FN Thomson Reuters Web of Science™ VR 1.0 PT S AU DiPirro, M Tuttle, J Jackson, M Canavan, E Warner, B Shirron, P AF DiPirro, M. Tuttle, J. Jackson, M. Canavan, E. Warner, B. Shirron, P. BE Weisend, JG Barclay, J Breon, S Demko, J DiPirro, M Kelley, JP Kittel, P Klebaner, A Lock, J Maddocks, J Peterson, T Pfotenhauer, J Rowe, A VanSciver, S Zeller, A TI Progress on a 4 K to 10 K continuously operating adiabatic demagnetization refrigerator SO Advances in Cryogenic Engineering, Vols 51A and B SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Cryogenic Engineering Conference 2005 CY AUG 29-SEP 02, 2005 CL Keystone, CO SP US DOE, Off High Energy Phys, Fermi Natl Accele Lab, Los Alamos Natl Lab, Off Naval Res & Naval Res Lab, Oak Ridge Natl Lab DE magnetic refrigeration; space telescopes; magnetic shielding AB An adiabatic demagnetization refrigerator (ADR) is under development for use in cooling relatively large loads (10-100 mW) at 4 K and rejecting that heat to a cryocooler operating at 10 K. ADRs can operate in this temperature range with an efficiency of 75% of Carnot, saving as much as 2/3 of the required overall input power. In addition this ADR can provide cooling down to 0.4 K. The ADR magnet consists of 8 short coils wired in series and arranged in a toroid to provide self-shielding of its magnetic field. Eliminating passive or active shields saves 30% of the mass of the system. The average field is 3 Tesla using 5 amps. In the first model the coils are wound with ordinary NbTi superconducting wire and operated at 4 K. A second version will then use fine Nb3Sn wire to provide complete 10 K operation. As a refrigerant for this temperature range we are using readily available gadolinium gallium garnet (GGG) crystals, which provide suitable performance. In the future we will switch to either GdLiF4 or GdF3, which have 13% or 30%, respectively, more cooling power per volume than GGG. We use gas gap heat switches to alternately connect the toroid to the cold load and the warm heat sink. A small continuous stage maintains the cold end at 4 K while the main toroid is recycled. Data on toroid magnet performance with respect to central field vs. current and fringing field vs. current are given. Data on the transient heating due to hysteresis losses within the superconductor are also presented. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP DiPirro, M (reprint author), NASA, Goddard Space Flight Ctr, Code 552, Greenbelt, MD 20771 USA. NR 6 TC 1 Z9 1 U1 5 U2 8 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0317-1 J9 AIP CONF PROC PY 2006 VL 823 BP 969 EP 976 PG 8 WC Thermodynamics; Physics, Multidisciplinary SC Thermodynamics; Physics GA BEL54 UT WOS:000237990200116 ER PT S AU Fesmire, JE Augustynowicz, SD Nagy, ZF Sojourner, SJ Morris, DL AF Fesmire, J. E. Augustynowicz, S. D. Nagy, Z. F. Sojourner, S. J. Morris, D. L. BE Weisend, JG Barclay, J Breon, S Demko, J DiPirro, M Kelley, JP Kittel, P Klebaner, A Lock, J Maddocks, J Peterson, T Pfotenhauer, J Rowe, A VanSciver, S Zeller, A TI Vibration and thermal cycling effects on bulk-fill insulation materials for cryogenic tanks SO Advances in Cryogenic Engineering, Vols 51A and B SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Cryogenic Engineering Conference 2005 CY AUG 29-SEP 02, 2005 CL Keystone, CO SP US DOE, Off High Energy Phys, Fermi Natl Accele Lab, Los Alamos Natl Lab, Off Naval Res & Naval Res Lab, Oak Ridge Natl Lab DE cryogenic tanks; thermal insulation; granular materials; mechanical compaction; vibration; performance testing AB Large-scale (1,000,000 liters or more) cryogenic storage tanks are typically perlite-insulated double-walled vessels. Associated problems with perlite, such as mechanical compaction and settling, could be greatly reduced by using newer bulk-fill materials such as glass bubbles or aerogel beads. Using the newer materials should translate to lower life cycle costs and improved system reliability. NASA Kennedy Space Center is leveraging its experience in the areas of materials development, insulation testing, and cryogenic systems design to develop an insulation retrofit option that will meet both industry and NASA requirements. A custom 10-liter dewar test apparatus, developed by the KSC Cryogenics Test Laboratory, was used to determine the vibration and thermal cycling effects on different bulk-fill insulation materials for cryogenic tanks. The testing included liquid-nitrogen boiloff testing and thermal cycling (with vibration) of a number of test dewars. Test results show that glass bubbles have better thermal performance and less mechanical compaction compared to perlite powder. The higher cost of the bulk material should be offset by reduced commodity loss from boiloff and improvements in material handling, evacuation, and vacuum retention. The long-term problem with settling and compaction of perlite should also be eliminated. Aerogel beads are superior for the no-vacuum condition and can now be considered in some applications. Further studies on large-scale systems are presently being pursued. C1 NASA, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA. RP Fesmire, JE (reprint author), NASA, Kennedy Space Ctr, YA-C2-T, Kennedy Space Ctr, FL 32899 USA. NR 6 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 0-7354-0317-1 J9 AIP CONF PROC PY 2006 VL 823 BP 1359 EP 1366 PG 8 WC Thermodynamics; Physics, Multidisciplinary SC Thermodynamics; Physics GA BEL54 UT WOS:000237990201039 ER PT S AU Zhang, BX Chui, TC AF Zhang, Burt. X. Chui, Talso. C. BE Weisend, JG Barclay, J Breon, S Demko, J DiPirro, M Kelley, JP Kittel, P Klebaner, A Lock, J Maddocks, J Peterson, T Pfotenhauer, J Rowe, A VanSciver, S Zeller, A TI Low temperature engineering applied to lunar in-situ resource utilization SO Advances in Cryogenic Engineering, Vols 51A and B SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Cryogenic Engineering Conference 2005 CY AUG 29-SEP 02, 2005 CL Keystone, CO SP US DOE, Off High Energy Phys, Fermi Natl Accele Lab, Los Alamos Natl Lab, Off Naval Res & Naval Res Lab, Oak Ridge Natl Lab DE lunar; cryogenic; regolith; thermal radiator AB In support of NASA's Exploration Mission low-temperature scientists and engineers have investigated the process of extracting volatile materials from the lunar regolith, their purification/liquefaction, and storage. Volatiles such as O-2, N-2, He and water can be used to support human habitation, while H-2 and O-2 can be used as rocket fuel. Using a sorption pump, passive thermal radiators, temperature control, and a small number of storage vessels and valves, a purification and storage system can be designed to operate inside a permanently shadowed polar crater where volatiles are expected to be most abundant. The basic approach can be used as the basis for a small experiment on a prospecting mission, which will serve as a proof of concept for a much bigger cryogenic fluids facility to support NASA's human exploration effort. A similar design with sufficient radiation shielding can be operated on the Moon's surface. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zhang, BX (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0317-1 J9 AIP CONF PROC PY 2006 VL 823 BP 1523 EP 1529 PG 7 WC Thermodynamics; Physics, Multidisciplinary SC Thermodynamics; Physics GA BEL54 UT WOS:000237990201059 ER PT S AU Rodriguez, JI Collins, SA Na-Nakornpanom, A Johnson, DL AF Rodriguez, J. I. Collins, S. A. Na-Nakornpanom, A. Johnson, D. L. BE Weisend, JG Barclay, J Breon, S Demko, J DiPirro, M Kelley, JP Kittel, P Klebaner, A Lock, J Maddocks, J Peterson, T Pfotenhauer, J Rowe, A VanSciver, S Zeller, A TI On-orbit performance of the TES pulse tube coolers and instrument - A first year in space SO Advances in Cryogenic Engineering, Vols 51A and B SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Cryogenic Engineering Conference 2005 CY AUG 29-SEP 02, 2005 CL Keystone, CO SP US DOE, Off High Energy Phys, Fermi Natl Accele Lab, Los Alamos Natl Lab, Off Naval Res & Naval Res Lab, Oak Ridge Natl Lab DE tES; EOS; Aura; cryocoolers; pulse tube; passive cooler; contamination; cryodeposit; MLI; remote sensing; interferometer AB Launched on NASA's Aura spacecraft on July 15, 2004, JPL's Tropospheric Emission Spectrometer (TES) instrument has completed a successful first year in space and captured a number of important lessons. The instrument contains four focal plane arrays in two separate housings cooled to 65 K by a pair of NGST pulse tube cryocoolers. The instrument includes a two-stage passive cooler to cool the optical bench to 180 K. The cryocooler system design is tightly coupled with the overall thermal control design to maximize performance. Soon after cooling the optical bench and focal planes to their operating temperatures on August 20, 2004, ice contamination of the focal planes led to the need of a decontamination cycle. Ice buildup of cryogenic surfaces led to increased cryocooler heat loads. After six months of successful science operations, plans were developed to increase the optics temperature to 187 K to improve the interferometer optical alignment and obtain higher quality science data. The plan is in place and will be implemented in the near future. This paper provides a general overview of the cryogenic system design and reviews the instrument cryogenic performance over the past year. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rodriguez, JI (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NR 7 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 0-7354-0317-1 J9 AIP CONF PROC PY 2006 VL 823 BP 1937 EP 1944 PG 8 WC Thermodynamics; Physics, Multidisciplinary SC Thermodynamics; Physics GA BEL54 UT WOS:000237990201108 ER PT S AU Schumann, J Liu, Y AF Schumann, Johann Liu, Yan BE Wang, J Yi, Z Zurada, JM Lu, BL Yin, H TI Performance estimation of a neural network-based controller SO ADVANCES IN NEURAL NETWORKS - ISNN 2006, PT 2, PROCEEDINGS SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 3rd International Symposium on Neural Networks (ISNN 2006) CY MAY 28-31, 2006 CL Chengdu, PEOPLES R CHINA SP Univ Electr Sci & Technol China, Chinese Univ Hong Kong, Asia Pacific Neural Network Assembly, European Neural Network Soc, IEEE Circuits & Syst Soc, IEEE Computat Intelligence Soc, Int Neural Network Soc, Natl Nat Sci Fdn China, KC Wong Educ Fdn Hong Kong AB Biologically inspired soft computing paradigms such as neural networks are popular learning models adopted in adaptive control systems for their ability to cope with a changing environment. However, continual changes induce uncertainty that limits the applicability of conventional validation techniques to assure a reliable system performance. In this paper, we present a dynamic approach to estimate the performance of two types of neural networks employed in an adaptive flight controller: the validity index for the outputs of a Dynamic Cell Structure (DCS) network and confidence levels for the outputs of a Sigma-Pi (or MLP) network. Both tools provide statistical inference of the neural network predictions and an estimate of the current performance of the network. We further evaluate how the quality of each parameter of the network (e.g., weight) influences the output of the network by defining a metric for parameter sensitivity and parameter confidence for DCS and Sigma-Pi networks. Experimental results on the NASA F-15 flight control system demonstrate that our techniques effectively evaluate the network performance and provide validation inferences in a real-time manner. C1 NASA Ames, RIACS, Moffett Field, CA 94035 USA. Motorola Labs, Schaumburg, IL 60193 USA. RP Schumann, J (reprint author), NASA Ames, RIACS, Moffett Field, CA 94035 USA. EM schumann@email.arc.nasa.gov; yanliu@motorola.com NR 18 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-34437-3 J9 LECT NOTES COMPUT SC PY 2006 VL 3972 BP 981 EP 990 PG 10 WC Computer Science, Artificial Intelligence; Computer Science, Theory & Methods SC Computer Science GA BET84 UT WOS:000239483000145 ER PT S AU Qian, T Li, XK Ayhan, B Xu, R Kwan, C Griffin, T AF Qian, Tao Li, Xiaokun Ayhan, Bulent Xu, Roger Kwan, Chiman Griffin, Tim BE Wang, J Yi, Z Zurada, JM Lu, BL Yin, H TI Application of support vector machines to vapor detection and classification for environmental monitoring of spacecraft SO ADVANCES IN NEURAL NETWORKS - ISNN 2006, PT 3, PROCEEDINGS SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 3rd International Symposium on Neural Networks (ISNN 2006) CY MAY 28-31, 2006 CL Chengdu, PEOPLES R CHINA SP Univ Electr Sci & Technol China, Chinese Univ Hong Kong, Asia Pacific Neural Network Assembly, European Neural Network Soc, IEEE Circuits & Syst Soc, IEEE Computat Intelligence Soc, Int Neural Network Soc, Natl Nat Sci Fdn China, KC Wong Educ Fdn Hong Kong AB Electronic noses (E-nose) have gained popularity in various applications such as food inspection, cosmetics quality control [1], toxic vapor detection to counter terrorism, detection of Improvised Explosive Devices (IED), narcotics detection, etc. In the paper, we summarized our results on the application of Support Vector Machines (SVM) to gas detection and classification using E-nose. First, based on experimental data from Jet Propulsion Lab. (JPL), we created three different data sets based on different pre-processing techniques. Second, we used SVM to detect gas sample data from non-gas background data, and used three sensor selection methods to improve the detection rate. We were able to achieve 85% correct detection of gases. Third, SVM gas classifier was developed to classify 15 different single gases and mixtures. Different sensor selection methods were applied and FSS & BSS feature selection method yielded the best performance. C1 Intelligent Automat Inc, Rockville, MD 20855 USA. NASA, Kennedy Space Ctr, TX USA. RP Qian, T (reprint author), Intelligent Automat Inc, 15400 Calhoun Dr,Suite 400, Rockville, MD 20855 USA. EM tqian@i-a-i.com; xli@i-a-i.com; bayhan@i-a-i.com; hgxu@i-a-i.com; ckwan@i-a-i.com NR 8 TC 1 Z9 1 U1 1 U2 2 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-34482-9 J9 LECT NOTES COMPUT SC PY 2006 VL 3973 BP 1216 EP 1222 PG 7 WC Computer Science, Artificial Intelligence; Computer Science, Theory & Methods SC Computer Science GA BET87 UT WOS:000239485300177 ER PT J AU Potter, AE Plymate, C Keller, C Killen, RM Morgan, TH AF Potter, A. E. Plymate, C. Keller, C. Killen, R. M. Morgan, T. H. TI Mapping sodium distribution in the exosphere of Mercury with tip-tilt image stabilization SO ADVANCES IN SPACE RESEARCH LA English DT Article DE mercury; sodium; exosphere; tip-tilt; image stabilizer; atmospheric models; exospheric models ID SOLAR-WIND; ATMOSPHERE; MAGNETOSPHERE; DISCOVERY; POTASSIUM; IONS; NA AB Mapping the sodium emission about Mercury is a difficult observational problem, since Mercury is seen either against the bright daytime sky, or against a dark sky at very high air masses. The distribution of sodium emission over the surface of Mercury is non-uniform, and changes over time. These effects give clues to the processes that produce the sodium and control its distribution, so that improved mapping of sodium emissions over the Mercury surface will help clarify their relative importance. We have adapted an image stabilizer utilizing a piezoelectric driven tip-tilt correction mirror for daytime spectral imaging of Mercury. The image stabilizer, which was originally developed for solar observations at the McMath-Pierce solar telescope, results in a noticeable improvement in spatial resolution of our Mercury sodium images. In this paper we give initial results from use of the tip-tilt image stabilizer for observations of Mercury's sodium exosphere. Further systematic observations and improvements are planned for the image stabilizer system, as well as experimental observations with a low-order adaptive optics system incorporating a commercially available 37-actuator deformable mirror. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Potter, A. E.; Plymate, C.; Keller, C.] Natl Solar Observ, Tucson Div, Tucson, AZ 85726 USA. [Killen, R. M.] Univ Maryland, College Pk, MD 20742 USA. [Morgan, T. H.] NASA Headquarters, Washington, DC USA. RP Potter, AE (reprint author), Natl Solar Observ, Tucson Div, POB 26732,950 N Cherry Ave, Tucson, AZ 85726 USA. EM apotter@noao.edu RI Killen, Rosemary/E-7127-2012; Morgan, Thomas/I-5943-2013 NR 22 TC 3 Z9 3 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 4 BP 599 EP 603 DI 10.1016/j.asr.2005.06.062 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FH UT WOS:000202988100008 ER PT J AU Baumjohann, W Matsuoka, A Glassmeier, KH Russell, CT Nagai, T Hoshino, M Nakagawa, T Balogh, A Slavin, JA Nakamura, R Magnes, W AF Baumjohann, W. Matsuoka, A. Glassmeier, K. H. Russell, C. T. Nagai, T. Hoshino, M. Nakagawa, T. Balogh, A. Slavin, J. A. Nakamura, R. Magnes, W. TI The magnetosphere of Mercury and its solar wind environment: Open issues and scientific questions SO ADVANCES IN SPACE RESEARCH LA English DT Article DE mercury; magnetosphere; shocks; reconnection; alfven waves; solar wind ID LION ROARS; ULF WAVES; ACCELERATION; SHOCKS; SPEED; ELECTRONS; SUBSTORMS; EXOSPHERE; CURRENTS; SURFACE AB The scant data from the historic Mariner-10 flybys indicate that the Hermean and terrestrial magnetospheres have many similarities. However, Mercury's differences, e.g., the absence of an ionosphere, high sodium content, small dimension, and the stronger forcing by the solar wind, make it likely that processes of lesser importance at Earth play a more major role at Mercury. In addition, the proximity of Mercury in time and space to the onset of solar events, places the magnetosphere in a heretofore unexplored environment. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Baumjohann, W.; Nakamura, R.; Magnes, W.] Akad Wissensch, Inst Weltraumforsch, A-8042 Graz, Austria. [Matsuoka, A.] Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Glassmeier, K. H.] Inst Geophys & Extraterrestr Phys, D-38106 Braunschweig, Germany. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Nagai, T.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Tokyo 1528551, Japan. [Hoshino, M.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. [Nakagawa, T.] Tohoku Inst Technol, Sendai, Miyagi 9828577, Japan. [Balogh, A.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Slavin, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Baumjohann, W (reprint author), Akad Wissensch, Inst Weltraumforsch, Schmiedlstr 6, A-8042 Graz, Austria. EM baumjohann@oeaw.ac.at RI Nakamura, Rumi/I-7712-2013; Baumjohann, Wolfgang/A-1012-2010; Slavin, James/H-3170-2012 OI Nakamura, Rumi/0000-0002-2620-9211; Baumjohann, Wolfgang/0000-0001-6271-0110; Slavin, James/0000-0002-9206-724X NR 34 TC 18 Z9 18 U1 0 U2 0 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. PY 2006 VL 38 IS 4 BP 604 EP 609 DI 10.1016/j.asr.2005.05.117 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FH UT WOS:000202988100009 ER PT J AU Taylor, FW Calcutt, SB Read, PL Lewis, SR McCleese, DJ Schofield, JT Zurek, RW AF Taylor, F. W. Calcutt, S. B. Read, P. L. Lewis, S. R. McCleese, D. J. Schofield, J. T. Zurek, R. W. TI Atmospheric temperature sounding on Mars, and the climate sounder on the 2005 reconnaissance orbiter SO ADVANCES IN SPACE RESEARCH LA English DT Article DE mars; atmosphere; climate AB Detailed measurements of the vertical profiles of atmospheric temperature, water vapour, dust and condensates in the Martian atmosphere are needed to characterize the present-day Martian climate and to understand the intricately related processes upon which it depends. Among the most important of these are accurate and extensive temperature measurements. Progress to date, key problems still to be addressed and upcoming new approaches to the measurement task are briefly reviewed, and expectations for the Mars Climate Sounder experiment on the 2005 Mars Reconnaissance Orbiter are described. Some even more advanced methods for temperature, humidity and condensate sounding in the decade beyond MCS/MRO, and promising approaches to achieving these are also considered. (c) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 [Taylor, F. W.; Calcutt, S. B.; Read, P. L.; Lewis, S. R.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [McCleese, D. J.; Schofield, J. T.; Zurek, R. W.] Jet Propuls Lab, Pasadena, CA USA. RP Taylor, FW (reprint author), Univ Oxford, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England. EM f.taylor@physics.ox.ac.uk NR 8 TC 3 Z9 3 U1 0 U2 0 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. PY 2006 VL 38 IS 4 BP 713 EP 717 DI 10.1016/j.asr.2005.03.072 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FH UT WOS:000202988100025 ER PT J AU Kwon, O Sartor, M Tomlinson, CR Millard, RW Olah, ME Sankovic, JM Banerjee, RK AF Kwon, Ohwon Sartor, Maureen Tomlinson, Craig R. Millard, Ronald W. Olah, Mark E. Sankovic, John M. Banerjee, Rupak K. TI Effect of simulated microgravity on oxidation-sensitive gene expression in PC12 cells SO ADVANCES IN SPACE RESEARCH LA English DT Article DE rotating wall vessel; simulated microgravity; gene expression; microarray ID FALSE DISCOVERY RATE; NERVE GROWTH-FACTOR; MOLECULAR MECHANISMS; MICROARRAY ANALYSIS; CDNA; WALL; HYPOXIA; CULTURE; DIFFERENTIATION; TRANSCRIPTION AB Oxygen utilization by and oxygen dependence of cellular processes may be different in biological systems that are exposed to microgravity (micro-g). A baseline in which cellular changes in oxygen sensitive molecular processes occur during micro-g conditions would be important to pursue this question. The objective of this research is to analyze oxidation-sensitive gene expression in a model cell line [rat pheochromocytoma (PC 12)] under simulated micro-g conditions. The PC 12 cell line is well characterized in its response to oxygen, and is widely recognized as a sensitive model for studying the responses of oxygen-sensitive molecular and cellular processes. This study uses the rotating wall vessel bioreactor (RAW) designed at NASA to simulate micro-g. Gene expression in PC 12 cells in response to micro-g was analyzed by DNA microarray technology. The microarray analysis of PC 12 cells cultured for 4 days under simulated micro-g under standardized oxygen environment conditions revealed more than 100 genes whose expression levels were changed at least twofold (up-regulation of 65 genes and down-regulation of 39 genes) compared with those from cells in the unit gravity (unit-g) control. This study observed that genes involved in the oxidoreductase activity category were most significantly differentially expressed under micro-g conditions. Also, known oxidation-sensitive transcription factors such as hypoxia-inducible factor-2 alpha, c-myc, and the peroxisome proliferator-activated receptor-gamma were changed significantly. Our initial results from the gene expression microarray studies may provide a context in which to evaluate the effect of varying oxygen environments on the background of differential gene regulation of biological processes under variable gravity conditions. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Kwon, Ohwon; Banerjee, Rupak K.] Univ Cincinnati, Dept Mech Engn, Cincinnati, OH 45221 USA. [Sartor, Maureen; Tomlinson, Craig R.] Univ Cincinnati, Dept Environm Hlth, Cincinnati, OH 45221 USA. [Sartor, Maureen] Univ Cincinnati, Ctr Environm Genet, Div Biostat & Epidemiol, Cincinnati, OH 45221 USA. [Tomlinson, Craig R.] Univ Cincinnati, Ctr Environm Genet, Div Environm Genet & Mol Toxicol, Cincinnati, OH 45221 USA. [Millard, Ronald W.; Olah, Mark E.] Univ Cincinnati, Dept Pharmacol & Cell Biophys, Cincinnati, OH 45221 USA. [Sankovic, John M.] NASA, Glen Res Ctr, Micrograv Sci Div, Cleveland, OH 44135 USA. [Banerjee, Rupak K.] Univ Cincinnati, Dept Biomed Engn, Cincinnati, OH 45221 USA. RP Banerjee, RK (reprint author), Univ Cincinnati, Dept Mech Engn, Cincinnati, OH 45221 USA. EM rupak.banerjee@uc.edu RI Tomlinson, Craig/F-1319-2017 NR 39 TC 0 Z9 0 U1 1 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 6 BP 1168 EP 1176 DI 10.1016/j.asr.2006.02.059 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FJ UT WOS:000202988300023 ER PT J AU Abyzov, SS Duxbury, NS Bobin, NE Fukuchi, M Hoover, RB Kanda, H Mitskevich, IN Mulyukin, AL Naganuma, T Poglazova, MN Ivanov, MV AF Abyzov, S. S. Duxbury, N. S. Bobin, N. E. Fukuchi, M. Hoover, R. B. Kanda, H. Mitskevich, I. N. Mulyukin, A. L. Naganuma, T. Poglazova, M. N. Ivanov, M. V. TI Super-long anabiosis of ancient microorganisms in ice and terrestrial models for development of methods to search for life on Mars, Europa and other planetary bodies SO ADVANCES IN SPACE RESEARCH LA English DT Article DE super-long anabiosis; Antarctic ice sheet; viable microorganisms; terrestrial analogs of martian habitats; Europa; icy satellites; Comets ID SPORE-FORMING BACTERIA; LAKE VOSTOK; ENVIRONMENT; PERMAFROST; STARVATION; CLATHRATE; SURVIVAL; GROWTH; VIBRIO; CELLS AB Successful missions to Mars, Europe and other bodies of the Solar system have created a prerequisite to search for extraterrestrial life. The first attempts of microbial life detection on the Martian surface by the Viking landed missions gave no biological results. Microbiological investigations of the Martian subsurface ground ice layers seem to be more promising. It is well substantiated to consider the Antarctic ice sheet and the Antarctic and Arctic permafrost as terrestrial analogues of Martian habitats. The results of our long-standing microbiological studies of the Antarctic ice would provide the basis for detection of viable microbial cells on Mars. Our microbiological investigations of the deepest and thus most ancient strata of the Antarctic ice sheet for the first time gave evidence for the natural phenomenon of long-term anabiosis (preservation of viability and vitality for millennia years). A combination of classical microbiological methods, epifluorescence microscopy, SEM, TEM, molecular diagnostics, radioisotope labeling and other techniques made it possible for us to obtain convincing proof of the presence of pro- and eukaryotes in the Antarctic ice sheet. In this communication, we will review and discuss some critical issues related to the detection of viable microorganisms in cold terrestrial environments with regard to future searches for microbial life and/or its biological signatures on extraterrestrial objects. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Abyzov, S. S.; Mitskevich, I. N.; Mulyukin, A. L.; Poglazova, M. N.; Ivanov, M. V.] Russian Acad Sci, Wingradsky Inst Microbiol, Moscow 117312, Russia. [Duxbury, N. S.] CALTECH, JPL, Pasadena, CA 91125 USA. [Bobin, N. E.] St Petersburg Min Inst, St Petersburg 199026, Russia. [Bobin, N. E.] Natl Inst Polar Res, Tokyo, Japan. [Hoover, R. B.] Dept Space Sci, Huntsville, AL 35805 USA. [Naganuma, T.] Hiroshima Univ, Sch Biosphere Sci, Higashihiroshima 724, Japan. RP Mulyukin, AL (reprint author), Russian Acad Sci, Wingradsky Inst Microbiol, Pr 60 Letiya Oktyabrya 7-2, Moscow 117312, Russia. EM abyzov@inmi.host.ru; spmi@mail.wplus.net; fukuchi@nipr.ac.jp; Richard.Hoover@msfc.nasa.gov; andylm@rambler.ru; takn@hiroshima-u.ac.jp NR 44 TC 1 Z9 1 U1 2 U2 10 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. PY 2006 VL 38 IS 6 BP 1191 EP 1197 DI 10.1016/j.asr.2005.05.034 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FJ UT WOS:000202988300026 ER PT J AU Coleman, M Rodgers, D Jones, J AF Coleman, Max Rodgers, David Jones, Jack TI A buoyant life investigating mobile platform (BLIMP) SO ADVANCES IN SPACE RESEARCH LA English DT Article DE life detection; astrobiology; airships; instrumentation; Mars; Titan; volcanic caldera ID TITANS SURFACE; ROCK COATINGS; BASALT; GLASS; SPECTROSCOPY; MINERALOGY; CHEMISTRY; HAWAII; MARS AB The search for life in new environments, e.g., Mars/Titan, will be scientifically challenging and have great engineering difficulties. In this paper the authors discuss an approach to field-testing methods relevant to three scientific thrusts in the detection of life and pre-biotic organics on other worlds. We describe how this can be accomplished through a series of field trials using a mobile aerial vehicle that is a proxy for the exploration approaches and instrument techniques necessary for the next stage of life detection on other planets. We do this by deploying a mobile organic laboratory on Earth to demonstrate the requisite techniques. We show how terrestrial field trials provide new insights on the colonization by life of fresh volcanic flows, and the competition between biotic and abiotic processes on a newly cooling piece of the Earth's crust. This paper suggests that such work could be very effectively conducted on Hawaii, where the erupted lava is basaltic, an important crustal component for terrestrial planets. The presence of water is generally agreed to be a prerequisite for planetary habitability but the combination of basalt and water is chemically unstable at the temperatures to which basalt cools after eruption. The subsequent chemical reactions occur because the total energy of the products is lower than that of the precursor materials and on Earth biological processes result from organisms harvesting that difference in energy. For life processes to succeed they must out-compete the rate at which abiotic chemistry might accomplish the same tasks. Monitoring the rate at which chemical processes occur is therefore a life-detection approach. Biotic involvement in the rate of weathering of basalts is the test case for this new, generic life detection paradigm. This approach would be applicable to the peri-glacial zones of Mars, if liquid water were proven to be present there. We show that a 15 m autonomous BLIMP could carry various instrument packages including camera, visible spectrometer, tunable diode laser spectrometer (TDLS) for gas and gas isotope analysis, gas chromatograph/mass spectrometer (GCMS). These could be calibrated followed by ground-truthing using field experiments in the interior of Meteor Crater in Arizona. This well understood system could then study the extreme environment of the still active volcanic caldera of Kilauea and the adjacent older lava flows. For Mars the BLIMP is a proxy for a lighter balloon or even a Martian Rover, which could carry a similar suite of instruments and take a similar set of measurements. For Titan, with its dense and high-molecular weight atmosphere calm winds and low gravity, a BLIMP will be the vehicle of choice. The experiments would be directly relevant. We discuss how a Titan BLIMP could search for organic compounds in the post-Cassini exploration of Titan. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Coleman, Max; Rodgers, David; Jones, Jack] Jet Prop Lab, Pasadena, CA 91109 USA. RP Rodgers, D (reprint author), Jet Prop Lab, MS 180-604,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM max.coleman@jpl.nasa.gov; David.H.Rodgers@jpl.nasa.gov; Jack.A.Jones@jpl.nasa.gov RI Coleman, Max/A-1303-2007 OI Coleman, Max/0000-0002-5514-1826 NR 37 TC 0 Z9 0 U1 0 U2 6 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. PY 2006 VL 38 IS 6 BP 1198 EP 1208 DI 10.1016/j.asr.2005.05.058 PG 11 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FJ UT WOS:000202988300027 ER PT J AU Giroux, R Berinstain, A Braham, S Graham, T Bamsey, M Boyd, K Silver, M Lussier-Desbien, A Lee, P Boucher, M Cowing, K Dixon, M AF Giroux, Richard Berinstain, Alain Braham, Stephen Graham, Thomas Bamsey, Matthew Boyd, Keegan Silver, Matthew Lussier-Desbien, Alexis Lee, Pascal Boucher, Marc Cowing, Keith Dixon, Michael TI Greenhouses in extreme environments: The Arthur Clarke Mars Greenhouse design and operation overview SO ADVANCES IN SPACE RESEARCH LA English DT Article C1 [Giroux, Richard; Berinstain, Alain; Bamsey, Matthew; Boyd, Keegan; Silver, Matthew; Lussier-Desbien, Alexis] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. [Braham, Stephen] Simon Fraser Univ, PolyLAB, Vancouver, BC V6B 5K3, Canada. [Berinstain, Alain; Graham, Thomas; Dixon, Michael] Univ Guelph, Dept Environm Biol, Guelph, ON N1G 2W1, Canada. [Lee, Pascal] SETI Inst, Mars Inst, Moffett Field, CA 94035 USA. [Lee, Pascal] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Boucher, Marc; Cowing, Keith] SpaceRef Interact Inc, Reston, VA 20195 USA. RP Berinstain, A (reprint author), Canadian Space Agcy, 6767 Route Aeroport, St Hubert, PQ J3Y 8Y9, Canada. EM Alain.Berinstain@space.gc.ca NR 16 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 6 BP 1248 EP 1259 DI 10.1016/j.asr.2006.07.010 PG 12 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FJ UT WOS:000202988300033 ER PT J AU Mann, IR Balmain, KG Blake, JB Boteler, D Bourdarie, S Clemmons, JH Dent, ZC Degeling, AW Fedosejeves, R Fennell, JF Fraser, BJ Green, JC Jordanova, VK Kale, A Kistler, LM Knudsen, DJ Lessard, MR Loto'aniu, TM Milling, DK O'Brien, TP Onsager, TG Ozeke, LG Rae, IJ Rankin, R Reeves, GD Ridley, AJ Sofko, GJ Summers, D Thomson, I Thorne, RM Tsui, YY Unick, C Vassiliadis, D Wygant, JR Yau, AW AF Mann, I. R. Balmain, K. G. Blake, J. B. Boteler, D. Bourdarie, S. Clemmons, J. H. Dent, Z. C. Degeling, A. W. Fedosejeves, R. Fennell, J. F. Fraser, B. J. Green, J. C. Jordanova, V. K. Kale, A. Kistler, L. M. Knudsen, D. J. Lessard, M. R. Loto'aniu, T. M. Milling, D. K. O'Brien, T. P. Onsager, T. G. Ozeke, L. G. Rae, I. J. Rankin, R. Reeves, G. D. Ridley, A. J. Sofko, G. J. Summers, D. Thomson, I. Thorne, R. M. Tsui, Y. Y. Unick, C. Vassiliadis, D. Wygant, J. R. Yau, A. W. TI The outer radiation belt injection, transport, acceleration and loss satellite (ORBITALS): A Canadian small satellite mission for ILWS SO ADVANCES IN SPACE RESEARCH LA English DT Article DE ILWS; radiation belts; ULF waves; inner magnetosphere; satellite missions ID WHISTLER-MODE CHORUS; RELATIVISTIC ELECTRON MICROBURSTS; SUBAURORAL POLARIZATION STREAM; ION COMPOSITION MEASUREMENTS; WAVE-PARTICLE INTERACTIONS; INNER MAGNETOSPHERE; RESONANT DIFFUSION; CYCLOTRON WAVES; SPACE WEATHER; STORM AB The outer radiation belt injection, transport, acceleration and loss satellite (ORBITALS) is a small satellite mission proposed as a Canadian contribution to the satellite infrastructure for the International Living With a Star (ILWS) program. The ORBITALS will monitor the energetic electron and ion populations in the inner magnetosphere across a wide range of energies (keV to tens of MeV) as well as the dynamic electric and magnetic fields, waves and cold plasma environment which govern the injection, transport, acceleration and loss of these energetic and space weather critical particle populations. ORBITALS will be launched around 2010-2012 into a low-inclination GTO-like orbit which maximizes the long-lasting apogee-pass conjunctions with both the ground-based instruments of the Canadian Geospace Monitoring (CGSM) array as well as with the GOES East and West and geosynchronous communications satellites in the North American sector. Specifically, the ORBITALS will make the measurements necessary to gain fundamental new understanding of the relative importance of different physical acceleration and loss processes which are hypothesised to shape the energetic particle populations in the inner magnetosphere. The ORBITALS will also provide the raw radiation measurements at MEO altitudes necessary for the development of the next-generation of radiation belt specification models, and on-board experiments will also monitor the dose, single-event upset, and deep-dielectric charging responses of electronic components on-orbit. In this paper we outline the scientific objectives of the ORBITALS mission, discuss how the ORBITALS will lead to solutions to outstanding questions in inner magnetospheric science, and examine how the ORBITALS will complement other proposed inner magnetosphere missions in the ILWS era. (C) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 [Mann, I. R.; Dent, Z. C.; Degeling, A. W.; Kale, A.; Loto'aniu, T. M.; Milling, D. K.; Ozeke, L. G.; Rae, I. J.; Rankin, R.] Univ Alberta, Dept Phys, Edmonton, AB, Canada. [Balmain, K. G.] Univ Toronto, Dept Elect & Comp Engn, Toronto, ON, Canada. [Blake, J. B.; Clemmons, J. H.; Fennell, J. F.; O'Brien, T. P.] Aerosp Corp, Los Angeles, CA USA. [Boteler, D.] Geol Survey Canada, Ottawa, ON, Canada. [Fedosejeves, R.; Tsui, Y. Y.; Unick, C.] Univ Alberta, Dept Elect & Comp Engn, Edmonton, AB, Canada. [Fraser, B. J.] Univ Newcastle, Sch Math & Phys Sci, Newcastle, NSW 2308, Australia. [Green, J. C.; Onsager, T. G.] NOAA, Space Environm Ctr, Boulder, CO USA. [Jordanova, V. K.; Kistler, L. M.; Lessard, M. R.] Univ New Hampshire, Durham, NH 03824 USA. [Knudsen, D. J.; Yau, A. W.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Reeves, G. D.] LANL, Los Alamos, NM USA. [Ridley, A. J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Sofko, G. J.] Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK, Canada. [Summers, D.] Mem Univ Newfoundland, Dept Math & Stat, St John, NF A1C 5S7, Canada. [Thomson, I.] Thomson Nielsen, Ottawa, ON, Canada. [Thorne, R. M.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA. [Vassiliadis, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wygant, J. R.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. RP Mann, IR (reprint author), Univ Alberta, Dept Phys, Edmonton, AB, Canada. EM ian.mann@ualberta.ca RI Rankin, Robert/C-5435-2013; Rae, Jonathan/D-8132-2013; Yau, Andrew/E-7007-2013; Ridley, Aaron/F-3943-2011; Reeves, Geoffrey/E-8101-2011; Degeling, Alexander/F-1091-2016; OI Rankin, Robert/0000-0003-0151-6343; Yau, Andrew/0000-0002-8210-0392; Ridley, Aaron/0000-0001-6933-8534; Reeves, Geoffrey/0000-0002-7985-8098; Degeling, Alexander/0000-0001-7338-9270; Clemmons, James/0000-0002-5298-5222; Jordanova, Vania/0000-0003-0475-8743 NR 94 TC 12 Z9 12 U1 0 U2 4 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. PY 2006 VL 38 IS 8 BP 1838 EP 1860 DI 10.1016/j.asr.2005.11.009 PG 23 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FL UT WOS:000202988500039 ER PT J AU Rodgers, SD Charnley, SB AF Rodgers, S. D. Charnley, S. B. TI Sulfur chemistry in cometary comae SO ADVANCES IN SPACE RESEARCH LA English DT Article DE comets; general; astrochemistry; molecular processes ID C/1996 B2 HYAKUTAKE; O1 HALE-BOPP; RADIO TELESCOPES; NITROGEN SULFIDE; HYDROGEN-SULFIDE; HOT CORES; CS; MOLECULES; ENVELOPES; EVOLUTION AB We have modelled the chemistry which occurs in cometary comae following the sublimation of sulfuretted parent molecules from the nucleus. Our aim is to determine which of the S-bearing molecules observed in comets must be present in the icy nucleus and which may plausibly be produced in the coma. We find that, although chemical reactions are able to generate considerable amounts of some daughter molecules, they cannot produce the observed abundances. In particular, we demonstrate that previously suggested mechanisms for the formation Of S(2) in the inner coma are unlikely to be important in comets. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Rodgers, S. D.; Charnley, S. B.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Rodgers, SD (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-3, Moffett Field, CA 94035 USA. EM rodgers@dusty.arc.nasa.gov RI Charnley, Steven/C-9538-2012 NR 37 TC 1 Z9 1 U1 0 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 9 BP 1928 EP 1931 DI 10.1016/j.asr.2005.10.006 PG 4 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FM UT WOS:000202988600005 ER PT J AU Zender, J Grayzeck, E AF Zender, J. Grayzeck, E. TI Lessons learned from planetary science archiving SO ADVANCES IN SPACE RESEARCH LA English DT Article DE planetary data system; planetary science archive; archiving; long-term data preservation AB The need for scientific archiving of past, current, and future planetary scientific missions, laboratory data, and modeling efforts is indisputable. To quote from a message by G. Santayama carved over the entrance of the US Archive in Washington DC - "Those who can not remember the past are doomed to repeat it." The design, implementation, maintenance, and validation of planetary science archives are however disputed by the involved parties. The inclusion of the archives into the scientific heritage is problematic. For example, there is the imbalance between space agency requirements and institutional and national interests. The disparity of long-term archive requirements and immediate data analysis requests are significant. The discrepancy between the space missions archive budget and the effort required to design and build the data archive is large. An imbalance exists between new instrument development and existing, well-proven archive standards. The authors present their view on the problems and risk areas in the archiving concepts based on their experience acquired within NASA's Planetary Data System (PDS) and ESA's Planetary Science Archive (PSA). Individual risks and potential problem areas are discussed based on a model derived from a system analysis done upfront. The major risk for a planetary mission science archive is seen in the combination of minimal involvement by Mission Scientists and inadequate funding. The authors outline how the risks can be reduced. The paper ends with the authors view on future planetary archive implementations including the archive interoperability aspect. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Zender, J.] ESTEC, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands. [Grayzeck, E.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Data Serv Off, Greenbelt, MD 20771 USA. RP Zender, J (reprint author), ESTEC, European Space Agcy, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. EM joe.zender@rssd.esa.int; edwin.j.grayzeck@nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 9 BP 2013 EP 2022 DI 10.1016/j.asr.2005.10.019 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FM UT WOS:000202988600021 ER PT J AU Russell, CT Capaccioni, F Coradini, A Christensen, U De Sanctis, MC Feldman, WC Jaumann, R Keller, HU Konopliv, A McCord, TB McFadden, LA McSween, HY Mottola, S Neukum, G Pieters, CM Prettyman, TH Raymond, CA Smith, DE Sykes, MV Williams, B Zuber, MT AF Russell, C. T. Capaccioni, F. Coradini, A. Christensen, U. De Sanctis, M. C. Feldman, W. C. Jaumann, R. Keller, H. U. Konopliv, A. McCord, T. B. McFadden, L. A. McSween, H. Y. Mottola, S. Neukum, G. Pieters, C. M. Prettyman, T. H. Raymond, C. A. Smith, D. E. Sykes, M. V. Williams, B. Zuber, M. T. TI Dawn discovery mission to vesta and ceres: Present status SO ADVANCES IN SPACE RESEARCH LA English DT Article DE vesta; ceres; discovery mission; asteroid AB Dawn, the ninth Discovery mission, is a journey to the main belt asteroids Vesta and Ceres to attempt to understand the building blocks of the solar system and the processes occurring at the solar system's earliest epoch. It does this with a spacecraft that utilizes ion propulsion to reach its targets and to maneuver into orbit about these bodies. It carries a framing camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron detector. The mission has passed its critical design review and is scheduled to be launched in June 2006 with arrival at Vesta in 2011 and Ceres in 2015. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Capaccioni, F.; Coradini, A.] IFSI, I-00133 Rome, Italy. [Christensen, U.; Keller, H. U.] MPS, Katlenburg Lindau, Germany. [De Sanctis, M. C.] IAFS, I-00133 Rome, Italy. [Feldman, W. C.; Prettyman, T. H.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Jaumann, R.; Mottola, S.] DLR, D-12489 Berlin, Germany. [Konopliv, A.; Raymond, C. A.; Williams, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McCord, T. B.] Univ Hawaii, Honolulu, HI 96822 USA. [McFadden, L. A.] Univ Maryland, College Pk, MD 20742 USA. [McSween, H. Y.] Univ Tennessee, Knoxville, TN 37996 USA. [Neukum, G.] Free Univ Berlin, D-12249 Berlin, Germany. [Pieters, C. M.] Brown Univ, Providence, RI 02912 USA. [Smith, D. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sykes, M. V.] Univ Arizona, Tucson, AZ 85721 USA. [Zuber, M. T.] MIT, Cambridge, MA 02139 USA. RP Russell, CT (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, 603 Charles Young Dr E,3845 Slichter Hall, Los Angeles, CA 90095 USA. EM nina@igpp.ucla.edu RI McFadden, Lucy-Ann/I-4902-2013; De Sanctis, Maria Cristina/G-5232-2013 OI McFadden, Lucy-Ann/0000-0002-0537-9975; De Sanctis, Maria Cristina/0000-0002-3463-4437 NR 2 TC 5 Z9 5 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 9 BP 2043 EP 2048 DI 10.1016/j.asr.2004.12.041 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FM UT WOS:000202988600025 ER PT J AU Johnson, NL AF Johnson, Nicholas L. TI The new Jettison Policy for the International Space Station SO ADVANCES IN SPACE RESEARCH LA English DT Article DE space debris; International Space Station AB During more than seven years of operations by the International Space Station, approximately three dozen pieces of debris were released and subsequently cataloged by the U.S. Space Surveillance Network. The individual mass of these objects ranged from less than I to 70 kg. Although some of these debris were separated from the International Space Station accidentally, some were intentionally castoff, especially the larger items. In addition, small operational satellites are candidates for launch from the International Space Station, such as the TNS-0 satellite deployed from International Space Station in March 2005. Recently an official International Space Station Jettison Policy was developed to ensure that decisions to deliberately release objects in the future were based upon a complete evaluation of the benefits and risks to the International Space Station, other resident space objects, and people on the Earth. The policy identifies four categories of items which might be considered for release: (1) items that pose a safety issue for return on-board a visiting vehicle, (2) items that negatively impact International Space Station utilization, return, or on-orbit stowage manifests, (3) items that permit a reduction in the duration of an extravehicular activity, and (4) items that are designed for jettison. Some of the principal issues to be addressed during this evaluation process are the potential for the object to recontact the International Space Station within the first two days after jettison, the potential of the object to break up prior to reentry, the ability of the U.S. Space Surveillance Network to track the object, and the risk to people on Earth from components which might survive reentry. This paper summarizes the history of objects released from International Space Station, examines the specifics of the International Space Station Jettison Policy, and addresses the overall impact of International Space Station debris on the space environment. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, NASA Johnson Space Ctr, Orbital Debris Program Off, Houston, TX 77058 USA. RP Johnson, NL (reprint author), NASA, NASA Johnson Space Ctr, Orbital Debris Program Off, 2101 NASA Pkwy, Houston, TX 77058 USA. EM nicholas.l.johnson@nasa.gov NR 4 TC 0 Z9 0 U1 2 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 9 BP 2077 EP 2083 DI 10.1016/j.asr.2006.09.006 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FM UT WOS:000202988600030 ER PT J AU Srama, R Altobelli, N de Kam, J Kempf, S Kruger, H Lera, S Moragas-Klostermeyer, G Rachev, M Srowig, A Landgraf, M Vo, Q Grun, E AF Srama, R. Altobelli, N. de Kam, J. Kempf, S. Krueger, H. Lera, S. Moragas-Klostermeyer, G. Rachev, M. Srowig, A. Landgraf, M. Vo, Q. Gruen, E. TI DUNE-eXpress - Dust astronomy with ConeXpress SO ADVANCES IN SPACE RESEARCH LA English DT Article DE ConeXpress; dust astronomy; interstellar dust; interplanetary dust; trajectory sensor; spectrometer; dust detector; dust telescope; DUNE ID INTERSTELLAR DUST; ULYSSES SPACECRAFT; GRAINS; IDENTIFICATION; PARTICLES; CASSINI; GALILEO; VENUS; EARTH; FLUX AB DUNE-eXpress (DUst measurement near Earth) is a scientific application of the ConeXpress platform developed by Dutch Space [Scholten, H., Nugteren, P.R., de Kam, J., Cruijssen, H. ConeXpress - low cost access to space, white paper Dutch Space, Leiden, The Netherlands, 2003; Kassebom, M., Mahal, S., Scholten, H., et al. ConeXpress - a low cost satellite solution for GEO applications, DGLR-2003-115, in: Olbert, F. (Ed.), German Aerospace Congress, Munich, Germany, 2003] The goal of this mission is to investigate in situ the physical and dynamical properties of interstellar and interplanetary dust. The Dust Telescope on-board DUNE-eXpress consists of two large area mass analyzer (LAMA) instrument modules and four dust Trajectory Sensors with a total weight of 60 kg. LAMA measures the chemical composition of individual dust grains whereas the Trajectory Sensor determines their orbital parameters. DUNE-eXpress reaches an orbit outside the geostationary distance in order to avoid interferences with the Earth debris and magnetosphere environment. A position at the Sun-Earth Lagrange points L1 and L2 is well suited and reachable with DUNE-eXpress. A mission scenario based on the SMART I mission is presented. (C) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Srama, R.; Altobelli, N.; Kempf, S.; Lera, S.; Moragas-Klostermeyer, G.; Rachev, M.; Srowig, A.; Gruen, E.] MPI Nucl Phys, D-69117 Heidelberg, Germany. [Altobelli, N.] JPL, Pasadena, CA USA. [Krueger, H.] MPI Solar Syst Res, Katlenburg Lindau, Germany. [de Kam, J.; Vo, Q.] Dutch Space, Leiden, Netherlands. [Landgraf, M.] ESOC, Darmstadt, Germany. [Gruen, E.] Univ Hawaii, HIGP, Honolulu, HI 96822 USA. RP Srama, R (reprint author), MPI Nucl Phys, Postfach 103980, D-69117 Heidelberg, Germany. EM ralf.srama@mpi-hd.mpg.de OI KEMPF, SASCHA/0000-0001-5236-3004 NR 23 TC 2 Z9 2 U1 0 U2 1 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. PY 2006 VL 38 IS 9 BP 2093 EP 2101 DI 10.1016/j.asr.2005.09.009 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FM UT WOS:000202988600032 ER PT J AU Jiang, JH Eckermann, SD Wu, DL Wang, DY AF Jiang, Jonathan H. Eckermann, Stephen D. Wu, Dong L. Wang, Ding Yi TI Inter-annual variation of gravity waves in the Arctic and Antarctic winter middle atmosphere SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Arctic; Antarctic; middle atmosphere; gravity wave; UARS MLS; satellite observation ID LIMB SOUNDER OBSERVATIONS; MOUNTAIN WAVES; STRATOSPHERE; MLS; CLIMATOLOGY; SPECTRA; CLOUDS AB High latitude, middle atmospheric (28-80 km) gravity wave observations from the Microwave Limb sounder (MLS) on the Upper Atmosphere Research Satellite (UARS) are available during five Arctic and Antarctic winters between 1991 and 1997. Newer data from NOAA Advanced Microwave Sounding Unit (AMSU) instruments have been introduced recently, in order to extend the gravity wave measurements from 1998 to present. Analyses of MLS and AMSU data show substantial inter-annual variability in both magnitude and spatial patterns of gravity wave activity at both Arctic and Antarctic latitudes. (C) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Jiang, Jonathan H.; Wu, Dong L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eckermann, Stephen D.] USN, Res Lab, Middle Atmosphere Dynam Sect, Washington, DC USA. [Wang, Ding Yi] Forschungszentrum Karlsruhe, Karlsruhe, Germany. [Wang, Ding Yi] Univ Karlsruhe, Inst Meteorol & Klimaforsch, Karlsruhe, Germany. RP Jiang, JH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 183-701, Pasadena, CA 91109 USA. EM jonathan@mlsjpl.nasa.gov NR 23 TC 5 Z9 5 U1 1 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 11 BP 2418 EP 2423 DI 10.1016/j.asr.2005.09.036 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FO UT WOS:000202988800018 ER PT J AU Justus, CG Duvall, A Keller, VW AF Justus, C. G. Duvall, Aleta Keller, Vernon W. TI Trace constituent updates in the Marshall engineering thermosphere and global reference atmospheric model SO ADVANCES IN SPACE RESEARCH LA English DT Article DE air density model; GRAM-99; atmospheric models AB Global reference atmospheric model (GRAM-99) is an engineering-level model of Earth's atmosphere. It provides both mean values and perturbations for density, temperature, pressure, and winds, as well as monthly and geographically varying trace constituent concentrations. From 0 to 27 km, GRAM thermodynamics and winds are based on National Oceanic and Atmospheric Administration Global Upper Air Climatic Atlas (GUACA) climatology. Above 120 km, GRAM is based on the NASA Marshall engineering thermosphere (MET) model. In the intervening altitude region, GRAM is based on middle atmosphere program (MAP) climatology that also forms the basis of the 1986 COSPAR International reference atmosphere (CIRA). Atmospheric composition is represented in GRAM by concentrations of both major and minor species. Above 120 km, MET provides concentration values for N-2, O-2, Ar, O, He, and H. Below 120 km, represented species also include H2O, O-3, N2O, CO, CH4, and CO2. At 34th COSPAR a comparison was made between GRAM constituents below 120 km and those provided by Naval Research Laboratory (NRL) climatology. No current need to update GRAM constituent climatology in that height range was identified. This report examines GRAM/MET constituents between 100 and 1000 km altitudes. Internal discrepancies are noted between GRAM/MET constituent number densities and mass density or molecular weight. Near 110 km altitude, there is up to about 25% discrepancy between MET number density and mass density (with mass density being valid and number densities requiring adjustment). Near 700 km altitude there is also up to about 25% discrepancy between MET number density and mean molecular weight (with molecular weight requiring adjustment). In neither case are MET mass density estimates invalidated. The discrepancies have been traced to MET subroutines SLV (which affects 90-170 km height range) and SLVH (which affects helium above 440 km altitude). With these discrepancies corrected, results are presented to illustrate GRAM/MET constituent mole fractions in terms of height-latitude cross-sections from 100 to 1000 km altitude, and latitude-longitude "maps" at 450 km. Plans are discussed for an update of MET and GRAM to correct these constituent inconsistencies, and to incorporate several new thermospheric model features. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Justus, C. G.; Duvall, Aleta] Morgan Res Corp, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Keller, Vernon W.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Justus, CG (reprint author), Morgan Res Corp, George C Marshall Space Flight Ctr, ED44 Morgan, Huntsville, AL 35812 USA. EM jere.justus@msfc.nasa.gov; aleta.duvall@msfe.nasa.gov; vernon.keller@nasa.gov NR 15 TC 0 Z9 0 U1 0 U2 0 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. PY 2006 VL 38 IS 11 BP 2429 EP 2432 DI 10.1016/j.asr.2006.05.028 PG 4 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FO UT WOS:000202988800020 ER PT J AU Justus, CG Duvall, A Keller, VW AF Justus, C. G. Duvall, Aleta Keller, Vernon W. TI Validation of Mars Global Reference Atmospheric Model (Mars-GRAM 2001) and planned new features SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Mars Global Reference Atmospheric Model; Mars-GRAM 2001; Mars International Reference Atmosphere; MIRA ID SURVEYOR AB For altitudes below 80 km, Mars Global Reference Atmospheric Model (Mars-GRAM 2001) is based on output climatology from NASA Ames Mars General Circulation Model (MGCM). At COSPAR 2002, results were presented of validation tests of Mars-GRAM versus data from Mars Global Surveyor Thermal Emission Spectrometer (TES) and Radio Science (RS) experiment. Further validation tests are presented comparing Mars-GRAM densities with those from the European Mars Climate Database (MCD), and comparing densities from both Mars-GRAM and MCD against TES observations. Throughout most of the height and latitude range of TES data (0-40 km and 70S to 70N), good agreement is found between atmospheric densities from Mars-GRAM and MCD. However, at the season and latitude zone for Mars Phoenix arrival and landing (L(s) = 65 degrees-80 degrees and latitude 65N to 75N), Mars-GRAM densities are about 30%-45% higher than MCD densities near 40 kin altitude. Further evaluation is warranted concerning potential impact of these model differences on planning for Phoenix entry and descent. Three planned features for Mars-GRAM update are also discussed: (1) new MGCM and Thermospheric General Circulation Model data sets to be used as a revised basis for Mars-GRAM mean atmosphere, (2) a new feature to represent planetary-scale traveling waves for upper altitude density variations (such as found during Mars Odyssey aerobraking), and (3) a new model for effects of high resolution topographic slope on winds near the surface (0-4.5 km above Mars Orbiter Laser Altimeter topography level). Mars-GRAM slope winds will be computed from a diagnostic (algebraic) relationship based on Ye et al. [Ye, Z.J., Segal, M., Pielke, R.A., A comparative study of daytime thermally induced upslope flow on Mars and Earth, J. Atmos. Sci. 47(5), 612-628, 1990]. This approach differs from mesoscale models (such as Mars Regional Atmospheric Modeling System and Mars Mesoscale Model Version 5), which use prognostic, full-physics solutions of the time- and space-dependent differential equations of motion. As such, slope winds in Mars-GRAM will be consistent with its "engineering-level" approach, and will be extremely fast and easy to evaluate, compared with mesoscale model solutions. Mars-GRAM slope winds are not being suggested as a replacement for sophisticated, full-physics Mars mesoscale models, but may have value, particularly for preliminary screening of large numbers of candidate landing sites for future Mars missions, such as Phoenix and Mars Science Laboratory. Test output is presented from Mars-GRAM slope winds in the area of Gusev Crater and Valles Marineris. (C) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 [Justus, C. G.; Duvall, Aleta] Morgan Res Corp, ED44 Morgan, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Keller, Vernon W.] NASA, Marshall Space Flight Ctr, ED44, Huntsville, AL 35812 USA. RP Justus, CG (reprint author), Morgan Res Corp, ED44 Morgan, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM jere.justus@msfc.nasa.gov; aleta.duvall@msfc.nasa.gov; vernon.keller@nasa.gov NR 21 TC 1 Z9 1 U1 1 U2 10 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. PY 2006 VL 38 IS 11 BP 2633 EP 2638 DI 10.1016/j.asr.2006.07.007 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FO UT WOS:000202988800052 ER PT J AU Bhattacharyya, S Miller, MC Strohmayer, TE Lamb, FK Markwardt, CB AF Bhattacharyya, Sudip Miller, M. Coleman Strohmayer, Tod E. Lamb, Frederick K. Markwardt, Craig B. TI Understanding high-density matter through analysis of surface spectral lines and burst oscillations from accreting neutron stars SO ADVANCES IN SPACE RESEARCH LA English DT Article DE equation of state; line : profiles; relativity; stars : neutron; X-rays : binaries; X-rays : bursts ID GENERAL-RELATIVISTIC SPECTRA; SPIN FREQUENCY; DISKS; STATE AB We discuss millisecond period brightness oscillations and surface atomic spectral lines observed during type I X-ray bursts from a neutron star in a low mass X-ray binary system. We show that modeling of these phenomena can constrain models of the dense cold matter at the cores of neutron stars. We demonstrate that, even for a broad and asymmetric spectral line, the stellar radius-to-mass ratio can be inferred to better than 5%. We also fit our theoretical models to the burst oscillation data of the low mass X-ray binary XTE J1814-338, and find that the 90% confidence lower limit of the neutron star's dimensionless radius-to-mass ratio is 4.2. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Bhattacharyya, Sudip; Miller, M. Coleman; Markwardt, Craig B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bhattacharyya, Sudip; Strohmayer, Tod E.; Markwardt, Craig B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lamb, Frederick K.] Univ Illinois, Dept Phys & Astron, Urbana, IL 61801 USA. RP Bhattacharyya, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM sudip@milkyway.gsfc.nasa.gov NR 14 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. PY 2006 VL 38 IS 12 BP 2765 EP 2767 DI 10.1016/j.asr.2005.10.049 PG 3 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900021 ER PT J AU Muslicitzky, R AF Muslicitzky, Richard TI Ultra-luminous sources in nearby galaxies SO ADVANCES IN SPACE RESEARCH LA English DT Article DE astrophysics; ultra-luminous sources; galactic X-ray sources ID X-RAY SOURCE; MASS BLACK-HOLES; OPTICAL COUNTERPART; IC-342; DISCOVERY; NGC-4559; NGC-5204; BINARY; OBJECT; PERIOD AB This paper presents an update of what we have learned in the last year about the ULX phenomenon. New results are presented on radio emission from Holmberg II and a review is given on the recent X-ray data on timing and spectra. The new X-ray spectroscopic and optical imaging survey of nearby ULX with XMM allows us, for the first time, to place the average properties of these objects oil a statistical basis. Direct examination of the sites of ULXs in nearby galaxies shows that similar to 1/3 of them are not in or near star forming regions, indicating that a substantial fraction of ULX are not directly associated with young star formation. There are two ULX which have been identified with B stars as the optical counterparts on the basis of optical spectroscopy. Radio imaging of the Holmberg 11 ULX shows that it lies in a luminous extended radio source and that the radio emission is not beamed. A statistical study of ULX spectra in nearby galaxies shows that the ratio of 'high state' to 'low state' ULXs is similar to 1:1 and that the high state objects, in general, are best fit with low temperature black bodies with a steep power law index. The objects with high state spectra are systematically more luminous than the objects with low state spectra consistent with the hypothesis that both are drawn from a population which shows state changes similar to those of black holes in the Milky Way. If this is true then the masses implied for the objects with the low state spectra are greater than 50M(circle dot). (C) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Muslicitzky, R (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. EM richard@milkyway.gsfc.nasa.gov NR 40 TC 0 Z9 0 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. PY 2006 VL 38 IS 12 BP 2793 EP 2800 DI 10.1016/j.asr.2006.08.005 PG 8 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900030 ER PT J AU Ebisawa, K Kawaguchi, T AF Ebisawa, Ken Kawaguchi, Toshihiro TI X-ray observations of black-hole accretion disks SO ADVANCES IN SPACE RESEARCH LA English DT Article DE black hole accretion disk; X-ray observations; astrophysics ID NEARBY SPIRAL GALAXIES; GRO J1655-40; LMC X-3; SPECTRA; BINARIES; MODEL; CANDIDATES; DISCS; STATE; SPIN AB Our current theoretical and observational understandings of the accretion disks around Galactic black-holes are reviewed. Historically, a simple phenomenological accretion disk model has been used to interpret X-ray observations. Although such a phenomenological interpretation is still useful, high quality X-ray data from contemporary instruments allow us to test more realistic accretion disk models. In a simple and ideal case, the standard optically thick accretion disk model is successful to explain observations, such that the inner disk radius is constant at three times the Schwarzschild radius over large luminosity variations. However, when disk luminosity is close to or exceeds the Eddington luminosity, the standard disk model breaks, and we have to consider the "slim disk" solution in which radial energy advection is dominant. Recent observations of Ultra-luminous X-ray sources (ULXs), which may not be explained by the standard disk model, strongly suggest the slim disk solution. We compare theoretical X-ray spectra from the slim disk with observed X-ray spectra of ULXs. We have found that the slim disk model is successful to explain ULX spectra, in terms of the massive stellar black-holes with several tens of solar mass and the super-Eddington mass accretion rates. In order to explain the large luminosities (> 10(40) ergs s(-1)) of ULXs, "intermediate black-holes" (>100M(circle dot)) are not required. Slim disks around massive stellar black-holes of up to several tens of solar mass would naturally explain the observed properties of ULXs. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Ebisawa, Ken] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. [Kawaguchi, Toshihiro] Natl Astron Observ Japan, Div Opt & Infrared Astron, Mitaka, Tokyo 1818588, Japan. RP Ebisawa, K (reprint author), NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Code 662, Greenbelt, MD 20771 USA. EM ebisawa@subaru.gsfc.nasa.gov NR 31 TC 0 Z9 0 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. PY 2006 VL 38 IS 12 BP 2862 EP 2866 DI 10.1016/j.asr.2006.06.016 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900045 ER PT J AU Weisskopf, MC AF Weisskopf, Martin C. TI Observations of compact X-ray binaries with the Chandra X-ray Observatory SO ADVANCES IN SPACE RESEARCH LA English DT Article DE X-ray astronomy; X-ray binaries; compact objects ID SPECTRUM; SS-433 AB The Chandra X-ray Observatory was launched on July 23, 1999. The first X-ray photons were detected on August 12 of that same year. Subsequently observations with the Observatory, which features sub-arcsecond angular resolution, have revolutionized our understanding of the X-ray emitting sky providing hosts of spectacular energy-resolved images and high-resolution spectra. Here we present a brief overview of Chandra X-ray Observatory observations of compact X-ray binaries. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, MSFC, Huntsville, AL 35812 USA. RP Weisskopf, MC (reprint author), NASA, MSFC, Huntsville, AL 35812 USA. EM martin@smoker.msfc.nasa.gov NR 12 TC 0 Z9 0 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. PY 2006 VL 38 IS 12 BP 2953 EP 2958 DI 10.1016/j.asr.2006.02.071 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900065 ER PT J AU Swank, JH AF Swank, J. H. TI The Rossi X-ray timing explorer: Capabilities, achievements and aims SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Rossi X-ray timing explorer; RXTE; astrophysics; black holes; neutron stars; acereting white dwarfs AB The prime scientific objectives of the Rossi X-ray Timing Explorer (RXTE) were the study of astrophysical compact objects: black holes (galactic and extragalactic), many types of neutron stars, and accreting white dwarfs. RXTE was successful in achieving its original observing objectives of large area and high time resolution observations with broadband (2-200 keV) spectra, scheduled flexibly enough to enable observations of targets Of Opportunity on any timescale greater than a few hours. These capabilities enabled qualitatively new discoveries about dynamical tirnescale phenomena related to neutron stars and black holes, phenomena which probe basic physics in the most extreme environments of gravity, density, and magnetic fields. RXTE has extended its lifetime by applying the proportional counter area selectively and maintains schedule flexibility by making use of the distribution of targets around the sky. Proposed future observations emphasize opportunity to discover and study additional millisecond pulsars, pursue the high frequency quasi-periodic oscillations in black hole transients, and connect high frequency phenomena with longer-term characteristics. RXTE will continue to strongly support, for both galactic and extragalactic targets, combining RXTE observations with other wavelengths (from IR to TeV) or with other capabilities, such as high spectral resolution. (C) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20740 USA. RP Swank, JH (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20740 USA. EM swank@milkyway.gsfc.nasa.gov RI Swank, Jean/F-2693-2012 NR 8 TC 1 Z9 1 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 12 BP 2959 EP 2963 DI 10.1016/j.asr.2006.07.009 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900066 ER PT J AU Ramsey, BD AF Ramsey, Brian D. TI The development of focusing optics for the hard-X-ray region SO ADVANCES IN SPACE RESEARCH LA English DT Article DE X-ray optics; grazing incidence; multilayers; cadmium zinc-telluride ID BALLOON EXPERIMENT; TELESCOPE; HEFT AB Grazing-incidence optics has revolutionized soft-X-ray astronomy yet the scientifically important hard-X-ray region has gone relatively unexplored at high sensitivity and fine angular scales. This situation is now changing with several flight-ready balloon-borne focusing telescopes and planned satellite-borne observatories. This review discusses some of the developments in mirror and focal plane technologies that are making these payloads possible. (C) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Ramsey, BD (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM brian.ramsey@msfc.nasa.gov NR 15 TC 2 Z9 2 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PY 2006 VL 38 IS 12 BP 2985 EP 2988 DI 10.1016/j.asr.2005.10.059 PG 4 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA V44FP UT WOS:000202988900070 ER PT S AU Webb, PA Benson, RF Grebowsky, J AF Webb, P. A. Benson, R. F. Grebowsky, J. BE Bilitza, D Reinisch, B TI Altitude variations of middle-latitude topside ionospheric electron-density profiles SO ADVANCES IN SPECIFYING PLASMA TEMPERATURES AND ION COMPOSITION IN THE IONOSPHERE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE electron density profiles; topside ionosphere; ion composition; O+/H+ transition height; topside sounding ID PLASMASPHERE; MODEL; TEMPERATURES; ATMOSPHERE AB An approach to determine the dependence of the mid-latitude topside ionospheric electron number density (N-e) altitude distributions and ion composition changes on long-term solar-cycle variations and short-term solar-wind and magnetic disturbances has been developed. This approach focuses on N-e altitude profiles from the height of the ionospheric N-e maximum to similar to 3000 km as deduced from ISIS (International Satellites for Ionospheric Studies) topside-sounder data. These data, obtained over a two-decade time interval, can be used to investigate secular changes in the topside N-e profiles, which reflect altitude changes in plasma temperature and ion composition, over more than a solar cycle. The approach is to determine the locations of mid-latitude O+/H+ transition altitudes deduced by fitting the topside N-e profiles to modeled H+ and O+ profiles using the base electron temperatures and constant temperature gradients as variables. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Nomad Res Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Webb, PA (reprint author), NASA, Goddard Space Flight Ctr, Code 612-3, Greenbelt, MD 20771 USA. EM pwebb@pop600.gsfc.nasa.gov RI Grebowsky, Joseph/I-7185-2013 NR 17 TC 8 Z9 8 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 37 IS 5 BP 951 EP 957 DI 10.1016/j.asr.2005.05.130 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BEO08 UT WOS:000238387900011 ER PT B AU Barnes, NP AF Barnes, Norman P. BE DiBartolo, B Forte, O TI Challenges for current spectroscopy: Detection of security threats SO Advances in Spectroscopy for Lasers and Sensing SE NATO SCIENCE SERIES, SERIES II: MATHEMATICS, PHYSICS AND CHEMISTRY LA English DT Proceedings Paper CT NATO Advanced-Study-Institute on New Developments in Optics and Related Fields CY JUN 06-21, 2005 CL Erice, ITALY SP NATO C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Barnes, NP (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-4787-8 J9 NATO SCI SER II MATH PY 2006 VL 231 BP 63 EP 72 DI 10.1007/1-4020-4789-4_4 PG 10 WC Optics; Physics, Applied; Spectroscopy SC Optics; Physics; Spectroscopy GA BEX75 UT WOS:000240038000004 ER PT B AU Barnes, NP AF Barnes, Norman P. BE DiBartolo, B Forte, O TI Sources for threat detection SO Advances in Spectroscopy for Lasers and Sensing SE NATO SCIENCE SERIES, SERIES II: MATHEMATICS, PHYSICS AND CHEMISTRY LA English DT Proceedings Paper CT NATO Advanced-Study-Institute on New Developments in Optics and Related Fields CY JUN 06-21, 2005 CL Erice, ITALY SP NATO C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Barnes, NP (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-4787-8 J9 NATO SCI SER II MATH PY 2006 VL 231 BP 73 EP 81 DI 10.1007/1-4020-4789-4_5 PG 9 WC Optics; Physics, Applied; Spectroscopy SC Optics; Physics; Spectroscopy GA BEX75 UT WOS:000240038000005 ER PT B AU Walsh, BM AF Walsh, Brian M. BE DiBartolo, B Forte, O TI Judd-Ofelt theory: Principles and practices SO Advances in Spectroscopy for Lasers and Sensing SE NATO SCIENCE SERIES, SERIES II: MATHEMATICS, PHYSICS AND CHEMISTRY LA English DT Proceedings Paper CT NATO Advanced-Study-Institute on New Developments in Optics and Related Fields CY JUN 06-21, 2005 CL Erice, ITALY SP NATO ID RARE-EARTH IONS; COOPERATIVE OPTICAL TRANSITIONS; DOPED INORGANIC MATERIALS; TRIVALENT LANTHANIDES; SPECTRAL INTENSITIES; COMPLEX SPECTRA; ABSORPTION INTENSITIES; ENERGY-TRANSFER; CRYSTAL FIELDS; F TRANSITIONS C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Walsh, BM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 54 TC 66 Z9 66 U1 2 U2 22 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-4787-8 J9 NATO SCI SER II MATH PY 2006 VL 231 BP 403 EP 433 DI 10.1007/1-4020-4789-4_21 PG 31 WC Optics; Physics, Applied; Spectroscopy SC Optics; Physics; Spectroscopy GA BEX75 UT WOS:000240038000020 ER PT S AU Lawson, PR AF Lawson, Peter R. BE Monnier, JD Scholler, M Danchi, WC TI Advances in science with stellar interferometers 2004-2006 - art. no. 626801 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE astronomy; interferometry; optical; infrared; stellar parameters; binary stars; circumstellar matter ID PROTOTYPE OPTICAL INTERFEROMETER; NEAR-INFRARED INTERFEROMETRY; HIGH-RESOLUTION SPECTROSCOPY; BASE-LINE INTERFEROMETRY; WATER-VAPOR ENVELOPE; HERBIG-AE/BE STARS; T-TAURI STARS; MIRA VARIABLES; CHARA ARRAY; MIDINFRARED INTERFEROMETRY AB This paper presents an overview of contributions in astrophysics made since 2004 through the use of long-baseline optical/infrared interferometers. Emphasis is placed on new results at near- and mid-infrared wavelengths. These results include new insights into our understanding of Cepheid and Mira variables, Young Stellar Objects, dust shells, spectroscopic binaries, and the limb-darkening of rapidly rotating stars. Plans for future work are also described. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lawson, PR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 301-451, Pasadena, CA 91109 USA. NR 98 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26801 EP 26801 AR 626801 DI 10.1117/12.670288 PG 14 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800003 ER PT S AU Colavita, MM Serabyn, G Wizinowich, PL Akeson, RL AF Colavita, M. Mark Serabyn, Gene Wizinowich, Peter L. Akeson, Rachel L. BE Monnier, JD Scholler, M Danchi, WC TI Nulling at the Keck Interferometer - art. no. 626803 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE interferometry; nulling; Keck ID PALOMAR TESTBED INTERFEROMETER; NULLER; PERFORMANCE; SCIENCE; SYSTEM AB The nulling mode of the Keck Interferometer is being commissioned at the Mauna Kea summit. The nuller combines the two Keck telescope apertures in a split-pupil mode to cancel the on-axis starlight and coherently detect the residual signal. The nuller, working at 10 um, is tightly integrated with the other interferometer subsystems including the fringe and angle trackers, the delay lines and laser metrology, and the real-time control system. Since first 10 um light in August 2004, the system integration is proceeding with increasing functionality and performance, leading to demonstration of a 100:1 on-sky null in 2005. That level of performance has now been extended to observations with longer coherent integration times. An overview of the overall system is presented, with emphasis on the observing sequence, phasing system, and differences with respect to the V-2 system, along with a presentation of some recent engineering data. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Colavita, MM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 19 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26803 EP 26803 AR 626803 DI 10.1117/12.672651 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800005 ER PT S AU Serabyn, E Booth, A Colavita, MM Crawford, S Garcia, J Gathright, J Hrynevych, M Koresko, C Ligon, R Mennesson, B Panteleeva, T Ragland, S Summers, K Traub, W Tsubota, K Wetherell, E Wizinowich, P Woilluz, J AF Serabyn, E. Booth, A. Colavita, M. M. Crawford, S. Garcia, J. Gathright, J. Hrynevych, M. Koresko, C. Ligon, R. Mennesson, B. Panteleeva, T. Ragland, S. Summers, K. Traub, W. Tsubota, K. Wetherell, E. Wizinowich, P. Woilluz, J. BE Monnier, JD Scholler, M Danchi, WC TI Science observations with the Keck Interferometer Nuller - art. no. 626815 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE nulling interferometry ID VEGA AB The Keck Interferometer Nuller (KIN) is now largely in place at the Keck Observatory, and functionalities and performance are increasing with time. The main goal of the KIN is to examine nearby stars for the presence of exozodiacal emission, but other sources of circumstellar emission, such as disks around young stars, and hot exoplanets are also potential targets. To observe with the KIN in nulling mode, knowledge of the intrinsic source spectrum is essential, because of the wide variety of wavelengths involved in the various control loops - the AO system operates at visible wavelengths, the pointing loops use the J-band, the high-speed fringe tracker operates in the K-band, and the nulling observations take place in the N-band. Thus, brightness constraints apply at all of these wavelengths. In addition, source structure plays a role at both K-band and N-band, through the visibility. In this talk, the operation of the KIN is first briefly described, and then the sensitivity and performance of the KIN is summarized, with the aim of presenting an overview of the parameter space accessible to the nuller. Finally, some of the initial observations obtained with the KIN are described. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Serabyn, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 14 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26815 EP 26815 AR 626815 DI 10.1117/12.672621 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800039 ER PT S AU Martin, SR Szwaykowski, P Loya, FM Liewer, K AF Martin, Stefan R. Szwaykowski, Piotr Loya, Frank M. Liewer, Kurt BE Monnier, JD Scholler, M Danchi, WC TI Progress in testing exo-planet signal extraction on the TPF-I Planet Detection Testbed - art. no. 626818 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE nulling; stellar interferometry; exoplanet ID INTERFEROMETER AB The Terrestrial Planet Finder Interferometer (TPF-I) concept is being studied at the Jet Propulsion Laboratory and the TPF-I Planet Detection Testbed has been developed to simulate the detection process for an earthlike planet orbiting a star within about 15 pc. The testbed combines four beams of infrared light simulating the operation of a dual chopped Bracewell interferometer observing a star and a faint planet. This paper describes the results obtained this year including nulling of the starlight on four input beams at contrast ratios up to 250,000 to 1, and detection of faint planet signals at contrast ratios with the star of 2 million to 1. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Martin, SR (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. NR 13 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26818 EP 26818 AR 626818 DI 10.1117/12.672646 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800042 ER PT S AU Danchi, WC Barry, RK Deming, D Kuchner, M Monnier, JD Mundy, LG Rajagopal, J Richardson, J Seager, S Traub, W AF Danchi, W. C. Barry, R. K. Deming, D. Kuchner, M. Monnier, J. D. Mundy, L. G. Rajagopal, J. Richardson, J. Seager, S. Traub, W. BE Monnier, JD Scholler, M Danchi, WC TI Scientific rationale for exoplanet characterization from 3-8 microns: The FKSI mission - art. no. 626820 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE nulling interferometer; extrasolar planets; planet formation; debris disks; active galactic nuclei ID EXTRASOLAR GIANT PLANETS; B-LIKE PLANETS; INTERFEROMETER; ATMOSPHERE; EMISSION; SYSTEM AB During the last few years, considerable effort has been directed towards large-scale (> $1 Billion) missions to detect and characterize earth-like planets around nearby stars, such as the Terrestrial Planet Finder Interferometer and Darwin missions. However, technological issues such as formation flying, cryocooling, obtaining sufficient null depth for broadband signals, and control of systematic noise sources will likely prevent these missions from entering Phase A until at least the end of the present decade. Futhermore, a large mission like TPF-I will also need the endorsement of the next Astronomical Decadal Survey to obtain a Phase A start in the next decade. Thus, given the present circumstances, we can expect TPF-I to launch no earlier than about 2020 or even as late as 2025. Presently more than 168 planets have been discovered by precision radial velocity survey techniques, and little is known about the majority of them. A simplified nulling interferometer operating in the near- to mid-infrared (e.g. similar to 3-8 microns), like the Fourier Kelvin Stellar Interferometer (FKSI), can characterize the atmospheres of a large sample of the known planets. Many other scientific problems can be addressed with a system like FKSI, including the imaging of debris disks, active galactic nuclei, and low mass companions around nearby stars. We discuss the rationale, both scientific and technological, for a competed mission in the $450-600 Million range, of which FKSI is an example. Such a mission is essential to develop our community and keep the larger community, including young scientists, engaged in the long-term effort towards the detection of Earth-like planets. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Danchi, WC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Kuchner, Marc/E-2288-2012 NR 24 TC 4 Z9 4 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26820 EP 26820 AR 626820 DI 10.1117/12.672817 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800064 ER PT S AU Carpenter, KG Schrijver, CJ Karovska, M AF Carpenter, Kenneth G. Schrijver, Carolus J. Karovska, Margarita CA SI Vision Mission Study Team BE Monnier, JD Scholler, M Danchi, WC TI The Stellar Imager (SI) vision mission - art. no. 626821 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE interferometry; future space missions; stellar activity; high angular resolution; magnetic processes AB The Stellar Imager (SI) is a UV-Optical, Space-Based Interferometer designed to enable 0.1 milli-aresecond (mas) spectral imaging of stellar surfaces and of the Universe in general and asteroseismic imaging of stellar interiors. SI is identified as a "Flagship and Landmark Discovery Mission" in the 2005 Sun Solar System Connection (SSSC) Roadmap and as a candidate for a "Pathways to Life Observatory" in the Exploration of the Universe Division (EUD) Roadmap (May, 2005). SI will revolutionize our view of many dynamic astrophysical processes: its resolution will transform point sources into extended sources, and snapshots into evolving views. SI's science focuses on the role of magnetism in the Universe, particularly on magnetic activity on the surfaces of stars like the Sun. SI's prime goal is to enable long-term forecasting of solar activity and the space weather that it drives. SI will also revolutionize our understanding of the formation of planetary systems, of the habitability and climatology of distant planets, and of many magneto-hydrodynamically controlled processes in the Universe. The results of the SI "Vision Mission" Study are presented in this paper. Additional information on the SI mission concept and related technology development can be found at URL: http://hires.gsfc.nasa.gov/si/. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Carpenter, KG (reprint author), NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA. RI Carpenter, Kenneth/D-4740-2012 NR 4 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26821 EP 26821 AR 626821 DI 10.1117/12.669713 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800065 ER PT S AU Marr-Iv, JC AF Marr-Iv, James C. BE Monnier, JD Scholler, M Danchi, WC TI SIM-PlanetQuest: Progress report - art. no. 626822 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE Interferometer; Interferometry; astrometry; SIM; PlanetQuest; exo-planets; planet-finding AB SIM-PlanetQuest is a NASA astrophysics mission that is implementing the National Research Counsel's recommended Astrometric Interferometry Mission (AIM) to develop the first, in-space, optical, long-baseline Michelson Stellar Interferometer for performing micro-arcsecond-level astrometry. This level of astrometric precision will enable characterization of planetary systems around nearby stars and enable a number of key investigations in astrophysics including calibration of the cosmological distance scale, stellar and galactic structure and evolution, and dark matter/energy distribution. This paper provides an update on the SIM-PlanetQuest Mission covering the results of the 2005 mission redesign and the recent completion of the last in a series of technology "gates". The SIM-PlanetQuest mission redesign was directed by NASA to recover eroded mass and power margins and to meet specific implementation cost targets. The resulting mission redesign met all redesign objectives with minimal impact to mission science performance. This paper provides the mission redesign objectives and describes the resulting mission and system design including changes in science capability. SIM-PlanetQuest also completed the last of eight major technology development gates that were established in 2001 by NASA, completing the enabling technology development. The technology development program, the last gate, and its significance to the project's flight verification and validation (V&V) approach are briefly described (covered in more detail in a separate paper at this conference). An update on project programmatic status and plans is also provided. C1 NASA, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA. RP Marr-Iv, JC (reprint author), NASA, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA. NR 7 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26822 EP 26822 AR 626822 DI 10.1117/12.670512 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800066 ER PT S AU Laskin, RA AF Laskin, Robert A. BE Monnier, JD Scholler, M Danchi, WC TI Successful completion of SIM-PlanetQuest technology - art. no. 626823 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE interferometry; metrology; pointing; control; nanometer; picometer; optics; lasers ID SPATIAL INTERFEROMETRY; METROLOGY GAUGES; KECK INTERFEROMETER; EXTERNAL METROLOGY AB Optical interferometry will open new vistas for astronomy over the next decade. The Space Interferometry Mission (SIM-PlanetQuest), operating unfettered by the Earth's atmosphere, will offer unprecedented astrometric precision that promises the discovery of Earth-class extra-solar planets as well as a wealth of important astrophysics. Optical interferometers also present severe technological challenges: laser metrology systems must perform with sub-nanometer precision; mechanical vibrations must be controlled to nanometers requiring orders of magnitude disturbance rejection; a multitude of actuators and sensors must operate flawlessly and in concert. The Jet Propulsion Laboratory, with the support of Lockheed Martin Advanced Technology Center (LM ATC) and Northrop Grumman Space Technology (NGST), has addressed these challenges with a technology development program that is now complete. Technology transfer to the SIM flight team is now well along and the project is proceeding toward Preliminary Design Review (PDR) with a quickening pace. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Laskin, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. NR 131 TC 10 Z9 10 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26823 EP 26823 AR 626823 DI 10.1117/12.670849 PG 24 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800067 ER PT S AU Goullioud, R Lindensmith, CA Hahn, I AF Goullioud, R. Lindensmith, C. A. Hahn, I. BE Monnier, JD Scholler, M Danchi, WC TI Results from SIM's Thermo-Opto-Mechanical (TOM3) testbed - art. no. 626824 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE interferometry; metrology; wavefront; thermal; model; SIM AB Future space-based optical interferometers, such as the Space Interferometer Mission Planet Quest (SIM), require thermal stability of the optical wavefront to the level of picometers in order to produce astrometric data at the microarc-second level. In SIM, the internal path of the interferometer will be measured with a small metrology beam whereas the starlight fringe position is estimated from a large concentric annular beam. To achieve the micro-arc-second observation goal for SIM, it is necessary to maintain the optical path difference between the central and the outer annulus portions of the wavefront of the front-end telescope optics to a few tens of picometers. The Thermo-Opto-Mechanical testbed (TOM3) was developed at the Jet Propulsion Laboratory to measure thermally induced optical deformations of a full-size flight-like beam compressor and siderostat, the two largest optics on SIM, in flight-like thermal environments. A Common Path Heterodyne Interferometer (COPHI) developed at JPL was used for the fine optical path difference measurement as the metrology sensor. The system was integrated inside a large vacuum chamber in order to mitigate the atmospheric and thermal disturbances. The siderostat was installed in a temperature-controlled thermal shroud inside the vacuum chamber, creating a flight-like thermal environment. Detailed thermal and structural models of the test articles (siderostat and compressor) were also developed for model prediction and correlation of the thermal deformations. Experimental data shows SIM required thermal stability of the test articles and good agreement with the model predictions. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Goullioud, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 11 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26824 EP 26824 AR 626824 DI 10.1117/12.670623 PG 16 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800068 ER PT S AU Brugarolas, PB Kang, BH AF Brugarolas, Paul B. Kang, Bryan H. BE Monnier, JD Scholler, M Danchi, WC TI Instrument Pointing Control System for the Stellar Interferometry Mission - Planet Quest - art. no. 626825 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE pointing; tracking; control; interferometry AB This paper describes the high precision Instrument Pointing Control System (PCS) for the Stellar Interferometry Mission (SIM)-Planet Quest. The PCS system provides front-end pointing, compensation for spacecraft motion, and feedforward stabilization, which are needed for proper interference. Optical interferometric measurements require very precise pointing (0.03 as, 1-sigma radial) for maximizing the interference pattern visibility. This requirement is achieved by fine pointing control of articulating pointing mirrors with feedback from angle tracking cameras. The overall pointing system design concept is presented. Functional requirements and an acquisition concept are given. Guide and Science pointing control loops are discussed. Simulation analyses demonstrate the feasibility of the design. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Brugarolas, PB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 2 Z9 2 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26825 EP 26825 AR 626825 DI 10.1117/12.671043 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800069 ER PT S AU Lawson, PR Ahmed, A Gappinger, RO Ksendzov, A Lay, OP Martin, SR Peters, RD Scharf, DP Wallace, JK Ware, B AF Lawson, P. R. Ahmed, A. Gappinger, R. O. Ksendzov, A. Lay, O. P. Martin, S. R. Peters, R. D. Scharf, D. P. Wallace, J. K. Ware, B. BE Monnier, JD Scholler, M Danchi, WC TI Terrestrial Planet Finder Interferometer technology status and plans - art. no. 626828 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE interferometry; astronomy; extrasolar planets; nulling; formation flying ID NULLING INTERFEROMETERS; SYSTEMATIC-ERRORS AB This paper reviews recent progress with technology being developed for the Terrestrial Planet Finder Interferometer (TPF-I). TPF-I is a mid-infrared space interferometer being designed with the capability of detecting Earth-like planets in the habitable zones around nearby stars. TPF-I is in the early phase of its development. The science requirements of the mission are described along with the current design of the interferometer. The goals of the nulling and formation flying testbeds are reviewed. Progress with TPF-I technology milestones are highlighted. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Lawson, PR (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 9 TC 3 Z9 3 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26828 EP 26828 AR 626828 DI 10.1117/12.670318 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800072 ER PT S AU Mennesson, B Haguenauer, P Serabyn, E Liewer, K AF Mennesson, B. Haguenauer, P. Serabyn, E. Liewer, K. BE Monnier, JD Scholler, M Danchi, WC TI Deep broad-band infrared nulling using a single-mode fiber beam combiner and baseline rotation - art. no. 626830 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE nulling; interferometry; infrared; high contrast Imaging AB The basic advantage of single-mode fibers for deep nulling applications resides in their spatial filtering ability, and has now long been known. However, and as suggested more recently, a single-mode fiber can also be used for direct coherent recombination of spatially separated beams, i.e. in a "multi-axial" nulling scheme. After the first successful demonstration of deep (< 2e-6) visible LASER nulls using this technique (Haguenauer & Serabyn, Applied Optics 2006), we decided to work on an infrared extension for ground based astronomical observations, e.g. using two or more off-axis sub-apertures of a large ground based telescope. In preparation for such a system, we built and tested a laboratory infrared fiber miller working in a wavelength regime where atmospheric turbulence can be efficiently corrected, over a pass band (similar to 1.5 to 1.8 micron) broad enough to provide reasonable sensitivity. In addition, since no snapshot images are readily accessible with a (single) fiber nuller, we also tested baseline rotation as an approach to detect off-axis companions while keeping a central null. This modulation technique is identical to the baseline rotation envisioned for the TPF-I space mission. Within this context, we report here on early laboratory results showing deep stable broad-band dual polarization infrared nulls < 5e-4 (currently limited by detector noise), and visible LASER nulls better than 3e-4 over a 360 degree rotation of the baseline. While further work will take place in the laboratory to achieve deeper stable broad-band nulls and test off-axis sources detection through rotation, the emphasis will be put on bringing such a system to a telescope as soon as possible. Detection capability at the 500:1 contrast ratio in the K band (similar to 2.2 microns) seem readily accessible within 50-100 mas of the optical axis, even with a first generation system mounted on a > 5m AO equipped telescope such as the Palomar Hale 200 inch, the Keck, Subaru or Gemini telescopes. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mennesson, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 1 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26830 EP 26830 AR 626830 DI 10.1117/12.672157 PG 7 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800097 ER PT S AU Rinehart, SA Armstrong, T Frey, BJ Jung, J Kirk, J Leisawitz, DT Leviton, DB Lyon, R Martino, AJ Mundy, LG Pauls, T Thompson, AK AF Rinehart, S. A. Armstrong, T. Frey, Bradley J. Jung, J. Kirk, J. Leisawitz, David T. Leviton, Douglas B. Lyon, R. Martino, Anthony J. Mundy, Lee G. Pauls, T. Thompson, A. K. BE Monnier, JD Scholler, M Danchi, WC TI The Wide-Field Imaging Interferometry Testbed: Recent results - art. no. 626836 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE interferometry; Michelson interferometer; wide-field imaging; synthesis imaging; testbed AB We present recent results from the Wide-Field Imaging Interferometry Testbed (WIIT). The data acquired with the WIIT is "double Fourier" data, including both spatial and spectral information within each data cube. We have been working with this data, and starting to develop algorithms, implementations, and techniques for reducing this data. Such algorithms and tools are of great import for a number of future missions, including the Space Infrared Interferometric Telescope (SPIRIT), the Submillimeter Probe of the Evolution of Cosmic Structure (SPECS), and the Terrestrial Planet Finder Interferometer (TPF-I)/Darwin. Recent results are discussed and future study directions are described. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rinehart, SA (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 665, Greenbelt, MD 20771 USA. RI Lyon, Richard/D-5022-2012 NR 18 TC 6 Z9 6 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26836 EP 26836 AR 626836 DI 10.1117/12.672110 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800102 ER PT S AU Ksendzov, A Bloemhof, E White, V Wallace, JK Gappinger, RO Sanghera, JS Busse, LE Kim, WJ Pureza, PC Nguyen, VQ Aggarwal, ID Shalem, S Katzir, A AF Ksendzov, A. Bloemhof, E. White, V. Wallace, J. K. Gappinger, R. O. Sanghera, J. S. Busse, L. E. Kim, W. J. Pureza, P. C. Nguyen, V. Q. Aggarwal, I. D. Shalem, S. Katzir, A. BE Monnier, JD Scholler, M Danchi, WC TI Measurement of spatial filtering capabilities of single mode infrared fibers - art. no. 626838 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE infrared fiber; single mode; testing AB Spatial filtering is necessary to achieve deep nulls in optical interferometer and single mode infrared fibers can serve as spatial filters. The filtering function is based on the ability of these devices to perform the mode-cleaning function: only the component of the input field that is coupled to the single bound (fundamental) mode of the device propagates to the output without substantial loss. In practical fiber devices, there are leakage channels that cause light not coupled into the fundamental mode to propagate to the output. These include propagation through the fiber cladding and by means of a leaky mode. We propose a technique for measuring the magnitude of this leakage and apply it to infrared fibers made at the Naval Research Laboratory and at Tel Aviv University. All measurements are performed at 10.5 mu m wavelength. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ksendzov, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26838 EP 26838 AR 626838 DI 10.1117/12.673388 PG 6 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800104 ER PT S AU Tanner, AM Catanzarite, J Shao, M AF Tanner, A. M. Catanzarite, J. Shao, M. BE Monnier, JD Scholler, M Danchi, WC TI Detection and mass characterization of terrestrial planets in the habitable zone with SIM PlanetQuest - art. no. 626847 SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE exoplanets; stellar populations; interferometry ID SPACE-INTERFEROMETRY-MISSION; EXTRASOLAR PLANETS; SYSTEMS AB SIM PlanetQuest is a space-borne Michelson interferometer with a nine meter baseline that will survey similar to 200 stars within 30 parsecs for terrestrial mass planets. Ultra-precise astrometric observations will reveal the gravitational wobble of the target star (due to a planetary companion) against an inertial frame of reference stars located within a 1.5 degree radius. Here, we report the results of multiple Monte Carlo simulations which have modeled SIM's ability to detect and determine the orbital parameters and masses of the terrestrial mass planets around its potential sample of target stars. We find that SIM will detect 80% of the planets in the 60 star sample. Out of those planets SIM detects, we will be able to estimate the masses of at least 50% of the planets to 30%. Whether SIM should observer 60 or 240 stars, will be aided by the results of the Kepler mission which will provide statistics on the frequency of terrestrial-mass planets around solar type stars. By determining the orbital phase of the planet, SIM will be able to assist TPF-C by telling it when to look to ensure that the planet will be outside the TPF-C 62 mas inner working angle. Furthermore, the masses determined by SIM will not suffer from the msini ambiguity inherent in radial velocity surveys. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tanner, AM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP 26847 EP 26847 AR 626847 DI 10.1117/12.671877 PG 6 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800135 ER PT S AU Lay, OP AF Lay, Oliver P. BE Monnier, JD Scholler, M Danchi, WC TI Removing instability noise in nulling interferometers - art. no. 62681A SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE optical interferometry; nulling; planet detection ID SYSTEMATIC-ERRORS; PLANETS AB The NASA Terrestrial Planet Finder Interferometer (TPF-I) and ESA Darwin missions are designed to directly detect mid-infrared photons from earth-like planets around nearby stars. The technique of nulling interferometry is used to suppress the light from the parent star, typically 107 times brighter than the planet, with an angular offset of 10-100 mas. There are two classes of noise: photon shot noise from the stellar leakage, local- and exo-zodiacal dust, and instability noise from variations in the instrument response. Shot noise requires that the instrument null depth is at least 10(-5). The instability noise requires a null depth of similar to 10(-6), corresponding to control of the optical paths at similar to 1 nm rms, and control of relative intensities at similar to 0.2%; it is these requirements that currently drive the design of the instrument. This paper describes a new technique that effectively removes the effect of instability noise. This relaxes the nulling requirement by a factor similar to 10 and makes planet detection robust to instrument variations. At the same time, the integration period needed to detect and characterize planets is reduced and the angular resolution of the array is significantly improved. Analysis and simulations are presented, and implications for the array architecture are discussed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lay, OP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 11 TC 6 Z9 6 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP A2681 EP A2681 AR 62681A DI 10.1117/12.670603 PG 13 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800044 ER PT S AU Pan, XP AF Pan, Xiaopei BE Monnier, JD Scholler, M Danchi, WC TI Analysis of calibration errors for both short and long stroke white light experiments - art. no. 62684B SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE space interferometry; white light fringe; bias calibration AB The SIM PlanetQuest mission can provide microarcsecond (mu as) accuracy for exoplanet searches and critical astrophysical research. SIM is the only mission which can measure angular wobbles caused by planets for determination of planetary masses. In order to reach mu as accuracy the SIM instrument must be able to measure fringe parameters to the accuracy of picometers. It is necessary to investigate calibration techniques and to carefully analyze influences from ghost images in white light fringe measurements. This work will analyze focusing and tilt variations introduced by thermal changes in calibration processes. In particular the accuracy limits are presented for common short- and long-stroke experiments. A new, simple, practical calibration scheme is proposed and analyzed based on the SIM PlanetQuest's Micro-Arcsecond Metrology (MAM) testbed experiments. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pan, XP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 7 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP B2684 EP B2684 AR 62684B DI 10.1117/12.669849 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800139 ER PT S AU Peters, RD Lay, OP Hirai, A Jeganathan, M AF Peters, Robert D. Lay, Oliver P. Hirai, Akiko Jeganathan, Muthu BE Monnier, JD Scholler, M Danchi, WC TI Adaptive nulling for the terrestrial planet finder interferometer - art. no. 62681C SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE nulling interferometry; planet detection; deformable mirror; dispersion compensator; nulling; amplitude and phase correction; adaptive nuller AB Deep, stable starlight nulls are needed for the direct detection of Earth-like planets and require careful control of the intensity and phases of the beams that are being combined. We are testing a novel compensator based on a deformable mirror to correct the intensity and phase at each wavelength and polarization across the nulling bandwidth. We have successfully demonstrated intensity and phase control using a deformable mirror across a 100nm wide band in the near-IR, and are in the process of conducting experiments in the mid-IR wavelengths. This paper covers the current results and in the mid-IR. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Peters, RD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP C2681 EP C2681 AR 62681C DI 10.1117/12.672170 PG 7 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800046 ER PT S AU Tang, H Zhao, F AF Tang, Hong Zhao, Feng BE Monnier, JD Scholler, M Danchi, WC TI An analysis of the phase dispersion in the symmetric beam combiner - art. no. 62683F SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE beam combiner; beamsplitter; coatings; dispersion; retardance AB An astronomical beam combiner combines the two beams of starlight to form white-light fringes. It is desirable that the dispersion of the beam combiner be minimized across the observation wavelength range. We present here an analysis of the phase dispersion from coatings for a symmetric beam combiner. The sensitivity of the dispersion to a slight mismatch in beamsplitter coatings is also studied. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tang, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 2 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP F2683 EP F2683 AR 62683F DI 10.1117/12.674156 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800111 ER PT S AU Demers, RT An, X Tang, H Rud, M Kissil, A Kwack, EY AF Demers, Richard T. An, Xin Tang, Hong Rud, Mayer Kissil, Andrew Kwack, Eug-Yun BE Monnier, JD Scholler, M Danchi, WC TI Demonstration of spectral calibration for stellar interferometry - art. no. 62682H SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon AB A breadboard is under development to demonstrate the calibration of spectral errors in microarcsecond stellar interferometers. Analysis shows that thermally and mechanically stable hardware in addition to careful optical design can reduce the wavelength dependent error to tens of nanometers. Calibration of the hardware can further reduce the error to the level of picometers. The results of thermal, mechanical and optical analysis supporting the breadboard design will be shown. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Demers, RT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 171-113, Pasadena, CA 91109 USA. NR 1 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP H2682 EP H2682 AR 62682H DI 10.1117/12.672604 PG 9 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800079 ER PT S AU Kuan, GM Dekens, FG AF Kuan, Gary M. Dekens, Frank G. BE Monnier, JD Scholler, M Danchi, WC TI Picometer level modeling of a shared vertex double corner cube in the Space Interferometry Mission kite testbed - art. no. 62682L SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE picometer metrology; interferomety; optical interferometer; corner cube; SIM; Space Interferometry Mission; calibration; modeling ID EXTERNAL METROLOGY; SIM AB The Space Interferometry Mission (SIM) is a microarcsecond interferometric space telescope that requires picometer level precision measurements of its truss and interferometer baselines. Single-gauge metrology errors due to non-ideal physical characteristics of corner cubes reduce the angular measurement capability of the science instrument. Specifically, the non-common vertex error (NCVE) of a shared vertex, double corner cube introduces micrometer level single-gauge errors in addition to errors due to dihedral angles and reflection phase shifts. A modified SIM Kite Testbed containing an articulating double corner cube is modeled and the results are compared to the experimental testbed data. The results confirm modeling capability and viability of calibration techniques. C1 CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Kuan, GM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP L2682 EP L2682 AR 62682L DI 10.1117/12.672489 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800083 ER PT S AU Booth, AJ Colavita, MM Garcia, JI Koresko, C AF Booth, Andrew J. Colavita, M. Mark Garcia, Jean I. Koresko, Chris BE Monnier, JD Scholler, M Danchi, WC TI The control system for the Keck interferometer nuller - art. no. 62681M SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE interferometry; nulling; real time control ID PALOMAR TESTBED INTERFEROMETER AB The Keck Interferometer links the two 10m Keck Telescopes located atop Mauna Kea in Hawaii. It was the first 10m class, fully AO equipped interferometer to enter operation. Further, it is the first large interferometer to implement a nuller, whereby the on axis light from a bright point source (e.g. a star) can be removed interferometrically, allowing study of light from nearby, low contrast sources (e.g. exo-zodiacal dust). This paper describes the control system we have implemented to enable operation of the Keck interferometer nuller. We give a general overview of the control system, plus details of how control differs from the already implemented and operational, standard visibility science mode of the interferometer. The nuller is challenging in its requirements for control because of the necessary control precision and the complexity of the number of points of control. We have implemented some novel control methods to meet these requirements and we describe those here. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Booth, AJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 13 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP M2681 EP M2681 AR 62681M DI 10.1117/12.664522 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800054 ER PT S AU Zhai, CX Milman, M Regehr, M AF Zhai, Chengxing Milman, Mark Regehr, Martin BE Monnier, JD Scholler, M Danchi, WC TI The least-squares calibration on the micro-arcsecond metrology test bed - art. no. 62682N SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE interferometry; calibration; estimation; least-squares AB The Space Interferometry Mission(SIM) will measure optical path differences (OPDs) with an accuracy of tens of picometers, requiring precise calibration of the instrument. In this article, we present a calibration approach based on fitting star light interference fringes in the interferometer using a least-squares algorithm. The algorithm is first analyzed for the case of a monochromatic light source with a monochromatic fringe model. Using fringe data measured on the Micro-Arcsecond Metrology(MAM) testbed with a laser source, the error in the determination of the wavelength is shown to be less than 10pm. By using a quasi-monochromatic fringe model, the algorithm can be extended to the case of a white light source with a narrow detection bandwidth. In SIM, because of the finite bandwidth of each CCD pixel, the effect of the fringe envelope can not be neglected, especially for the larger optical path difference range favored for the wavelength calibration. We eliminate the fringe envelope effect by "projecting away" the fringe envelope, i.e. working in a subspace orthogonal to the envelope signal. The resulting fringe envelope parameters are needed for subsequent OPD estimation in SIM. We show the sensitivities to various errors. The algorithm is validated using both simulation and the fringe data obtained on the MAM test bed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zhai, CX (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP N2682 EP N2682 AR 62682N DI 10.1117/12.670091 PG 14 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800085 ER PT S AU Wang, X Korechoff, R Heflin, M Sievers, L AF Wang, Xu Korechoff, Robert Heflin, Mike Sievers, Lisa BE Monnier, JD Scholler, M Danchi, WC TI Corner cube model for internal metrology system of Space Interferometer Mission (SIM) - art. no. 62682P SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE corner cube; laser metrology; picometer metrology; and interferometer AB A corner cube (CC) articulation model has been developed to evaluate the SIM internal metrology (IntMet) optical delay bias (with the accuracy of picometer) due to the component imperfections, such as vertex offset, reflection coating index error, dihedral error, and surface figure error at each facet. This physics-based and MATLAB-implemented geometric optics model provides useful guidance on the flight system design, integration, and characterization. The first portion of this paper covers the CC model details. Then several feature of the model, such as metrology beam footprint visualization, roofline straddling/crossing analysis, and application to drive the sub-system design and the error budget flow-down, are demonstrated in the second part. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wang, X (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 6 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP P2682 EP P2682 AR 62682P DI 10.1117/12.670105 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800087 ER PT S AU Nemati, B AF Nemati, Bijan BE Monnier, JD Scholler, M Danchi, WC TI SIM PlanetQuest: Status and recent progress - art. no. 62680Q SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE SIM; interferometry; astrometry; metrology AB SIM PlanetQuest will investigate, using stellar interferometry from space, a broad range of topics in astronomy and astrophysics. Chief among its scientific goals is a search of nearby stars for terrestrial planets in the circumstellar habitable zone. Composed of three astrometric interferometers each capable of resolving approximately one billionth of a degree, SIM is poised to revolutionize our understanding of the Universe in a number of areas. With the completion of its technology development phase, SIM is now on a sure footing for the development of requirements for the flight instrument. The preliminary design of SIM is in place and many key brassboards have been built. Here we review the project status and recent progress. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Nemati, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 301-486, Pasadena, CA 91109 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP Q2680 EP Q2680 AR 62680Q DI 10.1117/12.665678 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800025 ER PT S AU Traub, WA Levine, M Shaklan, S Kasting, J Angel, JR Brown, ME Brown, RA Burrows, C Clampin, M Dressler, A Ferguson, HC Hammel, HB Heap, SR Horner, SD Illingworth, GD Kasdin, NJ Kuchner, MJ Lin, D Marley, MS Meadows, V Noecker, C Oppenheimer, BR Seager, S Shao, M Stapelfeldt, KR Trauger, JT AF Traub, Wesley A. Levine, Marie Shaklan, Stuart Kasting, James Angel, J. Roger Brown, Michael E. Brown, Robert A. Burrows, Christopher Clampin, Mark Dressler, Alan Ferguson, Henry C. Hammel, Heidi B. Heap, Sara R. Horner, Scott D. Illingworth, Garth D. Kasdin, N. Jeremy Kuchner, Mark J. Lin, Douglas Marley, Mark S. Meadows, Victoria Noecker, Charley Oppenheimer, Ben R. Seager, Sara Shao, Michael Stapelfeldt, Karl R. Trauger, John T. BE Monnier, JD Scholler, M Danchi, WC TI TPF-C: Status and recent progress - art. no. 62680T SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE Terrestrial Planet Finder Coronagraph; TPF; TPF-C; exoplanets; extrasolar planets AB The Terrestrial Planet Finder Coronagraph (TPF-C) is a deep space mission designed to detect and characterize Earth-like planets around nearby stars. TPF-C will be able to search for signs of life on these planets. TPF-C will use spectroscopy to measure basic properties including the presence of water or oxygen in the atmosphere, powerful signatures in the search for habitable worlds. This capability to characterize planets is what allows TPF-C to transcend other astronomy projects and become an historical endeavor on a par with the discovery voyages of the great navigators. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Traub, WA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Clampin, mark/D-2738-2012; Stapelfeldt, Karl/D-2721-2012; Kuchner, Marc/E-2288-2012; Marley, Mark/I-4704-2013 NR 2 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP T2680 EP T2680 AR 62680T DI 10.1117/12.673608 PG 14 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800028 ER PT S AU Lawson, PR Cotton, WD Hummel, CA Baron, F Young, JS Kraus, S Hofmann, KH Weigelt, GP Ireland, M Monnier, JD Thiebaut, E Rengaswamy, S Chesneau, O AF Lawson, Peter R. Cotton, William D. Hummel, Christian A. Baron, Fabien Young, John S. Kraus, Stefan Hofmann, Karl-Heinz Weigelt, Gerd P. Ireland, Michael Monnier, John D. Thiebaut, Eric Rengaswamy, Sridharan Chesneau, Olivier BE Monnier, JD Scholler, M Danchi, WC TI 2006 Interferometry Imaging Beauty Contest - art. no. 62681U SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE Astronomical software; closure phase; aperture synthesis; imaging; optical; infrared; interferometry AB We present a formal comparison of the performance of algorithms used for synthesis imaging with optical/infrared long-baseline interferometers. Five different algorithms are evaluated based on their performance with simulated test data. Each set of test data is formatted in the OI-FITS format. The data are calibrated power spectra and bispectra measured with an array intended to be typical of existing imaging interferometers. The strengths and limitations of each algorithm are discussed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Lawson, PR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. OI Young, John/0000-0001-6583-7643 NR 8 TC 11 Z9 11 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP U2681 EP U2681 AR 62681U DI 10.1117/12.670409 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800061 ER PT S AU Crawford, SL Ragland, S Booth, A Colavita, MM Hovland, E AF Crawford, S. L. Ragland, S. Booth, A. Colavita, M. M. Hovland, E. BE Monnier, JD Scholler, M Danchi, WC TI Design and performance of the Keck angle tracker - art. no. 62683W SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE angle tracking; stellar interferometer; adaptive optics; infrared detectors ID LOW-TEMPERATURES; ZNSE AB The Keck Angle Tracker (KAT) is a key subsystem in the NASA-funded Keck Interferometer at the Keck Observatory on the summit of Mauna Kea in Hawaii. KAT, which has been in operation since the achievement of first fringes in March 2001, senses the tilt of the stellar wavefront for each of the beams from the interferometer telescopes and provides tilt error signals to fast tip/tilt mirrors for high-bandwidth, wavefront tilt correction. In addition, KAT passes low-bandwidth, desaturation offsets to the adaptive optics system of the Keck telescopes to correct for slow pointing drifts. We present an overview of the instrument design and recent performance of KAT in support of the V-2 science and nulling observing modes of the Keck Interferometer. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Crawford, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP W2683 EP W2683 AR 62683W DI 10.1117/12.672063 PG 9 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800126 ER PT S AU Vasisht, G Ligon, ER Bloemhof, EE Colavita, MM AF Vasisht, Gautam Ligon, E. Robert Bloemhof, Erik. E. Colavita, M. Mark BE Monnier, JD Scholler, M Danchi, WC TI Picometer differential-phase measurements in the laboratory - art. no. 62682X SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE stellar interferometry; differential phase; fringe tracking ID INTERFEROMETER AB We describe the results of laboratory experiments, using a mock-up stellar interferometer equipped with specialized hardware, undertaken to measure differential-phase to considerable precision (0.1 mrad) over an octave of bandwidth in the infrared. Differential-phase is a precision technique that can detect subtle temporal changes in the relative (color-dependent) photocenter of an astronomical target - making it useful for direct detection of some hot-Jupiter planets from the ground. The set up described herein was built as part of the Keck Interferometer project. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vasisht, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 7 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP X2682 EP X2682 AR 62682X DI 10.1117/12.672619 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800094 ER PT S AU Shao, M AF Shao, Michael BE Monnier, JD Scholler, M Danchi, WC TI Search for terrestrial planets with SIM planet quest - art. no. 62681Z SO Advances in Stellar Interferometry Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advances in Stellar Interferometry CY MAY 25-30, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE exoplanets; terrestrial planets; astrometry; interferometry AB SIM is an astrometric mission that will be capable of 1 microarcsec relative astrometric accuracy in a single measurement of similar to 1000 sec. The search for terrestrial planets in the habitable zone around nearby stars is one of the main science goals of the project. In 2001, NASA through the peer review process selected 10 key projects, two of which had as its goal, the search for terrestrial planets around nearby stars. The two teams, one led by G. Marcy (UC Berkeley) and one lead by M. Shao (JPL), have an extensive preparatory science program underway. This paper describes the status of this activity as well as the technology status of SIM's narrow angle astrometry capability, to reach 1 uas in a single epoch measure and its ability to average multiple epoch measurements to well below I uas. C1 CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Shao, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. NR 0 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 0-8194-6333-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6268 BP Z2681 EP Z2681 AR 62681Z DI 10.1117/12.671898 PG 6 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BEZ48 UT WOS:000240312800063 ER PT S AU Usabiaga, J Erol, A Bebis, G Boyle, R Twombly, X AF Usabiaga, Jorge Erol, Ali Bebis, George Boyle, Richard Twombly, Xander BE Bebis, G Boyle, R Parvin, B Koracin, D Remagnino, P Nefian, A Meenakshisundaram, G Pascucci, V Zara, J Molineros, J Theisel, H Malzbender, T TI Global hand pose estimation by multiple camera ellipse tracking SO Advances in Visual Computing, Pt 1 SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Proceedings Paper CT 2nd International Symposium on Visual Computing CY NOV 06-08, 2006 CL Lake Tahoe, NV SP UNR Comp Vis Lab, Desert Res Inst, NASA, Siemens, Intel, DigitalPersona, Equinox Corp, HP, nVIDA, Ford Corp, Mitsubish, UtopiaCompression AB Immersive virtual environments with life-like interaction capabilities have very demanding requirements including high precision and processing speed. These issues raise many challenges for computer vision-based motion estimation algorithms. In this study, we consider the problem of hand tracking using multiple cameras and estimating its 3D global pose (i.e., position and orientation of the palm). Our interest is in developing an accurate and robust algorithm to be employed in an immersive virtual training environment, called "Virtual GloveboX" (VGX) [1], which is currently under development at NASA Ames. In this context, we present a marker-based, hand tracking and 3D global pose estimation algorithm that operates in a controlled, multi-camera, environment built to track the user's hand inside VGX. The key idea of the proposed algorithm is tracking the 3D position and orientation of an elliptical marker placed on the dorsal part of the hand using model-based tracking approaches and active camera selection. It should be noted that, the use of markers is well justified in the context of our application since VGX naturally allows for the use of gloves without disrupting the fidelity of the interaction. Our experimental results and comparisons illustrate that the proposed approach is more accurate and robust than related approaches. A byproduct of our multi-camera ellipse tracking algorithm is that, with only minor modifications, the same algorithm can be used to automatically re-calibrate (i.e., fine-tune) the extrinsic parameters of a multi-camera system leading to more accurate pose estimates. C1 Univ Nevada, Comp Vis Lab, Reno, NV 89557 USA. NASA, Ames Res Ctr, BioVis Lab, Moffett Field, CA 94035 USA. RP Usabiaga, J (reprint author), Univ Nevada, Comp Vis Lab, Reno, NV 89557 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-48628-3 J9 LECT NOTES COMPUT SC PY 2006 VL 4291 BP 122 EP 132 PG 11 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BFN03 UT WOS:000243131500013 ER PT S AU Twombly, X Boyle, R Colombano, S AF Twombly, Xander Boyle, Richard Colombano, Silvano BE Bebis, G Boyle, R Parvin, B Koracin, D Remagnino, P Nefian, A Meenakshisundaram, G Pascucci, V Zara, J Molineros, J Theisel, H Malzbender, T TI Active stabilization of images acquired on a walking robotic platform SO ADVANCES IN VISUAL COMPUTING, PT 2 SE Lecture Notes in Computer Science LA English DT Proceedings Paper CT 2nd International Symposium on Visual Computing CY NOV 06-08, 2006 CL Lake Tahoe, NV SP UNR Comp Vis Lab, Desert Res Inst, NASA, Siemens, Intel, DigitalPersona, Equinox Corp, HP, nVIDA, Ford Corp, Mitsubish, UtopiaCompression ID INERTIAL MOTION; OTOLITH; ORIENTATION; MODEL; TILT; CUES AB To increase the quality of scientific data collected from autonomous mobile agents such as rovers and walking robotic devices, biological methods can be mimicked for better navigation and balance control of both the agent itself and the manipulation of scientific instruments. Drawing on the design of the neuro-vestibular control system, the EarBot controller is designed to stabilize a multi-axis camera system mounted atop a moving agent. An eight-legged robot called the SCORPION, designed to navigate and explore rough terrain considered inhospitable to wheeled rovers, is used as the testbed to analyze the EarBot's functionality and behavior. Eventually, the EarBot will be used to control the balance the robot itself through expanded modelling of the vestibulo-motor control loops used in postural control. This paper presents the theoretical concepts and initial controller implementations for stabilizing the camera during walking motion of the SCORPION. C1 [Twombly, Xander; Boyle, Richard; Colombano, Silvano] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Twombly, X (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM xtwombly@mail.arc.nasa.gov; Richard.Boyle@nasa.gov; Silvano.P.Colombano@nasa.gov NR 9 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 J9 LECT NOTES COMPUT SC PY 2006 VL 4292 BP 851 EP + PG 2 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BFN05 UT WOS:000243132300085 ER PT B AU Uttley, P AF Uttley, Philip BE Gaskell, CM McHardy, IM Peterson, BM Sergeev, SG TI The relationship between optical and X-ray variability in Seyfert galaxies SO AGN Variability From X-Rays to Radio Waves SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Acative Galactic Nuclei Variability from X-rays to Radio Waves CY JUN 14-16, 2004 CL Crimean Astrophys Observ, Crimea, UKRAINE HO Crimean Astrophys Observ ID ACTIVE GALACTIC NUCLEI; ULTRAVIOLET VARIABILITY; XMM-NEWTON; NGC 3516; LINE; EMISSION; NGC-4051; NGC-5548; RXTE; LONG AB Studying simultaneous optical and X-ray light curves of radioquiet AGN can help to probe the relationship between very different physical components - the cool, optically thick disk and hot, optically thin corona. Here, we review the relationship between optical and X-ray variability in Seyfert galaxies, which due to observing constraints was difficult to study for many years, but was given a huge boost with the launch of the RXTE satellite in 1995. We summarise the diverse results of several monitoring campaigns, which pose a challenge for standard theories relating optical and X-ray variability, with sources showing either correlated optical and X-ray flux variations, correlated optical flux and X-ray spectral variations, or no correlation at all. We discuss possible explanations for these results, some of which may be explained using a more standard AGN picture, while others may require additional components, such as the 2-phase accretion flows suggested to explain black hole X-ray binary behavior. