINOUS LMXBs IN NGC 3379: FIELD AND GLOBULAR CLUSTER SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 3379); X-rays: binaries; X-rays: galaxies ID ABSORPTION CROSS-SECTIONS; BLACK-HOLE ACCRETION; ELLIPTIC GALAXIES; DEEP CHANDRA; HIGH STATE; MASS; BINARIES; POPULATIONS; CONNECTION; DISTANCES AB From a deep multi-epoch Chandra observation of the elliptical galaxy NGC 3379 we report the spectral properties of eight luminous LMXBs (L-X > 1.2 x 10(38) erg s(-1)). We also present a set of spectral simulations, produced to aid the interpretation of low-count single-component spectral modeling. These simulations demonstrate that it is possible to infer the spectral states of X-ray binaries from these simple models and thereby constrain the properties of the source. Of the eight LMXBs studied, three reside within globular clusters (GCs) and one is a confirmed field source. Due to the nature of the luminosity cut, all sources are either neutron star (NS) binaries emitting at or above the Eddington luminosity or black hole (BH) binaries. The spectra from these sources are well described by single-component models, with parameters consistent with Galactic LMXB observations, where hard-state sources have a range in photon index of 1.5-1.9 and thermally dominant (TD) sources have inner-disk temperatures between similar to 0.7 and 1.55 keV. The large variability observed in the brightest GC source (L-X > 4 x 10(38) erg s(-1)) suggests the presence of a BH binary. At its most luminous this source is observed in a TD state with kT(in) = 1.5 keV, consistent with a BH mass of similar to 4 M-circle dot. This observation provides further evidence that GCs are able to retain such massive binaries. We also observed a source transitioning from a bright state (L-X similar to 1 x 10(39) erg s(-1)), with prominent thermal and non-thermal components, to a less luminous hard state (L-X = 3.8 x 10(38) erg s(-1), Gamma = 1.85). In its high flux emission, this source exhibits a cool-disk component of similar to 0.14 keV, similar to spectra observed in some ultraluminous X-ray sources (ULXs). Such a similarity indicates a possible link between "normal" stellar-mass BHs in a high accretion state and ULXs. C1 [Brassington, N. J.; Fabbiano, G.; Zezas, A.; Kim, D. -W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blake, S.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Blake, S.; Davies, R. L.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Angelini, L.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [King, A. R.] Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. [Kundu, A.; Zepf, S.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Trinchieri, G.] INAF Osservatorio Astron Brera, I-20121 Milan, Italy. RP Brassington, NJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nbrassington@head.cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Trinchieri, Ginevra/0000-0002-0227-502X FU University of Southampton; Chandra G0 [G06-7079A, G06-7079B]; NASA [NAS8-39073]; NASA LTSA [NAG5-13056] FX We thank the CXC DS and SDS teams for their efforts in reducing the data and developing the software used for the reduction (SDP) and analysis (CIAO). We thank the anonymous referee whose detailed and careful report has helped improve this paper. This paper is based upon work performed by S.B. while visiting CfA as part of a student program sponsored by the University of Southampton. This work was supported by Chandra G0 grant G06-7079A (PI:Fabbiano) and subcontract G06-7079B (PI:Kalogera). We acknowledge partial support from NASA contract NAS8-39073(CXC). A.Z. acknowledges support from NASA LTSA grant NAG5-13056. NR 42 TC 27 Z9 27 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 2 BP 1805 EP 1823 DI 10.1088/0004-637X/725/2/1805 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300038 ER PT J AU Gliozzi, M Panessa, F La Franca, F Saviane, I Monaco, L Foschini, L Kedziora-Chudczer, L Satyapal, S Sambruna, RM AF Gliozzi, M. Panessa, F. La Franca, F. Saviane, I. Monaco, L. Foschini, L. Kedziora-Chudczer, L. Satyapal, S. Sambruna, R. M. TI Q2122-444: A NAKED ACTIVE GALACTIC NUCLEUS FULLY DRESSED SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: nuclei; X-rays: galaxies ID ACCRETING BLACK-HOLES; SEYFERT 2 GALAXIES; BROAD-LINE REGION; X-RAY; SKY-SUBTRACTION; RADIO LOUDNESS; GRO J1655-40; QUASARS; EMISSION; AGN AB Based on previous spectral and temporal optical studies, Q2122-444 has been classified as a naked active galactic nucleus (AGN) or true type 2 AGN, that is, an AGN that genuinely lacks a broad-line region (BLR). Its optical spectrum seemed to possess only narrow forbidden emission lines that are typical of type 2 (obscured) AGNs, but the long-term optical light curve, obtained from a monitoring campaign over more than two decades, showed strong variability, apparently ruling out the presence of heavy obscuration. Here we present the results from a similar to 40 ks XMM-Newton observation of Q2122-444 carried out to shed light on the energetics of this enigmatic AGN. The X-ray analysis was complemented with Australia Telescope Compact Array radio data to assess the possible presence of a jet, and with new NTT/EFOSC2 optical spectroscopic data to verify the actual absence of a BLR. The higher-quality optical data revealed the presence of strong and broad Balmer lines that are at odds with the previous spectral classification of this AGN. The lack of detection of radio emission rules out the presence of a jet. The X-ray data combined with simultaneous UV observations carried out by the Optical Monitor (OM) aboard XMM-Newton confirm that Q2122-444 is a typical type 1 AGN without any significant intrinsic absorption. New estimates of the black hole mass independently obtained from the broad Balmer lines and from a new scaling technique based on X-ray spectral data suggest that Q2122-444 is accreting at a relatively high rate in Eddington units. C1 [Gliozzi, M.; Satyapal, S.] George Mason Univ, Fairfax, VA 22030 USA. [Panessa, F.] Ist Astrofis Spaziale & Fis Cosm IASF INAF, I-00133 Rome, Italy. [La Franca, F.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Saviane, I.; Monaco, L.] European So Observ, Santiago 19, Chile. [Foschini, L.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Kedziora-Chudczer, L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Sambruna, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gliozzi, M (reprint author), George Mason Univ, 4400 Univ Dr, Fairfax, VA 22030 USA. RI La Franca, Fabio/G-9631-2012; Foschini, Luigi/H-3833-2012; OI Foschini, Luigi/0000-0001-8678-0324; Panessa, Francesca/0000-0003-0543-3617; La Franca, Fabio/0000-0002-1239-2721 FU NASA [NNX08AB67G]; NASA ADP [NNXIOAD51G] FX We thank the anonymous referee for the very constructive suggestions that have improved the clarity of the paper. M.G. acknowledges support by the XMM-Newton Guest Investigator Program under NASA grant NNX08AB67G and by the NASA ADP grant NNXIOAD51G. We thank Ranjani Sarma for helping with the X-ray spectral analysis. NR 58 TC 6 Z9 6 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 2 BP 2071 EP 2077 DI 10.1088/0004-637X/725/2/2071 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300057 ER PT J AU Kocharov, L Reiner, MJ Klassen, A Thompson, BJ Valtonen, E AF Kocharov, L. Reiner, M. J. Klassen, A. Thompson, B. J. Valtonen, E. TI OBSERVED CORE OF A GRADUAL SOLAR ENERGETIC PARTICLE EVENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; shock waves; Sun: particle emission ID GAMMA-RAY SPECTROSCOPY; WHITE-LIGHT OBSERVATIONS; CORONAL MASS EJECTIONS; SHOCK-WAVE; RADIO EVIDENCE; ABUNDANCES; HELIUM; FLARE; PLASMA; PROTON AB Using space-borne particle and EUV detection and radio spectrograms from both ground-based and space-borne instruments, we study the first phase of the major solar energetic particle (SEP) event associated with the western solar flare and fast and wide coronal mass ejection (CME) on 2000 April 4. The SEP event being observed at the magnetic connection to the eruption's center starts with deka-MeV nucl(-1) helium-and relativistic electron-rich production from coronal sources identified with the electromagnetic diagnostics and the SEP event modeling. The broadband observations and modeling of the initial phase of the "well-connected" major SEP event support the idea that acceleration of SEPs starts in the helium-rich plasma of the eruption's core in association with coronal shocks and magnetic reconnections caused by the CME liftoff, and that the coronal component dominates during the first hour of the SEP event considered, not yet being shielded by the CME bow shock in the solar wind. The first phase of the SEP event is followed by a second phase of SEP production associated with a decelerating CME-driven shock wave in the solar wind, which accelerates ions from a distinct, helium-poor seed particle population that may originate from the CME interaction with a coronal streamer. C1 [Kocharov, L.; Valtonen, E.] Univ Turku, Dept Phys & Astron, Space Res Lab, FI-20014 Turku, Finland. [Reiner, M. J.; Thompson, B. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Klassen, A.] Univ Kiel, Inst Expt & Angew Phys, D-24098 Kiel, Germany. RP Kocharov, L (reprint author), Univ Turku, Dept Phys & Astron, Space Res Lab, FI-20014 Turku, Finland. RI Thompson, Barbara/C-9429-2012 NR 53 TC 6 Z9 6 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 2 BP 2262 EP 2269 DI 10.1088/0004-637X/725/2/2262 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300072 ER PT J AU Ardila, DR Van Dyk, SD Makowiecki, W Stauffer, J Song, I Rho, J Fajardo-Acosta, S Hoard, DW Wachter, S AF Ardila, David R. Van Dyk, Schuyler D. Makowiecki, Wojciech Stauffer, John Song, Inseok Rho, Jeonghee Fajardo-Acosta, Sergio Hoard, D. W. Wachter, Stefanie TI THE SPITZER ATLAS OF STELLAR SPECTRA (SASS) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astronomical databases: miscellaneous; catalogs; Hertzsprung-Russell and C-M diagrams; stars: atmospheres; stars: fundamental parameters; techniques: spectroscopic ID WOLF-RAYET STARS; LARGE-MAGELLANIC-CLOUD; INFRARED SPECTROGRAPH IRS; SHORT-WAVELENGTH SPECTROMETER; LOW-RESOLUTION SPECTRA; FIELD BLUE STRAGGLERS; SPACE-TELESCOPE; MICRON SPECTRA; IRRADIANCE CALIBRATION; EFFECTIVE TEMPERATURE AB We present the Spitzer Atlas of Stellar Spectra, which includes 159 stellar spectra (5-32 mu m; R similar to 100) taken with the Infrared Spectrograph on the Spitzer Space Telescope. This Atlas gathers representative spectra of a broad section of the Hertzsprung-Russell diagram, intended to serve as a general stellar spectral reference in the mid-infrared. It includes stars from all luminosity classes, as well as Wolf-Rayet (WR) objects. Furthermore, it includes some objects of intrinsic interest, such as blue stragglers and certain pulsating variables. All of the spectra have been uniformly reduced, and all are available online. For dwarfs and giants, the spectra of early-type objects are relatively featureless, characterized by the presence of hydrogen lines in A spectral types. Besides these, the most noticeable photospheric features correspond to water vapor and silicon monoxide in late-type objects and methane and ammonia features at the latest spectral types. Most supergiant spectra in the Atlas present evidence of circumstellar gas and/or dust. The sample includes five M supergiant spectra, which show strong dust excesses and in some cases polycyclic aromatic hydrocarbon features. Sequences of WR stars present the well-known pattern of lines of He I and He II, as well as forbidden lines of ionized metals. The characteristic flat-top shape of the [Ne III] line is evident even at these low spectral resolutions. Several Luminous Blue Variables and other transition stars are present in the Atlas and show very diverse spectra, dominated by circumstellar gas and dust features. We show that the [8]-[24] Spitzer colors (IRAC and MIPS) are poor predictors of spectral type for most luminosity classes. C1 [Ardila, David R.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Van Dyk, Schuyler D.; Makowiecki, Wojciech; Stauffer, John; Rho, Jeonghee; Fajardo-Acosta, Sergio; Hoard, D. W.; Wachter, Stefanie] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Rho, Jeonghee] NASA, Ames Res Ctr, SOFIA Sci Ctr, USRA, Moffett Field, CA 94035 USA. [Fajardo-Acosta, Sergio] CALTECH, WISE Sci Data Ctr, Pasadena, CA 91125 USA. RP Ardila, DR (reprint author), CALTECH, NASA Herschel Sci Ctr, Mail Code 100-22, Pasadena, CA 91125 USA. EM ardila@ipac.caltech.edu OI Van Dyk, Schuyler/0000-0001-9038-9950 FU National Aeronautics and Space Administration (NASA); National Science Foundation FX This work is based on observations and archival data from the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech) under a contract with National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA through an award issued by JPL/Caltech. This research has also made use of the NASA/Infrared Processing and Analysis Center (IPAC) Science Archive, operated by the JPL, Caltech, under contract with NASA; the SIMBAD database and the Vizier service, operated at CDS, Strasbourg, France; the data products from the Two Micron All Sky Survey (2MASS), a joint project of the University of Massachusetts and IPAC/Caltech, funded by NASA and the National Science Foundation. NR 84 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2010 VL 191 IS 2 BP 301 EP 339 DI 10.1088/0067-0049/191/2/301 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692VY UT WOS:000285185200008 ER PT J AU Chen, YA Mojarradi, M Suehle, J Westergard, L AF Chen, Yuan Mojarradi, Mohammad Suehle, John Westergard, Lynett TI Introduction to the Extreme Environment Technology and Reliability Special Issue SO IEEE TRANSACTIONS ON DEVICE AND MATERIALS RELIABILITY LA English DT Editorial Material C1 [Chen, Yuan] NASA, Hampton, VA USA. [Mojarradi, Mohammad] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Suehle, John] NIST, Gaithersburg, MD 20899 USA. [Westergard, Lynett] ON Semicond, Phoenix, AZ 85008 USA. RP Chen, YA (reprint author), NASA, Hampton, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-4388 J9 IEEE T DEVICE MAT RE JI IEEE Trans. Device Mater. Reliab. PD DEC PY 2010 VL 10 IS 4 BP 417 EP 417 DI 10.1109/TDMR.2010.2088810 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 712PZ UT WOS:000286680000001 ER PT J AU Johnston, AH AF Johnston, Allan H. TI Space Radiation Effects and Reliability Considerations for Micro- and Optoelectronic Devices SO IEEE TRANSACTIONS ON DEVICE AND MATERIALS RELIABILITY LA English DT Article DE Microelectronics; optoelectronics; radiation damage; reliability; space radiation ID BIPOLAR-DEVICES; MICROELECTRONICS; CIRCUITS; DAMAGE; DEGRADATION; THRESHOLD; HYDROGEN AB The interplay between radiation effects and reliability is discussed for micro- and optoelectronic devices. Topics discussed include basic approaches such as burn-in and electrical screening that are used to improve component reliability, synergistic effects between reliability and radiation effects, the impact of microdose damage from heavy ions on reliability of high-density digital circuits, and assessing the overall risk to components in space that are subjected to overstress conditions. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnston, AH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM allan.h.johnston@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 31 TC 5 Z9 5 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-4388 J9 IEEE T DEVICE MAT RE JI IEEE Trans. Device Mater. Reliab. PD DEC PY 2010 VL 10 IS 4 BP 449 EP 459 DI 10.1109/TDMR.2010.2048111 PG 11 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 712PZ UT WOS:000286680000005 ER PT J AU Mikellides, IG Goebel, DM Snyder, JS Katz, I Herman, DA AF Mikellides, Ioannis G. Goebel, Dan M. Snyder, John Steven Katz, Ira Herman, Daniel A. TI The discharge plasma in ion engine neutralizers: Numerical simulations and comparisons with laboratory data SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID HOLLOW-CATHODE THEORY; ACOUSTIC-WAVES; COLLISIONS AB Numerical simulations of neutralizer hollow cathodes at various operating conditions and orifice sizes are presented. The simulations were performed using a two-dimensional axisymmetric model that solves numerically an extensive system of conservation laws for the partially ionized gas in these devices. The results for the plasma are compared directly with Langmuir probe measurements. The computed keeper voltages are also compared with the observed values. Whenever model inputs and/or specific physics of the cathode discharge were uncertain or unknown additional sensitivity calculations have been performed to quantify the uncertainties. The model has also been employed to provide insight into recent ground test observations of the neutralizer cathode in NASA's evolutionary xenon thruster. It is found that a likely cause of the observed keeper voltage drop in a long duration test of the engine is cathode orifice erosion. (C) 2010 American Institute of Physics. [doi:10.1063/1.3514560] C1 [Mikellides, Ioannis G.; Goebel, Dan M.; Snyder, John Steven; Katz, Ira] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herman, Daniel A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Mikellides, IG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ioannis.g.mikellides@jpl.nasa.gov FU NASA FX The research described in this paper was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government or the Jet Propulsion Laboratory, California Institute of Technology. Portions of the work described herein were funded by NASA's In-Space Propulsion Technology Program under the NEXT Project, led by the NASA Glenn Research Center, with Scott Benson as the Project Manager and Mike Patterson as the Principal Investigator. Finally, the authors wish to acknowledge Ibrahim Abiola who developed the new sputtering yield fit based on his numerical simulations of the NSTAR NHC during a student summer internship at JPL. NR 20 TC 8 Z9 8 U1 4 U2 12 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD DEC 1 PY 2010 VL 108 IS 11 AR 113308 DI 10.1063/1.3514560 PG 12 WC Physics, Applied SC Physics GA 696XG UT WOS:000285474100028 ER PT J AU Rosenqvist, A Shimada, M Lucas, R Chapman, B Paillou, P Hess, L Lowry, J AF Rosenqvist, Ake Shimada, Masanobu Lucas, Richard Chapman, Bruce Paillou, Philippe Hess, Laura Lowry, John TI The Kyoto & Carbon Initiative - A Brief Summary SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Editorial Material C1 [Rosenqvist, Ake] SoloEO, Tokyo 1040054, Japan. [Shimada, Masanobu] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki 3058505, Japan. [Lucas, Richard] Aberystwyth Univ, Aberystwyth SY23 3DB, Dyfed, Wales. [Chapman, Bruce] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Paillou, Philippe] Univ Bordeaux, F-33271 Floirac, France. [Hess, Laura] Univ Calif Santa Barbara, Inst Computat Earth Syst Sci, Santa Barbara, CA 93106 USA. [Lowry, John] Dept Sustainabil Environm Water Populat & Communi, Darwin, NT 0801, Australia. RP Rosenqvist, A (reprint author), SoloEO, Tokyo 1040054, Japan. NR 3 TC 5 Z9 5 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD DEC PY 2010 VL 3 IS 4 BP 551 EP 553 DI 10.1109/JSTARS.2010.2086270 PN 2 PG 3 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 695GA UT WOS:000285357400001 ER PT J AU McClanahan, TP Ivatury, V Milikh, G Nandikotkur, G Puetter, RC Sagdeev, RZ Usikov, D Mitrofanov, IG AF McClanahan, T. P. Ivatury, V. Milikh, G. Nandikotkur, G. Puetter, R. C. Sagdeev, R. Z. Usikov, D. Mitrofanov, I. G. TI Comparison of image restoration methods for lunar epithermal neutron emission mapping SO COMPUTERS & GEOSCIENCES LA English DT Article DE Geochemistry; Image restoration; Image reconstruction; Neutron; LEND; LRO; Gamma-ray ID RECONSTRUCTION ALGORITHM; RECONNAISSANCE ORBITER; HYDROGEN DEPOSITS; INSTRUMENT SUITE; MARS ODYSSEY; GAMMA-RAY; MOON; PROSPECTOR; ICE; POLES AB Orbital measurements of neutrons by the Lunar Exploring Neutron Detector (LEND) onboard the Lunar Reconnaissance Orbiter are being used to quantify the spatial distribution of near surface hydrogen (H). Inferred H concentration maps have low signal-to-noise (SN) and image restoration (IR) techniques are being studied to enhance results. A single-blind, two-phase study is described in which four teams of researchers independently developed image restoration techniques optimized for LEND data. Synthetic lunar epithermal neutron emission maps were derived from LEND simulations. These data were used as ground truth to determine the relative quantitative performance of the IR methods vs. a default denoising (smoothing) technique. We review and used factors influencing orbital remote sensing of neutrons emitted from the lunar surface to develop a database of synthetic "true" maps for performance evaluation. A prior independent training phase was implemented for each technique to assure methods were optimized before the blind trial. Method performance was determined using several regional root-mean-square error metrics specific to epithermal signals of interest. Results indicate unbiased IR methods realize only small signal gains in most of the tested metrics. This suggests other physically based modeling assumptions are required to produce appreciable signal gains in similar low SN IR applications. Published by Elsevier Ltd. C1 [McClanahan, T. P.; Ivatury, V.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. [Ivatury, V.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA. [Milikh, G.; Nandikotkur, G.; Sagdeev, R. Z.; Usikov, D.] Univ Maryland, College Pk, MD 20742 USA. [Puetter, R. C.] Pixon Imaging LLC, San Diego, CA 92117 USA. [Mitrofanov, I. G.] Russian Acad Sci, Inst Space Res, Moscow V71, Russia. RP McClanahan, TP (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Bldg 34,Room W218, Greenbelt, MD 20771 USA. EM timothy.p.mcclanahan@nasa.gov RI McClanahan, Timothy/C-8164-2012 NR 41 TC 1 Z9 1 U1 1 U2 6 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 DEC PY 2010 VL 36 IS 12 BP 1484 EP 1493 DI 10.1016/j.cageo.2009.11.011 PG 10 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA 707RP UT WOS:000286304000003 ER PT J AU Ruane, AC AF Ruane, Alex C. TI NARR's Atmospheric Water Cycle Components. Part II: Summertime Mean and Diurnal Interactions SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID AMERICAN REGIONAL REANALYSIS; WARM-SEASON PRECIPITATION; CONTERMINOUS UNITED-STATES; MESOSCALE ETA-MODEL; LOW-LEVEL JET; GLOBAL PRECIPITATION; MOISTURE TRANSPORT; NORTH-AMERICA; FREQUENCY; RAINFALL AB Summertime interactions in the North American Regional Reanalysis (NARR) atmospheric water cycle are examined from a user's perspective over the 1980-99 period with a particular emphasis on the diurnal cycle, the nocturnal maximum of precipitation over the Midwest, and the impacts of precipitation assimilation. NARR's full-year mean atmospheric water cycle and its annual variations are examined in Part I of this study. North American summertime (June-August) features substantial convective activity that is often organized on a diurnal scale, although diverse regional diurnal features are evident to various extents in high-resolution precipitation products. NARR's hourly assimilation of precipitation observations over the continental United States allows it to resolve diurnal effects on the water cycle, but in other regions the diurnal cycle of precipitation is imposed from an external reanalysis model. The prominent nocturnal maximum in precipitation across the upper Midwest is captured in NARR, but different precipitation assimilation sources disrupt the propagation of convective systems across the Canadian border. Normalized covariances of NARR's diurnal water cycle component interactions in the nocturnal maximum region reveal a strong relationship between moisture convergence and precipitation, and also measure the way in which the precipitable water column holds a lagged response between evaporation and precipitation. In many regions the diurnal cycle of rainfall is driven by interactions with water cycle components that differ from those driving the seasonal cycle. A comparison between NARR's precipitation and an estimate of the model precipitation prior to precipitation assimilation distinguishes the portion of the water cycle captured in full by the model and that which is value added by the assimilation routine. The nocturnal rainfall maximum is not present in the model precipitation estimate, leading to diurnal-scale biases in the evaporation and moisture flux convergence fields that are not directly modified by precipitation assimilation. C1 [Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ruane, Alex C.] Oak Ridge Associated Univ, NASA, Postdoctoral Program, New York, NY USA. [Ruane, Alex C.] Sigma Space Partners LLC, New York, NY USA. RP Ruane, AC (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM aruane@giss.nasa.gov FU NASA FX This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Institute for Space Studies, administered by Oak Ridge Associated Universities (ORAU) through a contract with NASA. The views expressed herein are those of the author and do not necessarily reflect the views of NASA or ORAU. The author would like to thank Ernesto Hugo Berbery and Fedor Mesinger for early discussions about NARR's water cycle, Ying Lin for extensive assistance in revisiting NARR's precipitation assimilation scheme, Perry Shafran and Wesley Ebisuzaki for insight into the sources of precipitation assimilation, Radley Horton for multiple edits, Masao Kanamitsu for helpful advice, and anonymous reviewers of this manuscript. Anonymous reviewers of Part I were also helpful in shaping the tone and structure of this companion article. NR 44 TC 17 Z9 17 U1 1 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2010 VL 11 IS 6 BP 1220 EP 1233 DI 10.1175/2010JHM1279.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 705ZE UT WOS:000286178800002 ER PT J AU Tian, YD Peters-Lidard, CD Eylander, JB AF Tian, Yudong Peters-Lidard, Christa D. Eylander, John B. TI Real-Time Bias Reduction for Satellite-Based Precipitation Estimates SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID DATA ASSIMILATION; UNITED-STATES; RAINFALL; RESOLUTION; SYSTEM; GAUGE; VALIDATION; PRODUCTS; RADAR AB A new approach to reduce biases in satellite-based estimates in real time is proposed and tested in this study. Currently satellite-based precipitation estimates exhibit considerable biases, and there have been many efforts to reduce these biases by merging surface gauge measurements with satellite-based estimates. Most of these efforts require timely availability of surface gauge measurements. The new proposed approach does not require gauge measurements in real time. Instead, the Bayesian logic is used to establish a statistical relationship between satellite estimates and gauge measurements from recent historical data. Then this relationship is applied to real-time satellite estimates when gauge data are not yet available. This new scheme is tested over the United States with six years of precipitation estimates from two real-time satellite products [i.e., the Tropical Rainfall Measuring Mission (TRMM) Multisatellite Precipitation Analysis (TMPA) research product 3B42RT and the NOAA Climate Prediction Center (CPC) Morphing technique (CMORPH)] and a gauge analysis dataset [i.e., the CPC unified analysis]. The first 4-yr period was used as the training period to establish a satellite-gauge relationship, which was then applied to the last 2 yr as the correction period, during which gauge data were withheld for training but only used for evaluation. This approach showed that satellite biases were reduced by 70%-100% for the summers in the correction period. In addition, even when sparse networks with only 600 or 300 gauges were used during the training period, the biases were still reduced by 60%-80% and 47%-63%, respectively. The results also show a limitation in this approach as it tends to overadjust both light and strong events toward more intermediate rain rates. C1 [Tian, Yudong; Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Eylander, John B.] USAF, Weather Agcy, Air & Space Models Integrat Branch, Offutt AFB, NE USA. RP Tian, YD (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Mail Code 614-3, Greenbelt, MD 20771 USA. EM Yudong.Tian@nasa.gov RI Measurement, Global/C-4698-2015; Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 FU Air Force Weather Agency MIPR [F2BBAJ6033GB01] FX This research is supported by the Air Force Weather Agency MIPR F2BBAJ6033GB01. The authors wish to thank Dr. Kenneth Harrison for reviewing our manuscript, and Mingyue Chen, Mathew Sapiano, Dan Braithwaite, Hiroko Kato Beaudoing, and Pingping Xie for helpful discussions and for assistance with data access. NR 26 TC 30 Z9 31 U1 3 U2 23 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2010 VL 11 IS 6 BP 1275 EP 1285 DI 10.1175/2010JHM1246.1 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 705ZE UT WOS:000286178800005 ER PT J AU Rhoden, AR Militzer, B Huff, EM Hurford, TA Manga, M Richards, MA AF Rhoden, Alyssa Rose Militzer, Burkhard Huff, Eric M. Hurford, Terry A. Manga, Michael Richards, Mark A. TI Constraints on Europa's rotational dynamics from modeling of tidally-driven fractures SO ICARUS LA English DT Article DE Europa; Tectonics; Rotational dynamics ID NONSYNCHRONOUS ROTATION; GALILEAN SATELLITES; SUBSURFACE OCEAN; ICE SHELLS; MECHANICS; FEATURES; PLANET; CRACKS; MOONS AB Cycloids, arcuate features observed on Europa's surface, have been interpreted as tensile cracks that form in response to diurnal tidal stress caused by Europa's orbital eccentricity. Stress from non-synchronous rotation may also contribute to tidal stress, and its influence on cycloid shapes has been investigated as well. Obliquity, fast precession, and physical libration would contribute to tidal stress but have often been neglected because they were expected to be negligibly small. However, more sophisticated analyses that include the influence of Jupiter's other large satellites and the state of Europa's interior indicate that perhaps these rotational parameters are large enough to alter the tidal stress field and the formation of tidally-driven fractures. We test tidal models that include obliquity, fast precession, stress due to non-synchronous rotation, and physical libration by comparing how well each model reproduces observed cycloids. To do this, we have designed and implemented an automated parameter-searching algorithm that relies on a quantitative measure of fit quality, which we use to identify the best fits to observed cycloids. We then apply statistical techniques to determine the tidal model best supported by the data. By incorporating obliquity, fits to observed southern hemisphere cycloids improve, and we can reproduce equatorial and equator-crossing cycloids. Furthermore, we find that obliquity plus physical libration is the tidal model best supported by the data. With this model, the obliquities range from 0.32 degrees to 1.35 degrees. The libration amplitudes are 0.72-2.44 degrees, and the libration phases are -6.04 degrees to 17.72 degrees with one outlier at 84.5 degrees. The variability in obliquity is expected if Europa's ice shell is mechanically decoupled from the interior, and the libration amplitudes are plausible in the presence of a subsurface ocean. Indeed, the presence of a decoupling ocean may result in feedbacks that cause all of these rotational parameters to become time-variable. (C) 2010 Elsevier Inc. All rights reserved. C1 [Rhoden, Alyssa Rose; Militzer, Burkhard; Manga, Michael; Richards, Mark A.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Militzer, Burkhard; Huff, Eric M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Huff, Eric M.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Hurford, Terry A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rhoden, AR (reprint author), Univ Calif Berkeley, Dept Earth & Planetary Sci, 307 McCone Hall, Berkeley, CA 94720 USA. EM alyssa@eps.berkeley.edu RI Hurford, Terry/F-2625-2012; Manga, Michael/D-3847-2013; OI Manga, Michael/0000-0003-3286-4682 FU NAI program; NESSF program FX The authors wish to thank J. Bernstein at Penguin Computing for use of computational resources, two anonymous reviewers for their constructive comments, and the NAI and NESSF programs for funding this work. NR 36 TC 13 Z9 13 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 DEC PY 2010 VL 210 IS 2 BP 770 EP 784 DI 10.1016/j.icarus.2010.07.018 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679RP UT WOS:000284178800017 ER PT J AU Iraci, LT Phebus, BD Stone, BM Colaprete, A AF Iraci, Laura T. Phebus, Bruce D. Stone, Bradley M. Colaprete, Anthony TI Water ice cloud formation on Mars is more difficult than presumed: Laboratory studies of ice nucleation on surrogate materials SO ICARUS LA English DT Article DE Mars; Ices; Mars, Atmosphere; Atmospheres, Composition ID MINERAL DUST PARTICLES; MARTIAN ATMOSPHERE; SUMMER MESOSPHERE; MODEL; VAPOR; TEMPERATURES; SIMULATIONS; ADSORPTION; CHEMISTRY; CHAMBER AB The role of water ice clouds in the martian water cycle and climate depends on cloud properties such as particle size and number distribution. These properties, in turn, depend on heterogeneous nucleation parameters which are poorly understood. Here we report laboratory experiments performed under martian temperature and water partial pressure conditions (158-185 K, 9 x 10(-7)-1 x 10(-4) Ton H2O) to determine the critical saturation ratio for ice onset, S-crit, as a function of temperature and dust composition. Using infrared spectroscopy to monitor ice nucleation and growth, we find a significant barrier to ice formation, with a pronounced temperature dependence. Even on clay minerals which show uptake of non-crystalline water before ice nucleation, we find a saturation ratio of 2.5 or more (RHice > 250%) is needed to begin ice growth at temperatures near 160 K. These results could lead to changes of four orders of magnitude in the nucleation rate relative to the presumptions used currently in Mars microphysical models, which commonly set the contact parameter, m, to a single value of 0.95. Our results range from m = 0.84 to m = 0.98. For ice nucleation on Arizona Test Dust, the temperature dependence is described by m = 0.0046 * T-nucl + 0.1085, while m = 0.0055 * T-nucl + 0.0003 on a smectite-rich clay sample. Our findings suggest that cloud formation will be more difficult than previously thought, potentially leading to areas of increased near-surface humidity but generally drier conditions in the atmosphere of Mars, overall. Published by Elsevier Inc. C1 [Iraci, Laura T.; Phebus, Bruce D.; Colaprete, Anthony] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Phebus, Bruce D.; Stone, Bradley M.] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA. RP Iraci, LT (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM laura.t.iraci@nasa.gov OI Phebus, Bruce/0000-0003-3489-5546 FU NASA FX The authors thank D. Scimeca, E. Quigley, R. Reed, and P. Deng for design and assembly of the apparatus. E. Jensen at KLA-Tencor imbedded the thermocouple for gradient measurements. O. Marcu and M. Sanchez made possible the micrographs of the clay samples; C. Dalle Ore counted the particle sizes, and T. Roush identified the mineralogy. M. Trainer graciously shared her data prior to publication. Two reviewers provided helpful comments, and useful discussions with B. Mar, R. Terrill, A. Maattanen, and M. Trainer are gratefully acknowledged. The initial assistance of R. Mastrapa is also appreciated. Funding for this work was provided by the NASA Planetary Atmospheres Program (P. Crane, Program Officer). NR 55 TC 19 Z9 19 U1 1 U2 13 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2010 VL 210 IS 2 BP 985 EP 991 DI 10.1016/j.icarus.2010.07.020 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679RP UT WOS:000284178800032 ER PT J AU Silan, JL Niemann, DL Maya, BP Rahman, M Meyyappan, M Nguyen, CV AF Silan, Jeremy L. Niemann, Darrell L. Maya, Bryan P. Rahman, Mahmud Meyyappan, M. Nguyen, Cattien V. TI Investigation of carbon nanotube field emitter geometry for increased current density SO SOLID-STATE ELECTRONICS LA English DT Article DE Carbon nanotube; Field emission; Edge effect; Emitter array ID EMISSION PROPERTIES; ARRAYS AB In this work we present field emission characteristics of four geometrically distinct carbon nanotube pillar arrays Each cathode has a unique geometric configuration with different structural parameters such as number of edges and vertices We present experimental data demonstrating a carbon nanotube cold field emitter with an emitted current density of 31 8 mA/cm(2) at an applied field of 11 V/mu m The performance of these cathodes can be directly attributed to the electric field being enhanced along the edges and vertices of the structures We investigated this phenomenon experimentally by changing the geometry of the carbon nanotube pillar structure We show that by increasing the number of edges and vertices of a structure to keep the electric field screening to a minimum the emission current can be increased (C) 2010 Elsevier Ltd All rights reserved C1 [Silan, Jeremy L.; Niemann, Darrell L.; Maya, Bryan P.; Rahman, Mahmud] Santa Clara Univ, Dept Elect Engn, Elect Devices Lab, Santa Clara, CA 95053 USA. [Nguyen, Cattien V.] ELORET Corp, Moffett Field, CA 94035 USA. [Silan, Jeremy L.; Niemann, Darrell L.; Maya, Bryan P.; Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Rahman, M (reprint author), Santa Clara Univ, Dept Elect Engn, Elect Devices Lab, Santa Clara, CA 95053 USA. NR 22 TC 6 Z9 7 U1 1 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-1101 J9 SOLID STATE ELECTRON JI Solid-State Electron. PD DEC PY 2010 VL 54 IS 12 BP 1543 EP 1548 DI 10.1016/j.sse.2010.07.004 PG 6 WC Engineering, Electrical & Electronic; Physics, Applied; Physics, Condensed Matter SC Engineering; Physics GA 677GV UT WOS:000283978000010 ER PT J AU Yoonessi, M Gaier, JR AF Yoonessi, Mitra Gaier, James R. TI Highly Conductive Multifunctional Graphene Polycarbonate Nanocomposites SO ACS NANO LA English DT Article DE nanocomposite; electrical conductivity; graphene; scattering ID CARBON NANOTUBE COMPOSITES; ELECTRICAL-CONDUCTIVITY; FUNCTIONALIZED GRAPHENE; PERCOLATION-THRESHOLD; DISORDERED SOLIDS; AC CONDUCTIVITY; GRAPHITE; MICROSCOPY; DC; SCATTERING AB Graphene nanosheet - bisphenol A polycarbonate nanocomposites (0.027-2.2 vol %) prepared by both emulsion mixing and solution blending methods, followed by compression molding at 287 degrees C, exhibited dc electrical percolation threshold of similar to 0.14 and similar to 0.38 vol %, respectively. The conductivities of 2.2 vol % graphene nanocomposites were 0.512 and 0.226 S/cm for emulsion and solution mixing. The 1.1 and 2.2 vol % graphene nanocomposites exhibited frequency-independent behavior. Inherent conductivity, extremely high aspect ratio, and nanostructure directed assembly of the graphene using PC nanospheres are the main factors for excellent electrical properties of the nanocomposites. Dynamic tensile moduli of nanocomposites increased with increasing graphene in the nanocomposite. The glass transition temperatures were decreased with increasing graphene for the emulsion series. High-resolution electron microscopy (HR-TEM) and small-angle neutron scattering (SANS) showed isolated graphene with no connectivity path for insulating nanocomposites and connected nanoparticles for the conductive nanocomposites. A stacked disk model was used to obtain the average particle radius, average number of graphene layers per stack, and stack spacing by simulation of the experimental SANS data. Morphology studies indicated the presence of well-dispersed graphene and small graphene stacking with infusion of polycarbonate within the stacks. C1 [Yoonessi, Mitra; Gaier, James R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Yoonessi, Mitra] Ohio Aerosp Inst, Cleveland, OH 44142 USA. RP Yoonessi, M (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM mitra.yoonessi@nasa.gov FU NASA [NNC07BA13B]; NIST [S23-59]; National Science Foundation [DMR-9986442] FX The NASA Aeronautics-Subsonic Fixed Wing Program is thanked for the funding through Contract NNC07BA13B. M.A. Meador is thanked for the invaluable support. R. Rogers, D. Hull, F. So la, and D. Scheiman of NASA-GRC, Y. Lin and D. Mildner of NCNR-NIST are thanked. R. Ruoff and J. Potts of University of Texas-Austin and S. Kline of NCNR-NIST are thanked for their helpful comments. NIST is thanked for funding (Proposal S23-59) to conduct neutron scattering experiments which were supported by National Science Foundation under agreement DMR-9986442. The mention of commercial products does not imply endorsement by NIST nor does it imply that the materials or equipment identified are necessarily the best available for the purpose. NR 41 TC 151 Z9 155 U1 17 U2 182 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1936-0851 J9 ACS NANO JI ACS Nano PD DEC PY 2010 VL 4 IS 12 BP 7211 EP 7220 DI 10.1021/nn1019626 PG 10 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA 696NW UT WOS:000285449100022 PM 21082818 ER PT J AU Erkmen, BI Shapiro, JH AF Erkmen, Baris I. Shapiro, Jeffrey H. TI Ghost imaging: from quantum to classical to computational SO ADVANCES IN OPTICS AND PHOTONICS LA English DT Article ID 2-PHOTON COHERENT STATES; OPTICAL COMMUNICATION; THERMAL LIGHT; INTERFERENCE; NOISE AB Ghost-imaging experiments correlate the outputs from two photodetectors: a high-spatial-resolution (scanning pinhole or CCD array) detector that measures a field that has not interacted with the object to be imaged, and a bucket (single-pixel) detector that collects a field that has interacted with the object. We give a comprehensive review of ghost imaging-within a unified Gaussian-state framework-presenting detailed analyses of its resolution, field of view, image contrast, and signal-to-noise ratio behavior. We consider three classes of illumination: thermal-state (classical), biphoton-state (quantum), and classical-state phase-sensitive light. The first two have been employed in a variety of ghost-imaging demonstrations. The third is the classical Gaussian state that produces ghost images that most closely mimic those obtained from biphoton illumination. The insights we develop lead naturally to a new, single-beam approach to ghost imaging, called computational ghost imaging, in which only the bucket detector is required. We provide quantitative results while simultaneously emphasizing the underlying physics of ghost imaging. The key to developing the latter understanding lies in the coherence behavior of a pair of Gaussian-state light beams with either phase-insensitive or phase-sensitive cross correlation. (C) 2010 Optical Society of America C1 [Erkmen, Baris I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shapiro, Jeffrey H.] MIT, Elect Res Lab, Cambridge, MA 02139 USA. RP Erkmen, BI (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM baris.i.erkmen@jpl.nasa.gov FU U.S. Army Research Office MURI grant [W911NF-05-0197]; W. M. Keck Foundation Center for Extreme Quantum Information Theory; DARPA Quantum Sensors Program FX The authors thank F. N. C. Wong for insightful discussions and for performing the speckle measurements whose results appear in Fig. 7. The research described in this paper was carried out at MIT with support from the U.S. Army Research Office MURI grant W911NF-05-0197, the W. M. Keck Foundation Center for Extreme Quantum Information Theory, and the DARPA Quantum Sensors Program. B. I. Erkmen's contribution to writing this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 65 TC 93 Z9 94 U1 7 U2 35 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1943-8206 J9 ADV OPT PHOTONICS JI Adv. Opt. Photonics PD DEC PY 2010 VL 2 IS 4 BP 405 EP 450 DI 10.1364/AOP.2.000405 PG 46 WC Optics SC Optics GA V30VX UT WOS:000208844600001 ER PT J AU Friedland, P AF Friedland, Peter TI The 2008 Classic Paper Award: Summary and Significance SO AI MAGAZINE LA English DT Editorial Material AB We at the NASA laboratory believed that our best work came when we simultaneously advanced AI theory and provided immediately usable solutions for current NASA problems. "Solving Large-Scale Constraint Satisfaction and Scheduling Problems Using a Heuristic Repair Method," by Steve Minton, Mark Johnston, Andy Phillips, and Phil Laird clearly achieved both. It proved that local search and repair was applicable to a wide class of constraint-satisfaction problems and clearly explicated the theory behind that proof. C1 [Friedland, Peter] NASA, Extens Collaborat Program Ind & Acad, Washington, DC USA. [Friedland, Peter] NASA, Ames Res Ctr, Artificial Intelligence Res Branch, Washington, DC USA. [Friedland, Peter] MOLGEN Project, Stanford, CA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD WIN PY 2010 VL 31 IS 4 BP 109 EP 110 PG 2 WC Computer Science, Artificial Intelligence SC Computer Science GA 713BV UT WOS:000286710900008 ER PT J AU Morris, PJ Miller, SAE AF Morris, Philip J. Miller, Steven A. E. TI Prediction of Broadband Shock-Associated Noise Using Reynolds-Averaged Navier-Stokes Computational Fluid Dynamics SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA/CEAS 15th Aeroacoustics Conference CY MAY 11-13, 2009 CL Miami, FL SP Amer Inst Aeronaut & Astronaut, CEAS ID EXPANDED SUPERSONIC JETS; MODEL; TURBULENCE AB Broadband shock associated noise is a component of jet noise generated by supersonic jets operating offdesign It is characterized by multiple broadband peaks and dominates the total noise at large angles to the jet downstream axis A new model is introduced for the prediction of broadband shock associated noise that uses the solution of the Reynolds averaged Navier-Stokes equations The noise model is an acoustic analogy based on the linearized Euler equations The equivalent source terms depend on the product of the fluctuations associated with the jet's shock cell structure and the turbulent velocity fluctuations in the jet shear layer The former are deterministic and are obtained from the Reynolds-averaged Navier Stokes solution A statistical model is introduced to describe the properties of the turbulence Only the geometry and operating conditions of the nozzle need to be known to make noise predictions This overcomes the limitations and empiricism present in previous broadband shock-associated noise models Results for various axisymmetric circular nozzles and a rectangular nozzle operating at various conditions are compared with experimental data to validate the model C1 [Morris, Philip J.] Penn State Univ, Dept Aerosp Engn, University Pk, PA 16803 USA. [Miller, Steven A. E.] NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23681 USA. RP Morris, PJ (reprint author), Penn State Univ, Dept Aerosp Engn, 229 Hammond Bldg, University Pk, PA 16803 USA. NR 25 TC 12 Z9 12 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD DEC PY 2010 VL 48 IS 12 BP 2931 EP 2944 DI 10.2514/1.J050560 PG 14 WC Engineering, Aerospace SC Engineering GA 689KJ UT WOS:000284926200018 ER PT J AU Merlo, JL Duley, AR Hancock, PA AF Merlo, James L. Duley, Aaron R. Hancock, Peter A. TI Cross-modal congruency benefits for combined tactile and visual signaling SO AMERICAN JOURNAL OF PSYCHOLOGY LA English DT Article ID MULTISENSORY INTEGRATION; SUPERIOR COLLICULUS; MOTION PERCEPTION; INFORMATION; MODEL; CAT; ATTENTION; NEURONS; VISION; TOUCH AB This series of experiments tested the assimilation and efficacy of tactile messages that were created based on five common military arm and hand signals. We compared the response times and accuracy rates for these tactile representations against responses to equivalent visual representations of the same messages. Experimentally, such messages were displayed in either tactile or visual forms alone, or using both modalities in combination. There was a performance benefit for concurrent message presentations, which showed superior response times and improved accuracy rates when compared with individual presentations in either modality alone. Such improvement was due largely to a reduction in premotor response time. These improvements occurred equally in military and nonmilitary samples. Potential reasons for this multimodal facilitation are discussed. On a practical level, these results confirm the utility of tactile messaging to augment visual messaging, especially in challenging and stressful environments where visual messaging is not feasible or effective. C1 [Merlo, James L.] US Mil Acad, West Point, NY 10996 USA. [Duley, Aaron R.] NASA, Ames Res Ctr, Washington, DC 20546 USA. [Hancock, Peter A.] Univ Cent Florida, Orlando, FL 32816 USA. RP Merlo, JL (reprint author), US Mil Acad, West Point, NY 10996 USA. EM james.merlo@usma.edu NR 36 TC 5 Z9 5 U1 0 U2 3 PU UNIV ILLINOIS PRESS PI CHAMPAIGN PA 1325 S OAK ST, CHAMPAIGN, IL 61820-6903 USA SN 0002-9556 J9 AM J PSYCHOL JI Am. J. Psychol. PD WIN PY 2010 VL 123 IS 4 BP 413 EP 424 PG 12 WC Psychology, Multidisciplinary SC Psychology GA 699UI UT WOS:000285688000004 PM 21291158 ER PT J AU Gurgiolo, C Goldstein, ML Vinas, AF Fazakerley, AN AF Gurgiolo, C. Goldstein, M. L. Vinas, A. F. Fazakerley, A. N. TI First measurements of electron vorticity in the foreshock and solar wind SO ANNALES GEOPHYSICAE LA English DT Article DE Interplanetary physics; Plasma waves and turbulence; Solar wind plasma; Instruments and techniques ID HELIOSPHERIC VORTEX STREET; NORTH-SOUTH FLOWS; BOW SHOCK; OUTER HELIOSPHERE; AU AB We describe the methodology used to set up and compute spatial derivatives of the electron moments using data acquired by the Plasma Electron And Current Experiment (PEACE) from the four Cluster spacecraft. The results are used to investigate electron vorticity in the fore-shock. We find that much of the measured vorticity, under nominal conditions, appears to be caused by changes in the flow direction of the return (either reflected or leakage from the magnetosheath) and strahl electron populations as they couple to changes in the magnetic field orientation. This in turn results in deflections in the total bulk velocity producing the measured vorticity. C1 [Gurgiolo, C.] Bitterroot Basic Res, Hamilton, MT USA. [Goldstein, M. L.; Vinas, A. F.] NASA, Goddard Space Flight Ctr, Geospace Sci Lab, Greenbelt, MD 20771 USA. [Fazakerley, A. N.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary Dorking RH5 6NT, Surrey, England. RP Gurgiolo, C (reprint author), Bitterroot Basic Res, Hamilton, MT USA. EM chris@gurgiolo.com RI Goldstein, Melvyn/B-1724-2008 FU NASA [NNX10AC90G] FX The authors would like to acknowledge the work and role the Cluster Active Archive (CAA) and thank the CIS, EFW, WHISPER and FGM teams for providing the data used in this study. We would also like to acknowledge the PEACE team at MSSL who worked on and are constantly improving the instrument calibration as well as the two referees for their thoughtful and excellent comments. CG would like to acknowledge support from NASA Grant NNX10AC90G. NR 28 TC 4 Z9 4 U1 0 U2 0 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PD DEC PY 2010 VL 28 IS 12 BP 2187 EP 2200 DI 10.5194/angeo-28-2187-2010 PG 14 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 698HL UT WOS:000285584800004 ER PT J AU Muterspaugh, MW Lane, BF Kulkarni, SR Konacki, M Burke, BF Colavita, MM Shao, M Wiktorowicz, SJ O'Connell, J AF Muterspaugh, Matthew W. Lane, Benjamin F. Kulkarni, S. R. Konacki, Maciej Burke, Bernard F. Colavita, M. M. Shao, M. Wiktorowicz, Sloane J. O'Connell, J. TI THE PHASES DIFFERENTIAL ASTROMETRY DATA ARCHIVE. I. MEASUREMENTS AND DESCRIPTION SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; binaries: close; binaries: visual; techniques: interferometric ID PALOMAR TESTBED INTERFEROMETER; STAR SYSTEM; PLANETS AB The Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES) monitored 51 subarcsecond binary systems to determine precision binary orbits, study the geometries of triple and quadruple star systems, and discover previously unknown faint astrometric companions as small as giant planets. PHASES measurements made with the Palomar Testbed Interferometer (PTI) from 2002 until PTI ceased normal operations in late 2008 are presented. Infrared differential photometry of several PHASES targets were measured with Keck Adaptive Optics and are presented. C1 [Muterspaugh, Matthew W.; O'Connell, J.] Tennessee State Univ, Coll Arts & Sci, Dept Math & Phys, Nashville, TN 37209 USA. [Muterspaugh, Matthew W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Lane, Benjamin F.] Draper Lab, Cambridge, MA 02139 USA. [Kulkarni, S. R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Konacki, Maciej] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. [Konacki, Maciej] Adam Mickiewicz Univ Poznan, Astron Observ, PL-60286 Poznan, Poland. [Burke, Bernard F.] MIT, Dept Phys, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Colavita, M. M.; Shao, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wiktorowicz, Sloane J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Muterspaugh, MW (reprint author), Tennessee State Univ, Coll Arts & Sci, Dept Math & Phys, Boswell Sci Hall, Nashville, TN 37209 USA. EM matthew1@coe.tsuniv.edu; blane@draper.com; maciej@ncac.torun.pl FU NASA [NAS7-03001 (JPL 1336910)]; National Science Foundation [AST 0300096, AST 0507590, AST 0505366]; Townes Fellowship Program; Tennessee State University; State of Tennessee through its Centers of Excellence program; California Institute of Technology Astronomy Department; National Aeronautics and Space Administration [NNG05GJ58G]; Foundation for Polish Science; Polish Ministry of Science and Higher Education [N203 3020 35] FX Though it has no impact on the current study, as an astrometry team we could not resist pointing out that-due to precession-PHASES target HD 149630 (sigma Her) was the pole star around 8250 BC. PHASES benefits from the efforts of the PTI collaboration members who have each contributed to the development of an extremely reliable observational instrument. Without this outstanding engineering effort to produce a solid foundation, advanced phase-referencing techniques would not have been possible. We thank PTI's night assistant Kevin Rykoski for his efforts to maintain PTI in excellent condition and operating PTI in phase-referencing mode every week. Part of the work described in this paper was performed at the Jet Propulsion Laboratory under contract with the National Aeronautics and Space Administration. Interferometer data were obtained at the Palomar Observatory with the NASA Palomar Testbed Interferometer, supported by NASA contracts to the Jet Propulsion Laboratory. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. M.W.M. acknowledges support from the Townes Fellowship Program, Tennessee State University, and the state of Tennessee through its Centers of Excellence program. Some of the software used for analysis was developed as part of the SIM Double Blind Test with support from NASA contract NAS7-03001 (JPL 1336910). PHASES is funded in part by the California Institute of Technology Astronomy Department, and by the National Aeronautics and Space Administration under grant no. NNG05GJ58G issued through the Terrestrial Planet Finder Foundation Science Program. This work was supported in part by the National Science Foundation through grants AST 0300096, AST 0507590, and AST 0505366. M.K. is supported by the Foundation for Polish Science through a FOCUS grant and fellowship, by the Polish Ministry of Science and Higher Education through grant N203 3020 35. NR 22 TC 13 Z9 13 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2010 VL 140 IS 6 BP 1579 EP 1622 DI 10.1088/0004-6256/140/6/1579 PG 44 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500002 ER PT J AU Muterspaugh, MW Hartkopf, WI Lane, BF O'Connell, J Williamson, M Kulkarni, SR Konacki, M Burke, BF Colavita, MM Shao, M Wiktorowicz, SJ AF Muterspaugh, Matthew W. Hartkopf, William I. Lane, Benjamin F. O'Connell, J. Williamson, M. Kulkarni, S. R. Konacki, Maciej Burke, Bernard F. Colavita, M. M. Shao, M. Wiktorowicz, Sloane J. TI THE PHASES DIFFERENTIAL ASTROMETRY DATA ARCHIVE. II. UPDATED BINARY STAR ORBITS AND A LONG PERIOD ECLIPSING BINARY SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; binaries: close; binaries: eclipsing; binaries: visual; techniques: interferometric ID RADIAL-VELOCITY OBSERVATIONS; PALOMAR TESTBED INTERFEROMETER; SOLAR-TYPE STARS; SPECTROSCOPIC BINARIES; PRECISION ASTROMETRY; ADAPTIVE OPTICS; SYSTEM; MULTIPLICITY; MASSES; TELESCOPE AB Differential astrometry measurements from the Palomar High-precision Astrometric Search for Exoplanet Systems have been combined with lower precision single-aperture measurements covering a much longer timespan ( from eyepiece measurements, speckle interferometry, and adaptive optics) to determine improved visual orbits for 20 binary stars. In some cases, radial velocity observations exist to constrain the full three-dimensional orbit and determine component masses. The visual orbit of one of these binaries-alpha Com ( HD 114378)-shows that the system is likely to have eclipses, despite its very long period of 26 years. The next eclipse is predicted to be within a week of 2015 January 24. C1 [Muterspaugh, Matthew W.; O'Connell, J.] Tennessee State Univ, Coll Arts & Sci, Dept Math & Phys, Nashville, TN 37209 USA. [Muterspaugh, Matthew W.; Williamson, M.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Hartkopf, William I.] USN Observ, Washington, DC 20392 USA. [Lane, Benjamin F.] Draper Lab, Cambridge, MA 02139 USA. [Kulkarni, S. R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Konacki, Maciej] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. [Konacki, Maciej] Adam Mickiewicz Univ Poznan, Astron Observ, PL-60286 Poznan, Poland. [Burke, Bernard F.] MIT, Dept Phys, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Colavita, M. M.; Shao, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wiktorowicz, Sloane J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Muterspaugh, MW (reprint author), Tennessee State Univ, Coll Arts & Sci, Dept Math & Phys, Boswell Sci Hall, Nashville, TN 37209 USA. EM matthew1@coe.tsuniv.edu; wih@usno.navy.mil; blane@draper.com; maciej@ncac.torun.pl FU National Aeronautics and Space Administration [NNG05GJ58G]; NASA [NAS7-03001 (JPL 1336910)]; National Science Foundation [AST 0300096, AST 0507590, AST 0505366]; Townes Fellowship Program; Tennessee State University; State of Tennessee through its Centers of Excellence program; California Institute of Technology Astronomy Department; Foundation for Polish Science; Polish Ministry of Science and Higher Education [N203 3020 35] FX PHASES benefits from the efforts of the PTI collaboration members who have each contributed to the development of an extremely reliable observational instrument. Without this outstanding engineering effort to produce a solid foundation, advanced phase-referencing techniques would not have been possible. We thank PTI's night assistant Kevin Rykoski for his efforts to maintain PTI in excellent condition and operating PTI in phase-referencing mode every week. Thanks are also extended to Ken Johnston and the U. S. Naval Observatory for their continued support of the USNO Double Star Program. Part of the work described in this paper was performed at the Jet Propulsion Laboratory under contract with the National Aeronautics and Space Administration. Interferometer data were obtained at the Palomar Observatory with the NASA Palomar Testbed Interferometer, supported by NASA contracts to the Jet Propulsion Laboratory. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. This research has made use of SAOImage DS9, developed by the Smithsonian Astrophysical Observatory. M.W.M. acknowledges support from the Townes Fellowship Program, Tennessee State University, and the state of Tennessee through its Centers of Excellence program. Some of the software used for analysis was developed as part of the SIM Double Blind Test with support from NASA contract NAS7-03001 (JPL 1336910). PHASES is funded in part by the California Institute of Technology Astronomy Department and by the National Aeronautics and Space Administration under grant No. NNG05GJ58G issued through the Terrestrial Planet Finder Foundation Science Program. This work was supported in part by the National Science Foundation through grants AST 0300096, AST 0507590, and AST 0505366. M.K. is supported by the Foundation for Polish Science through a FOCUS grant and fellowship, by the Polish Ministry of Science and Higher Education through grant N203 3020 35. NR 47 TC 26 Z9 26 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2010 VL 140 IS 6 BP 1623 EP 1630 DI 10.1088/0004-6256/140/6/1623 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500003 ER PT J AU Muterspaugh, MW Lane, BF Kulkarni, SR Konacki, M Burke, BF Colavita, MM Shao, M AF Muterspaugh, Matthew W. Lane, Benjamin F. Kulkarni, S. R. Konacki, Maciej Burke, Bernard F. Colavita, M. M. Shao, M. TI THE PHASES DIFFERENTIAL ASTROMETRY DATA ARCHIVE. III. LIMITS TO TERTIARY COMPANIONS SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; binaries: close; binaries: visual; techniques: interferometric ID SOLAR-TYPE STARS; PALOMAR TESTBED INTERFEROMETER; BINARY-SYSTEMS; GIANT PLANET; RADIAL-VELOCITIES; CORALIE SURVEY; IMAGING SURVEY; MULTIPLICITY; ORBITS; EXOPLANETS AB The Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES) monitored 51 subarcsecond binary systems to evaluate whether tertiary companions as small as Jovian planets orbited either the primary or secondary stars, perturbing their otherwise smooth Keplerian motions. Twenty-one of those systems were observed 10 or more times and show no evidence of additional companions. A new algorithm is presented for identifying astrometric companions and establishing the (companion mass)-(orbital period) combinations that can be excluded from existence with high confidence based on the PHASES observations, and the regions of mass-period phase space being excluded are presented for 21 PHASES binaries. C1 [Muterspaugh, Matthew W.] Tennessee State Univ, Coll Arts & Sci, Dept Math & Phys, Nashville, TN 37209 USA. [Muterspaugh, Matthew W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Lane, Benjamin F.] Draper Lab, Cambridge, MA 02139 USA. [Kulkarni, S. R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Konacki, Maciej] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. [Konacki, Maciej] Adam Mickiewicz Univ Poznan, Astron Observ, PL-60286 Poznan, Poland. [Burke, Bernard F.] MIT, Dept Phys, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Colavita, M. M.; Shao, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Muterspaugh, MW (reprint author), Tennessee State Univ, Coll Arts & Sci, Dept Math & Phys, Boswell Sci Hall, Nashville, TN 37209 USA. EM matthew1@coe.tsuniv.edu; blane@draper.com; maciej@ncac.torun.pl FU National Aeronautics and Space Administration [NNG05GJ58G]; NASA [NAS7-03001 (JPL 1336910)]; National Science Foundation [AST 0300096, AST 0507590, AST 0505366]; Townes Fellowship Program; Tennessee State University; State of Tennessee through its Centers of Excellence program; California Institute of Technology Astronomy Department; Foundation for Polish Science; Polish Ministry of Science and Higher Education [N203 3020 35] FX PHASES benefits from the efforts of the PTI collaboration members who have each contributed to the development of an extremely reliable observational instrument. Without this outstanding engineering effort to produce a solid foundation, advanced phase-referencing techniques would not have been possible. We thank PTI's night assistant Kevin Rykoski for his efforts to maintain PTI in excellent condition and operating PTI in phase-referencing mode every week. Part of the work described in this paper was performed at the Jet Propulsion Laboratory under contract with the National Aeronautics and Space Administration. Interferometer data were obtained at the Palomar Observatory with the NASA Palomar Testbed Interferometer, supported by NASA contracts to the Jet Propulsion Laboratory. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. M.W.M. acknowledges support from the Townes Fellowship Program, Tennessee State University, and the state of Tennessee through its Centers of Excellence program. Some of the software used for analysis was developed as part of the SIM Double Blind Test with support from NASA contract NAS7-03001 (JPL 1336910). PHASES is funded in part by the California Institute of Technology Astronomy Department, and by the National Aeronautics and Space Administration under grant no. NNG05GJ58G issued through the Terrestrial Planet Finder Foundation Science Program. This work was supported in part by the National Science Foundation through grants AST 0300096, AST 0507590, and AST 0505366. M. K. is supported by the Foundation for Polish Science through a FOCUS grant and fellowship, by the Polish Ministry of Science and Higher Education through grant N203 3020 35. NR 56 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2010 VL 140 IS 6 BP 1631 EP 1645 DI 10.1088/0004-6256/140/6/1631 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500004 ER PT J AU Muterspaugh, MW Fekel, FC Lane, BF Hartkopf, WI Kulkarni, SR Konacki, M Burke, BF Colavita, MM Shao, M Williamson, M AF Muterspaugh, Matthew W. Fekel, Francis C. Lane, Benjamin F. Hartkopf, William I. Kulkarni, S. R. Konacki, Maciej Burke, Bernard F. Colavita, M. M. Shao, M. Williamson, M. TI THE PHASES DIFFERENTIAL ASTROMETRY DATA ARCHIVE. IV. THE TRIPLE STAR SYSTEMS 63 Gem A AND HR 2896 SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; binaries: close; binaries: visual ID PALOMAR TESTBED INTERFEROMETER; BINARY-SYSTEMS; PLANET SEARCH; CHARA ARRAY; DETECTABILITY; ORBITS; MASS AB Differential astrometry measurements from the Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES) are used to constrain the astrometric orbit of the previously known less than or similar to 2 day subsystem in the triple system 63 Gem A and have detected a previously unknown two-year Keplerian wobble superimposed on the visual orbit of the much longer period (213 years) binary system HR 2896. 63 Gem A was already known to be triple from spectroscopic work, and absorption lines from all three stars can be identified and their individual Doppler shifts measured; new velocities for all three components are presented to aid in constraining the orbit and measuring the stellar masses. In fact, 63 Gem itself is a sextuple system: the hierarchical triple (Aa1-Aa2)-Ab (in which Aa1 and Aa2 orbit each other with a rapid period just under 2 days, and Ab orbits these every two years), plus three distant common proper motion companions. The very small astrometric perturbation caused by the inner pair in 63 Gem A stretches the limits of current astrometric capabilities, but PHASES observations are able to constrain the orientation of the orbit. The two bright stars comprising the HR 2896 long-period (213 year) system have a combined spectral type of K0III and the newly detected object's mass estimate places it in the regime of being an M dwarf. The motion of the stars are slow enough that their spectral features are always blended, preventing Doppler studies. The PHASES measurements and radial velocities (when available) have been combined with lower precision single-aperture measurements covering a much longer time frame (from eyepiece measurements, speckle interferometry, and adaptive optics) to improve the characterization of the long-period orbits in both binaries. The visual orbits of the short-and long-period systems are presented for both systems and used to calculate two possible values of the mutual inclinations between inner and outer orbits of 152 degrees +/- 12 degrees or a less likely value of 31 degrees +/- 11 degrees for 63 Gem A and 10.. 2 +/- 2 degrees.4 or 171 degrees.2 +/- 2 degrees.8 for HR 2896. The first is not coplanar, whereas the second is either nearly coplanar or anti-coplanar. C1 [Muterspaugh, Matthew W.] Tennessee State Univ, Coll Arts & Sci, Dept Math & Phys, Nashville, TN 37209 USA. [Muterspaugh, Matthew W.; Fekel, Francis C.; Williamson, M.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Lane, Benjamin F.] Draper Lab, Cambridge, MA 02139 USA. [Hartkopf, William I.] USN Observ, Washington, DC 20392 USA. [Kulkarni, S. R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Konacki, Maciej] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. [Konacki, Maciej] Adam Mickiewicz Univ Poznan, Astron Observ, PL-60286 Poznan, Poland. [Burke, Bernard F.] MIT, Dept Phys, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Colavita, M. M.; Shao, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Muterspaugh, MW (reprint author), Tennessee State Univ, Coll Arts & Sci, Dept Math & Phys, Boswell Sci Hall, Nashville, TN 37209 USA. EM matthew1@coe.tsuniv.edu; blane@draper.com; wih@usno.navy.mil; maciej@ncac.torun.pl FU National Aeronautics and Space Administration [NNG05GJ58G]; NASA [NAS7-03001 (JPL 1336910)]; National Science Foundation [AST 0300096, AST 0507590, AST 0505366]; Townes Fellowship Program; Tennessee State University; State of Tennessee through its Centers of Excellence program; California Institute of Technology, Astronomy Department; Foundation for Polish Science; Polish Ministry of Science and Higher Education [N203 3020 35] FX PHASES benefits from the efforts of the PTI collaboration members who have each contributed to the development of an extremely reliable observational instrument. Without this outstanding engineering effort to produce a solid foundation, advanced phase-referencing techniques would not have been possible. We thank PTI's night assistant Kevin Rykoski for his efforts to maintain PTI in excellent condition and operating PTI in phase-referencing mode every week. Thanks are also extended to Ken Johnston and the U. S. Naval Observatory for their continued support of the USNO Double Star Program. Part of the work described in this paper was performed at the Jet Propulsion Laboratory under contract with the National Aeronautics and Space Administration. Interferometer data were obtained at the Palomar Observatory with the NASA Palomar Testbed Interferometer, supported by NASA contracts to the Jet Propulsion Laboratory. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. This research has made use of SAOImage DS9, developed by the Smithsonian Astrophysical Observatory. M.W.M. acknowledges support from the Townes Fellowship Program, Tennessee State University, and the state of Tennessee through its Centers of Excellence program. Some of the software used for analysis was developed as part of the SIM Double Blind Test with support from NASA contract NAS7-03001 (JPL 1336910). PHASES is funded in part by the California Institute of Technology, Astronomy Department, and by the National Aeronautics and Space Administration under Grant No. NNG05GJ58G issued through the Terrestrial Planet Finder Foundation Science Program. This work was supported in part by the National Science Foundation through grants AST 0300096, AST 0507590, and AST 0505366. M.K. is supported by the Foundation for Polish Science through a FOCUS grant and fellowship, by the Polish Ministry of Science and Higher Education through grant N203 3020 35. NR 21 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2010 VL 140 IS 6 BP 1646 EP 1656 DI 10.1088/0004-6256/140/6/1646 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500005 ER PT J AU Muterspaugh, MW Lane, BF Kulkarni, SR Konacki, M Burke, BF Colavita, MM Shao, M Hartkopf, WI Boss, AP Williamson, M AF Muterspaugh, Matthew W. Lane, Benjamin F. Kulkarni, S. R. Konacki, Maciej Burke, Bernard F. Colavita, M. M. Shao, M. Hartkopf, William I. Boss, Alan P. Williamson, M. TI THE PHASES DIFFERENTIAL ASTROMETRY DATA ARCHIVE. V. CANDIDATE SUBSTELLAR COMPANIONS TO BINARY SYSTEMS SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; binaries: close; binaries: visual; techniques: interferometric ID PALOMAR TESTBED INTERFEROMETER; PRECISION RADIAL-VELOCITIES; HUBBLE-SPACE-TELESCOPE; GIANT PLANET FORMATION; EXTRA-SOLAR PLANETS; STAR CD-ROM; BARNARDS STAR; GRAVITATIONAL-INSTABILITY; CORALIE SURVEY; GJ 802B AB The Palomar High-precision Astrometric Search for Exoplanet Systems monitored 51 subarcsecond binary systems to evaluate whether tertiary companions as small as Jovian planets orbited either the primary or secondary stars, perturbing their otherwise smooth Keplerian motions. Six binaries are presented that show evidence of substellar companions orbiting either the primary or secondary star. Of these six systems, the likelihoods of two of the detected perturbations to represent real objects are considered to be "high confidence," while the remaining four systems are less certain and will require continued observations for confirmation. C1 [Muterspaugh, Matthew W.] Tennessee State Univ, Coll Arts & Sci, Dept Math & Phys, Nashville, TN 37209 USA. [Muterspaugh, Matthew W.; Williamson, M.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Lane, Benjamin F.] Draper Lab, Cambridge, MA 02139 USA. [Kulkarni, S. R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Konacki, Maciej] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. [Konacki, Maciej] Adam Mickiewicz Univ Poznan, Astron Observ, PL-60286 Poznan, Poland. [Burke, Bernard F.] MIT, Dept Phys, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Colavita, M. M.; Shao, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hartkopf, William I.] USN Observ, Washington, DC 20392 USA. [Boss, Alan P.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Muterspaugh, MW (reprint author), Tennessee State Univ, Coll Arts & Sci, Dept Math & Phys, Boswell Sci Hall, Nashville, TN 37209 USA. EM matthew1@coe.tsuniv.edu; blane@draper.com; maciej@ncac.torun.pl FU National Aeronautics and Space Administration [NNG05GJ58G]; NASA [NAS7-03001 (JPL 1336910)]; National Science Foundation [AST 0300096, AST 0507590, AST 0505366]; Townes Fellowship Program; Tennessee State University; State of Tennessee through its Centers of Excellence program; California Institute of Technology Astronomy Department; Foundation for Polish Science; Polish Ministry of Science and Higher Education [N203 3020 35] FX PHASES benefits from the efforts of the PTI collaboration members who have each contributed to the development of an extremely reliable observational instrument. Without this outstanding engineering effort to produce a solid foundation, advanced phase-referencing techniques would not have been possible. We thank PTI's night assistant Kevin Rykoski for his efforts to maintain PTI in excellent condition and operating PTI in phase-referencing mode every week. Thanks are also extended toKen Johnston and the U. S. Naval Observatory for their continued support of the USNO Double Star Program. Part of thework described in this paper was performed at the Jet Propulsion Laboratory under contract with the National Aeronautics and Space Administration. Interferometer data were obtained at the Palomar Observatory with the NASA Palomar Testbed Interferometer, supported by NASA contracts to the Jet Propulsion Laboratory. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. M.W.M. acknowledges support from the Townes Fellowship Program, Tennessee State University, and the state of Tennessee through its Centers of Excellence program. Some of the software used for analysis was developed as part of the SIM Double Blind Test with support from NASA contract NAS7-03001 (JPL 1336910). PHASES is funded in part by the California Institute of Technology Astronomy Department, and by the National Aeronautics and Space Administration under grant no. NNG05GJ58G issued through the Terrestrial Planet Finder Foundation Science Program. This work was supported in part by the National Science Foundation through grants AST 0300096, AST 0507590, and AST 0505366. M.K. is supported by the Foundation for Polish Science through a FOCUS grant and fellowship, by the Polish Ministry of Science and Higher Education through grant N203 3020 35. NR 64 TC 30 Z9 31 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2010 VL 140 IS 6 BP 1657 EP 1671 DI 10.1088/0004-6256/140/6/1657 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500006 ER PT J AU Schaefer, GH Gies, DR Monnier, JD Richardson, ND Touhami, Y Zhao, M Che, X Pedretti, E Thureau, N ten Brummelaar, T McAlister, HA Ridgway, ST Sturmann, J Sturmann, L Turner, NH Farrington, CD Goldfinger, PJ AF Schaefer, G. H. Gies, D. R. Monnier, J. D. Richardson, N. D. Touhami, Y. Zhao, M. Che, X. Pedretti, E. Thureau, N. ten Brummelaar, T. McAlister, H. A. Ridgway, S. T. Sturmann, J. Sturmann, L. Turner, N. H. Farrington, C. D. Goldfinger, P. J. TI MULTI-EPOCH NEAR-INFRARED INTERFEROMETRY OF THE SPATIALLY RESOLVED DISK AROUND THE BE STAR zeta TAU SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; stars: emission-line, Be; stars: individual (zeta Tau); techniques: interferometric ID ONE-ARMED OSCILLATIONS; LONG-TERM; OPTICAL INTERFEROMETRY; CIRCUMSTELLAR DISK; CHARA ARRAY; CYCLIC VARIABILITY; CANIS MAJORIS; STELLAR; ABUNDANCES; PARAMETERS AB We present interferometric observations of the Be star zeta Tau obtained using the MIRC beam combiner at the CHARA Array. We resolved the disk during four epochs in 2007-2009. We fit the data with a geometric model to characterize the circumstellar disk as a skewed elliptical Gaussian and the central Be star as a uniform disk. The visibilities reveal a nearly edge-on disk with an FWHM major axis of similar to 1.8 mas in the H band. The non-zero closure phases indicate an asymmetry within the disk. Interestingly, when combining our results with previously published interferometric observations of zeta Tau, we find a correlation between the position angle of the disk and the spectroscopic V/R ratio, suggesting that the tilt of the disk is precessing. This work is part of a multi-year monitoring campaign to investigate the development and outward motion of asymmetric structures in the disks of Be stars. C1 [Schaefer, G. H.; ten Brummelaar, T.; Sturmann, J.; Sturmann, L.; Turner, N. H.; Farrington, C. D.; Goldfinger, P. J.] Georgia State Univ, Mt Wilson Observ, CHARA Array, Mt Wilson, CA 91023 USA. [Gies, D. R.; Richardson, N. D.; Touhami, Y.; McAlister, H. A.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Gies, D. R.; Richardson, N. D.; Touhami, Y.; McAlister, H. A.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Monnier, J. D.; Che, X.] Univ Michigan, Ann Arbor, MI 48109 USA. [Zhao, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pedretti, E.; Thureau, N.] Univ St Andrews, St Andrews KY16 9AJ, Fife, Scotland. [Ridgway, S. T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Schaefer, GH (reprint author), Georgia State Univ, Mt Wilson Observ, CHARA Array, Mt Wilson, CA 91023 USA. EM schaefer@chara-array.org; gies@chara.gsu.edu FU National Science Foundation [AST-0606861, AST-0352723, AST-0707927, AST-0807577, AST-0606958, AST-0908253]; University of Michigan; NASA [NNH09AK731]; GSU College of Arts and Sciences; W.M. Keck Foundation; NASA Exoplanet Science Institute; David and Lucile Packard Foundation; Georgia State University FX We thank Christian Buil, Benjamin Mauclaire, Ernst Pollmann, and the other observers who contributed to the BeSS database of zeta Tau spectroscopy. We also thank K. Bjorkman, E. Hesselbach, E. Grundstrom, and V. McSwain for providing additional spectra contemporaneous with the MIRC observations. We thank the anonymous referee for providing comments that helped improve the paper. D.R.G. acknowledges support for this work provided by the National Science Foundation under grant AST-0606861. J.D.M., X.C., and M.Z. acknowledge funding from the University of Michigan and the National Science Foundation (AST-0352723, AST-0707927, AST-0807577). S.T.R. acknowledges partial support by NASA grant NNH09AK731. Operational funding for the CHARA Array is provided by the GSU College of Arts and Sciences, by the National Science Foundation through grants AST-0606958 and AST-0908253, by the W.M. Keck Foundation, and by the NASA Exoplanet Science Institute. We thank the Mount Wilson Institute for providing infrastructure support at Mount Wilson Observatory. The CHARA Array, operated by Georgia State University, was built with funding provided by the National Science Foundation, Georgia State University, the W.M. Keck Foundation, and the David and Lucile Packard Foundation. We gratefully acknowledge all of this support. This research has made use of the SIMBAD database and the VizieR catalog service operated at CDS, Strasbourg, France. NR 60 TC 16 Z9 16 U1 0 U2 3 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 DEC PY 2010 VL 140 IS 6 BP 1838 EP 1849 DI 10.1088/0004-6256/140/6/1838 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500019 ER PT J AU Wright, EL Eisenhardt, PRM Mainzer, AK Ressler, ME Cutri, RM Jarrett, T Kirkpatrick, JD Padgett, D McMillan, RS Skrutskie, M Stanford, SA Cohen, M Walker, RG Mather, JC Leisawitz, D Gautier, TN McLean, I Benford, D Lonsdale, CJ Blain, A Mendez, B Irace, WR Duval, V Liu, F Royer, D Heinrichsen, I Howard, J Shannon, M Kendall, M Walsh, AL Larsen, M Cardon, JG Schick, S Schwalm, M Abid, M Fabinsky, B Naes, L Tsai, CW AF Wright, Edward L. Eisenhardt, Peter R. M. Mainzer, Amy K. Ressler, Michael E. Cutri, Roc M. Jarrett, Thomas Kirkpatrick, J. Davy Padgett, Deborah McMillan, Robert S. Skrutskie, Michael Stanford, S. A. Cohen, Martin Walker, Russell G. Mather, John C. Leisawitz, David Gautier, Thomas N., III McLean, Ian Benford, Dominic Lonsdale, Carol J. Blain, Andrew Mendez, Bryan Irace, William R. Duval, Valerie Liu, Fengchuan Royer, Don Heinrichsen, Ingolf Howard, Joan Shannon, Mark Kendall, Martha Walsh, Amy L. Larsen, Mark Cardon, Joel G. Schick, Scott Schwalm, Mark Abid, Mohamed Fabinsky, Beth Naes, Larry Tsai, Chao-Wei TI THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE): MISSION DESCRIPTION AND INITIAL ON-ORBIT PERFORMANCE SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: general; space vehicles; surveys ID DIGITAL SKY SURVEY; SPECTRAL IRRADIANCE CALIBRATION; REDDENED QUASARS; MASS FUNCTION; LUMINOSITY FUNCTION; POPULATION; GALAXIES; DWARFS; DISCOVERY; CATALOG AB The all sky surveys done by the Palomar Observatory Schmidt, the European Southern Observatory Schmidt, and the United Kingdom Schmidt, the InfraRed Astronomical Satellite, and the Two Micron All Sky Survey have proven to be extremely useful tools for astronomy with value that lasts for decades. The Wide-field Infrared Survey Explorer (WISE) is mapping the whole sky following its launch on 2009 December 14. WISE began surveying the sky on 2010 January 14 and completed its first full coverage of the sky on July 17. The survey will continue to cover the sky a second time until the cryogen is exhausted (anticipated in 2010 November). WISE is achieving 5 sigma point source sensitivities better than 0.08, 0.11, 1, and 6 mJy in unconfused regions on the ecliptic in bands centered at wavelengths of 3.4, 4.6, 12, and 22 mu m. Sensitivity improves toward the ecliptic poles due to denser coverage and lower zodiacal background. The angular resolution is 6 ''.1, 6 ''.4, 6 ''.5, and 12 ''.0 at 3.4, 4.6, 12, and 22 mu m, and the astrometric precision for high signal-to-noise sources is better than 0 ''.15. C1 [Wright, Edward L.; McLean, Ian] UCLA Astron, Los Angeles, CA 90095 USA. [Eisenhardt, Peter R. M.; Mainzer, Amy K.; Ressler, Michael E.; Gautier, Thomas N., III; Irace, William R.; Duval, Valerie; Liu, Fengchuan; Royer, Don; Heinrichsen, Ingolf; Abid, Mohamed; Fabinsky, Beth] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cutri, Roc M.; Jarrett, Thomas; Kirkpatrick, J. Davy; Padgett, Deborah; Tsai, Chao-Wei] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [McMillan, Robert S.] Univ Arizona, Tucson, AZ 85721 USA. [Skrutskie, Michael] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] LLNL, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Cohen, Martin; Walker, Russell G.] Monterey Inst Res Astron, Marina, CA 93933 USA. [Mather, John C.; Leisawitz, David; Benford, Dominic] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lonsdale, Carol J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Mendez, Bryan] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Howard, Joan; Shannon, Mark; Kendall, Martha; Walsh, Amy L.] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. [Larsen, Mark; Cardon, Joel G.] Space Dynam Lab, N Logan, UT 84341 USA. [Schick, Scott] Practical Technol Solut Inc, N Logan, UT USA. [Schwalm, Mark] L 3 Commun SSG Tinsley, Wilmington, MA 01887 USA. [Naes, Larry] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. RP Wright, EL (reprint author), UCLA Astron, POB 951547, Los Angeles, CA 90095 USA. EM wright@astro.ucla.edu RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 FU National Aeronautics and Space Administration FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 66 TC 1980 Z9 1993 U1 10 U2 54 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 DEC PY 2010 VL 140 IS 6 BP 1868 EP 1881 DI 10.1088/0004-6256/140/6/1868 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500022 ER PT J AU Ressler, ME Cohen, M Wachter, S Hoard, DW Mainzer, AK Wright, EL AF Ressler, Michael E. Cohen, Martin Wachter, Stefanie Hoard, D. W. Mainzer, Amy K. Wright, Edward L. TI THE DISCOVERY OF INFRARED RINGS IN THE PLANETARY NEBULA NGC 1514 DURING THE WISE ALL-SKY SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; planetary nebulae: individual (NGC 1514); surveys ID NGC-1514; SPECTRA; PHOTOMETRY; HIPPARCOS; DISTANCES; EMISSION; STARS AB We report the discovery of a pair of infrared, axisymmetric rings in the planetary nebula NGC 1514 during the course of the WISE all-sky mid-infrared survey. Similar structures are seen at visible wavelengths in objects such as the "Engraved Hourglass Nebula" (MyCn 18) and the "Southern Crab Nebula" ( Hen 2-104). However, in NGC 1514 we see only a single pair of rings and they are easily observed only in the mid-infrared. These rings are roughly 0.2 pc in diameter, are separated by 0.05 pc, and are dominated by dust emission with a characteristic temperature of 160 K. We compare the morphology and color of the rings to the other nebular structures seen at visible, far-infrared, and radio wavelengths, and close with a discussion of a physical model and formation scenario for NGC 1514. C1 [Ressler, Michael E.; Mainzer, Amy K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cohen, Martin] Monterey Inst Res Astron, Marina, CA 93933 USA. [Wachter, Stefanie; Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Wright, Edward L.] UCLA Astron, Los Angeles, CA 90095 USA. RP Ressler, ME (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Michael.E.Ressler@jpl.nasa.gov FU National Aeronautics and Space Administration; NASA [1000-S-MA756, UCLA FAU 26311]; National Science Foundation; U.S. Government [NAGW-2166]; ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom); ISAS FX We thank our anonymous referee for the very thorough review of this manuscript and the suggestions which improved our discussion. We are grateful to Romano Corradi for his generous provision of the FITS files for the O III and H alpha images of NGC 1514, and to Roc Cutri and Frank Masci for explanations of the WISE processing pipeline. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. M. C. thanks NASA for supporting his participation in this work through UCLA Sub-Award 1000-S-MA756 with a UCLA FAU 26311 to MIRA. Finally, we acknowledge the many scientists and staff of all the WISE partners who spent many years making WISE successful.; This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.; This publication makes use of data products from the following facilities: the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration; the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA; the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation; the Digitized Sky Survey which was produced at the Space Telescope Science Institute under U.S. Government grant NAGW-2166 using photographic data obtained by the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope; the Infrared Space Observatory, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA; and the NRAO VLA Sky Survey (Condon et al. 1998) which was performed by the US National Radio Astronomy Observatory which is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. NR 41 TC 10 Z9 10 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 DEC PY 2010 VL 140 IS 6 BP 1882 EP 1890 DI 10.1088/0004-6256/140/6/1882 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500023 ER PT J AU Edwards, LOV Fadda, D Frayer, DT Neto, GBL Durret, F AF Edwards, Louise O. V. Fadda, Dario Frayer, David T. Lima Neto, Gastao B. Durret, Florence TI SPITZER OBSERVATIONS OF A1763. II. CONSTRAINING THE NATURE OF ACTIVITY IN THE CLUSTER-FEEDING FILAMENT WITH VLA AND XMM-NEWTON DATA SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (A1763, A1770); radio continuum: galaxies; X-rays: galaxies: clusters ID RELAXED GALAXY CLUSTERS; TAILED RADIO GALAXIES; STAR-FORMATION RATES; X-RAY-EMISSION; GALACTIC NUCLEI; ABELL CLUSTERS; STARBURST GALAXIES; HOST GALAXIES; LUMINOSITY FUNCTION; INFRARED GALAXIES AB The A1763 superstructure at z = 0.23 contains the first galaxy filament to be directly detected using mid-infrared observations. Our previous work has shown that the frequency of starbursting galaxies, as characterized by 24 mu m emission is much higher within the filament than at either the center of the rich galaxy cluster, or the field surrounding the system. New Very Large Array and XMM-Newton data are presented here. We use the radio and X-ray data to examine the fraction and location of active galaxies, both active galactic nuclei (AGNs) and starbursts (SBs). The radio far-infrared correlation, X-ray point source location, IRAC colors, and quasar positions are all used to gain an understanding of the presence of dominant AGNs. We find very few MIPS-selected galaxies that are clearly dominated by AGN activity. Most radio-selected members within the filament are SBs. Within the supercluster, three of eight spectroscopic members detected both in the radio and in the mid-infrared are radio-bright AGNs. They are found at or near the core of A1763. The five SBs are located further along the filament. We calculate the physical properties of the known wide angle tail (WAT) source which is the brightest cluster galaxy of A1763. A second double lobe source is found along the filament well outside of the virial radius of either cluster. The velocity offset of the WAT from the X-ray centroid and the bend of the WAT in the intracluster medium are both consistent with ram pressure stripping, indicative of streaming motions along the direction of the filament. We consider this as further evidence of the cluster-feeding nature of the galaxy filament. C1 [Edwards, Louise O. V.; Fadda, Dario] NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Frayer, David T.] NRAO, Green Bank, WV 24944 USA. [Lima Neto, Gastao B.] Univ Sao Paulo, Inst Astron & Geofis, BR-05508900 Sao Paulo, Brazil. [Durret, Florence] Inst Astrophys, FR-75014 Paris, France. RP Edwards, LOV (reprint author), NASA, Herschel Sci Ctr, Caltech 100-22, Pasadena, CA 91125 USA. EM louise@ipac.caltech.edu RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Lima Neto, Gastao/J-6117-2014 FU JPL/Caltech; ESA Member States; NASA; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council of England FX Support for this work was provided by NASA through an award issued by JPL/Caltech. This work is based in part on original observations using the Very Large Array operated by the NRAO. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work is also based in part on archival observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA and observations made with Spitzer, a space telescope operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, then Participating Institutions, the National Science Foundation, the US Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council of England. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions (see list at http://www.sdss.org/collaboration/credits.html). We have made use of the ROSAT Data Archive of the Max-Planck-Institut fur extraterrestrische Physik (MPE) at Garching, Germany as well as the XMM-Newton Data Archive. NR 74 TC 4 Z9 4 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2010 VL 140 IS 6 BP 1891 EP 1904 DI 10.1088/0004-6256/140/6/1891 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500024 ER PT J AU Lazio, TJW Shankland, PD Farrell, WM Blank, DL AF Lazio, T. Joseph W. Shankland, P. D. Farrell, W. M. Blank, D. L. TI RADIO OBSERVATIONS OF HD 80606 NEAR PLANETARY PERIASTRON SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: magnetic fields; planets and satellites: individual (HD 80606b); radio continuum: planetary systems ID EXTRASOLAR PLANETS; MAGNETOSPHERIC EMISSIONS; FREQUENCY INTERFERENCE; NEARBY STARS; COOL STARS; 74 MHZ; SEARCH; TRANSIT; SYSTEMS; ORBIT AB This paper reports Very Large Array observations at 325 and 1425 MHz (lambda 90 cm and lambda 20 cm) during and near the periastron passage of HD 80606b on HJD 2454424.86 (2007 November 20). We obtain flux density limits (3 sigma) of 1.7 mJy and 48 mu Jy at 325 and 1425 MHz, respectively, equivalent to planetary luminosity limits of 2.3x10(24) erg s(-1) and 2.7 x 10(23) erg s-1. Unfortunately, these are several orders of magnitude above the nominal Jovian value (at 40 MHz) of 2x10(18) erg s-1. The motivation for these observations was that the planetary magnetospheric emission is driven by a stellar wind-planetary magnetosphere interaction so that the planetary luminosity would be elevated near periastron. We estimate that, near periastron, HD 80606b might be as much as 3000 times more luminous than Jupiter. Recent transit observations of HD 80606b provide reasonably stringent constraints on the planetary mass and radius, and, because of the planet's highly eccentric orbit, its rotation period is likely to be "pseudo-synchronized" to its orbital period, allowing a robust estimate of the former. Consequently, we are able to make relatively robust estimates of the emission frequency of the planetary magnetospheric emission and find it to be around 60-90 MHz. While this is too low for our reported observations, we compare HD 80606b to other high-eccentricity systems and assess the detection possibilities for both near-term and more distant future systems. Of the known high-eccentricity planets, only HD 80606b is likely to be detectable, as the others (HD 20782B and HD 4113) are both lower mass and longer rotational periods, which imply weaker magnetic field strengths. We find that both the forthcoming "EVLA low band" system, which will operate as low as 65 MHz, and the Low Frequency Array may be able to improve upon our planetary luminosity limits for HD 80606b, and do so at a more optimum frequency. If the low-frequency component of the Square Kilometre Array (SKA-lo) and a future lunar radio array are able to approach their thermal noise limits, they should be able to detect an HD 80606b-like planet, unless the amount by which the planet's luminosity increases is substantially less than the factor of 3000 that we estimate; for the SKA-lo, which is to be located in the southern hemisphere, future planetary surveys will have to find southern hemisphere equivalents of HD 80606b. C1 [Lazio, T. Joseph W.; Farrell, W. M.] NASA, Lunar Sci Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lazio, T. Joseph W.] USN, Res Lab, Washington, DC 20375 USA. [Shankland, P. D.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blank, D. L.] James Cook Univ, Sch Math & Phys Sci, Ctr Astron, Townsville, Qld 4811, Australia. RP Lazio, TJW (reprint author), CALTECH, Jet Prop Lab, M-S 138-308,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Farrell, William/I-4865-2013 FU NASA Lunar Science Institute [NNA09DB30A]; 6.1 Base FX We thank G. Laughlin for the initial inspiration for these observations and for pointing out that HD 80606b should be in a state of pseudo-synchronization; J. Schneider for the Extrasolar Planets Encyclopedia; and P. Perley and W. Koski for helpful discussions. T.J.W.L. thanks USNO, where much of this paper was written, for its hospitality. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The LUNAR consortium is funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. Basic research at NRL is supported by 6.1 Base funding. NR 40 TC 13 Z9 13 U1 1 U2 3 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 DEC PY 2010 VL 140 IS 6 BP 1929 EP 1933 DI 10.1088/0004-6256/140/6/1929 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500028 ER PT J AU Lazio, TJW Clarke, TE Lane, WM Gross, C Kassim, NE Ray, PS Wood, D York, JA Kerkhoff, A Hicks, B Polisensky, E Stewart, K Dalal, NP Cohen, AS Erickson, WC AF Lazio, T. Joseph W. Clarke, Tracy E. Lane, W. M. Gross, C. Kassim, N. E. Ray, P. S. Wood, D. York, J. A. Kerkhoff, A. Hicks, B. Polisensky, E. Stewart, K. Dalal, N. Paravastu Cohen, A. S. Erickson, W. C. TI SURVEYING THE DYNAMIC RADIO SKY WITH THE LONG WAVELENGTH DEMONSTRATOR ARRAY SO ASTRONOMICAL JOURNAL LA English DT Article DE instrumentation: interferometers; methods: observational; radio continuum: general ID GAMMA-RAY BURSTS; STELLAR WIND CONDITIONS; EXTRASOLAR PLANETS; GIANT PULSES; CRAB PULSAR; AIR-SHOWERS; FREQUENCY OBSERVATIONS; ENERGY NEUTRINOS; COSMIC-RAYS; SEARCH AB This paper presents a search for radio transients at a frequency of 73.8 MHz (4 m wavelength) using the all-sky imaging capabilities of the Long Wavelength Demonstrator Array (LWDA). The LWDA was a 16-dipole phased array telescope, located on the site of the Very Large Array in New Mexico. The field of view of the individual dipoles was essentially the entire sky, and the number of dipoles was sufficiently small that a simple software correlator could be used to make all-sky images. From 2006 October to 2007 February, we conducted an all-sky transient search program, acquiring a total of 106 hr of data; the time sampling varied, being 5 minutes at the start of the program and improving to 2 minutes by the end of the program. We were able to detect solar flares, and in a special-purpose mode, radio reflections from ionized meteor trails during the 2006 Leonid meteor shower. We detected no transients originating outside of the solar system above a flux density limit of 500 Jy, equivalent to a limit of no more than about 10(-2) events yr(-1) deg(-2), having a pulse energy density greater than or similar to 1.5 x 10(-20) J m(-2) Hz(-1) at 73.8 MHz for pulse widths of about 300 s. This event rate is comparable to that determined from previous all-sky transient searches, but at a lower frequency than most previous all-sky searches. We believe that the LWDA illustrates how an all-sky imaging mode could be a useful operational model for low-frequency instruments such as the Low Frequency Array, the Long Wavelength Array station, the low-frequency component of the Square Kilometre Array, and potentially the Lunar Radio Array. C1 [Lazio, T. Joseph W.; Clarke, Tracy E.; Lane, W. M.; Gross, C.; Kassim, N. E.; Hicks, B.; Polisensky, E.; Stewart, K.] USN, Remote Sensing Div, Res Lab, Washington, DC 20375 USA. [Lazio, T. Joseph W.] NASA, Lunar Sci Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ray, P. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Wood, D.] Praxis Inc, Alexandria, VA 22303 USA. [York, J. A.; Kerkhoff, A.] Univ Texas Austin, Appl Res Labs, Austin, TX 78713 USA. [Dalal, N. Paravastu] Amer Soc Engn Educ, Washington, DC 20036 USA. [Cohen, A. S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Erickson, W. C.] Univ Tasmania, Sch Math & Sci, Sandy Bay, Tas 7005, Australia. RP Lazio, TJW (reprint author), CALTECH, Jet Prop Lab, M-S 138-308,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Joseph.Lazio@jpl.nasa.gov OI Ray, Paul/0000-0002-5297-5278 FU NASA Lunar Science Institute [NNA09DB30A]; 6.1 Base FX The LWDA was a joint project of NRL, the Applied Research Laboratories of the University of Texas at Austin, and the University of New Mexico. We thank the members of the University of New Mexico faculty and students who assisted with the infrastructure, construction, and maintenance of the LWDA and the many staff members of the NRAO who provided technical support in establishing the LWDA near the VLA. We thank K. Weiler, D. Munton, and L. J. Rickard for their guidance during various stages of the project. We thank J. Cordes for providing the software to generate Figure 7. This research has made use of NASA's Astrophysics Data System. The LUNAR consortium, headquartered at the University of Colorado, is funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. Basic research in radio astronomy at the NRL is supported by 6.1 Base funding. NR 112 TC 26 Z9 26 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2010 VL 140 IS 6 BP 1995 EP 2006 DI 10.1088/0004-6256/140/6/1995 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500035 ER PT J AU Barucci, MA Ore, CMD Alvarez-Candal, A de Bergh, C Merlin, F Dumas, C Cruikshank, D AF Barucci, M. A. Ore, C. Morea Dalle Alvarez-Candal, A. de Bergh, C. Merlin, F. Dumas, C. Cruikshank, D. TI (90377) SEDNA: INVESTIGATION OF SURFACE COMPOSITIONAL VARIATION SO ASTRONOMICAL JOURNAL LA English DT Article DE Kuiper belt objects: individual (Sedna); Oort Cloud; planets and satellites: formation; techniques: spectroscopic ID TRANS-NEPTUNIAN OBJECTS; INNER OORT CLOUD; OPTICAL-CONSTANTS; 2000 CR105; MU-M; PERIOD AB The dwarf planet (90377) Sedna is one of the most remote solar system objects accessible to investigations. To better constrain its surface composition and to investigate the possible heterogeneity of the surface of Sedna, several observations have been carried out at ESO-VLT with the powerful spectrometer SINFONI observing simultaneously the H and K bands. The analyzed spectra (obtained in 2005, 2007, and 2008) show a non-uniform spectral signature, particularly in the K band. Spectral modeling using the Shkuratov radiative transfer code for surface scattering has been performed using the various sets of data, including previous observations at visible wavelengths and photometry at 3.6 and 4.5 mu m by the Spitzer Space Telescope. The visible and near-infrared spectra can be modeled with organic materials (triton and titan tholin), serpentine, and H(2)O ice in fairly significant amounts, and CH(4), N(2), and C(2)H(6) in varying trace amounts. One of the spectra obtained in 2005 October shows a different signature in the K band and is best modeled with CH(3)OH in place of CH(4), with reduced amounts of serpentine and with the addition of olivine. The compositional surface heterogeneity can give input on the past history as well clues to the origin of this peculiar, distant object. C1 [Barucci, M. A.; de Bergh, C.; Merlin, F.] Observ Paris, LESIA, F-92195 Meudon, France. [Ore, C. Morea Dalle; Cruikshank, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ore, C. Morea Dalle] SETI Inst, Mountain View, CA 94043 USA. [Alvarez-Candal, A.; Dumas, C.] ESO, Santiago 19, Chile. RP Barucci, MA (reprint author), Observ Paris, LESIA, 5 Pl Jules Janssen, F-92195 Meudon, France. EM antonella.barucci@obspm.fr RI Alvarez-Candal, Alvaro/M-4834-2013 NR 40 TC 12 Z9 12 U1 1 U2 5 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 DEC PY 2010 VL 140 IS 6 BP 2095 EP 2100 DI 10.1088/0004-6256/140/6/2095 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500043 ER PT J AU Boquien, M Duc, PA Galliano, F Braine, J Lisenfeld, U Charmandaris, V Appleton, PN AF Boquien, M. Duc, P-A Galliano, F. Braine, J. Lisenfeld, U. Charmandaris, V. Appleton, P. N. TI STAR FORMATION IN COLLISION DEBRIS: INSIGHTS FROM THE MODELING OF THEIR SPECTRAL ENERGY DISTRIBUTION SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: interactions; galaxies: irregular; infrared: galaxies; stars: formation; ultraviolet: galaxies ID TIDAL DWARF GALAXIES; ABUNDANT MOLECULAR GAS; H-II REGIONS; STEPHANS QUINTET; INTERACTING GALAXIES; CLUSTER FORMATION; FORMING GALAXIES; VIRGO CLUSTER; IONIZED-GAS; HII REGION AB During galaxy-galaxy interactions, massive gas clouds can be injected into the intergalactic medium which in turn become gravitationally bound, collapse, and form stars, star clusters, or even dwarf galaxies. The objects resulting from this process are both "pristine," as they are forming their first generation of stars, and chemically evolved because the metallicity inherited from their parent galaxies is high. Such characteristics make them particularly interesting laboratories in which to study star formation. After having investigated their star-forming properties, we use photospheric, nebular, and dust modeling to analyze their spectral energy distribution (SED) from the far-ultraviolet to the mid-infrared regime for a sample of seven star-forming regions. Our analysis confirms that the intergalactic star-forming regions in Stephan's Quintet, around Arp 105 and NGC 5291, appear devoid of stellar populations older than 10(9) years. We also find an excess of light in the near-infrared regime (from 2 mu m to 4.5 mu m) which cannot be attributed to stellar photospheric or nebular contributions. This excess is correlated with the star formation rate intensity suggesting that it is probably due to emission by very small grains fluctuating in temperature as well as the polycyclic aromatic hydrocarbons line at 3.3 mu m. Comparing the attenuation via the Balmer decrement to the mid-infrared emission allows us to check the reliability of the attenuation estimate. It suggests the presence of embedded star-forming regions in NGC 5291 and NGC 7252. Overall the SED of star-forming regions in collision debris (and Tidal Dwarf Galaxies) resemble more that of dusty star-forming regions in galactic disks than to that of typical star-forming dwarf galaxies. C1 [Boquien, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Duc, P-A; Galliano, F.] Univ Paris Diderot, Lab AIM, CEA DSM, CNRS,IRFU Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Braine, J.] Univ Bordeaux 1, Lab Astrophys Bordeaux, OASU, CNRS INSU,UMR 5804, F-33270 Floirac, France. [Lisenfeld, U.] Univ Granada, Dept Fis Teor & Cosmos, Granada, Spain. [Charmandaris, V.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Charmandaris, V.] IESL Fdn Res & Technol Hellas, GR-71110 Iraklion, Greece. [Charmandaris, V.] Observ Paris, Chercheur Associe, F-75014 Paris, France. [Appleton, P. N.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. RP Boquien, M (reprint author), Univ Massachusetts, Dept Astron, LGRT B 619E, Amherst, MA 01003 USA. EM boquien@astro.umass.edu RI Charmandaris, Vassilis/A-7196-2008; Lisenfeld, Ute/A-1637-2015; Boquien, Mederic/J-5964-2015; OI Charmandaris, Vassilis/0000-0002-2688-1956; Lisenfeld, Ute/0000-0002-9471-5423; Boquien, Mederic/0000-0003-0946-6176; Appleton, Philip/0000-0002-7607-8766 FU Spanish Science Ministry [AYA 2007-67625-C02-02]; Junta de Andalucia; EU ToK [39965]; [FP7-REGPOT 206469] FX U.L. acknowledges financial support by the Spanish Science Ministry under grant AYA 2007-67625-C02-02 and by the Junta de Andalucia. V.C. acknowledges partial support from the EU ToK grant 39965 and FP7-REGPOT 206469. NR 69 TC 26 Z9 26 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2010 VL 140 IS 6 BP 2124 EP 2144 DI 10.1088/0004-6256/140/6/2124 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679EK UT WOS:000284143500046 ER PT J AU Kjeldsen, H Christensen-Dalsgaard, J Handberg, R Brown, TM Gilliland, RL Borucki, WJ Koch, D AF Kjeldsen, H. Christensen-Dalsgaard, J. Handberg, R. Brown, T. M. Gilliland, R. L. Borucki, W. J. Koch, D. TI The Kepler Asteroseismic Investigation: Scientific goals and first results SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 4th HELAS International Conference CY FEB 01-05, 2010 CL Canary Islands, SPAIN DE planetary systems; stars: evolution; stars: interiors; stars: oscillations; space vehicles ID SOLAR-TYPE STARS; OSCILLATIONS; MISSION; HAT-P-7B; FIELD AB Kepler is a NASA mission designed to detect exoplanets and characterize the properties of exoplanetary systems. Kepler also includes an asteroseismic programme which is being conducted through the Kepler Asteroseismic Science Consortium (KASC), whose 400 members are organized into 13 working groups by type of variable star. So far data have been available from the first 7 month of the mission containing a total of 2937 targets observed at a 1-min cadence for periods between 10 days and 7 months. The goals of the asteroseismic part of the Kepler project is to perform detailed studies of stellar interiors. The first results of the asteroseismic analysis are orders of magnitude better than seen before, and this bodes well for how the future analysis of Kepler data for many types of stars will impact our general understanding of stellar structure and evolution. (C) 2010 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim C1 [Kjeldsen, H.; Christensen-Dalsgaard, J.; Handberg, R.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Brown, T. M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Borucki, W. J.; Koch, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kjeldsen, H (reprint author), Aarhus Univ, Dept Phys & Astron, Bldg 1520, DK-8000 Aarhus C, Denmark. EM hans@phys.au.dk OI Handberg, Rasmus/0000-0001-8725-4502 NR 19 TC 21 Z9 21 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD DEC PY 2010 VL 331 IS 9-10 BP 966 EP 971 DI 10.1002/asna.201011437 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 693GD UT WOS:000285211700022 ER PT J AU Grigahcene, A Uytterhoeven, K Antoci, V Balona, L Catanzaro, G Daszynska-Daszkiewicz, J Guzik, JA Handler, G Houdek, G Kurtz, DW Marconi, M Monteiro, MJPFG Moya, A Ripepi, V Suarez, JC Borucki, WJ Brown, TM Christensen-Dalsgaard, J Gilliland, RL Jenkins, JM Kjeldsen, H Koch, D Bernabei, S Bradley, P Breger, M Di Criscienzo, M Dupret, MA Garcia, RA Hernandez, AG Jackiewicz, J Kaiser, A Lehmann, H Martin-Ruiz, S Mathias, P Molenda-Zakowicz, J Nemec, JM Nuspl, J Paparo, M Roth, M Szabo, R Suran, MD Ventura, R AF Grigahcene, A. Uytterhoeven, K. Antoci, V. Balona, L. Catanzaro, G. Daszynska-Daszkiewicz, J. Guzik, J. A. Handler, G. Houdek, G. Kurtz, D. W. Marconi, M. Monteiro, M. J. P. F. G. Moya, A. Ripepi, V. Suarez, J. -C. Borucki, W. J. Brown, T. M. Christensen-Dalsgaard, J. Gilliland, R. L. Jenkins, J. M. Kjeldsen, H. Koch, D. Bernabei, S. Bradley, P. Breger, M. Di Criscienzo, M. Dupret, M. -A. Garcia, R. A. Hernandez, A. Garcia Jackiewicz, J. Kaiser, A. Lehmann, H. Martin-Ruiz, S. Mathias, P. Molenda-Zakowicz, J. Nemec, J. M. Nuspl, J. Paparo, M. Roth, M. Szabo, R. Suran, M. D. Ventura, R. TI Kepler observations: Light shed on the hybrid gamma Doradus-delta Scuti pulsation phenomenon SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 4th HELAS International Conference CY FEB 01-05, 2010 CL Canary Islands, SPAIN DE stars: oscillations; delta Scuti stars; gamma Doradus stars ID SOLAR-LIKE OSCILLATIONS; AM STAR; EXCITATION; PHOTOMETRY; DISCOVERY; FREQUENCY; VARIABLES; TARGET AB Through the observational study of stellar pulsations, the internal structure of stars can be probed and theoretical models can be tested. The main sequence gamma Doradus (Dor) and delta Scuti (Sct) stars with masses 1.2-2.5 M-circle dot are particularly interesting for asteroseismic study. The gamma Dor stars pulsate in high-order gravity (g) modes, with pulsational periods of order of one day. The delta Sct stars, on the other hand, show low-order g and pressure (p) modes with periods of order of 2 hours. Theory predicts the existence of 'hybrid' stars, i.e. stars pulsating in both types of modes, in an overlap region between the instability strips of gamma Dor and delta Sct stars in the Hertzsprung-Russell diagram. Hybrid stars are particularly interesting as the two types of modes probe different regions of the stellar interior and hence provide complementary model constraints. Before the advent of Kepler, only a few hybrid stars had been confirmed. The Kepler satellite is providing a true revolution in the study of and search for hybrid stars. Analysis of the first 50 days of Kepler data of hundreds of gamma Dor and delta Sct candidates reveals extremely rich frequency spectra, with most stars showing frequencies in both the delta Sct and gamma Dor frequency range. As these results show that there are practically no pure delta Sct or gamma Dor pulsators, a new observational classification scheme is proposed by Grigahcene et al. (2010). We present their results and characterize 234 stars in terms of delta Sct, gamma Dor, delta Sct/gamma Dor or gamma Dor/delta Sct hybrids. (C) 2010 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim C1 [Grigahcene, A.; Monteiro, M. J. P. F. G.] Univ Porto, Ctr Astrofis, Oporto, Portugal. [Grigahcene, A.; Monteiro, M. J. P. F. G.] Univ Porto, Dep Fis & Astron, Fac Ciencias, Oporto, Portugal. [Uytterhoeven, K.; Garcia, R. A.] U Paris Diderot, CEA DSM CNRS, Lab AIM, IRFU SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Antoci, V.; Handler, G.; Houdek, G.; Breger, M.; Kaiser, A.] Inst Astron, A-1080 Vienna, Austria. [Balona, L.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Catanzaro, G.; Ventura, R.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Daszynska-Daszkiewicz, J.; Molenda-Zakowicz, J.] Uniwersytet Wroclawski, Inst Astron, PL-51622 Wroclaw, Poland. [Guzik, J. A.; Bradley, P.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England. [Marconi, M.; Ripepi, V.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Moya, A.] LAEX CAB INTA CSIC, Dept Astrofis Estelar & Exoplanetas, Madrid 28691, Spain. [Suarez, J. -C.; Hernandez, A. Garcia; Martin-Ruiz, S.] CSIC, Inst Astrofis Andalucia, Granada 3004, Spain. [Jenkins, J. M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Brown, T. M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bernabei, S.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Di Criscienzo, M.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Rome, Italy. [Dupret, M. -A.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Jackiewicz, J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88001 USA. [Lehmann, H.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Mathias, P.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-65000 Tarbes, France. [Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC, Canada. [Nuspl, J.; Paparo, M.; Szabo, R.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary. [Roth, M.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany. [Suran, M. D.] Acad Romana, Astron Inst, RO-40557 Bucharest, Romania. RP Grigahcene, A (reprint author), Univ Porto, Ctr Astrofis, Oporto, Portugal. EM ahmed.grigahcene@astro.up.pt RI Monteiro, Mario J.P.F.G./B-4715-2008; Martin-Ruiz, Susana/B-6768-2013; Suarez, Juan Carlos/C-1015-2009; Ventura, Rita/B-7524-2016; OI Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Suarez, Juan Carlos/0000-0003-3649-8384; Ventura, Rita/0000-0002-5152-0482; Catanzaro, Giovanni/0000-0003-4337-8612; Bradley, Paul/0000-0001-6229-6677 NR 35 TC 7 Z9 7 U1 0 U2 10 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD DEC PY 2010 VL 331 IS 9-10 BP 989 EP 992 DI 10.1002/asna.201011443 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 693GD UT WOS:000285211700027 ER PT J AU Abdo, AA Ackermann, M Ajello, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bellazzini, R Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bouvier, A Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Carrigan, S Casandjian, JM Charles, E Chaty, S Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J DeCesar, ME Dermer, CD de Palma, F Digel, SW Silva, EDE Drell, PS Dubois, R Dumora, D Favuzzi, C Fortin, P Frailis, M Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giordano, F Glanzman, T Godfrey, G Grenier, I Grondin, MH Grove, JE Guillemot, L Guiriec, S Hadasch, D Harding, AK Hays, E Jean, P Johannesson, G Johnson, TJ Johnson, WN Kamae, T Katagiri, H Kataoka, J Kerr, M Knodlseder, J Kuss, M Lande, J Latronico, L Lee, SH Lemoine-Goumard, M Garde, ML Longo, F Loparco, F Lovellette, MN Lubrano, P Makeev, A Mazziotta, MN Michelson, PF Mitthumsiri, W Mizuno, T Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Nolan, PL Norris, JP Nuss, E Ohsugi, T Omodei, N Orlando, E Ormes, JF Pancrazi, B Parent, D Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Reimer, A Reimer, O Reposeur, T Ripken, J Romani, RW Roth, M Sadrozinski, HFW Parkinson, PMS Sgro, C Siskind, EJ Smith, DA Spinelli, P Strickman, MS Suson, DJ Takahashi, H Takahashi, T Tanaka, T Thayer, JB Thayer, JG Tibaldo, L Torres, DF Tosti, G Tramacere, A Uchiyama, Y Usher, TL Vasileiou, V Venter, C Vilchez, N Vitale, V Waite, AP Wang, P Webb, N Winer, BL Yang, Z Ylinen, T Ziegler, M AF Abdo, A. A. Ackermann, M. Ajello, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bouvier, A. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Carrigan, S. Casandjian, J. M. Charles, E. Chaty, S. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. DeCesar, M. E. Dermer, C. D. de Palma, F. Digel, S. W. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Favuzzi, C. Fortin, P. Frailis, M. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giordano, F. Glanzman, T. Godfrey, G. Grenier, I. Grondin, M. -H. Grove, J. E. Guillemot, L. Guiriec, S. Hadasch, D. Harding, A. K. Hays, E. Jean, P. Johannesson, G. Johnson, T. J. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Kerr, M. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Lee, S. -H. Lemoine-Goumard, M. Garde, M. Llena Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Makeev, A. Mazziotta, M. N. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Omodei, N. Orlando, E. Ormes, J. F. Pancrazi, B. Parent, D. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Reimer, A. Reimer, O. Reposeur, T. Ripken, J. Romani, R. W. Roth, M. Sadrozinski, H. F. -W. Parkinson, P. M. Saz Sgro, C. Siskind, E. J. Smith, D. A. Spinelli, P. Strickman, M. S. Suson, D. J. Takahashi, H. Takahashi, T. Tanaka, T. Thayer, J. B. Thayer, J. G. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Uchiyama, Y. Usher, T. L. Vasileiou, V. Venter, C. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Webb, N. Winer, B. L. Yang, Z. Ylinen, T. Ziegler, M. TI A population of gamma-ray emitting globular clusters seen with the Fermi Large Area Telescope SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE pulsars: general; globular clusters: general; gamma rays: general ID TO-LIGHT RATIO; SPACE-TELESCOPE; OMEGA-CENTAURI; MILLISECOND PULSARS; 47 TUCANAE; GLOBULAR-CLUSTER-47 TUCANAE; COMPACT BINARIES; XMM-NEWTON; PHOTOMETRY; DISCOVERY AB Context. Globular clusters with their large populations of millisecond pulsars (MSPs) are believed to be potential emitters of high-energy gamma-ray emission. The observation of this emission provides a powerful tool to assess the millisecond pulsar population of a cluster, is essential for understanding the importance of binary systems for the evolution of globular clusters, and provides complementary insights into magnetospheric emission processes. Aims. Our goal is to constrain the millisecond pulsar populations in globular clusters from analysis of gamma-ray observations. Methods. We use 546 days of continuous sky-survey observations obtained with the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope to study the gamma-ray emission towards 13 globular clusters. Results. Steady point-like high-energy gamma-ray emission has been significantly detected towards 8 globular clusters. Five of them (47 Tucanae, Omega Cen, NGC 6388, Terzan 5, and M 28) show hard spectral power indices (0.7 < Gamma < 1.4) and clear evidence for an exponential cut-off in the range 1.0-2.6 GeV, which is the characteristic signature of magnetospheric emission from MSPs. Three of them (M 62, NGC 6440 and NGC 6652) also show hard spectral indices (1.0 < Gamma < 1.7), however the presence of an exponential cut-off can not be unambiguously established. Three of them (Omega Cen, NGC 6388, NGC 6652) have no known radio or X-ray MSPs yet still exhibit MSP spectral properties. From the observed gamma-ray luminosities, we estimate the total number of MSPs that is expected to be present in these globular clusters. We show that our estimates of the MSP population correlate with the stellar encounter rate and we estimate 2600-4700 MSPs in Galactic globular clusters, commensurate with previous estimates. Conclusions. The observation of high-energy gamma-ray emission from globular clusters thus provides a reliable independent method to assess their millisecond pulsar populations. C1 [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Abdo, A. A.; Cheung, C. C.] Natl Res Council Res Associate, Natl Acad Sci, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Glanzman, T.; Godfrey, G.; Johannesson, G.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Glanzman, T.; Godfrey, G.; Johannesson, G.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Sgro, C.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Chaty, S.; Grenier, I.; Naumann-Godo, M.; Tibaldo, L.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, CEA IRFU CNRS,Lab AIM, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brandt, T. J.; Jean, P.; Knoedlseder, J.; Pancrazi, B.; Vilchez, N.; Webb, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Brandt, T. J.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fortin, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France. [Conrad, J.; Garde, M. Llena; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden. [Conrad, J.; Garde, M. Llena; Ripken, J.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, Stockholm, Sweden. [DeCesar, M. E.; Gehrels, N.; Harding, A. K.; Hays, E.; Johnson, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [DeCesar, M. E.; Johnson, T. J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [DeCesar, M. E.; Johnson, T. J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Dumora, D.; Grondin, M. -H.; Lemoine-Goumard, M.; Reposeur, T.; Smith, D. A.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Fukazawa, Y.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [Guiriec, S.; Vitale, V.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Hadasch, D.; Torres, D. F.] ICREA, Barcelona, Spain. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Kerr, M.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Takahashi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA. [Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Venter, C.] North West Univ, ZA-2520 Potchefstroom, South Africa. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Royal Inst Technol KTH, Dept Phys, S-10691 Stockholm, Sweden. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, S-39182 Kalmar, Sweden. [Guillemot, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Abdo, AA (reprint author), USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. EM jurgen.knodlseder@cesr.fr; benoit.pancrazi@cesr.fr; natalie.webb@cesr.fr RI Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Harding, Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Venter, Christo/E-6884-2011; Gargano, Fabio/O-8934-2015 OI Chaty, Sylvain/0000-0002-5769-8601; Pesce-Rollins, Melissa/0000-0003-1790-8018; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Giordano, Francesco/0000-0002-8651-2394; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Venter, Christo/0000-0002-2666-4812; Gargano, Fabio/0000-0002-5055-6395 NR 53 TC 51 Z9 51 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2010 VL 524 AR A75 DI 10.1051/0004-6361/201014458 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685JP UT WOS:000284625300024 ER PT J AU Fletcher, LN Orton, GS de Pater, I Mousis, O AF Fletcher, L. N. Orton, G. S. de Pater, I. Mousis, O. TI Jupiter's stratospheric hydrocarbons and temperatures after the July 2009 impact from VLT infrared spectroscopy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: atmospheres; atmospheric effects; planets and satellites: composition; planets and satellites: individual: Jupiter ID COMET SHOEMAKER-LEVY-9; IMAGING SPECTROSCOPY; SL9 IMPACTS; HST; RETRIEVALS; COLLISION; PLANETARY; AMMONIA AB Aims. Thermal infrared imaging and spectroscopy of the July 19, 2009 Jupiter impact site has been used to identify unique features of the physical and chemical atmospheric response to this unexpected collision. Methods. Images and high-resolution spectra of methane, ethane and acetylene emission (7-13 mu m) from the 2009 impact site were obtained by the Very Large Telescope (VLT) mid-infrared camera/spectrometer instrument, VISIR. An optimal estimation retrieval algorithm was used to determine the atmospheric temperatures and hydrocarbon distribution in the month following the impact. Results. Ethane spectra at 12.25 mu m could not be explained by a rise in temperature alone. Ethane was enhanced by 1.7-3.2 times the background abundance on July 26, implying production as the result of shock chemistry in a high C/O ratio environment, favouring an asteroidal origin for the 2009 impactor. Small enhancements in acetylene emission were also observed over the impact site. However, no excess methane emission was found over the impact longitude, either with broadband 7.9-mu m imaging 21 h after the impact, or with center-to-limb scans of strong and weak methane lines between 7.9 and 8.1 mu m in the ensuing days, indicating either extremely rapid cooling in the initial stages, or an absence of heating in the upper stratosphere (p < 10 mbar) due to the near-horizontal orientation of the impact. Models of 12.3-mu m spectra are consistent with a approximate to 3 K rise in the lower stratosphere (p > 10 mbar), though this solution is highly dependent on the spectral properties of stratospheric debris. The enhanced ethane emission was localised over the impact streak, and was diluted in the ensuing weeks by redistribution of heated gases by zonal flow and mixing with the unperturbed jovian air. Conclusions. The different thermal energy deposition profiles, in addition to the highly reducing (C/O > 1) environment and shallow impactor angle, suggest that (a) the 2009 plume and shock-fronts did not reach the sub-microbar altitudes of the Shoemaker-Levy 9 plumes; and (b) models of a cometary impact are not directly applicable to the unique impact circumstances of July 2009. C1 [Fletcher, L. N.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [de Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mousis, O.] Univ Franche Comte, Inst UTINAM, CNRS, Observ Besancon,UMR 6213, F-25030 Besancon, France. RP Fletcher, LN (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England. EM fletcher@atm.ox.ac.uk RI Fletcher, Leigh/D-6093-2011 OI Fletcher, Leigh/0000-0001-5834-9588 FU University of Oxford; National Aeronautics and Space Administration; National Aeronautics and Space Administration, Science Mission Directorate [NNX-08AE38A]; NSF FX Fletcher was supported during this research by a Glasstone Science Fellowship at the University of Oxford. Orton carried out part of this research at the Jet Propulusion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank E. Pantin, B. Bezard, A. Sanchez-Lavega, R. Hueso, C. Palotai, T. Greathouse and P. Irwin for their helpful comments and suggestions during the writing of this manuscript. In particular, we thank J. I. Moses for a thorough review. We wish to thank observers at the VLT, IRTF and Gemini for their rapid and effective response to the 2009 impact on Jupiter. This work was partially based on the following observations: (1) VLT/VISIR observations from UT3/Melipal collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, under Directors Discretionary program ID 283.C-5043. (2) MIRSI observations in program 2009A-073 obtained at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. (3) MICHELLE observations obtained at the Gemini Observatory (Director Discretionary program GN-2009A-DD-7), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministrio da Cincia e Tecnologia (Brazil) and Ministerio de Ciencia, Tecnologa e InnovaciUn Productiva (Argentina). NR 35 TC 8 Z9 8 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2010 VL 524 AR A46 DI 10.1051/0004-6361/201015464 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685JP UT WOS:000284625300091 ER PT J AU Fukumura, K Shrader, CR Dong, JW Kazanas, D AF Fukumura, K. Shrader, C. R. Dong, J. W. Kazanas, D. TI QPOs in the time domain: an autocorrelation analysis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE black hole physics; stars: oscillations; X-rays: stars; binaries: general; X-rays: binaries ID QUASI-PERIODIC OSCILLATIONS; ACCRETING COMPACT SOURCES; X-RAY-BURSTS; BLACK-HOLE; XTE J1550-564; POWER SPECTRA; GRS 1915+105; CYGNUS X-2; DISCOVERY; BEHAVIOR AB Context. Motivated by the recent proposal that one can obtain quasi-periodic oscillations (QPOs) by photon echoes manifesting as non-trivial features in the autocorrelation function (ACF), we study the ACFs of the light curves of three accreting black hole candidates and a neutron star already known to exhibit QPOs namely, GRS 1915+105, XTE J1550-564, XTE J1859+226 and Cygnus X-2. Aims. We present a comparative study of the timing properties of these systems in the frequency and time domain in search for similarities/differences that may provide clues to the physics underlying the QPO phenomenon. Methods. We compute and focus on the form of the ACFs in search of systematics or specific temporal properties at the time scales associated with the known QPO frequencies in comparison with the corresponding PDS. Results. Even within our small object sample we find both similarities as well as significant and subtle differences in the form of the ACFs both amongst black holes and between black holes and neutron stars to warrant a closer look at the QPO phenomenon in the time domain: the QPO features manifest as an oscillatory behavior of the ACF at lags near zero; the oscillation damps exponentially on time scales equal to the inverse QPO width to a level of a percent or so. In black holes this oscillatory behavior is preserved and easily discerned at much longer lags while this is not the case for the neutron star system Cyg X-2. The ACF of GRS 1915+105 provides an exception to this general behavior in that its decay is linear in time indicating an undamped oscillation of coherent phase. We present simple ad hoc models that reproduce these diverse time domain behaviors and we speculate that their origin is the phase coherence of the underlying oscillation. Conclusions. It appears plausible that time domain analyses, complementary to the more common frequency domain ones, could impose tighter constraints and provide clues for the driving mechanisms behind the QPO phenomenon. C1 [Fukumura, K.; Shrader, C. R.; Kazanas, D.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Fukumura, K.] Univ Maryland Baltimore Cty, UMBC CRESST, Baltimore, MD 21250 USA. [Shrader, C. R.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Dong, J. W.] Columbia Univ, Dept Mech Engn, New York, NY 10027 USA. RP Fukumura, K (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM Keigo.Fukumura@nasa.gov; Chris.R.Shrader@nasa.gov; jianwdong@caa.columbia.edu; Demos.Kazanas@nasa.gov NR 22 TC 2 Z9 2 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2010 VL 524 AR A34 DI 10.1051/0004-6361/201014736 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685JP UT WOS:000284625300034 ER PT J AU Limousin, M Jullo, E Richard, J Cabanac, R Suyu, SH Halkola, A Kneib, JP Gavazzi, R Soucail, G AF Limousin, M. Jullo, E. Richard, J. Cabanac, R. Suyu, S. H. Halkola, A. Kneib, J. -P. Gavazzi, R. Soucail, G. TI Strong lensing as a probe of the mass distribution beyond the Einstein radius Mass and light in SL2S J08544-0121, a galaxy group at z=0.35 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: strong; dark matter ID GRAVITATIONAL LENSES; COSMIC-HORSESHOE; GROUP CONNECTION; CLUSTER; ENVIRONMENTS; ABELL-1689; SEPARATION; RESOLUTION; RINGS; SHEAR AB Strong lensing has been employed extensively to obtain accurate mass measurements within the Einstein radius. We here use strong lensing to probe mass distributions beyond the Einstein radius. We consider SL2SJ08544-0121, a galaxy group at redshift z = 0.35 with a bimodal light distribution and with a strong lensing system located at one of the two luminosity peaks separated by similar to 54 ''. The main arc and the counter-image of the strong lensing system are located at similar to 5 '' and similar to 8 '' from the lens galaxy centre. We find that a simple elliptical isothermal potential cannot satisfactorily reproduce the strong lensing observations. However, with a mass model for the group built from its light-distribution with a smoothing factor s and a mass-to-light ratio M/L, we obtain an accurate reproduction of the observations. We find M/L = 98 +/- 27 (i band, solar units, not corrected for evolution) and s = 20 '' +/- 9 (2 sigma confidence level). Moreover, we use weak lensing to independently estimate the mass of the group, and find a consistent M/L in the range 66-146 (1-sigma confidence level). This suggests that light is a good tracer of mass. Interestingly, this also shows that a strong lensing-only analysis (on scales of similar to 10 '') can constrain the properties of nearby objects (on scales of similar to 100 ''). We characterise the type of perturbed strong lensing system that allows such an analysis: a non dominant strong lensing system used as a test particle to probe the main potential. This kind of analysis needs to be validated with other systems because it could provide a quick way of probing the mass distribution of clusters and groups. This is particularly relevant in the context of forthcoming wide-field surveys, which will yield thousands of strong lenses, some of which perturbed enough to pursue the analysis proposed in this paper. C1 [Limousin, M.; Jullo, E.; Kneib, J. -P.] Univ Aix Marseille 1, UMR CNRS 6610, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Limousin, M.; Cabanac, R.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-65000 Tarbes, France. [Limousin, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Jullo, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Richard, J.] Univ Durham, Dept Phys & Astron, Durham DH3 1LE, England. [Richard, J.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Suyu, S. H.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Halkola, A.] Tech Univ Munich, Excellence Cluster Univ, D-85748 Garching, Germany. [Gavazzi, R.] Inst Astrophys, UMR 7095, CNRS, F-75014 Paris, France. [Gavazzi, R.] UPMC Univ Paris 06, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Soucail, G.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. RP Limousin, M (reprint author), Univ Aix Marseille 1, UMR CNRS 6610, Lab Astrophys Marseille, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France. EM marceau.limousin@oamp.fr RI Kneib, Jean-Paul/A-7919-2015 OI Kneib, Jean-Paul/0000-0002-4616-4989 NR 50 TC 11 Z9 11 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2010 VL 524 AR A95 DI 10.1051/0004-6361/200912747 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685JP UT WOS:000284625300005 ER PT J AU Pence, WD Chiappetti, L Page, CG Shaw, RA Stobie, E AF Pence, W. D. Chiappetti, L. Page, C. G. Shaw, R. A. Stobie, E. TI Definition of the Flexible Image Transport System (FITS), version 3.0 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: miscellaneous; methods: miscellaneous; techniques: miscellaneous; reference systems; standards; astronomical databases: miscellaneous ID REPRESENTATIONS; EXTENSION AB The Flexible Image Transport System (FITS) has been used by astronomers for over 30 years as a data interchange and archiving format; FITS files are now handled by a wide range of astronomical software packages. Since the FITS format definition document (the "standard") was last printed in this journal in 2001, several new features have been developed and standardized, notably support for 64-bit integers in images and tables, variable-length arrays in tables, and new world coordinate system conventions which provide a mapping from an element in a data array to a physical coordinate on the sky or within a spectrum. The FITS Working Group of the International Astronomical Union has therefore produced this new version 3.0 of the FITS standard, which is provided here in its entirety. In addition to describing the new features in FITS, numerous editorial changes were made to the previous version to clarify and reorganize many of the sections. Also included are some appendices which are not formally part of the standard. The FITS standard is likely to undergo further evolution, in which case the latest version may be found on the FITS Support Office Web site at http://fits.gsfc.nasa.gov/, which also provides many links to FITS-related resources. C1 [Pence, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chiappetti, L.] INAF IASF Milano, I-20133 Milan, Italy. [Page, C. G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Shaw, R. A.; Stobie, E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Pence, WD (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM william.pence@nasa.gov OI Chiappetti, Lucio/0000-0001-7857-7908 NR 24 TC 59 Z9 61 U1 3 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2010 VL 524 AR A42 DI 10.1051/0004-6361/201015362 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685JP UT WOS:000284625300085 ER PT J AU Srinivasan, S Sargent, BA Matsuura, M Meixner, M Kemper, F Tielens, AGGM Volk, K Speck, AK Woods, PM Gordon, K Marengo, M Sloan, GC AF Srinivasan, S. Sargent, B. A. Matsuura, M. Meixner, M. Kemper, F. Tielens, A. G. G. M. Volk, K. Speck, A. K. Woods, P. M. Gordon, K. Marengo, M. Sloan, G. C. TI The mass-loss return from evolved stars to the Large Magellanic Cloud III. Dust properties for carbon-rich asymptotic giant branch stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: carbon; circumstellar matter; stars: mass-loss; Magellanic Clouds; stars: individual: OGLE LMC LPV 28579 ID LONG-PERIOD VARIABLES; SPITZER-SPACE-TELESCOPE; GRAVITATIONAL LENSING EXPERIMENT; AGB-STARS; SILICON-CARBIDE; LOSS RATES; CIRCUMSTELLAR ENVELOPES; RADIATIVE-TRANSFER; OPTICAL-PROPERTIES; SIZE DISTRIBUTION AB We present a radiative transfer model for the circumstellar dust shell around a Large Magellanic Cloud (LMC) long-period variable (LPV) previously studied as part of the Optical Gravitational Lensing Experiment (OGLE) survey of the LMC. OGLE LMC LPV 28579 (SAGE J051306.40-690946.3) is a carbon-rich asymptotic giant branch (AGB) star for which we have Spitzer broadband photometry and spectra from the SAGE and SAGE-Spec programs along with broadband UBVIJHK(s) photometry. By modeling this source, we obtain a baseline set of dust properties to be used in the construction of a grid of models for carbon stars. We reproduce the spectral energy distribution of the source using a mixture of amorphous carbon and silicon carbide with 15% SiC by mass. The grain sizes are distributed according to the KMH model, with gamma = 3.5, a(min) = 0.01 mu m and a(0) = 1.0 mu m. The best-fit model produces an optical depth of 0.28 for the dust shell at the peak of the SiC feature (11.3 mu m), with an inner radius of about 1430 R(circle dot) or 4.4 times the stellar radius. The temperature at this inner radius is 1310 K. Assuming an expansion velocity of 10 km s(-1), we obtain a dust mass-loss rate of 2.5 x 10(-9) M(circle dot) yr(-1). We calculate a 15% variation in this mass-loss rate by testing the sensitivity of the fit to variation in the input parameters. We also present a simple model for the molecular gas in the extended atmosphere that could give rise to the 13.7 mu m feature seen in the spectrum. We find that a combination of CO and C(2)H(2) gas at an excitation temperature of about 1000 K and column densities of 3 x 10(21) cm(-2) and 10(19) cm(-2) respectively are able to reproduce the observations. Given that the excitation temperature is close to the temperature of the dust at the inner radius, most of the molecular contribution probably arises from this region. The luminosity corresponding to the first epoch of SAGE observations is 6580 L(circle dot). For an effective temperature of about 3000 K, this implies a stellar mass of 1.5-2 M(circle dot) and an age of 1-2.5 Gyr for OGLE LMC LPV 28579. We calculate a gas mass-loss rate of 5.0 x 10(-7) M(circle dot) yr(-1) assuming a gas: dust ratio of 200. This number is comparable to the gas mass-loss rates estimated from the period, color and 8 mu m flux of the source. C1 [Srinivasan, S.] Inst Astrophys Paris, F-75014 Paris, France. [Sargent, B. A.; Meixner, M.; Volk, K.; Gordon, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Matsuura, M.] UCL, Dept Phys & Astron, Astrophys Grp, UCL Inst Origins, London WC1E 6BT, England. [Matsuura, M.] Univ Coll London, Mullard Space Sci Lab, UCL Inst Origins, Dorking RH5 6NT, Surrey, England. [Kemper, F.; Woods, P. M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Tielens, A. G. G. M.] NASA, Ames Res Ctr, SOFIA Off, Moffett Field, CA 94035 USA. [Speck, A. K.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50010 USA. [Sloan, G. C.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. RP Srinivasan, S (reprint author), Inst Astrophys Paris, 98Bis Blvd Arago, F-75014 Paris, France. EM srinivas@iap.fr RI Kemper, Francisca/D-8688-2011 OI Kemper, Francisca/0000-0003-2743-8240 FU NASA [1407, NAG5-12595]; Spitzer [1310534] FX The authors would like to thank the anonymous referee for their helpful comments on the manuscript. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. The research in this paper has been funded by Spitzer grant 1310534 and NASA grant NAG5-12595. The authors have made use of the SIMBAD astronomical database and would like to thank those responsible for its upkeep. The authors also thank Bernie Shiao at STScI for his hard work on the SAGE database and his kind assistance. NR 91 TC 16 Z9 16 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2010 VL 524 AR A49 DI 10.1051/0004-6361/201014991 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 685JP UT WOS:000284625300050 ER PT J AU De Breuck, C Seymour, N Stern, D Willner, SP Eisenhardt, PRM Fazio, GG Galametz, A Lacy, M Rettura, A Rocca-Volmerange, B Vernet, J AF De Breuck, Carlos Seymour, Nick Stern, Daniel Willner, S. P. Eisenhardt, P. R. M. Fazio, G. G. Galametz, Audrey Lacy, Mark Rettura, Alessandro Rocca-Volmerange, Brigitte Vernet, Joeel TI THE SPITZER HIGH-REDSHIFT RADIO GALAXY SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: high-redshift; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; K-Z RELATION; SPECTRAL ENERGY-DISTRIBUTIONS; INFRARED ARRAY CAMERA; ELLIPTIC GALAXIES; X-RAY; SPACE-TELESCOPE; STAR-FORMATION; SKY SURVEY; KECK SPECTROPOLARIMETRY AB We present results from a comprehensive imaging survey of 70 radio galaxies at redshifts 1 < z < 5.2 using all three cameras on board the Spitzer Space Telescope. The resulting spectral energy distributions unambiguously show a stellar population in 46 sources and hot dust emission associated with the active nucleus in 59. Using a new rest-frame S-3 (mu m)/S-1.6 (mu m) versus S-5 (mu m)/S-3 (mu m) criterion, we identify 42 sources where the rest-frame 1.6 (mu m) emission from the stellar population can be measured. For these radio galaxies, the median stellar mass is high, 2 x 10(11) M-circle dot, and remarkably constant within the range 1 < z < 3. At z > 3, there is tentative evidence for a factor of two decrease in stellar mass. This suggests that radio galaxies have assembled the bulk of their stellar mass by z similar to 3, but confirmation by more detailed decomposition of stellar and active galactic nucleus (AGN) emission is needed. The rest-frame 500 MHz radio luminosities are only marginally correlated with stellar mass but are strongly correlated with the rest-frame 5 mu m hot dust luminosity. This suggests that the radio galaxies have a large range of Eddington ratios. We also present new Very Large Array 4.86 and 8.46 GHz imaging of 14 radio galaxies and find that radio core dominance-an indicator of jet orientation-is strongly correlated with hot dust luminosity. While all of our targets were selected as narrow-lined, type 2 AGNs, this result can be understood in the context of orientation-dependent models if there is a continuous distribution of orientations from obscured type 2 to unobscured type 1 AGNs rather than a clear dichotomy. Finally, four radio galaxies have nearby (<6 '') companions whose mid-IR colors are suggestive of their being AGNs. This may indicate an association between radio galaxy activity and major mergers. C1 [De Breuck, Carlos; Galametz, Audrey; Vernet, Joeel] European So Observ, D-85748 Garching, Germany. [Seymour, Nick] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Stern, Daniel; Eisenhardt, P. R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Willner, S. P.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lacy, Mark] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Rettura, Alessandro] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Rocca-Volmerange, Brigitte] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Rocca-Volmerange, Brigitte] Univ Paris 11, F-91405 Orsay, France. RP De Breuck, C (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM cdebreuc@eso.org OI Vernet, Joel/0000-0002-8639-8560; Seymour, Nicholas/0000-0003-3506-5536; De Breuck, Carlos/0000-0002-6637-3315 FU NASA through Jet Propulsion Laboratory/Caltech FX C.D.B. and N.S. thank the Jet Propulsion Laboratory and the California Institute of Technology for their hospitality during an extended visit in Spring 2010. We thank Patrick Ogle for stimulating discussions. This work is based on observations made with the Spitzer Space Telescope and made use of the NASA/IPAC Extragalactic Database (NED). Both NED and Spitzer are operated by the Jet Propulsion Laboratory, Caltech under contracts with NASA. The work of D. S. and P. R. M. E. was carried out at 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 the Jet Propulsion Laboratory/Caltech. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 125 TC 49 Z9 49 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 36 EP 62 DI 10.1088/0004-637X/725/1/36 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700006 ER PT J AU Guiriec, S Briggs, MS Connaugthon, V Kara, E Daigne, F Kouveliotou, C van der Horst, AJ Paciesas, W Meegan, CA Bhat, PN Foley, S Bissaldi, E Burgess, M Chaplin, V Diehl, R Fishman, G Gibby, M Giles, MM Goldstein, A Greiner, J Gruber, D von Kienlin, A Kippen, M McBreen, S Preece, R Rau, A Tierney, D Wilson-Hodge, C AF Guiriec, Sylvain Briggs, Michael S. Connaugthon, Valerie Kara, Erin Daigne, Frederic Kouveliotou, Chryssa van der Horst, Alexander J. Paciesas, William Meegan, Charles A. Bhat, P. N. Foley, Suzanne Bissaldi, Elisabetta Burgess, Michael Chaplin, Vandiver Diehl, Roland Fishman, Gerald Gibby, Melissa Giles, Misty M. Goldstein, Adam Greiner, Jochen Gruber, David von Kienlin, Andreas Kippen, Marc McBreen, Sheila Preece, Robert Rau, Arne Tierney, Dave Wilson-Hodge, Colleen TI TIME-RESOLVED SPECTROSCOPY OF THE THREE BRIGHTEST AND HARDEST SHORT GAMMA-RAY BURSTS OBSERVED WITH THE FERMI GAMMA-RAY BURST MONITOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma rays: general; radiation mechanisms: non-thermal ID RELATIVISTIC COLLISIONLESS SHOCKS; SPECTRAL COMPONENT; BATSE OBSERVATIONS; GRB 090510; EMISSION; MODEL; LUMINOSITY; EVOLUTION; CATALOG; PROMPT AB From 2008 July to 2009 October, the Gamma-ray Burst Monitor (GBM) on board the Fermi Gamma-ray Space Telescope has detected 320 gamma-ray bursts (GRBs). About 20% of these events are classified as short based on their T-90 duration below 2 s. We present here for the first time time-resolved spectroscopy at timescales as short as 2 ms for the three brightest short GRBs observed with GBM. The time-integrated spectra of the events deviate from the Band function, indicating the existence of an additional spectral component, which can be fit by a power law with index similar to -1.5. The time-integrated E-peak values exceed 2 MeV for two of the bursts and are well above the values observed in the brightest long GRBs. Their E-peak values and their low-energy power-law indices (alpha) confirm that short GRBs are harder than long ones. We find that short GRBs are very similar to long ones, but with light curves contracted in time and with harder spectra stretched toward higher energies. In our time-resolved spectroscopy analysis, we find that the E-peak values range from a few tens of keV up to more than 6 MeV. In general, the hardness evolutions during the bursts follow their flux/intensity variations, similar to long bursts. However, we do not always see the E-peak leading the light-curve rises and confirm the zero/short average light-curve spectral lag below 1 MeV, already established for short GRBs. We also find that the time-resolved low-energy power-law indices of the Band function mostly violate the limits imposed by the synchrotron models for both slow and fast electron cooling and may require additional emission processes to explain the data. Finally, we interpreted these observations in the context of the current existing models and emission mechanisms for the prompt emission of GRBs. C1 [Guiriec, Sylvain; Briggs, Michael S.; Connaugthon, Valerie; Paciesas, William; Bhat, P. N.; Burgess, Michael; Chaplin, Vandiver; Goldstein, Adam; Preece, Robert] Univ Alabama, NSSTC, Huntsville, AL 35805 USA. [Kara, Erin] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Daigne, Frederic] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Kouveliotou, Chryssa; Fishman, Gerald; Wilson-Hodge, Colleen] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [van der Horst, Alexander J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Meegan, Charles A.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. [Foley, Suzanne; Bissaldi, Elisabetta; Diehl, Roland; Greiner, Jochen; Gruber, David; von Kienlin, Andreas; Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gibby, Melissa; Giles, Misty M.] Jacobs Technol Inc, Huntsville, AL 35806 USA. [Kippen, Marc] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [McBreen, Sheila; Tierney, Dave] Univ Coll, Dublin 4, Ireland. RP Guiriec, S (reprint author), Univ Alabama, NSSTC, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM sylvain.guiriec@nasa.gov RI Bissaldi, Elisabetta/K-7911-2016; OI Bissaldi, Elisabetta/0000-0001-9935-8106; Preece, Robert/0000-0003-1626-7335; McBreen, Sheila/0000-0002-1477-618X FU German Bundesministerium fur Wirtschaft und Technologie (BMWi) via the Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [50 QV 0301, 50 OG 0502]; NASA at the MSFC; Irish Research Council for Science, Engineering, and Technology; Marie Curie Actions FX We thank the referee and the editor for their useful comments, which increased the quality of the paper. The GBM project is supported by the German Bundesministerium fur Wirtschaft und Technologie (BMWi) via the Deutsches Zentrum fur Luft- und Raumfahrt (DLR) under the contract numbers 50 QV 0301 and 50 OG 0502. A.J.v.d.H. was supported by an appointment to the NASA Postdoctoral Program at the MSFC, administered by Oak Ridge Associated Universities through a contract with NASA. S. F. acknowledges the support of the Irish Research Council for Science, Engineering, and Technology, cofunded by Marie Curie Actions under FP7. NR 73 TC 49 Z9 49 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 225 EP 241 DI 10.1088/0004-637X/725/1/225 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700040 ER PT J AU Fryer, CL Ruiter, AJ Belczynski, K Brown, PJ Bufano, F Diehl, S Fontes, CJ Frey, LH Holland, ST Hungerford, AL Immler, S Mazzali, P Meakin, C Milne, PA Raskin, C Timmes, FX AF Fryer, Chris L. Ruiter, Ashley J. Belczynski, Krzysztof Brown, Peter J. Bufano, Filomena Diehl, Steven Fontes, Christopher J. Frey, Lucille H. Holland, Stephen T. Hungerford, Aimee L. Immler, Stefan Mazzali, Paolo Meakin, Casey Milne, Peter A. Raskin, Cody Timmes, Francis X. TI SPECTRA OF TYPE IA SUPERNOVAE FROM DOUBLE DEGENERATE MERGERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; supernovae: general; white dwarfs ID GRAVITATIONALLY CONFINED DETONATION; WHITE-DWARFS; CIRCUMSTELLAR MEDIUM; HYDRODYNAMICS CODE; COMPACT OBJECTS; ACCRETION; EVOLUTION; EXPLOSION; RAY; SPECTROSCOPY AB The merger of two white dwarfs (aka double-degenerate merger) has often been cited as a potential progenitor of Type Ia supernovae. Here we combine population synthesis, merger, and explosion models with radiation-hydrodynamics light-curve models to study the implications of such a progenitor scenario on the observed Type Ia supernova population. Our standard model, assuming double-degenerate mergers do produce thermonuclear explosions, produces supernova light curves that are broader than the observed type Ia sample. In addition, we discuss how the shock breakout and spectral features of these double-degenerate progenitors will differ from the canonical bare Chandrasekhar-massed explosion models. We conclude with a discussion of how one might reconcile these differences with current observations. C1 [Fryer, Chris L.; Belczynski, Krzysztof; Diehl, Steven; Fontes, Christopher J.; Frey, Lucille H.; Hungerford, Aimee L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Fryer, Chris L.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Ruiter, Ashley J.; Mazzali, Paolo] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Belczynski, Krzysztof] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Brown, Peter J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Bufano, Filomena] Univ Padua, Dipartimento Astron, INAF Osservatoroio Astron Padova, I-35122 Padua, Italy. [Holland, Stephen T.; Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Raskin, Cody; Timmes, Francis X.] Arizona State Univ, SESE, Tempe, AZ 85287 USA. [Meakin, Casey; Milne, Peter A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Mazzali, Paolo] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Mazzali, Paolo] INAF OAPD, I-35122 Padua, Italy. RP Fryer, CL (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA. EM fryer@lanl.gov; ajr@mpa-garching.mpg.de; kbelczyn@nmsu.edu; grbpeter@yahoo.com; filomena.bufano@oapd.inaf.it; stevendiehl@gmail.com; cjf@lanl.gov; lfrey@lanl.gov; Stephen.T.Holland@nasa.gov; aimee@lanl.gov; stefan.m.immler@nasa.gov; mazzali@MPA-Garching.MPG.DE; pmilne511@cox.net; codyraskin@gmail.com OI Frey, Lucille/0000-0002-5478-2293 FU National Nuclear Security Administration of the U.S. Department of Energy at Los Alamos National Laboratory; [DE-AC52-06NA25396] FX This work was carried out in part under the auspices of the National Nuclear Security Administration of the U.S. Department of Energy at Los Alamos National Laboratory and supported by contract no. DE-AC52-06NA25396. NR 40 TC 46 Z9 46 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 296 EP 308 DI 10.1088/0004-637X/725/1/296 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700047 ER PT J AU Parkinson, PMS Dormody, M Ziegler, M Ray, PS Abdo, AA Ballet, J Baring, MG Belfiore, A Burnett, TH Caliandro, GA Camilo, F Caraveo, PA de Luca, A Ferrara, EC Freire, PCC Grove, JE Gwon, C Harding, AK Johnson, RP Johnson, TJ Johnston, S Keith, M Kerr, M Knodlseder, J Makeev, A Marelli, M Michelson, PF Parent, D Ransom, SM Reimer, O Romani, RW Smith, DA Thompson, DJ Watters, K Weltevrede, P Wolff, MT Wood, KS AF Parkinson, P. M. Saz Dormody, M. Ziegler, M. Ray, P. S. Abdo, A. A. Ballet, J. Baring, M. G. Belfiore, A. Burnett, T. H. Caliandro, G. A. Camilo, F. Caraveo, P. A. de Luca, A. Ferrara, E. C. Freire, P. C. C. Grove, J. E. Gwon, C. Harding, A. K. Johnson, R. P. Johnson, T. J. Johnston, S. Keith, M. Kerr, M. Knoedlseder, J. Makeev, A. Marelli, M. Michelson, P. F. Parent, D. Ransom, S. M. Reimer, O. Romani, R. W. Smith, D. A. Thompson, D. J. Watters, K. Weltevrede, P. Wolff, M. T. Wood, K. S. TI EIGHT gamma-RAY PULSARS DISCOVERED IN BLIND FREQUENCY SEARCHES OF FERMI LAT DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; open clusters and associations: individual (Westerlund 2); pulsars: general; pulsars: individual (PSR J1023-5746, PSR J1044-5737, PSR J1413-6205, PSR J1429-5911, PSR J1846+0919, PSR J1954+2836, PSR J1957+5033, PSR J2055+25); X-rays: individual (CXOU J102302.8-574606, XMMU J205549.4+253959) ID LARGE-AREA TELESCOPE; CLUSTER WESTERLUND-2; SOURCE LIST; RADIO; CATALOG; POPULATION; LUMINOSITIES; EMISSION AB We report the discovery of eight gamma-ray pulsars in blind frequency searches of similar to 650 source positions using the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. We present the timing models, light curves, and detailed spectral parameters of the new pulsars. PSRs J1023-5746, J1044-5737, J1413-5205, J1429-5911, and J1954+2836 are young (tau(c) < 100 kyr), energetic ((E) over dot greater than or similar to 10(36) erg s(-1)), and located within the Galactic plane (vertical bar b vertical bar < 3 degrees). The remaining three pulsars, PSRs J1846+0919, J1957+5033, and J2055+25, are less energetic, and located off the plane. Five pulsars are associated with sources included in the Fermi-LAT bright gamma-ray source list, but only one, PSR J1413-6205, is clearly associated with an EGRET source. PSR J1023-5746 has the smallest characteristic age (tau(c) = 4.6 kyr) and is the most energetic ((E) over dot = 1.1 x 10(37) erg s(-1)) of all gamma-ray pulsars discovered so far in blind searches. By analyzing > 100 ks of publicly available archival Chandra X-ray data, we have identified the likely counterpart of PSR J1023-5746 as a faint, highly absorbed source, CXOU J102302.8-574606. The large X-ray absorption indicates that this could be among the most distant gamma-ray pulsars detected so far. PSR J1023-5746 is positionally coincident with the TeV source HESS J1023-575, located near the young stellar cluster Westerlund 2, while PSR J1954+2836 is coincident with a 4.3 sigma excess reported by Milagro at a median energy of 35 TeV. PSRs J1957+5033 and J2055+25 have the largest characteristic ages (tau(c) similar to 1 Myr) and are the least energetic ((E) over dot similar to 5 x 10(33) erg s(-1)) of the newly discovered pulsars. We used recent XMM observations to identify the counterpart of PSR J2055+25 as XMMU J205549.4+253959. Deep radio follow-up observations of the eight pulsars resulted in no detections of pulsations and upper limits comparable to the faintest known radio pulsars, indicating that these pulsars can be included among the growing population of radio-quiet pulsars in our Galaxy being uncovered by the LAT, and currently numbering more than 20. C1 [Parkinson, P. M. Saz; Dormody, M.; Ziegler, M.; Belfiore, A.; Johnson, R. P.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Ray, P. S.; Abdo, A. A.; Grove, J. E.; Gwon, C.; Makeev, A.; Parent, D.; Wolff, M. T.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Ballet, J.] Univ Paris Diderot, Laboratoire AIM, CEA, IRFU,CNRS,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Belfiore, A.; Caraveo, P. A.; Marelli, M.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Belfiore, A.] Univ Pavia, DFNT, I-27100 Pavia, Italy. [Burnett, T. H.; Kerr, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caliandro, G. A.] CSIC, Inst Ciencies Espai, IEEC, Barcelona 08193, Spain. [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [de Luca, A.] IUSS, I-27100 Pavia, Italy. [Ferrara, E. C.; Harding, A. K.; Johnson, T. J.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Freire, P. C. C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Johnson, T. J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Johnson, T. J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Johnston, S.; Keith, M.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Knoedlseder, J.] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA. [Marelli, M.] Univ Insubria, I-21100 Varese, Italy. [Michelson, P. F.; Reimer, O.; Romani, R. W.; Watters, K.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Michelson, P. F.; Reimer, O.; Romani, R. W.; Thompson, D. J.; Watters, K.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Smith, D. A.] Ctr Etud Nucleaires Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France. [Smith, D. A.] Univ Bordeaux, Ctr Etud Nucleaires Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Ransom, S. M.] NRAO, Charlottesville, VA 22903 USA. [Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Weltevrede, P.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. RP Parkinson, PMS (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. EM pablo@scipp.ucsc.edu; mdormody@ucsc.edu; ziegler@scipp.ucsc.edu; Paul.Ray@nrl.navy.mil RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Reimer, Olaf/A-3117-2013; OI Thompson, David/0000-0001-5217-9135; Reimer, Olaf/0000-0001-6953-1385; Caraveo, Patrizia/0000-0003-2478-8018 FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; Associated Universities, Inc.; National Science Foundation; Commonwealth Government FX Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; The GBT is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; The Arecibo Observatory is part of the National Astronomy and Ionosphere Center, which is operated by Cornell University under a cooperative agreement with the National Science Foundation.; The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth Government for operation as a National Facility managed by CSIRO. NR 44 TC 72 Z9 72 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 DEC PY 2010 VL 725 IS 1 BP 571 EP 584 DI 10.1088/0004-637X/725/1/571 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700070 ER PT J AU Arendt, RG Dwek, E Blair, WP Ghavamian, P Hwang, U Long, KS Petre, R Rho, J Winkler, PF AF Arendt, Richard G. Dwek, Eli Blair, William P. Ghavamian, Parviz Hwang, Una Long, Knox S. Petre, Robert Rho, Jeonghee Winkler, P. Frank TI SPITZER OBSERVATIONS OF DUST DESTRUCTION IN THE PUPPIS A SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: ISM; ISM: individual objects (Puppis A); ISM: supernova remnants ID BRIGHT EASTERN KNOT; X-RAY-EMISSION; SPACE-TELESCOPE; INTERSTELLAR DUST; NEUTRAL HYDROGEN; EXTENDED SOURCES; VLA OBSERVATIONS; INFRARED SURVEY; EARLY UNIVERSE; DISCOVERY AB The interaction of the Puppis A supernova remnant (SNR) with a neighboring molecular cloud provides a unique opportunity to measure the amount of grain destruction in an SNR shock. Spitzer Space Telescope MIPS imaging of the entire SNR at 24, 70, and 160 mu m shows an extremely good correlation with X-ray emission, indicating that the SNR's IR radiation is dominated by the thermal emission of swept-up interstellar dust, collisionally heated by the hot shocked gas. Spitzer IRS spectral observations targeted both the Bright Eastern Knot (BEK) of the SNR where a small cloud has been engulfed by the supernova blast wave and outlying portions of the associated molecular cloud that are yet to be hit by the shock front. Modeling the spectra from both regions reveals the composition and the grain size distribution of the interstellar dust, both in front of and behind the SNR shock front. The comparison shows that the ubiquitous polycyclic aromatic hydrocarbons of the interstellar medium are destroyed within the BEK, along with nearly 25% of the mass of graphite and silicate dust grains. C1 [Arendt, Richard G.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. [Arendt, Richard G.; Dwek, Eli; Hwang, Una; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blair, William P.; Hwang, Una] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Ghavamian, Parviz; Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Rho, Jeonghee] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Rho, Jeonghee] NASA, Ames Res Ctr, Univ Space Res Assoc, Moffett Field, CA 94035 USA. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Arendt, RG (reprint author), Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. EM Richard.G.Arendt@nasa.gov RI Dwek, Eli/C-3995-2012; OI Arendt, Richard/0000-0001-8403-8548 FU NASA; NSF [AST-0908566] 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. We acknowledge the use of NASA's SkyView facility (http://skyview.gsfc.nasa.gov) located at NASA Goddard Space Flight Center. This research has made use of NASA's Astrophysics Data System Bibliographic Services. P.F.W. acknowledges additional funding from the NSF through grant AST-0908566. NR 56 TC 23 Z9 23 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 585 EP 597 DI 10.1088/0004-637X/725/1/585 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700071 ER PT J AU Tanvir, NR Rol, E Levan, AJ Svensson, K Fruchter, AS Granot, J O'Brien, PT Wiersema, K Starling, RLC Jakobsson, P Fynbo, J Hjorth, J Curran, PA van der Horst, AJ Kouveliotou, C Racusin, JL Burrows, DN Genet, F AF Tanvir, N. R. Rol, E. Levan, A. J. Svensson, K. Fruchter, A. S. Granot, J. O'Brien, P. T. Wiersema, K. Starling, R. L. C. Jakobsson, P. Fynbo, J. Hjorth, J. Curran, P. A. van der Horst, A. J. Kouveliotou, C. Racusin, J. L. Burrows, D. N. Genet, F. TI LATE-TIME OBSERVATIONS OF GRB 080319B: JET BREAK, HOST GALAXY, AND ACCOMPANYING SUPERNOVA SO ASTROPHYSICAL JOURNAL LA English DT Article DE high-redshift; gamma-ray burst: individual (GRB 080319B); supernovae: individual ID GAMMA-RAY BURST; MASS-METALLICITY RELATION; CORE-COLLAPSE SUPERNOVAE; AFTERGLOW LIGHT CURVES; MILKY-WAY; REDSHIFT; RADIATION; EMISSION; IMAGES; LIMITS AB The Swift-discovered GRB 080319B was by far the most distant source ever observed at naked-eye brightness, reaching a peak apparent magnitude of 5.3 at a redshift of z = 0.937. We present our late-time optical (Hubble Space Telescope, Gemini, and Very Large Telescope) and X-ray (Chandra) observations, which confirm that an achromatic break occurred in the power-law afterglow light curve at similar to 11 days post-burst. This most likely indicates that the gamma-ray burst (GRB) outflow was collimated, which for a uniform jet would imply a total energy in the jet E-jet greater than or similar to 10(52) erg. Our observations also show a late-time excess of red light, which is well explained if the GRB was accompanied by a supernova (SN), similar to those seen in some other long-duration GRBs. The latest observations are dominated by light from the host and show that the GRB took place in a faint dwarf galaxy (r(AB) approximate to 27.0, rest frame M-B approximate to -17.2). This galaxy is small even by the standards of other GRB hosts, which is suggestive of a low-metallicity environment. Intriguingly, the properties of this extreme event-a small host and bright SN-are entirely typical of the very low luminosity bursts such as GRB 980425 and GRB 060218. C1 [Tanvir, N. R.; Wiersema, K.; Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Rol, E.] Astron Inst Anton Pannekoek, NL-1090 SJ Amsterdam, Netherlands. [Levan, A. J.; Svensson, K.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Fruchter, A. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Granot, J.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Fynbo, J.; Hjorth, J.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Curran, P. A.] Ctr Saclay, AIM, CEA, CNRS,DSM,Irfu SAP, F-91191 Gif Sur Yvette, France. [van der Horst, A. J.; Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. [Racusin, J. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Genet, F.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. RP Tanvir, NR (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM nrt3@star.le.ac.uk RI Racusin, Judith/D-2935-2012; Curran, Peter/B-5293-2013; Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014; Jakobsson, Pall/L-9950-2015 OI Curran, Peter/0000-0003-3003-4626; Fynbo, Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306; Jakobsson, Pall/0000-0002-9404-5650 FU NASA [NAS 5-26555]; NSF; National Science Foundation (United States); Science and Technology Facilities Council (United Kingdom); National Research Council (Canada); CONICYT (Chile); Australian Research Council (Australia); Ministrio da Cincia e Tecnologia (Brazil); SECYT (Argentina); Danish National Research Foundation; STFC; Royal Society; NASA at the MSFC; NASA FX We are grateful to Matt Mountain for awarding director's discretionary time on HST to observe GRB 080319B under program GO/DD 11513 (PI: Tanvir). Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.; Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministrio da Cincia e Tecnologia (Brazil), and SECYT (Argentina).; The DARK Cosmology Centre is funded by the Danish National Research Foundation.; We particularly thank the staff of the VLT and Gemini for their efforts in obtaining the optical data, and those at CXC for their assistance in scheduling the Chandra observations. We also gratefully acknowledge the work of the wider Swift team that makes this research possible. N.R.T., E.R., and A.J.L. are supported by STFC. J.G. gratefully acknowledges a Royal Society Wolfson Research Merit Award. A.J.vdH. is supported by an appointment to the NASA Postdoctoral Program at the MSFC, administered by ORAU through a contract with NASA. NR 47 TC 26 Z9 27 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 625 EP 632 DI 10.1088/0004-637X/725/1/625 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700075 ER PT J AU Reeves, JN Gofford, J Braito, V Sambruna, R AF Reeves, J. N. Gofford, J. Braito, V. Sambruna, R. TI CHANDRA HIGH-RESOLUTION SPECTROSCOPY OF THE CIRCUMNUCLEAR MATTER IN THE BROAD-LINE RADIO GALAXY 3C 445 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (3C 445); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SOFT-X-RAY; QUASI-STELLAR OBJECTS; HELIUM-LIKE IONS; XMM-NEWTON; GRATING SPECTROMETER; ASCA OBSERVATIONS; OPTICAL-SPECTRA; EMISSION-LINES; CENTRAL MASSES AB We present evidence for X-ray line emitting and absorbing gas in the nucleus of the broad-line radio galaxy 3C 445. A 200 ks Chandra Low Energy Transmission Grating observation of 3C 445 reveals the presence of several highly ionized emission lines in the soft X-ray spectrum, primarily from the He-and H-like ions of O, Ne, Mg, and Si. Radiative recombination emission is detected from Ovii and Oviii, indicating that the emitting gas is photoionized. The He-like emission appears to be resolved into forbidden and intercombination line components, which implies a high density of >10(10) cm(-3), while the oxygen lines are velocity broadened with a mean width of similar to 2600 km s(-1) (FWHM). The density and widths of the ionized lines indicate an origin of the gas on sub-parsec scales in the broad-line region. The X-ray continuum of 3C 445 is heavily obscured either by a partial coverer or by a photoionized absorber of column density NH = 2 x 10(23) cm(-2) and ionization parameter log xi = 1.4 erg cm s(-1). However, the view of the X-ray line emission is unobscured, which requires the absorber to be located at radii well within any parsec-scale molecular torus. Instead we suggest that the X-ray absorber in 3C 445 may be associated with an outflowing but clumpy accretion disk wind, with an observed outflow velocity of similar to 10,000 km s(-1). C1 [Reeves, J. N.; Gofford, J.] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Sambruna, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reeves, J. N.] Univ Maryland Baltimore Cty, CSST, Baltimore, MD 21250 USA. RP Reeves, JN (reprint author), Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. EM jnr@astro.keele.ac.uk OI Braito, Valentina/0000-0002-2629-4989 FU NASA FX This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. R. S. acknowledges support from NASA through the Suzaku and Chandra programs. We also thank Tahir Yaqoob for assistance with the Chandra data analysis. NR 72 TC 15 Z9 15 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 803 EP 815 DI 10.1088/0004-637X/725/1/803 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700089 ER PT J AU Hayato, A Yamaguchi, H Tamagawa, T Katsuda, S Hwang, U Hughes, JP Ozawa, M Bamba, A Kinugasa, K Terada, Y Furuzawa, A Kunieda, H Makishima, K AF Hayato, Asami Yamaguchi, Hiroya Tamagawa, Toru Katsuda, Satoru Hwang, Una Hughes, John P. Ozawa, Midori Bamba, Aya Kinugasa, Kenzo Terada, Yukikatsu Furuzawa, Akihiro Kunieda, Hideyo Makishima, Kazuo TI EXPANSION VELOCITY OF EJECTA IN TYCHO's SUPERNOVA REMNANT MEASURED BY DOPPLER BROADENED X-RAY LINE EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: supernova remnants; supernovae: general; X-rays: individual (Tycho's SNR) ID BRAHES 1572 SUPERNOVA; XMM-NEWTON; IMAGING SPECTROMETER; SUZAKU OBSERVATIONS; CHARGE-INJECTION; IA SUPERNOVAE; SPECTROSCOPY; SPECTRUM; HYDROGEN; CHANDRA AB We show that the expansion of ejecta in Tycho's supernova remnant (SNR) is consistent with a spherically symmetric shell, based on Suzaku measurements of the Doppler broadened X-ray emission lines. All of the strong K alpha line emissions show broader widths at the center than at the rim, while the centroid energies are constant across the remnant (except for Ca). This is the pattern expected for Doppler broadening due to expansion of the SNR ejecta in a spherical shell. To determine the expansion velocities of the ejecta, we applied a model for each emission-line feature having two Gaussian components separately representing red-and blueshifted gas, and inferred the Doppler velocity difference between these two components directly from the fitted centroid energy difference. Taking into account the effect of projecting a three-dimensional shell to the plane of the detector, we derived average spherical expansion velocities independently for the K alpha emission of Si, S, Ar, and Fe, and K beta of Si. We found that the expansion velocities of Si, S, and Ar ejecta of 4700 +/- 100 km s(-1) are distinctly higher than that obtained from Fe K alpha emission, 4000 +/- 300 km s(-1), which is consistent with segregation of the Fe in the inner ejecta. Combining the observed ejecta velocities with the ejecta proper-motion measurements by Chandra, we derived a distance to Tycho's SNR of 4 +/- 1 kpc. C1 [Hayato, Asami; Yamaguchi, Hiroya; Tamagawa, Toru; Makishima, Kazuo] RIKEN, Wako, Saitama 3510198, Japan. [Hayato, Asami; Katsuda, Satoru; Hwang, Una] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Ozawa, Midori] Kyoto Univ, Dept Phys, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. [Bamba, Aya] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Bamba, Aya] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Tyuo Ku, Kanagawa 2525210, Japan. [Kinugasa, Kenzo] Gunma Astron Observ, Takayama, Gunma 3770702, Japan. [Terada, Yukikatsu] Saitama Univ, Dept Phys, Sakura, Saitama 3388570, Japan. [Furuzawa, Akihiro; Kunieda, Hideyo] Nagoya Univ, Div Particle & Astrophys Sci, Grad Sch Sci, Nagoya, Aichi 4648602, Japan. [Makishima, Kazuo] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. RP Hayato, A (reprint author), RIKEN, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. EM asami.hayato@nasa.gov RI Terada, Yukikatsu/A-5879-2013; XRAY, SUZAKU/A-1808-2009 OI Terada, Yukikatsu/0000-0002-2359-1857; FU Japan Society for the Promotion of Science (JSPS); NASA [NNG05GP87G] FX We gratefully acknowledge all members of the Suzaku hardware and software teams and the Science Working Group. A. H. is Research Fellow of the Japan Society for the Promotion of Science (JSPS). S. K. is supported by JSPS Postdoctoral Fellowships for Research Abroad. J.P.H. was supported by NASA grant NNG05GP87G. NR 35 TC 48 Z9 48 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 DEC PY 2010 VL 725 IS 1 BP 894 EP 903 DI 10.1088/0004-637X/725/1/894 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700097 ER PT J AU Natale, G Tuffs, RJ Xu, CK Popescu, CC Fischera, J Lisenfeld, U Lu, N Appleton, P Dopita, M Duc, PA Gao, Y Reach, W Sulentic, J Yun, M AF Natale, G. Tuffs, R. J. Xu, C. K. Popescu, C. C. Fischera, J. Lisenfeld, U. Lu, N. Appleton, P. Dopita, M. Duc, P. -A. Gao, Y. Reach, W. Sulentic, J. Yun, M. TI DUST EMISSION AND STAR FORMATION IN STEPHAN'S QUINTET SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: groups: individual (HGC92); galaxies: interactions; galaxies: star formation; infrared: general; intergalactic medium ID SPECTRAL ENERGY-DISTRIBUTION; ABUNDANT MOLECULAR GAS; FAR-INFRARED EMISSION; INTRACLUSTER DUST; INTERSTELLAR GRAINS; COMA CLUSTER; INTERGALACTIC MEDIUM; STARBURST GALAXIES; INTRAGROUP MEDIUM; FORMING GALAXIES AB We analyze a comprehensive set of MIR/FIR observations of Stephan's Quintet (SQ), taken with the Spitzer Space Telescope. Our study reveals the presence of a luminous (L-IR approximate to 4.6x10(43) erg s(-1)) and extended component of infrared dust emission, not connected with the main bodies of the galaxies, but roughly coincident with the X-ray halo of the group. We fitted the inferred dust emission spectral energy distribution of this extended source and the other main infrared emission components of SQ, including the intergalactic shock, to elucidate the mechanisms powering the dust and polycyclic aromatic hydrocarbon emission, taking into account collisional heating by the plasma and heating through UV and optical photons. Combining the inferred direct and dust-processed UV emission to estimate the star formation rate (SFR) for each source we obtain a total SFR for SQ of 7.5 M-circle dot yr(-1), similar to that expected for non-interacting galaxies with stellar mass comparable to the SQ galaxies. Although star formation in SQ is mainly occurring at, or external to the periphery of the galaxies, the relation of SFR per unit physical area to gas column density for the brightest sources is similar to that seen for star formation regions in galactic disks. We also show that available sources of dust in the group halo can provide enough dust to produce up to L-IR approximate to 10(42) erg s(-1) powered by collisional heating. Though a minority of the total infrared emission (which we infer to trace distributed star-formation), this is several times higher than the X-ray luminosity of the halo, so could indicate an important cooling mechanism for the hot intergalactic medium (IGM) and account for the overall correspondence between FIR and X-ray emission. We investigate two potential modes of star formation in SQ consistent with the data, fueled either by gas from a virialized hot IGM continuously accreting onto the group, whose cooling is enhanced by grains injected from an in situ population of intermediate mass stars, or by interstellar gas stripped from the galaxies. The former mode offers a natural explanation for the observed baryon deficiency in the IGM of SQ as well as for the steep L-X-T-X relation of groups such as SQ with lower velocity dispersions. C1 [Natale, G.; Tuffs, R. J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Xu, C. K.; Lu, N.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Popescu, C. C.] Univ Cent Lancashire, Preston PR1 2HE, Lancs, England. [Fischera, J.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Lisenfeld, U.] Univ Granada, Dept Fis Teor & Cosmos, Granada, Spain. [Appleton, P.] CALTECH, NASA, Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA. [Dopita, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Duc, P. -A.] Univ Paris Diderot, Lab AIM, CEA DSM CNRS, CEA Saclay,Dapnia Serv Astrophys, F-91191 Gif Sur Yvette, France. [Gao, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Reach, W.] CALTECH, Spitzer Sci Ctr, IPAC, Pasadena, CA 91125 USA. [Sulentic, J.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Yun, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Natale, G (reprint author), Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany. EM giovanni.natale@mpi-hd.mpg.de; richard.buffs@mpi-hd.mpg.de RI Lisenfeld, Ute/A-1637-2015; Dopita, Michael/P-5413-2014; OI Lisenfeld, Ute/0000-0002-9471-5423; Dopita, Michael/0000-0003-0922-4986; Appleton, Philip/0000-0002-7607-8766; Reach, William/0000-0001-8362-4094 FU International Max-Planck Research School (IMPRS) Heidelberg; NASA FX We thank Pierre Guillard for fruitful discussions on the shock region of SQ, and Francois Boulanger and Fabian Walter for discussions and comments on the manuscript. G.N. acknowledges support from the International Max-Planck Research School (IMPRS) Heidelberg. 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. NR 84 TC 17 Z9 17 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 955 EP 984 DI 10.1088/0004-637X/725/1/955 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700102 ER PT J AU Kim, YS Kaiser, RI AF Kim, Y. S. Kaiser, R. I. TI ABIOTIC FORMATION OF CARBOXYLIC ACIDS (RCOOH) IN INTERSTELLAR AND SOLAR SYSTEM MODEL ICES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; astrochemistry; cosmic rays; ISM: molecules; methods: laboratory; planets and satellites: general ID HOT MOLECULAR CORES; QUADRUPOLE MASS-SPECTROMETRY; ACETIC-ACID; ORGANIC-MOLECULES; CARBONACEOUS METEORITES; ULTRAVIOLET PHOTOLYSIS; INFRARED-SPECTROSCOPY; MONOCARBOXYLIC ACIDS; BEARING MOLECULES; HYDROGEN-PEROXIDE AB The present laboratory study simulated the abiotic formation of carboxylic acids (RCOOH) in interstellar and solar system model ices of carbon dioxide (CO(2))-hydrocarbon mix C(n)H(2n+2) (n = 1-6). The pristine model ices were irradiated at 10 K under contamination-free, ultrahigh vacuum conditions with energetic electrons generated in the track of galactic cosmic-ray particles. The chemical processing of the ices was monitored by a Fourier transform infrared spectrometer and a quadrupole mass spectrometer during the irradiation phase and subsequent warm-up phases on line and in situ in order to extract qualitative (carriers) and quantitative (rate constants and yields) information on the newly synthesized species. Carboxylic acids were identified to be the main carrier, together with carbon monoxide (CO) and a trace of formyl (HCO) and hydroxycarbonyl (HOCO) radicals at 10 K. The upper limit of acid column density at 10 K was estimated as much as (1.2 +/- 0.1) x 10(17) molecules cm(-2) at doses of 17 +/- 2 eV molecule(-1), or the yield of 39% +/- 4% from the initial column density of carbon dioxide. The temporal column density profiles of the products were then numerically fit using two independent kinetic schemes of reaction mechanisms. Finally, we transfer this laboratory simulation to star-forming regions of the interstellar medium, wherein cosmic-ray-induced processing of icy grains at temperatures as low as 10 K could contribute to the current level of chemical complexity as evidenced in astronomical observations and in extracts of carbonaceous meteorites. C1 [Kim, Y. S.; Kaiser, R. I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Kaiser, R. I.] Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA. RP Kim, YS (reprint author), Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. EM ralfk@hawaii.edu FU National Aeronautics Space Administration (NASA) Astrobiology Institute through the Office of Space Science [NNA09DA77 A] FX This work was supported by the National Aeronautics Space Administration (NASA) Astrobiology Institute under Cooperative Agreement No. NNA09DA77 A issued through the Office of Space Science. Special thanks to Dr. C. Ennis (University of Hawaii) for comments on this manuscript. NR 55 TC 8 Z9 8 U1 0 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 1002 EP 1010 DI 10.1088/0004-637X/725/1/1002 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700105 ER PT J AU Vanzella, E Giavalisco, M Inoue, AK Nonino, M Fontanot, F Cristiani, S Grazian, A Dickinson, M Stern, D Tozzi, P Giallongo, E Ferguson, H Spinrad, H Boutsia, K Fontana, A Rosati, P Pentericci, L AF Vanzella, E. Giavalisco, M. Inoue, A. K. Nonino, M. Fontanot, F. Cristiani, S. Grazian, A. Dickinson, M. Stern, D. Tozzi, P. Giallongo, E. Ferguson, H. Spinrad, H. Boutsia, K. Fontana, A. Rosati, P. Pentericci, L. TI THE GREAT OBSERVATORIES ORIGINS DEEP SURVEY: CONSTRAINTS ON THE LYMAN CONTINUUM ESCAPE FRACTION DISTRIBUTION OF LYMAN-BREAK GALAXIES AT 3.4 < z < 4.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation; galaxies: distances and redshifts; galaxies: evolution; galaxies: high-redshift; intergalactic medium ID STAR-FORMING GALAXIES; GOODS-SOUTH FIELD; QUASAR LUMINOSITY FUNCTION; SPACE-TELESCOPE SEARCH; HIGH-REDSHIFT GALAXIES; SIMILAR-TO 3; IONIZING-RADIATION; VLT/FORS2 SPECTROSCOPY; STELLAR POPULATIONS; PHYSICAL-PROPERTIES AB We use ultra-deep ultraviolet VLT/VIMOS intermediate-band and VLT/FORS1 narrowband imaging in the GOODS Southern field to derive limits on the distribution of the escape fraction (f(esc)) of ionizing radiation for L >= L-z=3* Lyman-break galaxies (LBGs) at redshift 3.4-4.5. Only one LBG, at redshift z = 3.795, is detected in its Lyman continuum (LyC; S/N similar or equal to 5.5), the highest redshift galaxy currently known with a direct detection. Its ultraviolet morphology is quite compact (R-eff = 0.8 kpc physical). Three out of seven active galactic nuclei are also detected in their LyC, including one at redshift z = 3.951 and z(850) = 26.1. From stacked data (LBGs), we set an upper limit to the average f(esc) in the range 5%-20%, depending on how the data are selected (e. g., by magnitude and/or redshift). We undertake extensive Monte Carlo simulations that take into account intergalactic attenuation, stellar population synthesis models, dust extinction, and photometric noise in order to explore the moments of the distribution of the escaping radiation. Various distributions (exponential, log-normal, and Gaussian) are explored. We find that the median f(esc) is lower than similar or equal to 6% with an 84% percentile limit not larger than 20%. If this result remains valid for fainter LBGs down to current observational limits, then the LBG population might be not sufficient to account for the entire photoionization budget at the redshifts considered here, with the exact details dependent upon the assumed ionizing background and QSO contribution thereto. It is possible that f(esc) depends on the UV luminosity of the galaxies, with fainter galaxies having higher f(esc), and estimates of f(esc) from a sample of faint LBGs from HUDF (i775 <= 28.5) are in broad quantitative agreement with such a scenario. C1 [Vanzella, E.; Nonino, M.; Fontanot, F.; Cristiani, S.; Tozzi, P.] INAF Trieste Astron Observ, I-40131 Trieste, Italy. [Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Inoue, A. K.] Osaka Sangyo Univ, Coll Gen Educ, Osaka 5748530, Japan. [Grazian, A.; Giallongo, E.; Boutsia, K.; Fontana, A.; Pentericci, L.] INAF Rome Astron Observ, I-00040 Rome, Italy. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ferguson, H.] STScI, Baltimore, MD 21218 USA. [Spinrad, H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Rosati, P.] ESO, D-85748 Garching, Germany. RP Vanzella, E (reprint author), INAF Trieste Astron Observ, Via GB Tiepolo 11, I-40131 Trieste, Italy. OI Nonino, Mario/0000-0001-6342-9662; Cristiani, Stefano/0000-0002-2115-5234; Giallongo, Emanuele/0000-0003-0734-1273; Vanzella, Eros/0000-0002-5057-135X; fontana, adriano/0000-0003-3820-2823 FU ASI/COFIN [I/016/07/0]; PRIN INAF; NASA FX We thank the anonymous referee, whose insightful comments improved the paper. We are grateful to the ESO staff in Paranal and Garching who greatly helped in the development of program. We acknowledge financial contribution from contract ASI/COFIN I/016/07/0 and PRIN INAF 2007 "A Deep VLT and LBT view of the Early Universe." We thank D. Schaerer for useful discussions about the single LBG detection and E. Glikman for the recent estimates of the QSO luminosity function at the faint end at redshift 4. The work of D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 76 TC 75 Z9 75 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 1011 EP 1031 DI 10.1088/0004-637X/725/1/1011 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700106 ER PT J AU Hathaway, DH Williams, PE Dela Rosa, K Cuntz, M AF Hathaway, David H. Williams, Peter E. Dela Rosa, Kevin Cuntz, Manfred TI THE ADVECTION OF SUPERGRANULES BY THE SUN'S AXISYMMETRIC FLOWS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: granulation; Sun: photosphere; Sun: rotation; Sun: surface magnetism ID MICHELSON DOPPLER IMAGER; SPHERICAL HARMONIC-ANALYSIS; STEADY PHOTOSPHERIC FLOWS; WAVE-LIKE PROPERTIES; SOLAR ROTATION; VELOCITY-FIELDS; MERIDIONAL FLOW; DIFFERENTIAL ROTATION; ANGULAR VELOCITY; MAGNETIC-FIELDS AB We show that the motions of supergranules are consistent with a model in which they are simply advected by the axisymmetric flows in the Sun's surface shear layer. We produce a 10 day series of simulated Doppler images at a 15 minute cadence that reproduces most spatial and temporal characteristics seen in the SOHO/MDI Doppler data. Our simulated data have a spectrum of cellular flows with just two components-a granule component that peaks at spherical wavenumbers of about 4000 and a supergranule component that peaks at wavenumbers of about 110. We include the advection of these cellular components by the axisymmetric flows-differential rotation and meridional flow-whose variations with latitude and depth (wavenumber) are consistent with observations. We mimic the evolution of the cellular pattern by introducing random variations to the phases of the spectral components at rates that reproduce the levels of cross-correlation as functions of time and latitude. Our simulated data do not include any wave-like characteristics for the supergranules yet can reproduce the rotation characteristics previously attributed to wave-like behavior. We find rotation rates which appear faster than the actual rotation rates and attribute this to projection effects. We find that the measured meridional flow does accurately represent the actual flow and that the observations indicate poleward flow to 65 degrees-70 degrees latitude with equatorward countercells in the polar regions. C1 [Hathaway, David H.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Williams, Peter E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dela Rosa, Kevin] Carnegie Mellon Univ, Sch Comp Sci, Pittsburgh, PA 15213 USA. [Cuntz, Manfred] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM david.hathaway@nasa.gov; peter.williams@nasa.gov; cuntz@uta.edu FU NASA FX We thank NASA for its support of this research through a grant from the Heliophysics Guest Investigator Program to NASA Marshall Space Flight Center; SOHO, which is a project of international cooperation between ESA and NASA; John Beck, who prepared the 31 minute filtered SOHO/MDI data used in this paper; and an anonymous referee whose comments led to significant improvements in both content and presentation. NR 48 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 1082 EP 1090 DI 10.1088/0004-637X/725/1/1082 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700111 ER PT J AU Greene, TP Barsony, M Weintraub, DA AF Greene, Thomas P. Barsony, Mary Weintraub, David A. TI NEAR-IR H-2 EMISSION OF PROTOSTARS: PROBING CIRCUMSTELLAR ENVIRONMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; ISM: jets and outflows; stars: formation; stars: pre-main sequence; techniques: spectroscopic ID T-TAURI STARS; YOUNG STELLAR OBJECTS; MOLECULAR-HYDROGEN EMISSION; SPECTRAL ENERGY-DISTRIBUTIONS; HIGH-RESOLUTION SPECTROSCOPY; RHO-OPHIUCHI CLOUD; PROTOPLANETARY DISKS; II EMISSION; EVOLUTIONARY STATUS; INFRARED RESPONSE AB We present new observations of near-infrared molecular hydrogen (H-2) line emission in a sample of 18 Class I and flat-spectrum low-mass protostars, primarily in the Tau-Aur and rho Oph dark clouds. The line emission is extended by up to several arcseconds (several hundred AU) for most objects, and there is little night-to-night variation in line strength coincident with the continuum point source. Flux ratios of H-2 nu = 2-1 S(1) and nu = 1-0 S(1) lines are consistent with this emission arising in jets or winds in many objects. However, most objects have only small offsets (under 10 km s(-1)) between their H-2 and photospheric radial velocities. No objects have line ratios which are clearly caused solely by UV excitation, but the H-2 emission of several objects may be caused by UV or X-ray excitation in the presence of circumstellar dust. There are several objects in the sample whose observed velocities and line fluxes suggest quiescent, non-mechanical origins for their molecular hydrogen emissions. Overall, we find the H-2 emission properties of these protostars to be similar to the T Tauri stars studied in previous surveys. C1 [Greene, Thomas P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barsony, Mary] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Barsony, Mary] Space Sci Inst, Boulder, CO 80301 USA. [Weintraub, David A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. RP Greene, TP (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM tom.greene@nasa.gov; mbarsony@SpaceScience.org; david.a.weintraub@vanderbilt.edu FU W. M. Keck Foundation; NASA [WBS 811073.02.07.01.89] FX The data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.; We thank D. Hollenbach and U. Gorti for helpful discussions of our data and their interpretation via theoretical models. We also thank G. Herczeg for discussing pre-publication data and thank the anonymous referee for thoughtful suggestions that improved this paper. The Keck Observatory Observing Assistants H. Hershley and C. Parker are gratefully acknowledged for assistance with the observations. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. T.P.G. acknowledges support from NASA's Origins of Solar Systems program via WBS 811073.02.07.01.89. M.B. and T.P.G. acknowledge NASA support via NExScI for travel expenses to the W. M. Keck Observatory for acquiring the observations for this project. NR 72 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 1100 EP 1110 DI 10.1088/0004-637X/725/1/1100 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700113 ER PT J AU Stothers, RB AF Stothers, Richard B. TI GIANT CONVECTION CELL TURNOVER AS AN EXPLANATION OF THE LONG SECONDARY PERIODS IN SEMIREGULAR RED VARIABLE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE convection; stars: interiors; stars: late-type; stars: oscillations; stars: variables: general ID TURBULENT COMPRESSIBLE CONVECTION; MIXING-LENGTH THEORY; ALPHA-ORIONIS; EFFECTIVE TEMPERATURES; SOLAR SUPERGRANULATION; VELOCITY VARIATIONS; STELLAR ENVELOPES; SUPERGIANT STARS; RADIAL-VELOCITY; BRANCH STARS AB Giant convection cells in the envelopes of massive red supergiants turn over in a time comparable in order of magnitude with the observed long secondary periods in these stars, according to a theory proposed some years ago by Stothers & Leung. This idea is developed further here by using improved theoretical data, especially a more accurate convective mixing length and a simple calculation of the expected radial-velocity variations at the stellar surface. The theory is applied to the two best-observed red supergiants, Betelgeuse and Antares, with more success than in the earlier study. The theory can also explain the long secondary periods seen in the low-mass red giants, thus providing a uniform and coherent picture for all of the semiregular red variables. How the turnover of a giant convection cell might account for the observed slow light and radial-velocity variations, their relative phasing, and the absence of these variations in certain stars is discussed here in a qualitative way, but follows naturally from the theory. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Stothers, RB (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. NR 92 TC 21 Z9 21 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 1170 EP 1174 DI 10.1088/0004-637X/725/1/1170 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700012 ER PT J AU Monnier, JD Townsend, RHD Che, X Zhao, M Kallinger, T Matthews, J Moffat, AFJ AF Monnier, J. D. Townsend, R. H. D. Che, X. Zhao, M. Kallinger, T. Matthews, J. Moffat, A. F. J. TI ROTATIONALLY MODULATED g-MODES IN THE RAPIDLY ROTATING delta SCUTI STAR RASALHAGUE (alpha OPHIUCHI) SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: individual: alpha Oph, Rasalhague; stars: variables: delta Scuti; techniques: photometric ID Y-2 ISOCHRONES; A-TYPE; ANGULAR-DEPENDENCE; EPSILON-OPHIUCHI; MAIN-SEQUENCE; CHARA ARRAY; F-TYPE; PHOTOMETRY; OSCILLATIONS; SPACE AB Despite a century of remarkable progress in understanding stellar interiors, we know surprisingly little about the inner workings of stars spinning near their critical limit. New interferometric imaging of these so-called rapid rotators combined with breakthroughs in asteroseismology promise to lift this veil and probe the strongly latitude-dependent photospheric characteristics and even reveal the internal angular momentum distribution of these luminous objects. Here, we report the first high-precision photometry on the low-amplitude delta Scuti variable star Rasalhague (alpha Oph, A5IV, 2.18 M-circle dot, omega/omega(c) similar to 0.88) based on 30 continuous days of monitoring using the MOST satellite. We have identified 57 +/- 1 distinct pulsation modes above a stochastic granulation spectrum with a cutoff of similar to 26 cycles day(-1). Remarkably, we have also discovered that the fast rotation period of 14.5 hr modulates low-frequency modes (1-10 day periods) that we identify as a rich family of g-modes (broken vertical bar m broken vertical bar up to 7). The spacing of the g-modes is surprisingly linear considering Coriolis forces are expected to strongly distort the mode spectrum, suggesting we are seeing prograde "equatorial Kelvin" waves (modes l = m). We emphasize the unique aspects of Rasalhague motivating future detailed asteroseismic modeling-a source with a precisely measured parallax distance, photospheric oblateness, latitude temperature structure, and whose low-mass companion provides an astrometric orbit for precise mass determinations. C1 [Monnier, J. D.; Che, X.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Townsend, R. H. D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Zhao, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kallinger, T.; Matthews, J.] Univ British Columbia, Vancouver, BC V6T 1Z1, Canada. [Moffat, A. F. J.] Univ Montreal, Montreal, PQ H3C 3J7, Canada. RP Monnier, JD (reprint author), Univ Michigan, Dept Astron, 941 Dennison Bldg, Ann Arbor, MI 48109 USA. EM monnier@umich.edu OI Kallinger, Thomas/0000-0003-3627-2561 FU Canadian Space Agency; Austrian Science Fund; NSERC (Canada); FQRNT (Quebec); NASA [NNX09AH29G]; NSF [AST-0707927] FX We thank C. Matzner for discussion and insights. T. K. is supported by the Canadian Space Agency and the Austrian Science Fund. A.F.J.M. is grateful for financial aid from NSERC (Canada) and FQRNT (Quebec). We acknowledge support from the NASA MOST guest observer program NNX09AH29G and NSF AST-0707927. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System (ADS) Bibliographic Services. NR 49 TC 21 Z9 21 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 DEC PY 2010 VL 725 IS 1 BP 1192 EP 1201 DI 10.1088/0004-637X/725/1/1192 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700014 ER PT J AU Siegel, MH Hoversten, EA Roming, PWA Landsman, WB Prieto, CA Breeveld, AA Brown, P Holland, ST Kuin, NPM Page, MJ Berk, DEV AF Siegel, Michael H. Hoversten, Erik A. Roming, Peter W. A. Landsman, Wayne B. Prieto, Carlos Allende Breeveld, Alice A. Brown, Peter Holland, Stephen T. Kuin, N. P. M. Page, Mathew J. Berk, Daniel E. Vanden TI FAINT NEAR-ULTRAVIOLET/FAR-ULTRAVIOLET STANDARDS FROM SWIFT/UVOT, GALEX, AND SDSS PHOTOMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE techniques: photometric; ultraviolet: general; ultraviolet: stars; white dwarfs ID DIGITAL SKY SURVEY; DA WHITE-DWARFS; SPECTROPHOTOMETRIC STANDARDS; FAR-ULTRAVIOLET; DATA RELEASE; TELESCOPE; CALIBRATION; CATALOG; STARS; DUST AB At present, the precision of deep ultraviolet photometry is somewhat limited by the dearth of faint ultraviolet standard stars. In an effort to improve this situation, we present a uniform catalog of 11 new faint (u similar to 17) ultraviolet standard stars. High-precision photometry of these stars has been taken from the Sloan Digital Sky Survey and Galaxy Evolution Explorer archives and combined with new data from the Swift Ultraviolet Optical Telescope to provide precise photometric measures extending from the near-infrared to the far-ultraviolet. These stars were chosen because they are known to be hot (20,000 < T-eff < 50,000 K) DA white dwarfs with published Sloan spectra that should be photometrically stable. This careful selection allows us to compare the combined photometry and Sloan spectroscopy to models of pure hydrogen atmospheres to both constrain the underlying properties of the white dwarfs and test the ability of white dwarf models to predict the photometric measures. We find that the photometry provides good constraints on white dwarf temperatures, which demonstrates the ability of Swift/UVOT to investigate the properties of hot luminous stars. We further find that the models reproduce the photometric measures in all 11 passbands to within their systematic uncertainties. Within the limits of our photometry, we find the standard stars to be photometrically stable. This success indicates that the models can be used to calibrate additional filters to our standard system, permitting easier comparison of photometry from heterogeneous sources. The largest source of uncertainty in the model fitting is the uncertainty in the foreground reddening curve, a problem that is especially acute in the UV. C1 [Siegel, Michael H.; Hoversten, Erik A.; Roming, Peter W. A.; Brown, Peter] Penn State Univ, Dept Astron, University Pk, PA 16802 USA. [Landsman, Wayne B.; Holland, Stephen T.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Prieto, Carlos Allende; Breeveld, Alice A.; Kuin, N. P. M.; Page, Mathew J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Berk, Daniel E. Vanden] St Vincent Coll, Dept Phys, Latrobe, PA 15650 USA. RP Siegel, MH (reprint author), Penn State Univ, Dept Astron, 525 Davey Lab, University Pk, PA 16802 USA. EM siegel@astro.psu.edu; hoversten@astro.psu.edu; roming@astro.psu.edu; wayne.b.landsman@nasa.gov; cap@mssl.ucl.ac.uk; aab@mssl.ucl.ac.uk; brown@astro.psu.edu; Stephen.T.Holland@nasa.gov; npmk@mssl.ucl.ac.uk; mjp@mssl.ucl.ac.uk; daniel.vandenberk@email.stvincent.edu FU GALEX [NNX08AK62G]; NASA [NAS5-00136] FX The authors acknowledge support in the form of GALEX grant NNX08AK62G and sponsorship at PSU by NASA contract NAS5-00136. We thank I. Hubeny for assistance with the TLUSTY software and the anonymous referee for useful comments. NR 39 TC 4 Z9 5 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 1215 EP 1225 DI 10.1088/0004-637X/725/1/1215 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700016 ER PT J AU Steffen, JH Batalha, NM Borucki, WJ Buchhave, LA Caldwell, DA Cochran, WD Endl, M Fabrycky, DC Fressin, F Ford, EB Fortney, JJ Haas, MJ Holman, MJ Howell, SB Isaacson, H Jenkins, JM Koch, D Latham, DW Lissauer, JJ Moorhead, AV Morehead, RC Marcy, G MacQueen, PJ Quinn, SN Ragozzine, D Rowe, JF Sasselov, DD Seager, S Torres, G Welsh, WF AF Steffen, Jason H. Batalha, Natalie M. Borucki, William J. Buchhave, Lars A. Caldwell, Douglas A. Cochran, William D. Endl, Michael Fabrycky, Daniel C. Fressin, Francois Ford, Eric B. Fortney, Jonathan J. Haas, Michael J. Holman, Matthew J. Howell, Steve B. Isaacson, Howard Jenkins, Jon M. Koch, David Latham, David W. Lissauer, Jack J. Moorhead, Althea V. Morehead, Robert C. Marcy, Geoffrey MacQueen, Phillip J. Quinn, Samuel N. Ragozzine, Darin Rowe, Jason F. Sasselov, Dimitar D. Seager, Sara Torres, Guillermo Welsh, William F. TI FIVE KEPLER TARGET STARS THAT SHOW MULTIPLE TRANSITING EXOPLANET CANDIDATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (KIC 8394721, KIC 5972334, KIC 10723750, KIC 7287995, KIC 7825899); techniques: photometric; techniques: spectroscopic ID EXTRASOLAR PLANETARY SYSTEMS; MASS-RADIUS RELATIONSHIPS; TIMING VARIATIONS; SUPER-EARTHS; TERRESTRIAL PLANETS; SOLID EXOPLANETS; GIANT IMPACTS; DETECTABILITY; ECCENTRICITY; CONSTRAINTS AB We present and discuss five candidate exoplanetary systems identified with the Kepler spacecraft. These five systems show transits from multiple exoplanet candidates. Should these objects prove to be planetary in nature, then these five systems open new opportunities for the field of exoplanets and provide new insights into the formation and dynamical evolution of planetary systems. We discuss the methods used to identify multiple transiting objects from the Kepler photometry as well as the false-positive rejection methods that have been applied to these data. One system shows transits from three distinct objects while the remaining four systems show transits from two objects. Three systems have planet candidates that are near mean motion commensurabilities-two near 2:1 and one just outside 5:2. We discuss the implications that multi-transiting systems have on the distribution of orbital inclinations in planetary systems, and hence their dynamical histories, as well as their likely masses and chemical compositions. A Monte Carlo study indicates that, with additional data, most of these systems should exhibit detectable transit timing variations (TTVs) due to gravitational interactions, though none are apparent in these data. We also discuss new challenges that arise in TTV analyses due to the presence of more than two planets in a system. C1 [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Borucki, William J.; Caldwell, Douglas A.; Haas, Michael J.; Jenkins, Jon M.; Koch, David; Lissauer, Jack J.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Buchhave, Lars A.; Fabrycky, Daniel C.; Fressin, Francois; Holman, Matthew J.; Latham, David W.; Quinn, Samuel N.; Ragozzine, Darin; Sasselov, Dimitar D.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Caldwell, Douglas A.; Jenkins, Jon M.] SETI Inst, Mountain View, CA 94043 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Ford, Eric B.; Moorhead, Althea V.; Morehead, Robert C.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Isaacson, Howard; Marcy, Geoffrey] Univ Calif Berkeley, Dept Astron, Berkeley, CA USA. [Seager, Sara] MIT, Dept Phys, Cambridge, MA 02139 USA. [Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA. RP Steffen, JH (reprint author), Fermilab Ctr Particle Astrophys, POB 500, Batavia, IL 60510 USA. RI Steffen, Jason/A-4320-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU National Science Foundation FX IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. NR 57 TC 50 Z9 51 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 1 BP 1226 EP 1241 DI 10.1088/0004-637X/725/1/1226 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700017 ER PT J AU Burlaga, LF Ness, NF AF Burlaga, L. F. Ness, N. F. TI SECTORS AND LARGE-SCALE MAGNETIC FIELD STRENGTH FLUCTUATIONS IN THE HELIOSHEATH NEAR 110 AU: VOYAGER 1, 2009 SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: heliosphere ID TERMINATION SHOCK; SOLAR-WIND; DISTANT HELIOSPHERE; 3-DIMENSIONAL FEATURES; MULTIFRACTAL STRUCTURE; STATISTICAL-MECHANICS; VELOCITY FLUCTUATION; TSALLIS STATISTICS; OUTER HELIOSPHERE; NEUTRAL HYDROGEN AB This paper describes observations of daily averages of the magnetic field strength B and the magnetic polarity measured by Voyager 1 (V1) in the heliosheath during 2009 between 108.5 and 112.1 AU and at heliographic latitude 34 degrees.4. A negative magnetic polarity sector was observed during 2009 DOY 43-255. A positive polarity sector was observed during 2009 DOY 256-365. We offer the hypothesis that the existence of the two sectors is the result of the displacement of the wavy heliospheric current sheet to the position of V1 as a result of northward flow in the heliosheath. The large size of the sectors is caused by the slow radial motion of the flow observed by V1 in the heliosheath. The distribution of B during 2009 was lognormal, in contrast to the Gaussian distributions observed by V1 in the heliosheath prior to 2009. The large-scale fluctuations of B, described by the distribution of increments of daily averages of B, have a Tsallis distribution with q = 1.6. The large-scale fluctuations of B observed by V1 during 2009 have a multifractal spectrum with the same parameters that V1 observed during 2005 close to the termination shock at 94 AU. These results suggest that the large-scale magnetic fluctuations of B are in a metastable equilibrium state in the heliosheath between 94 AU and 112.1 AU. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA. EM lburlagahsp@verizon.net; nfnudel@yahoo.com FU NASA [NNX07AW09G, NNX09AT41G] FX T. McClanahan and S. Kramer provided support in the processing of the data. Daniel Berdichevsky computed the zero level offsets for the instrument for the data. N. F. Ness was partially supported by NASA Grants NNX07AW09G and NNX09AT41G to CUA. NR 62 TC 31 Z9 31 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 DEC PY 2010 VL 725 IS 1 BP 1306 EP 1316 DI 10.1088/0004-637X/725/1/1306 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 684UN UT WOS:000284576700023 ER PT J AU Cannizzo, JK Still, MD Howell, SB Wood, MA Smale, AP AF Cannizzo, J. K. Still, M. D. Howell, S. B. Wood, M. A. Smale, A. P. TI THE KEPLER LIGHT CURVE OF V344 Lyrae: CONSTRAINING THE THERMAL-VISCOUS LIMIT CYCLE INSTABILITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars: dwarf novae; stars: individual (V344 Lyr); white dwarfs ID DWARF-NOVA OUTBURSTS; ENHANCED MASS-TRANSFER; SU UMA-TYPE; PARTICLE HYDRODYNAMICS SIMULATIONS; DRIVEN ECCENTRIC INSTABILITIES; FINE MESH CALCULATIONS; CLOSE BINARY-SYSTEMS; URSAE MAJORIS STARS; LONG-TERM BEHAVIOR; ACCRETION DISKS AB We present time-dependent modeling based on the accretion disk limit cycle model for a 270 d light curve of the short-period SU UMa-type dwarf nova V344 Lyr taken by Kepler. The unprecedented precision and cadence (1 minute) far surpass that generally available for long-term light curves. The data encompass two superoutbursts and 17 normal (i.e., short) outbursts. The main decay of the superoutbursts is nearly perfectly exponential, decaying at a rate similar to 12 d mag(-1), while the much more rapid decays of the normal outbursts exhibit a faster-than-exponential shape. Our modeling using the basic accretion disk limit cycle can produce the main features of the V344 Lyr light curve, including the peak outburst brightness. Nevertheless, there are obvious deficiencies in our model light curves. (1) The rise times we calculate, both for the normal and superoutbursts, are too fast. (2) The superoutbursts are too short. (3) The shoulders on the rise to superoutburst have more structure than the shoulders in the observed superoutbursts and are too slow, comprising about a third to half of the total viscous plateau, rather than the similar to 10% observed. However, one of the <-> alpha(hot). ahot interpolation schemes we investigate (one that is physically motivated) does yield longer superoutbursts with suitably short, less structured shoulders. C1 [Cannizzo, J. K.] Univ Maryland, CRESST Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Cannizzo, J. K.; Smale, A. P.] NASA, Astroparticle Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Still, M. D.] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA. [Still, M. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Howell, S. B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Wood, M. A.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. RP Cannizzo, JK (reprint author), Univ Maryland, CRESST Joint Ctr Astrophys, Baltimore, MD 21250 USA. EM John.K.Cannizzo@nasa.gov; Martin.D.Still@nasa.gov NR 89 TC 36 Z9 36 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 2 BP 1393 EP 1404 DI 10.1088/0004-637X/725/2/1393 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300001 ER PT J AU Burgasser, AJ Simcoe, RA Bochanski, JJ Saumon, D Mamajek, EE Cushing, MC Marley, MS McMurtry, C Pipher, JL Forrest, WJ AF Burgasser, Adam J. Simcoe, Robert A. Bochanski, John J. Saumon, Didier Mamajek, Eric E. Cushing, Michael C. Marley, Mark S. McMurtry, Craig Pipher, Judith L. Forrest, William J. TI CLOUDS IN THE COLDEST BROWN DWARFS: FIRE SPECTROSCOPY OF ROSS 458C SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; planetary systems; stars: fundamental parameters; stars: individual (Ross 458C, ULAS J130041.72+122114.7, ULAS J133553.45+113005.2, SDSS J141624.08+134826.7B, ULAS J141623.94+134836.3); stars: low-mass ID LATE-TYPE STARS; NEAR-INFRARED SPECTRA; DIGITAL SKY SURVEY; LOW-MASS STARS; SPITZER-SPACE-TELESCOPE; COMMON PROPER MOTION; MAIN-SEQUENCE STARS; YOUNG MOVING GROUPS; X-RAY-EMISSION; FIELD L-DWARFS AB Condensate clouds are a salient feature of L dwarf atmospheres, but have been assumed to play little role in shaping the spectra of the coldest T-type brown dwarfs. Here we report evidence of condensate opacity in the near-infrared spectrum of the brown dwarf candidate Ross 458C, obtained with the Folded-Port Infrared Echellette (FIRE) spectrograph at the Magellan Telescopes. These data verify the low-temperature nature of this source, indicating a T8 spectral classification, log(10) L-bol/L-circle dot = -5.62 +/- 0.03, T-eff = 650 +/- 25 K, and a mass at or below the deuterium burning limit. The data also reveal enhanced emission at the K band associated with youth (low surface gravity) and supersolar metallicity, reflecting the properties of the Ross 458 system (age = 150-800 Myr, [Fe/H] = +0.2 to +0.3). We present fits of FIRE data for Ross 458C, the T9 dwarf ULAS J133553.45+113005.2, and the blue T7.5 dwarf SDSS J141624.08+134826.7B, to cloudless and cloudy spectral models from Saumon & Marley. For Ross 458C, we confirm a low surface gravity and supersolar metallicity, while the temperature differs depending on the presence (635(-35)(+25) K) or absence (760(-45)(+70) K) of cloud extinction. ULAS J1335+1130 and SDSS J1416+1348B have similar temperatures (595(-45)(+25) K), but distinct surface gravities (log g = 4.0-4.5 cgs versus 5.0-5.5 cgs) and metallicities ([M/H] approximate to +0.2 versus -0.2). In all three cases, cloudy models provide better fits to the spectral data, significantly so for Ross 458C. These results indicate that clouds are an important opacity source in the spectra of young cold T dwarfs and should be considered when characterizing planetary-mass objects in young clusters and directly imaged exoplanets. The characteristics of Ross 458C suggest that it could itself be regarded as a planet, albeit one whose cosmogony does not conform with current planet formation theories. C1 [Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Burgasser, Adam J.; Simcoe, Robert A.; Bochanski, John J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Mamajek, Eric E.; McMurtry, Craig; Pipher, Judith L.; Forrest, William J.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Cushing, Michael C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Burgasser, AJ (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. EM aburgasser@ucsd.edu RI Marley, Mark/I-4704-2013; OI Marley, Mark/0000-0002-5251-2943 FU NASA through the Spitzer Science Center FX The authors also thank B. Burningham and S. Leggett for providing their spectral data of ULAS J1335+1130, and J. D. Kirkpatrick for providing his spectrum of Ross 458AB used in the analysis. Support for the modeling work of D. S. was provided by NASA through the Spitzer Science Center. This research has benefited from the M, L, and T dwarf compendium housed at DwarfArchives.org and maintained by Chris Gelino, Davy Kirkpatrick, and Adam Burgasser. NR 163 TC 60 Z9 60 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 2 BP 1405 EP 1420 DI 10.1088/0004-637X/725/2/1405 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300002 ER PT J AU Corcoran, MF Hamaguchi, K Pittard, JM Russell, CMP Owocki, SP Parkin, ER Okazaki, A AF Corcoran, M. F. Hamaguchi, K. Pittard, J. M. Russell, C. M. P. Owocki, S. P. Parkin, E. R. Okazaki, A. TI RECENT X-RAY VARIABILITY OF eta CARINAE: THE QUICK ROAD TO RECOVERY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; stars: early-type; stars: individual (Eta Carinae); X-rays: stars ID SPECTROSCOPIC EVENT; WIND COLLISION; STELLAR WIND; LIGHT-CURVE; ACCRETION; PARAMETERS; COMPANION; MINIMUM; CYCLE; MASS AB We report continued monitoring of the superluminous binary system eta Car by the Proportional Counter Array on the Rossi X-ray Timing Observatory (RXTE) through the 2009 X-ray minimum. The RXTE campaign shows that the minimum began on 2009 January 16, consistent with the phasings of the two previous minima, and overall, the temporal behavior of the X-ray emission was similar to that observed by RXTE in the previous two cycles. However, important differences did occur. The 2-10 keV X-ray flux and X-ray hardness decreased in the 2.5 year interval leading up to the 2009 minimum compared to the previous cycle. Most intriguingly, the 2009 X-ray minimum was about 1 month shorter than either of the previous two minima. During the egress from the 2009 minimum the X-ray hardness increased markedly as it had during egress from the previous two minima, although the maximum X-ray hardness achieved was less than the maximum observed after the two previous recoveries. We suggest that the cycle-to-cycle variations, especially the unexpectedly early recovery from the 2009 X-ray minimum, might have been the result of a decline in eta Car's wind momentum flux produced by a drop in eta Car's mass loss rate or wind terminal velocity (or some combination), though if so the change in wind momentum flux required to match the X-ray variation is surprisingly large. C1 [Corcoran, M. F.; Hamaguchi, K.] CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.; Hamaguchi, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Hamaguchi, K.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Pittard, J. M.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Russell, C. M. P.; Owocki, S. P.] Univ Delaware, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 USA. [Parkin, E. R.] Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium. [Okazaki, A.] Hokkai Gakuen Univ, Fac Engn, Toyohira Ku, Sapporo, Hokkaido 0628605, Japan. RP Corcoran, MF (reprint author), CRESST, Greenbelt, MD 20771 USA. FU NASA [NNG06EO90A]; [GO0-11039A]; [G07-8022A]; [G09-0016A]; [G08-9018A] FX We thank the referee for helpful comments that substantially improved the paper, and Ted Gull for many useful and enjoyable discussions. We gratefully acknowledge the superlative assistance by the RXTE Guest Observer Facility and Science Operations Facility, the Chandra X-ray Center, and the XMM-Newton Guest Observer Facility. The Chandra observations have been supported by grants GO0-11039A, G07-8022A, G09-0016A, and G08-9018A. This support is gratefully acknowledged. This work has also been supported in part by NASA Cooperative Agreement NNG06EO90A. This research has made use of NASA's Astrophysics Data System Bibliographic Services, an indispensable tool. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center, also an indispensable resource for the high energy astrophysicist. NR 30 TC 43 Z9 43 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 DEC PY 2010 VL 725 IS 2 BP 1528 EP 1535 DI 10.1088/0004-637X/725/2/1528 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300013 ER PT J AU Cluver, ME Jarrett, TH Kraan-Korteweg, RC Koribalski, BS Appleton, PN Melbourne, J Emonts, B Woudt, PA AF Cluver, M. E. Jarrett, T. H. Kraan-Korteweg, R. C. Koribalski, B. S. Appleton, P. N. Melbourne, J. Emonts, B. Woudt, P. A. TI ACTIVE DISK BUILDING IN A LOCAL H I-MASSIVE LIRG: THE SYNERGY BETWEEN GAS, DUST, AND STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (HIZOA J0836-43); galaxies: starburst; infrared: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; SURFACE BRIGHTNESS GALAXIES; MOLECULAR GAS; NEARBY GALAXIES; FORMING GALAXIES; INTERSTELLAR-MEDIUM; STARBURST GALAXIES; LUMINOUS GALAXIES AB HIZOA J0836-43 is the most Hi-massive (M-HI = 7.5 x 10(10) M-circle dot) galaxy detected in the HIPASS volume (delta = -90 degrees to + 25 degrees, nu < 12,700 km s(-1)) and lies optically hidden behind the Milky Way. Markedly different from other extreme Hi disks in the local universe, it is a luminous infrared galaxy (LIRG) with an actively star-forming disk (>50 kpc), central to its similar to 130 kpc gas disk, with a total star formation rate (SFR) of similar to 20.5 M-circle dot yr(-1). Spitzer spectroscopy reveals an unusual combination of powerful polycyclic aromatic hydrocarbon (PAH) emission coupled to a relatively weak warm dust continuum, suggesting photodissociation-region-dominated emission. Compared to a typical LIRG with similar total infrared luminosity (L-TIR = 10(11) L-circle dot), the PAHs in HIZOA J0836-43 are more than twice as strong, whereas the warm dust continuum (lambda > 20 mu m) is best fit by a star-forming galaxy with L-TIR = 10(10) L-circle dot. Mopra CO observations suggest an extended molecular gas component (H-2+He > 3.7x10(9) M-circle dot) and a lower limit of similar to 64% for the gas-mass fraction; this is above average compared to local disk systems, but similar to that of z similar to 1.5 BzK galaxies (similar to 57%). However, the star formation efficiency (SFE = L-TR/L-CO(')) for HIZOA J0836-43 of 140 L-circle dot (K km s(-1) pc(2))(-1) is similar to that of local spirals and other disk galaxies at high redshift, in strong contrast to the increased SFE seen in merging and strongly interacting systems. HIZOA J0836-43 is actively forming stars and building a massive stellar disk. Its evolutionary phase of star formation (M-stellar, SFR, and gas fraction) compared to more distant systems suggests that it would be considered typical at redshift z similar to 1. This galaxy provides a rare opportunity in the nearby universe for studying (at z similar to 0.036) how disks were building and galaxies evolving at z similar to 1, when similarly large gas fractions were likely more common. C1 [Cluver, M. E.; Jarrett, T. H.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Cluver, M. E.; Kraan-Korteweg, R. C.; Woudt, P. A.] Univ Cape Town, Dept Astron, Ctr Astrophys Cosmol & Grav, ZA-7700 Rondebosch, South Africa. [Koribalski, B. S.; Emonts, B.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Appleton, P. N.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Melbourne, J.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Cluver, ME (reprint author), CALTECH, IPAC, Pasadena, CA 91125 USA. OI Appleton, Philip/0000-0002-7607-8766; Cluver, Michelle/0000-0002-9871-6490 FU NASA; NRF (South Africa) FX We thank Danny Dale and SINGS, Lee Armus and GOALS for data access. We are grateful to Steve Lord, Ray Norris, Joe Mazzarella, and Justin Howell for valuable discussions and inputs. We thank the ATNF for hosting us (in Epping and Narrabri), and in particular Balt Indermuehle for his input regarding our Mopra observations. Support for this work was provided by NASA through an award issued by JPL/Caltech. M.E.C., R.K.-K., and P.A.W. thank the NRF (South Africa) for financial support. NR 79 TC 12 Z9 12 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 DEC PY 2010 VL 725 IS 2 BP 1550 EP 1562 DI 10.1088/0004-637X/725/2/1550 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300015 ER PT J AU Howell, SB Rowe, JF Sherry, W von Braun, K Ciardi, DR Bryson, ST Feldmeier, JJ Horch, E van Belle, GT AF Howell, Steve B. Rowe, Jason F. Sherry, William von Braun, Kaspar Ciardi, David R. Bryson, Stephen T. Feldmeier, John J. Horch, Elliott van Belle, Gerard T. TI KEPLER OBSERVATIONS OF THREE PRE-LAUNCH EXOPLANET CANDIDATES: DISCOVERY OF TWO ECLIPSING BINARIES AND A NEW EXOPLANET SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; brown dwarfs; planetary systems ID LIGHT CURVES; PLANET; STELLAR AB Three transiting exoplanet candidate stars were discovered in a ground-based photometric survey prior to the launch of NASA's Kepler mission. Kepler observations of them were obtained during Quarter 1 of the Kepler mission. All three stars are faint by radial velocity follow-up standards, so we have examined these candidates with regard to eliminating false positives and providing high confidence exoplanet selection. We present a first attempt to exclude false positives for this set of faint stars without high-resolution radial velocity analysis. This method of exoplanet confirmation will form a large part of the Kepler mission follow-up for Jupiter-sized exoplanet candidates orbiting faint stars. Using the Kepler light curves and pixel data, as well as medium-resolution reconnaissance spectroscopy and speckle imaging, we find that two of our candidates are binary stars. One consists of a late-F star with an early M companion, while the other is a K0 star plus a late M-dwarf/brown dwarf in a 19 day elliptical orbit. The third candidate (BOKS-1) is an r = 15 G8V star hosting a newly discovered exoplanet with a radius of 1.12 R-Jupiter in a 3.9 day orbit. C1 [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Rowe, Jason F.; Bryson, Stephen T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sherry, William] Natl Solar Observ, Tucson, AZ 85719 USA. [von Braun, Kaspar; Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Feldmeier, John J.] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA. [Horch, Elliott] So Connecticut State Univ, New Haven, CT 06515 USA. [van Belle, Gerard T.] European So Observ, D-85478 Garching, Germany. RP Howell, SB (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. OI Ciardi, David/0000-0002-5741-3047; Feldmeier, John/0000-0003-2908-2620 FU National Science Foundation; NASA FX We thank Brandon Tingley for his timely review and very helpful comments on our original manuscript. The authors thank the Kepler Science Office and the Science Operations Center personal, particularly Natalie Batalha, Jon Jenkins, and Tim Brown, for their dedicated effort to themission and for providing us access to the science office data products. The ground-based observations reported herein were obtained at Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. The Kepler Science Team is thanked for their help and support of the mission and its scientific output. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA. NR 27 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 2 BP 1633 EP 1643 DI 10.1088/0004-637X/725/2/1633 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300023 ER PT J AU Fabbiano, G Brassington, NJ Lentati, L Angelini, L Davies, RL Gallagher, J Kalogera, V Kim, DW King, AR Kundu, A Pellegrini, S Richings, AJ Trinchieri, G Zezas, A Zepf, S AF Fabbiano, G. Brassington, N. J. Lentati, L. Angelini, L. Davies, R. L. Gallagher, J. Kalogera, V. Kim, D. -W. King, A. R. Kundu, A. Pellegrini, S. Richings, A. J. Trinchieri, G. Zezas, A. Zepf, S. TI FIELD AND GLOBULAR CLUSTER LOW-MASS X-RAY BINARIES IN NGC 4278 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 4278); X-rays: binaries; X-rays: galaxies ID CHANDRA MONITORING OBSERVATIONS; EARLY-TYPE GALAXIES; BLACK-HOLE; ELLIPTIC GALAXIES; DEEP CHANDRA; H-I; METALLICITY; CONNECTION; DISTANCES; POPULATIONS AB We report a detailed spectral analysis of the population of low-mass X-ray binaries (LMXBs) detected in the elliptical galaxy NGC 4278 with Chandra. Seven luminous sources were studied individually, four in globular clusters (GCs) and three in the stellar field. The range of (0.3-8 keV) L-X for these sources is similar to(3-8) x 10(38) erg s(-1), suggesting that they may be black hole binaries (BHBs). Fitting the data with either single thermal accretion disk or power-law (PO) models results in best-fit temperatures of similar to 0.7-1.7 keV and Gamma similar to 1.2-2.0, consistent with those measured in Galactic BHBs. Comparison of our results with simulations allows us to discriminate between disk and power-law-dominated emission, pointing to spectral/luminosity variability, reminiscent of Galactic BHBs. The BH masses derived from a comparison of our spectral results with the L-X similar to T-in(4) relation of Galactic BHBs are in the 5-15 M-circle dot range, as observed in the Milky Way. The analysis of joint spectra of sources selected in three luminosity ranges (L-X >= 1.5 x 10(38) erg s(-1), 6 x 10(37) erg s(-1) <= L-X < 1.5 x 10(38) erg s(-1), and L-X < 6 x 10(37) erg s(-1)) suggests that while the high-luminosity sources have prominent thermal disk emission components, power-law components are likely to be important in the mid-and low-luminosity spectra. Comparing low-luminosity average spectra, we find a relatively larger N-H in the GC spectrum; we speculate that this may point to either a metallicity effect or to intrinsic physical differences between field and GC accreting binaries. Analysis of average sample properties uncovers a previously unreported L-X-R-G correlation (where R-G is the galactocentric radius) in the GC-LMXB sample, implying richer LMXB populations in more central GCs. No such trend is seen in the field LMXB sample. We can exclude that the GC L-X-R-G correlation is the by-product of a luminosity effect and suggest that it may be related to the presence of more compact GCs at smaller galactocentric radii, fostering more efficient binary formation. C1 [Fabbiano, G.; Brassington, N. J.; Kim, D. -W.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Angelini, L.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Lentati, L.; Richings, A. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Davies, R. L.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [King, A. R.] Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. [Kundu, A.; Zepf, S.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Trinchieri, G.] INAF Osservatorio Astron Brera, I-20212 Milan, Italy. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gfabbiano@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Trinchieri, Ginevra/0000-0002-0227-502X FU Chandra GO [G06-7079A]; NASA [NAS8-39073]; Southampton University; CXC CIAO software; CALDB FX This work was supported by the Chandra GO grant G06-7079A (PI:Fabbiano) and NASA contract NAS8-39073 (CXC). This paper is partly based on work performed by L.L. while visiting CfA as part of a visiting student program sponsored by Southampton University, and these results were included in his Master's thesis presentation. A.J.R. also acknowledges support by the Southampton University CfA visiting program. The data analysis was supported by the CXC CIAO software and CALDB. We have used the NASA NED and ADS facilities and have extracted archival data from the Chandra archives. NR 54 TC 16 Z9 16 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 2 BP 1824 EP 1847 DI 10.1088/0004-637X/725/2/1824 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300039 ER PT J AU Webb, GM Hu, Q Dasgupta, B Roberts, DA Zank, GP AF Webb, G. M. Hu, Q. Dasgupta, B. Roberts, D. A. Zank, G. P. TI ALFVEN SIMPLE WAVES: EULER POTENTIALS AND MAGNETIC HELICITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); solar wind; Sun: magnetic topology; waves ID PLASMA HEAT-CONDUCTIVITY; SOLAR-WIND FLUCTUATIONS; MAGNETOHYDRODYNAMIC TURBULENCE; PARAMETRIC-INSTABILITIES; FINITE-AMPLITUDE; CURRENT SHEET; FIELD LINES; FLUX TUBE; EVOLUTION; TRANSPORT AB The magnetic helicity characteristics of fully nonlinear, multi-dimensional Alfven simple waves are investigated, by using relative helicity formulae and also by using an approach involving poloidal and toroidal decomposition of the magnetic field and magnetic vector potential. Different methods to calculate the magnetic vector potential are used, including the homotopy and Biot-Savart formulae. Two basic Alfven modes are identified: (1) the plane one-dimensional Alfven simple wave given in standard texts, in which the Alfven wave propagates along the z-axis with wave phase phi = k(0)(z - lambda t), where k(0) is the wave number and lambda is the group velocity of the wave and (2) the generalized Barnes simple Alfven wave in which the wave normal n moves in a circle in the xy-plane perpendicular to the mean field, which is directed along the z-axis. The plane Alfven wave (1) is analogous to the slab Alfven mode and the generalized Barnes solution (2) is analogous to the two-dimensional mode in Alfvenic, incompressible turbulence. The helicity characteristics of these two basic Alfven modes are distinct. The helicity characteristics of more general multi-dimensional simple Alfven waves are also investigated. Applications to nonlinear Alfvenic fluctuations and structures observed in the solar wind are discussed. C1 [Webb, G. M.; Hu, Q.; Dasgupta, B.; Zank, G. P.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA. [Roberts, D. A.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA. [Zank, G. P.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. RP Webb, GM (reprint author), Univ Alabama, CSPAR, Huntsville, AL 35805 USA. EM gary.webb@uah.edu RI Roberts, Dana/D-4625-2012 FU NASA [NN05GG83G, NNX07AO73G, NNX08AH46G]; NSF [ATM-03-17509, ATM-04-28880] FX G.M.W. and G.P.Z. were supported in part by NASA grants NN05GG83G and NSF grant Nos. ATM-03-17509 and ATM-04-28880. Q.H., B.D., and G.M.W. were supported in part by NASA grants NNX07AO73G and NNX08AH46G. NR 86 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC PY 2010 VL 725 IS 2 BP 2128 EP 2151 DI 10.1088/0004-637X/725/2/2128 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 697GN UT WOS:000285501300063 ER PT J AU Wahhaj, Z Cieza, L Koerner, DW Stapelfeldt, KR Padgett, DL Case, A Keller, JR Merin, B Evans, NJ Harvey, P Sargent, A van Dishoeck, EF Allen, L Blake, G Brooke, T Chapman, N Mundy, L Myers, PC AF Wahhaj, Zahed Cieza, Lucas Koerner, David W. Stapelfeldt, Karl R. Padgett, Deborah L. Case, April Keller, James R. Merin, Bruno Evans, Neal J., II Harvey, Paul Sargent, Anneila van Dishoeck, Ewine F. Allen, Lori Blake, Geoff Brooke, Tim Chapman, Nicholas Mundy, Lee Myers, Philip C. TI THE SPITZER c2d SURVEY OF WEAK-LINE T TAURI STARS. III. THE TRANSITION FROM PRIMORDIAL DISKS TO DEBRIS DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; planetary systems; protoplanetary disks; stars: pre-main sequence ID MAIN-SEQUENCE STARS; HIGH-RESOLUTION SPECTROSCOPY; TERRESTRIAL PLANET FORMATION; CENTAURUS OB ASSOCIATION; HUBBLE-SPACE-TELESCOPE; SUN-LIKE STARS; LOW-MASS STARS; BINARY-SYSTEMS; CIRCUMSTELLAR DISKS; INTERSTELLAR CLOUDS AB We present 3.6 to 70 mu m Spitzer photometry of 154 weak-line T Tauri stars (WTTSs) in the Chamaeleon, Lupus, Ophiuchus, and Taurus star formation regions, all of which are within 200 pc of the Sun. For a comparative study, we also include 33 classical T Tauri stars which are located in the same star-forming regions. Spitzer sensitivities allow us to robustly detect the photosphere in the IRAC bands (3.6 to 8 mu m) and the 24 mu m MIPS band. In the 70 mu m MIPS band, we are able to detect dust emission brighter than roughly 40 times the photosphere. These observations represent the most sensitive WTTSs survey in the mid-to far-infrared to date and reveal the frequency of outer disks (r = 3-50 AU) around WTTSs. The 70 mu m photometry for half the c2d WTTSs sample (the on-cloud objects), which were not included in the earlier papers in this series, those of Padgett et al. and Cieza et al., are presented here for the first time. We find a disk frequency of 19% for on-cloud WTTSs, but just 5% for off-cloud WTTSs, similar to the value reported in the earlier works. WTTSs exhibit spectral energy distributions that are quite diverse, spanning the range from optically thick to optically thin disks. Most disks become more tenuous than L(disk)/L(*) = 2 x 10(-3) in 2 Myr and more tenuous than L(disk)/L(*) = 5 x 10(-4) in 4 Myr. C1 [Wahhaj, Zahed; Cieza, Lucas] Univ Hawaii, Inst Astron, Honolulu, HI 96814 USA. [Koerner, David W.; Case, April] No Arizona Univ, Flagstaff, AZ 86011 USA. [Stapelfeldt, Karl R.; Chapman, Nicholas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Padgett, Deborah L.; Brooke, Tim] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Keller, James R.] Oregon State Univ, Dept Phys, Corvallis, OR 97331 USA. [Merin, Bruno] European Space Astron Ctr ESA, Herschel Sci Ctr, Villanueva De La Canada 28691, Madrid, Spain. [Evans, Neal J., II; Harvey, Paul] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Sargent, Anneila] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [van Dishoeck, Ewine F.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Allen, Lori] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Blake, Geoff] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Mundy, Lee] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Wahhaj, Z (reprint author), Univ Hawaii, Inst Astron, Honolulu, HI 96814 USA. RI Stapelfeldt, Karl/D-2721-2012; OI Merin, Bruno/0000-0002-8555-3012 FU NASA [1224608, 1230782, 1230799, 1407]; National Science Foundation FX Support for this work, which is part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608, 1230782, and 1230799 issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center funded by NASA and the National Science Foundation. We also acknowledge use of the SIMBAD database. NR 97 TC 33 Z9 33 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 835 EP 854 DI 10.1088/0004-637X/724/2/835 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000002 ER PT J AU Hopkins, PF Croton, D Bundy, K Khochfar, S van den Bosch, F Somerville, RS Wetzel, A Keres, D Hernquist, L Stewart, K Younger, JD Genel, S Ma, CP AF Hopkins, Philip F. Croton, Darren Bundy, Kevin Khochfar, Sadegh van den Bosch, Frank Somerville, Rachel S. Wetzel, Andrew Keres, Dusan Hernquist, Lars Stewart, Kyle Younger, Joshua D. Genel, Shy Ma, Chung-Pei TI MERGERS IN Lambda CDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; galaxies: active; galaxies: evolution; galaxies: formation ID COLD DARK-MATTER; GALAXY REDSHIFT SURVEY; DIGITAL-SKY-SURVEY; HALO OCCUPATION DISTRIBUTION; SUPERMASSIVE BLACK-HOLES; TULLY-FISHER RELATION; STAR-FORMATION HISTORY; N-BODY SIMULATIONS; HIERARCHICAL SATELLITE ACCRETION; ACTIVE GALACTIC NUCLEI AB Different theoretical methodologies lead to order-of-magnitude variations in predicted galaxy-galaxy merger rates. We examine how this arises and quantify the dominant uncertainties. Modeling of dark matter and galaxy inspiral/merger times contribute factor of similar to 2 uncertainties. Different estimates of the halo-halo merger rate, the subhalo "destruction" rate, and the halo merger rate with some dynamical friction time delay for galaxy-galaxy mergers, agree to within this factor of similar to 2, provided proper care is taken to define mergers consistently. There are some caveats: if halo/subhalo masses are not appropriately defined the major-merger rate can be dramatically suppressed, and in models with "orphan" galaxies and under-resolved subhalos the merger timescale can be severely overestimated. The dominant differences in galaxy-galaxy merger rates between models owe to the treatment of the baryonic physics. Cosmological hydrodynamic simulations without strong feedback and some older semi-analytic models (SAMs), with known discrepancies in mass functions, can be biased by large factors (similar to 5) in predicted merger rates. However, provided that models yield a reasonable match to the total galaxy mass function, the differences in properties of central galaxies are sufficiently small to alone contribute small (factor of similar to 1.5) additional systematics to merger rate predictions. But variations in the baryonic physics of satellite galaxies in models can also have a dramatic effect on merger rates. The well-known problem of satellite "over-quenching" in most current SAMs-whereby SAM satellite populations are too efficiently stripped of their gas-could lead to order-of-magnitude under-estimates of merger rates for low-mass, gas-rich galaxies. Models in which the masses of satellites are fixed by observations (or SAMs adjusted to resolve this "over-quenching") tend to predict higher merger rates, but with factor of similar to 2 uncertainties stemming from the uncertainty in those observations. The choice of mass used to define "major" and "minor" mergers also matters: stellar-stellar major mergers can be more or less abundant than halo-halo major mergers by an order of magnitude. At low masses, most true major mergers (mass ratio defined in terms of their baryonic or dynamical mass) will appear to be minor mergers in their stellar mass ratio-observations and models using just stellar criteria could underestimate major-merger rates by factors of similar to 3-5. We discuss the uncertainties in relating any merger rate to spheroid formation (in observations or theory): in order to achieve better than factor of similar to 3 accuracy, it is necessary to account for the distribution of merger orbital parameters, gas fractions, and the full efficiency of merger-induced effects as a function of mass ratio. C1 [Hopkins, Philip F.; Bundy, Kevin; Wetzel, Andrew; Ma, Chung-Pei] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Croton, Darren] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Khochfar, Sadegh; Hernquist, Lars; Genel, Shy] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [van den Bosch, Frank] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Somerville, Rachel S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Somerville, Rachel S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Keres, Dusan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stewart, Kyle] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Younger, Joshua D.] Inst Adv Study, Princeton, NJ 08540 USA. RP Hopkins, PF (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. FU Miller Institute for Basic Research in Science, University of California, Berkeley FX We thank Simon White, Gabriella de Lucia, Owen Parry, Carlos Frenk, Andrew Benson, Shardha Jogee, Thorsten Naab, Eyal Neistein, Simone Weinmann, Volker Springel, Martin White, Joanne Cohn, Carrie Bridge, Jennifer Lotz, T. J. Cox, and Eliot Quataert for helpful discussions throughout the development of this work. Support for P.F.H. was provided by the Miller Institute for Basic Research in Science, University of California, Berkeley. NR 264 TC 117 Z9 118 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 915 EP 945 DI 10.1088/0004-637X/724/2/915 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000010 ER PT J AU Stacey, GJ Hailey-Dunsheath, S Ferkinhoff, C Nikola, T Parshley, SC Benford, DJ Staguhn, JG Fiolet, N AF Stacey, G. J. Hailey-Dunsheath, S. Ferkinhoff, C. Nikola, T. Parshley, S. C. Benford, D. J. Staguhn, J. G. Fiolet, N. TI A 158 mu m [C II] LINE SURVEY OF GALAXIES AT z similar to 1-2: AN INDICATOR OF STAR FORMATION IN THE EARLY UNIVERSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: high-redshift; galaxies: ISM; galaxies: starburst; infrared: galaxies; submillimeter: galaxies ID HYPERLUMINOUS INFRARED GALAXIES; SUBMILLIMETER-SELECTED GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; ISO-LWS SPECTROSCOPY; RADIO GALAXIES; HIGH-REDSHIFT; MOLECULAR GAS; PHOTODISSOCIATION REGIONS AB We have detected the 158 mu m [C II] line from 12 galaxies at z similar to 1-2. This is the first survey of this important star formation tracer at redshifts covering the epoch of maximum star formation in the universe and quadruples the number of reported high-z [C II] detections. The line is very luminous, between <0.024% and 0.65% of the far-infrared (FIR) continuum luminosity of our sources, and arises from photodissociation regions on molecular cloud surfaces. An exception is PKS 0215+015, where half of the [C II] emission could arise from X-ray-dominated regions near the central active galactic nucleus (AGN). The L([C) (II])/L(FIR) ratio in our star formation-dominated systems is similar to 8 times larger than that of our AGN-dominated systems. Therefore this ratio selects for star formation-dominated systems. Furthermore, the L([C) (II])/L(FIR) and L([C) (II])/L((CO(1-0))) ratios in our star-forming galaxies and nearby starburst galaxies are the same, so that luminous star-forming galaxies at earlier epochs (z similar to 1-2) appear to be scaled-up versions of local starbursts entailing kiloparsec-scale starbursts. Most of the FIR and [C II] radiation from our AGN-dominated sample (excepting PKS 0215+015) also arises from kiloparsec-scale star formation, but with far-UV radiation fields similar to 8 times more intense than in our star formation-dominated sample. We speculate that the onset of AGN activity stimulates large-scale star formation activity within AGN-dominated systems. This idea is supported by the relatively strong [O III] line emission, indicating very young stars, that was recently observed in high-z composite AGN/starburst systems. Our results confirm the utility of the [C II] line, and in particular, the L([C) (II])/L((FIR)) and L([C) (II])/L(CO(1-0)) ratios as tracers of star formation in galaxies at high redshifts. C1 [Stacey, G. J.; Hailey-Dunsheath, S.; Ferkinhoff, C.; Nikola, T.; Parshley, S. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Benford, D. J.; Staguhn, J. G.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Staguhn, J. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Fiolet, N.] Univ Paris 06, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Fiolet, N.] CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. RP Stacey, GJ (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM stacey@astro.cornell.edu; steve@mpe.mpg.de RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 FU NSF [AST-0096881, AST-0352855, AST-0705256, AST-0722220]; NASA [NGT5-50470, NNG05GK70H] FX We thank an anonymous referee for helpful comments on a previous draft of this paper. This work was supported by NSF grants AST-0096881, AST-0352855, AST-0705256, and AST-0722220 and by NASA grants NGT5-50470 and NNG05GK70H. We thank the CSO staff for their excellent support of ZEUS operations. NR 123 TC 128 Z9 128 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 957 EP 974 DI 10.1088/0004-637X/724/2/957 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000012 ER PT J AU Jenkins, JM Borucki, WJ Koch, DG Marcy, GW Cochran, WD Welsh, WF Basri, G Batalha, NM Buchhave, LA Brown, TM Caldwell, DA Dunham, EW Endl, M Fischer, DA Gautier, TN Geary, JC Gilliland, RL Howell, SB Isaacson, H Johnson, JA Latham, DW Lissauer, JJ Monet, DG Rowe, JF Sasselov, DD Howard, AW MacQueen, P Orosz, JA Chandrasekaran, H Twicken, JD Bryson, ST Quintana, EV Clarke, BD Li, J Allen, C Tenenbaum, P Wu, HL Meibom, S Klaus, TC Middour, CK Cote, MT McCauliff, S Girouard, FR Gunter, JP Wohler, B Hall, JR Ibrahim, K Uddin, AKMK Wu, MS Bhavsar, PA Van Cleve, J Pletcher, DL Dotson, JL Haas, MR AF Jenkins, Jon M. Borucki, William J. Koch, David G. Marcy, Geoffrey W. Cochran, William D. Welsh, William F. Basri, Gibor Batalha, Natalie M. Buchhave, Lars A. Brown, Timothy M. Caldwell, Douglas A. Dunham, Edward W. Endl, Michael Fischer, Debra A. Gautier, Thomas N., III Geary, John C. Gilliland, Ronald L. Howell, Steve B. Isaacson, Howard Johnson, John Asher Latham, David W. Lissauer, Jack J. Monet, David G. Rowe, Jason F. Sasselov, Dimitar D. Howard, Andrew W. MacQueen, Phillip Orosz, Jerome A. Chandrasekaran, Hema Twicken, Joseph D. Bryson, Stephen T. Quintana, Elisa V. Clarke, Bruce D. Li, Jie Allen, Christopher Tenenbaum, Peter Wu, Hayley Meibom, Soren Klaus, Todd C. Middour, Christopher K. Cote, Miles T. McCauliff, Sean Girouard, Forrest R. Gunter, Jay P. Wohler, Bill Hall, Jennifer R. Ibrahim, Khadeejah Uddin, A. K. M. Kamal Wu, Michael S. Bhavsar, Paresh A. Van Cleve, Jeffrey Pletcher, David L. Dotson, Jessie L. Haas, Michael R. TI DISCOVERY AND ROSSITER-McLAUGHLIN EFFECT OF EXOPLANET KEPLER-8b SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio lines: planetary systems; stars: fundamental parameters; stars: individual (Kepler-8, KIC 6822244, 2MASS 18450914+4227038) ID SPIN-ORBIT ALIGNMENT; EXTRASOLAR PLANETARY SYSTEMS; SPECTROSCOPIC TRANSIT; DYNAMICAL RELAXATION; RETROGRADE ORBIT; Y-2 ISOCHRONES; HD 147506B; PARAMETERS; ECCENTRICITY; MISALIGNMENT AB We report on the discovery and the Rossiter-McLaughlin (R-M) effect of Kepler-8b, a transiting planet identified by the NASA Kepler Mission. Kepler photometry and Keck-HIRES radial velocities yield the radius and mass of the planet around this F8IV subgiant host star. The planet has a radius R(P) = 1.419 R(J) and a mass M(P) = 0.60 M(J), yielding a density of 0.26 g cm(-3), one of the lowest planetary densities known. The orbital period is P = 3.523 days and the orbital semimajor axis is 0.0483(-0.0012)(+0.0006) AU. The star has a large rotational v sin i of 10.5 +/- 0.7 kms(-1) and is relatively faint (V approximate to 13.89 mag); both properties are deleterious to precise Doppler measurements. The velocities are indeed noisy, with scatter of 30 ms(-1), but exhibit a period and phase that are consistent with those implied by transit photometry. We securely detect the R-M effect, confirming the planet's existence and establishing its orbit as prograde. We measure an inclination between the projected planetary orbital axis and the projected stellar rotation axis of lambda = -26 degrees.4 +/- 10 degrees.1, indicating a significant inclination of the planetary orbit. R-M measurements of a large sample of transiting planets from Kepler will provide a statistically robust measure of the true distribution of spin-orbit orientations for hot Jupiters around F and early G stars. C1 [Jenkins, Jon M.; Caldwell, Douglas A.; Chandrasekaran, Hema; Twicken, Joseph D.; Quintana, Elisa V.; Clarke, Bruce D.; Li, Jie; Tenenbaum, Peter; Wu, Hayley; Van Cleve, Jeffrey] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Marcy, Geoffrey W.; Basri, Gibor; Isaacson, Howard; Howard, Andrew W.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip] Univ Texas Austin, Austin, TX 78712 USA. [Welsh, William F.; Orosz, Jerome A.] San Diego State Univ, San Diego, CA 92182 USA. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Buchhave, Lars A.; Geary, John C.; Latham, David W.; Sasselov, Dimitar D.; Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Fischer, Debra A.] Radcliffe Inst, Cambridge, MA USA. [Fischer, Debra A.] Yale Univ, New Haven, CT USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Monet, David G.] USN Observ, Flagstaff, AZ 86001 USA. [Allen, Christopher; Klaus, Todd C.; Middour, Christopher K.; McCauliff, Sean; Girouard, Forrest R.; Gunter, Jay P.; Wohler, Bill; Hall, Jennifer R.; Ibrahim, Khadeejah; Uddin, A. K. M. Kamal] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. [Wu, Michael S.] NASA, Ames Res Ctr, Bast Technol, Moffett Field, CA 94035 USA. RP Jenkins, JM (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. EM Jon.Jenkins@nasa.gov RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; OI Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars A./0000-0003-1605-5666; Fischer, Debra/0000-0003-2221-0861 FU W. M. Keck Foundation; NASA's Science Mission Directorate; NASA [NNX06AH52G] FX Based in part on observations obtained at the W. M. Keck Observatory, which is operated as a scientific partnership between 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.; Funding for this mission is provided by NASA's Science Mission Directorate. Many people have contributed to the success of the Kepler Mission, and it is impossible to acknowledge them all. Valuable advice and assistance were provided by Willie Torres, Riley Duren, M. Crane, D. Ciardi, and Josh Winn. Special technical help was provided by Carly Chubak, G. Mandushev, and Josh Winn. We thank E. Bachtel and his team at Ball Aerospace for their work on the Kepler photometer and R. Thompson for key contributions to engineering, and C. Botosh for able management. G.W.M. thanks and acknowledges support from NASA Cooperative Agreement NNX06AH52G. NR 74 TC 67 Z9 67 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 1108 EP 1119 DI 10.1088/0004-637X/724/2/1108 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000021 ER PT J AU Gibson, SE Kucera, TA Rastawicki, D Dove, J De Toma, G Hao, J Hill, S Hudson, HS Marque, C McIntosh, PS Rachmeler, L Reeves, KK Schmieder, B Schmit, DJ Seaton, DB Sterling, AC Tripathi, D Williams, DR Zhang, M AF Gibson, S. E. Kucera, T. A. Rastawicki, D. Dove, J. De Toma, G. Hao, J. Hill, S. Hudson, H. S. Marque, C. McIntosh, P. S. Rachmeler, L. Reeves, K. K. Schmieder, B. Schmit, D. J. Seaton, D. B. Sterling, A. C. Tripathi, D. Williams, D. R. Zhang, M. TI THREE-DIMENSIONAL MORPHOLOGY OF A CORONAL PROMINENCE CAVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: filaments, prominences; Sun: magnetic topology ID TOTAL SOLAR ECLIPSE; WHOLE SUN MONTH; MULTIWAVELENGTH OBSERVATIONS; DIAGNOSTIC SPECTROMETER; MASS EJECTIONS; TEMPERATURES; CALIBRATION; DENSITIES; TRACE; TOMOGRAPHY AB We present a three-dimensional density model of coronal prominence cavities, and a morphological fit that has been tightly constrained by a uniquely well-observed cavity. Observations were obtained as part of an International Heliophysical Year campaign by instruments from a variety of space-and ground-based observatories, spanning wavelengths from radio to soft X-ray to integrated white light. From these data it is clear that the prominence cavity is the limb manifestation of a longitudinally extended polar-crown filament channel, and that the cavity is a region of low density relative to the surrounding corona. As a first step toward quantifying density and temperature from campaign spectroscopic data, we establish the three-dimensional morphology of the cavity. This is critical for taking line-of-sight projection effects into account, since cavities are not localized in the plane of the sky and the corona is optically thin. We have augmented a global coronal streamer model to include a tunnel-like cavity with elliptical cross-section and a Gaussian variation of height along the tunnel length. We have developed a semi-automated routine that fits ellipses to cross-sections of the cavity as it rotates past the solar limb, and have applied it to Extreme Ultraviolet Imager observations from the two Solar Terrestrial Relations Observatory spacecraft. This defines the morphological parameters of our model, from which we reproduce forward-modeled cavity observables. We find that cavity morphology and orientation, in combination with the viewpoints of the observing spacecraft, explain the observed variation in cavity visibility for the east versus west limbs. C1 [Gibson, S. E.; De Toma, G.; Rachmeler, L.] HAO NCAR, Boulder, CO 80307 USA. [Kucera, T. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rastawicki, D.] Stanford Univ, Stanford, CA 94305 USA. [Dove, J.] Metropolitan State Coll, Denver, CO 80217 USA. [Hao, J.; Zhang, M.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Hill, S.] NOAA, Natl Weather Serv, Space Weather Predict Ctr, Boulder, CO 80305 USA. [Hudson, H. S.] Univ Calif Berkeley, Space Sci Labs, Berkeley, CA 94720 USA. [Marque, C.; Seaton, D. B.] Royal Observ Belgium, B-1180 Brussels, Belgium. [McIntosh, P. S.] HelioSynopt Inc, Boulder, CO 80301 USA. [Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schmieder, B.] LESIA, Observ Paris, Sect Meudon, Paris, France. [Schmit, D. J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80305 USA. [Sterling, A. C.] NASA, Marshall Space Flight Ctr, Space Sci Dept SD50, Huntsville, AL 35812 USA. [Tripathi, D.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England. [Williams, D. R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Gibson, SE (reprint author), HAO NCAR, POB 3000, Boulder, CO 80307 USA. RI Williams, David/E-6676-2011; Kucera, Therese/C-9558-2012; Tripathi, Durgesh/D-9390-2012; Reeves, Katharine/P-9163-2014; OI Williams, David/0000-0001-9922-8117; Tripathi, Durgesh/0000-0003-1689-6254; Kucera, Therese/0000-0001-9632-447X; SEATON, DANIEL/0000-0002-0494-2025 FU International Space Science Institute (ISSI); NASA; National Science Foundation FX We thank the International Space Science Institute (ISSI), which funded a Working Group on Coronal Cavities involving many of the co-authors. We thank Alice Lecinski for internal HAO review, Joan Burkepile for assistance with the Mk4 data, and Arnaud Thernisien for assistance with the STEREO Carrington maps. A.C.S. and T.A.K. were supported by the NASA SHP program. SOHO is a project of international collaboration between ESA and NASA. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). The STEREO/SECCHI data used here are produced by 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 fr Sonnensystemforschung (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Thorique et Applique (France), and Institut d'Astrophysique Spatiale (France). The National Center for Atmospheric Research is supported by the National Science Foundation. NR 46 TC 48 Z9 48 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 1133 EP 1146 DI 10.1088/0004-637X/724/2/1133 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000023 ER PT J AU Titarchuk, L Shaposhnikov, N AF Titarchuk, Lev Shaposhnikov, Nikolai TI IMPLICATION OF THE OBSERVED SPECTRAL CUTOFF ENERGY EVOLUTION IN XTE J1550-564 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; radiation mechanisms: non-thermal; stars: individual (XTE J1550-564) ID OSCILLATION FREQUENCY CORRELATION; BLACK-HOLE BINARIES; X-RAY; INTRINSIC SIGNATURE; MONTE-CARLO; POWER-LAW; COMPTONIZATION; STATES; INDEX; TRANSITION AB The physical mechanisms responsible for the production of non-thermal emission in accreting black holes (BHs) should be imprinted in the observational appearances of the power-law tails in the X-ray spectra from these objects. Phenomenology of different spectral states exhibited by galactic BH binaries allows us to establish the physics of the photon upscattering under different accretion regimes. We revisit the data collected by the Rossi X-ray Timing Explorer from the BH X-ray binary XTE J1550-564 during two periods of X-ray activity in 1998 and 2000 focusing on the behavior of the high-energy cutoff of the power-law part of the spectrum. For the 1998 outburst, the transition from the low-hard state to the intermediate state was accompanied by a gradual decrease in the cutoff energy. This was followed by an extended minimum which then showed an abrupt reversal to a clear increasing trend as the source evolved to the very high and high-soft states. The 2000 outburst showed only the decreasing and extended minimum portions of this pattern. We attribute this difference in the cutoff energy behavior to the different partial contributions of the thermal and non-thermal (bulk motion) Comptonization. Namely, during the 1998 event the higher accretion rate presumably provided more cooling to the Comptonizing media and thus reducing the effectiveness of the thermal upscattering process. Under these conditions, the bulk motion takes a leading role in boosting the input soft photons. Recent Monte Carlo simulations by Laurent & Titarchuk strongly support this scenario. C1 [Titarchuk, Lev] Univ Ferrara, Dept Phys, I-44100 Ferrara, Italy. [Titarchuk, Lev; Shaposhnikov, Nikolai] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Titarchuk, Lev] George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Shaposhnikov, Nikolai] Univ Maryland, CRESST, Dept Astron, College Pk, MD 20742 USA. RP Titarchuk, L (reprint author), Univ Ferrara, Dept Phys, Via Saragat 1, I-44100 Ferrara, Italy. EM lev@milkyway.gsfc.nasa.gov; nikolai.v.shaposhnikov@nasa.gov FU NASA [NNX09AF02G] FX The authors appreciate the deep analysis of the paper's content by the referee. The RXTE data for this work were acquired through HEASARC. Authors acknowledge the support of this research by NASA grant NNX09AF02G. NR 21 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 1147 EP 1152 DI 10.1088/0004-637X/724/2/1147 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000024 ER PT J AU Stock, ND Su, KYL Liu, W Hinz, PM Rieke, GH Marengo, M Stapelfeldt, KR Hines, DC Trilling, DE AF Stock, Nathan D. Su, Kate Y. L. Liu, Wilson Hinz, Phil M. Rieke, George H. Marengo, Massimo Stapelfeldt, Karl R. Hines, Dean C. Trilling, David E. TI THE STRUCTURE OF THE beta LEONIS DEBRIS DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; planetary systems; stars: individual (beta Leo, o Leo); techniques: interferometric ID MULTIBAND IMAGING PHOTOMETER; SPITZER-SPACE-TELESCOPE; ROTATING STAR ACHERNAR; MAIN-SEQUENCE STARS; ABSOLUTE CALIBRATION; PLANETARY SYSTEMS; MU-M; INFRARED SPECTROGRAPH; EVOLUTION; DUST AB We combine nulling interferometry at 10 mu m using the MMT and Keck Telescopes with spectroscopy, imaging, and photometry from 3 to 100 mu m using Spitzer to study the debris disk around beta Leo over a broad range of spatial scales, corresponding to radii of 0.1 to similar to 100 AU. We have also measured the close binary star o Leo with both Keck and MMT interferometers to verify our procedures with these instruments. The beta Leo debris system has a complex structure: (1) relatively little material within 1 AU; (2) an inner component with a color temperature of similar to 600 K, fitted by a dusty ring from about 2-3 AU; and (3) a second component with a color temperature of similar to 120 K fitted by a broad dusty emission zone extending from about similar to 5 AU to similar to 55 AU. Unlike many other A-type stars with debris disks, beta Leo lacks a dominant outer belt near 100 AU. C1 [Stock, Nathan D.; Su, Kate Y. L.; Hinz, Phil M.; Rieke, George H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Liu, Wilson] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Marengo, Massimo] Iowa State Univ, Dept Phys & Astron, Ames, IA 50010 USA. [Stapelfeldt, Karl R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hines, Dean C.] Space Sci Inst, Boulder, CO 80301 USA. [Trilling, David E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. RP Stock, ND (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM nstock@as.arizona.edu RI Stapelfeldt, Karl/D-2721-2012 FU National Aeronautics and Space Administration; NASA Exoplanet Science Institute at the California Institute of Technology; JPL/Caltech [1255094]; KI [1330562] FX We thank R. Akeson and R. Millan-Gabet for extensive assistance with the KIN observations. We are grateful to M. Colavita for reduction of the 2008 February beta Leo data, J. Bouwman for providing the FEPS IRS reduction pipeline and slit offset correction software, and P. Smith for reduction of the MIPS-SED data. We also thank R. Akeson and O. Absil for discussion of the K-band excess. Some observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona, and by the Keck Interferometer, which is funded by the National Aeronautics and Space Administration as part of its Navigator program. This work has made use of services produced by the NASA Exoplanet Science Institute at the California Institute of Technology. This work was supported by KI subcontract 1330562 and contract 1255094 from JPL/Caltech to the University of Arizona. NR 52 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 1238 EP 1255 DI 10.1088/0004-637X/724/2/1238 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000030 ER PT J AU Joyce, CJ Smith, CW Isenberg, PA Murphy, N Schwadron, NA AF Joyce, Colin J. Smith, Charles W. Isenberg, Philip A. Murphy, Neil Schwadron, Nathan A. TI EXCITATION OF LOW-FREQUENCY WAVES IN THE SOLAR WIND BY NEWBORN INTERSTELLAR PICKUP IONS H+ AND He+ AS SEEN BY VOYAGER AT 4.5 AU SO ASTROPHYSICAL JOURNAL LA English DT Article DE instabilities; ISM: abundances; solar wind; waves ID INTERPLANETARY MAGNETIC-FIELD; ROTATING RAREFACTION REGIONS; DISSIPATION RANGE; TURBULENCE; HELIOSPHERE; PROTONS; FLUCTUATIONS; IONIZATION; SCATTERING; HYDROGEN AB We report the observation of a spectral enhancement in the magnetic field fluctuations measured by the MAG instrument on the Voyager 2 spacecraft during 4.5 hr on DOY 7, 1979 at a heliocentric radial position of 4.5 AU. This time period is contained within a solar wind rarefaction when the large-scale interplanetary magnetic field was nearly radial. The frequency range and polarization of the enhanced fluctuations are consistent with waves generated by newly ionized interstellar H+ and He+. We show sunward propagation of the waves via a cross-helicity analysis. We compare the observation with a theoretical model and find reasonable agreement given the model assumptions. This event is the first indication of pickup ion-generated waves seen at Voyager. It is also the first identification of pickup He+ waves by any spacecraft. C1 [Joyce, Colin J.; Smith, Charles W.; Isenberg, Philip A.] Univ New Hampshire, Ctr Space Sci, Dept Phys, Durham, NH 03824 USA. [Murphy, Neil] CALTECH, Jet Prop Lab, Space & Astrophys Plasmas Grp, Pasadena, CA USA. [Schwadron, Nathan A.] Boston Univ, Dept Astron, Ctr Space Phys, Boston, MA 02215 USA. RP Joyce, CJ (reprint author), Univ New Hampshire, Ctr Space Sci, Dept Phys, Durham, NH 03824 USA. EM cjl46@unh.edu; Charles.Smith@unh.edu; Phil.Isenberg@unh.edu; Neil.Murphy@jpl.nasa.gov; nathanas@bu.edu FU NASA [NNX07AH75G]; NSF [ATM0635863] FX This work was supported in part by NASA Guest Investigator grant NNX07AH75G and NSF grant ATM0635863. C.J.J. is an undergraduate in the Physics program at UNH. The authors acknowledge helpful conversations with B. J. Vasquez. NR 40 TC 17 Z9 17 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 1256 EP 1261 DI 10.1088/0004-637X/724/2/1256 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000031 ER PT J AU Tamura, Y Iono, D Wilner, DJ Kajisawa, M Uchimoto, YK Alexander, DM Chung, A Ezawa, H Hatsukade, B Hayashino, T Hughes, DH Ichikawa, T Ikarashi, S Kawabe, R Kohno, K Lehmer, BD Matsuda, Y Nakanishi, K Takata, T Wilson, GW Yamada, T Yun, MS AF Tamura, Y. Iono, D. Wilner, D. J. Kajisawa, M. Uchimoto, Y. K. Alexander, D. M. Chung, A. Ezawa, H. Hatsukade, B. Hayashino, T. Hughes, D. H. Ichikawa, T. Ikarashi, S. Kawabe, R. Kohno, K. Lehmer, B. D. Matsuda, Y. Nakanishi, K. Takata, T. Wilson, G. W. Yamada, T. Yun, M. S. TI SUBMILLIMETER ARRAY IDENTIFICATION OF THE MILLIMETER-SELECTED GALAXY SSA22-AzTEC1: A PROTOQUASAR IN A PROTOCLUSTER? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: formation; galaxies: starburst; infrared: galaxies; quasars: general; submillimeter: galaxies; X-rays: galaxies ID STAR-FORMING GALAXIES; HUBBLE-DEEP-FIELD; ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; SUPERMASSIVE BLACK-HOLES; SPITZER-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; DEGREE EXTRAGALACTIC SURVEY; RAY SPECTRAL PROPERTIES; LARGE-SCALE STRUCTURE AB We present results from Submillimeter Array (SMA) 860 mu m subarcsecond astrometry and multiwavelength observations of the brightest millimeter (S-1.1mm = 8.4 mJy) source, SSA22-AzTEC1, found near the core of the SSA22 protocluster that is traced by Ly alpha-emitting galaxies at z = 3.09. We identify a 860 mu m counterpart with a flux density of S-860 mu m = 12.2 +/- 2.3 mJy and absolute positional accuracy that is better than 0 ''.3. At the SMA position, we find radio-to-mid-infrared counterparts, whilst no object is found in Subaru optical and near-infrared deep images at wavelengths <= 1 mu m (J > 25.4 in AB, 2 sigma). The photometric redshift estimate, using flux densities at >= 24 mu m, indicates z(phot) = 3.19(-0.35)(+0.26) , consistent with the protocluster redshift. We then model the near-to-mid-infrared spectral energy distribution (SED) of SSA22-AzTEC1, and find that the SED modeling requires a large extinction (A(V) approximate to 3.4 mag) of starlight from a stellar component with M-star similar to 10(10.9) M-circle dot, assuming z = 3.1. Additionally, we find a significant X-ray counterpart with a very hard spectrum (Gamma(eff) = -0.34(-0.61)(+0.57)), strongly suggesting that SSA22-AzTEC1 harbors a luminous active galactic nuclei (AGNs; L-X approximate to 3 x 10(44) erg s(-1)) behind a large hydrogen column (N-H similar to 10(24) cm(-2)). The AGN, however, is responsible for only similar to 10% of the bolometric luminosity of the host galaxy, and therefore the star formation activity likely dominates the submillimeter emission. It is possible that SSA22-AzTEC1 is the first example of a protoquasar growing at the bottom of the gravitational potential underlying the SSA22 protocluster. C1 [Tamura, Y.; Iono, D.; Hatsukade, B.; Kawabe, R.] Natl Inst Nat Sci, Natl Astron Observ Japan, Nobeyama Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan. [Tamura, Y.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Wilner, D. J.; Chung, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kajisawa, M.; Hayashino, T.; Ichikawa, T.; Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Kajisawa, M.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Uchimoto, Y. K.; Hatsukade, B.; Ikarashi, S.; Kohno, K.] Univ Tokyo, Inst Astron, Tokyo 1810015, Japan. [Alexander, D. M.; Lehmer, B. D.; Matsuda, Y.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Chung, A.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Ezawa, H.; Nakanishi, K.; Takata, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. [Kawabe, R.] Grad Univ Adv Studies, Sch Sci, Dept Astron, Mitaka, Tokyo 1818588, Japan. [Kohno, K.] Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. [Lehmer, B. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wilson, G. W.; Yun, M. S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Tamura, Y (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, Nobeyama Radio Observ, Minamisa Ku, 462-2 Nobeyama, Minamimaki, Nagano 3841305, Japan. EM yoichi.tamura@nao.ac.jp OI Alexander, David/0000-0002-5896-6313 FU Japan Society for the Promotion of Science (JSPS); Royal Society; Smithsonian Institution; Academia Sinica; Philip Leverhulme Prize FX We are grateful to the referee for constructive suggestions which improved the presentation of this work. Y.T. thanks N. Kawakatu, T. Kodama, K. Kawara, and T. Oshima for fruitful discussions. Y.T. and B.H. are financially supported by the Japan Society for the Promotion of Science (JSPS) for Young Scientists. D.M.A. thanks the Royal Society and a Philip Leverhulme Prize for funding. The Nobeyama Radio Observatory is a branch of the National Astronomical Observatory of Japan, the National Institute of Natural Sciences (NINS). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This work is based in part on archival data obtained with the NASA Spitzer Space Telescope. NR 152 TC 26 Z9 26 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 1270 EP 1282 DI 10.1088/0004-637X/724/2/1270 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000033 ER PT J AU Goncalves, TS Basu-Zych, A Overzier, R Martin, DC Law, DR Schiminovich, D Wyder, TK Mallery, R Rich, RM Heckman, TH AF Goncalves, Thiago S. Basu-Zych, Antara Overzier, Roderik Martin, D. Christopher Law, David R. Schiminovich, David Wyder, Ted K. Mallery, Ryan Rich, R. Michael Heckman, Timothy H. TI THE KINEMATICS OF IONIZED GAS IN LYMAN-BREAK ANALOGS AT z similar to 0.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: kinematics and dynamics; galaxies: starburst ID STAR-FORMING GALAXIES; ULTRAVIOLET-LUMINOUS GALAXIES; INTEGRAL-FIELD SPECTROSCOPY; ADAPTIVE OPTICS SYSTEM; HIGH-REDSHIFT GALAXIES; TULLY-FISHER RELATION; ULTRA DEEP FIELD; INTERSTELLAR-MEDIUM; CHAIN GALAXIES; DISK GALAXIES AB We present results for 19 "Lyman-break analogs" observed with Keck/OSIRIS with an adaptive-optics-assisted spatial resolution of less than 200 pc. We detect satellites/companions, diffuse emission, and velocity shear, all with high signal-to-noise ratios. These galaxies present remarkably high velocity dispersion along the line of sight (similar to 70 km s(-1)), much higher than standard star-forming spirals in the low-redshift universe. We artificially redshift our data to z similar to 2.2 to allow for a direct comparison with observations of high-z Lyman-break galaxies and find striking similarities between both samples. This suggests that either similar physical processes are responsible for their observed properties, or, alternatively, that it is very difficult to distinguish between different mechanisms operating in the low- versus high-redshift starburst galaxies based on the available data. The comparison between morphologies in the UV/optical continuum and our kinemetry analysis often shows that neither is by itself sufficient to confirm or completely rule out the contribution from recent merger events. We find a correlation between the kinematic properties and stellar mass, in that more massive galaxies show stronger evidence for a disk-like structure. This suggests a co-evolutionary process between the stellar mass buildup and the formation of morphological and dynamical substructure within the galaxy. C1 [Goncalves, Thiago S.; Martin, D. Christopher; Wyder, Ted K.] CALTECH, Pasadena, CA 91125 USA. [Basu-Zych, Antara] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Overzier, Roderik] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Law, David R.; Mallery, Ryan; Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Div Astron & Astrophys, Los Angeles, CA 90095 USA. [Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Heckman, Timothy H.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Goncalves, TS (reprint author), CALTECH, MC 278-17, Pasadena, CA 91125 USA. EM tsg@astro.caltech.edu NR 71 TC 50 Z9 50 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 1373 EP 1388 DI 10.1088/0004-637X/724/2/1373 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000042 ER PT J AU Krco, M Goldsmith, PF AF Krco, Marko Goldsmith, Paul F. TI A SURVEY OF HI NARROW SELF-ABSORPTION IN MOLECULAR CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: atoms; ISM: clouds; ISM: molecules ID OPHIUCHUS DARK CLOUD; NEUTRAL HYDROGEN; ATOMIC-HYDROGEN; DUST CLOUDS; EVOLUTION; COMPLEX; TAURUS; REGION; GAS AB The study of cold atomic hydrogen (HI) in molecular clouds has the potential to significantly improve our understanding of the formation of molecular clouds, the atomic to molecular hydrogen conversion process, and star formation. Results from the first large survey of Hi Narrow Self Absorption (HINSA) features outside of the Taurus Molecular Cloud Complex are presented. Previous hypotheses that cold atomic hydrogen represents the third largest constituent of molecular clouds are confirmed with a mean abundance of 10(-2.8) in comparison with the total proton column density. HINSA features are observed in over 80% of the observed clouds, accompanied by indications that cold Hi probably exists in all clouds. We find that HINSA features are observable to distances of at least 700 pc. Nine clouds have been mapped in detail revealing that HINSA abundances can vary significantly within a cloud both spatially and in an individual velocity component. Possible explanations for this phenomenon are briefly discussed. C1 [Krco, Marko] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Krco, M (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM marko@astro.cornell.edu RI Goldsmith, Paul/H-3159-2016 FU National Science Foundation [AST 0404770, AST 0407019]; National Radio Astronomy Observatory Student Support Program; National Aeronautics and Space Administration; Greenbank Telescope of the National Radio Astronomy Observatory FX This research was supported in part by the National Science Foundation through grants AST 0404770 and AST 0407019, as well as the National Radio Astronomy Observatory Student Support Program. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The data used in this paper were obtained with the Five College Radio Observatory which is supported by the National Science Foundation with permission of the Metropolitan District Commission, and with the Greenbank Telescope of the National Radio Astronomy Observatory. We thank Mark Heyer and Jay Lockman for assistance in carrying out the observation. The program used for regridding the data in this work was modified from the original version developed by Tim Robishaw. NR 41 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 1402 EP 1429 DI 10.1088/0004-637X/724/2/1402 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000045 ER PT J AU Miller, JM D'Ai, A Bautz, MW Bhattacharyya, S Burrows, DN Cackett, EM Fabian, AC Freyberg, MJ Haberl, F Kennea, J Nowak, MA Reis, RC Strohmayer, TE Tsujimoto, M AF Miller, J. M. D'Ai, A. Bautz, M. W. Bhattacharyya, S. Burrows, D. N. Cackett, E. M. Fabian, A. C. Freyberg, M. J. Haberl, F. Kennea, J. Nowak, M. A. Reis, R. C. Strohmayer, T. E. Tsujimoto, M. TI ON RELATIVISTIC DISK SPECTROSCOPY IN COMPACT OBJECTS WITH X-RAY CCD CAMERAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; instrumentation: spectrographs; methods: analytical; X-rays: binaries ID BLACK-HOLE SPIN; RXTE SPECTRAL OBSERVATIONS; PHOTON IMAGING CAMERA; IRON EMISSION-LINES; XMM-NEWTON; ACCRETION DISK; LOW/HARD STATE; 4U 1705-44; GX 339-4; SAX J1808.4-3658 AB X-ray charge-coupled devices (CCDs) are the workhorse detectors of modern X-ray astronomy. Typically covering the 0.3-10.0 keV energy range, CCDs are able to detect photoelectric absorption edges and K shell lines from most abundant metals. New CCDs also offer resolutions of 30-50 (E/Delta E), which is sufficient to detect lines in hot plasmas and to resolve many lines shaped by dynamical processes in accretion flows. The spectral capabilities of X-ray CCDs have been particularly important in detecting relativistic emission lines from the inner disks around accreting neutron stars and black holes. One drawback of X-ray CCDs is that spectra can be distorted by photon "pile-up," wherein two or more photons may be registered as a single event during one frame time. We have conducted a large number of simulations using a statistical model of photon pile-up to assess its impacts on relativistic disk line and continuum spectra from stellar-mass black holes and neutron stars. The simulations cover the range of current X-ray CCD spectrometers and operational modes typically used to observe neutron stars and black holes in X-ray binaries. Our results suggest that severe photon pile-up acts to falsely narrow emission lines, leading to falsely large disk radii and falsely low spin values. In contrast, our simulations suggest that disk continua affected by severe pile-up are measured to have falsely low flux values, leading to falsely small radii and falsely high spin values. The results of these simulations and existing data appear to suggest that relativistic disk spectroscopy is generally robust against pile-up when this effect is modest. C1 [Cackett, E. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [D'Ai, A.] Univ Palermo, Dipartimento Sci Fis & Astron, Palermo, Italy. [Bautz, M. W.; Nowak, M. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bhattacharyya, S.] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. [Burrows, D. N.; Kennea, J.] Penn State Univ, Dept Astron & Astrophys, College Pk, PA 16802 USA. [Fabian, A. C.; Reis, R. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Freyberg, M. J.; Haberl, F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Strohmayer, T. E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Tsujimoto, M.] Japan Aerosp Explorat Agcy, Inst Space & Astron Sci, Sagamihara, Kanagawa 2298510, Japan. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu RI D'Ai, Antonino/B-3962-2012; OI D'Ai, Antonino/0000-0002-5042-1036; reis, rubens/0000-0002-6618-2412; Haberl, Frank/0000-0002-0107-5237 NR 89 TC 32 Z9 32 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2010 VL 724 IS 2 BP 1441 EP 1455 DI 10.1088/0004-637X/724/2/1441 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GE UT WOS:000284149000047 ER PT J AU Borkowski, KJ Reynolds, SP Green, DA Hwang, U Petre, R Krishnamurthy, K Willett, R AF Borkowski, Kazimierz J. Reynolds, Stephen P. Green, David A. Hwang, Una Petre, Robert Krishnamurthy, Kalyani Willett, Rebecca TI RADIOACTIVE SCANDIUM IN THE YOUNGEST GALACTIC SUPERNOVA REMNANT G1.9+0.3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (G1.9+0.3); ISM: supernova remnants; nuclear reactions, nucleosynthesis, abundances; X-rays: ISM ID RAY LINE EMISSION; RX J0852.0-4622; IA SUPERNOVAE; TI-44; CASSIOPEIA; NUCLEOSYNTHESIS; MODELS; DECAY; SEARCH; SUZAKU AB We report the discovery of thermal X-ray emission from the youngest Galactic supernova remnant G1.9+0.3, from a 237 ks Chandra observation. We detect strong K alpha lines of Si, S, Ar, Ca, and Fe. In addition, we detect a 4.1 keV line with 99.971% confidence which we attribute to Sc-44, produced by electron capture from Ti-44. Combining the data with our earlier Chandra observation allows us to detect the line in two regions independently. For a remnant age of 100 yr, our measured total line strength indicates synthesis of (1-7) x 10(-5) M-circle dot of Ti-44, in the range predicted for both Type Ia and core-collapse supernovae (SNe), but somewhat smaller than the 2 x 10(-4) M-circle dot reported for Cas A. The line spectrum indicates supersolar abundances. The Fe emission has a width of about 28,000 km s(-1), consistent with an age of similar to 100 yr and with the inferred mean shock velocity of 14,000 km s(-1) deduced assuming a distance of 8.5 kpc. Most thermal emission comes from regions of lower X-ray but higher radio surface brightness. Deeper observations should allow more detailed spatial mapping of Sc-44, with significant implications for models of nucleosynthesis in Type Ia SNe. C1 [Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Green, David A.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Hwang, Una; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krishnamurthy, Kalyani; Willett, Rebecca] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA. RP Borkowski, KJ (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. EM kborkow@unity.ncsu.edu RI Green, David/E-9609-2010; Willett, Rebecca/G-6930-2012 OI Willett, Rebecca/0000-0002-8109-7582; Green, David/0000-0003-3189-9998; FU NASA [SAO GO6-7059X] FX This work was supported by NASA through Chandra General Observer Program grant SAO GO6-7059X. NR 33 TC 33 Z9 33 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2010 VL 724 IS 2 BP L161 EP L165 DI 10.1088/2041-8205/724/2/L161 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GU UT WOS:000284150700008 ER PT J AU Valiante, E Ade, PAR Bock, JJ Braglia, FG Chapin, EL Devlin, MJ Griffin, M Gundersen, JO Halpern, M Hargrave, PC Hughes, DH Klein, J Marsden, G Mauskopf, P Netterfield, CB Olmi, L Pascale, E Patanchon, G Rex, M Scott, D Scott, K Semisch, C Stabenau, H Thomas, N Truch, MDP Tucker, C Tucker, GS Viero, MP Wiebe, DV AF Valiante, Elisabetta Ade, Peter A. R. Bock, James J. Braglia, Filiberto G. Chapin, Edward L. Devlin, Mark J. Griffin, Matthew Gundersen, Joshua O. Halpern, Mark Hargrave, Peter C. Hughes, David H. Klein, Jeff Marsden, Gaelen Mauskopf, Philip Netterfield, Calvin B. Olmi, Luca Pascale, Enzo Patanchon, Guillaume Rex, Marie Scott, Douglas Scott, Kimberly Semisch, Christopher Stabenau, Hans Thomas, Nicholas Truch, Matthew D. P. Tucker, Carole Tucker, Gregory S. Viero, Marco P. Wiebe, Donald V. TI BLAST OBSERVATIONS OF THE SOUTH ECLIPTIC POLE FIELD: NUMBER COUNTS AND SOURCE CATALOGS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; galaxies: statistics; methods: data analysis; submillimeter: galaxies ID APERTURE SUBMILLIMETER TELESCOPE; GALAXIES; MAPS; HALF AB We present results from a survey carried out by the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) on a 9 deg(2) field near the South Ecliptic Pole at 250, 350, and 500 mu m. The median 1 sigma depths of the maps are 36.0, 26.4, and 18.4 mJy, respectively. We apply a statistical method to estimate submillimeter galaxy number counts and find that they are in agreement with other measurements made with the same instrument and with the more recent results from Herschel/SPIRE. Thanks to the large field observed, the new measurements give additional constraints on the bright end of the counts. We identify 132, 89, and 61 sources with S/N >= 4 at 250, 350, 500 mu m, respectively and provide a multi-wavelength combined catalog of 232 sources with a significance >= 4 sigma in at least one BLAST band. The new BLAST maps and catalogs are available publicly at http://blastexperiment.info. C1 [Valiante, Elisabetta; Braglia, Filiberto G.; Chapin, Edward L.; Halpern, Mark; Marsden, Gaelen; Scott, Douglas; Wiebe, Donald V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Ade, Peter A. R.; Griffin, Matthew; Hargrave, Peter C.; Mauskopf, Philip; Pascale, Enzo; Tucker, Carole] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bock, James J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, James J.] CALTECH, Pasadena, CA 91125 USA. [Devlin, Mark J.; Klein, Jeff; Scott, Kimberly; Semisch, Christopher; Stabenau, Hans; Truch, Matthew D. P.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Gundersen, Joshua O.; Thomas, Nicholas] Univ Miami, Dept Phys, Carol Gables, FL 33146 USA. [Hughes, David H.] INAOE, Puebla 72000, Mexico. [Netterfield, Calvin B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Netterfield, Calvin B.; Viero, Marco P.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Olmi, Luca] Ist Radioastron, I-50125 Florence, Italy. [Olmi, Luca] Univ Puerto Rico, UPR Stn, Dept Phys, San Juan, PR 00936 USA. [Patanchon, Guillaume] Lab APC, F-75205 Paris, France. [Rex, Marie] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Tucker, Gregory S.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Valiante, E (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. EM valiante@phas.ubc.ca RI Klein, Jeffrey/E-3295-2013; OI Olmi, Luca/0000-0002-1162-7947; Scott, Douglas/0000-0002-6878-9840 FU NASA [NAG5-12785, NAG5-13301, NNGO-6GI11G]; NSF Office of Polar Programs; Canadian Space Agency; Natural Sciences and Engineering Research Council (NSERC) of Canada; UK Science and Technology Facilities Council (STFC) FX BLAST acknowledges the support of NASA through grant numbers NAG5-12785, NAG5-13301, and NNGO-6GI11G, the NSF Office of Polar Programs, the Canadian Space Agency, the Natural Sciences and Engineering Research Council (NSERC) of Canada, and the UK Science and Technology Facilities Council (STFC). This research has been enabled by the use of WestGrid computing resources. NR 26 TC 8 Z9 8 U1 0 U2 4 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 DEC PY 2010 VL 191 IS 2 BP 222 EP 231 DI 10.1088/0067-0049/191/2/222 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692VY UT WOS:000285185200003 ER PT J AU Hincks, AD Acquaviva, V Ade, PAR Aguirre, P Amiri, M Appel, JW Barrientos, LF Battistelli, ES Bond, JR Brown, B Burger, B Chervenak, J Das, S Devlin, MJ Dicker, SR Doriese, WB Dunkley, J Dunner, R Essinger-Hileman, T Fisher, RP Fowler, JW Hajian, A Halpern, M Hasselfield, M Hernandez-Monteagudo, C Hilton, GC Hilton, M Hlozek, R Huffenberger, KM Hughes, DH Hughes, JP Infante, L Irwin, KD Jimenez, R Juin, JB Kaul, M Klein, J Kosowsky, A Lau, JM Limon, M Lin, YT Lupton, RH Marriage, TA Marsden, D Martocci, K Mauskopf, P Menanteau, F Moodley, K Moseley, H Netterfield, CB Niemack, MD Nolta, MR Page, LA Parker, L Partridge, B Quintana, H Reid, B Sehgal, N Sievers, J Spergel, DN Staggs, ST Stryzak, O Swetz, DS Switzer, ER Thornton, R Trac, H Tucker, C Verde, L Warne, R Wilson, G Wollack, E Zhao, Y AF Hincks, A. D. Acquaviva, V. Ade, P. A. R. Aguirre, P. Amiri, M. Appel, J. W. Barrientos, L. F. Battistelli, E. S. Bond, J. R. Brown, B. Burger, B. Chervenak, J. Das, S. Devlin, M. J. Dicker, S. R. Doriese, W. B. Dunkley, J. Duenner, R. Essinger-Hileman, T. Fisher, R. P. Fowler, J. W. Hajian, A. Halpern, M. Hasselfield, M. Hernandez-Monteagudo, C. Hilton, G. C. Hilton, M. Hlozek, R. Huffenberger, K. M. Hughes, D. H. Hughes, J. P. Infante, L. Irwin, K. D. Jimenez, R. Juin, J. B. Kaul, M. Klein, J. Kosowsky, A. Lau, J. M. Limon, M. Lin, Y. -T. Lupton, R. H. Marriage, T. A. Marsden, D. Martocci, K. Mauskopf, P. Menanteau, F. Moodley, K. Moseley, H. Netterfield, C. B. Niemack, M. D. Nolta, M. R. Page, L. A. Parker, L. Partridge, B. Quintana, H. Reid, B. Sehgal, N. Sievers, J. Spergel, D. N. Staggs, S. T. Stryzak, O. Swetz, D. S. Switzer, E. R. Thornton, R. Trac, H. Tucker, C. Verde, L. Warne, R. Wilson, G. Wollack, E. Zhao, Y. TI THE ATACAMA COSMOLOGY TELESCOPE (ACT): BEAM PROFILES AND FIRST SZ CLUSTER MAPS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: general; methods: data analysis ID MICROWAVE BACKGROUND ANISOTROPY; MASSIVE GALAXY CLUSTERS; FLUX-LIMITED SAMPLE; X-RAY-PROPERTIES; ALL-SKY SURVEY; SCALING RELATIONS; POWER SPECTRUM; PHYSICAL-PROPERTIES; ARRAY CAMERA; 1E 0657-56 AB The Atacama Cosmology Telescope (ACT) is currently observing the cosmic microwave background with arcminute resolution at 148 GHz, 218 GHz, and 277 GHz. In this paper, we present ACT's first results. Data have been analyzed using a maximum-likelihood map-making method which uses B-splines to model and remove the atmospheric signal. It has been used to make high-precision beam maps from which we determine the experiment's window functions. This beam information directly impacts all subsequent analyses of the data. We also used the method to map a sample of galaxy clusters via the Sunyaev-Zel'dovich (SZ) effect and show five clusters previously detected with X-ray or SZ observations. We provide integrated Compton-y measurements for each cluster. Of particular interest is our detection of the z = 0.44 component of A3128 and our current non-detection of the low-redshift part, providing strong evidence that the further cluster is more massive as suggested by X-ray measurements. This is a compelling example of the redshift-independent mass selection of the SZ effect. C1 [Hincks, A. D.; Appel, J. W.; Das, S.; Dunkley, J.; Essinger-Hileman, T.; Fisher, R. P.; Fowler, J. W.; Hajian, A.; Lau, J. M.; Limon, M.; Martocci, K.; Niemack, M. D.; Page, L. A.; Parker, L.; Reid, B.; Staggs, S. T.; Stryzak, O.; Switzer, E. R.; Zhao, Y.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Acquaviva, V.; Hughes, J. P.; Menanteau, F.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Acquaviva, V.; Das, S.; Dunkley, J.; Hajian, A.; Lin, Y. -T.; Lupton, R. H.; Marriage, T. A.; Spergel, D. N.; Trac, H.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Ade, P. A. R.; Mauskopf, P.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aguirre, P.; Barrientos, L. F.; Duenner, R.; Infante, L.; Juin, J. B.; Lin, Y. -T.; Quintana, H.] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Amiri, M.; Battistelli, E. S.; Burger, B.; Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Battistelli, E. S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Bond, J. R.; Hajian, A.; Nolta, M. R.; Sievers, J.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Brown, B.; Kosowsky, A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Chervenak, J.; Moseley, H.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Das, S.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Das, S.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Devlin, M. J.; Dicker, S. R.; Kaul, M.; Klein, J.; Limon, M.; Marsden, D.; Swetz, D. S.; Thornton, R.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Doriese, W. B.; Hilton, G. C.; Irwin, K. D.; Niemack, M. D.; Swetz, D. S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Dunkley, J.; Hlozek, R.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Hernandez-Monteagudo, C.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hilton, M.; Moodley, K.; Warne, R.] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Hilton, M.; Moodley, K.] Ctr High Performance Comp, Cape Town, South Africa. [Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Hughes, D. H.] INAOE, Puebla, Mexico. [Lau, J. M.; Sehgal, N.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Jimenez, R.; Reid, B.; Verde, L.] Univ Barcelona, ICREA, E-08028 Barcelona, Spain. [Jimenez, R.; Reid, B.; Verde, L.] Univ Barcelona, ICC, E-08028 Barcelona, Spain. [Lau, J. M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Lin, Y. -T.] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan. [Marriage, T. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Martocci, K.; Switzer, E. R.] Kavli Inst Cosmol Phys, Lab Astrophys & Space Res, Chicago, IL 60637 USA. [Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Partridge, B.] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Thornton, R.] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA. [Trac, H.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wilson, G.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Hincks, AD (reprint author), Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA. RI Moseley, Harvey/D-5069-2012; Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; OI Verde, Licia/0000-0003-2601-8770; Jimenez, Raul/0000-0002-3370-3103; Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Huffenberger, Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074; Limon, Michele/0000-0002-5900-2698 FU National Aeronautics and Space Administration; U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731, PIRE-0507768]; Princeton University; University of Pennsylvania; Natural Science and Engineering Research Council of Canada (NSERC); NSF [AST-0546035, AST-0606975, AST 0707731]; FONDAP Centro de Astrofisica; NSF Physics Frontier Center [PHY-0114422]; South African National Research Foundation (NRF); Meraka Institute; Rhodes Trust; FONDECYT [3085031]; [FP7-PEOPLE-2007-4-3 IRG]; [202182] FX The ACT project was proposed in 2000 and funded 2004 January 1. Many have contributed to the project since its inception. We especially wish to thank Asad Aboobaker, Christine Allen, Dominic Benford, Paul Bode, Kristen Burgess, Angelica de Oliveria-Costa, Peter Hargrave, Norm Jarosik, Amber Miller, Carl Reintsema, Uros Seljak, Martin Spergel, Johannes Staghun, Carl Stahle, Max Tegmark, Masao Uehara, and Ed Wishnow. It is a pleasure to acknowledge Bob Margolis, ACT's project manager. Reed Plimpton and David Jacobson worked at the telescope during the 2008 season. ACT is on the Chajnantor Science preserve which was made possible by CONICYT. We are grateful for the assistance we received at various times from the ALMA, APEX, ASTE, CBI/QUIET, and NANTEN2 groups. The PWV data come from the public APEX weather site. Field operations were based at the Don Esteban facility run by Astro-Norte. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Satoshi Nozawa and Naoki Itoh kindly shared their code for calculating relativistic corrections to the SZ effect. We also thank William Holzapfel and an anonymous referee who provided helpful feedback on an earlier version of this paper. We thank the members of our external advisory board-Tom Herbig (chair), Charles Alcock, Walter Gear, Cliff Jackson, Amy Newbury, and Paul Steinhardt-who helped guide the project to fruition. This work was supported by the U.S. National Science Foundation through awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731, and PIRE-0507768. Funding was also provided by Princeton University and the University of Pennsylvania. A.D.H. received additional support from a Natural Science and Engineering Research Council of Canada (NSERC) PGS-D scholarship. A.K. and B.P. were partially supported through NSF AST-0546035 and AST-0606975, respectively, for work on ACT. H.Q. and L.I. acknowledge partial support from FONDAP Centro de Astrofisica. E.S. acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics. K.M., M.H., and R.W. received financial support from the South African National Research Foundation (NRF), the Meraka Institute via funding for the South African Centre for High Performance Computing (CHPC), and the South African Square Kilometer Array (SKA) Project. R.H. received funding from the Rhodes Trust. L.V. acknowledges support from NSF-AST 0707731 and FP7-PEOPLE-2007-4-3 IRG no. 202182. J.B.J. acknowledges for support from FONDECYT (no. 3085031). NR 70 TC 57 Z9 59 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2010 VL 191 IS 2 BP 423 EP 438 DI 10.1088/0067-0049/191/2/423 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 692VY UT WOS:000285185200013 ER PT J AU Durden, SL AF Durden, Stephen L. TI Remote Sensing and Modeling of Cyclone Monica near Peak Intensity SO ATMOSPHERE LA English DT Article DE hurricane; typhoon; tropical cyclone; Cyclone Monica; remote sensing AB Cyclone Monica was an intense Southern Hemisphere tropical cyclone of 2006. Although no in situ measurements of Monica's inner core were made, microwave, infrared, and visible satellite instruments observed Monica before and during peak intensity through landfall on Australia's northern coast. The author analyzes remote sensing measurements in detail to investigate Monica's intensity. While Dvorak analysis of its imagery argues that it was of extreme intensity, infrared and microwave soundings indicate a somewhat lower intensity, especially as it neared landfall. The author also describes several numerical model runs that were made to investigate the maximum possible intensity for the observed environmental conditions; these simulations also suggest a lower intensity than estimates from Dvorak analysis alone. Based on the evidence from the various measurements and modeling, the estimated range for the minimum sea level pressure at peak intensity is 900 to 920 hPa. The estimated range for the one-minute averaged maximum wind speed at peak intensity is 72 to 82 m/s. These maxima were likely reached about 24 hours prior to landfall, with some weakening occurring afterward. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Durden, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sdurden@jpl.nasa.gov NR 46 TC 2 Z9 2 U1 0 U2 3 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2073-4433 J9 ATMOSPHERE-BASEL JI Atmosphere PD DEC PY 2010 VL 1 IS 1 BP 15 EP 33 DI 10.3390/atmos1010015 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA V29EP UT WOS:000208732000003 ER PT J AU Menzies, T Jalali, O Hihn, J Baker, D Lum, K AF Menzies, Tim Jalali, Omid Hihn, Jairus Baker, Dan Lum, Karen TI Stable rankings for different effort models SO AUTOMATED SOFTWARE ENGINEERING LA English DT Article DE COCOMO; Effort estimation; Data mining; Evaluation ID SOFTWARE COST ESTIMATION; SELECTION AB There exists a large and growing number of proposed estimation methods but little conclusive evidence ranking one method over another. Prior effort estimation studies suffered from "conclusion instability", where the rankings offered to different methods were not stable across (a) different evaluation criteria; (b) different data sources; or (c) different random selections of that data. This paper reports a study of 158 effort estimation methods on data sets based on COCOMO features. Four "best" methods were detected that were consistently better than the "rest" of the other 154 methods. These rankings of "best" and "rest" methods were stable across (a) three different evaluation criteria applied to (b) multiple data sets from two different sources that were (c) divided into hundreds of randomly selected subsets using four different random seeds. Hence, while there exists no single universal "best" effort estimation method, there appears to exist a small number (four) of most useful methods. This result both complicates and simplifies effort estimation research. The complication is that any future effort estimation analysis should be preceded by a "selection study" that finds the best local estimator. However, the simplification is that such a study need not be labor intensive, at least for COCOMO style data sets. C1 [Menzies, Tim; Jalali, Omid; Baker, Dan] W Virginia Univ, Lane Dept Comp Sci & Elect Engn, Morgantown, WV 26506 USA. [Hihn, Jairus; Lum, Karen] NASA, Jet Prop Lab, Pasadena, CA USA. RP Menzies, T (reprint author), W Virginia Univ, Lane Dept Comp Sci & Elect Engn, Morgantown, WV 26506 USA. EM tim@menzies.us; ojalali@mix.wvu.edu; jhihn@mail3.jpl.nasa.gov; danielryanbaker@gmail.com; karen.t.lum@jpl.nasa.gov FU US National Aeronautics and Space Administration FX The research described in this paper was carried out at West Virginia University and the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the US National Aeronautics and Space Administration. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise does not constitute or imply its endorsement by the US Government. NR 53 TC 17 Z9 17 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0928-8910 J9 AUTOMAT SOFTW ENG JI Automat. Softw. Eng. PD DEC PY 2010 VL 17 IS 4 BP 409 EP 437 DI 10.1007/s10515-010-0070-z PG 29 WC Computer Science, Software Engineering SC Computer Science GA 630EZ UT WOS:000280257100003 ER PT J AU Gay, G Menzies, T Davies, M Gundy-Burlet, K AF Gay, Gregory Menzies, Tim Davies, Misty Gundy-Burlet, Karen TI Automatically finding the control variables for complex system behavior SO AUTOMATED SOFTWARE ENGINEERING LA English DT Article DE Contrast-set learning; Search-based software engineering; Simulation; Optimization; Monte Carlo filtering ID MONTE-CARLO; MODELS; UNCERTAINTY; RULES AB Testing large-scale systems is expensive in terms of both time and money. Running simulations early in the process is a proven method of finding the design faults likely to lead to critical system failures, but determining the exact cause of those errors is still time-consuming and requires access to a limited number of domain experts. It is desirable to find an automated method that explores the large number of combinations and is able to isolate likely fault points. Treatment learning is a subset of minimal contrast-set learning that, rather than classifying data into distinct categories, focuses on finding the unique factors that lead to a particular classification. That is, they find the smallest change to the data that causes the largest change in the class distribution. These treatments, when imposed, are able to identify the factors most likely to cause a mission-critical failure. The goal of this research is to comparatively assess treatment learning against state-of-the-art numerical optimization techniques. To achieve this, this paper benchmarks the TAR3 and TAR4.1 treatment learners against optimization techniques across three complex systems, including two projects from the Robust Software Engineering (RSE) group within the National Aeronautics and Space Administration (NASA) Ames Research Center. The results clearly show that treatment learning is both faster and more accurate than traditional optimization methods. C1 [Gay, Gregory; Menzies, Tim] W Virginia Univ, Morgantown, WV 26506 USA. [Davies, Misty; Gundy-Burlet, Karen] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gay, G (reprint author), W Virginia Univ, Morgantown, WV 26506 USA. EM greg@greggay.com; tim@menzies.us; misty.d.davies@nasa.gov; karen.gundy-burlet@nasa.gov OI Davies, Misty/0000-0002-6245-9568; Gay, Gregory/0000-0001-6794-9585 FU National Aeronautics and Space Administration FX This research was conducted at West Virginia University and the Ames Research Center under a contract with the National Aeronautics and Space Administration. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government. NR 58 TC 7 Z9 7 U1 3 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0928-8910 J9 AUTOMAT SOFTW ENG JI Automat. Softw. Eng. PD DEC PY 2010 VL 17 IS 4 BP 439 EP 468 DI 10.1007/s10515-010-0072-x PG 30 WC Computer Science, Software Engineering SC Computer Science GA 630EZ UT WOS:000280257100004 ER PT J AU De Witt, JK Perusek, GP Lewandowski, BH Gilkey, KM Savina, MC Samorezov, S Edwards, WB AF De Witt, John K. Perusek, Gail P. Lewandowski, Beth H. Gilkey, Kelly M. Savina, Mark C. Samorezov, Sergey Edwards, W. Brent TI Locomotion in Simulated and Real Microgravity: Horizontal Suspension vs. Parabolic Flight SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE biomechanics; ground reaction forces; kinematics ID GROUND REACTION FORCES; GRAVITY REPLACEMENT AB Introduction The effect of reducing gravity on locomotion has been studied using microgravity analogues However there is no known literature comparing locomotion in actual microgravity (AM) to locomotion in simulated microgravity (SM) Methods Five subjects were tested while walking at 1 34 m s(-1) and running at 3 13 m s(-1) on a treadmill during parabolic flight and on a microgravity simulator The external load (EL) in AM and SM was provided by elastomer bungees at approximately 55% (low) and (high of the subjects bodyweight (BW) lower body joint kinematics and ground reaction forces were measured during each condition Effect size and its 95% confidence interval were computed between gravitational conditions for each outcome variable Results In AM, subjects attained approximately 15-21 degrees greater hip flex ton during walking and 19-25 degrees greater hip flexion during running Hip range of motion was greater in AM during running by approximately 12-17 degrees Trunk motion was 4 degrees less in SM than AM during walking Peak impact force was greater in SM than in AM during walking with a low EL (SM = 0 95 +/- 0 04 BW AM = 0 76 +/- 0 04 BW and contact times were greater in SM Conclusions Subtle differences exist in locomotion pat terns temporal kinematics and peak impact ground reaction forces be tween AM and SM The differences suggest possible adaptations in the motor coordination required between gravitational condition, and potential differences in adaptations that are dependent upon it training occurs in actual or simulated microgravity C1 [De Witt, John K.] Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA. NASA, Glenn Res Ctr, Cleveland, OH USA. ZIN Technol, Cleveland, OH USA. Iowa State Univ, Ames, IA USA. RP De Witt, JK (reprint author), Wyle Integrated Sci & Engn Grp, 1290 Hercules,Ste 120, Houston, TX 77058 USA. FU NASA-Johnson Space Center FX This work is dedicated to the memory of R Donald Hagan Ph D, who left this world during the completion of this report We would like to thank the Exercise Countermeasures Program at NASA-Johnson Space Center for funding this work We would also like to thank members of the NASA JSC Exercise Physiology Laboratory and the NASA-CRC Exercise Countermeasures Laboratory for their help during data collection NR 14 TC 12 Z9 12 U1 0 U2 4 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 DEC PY 2010 VL 81 IS 12 BP 1092 EP 1099 DI 10.3357/ASEM.2413.2010 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 690EF UT WOS:000284984600004 PM 21197853 ER PT J AU Dominique, F Gerlach, CG Gopalakrishnan, N Rao, A Seymour, JP Soni, R Stolyar, A Viswanathan, H Weaver, C Weber, A AF Dominique, Francis Gerlach, Christian G. Gopalakrishnan, Nandu Rao, Anil Seymour, James P. Soni, Robert Stolyar, Aleksandr Viswanathan, Harish Weaver, Carl Weber, Andreas TI Self-Organizing Interference Management for LTE SO BELL LABS TECHNICAL JOURNAL LA English DT Article AB In orthogonal frequency division multiple access (OFDMA) systems such as Long Term Evolution (LTE), it is extremely important to reduce interference between neighboring cells, especially for cell edge users, since the only interference in LTE is inter-cell interference due to the orthogonality of the sub-carriers used in the transmissions. This paper describes a few self-organizing and self-optimizing techniques to manage and reduce this inter-cell interference. These self-optimizing network (SON)-based techniques are inter-cell interference coordination (ICIC) and uplink (UL) interference over thermal (IoT) control. Simulation results are presented showing the improvements that can be obtained with the use of such techniques in interference limited operating scenarios. (C) 2010 Alcatel-Lucent. C1 [Gerlach, Christian G.] Alcatel Lucent Bell Labs, MAC, Stuttgart, Germany. [Gerlach, Christian G.] Alcatel Lucent Bell Labs, Adv Packet Scheduler Dept, Stuttgart, Germany. [Gerlach, Christian G.] Texas Instruments Inc, Dallas, TX 75265 USA. [Rao, Anil] NASA, Jet Prop Lab, Washington, DC USA. [Seymour, James P.] Alcatel Lucent Wireless Networks CTO Org, RAN Strategy, Naperville, IL USA. [Soni, Robert] Alcatel Lucents Wireless Business Grp, Murray Hill, NJ USA. [Soni, Robert] Columbia Univ, New York, NY USA. [Soni, Robert] New Jersey Inst Technol, Newark, NJ 07102 USA. [Viswanathan, Harish] Alcatel Lucent Bell Labs CTO Org, CTO Advisory Grp, Murray Hill, NJ USA. [Weber, Andreas] Alcatel Lucent Bell Labs, Mobile Syst Performance Evaluat Grp, Stuttgart, Germany. [Gerlach, Christian G.] Alcatel Res, Stuttgart, Germany. [Rao, Anil] Natl Sci Fdn, Arlington, VA 22230 USA. [Weaver, Carl] Raytheon Co, Terr Point To Point Microwave Syst, Waltham, MA USA. [Weaver, Carl] Raytheon Co, Secure Satellite Commun Syst, Waltham, MA USA. [Weaver, Carl] Raytheon Co, Space Based Radar, Waltham, MA USA. NR 8 TC 3 Z9 3 U1 0 U2 3 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1089-7089 J9 BELL LABS TECH J JI Bell Labs Tech. J. PD DEC PY 2010 VL 15 IS 3 BP 19 EP 42 DI 10.1002/bltj.20455 PG 24 WC Computer Science, Information Systems; Engineering, Electrical & Electronic; Telecommunications SC Computer Science; Engineering; Telecommunications GA 685TZ UT WOS:000284652300003 ER PT J AU Gerlach, CG Karla, I Weber, A Ewe, L Bakker, H Kuehn, E Rao, A AF Gerlach, Christian G. Karla, Ingo Weber, Andreas Ewe, Lutz Bakker, Hajo Kuehn, Edgar Rao, Anil TI ICIC in DL and UL With Network Distributed and Self-Organized Resource Assignment Algorithms in LTE SO BELL LABS TECHNICAL JOURNAL LA English DT Article ID INTERFERENCE COORDINATION AB Inter-cell Interference coordination (ICIC) has gained much interest in the 3rd Generation Partnership Project's (3GPP's) Long Term Evolution (LTE) standardization of a new air interface. Due to the new physical layer, interference can now be predicted and avoided on a frequency basis. Such schemes are based on cell wise usage restrictions or resource preferences. After explaining the general degrees of freedom, we present an "inverted" reuse scheme for downlink and uplink and explain its advantages. This is supported by 3GPP-compliant system simulations. The question of assignment of restrictions or preferences naturally leads to a need for self-organization. For that, the concept of semi-static ICIC based on a request-grant mechanism applicable to load balancing is explained. For the static ICIC case with frequency planning, a novel and fully distributed algorithm provides optimized assignment of resource restrictions to the cells in a self-organizing way. It is capable of resolving sub-optimal aspects and comprises methods to detect and prevent possible system instabilities. The algorithms presented lead to an integrated ICIC-self-organizing network (SON) concept that can be realized in a multi-cell network solution. (C) 2010 Alcatel-Lucent. C1 [Gerlach, Christian G.] Alcatel Lucent Bell Labs, MAC, Stuttgart, Germany. [Gerlach, Christian G.] Alcatel Lucent Bell Labs, Adv Packet Scheduler Dept, Stuttgart, Germany. [Gerlach, Christian G.] Texas Instruments Inc, Dallas, TX USA. [Gerlach, Christian G.] Alcatel Res, Stuttgart, Germany. [Karla, Ingo; Ewe, Lutz; Kuehn, Edgar] Alcatel Lucent Bell Labs, Radio Syst Optimizat Dept, Stuttgart, Germany. [Weber, Andreas] Alcatel Lucent Bell Labs, Mobile Syst Performance Evaluat Grp, Stuttgart, Germany. [Karla, Ingo; Weber, Andreas; Kuehn, Edgar] Bell Labs, Murray Hill, NJ USA. [Bakker, Hajo] Alcatel Lucent Bell Labs, Syst Optimizat Dept, Stuttgart, Germany. [Rao, Anil] Natl Sci Fdn, Arlington, VA 22230 USA. [Rao, Anil] NASA, Jet Prop Lab, Washington, DC USA. RP Gerlach, CG (reprint author), Alcatel Lucent Bell Labs, MAC, Stuttgart, Germany. NR 41 TC 14 Z9 14 U1 0 U2 9 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1089-7089 J9 BELL LABS TECH J JI Bell Labs Tech. J. PD DEC PY 2010 VL 15 IS 3 BP 43 EP 62 DI 10.1002/bltj.20456 PG 20 WC Computer Science, Information Systems; Engineering, Electrical & Electronic; Telecommunications SC Computer Science; Engineering; Telecommunications GA 685TZ UT WOS:000284652300004 ER PT J AU Chang, R Emami, K Wu, HL Sun, W AF Chang, Robert Emami, Kamal Wu, Honglu Sun, Wei TI Biofabrication of a three-dimensional liver micro-organ as an in vitro drug metabolism model SO BIOFABRICATION LA English DT Article ID CELL-CULTURE ANALOG; MICROFLUIDIC CHANNELS; HEPATOCYTE CULTURE; DISCOVERY; FABRICATION; BIOREACTOR; CHALLENGES; DEPOSITION; SCAFFOLDS; HYDROGEL AB In their normal in vivo matrix milieu, tissues assume complex well-organized three-dimensional architectures. Therefore, the primary aim in the tissue engineering design process is to fabricate an optimal analog of the in vivo scenario. This challenge can be addressed by applying emerging layered biofabrication approaches in which the precise configuration and composition of cells and bioactive matrix components can recapitulate the well-defined three-dimensional biomimetic microenvironments that promote cell-cell and cell-matrix interactions. Furthermore, the advent of and refinements in microfabricated systems can present physical and chemical cues to cells in a controllable and reproducible fashion unmatched with conventional cultures, resulting in the precise construction of engineered biomimetic microenvironments on the cellular length scale in geometries that are readily parallelized for high throughput in vitro models. As such, the convergence of layered solid freeform fabrication (SFF) technologies along with microfabrication techniques enables the creation of a three-dimensional micro-organ device to serve as an in vitro platform for cell culture, drug screening or to elicit further biological insights, particularly for NASA's interest in a flight-suitable high-fidelity microscale platform to study drug metabolism in space and planetary environments. The proposed model in this paper involves the combinatorial setup of an automated syringe-based, layered direct cell writing bioprinting process with micro-patterning techniques to fabricate a microscale in vitro device housing a chamber of bioprinted three-dimensional liver cell-encapsulated hydrogel-based tissue constructs in defined design patterns that biomimic the cell's natural microenvironment for enhanced biological functionality. In order to assess the structural formability and biological feasibility of such a micro-organ, reproducibly fabricated tissue constructs were biologically characterized for liver cell-specific function. Another key facet of the in vivo microenvironment that was recapitulated with the in vitro system included the necessary dynamic perfusion of the three-dimensional microscale liver analog with cells probed for their collective drug metabolic function and suitability as a drug metabolism model. This paper details the principles and methods that undergird the direct cell writing biofabrication process development and adaptation of microfluidic devices for the creation of a drug screening model, thereby establishing a novel drug metabolism study platform for NASA's interest to adopt a microfluidic microanalytical device with an embedded three-dimensional microscale liver tissue analog to assess drug pharmacokinetic profiles in planetary environments. C1 [Chang, Robert; Sun, Wei] Drexel Univ, Dept Mech Engn & Mech, Philadelphia, PA 19104 USA. [Emami, Kamal; Wu, Honglu] NASA, Lyndon B Johnson Space Ctr, Radiat Biophys Lab, Human Adaptat & Countermeasures Off, Houston, TX 77058 USA. RP Sun, W (reprint author), Drexel Univ, Dept Mech Engn & Mech, Philadelphia, PA 19104 USA. EM rcc34@drexel.edu; kamal.emami-1@nasa.gov; honglu.wu-1@nasa.gov; sunwei@drexel.edu FU NASA USRA [09940-008] FX Support from NASA USRA subcontract grant no 09940-008 to this research was acknowledged. NR 34 TC 52 Z9 56 U1 10 U2 89 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1758-5082 J9 BIOFABRICATION JI Biofabrication PD DEC PY 2010 VL 2 IS 4 AR 045004 DI 10.1088/1758-5082/2/4/045004 PG 11 WC Engineering, Biomedical; Materials Science, Biomaterials SC Engineering; Materials Science GA 694XB UT WOS:000285334000005 PM 21079286 ER PT J AU Andersen, MPS Sander, SP Nielsen, OJ Wagner, DS Sanford, TJ Wallington, TJ AF Andersen, M. P. Sulbaek Sander, S. P. Nielsen, O. J. Wagner, D. S. Sanford, T. J., Jr. Wallington, T. J. TI Inhalation anaesthetics and climate change(dagger) SO BRITISH JOURNAL OF ANAESTHESIA LA English DT Article DE global warming potential; greenhouse gas; infrared absorption; radiative forcing; spectra ID OH RADICALS; ATMOSPHERIC CHEMISTRY; INHALED ANESTHETICS; RATE CONSTANTS; CL ATOMS; LIFETIMES AB Although the increasing abundance of CO(2) in our atmosphere is the main driver of the observed climate change, it is the cumulative effect of all forcing agents that dictate the direction and magnitude of the change, and many smaller contributors are also at play. Isoflurane, desflurane, and sevoflurane are widely used inhalation anaesthetics. Emissions of these compounds contribute to radiative forcing of climate change. To quantitatively assess the impact of the anaesthetics on the forcing of climate, detailed information on their properties of heat (infrared, IR) absorption and atmospheric lifetimes are required. We have measured the IR spectra of these anaesthetics and conducted calculations of their contribution to radiative forcing of climate change recognizing the important fact that radiative forcing is strongly dependent on the wavelength of the absorption features. Radiative efficiencies of 0.453, 0.469, and 0.351 W m(-2) ppb(-1) and global warming potentials (GWPs) of 510, 1620, and 210 (100 yr time horizon) were established for isoflurane, desflurane, and sevoflurane, respectively. On the basis of the derived 100 yr GWPs, the average climate impact per anaesthetic procedure at the University of Michigan is the same as the emission of similar to 22 kg CO(2). We estimate that the global emissions of inhalation anaesthetics have a climate impact which is comparable with that from the CO(2) emissions from one coal-fired power plant or 1 million passenger cars. C1 [Andersen, M. P. Sulbaek; Sander, S. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nielsen, O. J.] Univ Copenhagen, Dept Chem, DK-2100 Copenhagen, Denmark. [Wagner, D. S.] Univ Michigan, Coll Pharm, Dept Clin Sci, Ann Arbor, MI 48109 USA. [Sanford, T. J., Jr.] Univ Michigan, Dept Anesthesiol, Sch Med, Ann Arbor, MI 48109 USA. [Wallington, T. J.] Ford Motor Co, Syst Analyt & Environm Sci Dept, Dearborn, MI 48121 USA. RP Andersen, MPS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 183-901, Pasadena, CA 91109 USA. EM mads@sulbaek.dk RI Sulbaek Andersen, Mads/C-4708-2008; Nielsen, Ole/B-9988-2011 OI Sulbaek Andersen, Mads/0000-0002-7976-5852; Nielsen, Ole/0000-0002-0088-3937 FU National Aeronautics and Space Administration; Danish Natural Science Research Council; Villum Kann Rasmussen Foundation for the Copenhagen Center for Atmospheric Research (CCAR); EUROCHAMP2 FX This work was performed partly at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank David Wallington for a careful reading of the manuscript.; O.J.N. acknowledges financial support from the Danish Natural Science Research Council, EUROCHAMP2, and the Villum Kann Rasmussen Foundation for the Copenhagen Center for Atmospheric Research (CCAR). M. P. S. A. is supported by an appointment to the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. NR 22 TC 23 Z9 23 U1 0 U2 10 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0007-0912 J9 BRIT J ANAESTH JI Br. J. Anaesth. PD DEC PY 2010 VL 105 IS 6 BP 760 EP 766 DI 10.1093/bja/aeq259 PG 7 WC Anesthesiology SC Anesthesiology GA 682VR UT WOS:000284431600005 ER PT J AU Masunaga, H Matsui, T Tao, WK Hou, AY Kummerow, CD Nakajima, T Bauer, P Olson, WS Sekiguchi, M Nakajima, TY AF Masunaga, Hirohiko Matsui, Toshihisa Tao, Wei-kuo Hou, Arthur Y. Kummerow, Christian D. Nakajima, Teruyuki Bauer, Peter Olson, William S. Sekiguchi, Miho Nakajima, Takashi Y. TI Satellite Data Simulator Unit A Multisensor, Multispectral Satellite Simulator Package SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID RADIATIVE-TRANSFER; PRECIPITATION PROFILES; RADIANCE OBSERVATIONS; RETRIEVAL; ALGORITHM; RADAR; ASSIMILATION; MODEL C1 [Masunaga, Hirohiko] Nagoya Univ, Hydrospher Atmospher Res Ctr, Nagoya, Aichi 4648601, Japan. [Matsui, Toshihisa; Tao, Wei-kuo; Hou, Arthur Y.; Olson, William S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kummerow, Christian D.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Nakajima, Teruyuki] Univ Tokyo, Atmosphere & Ocean Res Inst, Chiba, Japan. [Bauer, Peter] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Sekiguchi, Miho] Tokyo Univ Marine Sci & Technol, Fac Marine Technol, Tokyo, Japan. [Nakajima, Takashi Y.] Tokai Univ, Res & Informat Ctr, Tokyo 151, Japan. RP Masunaga, H (reprint author), Nagoya Univ, Hydrospher Atmospher Res Ctr, F3-1 200 Furocho Chikusa Ku, Nagoya, Aichi 4648601, Japan. EM masunaga@hyarc.nagoya-u.ac.jp RI Masunaga, Hirohiko/C-2488-2008; Nakajima, Takashi/C-2747-2009; Hou, Arthur/D-8578-2012; Nakajima, Teruyuki/H-2370-2013; PMM, JAXA/K-8537-2016 OI Masunaga, Hirohiko/0000-0002-6336-5002; Nakajima, Teruyuki/0000-0002-9042-504X; NR 18 TC 32 Z9 33 U1 0 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD DEC PY 2010 VL 91 IS 12 BP 1625 EP 1632 DI 10.1175/2010BAMS2809.1 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 707TI UT WOS:000286310600001 ER PT J AU Hurrell, JW Meehl, GA Bader, D Delworth, TL Kirtman, B Wielick, B AF Hurrell, James W. Meehl, Gerald A. Bader, Dave Delworth, Thomas L. Kirtman, Ben Wielick, Bruce TI Comments on "A Unified Modeling Approach to Climate System Prediction" Reply SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Editorial Material C1 [Hurrell, James W.; Meehl, Gerald A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Bader, Dave] Oak Ridge Natl Lab, Oak Ridge, TN USA. [Delworth, Thomas L.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Kirtman, Ben] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Kirtman, Ben] Ctr Ocean Land Atmosphere Studies, Calverton, MD USA. [Wielick, Bruce] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Hurrell, JW (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. RI Bader, David/H-6189-2011; Delworth, Thomas/C-5191-2014 OI Bader, David/0000-0003-3210-339X; NR 7 TC 2 Z9 2 U1 0 U2 7 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD DEC PY 2010 VL 91 IS 12 BP 1702 EP 1703 DI 10.1175/2010BAMS3118.1 PG 2 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 707TI UT WOS:000286310600009 ER PT J AU Kiely, A Xu, MS Song, WZ Huang, RJ Shirazi, B AF Kiely, Aaron Xu, Mingsen Song, Wen-Zhan Huang, Renjie Shirazi, Behrooz TI Adaptive Linear Filtering Compression on Realtime Sensor Networks SO COMPUTER JOURNAL LA English DT Article DE adaptive linear filtering compression (ALFC); lossless compression; wireless sensor networks ID WAVE-FORM DATA; LOSSLESS COMPRESSION; TRANSMISSION; ALGORITHM; STORAGE AB We present a lightweight lossless compression algorithm for realtime sensor networks. Our proposed adaptive linear filtering compression (ALFC) algorithm performs predictive compression using adaptive linear filtering to predict sample values followed by entropy coding of prediction residuals, encoding a variable number of samples into fixed-length packets. Adaptive prediction eliminates the need to determine prediction coefficients a priori and, more importantly, allows compression to dynamically adjust to a changing source. The algorithm requires only integer arithmetic operations and thus is compatible with sensor platforms that do not support floating-point operations. Significant robustness to packets losses is provided by including small but sufficient overhead data to allow each packet to be independently decoded. Real-world evaluations on seismic data from a wireless sensor network testbed show that ALFC provides more effective compression and uses less resources than an alternative recent work of lossless compression, S-LZW. Experiments in a multi-hop sensor network also show that ALFC can significantly improve raw data throughput and energy efficiency. We also implement the algorithm in our real sensor network, and show that our linear prediction based compression algorithm significantly improves data reliability and network efficiency. C1 [Xu, Mingsen; Song, Wen-Zhan; Huang, Renjie; Shirazi, Behrooz] Washington State Univ, Sensorweb Res Lab, Vancouver, WA 98686 USA. [Kiely, Aaron] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Xu, MS (reprint author), Washington State Univ, Sensorweb Res Lab, Vancouver, WA 98686 USA. EM mingsen_xu@wsu.edu FU NASA; USGS [NNX06AE42G] FX The research described in this paper was supported by NASA ESTOAIST program and USGS Volcano Hazard program under the research grant NNX06AE42G. NR 38 TC 2 Z9 2 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0010-4620 J9 COMPUT J JI Comput. J. PD DEC PY 2010 VL 53 IS 10 BP 1606 EP 1620 DI 10.1093/comjnl/bxp128 PG 15 WC Computer Science, Hardware & Architecture; Computer Science, Information Systems; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA 689UG UT WOS:000284954700005 ER PT J AU Vargas-Angel, B AF Vargas-Angel, Bernardo TI Crustose coralline algal diseases in the US-Affiliated Pacific Islands SO CORAL REEFS LA English DT Article DE US Pacific; Crustose coralline algae; Disease; CLOD; Fungal disease ID GREAT-BARRIER-REEF; NORTHWESTERN HAWAIIAN-ISLANDS; BLACK-BAND DISEASE; PRODUCTIVITY; SETTLEMENT; COMMUNITIES; PREVALENCE; PATHOGEN; ECOLOGY; CLOD AB Despite the critical role of crustose coralline algae (CCA) in coral reef formation, maintenance, and ecology, little is known about coralline algal disease abundance, distribution, etiology, or the potential implications of declining CCA flora. This paper presents the first quantitative study of CCA disease on U.S. Pacific coral reefs, based on Rapid Ecological Assessments conducted at 337 discrete sites, at 42 different U.S.-Affiliated Pacific Islands and Atolls, within 5 major geographical regions: main Hawaiian Islands, Northwestern Hawaiian Islands, American Samoa, the Pacific Remote Island Areas (PRIA), and Guam and the Commonwealth of the Northern Mariana Islands (CNMI). Five major disease categories were enumerated, and a disease occurrence index was estimated, based on case counts relative to percent CCA cover. CCA disease occurrence exhibited considerable spatial variability both between and within islands/atolls, with some regions being disproportionately affected by disease. No diseases were observed at remote Johnston and Wake Atolls, or the main Hawaiian Islands. Diseases were rare in the Northwestern Hawaiian Islands and the Northern Mariana Islands; occasional to common around the PRIA, and common to abundant in American Samoa, Guam, and the Southern Mariana Islands. Pacific-wide, disease occurrence was statistically associated with CCA percent cover and sea surface temperatures (SSTs) but not with human population density; nonetheless, disease occurrence and population density were statistically correlated for those islands containing disease. Although Pacific-wide, the occurrence of disease was low, with no active outbreaks detected in any region, hot spots of disease were detected around Guam, the southern CNMI, American Samoa, and the PRIA. The high levels of spatial and temporal variability in disease occurrence herein underscore the patchy nature and fluctuating distribution dynamics of these afflictions. Also, the widespread dispersal capabilities and extraordinary infective properties of some of these pathogens highlight the importance of better understanding CCA disease dynamics and discerning the relative threat levels on coral reef ecosystems. C1 Univ Hawaii, Joint Inst Marine & Atmospher Res, Natl Ocean & Atmospher Adm,Coral Reef Ecosyst Div, Natl Marine Fisheries Serv,Pacif Isl Fisheries Sc, Honolulu, HI 96814 USA. RP Vargas-Angel, B (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, Natl Ocean & Atmospher Adm,Coral Reef Ecosyst Div, Natl Marine Fisheries Serv,Pacif Isl Fisheries Sc, 1125 B Ala Moana Blvd, Honolulu, HI 96814 USA. EM Bernardo.VargasAngel@noaa.gov FU NOAA; NOAA Pacific Islands Fisheries Science Center's Coral Reef Ecosystem Division; NOAA Ship Hi'ialakai FX This work was supported by the NOAA Coral Reef Conservation Program. Institutional, logistic, and financial support were also provided by the NOAA Pacific Islands Fisheries Science Center's Coral Reef Ecosystem Division. Permission to work in different geographical regions was granted by: State of Hawaii Department of Land and Aquatic Resources, Papahanaumokuakea Marine National Monument, U. S. Fish and Wildlife Service, U. S. Air Force, American Samoa Department of Marine and Wildlife Resources, Fagatele Bay National Marine Sanctuary, U. S. National Park Service, Guam Department of Aquatic and Wildlife Resources, CNMI Department of Environmental Quality, and CNMI Coastal Resources Management Office. The officers and crew of the NOAA Ship Hi'ialakai are also gratefully acknowledged for support with dive and small boat operations. B Wheeler and J Kenyon assisted with a portion of data collection around the main Hawaiian Islands (2006) and American Samoa (2008), respectively. F Mancini extracted and compiled island-wide, mean annual SSTs based on NOAA's array of subsurface temperature recorder instrumentation deployed at selected locations across the U. S. Pacific Islands. M Littler provided support with disease identification and R Riosmena with selected CCA taxa identification. S Schopmeyer, J Helyer and E Looney assisted with disease data compilation; K Grimshaw, E Looney, T Acoba, and A Toperoff provided assistance with preparation of figures. The author also wants to thank E Looney, C Richards, P Vroom, and R Brainard, as well as three anonymous reviewers, whose comments improved this manuscript. NR 46 TC 13 Z9 13 U1 0 U2 14 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD DEC PY 2010 VL 29 IS 4 BP 943 EP 956 DI 10.1007/s00338-010-0646-x PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 676TE UT WOS:000283940700016 ER PT J AU Gibson, EK Pillinger, CT Waugh, LJ AF Gibson, Everett K. Pillinger, Colin T. Waugh, Lester J. TI Lunar Beagle and Lunar Astrobiology SO EARTH MOON AND PLANETS LA English DT Article DE Lunar astrobiology; Beagle 2; Lunar beagle; Volatiles; Polar volatiles; Lunar exosphere; Solar wind ID WATER-ICE; SOUTH-POLE; MOON; DEPOSITS; SURFACE; ATMOSPHERE; SOIL AB The study of the elements and molecules of astrobiological interest on the Moon can be made with the Gas Analysis Package (GAP) and associated instruments developed for the Beagle 2 Mars Express Payload. The permanently shadowed polar regions of the Moon may offer a unique location for the "cold-trapping" of the light elements (i.e. H, C, N, O, etc.) and their simple compounds. Studies of the returned lunar samples have shown that lunar materials have undergone irradiation with the solar wind and adsorb volatiles from possible cometary and micrometeoroid impacts. The Beagle 2's analytical instrument package including the sample processing facility and the GAP mass spectrometer can provide vital isotopic information that can distinguish whether the lunar volatiles are indigenous to the moon, solar wind derived, cometary in origin or from meteoroids impacting on the Moon. As future Lunar Landers are being considered, the suite of instruments developed for the Mars Beagle 2 lander can be consider as the baseline for any lunar volatile or resource instrument package. C1 [Gibson, Everett K.] NASA, KR, Astromat Res Off, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Pillinger, Colin T.] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. [Waugh, Lester J.] EADS Astrium Ltd, Stevenage SG1 2AS, Herts, England. RP Gibson, EK (reprint author), NASA, KR, Astromat Res Off, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM everett.k.gibson@nasa.gov FU The Science Mission Directorate (SMD) of NASA Headquarters; The Astromaterials Research and Space Exploration (ARES) Directorate; The Planetary Sciences and Space Research Institute of the Open University; SMD of NASA Headquarters; Planetary Sciences and Space Research Institute (PSSRI) of the Open University; EADS Astrium, Stevenage; The German Space Agency (DLR) FX The authors would like to recognize the assistance and support of their respective organizations. The Science Mission Directorate (SMD) of NASA Headquarters who funded the Lunar Science Sortie Opportunity (LSSO) Concept Study is recognized for their foresight in recognizing the need for technical and scientific study of future lunar scientific investigations (Gibson et al. 2009). The Astromaterials Research and Space Exploration (ARES) Directorate of the Johnson Space Center has provided leadership through the scientific analyses of lunar and extraterrestrial materials over the past five decades and has allowed interactions with colleagues carrying out state of the art research. The Planetary Sciences and Space Research Institute of the Open University has developed cutting edge scientific instruments for laboratory analyses and spacecraft hardware which has been sent to the outer reaches of our solar system. EADS Astrium personnel are acknowledged as leaders in the development of payloads for space exploration and satellite technology. Funding for the Concept Study "Beagle to the Moon in Search of Hydrogen, Water and Volatiles'' submitted by Everett Gibson was provided by the SMD of NASA Headquarters. Financial support from the Planetary Sciences and Space Research Institute (PSSRI) of the Open University is acknowledged. The engineering, technical and financial support of EADS Astrium, Stevenage is sincerely appreciated. Matthew Stuttard and Justin Byrne are especially recognized for their support of the Lunar Beagle Concept study. The German Space Agency (DLR) is recognized for their support of the lunar mole studies. The Intellectual Property, with respect to information supplied herein, remains vested with the UK PI and the Beagle Team. The manuscript could not have been completed without the tireless efforts of Karen Guyler, of the PSSRI. NR 46 TC 4 Z9 4 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2010 VL 107 IS 1 BP 25 EP 42 DI 10.1007/s11038-010-9364-1 PG 18 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 732FZ UT WOS:000288171700004 ER PT J AU Crawford, IA Fagents, SA Joy, KH Rumpf, ME AF Crawford, Ian A. Fagents, Sarah A. Joy, Katherine H. Rumpf, M. Elise TI Lunar Palaeoregolith Deposits as Recorders of the Galactic Environment of the Solar System and Implications for Astrobiology SO EARTH MOON AND PLANETS LA English DT Article DE Moon; Lunar regolith; Galactic history; Galactic structure; Lunar exploration; Astrobiology ID ICE-AGE EPOCHS; COSMIC-RAYS; FOSSIL DIVERSITY; MARE COGNITUM; NOBLE-GAS; MOON; STRATIGRAPHY; METEORITES; SOILS; EARTH AB One of the principal scientific reasons for wanting to resume in situ exploration of the lunar surface is to gain access to the record it contains of early Solar System history. Part of this record will pertain to the galactic environment of the Solar System, including variations in the cosmic ray flux, energetic galactic events (e.g., supernovae and/or gamma-ray bursts), and passages of the Solar System through dense interstellar clouds. Much of this record is of astrobiological interest as these processes may have affected the evolution of life on Earth, and perhaps other Solar System bodies. We argue that this galactic record, as for that of more local Solar System processes also of astrobiological interest, will be best preserved in ancient, buried regolith ('palaeoregolith') deposits in the lunar near sub-surface. Locating and sampling such deposits will be an important objective of future lunar exploration activities. C1 [Crawford, Ian A.] Univ London, Birkbeck Coll, Dept Earth & Planetary Sci, London WC1E 7HX, England. [Crawford, Ian A.; Joy, Katherine H.] UCL, UCL Birkbeck, Ctr Planetary Sci, London WC1E 6BT, England. [Fagents, Sarah A.; Rumpf, M. Elise] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Joy, Katherine H.] Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA. [Joy, Katherine H.] NASA, Lunar Sci Inst, Houston, TX USA. RP Crawford, IA (reprint author), Univ London, Birkbeck Coll, Dept Earth & Planetary Sci, Malet St, London WC1E 7HX, England. EM i.crawford@ucl.ac.uk RI Crawford, Ian/H-7510-2012; Fagents, Sarah/B-3983-2014; OI Crawford, Ian/0000-0001-5661-7403; Joy, Katherine/0000-0003-4992-8750 FU NASA [NNX08AY75G, NSF-GRFP] FX We would like to thank Robert Wimmer-Schweingruber for helpful correspondence regarding the possibility of identifying interstellar pickup ions in lunar regolith grains, and two anonymous referees for helpful comments. SAF and MER acknowledge support from the NASA Lunar Advanced Science and Exploration Research (LASER) program through grant NNX08AY75G and NSF-GRFP. This is LPI contribution number 1596. NR 63 TC 16 Z9 16 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2010 VL 107 IS 1 BP 75 EP 85 DI 10.1007/s11038-010-9358-z PG 11 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 732FZ UT WOS:000288171700008 ER PT J AU Glavin, DP Dworkin, JP Lupisella, M Williams, DR Kminek, G Rummel, JD AF Glavin, Daniel P. Dworkin, Jason P. Lupisella, Mark Williams, David R. Kminek, Gerhard Rummel, John D. TI In Situ Biological Contamination Studies of the Moon: Implications for Planetary Protection and Life Detection Missions SO EARTH MOON AND PLANETS LA English DT Article DE Moon; Contamination; Apollo; Planetary protection; Mars ID AMINO-ACIDS; LUNAR; ORGANISMS; SURVIVAL; SEARCH AB NASA and ESA have outlined visions for solar system exploration that will include a series of lunar robotic precursor missions to prepare for, and support a human return to the Moon, and future human exploration of Mars and other destinations, including possibly asteroids. One of the guiding principles for exploration is to pursue compelling scientific questions about the origin and evolution of life. The search for life on objects such as Mars will require careful operations, and that all systems be sufficiently cleaned and sterilized prior to launch to ensure that the scientific integrity of extraterrestrial samples is not jeopardized by terrestrial organic contamination. Under the Committee on Space Research's (COSPAR's) current planetary protection policy for the Moon, no sterilization procedures are required for outbound lunar spacecraft, nor is there a different planetary protection category for human missions, although preliminary COSPAR policy guidelines for human missions to Mars have been developed. Future in situ investigations of a variety of locations on the Moon by highly sensitive instruments designed to search for biologically derived organic compounds would help assess the contamination of the Moon by lunar spacecraft. These studies could also provide valuable "ground truth" data for Mars sample return missions and help define planetary protection requirements for future Mars bound spacecraft carrying life detection experiments. In addition, studies of the impact of terrestrial contamination of the lunar surface by the Apollo astronauts could provide valuable data to help refine future Mars surface exploration plans for a human mission to Mars. C1 [Glavin, Daniel P.; Dworkin, Jason P.; Lupisella, Mark; Williams, David R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kminek, Gerhard] European Space Agcy, DG X, NL-2200 AG Noordwijk, Netherlands. [Rummel, John D.] E Carolina Univ, Inst Coastal Sci & Policy, Greenville, NC 27858 USA. RP Glavin, DP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM daniel.p.glavin@nasa.gov RI Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012 OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 FU NASA Astrobiology Institute FX We appreciate the helpful comments of Ian Crawford, Everett Gibson, and one anonymous reviewer. We are grateful for support from the NASA Astrobiology Institute. NR 37 TC 1 Z9 1 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2010 VL 107 IS 1 BP 87 EP 93 DI 10.1007/s11038-010-9361-4 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 732FZ UT WOS:000288171700009 ER PT J AU Loftus, DJ Rask, JC McCrossin, CG Tranfield, EM AF Loftus, D. J. Rask, J. C. McCrossin, C. G. Tranfield, E. M. TI The Chemical Reactivity of Lunar Dust: From Toxicity to Astrobiology SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT Meeting of the Royal-Astronomical-Society CY MAY 14, 2010 CL London, ENGLAND SP Royal Astronom Soc DE Moon; Lunar dust; Chemical reactivity; Radiation; Ultraviolet light; Free radical; Hydroxyl radical ID SAMPLES; CARBON; SILICA; SPACE AB The chemical reactivity of lunar dust is an important topic of inquiry, of fundamental scientific value and of practical relevance to human exploration of the Moon. Lunar specimens brought back to Earth by the Apollo astronauts provide a key resource for ground-based studies which help to define the initial avenues of inquiry. Even among the limited samples obtained from equatorial exploration sites, however, chemical reactivity analyses indicates that lunar dust is heterogeneous, a finding that parallels heterogeneity revealed by remote sensing studies. The region-to-region variability of lunar dust argues that a full understanding of its chemical reactivity will require in situ analysis, on a region-to-region basis. The data from such investigations will help to shape our understanding of the potential for lunar dust toxicity, and will provide insight into the types of reactions that may occur with when lunar dust interacts with organic molecules on the surface of the Moon. C1 [Loftus, D. J.; Rask, J. C.; McCrossin, C. G.; Tranfield, E. M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Loftus, DJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM David.j.loftus@nasa.gov OI Tranfield, Erin/0000-0002-1542-7459 NR 32 TC 7 Z9 7 U1 2 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2010 VL 107 IS 1 BP 95 EP 105 DI 10.1007/s11038-010-9376-x PG 11 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 732FZ UT WOS:000288171700010 ER PT J AU Curtis, SA Clark, PE Marshall, JR Nuth, JA Minetto, FA Calle, CI AF Curtis, S. A. Clark, P. E. Marshall, J. R. Nuth, J. A. Minetto, F. A. Calle, C. I. TI Observed Weak Electron Beam Discharge Driven Grain Acceleration/Accretion with Implications for Planet Formation SO EARTH MOON AND PLANETS LA English DT Article DE Grain accretion; Weak discharge; Electrostatic mechanism; Solar system formation; Protoplanetary nebula ID MAGNETICALLY ENHANCED COAGULATION; SMALL IRON GRAINS; SOLAR NEBULA; PROTOPLANETARY DISKS; GROWTH; PLANETESIMALS; DUST; INSTABILITY; PARTICLES; FORM AB Work presented here addresses the issue of grain accretion, an essential yet poorly understood process in planetary system formation, linking the dynamically modeled steps of temperature-dependent condensation of gases after proto-sun gravitational collapse to coalescence of kilometer-size planetesimals into planets. The mechanism for grain accretion has proven difficult to model dynamically. Here, we attempt to test the thesis that the accretion process is electrostatically-driven by non-uniform charging of grains in a low discharge/weak field environment equivalent to periodic conditions in protoplanetary nebulae during solar discharge events such as flares. We simulate in the laboratory the behavior of grains in relationship to surfaces in such an environment. The nature of the observed disaggregation, repulsion, and acceleration of grains away from initial surfaces, and their reaggregation as coatings on surrounding oppositely charged surfaces, provide an empirical experimental basis for an electrostatically-driven model for grain behavior and accretion. Similar weak discharge processes in the protoplanetary disk solar nebula could give rise to increased grain acceleration and collisional compression induced surface coating, necessary conditions for increased accretion. The frequency, timing, and level of energetic output of the proto-sun would influence the effectiveness of such processes in developing stable aggregates, and the nature of the solar system that would result. C1 [Clark, P. E.] Catholic Univ Amer, Washington, DC 20064 USA. [Curtis, S. A.; Nuth, J. A.; Minetto, F. A.] NASA GSFC, Greenbelt, MD 20771 USA. [Marshall, J. R.] SETI Inst, Mountain View, CA 94943 USA. [Calle, C. I.] NASA KSC, Cape Kennedy, FL 32899 USA. RP Clark, PE (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM pamela.e.clark@nasa.gov RI Nuth, Joseph/E-7085-2012 NR 29 TC 0 Z9 0 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2010 VL 107 IS 2-4 BP 147 EP 155 DI 10.1007/s11038-010-9356-1 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 744PR UT WOS:000289107100001 ER PT J AU Zhang, YB Smith, SJ Kyle, GP Stackhouse, PW AF Zhang, Yabei Smith, Steven J. Kyle, G. Page Stackhouse, Paul W., Jr. TI Modeling the potential for thermal concentrating solar power technologies SO ENERGY POLICY LA English DT Article DE Solar; CSP; Thermal storage ID CLIMATE AB In this paper we explore the tradeoffs between thermal storage capacity, cost, and other system parameters in order to examine possible evolutionary pathways for thermal concentrating solar power (CSP) technologies A representation of CSP performance that is suitable for incorporation into economic modeling tools is developed We also combined existing data in order to estimate the global solar resource characteristics needed for analysis of CSP technologies We find that, as the fraction of electricity supplied by CSP technologies grows, the application of thermal CSP technologies might progress from current hybrid plants, to plants with a modest amount of thermal storage, and potentially even to plants with sufficient thermal storage to provide base load generation capacity. The regional and global potential of thermal CSP technologies was then examined using the GCAM long-term integrated assessment model. (C) 2010 Elsevier Ltd All rights reserved C1 [Zhang, Yabei] Univ Maryland, Joint Global Change Res Inst, College Pk, MD 20742 USA. [Zhang, Yabei] Univ Maryland, Dept Agr & Resource Econ, College Pk, MD 20742 USA. [Smith, Steven J.; Kyle, G. Page] Pacific NW Natl Lab, Joint Global Change Res Inst, College Pk, MD 20740 USA. [Stackhouse, Paul W., Jr.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Smith, SJ (reprint author), World Bank, Washington, DC 20433 USA. FU Battelle Memorial Institute, Pacific Northwest Division [DE-AC05-76RL01830]; US Department of Energy FX This manuscript has been authored by Battelle Memorial Institute, Pacific Northwest Division, under Contract no DE-AC05-76RL01830 with the US Department of Energy The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes NR 33 TC 22 Z9 22 U1 0 U2 12 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0301-4215 EI 1873-6777 J9 ENERG POLICY JI Energy Policy PD DEC PY 2010 VL 38 IS 12 BP 7884 EP 7897 DI 10.1016/j.enpol.2010.09.008 PG 14 WC Energy & Fuels; Environmental Sciences; Environmental Studies SC Energy & Fuels; Environmental Sciences & Ecology GA 690TU UT WOS:000285032000035 ER PT J AU Turyshev, SG Farr, W Folkner, WM Girerd, AR Hemmati, H Murphy, TW Williams, JG Degnan, JJ AF Turyshev, Slava G. Farr, William Folkner, William M. Girerd, Andre R. Hemmati, Hamid Murphy, Thomas W., Jr. Williams, James G. Degnan, John J. TI Advancing tests of relativistic gravity via laser ranging to Phobos SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Tests of general relativity; Interplanetary laser ranging; Phobos ID INVERSE-SQUARE LAW; EQUIVALENCE PRINCIPLE; GENERAL-RELATIVITY; SOLAR-SYSTEM; INTERIOR STRUCTURE; MARS PATHFINDER; CRATERING RATE; TIME TRANSFER; MASSES; PERTURBATIONS AB Phobos Laser Ranging (PLR) is a concept for a space mission designed to advance tests of relativistic gravity in the solar system. PLR's primary objective is to measure the curvature of space around the Sun, represented by the Eddington parameter gamma, with an accuracy of two parts in 10(7), thereby improving today's best result by two orders of magnitude. Other mission goals include measurements of the time-rate-of-change of the gravitational constant, G and of the gravitational inverse square law at 1.5-AU distances-with up to two orders-of-magnitude improvement for each. The science parameters will be estimated using laser ranging measurements of the distance between an Earth station and an active laser transponder on Phobos capable of reaching mm-level range resolution. A transponder on Phobos sending 0.25-mJ, 10-ps pulses at 1 kHz, and receiving asynchronous 1-kHz pulses from earth via a 12-cm aperture will permit links that even at maximum range will exceed a photon per second. A total measurement precision of 50 ps demands a few hundred photons to average to 1-mm (3.3 ps) range precision. Existing satellite laser ranging (SLR) facilities-with appropriate augmentation-may be able to participate in PLR. Since Phobos' orbital period is about 8 h, each observatory is guaranteed visibility of the Phobos instrument every Earth day. Given the current technology readiness level, PLR could be started in 2011 for launch in 2016 for 3 yr of science operations. We discuss the PLR's science objectives, instrument, and mission design. We also present the details of science simulations performed to support the mission's primary objectives. C1 [Turyshev, Slava G.; Farr, William; Folkner, William M.; Girerd, Andre R.; Hemmati, Hamid; Williams, James G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Murphy, Thomas W., Jr.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Degnan, John J.] Sigma Space Corp, Lanham, MD 20706 USA. RP Turyshev, SG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM turyshev@jpl.nasa.gov FU National Aeronautics and Space Administration FX The work described in this report was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship acknowledged. The anonymous referee is thanked for valuable suggestions that improved the text and made it more readable. NR 96 TC 29 Z9 30 U1 1 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 DEC PY 2010 VL 28 IS 2-3 BP 209 EP 249 DI 10.1007/s10686-010-9199-9 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 678XK UT WOS:000284116600006 ER PT J AU Adams, CF Harris, BP Marino, MC Stokesbury, KDE AF Adams, Charles F. Harris, Bradley P. Marino, Michael C. Stokesbury, Kevin D. E. TI Quantifying sea scallop bed diameter on Georges Bank with geostatistics SO FISHERIES RESEARCH LA English DT Article DE Geostatistics; Placopecten magellanicus; Scallop bed; Sea scallop; Variogram ID PLACOPECTEN-MAGELLANICUS; CLOSED AREAS; NORTH-SEA; SPATIAL STRUCTURE; ABUNDANCE; FISHERY; VARIOGRAM; BIOMASS; USA; VARIABILITY AB Spatially explicit management strategies require the identification of appropriate spatial scales for the observation analysis and management of fisheries Although the mesoscale (km) is the domain of traditional fisheries stock units there have been few attempts to describe mesoscale aggregations of scallops typically referred to as beds We quantified the average bed diameter of sea scallops (Placopecten magellanicus) using geostatistics Data were collected between 1999 and 2007 in the Northern Edge (NE) of Closed Area II and the Nantucket Lightship (NL) Closed Area on Georges Bank Average bed diameter in the NE varied between 65 and 8 6 km with classical variograms and 7 6-9 8 km with robust variograms Average bed diameter in the NL varied between 30 and 10 1 km with classical variograms and 40-13 22 km with robust variograms There was more spatial structure in the NE The spatial structure of the NL was less clearly defined and/or more variable Kriged maps indicate the presence of multiple beds in both areas Densities of ca 1 24 scallops/m(2) appeared to correspond well with the average bed diameters given by variograms These results can be used as guidelines for the observation and analysis of the sea scallop resource in the NE and NL Published by Elsevier B V C1 [Adams, Charles F.; Harris, Bradley P.; Marino, Michael C.; Stokesbury, Kevin D. E.] Univ Massachusetts Dartmouth, Sch Marine Sci & Technol, New Bedford, MA 02744 USA. RP Adams, CF (reprint author), Natl Marine Fisheries Serv, Fisheries Stat Off, 55 Great Republ Dr, Gloucester, MA 01930 USA. FU SMAST the Massachusetts Division of Marine Fisheries NOAA [NA08NMF4720554]; Sea scallop fishery and supporting industries FX We thank the owners captains and crews who sailed with us P Christopher D Frei R Silva (NMFS) and L Gavlin (USCG) provided the Letters of Authorization Aid was provided by SMAST the Massachusetts Division of Marine Fisheries NOAA award NA08NMF4720554 and the sea scallop fishery and supporting industries The views expressed herein are those of the authors and do not necessarily reflect the views of NOAA or any other agencies NR 44 TC 2 Z9 2 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 J9 FISH RES JI Fish Res. PD DEC PY 2010 VL 106 IS 3 BP 460 EP 467 DI 10.1016/j.fishres.2010.09.021 PG 8 WC Fisheries SC Fisheries GA 691JW UT WOS:000285077100025 ER PT J AU Russell, MJ Hall, AJ Martin, W AF Russell, M. J. Hall, A. J. Martin, W. TI Serpentinization as a source of energy at the origin of life SO GEOBIOLOGY LA English DT Review ID CITY HYDROTHERMAL FIELD; MID-ATLANTIC RIDGE; IRON-SULFUR CLUSTERS; EAST PACIFIC RISE; LOST-CITY; EARLY EARTH; ULTRAMAFIC ROCKS; SEA-FLOOR; ORGANIC-COMPOUNDS; OXIDATION-STATE AB For life to have emerged from CO2, rocks, and water on the early Earth, a sustained source of chemically transducible energy was essential. The serpentinization process is emerging as an increasingly likely source of that energy. Serpentinization of ultramafic crust would have continuously supplied hydrogen, methane, minor formate, and ammonia, as well as calcium and traces of acetate, molybdenum and tungsten, to off-ridge alkaline hydrothermal springs that interfaced with the metal-rich carbonic Hadean Ocean. Silica and bisulfide were also delivered to these springs where cherts and sulfides were intersected by the alkaline solutions. The proton and redox gradients so generated represent a rich source of naturally produced chemiosmotic energy, stemming from geochemistry that merely had to be tapped, rather than induced, by the earliest biochemical systems. Hydrothermal mounds accumulating at similar sites in today's oceans offer conceptual and experimental models for the chemistry germane to the emergence of life, although the ubiquity of microbial communities at such sites in addition to our oxygenated atmosphere preclude an exact analogy. C1 [Russell, M. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Hall, A. J.] Univ Glasgow, Dept Archaeol, Glasgow, Lanark, Scotland. [Martin, W.] Univ Dusseldorf, Inst Bot 3, Dusseldorf, Germany. RP Russell, MJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM mrussell@jpl.nasa.gov RI Martin, William/C-5680-2008; Martin, William /O-5446-2015 OI Martin, William /0000-0003-1478-6449 FU National Aeronautics and Space Administration for Astrobiology; NASA's Astrobiology Institute (Icy Worlds); California Institute of Technology; European Research Council; Deutsche Forschungsgemeinschaft FX We thank Wolfgang Nitschke, Tony Fallick, Kevin Hand, Susan Lang, Isik Kanik, Shawn McGlynn, Randy Mielke, Victoria Orphan, Mark Skidmore and Steve Vance for discussions and support. Anonymous referees gave helpful critiques. M.J.R.'s research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration for Astrobiology: Exobiology and Evolutionary Biology and supported by NASA's Astrobiology Institute (Icy Worlds). Copyright 2010 California Institute of Technology, Government sponsorship acknowledged. W.M.'s research is supported by grants from the European Research Council and the Deutsche Forschungsgemeinschaft. NR 196 TC 102 Z9 111 U1 12 U2 136 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1472-4677 EI 1472-4669 J9 GEOBIOLOGY JI Geobiology PD DEC PY 2010 VL 8 IS 5 BP 355 EP 371 DI 10.1111/j.1472-4669.2010.00249.x PG 17 WC Biology; Environmental Sciences; Geosciences, Multidisciplinary SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Geology GA 678LE UT WOS:000284074600001 PM 20572872 ER PT J AU Finlay, CC Maus, S Beggan, CD Bondar, TN Chambodut, A Chernova, TA Chulliat, A Golovkov, VP Hamilton, B Hamoudi, M Holme, R Hulot, G Kuang, W Langlais, B Lesur, V Lowes, FJ Luhr, H Macmillan, S Mandea, M McLean, S Manoj, C Menvielle, M Michaelis, I Olsen, N Rauberg, J Rother, M Sabaka, TJ Tangborn, A Toffner-Clausen, L Thebault, E Thomson, AWP Wardinski, I Wei, Z Zvereva, TI AF Finlay, C. C. Maus, S. Beggan, C. D. Bondar, T. N. Chambodut, A. Chernova, T. A. Chulliat, A. Golovkov, V. P. Hamilton, B. Hamoudi, M. Holme, R. Hulot, G. Kuang, W. Langlais, B. Lesur, V. Lowes, F. J. Luehr, H. Macmillan, S. Mandea, M. McLean, S. Manoj, C. Menvielle, M. Michaelis, I. Olsen, N. Rauberg, J. Rother, M. Sabaka, T. J. Tangborn, A. Toffner-Clausen, L. Thebault, E. Thomson, A. W. P. Wardinski, I. Wei, Z. Zvereva, T. I. CA Int Assoc Geomagnetism Aeronomy Wo TI International Geomagnetic Reference Field: the eleventh generation SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Magnetic field; Satellite magnetics ID IGRF; MODELS; SPACE AB The eleventh generation of the International Geomagnetic Reference Field (IGRF) was adopted in December 2009 by the International Association of Geomagnetism and Aeronomy Working Group V-MOD. It updates the previous IGRF generation with a definitive main field model for epoch 2005.0, a main field model for epoch 2010.0, and a linear predictive secular variation model for 2010.0-2015.0. In this note the equations defining the IGRF model are provided along with the spherical harmonic coefficients for the eleventh generation. Maps of the magnetic declination, inclination and total intensity for epoch 2010.0 and their predicted rates of change for 2010.0-2015.0 are presented. The recent evolution of the South Atlantic Anomaly and magnetic pole positions are also examined. C1 [Finlay, C. C.] ETH, Inst Geophys, Earth & Planetary Magnetism Grp, CH-8092 Zurich, Switzerland. [Maus, S.; McLean, S.; Manoj, C.] Univ Colorado, NOAA NGDC, Boulder, CO 80309 USA. [Maus, S.; McLean, S.; Manoj, C.] Univ Colorado, CIRES, Boulder, CO 80309 USA. [Beggan, C. D.; Hamilton, B.; Macmillan, S.; Thomson, A. W. P.] British Geol Survey, Edinburgh EH9 3LA, Midlothian, Scotland. [Bondar, T. N.; Chernova, T. A.; Golovkov, V. P.; Zvereva, T. I.] IZMIRAN, Pushkov Inst Terr Magnetism Ionosphere & Radio Wa, Troitsk 142190, Moscow Reg, Russia. [Chambodut, A.] Univ Strasbourg, EOST, CNRS, Inst Phys Globe Strasbourg,UMR 7516, Strasbourg, France. [Chulliat, A.; Hulot, G.; Thebault, E.] Univ Paris Diderot, CNRS INSU, UMR 7154, Equipe Geomagnetisme,Inst Phys Globe Paris, Paris, France. [Hamoudi, M.; Lesur, V.; Luehr, H.; Michaelis, I.; Rauberg, J.; Rother, M.; Wardinski, I.] GFZ German Res Ctr Geosci, Helmholtz Ctr Potsdam, D-14473 Potsdam, Germany. [Holme, R.] Univ Liverpool, Sch Environm Sci, Liverpool L69 3BX, Merseyside, England. [Kuang, W.; Sabaka, T. J.] NASA GSFC, Planetary Geodynam Lab, Greenbelt, MD USA. [Langlais, B.] Univ Nantes, CNRS, UMR 6112, Lab Planetol & Geodynam Nantes, Nantes, France. [Lowes, F. J.] Newcastle Univ, Sch Chem, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Mandea, M.] Univ Paris Diderot, IPG Paris, F-75013 Paris, France. [Menvielle, M.] Univ Paris 11, Dept Sci Terre, Orsay, France. [Menvielle, M.] Univ Versailles St Quentin, CNRS INSU, LATMOS IPSL, Paris, France. [Olsen, N.; Toffner-Clausen, L.] DTU Space, DK-2100 Copenhagen, Denmark. [Tangborn, A.; Wei, Z.] UMBC, Joint Ctr Earth Syst Technol, Catonsville, MD USA. RP Finlay, CC (reprint author), ETH, Inst Geophys, Earth & Planetary Magnetism Grp, Sonneggstr 5, CH-8092 Zurich, Switzerland. EM cfinlay@erdw.ethz.ch RI Hulot, Gauthier/A-5627-2011; Chulliat, Arnaud/A-5747-2011; Olsen, Nils/H-1822-2011; Sabaka, Terence/D-5618-2012; MANDEA, Mioara/E-4892-2012; Langlais, Benoit/K-5366-2012; Kuang, Weijia/K-5141-2012; Thebault, Erwan/A-5670-2011; Finlay, Christopher/B-5062-2014; Lesur, Vincent/H-1031-2012; CHAMBODUT, Aude/E-9615-2017 OI Maus, Stefan/0000-0002-9604-3878; Chulliat, Arnaud/0000-0001-7414-9631; Olsen, Nils/0000-0003-1132-6113; Langlais, Benoit/0000-0001-5207-304X; Kuang, Weijia/0000-0001-7786-6425; Finlay, Christopher/0000-0002-4592-2290; Lesur, Vincent/0000-0003-2568-320X; CHAMBODUT, Aude/0000-0001-8793-1315 FU Space Agency of the German Aerospace Centre (DLR) through Federal Ministry of Economics and Technology [50EE0944]; NASA; ESA; CNES; DARA; Thomas B. Thriges Foundation; CONAE; DMI/DTU Space; NSF FX The CHAMP mission is sponsored by the Space Agency of the German Aerospace Centre (DLR) through funds of the Federal Ministry of Economics and Technology, following a decision of the German Federal Parliament (grant code 50EE0944). Data retrieval and operation of the CHAMP satellite by the German Space Operations Centre (GSOC) is acknowledged. The Orsted Project was made possible by extensive support from the Danish Government, NASA, ESA, CNES, DARA and the Thomas B. Thriges Foundation. The SAC-C mission was supported by CONAE together with NASA and DMI/DTU Space. The institutes that support magnetic observatories together with INTERMAGNET are thanked for promoting high standards of observatory practice. This is IPGP contribution no. 300(1). W.K., A.T. and Z.W. were funded by NASA and the NSF. The IGRF-11 task force finally wishes to express their gratitude to C. Manoj for maintaining the IGRF web pages at NGDC. NR 26 TC 491 Z9 512 U1 9 U2 68 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0956-540X J9 GEOPHYS J INT JI Geophys. J. Int. PD DEC PY 2010 VL 183 IS 3 BP 1216 EP 1230 DI 10.1111/j.1365-246X.2010.04804.x PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 680YZ UT WOS:000284274700010 ER PT J AU Hergt, JM Arevalo, R Bedard, LP Bellucci, J Enzweiler, J Jochum, KP Linge, KL McDonough, WF Mertz-Kraus, R Wiedenbeck, M Wang, XH Woodhead, JD AF Hergt, Janet M. Arevalo, Ricardo, Jr. Bedard, L. Paul Bellucci, Jeremy Enzweiler, Jacinta Jochum, Klaus Peter Linge, Kathryn L. McDonough, William F. Mertz-Kraus, Regina Wiedenbeck, Michael Wang, Xiaohong Woodhead, Jon D. TI GGR Critical Review of Analytical Developments in 2008-2009: An Introduction SO GEOSTANDARDS AND GEOANALYTICAL RESEARCH LA English DT Article DE reference materials; SIMS; stable isotopes; geochronology; trace elements; laser ablation; MC-ICP-MS; ICP-AES; isotope ratios; TIMS; XRF; AAS; INAA; measurement uncertainties AB This collection of articles represents the fourth in a series of reviews in which authors have aimed at capturing the key advances in a range of analytical fields (Hergt et al. 2005, 2006, 2008). The publication period under review is 2008-2009 and the intention here is to provide readers with a summary of the most influential developments published during this period, across a broad range of topics appropriate to the Earth and environmental sciences. Most authors comment on the ways in which the emphases of research in their specific fields of examination have changed over time. All note an increase in rigour and focus on data quality. Whether advances have taken place in instrumentation, sample manipulation or data deconvolution, there are a large number of dedicated scientists out there contributing to the high quality of geochemical data employed in geological and environmental research. C1 [Hergt, Janet M.; Woodhead, Jon D.] Univ Melbourne, Sch Earth Sci, Melbourne, Vic 3010, Australia. [Arevalo, Ricardo, Jr.] NASA, Planetary Environm Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bedard, L. Paul] Univ Quebec & Chicoutimi, Chicoutimi, PQ G7H 2B1, Canada. [Bellucci, Jeremy; McDonough, William F.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Enzweiler, Jacinta] Univ Campinas UNICAMP, Inst Geosci, BR-13083970 Campinas, SP, Brazil. [Jochum, Klaus Peter; Mertz-Kraus, Regina] Max Planck Inst Chem, D-55020 Mainz, Germany. [Linge, Kathryn L.] Curtin Univ Technol, Curtin Water Qual Res Ctr, Dept Chem, Perth, WA 6845, Australia. [Wiedenbeck, Michael] Deutsch GeoForschungsZentrum, Helmholtz Zentrum Potsdam, Sect Inorgan & Isotope Geochem 4 2, D-14473 Potsdam, Germany. [Wang, Xiaohong] Chinese Acad Geol Sci, Natl Res Ctr Geoanal, Beijing 100037, Peoples R China. RP Hergt, JM (reprint author), Univ Melbourne, Sch Earth Sci, Melbourne, Vic 3010, Australia. EM jhergt@unimelb.edu.au RI Arevalo, Ricardo/F-3487-2012; McDonough, William/C-4791-2009; Enzweiler, Jacinta/B-9023-2012; Linge, Kathryn/B-8095-2008; Mertz-Kraus, Regina/K-3558-2014; McDonough, William/I-7720-2012 OI McDonough, William/0000-0001-9154-3673; Linge, Kathryn/0000-0002-3743-0640; Bedard, L.Paul/0000-0003-3062-5506; Hergt, Janet/0000-0003-3410-1670; Woodhead, Jon/0000-0002-7614-0136; Mertz-Kraus, Regina/0000-0002-5122-4480; McDonough, William/0000-0001-9154-3673 NR 3 TC 1 Z9 1 U1 0 U2 7 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1639-4488 J9 GEOSTAND GEOANAL RES JI Geostand. Geoanal. Res. PD DEC PY 2010 VL 34 IS 4 BP 325 EP 326 DI 10.1111/j.1751-908X.2010.00936.x PG 2 WC Geosciences, Multidisciplinary SC Geology GA 706JC UT WOS:000286213300004 ER PT J AU Arevalo, R Bellucci, J McDonough, WF AF Arevalo, Ricardo, Jr. Bellucci, Jeremy McDonough, William F. TI GGR Biennial Review: Advances in Laser Ablation and Solution ICP-MS from 2008 to 2009 with Particular Emphasis on Sensitivity Enhancements, Mitigation of Fractionation Effects and Exploration of New Applications SO GEOSTANDARDS AND GEOANALYTICAL RESEARCH LA English DT Article DE LA-ICP-MS; solution ICP-MS; isotopic fractionation; RMs; calibrators; nuclear materials; forensic applications ID PLASMA-MASS SPECTROMETRY; TETRAMETHYLAMMONIUM HYDROXIDE SOLUBILIZATION; IN-SITU DETERMINATION; ISOTOPE RATIOS; INTERNAL STANDARD; ROOM-TEMPERATURE; HUMAN HAIR; LA-ICPMS; SAMPLES; ELEMENTS AB Recent developments from 2008 to 2009 in ICP-MS engineering, methods and applications are reviewed here. Of particular emphasis are advances in: (a) maximising sensitivity and reducing elemental/isotopic fractionation during laser ablation processing; (b) developing new analytical techniques to measure major, minor and trace element abundances without depending on matrix-matched calibrating materials, pre-determined internal standard concentrations and/or multiple analytical methods; (c) applying in situ and solution-based ICP-MS techniques to the analysis of forensic materials for criminal and/or nuclear investigations; and (d) improving precision and limits of detection of laser ablation multi-collector ICP-MS measurements of (ultra) trace elemental and isotopic abundances. C1 [Bellucci, Jeremy; McDonough, William F.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Arevalo, Ricardo, Jr.] NASA, Planetary Environm Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP McDonough, WF (reprint author), Univ Maryland, Dept Geol, 237 Regents Dr, College Pk, MD 20742 USA. EM mcdonoug@umd.edu RI Arevalo, Ricardo/F-3487-2012; McDonough, William/C-4791-2009; McDonough, William/I-7720-2012 OI McDonough, William/0000-0001-9154-3673; McDonough, William/0000-0001-9154-3673 NR 55 TC 6 Z9 6 U1 1 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1639-4488 J9 GEOSTAND GEOANAL RES JI Geostand. Geoanal. Res. PD DEC PY 2010 VL 34 IS 4 BP 327 EP 341 DI 10.1111/j.1751-908X.2010.00934.x PG 15 WC Geosciences, Multidisciplinary SC Geology GA 706JC UT WOS:000286213300005 ER PT J AU Malhi, Y Silman, M Salinas, N Bush, M Meir, P Saatchi, S AF Malhi, Y. Silman, M. Salinas, N. Bush, M. Meir, P. Saatchi, S. TI Introduction: Elevation gradients in the tropics: laboratories for ecosystem ecology and global change research SO GLOBAL CHANGE BIOLOGY LA English DT Article ID CLIMATE-CHANGE; ICE-AGE; FOREST; IMPACTS; RECORD; ANDES C1 [Malhi, Y.] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England. [Silman, M.] Wake Forest Univ, Dept Biol, Winston Salem, NC 27106 USA. [Salinas, N.] Univ San Antonio Abad, Cuzco, Peru. [Bush, M.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9XP, Midlothian, Scotland. [Meir, P.] Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. [Saatchi, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Malhi, Y (reprint author), Univ Oxford, Sch Geog & Environm, Environm Change Inst, S Parks Rd, Oxford OX1 3QY, England. EM yadvinder.malhi@ouce.ox.ac.uk RI Silman, Miles/H-1280-2011; Meir, Patrick/J-8344-2012; Salinas, Norma/K-8960-2015; OI Salinas, Norma/0000-0001-9941-2109; Bush, Mark/0000-0001-6894-8613 FU Gordon and Betty Moore Foundation; National Science Foundation (USA); Natural Environment Research Council (UK); Asociacion para la Conservacion de la Cuenca Amazonica (ACCA); Blue Moon Fund; Microsoft Research FX The study in Peru that is the focus on this special section is an activity of the Andes Biodiversity and Ecosystems Research Group (ABERG), and has been supported by grants from the Andes-Amazon programme of the Gordon and Betty Moore Foundation, the National Science Foundation (USA), the Natural Environment Research Council (UK), the Asociacion para la Conservacion de la Cuenca Amazonica (ACCA), The Blue Moon Fund, and Microsoft Research. We also thank ACCA, Explorers Inn Tambopata, Manu National Park and INRENA for access to the field research sites. NR 33 TC 73 Z9 79 U1 8 U2 71 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD DEC PY 2010 VL 16 IS 12 BP 3171 EP 3175 DI 10.1111/j.1365-2486.2010.02323.x PG 5 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 674GY UT WOS:000283726600001 ER PT J AU Mouginot, J Pommerol, A Kofman, W Beck, P Schmitt, B Herique, A Grima, C Safaeinili, A Plaut, JJ AF Mouginot, J. Pommerol, A. Kofman, W. Beck, P. Schmitt, B. Herique, A. Grima, C. Safaeinili, A. Plaut, J. J. TI The 3-5 MHz global reflectivity map of Mars by MARSIS/Mars Express: Implications for the current inventory of subsurface H2O SO ICARUS LA English DT Article DE Mars, Surface; Radar observations; Data reduction techniques ID MARTIAN TOPOGRAPHY; SURFACE PROPERTIES; NEAR-SURFACE; GROUND ICE; RADAR; HYDROGEN; DEPOSITS; ODYSSEY; IONOSPHERE; IMPACT AB We extracted the surface echo power from 2 years of MARSIS measurements. The retrieved values are calibrated to compensate for changes in the distance of the spacecraft to the surface and for the attenuation of the signal by the ionosphere. The results are used to build the first global map of surface echo power at 3-5 MHz. The surface echo power variations are primarily caused by kilometer-scale surface roughness. Then, we derive the values of dielectric constant of the shallow subsurface materials by normalizing the surface echo power map using a simulation of MARSIS signal from the MOLA topography. As a result, we obtain a map that characterizes the dielectric properties of the materials down to a few decameters below the surface. Dielectric properties vary with latitude, with high values in mid-latitudes belts (20-40 degrees) and lower values at both equatorial and high latitudes. From the comparison of MARSIS reflectivity map to GRS observations, we conclude that the reflectivity decrease observed poleward of 50-60 degrees corresponds to the onset of water-ice occurrence within the regolith. Assuming homogenous ground composition and texture at the scale of the MARSIS resolution cell, our inferred volume of ground water ice is of 10(6) km(3), equivalent to a polar cap. Low reflectivity areas are also observed in equatorial regions. From radar studies alone, equatorial low dielectric constant values could have different interpretations but the correlation with GRS hydrogen distribution rather points toward a water-related explanation. Published by Elsevier Inc. C1 [Mouginot, J.; Pommerol, A.; Kofman, W.; Beck, P.; Schmitt, B.; Herique, A.; Grima, C.] UJF Grenoble 1, CNRS, Lab Planetol Grenoble, F-38041 Grenoble 9, France. [Mouginot, J.] Univ Calif Irvine, Irvine, CA 92697 USA. [Pommerol, A.] Univ Bern, Inst Phys, Space Res & Planetary Sci Div, CH-3012 Bern, Switzerland. [Safaeinili, A.; Plaut, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mouginot, J (reprint author), Univ Calif Irvine, Irvine, CA 92717 USA. EM jmougino@uci.edu RI Schmitt, Bernard/A-1064-2009; Beck, Pierre/F-3149-2011; Grima, Cyril/E-9800-2013; Mouginot, Jeremie/G-7045-2015; Kofman, Wlodek/C-4556-2008; Herique, Alain/E-7210-2017 OI Schmitt, Bernard/0000-0002-1230-6627; Grima, Cyril/0000-0001-7135-3055; Herique, Alain/0000-0003-3699-883X FU French space agency (CNES) FX We acknowledge the support of the space agencies of Italy (ASI) and the United States (NASA), for the development and science operations of MARSIS. Operations of the Mars Express spacecraft by the European Space Agency (ESA) are gratefully acknowledged. The French space agency (CNES) supports these studies in Laboratoire de Planetologie de Grenoble. NR 51 TC 38 Z9 38 U1 1 U2 15 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 DEC PY 2010 VL 210 IS 2 BP 612 EP 625 DI 10.1016/j.icarus.2010.07.003 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679RP UT WOS:000284178800005 ER PT J AU de Pater, I Fletcher, LN Perez-Hoyos, S Hammel, HB Orton, GS Wong, MH Luszcz-Cook, S Sanchez-Lavega, A Boslough, M AF de Pater, Imke Fletcher, Leigh N. Perez-Hoyos, Santiago Hammel, Heidi B. Orton, Glenn S. Wong, Michael H. Luszcz-Cook, Statia Sanchez-Lavega, Agustin Boslough, Mark TI A multi-wavelength study of the 2009 impact on Jupiter: Comparison of high resolution images from Gemini, Keck and HST SO ICARUS LA English DT Article DE Jupiter, Atmosphere; Impact processes; Hubble Space Telescope observations; Infrared observations; Adaptive optics ID GALILEO PROBE; CLOUD STRUCTURE; RED SPOT; MU-M; ATMOSPHERE; SHOEMAKER-LEVY-9; TEMPERATURE; RETRIEVAL; SPECTRA; AMMONIA AB Within several days of A. Wesley's announcement that Jupiter was hit by an object on UT 19 July 2009, we observed the impact site with (1) the Hubble Space Telescope (HST) at UV through visible (225-924 nm) wavelengths, (2) the 10-m W.M. Keck II telescope in the near-infrared (1-5 mu m), and (3) the 8-m Gemini-North telescope in the mid-infrared (7.7-18 mu m). All observations reported here were obtained between 22 and 25 July 2009. Observations at visible and near-infrared wavelengths show that large (similar to 0.75-mu m radius) dark (imaginary index of refraction m(i) similar to 0.01-0.1) particulates were deposited at atmospheric pressures between 10 and 200-300 mbar; analysis of HST-UV data reveals that in addition smaller-sized (similar to 0.1 mu m radius) material must have been deposited at the highest altitudes (similar to 10 mbar). Differences in morphology between the UV and visible/near-IR images suggest three-dimensional variations in particle size and density across the impact site, which probably were induced during the explosion and associated events. At mid-infrared wavelengths the brightness temperature increased due to both an enhancement in the stratospheric NH(3) gas abundance and the physical temperature of the atmosphere. This high brightness temperature coincides with the center part of the impact site as seen with HST. This observation, combined with (published) numerical simulations of the Shoemaker-Levy 9 impacts on Jupiter and the Tunguska airburst on Earth, suggests that the downward jet from the terminal explosion probably penetrated down to the similar to 700-mbar level. (C) 2010 Elsevier Inc. All rights reserved. C1 [de Pater, Imke; Wong, Michael H.; Luszcz-Cook, Statia] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fletcher, Leigh N.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. [Hammel, Heidi B.] Space Sci Inst, Boulder, CO 80301 USA. [Orton, Glenn S.; Sanchez-Lavega, Agustin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boslough, Mark] Sandia Natl Labs, Albuquerque, NM 87185 USA. RP de Pater, I (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM imke@berkeley.edu RI Fletcher, Leigh/D-6093-2011; Perez-Hoyos, Santiago/L-7543-2014; OI Fletcher, Leigh/0000-0001-5834-9588; Perez-Hoyos, Santiago/0000-0002-2587-4682; Sanchez-Lavega, Agustin/0000-0001-7355-1522 FU W.M. Keck Foundation; NASA through Space Telescope Science Institute [NAS 5-26555, GO/DD-12003]; National Science Foundation Science and Technology Center for Adaptive Optics [AST 98-76783]; University of Oxford; Spanish MICIIN [AYA2009-10701]; FEDER; Grupos Gobierno Vasco [IT-464-07] FX The near-infrared data were obtained with the W.M. Keck Observatory, which is operated by the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The observations reported here were conducted under IdP and HBH's general observing programs; they fortuitously were scheduled on the telescope only a few days after the impact. We thank Al Conrad for his support during the observations. The Keck Observatory was made possible by the generous financial support of the W.M. Keck Foundation.; The visible wavelength data were obtained with the NASA/ESA Hubble Space Telescope. These observations are associated with HST program GO/DD-12003, with support provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA Contract NAS 5-26555.; This work was further supported in part by the National Science Foundation Science and Technology Center for Adaptive Optics, managed by the University of California at Santa Cruz under cooperative agreement AST 98-76783. Fletcher was supported by an Glasstone Science Fellowship at the University of Oxford.; SPH and ASL supported by the Spanish MICIIN AYA2009-10701 with FEDER and Grupos Gobierno Vasco IT-464-07. NR 40 TC 21 Z9 21 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 DEC PY 2010 VL 210 IS 2 BP 722 EP 741 DI 10.1016/j.icarus.2010.07.010 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679RP UT WOS:000284178800014 ER PT J AU Vinatier, S Bezard, B de Kok, R Anderson, CM Samuelson, RE Nixon, CA Mamoutkine, A Carlson, RC Jennings, DE Guandique, EA Bjoraker, GL Flasar, FM Kunde, VG AF Vinatier, Sandrine Bezard, Bruno de Kok, Remco Anderson, Carrie M. Samuelson, Robert E. Nixon, Conor A. Mamoutkine, Andrei Carlson, Ronald C. Jennings, Donald E. Guandique, Ever A. Bjoraker, Gordon L. Flasar, F. Michael Kunde, Virgil G. TI Analysis of Cassini/CIRS limb spectra of Titan acquired during the nominal mission II: Aerosol extinction profiles in the 600-1420 cm(-1) spectral range SO ICARUS LA English DT Article DE Titan; Abundances, Atmospheres; Infrared observations ID NORTH POLAR STRATOSPHERE; CONDENSATE CLOUDS; ATMOSPHERE; HAZE; WINDS; HYDROCARBONS; ABUNDANCES; THOLINS; MODEL AB We have analyzed the continuum emission of limb spectra acquired by the Cassini/CIRS infrared spectrometer in order to derive information on haze extinction in the 3-0.02 mbar range (similar to 150-350 km). We focused on the 600-1420 cm(-1) spectral range and studied nine different limb observations acquired during the Cassini nominal mission at 55 degrees S, 20 degrees S, 5 degrees N, 30 degrees N, 40 degrees N, 45 degrees N, 55 degrees N, 70 degrees N and 80 degrees N. By means of an inversion algorithm solving the radiative transfer equation, we derived the vertical profiles of haze extinction coefficients from 17 spectral ranges of 20-cm(-1) wide at each of the nine latitudes. At a given latitude, all extinction vertical profiles retrieved from various spectral intervals between 600 and 1120 cm(-1) display similar vertical slopes implying similar spectral characteristics of the material at all altitudes. We calculated a mean vertical extinction profile for each latitude and derived the ratio of the haze scale height (H-haze) to the pressure scale height (H-gas) as a function of altitude. We inferred H-haze/H-gas values varying from 0.8 to 2.4. The aerosol scale height varies with altitude and also with latitude. Overall, the haze extinction does not show strong latitudinal variations but, at 1 mbar, an increase by a factor of 1.5 is observed at the north pole compared to high southern latitudes. The vertical optical depths at 0.5 and 1.7 mbar increase from 55 degrees S to 5 degrees N, remain constant between 5 degrees N and 30 degrees N and display little variation at higher latitudes, except the presence of a slight local maximum at 45 degrees N. The spectral dependence of the haze vertical optical depth is uniform with latitude and displays three main spectral features centered at 630 cm(-1), 745 cm(-1) and 1390 cm(-1), the latter showing a wide tail extending down to similar to 1000 cm(-1). From 600 to 750 cm(-1), the optical depth increases by a factor of 3 in contrast with the absorbance of laboratory tholins, which is generally constant. We derived the mass mixing ratio profiles of haze at the nine latitudes. Below the 0.4-mbar level all mass mixing ratio profiles increase with height. Above this pressure level, the profiles at 40 degrees N, 45 degrees N, 55 degrees N, at the edge of the polar vortex, display a decrease-with-height whereas the other profiles increase. The global increase with height of the haze mass mixing ratio suggest a source at high altitudes and a sink at low altitudes. An enrichment of haze is observed at 0.1 mbar around the equator, which could be due to a more efficient photochemistry because of the strongest insolation there or an accumulation of haze due to a balance between sedimentation and upward vertical drag. (C) 2010 Elsevier Inc. All rights reserved. C1 [Vinatier, Sandrine; Anderson, Carrie M.; Samuelson, Robert E.; Nixon, Conor A.; Mamoutkine, Andrei; Carlson, Ronald C.; Jennings, Donald E.; Guandique, Ever A.; Bjoraker, Gordon L.; Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vinatier, Sandrine; Bezard, Bruno] Observ Paris, LESIA, F-92195 Meudon, France. [de Kok, Remco] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Samuelson, Robert E.; Nixon, Conor A.; Kunde, Virgil G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mamoutkine, Andrei; Guandique, Ever A.] ADNET Syst Inc, Rockville, MD 20852 USA. [Carlson, Ronald C.] Catholic Univ Amer, Washington, DC 20064 USA. RP Vinatier, S (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA. EM sandrine.vinatier@obspm.fr RI Nixon, Conor/A-8531-2009; Anderson, Carrie/C-8097-2012; Flasar, F Michael/C-8509-2012; Bjoraker, Gordon/D-5032-2012; Jennings, Donald/D-7978-2012 OI Nixon, Conor/0000-0001-9540-9121; FU NASA, NASA Goddard Space Flight Center; Centre National d'Etudes Spatiales; Programme National de Planetologie (INSU) FX The authors would like to thank warmly all the CIRS Team for the large amount of work they do regarding the data preparation and processing. The authors would also like to thank Pascal Rannou for helpful discussion about aerosols and for providing the extinction spectral dependence of a fractal aerosol. We are also grateful to J. Vander Auwera for providing the files of C2H4 spectroscopic parameters. This research was supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This work was also funded by the Centre National d'Etudes Spatiales and the Programme National de Planetologie (INSU). NR 42 TC 22 Z9 22 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2010 VL 210 IS 2 BP 852 EP 866 DI 10.1016/j.icarus.2010.06.024 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679RP UT WOS:000284178800023 ER PT J AU Merlin, F Barucci, MA de Bergh, C DeMeo, FE Alvarez-Candal, A Dumas, C Cruikshank, DP AF Merlin, F. Barucci, M. A. de Bergh, C. DeMeo, F. E. Alvarez-Candal, A. Dumas, C. Cruikshank, D. P. TI Chemical and physical properties of the variegated Pluto and Charon surfaces SO ICARUS LA English DT Article DE Pluto; Charon; Ices; Spectroscopy ID KUIPER-BELT OBJECTS; NEAR-INFRARED SPECTROSCOPY; HUBBLE-SPACE-TELESCOPE; ION IRRADIATION; METHANE ICE; CRYSTALLINE WATER; 2003 UB313; PURE ICES; H2O ICE; MU-M AB We present new photometric and spectroscopic observations of the Pluto-Charon system carried out at the VLT-ESO (Chile) with two 8-m telescopes equipped with the FORS2, ISAAC and SINFONI instruments. The spectra were obtained in the 0.6-2.45 mu m range with a spectral resolution from 300 to 1500. The SINFONI data were obtained using adaptive optics, allowing a complete separation of the two bodies. We derive both objects' magnitudes in the near infrared and convert them into albedo values. These first near infrared photometric data allow to adjust the different parts of Pluto's spectrum, provided by the three instruments. We run spectral models in order to give chemical and physical constraints on the surface of Pluto and Charon. We discuss the dilution properties of the methane ice and its implications on Pluto's surface. The heterogeneities of the pure and diluted methane ice on Pluto's surface is also investigated. The high signal-to-noise level of the data and our analyses may support the presence of ethane ice on the surface of Pluto, which is one of the main products of the methane irradiation and photolysis. The analyses of the spectra of Charon suggest that the water ice is almost completely in its crystalline form and that the ammonia compound is hydrated on the surface of this satellite. Published by Elsevier Inc. C1 [Merlin, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Merlin, F.; Barucci, M. A.; de Bergh, C.; DeMeo, F. E.] Observ Paris, LESIA, F-92195 Meudon, France. [Alvarez-Candal, A.; Dumas, C.] European So Observ, Santiago 19, Chile. [Cruikshank, D. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Merlin, F (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM merlin@astro.umd.edu RI Alvarez-Candal, Alvaro/M-4834-2013 NR 52 TC 25 Z9 25 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 DEC PY 2010 VL 210 IS 2 BP 930 EP 943 DI 10.1016/j.icarus.2010.07.028 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679RP UT WOS:000284178800028 ER PT J AU Talukder, A Panangadan, A Georgas, N Herrington, T Blumberg, AF AF Talukder, Ashit Panangadan, AnandV. Georgas, Nickitas Herrington, Thomas Blumberg, Alan F. TI Integrated Operational Control of Unattended Distributed Coastal Sensor Web Systems With Mobile Autonomous Robots SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Adaptive control; autonomy; coastal sensor web; resource management; unmanned vehicles ID MODEL-PREDICTIVE CONTROL; OPTIMIZATION AB Unattended autonomous systems of the future will involve groups of static and mobile sensors functioning in coordination to achieve overall task objectives. Such systems can be viewed as wirelessly networked unmanned heterogeneous sensor networks. We discuss a distributed heterogeneous sensing system with static sensors and mobile robots with novel adaptive control optimization algorithms for dynamic adaptation, coordinated control and end to end resource management of all sensors in response to detected events to achieve overall system goals and objectives. While our system design is applicable to a host of domains, it has been applied to and tested offline on an existing, functional maritime sensor web system, the New York Harbor Observation and Prediction System (NYHOPS) comprised of a host of maritime ocean and land sensors. Our goal is to enable adaptive control technologies to make the NYHOPS sensor web react faster and more effectively to threats or changing conditions, and to further maritime homeland security for the New York Harbor. Our contribution allows static sensors to work seamlessly with unmanned vehicles that can be deployed autonomously in response to detected events, and dynamically adjust operational parameters of static and mobile assets in the sensor web. Results for large area coastal monitoring are presented. Offline results using actual modeled data from in situ sensory measurements from the NYHOPS sensor web demonstrate how the sensor parameters can be adapted to maximize observability of a freshwater plume while ensuring that individual system components operate within their physical limitations. C1 [Talukder, Ashit] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Georgas, Nickitas; Herrington, Thomas; Blumberg, Alan F.] Stevens Inst Technol, Dept Civil Environm & Ocean Engn, Hoboken, NJ 07030 USA. RP Talukder, A (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ashit.talukder@jpl.nasa.gov OI Georgas, Nickitas/0000-0003-0917-4907 FU NASA [AIST-QRS-060017]; Office of Naval Research under ONR [N00014-08-1-0782] FX This work has been sponsored by the NASA Applied Information Systems Technology Program under AIST-QRS Award AIST-QRS-060017, and supported in part by the Office of Naval Research under ONR Grant Number N00014-08-1-0782. The research described in this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 27 TC 3 Z9 3 U1 1 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD DEC PY 2010 VL 3 IS 4 BP 442 EP 450 DI 10.1109/JSTARS.2010.2050463 PN 1 PG 9 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 695GN UT WOS:000285358700005 ER PT J AU Tian, YD Geiger, JV Su, HB Kumar, SV Houser, PR AF Tian, Yudong Geiger, James V., Jr. Su, Hongbo Kumar, Sujay V. Houser, Paul R. TI Middleware-Based Sensor Web Integration SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Distributed information systems; enterprise application integration; land information system; messaging; middleware; sensor web; service-oriented architecture ID SYSTEM AB The Earth observation sensor web enables multiple-way interaction between earth observing sensors, sensor networks, Earth science models, and decision support systems. To achieve this goal, flexible and reliable integration between these disparate components is needed. In this study, a middleware-based, message-driven integration paradigm is proposed and implemented with the Land Information Sensor Web (LISW), to link a high-performance land surface modeling system with sensor simulators and other sensor web components, under a service-oriented architecture. OGC Sensor Web Enablement standard is adopted for interoperability. The middleware played a key role in enabling an integrated real-time sensor web with demonstrated simplicity, resilience and flexibility. We recommend that middleware-based integration should be adopted as a standard model in a wide range of sensor web applications, to replace the conventional point-to-point, client-server model. C1 [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Geiger, James V., Jr.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Su, Hongbo] Ctr Res Environm & Water, Calverton, MD 20705 USA. [Kumar, Sujay V.] Sci Applicat Int Corp, Beltsville, MD 20705 USA. [Houser, Paul R.] George Mason Univ, Dept Geog & Geoinformat Sci, Fairfax, VA 22030 USA. RP Tian, YD (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. EM yudong.tian@nasa.gov RI Su, Hongbo/C-9490-2009; Houser, Paul/J-9515-2013; Kumar, Sujay/B-8142-2015 OI Houser, Paul/0000-0002-2991-0441; FU National Aeronautics and Space Administration [AIST-05-0093] FX This work was supported by the National Aeronautics and Space Administration Advanced Information Systems Technology Program under Grant AIST-05-0093. NR 14 TC 3 Z9 3 U1 1 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD DEC PY 2010 VL 3 IS 4 BP 467 EP 472 DI 10.1109/JSTARS.2010.2049732 PN 1 PG 6 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 695GN UT WOS:000285358700007 ER PT J AU Garay, MJ Burl, MC AF Garay, Michael J. Burl, Michael C. TI Adaptive Sky: From Instrument Pixels to a Sensor Web Gestalt SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Image analysis; image segmentation; intelligent systems; multisensor systems; object detection; software packages; remote sensing ID SYSTEM AB A variety of sensors have been developed and deployed to monitor the Earth, ranging from in situ seismographic networks to hyperspectral imaging instruments carried onboard NASA satellites. Despite an impressive collection of sensing assets, there is still much untapped potential, as evidenced by the limited number of studies that successfully employ high-resolution data from multiple instruments. Sensor webs offer the potential to go beyond simple data fusion by dynamically combining sensing assets into coordinated, multi-instrument observers of specific geophysical objects, phenomena, and processes. In this paper, we describe Adaptive Sky, an algorithm package for sensor webs developed through funding from the NASA Earth Science Technology Office under the Advanced Information Systems Technology program. Fundamentally, Adaptive Sky aims to relate the observations from one sensor at time to the observations from another sensor at time t', providing a "gestalt," or unified, perspective that is more than the sum of its parts. A scenario involving the eruption of Bezymianny Volcano on the remote Kamchatka Peninsula on 14 October 2007 demonstrates conceptually how Adaptive Sky can be leveraged to create unprecedented spatio-temporal and phenomenological coverage of a complex geophysical event of interest, despite limitations inherent in the individual sensors. C1 [Garay, Michael J.] Raytheon Co, Pasadena, CA 91101 USA. [Burl, Michael C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Garay, MJ (reprint author), Raytheon Co, Pasadena, CA 91101 USA. EM michael.j.garay@jpl.nasa.gov FU National Aeronautics and Space Administration FX This research was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. The MISR and CALIPSO data were obtained from the NASA Langley Research Atmospheric Science Data Center. The MODIS data were obtained from the Level 1 and Atmosphere Archive and Distribution System. The GOES-West data were obtained from the NOAA Comprehensive Large Array-data Stewardship System (CLASS). Funding was provided by NASA ESTO under the AIST program. NR 32 TC 0 Z9 0 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD DEC PY 2010 VL 3 IS 4 BP 481 EP 487 DI 10.1109/JSTARS.2010.2052790 PN 1 PG 7 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 695GN UT WOS:000285358700009 ER PT J AU Howe, BM Chao, Y Arabshahi, P Roy, S McGinnis, T Gray, A AF Howe, Bruce M. Chao, Yi Arabshahi, Payman Roy, Sumit McGinnis, Tim Gray, Andrew TI A Smart Sensor Web for Ocean Observation: Fixed and Mobile Platforms, Integrated Acoustics, Satellites and Predictive Modeling SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Acoustic communication; acoustic navigation; mission planning; moored profilers; inductive power transfer; underwater gliders ID MONTEREY BAY; SYSTEM; TIDES; CALIFORNIA AB In many areas of Earth science, including climate change research and operational oceanography, there is a need for near real-time integration of data from heterogeneous and spatially distributed sensors, in particular in situ and space-based sensors. The data integration, as provided by a smart sensor web, enables numerous improvements, namely, 1) adaptive sampling for more efficient use of expensive space-based and in situ sensing assets, 2) higher fidelity information gathering from data sources through integration of complementary data sets, and 3) improved sensor calibration. Our ocean-observing smart sensor web presented herein is composed of both mobile and fixed underwater in situ ocean sensing assets and Earth Observing System satellite sensors providing larger-scale sensing. An acoustic communications network forms a critical link in the web, facilitating adaptive sampling and calibration. We report on the development of various elements of this smart sensor web, including (a) a cable-connected mooring system with a profiler under real-time control with inductive battery charging; (b) a glider with integrated acoustic communications and broadband receiving capability; (c) an integrated acoustic navigation and communication network; (d) satellite sensor elements; and (e) a predictive model via the Regional Ocean Modeling System interacting with satellite sensor control. C1 [Howe, Bruce M.] Univ Hawaii Manoa, Dept Ocean & Resources Engn, Honolulu, HI 96822 USA. [Chao, Yi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chao, Yi] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Arabshahi, Payman; McGinnis, Tim] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA. [Roy, Sumit; Gray, Andrew] Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA. RP Howe, BM (reprint author), Univ Hawaii Manoa, Dept Ocean & Resources Engn, Honolulu, HI 96822 USA. EM bhowe@hawaii.edu RI Howe, Bruce/J-2807-2012 OI Howe, Bruce/0000-0001-5711-5253 FU NASA Earth Science Technology Office; National Science Foundation (NSF) [OCE 0330082]; Office of Naval Research (ONR) [N00014-05-1-0907] FX This work was supported in part by three projects. The integrated underwater/satellite sensor network science and technology development was funded by the NASA Earth Science Technology Office's Advanced Information Systems Technology (AIST) Program under Award AIST-05-0030. The mooring work was funded by the National Science Foundation (NSF) Ocean Technology and Interdisciplinary Coordination (OTIC) program, Grant OCE 0330082. The acoustic Seaglider work was funded by the Office of Naval Research (ONR), Grant N00014-05-1-0907. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). Computing support from the JPL Supercomputing Project is acknowledged. NR 33 TC 22 Z9 24 U1 2 U2 29 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD DEC PY 2010 VL 3 IS 4 BP 507 EP 521 DI 10.1109/JSTARS.2010.2052022 PN 1 PG 15 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 695GN UT WOS:000285358700012 ER PT J AU Song, WZ Shirazi, B Huang, RJ Xu, MS Peterson, N LaHusen, R Pallister, J Dzurisin, D Moran, S Lisowski, M Kedar, S Chien, S Webb, F Kiely, A Doubleday, J Davies, A Pieri, D AF Song, Wen-Zhan Shirazi, Behrooz Huang, Renjie Xu, Mingsen Peterson, Nina LaHusen, Rick Pallister, John Dzurisin, Dan Moran, Seth Lisowski, Mike Kedar, Sharon Chien, Steve Webb, Frank Kiely, Aaron Doubleday, Joshua Davies, Ashley Pieri, David TI Optimized Autonomous Space In-Situ Sensor Web for Volcano Monitoring SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE In-situ sensor web; volcano monitoring; wireless sensor network AB In response to NASA's announced requirement for Earth hazard monitoring sensor-web technology, a multidisciplinary team involving sensor-network experts (Washington State University), space scientists (JPL), and Earth scientists (USGS Cascade Volcano Observatory (CVO)), have developed a prototype of dynamic and scalable hazard monitoring sensor-web and applied it to volcano monitoring. The combined Optimized Autonomous Space -In-situ Sensor-web (OASIS) has two-way communication capability between ground and space assets, uses both space and ground data for optimal allocation of limited bandwidth resources on the ground, and uses smart management of competing demands for limited space assets. It also enables scalability and seamless infusion of future space and in-situ assets into the sensor-web. The space and in-situ control components of the system are integrated such that each element is capable of autonomously tasking the other. The ground in-situ was deployed into the craters and around the flanks of Mount St. Helens in July 2009, and linked to the command and control of the Earth Observing One (EO-1) satellite. C1 [Song, Wen-Zhan; Shirazi, Behrooz; Huang, Renjie; Xu, Mingsen; Peterson, Nina] Washington State Univ, Sensorweb Res Lab, Vancouver, WA 98686 USA. [LaHusen, Rick; Pallister, John; Dzurisin, Dan; Moran, Seth; Lisowski, Mike] US Geol Survey, Cascades Volcano Observ, Vancouver, WA 98683 USA. [Kedar, Sharon; Chien, Steve; Webb, Frank; Kiely, Aaron; Doubleday, Joshua; Davies, Ashley; Pieri, David] CALTECH, Jet Prop Lab, San Marino, CA 91108 USA. RP Song, WZ (reprint author), Washington State Univ, Sensorweb Res Lab, Vancouver, WA 98686 USA. EM songwz@wsu.edu; shirazi@wsu.edu; renjie_huang@wsu.edu; mingsen_xu@wsu.edu; npicone@wsu.edu; rlahusen@usgs.gov; jpallist@usgs.gov; dzurisin@usgs.gov; smoran@usgs.gov; mlisowski@usgs.gov; sharon.kedar@jpl.nasa.gov; steve.chien@jpl.nasa.gov; frank.webb@jpl.nasa.gov; aaron.b.kiely@jpl.nasa.gov; jdou-bled@jpl.nasa.gov; ashley.davies@jpl.nasa.gov; david.pieri@jpl.nasa.gov FU NASA ESTO AIST; USGS [NNX06AE42G] FX This work was supported by NASA ESTO AIST program and USGS Volcano Hazard program under the research grant NNX06AE42G. NR 17 TC 8 Z9 8 U1 0 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD DEC PY 2010 VL 3 IS 4 BP 541 EP 546 DI 10.1109/JSTARS.2010.2066549 PN 1 PG 6 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 695GN UT WOS:000285358700015 ER PT J AU Paillou, P Lopez, S Farr, T Rosenqvist, A AF Paillou, Philippe Lopez, Sylvia Farr, Tom Rosenqvist, Ake TI Mapping Subsurface Geology in Sahara Using L-Band SAR: First Results From the ALOS/PALSAR Imaging Radar SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE ALOS; craters; K&C initiative; paleo-hydrology; PALSAR; Sahara; subsurface geology; water resources ID GILF KEBIR REGION; EASTERN SAHARA; IMPACT CRATER; BIR-SAFSAF; EGYPT; FIELD; PALEODRAINAGE; PENETRATION; DISCOVERY; ORIGIN AB Within the framework of Kyoto & Carbon Initiative of the Japanese Space Agency (JAXA), we used JERS-1 and ALOS/PALSAR radar images to build regional and continental scale mosaics of Sahara. The unique capability of L-band SAR to map subsurface structures in arid areas revealed previously unknown geological features: craters, faults, paleo-rivers. The latter are of particular interest for water resource detection in arid regions. C1 [Paillou, Philippe; Lopez, Sylvia] Univ Bordeaux, UMR Lab, OASU, F-33271 Floirac, France. [Farr, Tom] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rosenqvist, Ake] SoloEO, S-14135 Stockholm, Sweden. RP Paillou, P (reprint author), Univ Bordeaux, UMR Lab, OASU, F-33271 Floirac, France. OI Farr, Thomas/0000-0001-5406-2096 FU CNES FX This work was done within the framework of the JAXA Kyoto & Carbon Initiative. JERS-1 and ALOS/PALSAR data were provided by JAXA EORC. The work was supported in part by CNES. NR 27 TC 9 Z9 9 U1 1 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD DEC PY 2010 VL 3 IS 4 BP 632 EP 636 DI 10.1109/JSTARS.2010.2056915 PN 2 PG 5 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 695GA UT WOS:000285357400008 ER PT J AU Cossio, TK Slatton, KC Carter, WE Shrestha, KY Harding, D AF Cossio, Tristan K. Slatton, K. Clint Carter, William E. Shrestha, Kris Y. Harding, David TI Predicting Small Target Detection Performance of Low-SNR Airborne Lidar SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Bathymetry; lidar; object detection; simulation ID LASER; ALTIMETERS; SPECTROMETRY; BACKSCATTER; SURFACE AB Recent technological advances in the performance of small micro-lasers and multi-channel multi-event photo-detectors have enabled the development of experimental airborne lidar (light detection and ranging) systems based on a low-SNR (LSNR) paradigm. Due to dense point spacing (tens of points per square meter) and sub-decimeter range resolution, LSNR lidar can likely enable detection of meter-scale targets that would go unnoticed by traditional lidar technology. Small vehicle obstructions and other similar targets in the beach and littoral zones are of particular interest, because of LSNR lidar's applicability to the near-shore environment and the general desire to improve detection of antivehicle and antipersonnel obstacles in the coastal zone. A target detection procedure is presented that exploits the detailed information available from LSNR lidar data while diminishing the effect of spurious noise events. Consideration is given to detection in both topographic and bathymetric scenarios. Data sets for target detection analysis are supplied by a numerical sensor simulator developed at the University of Florida. Target detection performance is evaluated as a function of environmental characteristics, such as water clarity and depth, and system parameters, specifically transmitted pulse energy and laser pulse repetition frequency. Analysis of results with regards to consideration for future system design is discussed. C1 [Cossio, Tristan K.] Johns Hopkins Univ, Appl Phys Lab, Natl Secur Technol Dept, Laurel, MD 21218 USA. [Carter, William E.; Shrestha, Kris Y.] Univ Florida, Dept Civil & Coastal Engn, Gainesville, FL 32611 USA. [Harding, David] NASA GSFC, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Cossio, TK (reprint author), Johns Hopkins Univ, Appl Phys Lab, Natl Secur Technol Dept, Laurel, MD 21218 USA. EM tristan.cossio@jhuapl.edu; bcarter@ce.ufl.edu; kshres@gmail.com; david.j.harding@nasa.gov RI Harding, David/F-5913-2012 NR 38 TC 19 Z9 20 U1 0 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD DEC PY 2010 VL 3 IS 4 BP 672 EP 688 DI 10.1109/JSTARS.2010.2053349 PN 2 PG 17 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 695GA UT WOS:000285357400011 ER PT J AU Xu, XL Liang, D Tsang, L Andreadis, KM Josberger, EG Lettenmaier, DP Cline, DW Yueh, SH AF Xu, Xiaolan Liang, Ding Tsang, Leung Andreadis, Konstantinos M. Josberger, Edward G. Lettenmaier, Dennis P. Cline, Donald W. Yueh, Simon H. TI Active Remote Sensing of Snow Using NMM3D/DMRT and Comparison With CLPX II Airborne Data SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE CLPX; dense media radiative transfer; numerical Maxwell model; QCA; snow; VIC ID RADIATIVE-TRANSFER THEORY; SIMULATIONS; EXTINCTION; SCATTERING; MODEL AB We applied the Numerical Maxwell Model of three-dimensional simulations (NMM3D) in the Dense Media Radiative Theory (DMRT) to calculate backscattering coefficients. The particles' positions are computer-generated and the subsequent Foldy-Lax equations solved numerically. The phase matrix in NMM3D has significant cross-polarization, particularly when the particles are densely packed. The NMM3D model is combined with DMRT in calculating the microwave scattering by dry snow. The NMM3D/DMRT equations are solved by an iterative solution up to the second order in the case of small to moderate optical thickness. The numerical results of NMM3D/DMRT are illustrated and compared with QCA/DMRT. The QCA/DMRT and NMM3D/DMRT results are also applied to compare with data from two specific datasets from the second Cold Land Processes Experiment (CLPX II) in Alaska and Colorado. The data are obtained at the Ku-band (13.95 GHz) observations using airborne imaging polarimetric scatterometer (POLSCAT). It is shown that the model predictions agree with the field measurements for both co-polarization and cross-polarization. For the Alaska region, the average snow depth and snow density are used as the inputs for DMRT. The grain size, selected from within the range of the ground measurements, is used as a best-fit parameter within the range. For the Colorado region, we use the Variable Infiltration Capacity Model (VIC) to obtain the input snow profiles for NMM3D/DMRT. C1 [Xu, Xiaolan; Liang, Ding; Tsang, Leung] Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA. [Andreadis, Konstantinos M.; Lettenmaier, Dennis P.] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. [Josberger, Edward G.] US Geol Survey, Washington Water Sci Ctr, Tacoma, WA 98402 USA. [Cline, Donald W.] NOAA, Natl Operat Hydrol Remote Sensing Ctr, Chanhassen, MN 55317 USA. [Yueh, Simon H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Xu, XL (reprint author), Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA. EM xlxu@uw.edu RI Liang, Ding/F-7460-2012; Liang, Ding/K-6959-2012; lettenmaier, dennis/F-8780-2011 OI lettenmaier, dennis/0000-0003-3317-1327 FU National Aeronautics and Space Administration FX This work was supported in part by the National Aeronautics and Space Administration. NR 22 TC 11 Z9 12 U1 2 U2 19 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD DEC PY 2010 VL 3 IS 4 BP 689 EP 697 DI 10.1109/JSTARS.2010.2053919 PN 2 PG 9 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA 695GA UT WOS:000285357400012 ER PT J AU Barsoum, MF Moision, B Fitz, MP Divsalar, D Hamkins, J AF Barsoum, Maged F. Moision, Bruce Fitz, Michael P. Divsalar, Dariush Hamkins, Jon TI EXIT Function Aided Design of Iteratively Decodable Codes for the Poisson PPM Channel SO IEEE TRANSACTIONS ON COMMUNICATIONS LA English DT Article DE Error control coding; pulse position modulation; optical modulation; optical communication ID DETECTION PHOTON CHANNEL; PARITY-CHECK CODES; REED-SOLOMON; CAPACITY; COMMUNICATION; CONVERGENCE; MODULATION; SYSTEMS AB This paper presents and compares two iterative coded modulation techniques for deep-space optical communications using pulse-position modulation (PPM). The first code, denoted by SCPPM, consists of the serial concatenation of an outer convolutional code, an interleaver, a bit accumulator, and PPM. The second code, denoted by LDPC-PPM, consists of the serial concatenation of an LDPC code and PPM. We employ Extrinsic Information Transfer (EXIT) charts for their analysis and design. Under conditions typical of a communications link from Mars to Earth, SCPPM is 1 dB away from capacity, while LDPC-PPM is 1.4 dB away from capacity, at a Bit Error Rate (BER) of approximately 10(-5). However, LDPC-PPM lends itself naturally to low latency parallel processing in contrast to SCPPM. C1 [Moision, Bruce; Divsalar, Dariush; Hamkins, Jon] CALTECH, Jet Prop Lab, Informat Proc Grp, Pasadena, CA USA. [Fitz, Michael P.] Northrop Grumman Space Technol, Redondo Beach, CA 90278 USA. [Fitz, Michael P.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. EM maged.barsoum@engineering.ucla.edu; bmoision@jpl.nasa.gov; michael.fitz@ngc.com; dariush.divsalar@jpl.nasa.gov; jon.hamkins@jpl.nasa.gov FU IND Technology Program; National Aeronautics and Space Administration FX This work was funded by the IND Technology Program and performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The material in this paper was presented in part at the 2007 IEEE Information Theory Workshop, Lake Tahoe, California, September 2007. NR 34 TC 6 Z9 6 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0090-6778 EI 1558-0857 J9 IEEE T COMMUN JI IEEE Trans. Commun. PD DEC PY 2010 VL 58 IS 12 BP 3573 EP 3582 DI 10.1109/TCOMM.2010.110310.060572 PG 10 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 695FY UT WOS:000285357200028 ER PT J AU Zubko, V Leptoukh, GG Gopalan, A AF Zubko, Viktor Leptoukh, Gregory G. Gopalan, Arun TI Study of Data-Merging and Interpolation Methods for Use in an Interactive Online Analysis System: MODIS Terra and Aqua Daily Aerosol Case SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Aerosol optical thickness (AOT); Aqua; data fusion; data merging; interpolation; MODerate resolution Imaging Spectroradiometer (MODIS); optimal estimation; remote sensing; satellite applications; Terra ID OCEAN COLOR DATA; OPTICAL-THICKNESS; OBJECTIVE ANALYSIS; GOCART MODEL; SATELLITE; CLOUD; DISTRIBUTIONS; CLIMATOLOGY; INTEGRATION; RETRIEVALS AB Data merging with interpolation is a method of combining near-coincident satellite observations to provide complete global or regional maps for comparison with models and ground station observations. We investigate various methods and limitations of data merging (or data fusion), with and without interpolation, as a first step toward merging data sets archived in the National Aeronautics and Space Administration Goddard Earth Sciences Data and Information Services Center and made public through the Goddard Interactive Online Visualization and ANalysis Infrastructure (Giovanni) data portals. As a prototype for the data-merging algorithm, this paper uses daily global observations of aerosol optical thickness (AOT), as measured by the MODerate resolution Imaging Spectroradiometer onboard the Terra and Aqua satellites. The goal is to develop a very fast and accurate online method of data merging for implementation into Giovanni. We demonstrate three different methods for pure merging (without interpolation): simple arithmetic averaging (SAA), maximum likelihood estimate (MLE), and weighting by pixel counts. All three methods are roughly comparable, with the MLE (SAA) being slightly preferable when validating with respect to the AOT standard deviations (AOT means). To evaluate the merged product, we introduce two confidence functions, which characterize the percentage of the merged AOT pixels as a function of the relative deviation of the merged AOT from the initial Terra and Aqua AOTs. Eight combinations of merging-interpolation are applied to scenes with regular and irregular data gap patterns. Our results show that the merging-interpolation procedure can produce complete spatial fields with acceptable errors. C1 [Zubko, Viktor] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Leptoukh, Gregory G.; Gopalan, Arun] NASA, Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr, Greenbelt, MD 20771 USA. [Gopalan, Arun] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Zubko, V (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM Viktor.Zubko-1@nasa.gov; Gregory.Leptoukh@nasa.gov; Arun.Gopalan-1@nasa.gov NR 41 TC 5 Z9 6 U1 2 U2 16 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2010 VL 48 IS 12 BP 4219 EP 4235 DI 10.1109/TGRS.2010.2050893 PG 17 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 681YY UT WOS:000284361800007 ER PT J AU Ryu, D Jackson, TJ Bindlish, R Le Vine, DM Haken, M AF Ryu, Dongryeol Jackson, Thomas J. Bindlish, Rajat Le Vine, David M. Haken, Michael TI Soil Moisture Retrieval Using a Two-Dimensional L-Band Synthetic Aperture Radiometer in a Semiarid Environment SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Aperture synthesis; microwave radiometry; remote sensing; soil moisture ID WATER-CONTENT; DATA ASSIMILATION; SMOS MISSION; VEGETATION; TOPOGRAPHY; AIRCRAFT; CAMPAIGN AB Surface soil moisture was retrieved from the L-band radiometer data collected in semiarid regions during the Soil Moisture Experiment in 2004. The 2-D synthetic aperture radiometer (2D-STAR) was flown over regional-scale study sites located in AZ, USA, and Sonora, Mexico (SO). The study sites are characterized by a range of topographic relief with a land cover that varies from bare soil to grass and scrubland and includes areas with high rock fraction near the soil surface. The 2D-STAR retrieval of soil moisture was in good agreement with the ground-based estimates of surface soil moisture in both AZ (rmse = 0.012 m(3) m(-3)) and SO (rmse = 0.011 m(3) m(-3)). The 2D-STAR also showed a good performance in the Walnut Gulch Experimental Watershed (rmse = 0.014 m(3) m(-3)) where the surface soil featured high rock fraction was as high as 60%. Comparison of the results with the Polarimetric Scanning Radiometer at the C-and X-band data indicates the superior soil moisture retrieval performance of the L-band data over the regions with high rock fraction and moderate vegetation density. C1 [Ryu, Dongryeol] Univ Melbourne, Dept Civil & Environm Engn, Melbourne, Vic 3010, Australia. [Jackson, Thomas J.; Bindlish, Rajat] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. [Bindlish, Rajat; Haken, Michael] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Le Vine, David M.] NASA, Goddard Space Flight Ctr, Ocean Sci Branch, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Ryu, D (reprint author), Univ Melbourne, Dept Civil & Environm Engn, Melbourne, Vic 3010, Australia. EM Tom.Jackson@ars.usda.gov RI Ryu, Dongryeol/C-5903-2008 OI Ryu, Dongryeol/0000-0002-5335-6209 NR 40 TC 10 Z9 10 U1 0 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2010 VL 48 IS 12 BP 4273 EP 4284 DI 10.1109/TGRS.2010.2051677 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 681YY UT WOS:000284361800011 ER PT J AU Zebker, HA Hensley, S Shanker, P Wortham, C AF Zebker, Howard A. Hensley, Scott Shanker, Piyush Wortham, Cody TI Geodetically Accurate InSAR Data Processor SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Interferometric synthetic aperture radar (InSAR); motion compensation; radar interferometry; SAR processing; synthetic aperture radar (SAR) ID SYNTHETIC-APERTURE RADAR; PRECISE ORBIT DETERMINATION; GREENLAND ICE-SHEET; SAR INTERFEROMETRY; PERMANENT SCATTERERS; SATELLITE RADAR; SURFACE DEFORMATION; LANDERS EARTHQUAKE; SUBSIDENCE; CALIFORNIA AB We present a new interferometric synthetic aperture radar (InSAR) processing approach that capitalizes on the precise orbit tracking that is available with modern radar satellites. Our method uses an accurate orbit information along with motion-compensation techniques to propagate the radar echoes to positions along a noninertial virtual orbit frame in which the location and focusing equations are particularly simple, so that images are focused without requiring autofocus techniques and are computed efficiently. Motion compensation requires two additional focus correction phase terms that are implemented in the frequency domain. If the images from an interferometric pair or stack are all computed along the same reference orbit, flat-Earth topographic correction is not needed, and image coregistration is simplified, obviating many difficulties that are often encountered in InSAR processing. We process several data sets collected by the ALOS PALSAR instrument and find that the geodetic accuracy of the radar images is 10-20 m, with up to 20 m of additional image distortion needed to align 100 km x 100 km scenes with reference digital elevation models. We validated the accuracy by using both known radar corner reflector locations and by the registration of the interferograms with digital maps. The topography-corrected interferograms are free from all geometric phase terms, and they clearly show the geophysical observables of crustal deformation, atmospheric phase, and ionospheric phase. C1 [Zebker, Howard A.; Shanker, Piyush; Wortham, Cody] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Zebker, Howard A.; Shanker, Piyush; Wortham, Cody] Stanford Univ, Dept Geophys, Stanford, CA 94305 USA. [Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zebker, HA (reprint author), Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. EM zebker@stanford.edu NR 49 TC 17 Z9 21 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2010 VL 48 IS 12 BP 4309 EP 4321 DI 10.1109/TGRS.2010.2051333 PG 13 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 681YY UT WOS:000284361800014 ER PT J AU Woodard, SE AF Woodard, Stanley E. TI Functional Electrical Sensors as Single Component Electrically Open Circuits Having No Electrical Connections SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT LA English DT Article DE Fluid-level sensor; magnetic field response sensor; open-circuit sensor; SansEC; self-health monitoring sensor; wireless passive sensor ID DISTRIBUTED-CAPACITANCE MODEL; CHIP SPIRAL INDUCTORS; WIRELESS AB Closed circuits have been used in electrical systems since Alessandro Volta's invention of the modern battery in 1800 made the first closed electrical circuits possible. Even though a capacitor in a circuit could be considered as an open circuit, its use requires electrical connections to a circuit. This paper reports successful measurement of fluid level using a self-resonating planar pattern of electrically conductive material that is an open-circuit single-component sans electrical connections that is wirelessly powered using external oscillating magnetic fields. The circuit responded with its own magnetic harmonic that changed monotonically with the fluid level. The same external antenna received the circuit response providing a means of interrogating the sensor. By eliminating electrical connections, there is no single point that, if damaged, prevents the circuit from being powered and interrogated, thus, eliminating a key failure mode of electrical devices. Sensors used for the initial fluid-level measurements have portions of their circuits severed from the other portions. The damaged sensors were then successfully used to measure the fluid level. Although the results for fluid-level measurement are presented herein, theoretically, many electrical devices whose functions depend on the use of electric fields, magnetic fields or resistance could be developed as open circuits. The applications are far-reaching, from safer damage-resilient self-sensing human-implanted medical sensors to applications with vehicle systems, buildings, food processing and storage, package tamper detection and other measurements that can be related to capacitance, inductance or resistance. Furthermore, this work lays the foundation for developing other electrical components that can be designed without the use of closed circuits or electrical connections. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Woodard, SE (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. FU NASA Langley Research Center Institute of Creativity and Innovation; Advanced Planning and Partnership Office FX This work was supported by the NASA Langley Research Center Institute of Creativity and Innovation and the Advanced Planning and Partnership Office. The Associate Editor coordinating the review process for this paper was Dr. Tadeusz Dobrowiecki. NR 26 TC 6 Z9 6 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9456 J9 IEEE T INSTRUM MEAS JI IEEE Trans. Instrum. Meas. PD DEC PY 2010 VL 59 IS 12 BP 3206 EP 3213 DI 10.1109/TIM.2010.2047546 PG 8 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 678LN UT WOS:000284076000016 ER PT J AU Ponchak, GE AF Ponchak, George E. TI MINI-SPECIAL ISSUE ON ASIA-PACIFIC MICROWAVE CONFERENCE SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Editorial Material C1 [Ponchak, George E.] NASA Glenn Res Ctr, Commun Instrumentat & Controls Div, Cleveland, OH USA. [Ponchak, George E.] Case Western Reserve Univ, Cleveland, OH 44106 USA. [Ponchak, George E.] Cleveland Microwave Theory & Tech Soc MTT S, Cleveland, OH USA. [Ponchak, George E.] Antennas & Propagt Soc AP S, Cleveland Microwave Theory & Tech Soc, Cleveland, OH USA. RP Ponchak, GE (reprint author), NASA Glenn Res Ctr, Commun Instrumentat & Controls Div, Cleveland, OH USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9480 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD DEC PY 2010 VL 58 IS 12 BP 3391 EP 3397 DI 10.1109/TMTT.2010.2085150 PN 1 PG 7 WC Engineering, Electrical & Electronic SC Engineering GA 693SU UT WOS:000285246500001 ER PT J AU Ponchak, GE AF Ponchak, George E. TI SPECIAL ISSUE ON 2010 INTERNATIONAL MICROWAVE SYMPOSIUM SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Editorial Material C1 Nasa Glenn Res Ctr, Cleveland, OH 44135 USA. RP Ponchak, GE (reprint author), Nasa Glenn Res Ctr, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9480 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD DEC PY 2010 VL 58 IS 12 SI SI BP 3871 EP 3871 DI 10.1109/TMTT.2010.2088190 PN 2 PG 1 WC Engineering, Electrical & Electronic SC Engineering GA 693TA UT WOS:000285247100001 ER PT J AU Marshall, CJ Marshall, PW Ladbury, RL Waczynski, A Arora, R Foltz, RD Cressler, JD Kahle, DM Chen, DK Delo, GS Dodds, NA Pellish, JA Kan, E Boehm, N Reed, RA LaBel, KA AF Marshall, Cheryl J. Marshall, Paul W. Ladbury, Raymond L. Waczynski, Augustyn Arora, Rajan Foltz, Roger D. Cressler, John D. Kahle, Duncan M. Chen, Dakai Delo, Gregory S. Dodds, Nathaniel A. Pellish, Jonathan A. Kan, Emily Boehm, Nicholas Reed, Robert A. LaBel, Kenneth A. TI Mechanisms and Temperature Dependence of Single Event Latchup Observed in a CMOS Readout Integrated Circuit From 16-300 K SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Cryogenic latchup; low temperature electronics; readout integrated circuit; single event effects; single event latchup ID SILICON BIPOLAR-TRANSISTORS; BULK CMOS; DEVICES; BASE; GAIN AB Heavy ion-induced single event latchup (SEL) is characterized in a commercially available CMOS readout integrated circuit operating at cryogenic temperatures. SEL observed at 24 K and below is believed to be possible when free carriers produced by an ion strike initiate an exponential increase in the free carrier density via shallow-level impact ionization (SLII). This results in a large current increase that proceeds to a sustained latched state, even though the classic condition for parasitic bipolar gain product is not met since it is much less than unity. The LET threshold for SEL is significantly lower at 20 K as compared to 300 K although the saturated cross section is 2-3 times higher at 300 K. The temperature dependence of the SEL cross section is characterized from 16-300 K. SEL behavior attributed to the classical cross-coupled parasitic bipolar model is observed from similar to 135-300 K, and the reduction in the SEL cross section is remarkably modest as the temperature is lowered from room temperature to similar to 200 K. Temperature dependent electrical latchup characterization of a 130 nm pnpn test structure also indicates a change in the latchup behavior at similar to 50 K consistent with the SLII mechanism. C1 [Marshall, Cheryl J.; Ladbury, Raymond L.; Waczynski, Augustyn; Foltz, Roger D.; Kahle, Duncan M.; Pellish, Jonathan A.; Kan, Emily; LaBel, Kenneth A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Arora, Rajan; Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Chen, Dakai] MEI Technol Inc, Greenbelt, MD 20771 USA. [Delo, Gregory S.; Boehm, Nicholas] Global Sci & Technol Inc, Greenbelt, MD 20771 USA. [Dodds, Nathaniel A.; Reed, Robert A.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37235 USA. RP Marshall, CJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM cheryl.j.marshall@nasa.gov; pwmarshall@aol.com; raymond.l.lad-bury@nasa.gov; augustyn.waczynski-1@nasa.gov; arora@ece.gatech.edu; roger.d.foltz@nasa.gov; cressler@ece.gatech.edu; duncan.m.kahle@nasa.gov; dakai.chen-1@nasa.gov; gregory.s.delo@nasa.gov; nathaniel.dodds@vanderbilt.edu; jonathan.a.pellish@nasa.gov; emily.kan@nasa.gov; nicholas.boehm@nasa.gov; robert.reed@vanderbilt.edu; kenneth.a.label@nasa.gov FU NASA; NASA GSFC Internal Research and Development; NASA GSFC FX This work was supported in part by the NASA Electronic Parts and Packaging Program, NASA GSFC Internal Research and Development, and NASA GSFC flight projects. NR 24 TC 2 Z9 2 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3078 EP 3086 DI 10.1109/TNS.2010.2085018 PN 1 PG 9 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200011 ER PT J AU Kim, W Jun, I Kokorowski, M AF Kim, Wousik Jun, Insoo Kokorowski, Michael TI Internal Electrostatic Discharge Monitor (IESDM) SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Internal electrostatic discharge (IESD); radiation induced conductivity AB An internal electrostatic discharge monitor (IESDM) is being developed at JPL that measures the depth profile of potential in dielectrics. The JPL IESDM is described in this paper with an initial test result using electron beam. C1 [Kim, Wousik; Jun, Insoo; Kokorowski, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kim, W (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Wousik.Kim@jpl.nasa.gov; Insoo.Jun@jpl.nasa.gov; Michael.Kokorowski@jpl.nasa.gov NR 9 TC 3 Z9 3 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3143 EP 3147 DI 10.1109/TNS.2010.2084594 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200020 ER PT J AU O'Neill, PM AF O'Neill, Patrick M. TI Badhwar-O'Neill 2010 Galactic Cosmic Ray Flux Model-Revised SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Advanced composition explorer; galactic cosmic rays (GCRs); heliosphere; radiation environment; single-event effect; solar modulation; sunspot number ID ENERGY-SPECTRA; CHARGE COMPOSITION; NUCLEI; IRON; ABUNDANCES AB The Badhwar-O'Neill galactic cosmic ray (GCR) model has been revised to model all balloon and satellite GCR measurements since 1955. This includes the newer 1997-2010 Advanced Composition Explorer (ACE) measurements and spans six solar cycles. C1 NASA, Avion Syst Div, Johnson Space Ctr, Houston, TX 77058 USA. RP O'Neill, PM (reprint author), NASA, Avion Syst Div, Johnson Space Ctr, Houston, TX 77058 USA. EM patrick.m.oneill@.nasa.gov NR 24 TC 68 Z9 68 U1 0 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3148 EP 3153 DI 10.1109/TNS.2010.2083688 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200021 ER PT J AU Pellish, JA Xapsos, MA Stauffer, CA Jordan, TM Sanders, AB Ladbury, RL Oldham, TR Marshall, PW Heidel, DF Rodbell, KP AF Pellish, Jonathan A. Xapsos, Michael A. Stauffer, Craig A. Jordan, Thomas M. Sanders, Anthony B. Ladbury, Raymond L. Oldham, Timothy R. Marshall, Paul W. Heidel, David F. Rodbell, Kenneth P. TI Impact of Spacecraft Shielding on Direct Ionization Soft Error Rates for Sub-130 nm Technologies SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Direct ionization; radiation transport; soft error rate; space environment ID SINGLE-EVENT-UPSETS; MEMORY CELLS; SOI SRAM; ENERGY; MODEL; MICROELECTRONICS; DEPENDENCE AB We use ray tracing software to model various levels of spacecraft shielding complexity and energy deposition pulse height analysis to study how it affects the direct ionization soft error rate of microelectronic components in space. The analysis incorporates the galactic cosmic ray background, trapped proton, and solar heavy ion environments as well as the October 1989 and July 2000 solar particle events. C1 [Pellish, Jonathan A.; Oldham, Timothy R.] NASA, Goddard Space Flight Ctr, Perot Syst Govt Serv Inc, Greenbelt, MD 20771 USA. [Stauffer, Craig A.] MEI Technol, Seabrook, MD 20706 USA. [Jordan, Thomas M.] EMPC, Gaithersburg, MD 20885 USA. [Marshall, Paul W.] NASA, Brookneal, VA 24528 USA. [Heidel, David F.; Rodbell, Kenneth P.] IBM Corp, Thomas J Watson Res Ctr, Yorktown Hts, NY 10598 USA. RP Pellish, JA (reprint author), NASA, Goddard Space Flight Ctr, Perot Syst Govt Serv Inc, Code 561-4, Greenbelt, MD 20771 USA. EM jonathan.a.pellish@nasa.gov; michael.a.xapsos@nasa.gov; craig.a.stauffer@nasa.gov; tj@empc.com; anthony.b.sanders@nasa.gov; raymond.l.lad-bury@nasa.gov; tim-othy.r.oldham@nasa.gov; pwmarshall@aol.com; heidel@us.ibm.com; rodbell@us.ibm.com FU NASA/GSFC; NASA; Defense Threat Reduction Agency [09-4587I, 10-4977I] FX Manuscript received July 16, 2010; revised September 28, 2010; accepted September 29, 2010. Date of current version December 15, 2010. This work was supported in part by NASA/GSFC's Internal Research and Development program, the NASA Magnetospheric MultiScale mission, the NASA Electronic Parts and Packaging program, and the Defense Threat Reduction Agency Radiation Hardened Microelectronics program under IACROs #09-4587I and #10-4977I to NASA. NR 31 TC 10 Z9 10 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3183 EP 3189 DI 10.1109/TNS.2010.2084595 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200026 ER PT J AU Xu, ZY Niu, GF Luo, L Cressler, JD Alles, ML Reed, R Mantooth, HA Holmes, J Marshall, PW AF Xu, Ziyan Niu, Guofu Luo, Lan Cressler, John D. Alles, Michael L. Reed, Robert Mantooth, H. Alan Holmes, James Marshall, Paul W. TI Charge Collection and SEU in SiGe HBT Current Mode Logic Operating at Cryogenic Temperatures SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Charge collection; cryogenic temperature; SiGe HBT; single-event upset ID EXTREME ENVIRONMENT ELECTRONICS; DIGITAL LOGIC; PERFORMANCE; TRANSIENTS; CIRCUITS; IMPACT AB This paper investigates cryogenic temperature charge collection and single-event upset (SEU) in SiGe HBT devices and logic circuits using 3-D device simulation and circuit simulation. Cryogenic temperature circuit simulation is enabled by a new SiGe HBT compact model developed for wide temperature range operation. Incomplete ionization was found to impact charge collection below 130 K. With cooling, collector-substrate (CS) junction peak current I-CS and integral charge Q(CS) first increase, and then decrease below 130 K. Circuit SEU immunity is found to be nearly independent of temperature above 150 K and improve with further cooling, suggesting no additional hardening is required for cryogenic temperature operation. C1 [Xu, Ziyan; Niu, Guofu; Luo, Lan] Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. [Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Alles, Michael L.; Reed, Robert] Vanderbilt Univ, Nashville, TN 37235 USA. [Mantooth, H. Alan] Univ Arkansas, Fayetteville, AR 72701 USA. [Holmes, James] Lynguent Inc, Fayetteville, AR 72701 USA. [Marshall, Paul W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Xu, ZY (reprint author), Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. EM zzx0001@auburn.edu FU NASA ETDP [NNL06AA29C] FX Manuscript received July 16, 2010; revised August 27, 2010; accepted August 30, 2010. Date of current version December 15, 2010. This work was supported by NASA ETDP under Grant NNL06AA29C. NR 19 TC 4 Z9 4 U1 2 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3206 EP 3211 DI 10.1109/TNS.2010.2085050 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200029 ER PT J AU Sierawski, BD Mendenhall, MH Reed, RA Clemens, MA Weller, RA Schrimpf, RD Blackmore, EW Trinczek, M Hitti, B Pellish, JA Baumann, RC Wen, SJ Wong, R Tam, N AF Sierawski, Brian D. Mendenhall, Marcus H. Reed, Robert A. Clemens, Michael A. Weller, Robert A. Schrimpf, Ronald D. Blackmore, Ewart W. Trinczek, Michael Hitti, Bassam Pellish, Jonathan A. Baumann, Robert C. Wen, Shi-Jie Wong, Rick Tam, Nelson TI Muon-Induced Single Event Upsets in Deep-Submicron Technology SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Direct ionization; Geant4; Monte Carlo; muons; single event upset (SEU); static random access memory (SRAM) ID SILICON-ON-INSULATOR; MEMORY CELLS; STATIC RAMS; LATCHES AB Experimental data are presented that show low-energy muons are able to cause single event upsets in 65 nm, 45 nm, and 40 nm CMOS SRAMs. Energy deposition measurements using a surface barrier detector are presented to characterize the kinetic energy spectra produced by the M20B surface muon beam at TRIUMF. A Geant4 application is used to simulate the beam and estimate the energy spectra incident on the memories. Results indicate that the sensitivity to this mechanism will increase for scaled technologies. C1 [Sierawski, Brian D.] Vanderbilt Univ, Inst Space & Def Elect, Nashville, TN 37203 USA. [Mendenhall, Marcus H.; Reed, Robert A.; Clemens, Michael A.; Weller, Robert A.; Schrimpf, Ronald D.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37203 USA. [Blackmore, Ewart W.; Trinczek, Michael; Hitti, Bassam] TRIUMF, Vancouver, BC V6T 2A3, Canada. [Pellish, Jonathan A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Baumann, Robert C.] Texas Instruments Inc, Dallas, TX 75243 USA. [Wen, Shi-Jie; Wong, Rick] Cisco Syst Inc, San Jose, CA 95134 USA. [Tam, Nelson] Marvell Semicond Inc, Santa Clara, CA 95054 USA. RP Sierawski, BD (reprint author), Vanderbilt Univ, Inst Space & Def Elect, Nashville, TN 37203 USA. EM brian.sierawski@vander-bilt.edu RI Schrimpf, Ronald/L-5549-2013 OI Schrimpf, Ronald/0000-0001-7419-2701 FU Defense Threat Reduction Agency [HDTRA1-08-1-003, HDTRA1-08-1-0034, IACROs 09-45871, 10-49771]; NASA FX Manuscript received July 16, 2010; revised September 10, 2010; accepted September 12, 2010. Date of current version December 15, 2010. This work was supported in part by Defense Threat Reduction Agency Grants HDTRA1-08-1-003 and HDTRA1-08-1-0034, the Defense Threat Reduction Agency Radiation Hardened Microelectronics Program under IACROs 09-45871 and 10-49771 to NASA, and the NASA Electronic Parts and Packaging Program. NR 16 TC 35 Z9 36 U1 0 U2 17 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3273 EP 3278 DI 10.1109/TNS.2010.2080689 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200040 ER PT J AU Johnston, AH Swimm, RT Miyahira, TF AF Johnston, A. H. Swimm, R. T. Miyahira, T. F. TI Low Dose Rate Effects in Shallow Trench Isolation Regions SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE CMOS; modeling; radiation effects; shallow trench isolation (STI); total dose ID X-RAY; BIPOLAR-DEVICES; OXIDES; CIRCUITS; CO-60; TRANSISTORS; LEAKAGE AB Dose-rate effects are studied in shallow trench isolation regions. Increased damage is observed at low dose rate, with a different dose dependence compared to tests done at high dose rate. A three-dimensional modeling program was used to show that charge trapping occurs much deeper in the trench region when sufficient charge is present to reduce the field in the trench. C1 [Johnston, A. H.; Swimm, R. T.; Miyahira, T. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnston, AH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM allan.h.johnston@jpl.nasa.gov; randall.t.swimm@jpl.nasa.gov; tetsuo.f.miyahira@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA) FX Manuscript received July 23, 2010; revised September 10, 2010, September 15, 2010, and October 01, 2010; accepted October 04, 2010. Date of current version December 15, 2010. This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). NR 20 TC 10 Z9 10 U1 1 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3279 EP 3287 DI 10.1109/TNS.2010.2085452 PN 1 PG 9 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200041 ER PT J AU Wilcox, EP Phillips, SD Cheng, P Thrivikraman, T Madan, A Cressler, JD Vizkelethy, G Marshall, PW Marshall, C Babcock, JA Kruckmeyer, K Eddy, R Cestra, G Zhang, BY AF Wilcox, Edward P. Phillips, Stanley D. Cheng, Peng Thrivikraman, Tushar Madan, Anuj Cressler, John D. Vizkelethy, Gyorgy Marshall, Paul W. Marshall, Cheryl Babcock, Jeff A. Kruckmeyer, Kirby Eddy, Robert Cestra, Greg Zhang, Benyong TI Single Event Transient Hardness of a New Complementary (npn plus pnp) SiGe HBT Technology on Thick-Film SOI SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Radiation hardening; silicon-germanium; silicon on insulator; single event upset ID INDUCED CHARGE COLLECTION; PERFORMANCE; SIMULATION; CIRCUITS; PROTON; LOGIC AB We report heavy-ion microbeam and total dose data for a new complementary (npn + pnp) SiGe on thick-film SOI technology. Measured transient waveforms from heavy-ion strikes indicate a significantly shortened single-event-induced transient current, while maintaining the total dose robustness associated with SiGe devices. Heavy-ion broad-beam data confirm a reduced single event upset (SEU) cross-section in a high-speed shift register circuit. C1 [Phillips, Stanley D.; Cheng, Peng; Thrivikraman, Tushar; Madan, Anuj; Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Vizkelethy, Gyorgy] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Marshall, Paul W.] NASA, Goddard Space Flight Ctr, Brookneal, VA 24538 USA. [Babcock, Jeff A.; Kruckmeyer, Kirby; Eddy, Robert; Cestra, Greg; Zhang, Benyong] Natl Semicond Corp, Santa Clara, CA 95052 USA. RP Wilcox, EP (reprint author), NASA, Goddard Space Flight Ctr, MEI Technol, Code 561-4, Greenbelt, MD 20771 USA. EM gvizkel@sandia.gov FU National Semiconductor; NASA-GSFC under the NASA; AFOSR MURI; United States Department of Energy's National Nuclear Security Administration [DE-AC04-94AL8500] FX Manuscript received July 16, 2010; revised August 26, 2010 and September 09, 2010; accepted September 10, 2010. Date of current version December 15, 2010. This work was supported by National Semiconductor, NASA-GSFC under the NASA Electronic Parts and Packaging (NEPP) program, an AFOSR MURI program, and Sandia National Labs, a multi-program laboratory operated by Sandia Corporation, a Lockheed Martin Company, for the United States Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL8500. NR 16 TC 10 Z9 10 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3293 EP 3297 DI 10.1109/TNS.2010.2085014 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200043 ER PT J AU Turowski, M Pellish, JA Moen, KA Raman, A Cressler, JD Reed, RA Niu, GF AF Turowski, Marek Pellish, Jonathan A. Moen, Kurt A. Raman, Ashok Cressler, John D. Reed, Robert A. Niu, Guofu TI Reconciling 3-D Mixed-Mode Simulations and Measured Single-Event Transients in SiGe HBTs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Mixed mode; nuclear and space radiation effects; radiation hardening; SiGe HBT; single event effects; single event transients; 3D semiconductor device modeling ID CHARGE COLLECTION; TRANSISTORS AB Comprehensive 3-D mixed-mode simulations, including accurate modeling of parasitic elements present in the experimental setup, resulted in close agreement between simulated and experimentally-measured heavy-ion-induced transients in first-generation SiGe HBTs. We have identified the key factors affecting previous simulations and observed experimental differences. The approach employed is also applicable to other submicron, high-speed technologies. Furthermore, we present a plausible answer to the previously unexplained issue of higher collector currents in single-transistor SiGe HBT single-event transients under positive collector bias. The new observations and conclusions facilitate improved understanding and potential mitigation options. C1 [Turowski, Marek; Raman, Ashok] CFD Res Corp CFDRC, Huntsville, AL 35805 USA. [Pellish, Jonathan A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Moen, Kurt A.; Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Reed, Robert A.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37235 USA. [Niu, Guofu] Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. RP Turowski, M (reprint author), CFD Res Corp CFDRC, Huntsville, AL 35805 USA. EM mt@cfdrc.com; jonathan.a.pellish@nasa.gov; cressler@ece.gatech.edu; robert.reed@vanderbilt.edu; niuguof@auburn.edu OI Moen, Kurt/0000-0001-7697-8636 FU NASA [NNM08AA07C, NNL06AA29C]; DTRA [IACROs 08-4343I, 09-4587I]; AFOSR MURI FX Manuscript received July 16, 2010; revised August 29, 2010; accepted August 31, 2010. Date of publication October 07, 2010; date of current version December 15, 2010. This work was supported in part by a NASA SBIR (Contract NNM08AA07C), the NASA Electronic Parts and Packaging Program, NASA ETDP project NNL06AA29C, the DTRA Radiation Hardened Microelectronics Program under Grants IACROs #08-4343I and #09-4587I to NASA, and in part by an AFOSR MURI grant. NR 21 TC 12 Z9 12 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3342 EP 3348 DI 10.1109/TNS.2010.2076835 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200050 ER PT J AU Horst, SJ Phillips, SD Saha, P Cressler, JD McMorrow, D Marshall, P AF Horst, Stephen J. Phillips, Stanley D. Saha, Prabir Cressler, John D. McMorrow, Dale Marshall, Paul TI A Theory of Single-Event Transient Response in Cross-Coupled Negative Resistance Oscillators SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE HBT; microwave oscillators; radiation effects; radiation hardening; SiGe; silicon-germanium; VCO ID VOLTAGE-CONTROLLED OSCILLATORS; TECHNOLOGY; HBTS AB A theory of the circuit-based response to SET phenomena in resonant tank oscillators is presented. Transients are shown to be caused by a change in the voltage state of the circuit's characteristic differential equation. The SET amplitude and phase response is derived for arbitrary strike waveforms and shown to be time-variant based on the strike time relative to the period of oscillation. Measurements in the time-domain are used to support the theory, while the frequency-domain is used to gauge potential impact on system performance. A design-oriented analysis of the relevant trade-offs is also presented. C1 [Horst, Stephen J.; Phillips, Stanley D.; Saha, Prabir; Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [McMorrow, Dale] USN, Res Lab, Washington, DC 20375 USA. [Marshall, Paul] NASA, Washington, DC 20024 USA. RP Horst, SJ (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM shorst@gatech.edu FU NASA; Defense Threat Reduction Agency [HDTRA1-09-C-0031] FX Manuscript received July 15, 2010; revised August 27, 2010, September 07, 2010; accepted September 07, 2010. Date of publication October 07, 2010; date of current version December 15, 2010. This work was supported in part by NASA and the Defense Threat Reduction Agency under HDTRA1-09-C-0031. NR 24 TC 10 Z9 10 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3349 EP 3357 DI 10.1109/TNS.2010.2076834 PN 1 PG 9 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200051 ER PT J AU Phillips, SD Moen, KA Najafizadeh, L Diestelhorst, RM Sutton, AK Cressler, JD Vizkelethy, G Dodd, PE Marshall, PW AF Phillips, Stan D. Moen, Kurt A. Najafizadeh, Laleh Diestelhorst, Ryan M. Sutton, Akil Khamsi Cressler, John D. Vizkelethy, Gyorgy Dodd, Paul E. Marshall, Paul W. TI A Comprehensive Understanding of the Efficacy of N-Ring SEE Hardening Methodologies in SiGe HBTs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE HBT; N-ring hardening; RHBD; SEE; SEU; SiGe; silicon-germanium technology ID SINGLE-EVENT TRANSIENTS; DEEP TRENCH ISOLATION; CIRCUITS; CHARGE; ANALOG; MITIGATION; COLLECTION; SIMULATION; DEVICES; CMOS AB We investigate the efficacy of mitigating radiation-based single event effects (SEE) within circuits incorporating SiGe heterojunction bipolar transistors (HBTs) built with an N-Ring, a transistor-level layout-based radiation hardened by design (RHBD) technique. Previous work of single-device ion-beam induced charge collection (IBICC) studies has demonstrated significant reductions in peak collector charge collection and sensitive area for charge collection; however, few circuit studies using this technique have been performed. Transient studies performed with Sandia National Laboratory's (SNL) 36 MeV O-16 microbeam on voltage references built with N-Ring SiGe HBTs have shown mixed results, with reductions in the number of large voltage disruptions in addition to new sensitive areas of low-level output voltage disturbances. Similar discrepancies between device-level IBICC results and circuit measurements are found for the case of digital shift registers implemented with N-Ring SiGe HBTs irradiated in a broadbeam environment at Texas A&M's Cyclotron Institute. The error cross-section curve of the N-Ring based register is found to be larger at larger ion LETs than the standard SiGe register, which is clearly counter-intuitive. We have worked to resolve the discrepancy between the measured circuit results and the device-level IBICC measurements, by re-measuring single-device N-Ring SiGe HBTs using a time-resolved ion beam induced charge (TRIBIC) set-up that allows direct capture of nodal transients. Coupling these measurements with full 3-D TCAD simulations provides complete insight into the origin of transient currents in an N-Ring SiGe HBT. The detailed structure of these transients and their bias dependencies are discussed, together with the ramifications for the design of space-borne analog and digital circuits using SiGe HBTs. C1 [Phillips, Stan D.; Moen, Kurt A.; Najafizadeh, Laleh; Diestelhorst, Ryan M.; Sutton, Akil Khamsi; Cressler, John D.] Georgia Inst Technol, Atlanta, GA 30308 USA. [Vizkelethy, Gyorgy; Dodd, Paul E.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Marshall, Paul W.] NASA, GSFC, Brookneal, VA 24528 USA. RP Phillips, SD (reprint author), Georgia Inst Technol, Atlanta, GA 30308 USA. EM stan.phillips@gatech.edu OI Moen, Kurt/0000-0001-7697-8636 FU Department of Energy; AFOSR MURI; NASA; DTRA; Sandia National Laboratories; U.S. Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000] FX Manuscript received July 15, 2010; revised August 23, 2010; accepted September 02, 2010. Date of current version December 15, 2010. This work was supported by the Department of Energy, AFOSR MURI, NASA, DTRA, and Sandia National Laboratories. Sandia National Laboratories is a multi-program laboratory operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Company, for the U.S. Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL85000. NR 20 TC 3 Z9 3 U1 1 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3400 EP 3406 DI 10.1109/TNS.2010.2077651 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200058 ER PT J AU Pease, RL Adell, PC Rax, B McClure, S Barnaby, HJ Kruckmeyer, K Triggs, B AF Pease, Ronald L. Adell, Philippe C. Rax, Bernard McClure, Steven Barnaby, Hugh J. Kruckmeyer, Kirby Triggs, B. TI Evaluation of an Accelerated ELDRS Test Using Molecular Hydrogen SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Bipolar linear circuits; discrete bipolar transistors; dose rate; enhanced low-dose-rate sensitivity (ELDRS); hydrogen; radiation effects; total ionizing dose ID BIPOLAR LINEAR CIRCUITS; LOW-DOSE-RATE; RATE SENSITIVITY ELDRS; RATE RESPONSE; RADIATION AB An accelerated total ionizing dose (TID) hardness assurance test for enhanced low dose rate sensitive (ELDRS) bipolar linear circuits, using high dose rate tests on parts that have been exposed to molecular hydrogen, has been proposed and demonstrated on several ELDRS part types. In this study several radiation-hardened "ELDRS-free" part types have been tested using this same approach to see if the test is overly conservative. C1 [Pease, Ronald L.] RLP Res, Los Lunas, NM 87031 USA. [Adell, Philippe C.; Rax, Bernard; McClure, Steven] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Barnaby, Hugh J.] Arizona State Univ, Tempe, AZ 85287 USA. [Kruckmeyer, Kirby] Natl Semicond Corp, Santa Clara, CA 95052 USA. [Triggs, B.] Semicoa Corp, Costa Mesa, CA 92626 USA. RP Pease, RL (reprint author), RLP Res, Los Lunas, NM 87031 USA. EM lsrlpease@wildblue.net; philippe.c.adell@jpl.nasa.gov; benard.g.rax@jpl.nasa.gov; stephen.s.mcclure@jpl.nasa.gov; hbarnaby@asu.edu; Kirby.kruckmeyer@nsc.com; btriggs@semicoa.com FU Defense Threat Reduction Agency [HDTRA1-09-C-0036]; Micro RDC; NASA FX This work was supported by the Defense Threat Reduction Agency through Contract HDTRA1-09-C-0036 with Micro RDC and by the NASA Electronic Parts and Packaging Program. NR 21 TC 1 Z9 1 U1 1 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3419 EP 3425 DI 10.1109/TNS.2010.2070806 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200061 ER PT J AU Allen, GR Edmonds, L Tseng, CW Swift, G Carmichael, C AF Allen, Gregory R. Edmonds, Larry Tseng, Chen Wei Swift, Gary Carmichael, Carl TI Single-Event Upset (SEU) Results of Embedded Error Detect and Correct Enabled Block Random Access Memory (Block RAM) Within the Xilinx XQR5VFX130 SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Error detect and correct; field programmable gate arrays (FPGA); single-event effects (SEV); upset mitigation ID MITIGATION; FPGAS AB Recent heavy ion measurements of the single-event upset (SEU) cross section for 65 nm embedded block random access memory (Block RAM) are presented. Results of initial investigation into the on-chip Error Detection and Correction (EDAC) are also discussed. C1 [Allen, Gregory R.; Edmonds, Larry] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tseng, Chen Wei; Swift, Gary; Carmichael, Carl] Xilinx Inc, San Jose, CA 95124 USA. RP Allen, GR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Gregory.R.Allen@jpl.nasa.gov; Larry.D.Edmonds@jpl.nasa.gov FU National Aeronautic and Space Administration (NASA) FX This work was supported in part by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautic and Space Administration (NASA) with funding from the NASA Electronics Parts Program (NEPP). NR 9 TC 8 Z9 8 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3426 EP 3431 DI 10.1109/TNS.2010.2085447 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200062 ER PT J AU Ladbury, R AF Ladbury, R. TI Statistical Techniques for Analyzing Process or "Similarity" Data in TID Hardness Assurance SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Quality assurance; radiation effects; reliability estimation AB We investigate techniques for estimating the contributions to TID hardness variability for families of linear bipolar technologies, determining how part-to-part and lot-to-lot variability change for different part types in the process. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ladbury, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Raymond.L.Ladbury.1@gsfc.nasa.gov FU NASA; Landsat Data Continuity Mission FX This research was supported in part by NASA's Electronic Parts and Packaging (NEPP) program and the Landsat Data Continuity Mission. NR 11 TC 1 Z9 1 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3432 EP 3437 DI 10.1109/TNS.2010.2086480 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200063 ER PT J AU Lauenstein, JM Ladbury, RL Goldsman, N Kim, HS Batchelor, DA Phan, AM AF Lauenstein, Jean-Marie Ladbury, Raymond L. Goldsman, Neil Kim, Hak S. Batchelor, David A. Phan, Anthony M. TI Interpreting Space-Mission LET Requirements for SEGR in Power MOSFETs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Heavy ion; linear enery transfer (LET); single-event gate rupture (SEGR); vertical power MOSFET ID SINGLE-EVENT BURNOUT; ENERGY DEPOSITION; GATE RUPTURE; ION ENERGY; DMOSFETS; EXPRESSION; FAILURE AB A TCAD simulation-based method is developed to evaluate whether derating of high-energy heavy-ion accelerator test data bounds the risk for single-event gate rupture (SEGR) from much higher energy on-orbit ions for a mission linear energy transfer (LET) requirement. It is shown that a typical derating factor of 0.75 applied to a single-event effect (SEE) response curve defined by high-energy accelerator SEGR test data provides reasonable on-orbit hardness assurance, although in a high-voltage power MOSFET, it did not bound the risk of failure. C1 [Lauenstein, Jean-Marie; Ladbury, Raymond L.; Batchelor, David A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Goldsman, Neil] Univ Maryland, Dept Elect & Comp Engn, College Pk, MD 20742 USA. [Kim, Hak S.; Phan, Anthony M.] MEI Technol Inc, Seabrook, MD 20706 USA. RP Lauenstein, JM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jean.m.lauen-stein@nasa.gov FU National Aeronautics and Space Administration's (NASA); Defense Threat Reduction Agency [IACRO10-4977I]; NASA Goddard Space Flight Center FX This work was supported in part by the National Aeronautics and Space Administration's (NASA) Electronic Parts and Packaging Program, NASA Flight Projects, the Defense Threat Reduction Agency under IACRO10-4977I, and the NASA Goddard Space Flight Center Internal Research and Development Program. This work was conducted in part using the resources of the Advanced Computing Center for Research and Education at Vanderbilt University, Nashville, TN. NR 25 TC 3 Z9 6 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3443 EP 3449 DI 10.1109/TNS.2010.2086486 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200065 ER PT J AU Edmonds, LD Scheick, LZ AF Edmonds, L. D. Scheick, L. Z. TI Effect of Shielding on Single-Event Rates in Devices That Are Sensitive to Particle Range SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Low-energy rate; single-event gate rupture (SEGR); single-event rate ID POWER MOSFETS; SEGR; DMOSFETS; ENERGY AB Single-event rates in space can include contributions from low-energy particles such that the LET is not constant. A rate calculation algorithm for such a situation is derived. C1 [Edmonds, L. D.; Scheick, L. Z.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Edmonds, LD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM larry.d.edmonds@jpl.nasa.gov; leif.z.scheick@jpl.nasa.gov FU National Aeronautics and Space Administration FX Manuscript received July 15, 2010; revised September 09, 2010; accepted September 12, 2010. Date of current version December 15, 2010. The research in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Reference herein to any specific commercial product, process, or service by trade name, manufacturer, or otherwise, does not constitute or imply its endorsement by the U.S. Government or the Jet Propulsion Laboratory, California Institute of Technology. NR 8 TC 4 Z9 4 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3560 EP 3569 DI 10.1109/TNS.2010.2078835 PN 1 PG 10 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200081 ER PT J AU Dodds, NA Hutson, JM Pellish, JA Reed, RA Kim, HS Berg, MD Friendlich, MR Phan, AM Seidleck, CM Xapsos, MA Deng, X Baumann, RC Schrimpf, RD King, MP Massengill, LW Weller, RA AF Dodds, N. A. Hutson, J. M. Pellish, J. A. Reed, R. A. Kim, H. S. Berg, M. D. Friendlich, M. R. Phan, A. M. Seidleck, C. M. Xapsos, M. A. Deng, X. Baumann, R. C. Schrimpf, R. D. King, M. P. Massengill, L. W. Weller, R. A. TI Selection of Well Contact Densities for Latchup-Immune Minimal-Area ICs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Design rule; external resistor; hardening by design; latchup test structure; single-event latchup ID SINGLE-EVENT LATCHUP; CMOS TECHNOLOGY; ENERGY; NM; ANGLE AB Heavy ion data for custom SRAMs fabricated in a 45-nm CMOS technology demonstrate the effects of N- and P-well contact densities on single-event latchup. Although scaling has improved latchup robustness, process-level immunity has not been achieved, indicating a continued need for latchup mitigation techniques. A simple, algorithmic approach for selecting N-and P-well contact densities is described that ensures latchup immunity while minimizing the area penalty. C1 [Dodds, N. A.; Reed, R. A.; Schrimpf, R. D.; King, M. P.; Massengill, L. W.; Weller, R. A.] Vanderbilt Univ, Nashville, TN 37203 USA. [Hutson, J. M.] Northrop Grumman Corp, Woodland Hills, CA 91367 USA. [Pellish, J. A.; Xapsos, M. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kim, H. S.; Berg, M. D.; Friendlich, M. R.; Phan, A. M.; Seidleck, C. M.] MEI Technol, Seabrook, MD 20706 USA. [Deng, X.; Baumann, R. C.] Texas Instruments Inc, Dallas, TX 75243 USA. RP Dodds, NA (reprint author), Vanderbilt Univ, Nashville, TN 37203 USA. EM nathaniel.dodds@vanderbilt.edu RI Schrimpf, Ronald/L-5549-2013 OI Schrimpf, Ronald/0000-0001-7419-2701 FU Defense Threat Reduction Agency [HDTRA1-08-1-0033, HDTRA1-08-1-0034, 09-4587I]; NASA FX Manuscript received July 14, 2010; revised August 30, 2010; accepted September 07, 2010. Date of current version December 15, 2010. This work was supported by the Defense Threat Reduction Agency under HDTRA1-08-1-0033 and HDTRA1-08-1-0034, by the DTRA Radiation Hardened Microelectronics Program under IACRO # 09-4587I to NASA, by the NASA Electronics Parts and Packaging Program, and by the NASA Graduate Student Researchers Program. NR 20 TC 8 Z9 8 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3575 EP 3581 DI 10.1109/TNS.2010.2082562 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200083 ER PT J AU Thrivikraman, TK Wilcox, E Phillips, SD Cressler, JD Marshall, C Vizkelethy, G Dodd, P Marshall, P AF Thrivikraman, Tushar K. Wilcox, Edward Phillips, Stanley D. Cressler, John D. Marshall, Cheryl Vizkelethy, Gyorgy Dodd, Paul Marshall, Paul TI Design of Digital Circuits Using Inverse-Mode Cascode SiGe HBTs for Single Event Upset Mitigation SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Digital circuits; heterojunction bipolar transistors; radiation hardening; silicon germanium ID LOGIC; PERFORMANCE; ELECTRONICS; ENVIRONMENT; TOLERANCE AB We report on the design and measured results of a new SiGe HBT radiation hardening by design technique called the "inverse- mode cascode" (IMC). A third-generation SiGe HBT IMC device was tested in a time resolved ion beam induced charge collection (TRIBICC) system, and was found to have over a 75% reduction in peak current transients with the use of an n-Tiedown on the IMC sub-collector node. Digital shift registers in a 1st-generation SiGe HBT technology were designed and measured under a heavy-ion beam, and shown to increase the LET threshold over standard npn only shift registers. Using the CREME96 tool, the expected orbital bit-errors/day were simulated to be approximately 70% lower with the IMC shift register. These measured results help demonstrate the efficacy of using the IMC device as a low-cost means for improving the SEE radiation hardness of SiGe HBT technology without increasing area or power. C1 [Thrivikraman, Tushar K.; Wilcox, Edward; Phillips, Stanley D.; Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Marshall, Cheryl] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vizkelethy, Gyorgy; Dodd, Paul] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Marshall, Paul] NASA, Brookneal, VA 24528 USA. RP Thrivikraman, TK (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM tthrivi@ece.gatech.edu FU NASA; Defense Threat Reduction Agency; AFOSR; U.S. Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000] FX Manuscript received July 15, 2010; revised August 31, 2010; accepted August 31, 2010. Date of current version December 15, 2010. This work was supported by the NASA SiGe ETDP program, the Defense Threat Reduction Agency under the Radiation Hardened Microelectronics Program, and NASA-GSFC under the NASA Electronic Parts and Packaging (NEPP) program, an AFOSR MURI program. Sandia National Laboratories is a multi-program laboratory operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin company, for the U.S. Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL85000. NR 11 TC 15 Z9 15 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3582 EP 3587 DI 10.1109/TNS.2010.2074214 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200084 ER PT J AU Adell, PC Vo, T Del Castillo, L Miyahira, T Thornbourn, D Mojarradi, M AF Adell, Philippe C. Vo, Tuan Del Castillo, Linda Miyahira, Tetsuo Thornbourn, Dennis Mojarradi, Mohammad TI A Rad-Hard Miniaturized Switching Module for High-Voltage Applications SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE Annealing; double-diffused metal-oxide semiconductor (DMOS) transistors; high-voltage power supply; radiation effects; radiation-hardening-by-design (RHBD); total dose AB A miniaturized, scalable, and rad-hard high-voltage module is demonstrated as a "proof-of-concept." The module is suitable for space applications. The design uses a commercial process that combines 0.25-mu m complementary metal-oxide semiconductor (CMOS) transistors with a high-voltage lateral double-diffused metal-oxide-semiconductor (DMOS) device (>600 V). The design was simulated, fabricated, and tested and shows functionality up to 2.5 kV. Several radiation-hardening-by-design (RHBD) techniques were used to improve radiation hardness over 100 krad. C1 [Adell, Philippe C.; Vo, Tuan; Del Castillo, Linda; Miyahira, Tetsuo; Thornbourn, Dennis; Mojarradi, Mohammad] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Adell, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM philippe.c.adell@jpl.nasa.gov FU NASA FX Manuscript received July 18, 2010; revised September 02, 2010; accepted September 06, 2010. Date of current version December 15, 2010. This work was supported by the NASA-JPL Research and Technology Development Program. NR 8 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3596 EP 3601 DI 10.1109/TNS.2010.2083692 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200086 ER PT J AU Wang, T Wang, K Chen, L Dinh, A Bhuva, B Shuler, R AF Wang, Tao Wang, Kuande Chen, Li Dinh, Anh Bhuva, Bharat Shuler, Robert TI A RHBD LC-Tank Oscillator Design Tolerant to Single-Event Transients SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT NUCLEAR AND SPACE RADIATION EFFECTS CONFERENCE (NSREC) CY JUL 19-23, 2010 CL Denver, CO DE LC-tank voltage-controlled oscillator (VCO); radiation-hardened-by-design (RHBD); single-event transients (SETs) ID VOLTAGE-CONTROLLED OSCILLATORS; PHASE-LOCKED LOOPS; TECHNOLOGY AB A single-event transients (SETs) tolerant LC-tank oscillator was designed, simulated, and fabricated using CMOS 90 nm technology. The simulation and experimental results indicate that the bias current of the oscillator greatly affects the SET-tolerance of an LC-tank oscillator. Adding a decoupling resistor to the bias circuit is an effective way to mitigate the effect of SETs to the oscillator. Laser testing and simulation results show significant reduction in the SET-induced amplitude and phase shifts of the VCO output. C1 [Wang, Tao; Wang, Kuande; Chen, Li; Dinh, Anh] Univ Saskatchewan, Dept Elect & Comp Engn, Saskatoon, SK S7N 5A9, Canada. [Bhuva, Bharat] Vanderbilt Univ, Elect Engn & Comp Sci Dept, Nashville, TN 37235 USA. [Shuler, Robert] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Wang, T (reprint author), Univ Saskatchewan, Dept Elect & Comp Engn, Saskatoon, SK S7N 5A9, Canada. EM li.chen@usask.ca FU National Sciences and Engineering Research Council of Canada (NSERC) [RGPIN-341549-2007, 407458] FX Manuscript received July 16, 2010; revised August 27, 2010 and September 10, 2010; accepted September 10, 2010. Date of current version December 15, 2010. This work was supported in part by the National Sciences and Engineering Research Council of Canada (NSERC) under Discovery Grant RGPIN-341549-2007 and Strategy Project Grant 407458. NR 15 TC 6 Z9 6 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2010 VL 57 IS 6 BP 3620 EP 3625 DI 10.1109/TNS.2010.2084593 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 695FE UT WOS:000285355200090 ER PT J AU Ivancic, W Eddy, WM Stewart, D Wood, L Northam, J Jackson, C AF Ivancic, W. Eddy, W. M. Stewart, D. Wood, L. Northam, J. Jackson, C. TI Experience with Delay-Tolerant Networking from orbit SO INTERNATIONAL JOURNAL OF SATELLITE COMMUNICATIONS AND NETWORKING LA English DT Article; Proceedings Paper CT 4th Advanced Satellite Mobile Systems (ASMS) Conference CY AUG 26-28, 2008 CL Univ Bolgna, Bologna, ITALY HO Univ Bolgna DE Internet; UK-DMC; satellite; Delay-Tolerant Networking (DTN); Bundle Protocol AB We describe the first use from space of the Bundle Protocol for Delay-Tolerant Networking (DTN) and lessons learned from experiments made and experience gained with this protocol. The Disaster Monitoring Constellation (DMC), constructed by Surrey Satellite Technology Ltd (SSTL), is a multiple-satellite Earth-imaging low-Earth-orbit sensor network in which recorded image swaths are stored onboard each satellite and later downloaded from the satellite payloads to a ground station. Store-and-forward of images with capture and later download gives each satellite the characteristics of a node in a disruption-tolerant network. Originally developed for the 'Interplanetary Internet,' DTNs are now under investigation in an Internet Research Task Force (IRTF) DTN research group (RG), which has developed a 'bundle' architecture and protocol. The DMC is technically advanced in its adoption of the Internet Protocol (IP) for its imaging payloads and for satellite command and control, based around reuse of commercial networking and link protocols. These satellites' use of IP has enabled earlier experiments with the Cisco router in Low Earth Orbit (CLEO) onboard the constellation's UK-DMC satellite. Earth images are downloaded from the satellites using a custom IP-based high-speed transfer protocol developed by SSTL, Saratoga, which tolerates unusual link environments. Saratoga has been documented in the Internet Engineering Task Force (IETF) for wider adoption. We experiment with the use of DTNRG bundle concepts onboard the UK-DMC satellite, by examining how Saratoga can be used as a DTN 'convergence layer' to carry the DTNRG Bundle Protocol, so that sensor images can be delivered to ground stations and beyond as bundles. Our practical experience with the first successful use of the DTNRG Bundle Protocol in a space environment gives us insights into the design of the Bundle Protocol and enables us to identify issues that must be addressed before wider deployment of the Bundle Protocol. Published in 2010 by John Wiley & Sons, Ltd. C1 [Ivancic, W.; Eddy, W. M.; Stewart, D.] NASA, Glenn Res Ctr, Cleveland, OH USA. [Eddy, W. M.; Stewart, D.] Verizon Fed Network Syst, Cleveland, OH USA. [Wood, L.] Cisco Syst Global Govt Solut Grp, London, England. [Northam, J.] Univ Surrey, Surrey Satellite Technol Ltd, Ground Syst Grp, Guildford GU2 7XH, Surrey, England. RP Wood, L (reprint author), Univ Surrey, Ctr Commun Syst Res, Guildford GU2 7XH, Surrey, England. EM wivancic@grc.nasa.gov; wes@mti-systems.com; dstewart@grc.nasa.gov; L.Wood@surrey.ac.uk; J.Northam@sstl.co.uk; C.Jackson@sstl.co.uk NR 24 TC 11 Z9 14 U1 1 U2 8 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 1542-0973 J9 INT J SATELL COMM N JI Int. J. Satell. Commun. Netw. PD DEC PY 2010 VL 28 IS 5-6 SI SI BP 335 EP 351 DI 10.1002/sat.966 PG 17 WC Engineering, Aerospace; Telecommunications SC Engineering; Telecommunications GA 662WO UT WOS:000282845200007 ER PT J AU Ferlay, N Thieuleux, F Cornet, C Davis, AB Dubuisson, P Ducos, F Parol, F Riedi, J Vanbauce, C AF Ferlay, Nicolas Thieuleux, Francois Cornet, Celine Davis, Anthony B. Dubuisson, Philippe Ducos, Fabrice Parol, Frederic Riedi, Jerome Vanbauce, Claudine TI Toward New Inferences about Cloud Structures from Multidirectional Measurements in the Oxygen A Band: Middle-of-Cloud Pressure and Cloud Geometrical Thickness from POLDER-3/PARASOL SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID MOLECULAR LINE ABSORPTION; DENSITY-FUNCTION DERIVATION; PHOTON PATH-LENGTH; GREAT-PLAINS SITE; TOP PRESSURE; A-BAND; MULTIPLE-SCATTERING; JOINT STATISTICS; LIDAR RETURNS; OPTICAL DEPTH AB New evidence from collocated measurements, with support from theory and numerical simulations, that multidirectional measurements in the oxygen A band from the third Polarization and Directionality of the Earth's Reflectances (POLDER-3) instrument on the Polarization and Anisotropy of Reflectances for Atmospheric Sciences coupled with Observations from a Lidar (PARASOL) satellite platform within the "A-Train" can help to characterize the vertical structure of clouds is presented. In the case of monolayered clouds, the standard POLDER cloud oxygen pressure product P(O2) is shown to be sensitive to the cloud geometrical thickness H in two complementary ways: 1) P(O2) is, on average, close to the pressure at the geometrical middle of the cloud layer (MCP) and methods are proposed for reducing the pressure difference P(O2) MCP and 2) the angular standard deviation of P(O2) and the cloud geometrical thickness H are tightly correlated for liquid clouds. Accounting for cloud phase, there is thus the potential to obtain a statistically reasonable estimate of H. Such derivation from passive measurements, as compared with or supplementing other observations, is expected to be of interest in a broad range of applications for which it is important to define better the macrophysical cloud parameters in a practical way. C1 [Ferlay, Nicolas; Thieuleux, Francois; Cornet, Celine; Dubuisson, Philippe; Ducos, Fabrice; Parol, Frederic; Riedi, Jerome; Vanbauce, Claudine] Univ Lille 1, UFR Phys, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. [Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Ferlay, N (reprint author), Univ Lille 1, UFR Phys, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. EM nicolas.ferlay@univ-lille1.fr FU French research CNRS; CNES FX This study has been financed through grants from the French research CNRS program Programme National de Teledetection Spatiale (PNTS) and the CNES program Terre, Ocean, Surfaces Continentales, Atmosphere (TOSCA). CALIOP-collocated PARASOL and MODIS data were provided in digest form by the ICARE Thematic Center (Universite Lille 1; http://www.icare.univ-lille1.fr/) through the MULTI_SENSOR data project. We thank the CloudSat Data Processing Center (Colorado State University Cooperative Institute for Research in the Atmosphere; http://www.cloudsat.cira.colostate.edu/) for providing the CloudSat 2B-GEOPROF-Lidar data. NR 64 TC 16 Z9 16 U1 1 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD DEC PY 2010 VL 49 IS 12 BP 2492 EP 2507 DI 10.1175/2010JAMC2550.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 702KV UT WOS:000285894500007 ER PT J AU Pryce, TO Abrams, MJ AF Pryce, T. O. Abrams, M. J. TI Direct detection of Southeast Asian smelting sites by ASTER remote sensing imagery: technical issues and future perspectives SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Archaeometallurgy; ASTER; GIS; Remote sensing; Smelting; Thailand AB Satellite-based multi-spectral remote sensing data were used in an attempt to identify control signatures for known prehistoric copper smelting sites in Thailand. It had been hoped that these characteristic signals could then be used as a reference for the detection of unknown Southeast Asian metal production sites, with the overall intention of strengthening the evidence base for early technological interactions with China and India. Regrettably, control signatures were not identified from the ASTER data due to issues of scale, chemistry, and vegetation, but we are able to offer reasons for this setback that might lead other scholars to develop successful applications of this methodology in more amenable (non-tropical) environments. Combined with ground truthing, intensive survey, excavation, and the technological analysis of metallurgical assemblages, this potentially useful and cost effective approach could lead to improved data density for the metal technology transmission discussions currently spanning Eurasia. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Pryce, T. O.] Univ Oxford, Archaeol & Hist Art Res Lab, Oxford OX1 3QY, England. [Pryce, T. O.] Univ Paris 10, Lab Prehist & Technol, UMR 7055, F-92001 Nanterre, France. [Abrams, M. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Pryce, TO (reprint author), Univ Oxford, Archaeol & Hist Art Res Lab, S Parks Rd, Oxford OX1 3QY, England. EM opryce@gmail.com; michael.j.abrams@jpl.nasa.gov FU Institute for Archaeo-metallurgical Studies FX The lead author would like to thank the Institute for Archaeo-metallurgical Studies for funding the meeting between the authors in Rome in November 2007, and also Etleva Nalbani and Samir Shpuza for kindly sharing their home. Work done by Abrams was performed at the Jet Propulsion Laboratory/California Institute of Technology under contract with the National Aeronautics and Space Administration. Optical satellite images are provided courtesy of Google Earth (TM) mapping service. We gratefully acknowledge the input, support, and editorial contribution of Andrew Bevan and Vincent C. Pigott of the UCL Institute of Archaeology, and also Georges Kozminski of the Bureau de Recherches Geologiques et Minieres. Any errors remain our own. NR 30 TC 4 Z9 4 U1 2 U2 4 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD DEC PY 2010 VL 37 IS 12 BP 3091 EP 3098 DI 10.1016/j.jas.2010.07.009 PG 8 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 676IF UT WOS:000283903500014 ER PT J AU Park, SH Panicker, AS Lee, DI Jung, WS Jang, SM Jang, M Kim, D Kim, YW Jeong, H AF Park, Sung-Hwa Panicker, A. S. Lee, Dong-In Jung, Woon-Seon Jang, Sang-Min Jang, Min Kim, Dongchul Kim, Yu-Won Jeong, Harrison TI Characterization of chemical properties of atmospheric aerosols over Anmyeon (South Korea), a super site under Global Atmosphere Watch SO JOURNAL OF ATMOSPHERIC CHEMISTRY LA English DT Article DE Aerosols; TSP; PM(10); PM(2),(5) ID URBAN SITE; TRANSPORT; SULFATE; CLOUDS; CHINA; PM2.5; DUST; PM10 AB This paper reports aerosol chemical properties for the first time over a Korean Global Atmosphere Watch (GAW) supersite, Anmyeon (36A degrees 32'N; 126A degrees 19'E), during 2003-2004 period. Total suspended Particulates (TSP) showed significant seasonal variation with consistent higher mass concentrations during spring season (average of up to 230 A +/- 190 mu g/m(3)). PM(10) also followed similar trend with higher concentrations during spring (average of up to 170 A +/- 130 mu g/m(3)) and showed reduced concentrations during summer. PM(2.5) showed a significant increase during summer (average of up to 60 A +/- 25 mu g/m(3)), which could be due to the influx of fine mode sea salt aerosols associated with the Changma front (summer monsoon). Chemical composition analysis showed enhanced presence of acidic fractions, majorly contributed by sulphates (SO (4) (2-) ) and nitrates (NO (3) (-) ) in TSP, PM(10) and PM(2.5) during different seasons. Enhanced presence of Calcium (Ca(2+)) was observed during sand storm days during spring. The high correlation obtained on matrix analysis between crustal ions and acidic ions suggests that the ionic compositions over the site are mainly contributed by terrestrial sources of similar origin. The neutralization factors has been estimated to find the extend of neutralization of acidicity by main basic components, and found to have higher value for Ammonium (up to 1.1) in different seasons, indicating significant neutralization of acidic components over the region by NH (4) (+) . Back trajectory analysis has been performed during different seasons to constrain the possible sources of aerosol origin and the results are discussed in detail. C1 [Panicker, A. S.; Lee, Dong-In] Pukyong Natl Univ, Dept Environm Atmospher Sci, Pusan 608737, South Korea. [Park, Sung-Hwa; Jang, Sang-Min; Jang, Min] Pukyong Natl Univ, Atmospher Environm Res Inst, Pusan 608737, South Korea. [Jung, Woon-Seon] Pukyong Natl Univ, Interdisciplinary Program Earth Environm Engn, Pusan 608737, South Korea. [Kim, Dongchul] Univ Maryland Baltimore Country, Goddard Earth Sci & Technol Ctr, Baltimore, MD USA. [Kim, Dongchul] Univ Space Res Assoc, Columbia, MD USA. [Kim, Yu-Won; Jeong, Harrison] Korea Meteorol Adm, Korea Global Atmosphere Watch Ctr, Seoul, South Korea. RP Lee, DI (reprint author), Pukyong Natl Univ, Dept Environm Atmospher Sci, 599-1 Daeyong 3 Dong, Pusan 608737, South Korea. EM leedi@pknu.ac.kr RI Kim, Dongchul/H-2256-2012 OI Kim, Dongchul/0000-0002-5659-1394 FU National Research Foundation of Korea (NRF) through Korean Ministry of Education, Science & Technology (MEST) [K20607010000] FX This work is supported by National Research Foundation of Korea (NRF) through a grant provided by the Korean Ministry of Education, Science & Technology (MEST) in 2011 (No. K20607010000). The aerosol chemical datasets maintained in Anmyeon-do GAW center used in this study is gratefully acknowledged. Back trajectories obtained from HYSPLIT model are acknowledged with thanks. We thank two anonymous referees for their kind suggestions. NR 28 TC 9 Z9 9 U1 1 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-7764 J9 J ATMOS CHEM JI J. Atmos. Chem. PD DEC PY 2010 VL 67 IS 2-3 BP 71 EP 86 DI 10.1007/s10874-011-9205-2 PG 16 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 870GI UT WOS:000298656900001 ER PT J AU Bryan, FO Tomas, R Dennis, JM Chelton, DB Loeb, NG McClean, JL AF Bryan, Frank O. Tomas, Robert Dennis, John M. Chelton, Dudley B. Loeb, Norman G. McClean, Julie L. TI Frontal Scale Air-Sea Interaction in High-Resolution Coupled Climate Models SO JOURNAL OF CLIMATE LA English DT Article ID NUMERICAL WEATHER PREDICTION; EASTERN EQUATORIAL PACIFIC; SURFACE WIND STRESS; SATELLITE-OBSERVATIONS; TEMPERATURE; OCEAN; SYSTEM; VARIABILITY; GRADIENTS; CLOUDS AB The emerging picture of frontal scale air sea interaction derived from high resolution satellite observations of surface winds and sea surface temperature (SST) provides a unique opportunity to test the fidelity of high resolution coupled climate simulations Initial analysis of the output of a suite of Community Climate System Model (CCSM) experiments indicates that characteristics of frontal scale ocean atmosphere interaction such as the positive correlation between SST and surface wind stress are realistically captured only when the ocean component is eddy resolving The strength of the coupling between SST and surface stress is weaker than observed however as has been found previously for numerical weather prediction models and other coupled climate models The results are similar when the atmospheric component model grid resolution is doubled from 0 5 degrees to 0 25 degrees an indication that shortcomings in the representation of subgrid scale atmospheric planetary boundary layer processes rather than resolved scale processes are responsible for the weakness of the coupling In the coupled model solutions the response to mesoscale SST features is strongest in the atmospheric boundary layer but there is a deeper reaching response of the atmospheric circulation apparent in free tropospheric clouds This simulated response is shown to be consistent with satellite estimates of the relationship between mesoscale SST and all sky albedo C1 [Bryan, Frank O.] Natl Ctr Atmospher Res, Oceanog Sect, Boulder, CO 80303 USA. [Chelton, Dudley B.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Loeb, Norman G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [McClean, Julie L.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Bryan, FO (reprint author), Natl Ctr Atmospher Res, Oceanog Sect, POB 3000, Boulder, CO 80303 USA. RI Bryan, Frank/I-1309-2016 OI Bryan, Frank/0000-0003-1672-8330 FU National Science Foundation [NSF01]; NCAR; NSF [OCI-0749206, OCE-0825754]; Department of Energy [DE-PS02-07ER07-06]; NASA [NAS5-32965]; DOE [DE-FG02-05ER64119]; LLNL FX We thank David Bailey, Tony Craig, Detelina Ivanova, Art Mirin, Nancy Norton, and Mariana Vertenstein for their assistance in configuring and running these experiments Computing time for the experiments described in this paper was provided by the Department of Energy as part of the Multiprogramatic and Institutional Computing Initiative at Lawrence Livermore National Laboratory (LLNL), under the Office of Science (BER), U S Department of Energy, through Cooperative Agreement DE FC02-97ER62402 at the National Energy Supercomputing Center, and by NCAR FOB, RT, and JD are supported through National Science Foundation Cooperative Grant NSF01, which funds NCAR JD was additionally supported by NSF Grants OCI-0749206 and OCE-0825754 and the Department of Energy, through CCPP Program Grant DE-PS02-07ER07-06 DBC was supported by NASA Grant NAS5-32965 for funding of Ocean Vector Winds Science Team activities JLM was supported by the DOE, CCPP Program Grant DE-FG02-05ER64119, and an LLNL subcontract NR 33 TC 49 Z9 51 U1 1 U2 15 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD DEC 1 PY 2010 VL 23 IS 23 BP 6277 EP 6291 DI 10.1175/2010JCLI3665.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 696HP UT WOS:000285432800011 ER PT J AU Han, SC Ray, RD Luthcke, SB AF Han, Shin-Chan Ray, Richard D. Luthcke, Scott B. TI One centimeter-level observations of diurnal ocean tides from global monthly mean time-variable gravity fields SO JOURNAL OF GEODESY LA English DT Article DE Ocean tides; Time-variable gravity; Aliasing ID MODELS AB A method of analyzing GRACE satellite-to-satellite ranging data is presented which accentuates signals from diurnal ocean tides and dampens signals from long-period non-tidal phenomena. We form a time series of differences between two independent monthly mean gravity solutions, one set computed from range-rate data along strictly ascending arcs and the other set computed from data along descending arcs. The solar and lunisolar diurnal tides having alias periods longer than a few months, such as K (1), P (1), and S (1), present noticeable variations in the monthly ascending and descending 'difference' solutions, while the climate-related signals are largely cancelled. By computing tidal arguments evaluated along the actual GRACE orbits, we decompose and estimate residual tidal signals with respect to our adopted prior model GOT4.7. The adjustment in the tidal height is small yet significant, yielding maximum amplitudes of 4 cm mostly under the Antarctic ice shelves and similar to 1 cm in general at spatial scales of several hundred kilometer. Moreover, the results suggest there are possible 1-cm errors in the tide model even over oceans well-covered by decades of radar altimetry missions. Independent validation of such small adjustments covering wide areas, however, is difficult, particularly with limited point measurements such as tide gauge. C1 [Han, Shin-Chan; Ray, Richard D.; Luthcke, Scott B.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Han, Shin-Chan] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Han, SC (reprint author), NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA. EM Shin-Chan.Han@nasa.gov RI Ray, Richard/D-1034-2012; Luthcke, Scott/D-6283-2012; Han, Shin-Chan/A-2022-2009 FU GRACE; U.S. National Aeronautical and Space Administration FX This work was supported by GRACE projects and the Earth Surface and Interior program under the U.S. National Aeronautical and Space Administration. David Rowlands is acknowledged for useful discussion and help on processing GRACE data. We would like to thank the German Space Operations Center of the German Aerospace Center, DLR, for providing continuously and nearly 100% of the raw telemetry data of the twin GRACE satellites. Three reviewers and the associate editor helped greatly to improve the manuscript. NR 29 TC 7 Z9 7 U1 0 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 J9 J GEODESY JI J. Geodesy PD DEC PY 2010 VL 84 IS 12 BP 715 EP 729 DI 10.1007/s00190-010-0405-3 PG 15 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 681QJ UT WOS:000284331600002 ER PT J AU Ruane, AC AF Ruane, Alex C. TI NARR's Atmospheric Water Cycle Components. Part I: 20-Year Mean and Annual Interactions SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID AMERICAN REGIONAL REANALYSIS; MESOSCALE ETA-MODEL; NORTH-AMERICA; ENERGY BUDGETS; UNITED-STATES; HYDROCLIMATE VARIABILITY; PHYSICAL INITIALIZATION; GLOBAL PRECIPITATION; MOISTURE TRANSPORT; VAPOR TRANSPORT AB The North American Regional Reanalysis (NARR) atmospheric water cycle is examined from 1980 to 1999 using a budget approach, with a particular emphasis on annual component interactions and the role of hourly precipitation assimilation. NARR's summertime atmospheric water cycle and diurnal component interactions are examined in Part II of this study. NARR's high-resolution reanalysis and precipitation assimilation allow an improved climatology of mean water cycle components over North America, which is very attractive for applications, climate impact assessments, and as a basis for comparison with other products. A 20-yr climatology of precipitation, evaporation, moisture flux convergence, and the residual error term are produced for comparison to observations, other reanalyses and models, and future climate scenarios. Maps of the normalized covariance of annual precipitation with each of the other water cycle components identify regimes of seasonal interaction that form an additional basis for comparison. The annual cycle of assimilated precipitation is compared to high-resolution precipitation products as an example, and points of interest for continuing studies are identified. Analysis of the mean and transient balances reveals a significant effect from NARR's precipitation assimilation scheme, which is investigated using an estimate of NARR's underlying model precipitation (before assimilation), generated using the precipitation assimilation increment as a proxy. Biases of the precipitation assimilation scheme are then characterized spatially and temporally to inform the interpretation of NARR applications and comparisons. These model precipitation estimates reveal a more tightly closed atmospheric water cycle with predominantly excessive precipitation, resulting in too vigorous evaporation and moisture flux convergences. The sign and magnitude of evaporation and moisture flux convergence biases are found to be related to the precipitation assimilation correction and are important to consider in applications of NARR output. C1 [Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ruane, Alex C.] Oak Ridge Associated Univ, NASA, Postdoctoral Program, New York, NY USA. [Ruane, Alex C.] Sigma Space Partners LLC, New York, NY USA. RP Ruane, AC (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM aruane@giss.nasa.gov FU NASA FX This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Institute for Space Studies, administered by Oak Ridge Associated Universities (ORAU) through a contract with NASA. The views expressed herein are those of the author and do not necessarily reflect the views of NASA or ORAU. The author would like to thank Ernesto Hugo Berbery and Fedor Mesinger for their early discussions about NARR's water cycle, Ying Lin for her extensive assistance in revisiting NARR's precipitation assimilation scheme, Radley Horton for his multiple edits, Masao Kanamitsu for his helpful advice, and three anonymous reviewers for their helpful comments. NR 51 TC 19 Z9 19 U1 1 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2010 VL 11 IS 6 BP 1205 EP 1219 DI 10.1175/2010JHM1193.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 705ZE UT WOS:000286178800001 ER PT J AU Tang, L Hossain, F Huffman, GJ AF Tang, Ling Hossain, Faisal Huffman, George J. TI Transfer of Satellite Rainfall Uncertainty from Gauged to Ungauged Regions at Regional and Seasonal Time Scales SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID CONTINENTAL UNITED-STATES; HYDROLOGIC RESPONSE; PASSIVE-MICROWAVE; FLOOD PREDICTION; PRECIPITATION; ERROR; RADAR; SIMULATION; ALGORITHM; PRODUCTS AB Hydrologists and other users need to know the uncertainty of the satellite rainfall datasets across the range of time-space scales over the whole domain of the dataset. Here, "uncertainty'' refers to the general concept of the "deviation'' of an estimate from the reference (or ground truth) where the deviation may be defined in multiple ways. This uncertainty information can provide insight to the user on the realistic limits of utility, such as hydrologic predictability, which can be achieved with these satellite rainfall datasets. However, satellite rainfall uncertainty estimation requires ground validation (GV) precipitation data. On the other hand, satellite data will be most useful over regions that lack GV data, for example developing countries. This paper addresses the open issues for developing an appropriate uncertainty transfer scheme that can routinely estimate various uncertainty metrics across the globe by leveraging a combination of spatially dense GV data and temporally sparse surrogate (or proxy) GV data, such as the Tropical Rainfall Measuring Mission (TRMM) Precipitation Radar and the Global Precipitation Measurement (GPM) mission dual-frequency precipitation radar. The TRMM Multisatellite Precipitation Analysis (TMPA) products over the United States spanning a record of 6 yr are used as a representative example of satellite rainfall. It is shown that there exists a quantifiable spatial structure in the uncertainty of satellite data for spatial interpolation. Probabilistic analysis of sampling offered by the existing constellation of passive microwave sensors indicate that transfer of uncertainty for hydrologic applications may be effective at daily time scales or higher during the GPM era. Finally, a commonly used spatial interpolation technique (kriging), which leverages the spatial correlation of estimation uncertainty, is assessed at climatologic, seasonal, monthly, and weekly time scales. It is found that the effectiveness of kriging is sensitive to the type of uncertainty metric, time scale of transfer, and the density of GV data within the transfer domain. Transfer accuracy is lowest at weekly time scales with the error doubling from monthly to weekly. However, at very low GV data density (<20% of the domain), the transfer accuracy is too low to show any distinction as a function of the time scale of transfer. C1 [Tang, Ling; Hossain, Faisal] Tennessee Technol Univ, Dept Civil & Environm Engn, Cookeville, TN 38505 USA. [Huffman, George J.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. RP Hossain, F (reprint author), Tennessee Technol Univ, Dept Civil & Environm Engn, 1020 Stadium Dr,Box 5015, Cookeville, TN 38505 USA. EM fhossain@tntech.edu RI Huffman, George/F-4494-2014; Measurement, Global/C-4698-2015 OI Huffman, George/0000-0003-3858-8308; FU NASA [NNX08AR32G] FX The first author (Tang) was supported by the NASA Earth System Science Fellowship (2008-11). The second author (Hossain) was supported by the NASA New Investigator Program Award (NNX08AR32G). NR 33 TC 5 Z9 5 U1 0 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2010 VL 11 IS 6 BP 1263 EP 1274 DI 10.1175/2010JHM1296.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 705ZE UT WOS:000286178800004 ER PT J AU Behrangi, A Imam, B Hsu, KL Sorooshian, S Bellerby, TJ Huffman, GJ AF Behrangi, Ali Imam, Bisher Hsu, Kuolin Sorooshian, Soroosh Bellerby, Timothy J. Huffman, George J. TI REFAME: Rain Estimation Using Forward-Adjusted Advection of Microwave Estimates SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article ID CLOUD CLASSIFICATION-SYSTEM; COMBINED PASSIVE MICROWAVE; PRECIPITATION ESTIMATION; SATELLITE; ALGORITHM; RESOLUTION; VALIDATION; IMAGERY; PRODUCTS; LMODEL AB A new multiplatform multisensor satellite rainfall estimation technique is proposed in which sequences of Geostationary Earth Orbit infrared (GEO-IR) images are used to advect microwave (MW)-derived precipitation estimates along cloud motion streamlines and to further adjust the rainfall rates using local cloud classification. The main objective of the Rain Estimation using Forward-Adjusted advection of Microwave Estimates (REFAME) is to investigate whether inclusion of GEO-IR information can help to improve the advected MW precipitation rate as it gets farther in time from the previous MW overpass. The technique comprises three steps. The first step incorporates a 2D cloud tracking algorithm to capture cloud motion streamlines through successive IR images. The second step classifies cloudy pixels to a number of predefined clusters using brightness temperature (Tb) gradients between successive IR images along the cloud motion streamlines in combination with IR cloud-top brightness temperatures and textural features. A mean precipitation rate for each cluster is calculated using available MW-derived precipitation estimates. In the third step, the mean cluster precipitation rates are used to adjust MW precipitation intensities advected between available MW overpasses along cloud motion streamlines. REFAME is a flexible technique, potentially capable of incorporating diverse precipitation-relevant information, such as multispectral data. Evaluated over a range of spatial and temporal scales over the conterminous United States, the performance of the full REFAME algorithm compared favorably with products incorporating either no cloud tracking or no intensity adjustment. The observed improvements in root-mean-square error and especially in correlation coefficient between REFAME outputs and ground radar observations demonstrate that the new approach is effective in reducing the uncertainties and capturing the variation of precipitation intensity along cloud advection streamlines between MW sensor overpasses. An extended REFAME algorithm combines the adjusted advected MW rainfall rates with infrared-derived precipitation rates in an attempt to capture precipitation events initiating and decaying during the interval between two consecutive MW overpasses. Evaluation statistics indicate that the extended algorithm is effective to capture the life cycle of the convective precipitation, particularly for the interval between microwave overpasses in which precipitation starts or ends. C1 [Behrangi, Ali; Imam, Bisher; Hsu, Kuolin; Sorooshian, Soroosh] Univ Calif Irvine, Ctr Hydrometeorol & Remote Sensing, Henry Samueli Sch Engn, Irvine, CA USA. [Behrangi, Ali; Imam, Bisher; Hsu, Kuolin; Sorooshian, Soroosh] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA USA. [Bellerby, Timothy J.] Univ Hull, Kingston Upon Hull HU6 7RX, N Humberside, England. [Huffman, George J.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Huffman, George J.] Sci Syst & Applicat Inc, Greenbelt, MD USA. RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-301, Pasadena, CA 91109 USA. EM ali.behrangi@jpl.nasa.gov RI sorooshian, soroosh/B-3753-2008; Huffman, George/F-4494-2014 OI sorooshian, soroosh/0000-0001-7774-5113; Huffman, George/0000-0003-3858-8308 FU NASA Earth; Space Science Fellowship [NNX08AU78H]; NASA-PMM [NNG04GC74G]; NOAA/NESDIS GOES-R Program Office (GPO) via the GOES-R Algorithm Working Group (AWG); NSF STC [EAR-9876800]; NASA NEWS [NNX06AF934] FX Partial financial support was made available from NASA Earth and Space Science Fellowship (NESSF Award NNX08AU78H), NASA-PMM (Grant NNG04GC74G), NOAA/NESDIS GOES-R Program Office (GPO) via the GOES-R Algorithm Working Group (AWG), NSF STC for Sustainability of Semi-Arid Hydrology and Riparian Areas (SAHRA; Grant EAR-9876800), and NASA NEWS (Grant NNX06AF934) programs. The authors thank Mr. Dan Braithwaite for his technical assistance on processing the satellite/radar data for this experiment. NR 38 TC 24 Z9 26 U1 1 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2010 VL 11 IS 6 BP 1305 EP 1321 DI 10.1175/2010JHM1248.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 705ZE UT WOS:000286178800007 ER PT J AU Bloebaum, CL McGowan, AMR AF Bloebaum, Christina L. McGowan, Anna-Maria R. TI Design of Complex Engineered Systems SO JOURNAL OF MECHANICAL DESIGN LA English DT Editorial Material C1 [Bloebaum, Christina L.] SUNY Buffalo, Natl Sci Fdn, Buffalo, NY 14260 USA. [McGowan, Anna-Maria R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Bloebaum, CL (reprint author), SUNY Buffalo, Natl Sci Fdn, Buffalo, NY 14260 USA. NR 0 TC 2 Z9 2 U1 0 U2 2 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA SN 1050-0472 J9 J MECH DESIGN JI J. Mech. Des. PD DEC PY 2010 VL 132 IS 12 AR 120301 DI 10.1115/1.4003033 PG 2 WC Engineering, Mechanical SC Engineering GA 695IC UT WOS:000285362800002 ER PT J AU Stoner, AW Ottmar, ML Haines, SA AF Stoner, Allan W. Ottmar, Michele L. Haines, Scott A. TI TEMPERATURE AND HABITAT COMPLEXITY MEDIATE CANNIBALISM IN RED KING CRAB: OBSERVATIONS ON ACTIVITY, FEEDING, AND PREY DEFENSE MECHANISMS SO JOURNAL OF SHELLFISH RESEARCH LA English DT Article DE temperature; habitat complexity; predation; cannibalism; aquaculture; Paralithodes camtschaticus ID PARALITHODES-CAMTSCHATICUS TILESIUS; EASTERN BERING-SEA; BLUE-CRAB; CHIONOECETES-OPILIO; CALLINECTES-SAPIDUS; CHESAPEAKE-BAY; INTERTIDAL HABITATS; OXYGEN-CONSUMPTION; TEMPORAL VARIATION; PREDATION RATES AB Laboratory experiments were conducted to evaluate how water temperature mediates the cannibalistic relationship between age 0 and age 1 red king crab (RKC) (Paralithodes camtschaticus), and the role of habitat structure in providing refuge for prey. We also observed the activity levels of age 1 crabs under light and dark conditions, and predator avoidance behavior by the age 0 crabs. Age 1 crabs (15-20 mm in carapace length (CL)) were active 24 h/day, but motion was about 33% higher in light than in dark conditions, and increased in direct proportion with water temperature (2-10 degrees C). Feeding rate was also directly related with temperature for age 1 crabs, which consumed 7% of body weight per day at 2 degrees C, and 20% at 10 degrees C. Both temperature and habitat complexity had significant effects on survival of age 0 RKC (CW, 2.2-2.6 mm) when exposed to age 1 crabs (CL, 17-19 mm), with no significant interaction. Survival diminished 31% in a linear relationship from 2-10 degrees C, and was twice as high in a complex structural environment compared with bare sand habitat. Predator avoidance behavior by age 0 RKC improved from juvenile molt stage 2 to stage 4. Increasing water temperature may serve to increase mortality by cannibalism in RKC, both in aquaculture and in the field, but survival will increase substantially in structurally complex environments. C1 [Stoner, Allan W.; Ottmar, Michele L.; Haines, Scott A.] NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Stoner, AW (reprint author), NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2030 S Marine Sci Dr, Newport, OR 97365 USA. EM al.stoner@noaa.gov RI Gebauer, Radek/G-6749-2015 FU National Oceanic and Atmospheric Administration; Alaska Sea Grant College FX This study was conducted as part of the AKCRRAB Program (Alaska King Crab Research, Rehabilitation, and Biology) funded by the National Oceanic and Atmospheric Administration Aquaculture Program and the Alaska Sea Grant College Program. Crabs were provided by the Alutiiq Pride Shellfish Hatchery, Seward, Alaska, with special thanks to B. Daly and J. Swingle, who cared for and shipped crabs, and offered advice on crab husbandry. R. Titgen assisted in building experimental apparatus, and C. Ryer provided constructive criticism for the manuscript. NR 56 TC 23 Z9 23 U1 4 U2 21 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 J9 J SHELLFISH RES JI J. Shellfish Res. PD DEC PY 2010 VL 29 IS 4 BP 1005 EP 1012 DI 10.2983/035.029.0401 PG 8 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 699NM UT WOS:000285670100027 ER PT J AU Oravec, HA Zeng, X Asnani, VM AF Oravec, H. A. Zeng, X. Asnani, V. M. TI Design and characterization of GRC-1: A soil for lunar terramechanics testing in Earth-ambient conditions SO JOURNAL OF TERRAMECHANICS LA English DT Article DE Apollo; Lunar soil simulant; Moon wheels; NASA; Penetrometer; Roving vehicle AB Earth experiments must be carried out on terrain that deforms similarly to the lunar terrain to assess the tractive performances of lunar vehicles. Most notably, terrain compaction and shear response underneath the lunar vehicle wheels must represent that of the Moon. This paper discusses the development of a new lunar soil simulant, Glenn Research Center lunar soil simulant #1 (GRC-1), which meets this need. A semi-empirical design approach was followed in which the soil was created by mixing readily available manufactured sands to a particle size distribution similar to the coarse fraction of lunar soil. By varying terrain density, a broad range of in situ cone penetration measurements collected by the Apollo mission astronauts can be replicated. An extensive set of characterization data is provided in this article to facilitate the use of this material. For reference, the index and geotechnical properties of GRC-1 are compared to the lunar soil and existing lunar soil simulants. Published by Elsevier Ltd. on behalf of ISTVS. C1 [Asnani, V. M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Oravec, H. A.; Zeng, X.] Case Western Reserve Univ, Dept Civil Engn, Cleveland, OH 44106 USA. RP Asnani, VM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 23-3, Cleveland, OH 44135 USA. EM vivake.m.asnani@nasa.gov FU NASA [NNC06AA25A]; Ohio Space Grant Consortium FX The work reported herein was carried out with support from NASA Grant NNC06AA25A and the Ohio Space Grant Consortium Fellowship. The opinions expressed in this paper are those of the authors and do not represent the official policies of the funding agencies. NR 39 TC 25 Z9 28 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4898 J9 J TERRAMECHANICS JI J. Terramech. PD DEC PY 2010 VL 47 IS 6 BP 361 EP 377 DI 10.1016/j.jterra.2010.04.006 PG 17 WC Engineering, Environmental SC Engineering GA 656SX UT WOS:000282358000001 ER PT J AU Bigelow, GS Padula, SA Garg, A Gaydosh, D Noebe, RD AF Bigelow, Glen S. Padula, Santo A., II Garg, Anita Gaydosh, Darrell Noebe, Ronald D. TI Characterization of Ternary NiTiPd High-Temperature Shape-Memory Alloys under Load-Biased Thermal Cycling SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID NI ALLOYS; TRANSFORMATIONS; DEFORMATION; IMPROVEMENT; TITANIUM AB While NiTiPd alloys have been extensively studied for proposed use in high-temperature shape-memory applications, little is known about the shape-memory response of these materials under stress. Consequently, the isobaric thermal cyclic responses of five (Ni,Pd)(49.5)Ti(50.5) alloys with constant stoichiometry and Pd contents ranging from 15 to 46 at. pct were investigated. From these tests, transformation temperatures, transformation strain (which is proportional to work output), and unrecovered strain per cycle (a measure of dimensional instability) were determined as a function of stress for each alloy. It was found that increasing the Pd content over this range resulted in a linear increase in transformation temperature, as expected. At a given stress level, work output decreased while the amount of unrecovered strain produced during each load-biased thermal cycle increased with increasing Pd content, during the initial thermal cycles. However, continued thermal cycling at constant stress resulted in a saturation of the work output and nearly eliminated further unrecovered strain under certain conditions, resulting in stable behavior amenable to many actuator applications. C1 [Bigelow, Glen S.; Padula, Santo A., II; Noebe, Ronald D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Garg, Anita] Univ Toledo, Toledo, OH 43606 USA. [Gaydosh, Darrell] Ohio Aerosp Inst, Cleveland, OH 44142 USA. RP Bigelow, GS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM glen.s.bigelow@nasa.gov FU NASA FX This work was supported by NASA's Fundamental Aeronautics Program, Subsonic Fixed Wing Project. NR 39 TC 54 Z9 54 U1 3 U2 18 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD DEC PY 2010 VL 41A IS 12 BP 3065 EP 3079 DI 10.1007/s11661-010-0365-5 PG 15 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 669SX UT WOS:000283371600005 ER PT J AU Glavin, DP Callahan, MP Dworkin, JP Elsila, JE AF Glavin, Daniel P. Callahan, Michael P. Dworkin, Jason P. Elsila, Jamie E. TI The effects of parent body processes on amino acids in carbonaceous chondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID INTERSTELLAR ICE ANALOGS; EARLY SOLAR SYSTEM; MURCHISON METEORITE; ORGANIC-MATTER; AQUEOUS ALTERATION; ASYMMETRIC AUTOCATALYSIS; BIOMOLECULAR CHIRALITY; CATALYTIC SYNTHESIS; MASS SPECTROMETRY; ALKANOIC ACIDS AB To investigate the effect of parent body processes on the abundance, distribution, and enantiomeric composition of amino acids in carbonaceous chondrites, the water extracts from nine different powdered CI, CM, and CR carbonaceous chondrites were analyzed for amino acids by ultra performance liquid chromatography-fluorescence detection and time-of-flight mass spectrometry (UPLC-FD/ToF-MS). Four aqueously altered type 1 carbonaceous chondrites including Orgueil (CI1), Meteorite Hills (MET) 01070 (CM1), Scott Glacier (SCO) 06043 (CM1), and Grosvenor Mountains (GRO) 95577 (CR1) were analyzed using this technique for the first time. Analyses of these meteorites revealed low levels of two- to five-carbon acyclic amino alkanoic acids with concentrations ranging from approximately 1 to 2,700 parts-per-billion (ppb). The type 1 carbonaceous chondrites have a distinct distribution of the five-carbon (C-5) amino acids with much higher relative abundances of the gamma- and delta-amino acids compared to the type 2 and type 3 carbonaceous chondrites, which are dominated by alpha-amino acids. Much higher amino acid abundances were found in the CM2 chondrites Murchison, Lonewolf Nunataks (LON) 94102, and Lewis Cliffs (LEW) 90500, the CR2 Elephant Moraine (EET) 92042, and the CR3 Queen Alexandra Range (QUE) 99177. For example, alpha-aminoisobutyric acid (alpha-AIB) and isovaline were approximately 100 to 1000 times more abundant in the type 2 and 3 chondrites compared to the more aqueously altered type 1 chondrites. Most of the chiral amino acids identified in these meteorites were racemic, indicating an extraterrestrial abiotic origin. However, nonracemic isovaline was observed in the aqueously altered carbonaceous chondrites Murchison, Orgueil, SCO 06043, and GRO 95577 with l-isovaline excesses ranging from approximately 11 to 19%, whereas the most pristine, unaltered carbonaceous chondrites analyzed in this study had no detectable l-isovaline excesses. These results are consistent with the theory that aqueous alteration played an important role in amplification of small initial left handed isovaline excesses on the parent bodies. C1 [Glavin, Daniel P.; Callahan, Michael P.; Dworkin, Jason P.; Elsila, Jamie E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Glavin, DP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM daniel.p.glavin@nasa.gov RI Elsila, Jamie/C-9952-2012; Callahan, Michael/D-3630-2012; Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012 OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 FU NASA Astrobiology Institute; Goddard Center for Astrobiology; NASA; NASA at the Goddard Space Flight Center through a contract with NASA FX The authors would like to thank K. Righter, T. McCoy, L. Welzenbach, and P. Ehrenfreund for providing the meteorite samples used in this study; S. Pizzarello, S. Miller, S. Davies, and R. Duke for several amino acid standards; A. Lewis and M. Martin for help optimizing the LC analytical separation conditions; C. Alexander, J. Bada, K. Righter, and R. Clayton for helpful discussions; and O. Botta for assistance with the meteorite extractions. We also thank M. Sephton, S. Sandford, and an anonymous reviewer for helpful comments. We are grateful for funding support from the NASA Astrobiology Institute and the Goddard Center for Astrobiology, and the NASA Cosmochemistry Program. M. P. C. acknowledges support from the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 83 TC 47 Z9 51 U1 1 U2 25 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2010 VL 45 IS 12 BP 1948 EP 1972 DI 10.1111/j.1945-5100.2010.01132.x PG 25 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 706HQ UT WOS:000286209200006 ER PT J AU Noble, SK Keller, LP Pieters, CM AF Noble, Sarah K. Keller, Lindsay P. Pieters, Carle M. TI Evidence of space weathering in regolith breccias II: Asteroidal regolith breccias SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID LUNAR SOIL; ORDINARY CHONDRITES; OPTICAL-PROPERTIES; KAPOETA METEORITE; FINEST FRACTION; SIMULATION; SAMPLES; EVOLUTION; SURFACES; HISTORY AB Space weathering products, such as agglutinates and nanophase iron-bearing rims are easily preserved through lithification in lunar regolith breccias, thus such products, if produced, should be preserved in asteroidal regolith breccias as well. A study of representative regolith breccia meteorites, Fayetteville (H4) and Kapoeta (howardite), was undertaken to search for physical evidence of space weathering on asteroids. Amorphous or npFe0-bearing rims cannot be positively identified in Fayetteville, although possible glass rims were found. Extensive friction melt was discovered in the meteorite that is difficult to differentiate from weathered materials. Several melt products, including spherules and agglutinates, as well as one irradiated rim and one possible npFe0-bearing rim were identified in Kapoeta. The existence of these products suggests that lunar-like space weathering processes are, or have been, active on asteroids. C1 [Noble, Sarah K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Keller, Lindsay P.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. RP Noble, SK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM sarah.k.noble@nasa.gov RI Noble, Sarah/D-7614-2012 FU NASA [NGT9-66, NAG5-11763, RTOP 344-31-40-07] FX NASA support (NGT9-66, SKN), (NAG5-11763, CMP), and (RTOP 344-31-40-07, LPK) is gratefully acknowledged. We thank A. Basu and S. Sasaki for thorough reviews that improved the quality of this manuscript. The authors express their thanks to the Smithsonian, American Museum of Natural History, and the Field Museum for providing meteorite samples. NR 41 TC 12 Z9 12 U1 0 U2 6 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2010 VL 45 IS 12 BP 2007 EP 2015 DI 10.1111/j.1945-5100.2010.01151.x PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 706HQ UT WOS:000286209200009 ER PT J AU Wang, DH Li, XF Tao, WK AF Wang, Donghai Li, Xiaofan Tao, Wei-Kuo TI Torrential rainfall responses to radiative and microphysical processes of ice clouds during a landfall of severe tropical storm Bilis (2006) SO METEOROLOGY AND ATMOSPHERIC PHYSICS LA English DT Article ID DEEP CONVECTIVE REGIME; NUMERICAL SIMULATIONS; SQUALL-LINE; MICROSCALE STRUCTURE; STRATIFORM REGIONS; EQUILIBRIUM STATES; FRONTAL RAINBANDS; PRECIPITATION; ORGANIZATION; MESOSCALE AB Ice clouds are an important component in precipitation systems. The radiative processes of ice clouds directly impact radiation in heat budget and the microphysical processes of ice clouds directly affect latent heat and net condensation through deposition processes, which may eventually change surface rainfall. Thus, torrential rainfall responses to radiative and microphysical processes of ice clouds during a landfall of severe tropical storm Bilis (2006) are investigated with the analysis of sensitivity experiments. The two-dimensional cloud-resolving model is integrated for 3 days with imposed zonally uniform vertical velocity, zonal wind, horizontal temperature and vapor advection from NCEP/GDAS data. One sensitivity experiment excludes the radiative effects of ice clouds and the other sensitivity experiment excludes ice microphysics and associated radiative and microphysical processes. Model domain mean surface rain rate is barely changed by the exclusion of radiative effects of ice clouds due to the small decrease in net condensation associated with the small reduction in latent heat as a result of the offset between the increase in radiative cooling and the decrease in heat divergence. The exclusion of microphysical effects of ice clouds decreases the mean rain rate simply through the suppression of latent heat as a result of the removal of deposition processes. The total exclusion of ice microphysics decreases the mean rain rate mainly through the exclusion of microphysical effects of ice clouds. C1 [Wang, Donghai] Chinese Acad Meteorol Sci, State Key Lab Severe Weather LaSW, Beijing, Peoples R China. [Wang, Donghai] Sci Syst & Applicat Inc, Lanham, MD USA. [Li, Xiaofan] NOAA, NESDIS, Ctr Satellite Applicat & Res, Camp Springs, MD USA. [Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wang, DH (reprint author), Chinese Acad Meteorol Sci, State Key Lab Severe Weather LaSW, Beijing, Peoples R China. EM d.wang@hotmail.com RI Li, Xiaofan/F-5605-2010; Li, Xiaofan/G-2094-2014 FU State Key Basic Research Development Program [2009CB421504]; National Natural Science Foundation [40633016, 40875022, 40830958] FX The authors thank two anonymous reviewers for their constructive comments. This research was supported by the State Key Basic Research Development Program (2009CB421504), and the National Natural Science Foundation under the Grant No. 40633016, 40875022 and 40830958. NR 33 TC 5 Z9 8 U1 0 U2 4 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0177-7971 J9 METEOROL ATMOS PHYS JI Meteorol. Atmos. Phys. PD DEC PY 2010 VL 109 IS 3-4 BP 107 EP 114 DI 10.1007/s00703-010-0097-5 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 680YB UT WOS:000284272300003 ER PT J AU Rowlinson, A O'Brien, PT Tanvir, NR Zhang, B Evans, PA Lyons, N Levan, AJ Willingale, R Page, KL Onal, O Burrows, DN Beardmore, AP Ukwatta, TN Berger, E Hjorth, J Fruchter, AS Tunnicliffe, RL Fox, DB Cucchiara, A AF Rowlinson, A. O'Brien, P. T. Tanvir, N. R. Zhang, B. Evans, P. A. Lyons, N. Levan, A. J. Willingale, R. Page, K. L. Onal, O. Burrows, D. N. Beardmore, A. P. Ukwatta, T. N. Berger, E. Hjorth, J. Fruchter, A. S. Tunnicliffe, R. L. Fox, D. B. Cucchiara, A. TI The unusual X-ray emission of the short Swift GRB 090515: evidence for the formation of a magnetar? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-ray burst: individual: 090515; stars: neutron ID NEUTRON-STARS; ENERGY INJECTION; MILLISECOND PULSARS; OPTICAL AFTERGLOW; EXTENDED EMISSION; HOST GALAXY; SPECTRAL LAGS; LIGHT CURVES; BURSTS; FLARES AB The majority of short gamma-ray bursts (SGRBs) are thought to originate from the merger of compact binary systems collapsing directly to form a black hole. However, it has been proposed that both SGRBs and long gamma-ray bursts (LGRBs) may, on rare occasions, form an unstable millisecond pulsar (magnetar) prior to final collapse. GRB 090515, detected by the Swift satellite was extremely short, with a T-90 of 0.036 +/- 0.016 s, and had a very low fluence of 2 x 10(-8) erg cm(-2) and faint optical afterglow. Despite this, the 0.3-10 keV flux in the first 200 s was the highest observed for an SGRB by the Swift X-ray Telescope (XRT). The X-ray light curve showed an unusual plateau and steep decay, becoming undetectable after similar to 500 s. This behaviour is similar to that observed in some long bursts proposed to have magnetars contributing to their emission. In this paper, we present the Swift observations of GRB 090515 and compare it to other gamma-ray bursts (GRBs) in the Swift sample. Additionally, we present optical observations from Gemini, which detected an afterglow of magnitude 26.4 +/- 0.1 at T+1.7 h after the burst. We discuss potential causes of the unusual 0.3-10 keV emission and suggest it might be energy injection from an unstable millisecond pulsar. Using the duration and flux of the plateau of GRB 090515, we place constraints on the millisecond pulsar spin period and magnetic field. C1 [Rowlinson, A.; O'Brien, P. T.; Tanvir, N. R.; Evans, P. A.; Lyons, N.; Willingale, R.; Page, K. L.; Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Zhang, B.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [Levan, A. J.; Tunnicliffe, R. L.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Onal, O.] Istanbul Univ, Dept Astron & Space Sci, Fac Sci, TR-34119 Istanbul, Turkey. [Burrows, D. N.; Fox, D. B.; Cucchiara, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Ukwatta, T. N.] George Washington Univ, Washington, DC 20052 USA. [Ukwatta, T. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hjorth, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Fruchter, A. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Rowlinson, A (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM bar7@star.le.ac.uk RI Hjorth, Jens/M-5787-2014 OI Hjorth, Jens/0000-0002-4571-2306 FU Science and Technology Funding Council; NASA [NAS5-00136]; DNRF FX AR, NRT, PAE, NL, AJL, KLP and APB would like to acknowledge funding from the Science and Technology Funding Council. This work makes use of data supplied by the UK Swift Science Data Centre at the University of Leicester and the Swift satellite funded by NASA and the Science and Technology Funding Council. Swift funding at PSU comes from NASA contract NAS5-00136. The Dark Cosmology Centre is funded by the DNRF. NR 98 TC 66 Z9 67 U1 3 U2 9 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2010 VL 409 IS 2 BP 531 EP 540 DI 10.1111/j.1365-2966.2010.17354.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 681BX UT WOS:000284282300006 ER PT J AU Mouschovias, TC Tassis, K AF Mouschovias, Telemachos Ch Tassis, Konstantinos TI Self-consistent analysis of OH-Zeeman observations: too much noise about noise SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE diffusion; MHD; turbulence; stars: formation; ISM: clouds; ISM: magnetic fields ID STAR-FORMATION; INTERSTELLAR CLOUDS; MOLECULAR GAS; DARK CLOUDS; CONTRACTION AB We have recently re-analysed in a self-consistent way OH-Zeeman observations in four molecular-cloud envelopes and we have shown that, contrary to claims by Crutcher et al., there is no evidence that the mass-to-flux ratio decreases from the envelopes to the cores of these clouds. The key difference between our data analysis and the earlier one by Crutcher et al. is the relaxation of the overly restrictive assumption made by Crutcher et al, that the magnetic field strength is independent of position in each of the four envelopes. In a more recent paper, Crutcher et al. (1) claim that our analysis is not self-consistent, in that it misses a cosine factor, and (2) present new arguments to support their contention that the magnetic field strength is indeed independent of position in each of the four envelopes. We show that the claim of the missing cosine factor is false; that the new arguments contain even more serious problems than the Crutcher et al. original data analysis; and we present new observational evidence, independent of the OH-Zeeman data, that suggests significant variations in the magnetic field strength in the four cloud envelopes. C1 [Mouschovias, Telemachos Ch] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Mouschovias, Telemachos Ch] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Tassis, Konstantinos] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mouschovias, TC (reprint author), Univ Illinois, Dept Phys, 1002 W Green St, Urbana, IL 61801 USA. EM tchm@astro.uiuc.edu RI Tassis, Konstantinos/C-3155-2011; OI Tassis, Konstantinos/0000-0002-8831-2038 FU National Science Foundation [NSF AST-07-09206]; National Aeronautics and Space Administration FX We are grateful to Nicholas Chapman for providing Figs 1 and 2 and for invaluable discussions on observational issues. TM's work was supported in part by the National Science Foundation under grant NSF AST-07-09206 to the University of Illinois. Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 13 TC 14 Z9 14 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 DEC PY 2010 VL 409 IS 2 BP 801 EP 807 DI 10.1111/j.1365-2966.2010.17345.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 681BX UT WOS:000284282300028 ER PT J AU Tian, BJ Waliser, DE Fetzer, EJ Yung, YL AF Tian, Baijun Waliser, Duane E. Fetzer, Eric J. Yung, Yuk L. TI Vertical Moist Thermodynamic Structure of the Madden-Julian Oscillation in Atmospheric Infrared Sounder Retrievals: An Update and a Comparison to ECMWF Interim Re-Analysis SO MONTHLY WEATHER REVIEW LA English DT Article ID MJO SIMULATION DIAGNOSTICS; PACIFIC WARM POOL; CLIMATE MODELS; INDIAN-OCEAN; VARIABILITY; MISMO AB The large-scale vertical moist thermodynamic structure of the Madden-Julian oscillation (MJO) was documented using the first 2.5 yr (2002-05) of version 4 atmospheric specific humidity and temperature profiles from the Atmospheric Infrared Sounder (AIRS). In this study, this issue is further examined using currently available 7-yr version 5 AIRS data (2002-09) to test its dependence on the AIRS data record lengths, AIRS retrieval versions, and MJO event selection and compositing methods employed. The results indicate a strong consistency of the large-scale vertical moist thermodynamic structure of the MJO between different AIRS data record lengths (2.5 vs 7 yr), different AIRS retrieval versions (4 vs 5), and different MJO analysis methods [the extended empirical orthogonal function (EEOF) method vs the multivariate empirical orthogonal function (MEOF) method]. The large-scale vertical moist thermodynamic structures of the MJO between the AIRS retrievals and the ECMWF Interim Re-Analysis (ERA-Interim) products are also compared. The results indicate a much better agreement of the MJO vertical structure between AIRS and ERA-Interim than with the NCEP-NCAR reanalysis, although a significant difference exists in the magnitude of moisture anomalies between ERA-Interim and AIRS. This characterization of the vertical moist thermodynamic structure of the MJO by AIRS and ERA-Interim offers a useful observation-based metric for general circulation model diagnostics. C1 [Tian, Baijun; Waliser, Duane E.; Fetzer, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA. RP Tian, BJ (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM baijun.tian@jpl.nasa.gov RI Tian, Baijun/A-1141-2007 OI Tian, Baijun/0000-0001-9369-2373 FU NASA; JPL; NSF [ATM-0840755] FX This research was carried out at JPL/Caltech under a contract with NASA and supported by the AIRS project at JPL and the NSF through Grant ATM-0840755 to UCLA. Comments from M. Wheeler, three anonymous reviewers, and conversations with P. Bauer, M. Goldberg, B. Kahn, E. Maiming, E. Olsen, J. Susskind, J. Teixeira, and F. Vitart all helped to improve this paper. NR 28 TC 40 Z9 42 U1 0 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 J9 MON WEATHER REV JI Mon. Weather Rev. PD DEC PY 2010 VL 138 IS 12 BP 4576 EP 4582 DI 10.1175/2010MWR3486.1 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 702QR UT WOS:000285909700019 ER PT J AU Wang, XY Huang, Y Nguyen, N AF Wang, Xiaoyu Huang, Yong Nguyen, Nhan TI Robustness quantification of recurrent neural network using unscented transform SO NEUROCOMPUTING LA English DT Article DE Recurrent neural network; Robustness; Uncertainty propagation; Unscented transform ID BACKPROPAGATION; TIME AB Artificial recurrent neural network has been proved to be a valuable tool in modeling nonlinear dynamical systems Robustness study of recurrent neural network is critical to its successful implementation The goal of robustness study is to reduce the sensitivity of modeling capability to parametric uncertainties or make the network fault tolerant In this study an uncertainty propagation analysis is performed to quantify the robustness of a recurrent neural network output due to perturbations in its trained weights An uncertainty propagation analysis-based robustness measure has been proposed accordingly and further compared with available performance loss-based and sensitivity matrix-based approaches Results show that the proposed robustness measure approach is more efficient generic and flexible to quantify the robustness of a recurrent neural network (C) 2010 Elsevier B V All rights reserved C1 [Wang, Xiaoyu; Huang, Yong] Clemson Univ, Dept Mech Engn, Clemson, SC 29634 USA. [Nguyen, Nhan] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. RP Huang, Y (reprint author), Clemson Univ, Dept Mech Engn, Clemson, SC 29634 USA. FU South Carolina Space Grant Consortium; NASA Ames Research Center FX The authors would like to acknowledge the financial support from the South Carolina Space Grant Consortium and the NASA Ames Research Center The stimulating discussion with Dr K. KrishnaKumar of NASA Ames was also crucial in this robustness study NR 30 TC 1 Z9 1 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-2312 J9 NEUROCOMPUTING JI Neurocomputing PD DEC PY 2010 VL 74 IS 1-3 SI SI BP 354 EP 361 DI 10.1016/j.neucom.2010.03.010 PG 8 WC Computer Science, Artificial Intelligence SC Computer Science GA 701GG UT WOS:000285805800033 ER PT J AU Abadie, J Abbott, BP Abbott, R Abernathy, M Adams, C Adhikari, R Ajith, P Allen, B Allen, G Ceron, EA Amin, RS Anderson, SB Anderson, WG Arain, MA Araya, M Aronsson, M Aso, Y Aston, S Atkinson, DE Aufmuth, P Aulbert, C Babak, S Baker, P Ballmer, S Barkers, D Barnum, S Barr, B Barriga, P Barsotti, L Barton, MA Bartos, I Bassiri, R Bastarrika, M Bauchrowitz, J Behnke, B Benacquista, M Bertolini, A Betzwieser, J Beveridge, N Beyersdorf, PT Bilenko, IA Billingsley, G Birch, J Biswas, R Black, E Blackburn, JK Blackburn, L Blaii, D Bland, B Bock, O Bodiya, TP Bondarescu, R Bork, R Born, M Bose, S Boyle, M Brady, PR Braginsky, VB Brau, JE Breyer, J Bridges, DO Brinkmann, M Britzger, M Brooks, AF Brown, DA Buonanno, A Burguet-Castell, J Burmeister, O Byer, RL Cadonati, L Cain, J Camp, JB Campsie, P Cannizzo, J Cannon, KC Cao, J Capano, C Caride, S Caudill, S Cavaglia, M Cepeda, C Chalermsongsak, T Chalkley, E Charlton, P Chelkowski, S Chen, Y Christensen, N Chua, SSY Chung, CTY Clark, D Clark, J Clayton, JH Conte, R Cook, D Corbitt, TR Cornish, N Costa, CA Coward, DM Coyne, DC Creighton, JDE Creighton, TD Cruise, AM Culter, RM Cumming, A Cunningham, L Dahl, K Danilishin, SL Dannenberg, R Danzmann, K Das, K Daudert, B Davies, G Davis, A Daw, EJ Dayanga, T Debra, D Degallaix, J Dergachev, V DeRosa, R DeSalvo, R Devanka, P Dhurandhar, S Di Palma, I Diaz, M Donovan, F Dooley, KL Doomes, EE Dorsher, S Douglas, ESD Drever, RWP Driggers, JC Dueck, J Dumas, JC Eberle, T Edgar, M Edwards, M Effler, A Ehrens, P Engel, R Etzel, T Evans, M Evans, T Fairhurst, S Fan, Y Farr, BF Fazi, D Fehrmann, H Feldbaum, D Finn, LS Flanigan, M Flasch, K Foley, S Forrest, C Forsi, E Fotopoulos, N Irede, M Frei, M Frei, Z Freise, A Frey, R Fricke, TT Friedrich, D Fritschel, P Frolov, VV Fulda, P Fyffe, M Garofoli, JA Gholami, I Ghosh, S Giaime, JA Giampanis, S Giardina, KD Gill, C Goetz, E Goggin, LM Gonzalez, G Gorodetsky, ML Gossler, S Craef, C Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Grosso, R Grote, H Grunewald, S Gustafson, EK Gustafson, R Hage, B Hall, P Hallam, JM Hammer, D Hammond, G Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Haughian, K Hayama, K Hayler, T Heefner, J Heng, IS Heptonstall, AW Hewitson, M Hild, S Hirose, E Hoak, D Hodge, KA Holt, K Hosken, DJ Hough, J Howell, EJ Hoyland, D Hughey, B Husa, S Huttner, SH Huynh-Dinh, T Ingram, DR Inta, R Isogai, T Ivanov, A Johnson, WW Jones, DI Jones, G Jones, R Ju, L Kalmus, P Kalogera, V Kandhasamy, S Kanner, JB Katsavounidis, E Kawabe, K Kawamura, S Kawazoe, F Kells, W Keppel, DG Khalaidovski, A Khalil, FY Khazanov, EA Kim, H King, PJ Kinzel, DL Kissel, JS Klimenko, S Kondrashov, V Kopparapu, R Koranda, S Kozak, D Krause, T Kringel, V Krishnamurthy, S Krishnan, B Kuehn, G Kullman, J Kumar, R Kwee, P Landry, M Lang, M Lantz, B Lastzka, N Lazzarini, A Leaci, P Leong, J Leonor, I Li, J Lin, H Lindquist, PE Lockerbie, NA Lodhia, D Lormand, M Lu, P Luan, J Lubinski, M Lucianetti, A Luck, H Lundgren, A Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Mak, C Mandel, I Mandic, V Marka, S Marka, Z Maros, E Martin, IW Martin, RM Marx, JN Mason, K Matichard, F Matone, L Matzner, RA Mavalvala, N McCarthy, R McClelland, DE McGuire, SC McIntyre, G McIvor, G McKechan, DJA Meadors, G Mehmet, M Meier, T Melatos, A Melissinos, AC Mendell, G Menendez, DF Mercer, RA Merill, L Meshkov, S Messenger, C Meyer, MS Miao, H Miller, J Mino, Y Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Moe, B Mohanty, SD Mohapatra, SRP Moraru, D Moreno, G Morioka, T Mors, K Mossavi, K MowLowry, CM Mueller, G Mukherjee, S Mullavey, A Muller-Ebhardt, H Munch, J Murray, PG Nash, T Nawrodt, R Nelson, J Newton, G Nishizawa, A Nolting, D Ochsner, E O'Dell, J Ogin, GH Oldenburg, RG O'Reilly, B O'Shaughnessy, R Osthelder, C Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Page, A Pan, Y Pankow, C Papa, MA Pareja, M Patel, P Pathak, D Pedraza, M Pekowsky, L Penn, S Peralta, C Perreca, A Pickenpack, M Pinto, IM Pitkin, M Pletsch, HJ Plissi, MV Postiglione, F Predoi, V Price, LR Prijatelj, M Principe, M Prix, R Prokhorov, L Puncken, O Quetschke, V Raab, FJ Radke, T Radkins, H Raffai, P Rakhmanov, M Rankins, B Raymond, V Reed, CM Reed, T Reid, S Reitze, DH Riesen, R Riles, K Roberts, P Robertson, NA Robinson, C Robinson, EL Roddy, S Rover, C Rollins, J Romano, JD Romie, JH Rowan, S Rudiger, A Ryan, K Sakata, S Sakosky, M Salemi, F Sammut, L de la Jordana, LS Sandberg, V Sannibale, MV Santamaria, L Santostasi, G Saraf, S Sathyaprakash, BS Sato, S Satterthwaite, M Saulson, PR Savage, R Schilling, R Schnabel, R Schofield, RMS Schulz, B Schutz, BF Schwinberg, P Scott, J Scott, SM Searle, AC Seifert, F Sellers, D Sengupta, AS Sergeev, A Shaddock, DA Shapiro, B Shawhan, P Shoemaker, DH Sibley, A Siemens, X Sigg, D Singer, A Suites, AM Skelton, G Slagmolen, BJJ Slutsky, J Smith, JR Smith, MR Smith, ND Somiya, K Sorazu, B Speirits, FC Stein, AJ Stein, LC Steinlechner, S Steplewski, S Stochino, A Stone, R Strain, KA Strigin, S Stroeer, A Stuver, AL Summerscales, TZ Sung, M Susmithan, S Sutton, P Szokoly, GP Talukder, D Tanner, DB Tarabrin, SP Taylor, JR Taylor, R Thomas, P Thorne, KA Thorne, KS Thrane, E Thuring, A Titsler, C Tokmakov, KV Torres, C Torrie, CI Traylor, G Trias, M Tseng, K Turner, L Ugolini, D Urbanek, K Vahlbruch, H Vaishnav, B Vallisneri, M Van den Broeck, C van der Sluys, MV van Veggel, AA Vass, S Vaulin, R Vecchio, A Veitch, J Veitch, PJ Veltkamp, C Villar, AE Vorvick, C Vyachanin, SP Waldman, SJ Wallace, L Wanner, A Ward, RL Wei, P Weinert, M Weinstein, AJ Weiss, R Wen, L Wen, S Wessels, P West, M Westphal, T Wette, K Whelan, JT Whitcomb, SE White, DJ Whiting, BF Wilkinson, C Willems, PA Williams, L Wilike, B Winkelmann, L Winkler, W Wipf, CC Wiseman, AG Woan, G Wooley, R Worden, J Yakushin, I Yamamoto, H Yamamoto, K Yeaton-Massey, D Yoshida, S Yu, PP Zanolin, M Zhang, L Zhang, Z Zhao, C Zotov, N Zucker, ME Zweizig, J AF Abadie, J. Abbott, B. P. Abbott, R. Abernathy, M. Adams, C. Adhikari, R. Ajith, P. Allen, B. Allen, G. Ceron, E. Amador Amin, R. S. Anderson, S. B. Anderson, W. G. Arain, M. A. Araya, M. Aronsson, M. Aso, Y. Aston, S. Atkinson, D. E. Aufmuth, P. Aulbert, C. Babak, S. Baker, P. Ballmer, S. Barkers, D. Barnum, S. Barr, B. Barriga, P. Barsotti, L. Barton, M. A. Bartos, I. Bassiri, R. Bastarrika, M. Bauchrowitz, J. Behnke, B. Benacquista, M. Bertolini, A. Betzwieser, J. Beveridge, N. Beyersdorf, P. T. Bilenko, I. A. Billingsley, G. Birch, J. Biswas, R. Black, E. Blackburn, J. K. Blackburn, L. Blaii, D. Bland, B. Bock, O. Bodiya, T. P. Bondarescu, R. Bork, R. Born, M. Bose, S. Boyle, M. Brady, P. R. Braginsky, V. B. Brau, J. E. Breyer, J. Bridges, D. O. Brinkmann, M. Britzger, M. Brooks, A. F. Brown, D. A. Buonanno, A. Burguet-Castell, J. Burmeister, O. Byer, R. L. Cadonati, L. Cain, J. Camp, J. B. Campsie, P. Cannizzo, J. Cannon, K. C. Cao, J. Capano, C. Caride, S. Caudill, S. Cavaglia, M. Cepeda, C. Chalermsongsak, T. Chalkley, E. Charlton, P. Chelkowski, S. Chen, Y. Christensen, N. Chua, S. S. Y. Chung, C. T. Y. Clark, D. Clark, J. Clayton, J. H. Conte, R. Cook, D. Corbitt, T. R. Cornish, N. Costa, C. A. Coward, D. M. Coyne, D. C. Creighton, J. D. E. Creighton, T. D. Cruise, A. M. Culter, R. M. Cumming, A. Cunningham, L. Dahl, K. Danilishin, S. L. Dannenberg, R. Danzmann, K. Das, K. Daudert, B. Davies, G. Davis, A. Daw, E. J. Dayanga, T. DeBra, D. Degallaix, J. Dergachev, V. DeRosa, R. DeSalvo, R. Devanka, P. Dhurandhar, S. Di Palma, I. Diaz, M. Donovan, F. Dooley, K. L. Doomes, E. E. Dorsher, S. Douglas, E. S. D. Drever, R. W. P. Driggers, J. C. Dueck, J. Dumas, J-C Eberle, T. Edgar, M. Edwards, M. Effler, A. Ehrens, P. Engel, R. Etzel, T. Evans, M. Evans, T. Fairhurst, S. Fan, Y. Farr, B. F. Fazi, D. Fehrmann, H. Feldbaum, D. Finn, L. S. Flanigan, M. Flasch, K. Foley, S. Forrest, C. Forsi, E. Fotopoulos, N. Irede, M. Frei, M. Frei, Z. Freise, A. Frey, R. Fricke, T. T. Friedrich, D. Fritschel, P. Frolov, V. V. Fulda, P. Fyffe, M. Garofoli, J. A. Gholami, I. Ghosh, S. Giaime, J. A. Giampanis, S. Giardina, K. D. Gill, C. Goetz, E. Goggin, L. M. Gonzalez, G. Gorodetsky, M. L. Gossler, S. Craef, C. Grant, A. Gras, S. Gray, C. Greenhalgh, R. J. S. Gretarsson, A. M. Grosso, R. Grote, H. Grunewald, S. Gustafson, E. K. Gustafson, R. Hage, B. Hall, P. Hallam, J. M. Hammer, D. Hammond, G. Hanks, J. Hanna, C. Hanson, J. Harms, J. Harry, G. M. Harry, I. W. Harstad, E. D. Haughian, K. Hayama, K. Hayler, T. Heefner, J. Heng, I. S. Heptonstall, A. W. Hewitson, M. Hild, S. Hirose, E. Hoak, D. Hodge, K. A. Holt, K. Hosken, D. J. Hough, J. Howell, E. J. Hoyland, D. Hughey, B. Husa, S. Huttner, S. H. Huynh-Dinh, T. Ingram, D. R. Inta, R. Isogai, T. Ivanov, A. Johnson, W. W. Jones, D. I. Jones, G. Jones, R. Ju, L. Kalmus, P. Kalogera, V. Kandhasamy, S. Kanner, J. B. Katsavounidis, E. Kawabe, K. Kawamura, S. Kawazoe, F. Kells, W. Keppel, D. G. Khalaidovski, A. Khalil, F. Y. Khazanov, E. A. Kim, H. King, P. J. Kinzel, D. L. Kissel, J. S. Klimenko, S. Kondrashov, V. Kopparapu, R. Koranda, S. Kozak, D. Krause, T. Kringel, V. Krishnamurthy, S. Krishnan, B. Kuehn, G. Kullman, J. Kumar, R. Kwee, P. Landry, M. Lang, M. Lantz, B. Lastzka, N. Lazzarini, A. Leaci, P. Leong, J. Leonor, I. Li, J. Lin, H. Lindquist, P. E. Lockerbie, N. A. Lodhia, D. Lormand, M. Lu, P. Luan, J. Lubinski, M. Lucianetti, A. Luck, H. Lundgren, A. Machenschalk, B. MacInnis, M. Mageswaran, M. Mailand, K. Mak, C. Mandel, I. Mandic, V. Marka, S. Marka, Z. Maros, E. Martin, I. W. Martin, R. M. Marx, J. N. Mason, K. Matichard, F. Matone, L. Matzner, R. A. Mavalvala, N. McCarthy, R. McClelland, D. E. McGuire, S. C. McIntyre, G. McIvor, G. McKechan, D. J. A. Meadors, G. Mehmet, M. Meier, T. Melatos, A. Melissinos, A. C. Mendell, G. Menendez, D. F. Mercer, R. A. Merill, L. Meshkov, S. Messenger, C. Meyer, M. S. Miao, H. Miller, J. Mino, Y. Mitra, S. Mitrofanov, V. P. Mitselmakher, G. Mittleman, R. Moe, B. Mohanty, S. D. Mohapatra, S. R. P. Moraru, D. Moreno, G. Morioka, T. Mors, K. Mossavi, K. MowLowry, C. M. Mueller, G. Mukherjee, S. Mullavey, A. Muller-Ebhardt, H. Munch, J. Murray, P. G. Nash, T. Nawrodt, R. Nelson, J. Newton, G. Nishizawa, A. Nolting, D. Ochsner, E. O'Dell, J. Ogin, G. H. Oldenburg, R. G. O'Reilly, B. O'Shaughnessy, R. Osthelder, C. Ottaway, D. J. Ottens, R. S. Overmier, H. Owen, B. J. Page, A. Pan, Y. Pankow, C. Papa, M. A. Pareja, M. Patel, P. Pathak, D. Pedraza, M. Pekowsky, L. Penn, S. Peralta, C. Perreca, A. Pickenpack, M. Pinto, I. M. Pitkin, M. Pletsch, H. J. Plissi, M. V. Postiglione, F. Predoi, V. Price, L. R. Prijatelj, M. Principe, M. Prix, R. Prokhorov, L. Puncken, O. Quetschke, V. Raab, F. J. Radke, T. Radkins, H. Raffai, P. Rakhmanov, M. Rankins, B. Raymond, V. Reed, C. M. Reed, T. Reid, S. Reitze, D. H. Riesen, R. Riles, K. Roberts, P. Robertson, N. A. Robinson, C. Robinson, E. L. Roddy, S. Rover, C. Rollins, J. Romano, J. D. Romie, J. H. Rowan, S. Rudiger, A. Ryan, K. Sakata, S. Sakosky, M. Salemi, F. Sammut, L. de la Jordana, L. Sancho Sandberg, V. Sannibale, M. V. Santamaria, L. Santostasi, G. Saraf, S. Sathyaprakash, B. S. Sato, S. Satterthwaite, M. Saulson, P. R. Savage, R. Schilling, R. Schnabel, R. Schofield, R. M. S. Schulz, B. Schutz, B. F. Schwinberg, P. Scott, J. Scott, S. M. Searle, A. C. Seifert, F. Sellers, D. Sengupta, A. S. Sergeev, A. Shaddock, D. A. Shapiro, B. Shawhan, P. Shoemaker, D. H. Sibley, A. Siemens, X. Sigg, D. Singer, A. Suites, A. M. Skelton, G. Slagmolen, B. J. J. Slutsky, J. Smith, J. R. Smith, M. R. Smith, N. D. Somiya, K. Sorazu, B. Speirits, F. C. Stein, A. J. Stein, L. C. Steinlechner, S. Steplewski, S. Stochino, A. Stone, R. Strain, K. A. Strigin, S. Stroeer, A. Stuver, A. L. Summerscales, T. Z. Sung, M. Susmithan, S. Sutton, P. Szokoly, G. P. Talukder, D. Tanner, D. B. Tarabrin, S. P. Taylor, J. R. Taylor, R. Thomas, P. Thorne, K. A. Thorne, K. S. 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TI Calibration of the LIGO gravitational wave detectors in the fifth science run SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Interferometer; Calibration; Control systems; Gravitational waves AB The Laser Interferometer Gravitational Wave Observatory (LIGO) is a network of three detectors built to detect local perturbations in the space-time metric from astrophysical sources These detectors two in Hanford WA and one in Livingston LA are power-recycled Fabry-Perot Michelson interferometers In their fifth science run (S5) between November 2005 and October 2007 these detectors accumulated one year of triple coincident data while operating at their designed sensitivity In this paper we describe the calibration of the instruments in the S5 data set including measurement techniques and uncertainty estimation (C) 2010 Elsevier B V All rights reserved C1 [Kissel, J. 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RI Howell, Eric/H-5072-2014; Biswas, Rahul/H-7474-2016; Sigg, Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms, Jan/J-4359-2012; Bartos, Imre/A-2592-2017; Frey, Raymond/E-2830-2016; Sergeev, Alexander/F-3027-2017; Ward, Robert/I-8032-2014; Miao, Haixing/O-1300-2013; Khazanov, Efim/B-6643-2014; Salemi, Francesco/F-6988-2014; Lucianetti, Antonio/G-7383-2014; Nawrodt, Ronny/J-5155-2014; Danilishin, Stefan/K-7262-2012; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Finn, Lee Samuel/A-3452-2009; Ottaway, David/J-5908-2015; Postiglione, Fabio/O-4744-2015; Gehring, Tobias/A-8596-2016; Graef, Christian/J-3167-2015; Costa, Cesar/G-7588-2012; Prokhorov, Leonid/I-2953-2012; Gorodetsky, Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Steinlechner, Sebastian/D-5781-2013; Pitkin, Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Santamaria, Lucia/A-7269-2012; Hammond, Giles/B-7861-2009; Shaddock, Daniel/A-7534-2011; McClelland, David/E-6765-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; Martin, Iain/A-2445-2010; Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Freise, Andreas/F-8892-2011; Abernathy, Matthew/G-1113-2011; Kawabe, Keita/G-9840-2011; Hild, Stefan/A-3864-2010 OI Veitch, John/0000-0002-6508-0713; Principe, Maria/0000-0002-6327-0628; Papa, M.Alessandra/0000-0002-1007-5298; Douglas, Ewan/0000-0002-0813-4308; Kanner, Jonah/0000-0001-8115-0577; Sorazu, Borja/0000-0002-6178-3198; Zweizig, John/0000-0002-1521-3397; O'Shaughnessy, Richard/0000-0001-5832-8517; Pathak, Devanka/0000-0002-1768-8353; Aulbert, Carsten/0000-0002-1481-8319; Fairhurst, Stephen/0000-0001-8480-1961; Matichard, Fabrice/0000-0001-8982-8418; Husa, Sascha/0000-0002-0445-1971; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Hallam, Jonathan Mark/0000-0002-7087-0461; Nishizawa, Atsushi/0000-0003-3562-0990; Howell, Eric/0000-0001-7891-2817; Biswas, Rahul/0000-0002-0774-8906; Sigg, Daniel/0000-0003-4606-6526; Frey, Raymond/0000-0003-0341-2636; Stein, Leo/0000-0001-7559-9597; Goetz, Evan/0000-0003-2666-721X; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; Miao, Haixing/0000-0003-4101-9958; Danilishin, Stefan/0000-0001-7758-7493; Vecchio, Alberto/0000-0002-6254-1617; Finn, Lee Samuel/0000-0002-3937-0688; Postiglione, Fabio/0000-0003-0628-3796; Gehring, Tobias/0000-0002-4311-2593; Graef, Christian/0000-0002-4535-2603; Gorodetsky, Michael/0000-0002-5159-2742; Allen, Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401; Steinlechner, Sebastian/0000-0003-4710-8548; Pitkin, Matthew/0000-0003-4548-526X; Shaddock, Daniel/0000-0002-6885-3494; McClelland, David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355; Lueck, Harald/0000-0001-9350-4846; FU United States National Science Foundation; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Australian Research Council; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Educacion y Ciencia; Conselleria d Economia Hisenda i Innovacio of the Govern de les Illes Balears; Royal Society; Scottish Funding Council the Scottish Universities Physics Alliance; National Aeronautics and Space Administration; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P Sloan Foundation; California Institute of Technology; Massachusetts Institute of Technology; National Science Foundation [PHY-0107417] FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Science and Technology Facilities Council of the United Kingdom the Max-Planck-Society and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council the Council of Scientific and Industrial Research of India the Istituto Nazionale di Fisica Nucleare of Italy the Spanish Ministerio de Educacion y Ciencia the Conselleria d Economia Hisenda i Innovacio of the Govern de les Illes Balears the Royal Society the Scottish Funding Council the Scottish Universities Physics Alliance The National Aeronautics and Space Administration the Carnegie Trust the Leverhulme Trust the David and Lucile Packard Foundation the Research Corporation and the Alfred P Sloan Foundation; LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-0107417 This paper has LIGO Document Number LIGO-P0900120 NR 37 TC 91 Z9 91 U1 3 U2 25 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD DEC 1 PY 2010 VL 624 IS 1 BP 223 EP 240 DI 10.1016/j.nima.2010.07.089 PG 18 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 681IC UT WOS:000284303600031 ER PT J AU Lindstrom, EJ Maximenko, N AF Lindstrom, Eric J. Maximenko, Nikolai TI THE FUTURE OF OCEANOGRAPHY FROM SPACE INTRODUCTION TO THE SPECIAL ISSUE SO OCEANOGRAPHY LA English DT Editorial Material C1 [Lindstrom, Eric J.] NASA, Phys Oceanog Program, Sci Mission Directorate, Div Earth Sci, Washington, DC 20546 USA. [Maximenko, Nikolai] Univ Hawaii, Int Pacific Res Ctr, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. RP Lindstrom, EJ (reprint author), NASA, Phys Oceanog Program, Sci Mission Directorate, Div Earth Sci, Washington, DC 20546 USA. EM eric.j.lindstrom@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD DEC PY 2010 VL 23 IS 4 SI SI BP 12 EP 13 PG 2 WC Oceanography SC Oceanography GA 697DS UT WOS:000285493400005 ER PT J AU Fu, LL Chelton, DB Le Traon, PY Morrow, R AF Fu, Lee-Lueng Chelton, Dudley B. Le Traon, Pierre-Yves Morrow, Rosemary TI EDDY DYNAMICS FROM SATELLITE ALTIMETRY SO OCEANOGRAPHY LA English DT Article ID MESOSCALE VARIABILITY; GEOSAT ALTIMETRY; SOUTHERN-OCEAN; SEASAT ALTIMETER; NORTH PACIFIC; TOPEX/POSEIDON; VELOCITY; TRANSPORT; EDDIES; HEAT AB Most of the kinetic energy of ocean circulation is contained in ubiquitous mesoscale eddies. Their prominent signatures in sea surface height have rendered satellite altimetry highly effective in observing global ocean eddies. Our knowledge of ocean eddy dynamics has grown by leaps and bounds since the advent of satellite altimetry in the early 1980s. A satellite's fast sampling allows a broad view of the global distribution of eddy variability and its spatial structures. Since the early 1990s, the combination of data available from two simultaneous flying altimeters has resulted in a time-series record of global maps of ocean eddies. Despite the moderate resolution, these maps provide an opportunity to study the temporal and spatial variability of the surface signatures of eddies at a level of detail previously unavailable. A global census of eddies has been constructed to assess their population, polarity, intensity, and nonlinearity. The velocity and pattern of eddy propagation, as well as eddy transports of heat and salt, have been mapped globally. For the first time, the cascade of eddy energy through various scales has been computed from observations, providing evidence for the theory of ocean turbulence. Notwithstanding the tremendous progress made using existing observations, their limited resolution has prevented study of variability at wavelengths shorter than 100 km, where important eddy processes take place, ranging from energy dissipation to mixing and transport of water properties that are critical to understanding the ocean's roles in Earth's climate. The technology of radar interferometry promises to allow wide-swath measurement of sea surface height at a resolution that will resolve eddy structures down to 10 km. This approach holds the potential to meet the challenge of extending the observations to submesoscales and to set a standard for future altimetric measurement of the ocean. C1 [Fu, Lee-Lueng] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Chelton, Dudley B.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Le Traon, Pierre-Yves] Ifremer, Ctr Brest, F-29280 Plouzane, France. [Morrow, Rosemary] Ctr Natl Etud Spatiales, Lab Etud Geophys & Oceanog Spatiales, F-31055 Toulouse, France. RP Fu, LL (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM lee-lueng.fu@jpl.nasa.gov FU National Aeronautics and Space Administration; Ocean Surface Topography Science Team through NASA [NNX08AR37G]; Jason-1 Project; OSTM/Jason-2 project FX We are grateful to Patrice Klein of Ifremer for helpful discussions during the preparation of the paper. The research presented in the paper was carried out in part (LLF) at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Support from the Jason-1 and OSTM/Jason-2 projects is acknowledged. The contributions from DBC were supported as part of the Ocean Surface Topography Science Team through NASA grant NNX08AR37G. NR 49 TC 72 Z9 74 U1 0 U2 12 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD DEC PY 2010 VL 23 IS 4 SI SI BP 14 EP 25 PG 12 WC Oceanography SC Oceanography GA 697DS UT WOS:000285493400006 ER PT J AU Willis, JK Chambers, DP Kuo, CY Shum, CK AF Willis, Josh K. Chambers, Don P. Kuo, Chung-Yen Shum, C. K. TI Global Sea Level Rise RECENT PROGRESS AND CHALLENGES FOR THE DECADE TO COME SO OCEANOGRAPHY LA English DT Article ID UPPER-OCEAN; TOPEX; GREENLAND; CRITIQUE; CLIMATE; BUDGET AB The study of sea level rise is a highly interdisciplinary endeavor with important implications for our society as it adapts to a warming climate. Although-the past two decades have revolutionized our understanding of sea level rise and its causes (primarily mass input, and ocean warming), major scientific challenges must be met before useful predictions can be Made. The rate of sea level rise has accelerated considerably relative to the pre-industrial era. Over the twentieth century, global sea level increased at an average rate of about 2 mm yr(-1), which is substantially larger than the rate of the previous three millennia. Furthermore, evidence now exists for additional acceleration during the twentieth century. Nevertheless, accurate prediction of future sea level rise requires continued observations as well as significant advances in modeling of the coupled ice-ocean-land-atmosphere climate. A major effort is needed to sustain data recording from satellite altimeters (e.g., the Jason series), from time-variable gravity missions (e.g., Gravity Recovery And Climate Experiment, or GRACE), and from autonomous ocean observing systems (e.g., Argo). In addition, an interdisciplinary research effort is required to address major problems, including improvement of the historical records of sea level rise and ocean warming, the separation of other geophysical processes from sea level rise signals, and a more complete understanding of interactions between the ocean and ice sheets. C1 [Willis, Josh K.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Chambers, Don P.] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. [Kuo, Chung-Yen] Natl Cheng Kung Univ, Dept Geomat, Tainan 70101, Taiwan. [Shum, C. K.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. RP Willis, JK (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM joshua.k.willis@jpl.nasa.gov OI Chambers, Don/0000-0002-5439-0257 FU US National Aeronautics and Space Administration (NASA); NASA Interdisciplinary Science Team; National Research Council, Taiwan; NASA [NNX09AF42G]; OSU FX This work was carried out in part at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the US National Aeronautics and Space Administration (NASA). Work at the University of South Florida was carried out under a grant from the NASA Interdisciplinary Science Team. Research at National Cheng-Kung University is funded by the National Research Council, Taiwan. The Ohio State University (OSU) component of this work is supported by NASA's Physical Oceanography Program (NNX09AF42G) and by OSU's Climate, Water and Carbon Program (http://cwc/osu.edu). The GRACE data are from University of Texas Center for Space Research (UTCSR), the German Research Center for Geosciences (GFZ), and JPL, and the altimeter data are from NASA, Centre National d'Etudes Spatiales, European Space Agency, and US Navy via the National Oceanic and Atmospheric Administration. We thank A. Cazenave, W. Llovel, E. Leuliette, and S. Nerem for providing their processed satellite altimetry sea level time series for this study. We acknowledge reviewers Anny Cazenave, Steve Nerem, and Neil White for their constructive comments. NR 45 TC 30 Z9 31 U1 0 U2 17 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD DEC PY 2010 VL 23 IS 4 SI SI BP 26 EP 35 PG 10 WC Oceanography SC Oceanography GA 697DS UT WOS:000285493400007 ER PT J AU Bourassa, MA Gille, ST Jackson, DL Roberts, JB Wick, GA AF Bourassa, Mark A. Gille, Sarah T. Jackson, Darren L. Roberts, J. Brent Wick, Gary A. TI Ocean Winds and Turbulent Air-Sea Fluxes Inferred From Remote Sensing SO OCEANOGRAPHY LA English DT Article ID EQUATORIAL PACIFIC-OCEAN; SENSOR MICROWAVE IMAGER; LATENT-HEAT FLUX; SURFACE TEMPERATURE; SAMPLING ERRORS; GLOBAL OCEANS; BULK PARAMETERIZATION; VOS OBSERVATIONS; HIGH-RESOLUTION; GAS TRANSFER AB Surface turbulent fluxes are key pathways through which the atmosphere is coupled with the ocean. They provide mechanisms through which momentum, energy, moisture, and materials such as CO2 are transferred between the ocean and atmosphere. Surface fluxes are also important players in vertical and horizontal transport in the atmosphere and the ocean. There have been attempts to estimate surface fluxes directly from satellite observations; however, they are typically calculated from observations of surface and near-surface variables. Recent improvements in the measurement of vector winds, air temperatures, and atmospheric humidities have all contributed to better estimation of surface fluxes from satellite observations. These advances are discussed in the context of applications, with examples from a tropical cyclone and a very strong mid-latitude storm. Proposed future systems that use improved instrumentation and collecate observations of winds, temperatures, and humidities will increase the accuracy beyond current capabilities. Targets for a variety of important climate-related processes are provided. C1 [Bourassa, Mark A.] Florida State Univ, COAPS, Tallahassee, FL 32306 USA. [Bourassa, Mark A.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. [Gille, Sarah T.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Jackson, Darren L.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Roberts, J. Brent] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA. [Wick, Gary A.] NOAA, Satellite Applicat Grp, Natl Earth Syst Res Lab, Boulder, CO USA. RP Bourassa, MA (reprint author), Florida State Univ, COAPS, Tallahassee, FL 32306 USA. EM bourassa@coaps.fsu.edu RI Gille, Sarah/B-3171-2012; Jackson, Darren/D-5506-2015 OI Jackson, Darren/0000-0001-5211-7866 NR 72 TC 15 Z9 15 U1 0 U2 9 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD DEC PY 2010 VL 23 IS 4 SI SI BP 36 EP 51 PG 16 WC Oceanography SC Oceanography GA 697DS UT WOS:000285493400008 ER PT J AU Lee, T Hakkinen, S Kelly, K Qiu, B Bonekamp, H Lindstrom, EJ AF Lee, Tong Hakkinen, Sirpa Kelly, Kathie Qiu, Bo Bonekamp, Hans Lindstrom, Eric J. TI SATELLITE OBSERVATIONS OF OCEAN CIRCULATION CHANGES ASSOCIATED WITH CLIMATE VARIABILITY SO OCEANOGRAPHY LA English DT Article ID MERIDIONAL OVERTURNING CIRCULATION; NORTH-ATLANTIC OSCILLATION; PACIFIC-OCEAN; DECADAL VARIABILITY; GULF-STREAM; INTERANNUAL VARIABILITY; ATMOSPHERE; GYRE; GREENLAND; ANOMALIES AB Decades of satellite observations have greatly improved our understanding of large-scale ocean circulation changes associated with climate variability, related air-sea interaction, and interbasic linkages. The continuation and enhancement (e.g., increased spatial resolution and frequency) of these satellite measurements and observations of additional parameters (e.g., sea surface salinity) in the coming decades are critical to further advancing our ability to monitor and understand decadal and longer variations in ocean circulation and determining the extent to which these changes result from natural climate variability or anthropogenic inputs. C1 [Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Hakkinen, Sirpa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kelly, Kathie] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA. [Qiu, Bo] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Dept Oceanog, Honolulu, HI 96822 USA. [Bonekamp, Hans] European Org Exploitat Meteorol Satellites EUMETS, Darmstadt, Germany. [Lindstrom, Eric J.] NASA Headquarters, Washington, DC USA. RP Lee, T (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM tlee@jpl.nasa.gov RI Hakkinen, Sirpa/E-1461-2012; Qiu, Bo/D-9569-2017 FU National Aeronautics and Space Administration (NASA); California Institute of Technology FX The research described in this paper was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA) with support from the NASA Physical Oceanography Program. Copyright 2010 California Institute of Technology. Government sponsorship acknowledged. NR 54 TC 4 Z9 5 U1 0 U2 14 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD DEC PY 2010 VL 23 IS 4 SI SI BP 70 EP 81 PG 12 WC Oceanography SC Oceanography GA 697DS UT WOS:000285493400010 ER PT J AU Kwok, R Sulsky, D AF Kwok, Ron Sulsky, Deborah TI Arctic Ocean Sea Ice Thickness and Kinematics SATELLITE RETRIEVALS AND MODELING SO OCEANOGRAPHY LA English DT Article ID THERMODYNAMIC MODEL AB Sea ice in the Arctic Ocean ranges from thin new ice to thick deformed ridges. Changes in thickness are due to melting and freezing, and to physical rearrangement of existing ice to form leads and pressure ridges. As a brittle solid, fractures are created when the ice cover moves and deforms. Openings along fractures are sites of local heat exchange between the atmosphere and ocean, and of local ice production in the winter as ocean water freezes when exposed to the colder atmosphere. Closing of the ice forces it to raft or pile up into pressure ridges and to be forced down into keels, increasing the volume of sea ice that can be stored within a given area of the Arctic Ocean. This mechanical redistribution of sea ice affects ice strength and has a profound impact on ice behavior over a wide range of temporal and spatial scales. Accurate observation and simulation of the relative contributions of thermodynamics and dynamics to ice thickness distribution are thus critical for understanding the ice cover in terms of how it changes, and its vulnerability in a warming climate. Recent satellite altimetry and high-resolution synthetic aperture radar imaging have provided near-basin-scale views of ice thickness and motion for use in quantifying changes, and for assessment and refinerneut of models. During this coming decade, several satellite missions are poised to provide improved, coordinated, and near-continuous measurements of thickness and motion that will advance our understanding of Arctic ice cover. Here, we provide an overview of our current capabilities and the future prospects for observing these parameters from space. C1 [Kwok, Ron] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Sulsky, Deborah] Univ New Mexico, Dept Math & Stat, Albuquerque, NM 87131 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM ronald.kwok@jpl.nasa.gov RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 FU National Aeronautics and Space Administration; National Science Foundation [ARC-0621173] FX RK performed this work at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. DS was supported by the National Science Foundation under grant ARC-0621173. NR 33 TC 13 Z9 13 U1 2 U2 9 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD DEC PY 2010 VL 23 IS 4 SI SI BP 134 EP 143 PG 10 WC Oceanography SC Oceanography GA 697DS UT WOS:000285493400015 ER PT J AU Stramel, AA Gupta, MC Lee, HR Yu, J Edwards, WC AF Stramel, A. A. Gupta, M. C. Lee, H. R. Yu, J. Edwards, W. C. TI Pulsed laser deposition of carbon nanotube and polystyrene-carbon nanotube composite thin films SO OPTICS AND LASERS IN ENGINEERING LA English DT Article DE Laser ablation; Carbon nanotubes; CNT; Thin films ID TRANSPARENT AB In this work, we report on the fabrication of carbon nanotube thin films via pulsed laser deposition using a pulsed, diode pumped, Tm:Ho:LuLF laser with 2 mu m wavelength. The thin films were deposited on silicon substrates using pure carbon nanotube targets and polystyrene-carbon nanotube composite targets. Raman spectra, scanning electron micrographs, and transmission electron micrographs show that carbon nanotubes are present in the deposited thin films, and that the pulsed laser deposition process causes minimal degradation to the quality of the nanotubes when using pure carbon nanotube targets. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Stramel, A. A.; Gupta, M. C.] Univ Virginia, Charles L Brown Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. [Lee, H. R.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Yu, J.; Edwards, W. C.] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Gupta, MC (reprint author), Univ Virginia, Charles L Brown Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. EM mgupta@virginia.edu NR 16 TC 9 Z9 12 U1 0 U2 10 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0143-8166 J9 OPT LASER ENG JI Opt. Lasers Eng. PD DEC PY 2010 VL 48 IS 12 BP 1291 EP 1295 DI 10.1016/j.optlaseng.2010.06.002 PG 5 WC Optics SC Optics GA 657YS UT WOS:000282456000021 ER PT J AU Benning, LG Villar, SJ Eigenbrode, JL Tobler, DJ Fogel, ML Steele, A Edwards, HGM AF Benning, L. G. Villar, S. J. Eigenbrode, J. L. Tobler, D. J. Fogel, M. L. Steele, A. Edwards, H. G. M. CA AMASE TI Cryophile Biosignature Preservation in Arctic Glacial Ice 'Survival of the Fittest' and What Does this Mean for Planetary Exploration? SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Meeting Abstract C1 [Benning, L. G.; Tobler, D. J.] Univ Leeds, Earth & Biosphere Inst, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Villar, S. J.] Univ Burgos, Area Geodynam Interna, Fac Humanidades & Educ, Burgos, Spain. [Eigenbrode, J. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fogel, M. L.; Steele, A.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20005 USA. [Edwards, H. G. M.] Univ Bradford, Bradford BD7 1DP, W Yorkshire, England. RI Eigenbrode, Jennifer/D-4651-2012; Benning, Liane/E-7071-2011; Tobler, Dominique/G-3213-2012; Jorge-Villar, Susana/A-8927-2011 OI Benning, Liane/0000-0001-9972-5578; Tobler, Dominique/0000-0001-8532-1855; Jorge-Villar, Susana/0000-0003-1676-4438 NR 0 TC 0 Z9 0 U1 0 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2010 VL 40 IS 6 SI SI BP 534 EP 534 PG 1 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 691GX UT WOS:000285069400027 ER PT J AU Billi, D Ghelardini, P Grenga, L Warren-Rhodes, KA Mckay, CP AF Billi, D. Ghelardini, P. Grenga, L. Warren-Rhodes, K. A. McKay, C. P. TI Unravelling the DNA Protection and Repair Mechanisms in Desert Strains of Chroococcidiopsis under Extreme Terrestrial and Extraterrestrial Environments SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Meeting Abstract ID CYANOBACTERIUM C1 [Billi, D.; Ghelardini, P.; Grenga, L.] Univ Roma Tor Vergata, Dipartimento Biol, I-00173 Rome, Italy. [Ghelardini, P.] CNR, Ist Biol & Patol Mol, Rome, Italy. [Warren-Rhodes, K. A.; McKay, C. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 4 TC 0 Z9 0 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2010 VL 40 IS 6 SI SI BP 535 EP 536 PG 2 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 691GX UT WOS:000285069400028 ER PT J AU Leuko, S Neilan, BA Rothschild, LJ AF Leuko, S. Neilan, B. A. Rothschild, L. J. TI Modern Extreme Environments The Key to Study the Evolution of Life? SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Meeting Abstract C1 [Leuko, S.; Rothschild, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Neilan, B. A.] Australian Ctr Astrobiol, Sydney, NSW, Australia. NR 0 TC 0 Z9 0 U1 1 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2010 VL 40 IS 6 SI SI BP 555 EP 555 PG 1 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 691GX UT WOS:000285069400051 ER PT J AU Conley, C AF Conley, C. TI Biodiversity in the Context of Planetary Protection SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Meeting Abstract C1 [Conley, C.] NASA Headquarters, Washington, DC USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2010 VL 40 IS 6 SI SI BP 576 EP 577 PG 2 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 691GX UT WOS:000285069400079 ER PT J AU Cleaves, HJ Dworkin, JP AF Cleaves, H. J., II Dworkin, J. P. TI The Amino Acids Produced from HCN and Mixed HCN/HCHO Reactions Implications for Organic Chemistry in Extraterrestrial Bodies SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Meeting Abstract C1 [Cleaves, H. J., II] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Dworkin, J. P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RI Dworkin, Jason/C-9417-2012 OI Dworkin, Jason/0000-0002-3961-8997 NR 0 TC 1 Z9 1 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2010 VL 40 IS 6 SI SI BP 587 EP 588 PG 2 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 691GX UT WOS:000285069400093 ER PT J AU Brooks, KR Stone, LS AF Brooks, Kevin R. Stone, Leland S. TI ACCURACY OF STEREOMOTION SPEED PERCEPTION WITH PERSISTING AND DYNAMIC TEXTURES SO PERCEPTUAL AND MOTOR SKILLS LA English DT Article ID MOTION-IN-DEPTH; OCULAR VELOCITY DIFFERENCES; TIME-TO-COLLISION; CHANGING-DISPARITY; DISCRIMINATION; INFORMATION; DIRECTION; CUE; SIZE AB It has been established that the motion in depth of stimuli visible to both eyes may be signalled binocularly either by a change of disparity over time or by the difference in the velocity of the images projected on each retina, known as an interocular velocity difference. A two-interval forced-choice stereomotion speed discrimination experiment was performed on four participants to ascertain the relative speed of a persistent random dot stereogram (RDS) and a dynamic RDS undergoing directly approaching or receding motion in depth. While the persistent RDS pattern involved identical dot patterns translating in opposite directions in each eye, and hence included both changing disparity and interocular velocity difference cues, the dynamic RDS pattern (which contains no coherent monocular motion signals) specified motion in depth through changing disparity, but no motion through interocular velocity difference. Despite an interocular velocity difference speed signal of zero motion in depth, the dynamic RDS stimulus appeared to move more rapidly. These observations are consistent with a scheme in which cues that rely on coherent monocular motion signals (such as looming and the interocular velocity difference cue) are less influential in dynamic stimuli due to their lack of reliability (i.e., increased noise). While dynamic RDS stimuli may be relatively unaffected by the contributions of such cues when they signal that the stimulus did not move in depth, the persistent RDS stimulus may retain a significant and conflicting contribution from the looming cue, resulting in a lower perceived speed. C1 [Brooks, Kevin R.] Macquarie Univ, Dept Psychol, N Ryde, NSW 2109, Australia. [Brooks, Kevin R.; Stone, Leland S.] NASA, Ames Res Ctr, Washington, DC 20546 USA. RP Brooks, KR (reprint author), Macquarie Univ, Dept Psychol, N Ryde, NSW 2109, Australia. EM kevin.brooks@mq.edu.au OI Brooks, Kevin/0000-0003-1424-4092 NR 39 TC 2 Z9 2 U1 0 U2 1 PU AMMONS SCIENTIFIC, LTD PI MISSOULA PA PO BOX 9229, MISSOULA, MT 59807-9229 USA SN 0031-5125 J9 PERCEPT MOTOR SKILL JI Percept. Mot. Skills PD DEC PY 2010 VL 111 IS 3 BP 921 EP 935 DI 10.2466/15.24.27.PMS.111.6.921-935 PG 15 WC Psychology, Experimental SC Psychology GA 704UT UT WOS:000286081800025 PM 21319629 ER PT J AU Nishino, T Hahn, S Shariff, K AF Nishino, Takafumi Hahn, Seonghyeon Shariff, Karim TI Large-eddy simulations of a turbulent Coanda jet on a circulation control airfoil SO PHYSICS OF FLUIDS LA English DT Article ID WALL-JET; FLOWS; CYLINDER AB Large-eddy simulations are performed of a turbulent Coanda jet separating from a rounded trailing edge of a simplified circulation control airfoil model. The freestream Reynolds number based on the airfoil chord is 0.49 x 10(6), the jet Reynolds number based on the jet slot height is 4470, and the ratio of the peak jet velocity to the freestream velocity is 3.96. Three different grid resolutions are used to show that their effect is very small on the mean surface pressure distribution, which agrees very well with experiments, as well as on the mean velocity profiles over the Coanda surface. It is observed that the Coanda jet becomes fully turbulent just downstream of the jet exit, accompanied by asymmetric alternating vortex shedding behind a thin (but blunt) jet blade splitting the jet and the external flow. A number of "backward-tilted" hairpin vortices (i.e., the head of each hairpin being located upstream of the legs) are observed around the outer edge of the jet over the Coanda surface. These hairpins create strong upwash between the legs and weak downwash around them, contributing to turbulent mixing of the high-momentum jet below the hairpins and the low-momentum external flow above them. The probability density distribution of velocity fluctuations is shown to be highly asymmetric in this region, consistent with the observation that the hairpin vortices create strong upwash and weak downwash. Turbulent structures inside the jet, its spreading rate, and self-similarity are also discussed. (C) 2010 American Institute of Physics. [doi:10.1063/1.3526757] C1 [Nishino, Takafumi; Shariff, Karim] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hahn, Seonghyeon] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. RP Nishino, T (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM takafumi.nishino@nasa.gov; karim.r.shariff@nasa.gov RI Nishino, Takafumi/A-2685-2012; OI Nishino, Takafumi/0000-0001-6306-7702; Shariff, Karim/0000-0002-7256-2497 FU NASA FX The present work has been supported by the Subsonic Fixed Wing Project of the Fundamental Aeronautics Program at NASA. The first author has been supported by the NASA Postdoctoral Program (NPP) administrated by Oak Ridge Associated Universities (ORAU). Computing resources and support were provided by the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. The authors would like to thank Dr. Greg Jones and Dr. Brian Allan of Langley Research Center for providing the experimental data, and Dr. Mike Rogers and Dr. Nateri Madavan of Ames Research Center for many helpful discussions. NR 28 TC 5 Z9 6 U1 1 U2 11 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 DEC PY 2010 VL 22 IS 12 AR 125105 DI 10.1063/1.3526757 PG 15 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 700UQ UT WOS:000285770200032 ER PT J AU Gazis, PR Levit, C Way, MJ AF Gazis, P. R. Levit, C. Way, M. J. TI Viewpoints: A High-Performance High-Dimensional Exploratory Data Analysis Tool SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID DIGITAL SKY SURVEY; VISUALIZATION AB Scientific data sets continue to increase in both size and complexity. In the past, dedicated graphics systems at supercomputing centers were required to visualize large data sets, but as the price of commodity graphics hardware has dropped and its capability has increased, it is now possible, in principle, to view large complex data sets on a single workstation. To do this in practice, an investigator will need software that is written to take advantage of the relevant graphics hardware. The Viewpoints visualization package described herein is an example of such software. Viewpoints is an interactive tool for exploratory visual analysis of large high-dimensional (multivariate) data. It leverages the capabilities of modern graphics boards (GPUs) to run on a single workstation or laptop. Viewpoints is minimalist: it attempts to do a small set of useful things very well (or at least very quickly) in comparison with similar packages today. Its basic feature set includes linked scatter plots with brushing, dynamic histograms, normalization, and outlier detection/removal. Viewpoints was originally designed for astrophysicists, but it has since been used in a variety of fields that range from astronomy, quantum chemistry, fluid dynamics, machine learning, bioinformatics, and finance to information technology server log mining. In this article, we describe the Viewpoints package and show examples of its usage. C1 [Way, M. J.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Gazis, P. R.] SETI Inst, Mountain View, CA 94043 USA. [Way, M. J.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Way, MJ (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. EM pgazis@sbcglobal.net; Creon.Levit@nasa.gov; Michael.J.Way@nasa.gov RI Way, Michael/D-5254-2012; OI Way, Michael/0000-0003-3728-0475 FU NASA FX Many thanks go to Chris Henze and Jeff Scargle for their input and ideas. The authors would also like to thank Joe Bredekamp and his NASA Applied Information Systems Research Program for pilot funding of Viewpoints. M. J. W. would like to thank the Astronomy Department of Uppsala University for their kind hospitality. This research has made use of NASA's Astrophysics Data System. Viewpoints has been released under the NASA Open Source Agreement and is considered an open source license. The source code and precompiled binaries can be freely downloaded from the Viewpoints Web site. If you use Viewpoints in your research, please consider referencing this work. NR 24 TC 6 Z9 6 U1 0 U2 4 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 DEC PY 2010 VL 122 IS 898 BP 1518 EP 1525 DI 10.1086/657902 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 694XN UT WOS:000285335300010 ER PT J AU Chappell, LJ Whalen, MK Gurai, S Ponomarev, A Cucinotta, FA Pluth, JM AF Chappell, Lori J. Whalen, Mary K. Gurai, Sheena Ponomarev, Artem Cucinotta, Francis A. Pluth, Janice M. TI Analysis of Flow Cytometry DNA Damage Response Protein Activation Kinetics after Exposure to X Rays and High-Energy Iron Nuclei SO RADIATION RESEARCH LA English DT Article ID DOUBLE-STRAND BREAKS; PHOSPHORYLATED HISTONE H2AX; HUMAN FIBROBLASTS; CELL-CYCLE; TRANSCRIPTION FACTOR; IONIZING-RADIATION; SPACE EXPLORATION; GAMMA-H2AX FOCI; CHROMATIN LOOPS; REPAIR AB We developed a mathematical method to analyze flow cytometry data to describe the kinetics of gamma-H2AX and pATF2 phosphorylation in normal human fibroblast cells after exposure to various qualities of low-dose radiation. Previously reported flow cytometry kinetics for these DSB repair phospho-proteins revealed that distributions of intensity were highly skewed, severely limiting the detection of differences in the very low-dose range. Distributional analysis revealed significant differences between control and low-dose samples when distributions were compared using the Kolmogorov-Smirnov test. Differences in radiation quality were found in the distribution shapes and when a nonlinear model was used to relate dose and time to the decay of the mean ratio of phospho-protein intensities of irradiated samples to controls. We analyzed cell cycle phase- and radiation quality-dependent characteristic repair times and residual phospho-protein levels with these methods. Characteristic repair times for gamma-H2AX were higher after exposure to iron nuclei compared to X rays in G(1) cells and in SIG(2) cells. The RBE in G(1) cells for iron nuclei relative to X rays for gamma-H2AX was 2.1 +/- 0.6 and 5.0 +/- 3.5 at 2 and 24 h after irradiation, respectively. For pATF2, a saturation effect was observed with reduced expression at high doses, especially for iron nuclei, with much slower characteristic repair times (>7 h) compared to X rays. RBEs for pATF2 were 0.7 +/- 0.1 and 1.7 +/- 0.5 at 2 and 24 h, respectively. Significant differences in gamma-H2AX and pATF2 levels when irradiated samples were compared to controls were noted even at the lowest dose analyzed (0.05 Gy). These results show that mathematical models can be applied to flow cytometry data to identify important and subtle differences after exposure to various qualities of low-dose radiation. (C) 2010 by Radiation Research Society C1 [Whalen, Mary K.; Gurai, Sheena; Pluth, Janice M.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Life Sci, Berkeley, CA 94720 USA. [Chappell, Lori J.; Ponomarev, Artem] USRA, Div Space Life Sci Div, Houston, TX 77058 USA. [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Pluth, JM (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, Div Life Sci, 1 Cyclotron Rd, Berkeley, CA 94720 USA. EM JMPluth@lbl.gov FU NASA [03-OBPR-07-0032-0027]; U.S. DOE [DE-A103-05ER64843] FX We gratefully acknowledge partial financial support provided by the NASA Space Radiation Program (03-OBPR-07-0032-0027) and the U.S. DOE (DE-A103-05ER64843). NR 47 TC 10 Z9 10 U1 0 U2 1 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 DEC PY 2010 VL 174 IS 6 BP 691 EP 702 DI 10.1667/RR2204.1 PN 1 PG 12 WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology, Nuclear Medicine & Medical Imaging GA 690TQ UT WOS:000285031500003 PM 21128792 ER PT J AU Moreno-Madrinan, MJ Al-Hamdan, MZ Rickman, DL Muller-Karger, FE AF Moreno-Madrinan, Max J. Al-Hamdan, Mohammad Z. Rickman, Douglas L. Muller-Karger, Frank E. TI Using the Surface Reflectance MODIS Terra Product to Estimate Turbidity in Tampa Bay, Florida SO REMOTE SENSING LA English DT Article DE water quality; light attenuation; turbidity; estuarine remote sensing; rainfall; color AB Turbidity is a commonly-used index of the factors that determine light penetration in the water column. Consistent estimation of turbidity is crucial to design environmental and restoration management plans, to predict fate of possible pollutants, and to estimate sedimentary fluxes into the ocean. Traditional methods monitoring fixed geographical locations at fixed intervals may not be representative of the mean water turbidity in estuaries between intervals, and can be expensive and time consuming. Although remote sensing offers a good solution to this limitation, it is still not widely used due in part to required complex processing of imagery. There are satellite-derived products, including the Moderate Resolution Imaging Spectroradiometer (MODIS) Terra surface reflectance daily product (MOD09GQ) Band 1 (620-670 nm) which are now routinely available at 250 m spatial resolution and corrected for atmospheric effect. This study shows this product to be useful to estimate turbidity in Tampa Bay, Florida, after rainfall events (R-2 = 0.76, n = 34). Within Tampa Bay, Hillsborough Bay (HB) and Old Tampa Bay (OTB) presented higher turbidity compared to Middle Tampa Bay (MTB) and Lower Tampa Bay (LTB). C1 [Al-Hamdan, Mohammad Z.] NASA, Univ Space Res Assoc,Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA. [Rickman, Douglas L.] NASA, Earth Sci Off,Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA. [Muller-Karger, Frank E.] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. RP Moreno-Madrinan, MJ (reprint author), NASA, Univ Space Res Assoc,Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA. EM max.j.moreno-madrinan@nasa.gov; mohammad.alhamdan@nasa.gov; douglas.l.rickman@nasa.gov; carib@marine.usf.edu OI Rickman, Doug/0000-0003-3409-2882 FU NASA FX This research was supported by an appointment to the NASA Postdoctoral Program at the Marshall Space Flight Center/National Space Science and Technology Center/NASA Global Hydrology and Climate Center in Huntsville, AL; administered by Oak Ridge Associated Universities through a contract with NASA. We express our great appreciation to the Environmental Protection Commission of Hillsborough County (EPCHC) for sharing Tampa Bay water quality data and particularly to Rick Garrity, Richard Boler, and Joe Barron from EPCHC for their assistance. NR 34 TC 14 Z9 16 U1 0 U2 10 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD DEC PY 2010 VL 2 IS 12 BP 2713 EP 2728 DI 10.3390/rs2122713 PG 16 WC Remote Sensing SC Remote Sensing GA V24HT UT WOS:000208402200005 ER PT J AU Yang, XA Tanaka, Z Newhouse, R Xu, QA Chen, B Chen, SW Zhang, JZ Gu, C AF Yang, Xuan Tanaka, Zuki Newhouse, Rebecca Xu, Qiao Chen, Bin Chen, Shaowei Zhang, Jin Z. Gu, Claire TI Portable fiber sensors based on surface-enhanced Raman scattering SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID PHOTONIC CRYSTAL FIBER; SILVER; PROBE; NANOPARTICLES AB Two portable molecular sensing systems based on surface-enhanced Raman scattering (SERS) have been experimentally demonstrated using either a tip-coated multimode fiber (TCMMF) or a liquid core photonic crystal fiber (LCPCF) as the SERS probe. With Rhodamine 6G as a test molecule, the TCMMF-portable SERS system achieved 2-3 times better sensitivity than direct sampling (focusing the laser light directly into the sample without the fiber probe), and a highly sensitive LCPCF-portable SERS system reached a sensitivity up to 59 times that of direct sampling, comparable to the sensitivity enhancement achieved using fiber probes in the bulky Renishaw system. These fiber SERS probes integrated with a portable Raman spectrometer provide a promising scheme for a compact and flexible molecular sensing system with high sensitivity and portability. (C) 2010 American Institute of Physics. [doi:10.1063/1.3518957] C1 [Yang, Xuan; Tanaka, Zuki; Chen, Bin; Gu, Claire] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA. [Yang, Xuan; Tanaka, Zuki; Chen, Bin; Gu, Claire] NASA, Ames Res Ctr, Adv Studies Labs, Moffett Field, CA 94035 USA. [Newhouse, Rebecca; Xu, Qiao; Chen, Shaowei; Zhang, Jin Z.] Univ Calif Santa Cruz, Dept Chem & Biochem, Santa Cruz, CA 95064 USA. RP Yang, XA (reprint author), Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA. EM claire@soe.ucsc.edu RI Yang, Xuan/G-5620-2012 FU National Science Foundation [ECCS-0823921]; UC; UARC/NASA; UCSC FX We acknowledge the support from the National Science Foundation, ECCS-0823921, the UC MICRO grant, UARC/NASA, and the UCSC Special Research Grant. NR 24 TC 11 Z9 11 U1 5 U2 44 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD DEC PY 2010 VL 81 IS 12 AR 123103 DI 10.1063/1.3518957 PG 5 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 700UW UT WOS:000285770800004 PM 21198010 ER PT J AU Qin, GX Jiang, NY Seo, JH Cho, NK Ponchak, GE van der Weide, D Ma, PX Stetson, S Racanelli, M Ma, ZQ AF Qin, Guoxuan Jiang, Ningyue Seo, Jung-Hun Cho, Namki Ponchak, George E. van der Weide, Daniel Ma, Pingxi Stetson, Scott Racanelli, Marco Ma, Zhenqiang TI Cryogenic operation of a 24 GHz MMIC SiGe HBT medium power amplifier SO SEMICONDUCTOR SCIENCE AND TECHNOLOGY LA English DT Article ID BIPOLAR-TRANSISTORS; BASE; OPTIMIZATION; TECHNOLOGY; CIRCUITS; SILICON; DESIGN AB The performance of a SiGe heterojunction bipolar transistor (HBT) millimetre-wave power amplifier (PA) operating at cryogenic temperature was reported and analysed for the first time. A 24 GHz two-stage medium PA employing common-emitter and common-base SiGe power HBTs in the first and the second stage, respectively, showed a significant power gain increase at 77 K in comparison with that measured at room temperature. Detailed analyses indicate that cryogenic operation of SiGe HBT-based PAs mainly affects (improves) the performance of the SiGe HBTs in the circuits due to transconductance enhancement through magnified, favourable changes of SiGe bandgap due to cooling (Delta E(g)/kT) and minimized thermal effects, with little influence on the passive components of the circuits. C1 [Qin, Guoxuan; Jiang, Ningyue; Seo, Jung-Hun; Cho, Namki; van der Weide, Daniel; Ma, Zhenqiang] Univ Wisconsin, Dept Elect & Comp Engn, Madison, WI 53706 USA. [Ponchak, George E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Ma, Pingxi; Stetson, Scott; Racanelli, Marco] Jazz Semicond Inc, Newport Beach, CA 92660 USA. RP Qin, GX (reprint author), Tianjin Univ, Dept Elect Sci & Technol, Tianjin 300072, Peoples R China. EM mazq@engr.wisc.edu RI Seo, Jung-Hun/G-2659-2012 OI Seo, Jung-Hun/0000-0002-5039-2503 NR 19 TC 5 Z9 5 U1 1 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0268-1242 J9 SEMICOND SCI TECH JI Semicond. Sci. Technol. PD DEC PY 2010 VL 25 IS 12 AR 125002 DI 10.1088/0268-1242/25/12/125002 PG 5 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA 684DK UT WOS:000284527500002 ER PT J AU Okraku, EW Gupta, MC Wright, KD AF Okraku, E. W. Gupta, M. C. Wright, K. D. TI Pulsed laser annealing of P3HT/PCBM organic solar cells SO SOLAR ENERGY MATERIALS AND SOLAR CELLS LA English DT Article DE Laser annealing; Organic solar cells; P3HT; PCBM ID SELF-ORGANIZATION; HEAT-TREATMENT; POLYMER; MORPHOLOGY; BLENDS AB A pulsed laser heating method has been investigated as a thermal annealing process for the improvement of P3HT/PCBM organic solar cell performance. We have shown that pulsed laser annealing can be used as an alternative to hot-plate annealing and produces comparable photovoltaic properties in P3HT/PCBM organic solar cells. Performance improvements can be achieved by irradiating either the ITO or aluminum electrodes. The increases in efficiency with laser annealing are due to increases in short circuit current density. Also, we have shown that morphology changes induced by rapid laser heating and cooling are similar to slower hot-plate annealing. (C) 2010 Elsevier B.V. All rights reserved. C1 [Okraku, E. W.; Gupta, M. C.] Univ Virginia, Charles L Brown Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. [Wright, K. D.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Gupta, MC (reprint author), Univ Virginia, Charles L Brown Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. EM mgupta@virginia.edu FU NASA-Langley through the NIA Langley FX We thank Dr. Teh-Hwa Wong of University of Virginia for the helpful discussions. We also acknowledge the help of Dr. Phillip Williams and Mr. Vincent Cruz of the NASA-Langley Research Center, for the use of the AFM and fabricating the solar cells, respectively. Thanks to NASA-Langley for their financial support through the NIA Langley Professor Program. NR 23 TC 11 Z9 14 U1 2 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-0248 J9 SOL ENERG MAT SOL C JI Sol. Energy Mater. Sol. Cells PD DEC PY 2010 VL 94 IS 12 BP 2013 EP 2017 DI 10.1016/j.solmat.2010.06.004 PG 5 WC Energy & Fuels; Materials Science, Multidisciplinary; Physics, Applied SC Energy & Fuels; Materials Science; Physics GA 676ZU UT WOS:000283959500006 ER PT J AU Lammer, H Dvorak, R Deleuil, M Barge, P Deeg, HJ Moutou, C Erikson, A Csizmadia, S Tingley, B Bruntt, H Havel, M Aigrain, S Almenara, JM Alonso, R Auvergne, M Baglin, A Barbieri, M Benz, W Bonomo, AS Borde, P Bouchy, F Cabrera, J Carone, L Carpano, S Ciardi, D Ferraz-Mello, S Fridlund, M Gandolfi, D Gazzano, JC Gillon, M Gondoin, P Guenther, E Guillot, T den Hartog, R Hasiba, J Hatzes, A Hidas, M Hebrard, G Jorda, L Kabath, P Leger, A Lister, T Llebaria, A Lovis, C Mayor, M Mazeh, T Mura, A Ollivier, M Ottacher, H Patzold, M Pepe, F Pont, F Queloz, D Rabus, M Rauer, H Rouan, D Samuel, B Schneider, J Shporer, A Stecklum, B Steller, M Street, R Udry, S Weingrill, J Wuchterl, G AF Lammer, H. Dvorak, R. Deleuil, M. Barge, P. Deeg, H. J. Moutou, C. Erikson, A. Csizmadia, Sz. Tingley, B. Bruntt, H. Havel, M. Aigrain, S. Almenara, J. M. Alonso, R. Auvergne, M. Baglin, A. Barbieri, M. Benz, W. Bonomo, A. S. Borde, P. Bouchy, F. Cabrera, J. Carone, L. Carpano, S. Ciardi, D. Ferraz-Mello, S. Fridlund, M. Gandolfi, D. Gazzano, J. -C. Gillon, M. Gondoin, P. Guenther, E. Guillot, T. den Hartog, R. Hasiba, J. Hatzes, A. Hidas, M. Hebrard, G. Jorda, L. Kabath, P. Leger, A. Lister, T. Llebaria, A. Lovis, C. Mayor, M. Mazeh, T. Mura, A. Ollivier, M. Ottacher, H. Paetzold, M. Pepe, F. Pont, F. Queloz, D. Rabus, M. Rauer, H. Rouan, D. Samuel, B. Schneider, J. Shporer, A. Stecklum, B. Steller, M. Street, R. Udry, S. Weingrill, J. Wuchterl, G. TI Exoplanet discoveries with the CoRoT space observatory SO SOLAR SYSTEM RESEARCH LA English DT Article ID ENERGETIC NEUTRAL ATOMS; TRANSITING EXOPLANETS; HOT JUPITERS; HD 209458B; MISSION; COROT-EXO-4B; PLANET AB The CoRoT space observatory is a project which is led by the French space agency CNES and leading space research institutes in Austria, Brazil, Belgium, Germany and Spain and also the European Space Agency ESA. CoRoT observed since its launch in December 27, 2006 about 100 000 stars for the exoplanet channel, during 150 days uninterrupted high-precision photometry. Since the The CoRoT-team has several exoplanet candidates which are currently analyzed under its study, we report here the discoveries of nine exoplanets which were observed by CoRoT. Discovered exoplanets such as CoRoT-3b populate the brown dwarf desert and close the gap of measured physical properties between usual gas giants and very low mass stars. CoRoT discoveries extended the known range of planet masses down to about 4.8 Earth-masses (CoRoT-7b) and up to 21 Jupiter masses (CoRoT-3b), the radii to about 1.68 x 0.09 R (Earth) (CoRoT-7b) and up to the most inflated hot Jupiter with 1.49 x 0.09 R (Earth) found so far (CoRoT-1b), and the transiting exoplanet with the longest period of 95.274 days (CoRoT-9b). Giant exoplanets have been detected at low metallicity, rapidly rotating and active, spotted stars. Two CoRoT planets have host stars with the lowest content of heavy elements known to show a transit hinting towards a different planethost-star-metallicity relation then the one found by radial-velocity search programs. Finally the properties of the CoRoT-7b prove that rocky planets with a density close to Earth exist outside the Solar System. Finally the detection of the secondary transit of CoRoT-1b at a sensitivity level of 10(-5) and the very clear detection of the "super-Earth" CoRoT-7b at 3.5 x 10(-4) relative flux are promising evidence that the space observatory is being able to detect even smaller exoplanets with the size of the Earth. C1 [Lammer, H.; Hasiba, J.; Ottacher, H.; Steller, M.; Weingrill, J.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Dvorak, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Deleuil, M.; Barge, P.; Moutou, C.; Barbieri, M.; Bonomo, A. S.; Gazzano, J. -C.; Jorda, L.; Llebaria, A.] CNRS, Lab Astrophys Marseille, F-13388 Marseille, France. [Deeg, H. J.; Tingley, B.; Almenara, J. M.; Rabus, M.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Deeg, H. J.; Tingley, B.; Almenara, J. M.; Rabus, M.] Univ La Laguna, Dept Astrofis, E-38200 Tenerife, Spain. [Erikson, A.; Csizmadia, Sz.; Cabrera, J.; Kabath, P.; Rauer, H.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [Cabrera, J.; Schneider, J.] Observ Paris, CNRS, LUTH, F-92195 Meudon, France. [Havel, M.; Guillot, T.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, UMR 6202, Nice, France. [Aigrain, S.; Pont, F.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Aigrain, S.] Univ Oxford, Oxford OX1 3RH, England. [Alonso, R.; Mayor, M.; Pepe, F.; Queloz, D.; Udry, S.] Observ Univ Geneve, CH-1290 Sauverny, Switzerland. [Barbieri, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Benz, W.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Borde, P.; Leger, A.; Ollivier, M.; Samuel, B.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Bouchy, F.; Hebrard, G.] IAP, F-75014 Paris, France. [Bouchy, F.] Observ Haute Provence, CNRS OAMP, St Michel Observ, F-04870 St Michel, France. [Cabrera, J.; Schneider, J.] Univ Paris Diderot, F-92195 Meudon, France. [Carone, L.; Paetzold, M.] Univ Cologne, Rhein Inst Umweltforsch, D-50931 Cologne, Germany. [Carpano, S.; Fridlund, M.; Gondoin, P.; den Hartog, R.] ESTEC ESA, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Ciardi, D.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Ferraz-Mello, S.; Lovis, C.] Univ Sao Paulo, Inst Astron Geophys & Atmospher Sci, BR-05508 Sao Paulo, Brazil. [Gandolfi, D.; Guenther, E.; Hatzes, A.; Stecklum, B.; Wuchterl, G.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Gillon, M.] Univ Liege, B-1 Liege, Belgium. [Hidas, M.; Lister, T.; Street, R.] Las Cumbres Observ Global Telescope Network Inc, Santa Barbara, CA 93117 USA. [Hidas, M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Mazeh, T.; Shporer, A.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Mura, A.] CNR, Inst Fis Spacio Interplanetario, Rome, Italy. [Rauer, H.] TU Berlin, Ctr Astron & Astrophys, D-10623 Berlin, Germany. RP Lammer, H (reprint author), Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria. RI Alonso, Roi/D-8799-2014; Tingley, Brandon/E-5146-2014; Ferraz-Mello, Sylvio/B-7529-2013; OI Gandolfi, Davide/0000-0001-8627-9628; Alonso, Roi/0000-0001-8462-8126; Tingley, Brandon/0000-0003-4483-2661; Barbieri, Mauro/0000-0001-8362-3462; Carone, Ludmila/0000-0001-9355-3752; Mura, Alessandro/0000-0002-4552-4292; Ciardi, David/0000-0002-5741-3047 FU Austrian Ministry bm:bwk; ASA FX H. Lammer, M. Fridlund, J. Schneider and A. Mura acknowledge the International Space Science Institute (ISSI; Bern, Switzerland) and the ISSI team "Evolution of Exoplanet Atmospheres and their Characterization". H. Lammer and A. Mura also acknowledge fruitful discussions during various meetings related to the Europlanet N2 activities as well as within the N2 discipline working groups WG 4 and WG5. H. Lammer, R. Dvorak, J. Hasiba, H. Ottacher and M. Steller also thank the Austrian Ministry bm:bwk and ASA for funding the CoRoT project. NR 23 TC 3 Z9 3 U1 0 U2 3 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 0038-0946 J9 SOLAR SYST RES+ JI Solar Syst. Res. PD DEC PY 2010 VL 44 IS 6 BP 520 EP 526 DI 10.1134/S0038094610060055 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 691QS UT WOS:000285096500005 ER PT J AU Foster, AR Smith, RK Brickhouse, NS Kallman, TR Witthoeft, MC AF Foster, A. R. Smith, R. K. Brickhouse, N. S. Kallman, T. R. Witthoeft, M. C. TI The Challenges of Plasma Modeling: Current Status and Future Plans SO SPACE SCIENCE REVIEWS LA English DT Review DE Atomic data; X-ray astronomy; Atomic processes ID HELIUM-LIKE IONS; LINE DIAGNOSTICS; ATOMIC DATABASE; CHARGE-TRANSFER; RECOMBINATION; EMISSION; SCATTERING; HYDROGEN; ELEMENTS; SPECTRA AB Successfully modeling X-ray emission from astrophysical plasmas requires a wide range of atomic data to be rapidly accessible by modeling codes, enabling calculation of synthetic spectra for fitting with observations. Over many years the astrophysical databases have roughly kept pace with the advances in detector and spectrometer technology. We outline here the basic atomic processes contributing to the emission from different types of plasmas and briefly touch on the difference between the methods used to calculate this data. We then discuss in more detail the different issues addressed by atomic databases in regards to what data to store and how to make it accessible. Finally, the question of the effect of uncertainties in atomic data is explored, as a reminder to observers that atomic data is not known to infinite precision, and should not be treated as such. C1 [Foster, A. R.; Smith, R. K.; Brickhouse, N. S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kallman, T. R.; Witthoeft, M. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Smith, RK (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM afoster@cfa.harvard.edu; rsmith@cfa.harvard.edu OI Brickhouse, Nancy/0000-0002-8704-4473 NR 38 TC 14 Z9 14 U1 2 U2 4 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 DEC PY 2010 VL 157 IS 1-4 BP 135 EP 154 DI 10.1007/s11214-010-9732-1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 732GE UT WOS:000288172200009 ER PT J AU Kallman, TR AF Kallman, T. R. TI Modeling of Photoionized Plasmas SO SPACE SCIENCE REVIEWS LA English DT Review DE X-ray spectroscopy; Modeling ID ACTIVE GALACTIC NUCLEI; X-RAY-ABSORPTION; DIELECTRONIC RECOMBINATION; HYDRODYNAMICAL MODEL; THERMAL-INSTABILITY; EMISSION-LINES; TORUS WIND; K-LINES; IRON; FEATURES AB In this paper I review the motivation and current status of modeling of plasmas exposed to strong radiation fields, as it applies to the study of cosmic X-ray sources. This includes some of the astrophysical issues which can be addressed, the ingredients for the models, the current computational tools, the limitations imposed by currently available atomic data, and the validity of some of the standard assumptions. I will also discuss ideas for the future: challenges associated with future missions, opportunities presented by improved computers, and goals for atomic data collection. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kallman, TR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Timothy.R.Kallman@nasa.gov NR 40 TC 16 Z9 16 U1 0 U2 2 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 DEC PY 2010 VL 157 IS 1-4 BP 177 EP 191 DI 10.1007/s11214-010-9711-6 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 732GE UT WOS:000288172200012 ER PT J AU Medina, M Sherry, L Feary, M AF Medina, Maricel Sherry, Lance Feary, Michael TI Automation for task analysis of next generation air traffic management systems SO TRANSPORTATION RESEARCH PART C-EMERGING TECHNOLOGIES LA English DT Article; Proceedings Paper CT Internation Symposium on Transportation Simulation CY AUG, 2008 CL Gold Coast, AUSTRALIA DE Human-computer interaction; Usability analysis; Task analysis; Probability of failure-to-complete a task; Trials-to-mastery AB The increasing span of control of Air Traffic Control enterprise automation (e.g. Flight Schedule Monitor, Departure Flow Management), along with lean-processes and pay-for-performance business models, has placed increased emphasis on operator training time and error rates. There are two traditional approaches to the design of human-computer interaction (HCI) to minimize training time and reduce error rates: (1) experimental user testing provides the most accurate assessment of training time and error rates, but occurs too late in the development cycle and is cost prohibitive, (2) manual review methods (e.g. cognitive walkthrough) can be used earlier in the development cycle, but suffer from poor accuracy and poor inter-rater reliability. Recent development of "affordable" human performance models provide the basis for the automation of task analysis and HCI design to obtain low cost, accurate, estimates of training time and error rates early in the development cycle. This paper describes a usability/HCI analysis tool that this intended for use by design engineers in the course of their software engineering duties. The tool computes estimates of trials-to-mastery (i.e. time to competence for training) and the probability of failure-to-complete for each task. The HCI required to complete a task on the automation under development is entered into the web-based tool via a form. Assessments of the salience of visual cues to prompt operator actions for the proposed design are used to compute training time and error rates. The web-based tool enables designers in multiple locations to review and contribute to the design. An example analysis is provided along with a discussion of the limitations of the tool and directions for future research. (c) 2010 Elsevier Ltd. All rights reserved. C1 [Medina, Maricel; Sherry, Lance] George Mason Univ, Ctr Air Transportat Syst Res, Fairfax, VA 22030 USA. [Feary, Michael] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Medina, M (reprint author), George Mason Univ, Ctr Air Transportat Syst Res, Fairfax, VA 22030 USA. EM mmedinam@gmu.edu; lsherry@gmu.edu; Michael.feary@nasa.gov NR 27 TC 6 Z9 6 U1 1 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0968-090X J9 TRANSPORT RES C-EMER JI Transp. Res. Pt. C-Emerg. Technol. PD DEC PY 2010 VL 18 IS 6 SI SI BP 921 EP 929 DI 10.1016/j.trc.2010.03.006 PG 9 WC Transportation Science & Technology SC Transportation GA 652HD UT WOS:000281993500009 ER PT J AU Kirk, BS AF Kirk, Benjamin S. TI Adiabatic shock capturing in perfect gas hypersonic flows SO INTERNATIONAL JOURNAL FOR NUMERICAL METHODS IN FLUIDS LA English DT Article DE SUPG; finite element; adiabatic compressible flows; shock capturing; adiabatic perfect gas; hypersonic flows ID COMPUTATIONAL FLUID-DYNAMICS; FINITE-ELEMENT FORMULATION; NAVIER-STOKES EQUATIONS; ADVECTIVE-DIFFUSIVE SYSTEMS; COMPRESSIBLE EULER; OPERATOR AB This paper considers the streamline-upwind Petrov/Galerkin (SUPG) method applied to the compressible Euler and Navier-Stokes equations in conservation-variable form. The spatial discretization, including a modified approach for interpolating the inviscid flux terms in the SUPG finite element formulation, is briefly reviewed. Of particular interest is the behavior of the shock-capturing operator, which is required to regularize the scheme in the presence of strong, shock-induced gradients. A standard shock-capturing operator that has been widely used in previous studies by several authors is presented and discussed. Specific modifications are then made to this standard operator that is designed to produce a more physically consistent discretization in the presence of strong shock waves. The actual implementation of the term in a finite-dimensional approximation is also discussed. The behavior of the standard and modified scheme is then compared for several supersonic/hypersonic flows. The modified shock-capturing operator is found to preserve enthalpy in the inviscid portion of the flowfield substantially better than the standard operator. Published in 2009 by John Wiley & Sons, Ltd. C1 [Kirk, Benjamin S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Kirk, BS (reprint author), Mail Code EG3,2101 NASA Pkwy, Houston, TX 77058 USA. EM benjamin.kirk@nasa.gov NR 32 TC 2 Z9 2 U1 0 U2 3 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0271-2091 J9 INT J NUMER METH FL JI Int. J. Numer. Methods Fluids PD NOV 30 PY 2010 VL 64 IS 9 BP 1041 EP 1062 DI 10.1002/fld.2195 PG 22 WC Computer Science, Interdisciplinary Applications; Mathematics, Interdisciplinary Applications; Mechanics; Physics, Fluids & Plasmas SC Computer Science; Mathematics; Mechanics; Physics GA 680BC UT WOS:000284205200005 ER PT J AU Geissler, PE Sullivan, R Golombek, M Johnson, JR Herkenhoff, K Bridges, N Vaughan, A Maki, J Parker, T Bell, J AF Geissler, P. E. Sullivan, R. Golombek, M. Johnson, J. R. Herkenhoff, K. Bridges, N. Vaughan, A. Maki, J. Parker, T. Bell, J. TI Gone with the wind: Eolian erasure of the Mars Rover tracks SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MERIDIANI-PLANUM; LANDING SITE; CRATER AB The wheel tracks left by the Mars Exploration Rovers Spirit and Opportunity are unique artificial markings on the surface of Mars. The tracks stretch several kilometers across diverse terrain in two widely separated regions of the planet. The initial appearance and characteristics of the tracks were well documented by the science and navigation cameras aboard the vehicles at the time the tracks were formed. Orbital observations by Mars Global Surveyor and Mars Reconnaissance Orbiter document the erasure of the tracks over a period of more than 2 Mars years. Close-up examinations of track crossings, where the rovers encountered tracks made hundreds of Martian solar days earlier, provide insights into the mechanisms and time scales of eolian alteration on Mars. These observations suggest that fallout of atmospheric dust plays only a minor role in obscuring rover tracks over time. Instead, track erasure is dominated by sediment that is transported by surface winds. Both deposition and erosion act to erase the rover tracks. The length scales for eolian sediment transport are hundreds of meters at least, much larger than the size of the tracks. Gradual processes such as dust devils and sand saltation have minor effects that can nonetheless erase rover tracks over long time periods. However, short-lived strong wind events associated with seasonal dust storms have much more pronounced effects, significantly altering the tracks on time scales of days. These episodic strong winds tend to occur annually during the perihelion season. The time scale for track erasure is typically only 1 Martian year. C1 [Geissler, P. E.; Johnson, J. R.; Herkenhoff, K.; Vaughan, A.] US Geol Survey, Flagstaff, AZ 86001 USA. [Sullivan, R.; Bell, J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Golombek, M.; Maki, J.; Parker, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bridges, N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Geissler, PE (reprint author), US Geol Survey, Flagstaff, AZ 86001 USA. EM pgeissler@usgs.gov; rjs33@cornell.edu; mgolombek@jpl.nasa.gov; jrjohnson@usgs.gov; kherkenhoff@usgs.gov; nathan.bridges@jhuapl.edu; afvaughan@usgs.gov; timothy.j.parker@jpl.nasa.gov; jfb8@cornell.edu RI Johnson, Jeffrey/F-3972-2015 NR 25 TC 17 Z9 17 U1 0 U2 12 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 NOV 30 PY 2010 VL 115 AR E00F11 DI 10.1029/2010JE003674 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 690QO UT WOS:000285019500001 ER EF