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20815 USA. RP Uttley, P (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20815 USA. NR 23 TC 8 Z9 8 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-28-0 J9 ASTR SOC P PY 2006 VL 360 BP 101 EP 110 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGF83 UT WOS:000246502800019 ER PT B AU Stoica, A Ramesham, R Zebulum, RS Neff, J Keymeulen, D Katkoori, S AF Stoica, Adrian Ramesham, Rajeshuni Zebulum, Ricardo S. Neff, Joseph Keymeulen, Didier Katkoori, Srinivas BE Stoica, A Arslan, T Suess, M Yalcin, S Keymeulen, D Higuchi, T Zebulum, R Aydin, N TI Temperature-adaptive circuits on reconfigurable analog arrays SO AHS 2006: FIRST NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND SYSTEMS, PROCEEDINGS LA English DT Proceedings Paper CT 1st NASA/ESA Conference on Adaptive Hardware and Systems CY JUN 15-18, 2006 CL Bahcesehir Univ, Istanbul, TURKEY SP NASA Jet Propuls Lab, European Space Agcy, Tech Res Council Turkey, Bio-Inspired Technol & Syst, Univ Edinburgh, Inst Syst Level Integrat, Spiral Gateway Ltd, European Ctr Secure Informat & Syst, Uk, IEEE Working Grp Evolvable Hardware HO Bahcesehir Univ AB This paper describes a new reconfigurable analog array (RAA) architecture and integrated circuit (IC) used to map analog circuits that can adapt to extreme temperatures under programmable control. Algorithm-driven adaptation takes place on the RAA IC. The algorithms are implemented in a separate Field Programmable Gate Array (FPGA) IC, co-located with the RAA in the extreme temperature environment. The experiments demonstrate circuit adaptation over a wide temperature range, from extremely low temperature of -180 degrees C to high 120 degrees. C1 [Stoica, Adrian; Ramesham, Rajeshuni; Zebulum, Ricardo S.; Keymeulen, Didier] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Neff, Joseph] SPAWAR, San Diego, CA 92103 USA. [Katkoori, Srinivas] Univ S Florida, Tampa, FL 33620 USA. RP Stoica, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM adrian.stoica@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA) FX The work described in this chapter was performed at the Jet Propulsion Laboratory, California Institute of Technology, and was sponsored by the National Aeronautics and Space Administration (NASA). NASA Program Managers for the effort are Drs. Chris Moore, Mita Desai, and Michael Watson. NR 9 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2614-4 PY 2006 BP 28 EP + PG 2 WC Computer Science, Hardware & Architecture SC Computer Science GA BEQ55 UT WOS:000238918600005 ER PT B AU Stefatos, EF Arslan, T Keymeulen, D Ferguson, I AF Stefatos, Evangelos F. Arslan, Tughrul Keymeulen, Didier Ferguson, Ian BE Stoica, A Arslan, T Suess, M Yalcin, S Keymeulen, D Higuchi, T Zebulum, R Aydin, N TI Towards the integration of drive control loop electronics of the JPL/Boeing gyroscope within an autonomous robust custom-reconfigurable platform SO AHS 2006: FIRST NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND SYSTEMS, PROCEEDINGS LA English DT Proceedings Paper CT 1st NASA/ESA Conference on Adaptive Hardware and Systems CY JUN 15-18, 2006 CL Bahcesehir Univ, Istanbul, TURKEY SP NASA Jet Propuls Lab, European Space Agcy, Tech Res Council Turkey, Bio-Inspired Technol & Syst, Univ Edinburgh, Inst Syst Level Integrat, Spiral Gateway Ltd, European Ctr Secure Informat & Syst, Uk, IEEE Working Grp Evolvable Hardware HO Bahcesehir Univ AB This paper presents an autonomous architecture for the implementation of the JPL/Boeing gyroscope. The central point of the architecture is a unified reconfigurable fabric, which integrates two custom especially tailored reconfigurable units. The former fabric enables the reconfiguration of integer based computations, whereas the later deals with those requiring fractional accuracy. The architecture employs a number of other techniques such as primitive operators and a hybrid evolutionary strategy in order to allow the real-time adaptation of high quality circuits with low power consumption and high degree of fault-tolerance. Simulation results prove that our proposed architecture is able to adapt, in the presence of Single-Hard-Errors, the functionality of high-order Finite-Impulse-Respnse filters and Proportional-Integral controllers very efficiently in terms of speed, accuracy and hardware utilization. Power analysis demonstrates the near ASIC performance of our architecture. C1 [Stefatos, Evangelos F.; Arslan, Tughrul] Univ Edinburgh, Sch Engn & Elect, Kings Bldg,Mayfield Rd, Edinburgh EH9 3JL, Midlothian, Scotland. [Keymeulen, Didier; Ferguson, Ian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Stefatos, EF (reprint author), Univ Edinburgh, Sch Engn & Elect, Kings Bldg,Mayfield Rd, Edinburgh EH9 3JL, Midlothian, Scotland. EM Evangelos.Stefatos@ee.ed.ac.uk; Didler.Keymeulen@jpl.nasa.gov NR 7 TC 1 Z9 1 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2614-4 PY 2006 BP 207 EP + PG 2 WC Computer Science, Hardware & Architecture SC Computer Science GA BEQ55 UT WOS:000238918600029 ER PT B AU Baloch, S Arslan, T Stoica, A AF Baloch, Sajid Arslan, Tughrul Stoica, Adrian BE Stoica, A Arslan, T Suess, M Yalcin, S Keymeulen, D Higuchi, T Zebulum, R Aydin, N TI Embedded reconfigurable array fabrics for efficient implementation of image compression techniques SO AHS 2006: FIRST NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND SYSTEMS, PROCEEDINGS LA English DT Proceedings Paper CT 1st NASA/ESA Conference on Adaptive Hardware and Systems CY JUN 15-18, 2006 CL Bahcesehir Univ, Istanbul, TURKEY SP NASA Jet Propuls Lab, European Space Agcy, Tech Res Council Turkey, Bio-Inspired Technol & Syst, Univ Edinburgh, Inst Syst Level Integrat, Spiral Gateway Ltd, European Ctr Secure Informat & Syst, Uk, IEEE Working Grp Evolvable Hardware HO Bahcesehir Univ AB The discrete wavelet Transform (DWT), as defined by the Image Compression Standard JPEG-2000, is one of the most time-consuming computations which cannot be efficiently executed on current hardware architectures. This paper presents and compares a number of new, different architectures for domain-specific arrays to efficiently implement various DWT algorithms. A number of different algorithms are mapped to demonstrate the flexibility of these new embedded configurable SoC architectures and their ability to support different implementations having different performance characteristics. Our results demonstrate up to 59 percent improvement to the previous work in literature. C1 [Baloch, Sajid; Arslan, Tughrul; Stoica, Adrian] Univ Edinburgh, Sch Elect & Engn, Kings Bldg,Mayfield Rd, Edinburgh EH9 3JL, Midlothian, Scotland. [Baloch, Sajid; Arslan, Tughrul] Inst Syst Level Integrat, Alba Ctr, Livingston EH54 7EG, Scotland. [Stoica, Adrian] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Baloch, S (reprint author), Univ Edinburgh, Sch Elect & Engn, Kings Bldg,Mayfield Rd, Edinburgh EH9 3JL, Midlothian, Scotland. NR 11 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2614-4 PY 2006 BP 270 EP + PG 3 WC Computer Science, Hardware & Architecture SC Computer Science GA BEQ55 UT WOS:000238918600038 ER PT B AU Baloch, S Arslan, T Stoica, A AF Baloch, Sajid Arslan, Tughrul Stoica, Adrian BE Stoica, A Arslan, T Suess, M Yalcin, S Keymeulen, D Higuchi, T Zebulum, R Aydin, N TI An efficient technique for preventing single event disruptions in synchronous and reconfigurable architectures SO AHS 2006: FIRST NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND SYSTEMS, PROCEEDINGS LA English DT Proceedings Paper CT 1st NASA/ESA Conference on Adaptive Hardware and Systems CY JUN 15-18, 2006 CL Bahcesehir Univ, Istanbul, TURKEY SP NASA Jet Propuls Lab, European Space Agcy, Tech Res Council Turkey, Bio-Inspired Technol & Syst, Univ Edinburgh, Inst Syst Level Integrat, Spiral Gateway Ltd, European Ctr Secure Informat & Syst, Uk, IEEE Working Grp Evolvable Hardware HO Bahcesehir Univ AB This paper presents a unique SEU (single Event Upset) mitigation technique based upon Temporal Data Sampling for synchronous circuits and configuration bit storage for programmable devices. The design technique addresses both conventional static SEUs and SETs (Single Event Transients) induced errors that can result in data loss for any synchronous and reconfigurable architecture. The proposed scheme may be employed in circuits to eliminate all SEUs and SETs for performance critical applications.. This approach permits FPGAs and other microcircuits with deep submicron feature size to be used in hostile space environments. Results included show that the proposed scheme is approximately 55% area and 63% power efficient than previously introduced schemes. C1 [Baloch, Sajid; Arslan, Tughrul; Stoica, Adrian] Univ Edinburgh, Sch Elect & Engn, Kings Bldg,Mayfield Rd, Edinburgh EH9 3JL, Midlothian, Scotland. [Baloch, Sajid; Arslan, Tughrul] Inst Syst Level Integrat, Alba Ctr, Livingston EH54 7EG, Scotland. [Stoica, Adrian] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Baloch, S (reprint author), Univ Edinburgh, Sch Elect & Engn, Kings Bldg,Mayfield Rd, Edinburgh EH9 3JL, Midlothian, Scotland. NR 12 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2614-4 PY 2006 BP 292 EP + PG 2 WC Computer Science, Hardware & Architecture SC Computer Science GA BEQ55 UT WOS:000238918600041 ER PT B AU Keymeulen, D Zebulum, R Rajeshuni, R Stoica, A Katkoori, S Graves, S Novak, F Antill, C AF Keymeulen, Didier Zebulum, Ricardo Rajeshuni, Ramesham Stoica, Adrian Katkoori, Srinivas Graves, Sharon Novak, Frank Antill, Charles BE Stoica, A Arslan, T Suess, M Yalcin, S Keymeulen, D Higuchi, T Zebulum, R Aydin, N TI Self-adaptive system based on field programmable gate array for extreme temperature electronics SO AHS 2006: FIRST NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND SYSTEMS, PROCEEDINGS LA English DT Proceedings Paper CT 1st NASA/ESA Conference on Adaptive Hardware and Systems CY JUN 15-18, 2006 CL Bahcesehir Univ, Istanbul, TURKEY SP NASA Jet Propuls Lab, European Space Agcy, Tech Res Council Turkey, Bio-Inspired Technol & Syst, Univ Edinburgh, Inst Syst Level Integrat, Spiral Gateway Ltd, European Ctr Secure Informat & Syst, Uk, IEEE Working Grp Evolvable Hardware HO Bahcesehir Univ AB Space missions often require radiation and extreme-temperature hardened electronics to survive the harsh environments beyond earth's atmosphere. Traditional approaches to preserve electronics incorporate radiation shielding, insulation and redundancy at the expense of power and weight. In this work, we report the implementation of a self-adaptive system using a field programmable gate array (FPGA) and data converters. The self-adaptive system can autonomously recover the lost functionality of a reconfigurable analog array (RAA) integrated circuit (IC) [3]. Both the RAA IC and the self-adaptive system are operating in extreme temperatures (from 120 degrees C down to -180 degrees C). The RAA IC consists of reconfigurable analog blocks interconnected by several switches and programmable by bias voltages. It implements filters/amplifiers with bandwidth up to 20 MHz. The self-adaptive system controls the RAA IC and is realized on Commercial-Off-The-Shelf (COTS) parts. It implements a basic compensation algorithm that corrects a RAA IC in less than a few milliseconds. Experimental results for the cold temperature environment (down to -180 degrees C) demonstrate the feasibility of this approach. C1 [Keymeulen, Didier; Zebulum, Ricardo; Rajeshuni, Ramesham; Stoica, Adrian] NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Katkoori, Srinivas] Univ S Florida, CSE Dept, Tampa, FL 33620 USA. [Graves, Sharon; Novak, Frank; Antill, Charles] NASA, LaRC, Hampton, VA 23681 USA. RP Keymeulen, D (reprint author), NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM didier.keymeulen@jpl.nasa.gov; katkoori@cse.usf.edu; Sharon.s.graves@nasa.gov FU National Aeronautics and Space Administration (NASA); NASA Marshall Space Flight Center; NASA Program FX The work described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, and NASA Langley Research Center and was sponsored by the National Aeronautics and Space Administration (NASA). We are grateful for encouragement and support from Project Manager Dr. Michael Watson from NASA Marshall Space Flight Center, and NASA Program Managers Dr. Mita Desai and Dr. Chris Moore. NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2614-4 PY 2006 BP 296 EP + PG 2 WC Computer Science, Hardware & Architecture SC Computer Science GA BEQ55 UT WOS:000238918600042 ER PT B AU Chau, S Dang, V Xu, J Lu, J AF Chau, Savio Dang, Van Xu, Joseph Lu, James BE Stoica, A Arslan, T Suess, M Yalcin, S Keymeulen, D Higuchi, T Zebulum, R Aydin, N TI An automatic technique to synthesize Avionics Architecture SO AHS 2006: FIRST NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND SYSTEMS, PROCEEDINGS LA English DT Proceedings Paper CT 1st NASA/ESA Conference on Adaptive Hardware and Systems CY JUN 15-18, 2006 CL Bahcesehir Univ, Istanbul, TURKEY SP NASA Jet Propuls Lab, European Space Agcy, Tech Res Council Turkey, Bio-Inspired Technol & Syst, Univ Edinburgh, Inst Syst Level Integrat, Spiral Gateway Ltd, European Ctr Secure Informat & Syst, Uk, IEEE Working Grp Evolvable Hardware HO Bahcesehir Univ AB In conventional avionics system design process, changing the avionics system architecture involves a large team of engineers and requires months to years of redesign time. This paper describes the Avionics Architecture Tool (AST) developed by JPL that can automatically synthesize architecture for the avionics-system-on-a-chip. As the synthesis is based on Genetic Algorithm and driven by requirements that are imposed by the environment, the synthesized architecture can quickly adapt to environmental changes. Furthermore, the AST can also guarantee that the synthesized architecture is viable and workable through the use of Viability Tree. C1 [Chau, Savio; Dang, Van] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Xu, Joseph; Lu, James] Univ Michigan, Ann Arbor, MI 48109 USA. RP Chau, S (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM savio.n.chau@jpl.nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2614-4 PY 2006 BP 313 EP + PG 2 WC Computer Science, Hardware & Architecture SC Computer Science GA BEQ55 UT WOS:000238918600046 ER PT B AU Arslan, T Haridas, N Yang, E Erdogan, AT Barton, N Walton, AJ Thompson, JS Stoica, A Vladimirova, T McDonald-Maier, KD Howells, WGJ AF Arslan, T. Haridas, N. Yang, E. Erdogan, A. T. Barton, N. Walton, A. J. Thompson, J. S. Stoica, A. Vladimirova, T. McDonald-Maier, K. D. Howells, W. G. J. BE Stoica, A Arslan, T Suess, M Yalcin, S Keymeulen, D Higuchi, T Zebulum, R Aydin, N TI ESPACENET: A framework of evolvable and reconfigurable sensor networks for aerospace-based monitoring and diagnostics SO AHS 2006: FIRST NASA/ESA CONFERENCE ON ADAPTIVE HARDWARE AND SYSTEMS, PROCEEDINGS LA English DT Proceedings Paper CT 1st NASA/ESA Conference on Adaptive Hardware and Systems CY JUN 15-18, 2006 CL Bahcesehir Univ, Istanbul, TURKEY SP NASA Jet Propuls Lab, European Space Agcy, Tech Res Council Turkey, Bio-Inspired Technol & Syst, Univ Edinburgh, Inst Syst Level Integrat, Spiral Gateway Ltd, European Ctr Secure Informat & Syst, Uk, IEEE Working Grp Evolvable Hardware HO Bahcesehir Univ ID LOW-POWER; CORES AB There is an increasing need to develop flexible, reconfigurable, and intelligent multi-spacecraft sensing networks for aerospace-based monitoring and diagnostics. Technical advancements in ad hoe networking, MEMS devices, low-power electronics, adaptive and reconfigurable hardware, microspacecraft, and micro-sensors have enabled the design and development of such highly integrated space wireless sensor networks. This paper proposes the framework for an Evolvable Sensor Network Architecture, investigated as part of the ESPACENET project, collocated at the University of Edinburgh, Essex, Kent and Surrey. The aim is to design a flexible and intelligent embedded network of reconfigurable piconodes optimised by a hierarchical multi-objective algorithm. Although the project is targeted at aerospace applications, the same intelligent network can be used for many earth bound applications such as environmental and medical diagnostics. C1 [Arslan, T.; Haridas, N.; Yang, E.; Erdogan, A. T.; Walton, A. J.; Thompson, J. S.; Stoica, A.] Univ Edinburgh, Sch Engn & Elect, Edinburgh EH9 3JL, Midlothian, Scotland. [Barton, N.] Univ Edinburgh, Sch Biol Sci, Edinburgh EH9 3JL, Midlothian, Scotland. [Stoica, A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Vladimirova, T.] Univ Surrey, Sch Elect & Phys Sci, Guildford GU2 7XH, Surrey, England. [McDonald-Maier, K. D.] Univ Essex, Dept Comp Sci, Colchester CO4 3SQ, Essex, England. [Howells, W. G. J.] Univ Kent, Dept Elect, Canterbury CT2 7NT, Kent, England. RP Arslan, T (reprint author), Univ Edinburgh, Sch Engn & Elect, Edinburgh EH9 3JL, Midlothian, Scotland. EM T.Arslan@edac.uk RI Walton, Anthony/B-9108-2009; Walton, Anthony/A-1550-2010; OI Yang, Erfu/0000-0003-1813-5950 NR 14 TC 0 Z9 0 U1 0 U2 1 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2614-4 PY 2006 BP 323 EP + PG 3 WC Computer Science, Hardware & Architecture SC Computer Science GA BEQ55 UT WOS:000238918600048 ER PT J AU Melton, LP Yao, CS Seifert, A AF Melton, LP Yao, CS Seifert, A TI Active control of separation from the flap of a supercritical airfoil SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 33rd Fluid Dynamics Conference CY JUN 22-26, 2003 CL ORLANDO, FL SP Amer Inst Aeronaut & Astronaut ID HIGH REYNOLDS-NUMBERS; PERIODIC EXCITATION; FLOW SEPARATION AB Zero-net-mass-flux periodic excitation was applied at several regions on a simplified high-lift system to delay the occurrence of flow separation. The NASA Energy Efficient Transport supercritical airfoil was equipped with a 15% chord simply hinged leading-edge flap and a 25% chord simply hinged truiling-edge flap. Detailed flow features were measured in an attempt to identify optimal actuator placement. The current paper describes the application of active separation control at several locations on the deflected trailing-edge flap. High- and low-frequency amplitude modulation of the high-frequency excitation were used for control. It was noted that the same performance gains were obtained with amplitude modulation and required only 30% of the momentum input required by pure sine excitation. Extreme sensitivity was found to the excitation location where the flap is highly curved. This sensitivity was reduced when using low-frequency amplitude modulation due to the long wavelengths generated by the excitation. It was found that for large flap deflections the majority of the lift increasing alteration of the surface pressures results from an upstream effect. Preliminary results of combining the excitations from leading- and trailing-edge devices are also presented. C1 NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA. Tel Aviv Univ, Flow Phys & Control Branch, IL-69978 Ramat Aviv, Israel. RP Melton, LP (reprint author), NASA, Langley Res Ctr, Flow Phys & Control Branch, MS 170, Hampton, VA 23681 USA. EM l.p.melton@larc.nasa.gov; c.s.yao@larc.nasa.gov; seifert@eng.tau.ac.il NR 12 TC 20 Z9 20 U1 0 U2 1 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 JAN PY 2006 VL 44 IS 1 BP 34 EP 41 PG 8 WC Engineering, Aerospace SC Engineering GA 000XZ UT WOS:000234497000003 ER PT J AU Rabelo, LC Sepulveda, J Compton, J Turner, R AF Rabelo, LC Sepulveda, J Compton, J Turner, R TI Simulation of range safety for the NASA space shuttle SO AIRCRAFT ENGINEERING AND AEROSPACE TECHNOLOGY LA English DT Article DE spacecraft; simulation; safety measures; aerospace industry; risk management AB Purpose - The main objective of this paper is to introduce the development of a decision-support environment for a complex problem: space range safety. Simulation modeling can provide a good environment to support range safety managers. Design/methodology/approach - The paper describes the different models and the processes to find the different knowledge sources. In addition, it investigates statistically the most important factors. This will help determine emergency management procedures and sources of variability. Findings - This case study provides guidance and an example to follow for other problems in aerospace (in particular new the analysis of new vehicles). There are important factors to consider in order to implement risk management in National Aeronautics and Space Administration. Research limitations/implications - There are several limitations; blast and debris effects need to be added. Practical implications - First, it provides a guide in order to persuade managers of the utilization of decision-support systems based on geographical information systems. Second, it shows that there is open source software (Calpuff in our environment) which can be used and integrated to make a more comprehensive environment. Validation is a big issue. In addition, simulation can help make decisions about future vehicles or events. Originality/value - This is the first implementation of a virtual range (there is not an integrated system similar to this one available). This will be valuable to other safety managers not only for space exploration but also environmentalists and homeland security managers. C1 Univ Cent Florida, Ind Engn & Management Syst Dept, Orlando, FL 32816 USA. NASA, Kennedy Space Ctr, Orlando, FL USA. RP Rabelo, LC (reprint author), Univ Cent Florida, Ind Engn & Management Syst Dept, Orlando, FL 32816 USA. EM lrabelo@mail.ucf.edu NR 11 TC 3 Z9 3 U1 0 U2 1 PU EMERALD GROUP PUBLISHING LIMITED PI BRADFORD PA 60/62 TOLLER LANE, BRADFORD BD8 9BY, W YORKSHIRE, ENGLAND SN 1748-8842 J9 AIRCR ENG AEROSP TEC JI Aircr. Eng. Aerosp. Technol. PY 2006 VL 78 IS 2 BP 98 EP 106 DI 10.1108/17488840610653405 PG 9 WC Engineering, Aerospace SC Engineering GA 034SL UT WOS:000236950800002 ER PT S AU Susskind, J AF Susskind, Joel BE Shen, SS Lewis, PE TI Improved soundings and error estimates using AIRS/AMSU data - art. no. 623319 SO Algorithms and Technologies for Multispectral, Hyperspectral, and Ultraspectral Imagery XII Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Algorithms and Technologies for Multispectral, Hyperspectral, and Ultraspectral Imagery XII CY APR 17-20, 2006 CL Kissimmee, FL DE infra-red; microwave; remote sensing; temperature; moisture; high spectral resolution ID AIRS AB AIRS was launched on EOS Aqua on May 4, 2002, together with AMSU A and HSB, to form a next generation polar orbiting infrared and microwave atmospheric sounding system. The primary products of AIRS/AMSU are twice daily global fields of atmospheric temperature-humidity profiles, ozone profiles, sea/land surface skin temperature, and cloud related parameters including OLR. The sounding goals of AIRS are to produce 1 km tropospheric layer mean temperatures with an rms error of 1 K, and layer precipitable water with an rms error of 20 percent, in cases with up to 80 percent effective cloud cover. The basic theory used to analyze AIRS/AMSU/HSB data in the presence of clouds, called the at-launch algorithm, and a post-launch algorithm which differed only in the minor details from the at-launch algorithm, have been described previously. The post-launch algorithm, referred to as AIRS Version 4.0, has been used by the Goddard DAAC to analyze and distribute AIRS retrieval products. In this paper we show progress made toward the AIRS Version 5.0 algorithm which will be used by the Goddard DAAC starting late in 2006. A new methodology has been developed to provide accurate case by case error estimates for retrieved geophysical parameters and for the channel by channel cloud cleared radiances used to derive the geophysical parameters from the AIRS/AMSU observations. These error estimates are in turn used for quality control of the derived geophysical parameters and clear column radiances. Improvements made to the retrieval algorithm since Version 4.0 are described as well as results comparing Version 5.0 retrieval accuracy and spatial coverage with those obtained using Version 4.0. C1 NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Susskind, J (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 5 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6289-6 J9 P SOC PHOTO-OPT INS PY 2006 VL 6233 BP 23319 EP 23319 AR 623319 DI 10.1117/12.665018 PN 1&2 PG 12 WC Instruments & Instrumentation; Remote Sensing; Optics; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Optics; Imaging Science & Photographic Technology GA BES78 UT WOS:000239353500043 ER PT S AU Susskind, J Kouvaris, L AF Susskind, Joel Kouvaris, Louis BE Shen, SS Lewis, PE TI Contribution of the AIRS shortwave sounding channels to retrieval accuracy SO Algorithms and Technologies for Multispectral, Hyperspectral, and Ultraspectral Imagery XII Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Algorithms and Technologies for Multispectral, Hyperspectral, and Ultraspectral Imagery XII CY APR 17-20, 2006 CL Kissimmee, FL DE infra-red; microwave; remote sensing; temperature; moisture; high spectral resolution ID CLOUDY ATMOSPHERES AB AIRS contains 2376 high spectral resolution channels between 650 cm(-1) and 2665 cm(-1), including channels in both the 15 micron (near 667 cm(-1)) and 4.2 micron (near 2400 cm(-1)) CO2 sounding bands. Use of temperature sounding channels in the 15 micron CO2 band has considerable heritage in infra-red remote sensing. Channels in the 4.2 micron CO2 band have potential advantages for temperature sounding purposes because they are essentially insensitive to absorption by water vapor and ozone, and also have considerably sharper lower tropospheric temperature sounding weighting functions than do the 15 micron temperature sounding channels. Potential drawbacks with regard to use of 4.2 micron channels arise from effects on the observed radiances of solar radiation reflected by the surface and clouds, as well as effects of non-local thermodynamic equilibrium on shortwave observations during the day. These are of no practical consequences, however, when properly accounted for. We show results of experiments performed utilizing different spectral regions of AIRS, conducted with the AIRS Science Team candidate Version 5 algorithm. Experiments were performed using temperature sounding channels within the entire AIRS spectral coverage, within only the spectral region 650 cm(-1) to 1614 cm(-1); and within only the spectral region 1000 cm(-1)-2665 cm(-1). These show the relative importance of utilizing only 15 micron temperature sounding clouds, only the 4.2 micron temperature sounding channels, and both, with regards to sounding accuracy. The spectral region 2380 cm(-1) to 2400 cm(-1) is shown to, contribute significantly to improve sounding accuracy in the lower troposphere, both day and night. C1 NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Susskind, J (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 9 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6289-6 J9 P SOC PHOTO-OPT INS PY 2006 VL 6233 BP A2331 EP A2331 AR UNSP 62331A DI 10.1117/12.665061 PN 1&2 PG 10 WC Instruments & Instrumentation; Remote Sensing; Optics; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Optics; Imaging Science & Photographic Technology GA BES78 UT WOS:000239353500044 ER PT S AU Jedlovec, GJ Chou, SH Zavodsky, BT Lapenta, W AF Jedlovec, Gary J. Chou, Shih-Hung Zavodsky, Bradley T. Lapenta, William BE Shen, SS Lewis, PE TI The use of error estimates with AIRS profiles to improve short-term weather forecasts - art. no. 62331B SO Algorithms and Technologies for Multispectral, Hyperspectral, and Ultraspectral Imagery XII Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Algorithms and Technologies for Multispectral, Hyperspectral, and Ultraspectral Imagery XII CY APR 17-20, 2006 CL Kissimmee, FL DE SPoRT; AIRS; data assimilation; numerical weather prediction; quality control; forecast improvement; satellite-retrieved profiles; ADAS; WRF ID MODEL; PREDICTION; TERRAIN; SYSTEM AB The hyperspectral resolution measurements from the NASA Atmospheric Infrared Sounder (AIRS) are advancing climate research by mapping atmospheric temperature, moisture, and trace gases on a global basis with unprecedented accuracy. Using a sophisticated retrieval scheme, the AIRS is capable of diagnosing the atmospheric temperature in the troposphere with accuracies of less than I K over I kin-thick layers and 10-20% relative humidity over 2 km-thick layers, under both clear and cloudy conditions. A unique aspect of the retrieval procedure is the specification of a vertically varying error estimate for the temperature and moisture profile for each retrieval. The error specification allows for the more selective use of the profiles in subsequent processing, In this paper, we describe a procedure to assimilate AIRS data into the Weather Research and Forecasting (WRF) model to improve short-term weather forecasts. The ARPS Data Analysis System (ADAS) developed by the University of Oklahoma is configured to optimally blend AIRS data with model background fields based on the AIRS error profiles. The WRF short-term forecasts with selected AIRS data show improvement over the control forecast. The use of the AIRS error profiles maximizes the impact of high quality AIRS data from portions of the profile in the assimilation/forecast process without degradation from lower quality data in the other portions of the profile. C1 Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Jedlovec, GJ (reprint author), Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA. NR 11 TC 2 Z9 2 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 0-8194-6289-6 J9 P SOC PHOTO-OPT INS PY 2006 VL 6233 BP B2331 EP B2331 AR 62331B DI 10.1117/12.665724 PN 1&2 PG 9 WC Instruments & Instrumentation; Remote Sensing; Optics; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Optics; Imaging Science & Photographic Technology GA BES78 UT WOS:000239353500045 ER PT S AU Aumann, HH Elliott, D Gregorich, D AF Aumann, Hartmut H. Elliott, Denis Gregorich, Dave BE Shen, SS Lewis, PE TI Lessons from three years of hyperspectral data from the Atmospheric InfraRed Sounder (AIRS) on the EOS AQUA SO ALGORITHMS AND TECHNOLOGIES FOR MULTISPECTRAL, HYPERSPECTRAL, AND ULTRASPECTRAL IMAGERY XII PTS 1 AND 2 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Algorithms and Technologies for Multispectral, Hyperspectral, and Ultraspectral Imagery XII CY APR 17-20, 2006 CL Kissimmee, FL DE infrared; temperature sounder; hyperspectral; climate AB More than three years of data from the Atmospheric InfraRed Sounder (AIRS) have given many new insights into infrared hyperspectral sounding from space. Among other things they have shown that 1) Absolute accuracy at the 200 mK level and stability at the better than 20 mK/year level can be deduced for the AIRS data by comparing the observed brightness temperatures with those predicted by NOAA/NCEP's RTGSST for surface channels and those predicted from the ECMWF temperature and moisture profiles for all channels except those sensitive to stratospheric temperatures or water vapor. While the 2616 cm(-1) window channel used with AIRS for the validation of the calibration relative to the RTGSST is superior, the 1231 cm-1 window channel can be used for IASI and CRIS with slightly degraded accuracy. 2) Residual cloud contamination of about 240 mK for tightly cloud-filtered data establishes an effective noise floor for channels with weighting function below the cloud tops. With the AIRS 13.5 km footprints and mean NeDT of 0.2 K, the noise floor is reached by filtering out all but 2% of the spectra. 3) The absolute value of the difference between adjacent clear ocean footprints at night provides an excellent estimate of the NeDT in all spectral regions not affected by water vapor. Water vapor spatial scene inhomogeneity on a 13.5 km scale even in clear footprints acts as a source of noise up to a factor of six larger than the NeDT in water sensitive channels. The methodology established by AIRS for system performance evaluation and trend analysis; including the use of the RTGSST and the ECMWF profiles, lays the foundation and establishes the benchmark for the validation of the performance of future hyperspectral sounders. AIRS was launched into polar 705 kin altitude orbit on the EOS Aqua spacecraft on May 4, 2002. It covers the 3.7 to 15.4 micron region of the thermal infrared spectrum with spectral resolution of 1200. Since the start of routine data gathering in September 2002 AIRS has returned 2.9 million spectra of the upwelling radiance each day. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Aumann, HH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 11 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 0-8194-6289-6 J9 PROC SPIE PY 2006 VL 6233 AR 623318 DI 10.1117/12.666222 PN 1&2 PG 10 WC Instruments & Instrumentation; Remote Sensing; Optics; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Optics; Imaging Science & Photographic Technology GA BES78 UT WOS:000239353500042 ER PT S AU Domack, MS Taminger, KMB Begley, M AF Domack, Marcia S. Taminger, Karen M. B. Begley, Matthew BE Poole, WJ Wells, MA Lloyd, DJ TI Metallurgical mechanisms controlling mechanical properties of aluminum alloy 2219 produced by electron beam freeform fabrication SO ALUMINIUM ALLOYS 2006, PTS 1 AND 2: RESEARCH THROUGH INNOVATION AND TECHNOLOGY SE MATERIALS SCIENCE FORUM LA English DT Article; Proceedings Paper CT 10th International Conference on Aliminium Alloys (ICAA-10) CY JUL 09-13, 2006 CL Vancouver, CANADA DE aluminum alloy 2219; electron beam deposition; mechanical properties; microstructural analysis AB The electron beam freeform fabrication (EBF3) layer-additive manufacturing process has been developed to directly fabricate complex geometry components. EBF3 introduces metal wire into a molten pool created on the surface of a substrate by a focused electron beam. Part geometry is achieved by translating the substrate with respect to the beam to build the part one layer at a time. Tensile properties have been demonstrated for electron beam deposited aluminum and titanium alloys that are comparable to wrought products, although the microstructures of the deposits exhibit features more typical of cast material. Understanding the metallurgical mechanisms controlling mechanical properties is essential to maximizing application of the EBF3 process. In the current study, mechanical properties and resulting microstructures were examined for aluminum alloy 2219 fabricated over a range of EBF3 process variables. Material performance was evaluated based on tensile properties and results were compared with properties of Al 2219 wrought products. Unique microstructures were observed within the deposited layers and at interlayer boundaries, which varied within the deposit height due to microstructural evolution associated with the complex thermal history experienced during subsequent layer deposition. Microstructures exhibited irregularly shaped grains, typically with interior dendritic structures, which were described based on overall grain size, morphology, distribution, and dendrite spacing, and were correlated with deposition parameters. Fracture features were compared with microstructural elements to define fracture paths and aid in definition of basic processing-microstructure-property correlations. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Domack, MS (reprint author), NASA, Langley Res Ctr, Mail Stop 188A, Hampton, VA 23681 USA. EM Marcia.S.Domack@nasa.gov; Karen.M.Taminger@nasa.gov NR 6 TC 10 Z9 10 U1 1 U2 18 PU TRANS TECH PUBLICATIONS LTD PI ZURICH-UETIKON PA BRANDRAIN 6, CH-8707 ZURICH-UETIKON, SWITZERLAND SN 0255-5476 BN 0-87849-408-1 J9 MATER SCI FORUM PY 2006 VL 519-521 BP 1291 EP 1296 PN 1-2 PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA BEZ41 UT WOS:000240309000205 ER PT S AU Taminger, KM Hafley, RA Domack, MS AF Taminger, Karen M. Hafley, Robert A. Domack, Marcia S. BE Poole, WJ Wells, MA Lloyd, DJ TI Evolution and control of 2219 aluminum microstructural features through electron beam freeform fabrication SO ALUMINIUM ALLOYS 2006, PTS 1 AND 2: RESEARCH THROUGH INNOVATION AND TECHNOLOGY SE MATERIALS SCIENCE FORUM LA English DT Article; Proceedings Paper CT 10th International Conference on Aliminium Alloys (ICAA-10) CY JUL 09-13, 2006 CL Vancouver, CANADA DE aluminum; microstructure; freeform; fabrication; electron beam; rapid prototyping; manufacturing; process control AB Electron beam freeform fabrication (EBF3) is a new layer-additive process that has been developed for near-net shape fabrication of complex structures. EBF3 uses an electron beam to create a molten pool on the surface of a substrate. Wire is fed into the molten pool and the part translated with respect to the beam to build up a 3-dimensional structure one layer at a time. Unlike many other freeform fabrication processes, the energy coupling of the electron beam is extremely well suited to processing of aluminum allo S. The layer-additive nature of the EBF3 process results in a tortuous thermal path producing complex microstructures including: small homogeneous equiaxed grains; dendritic growth contained within larger grains; and/or pervasive dendritic formation in the interpass regions of the deposits. Several process control variables contribute to the formation of these different microstructures, including translation speed, wire feed rate, beam current and accelerating voltage. In electron beam processing, higher accelerating voltages embed the energy deeper below the surface of the substrate. Two EBF3 systems have been established at NASA Langley, one with a low-voltage (10-30kV) and the other a high-voltage (30-60kV) electron beam gun. Aluminum alloy 2219 was processed over a range of different variables to explore the design space and correlate the resultant microstructures with the processing parameters. This report is specifically exploring the impact of accelerating voltage. Of particular interest is correlating energy to the resultant material characteristics to determine the potential of achieving microstructural control through precise management of the heat flux and cooling rates during deposition. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Taminger, KM (reprint author), NASA, Langley Res Ctr, Mail Stop 188A, Hampton, VA 23681 USA. EM Karen.M.Taminger@nasa.gov; Robert.A.Hafley@nasa.gov; Marcia.S.Domack@nasa.gov NR 7 TC 5 Z9 5 U1 4 U2 22 PU TRANS TECH PUBLICATIONS LTD PI ZURICH-UETIKON PA BRANDRAIN 6, CH-8707 ZURICH-UETIKON, SWITZERLAND SN 0255-5476 BN 0-87849-408-1 J9 MATER SCI FORUM PY 2006 VL 519-521 BP 1297 EP 1302 PN 1-2 PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA BEZ41 UT WOS:000240309000206 ER PT S AU Cho, A Long, Z Lisagor, B Bales, T Domack, M Wagner, J AF Cho, A. Long, Z. Lisagor, B. Bales, T. Domack, M. Wagner, J. BE Poole, WJ Wells, MA Lloyd, DJ TI Effect of thermomechanical processing on texture and mechanical properties of Al-Cu-Li alloy plate SO ALUMINIUM ALLOYS 2006, PTS 1 AND 2: RESEARCH THROUGH INNOVATION AND TECHNOLOGY SE MATERIALS SCIENCE FORUM LA English DT Article; Proceedings Paper CT 10th International Conference on Aliminium Alloys (ICAA-10) CY JUL 09-13, 2006 CL Vancouver, CANADA DE Al-Li alloy; alloy 2195; aluminum alloy plate; anisotropy; thermomechanical processing; TMP; crystallographic texture; mechanical properties ID SHEET AB For 2195-T8 plate, design properties are based on the mechanical properties at the near surface location, corresponding to the load carrying thin membrane location in machined integrally stiffened structure. Mechanical properties at the near surface location are lower than those at the t/4 and t/2 locations. This work examined the effect of alternate temper and hot rolling practices on near surface strength levels. Results showed that alternate hot rolling practice were very effective in raising near surface strengths and improving property uniformity, and were well correlated with crystallographic texture measurements. C1 Alcan Rolled Prod, Ravenswood, WV USA. SECAT, Lexington, KY USA. Analyt Serv & Mat Inc, Hampton, VA 23666 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Cho, A (reprint author), Alcan Rolled Prod, Ravenswood, WV USA. EM alex.cho@alcan.com; zlong@secat.net; brlisag1@aol.com; ttbales@cox.net; marcia.s.domack@nasa.gov; john.a.wagner@nasa.gov NR 8 TC 3 Z9 3 U1 0 U2 1 PU TRANS TECH PUBLICATIONS LTD PI ZURICH-UETIKON PA BRANDRAIN 6, CH-8707 ZURICH-UETIKON, SWITZERLAND SN 0255-5476 BN 0-87849-408-1 J9 MATER SCI FORUM PY 2006 VL 519-521 BP 1585 EP 1590 PN 1-2 PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA BEZ41 UT WOS:000240309000251 ER PT S AU Muller, JR Aydin, A Wright, TJ AF Muller, Jordan R. Aydin, Atilla Wright, Tim J. BE Buiter, SJH Schreurs, G TI Using an elastic dislocation model to investigate static Coulomb stress change scenarios for earthquake ruptures in the eastern Marmara Sea region, Turkey SO ANALOGUE AND NUMERICAL MODELLING OF CRUSTAL-SCALE PROCESSES SE Geological Society Special Publication LA English DT Proceedings Paper CT International Meeting on Analogue and Numerical Modelling of Geological Processes CY JUN, 2004 CL SWITZERLAND ID 1999 IZMIT EARTHQUAKE; NORTH ANATOLIAN FAULT; POSITIONING SYSTEM MEASUREMENTS; 17 AUGUST; SLIP DISTRIBUTION; SOUTHERN CALIFORNIA; SEISMIC-REFLECTION; JOINT INVERSION; ACTIVE FAULTS; AEGEAN SEA AB Using an elastic dislocation model, we incorporate a historical earthquake catalog. mapped Marmara Sea fault traces, and fault slip distributions for the 1999 Izinit earthquake inferred from InSAR and GPS data to determine various stress change scenarios crucial for evaluating future earthquake potential in the eastern Marmara Sea. We have tested six plausible past rupture configurations arising from the uncertainty in the location of the western termination of 1999 lmrit earthquake rupture and the location of the 1963 Yalova earthquake rupture. Coulomb stresses calculated are increased on the Princes' Islands, Cinarcik, and Armutlu fault segments in each case. In four of the six plausible configurations of previous ruptures, the Cinarcik fault receives the greatest average stress change. In one other configuration, the average stress increase on the Princes' Islands fault is greatest. In another, the stress changes on the Cinarcik and Princes' Islands faults are comparable. Moreover, we show that rupture initiating on either the Princes' Islands or Armutlu faults would be favoured to propagate onto the Central Marmara, or Imrali fault. respectively, based on the favourable geometries of the respective fault intersections. Rupture initiating on the Cinarcik fault, however would be limited to a much shorter length based on its mapped western termination. Therefore. while the earthquake-induced stress changes may, in most cases, be greatest on the Cinarcik fault, an earthquake initiating on this fault segment may produce a shorter cumulative rupture compared to rupture initiated on the two other major eastern Marmara Sea fault segments. These results are encouraging for the use of geomechanical modelling tools in addressing uncertainties inherent in most geological and geophysical data applied to earthquake-related problems. C1 NASA, Goddard Space Flight Ctr, Geodynam Branch, Greenbelt, MD 20771 USA. RP Muller, JR (reprint author), NASA, Goddard Space Flight Ctr, Geodynam Branch, Mail Code 921, Greenbelt, MD 20771 USA. EM jmuller@core2.gsfc.nasa.gov RI Wright, Tim/A-5892-2011 OI Wright, Tim/0000-0001-8338-5935 NR 53 TC 8 Z9 8 U1 0 U2 1 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0305-8719 BN 1-86239-191-2 J9 GEOL SOC SPEC PUBL JI Geol. Soc. Spec. Publ. PY 2006 VL 253 BP 397 EP 414 DI 10.1144/GSL.SP.2006.253.01.21 PG 18 WC Geology SC Geology GA BEJ68 UT WOS:000237452000021 ER PT J AU Ye, CF Gao, HX Boatz, JA Drake, GW Twamley, B Shreeve, JM AF Ye, Chengfeng Gao, Haixiang Boatz, Jerry A. Drake, Gregory W. Twamley, Brendan Shreeve, Jean'ne M. TI Polyazidopyrimidines: High-energy compounds and precursors to carbon nanotubes SO ANGEWANDTE CHEMIE-INTERNATIONAL EDITION LA English DT Article DE azides; explosives; heats of formation; nanotubes; nitrogen ID TRIMETHYLSILYL AZIDE; NITROGEN; DETONATION; NITRIDES; CHEMISTRY; SALTS C1 Univ Idaho, Dept Chem, Moscow, ID 83844 USA. USAF, Res Lab, Space & Missile Prop Div, Edwards AFB, CA 93524 USA. NASA, Solid Propellants Branch ER22, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Shreeve, JM (reprint author), Univ Idaho, Dept Chem, Moscow, ID 83844 USA. EM jshreeve@uidaho.edu NR 34 TC 83 Z9 89 U1 0 U2 12 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 1433-7851 J9 ANGEW CHEM INT EDIT JI Angew. Chem.-Int. Edit. PY 2006 VL 45 IS 43 BP 7262 EP 7265 DI 10.1002/anie.200602778 PG 4 WC Chemistry, Multidisciplinary SC Chemistry GA 109DU UT WOS:000242288900025 PM 16969890 ER PT J AU Lepping, RP Berdichevsky, DB Wu, CC Szabo, A Narock, T Mariani, F Lazarus, AJ Quivers, AJ AF Lepping, RP Berdichevsky, DB Wu, CC Szabo, A Narock, T Mariani, F Lazarus, AJ Quivers, AJ TI A summary of WIND magnetic clouds for years 1995-2003: model-fitted parameters, associated errors and classifications SO ANNALES GEOPHYSICAE LA English DT Review DE interplanetary physics; interplanetary magnetic fields; solar wind plasma; solar physics, astrophysics and astronomy; flares and mass ejections ID CORONAL MASS EJECTIONS; SOLAR-WIND; FLUX-ROPES; 1 AU; GEOMAGNETIC STORMS; INNER HELIOSPHERE; COMPLEX EJECTA; OCTOBER 18-20; SPACECRAFT; SHOCK AB Interplanetary magnetic clouds (MCs) have been identified for the first 8.6 years of' the WIND mission, and their magnetic field structures have been parameter-fitted by a static, force free, cylindrically-symmetric model (Lepping et al., 1990) with various levels of success. This paper summarizes various aspects of the results of the model fitting by providing: seven estimated model fit-parameter values for each of the 82 MCs found, their objectively determined quality estimates, closest approach vectors (in two coordinate frames), fit-parameter errors for the cases of acceptable quality (50 cases, or 61%), axial magnetic fluxes, axial current densities, and total axial current - as well as some examples of MC profiles for various conditions and "categories" for each case (e.g. B(z): N -> S or S -> N, etc.). MC quality is estimated from a quantitative consideration of a large set of parameters, such as the chi-squared of the model fit, degree of asymmetry of the B profile, and a comparison of two means of estimating radius. This set of MCs was initially identified by visual inspection of relevant field and plasma data. Each resulting MC candidate is then tested through the use of the MC parameter model, for various adjusted durations to determine the best fit, which helps to refine the boundary-times. The resulting MC set is called Set 1. Another, larger, set (Set 2) of MCs is identified through an automated program whose criteria are based on general MC plasma and field characteristics at I AU determined through past experience. Set I is almost fully contained within Set 2, whose frequency of occurrence better matches that of the sunspot cycle than Set 1. The difference-set (Set 2-Set 1) is referred to as the magnetic cloud-like (MCL) set, whose members do not very well represent good flux ropes through modeling. We present a discussion of how a MC's front boundary is specifically identified in terms of multi-parameter considerations (i.e. any one or more of: increase in B, directional discontinuity, magnetic hole in B, drop in proton plasma beta, B-fluctuation level change, proton temperature drop, etc.), as well as through the application of the flux rope model. Also presented are examples of unusual MCs, as well as some commonly occurring relationships, such as the existence and frequency (approx. 1/2 the time) of upstream interplanetary shocks, and less frequent internal shocks. C1 NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. L3 Govt Serv Inc, Largo, MD 20774 USA. Univ Alabama, Huntsville, AL 35899 USA. Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Woodlawn Magnet High Sch Woodlawn, Woodlawn, MD 21228 USA. RP Lepping, RP (reprint author), NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Code 661, Greenbelt, MD 20771 USA. EM ronald.p.lepping@nasa.gov NR 104 TC 111 Z9 111 U1 1 U2 6 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 1 BP 215 EP 245 PG 31 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 030CM UT WOS:000236610900017 ER PT J AU Henderson, PD Owen, CJ Alexeev, IV Slavin, J Fazakerley, AN Lucek, E Reme, H AF Henderson, P. D. Owen, C. J. Alexeev, I. V. Slavin, J. Fazakerley, A. N. Lucek, E. Reme, H. TI Cluster observations of flux rope structures in the near-tail SO ANNALES GEOPHYSICAE LA English DT Article DE magnetospheric physics; magnetotail; plasma sheet; storms and substorms ID PLASMA SHEET AB An investigation of the 2003 Cluster tail season has revealed small flux ropes in the near-tail plasma sheet of Earth. These flux ropes manifest themselves as a bipolar magnetic field signature (usually predominantly in the Z-component) associated with a strong transient peak in one or more of the other components (usually the Y-component). These signatures are interpreted as the passage of a cylindrical magnetic structure with a strong axial magnetic field over the spacecraft position. On the 2 October 2003 all four Cluster spacecraft observed a flux rope in the plasma sheet at X (GSM) similar to-17 R-E. The flux rope was travelling Earthward and duskward at similar to 160kms(-1), as determined from multi-spacecraft timing. This is consistent with the observed south-then-north bipolar B-Z signature and corresponds to a size of similar to 0.3 R-E (a lower estimate, measuring between the inflection points of the bipolar signature). The axis direction, determined from multi-spacecraft timing and the direction of the strong core field, was close to the intermediate variance direction of the magnetic field. The current inside the flux rope, determined from the curlometer technique, was predominantly parallel to the magnetic field. However, throughout the flux rope, but more significant in the outer sections, a non-zero component of current perpendicular to the magnetic field existed. This shows that the flux rope was not in a "constant alpha" force-free configuration, i.e. the magnetic force, JxB was also non-zero. In the variance frame of the magnetic field, the components of JxB suggest that the magnetic pressure force was acting to expand the flux rope, i.e. directed away from the centre of the flux rope, whereas the smaller magnetic tension force was acting to compress the flux rope. The plasma pressure is reduced inside the flux rope. A simple estimate of the total force acting on the flux rope from the magnetic forces and surrounding plasma suggests that the flux rope was experiencing an expansive total force. On 13 August 2003 all four Cluster spacecraft observed a flux rope at X (GSM) similar to-18 R-E. This flux rope was travelling tailward at 200 kms(-1), consistent with the observed north-then-south bipolar B-Z signature. The bipolar signature corresponds to a size of similar to 0.3 R-E (lower estimate). In this case, the axis, determined from multi-spacecraft timing and the direction of the strong core field, was directed close to the maximum variance direction of the magnetic field. The current had components both parallel and perpendicular to the magnetic field, and JxB was again larger in the outer sections of the flux rope than in the centre. This flux rope was also under expansive magnetic pressure forces from JxB, i.e. directed away from the centre of the flux rope, and had a reduced plasma pressure inside the flux rope. A simple total force calculation suggests that this flux rope was experiencing a large expansive total force. The observations of a larger JxB signature in the outer sections of the flux ropes when compared to the centre may be explained if the flux ropes are observed at an intermediate stage of their evolution after creation by reconnection at multiple X lines near the Cluster apogee. It is suggested that these flux ropes are in the process of relaxing towards the force-free like configuration often observed further down the tail. The centre of the flux ropes may contain older reconnected flux at a later evolutionary stage and may therefore be more force-free. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. Univ London Imperial Coll Sci Technol & Med, London SW7 2BZ, England. Ctr Etud Spatiale Rayonnements, Toulouse, France. RP Henderson, PD (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM pdh@mssl.uci.ac.uk RI Owen, Christopher/C-2999-2008; Slavin, James/H-3170-2012 OI Owen, Christopher/0000-0002-5982-4667; Slavin, James/0000-0002-9206-724X NR 20 TC 27 Z9 28 U1 0 U2 4 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 EI 1432-0576 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 2 BP 651 EP 666 PG 16 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 046CG UT WOS:000237788400019 ER PT J AU Zheng, Y Lui, ATY Mann, IR Takahashi, K Watermann, J Chen, SH Rae, IJ Mukai, T Russell, CT Balogh, A Pfaff, RF Reme, H AF Zheng, Y Lui, ATY Mann, IR Takahashi, K Watermann, J Chen, SH Rae, IJ Mukai, T Russell, CT Balogh, A Pfaff, RF Reme, H TI Coordinated observation of field line resonance in the mid-tail SO ANNALES GEOPHYSICAE LA English DT Article DE magnetospheric physics; magnetotail; MHD waves and instabilities; plasma waves and instabilities; solar wind-magnetosphere interactions ID PERIOD MAGNETIC PULSATIONS; MHD WAVE-GUIDES; EARTHS MAGNETOSPHERE; ELECTRIC-FIELD; AURORAL ARC; ULF WAVES; HF RADAR; EXCITATION; MULTISATELLITE; OSCILLATIONS AB Standing Alfven waves of 1.1 mHz (similar to 15 min in period) were observed by the Cluster satellites in the mid-tail during 06:00-07:00 UT on 8 August 2003. Pulsations with the same frequency were also observed at several ground stations near Cluster's footpoint. The standing wave properties were determined from the electric and magnetic field measurements of Cluster. Data from the ground magnetometers indicated a latitudinal amplitude and phase structure consistent with the driven field line resonance (FLR) at 1.1 mHz. Simultaneously, quasi-periodic oscillations at different frequencies were observed in the post-midnight/early morning sector by GOES 12 (l(0) approximate to 8.7), Polar (l(0) approximate to 11-14) and Geotail (l(0) approximate to 9.8). The 8 August 2003 event yields rare and interesting datasets. It provides, for the first time, coordinated in situ and ground-based observations of a very low frequency FLR in the mid-tail on stretched field lines. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Univ Alberta, Dept Phys, Space Phys Grp, Edmonton, AB, Canada. NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. JAXA, ISAS, Sagamihara, Kanagawa 2298510, Japan. Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. Univ London Imperial Coll Sci Technol & Med, Dept Space & Atmospher Phys, London, England. NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. CESR, F-31028 Toulouse 4, France. RP Zheng, Y (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM yihua.zheng@jhuapl.edu RI Zheng, Yihua/D-7368-2012; Pfaff, Robert/F-5703-2012; Rae, Jonathan/D-8132-2013; OI Pfaff, Robert/0000-0002-4881-9715; Russell, Christopher/0000-0003-1639-8298 NR 44 TC 8 Z9 8 U1 0 U2 4 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 2 BP 707 EP 723 PG 17 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 046CG UT WOS:000237788400023 ER PT J AU Viljanen, A Tanskanen, EI Pulkkinen, A AF Viljanen, A. Tanskanen, E. I. Pulkkinen, A. TI Relation between substorm characteristics and rapid temporal variations of the ground magnetic field SO ANNALES GEOPHYSICAE LA English DT Article DE geomagnetism and paleornagnetism; rapid time variations; ionosphere; auroral ionosphere; magnetospheric physics; storms and substorms ID GEOMAGNETICALLY INDUCED CURRENTS; ELEMENTARY CURRENT SYSTEMS AB Auroral substorms are one of the major causes of large geomagnetically induced currents (GIC) in technological systems. This study deals with different phases of the auroral substorm concerning their severity from the GIC viewpoint. Our database consists of 833 substorms observed by the IMAGE magnetometer network in 1997 (around sunspot minimum) and 1999 (rising phase of the sunspot cycle), divided into two classes according to the D-st index: non-storm (D-st >-40 nT, 696 events) and storm-time ones (Dst <-40 nT, 137 events). The key quantity concerning GIC is the time derivative of the horizontal magnetic field vector (dH/dt) whose largest values during substorms occur most probably at about 5 min after the onset at stations with CGM latitude less than 72 deg. When looking at the median time of the occurrence of the maximum dH/dt after the expansion onset, it increases as a function of latitude from about 15 min at CGM lat = 56 deg to about 45 min at CGM lat = 75 deg for non-storm substorms. For storm-time events, these times are about 5 min longer. Based on calculated ionospheric equivalent currents, large dH/dt occur mostly during the substorm onset when the amplitude of the westward electrojet increases rapidly. C1 Finnish Meteorol Inst, Space Res Unit, FI-00101 Helsinki, Finland. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. RP Viljanen, A (reprint author), Finnish Meteorol Inst, Space Res Unit, POB 503, FI-00101 Helsinki, Finland. EM ari.viljanen@fmi.fi NR 27 TC 20 Z9 20 U1 1 U2 3 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 EI 1432-0576 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 2 BP 725 EP 733 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 046CG UT WOS:000237788400024 ER PT J AU Milan, SE Wild, JA Hubert, B Carr, CM Lucek, EA Bosqued, JM Watermann, JF Slavin, JA AF Milan, SE Wild, JA Hubert, B Carr, CM Lucek, EA Bosqued, JM Watermann, JF Slavin, JA TI Flux closure during a substorm observed by Cluster, Double Star, IMAGE FUV, SuperDARN, and Greenland magnetometers SO ANNALES GEOPHYSICAE LA English DT Article DE magnetospheric physics; magnetotail; solar wind-magnetosphere interactions; storms and substorms ID ADVANCED COMPOSITION EXPLORER; SPECTROMETRY CIS EXPERIMENT; HIGH-LATITUDE CONVECTION; MAGNETIC-FIELD; MAGNETOSPHERE; MAGNETOTAIL; DYNAMICS; SPACECRAFT; NETWORK; MISSION AB We examine magnetic flux closure during an extended substorm interval on 29 August 2004 involving a two-stage onset and subsequent re-intensifications. Cluster and Double Star provide observations of magnetotail dynamics, while the corresponding auroral evolution, convection response, and substorm current wedge development are monitored by IMAGE FUV, SuperDARN, and the Greenland magnetometer chain, respectively. The first stage of onset is associated with the reconnection of closed flux in the plasma sheet; this is accompanied by a short-lived auroral intensification, a modest substorm current wedge magnetic bay, but no significant ionospheric convection enhancement. The second stage follows the progression of reconnection to the open field lines of the lobes; accompanied by prolonged auroral bulge and westward-travelling surge development, enhanced magnetic bays and convection. We find that the tail dynamics are highly influenced by ongoing dayside creation of open flux, leading to flux pile-up in the near-tail and a step-wise down-tail motion of the tail reconnection site. In all, 5 dipolarizations are observed, each associated with the closure of similar to 0.1 GWb of flux. Very simple calculations indicate that the X-line should progress down-tail at a speed of 20 km s(-1) or 6 R-E between each dipolarization. C1 Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Lancaster, Dept Commun Syst, Lancaster LA1 4WA, England. Univ Liege, Lab Planetary & Atmospher Phys, B-4000 Cointe Ougree, Belgium. Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. CNRS, CESR, F-31028 Toulouse, France. Danish Metrol Inst, DK-2100 Copenhagen, Denmark. NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. RP Milan, SE (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM steve.milan@ion.le.ac.uk RI Slavin, James/H-3170-2012; OI Slavin, James/0000-0002-9206-724X; Wild, James/0000-0001-8025-8869 NR 39 TC 5 Z9 5 U1 0 U2 3 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 2 BP 751 EP 767 PG 17 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 046CG UT WOS:000237788400026 ER PT J AU Pulinets, SA Ouzounov, D Ciraolo, L Singh, R Cervone, G Leyva, A Dunajecka, M Karelin, AV Boyarchuk, KA Kotsarenko, A AF Pulinets, S. A. Ouzounov, D. Ciraolo, L. Singh, R. Cervone, G. Leyva, A. Dunajecka, M. Karelin, A. V. Boyarchuk, K. A. Kotsarenko, A. TI Thermal, atmospheric and ionospheric anomalies around the time of the Colima M7.8 earthquake of 21 January 2003 SO ANNALES GEOPHYSICAE LA English DT Article DE atmospheric composition and structure; ion chemistry of the atmosphere; meteorology and atmospheric dynamics; atmospheric electricity; ionosphere; ionosphere-atmosphere interactions ID SEISMICALLY ACTIVE AREAS; WAVELET MAXIMA CURVES; PRECURSORS; SURFACE; GPS AB The paper examines the possible relationship of anomalous variations of different atmospheric and ionospheric parameters observed around the time of a strong earthquake (M(u)) 7.8) which occurred in Mexico (state of Colima) on 21 January 2003. These variations are interpreted within the framework of the developed model of the Lithosphere-Atmosphere-Ionosphere coupling. The main attention is focused on the processes in the near ground layer of the atmosphere involving the ionization of air by radon, the water molecules' attachment to the formed ions, and the corresponding changes in the latent heat. Model considerations are supported by experimental measurements showing the local diminution of air humidity one week prior to the earthquake, accompanied by the anomalous thermal infrared (TIR) signals and surface latent heat flux (SLHF) and anomalous variations of the total electron content (TEC) registered over the epicenter of the impending earthquake three days prior to the main earthquake event. Statistical processing of the data of the GPS receivers network, together with various other atmospheric parameters demonstrate the possibility of an early warning of an impending strong earthquake. C1 Univ Nacl Autonoma Mexico, Inst Geophys, Mexico City, DF, Mexico. NASA, Goddard Space Flight Ctr, SSAI, Greenbelt, MD 20771 USA. CNR, Inst Appl Phys Nello Carrara, I-50127 Florence, Italy. Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India. George Mason Univ, Fairfax, VA 22030 USA. Univ Nacl Autonoma Mexico, Inst Geog, Mexico City, DF, Mexico. Russian Acad Sci, IZMIRAN, Troitsk, Russia. NPP VNIIEM, Moscow, Russia. Univ Nacl Autonoma Mexico, Inst Geosci, Mexico City, DF, Mexico. RP Pulinets, SA (reprint author), Univ Nacl Autonoma Mexico, Inst Geophys, Mexico City, DF, Mexico. EM pulse@geofisica.unam.mx RI Singh, Ramesh/G-7240-2012; Pulinets, Sergey/F-7462-2011; OI Pulinets, Sergey/0000-0003-3944-6686; Cervone, Guido/0000-0002-6509-0735 NR 36 TC 51 Z9 55 U1 0 U2 6 PU COPERNICUS PUBLICATIONS PI KATHLENBURG-LINDAU PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 3 BP 835 EP 849 PG 15 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 064FK UT WOS:000239074400004 ER PT J AU Fritts, DC Goldberg, RA AF Fritts, D. C. Goldberg, R. A. TI MaCWAVE: a rocket-lidar-radar program to study the polar mesosphere during summer and winter - Preface SO ANNALES GEOPHYSICAE LA English DT Editorial Material C1 NW Res Associates Inc, Colorado Res Associates Div, Boulder, CO USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Fritts, DC (reprint author), NW Res Associates Inc, Colorado Res Associates Div, Boulder, CO USA. RI Goldberg, Richard /E-1881-2012 NR 0 TC 1 Z9 1 U1 0 U2 0 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 4 BP 1157 EP 1158 PG 2 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 073EB UT WOS:000239724600001 ER PT J AU Goldberg, RA Fritts, DC Schmidlin, FJ Williams, BP Croskey, CL Mitchell, JD Friedrich, M Russell, JM Bium, U Fricke, KH AF Goldberg, R. A. Fritts, D. C. Schmidlin, F. J. Williams, B. P. Croskey, C. L. Mitchell, J. D. Friedrich, M. Russell, J. M., III Bium, U. Fricke, K. H. TI The MaCWAVE program to study gravity wave influences on the polar mesosphere SO ANNALES GEOPHYSICAE LA English DT Article DE atmospheric composition and structure; pressure density and temperature; meteorology and atmospheric dynamics; waves and tides; middle atmosphere dynamics ID DIURNAL PROPAGATING TIDE; MIDDLE ATMOSPHERE; SUMMER MESOPAUSE; MOMENTUM FLUXES; DYNAMICS; CIRCULATION; THERMOSPHERE; FLUCTUATIONS; STRATOSPHERE; TURBULENCE AB MaCWAVE (Mountain and Convective Waves Ascending VErtically) was a highly coordinated rocket, ground-based, and satellite program designed to address gravity wave forcing of the mesosphere and lower thermosphere (MLT). The MaCWAVE program was conducted at the Norwegian Andoya Rocket Range (ARR, 69.3 degrees N) in July 2002, and continued at the Swedish Rocket Range (Esrange, 67.9 degrees N) during January 2003. Correlative instrumentation included the ALOMAR MF and MST radars and RMR and Na lidars, Esrange MST and meteor radars and RMR lidar, radiosondes, and TIMED (Thermosphere Ionosphere Mesosphere Energetics and Dynamics) satellite measurements of thermal structures. The data have been used to define both the mean fields and the wave field structures and turbulence acneration leading to forcing of the large-scale flow. In summer, launch sequences coupled with ground-based measurements at ARR addressed the forcing of the summer mesopause environment by anticipated convective and shear generated gravity waves. These motions were measured with two 12-h rocket sequences, each involving one Terrier-Orion payload accompanied by a mix of MET rockets, all at ARR in Norway. The MET rockets were used to define the temperature and wind structure of the stratosphere and mesosphere. The Terrier-Orions were designed to measure small-scale plasma fluctuations and turbulence that might be induced by wave breaking in the mesosphere. For the summer series, three European MIDAS (Middle Atmosphere Dynamics and Structure) rockets were also launched from ARR in coordination with the MaCWAVE payloads. These were designed to measure plasma and neutral turbulence within the MLT. The summer program exhibited a number of indications of significant departures of the mean wind and temperature structures from "normal" polar summer conditions, including an unusually warm mesopause and a slowing of the formation of polar mesospheric summer echoes (PMSE) and noctilucent clouds (NLC). This was suggested to be due to enhanced planetary wave activity in the Southern Hemisphere and a surprising degree of interhemispheric coupling. The winter program was designed to study the upward propagation and penetration of mountain waves from northern Scandinavia into the MLT at a site favored for such penetration. As the major response was expected to be downstream (east) of Norway, these motions were measured with similar rocket sequences to those used in the summer campaign, but this time at Esrange. However, a major polar stratospheric warming just prior to the rocket launch window induced small or reversed stratospheric zonal winds, which prevented mountain wave penetration into the mesosphere. Instead, mountain waves encountered critical levels at lower altitudes and the observed wave structure in the mesosphere originated from other sources. For example, a large-amplitude semidiurnal tide was observed in the mesosphere on 28 and 29 January, and appears to have contributed to significant instability and small-scale structures at higher altitudes. The resulting energy deposition was found to be competitive with summertime values. Hence, our MaCWAVE measurements as a whole are the first to characterize influences in the MLT region of planetary wave activity and related stratospheric warmings during both winter and summer. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NW Res Assoc, Colorado Res Associates Div, Boulder, CO 80301 USA. NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. Penn State Univ, Dept Elect Engn, University Pk, PA 16802 USA. Graz Univ Technol, A-8010 Graz, Austria. Hampton Univ, Ctr Atmospher Res, Hampton, VA 23681 USA. Forsvarets Forskningsinst, NO-2027 Kjeller, Norway. Univ Bonn, Inst Phys, D-53115 Bonn, Germany. RP Goldberg, RA (reprint author), NASA, Goddard Space Flight Ctr, Code 612-3, Greenbelt, MD 20771 USA. EM richard.a.goldberg@nasa.gov RI Goldberg, Richard /E-1881-2012 NR 41 TC 17 Z9 17 U1 1 U2 5 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 EI 1432-0576 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 4 BP 1159 EP 1173 PG 15 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 073EB UT WOS:000239724600002 ER PT J AU Williams, BP Fritts, DC She, CY Goldberg, RA AF Williams, B. P. Fritts, D. C. She, C. Y. Goldberg, R. A. TI Gravity wave propagation through a large semidiurnal tide and instabilities in the mesosphere and lower thermosphere during the winter 2003 MaCWAVE rocket campaign SO ANNALES GEOPHYSICAE LA English DT Article DE meteorology and atmospheric dynamics; middle atmosphere dynamics; waves and tides; thermospheric dynamics ID MIDDLE ATMOSPHERE; STABILITY; DYNAMICS; LIDAR AB The winter MaCWAVE (Mountain and convective waves ascending vertically) rocket campaign took place in January 2003 at Esrange, Sweden and the ALOMAR observatory in Andenes, Norway. The campaign combined balloon, lidar, radar, and rocket measurements to produce full temperature and wind profiles from the ground to 105 km. This paper will investigate gravity wave propagation in the mesosphere and lower thermosphere using data from the Weber sodium lidar on 28-29 January 2003. A very large semidiurnal tide was present in the zonal wind above 80 km that grew to a 90 m/s amplitude at 100 km. The superposition of smaller-scale gravity waves and the tide caused small regions of possible convective or shear instabilities to form along the downward progressing phase fronts of the tide. The gravity waves had periods ranging from the Nyquist period of 30 min up to 4 h, vertical wavelengths ranging from 7 km to more than 20 km, and the frequency spectra had the expected -5/3 slope. The dominant gravity waves had long vertical wavelengths and experienced rapid downward phase progression. The gravity wave variance grew exponentially with height up from 86 to 94 km, consistent with the measured scale height, suggesting that the waves were not dissipated strongly by the tidal gradients and resulting unstable regions in this altitude range. C1 NW Res Associates, Colorado Res Associates Div, Boulder, CO USA. Colorado State Univ, Dept Phys, Ft Collins, CO 80523 USA. NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. RP Williams, BP (reprint author), NW Res Associates, Colorado Res Associates Div, Boulder, CO USA. EM biff@cora.nwra.com RI Goldberg, Richard /E-1881-2012 NR 13 TC 25 Z9 25 U1 0 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 EI 1432-0576 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 4 BP 1199 EP 1208 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 073EB UT WOS:000239724600005 ER PT J AU Wang, L Fritts, DC Williams, BP Goldberg, RA Schmidlin, FJ Bium, U AF Wang, L. Fritts, D. C. Williams, B. P. Goldberg, R. A. Schmidlin, F. J. Bium, U. TI Gravity waves in the middle atmosphere during the MaCWAVE winter campaign: evidence of mountain wave critical level encounters SO ANNALES GEOPHYSICAE LA English DT Article DE meteorology and atmospheric dynamics; middle atmosphere dynamics; waves and tides; turbulence ID GENERAL-CIRCULATION; MESOSCALE VARIABILITY; STRATOSPHERE; PARAMETERS; DRAG; MESOSPHERE; EXCITATION; TURBULENCE; BREAKING; ESRANGE AB Falling sphere and balloon wind and temperature data from the MaCWAVE winter campaign, which was conducted in northern Scandinavia during January 2003, are analyzed to investigate gravity wave characteristics in the stratosphere and mesosphere. There were two stratospheric warming events occurring during the campaign, one having a maximum temperature perturbation at similar to 45 km during 1719 January, and the other having a maximum perturbation at similar to 30 km during 24-27 January. The former was a major event, whereas the latter was a minor one. Both warmings were accompanied by upper mesospheric coolings, and during the second warming, the upper mesospheric cooling propagated downward. Falling sphere data from the two salvos on 24-25 January and 28 January were analyzed for gravity wave characteristics. Gravity wave perturbations maximized at similar to 45-50 km, with a secondary maximum at 60 km during Salvo 1; for Salvo 2, wave activity was most pronounced at similar to 60 km and above. Gravity wave horizontal propagation directions are estimated using the conventional hodographic analysis combined with the S-transform (a Gaussian wavelet analysis method). The results are compared with those from a Stokes analysis. They agree in general, though the former appears to provide better estimates for some cases, likely due to the capability of the S-transform to obtain robust estimates of wave amplitudes and phase differences between different fields. For Salvo 1 at similar to 60 km and above, gravity waves propagated towards the southeast, whereas for Salvo 2 at similar altitudes, waves propagated predominantly towards the northwest or west. These waves were found not to be topographic waves. Gravity wave motions at similar to 45-50 km in Salvo 1 were more complicated, but they generally had large amplitudes, short vertical scales, and their hodographs revealed a northwest-southeast orientation. In addition, the ratios between wave amplitudes and intrinsic phase speeds generally displayed a marked peak at similar to 45-50 km and decreased sharply at similar to 50 km, where the background winds were very weak. These results suggest that these wave motions were most likely topographic waves approaching their critical levels. Waves were more nearly isotropic in the lower stratosphere. C1 NW Res Associates Inc, Colorado Res Associates Div, Boulder, CO 80301 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. Forsvarets Forskningsinst, NO-2027 Kjeller, Norway. RP Wang, L (reprint author), NW Res Associates Inc, Colorado Res Associates Div, 3380 Mitchell Lane, Boulder, CO 80301 USA. EM lwang@cora.nwra.com RI Goldberg, Richard /E-1881-2012 NR 44 TC 19 Z9 21 U1 0 U2 1 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 EI 1432-0576 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 4 BP 1209 EP 1226 PG 18 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 073EB UT WOS:000239724600006 ER PT J AU Nielsen, K Taylor, MJ Pautet, PD Fritts, DC Mitchell, N Beldon, C Williams, BP Singer, W Schmidlin, FJ Goldberg, RA AF Nielsen, K. Taylor, M. J. Pautet, P. -D. Fritts, D. C. Mitchell, N. Beldon, C. Williams, B. P. Singer, W. Schmidlin, F. J. Goldberg, R. A. TI Propagation of short-period gravity waves at high-latitudes during the MaCWAVE winter campaign SO ANNALES GEOPHYSICAE LA English DT Article DE atmospheric composition and structure; air-glow and aurora); meteorology and atmospheric dynamics; middle atmospheric dynamics; waves and tides ID 2-DIMENSIONAL SPECTRAL-ANALYSIS; NIGHTGLOW EMISSIONS; NOCTILUCENT CLOUDS; IMAGE MEASUREMENTS; LOWER THERMOSPHERE; MIDDLE ATMOSPHERE; OI(557.7 NM); OH AIRGLOW; MESOSPHERE; AUSTRALIA AB As part of the MaCWAVE (Mountain and Convective Waves Ascending Vertically) winter campaign an all-sky monochromatic CCD imager has been used to investigate the properties of short-period mesospheric gravity waves at high northern latitudes. Sequential measurements of several nightglow emissions were made from Esrange, Sweden, during a limited period from 27-31 January 2003. Coincident wind measurements over the altitude range (similar to 80-100km) using two meteor radar systems located at Esrange and Andenes have been used to perform a novel investigation of the intrinsic properties of five distinct wave events observed during this period. Additional lidar and MSIS model temperature data have been used to investigate their nature (i.e. freely propagating or ducted). Four of these extensive wave events were found to be freely propagating with potential source regions to the north of Scandinavia. No evidence was found for strong orographic forcing by short-period waves in the airglow emission layers. The fifth event was most unusual exhibiting an extensive, but much smaller and variable wavelength pattern that appeared to be embedded in the back-ground wind field. Coincident wind measurements indicated the presence of a strong shear suggesting this event was probably due to a large-scale Kelvin-Helmholtz instability. C1 Utah State Univ, Ctr Atmospher & Space Sci, Logan, UT 84322 USA. Utah State Univ, Dept Phys, Logan, UT 84322 USA. NW Res Associates, Colorado Res Associates, Boulder, CO 80301 USA. Univ Bath, Dept Elect & Elect Engn, Bath BA2 7AY, Avon, England. Leibniz Inst Atmospharenphys, Kuhlungsborn, Germany. NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nielsen, K (reprint author), Utah State Univ, Ctr Atmospher & Space Sci, Logan, UT 84322 USA. EM knielsen@cc.usu.edu RI Goldberg, Richard /E-1881-2012 NR 50 TC 17 Z9 17 U1 0 U2 2 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 4 BP 1227 EP 1243 PG 17 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 073EB UT WOS:000239724600007 ER PT J AU Kirkwood, S Belova, E Blum, U Croskey, C Dalin, P Fricke, KH Goldberg, RA Manninen, J Mitchel, JD Schmidlin, R AF Kirkwood, S. Belova, E. Blum, U. Croskey, C. Dalin, P. Fricke, K. -H. Goldberg, R. A. Manninen, J. Mitchel, J. D. Schmidlin, R. TI Polar mesosphere winter echoes during MaCWAVE SO ANNALES GEOPHYSICAE LA English DT Article DE meteorology and atmospheric dynamics; turbulence; middle atmosphere dynamics; ionosphere; polar ionosphere ID PITCH-ANGLE DIFFUSION; ENERGY-DISSIPATION RATES; VHF RADAR ECHOES; LOWER THERMOSPHERE; MIDDLE ATMOSPHERE; SUMMER ECHOES; TURBULENCE; EISCAT; LATITUDES; FLUXES AB During the MaCWAVE winter campaign in January 2003, layers of enhanced echo power known as PMWE (Polar Mesosphere Winter Echoes) were detected by the ESRAD 52 MHz radar on several occasions. The cause of these echoes is unclear and here we use observations by meteorological and sounding rockets and by lidar to test whether neutral turbulence or aerosol layers might be responsible. PMWE were detected within 30 min of meteorological rocket soundings (falling spheres) on 5 separate days. The observations from the meteorological rockets show that, in most cases, conditions likely to be associated with neutral atmospheric turbulence are not observed at the heights of the PMWE. Observations by instrumented sounding rockets confirm low levels of turbulence and indicate considerable small-scale structure in charge density profiles. Comparison of falling sphere and lidar data, on the other hand, show that any contribution of aerosol scatter to the lidar signal at PMWE heights is less than the detection threshold of about 10%. C1 Swedish Inst Space Phys, S-98128 Kiruna, Sweden. Univ Bonn, Inst Phys, D-53115 Bonn, Germany. Penn State Univ, EE Dept, University Pk, PA 16802 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sodankyla Geophys Observ, FIN-99600 Sodankyla, Finland. NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. RP Kirkwood, S (reprint author), Swedish Inst Space Phys, Box 812, S-98128 Kiruna, Sweden. EM sheila.kirkwood@irf.se RI Goldberg, Richard /E-1881-2012 NR 29 TC 9 Z9 9 U1 0 U2 0 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 4 BP 1245 EP 1255 PG 11 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 073EB UT WOS:000239724600008 ER PT J AU Williams, BP Croskey, CL She, CY Mitchell, JD Goldberg, RA AF Williams, B. P. Croskey, C. L. She, C. Y. Mitchell, J. D. Goldberg, R. A. TI Sporadic sodium and E layers observed during the summer 2002 MaCWAVE/MIDAS rocket campaign SO ANNALES GEOPHYSICAE LA English DT Article DE atmospheric composition and structure; ion chemistry of the atmosphere; thermosphere-composition and chemistry; ionosphere; ionospheric irregularities ID ELECTRON-DENSITY IRREGULARITIES; NEUTRAL-WIND; E-REGION; LOWER THERMOSPHERE; VERTICAL MOVEMENT; MESOPAUSE REGION; ION LAYERS; MIDLATITUDE; IONOSPHERE; MESOSPHERE AB On 5 July 2002, a MaCWAVE (Mountain and Convective Waves Ascending VErtically) payload launched from Andoya Rocket Range, Norway, observed narrow enhanced layers of electron density that were nearly coincident with sporadic sodium layers measured by the Weber sodium lidar at the nearby ALOMAR Observatory. We investigate the formation mechanism of these layers using the neutral wind and temperature profiles measured directly by the lidar and the vertical motion deduced from the sodium mixing ratio. Through comparisons of the lidar data to the sporadic E in situ data, we find support for the concentration and downward motion of ions to an altitude where chemical models predict the rapid conversion of sodium ions to neutral sodium. C1 NW Res Associates, Colorado Res Associates Div, Boulder, CO USA. Penn State Univ, Commun & Space Sci Lab, Dept Elect Engn, University Pk, PA 16802 USA. Colorado State Univ, Dept Phys, Ft Collins, CO 80523 USA. NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. RP Williams, BP (reprint author), NW Res Associates, Colorado Res Associates Div, Boulder, CO USA. EM biff@cora.nwra.com RI Goldberg, Richard /E-1881-2012 NR 46 TC 13 Z9 14 U1 0 U2 9 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 4 BP 1257 EP 1266 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 073EB UT WOS:000239724600009 ER PT J AU Croskey, CL Mitchell, JD Friedrich, M Schmidlin, FJ Goldberg, RA AF Croskey, C. L. Mitchell, J. D. Friedrich, M. Schmidlin, F. J. Goldberg, R. A. TI In-situ electron and ion measurements and observed gravity wave effects in the polar mesosphere during the MaCWAVE program SO ANNALES GEOPHYSICAE LA English DT Article DE atmospheric composition and structure; aerosols and particles; meteorology and atmospheric dynamics; middle atmosphere dynamics; turbulence ID SUMMER ECHOES; MIDDLE ATMOSPHERE; D-REGION; NOCTILUCENT CLOUDS; SCALE STRUCTURE; SCHMIDT NUMBER; PMSE; DENSITY; IONOSPHERE; PARTICLES AB Langmuir probe electron and ion measurements from four instrumented rockets flown during the MaCWAVE (Mountain and Convective Waves Ascending VErtically) program are reported. Two of the rockets were launched from Andoya Rocket Range, Norway, in the summer of 2002. Electron scavenging by ice particulates produced reductions of the electron density in both sharp narrow (approximate to 1-2 km) layers and as a broad (approximate to 13 km) depletion. Small-scale irregularities were observed in the altitude regions of both types of electron depletion. The scale of the irregularities extended to wavelengths comparable to those used by ground-based radars in observing PMSE. In regions where ice particles were not present, analysis of the spectral signatures provided reasonable estimates of the energy deposition from breaking Gravity waves. C1 Penn State Univ, Dept Elect Engn, University Pk, PA 16802 USA. Graz Univ Technol, A-8010 Graz, Austria. NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20771 USA. RP Croskey, CL (reprint author), Penn State Univ, Dept Elect Engn, University Pk, PA 16802 USA. EM ccroskey@psu.edu RI Goldberg, Richard /E-1881-2012 NR 40 TC 3 Z9 3 U1 0 U2 3 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 EI 1432-0576 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 4 BP 1267 EP 1278 PG 12 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 073EB UT WOS:000239724600010 ER PT J AU Darrouzet, F De Keyser, J Decreau, PME Gallagher, DL Pierrard, V Lemaire, JR Sandel, BR Dandouras, I Matsui, H Dunlop, M Cabrera, J Masson, A Canu, P Trotignon, JG Rauch, JL Andre, M AF Darrouzet, F. De Keyser, J. Decreau, P. M. E. Gallagher, D. L. Pierrard, V. Lemaire, J. R. Sandel, B. R. Dandouras, I. Matsui, H. Dunlop, M. Cabrera, J. Masson, A. Canu, P. Trotignon, J. G. Rauch, J. L. Andre, M. TI Analysis of plasmaspheric plumes: CLUSTER and IMAGE observations SO ANNALES GEOPHYSICAE LA English DT Article DE magnetospheric physics; magnetospheric configuration and dynamics; plasmasphere; instruments and techniques ID EXTREME-ULTRAVIOLET IMAGER; DETACHED PLASMA REGIONS; MAGNETIC-FIELD; ELECTRIC-FIELD; POTENTIAL MEASUREMENTS; BOUNDARY-LAYER; DUSK SECTOR; DENSITY; CONVECTION; MAGNETOSPHERE AB Plasmaspheric plumes have been routinely observed by CLUSTER and IMAGE. The CLUSTER mission provides high time resolution four-point measurements of the plasmasphere near perigee. Total electron density profiles have been derived from the electron plasma frequency identified by the WHISPER sounder supplemented, in-between soundings, by relative variations of the spacecraft potential measured by the electric field instrument EFW; ion velocity is also measured onboard these satellites. The EUV imager onboard the IMAGE spacecraft provides global images of the plasmasphere with a spatial resolution of 0.1 RE every 10 min; such images acquired near apogee from high above the pole show the geometry of plasmaspheric plumes, their evolution and motion. We present coordinated observations of three plume events and compare CLUSTER in-situ data with global images of the plasmasphere obtained by IMAGE. In particular, we study the geometry and the orientation of plasmaspheric plumes by using four-point analysis methods. We compare several aspects of plume motion as determined by different methods: (i) inner and outer plume boundary velocity calculated from time delays of this boundary as observed by the wave experiment WHISPER on the four spacecraft, (ii) drift velocity measured by the electron drift instrument EDI onboard CLUSTER and (iii) global velocity determined from successive EUV images. These different techniques consistently indicate that plasmaspheric plumes rotate around the Earth, with their foot fully co-rotating, but with their tip rotating slower and moving farther out. C1 IASB, BIRA, Brussels, Belgium. CNRS, LPCE, Orleans, France. Univ Orleans, Orleans, France. NASA, MSFC, Huntsville, AL USA. CSR, Louvain, Belgium. Univ Arizona, LPL, Tucson, AZ USA. CNRS, CESR, Toulouse, France. Univ New Hampshire, SSC, Durham, NH USA. RAL, SSTD, Didcot, Oxon, England. Estec, ESA, RSSD, Noordwijk, Netherlands. CNRS, CETP, Velizy Villacoublay, France. IRFU, Uppsala Div, Uppsala, Sweden. RP Darrouzet, F (reprint author), IASB, BIRA, Brussels, Belgium. EM fabien.darrouzet@oma.be RI Cabrera, Juan/C-2908-2008; OI Cabrera, Juan/0000-0003-1551-8665; Dandouras, Iannis/0000-0002-7121-1118; Darrouzet, Fabien/0000-0002-2927-6858; Pierrard, Viviane/0000-0001-5014-7682 NR 59 TC 27 Z9 27 U1 0 U2 3 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 6 BP 1737 EP 1758 PG 22 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 073EA UT WOS:000239724500022 ER PT J AU Huang, FT Mayr, HG Reber, CA Russell, JM Mlynczak, M Mengel, JG AF Huang, F. T. Mayr, H. G. Reber, C. A. Russell, J. M. Mlynczak, M. Mengel, J. G. TI Stratospheric and mesospheric temperature variations for the quasi-biennial and semiannual (QBO and SAO) oscillations based on measurements from SABER (TIMED) and MLS (UARS) SO ANNALES GEOPHYSICAE LA English DT Article DE meteorology and atmospheric dynamics; middle atmosphere dynamics; thermospheric dynamics; atmospheric composition and structure; pressure, density, and temperature ID ATMOSPHERE RESEARCH SATELLITE; DOPPLER-SPREAD PARAMETERIZATION; GENERAL-CIRCULATION MODEL; EQUATORIAL MIDDLE ATMOSPHERE; WAVE MOMENTUM DEPOSITION; GRAVITY-WAVES; ZONAL WIND; TROPICAL STRATOSPHERE; LOWER THERMOSPHERE; KELVIN WAVE AB We present the zonal mean temperature variations for the quasi-biennial oscillation (QBO) and the semiannual oscillation (SAO) based on data from SABER on the TIMED spacecraft (years 2002 to 2004) and from MLS on the UARS mission (1992 to 1994). The SABER measurements provide the rare opportunity to analyze data from one instrument over a wide altitude range (15 to 95 km), while MLS data were taken in the 16 to 55 km altitude range a decade earlier. The results are presented for latitudes from 48 degrees S to 48 degrees N. New results are obtained for the QBO, especially in the upper stratosphere and mesosphere, and at mid-latitudes. At Equatorial latitudes, the QBO amplitudes show local peaks, albeit small, that occur at different altitudes. From about 20 to 40 km, and within about 15 degrees of the Equator, the amplitudes can approach 3.5 degrees K for the stratospheric QBO (SQBO). For the mesospheric QBO (MQBO), we find peaks near 70 km, with temperature amplitudes reaching 3.5 degrees K, and near 85 km, the amplitudes approach 2.5 degrees K. Morphologically, the amplitude and phase variations derived from the SABER and MLS measurements are in qualitative agreement. As a function of latitude, the QBO amplitudes tend to peak at the Equator but then increase again pole-ward of about 15 degrees to 20 degrees. The phase progression with altitude varies more gradually at the Equator than at mid-latitudes. Many of the SAO results presented are also new, in part because measurements were not previously available or were more limited in nature. At lower altitudes near 45 km, within about 15 degrees of the Equator, the temperature amplitudes for the stratospheric SAO (SSAO) reveal a local maximum of about 5 degrees K. At higher altitudes close to the Equator, our results show separate peaks of about 7 degrees K near 75 and 90 km for the mesospheric SAO (MSAO). In the SAO results, significant inter-annual differences are evident, with the amplitudes being largest in 2002 relative to 2003 and 2004. As in the case for the QBO, the SAO temperature amplitudes go through minima away from the Equator, and then increase towards mid latitudes, especially at altitudes above 55 km. We compare our findings with previously published empirical results, and with corresponding results from the numerical spectral model (NSM). Although not a focus of this study, we also show results for the inter-annual variations (which appear to be generated at least in part by the QBO) of the migrating diurnal tide. In the upper mesosphere, their amplitudes can approach 20 degrees K, and they are derived jointly with the zonal-mean components. C1 Creat Comp Solut Inc, Rockville, MD 20850 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Sci Syst & Applicat, Lanham, MD 20706 USA. RP Huang, FT (reprint author), Creat Comp Solut Inc, Rockville, MD 20850 USA. EM fthuang@comcast.net RI Mlynczak, Martin/K-3396-2012 NR 69 TC 45 Z9 48 U1 1 U2 5 PU COPERNICUS PUBLICATIONS PI KATHLENBURG-LINDAU PA MAX-PLANCK-STR 13, KATHLENBURG-LINDAU, 37191, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 8 BP 2131 EP 2149 PG 19 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 095AP UT WOS:000241280900006 ER PT J AU Feldstein, YI Popov, VA Cumnock, JA Prigancova, A Blomberg, LG Kozyra, JU Tsurutani, BT Gromova, LI Levitin, AE AF Feldstein, Y. I. Popov, V. A. Cumnock, J. A. Prigancova, A. Blomberg, L. G. Kozyra, J. U. Tsurutani, B. T. Gromova, L. I. Levitin, A. E. TI Auroral electrojets and boundaries of plasma domains in the magnetosphere during magnetically disturbed intervals SO ANNALES GEOPHYSICAE LA English DT Article DE magnetospheric physics; current systems; electric fields; magnetosphere-ionosphere interactions; storms and substorms ID FIELD-ALIGNED CURRENTS; RING CURRENT; IONOSPHERIC CURRENTS; ELECTRIC-FIELDS; POLAR-CAP; STORMS; PRECIPITATION; SUBSTORMS; WIND; CONVECTION AB We investigate variations in the location and intensity of the auroral electrojets during magnetic storms and substorms using a numerical method for estimating the equivalent ionospheric currents based on data from meridian chains of magnetic observatories. Special attention was paid to the complex structure of the electrojets and their interrelationship with diffuse and discrete particle precipitation and field-aligned currents in the dusk sector. During magnetospheric substorms the eastward electrojet (EE) location in the evening sector changes with local time from cusp latitudes (Phi similar to 77 degrees) during early afternoon to latitudes of diffuse auroral precipitation (Phi similar to 65 degrees) equatorward of the auroral oval before midnight. During the main phase of an intense magnetic storm the eastward currents in the noon-early evening sector adjoin to the cusp at Phi similar to 65 degrees and in the pre-midnight sector are located at subauroral latitude Phi similar to 57 degrees. The westward electrojet (WE) is located along the auroral oval from evening through night to the morning sector and adjoins to the polar electrojet (PE) located at cusp latitudes in the day-side sector. The integrated values of the eastward (westward) equivalent ionospheric current during the intense substorm are similar to 0.5 MA (similar to 1.5 MA), whereas they are 0.7 MA (3.0 MA) during the storm main phase maximum. The latitudes of auroral particle precipitation in the dusk sector are identical with those of both electrojets. The EE in the evening sector is accompanied by particle precipitation mainly from the Alfven layer but also from the near-Earth part of the central plasma sheet. In the lower-latitude part of the EE the field-aligned currents (FACs) flow into the ionosphere (Region 2 FAC), and at its higher-latitude part the FACs flow out of the ionosphere (Region 1 FAC). During intense disturbances, in addition to the Region 2 FAC and the Region 1 FAC, a Region 3 FAC with the downward current was identified. This FAC is accompanied by diffuse electron precipitation from the plasma sheet boundary layer. Actually, the triple system of FAC is observed in the evening sector and, as a consequence, the WE and the EE overlap. The WE in the evening sector comprises only the high-latitude periphery of the plasma precipitation region and corresponds to the Hall current between the Region 1 FAC and Region 3 FAC. During the September 1998 magnetic storm, two velocity bursts (similar to 2-4 km/s) in the magnetospheric convection were observed at the latitudes of particle precipitation from the central plasma sheet and at subauroral latitudes near the ionospheric trough. These kind of bursts are known as subauroral polarization streams (SAPS). In the evening sector the Alfven layer equatorial boundary for precipitating ions is located more equatorward than that for electrons. This may favour northward electric field generation between these boundaries and may cause high speed westward ions drift visualized as SAPS. Meanwhile, high speed ion drifts cover a wider range of latitudes than the distance between the equatorward boundaries of ions and electrons precipitation. To summarize the results obtained a new scheme of 3-D currents in the magnetosphere-ionosphere system and a clarified view of interrelated 3-D currents and magnetospheric plasma domains are proposed. C1 Slovak Acad Sci, Geophys Inst, Bratislava, Slovakia. Royal Inst Technol, Alfven Lab, Stockholm, Sweden. Inst Terr Magnetism Ionosphere & Radio Wave P, Troitsk, Moscow Region, Russia. Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA. Jet Prop Lab, Pasadena, CA USA. RP Prigancova, A (reprint author), Slovak Acad Sci, Geophys Inst, Bratislava, Slovakia. EM geofpria@savba.sk NR 66 TC 18 Z9 20 U1 0 U2 1 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 8 BP 2243 EP 2276 PG 34 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 095AP UT WOS:000241280900016 ER PT J AU Hoffmann, P Serafimovich, A Peters, D Dalin, P Goldberg, R Latteck, R AF Hoffmann, P. Serafimovich, A. Peters, D. Dalin, P. Goldberg, R. Latteck, R. TI Inertia gravity waves in the upper troposphere during the MaCWAVE winter campaign - Part 1: Observations with collocated radars SO ANNALES GEOPHYSICAE LA English DT Article DE meteorology and atmospheric dynamics; mesoscale meteorology; middle atmosphere dynamics; waves and tides ID MIDDLE ATMOSPHERE; MOUNTAIN WAVES; MST RADAR; MACQUARIE ISLAND; STRATOSPHERE; SATURATION; AUSTRALIA; MOTIONS AB During the MaCWAVE campaign, combined rocket, radiosonde and ground-based measurements have been performed at the Norwegian Andoya Rocket Range (ARR) near Andenes and the Swedish Rocket Range (ESRANGE) near Kiruna in January 2003 to study gravity waves in the vicinity of the Scandinavian mountain ridge. The investigations presented here are mainly based on the evaluation of continuous radar measurements with the ALWIN VHF radar in the upper troposphere/lower stratosphere at Andenes (69.3 degrees N, 16.0 degrees E) and the ESRAD VHF radar near Kiruna (67.9 degrees N, 21.9 degrees E). Both radars are separated by about 260 km. Based on wavelet transformations of both data sets, the strongest activity of inertia gravity waves in the upper troposphere has been detected during the first period from 2426 January 2003 with dominant vertical wavelengths of about 4-5 km as well as with dominant observed periods of about 13-14 h for the altitude range between 5 and 8 km under the additional influence of mountain waves. The results show the appearance of dominating inertia gravity waves with characteristic horizontal wavelengths of similar to 200 km moving in the opposite direction than the mean background wind. The results show the appearance of dominating inertia gravity waves with intrinsic periods in the order of similar to 5 h and with horizontal wavelengths of 200 km, moving in the opposite direction than the mean background wind. From the derived downward energy propagation it is supposed, that these waves are likely generated by a jet streak in the upper troposphere. The parameters of the jet-induced gravity waves have been estimated at both sites separately. The identified gravity waves are coherent at both locations and show higher amplitudes on the east-side of the Scandinavian mountain ridge, as expected by the influence of mountains. C1 Leibniz Inst Atmospharenphys, Kuhlungsborn, Germany. Swedish Inst Space Phys, S-98128 Kiruna, Sweden. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hoffmann, P (reprint author), Leibniz Inst Atmospharenphys, Kuhlungsborn, Germany. EM hoffmann@iap-kborn.de RI Goldberg, Richard /E-1881-2012 NR 27 TC 8 Z9 8 U1 0 U2 1 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 EI 1432-0576 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 11 BP 2851 EP 2862 PG 12 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 125GS UT WOS:000243431000008 ER PT J AU Wu, CC Lepping, RP AF Wu, C. -C. Lepping, R. P. TI Solar cycle effect on geomagnetic storms caused by interplanetary magnetic clouds SO ANNALES GEOPHYSICAE LA English DT Article DE interplanetary physics; interplanetary magnetic fields; solar wind plasma; magnetospheric physics; storms and substorms ID WIND; MAGNETOSPHERE; INTENSITY; FIELD; DST AB We investigated geomagnetic activity which was induced by interplanetary magnetic clouds during the past four solar cycles, 1965-1998. We have found that the intensity of such geomagnetic storms is more severe in solar maximum than in solar minimum. In addition, we affirm that the average solar wind speed of magnetic clouds is faster in solar maximum than in solar minimum. In this study, we find that solar activity level plays a major role on the intensity of geomagnetic storms. In particular, some new statistical results are found and listed as follows. (I) The intensity of a geomagnetic storm in a solar active period is stronger than in a solar quiet period. (2) The magnitude of negative Bz(min) is larger in a solar active period than in a quiet period. (3) Solar wind speed in an active period is faster than in a quiet period. (4) VBs(max) in an active period is much larger than in a quiet period. (5) Solar wind parameters, BZ(min), V-max and VBs(max) are correlated well with geomagnetic storm intensity, Dst(min) during a solar active period. (6) Solar wind parameters, BZ(min), and V Bs(max) are not correlated well (very poorly for V-max) with geomagnetic storm intensity during a solar quiet period. (7) The speed of the solar wind plays a key role in the correlation of solar wind parameters vs. the intensity of a geomagnetic storm. (8) More severe storms with Dst(min) <=-100 nT caused by MCs occurred in the solar active period than in the solar quiet period. C1 Univ Alabama, CSPAR, Huntsville, AL 35899 USA. Chinese Acad Sci, Key State Lab Space Weather, Beijing 100080, Peoples R China. NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Wu, CC (reprint author), Univ Alabama, CSPAR, Huntsville, AL 35899 USA. EM wuc@cspar.uah.edu NR 28 TC 7 Z9 7 U1 0 U2 1 PU EUROPEAN GEOSCIENCES UNION PI KATLENBURG-LINDAU PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY SN 0992-7689 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 12 BP 3383 EP 3389 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 135IS UT WOS:000244147900016 ER PT J AU Balasis, G Daglis, IA Kapiris, P Mandea, M Vassiliadis, D Eftaxias, K AF Balasis, G. Daglis, I. A. Kapiris, P. Mandea, M. Vassiliadis, D. Eftaxias, K. TI From pre-storm activity to magnetic storms: a transition described in terms of fractal dynamics SO ANNALES GEOPHYSICAE LA English DT Article DE magnetospheric physics; magnetospheric configuration and dynamics; solar wind-magnetosphere interactions; storms and substorms ID SELF-ORGANIZED CRITICALITY; TOPOLOGICAL PHASE-TRANSITIONS; SPACE PLASMAS; 1/F NOISE; INTERMITTENT TURBULENCE; WAVELET ANALYSIS; FIELD TOPOLOGY; AURORAL-ZONE; TIME-SERIES; COMPLEXITY AB We show that distinct changes in scaling parameters of the D-st index time series occur as an intense magnetic storm approaches, revealing a gradual reduction in complexity. The remarkable acceleration of energy release - manifested in the increase in susceptibility - couples to the transition from anti-persistent (negative feedback) to persistent (positive feedback) behavior and indicates that the occurence of an intense magnetic storm is imminent. The main driver of the D-st index, the V B-South electric field component, does not reveal a similar transition to persistency prior to the storm. This indicates that while the magnetosphere is mostly driven by the solar wind the critical feature of persistency in the magnetosphere is the result of a combination of solar wind and internal magnetospheric activity rather than solar wind variations alone. Our results suggest that the development of an intense magnetic storm can be studied in terms of "intermittent criticality" that is of a more general character than the classical self-organized criticality phenomena, implying the predictability of the magnetosphere. C1 Natl Observ Athens, Inst Space Applicat & Remote Sensing, Athens 15236, Greece. Geoforschungszentrum Potsdam, D-14473 Potsdam, Germany. Univ Athens, Solid State Sect, Dept Phys, Athens 15784, Greece. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Balasis, G (reprint author), Natl Observ Athens, Inst Space Applicat & Remote Sensing, Metaxa & Vas Pavlou St, Athens 15236, Greece. EM gbalasis@space.noa.gr RI MANDEA, Mioara/E-4892-2012; Balasis, Georgios/G-8680-2012; Daglis, Ioannis/L-6100-2013 OI Balasis, Georgios/0000-0001-7342-0557; Daglis, Ioannis/0000-0002-0764-3442 NR 54 TC 46 Z9 46 U1 1 U2 3 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 0992-7689 EI 1432-0576 J9 ANN GEOPHYS-GERMANY JI Ann. Geophys. PY 2006 VL 24 IS 12 BP 3557 EP 3567 PG 11 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 135IS UT WOS:000244147900031 ER PT S AU Markus, T Cavalieri, DJ AF Markus, Thorsten Cavalieri, Donald J. BE Langhorne, P Squire, V TI Interannual and regional variability of Southern Ocean snow on sea ice SO Annals of Glaciology, Vol 44, 2006 SE ANNALS OF GLACIOLOGY LA English DT Proceedings Paper CT International Symposium on Sea Ice CY DEC 05-09, 2005 CL Dunedin, NEW ZEALAND SP Int Glaciol Soc, Univ Otago, Natl Inst Water & Atmospher Res, Royal Soc New Zealand ID PRECIPITATION; CYCLONES AB Snow depth on sea ice plays a critical role in the heat exchange between ocean and atmosphere because of its thermal insulation property. Furthermore, a heavy snow load on the relatively thin Southern Ocean sea-ice cover submerges the ice floes below sea level, causing snow-to-ice conversion. Snowfall is also an important freshwater source into the weakly stratified ocean. Snow-depth on sea-ice information can be used as an indirect measure of solid precipitation. Satellite passive microwave data are used to investigate the interannual and regional variability of the snow cover on sea ice. In this study we make use of 12 years (1992-2003) of Special Sensor Microwave/Imager (SSM/I) radiances to calculate average monthly snow depth on the Antarctic sea-ice cover. For the Antarctic sea-ice region as a whole, we find that September snow depth and sea-ice area are negatively correlated, which is not the case for individual regions. An analysis of the snow depth around Antarctica was undertaken. The results show an overall increase in snow depth for each of the five Antarctic sectors and the region as a whole, but only the Indian Ocean sector and the entire Southern Ocean show a statistically significant increase. There is a partial eastward propagation of maximum snow depths, which may be related to the Antarctic Circumpolar Wave. The overall trend and the variability of regional snow-depth distributions are also in agreement with cyclone density. C1 NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Markus, T (reprint author), NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Code 661, Greenbelt, MD 20771 USA. RI Markus, Thorsten/D-5365-2012 NR 20 TC 4 Z9 4 U1 0 U2 3 PU INT GLACIOLOGICAL SOC PI CAMBRIDGE PA LENSFIELD RD, CAMBRIDGE CB2 1ER, ENGLAND SN 0260-3055 BN 978-0-946417-39-1 J9 ANN GLACIOL PY 2006 VL 44 BP 53 EP 57 DI 10.3189/172756406781811475 PG 5 WC Geochemistry & Geophysics; Geosciences, Multidisciplinary; Oceanography SC Geochemistry & Geophysics; Geology; Oceanography GA BGG56 UT WOS:000246685800009 ER PT S AU Comiso, JC AF Comiso, Josefino C. BE Langhorne, P Squire, V TI Impacts of the variability of second-year ice types on the decline of the Arctic perennial sea-ice cover SO Annals of Glaciology, Vol 44, 2006 SE ANNALS OF GLACIOLOGY LA English DT Proceedings Paper CT International Symposium on Sea Ice CY DEC 05-09, 2005 CL Dunedin, NEW ZEALAND SP Int Glaciol Soc, Univ Otago, Natl Inst Water & Atmospher Res, Royal Soc New Zealand ID SATELLITE-OBSERVATIONS; SURFACE; TRENDS; OCEAN AB The observed rapid decline in the Arctic perennial ice cover is one of the most remarkable signals of change in the Arctic region. Updated data now show an even higher rate of decline of 9.8% decade(-1) (1978-2005) than the previous report of 8.9% decade(-1) (1978-2000). To gain insights into this decline, the variability of the second-year ice, which is the relatively thin component of the perennial ice cover, is studied. The perennial ice cover in the 1990s was observed to be highly variable, leading to relatively high production of second-year ice that may in part explain the observed ice thinning during the period and have triggered further decline. The microwave signature of second-year ice is shown to be different from that of the older multi-year ice types and, surprisingly, more similar to that of first-year ice. This in part explains why previous estimates of the area of multi-year ice during the winter period are considerably lower than the area of the perennial ice cover during the preceding summer. Analysis of multichannel cluster maps in conjunction with submarine ice-draft data indicates ability to detect regions covered primarily by second-year ice and hence to infer ice-thickness information from the microwave data. The periodic increase of second-year ice in the 1990s was apparently followed by continuous decline due in part to anomolously warm temperatures during the latter period that shortened the ice season and kept first-year ice from getting thick enough to survive the summer and become second year ice. C1 NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614-1, Greenbelt, MD 20771 USA. NR 17 TC 2 Z9 2 U1 0 U2 1 PU INT GLACIOLOGICAL SOC PI CAMBRIDGE PA LENSFIELD RD, CAMBRIDGE CB2 1ER, ENGLAND SN 0260-3055 BN 978-0-946417-39-1 J9 ANN GLACIOL PY 2006 VL 44 BP 375 EP 382 DI 10.3189/172756406781811673 PG 8 WC Geochemistry & Geophysics; Geosciences, Multidisciplinary; Oceanography SC Geochemistry & Geophysics; Geology; Oceanography GA BGG56 UT WOS:000246685800058 ER PT S AU Brall, A Hagen, W Tran, H AF Brall, Aron Hagen, William Tran, Hung GP IEEE TI Reliability block diagram modeling - Comparisons of three software packages SO ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM, 2007 PROCEEDINGS SE Reliability and Maintainability Symposium LA English DT Proceedings Paper CT 53rd Annual Reliability and Maintainability Symposium (RAMS) CY JAN 22-25, 2007 CL Orlando, FL DE reliability modeling; reliability software; simulation AB The use of commercially available software for analyzing Reliability Block Diagrams (RBD) has become the rule for the vast majority of Reliability Analysts and Engineers. After a model has been developed and checked, a software package is generally used to evaluate the model. For the evaluation of system maintenance, especially in complex redundancy schemes, simulation is required to resolve the availability performance of the model. The results produced by the software packages are usually presented by the analyst without significant questions about the algorithms, simulation methodology, etc used by the particular software package the analyst uses. This paper provides a comparison of the results of three competitive packages. It was hypothesized that there would be differences in results due to differences in algorithms and simulation methodologies, particularly for complex models. It was not the intent of this paper to judge the relative accuracy of the results produced. The purpose of this paper is to provide awareness- to analysts that all. results of Reliability Modeling, including those produced by computer simulation packages, need to be understood in the context of the modeling methodology and solution algorithms and methodologies. It is also necessary that the results are presented with the assumptions used by the particular software package. The three software packages that were compared are Reliasoft BlockSim - Version 6.5.2, ARINC Raptor - Version 7.0.07, and Relex Software Reliability Block Diagram. This evaluation was performed with the cooperation of the software suppliers to the maximum extent possible., The results, particularly any differences, will be reviewed with the suppliers prior to this paper's presentation at RAMS 2007. The methodology used a one block diagram, a simple diagram, a complex diagram, and a project diagram. The project diagram was based on actual hardware. The other models were hypothetical. The only restriction placed on the models was that each model must be capable of being run on all of the software packages (after conversion to each software package's protocols). Special features that might be available in one or two software packages would not be evaluated. The primary effort was to assess the differences in results created by the differences in algorithms and simulation methodologies. The hypothesis was verified, even in the single block model!. C1 [Brall, Aron; Tran, Hung] NASA, Goddard Space Flight Ctr, SRS Technol Mission Support Div, Code 302-9,Bldg 6, Greenbelt, MD 20771 USA. [Hagen, William] Ford Motor Co, Greenbelt, MD USA. RP Brall, A (reprint author), NASA, Goddard Space Flight Ctr, SRS Technol Mission Support Div, Code 302-9,Bldg 6, Greenbelt, MD 20771 USA. EM abrall@pop300.gsfc.nasa.gov; whagen2@ford.com; htran@pop300.gsfc.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0149-144X BN 978-0-7803-9766-8 J9 P REL MAINT S PY 2006 BP 119 EP + PG 3 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BGS99 UT WOS:000250381800021 ER PT S AU Lee, LL Ingegneri, AJ Li, M Everett, DF AF Lee, Lydia Lam Ingegneri, Antonino J. Li, Ming Everett, David F. GP IEEE TI Probabilistic risk assessment: A practical & cost effective approach SO ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM, 2007 PROCEEDINGS SE Reliability and Maintainability Symposium LA English DT Proceedings Paper CT 53rd Annual Reliability and Maintainability Symposium (RAMS) CY JAN 22-25, 2007 CL Orlando, FL DE Probabilistic risk assessment; PRA; reliability AB This paper describes the approach taken for the reliability analyses, including Probabilistic Risk Assessments (PRAs), of the Lunar Reconnaissance Orbiter (LRO) that have been performed concurrently with the designs to identify problem areas and. ensure corrective actions were taken in a timely manner: The LRO is a large system with more than 14,000 piece-parts and over 120 purchased or contractor-built components. These analyses formulate the probability of failure for each of the components of the system. PRA then integrates these analytical techniques and results to assess the potential for failure and to help find ways to reduce the mission risks. By utilizing the traditional and innovative methods to perform reliability analyses, such as reliability predictions, Failure Modes and Effects Analysis (FMEA), and Fault Tree Analysis (FTA), the LRO project office, with close collaboration with the reliability team, has improved the probability of mission success, from 0.72 to 0.81, within a tight schedule and limited budget. As more data from the manufacturers and GSFC designs become available, the reliability and system teams will continue to update the analyses to assess risks throughout the entire lifecycle of the mission. C1 [Lee, Lydia Lam; Everett, David F.] NASA, Goddard Space Flight Ctr, Code 302, Greenbelt, MD 20771 USA. [Ingegneri, Antonino J.; Li, Ming] SRS Technol, Greenbelt, MD USA. RP Ingegneri, AJ (reprint author), NASA, Goddard Space Flight Ctr, Code 302, Greenbelt, MD 20771 USA. EM Antonino.J.Ingegneri.l@gsfc.nasa.gov; Ming.Li.l@gsfc.nasa.gov; David.F.Everett@nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0149-144X BN 978-0-7803-9766-8 J9 P REL MAINT S PY 2006 BP 147 EP + PG 3 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BGS99 UT WOS:000250381800026 ER PT S AU Rusick, JJ AF Rusick, Jeffrey J. GP IEEE TI New approach to create future high reliability NASA launch vehicle systems SO ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM, 2007 PROCEEDINGS SE Reliability and Maintainability Symposium LA English DT Proceedings Paper CT 53rd Annual Reliability and Maintainability Symposium (RAMS) CY JAN 22-25, 2007 CL Orlando, FL DE probabilistic physics-based; design margin; uncertainty; reliability; risk; design; test and evaluation AB A. new NASA approach to Launch Vehicle (LV) design and development is recommended, which will increase human rated LV reliability in the future. At its core, the new approach includes probabilistic modeling and simulation methods, which will enable the low design margins and large loading uncertainties inherent in LV's to be quantified and addressed, like they have not been on past LV programs. In order to implement the new approach, NASA will need to emphasize probabilistic modeling and simulation in its new Vision for Space Exploration (VSE) programs, like Crew Exploration Vehicle (CEV), Cargo Launch Vehicle (CaLV), and Crew Launch Vehicle (CLV), in order to move towards more reliable systems. This will require increased investment in probabilistic modeling and simulation analysis upfront. Unfortunately, the current approach to fielding these new systems in NASA is to use heritage hardware, which inherently has unquantified low design margins and large loading uncertainties, due to the way past programs have been implemented. The current approach unmodified will result in LV systems that have the same low reliability as past fielded systems. Therefore, it is recommended that NASA increase its investment in probabilistic modeling and simulation for the new VSE programs, CEV, CLV, and CaLV. One possible solution to increasing the NASA investment in probabilistic modeling and simulation for the VSE, in times of limited budget, is to obtain support from the Aeronautics Research Mission Directorate (ARMD), where the current Associate Administrator, Lisa Porter, is emphasizing probabilistic modeling and simulation. It is recommended that the ARMD probabilistic modeling and simulation expertise and Research & Technology be focused on the VSE program needs, in order to assure the development of more reliable LV systems in the future. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Rusick, JJ (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd MS 50-4, Cleveland, OH 44135 USA. EM jeffreyj.rusick@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0149-144X BN 978-0-7803-9766-8 J9 P REL MAINT S PY 2006 BP 152 EP 154 PG 3 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BGS99 UT WOS:000250381800027 ER PT S AU Huang, B Rodriguez, M Li, M Smidts, C AF Huang, Bing Rodriguez, Manuel Li, Ming Smidts, Carol GP IEEE TI On the development of fault injection profiles SO ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM, 2007 PROCEEDINGS SE Reliability and Maintainability Symposium LA English DT Proceedings Paper CT 53rd Annual Reliability and Maintainability Symposium (RAMS) CY JAN 22-25, 2007 CL Orlando, FL DE fault injection; hardware failures; probability profiles; reliability prediction; space systems ID DEPENDABILITY AB The impact of hardware failures on software has attracted substantial attention in the study of dependable systems. Fault injection techniques have emerged as a major means to evaluate software behavior in the presence of hardware failures. However, due to the lack of knowledge of the fault distribution information, the fault location and time are randomly selected. One major drawback of this approach is that the injected faults do not represent the system's operational situation, thus software reliability cannot be credibly assessed. This paper aims at extending the use of fault injection to the reliability prediction of hardware faults. To do so, we have developed a set of analytical and simulation based methods capable of statistically reproducing the underlying physics and phenomena leading to hardware failures in a given system operational context. Such distributions are referred to as fault injection profiles, and are the basis to extend the fault injection technique with fault models that represent the actual conditions under which hardware faults occur. C1 [Huang, Bing; Rodriguez, Manuel; Smidts, Carol] Univ Maryland, Ctr Reliabil Engn, College Pk, MD 20740 USA. [Li, Ming] NASA, Goddard Space Flight Ctr, SRS Technol, Greenbelt, MD 20771 USA. RP Huang, B (reprint author), Univ Maryland, Ctr Reliabil Engn, College Pk, MD 20740 USA. EM hbing@eng.umd.edu; manuel@umd.edu; mli@pop300.gsfc.nasa.gov; csmidts@eng.umd.edu FU Space Vehicle Technology Institute [NCC3-989]; NASA and DOD; NASA Constellation University Institutes; Office of Safety and Mission Assurance; NASA HQ, through the SARP Program FX This work was supported by the Space Vehicle Technology Institute under grant NCC3-989 jointly funded by NASA and DOD within the NASA Constellation University Institutes Project, with Claudia Meyer as the project manager. This work was also supported by the Office of Safety and Mission Assurance, NASA HQ, through the SARP Program managed by NASA IV&V. NR 19 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0149-144X BN 978-0-7803-9766-8 J9 P REL MAINT S PY 2006 BP 226 EP + PG 3 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BGS99 UT WOS:000250381800040 ER PT S AU Venkataraman, S Strack, WC Nagpal, V Pai, SS AF Venkataraman, Satchi Strack, William C. Nagpal, Vinod Pai, Shantaram S. GP IEEE TI Incorporating distribution parameter uncertainty in reliability calculation SO ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM, 2007 PROCEEDINGS SE Reliability and Maintainability Symposium LA English DT Proceedings Paper CT 53rd Annual Reliability and Maintainability Symposium (RAMS) CY JAN 22-25, 2007 CL Orlando, FL DE parameter uncertainty; confidence intervals; sensitivity ID SENSITIVITY ESTIMATION AB Probabilistic methods for risk and reliability assessment require knowledge of statistical variation of design parameters. Often the parameters themselves are uncertain. In such cases it is important to understand how parameter uncertainties will affect the reliability measures, probability of failure or reliability index calculations. This article presents the different methods that have been developed to calculate sensitivities of reliability index (ss) or probability of failure ( P-f) to the distribution parameters. Different point and interval estimates for reliability measures in the presence of parameter uncertainty are discussed. C1 [Venkataraman, Satchi] San Diego State Univ, Dept Aerosp Engn, Mail Code 1308,5500 Campanile Dr, San Diego, CA 92182 USA. [Strack, William C.; Nagpal, Vinod] N & R Engn & Management Serv Corp, Cleveland, OH 44130 USA. [Pai, Shantaram S.] NASA, Glen Res Ctr, Cleveland, OH 44135 USA. RP Venkataraman, S (reprint author), San Diego State Univ, Dept Aerosp Engn, Mail Code 1308,5500 Campanile Dr, San Diego, CA 92182 USA. EM satchi@mail.sdsu.edu; bstrack@wowway.com; vnagpal@nrengineering.com; shantaram.s.pai@grc.nasa.gov NR 15 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0149-144X BN 978-0-7803-9766-8 J9 P REL MAINT S PY 2006 BP 298 EP + PG 3 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BGS99 UT WOS:000250381800053 ER PT S AU Datta, K AF Datta, Koushik GP IEEE TI The application of NASA risk management to the SOFIA program SO ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM, 2007 PROCEEDINGS SE Reliability and Maintainability Symposium LA English DT Proceedings Paper CT 53rd Annual Reliability and Maintainability Symposium (RAMS) CY JAN 22-25, 2007 CL Orlando, FL DE SOFIA; risk management; PRA; hazard mitigation AB NASA and DLR (German Aerospace Center) have been working together to create the Stratospheric Observatory For Infrared Astronomy (SOFIA). SOFIA is a Boeing 747SP (Special Performance) aircraft extensively modified to accommodate a 2.5 meter reflecting telescope and airborne mission control system. This paper shows how the SOFIA program handled one safety issue through appropriate use of NASA's Risk Management Process. The safety issue was identified while reviewing the Probabilistic Risk Assessment (PRA) of a depressurization scenario in the telescope cavity. The failure scenario itself was previously known where a leak in the telescope cavity door seal sucks air out from the telescope cavity creating a negative pressure differential between the telescope cavity and the aft cavity. Two negative pressure relief valves were designed to handle this and other cavity negative pressure scenarios. However, the proposed new scenario had a leak area that was beyond the original design basis. This failure scenario was deemed credible but with a lower probability of occurrence. After identification of the safety issue, both the Risk Management and the Engineering processes required an analysis of this depressurization scenario. Multiple models of the depressurization scenarios were created and analyzed at peak dynamic pressures. The results revealed that under some failure scenarios the relief valves might not be redundant. Both valves need to function for adequate pressure equalization without exceeding structural design loads. These conditions created a program risk state that needed to be mitigated. As a result, the program started a risk mitigation plan where by a test will be performed to characterize the seal failure scenario by intentionally deflating the seal at lower dynamic pressures. The test is inherently safe at lower dynamic pressures. This paper describes the Risk Management process for this technical risk and ends by describing how the program continues to track this risk and program options for controlling the risk. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Datta, K (reprint author), NASA, Ames Res Ctr, MS 218-7, Moffett Field, CA 94035 USA. EM Koushik.Datta@nasa.gov NR 2 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0149-144X BN 978-0-7803-9766-8 J9 P REL MAINT S PY 2006 BP 410 EP 413 PG 4 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BGS99 UT WOS:000250381800072 ER PT S AU Werner, M Fazio, G Rieke, G Roellig, TL Watson, DM AF Werner, Michael Fazio, Giovanni Rieke, George Roellig, Thomas L. Watson, Dan M. TI First fruits of the Spitzer Space Telescope: Galactic and solar system studies SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS SE Annual Review of Astronomy and Astrophysics LA English DT Article; Book Chapter DE brown dwarfs; circumstellar disks; exoplanets; infrared astronomy; planetary system formation; space technology; star formation; stellar evolution ID LARGE-MAGELLANIC-CLOUD; YOUNG STELLAR OBJECTS; SUPERNOVA REMNANT CASSIOPEIA; MAIN-SEQUENCE STARS; T-TAURI STARS; TERRESTRIAL PLANET FORMATION; VEGA-LIKE STARS; KUIPER-BELT; BETA-PICTORIS; DEBRIS DISKS AB The Spitzer Space Telescope, launched in August 2003, is the infrared member of NASAs Great Observatory family. Spitzer combines the intrinsic sensitivity of a cryogenic telescope in space with the imaging and spectroscopic power of modern infrared detector arrays. This review covers early results from Spitzer that have produced major advances in our understanding of our own solar system and phenomena within the Galaxy. Spitzer has made the first detection of light from extrasolar planets, characterized planet-forming and planetary debris disks around solar-type stars, showed that substellar objects with masses smaller than 10 M(Jup) form through the same processes as do solar-mass stars, and studied in detail the composition of cometary ejecta in our Solar System. Spitzer major technical advances will pave the way for yet more powerful future instruments. Spitzer should operate with full capabilities well into 2009, enabling several additional cycles of discovery and follow-up. C1 CALTECH, Jet Prop Lab, Astron & Phys Directorate, Pasadena, CA 91109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Werner, M (reprint author), CALTECH, Jet Prop Lab, Astron & Phys Directorate, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mwerner@sirtfweb.jpl.nasa.gov; gfazio@cfa.harvard.edu; grieke@as.arizona.edu; thomas.l.roellig@nasa.gov; dmw@pas.rochester.edu NR 193 TC 33 Z9 33 U1 0 U2 3 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 BN 978-0-8243-0944-2 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2006 VL 44 BP 269 EP 321 DI 10.1146/annurev.astro.44.051905.092544 PG 53 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 105MU UT WOS:000242035100008 ER PT S AU Bottke, WF Vokrouhlicky, D Rubincam, DP Nesvorny, D AF Bottke, William F., Jr. Vokrouhlicky, David Rubincam, David P. Nesvorny, David TI The Yarkovsky and YORP effects: Implications for asteroid dynamics SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES SE Annual Review of Earth and Planetary Sciences LA English DT Review; Book Chapter DE asteroids; meteorites; asteroids-dynamics; celestial mechanics; nongravitational forces ID NEAR-EARTH ASTEROIDS; MEAN MOTION RESONANCE; SOLAR-SYSTEM; MAIN-BELT; SIZE DISTRIBUTION; KORONIS FAMILY; THERMAL DRAG; DETECTION OPPORTUNITIES; NUMERICAL EVALUATION; NONLINEARIZED THEORY AB The Yarkovsky and YORP (Yarkovsky-O'Keefe-Radzievskii-Paddack) effects are thermal radiation forces and torques that cause small objects to undergo semimajor axis drift and spin vector modifications, respectively, as a function of their spin, orbit, and material properties. These mechanisms help to (a) deliver asteroids (and meteoroids) with diameter D < 40 km from their source locations in the main belt to chaotic resonance zones capable of transporting this material to Earth-crossing orbits; (b) disperse asteroid families, with drifting bodies jumping or becoming trapped in mean-motion and secular resonances within the main belt; (c) modify the rotation rates and obliquities of D < 40 km asteroids; and (d) allow asteroids to enter into spin-orbit resonances, which affect the evolution of their spin vectors and feedback into the Yarkovsky-driven semimajor axis evolution. Accordingly, we suggest that nongravitational forces should now be considered as important as collisions and gravitational perturbations to our overall understanding of asteroid evolution. C1 SW Res Inst, Boulder, CO 80302 USA. Charles Univ Prague, Inst Astron, CR-18000 Prague 8, Czech Republic. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bottke, WF (reprint author), SW Res Inst, Boulder, CO 80302 USA. EM bottke@boulder.swri.edu RI Rubincam, David/D-2918-2012 NR 105 TC 269 Z9 271 U1 5 U2 18 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0084-6597 BN 978-0-8243-2034-8 J9 ANNU REV EARTH PL SC JI Annu. Rev. Earth Planet. Sci. PY 2006 VL 34 BP 157 EP 191 DI 10.1146/annurev.earth.34.031405.125154 PG 35 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 054MI UT WOS:000238380600007 ER PT J AU Parkinson, CL AF Parkinson, Claire L. TI Earth's cryosphere: Current state and recent changes SO ANNUAL REVIEW OF ENVIRONMENT AND RESOURCES SE Annual Review of Environment and Resources LA English DT Review; Book Chapter DE climate change; glaciers; ice sheets; ice shelves; permafrost; sea ice; sea level rise ID ARCTIC-SEA-ICE; HEMISPHERE SNOW EXTENT; RECENT CLIMATE-CHANGE; MASS-BALANCE; NORTHERN-HEMISPHERE; ANTARCTIC PENINSULA; WEST ANTARCTICA; EAST ANTARCTICA; TIME-SERIES; LEVEL RISE AB Earth continues to have a third of the ice that it had at the peak of the last ice age, although that ice continues to decrease, as it has, overall, for the past 18,000 years. Over the last 100 years, the retreat signal has been especially strong in ice shelves of the Arctic and along the Antarctic Peninsula, with a more mixed signal elsewhere. For instance, since the early 1990s, the massive Greenland and Antarctic ice sheets have thinned along the coasts but thickened in the interior, and since the late 1970s, sea ice has decreased in the Arctic but increased (slightly) in the Antarctic. Major difficulties in the interpretations of the climate record come from the high interannual variability of most cryosphere components and the lack of consistent long-term global data records; the latter problem is now being slowly remedied, in part, through satellite technology. C1 NASA Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. RP Parkinson, CL (reprint author), NASA Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614-1, Greenbelt, MD 20771 USA. EM claire.l.parkinson@nasa.gov RI Parkinson, Claire/E-1747-2012 OI Parkinson, Claire/0000-0001-6730-4197 NR 107 TC 8 Z9 9 U1 3 U2 18 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 1543-5938 J9 ANNU REV ENV RESOUR JI Annu. Rev. Environ. Resour. PY 2006 VL 31 BP 33 EP 60 DI 10.1146/annurev.energy.31.041105.095552 PG 32 WC Environmental Sciences; Environmental Studies SC Environmental Sciences & Ecology GA 109QZ UT WOS:000242324900003 ER PT S AU Bushnell, DM AF Bushnell, DM TI Scaling: Wind tunnel to flight SO ANNUAL REVIEW OF FLUID MECHANICS SE Annual Review of Fluid Mechanics LA English DT Review; Book Chapter DE aeronautics; wind tunnel; scaling; flight; corrections AB Wind tunnels have wide-rangiug functionality, including many applicitions beyond aeronautics, and historically have been the major source of information for tech. nological aerodynamics/aeronautical applications. There are a myriad of scaling issues/differences from flight to wind tunnel, and their study and impacts are uneven and a function of the particular type of extant flow phenomena. Typically, the most serious discrepancies are associated with flow separation The tremendous on. going increases in numerical siumlation capability are changing and in many aspects have changed the function of the wind tunnel from a (scaled) "predictor" to a source of computational calibration/validation imformation with the computation then utilized as the flight prediction/scaling tool. Numerical simulations call increasingly include the influences of the various scaling issues. This wind tunnel role change has been occurring for decades as computational capability improves in all aspects. Additional issues driving this trend are the increasing cost (and time) disparity between physical experiments and computations, and increasingly stringent accuracy requirements. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Bushnell, DM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM Dennis.M.Bushnell@nasa.gov NR 116 TC 11 Z9 12 U1 0 U2 11 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4189 BN 978-0-8243-0738-7 J9 ANNU REV FLUID MECH JI Annu. Rev. Fluid Mech. PY 2006 VL 38 BP 111 EP 128 DI 10.1146/annurev.fluid.38.050304.092208 PG 18 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 012XJ UT WOS:000235373900005 ER PT J AU Wang, M Freund, JB Lele, SK AF Wang, M Freund, JB Lele, SK TI Computational prediction of flow-generated sound SO ANNUAL REVIEW OF FLUID MECHANICS SE Annual Review of Fluid Mechanics LA English DT Review; Book Chapter DE aeroacoustics; flow noise; computational methods; acoustic analogy; turbulence simulation; noise control ID LARGE-EDDY SIMULATION; TRAILING-EDGE NOISE; FINITE-DIFFERENCE SCHEMES; FINE-SCALE TURBULENCE; SUPERSONIC JET NOISE; LOW-REYNOLDS-NUMBER; ACOUSTIC ANALOGY; BOUNDARY-LAYER; MIXING NOISE; ISOTROPIC TURBULENCE AB This article provides a critical review of computational techniques for flow-noise prediction and the underlying theories. Hybrid approaches, in which the turbulent noise source field is computed and/or modeled separately from the far-field calculation, are afforded particular attention. Numerical methods and modern flow simulation techniques are discussed in terms of their suitability and accuracy for flow-noise calculations. Other topics highlighted include some important formulation and computational issues in the application of aeroacoustic theories, generalized acoustic analogies with better accounts of flow-sound interaction, and recent computational investigations of noise-control strategies. The review ends with an analysis of major challenges and key areas for improvement in order to advance the state of the art of computational aeroacoustics. C1 Stanford Univ, NASA, Ames Res Ctr, Ctr Turbulence Res, Stanford, CA 94305 USA. Univ Illinois, Dept Theoret & Appl Mech, Urbana, IL 61801 USA. Stanford Univ, Dept Mech Engn, Stanford, CA 94305 USA. Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. RP Stanford Univ, NASA, Ames Res Ctr, Ctr Turbulence Res, Stanford, CA 94305 USA. EM wangm@stanford.edu; jbfreund@uiuc.edu; lele@stanford.edu RI Wang, Meng/C-1622-2012; Freund, Jonathan/A-6409-2014 NR 127 TC 133 Z9 155 U1 9 U2 81 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4189 J9 ANNU REV FLUID MECH JI Annu. Rev. Fluid Mech. PY 2006 VL 38 BP 483 EP 512 DI 10.1146/annurev.fluid.38.050304.092036 PG 30 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 012XJ UT WOS:000235373900018 ER PT S AU Lu, S El-Sharkawi, MA Kirkham, H Howe, BM AF Lu, S El-Sharkawi, MA Kirkham, H Howe, BM GP IEEE TI NEPTUNE power system: Startup power supply for 10 kV to 400 V Dc-Dc converters SO APEC 2006: TWENTY-FIRST ANNUAL IEEE APPLIED POWER ELECTRONICS CONFERENCE AND EXPOSITION, VOLS 1-3 SE Annual IEEE Applied Power Electronics Conference and Exposition (APEC) LA English DT Proceedings Paper CT 21st Annual IEEE Applied Power Electronics Conference (APEC 2006) CY MAR 19-23, 2006 CL Dallas, TX SP IEEE, PELS, IEEE Ind Applicat Soc, Power Sources Manufacturers Assoc AB NEPTUNE (North-East Pacific Time-series Undersea Networked Experiments) is an underwater power and communications network for scientific experiments. It is proposed for the ocean floor of the Juan de Fuca tectonic plate in the Northeast Pacific Ocean. In the science nodes connected to NEPTUNE network, 10 kV to 400 V dc-dc converters are used to power various scientific instruments and underwater vehicles. The focus of this paper is the startup of the science node converters. The configuration of the NEPTUNE power system is introduced and the challenges of the system resulting from its location on the seafloor are addressed. The set of operations designed to start the 10 kV converters, which includes the control of the 10 kV switches connecting cables to converters, checking faults, and the starting of these converters, is described. These operations require a low voltage startup power supply which obtains energy directly from the 10 kV line. Several commonly used converter startup techniques are reviewed and their capabilities to solving this problem are discussed. Then the proposed circuit design of the startup power supply is presented. The circuit has been implemented and tested. Test results are provided. C1 Univ Washington, Dept EE, Seattle, WA 98195 USA. CALTECH, JPL, Pasadena, CA USA. Washington Univ, APL, St Louis, MO USA. RP Univ Washington, Dept EE, Seattle, WA 98195 USA. EM lushuai@u.washington.edu OI Howe, Bruce/0000-0001-5711-5253; Kirkham, Harold/0000-0003-2893-7586 FU National Science Foundation [OCE 0116750]; "Development of a Power System for Cabled Ocean Observatories" FX This development effort is sponsored by the National Science Foundation grant OCE 0116750, "Development of a Power System for Cabled Ocean Observatories." NR 9 TC 1 Z9 2 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1048-2334 BN 0-7803-9547-6 J9 APPL POWER ELECT CO PY 2006 BP 1385 EP 1389 PG 5 WC Engineering, Electrical & Electronic SC Engineering GA BEB94 UT WOS:000236635700213 ER PT J AU Cottrell, MT Mannino, A Kirchman, DL AF Cottrell, MT Mannino, A Kirchman, DL TI Aerobic anoxygenic phototrophic bacteria in the Mid-Atlantic Bight and the North Pacific Gyre SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID LEUCINE INCORPORATION; AQUATIC ENVIRONMENTS; BIOMASS PRODUCTION; SARGASSO SEA; GROWTH-RATE; OCEAN; BACTERIOCHLOROPHYLL; BACTERIOPLANKTON; LIGHT; PROTEOBACTERIA AB The abundance of aerobic anoxygenic phototrophic (AAP) bacteria, cyanobacteria, and heterotrophs was examined in the Mid-Atlantic Bight and the central North Pacific Gyre using infrared fluorescence microscopy coupled with image analysis and flow cytometry. AAP bacteria comprised 5% to 16% of total prokaryotes in the Atlantic Ocean but only 5% or less in the Pacific Ocean. In the Atlantic, AAP bacterial abundance was as much as 2-fold higher than that of Prochlorococcus spp. and 10-fold higher than that of Synechococcus spp. In contrast, Prochlorococcus spp. outnumbered AAP bacteria 5- to 50-fold in the Pacific. In both oceans, subsurface abundance maxima occurred within the photic zone, and AAP bacteria were least abundant below the 1% light depth. The abundance of AAP bacteria rivaled some groups of strictly heterotrophic bacteria and was often higher than the abundance of known AAP bacterial genera (Erythrobacter and Roseobacter spp.). Concentrations of bacteriochlorophyll a (BChl a) were low (similar to 1%) compared to those of chlorophyll a in the North Atlantic. Although the BChl a content of AAP bacteria per cell was typically 20- to 250-fold lower than the divinyl-chlorophyll a content of Prochlorococcus, the pigment content of AAP bacteria approached that of Prochlorococcus in shelf break water. Our results suggest that AAP bacteria can be quite abundant in some oceanic regimes and that their distribution in the water column is consistent with phototrophy. C1 Univ Delaware, Coll Marine Studies, Lewes, DE 19958 USA. NASA, Goddard Space Flight Ctr, Lab Hydrospher Proc, Greenbelt, MD 20771 USA. RP Cottrell, MT (reprint author), Univ Delaware, Coll Marine Studies, 700 Pilottown Rd, Lewes, DE 19958 USA. EM mattcott@udel.edu RI Mannino, Antonio/I-3633-2014; Cottrell, Matthew/C-3266-2009 NR 40 TC 85 Z9 88 U1 2 U2 17 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD JAN PY 2006 VL 72 IS 1 BP 557 EP 564 DI 10.1128/AEM.72.1.557-564.2006 PG 8 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 003DW UT WOS:000234662800073 PM 16391092 ER PT J AU Liu, X Smith, WL Zhou, DK Larar, A AF Liu, X Smith, WL Zhou, DK Larar, A TI Principal component-based radiative transfer model for hyperspectral sensors: theoretical concept SO APPLIED OPTICS LA English DT Article ID ACCURATE TRANSMITTANCE MODEL; INHOMOGENEOUS ATMOSPHERES; ABSORBING GAS; COMPUTATIONALLY FAST; SPECTRAL RADIANCES; TROPOSPHERIC OZONE; MIXING RATIOS; IMPROVEMENTS; SIMULATIONS; ABSORPTION AB Modern infrared satellite sensors such as the Atmospheric Infrared Sounder (AIRS), the Cross-Track Infrared Sounder (CrIS), the Tropospheric Emission Spectrometer (TES), the Geosynchronous Imaging Fourier Transform Spectrometer (GIFTS), and the Infrared Atmospheric Sounding Interferometer (IASI) are capable of providing high spatial and spectral resolution infrared spectra. To fully exploit the vast amount of spectral information from these instruments, superfast radiative transfer models are needed. We present a novel radiative transfer model based on principal component analysis. Instead of predicting channel radiance or transmittance spectra directly, the principal component-based radiative transfer model (PCRTM) predicts the principal component (PC) scores of these quantities. This prediction ability leads to significant savings in computational time. The parameterization of the PCRTM model is derived from the properties of PC scores and instrument line-shape functions. The PCRTM is accurate and flexible. Because of its high speed and compressed spectral information format, it has great potential for superfast one-dimensional physical retrieval and for numerical weather prediction large volume radiance data assimilation applications. The model has been successfully developed for the NAST-I and AIRS instruments. The PCRTM model performs monochromatic radiative transfer calculations and is able to include multiple scattering calculations to account for clouds and aerosols. (c) 2006 Optical Society of America. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Hampton Univ, Hampton, VA 23668 USA. RP Liu, X (reprint author), NASA, Langley Res Ctr, MS401A, Hampton, VA 23681 USA. EM xu.liu-1@nasa.gov NR 43 TC 60 Z9 62 U1 2 U2 6 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD JAN 1 PY 2006 VL 45 IS 1 BP 201 EP 209 DI 10.1364/AO.45.000201 PG 9 WC Optics SC Optics GA 001RI UT WOS:000234553600027 PM 16422339 ER PT S AU Xiang, G Starks, SA Kreinovich, V Longpre, L AF Xiang, G Starks, SA Kreinovich, V Longpre, L BE Dongarra, J Madsen, K Wasniewski, J TI New algorithms for statistical analysis of interval data SO APPLIED PARALLEL COMPUTING: STATE OF THE ART IN SCIENTIFIC COMPUTING SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 7th International Workshop on State of the Art in Scientific Computing CY JUN 20-23, 2004 CL Lyngby, DENMARK SP Tech Univ Denmark, Dept Informat & Math Modelling, High Performance Comp, Numerical Algorithms Grp Ltd, Comsol A/S Denmark, Sun Microsyst Denmark, UNI C Danish Comp Ctr Denmark, Microsoft Denmark, IBM, Denmark AB It is known that in general, statistical analysis of interval data is an NP-hard problem: even computing the variance of interval data is, in general, NP-hard. Until now, only one case was known for which a feasible algorithm can compute the variance of interval data: the case when all the measurements are accurate enough - so that even after the measurement, we can distinguish between different measured values (x) over tilde (i). In this paper, we describe several new cases in which feasible algorithms are possible - e.g., the case when all the measurements are done by using the same (not necessarily very accurate) measurement instrument - or at least a limited number of different measuring instruments. C1 Univ Texas, NASA, Pan Amer Ctr Earth & Environm Studies, El Paso, TX 79968 USA. RP Xiang, G (reprint author), Univ Texas, NASA, Pan Amer Ctr Earth & Environm Studies, El Paso, TX 79968 USA. EM vladik@cs.utep.edu NR 4 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-29067-2 J9 LECT NOTES COMPUT SC PY 2006 VL 3732 BP 189 EP 196 PG 8 WC Computer Science, Theory & Methods SC Computer Science GA BEE79 UT WOS:000237003200021 ER PT S AU Jost, G Chun, R Jin, HQ Labarta, J Gimenez, J AF Jost, G Chun, R Jin, HQ Labarta, J Gimenez, J BE Dongarra, J Madsen, K Wasniewski, J TI An expert assistant for computer aided parallelization SO APPLIED PARALLEL COMPUTING: STATE OF THE ART IN SCIENTIFIC COMPUTING SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 7th International Workshop on State of the Art in Scientific Computing CY JUN 20-23, 2004 CL Lyngby, DENMARK SP Tech Univ Denmark, Dept Informat & Math Modelling, High Performance Comp, Numerical Algorithms Grp Ltd, Comsol A/S Denmark, Sun Microsyst Denmark, UNI C Danish Comp Ctr Denmark, Microsoft Denmark, IBM, Denmark AB The prototype implementation of an expert system was developed to assist the user in the computer aided parallelization process. The system interfaces to tools for automatic parallelization and performance analysis. By fusing static program structure information and dynamic performance analysis data the expert system can help the user to filter, correlate, and interpret the data gathered by the existing tools. Sections of the code that show poor performance and require further attention are rapidly identified and suggestions for improvements are presented to the user. In this paper we describe the components of the expert system and discuss its interface to the existing tools. We present a case study to demonstrate the successful use in full scale scientific applications. C1 NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA. San Jose State Univ, Dept Comp Sci, San Jose, CA 95192 USA. Tech Univ Catalonia, CEPBA UPC, European Ctr Parallelism Barcelona, Barcelona 08034, Spain. RP Jost, G (reprint author), NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA. EM gjost@nas.nasa.gov; Robert.Chun@sjsu.edu; hjin@nas.nasa.gov; jesus@cepba.upc.es; judit@cepba.upc.es RI Labarta, Jesus/G-5256-2015 OI Labarta, Jesus/0000-0002-7489-4727 NR 7 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-29067-2 J9 LECT NOTES COMPUT SC PY 2006 VL 3732 BP 665 EP 674 PG 10 WC Computer Science, Theory & Methods SC Computer Science GA BEE79 UT WOS:000237003200080 ER PT S AU Howard, A Tunstel, E AF Howard, Ayanna Tunstel, Edward BE Abraham, A DeBaets, B Koppen, M Nickolay, B TI A self-contained traversability sensor for safe mobile robot guidance in unknown terrain SO APPLIED SOFT COMPUTING TECHNOLOGIES: THE CHALLENGE OF COMPLEXITY SE ADVANCES IN SOFT COMPUTING LA English DT Proceedings Paper CT 9th Online Conference on Soft Computing in Industrial Applications CY SEP 20-OCT 08, 2004 CL ELECTR NETWORK SP World Federat Soft Comp, Elsevier, Springer, IEEE Syst, Man & Cybernet Soc, NAFIPS, European Soc Fuzzy Log & Technol, Int Fuzzy Syst Assoc DE mobile robot; rover; traversability; cognitive sensor; fuzzy logic; distributed processing ID PLANETARY ROVERS AB Autonomous mobile robots capable of intelligent behavior must operate with minimal human interaction, have the capability to utilize local resources, and routinely make closed-loop decisions in real-time based on sensor data inputs. One of the bottlenecks in achieving this is an often computationally intensive perception process. In this paper, we discuss a class of cognitive sensor devices capable of intelligent perception that can facilitate intelligent behavior. The primary emphasis is on achieving safe mobile guidance for planetary exploration by distributing some of the perception functionality to self-contained sensors. An example cognitive sensor, called the traversability sensor, is presented, which consists of a camera and embedded processor coupled with an intelligent visual perception algorithm. The sensor determines local terrain traversability in natural outdoor environments and, accordingly, directs movement of a mobile robot toward the safest visible terrain area in a self-contained fashion, placing minimal burden on the main processor. A cognitive sensor design approach is presented and a traversability sensor prototype is described. C1 [Howard, Ayanna; Tunstel, Edward] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Howard, A (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. EM howard@robotics.jpl.nasa.gov; tunstel@robotics.jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 22 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 1615-3871 BN 3-540-31649-3 J9 ADV SOFT COMP PY 2006 VL 34 BP 731 EP 748 DI 10.1007/3-540-31662-0_56 PG 18 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications SC Computer Science GA BEN47 UT WOS:000238287700056 ER PT S AU Denney, E Fischer, B AF Denney, Ewen Fischer, Bernd GP IEEE COMPUTER SOC TI Annotation inference for safety certification of automatically generated code (extended abstract) SO ASE 2006: 21ST IEEE INTERNATIONAL CONFERENCE ON AUTOMATED SOFTWARE ENGINEERING, PROCEEDINGS SE IEEE ACM International Conference on Automated Software Engineering LA English DT Proceedings Paper CT 21st IEEE International Conference on Automated Software Engineering CY SEP 22, 2006 CL Tokyo, JAPAN SP IEEE Comp Soc TCSE, ACM SIGSOFT, ACM SIGART, ACM, Japan Chapter, Informat Proc Soc Japan, ASE Program Comm, Natl Inst Informat Japan, Univ Toronto, CSK Holdings Corp, Hatachi Ltd, NEC Corp, NTT Data Corp, Toshiba Corp, Toshiba Informat Syst Corp C1 [Denney, Ewen] NASA, USRA RIACS, Moffett Field, CA 94035 USA. [Fischer, Bernd] Univ Southampton, ECS, Southampton SO9 5NH, Hants, England. RP Denney, E (reprint author), NASA, USRA RIACS, Moffett Field, CA 94035 USA. EM edenney@email.arc.nasa.gov; B.Fischer@ecs.soton.ac.uk NR 9 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA SN 1527-1366 BN 0-7695-2579-2 J9 IEEE INT CONF AUTOM PY 2006 BP 265 EP 268 PG 4 WC Computer Science, Software Engineering SC Computer Science GA BFI73 UT WOS:000242043600029 ER PT S AU Jackson, WM Glaz, M Cochran, AL Meech, KJ AF Jackson, William M. Glaz, Micah Cochran, Anita L. Meech, Karen J. BE Kaiser, RI Bernath, P Osamura, Y Petrie, S Mebel, AM TI An astronomical pump probe experiment with deep impact and the keck telescope SO ASTROCHEMISTRY: FROM LABORATORY STUDIES TO ASTRONOMICAL OBSERVATIONS SE AIP Conference Proceedings LA English DT Proceedings Paper CT Symposium on Astrochemistry - From Laboratory Studies to Astronomical Observations CY DEC 18-20, 2005 CL Honolulu, HI SP Amer Chem Soc, Natl Sci Fdn DE deep impact encounter; cometary molecules; cometary radicals; spectrometry; primordial material ID PHOTODISSOCIATION DYNAMICS; 193 NM; BRANCHING RATIOS; COMETS; C-2; C2H; PHOTOCHEMISTRY; ALLENE; ISOMERIZATION; PHOTOLYSIS AB High resolution spectra from 3050-5800 A from the emissions from the coma of comet 9P/Tempel 1 were recorded using the high resolution echelle spectrograph, HIRES, attached to the Keck 1 telescope. The spectra were taken before the Deep Impact encounter in May as well as during and after it on July 4, 5, and 6. All of the typical cometary radicals such as OH, NE, NH2, CN, C-2, and C-3 have been identified. The O(S-1) emission from the comet has clearly been separated from the auroral line and identified. The spectral distributions of the emissions observed in May before impact was similar to those after the impact in July. This indicates that in this comet the material that was evacuated 20 meters under the surface of the comet was similar to the material at the surface of the comet. It suggests that solar processing of surface material does not significantly affect the UV and visible emissions from comets so that variations in the spectra are probably useful for inferring the region where the comets are formed in the early solar system. No new emissions or prompt emissions stand out in the data. The chemical mechanism for the production of these radicals is described, along with gaps in our knowledge that needs to be addressed. C1 [Jackson, William M.; Glaz, Micah] Univ Calif Davis, Dept Chem, 1 Shields Ave, Davis, CA 95618 USA. [Cochran, Anita L.] Univ Texas Austin, Univ Stn 1, McDonald Observ, Austin, TX 78712 USA. [Meech, Karen J.] Univ Hawaii, NASA Astrobiol Inst, Inst Astron, Honolulu, HI 96822 USA. RP Jackson, WM (reprint author), Univ Calif Davis, Dept Chem, 1 Shields Ave, Davis, CA 95618 USA. NR 26 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 0-7354-0351-1 J9 AIP CONF PROC PY 2006 VL 855 BP 183 EP + PG 3 WC Astronomy & Astrophysics; Chemistry, Analytical SC Astronomy & Astrophysics; Chemistry GA BFD89 UT WOS:000241319800022 ER PT S AU Lyons, DT Desai, PN AF Lyons, Daniel T. Desai, Prasun N. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Adventures in parallel processing: Entry, descent and landing simulation for the Genesis and Stardust missions SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB This paper will describe the Entry, Descent and Landing simulation tradeoffs and techniques that were used to provide the Monte Carlo data required to approve entry during a critical period just before entry of the Genesis Sample Return Capsule. The same techniques will be used again when Stardust returns on January 15, 2006. Only one hour was available for the simulation which propagated 2000 dispersed entry states to the ground. Creative simulation tradeoffs combined with parallel processing were needed to provide the landing footprint statistics that were an essential part of the Go/NoGo decision that authorized release of the Sample Return Capsule a few hours before entry. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lyons, DT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 273 EP 284 PN 1-3 PG 12 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804700016 ER PT S AU Buffington, B Strange, N Ionasescu, R AF Buffington, Brent Strange, Nathan Ionasescu, Rodica BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Addition of a low altitude Tethys flyby to the nominal Cassini tour SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB Of the eight Saturnian icy satellites, all but Mimas and Tethys had low altitude targeted flybys during the 4-year primary Cassini spacecraft tour of the Saturnian system. In November 2004, the existence of a potential low-altitude Tethys flyby was discovered; this low-altitude flyby, added to the nominal tour in March 2005, corresponds to a 1500 km non-targeted periapsis altitude on September 24, 2005 with an associated Delta v cost of approximately 8 m/s. This paper details the methods used to determine the Rev-15 non-targeted Tethys flyby altitude, driven by navigational requirements and operational constraints, in addition to several trajectory modifications implemented to reduce total Delta v costs, and in some cases, render simultaneous increases in scientific return. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Buffington, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 325 EP 344 PN 1-3 PG 20 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804700019 ER PT S AU Beckman, M Janes, L AF Beckman, Mark Janes, Leigh BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Finding acceptable James Webb Space Telescope mission orbits from a fixed Ariane flight profile SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB The James Webb Space Telescope (JWST) will be launched into orbit about the Sun/Earth L2 libration point. Trajectory design was recently completed which included expected separation states from the Ariane launch vehicle, constraints such as eclipses, maximum orbit size, maximum Sun-Vehicle-Earth/Moon angles, and launch opportunities. The results of this trajectory design give a set of possible trajectories for JWST with bounded stray light zones and provide a complete launch window. This data is also used to design the initial trajectory correction maneuver such that a maneuver towards the Sun is not required. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Beckman, M (reprint author), NASA, Goddard Space Flight Ctr, Code 595, Greenbelt, MD 20771 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 345 EP 356 PN 1-3 PG 12 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804700020 ER PT S AU Folta, DC Vaughn, FJ Westmeyer, PA Rawitscher, GS Bordi, F AF Folta, David C. Vaughn, Frank J., Jr. Westmeyer, Paul A. Rawitscher, Gary S. Bordi, Francesco BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Enabling exploration missions now: Applications of on-orbit staging SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB Future NASA exploration objectives are difficult to meet using current propulsion architectures and fuel-optimal trajectories. We introduce the concept of On-Orbit Staging and combine it with the idea of pre-positioned fuel and supply depots to increase payload mass and reduce overall cost, schedule, and risk for missions proposed as a part of the NASA Vision for Space Exploration. The On-Orbit Staging concept extends the implementation of ideas originally put forth by Tsiolkovsky, Oberth and Von Braun to address the total mission design. Applying the basic staging concept to all major propulsive (orbit) events and utilizing technological advances in propulsion efficiency and architecture allows us to demonstrate that exploration and science goals can be met more effectively and efficiently. As part of this architecture, we assume the readiness of automated rendezvous, docking/berthing, and assembly technology, all of which will be required for any credible exploration architecture. Primary cost drivers are identified and strategies that utilize On-Orbit Staging to reduce these costs are discussed. C1 NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Greenbelt, MD 20771 USA. RP Folta, DC (reprint author), NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Code 595, Greenbelt, MD 20771 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 377 EP 396 PN 1-3 PG 20 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804700022 ER PT S AU Raofi, B AF Raofi, Behzad BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Flight path control strategies and preliminary Delta V requirements for the 2007 Mars Phoenix (PHX) Mission SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB In August 2007, the Mars Phoenix (PHX) Project will launch a spacecraft to Mars whose objective is to deliver a stationary lander to a landing site in the latitude band from 65 degrees N to 72 degrees N. Instruments on the lander will perform in-situ and remote-sensing investigations to characterize the chemistry of materials at the local surface, subsurface, and atmosphere. Lander instruments will also identify the potential provenance of key indicator elements of significance to the biological potential of Mars, including potential organics within any accessible water ice. This paper describes the methods used to estimate the statistical Delta V requirements for the propulsive maneuvers that will deliver the spacecraft to its target landing site while satisfying planetary protection requirements. The paper presents flight path control analysis results for three different trajectories, Open, Middle, and Close of launch period for the mission. The results for a representative landing site (70 degrees N, 230 degrees E) indicate that the open case involves the most demanding Delta V requirement (52.4 m/s) and that the inertial atmospheric entry flight path angle delivery requirement of -12.5 +/- 0.27 (3 sigma) degrees is achievable. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Raofi, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 567 EP 584 PN 1-3 PG 18 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804700032 ER PT S AU Goodson, T Buffington, B Hahn, Y Strange, N Wagner, S Wong, M AF Goodson, T. D. Buffington, B. B. Hahn, Y. Strange, N. J. Wagner, S. V. Wong, M. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Cassini-Huygens maneuver experience: Cruise and arrival at Saturn SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB The Cassini-Huygens mission to Saturn and Titan was launched in 1997. It is an international effort to study the Saturnian system. Cassini-Huygens' interplanetary cruise delivered the spacecraft to Saturn in 2004. It also made use of many propulsive maneuvers, both statistical and deterministic. Maneuver-related analysis and performance for the latter half of cruise is reported. The system has performed more accurately than the pre-launch expectations and requirements. Additionally, some maneuvers have already been skipped, saving propellant and flight team effort. Analysis of historical execution error data is presented. C1 CALTECH, Jet Prop Lab, Cassini Navigat Team, Pasadena, CA 91109 USA. RP Goodson, T (reprint author), CALTECH, Jet Prop Lab, Cassini Navigat Team, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 34 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 585 EP 607 PN 1-3 PG 23 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804700033 ER PT S AU Wagner, SV Buffington, BB Goodson, TD Hahn, Y Strange, NJ Wong, MC AF Wagner, Sean V. Buffington, Brent B. Goodson, Troy D. Hahn, Yungsun Strange, Nathan J. Wong, Mau C. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Cassini-Huygens maneuver experience: First year of Saturn tour SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB This paper documents the maneuver experience gained from the Cassini-Huygens mission during the first year of Saturn tour. Since Saturn arrival, the Cassini spacecraft has made several flybys of Saturn's satellites and has delivered the Huygens probe to Titan. Of the 20+ maneuvers executed in the first year of tour, the Periapsis Raise Maneuver, the Probe Targeting Maneuver, and the Orbiter Deflection Maneuver were the most defining. Highlights of this paper include tour maneuver strategies and a preliminary analysis of the execution errors of maneuvers performed to date. In its first year at Saturn, Cassini has been navigated with great success. C1 CALTECH, Jet Prop Lab, Cassini Navigat Team, Pasadena, CA 91109 USA. RP Wagner, SV (reprint author), CALTECH, Jet Prop Lab, Cassini Navigat Team, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 609 EP 628 PN 1-3 PG 20 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804700034 ER PT S AU Gaskell, RW AF Gaskell, Robert W. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Landmark navigation and target characterization in a simulated Itokawa encounter SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB A simulated asteroid Itokawa was constructed from the latest radar model (Ostro, 2004) by adding craters, rocks and fractal surfacing. Images were constructed from this simulation with known spacecraft positions and orientations, and asteroid pole and shape as "ground truth", using available values for the Hayabusa camera parameters, and following the proposed encounter scenario. The nominal values of these quantities were given realistic errors. The images were analyzed with landmark navigation and target characterization software to determine how well ground truth could be reproduced. Calculated spacecraft locations during approach to the surface agreed with the true values to less than a meter. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gaskell, RW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 301-150, Pasadena, CA 91109 USA. NR 8 TC 0 Z9 1 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 629 EP 644 PN 1-3 PG 16 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804700035 ER PT S AU Russell, RP AF Russell, Ryan P. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Global search for planar and three-dimensional periodic orbits near Europa SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc ID RESTRICTED 3-BODY PROBLEM; STABILITY; FAMILIES; POINTS AB A global grid search is performed to find axi- and doubly-symmetric periodic orbits in the Restricted Three Body Problem using the dimensioned parameters associated with the Jupiter-Europa system. Derived local differential correctors are applied to regions of the initial condition phase space that appear to be near solutions. The volume inside a three-dimensional initial condition mesh with billions of nodes is evaluated, and over 600,000 periodic solutions are found. Families of direct and retrograde solutions, both new and previously published, are identified and discussed. Stability is analyzed for each solution and general regions of stability are noted. Of the most promising results is the observation and characterization of a large class of stable yet highly-inclined direct orbits. Finally, all of the solutions and associated properties are archived. The resulting database is a practical reference for preliminary design of missions to Europa. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Russell, RP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-140L, Pasadena, CA 91109 USA. NR 24 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 647 EP 672 PN 1-3 PG 26 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804700036 ER PT S AU Sweetser, TH AF Sweetser, Theodore H. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Epicycles and oscillations: The dynamics of the LISA orbits SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB This paper presents a modem treatment of epicycle theory, which is an exact series representation of Keplerian motion, and uses that theory to develop the first analytic method for analyzing the higher order dynamics of the LISA orbits. LISA, the Laser Interferometer Space Antenna mission, uses a constellation of three spacecraft in heliocentric space and takes advantage of particular solutions of the Clohessy-Wiltshire equations, a first-order approximation of gravitational dynamics, to keep the constellation an equilateral triangle. The higher-order analysis presented here suggests a modification of the basic LISA orbit architecture which may improve the stability of the constellation. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Sweetser, TH (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. NR 11 TC 1 Z9 1 U1 0 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 693 EP 711 PN 1-3 PG 19 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804700038 ER PT S AU Roth, D Antreasian, P Bordi, J Criddle, K Ionasescu, R Jacobson, R Jones, J Meek, MC Roundhill, I Stauch, J AF Roth, Duane Antreasian, Peter Bordi, John Criddle, Kevin Ionasescu, Rodica Jacobson, Robert Jones, Jeremy Meek, M. Cameron Roundhill, Ian Stauch, Jason BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Cassini orbit reconstruction from Jupiter to Saturn SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB After nearly seven years of interplanetary cruise and four planetary gravity assists, the Cassini spacecraft was successfully captured into orbit around Saturn on I July 2004. For the first time during the Cassini mission, optical navigation images were obtained and integrated with radio-metric data. Navigators contended with optical navigation images that were potentially biased by Titan's dense atmosphere and Iapetus' albedo variations. Radio-metric data quality was degraded because of small Sun-Earth-probe angles near orbit insertion. The Jupiter to Saturn leg of the spacecraft's trajectory has been reconstructed and is used to provide a metric on navigation performance and maneuver execution errors. in particular, the reconstructed trajectory is compared to trajectory predictions at closest approach to Phoebe, the largest of Saturn's known irregular moons, and at ascending and descending Saturn ring plane crossings. Seven trajectory correction maneuvers, including the Saturn Orbit Insertion bum, are also evaluated and compared to design values. C1 CALTECH, Jet Prop Lab, Guidance Navigat & Control Sect, Pasadena, CA 91109 USA. RP Roth, D (reprint author), CALTECH, Jet Prop Lab, Guidance Navigat & Control Sect, Pasadena, CA 91109 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 913 EP 931 PN 1-3 PG 19 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804701001 ER PT S AU Ely, TA Lieb, E AF Ely, Todd A. Lieb, Erica BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Constellations of elliptical inclined lunar orbits providing polar and global coverage SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB Prior results have developed a methodology for selecting a long-lived constellation of 3 satellites that provide persistent, stable coverage to either the North or South Pole with no requirement for stationkeeping under the influence of only gravitational perturbations. In the present study, the sensitivity of this coverage in the presence of non-gravitational forces is determined, and a design strategy is formulated that minimizes any potential sensitivity to these accelerations. The class of orbits and methods are extended to the search for global coverage constellations of 6 satellites. Two constellations are designed that provide 99.999% global coverage for a 10 year period also without the need for any deterministic orbit maintenance. C1 CALTECH, Jet Prop Lab, Guidance Navigat & Control Sect, Pasadena, CA 91109 USA. RP Ely, TA (reprint author), CALTECH, Jet Prop Lab, Guidance Navigat & Control Sect, 4800 Oak Grove Dr,MS 301-125L, Pasadena, CA 91109 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 1447 EP 1462 PN 1-3 PG 16 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804701030 ER PT S AU Fahnestock, EG Scheeres, DJ McClamroch, NH Werner, RA AF Fahnestock, Eugene G. Scheeres, Daniel J. McClamroch, N. Harris Werner, Robert A. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Simulation and analysis of binary asteroid dynamics using mutual potential and potential derivatives formulation SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB We investigate the coupled orbital and rotational dynamics of two arbitrarily shaped bodies, modeled as uniform density polyhedra, under the influence of their mutual gravitational potential. A method of calculating the mutual potential's derivatives with respect to relative position and attitude is derived. Equations of motion for the binary system are presented and a dynamic simulation software package is described. Results obtained with the package are presented for three cases to validate the package. This simulation capability is also useful for enabling spacecraft missions to binary asteroids. C1 Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fahnestock, EG (reprint author), Univ Michigan, Dept Aerosp Engn, 1320 Beal Ave, Ann Arbor, MI 48109 USA. NR 4 TC 0 Z9 0 U1 0 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 1641 EP 1666 PN 1-3 PG 26 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804701042 ER PT S AU McIntosh, RJ Newman, LK AF McIntosh, Richard J. Newman, Lauri Kraft BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI EOS Aura ascent planning - Establishing the Earth Science Afternoon Constellation SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB This paper describes the trajectory planning and operations efforts of the NASA Goddard Space Flight Center Flight Dynamics team to place the Earth Observing System (EOS) Aura spacecraft in its mission orbit to form the fundamental beginnings of the Earth Science Afternoon Constellation. Aura is required to fly in a particular location relative to the World Reference System-2 (WRS-2) path of EOS Aqua. Pre-mission analysis is discussed, including choice of launch window start and duration to meet constellation requirements, nominal ascent scenarios, and contingency plans. Actual as-flown orbit-raising maneuvers are also documented, including operational maneuver constraints, maneuver calibration results, conjunction assessments for collision avoidance, and backup bum options. C1 Syst Engn AI Solut Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Greenbelt, MD 20771 USA. RP McIntosh, RJ (reprint author), Syst Engn AI Solut Inc, Lanham, MD 20706 USA. NR 5 TC 0 Z9 0 U1 1 U2 2 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 1747 EP 1764 PN 1-3 PG 18 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804701048 ER PT S AU Rand, DK Newman, LK Work, KT AF Rand, David K. Newman, Lauri Kraft Work, Kevin T. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Inclination adjust maneuver planning and execution for the Earth Science Afternoon Constellation SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB Following a series of orbit-raising maneuvers, Earth Observing System (EOS) Aura joined it's sister spacecraft, EOS Aqua, in their desired mission orbits on August 9, 2004 to form the beginning of the Earth Science Afternoon Constellation. Member missions of this Constellation are independently funded and operated by their responsible organizations; however, each controls its orbit to remain within a pre-designated control box to ensure safety for the other members. While this control box philosophy works for in-plane orbit control, it does not account for plane change maneuvers. If one mission performs a plane change, the rest are forced to follow suit or break the Constellation. Prior to Aura launch, the Aqua Project had agreed with some Constellation members to perform a set of required inclination adjust maneuvers prior to April 2005. Since Aura was then on orbit, it had to perform matching maneuvers to remain in the Constellation. This paper details the planning that was performed to execute the combined inclination maneuvers, including leveraging Aqua lessons learned, examining various maneuver date options in concert with Aura ascent planning, contingency planning, and collaboration between the Flight Operations Teams to ensure that the maneuvers could be executed from the shared control center by shared personnel without issue. In addition, the actual maneuver results are documented along with lessons learned. Some discussion of performing inclination maneuvers in the future. with more than two Constellation members is also provided. C1 Syst Engn AI Solut Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Greenbelt, MD 20771 USA. Lockheed Martin Space Operat, Flight Dynam Engn, Greenbelt, MD 20770 USA. RP Rand, DK (reprint author), Syst Engn AI Solut Inc, Lanham, MD 20706 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 1765 EP 1782 PN 1-3 PG 18 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804701049 ER PT S AU Demarest, P Richon, KV Wright, F AF Demarest, Peter Richon, Karen V. Wright, Frank BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Analysis for monitoring the Earth Science Afternoon Constellation SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB The Earth Science Afternoon Constellation consists of Aqua, Aura, PARASOL, CALIPSO, CloudSat, and the Orbiting Carbon Observatory (OCO). The coordination of flight dynamics activities between these missions is critical to the safety and success of the Afternoon Constellation. This coordination is based on two main concepts, the control box and the zone-of-exclusion. This paper describes how these two concepts are implemented in the Constellation Coordination System (CCS). The CCS is a collection of tools that enables the collection and distribution of flight dynamics products among the missions, allows cross-mission analyses to be performed through a web-based interface, performs automated analyses to monitor the overall constellation, and notifies the missions of changes in the status of the other missions. C1 Miss Anal AI Solut Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Flight Dynam Anal Branch, Greenbelt, MD 20771 USA. RP Demarest, P (reprint author), Miss Anal AI Solut Inc, Lanham, MD 20706 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 1827 EP 1840 PN 1-3 PG 14 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804701053 ER PT S AU Richon, KV Case, W AF Richon, Karen V. Case, Warren BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI An overview of the Earth Science Afternoon Constellation contingency procedures SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB The Earth Science Afternoon Constellation comprises NASA missions Aqua, Aura, CloudSat and the Orbiting Carbon Observatory (OCO), the joint NASA/CNES mission CALIPSO and the CNES mission PARASOL. Both NASA and CNES offices are responsible for ensuring that contingency plans or other arrangements exist to cope with contingencies within their respective jurisdictions until the conclusion of all Afternoon Constellation operations. The Mission Operations Working Group, comprised of members from each of the missions, has developed the high-level procedures for maintaining the safety of this constellation. Each contingency situation requires detailed analyses before any decisions are made. This paper describes these procedures, and includes defining what constitutes a contingency situation, the pertinent parameters involved in the contingency analysis and guidelines for the actions required, based on the results of the contingency analyses. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Richon, KV (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 1841 EP 1858 PN 1-3 PG 18 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804701054 ER PT S AU Phong, C Sweetser, TH AF Phong, Connie Sweetser, Theodore H. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Minimum impulse transfers to rotate the line of apsides SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB In-plane rotations of apsides of orbits are occasionally necessary in the operation of space missions. A first level mission design rule of thumb states that a two-impulse transfer to rotate apsides requires about half as much Delta V as a single impulse transfer for the same rotation. Numerical comparisons with a trajectory optimization program show that the rule of thumb is excellent for near-circular orbits but quickly becomes increasingly conservative at higher eccentricities and degrees of rotation. To address these dependencies we develop an improved AV estimator based entirely on our empirical results. The improved rule of thumb compares well with another known approximate solution to the problem of optimal two-impulse transfers to rotate apsides that has been derived from first principles. Our analysis shows that the rule of thumb, although conservative, is ideal for first level mission design analysis because of its accessibility. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Phong, C (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 1901 EP 1910 PN 1-3 PG 10 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702003 ER PT S AU Desai, PN Conway, BA AF Desai, Prasun N. Conway, Bruce A. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Six-degree-of-freedom trajectory optimization utilizing a two-timescale collocation architecture SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc ID HL-20 AB Six-degree-of-freedom (6DOF) trajectory optimization of a reentry vehicle is solved using a two-timescale collocation methodology. This class of 6DOF trajectory problems are characterized by two distinct timescales in their governing equations, where a subset of the states have high-frequency dynamics (the rotational equations of motion) while the remaining states (the translational equations of motion) vary comparatively slowly. With conventional collocation methods, the 6DOF problem size becomes extraordinarily large and difficult to solve. Utilizing the two-timescale collocation architecture, the problem size is reduced significantly. The converged solution shows a realistic landing profile and captures the appropriate high-frequency rotational dynamics. A large reduction in the overall problem size (by 55%) is attained with the two-timescale architecture as compared to the conventional single-timescale collocation method. Consequently, optimum 6DOF trajectory problems can now be solved efficiently using collocation, which was not previously possible for a system with two distinct timescales in the governing states. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Desai, PN (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 12 TC 0 Z9 0 U1 0 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 1949 EP 1963 PN 1-3 PG 15 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702006 ER PT S AU Aiello, J AF Aiello, John BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Numerical investigation of mapping orbits about Jupiter's icy moons SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc ID EUROPA; SATELLITES AB A proposed mission that would orbit Callisto, Ganymede, and Europa will require low altitude, high inclination orbits for gravity and surface mapping. The inherent instability of these orbits poses a particular challenge to gravity field mapping which requires tracking of a spacecraft unperturbed by orbit maintenance maneuvers. Analytical investigations identify conditions that allow for an uncontrolled orbit over the time scales necessary for gravity mapping, yet these are typically obtained via a Hill model with various approximations to the force models. This paper explores the dynamics of these orbits by direct propagation against an ephemeris model. Initial conditions within the context of a mapping mission's likely requirements are considered. The results complement the analytical studies and reveal additional dependencies. C1 CALTECH, Jet Prop Lab, Outer Planets Miss Anal Grp, Guidance Navigat & Control Sect, Pasadena, CA 91109 USA. RP Aiello, J (reprint author), CALTECH, Jet Prop Lab, Outer Planets Miss Anal Grp, Guidance Navigat & Control Sect, 4800 Oak Grove Dr,Mail Stop 301-150, Pasadena, CA 91109 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 1965 EP 1980 PN 1-3 PG 16 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702007 ER PT S AU Hirani, AN Lo, MW AF Hirani, Anil N. Lo, Martin W. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Surface structure of an invariant manifold of a halo orbit SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB We extract the surface structure of the unstable invariant manifold tube projected into position space, of a halo orbit near L-2 in the circular restricted three body model. We do this by using transversal planes to intersect trajectories that approximate the tube. From these intersection points we construct spline-interpolated cross section curves which give a good idea of the structure of the tube. For example, we show that, for the value of mu we use, the tube pinches, develops a self-intersection, develops loop-inside-tube structure, pinches some more, and so on. We also construct surfaces made of quadrilaterals and triangles from these cross-sections. The transversal planes are obtained by taking planes orthogonal to a curve that follows the general shape of the tube. One such curve we use, is the unstable invariant manifold of the equilibrium point L-2 itself. In another example, we take a circle that follows the tube, as the curve for finding planes transversal to the tube. We also show that tubes of different energies, that start out in certain ordering, do not obey the ordering after a while. Our method is complementary to the method of taking cross-sections of constant time (the isochronous method), as used by some other researchers. The isochronous method is good at revealing the temporal structure of trajectories on a tube. However, due to the unequal speeds of different trajectories, it is harder to use for long length surface extraction. In contrast, using our method, we show cross-sections of the tube through an angular extent of nearly pi during which the tube becomes extremely convoluted. Our work is motivated by applications to space mission design. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hirani, AN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2003 EP 2025 PN 1-3 PG 23 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702009 ER PT S AU Ling, L Tuckness, D Salama, A McRonald, A AF Ling, Lisa Tuckness, Dan Salama, Ahmed McRonald, Angus BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Vehicle breakup analysis for applications in aerospace nuclear safeety SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB For decades, vehicle breakup analysis had been performed for space missions using nuclear heater or power units to assess aerospace nuclear safety in the event of a launch failure leading to inadvertent atmospheric reentry. Such pre-launch risk analysis is imperative to assess environmental impact, obtain launch approval, and for launch contingency planning. Work devoted to this area had been ongoing since 1959 and has been well-documented. This document discusses the background, objectives, and process of performing vehicle breakup analysis for applications in aerospace nuclear safety, specifically those conducted at the Jet Propulsion Laboratory (JPL) for launch approval. An example of prelaunch vehicle breakup analysis performed for the Mars Exploration Rover (MER) mission is also given. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ling, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 21 TC 0 Z9 0 U1 0 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2117 EP 2137 PN 1-3 PG 21 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702015 ER PT S AU Salama, A Ling, L AF Salama, Ahmed Ling, Lisa BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI A methodology of MSL breakup analysis for Earth accidental reentry and its application to breakup analysis for Mars off-nominal entry SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB Vehicle breakup analysis has been performed for missions that may carry nuclear fuel for heating or power purposes to assess nuclear safety in case of launch failure leading to atmospheric reentry. Also, failure scenarios exist which could lead to breakup during Entry/Descent/Landing (EDL) at Mars due to off-nominal entries, with implications for planetary protection requirements. Since the Mars Science Laboratory (MSL) spacecraft may include a Multi-Misssion Radioisotope Thermoelectric Generator (MMRTG), an analysis of breakup in case of launch failure is required. Also, breakup during Mars EDL due to off-nominal entries could release the RTG heat source that has implications for planetary protection requirements. This paper presents a methodology of MSL breakup analysis for launch failure with application to Mars off-nominal entry. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Salama, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2139 EP 2154 PN 1-3 PG 16 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702016 ER PT S AU Salama, A Ling, L McRonald, A AF Salama, Ahmed Ling, Lisa McRonald, Angus BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI A Genesis breakup and burnup analysis in off-nominal Earth return and atmospheric entry SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB The Genesis capsule returned to Earth on September 8, 2004, carrying samples of solar wind charged particles. The Genesis project conducted a detailed breakup/burnup analysis before the Earth return to determine if any spacecraft component could survive and reach the ground intact in case of an off-nominal entry. In addition, an independent JPL team was chartered with the responsibility of analyzing several definitive breakup scenarios to verify the official project analysis. This paper presents the analysis and results of this independent team. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Salama, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2155 EP 2169 PN 1-3 PG 15 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702017 ER PT S AU Ling, L Tuckness, D AF Ling, Lisa Tuckness, Dan BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Development of hypersonic aerodynamic coefficients for arbitrary-shaped body obtained from Newtonian theory using triangular panels SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB Vehicle breakup analysis is performed for the assessment of aerospace nuclear safety required for launch approval and contingency planning for space missions using nuclear heater or power units. Vehicle breakup typically occurs during the hypersonic regime of the reentry. Therefore, hypersonic aerodynamic coefficients of various vehicle configurations are needed for trajectory propagation and breakup analysis. This paper presents the derivation of the equations used to develop a panel code employing triangular panels for the calculation of hypersonic aerodynamic coefficients of an arbitrary-shaped body based on Newtonian theory for hypersonic flow. Validation of the panel code against two test cases is presented, and an example of application is also given. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ling, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2171 EP 2184 PN 1-3 PG 14 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702018 ER PT S AU Ling, L Tuckness, D AF Ling, Lisa Tuckness, Dan BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Development of non-arbitrary atmospheric entry points for impact footprint determination in an inadvertent Earth reentry during launch contingency SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB In space missions using nuclear heater or power units, vehicle breakup analysis performed for risk assessment required for launch approval provides predictions of vehicle breakup and impact point of the nuclear power system for various launch contingency scenarios. During launch, a failure occurring while in the parking orbit could lead to an out-of-orbit reentry. In order to predict the resulting impact point of the nuclear power system, a non-arbitrary entry point is needed for trajectory propagation and breakup analysis. The derivation of the modeling of inertial-fixed thrust and the calculation of non-arbitrary entry condition in an out-of-orbit reentry is presented in this paper. Validation of the entry condition is also presented. To demonstrate the application of the non-arbitrary entry condition, an example of an inadvertent reentry with vehicle breakup analysis and the resulting prediction of impact point are given. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ling, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 3 TC 0 Z9 0 U1 1 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2185 EP 2200 PN 1-3 PG 16 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702019 ER PT S AU Ling, L Tuckness, D AF Ling, Lisa Tuckness, Dan BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Modeling of local winds and real-time application in impact point prediction for inadvertent Earth reentry during launch contingency SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB In the event of a launch failure leading to inadvertent Earth reentry in a space mission using nuclear heater or power units, impact point prediction is required of the nuclear power system as specified in the launch contingency plan. To enhance the accuracy of the footprint prediction, the effects of real-time local winds obtained from the website of the National Oceanic and Atmospheric Administration are included in the trajectory propagation. This paper presents the derivation of the modeling of local winds and an example of its application to the prelaunch vehicle breakup analysis performed for the Mars Exploration Rover mission. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ling, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2201 EP 2209 PN 1-3 PG 9 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702020 ER PT S AU Bonfiglio, EP Oh, D Yen, CW AF Bonfiglio, Eugene P. Oh, David Yen, Chen-Wan BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Analysis of chemical, REP, and SEP missions to the Trojan asteroids SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB Recent studies suggest significant benefits from using 1(st) and 2(nd) generation Radioisotope Power Systems (RPS) as a power source for electric propulsion (EP) missions to the outer planets. This study focuses on trajectories to the Trojan asteroids. A high level analysis is performed with chemical trajectories to determine potential candidates for REP trajectory optimization. Extensive analysis of direct trajectories using REP is performed on these candidates. Solar Electric Propulsion (SEP) trajectories are also considered for comparison against REP trajectories. A spacecraft mass is derived for the different types of missions, providing insight to how the REP (both 1(st) and 2(nd) generation) missions compare with chemical and SEP missions. C1 CALTECH, Jet Prop Lab, Guidance Navigat & Control Sect, Pasadena, CA 91109 USA. RP Bonfiglio, EP (reprint author), CALTECH, Jet Prop Lab, Guidance Navigat & Control Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2301 EP 2320 PN 1-3 PG 20 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702026 ER PT S AU Parcher, DW Sims, JA AF Parcher, Daniel W. Sims, Jon A. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Earth gravity-assist trajectories to Jupiter using nuclear electric propulsion SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc ID MISSIONS AB This paper examines optimal low-thrust gravity-assist trajectories to Jupiter using nuclear electric propulsion. The scope of the discussion will be limited to single and double Earth gravity assists. For both of these cases, multiple locally optimal trajectory families, differentiated by transfer resonance between flybys and by flyby type, are considered. Trajectories that minimize initial injection energy by using low resonance transfers or several heliocentric revolutions to the first flyby offer the most delivered mass given sufficient flight time. C1 CALTECH, Jet Prop Lab, Guidance Navigat & Control Sect, Pasadena, CA 91109 USA. RP Parcher, DW (reprint author), CALTECH, Jet Prop Lab, Guidance Navigat & Control Sect, Mail Stop 230-205,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 6 TC 0 Z9 0 U1 0 U2 2 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2321 EP 2332 PN 1-3 PG 12 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702027 ER PT S AU Parcher, DW Sims, JA AF Parcher, Daniel W. Sims, Jon A. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Gravity-assist trajectories to Jupiter using nuclear electric propulsion SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc ID MISSIONS AB This paper examines optimal low-thrust gravity-assist trajectories to Jupiter using nuclear electric propulsion. Three different Venus-Earth Gravity Assist (VEGA) types are presented and compared to other gravity-assist trajectories using combinations of Earth, Venus, and Mars. Families of solutions for a given gravity-assist combination are differentiated by the approximate transfer resonance or number of heliocentric revolutions between flybys and by the flyby types. Trajectories that minimize initial injection energy by using low resonance transfers or additional heliocentric revolutions on the first leg of the trajectory offer the most delivered mass given sufficient flight time. Trajectory families that use only Earth gravity assists offer the most delivered mass at most flight times examined, and are available frequently with little variation in performance. However, at least one of the VEGA trajectory types is among the top performers at all of the flight times considered. C1 CALTECH, Jet Prop Lab, Guidance Navigat & Control Sect, Pasadena, CA 91109 USA. RP Parcher, DW (reprint author), CALTECH, Jet Prop Lab, Guidance Navigat & Control Sect, Mail Stop 230-205,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 TC 0 Z9 0 U1 0 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2333 EP 2350 PN 1-3 PG 18 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702028 ER PT S AU Beckman, M Folta, D AF Beckman, Mark Folta, Dave BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI Mission design of the first robotic lunar exploration program mission: The lunar reconnaissance orbiter SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB The Lunar Reconnaissance Orbiter (LRO) is the first of the Robotic Lunar Exploration Program's (RLEP) missions to the moon. LRO is a one-year mission to be flown in a low (50 km) polar lunar orbit. It will be launched on a Delta II class launch vehicle in late 2008 onto a short coast minimum energy transfer, with the proper lighting conditions, and with a launch window of about six days per month. During the nominal mission, orbit determination is required to be accurate to 500 m in total position and 18 m radially, but is expected to be a factor of two to three better. The two-month commissioning orbit, and possibly the extended mission, will be in a lunar frozen orbit at 30 x 216 km altitude, which minimizes stationkeeping fuel costs. C1 Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Beckman, M (reprint author), Goddard Space Flight Ctr, Code 595, Greenbelt, MD 20771 USA. NR 5 TC 1 Z9 1 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2497 EP 2511 PN 1-3 PG 15 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702037 ER PT S AU Fink, DR AF Fink, Dale R. BE Williams, BG DAmario, LA Howell, KC Hoots, FR TI WMAP solar radiation pressure modeling during February 2005 reaction wheel power off anomaly SO Astrodynamics 2005, Vol 123, Pts 1-3 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT AIAA/AAS Astrodynamics Specialist Conference CY AUG 07-11, 2005 CL Lake Tahoe, CA SP Amer Inst Aeronaut & Astronaut, Amer Astronaut Soc AB The Wilkinson Microwave Anisotropy Probe (WMAP) satellite in orbit about L2 experienced an anomaly on February 17, 2005 when a reaction wheel powered off. During the anomaly, the trajectory changed as solar radiation pressure acted on the spacecraft in its safemode attitude. To keep the predicted ephemeris as accurate as possible, the trajectory was modeled by propagating the state before the anomaly with appropriate solar radiation coefficients for each phase of the anomaly. This paper describes the modeling that was done in real time to respond to the anomaly, and its effect as a solar sail maneuver. C1 Comp Sci Corp, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Fink, DR (reprint author), Comp Sci Corp, Goddard Space Flight Ctr, Bldg 3,Room S003,Mail Code 582-0, Greenbelt, MD 20771 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-8770-3527-X J9 ADV ASTRONAUT SCI PY 2006 VL 123 BP 2729 EP 2735 PN 1-3 PG 7 WC Engineering, Aerospace SC Engineering GA BEL45 UT WOS:000237804702050 ER PT J AU Peterson, KC Gallagher, SC Hornschemeier, AE Muno, MP Bullard, EC AF Peterson, KC Gallagher, SC Hornschemeier, AE Muno, MP Bullard, EC TI Seyfert galaxies and the hard X-ray background: Artificial Chandra observations of z=0.3 active galaxies SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : Seyfert; X-rays : diffuse background; X-rays : galaxies ID CCD IMAGING SPECTROMETER; FIELD NORTH SURVEY; STAR-FORMING DISK; ROSAT DEEP SURVEY; XMM-NEWTON; GALACTIC NUCLEUS; OPTICAL-IDENTIFICATION; SOURCE POPULATION; STARBURST GALAXY; SKY SURVEY AB Deep X-ray surveys have resolved much of the X-ray background radiation below 2 keV into discrete sources, but the background above 8 keVremains largely unresolved. The obscured ( type 2) active galactic nuclei (AGNs) that are expected to dominate the hard X-ray background have not yet been detected in sufficient numbers to account for the observed background flux. However, deep X-ray surveys have revealed large numbers of faint quiescent and star-burst galaxies at moderate redshifts. In hopes of recovering the missing AGN population, it has been suggested that the defining optical spectral features of low-luminosity Seyfert nuclei at large distances may be overwhelmed by their host galaxies, causing them to appear optically quiescent in deep surveys. We test this possibility by artificially red-shifting a sample of 23 nearby, well-studied active galaxies to z = 0.3, testing them for X-ray AGN signatures, and comparing them to the objects detected in deep X-ray surveys. We find that these redshifted galaxies have properties consistent with the deep-field normal and optically bright, X-ray-faint galaxy (OBXF) populations, supporting the hypothesis that the numbers of AGNs in deep X-ray surveys are being underestimated and suggesting that OBXFs should not be ruled out as candidate AGN hosts that could contribute to the hard X-ray background source population. C1 Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Peterson, KC (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Mail Code 154705,475 Portola Plaza, Los Angeles, CA 90095 USA. EM kptrson@astro.ucla.edu; sgall@astro.ucla.edu; annh@milkyway.gsfc.nasa.gov; mmuno@astro.ucla.edu; ebullard@mit.edu NR 69 TC 14 Z9 14 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2006 VL 131 IS 1 BP 133 EP 142 DI 10.1086/498342 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001TU UT WOS:000234561300011 ER PT J AU de Mello, DF Wadadekar, Y Dahlen, T Casertano, S Gardner, JP AF de Mello, DF Wadadekar, Y Dahlen, T Casertano, S Gardner, JP TI Star-forming galaxies at intermediate redshifts: Morphology, ages, and sizes SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : formation; galaxies : starburst ID HUBBLE DEEP FIELD; STELLAR POPULATIONS; EVOLUTION; SOUTH; CLASSIFICATION; STARBURST99; ULTRAVIOLET; SPECTRA; NORTH AB We present an analysis of the deepest near-UV image obtained with the Hubble Space Telescope using the WFPC2 (F300W) as part of the parallel observations of the Hubble Ultra Deep Field campaign. The U-band 10 sigma limiting magnitude measured over 0.2 arcsec(2) is m(AB) = 27.5, which is 0.5 mag deeper than that in the Hubble Deep Field North. We matched the U-band catalogs with those from the ACS (BViz) taken during the Great Observatories Origins Deep Survey observations of the Chandra Deep Field-South and obtained photometric redshifts for 306 matched objects. We find that the UV-selected galaxies span all the major morphological types at 0.2 < z(phot) < 1.2. However, disks are more common at lower redshifts, 0.2 < zphot < 0.8. Higher redshift objects ( 0.7 < zphot < 1.2) are on average bluer than lower z and have spectral types typical of starbursts. They have compact, peculiar, or low surface brightness morphologies. Despite the selection by UV, 13 objects have spectral types of early-type galaxies; two of them are spheroids with blue cores. The evolutionary synthesis code Starburst 99 was used to age-date the UV-selected galaxies, which were found to have rest-frame colors typical of stellar populations with mean ages > 100 Myr. The average half-light radius ( rest-frame 1200 - 1800 angstrom) of the UV-selected galaxies at 0.66 < zphot < 1.5 is 0''.26 +/- 0''.01 ( 2.07 +/- 0.08 kpc). The UV-selected galaxies are on average fainter ( M-B = 18.43 +/- 0.13) than Lyman break galaxies (LBGs; M-B = - 23 +/- 1). Our sample includes early-type galaxies that are presumably massive and forming stars only in their cores, as well as starburst-type systems that are more similar to the LBGs, although much less luminous. This implies that even the starbursts in our sample are either much less massive than LBGs or forming stars at a much lower rate, or both. The low surface brightness galaxies have no overlap with the LBGs and form an interesting new class of their own. C1 NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Greenbelt, MD 20771 USA. Catholic Univ Amer, Washington, DC 20064 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. RP de Mello, DF (reprint author), NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. NR 30 TC 21 Z9 21 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2006 VL 131 IS 1 BP 216 EP 225 DI 10.1086/498681 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001TU UT WOS:000234561300017 ER PT J AU Covey, KR Greene, TP Doppmann, GW Lada, CJ AF Covey, KR Greene, TP Doppmann, GW Lada, CJ TI The radial velocity distribution of class I and flat-spectrum protostars SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared : stars; stars : formation; stars : kinematics; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID T-TAURI STARS; MOLECULAR CLOUDS; BROWN DWARFS; MILKY-WAY; AURIGA; MULTIPLICITY; SPECTROSCOPY; ACCRETION; CLUSTERS; SYSTEMS AB We analyze radial velocities for a sample of 31 Class I and flat-spectrum protostars in Taurus-Auriga, rho Ophiuchi, and Serpens for evidence of the global dynamical state of extremely young stellar populations buried within parental molecular clouds. Comparing the radial velocity of each protostar to that of the local CO gas, we are able to constrain the one-dimensional radial velocity dispersion of Class I and flat-spectrum objects to similar to 2.5 km s(-1) or below. This upper limit to the protostellar velocity dispersion is consistent with the velocity dispersions of surrounding CO gas, which we measure to be similar to 1.4 km s(-1), suggesting that the motions of protostars and local CO gas are dynamically linked and are dominated by the gravitational potential of the molecular cloud. However, the upper limit on the protostellar velocity dispersion could still allow for slightly inflated motions of protostars relative to the local molecular gas. Four of the protostars analyzed appear to have velocities more than 3 sigma (7.5 km s(-1)) away from the central local CO gas velocity while showing spectroscopic indicators of youth and accretion such as H-2 emission, H I Br gamma emission, or K-band continuum veiling. These radial velocity outliers may represent protostellar spectroscopic binaries or ejected cluster members. C1 Univ Washington, Dept Astron, Seattle, WA 98195 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Covey, KR (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. OI Covey, Kevin/0000-0001-6914-7797 NR 38 TC 27 Z9 27 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2006 VL 131 IS 1 BP 512 EP 519 DI 10.1086/498064 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 001TU UT WOS:000234561300037 ER PT J AU Villar-Martin, M Sanchez, SF Peletier, R Vernet, J De Breuck, C Humphrey, A Alighieri, SD Fosbury, R Stern, D AF Villar-Martin, M Sanchez, SF Peletier, R Vernet, J De Breuck, C Humphrey, A Alighieri, SD Fosbury, R Stern, D TI The giant Ly alpha nebula associated with a z=2.5 radio galaxy SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT Granada Workshop on High Redshift Radio Galaxies CY APR 18-20, 2005 CL Inst Astrofis Andaluc, Granada, SPAIN HO Inst Astrofis Andaluc DE galaxies : active; galaxies : individual : MRC 2104-242; galaxies : evolution AB We present a kinematic and morphological study of the giant Ly alpha nebula associated with the radio galaxy MRC 2104-242 (z = 2.49) based on integral field spectroscopic VIMOS data from VLT. The galaxy appears to be embedded in a giant (greater than or similar to 120 kpc) gas reservoir that surrounds it completely. The kinematic properties of the nebula suggest that it is a rotating structure, which would imply a lower limit to the dynamical mass of similar to 3 x 10(11) M circle dot. An alternate scenario is that the gas is infalling. Such a process would be able to initiate and sustain significant central starburst activity, although it is likely to contribute with less than 10% of the total stellar mass of the galaxy. C1 CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Ctr Astron Hispano Aleman Calar Alto, Almeria 04004, Spain. Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. European So Observ, D-85748 Garching, Germany. Univ Hertfordshire, Dept Phys Sci, Hatfield AL10 9AB, Herts, England. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. ST ECF, D-85748 Garching, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Villar-Martin, M (reprint author), CSIC, Inst Astrofis Andalucia, Aptdo 3004, E-18080 Granada, Spain. EM montse@iaa.es RI Peletier, Reynier/B-9633-2012; di Serego Alighieri, Sperello/E-4067-2010; Humphrey, Andrew/M-4118-2013; Villar Martin, Montserrat/C-3126-2017; OI di Serego Alighieri, Sperello/0000-0001-8769-2692; Humphrey, Andrew/0000-0002-0510-2351; Villar Martin, Montserrat/0000-0003-2566-2126; Fosbury, Robert/0000-0001-9975-8003; Vernet, Joel/0000-0002-8639-8560 NR 19 TC 1 Z9 1 U1 0 U2 3 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. PY 2006 VL 327 IS 2-3 BP 187 EP 190 DI 10.1002/asna.200510504 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 025FS UT WOS:000236251300015 ER PT J AU Didkovsky, LV Judge, DL Jones, AR Rhodes, EJ Gurman, JB AF Didkovsky, LV Judge, DL Jones, AR Rhodes, EJ Gurman, JB TI Measuring proton energies and fluxes using EIT (SOHO) CCD areas outside the solar disk images SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE solar energetic particles; solar flare events; proton flux; proton spectra; space weather AB An indirect proton flux measuring tool based on discrimination of the energy deposited by protons in 128 x 128 pixel EIT CCD areas outside the solar disk images is presented. Single pixel intensity events are converted into proton incident energy flux using modeled energy deposition curves for angles of incidence +/- 60 degrees in four EIT spatial areas with different proton stopping power. The extracted proton flux is corrected for both the loss of one-pixel events in the range of angles of incidence as well as for the contribution to the single pixel events resulting from scattered middle-energy protons (low-energy or high-energy particles are stopped by the EIT components or pass through them, accordingly). A simple geometrical approach was found and applied to correct for a non-unique relation between the proton-associated CCD output signal and the incident proton energy. With this geometrical approximation four unique proton incident energy ranges were determined as 45-49, 145-154, 297-335, and 390-440 MeV The indirect proton flux measuring tool has been tested by comparing Solar Energetic Particles (SEP) flux temporal profiles extracted from the EIT CCD frames and downloaded from the GOES database for the Bastille Day (BD) of 2000 July 14 and the more recent 2005 January 20 events. The SEP flux temporal profiles and proton spectra extracted from the EIT in the relatively narrow energy ranges between 45 and 440 MeV reported here are consistent with the related GOES profiles. The four additional EIT extracted ranges provide higher energy resolution of the SEP data. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Univ So Calif, SHS, Los Angeles, CA 90089 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Didkovsky, LV (reprint author), Univ So Calif, SHS, 835 W 37th St, Los Angeles, CA 90089 USA. EM leonid@usc.edu NR 10 TC 4 Z9 4 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 4 BP 314 EP 320 DI 10.1002/asna.200510529 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 047GJ UT WOS:000237867500005 ER PT J AU Allan, A Hessman, F Bischoff, K Burgdorf, M Cavanagh, B Christian, D Clay, N Dickens, R Economou, F Fadavi, M Fraser, S Granzer, T Grosvenor, S Jenness, T Koratkar, A Lehner, M Mottram, C Naylor, T Saunders, E Solomos, N Steele, I Tuparev, G Vestrand, T White, R Yost, S AF Allan, A. Hessman, F. Bischoff, K. Burgdorf, M. Cavanagh, B. Christian, D. Clay, N. Dickens, R. Economou, F. Fadavi, M. Fraser, S. Granzer, T. Grosvenor, S. Jenness, T. Koratkar, A. Lehner, M. Mottram, C. Naylor, T. Saunders, E. Solomos, N. Steele, I. Tuparev, G. Vestrand, T. White, R. Yost, S. TI A protocol standard for heterogeneous telescope networks SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 1st Workshop on Heterogeneous Telescope Networks CY JUL 18-21, 2005 CL Exeter, ENGLAND DE instrumentation : miscellaneous; techniques : miscellaneous; methods : observational; telescopes; standards AB The scientific need for a standard protocol permitting the exchange of generic observing services is rapidly escalating as more observatories adopt service observing as a standard operating mode and as more remote or robotic telescopes are brought on-line. To respond to this need, we present the results of the first interoperability workshop for Heterogeneous Telescope Networks (HTN) held in Exeter. We present a draft protocol, designed to be independent of the specific instrumentation and software that controls the remote and/or robotic telescopes, allowing these telescopes to appear to the user with a unified interface despite any underlying architectural differences. (c) 2006 WILEY-VCH Verlag GmbH &Co. KGaA, Weinheim. C1 Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. Teleskoptech Halfmann, D-86356 Neusass Vogelsang, Germany. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Joint Astron Ctr, Hilo, HI 96720 USA. Queens Univ Belfast, Dept Phys & Astron, Belfast BT7 1NN, Antrim, North Ireland. Latterfrosken Software Dev Ltd, Walsall WS1 3QA, W Midlands, England. Jackson State Univ, Jackson, MS 39217 USA. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Catonsville, MD 21228 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Hellen Naval Acad, Phys Sector, Piraeus 18503, Greece. Natl Astron Ctr, Ainos Mt, Kefallinia Isla, Greece. Tuparev Technol Inc, Sofia 1612, Bulgaria. Los Alamos Natl Lab, Los Alamos, NM 87544 USA. Univ Michigan, Randall Lab, ROTSE, Ann Arbor, MI 48109 USA. RP Allan, A (reprint author), Univ Exeter, Sch Phys, Stocker Rd, Exeter EX4 4QL, Devon, England. EM aa@astro.ex.ac.uk RI Naylor, Tim /A-9465-2015; OI Economou, Frossie/0000-0002-8333-7615; Jenness, Tim/0000-0001-5982-167X NR 2 TC 12 Z9 12 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. PY 2006 VL 327 IS 8 BP 744 EP 750 DI 10.1002/asna.200610625 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089SI UT WOS:000240900600002 ER PT J AU White, RR Allan, A Barthelmy, S Bloom, J Graham, M Hessman, FV Marka, S Rots, A Scholberg, K Seaman, R Stoughton, C Vestrand, WT Williams, R Wozniak, PR AF White, R. R. Allan, A. Barthelmy, S. Bloom, J. Graham, M. Hessman, F. V. Marka, S. Rots, A. Scholberg, K. Seaman, R. Stoughton, C. Vestrand, W. T. Williams, R. Wozniak, P. R. TI Astronomical network event and observation notification SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 1st Workshop on Heterogeneous Telescope Networks CY JUL 18-21, 2005 CL Exeter, ENGLAND DE instrumentation : miscellaneous; methods : observational; standards; telescopes ID TELESCOPES; SKY AB Networks are becoming a key element in most current and all future, telescope and observatory projects. The ability to easily and efficiently pass observation data, alert data and instrumentation requests between distributed systems could enable science as never before. However, any effective large scale or meta-network of astronomical resources will require a common communication format or development resources will have to be continuously dedicated to creating interpreters. The necessary elements of any astronomy communication can be easily identified, efficiently described and rigidly formatted so that both robotic and human operations can use the same data. In this paper we will explore the current state of notification, what notification requirements are essential to create a successful standard and present a standard now under development by the International Virtual Observatory Alliance (IVOA), called the VOEvent. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Univ Exeter, Exeter, Devon, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. CALTECH, Pasadena, CA 91125 USA. Univ Gottingen, D-3400 Gottingen, Germany. Columbia Univ, New York, NY 10027 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. Duke Univ, Durham, NC 27706 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Fermilab Natl Accelerator Lab, Chicago, IL USA. RP White, RR (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA. EM rwhite@lanl.gov RI Barthelmy, Scott/D-2943-2012; OI Rots, Arnold/0000-0003-2377-2356; Wozniak, Przemyslaw/0000-0002-9919-3310 NR 7 TC 8 Z9 8 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. PY 2006 VL 327 IS 8 BP 775 EP 778 DI 10.1002/asna.200610631 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089SI UT WOS:000240900600008 ER PT J AU Yost, SA Aharonian, F Akerlof, CW Ashley, MCB Barthelmy, S Gehrels, N Gogus, E Guver, T Horns, D Kiziloglu, U Krimm, HA McKay, TA Ozel, M Phillips, A Quimby, RM Rowell, G Rujopakarn, W Rykoff, ES Schaefer, BE Smith, DA Swan, HF Vestrand, WT Wheeler, JC Wren, J Yuan, F AF Yost, S. A. Aharonian, F. Akerlof, C. W. Ashley, M. C. B. Barthelmy, S. Gehrels, N. Gogus, E. Guver, T. Horns, D. Kiziloglu, U. Krimm, H. A. McKay, T. A. Ozel, M. Phillips, A. Quimby, R. M. Rowell, G. Rujopakarn, W. Rykoff, E. S. Schaefer, B. E. Smith, D. A. Swan, H. F. Vestrand, W. T. Wheeler, J. C. Wren, J. Yuan, F. TI Status of the ROTSE-III telescope network SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 1st Workshop on Heterogeneous Telescope Networks CY JUL 18-21, 2005 CL Exeter, ENGLAND DE gamma rays : bursts; instrumentation : photometric; instrumentation : photometry; telescopes AB ROTSE-III is a homogeneous worldwide array of 4 robotic telescopes. They were designed to provide optical observations of gamma-ray burst (GRB) afterglows as close as possible to the start of gamma-ray emission. ROTSE-III is fulfilling its potential for GRB science, and provides optical observations for a variety of astrophysical sources in the interim between GRB events. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Univ Michigan, Randall Lab 2477, Ann Arbor, MI 48104 USA. Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sabanci Univ, TR-34956 Istanbul, Turkey. Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. Middle E Tech Univ, TR-06531 Ankara, Turkey. Canakkale Onsekiz Mart Univ, TR-17020 Canakkale, Turkey. Univ Texas, Dept Astron, Austin, TX 78712 USA. Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. Guilford Coll, Greensboro, NC 27410 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Yost, SA (reprint author), Univ Michigan, Randall Lab 2477, 450 Church St, Ann Arbor, MI 48104 USA. EM sayost@umich.edu RI Guver, Tolga/C-1408-2011; Horns, Dieter/C-9727-2011; Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Rujopakarn, Wiphu/E-7849-2012; McKay, Timothy/C-1501-2009; Guver, Tolga/B-1039-2014; OI McKay, Timothy/0000-0001-9036-6150; Guver, Tolga/0000-0002-3531-9842; Rowell, Gavin/0000-0002-9516-1581 NR 17 TC 8 Z9 8 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. PY 2006 VL 327 IS 8 BP 803 EP 805 DI 10.1002/asna.200610683 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089SI UT WOS:000240900600015 ER PT J AU Lehner, MJ Alcock, C Axelrod, T Bianco, F Byun, YI Chen, WP Cook, KH Dave, R de Pater, I Giammarco, J King, SK Lee, T Lissauer, J Marshall, SL Mondal, S Nihei, T Rice, J Schwamb, M Wang, A Wang, SY Wen, CY Zhang, ZW AF Lehner, M. J. Alcock, C. Axelrod, T. Bianco, F. Byun, Y. -I. Chen, W. -P. Cook, K. H. Dave, R. de Pater, I. Giammarco, J. King, S. -K. Lee, T. Lissauer, J. Marshall, S. L. Mondal, S. Nihei, T. Rice, J. Schwamb, M. Wang, A. Wang, S. -Y. Wen, C. -Y. Zhang, Z. -W. TI TAOS - The Taiwanese-American Occultation Survey SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 1st Workshop on Heterogeneous Telescope Networks CY JUL 18-21, 2005 CL Exeter, ENGLAND DE Kuiper Belt; occultations; methods : observational; telescopes ID KUIPER-BELT OBJECTS; BODIES AB The Taiwanese-American Occultation Survey (TAOS) seeks to determine the number and size spectrum for small (similar to 3 km) bodies in the Kuiper Belt. This will be accomplished by searching for the brief occultations of bright stars (R similar to 14) by these objects. We have designed and built a special purpose photometric monitoring system for this purpose. TAOS comprises four 50 cm telescopes, each equipped with a 2048 x 2048 pixel CCD camera, in a compact array located in the central highlands of Taiwan. TAOS will monitor up to 2 000 stars at 5 Hz. The system went into scientific operation in the autumn of 2005. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Yonsei Univ, Dept Astron, Seoul 120749, South Korea. Natl Cent Univ, Inst Astron, Taoyuan 320, Taiwan. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Natl Taiwan Univ, Condensed Matter Sci & Phys Dept, Taipei 106, Taiwan. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. RP Lehner, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mlehner@cfa.harvard.edu RI Lee, Typhoon/N-8347-2013; OI Lehner, Matthew/0000-0003-4077-0985 NR 7 TC 5 Z9 5 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 8 BP 814 EP 817 DI 10.1002/asna.200610688 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089SI UT WOS:000240900600018 ER PT J AU Nandra, K O'Neill, PM George, IM Reeves, JN Turner, TJ AF Nandra, K. O'Neill, P. M. George, I. M. Reeves, J. N. Turner, T. J. TI An XMM-Newton survey of broad iron lines in AGN SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE galaxies : active; galaxies : nuclei; X-rays : galaxies; line : profiles ID BLACK-HOLE; SEYFERT-1 GALAXIES; ASCA OBSERVATIONS; ACCRETION DISKS; EMISSION; PROFILES; SPECTRUM AB We report on the iron K alpha line properties of a sample of Seyfert galaxies observed with the XMM-Newton EPIC pn instrument. Using a systematic and uniform analysis, we find that complexity at iron-K is extremely common in the XMM-Newton spectra. Once appropriate soft X-ray absorption, narrow 6.4 keV emission and associated Compton reflection are accounted for, similar to 75% of the sample show an improvement when a further component is introduced. The typical properties of the broad emission are both qualitatively and quantitatively consistent with previous results from ASCA. The complexity is in general very well described by relativistic accretion disk models. In most cases the characteristic emission radius is constrained to be within similar to 50 R-g, where strong gravitational effects become important. We find in about 1/3 of the sample the accretion disk interpretation is strongly favoured over competing models. In a few objects no broad line is apparent. We find evidence for emission within 6R(g) in only two cases, both of which exhibit highly complex absorption. Evidence for black hole spin based on the X-ray spectra therefore remains tentative. (c) 2006 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim. C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. Univ Maryland Baltimore Cty, Dept Phys & Astron, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Nandra, K (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. EM k.nandra@imperial.ac.uk NR 25 TC 18 Z9 18 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 10 BP 1039 EP 1042 DI 10.1002/asna.200610641 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 120DG UT WOS:000243063300020 ER PT J AU Papadakis, IE Ioannou, Z Kazanas, D AF Papadakis, I. E. Ioannou, Z. Kazanas, D. TI Fourier-resolved spectroscopy of AGN using XMM-Newton data SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE galaxies : active; galaxies : Seyfert; methods : data analysis; X-rays : galaxies ID ACCRETING BLACK-HOLES; X-RAY VARIABILITY; ACTIVE GALACTIC NUCLEI; K-ALPHA LINE; LUMINOUS LMXBS; BOUNDARY-LAYER; MCG-6-30-15; EMISSION; REFLECTION; GALAXIES AB We present a brief account of the theory on which the novel method of 'Fourier-resolved spectroscopy' is based. We summarize the results from the past application of this method to the study of Galactic Black Hole candidate sources and MCG-6-30-15, and we present new results from the Fourier-resolved spectroscopy of archival XMM-Newton data of five AGN, namely, Mrk 766, NGC 3516, NGC 3783, NGC 4051 and Ark 564. When we combine all the past and present results from Galactic sources and AGN, we find that the slope of the Fourier-resolved spectra in accreting black hole systems decreases with increasing frequency as proportional to f(-0.25), irrespective of whether the system is in its High or Low state. We find significant evidence that the iron line in Mrk 766, NGC 3783 and NGC 4051 is variable on time scales similar to 1 day-1 hour. There is an indication that, just like in Galactic sources, the equivalent width of the line in the Fourier-resolved spectra of AGN decreases with increasing frequency. (c) 2006 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim. C1 Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. Fdn Res & Technol Hellas, IESL, GR-71110 Iraklion, Greece. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Papadakis, IE (reprint author), Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. EM jhep@physics.uoc.gr NR 27 TC 2 Z9 2 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 10 BP 1047 EP 1054 DI 10.1002/asna.200610642 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 120DG UT WOS:000243063300022 ER PT J AU Braito, V Reeves, JN Dewangan, G George, I Griffiths, R Markowitz, A Nandra, K Porquet, D Ptak, A Turner, TJ Yaqoob, T Weaver, K AF Braito, V. Reeves, J. N. Dewangan, G. George, I. Griffiths, R. Markowitz, A. Nandra, K. Porquet, D. Ptak, A. Turner, T. J. Yaqoob, T. Weaver, K. TI The iron emission line complex of MCG-5-23-16: the long XMM-Newton look SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE galaxies : active; galaxies : individual (MCG-5-23-16); galaxies : Seyfert; X-rays : galaxies ID ABSORPTION-LINES; BLACK-HOLE; REFLECTION; SPECTRUM; OUTFLOW AB We present the results of the simultaneous XMM-Newton and Chandra observations of the bright Seyfert 1.9 galaxy MCG-5-23-16, which is one of the best known examples of a relativistically broadened iron K alpha line, We find that: a) the soft X-ray emission is likely to be dominated by photoionized gas, b) the complex iron emission line is best modelled with a narrow and a broad component with a FWHM similar to 44000 km/s. This latter component has an EW similar to 50 eV and its profile is well described with an emission line mainly originating from the accretion disk a few tens of gravitational radii from the central black hole and viewed with an inclination angle similar to 40 degrees. We found evidence of a possible sporadic absorption line at similar to 7.7 keV which, if associated with Fe XXVI Ka resonance absorption, is indicative of a possible high velocity (v similar to 0.1c) outflow. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. C1 NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AW, England. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Braito, V (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 662, Greenbelt, MD 20771 USA. EM vale@milkyway.gsfc.nasa.gov RI Ptak, Andrew/D-3574-2012; OI Porquet, Delphine/0000-0001-9731-0352; Braito, Valentina/0000-0002-2629-4989 NR 18 TC 7 Z9 7 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 10 BP 1067 EP 1070 DI 10.1002/asna.200610694 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 120DG UT WOS:000243063300026 ER PT J AU Reeves, JN Fabian, AC Kataoka, J Kunieda, H Markowitz, A Miniutti, G Okajima, T Serlemitsos, P Takahashi, T Terashima, Y Yaqoob, T AF Reeves, J. N. Fabian, A. C. Kataoka, J. Kunieda, H. Markowitz, A. Miniutti, G. Okajima, T. Serlemitsos, P. Takahashi, T. Terashima, Y. Yaqoob, T. TI Suzaku observations of iron lines and reflection in AGN SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE X-rays : galaxies; galaxies : active; galaxies : Seyfert ID ACTIVE GALACTIC NUCLEI; RADIO GALAXY 3C-120; X-RAY ABSORPTION; FE K-ALPHA; XMM-NEWTON; COLD MATTER; BLACK-HOLE; LONG HARD; MCG-6-30-15; EMISSION AB Initial results on the iron K-shell line and reflection component in several AGN observed as part of the Suzaku Guaranteed Time program are reviewed. This paper discusses a small sample of Compton-thin Seyferts observed to date with Suzaku; namely MCG-5-23-16, MCG-6-30-15, NGC4051, NGC3516, NGC2110, 3C120 and NGC2992. The broad iron K alpha emission line appears to be present in all but one of these Seyfert galaxies, while the narrow core of the line from distant matter is ubiquitous in all the observations. The iron line in MCG-6-30-15 shows the most extreme relativistic blurring of all the objects, the red-wing of the line requires the inner accretion disk to extend inwards to within 2.2R(g) of the black hole, in agreement with the XMM-Newton observations. Strong excess emission in the Hard X-ray Detector (HXD) above 10 keV is observed in many of these Seyfert galaxies, consistent with the presence of a reflection component from reprocessing in Compton-thick matter (e.g. the accretion disk). Only one Seyfert galaxy (NGC 2110) shows neither a broad iron line nor a reflection component. The spectral variability of MCG-6-30-15, MCG-5-23-16 and NGC 4051 is also discussed. In all 3 cases, the spectra appear harder when the source is fainter, while there is little variability of the iron line or reflection component with source flux. This agrees with a simple two component spectral model, whereby the variable emission is the primary power-law, while the iron line and reflection component remain relatively constant. (c) 2006 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim. C1 NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. RP Reeves, JN (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 662, Greenbelt, MD 20771 USA. EM jnr@milkyway.gsfc.nasa.gov RI Miniutti, Giovanni/L-2721-2014; XRAY, SUZAKU/A-1808-2009 OI Miniutti, Giovanni/0000-0003-0707-4531; NR 39 TC 21 Z9 21 U1 1 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. PY 2006 VL 327 IS 10 BP 1079 EP 1086 DI 10.1002/asna.200610696 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 120DG UT WOS:000243063300029 ER PT J AU Markowitz, A Reeves, JN Serlemitsos, P Yaqoob, T Awaki, H Fabian, A Gallo, L Griffiths, RE Kunieda, H Miniutti, G Mushotzky, R Okajima, T AF Markowitz, A. Reeves, J. N. Serlemitsos, P. Yaqoob, T. Awaki, H. Fabian, A. Gallo, L. Griffiths, R. E. Kunieda, H. Miniutti, G. Mushotzky, R. Okajima, T. TI Suzaku observation of NGC 3516: complex absorption and the broad and narrow FeK lines SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE galaxies : active; galaxies : individual (NGC 3516); galaxies : Seyfert; X-rays : galaxies ID SEYFERT-1 GALAXY NGC-3516; ACTIVE GALACTIC NUCLEI; X-RAY-ABSORPTION; ALPHA PROFILE; BLACK-HOLE; VARIABILITY; EMISSION AB We present preliminary results from a 150 ks Suzaku observation of the Seyfert 1 galaxy NGC 3516. Suzaku's wide bandpass has enabled us to deconvolve the broadband emitting and absorbing components in this object, breaking model degeneracies inherent in previous, smaller-bandpass spectra. The primary power-law continuum is absorbed by an ionized absorber as well as a partial-covering absorber; the column density of the ionized absorber has increased by a factor of similar to 3 since XMM-Newton observations in 2001. We detect a soft power-law component which may be scattered emission. We confirm the presence of the broad Fe line, finding a 185(-70)(+130) eV equivalent width line that indicates emission extending down to a few Schwarzschild radii. Models which exclude either the broad line or the partial-covering absorber are rejected. Suzaku's high effective area and low background near 6 keV also allow us to resolve the narrow Fe K emission line; we find a FWHM velocity width near 4000 km s(-1), commensurate with Broad Line Region velocities. (c) 2006 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim. C1 NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. Johns Hopkins Univ, NASA Post Doc Res Associate, Baltimore, MD 21218 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Ehime Univ, Fac Sci, Dept Phys, Matsuyama, Ehime 7908577, Japan. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Markowitz, A (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. EM agm@milkyway.gsfc.nasa.gov RI Miniutti, Giovanni/L-2721-2014; XRAY, SUZAKU/A-1808-2009 OI Miniutti, Giovanni/0000-0003-0707-4531; NR 19 TC 5 Z9 5 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PY 2006 VL 327 IS 10 BP 1087 EP 1090 DI 10.1002/asna.200610697 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 120DG UT WOS:000243063300030 ER PT J AU Turner, TJ Miller, L George, IM Reeves, JN AF Turner, TJ Miller, L George, IM Reeves, JN TI Evidence for orbital motion of material close to the central black hole of Mrk 766 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; X-rays : individual : Mrk 766; accretion, accretion disks ID ACTIVE GALACTIC NUCLEI; LINE SEYFERT-1 GALAXIES; X-RAY REFLECTION; ASCA OBSERVATIONS; ACCRETION DISKS; EMISSION; FE; VARIABILITY; FEATURES; SPECTRA AB Time-resolved X-ray spectroscopy has been obtained for the narrow line Seyfert galaxy Mrk 766 from XMM-Newton observations. We present analysis in the energy-time plane of EPIC pn data in the 4-8 keV band with energy resolution R similar or equal to 50. A component of Fe K alpha emission detected in the maps shows a variation of photon energy with time that appears both to be statistically significant and to be consistent with sinusoidal variation. We investigate the interpretation that there exists a component of line emission from matter in a Keplerian orbit around a supermassive black hole. The orbit has a period similar to 165 ks and a line-of-sight velocity similar to 13 500 km s(-1). This yields a lower limit for the central mass of M > 4.9 x 10(5) M-circle dot within a radius of 3.6 x 10(13) cm (2.4 AU). The orbit parameters are consistent with higher black hole masses, but the lack of any substantial gravitational redshift of the orbit implies an upper limit to the black hole mass of 4.5 x 10(7) M-circle dot. C1 Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. Univ Oxford, Dept Phys, Oxford OX1 3RH, England. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Turner, TJ (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM turner@milkyway.gsfc.nasa.gov NR 29 TC 47 Z9 47 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2006 VL 445 IS 1 BP 59 EP 67 DI 10.1051/0004-6361:20053042 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993YI UT WOS:000233995600010 ER PT J AU Peeters, Z Rodgers, SD Charnley, SB Schriver-Mazzuoli, L Schriver, A Keane, JV Ehrenfreund, P AF Peeters, Z Rodgers, SD Charnley, SB Schriver-Mazzuoli, L Schriver, A Keane, JV Ehrenfreund, P TI Astrochemistry of dimethyl ether SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; methods : laboratory; ISM : molecules ID STAR-FORMING REGIONS; SPECTRAL-LINE SURVEY; HOT CORES; CHEMICAL DIFFERENTIATION; INTERSTELLAR CLOUDS; ORGANIC-MOLECULES; COMPLEX-MOLECULES; IRAS 16293-2422; ICE ANALOGS; AMINO-ACIDS AB Dimethyl ether (DME, CH3OCH3) is one of the largest organic molecules detected in the interstellar gas and shows high abundances in star-forming regions, known as hot molecular cores. The observed DME might be formed on grains or by secondary gas phase reactions from a precursor molecule, which in turn was sublimed into the gas phase from the grain surface. Studies on the stability and degradation pathways of DME therefore provide important constraints on the evolutionary cycle of large organic molecules and chemical pathways in the interstellar medium. We studied the UV photodestruction rate of DME in a solid argon matrix. DME was destroyed with a half- life of 54 seconds under laboratory conditions, which corresponds to 8.3 x 10(5) years in a dense cloud. We discuss the UV photochemistry of DME in the context of two issues: its formation mechanism and its chemistry in hot cores. Chemical models of shielded hot core regions indicate that UV photodestruction is relatively unimportant for DME, even by the internally-generated radiation field. These models clearly show that gas phase processes are almost certainly responsible for the formation of interstellar DME. C1 Leiden Univ, Inst Chem, NL-2300 RA Leiden, Netherlands. NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. Univ Paris 06, Dept Phys Chem, F-75005 Paris, France. RP Peeters, Z (reprint author), Leiden Univ, Inst Chem, POB 9502, NL-2300 RA Leiden, Netherlands. EM peters@strw.leidenuniv.nl RI Charnley, Steven/C-9538-2012 NR 61 TC 25 Z9 25 U1 0 U2 7 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 JAN PY 2006 VL 445 IS 1 BP 197 EP 204 DI 10.1051/0004-6361:20053651 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993YI UT WOS:000233995600020 ER PT J AU Gotz, D Mereghetti, S Molkov, S Hurley, K Mirabel, IF Sunyaev, R Weidenspointner, G Brandt, S Del Santo, M Feroci, M Gogus, E von Kienlin, A van der Klis, M Kouveliotou, C Lund, N Pizzichini, G Ubertini, P Winkler, C Woods, PM AF Gotz, D Mereghetti, S Molkov, S Hurley, K Mirabel, IF Sunyaev, R Weidenspointner, G Brandt, S Del Santo, M Feroci, M Gogus, E von Kienlin, A van der Klis, M Kouveliotou, C Lund, N Pizzichini, G Ubertini, P Winkler, C Woods, PM TI Two years of INTEGRAL monitoring of the soft gamma-ray repeater SGR 1806-20: from quiescence to frenzy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma rays : bursts; gamma rays : observations; stars : pulsars : general; stars : pulsars : individual : SGR 1806-20 ID GIANT FLARE; SGR 1806-20; EMISSION; BURSTS; 1ST; SPECTROMETER; MAGNETARS; CHANDRA; SPI AB SGR 1806-20 has been observed for more than 2 years with the INTEGRAL satellite. In this period the source went from a quiescent state into a very active one culminating in a giant flare on December 27, 2004. Here we report on the properties of all the short bursts detected with INTEGRAL before the giant flare. We derive their number-intensity distribution and confirm the hardness-intensity correlation for the bursts found by Gotz et al. (2004a, A&A, 417, L45). Our sample includes a very bright outburst that occurred on October 5, 2004, during which over one hundred bursts were emitted in 10 minutes, involving an energy release of 3 x 1042 erg. We present a detailed analysis of it and discuss our results in the framework of the magnetar model. C1 INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. Russian Acad Sci, Inst Space Res, Moscow 117997, Russia. Max Planck Inst Astrophys, D-85740 Munich, Germany. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. European So Observ, Santiago 19, Chile. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark. INAF, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. Sabanci Univ, Istanbul, Turkey. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. INAF, Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy. ESA, Estec, RSSD, NL-2201 AZ Noordwijk, Netherlands. Univ Manchester, Dept Phys, Manchester M60 1QD, Lancs, England. RP Gotz, D (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm, Via Bassini 15, I-20133 Milan, Italy. EM diego@mi.iasf.cnr.it OI Feroci, Marco/0000-0002-7617-3421; Del Santo, Melania/0000-0002-1793-1050; MEREGHETTI, SANDRO/0000-0003-3259-7801 NR 42 TC 28 Z9 28 U1 0 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 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2006 VL 445 IS 1 BP 313 EP 321 DI 10.1051/0004-6361:20053648 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993YI UT WOS:000233995600028 ER PT J AU Chen, XP Henning, T van Boekel, R Grady, CA AF Chen, XP Henning, T van Boekel, R Grady, CA TI VLT/NACO adaptive optics imaging of the Herbig Ae star HD 100453 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries : general; stars : individual : HD 100453; stars : pre-main sequence; techniques : high angular resolution ID AE/BE STARS; CIRCUMSTELLAR DISKS; ISO SPECTROSCOPY; BINARIES; COMPANIONS; MEMBERS; CONICA AB We report the detection of a companion candidate to the Herbig Ae star HD 100453, using the NACO instrument at the VLT UT4. The separation between the companion candidate and HD 100453 is 1.''06, and their brightness contrast is 5.1 mag at K-s and 4.2 mag at Br gamma. We discuss the possible nature of the newly detected star based on near-infrared photometry. The photometric data are consistent with a 0.3 M-circle dot companion to HD 100453, corresponding to a spectral type of M3-M5. This detection could have important implications for the structure of the disk around HD 100453. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. NASA, Explorat Universe Div, Eureka Sci & Goddard Space Flight Ctr, GSFC Greenbelt, Greenbelt, MD 20771 USA. RP Chen, XP (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM chen@mpia.de; henning@mpia.de; boekel@mpia.de; cgrady@echelle.gsfc.nasa.gov NR 32 TC 14 Z9 14 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 JAN PY 2006 VL 445 IS 1 BP 331 EP 335 DI 10.1051/0004-6361:20054122 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993YI UT WOS:000233995600030 ER PT J AU Pollock, AMT Corcoran, MF AF Pollock, AMT Corcoran, MF TI Evidence for colliding winds in WR 25 from XMM-Newton observations of X-ray variability SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : stars; stars : Wolf-Rayet; stars : individual : WR 25; stars : winds, outflows; stars : binaries : general ID STARS AB The Wolf-Rayet star WR 25 in the Carina Nebula is a surprisingly bright X-ray source, and amongst the brightest WR stars in X-rays. It is a suspected binary star, though its binary nature has been a matter of controversy. We report here observations of WR 25 from the XMM-Newton archive which showed an increase in X-ray luminosity of more than a factor of two. The X-ray absorption also increased. Such a large change in X-ray output is unknown in single massive stars, though large changes in X-ray brightness are seen in binaries. The most likely explanation of the observed X-ray variability is as a result of colliding- wind emission in a moderately eccentric binary with a period of about 4 years. The next periastron passage is expected in 2007. The X-ray spectrum is similar to that of the archetype colliding-wind binary WR 140. C1 European Space Agcy, European Space Astron Ctr, XMM Newton Sci Operat Ctr, Madrid, Spain. Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Seabrook, MD 20706 USA. RP European Space Agcy, European Space Astron Ctr, XMM Newton Sci Operat Ctr, Apartado 50727,Villafranca Castillo, Madrid, Spain. NR 9 TC 19 Z9 19 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2006 VL 445 IS 3 BP 1093 EP 1097 DI 10.1051/0004-6361:20053496 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999QH UT WOS:000234404500037 ER PT J AU Nilsson, H Ljung, G Lundberg, H Nielsen, KE AF Nilsson, H Ljung, G Lundberg, H Nielsen, KE TI The FERRUM project: improved experimental oscillator strengths in CrII SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE atomic data; line : identification ID TRANSITION-PROBABILITIES; BRANCHING RATIOS; LIFETIME MEASUREMENTS; RADIATIVE LIFETIMES; LINES; CHROMIUM; CR(II) AB We report absolute oscillator strengths for 119 Cr II transitions in the wavelength region 2050-4850 angstrom. The transition probabilities have been derived by combining radiative lifetimes, measured with time- resolved laser induced fluorescence, and branching fractions from intensity calibrated Fouirer transform spectrometer data. New radiative lifetimes for the 3d(4)(D-5)4p F-4, D-4 and P-6 terms are reported, adding up to a total of 25 energy levels with measured lifetimes used to derive this improved set of atomic data. C1 Lund Univ, Lund Observ, S-22100 Lund, Sweden. Lund Inst Technol, Dept Phys, S-22100 Lund, Sweden. Catholic Univ Amer, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. RP Nilsson, H (reprint author), Lund Univ, Lund Observ, Box 43, S-22100 Lund, Sweden. NR 18 TC 56 Z9 56 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2006 VL 445 IS 3 BP 1165 EP 1168 DI 10.1051/0004-6361;20054152 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999QH UT WOS:000234404500044 ER PT J AU Kulkarni, VP Woodgate, BE York, DG Thatte, DG Meiring, J Palunas, P Wassell, E AF Kulkarni, VP Woodgate, BE York, DG Thatte, DG Meiring, J Palunas, P Wassell, E TI A Fabry-Perot imaging search for Ly alpha emission in quasar absorbers at z 2.4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : evolution; galaxies : high-redshift; quasars : absorption lines ID STAR-FORMATION HISTORY; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; O-III EMISSION; ABSORPTION SYSTEMS; LINE OBJECTS; LUMINOSITY DENSITY; EMITTING GALAXIES; MODERATE-REDSHIFT; FORMING GALAXIES AB We have carried out a deep narrowband imaging survey of six fields with heavy-element quasar absorption lines, using the Goddard Fabry-Perot ( FP) system at the Apache Point Observatory ( APO) 3.5 m telescope. The aim of these observations was to search for redshifted Ly alpha emission from the galaxies underlying the absorbers at z = 2: 3 - 2: 5 and their companion galaxies. The 3 sigma sensitivity levels ranged between 1.9 x 10(-17) and 5.4 x 10(-17) ergs s(-1) cm(-2) in observed-frame Ly alpha flux. No significant Ly alpha emitters were detected at a level > 3 sigma. The absence of significant Ly alpha emission implies limits on the star formation rate ( SFR) of 0.9 - 2.7 M-circle dot yr(-1) per 2 pixel x 2 pixel region, if no dust attenuation is assumed. We compare our results with those from other emission-line studies of absorber fields and with predictions for the global average SFR based on the models of cosmic chemical evolution. Our limits are among the tightest existing constraints on Ly alpha emission from galaxies in absorber fields, but they are consistent with many other studies. In the absence of dust attenuation, these studies suggest that SFRs in a large fraction of objects in the absorber fields may lie below the global mean SFR. However, it is possible that dust attenuation is responsible for the low emission-line fluxes in some objects. It is also possible that the star-forming regions are compact and at smaller angular separations from the quasar than the width of our point-spread function and get lost in the quasar emission. We outline future observations that could help to distinguish between the various possibilities. C1 Univ S Carolina, Dept Phys & Astron, Columbia, SC 29208 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Catholic Univ Amer, Washington, DC 20064 USA. Thomas Aquinas Coll, Santa Paula, CA 93060 USA. RP Kulkarni, VP (reprint author), Univ S Carolina, Dept Phys & Astron, Columbia, SC 29208 USA. RI Woodgate, Bruce/D-2970-2012 NR 70 TC 42 Z9 42 U1 1 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2006 VL 636 IS 1 BP 30 EP 45 DI 10.1086/497885 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800004 ER PT J AU Borys, C Blain, AW Dey, A Le Floc'h, E Jannuzi, BT Barnard, V Bian, C Brodwin, M Menendez-Delmestre, K Thompson, D Brand, K Brown, MJI Dowell, CD Eisenhardt, P Farrah, D Frayer, DT Higdon, J Higdon, S Phillips, T Soifer, BT Stern, D Weedman, D AF Borys, C Blain, AW Dey, A Le Floc'h, E Jannuzi, BT Barnard, V Bian, C Brodwin, M Menendez-Delmestre, K Thompson, D Brand, K Brown, MJI Dowell, CD Eisenhardt, P Farrah, D Frayer, DT Higdon, J Higdon, S Phillips, T Soifer, BT Stern, D Weedman, D TI MIPS J142824.0+352619: A hyperluminous starburst galaxy at z=1.325 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : formation; galaxies : starburst ID ULTRALUMINOUS INFRARED GALAXIES; DEEP SUBMILLIMETER SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; CLERK-MAXWELL-TELESCOPE; EXTREMELY RED OBJECTS; SCUBA SUPER-MAP; NUMBER COUNTS; HIGH-REDSHIFT; SURVEY FIELDS; RADIO AB Using the SHARC-II camera at the Caltech Submillimeter Observatory to obtain 350 mu m images of sources detected with the MIPS instrument on Spitzer, we have discovered a remarkable object at z =1.325 +/- 0.002 with an apparent far-infrared luminosity of 3.2( +/- 0.7) x 10(13) L-circle dot. Unlike other z > 1 sources of comparable luminosity selected from mid-IR surveys, MIPS J142824.0 + 352619 lacks any trace of AGN activity, and is likely a luminous analog of galaxies selected locally by IRAS, or at high redshift in the submillimeter. This source appears to be lensed by a foreground elliptical galaxy at z = 1.034, although the amplification is likely modest ( less than or similar to 10). We argue that the contribution to the observed optical/near-IR emission from the foreground galaxy is small, and hence are able to present the rest-frame UV through radio spectral energy distribution of this galaxy. Due to its unusually high luminosity, MIPS J142824.0 + 352619 presents a unique chance to study a high-redshift dusty starburst galaxy in great detail. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Observ Paris, GEPI, F-92195 Meudon, France. Joint Astron Ctr, Hilo, HI 96720 USA. Jet Prop Lab, Pasadena, CA 91109 USA. Princeton Univ Observ, Princeton, NJ 08544 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Borys, C (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM borys@caltech.edu RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 NR 40 TC 29 Z9 29 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2006 VL 636 IS 1 BP 134 EP 139 DI 10.1086/497983 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800012 ER PT J AU Pedersen, K Hurley, K Hjorth, J Smith, DA Andersen, MI Christensen, L Cline, T Fynbo, JPU Goldsten, J Golenetskii, S Gorosabel, J Jakobsson, P Jensen, BL Milvang-Jensen, B McClanahan, T Moller, P Palshin, V Schartel, N Trombka, J Ulanov, M Watson, D AF Pedersen, K Hurley, K Hjorth, J Smith, DA Andersen, MI Christensen, L Cline, T Fynbo, JPU Goldsten, J Golenetskii, S Gorosabel, J Jakobsson, P Jensen, BL Milvang-Jensen, B McClanahan, T Moller, P Palshin, V Schartel, N Trombka, J Ulanov, M Watson, D TI Multiwavelength studies of the optically dark gamma-ray burst 001025A SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; X-rays : general ID AFTERGLOW EMISSION; BATSE OBSERVATIONS; HOST GALAXY; SUPERNOVA; BRIGHT; CONSTRAINTS; GRB-020124; DISCOVERY; UNIVERSE; SPECTRA AB We identify the fading X-ray afterglow of GRB 001025A from XMM-Newton observations obtained 1.9-2.3 days, 2 yr, and 2.5 yr after the burst. The nondetection of an optical counterpart to an upper limit of R = 25.5, 1.20 days after the burst, makes GRB 001025A a '' dark '' burst. Based on the X-ray afterglow spectral properties of GRB 001025A, we argue that some bursts appear optically dark because their afterglow is faint and their cooling frequency is close to the X-ray band. This interpretation is applicable to several of the few other dark bursts where the X- ray spectral index has been measured. The X-ray afterglow flux of GRB 001025A is an order of magnitude lower than for typical long-duration gamma-ray bursts. The spectrum of the X-ray afterglow can be fitted with an absorbed synchrotron emission model, an absorbed thermal plasma model, or a combination thereof. For the latter, an extrapolation to optical wavelengths can be reconciled with the R-band upper limit on the afterglow, without invoking any optical circumburst absorption, provided the cooling frequency is close to the X-ray band. Alternatively, if the X-ray afterglow is due to synchrotron emission only, 7 mag of extinction in the observed R-band is required to meet the R-band upper limit, making GRB 001025A much more obscured than bursts with detected optical afterglows. Based on the column density of X-ray-absorbing circumburst matter, an SMC gas-to-dust ratio is insufficient to produce this amount of extinction. The X-ray tail of the prompt emission enters a steep temporal decay excluding that the tail of the prompt emission is the onset of the afterglow. To within the astrometric uncertainty, this afterglow was coincident with an extended object, seen in a deep VLT R-band image, which we identify as the likely host galaxy of GRB 001025A. C1 Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. CSIC, IAA, E-18080 Granada, Spain. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. European So Observ, D-85748 Garching, Germany. ESA, XMM Newton Sci Operat Ctr, Madrid 28080, Spain. RP Pedersen, K (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. EM kp@astro.ku.dk; khurley@ssl.berkeley.edu; jens@astro.ku.dk; donaldas@umich.edu; mandersen@aip.de; lchristensen@aip.de; thomas.l.cline@nasa.gov; jfynbo@phys.au.dk; john.goldsten@jhuapl.edu; golen@mail.ioffe.ru; jgu@laeff.esa.es; pallja@astro.ku.dk; brian_j@astro.ku.dk; milvang@mpe.mpg.de; timothy.p.mcclanahan@nasa.gov; pmoller@eso.org; val@mail.ioffe.ru; nscharte@xmm.vilspa.esa.es; jacob.i.trombka.1@nasa.gov; mulanov@mail.ioffe.ru; darach@astro.ku RI McClanahan, Timothy/C-8164-2012; Pal'shin, Valentin/F-3973-2014; Fynbo, Johan/L-8496-2014; Christensen, Lise/M-5301-2014; Hjorth, Jens/M-5787-2014; Ulanov, Mikhail/B-3467-2015; Golenetskii, Sergey/B-3818-2015; Watson, Darach/E-4521-2015; Jensen, Brian Lindgren/E-1275-2015; Jakobsson, Pall/L-9950-2015 OI Fynbo, Johan/0000-0002-8149-8298; Christensen, Lise/0000-0001-8415-7547; Hjorth, Jens/0000-0002-4571-2306; Ulanov, Mikhail/0000-0002-0076-5228; Watson, Darach/0000-0002-4465-8264; Jensen, Brian Lindgren/0000-0002-0906-9771; Jakobsson, Pall/0000-0002-9404-5650 NR 57 TC 11 Z9 11 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2006 VL 636 IS 1 BP 381 EP 390 DI 10.1086/497948 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 997ZY UT WOS:000234288800031 ER PT J AU Brosius, JW AF Brosius, JW TI Thermal composition and Doppler velocities in a transequatorial loop at the solar limb SO ASTROPHYSICAL JOURNAL LA English DT Article DE sun : activity; sun : corona; sun : transition region; sun : UV radiation ID CORONAL DIAGNOSTIC SPECTROMETER; ACTIVE REGIONS; ATOMIC DATABASE; EMISSION-LINES; MASS EJECTION; ASSOCIATION; BALANCE; CHIANTI; SOHO; EIT AB We observed a transequatorial loop ( TEL) connecting NOAA Active Regions 10652 and 10653 at the west solar limb on 2004 July 29 with the Extreme-Ultraviolet Imaging Telescope ( EIT) and the Coronal Diagnostic Spectrometer ( CDS) aboard the Solar and Heliospheric Observatory. Only the loop's northern leg was observed with CDS. The loop appeared bright and cospatial in extreme-ultraviolet emission lines from ions formed over a wide range of temperature ( T, in kelvins), including He I ( log T = 4.0), O III ( log T = 4.9), O IV ( 5.2), O V ( 5.4), Ne VI ( 5.6), Ca X ( 5.9), Mg X ( 6.1), and Fe XII ( log T = 6.1). This indicates that the loop plasma was multithermal and covered roughly 2 orders of magnitude in temperature. Our measurement of He I, O III, and O IV line emission reveals the coolest plasma ever detected in a TEL. The most likely explanation for the wide range of cospatial temperatures in the TEL is that it consisted of numerous sub-resolution strands, all at different temperatures. Each of the lines that are formed at temperatures less than 106 K exhibited relative Doppler blueshifts in the TEL that correspond to velocities toward the observer larger than 30 km s(-1), where the two strongest cool lines ( He I at 584.3 (A) over circle and O V at 629.7 (A) over circle) yielded maximum values of 37 and 41 km s(-1), respectively. The presence of cool plasma in the TEL at heights several times those of the cool ions' scale heights suggests that the loop remained visible at low temperatures by maintaining a steady flow of cool plasma. C1 Catholic Univ Amer, Dept Phys, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Solar Phys Branch, Greenbelt, MD 20771 USA. RP Brosius, JW (reprint author), Catholic Univ Amer, Dept Phys, Code 661, Greenbelt, MD 20771 USA. EM brosius@comstoc.gsfc.nasa.gov NR 29 TC 4 Z9 4 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2006 VL 636 IS 1 BP L57 EP L60 DI 10.1086/500046 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998AB UT WOS:000234289100015 ER PT J AU Liu, X Zhang, SN AF Liu, X Zhang, SN TI A cross-correlation analysis of WMAP and EGRET data in wavelet space SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmic rays; diffuse radiation; methods : data analysis ID ANISOTROPY-PROBE DATA; DETECT NON-GAUSSIANITY; GAMMA-RAY EMISSION; SPHERICAL WAVELETS; GALACTIC PLANE; MAPS; FOREGROUNDS; SKY; MATTER; CMB AB We cross-correlate the first-year Wilkinson Microwave Anisotropy Probe (WMAP) data and the diffuse gamma-ray intensity maps from the Energetic Gamma-Ray Experiment Telescope (EGRET) using spherical-wavelet approaches. Correlations at the 99.7% significance level have been detected, at scales around 15 degrees in the WMAP foreground-cleaned W-band and Q-band maps, based on data from regions that are outside the most conservative WMAP foreground mask; no significant correlation is found with the Tegmark cleaned map. The detected correlation is most likely of Galactic origin and thus can help probe the origins of possible Galactic foreground residuals and ultimately remove them from measured microwave sky maps. C1 Tsing Hua Univ, Dept Phys, Beijing 100084, Peoples R China. Tsing Hua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China. Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100039, Peoples R China. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Space Sci Lab, Huntsville, AL 35812 USA. RP Liu, X (reprint author), Tsing Hua Univ, Dept Phys, Beijing 100084, Peoples R China. EM liux00@mails.tsinghua.edu.cn; zhangsn@tsinghua.edu.cn NR 45 TC 7 Z9 7 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2006 VL 636 IS 1 BP L1 EP L4 DI 10.1086/499804 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998AB UT WOS:000234289100001 ER PT J AU Brodwin, M Lilly, SJ Porciani, C McCracken, HJ Le Fevre, O Foucaud, S Crampton, D Mellier, Y AF Brodwin, M Lilly, SJ Porciani, C McCracken, HJ Le Fevre, O Foucaud, S Crampton, D Mellier, Y TI The Canada-France Deep Fields Survey. III. Photometric redshift distribution to I-AB=24 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies : distances and redshifts; galaxies : photometry; methods : data analysis; methods : statistical ID GALAXY LUMINOSITY FUNCTION; LYMAN-BREAK GALAXIES; DIGITAL SKY SURVEY; POWER SPECTRUM; EVOLUTION; SELECTION; ULTRAVIOLET; CATALOGS; DENSITY; OBJECTS AB We compute accurate redshift distributions to I-AB=24 and R-AB=24.5 using photometric redshifts estimated from six-band UBVRIZ photometry in the Canada-France Deep Fields Photometric Redshift Survey (CFDF-PRS). Our photometric redshift algorithm is calibrated using hundreds of CFRS spectroscopic redshifts in the same fields. The dispersion in redshift is sigma/(1+z)less than or similar to 0.04 to the CFRS depth of I-AB=22.5, rising to sigma/(1+z)less than or similar to 0.06 at our nominal magnitude and redshift limits of I-AB=24 and z <= 1.3, respectively. We describe a new method to compute N(z) that incorporates the full redshift likelihood functions in a Bayesian iterative analysis, and we demonstrate in extensive Monte Carlo simulations that it is superior to distributions calculated using simple maximum likelihood redshifts. The field-to-field differences in the redshift distributions, while not unexpected theoretically, are substantial even on 300 scales. We provide I-AB and R-AB redshift distributions, median redshifts, and parameterized fits of our results in various magnitude ranges, accounting for both random and systematic errors in the analysis. C1 Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. ETH Honggerberg, ETH Zurich, Swiss Fed Inst Technol, Dept Phys, CH-8093 Zurich, Switzerland. Inst Astrophys Paris, F-75014 Paris, France. Lab Astrophys Marseille, F-13376 Marseille 12, France. Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Brodwin, M (reprint author), Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. RI Le Fevre, Olivier/G-7389-2011 NR 45 TC 22 Z9 22 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JAN PY 2006 VL 162 IS 1 BP 20 EP 37 DI 10.1086/497990 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009RS UT WOS:000235130700002 ER PT S AU Sparvoli, R Basili, A Bencardino, R Casolino, M De Pascale, MP Furano, G Menicucci, A Minori, M Morselli, A Picozza, P Wischnewski, R Bakaldin, A Galper, AM Koldashov, SV Korotkov, MG Mikhailov, VV Voronov, SA Yurkin, Y Adriani, O Bonechi, L Bongi, M Papini, P Ricciarini, SB Spillantini, P Straulino, S Taccetti, F Vannuccini, E Castellini, G Boezio, M Bonvicini, M Mocchiutti, E Schiavon, P Vacchi, A Zampa, G Zampa, N Carlson, P Lund, J Lundquist, J Orsi, S Pearce, M Barbarino, GC Campana, D Osteria, G Rossi, G Russo, S Boscherini, M Menn, W Simon, M Bongiorno, L Ricci, M Ambriola, M Bellotti, R Cafagna, F Circella, M De Marzo, C Giglietto, N Mirizzi, N Romita, M Spinelli, P Bogomolov, E Krutkov, S Vasiljev, G Bazilevskaja, GA Kvashnin, AN Logachev, VI Makhmutov, VS Maksumov, OS Stozhkov, YI Mitchell, JW Streitmatter, RE Stochaj, SJ AF Sparvoli, R. Basili, A. Bencardino, R. Casolino, M. De Pascale, M. P. Furano, G. Menicucci, A. Minori, M. Morselli, A. Picozza, P. Wischnewski, R. Bakaldin, A. Galper, A. M. Koldashov, S. V. Korotkov, M. G. Mikhailov, V. V. Voronov, S. A. Yurkin, Y. Adriani, O. Bonechi, L. Bongi, M. Papini, P. Ricciarini, S. B. Spillantini, P. Straulino, S. Taccetti, F. Vannuccini, E. Castellini, G. Boezio, M. Bonvicini, M. Mocchiutti, E. Schiavon, P. Vacchi, A. Zampa, G. Zampa, N. Carlson, P. Lund, J. Lundquist, J. Orsi, S. Pearce, M. Barbarino, G. C. Campana, D. Osteria, G. Rossi, G. Russo, S. Boscherini, M. Menn, W. Simon, M. Bongiorno, L. Ricci, M. Ambriola, M. Bellotti, R. Cafagna, F. Circella, M. De Marzo, C. Giglietto, N. Mirizzi, N. Romita, M. Spinelli, P. Bogomolov, E. Krutkov, S. Vasiljev, G. Bazilevskaja, G. A. Kvashnin, A. N. Logachev, V. I. Makhmutov, V. S. Maksumov, O. S. Stozhkov, Yu. I. Mitchell, J. W. Streitmatter, R. E. Stochaj, S. J. BE Battiston, R Shea, MA Rakowski, C Chatterjee, S TI Space qualification tests of the PAMELA instrument SO ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE cosmic antimatter; satellite experiment; magnetic spectrometer AB PAMELA is a satellite-borne experiment which will measure the antiparticle component of cosmic rays over an extended energy range and with unprecedented accuracy. The apparatus consists of a permanent magnetic spectrometer equipped with a double-sided silicon microstrip tracking system and surrounded by a scintillator anticoincidence system. A silicon-tungsten imaging calorimeter, complemented by a scintillator shower tail catcher, and a transition radiation detector perform the particle identification task. Fast scintillators are used for Time-of-Flight measurements and to provide the primary trigger. A neutron detector is finally provided to extend the range of particle measurements to the TeV region. PAMELA will fly on-board of the Resurs-DKI satellite, which will be put into a semi-polar orbit in 2005 by a Soyuz rocket. We give a brief review of the scientific issues of the mission and report about the status of the experiment few months before the launch. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Roma Tor Vergata, Ist Nazl Fis Nucl, I-00133 Rome, Italy. Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. Moscow Engn & Phys Inst, RU-115409 Moscow, Russia. Univ Florence, Ist Nazl Fis Nucl, I-50019 Florence, Italy. Univ Florence, Dept Phys, I-50019 Florence, Italy. Ist Fis Applicata Nello Carrara, I-50127 Florence, Italy. Univ Trieste, Dept Phys, I-34147 Trieste, Italy. Univ Trieste, Ist Nazl Fis Nucl, I-34147 Trieste, Italy. Albanova Univ Ctr, Royal Inst Technol, SE-10691 Stockholm, Sweden. Univ Naples Federico II, Dept Phys, I-80126 Naples, Italy. Univ Naples Federico II, Ist Nazl Fis Nucl, I-80126 Naples, Italy. Univ Siegen, D-57068 Siegen, Germany. Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Frascati, Italy. Univ Bari, Dept Phys, I-70126 Bari, Italy. Univ Bari, Ist Nazl Fis Nucl, I-70126 Bari, Italy. AF Ioffe Phys Tech Inst, RU-194021 St Petersburg, Russia. PN Lebedev Phys Inst, RU-119991 Moscow, Russia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. New Mexico State Univ, Las Cruces, NM 88003 USA. RP Sparvoli, R (reprint author), Univ Roma Tor Vergata, Ist Nazl Fis Nucl, Via Ric Sci 1, I-00133 Rome, Italy. EM roberta.sparvoli@roma2.infn.it RI Cafagna, Francesco/A-9299-2010; Morselli, Aldo/G-6769-2011; giglietto, nicola/I-8951-2012; Mocchiutti, Emiliano/I-8049-2013; Mikhailov, Vladimir/B-5368-2014; Vasilyev, Gennady/E-4843-2014; Krutkov, Sergey/E-7561-2014; Vacchi, Andrea/C-1291-2010; Barbarino, Giancarlo/L-2559-2015; Bongi, Massimo/L-9417-2015; Stozhkov, Yuri/M-7433-2015; Makhmutov, Vladimir/N-2086-2015; Galper, Arkady/M-9610-2015; Voronov, Sergey/P-9654-2016; Logachev, Valery/O-1190-2015; Kvashnin, Aleksandr/M-8673-2015; OI Cafagna, Francesco/0000-0002-7450-4784; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Mocchiutti, Emiliano/0000-0001-7856-551X; Mikhailov, Vladimir/0000-0003-3851-2901; Vacchi, Andrea/0000-0003-3855-5856; Barbarino, Giancarlo/0000-0001-9253-3397; Bongi, Massimo/0000-0002-6050-1937; Voronov, Sergey/0000-0002-9209-0618; Picozza, Piergiorgio/0000-0002-7986-3321; Papini, Paolo/0000-0003-4718-2895; Boezio, Mirko/0000-0002-8015-2981; Kvashnin, Aleksandr/0000-0001-7218-6738; Taccetti, Francesco/0000-0003-2657-2990; Bellotti, Roberto/0000-0003-3198-2708; casolino, marco/0000-0001-6067-5104; Ricciarini, Sergio Bruno/0000-0001-6176-3368; Castellini, Guido/0000-0002-0177-0643; Sparvoli, Roberta/0000-0002-6314-6117 NR 6 TC 2 Z9 3 U1 8 U2 15 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2006 VL 37 IS 10 BP 1841 EP 1847 DI 10.1016/j.asr.2005.05.100 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BES66 UT WOS:000239306500002 ER PT S AU Casolino, M Altamura, F Basili, A Bencardino, R De Pascale, MP Marcelli, L Minori, M Morselli, A Nagni, M Picozza, P Russo, S Sparvoli, R Ambriola, M Bellotti, R Cafagna, FS Circella, M De Marzo, C Giglietto, N Mirizzi, N Romita, M Spinelli, P Adriani, O Bonechi, L Bongi, M Papini, P Ricciarini, SB Spillantini, P Straulino, S Taccetti, F Vannuccini, E Castellini, G Bongiorno, L Ricci, M Mitchell, JW Streitmatter, RE Stochaj, SJ Bazilevskaya, GA Kvashnin, AN Logachev, VI Makhmutov, VS Maksumov, OS Stozhkov, YI Bakaldin, A Galper, AM Koldashov, SV Korotkov, MG Mikhailov, VV Voronov, SA Yurkin, Y Barbarino, GC Campana, D Osteria, G Rossi, G Russo, S Bogomolov, EA Krutkov, S Vasiljev, G Boscherini, M Menn, W Simon, M Carlson, P Lund, J Lundquist, J Orsi, S Pearce, M Boezio, M Bonvicini, V Mocchiutti, E Schiavon, P Vacchi, A Zampa, G Zampa, N AF Casolino, M. Altamura, F. Basili, A. Bencardino, R. De Pascale, M. P. Marcelli, L. Minori, M. Morselli, A. Nagni, M. Picozza, P. Russo, S. Sparvoli, R. Ambriola, M. Bellotti, R. Cafagna, F. S. Circella, M. De Marzo, C. Giglietto, N. Mirizzi, N. Romita, M. Spinelli, P. Adriani, O. Bonechi, L. Bongi, M. Papini, P. Ricciarini, S. B. Spillantini, P. Straulino, S. Taccetti, F. Vannuccini, E. Castellini, G. Bongiorno, L. Ricci, M. Mitchell, J. W. Streitmatter, R. E. Stochaj, S. J. Bazilevskaya, G. A. Kvashnin, A. N. Logachev, V. I. Makhmutov, V. S. Maksumov, O. S. Stozhkov, Y. I. Bakaldin, A. Galper, A. M. Koldashov, S. V. Korotkov, M. G. Mikhailov, V. V. Voronov, S. A. Yurkin, Y. Barbarino, G. C. Campana, D. Osteria, G. Rossi, G. Russo, S. Bogomolov, E. A. Krutkov, S. Vasiljev, G. Boscherini, M. Menn, W. Simon, M. Carlson, P. Lund, J. Lundquist, J. Orsi, S. Pearce, M. Boezio, M. Bonvicini, V. Mocchiutti, E. Schiavon, P. Vacchi, A. Zampa, G. Zampa, N. BE Battiston, R Shea, MA Rakowski, C Chatterjee, S TI Cosmic-ray observations of the heliosphere with the PAMELA experiment SO ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE cosmic rays; satellite-borne experiment; solar wind; solar energetic particles; jovian particles ID ELECTRONS AB The PAMELA experiment is a multi-purpose apparatus built around a permanent magnet spectrometer, with the main goal of studying in detail the antiparticle component of cosmic rays. The apparatus will be carried in space by means of a Russian satellite, due to launch in 2005, for a three year-long mission. The characteristics of the detectors composing the instrument, alongside the long lifetime of the mission and the orbital characteristics of the satellite, will allow to address several items of cosmic-ray physics. In this paper, we will focus on the solar and heliospheric observation capabilities of PAMELA. (c) 2005 Published by Elsevier Ltd on behalf of COSPAR. C1 Univ Roma Tor Vergata, Ist Nazl Fis Nucl, I-00133 Rome, Italy. Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. Univ Bari, Dept Phys, I-70126 Bari, Italy. Univ Bari, Ist Nazl Fis Nucl, I-70126 Bari, Italy. Univ Florence, Dept Phys, I-50019 Sesto Fiorentino, Italy. Univ Florence, Ist Nazl Fis Nucl, I-50019 Sesto Fiorentino, Italy. CNR, Ist Fis Applicata, I-50127 Florence, Italy. Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Frascati, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. New Mexico State Univ, PAL, Las Cruces, NM 88003 USA. PN Lebedev Phys Inst, RU-119991 Moscow, Russia. Moscow Engn & Phys Inst, RU-115409 Moscow, Russia. Univ Naples Federico II, Dept Phys, I-80126 Naples, Italy. Univ Naples Federico II, Ist Nazl Fis Nucl, I-80126 Naples, Italy. AF Ioffe Phys Tech Inst, RU-194021 St Petersburg, Russia. Univ Siegen, D-57068 Siegen, Germany. Royal Inst Technol, SE-10691 Stockholm, Sweden. Univ Trieste, Dept Phys, I-34147 Trieste, Italy. Univ Trieste, Ist Nazl Fis Nucl, I-34147 Trieste, Italy. RP Casolino, M (reprint author), Univ Roma Tor Vergata, Ist Nazl Fis Nucl, I-00133 Rome, Italy. EM Marco.Casolino@roma2.infh.it RI Morselli, Aldo/G-6769-2011; giglietto, nicola/I-8951-2012; Cafagna, Francesco/A-9299-2010; Mocchiutti, Emiliano/I-8049-2013; Mikhailov, Vladimir/B-5368-2014; Vasilyev, Gennady/E-4843-2014; Krutkov, Sergey/E-7561-2014; Vacchi, Andrea/C-1291-2010; Barbarino, Giancarlo/L-2559-2015; Bongi, Massimo/L-9417-2015; Bazilevskaya, Galina/M-6175-2015; Stozhkov, Yuri/M-7433-2015; Makhmutov, Vladimir/N-2086-2015; Galper, Arkady/M-9610-2015; marcelli, laura/K-8860-2016; Voronov, Sergey/P-9654-2016; Logachev, Valery/O-1190-2015; Kvashnin, Aleksandr/M-8673-2015; OI Sparvoli, Roberta/0000-0002-6314-6117; Picozza, Piergiorgio/0000-0002-7986-3321; Papini, Paolo/0000-0003-4718-2895; Boezio, Mirko/0000-0002-8015-2981; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Cafagna, Francesco/0000-0002-7450-4784; Mocchiutti, Emiliano/0000-0001-7856-551X; Mikhailov, Vladimir/0000-0003-3851-2901; Vacchi, Andrea/0000-0003-3855-5856; Barbarino, Giancarlo/0000-0001-9253-3397; Bongi, Massimo/0000-0002-6050-1937; marcelli, laura/0000-0002-3180-1228; Voronov, Sergey/0000-0002-9209-0618; Kvashnin, Aleksandr/0000-0001-7218-6738; Taccetti, Francesco/0000-0003-2657-2990; Bellotti, Roberto/0000-0003-3198-2708; casolino, marco/0000-0001-6067-5104; Ricciarini, Sergio Bruno/0000-0001-6176-3368; Castellini, Guido/0000-0002-0177-0643 NR 16 TC 5 Z9 5 U1 8 U2 12 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2006 VL 37 IS 10 BP 1848 EP 1852 DI 10.1016/j.asr.2005.06.035 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BES66 UT WOS:000239306500003 ER PT S AU Banerdt, WB Chui, T Herrin, ET Rosenbaum, D Teplitz, VL AF Banerdt, W. Bruce Chui, Talso Herrin, Eugene T. Rosenbaum, Doris Teplitz, Vigdor L. BE Battiston, R Shea, MA Rakowski, C Chatterjee, S TI Lunar seismic search for strange quark matter SO ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE strange quark matter; moon; seismic detection ID SEISMOGRAPHIC STATION REPORTS; UNEXPLAINED SETS; NUGGET PASSAGE; NUCLEARITES; CONSISTENT; STAR AB It was pointed out in 1984 by Witten that strange quark matter (SQM) - matter made of up, down, and strange quarks (rather than just up and down, as are protons and neutrons) - might well be stable and the lowest energy state of matter. The reason is that it would be electrically neutral and have less Pauli-Principle repulsion. Binding would increase with numbers of quarks, and might not begin below thousands. It would have nuclear density. Neutron stars would be strange quark stars; and it might conceivably constitute dark matter. One way to detect ton-range SQM nuggets (SQNs) would be from seismic signals they would make passing through the Earth. We give a rough estimate on the relative advantage of attempting to detect SQNs on the Moon over Earth (about 50 times more detections). (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Low Temp Sci & Quantum Sensors Grp, Pasadena, CA 91109 USA. So Methodist Univ, Dept Geol, Dallas, TX 75275 USA. So Methodist Univ, Dept Phys, Dallas, TX 75275 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Chui, T (reprint author), CALTECH, Jet Prop Lab, Low Temp Sci & Quantum Sensors Grp, 4800 Oak Grove Dr,Mail Stop 79-24, Pasadena, CA 91109 USA. EM talso.c.chui@jpl.nasa.gov; Vigdor.L.Teplitz@nasa.gov NR 19 TC 9 Z9 10 U1 0 U2 1 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2006 VL 37 IS 10 BP 1889 EP 1893 DI 10.1016/j.asr.2005.06.034 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BES66 UT WOS:000239306500010 ER PT S AU Ptuskin, VS Jones, FC Seo, ES Sina, R AF Ptuskin, V. S. Jones, F. C. Seo, E. S. Sina, R. BE Battiston, R Shea, MA Rakowski, C Chatterjee, S TI Effect of random nature of cosmic ray sources - Supernova remnants - on cosmic ray intensity fluctuations, anisotropy, and electron energy spectrum SO ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE cosmic rays; supernova remnants AB The random nature of sources (the supernova remnants) leads to the fluctuations of cosmic ray intensity in space and time. We calculate the expected fluctuations in a flat-halo diffusion model for particles with energies from 0.1 to 10(3) TeV. The data on energy spectra and anisotropy of very high energy protons, nuclei and electrons, and the astronomical data on supernova remnants, the potential sources of cosmic rays, are used to constrain the value of the cosmic-ray diffusion coefficient and its dependence on energy. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 IZMIRAN, Inst Terr Magnetism Ionosphere & Radiowave Propag, Lab Astrophys Res, Moscow 142190, Russia. Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Ptuskin, VS (reprint author), IZMIRAN, Inst Terr Magnetism Ionosphere & Radiowave Propag, Lab Astrophys Res, Moscow 142190, Russia. EM vptuskin@hotmail.com OI Seo, Eun-Suk/0000-0001-8682-805X NR 16 TC 46 Z9 46 U1 0 U2 2 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 37 IS 10 BP 1909 EP 1912 DI 10.1016/j.asr.2005.08.036 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BES66 UT WOS:000239306500013 ER PT S AU Panov, AD Adams, JH Ahn, HS Bashindzhagyan, GL Batkov, KE Chang, J Christl, M Fazely, AR Ganel, O Gunasingha, RM Guzik, TG Isbert, J Kim, KC Kouznetsov, EN Panasyuk, MI Schmidt, WKH Seo, ES Sokolskaya, NV Wefel, JP Wu, J Zatsepin, VI AF Panov, A. D. Adams, J. H., Jr. Ahn, H. S. Bashindzhagyan, G. L. Batkov, K. E. Chang, J. Christl, M. Fazely, A. R. Ganel, O. Gunasingha, R. M. Guzik, T. G. Isbert, J. Kim, K. C. Kouznetsov, E. N. Panasyuk, M. I. Schmidt, W. K. H. Seo, E. S. Sokolskaya, N. V. Wefel, J. P. Wu, J. Zatsepin, V. I. BE Battiston, R Shea, MA Rakowski, C Chatterjee, S TI The energy spectra of heavy nuclei measured by the ATIC experiment SO ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE cosmic rays; heavy nuclei; energy spectra; propagation models ID CHARGE DETECTOR; SILICON MATRIX AB The preliminary energy spectra of heavy nuclei C, O, Ne, Mg, Si, and Fe in the primary cosmic rays measured by the ATIC-2 experiment are presented and compared to previous data and to propagation models. Using previous data to extend the ATIC-2 results for all heavy nuclei to higher energy, the combined spectra can be best fit with diffusion model with weak reacceleration and scattering on random magnetic field with a Kolmogorov spectrum fluctuations becoming dominant at high energy. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 119992, Russia. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. Max Planck Inst Aeron, D-37191 Katlenburg Lindau, Germany. Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. RP Panov, AD (reprint author), Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 119992, Russia. EM panov@decl.sinp.msu.ru RI Panasyuk, Mikhail/E-2005-2012; Zatsepin, Victor/J-2287-2012; Sokolskaya, Natalia/J-4609-2012; Panov, Alexander/K-3952-2012; OI Panov, Alexander/0000-0003-2290-6498; Seo, Eun-Suk/0000-0001-8682-805X NR 15 TC 18 Z9 19 U1 0 U2 3 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 37 IS 10 BP 1944 EP 1949 DI 10.1016/j.asr.2005.07.040 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BES66 UT WOS:000239306500020 ER PT S AU Ahn, HS Seo, ES Adams, JH Bashindzhagyan, G Batkov, KE Chang, J Christl, M Fazely, AR Ganel, O Gunasingha, RM Guzik, TG Isbert, J Kim, KC Kouznetsov, E Panasyuk, M Panov, A Schmidt, WKH Sina, R Sokolskaya, NV Wang, JZ Wefel, JP Wu, J Zatsepin, V AF Ahn, H. S. Seo, E. S. Adams, J. H. Bashindzhagyan, G. Batkov, K. E. Chang, J. Christl, M. Fazely, A. R. Ganel, O. Gunasingha, R. M. Guzik, T. G. Isbert, J. Kim, K. C. Kouznetsov, E. Panasyuk, M. Panov, A. Schmidt, W. K. H. Sina, R. Sokolskaya, N. V. Wang, J. Z. Wefel, J. P. Wu, J. Zatsepin, V. BE Battiston, R Shea, MA Rakowski, C Chatterjee, S TI The energy spectra of protons and helium measured with the ATIC experiment SO ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE balloon; cosmic rays; composition; energy spectra ID COSMIC-RAY PROTON; BALLOON EXPERIMENT; SPECTROMETER AB The Advanced Thin Ionization Calorimeter (ATIC) balloon experiment is designed to investigate the composition and energy spectra of cosmic rays at the highest energies currently accessible by direct measurements, i.e., the region up to 100 TeV. The instrument consists of a silicon matrix for charge measurement, a graphite target (0.75 nuclear interaction length) to induce hadronic interactions, three layers of scintillator strip hodoscopes for triggering and trajectory reconstruction, and a Bismuth Germanate (BGO) crystal calorimeter (18 radiation lengths) to measure particle energies. ATIC has had two successful Long Duration Balloon (LDB) flights from McMurdo, Antarctica: one from 12/28/00 to 01/13/01 and the other from 12/29/02 to 01/18/03. We present the energy spectra of protons and helium extracted from the first flight, over the energy range from 100 GeV to 100 TeV, and compare them with the results from other experiments at both the lower and higher energies. ATIC-I results do not indicate significant differences in spectral shape between protons and helium over the investigated energy range. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Maryland, Inst Phys Sci & Technol, CSS, College Pk, MD 20742 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 119899, Russia. Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. Southern Univ, Dept Phys, Baton Rouge, LA USA. Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. RP Ahn, HS (reprint author), Univ Maryland, Inst Phys Sci & Technol, CSS, Bldg 224, College Pk, MD 20742 USA. EM hsahn@cosmicray.umd.edu RI Panasyuk, Mikhail/E-2005-2012; Zatsepin, Victor/J-2287-2012; Panov, Alexander/K-3952-2012; OI Panov, Alexander/0000-0003-2290-6498; Seo, Eun-Suk/0000-0001-8682-805X NR 20 TC 15 Z9 16 U1 0 U2 5 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2006 VL 37 IS 10 BP 1950 EP 1954 DI 10.1016/j.asr.2005.09.031 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BES66 UT WOS:000239306500021 ER PT S AU Geier, S Barbier, LM Binns, WR Christian, ER Cummings, JR deNolfo, GA Hink, PL Israel, MH Labrador, AW Link, JT Mewaldt, RA Mitchell, JW Rauch, BF Schindler, SM Scott, LM Stone, EC Streitmatter, RE Waddington, CJ AF Geier, S. Barbier, L. M. Binns, W. R. Christian, E. R. Cummings, J. R. deNolfo, G. A. Hink, P. L. Israel, M. H. Labrador, A. W. Link, J. T. Mewaldt, R. A. Mitchell, J. W. Rauch, B. F. Schindler, S. M. Scott, L. M. Stone, E. C. Streitmatter, R. E. Waddington, C. J. BE Battiston, R Shea, MA Rakowski, C Chatterjee, S TI A search for the signature of microquasars in the cosmic ray iron spectrum measured by TIGER SO ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE cosmic rays; microquasars ID SUPERNOVA-REMNANTS; SOLAR MODULATION; RATIO AB In a recent paper Heinz and Sunyaev suggest that relativistic jets observed in microquasars might result in narrow features in the energy spectra of heavy cosmic rays with approximate to 1 to approximate to 10 GeV/nuc. They further argue that such features might be observable if there has been one or more microquasars nearby within the last few million years. We report preliminary results of a search for evidence of such features using data from a 32-day balloon flight of the Trans-Iron Galactic Element Recorder (TIGER). Although this flight took place near solar maximum, calculations of the broadening effects of solar modulation indicate that a narrow feature of sufficient intensity should still be observable. An energy spectrum for iron with high statistical significance has been derived from 100,000 Fe events in the energy range from about 2.5 to 10 GeV/nuc. Although our preliminary results do not reveal any obvious features, we will discuss the possibility of observing such features with TIGER and other instruments. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 CALTECH, Pasadena, CA 91125 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Washington Univ, St Louis, MO 63130 USA. Univ Minnesota, Tate Lab Phys, Minneapolis, MN 55455 USA. RP Geier, S (reprint author), CALTECH, 1200 California Blvd,MC 220-77, Pasadena, CA 91125 USA. EM sgeier@caltech.edu RI de Nolfo, Georgia/E-1500-2012; Christian, Eric/D-4974-2012 OI Christian, Eric/0000-0003-2134-3937 NR 8 TC 2 Z9 2 U1 0 U2 2 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2006 VL 37 IS 10 BP 1955 EP 1959 DI 10.1016/j.asr.2005.10.037 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BES66 UT WOS:000239306500022 ER PT J AU Lorenzini, E Bombardelli, C Cosmo, M Harwit, M Leisawitz, D Farley, R Rinehart, S Quinn, D Miller, D AF Lorenzini, Enrico Bombardelli, Claudio Cosmo, Mario Harwit, Martin Leisawitz, David Farley, Rodger Rinehart, Stephen Quinn, David Miller, David TI Far-infrared/submillimeter astronomical interferometry with spaceborne tether formations SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE instrumentation : miscellaneous; space vehicles : miscellaneous; techniques : miscellaneous; astronomical data bases : miscellaneous ID PROBE WMAP OBSERVATIONS; 1ST STARS; SYSTEM; EMISSION; DYNAMICS AB Through the continuing development of improved detectors and detector arrays, far-infrared/submillimeter astronomical space missions have had enormous successes in recent years. Despite these advances, the diffraction-limited angular resolving power has remained virtually constant. The advent of telescopes with apertures of several meters will improve this capability, but will still leave image resolution many orders of magnitude poorer than in most other spectral ranges. Here we point out that the only foreseeable way to improve image quality to rival that of modem optical telescopes will be with interferometers whose light collectors are connected by tethers. After making the scientific case for high spatial resolution far-infrared/submillimeter imaging and the use of interferometry as the most immediate way of producing results, we discuss recent advances in dynamic analysis and control of tethered formations, and argue that the further development and testing of tethers in space is a first step toward providing improved far-infrared/submillimeter angular resolution and astronomical image quality. C1 Cornell Univ, Ithaca, NY USA. Univ Padua, Dept Engn Mech, Padua, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. MIT, Cambridge, MA 02139 USA. RP Harwit, M (reprint author), 511 H St SW, Washington, DC 20024 USA. EM harwit@verizon.net NR 28 TC 10 Z9 10 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2006 VL 302 IS 1-4 BP 225 EP 239 DI 10.1007/s10509-006-9038-7 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 074VP UT WOS:000239840200027 ER PT J AU Cosmovici, CB Bratina, V Schwarz, G Tozzi, G Mumma, MJ Stalio, R AF Cosmovici, CB Bratina, V Schwarz, G Tozzi, G Mumma, MJ Stalio, R TI Comet Hale-Bopp (C/1995 O1): UVSTAR-FUV spectroscopy from the space shuttle SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE Comet Hale-Bopp; space shuttle; FUV spectroscopy; airglow ID X-RAYS; POSTPERIHELION; TELESCOPE; HYAKUTAKE; ABUNDANCE; SEARCH; AUSTIN; ARGON AB We report here on unique post-perihelion (2.3 AU) measurements of Comet Hale-Bopp in the FUV-range (950-1250 angstrom) by means of the UVSTAR spectrometer from the space shuttle with the main purpose of searching for argon and other FUV emitters. New methods for separating the strong airglow emission at shuttle altitudes are here discussed in detail. Due to our low resolution (15 angstrom) and S/N ratio the possible rocket-borne detection of argon near perihelion (0.9 AU) could not be confirmed. New species as N-2 are suspected but difficult to separate from the strong airglow emission at shuttle altitudes. From the Ly alpha brightness (1.30 +/- 0.08 kRy) a water production rate Q = 5.9 +/- 0.4 x 10(29) molecules s(-1) could be derived and compared with other post-perihelion observations. C1 INAF, Ist Fis Spazio Interplanetario, Rome, Italy. CARSO, Area Ric, Trieste, Italy. DLR, D-82230 Oberpfaffenhofen, Germany. Osservatorio Arcetri, Florence, Italy. NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. RP Cosmovici, CB (reprint author), INAF, Ist Fis Spazio Interplanetario, 100 Fosso Cavaliere, Rome, Italy. EM cosmo@ifsi.rm.cnr.it RI mumma, michael/I-2764-2013; OI Tozzi, Gian Paolo/0000-0003-4775-5788 NR 20 TC 0 Z9 0 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD JAN PY 2006 VL 301 IS 1-4 BP 135 EP 143 DI 10.1007/s10509-006-0180-z PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 011CU UT WOS:000235246200018 ER PT B AU Moos, HW Sonneborn, G AF Moos, H. W. Sonneborn, G. BE Sonneborn, G Moos, HW Andersson, BG TI A brief history of the FUSE mission SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria AB A brief history of the FUSE mission is given from the point of view of two participants, the Principal Investigator and the NASA Project Scientist. C1 [Moos, H. W.] Johns Hopkins Univ, 3400 N Charles St, Baltimore, MD 21218 USA. [Sonneborn, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Moos, HW (reprint author), Johns Hopkins Univ, 3400 N Charles St, Baltimore, MD 21218 USA. EM hwm@jhu.edu; George.sonneborn-1@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 4 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300001 ER PT B AU Massa, D Fullerton, AW Prinja, RK AF Massa, D. Fullerton, A. W. Prinja, R. K. BE Sonneborn, G Moos, HW Andersson, BG TI PV and the mass loss discrepancy in O stars SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID STELLAR; WINDS AB Building upon a previous analysis of P v wind lines in LMC O stars, we analyze the P v wind lines in a sample of Galactic O stars which have empirical mass loss rates determined from either their radio fluxes or Ha profiles. Since the wind analysis provides a measure of A q where q is the ionization fraction of the ion, we determine q(P v) observationally. In spite of model predictions that, q similar to 1 for mid-O stars, we find q(P v) <= 0.15 throughout the O stars. We discuss the origin of this discrepancy. C1 [Massa, D.] NASA, Goddard Space Flight Ctr, SGT Inc, Code 665, Greenbelt, MD 20901 USA. [Fullerton, A. W.] Univ Victoria, Victoria, BC V8W 2Y2, Canada. [Fullerton, A. W.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Prinja, R. K.] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Massa, D (reprint author), NASA, Goddard Space Flight Ctr, SGT Inc, Code 665, Greenbelt, MD 20901 USA. EM massa@taotaomona.gsfc.nasa.gov; awf@pha.jhu.edu NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 118 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300019 ER PT B AU Blair, WP Sankrit, R Hoopes, C Fullerton, AW Danforth, CW Sembach, KR Walborn, N Chu, YH Howk, JC Welty, D Massa, D Staveley-Smith, L Crowther, P AF Blair, W. P. Sankrit, R. Hoopes, C. Fullerton, A. W. Danforth, C. W. Sembach, K. R. Walborn, N. Chu, Y. -H. Howk, J. C. Welty, D. Massa, D. Staveley-Smith, L. Crowther, P. BE Sonneborn, G Moos, HW Andersson, BG TI The FUSE legacy in the Magellanic Clouds SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID INTERSTELLAR OVI; ATLAS AB We have embarked on a two-year FUSE Legacy program to obtain spectra of 45 additional key sight lines to stars in both the Large and Small Magellanic Clouds. The new sight lines have been selected to address scientific goals pertaining to both interstellar medium and stellar programs, building oil the large body of existing MC data in meaningful ways. Our team is also committed to producing a set of standardized products not only for these new sight lilies but for all useful MC stellar sight lilies obtained previously with FUSE. These standardized products will be made available through the MAST High-Level Science Products program. We present a brief outline of our plans for these products. C1 [Blair, W. P.; Sankrit, R.; Hoopes, C.; Fullerton, A. W.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. [Danforth, C. W.] Univ Colorado, Boulder, CO 80309 USA. [Sembach, K. R.; Walborn, N.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Chu, Y. -H.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Howk, J. C.] Univ Calif San Diego, La Jolla, CA 92093 USA. [Welty, D.] Univ Chicago, Chicago, IL 60637 USA. [Massa, D.] NASA, Goddard Space Flight Ctr, SGT Inc, Greenbelt, MD 20771 USA. [Staveley-Smith, L.] CSIRO, Australia Telescope Compact Array, Melbourne, Vic 3001, Australia. [Crowther, P.] Univ Sheffield, Sheffield S3 7RH, S Yorkshire, England. RP Blair, WP (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM wpb@pha.jhu.edu; ravi@pha.jhu.edu; choopes@pha.jhu.edu; awf@pha.jhu.edu; danforth@pha.jhu.edu; sembach@stsci.edu; howk@ucsd.edu RI Staveley-Smith, Lister/A-1683-2011 OI Staveley-Smith, Lister/0000-0002-8057-0294 FU NASA [NAG-513704] FX This work is supported by NASA grants NAG-513704 and a grant in preparation for Cycle 5 FUSE program E511, both to the Johns Hopkins University. NR 8 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 127 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300022 ER PT B AU Fullerton, AW Massa, DL Prinja, RK Howarth, ID Willis, AJ Owocki, SP AF Fullerton, A. W. Massa, D. L. Prinja, R. K. Howarth, I. D. Willis, A. J. Owocki, S. P. BE Sonneborn, G Moos, HW Andersson, BG TI FUSE observations of variability in hot-star winds SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria AB New constraints on the large-scale wind structures responsible for discrete absorption components are obtained from far-ultraviolet time-series observations of O supergiants in the Large Magellanic Cloud. C1 [Fullerton, A. W.] Univ Victoria, Dept Phys & Astron, POB 3055, Victoria, BC V8W 3P6, Canada. [Massa, D. L.] NASA, Goddard Space Flight Ctr, SGT Inc, Greenbelt, MD 20771 USA. [Prinja, R. K.; Howarth, I. D.; Willis, A. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Owocki, S. P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. RP Fullerton, AW (reprint author), Univ Victoria, Dept Phys & Astron, POB 3055, Victoria, BC V8W 3P6, Canada. EM awf@pha.jhu.edu; massa@taotaomona.gsfc.nasa.gov; ajw@star.ucl.ac.uk FU NASA [NAG-32985] FX The NASACNESCSA Far Ultraviolet Spectroscopic Explorer is operated by the Johns Hopkins University for NASA under contract NAG-32985. NR 2 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 130 EP 132 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300023 ER PT B AU Iping, RC Sonneborn, G Cull, TR AF Iping, R. C. Sonneborn, G. Cull, T. R. BE Sonneborn, G Moos, HW Andersson, BG TI FUSE observations of eta carinae SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID EVENT AB eta Carinae was observed by FUSE through the LWRS (30"x30") and HIRS (1.25"x20") apertures in March and April 2004. There are significant differences between the two spectra. About half of the LWRS flux appears to be due to two B-type stars near the edge of the LWRS aperture, 14" from eta Car. The HIRS spectrum (LiF1 channel) therefore reveals the intrinsic FUV spectrum of eta Car without this stellar contamination. The HIRS spectrum contains strong interstellar H-2 having high rotational excitation (up to J = 8). Most of the atomic species with prominent ISM features (C II, Fe II, Ar I, P II, etc) also have strong blue-shifted absorption to v similar to -580 km/s that is associated with expanding debris from the 1840 eruption. C1 [Iping, R. C.; Sonneborn, G.; Cull, T. R.] NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. RP Iping, RC (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. EM Rosina.C.iping.1@gsfc.nasa.gov; George.sonneborn-1@nasa.gov RI Gull, Theodore/D-2753-2012 OI Gull, Theodore/0000-0002-6851-5380 NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 133 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300024 ER PT B AU Rauch, T Reiff, E Werner, K Herwig, F Koesterke, L Kruk, JW AF Rauch, T. Reiff, E. Werner, K. Herwig, F. Koesterke, L. Kruk, J. W. BE Sonneborn, G Moos, HW Andersson, BG TI On the evolutionary status of extremely hot helium stars - are O(He) stars successors of RCrB stars? SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID POST-AGB STARS; PLANETARY-NEBULAE; WINDS AB 95% of all stars end their lives as white dwarfs. About 20% of the hot post-AGB stars are hydrogen deficient. Most of these are the result of a late helium-shell flash, but the evolutionary status of a fraction of about 10-20% of the hottest hydrogen-deficient stars, namely four O(He) stars, is as yet unexplained. They could be the long-searched hot successors of RCrB stars, which have not been identified up to now. If this turns out to be true, then a third post-AGB evolutionary sequence is revealed, which is probably the result of a double degenerate merging process. More generally, understanding details of merging double degenerate stars is of interest in the context of SN Ia events and hence cosmology. C1 [Rauch, T.] Dr Remeis Sternwarte, D-96049 Bamberg, Germany. [Rauch, T.; Reiff, E.] Inst Astron & Astrohys, D-72076 Tubingen, Germany. [Herwig, F.] Los Alamos Natl Lab, Los Alamos, NM USA. [Koesterke, L.] Goddard Space Flight Ctr, Greenbelt, MD USA. [Kruk, J. W.] Johns Hopkins Univ, Baltimore, MD USA. RP Rauch, T (reprint author), Dr Remeis Sternwarte, D-96049 Bamberg, Germany. EM Thomas.Rauch@sternwarte.uni-erlangen.de; werner@astro.uni-tuebingen.de; kruk@pha.jhu.edu RI Kruk, Jeffrey/G-4047-2012 NR 8 TC 9 Z9 9 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 194 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300037 ER PT B AU Dixon, WV Brown, TM Howk, JC Landsman, WB AF Dixon, W. V. Brown, T. M. Howk, J. C. Landsman, W. B. BE Sonneborn, G Moos, HW Andersson, BG TI Does the line of sight to M5 intersect a highly-ionized high-velocity cloud? SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID GAS AB FUSE and HST/STIS observations of the post-asymptotic giant branch (PACB) star ZNG 1 in the globular cluster M5 (NGC 5904) reveal high-velocity absorption in O VI, C IV, Si IV, and other species. With LSR velocities between -150 and -100 km s(-1), this complex of absorbing components is blue-shifted by roughly -180 km s(-1) relative to the stellar photosphere. The absorption represents either circumstellar material (e.g., gas ejected during the star's AGB phase and now shock-heated by the fast PAGB wind) or a high-ionization high-velocity cloud (HVC) along the line of sight to M5. If the latter, it would be the first evidence that highly-ionized HVCs may be found near the Galactic disk. C1 [Dixon, W. V.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. [Brown, T. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howk, J. C.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Landsman, W. B.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. RP Dixon, WV (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM wvd@pha.jhu.edu; ab@casa.colorado.edu; howk@ucsd.edu NR 5 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 218 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300045 ER PT B AU Iping, RC Sonneborn, G Kaper, L Hammerschlag-Hensberge, G AF Iping, R. C. Sonneborn, G. Kaper, L. Hammerschlag-Hensberge, G. BE Sonneborn, G Moos, HW Andersson, BG TI Phase-dependent changes in the wind lines in the HMXRBs SMC X-1 and 4UI700-37 SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria AB The High Mass X-ray Binaries (HMXRB's) SMC X-1 and 4U170037 have been observed with FUSE to study the effect of the X-ray source on the stellar wind of the primary. In both systems phase dependent changes in the wind lines have been observed, indicating the creation of a X-ray ionization zone in the stellar wind. The high X-ray luminosity of SMC X-1 ionizes much of the wind and leaves a Stromgren zone. This disrupts the resonance-line acceleration of the wind in portions of the orbit, quencing the wind and disrupting the mass flow. A similar but less dramatic effect was found for the first time in 4UI700-37. This so-called Hatchett-McCray (HM) effect had been predicted for 4UI700-37, but was not previously detected. C1 [Iping, R. C.; Sonneborn, G.] NASA, Goddard Space Flight Ctr, Code 681, Greenbelt, MD 20771 USA. [Kaper, L.; Hammerschlag-Hensberge, G.] Univ Amsterdam, NL-1098 SJ Amsterdam, Netherlands. RP Iping, RC (reprint author), NASA, Goddard Space Flight Ctr, Code 681, Greenbelt, MD 20771 USA. EM Rosina.C.iping.1@gsfc.nasa.gov; George.sonneborn-1@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 263 EP 265 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300057 ER PT B AU Grady, CA Williger, GM Bouret, JC Roberge, A Sahu, M Woodgate, BE AF Grady, C. A. Williger, Gerard M. Bouret, Jean-Claude Roberge, Aki Sahu, Meena Woodgate, Bruce E. BE Sonneborn, G Moos, HW Andersson, BG TI The evolution of planetary systems: FUSEs view of the first 20-30 Myr SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID HERBIG-AE/BE STARS; T-TAURI STARS; MAIN-SEQUENCE STARS; FALLING EVAPORATING BODIES; FLUORESCENT H-2 EMISSION; FAR-ULTRAVIOLET SPECTRUM; INTERMEDIATE-MASS STARS; HUBBLE-SPACE-TELESCOPE; CIRCUMSTELLAR GAS; BETA-PICTORIS AB We review the contribution of FUV spectroscopy in furthering our understanding of planetary system evolution over the first 20-30 Myr. In tandem with high spatial resolution imagery of circumstellar disks, secure dating of young stars, and IR. and x-ray data, FUSE has established that the disks around stars with 0.7 <= M <= 2.5 M-circle dot evolve on similar timescales and in the same way. FUSE has unequivocably demonstrated that Herbig Ae stars closely resemble T Tauri stars while actively accreting. Absorption-line studies of ZAMS A stars have revealed the presence of planetesimals in the disks, including icy bodies up to 20 AU from the star. Most importantly, FUSE constrains the epoch of gaseous giant planet formation to be <= 12 Myr both for A stars and for M stars. With the recognition, and dating of additional debris disks in our immediate vicinity, FUSE is poised to extend these studies to additional intermediate-mass stars and to nearby, post-T Tauri stars. C1 [Grady, C. A.] Eureka Sci, Greenbelt, MD 20771 USA. [Grady, C. A.] GSFC, Greenbelt, MD 20771 USA. [Williger, Gerard M.] Johns Hopkins Univ Hosp, Baltimore, MD 21287 USA. [Bouret, Jean-Claude] Astrophys Lab, Marseille, France. [Roberge, Aki] Carnegie Inst Sci, DTM, Washington, DC USA. [Sahu, Meena] Goddard Space Flight Ctr, JWST Project, Greenbelt, MD 20771 USA. [Woodgate, Bruce E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Grady, CA (reprint author), Eureka Sci, Greenbelt, MD 20771 USA. EM cgrady@echelle.gsfc.nasa.gov; williger@pha.jhu.edu; Jean-Claude.Bouret@oamp.fr; akir@dtm.ciw.edu RI Roberge, Aki/D-2782-2012; Woodgate, Bruce/D-2970-2012 OI Roberge, Aki/0000-0002-2989-3725; NR 60 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 281 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300062 ER PT B AU Dinerstein, HL Sterling, NC Bowers, CW AF Dinerstein, H. L. Sterling, N. C. Bowers, C. W. BE Sonneborn, G Moos, HW Andersson, BG TI Absorption-line spectroscopy of planetary nebulae with FUSE: Probing the molecular, atomic, and ionized gas SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID PHOTODISSOCIATION REGIONS; EXCITATION; HYDROGEN AB The central stars of planetary nebulae (PNe) are natural targets for FUSE due to their UV brightness. The FUSE spectra of many PNe show absorption features due to circumstellar material in species ranging from H-2 and neutrals in the photodissociation region (PDR) to ions resident in the H II region. We report results from a program designed to search for nebular components in the H-2 Lyman and Werner resonance lines that are responsible for the fluorescent excitation of H-2 in strong FUV radiation fields. Our failure to detect H-2 in absorption in several PNe with strong near-infrared H-2 emission indicates that the molecular material has an asymmetrical or clumpy distribution. We also detect enrichments in the s-process product Ge, find that Fe is not depleted into dust along at least one line of sight through a PN, and show that starlight fluorescence can affect the populations of the excited fine-structure levels of O I. C1 [Dinerstein, H. L.; Sterling, N. C.] Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. [Bowers, C. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Dinerstein, HL (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. EM harriet@astro.as.utexas.edu FU FUSE project; NASA Goddard Space Flight Center through data analysis [NAG 5-9239, 5-11597, 5-12731] FX We thank the operations and user-support staff of the FUSE project for all their help in planning and executing this observing program. Support for this research was provided by NASA Goddard Space Flight Center through data analysis grants NAG 5-9239, 5-11597, and 5-12731. NR 10 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 328 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300072 ER PT B AU Wannier, PG Andersson, BG Sonneborn, G AF Wannier, P. G. Andersson, B-G Sonneborn, G. BE Sonneborn, G Moos, HW Andersson, BG TI Gas on the QSO 0045+3926 sightline: High-velocity features in our local group SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID HYDROGEN; HALO; M31 AB The QSO 0045+3926 (10 And) sightline is an intriguing one for studying high-velocity gas in our Local Group, and it also yields information about more distant, extra-galactic material. Exploratory FUSE observations (8 ksec, Cycle 2) revealed four components: a local Galactic one, two red-shifted ones associated with the quasar, and one blue-shifted component originating within our Local Group. Additional data clarify these early results, providing better column densities, and revealing a pair of additional components probably arising in or near another intervening galaxy. Additional Cycle 4 observations, eventually totaling 200 ksec, have yet to be obtained. C1 [Wannier, P. G.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Andersson, B-G] Johns Hopkins Univ, CAS, Baltimore, MD 21218 USA. [Andersson, B-G] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wannier, PG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM peter.wannier@jpl.nasa.gov; bg@pha.jhu.edu; George.sonneborn-1@nasa.gov NR 6 TC 0 Z9 0 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 369 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300082 ER PT B AU Andersson, BG Knauth, DC Snowden, SL Shelton, RL Wannier, PG AF Andersson, B-G Knauth, D. C. Snowden, S. L. Shelton, R. L. Wannier, P. G. BE Sonneborn, G Moos, HW Andersson, BG TI A multi-wavelength study of the Southern Coalsack SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID HIGH-RESOLUTION OBSERVATIONS AB We present a multi-wavelength study of the Southern Coalsack and its hot halo. The Coalsack is a well-defined dark cloud at a reliably determined distance, shown by ROSAT imaging to be surrounded by a hot halo. We have used FUSE and HST/STIS data to show that the halo contains O VI, and other ions in high ionization states. Based on location and energetics we argue that the heating is by the hot interior of the Upper Centaurus-Lupus Superbubble. Combining O VI & C IV data we show that the most likely energy transport mechanism between the hot and cold gas is conduction. However, the transport does not seem to be spatially dependent on the strong magnetic field (similar to 90 mu G), derived from high sampling-density optical polarimetry. C1 [Andersson, B-G] Johns Hopkins Univ, CAS, 3400 N Charles St, Baltimore, MD 21218 USA. [Knauth, D. C.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Snowden, S. L.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. [Shelton, R. L.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Wannier, P. G.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Andersson, BG (reprint author), Johns Hopkins Univ, CAS, 3400 N Charles St, Baltimore, MD 21218 USA. EM bg@pha.jhu.edu; dknauth@pha.jhu.edu; peter.wannier@jpl.nasa.gov RI Snowden, Steven/D-5292-2012 FU FUSE [NAG5-1360] FX This work was supported thrugh the FUSE grant NAG5-1360 to GHU. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 424 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300093 ER PT B AU Vennes, S Chayer, P Dupuis, J Moos, HW Lanz, T AF Vennes, S. Chayer, P. Dupuis, J. Moos, H. W. Lanz, T. BE Sonneborn, G Moos, HW Andersson, BG TI Hydrogen column density measurements toward white dwarfs for D/H studies SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria ID LOCAL INTERSTELLAR-MEDIUM; FUSE MISSION; DEUTERIUM; ABUNDANCES; NITROGEN; OXYGEN AB Hot white dwarfs provide sources of extreme ultraviolet (EUV) radiation against which the photoionization continua of interstellar H I, He I, and He H are measured. The column density measurements depend on a detailed knowledge of the intrinsic EUV luminosity of the sources. We discuss recent progress in the study of low- and high-metallicity white dwarfs enabling a study of interstellar hydrogen and helium continuum absorptions toward many lines of sight. We compare the EUV-based measurements to recent hydrogen column density measurements based on Ly alpha line profiles and discuss the implications for D/H and O/H ratios in the local interstellar medium. C1 [Vennes, S.; Chayer, P.; Dupuis, J.; Moos, H. W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Lanz, T.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lanz, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Vennes, S (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM vennes@pha.jhu.edu; chayer@pha.jhu.edu; jdupuis@pha.jhu.edu; hwm@jhu.edu; tlanz@umd.edu RI Vennes, Stephane/G-9903-2014 FU NASA [NAS5-32985]; LTSA NASA [NAGS-11844] FX Financial support to U.S. participants has been provided by NASA contract NAS5-32985. We acknowledge support from LTSA NASA grant NAGS-11844. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 460 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300105 ER PT B AU Godard, B Dixon, WV Dupuis, J Robinson, RD Sahnow, DJ Sonnentrucker, P Fullerton, AW Kaiser, ME Massa, D Lindler, DJ Barrett, P Hsu, JC Romelfanger, ML AF Godard, B. Dixon, W. V. Dupuis, J. Robinson, R. D. Sahnow, D. J. Sonnentrucker, P. Fullerton, A. W. Kaiser, M. E. Massa, D. Lindler, D. J. Barrett, P. Hsu, J. -C. Romelfanger, M. L. BE Sonneborn, G Moos, HW Andersson, BG TI FUSE calibration pipeline version 3.0 SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria AB The latest version (3.0) of the calibration pipeline for the Far Ultraviolet Spectroscopic Explorer (FUSE) is considerably faster, easier to maintain and more flexible for the end users than the older versions. It represents a major design change. Data are stored as a photon events (time of arrival, location, pulse height...) list throughout the pipeline. This allows time dependent corrections for such effects as spacecraft jitter and mirror or grating motions. Moreover users can now select and extract subsets of the data without rerunning the pipeline. C1 [Godard, B.; Dixon, W. V.; Dupuis, J.; Robinson, R. D.; Sahnow, D. J.; Sonnentrucker, P.; Fullerton, A. W.; Kaiser, M. E.; Romelfanger, M. L.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. [Godard, B.] IAP, F-75014 Paris, France. [Robinson, R. D.] Catholic Univ Amer, Inst Astrophys & CompSci, Washington, DC 20064 USA. [Fullerton, A. W.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Massa, D.] SGT Inc, Greenbelt, MD 20771 USA. [Lindler, D. J.] NASA, Goddard Space Flight Ctr, Lab Exoplant & Stellar Astrophys, Greenbelt, MD 20771 USA. [Barrett, P.; Hsu, J. -C.] STScl, Baltimore, MD 21218 USA. RP Godard, B (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM godard@pha.jhu.edu; wvd@pha.jhu.edu; jdupuis@pha.jhu.edu; sahnow@pha.jhu.edu; sonnentr@pha.jhu.edu; awf@pha.jhu.edu; kaiser@pha.jhu.edu; massa@taotaomona.gsfc.nasa.gov; pebarrett@gmail.com NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 550 EP 552 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300125 ER PT B AU Green, J Bally, J Brown, R Ebbets, D Freedman, W Grunsfeld, J Huchra, J Kilston, S Kimble, R Morse, J O'Connell, R Sembach, K Shull, M Siegmund, O Wilkinson, E AF Green, James Bally, John Brown, Robert Ebbets, Dennis Freedman, Wendy Grunsfeld, John Huchra, John Kilston, Steve Kimble, Randy Morse, Jon O'Connell, Robert Sembach, Kenneth Shull, Michael Siegmund, Oswald Wilkinson, Erik BE Sonneborn, G Moos, HW Andersson, BG TI Scientific rationale for a 10 meter UV-optical telescope SO ASTROPHYSICS IN THE FAR ULTRAVIOLET: FIVE YEARS OF DISCOVERY WITH FUSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Astrophysics in the Far Ultraviolet - Five Years of Discovery with FUSE CY AUG 02-06, 2004 CL Univ Victoria, Victoria, CANADA SP NASA, Herzberg Inst Astrophys, Orbital Sci Corp, Swales Aerosp HO Univ Victoria C1 [Green, James; Bally, John; Shull, Michael; Siegmund, Oswald] Univ Colorado, CASA, Campus Box 389, Boulder, CO 80304 USA. [Brown, Robert] Space Telescope Sci Inst, Baltimore, MD 80305 USA. [Ebbets, Dennis; Kilston, Steve] Ball Aerosp & Technol Corp, Syst Div, Boulder, CO 80305 USA. [Freedman, Wendy] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Grunsfeld, John] NASA, HQ, Washington, DC 20546 USA. [Huchra, John] Harvard Smithsonian Cfa, Cambridge, MA 02138 USA. [Kimble, Randy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Morse, Jon] Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. [O'Connell, Robert] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. RP Green, J (reprint author), Univ Colorado, CASA, Campus Box 389, Boulder, CO 80304 USA. EM jgreen@casa.colorado.edu; ab@casa.colorado.edu; sembach@stsci.edu; mshull@casa.colorado.edu NR 4 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-216-4 J9 ASTR SOC P PY 2006 VL 348 BP 559 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BET01 UT WOS:000239376300127 ER PT B AU Strohmayer, TE AF Strohmayer, T. E. BE Mason, JW TI Neutron Star Structure and Fundamental Physics SO ASTROPHYSICS UPDATE 2 SE Springer Praxis Books LA English DT Article; Book Chapter ID X-RAY-BURSTS; SOFT GAMMA-REPEATERS; EQUATION-OF-STATE; PERIODIC BRIGHTNESS OSCILLATIONS; MILLISECOND PULSAR; RELATIVISTIC STARS; LIGHT CURVES; R-MODES; NONRADIAL OSCILLATIONS; COHERENT OSCILLATIONS AB Neutron stars provide a natural laboratory for the study of matter under the most extreme conditions of density, pressure and magnetic fields known. Precise measurements of neutron star masses and radii may provide one of the only means to constrain important aspects of dense matter physics as well as fundamental particle physics. Moreover, neutron stars may contain states of matter not present anywhere else in the observable universe, for example, an exotic color-favor-locked (CFL), super fluid quark matter phase. Here, I discuss and review recent efforts to measure neutron star masses and radii in order to use them as probes of fundamental physics. Such efforts have focused on measurements of X-ray pulsation signals from both isolated and accreting neutron stars, as well as observations of the thermal emission from neutron star surfaces. Indeed, recent X-ray observations have provided the first evidence of discrete, redshifted spectral features from neutron star surfaces, which may eventually provide precise mass and radii estimates, however, uncertainties remain in their interpretation. Fast X-ray timing observations of X-ray bursting neutron stars have revealed spin modulation pulsations, and recent studies of "magnetar" giant flares have found fast oscillations which may be signatures of global vibrations of neutron star crusts. I will describe how these observations are yielding new insights on neutron star structure. C1 NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. RP Strohmayer, TE (reprint author), NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. EM tod.e.strohmayer@nasa.gov NR 94 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-30313-8 J9 SPRINGER-PRAX BOOKS PY 2006 BP 29 EP 54 DI 10.1007/3-540-30313-8_2 D2 10.1007/3-540-30313-8 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BLP45 UT WOS:000270727100002 ER PT J AU Weisskopf, MC Hughes, JP AF Weisskopf, M. C. Hughes, J. P. BE Mason, JW TI Six Years of Chandra Observations of Supernova Remnants SO ASTROPHYSICS UPDATE 2 SE Springer Praxis Books LA English DT Article; Book Chapter ID X-RAY-EMISSION; LARGE-MAGELLANIC-CLOUD; PULSAR WIND NEBULA; COMPACT CENTRAL OBJECT; ISOLATED NEUTRON-STAR; MAGNETIC-FIELD AMPLIFICATION; XMM-NEWTON OBSERVATION; POWERED BOW SHOCK; CASSIOPEIA-A; CRAB-NEBULA AB We present a review of the first six years of Chandra X-ray Observatory observations of supernova remnants. From the official "first-light" observation of Cassiopeia A that revealed for the first time the compact remnant of the explosion, to the recent million-second spectrally-resolved observation that revealed new details of the stellar composition and dynamics of the original explosion, Chandra observations have provided new insights into the supernova phenomenon. We present an admittedly biased overview of six years of these observations, highlighting new discoveries made possible by Chandra's unique capabilities. C1 [Weisskopf, M. C.] NASA, George C Marshall Space Flight Ctr, Space Sci Directorate, Huntsville, AL 35812 USA. [Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Weisskopf, MC (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Directorate, XD01, Huntsville, AL 35812 USA. EM martin.weisskopf@msfc.nasa.gov; jph@physics.rutgers.edu NR 206 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-30313-8 J9 SPRINGER-PRAX BOOKS PY 2006 BP 55 EP 113 DI 10.1007/3-540-30313-8_3 D2 10.1007/3-540-30313-8 PG 59 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BLP45 UT WOS:000270727100003 ER PT B AU Ao, CO Hajj, GA Iijima, BA Mannucci, AJ Schroder, TM Juarez, MDLT Leroy, SS AF Ao, C. O. Hajj, G. A. Iijima, B. A. Mannucci, A. J. Schroder, T. M. Juarez, M. de la Torre Leroy, S. S. BE Foelsche, U Kirchengast, G Steiner, A TI Sensitivity of stratospheric retrievals from radio occultations on upper boundary conditions SO ATMOSPHERE AND CLIMATE: STUDIES BY OCCULTATION METHODS LA English DT Proceedings Paper CT 2nd International Workshop on Occultations for Probing Atmosphere and Climate (OPAC-2) CY SEP 13-17, 2004 CL Graz, AUSTRIA ID ERROR ANALYSIS; ATMOSPHERE; VALIDATION; INVERSION; SYSTEM AB The main uncertainty in the stratospheric retrievals from GPS radio occultation (110) measurements comes from the lack of reliable measurements in the upper stratosphere and above where the bending due to the neutral atmosphere is weak and residual ionospheric effects are strong. In this work, we quantify the bias and uncertainty of the refractivity and temperature retrievals due to different upper boundary strategies using a simulation study. We use refractivity profile derived from lidar pressure and temperature profiles as the input states in generating the synthetic occultations. Random noise levels commensurate with the CHAMP RO measurements are added to the simulated data. We examine the sensitivity of stratospheric retrievals to two different upper boundary methods, one based on exponential extrapolation and the other on MSIS climatology. The simulation results show that both methods lead to comparable levels of temperature bias (less than 0.5 K below 30 km altitude), provided that the upper boundary heights are set above 55 km. C1 [Ao, C. O.; Hajj, G. A.; Iijima, B. A.; Mannucci, A. J.; Schroder, T. M.; Juarez, M. de la Torre] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. [Juarez, M. de la Torre] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. RP Ao, CO (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM chi.o.ao@jpl.nasa.gov NR 12 TC 5 Z9 5 U1 0 U2 3 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-34116-1 PY 2006 BP 17 EP + DI 10.1007/3-540-34121-8_2 PG 3 WC Instruments & Instrumentation; Meteorology & Atmospheric Sciences; Remote Sensing SC Instruments & Instrumentation; Meteorology & Atmospheric Sciences; Remote Sensing GA BER86 UT WOS:000239155400002 ER PT S AU Mannucci, AJ Ao, CO Yunck, TP Young, LE Hajj, GA Iijima, BA Kuang, D Meehan, TK Leroy, SS AF Mannucci, Anthony J. Ao, Chi O. Yunck, Thomas P. Young, Larry E. Hajj, George A. Iijima, Byron A. Kuang, Da Meehan, Thomas K. Leroy, Stephen S. BE Huang, AHL Bloom, HJ TI Generating climate benchmark atmospheric soundings using GPS occultation data - art. no. 630108 SO Atmospheric and Environmental Remote Sensing Data Processing and Utilization II: Perspective on Calibration/Validation Initiatives and Strategies SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Atmospheric and Environmental Remote Sensing Data Processing and Utilization II CY AUG 16-17, 2006 CL San Diego, CA SP SPIE DE climate benchmark; GPS radio occultation; temperature sounding; remote sensing; COSMIC; SI-traceability; global climate ID GLOBAL POSITIONING SYSTEM; EARTHS ATMOSPHERE; RADIO; CALIBRATION AB Atmospheric soundings derived from Global Positioning System radio occultations (GPSRO) acquired in low-Earth orbit have the potential to be global climate benchmark observations of significant value to the Global Climate Observing System (GCOS). Geophysical observables such as atmospheric pressure and temperature are derived by measuring propagation delay induced by the atmosphere, a measurement whose fundamental unit-the second-is absolutely determined by calibration against atomic clocks. In this paper, we analyze the sources of systematic and random error for GPSRO soundings to determine the steps needed to establish GPSRO as a climate benchmark observation. Benchmarks require specific processing strategies and specific forms of documentation so that confidence in the accuracy and precision of the measurements is assured. Establishing calibration traceability to absolute standards (SI-traceability) is an essential strategy. We discuss a wide range of error sources in a geophysical retrieval, such as orbit determination error, signal delay in the Earth's ionosphere, and quality control strategies. Uncalibrated ionospheric delay is identified as the error source deserving the most attention in establishing SI-traccability of the retrievals, to meet stringent climate observation requirements of 0.5 K accuracy and 0.04 K stability. Profile comparisons from the recently launched COSMIC constellation establish strong upper limits on systematic error arising from the individual instruments. These encouraging results suggest that GPSRO should become a permanent resource for the GCOS. These highly precise and accurate instruments can be deployed on future Earth Observation satellites at a low per-sensor cost and minimal interference to existing and planned observational programs. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mannucci, AJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Mannucci, Anthony/0000-0003-2391-8490 NR 26 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6380-9 J9 P SOC PHOTO-OPT INS PY 2006 VL 6301 BP 30108 EP 30108 AR 630108 DI 10.1117/12.683973 PG 14 WC Remote Sensing SC Remote Sensing GA BFG54 UT WOS:000241728000006 ER PT S AU Aumann, HH Gregorich, D AF Aumann, Hartmut H. Gregorich, David BE Huang, AHL Bloom, HJ TI AIRS observations of deep convective clouds - art. no. 63010J SO Atmospheric and Environmental Remote Sensing Data Processing and Utilization II: Perspective on Calibration/Validation Initiatives and Strategies SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Atmospheric and Environmental Remote Sensing Data Processing and Utilization II CY AUG 16-17, 2006 CL San Diego, CA SP SPIE DE infrared hyperspectral; temperature sounding; climate hurricane; EOS Aqua AB Large thunderstorms can be identified in the AIRS data as areas where the brightness temperature of the 1231 cm(-1) atmospheric window channel in non-polar areas is less than 210 K. Each day about 6000 large thunderstorms are identified by this test, almost exclusively within 30 degrees of the equator. Since the size of the AIRS footprint at nadir is 13.5 km, a brightness temperature of less than 2 10 K indicates that the top of the anvil of the thunderstorm protrudes well into the tropopause. Such objects are commonly referred to as Deep Convective Clouds (DCC). Our interest in DCC was motivated by the question "Are severe weather events increasing due to global warming". Each DCC is a severe weather event, although not on the scale of the much less frequent hurricanes, which can be identified in the AIRS data as clusters of several hundred DCC. For the past four years the number of DCC per day has been fairly stable for all tropical oceans combined, but a significant increase can be seen day and night in the Atlantic Ocean. This increase may be related to the slowing of the Atlantic meridional overturning circulation. The most prominent features in brightness temperature spectra of DCC are due to stratospheric CO2, Ozone and Methane. In the channels with weighting functions below the stratosphere the brightness temperature is typically 205 K, with a characteristic I to 2.5 K drop between 1000 and 750 cm(-1), equivalent to a 2-4 % drop in emissivity. This is likely due to the presence of cirrus (ice) particles. Firmer conclusions about the significance of the DCC count require a considerably longer data set than the currently available four years from AIRS. We plan to continue this analysis with AIRS data. Extension of the analysis to past operational sounders in polar orbit requires independent validation of the stability and absolute accuracy of the radiometric calibration at 210 K. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Aumann, HH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 5 TC 10 Z9 10 U1 2 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 0-8194-6380-9 J9 P SOC PHOTO-OPT INS PY 2006 VL 6301 BP J3010 EP J3010 AR 63010J DI 10.1117/12.681201 PG 7 WC Remote Sensing SC Remote Sensing GA BFG54 UT WOS:000241728000014 ER PT J AU Dey, S Tripathi, SN Singh, RP Holben, BN AF Dey, S Tripathi, SN Singh, RP Holben, BN TI Retrieval of black carbon and specific absorption over Kanpur city, northern India during 2001-2003 using AERONET data SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE aerosols; black carbon; specific absorption; internal mixing; effective medium approximation ID AEROSOL OPTICAL-PROPERTIES; SKY RADIANCE MEASUREMENTS; REFRACTIVE-INDEX; OCEAN EXPERIMENT; CLIMATE; MODEL; DISTRIBUTIONS; EXTINCTION; NETWORK; INDOEX AB Column-integrated aerosol black carbon (BC) concentration, [BC] has been retrieved over Kanpur (an industrial city in the Gangetic basin, northern India) during 2001-2003 for the first time. [BC] is derived from BC volume fraction and AERONET-retrieved size distribution using Maxwell-Garnett and Bruggernan mixing rules in a mixture of water, BC and (NH4)(2)SO4. In addition partly absorbing components like organic carbon (OC) and dust are added to the Maxwell-Garnett mixture depending on the season to investigate their role in the retrieval of [BC]. The volume fraction of each component is retrieved by matching the mixture refractive index (real, n(lambda) and imaginary, k(lambda)) with AERONET-retrieved refractive index. [BC] shows seasonal variations with high values (> 10mg m(-2)) observed during the post-monsoon and winter seasons and low values (< 6 mg m(-2)) during the monsoon season. Specific absorption cross-section (alpha(a)) decreases non-linearly with the increase in [BC], however, the decrease becomes linear when other absorbing components are present. Yearly averaged [BC] and a. are 9.99 +/- 1.95, 5.52 +/- 1.07, 7.9 +/- 1.53 mg m(-2) and 7.9 +/- 1.83 and 9.67 +/- 3.45, 12.74 +/- 2.92m(2) g(-1) for 2001, 2002 and 2003, respectively, using Maxwell-Garnett mixing, which differ by similar to 15 % from those using Bruggeman mixing. [BC] shows diurnal variation with morning and afternoon peaks and mid-day minimum. The amplitude is subdued as it represents the total column, which is more influenced by anthropogenic activities than by boundary layer dynamics. In order to estimate [BC] accurately, OC has to be considered when the absolute difference between k(0.44 mu m) and k(1.02 mu m) becomes higher than 0.0015. The sensitivity of [BC] due to dust n(lambda) becomes important during the intense dust loading period. It was found that [BC] is more sensitive to dust k(lambda) than dust n(lambda), as [BC] increases similar to 10-13% for 10% rise in k(lambda). Retrieved [BC] shows good agreement with the in situ measurements. Therefore our retrieval can be used as an alternate method to infer BC and OC specific absorption globally. (c) 2005 Elsevier Ltd. All rights reserved. C1 Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tripathi, SN (reprint author), Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India. EM snt@iitk.ac.in RI Singh, Ramesh/G-7240-2012; Tripathi, Sachchida/J-4840-2016 NR 46 TC 20 Z9 21 U1 0 U2 9 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 JAN PY 2006 VL 40 IS 3 BP 445 EP 456 DI 10.1016/j.atmosenv.2005.09.053 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 012GD UT WOS:000235325300004 ER PT S AU Wu, DL Preusse, P Eckermann, SD Jiang, JH Juarez, MDLT Coy, L Wang, DY AF Wu, Dong L. Preusse, Peter Eckermann, Stephen D. Jiang, Jonathan H. Juarez, Manuel de la Torre Coy, Lawrence Wang, Ding Y. BE Burrows, JP Eichmann, KU LLewellyn, EJ TI Remote sounding of atmospheric gravity waves with satellite limb and nadir techniques SO ATMOSPHERIC REMOTE SENSING: EARTH'S SURFACE, TROPOSPHERE, STRATOSPHERE AND MESOSPHERE - II SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE gravity waves; satellite observations; instrument filter; wave sources ID MLS OBSERVATIONS; STRATOSPHERE; VARIANCE AB Recent advances in satellite techniques hold great potential for mapping global gravity wave (GW) processes at various altitudes. Poor understanding of small-scale GWs has been a major limitation to numerical climate and weather models for making reliable forecasts. Observations of short-scale features have important implication for validating and improving future high-resolution numerical models. This paper summarizes recent GW observations and sensitivities from several satellite instruments, including MLS, AMSU-A, AIRS, GPS, and CLAES. It is shown in an example that mountain waves with horizontal wavelengths as short as similar to 30 km now can be observed by AIRS, reflecting the superior horizontal resolution in these modern satellite instruments. Our studies show that MLS, AMSU-A and AIRS observations reveal similar GW characteristics, with the observed variances correlated well with background winds. As a complementary technique, limb sounding instruments like CRISTA, CLAES, and GPS can detect GWs with better vertical but poorer horizontal resolutions. To resolve different parts of the broad GW spectrum, both satellite limb and nadir observing techniques are needed, and a better understanding of GW complexities requires joint analyses of these data and dedicated hieh-resolution model simulations. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wu, DL (reprint author), CALTECH, Jet Prop Lab, MS 183-701, Pasadena, CA 91109 USA. EM dwu@mls.jpl.nasa.gov RI Preusse, Peter/A-1193-2013; Wu, Dong/D-5375-2012 OI Preusse, Peter/0000-0002-8997-4965; NR 21 TC 64 Z9 64 U1 5 U2 11 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 37 IS 12 BP 2269 EP 2277 DI 10.1016/j.asr.2005.07.031 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Remote Sensing SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences; Remote Sensing GA BEY20 UT WOS:000240088800018 ER PT J AU Bhatia, AK Landi, E Eissner, W AF Bhatia, AK Landi, E Eissner, W TI Atomic data and spectral line intensities for MgV SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article ID EXTREME-ULTRAVIOLET SPECTRUM; OPTICALLY THIN PLASMAS; ISOELECTRONIC SEQUENCE; FORBIDDEN TRANSITIONS; GROUND CONFIGURATION; COLLISION STRENGTHS; 2P4 CONFIGURATION; RATE COEFFICIENTS; CROSS-SECTIONS; EMISSION-LINES AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Mg V. The configurations used are 2s(2)2p(4), 2s2p(5), 2p(6), 2s(2)2p(3)3s, 2s(2)2p(3)3p, and 2s(2)2p(3)3d, giving rise to 86 fine-structure levels in intermediate coupling. Collision strengths are calculated at five incident energies, 10, 20, 30, 40, and 50 Ry, in the distorted wave approximation. Excitation rate coefficients (not tabulated here) are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. To calculate excitation rate coefficients, collision strengths at low and high energy limits are calculated by a method described by Burgess and Tully. Using the excitation rate coefficients and the radiative transition rates, statistical equilibrium equations for level populations are solved at electron densities covering the range of 10(8)-10(14) cm(-3) at an electron temperature of log T-e = 5.4, corresponding to the maximum abundance of Mg V. Fractional level populations and relative spectral line intensities are also calculated. Our calculated intensities are compared with the active region observations from the solar EUV rocket telescope and spectrograph (SERTS) and the diagnostic properties of Mg V are discussed. This dataset will be made available in the next version of the CHIANTI database. (c) 2005 Elsevier Inc. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. USN, Res Lab, ARTEP Inc, Washington, DC 20375 USA. Teilinst 1, Inst Theoret Phys, D-70550 Stuttgart, Germany. RP Bhatia, AK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Anand.K.Bhatia@nasa.gov RI Landi, Enrico/H-4493-2011 NR 31 TC 7 Z9 7 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0092-640X J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD JAN PY 2006 VL 92 IS 1 BP 105 EP 175 DI 10.1016/j.adt.2005.09.002 PG 71 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA 000DO UT WOS:000234441300003 ER PT J AU Anderson, WE Ryan, HM Santoro, RJ AF Anderson, William E. Ryan, Harry M., III Santoro, Robert J. TI Impact wave-based model of impinging jet atomization SO ATOMIZATION AND SPRAYS LA English DT Article ID LIQUID SHEETS; AERODYNAMIC INSTABILITY; FLOW; DISINTEGRATION; SPRAYS AB Previous studies of impinging jet atomizers indicated that "impact waves" may dominate the atomization of high-speed turbulent impinging jets. An experiment was conducted to characterize the formation and effects of impact waves on the atomization process. The model flow consisted of opposed turbulent water jets at atmospheric conditions. The impact waves are formed with a characteristic wavelength of about one jet diameter, and the distance between the waves was found to increase with distance from the impingement point due to wave merging, which helps explain discrepancies reported in the previous studies. A computational study of the flow structure around the stagnation point showed that the effects of impingement extend about one jet diameter upstream and that maximum gradients and incipient disruption of the surface occur at a normalized radius of 1.2, where an inflection in the jet flow from predominantly axial to predominantly radial occurs. Using these observations and measurements, and existing correlations for breakup length and drop size, a three-step phenomenological model of atomization (impact wave formation and propagation, sheet breakup into ligaments, and ligament disintegration into drops) was developed. C1 Purdue Univ, W Lafayette, IN 47907 USA. NASA, Stennis Space Ctr, MS 39529 USA. Penn State Univ, University Pk, PA 16802 USA. RP Anderson, WE (reprint author), Purdue Univ, 315 N Grant St, W Lafayette, IN 47907 USA. NR 31 TC 4 Z9 5 U1 2 U2 11 PU BEGELL HOUSE INC PI REDDING PA 50 CROSS HIGHWAY, REDDING, CT 06896 USA SN 1044-5110 J9 ATOMIZATION SPRAY JI Atom. Sprays PY 2006 VL 16 IS 7 BP 791 EP 805 PG 15 WC Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA 122EP UT WOS:000243208800006 ER PT J AU Trinh, HP Chen, CA AF Trinh, Huu P. Chen, C. A. TI Development of liquid jet atomization and breakup models including turbulence effects SO ATOMIZATION AND SPRAYS LA English DT Article ID STILL GASES; SURFACE AB Recent experimental investigations and physical modeling studies have indicated that turbulence behaviors within a liquid jet have considerable effects on the atomization process. This study aims to model the turbulence effect in the atomization process of a cylindrical liquidjet. Two widely used models, the Kelvin-Helmholtz instability of Reitz [8] (the blob model) and the Taylor-Analogy-Breakup (TAB) secondary droplet breakup by O'Rourke and Amsden [9], are further extended to include turbulence effects. In the primary break-tip model, the level of the turbulence effect on the liquid breakup depends on the characteristic scales and the initial flow conditions. For the secondary breakup, an additional turbulence force, acted on parent drops, is modeled and integrated into the TAB governing equation. The drop size formed from this break-zip regime is estimated based on the energy balance before and after the breakup occurrence. This article describes theoretical development and assessment of the current models, called T-blob and T-TAB, for primary and secondary breakup, respectively. C1 Univ Alabama, Dept Chem & Mat Engn, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Chen, CA (reprint author), Univ Alabama, Dept Chem & Mat Engn, Huntsville, AL 35899 USA. EM cchen@chc.uah.edu NR 31 TC 13 Z9 13 U1 2 U2 12 PU BEGELL HOUSE INC PI REDDING PA 50 CROSS HIGHWAY, REDDING, CT 06896 USA SN 1044-5110 J9 ATOMIZATION SPRAY JI Atom. Sprays PY 2006 VL 16 IS 8 BP 907 EP 932 DI 10.1615/AtomizSpr.v16.i8.40 PG 26 WC Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA 142NN UT WOS:000244656800004 ER PT S AU Xia, S Di Vito, B Munoz, C AF Xia, Songtao Di Vito, Ben Munoz, Cesar BE Graf, S Zhang, W TI Predicate abstraction of programs with non-linear computation SO AUTOMATED TECHNOLOGY FOR VERIFICATION AND ANALYSIS, PROCEEDINGS SE Lecture Notes in Computer Science LA English DT Article; Proceedings Paper CT 4th International Symposium on Automated Technology for Verification and Analysis CY OCT 23-26, 2006 CL Beijing, PEOPLES R CHINA SP Chinese Acad Sci, Inst Software, Lab Comp Sci AB Verification of programs relies on reasoning about the computations they perform. In engineering programs, many of these computations are non-linear. Although predicate abstraction enables model checking of programs with large state spaces, the decision procedures that currently support predicate abstraction are not able to handle such nonlinear computations. In this paper, we propose an approach to model checking a class of data-flow properties for engineering programs that contain non-linear products and transcendental functions. The novelty of our approach is the integration of interval constraint solving techniques into the automated predicate discovery/predicate abstraction process, which extends the expressive power of predicate abstraction-based model checking. Using this approach, we construct a prototype model checker for C programs called VISA (Verification of Industrial-Strength Applications). VISA is built on top of Berkeley's BLAST and University of Nantes' Realpaver. We successfully apply VISA to scientific computation libraries and avionics applications to verify the absence of certain runtime arithmetic errors. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. Natl Inst Aerosp, Hampton, VA 23665 USA. RP Xia, S (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 42 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 3-540-47237-1 J9 LECT NOTES COMPUT SC PY 2006 VL 4218 BP 352 EP 368 PG 17 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BFF99 UT WOS:000241648200027 ER PT J AU Reschke, MF Somers, JT Ford, G AF Reschke, MF Somers, JT Ford, G TI Stroboscopic vision as a treatment for motion sickness: Strobe lighting vs. shutter glasses SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE ocular motility; spaceflight; visual acuity; retinal slip ID SPACEFLIGHT AB Introduction: Countermeasures (e.g., drugs, training, etc.) designed to combat the problem of space motion sickness (SMS) have had only limited successes. A possible solution for SMS and terrestrial motion sickness may rest in preventing retinal slip via stroboscopic vision. Methods: There were 32 subjects who participated in a study to investigate the effect of stroboscopic illumination on motion sickness using either a strobe light or liquid crystal display (LCD) shutter glasses. There were 19 subjects who read text and made +/- 20 degrees head movements in the horizontal plane (yaw) at 0.2 Hz while wearing left-right reversing prisms and exposed to 4-Hz stroboscopic or normal room illumination (control condition). Motion sickness was scored using the Miller and Graybiel scale and subjective self-ratings. In a crossover design, testing was repeated using stroboscopic LCD shutter glasses with an additional 13 subjects and 6 subjects from the first condition. Results: During the experiment with a strobe light, motion sickness scores were significantly lower than in the control condition (chi 0.32 strobe vs. chi 3.79 light = p < 0.003). Results with the LCD shutter glasses corresponded with those when the environment was strobed in an otherwise dark room (chi 1.0 glasses vs. chi 4.1 light = p < 0.001). Conclusions: Stroboscopic illumination reduced the severity of motion sickness symptoms, and shutter glasses with a flash frequency of 4 Hz are as effective as a strobe light. Stroboscopic illumination appears to be an effective countermeasure where retinal slip is a significant factor in eliciting motion sickness due to either self-or surround-motion. C1 Wyle Labs, Houston, TX USA. NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA. RP Reschke, MF (reprint author), 2101 NASA Pkwy,SK272, Houston, TX 77058 USA. EM millard.f.reschke@nasa.gov NR 11 TC 9 Z9 9 U1 1 U2 7 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 JAN PY 2006 VL 77 IS 1 BP 2 EP 7 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA 001IA UT WOS:000234525600002 PM 16422446 ER PT J AU Moehler, S Sweigart, AV AF Moehler, S Sweigart, AV TI The nature of the hot stars in the bulge of globular cluster NGC 6388 SO BALTIC ASTRONOMY LA English DT Article; Proceedings Paper CT 2nd Meeting on Hot Subdwarf Stars and Related Objects CY JUN 06-10, 2005 CL Santa Cruz de la Palma, SPAIN DE stars : horizontal branch; stars : evolution; globular clusters : individual : NGC 6388 ID BLUE HORIZONTAL-BRANCH; NGC 6441; VARIABLE-STARS; NGC-2808 AB The metal-rich bulge globular clusters NGC6388 and NGC6441 show, distinct blue horizontal-branch tails in their color-magnitude diagrams. They, are thus strong cases of the well known Second Parameter Problem. In addition, the horizontal branches in these globular clusters show an upward tilt toward bluer colors, which cannot be explained by canonical evolutionary models. We will discuss several scenarios which have been proposed to explain these two features and present observations obtained to test these scenarios. C1 Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Moehler, S (reprint author), Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. OI Moehler, Sabine/0000-0002-4152-9643 NR 17 TC 4 Z9 4 U1 0 U2 1 PU INST THEORETICAL PHYSICS ASTRONOMY PI MOLETAI PA MOLETAI LT-4150, LITHUANIA SN 1392-0049 J9 BALT ASTRON JI Balt. Astron. PY 2006 VL 15 IS 1 BP 41 EP 48 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 032SQ UT WOS:000236795400007 ER PT S AU Pohorille, A Darve, E AF Pohorille, Andrew Darve, Eric BE MohammadDjafari, A TI A Bayesian approach to calculating free energies in chemical and biological systems SO BAYESIAN INFERENCE AND MAXIMUM ENTROPY METHODS IN SCIENCE AND ENGINEERING SE AIP Conference Proceedings LA English DT Proceedings Paper CT 26th International Workshop on Bayesian Inference and Maximum Entropy Methods in Science and Engineering CY JUL 08-13, 2006 CL Paris, FRANCE SP ET Jaynes Fdn, CNRS, Signal & Syst Lab, Univ Paris 11, GRD ISIS, French Def Minist, Res & Dev Sect, Int Soc Bayesian Anal DE free energy; Gram-Charlier polynomials; Maximum Likelihood AB A common objective of molecular simulations in chemistry and biology is to calculate the free energy difference between systems of interest. We propose to improve estimates of these free energies by modeling the underlying probability distribution as a the square of a "wave function", which is a linear combination of Gram-Charlier polynomials. The number of terms, N, in this expansion is determined by calculating the posterior probability, P(N X), where X stands for all energy differences sampled in a simulation. The method offers significantly improved free energy estimates when the probability distribution is broad and non-Gaussian, which makes it applicable to challenging problems, such as protein-drug interactions. C1 [Pohorille, Andrew] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, Moffett Field, CA 94035 USA. [Darve, Eric] Stanford Univ, Dept Engn Mech, Stanford, CA 94305 USA. RP Pohorille, A (reprint author), NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, Moffett Field, CA 94035 USA. NR 4 TC 3 Z9 3 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 978-0-7354-0371-0 J9 AIP CONF PROC PY 2006 VL 872 BP 23 EP + PG 2 WC Physics, Multidisciplinary; Statistics & Probability SC Physics; Mathematics GA BFT22 UT WOS:000244484400003 ER PT S AU Salasoo, L Moder, JP Myrabo, LN Nelson, JK AF Salasoo, L. Moder, J. P. Myrabo, L. N. Nelson, J. K. BE Komurasaki, K Yabe, T Uchida, S Sasoh, A TI Analysis of charge cloud geometries for ion propulsion of microwave lightcraft SO BEAMED ENERGY PROPULSION SE AIP Conference Proceedings LA English DT Proceedings Paper CT 4th International Symposium on Beamed Energy Propulsion CY NOV 15-18, 2005 CL Nara, JAPAN SP Commemorat Org Japan World Exposit 1970, Tokyo Inst Technol, Entropia Laser Initiat, Inst Laser Technol AB The thrust and flight performance of a novel airbreathing ion propulsion concept was analyzed for a 20-m diameter microwave-propelled Lightcraft. Two sample vehicle/charge cloud geometries were modeled using an axisymmetric Finite Element Analysis (FEM) electrostatic package to determine the charge and electric field distributions, as well as the thrust force on the vehicle. A 2-D cartesian analysis was then employed to approximately model three additional geometries in which the vehicle and charge cloud axes of symmetry did not coincide. In each case, the amount of charge ejected from the vehicle was such that the maximum electric field at the vehicle surface corresponded to the breakdown value for NTP air, similar to 2.99 MV/m. The maximum electrostatic force was calculated for each of the three cloud/vehicle configurations. Estimates of the characteristic velocities for equilibrium flight were calculated, and variations in vehicle flight orientation were considered in order to achieve a compromise between aerodynamic benefits and maximum electrostatic force. C1 [Salasoo, L.; Nelson, J. K.] Rensselaer Polytech Inst, 110 8th St, Troy, NY 12180 USA. [Salasoo, L.] Gen Elect R&D Ctr, Schenectady, NY USA. [Moder, J. P.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Salasoo, L (reprint author), Rensselaer Polytech Inst, 110 8th St, Troy, NY 12180 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0322-8 J9 AIP CONF PROC PY 2006 VL 830 BP 637 EP + PG 2 WC Optics; Physics, Applied; Physics, Multidisciplinary SC Optics; Physics GA BEM36 UT WOS:000238124400065 ER PT B AU Gor, V Shapiro, BE Jonsson, H Heisler, M Reddy, GV Meyerowitz, EM Mjolsness, E AF Gor, V Shapiro, BE Jonsson, H Heisler, M Reddy, GV Meyerowitz, EM Mjolsness, E BE Kolchanov, N Hoffestaedt, R Milanesi, L TI A software architecture for developmental modeling in plants: The computable plant project SO BIOINFORMATICS OF GENOME REGULATION AND STRUCTURE II LA English DT Proceedings Paper CT 4th International Conference on Bioinformatics of Genome Regulation and Structure (BGRS 2004) CY JUL 25-30, 2004 CL Novosibirsk, RUSSIA SP Russian Acad Sci, Siberian Branch, Inst Cytol & Genet, Lab Theoret Genet DE Arabidopsis; cellerator; correspondence; Delaunay triangulation; meristem; SAM; SBML; softassign; Voronoi diagram AB We present the software architecture of the Computable Plant Project, a multidisciplinary computationally based approach to the study of plant development. Arabidopsis thaliana is used as a model organism, and shoot apical meristem (SAM) development as a model process. SAMs are the plant tissues where regulated cell division and differentiation lead to plant parts such as flowers and leaves. We are using green fluorescent proteins to mark specific cell types and acquire time series of three-dimensional images via laser scanning confocal microscopy. To support this, we have developed an interoperable architecture for experiment design that involves automated code generation, computational modeling, and image analysis. Automated image analysis, model flitting, and code generation allow us to explore alternative hypothesis in silico and guide in vivo experimental design. These predictions are tested using standard techniques, such as inducible mutants and altered hormone gradients. The present paper focuses on the automated code generation architecture. C1 CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. Lund Univ, Dept Theoret Phys, Complex Syst Div, S-22100 Lund, Sweden. CALTECH, Div Biol, Pasadena, CA 91125 USA. Univ Calif Irvine, Bren Sch Informat & Comp Sci, Inst Genom & Bioinformat, Irvine, CA 92717 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM emj@uci.edu RI heisler, marcus/B-9738-2015 OI heisler, marcus/0000-0001-5644-8398 FU United States National Science Foundation (NSF) under Frontiers in Integrative Biological Research (FIBR) [EF-0330786]; Knut and Alice Wallenberg Foundation through Swegene FX This work was supported by the United States National Science Foundation (NSF) under Frontiers in Integrative Biological Research (FIBR) grant No. EF-0330786. HJ was supported, in part, by the Knut and Alice Wallenberg Foundation through Swegene. Portions of the research described in this paper were performed at the California Institute of Technology. NR 0 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 0-387-29450-3 PY 2006 BP 345 EP 354 DI 10.1007/0-387-29455-4_33 PG 10 WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Computer Science, Interdisciplinary Applications; Genetics & Heredity; Mathematics, Interdisciplinary Applications SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Computer Science; Genetics & Heredity; Mathematics GA BDN75 UT WOS:000234508700034 ER PT J AU Carter, GM Stolen, ED Breininger, DR AF Carter, GM Stolen, ED Breininger, DR TI A rapid approach to modeling species-habitat relationships SO BIOLOGICAL CONSERVATION LA English DT Article DE Florida scrub-jay; Aphelocoma coerulescens; species-habitat model; occupancy; habitat mapping; model selection; scale; logistic regression modeling; grid cell mapping ID FLORIDA SCRUB JAY; ESTIMATING SITE OCCUPANCY; DEMOGRAPHIC SUCCESS; SUITABILITY; DISTRIBUTIONS; PROBABILITIES; POPULATION; PREDICTION; SCALE; BIRD AB A basic element in the success of managing species of conservation concern is knowledge of the species' habitat occupancy Often, predictive species-habitat models are developed from GIS data sources that were intended for purposes other than predicting species habitat occupancy and are of inappropriate scale. In addition, the techniques used to quantify predictor variables from such data sources are often time consuming and cannot be repeated efficiently to reflect changing conditions. We used digital orthophotos and a grid cell classification scheme to develop an efficient technique to quantify predictor variables to model Florida scrub-jay habitat occupancy. We combined our classification scheme with a priori hypothesis development using expert knowledge and a previously published habitat suitability index and used an objective model selection procedure to choose candidate models. We classified a large area (43,000 ha) in a fraction of the time that would be required to map vegetation classes and were able to test models at varying scales using a grid-cell windowing process. Interpretation of the selected models confirmed existing knowledge of factors important to Florida scrub-jay habitat occupancy. The potential uses and advantages of using a grid cell classification scheme in conjunction with expert knowledge and an objective model selection procedure are discussed. (c) 2005 Elsevier Ltd. All rights reserved. C1 NASA, John F Kennedy Space Ctr, Dynamac Corp, Dyn 2,Ecol Programs, Kennedy Space Ctr, FL 32899 USA. RP Carter, GM (reprint author), NASA, John F Kennedy Space Ctr, Dynamac Corp, Dyn 2,Ecol Programs, Kennedy Space Ctr, FL 32899 USA. EM Cartegm@kscems.ksc.nasa.gov NR 41 TC 31 Z9 32 U1 1 U2 16 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD JAN PY 2006 VL 127 IS 2 BP 237 EP 244 DI 10.1016/j.biocon.2005.08.012 PG 8 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 000GK UT WOS:000234448800012 ER PT B AU Ocampo, A Vajda, V Buffetaut, E AF Ocampo, A Vajda, V Buffetaut, E BE Cockell, C Koeberl, C Gilmour, I TI Unravelling the Cretaceous-Paleogene (KT) turnover, evidence from flora, fauna and geology SO BIOLOGICAL PROCESSES ASSOCIATED WITH IMPACT EVENTS SE IMPACT STUDIES LA English DT Proceedings Paper CT 10th European-Science-Foundation IMPACT Workshop CY MAR 29-APR 01, 2003 CL Kings Coll, Cambridge, ENGLAND HO Kings Coll ID HELL CREEK FORMATION; TERTIARY BOUNDARY; IMPACT CRATER; NORTH-DAKOTA; DINOSAUR EXTINCTION; WESTERN CANADA; CONTIGUOUS STRATA; CHICXULUB CRATER; MASS EXTINCTION; OBLIQUE IMPACTS AB The global devastation of ecosystems as a consequence of a meteorite Impact 65 million years ago is clearly detectable in palaeontological and geological records all over the globe. Here we compare and contrast the consequences of the impact expressed in the vegetation, vertebrate fossil record and geological signatures left by the devastation, including information from new proximal KT boundary exposures and new palynological data. The geological evidence of the Chicxulub irnpact crater shows that the target rock was composed by higher percentages of anhydrite (sulfur source) than carbonates. Atmospheric radiative transfer models Suggest that the vaporized target rock rapidly converted into sulfuric acid H2SO4 aerosols where it was injected in the stratosphere by the force of the impact and globally distributed. It took at least 10 years for the H2SO4 to dissipate, making the Earth's atmosphere opaque to sunlight, leading to a reduction of solar transmission to 10-20% of normal for that period. Southern Hemisphere terrestrial Cretaceous-Paleogene boundary sediments in New Zealand reveal that a diverse Late Cretaceous vegetation was abruptly followed by a short interval dominated by fungi, before the pioneer vegetation of ferns re-conquered the soil. The fern dominated interval, so called fern spike is also evident from Northern Hemisphere Cretaceous-Paleogene boundary sections. The massive depletion in spore-pollen diversity is interpreted to reflect devastation of photosynthetic plant communities, a scenario that agrees well with the atmospheric radiative transfer models. The pattern of vertebrate extinctions revealed by the fossil record accords with the temporary, global devastation of photosynthetic plant communities. Vegetation depletion at high latitudes may also explain the extinction of polar dinosaurs, which apparently were able to withstand relatively cool temperatures and periods of low light intensity: the main reason for their disappearance appears to have been lack of food rather than darkness and cooling. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ocampo, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM adriana.c.ocampo@jpl.nasa.gov; vivi.vajda@geol.lu.se; eric.buffetaut@wanadoo.fr OI Vajda, Vivi/0000-0003-2987-5559 NR 98 TC 9 Z9 9 U1 2 U2 34 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-25735-7 J9 IMPACT STUD PY 2006 BP 197 EP 219 DI 10.1007/3-540-25736-5_9 PG 23 WC Geosciences, Multidisciplinary; Paleontology SC Geology; Paleontology GA BEH52 UT WOS:000237271800009 ER PT S AU Hinchey, MG Sterritt, R AF Hinchey, Michael G. Sterritt, Roy BE Pan, Y Rammig, FJ Schmeck, H Solar, M TI 99%. (biological) inspiration ... SO BIOLOGICALLY INSPIRED COOPERATIVE COMPUTING SE International Federation for Information Processing LA English DT Proceedings Paper CT 1st IFIP International Conference on Biologically Inspired Computing held at the 19th World Computer Congress CY AUG 21-24, 2006 CL Santiago, CHILE SP IFIP TC 10 AB Greater understanding of biology in modem times has enabled significant breakthroughs in improving healthcare, quality of life, and eliminating many diseases and congenital illnesses. Simultaneously there is a move towards emulating nature and copying many of the wonders uncovered in biology, resulting in "biologically inspired" systems. Significant results have been reported in a wide range of areas, with systems inspired by nature enabling exploration, communication, and advances that were never dreamed possible just a few years ago. We warn, that as in many other fields of endeavor, we should be inspired by nature and biology, not engage in mimicry. We describe some results of biological inspiration that augur promise in terms of improving the safety and security of systems, and in developing self-managing systems, that we hope will ultimately lead to self-governing systems. C1 [Hinchey, Michael G.; Sterritt, Roy] Univ Ulster, Sch Comp & Math, Coleraine BT52 1SA, Londonderry, North Ireland. RP Sterritt, R (reprint author), Univ Ulster, Sch Comp & Math, Coleraine BT52 1SA, Londonderry, North Ireland. FU NASA Office of Systems and Mission Assurance (OSMA) through its Software Assurance Research Program (SARP); Computer Science research Institute (CSRI); Centre for Software Process Technologies (CSPT); NI through the Centres of Excellence Programme under the EU Peace II initiative FX Part of this work has been supported by the NASA Office of Systems and Mission Assurance (OSMA) through its Software Assurance Research Program (SARP)project, Formal Approaches to Swarm Technologies (FAST), and by NASA SoftwareEngineering Laboratory, Goddard Space Flight Center (Code 581). This research is partly supported at University of Ulster by the Computer Science research Institute (CSRI) and the Centre for Software Process Technologies (CSPT) which is funded by Invest NI through the Centres of Excellence Programme, under the EU Peace II initiative. NR 30 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES SN 1571-5736 BN 0-387-34632-5 J9 INT FED INFO PROC PY 2006 VL 216 BP 7 EP + PG 3 WC Computer Science, Theory & Methods SC Computer Science GA BEX39 UT WOS:000239985100002 ER PT J AU Patel, OV Lintault, L Zakrzewska, E Maple, R Baer, L Ronca, A Wade, C Plaut, K AF Patel, Osman V. Lintault, Laura Zakrzewska, Elzbieta Maple, Rhonda Baer, Lisa Ronca, April Wade, Charles Plaut, Karen TI Hypergravity induced suppression of lactation in periparturient rats: Differential dynamics of prolactin receptor isoform expression following prolactin and bromocryptine supplementation in rats. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 39th Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 29-AUG 01, 2006 CL Univ Nebraska Med Ctr, Omaha, NE SP Soc Study Reprod HO Univ Nebraska Med Ctr C1 Michigan State Univ, Dept Anim Sci, E Lansing, MI 48824 USA. Univ Vermont, Dept Anim Sci, Burlington, VT 05405 USA. Univ Vermont, Coll Med, Burlington, VT 05405 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Wake Forest Univ, Sch Med, Winston Salem, NC 27109 USA. USA, Inst Surg Res, Ft Sam Houston, TX 78234 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2006 SI SI BP 117 EP 117 PG 1 WC Reproductive Biology SC Reproductive Biology GA 063ZW UT WOS:000239059500254 ER PT B AU Wilson, WC Atkinson, GM AF Wilson, W. C. Atkinson, G. M. GP IEEE TI Mixed modeling of a SAW delay line using VHDL SO BMAS 2006: PROCEEDINGS OF THE 2006 IEEE INTERNATIONAL BEHAVIORAL MODELING AND SIMULATION WORKSHOP LA English DT Proceedings Paper CT IEEE International Behavioral Modeling and Simulation Workshop CY SEP 14-15, 2006 CL San Jose, CA AB To aid in the development of SAW sensors for aerospace applications we have created a model of a SAW Delay line using VHDL. The model implements the Impulse Response method to calculate the frequency response, impedance, and insertion loss. The model includes optimization for the number of finger pairs in the IDTs and for the aperture height. This paper presents the model and the results from the model for a SAW delay line design. C1 [Wilson, W. C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Atkinson, G. M.] Virginia Commonwealth Univ, Richmond, VA 23284 USA. RP Wilson, WC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM william.c.wilson@nasa.gov; gmatkins@vcu.edu NR 12 TC 1 Z9 1 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-9742-8 PY 2006 BP 34 EP + PG 2 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BFI67 UT WOS:000242041200006 ER PT S AU Lund, EJ Farrugia, CJ Sandholt, PE Kistler, LM Fairfield, DH Gratton, FT Cowley, SWH Wild, JA MoulkiS, CG Dunlop, MW Reme, H Carlson, CW AF Lund, EJ Farrugia, CJ Sandholt, PE Kistler, LM Fairfield, DH Gratton, FT Cowley, SWH Wild, JA MoulkiS, CG Dunlop, MW Reme, H Carlson, CW BE Lakhina, GS TI The changing topology of the duskside magnetopause boundary layer in relation to IMF orientation SO BOUNDARY LAYERS, WAVES AND NON-LINEAR DYNAMICAL PROCESSES SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE boundary layers; solar wind-magnetosphere coupling; multispacecraft measurements; reconnection; Kelvin-Helmholtz instability ID DAYSIDE MAGNETOPAUSE; MAGNETIC-FIELD AB On 7 December 2000, Cluster made an extended outbound radial traversal of the duskside magnetopause boundary layer. The long duration of the crossing, during which Cluster spent several hours within 2R(E) of the nominal magnetopause, allows us to deconvolve the structure of this boundary layer in its dependence on interplanetary parameters. We present evidence that as the interplanetary magnetic field (IMF) changed in discontinuous jumps from southward to northward, the magnetic topology of the boundary layer evolved from open to closed. Reconnection signatures, including enhanced flows observed locally at Cluster and ion energy dispersion signatures observed by FAST near Cluster's magnetic footpoint, appeared while the IMF was southward. When the IMF turned nearly due northward, Cluster observed 75-s (Pc 4) oscillations which we attribute to the Kelvin-Helmholtz instability. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. Univ Oslo, Dept Phys, N-0316 Oslo, Norway. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Consejo Nacl Invest Cient & Tecn, INFIP, RA-1033 Buenos Aires, DF, Argentina. Univ Buenos Aires, Fac Ciencias Exactas & Nat, Buenos Aires, DF, Argentina. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. Ctr Etud Spatiale Rayonnements, F-31029 Toulouse, France. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Lund, EJ (reprint author), Univ New Hampshire, Ctr Space Sci, Morse Hall, Durham, NH 03824 USA. EM eric.lund@unh.edu NR 9 TC 2 Z9 3 U1 0 U2 1 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2006 VL 37 IS 3 BP 497 EP 500 DI 10.1016/j.asr.2004.11.035 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BEL22 UT WOS:000237702900008 ER PT S AU Uritsky, VM Klimas, AJ Vassilladis, D AF Uritsky, Vadim M. Klimas, Alexander J. Vassilladis, Dimitris BE Lakhina, GS TI Analysis and prediction of high-latitude geomagnetic disturbances based on a self-organized criticality framework SO BOUNDARY LAYERS, WAVES AND NON-LINEAR DYNAMICAL PROCESSES SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE substorms; fractal analysis; POLAR UVI; self-organized criticality; space weather ID AURORAL EMISSIONS; MAGNETOSPHERE; FLUCTUATIONS; EVOLUTION; INDEX AB The activity of Earth's magnetosphere is frequently dominated by sporadic perturbations involving broad ranges of spatial and temporal scales. This complex behavior has recently been shown to possess power-law intermittency statistics implying global and/ or local self-organized critical dynamics of the magnetotail plasma sheet. In the present paper, we show that under nonstationary driving conditions, the magnetosphere can deviate from its steady critical state. This transient dynamics is revealed based on spatial fractal analysis of critical fluctuations associated with multiscale turbulent activity in the tail. More specifically, we analyze multiscale correlations of an extended set of high-resolution ultraviolet images of the nighttime sector of the northern aurora provided by the UVI instrument onboard the POLAR spacecraft. The images are represented as an evolving activity surface characterized by a time-dependent roughness critical exponent. We show that the fractal structure of this surface undergoes a systematic reorganization during substorm phases. The expansion phase is typically preceded by a transition from sub- to super-critical behavior associated with enhanced correlations and decreased fractal dimension of the auroral activity surface. This transition manifests itself in increased values of the roughness exponent and the scaling error characterizing the quality of auroral emissions fractal scaling, as well as in the number of simultaneously observed emission events. The results obtained indicate that scaling analysis of critical auroral fluctuations can be a helpful tool for developing spatiotemporal prediction models of high-latitude geomagnetic activity. (C) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 St Petersburg State Univ, Inst Phys, St Petersburg 198904, Russia. NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. RP Uritsky, VM (reprint author), St Petersburg State Univ, Inst Phys, Ulyanovskaya 1, St Petersburg 198904, Russia. EM uritsky@geo.phys.spbu.ru NR 29 TC 16 Z9 16 U1 0 U2 1 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2006 VL 37 IS 3 BP 539 EP 546 DI 10.1016/j.asr.2004.12.059 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BEL22 UT WOS:000237702900015 ER PT B AU Flom, Y AF Flom, Yury BE Stephens, JJ Weil, KS TI ELECTRON BEAM BRAZING OF TITANIUM FOR CONSTRUCTION IN SPACE SO BRAZING AND SOLDERING, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Brazing and Soldering Conference CY APR 24-26, 2006 CL San Antonio, TX SP ASM Int, AWS AB An extended presence of humans in space requires an in-situ capability to construct various permanent structures to support scientific research, power generation, communication, radiation shielding and other functions. Electron Beam (EB) vacuum brazing has been identified as one of the best joining processes for in-space joining, particular for making a large quantity of permanent joints as required for construction of the sizeable truss structures. Thin wall titanium tubes are perhaps the best choice because of their high stiffness, excellent strength-to-weight ratio and great metal forming and joining ability. An innovative EB vacuum spot brazing process is being developed at Goddard Space Flight Center to be used for robotic as well as human-assisted construction in space. This paper describes experimental results obtained during the initial effort of EB brazing of titanium tubes with the special emphasis on low temperature aluminum filler metals. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Flom, Y (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. EM YURY.A.FLOM@NASA.GOV NR 9 TC 0 Z9 0 U1 0 U2 1 PU ASM INTERNATIONAL PI MATERIALS PARK PA 9503 KINSMAN RD, MATERIALS PARK, OH 44073 USA BN 978-0-87170-838-0 PY 2006 BP 1 EP 5 PG 5 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA BPY36 UT WOS:000280337000001 ER PT B AU Singh, M Shpargel, T Asthana, R Morscher, GN AF Singh, M. Shpargel, Tarah Asthana, Rajiv Morscher, Gregory N. BE Stephens, JJ Weil, KS TI Effect of Composite Substrate Properties on the Mechanical Behavior of Brazed Joints in Metal-Composite System SO BRAZING AND SOLDERING, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Brazing and Soldering Conference CY APR 24-26, 2006 CL San Antonio, TX SP ASM Int, AWS AB Advanced composite components are being considered for a wide variety of demanding applications in aerospace, space exploration, and ground-based systems. A number of these applications require robust integration technologies to join dissimilar materials (metal/composites) into complex structural components. In this study, three types of ceramic composites (C-C, C-SiC, and SiC-SiC) were vacuum brazed to commercially pure Ti using the Cusil-ABA (63Ag-35.3Cu-1.75Ti) active metal braze alloy. Composite substrates with as-fabricated and polished surfaces were used for brazing. The joint microstructure examined using scanning electron microscopy (SEM) showed sound metallurgical bonding in Ti/C-C and Ti/SiC-SiC joints. In Ti/C-SiC joints, interlaminar shear failure within the composite was observed although the joint interfaces appeared to be sound. The joint interface examination using the energy dispersive x-ray spectroscopy (EDS) showed Si and Ti enrichments at the Ti-side of the joints in all composites. No significant difference in the Knoop microhardness profiles in the Ti near the joint region was observed between polished and unpolished samples. However, the butt-strap tensile (BST) tests on bonded specimens at room temperature revealed a higher shear strength in joints made using polished SiC-SiC composite. These observations are discussed in the light of the wetting properties of the braze alloy, substrate composition, and interlaminar properties. C1 [Singh, M.; Shpargel, Tarah] NASA, Glenn Res Ctr, QSS Grp Inc, Cleveland, OH 44135 USA. RP Singh, M (reprint author), NASA, Glenn Res Ctr, QSS Grp Inc, MS 106-5, Cleveland, OH 44135 USA. EM msingh@grc.nasa.gov NR 21 TC 6 Z9 6 U1 1 U2 2 PU ASM INTERNATIONAL PI MATERIALS PARK PA 9503 KINSMAN RD, MATERIALS PARK, OH 44073 USA BN 978-0-87170-838-0 PY 2006 BP 246 EP 251 PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA BPY36 UT WOS:000280337000040 ER PT B AU Morscher, GN Singh, M Shpargel, T AF Morscher, Gregory N. Singh, Mrityunjay Shpargel, Tarah BE Stephens, JJ Weil, KS TI Comparison of Different Braze and Solder Materials for Joining Titanium to High-Conductivity C/C Composites SO BRAZING AND SOLDERING, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Brazing and Soldering Conference CY APR 24-26, 2006 CL San Antonio, TX SP ASM Int, AWS AB Joining titanium (Ti) and carbon-carbon (C/C) composites can be quite challenging due to thermo-elastic mismatch. However, several space-based applications require these types of joints. One approach under consideration is the use of conventional brazes and/or solders. A preliminary study into the effectiveness of several brazes and one solder was performed for bonding of Ti to high-conductivity carbon fiber (P120)-based C/C composites. Two types of joined structures were analyzed: Ti tubes joined to flat pieces of C/C and flat pieces of Ti joined to flat pieces of C/C. The former was used to determine the tensile load-carrying ability of the joints for a curved surface. The latter was used to determine the shear strength of the joints in the configuration of a butt-strap lap test. The factors relating to joint strength will be discussed including the effectiveness of braze/solder bonding and spreading and the thermal strains induced upon cooling of the structures from the processing (liquidus) temperature. C1 [Morscher, Gregory N.] NASA, Ohio Aerosp Inst, Glenn Res Ctr, Cleveland, OH USA. RP Morscher, GN (reprint author), NASA, Ohio Aerosp Inst, Glenn Res Ctr, Cleveland, OH USA. EM Gregory.N.Morscher@grc.nasa.gov NR 7 TC 3 Z9 3 U1 0 U2 2 PU ASM INTERNATIONAL PI MATERIALS PARK PA 9503 KINSMAN RD, MATERIALS PARK, OH 44073 USA BN 978-0-87170-838-0 PY 2006 BP 257 EP 261 PG 5 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA BPY36 UT WOS:000280337000042 ER PT J AU Higgins, W Ahijevych, D Amador, J Barros, A Berbery, EH Caetano, E Carbone, R Ciesielski, P Cifelli, R Cortez-Vazquez, M Douglas, A Douglas, M Emmanuel, G Fairall, C Gochis, D Gutzler, D Jackson, T Johnson, R King, C Lang, T Lee, MI Lettenmaier, D Lobato, R Magana, V Meiten, J Mo, K Nesbitt, S Ocampo-Torres, F Pytlak, E Rogers, P Rutledge, S Schemm, J Schubert, S White, A Williams, C Wood, A Zamora, R Zhang, CD AF Higgins, W Ahijevych, D Amador, J Barros, A Berbery, EH Caetano, E Carbone, R Ciesielski, P Cifelli, R Cortez-Vazquez, M Douglas, A Douglas, M Emmanuel, G Fairall, C Gochis, D Gutzler, D Jackson, T Johnson, R King, C Lang, T Lee, MI Lettenmaier, D Lobato, R Magana, V Meiten, J Mo, K Nesbitt, S Ocampo-Torres, F Pytlak, E Rogers, P Rutledge, S Schemm, J Schubert, S White, A Williams, C Wood, A Zamora, R Zhang, CD TI The NAME 2004 field campaign and modelling strategy SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID NORTH-AMERICAN MONSOON; CALIFORNIA MOISTURE SURGES; UNITED-STATES; PRECIPITATION; SYSTEM AB The North American Monsoon Experiment (NAME) is an internationally coordinated process study aimed at determining the sources and limits of predictability of warm-season precipitation over North America. The scientific objectives of NAME are to promote a better understanding and more realistic simulation of warm-season convective processes in complex terrain, intraseasonal variability of the monsoon, and the response of the warm-season atmospheric circulation and precipitation patterns to slowly varying, potentially predictable surface boundary conditions. During the summer of 2004, the NAME community implemented an international (United States, Mexico, Central America), multiagency (NOAA, NASA, NSF, USDA) field experiment called NAME 2004. This article presents early results from the NAME 2004 campaign and describes how the NAME modeling community will leverage the NAME 2004 data to accelerate improvements in warm-season precipitation forecasts for North America. C1 NOAA, NCEP, Climate Predict Ctr, 5200 Auth Rd,Room 605A, Camp Springs, MD 20746 USA. NCAR, Boulder, CO USA. Univ Costa Rica, San Jose, Costa Rica. Duke Univ, Durham, NC USA. Univ Maryland, College Pk, MD 20742 USA. Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. Colorado State Univ, Ft Collins, CO 80523 USA. Serv Meteorol Nacl, Mexico City, DF, Mexico. Creighton Univ, Omaha, NE 68178 USA. NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. UCAR, JOSS, Boulder, CO USA. NOAA, ETL, Boulder, CO USA. Univ New Mexico, Albuquerque, NM 87131 USA. ARS, USDA, Beltsville, MD USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Washington, Seattle, WA 98195 USA. Inst Mexicano Tecnol Agua, Jiutepec, Mexico. Ctr Invest Cient & Educ Super Ensenada, Ensenada, Baja California, Mexico. NWS, NOAA, Tucson, AZ USA. Univ Colorado, Boulder, CO 80309 USA. NOAA, Aeron Lab, Boulder, CO 80303 USA. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. RP NOAA, NCEP, Climate Predict Ctr, 5200 Auth Rd,Room 605A, Camp Springs, MD 20746 USA. EM Wayne.Higgins@noaa.gov RI Nesbitt, Stephen/A-9366-2008; Wood, Andrew/L-5133-2013; lettenmaier, dennis/F-8780-2011; Berbery, Ernesto/F-4560-2010; Williams, Christopher/A-2723-2015; Barros, Ana/A-3562-2011; Nesbitt, Stephen/I-3965-2013 OI Wood, Andrew/0000-0002-6231-0085; lettenmaier, dennis/0000-0003-3317-1327; Berbery, Ernesto/0000-0003-2587-3345; Williams, Christopher/0000-0001-9394-8850; Barros, Ana/0000-0003-4606-3106; Nesbitt, Stephen/0000-0003-0348-0452 NR 17 TC 48 Z9 48 U1 1 U2 14 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD JAN PY 2006 VL 87 IS 1 BP 79 EP 94 DI 10.1175/BAMS-87-1-79 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 009VB UT WOS:000235140400017 ER PT J AU Behar, A Matthews, J Venkateswaran, K Bruckner, J Jonsson, J AF Behar, Alberto Matthews, Jaret Venkateswaran, Kasthuri Bruckner, James Jonsson, Jonas TI A deep sea hydrothermal vent bio-sampler for large volume in-situ filtration of hydrothermal vent fluids SO CAHIERS DE BIOLOGIE MARINE LA English DT Article; Proceedings Paper CT 3rd International Symposium on Hydrothermal Vent and Seep Biology CY SEP 12-16, 2006 CL La Jolla, CA SP Natl Sci Fdn, Ridge 2000 Program, Scripps Inst Oceanog, Census Marine Life, NOAA Undersea Res Program, Minerals Management Serv, NOAAs Off Ocean Explorat, InterRidge, New EnglandBiolabs DE hydrothermal vents; water sampler; in situ filtration; high temperature; high pressure; pristine samples AB The Hydrothermal Vent BioSampler (HVB) currently being developed at the Jet Propulsion Laboratory is designed to collect large-volume hydrothermal vent samples, operating with fluid temperatures reaching 400 degrees C and at vent depths of up to 6,500 metres. The primary goal of the project is to collect 'pristine' samples untainted by the surrounding waters. Analysis of the collected samples can reveal the existence of thermophillic organisms within the vent fluid, extending the upper limits of life with respect to thermo-tolerance. Any biology found at such environments can contribute to research in astrobiology, while the technology developed for the system can contribute to bio-containment techniques useful for Arctic and planetary exploration. The HVB performs in-situ filtering of hydrothermal vent fluids to concentrate a large sample volume to a smaller volume more suitable for transport. The HVB system is currently in the development phase. This paper provides a physical description of the current system, as well as a summary of the preliminary tests conducted in 2005 and 2006: pressure chamber tests and a two dive operations at a hydrothermal vent off the northern coast of Iceland. C1 NASA, Jet Prop Lab, Pasadena, CA 91109 USA. Lulea Univ Technol, S-97187 Lulea, Sweden. RP Behar, A (reprint author), NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Alberto.Behar@jpl.nasa.gov NR 6 TC 5 Z9 5 U1 2 U2 3 PU CAHIERS DE BIOLOGIE MARINE PI ROSCOFF PA STATION BIOLOGIQUE PLACE GEORGES TEISSIER, 29680 ROSCOFF, FRANCE SN 0007-9723 J9 CAH BIOL MAR JI Cah. Biol. Mar. PY 2006 VL 47 IS 4 BP 443 EP 447 PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 129SV UT WOS:000243751300018 ER PT J AU Clancey, WJ AF Clancey, William J. BE Ericsson, KA Charness, N Feltovich, PJ Hoffman, RR TI Observation of Work Practices in Natural Settings SO CAMBRIDGE HANDBOOK OF EXPERTISE AND EXPERT PERFORMANCE LA English DT Article; Book Chapter DE Ethnography; Workplace Study; Practice; Participant Observation; Ethnomethodology; Lived Work ID DESIGN C1 NASA, Ames Res Ctr, Washington, DC 20546 USA. RP Clancey, WJ (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA. NR 70 TC 13 Z9 13 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-0-52184-097-2 PY 2006 BP 127 EP 145 D2 10.2277/ 0521600812 PG 19 WC Psychology, Multidisciplinary SC Psychology GA BXQ34 UT WOS:000296708200008 ER PT J AU Watson, KA Connell, JW AF Watson, Kent A. Connell, John W. BE Dai, L TI Polymer and carbon nanotube composites for space applications SO CARBON NANOTECHNOLOGY: RECENT DEVELOPMENTS IN CHEMISTRY, PHYSICS, MATERIALS SCIENCE AND DEVICE APPLICATIONS LA English DT Article; Book Chapter ID ORBIT ATOMIC OXYGEN; ENVIRONMENTALLY STABLE POLYIMIDES; POLY(ARYLENE ETHER HETEROCYCLE)S; ELECTROSTATIC CHARGE MITIGATION; OXIDE-CONTAINING POLYIMIDES; MECHANICAL-PROPERTIES; MATRIX COMPOSITES; RADIATION; EXPOSURE; COATINGS C1 [Watson, Kent A.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Connell, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Watson, KA (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA. NR 97 TC 3 Z9 3 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS BN 978-0-08-045932-5 PY 2006 BP 677 EP 698 DI 10.1016/B978-044451855-2/50022-X PG 22 WC Nanoscience & Nanotechnology; Physics, Condensed Matter SC Science & Technology - Other Topics; Physics GA BCQ51 UT WOS:000311028400021 ER PT S AU Bhartia, R Hug, WF Salas, EC Sijapati, K Lane, AL Reid, RD Conrad, PG AF Bhartia, R. Hug, W. F. Salas, E. C. Sijapati, K. Lane, A. L. Reid, R. D. Conrad, P. G. BE Gardner, PJ Fountain, AW TI Biochemical detection and identification false alarm rate dependence on wavelength using laser induced native fluorescence - art. no. 62180J SO Chemical and Biological Sensing VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Chemical and Biological Sensing VII CY APR 19-21, 2006 CL Kissimmee, FL SP SPIE DE native fluorescence; biological and chemical; detection and classification AB Most organic and many inorganic materials absorb strongly in specific wavelength ranges in the deep UV between about 220nm and 300nm. Excitation within these absorption bands results in native fluorescence emission. Each compound or composite material, such as a bacterial spore, has a unique excitation-emission fingerprint that can be used to provide information about the material. The sensitivity and specificity with which these materials can be detected and identified depends on the excitation wavelength and the number and location of observation wavelengths. We will present data on our deep ultraviolet Targeted Ultraviolet Chemical Sensors that demonstrate the sensitivity and specificity of the sensors. In particular, we will demonstrate the ability to quantitatively differentiate a wide range of biochemical agent targets against a wide range of background materials. We will describe the relationship between spectral resolution and specificity in target identification, as well as simple, fast, algorithms to identify materials. Hand-held, battery operated instruments using a deep UV laser and multi-band detection have been developed and deployed on missions to the Antarctic, the Arctic, and the deep ocean with the capability of detecting a single bacterial spore and to differentiate a wide range of organic and biological compounds. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bhartia, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Conrad, Pamela/F-1506-2012 OI Conrad, Pamela/0000-0001-8805-7981 NR 6 TC 3 Z9 3 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 0-8194-6274-8 J9 P SOC PHOTO-OPT INS PY 2006 VL 6218 BP J2180 EP J2180 AR 62180J DI 10.1117/12.674404 PG 9 WC Instruments & Instrumentation SC Instruments & Instrumentation GA BES56 UT WOS:000239300700017 ER PT J AU Krot, AN Yurimoto, H McKeegan, KD Leshin, L Chaussidon, M Libourel, G Yoshitake, M Huss, GR Guan, YB Zanda, B AF Krot, Alexander N. Yurimoto, Hisayoshi McKeegan, Kevin D. Leshin, Laurie Chaussidon, Marc Libourel, Guy Yoshitake, Miwa Huss, Gary R. Guan, Yunbin Zanda, Brigitte TI Oxygen isotopic compositions of chondrules: Implications for evolution of oxygen isotopic reservoirs in the inner solar nebula SO CHEMIE DER ERDE-GEOCHEMISTRY LA English DT Review DE oxygen isotopes; chondrules; refractory inclusions; chondrites; solar nebula ID ALUMINUM-RICH INCLUSIONS; UNEQUILIBRATED ENSTATITE CHONDRITES; CR CARBONACEOUS CHONDRITES; ALLENDE METEORITE; CV CHONDRITES; LOW-FEO; FERROMAGNESIAN CHONDRULES; CONTEMPORANEOUS FORMATION; REFRACTORY INCLUSIONS; PROTOPLANETARY DISK AB We review the oxygen isotopic compositions of minerals in chondrules and compound objects composed of a chondrule and a refractory inclusion, and bulk oxygen isotopic compositions of chondrules in unequilibrated ordinary, carbonaceous, enstatite, and Kakangari-like chondrites, focusing on data acquired using secondary ion mass-spectrometry and laser fluorination coupled with mass-spectrometry over the last decade. Most ferromagnesian chondrules from primitive (unmetamorphosed) chondrites are isotopically uniform (within 3-4 parts per thousand in Delta O-17) and depleted in O-16 (Delta O-17 > -7 parts per thousand) relative to amoeboid olivine aggregates (AOAs) and most calcium-aluminum-rich inclusions (CAIs) (Delta O-17 < -20 parts per thousand), suggesting that these classes of objects formed in isotopically distinct gaseous reservoirs, O-16-poor and O-16-rich, respectively. Chondrules uniformly enriched in O-16 (Delta O-17 < -15 parts per thousand) are exceptionally rare and have been reported only in CH chondrites. Oxygen isotopic heterogeneity in chondrules is mainly due to the presence of relict grains. These appear to consist of chondrules of earlier generations and rare refractory inclusions; with rare exceptions, the relict grains are O-16-enriched relative to chondrule phenocrysts and mesostasis. Within a chondrite group, the magnesium-rich (Type I) chondrules tend to be O-16-enriched relative to the ferrous (Type II) chondrules. Aluminum-rich chondrules in ordinary, enstatite, CR, and CV chondrites are generally O-16-enriched relative to ferromagnesian chondrules. No systematic differences in oxygen isotopic compositions have been found among these chondrule types in CB chondrites. Aluminum-rich chondrules in carbonaceous chondrites often contain relict refractory inclusions. Aluminum-rich chondrules with relict CAIs have heterogeneous oxygen isotopic compositions (Delta O-17 ranges from -20 parts per thousand to 0 parts per thousand). Aluminum-rich chondrules without relict CAIs are isotopically uniform and have oxygen isotopic compositions similar to, or approaching, those of ferromagnesian chondrules. Phenocrysts and mesostases of the CAI-bearing chondrules show no clear evidence for O-16-enrichment compared to the CAI-free chondrules. Spinel, hibonite, and forsterite of the relict refractory inclusions largely retained their original oxygen isotopic compositions. In contrast, plagioclase and melilite of the relict CAIs experienced melting and O-16-depletion to various degrees, probably due to isotopic exchange with an O-16-poor nebular gas. Several igneous CAIs experienced isotopic exchange with an O-16-poor nebular gas during late-stage remelting in the chondrule-forming region. On a three-isotope diagram, bulk oxygen isotopic compositions of most chondrules in ordinary, enstatite, and carbonaceous chondrites plot above, along, and below the terrestrial fractionation line, respectively. Bulk oxygen isotopic compositions of chondrules in altered and/or metamorphosed chondrites show evidence for mass-dependent fractionation, reflecting either interaction with a gaseous/fluid reservoir on parent asteroids or open-system thermal metamorphism. Bulk oxygen isotopic compositions of chondrules and oxygen isotopic compositions of individual minerals in chondrules and refractory inclusions from primitive chondrites plot along a common line of slope of similar to 1, suggesting that only two major reservoirs (ga and solids) are needed to explain the observed variations. However, there is no requirement that each had a permanently fixed isotopic composition. The absolute (Pb-207-Pb-206) and relative (Al-27-Mg-26) chronologies of CAIs and chondrules and the differences in oxygen isotopic compositions of most chondrules (O-16-poor) and most refractory inclusions (O-16-rich) can be interpreted in terms of isotopic self-shielding during UV photolysis of CO in the initially O-16-rich (Delta O-17 similar to-25 parts per thousand) parent molecular cloud or protoplanetary disk. According to these models, the UV photolysis preferentially dissociates (CO)-O-17 and (CO)-O-18 in the parent molecular cloud and in the peripheral zones of the protoplanetary disk. If this process occurs in the stability field of water ice, the released atomic O-17 and O-18 are incorporated into water ice, while the residual CO gas becomes enriched in O-16. During the earliest stages of evolution of the protoplanetary disk, the inner solar nebula had a solar H2O/CO ratio and was O-16-rich. During this time, AOAs and the O-16-rich CAIs and chondrules formed. Subsequently, the inner solar nebula became H2O- and O-16-depleted, because ice-rich dust particles, which were depleted in O-16, agglomerated outside the snowline (similar to 5AU), drifted rapidly towards the Sun and evaporated. During this time, which may have lasted for similar to 3 Myr, most chondrules and the O-16-depleted igneous CAIs formed. We infer that most chondrules formed from isotopically heterogeneous, but O-16-depleted precursors, and experienced isotopic exchange with an O-16-poor nebular gas during melting. Although the relative roles of the chondrule precursor materials and gas-melt isotopic exchange in establishing oxygen isotopic compositions of chondrules have not been quantified yet, mineralogical, chemical, and isotopic evidence indicate that Type I chondrules may have formed in chemical and isotopic equilibrium with nebular gas of variable isotopic composition. Whether these variations were spatial or temporal are not known yet. (C) 2006 Elsevier GmbH. All rights reserved. C1 Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. Hokkaido Univ, Sapporo, Hokkaido 0600810, Japan. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Ctr Rech Petrog & Geochim, CNRS, UPR2300, Nancy, France. INPL, Ecole Natl Super Geol, F-54501 Vandoeuvre Les Nancy, France. Kobe Univ, Dept Earth & Planetary Sci, Kobe, Hyogo 6578501, Japan. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Museum Natl Hist Nat, Lab Etud Mat Extraterr, F-75005 Paris, France. RP Krot, AN (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, 2525 Correa Rd, Honolulu, HI 96822 USA. EM sasha@soest.hawaii.edu RI McKeegan, Kevin/A-4107-2008; Zanda, Brigitte/D-6787-2015; UCLA, SIMS/A-1459-2011; Chaussidon, Marc/E-7067-2017 OI McKeegan, Kevin/0000-0002-1827-729X; Zanda, Brigitte/0000-0002-4210-7151; NR 142 TC 50 Z9 53 U1 2 U2 18 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0009-2819 J9 CHEM ERDE-GEOCHEM JI Chem Erde-Geochem. PY 2006 VL 66 IS 4 BP 249 EP 276 DI 10.1016/j.chemer.2006.07.002 PG 28 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 120QC UT WOS:000243098900001 ER PT J AU Gonthier, PL Story, SA Giacherio, BM Arevalo, RA Harding, AK AF Gonthier, P. L. Story, S. A. Giacherio, B. M. Arevalo, R. A. Harding, A. K. TI Developing radio beam geometry and luminosity models of pulsars SO CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS LA English DT Article; Proceedings Paper CT Lake Hanas International Pulsar Symposium 2005 CY AUG 02-07, 2005 CL Xinjiang, PEOPLES R CHINA SP Urumqui Observatory, Natl Astron Observatories, Chinese Acad Sci, Natl Nat Sci Fdn China, Chinese Astron Soc, Key Lab Radio Astron Chinese Acad Sci, Foreign Experts Bureau Xinjiang Uygar Autonomous Reg, Xinjiang Assoc Sci & Technol DE radiation mechanisms : non-thermal; stars : magnetic fields; stars : neutron; pulsars : general ID GAMMA-RAY PULSARS; EMISSION; SHAPE AB Our recent studies of pulsar population statistics suggest that improvements of radio and gamma-ray beam geometry and luminosity models require further refinement. The goal of this project is to constrain the viewing geometry for some radio pulsars, especially three-peaked pulse profiles, in order to limit the uncertainty of the magnetic inclination and impact angles. We perform fits of the pulse profile and position angle sweep of radio pulsars for the available frequencies. We assume a single core and conal beams described by Gaussians. We incorporate three different size cones with frequency dependence from the work of Mitra & Deshpande (1999). We obtain separate spectral indices for the core and cone beams and explore the trends of the ratio of core to cone peak fluxes. This ratio is observed to have some dependence with period. However, we cannot establish the suggested functional form of this ratio as indicated by the work of Arzoumanian, Chernoff & Cordes (2002). C1 Hope Coll, Dept Phys, Holland, MI 49424 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Gonthier, PL (reprint author), Hope Coll, Dept Phys, 27 Graves Pl, Holland, MI 49424 USA. EM gonthier@hope.edu RI Harding, Alice/D-3160-2012 NR 14 TC 5 Z9 5 U1 0 U2 0 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1009-9271 J9 CHINESE J ASTRON AST JI Chin. J. Astron. Astrophys. PY 2006 VL 6 SU 2 BP 97 EP 104 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156EX UT WOS:000245632000023 ER PT J AU Steinle, H Bhat, NP Briggs, MS Connaughton, V Diehl, R Fishman, GJ Greiner, J Kippen, RM von Kienlin, A Kouveliotou, C Lichti, GG Meegan, CA Paciesas, WS Preece, RD Wilson, RB AF Steinle, Helmut Bhat, N. P. Briggs, M. S. Connaughton, V. Diehl, R. Fishman, G. J. Greiner, J. Kippen, R. M. von Kienlin, A. Kouveliotou, C. Lichti, G. G. Meegan, C. A. Paciesas, W. S. Preece, R. D. Wilson, R. B. TI Measurements of Gamma-Ray Bursts with GLAST SO CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS LA English DT Article; Proceedings Paper CT 14th International Carotenoid Symposium CY JUL 20-25, 2005 CL Edinburgh, SCOTLAND DE instrumentation : detectors; gamma-rays : bursts ID 28 FEBRUARY 1997; ERROR BOX; SUPERNOVA; DISCOVERY; MISSION; MODELS AB The next large NASA mission in the field of gamma-ray astronomy is the Gamma-Ray Large Area Space Telescope (GLAST), which is scheduled for a launch end of 2007. This satellite consists of the main instrument LAT (Large-Area Telescope) which is sensitive in the energy range between 10 MeV and > 300 GeV, and a secondary instrument, the Gamma-Ray Burst Monitor (GBM), sensitive from 10 keV to 30 MeV. This omnidirectional monitor is an important instrument for gamma-ray burst (GRB) science with GLAST, as it provides the link between the majority of the gamma-ray busts emitting at lower energies and the high-energy events of gamma-ray bursts and other transients. It will also serve as a trigger to increase the detection rate of gamma-ray burst with the LAT. The GBM will provide real-time burst locations over a wide field-of-view (FoV) with sufficient accuracy to repoint the whole GLAST spacecraft. Time-resolved spectra of bursts recorded with LAT and the burst monitor will allow the investigation of the relation between the keV and the MeV-GeV emission from GRBs over seven decades in energy and will provide new insights into the physics of GRBs in general. In addition, the excellent localization of GRBs by the LAT will stimulate follow-up observations at other wavelengths which may yield clues about the nature of the burst sources. C1 Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Alabama, Huntsville, AL 35899 USA. Los Alamos Natl Lab, ISR 2, Los Alamos, NM USA. RP Steinle, H (reprint author), Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. EM hcs@mpe.mpg.de NR 16 TC 3 Z9 4 U1 0 U2 0 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1009-9271 J9 CHINESE J ASTRON AST JI Chin. J. Astron. Astrophys. PY 2006 VL 6 SU 1 SI SI BP 365 EP 368 DI 10.1088/1009-9271/6/S1/48 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 138VX UT WOS:000244392500066 ER PT J AU Bloser, PF Ryan, JM McConnell, ML Macri, JR Bravar, U Kanbach, G Andritschke, R Ajello, M Zoglauer, A Hunter, SD Phlips, BF Wulf, EA Hartmann, DH Miller, RS Paciesas, WS Zych, AD Kippen, RM Vestrand, T Cherry, ML Guzik, TG Stacy, JG Wefel, JP Reglero, V Di Cocco, G Cravens, JP AF Bloser, P. F. Ryan, J. M. McConnell, M. L. Macri, J. R. Bravar, U. Kanbach, G. Andritschke, R. Ajello, M. Zoglauer, A. Hunter, S. D. Phlips, B. F. Wulf, E. A. Hartmann, D. H. Miller, R. S. Paciesas, W. S. Zych, A. D. Kippen, R. M. Vestrand, T. Cherry, M. L. Guzik, T. G. Stacy, J. G. Wefel, J. P. Reglero, V. Di Cocco, G. Cravens, J. P. TI The MEGA project for Medium Energy Gamma-ray Astronomy SO CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS LA English DT Article; Proceedings Paper CT 14th International Carotenoid Symposium CY JUL 20-25, 2005 CL Edinburgh, SCOTLAND DE gamma-rays : observations; instrumentation : detectors; instrumentation : polarimeters; space vehicles : instruments ID TELESCOPE; CALIBRATION; PROTOTYPE AB The Medium Energy Gamma-ray Astronomy (MEGA) telescope concept will soon be proposed as a MIDEX mission. This mission would enable a sensitive all-sky survey of the medium-energy gamma-ray sky (0.4-50 MeV) and bridge the huge sensitivity gap between the COMPTEL and OSSE experiments on the Compton Gamma Ray Observatory and the visionary Advanced Compton Telescope (ACT) mission. The scientific goals include compiling a much larger catalog of sources in this energy range, performing far deeper searches for supernovae, better measuring the galactic continuum and line emissions, and identifying the components of the cosmic diffuse gamma-ray emission. MEGA records and images gamma rays by completely tracking Compton and pair creation events in a stack of double-sided Si strip detectors surrounded by a pixellated CsI calorimeter. A prototype instrument has been developed and calibrated in the laboratory and at a gamma-ray beam facility. We present calibration results from the prototype and describe the proposed satellite mission. C1 Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. USN, Res Lab, Washington, DC 20375 USA. Clemson Univ, Dept Phys, Clemson, SC USA. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. Univ Calif Riverside, Inst Geophys & Planetary Phys, Riverside, CA 92521 USA. Los Alamos Natl Lab, Los Alamos, NM USA. Louisiana State Univ, Dept Phys, Baton Rouge, LA 70803 USA. Univ Valencia, Grp Astron & Ciencias Espacio, Valencia, Spain. Ist Astrofis Spaziale & Fis Cosm, Bologna, Italy. SW Res Inst, San Antonio, TX USA. RP Bloser, PF (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM Peter.Bloser@unh.edu RI Wulf, Eric/B-1240-2012; Hunter, Stanley/D-2942-2012 NR 13 TC 1 Z9 1 U1 0 U2 3 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1009-9271 J9 CHINESE J ASTRON AST JI Chin. J. Astron. Astrophys. PY 2006 VL 6 SU 1 SI SI BP 388 EP 392 DI 10.1088/1009-9271/6/S1/53 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 138VX UT WOS:000244392500073 ER PT J AU Wang, HM Song, H Jing, J Yurchyshyn, V Deng, YY Zhang, HQ Falconer, D Li, J AF Wang, Hai-Min Song, Hui Jing, Ju Yurchyshyn, Vasyl Deng, Yuan-Yong Zhang, Hong-Qi Falconer, David Li, Jing TI The relationship between magnetic gradient and magnetic shear in five super active regions producing great flares SO CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS LA English DT Article DE Sun : activity; Sun : flares; Sun : magnetic fields; Sun : coronal mass ejections (CMEs) ID 2000 JULY 14; IMAGING VECTOR MAGNETOGRAPH; ROPE STRUCTURE; DELTA-SPOTS; SOLAR-FLARE; EVOLUTION AB We study the magnetic structure of five well-known active regions that produced great flares (X5 or larger). The six flares under investigation are the X12 flare on 1991 June 9 in AR 6659, the X5.7 flare on 2000 July 14 in AR 9077, the X5.6 flare on 2001 April 6 in AR 9415, the X5.3 flare on 2001 August 25 in AR 9591, the X17 flare on 2003 October 28 and the X 10 flare on 2003 October 29, both in AR 10486. The last five events had corresponding LASCO observations and were all associated with Halo CMEs. We analyzed vector magnetograms from Big Bear Solar Observatory, Huairou Solar Observing Station, Marshall Space Flight Center and Mees Solar Observatory. In particular, we studied the magnetic gradient derived from line-of-sight magnetograms and magnetic shear derived from vector magnetograms, and found an apparent correlation between these two parameters at a level of about 90%. We found that the magnetic gradient could be a better proxy than the shear for predicting where a major flare might occur: all six flares occurred in neutral lines with maximum gradient. The mean gradient of the flaring neutral lines ranges from 0.14 to 0.50 G km(-1), 2.3 to 8 times the average value for all the neutral lines in the active regions. If we use magnetic shear as the proxy, the flaring neutral line in at least one, possibly two, of the six events would be mis-identified. C1 Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Wang, HM (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. EM haimin@flare.njit.edu NR 27 TC 18 Z9 19 U1 0 U2 0 PU SCIENCE CHINA PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1009-9271 J9 CHINESE J ASTRON AST JI Chin. J. Astron. Astrophys. PY 2006 VL 6 IS 4 BP 477 EP 488 DI 10.1088/1009-9271/6/4/11 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075RL UT WOS:000239902800011 ER PT J AU Renssen, H Goosse, H Muscheler, R AF Renssen, H. Goosse, H. Muscheler, R. TI Coupled climate model simulation of Holocene cooling events: oceanic feedback amplifies solar forcing SO CLIMATE OF THE PAST LA English DT Article ID NORTH-ATLANTIC CLIMATE; MAUNDER MINIMUM; VEGETATION MODEL; HIGH-RESOLUTION; WESTERN NORWAY; CARBON-CYCLE; NORDIC SEAS; VARIABILITY; ATMOSPHERE; RECORD AB The coupled global atmosphere-ocean-vegetation model ECBilt-CLIO-VECODE is used to perform transient simulations of the last 9000 years, forced by variations in orbital parameters, atmospheric greenhouse gas concentrations and total solar irradiance (TSI). The objective is to study the impact of decadal-to-centennial scale TSI variations on Holocene climate variability. The simulations show that negative TSI anomalies increase the probability of temporary relocations of the site with deepwater formation in the Nordic Seas, causing an expansion of sea ice that produces additional cooling. The consequence is a characteristic climatic anomaly pattern with cooling over most of the North Atlantic region that is consistent with proxy evidence for Holocene cold phases. Our results thus suggest that the ocean is able to play an important role in amplifying centennial-scale climate variability. C1 Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands. Catholic Univ Louvain, Inst Astron & Geophys G Lemaitre, B-1348 Louvain, Belgium. NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA. RP Renssen, H (reprint author), Vrije Univ Amsterdam, Fac Earth & Life Sci, De Boelelaan 1085, NL-1081 HV Amsterdam, Netherlands. EM hans.renssen@geo.falw.vu.nl RI Renssen, Hans/C-9927-2010 NR 75 TC 51 Z9 52 U1 2 U2 8 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1814-9324 EI 1814-9332 J9 CLIM PAST JI Clim. Past. PY 2006 VL 2 IS 2 BP 79 EP 90 PG 12 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA 140LK UT WOS:000244506500002 ER PT B AU Kennedy, B Okon, A Aghazarian, H Garrett, M Huntsberger, T Magnone, L Robinson, M Townsend, J AF Kennedy, Brett Okon, Avi Aghazarian, Hrand Garrett, Mike Huntsberger, Terry Magnone, Lee Robinson, Matthew Townsend, Julie BE Tokhi, MO Virk, GS Hossain, MA TI The Lemur II-class robots for inspection and maintenance of orbital structures: A system description SO CLIMBING AND WALKING ROBOTS LA English DT Proceedings Paper CT 8th International Conference on Climbing and Walking Robots (CLAWAR 2005) CY SEP 13-15, 2005 CL London, ENGLAND DE limbs; space; assembly; inspection; modular AB The assembly, inspection, and maintenance requirements of permanent installations in space demand robots that provide a high level of operational flexibility relative to mass and volume. Such demands point to robots that are dexterous, have significant processing and sensing capabilities, and can be easily reconfigured (both physically and algorithmically). Evolving from Lemur I, Lemur Ha is an extremely capable system that both explores mechanical design elements and provides an infrastructure for the development of algorithms (such as force control for mobility and manipulation and adaptive visual feedback). The physical layout of the system consists of six, 4-degree-of-freedom limbs arranged axisymmetrically about a hexagonal body platform. These limbs incorporate a "quick-connect" end-effector feature below the distal Joint that allows the rapid change-out of any of its tools. The other major subsystem is a stereo camera set that travels along a ring track, allowing omnidirectional vision. The current Lemur IIa platform represents the jumping-off point toward more advanced robotic platforms that will support NASA's Vision for Space Exploration, which calls for a sustained presence in space. This paper lays out the mechanical, electrical, and algorithmic elements of Lemur Ha and discusses the future directions of development in those areas. C1 [Kennedy, Brett; Okon, Avi; Aghazarian, Hrand; Garrett, Mike; Huntsberger, Terry; Magnone, Lee; Robinson, Matthew; Townsend, Julie] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Kennedy, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Brett.A.Kennedy@jpl.nasa.gov FU Jet Propulsion Laboratory California Institute of Technology; National Aeronautics and Space Administration FX The research described in this (publication or paper) was carried out at the Jet Propulsion Laboratory California Institute of Technology under a contract with the National Aeronautics and Space Administration. NR 7 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-26413-2 PY 2006 BP 1069 EP 1076 DI 10.1007/3-540-26415-9_128 PG 8 WC Robotics SC Robotics GA BEF01 UT WOS:000237058000128 ER PT B AU Kennedy, B Okon, A Aghazarian, H Badescu, M Bao, XQ Bar-Cohen, Y Chang, ZS Dabiri, BE Garrett, M Magnone, L Sherrit, S AF Kennedy, Brett Okon, Avi Aghazarian, Hrand Badescu, Mircea Bao, Xiaoqi Bar-Cohen, Yoseph Chang, Zensheu Dabiri, Borna E. Garrett, Mike Magnone, Lee Sherrit, Stewart BE Tokhi, MO Virk, GS Hossain, MA TI Lemur IIb: a robotic system for steep terrain access SO CLIMBING AND WALKING ROBOTS LA English DT Proceedings Paper CT 8th International Conference on Climbing and Walking Robots (CLAWAR 2005) CY SEP 13-15, 2005 CL London, ENGLAND DE climbing; steep terrain; drilling; autonomy; force control AB To extract the full science potential from planetary surface operations, robots must be able to access the entire surface of the planetary body, not just the relatively level areas. Buoyed by the success of top-to-bottom strategies employing tethered robots, the stage is set for bottom-to-top technologies and techniques to be investigated. To this end, we have designed and built Lemur IIb, a 4-limbed robotic system that is being used to investigate several aspects of climbing system design including the mechanical system (novel end-effectors, kinematics, joint design), sensing (force, attitude, vision), low-level control (force-control for tactile sensing and stability management), and planning (joint trajectories for stability). The technologies developed on this platform will be used to build an advanced system that will climb slopes up to and including vertical faces and overhangs and be able to react forces to maintain stability and do useful work (e.g., sample acquisition/instrument placement). Among the most advanced of these technologies is a new class of Ultrasonic/Sonic Driller/Corer (USDC) end-effectors capable of creating "holds" in rock and soil as well as sampling those substrates. This paper lays out the mechanical, electrical, and algorithmic elements of the Lemur Hb robot and discusses the future directions of development in those areas. C1 [Kennedy, Brett; Okon, Avi; Aghazarian, Hrand; Badescu, Mircea; Bao, Xiaoqi; Bar-Cohen, Yoseph; Chang, Zensheu; Dabiri, Borna E.; Garrett, Mike; Magnone, Lee; Sherrit, Stewart] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Kennedy, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM brett.a.kennedy@jpl.nasa.gov NR 12 TC 0 Z9 0 U1 0 U2 2 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-26413-2 PY 2006 BP 1077 EP 1084 DI 10.1007/3-540-26415-9_129 PG 8 WC Robotics SC Robotics GA BEF01 UT WOS:000237058000129 ER PT J AU Harstad, K Bellan, J AF Harstad, K Bellan, J TI Global analysis and parametric dependencies for potential unintended hydrogen-fuel releases SO COMBUSTION AND FLAME LA English DT Article DE hydrogen-safety global analysis ID NUMERICAL SIMULATIONS; DIFFUSION FLAMES; DEFLAGRATION; DETONATION; JET; TRANSITION; STORAGE; FLOWS; EXPLOSIONS; RADIATION AB Global, simplified analyses of gaseous-hydrogen releases from a high-pressure vessel and liquid-hydrogen pools are conducted for two purposes: (1) establishing order-of-magnitude values of characteristic times and (2) determining parametric dependencies of these characteristic times on the physical properties of the configuration and on the thermophysical properties of hydrogen. According to the ratio of the characteristic release time to the characteristic mixing time, two limiting configurations are identified: (1) a rich cloud exists when this ratio is much smaller than unity, and (2) a jet exists when this ratio is much larger than unity. In all cases, it is found that the characteristic release time is proportional to the total released mass and inversely proportional to a characteristic area. The approximate size, convection velocity, and circulation time of unconfined burning-cloud releases scale with the cloud mass at powers 1/3, 1/6, and 1/6, respectively, multiplied by an appropriately dimensional constant; the influence of cross flow can only be important if its velocity exceeds that of internal convection. It is found that the fireball lifetime is approximately the maximum of the release time and thrice the convection-associated characteristic time. Transition from deflagration to detonation can occur only if the size of unconfined clouds exceeds by a factor of 0(l 0) that of a characteristic detonation cell, which ranges from 0.015 in under stoichiometric conditions to approximately I m under extreme rich/lean conditions. For confined vapor pockets, transition occurs only for pocket sizes larger than the cell size. In jets, the release time is inversely proportional to the initial vessel pressure and has a square root dependence on the vessel temperature. Jet velocities are a factor of 10 larger than convective velocities in fireballs and combustion is possible only in the subsonic, downstream region where entrainment may occur. (c) 2005 The Combustion Institute. Published by Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bellan, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 125-109, Pasadena, CA 91109 USA. EM josette.bellan@jpl.nasa.gov NR 31 TC 15 Z9 15 U1 1 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0010-2180 J9 COMBUST FLAME JI Combust. Flame PD JAN PY 2006 VL 144 IS 1-2 BP 89 EP 102 DI 10.1016/j.combustflame.2005.07.005 PG 14 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical SC Thermodynamics; Energy & Fuels; Engineering GA 002CF UT WOS:000234588300008 ER PT J AU Bellan, J AF Bellan, J TI Theory, modeling and analysis of turbulent supercritical mixing SO COMBUSTION SCIENCE AND TECHNOLOGY LA English DT Article DE high-pressure turbulence; mixing ID DIRECT NUMERICAL SIMULATIONS; MASS DIFFUSION-COEFFICIENTS; DENSITY INTERFACE; BOUNDARY-CONDITIONS; SHEAR-LAYER; BINARY; PRESSURE; FLUID; NITROGEN; HEPTANE AB Previous studies of supercritical three-dimensional mixing layers are reviewed to derive a unified understanding of supercritical turbulence and mixing. These studies consisted of Direct Numerical Simulations of mixing layers having initially a single chemical species in each of the two free streams. Each mixing layer was initially perturbed, which led to a double pairing of four initial spanwise vortices. These pairings yielded in each case an ultimate vortex within which small scales proliferated, resulting in a state having turbulence characteristics, called a transitional state. The evolution of the layer to this transitional state and the state itself were previously analyzed to elucidate the features of supercritical turbulence and mixing. This analysis is here used to classify those supercritical turbulent mixing characteristics that are species-system independent or species-system dependent. Finally, comments are offered on future prospects of developing small-scale models particularly suited for Large Eddy Simulations of supercritical turbulent mixing. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bellan, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM josette.bellan@jpl.nasa.gov NR 51 TC 41 Z9 41 U1 0 U2 10 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0010-2202 J9 COMBUST SCI TECHNOL JI Combust. Sci. Technol. PD JAN PY 2006 VL 178 IS 1-3 BP 253 EP 281 DI 10.1080/00102200500292241 PG 29 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical SC Thermodynamics; Energy & Fuels; Engineering GA 993XY UT WOS:000233993000009 ER PT B AU Barth, T AF Barth, Timothy BE Arnold, DN Boche, PB Lehoucq, RB Nicolaides, RA Shashkov, M TI On the role of involutions in the discontinuous Galerkin discretization of Maxwell and magnetohydrodynamic systems SO COMPATIBLE SPATIAL DISCRETIZATIONS SE IMA Volumes in Mathematics and its Applications LA English DT Proceedings Paper CT IMA Hot Topics Workshop on Compatible Spatial Discretizations CY MAY 11-15, 2004 CL Univ Minnesota, Minneapolis, MN SP IMA HO Univ Minnesota DE nonlinear conservation laws; energy stability; Maxwell equations; magnetohydrodynamics; symmetrization; discontinuous Galerkin finite element method ID FINITE-ELEMENT METHOD; HYPERBOLIC CONSERVATION-LAWS; NUMERICAL-SOLUTION; EQUATIONS AB The role of involutions in energy stability of the discontinuous Galerkin (DG) discretization of Maxwell and magnetohydrodynamic (MHD) systems is examined. Important differences are identified in the symmetrization of the Maxwell and MHD systems that impact the construction of energy stable discretizations using the DG method. Specifically, general sufficient conditions to be imposed on the DC numerical flux and approximation space are given so that energy stability is retained. These sufficient conditions reveal the favorable energy consequence of imposing continuity in the normal component of the magnetic induction field at interelement boundaries for MHD discretizations. Counterintuitively, this condition is not required for stability of Maxwell discretizations using the discontinuous Galerkin method. C1 [Barth, Timothy] NASA, Ames Res Ctr, MS T27A-1, Moffett Field, CA 94035 USA. RP Barth, T (reprint author), NASA, Ames Res Ctr, MS T27A-1, Moffett Field, CA 94035 USA. EM Timothy.J.Barth@nasa.gov NR 33 TC 10 Z9 10 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 0-387-30916-0 J9 IMA VOL MATH APPL PY 2006 VL 142 BP 69 EP + PG 4 WC Mathematics, Applied SC Mathematics GA BEX78 UT WOS:000240040100004 ER PT S AU Wolpert, DH AF Wolpert, David H. BE Namatame, A Kaizouji, T Aruka, Y TI What Information Theory Says About Bounded Rational Best Response SO COMPLEX NETWORKS OF ECONOMIC INTERACTIONS: ESSAYS IN AGENT-BASED ECONOMICS AND ECONOPHYSICS SE Lecture Notes in Economics and Mathematical Systems LA English DT Article; Book Chapter AB Probability Collectives (PC) provides the information-theoretic extension of conventional full-rationality game theory to bounded rational games. Here an explicit solution to the equations giving the bounded rationality equilibrium of a game is presented. Then PC is used to investigate games in which the players use bounded rational best-response strategies. Next it is shown that in the continuum-time limit, bounded rational best response games result in a variant of the replicator dynamics of evolutionary game theory. It is then shown that for team (shared-payoff) games, this variant of replicator dynamics is identical to Newton-Raphson iterative optimization of the shared utility function. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wolpert, DH (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM dhw@email.arc.nasa.gov NR 29 TC 1 Z9 2 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0075-8442 BN 978-3-540-28727-8 J9 LECT NOTES ECON MATH PY 2006 VL 567 BP 293 EP 306 D2 10.1007/3-540-28727-2 PG 14 WC Economics; Mathematics, Interdisciplinary Applications SC Business & Economics; Mathematics GA BLL76 UT WOS:000270461100021 ER PT J AU Camanho, PP Davila, CG Pinho, ST Iannucci, L Robinson, P AF Camanho, PP Davila, CG Pinho, ST Iannucci, L Robinson, P TI Prediction of in situ strengths and matrix cracking in composites under transverse tension and in-plane shear SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING LA English DT Article; Proceedings Paper CT 2nd International Conference on Composites Testing and Model Identification (CompTest 200) CY SEP 21-23, 2004 CL Univ Bristol, Bristol, ENGLAND HO Univ Bristol DE failure criterion; in situ strengths; fracture ID THERMOMECHANICAL CONSTITUTIVE THEORY; CURRENT FAILURE THEORIES; LAMINATED COMPOSITES; STIFFNESS REDUCTION; DISTRIBUTED DAMAGE; ELASTIC COMPOSITES; CAPABILITIES; EXERCISE; GRAPHITE AB A criterion for matrix failure of laminated composite plies in transverse tension and in-plane shear is developed by examining the mechanics of transverse matrix crack growth. Matrix cracks are assumed to initiate from manufacturing defects and can propagate within planes parallel to the fiber direction and normal to the ply mid-plane. Fracture mechanics models of cracks in unidirectional laminates, embedded plies and outer plies are used to determine the onset and direction of propagation of crack growth. The models for each ply configuration relate ply thickness and ply toughness to the corresponding in situ ply strength. Calculated results for several materials are shown to correlate well with experimental results. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ Porto, Fac Engn, DEMEGI, P-4200465 Oporto, Portugal. NASA, Langley Res Ctr, Hampton, VA 23666 USA. Univ London Imperial Coll Sci & Technol, Dept Aeronaut, London SW7 2BY, England. RP Camanho, PP (reprint author), Univ Porto, Fac Engn, DEMEGI, Rua Dr Roberto Frias, P-4200465 Oporto, Portugal. EM pcamanho@fe.up.pt RI Pinho, Silvestre/B-4618-2012; Davila, Carlos/D-8559-2011; OI Pinho, Silvestre/0000-0001-5727-7041; Camanho, Pedro/0000-0003-0363-5207 NR 39 TC 112 Z9 115 U1 3 U2 28 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1359-835X J9 COMPOS PART A-APPL S JI Compos. Pt. A-Appl. Sci. Manuf. PY 2006 VL 37 IS 2 BP 165 EP 176 DI 10.1016/j.compositesa.2005.04.023 PG 12 WC Engineering, Manufacturing; Materials Science, Composites SC Engineering; Materials Science GA 020SQ UT WOS:000235931100003 ER PT J AU Ghose, S Watson, KA Delozier, DM Working, DC Siochi, EJ Connell, JW AF Ghose, S Watson, KA Delozier, DM Working, DC Siochi, EJ Connell, JW TI Incorporation of multi-walled carbon nanotubes into high temperature resin using dry mixing techniques SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING LA English DT Article DE nanostructure; polymer matrix composites; thermosetting resin; extrusion ID BALL-MILLED CARBON; COMPOSITES; PHENYLETHYNYL; FABRICATION; MORPHOLOGY; BEHAVIOR; BLENDS AB As part of an ongoing effort to develop multi-functional advanced composites, blends of PETI-330 and multi-walled carbon nanotubes (MWNTs) were prepared and characterized. Dry mixing techniques were employed and the maximum loading level of the MWNT chosen was based primarily on its effect on melt viscosity. The PETI-330/MWNT mixtures were prepared at concentrations ranging from 3 to 25 wt%. The resulting powders were characterized for homogeneity, thermal and rheological properties and extrudability as continuous fibers. Based on the characterization results, samples containing 10, 15 and 20 wt% MWNTs were chosen for more comprehensive evaluation. Samples were also prepared using in situ polymerization and solution mixing techniques and their properties were compared with the ball-mill prepared samples. The significance of this research is that high loading levels of MWCNTs were added to a high temperature matrix without affecting the processing characteristics of the resin. The preparation and characterization of PETI-330/MWNT nanocomposites are discussed herein. (c) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. NASA, LaRC, Natl Res Council Res Associate, Hampton, VA 23681 USA. Natl Inst Aerosp, Hampton, VA 23666 USA. RP Connell, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM john.w.connell@nasa.gov NR 35 TC 24 Z9 24 U1 0 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1359-835X J9 COMPOS PART A-APPL S JI Compos. Pt. A-Appl. Sci. Manuf. PY 2006 VL 37 IS 3 BP 465 EP 475 DI 10.1016/j.compositesa.2005.03.033 PG 11 WC Engineering, Manufacturing; Materials Science, Composites SC Engineering; Materials Science GA 019GZ UT WOS:000235824900011 ER PT J AU Gyekenyesi, AL Morscher, GN Cosgriff, LM AF Gyekenyesi, AL Morscher, GN Cosgriff, LM TI In situ monitoring of damage in SiC/SiC composites using acousto-ultrasonics SO COMPOSITES PART B-ENGINEERING LA English DT Article DE non-destructive testing; mechanical testing; ultrasonics; damage tolerance ID MATRIX COMPOSITES; MECHANICS; CRACKING; WAVES AB Acousto-ultrasonics (AU) is a nondestructive evaluation (NDE) technique that utilizes two ultrasonic transducers to interrogate the condition of a test specimen. The sending transducer introduces an ultrasonic pulse at a point on the surface of the specimen while a receiving transducer detects the signal after it has passed through the material. The aim of the method is to correlate certain empirical parameters of the detected waveform to characteristics of the material between the two transducers. The waveform parameter of interest is the attenuation due to internal damping for which information is being garnered from the frequency domain. Here, the three parameters utilized to indirectly quantify the attenuation are the ultrasonic decay rate, the mean square value of the power spectrum, and the centroid of the power spectrum. The sensitivity for each of these AU parameters was assessed with respect to the damage state of two types of SiC/SiC ceramic matrix composites (CMC). The two composite systems both had Hi-Nicalon (TM) fibers with a carbon interface but had different matrix compositions that led to considerable differences in damage accumulation. Load/unload/reload tensile tests were performed and in situ AU measurements were made over the entire stress range. After analyzing the AU parameters, the overall sensitivity of the AU technique to material change or damage was quantified and shown to correlate well with the observed damage mechanisms for both material systems. In addition, the AU response was shown to be dependent on the stress state of the composites. This stress dependent behavior was observed while unloading the specimens from the maximum stress, thereby, maintaining a constant damage state. (c) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr, OAI, Cleveland, OH 44135 USA. Cleveland State Univ, NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Gyekenyesi, AL (reprint author), NASA, Glenn Res Ctr, OAI, 21000 Brookpk Rd MS 6-1, Cleveland, OH 44135 USA. EM andrew.l.gyekenyesi@grc.nasa.gov NR 22 TC 20 Z9 20 U1 2 U2 19 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1359-8368 J9 COMPOS PART B-ENG JI Compos. Pt. B-Eng. PY 2006 VL 37 IS 1 BP 47 EP 53 DI 10.1016/j.compositesb.2005.05.010 PG 7 WC Engineering, Multidisciplinary; Materials Science, Composites SC Engineering; Materials Science GA 967LS UT WOS:000232093300006 ER PT J AU Hadjiev, VG Lagoudas, DC Oh, ES Thakre, P Davis, D Files, BS Yowell, L Arepalli, S Bahr, JL Tour, JM AF Hadjiev, VG Lagoudas, DC Oh, ES Thakre, P Davis, D Files, BS Yowell, L Arepalli, S Bahr, JL Tour, JM TI Buckling instabilities of octadecylamine functionalized carbon nanotubes embedded in epoxy SO COMPOSITES SCIENCE AND TECHNOLOGY LA English DT Article DE polymer-matrix composites (PMCs); fibre/matrix bond; buckling; Raman spectroscopy; TEM ID RAMAN-SPECTROSCOPY; FIBROUS COMPOSITES; FIBERS AB We demonstrate effects of nanotubes buckling and debonding in octadecylamine (ODA) derivatized single wall carbon nanotubes (SWCNT)/epoxy nanocomposites under mechanical and thermal loads uniquely detected by means of Raman spectroscopy and documented by TEM imaging. It is shown that ODA functionalization of SWCNTs provides weak sidewall interactions between the nanotubes and epoxy matrix, which make axially compressed ODA-SWCNTs susceptible to buckling. The feasibility of ODA-SWCNTs buckling in epoxy matrix is also supported by the structural mechanics calculations. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ Houston, Texas Ctr Superconduct & Adv Mat, Sci Ctr 202, Houston, TX 77204 USA. Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Rice Univ, Dept Chem, Houston, TX 77005 USA. Rice Univ, Dept Chem Engn & Mat Sci, Houston, TX 77005 USA. Rice Univ, Ctr Nanoscale Sci & Technol, Houston, TX 77005 USA. RP Hadjiev, VG (reprint author), Univ Houston, Texas Ctr Superconduct & Adv Mat, Sci Ctr 202, Houston, TX 77204 USA. EM vhadjiev@uh.edu RI Arepalli, Sivaram/A-5372-2010; Hadjiev, Viktor/A-7069-2008; OI Tour, James/0000-0002-8479-9328; Hadjiev, Viktor/0000-0001-8579-9357; Lagoudas, Dimitris/0000-0002-0194-5933 NR 28 TC 27 Z9 30 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0266-3538 J9 COMPOS SCI TECHNOL JI Compos. Sci. Technol. PD JAN PY 2006 VL 66 IS 1 BP 128 EP 136 DI 10.1016/j.compscitech.2005.01.004 PG 9 WC Materials Science, Composites SC Materials Science GA 985RT UT WOS:000233396700011 ER PT B AU Knuth, KH Castle, JP Wheeler, KR AF Knuth, Kevin H. Castle, J. Patrick Wheeler, Kevin R. BE Rizzi, A Vichi, M TI Identifying excessively rounded or truncated data SO COMPSTAT 2006: PROCEEDINGS IN COMPUTATIONAL STATISTICS LA English DT Proceedings Paper CT 17th Symposium on Computational Statistics (COMSTAT 2006) CY AUG 28-SEP 01, 2006 CL Rome, ITALY DE data; information; truncated; rounded; Bayesian; histogram AB All data are digitized, and hence are essentially integers rather than true real numbers. Ordinarily this causes no difficulties since the truncation or rounding usually occurs below the noise level. However, in some instances, when the instruments or data delivery and storage systems are designed with less than optimal regard for the data or the subsequent data analysis, the effects of digitization may be comparable to important features contained within the data. In these cases, information has been irrevocably lost in the truncation process. While there exist techniques for dealing with truncated data, we propose a straightforward method that will allow us to detect this problem before the data analysis stage. It is based on an optimal histogram binning algorithm that can identify when the statistical structure of the digitization is on the order of the statistical structure of the data set itself. C1 [Knuth, Kevin H.] SUNY Albany, Dept Phys, Albany, NY 12222 USA. [Castle, J. Patrick] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA. [Wheeler, Kevin R.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. RP Knuth, KH (reprint author), SUNY Albany, Dept Phys, Albany, NY 12222 USA. EM kknuth@albany.edu; pcastle@email.arc.nasa.gov; kevinwheeler@ieee.org FU NASA Earth Science Technology Office (ESTO) [AIST-QRS-04-3010-T] FX This work was supported by the NASA Earth Science Technology Office (ESTO) AIST-QRS-04-3010-T. The authors would also like to thank William Rossow his assistance with the ISCCP data and the mutual information research. NR 11 TC 0 Z9 0 U1 0 U2 0 PU PHYSICA-VERLAG GMBH & CO PI HEIDELBERG PA TIERGARTENSTR 17, D-69121 HEIDELBERG, GERMANY BN 3-7908-1708-2 PY 2006 BP 313 EP + DI 10.1007/978-3-7908-1709-6_24 PG 2 WC Computer Science, Artificial Intelligence; Statistics & Probability SC Computer Science; Mathematics GA BFJ07 UT WOS:000242170000024 ER PT B AU Bailey, FR AF Bailey, F. Ronald BE Groth, C Zingg, DW TI High-End Computing challenges in aerospace design and engineering SO Computational Fluid Dynamics 2004, Proceedings LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res AB High-End Computing (HEC) has had significant impact on aerospace design and engineering and is poised to make even more in the future. In this paper we describe four aerospace design and engineering challenges: Digital Flight, Launch Simulation, Liquid Rocket Engine Fuel System and Digital Astronaut. The paper discusses modeling capabilities needed for each challenge and presents projections of future near and far-term HEC computing requirements. NASA's HEC Project Columbia is described and programming strategies presented that are necessary to achieve high real performance. C1 NASA, Ames Res Ctr, Adv Management Technol Inc, Moffett Field, CA 94035 USA. RP Bailey, FR (reprint author), NASA, Ames Res Ctr, Adv Management Technol Inc, M-S 258-6, Moffett Field, CA 94035 USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 13 EP 26 DI 10.1007/3-540-31801-1_2 PG 14 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500002 ER PT B AU Jorgensoni, PCE Loh, CY AF Jorgensoni, Philip C. E. Loh, Ching Y. BE Groth, C Zingg, DW TI Numerical simulation of the oscillations in a mixer - An internal aeroacoustic feedback system SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res AB The space-time conservation element and solution element method is employed to numerically study the acoustic feedback system in a high temperature, high speed wind tunnel mixer. The computation captures the self-sustained feedback loop between reflecting Mach waves and the shear layer. This feedback loop results in violent instabilities that are suspected of causing damage to some tunnel components. The computed frequency is in good agreement with the available experimental data. The physical phenomena are explained based on the numerical results. C1 [Jorgensoni, Philip C. E.] NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. [Loh, Ching Y.] Taitech Inc, Cleveland, OH 44135 USA. RP Jorgensoni, PCE (reprint author), NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. FU Quiet Aircraft Technology; NASA FX This work was supported by the Quiet Aircraft Technology Program at the NASA John H. Glenn Research Center, Lewis Field. NR 5 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 83 EP + DI 10.1007/3-540-31801-1_7 PG 2 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500007 ER PT B AU Wang, XY Himansu, A Chang, SC Jorgensen, P AF Wang, X. Y. Himansu, A. Chang, S. C. Jorgensen, P. BE Groth, C Zingg, DW TI Computation on wake/stator interaction in a 2D cascade SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res AB Numerical simulations of rotor-stator interaction using the space-time conservation element and solution element (CE/SE) method are presented. The wake generated by the rotor is specified through the unsteady inlet boundary condition of the stator, over which the time-marching is performed. The Giles approach is incorporated with the CE/SE method such that numerical simulations involving rotor and stator rows with unequal blade counts can be carried out using a single or a few flow passages instead of using the full set of passages. The benchmark problems 3.2 of the 2nd and 4th CAA Workshops are used to validate the Giles approach with the CE/SE method. For Prob. 3.2 of the 2nd CAA Workshop, both numerical results obtained by using a single passage and the full set of passages are presented and compared with the analytical solution, while for the problem of the 4th CAA Workshop, the numerical solution obtained by using two passages is presented. C1 [Wang, X. Y.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Himansu, A.] Taitech Inc, NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Chang, S. C.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Jorgensen, P.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Wang, XY (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM xiao-yen.wang@grc.nasa.gov; ananda.himansu@grc.nasa.gov; sin-chung.chang@grc.nasa.gov; jorgenson@grc.nasa.gov FU Engine System Noise Reduction; Quiet Aircraft Technology Program at NASA Glenn Research Cente FX This work was supported by Engine System Noise Reduction Project which is part of Quiet Aircraft Technology Program at NASA Glenn Research Center. NR 10 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 95 EP + DI 10.1007/3-540-31801-1_9 PG 3 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500009 ER PT B AU Gea, LM Vicker, D AF Gea, L. M. Vicker, D. BE Groth, C Zingg, DW TI CFD simulation of the space shuttle launch vehicle with booster separation motor and reaction control system plumes SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res AB The primary objective of this paper is to demonstrate the capability of computational fluid dynamics (CFD) to simulate a very complicated flow field encountered during the space shuttle ascent. The flow field features nozzle plumes from booster separation motor (BSM) and reaction control system (RCS) jets with a supersonic incoming cross flow at speed of Mach 4. The overset Navier-Stokes code OVERFLOW [1], was used to simulate the flow field surrounding the entire space shuttle launch vehicle (SSLV) with high geometric fidelity. The variable gamma option was chosen due to the high temperature nature of nozzle flows and different plume species. CFD predicted Mach contours are in good agreement with the schlieren photos from wind tunnel test. Flow fields are discussed in detail and the results are used to support the debris analysis for the space shuttle Return To Flight (RTF) task. C1 [Gea, L. M.] Boeing Co, 5301 Bolsa Ave,MC H013-B308, Huntington Beach, CA 92647 USA. [Vicker, D.] NASA, Lyndon B Johnson Space Ctr, Appl Aerosci EG3, Houston, TX 77058 USA. RP Gea, LM (reprint author), Boeing Co, 5301 Bolsa Ave,MC H013-B308, Huntington Beach, CA 92647 USA. EM lie-mine.gea@boeing.com; darby.vicker@nasa.gov NR 11 TC 1 Z9 1 U1 0 U2 2 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 233 EP + DI 10.1007/3-540-31801-1_30 PG 2 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500030 ER PT B AU Chaderjan, NM Rogers, SE Aftosmis, MJ Pandya, SA Ahmad, JU Tejnil, E AF Chaderjan, Neal M. Rogers, Stuart E. Aftosmis, Mike J. Pandya, Shishir A. Ahmad, Jasim U. Tejnil, Edward BE Groth, C Zingg, DW TI Automated Euler and Navier-Stokes database generation for a glide-back booster SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res ID INFRASTRUCTURE AB AeroDB is a database generation framework that is used to compute thousands of Euler and Navier-Stokes solutions for a 2nd generation glide-back booster in one week using the NASA Information Power Grid. Process automation and web-based access is used to greatly simplify and reduce the user workload. The solutions are validated with experimental data, and stability derivatives are computed using a monotone cubic-spline procedure. Flow visualization and three-dimensional surface plots are used to interpret and characterize the nature of computed flow fields. C1 [Chaderjan, Neal M.; Rogers, Stuart E.; Aftosmis, Mike J.; Pandya, Shishir A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ahmad, Jasim U.; Tejnil, Edward] Eloret Inst, Moffett Field, CA USA. RP Chaderjan, NM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Neal.M.Chaderjian@nasa.gov; rogers@nas.nasa.gov; Michael.J.Aftosmis@nasa.gov; Shishir.A.Pandya@nasa.gov; ahmad@nas.nasa.gov; tejnil@nas.nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 251 EP + DI 10.1007/3-540-31801-1_33 PG 2 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500033 ER PT B AU Cheer, AY Cheung, S Sanderson, SL AF Cheer, A. Y. Cheung, S. Sanderson, S. L. BE Groth, C Zingg, DW TI Computational fluid dynamics of crossflow filtration in suspension-feeding fishes SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res DE crossflow filtration; suspension feeding AB Suspension-feeding fishes such as herring and anchovies engulf particle-concentrated water through their mouths and release the water through the posterior oral cavity. Food particles are separated from the water at the gill rakers that act like modern crossflow filters. This paper uses Computational Fluid Dynamic (CFD) techniques to study the feeding mechanism of these suspension feeders. By understanding how food is separated from the water, we can elucidate why fish gill rakers do not get clogged with particles in the same manner that industrial crossfiow filters eventually become fouled. C1 [Cheer, A. Y.] Univ Calif Davis, Dept Math, Davis, CA 95616 USA. [Cheung, S.] NASA, Ames Res Ctr, Moffett Field, CA USA. [Sanderson, S. L.] Coll William & Mary, Dept Biol, Williamsburg, VA USA. RP Cheer, AY (reprint author), Univ Calif Davis, Dept Math, Davis, CA 95616 USA. EM cheer@math.ucdavis.edu; cheung@nas.nasa.gov; slsand@wm.edu FU NSF [DMS-0079760, IBN-0131293]; DOE [DE-FG03-99ER25375]; UCD FX This study is supported in part by NSF grant DMS-0079760, DOE: DE-FG03-99ER25375 and UCD Fellowship to A.Y.C. and by NSF grant IBN-0131293 to S.L.S. NR 16 TC 1 Z9 1 U1 1 U2 3 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 301 EP + DI 10.1007/3-540-31801-1_41 PG 2 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500041 ER PT B AU Rumsey, CL AF Rumsey, Christopher L. BE Groth, C Zingg, DW TI Reynolds-averaged Navier-Stokes computations of a synthetic jet in a turbulent boundary layer SO Computational Fluid Dynamics 2004, Proceedings LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res ID CROSS-FLOW; ROUND JET AB An unsteady Reynolds-averaged Navier-Stokes (URANS) computation is performed for the flow of a synthetic jet issuing into a turbulent boundary layer through a circular orifice. Several numerical parameters are investigated, and the effects of three different turbulence models are explored. Results are compared to experiment. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Rumsey, CL (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 355 EP 360 DI 10.1007/3-540-31801-1_49 PG 6 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500049 ER PT B AU Yee, HC Sjogreen, B AF Yee, H. C. Sjogreen, B. BE Groth, C Zingg, DW TI Adaptive numerical dissipation control in high order schemes for multi-D non-ideal MHD SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res C1 [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sjogreen, B.] Royal Inst Technol, S-10044 Stockholm, Sweden. RP Yee, HC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 407 EP + DI 10.1007/3-540-31801-1_57 PG 2 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500057 ER PT B AU Liu, Y Vinokur, M Wang, ZJ AF Liu, Yen Vinokur, Marcel Wang, Z. J. BE Groth, C Zingg, DW TI Discontinuous spectral difference method for conservation laws on unstructured grids SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res AB A new, high-order, conservative, and efficient method for conservation laws on unstructured grids is developed. The concept of discontinuous and high-order local representations to achieve conservation and high accuracy is utilized in a manner similar to the Discontinuous Calerkin (DG)[1] and the Spectral Volume (SV)[2] methods, but while these methods are based on the integrated forms of the equations, the new method is based on the differential form to attain a simpler formulation and higher efficiency. Conventional unstructured finite-difference (FD)[3] and finite-volume (FV)[4] methods require data reconstruction based on the least-squares formulation using neighboring point or cell data. Since each unknown employs a different stencil, one must repeat the least-squares inversion for every point or cell at each time step, or store the inversion coefficients. In a high-order, three-dimensional computation, the former would involve impractically large CPU time, while for the latter the memory requirement becomes prohibitive. In addition, the finite-difference method does not satisfy the integral conservation in general. By contrast, the DG and SV methods employ a local, universal reconstruction of a given order of accuracy in each cell in terms of internally defined conservative unknowns. Since the solution is discontinuous across cell boundaries, a Riemann solver is necessary to evaluate boundary flux terms and maintain conservation. In the DC method, a Galerkin finite-element method is employed to update the nodal unknowns within each cell. This requires the inversion of a mass matrix, and the use of quadratures of twice the order of accuracy of the reconstruction to evaluate the surface integrals and additional volume integrals for non-linear flux functions. In the SV method, the integral conservation law is used to update volume averages over subcells defined by a geometrically similar partition of each grid cell. As the order of accuracy increases, the partitioning for 3D requires the introduction of a large number of parameters, whose optimization to achieve convergence becomes increasingly more difficult. Also, the number of interior facets required to subdivide non-planar faces, and the additional increase in the number of quadrature points for each facet, increases the computational cost greatly. In the spectral difference (SD) method, the conservative unknowns in each cell are the number of nodal values required to support a reconstruction of a given order of accuracy. Their locations are chosen so that a quadrature approximation for the volume integral exists at least to the same order of accuracy. The fluxes are calculated at a different set of nodes, whose number will support a reconstruction of one order higher accuracy, since the flux derivatives are used to update the conservative unknowns. They are located so that quadrature approximations for surface integrals over the cell boundaries exist to a required order of accuracy. In addition, the locations of the conservative nodes and the flux nodes must be such that the integral conservation law is satisfied for the cell to the desired order of accuracy. If the nodes are distributed in a geometrically similar manner for all cells, the discretizations become universal, and can be expressed as the same weighted sums of the products of the local metrics and fluxes. These metrics are constants for the line, triangle, and tetrahedron elements, and can be computed analytically for curved elements. We can also show that the number of flux nodes is far less than the number of quadrature points in the SV method. Since all unknowns are decoupled, no mass matrix inversion is required. The SD formulation for the line element is a generalization of the multidomain spectral method[5]. Its tensor products can be used for quadrilateral and hexahedral elements. C1 [Liu, Yen] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Vinokur, Marcel] Eloret Corp, Sunnyvale, CA 94087 USA. [Wang, Z. J.] Michigan State Univ, E Lansing, MI 48824 USA. RP Liu, Y (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Yen.Liu@nasa.gov; vinokur@nas.nasa.gov; zjw@egr.msu.edu NR 5 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 449 EP + DI 10.1007/3-540-31801-1_63 PG 3 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500063 ER PT B AU Kiris, C Housman, J Kwak, D AF Kiris, Cetin Housman, Jeffrey Kwak, Dochan BE Groth, C Zingg, DW TI Comparison of artificial compressibility methods SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res AB Various artificial compressibility methods for calculating the three-dimensional incompressible Navier-Stokes equations are compared. Each method is described and numerical solutions to test problems are conducted. A comparison based on convergence behavior, accuracy, and robustness is given. C1 [Kiris, Cetin; Kwak, Dochan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Housman, Jeffrey] Univ Calif Davis, Davis, CA USA. RP Kiris, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM ckiris@mail.arc.nasa.gov; jhousman@math.ucdavis.edu; dkwak@mail.arc.nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 475 EP + DI 10.1007/3-540-31801-1_67 PG 2 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500067 ER PT B AU Forsythe, JR Fremaux, CM Hall, RM AF Forsythe, James R. Fremaux, Charles M. Hall, Robert M. BE Groth, C Zingg, DW TI Calculation of static and dynamic stability derivatives of the F/A-18E in abrupt wing stall using RANS and DES SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res C1 [Forsythe, James R.] Cobalt Solut LLC, Springfield, OH USA. [Fremaux, Charles M.; Hall, Robert M.] NASA Langley Res Ctr, Hampton, VA 23666 USA. RP Forsythe, JR (reprint author), Cobalt Solut LLC, Springfield, OH USA. EM forsythe@cobaltcfd.com; c.m.fremaux@larc.nasa.gov; r.m.hall@larc.nasa.gov NR 9 TC 3 Z9 4 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 537 EP + DI 10.1007/3-540-31801-1_76 PG 2 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500076 ER PT B AU Nourgaliev, RR Dinh, TN Liou, MS Theofanous, TG AF Nourgaliev, R. R. Dinh, T. N. Liou, M. -S. Theofanous, T. G. BE Groth, C Zingg, DW TI The Characteristics-Based Matching method (CBM) for high-speed fluid-fluid flows SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res ID MULTIMATERIAL FLOWS; SHOCK; DYNAMICS C1 [Nourgaliev, R. R.; Dinh, T. N.; Theofanous, T. G.] Univ Calif Santa Barbara, Ctr Risk Studies & Safety, Santa Barbara, CA 93106 USA. [Liou, M. -S.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Nourgaliev, RR (reprint author), Univ Calif Santa Barbara, Ctr Risk Studies & Safety, Santa Barbara, CA 93106 USA. EM robert@engr.ucsb.edu; nam@engr.ucsb.edu; Meng-Sing.Liou-1@nasa.gov; theo@engr.ucsb.edu FU Lawrence Livermore National Laboratory FX This work is sponsored by the Lawrence Livermore National Laboratory ("ALPHA" and "MIX" projects). Support of Drs. Frank Handler, Glen Nakafuji and Dan Klem are gratefully acknowledged. NR 11 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 607 EP + DI 10.1007/3-540-31801-1_87 PG 2 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500087 ER PT B AU Chang, CH Liou, MS AF Chang, Chih-Hao Liou, Meng-Sing BE Groth, C Zingg, DW TI Simulation of multifluid multiphase flows with AUSM(+)-up scheme SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res AB An accurate and robust method is proposed for the simulation of two dimensional compressible multifluid flows. Our method incorporates the AUSM(+)-up scheme and the stratified flow model to discretize compressible single-pressure multifluid equations. This method satisfies the pressure-undisturbed condition and can capture the moving discontinuities accurately. It's also able to compute a very strong shock wave propagating across the gas-liquid interface. Two test problems, including the shock-bubble interaction problem and the shock-water column interaction problem, will be demonstrated in this paper. C1 [Chang, Chih-Hao; Liou, Meng-Sing] NASA, Glenn Res Ctr, Lewis Field, Cleveland, OH 44135 USA. RP Chang, CH (reprint author), NASA, Glenn Res Ctr, Lewis Field, Cleveland, OH 44135 USA. EM chih_hao_chang@hotmail.com; MENG-SING.LIOU-1@nasa.gov NR 9 TC 1 Z9 2 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 613 EP + DI 10.1007/3-540-31801-1_88 PG 2 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500088 ER PT B AU Nemec, M Aftosmis, MJ Pulliam, TH AF Nemec, Marian Aftosmis, Michael J. Pulliam, Thomas H. BE Groth, C Zingg, DW TI On the use of parametric-CAD systems and Cartesian methods for aerodynamic design SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res C1 [Nemec, Marian] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Nemec, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM nemec@nas.nasa.gov; aftosmis@nas.nasa.gov; tpulliam@mail.arc.nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 699 EP + DI 10.1007/3-540-31801-1_101 PG 2 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500101 ER PT B AU Huynh, HT AF Huynh, H. T. BE Groth, C Zingg, DW TI An upwind moment scheme for conservation laws SO COMPUTATIONAL FLUID DYNAMICS 2004, PROCEEDINGS LA English DT Proceedings Paper CT 3rd International Conference on Computational Fluid Dynamics CY JUL 12-16, 2004 CL Toronto, CANADA SP NASA, Natl Res Council Canada, Inst Aerosp Res AB A new piecewise linear scheme called upwind moment scheme is presented. Similar to the standard upwind scheme, the cell average values are updated by using a linear function in each cell, a march to the half time level by a Taylor series expansion, and a flux calculation that takes into account the wind direction. The slopes, however, are updated by evaluating the moment about the cell center in a manner similar to that of the discontinuous Galerkin method. The resulting scheme is third-order accurate in both space and time; in addition, the leading error, which is a dissipative error, is only 1/9 that of the standard piecewise-parabolic upwind method. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Huynh, HT (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM huynh@grc.nasa.gov NR 7 TC 1 Z9 1 U1 1 U2 2 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-31800-3 PY 2006 BP 761 EP 766 DI 10.1007/3-540-31801-1_110 PG 6 WC Mechanics SC Mechanics GA BFA96 UT WOS:000240583500110 ER PT S AU Mussa, HY Lary, DJ Glen, RC AF Mussa, Hamse Y. Lary, David J. Glen, Robert C. BE Berthold, MR Glen, R Fischer, I TI Building structure-property predictive models using data assimilation SO COMPUTATIONAL LIFE SCIENCES II, PROCEEDINGS SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 2nd International Symposium on Computational Life Sciences CY SEP 27-29, 2006 CL Cambridge, ENGLAND SP Mol Graph Modelling Soc, ALTANA Pharma AG, AstraZeneca R&D, Boehringer Ingelheim, Inpharmatica, Unilever R&D Port Sunlight, Unilever Corp Res ID ARTIFICIAL NEURAL-NETWORKS; CHROMATOGRAPHY AB In Chernometrics it is often the norm to develop regression methods for analysing non-linear multivariate data by using the observations (measurements) as the sole constraint. This is the case regardless of the nature of the regression method (parametric or non-parametric) [1]. In this article we present the development of a regression model using data assimilation(2) - A technique that takes into account additional available information about the "system" which the model is to represent. The new approach shows substantial improvement over the "conventional" methods[3] against which it has been compared. C1 Univ Cambridge, Dept Chem, Unilever Ctr Mol Sci Informat, Cambridge CB2 1EW, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20071 USA. RP Mussa, HY (reprint author), Univ Cambridge, Dept Chem, Unilever Ctr Mol Sci Informat, Lensfield Rd, Cambridge CB2 1EW, England. EM rcg28@cam.ac.uk RI Lary, David/A-6163-2010 NR 19 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-45767-4 J9 LECT NOTES COMPUT SC PY 2006 VL 4216 BP 64 EP 73 PG 10 WC Biochemical Research Methods; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Biochemistry & Molecular Biology; Computer Science GA BFI96 UT WOS:000242127600007 ER PT S AU Gutsev, GL Mochena, MD Bauschlicher, CW AF Gutsev, G. L. Mochena, M. D. Bauschlicher, C. W., Jr. BE Alexandrov, VN VanAlbada, GD Sloot, PMA Dongarra, J TI All-electron DFT modeling of SWCNT growth initiation by iron catalyst SO COMPUTATIONAL SCIENCE - ICCS 2006, PT 3, PROCEEDINGS SE Lecture Notes in Computer Science LA English DT Article; Proceedings Paper CT 6th International Conference on Computational Science (ICCS 2006) CY MAY 28-31, 2006 CL Reading, ENGLAND SP Intel Corp, IBM, SGI, Microsoft Res, EPSRC, Springer, ACET Ctr, Univ Reading, SIAM, IMACS, UK e Sci Programme ID WALLED CARBON NANOTUBES; GAS-PHASE; MOLECULAR-DYNAMICS; FE-N; NUCLEATION; CLUSTERS; SIMULATIONS; ENERGIES; MONOXIDE AB Electronic and geometrical structures of Fe4Cn(CO)(m) (n+m <= 6) and Fe4Cn (n=7-16) clusters along with their singly negatively and positively charged ions are computed using density functional theory with generalized gradient approximation (DFT-GGA). Isomers with CO bonded directly to the iron atoms and bonded to a carbon atom chemisorbed on the cluster surface are optimized for the Fe4C2CO, Fe4C2(CO)(2), Fe4C3CO, and Fe4C4CO series. The computed total energies are used to estimate the energetics of the Boudouard disproportionation reactions Fe4Cn(CO)(m) + CO -> Fe4Cn+1(CO)(m-1) + CO2. Optimizations of the Fe4C4-Fe4C16 clusters have shown that dimers C-2 are formed in the lowest energy states of Fe4C4,, trimers C-3 - in Fe4C5 and Fe4C6, tetramers C-4-in Fe4C7 and Fe4C8, a pentamer C-5 - in Fe4C9, and a hexamer C-6 - in Fe4C10. Cn rings attached to a Fe-3 face are formed in the lowest energy states of Fe4C. beginning with n = 11. C1 Florida A&M Univ, Dept Phys, Tallahassee, FL 32307 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gutsev, GL (reprint author), Florida A&M Univ, Dept Phys, Tallahassee, FL 32307 USA. EM gennady.gutsev@famu.edu NR 26 TC 0 Z9 0 U1 1 U2 3 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-34383-0 J9 LECT NOTES COMPUT SC PY 2006 VL 3993 BP 128 EP 135 PG 8 WC Computer Science, Theory & Methods SC Computer Science GA BEO20 UT WOS:000238417300019 ER PT J AU Bowen, JP Hinchey, MG AF Bowen, JP Hinchey, MG TI Ten Commandments of formal methods ... Ten years later SO COMPUTER LA English DT Article AB More than a decade ago, the authors offered practical guidelines for projects that sought to use formal methods. Over the years, that article has been widely cited and generated much positive feedback. However, despite this apparent enthusiasm, formal methods use has not greatly increased and some of the same attitudes about the infeasibility of adopting them persist. Yet 10 years later, the original formal methods commandments remain valid. The use of formal methods is not as prevalent as hoped, but formal approaches will always have a niche in computer-based systems development, especially when correct functioning is critical. The next 10 years should see some significant progress in integrating formal methods and traditional development practices. C1 S Bank Univ, Inst Comp Res, London SE1 0AA, England. NASA, Software Engn Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. Loyola Coll, Baltimore, MD 21210 USA. RP Bowen, JP (reprint author), S Bank Univ, Inst Comp Res, London SE1 0AA, England. EM jonathan.bowen@lsbu.ac.uk; michael.g.hinchey@nasa.gov OI Bowen, Jonathan/0000-0002-8748-6140 NR 14 TC 27 Z9 27 U1 1 U2 3 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0018-9162 J9 COMPUTER JI Computer PD JAN PY 2006 VL 39 IS 1 BP 40 EP + DI 10.1109/MC.2006.35 PG 10 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering SC Computer Science GA 001DB UT WOS:000234512700011 ER PT J AU Cooke, DE Barry, M Lowry, M Green, C AF Cooke, DE Barry, M Lowry, M Green, C TI NASA's exploration agenda and capability engineering SO COMPUTER LA English DT Article AB Past NASA missions have been scripted, meaning that engineers developed hardware and software systems to respond mainly to foreseen circumstances, making them less able to handle unforeseen problems or exploration opportunities. The primary responsibility for handling unanticipated situations resides with humans, either onboard the spacecraft or in mission control. The authors posit that software development will not achieve the level of hardware development without the introduction and use of model-based languages. Further, model-based development will not be widely accepted without risk analysis methodologies on par with those employed in hardware development. C1 Texas Tech Univ, Dept Comp Sci, Lubbock, TX 79409 USA. Jet Prop Lab, Pasadena, CA USA. NASA, Ames Res Ctr, Robust Software Engn Grp, Moffett Field, CA 94035 USA. Kestrel Inst, Palo Alto, CA USA. RP Cooke, DE (reprint author), Texas Tech Univ, Dept Comp Sci, Lubbock, TX 79409 USA. EM dcooke@coe.ttu.edu; matthew.r.barry@nasa.gov; michael.r.lowry@nasa.gov; green@kestrel.edu NR 9 TC 3 Z9 4 U1 0 U2 1 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0018-9162 J9 COMPUTER JI Computer PD JAN PY 2006 VL 39 IS 1 BP 63 EP + DI 10.1109/MC.2006.27 PG 12 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering SC Computer Science GA 001DB UT WOS:000234512700013 ER PT J AU Barth, T AF Barth, T TI On discontinuous Galerkin approximations of Boltzmann moment systems with Levermore closure SO COMPUTER METHODS IN APPLIED MECHANICS AND ENGINEERING LA English DT Article DE nonlinear conservation laws; kinetic Boltzmann equation; Levermore Boltzmann moment closure; entropy symmetrization; discontinuous Galerkin finite element method ID FINITE-ELEMENT METHOD; COMPUTATIONAL FLUID-DYNAMICS; HYPERBOLIC CONSERVATION-LAWS; GAS-DYNAMICS; ENTROPY CONDITION; SCHEMES; CONVERGENCE; FORMULATION; EQUATIONS; FORM AB This work considers the discontinuous Galerkin (DG) finite element discretization of first-order systems of conservation laws derivable as moments of the kinetic Boltzmann equation with Levermore [C.D. Levermore, Moment closure hierarchies for kinetic theories, J. Statist. Phys. 83 (5-6) (1996) 1021-1065] closure. Using standard energy analysis techniques, a new class of energy stable numerical flux functions are devised for the DG discretization of Boltzmann moment systems. Simplified energy stable numerical fluxes are then constructed which replace exact state space integration in the numerical flux with Gauss-Lobatto quadrature. Numerical results for supersonic flow over a cylinder geometry in the continuum and transitional regimes using 5 and 10 moment approximations are presented using the newly devised DG discretizations. (c) 2005 Elsevier B.V. All rights reserved. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Barth, T (reprint author), NASA, Ames Res Ctr, Mail Stop T27A-1, Moffett Field, CA 94035 USA. EM Timothy.J.Barth@nasa.gov NR 39 TC 8 Z9 8 U1 0 U2 0 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0045-7825 J9 COMPUT METHOD APPL M JI Comput. Meth. Appl. Mech. Eng. PY 2006 VL 195 IS 25-28 BP 3311 EP 3330 DI 10.1016/j.cma.2005.06.016 PG 20 WC Engineering, Multidisciplinary; Mathematics, Interdisciplinary Applications; Mechanics SC Engineering; Mathematics; Mechanics GA 042DF UT WOS:000237507000008 ER PT J AU Diethelm, K Freed, AD AF Diethelm, K Freed, AD TI An efficient algorithm for the evaluation of convolution integrals SO COMPUTERS & MATHEMATICS WITH APPLICATIONS LA English DT Article DE convolution integral; numerical approximation; quadrature; logarithmic memory; viscoelasticity; Mittag-Leffler function AB We propose an algorithm for the numerical evaluation of convolution integrals of the form integral(0)(x) k(x - y)f(y, x) dy, for x is an element of [0, X]. Our method is especially suitable in situations where the fundamental interval [0, X] is very long and the kernel function k is expensive to calculate. Separate versions are provided where the forcing function f is known in advance, and where it must be determined step-by-step along the solution path. These methods are efficient with respect to both run time and memory requirements. (c) 2006 Elsevier Ltd. All rights reserved. C1 NASA, Glenn Res Ctr, Bio Sci & Technol Branch, Cleveland, OH 44135 USA. Tech Univ Carolo Wilhelmina Braunschweig, Inst Computat Math, D-38106 Braunschweig, Germany. GNS Gesellsch Numer Simulat MbH, D-38114 Braunschweig, Germany. RP Freed, AD (reprint author), NASA, Glenn Res Ctr, Bio Sci & Technol Branch, 21000 Brookpk Rd,MS 49-3, Cleveland, OH 44135 USA. EM diethelm@gns-mbh.com; Alan.D.Freed@nasa.gov OI Freed, Alan/0000-0002-3492-0628 NR 14 TC 14 Z9 15 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0898-1221 J9 COMPUT MATH APPL JI Comput. Math. Appl. PD JAN PY 2006 VL 51 IS 1 BP 51 EP 72 DI 10.1016/j.camwa.2005.07.010 PG 22 WC Mathematics, Applied SC Mathematics GA 009II UT WOS:000235104700005 ER PT B AU Xu, LH Shi, H Fisher, J Lees, RM Pearson, JC Drouin, BJ AF Xu, Li-Hong Shi, Hongyu Fisher, Jonathan Lees, R. M. Pearson, John C. Drouin, Brian J. BE Shen, XC Lu, W Zhang, J Dou, WB TI New terahertz methanol spectroscopy for HIFI on the Herschel mission SO CONFERENCE DIGEST OF THE 2006 JOINT 31ST INTERNATIONAL CONFERENCE ON INFRARED AND MILLIMETER WAVES AND 14TH INTERNATIONAL CONFERENCE ON TERAHERTZ ELECTRONICS LA English DT Proceedings Paper CT Joint 31st International Conference on Infrared and Millimeter Waves/14th International Conference on Terahertz Electronics CY SEP 18-22, 2006 CL Shanghai, PEOPLES R CHINA SP Chinese Acad Sci, Shanghai Inst Tech Phys, SE Univ, Chinese Acad Sci, Natl Nat Sci Fdn China, IEEE MTT S, IEEE Nanjing Joint Chapter, IEEE Shanghai Sub Sect, Shanghai Int Culture Assoc, Chinese Phys Soc, Chinese Opt Soc, Chinese Inst Elect C1 [Xu, Li-Hong; Shi, Hongyu; Fisher, Jonathan; Lees, R. M.] Univ New Brunswick, Ctr Laser Atom & Mol Sci, Dept Phys Sci, St John, NB E2L 4L5, Canada. [Pearson, John C.; Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Xu, LH (reprint author), Univ New Brunswick, Ctr Laser Atom & Mol Sci, Dept Phys Sci, St John, NB E2L 4L5, Canada. EM xuli@unb.ca FU Natural Sciences and Engineering Research Council of Canada (NSERC); Canadian Space Agency (CSA); National Aeronautics and Space Administration (NASA) FX We gratefully acknowledge financial support for this project from the Natural Sciences and Engineering Research Council of Canada (NSERC), the Canadian Space Agency (CSA), and the National Aeronautics and Space Administration (NASA). NR 3 TC 0 Z9 0 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-0399-8 PY 2006 BP 228 EP 228 PG 1 WC Engineering, Electrical & Electronic SC Engineering GA BGH25 UT WOS:000246942200226 ER PT B AU Maestrini, A Tripon-Canseliet, C Ward, JS Gill, JJ Mehdi, I AF Maestrini, Alain Tripon-Canseliet, Charlotte Ward, John S. Gill, John J. Mehdi, Imran BE Shen, XC Lu, W Zhang, J Dou, WB TI A 260-340 GHz dual chip frequency tripler for THz frequency multiplier chains SO CONFERENCE DIGEST OF THE 2006 JOINT 31ST INTERNATIONAL CONFERENCE ON INFRARED AND MILLIMETER WAVES AND 14TH INTERNATIONAL CONFERENCE ON TERAHERTZ ELECTRONICS LA English DT Proceedings Paper CT Joint 31st International Conference on Infrared and Millimeter Waves/14th International Conference on Terahertz Electronics CY SEP 18-22, 2006 CL Shanghai, PEOPLES R CHINA SP Chinese Acad Sci, Shanghai Inst Tech Phys, SE Univ, Chinese Acad Sci, Natl Nat Sci Fdn China, IEEE MTT S, IEEE Nanjing Joint Chapter, IEEE Shanghai Sub Sect, Shanghai Int Culture Assoc, Chinese Phys Soc, Chinese Opt Soc, Chinese Inst Elect AB We designed and fabricated a fix-tuned balanced frequency tripler working in the 260-340 GHz band to be the first stage of a x3x3x3 multiplier chain to 2.7 THz. The design of a dual-chip version of this multiplier featuring an input splitter / output combiner as part of the input / output matching networks of both chips - with no degradation of the expected bandwidth and efficiency- will be presented. C1 [Maestrini, Alain; Tripon-Canseliet, Charlotte] Univ Paris 06, LISIF, 4 Pl Jussieu, F-75252 Paris, France. [Ward, John S.; Gill, John J.; Mehdi, Imran] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Maestrini, Alain] Observ Paris, LERMA, F-75014 Paris, France. RP Maestrini, A (reprint author), Univ Paris 06, LISIF, 4 Pl Jussieu, F-75252 Paris, France. EM alain.maestrini@lisif.jussieu.fr NR 3 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-0399-8 PY 2006 BP 336 EP 336 PG 1 WC Engineering, Electrical & Electronic SC Engineering GA BGH25 UT WOS:000246942200334 ER PT B AU Dengler, RJ Maiwald, F Siegel, PH AF Dengler, Robert J. Maiwald, Frank Siegel, Peter H. BE Shen, XC Lu, W Zhang, J Dou, WB TI A Compact Electronically-Tuned Vector Measurement System For Submillimeter-Wave Imaging SO CONFERENCE DIGEST OF THE 2006 JOINT 31ST INTERNATIONAL CONFERENCE ON INFRARED AND MILLIMETER WAVES AND 14TH INTERNATIONAL CONFERENCE ON TERAHERTZ ELECTRONICS LA English DT Proceedings Paper CT Joint 31st International Conference on Infrared and Millimeter Waves/14th International Conference on Terahertz Electronics CY SEP 18-22, 2006 CL Shanghai, PEOPLES R CHINA SP Chinese Acad Sci, Shanghai Inst Tech Phys, SE Univ, Chinese Acad Sci, Natl Nat Sci Fdn China, IEEE MTT S, IEEE Nanjing Joint Chapter, IEEE Shanghai Sub Sect, Shanghai Int Culture Assoc, Chinese Phys Soc, Chinese Opt Soc, Chinese Inst Elect AB An electronically tunable compact submillimeter wave transmission/reflection measurement system has been demonstrated at 560-635 GHz. The measured dynamic range is as high as 90 dB (60 dB across the entire frequency range), with less than 21 of peak phase noise. The frequency agility of the system can be exploited to provide near real-time imaging capability using only a single pixel. This is accomplished by scanning the transmit and receive beams through the use of a frequency steerable lens placed at the transmitter and receiver. C1 [Dengler, Robert J.; Maiwald, Frank] CALTECH, Jet Propuls Lab, 4800 Oak Grove Dr MS 168-314, Pasadena, CA 91109 USA. [Siegel, Peter H.] CALTECH, Beckman Inst, Pasadena, CA 91125 USA. RP Dengler, RJ (reprint author), CALTECH, Jet Propuls Lab, 4800 Oak Grove Dr MS 168-314, Pasadena, CA 91109 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-0399-8 PY 2006 BP 374 EP 374 PG 1 WC Engineering, Electrical & Electronic SC Engineering GA BGH25 UT WOS:000246942200372 ER PT B AU Hubbard, SM Wilt, D Bailey, S Byrnes, D Raffaelle, R AF Hubbard, Seth M. Wilt, David Bailey, Sheila Byrnes, Daniel Raffaelle, Ryne GP IEEE TI OMVPE grown InAs quantum dots for application in nanostructured photovoltaics SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc ID CHEMICAL-VAPOR-DEPOSITION; SOLAR-CELLS; TRANSITIONS AB We have grown InAs QDs on two types of vicinal GaAs substrates and under various growth conditions. QDs grown on 2 degrees offcut substrates show superior optical characteristics compared to QDs on 60 offcut substrates, which showed no QD luminescence. The InAs growth temperature was shown to have an impact on QD nucleation, with higher growth temperature leading to both improved dot densities and coherence. Finally, the Will ratio during InAs growth dramatically effects the uniformity of the QD luminescence. Our best QDs were grown at 495 degrees C using a Will ratio of 12. These QDs were 7x40nm in size with a density of 5(+/- 0.5)x10(10) cm(-2). The spatial PL, peaking at 1220 nm, had a wavelength and intensity deviation across the 2" wafer of 0.3% and 16%, respectively. C1 [Hubbard, Seth M.; Wilt, David; Bailey, Sheila] NASA, Glenn Res Ctr, Photovolta & Space Environm Branch, Cleveland, OH 44135 USA. [Byrnes, Daniel; Raffaelle, Ryne] Rochester Inst Technol, Rochester, NY 14623 USA. RP Hubbard, SM (reprint author), NASA, Glenn Res Ctr, Photovolta & Space Environm Branch, Cleveland, OH 44135 USA. EM seth.m.hubbard@grc.nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 118 EP 121 PG 4 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251600030 ER PT B AU Raffaelle, RP Sinharoy, S Wilt, DM Bailey, SG AF Raffaelle, Ryne P. Sinharoy, Samar Wilt, David M. Bailey, Sheila G. GP IEEE TI Multi-junction solar cell spectral tuning with quantum dots SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB We have theoretically analyzed the potential efficiency improvement to multi-junction solar cell efficiencies which are available through the incorporation of quantum dot using detailed balance calculations. We have also experimentally investigated the Stranski-Krastanov growth of self-organized InAs quantum dots and quantum dot arrays on lattice-matched GaAs by metallorganic vapor phase epitaxy (MOVPE). The morphology of the quantum dots were investigated as a function of their growth parameters by atomic force microscopy (AFM). Photluminescence and optical absorption measurements have demonstrated that the incorporation of InAs quantum dots (QD) into a GaAs structure can provide sub-GaAs bandgap electronic states. C1 [Raffaelle, Ryne P.; Sinharoy, Samar] Rochester Inst Technol, 85 Lomb Mem Dr, Rochester, NY 14623 USA. [Wilt, David M.; Bailey, Sheila G.] NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. RP Raffaelle, RP (reprint author), Rochester Inst Technol, 85 Lomb Mem Dr, Rochester, NY 14623 USA. FU NASA Glenn Research Center; David Forbes of Essential Research Incorporated; Air Force Office of Scientific Research; National Reconnaissance Office; Luke Lestor and Dianna Huffaker of the University of New Mexico FX The authors would like to acknowledge the support of the NASA Glenn Research Center, David Forbes of Essential Research Incorporated, the Air Force Office of Scientific Research, the National Reconnaissance Office, and Luke Lestor and Dianna Huffaker of the University of New Mexico. NR 9 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 162 EP 166 PG 5 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251600041 ER PT B AU Raffaelle, RP Landi, BJ Evans, CM Cress, CD Andersen, J Castro, SL Bailey, SG AF Raffaelle, Ryne P. Landi, Brian J. Evans, Christopher M. Cress, Cory D. Andersen, John Castro, Stephanie L. Bailey, Sheila G. GP IEEE TI Nanomaterial development for polymeric solar cells SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc ID PHOTOVOLTAIC DEVICES AB Photoactive nanomaterials are being investigated as multifunctional additives in polymeric photovoltaic devices. Polymer photovoltaic devices which rely solely on photon absorption by the conducting polymer are bandgap-limited (typically > 2 eV) with regard to the solar spectrum. Therefore, nanomaterials with optical absorption below the conducting polymer bandgap can allow composite devices to absorb a larger portion of the solar spectrum. In addition, nanomaterials may play a role in polymer exciton disassociation and transport. We have investigated the use of rare-earth-doped oxide nanoparticles to absorb light in the lower energy region of the solar spectrum, and "up-convert" photons to energies above the polymer bandgap. In addition, we will highlight the synthesis of novel semiconducting quantum dots (QDs) namely, InSb, for absorption in the ideal region of the solar spectrum. Spectroscopy will be provided for both types of materials in addition to the photovoltaic performance of devices incorporating various up-converting nanoparticles. The prospect of coupling single-walled carbon nanotubes to the various upconverting nanoparticles and QDs will be discussed in terms of their previously demonstrated utility in prototype devices. C1 [Castro, Stephanie L.; Bailey, Sheila G.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Raffaelle, Ryne P.; Landi, Brian J.; Evans, Christopher M.; Cress, Cory D.; Andersen, John] Rochester Inst Technol, 85 Lomb Memorial Dr, Rochester, NY 14623 USA. RP Raffaelle, RP (reprint author), Rochester Inst Technol, 85 Lomb Memorial Dr, Rochester, NY 14623 USA. RI Cress, Cory/A-8673-2009 NR 9 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 186 EP 189 PG 4 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251600047 ER PT B AU Granata, JE SahIstrom, TD Hausgen, P Messenger, SR Walters, RJ Lorentzen, JR Liu, S Helizon, R AF Granata, J. E. SahIstrom, T. D. Hausgen, P. Messenger, S. R. Walters, R. J. Lorentzen, J. R. Liu, Simon Helizon, Roger GP IEEE TI Thin-film photovoltaic proton and electron radiation testing for a MEO orbit SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB A radiation test plan for thin-film photovoltaic technologies focused on a MEO flight experiment is outlined. The proton and electron radiation response of thin film, amorphous Si solar cells and CulnGaSe(2) solar cells, with and without space coatings, is presented. The degradation of the photovoltaic output under penetrating and junction-damaging proton irradiation, and 0.6 MeV and 1 MeV electron irradiation, is measured and examined. The experimental data are presented and analyzed. These data will form the basis for an on-orbit prediction model as applied to a high-radiation MEO orbit. C1 [Granata, J. E.] Aerosp Corp, Albuquerque, NM 87198 USA. [SahIstrom, T. D.] Dynacs Mil & Def Inc, Albuquerque, NM USA. [Hausgen, P.] Air Force Res Lab, Space Vech Directorate, Albuquerque, NM USA. [Messenger, S. R.; Lorentzen, J. R.] SFA Inc, Largo, MD 20774 USA. [Walters, R. J.] US Naval Res Lab, Washington, DC 20375 USA. [Liu, Simon] Aerosp Corp, El Segundo, CA USA. [Helizon, Roger] Jet Prop Lab, Pasadena, CA USA. RP Granata, JE (reprint author), Aerosp Corp, Albuquerque, NM 87198 USA. EM jennifer.granata@aero.org NR 8 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1773 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601129 ER PT B AU Endicter, S Aiken, DJ Stella, PM Mardesich, N AF Endicter, Scott Aiken, Daniel J. Stella, Paul M. Mardesich, Nick GP IEEE TI Modification of triple junction solar cells for martian surface conditions SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB Triple junction solar cells have been designed and fabricated to operate optimally with a Martian 60 degrees latitude solar spectrum. Efficiencies as high as 27.4% have been achieved. Future missions to the surface of Mars will require cells optimized for Martian conditions, which include solar intensities reduced by as much as 85%, a red-rich solar spectrum, low surface temperatures, and a relatively passive radiation environment. Under the direction of Jet Propulsion Laboratories (JPL) a solar cell design was created which is based on the current generation of Emcore space qualified triple junction solar cells, yet is optimized for the Martian solar spectrum at 600 latitude. When tested at JPL with a solar simulator that has been modified to produce this Martian spectrum, this design has demonstrated improved efficiency of 2.2% absolute over AM0 optimized designs. C1 [Endicter, Scott; Aiken, Daniel J.] Emcore Photovolta, 10420 Res Rd SE, Albuquerque, NM 87123 USA. [Stella, Paul M.; Mardesich, Nick] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Endicter, S (reprint author), Emcore Photovolta, 10420 Res Rd SE, Albuquerque, NM 87123 USA. EM scott_endicter@emcore.com NR 1 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1808 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601138 ER PT B AU Vayner, B Ferguson, D Galofaro, J AF Vayner, Boris Ferguson, Dale Galofaro, Joel GP IEEE TI Quartz-indium tin oxide-magnesium flouride sandwich in a low density plasma SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB Indium tin oxide (ITO) coatings of solar cell coverglasses have been used for a long time to prevent electrostatic discharges on the array surface of a spacecraft in Geosynchronous Orbit. An antireflection layer of magnesium fluoride is also a common feature of solar cell design that allows increasing array efficiency by a few percent. Currently, some spacecraft in geosynchronous orbit have solar arrays with ITO-MgF2 coatings, and their power systems have experienced significant degradations. Analysis of telemetric data from these satellites shows strong correlations between the events of the sudden power losses and station keeping thruster firing time intervals. The main features of this solar array behavior in an arc jet plume plasma have been reproduced in an experiment in a plasma chamber. C1 [Vayner, Boris] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Ferguson, Dale] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Galofaro, Joel] NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Vayner, B (reprint author), Ohio Aerosp Inst, Cleveland, OH 44142 USA. EM vayner@gre.nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1830 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601144 ER PT B AU Stella, PM Mardesich, N Ewell, RC Mueller, RL Endicter, S Aiken, D Edmondson, K Fetzer, C AF Stella, Paul M. Mardesich, Nick Ewell, Richard C. Mueller, Robert L. Endicter, Scott Aiken, Daniel Edmondson, Kenneth Fetzer, Chris GP IEEE TI Multijunction solar cell technology for Mars surface applications SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB Solar cells used for Mars surface applications have been commercial space qualified AM0 optimized devices. Due to the Martian atmosphere, these cells are not optimized for the Mars surface and as a result operate at a reduced efficiency. A multi-year program, MOST (Mars Optimized Solar Cell Technology), managed by JPL Science Mission Directorate (SMD) and funded by NASA Code S, was initiated in 2004, to develop tools to modify commercial AMO cells for the Mars surface solar spectrum and to fabricate Mars optimized devices for verification. This effort required defining the surface incident spectrum, developing an appropriate laboratory solar simulator measurement capability, and to develop and test commercial cells modified for the Mars surface spectrum. This paper discusses the program, including results for the initial modified cells. Simulated Mars surface measurements of MER cells and Phoenix Lander cells (2007 launch) are provided to characterize the performance loss for those missions. In addition, the performance of the MER rover solar arrays is updated to reflect their more than two (2) year operation. C1 [Stella, Paul M.; Mardesich, Nick; Ewell, Richard C.; Mueller, Robert L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Endicter, Scott; Aiken, Daniel] Emcore Photovolta, Albuquerque, NM USA. [Edmondson, Kenneth; Fetzer, Chris] Spectrolab Inc, Sylmar, CA USA. RP Stella, PM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM paul.m.stella@jpl.nasa.gov FU National Aeronautics and Space Administration FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. NR 2 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1907 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601164 ER PT B AU Wilt, DM Ringel, SA Fitzgerald, EA Jenkins, PP AF Wilt, David M. Ringel, Steven A. Fitzgerald, Eugene A. Jenkins, Phillip P. GP IEEE TI Preliminary on-orbit performance data from GaAs on Si solar cells aboard misses SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc ID LAYERS AB GaAs on Si (GaAs/Si) solar cells grown on Si substrates coated with a step graded buffer of SixGe1-x alloys graded to 100% Ge have demonstrated AM0 efficiencies in excess of 17%. This technology offers the potential for significant increases in mass specific power (kW/kg) due to the low density and robust nature of the silicon substrate. Concerns exist that this III-V on Si technology may degrade when used in an application with significant thermal cycles due to the similar to 60% difference in thermal expansion coefficients. To examine this potential problem, devices were developed and launched to the International Space Station for on-orbit testing aboard Materials International Space Station Experiment number 5 (MISSE5). In low Earth orbit, the devices are experiencing up to 100 degrees C thermal cycles every 90 minutes. Data telemetered from MISSE5 indicates that the devices have successfully completed > 6months of on-orbit testing with no degradation observed. C1 [Wilt, David M.] NASA, Glenn Res Ctr, Cleveland, OH USA. [Ringel, Steven A.] Ohio State Univ, Columbus, OH USA. [Fitzgerald, Eugene A.] MIT, Cambridge, MA USA. [Jenkins, Phillip P.] OAI, Cleveland, OH USA. RP Wilt, DM (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM david.m.wilt@nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1915 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601166 ER PT B AU Landis, GA AF Landis, Geoffrey A. GP IEEE TI Re-evaluating satellite solar power systems for Earth SO Conference Record of the 2006 IEEE 4th World Conference on Photovoltaic Energy Conversion, Vols 1 and 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB The Solar Power Satellite System is a concept to collect solar power in space, and then transport it to the surface of the Earth by microwave (or possibly laser) beam, where it is converted into electrical power for terrestrial use. The recent increase in energy costs, predictions of the near-term exhaustion of oil, and prominence of possible climate change due to the "greenhouse effect" from burning of fossil fuels has again brought alternative energy sources to public attention, and the time is certainly appropriate to reexamine the economics of space based power. Several new concepts for Satellite Power System designs were evaluated to make the concept more economically feasible. C1 NASA, John Glenn Res Ctr, Cleveland, OH 44135 USA. RP Landis, GA (reprint author), NASA, John Glenn Res Ctr, 21000 Brookpk Rd,M-S 302-1, Cleveland, OH 44135 USA. NR 17 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1939 EP 1942 PG 4 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601172 ER PT B AU Landis, GA Bailey, SG Tischler, R AF Landis, Geoffrey A. Bailey, Sheila G. Tischler, Renee GP IEEE TI Causes of power-related satellite failures SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB Satellite on-orbit failures are rare, but costly. Failures cumulatively account for losses that total many billions of dollars. In order to understand the causes of power-system related failures, publicly-available data sources were analyzed to determine the origin of power-system related failures of spacecraft. Data from reported failures and anomalies of commercial and scientific satellites from the period 1990-2006 were analyzed. Military, GPS, and reconnaissance satellites were not included in the data set. The major failures were divided into nine primary categories: Impact or collision induced failures, battery failures, solar array mechanical failures, attitude control failures, failures due to plasma-discharge events, cell failures, other array failures, darkening of glass or solar reflectors, and cell interconnect failure. These failures account for a reported cumulative loss of 4.4 billion dollars. These data were analyzed to show the cause of each type of failure as a percentage of the total number of failures, and the net cost of each type of failure. C1 [Landis, Geoffrey A.; Bailey, Sheila G.] NASA, Glenn Res Ctr, 21000 Brookpk Rd,M-S 302-1, Cleveland, OH 44135 USA. [Tischler, Renee] Parma Senior High Sch, Parma, OH 44129 USA. RP Landis, GA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,M-S 302-1, Cleveland, OH 44135 USA. EM geoffrey.a.landis@nasa.gov NR 13 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1943 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601173 ER PT B AU Spence, B White, S Jones, A Wachholz, J Wilder, N Cronin, P Gregory, T Barker, P Allmandinger, T Mardesich, N Piszczor, M Sharps, P Fatemi, N AF Spence, Brian White, Steve Jones, Alan Wachholz, Jim Wilder, Nick Cronin, Paul Gregory, Todd Barker, Peter Allmandinger, Tiffany Mardesich, Nick Piszczor, Michael Sharps, Paul Fatemi, Navid GP IEEE TI UltraFlex-175 solar array technology maturation achievements for NASA's New Millennium Program (NMP) Space Technology 8 (ST8) SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB ATK Space Systems (ATK) in collaboration with the NASA Glenn Research Center (GRC), the Jet Propulsion Laboratory (JPL), and EMCORE Photovoltaics (EPV), is executing NASA's New Millennium Program (NMP) Space Technology 8 (ST8) Project Formulation Refinement Phase to develop and validate through spaceflight a state-of-the-art solar array system called UltraFlex-175. UltraFlex-175 is a highly evolved and scaled version of the previously flight qualified Mars 01-Lander UltraFlex and employs many advanced technologies. The UltraFlex-1175 system promises very high specific power (175 W/g -220 W/kg BOL), compact stowage volume (> 33 kW/m), high reliability, scalability beyond 7 kW wing sizes, and operational capability for standard, high voltage, multi-A.U., and/or high temperature applications. Key technology maturation activities performed (deployment kinematics, deployed dynamics, and power production / survivability) that demonstrate TRL 5-6 achievement will be presented. Subsystem and system level design, development, experimental hardware builds, conducted testing and results, and analytical model correlation activities will be presented. Technology scale-up performance to 7 kW wing sizes and the planned UltraFlex-1175 flight experiment will also be presented. C1 [Spence, Brian; White, Steve; Jones, Alan; Wachholz, Jim; Wilder, Nick; Cronin, Paul; Gregory, Todd; Barker, Peter; Allmandinger, Tiffany] ATK Space Syst, Goleta, CA 93117 USA. [Mardesich, Nick] Jet Prop Lab, Pasadena, CA 91109 USA. [Piszczor, Michael] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Sharps, Paul; Fatemi, Navid] EMCORE Photovolta, Albuquerque, NM 87123 USA. RP Spence, B (reprint author), ATK Space Syst, Goleta, CA 93117 USA. NR 3 TC 0 Z9 0 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1946 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601174 ER PT B AU Walters, RJ Garner, JC Lam, SN Vasquez, JA Braun, WR Ruth, RE Warner, JH Lorentzen, JR Messenger, SR Bruniga, R Jenkins, PP Flatico, JM Wilt, DM Piszczor, MF Greer, LC Krasowski, MJ AF Walters, R. J. Garner, J. C. Lam, S. N. Vasquez, J. A. Braun, W. R. Ruth, R. E. Warner, J. H. Lorentzen, J. R. Messenger, S. R. Bruniga, R. Jenkins, P. P. Flatico, J. M. Wilt, D. M. Piszczor, M. F. Greer, L. C. Krasowski, M. J. GP IEEE TI Materials on the International Space Station experiment-5, Forward Technology Solar Cell Experiment: First on-orbit data SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB First on-orbit data from the Forward Technology Solar Cell Experiment (FTSCE) are presented. FTSCE is housed within the 5(th) Materials on the International Space Station Experiment (MISSE-5), and currently resides on the exterior of the ISS. A range of solar cell technologies are included in the experiment including triple junction (3J) InGaP/GaAs/Ge solar cells from several vendors, thin film amorphous Si and Culn(Ga)Se-2 cells, and next-generation technologies like single-junction GaAs cells grown on Si wafers and metamorphic InGaP/InGaAs/Ge triple-junction cells. Measured current vs. voltage (IV) curves from onboard experiments are analyzed. All of the solar cell technologies are showing nominal performance with no obvious signs of degradation. C1 [Walters, R. J.; Garner, J. C.; Lam, S. N.; Vasquez, J. A.; Braun, W. R.; Ruth, R. E.; Warner, J. H.] USN, Res Lab, Washington, DC 20375 USA. [Lorentzen, J. R.; Messenger, S. R.] SFA Inc, Crofton, MD 21114 USA. [Bruniga, R.] US Naval Acad, Annapolis, MD 21402 USA. [Jenkins, P. P.] Ohio Aerosp Inst, Cleveland, OH 44135 USA. [Flatico, J. M.] QSS, Cleveland, OH 44135 USA. [Wilt, D. M.; Piszczor, M. F.; Greer, L. C.; Krasowski, M. J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Walters, RJ (reprint author), USN, Res Lab, Washington, DC 20375 USA. EM robert.walters@nrl.navy.mil NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1951 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601175 ER PT B AU Ferguson, DC AF Ferguson, Dale C. GP IEEE TI Standard for solar array arc-prevention in LEO-NASA STD-4005 SO Conference Record of the 2006 IEEE 4th World Conference on Photovoltaic Energy Conversion, Vols 1 and 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB Spacecraft charging in Low Earth Orbit (LEO) is commonly caused by the high voltage (> 55 V) solar array power system. Conversely, arcing on the solar arrays is an undesirable consequence of the spacecraft charging. The new NASA Low Earth Orbit Spacecraft Charging Design Standard and Information Handbook (NASA STD-4005) presents a standard and all the necessary background information to understand how to eliminate solar array arcing on LEO spacecraft in the design stage, before the spacecraft is built, and before costly retrofits are needed. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Ferguson, DC (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1959 EP 1960 PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601177 ER PT B AU Galofaro, JT Vayner, BV AF Galofaro, J. T. Vayner, B. V. GP IEEE TI Ground based experimental results of thin-film photovoltaic cells in a low density LEO plasma environment SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB Plasma ground testing results, conducted at the Glenn Research Center (GRC) National Plasma Interaction (N-PI) Facility, are presented for a number of thin-film photovoltaic cells. The cells represent a mix of promising new technologies identified by the Air Force Research Laboratory (NFRL) under the CYGNUS Space Science Technology Experiment (SSTE-4) Program. Measurements of parasitic current loss, charging/dielectric breakdown of cover-slide coatings and arcing threshold tests are performed for each individual cell. These measurements are followed by a series of experiments designed to test for catastrophic arc failure mechanisms. A special type of power supply, called a solar array simulator (SAS) with adjustable voltage and current limits on the supply's output, is employed to bias two adjacent cells at a predetermined voltage and current. The bias voltage is incrementally ramped up until a sustained arc results. Sustained arcs are precursors to catastrophic arc failure were the arc current rises to a maximum value for long timescales (often ranging between 30 to 100 microsecond times). Normal arcs by comparison, are short lived events with a timescale between 10 and 30 microseconds). Sustained arcs lead to pyrolization with extreme cell damage and have been shown to cause the loss of entire array strings in solar arrays. The collected data will be used to evaluate the suitability of thin-film photovoltaic technologies for future space operations. C1 [Galofaro, J. T.] NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. [Vayner, B. V.] Ohio Aerosp Inst, Cleveland, OH USA. RP Galofaro, JT (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Joel.T.Galofaro@nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1964 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601179 ER PT B AU Jenkins, P Scheiman, D Goodbody, C Baur, C Sharps, P Imaizumi, M Yoo, H Sahlstrom, T Walters, R Lorentzen, J Nocerino, J Khan, O Cravens, R Valles, J Toporow, C Gomez, T Bazan, LP Bailey, S AF Jenkins, Phillip Scheiman, David Goodbody, Chris Baur, Carsten Sharps, Paul Imaizumi, Mitsuru Yoo, Henry Sahlstrom, Ted Walters, Robert Lorentzen, Justin Nocerino, John Khan, Osman Cravens, Robert Valles, Juan Toporow, Chantal Gomez, Trinidad Bazan, Loreto Pazos Bailey, Sheila GP IEEE TI Results from an international measurement round robin of III-V triple-junction solar cells under air mass zero SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB This paper reports the results of an international measurement round robin of monolithic, triple-junction, GaInP/GaAs/Ge space solar cells. Eight laboratories representing national labs, solar cell vendors and space solar cell consumers, measured cells using in-house reference cells and compared those results to measurements made where each lab used the same set of reference cells. The results show that most of the discrepancy between laboratories is likely due to the quality of the standard cells rather than the measurement system or solar simulator used. C1 [Jenkins, Phillip; Scheiman, David] Ohio Aerosp Inst, NASA, GRC, MS 302-1, Cleveland, OH 44135 USA. [Goodbody, Chris] QinetiQ, Farnborough, Hants, England. [Baur, Carsten] Fraunhofer Inst Solar Energy Syst, Freiburg, Germany. [Sharps, Paul] Emcore Corp, Albuquerque, NM USA. [Imaizumi, Mitsuru] JAXA Tsukuba Space Ctr, Tsukuba, Ibaraki, Japan. [Yoo, Henry] VSSV, Air Force Res Lab, Albuquerque, NM USA. [Sahlstrom, Ted] Dynacs Inc, Palm Harbor, FL USA. [Walters, Robert] US Naval Res Lab, Washington, DC USA. [Lorentzen, Justin] SFA Inc, Orlando, FL USA. [Nocerino, John] Aerosp Corp, El Segundo, CA USA. [Khan, Osman; Cravens, Robert; Valles, Juan] Spectrolab, Sylmar, CA USA. [Toporow, Chantal] Northrop Grumman, Falls Church, VA USA. [Gomez, Trinidad; Bazan, Loreto Pazos] INTA SPASOLAB, Madrid, Spain. [Bailey, Sheila] NASA, Glenn Res Ctr, Washington, DC 20546 USA. RP Jenkins, P (reprint author), Ohio Aerosp Inst, NASA, GRC, MS 302-1, Cleveland, OH 44135 USA. EM Phil.Jenkins@grc.nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1968 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601180 ER PT B AU Landis, GA Hyatt, D AF Landis, Geoffrey A. Hyatt, Dan CA MER Athena Science Team GP IEEE TI The solar spectrum on the Martian surface and its effect on photovoltaic performance SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc ID MARS AB Solar cells operating on the surface of Mars receive a spectrum of illumination different from the AMO spectrum, since the sunlight is filtered by dust suspended in the atmosphere. This spectrum changes with the amount of dust in the atmosphere, as well as with air mass change due to time of day and season. This spectral variation affects the performance of solar cells. We used data from Mars Exploration Rovers to measure this spectrum. By comparing the measured intensity with the known reflectance of the pancam calibration target on the rovers Spirit and Opportunity, we measure the solar spectrum reaching the surface. The effect of this spectrum on the performance of solar cells is then calculated based on the spectral response of several different solar cell types. C1 [Landis, Geoffrey A.] NASA, Glenn Res Ctr, 21000 Brookpark Rd,M-S 302, Cleveland, OH 44135 USA. [Hyatt, Dan] NASA, Elyria High Sch, SHARP Program, Elyria, OH 44035 USA. RP Landis, GA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd,M-S 302, Cleveland, OH 44135 USA. EM geoffrey.a.landis@nasa.gov NR 13 TC 0 Z9 0 U1 1 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1979 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601183 ER PT B AU O'Neill, M Howe, J Fikes, J Fork, R Phillips, D Aiken, D McDanal, AJ AF O'Neill, Mark Howe, Joe Fikes, John Fork, Richard Phillips, Dane Aiken, Dan McDanal, A. J. GP IEEE TI Stretched Lens Array (SLA) for collection and conversion of infrared laser light: 45% efficiency demonstrated for near-term 800 W/kg space power system SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB For the past 21/2 years, our team has been developing a unique photovoltaic concentrator array for collection and conversion of infrared laser light. This laser-receiving array has evolved from the solar-receiving Stretched Lens Array (SLA). The laser-receiving version of SLA is being developed for space power applications when or where sunlight is not available (e.g., the eternally dark lunar polar craters). The laser-receiving SLA can efficiently collect and convert beamed laser power from orbiting spacecraft or other sources (e.g., solar-powered lasers on the permanently illuminated ridges of lunar polar craters). A dual-use version of SLA can produce power from sunlight during sunlit portions of the mission, and from beamed laser light during dark portions of the mission. SLA minimizes the cost and mass of photovoltaic cells by using gossamer-like Fresnel lenses to capture and focus incoming light (solar or laser) by a factor of 8.5X, thereby providing a cost-effective, ultra-light space power system. C1 [O'Neill, Mark; McDanal, A. J.] ENTECH Inc, Keller, TX 76248 USA. [Howe, Joe; Fikes, John] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Fork, Richard; Phillips, Dane] Univ Alabama, Huntsville, AL 35899 USA. [Aiken, Dan] EMCORE Photovolta, Albuquerque, NM 87123 USA. RP O'Neill, M (reprint author), ENTECH Inc, Keller, TX 76248 USA. FU NASA FX The authors gratefully acknowledge NASAs support of the work presented in this paper. NR 5 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 1998 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601188 ER PT B AU O'Neill, M Piszczor, M Brandhorse, H Carpenter, C McDanal, AJ AF O'Neill, Mark Piszczor, Michael Brandhorse, Henry Carpenter, Christian McDanal, A. J. GP IEEE TI Stretched Lens Array (SLA) Solar Electric Propulsion (SEP) space tug: SLA-SEP offers multi-billion-dollar savings delivering lunar exploration cargo SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB For the past three years, our team has been developing, refining, and maturing a unique solar array technology known as the Stretched Lens Array (SLA). SLA is a cost-effective, modular, scalable, and mass-producible space power technology, offering an unprecedented portfolio of near-term performance metrics, including > 300 W/m(2) power density, > 300 W/kg specific power, > 80 kW/m(3) stowed power, and 300-600 V operating voltage. In addition, SLA enables super-shielding of the solar cells for excellent radiation hardness at low mass penalty. These attributes make SLA ideally suited for reusable Solar Electric Propulsion (SEP) space tugs, especially those which haul cargo from low earth orbit (LEO) to the Moon. NASA's lunar exploration program will require hundreds of metric tons (MT) of cargo to be delivered to the Moon in the 2020 timeframe. As shown in this paper, SLA-SEP tugs will offer multi-billion-dollar savings over conventional chemically fueled lunar cargo delivery approaches. C1 [O'Neill, Mark; McDanal, A. J.] ENTECH Inc, Keller, TX 76248 USA. [Piszczor, Michael] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Brandhorse, Henry] Auburn Univ, Auburn, AL 36849 USA. [Carpenter, Christian] Aerojet, Redmond, WA 98052 USA. RP O'Neill, M (reprint author), ENTECH Inc, Keller, TX 76248 USA. FU NASA FX The authors gratefully acknowledge NASAs support of the work presented in this paper. NR 5 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 2002 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601189 ER PT B AU O'Neill, M Howe, J Fikes, J Lollar, L Carrington, C Suzuki, N Piszozor, M Hoppe, D Eskenazi, M Aiken, D Fulton, M Brandhorst, H Schuller, M McDanal, AJ AF O'Neill, Mark Howe, Joe Fikes, John Lollar, Louis Carrington, Connie Suzuki, Nantel Piszozor, Michael Hoppe, David Eskenazi, Michael Aiken, Dan Fulton, Michael Brandhorst, Henry Schuller, Michael McDanal, A. J. GP IEEE TI Stretched Lens Array SquareRigger (SLASR): A new space array for high-power missions SO CONFERENCE RECORD OF THE 2006 IEEE 4TH WORLD CONFERENCE ON PHOTOVOLTAIC ENERGY CONVERSION, VOLS 1 AND 2 LA English DT Proceedings Paper CT 4th World Conference on Photovoltaic Energy Conversion CY MAY 07-12, 2006 CL Waikoloa, HI SP IEEE Electron Devices Soc AB For the past three years, our team has been developing, refining, and maturing a unique solar array technology known as Stretched Lens Array SquareRigger (SLASR). As described in this paper, SLASR offers an unprecedented portfolio of performance metrics, including: Areal Power Density = 300 - 400 W/m(2) Specific Power 300 W/kg - 500 W/kg Stowed Power 80 - 120 kW/m(3) Scalable Array Power = 4 kW to 100's of kWs Super-Insulated Small Cell Circuit = High-Voltage (300600 V) Operation at Low Mass Penalty Super-Shielded Small Cell Circuit = Excellent Radiation Hardness at Low Mass Penalty 85% Cell Area Savings = 66% to 75% Lower Array Cost per Waft than One-Sun Array Modular, Scalable, & Mass-Producible at MW's per Year Using Existing Capacities. C1 [O'Neill, Mark; McDanal, A. J.] ENTECH Inc, Keller, TX 76248 USA. [Howe, Joe; Fikes, John; Lollar, Louis; Carrington, Connie; Hoppe, David] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Suzuki, Nantel] NASA, Washington, DC 20546 USA. [Piszozor, Michael] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Eskenazi, Michael] ATK Space Syst, Goleta, CA 93117 USA. [Aiken, Dan] EMCORE Photovolta, Albuquerque, NM 87123 USA. [Fulton, Michael] Ion Beam Opt, Thousand Oaks, CA 91362 USA. [Brandhorst, Henry] Auburn Univ, Auburn, AL 36849 USA. [Schuller, Michael] Texas A&M Univ, College Stn, TX 77843 USA. RP O'Neill, M (reprint author), ENTECH Inc, Keller, TX 76248 USA. FU NASA FX The authors gratefully acknowledge NASAs support of the work presented in this paper. NR 5 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0016-3 PY 2006 BP 2006 EP + PG 2 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFD80 UT WOS:000241251601190 ER PT J AU Ladner, R Petry, F Warner, E Gupta, K AF Ladner, Roy Petry, Frederick Warner, Elizabeth Gupta, Kaylan TI Using Web Services to enhance Geographic Information Systems SO CONTROL AND CYBERNETICS LA English DT Article DE ontology; Web Services; spatial data; GIS AB In this paper we describe an approach to the extension of geographic information systems to take advantage of the continuing development of capabilities of the Semantic Web. This is presented in the context of a portal based Geospatial Information Database (GIDB (TM)), an object-oriented spatial database capable of storing multiple data types from multiple sources. We have developed our approach for a specific domain, spatially oriented, meteorological and oceanographic, but this can clearly be applied to other spatial data domains. Finally we illustrate the use of the ontology development system based on Generative Sublanguage Ontologies (GSO), a type of linguistic ontology inspired by the Generative Lexicon Theory, to develop effective domain ontologies. C1 DMAP, Naval Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS USA. AES, ITT Ind, Alexandria, VA USA. USN, Res Lab, Washington, DC USA. RP Ladner, R (reprint author), DMAP, Naval Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS USA. RI Petry, Frederick/F-9894-2010 NR 28 TC 0 Z9 0 U1 0 U2 3 PU POLISH ACAD SCIENCES SYSTEMS RESEARCH INST PI WARSAW PA NEWELSKA 6, 01-447 WARSAW, POLAND SN 0324-8569 J9 CONTROL CYBERN JI Control Cybern. PY 2006 VL 35 IS 1 BP 29 EP 46 PG 18 WC Automation & Control Systems; Computer Science, Cybernetics SC Automation & Control Systems; Computer Science GA 100SQ UT WOS:000241689400003 ER PT S AU Farrugia, CJ Matsui, H Kucharek, H Jordanova, VK Torbert, RB Ogilvie, KW Berdichevsky, DB Smith, CW Skoug, R AF Farrugia, C. J. Matsui, H. Kucharek, H. Jordanova, V. K. Torbert, R. B. Ogilvie, K. W. Berdichevsky, D. B. Smith, C. W. Skoug, R. BE Cohen, C TI Survey of intense Sun-Earth connection events (1995-2003) SO CORONAL MASS EJECTIONS AND SOLAR PARTICLE EVENTS IN SOLAR CYCLE 23 SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE strongly geoeffective configurations in cycle 23; interacting ejecta as cause of intense storms ID SOLAR-WIND; GEOMAGNETIC-ACTIVITY; MAGNETOSPHERE; EJECTA AB We survey the interplanetary (IP) configurations associated with the largest energy and/or power inputs to the magnetosphere in 1995-2003, i.e., from the last 2 years of solar cycle 22 to the descending phase of solar cycle 23. We work in the "epsilon" formulation of [Perreault, P., Akasofu, S.-L A study of geomagnetic storms, Geophys. J.R. Astron. Soc., 54, 547, 1978]. Using this, we calculate the energy extracted by the magnetosphere from the solar wind, and the powering of the magnetosphere by the solar wind. We carry out a statistical survey to obtain the distribution of power deposition and energy input during this 9-year period. Large events are then defined as those whose energy exceeds 10 J m(-2) and/or whose power exceeds 0.3 mW m(-2). We then correlate the large events with the strength of geomagnetic disturbances they elicited, as measured by the Dst storm index. Finally, the large events are classified in terms of the IP structures involved. (C) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. NASA, Goddard Space Flight Ctr, Space Sci Sect, L3 Govt Serv Inc, Greenbelt, MD 20771 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Farrugia, CJ (reprint author), Univ New Hampshire, Ctr Space Sci, 39 Coll Rd,Morse Hall Room 414, Durham, NH 03824 USA. EM charlie.farrugia@unh.edu OI Jordanova, Vania/0000-0003-0475-8743 NR 20 TC 10 Z9 10 U1 0 U2 1 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 3 BP 498 EP 502 DI 10.1016/j.asr.2005.05.051 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFM60 UT WOS:000243095700019 ER PT S AU Aguilar-Rodriguez, E Blanco-Cano, X Gopalswamy, N AF Aguilar-Rodriguez, E. Blanco-Cano, X. Gopalswamy, N. BE Cohen, C TI Composition and magnetic structure of interplanetary coronal mass ejections at 1 AU SO CORONAL MASS EJECTIONS AND SOLAR PARTICLE EVENTS IN SOLAR CYCLE 23 SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE interplanetary coronal mass ejections; magnetic clouds; ejecta; charge state ratio; solar wind ID SOLAR-WIND; IONIZATION STATE; DISCONTINUITIES; PLASMA; IMP-8; SHOCK; IONS AB We study the magnetic structure and charge state ratio of interplanetary coronal mass ejections (ICMEs) observed by ACE and Wind spacecraft. Measurements of abundances and charge state ratio of heavy ions (e.g. O(7+)/O(6+)/C(6+)/C(5+), and Mg(10+)/O(6+)) in the plasma as well as magnetic field structure are important tracers for physical conditions and processes in the source regions of ICMEs. We used ion composition (from ACE), plasma (from Wind) and magnetic field (from Wind and ACE) data from 1998 to 2002. Using the low proton temperature criterion, a common plasma signature of ICMEs, we identified 154 events which include magnetic clouds, non-cloud ejecta and complex ICMEs. The latter one refers to compound events resulting from the overtaking of successive ICMEs which can include both magnetic clouds and non-cloud ejecta. We find that there is a close relationship between the increase in the charge state ionization factor and the magnetic structure of ICMEs. Events with magnetic cloud topology show higher Q(O7+/O6+) and Q(Mg10+/O6+) charge state ratios than those with non-magnetic cloud structure. However, both magnetic cloud and non-cloud events show an increase in these ratios when compared with the ambient solar wind. In contrast, perhaps due to instrumental effects, the charge state ratio Q(C6+/C5+) for all events does not show a real enhancement when compared with the ambient solar wind. The difference in ionization states between non-cloud ejecta and magnetic clouds is more pronounced in fast solar wind than when events are embedded in slow wind. (C) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico. Catholic Univ Amer, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. RP Aguilar-Rodriguez, E (reprint author), Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico. EM ernesto@lepvax.gsfc.nasa.gov; xbc@geofisica.unam.mx; gopals@fugee.gsfc.nasa.gov RI Gopalswamy, Nat/D-3659-2012 NR 24 TC 3 Z9 3 U1 0 U2 2 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 3 BP 522 EP 527 DI 10.1016/j.asr.2005.01.051 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFM60 UT WOS:000243095700023 ER PT S AU Richardson, JD Liu, Y Wang, C Burlaga, LF AF Richardson, J. D. Liu, Y. Wang, C. Burlaga, L. F. BE Cohen, C TI ICMES at very large distances SO CORONAL MASS EJECTIONS AND SOLAR PARTICLE EVENTS IN SOLAR CYCLE 23 SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE ICMEs; solar wind; heliosphere ID CORONAL MASS EJECTION; VOYAGER 2 OBSERVATIONS; SOLAR-WIND; AU; SHOCK; HELIOSPHERE; DENSITY; ULYSSES; FLOWS AB This paper reviews recent work on the observations and evolution of interplanetary coronal mass ejections (ICMEs) in the outer heliosphere. Several case studies are shown following ICMEs or their preceding shocks from 1 AU to Voyager 2 at large (>50 AU) distances. Low temperature/speed ratios and high helium abundances have been used to create lists of ICMEs. We combine lists from the inner (0.3-5.3 AU) and outer (1-30 AU) heliosphere to perform a statistical study of ICME evolution. ICMEs expand, on average, by a factor of 5 in width between 1 and 10-15 AU, then maintain a constant width as they move beyond 15 AU. The density and magnetic field decrease more rapidly in ICMEs than the solar wind, consistent with ICME expansion. The temperature, however, decreases less rapidly in ICMEs despite their expansion, indicating that ICMEs are preferentially heated. At solar maximum, ICMEs interact with the ambient solar wind to form large pressure pulses in the outer heliosphere with correlated speed, density, and magnetic field increases. (C) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. Chinese Acad Sci, Lab Space Weather, Beijing, Peoples R China. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Richardson, JD (reprint author), MIT, Kavli Ctr Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM jdr@space.mit.edu OI Liu, Ying/0000-0002-3483-5909 NR 33 TC 15 Z9 15 U1 0 U2 18 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 3 BP 528 EP 534 DI 10.1016/j.asr.2005.06.049 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFM60 UT WOS:000243095700024 ER PT J AU Lee, AK Buehler, MG Newman, DK AF Lee, AK Buehler, MG Newman, DK TI Influence of a dual-species biofilm on the corrosion of mild steel SO CORROSION SCIENCE LA English DT Article DE carbon steel (A); EIS (B); microbiological corrosion (C) ID MICROBIALLY INFLUENCED CORROSION; DESULFOVIBRIO-DESULFURICANS; IRON RESPIRATION; CARBON-STEEL; CULTURES; INHIBITION; PRODUCTS; SULFIDE AB The effect of a dual-species biofilm on the corrosion of carbon steel was examined using two bacterial species: the iron-reducer, Shewanella oneidensis (MR-1), and the sulfate-reducer, Desulfovibrio desufuricans (G20). These experiments exploit the fact that the products of their metabolism (ferrous iron or sulfide) affect the corrosion rate of carbon steel in opposite ways. Electrochemical impedance spectroscopy (EIS) shows that over a short time period, co-cultures of MR-1 and G20 protect steel from corrosion. The fact that an iron-reducing bacterium can inhibit corrosion when a corrosion-enhancing bacterium is present warrants future study with respect to its potential applicability to the design of biological corrosion-control measures. (C) 2005 Elsevier Ltd. All rights reserved. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Newman, DK (reprint author), CALTECH, Div Geol & Planetary Sci, MS 100-23, Pasadena, CA 91125 USA. EM dkn@caltech.edu NR 21 TC 28 Z9 36 U1 1 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0010-938X J9 CORROS SCI JI Corrosion Sci. PD JAN PY 2006 VL 48 IS 1 BP 165 EP 178 DI 10.1016/j.corsci.2004.11.013 PG 14 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA 002NS UT WOS:000234618800012 ER PT S AU Palacios, DM Swartzander, GA AF Palacios, David M. Swartzander, G. A., Jr. BE Mouroulis, PZ Smith, WJ Johnson, RB TI The high contrast performance of an optical vortex coronagraph SO CURRENT DEVELOPMENTS IN LENS DESIGN AND OPTICAL ENGINEERING VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Current Developments in Lens Design and Optical Engineering VII CY AUG 14-15, 2006 CL San Diego, CA SP SPIE DE coronagraphs; terrestrial planets; optical vortices ID PHASE MASK CORONAGRAPH AB The goal of the Terrestrial Planet Finder Mission is to detect and characterize Earth-Re planets. Detection of these faint objects, which appear very close to their parent stars, requires a coronagraph capable of achieving better than 100 starlight suppression within a few Airy rings of the stellar image. The coronagraph is also required to maintain this high stellar extinction over a 100nm spectral bandwidth. To ease requirements on the telescope, a high planet light throughput and low sensitivity to wave front aberrations are also desirable features. An optical vortex coronagraph is a promising candidate architecture, which makes use of a spiral phase plate placed in an intermediate image plane to null out the stellar signal. This architecture has the advantage of high stellar extinction, high planet light throughput, and low sensitivity to wave front aberrations. Here we report the high contrast performance of an optical vortex coronagraph limited by the manufacturability of the spiral phase plate. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Palacios, DM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM David.M.Palacios@jpl.nasa.gov; grovers@u.arizona.edu OI Swartzlander, Grover/0000-0003-3513-2225 NR 22 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 0-8194-6367-1 J9 P SOC PHOTO-OPT INS PY 2006 VL 6288 AR 62880B DI 10.1117/12.682088 PG 12 WC Optics SC Optics GA BFG48 UT WOS:000241726900010 ER PT B AU Dai, YS Hinchey, M Madhusoodan, M Rash, JL Zou, X AF Dai, Yuan-Shun Hinchey, Michael Madhusoodan, Manish Rash, James L. Zou, Xukai TI A prototype model for self-healing and self-reproduction in swarm robotics system SO DASC 2006: 2ND IEEE INTERNATIONAL SYMPOSIUM ON DEPENDABLE, AUTONOMIC AND SECURE COMPUTING, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Symposium on Depenable, Autonomic and Secure Computing CY SEP 30-OCT 01, 2006 CL Indianapolis, IN SP IEEE Comp Soc, Task Force Autonomous & Auton Syst, Indiana Univ-Purdue Univ AB A Swarm Robotics System is a special type of wide-area and large-scale distributed system, which focuses on a group of robots cooperating to achieve the same goal using Swarm Intelligence. To treat the Swarm Robotics System with the self-healing and self-reproduction functions, this paper studied a prototype model based on the virtual neurons, autonomous self-diagnosis, consequence-oriented prescription, autonomous selfcuring, and setf-reproduction. This prototype system with self-healing has been implemented in the Trusted Electronics and Grid Obfuscation (TEGO) research center. Several practical cases were studied to show the effectiveness and efficiency of the model. The results demonstrate that the self-healing mechanism makes the system more reliable and the performance much improved, not only against failures, but also against failure propagations. C1 [Dai, Yuan-Shun; Madhusoodan, Manish; Zou, Xukai] Indiana Univ Purdue Univ, Dept Comp & Informat Sci, Sch Sci, Indianapolis, IN 46202 USA. [Hinchey, Michael; Rash, James L.] NASA, Goddard Space Flight Ctr, Informat Syst Div, Greenbelt, MD 20771 USA. RP Dai, YS (reprint author), Indiana Univ Purdue Univ, Dept Comp & Informat Sci, Sch Sci, Indianapolis, IN 46202 USA. NR 18 TC 2 Z9 2 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2539-3 PY 2006 BP 3 EP + PG 2 WC Computer Science, Theory & Methods SC Computer Science GA BFG35 UT WOS:000241699300001 ER PT B AU Pena, J Hinchey, MG Sterritt, R Ruiz-Cortes, A Resinas, M AF Pena, Joaquin Hinchey, Michael G. Sterritt, Roy Ruiz-Cortes, Antonio Resinas, Manuel TI A model-driven architecture approach for modeling, specifying and deploying policies in autonomous and autonomic systems SO DASC 2006: 2ND IEEE INTERNATIONAL SYMPOSIUM ON DEPENDABLE, AUTONOMIC AND SECURE COMPUTING, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Symposium on Depenable, Autonomic and Secure Computing CY SEP 30-OCT 01, 2006 CL Indianapolis, IN SP IEEE Comp Soc, Task Force Autonomous & Auton Syst, Indiana Univ-Purdue Univ AB Autonomic Computing (AC), self-management based on high level guidance from humans, is increasingly gaining momentum as the way forward in designing reliable systems that hide complexity and conquer IT management costs. Effectively, AC may be viewed as Policy-Based Self-Management. The Model Driven Architecture (MDA) approach focuses on building models that can be transformed into code in an automatic manner In this paper we look at ways to implement Policy-Based Self-Management by means of models that can he converted to code using transformations that follow the MDA philosophy. We propose a set of UML-hased models to specify autonomic and autonomous features along with the necessary procedures, based on modification and composition of models, to deploy a policy as an executing system. C1 [Pena, Joaquin; Ruiz-Cortes, Antonio; Resinas, Manuel] Univ Seville, Seville, Spain. [Hinchey, Michael G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Sterritt, Roy] Univ Ulster, Coleraine BT52 1SA, Londonderry, North Ireland. RP Pena, J (reprint author), Univ Seville, Seville, Spain. EM joaquinp@us.es; Michael.G.Hinchey@nasa.gov; r.sterritt@ulster.ac.uk; aruiz@us.es; resman@tdg.lsi.us.es RI Resinas, Manuel/B-3063-2008; Ruiz-Cortes, Antonio/B-9056-2008; Pena, Joaquin /K-8217-2012 OI Resinas, Manuel/0000-0003-1575-406X; Ruiz-Cortes, Antonio/0000-0001-9827-1834; Pena, Joaquin /0000-0001-9216-9695 NR 16 TC 6 Z9 6 U1 0 U2 2 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2539-3 PY 2006 BP 19 EP + PG 3 WC Computer Science, Theory & Methods SC Computer Science GA BFG35 UT WOS:000241699300003 ER PT B AU Dai, YS Hinchey, M Qi, MR Zou, XK AF Dai, Yuan-Shun Hinchey, Michael Qi, Mingrui Zou, Xukai TI Autonomic security and self-protection based on feature-recognition with virtual neurons SO DASC 2006: 2ND IEEE INTERNATIONAL SYMPOSIUM ON DEPENDABLE, AUTONOMIC AND SECURE COMPUTING, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Symposium on Depenable, Autonomic and Secure Computing CY SEP 30-OCT 01, 2006 CL Indianapolis, IN SP IEEE Comp Soc, Task Force Autonomous & Auton Syst, Indiana Univ-Purdue Univ AB The Internet and networks are not security-oriented by design so that myriad problems are compromising today's computer systems. This paper presented an autonomic security mechanism based on the virtual neurons and feature recognition. A prototype model of the virtual neuron is designed and the distributed virtual neurons are organized in a compound peer-to-peer and hierarchical structure. Then, the autonomic security mechanism is implemented via features recognized by the distributed virtual neurons. The paper presented. how the feature recognition and virtual neurons work to automatically detect various security problems that are currently hard to defend against, including Eavesdropping, Replay, Masquerading, Spoofing, and DoS. A simulation system was developed and different cases were studied. C1 [Dai, Yuan-Shun; Qi, Mingrui; Zou, Xukai] IUPUI, Dept Comp & Informat Sci, Indiana, PA USA. [Hinchey, Michael] NASA, Goddard Space Flight Ctr, Informat Syst Div, Indiana, PA 20771 USA. RP Dai, YS (reprint author), IUPUI, Dept Comp & Informat Sci, Indiana, PA USA. EM ydai@cs.iupui.edu; michael.g.hinchey@nasa.gov; qim@cs.iupui.edu; xkzou@cs.iupui.edu NR 22 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2539-3 PY 2006 BP 227 EP + PG 2 WC Computer Science, Theory & Methods SC Computer Science GA BFG35 UT WOS:000241699300028 ER PT B AU Stakhanova, N Basu, S Lutz, RR Wong, J AF Stakhanova, Natalia Basu, Samik Lutz, Robyn R. Wong, Johnny TI Automated caching of behavioral patterns for efficient run-time monitoring SO DASC 2006: 2ND IEEE INTERNATIONAL SYMPOSIUM ON DEPENDABLE, AUTONOMIC AND SECURE COMPUTING, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Symposium on Depenable, Autonomic and Secure Computing CY SEP 30-OCT 01, 2006 CL Indianapolis, IN SP IEEE Comp Soc, Task Force Autonomous & Auton Syst, Indiana Univ-Purdue Univ AB Run-time monitoring is a powerful approach for dynamically detecting faults or malicious activity of software systems. However there are often two obstacles to the implementation of this approach in practice: (1) that developing correct and/or faulty behavioral patterns can be a difficult, labor-intensive process, and (2) that use of such pattern-monitoring must provide rapid turn-around or response time. We present a novel data structure, called extended action graph, and associated algorithms to overcome these drawbacks. At its core, our technique relies on effectively identifying and caching specifications from (correct/faulty) patterns learned via machine-learning algorithm. We describe the design and implementation of our technique and show its practical applicability in the domain of security monitoring of sendmail software. C1 [Stakhanova, Natalia; Basu, Samik; Lutz, Robyn R.; Wong, Johnny] Iowa State Univ, Dept Comp Sci, Ames, IA 50011 USA. [Lutz, Robyn R.] CALTECH, Jet Prop Lab, Ctr Infrared Proc & Anal, Pasadena, CA 91109 USA. RP Stakhanova, N (reprint author), Iowa State Univ, Dept Comp Sci, Ames, IA 50011 USA. EM ndubrov@iastate.edu; sbasu@iastate.edu; rlutz@iastate.edu; wong@iastate.edu FU NSF [0204139, 0205588, 0541163] FX The author is supported in part by NSF grants 0204139, 0205588, & 0541163. It was performed in part at the Univ. of WI. NR 20 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2539-3 PY 2006 BP 333 EP + PG 2 WC Computer Science, Theory & Methods SC Computer Science GA BFG35 UT WOS:000241699300041 ER PT J AU Sydeman, WJ Brodeur, RD Grimes, CB Bychkov, AS McKinnell, S AF Sydeman, William J. Brodeur, Richard D. Grimes, Churchill B. Bychkov, Alexander S. McKinnell, Stewart TI Marine habitat "hotspots" and their use by migratory species and top predators in the North Pacific Ocean: Introduction SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Editorial Material ID RESERVES C1 PRBO Conservat Sci, Marine Ecol Div, Stinson Beach, CA 94970 USA. Natl Marine Fisheries Serv, Newport, OR 97365 USA. Natl Marine Fisheries Serv, Santa Cruz, CA 95060 USA. Natl Pacific Marine Sci Org, Sidney, BC V8L 4B2, Canada. RP Sydeman, WJ (reprint author), PRBO Conservat Sci, Marine Ecol Div, 4990 Shoreline Highway, Stinson Beach, CA 94970 USA. EM wsydeman@prbo.org; bychkov@pices.int NR 9 TC 37 Z9 39 U1 1 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PY 2006 VL 53 IS 3-4 BP 247 EP 249 DI 10.1016/j.dsr2.2006.03.001 PG 3 WC Oceanography SC Oceanography GA 066AO UT WOS:000239201900001 ER PT J AU Reese, DC Brodeur, RD AF Reese, D. C. Brodeur, R. D. TI Identifying and characterizing biological hotspots in the northern California Current SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article; Proceedings Paper CT 13th Annual Meeting of the North-Pacific-Marine-Science-Organization (PICES) CY OCT 14-24, 2004 CL Honolulu, HI SP N Pacific Marine Sci Org DE hotspots; nekton; community composition; species diversity; geostatistics; habitats; California Current ID MARINE PROTECTED AREAS; CURRENT SYSTEM; BIODIVERSITY; ECOSYSTEM; ZOOPLANKTON; OCEAN; CONSERVATION; ECOLOGY; REVEAL AB Understanding how marine animals utilize their environment and identifying important habitats are crucial for understanding how marine ecosystems function. The goal of the present study is to identify biologically rich areas within the northern California Current and to determine the environmental characteristics occurring within these areas. We analyzed how surface nekton are distributed in the northern California Current, not only in space and time but also with reference to species assemblages, habitat characteristics, and environmental factors. Sampling was conducted during June and August of 2000 and 2002 as part of the US GLOBEC mesoscale surveys from Newport, Oregon, in the north to Crescent City, California, in the south. A geostatistical approach was used to create surfaces to be used in a GIS to determine the presence or absence of biological hotspots throughout the region. Two biological hotspots were identified and determined to persist in space and time, yet differed with respect to biological and physical features and in the amount of area covered. We used indicator species analyses (ISA) and non-metric multidimensional scaling (NMS) to explore patterns in community structure. Results indicate that although the locations of the biological hotspots persisted over the course of the study, the habitat characteristics and nekton community composition within each hotspot varied over time. The most consistent environmental parameters explaining the distributions were sea-surface temperature, salinity, and density, indicating the likely structuring mechanism of the hotspots is related to the flow through the region and differing patterns of circulation. (c) 2006 Elsevier Ltd. All rights reserved. C1 Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Reese, DC (reprint author), Oregon State Univ, Coll Ocean & Atmospher Sci, 104 COAS Admin Bldg, Corvallis, OR 97331 USA. EM dreese@lifetime.oregonstate.edu NR 47 TC 36 Z9 37 U1 1 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PY 2006 VL 53 IS 3-4 BP 291 EP 314 DI 10.1016/j.dsr2.2006.01.014 PG 24 WC Oceanography SC Oceanography GA 066AO UT WOS:000239201900004 ER PT J AU Gende, SM Sigler, MF AF Gende, Scott M. Sigler, Michael F. TI Persistence of forage fish 'hot spots' and its association with foraging Steller sea lions (Eumetopias jubatus) southeast Alaska SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article; Proceedings Paper CT 13th Annual Meeting of the North-Pacific-Marine-Science-Organization (PICES) CY OCT 14-24, 2004 CL Honolulu, HI SP N Pacific Marine Sci Org DE Steller sea lions; herring; hot spot persistence; foraging effort ID HERRING CLUPEA-HARENGUS; ANTARCTIC FUR SEALS; ARCTOCEPHALUS-GAZELLA; SPATIAL-DISTRIBUTION; MARINE PREDATOR; PREY; PREDICTABILITY; AGGREGATIONS; ALBATROSSES; STRATEGIES AB Whereas primary and secondary productivity at oceanic 'hotspots' may be a function of upwelling and temperature fronts, the aggregation of higher-order vertebrates is a function of their ability to search for and locate these areas. Thus, understanding how predators aggregate at these productive foraging areas is germane to the study of oceanic hot spots. We examined the spatial distribution of forage fish in southeast Alaska for three years to better understand Steller sea lion (Eumetopias jubatus) aggregations and foraging behavior. Energy densities (millions KJ/km(2)) of forage fish were orders of magnitude greater during the winter months (November-February), due to the presence of schools of overwintering Pacific herring (Clupea pallasi). Within the winter months, herring consistently aggregated at a few areas, and these areas persisted throughout the season and among years. Thus, our study area was characterized by seasonally variable, highly abundant but highly patchily distributed forage fish hot spots. More importantly, the persistence of these forage fish hot spots was an important characteristic in determining whether foraging sea lions utilized them. Over 40% of the variation in the distribution of sea lions on our surveys was explained by the persistence of forage fish hot spots. Using a simple spatial model, we demonstrate that when the density of these hot spots is low, effort necessary to locate these spots is minimized when those spots persist through time. In contrast, under similar prey densities but lower persistence, effort increases dramatically. Thus an important characteristic of pelagic hot spots is their persistence, allowing predators to predict their locations and concentrate search efforts accordingly. (c) 2006 Elsevier Ltd. All rights reserved. C1 Natl Pk Serv, Coastal Program, Juneau, AK 99801 USA. NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Juneau, AK 99801 USA. RP Gende, SM (reprint author), Natl Pk Serv, Coastal Program, Glacier Bay Field Stn,3100 Natl Pk Rd, Juneau, AK 99801 USA. EM scott_gende@nps.gov; Mike.Sigler@noaa.gov NR 40 TC 39 Z9 42 U1 2 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PY 2006 VL 53 IS 3-4 BP 432 EP 441 DI 10.1016/j.dsr2.2006.01.005 PG 10 WC Oceanography SC Oceanography GA 066AO UT WOS:000239201900013 ER PT J AU Carr, ME Friedrichs, MAM Schmeltz, M Aita, MN Antoine, D Arrigo, KR Asanuma, I Aumont, O Barber, R Behrenfeld, M Bidigare, R Buitenhuis, ET Campbell, J Ciotti, A Dierssen, H Dowell, M Dunne, J Esaias, W Gentili, B Gregg, W Groom, S Hoepffner, N Ishizaka, J Kameda, T Le Quere, C Lohrenz, S Marra, J Melin, F Moore, K Morel, A Reddy, TE Ryan, J Scardi, M Smyth, T Turpie, K Tilstone, G Waters, K Yamanaka, Y AF Carr, Mary-Elena Friedrichs, Marjorie A. M. Schmeltz, Marjorie Aita, Maki Noguchi Antoine, David Arrigo, Kevin R. Asanuma, Ichio Aumont, Olivier Barber, Richard Behrenfeld, Michael Bidigare, Robert Buitenhuis, Erik T. Campbell, Janet Ciotti, Aurea Dierssen, Heidi Dowell, Mark Dunne, John Esaias, Wayne Gentili, Bernard Gregg, Watson Groom, Steve Hoepffner, Nicolas Ishizaka, Joji Kameda, Takahiko Le Quere, Corinne Lohrenz, Steven Marra, John Melin, Frederic Moore, Keith Morel, Andre Reddy, Tasha E. Ryan, John Scardi, Michele Smyth, Tim Turpie, Kevin Tilstone, Gavin Waters, Kirk Yamanaka, Yasuhiro TI A comparison of global estimates of marine primary production from ocean color SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article ID SATELLITE CHLOROPHYLL; BIOOPTICAL PROPERTIES; REGIONAL SCALES; MODEL; PHYTOPLANKTON; WATERS; SEA; PHOTOSYNTHESIS; BIOSPHERE; GROWTH AB The third primary production algorithm round robin (PPARR3) compares output from 24 models that estimate depth-integrated primary production from satellite measurements of ocean color, as well as seven general circulation models (GCMs) coupled with ecosystem or biogeochemical models. Here we compare the global primary production fields corresponding to eight months of 1998 and 1999 as estimated from common input fields of photosynthetically-available radiation (PAR), sea-surface temperature (SST), mixed-layer depth, and chlorophyll concentration. We also quantify the sensitivity of the ocean-color-based models to perturbations in their input variables. The pair-wise correlation between ocean-color models was used to cluster them into groups or related output, which reflect the regions and environmental conditions under which they respond differently. The groups do not follow model complexity with regards to wavelength or depth dependence, though they are related to the manner in which temperature is used to parameterize photosynthesis. Global average PP varies by a factor of two between models. The models diverged the most for the Southern Ocean, SST under 10 degrees C, and chlorophyll concentration exceeding 1 mg Chlm(-3). Based on the conditions under which the model results diverge most, we conclude that current ocean-color-based models are challenged by high-nutrient low-chlorophyll conditions, and extreme temperatures or chlorophyll concentrations. The GCM-based models predict comparable primary production to those based on ocean color: they estimate higher values in the Southern Ocean, at low SST, and in the equatorial band, while they estimate lower values in eutrophic regions (probably because the area of high chlorophyll concentrations is smaller in the GCMs). Further progress in primary production modeling requires improved understanding of the effect of temperature on photosynthesis and better parameterization of the maximum photosynthetic rate. (c) 2006 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91101 USA. Old Dominion Univ, Ctr Coastal Phys Oceanog, Norfolk, VA 23529 USA. Fontier Res Ctr Global Change, Ecosyst Change Res Program, Yokohama, Kanagawa 2360001, Japan. Oceanog Lab, F-06238 Villefranche Sur Mer, France. Stanford Univ, Dept Geophys, Stanford, CA 94305 USA. Tokyo Univ Informat Sci, Chiba 2658501, Japan. Univ Paris 06, Lab Oceanog Dynam & Climatol, CNRS, MHNN,IRD, F-75252 Paris 05, France. Duke Univ, Marine Lab, Beaufort, NC 28516 USA. Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. Univ Hawaii, Dept Oceanog, Honolulu, HI 96822 USA. Max Planck Inst Biogeochem, D-07701 Jena, Germany. Univ New Hampshire, Durham, NH 03824 USA. Univ Estadual Paulista, BR-11330900 Sao Paulo, Brazil. Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. Joint Res Ctr, Inland & Marine Waters Unit, I-21020 Ispra, Italy. NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA. NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. Plymouth Marine Lab, Remote Sensing Grp, Plymouth PL1 3DH, Devon, England. Nagasaki Univ, Fac Fisheries, Nagasaki 8528521, Japan. Natl Res Inst Far Seas Fisheries, Grp Oceanog, Shizuoka 4248633, Japan. Univ E Anglia, Norwich NR4 7TJ, Norfolk, England. British Antarctic Survey, Norwich NR4 7TJ, Norfolk, England. Stennis Space Ctr, Dept Marine Sci, Stennis Space Ctr, MS 39529 USA. Lamont Doherty Earth Observ, Palisades, NY 10964 USA. Univ Calif Irvine, Irvine, CA 92697 USA. MBARI, Moss Landing, CA 95039 USA. Univ Roma Tor Vergata, Dept Biol, I-00133 Rome, Italy. NOAA, Coastal Serv Ctr, Charleston, SC 29405 USA. Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. RP Carr, ME (reprint author), CALTECH, Jet Propuls Lab, 4800 Oak Grove Dr, Pasadena, CA 91101 USA. EM Mary-Elena.Carr@jpl.nasa.gov RI Ciotti, Aurea Maria/B-7188-2011; Groom, Steve/A-1355-2012; Buitenhuis, Erik/A-7692-2012; Smyth, Tim/D-2008-2012; Dunne, John/F-8086-2012; Antoine, David/C-3817-2013; Aumont, Olivier/G-5207-2016; Yamanaka, Yasuhiro/H-7393-2012; Le Quere, Corinne/C-2631-2017 OI Tilstone, Gavin/0000-0002-9347-1682; Friedrichs, Marjorie/0000-0003-2828-7595; Ciotti, Aurea Maria/0000-0001-7163-8819; Lohrenz, Steven/0000-0003-3811-2975; Buitenhuis, Erik/0000-0001-6274-5583; Dunne, John/0000-0002-8794-0489; Antoine, David/0000-0002-9082-2395; Aumont, Olivier/0000-0003-3954-506X; Yamanaka, Yasuhiro/0000-0003-3369-3248; Le Quere, Corinne/0000-0003-2319-0452 NR 54 TC 254 Z9 264 U1 10 U2 107 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PY 2006 VL 53 IS 5-7 BP 741 EP 770 DI 10.1016/j.dsr2.2006.01.028 PG 30 WC Oceanography SC Oceanography GA 067EX UT WOS:000239285700013 ER PT S AU Degani, A Shafto, M Olson, L AF Degani, Asaf Shafto, Michael Olson, Leonard BE BarkerPlummer, D Cox, R Swoboda, N TI Canonical correlation analysis: Use of composite heliographs for representing multiple patterns SO DIAGRAMMATIC REPRESENTATION AND INFERENCE, PROCEEDINGS SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 4th International Conference on Diagrammatic Representation and Inference CY JUN 28-30, 2006 CL Stanford, CA SP Apple Comp Inc, Cognit Sci Soc, Google Inc, Microsoft Corp, Royal Soc, Stanfor Univ, Stanford Univ, Ctr Study Language & Informat, Ctr Study Language & Informat Publ AB In a study of crew interaction with the automatic flight control system of the Boeing 757/767 aircraft, we observed 60 flights and recorded every change in the aircraft control modes, as well as every observable change in the operational environment. To quantify the relationships between the state of the operating environment and pilots' actions and responses, we used canonical correlation because of its unique suitability for finding multiple patterns in large datasets. Traditionally, the results of canonical correlation analysis are presented by means of numerical tables, which are not conducive to recognizing multidimensional patterns in the data. We created a sun-ray-like diagram (which we call a heliograph) to present the multiple patterns that exist in the data by employing Alexander's theory of centers. The theory describes 15 heuristic properties that help create wholeness in a design, and can be extended to the problem of information abstraction and integration as well as packing of large amounts of data for visualization. C1 NASA, Ames Res Ctr, Mountain View, CA USA. RP Degani, A (reprint author), NASA, Ames Res Ctr, Mountain View, CA USA. EM adegani@mail.arc.nasa.gov; rashafto@mail.arc.nasa.gov; lolson@mail.arc.nasa.gov NR 5 TC 4 Z9 4 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-35623-1 J9 LECT NOTES COMPUT SC PY 2006 VL 4045 BP 93 EP 97 PG 5 WC Computer Science, Artificial Intelligence SC Computer Science GA BEV64 UT WOS:000239625600010 ER PT S AU Chakraborty, D Saha, S Sen, S Clement, B AF Chakraborty, Doran Saha, Sabyasachi Sen, Sandip Clement, Bradley BE Chaudhuri, S Das, SR Paul, HS Tirthapura, S TI Negotiating monitoring task allocation for orbiters SO DISTRIBUTED COMPUTING AND NETWORKING, PROCEEDINGS SE Lecture Notes in Computer Science LA English DT Proceedings Paper CT 8th International Conference on Distributed Computing and Networking CY DEC 27-30, 2006 CL Guwahati, INDIA AB We are interested in the problem of coordination of ground-based control stations and orbiting space probes for allocating monitoring tasks for emerging environmental situations that have the potential to become catastrophic events threatening life and property. We assume that ground based sensor networks have recognized seismic, geological, atmospheric, or some other natural phenomena that has created a rapidly evolving event which needs immediate, detailed and continuous monitoring. Control stations can calculate the resources needed to monitor such situations, but must concurrently negotiate with multiple autonomous orbiters to allocate the monitoring tasks. While control stations may prefer some orbiters over others based on their position, trajectory, equipment, etc, orbiters too have prior commitments to fulfill. We evaluate three different negotiation schemes that, can be used by the control station and the orbiters to complete the monitoring task assignment. We use utilitarian and egalitarian social welfare as the metric to be maximized and discuss the relative performances of these mechanisms under different preference and resource constraints. C1 [Chakraborty, Doran; Saha, Sabyasachi; Sen, Sandip] Univ Tulsa, Dept Math & Comp Sci, Tulsa, OK 74104 USA. [Clement, Bradley] Jet Prop Lab, Pasadena, CA USA. RP Chakraborty, D (reprint author), Univ Tulsa, Dept Math & Comp Sci, Tulsa, OK 74104 USA. EM doran@utulsa.edu; saby@utulsa.edu; sandip@utulsa.edu; bclement@aig.jpl.nasa.gov FU 2006 Oklahoma NASA EPSCoR Research Initiation Grant FX This work has been supported by a 2006 Oklahoma NASA EPSCoR Research Initiation Grant NR 3 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 978-3-540-68139-7 J9 LECT NOTES COMPUT SC PY 2006 VL 4308 BP 282 EP 287 PG 6 WC Computer Science, Theory & Methods; Telecommunications SC Computer Science; Telecommunications GA BFV46 UT WOS:000244800000031 ER PT B AU Frye, SW Goldberg, MD Habib, S Talabac, S AF Frye, Stuart W. Goldberg, Mitchell D. Habib, Shahid Talabac, Stephen BE Ceballos, S TI Sensor webs: Where they are today and what are the future needs? SO DSSNS 2006: SECOND IEEE WORKSHOP ON DEPENDABILITY AND SECURITY IN SENSOR NETWORKS AND SYSTEMS LA English DT Proceedings Paper CT 2nd IEEE Workshop on Dependability and Security in Sensor Networks and Systems CY APR 24-28, 2006 CL Columbia, MD SP IEEE Comp Soc TC Complex Comp C1 [Frye, Stuart W.; Habib, Shahid; Talabac, Stephen] NASA, Goddard Space Flight Ctr, 300 E St SW, Washington, DC 20546 USA. [Goldberg, Mitchell D.] Natl Ocean & Atmospher Adm, Off Res & Applicat, Washington, DC 98115 USA. RP Frye, SW (reprint author), NASA, Goddard Space Flight Ctr, 300 E St SW, Washington, DC 20546 USA. EM Stuart.Frye@gsfc.nasa.gov; Mitch.Goldberg@noaa.gov; Shahid.Habib@nasa.gov; Stephen.J.Talabac@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2529-6 PY 2006 BP 65 EP + PG 2 WC Telecommunications SC Telecommunications GA BEN71 UT WOS:000238344700007 ER PT S AU Goldstein, ML Escoubet, CP Laakso, H AF Goldstein, M. L. Escoubet, C. P. Laakso, H. BE Steiger, RV Gedalin, M TI Multiscale, multipoint measurements from Cluster: Advancing our scientific understanding of geospace SO DYNAMICAL PROCESSES IN CRITICAL REGIONS OF THE HELIOSPHERE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 1st Isradynamics Workshop CY MAR 03-10, 2004 CL ISRAEL DE cluster mission; magnetosphere boundaries; multi-point measurements; magnetosphere dynamics; magnetosphere structure ID MINIMUM-VARIANCE; MAGNETOPAUSE; ORIENTATION; MOTION; SHOCKS; WAVES AB Cluster is the first multispacecraft mission with identical instrumentation designed to resolve spatial and temporal structures in geospace. The orbits of the four Cluster spacecraft are variable and are adjusted periodically to place the spacecraft into configurations that optimize the three-dimensional capabilities of the instrumentation. During the mission, the relative distances between the spacecraft achieved so far have ranged from 100 to 5000 km. In the summer of 2005, the maximum separations were increased to 10,000 km. The primary results of Cluster include: determining the spatial scales of such transient three-dimensional phenomena as the short large amplitude magnetic structures (SLAMS) ahead of the parallel bow shock, the scale of Earth's bow shock, the properties of bursty bulk flows in the plasmasheet, detailed measurements of the diffusion regions characteristic of magnetic reconnection events both in the magnetotail, at the magnetopause, and in the dayside polar cusps, and determinations of the source locations of both continuum radiation and auroral kilometric radiation. Space restrictions only permit a subset of those results to be mentioned. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. ESA ESTEC, SCI SH, NL-2200 AG Noordwijk, Netherlands. RP Goldstein, ML (reprint author), NASA, Goddard Space Flight Ctr, Code 692, Greenbelt, MD 20771 USA. EM melvyn.goldstein@gsfc.nasa.gov RI Goldstein, Melvyn/B-1724-2008; Gedalin, Michael/A-5153-2012 OI Gedalin, Michael/0000-0003-1236-4787 NR 27 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 1 BP 21 EP 36 DI 10.1016/j.asr.2005.01.114 PG 16 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFG32 UT WOS:000241698700004 ER PT S AU Ofman, L AF Ofman, Leon BE Steiger, RV Gedalin, M TI Wave acceleration of the fast solar wind SO DYNAMICAL PROCESSES IN CRITICAL REGIONS OF THE HELIOSPHERE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 1st Isradynamics Workshop CY MAR 03-10, 2004 CL ISRAEL DE solar corona; solar wind; Alfven waves; ion-cyclotron waves; numerical modelling; three-fluid model; hybrid model ID INTERPLANETARY SCINTILLATION MEASUREMENTS; CORONAL HOLES; SOLITARY WAVES; ALFVEN WAVES; MINOR IONS; MODEL; TEMPERATURE; 2-FLUID; ULYSSES; SIMULATIONS AB Observations show that the solar wind exhibits two modes of outflow: the slow (similar to 400 km s(-1)), high density, highly variable wind that emerges from equatorial solar regions, and the high latitude, fast (similar to 800 km s(-1)), low density, steady solar wind. The bi-modal solar wind outflow is most evident near minima of solar activity. Theoretical studies of the fast solar wind in open magnetic structures motivated by SOHO, Ulysses, and Helios observations indicate that both, high frequency kinetic waves, and low frequency MHD waves play a role in its acceleration and heating. Ion-cyclotron waves have been suggested as the main energy source of the solar wind. However, there are theoretical difficulties with the ion-cyclotron wave heating of the protons, and these waves do not heat electrons. Low frequency MHD waves are still the best candidates to transport momentum and energy far from the Sun, to accelerate the solar wind on large spatial scales. I will present recently developed two-dimensional three-fluid model that includes explicit wave acceleration, and visco-resistive dissipation. The model describes electrons, protons, and minor ions as three coupled fluids that are heated by different heating processes with the parameters constrained by observations. I will present the results of 2.5D three-fluid simulations of the fast solar wind plasma that combine the effects of MHD waves self-consistently, and ion-cyclotron waves parametrically on the acceleration and heating processes. I will present the results of hybrid kinetic models of ion-cyclotron wave heating of the heavy ions in the solar wind plasma. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Catholic Univ Amer, NASA Goddard Space Flight Ctr, Dept Phys, Greenbelt, MD 20771 USA. RP Ofman, L (reprint author), Catholic Univ Amer, NASA Goddard Space Flight Ctr, Dept Phys, Code 612-1, Greenbelt, MD 20771 USA. EM leon.ofman@gsfc.nasa.gov RI Gedalin, Michael/A-5153-2012 OI Gedalin, Michael/0000-0003-1236-4787 NR 53 TC 4 Z9 4 U1 1 U2 5 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 1 BP 64 EP 74 DI 10.1016/j.asr.2005.05.133 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFG32 UT WOS:000241698700008 ER PT J AU Kimball, JS McDonald, KC Zhao, M AF Kimball, J. S. McDonald, K. C. Zhao, M. TI Terrestrial vegetation productivity in the western arctic observed from satellite microwave and optical remote sensing SO EARTH INTERACTIONS LA English DT Article DE AVHRR; boreal; Arctic; carbon; NPP; GPP; LAI; phenology; freeze-thaw; SSM/I; WALE ID NET PRIMARY PRODUCTION; NASA SCATTEROMETER NSCAT; LEAF-AREA INDEX; CARBON-DIOXIDE; BOREAL FOREST; DATA SET; FIRE DISTURBANCE; ATMOSPHERIC CO2; WHITE SPRUCE; PLANT-GROWTH AB Global satellite remote sensing records show evidence of recent vegetation greening and an advancing growing season at high latitudes. Satellite remote sensing-derived measures of photosynthetic leaf area index (LAI) and vegetation gross and net primary productivity (GPP and NPP) from the NOAA Advanced Very High Resolution Radiometer (AVHRR) Pathfinder record are utilized to assess annual variability in vegetation productivity for Alaska and northwest Canada in association with the Western Arctic Linkage Experiment (WALE). These results are compared with satellite microwave remote sensing measurements of springtime thaw from the Special Sensor Microwave Imager (SSM/I). The SSM/I-derived timing of the primary springtime thaw event was well correlated with annual anomalies in maximum LAI in spring and summer (P <= 0.009; n = 13), and GPP and NPP (P <= 0.0002) for the region. Mean annual variability in springtime thaw was on the order of +/- 7 days, with corresponding impacts to annual productivity of approximately 1% day(-1). Years with relatively early seasonal thawing showed generally greater LAI and annual productivity, while years with delayed seasonal thawing showed corresponding reductions in canopy cover and productivity. The apparent sensitivity of LAI and vegetation productivity to springtime thaw indicates that a recent advance in the seasonal thaw cycle and associated lengthening of the potential period of photosynthesis in spring is sufficient to account for the sign and magnitude of an estimated positive vegetation productivity trend for the western Arctic from 1982 to 2000. C1 Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. Univ Montana, Coll Forestry & Conservat, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. RP Kimball, JS (reprint author), Univ Montana, Flathead Lake Biol Stn, 311 Biostn Lane, Polson, MT 59860 USA. EM johnk@ntsg.umt.edu RI Zhao, Maosheng/G-5706-2010 NR 57 TC 10 Z9 10 U1 0 U2 7 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1087-3562 J9 EARTH INTERACT JI Earth Interact. PY 2006 VL 10 AR 21 PG 22 WC Geosciences, Multidisciplinary SC Geology GA 124OP UT WOS:000243378400001 ER PT J AU Pongratz, J Bounoua, L DeFries, RS Morton, DC Anderson, LO Mauser, W Klink, CA AF Pongratz, Julia Bounoua, Lahouari DeFries, Ruth S. Morton, Douglas C. Anderson, Liana O. Mauser, Wolfram Klink, Carlos A. TI The impact of land cover change on surface energy and water balance in Mato Grosso, Brazil SO EARTH INTERACTIONS LA English DT Article DE land cover change; surface climate; Amazon; deforestation ID DOUBLED ATMOSPHERIC CO2; PARAMETERIZATION SIB2; CLIMATE CHANGE; TROPICAL DEFORESTATION; AMAZON DEFORESTATION; REGIONAL CLIMATE; CARBON; VEGETATION; MODEL; SCALE AB The sensitivity of surface energy and water fluxes to recent land cover changes is simulated for a small region in northern Mato Grosso, Brazil. The Simple Biosphere Model (SiB2) is used, driven by biophysical parameters derived from the Moderate Resolution Imaging Spectroradiometer ( MODIS) at 250-m resolution, to compare the effects of different land conversion types. The mechanisms through which changes in vegetation alter surface fluxes of energy, momentum, water, and carbon are analyzed for both wet and dry seasons. It is found that morphological changes contribute to warming and drying of the atmosphere while physiological changes, particularly those associated with a plant's photosynthetic pathway, counterbalance or exacerbate the warming depending on the type of conversion and the season. Furthermore, this study's results indicate that initial clearing of evergreen and transition forest to bare ground increases canopy temperature by up to 1.7 degrees C. For subsequent land use such as pasture or cropland, the largest effect is seen for the conversion of evergreen forest to C3 cropland during the wet season, with a 21% decrease of the latent heat flux and 0.4 degrees C increase in canopy temperature. The secondary conversion of pasture to cropland resulted in slight warming and drying during the wet season driven mostly by the change in carbon pathway from C4 to C3. For all conversions types, the daily temperature range is amplified, suggesting that plants replacing forest clearing require more temperature tolerance than the trees they replace. The results illustrate that the effect of deforestation on climate depends not only on the overall extent of clearing but also on the subsequent land use type. C1 Univ Maryland, Dept Geog, College Pk, MD 20742 USA. Univ Munich, Dept Earth & Environm Sci, Munich, Germany. Max Planck Inst Meteorol, Hamburg, Germany. NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, Brazil. Univ Brasilia, Dept Ecol, Brasilia, DF, Brazil. RP DeFries, RS (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA. EM rdefries@mail.umd.edu RI Morton, Douglas/D-5044-2012; Anderson, Liana/G-8389-2012 OI Anderson, Liana/0000-0001-9545-5136 NR 39 TC 10 Z9 10 U1 2 U2 14 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1087-3562 J9 EARTH INTERACT JI Earth Interact. PY 2006 VL 10 AR 19 PG 17 WC Geosciences, Multidisciplinary SC Geology GA 121NQ UT WOS:000243164700001 ER PT J AU Potter, C Klooster, S Hiatt, S Fladeland, M Genovese, V Gross, P AF Potter, Christopher Klooster, Steven Hiatt, Seth Fladeland, Matthew Genovese, Vanessa Gross, Peggy TI Wetlands in the United States: Satellite-derived estimation based on ecosystem carbon SO EARTH INTERACTIONS LA English DT Article DE methane; wetlands; landsat ID METHANE EMISSIONS; NATURAL WETLANDS; MINNESOTA PEATLAND; NORTHERN ONTARIO; MODEL; FLUX; CLIMATE; EXCHANGE; CANADA; FOREST AB Wetlands are an important natural source of methane to the atmosphere. The amounts of methane emitted from inundated ecosystems in the United States can vary greatly from area to area. Seasonal temperature, water table dynamics, and carbon content of soils are principal controlling factors. To calculate the effect of wetlands (and their potential conversion to other land uses) on global greenhouse gas emissions, information on area covered by various wetland types is needed, along with verified projections of spatial variation in net methane emissions. Both of these variables are poorly known, and estimates are largely unavailable at the country level. Nationwide satellite datasets for the coterminous United States (excluding Alaska) have been combined with ecosystem model predictions of monthly net carbon exchange with the atmosphere to produce the first detailed mapping of methane fluxes from natural wetlands on a monthly and annual basis. The Carnegie-Ames-Stanford Approach (CASA) model's predicted mean emission flux of methane from wetlands of the continental United States totaled 5.5 Tg CH(4) per year. Ranked in terms of total annual flux, the 10 states with the highest predicted emissions (not considering Alaska) are all located in the Great Lakes region and the southern coastal regions of the country. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Calif State Univ, Seaside, CA USA. Educ Associates, Moffett Field, CA USA. San Jose State Univ, San Jose, CA 95192 USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Mail Stop 242-4, Moffett Field, CA 94035 USA. EM cpotter@mail.arc.nasa.gov NR 40 TC 18 Z9 21 U1 3 U2 16 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1087-3562 J9 EARTH INTERACT JI Earth Interact. PY 2006 VL 10 AR 22 DI 10.1175/EI200.1 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 124OQ UT WOS:000243378500001 ER PT J AU Wang, WL Anderson, BT Entekhabi, D Huang, D Kaufmann, RK Potter, C Myneni, RB AF Wang, Weile Anderson, Bruce T. Entekhabi, Dara Huang, Dong Kaufmann, Robert K. Potter, Christopher Myneni, Ranga B. TI Feedbacks of vegetation on summertime climate variability over the North American Grasslands. Part II: A coupled stochastic model SO EARTH INTERACTIONS LA English DT Article DE land-atmosphere interactions; vegetation feedbacks; soil water balance ID SOIL-MOISTURE; NONLINEAR DYNAMICS; BIOSPHERE MODEL; SURFACE; PRECIPITATION; HYDROLOGY; BALANCE; SYSTEM; SCALES; SAHEL AB A coupled linear model is derived to describe interactions between anomalous precipitation and vegetation over the North American Grasslands. The model is based on biohydrological characteristics in the semiarid environment and has components to describe the water-related vegetation variability, the long-term balance of soil moisture, and the local soil - moisture precipitation feedbacks. Analyses show that the model captures the observed vegetation dynamics and characteristics of precipitation variability during summer over the region of interest. It demonstrates that vegetation has a preferred frequency response to precipitation forcing and has intrinsic oscillatory variability at time scales of about 8 months. When coupled to the atmospheric fields, such vegetation signals tend to enhance the magnitudes of precipitation variability at interannual or longer time scales but damp them at time scales shorter than 4 months; the oscillatory variability of precipitation at the growing season time scale (i.e., the 8-month period) is also enhanced. Similar resonance and oscillation characteristics are identified in the power spectra of observed precipitation datasets. The model results are also verified using Monte Carlo experiments. C1 Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. MIT, Dept Civil & Environm Engn, Ralph M Parsons Lab, Cambridge, MA 02139 USA. NASA, Ames Res Ctr, Ecosyst Sci & Technol Branch, Moffett Field, CA 94035 USA. RP Wang, WL (reprint author), Boston Univ, Dept Geog & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA. EM wlwang@bu.edu RI Huang, Dong/H-7318-2014; Myneni, Ranga/F-5129-2012 OI Huang, Dong/0000-0001-9715-6922; NR 39 TC 1 Z9 1 U1 2 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1087-3562 J9 EARTH INTERACT JI Earth Interact. PY 2006 VL 10 AR 16 PG 30 WC Geosciences, Multidisciplinary SC Geology GA 096XO UT WOS:000241410300001 ER PT J AU Wang, WL Anderson, BT Phillips, N Kaufmann, RK Potter, C Myneni, RB AF Wang, Weile Anderson, Bruce T. Phillips, Nathan Kaufmann, Robert K. Potter, Christopher Myneni, Ranga B. TI Feedbacks of vegetation on summertime climate variability over the North American grasslands. Part I: Statistical analysis SO EARTH INTERACTIONS LA English DT Article DE land-atmosphere interaction; vegetation feedbacks ID LONG-TERM VARIABILITY; SOIL-MOISTURE; DESERT WORLD; GREEN PLANET; PRECIPITATION; ATMOSPHERE; MODEL; WATER; TEMPERATURE; SATELLITE AB Feedbacks of vegetation on summertime climate variability over the North American Grasslands are analyzed using the statistical technique of Granger causality. Results indicate that normalized difference vegetation index (NDVI) anomalies early in the growing season have a statistically measurable effect on precipitation and surface temperature late in summer. In particular, higher means and/or decreasing trends of NDVI anomalies tend to be followed by lower rainfall but higher temperatures during July through September. These results suggest that initially enhanced vegetation may deplete soil moisture faster than normal and thereby induce drier and warmer climate anomalies via the strong soil moisture - precipitation coupling in these regions. Consistent with this soil moisture - precipitation feedback mechanism, interactions between temperature and precipitation anomalies in this region indicate that moister and cooler conditions are also related to increases in precipitation during the preceding months. Because vegetation responds to soil moisture variations, interactions between vegetation and precipitation generate oscillations in NDVI anomalies at growing season time scales, which are identified in the temporal and the spectral characteristics of the precipitation NDVI system. Spectral analysis of the precipitation - NDVI system also indicates that 1) long-term interactions (i.e., interannual and longer time scales) between the two anomalies tend to enhance one another, 2) short-term interactions ( less than 2 months) tend to damp one another, and 3) intermediary-period interactions ( 4 - 8 months) are oscillatory. Together, these results support the hypothesis that vegetation may influence summertime climate variability via the land - atmosphere hydrological cycles over these semiarid grasslands. C1 Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA. NASA, Ames Res Ctr, Ecosyst Sci & Technol Branch, Moffett Field, CA 94035 USA. RP Wang, WL (reprint author), Boston Univ, Dept Geog & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA. EM wlwang@bu.edu RI Myneni, Ranga/F-5129-2012 NR 30 TC 7 Z9 7 U1 0 U2 13 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1087-3562 J9 EARTH INTERACT JI Earth Interact. PY 2006 VL 10 AR 17 PG 27 WC Geosciences, Multidisciplinary SC Geology GA 096XP UT WOS:000241410400001 ER PT S AU Wolfe, RE Esaias, W Lyapustin, A Xiong, X AF Wolfe, R. E. Esaias, W. Lyapustin, A. Xiong, X. BE Butler, JJ Xiong, J TI MODIS solar diffuser Earthshine modeling and analysis - art. no. 629606 SO Earth Observing Systems XI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Earth Observing Systems XI CY AUG 14-16, 2006 CL San Diego, CA DE MODlS; EOS; Earthshine; calibration; solar diffuser ID SYSTEM AB MODIS's solar diffuser is one of the key calibration sources for its reflective bands. Geometric optical modeling shows that Earthshine illuminating the solar diffuser contaminates measurements of the direct solar irradiance. Before launch, a simple model was used that did not consider the non-diffuse component and the atmospheric transfer of the Earthshine contamination. Recently, a more detailed Earthshine model has been recently developed to better determine the magnitude and characteristics of Earthshine contamination. The model includes a geometric optical model of the instrument, a model of the Earth/Sun/instrument geometry during the calibration interval, an atmospheric model, and various bi-directional models of Earth surface types. Several types of vegetation and open-ocean with different wind speeds are modeled. Analysis was performed of the solar diffuser data with particular emphasis on the surface type at the Earth locations where specular reflections (glint) might occur, i.e., where the solar and view zenith angles are almost the same and the relative azimuth angle is near 180 degrees. The new model compares well with detailed analysis of the solar diffuser data, both over open-ocean with glint, and over vegetation. Both the modeling and analysis show a spectral dependence in the non-diffuse radiation that increases with wavelength. The modeling and analysis give lower and upper bounds on the Earthshine contamination and suggest approaches for minimizing its impact on the MODIS calibration. C1 NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. RP Wolfe, RE (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. RI Wolfe, Robert/E-1485-2012; Xiong, Xiaoxiong (Jack)/J-9869-2012; Lyapustin, Alexei/H-9924-2014 OI Wolfe, Robert/0000-0002-0915-1855; Lyapustin, Alexei/0000-0003-1105-5739 NR 11 TC 2 Z9 2 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 0-8194-6375-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6296 BP 29606 EP 29606 AR 629606 DI 10.1117/12.681100 PG 8 WC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BFI34 UT WOS:000241988000005 ER PT S AU Xiong, X Che, N Pan, C Xie, X Sun, J Barnes, WL Guenther, B AF Xiong, X. Che, N. Pan, C. Xie, X. Sun, J. Barnes, W. L. Guenther, B. BE Butler, JJ Xiong, J TI Results and lessons from MODIS reflective solar bands calibration: Pre-launch to on-orbit - art. no. 629607 SO Earth Observing Systems XI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Earth Observing Systems XI CY AUG 14-16, 2006 CL San Diego, CA DE Terra; Aqua; MODIS; reflective solar bands; solar diffuser; calibration ID IMAGING SPECTRORADIOMETER MODIS; ALGORITHM; EOS-AM1 AB MODIS is a major instrument for NASA's EOS missions, currently operating aboard the EOS Terra and Aqua spacecraft launched in December 1999 and May 2002, respectively. It was designed to extend heritage sensor measurements and data records and to enable new research studies of the Earth's land, oceans, and atmosphere. MODIS has 36 spectral bands (0.41 - 14.4 mu m) located on four focal plane assemblies (FPA). It makes measurements at three nadir spatial resolutions: 0.25km, 0.5km, and 1km. Because of instrument design complexity and more stringent calibration requirements, extensive calibration and characterization activities were conducted pre-launch by the sensor vendor for both Terra and Aqua MODIS. For the 20 reflective solar bands (RSB) with wavelengths below 2.2 mu m, these activities include detector noise characterization, radiometric response at different instrument temperatures and at different scan angles, and relative spectral response. On-orbit RSB calibration is performed using a solar diffuser (SD) and a solar diffuser stability monitor (SDSM). In addition, regular lunar observations are made to track RSB radiometric stability. This paper provides a summary of Terra and Aqua MODIS RSB pre-launch and on-orbit calibration and characterization activities, methodologies, data analysis results, and lessons learned. It focuses on major issues that could impact MODIS RSB calibration and data product quality. Results presented in this paper include RSB detector noise characterization, response versus scan angle and instrument temperature, SD bi-directional reflectance factors characterization, and on-orbit calibration stability. Similar discussions on MODIS thermal emissive bands (TEB) are presented in a separate paper in these proceedings (Xiong et. al). C1 NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. RP Xiong, X (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 15 TC 4 Z9 4 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6375-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6296 BP 29607 EP 29607 AR 629607 DI 10.1117/12.679144 PG 11 WC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BFI34 UT WOS:000241988000006 ER PT S AU Meister, G Kwiatkowska, EJ McClain, CR AF Meister, Gerhard Kwiatkowska, Ewa J. McClain, Charles R. BE Butler, JJ Xiong, J TI Analysis of image striping due to polarization correction artifacts in remotely sensed ocean scenes - art. no. 629609 SO Earth Observing Systems XI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Earth Observing Systems XI CY AUG 14-16, 2006 CL San Diego, CA DE remote sensing; scanners; on-orbit calibration; polarization ID MODIS AB The characterization of the polarization sensitivity of a remote sensing sensor can have a large impact on the data quality of the top-of-atmosphere radiances measured by optical sensors on earth-orbiting satellites. This paper describes an algorithm to improve the polarization characterization of certain elements of an imaging sensor (e.g. detectors, or mirror sides) relative to each other, as well as the application to an ocean color sensor. The key step in the analysis is the separation of the measured radiances into two groups: those that are increased by the polarization correction, and those that are decreased. C1 NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Futuretech Corp, Greenbelt, MD 20771 USA. RP Meister, G (reprint author), NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Futuretech Corp, Code 614-2, Greenbelt, MD 20771 USA. RI Meister, Gerhard/F-7159-2012 NR 12 TC 4 Z9 4 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 0-8194-6375-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6296 BP 29609 EP 29609 AR 629609 DI 10.1117/12.679309 PG 12 WC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BFI34 UT WOS:000241988000008 ER PT S AU Pagano, TS Aumann, HH Chahine, MT O'Callaghan, FG AF Pagano, Thomas S. Aumann, Hartmut H. Chahine, Moustafa T. O'Callaghan, Fred G. BE Butler, JJ Xiong, J TI Instrument requirements for a next generation 1km resolution hyperspectral imaging spectrometer - art. no. 629617 SO Earth Observing Systems XI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Earth Observing Systems XI CY AUG 14-16, 2006 CL San Diego, CA DE AIRS; MODIS; ARIES; Imaging Spectrometer; remote sensing AB The combined performance of the Atmospheric Infrared Sounder (AIRS) and the Moderate Resolution Imaging Spectroradiometer (MODIS) on the Earth Observing System (EOS) Aqua spacecraft is possible in a single instrument with today's technology. Combining the capability allows better accuracy and resolution of products produced by both instruments. This paper describes the top level requirements expected from such an instrument, the types of products anticipated, and discusses technology readiness. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pagano, TS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 6 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 0-8194-6375-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6296 BP 29617 EP 29617 AR 629617 DI 10.1117/12.682271 PG 6 WC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BFI34 UT WOS:000241988000038 ER PT S AU Xiong, X Chiang, K Chen, N Xiong, S Barnes, WL Guenther, B AF Xiong, X. Chiang, K. Chen, N. Xiong, S. Barnes, W. L. Guenther, B. BE Butler, JJ Xiong, J TI Results and lessons from MODIS thermal emissive bands calibration: Pre-launch to on-orbit - art. no. 62960A SO Earth Observing Systems XI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Earth Observing Systems XI CY AUG 14-16, 2006 CL San Diego, CA DE Terra; Aqua; MODIS; thermal emissive bands; blackbody; calibration; noise characterization ID IMAGING SPECTRORADIOMETER MODIS; EOS-AM1 AB The Moderate Resolution Imaging Spectroradiometer (MODIS) is a major instrument for NASA's Earth Observing System (EOS), currently operating on-board the EOS Terra spacecraft, launched in December 1999, and Aqua spacecraft, launched in May 2002. MODIS is a whiskbroom scanning radiometer using a double-sided paddle wheel scan mirror. It makes measurements in 36 spectral bands with wavelengths from visible (VIS) to long-wave infrared (LWIR). Bands 20-25 and 27-36 are the thermal emissive bands (TEB) covering wavelengths from 3.5 to 14.4 mu m. During pre-launch thermal vacuum measurements, a laboratory blackbody calibration source (BCS) was used as the primary calibration source for the TEB. For on-orbit operation, an on-board blackbody (BB) source and a space view (SV) port are used together for the TEB calibration on a scan-by-scan basis. This paper provides an overview of Terra and Aqua MODIS pre-launch and on-orbit calibration and characterization activities, methodologies, data analysis results, and lessons learned for the thermal emissive bands. It focuses on major issues that could impact MODIS TEB calibration and data quality. Results presented in this paper include detector noise characterization, response versus scan angle (RVS), and response versus instrument and focal plane temperatures. Similar discussions for the MODIS reflective solar bands (RSB) are presented in a separate paper in these proceedings (Xiong et. al). C1 NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. RP Xiong, X (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 13 TC 8 Z9 8 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 0-8194-6375-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6296 BP A2960 EP A2960 AR 62960A DI 10.1117/12.680992 PG 12 WC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BFI34 UT WOS:000241988000009 ER PT S AU Xiong, X Wu, A Sun, J Wenny, B AF Xiong, X. Wu, A. Sun, J. Wenny, B. BE Butler, JJ Xiong, J TI An overview of inter-comparison methodologies for Terra and Aqua MODIS calibration - art. no. 62960C SO Earth Observing Systems XI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Earth Observing Systems XI CY AUG 14-16, 2006 CL San Diego, CA DE Terra; Aqua; MODIS; sensor; calibration; inter-comparison; Moon; AVHRR ID IMAGING SPECTRORADIOMETER MODIS; EOS-AM1 AB With increasing efforts on data-fusion and long-term climate data records (CDR) using observations made by multiple sensors on the same or different platforms, sensor cross-calibration has become increasingly important. It is known that the uncertainty of climate models or science data records depends not only on the calibration quality of individual sensors but also on their calibration consistency. This paper provides an overview of inter-comparison methodologies applied by the MODIS Characterization Support Team (MCST) at NASA/GSFC for the studies of Terra and Aqua MODIS on-orbit calibration consistency. Improved over heritage sensors, MODIS was built with a set of on-board calibrators (OBC) that include a blackbody (BB), a space view (SV) port, a solar diffuser (SD), and a solar diffuser stability monitor (SDSM). The BB is primarily used for the thermal emissive bands (TEB) calibration and the SD/SDSM system for the reflective solar bands (RSB) calibration. Detector responses to the SV provide measurements for the instrument background. Although instrument design requirements and calibration approaches are nearly identical for both Terra and Aqua MODIS and they all went through extensive and similar pre-launch calibration and characterization activities, their on-orbit calibration consistency still has to be carefully examined and validated as many science products are generated from observations made by both instruments. Methodologies discussed in this paper include intercomparison studies using the Moon, a third sensor, and ground targets. Our results show that Terra and Aqua reflective solar bands and thermal emissive bands have been calibrated consistently to within their combined uncertainty requirements. For the 11 mu m and 12 mu m bands used for surface temperature measurements, the calibration differences between Terra and Aqua MODIS are less than +/- 0.15K at scene temperatures from 240-280K and less than +/- 0.50K at cold scene temperatures from 190 to 230K (before corrections). For most reflective solar bands, their reflectance calibration differences are typically less than +/- 2%. C1 NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. RP Xiong, X (reprint author), NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 18 TC 6 Z9 6 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 0-8194-6375-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6296 BP C2960 EP C2960 AR 62960C DI 10.1117/12.679162 PG 11 WC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BFI34 UT WOS:000241988000011 ER PT S AU Barsi, JA Hook, SJ Palluconi, FD Schott, JR Raqueno, NG AF Barsi, Julia A. Hook, Simon J. Palluconi, Frank D. Schott, John R. Raqueno, Nina G. BE Butler, JJ Xiong, J TI Landsat TM and ETM plus thermal band calibration - art. no. 62960F SO Earth Observing Systems XI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Earth Observing Systems XI CY AUG 14-16, 2006 CL San Diego, CA DE Landsat; Enhanced Thematic Mapper Plus (ETM plus ); Thematic Mapper (TM); calibration; thermal band AB Landsat-5 Thematic Mapper (TM) has been imaging the Earth since March 1984 and Landsat-7 Enhanced Thematic Mapper Plus (ETM+) was added to the series of Landsat instruments in April 1999. The stability and calibration of the ETM+ has been monitored extensively since launch. Though not monitored for many years, TM now has a similar system in place to monitor stability and calibration. University teams have been evaluating the on-board calibration of the instruments through ground-based measurements since 1999. This paper considers the calibration efforts for the thermal band, Band 6, of both the Landsat-5 and Landsat-7 instruments. Initial calibration results for the Landsat-7 ETM+ thermal band found a bias error which was corrected through changes in the processing systems in late 2000. Recent results are suggesting a calibration error in gain, apparent with high Ltemperature targets. For typical earth temperature targets, from about 5-20C, the gain error is small enough to be within the noise of the vicarious calibration process. However, for very high temperature targets (greater then 35C), Landsat-7 appears to be predicting several degrees too low. Questions remain on whether the change happened suddenly or is varying slowly, so the team will wait for another collection season before making any updates to the calibration. The calibration efforts for Landsat-5 TM considers only data collected since 1999, though there are efforts underway to extend the calibration history prior to the Landsat-7 launch. The latest data suggests that the Landsat-5 thermal band has a bias error of about 0.65K too low since 1999. Studies early in the life of Landsat-5 show that the instrument was calibrated within the error of the calibration process. It is impossible to tell, at this point, when or how the change in bias may have occurred. A correction will be calculated and implemented in the US processing system in 2006 for data acquired since April 1999. C1 NASA, GSFC, Space Sci & Applicat Inc, Greenbelt, MD 20781 USA. RP Barsi, JA (reprint author), NASA, GSFC, Space Sci & Applicat Inc, Code 614-4, Greenbelt, MD 20781 USA. NR 9 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6375-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6296 BP F2960 EP F2960 AR 62960F DI 10.1117/12.683212 PG 9 WC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BFI34 UT WOS:000241988000014 ER PT S AU Georgieva, E Wilson, E Heaps, WS AF Georgieva, E. Wilson, E. Heaps, W. S. BE Butler, JJ Xiong, J TI Precise measurement of CO2 from space using Fabry-Perot based optical setup - current status and development - art. no. 62961G SO Earth Observing Systems XI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Earth Observing Systems XI CY AUG 14-16, 2006 CL San Diego, CA DE instrumentation; measurement and metrology (120.0120); remote sensing (280.0280); atmospheric composition (010.1280); optical instruments (120.4640); absorption (300.1030); interferometry (120.3180); Fabry-Perot (120.2230); Planetology : Solar System Objects (6225): Earth; Mars; Martian atmosphere ID SUN GLINT; ATMOSPHERE; ABSORPTION; EVOLUTION; METHANE; MARS AB The FPICC (Fabry-Perot Interferometer for Column CO2) is a new instrument developed under the Instrument Incubator Program that uses a novel technique for measuring the absorption Of CO2 sunlight reflected from the Earth. The optical setup consists of three channels. The first channel is built to measure carbon dioxide by using a solid Fabry-Perot etalon to restrict the measurement to light in CO2 absorption bands. The second and third channels focus on the O-2 A band (759-771 nm) composed of about 300 absorption lines, which vary in strength and width according to pressure and temperature. We performed measurements using solid Fabry-Perot etalons with different FSR and different pre-filters. We demonstrated the instrument's significant capability to detect CO2 and O-2 in laboratory, as well as in ground based and airborne experiments. The initial tests indicate that when the instrument is used with a sun tracker the sensitivity for CO2 detection is 2.1 ppm in one second average, and the sensitivity to the oxygen column pressure changes is as low as 0.88 mbar. The reduced sensitivity for the airborne experiments arises because the atmospheric scattering processes make the path length more variable and uncertain. One solution to this problem is to use the glint reflection from water surfaces. For this purpose we design and perform a theoretical study to build a different version of the FPICC instrument to be used on a satellite orbiting the Earth and working in a glint mode. This Fabry-Perot based technique is applicable to other species as well. For example one could use the FPICC instrument for fractionations measurements of the stable carbon isotope (C-13/C-12). The instrument can be used to study the atmosphere of Mars, which consists primarily Of CO2. A theoretical study and design of a version of the instrument for Mars for CO2 and CH4 measurements will be presented. We report results on the recent calibration of the instrument, recent data from ground tests at Goddard, design versions, and theoretical models for the Earth and Mars instruments. C1 Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Georgieva, E (reprint author), Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RI Wilson, Emily/C-9158-2012 OI Wilson, Emily/0000-0001-5634-3713 NR 22 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 0-8194-6375-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6296 BP G2961 EP G2961 AR 62961G DI 10.1117/679653 PG 12 WC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BFI34 UT WOS:000241988000044 ER PT S AU Broberg, SE Aumann, HH Gregorich, DT Xiong, X AF Broberg, Steven E. Aumann, Hartmut H. Gregorich, David T. Xiong, X. BE Butler, JJ Xiong, J TI Evaluation of AIRS, MODIS, and HIRS 11 micron brightness temperature difference changes from 2002 through 2006 SO EARTH OBSERVING SYSTEMS XI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Earth Observing Systems XI CY AUG 14-16, 2006 CL San Diego, CA DE AIRS; MODIS; HIRS; spectrometer; radiometer; validation AB In an effort to validate the accuracy and stability of AIRS data at low scene temperatures (200-250 K range), we evaluated brightness temperatures at 11 microns with Aqua MODIS band 31 and HIRS/3 channel 8 for Antarctic granules between September 2002 and May 2006. We found excellent agreement with MODIS (at the 0.2 K level) over the full temperature range in data from early in the Aqua mission. However, in more recent data, starting in April 2005, we found a scene temperature dependence in MODIS-AIRS brightness temperature differences, with a discrepancy of 1-1.5 K at 200 K. The comparison between AIRS and HIRS/3 (channel 8) on NOAA 16 for the same time period yields excellent agreement. The cause and time dependence of the disagreement with MODIS is under evaluation, but the change was coincident with a change in the MODIS production software from collection 4 to 5. AIRS and MODIS (Flight Model 1) are onboard the EOS Aqua spacecraft, launched into a 1:30 PM polar orbit on May 4, 2002. AIRS has 2378 infrared channels with high spectral resolution (1200) covering the 3.7 to 15.4 micron wavelength range, with a nominal spatial resolution of 13.5 km. MODIS has 36 relatively broad spectral bands with spatial resolution of 1 krn for the LWIR bands. HIRS/3 is onboard NOAA-16 (L), launched into a 2:00 PM polar orbit on Sep. 21, 2000. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Broberg, SE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sbroberg@jpl.nasa.gov RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 5 TC 1 Z9 1 U1 0 U2 5 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6375-2 J9 PROC SPIE PY 2006 VL 6296 AR 62960J DI 10.1117/12.681049 PG 7 WC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BFI34 UT WOS:000241988000018 ER PT S AU Elliott, DA Pagano, TS Aumann, HH AF Elliott, Denis A. Pagano, Thomas S. Aumann, H. H. BE Butler, JJ Xiong, J TI The impact of the AIRS spatial response on channel-to-channel and multi-instrument data analyses SO EARTH OBSERVING SYSTEMS XI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Earth Observing Systems XI CY AUG 14-16, 2006 CL San Diego, CA AB The Atmospheric Infrared Sounder (AIRS) measures the infrared spectrum in 2378 channels between 3.7 and 15.4 microns with a very high spectral resolution of approximately 1200. AIRS footprints are approximately 1.1 by 0.6 degrees. Because AIRS is a grating spectrometer, each channel has a unique spatial response. Image rotation due to the scan mirror causes these spatial responses to rotate. In effect, each channel has 90 spatial responses, one for each scene footprint in the scan line. Although the spatial response for most channels is symmetric and nearly uniform, some channels have significantly asymmetric response. This paper reviews and describes the prelaunch measurements that characterized the spatial response functions. Next, it describes the conversion of the ground-based results into footprint-specific response functions valid in flight. Then we describe the postlaunch validation of the measurements, including centroid location, axes orientations, and a check on the full two-dimensional response functions. This latter check involves comparison of AIRS data with that of the Moderate Resolution Imaging Spectrometer (MODIS), which flies on the same platform as AIRS. An important result is that AIRS/MODIS brightness temperature comparisons are significantly improved (scatter reduced) when the AIRS spatial response is explicitly taken into account. Finally, a status report is given on attempts to fully verify the prelaunch measurements by deriving the AIRS spatial response from flight data alone. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Elliott, DA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 6 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6375-2 J9 PROC SPIE PY 2006 VL 6296 AR 62960I DI 10.1117/12.679542 PG 9 WC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology SC Instruments & Instrumentation; Remote Sensing; Imaging Science & Photographic Technology GA BFI34 UT WOS:000241988000017 ER PT J AU Fujita, M Ishikawa, T Mochizuki, M Sato, M Toyama, S Katayama, M Kawai, K Matsumoto, Y Yabuki, T Asada, A Colombo, OL AF Fujita, M Ishikawa, T Mochizuki, M Sato, M Toyama, S Katayama, M Kawai, K Matsumoto, Y Yabuki, T Asada, A Colombo, OL TI GPS/acoustic seafloor geodetic observation: method of data analysis and its application SO EARTH PLANETS AND SPACE LA English DT Article DE GPS/acoustic; seafloor geodetic observation; linear inversion; Off Miyagi; intraplate deformation ID DEFORMATION MEASUREMENTS; POSITIONING SYSTEM; GPS; PRECISE; JAPAN; SOUND AB We have been developing a system for detecting seafloor crustal movement by combining kinematic GPS and acoustic ranging techniques. A linear inversion method is adopted to determine the position of seafloor stations from coordinates of a moving survey vessel and measured travel times of acoustic waves in seawater. The positioning accuracy is substantially improved by estimating the temporal variation of the acoustic velocity structure. We apply our method to the ranging data acquired at the seafloor reference point, MYGI, located off Miyagi Prefecture, in northeast Japan, where a huge earthquake is expected to occur in the near future. A time series of horizontal coordinates of MYGI obtained from seven campaign observations for the period 2002-2005 exhibits a linear trend with a scattering rms of about 2 cm. A linear fit to the time series gives an intraplate crustal velocity of more than several centimeters per year towards the WNW, which implies strong interplate Coupling around this region. The precision of each campaign solution was examined at MYGI and other seafloor reference points along the Nankai Trough through comparison of independent one-day subset solutions within the campaign. The resultant repeatability looks to be well-correlated with the temporal and spatial stability of the acoustic velocity structure in the seawater depending oil the region as well as the season. C1 Japan Coast Guard, Hydrog & Oceanog Dept, Chuo Ku, Tokyo 1040045, Japan. Univ Tokyo, Inst Ind Sci, Minato Ku, Tokyo 1538505, Japan. NASA, Goddard Space Flight Ctr, GEST, Greenbelt, MD 20771 USA. RP Fujita, M (reprint author), Japan Coast Guard, Hydrog & Oceanog Dept, Chuo Ku, 5-3-1 Tsukiji, Tokyo 1040045, Japan. EM masayuki-fujita@kaiho.mlit.go.jp NR 40 TC 49 Z9 49 U1 1 U2 6 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2006 VL 58 IS 3 BP 265 EP 275 PG 11 WC Geosciences, Multidisciplinary SC Geology GA 025TP UT WOS:000236290100001 ER PT J AU Olsen, N Haagmans, R Sabaka, TJ Kuvshinov, A Maus, S Purucker, ME Rother, M Lesur, V Mandea, M AF Olsen, N Haagmans, R Sabaka, TJ Kuvshinov, A Maus, S Purucker, ME Rother, M Lesur, V Mandea, M TI The Swarm End-to-End mission simulator study: A demonstration of separating the various contributions to Earth's magnetic field using synthetic data SO EARTH PLANETS AND SPACE LA English DT Article DE Earth's magnetic field; comprehensive inversion; electromagnetic induction; ionosphere; lithosphere; magnetosphere ID ANOMALIES; OCEAN; MODEL AB Swarm, a satellite constellation to measure Earth's magnetic field with unpreceded accuracy, has been selected by ESA for launch in 2009. The mission will provide the best ever survey of the geomagnetic field and its temporal evolution, in order to gain new insights into the Earth system by improving our understanding of the Earth's interior and climate. An End-to-End mission performance simulation was carried out during Phase A of the mission, with the aim of analyzing the key system requirements, particularly with respect to the number of Swarm satellites and their orbits related to the science objectives of Swarm. In order to be able to use realistic parameters of the Earth's environment, the mission simulation starts at January 1, 1997 and lasts until re-entry of the lower satellites five years later. Synthetic magnetic field values were generated for all relevant contributions to Earth's magnetic field: core and lithospheric fields, fields due to currents in the ionosphere and magnetosphere, due to their secondary, induced, currents in the oceans, lithosphere and mantle, and fields due to currents coupling the ionosphere and magnetosphere. Several independent methods were applied to the synthetic data to analyze various aspects of field recovery in relation to different number of satellites, different constellations and realistic noise sources. This paper gives an overview of the study activities, describes the generation of the synthetic data, and assesses the obtained results. C1 Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark. ESA, ESTEC, Directorate Earth Observ Programmes, NL-2200 AG Noordwijk ZH, Netherlands. NASA, Goddard Space Flight Ctr, Geodynam Branch, Greenbelt, MD 20771 USA. NOAA, Natl Geophys Data Ctr, Boulder, CO 80305 USA. Geoforschungszentrum Potsdam, D-14473 Potsdam, Germany. British Geol Survey, Edinburgh EH9 3LA, Midlothian, Scotland. Inst Phys Globe, F-75252 Paris, France. RP Olsen, N (reprint author), Danish Natl Space Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. EM nio@spacecenter.dk RI Olsen, Nils/H-1822-2011; Sabaka, Terence/D-5618-2012; MANDEA, Mioara/E-4892-2012; Lesur, Vincent/H-1031-2012 OI Olsen, Nils/0000-0003-1132-6113; Lesur, Vincent/0000-0003-2568-320X NR 30 TC 36 Z9 37 U1 2 U2 9 PU TERRA SCIENTIFIC PUBL CO PI TOKYO PA 2003 SANSEI JIYUGAOKA HAIMU, 5-27-19 OKUSAWA, SETAGAYA-KU, TOKYO, 158-0083, JAPAN SN 1343-8832 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2006 VL 58 IS 4 BP 359 EP 370 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 037ZB UT WOS:000237185700003 ER PT J AU Sabaka, TJ Olsen, N AF Sabaka, TJ Olsen, N TI Enhancing comprehensive inversions using the Swarm constellation SO EARTH PLANETS AND SPACE LA English DT Article DE Earth's magnetic field; comprehensive modelling; electromagnetic induction; ionosphere; lithosphere; magnetosphere ID MAGNETIC ANOMALY MAPS; MAGSAT DATA; GLOBAL VECTOR; EARTH; FIELD; LITHOSPHERE; MODELS AB This paper reports on the findings of a simulation study designed to test various satellite configurations suggested for the upcoming Swarm magnetic mapping mission. The test is to see whether the mission objectives of recovering small-scale core secular variation (SV) and lithospheric magnetic signals, as well as information about mantle conductivity structure, can be met. The recovery method used in this paper is known as comprehensive inversion (CI) and involves the parameterization of all major fields followed by a co-estimation of these parameters in a least-squares sense in order to achieve proper signal separation. ne advantage of co-estimation over serial estimation of parameters is demonstrated by example. Synthetic data were calculated for a pool of six Swarm satellites from a model based heavily on the CM4 comprehensive model, but which has more small-scale lithospheric structure, a more complicated magnetospheric field, and an induced field reflecting a 3-D conductivity model. These data also included realistic magnetic noise from spacecraft and payload. Though the parameterization for the CI is based upon that of CM4, modifications have been made to accommodate these new magnetospheric and induced fields, in particular with orthogonality constraints defined so as to avoid covariance between slowly varying induced fields and SV. The use of these constraints is made feasible through an efficient numerical implementation. Constellations of 4, 3, 2, and 1 satellites were considered; that with 3 was able to meet the mission objectives, consistently resolving the SV to about spherical harmonic (SH) degree n = 15 and the lithosphere to a limited n < 90 due to external field leakage, while those with 2 and 1 were not; 4 was an improvement over 3, but was much less than the improvement from 2 to 3. The resolution of the magnetospheric and induced SH time-series from the 3 satellite configuration was sufficient enough to allow the detection of 3-D mantle conductivity structure in a companion study. C1 NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Raytheon, Greenbelt, MD 20771 USA. Danish Natl Space Ctr, DK-2100 Copenhagen O, Denmark. RP Sabaka, TJ (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Raytheon, Greenbelt, MD 20771 USA. EM sabaka@geomag.gsfc.nasa.gov RI Olsen, Nils/H-1822-2011; Sabaka, Terence/D-5618-2012 OI Olsen, Nils/0000-0003-1132-6113; NR 29 TC 25 Z9 28 U1 0 U2 3 PU TERRA SCIENTIFIC PUBL CO PI TOKYO PA 2003 SANSEI JIYUGAOKA HAIMU, 5-27-19 OKUSAWA, SETAGAYA-KU, TOKYO, 158-0083, JAPAN SN 1343-8832 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2006 VL 58 IS 4 BP 371 EP 395 PG 25 WC Geosciences, Multidisciplinary SC Geology GA 037ZB UT WOS:000237185700004 ER PT J AU Maus, S Luhr, H Purucker, M AF Maus, S Luhr, H Purucker, M TI Simulation of the high-degree lithospheric field recovery for the Swarm constellation of satellites SO EARTH PLANETS AND SPACE LA English DT Article DE geomagnetic field; magnetic field modeling; crustal magnetic field ID MAGNETIC ANOMALY MAPS; GLOBAL VECTOR; MAGSAT DATA AB A primary objective of the Swarm constellation mission is to resolve the lithospheric magnetic field with the best achievable accuracy in order to bridge the spectral gap between satellite and airborne/marine magnetic surveys. In a series of end-to-end simulations, the possibilities of high degree field recovery were investigated. The proposed constellation consists of a higher and a lower pair of satellites. It was soon found that a constellation as such does not yet guarantee improved high degree field recovery. Of crucial importance is the orbit constellation of the lower pair of satellites. If the lower satellites follow each other, as investigated in Constellation 1, the gain of a constellation turns out to be marginal, compared to a single satellite. For Constellation 2, the lower satellites were separated in the E/W direction. In this setup, one can use the instantaneous E/W magnetic field gradient between the satellites, as well as the N/S along track gradients. Incorporating this vector gradient information results in significantly improved field resolution. Indeed, the final simulation suggests that the envisaged Swarm constellation will enable the recovery of the lithospheric field to beyond spherical harmonic degree 130. C1 NASA, Goddard Space Flight Ctr, Geodynam Branch, Raytheon ITSS, Greenbelt, MD 20771 USA. Geoforschungszentrum Potsdam, D-14473 Potsdam, Germany. RP Maus, S (reprint author), Univ Colorado, CIRES, Boulder, CO 80309 USA. EM Stefan.Maus@noaa.gov NR 12 TC 10 Z9 14 U1 0 U2 2 PU TERRA SCIENTIFIC PUBL CO PI TOKYO PA 2003 SANSEI JIYUGAOKA HAIMU, 5-27-19 OKUSAWA, SETAGAYA-KU, TOKYO, 158-0083, JAPAN SN 1343-8832 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2006 VL 58 IS 4 BP 397 EP 407 PG 11 WC Geosciences, Multidisciplinary SC Geology GA 037ZB UT WOS:000237185700005 ER PT J AU Kuvshinov, A Sabaka, T Olsen, N AF Kuvshinov, A Sabaka, T Olsen, N TI 3-D electromagnetic induction studies using the Swarm constellation: Mapping conductivity anomalies in the Earth's mantle SO EARTH PLANETS AND SPACE LA English DT Article DE satellite magnetic observations; 3-D electromagnetic induction; C-responses; mantle conductivity anomalies ID ELECTRICAL-CONDUCTIVITY; MAGNETIC-FIELD; SATELLITE ALTITUDE; PACIFIC-OCEAN; C-RESPONSES; MID-MANTLE; BENEATH; VELOCITY; SHEAR; TEMPERATURE AB An approach is presented to detect deep-seated regional conductivity anomalies by analysis of magnetic observations taken by low-Earth-orbiting satellites. The approach deals with recovery of C-responses on a regular grid and starts with a determination of time series of external and internal coefficients of the magnetic potential. From the coefficients, time series of the magnetic vertical component and of the horizontal divergence of the horizontal components are synthesized oil the grid and the C-responses are determined by means of signal processing of the corresponding time series. For validation of the approach, 3 years of realistic synthetic data at Simulated orbits of the forthcoming Swarm constellation of 3 satellites have been used. To obtain the synthetic data for a given 3-D conductivity Earth's model a time-domain scheme has been applied which relies oil a Fourier transformation of the inducing field, and oil a frequency domain forward modelling. The conductivity model consists of a thin Surface layer of realistic conductance and a 3-D mantle that incorporates a hypothetic deep regional anomaly beneath the Pacific Ocean plate. To establish the ability of the approach to capture the geometry of the mantle heterogeneities used in the forward approach. numerical experiments have been undertaken using various satellite combinations, sampling periods of the resulting time series, and numbers of internal coefficients. The possibility of the approach to map anomalies in the mantle using satellite data that contain contributions from the core and lithosphere, from the rnagnetosphere and ionosphere (and their Earth-induced counterparts), as well as payload noise has been investigated. The model Studies have shown that C-responses obtained oil a regular grid might be used to map regional deep-seated conductivity anomalies. Moreover, it has been demonstrated that these C-responses are successfully recovered from magnetic data collected by the proposed Swarm constellation of 3 satellites. C1 Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark. NASA, Goddard Space Flight Ctr, Geodynam Branch, Greenbelt, MD 20771 USA. RP Kuvshinov, A (reprint author), Danish Natl Space Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. EM alexei@spacecenter.dk RI Olsen, Nils/H-1822-2011; Sabaka, Terence/D-5618-2012 OI Olsen, Nils/0000-0003-1132-6113; NR 45 TC 27 Z9 27 U1 0 U2 7 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2006 VL 58 IS 4 BP 417 EP 427 PG 11 WC Geosciences, Multidisciplinary SC Geology GA 037ZB UT WOS:000237185700007 ER PT J AU Moretto, T Vennerstrom, S Olsen, N Rastatter, L Raeder, J AF Moretto, T Vennerstrom, S Olsen, N Rastatter, L Raeder, J TI Using global magnetospheric models for simulation and interpretation of Swarm external field measurements SO EARTH PLANETS AND SPACE LA English DT Article DE ionospheric currents; field-aligned currents; global magnetospheric simulation; low-altitude satellites ID MAGNETIC-FIELDS; ELECTRIC-FIELDS; QUIET-TIME; IONOSPHERE; CURRENTS; CONDUCTANCES; FLUX; IMF AB We have used a global model of the solar wind magnetosphere interaction to model the high latitude part of the external contributions to the geomagnetic field near the Earth. The model also provides corresponding values for the electric field. Geomagnetic quiet conditions were modeled to provide simulated external contributions relevant for internal field modeling. These have proven very valuable for the design and planning of the up-coming multi-satellite Swarm mission. In addition, a real event simulation was carried out for a moderately active time interval when observations from the Orsted and CHAMP sattelites were available. Comparisons between the simulation results and the satellite observations for this event demonstrate the current level of validity of the global model. We find that the model reproduces quite well the region 1 current system and nightside region 2 currents whereas it consistently underestimates the dayside region 2 currents and overestimates the horizontal ionospheric closure currents in the dayside polar cap. Furthermore, with this example we illustrate the great benefit of utilizing the global model for the interpretation of Swarm external field observations and, likewise, the potential of using Swarm measurements to test and improve the global model. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Danish Natl Space Ctr, Copenhagen, Denmark. Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. RP Moretto, T (reprint author), Natl Sci Fdn, Div Atmospher Sci, 4201 Wilson Blvd, Arlington, VA 22230 USA. EM tjorgens@nsf.gov RI Olsen, Nils/H-1822-2011; Rastaetter, Lutz/D-4715-2012; Moretto, Therese/B-6846-2013 OI Olsen, Nils/0000-0003-1132-6113; Rastaetter, Lutz/0000-0002-7343-4147; Moretto, Therese/0000-0002-2403-5561 NR 32 TC 7 Z9 10 U1 0 U2 2 PU TERRA SCIENTIFIC PUBL CO PI TOKYO PA 2003 SANSEI JIYUGAOKA HAIMU, 5-27-19 OKUSAWA, SETAGAYA-KU, TOKYO, 158-0083, JAPAN SN 1343-8832 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2006 VL 58 IS 4 BP 439 EP 449 PG 11 WC Geosciences, Multidisciplinary SC Geology GA 037ZB UT WOS:000237185700009 ER PT J AU Vennerstrom, S Moretto, T Rastatter, L Raeder, J AF Vennerstrom, S Moretto, T Rastatter, L Raeder, J TI Modeling and analysis of solar wind generated contributions to the near-Earth magnetic field SO EARTH PLANETS AND SPACE LA English DT Article DE Earth's magnetic field; MHD modeling; solar wind; ionosphere; magnetosphere; quiet conditions ID CONDUCTIVITY; CURRENTS AB Solar wind generated magnetic disturbances are currently one of the major obstacles for improving the accuracy in the determination of the magnetic field due to sources internal to the Earth. In the present study a global MHD model of solar wind magnetosphere interaction is used to obtain a physically consistent, divergence-free model of ionospheric, field-aligned and magnetospheric currents in a realistic magnetospheric geometry. The magnetic field near the Earth due to these currents is analyzed by estimating and comparing the contributions from the various parts of the system, with the aim of identifying the most important aspects of the solar wind disturbances in an internal field modeling context. The contribution from the distant magnetospheric currents is found to consist of two, mainly opposing, contributions from respectively the dayside magnetopause currents and the cross-tail current. At high latitudes the field-aligned component is of partidular interest in connection with internal field-modelling. In the attitude regime of 400-800 km (typical for low Earth orbit satellites) the ionospheric currents are found to contribute significantly to the disturbancance, and account for more than 90% of the field-aligned disturbance. The magnetic disturbance field from field-aligned currents (FACs) is basically transverse to the main field, and they therefore contribute with less than 2% to the disturbance in total field intensity. Inhomogeneity in ionospheric conductance is identified as the main cause of main-field disturbance in the field-aligned direction. These disturbances are associated with the ionospheric Pedersen currents, and may introduce systematic errors in internal field models. C1 Danish Natl Space Ctr, DK-2100 Copenhagen, Denmark. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RP Vennerstrom, S (reprint author), Danish Natl Space Ctr, Juliane Marie Vej 30, DK-2100 Copenhagen, Denmark. EM sv@spacecenter.dk RI Rastaetter, Lutz/D-4715-2012; Moretto, Therese/B-6846-2013 OI Rastaetter, Lutz/0000-0002-7343-4147; Moretto, Therese/0000-0002-2403-5561 NR 14 TC 8 Z9 8 U1 0 U2 1 PU TERRA SCIENTIFIC PUBL CO PI TOKYO PA 2003 SANSEI JIYUGAOKA HAIMU, 5-27-19 OKUSAWA, SETAGAYA-KU, TOKYO, 158-0083, JAPAN SN 1343-8832 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2006 VL 58 IS 4 BP 451 EP 461 PG 11 WC Geosciences, Multidisciplinary SC Geology GA 037ZB UT WOS:000237185700010 ER PT J AU Papitashvili, VO Petrov, VG Saxena, AB Clauer, CR Papitashvili, NE AF Papitashvili, VO Petrov, VG Saxena, AB Clauer, CR Papitashvili, NE TI A Virtual Global Magnetic Observatory network: VGMO.NET SO EARTH PLANETS AND SPACE LA English DT Article; Proceedings Paper CT IAGA Workshop on Geomagnetic Observatory Instruments CY NOV 09-17, 2004 CL Kakioka, JAPAN SP Int Assoc Geomagnetism & Aeron DE geomagnetic field; data management; virtual observatory AB Since the mid-1990s, many geomagnetic datasets began appearing on the World Wide Web. Often these data were not submitted to the World Data Centers as recommended since the International Geophysical Year (195758). As a result, existing data become naturally distributed creating an urgent need for more sophisticated search engines capable of identifying and retrieving the data from Web for scientific analyses. We introduce a Virtual Global Magnetic Observatory concept for "pulling" geomagnetie data distributed worldwide. The VGMO moves information exchange from simple file transfers to a higher level of abstraction, forming the distributed databases through establishment of self-organizing data nodes. We present the first working VGMO prototype: an "on-demand" objects-building Internet application that is transparent in its internal data management to the external users/clients. The VGMO server continuously builds data-objects only from client requests by going through a pre-set list of Web-based data nodes (including WDCs). As the retrieved data are added to the server (or node) database, future requests of the same interval would not force a new Web search. Furthermore, new nodes can be made available to others through the VGMO network, building the worldwide geomagnetic data "fabric" in a platform-independent and location-neutral environment of newly "webbed" digital data. Application is on a server at http://mist.engin.umich.edu. C1 Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA. NASA, Goddard Space Flight Ctr, Space Phys Data Facil, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, QSS Grp Inc, Greenbelt, MD 20771 USA. Natl Sci Fdn, Arlington, VA 22230 USA. IZMIRAN, Troitsk 142092, Moscow Region, Russia. RP Papitashvili, VO (reprint author), Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA. EM papita@umich.edu; vpetrov@engin.umich.edu; anshuman.saxena@tcs.com; bob.clauer@umich.edu; natasha@mail630.gsfc.nasa.gov OI Papitashvili, Vladimir/0000-0001-6955-4894 NR 13 TC 1 Z9 1 U1 0 U2 1 PU TERRA SCIENTIFIC PUBL CO PI TOKYO PA 2003 SANSEI JIYUGAOKA HAIMU, 5-27-19 OKUSAWA, SETAGAYA-KU, TOKYO, 158-0083, JAPAN SN 1343-8832 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2006 VL 58 IS 6 BP 765 EP 774 PG 10 WC Geosciences, Multidisciplinary SC Geology GA 054CC UT WOS:000238352600012 ER PT B AU Reber, CA Ramapriyan, HK AF Reber, Carl A. Ramapriyan, H. K. BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI Earth science satellite remote sensing data from the EOS data and information system SO EARTH SCIENCE SATELLITE REMOTE SENSING: DATA, COMPUTATIONAL PROCESSING, AND TOOLS, VOL 2 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ C1 [Reber, Carl A.; Ramapriyan, H. K.] NASA, Goddard Space Flight Ctr, Code 423-0, Greenbelt, MD 20771 USA. RP Reber, CA (reprint author), NASA, Goddard Space Flight Ctr, Code 423-0, Greenbelt, MD 20771 USA. EM skip.reber@gmail.com; ramapriyan@gsfc.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-540-35630-1 PY 2006 BP 11 EP + DI 10.1007/978-3-540-37294-3_2 PG 2 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY54 UT WOS:000245437100002 ER PT B AU Coronado, PL Brentzel, KW AF Coronado, Patrick L. Brentzel, Kelvin W. BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI NASA direct readout for its polar orbiting satellites SO EARTH SCIENCE SATELLITE REMOTE SENSING: DATA, COMPUTATIONAL PROCESSING, AND TOOLS, VOL 2 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Coronado, PL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM patrick.l.coronado@nasa.gov; kelvin.w.brentzel@gsfc.nasa.gov FU NPOESS Preparatory Project (NPP) FX Research and development discussed in this chapter have been supported by the NPOESS Preparatory Project (NPP) and Dr. James Dodge at NASA former Code YS Earth Sciences Division. Special recognition is also given to Mr. Charles Vermillion and Mr. Fran Stetina, former NASA civil servants for their pioneering work in DB and DR systems. NR 4 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-540-35630-1 PY 2006 BP 52 EP + DI 10.1007/978-3-540-37294-3_4 PG 2 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY54 UT WOS:000245437100004 ER PT B AU Xiong, XX Barnes, W AF Xiong, Xiaoxiong Barnes, William BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI MODIS calibration and characterization SO EARTH SCIENCE SATELLITE REMOTE SENSING: DATA, COMPUTATIONAL PROCESSING, AND TOOLS, VOL 2 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID RESOLUTION IMAGING SPECTRORADIOMETER; REFLECTIVE SOLAR BANDS; EOS-AM1 C1 [Xiong, Xiaoxiong] NASA Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. [Barnes, William] Univ Maryland, Baltimore, MD 21250 USA. RP Xiong, XX (reprint author), NASA Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. EM jxiong@ltpmail.gsfc.nasa.gov; wbarnes@neptune.gsfc.nasa.gov RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 17 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-540-35630-1 PY 2006 BP 77 EP + DI 10.1007/978-3-540-37294-3_5 PG 3 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY54 UT WOS:000245437100005 ER PT B AU Barnes, W Xiong, XX Eplee, R Sun, JQ Lyu, CH AF Barnes, William Xiong, Xiaoxiong Eplee, Robert Sun, Junqiang Lyu, Cheng-Hsuan BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI Use of the moon for calibration and characterization of MODIS, SeaWiFS, and VIRS SO EARTH SCIENCE SATELLITE REMOTE SENSING: DATA, COMPUTATIONAL PROCESSING, AND TOOLS, VOL 2 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID RAINFALL MEASURING MISSION; ON-ORBIT CALIBRATIONS; RADIOMETRIC CALIBRATION; PHOTOMETRIC FUNCTION; INFRARED SCANNER; LUNAR C1 [Barnes, William] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Earth Sciences Directorate, Greenbelt, MD 20771 USA. [Eplee, Robert] Sci Appl Int Corperat, Beltsville, MD 20705 USA. [Sun, Junqiang] NASA, GSFC, Greenbelt, MD USA. [Lyu, Cheng-Hsuan] Sci Syst & Appl Inc, Lanham, MD 10210 USA. RP Barnes, W (reprint author), Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. EM wbarnes@neptune.gsfc.nasa.gov; jxiong@ltpmail.gsfc.nasa.gov; eplee@seawifs.gsfc.nasa.gov; junqiang_sun@ssaihq.com RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 17 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-540-35630-1 PY 2006 BP 98 EP + DI 10.1007/978-3-540-37294-3_6 PG 3 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY54 UT WOS:000245437100006 ER PT B AU Lynnes, C AF Lynnes, Christopher BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI A simple, scalable, script-based science processor SO EARTH SCIENCE SATELLITE REMOTE SENSING: DATA, COMPUTATIONAL PROCESSING, AND TOOLS, VOL 2 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lynnes, C (reprint author), NASA, Goddard Space Flight Ctr, Code 902, Greenbelt, MD 20771 USA. EM clynnes@pop600.gsfc.nasa.gov RI Lynnes, Christopher/B-4506-2010 OI Lynnes, Christopher/0000-0001-6744-3349 NR 8 TC 0 Z9 1 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-540-35630-1 PY 2006 BP 146 EP 161 DI 10.1007/978-3-540-37294-3_8 PG 16 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY54 UT WOS:000245437100008 ER PT B AU Chiu, LS Liu, Z Rui, HL Teng, WL AF Chiu, Long S. Liu, Zhong Rui, Hualan Teng, William L. BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI Tropical rainfall measuring mission data and access tools SO EARTH SCIENCE SATELLITE REMOTE SENSING: DATA, COMPUTATIONAL PROCESSING, AND TOOLS, VOL 2 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ C1 [Chiu, Long S.; Liu, Zhong; Rui, Hualan; Teng, William L.] NASA, GES, Data & Informat Serv, Code 610-2, Greenbelt, MD 20771 USA. RP Chiu, LS (reprint author), NASA, GES, Data & Informat Serv, Code 610-2, Greenbelt, MD 20771 USA. EM lchiu@gmu.edu; zliu@eosdata.gsfc.nasa.gov; rui@daac.gsfc.nasa.gov; teng@daac.gsfc.nasa.gov NR 10 TC 2 Z9 3 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-540-35630-1 PY 2006 BP 202 EP + DI 10.1007/978-3-540-37294-3_12 PG 3 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY54 UT WOS:000245437100012 ER PT B AU Di, LP McDonald, KR AF Di, Liping McDonald, Kenneth R. BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI The NASA HDF-EOS Web GIS software suite SO EARTH SCIENCE SATELLITE REMOTE SENSING: DATA, COMPUTATIONAL PROCESSING, AND TOOLS, VOL 2 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ C1 [Di, Liping] George Mason Univ, LAITS, 6301 Ivy Lane,Suite 620, Greenbelt, MD 20770 USA. [McDonald, Kenneth R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Di, LP (reprint author), George Mason Univ, LAITS, 6301 Ivy Lane,Suite 620, Greenbelt, MD 20770 USA. EM lpd@rattler.gsfc.nasa.gov FU NASA Earth Science Data and Information Project(ESDISP); NASA Earth Science Technology Office (ESTO); Open Geospatial Consortium (OGC) FX This project has been supported by research grants from the NASA Earth Science Data and Information Project (ESDISP), NASA Earth Science Technology Office (ESTO), and Open Geospatial Consortium (OGC). NR 17 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 978-3-540-35630-1 PY 2006 BP 245 EP + DI 10.1007/978-3-540-37294-3_15 PG 2 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY54 UT WOS:000245437100015 ER PT B AU Salomonson, VV Barnes, W Masuoka, EJ AF Salomonson, Vincent V. Barnes, William Masuoka, Edward J. BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI Introduction to MODIS and an overview of associated activities SO EARTH SCIENCE SATELLITE REMOTE SENSING: SCIENCE AND INSTRUMENTS, VOL 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID EARTH C1 [Salomonson, Vincent V.] Univ Utah, Salt Lake City, UT 84112 USA. [Barnes, William] Univ Maryland, Baltimore, MD 21250 USA. NASA, Goddard Space Flight, Earth Sun Div, Greenbelt, MD 20711 USA. RP Salomonson, VV (reprint author), Univ Utah, Salt Lake City, UT 84112 USA. EM vincent.v.salomonson@nasa.gov; wbarnes@neptune.gsfc.nasa.gov NR 25 TC 3 Z9 3 U1 1 U2 2 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 12 EP + DI 10.1007/978-3-540-37293-6_2 PG 3 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900002 ER PT B AU Xiaoxiong, Isaacman, A Barnes, W AF Xiong, Xiaoxiong Isaacman, Alice Barnes, William BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI MODIS level-1B products SO EARTH SCIENCE SATELLITE REMOTE SENSING: SCIENCE AND INSTRUMENTS, VOL 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID RESOLUTION IMAGING SPECTRORADIOMETER; CALIBRATION; EOS-AM1; SYSTEM; EARTH C1 [Isaacman, Alice] NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Code 661, Greenbelt, MD 20771 USA. RP Isaacman, A (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Code 661, Greenbelt, MD 20771 USA. EM wbarnes@neptune.gsfc.nasa.gov RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 15 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 33 EP + PG 3 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900003 ER PT B AU Wolfe, RE AF Wolfe, Robert E. BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI MODIS geolocation SO Earth Science Satellite Remote Sensing: Science and Instruments, Vol 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID IMAGING SPECTRORADIOMETER MODIS; GEOMETRIC CORRECTION; LAND; MISREGISTRATION; INSTRUMENT; NAVIGATION; ACCURACY; IMPACT C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wolfe, RE (reprint author), NASA, Goddard Space Flight Ctr, Code 992, Greenbelt, MD 20771 USA. RI Wolfe, Robert/E-1485-2012 OI Wolfe, Robert/0000-0002-0915-1855 NR 28 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 50 EP 73 DI 10.1007/978-3-540-37293-6_4 PG 24 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900004 ER PT B AU Baum, BA Platnick, S AF Baum, Bryan A. Platnick, Steven BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI Introduction to MODIS cloud products SO EARTH SCIENCE SATELLITE REMOTE SENSING: SCIENCE AND INSTRUMENTS, VOL 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID AIRBORNE SIMULATOR IMAGERY; SIZE DISTRIBUTIONS; CIRRUS; WATER; TEMPERATURE; MODELS; TERRA C1 [Baum, Bryan A.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA. [Platnick, Steven] NASA, Goddard Space Flight Ctr, Lab Atmospheres, Greenbelt, MD 20771 USA. RP Baum, BA (reprint author), NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA. EM bryan.baum@ssec.wisc.edu; steven.e.platnick@nasa.gov RI Platnick, Steven/J-9982-2014; Baum, Bryan/B-7670-2011 OI Platnick, Steven/0000-0003-3964-3567; Baum, Bryan/0000-0002-7193-2767 NR 24 TC 6 Z9 6 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 74 EP + DI 10.1007/978-3-540-37293-6_5 PG 3 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900005 ER PT B AU Chu, DA Remer, L AF Chu, D. Allen Remer, Lorraine BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI MODIS observation of aerosol loading from 2000 to 2004 SO EARTH SCIENCE SATELLITE REMOTE SENSING: SCIENCE AND INSTRUMENTS, VOL 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID OPTICAL-THICKNESS; AIR-QUALITY; SATELLITE; REFLECTANCE; RETRIEVALS; VALIDATION; ALGORITHM; OCEAN C1 [Chu, D. Allen] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Remer, Lorraine] NASA, Goddard Space Flight Ctr, Lab Atmospheres, Greenbelt, MD USA. RP Chu, DA (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. EM achu@climate.gsfc.nasa.gov; remer@climate.gsfc.nasa.gov NR 27 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 92 EP + DI 10.1007/978-3-540-37293-6_6 PG 4 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900006 ER PT B AU Wolfe, RE Saleous, N AF Wolfe, Robert E. Saleous, Nazmi BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI MODIS land products and data processing SO EARTH SCIENCE SATELLITE REMOTE SENSING: SCIENCE AND INSTRUMENTS, VOL 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID VALIDATION; AREA C1 [Wolfe, Robert E.; Saleous, Nazmi] NASA, Goddard Space Flight Ctr, Raytheon ITSS, Code 922, Greenbelt, MD 20771 USA. RP Wolfe, RE (reprint author), NASA, Goddard Space Flight Ctr, Raytheon ITSS, Code 922, Greenbelt, MD 20771 USA. EM rwolfe@pop900.gsfc.nasa.gov; nazmi@kratmos.gsfc.nasa.gov RI Wolfe, Robert/E-1485-2012 OI Wolfe, Robert/0000-0002-0915-1855 FU MODIS Science Team; MODIS Science Data Support Team; NASA GSFC [NAS5-32350] FX The author acknowledges support provided by the MODIS Science Team and the MODIS Science Data Support Team. This work was performed under the direction of the MODIS Science Team in the Terrestrial Information Systems Branch (Code 614.5) of the Hydrospheric and Biospheric Sciences Laboratory (Code 614) at NASA GSFC. The work was funded under NASA GSFC contract NAS5-32350. NR 19 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 110 EP + PG 3 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900007 ER PT B AU Vermote, EF Saleous, NZ AF Vermote, Eric F. Saleous, Nazmi Z. BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI Operational atmospheric correction of MODIS visible to middle infrared land surface data in the case of an infinite Lambertian target SO EARTH SCIENCE SATELLITE REMOTE SENSING: SCIENCE AND INSTRUMENTS, VOL 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID TROPOSPHERIC AEROSOL; VALIDATION C1 [Vermote, Eric F.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Saleous, Nazmi Z.] NASA, Goddard Space Flight Ctr, Raytheon ITS, Greenbelt, MD USA. RP Vermote, EF (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA. EM eric@kratmos.gsfc.nasa.gov; nazmi@kratmos.gsfc.nasa.gov RI Vermote, Eric/K-3733-2012 NR 17 TC 3 Z9 3 U1 0 U2 3 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 123 EP + DI 10.1007/978-3-540-37293-6_8 PG 3 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900008 ER PT B AU Hall, DK Riggs, GA Salomonson, VV AF Hall, Dorothy K. Riggs, George A. Salomonson, Vincent V. BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI MODIS snow and sea ice products SO EARTH SCIENCE SATELLITE REMOTE SENSING: SCIENCE AND INSTRUMENTS, VOL 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID RESOLUTION IMAGING SPECTRORADIOMETER; LANDSAT THEMATIC MAPPER; SURFACE-TEMPERATURE; COVER PRODUCTS; SATELLITE DATA; GRAIN-SIZE; VALIDATION; EXTENT; CLOUD; VARIABILITY C1 [Hall, Dorothy K.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614-1, Greenbelt, MD 20771 USA. [Riggs, George A.] SSAI, Lanham, MD USA. [Salomonson, Vincent V.] Univ Utah, Salt Lake City, UT 84112 USA. [Salomonson, Vincent V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20711 USA. RP Hall, DK (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Code 614-1, Greenbelt, MD 20771 USA. EM dhall@glacier.gsfc.nasa.gov; griggs@ltpmail.gsfc.nasa.gov; vincent.v.salomonson@nasa.gov RI Hall, Dorothy/D-5562-2012 NR 67 TC 4 Z9 5 U1 0 U2 8 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 154 EP + DI 10.1007/978-3-540-37293-6_9 PG 6 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900009 ER PT B AU Murphy, RE AF Murphy, Robert E. BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI The NPOESS preparatory project SO Earth Science Satellite Remote Sensing: Science and Instruments, Vol 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ C1 NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. RP Murphy, RE (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 182 EP 198 DI 10.1007/978-3-540-37293-6_10 PG 17 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900010 ER PT B AU Murphy, RE Ardanuy, P Deluccia, FJ Clement, JE Schueler, CF AF Murphy, R. E. Ardanuy, Phillip Deluccia, Frank J. Clement, J. E. Schueler, Carl F. BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI The visible infrared imaging radiometer suite SO EARTH SCIENCE SATELLITE REMOTE SENSING: SCIENCE AND INSTRUMENTS, VOL 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ C1 [Murphy, R. E.] NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Code 661, Greenbelt, MD 20771 USA. [Ardanuy, Phillip] Raytheon Informat Solut, Reston, VA 20191 USA. [Deluccia, Frank J.] Aerosp Corp, Los Angeles, CA 90009 USA. [Clement, J. E.; Schueler, Carl F.] Raytheon Santa Barbara Remote Sensing, Goleta, CA 93117 USA. RP Murphy, RE (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Code 661, Greenbelt, MD 20771 USA. EM robert.murphy@noaa.gov NR 2 TC 3 Z9 3 U1 0 U2 2 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 199 EP + DI 10.1007/978-3-540-37293-6_11 PG 2 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900011 ER PT B AU Susskind, J AF Susskind, Joel BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI Introduction to AIRS and CrIS SO Earth Science Satellite Remote Sensing: Science and Instruments, Vol 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID SOUNDER C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Susskind, J (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 661, Greenbelt, MD 20771 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 254 EP 278 DI 10.1007/978-3-540-37293-6_14 PG 25 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900014 ER PT B AU Chiu, LS Shin, DB Kwiatkowski, J AF Chiu, Long S. Shin, Dong-Bin Kwiatkowski, John BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI Surface rain rates from tropical rainfall measuring mission satellite algorithms SO EARTH SCIENCE SATELLITE REMOTE SENSING: SCIENCE AND INSTRUMENTS, VOL 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID TRMM PRECIPITATION RADAR; GLOBAL PRECIPITATION; PROFILING ALGORITHM; MICROWAVE IMAGER; VALIDATION; RETRIEVALS; DATASET; SITE C1 [Chiu, Long S.] George Mason Univ, Ctr Earth Observing & Space Res, Sch Computat Sci, Fairfax, VA 22030 USA. [Shin, Dong-Bin] George Mason Univ, Sch Computat Sci, Ctr Earth Observ & Space Res, Fairfax, VA 22030 USA. [Kwiatkowski, John] George Mason Univ, NASA, Goddard Space Flight Ctr, TRMM Sci Data & Informat Syst, Greenbelt, MD 20771 USA. RP Chiu, LS (reprint author), George Mason Univ, Ctr Earth Observing & Space Res, Sch Computat Sci, Fairfax, VA 22030 USA. EM lchiu@gmu.edu; dshin@scs.gmu.edu; johnk@tsdis.gsfc.nasa.gov FU NASA TRMM program; NASA REASoN program and NASA [NNG04GB02G] FX We thanked Drs. Roberrt Adler, George Huffman, and an anomynous reviewer for useful comments, Dr. Yimin Ji and Mr. John Stout for computing statistics for February 1998 data for V6. The authors acknowledge support from the NASA TRMM program. LSC is also partially supported by the NASA REASoN program and NASA grant NNG04GB02G. The TRMM data is processed by TSDIS and distributed by the NASA GSFC DAAC NR 32 TC 0 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 317 EP + DI 10.1007/978-3-540-37293-6_17 PG 4 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900017 ER PT B AU Ji, YM Stocker, E AF Ji, Yimin Stocker, Erich BE Qu, JJ Gao, W Kafatos, M Murphy, RE Salomonson, VV TI TRMM fire algorithm, product and applications SO EARTH SCIENCE SATELLITE REMOTE SENSING: SCIENCE AND INSTRUMENTS, VOL 1 LA English DT Proceedings Paper CT 2nd Workshop of the Earth Science Satellite Remote Sensing CY OCT 15-22, 2002 CL George Mason Univ, Fairfax, VA HO George Mason Univ ID TROPICS; TEMPERATURE; SMOKE; IDENTIFICATION; PRECIPITATION; OSCILLATION; RESOLUTION; DYNAMICS; AEROSOLS; CLIMATE C1 [Ji, Yimin] George Mason Univ, Sch Computat Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Stocker, Erich] NASA, Goddard Space Flight Ctr, TRMM TSDIS, Greenbelt, MD 20770 USA. RP Ji, YM (reprint author), George Mason Univ, Sch Computat Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. EM yji@tsdis.gsfc.nasa.gov; stocker@tsdis.gsfc.nasa.gov NR 41 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-35606-6 PY 2006 BP 363 EP + DI 10.1007/978-3-540-37293-6_19 PG 4 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing SC Engineering; Instruments & Instrumentation; Remote Sensing GA BFY52 UT WOS:000245436900019 ER PT J AU Zhong, ZM AF Zhong, ZM TI Bismuth ruthenate-based pyrochlores for IT-SOFC applications SO ELECTROCHEMICAL AND SOLID STATE LETTERS LA English DT Article ID OXIDE FUEL-CELLS; RESISTANT CE0.8SM0.2O1.9 ELECTROLYTE; THIN BACE1-XSMXO3-ALPHA; METALLIC INTERCONNECTS; COMBUSTION SYNTHESIS; TEMPERATURE SOFCS; CONTAINING ALLOY; CATHODES; LAYER; PERFORMANCE AB The densification and electrochemical activity for oxygen reduction of the bismuth ruthenate pyrochlores, Bi-2(Ru2-xBix)O7-delta (x = 0.0 - 0.8) synthesized by the Pechini method, have been investigated as the interconnect and cathode materials for intermediate temperature solid oxide fuel cells (IT-SOFCs). The substitution of bismuth on the ruthenium site significantly improves the densification process. Some compositions of the pyrochlore family are promising coating materials for metallic interconnects. Anode-supported fuel cells with doped ceria as the electrolyte have been fabricated and tested. Impedance spectra of the fuel cells demonstrate high catalytic activity for oxygen reduction. The area-specific resistance at 600 degrees C is less than 1.0 Omega cm(2). (c) 2006 The Electrochemical Society. C1 NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Zhong, ZM (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. EM zhong11135@yahoo.com NR 24 TC 11 Z9 11 U1 1 U2 6 PU ELECTROCHEMICAL SOC INC PI PENNINGTON PA 65 SOUTH MAIN STREET, PENNINGTON, NJ 08534 USA SN 1099-0062 J9 ELECTROCHEM SOLID ST JI Electrochem. Solid State Lett. PY 2006 VL 9 IS 4 BP A215 EP A219 DI 10.1149/1.2176887 PG 5 WC Electrochemistry; Materials Science, Multidisciplinary SC Electrochemistry; Materials Science GA 014KU UT WOS:000235479800010 ER PT S AU Choi, SH Elliott, JR King, GC AF Choi, Sang H. Elliott, James R. King, Glen C. BE Shwaery, GT Blitch, JG Land, C TI Power budget analysis for high altitude airships - art. no. 62190C SO Enabling Technologies and Design of Nonlethal Weapons SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Enabling Technologies and Design of Nonlethal Weapons CY APR 18-19, 2006 CL Kissimmee, FL SP SPIE ID MICROWAVE AB The High Altitude Airship (HAA) has various potential applications and mission scenarios that require onboard energy harvesting and power distribution systems. The energy source considered for the HAA's power budget is solar photon energy that allows the use of either photovoltaic (PV) cells or advanced thermoelectric (ATE) converters. Both PV cells and an ATE system utilizing high performance thermoelectric materials were briefly compared to identify the advantages of ATE for HAA applications in this study. The ATE can generate a higher quantity of harvested energy than PV cells by utilizing the cascaded efficiency of a three-staged ATE in a tandem mode configuration. Assuming that each stage of ATE material has the figure of merit of 5, the cascaded efficiency of a three-staged ATE system approaches the overall conversion efficiency greater than 60%. Based on this estimated efficiency, the configuration of a HAA and the power utility modules are defined. C1 NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Choi, SH (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA. NR 20 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 0-8194-6275-6 J9 P SOC PHOTO-OPT INS PY 2006 VL 6219 BP C2190 EP C2190 AR 62190C DI 10.1117/12.663586 PG 12 WC Engineering, Multidisciplinary; Engineering, Biomedical SC Engineering GA BES57 UT WOS:000239301000010 ER PT J AU El-Genk, MS Saber, HH Caillat, T Sakamoto, J AF El-Genk, MS Saber, HH Caillat, T Sakamoto, J TI Tests results and performance comparisons of coated and un-coated skutterudite based segmented unicouples SO ENERGY CONVERSION AND MANAGEMENT LA English DT Article DE thermoelectric conversion; skutterudite; metallic coating; performance tests AB Skutterudite based thermoelectric unicouples are being considered for use in Advanced Radioisotope Power Systems (ARPSs) to support NASA's planetary exploration missions. For these systems, which would be much lighter than state of the art Radioisotope Thermoelectric Generators (RTGs), it is important to ensure minimal degradation in the performance of unicouples that may be caused by material sublimation. In this work, two unicouples, JAN-04 with a thin metallic coating on the legs near the hot junction to suppress antimony sublimation and SEP-03 without coating, are tested for >1000 and 3600 h, respectively. The legs in the two unicouples are of almost the same dimensions and compositions; the p-legs are made of CeFe3.5Co0.5Sb12 and Bi0.4Sb1.6Te3 segments and the n-legs are made of CoSb3 and Bi2Te2.95Se0.05 segments. SEP-03 is tested at average hot and cold junction temperatures of 961.5 +/- 22.0 and 296.3 +/- 5.7 K, respectively, in argon gas at similar to 0.068 MPa, and JAN-04 is tested at 962.8 +/- 20.5 and 294.5 +/- 3.3 K, respectively, initially in argon gas at the same pressure for similar to 26.5 h then in vacuum similar to 9.0 X 10(-7) Torr for >973.5 h. The measured open circuit voltage V-oc (240 mV) and peak electrical power (1.64 W-e) for SEP-03 at the beginning of test (BOT) are higher than those for JAN-04 (188 mV and 0.84 W-e, respectively). Although the argon gas effectively decreased the antimony loss from the legs of SEP-03, marked degradations in performance occurred. The estimated peak efficiency for SEP-03 decreased from 13.8% at BOT to 5.8% at end of test (EOT), and the peak power decreased from 1.64 W-e at BOT to 0.48 W-e at EOT, however, V-oc decreased by similar to 14%. The latter for JAN-04 decreased only by similar to 3%, the estimated peak efficiency (similar to 12%) changed very little and the peak power decreased by similar to 20%. Unlike SEP-03, the measured total and contact resistances of the legs in JAN-04 changed very little. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ New Mexico, Dept Chem & Nucl Engn, Albuquerque, NM 87131 USA. Univ New Mexico, Inst Space & Nucl Power Studies, Albuquerque, NM 87131 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Univ New Mexico, Dept Chem & Nucl Engn, Albuquerque, NM 87131 USA. EM mgenk@unm.edu NR 17 TC 59 Z9 59 U1 1 U2 32 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0196-8904 EI 1879-2227 J9 ENERG CONVERS MANAGE JI Energy Conv. Manag. PD JAN PY 2006 VL 47 IS 2 BP 174 EP 200 DI 10.1016/j.enconman.2005.03.023 PG 27 WC Thermodynamics; Energy & Fuels; Mechanics SC Thermodynamics; Energy & Fuels; Mechanics GA 978BR UT WOS:000232847700002 ER PT S AU Hines, GD Rahman, ZU Jobson, DJ Woodell, GA AF Hines, Glenn D. Rahman, Zia-ur Jobson, Daniel J. Woodell, Glenn A. BE Verly, JG Guell, JJ TI Real-time enhancement, registration, and fusion for a multi-sensor enhanced vision system - art. no. 622609 SO Enhanced and Synthetic Vision 2006 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Enhanced and Synthetic Vision 2006 Conference CY APR 17-18, 2006 CL Kissimmee, FL SP SPIE DE enhanced vision system; image enhancement; retinex; digital signal processing; sensor fusion ID RETINEX AB Over the last few years NASA Langley Research Center (LaRC) has been developing an Enhanced Vision System (EVS) to aid pilots while flying in poor visibility conditions. The EVS captures imagery using two infrared video cameras. The cameras are placed in an enclosure that is mounted and flown forward-looking underneath the NASA LaRC ARIES 757 aircraft. The data streams from the cameras are processed in real-time and displayed on monitors on-board the aircraft. With proper processing the camera system can provide better-than-human-observed imagery particularly during poor visibility conditions. However, to obtain this goal requires several different stages of processing including enhancement, registration, and fusion, and specialized processing hardware for real-time performance. We are using a real-time implementation of the Retinex algorithm for image enhancement, affine transformations for registration, and weighted sums to perform fusion. All of the algorithms are executed on a single TI DM642 digital signal processor (DSP) clocked at 720 MHz. The image processing components were added to the EVS system, tested, and demonstrated during flight tests in August and September of 2005. In this paper we briefly discuss the EVS image processing hardware and algorithms. We then discuss implementation issues and show examples of the results obtained during flight tests. C1 NASA, Langley Res Ctr, Hampton, VA 23861 USA. RP Hines, GD (reprint author), NASA, Langley Res Ctr, Hampton, VA 23861 USA. NR 8 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 0-8194-6282-9 J9 P SOC PHOTO-OPT INS PY 2006 VL 6226 BP 22609 EP 22609 AR 622609 DI 10.1117/12.665853 PG 8 WC Computer Science, Artificial Intelligence SC Computer Science GA BEU95 UT WOS:000239569900009 ER PT S AU Bailey, RE Kramer, LJ Prinzel, LJ AF Bailey, Randall E. Kramer, Lynda J. Prinzel, Lawrence J., III BE Verly, JG Guell, JJ TI Crew and display concepts evaluation for synthetic/enhanced vision systems - art. no. 62260G SO Enhanced and Synthetic Vision 2006 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Enhanced and Synthetic Vision 2006 Conference CY APR 17-18, 2006 CL Kissimmee, FL SP SPIE DE synthetic vision system; enhanced vision system; enhanced flight vision system; image fusion; Head-Up Display; crew resource management; FLIR; runway incursions; aviation safety AB NASA's Synthetic Vision Systems (SVS) project is developing technologies with practical applications that strive to eliminate low-visibility conditions as a causal factor to civil aircraft accidents and replicate the operational benefits of clear day flight operations, regardless of the actual outside visibility condition. Enhanced Vision System (EVS) technologies are analogous and complementary in many respects to SVS, with the principle difference being that EVS is an imaging sensor presentation, as opposed to a database-derived image. The use of EVS in civil aircraft is projected to increase rapidly as the Federal Aviation Administration recently changed the aircraft operating rules under Part 91, revising the flight visibility requirements for conducting operations to civil airports. Operators conducting straight-in instrument approach procedures may now operate below the published approach minimums when using an approved EVS that shows the required visual references on the pilot's Head-Up Display. An experiment was conducted to evaluate the complementary use of SVS and EVS technologies, specifically focusing on new techniques for integration and/or fusion of synthetic and enhanced vision technologies and crew resource management while operating under the newly adopted FAA rules which provide operating credit for EVS. Overall, the experimental data showed that significant improvements in SA without concomitant increases in workload and display clutter could be provided by the integration and/or fusion of synthetic and enhanced vision technologies for the pilot-flying and the pilot-not-flying. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Bailey, RE (reprint author), NASA, Langley Res Ctr, MS 152, Hampton, VA 23681 USA. NR 19 TC 1 Z9 1 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 0-8194-6282-9 J9 P SOC PHOTO-OPT INS PY 2006 VL 6226 BP G2260 EP G2260 AR 62260G DI 10.1117/12.666711 PG 18 WC Computer Science, Artificial Intelligence SC Computer Science GA BEU95 UT WOS:000239569900016 ER PT S AU Arthur, JJ Prinzel, LJ Williams, SP Kramer, LJ AF Arthur, Jarvis (Trey) J., III Prinzel, Lawrence J., III Williams, Steven P. Kramer, Lynda J. BE Verly, JG Guell, JJ TI Synthetic vision enhanced surface operations and flight procedures rehearsal tool - art. no. 62260I SO Enhanced and Synthetic Vision 2006 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Enhanced and Synthetic Vision 2006 Conference CY APR 17-18, 2006 CL Kissimmee, FL SP SPIE DE synthetic vision; head-worn displays; helmet-mounted displays; surface operations; electronic flight bag; mission rehearsal ID DISPLAY CONCEPTS AB Limited visibility has been cited as predominant causal factor for both Controlled-Flight-Into-Terrain (CFIT) and runway incursion accidents. NASA is conducting research and development of Synthetic Vision Systems (SVS) technologies which may potentially mitigate low visibility conditions as a causal factor to these accidents while replicating the operational benefits of clear day flight operations, regardless of the actual outside visibility condition. Two experimental evaluation studies were performed to determine the efficacy of two concepts: 1) head-worn display application of SVS technology to enhance transport aircraft surface operations, and 2) three-dimensional SVS electronic flight bag display concept for flight plan preview, mission rehearsal and controller-pilot data link communications interface of flight procedures. In the surface operation study, pilots evaluated two display devices and four display modes during taxi under unlimited and CAT 11 visibility conditions. In the mission rehearsal study, pilots flew approaches and departures in an operationally-challenged airport environment, including CFIT scenarios. Performance using the SVS concepts was compared to traditional baseline displays with paper charts only or EFB information. In general, the studies evince the significant situation awareness and enhanced operational capabilities afforded from these advanced SVS display concepts. The experimental results and conclusions from these studies are discussed along with future directions. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Arthur, JJ (reprint author), NASA, Langley Res Ctr, 24 W Taylor St, Hampton, VA 23681 USA. NR 17 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 0-8194-6282-9 J9 P SOC PHOTO-OPT INS PY 2006 VL 6226 BP I2260 EP I2260 AR 62260I DI 10.1117/12.666636 PG 20 WC Computer Science, Artificial Intelligence SC Computer Science GA BEU95 UT WOS:000239569900018 ER PT S AU Szoboszlay, Z Jennings, C Tiana, C AF Szoboszlay, Zoltan Jennings, Chad Tiana, Carlo BE Verly, JG Guell, JJ TI Synthetic vision for rotorcraft: Low level flight - art. no. 62260N SO Enhanced and Synthetic Vision 2006 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Enhanced and Synthetic Vision 2006 Conference CY APR 17-18, 2006 CL Kissimmee, FL SP SPIE DE synthetic vision; flight path marker; radar; fusion; ATP-FPM; IMSIS AB Two topics are discussed in this paper. The first is the Integrated Multi-sensor Synthetic Imagery System (IMSIS), being developed under an Army SBIR contract. The system updates on-board, pre-stored, terrain elevation data with 3D terrain elevation sensor data (such as radar). The system also merges 2D image contrast sensor data (such as infrared imagery) with the updated 3D terrain elevation data to render a synthetic image of the terrain on the rotorcraft pilot's display. The second topic is the testing of a new flight path marker, to show the pilot the predicted location of the aircraft with respect to the synthetic terrain (at 100m distance), as well as the predicted height above the terrain, the desired height above the terrain, and the point on the terrain the aircraft is expected to fly over. The Altitude and ground Track Predicting Flight Path Marker (ATP-FPM) symbol takes advantage of knowledge of terrain elevations ahead of the aircraft from a synthetic vision system, such as IMSIS. In simulation, the maximum low altitude error and maximum ground track error were both reduced by a factor of 2 with the ATP-FPM compared to the traditional instantaneous flight path marker. Pilot-to-pilot variations in performance were reduced and workload decreased with the ATP-FPM. C1 USA, Res Dev & Engn Command, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA 94035 USA. RP Szoboszlay, Z (reprint author), USA, Res Dev & Engn Command, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, Moffett Field, CA 94035 USA. NR 13 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 0-8194-6282-9 J9 P SOC PHOTO-OPT INS PY 2006 VL 6226 BP N2260 EP N2260 AR 62260N DI 10.1117/12.667891 PG 12 WC Computer Science, Artificial Intelligence SC Computer Science GA BEU95 UT WOS:000239569900023 ER PT S AU Chapman, BM Huang, L Jin, HQ Jost, G de Supinski, BR AF Chapman, Barbara M. Huang, Lei Jin, Haoqiang Jost, Gabriele de Supinski, Bronis R. BE Nagel, WE Walter, WV Lehner, W TI Toward enhancing OpenMP's work-sharing directives SO EURO-PAR 2006 PARALLEL PROCESSING SE Lecture Notes in Computer Science LA English DT Article; Proceedings Paper CT 12th International Euro-Par Conference on Parallel Processing CY AUG 28-SEP 01, 2006 CL Dresden, GERMANY AB OpenMP provides a portable programming interface for shared memory parallel computers (SMPs). Although this interface has proven successful for small SMPs, it requies greater flexibility in light of the steadily growing size of individual SMPs and the recent advent of multithreaded chips. In this paper, we describe two application development experiences that exposed these expressivity problems in the current OpenMP specification. We then propose mechanisms to overcome these limitations, including thread subteams and thread topologies. Thus, we identify language features that improve OpenMP application performance on emerging and large-scale platforms while preserving ease of programming. C1 Univ Houston, Houston, TX 77004 USA. NASA, Ames Res Ctr, Mountain View, CA USA. Lawrence Livermore Natl Lab, Livermore, CA USA. RP Chapman, BM (reprint author), Univ Houston, Houston, TX 77004 USA. EM chapman@cs.uh.edu; leihuang@cs.uh.edu; hjin@nas.nasa.gov; gabriele.jost@sun.com; bronis@llnl.gov NR 14 TC 9 Z9 9 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-37783-2 J9 LECT NOTES COMPUT SC PY 2006 VL 4128 BP 645 EP 654 PG 10 WC Computer Science, Theory & Methods SC Computer Science GA BFE49 UT WOS:000241469500058 ER PT S AU Maimone, M Johnson, A Cheng, Y Willson, R Matthies, L AF Maimone, M Johnson, A Cheng, Y Willson, R Matthies, L BE Ang, MH Khatib, O TI Autonomous navigation results from the Mars Exploration Rover (MER) mission SO EXPERIMENTAL ROBOTICS IX SE Springer Tracts in Advanced Robotics LA English DT Proceedings Paper CT 9th International Symposium on Experimental Robotics (ISER) CY JUN 18-21, 2004 CL Singapore, SINGAPORE AB In January, 2004, the Mars Exploration Rover (MER) mission landed two rovers, Spirit and Opportunity, oil the surface of Mars. Several autonomous navigation capabilities were employed in space for the first time in this mission. In the Entry, Descent, and Landing (EDL) phase, both landers used a vision system called the Descent Image Motion Estimation System (DIMES) to estimate horizontal velocity during the last 2000 meters (m) of descent, by tracking features on the ground with a downlooking camera, in order to control retro-rocket firing to reduce horizontal velocity before impact. During surface operations, the rovers navigate autonomously using stereo vision for local terrain mapping and a local, reactive planning algorithm called Grid-based Estimation of Surface Traversability Applied to Local Terrain (GESTALT) for obstacle avoidance. In areas of high slip, stereo vision-based visual odometry has been used to estimate rover motion. As of mid-June, Spirit had traversed 3405 m, of which 1253 m were done autonomously; Opportunity had traversed 1264 m, of which 224 in were autonomous. These results have contributed substantially to the success of the mission and paved the way for increased levels of autonomy in future missions. C1 CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mark.maimone@jpl.nasa.gov; andrew.johnson@jpl.nasa.gov; yang.cheng@jpl.nasa.gov; reg.willson@jpl.nasa.gov; larry.matthies@jpl.nasa.gov NR 7 TC 7 Z9 7 U1 2 U2 7 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 1610-7438 BN 3-540-28816-3 J9 SPRINGER TRAC ADV RO PY 2006 VL 21 BP 3 EP + PG 2 WC Robotics SC Robotics GA BED74 UT WOS:000236887500001 ER PT S AU Bretl, T Rock, S Latombe, JC Kennedy, B Aghazarian, H AF Bretl, T Rock, S Latombe, JC Kennedy, B Aghazarian, H BE Ang, MH Khatib, O TI Free-climbing with a multi-use robot SO EXPERIMENTAL ROBOTICS IX SE Springer Tracts in Advanced Robotics LA English DT Proceedings Paper CT 9th International Symposium on Experimental Robotics (ISER) CY JUN 18-21, 2004 CL Singapore, SINGAPORE ID PROBABILISTIC ROADMAPS; SYSTEMS AB This paper presents a new four-limbed robot, LEMUR IIb (Legged Excursion Mechanical Utility Rover), that can free-climb vertical rock surfaces. This robot was designed to have a number of capabilities in addition to climbing (e.g., assembly, inspection, maintenance, transport, intervention) and to be able to traverse a variety of other types of terrain (e.g., roads, talus, dirt, urban rubble). To maximize its flexibility in this regard, LEMUR IIb will need to exploit sophisticated control, planning, and sensing techniques in order to climb, rather than rely on specific hardware modifications. In particular, this paper describes a new algorithm for planning safe one-step climbing moves, which has already enabled LEMUR IIb to climb an indoor, near-vertical surface with small, arbitrarily distributed, natural features. To the authors' knowledge, this is the first experimental demonstration of a multi-use, multi-limbed robot climbing such terrain using only friction at contact points (i.e., free-climbing). C1 Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. Stanford Univ, Dept Comp Sci, Stanford, CA 94305 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. EM tbretl@stanford.edu; rock@stanford.edu; latombe@cs.stanford.edu; bkennedy@helios.jpl.nasa.gov; hrand@helios.jpl.nasa.gov FU Herbert Kunzel Fellowship FX T. Bretl is supported by a Herbert Kunzel Fellowship. The authors would like to thank T. Miller, D. Black-Schaffer, and K. Hauser for their contributions NR 26 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 1610-7438 BN 3-540-28816-3 J9 SPRINGER TRAC ADV RO PY 2006 VL 21 BP 449 EP + PG 3 WC Robotics SC Robotics GA BED74 UT WOS:000236887500043 ER PT J AU Lee, DJ Cha, SS Ramachandran, N AF Lee, DJ Cha, SS Ramachandran, N TI Application of stereoscopic tracking velocimetry for experimental and numerical investigation of directional solidification SO EXPERIMENTAL THERMAL AND FLUID SCIENCE LA English DT Article DE directional solidification; particle tracking; velocimetry; stereoscopic tracking ID CRYSTAL-GROWTH; CONVECTION; BUOYANCY; FORCES AB A previously reported stereoscopic tracking velocimetry (STV) is further refined and applied to measure directional solidification. The flow involves complicated three-dimensional (3-D) convection, being subject to both buoyancy and surface tension forces in addition to conjugate conduction. For our STV, the 3-D tracking of numerous particles is the most important and challenging process. Here, the performances of the tracking algorithms, which are based on artificial neural networks, are first presented with a brief summary of the STV principles. The 3-D experiment measurements of the convective phenomena are then discussed together with the results from two-dimensional numerical modeling for qualitative comparison. (c) 2005 Elsevier Inc. All rights reserved. C1 Univ Illinois, Dept Mech & Ind Engn, Chicago, IL 60607 USA. Univ Illinois, Chicago, IL 60607 USA. NASA, George C Marshall Space Flight Ctr, BAE Syst Analyt Solut Inc, Huntsville, AL 35812 USA. RP Cha, SS (reprint author), Univ Illinois, Dept Mech & Ind Engn, MIC 251,842 W Taylor St, Chicago, IL 60607 USA. EM sscha@uic.edu NR 16 TC 2 Z9 2 U1 1 U2 1 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0894-1777 J9 EXP THERM FLUID SCI JI Exp. Therm. Fluid Sci. PD JAN PY 2006 VL 30 IS 3 BP 203 EP 212 DI 10.1016/j.expthermflusci.2005.05.007 PG 10 WC Thermodynamics; Engineering, Mechanical; Physics, Fluids & Plasmas SC Thermodynamics; Engineering; Physics GA 005AC UT WOS:000234793000005 ER PT J AU Vander Wal, RL Berger, GM Mozes, SD AF Vander Wal, RL Berger, GM Mozes, SD TI The combined influence of a rough surface and thin fluid film upon the splashing threshold and splash dynamics of a droplet impacting onto them SO EXPERIMENTS IN FLUIDS LA English DT Article ID SOLID-SURFACE; CROWN FORMATION; SINGLE DROP; LIQUID-FILM; WATER DROPS; ENTRAINMENT; COLLISIONS; WALL AB Surface roughness can have a critical effect upon the splashing threshold and dynamics of a drop impacting on either a dry or rough solid surface or one coated by a thin fluid film. As most coating applications and spray systems quickly evolve to a state where the droplets impinge upon fluid deposited by preceding droplets, the combined contributions of surface roughness and a pre-deposited thin liquid film of comparable thickness upon droplet impingement dynamics are examined. For comparison, we include results for droplets impacting on a smooth, dry surface and a smooth surface wetted by a thin fluid film. The inclusion of surface roughness considerably lowers the splashing threshold and alters the splashing dynamics such that differences in fluid surface tensions between 20.1 and 72.8 dynes/cm or viscosities between 0.4 and 3.3 cP have little effect. C1 NASA Glenn, Cleveland, OH 44135 USA. RP Vander Wal, RL (reprint author), NASA Glenn, MS 110-3,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM randy@rvander.grc.nasa.gov NR 33 TC 17 Z9 17 U1 4 U2 24 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0723-4864 J9 EXP FLUIDS JI Exp. Fluids PD JAN PY 2006 VL 40 IS 1 BP 23 EP 32 DI 10.1007/s00348-005-0043-3 PG 10 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 991OF UT WOS:000233822600003 ER PT J AU Vander Wal, RL Berger, GM Mozes, SD AF Vander Wal, RL Berger, GM Mozes, SD TI Droplets splashing upon films of the same fluid of various depths SO EXPERIMENTS IN FLUIDS LA English DT Article ID SOLID-SURFACE; CROWN FORMATION; SINGLE DROP; LIQUID-FILM; WATER DROPS; IMPACT; WALL; ROUGHNESS; EVOLUTION; SPRAY AB We explore the effects of fluid films of variable depths on droplets impacting into them. Corresponding to a range of fluid "film'' depths, a non-dimensional parameter-H*, defined as the ratio of the film thickness to the droplet diameter-is varied in the range 0.1 <= H* <= 10. In general, the effect of the fluid film imposes a dramatic difference on the dynamics of the droplet-surface interaction when compared to a similar impact on a dry surface. This is illustrated by the size distribution and number of the splash products. While thin fluid films (H*approximate to 0.1) promote splashing, thicker films (1 <= H* <= 10) act to inhibit it. The relative roles of surface tension and viscosity are investigated by comparison of a matrix of fluids with low and high values of these properties. Impingement conditions, as characterized by Reynolds and Weber numbers, are varied by velocity over a range from 1.34 to 4.22 m/s, maintaining a constant droplet diameter of 2.0 mm. The dependence of splashing dynamics, characterized by splash product size and number, on the fluid surface tension and viscosity and film thickness are discussed. C1 NASA Glenn, Cleveland, OH 44135 USA. RP Vander Wal, RL (reprint author), NASA Glenn, MS 110-3,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM randy@rvander.grc.nasa.gov NR 39 TC 64 Z9 65 U1 4 U2 30 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0723-4864 J9 EXP FLUIDS JI Exp. Fluids PD JAN PY 2006 VL 40 IS 1 BP 33 EP 52 DI 10.1007/s00348-005-0044-2 PG 20 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 991OF UT WOS:000233822600004 ER PT J AU Vander Wal, RL Berger, GM Mozes, SD AF Vander Wal, RL Berger, GM Mozes, SD TI The splash/non-splash boundary upon a dry surface and thin fluid film SO EXPERIMENTS IN FLUIDS LA English DT Article ID LIQUID-DROP IMPACT; SOLID-SURFACE; WATER DROPS; CROWN FORMATION; HEAT-TRANSFER; SINGLE DROP; SUBSTRATE; TENSION; DEFORMATION; COLLISION AB On the basis of empirical data, power-law boundary relations are formulated to delineate the splash and non-splash regions on dry surfaces or thin films under isothermal conditions, using the Ohnesorge and Reynolds numbers. Approximation of the relations permits cancellation of fundamental fluid physical constants to give simplified formulas which provide insight into the governing parameters describing splashing and non-splashing behaviors. Thus, for a droplet impinging upon a dry solid surface, the splash/non-splash border is well described by root Ca = 0.35. For a drop impinging upon a thin fluid film, the analytical simplification yields a boundary described by root We = 20. For both expressions, values greater than the numerical value result in splashing. C1 NASA Glenn, Cleveland, OH 44135 USA. RP Vander Wal, RL (reprint author), NASA Glenn, MS 110-3,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM randy@rvander.grc.nasa.gov NR 62 TC 51 Z9 51 U1 1 U2 27 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0723-4864 J9 EXP FLUIDS JI Exp. Fluids PD JAN PY 2006 VL 40 IS 1 BP 53 EP 59 DI 10.1007/s00348-005-0045-1 PG 7 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 991OF UT WOS:000233822600005 ER PT J AU Buckle, JV Rodgers, SD Wirstrom, ES Charnley, SB Markwick-Kemper, AJ Butner, HM Takakuwa, S AF Buckle, Jane V. Rodgers, Steven D. Wirstrom, Eva S. Charnley, Steven B. Markwick-Kemper, Andrew J. Butner, Harold M. Takakuwa, Shigehisa TI Observations of chemical differentiation in clumpy molecular clouds SO FARADAY DISCUSSIONS LA English DT Article; Proceedings Paper CT General Discussion on Chemical Evolution of the Universe CY APR 24-26, 2006 CL St Jacut, FRANCE ID MASS STAR-FORMATION; DISSOCIATIVE RECOMBINATION; DENSE CORES; DARK CLOUD; ORGANIC-MOLECULES; LINE OBSERVATIONS; CHEMISTRY; TMC-1; DEPLETION; SUBMILLIMETER AB We have extensively mapped a sample of dense molecular clouds (L1512, TMC-1C, L1262, Per7, L1389, L1251E) in lines of HC3N, CH3OH, SO and (CO)-O-18. We demonstrate that a high degree of chemical differentiation is present in all of the observed clouds. We analyse the molecular maps for each cloud, demonstrating a systematic chemical differentiation across the sample, which we relate to the evolutionary state of the cloud. We relate our observations to the cloud physical, kinematical and evolutionary properties, and also compare them to the predictions of simple chemical models. The implications of this work for understanding the origin of the clumpy structures and chemical differentiation observed in dense clouds are discussed. C1 Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. Chalmers, Onsala Space Observ, SE-43992 Onsala, Sweden. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Joint Astron Ctr, Hilo, HI 96720 USA. Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. Natl Astron Observ Japan, ALMA Off, Tokyo 1818588, Japan. RP Buckle, JV (reprint author), Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. EM j.buckle@mrao.cam.ac.uk RI Charnley, Steven/C-9538-2012; OI Butner, Harold/0000-0003-4899-2064; Wirstrom, Eva/0000-0002-0656-876X NR 70 TC 9 Z9 9 U1 1 U2 3 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PY 2006 VL 133 BP 63 EP 82 DI 10.1039/b516772h PG 20 WC Chemistry, Physical SC Chemistry GA 102BQ UT WOS:000241786200006 PM 17191443 ER PT J AU Matthews Dalgarno Smith Chakrabarti Black Rawlings Yates Viti Garcia-Burillo van Dishoeck Richards van der Loo Duley Lintott Ehrenfreund Minard Ali Herbst Fuente Plane McCoustra Rowe Ward-Thompson Al-Halabi Geppert Chakrabarti Fraser Schram Palumbo Pilling Buckle Williams Acharyya Yates Semenov AF Matthews Dalgarno Smith Chakrabarti Black Rawlings Yates Viti Garcia-Burillo van Dishoeck Richards van der Loo Duley Lintott Ehrenfreund Minard Ali Herbst Fuente Plane McCoustra Rowe Ward-Thompson Al-Halabi Geppert Chakrabarti Fraser Schram Palumbo Pilling Buckle Williams Acharyya Yates Semenov TI General discussion SO FARADAY DISCUSSIONS LA English DT Editorial Material ID DENSE INTERSTELLAR CLOUDS; UNIMOLECULAR RATE THEORY; YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; DISSOCIATIVE CHEMISORPTION; CHEMICAL EVOLUTION; LARGE HYDROCARBONS; MOLECULAR CLOUDS; CARBON CLUSTERS; LINE EMISSION C1 Ctr Space Phys, Kolkata, W Bengal, India. Leiden Univ, NL-2300 RA Leiden, Netherlands. Univ Cambridge, Cambridge CB2 1TN, England. Chalmers, S-41296 Gothenburg, Sweden. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Waterloo, Waterloo, ON N2L 3G1, Canada. Univ Amsterdam, NL-1012 WX Amsterdam, Netherlands. SN Bose Natl Ctr Basic Sci, Kolkata 700064, W Bengal, India. Leiden Univ, Leiden Inst Chem, NL-2300 RA Leiden, Netherlands. Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland. Observ Astron Nacl, Madrid, Spain. UCL, London WC1E 6BT, England. Ohio State Univ, Columbus, OH 43210 USA. Univ Stockholm, Alba Nova, S-10691 Stockholm, Sweden. Jodrell Bank Observ, Macclesfield, Cheshire, England. Penn State Univ, University Pk, PA 16802 USA. Univ Nottingham, Nottingham NG7 2RD, England. Univ Leeds, Leeds LS2 9JT, W Yorkshire, England. Univ Rennes 1, F-35014 Rennes, France. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Eindhoven Univ Technol, NL-5600 MB Eindhoven, Netherlands. Osserv Astrofis Catania, I-95125 Catania, Italy. Cardiff Univ, Cardiff, Wales. Leiden Observ, Leiden, Netherlands. Inst Theoret Chem, Nijmegen, Netherlands. NR 72 TC 0 Z9 0 U1 2 U2 5 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1359-6640 EI 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PY 2006 VL 133 BP 83 EP 102 PG 20 WC Chemistry, Physical SC Chemistry GA 102BQ UT WOS:000241786200007 ER PT J AU Owen, TC Niemann, H Atreya, S Zolotov, MY AF Owen, Tobias C. Niemann, Hasso Atreya, Sushil Zolotov, Mikhail Y. TI Between heaven and Earth: the exploration of Titan SO FARADAY DISCUSSIONS LA English DT Article; Proceedings Paper CT General Discussion on Chemical Evolution of the Universe CY APR 24-26, 2006 CL St Jacut, FRANCE ID MASS-SPECTROMETER; ATMOSPHERE; EVOLUTION; NITROGEN; COMETS; PROBE AB The atmosphere of Titan represents a bridge between the early solar nebula and atmospheres like ours. The low abundances of primordial noble gases in Titan's atmosphere relative to N-2 suggest that the icy planetesimals that formed the satellite must have originated at temperatures higher than 75 - 100 K. Under these conditions, N2 would also be very poorly trapped and thus Titan's nitrogen, like ours, must have arrived as nitrogen compounds, of which ammonia was likely the major component. This temperature constraint also argues against the trapping of methane. Production of this gas on the satellite after formation appears reasonable based on terrestrial examples of serpentinization, disproportionation and reduction of carbon. These processes require rocks, water, suitable catalysts and the variety of primordial carbon compounds that were plausibly trapped in Titan's ices. Application of this same general scenario to Ganymede, Callisto, KBOs and conditions on the very early Earth seems promising. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. RP Owen, TC (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM owen@ifa.hawaii.edu; hasso.b.niemann@nasa.gov; atreya@umich.edu; zolotov@asu.edu NR 28 TC 11 Z9 11 U1 1 U2 5 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1359-6640 EI 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PY 2006 VL 133 BP 387 EP 391 DI 10.1039/b517174a PG 5 WC Chemistry, Physical SC Chemistry GA 102BQ UT WOS:000241786200024 PM 17191458 ER PT J AU Macleod, TC Phillips, TA Ho, FD AF Macleod, T. C. Phillips, T. A. Ho, F. D. TI Characteristics of ferroelectric logic gates using a SPICE-based model SO FERROELECTRICS LA English DT Article; Proceedings Paper CT 11th IMF 2005 Conference CY SEP, 2005 CL Foz do Iguacu, BRAZIL SP IMF DE ferroelectric; logic gate; SPICE mode AB A SPICE-based model of an n-channel ferroelectric field effect transistor has been developed based on both theoretical and empirical data. This model was used to generate the I-V characteristic of several logic gates. The use of ferroelectric field effect transistors in memory circuits is being developed by several organizations. The ability of FFETs to have different characteristics depending on the initial polarization can be used to create logic gates. These gates can have properties not available to standard CMOS logic gates, such as memory, reconfigurability and memory. This paper investigates basic properties of FFET logic gates. C1 NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Alabama, Huntsville, AL 35899 USA. RP Macleod, TC (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM todd.macleod@nasa.gov NR 5 TC 1 Z9 1 U1 0 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0015-0193 J9 FERROELECTRICS JI Ferroelectrics PY 2006 VL 333 BP 165 EP 175 DI 10.1080/00150190600700717 PG 11 WC Materials Science, Multidisciplinary; Physics, Condensed Matter SC Materials Science; Physics GA 063AV UT WOS:000238989200020 ER PT J AU Phillips, TA Macleod, TC Ho, FD AF Phillips, T. A. Macleod, T. C. Ho, F. D. TI Modeling of a metal-ferroelectric-semiconductor field-effect transistor NAND gate SO FERROELECTRICS LA English DT Article; Proceedings Paper CT 11th IMF 2005 Conference CY SEP, 2005 CL Foz do Iguacu, BRAZIL SP IMF DE ferroelectric; transistor; model; NAND gate AB The modeling of a NAND gate constructed of Metal-Ferroelectric-Semiconductor Field Effect Transistors (MFSFETs) has been investigated. Initially, an inverter circuit was modeled using a n-channel MFSFET with positive polarization for a standard CMOS inverter n-channel transistor and a n-channel MFSFET with negative polarization for the standard CMOS inverter p-channel transistor. The MFSFETs were simulated by using a previously developed MFSFET model which utilized a partitioned ferroelectric layer. Then a 2-input NAND gate was modeled similar to the inverter gate. The data shows that it is feasible to construct a NAND gate with MFSFET transistors. C1 NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Alabama, Dept Elect & Comp Engn, Huntsville, AL 35899 USA. RP Macleod, TC (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM todd.macleod@nasa.gov NR 3 TC 2 Z9 2 U1 1 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0015-0193 J9 FERROELECTRICS JI Ferroelectrics PY 2006 VL 333 BP 177 EP 181 DI 10.1080/00150190600700758 PG 5 WC Materials Science, Multidisciplinary; Physics, Condensed Matter SC Materials Science; Physics GA 063AV UT WOS:000238989200021 ER PT S AU Kaestner, R Thrun, S Montemerlo, M Whalley, M AF Kaestner, Ralf Thrun, Sebastian Montemerlo, Michael Whalley, Matt BE Corke, P Sukkarieh, S TI A non-rigid approach to scan alignment and change detection using range sensor data SO FIELD AND SERVICE ROBOTICS SE Springer Tracts in Advanced Robotics LA English DT Proceedings Paper CT 5th International Conference on Field and Service Robotics CY JUL 29-31, 2005 CL Port Douglas, AUSTRALIA SP CSIRO ICT, Australian Robot & Automat Assoc ID REGISTRATION; IMAGES AB We present a probabilistic technique for alignment and subsequent change detection using range sensor data. The alignment method is derived from a novel, non-rigid approach to register point clouds induced by pose-related range observations that are particularly erroneous. It allows for high scan estimation errors to be compensated distinctly, whilst considering temporally successive measurements to be correlated. Based on the alignment, changes between data sets are detected using a probabilistic approach that is capable of differentiating between likely and unlikely changes. When applied to observations containing even small differences, it reliably identifies intentionally introduced modifications. C1 [Kaestner, Ralf; Thrun, Sebastian; Montemerlo, Michael] Stanford Univ, Dept Comp Sci, Robot Lab, Stanford, CA 94305 USA. [Whalley, Matt] Army NASA Rotorcraft Div, AMRDEC, Ames, IA USA. [Whalley, Matt] Ames Res Ctr, US Army Res, Dev & Engn Command, Ames, IA USA. RP Kaestner, R (reprint author), Stanford Univ, Dept Comp Sci, Robot Lab, Stanford, CA 94305 USA. EM ralfk@cs.stanford.edu; thrun@stanford.edu; mmde@stanford.edu; mwhalley@mail.arc.nasa.gov NR 15 TC 6 Z9 6 U1 1 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 1610-7438 BN 3-540-33452-1 J9 SPRINGER TRAC ADV RO PY 2006 VL 25 BP 179 EP + PG 3 WC Robotics SC Robotics GA BFE25 UT WOS:000241438000016 ER PT S AU Diaz-Calderon, A Kelly, A AF Diaz-Calderon, Antonio Kelly, Alonzo BE Yuta, S Asama, H Thrun, S Prassler, E Tsubouchi, T TI Development of a terrain adaptive stability prediction system for mass articulating mobile robots SO FIELD AND SERVICE ROBOTICS: RECENT ADVANCES IN RESEARCH AND APPLICATIONS SE Springer Tracts in Advanced Robotics LA English DT Proceedings Paper CT 4th International Conference on Field and Service Robotics CY JUL 14-16, 2003 CL Mt Fuji, JAPAN AB Dynamic stability is an important issue for vehicles which move heavy loads, turn at speed, or operate on sloped terrain. In many cases, vehicles face more than one of these challenges simultaneously. This paper presents a methodology for deriving proximity to tipover for autonomous field robots, which must be productive, effective, and self reliant under such challenging circumstances. The technique is based on explicit modeling of mass articulations and determining the motion of the center of gravity, as well as the attitude, in an optimal estimation framework. Inertial sensing, articulation sensing, and terrain relative motion sensing are employed. The implementation of the approach on a commercial industrial lift truck is presented. C1 [Diaz-Calderon, Antonio] CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. [Kelly, Alonzo] Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. RP Diaz-Calderon, A (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. EM adiaz@jpl.nasa.gov; alonzo@ri.cmu.edu NR 11 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 1610-7438 BN 3-540-32801-7 J9 SPRINGER TRAC ADV RO PY 2006 VL 24 BP 343 EP + PG 2 WC Robotics SC Robotics GA BEV78 UT WOS:000239653600033 ER PT J AU Schirripa, MJ Colbert, JJ AF Schirripa, MJ Colbert, JJ TI Interannual changes in sablefish (Anoplopoma fimbria) recruitment in relation to oceanographic conditions within the California Current System SO FISHERIES OCEANOGRAPHY LA English DT Article DE environment; oceanographic variables; recruitment; sablefish ID EARLY-LIFE-HISTORY; OREGON; ZOOPLANKTON; MANAGEMENT; COAST; WASHINGTON; FECUNDITY; GROWTH; WATERS; OCEAN AB Sablefish (Anoplopoma fimbria) Supports substantial fisheries in both the eastern and western Pacific Oceans. juvenile recruitment along the west coast of the continental United States has been highly variable over the past three decades. Using a generalized additive model, we demonstrate that physical oceanographic variables within the California Current System have significant effects on sablefish recruitment. Significant relationships were found between juvenile recruitment and northward Ekman transport, eastward Ekman transport, and sea level during key times and at key locations within the habitat of this species. The model explains nearly 70% of the variability in sablefish recruitment between the years 1974 and 2000. The predictive power of the model was demonstrated by refitting without the last 5 yr of data and subsequent prediction of those years. Bootstrap assessments of bias associated with parameter estimates and jackknife-after-bootstrap assessments of the influence of individual data on parameter estimates are presented and discussed. Using this model, it is possible to draw preliminary Conclusions concerning year-class strength of cohorts not yet available to the Survey gear as well as historic year-class strengths. We discuss changes in zooplankton abundance and shifts in species of copepods associated With fluctuations in the physical variables that appear to have a major influence on sablefish recruitment. C1 Hatfield Marine Sci Ctr, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Newport, OR 97365 USA. Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. RP Schirripa, MJ (reprint author), Hatfield Marine Sci Ctr, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, 2032 S OSU Dr, Newport, OR 97365 USA. EM michael.schirripa@noaa.gov RI Bizzarro, Joseph/A-2988-2012 NR 33 TC 29 Z9 30 U1 1 U2 10 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 1054-6006 J9 FISH OCEANOGR JI Fish Oceanogr. PD JAN PY 2006 VL 15 IS 1 BP 25 EP 36 DI 10.1111/j.1365-2419.2005.00352.x PG 12 WC Fisheries; Oceanography SC Fisheries; Oceanography GA 014YY UT WOS:000235520300002 ER PT J AU Busby, MS Mier, KL Brodeur, RD AF Busby, MS Mier, KL Brodeur, RD TI Habitat associations of demersal fishes and crabs in the Pribilof Islands region of the Bering Sea (vol 75, pg 15, 2005) SO FISHERIES RESEARCH LA English DT Correction C1 Natl Marine Fisheries Serv, NOAA, Alaska Fisheries Sci Ctr, Resource Assessment & Conservat Engn Div, Seattle, WA 98115 USA. Natl Marine Fisheries Serv, NOAA, NW Fisheries Sci Ctr, Estuarine & Ocean Ecol Program,Hatfield Marine Sc, Newport, OR 97365 USA. RP Busby, MS (reprint author), Natl Marine Fisheries Serv, NOAA, Alaska Fisheries Sci Ctr, Resource Assessment & Conservat Engn Div, 7600 Sand Point Way NE,Bldg 4, Seattle, WA 98115 USA. EM morgan.busby@noaa.gov NR 1 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 J9 FISH RES JI Fish Res. PD JAN PY 2006 VL 77 IS 1 BP 122 EP 123 DI 10.1016/j.fishres.2005.11.001 PG 2 WC Fisheries SC Fisheries GA 004QQ UT WOS:000234767700017 ER PT S AU Maluf, D Bell, D Ashish, N Putz, P Gawdiak, Y AF Maluf, David Bell, David Ashish, Naveen Putz, Peter Gawdiak, Yuri BE Esposito, F Ras, ZW Malerba, D Semeraro, G TI Business intelligence in large organizations: Integrating which data? SO FOUNDATIONS OF INTELLIGENT SYSTEMS, PROCEEDINGS SE LECTURE NOTES IN ARTIFICIAL INTELLIGENCE LA English DT Article; Proceedings Paper CT 16th International Symposium on Methodologies for Intelligent Systems CY SEP 27-29, 2006 CL Bari, ITALY SP Univ Bari, Dept Comp Sci, Univ Studi Bari, Dipartimento Informat AB This paper describes a novel approach to business intelligence and program management for large technology enterprises like the U.S. National Aeronautics and Space Administration (NASA). Two key distinctions of the approach are that 1) standard business documents are the user interface, and 2) a "schema-less" XML1 database enables flexible integration of technology information for use by both humans and machines in a highly dynamic environment. The implementation utilizes patent-pending NASA software called the NASA Program Management Tool (PMT) and its underlying "schema-less" XML database called Netmark. Initial benefits of PMT include elimination of discrepancies between business documents that use the same information and "paperwork reduction" for program and project management in the form of reducing the effort required to understand standard reporting requirements and to comply with those reporting requirements. We project that the underlying approach to business intelligence will enable significant benefits in the timeliness, integrity and depth of business information available to decision makers on all organizational levels. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Space Res Assoc, NASA Headquarters, Washington, DC 20546 USA. Univ Calif Irvine, Irvine, CA 92697 USA. RP Maluf, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM David.A.Maluf@nasa.gov; ashish@ics.uci.edu; Yuri.O.Gawdiak@nasa.gov NR 3 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-45764-X J9 LECT NOTES ARTIF INT PY 2006 VL 4203 BP 248 EP 257 PG 10 WC Computer Science, Artificial Intelligence SC Computer Science GA BFF98 UT WOS:000241647800028 ER PT S AU Biswas, A Boroson, D Edwards, B AF Biswas, A. Boroson, D. Edwards, B. BE Mecherle, GS TI Mars laser communication demonstration: What it would have been - art. no. 610502 SO Free-Space Laser Communication Technologies XVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Free-Space Laser Communication Technologies XVIII CY JAN 24-25, 2006 CL San Jose, CA DE laser communications; Mars ID OPTICAL RECEIVER; HALE TELESCOPE; SYSTEM AB The Mars Laser Communications Demonstration Project completed a preliminary system design for sending data at 1-30 Mbps from a spacecraft orbiting Mars. The flight transceiver diameter was 30.6 cm, transmitting 5 W average laser power at 1064 nm and using 32- and 64-ary pulse position modulation (PPM). A ground network comprised of two receive terminals (5-m and 1.6-m effective diameter) and two transmit terminals for sending 1076 rim lasers would have been used to communicate with the transceiver. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Biswas, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 23 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6147-4 J9 P SOC PHOTO-OPT INS PY 2006 VL 6105 BP 10502 EP 10502 AR 610502 DI 10.1117/12.669551 PG 12 WC Optics; Telecommunications SC Optics; Telecommunications GA BEF93 UT WOS:000237168400001 ER PT S AU Chen, CC Hemmati, H Biswas, A Ortiz, G Farr, W Pedreiro, N AF Chen, Chien-Chung Hemmati, Hamid Biswas, Abhijit Ortiz, Gerardo Farr, William Pedreiro, Nelson BE Mecherle, GS TI Simplified lasercom system architecture using a disturbance-free platform - art. no. 610505 SO Free-Space Laser Communication Technologies XVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Free-Space Laser Communication Technologies XVIII CY JAN 24-25, 2006 CL San Jose, CA DE laser communications; deep-space AB A simplified laser communications (lasercom) system architecture, primarily for a deep-space flight transceivers, can be realized by decoupling the lasercom optical components from the host spacecraft using a disturbance-free platform (DFP) developed by Lockheed Martin Space System Company. Unlike conventional lasercom system architectures where a high bandwidth control loop is used to stabilize the optical line-of-sight in the presence of platform disturbance, the DFP package isolates the optical train from the high frequency platform jitter produced by the host. By preventing the vibration from coupling into the optics train, the need for a high bandwidth beam stabilization control loop (including fast steering mirror, detectors, controls and the associated relay optics) is eliminated with possible mass savings. Effective isolation of the platform jitter also enables the optical focal plane array to operate at a much longer integration time, thus enabling the use of either faint stars or a weak beacon as a pointing reference. This feature can allow the same lasercorn system architecture to be employed for deep space and some near Earth applications, and can potentially enable deep space return signal pointing without the need of an uplink beacon. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chen, CC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 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 0-8194-6147-4 J9 P SOC PHOTO-OPT INS PY 2006 VL 6105 BP 10505 EP 10505 AR 610505 DI 10.1117/12.660264 PG 6 WC Optics; Telecommunications SC Optics; Telecommunications GA BEF93 UT WOS:000237168400004 ER PT S AU Vilnrotter, V Lau, CW Andrews, K Vo, P Srinivasan, M Lee, D AF Vilnrotter, V. Lau, C. -W. Andrews, K. Vo, P. Srinivasan, M. Lee, D. BE Mecherle, GS TI Real-time combining of optical array signals - art. no. 610508 SO Free-Space Laser Communication Technologies XVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Free-Space Laser Communication Technologies XVIII CY JAN 24-25, 2006 CL San Jose, CA AB The results of field experiments designed to demonstrate key enabling concepts of optical array receivers are presented, in a field environment similar to actual operating conditions. The theoretical framework and analytical evaluation of optical array receivers have been developed and documented in previous articles. This article describes the implementation and field evaluation of a two-element optical array receiver incorporating photon-counting, signal conditioning, high-speed digital sample distribution, adaptive delay compensation and sample combining operations required for array reception of intensity-modulated optical pulse-position modulated (PPM) signals. Data collected in the field was processed offline to determine communications performance of a two-element optical array, and demonstrate the inherent advantages of optical array reception. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vilnrotter, V (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 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 0-8194-6147-4 J9 P SOC PHOTO-OPT INS PY 2006 VL 6105 BP 10508 EP 10508 AR 610508 DI 10.1117/12.660266 PG 11 WC Optics; Telecommunications SC Optics; Telecommunications GA BEF93 UT WOS:000237168400006 ER PT S AU Ortiz, GG Lee, S AF Ortiz, Gerardo G. Lee, Shinhak BE Mecherle, GS TI Star tracker based ATP system conceptual design and ointing accuracy estimation - art. no. 61050D SO Free-Space Laser Communication Technologies XVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Free-Space Laser Communication Technologies XVIII CY JAN 24-25, 2006 CL San Jose, CA DE acquisition; tracking; and pointing system; deep-space optical communications; star tracker AB A star tracker based beaconless (a.k.a. non-cooperative beacon) acquisition, tracking and pointing concept for precisely pointing an optical communication beam is presented as an innovative approach to extend the range of high bandwidth (> 100 Mbps) deep space optical communication links throughout the solar system and to remove the need for a ground based high power laser as a beacon source. The basic approach for executing the ATP functions involves the use of stars as the reference sources from which the attitude knowledge is obtained and combined with high bandwidth gyroscopes for propagating the pointing knowledge to the beam pointing mechanism. Details of the conceptual design are presented including selection of an orthogonal telescope configuration and the introduction of an optical metering scheme to reduce misalignment error. Also, estimates are presented that demonstrate that aiming of the communications beam to the Earth based receive terminal can be achieved with a total system pointing accuracy of better than 850 nanoradians (3 sigma) from anywhere in the solar system. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ortiz, GG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 10 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 0-8194-6147-4 J9 P SOC PHOTO-OPT INS PY 2006 VL 6105 BP D1050 EP D1050 AR 61050D DI 10.1117/12.660263 PG 10 WC Optics; Telecommunications SC Optics; Telecommunications GA BEF93 UT WOS:000237168400011 ER PT S AU Chen, Y Ortiz, GG Hemmati, H Lee, S AF Chen, Y. Ortiz, G. G. Hemmati, H. Lee, S. BE Mecherle, GS TI Centroiding accuracy of infrared Earth images mitigating impact of blurring and Earth non-uniformity - art. no. 61050E SO Free-Space Laser Communication Technologies XVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Free-Space Laser Communication Technologies XVIII CY JAN 24-25, 2006 CL San Jose, CA DE free space optical communications; Earth tracking; centroiding accuracy; deconvolution algorithm AB Infrared (IR) Earth thermal image tracking has potential to enable optical communications throughout the solar system and is a promising alternative to traditionally proposed laser beacon tracking. Image blurring due to finite receiver aperture size introduces distortions to IR Earth image in the presence of Earth's non-uniform ernissivity and reduces the centroiding accuracy in identifying the center of the Earth. The impact is largest in the 0.5 to 2 AU range. We demonstrate that a deconvolution algorithm can mitigate the effect of blurring associated with IR Earth non-uniformity and improve centroiding edge detection accuracy. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chen, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. 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 0-8194-6147-4 J9 P SOC PHOTO-OPT INS PY 2006 VL 6105 BP E1050 EP E1050 AR 61050E DI 10.1117/12.660269 PG 9 WC Optics; Telecommunications SC Optics; Telecommunications GA BEF93 UT WOS:000237168400012 ER PT S AU Roberts, WT Ortiz, GG Boyd, TA AF Roberts, W. Thomas Ortiz, Gerardo G. Boyd, Timothy A. BE Mecherle, GS TI Daytime use of astronomical telescopes for deep-space optical links - art. no. 61050G SO Free-Space Laser Communication Technologies XVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Free-Space Laser Communication Technologies XVIII CY JAN 24-25, 2006 CL San Jose, CA AB Tests at the 200-inch Hale Telescope on Palomar Mountain have demonstrated this telescope's ability to withstand considerable thermal stress, and subsequently produce remarkably unaffected results. During the day of June 29, 2005, the Hale telescope dome was left open, and the telescope was exposed to outside air and direct sunlight for 8 hours. During this time, portions of the telescope structure in the telescope's optical path experienced temperature elevations of 30 C, while the primary mirror experienced unprecedented heating of over 3 C. The telescope's measured blind pointing accuracy after this exposure was not noticeably degraded from the measurements taken before exposure. More remarkably, the telescope consistently produced stellar images which were significantly better after exposure of the telescope (1.2 arcsec) than before (1.6 arcsec), even though the conditions of observation were similar. This data is the first step in co-opting astronomical telescopes for daytime use as astronomical receivers, and supports the contention that deleterious effects from daytime exposure of the telescope can be held to an acceptable level for interleaved communications and astronomy. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Roberts, WT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 2 Z9 2 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 0-8194-6147-4 J9 P SOC PHOTO-OPT INS PY 2006 VL 6105 BP G1050 EP G1050 AR 61050G DI 10.1117/12.660256 PG 10 WC Optics; Telecommunications SC Optics; Telecommunications GA BEF93 UT WOS:000237168400013 ER PT S AU Lau, CW Vilnrotter, VA Dolinar, S Geremia, JM Mabuchi, H AF Lau, Chi-Wung Vilnrotter, Victor A. Dolinar, Sam Geremia, J. M. Mabuchi, Hideo BE Mecherle, GS TI Binary quantum receiver concept demonstration - art. no. 61050J SO Free-Space Laser Communication Technologies XVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Free-Space Laser Communication Technologies XVIII CY JAN 24-25, 2006 CL San Jose, CA DE quantum detection; Kennedy receiver; Dolinar receiver; quantum communications AB An experimental demonstration of a quantum-optimal receiver for optical binary signals, developed as a joint effort by the Jet Propulsion Laboratory and the California Institute if Technology, is described in this article. A brief summary of the classical, quantum-optimal, and quantum near optimal solutions to detecting binary signals is first presented. The components and experimental setup used to implement the receivers is then discussed. Experimental performance and results for both optimal and near-optimal receivers are presented and compared to theoretical limits. Finally, experimental shortcomings are discussed along with possible solutions and future direction. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lau, CW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 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 0-8194-6147-4 J9 P SOC PHOTO-OPT INS PY 2006 VL 6105 BP J1050 EP J1050 AR 61050J DI 10.1117/12.660268 PG 7 WC Optics; Telecommunications SC Optics; Telecommunications GA BEF93 UT WOS:000237168400016 ER PT S AU Hemmati, H Chen, YJ Crossfield, I AF Hemmati, Hamid Chen, Yijiang Crossfield, Ian BE Mecherle, GS TI Telescope wavefront aberration compensation witb a deformable mirror in an adaptive optics system - art. no. 61050O SO Free-Space Laser Communication Technologies XVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Free-Space Laser Communication Technologies XVIII CY JAN 24-25, 2006 CL San Jose, CA DE laser communications; active optics AB With the goal of reducing the surface wavefront error of low-cost multi-meter-diameter mirrors from about 10 waves peak-to-valley (P-V), at I pm wavelength, to approximately 1-wave or less, we describe a method to compensate for slowly varying wavefront aberrations of telescope mirrors. A deformable mirror is utilized in an active optical compensation system. The RMS wavefront error of a 0.3m telescope improved to 0.05 waves (0.26 waves P-V) from the original value of 1.4 waves RMS (6.5 waves P-V), measured at 633nm, and the Strehl ratio improved to 89% from the original value of 0.08%. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 13 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 0-8194-6147-4 J9 P SOC PHOTO-OPT INS PY 2006 VL 6105 BP O1050 EP O1050 AR 61050O DI 10.1117/12.660262 PG 4 WC Optics; Telecommunications SC Optics; Telecommunications GA BEF93 UT WOS:000237168400020 ER PT S AU Hemmati, H AF Hemmati, Hamid BE Majumdar, AK Davis, CC TI Low-cost large aperture telescopes for optical communications SO Free-Space Laser Communications VI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Free-Space Laser Communications VI CY AUG 15-17, 2006 CL San Diego, CA SP SPIE DE laser communications; telescope ID RECEIVER AB Low-cost, large-aperture optical receivers are required to form an affordable optical ground receiver network for laser communications. Among the ground receiver station's multiple subsystems, here, we only discuss the ongoing research activities aimed at reducing the cost of the large-size optics on the receiver. Experimental results of two different approaches for fabricating low-cost mirrors of wavefront quality on the order of 100-200X the diffraction limit are described. Laboratory-level effort are underway to improve the surface figure to better than 20X the diffraction limit. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hemmati, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 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 0-8194-6383-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6304 BP U188 EP U192 DI 10.1117/12.682684 PG 5 WC Instruments & Instrumentation; Optics; Telecommunications SC Instruments & Instrumentation; Optics; Telecommunications GA BFI04 UT WOS:000241946400018 ER PT J AU McDonough, KH Virag, JI AF McDonough, KH Virag, JI TI Sepsis-induced myocardial dysfunction and myocardial protection from ischemia/reperfusion injury SO FRONTIERS IN BIOSCIENCE LA English DT Article DE sepsis; infection; heart; cardiovascular; physiology; myocardium; ischemia; reperfusion injury; preconditioning; review ID ISCHEMIA-REPERFUSION INJURY; BETA-ADRENERGIC STIMULATION; SHOCKED GUINEA-PIGS; ISOLATED RAT HEARTS; SEPTIC SHOCK; NITRIC-OXIDE; CONTRACTILE DYSFUNCTION; HYPERMETABOLIC SEPSIS; PKC-EPSILON; LATE-PHASE AB Sepsis, bacteremia and inflammation cause myocardial depression. The mechanism of the dysfunction is not clearly established partly because dysfunction can be elicited by many different mechanisms which can all manifest in disruption of myocardial mechanical function. In addition the models of sepsis and bacteremia and inflammation may vary drastically in the sequence of the coordinated immune response to the inflammatory or septic stimulus. Patterns of cytokine expression can vary as can other responses of the immune system. Patterns of neurohumoral activation in response to the stress of sepsis or bacteremia or inflammation can also vary in both magnitude of response and temporal sequence of response. Stress induced activation of the sympathetic nervous system and humoral responses to stress have a wide range of intensity that can be elicited. The fairly uniform response of the myocardium indicating cardiac dysfunction is surprisingly constant. Systolic performance, as measured by stroke volume or cardiac output and pressure work as estimated by ventricular pressure, are impaired when myocardial contraction is compromised. At times, diastolic function, assessed by ventricular relaxation and filling, is impaired. In addition to the dysfunction that occurs, there is a longer term response of the myocardium to sepsis, and this response is similar to that which is elicited in the heart by multiple brief ischemia/ reperfusion episodes and by numerous pharmacological agents as well as heat stress and modified forms of lipopolysaccharide. The myocardium develops protection after an initial stress such that during a second stress, the myocardium does not exhibit as much damage as does a non- protected heart. Many agents can induce this protection which has been termed preconditioning. Both early preconditioning ( protection that is measurable min to hours after the initial stimulus) and late preconditioning ( protection that is measurable hours to days after the initial trigger or stimulus) are effective in protecting the heart from prolonged ischemia and reperfusion injury. Understanding the mechanisms of sepsis/ bacteremia induced dysfunction and protection and if the dysfunction and protection are the products of the same intracellular pathways is important in protecting the heart from failing to perform adequately during severe sepsis and/ or septic shock and for understanding the multitude of mechanism by which the myocardium maintains reserve capacity. C1 Louisiana State Univ, Hlth Sci Ctr, Dept Physiol, New Orleans, LA 70112 USA. Univ Space Res Assoc, NASA, Johnson Space Ctr Cardiovasc Lab, Div Space Life Sci, Houston, TX 77058 USA. RP McDonough, KH (reprint author), Louisiana State Univ, Hlth Sci Ctr, Dept Physiol, 1901 Perdido St, New Orleans, LA 70112 USA. EM kmcdon@lsuhsc.edu RI Virag, Jitka/B-3387-2017 OI Virag, Jitka/0000-0003-3321-9861 NR 67 TC 7 Z9 8 U1 1 U2 5 PU FRONTIERS IN BIOSCIENCE INC PI MANHASSET PA C/O NORTH SHORE UNIV HOSPITAL, BIOMEDICAL RESEARCH CENTER, 350 COMMUNITY DR, MANHASSET, NY 11030 USA SN 1093-9946 J9 FRONT BIOSCI JI Front. Biosci. PD JAN 1 PY 2006 VL 11 BP 23 EP 32 DI 10.2741/1777 PG 10 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 973MX UT WOS:000232528000003 PM 16146711 ER PT B AU Abedin, MN Refaat, TF Sulima, OV Singh, UN AF Abedin, M. Nurul Refaat, Tamer F. Sulima, Oleg V. Singh, Upendra N. BE Iwai, H Nishi, Y Shur, MS Wong, H TI Recent development of Sb-based phototransistors in the 0.9- to 2.2-mu m wavelength range for applications to laser remote sensing SO Frontiers in Electronics SE SELECTED TOPICS IN ELECTRONICS AND SYSTEMS LA English DT Proceedings Paper CT Workshop on Frontiers in Electronics (WOFE-04) CY DEC 17-23, 2004 CL Aruba, NETHERLANDS SP IEEE EDS, IEEE Sensors Council ID MIDINFRARED WAVELENGTHS; INASSBP PHOTODETECTORS; ALGAASSB/INGAASSB PHOTOTRANSISTORS; AVALANCHE PHOTODETECTORS; GAINASSB; MULTIPLICATION AB We have investigated commercially available photodiodes and also recent developed Sb-based phototransistors in order to compare their performances for applications to laser remote sensing. A custom-designed phototransistor in the 0.9- to 2.2-mu m wavelength range has been developed at AstroPower and characterized at NASA Langley's Detector Characterization Laboratory. The phototransistor's performance greatly exceeds the previously reported results at this wavelength range in the literature. The detector testing included spectral response, dark current and noise measurements. Spectral response measurements were carried out to determine the responsivity at 2-mu m wavelength at different bias voltages with fixed temperature; and different temperatures with fixed bias voltage. Current versus voltage characteristics were also recorded at different temperatures. Results show high responsivity of 2650 A/W corresponding to an internal gain of three orders of magnitude, and high detectivity (D*) of 3.9x10(11) cm.Hz(1/2)/W that is equivalent to a noise-equivalent-power of 4.6 x 10(-14) W/Hz(1/2) (40 V @ -20 degrees C) with a light collecting area diameter of 200-mu m. It appears that this recently developed 2-mu m phototransistor's performances such as responsivity, detectivity, and gain are improved significantly as compared to the previously published APD and SAM APD using similar materials. These detectors are considered as phototransistors based-on their structures and performance characteristics and may have great potential for high sensitivity differential absorption lidar (DIAL) measurements of carbon dioxide and water vapor at 2.05-mu m and 1.9-mu m respectively. C1 NASA, Langley Res Ctr, Passive Sensor Syst Branch, Hampton, VA 23681 USA. RP Abedin, MN (reprint author), NASA, Langley Res Ctr, Passive Sensor Syst Branch, MS 468,5 N Dryden St, Hampton, VA 23681 USA. NR 34 TC 0 Z9 0 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 981-256-884-0 J9 SEL TOP ELECTR SYST PY 2006 VL 41 BP 567 EP 582 DI 10.1142/9789812773081_0035 PG 16 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology SC Engineering; Science & Technology - Other Topics GA BFC82 UT WOS:000241022300035 ER PT J AU Abdel-Fattah, T Siochi, EJ Crooks, RE AF Abdel-Fattah, Tarek Siochi, Emilie J. Crooks, Roy E. TI Pyrolytic synthesis of carbon nanotubes from sucrose on a mesoporous silicate SO FULLERENES NANOTUBES AND CARBON NANOSTRUCTURES LA English DT Article DE pyrolytic synthesis; multi-wall carbon nanotubes; mesopourous; templates ID MOLECULAR-SIEVES; SINGLE; CHANNELS; CRYSTAL; RAMAN AB Multi-wall carbon nanotubes were synthesized from sucrose by a pyrolytic technique using mesopourous MCM-41 silicate templates without transition metal catalysts. The nanotubes were examined in the carbon/silicate composite and after dissolution of the silicate. High-resolution transmission electron microscopy study of the multi-wall nanotubes showed them to be 15 nm in diameter, 200 nm in length and close-ended. There was variation in crystallinity with some nanotubes showing disordered wall structures. C1 Christopher Newport Univ, Dept Chem Bio & Environm Sci, Newport News, VA 23606 USA. NASA, Adv Mat & Proc Branch, Hampton, VA USA. Natl Inst Aerosp, Hampton, VA USA. RP Abdel-Fattah, T (reprint author), Christopher Newport Univ, Dept Chem Bio & Environm Sci, Newport News, VA 23606 USA. EM fattah@cnu.edu NR 30 TC 24 Z9 24 U1 1 U2 10 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1536-383X J9 FULLER NANOTUB CAR N JI Fuller. Nanotub. Carbon Nanostruct. PY 2006 VL 14 IS 4 BP 585 EP 594 DI 10.1080/15363830600811995 PG 10 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Atomic, Molecular & Chemical SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 107YR UT WOS:000242207400001 ER PT S AU Reeves, JN Watson, D Vaughan, S Osborne, J O'Brien, PT Levan, A Willingale, R AF Reeves, J. N. Watson, D. Vaughan, S. Osborne, J. O'Brien, P. T. Levan, A. Willingale, R. BE Gehrels, N Courvoisier, TJL Wilkes, B Diehl, R Williams, DR TI XMM-Newton observation of a dust echo and X-ray flash in GRB 031203 SO GALACTIC AND EXTRAGALACTIC ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE XMM-Newton observations; gamma-ray bursts; X-ray afterglows; dust scattering ID LOW-LUMINOSITY; BURST AB We present XMM-Newton observations of the X-ray afterglow of GRB 031203, approximately 6 It after the initial burst detection by Integral. At z = 0.105, GRB 031203 is one of the least luminous gamma-ray bursts, with an equivalent isotropic gamma-ray energy of similar to 3 x 10(49) ergs. The XMM-Newton images reveal an expanding X-ray halo around GRB 031203, in the form of two concentric rings centred on the afterglow position. The rings expand radially outwards with time as t(0.5), consistent with small angle scattering of burst X-rays off dust in our own galaxy. The total X-ray fluence derived from the dust echo of 2 x 10(-6) ergs cm(-2) keV(-1) (at 1 keV) implies that a strong X-ray flash is likely to have occurred from GRB 031203. The estimate of the X-ray fluence is robust to the determination of the total dust extinction in the scatterer. However the classification of GRB 031203 as an X-ray Flash appears at odds with the prompt (20-400 keV) Integral emission from this burst, which has a hard photon index of Gamma = 1.6 and a peak energy of > 190 keV. Thus either GRB 031203 is highly unusual and has a double peaked spectral energy distribution, or a second flash occurred later in soft X-rays, at least equal in total energy to that of the initial gamma-ray burst. (c) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Reeves, JN (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. EM jnr@milkyway.gsfc.nasa.gov RI Watson, Darach/E-4521-2015 OI Watson, Darach/0000-0002-4465-8264 NR 9 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 7 BP 1287 EP 1290 DI 10.1016/j.asr.2005.01.050 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW01 UT WOS:000245034500003 ER PT S AU Nishikawa, KI Hardee, P Hededal, CB Richardson, G Preece, R Sol, H Fishman, GJ AF Nishikawa, K-, I Hardee, P. Hededal, C. B. Richardson, G. Preece, R. Sol, H. Fishman, G. J. BE Gehrels, N Courvoisier, TJL Wilkes, B Diehl, R Williams, DR TI Particle acceleration, magnetic field generation, and emission in relativistic shocks SO GALACTIC AND EXTRAGALACTIC ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE relativistic shocks; Weibel instability; particle acceleration; magnetic field generation; radiation ID PLASMA AB Shock acceleration is a ubiquitous phenomenon in astrophysical plasmas. Plasma waves and their associated instabilities (e.g., Buneman, Weibel and other two-stream instabilities) created in collisionless shocks are responsible for particle (electron, positron, and ion) acceleration. Using a 3D relativistic electromagnetic particle code, we have investigated particle acceleration associated with a relativistic jet front propagating into an ambient plasma. We find small differences in the results for no ambient and modest ambient magnetic fields. Simulations show that the Weibel instability created in the collisionless shock front accelerates jet and ambient particles both perpendicular and parallel to the jet propagation direction. The small scale magnetic field structure generated by the Weibel instability is appropriate to the generation of "jitter" radiation from defected electrons (positrons) as opposed to synchrotron radiation. The jitter radiation resulting from small scale magnetic field structures may be important for understanding the complex time structure and spectral evolution observed in gamma-ray bursts or other astrophysical sources containing relativistic jets and relativistic collisionless shocks. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Nishikawa, K-, I; Preece, R.] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. [Hardee, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Hededal, C. B.] Niels Bohr Inst, Dept Astrophys, DK-2100 Copenhagen, Denmark. [Hededal, C. B.] Univ Alabama, Dept Mech & Aerosp Engn, Huntsville, AL 35899 USA. [Preece, R.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Sol, H.] Observ Paris, LUTH, F-92195 Meudon, France. [Fishman, G. J.] NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. RP Nishikawa, KI (reprint author), Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. EM Ken-ichi.nishikawa@nsstc.nasa.gov RI Gehrels, Neil/D-2971-2012; OI Preece, Robert/0000-0003-1626-7335 FU National Science Foundation [ATM-0100997, INT-9981508]; National Space Science and Technology (NSSTC/NASA) FX K. Nishikawa is a NRC Senior Research Fellow at NASA Marshall Space Flight Center. This research (K.N.) is partially supported by the National Science Foundation awards ATM-0100997, and INT-9981508. P. Hardee acknowledges partial support by a National Space Science and Technology (NSSTC/NASA) award. The simulations have been performed on ORIGIN 2000 and IBM p690 (Copper) at the National Center for Super-computing Applications (NCSA) which is supported by the National Science Foundation. NR 11 TC 3 Z9 3 U1 1 U2 1 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 7 BP 1316 EP + DI 10.1016/j.asr.2005.01.036 PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW01 UT WOS:000245034500010 ER PT S AU Sylwester, J Sylwester, B Phillips, KJH Culhane, JL Brown, C Lang, J Stepanov, AI AF Sylwester, J. Sylwester, B. Phillips, K. J. H. Culhane, J. L. Brown, C. Lang, J. Stepanov, A. I. BE Gehrels, N Courvoisier, TJL Wilkes, B Diehl, R Williams, DR TI Analysis of potassium abundance in a large number of flares SO GALACTIC AND EXTRAGALACTIC ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE sun; X-ray; spectra; abundance; potassium ID SOLAR; LINES; ARGON; RESIK AB An initial study of spectra observed in the shortest wavelength channel (3.40-3.80 angstrom) of the RESIK X-ray spectrometer on CORONA S-F indicates the presence of substantial flare-to-flare variations in the line-to-continuum ratio of several lines, in particular He-like potassium (K XVIII) lines, occurring in the range 3.53-3.57 angstrom The observed variations are larger than those expected from temperature variations. This has motivated a study of possible variations in the potassium abundance in the observed spectra. With a new RESIK calibration available, we have obtained absolute fluxes of the K XVIII resonance line as well as the continuum and lines observed in other RESIK channels (3.40-6.05 angstrom) for some 1163 intervals observed early in 2003. Analysis of these observations allowed us to determine the average absolute potassium abundance for the period studied and investigate the variability of abundance. The results obtained are presented and discussed. (c) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 [Sylwester, J.; Sylwester, B.] Polish Acad Sci, Space Res Ctr, Kopernika 11, PL-51622 Wroclaw, Poland. [Phillips, K. J. H.] NASA, Goddard Space Flight Ctr, Natl Res Council Senior Res Assoc, Greenbelt, MD 20771 USA. [Culhane, J. L.] Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Brown, C.] EO Hulburt Ctr Space Res, Naval Res Lab, Washington, DC 20375 USA. [Lang, J.] Rutherford Appleton Lab, Dept Space Sci, Didcot OX11 0QX, Oxon, England. [Stepanov, A. I.] Russian Acad Sci, IZMIRAN, R-142190 Troitsk, Russia. RP Sylwester, J (reprint author), Polish Acad Sci, Space Res Ctr, Kopernika 11, PL-51622 Wroclaw, Poland. EM js@cbk.pan.wroc.pl RI Gehrels, Neil/D-2971-2012 FU Polish Committee for Scientific Research [2.P03D.002.22, BPZ-KBN-054/P03/2001]; US National Research Council Research FX B.S. and J.S. acknowledge support from Grants 2.P03D.002.22 and BPZ-KBN-054/P03/2001 of the Polish Committee for Scientific Research. K.J.H.P. acknowledges support from the US National Research Council Research Associateship Program. NR 8 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 7 BP 1490 EP + DI 10.1016/j.asr.2005.08.026 PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW01 UT WOS:000245034500045 ER PT S AU Reed, D Church, MJ Dotani, T Balucinska-Church, M Smale, AP AF Reed, D. Church, M. J. Dotani, T. Balucinska-Church, M. Smale, A. P. BE Gehrels, N Courvoisier, TJL Wilkes, B Diehl, R Williams, DR TI Discovery of ADC absorption in the LMXB XB 1323-619 with XMM-Newton SO GALACTIC AND EXTRAGALACTIC ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE accretion discs; close binaries; X-ray binaries; Neutron stars; XB 1323-619 ID ACCRETION DISC CORONA; RAY SOURCES; FEATURES; CATALOG; LINE AB In our observation of the LMXB XB 1323-619 made with XMM-Newton in January 2003, a number of absorption lines were discovered, notably at 6.70 and 6.98 keV which we identify with scattering by high ionization state ions Fe XXV and Fe XXVI. Curve of growth analysis provided a consistent solution for collisional ionization for a plasma temperature kT = 31 keV, close to the electron temperature we previously obtained for the accretion disc corona (ADC) in this source. Thus, for the first time we can explain the absorption features found in recent years in dipping sources as originating in the ADC. We also find a remarkable linear increase in the rate of X-ray bursts with time implying that the gap between bursts will become zero on January 11 (+/- 4), 2008. We expect the source to undergo a transition from X-ray bursting to X-ray flaring confirming that flaring is unstable nuclear burning. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Reed, D.; Church, M. J.; Balucinska-Church, M.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Church, M. J.; Balucinska-Church, M.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Dotani, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Smale, A. P.] NASA, Div Phys & Astron, Off Space Sci, Washington, DC 20546 USA. RP Reed, D (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM dr@star.sr.bham.ac.uk RI Gehrels, Neil/D-2971-2012 FU Polish KBN [KBN-1528/P03/2003/25] FX This work was supported in part by the Polish KBN Grant KBN-1528/P03/2003/25. NR 18 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 7 BP 1524 EP + DI 10.1016/j.asr.2006.02.019 PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW01 UT WOS:000245034500050 ER PT S AU Sylwester, B Sylwester, J Siarkowski, M Phillips, KJH Culhane, JL Lang, J Brown, C Kuznetsov, VD AF Sylwester, B. Sylwester, J. Siarkowski, M. Phillips, K. J. H. Culhane, J. L. Lang, J. Brown, C. Kuznetsov, V. D. BE Gehrels, N Courvoisier, TJL Wilkes, B Diehl, R Williams, DR TI Lines in the range 3.2-6.1 angstrom observed in RESIK spectra SO GALACTIC AND EXTRAGALACTIC ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE Sun; X-ray; spectra; line identification ID X-RAY-SPECTRA; PLASMA COMPOSITION; SOLAR-FLARES; SPECTROMETER; EMISSION AB RESIK is a Bragg bent crystal X-ray spectrometer on board the CORONAS-F satellite. Between 24 August 2002 and 22 May 2003 RESIK collected a large number of solar X-ray spectra in four energy bands covering the range 3.2-6.1 angstrom. A recent absolute calibration has allowed us to make detailed identification of observed spectral features, and from observed line and continuum fluxes to get temperature, emission measure, etc. The lines were identified using spectra averaged over periods of various solar activity levels. These averaged spectra contain a number of strong lines with transitions in H- and He-like ions of K, Ar, S and Si. Some of them are resonance parent lines and their satellites which were observed with other spectrometers and have been described elsewhere. Here, we report detection of several lines not previously observed in solar spectra, including lines of H-like and He-like S and Si ions with transitions Is-np and Is(2)-1snp, n up to 10. In addition we provide identification of the He-like Cl (CI x(VI)) triplet in the range 4.43-4.45 A. The feature at 4.182 angstrom, which is the wavelength of the H-like CI (CI x(VII)) Ly alpha line, is probably a blend of S x(IV) satellites from cooler plasma. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Sylwester, B.; Sylwester, J.; Siarkowski, M.] Polish Acad Sci, Solar Phys Div, Ctr Space Res, Ul Kopernika 11, PL-51622 Wroclaw, Poland. [Phillips, K. J. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Culhane, J. L.] Univ Coll London, Mullard Space Sci Lab, Surrey, England. [Lang, J.] Space Sci & Technol Dept, Rutherford Appleton Lab, Chilton, England. [Brown, C.] Hulburt Ctr Space Res, Naval Res Lab, Washington, DC 20375 USA. [Kuznetsov, V. D.] Russian Acad Sci, IZMIRAN, Moscow, Russia. RP Sylwester, B (reprint author), Polish Acad Sci, Solar Phys Div, Ctr Space Res, Ul Kopernika 11, PL-51622 Wroclaw, Poland. EM bs@cbk.pan.wroc.pl RI Gehrels, Neil/D-2971-2012 FU Polish Committee for Scientific Research [2.P03D.002.22, BPZ-KBN-054/P03/2001] FX B.S, J.S. and M.S. acknowledge support from Grants 2.P03D.002.22 and BPZ-KBN-054/P03/2001 of the Polish Committee for Scientific Research. NR 15 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 7 BP 1534 EP + DI 10.1016/j.asr.2005.08.027 PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW01 UT WOS:000245034500052 ER PT S AU Kepa, A Sylwester, J Sylwester, B Siarkowski, M Phillips, KJH Kuznetsov, VD AF Kepa, A. Sylwester, J. Sylwester, B. Siarkowski, M. Phillips, K. J. H. Kuznetsov, V. D. BE Gehrels, N Courvoisier, TJL Wilkes, B Diehl, R Williams, DR TI Observations of 1s(2)-1s np and 1s-np lines in RESIK soft X-ray spectra SO GALACTIC AND EXTRAGALACTIC ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE sun; X-ray; spectra; high-n transitions ID ACTIVE REGIONS; SOLAR-FLARES; TEMPERATURE DIAGNOSTICS; ELECTRON-TEMPERATURE; EMISSION; RATIOS; ALUMINUM; SILICON; ATOMS; IONS AB RESIK is the X-ray bent crystal spectrometer on the CORONAS-F satellite. Between 2002 and 2003, RESIK collected numerous spectra of active regions and flares in the wavelength range from 3.37 to 6.09 angstrom. This range includes many strong emission lines due to transitions 1s(2) - 1s np and 1s - np, in He-like and H-like ions, respectively; the n = 2 and 3 lines are routinely observed for Si, S and Ar ions. For some flares RESIK has observed enhanced emission in spectral features coinciding with lines due to transitions for n up to 9 or 10. Identifications of these features, not previously observed in astrophysical spectra, are presented in this paper. Their observed intensities are compared with those from theory. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Kepa, A.; Sylwester, J.; Sylwester, B.; Siarkowski, M.] Polish Acad Sci, Space Res Ctr, Solar Phys Div, Ul Kopernika 11, PL-51622 Wroclaw, Poland. [Phillips, K. J. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kuznetsov, V. D.] Russian Acad Sci, IZMIRAN, Moscow, Russia. RP Kepa, A (reprint author), Polish Acad Sci, Space Res Ctr, Solar Phys Div, Ul Kopernika 11, PL-51622 Wroclaw, Poland. EM ak@cbk.pan.wroc.pl RI Gehrels, Neil/D-2971-2012 FU Polish Committee for Scientific Research [2.P03D.002.22]; [BPZKBN-054/P03/2001] FX RESIK (PI: J. Sylwester) is a common project between NRL (USA), MSSL and RAL (UK), IZMIRAN (Russia) and SRC (Poland). RESIK is placed aboard the CORONAS-F satellite. The authors acknowledge support from Grant 2.P03D.002.22 of the Polish Committee for Scientific Research. B. Sylwester, J. Sylwester and M. Siarkowski acknowledge support from the BPZKBN-054/P03/2001 Grant. NR 16 TC 7 Z9 7 U1 0 U2 2 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 7 BP 1538 EP + DI 10.1016/j.asr.2005.08.012 PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW01 UT WOS:000245034500053 ER PT S AU Phillips, KJH Dubau, J Sylwester, J Sylwester, B Culhane, JL Doschek, GA Lang, J AF Phillips, K. J. H. Dubau, J. Sylwester, J. Sylwester, B. Culhane, J. L. Doschek, G. A. Lang, J. BE Gehrels, N Courvoisier, TJL Wilkes, B Diehl, R Williams, DR TI Temperature-sensitive line ratio diagnostics based on Si satellite-to-resonance line ratios for 1s(2)-1snp transitions SO GALACTIC AND EXTRAGALACTIC ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE sun; X-ray; spectra ID EMISSION-LINES; SOLAR; POTASSIUM; ARGON; RESIK AB Dielectronic satellite lines due to 1s(2)n'l' - 1snpn'l' (n = 3,4) transitions in Li-like Si (Si XII) occur at 5.818 and 5.565 angstrom, on the long wavelength side of the He-like Si (Si XIII) 1s(2) - 1s3p and 1s(2) - 1s4p lines at 5.681 and 5.384 angstrom, respectively. They have been extensively observed with the RESIK crystal spectrometer on the Russian spacecraft CORONAS-F. As with corresponding satellites 1s(2)nl-ls2pn1 on the long-wavelength side of the Si XIII 1s(2)-1s2p resonance line, there is an inverse temperature dependence of the intensity ratio of the satellites to the He-like ion lines (I-sat/I-He). New atomic data are used to calculate the Si XII satellite line intensities and thus the I-sat/I-He ratio. RESIK observations of the ratio in solar flares, together with temperatures from the ratio of the two GOES X-ray channels, are compared with theoretical variation of the ratio with temperature. The good agreement indicates this to be a valuable temperature diagnostic for solar flares and laboratory plasmas such as tokamaks. There are implications for similar satellites in Fe line spectra which are observed with broad-band resolution by the RHESSI solar flare mission. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Phillips, K. J. H.] NASA, Goddard Space Flight Ctr, Natl Res Council, Code 612, Greenbelt, MD 20771 USA. [Dubau, J.] Observ Paris, Meudon Sect, F-92195 Meudon, France. [Sylwester, J.; Sylwester, B.] Polish Acad Sci, Space Res Ctr, Wroclaw, Poland. [Culhane, J. L.] Mullard Space Sci Lab, Surrey, England. [Doschek, G. A.] Hullburt Ctr Space Res, Naval Res Lab, Washington, DC 20375 USA. [Lang, J.] Dept Space Sci, Rutherford Appleton Lab, Didcot, Oxon, England. RP Phillips, KJH (reprint author), NASA, Goddard Space Flight Ctr, Natl Res Council, Code 612, Greenbelt, MD 20771 USA. EM Kenneth.J.Phillips.1@gsfc.nasa.gov FU Polish Committee for Scientific Research [2.P03D.002.22, BPZ-KBN-054/P03/2001]; US National Research Council Research FX B.S., J.S. and M.S. acknowledge support from Grants 2.P03D.002.22 and BPZ-KBN-054/P03/2001 of the Polish Committee for Scientific Research. K.J.H.P. acknowledges support from the US National Research Council Research Associateship Program. NR 9 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 7 BP 1543 EP + DI 10.1016/j.asr.2005.08.025 PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW01 UT WOS:000245034500054 ER PT S AU de Nolfo, GA Moskalenko, IV Binns, WR Christian, ER Cummings, AC Davis, AJ George, JS Hink, PL Israel, MH Leske, RA Lijowski, M Mewaldt, RA Stone, EC Strong, AW von Rosenvinge, TT Wiedenbeck, ME Yanasak, NE AF de Nolfo, G. A. Moskalenko, I. V. Binns, W. R. Christian, E. R. Cummings, A. C. Davis, A. J. George, J. S. Hink, P. L. Israel, M. H. Leske, R. A. Lijowski, M. Mewaldt, R. A. Stone, E. C. Strong, A. W. von Rosenvinge, T. T. Wiedenbeck, M. E. Yanasak, N. E. BE Gehrels, N Courvoisier, TJL Wilkes, B Diehl, R Williams, DR TI Observations of the Li, Be, and B isotopes and constraints on cosmic-ray propagation SO GALACTIC AND EXTRAGALACTIC ASTROPHYSICS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT 35th COSPAR Scientific Assembly CY JUL 18-25, 2004 CL Paris, FRANCE SP Comm Space Res DE cosmic rays; Galaxy, general; Galaxy, abundances; Galaxy, evolution; ISM, general ID PRODUCTION CROSS-SECTIONS; ENERGY-SPECTRA; SOLAR MODULATION; NUCLEI; BE-10; GALAXY; AGE; HELIOSPHERE; ABUNDANCE; ULYSSES AB The abundance of Li, Be, and B isotopes in galactic cosmic rays (GCRs) between E = 50 and 200 MeV/nucleon has been observed by the Cosmic Ray Isotope Spectrometer (CRIS) on NASA's ACE mission since 1997 with high statistical accuracy. Precise observations of Li, Be, and B can be used to constrain GCR propagation models. We find that a diffusive reacceleration model with parameters that best match CRIS results (e.g., B/C, Li/C, etc.) are also consistent with other GCR observations. A -15-20% overproduction of Li and Be in the model predictions is attributed to uncertainties in the production cross-section data. The latter becomes a significant limitation to the study of rare GCR species that are generated predominantly via spallation. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [de Nolfo, G. A.; Moskalenko, I. V.; von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. [Moskalenko, I. V.] HEPL & KIP ACI Stanford Univ, Stanford, CA 94305 USA. [Binns, W. R.; Hink, P. L.; Israel, M. H.; Lijowski, M.] Washington Univ, Dept Phys & Space Sci, Mcdonnrll Ctr Space Sci, St Louis, MO 63130 USA. [Christian, E. R.] NASA, Washington, DC 20546 USA. [Cummings, A. C.; Davis, A. J.; George, J. S.; Leske, R. A.; Mewaldt, R. A.; Stone, E. C.; Yanasak, N. E.] CALTECH, Int Space Radiat Lab, Pasadena, CA 91125 USA. [George, J. S.] Aerosp Corp, Los Angeles, CA 90009 USA. [Strong, A. W.] Max Planck Inst Extraterrestrische Phys, D-85740 Garching, Germany. [Wiedenbeck, M. E.] Calf Inst Technol, Jet Prop Lab, Pasadena, CA 91109 USA. RP de Nolfo, GA (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM georgia@milkyway.gsfc.nasa.gov RI Christian, Eric/D-4974-2012; Gehrels, Neil/D-2971-2012; de Nolfo, Georgia/E-1500-2012; Moskalenko, Igor/A-1301-2007 OI Christian, Eric/0000-0003-2134-3937; Moskalenko, Igor/0000-0001-6141-458X FU NASA at NASA/Goddard Space Flight Center; California Institute of Technology [NAG5-6912]; Jet Propulsion Laboratory; Washington University FX This research was supported by NASA at the NASA/Goddard Space Flight Center, the California Institute of Technology, (Grant NAG5-6912), the Jet Propulsion Laboratory,and Washington University. I.V.M. acknowledges partial support from NASA Astrophysics Theory Program (ATP) grant and NASA Astronomy and Physics Research and Analysis Program (APRA) grant. NR 63 TC 25 Z9 25 U1 0 U2 2 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 7 BP 1558 EP + DI 10.1016/j.asr.2006.09.008 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW01 UT WOS:000245034500056 ER PT S AU Simpson, JP Colgan, SWJ Cotera, AS Erickson, EF Hollenbach, DJ Kaufman, MJ Rubin, RH AF Simpson, Janet P. Colgan, Sean W. J. Cotera, Angela S. Erickson, Edwin F. Hollenbach, David J. Kaufman, Michael J. Rubin, Robert H. BE Schodel, R Bower, GC Muno, MP Nayakshin, S Ott, T TI Spitzer IRS observations of the galactic center SO GALACTIC CENTER WORKSHOP 2006: FROM THE CENTER OF THE MILKY WAY TO NEARBY LOW-LUMINOSITY GALACTIC NUCLEI SE Journal of Physics Conference Series LA English DT Proceedings Paper CT Galactic Center Workshop From the Center of the Milky Way to Nearby Low-Luminosity Galactic Nuclei CY APR 18-22, 2006 CL Bad Honnef, GERMANY ID INFRARED SPECTROGRAPH; SPACE-TELESCOPE; CENTER REGION; FILAMENTS; CLUSTERS; EMISSION; COMPLEX; LINE AB We present Spitzer IRS R similar to 600 spectra (10 - 38 mu m) of 38 positions in the Galactic Center (CC), all at the same Galactic longitude of and including the Arches Cluster. Our positions include the Arched Filaments, regions near the Quintuplet Cluster, the "Bubble" lying along the same line-of-sight as the molecular cloud M0.13-0.13, and the diffuse interstellar gas along the line of sight at higher Galactic latitudes. From measurements of the [O IV], [Ne II], [Ne III], [Si II], [S III], [Fe II], [Fe III], and H-2 S(0), S(1), and S(2) lines we determine the gas excitation and ionic abundance ratios. The main source of excitation is photoionization, with the Arches Cluster ionizing the Arched Filaments and the Quintuplet Cluster ionizing the gas nearby and at lower Galactic latitudes including the far side of the Bubble. In addition, strong shocks ionize gas to O+3 and destroy dust grains, releasing iron into the interstellar medium (ISM); the shock effects are particularly noticeable in the center of the Bubble but the highly ionized gas is present in all positions. The H-2 lines are formed both in photodissociation regions in the GC and along the line of sight to the CC. C1 [Simpson, Janet P.; Colgan, Sean W. J.; Erickson, Edwin F.; Rubin, Robert H.] NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA. [Simpson, Janet P.; Cotera, Angela S.] SETI Inst, Mountain View, CA 94043 USA. [Hollenbach, David J.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Kaufman, Michael J.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. [Rubin, Robert H.] Orion Enterprises, Hyderabad, Andhra Pradesh, India. RP Simpson, JP (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA. EM simpson@cygnus.arc.nasa.gov RI Colgan, Sean/M-4742-2014 FU Jet Propulsion Laboratory, California Institute of Technology under NASA [1407] 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. NR 18 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2006 VL 54 BP 161 EP + DI 10.1088/1/1742-6596/54/1/027 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGD82 UT WOS:000246202100027 ER PT S AU Gezari, DY Arendt, RG Smith, R Stolovy, S Yusef-Zadeh, F Law, C Smith, HA Moseley, H Ramirez, S Karr, J Cotera, A Sellgren, K AF Gezari, D. Y. Arendt, R. G. Smith, R. Stolovy, S. Yusef-Zadeh, F. Law, C. Smith, H. A. Moseley, H. Ramirez, S. Karr, J. Cotera, A. Sellgren, K. BE Schodel, R Bower, GC Muno, MP Nayakshin, S Ott, T TI Comparison of Spitzer/IRAC Galactic Center 3.6-8.0 mu m survey results with X-ray emission in the central 40x40 parsecs SO GALACTIC CENTER WORKSHOP 2006: FROM THE CENTER OF THE MILKY WAY TO NEARBY LOW-LUMINOSITY GALACTIC NUCLEI SE Journal of Physics Conference Series LA English DT Proceedings Paper CT Galactic Center Workshop From the Center of the Milky Way to Nearby Low-Luminosity Galactic Nuclei CY APR 18-22, 2006 CL Bad Honnef, GERMANY ID A-ASTERISK AB We have studied the correlation between 2357 Chandra X-ray point sources identified by Muno et al. (2003) in a 40 x 40 parsec field and similar to 20, 000 infrared sources we observed in the corresponding subset of our 2 x 1.5 degree Spitzer/IRAC Galactic Center Survey at 3.68.0 mu m (see Stolovy et al.; this conference), using various spatial and brightness thresholds. The correlation was determined for source separations of less than 0.5, 1.0 or 2.0 arcsec. No significant correlation was found between the X-ray and infrared point sources on these scales. Only one compact infrared source, IRS 13, can be identified with any of the dozen prominent X-ray emission features in the 3x3 parsec region centered on Sgr A*, and the diffuse X-ray and infrared emission around Sgr A* seems to be anti-correlated on a few-arcsecond scale. We compare our results with previous identifications of near infrared companions to Chandra X-ray sources. C1 NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA. RP Gezari, DY (reprint author), NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA. EM Daniel.Y.Gezari@nasa.gov RI Moseley, Harvey/D-5069-2012 NR 12 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2006 VL 54 BP 171 EP + DI 10.1088/1/1742-6596/54/1/029 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGD82 UT WOS:000246202100029 ER PT S AU Gehrels, N AF Gehrels, N. CA Swift Team BE Holt, SS Gehrels, N Nousek, JA TI The Swift gamma-ray burst mission: First results SO Gamma-Ray Bursts in the Swift Era SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma ray bursts; astrophysics ID 28 FEBRUARY 1997; AFTERGLOW; TELESCOPE; EMISSION AB Since its launch on 20 November 2004, the Swift mission is detecting similar to 100 new gamma-ray bursts GRBs) each year, and immediately (within tens of seconds) starting simultaneous X-ray and UV/optical observations of the afterglow. It has already collected am impressive database of bursts, including prompt emission to higher sensitivity than BATSE, uniform monitoring of afterglows, and rapid follow-up by other observatories notified through the GCN. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gehrels, N (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 23 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 14 EP 22 PG 9 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000002 ER PT S AU Sakamoto, T Barbier, L Barthelmy, S Cummings, J Fenimore, E Gehrels, N Hullinger, D Krimm, H Markwardt, C Palmer, D Parsons, A Sato, G Tueller, J Aptekar, R Cline, T Golenetskii, S Mazets, E Pal'shin, V Ricker, G Lamb, D Atteia, JL Kawai, N AF Sakamoto, T. Barbier, L. Barthelmy, S. Cummings, J. Fenimore, E. Gehrels, N. Hullinger, D. Krimm, H. Markwardt, C. Palmer, D. Parsons, A. Sato, G. Tueller, J. Aptekar, R. Cline, T. Golenetskii, S. Mazets, E. Pal'shin, V. Ricker, G. Lamb, D. Atteia, J. -L. Kawai, N. CA Swift-BAT Konus-Wind Team, H2 BE Holt, SS Gehrels, N Nousek, JA TI Are short GRBs really hard? SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE prompt gamma-ray emission; short GRBs ID GAMMA-RAY BURSTS AB Thanks to the rapid position notice and response by HETE-2 and Swift, the X-ray afterglow emissions have been found for four recent short gamma-raybursts (GRBs; GRB 050509b, GRB 050709, GRB 050724, and GRB 050813). The positions of three out of four short GRBs are coincident with galaxies with no current or recent star formation. This discovery tightens the case for a different origin for short and long GRBs. On the other hand, from the prompt emission point of view, a short GRB shows a harder spectrum comparing to that of the long duration GRBs according to the BATSE observations. We investigate the prompt emission properties of four short GRBs observed by Swift/BAT. We found that the hardness of all four BAT short GRBs is in between the BATSE range for short and long GRBs. We will discuss the spectral properties of short GRBs including the short GRB sample of Konus-Wind and HETE-2 to understand the hard nature of the BATSE short GRBs. C1 [Sakamoto, T.; Barbier, L.; Barthelmy, S.; Cummings, J.; Gehrels, N.; Hullinger, D.; Krimm, H.; Markwardt, C.; Parsons, A.; Tueller, J.; Cline, T.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. [Sakamoto, T.; Cummings, J.] CNR, Washington, DC USA. [Fenimore, E.; Palmer, D.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA. [Hullinger, D.] Univ Maryland, Baltimore, MD 21228 USA. [Krimm, H.; Markwardt, C.] Univ Space Res Assoc, Maryland, MA USA. [Sato, G.] Inst Space & Astronaut Sci, Tokyo, Japan. [Golenetskii, S.; Mazets, E.; Pal'shin, V.] AF Ioffe Phys Tech Inst, St Petersburg, Russia. [Ricker, G.] MIT, Cambridge, MA 02139 USA. [Lamb, D.] Univ Chicago, Chicago, IL 60637 USA. [Atteia, J. -L.] Observ Midi Pyrenees, Toulouse, France. [Kawai, N.] Tokyo Inst Technol, Tokyo, Japan. RP Sakamoto, T (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM gehrels@milkyway.gsfc.nasa.gov RI Barthelmy, Scott/D-2943-2012; Tueller, Jack/D-5334-2012; Parsons, Ann/I-6604-2012; Pal'shin, Valentin/F-3973-2014; Aptekar, Raphail/B-3456-2015; Golenetskii, Sergey/B-3818-2015 NR 10 TC 8 Z9 8 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 43 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000005 ER PT S AU O'Brien, PT Willingale, R Osborne, J Goad, MR Page, KL Beardmore, AP Godet, O Burrows, DN Gehrels, N AF O'Brien, P. T. Willingale, R. Osborne, J. Goad, M. R. Page, K. L. Beardmore, A. P. Godet, O. Burrows, D. N. Gehrels, N. BE Holt, SS Gehrels, N Nousek, JA TI The Swift prompt sample SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma-ray bursts ID GAMMA-RAY BURSTS; AFTERGLOW EMISSION AB We have analysed BAT and XRT data for 40 gamma-ray bursts (GRBs) observed using the Swift satellite. The earliest X-ray light curve can be well described by an exponential which relaxes into a power law, often with flares superimposed. The transition time between the exponential and the power law gives a physically defined timescale for the burst duration. In most GRBs the power law decay changes to a shallower decay within the first hour. The resultant "late emission hump" can last for several tens of ks. In other bursts the late hump is weak or absent. The observed variety in light curve shape can be explained as a combination of three components: prompt emission from the central engine; afterglow; and the late hump, which may also be due to the central engine. GRBs with stronger afterglow components are more likely to have brighter early optical emission. The late emission hump can have a total fluence equivalent to that of the prompt phase. C1 [O'Brien, P. T.; Willingale, R.; Osborne, J.; Goad, M. R.; Page, K. L.; Beardmore, A. P.; Godet, O.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP O'Brien, PT (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM gehrels@milkyway.gsfc.nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 85 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000013 ER PT S AU Kazanas, D Mastichiadis, A Georganopoulos, M AF Kazanas, Demosthenes Mastichiadis, Apostolos Georganopoulos, Markos BE Holt, SS Gehrels, N Nousek, JA TI The "Supercritical Pile" model of GRB: Spectra and their time development SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam ID GAMMA-RAY-BURSTS; F-NU PEAK; EMISSION; BATSE AB The essence of the "Supercritical Pile" GRB model is a process for converting the energy stored in the relativistic protons of a Relativistic Blast Wave (RBW) of Lorentz factor Gamma into electron - positron pairs of similar Lorentz factor. This is achieved by scattering the synchrotron radiation emitted by the RBW in an upstream located "mirror" and then re-intercepting it by the RBW. The repeated scatterings of radiation between the RBW and the "mirror", along with the threshold of the pair production reaction p gamma -> pe(-) e(+), lead to a maximum in the GRB spectral luminosity at an energy E-p similar or equal to 1 MeV, in general agreement with observation, independent of the value of Gamma. Furthermore, the same threshold implies that the prompt gamma-ray emission is only possible for Gamma larger than a minimum value, thereby providing a "natural" account for the termination of this stage of the GRB as the RBW slows down. Within this model the gamma-ray (E similar to 100 keV - 1 MeV) emission process is due to bulk Inverse Compton scattering and it is thus expected to be highly polarized if viewed at angles theta similar or equal to 1/Gamma to the direction of the RBW. We have simulated the process of spectral formation by following the time development of the proton, electron and photon distribution functions. We present the results these calculations. C1 [Kazanas, Demosthenes; Mastichiadis, Apostolos] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Georganopoulos, Markos] Univ Athens, Dept Astron, Athens 15784, Greece. RP Kazanas, D (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. FU program Pythagoras at the Univsrsity of Athens; INTEGRAL GO grant; GSFC; UMBC FX This work has been supported by the program Pythagoras at the Univsrsity of Athens and an INTEGRAL GO grant at GSFC and UMBC. NR 9 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 137 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000024 ER PT S AU Krimm, HA Hurkett, C Pal'shin, V Norris, JP Zhang, B Barthelmy, SD Burrows, DN Gehrels, N Golenetskii, S Osborne, JP Parsons, AM Perri, M AF Krimm, H. A. Hurkett, C. Pal'shin, V. Norris, J. P. Zhang, B. Barthelmy, S. D. Burrows, D. N. Gehrels, N. Golenetskii, S. Osborne, J. P. Parsons, A. M. Perri, M. BE Holt, SS Gehrels, N Nousek, JA TI GRB 050717: A long, short-lag burst observed by swift and konus SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma-ray bursts; gamma-ray telescopes ID GAMMA-RAY BURSTS; LUMINOSITY AB The long burst GRB 050717 was observed simultaneously by the Burst Alert Telescope (BAT) on Swift and the Konus instrument on Wind. Significant hard to soft spectral evolution was seen. Early gamma-ray and X-ray emission was detected by both BAT and the X-Ray Telescope (XRT) on Swift. The XRT continued to observe the burst for 7.1 days and detect it for 1.4 days. The X-ray light curve showed a classic decay pattern including evidence of the onset of the external shock emission at similar to 45 s after the trigger; the afterglow was too faint for a jet break to be detected. No optical, infrared or ultraviolet counterpart was discovered despite deep searches within 14 hours of the burst. The spectral lag for GRB 050717 was determined to be 2.5 +/- 2.6 ms, consistent with zero and unusually short for a long burst. This lag measurement suggests that this burst has a high intrinsic luminosity and hence is at high redshift (z > 2.7). GRB 050717 provides a good example of classic prompt and afterglow behavior for a gamma-ray burst. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Universities Space Res Associat, Columbia, MD 21044 USA. [Hurkett, C.; Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Pal'shin, V.; Golenetskii, S.] Ioffe Physico Tech Inst, Lab Expt Astrophys, St Petersburg 194021, Russia. [Zhang, B.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Perri, M.] ASI Sci Data Ctr, I-00044 Frascati, Italy. RP Krimm, HA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Gehrels, Neil/D-2971-2012; Parsons, Ann/I-6604-2012; Pal'shin, Valentin/F-3973-2014; Golenetskii, Sergey/B-3818-2015; OI Perri, Matteo/0000-0003-3613-4409 FU NASA; University of Leicester; Particle Physics and Astronomy Research Council (PPARC); PPARC; Russian Space Agency contract and RFBR [06-02-16070] FX H. A. K. was supported in this work by the Swift project, funded by NASA. This work is supported at the University of Leicester by the Particle Physics and Astronomy Research Council (PPARC). C. P. H. gratefully acknowledges support from a PPARC studentship. The Wind Konus experiment is supported by Russian Space Agency contract and RFBR grant 06-02-16070. H. A. K. is also grateful for useful discussions with T. Sakamoto, P. OBrien, and Y. Kaneko NR 10 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 141 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000025 ER PT S AU Krimm, HA Barthelmy, SD Gehrels, N Hullinger, D Sakamoto, T Donaghy, T Lamb, DQ Pal'shin, V Golenetskii, S Ricker, GR Atteia, JL Kawai, N Sato, G AF Krimm, H. A. Barthelmy, S. D. Gehrels, N. Hullinger, D. Sakamoto, T. Donaghy, T. Lamb, D. Q. Pal'shin, V. Golenetskii, S. Ricker, G. R. Atteia, J-L Kawai, N. Sato, G. BE Holt, SS Gehrels, N Nousek, JA TI Correlative analysis of GRBs detected by Swift, Konus and HETE SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma-ray bursts; gamma-ray telescopes ID GAMMA-RAY BURSTS; PEAK ENERGY AB Swift has now detected a large enough sample of gamma-ray bursts (GRBs) to allow correlation studies of burst parameters. Such studies of earlier data sets have yielded important results leading to further understanding of burst parameters and classifications. This work focusses on seventeen Swift bursts that have also been detected either by Konus-Wind or HETE-II, providing high energy spectra and fits to E-peak. Eight of these bursts have spectroscopic redshifts and for others we can estimate redshifts using the variability/lummosity relationship. We can also compare E-peak with E-iso and for those bursts for which a jet break was observed in the afterglow we can derive Eg and test the relationship between E-peak and E-gamma. For all bursts we can derive durations and hardness ratios from the prompt emission. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Hullinger, D.] Univ Maryland, College Pk, MD 21228 USA. [Sakamoto, T.] CNR, Washington, DC USA. [Lamb, D. Q.] Univ Chicago, Chicago, IL 60637 USA. [Pal'shin, V.; Golenetskii, S.] Ioffe physico Tech Inst, Lab Expt Astrophys, St Petersburg 194021, Russia. [Ricker, G. R.] MIT, Cambridge, MA 02139 USA. [Atteia, J-L] Observatoire Midi Pyrenee, Toulouse, France. [Kawai, N.] Tokyo Inst Technol, Tokyo, Japan. [Sato, G.] Inst Space & Astronaut Sci, Kanagawa, Japan. [Sato, G.] Univ Tokyo, Tokyo 1138654, Japan. RP Krimm, HA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Pal'shin, Valentin/F-3973-2014; Golenetskii, Sergey/B-3818-2015 NR 5 TC 12 Z9 12 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 145 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000026 ER PT S AU Nakagawa, YE Yoshida, A Maetou, M Suzuki, M Tamagawa, T Sakamoto, T Kawai, N Shirasaki, Y Tanaka, K Matsuoka, M Fenimore, EE Galassi, M Atteia, JL Hurley, K Ricker, GR AF Nakagawa, Y. E. Yoshida, A. Maetou, M. Suzuki, M. Tamagawa, T. Sakamoto, T. Kawai, N. Shirasaki, Y. Tanaka, K. Matsuoka, M. Fenimore, E. E. Galassi, M. Atteia, J. -L. Hurley, K. Ricker, G. R. BE Holt, SS Gehrels, N Nousek, JA TI Temporal and spectral analyses of SGRs observed by HETE-2 SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE neutron stars ID RAY; SGR-1900+14; BURST; PERFORMANCE; FREGATE AB HETE-2 localized 63 flares from SGR1806-20 and 6 flares from SGR1900+14 in the summer periods from June 18 2001 through August 7 2005. We report on the temporal and spectral analyses of short flares from those SGRs. The estimation of T-90 durations in 2-30 keV and 30-100 keV revealed that there is no difference between them with a few exceptions. For these exceptional short flares, there seems softening or possibly hardening during flares, but these spectral evolution are not common. We also found a good linear correlation between the rise and decay time, and they do not depend on a peak flux. We also found that the spectra are well reproduced by a sum of two blackbody models for all short flares. The temperatures are lying around 4 keV and I I keV which are consistent with previous studies. T'hey are not depend on either the magnitude of flare, the event morphology or the source. C1 [Nakagawa, Y. E.; Yoshida, A.; Maetou, M.; Tanaka, K.] Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2298558, Japan. [Suzuki, M.; Tamagawa, T.] RIKEN, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. [Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. [Shirasaki, Y.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Matsuoka, M.] Japan Aerosp Explorat Agcy, Tsukuba Space Ctr, Tsukuba, Ibaraki 3048505, Japan. [Fenimore, E. E.; Galassi, M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Atteia, J. -L.] Observ Midi Pyrenees, Astrophys Lab, F-31400 Toulouse, France. [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Ricker, G. R.] MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Nakagawa, YE (reprint author), Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2298558, Japan. NR 12 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 173 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000033 ER PT S AU Shrader, CR AF Shrader, C. R. BE Holt, SS Gehrels, N Nousek, JA TI INTEGRAL observations of the nearby, under-luminous gamma-ray burst GRB 031203 SO Gamma-Ray Bursts in the Swift Era SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma-ray bursts; GRB 031203; lag-luminosity relation; E-iso-E-peak relation ID REDSHIFTS AB GRB 031203 was discovered by the INTEGRAL burst analysis system in near real time. It was about 10 degrees off axis, thus well within the partially coded IBIS FoV and within the SPI fully coded FoV. This led to prompt follow up observations, reported on elsewhere, which resulted in red shift and luminosity information and estimates of the prompt soft X-ray intensity. Here we have revisited the INTEGRAL observations, notably including an analysis of the SPI germanium spectrograph data, which allows improved characterization of the spectral energy distribution to energies in excess of 200 keV. We explore the possibility of imposing new constraints on E-peak and on the hard-soft temporal lag determination. C1 NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. RP Shrader, CR (reprint author), NASA, Goddard Space Flight Ctr, Explorat Universe Div, Code 661, Greenbelt, MD 20771 USA. NR 9 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 185 EP 188 PG 4 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000036 ER PT S AU Nishikawa, KI Hardee, P Hededal, C Kouvehotou, C Fishman, GJ Mizuno, Y AF Nishikawa, K. -I. Hardee, P. Hededal, C. Kouvehotou, C. Fishman, G. J. Mizuno, Y. BE Holt, SS Gehrels, N Nousek, JA TI Simulation studies of early afterglows observed with SWIFT SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE relativistic jets; Weibel instability; particle acceleration; emission ID MAGNETIC-FIELD GENERATION; SYNCHROTRON SHOCK MODEL; RAY BURST SHOCKS; PARTICLE-ACCELERATION; PLASMA SHOCKS; REVERSE SHOCK; EMISSION; INSTABILITY AB We have applied numerical simulations and modeling to the particle acceleration, magnetic field generation, and emission from relativistic shocks and plan to compare them with the observed gamma-ray burst emission. In collisionless shocks, plasma waves and their associated instabilities (e.g., the Weibel, Buneman and other two-stream instabilities) are responsible for particle (electron, positron, and ion) acceleration and magnetic field generation. A 3-D relativistic electromagnetic particle (REMP) code is used to study shock processes including spatial and temporal evolution of shocks in unmagnetized electron-positron plasmas with three different jet velocity distributions. The "jitter" radiation from the shocks is different from synchrotron radiation. The dynamics of shock microscopic process evolution may provide some insight into early afterglows. Our simulation studies provide insight into new GRB observations with Swift. C1 [Nishikawa, K. -I.] NSSTC, 320 Sparkman Dr XD12, Huntsville, AL 35805 USA. [Hardee, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Hededal, C.] Niels Bohr Inst, Dark Cosmol Ctr, Copenhagen 2100, Denmark. [Kouvehotou, C.; Fishman, G. J.; Mizuno, Y.] NASA Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville 35805, AL USA. RP Nishikawa, KI (reprint author), NSSTC, 320 Sparkman Dr XD12, Huntsville, AL 35805 USA. RI Mizuno, Yosuke/D-5656-2017 OI Mizuno, Yosuke/0000-0002-8131-6730 FU NSF [ATM-0100997, INT-9981508, AST-0506719., AST-0506666]; National Space Science & Technology (NSSTC/NASA) [NCC8-256]; IBM [p690]; National Center for Supercomputing Applications(NCSA) FX K.I. Nishikawa was a NRC Senior Research Fellow at NASA Marshall Space Flight Center until June 2005. We thank Enrico Ramirez-Ruiz for suggesting a widely distributed velocity distribution for injected pair jets. This research (K.N.) is partially supported by the NSF awards ATM-0100997, INT-9981508, and AST-0506719. P. Hardee acknowledges partial support by a National Space Science & Technology (NSSTC/NASA) cooperative agreement NCC8-256 and NSF award AST-0506666. The simulations have been performed on IBM p690 at the National Center for Supercomputing Applications(NCSA) which is supported by the NSF. NR 30 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 265 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000049 ER PT S AU Moretti, A De Luca, A Malesani, D Campana, S Tiengo, A Reeves, JN Capalbi, M Chincarini, G Covino, S Cusumano, G Giommo, P La Parola, V Mangano, V Mineo, T Perro, M Romano, P Tagliaferri, G AF Moretti, A. De Luca, A. Malesani, D. Campana, S. Tiengo, A. Reeves, J. N. Capalbi, M. Chincarini, G. Covino, S. Cusumano, G. Giommo, P. La Parola, V. Mangano, V. Mineo, T. Perro, M. Romano, P. Tagliaferri, G. BE Holt, SS Gehrels, N Nousek, JA TI Swift and XMM observations of the dark GRB 050326 SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma rays; bursts - X-rays; individual (GRB 050326) AB We present a detailed analysis of the GRB 050326 prompt and afterglow emission. The combined capabilities of Swift (which sampled the light curve for a relatively long time span) and XMM (which ensured a large statistics) allowed to obtain a thorough characterization of the afterglow properties. C1 [Moretti, A.; Campana, S.; Chincarini, G.; Covino, S.; Tagliaferri, G.] Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, LC, Italy. [De Luca, A.; Tiengo, A.] Inst Astrofis Spaziale & Fis Cosmica Milano, INAF, I-20133 Milan, Italy. [Malesani, D.] SISSA ISAS, Int Sch Adv Studies, I-34014 Trieste, Italy. [Reeves, J. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Capalbi, M.; Giommo, P.; Perro, M.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Cusumano, G.; La Parola, V.; Mangano, V.; Mineo, T.] INAF, Inst Astrofis Spaziale & Fis Cosmica Palermo, I-90146 Palermo, Italy. RP Moretti, A (reprint author), Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, LC, Italy. OI Mineo, Teresa/0000-0002-4931-8445; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; Perri, Matteo/0000-0003-3613-4409; La Parola, Valentina/0000-0002-8087-6488; De Luca, Andrea/0000-0001-6739-687X; Covino, Stefano/0000-0001-9078-5507; Tagliaferri, Gianpiero/0000-0003-0121-0723 NR 8 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 285 EP + PG 3 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000053 ER PT S AU Hill, JE Morris, DC Sakamoto, T Sato, G Burrows, DN Angelini, L Pagani, C Moretti, A Abbey, AF Barthelmy, S Beardmore, AP Biryukov, VV Campana, S Capalbi, M Cumnano, G Giommi, P Ibrahimov, MA Kennea, JA Kobayashi, S Ioka, K Markwardt, C Meszaros, P O'Brien, PT Osbome, JP Pozanenko, AS Perri, M Rumyantsev, VV Schady, P Sharapov, DA Tagliaferri, G Zhang, B Chincarini, G Gehrels, N Wells, A Nousek, JA AF Hill, J. E. Morris, D. C. Sakamoto, T. Sato, G. Burrows, D. N. Angelini, L. Pagani, C. Moretti, A. Abbey, A. F. Barthelmy, S. Beardmore, A. P. Biryukov, V. V. Campana, S. Capalbi, M. Cumnano, G. Giommi, P. Ibrahimov, M. A. Kennea, J. A. Kobayashi, S. Ioka, K. Markwardt, C. Meszaros, P. O'Brien, P. T. Osbome, J. P. Pozanenko, A. S. Perri, M. Rumyantsev, V. V. Schady, P. Sharapov, D. A. Tagliaferri, G. Zhang, B. Chincarini, G. Gehrels, N. Wells, A. Nousek, J. A. BE Holt, SS Gehrels, N Nousek, JA TI GRB 050117: simultaneous gamma-ray and X-ray observations with the Swift satellite SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma rays; bursts - general; gamma-rays; X-rays - individual (GRB 050117) ID AFTERGLOW EMISSION; BURSTS AB The Swift Gamma-Ray Burst Explorer performed its first autonomous, X-ray follow-up to a newly detected GRB on 2005 January 17, within 193 seconds of the burst trigger by the Swift Burst Alert Telescope. While the burst was still in progress, the X-ray Telescope obtained a position and an image for an un-catalogued X-ray source; simultaneous with the gamma-ray observation. The XRT observed flux during the prompt emission was 1.1 x 10(-8) ergs CM,2 s(-1) in the 0.5-10 kcV energy band. The emission in the X-ray band decreased by three orders of magnitude within 700 seconds, following the prompt emission. This is found to be consistent with the gamma-ray decay when extrapolated into the XRT energy band. During the following 6.3 hours, the XRT observed the afterglow in an automated sequence for an additional 947 seconds, until the burst became fully obscured by the Earth limb. A faint, extremely slowly decaying afterglow, alpha=-0.21, was detected. Finally, a break in the lightcurve occurred and the flux decayed with alpha <-1.2. The X-ray position triggered many follow-up observations: no optical afterglow could be confirmed, although a candidate was identified 3 arcsecs from the XRT position. C1 [Hill, J. E.; Sakamoto, T.; Angelini, L.; Markwardt, C.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hill, J. E.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Morris, D. C.; Burrows, D. N.; Pagani, C.; Kennea, J. A.; Kobayashi, S.; Ioka, K.; Wells, A.; Nousek, J. A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Sato, G.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Angelini, L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Pagani, C.; Moretti, A.; Tagliaferri, G.; Chincarini, G.] INAF, Osservtorio Astron Brera, I-23807 Merate, Italy. [Abbey, A. F.; Wells, A.] Univ Leicester, Space Res Ctr, Leicester LE1 7RH, Leics, England. [Beardmore, A. P.; Osbome, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Biryukov, V. V.] Moscow MV Lomonosov State Univ, Stemberg Astron Inst, Moscow, Russia. [Capalbi, M.; Giommi, P.; Perri, M.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Cumnano, G.] INAF, Inst Astrofis Spaziale & Fis Cosm sezione Palermo, I-90146 Palermo, Italy. [Ibrahimov, M. A.] Ulugh Beg Astron Inst, Tashkent 700052, Uzbekistan. [Kobayashi, S.] Penn State Univ, Ctr Graviational Wave Phys, University Pk, PA 16802 USA. [Pozanenko, A. S.] Moscow Space Res Inst, Moscow 117810, Russia. [Schady, P.] Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Zhang, B.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. RP Hill, JE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; OI Campana, Sergio/0000-0001-6278-1576; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; Rumyantsev, Vasilij/0000-0003-1894-7019; Perri, Matteo/0000-0003-3613-4409; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU NASA [NAS5-00136]; University of Leicester by the Particle Physics and Astronomy Research Council [PPA/Z/S/2003/00507]; AS1 [I/R/039/04] FX This work is supported at Penn State by NASA contract NAS5-00136; at the University of Leicester by the Particle Physics and Astronomy Research Council on grant number PPA/Z/S/2003/00507; and at OAB by funding from AS1 on grant number I/R/039/04. We gratefully acknowledge the contributions of dozens of members of the Swgt team at PSU, University of Leicester, OAB, GSFC, ASDC and our subcontractors, who helped make this Observatory possible and to the Flight Operations Team for their dedication and support. NR 5 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 289 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000054 ER PT S AU Hill, JE Angelini, L Moretti, A Morris, DC Racusin, J Burrows, DN Beardmore, AP Campana, S Capalbi, M Kennea, JA Osborne, JP Pagani, C Tagliaferri, G Chincarini, G Gehrels, N Wells, A Nousek, JA AF Hill, J. E. Angelini, L. Moretti, A. Morris, D. C. Racusin, J. Burrows, D. N. Beardmore, A. P. Campana, S. Capalbi, M. Kennea, J. A. Osborne, J. P. Pagani, C. Tagliaferri, G. Chincarini, G. Gehrels, N. Wells, A. Nousek, J. A. BE Holt, SS Gehrels, N Nousek, JA TI Rapid centroids and the refined position accuracy of the Swift gamma-ray burst catalogue SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma-ray bursts; X-rays; CCDs; centroiding AB The Swift X-ray Telescope autonomously refines the Burst Alert Telescope positions (similar to 1-4' uncertainty) to better than 5 arcsec, within 5 seconds of target acquisition by the observatory for typical bursts. The results of the rapid positioning capability of the XRT are presented here for both known sources and newly discovered GRBs, demonstrating the ability to automatically utilise one of two integration times according to the burst brightness, and to correct the position for alignment offsets caused by the fast pointing performance and variable thermal environment of the satellite as measured by the Telescope Alignment Monitor. We present an evaluation of the position accuracy for both the onboard centroiding software and the ground software for the calibration targets and show that a significant improvement in position accuracy is obtained if the boresight detector position is optimised relative to the spacecraft pointing. Finally, we present an updated catalogue of Swift GRB X-ray positions obtained in Photon Counting Mode using the improved, calibrated boresight. C1 [Hill, J. E.; Angelini, L.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hill, J. E.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Angelini, L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Moretti, A.; Tagliaferri, G.; Chincarini, G.] INAF, Osservat Astron Brera, Merate, Italy. [Morris, D. C.; Racusin, J.; Burrows, D. N.; Kennea, J. A.; Wells, A.; Nousek, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Beardmore, A. P.; Osborne, J. P.; Wells, A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Capalbi, M.] ASI Sci data Ctr, I-00044 Frascati, Italy. RP Hill, JE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Racusin, Judith/D-2935-2012; OI Tagliaferri, Gianpiero/0000-0003-0121-0723 FU NASA [NAS5-00136]; University of Leicester by the Particle Physics and Astronomy Research Council [PPA/Z/S/2003/00507]; AS1 [IN03 9/04] FX This work is supported at Penn State by NASA contract NAS5-00136; at the University of Leicester by the Particle Physics and Astronomy Research Council on grant number PPA/Z/S/2003/00507; and at OAB by funding from AS1 on grant number IN03 9/04. NR 3 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 297 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000056 ER PT S AU Marshall, FE AF Marshall, F. E. CA The Swift Team BE Holt, SS Gehrels, N Nousek, JA TI Rapid identification of GRB afterglows with Swift/UVOT SO Gamma-Ray Bursts in the Swift Era SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma-ray bursts; gamma-ray telescopes AB As part of the automated response to a new GRB, the UVOT instrument on Swift starts a 200-second exposure with the V filter within similar to 100 seconds of the BAT burst trigger. The instrument searches for sources in a 8' x 8' region, and sends the list of sources and a 160" x 160" sub-image centered on the burst position to the ground via TDRSS. These raw products and additional products calculated on the ground are then distributed through the GCN within a few minutes of the trigger. We describe the sensitivity of these data for detecting afterglows, summarize current results, and outline plans for rapidly distributing future detections. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Marshall, FE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 309 EP 312 PG 4 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000059 ER PT S AU Falcone, AD Burrows, DN Romano, P Kobayashi, S Lazzati, D Zhang, B Campana, S Chincarini, G Cusumano, G Gehrels, N Giommi, P Goad, MR Godet, O Hill, JE Kennea, JA Meszaros, P Morris, D Nousek, JA O'Brien, PT Osborne, JP Pagani, C Pagei, K Tagliaferri, G AF Falcone, A. D. Burrows, D. N. Romano, P. Kobayashi, S. Lazzati, D. Zhang, B. Campana, S. Chincarini, G. Cusumano, G. Gehrels, N. Giommi, P. Goad, M. R. Godet, O. Hill, J. E. Kennea, J. A. Meszaros, P. Morris, D. Nousek, J. A. O'Brien, P. T. Osborne, J. P. Pagani, C. Pagei, K. Tagliaferri, G. CA The Swift XRT Team BE Holt, SS Gehrels, N Nousek, JA TI Late-time x-ray flares during GRB afterglows: Extended internal engine activity SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma ray bursts; x-rays ID BURST AFTERGLOWS AB Observations of gamma ray bursts (GRBs) with Swift produced the initially surprising result that many bursts have large X-ray flares superimposed on the underlying afterglow. These flares were sometimes intense, rapid, and late relative to the nominal prompt phase. The most intense of these flares was observed by XRT with a flux > 500x the afterglow. This burst then surprised observers by flaring again after > 10000 s. The intense flare can be most easily understood within the context of the standard fireball model, if the internal engine that powers the prompt GRB emission is still active at late times. Recent observations indicate that X-ray flares are detected in similar to 1/3 of XRT detected afterglows. By studying the properties of the varieties of flares (such as rise/fall time, onset time, spectral variability, etc.) and relating them to overall burst properties, models of flare production and the GRB internal engine can be constrained. C1 [Falcone, A. D.; Burrows, D. N.; Kobayashi, S.; Kennea, J. A.; Meszaros, P.; Morris, D.; Nousek, J. A.; Pagani, C.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Romano, P.; Campana, S.; Chincarini, G.; Goad, M. R.; Tagliaferri, G.] INAF, Oddervatorio Astronomico Brera, I-23807 Merate, Italy. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LL, Merseyside, England. [Lazzati, D.; Gehrels, N.; The Swift XRT Team] Univ Colorado, JILA, Boulder, CO 80309 USA. [Zhang, B.] Univ Nevada, Dept Phys, Las Vegas, NV USA. [Chincarini, G.; Goad, M. R.] Univ Milano Bicocca, Dipartmento Fisica, Milan, Italy. [Cusumano, G.] INAF, Istituto Fis Spazialee Fis Cosmica Sezione, Palermo, Italy. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenmbelt, MD USA. [Giommi, P.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Godet, O.; O'Brien, P. T.; Osborne, J. P.; Pagei, K.] Univ Leicester, Dept Phys & Astronom, Leicester, Leics, England. [Kobayashi, S.; Hill, J. E.] USRA, Columbia, MD 21044 USA. [Meszaros, P.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. RP Falcone, AD (reprint author), Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. OI giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU NASA [NAS5-00 136]; Univ. of Leicester by the Particle Physics and Astronomy Research Council [PPA/Z/S/2003/00507]; ASI [I/R/039/04] FX This work is supported at Penn State by NASA contract NAS5-00 136; at the Univ. of Leicester by the Particle Physics and Astronomy Research Council under grant PPA/Z/S/2003/00507; and at OAB by funding from ASI under grant I/R/039/04 NR 31 TC 5 Z9 5 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 386 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000075 ER PT S AU Holland, ST Blustin, AJ AF Holland, Stephen T. Blustin, Alex J. CA Swift Science Team BE Holt, SS Gehrels, N Nousek, JA TI Swift panchromatic observations of the bright gamma-ray burst GRB 050525A SO Gamma-Ray Bursts in the Swift Era SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma rays; bursts ID DUST AB The Swift observatory discovered and observed GRB 050525A. The X-ray and optical/ultraviolet afterglow decay curves exhibit an achromatic break approximately 0.15 days after the burst. This break, and the total gamma-ray energy of the burst, implies a jet opening angle of 2.degrees 5. Prior to the break the X-ray spectrum can be modelled by a power law with beta(X) = - 1.2. A short X-ray flare occurred 300 s after the burst. The optical/ultraviolet data have a complex decay, with evidence of a reverse shock dominating in the first few minutes and a forward shock dominating at later times. The X-ray/ultraviolet/optical spectrum suggests that a cooling break moved through the optical between 800 and 25 000 s after the burst. The temporal decay and spectral indices agree with the standard fireball model, assuming a uniform interstellar medium. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Holland, ST (reprint author), NASA, Goddard Space Flight Ctr, Code 660-1, Greenbelt, MD 20771 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 436 EP 439 PG 4 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000084 ER PT S AU Cusumano, G Mangano, V Chincarini, G Panaitescu, A Burrows, DN La Parola, V Sakamoto, T Campana, S Mineo, T Tagliaferri, G Angelini, L Barthelemy, SD Beardmore, AP Boyd, PT Cominsky, LR Gronwall, C Fenimore, EE Gehrels, N Giommi, P Goad, M Hurley, K Kennea, JA Mason, KO Marshall, F Meszaros, P Nousek, JA Osborne, JP Palmer, DM Roming, PWA Wells, A White, NE Zhang, B AF Cusumano, G. Mangano, V. Chincarini, G. Panaitescu, A. Burrows, D. N. La Parola, V. Sakamoto, T. Campana, S. Mineo, T. Tagliaferri, G. Angelini, L. Barthelemy, S. D. Beardmore, A. P. Boyd, P. T. Cominsky, L. R. Gronwall, C. Fenimore, E. E. Gehrels, N. Giommi, P. Goad, M. Hurley, K. Kennea, J. A. Mason, K. O. Marshall, F. Meszaros, P. Nousek, J. A. Osborne, J. P. Palmer, D. M. Roming, P. W. A. Wells, A. White, N. E. Zhang, B. BE Holt, SS Gehrels, N Nousek, JA TI GRB 050904: The oldest cosmic explosion ever observed in the Universe SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma ray bursts; X-rays ID GAMMA-RAY BURSTS; ENERGY; ENERGETICS; SPECTRA; JETS AB Swift discovered the high redshift (z=6.29) GRB 050904 with the Burst Alert Telescope and began observing with its narrow field instruments only 161 s after the burst onset. GRB 050904 was a long, multi-peaked, bright GRB with a presence of flaring activity lasting up to 1-2 hours after the burst onset. The spectral energy distribution shows a clear softening trend along the burst evolution with a photon index decreasing from -1.2 up to -1.9. The observed variability is more dramatic than the typical Swift afterglow, the amplitude and rise/fall times of the flares are consistent with the behavior of nearby (z <= 1) long GRBs and suggest the interpretation of the BAT and XRT data as a single continuous observation of long lasting prompt emission. C1 [Cusumano, G.; Mangano, V.; La Parola, V.; Mineo, T.] INAF, Ist Astrofis Spaziale & Fis Cosm Palermo, Via Ugo La Malfa 153, I-90146 Palermo, Italy. [Chincarini, G.; Campana, S.; Tagliaferri, G.] INAF, Osservatorio Astronom Brera, I-23807 Merate, Italy. [Chincarini, G.] Univ Degil Studi Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy. [Panaitescu, A.; Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Burrows, D. N.; Gronwall, C.; Kennea, J. A.; Meszaros, P.; Roming, P. W. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Sakamoto, T.; Angelini, L.; Barthelemy, S. D.; Boyd, P. T.; Gehrels, N.; Marshall, F.; White, N. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sakamoto, T.] CNR, Washington, DC 20418 USA. [Goad, M.; Osborne, J. P.; Wells, A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Fenimore, E. E.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Giommi, P.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Mason, K. O.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Meszaros, P.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Zhang, B.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. RP Cusumano, G (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm Palermo, Via Ugo La Malfa 153, I-90146 Palermo, Italy. RI Boyd, Patricia/D-3274-2012; OI Mineo, Teresa/0000-0002-4931-8445; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; La Parola, Valentina/0000-0002-8087-6488; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU ASI; NASA; PPARC FX The authors acknowledge support from ASI, NASA and PPARC. NR 24 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 564 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000105 ER PT S AU Sakamoto, T Barbier, L Barthelmy, S Cummings, J Fenimore, E Gehrels, N Hullinger, D Krimm, H Markwardt, C Palmer, D Parsons, A Sato, G Tueller, J AF Sakamoto, T. Barbier, L. Barthelmy, S. Cummings, J. Fenimore, E. Gehrels, N. Hullinger, D. Krimm, H. Markwardt, C. Palmer, D. Parsons, A. Sato, G. Tueller, J. BE Holt, SS Gehrels, N Nousek, JA TI Confirmation of the E-peak(src)-E-iso (Amati) relation from the X-ray flash XRE 050416A observed by Swift/BAT SO Gamma-Ray Bursts in the Swift Era SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE prompt gamma-ray emission; X-ray flash ID INTRINSIC SPECTRA; BURSTS; ENERGETICS; XRF-020903; CATALOG; ENERGY AB We report Swift Burst Alert Telescope (BAT) observations of the X-ray Flash (XRF) XRF 050416A. The fluence ratio between the 15-25 and 25-50 keV bands of this event is 1.1, thus making it the softest gamma-ray burst (GRB) observed by BAT so far. The spectrum is well fitted by the Band function with E-peak(obs) of 15.6(-2.7)(+2.3) keV. Assuming the redshift of the host galaxy (z=0.6535), the isotropic-equivalent energy E-iso and the E-peak energy at the GRB rest frame (E-peak(src)) of XRF 050416A are not only consistent with the correlation found by Amati et al. and extended to XRFs by Sakamoto et al., but also fill-in the gap of this relation around 30-80 keV range of E-peak(src). This result tightens the validity of the E-peak(src)-E-iso relation form XRFs to GRBs. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sakamoto, T (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Tueller, Jack/D-5334-2012; Parsons, Ann/I-6604-2012 NR 20 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 578 EP 581 PG 4 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000108 ER PT S AU Stamatikos, M Band, DL AF Stamatikos, Michael Band, David L. BE Holt, SS Gehrels, N Nousek, JA TI A new search paradigm for correlated neutrino emission from discrete GRBs using antarctic Cherenkov telescopes in the swift era SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma-ray; bursts; radiation mechanisms; nonthermal; neutrinos ID GAMMA-RAY BURSTS; SPECTRA AB We describe the theoretical modeling and analysis techniques associated with a preliminary. search for correlated neutrino emission from GRB980703a, which triggered the Burst and Transient Source Experiment (BATSE GRB trigger 6891), using archived data from the Antarctic Muon and Neutrino Detector Array (AMANDA-B10). Under the assumption of associated hadronic acceleration, the expected observed neutrino energy flux is directly derived, based upon confronting the fireball phenomenology with the discrete set of observed electromagnetic parameters of GRB980703a, gleaned from ground-based and satellite observations, for four models, corrected for oscillations. Models 1 and 2, based upon spectral analysis featuring a prompt photon energy fit to the Band function, utilize an observed spectroscopic redshift, for isotropic and anisotropic emission geometry, respectively. Model 3 is based upon averaged burst parameters, assuming isotropic emission. Model 4 based upon a Band fit features an estimated redshift from the lag-luminosity relation, with isotropic emission. Consistent with our AMANDA-II analysis of GRB030329, which resulted in a flux upper limit of similar to 0.150GeV/cm(2)/s for model 1, we find differences in excess of an order of magnitude in the response of AMANDA-B10, among the various models for GRB980703a. Implications for future searches in the era of Swift and IceCube are discussed. C1 [Stamatikos, Michael] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Band, David L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Band, David L.] UMBC, JCA, Baltimore, MD 21250 USA. RP Stamatikos, M (reprint author), Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. NR 14 TC 7 Z9 7 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 599 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000111 ER PT S AU McEnery, J Ritz, S AF McEnery, Julie Ritz, Steve CA The GLAST Mission Team BE Holt, SS Gehrels, N Nousek, JA TI The Gamma-ray large area space telescope and Gamma-ray Bursts SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam ID HIGH-ENERGY AB The Gamma-ray Large Area Telescope (GLAST) is a satellite-based observatory to study the high energy gamma-ray sky. The main instrument on GLAST, the Large Area Telescope (LAT) is a pair-conversion telescope that will survey the sky from 20 MeV to greater than 300 GeV With the GLAST launch in 2007, the LAT will open a new and important window on a wide variety of high energy phenomena, including supermassive black holes and active galactic nuclei, gamma-my bursts, supernova remnants and cosmic ray acceleration and dark matter. A second instrument, the GLAST Burst Monitor (GBM), greatly enhances GLAST's capability to study GRB by providing important spectral and timing information in the 10 keV to 30 MeV range. We describe how the instruments, spacecraft and ground system work together to provide observations of gamma-ray bursts from 8 keV - 300 GeV and to provide rapid notification of bursts to the wider gamma-ray burst community. C1 [McEnery, Julie; Ritz, Steve; The GLAST Mission Team] NASA, Goddard Space Flight Ctr, Lab Astropart Phys, Mail Code 661, Greenbelt, MD 20771 USA. RP McEnery, J (reprint author), NASA, Goddard Space Flight Ctr, Lab Astropart Phys, Mail Code 661, Greenbelt, MD 20771 USA. RI McEnery, Julie/D-6612-2012 NR 2 TC 3 Z9 3 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 660 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000121 ER PT S AU Cusumano, G Campana, S Romano, P Mangano, V Moretti, A Abbey, AF Angelini, L Beardmore, AP Burrows, DN Capalbi, M Chincarini, G Citterio, O Giommi, P Goad, MR Godet, O Hartner, GD Hill, JE Kennea, JA La Parola, V Mineo, T Morris, D Nousek, JA Osborne, JP Page, K Pagani, C Perri, M Tagliaferri, G Tamburelli, F Wells, A AF Cusumano, G. Campana, S. Romano, P. Mangano, V. Moretti, A. Abbey, A. F. Angelini, L. Beardmore, A. P. Burrows, D. N. Capalbi, M. Chincarini, G. Citterio, O. Giommi, P. Goad, M. R. Godet, O. Hartner, G. D. Hill, J. E. Kennea, J. A. La Parola, V. Mineo, T. Morris, D. Nousek, J. A. Osborne, J. P. Page, K. Pagani, C. Perri, M. Tagliaferri, G. Tamburelli, F. Wells, A. BE Holt, SS Gehrels, N Nousek, JA TI In-flight calibration of the Swift XRT effective area SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE X-ray Telescope; X-ray AB The Swift X-ray Telescope is designed to make astrometric, spectroscopic and photometric observations of the X-ray emission from Gamma-Ray Bursts and their afterglows in the 0.2-10 keV energy band. Here we report some results on the in-flight calibration of the Swift XRT effective area obtained analyzing observations of cosmic sources with different the analysis of cosmic sources intrinsic spectra and using the on-ground calibration and ray-tracing simulations as a starting point. Our analysis includes the study of the effective area for different XRT operating modes. C1 [Cusumano, G.; Mangano, V.; La Parola, V.; Mineo, T.] INAF, Ist Astrofis Spaziale & Fis Cosm Palermo, Via Ugo La Malfa 153, I-90146 Palermo, Italy. [Campana, S.; Romano, P.; Moretti, A.; Chincarini, G.; Citterio, O.; Pagani, C.; Tagliaferri, G.] INAF, Osservatorio Astronom Brera, I-23807 Merate, Italy. [Abbey, A. F.; Beardmore, A. P.; Goad, M. R.; Godet, O.; Morris, D.; Osborne, J. P.; Page, K.; Wells, A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Angelini, L.; Hill, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burrows, D. N.; Kennea, J. A.; Nousek, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Capalbi, M.; Perri, M.; Tamburelli, F.] IASI Sci Data Ctr, I-00044 Frascati, Italy. [Chincarini, G.] Univ Degli Studi Milano Bicocca, Dip Fis, I-20126 Milan, Italy. [Giommi, P.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Hartner, G. D.] Max Planck Inst Extraterr Phys, Munich, Germany. [Pagani, C.] Penn State Univ, University Pk, PA 16802 USA. RP Cusumano, G (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm Palermo, Via Ugo La Malfa 153, I-90146 Palermo, Italy. OI Mineo, Teresa/0000-0002-4931-8445; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; Perri, Matteo/0000-0003-3613-4409; La Parola, Valentina/0000-0002-8087-6488; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU ASI [I/R/039/04]; NASA [NAS5-00136]; PPARC [PPA/G/S/00524, PPA/Z/S/2003/00507] FX This work is supported at OAB by ASI grant I/R/039/04, at Penn State by NASA contract NAS5-00136 and at the University of Leicester by PPARC of grants PPA/G/S/00524 and PPA/Z/S/2003/00507. We gratefully acknowledge the contributions of dozens of members of the XRT team at OAB, PSU, UL, GSFC, ASDC, and MSSL and our subcontractors, who helped make this instrument possible. NR 9 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 664 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000122 ER PT S AU Moretti, A Campana, S Capalbi, M Chincarini, G Covino, S Cusumano, G Giommi, P La Parola, V Mangano, V Mineo, T Perri, M Romano, P Tagliaferri, G AF Moretti, A. Campana, S. Capalbi, M. Chincarini, G. Covino, S. Cusumano, G. Giommi, P. La Parola, V. Mangano, V. Mineo, T. Perri, M. Romano, P. Tagliaferri, G. BE Holt, SS Gehrels, N Nousek, JA TI In-flight calibration of the swift XRT point spread function SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE swift; XRT; PSF AB The Swifi X-ray Telescope (XRT) is designed to make astrometric, spectroscopic and photometric observations of the X-ray emission from Gamma-ray bursts and their afterglows, in the energy band 0.2-10 keV. Here we report the results of the analysis of Swift XRT Point Spread Function (PSF) as measured in the first four months of the mission during the instrument calibration phase. The analysis includes the study of the PSF of different point-like sources both on-axis and off-axis with different spectral properties. We compare the in-flight data with the expectations from the on-ground calibration. On the basis of the calibration data we built an analytical model to reproduce the PSF as a function of the energy and the source position within the detector which can be applied in the PSF correction calculation for any extraction region geometry. All the results of this study are implemented in the standard public software. C1 INAF, Osserv Astron Brera, Via Bianchi 46, I-23087 Merate, LC, Italy. [Cusumano, G.; La Parola, V.; Mangano, V.; Mineo, T.] INAF, IASF, I-90146 Palermo, Italy. Univ Leicester, Leicester LE1 7RH, Leics, England. NASA, GSFC, Greenbelt, MD 20771 USA. Penn State Univ, University Pk, PA 16802 USA. [Capalbi, M.; Giommi, P.; Perri, M.] ASI ASDC, I-00044 Frascati, Italy. Max Planck Inst Extraterr Phys, Garching, Germany. RP Moretti, A (reprint author), INAF, Osserv Astron Brera, Via Bianchi 46, I-23087 Merate, LC, Italy. OI Tagliaferri, Gianpiero/0000-0003-0121-0723; Mineo, Teresa/0000-0002-4931-8445; giommi, paolo/0000-0002-2265-5003; Cusumano, Giancarlo/0000-0002-8151-1990; Perri, Matteo/0000-0003-3613-4409; La Parola, Valentina/0000-0002-8087-6488; Covino, Stefano/0000-0001-9078-5507 NR 4 TC 4 Z9 4 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 676 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000125 ER PT S AU Band, DL AF Band, David L. BE Holt, SS Gehrels, N Nousek, JA TI Burst detector sensitivity: Past, present & future SO Gamma-Ray Bursts in the Swift Era SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma-ray bursts; detectors AB I compare the burst detection sensitivity of CGRO's BATSE, Swift's BAT, the GLAST Burst Monitor (GBM) and EXIST as a function of a burst's spectrum and duration. A detector's overall burst sensitivity depends on its energy sensitivity and set of accumulations times At, these two factors shape the detected burst population. For example, relative to BATSE, the BAT's softer energy band decreases the detection rate of short hard bursts, while the BAT's longer accumulation times increase the detection rate of long, soft bursts. Consequently, Swift is detecting long, low fluence bursts (2-3 x fainter than BATSE). C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Band, DL (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 5 TC 4 Z9 4 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 704 EP 707 PG 4 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000132 ER PT S AU Beardmore, AP Godet, O Abbey, AF Osborne, JP Page, KL Wells, AA Goad, MR AF Beardmore, A. P. Godet, O. Abbey, A. F. Osborne, J. P. Page, K. L. Wells, A. A. Goad, M. R. BE Holt, SS Gehrels, N Nousek, JA TI The in-flight spectroscopic calibration of the Swift XRT CCD camera SO GAMMA-RAY BURSTS IN THE SWIFT ERA SE AIP Conference Proceedings LA English DT Proceedings Paper CT 16th Annual Astrophysics Conference CY NOV 29-DEC 02, 2005 CL Washington, DC SP NASA, Goddard Space Flight Ctr, Univ Maryland, Gen Dynam DE gamma-ray bursts AB The Swift X-ray Telescope (XRT) focal plane camera houses a front-illuminated MOS CCD, providing a spectral response of 145 eV FWHM at 5.9 keV. We describe the status of the CCD X-ray spectral redistribution matrices, which are made using a Monte-Carlo simulation technique based on physical models of the CCD response. We emphasize how the model has been refined following in-flight experience with celestial and on-board calibration sources. Residuals less than 10% are typically observed for astrophysical sources. C1 [Beardmore, A. P.; Godet, O.; Abbey, A. F.; Osborne, J. P.; Page, K. L.; Wells, A. A.; Goad, M. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. NASA, GSFC, Greenbelt, MD 20771 USA. Penn State Univ, University Pk, PA 16802 USA. INAF, Osservatorio Brera, I-23807 Merate, LC, Italy. INAF, IASF, I-90146 Palermo, Italy. ASI ASDC, I-00044 Frascati, Italy. USRA, Columbia, MD 21044 USA. RP Beardmore, AP (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. NR 4 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 0-7354-0326-0 J9 AIP CONF PROC PY 2006 VL 836 BP 708 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEM37 UT WOS:000238125000133 ER PT B AU Hornby, GS AF Hornby, Gregory S. BE Keijzer, M TI ALPS: The age-layered population structure for reducing the problem of premature convergence SO GECCO 2006: GENETIC AND EVOLUTIONARY COMPUTATION CONFERENCE, VOL 1 AND 2 LA English DT Proceedings Paper CT 8th Annual Genetic and Evolutionary Computation Conference CY JUL 08-12, 2006 CL Seattle, WA SP ACM SIGEVO DE age; computer-automated design; premature convergence; evolutionary algorithms; open-ended design AB To reduce the problem of premature convergence we define a new method for measuring an individual's age and propose the Age-Layered Population Structure (ALPS). This new measure of age measures how long the genetic material has been evolving in the population: offspring start with an age of 1 plus the age of their oldest parent instead of starting with an age of 0 as with traditional measures of age. ALPS differs from a typical evolutionary algorithm (EA) by segregating individuals into different age-layers by their age and by regularly introducing new, randomly generated individuals in the youngest layer. The introduction of randomly generated individuals at regular intervals results in an EA that is never completely converged and is always exploring new parts of the fitness landscape. By using age to restrict competition and breeding, younger individuals are able to develop without being dominated by older ones. Analysis of the search behavior of ALPS finds that the offspring of individuals that are randomly generated mid-way through a run are able to move the population out of mediocre local-optima to better parts of the fitness landscape. In comparison against a traditional EA, a multi-start EA and two other EAs with diversity maintenance schemes we find that ALPS produces significantly better designs with a higher reliability than the other EAs. C1 Univ Calif Santa Cruz, Univ Affiliated Res Ctr, NASA, Ames Res Ctr, Moffett Field, CA USA. RP Hornby, GS (reprint author), Univ Calif Santa Cruz, Univ Affiliated Res Ctr, NASA, Ames Res Ctr, Mailstop 269-3, Moffett Field, CA USA. EM hornby@email.arc.nasa.gov NR 18 TC 17 Z9 17 U1 0 U2 1 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 1515 BROADWAY, NEW YORK, NY 10036-9998 USA BN 978-1-59593-186-3 PY 2006 BP 815 EP 822 PG 8 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering SC Computer Science GA BGR10 UT WOS:000249917300124 ER PT B AU Agogino, A Turner, K AF Agogino, Adrian Turner, Kagan BE Keijzer, M TI Distributed evaluation functions for fault tolerant multi-rover systems SO GECCO 2006: Genetic and Evolutionary Computation Conference, Vol 1 and 2 LA English DT Proceedings Paper CT 8th Annual Genetic and Evolutionary Computation Conference CY JUL 08-12, 2006 CL Seattle, WA SP ACM SIGEVO DE multiagent; systems; robust optimization; genetic algorithms; neural networks AB The ability to evolve fault tolerant control strategies for large collections of agents is critical to the successful application of evolutionary strategies to domains where failures are common. Furthermore, while evolutionary algorithms have been highly successful in discovering single-agent control strategies, extending such algorithms to multi-agent domains has proven to be difficult. In this paper we present a method for shaping evaluation functions for agents that provide control strategies that are both tolerant to different types of failures and lead to coordinated behavior in a multi-agent setting. This method neither relies on a centralized strategy (susceptible to single points of failures) nor a distributed strategy where each agent uses a system wide evaluation function (severe credit assignment problem). In a multi-rover problem, we show that agents using our agent-specific evaluation perform up to 500% better than agents using the system evaluation. In addition we show that agents are still able to maintain a high level of performance when up to 60% of the agents fail due to actuator, communication or controller faults. C1 UC Santa Cruz, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Agogino, A (reprint author), UC Santa Cruz, NASA, Ames Res Ctr, Mailstop 269-3, Moffett Field, CA 94035 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 1515 BROADWAY, NEW YORK, NY 10036-9998 USA BN 978-1-59593-186-3 PY 2006 BP 1079 EP 1086 PG 8 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering SC Computer Science GA BGR10 UT WOS:000249917300151 ER PT J AU Gao, CJ Zhang, SN AF Gao, CJ Zhang, SN TI Higher dimensional Reissner-Nordstrom-FRW metric SO GENERAL RELATIVITY AND GRAVITATION LA English DT Article DE black hole; charge ID BLACK-HOLES; SPACE-TIME AB By inspecting some known solutions to Einstein's equations, we present the metric of higher dimensional Reissner-Nordstrom black hole in the background of a Friedman-Robertson-Walker universe. Then we verify the solution with a perfect fluid. The discussion of the event horizon of the black hole reveals that the scale of the black hole would increase with the expansion of the universe and decrease with the contraction of the universe. C1 Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. NASA, George C Marshall Space Flight Ctr, Space Sci Lab, Huntsville, AL 35812 USA. Chinese Acad Sci, Inst High Energy Phys, Lab Particle Astrophys, Beijing 100039, Peoples R China. RP Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. EM gaocj@mail.tsinghua.edu.cn; zhangsn@mail.tsinghua.edu.cn NR 28 TC 8 Z9 8 U1 0 U2 2 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0001-7701 EI 1572-9532 J9 GEN RELAT GRAVIT JI Gen. Relativ. Gravit. PD JAN PY 2006 VL 38 IS 1 BP 23 EP 32 DI 10.1007/s10714-005-0207-8 PG 10 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 002GX UT WOS:000234600600003 ER PT B AU Lohn, JD Hornby, GS Linden, DS AF Lohn, JD Hornby, GS Linden, DS BE Yu, T Riolo, R Worzel, B TI Rapid re-evolution of an X-band antenna for NASA'S Space Technology 5 mission SO GENETIC PROGRAMMING THEORY AND PRACTICE III SE GENETIC PROGRAMMING SERIES LA English DT Proceedings Paper CT 3rd Workshop on Genetic Programming, Theory and Practice CY MAY 12-14, 2005 CL Ann Arbor, MI DE design; computational design; evolutionary design; antenna; spacecraft AB One of the challenges in engineering design is adapting a set of created designs to a change in requirements. Previously we presented two four-arm, symmetric, evolved antennas for NASA's Space Technology 5 mission. However, the mission's orbital vehicle was changed, putting it into a much lower earth orbit, changing the specifications for the mission. With minimal changes to our evolutionary system, mostly in the fitness function, we were able to evolve antennas for the new mission requirements and, within one month of this change, two new antennas were designed and prototyped. Both antennas were tested and both had acceptable performance compared with the new specifications. This rapid response shows that evolutionary design processes are able to accommodate new requirements quickly and with minimal human effort. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. QSS Grp Inc, Fairfax, VA 22031 USA. JEM Engineerin, Laurel, MD 20707 USA. RP NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. FU Mission and Science Measurement Technology, NASA Headquarters; Ken Perko of Microwave Systems Branch at NASA Goddard and Bruce Blevins of the Physical Science Laboratory at New Mexico State University FX The work described in this paper was supported by Mission and Science Measurement Technology, NASA Headquarters, under its Computing, Information, and Conmiunications Technology Program. The work was performed at the Computational Sciences Division, NASA Ames Research Center, Linden Innovation Research and JEM Engineering, and NASA Goddard Space Flight Center. The support of Ken Perko of Microwave Systems Branch at NASA Goddard and Bruce Blevins of the Physical Science Laboratory at New Mexico State University is gratefully acknowledged. NR 6 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES BN 0-387-28110-X J9 GENET PROGR SER PY 2006 VL 9 BP 65 EP + DI 10.1007/0-387-28111-8_5 PG 2 WC Computer Science, Artificial Intelligence; Computer Science, Theory & Methods SC Computer Science GA BDP91 UT WOS:000234830700005 ER PT S AU Raskin, R AF Raskin, Rob BE Sinha, AK TI Development of ontologies for earth system science SO GEOINFORMATICS: DATA TO KNOWLEDGE SE Geological Society of America Special Papers LA English DT Article; Book Chapter DE ontology; metadata; earth system science; knowledge representation AB The Semantic Web for Earth and Environmental Terminology ( SWEET) is a NASA-funded prototype to explore the technological challenges in making the semantic Web a reality for earth system science data and information. SWEET includes an extensive collection of ontologies written in the Ontology Web Language ( OWL). These ontologies encompass both faceted (decomposed) concepts and integrative ( unifying) concepts. Taken together, these enable a representation of the two science processes of reductionism and synthesis. SWEET stores ontology elements optionally in a DBMS (database management system), with a two-way translator between the XML and DBMS representations. SWEET also includes wrappers for large external online databases (gazetteers, earthquakes, etc.) to enable their contents be virtual components of the ontologies (http://sweet.jpl.nasa.gov). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Raskin, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 TC 4 Z9 4 U1 0 U2 1 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2397-6 J9 GEOL SOC AM SPEC PAP PY 2006 VL 397 BP 195 EP 199 DI 10.1130/2006.2397(14) PG 5 WC Computer Science, Information Systems; Computer Science, Interdisciplinary Applications; Geology; Geosciences, Multidisciplinary SC Computer Science; Geology GA BLX56 UT WOS:000271295900015 ER PT S AU Benson, RF Webb, PA Green, JL Carpenter, DL Sonwalkar, VS James, HG Reinisch, BW AF Benson, RF Webb, PA Green, JL Carpenter, DL Sonwalkar, VS James, HG Reinisch, BW BE Labelle, JW Treumann, RA TI Active wave experiments in space plasmas: The Z mode SO GEOSPACE ELECTROMAGNETIC WAVES AND RADIATION SE Lecture Notes in Physics LA English DT Proceedings Paper CT Ringberg Workshop on High Frequency Waves in Geospace CY JUL 11-14, 2004 CL Ringberg, GERMANY SP INt Space Sci Inst Bern DE auroral kilometric radiation; Z-mode; free space radiation; wave transformation; radiation escape; cavity modes; active experiments ID ELECTRON-DENSITY IRREGULARITIES; IONOSPHERIC TOPSIDE SOUNDERS; MAGNETIC-FIELD; UPPER-HYBRID; PROPAGATION EXPERIMENTS; ANISOTROPIC PLASMA; MEDIUM FREQUENCIES; RAY TRAJECTORIES; AURORAL HISS; RADIO AB The term Z mode is space physics notation for the low-frequency branch of the extraordinary (X) mode. It is an internal, or trapped, mode of the plasma confined in frequency between the cutoff frequency f(z) and the upper-hybrid frequency f(uh) which is related to the electron plasma frequency f(pe) and the electron cyclotron frequency fee by the expression f(uh)(2) = f(pe)(2) + f(ce)(2); f(z) and f(ce). These characteristic frequencies are directly related to the electron number density N-e and the magnetic field strength vertical bar B vertical bar, i.e., f(pe)(kHz)(2) approximate to 80.6N(e)(cm(-3)) and f(ce)(kHz)(2) approximate to 0.028 vertical bar B vertical bar(nT). The Z mode is further classified as slow or fast depending on whether the phase velocity is lower or higher than the speed of light in vacuum. The Z mode provides a link between the short wavelength lambda (large wave number k = 2 pi/lambda) electrostatic (es) domain and the long lambda (small k) electromagnetic (em) domain. An understanding of the generation, propagation and reception of Z-mode waves in space plasma leads to fundamental information on wave/particle interactions, N-e, and field-aligned N-e irregularities (FAI) in both active and passive wave experiments. Here we review Z-mode observations and their interpretations from both radio sounders on rockets and satellites and from plasma-wave receivers on satellites. The emphasis will be on the scattering and ducting of sounder-generated Z-mode waves by FAI and on the passive reception of Z-mode waves generated by natural processes such is Cherenkov and cyclotron emission. The diagnostic applications of the observations to understanding ionospheric and magnetospheric plasma processes and structures benefit from the complementary nature of passive and active plasma-wave experiments. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Stanford Univ, Stanford, CA 94305 USA. Univ Alaska, Fairbanks, AK 99701 USA. Commun Res Ctr, Toronto, ON, Canada. Univ Massachusetts, Lowell, MA USA. RP NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Robert.F.Benson@nasa.gov; pwebb@pop600.gsfc.nasa.gov; James.L.Green@nasa.gov; dlc@nova.stanford.edu; ffvss@uaf.edu; gordon.james@crc.ca FU NASA [NNG04GI67G, 83822]; SwRI FX We are grateful to the reviewer for many helpful comments on the manuscript. The work at the University of Alaska Fairbanks was supported by NASA under contract NNG04GI67G. Support for B. W. R. was provided by NASA under subcontract 83822 from SwRI. NR 69 TC 10 Z9 10 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0075-8450 BN 3-540-30050-3 J9 LECT NOTES PHYS PY 2006 VL 687 BP 3 EP + PG 6 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BED15 UT WOS:000236865000001 ER PT J AU Tilton, JC Lawrence, WT Plaza, AJ AF Tilton, James C. Lawrence, William T. Plaza, Antonio J. TI Utilizing hierarchical segmentation to generate water and snow masks to facilitate monitoring change with remotely sensed image data SO GISCIENCE & REMOTE SENSING LA English DT Article AB The hierarchical segmentation (HSEG) algorithm is a hybrid of hierarchical step-wise optimization and constrained spectral clustering that produces a hierarchical set of image segmentations. This segmentation hierarchy organizes image data in a manner that makes the image's information content more accessible for analysis by enabling region-based analysis. This paper discusses data analysis with HSEG and describes several measures of region characteristics that may be useful analyzing segmentation hierarchies for various applications. Segmentation hierarchy analysis for generating land/water and snow/ice masks from MODIS (Moderate Resolution Imaging Spectroradiometer) data was demonstrated and compared with the corresponding MODIS standard products. The masks based on HSEG segmentation hierarchies compare very favorably to the MODIS standard products. Further, the HSEG based land/water mask was specifically tailored to the MODIS data and the HSEG snow/ice mask did not require the setting of a critical threshold as required in the production of the corresponding MODIS standard product. C1 NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Greenbelt, MD 20771 USA. Bowie State Univ, Dept Nat Sci, Bowie, MD 20715 USA. Univ Extremadura, Dept Comp Sci, E-10071 Caceres, Spain. RP Tilton, JC (reprint author), NASA, Goddard Space Flight Ctr, Computat & Informat Sci & Technol Off, Mail Code 606-3, Greenbelt, MD 20771 USA. EM James.C.Tilton@nasa.gov RI Plaza, Antonio/C-4455-2008 OI Plaza, Antonio/0000-0002-9613-1659 NR 8 TC 10 Z9 10 U1 0 U2 2 PU BELLWETHER PUBLISHING LTD PI COLUMBIA PA 8640 GUILFORD RD, STE 200, COLUMBIA, MD 21046 USA SN 1548-1603 J9 GISCI REMOTE SENS JI GISci. Remote Sens. PD JAN-MAR PY 2006 VL 43 IS 1 BP 39 EP 66 DI 10.2747/1548-1603.43.1.39 PG 28 WC Geography, Physical; Remote Sensing SC Physical Geography; Remote Sensing GA 132HW UT WOS:000243934900003 ER PT S AU Miller, AJ Gabric, AJ Moisan, JR Chai, F Neilson, DJ Pierce, DW Di Lorenzo, E AF Miller, Arthur J. Gabric, Albert J. Moisan, John R. Chai, Fei Neilson, Douglas J. Pierce, David W. Di Lorenzo, Emanuele BE Kawahata, H Awaya, Y TI Global Change and Oceanic Primary Productivity: Effects of Ocean-Atmosphere-Biological Feedbacks SO GLOBAL CLIMATE CHANGE AND RESPONSE OF CARBON CYCLE IN THE EQUATORIAL PACIFIC AND INDIAN OCEANS AND ADJACENT LANDMASSES SE Elsevier Oceanography Series LA English DT Article; Book Chapter DE global change; climate feedbacks; ocean ecosystem; Pacific ocean; physical-biological interactions ID CALIFORNIA CURRENT SYSTEM; EQUATORIAL PACIFIC-OCEAN; ANTARCTIC SOUTHERN-OCEAN; GENERAL-CIRCULATION MODELS; SEA-SURFACE TEMPERATURE; CARBON-CYCLE FEEDBACKS; CLIMATE-CHANGE; MIXED-LAYER; DIMETHYL SULFIDE; COASTAL OCEAN AB Our current understanding of how climate change due to increasing greenhouse gases is expected to affect oceanic biology and of how the physical-biological feedbacks may influence the evolving physical climate system is summarized. The primary effects of ocean biology on physical climate include its influence on the carbon cycle, the influence of oceanic phytoplankton on upper-ocean absorption, and the influence of DMS production by phytoplankton on atmospheric aerosols. The primary influences of physical climate on the ocean biology are the influence of aoelian dust deposition and the multitude of ways that community structure can be altered. The focus is on the tropical and midlatitude Pacific Ocean, with results from other ocean basins also noted. C1 [Miller, Arthur J.; Neilson, Douglas J.; Pierce, David W.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Gabric, Albert J.] Griffith Univ, Nathan, Qld 4111, Australia. [Moisan, John R.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. [Chai, Fei] Univ Maine, Sch Marine Sci, Orono, ME 04469 USA. [Di Lorenzo, Emanuele] Georgia Inst Technol, Atlanta, GA 30332 USA. RP Miller, AJ (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM ajmiller@ucsd.edu NR 139 TC 1 Z9 1 U1 3 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0422-9894 BN 978-0-08-046941-6; 978-0-444-52948-0 J9 ELSEV OCEANOGR SERIE JI Elsevier Oceanogr. Ser. PY 2006 VL 73 BP 27 EP 63 PG 37 WC Ecology; Environmental Sciences; Oceanography SC Environmental Sciences & Ecology; Oceanography GA BCT53 UT WOS:000311358100002 ER PT S AU Cheng, MK Moision, BE Hamkins, J Nakashima, MA AF Cheng, Michael K. Moision, Bruce E. Hamkins, Jon Nakashima, Michael A. GP IEEE TI Implementation of a Coded Modulation for Deep Space Optical Communications SO GLOBECOM 2006 - 2006 IEEE GLOBAL TELECOMMUNICATIONS CONFERENCE SE IEEE Global Telecommunications Conference (Globecom) LA English DT Proceedings Paper CT IEEE Global Telecommunications Conference (GLOBECOM 06) CY NOV 27-DEC 01, 2006 CL San Francisco, CA SP IEEE Commun Soc AB We present an efficient implementation of a coded modulation for the deep space optical channel. NASA designed this so called serially concatenated pulse position modulation (SCPPM) code to provide an optical link that can operate within one dB signal energy of the Shannon capacity during a nominal mission condition from Mars. Here, we describe some of the challenges in realizing the SCPPM decoder on a field-programmable gate array (FPGA). Through various architectural optimizations, we achieve a 6 Mbps decoder on a single FPGA. Moreover, we demonstrate that it is possible to communicate reliably on an efficient bits-per-photon count in an end-to-end SCPPM coded system.(1) C1 [Cheng, Michael K.; Moision, Bruce E.; Hamkins, Jon; Nakashima, Michael A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cheng, MK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1930-529X BN 978-1-4244-0356-1 J9 GLOB TELECOMM CONF PY 2006 PG 5 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BUC00 UT WOS:000288765602151 ER PT S AU Chowdhury, PK Atiquzzaman, M Ivancic, W AF Chowdhury, Pulak K. Atiquzzaman, Mohammed Ivancic, William GP IEEE TI Performance of End-to-End Mobility Management in Satellite IP Networks SO GLOBECOM 2006 - 2006 IEEE GLOBAL TELECOMMUNICATIONS CONFERENCE SE IEEE Global Telecommunications Conference (Globecom) LA English DT Proceedings Paper CT IEEE Global Telecommunications Conference (GLOBECOM 06) CY NOV 27-DEC 01, 2006 CL San Francisco, CA SP IEEE Commun Soc (ComSoc) AB IETF has developed Mobile IP to support mobility of IP hosts at the network layer. The National Aeronautics and Space Administration has implemented Mobile IP to handle handovers in space networks. Due to a number of limitations of Mobile IP, such as high handover latency, packet loss rate, and conflict with existing network security solutions, a new IP-diversity based mobility management scheme, called SIGMA, has been developed through collaborative efforts of NASA and University of Oklahoma. In this paper, we illustrate the performance of SIGMA for managing handovers in space networks. We show by simulation that SIGMA extends network connectivity from space to ground, and ensures smooth handover between spacecrafts for different space network scenarios. C1 [Chowdhury, Pulak K.; Atiquzzaman, Mohammed] Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA. [Ivancic, William] NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. RP Chowdhury, PK (reprint author), Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA. EM pulak@ou.edu; atiq@ou.edu; wivancic@grc.nasa.gov FU NASA [NAG3-2922] FX The research reported in this paper was funded by NASA Grant NAG3-2922. NR 11 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1930-529X BN 978-1-4244-0356-1 J9 GLOB TELECOMM CONF PY 2006 PG 5 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BUC00 UT WOS:000288765602147 ER PT S AU Divsalar, D Jones, C AF Divsalar, Dariush Jones, Christopher GP IEEE TI Protograph LDPC Codes with Node Degrees at Least 3 SO GLOBECOM 2006 - 2006 IEEE GLOBAL TELECOMMUNICATIONS CONFERENCE SE IEEE Global Telecommunications Conference (Globecom) LA English DT Proceedings Paper CT IEEE Global Telecommunications Conference (GLOBECOM 06) CY NOV 27-DEC 01, 2006 CL San Francisco, CA SP IEEE Commun Soc ID PARITY-CHECK CODES; CAPACITY AB In this paper we present protograph codes with degree-3 nodes and one high degree node. The iterative decoding threshold for proposed rate 1/2 codes are lower, by about 0.2 dB, than the best known irregular LDPC codes with degree at least 3. The main motivation is to construct rate-compatible protograph-based LDPC codes for fixed code block length (n) that simultaneously achieve low iterative decoding thresholds and guarantee minimum distance that is linearly increasing with n. We start with a rate 1/2 protograph LDPC code with degree-3 nodes and one high degree node. Higher rate codes are obtained by connecting check nodes with degree-2 non-transmitted nodes. This is equivalent to constraint combining in the protograph. The condition where all constraints are combined corresponds to the highest rate code. Through examples we show that iterative decoding thresholds as low as 0.544 dB can be achieved for small protographs with node degrees at least three. FPGA simulation results show that the proposed family of codes perform as predicted. C1 [Divsalar, Dariush; Jones, Christopher] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Divsalar, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Dariush.Divsalar@jpl.nasa.gov; christop@jpl.nasa.gov NR 22 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1930-529X BN 978-1-4244-0356-1 J9 GLOB TELECOMM CONF PY 2006 PG 5 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BUC00 UT WOS:000288765600073 ER PT S AU Hamkins, J AF Hamkins, Jon GP IEEE TI Modulation Classification of MPSK for Space Applications SO GLOBECOM 2006 - 2006 IEEE GLOBAL TELECOMMUNICATIONS CONFERENCE SE IEEE Global Telecommunications Conference (Globecom) LA English DT Proceedings Paper CT IEEE Global Telecommunications Conference (GLOBECOM 06) CY NOV 27-DEC 01, 2006 CL San Francisco, CA SP IEEE Commun Soc DE Detection and Estimation; Classification AB Space missions are being developed with increasing levels of autonomy, as a means to increase their science return, fault-tolerance, and longevity. In this paper, we present NASA's low-complexity techniques to autonomously identify the modulation order of an M-ary phase-shift-keying signal in the presence of additive white Gaussian noise. This is part of a larger program to develop an autonomous radio that receives a signal without a priori knowledge of its modulation type, modulation index, data rate, and pulse shape. For classification between binary and quaternary phase-shift keying, these techniques represent a lopsided trade-off in which a factor of 100 reduction in complexity results in less than a 0.2 dB loss in performance relative to the maximum likelihood modulation classifier. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Hamkins, J (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM jon.hamkins@jpl.nasa.gov NR 11 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1930-529X BN 978-1-4244-0356-1 J9 GLOB TELECOMM CONF PY 2006 PG 5 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BUC00 UT WOS:000288765602099 ER PT S AU Green, JL Boardsen, S AF Green, James L. Boardsen, Scott BE Clauer, CR Siscoe, G TI Duration and extent of the great auroral storm of 1859 SO GREAT HISTORICAL GEOMAGNETIC STORM OF 1859: A MODERN LOOK SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT Workshop on the 1859 Carrington Storm CY OCT, 2003 CL Univ Michigan, Ann Arbor, MI HO Univ Michigan DE Carrington event; Carrington event aurora AB The great geomagnetic storm of August 28 through September 3, 1859 is, arguably, the greatest and most famous space weather event in the last two hundred years. For the first time observations showed that the sun and aurora were connected and that auroras generated strong ionospheric currents. A significant portion of the world's 200,000 kin of telegraph lines were adversely affected, many of which were unusable for 8 It or more which had a real economic impact. In addition to published scientific measurements, newspapers, ship logs, and other records of that era provide an untapped wealth of first hand observations giving time and location along with reports of the auroral forms and colors. At its height, the aurora was described as a blood or deep crimson red that was so bright that one "could read a newspaper by." At its peak, the Type A red aurora lasted for several hours and was observed to reach extremely low geomagnetic latitudes on August 28-29 (similar to 25 degrees) and on September 2-3 (similar to 18 degrees). Auroral forms of all types and colors were observed below 50 degrees latitude for similar to 24 h on August 28-29 and similar to 42 h on September 2-3. From a large database of ground-based observations the extent of the aurora in corrected geomagnetic coordinates is presented over the duration of the storm event. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Goddard Space Flight Ctr, GSI, Greenbelt, MD 20771 USA. RP Green, JL (reprint author), NASA, Goddard Space Flight Ctr, GSI, Greenbelt, MD 20771 USA. EM James.Green@nasa.gov FU Headquarters NASA; Intramural NASA [N-999999]; Science Planetary Science NASA NR 19 TC 28 Z9 29 U1 0 U2 3 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2006 VL 38 IS 2 BP 130 EP 135 DI 10.1016/j.asr.2005.08.054 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFL06 UT WOS:000242567000002 PM 28066122 ER PT S AU Green, JL Boardsen, S Odenwald, S Humble, J Pazamickas, KA AF Green, James L. Boardsen, Scott Odenwald, Sten Humble, John Pazamickas, Katherine A. BE Clauer, CR Siscoe, G TI Eyewitness reports of the great auroral storm of 1859 SO GREAT HISTORICAL GEOMAGNETIC STORM OF 1859: A MODERN LOOK SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT Workshop on the 1859 Carrington Storm CY OCT, 2003 CL Univ Michigan, Ann Arbor, MI HO Univ Michigan DE Carrington event; Carrington event aurora; eyewitness reports; great aurora AB The great geomagnetic storm of 1859 is really composed of two closely spaced massive worldwide auroral events. The first event began on August 28th and the second began on September 2nd. It is the storm on September 2nd that results from the Carrington-Hodgson white light flare that occurred on the sun September 1st. In addition to published scientific measurements; newspapers, ship logs, and other records of that era provide an untapped wealth of first hand observations giving time and location along with reports of the auroral forms and colors. At its height, the aurora was described as a blood or deep crimson red that was so bright that one "could read a newspaper by". Several important aspects of this great geomagnetic storm are simply phenomenal. Auroral forms of all types and colors were observed to geographic latitudes of 25 degrees and lower. Significant portions of the world's 125,000 miles of telegraph lines were also adversely affected. Many of which were unusable for 8 h or more and had a small but notable economic impact. This paper presents only a select few available first hand accounts of the Great Auroral Event of 1859 in an attempt to give the modern reader a sense of how this spectacular display was received by the public from many places around the globe and present some other important historical aspects of the storm. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Commun SCI, Greenbelt, MD 20771 USA. QSS Grp Inc, Lanham, MD 20706 USA. Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. Lycoming Coll, Williamsport, PA 17701 USA. RP Green, JL (reprint author), NASA, Goddard Space Flight Ctr, Commun SCI, L3, Greenbelt, MD 20771 USA. EM James.Green@nasa.gov NR 46 TC 11 Z9 11 U1 0 U2 2 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2006 VL 38 IS 2 BP 145 EP 154 DI 10.1016/j.asr.2005.12.021 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFL06 UT WOS:000242567000004 ER PT S AU Li, XL Temerin, M Tsurutani, BT Alex, S AF Li, Xinlin Temerin, M. Tsurutani, B. T. Alex, S. BE Clauer, CR Siscoe, G TI Modeling of 1-2 September 1859 super magnetic storm SO GREAT HISTORICAL GEOMAGNETIC STORM OF 1859: A MODERN LOOK SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT Workshop on the 1859 Carrington Storm CY OCT, 2003 CL Univ Michigan, Ann Arbor, MI HO Univ Michigan DE Carrington event; magnetic storms; magnetic storm modeling; modeling the 1-2 September 1859 magnetic storm ID SEMIANNUAL VARIATION; GEOMAGNETIC-ACTIVITY; JANUARY 1997; SOLAR-WIND; CLOUD; DST AB Based on an estimated solar wind condition around 1-2 September 1859, we were able to reproduce the Carrington magnetic storm magnetometer record, with the H-component depression of -1600 nT, made at Colaba Observatory in Mumbai, India. We used an updated Dst prediction model from Temerin and Li (2002), which provides a prediction efficiency of 0.91 for 1995-2002 interval using a fixed set of modeling parameters. The negative depression in the magnetometer record could be explained by assumptions as to the condition of the solar wind that, though far more geoeffective than any that have ever been observed, do not seem improbable given the known average speed of the interplanetary shock for this event. The extremely fast recovery of the magnetometer record, however, required that the dynamic pressure of the solar wind also be substantially larger than has ever been observed. We also showed how the strength of the magnetic storm would have depended on the season and the time of day. For the same solar wind conditions in GSM coordinates, the largest magnetic storms occur around the fall equinox and at the time of day when the dipole axis is most perpendicular to the solar wind velocity. Given the assumed very fast solar wind with a very large negative interplanetary magnetic field (IMF) B-z directly impacting the Earth, our model together with the known magnetometer record indicates that a super magnetic storm with minimum Dst less than -1600 nT could have occurred and thus can occur again. For the magnetic storm of 1-2 September 1859, however, the extremely fast recovery of Dst requires an extremely large pressure enhancement. This suggests that this particular event was doubly unusual. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Colorado, Dept Aerosp Engn Sci, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Indian Inst Geomagnetism, Bombay 400005, Maharashtra, India. Chinese Acad Sci, Lab Space Weather, Beijing 100080, Peoples R China. RP Li, XL (reprint author), Univ Colorado, Dept Aerosp Engn Sci, Atmospher & Space Phys Lab, 1234 Innovat Dr, Boulder, CO 80303 USA. EM lix@lasp.colorado.edu NR 20 TC 22 Z9 24 U1 0 U2 3 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 2 BP 273 EP 279 DI 10.1016/j.asr.2005.06.070 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFL06 UT WOS:000242567000018 ER PT S AU Odenwald, S Green, J Taylor, W AF Odenwald, Sten Green, James Taylor, William BE Clauer, CR Siscoe, G TI Forecasting the impact of an 1859-calibre superstorm on satellite resources SO GREAT HISTORICAL GEOMAGNETIC STORM OF 1859: A MODERN LOOK SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT Workshop on the 1859 Carrington Storm CY OCT, 2003 CL Univ Michigan, Ann Arbor, MI HO Univ Michigan DE space weather; Satellite anomalies; Satellite failures; technology impacts; superstorms; radiation sickness; economic impacts ID PROTON EVENT FLUENCES; COSMIC-RAY EVENTS; PROBABILITY MODEL; SOLAR AB We have developed simple models to assess the economic impacts to the current satellite resource caused by the worst-case scenario of a hypothetical superstorm event occurring during the next sunspot cycle. Although the consequences may be severe, our worse-case scenario does not include the complete failure of the entire 937 operating satellites in the current population, which have a replacement value of similar to$170-230 billion, and supporting a similar to$90 billion/year industry. Our estimates suggest a potential economic loss of <$70 billion for lost revenue (similar to$44 billion) and satellite replacement for GEO satellites (similar to$24 billion) caused by a 'once a century' single storm similar to the 1859 superstorm. We estimate that 80 satellites (LEO, MEO, and GEO) may be disabled as a consequence of a superstorm event. Additional impacts may include the failure of many of the GPS, GLONASS, and Galileo satellite systems in MEO. Approximately 97 LEO satellites, which normally would not have re-entered for many decades, may prematurely de-orbit by ca 2021 as a result of the temporarily increased atmospheric drag caused by a superstorm event occurring in ca. 2012. The $100 billion International Space Station may lose significant altitude, placing it in critical need for re-boosting by an amount potentially outside the range of typical Space Shuttle operations, which are in any case scheduled to end in 2010. Currently, the ability to forecast extreme particle events and coronal mass ejections, or predict their fluences and geoseverity in the 24-h prior to the event, appears to be no better than 50/50. Our analysis of economic impacts is a first attempt at estimation whose approach will suggest ways in which better estimates may eventually be obtained. (c) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 QSS Grp Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Odenwald, S (reprint author), QSS Grp Inc, 4500 Forbes Blvd, Lanham, MD 20706 USA. NR 61 TC 20 Z9 21 U1 0 U2 2 PU ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD 0X5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2006 VL 38 IS 2 BP 280 EP 297 DI 10.1016/j.asr.2005.10.046 PG 18 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFL06 UT WOS:000242567000019 ER PT S AU Mainzer, AK Young, E Hong, J Hinz, P Werner, M Gorjan, V Ressler, ME AF Mainzer, A. K. Young, Erick Hong, John Hinz, Phil Werner, Mike Gorjan, Varoujan Ressler, Michael E. BE Mclean, IS Iye, M TI MegaMIR: A Fizeau thermal infrared camera for the LBTI - art. no. 626910 SO Ground-based and Airborne Instrumentation for Astronomy, Pts 1- 3 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Ground-Based and Airborne Instrumentation for Astronomy CY MAY 25-29, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon ID STAR-FORMATION; BETA-PICTORIS; RESOLUTION; GALAXIES; GLIMPSE; DISK AB The Megapixel Mid-infrared Instrument (MegaMIR) is a proposed Fizeau-mode camera for the Large Binocular Telescope operating at wavelengths between 5 and 28 mu m. The camera will be used in conjunction with the Large Binocular Telescope Interferometer (LBTI), a cryogenic optical system that combines the beams from twin 8.4-m telescopes in a phase coherent manner. Unlike other interferometric systems, the co-mounted telescopes on the LBT satisfy the sine condition, providing diffraction-limited resolution over the 40" field of view of the camera. With a 22.8-m baseline, MegaMIR will yield 0.1" angular resolution, making it the highest resolution wide field imager in the thermal infrared for at least the next decade. MegaMIR will utilize a newly developed 1024 x 1024 pixel Si:As detector array that has been optimized for use at high backgrounds. This new detector is a derivative of the Wide-field Infrared Survey Explorer (WISE) low-background detector. The combination of high angular resolution and Wide field imaging will be a unique scientific capability for astronomy. Key benefits will be realized in planetary science, galactic, and extra-galactic astronomy. High angular resolution is essential to disentangle highly complex sources, particularly in star formation regions and external galaxies, and MegaMIR provides this performance over a full field of view. Because of the great impact being made by space observatories like the Spitzer Space Telescope, the number of available targets for study has greatly increased in recent years, and MegaMIR will allow efficient follow up science. C1 Jet Prop Lab, Pasadena, CA 91109 USA. RP Mainzer, AK (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 26 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 0-8194-6334-5 J9 P SOC PHOTO-OPT INS PY 2006 VL 6269 BP 26910 EP 26910 AR 626910 DI 10.1117/12.670380 PN 1-3 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Spectroscopy SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Spectroscopy GA BEZ53 UT WOS:000240348500035 ER PT S AU Ennico, KA Keller, LD Mar, DJ Herter, TL Jaffe, DT Adams, JD Greene, TP AF Ennico, K. A. Keller, L. D. Mar, D. J. Herter, T. L. Jaffe, D. T. Adams, J. D. Greene, T. P. BE Mclean, IS Iye, M TI Grism performance for mid-infrared (5-40 micron) spectroscopy - art. no. 62691Q SO Ground-based and Airborne Instrumentation for Astronomy, Pts 1- 3 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Ground-Based and Airborne Instrumentation for Astronomy CY MAY 25-29, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE infrared; grisms; spectrograph; silicon; KRS-5; SOFIA; FORCAST ID POLYCYCLIC AROMATIC-HYDROCARBONS; INFRARED-SPECTROSCOPY; IMMERSION GRATINGS; SILICON GRISMS; SPECTROMETER; FABRICATION; TELESCOPE; ASTRONOMY; EMISSION; IMAGER AB This paper addresses the performance of a suite of grisms as part of an Astrobiology Science and Instrument Development (ASTID) Program to implement a moderate resolution spectroscopic capability in the mid/far-IR facility instrument FORCAST for the Stratospheric Observatory For Infrared Astronomy (SOFIA). A moderate resolution mid-IR spectrometer on SOFIA will offer advantages not available to either ground or space-based instruments after the Spitzer Space Telescope ceases operation in similar to 2008. SOFIA will begin operations in 2008 and will have an operational lifetime of similar to 20 years. From aircraft altitudes, it will be possible to cover a wide range of wavelengths, particularly in the critical 5-9 micron band, where detection of astrobiologically interesting molecules have key spectral signatures that are not accessible from the ground The FORCAST grism suite consists of six grisms: four monolithic Si grisms and two KRS-5 grisms. These devices will allow long-slit low-resolution (R = 100-300) and short-slit, cross-dispersed high-resolution spectroscopic modes (R = 800-1200) over select wavelengths in the 5-40 mu m spectral range and enable observing programs to gather both images and spectra in a single SOFIA flight. The silicon grisms demonstrate a new family of dispersive elements with good optical performance for spectroscopy from 1.2-8 mu m and beyond 18 mu m. After SOFIA flies, the grism modes in FORCAST will complement other first generation instruments on SOFIA and provide follow-up capability of bright sources observed with Infrared Spectrograph (IRS) on Spitzer. This paper highlights the design of the grism suite for FORCAST and the current laboratory cryogenic performance of the silicon grisms. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ennico, KA (reprint author), NASA, Ames Res Ctr, MS245-6, Moffett Field, CA 94035 USA. RI Ennico, Kimberly/L-9606-2014 NR 38 TC 2 Z9 2 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 0-8194-6334-5 J9 P SOC PHOTO-OPT INS PY 2006 VL 6269 BP Q2691 EP Q2691 AR 62691Q DI 10.1117/12.672256 PN 1-3 PG 10 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Spectroscopy SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics; Spectroscopy GA BEZ53 UT WOS:000240348500059 ER PT S AU Casey, SC AF Casey, Sean C. BE Stepp, LM TI The SOFIA program: Astronomers return to the stratosphere - art. no. 62670Q SO Ground-based and Airborne Telescopes, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Ground-Based and Airborne Telescopes CY MAY 24-31, 2006 CL Orlando, FL SP Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE SOFIA; airborne astronomy; far-infrared; instruments AB The Stratospheric Observatory for Infrared Astronomy (SOFIA) is the next generation of airborne astronomical observatories. Funded by the U.S. and German space agencies, SOFIA is scheduled for science flights beginning in late-2008. The observatory consists of a 747-SP modified to accommodate a 2.7-meter telescope with an open port design. Academic and government laboratories spanning both the U.S. and Germany are developing science instruments for SOFIA. Using state-of-the-art technologies, SOFIA will explore the emission of astronomical sources with an unprecedented level of angular resolution (theta[arc-seconds] = 0.1 x wavelength [mu m]) and spectral line sensitivity at infrared and sub-millimeter wavelengths. The current status of SOFIA is available from the observatory web site at http://sofia.arc.nasa.gov and is updated frequently. C1 NASA, Univ Space Res Assoc, Moffett Field, CA 94035 USA. RP Casey, SC (reprint author), NASA, Univ Space Res Assoc, MS 144-2, Moffett Field, CA 94035 USA. 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 0-8194-6332-9 J9 P SOC PHOTO-OPT INS PY 2006 VL 6267 BP Q2670 EP Q2670 AR 62670Q DI 10.1117/12.674475 PN 1&2 PG 10 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX64 UT WOS:000240018600025 ER PT S AU Erickson, EF Howe, DA Perry, JN Brown, TM Haas, MR AF Erickson, Edwin F. Howe, David A. Perry, John N. Brown, Ted M. Haas, Michael R. BE Stepp, LM TI The SOFIA cavity door - an unvignetted view: configuration, operation, and potential science implications - art. no. 62670U SO Ground-based and Airborne Telescopes, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Ground-Based and Airborne Telescopes CY MAY 24-31, 2006 CL Orlando, FL SP Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE SOFIA; cavity door; science implications AB The 2.5 meter (m) effective diameter telescope on SOFIA - the Stratospheric Observatory for Infrared Astronomy(1) will operate in an open-port cavity which will be closed below operating altitudes by a cavity-door assembly. When operating, the telescope will view the sky through an aperture defined by an aperture assembly (AA) with a nearly rectangular opening extending 112 inches (2.84 m) in elevation (roll) and 129 inches (3.27 m) in cross-elevation. The aperture will be servo-controlled in roll to track the telescope elevation (EL), and the aircraft heading will be adjusted to maintain the telescope centered on the aperture in cross-elevation (XEL). An upper rigid door (URD) and lower flexible door (LFD) move with the aperture to minimize the opening into the cavity containing the telescope. This paper describes basic parameters of the door system, and estimates possible science impacts of its specification, configuration and planned operation. Topics included are the geometry, expected aerodynamic disturbances, control system, gear life, influences of radiative and diffraction effects on science instrument performance, testing, operational considerations, and development status. As designed, the door system is expected not to limit the performance of science instruments or observatory operational efficiency, but several potential concerns are considered. These include modulation of stray and diffracted radiation, reliability, and maintainability. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Erickson, EF (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. NR 21 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 0-8194-6332-9 J9 P SOC PHOTO-OPT INS PY 2006 VL 6267 BP U2670 EP U2670 AR 62670U DI 10.1117/12.672639 PN 1&2 PG 11 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX64 UT WOS:000240018600029 ER PT S AU Traub, WA Kaltenegger, L Jucks, KW Turnbull, MC AF Traub, Wesley A. Kaltenegger, Lisa Jucks, Kenneth W. Turnbull, Margaret C. BE Stepp, LM TI Direct imaging of earth-like planets from space (TPF-C) SO GROUND-BASED AND AIRBORNE TELESCOPES, PTS 1 AND 2 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Ground-Based and Airborne Telescopes CY MAY 24-31, 2006 CL Orlando, FL SP Amer Astron Soc, Assoc Univ Res Astron, Ball Aerosp & Technol Corp, European SE Observ, Opt Infrared Coordinat Network, Particle Phys & Astron Res Council, UK Astron Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE Terrestrial Planet Finder Coronagraph; TPF; TPF-C; TPF-I; extrasolar planets AB The "big question" that the average person will ask an astronomer today is, "Are there Earth-like planets?" followed immediately by "Is there life on those planets?" We live in an age when we are privileged to be able to ask such a question, and have a reasonable expectation of receiving an answer, at least within the coming decade. As astronomers and physicists we are even more privileged to be the people who can provide those answers. This paper discusses the roles of four space missions that are planned by NASA to search for and characterize extrasolar planets: Kepler, Space Interferometer Mission (SIM-PlanetQuest), Terrestrial Planet Finder Coronagraph (TPF-C), and Terrestrial Planet finder Interferometer (TPF-I). The Kepler and SIM-PlanetQuest missions will search for and discover planets down to the few-Earth size and mass, around distant and nearby stars respectively. In favorable cases they will even be able to find Earth-size or mass planets. But to answer the questions "is a given planet habitable?" and "does it show signs of life?" we will need the TPF-C and TPF-I missions. Only these missions can isolate the light of the planet from the confusion of otherwise blinding starlight, and only these missions can perform spectroscopy on the planets. Visible and thermal infrared spectroscopy together will tell us if a planet is habitable and shows signs of life. TPF-C and TPF-I will build on the legacy of Kepler and SIM-PlanetQuest, and together these four missions will provide complete and unambiguous answers to our "big questions." This paper concentrates on the TPF-C mission. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Traub, WA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-451, Pasadena, CA 91109 USA. NR 11 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 0-8194-6332-9 J9 PROC SPIE PY 2006 VL 6267 AR 626502 DI 10.1117/12.676257 PN 1&2 PG 7 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX64 UT WOS:000240018600002 ER PT S AU Lisano, ME AF Lisano, Michael E. BE Jolly, SD Culp, RD TI Nonlinear consider covariance analysis using a sigma-point filter formulation SO Guidance and Control 2006 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 29th Annual AAS Rocky Mountain Guidance and Control Conference CY FEB 04-08, 2006 CL Breckenridge, CO SP Amer Astronaut Soc, Rocky Mt Sect AB The research reported here extends the mathematical formulation of nonlinear, sigma-point estimators to enable consider covariance analysis for dynamical systems. This paper presents a novel sigma-point consider filter algorithm, for consider-parameterized nonlinear estimation, following the unscented Kalman filter (UKF) variation on the sigma-point filter formulation, which requires no partial derivatives of dynamics models or measurement models with respect to the parameter list. It is shown that, consistent with the attributes of sigma-point estimators, a con sider-parameterized sigma-point estimator can be developed entirely without requiring the derivation of any partial-derivative matrices related to the dynamical system, the measurements, or the considered parameters, which appears to be an advantage over the formulation of a linear-theory sequential consider estimator. It is also demonstrated that a consider covariance analysis performed with this "partial-derivative-free" formulation yields equivalent results to the linear-theory consider filter, for purely linear problems. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lisano, ME (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 TC 2 Z9 2 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-877-03532-6 J9 ADV ASTRONAUT SCI PY 2006 VL 125 BP 129 EP 144 PG 16 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BFK34 UT WOS:000242467400010 ER PT S AU Miller, SA Bradley, AT Miller, NA Hodson, RF AF Miller, Samuel A. Bradley, Arthur T. Miller, Nathanael A. Hodson, Robert F. BE Jolly, SD Culp, RD TI Trinity, an oninidirectional robotic demonstrator for reconfigurable computing SO Guidance and Control 2006 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 29th Annual AAS Rocky Mountain Guidance and Control Conference CY FEB 04-08, 2006 CL Breckenridge, CO SP Amer Astronaut Soc, Rocky Mt Sect ID MOBILITY; DESIGN AB In this paper, we present the results of an unmanned ground vehicle robot development effort completed at NASA LaRC's Robotics and Intelligent Machines Laboratory. The robot is capable of conducting both tele-operation and autonomous activities. Novel omnidirectional mobility is achieved using three Mecanum wheels operating in a configuration not previously seen by this team. The robot is equipped with a suite of sensors, including a stereoscopic camera, FLIR, omnidirectional camera, ultrasonic range finders, 3-degree-of-freedom gyroscope, experimental acoustic eye, and ex-ray/visible spectrum fluoroscopes. The robot's architecture is designed to support reconfigurable scalable computing resources that can be dynamically adapted to changing mission requirements. This effort was funded as part of NASA's Office of Exploration Systems and is meant to demonstrate the utility of reconfigurable modular electronics. C1 NASA, Langley Res Ctr, Elect Syst Branch, Hampton, VA 23681 USA. RP Bradley, AT (reprint author), NASA, Langley Res Ctr, Elect Syst Branch, 5 N Dryden St, Hampton, VA 23681 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-877-03532-6 J9 ADV ASTRONAUT SCI PY 2006 VL 125 BP 145 EP 161 PG 17 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BFK34 UT WOS:000242467400011 ER PT S AU Bamford, W Naasz, B Moreau, MC AF Bamford, William Naasz, Bo Moreau, Michael C. BE Jolly, SD Culp, RD TI Navigation performance in high earth orbits using navigator GPS receiver SO Guidance and Control 2006 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 29th Annual AAS Rocky Mountain Guidance and Control Conference CY FEB 04-08, 2006 CL Breckenridge, CO SP Amer Astronaut Soc, Rocky Mt Sect AB NASA GSFC has developed a GPS receiver that can acquire and track GPS signals with sensitivity significantly lower than conventional GPS receivers. This opens up the possibility of using GPS based navigation for missions in high altitude orbits, such as Geostationary Operational Environmental Satellites (GOES) in a geostationary orbit, and the Magnetospheric MultiScale (MMS) Mission, in highly eccentric orbits extending to 12 Earth radii and higher. Indeed much research has been performed to study the feasibility of using GPS navigation in high Earth orbits and the performance achievable. Recently, GSFC has conducted a series of hardware in-the-loop tests to assess the performance of this new GPS receiver in various high Earth orbits of interest. Tracking GPS signals to down to approximately 22-25 dB-Hz, including signals from the GPS transmitter side-lobes, steady-state navigation performance in a geostationary orbit is on the order of 10 meters. This paper presents the results of these tests, as well as sensitivity analysis to such factors as ionosphere masks, use of GPS side-lobe signals, and GPS receiver sensitivity. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bamford, W (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 12 TC 2 Z9 2 U1 0 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-877-03532-6 J9 ADV ASTRONAUT SCI PY 2006 VL 125 BP 261 EP 276 PG 16 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BFK34 UT WOS:000242467400015 ER PT S AU Kubitschek, DG Mastrodemos, N Werner, RA Kennedy, BM Synnott, SP Null, GW Bhaskaran, S Riedel, JE Vaughan, AT AF Kubitschek, Daniel G. Mastrodemos, Nickolaos Werner, Robert A. Kennedy, Brian M. Synnott, Stephen P. Null, George W. Bhaskaran, Shyam Riedel, Joseph E. Vaughan, Andrew T. BE Jolly, SD Culp, RD TI Deep impact autonomous navigation: The trials of targeting the unknown SO GUIDANCE AND CONTROL 2006 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 29th Annual AAS Rocky Mountain Guidance and Control Conference CY FEB 04-08, 2006 CL Breckenridge, CO SP Amer Astronaut Soc, Rocky Mt Sect AB On July 4, 2005 at 05:44:34.2 UTC the Impactor Spacecraft (s/c) impacted comet Tempel 1 with a relative speed of 10.3 km/s capturing high-resolution images of the surface of the nucleus just seconds before impact. Meanwhile, the Flyby s/c captured the impact event using both the Medium Resolution Imager (MRI) and the High Resolution Imager (HRI) and tracked the nucleus for the entire 800 sec period between impact and shield attitude transition. The objective of the Impactor s/c was to impact in an illuminated area viewable from the Flyby s/c and capture high-resolution context images of the impact site. This was accomplished by using autonomous navigation (AutoNav) algorithms and precise attitude information from the attitude determination and control subsystem (ADCS). The Flyby s/c had two primary objectives: 1) capture the impact event with the highest temporal resolution possible in order to observe the ejecta plume expansion dynamics; and 2) track the impact site for at least 800 sec to observe the crater formation and capture the highest resolution images possible of the fully developed crater. These two objectives were met by estimating the Flyby s/c trajectory relative to Tempel I using the same AutoNav algorithms along with precise attitude information from ADCS and independently selecting the best impact site. This paper describes the AutoNav system, what happened during the encounter with Tempel I and what could have happened. C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Kubitschek, DG (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr,M-S 264-530, Pasadena, CA 91109 USA. EM daniel.kubitschek@jpl.nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-877-03532-6 J9 ADV ASTRONAUT SCI PY 2006 VL 125 BP 381 EP 406 PG 26 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BFK34 UT WOS:000242467400023 ER PT S AU Criddle, KE Antreasian, PG Bordi, JJ Ionasescu, R Jacobson, RA Mackenzie, RA Parcher, DW Pelletier, FJ Stauch, JR AF Criddle, K. E. Antreasian, P. G. Bordi, J. J. Ionasescu, R. Jacobson, R. A. Mackenzie, R. A. Parcher, D. W. Pelletier, F. J. Stauch, J. R. BE Jolly, SD Culp, RD TI Cassini orbit determination: The only targeted hyperion flyby of the prime mission SO Guidance and Control 2006 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 29th Annual AAS Rocky Mountain Guidance and Control Conference CY FEB 04-08, 2006 CL Breckenridge, CO SP Amer Astronaut Soc, Rocky Mt Sect AB On September 26, 2005, the Cassini spacecraft made its only targeted flyby of Saturn's moon Hyperion at an altitude of 488 km. With a dramatically compressed timeline, two deterministic maneuvers and a close (1500 km altitude) non-targeted Tethys flyby were planned in the six days prior to the Hyperion closest approach. Cassini orbit determination includes the estimation of Saturn's major satellite ephemerides, including Hyperion, using a combination of radio-metric and optical navigation data. Hyperion's irregular shape and chaotic rotation present another challenge by degrading the accuracy of the optical data which are used to improve its orbit knowledge prior to the encounter. This paper will compare post-flyby results to the orbit determination predictions. Operations preceding the encounter showed Hyperion's mass to be much lower than previously theorized. This unique flyby opportunity allowed Cassini to validate these estimates. C1 CALTECH, Jet Prop Lab, Cassini Navigat Team, Pasadena, CA 91109 USA. RP Criddle, KE (reprint author), CALTECH, Jet Prop Lab, Cassini Navigat Team, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-877-03532-6 J9 ADV ASTRONAUT SCI PY 2006 VL 125 BP 407 EP 424 PG 18 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BFK34 UT WOS:000242467400024 ER PT S AU Hughes, MP Schira, CN AF Hughes, Michael P. Schira, Charles N. BE Jolly, SD Culp, RD TI Deep Impact attitude estimator design and flight performance SO Guidance and Control 2006 SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 29th Annual AAS Rocky Mountain Guidance and Control Conference CY FEB 04-08, 2006 CL Breckenridge, CO SP Amer Astronaut Soc, Rocky Mt Sect AB In July, 2005 Deep Impact successfully impacted comet Tempel-1 and imaged the crater evolution. To achieve this, an onboard autonomous navigation system had to estimate the trajectory and maneuver the Impactor spacecraft into the comet's path. A similar system, operating on the Flyby spacecraft, independently calculated the impact location for imaging. At the heart of each autonomous navigation system is the attitude and gyro bias estimator using star trackers and gyros. The encounter geometry and timing placed stringent demands on attitude bias magnitude and drift calling for sequenced tuning of the respective filters. This paper describes the attitude and gyro bias estimator algorithms, the estimator flight performance and particular challenges overcome by the team leading up to a spectacular encounter. C1 NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hughes, MP (reprint author), NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 7 TC 1 Z9 1 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-877-03532-6 J9 ADV ASTRONAUT SCI PY 2006 VL 125 BP 441 EP 468 PG 28 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BFK34 UT WOS:000242467400026 ER PT J AU Rouner, D Lindsey, R AF Rouner, D Lindsey, R TI Female adolescent communication about sexually transmitted diseases SO HEALTH COMMUNICATION LA English DT Article; Proceedings Paper CT Meeting of the Association-for-Education-in-Journalism-and-Mass-Communication CY AUG, 2001 CL WASHINGTON, DC SP Assoc Educ Journalism & Mass Commun ID POSSIBLE SELVES; HEALTH RESEARCH; BEHAVIOR; SELF; EGOCENTRISM; INFORMATION; GUIDELINES; FREQUENCY; MESSAGES; STUDENTS AB Health researchers acknowledge a limited understanding of the social context of adolescents regarding their communication and decision making about sexually transmitted diseases (STDs). Using in-depth interviews, this study examines 18-year-old women regarding their self-concepts about STD communication, including their perceived and actual knowledge levels. Fifteen first-year college students from a Western university showed strong self-concepts and high perceived knowledge relative to sexual decision making and communication. The women's actual knowledge holding, however, was low. They demonstrated difficulty finding information from mediated sources with either high regard or mistrust of new information technologies for such information and limited use of interpersonal communication sources. C1 Colorado State Univ, Dept Journalism & Tech Commun, Ft Collins, CO 80523 USA. NASA, Earth Observ, Washington, DC 20546 USA. RP Rouner, D (reprint author), Colorado State Univ, Dept Journalism & Tech Commun, C233 Clark Bldg, Ft Collins, CO 80523 USA. EM donna.rouner@colostate.edu NR 62 TC 8 Z9 8 U1 1 U2 2 PU LAWRENCE ERLBAUM ASSOC INC PI MAHWAH PA 10 INDUSTRIAL AVE, MAHWAH, NJ 07430-2262 USA SN 1041-0236 J9 HEALTH COMMUN JI Health Commun. PY 2006 VL 19 IS 1 BP 29 EP 38 DI 10.1207/s15327027hc1901_4 PG 10 WC Communication; Health Policy & Services SC Communication; Health Care Sciences & Services GA 010AJ UT WOS:000235154900004 PM 16519590 ER PT J AU Borchert, M Lambert, J Sliney, D AF Borchert, M Lambert, J Sliney, D TI Validation of icnirp estimates of toxicity thresholds for NIR (785 NM) light in the retinas of pigmented rabbits SO HEALTH PHYSICS LA English DT Article DE ICNIRP; radiation; nonionizing; health effects; safety standards ID RADIATION; EXPOSURE; EYE AB The International Commission on Non-Ionizing Radiation Protection (ICNIRP) established eye-safe exposure limits for laser light based on estimates of the 50% exposure dose (ED50) for retinal damage in animals. The ED50 has not been determined for continuous-wave near-infrared (NIR) light, as may be used in instruments for spectroscopic analysis of the eye. The purpose of this study is to determine the ED50 of 785-nm light delivered by a Raman spectroscopy instrument on the retinas of pigmented rabbits, and to compare that ED50 to the ICNIRP estimates. Light of varying power was focused into the anterior chambers of rabbits for 4, 20, or 300 s. Estimates of spot size on the retina were determined by modifying the schematic rabbit eye with actual axial length and refractive error measurements. Masked examiners determined retinal burns from fundus photographs and fluorescein angiograms made immediately after exposure and again 48-72 h later. Thirty-five of 86 exposed eyes had retinal burns. In 12 of these the burn was not visible until 48-72 h. In 6 the burn was visible on color photographs, but not on fluorescein angiography. The ED50 retinal power density from probit analysis was 14,513 mW cm(-2), 10,369 mW cm(-2), and 5,237 MW cm(-2) for 4-s, 20-s, and 300-s exposures, respectively. Thus, the ED50 for retinal burns from 785-nm light is approximately 7 and 7.5 times the ICNIRP permitted limits for 4- and 20-s exposures, and 5.6 times the limit for 300-s exposures. This is consistent with the ICNIRP intention to set power limits several times less than ED50. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. Univ So Calif, Keck Sch Med, Childrens Hosp Los Angeles, Div Ophthalmol, Los Angeles, CA USA. Univ So Calif, Keck Sch Med, Dept Ophthalmol, Los Angeles, CA USA. USA, Ctr Hlth Promot & Prevent Med, Aberdeen, MD USA. RP Lambert, J (reprint author), CALTECH, Jet Propuls Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM james.l.lambert@jpl.nasa.gov NR 20 TC 0 Z9 0 U1 1 U2 3 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0017-9078 EI 1538-5159 J9 HEALTH PHYS JI Health Phys. PD JAN PY 2006 VL 90 IS 1 BP 3 EP 10 DI 10.1097/01.HP.0000175146.94650.4e PG 8 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA 015LG UT WOS:000235552300002 PM 16340602 ER PT S AU Traub, WA Kaltenegger, L Jucks, KW Turnball, MC AF Traub, Wesley A. Kaltenegger, Lisa Jucks, Kenneth W. Turnball, Margaret C. BE Dorn, DA Holland, AD TI Direct imaging of Earth-like planets from space (TPF-C) - art. no. 626502 SO High Energy, Optical, and Infrared Detectors for Astronomy II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on High Energy, Optical, and Infrared Detectors for Astronomy II CY MAY 24-27, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astronomy Inc, Ball Aerosp & Technol Corp, European SE Observat, Opt Infrared Coordinat Network, Particle Phys & Astronomy Res Council, UK Astronomy Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE Terrestrial Planet Finder Coronagraph; TPF; TPF-C; TPF-I; extrasolar planets ID SPECTRUM AB The "big question" that the average person will ask an astronomer today is, "Are there Earth-like planets?" followed immediately by "Is there life on those planets?" We live in an age when we are privileged to be able to ask such a question, and have a reasonable expectation of receiving an answer, at least within the coming decade. As astronomers and physicists we are even more privileged to be the people who can provide those answers. This paper discusses the roles of four space missions that are planned by NASA to search for and characterize extrasolar planets: Kepler, Space Interferometer Mission (SIM-PlanetQuest), Terrestrial Planet Finder Coronagraph (TPF-C), and Terrestrial Planet finder Interferometer (TPF-I). The Kepler and SIM-PlanetQuest missions will search for and discover planets down to the few-Earth size and mass, around distant and nearby stars respectively. In favorable cases they will even be able to find Earth-size or mass planets. But to answer the questions "is a given planet habitable?" and "does it show signs of life?" we will need the TPF-C and TPF-I missions. Only these missions can isolate the light of the planet from the confusion of otherwise blinding starlight, and only these missions can perform spectroscopy on the planets. Visible and thermal infrared spectroscopy together will tell us if a planet is habitable and shows signs of life. TPF-C and TPF-I will build on the legacy of Kepler and SIM-PlanetQuest, and together these four missions will provide complete and unambiguous answers to our "big questions." This paper concentrates on the TPF-C mission. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Traub, WA (reprint author), CALTECH, Jet Prop Lab, M-S 301-451,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 11 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 0-8194-6341-8 J9 P SOC PHOTO-OPT INS PY 2006 VL 6276 BP 26502 EP 26502 AR 626502 DI 10.1117/12.676257 PG 7 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BFB08 UT WOS:000240594700002 ER PT S AU Seshadri, S Cole, DM Hancock, B Ringold, P Peay, C Wrighley, C Bonati, M Brown, MG Schubnell, M Rahmer, G Guzman, D Figer, D Tarle, G Smith, RM Bebek, C AF Seshadri, S. Cole, D. M. Hancock, B. Ringold, P. Peay, C. Wrighley, C. Bonati, M. Brown, M. G. Schubnell, M. Rahmer, G. Guzman, D. Figer, D. Tarle, G. Smith, R. M. Bebek, C. BE Dorn, DA Holland, AD TI Characterization of NIR InGaAs imager arrays for the JDEM SNAP mission concept - art. no. 62760S SO High Energy, Optical, and Infrared Detectors for Astronomy II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on High Energy, Optical, and Infrared Detectors for Astronomy II CY MAY 24-27, 2006 CL Orlando, FL SP SPIE, Amer Astron Soc, Assoc Univ Res Astronomy Inc, Ball Aerosp & Technol Corp, European SE Observat, Opt Infrared Coordinat Network, Particle Phys & Astronomy Res Council, UK Astronomy Technol Ctr, Univ Florida, Univ Cent Florida, Coll Opt & Photon DE NIR; InGaAs; astronomy; low-temperature; focal plane array; imager; SNAP AB We present the results of a study of the performance of InGaAs detectors conducted for the SuperNova Acceleration Probe (SNAP) dark energy mission concept. Low temperature data from a nominal 1.7um cut-off wavelength 1kx1k InGaAs photodiode array, hybridized to a Rockwell HIRG multiplexer suggest that InGaAs detector performance is comparable to those of existing 1.7um cut-off HgCdTe arrays. Advances in 1.7um HgCdTe dark current and noise initiated by the SNAP detector research and development program makes it the baseline detector technology for SNAP. However, the results presented herein suggest that existing InGaAs technology is a suitable alternative for other future astronomy applications. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Seshadri, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6341-8 J9 P SOC PHOTO-OPT INS PY 2006 VL 6276 BP S2760 EP S2760 AR 62760S DI 10.1117/12.673252 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BFB08 UT WOS:000240594700027 ER PT J AU Harvey, DJ Das, SK Biswas, R AF Harvey, Daniel J. Das, Sajal K. Biswas, Rupak BE Yang, LT Guo, M TI A Workload Partitioner for Heterogeneous Grids SO HIGH-PERFORMANCE COMPUTING: PARADIGM AND INFRASTRUCTURE SE Wiley Series on Parallel and Distributed Computing LA English DT Article; Book Chapter ID ALGORITHM C1 [Harvey, Daniel J.] So Oregon Univ, Dept Comp Sci, Ashland, OR USA. [Biswas, Rupak] NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA. [Das, Sajal K.] Univ Texas Arlington, Dept Comp Sci, Arlington, TX 76019 USA. RP Harvey, DJ (reprint author), So Oregon Univ, Dept Comp Sci, Ashland, OR USA. NR 19 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE PUBL PI OXFORD PA OSNEY MEAD, OXFORD OX2 0EL, ENGLAND BN 978-0-471-73271-6 J9 WILEY SER PARA DIST PY 2006 BP 683 EP 703 DI 10.1002/0471732710.ch36 PG 21 WC Computer Science, Hardware & Architecture SC Computer Science GA BYB35 UT WOS:000297811800037 ER PT J AU Wang, XF Chao, DF Zhang, NL AF Wang, Xuefeng Chao, David F. Zhang, Nengli TI Three-dimensional model and numerical simulation of heat transfer in an anisotropic helical solid-mass with inner heat source SO HIGH TEMPERATURE MATERIAL PROCESSES LA English DT Article DE three-dimensional model; helical solid-mass; anisotropic; numerical grid generation; heat transfer ID THERMOSET COMPOSITES; PIPE-FLOW AB A three-dimensional model is established for heat transfer process in an anisotropic helical solid-mass with inner heat source. Based on this model, a numerical simulation procedure is suggested. Using numerical grid generation method, the transformed three-dimensional energy equation involving anisotropic thermal conductivities and the relevant boundary conditions in the computational domain are derived. The transformed equations are concise and regular, which solved through the finite volume method. The model is examined by available data to prove its validity. As an example, the model and the simulation procedure are applied to the on-line thermal curing of thermoset composites in filament winding. The results are compared to those obtained from previous simplified physical model and show that the simplified model is acceptable only for the cases of large diameter ratio of mandrel to tow while the proposed model in the present paper is efficient and more accurate. C1 NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. Univ Nebraska, Dept Mech Engn, Lincoln, NE 68588 USA. NASA, Glenn Res Ctr, Fluid Phys & Transport Branch, Cleveland, OH 44135 USA. RP Zhang, NL (reprint author), NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. EM nengli.zhang@grc.nasa.gov NR 12 TC 0 Z9 0 U1 0 U2 4 PU BEGELL HOUSE INC PI REDDING PA 50 CROSS HIGHWAY, REDDING, CT 06896 USA SN 1093-3611 J9 HIGH TEMP MATER P-US JI High Temp. Mater. Process PY 2006 VL 10 IS 2 BP 301 EP 316 DI 10.1615/HighTempMatProc.v10.i2.110 PG 16 WC Materials Science, Multidisciplinary SC Materials Science GA 097BX UT WOS:000241422400012 ER PT J AU Conway, EM AF Conway, Erik M. TI Drowning in data: Satellite oceanography and information overload in the Earth sciences SO HISTORICAL STUDIES IN THE PHYSICAL AND BIOLOGICAL SCIENCES LA English DT Article; Proceedings Paper CT Workshop on Climate Change Studies CY MAR, 2004 CL Univ Louis Pasteur, Strasbourg, FRANCE HO Univ Louis Pasteur DE satellite oceanography; remote sensing; NASA; Earth sciences ID HUMIDITY; OCEANS; SEASAT AB In the late 2011 century, remote sensing from space offered a means of resolving one of the principal challenges plaguing physical oceanographers, poor spatial sampling. But in fact, remote sensing offered an opposing problem-so much data that the traditional oceanographic institutions were not equipped to cope with it. NASA decided to resolve this problem by having the Jet Propulsion Laboratory construct an oceanographic data center at its Pasadena facility. This represents a new kind of scientific institution, whose purpose is the development, validation, and distribution of scientific data to third-party users. Since 1990, NASA has established several such facilities, each rooted in a subset of the Earth science disciplines and each making its data publicly available via the Internet. In so doing, it reversed a decades-old policy that had given an instrument's science team proprietary privileges. Agency leaders did this to expand scientific demand for NASA's capabilities, thus buttressing the agency's political support; because they believed remote sensing could enable great scientific strides; because they thought open access to data would foster competition and thus produce better scientific results; and because they believed that publicly-funded data should be public. In the process, they created a "market" for oceanographic data far larger than that represented by professional oceanographers. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Conway, EM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Erik.M.Conway@jpl.nasa.gov NR 47 TC 10 Z9 10 U1 0 U2 5 PU UNIV CALIFORNIA PRESS PI BERKELEY PA C/O JOURNALS DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0890-9997 J9 HIST STUD PHYS BIOL JI Hist. Stud. Phys. Biol. Sci. PY 2006 VL 37 BP 127 EP 151 DI 10.1525/hsps.2006.37.1.127 PN 1 PG 25 WC History & Philosophy Of Science SC History & Philosophy of Science GA 127FB UT WOS:000243569600006 ER PT S AU Peteet, DM Pederson, DC Kurdyla, D Guilderson, T AF Peteet, Dorothy M. Pederson, Dee Cabaniss Kurdyla, Dorothy Guilderson, Tom BE Waldman, JR Limburg, KE Strayer, DL TI Hudson River paleoecology from marshes: Environmental change and its implications for fisheries SO Hudson River Fishes and their Environment SE AMERICAN FISHERIES SOCIETY SYMPOSIUM LA English DT Proceedings Paper CT Conference on Hudson River Fishes and Their Environment CY MAR 20-21, 2003 CL Poughkeepsie, NY SP Amer Fisheries Soc ID ESTUARINE SEDIMENT ACCUMULATION; CHESAPEAKE BAY; PHRAGMITES-AUSTRALIS; TIDAL MARSH; NEW-YORK; DREISSENA-POLYMORPHA; LONG-ISLAND; COMMON REED; NEW-JERSEY; NEKTON USE AB Hudson riverine and coastal marshes provide a paleoecological archive consisting of information on climate and land use at both the local and watershed scales. The timing of formation of these marshes is documented using accelerator mass spectrometry (AMS) C-14 dating of identified plant macrofossils in basal marsh organic sediments. While the Staten Island marsh is oldest and dates to 11,000 years before present (BP), Piermont, Iona, and Croton marshes date to the mid-Holocene, and the Jamaica Bay marshes formed most recently. Pollen and spores, charcoal, and plant macrofossils in the marsh sediments document marked climatic shifts as well as anthropogenic impact in the region. Assessment of the inorganic and organic content of the sediments in the marshes reveals a pattern of decreasing inorganic supply with the arrival of the Europeans, possibly due to the construction of numerous Hudson River tributary dams. Piermont Marsh, because of its sensitive location in the Hudson River, records droughts and wet intervals through species which have specific salinity affinities. Throughout the marsh records, the ragweed Ambrosia pollen rise marks the anthropogenic impact at the landscape scale. The recorded changes in hydrology and salinity that occurred throughout the centuries and millennia would have had profound effects throughout the food web and estuarine ecosystem. Fish populations would have been affected by changes in the food supply due to shifts in runoff affecting turbidity and light penetration in the river. Local vegetation changes within marshes may also have affected juvenile fish populations. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Peteet, DM (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. NR 62 TC 1 Z9 1 U1 1 U2 8 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE, STE 110, BETHESDA, MD 20814-2199 USA SN 0892-2284 BN 978-1-888569-82-7 J9 AM FISH S S PY 2006 VL 51 BP 113 EP 128 PG 16 WC Fisheries SC Fisheries GA BFS93 UT WOS:000244447600007 ER PT S AU Ellis, SR AF Ellis, Stephen R. BE Rogowitz, BE Pappas, TN Daly, SJ TI Remembrance of scanpaths past: Experiments with Larry Stark - art. no. 605709 SO Human Vision and Electronic Imaging XI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Human Vision and Electronic Imaging XI CY JAN 16-18, 2006 CL San Jose, CA SP Soc Investigat Dermatol DE scanpaths; higher level control saccadic eye movements; Lawrence Stark; fragmented images; Necker cube ID EYE-MOVEMENTS AB A search for statistically defensible evidence for repetitive visual scanning of pictorial stimuli is reviewed using experimental approaches developed in Professor Stark's Berkeley laboratory. Examples of visual scanning at the instant of perceptual organization and of scanning during information seeking will be presented including photographs from Stark's laboratory. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ellis, SR (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 8 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 0-8194-6097-4 J9 P SOC PHOTO-OPT INS PY 2006 VL 6057 BP 5709 EP 5709 AR 605709 DI 10.1117/12.674144 PG 10 WC Computer Science, Information Systems; Ophthalmology; Optics; Imaging Science & Photographic Technology SC Computer Science; Ophthalmology; Optics; Imaging Science & Photographic Technology GA BEF36 UT WOS:000237083200008 ER PT S AU Ahumada, AJ San-Martin, MT Gille, J AF Ahumada, Albert J. San-Martin, Maite Trujillo Gille, Jennifer BE Rogowitz, BE Pappas, TN Daly, SJ TI Symbol discriminability models for improved flight displays - art. no. 605711 SO Human Vision and Electronic Imaging XI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Human Vision and Electronic Imaging XI CY JAN 16-18, 2006 CL San Jose, CA SP Soc Investigat Dermatol DE human vision models; cockpit display; symbology; image discrimination ID SPATIAL CONTRAST AB Aviation display system designers and evaluators need to know how discriminable displayed symbols will be over a wide range of conditions to assess the adequacy and effectiveness of flight display systems. If flight display symbols are to be safely recognized by pilots, it is necessary that they can be easily discriminated from each other. Sometimes psychophysical measurements can answer this question, but computational modeling may be required to assess the numerous conditions and even help design the empirical experiments that may be needed. Here we present an image discrimination model that includes position compensation. The model takes as input the luminance values for the pixels of two symbol images, the effective viewing distance, and gives as output the discriminability in just-noticeable-differences (d') and the x and y offset in pixels needed to minimize the discriminability. The model predictions are shown to be a useful upper bound for human symbol identification performance. C1 NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ahumada, AJ (reprint author), NASA Ames Res Ctr, MS 262-2, Moffett Field, CA 94035 USA. NR 15 TC 0 Z9 0 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6097-4 J9 P SOC PHOTO-OPT INS PY 2006 VL 6057 BP 5711 EP 5711 AR 605711 DI 10.1117/12.650875 PG 10 WC Computer Science, Information Systems; Ophthalmology; Optics; Imaging Science & Photographic Technology SC Computer Science; Ophthalmology; Optics; Imaging Science & Photographic Technology GA BEF36 UT WOS:000237083200036 ER PT S AU Moloney, P Huffman, C Springer, M Gorelik, O Nikolaev, P Sosa, E Arepalli, S Yowell, L AF Moloney, Padraig Huffman, Chad Springer, Micah Gorelik, Olga Nikolaev, Pasha Sosa, Edward Arepalli, Sivaram Yowell, Leonard BE Dillion, A Olk, C Filiou, C Ohi, J TI PEM fuel cell electrodes using single wall carbon nanotubes SO HYDROGEN CYCLE-GENERATION, STORAGE AND FUEL CELLS SE Materials Research Society Symposium Proceedings LA English DT Proceedings Paper CT Symposium on the Hydrogen Cycle held at the 2005 MRS Fall Meeting CY NOV 28-DEC 02, 2005 CL Boston, MA SP Mat Res Soc AB SWCNT continue to be investigated as an ideal catalyst support material for PEMFC. Theoretically, SWCNT are ideal for this role due to material advantages over the incumbent carbon black supports such as high surface areas, porosities, thermal and electrical conductivities [1,2]. This research is driven by the current space exploration effort at NASA which demands higher power densities and reliability from power and energy systems. The new space exploration effort soon to be embarked by NASA and its partners demands higher power densities and dependability. Previous research has suggested that the purity and thickness of SWCNT catalyst support or electrodes are dominant in catalyst support influences On PEMFC performance [3,4]. This study aims to confirm these findings through materials characterization and fuel cell testing. It also seeks to draw more thorough conclusions on optimal SWCNT morphologies by the variation of processing, fabrication and testing techniques. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Moloney, P (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 7 TC 2 Z9 2 U1 0 U2 1 PU MATERIALS RESEARCH SOC PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-839-X J9 MATER RES SOC SYMP P PY 2006 VL 885 BP 75 EP 80 PG 6 WC Chemistry, Physical; Electrochemistry; Energy & Fuels SC Chemistry; Electrochemistry; Energy & Fuels GA BEU27 UT WOS:000239520400009 ER PT S AU Good, BS AF Good, Brian S. BE Dillion, A Olk, C Filiou, C Ohi, J TI Structure and thermal conductivity of silica aerogels from computer simulations SO Hydrogen Cycle-Generation, Storage and Fuel Cells SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT Symposium on the Hydrogen Cycle held at the 2005 MRS Fall Meeting CY NOV 28-DEC 02, 2005 CL Boston, MA SP Mat Res Soc ID DIFFUSION-LIMITED AGGREGATION; POROUS MATERIALS; SCATTERING AB Aerogels are of current interest in the aerospace community due to their light weight and low thermal conductivity, making them suitable for a variety of applications, notably cryotank insulation. These gels typically exhibit a complex structure; the smallest feature is a "primary" particle of amorphous silica, typically 2-5nm in diameter. The primary particles aggregate to form "secondary" particles, typically an order of magnitude larger, and these, in turn, form pearl-necklace structures whose details depend on the density. The gels appear to exhibit fractal dimensionality, at least over a small range of length scales. In this work, we investigate the relationship between the structure of the gels, their dimensionality and density, and their thermal conductivity. We model the secondary-particle aggregate structure using a modified Diffusion Limited Cluster Aggregation (DLCA) model. The model produces qualitatively different structures at low and high densities that are consistent with experimental observation. At lower densities, we find evidence for a transition from fractal behavior at small length scales to approximately compact behavior at larger lengths. We model the thermal conductivity using a variant of the random resistor network approach that has been used to describe, e.g. hopping electrical conduction in doped serni conductors. In our model, each secondary particle is assigned an effective thermal conductance that depends on the particle's size, and on the details of its contacts with neighboring particles; the conductivity of the get network is obtained using standard numerical techniques. The scaling of the thermal conductivity with density and fractal dimension is discussed. C1 NASA, Glenn Res Ctr, Cleveland, OH 44026 USA. RP Good, BS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44026 USA. NR 16 TC 2 Z9 2 U1 0 U2 5 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-839-X J9 MATER RES SOC SYMP P PY 2006 VL 885 BP 227 EP 232 PG 6 WC Chemistry, Physical; Electrochemistry; Energy & Fuels SC Chemistry; Electrochemistry; Energy & Fuels GA BEU27 UT WOS:000239520400030 ER PT S AU Bowman, RC AF Bowman, Robert C., Jr. BE Myneni, GR Hjorvarsson, B TI Roles of hydrogen in space explorations SO Hydrogen in Matter SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 2nd International Symposium on Hydrogen in Matter CY JUN 13-17, 2005 CL Uppsala, SWEDEN SP Royal Swedish Acad Sci, Nobel Inst Phys, European Sci Fdn, Swedish Res Council, Swedish Energy Agcy, City Uppsala, DOE, Argonne Natl Lab, Jefferson Lab, Natl Inst Standards & Technol, NASA/Jet Propuls Lab, Reference Met Co Inc, ATI Wah Chang, Uppsala Univ DE hydrogen; space exploration; sorption cryocoolers; nickel-hydrogen batteries; cryogenic hydrogen storage; rocket propulsion; metal hydrides; energy conversion ID METAL HYDRIDE BATTERIES; CRYOGENICS; PROPULSION; MISSIONS; MARS AB The various roles of hydrogen in space technology are identified and discussed. The preeminent position of hydrogen as rocket fuel in launch vehicles is explained and illustrated for the NASA Space Shuttle. The history of hydrogen in launching space vehicles is also briefly summarized. The cryogenic aspects of hydrogen for cooling instruments during flight missions are covered for several past and current systems. The technology of Nickel-Hydrogen batteries is covered. The storage of cryogenic hydrogen to operate fuel cells and to provide potable water is described for the NASA Apollo and Shuttle Missions. Other less well-known applications of hydrogen and metal hydrides such as gas gap heat switches, fueling hypersonic scrarojet flights to Mach 10 speeds, in-situ resource utilization on lunar or Martian surfaces, and providing ultrapure reference hydrogen to scientific instruments are also described. Finally, some possible future roles for hydrogen in space exploration are identified. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bowman, RC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Bowman, Robert/0000-0002-2114-1713 NR 42 TC 2 Z9 2 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 0-7354-0329-5 J9 AIP CONF PROC PY 2006 VL 837 BP 175 EP 199 PG 25 WC Materials Science, Multidisciplinary; Physics, Condensed Matter SC Materials Science; Physics GA BEN58 UT WOS:000238327100021 ER PT J AU Rundle, JB Turcotte, DL Rundle, PB Shcherbakov, R Yakovlev, G Donnellan, A Klein, W AF Rundle, J. B. Turcotte, D. L. Rundle, P. B. Shcherbakov, R. Yakovlev, G. Donnellan, A. Klein, W. TI Pattern dynamics, pattern hierarchies, and forecasting in complex multi-scale earth systems SO HYDROLOGY AND EARTH SYSTEM SCIENCES LA English DT Article ID SYNTHETIC SEISMICITY MODEL; SOUTHERN-CALIFORNIA; THRESHOLD SYSTEMS; PHYSICAL MODEL; FAULT SYSTEMS; EARTHQUAKES; SIMULATIONS; PREDICTION; HAZARD AB Catastrophic disasters afflicting human society are often triggered by tsunamis, earthquakes, widespread flooding, and weather and climate events. As human populations increasingly move into geographic areas affected by these earth system hazards, forecasting the onset of these large and damaging events has become increasingly urgent. In this paper we consider the fundamental problem of forecasting in complex multi-scale earth systems when the basic dynamical variables are either unobservable or incompletely observed. In such cases, the forecaster must rely on incompletely determined, but "tunable" models to interpret observable space-time patterns of events. The sequence of observable patterns constitute an apparent pattern dynamics, which is related to the underlying but hidden dynamics by a complex dimensional reduction process. As an example, we examine the problem of earthquakes, which must utilize current and past observations of observables such as seismicity and surface strain to produce forecasts of future activity. We show that numerical simulations of earthquake fault systems are needed in order to relate the fundamentally unobservable nonlinear dynamics to the readily observable pattern dynamics. We also show that the space-time patterns produced by the simulations lead to a scale-invariant hierarchy of patterns, similar to other nonlinear systems. We point out that a similar program of simulations has been very successful in weather forecasting, in which current and past observations of weather patterns are routinely extrapolated forward in time via numerical simulations in order to forecast future weather patterns. C1 Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. Univ Calif Davis, Computat Sci & Engn Ctr, Davis, CA 95616 USA. Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. Boston Univ, Dept Phys, Boston, MA 02215 USA. RP Rundle, JB (reprint author), Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. EM jbrundle@ucdavis.edu RI Shcherbakov, Robert/I-1036-2012 OI Shcherbakov, Robert/0000-0002-3057-0851 NR 37 TC 4 Z9 4 U1 0 U2 3 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1027-5606 EI 1607-7938 J9 HYDROL EARTH SYST SC JI Hydrol. Earth Syst. Sci. PY 2006 VL 10 IS 6 BP 789 EP 796 PG 8 WC Geosciences, Multidisciplinary; Water Resources SC Geology; Water Resources GA 129TF UT WOS:000243752300002 ER PT J AU Litvak, ML Mitrofanov, IG Kozyrev, AS Sanin, AB Tretyakov, VI Boynton, WV Kelly, NJ Hamara, D Shinohara, C Saunders, RS AF Litvak, ML Mitrofanov, IG Kozyrev, AS Sanin, AB Tretyakov, VI Boynton, WV Kelly, NJ Hamara, D Shinohara, C Saunders, RS TI Comparison between polar regions of Mars from HEND/Odyssey data SO ICARUS LA English DT Article DE Mars, surface; Mars, atmosphere; Mars, climate; ices ID HEND INSTRUMENT ONBOARD; GENERAL-CIRCULATION MODEL; ODYSSEY SPACECRAFT; GROUND ICE; NEUTRON MEASUREMENTS; CARBON-DIOXIDE; SNOW DEPTH; WATER; TEMPERATURES; HEMISPHERE AB In this paper, we have analyzed neutron spectroscopy data gathered by the High Energy Neutron Detector (HEND) instrument onboard Mars Odyssey for comparison of polar regions. It is known that observation of the neutron albedo of Mars provides important information about the distribution of water-ice in subsurface layers and about peculiarities of the CO2 seasonal cycle. It was found that there are large water-rich permafrost areas with contents of up to similar to 50% water by mass fraction at both the north and south Mars polar regions. The water-ice layers at high northern latitudes are placed close to the surface, but in the south they are covered by a dry and relatively thick (10-20 cm) layer of soil. Analysis of temporal variations of neutron flux between summer and winter seasons allowed the estimation of the masses of the CO2 deposits which seasonally condense at the polar regions. The total mass of the southern seasonal deposition was estimated as 6.3 x 10(15) kg, which is larger than the total mass of the seasonal deposition at the north by 40-50%. These results are in good agreement with predictions from the NASA Ames Research Center General Circulation Model (GCM). But, the dynamics of the condensation and sublimation processes are not quite as consistent with these models: the peak accumulation of the condensed mass of CO2 occurred 10-15 degrees of L-s later than is predicted by the GCM. (c) 2005 Elsevier Inc. All rights reserved. C1 Inst Space Res, Moscow 117997, Russia. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. NASA Headquarters, Washington, DC 20546 USA. RP Inst Space Res, Profsojuznaya St 84-32, Moscow 117997, Russia. EM max@cgrsmx.iki.rssi.ru NR 47 TC 28 Z9 28 U1 1 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JAN PY 2006 VL 180 IS 1 BP 23 EP 37 DI 10.1016/j.icarus.2005.08.009 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000UR UT WOS:000234488400003 ER PT J AU Manning, CV McKay, CP Zahnle, KJ AF Manning, CV McKay, CP Zahnle, KJ TI Thick and thin models of the evolution of carbon dioxide on Mars SO ICARUS LA English DT Article DE Mars, atmosphere; evolution ID IMPACT EROSION; MARTIAN ATMOSPHERE; CHAOTIC OBLIQUITY; CLIMATE MODEL; LIQUID WATER; CO2; ICE; CONSTRAINTS; STABILITY; MERIDIANI AB We present results from a new simulation code that accounts for the evolution of the reservoirs of carbon dioxide on Mars, from its early years to the present. We establish a baseline model parameter set that produces results compatible with the present (i.e;, P-atm similar or equal to 6.5 mbar with permanent CO2 ice cap) for a wide range of initial inventories. We find that the initial inventory of CO2 broadly determines the evolutionary course of the reservoirs of CO2. The reservoirs include the atmosphere, ice cap, adsorbed CO2 in the regolith, and carbonate rocks. We track the evolution of the free inventory: the atmosphere, ice cap and regolith. Simulations begin at 4.53 Gyr before present with a rapid loss of free inventory to space in the early Noachian. Models that assume a relatively small initial inventory (less than or similar to 5 bar) have pronounced minima in the free inventory of CO2 toward the end of the Noachian. Under baseline parameters, initial inventories below similar to 4.5 bar result in a catastrophic loss of the free inventory to space. The current free inventory would be then determined by the balance between outgassing, sputtering losses and chemical weathering following the end of the late bombardment. We call these "thin" models. They generically predict small current free inventories in line with expectations of a small present CO2 ice cap. For "thick" models, with initial inventories greater than or similar to 5 bar, a surplus of 300-700 mbar of free CO2 remains during the late-Noachian. The histories of free inventory in time for thick models tend to converge within the last 3.5 Gyr toward a present with an ice cap plus atmospheric inventory of about 100 mbar. For thick models, the convergence is largely due to the effects of chemical weathering, which draws down higher free inventories more rapidly than the low. Thus, thick models have 450 mbar carbonate reservoirs, while thin models have; 200 mbar. Though both thick and thin scenarios can reproduce the current atmospheric pressure, the thick models imply a relatively large current CO2 ice cap and thin models, little or none. While the sublimation of a massive cap at a high obliquity would create a climate swing of greenhouse warming for thick models, under the thin model, mean temperatures and pressures would be essentially unaffected by increases in obliquity. (c) 2005 Elsevier Inc. All rights reserved. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM cmanning@arc.nasa.gov NR 62 TC 39 Z9 39 U1 1 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 EI 1090-2643 J9 ICARUS JI Icarus PD JAN PY 2006 VL 180 IS 1 BP 38 EP 59 DI 10.1016/j.icarus.2005.08.014 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000UR UT WOS:000234488400004 ER PT J AU Mosqueira, I Estrada, PR AF Mosqueira, I Estrada, PR TI Jupiter's obliquity and a long-lived circumplanetary disk SO ICARUS LA English DT Article DE Jupiter; satellites of Jupiter; rotational dynamics; obliquity ID GIANT PLANETS; SOLAR NEBULA; TERRESTRIAL PLANETS; REGULAR SATELLITES; SECULAR RESONANCE; TILTING SATURN; GASEOUS DISK; ACCRETION; ORIGIN; SYSTEM AB It has been claimed [Canup, R.M., Ward, W.R., 2002. Astron. J. 124, 3404-3423; Ward, W.R., 2003. In: AGU, Fall Meeting 2003] that a long-lived minimum mass circumplanetary gas disk is inconsistent with Jupiter's low obliquity. Here we find that while Jupiter's obliquity may constrain its characteristics it does not rule out a long-lived massive (compared to the mass of the Galilean satellites) disk. This is because the argument assumes a Solar System much like that of the present day with the one exception of a circumjovian disk which is then allowed to dissipate on a long timescale (10(6) - 10(7) yr). Given that the sequence of events in Solar System history that fit known constraints is non-unique, we choose for the sake of clarity of exposition the orbital architecture framework of Tsiganis et al. [Tsiganis, K., Gomes, R., Morbidelli, A., Levison, H.F., 2005. Nature 435, 459-461], in which Jupiter and Saturn were once in compact, nearly coplanar orbits, and show that in this case Jupiter's low obliquity is consistent with the SEMM (solids-enhanced minimum mass) satellite formation model of Mosqueira and Estrada [Mosqueira, I., Estrada, P.R., 2003a. Icarus 163, 198-231; Mosqueira, I., Estrada, P.R., 2003b. Icarus 163, 232-255]. We suggest that a low inclination starting condition may apply, but stress that our SEMM satellite formation model could be compatible with Jupiter's obliquity even for mutually inclined giant planets. (c) 2005 Elsevier Inc. All rights reserved. C1 NASA, Ames SETI Inst, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Mosqueira, I (reprint author), NASA, Ames SETI Inst, Mail Stop 245-3, Moffett Field, CA 94035 USA. EM mosqueir@cosmic.arc.nasa.gov; estrada@cosmic.arc.nasa.gov NR 38 TC 1 Z9 1 U1 0 U2 0 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD JAN PY 2006 VL 180 IS 1 BP 93 EP 97 DI 10.1016/j.icarus.2005.10.001 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000UR UT WOS:000234488400008 ER PT J AU Simon-Miller, AA Conrath, BJ Gierasch, PJ Orton, GS Achterberg, RK Flasar, FM Fisher, BM AF Simon-Miller, AA Conrath, BJ Gierasch, PJ Orton, GS Achterberg, RK Flasar, FM Fisher, BM TI Jupiter's atmospheric temperatures: From Voyager IRIS to Cassini CIRS SO ICARUS LA English DT Article DE Jupiter, atmosphere; atmospheres, dynamics; atmospheres, temperature ID PARA-HYDROGEN FRACTION; INFRARED OBSERVATIONS; OUTER PLANETS; SPATIAL-ORGANIZATION; JOVIAN ATMOSPHERE; THERMAL STRUCTURE; UPPER TROPOSPHERE; TIME-DEPENDENCE; STRATOSPHERE; OSCILLATION AB Retrievals performed on Cassim Composite Infrared Spectrometer data obtained during the distant Jupiter flyby in 2000/2001 have been used to generate global temperature maps of the planet in the troposphere and stratosphere, but to higher latitudes than were shown previously by Flasar et a]. [Flasar, F.M., 39 colleagues, 2004a. Nature 427, 132-135; Flasar, F.M., 44 colleagues, 2004b. Space Sci. Rev. 115, 169-297]. Similar retrievals were performed on Voyager I IRIS data to provide the first detailed IRIS map of the stratosphere, and high latitudes in the troposphere. Thermal winds were calculated for each data set and show strong vertical shears in the zonal winds at low latitudes, and meridional temperature gradients indicate the presence of circumpolar jets, as well. The temperatures retrieved from the two spacecraft were also compared with yearly ground-based data obtained over the intervening two decades. Tropospheric temperatures reveal gradual changes at low latitudes, with little obvious seasonal or short-term variation [Orton et al., 1994. Science 265, 625-6311. Stratospheric temperatures show much more complicated behavior over short timescales, consistent with quasi-quadrennial oscillations at low latitudes, as suggested in prior analyses of shorter intervals of ground-based data [Orton et al., 1991. Science 252, 537-542; Friedson, A.J., 1999. Icarus 137, 34-55]. A scaling analysis indicates that meridional motions, mechanically forced by wave or eddy convergence, play an important role in modulating the temperatures and winds in the upper troposphere and stratosphere on seasonal and shorter timescales. At latitudes away from the equator, the mechanical forcing can be derived simply from a temporal record of temperature and its vertical derivative. Ground-based observations with improved vertical resolution and/or long-term monitoring from spacecraft are required for this purpose, though the Voyager and Cassini data given indications that the magnitude of the forcing is very small. Published by Elsevier Inc. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Cornell Univ, Ithaca, NY 14853 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. SSAI, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Simon-Miller, AA (reprint author), NASA, Goddard Space Flight Ctr, Code 693-0, Greenbelt, MD 20771 USA. EM amy.simon@nasa.gov RI Flasar, F Michael/C-8509-2012; Simon, Amy/C-8020-2012 OI Simon, Amy/0000-0003-4641-6186 NR 47 TC 52 Z9 52 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 JAN PY 2006 VL 180 IS 1 BP 98 EP 112 DI 10.1016/j.icarus.2005.07.019 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000UR UT WOS:000234488400009 ER PT J AU Nuth, JA Johnson, NM AF Nuth, JA Johnson, NM TI Crystalline silicates in comets: How did they form? SO ICARUS LA English DT Article DE comets; comets, origin; solar nebula processes; silicate grains; interplanetary dust ID DIFFUSE INTERSTELLAR-MEDIUM; SOLAR NEBULA; INFRARED EXTINCTION; SIZE DISTRIBUTION; DUST; GRAINS; CONSTRAINTS; CHEMISTRY; OLIVINE; MODEL AB Two processes have been proposed to explain observations of crystalline silicate minerals in comets and in protostellar sources, both of which rely on the thermal annealing of amorphous grains. First, high temperatures generated by nebular shock processes can rapidly produce crystalline magnesium silicate grains and will simultaneously produce a population of crystalline iron silicates whose average grain size is similar to 10-15% that of the magnesium silicate minerals. Second, exposure of amorphous silicate grains to hot nebular environments can produce crystalline magnesium silicates that might then be transported outward to regions of comet formation. At the higher temperatures required for annealing amorphous iron silicates to crystallinity the evaporative lifetime of the grains is much shorter than a single orbital period where such temperatures are found in the nebula. Thermal annealing is therefore unable to produce crystalline iron silicate grains for inclusion into comets unless such grains are very quickly transported away from the hot inner nebula. It follows that observation of pure crystalline magnesium silicate minerals in comets or protostars is a direct measure of the importance of simple thermal annealing of grains in the innermost regions of protostellar nebulae followed by dust and gas transport to the outer nebula. The presence of crystalline iron silicates would signal the action of transient processes such as shock heating that can produce crystalline iron, magnesium and mixed iron-magnesium silicate minerals. These different scenarios result in very different predictions for the organic content of protostellar systems. (c) 2005 Elsevier Inc. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, NAS NRC, Greenbelt, MD 20771 USA. RP NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA. EM joseph.a.nuth@nasa.gov RI Johnson, Natasha/E-3093-2012; Nuth, Joseph/E-7085-2012 NR 51 TC 29 Z9 29 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JAN PY 2006 VL 180 IS 1 BP 243 EP 250 DI 10.1016/j.icarus.2005.09.003 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000UR UT WOS:000234488400020 ER PT J AU Loeffler, MJ Raut, U Vidal, RA Baragiola, RA Carlson, RW AF Loeffler, MJ Raut, U Vidal, RA Baragiola, RA Carlson, RW TI Synthesis of hydrogen peroxide in water ice by ion irradiation SO ICARUS LA English DT Article DE Europa; radiation chemistry; infrared observations; surfaces; Jupiter ID GALILEAN SATELLITES; OPTICAL-PROPERTIES; OZONE SYNTHESIS; XE MATRICES; EUROPA; H2O2; RADICALS; OXYGEN; RADIOLYSIS; GANYMEDE AB We present infrared absorption studies on the effects of 50-100 keV Ar+ and 100 keV H+ ion irradiation of water ice films at 20-120 K. The results support the view that energetic ions can produce hydrogen peroxide on the surface of icy satellites and rings in the outer Solar System, and on ice mantles on interstellar grains. The ion energies are characteristic of magnetospheric ions at Jupiter, and therefore the results support the idea that radiolysis by ion impact is the source of the H2O2 detected on Europa by the Galileo infrared spectrometer. We found that Ar+ ions, used to mimic S+ impacts, are roughly as efficient as H+ ions in producing H2O2, and that 100 keV H+ ions can produce hydrogen peroxide at 120 K. The synthesized hydrogen peroxide remained stable while warming the ice film after irradiation; the column density of the formed H2O2 is constant until the ice film begins to desorb, but the concentration of H2O2 increases with time during desorption because the water sublimes at a faster rate. Comparing the shape of the 3.5-mu m absorption feature of H2O2 to the one measured on Europa shows excellent agreement in both shape and position, further indicating that the H2O2 detected on Europa is likely caused by radiolysis of water ice. (c) 2005 Elsevier Inc. All rights reserved. C1 Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22904 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Loeffler, MJ (reprint author), Univ Virginia, Lab Atom & Surface Phys, Thornton Hall B113, Charlottesville, VA 22904 USA. EM mjl8r@virginia.edu RI Loeffler, Mark/C-9477-2012; OI Vidal, Ricardo/0000-0001-7082-9787 NR 44 TC 69 Z9 70 U1 2 U2 9 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 JAN PY 2006 VL 180 IS 1 BP 265 EP 273 DI 10.1016/j.icarus.2005.08.001 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000UR UT WOS:000234488400022 ER PT B AU Sterritt, R Hinchey, MG AF Sterritt, Roy Hinchey, Michael G. BE Kawada, S TI Biologically-inspired concepts for self-management of complexity SO ICECCS 2006: 11TH IEEE INTERNATIONAL CONFERENCE ON ENGINEERING OF COMPLEX COMPUTER SYSTEMS, PROCEEDINGS SE IEEE International Conference on Engineering Complex Computer Systems-ICECCS LA English DT Proceedings Paper CT 11th IEEE International Conference on Engineering of Complex Computer Systems CY AUG 15-17, 2006 CL Stanford, CA SP IEEE, IEEE Comp Soc TC Complex Comp ID DEATH AB Inherent complexity in large-scale applications may be impossible to eliminate or even ameliorate despite a number of promising advances. In such cases, the complexity must be tolerated and managed. Such management may be beyond the abilities of humans, or require such overhead as to make management by humans unrealistic. A number of initiatives inspired by concepts in biology have arisen for self-management of complex systems. We present some ideas and techniques we have been experimenting with, inspired by lesser-known concepts in biology that show promise in protecting complex systems and represent a step towards self-management of complexity. C1 [Sterritt, Roy] Univ Ulster, Jordanstown, North Ireland. [Hinchey, Michael G.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Sterritt, R (reprint author), Univ Ulster, Jordanstown, North Ireland. FU NASA Office of Systems and Mission Assurance (OSMA) through its Software Assurance Research Program (SARP) project; Formal Approaches to Swarm Technologies (FAST); NASA Software Engineering Laboratory; Computer Science Research Institute (CSRI); Centre for Software Process Technologies (CSPT); Invest NI through the Centres of Excellence Programme, under the EU Peace II initiative FX Part of this work has been supported by the NASA Office of Systems and Mission Assurance (OSMA) through its Software Assurance Research Program (SARP) project, Formal Approaches to Swarm Technologies (FAST), and by NASA Software Engineering Laboratory, Goddard Space Flight Center (Code 581). This research is partly supported at University of Ulster by the Computer Science Research Institute (CSRI) and the Centre for Software Process Technologies (CSPT) which is funded by Invest NI through the Centres of Excellence Programme, underthe EU Peace II initiative. NR 16 TC 2 Z9 2 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2530-X J9 IEEE INT C ENG COMP PY 2006 BP 163 EP + PG 2 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering SC Computer Science GA BFB85 UT WOS:000240909700017 ER PT B AU Lei, SL Palazzolo, A AF Lei, Shuliang Palazzolo, Alan BE Pan, JS Shi, P Zhao, Y TI Real time digital control of magnetic bearings with microprocessors SO ICICIC 2006: FIRST INTERNATIONAL CONFERENCE ON INNOVATIVE COMPUTING, INFORMATION AND CONTROL, VOL 2, PROCEEDINGS LA English DT Proceedings Paper CT 1st International Conference on Innovative Computing, Information and Control (ICICIC 2006) CY AUG 30-SEP 01, 2006 CL Beijing, PEOPLES R CHINA SP IEEE, ICIC Int, Natl Nat Sci Fdn China, Beijing Jiaotong Univ, Kaohsiung Univ Appl Sci AB This paper presents the work on the real time implementation of digital controllers applied to magnetic bearings to levitate high speed rotor systems. Microprocessor is employed for digital signal processing. The control loop consists of PID controller, tracking and fixed notch filters, lead compensators, and feedforward stage, etc. The controller is implemented with TI TMS320C67 processor incorporated with LabVIEW data acquisition and graphical user interface. Digital signal processing techniques including bilinear transformation, frequency pre-warping, digital filter design and I/O communications are applied to implement the control rule. The real time controller has been successfully applied to the levitations of a Revolver Test Rig in Vibration Control Lab at Texas A&M and the Energy Storage Flywheel System used by industries for vehicles. C1 [Lei, Shuliang] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Palazzolo, Alan] Texas A&M Univ, College Stn, TX 77843 USA. RP Lei, SL (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2616-0 PY 2006 BP 154 EP + PG 2 WC Automation & Control Systems; Computer Science, Artificial Intelligence; Computer Science, Theory & Methods; Engineering, Electrical & Electronic; Imaging Science & Photographic Technology SC Automation & Control Systems; Computer Science; Engineering; Imaging Science & Photographic Technology GA BFB64 UT WOS:000240868000038 ER PT S AU Zhang, YS Fu, JC Tai, AT Chau, S Vatan, F Fijany, A AF Zhang, Yansheng Fu, Jicheng Tai, Ann T. Chau, Savio Vatan, Farrokh Fijany, Amir GP IEEE Comp Soc TI QoS adaptive ISHM systems SO ICTAI-2006: EIGHTEENTH INTERNATIONAL CONFERENCE ON TOOLS WITH ARTIFICIAL INTELLIGENCE, PROCEEDINGS SE Proceedings-International Conference on Tools With Artificial Intelligence LA English DT Proceedings Paper CT 18th International Conference on Tools with Artificial Intelligence (ICTAI-2006) CY NOV 13-15, 2006 CL Washington, DC SP IEEE Comp Soc, Biol & Artificial Intelligence Soc, ITRI Wright State Univ, Virginia Tech CS Dept AB Embedded systems are becoming highly complex and increasingly being used in critical applications. Integrated system health management (ISHM) techniques have therefore been developed to ensure the proper operation of these systems. However, some ISHM systems are relatively complex and may consume a significant amount of resources. In some situations, activating the full ISHM system may cause resource contention and prevents the target system from timely completing critical tasks. Thus it is imperative to introduce the notion of adaptivity into ISHM systems. This paper systematically discusses the issues that need to be addressed in an adaptive ISHM system with a focus on adaptation in terms of QoS aspects. A novel model, Adaptive Diagnosis Quality-Oriented System Model (ADQSM), is proposed to model the QoS specification and fault diagnosis quality measurement issues as well as the abstraction of the adaptation problem. We then present the method to evaluate various diagnosability attributes based on a modified fault signature matrix. We further map the ADQSM model to the Particle Swarm Optimization (PSO) problem model and use PSO for rapid configuration decision making. C1 [Zhang, Yansheng; Fu, Jicheng] Univ Texas, Dallas, TX 75230 USA. [Tai, Ann T.] IA Tech Inc, Dallas, TX USA. [Chau, Savio; Vatan, Farrokh; Fijany, Amir] Jet Propuls Lab, Pasadena, CA USA. RP Zhang, YS (reprint author), Univ Texas, Dallas, TX 75230 USA. EM yxz037000@utdallas.edu; jxf024000@utdallas.edu; a.t.tai@ieee.org; savio.n.chau@jpl.nasa.gov; farrokh.vatan@jpl.nasa.gov; amir.fijany@jpl.nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA SN 1082-3409 BN 978-0-7695-2728-4 J9 PROC INT C TOOLS ART PY 2006 BP 47 EP + PG 2 WC Computer Science, Artificial Intelligence SC Computer Science GA BFW79 UT WOS:000245172700007 ER PT S AU Pathak, J Basu, S Lutz, R Honavar, V AF Pathak, Jyotishunan Basu, Samik Lutz, Robyn Honavar, Vasant GP IEEE Comp Soc TI Selecting and composing web services through iterative reformulation of functional specifications SO ICTAI-2006: EIGHTEENTH INTERNATIONAL CONFERENCE ON TOOLS WITH ARTIFICIAL INTELLIGENCE, PROCEEDINGS SE Proceedings-International Conference on Tools With Artificial Intelligence LA English DT Proceedings Paper CT 18th International Conference on Tools with Artificial Intelligence (ICTAI-2006) CY NOV 13-15, 2006 CL Washington, DC SP IEEE Comp Soc, Biol & Artificial Intelligence Soc, ITRI Wright State Univ, Virginia Tech CS Dept AB We propose a specification-driven approach to Web service composition. The proposed framework allows users to start with a high-level, possibly incomplete specification of a desired (goal),service that is to be realized using a subset of the available component services. These services are represented by the system using transition systems augmented with guards over variables with infinite domains and are used to determine a strategy for their composition that would realize the goal service. In the event that the goal service cannot be realized using the available services, the system identifies the cause(s) for such failure which can then be used by the developer to reformulate the goal specification. Thus, the system supports Web service composition though iterative refinement of the functional specifications. We present a prototype implementation in tabled-logic programming environment that illustrates the key features of the proposed approach. C1 [Pathak, Jyotishunan; Basu, Samik; Lutz, Robyn; Honavar, Vasant] Iowa State Univ, Dept Comp Sci, Ames, IA 50011 USA. [Pathak, Jyotishunan; Honavar, Vasant] Iowa State Univ, Ctr Comp Intelligence Learn & Discovery, Ames, IA 50011 USA. [Lutz, Robyn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pathak, J (reprint author), Iowa State Univ, Dept Comp Sci, Ames, IA 50011 USA. EM jpathak@cs.iastate.edu; sbasu@cs.iastate.edu; rlutz@cs.iastate.edu; honavar@cs.iastate.edu RI Honavar, Vasant/K-9835-2015 OI Honavar, Vasant/0000-0001-5399-3489 FU Iowa State University Center for Computational Intelligence Learning and Discovery; NSF-ITR [0219699]; NSF [0509340, 0541163] FX This research has been supported in parts by the Iowa State University Center for Computational Intelligence Learning and Discovery ( http://www.cild.iastate.edu), NSF-ITR grant 0219699 toVasant Honavar, NSF grant 0509340 to Samik Basu, and NSF grant 0541163 to Robyn Lutz NR 21 TC 2 Z9 2 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA SN 1082-3409 BN 978-0-7695-2728-4 J9 PROC INT C TOOLS ART PY 2006 BP 445 EP + PG 2 WC Computer Science, Artificial Intelligence SC Computer Science GA BFW79 UT WOS:000245172700058 ER PT B AU Florescu, M Scheel, S Lee, H Knight, PL Bowling, JP AF Florescu, Marian Scheel, Stefan Lee, Hwang Knight, Peter L. Bowling, Jonathan P. BE Marciniak, M TI Three-dimensional photonic band-gap structures for single-photon on demand sources SO ICTON 2006: 8TH INTERNATIONAL CONFERENCE ON TRANSPARENT OPTICAL NETWORKS, VOL 2, PROCEEDINGS: ESPC, NAON LA English DT Proceedings Paper CT 8th International Conference on Transparent Optical Networks CY JUN 18-22, 2006 CL Nottingham, ENGLAND SP IEEE Univ Nottingham, IEEE/LEOS, Univ Nottingham, George Green Inst Electromagnet Res, Natl Inst Telecommun, LEOS Poland Chapter, Photon Design, European Cooperat Field Sci & Tech Res, RSOFT Design Grp ID QUANTUM CRYPTOGRAPHY; TURNSTILE DEVICE; STATES; DOT AB We describe a practical implementation of a semi-deterministic photon gun based on the stimulated Raman adiabatic passage pumping and the nonlinear tuning of the photonic density of states in a photonic band-gap material. We show that this device allows deterministic and unidirectional production of single photons with a high repetition rate of the order of 100 kHz. We also discuss specific 3D photonic microstructure architectures in which our model can be realized and the feasibility of implementing such a device using Er3+ ions that produce single photons at the telecommunication wavelength of 1.55 microns. C1 [Florescu, Marian] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr,MS 126-347, Pasadena, CA 91109 USA. [Florescu, Marian; Lee, Hwang; Bowling, Jonathan P.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Scheel, Stefan; Knight, Peter L.] Imperial Coll London, QOLS, Blackett Lab, London, ON SW72BW, Canada. RP Florescu, M (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr,MS 126-347, Pasadena, CA 91109 USA. EM marian.florescu@jpl.nasa.gov NR 22 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 1-4244-0235-2 PY 2006 BP 40 EP + PG 2 WC Engineering, Electrical & Electronic; Optics; Telecommunications SC Engineering; Optics; Telecommunications GA BEZ67 UT WOS:000240400000011 ER PT S AU Yanushkevich, SN Stoica, A Shmerko, VR AF Yanushkevich, S. N. Stoica, A. Shmerko, V. R. GP IEEE TI Experience of design and prototyping of a multi-biometric early warning physical access control security system (PASS) and a training system (T-PASS) SO IECON 2006 - 32ND ANNUAL CONFERENCE ON IEEE INDUSTRIAL ELECTRONICS, VOLS 1-11 SE IEEE Industrial Electronics Society LA English DT Proceedings Paper CT 32nd Annual Conference of the IEEE-Industrial-Electronics-Society CY NOV 07-10, 2006 CL Paris, FRANCE SP IEEE Ind Elect Soc ID FACIAL EXPRESSIONS AB This paper presents a concept of biometric-based early-warning and intelligent support for physical access security system (PASS). The early warning principle exploits the real-time analysis of the biometrics of the individual being scanned. Binding all sources of information into an objective supported by intelligence tools not only provides for reliable identification of an individual, but also supplies data for situational awareness and risk management support. An intelligent approach serves for interpretation of biometric data in semantic form, as well as dialogue support between the officer and the customer. The training-extended PASS (T-PASS) is built on the PASS, and aims at assisting the security personnel in developing decision making skills. The PASS and T-PASS are directed at a wide spectrum of applications such as immigration service and border control airports, seaports, border-crossing, security of important public events, hospitals and banking. C1 [Yanushkevich, S. N.; Shmerko, V. R.] Univ Calgary, Dept Elect & Comp Engn, 2500 Univ Drive NW, Calgary, AB T2N 1N4, Canada. [Stoica, A.] NASA, CALTECH, Jet Prop Lab, Humanoid Robot Lab, Pasadena, CA USA. RP Yanushkevich, SN (reprint author), Univ Calgary, Dept Elect & Comp Engn, 2500 Univ Drive NW, Calgary, AB T2N 1N4, Canada. EM syanshk@ucalgary.ca; Adrian.Stoica@jpl.nasa.gov; vshmerko@ucalgary.ca FU Natural Sciences and Engineering Research Council of Canada (NSERC); Canadian Foundation for Innovations (CFI); Government of the Province of Alberta; Alberta Informatics Circle of Excellence (iCore) FX This Project is partially supported by the Natural Sciences and Engineering Research Council of Canada (NSERC), the Canadian Foundation for Innovations (CFI), the Government of the Province of Alberta, and Alberta Informatics Circle of Excellence (iCore). A part of the project has been implemented as an initiative within the JPLs Humanoid Robotics Laboratory . The authors acknowledge the valuable suggestions and remarks of Eur . Ing. Mr . Phil Phillips (Department of Information Security , Office of National Statistics, UK), Dr . M. S. Nixon (University of Southampton, UK), Dr . D. J . Hurle y (Analytical Engines Ltd., UK), Dr . P . P erner (Institute of Computer Vision and Applied Computer Science, Leipzig, Germany), and Dr . R. R. Yager (Machine Intelligence Institute, Iona College, New Rochelle, USA). We also acknowledge many people who help us to understand specific-area requirements and conditions of the physical access control security technology . NR 19 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1553-572X BN 978-1-4244-0135-2 J9 IEEE IND ELEC PY 2006 BP 4334 EP + PG 2 WC Automation & Control Systems; Computer Science, Artificial Intelligence; Engineering, Electrical & Electronic SC Automation & Control Systems; Computer Science; Engineering GA BGB30 UT WOS:000245905008058 ER PT J AU Venkatesan, J AF Venkatesan, Jaikrishna TI Novel version of the double-Y balun: Microstrip to coplanar strip transition SO IEEE ANTENNAS AND WIRELESS PROPAGATION LETTERS LA English DT Article DE balun; coplanar strip (CPS); double-Y; microstrip ID UNIPLANAR BALUN AB A novel version of the double-Y balun, transitioning from a microstrip to a coplanar strip (CPS) line, is designed to feed a complementary, spiral antenna. Attractive features of the new version of the double-Y balun presented in this work include: 1) little metal content, 2) broadband performance, and 3) improved junction performance when compared to various previous versions of the double-Y balun. Performance of the new balun is evaluated via VSWR and insertion loss measurements. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Venkatesan, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Jaikrishna.Venkatesan@jpl.nasa.gov NR 10 TC 7 Z9 7 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1536-1225 J9 IEEE ANTENN WIREL PR JI IEEE Antennas Wirel. Propag. Lett. PY 2006 VL 5 BP 172 EP 174 DI 10.1109/LAWP.2006.873952 PG 3 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 130RE UT WOS:000243815900046 ER PT J AU Pan, B Yoon, YK Ponchak, GE Allen, MG Papapolymerou, J Tentzeris, MM AF Pan, Bo Yoon, Yong-Kyu Ponchak, George E. Allen, Mark G. Papapolymerou, John Tentzeris, Manos M. TI Analysis and characterization of a high-performance Ka-band surface micromachined elevated patch antenna SO IEEE ANTENNAS AND WIRELESS PROPAGATION LETTERS LA English DT Article DE air-elevated antenna; antenna feeding; on-wafer radiation pattern measurement; surface micromachining AB A novel Ka-band surface micromachined air-elevated patch antenna is designed, fabricated, and characterized. It demonstrates a 10.5%-10-dB fractional bandwidth and 9.5-dBi directivity for an elevation of 600 pm. The elevated patch is fed by a vertical epoxy-core metal-coated micromachined probe and supported by several epoxy posts underneath. By the unique feeding technique and the substrate removal approach that are presented in this letter, the performance degradation for traditional microstrip antenna directly built on high-epsilon(r) substrate can be significantly alleviated. C1 Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Pan, B (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM panbo@ece.gatech.edu NR 12 TC 15 Z9 15 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1536-1225 J9 IEEE ANTENN WIREL PR JI IEEE Antennas Wirel. Propag. Lett. PY 2006 VL 5 BP 511 EP 514 DI 10.1109/LAWP.2006.886305 PG 4 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 130RE UT WOS:000243815900134 ER PT S AU Deal, WR Din, S Radisic, V Padilla, J Mei, XB Yoshida, W Liu, PH Uyeda, J Barsky, M Gaier, T Fung, A Samoska, L Lai, R AF Deal, W. R. Din, S. Radisic, V. Padilla, J. Mei, X. B. Yoshida, W. Liu, P. H. Uyeda, J. Barsky, M. Gaier, T. Fung, A. Samoska, L. Lai, R. GP IEEE TI Demonstration of a sub-millimeter wave integrated circuit (S-MMIC) using InPHEMT with a 35-nm gate SO IEEE COMPOUND SEMICONDUCTOR INTEGRATED CIRCUIT SYMPOSIUM - 2006 IEEE CSIC SYMPOSIUM, TECHNICAL DIGEST 2006 SE IEEE Compound Semiconductor Integrated Circuit Symposium Technical Digest LA English DT Proceedings Paper CT 3rd IEEE Compound Semiconductor Integrated Circuit Symposium CY NOV 12-15, 2006 CL San Antonio, TX SP IEEE Electron Devices Soc, IEEE Microwave Theory & Tech Soc, IEEE Solid State Circuits Soc DE low noise amplifier; HEMT; MMIC; S-MMIC; millimeter-wave; sub-millimeter wave; coplanar waveguide ID AMPLIFIER AB In this paper, we present two single stage MMIC amplifiers with the first demonstrating a measured S-21 gain of 3-dB at 280-GHz and the second demonstrating 2.5-dB gain at 300-GHz, which is the threshold of the sub-millimeter wave regime. The high-frequency operation is enabled by a high-speed InP HEMT with a 35-nm gate. This is the first demonstrated S-21 gain at sub-millimeter wave frequencies in a MMIC. C1 [Deal, W. R.; Din, S.; Radisic, V.; Padilla, J.; Mei, X. B.; Yoshida, W.; Liu, P. H.; Uyeda, J.; Barsky, M.] Northrop Grumman Space & Miss Syst, Redondo Beach, CA 90278 USA. [Gaier, T.; Fung, A.; Samoska, L.; Lai, R.] Jet Prop Lab, Pasadena, CA 91109 USA. RP Deal, WR (reprint author), Northrop Grumman Space & Miss Syst, Redondo Beach, CA 90278 USA. FU DARPA SWIFT Program; Army Research Laboratory under the ARL [W911QX-06-C-0050] FX This work was supported by the DARPA SWIFT Program and Army Research Laboratory under the ARL Contract no. W911QX-06-C-0050. The authors would like to thank Dr. Mark Rosker (DARPA) and Dr. Alfred Hung (ARL). This research 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 5 TC 9 Z9 9 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1550-8781 BN 978-1-4244-0126-0 J9 COMP SEMICOND INTEGR PY 2006 BP 33 EP 36 PG 4 WC Engineering, Electrical & Electronic SC Engineering GA BFU09 UT WOS:000244612000008 ER PT B AU Stefatos, EF Arslan, T Keymeulen, D Ferguson, I AF Stefatos, Evangelos F. Arslan, Tughrul Keymeulen, Didier Ferguson, Ian BE Becker, J Herkersdorf, A Mukherjee, A Smailagic, A TI Autonomous realization of Boeing/JPL sensor electronics based on reconfigurable system-on-chip technology SO IEEE COMPUTER SOCIETY ANNUAL SYMPOSIUM ON VLSI, PROCEEDINGS: EMERGING VLSI TECHNOLOGIES AND ARCHITECTURES LA English DT Proceedings Paper CT IEEE-Computer-Society Annual Symposium on VLSI CY MAR 02-03, 2006 CL Karlsruhe, GERMANY SP IEEE Comp Soc, TC VLSI AB This paper presents a reconfigurable architecture that is specifically tailored for the autonomous realization of the Boeing/JPL gyroscope and its interface circuitry. The overall architecture consists of a reconfigurable hardware substrate that suits the implementation of transposed form FIR filters and a custom non-stochastic search algorithm, which is in charge of autonomously providing the best binary configuration on the adaptive hardware. Preliminary simulation results show that our architecture is able to cope with single hard errors that occur on the reconfigurable substrate, while power analysis demonstrates that the proposed methodology is capable of implementing filters that consume almost 4.5 times less power, compared with industrial application specific reconfigurable fabrics. C1 [Stefatos, Evangelos F.; Arslan, Tughrul] Univ Edinburgh, Sch Engn & Elect, Kings Bldgs,Mayfield Rd, Edinburgh EH9 3JL, Midlothian, Scotland. [Keymeulen, Didier; Ferguson, Ian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Stefatos, EF (reprint author), Univ Edinburgh, Sch Engn & Elect, Kings Bldgs,Mayfield Rd, Edinburgh EH9 3JL, Midlothian, Scotland. EM Evangelos.Stefatos@ee.ed.ac.uk; Didier.Keymeulen@jpl.nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2533-4 PY 2006 BP 85 EP + PG 2 WC Computer Science, Hardware & Architecture SC Computer Science GA BEG58 UT WOS:000237225200013 ER PT J AU Koetz, B Morsdorf, F Sun, G Ranson, KJ Itten, K Allgower, B AF Koetz, B Morsdorf, F Sun, G Ranson, KJ Itten, K Allgower, B TI Inversion of a lidar waveform model for forest biophysical parameter estimation SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE biophysical parameters; fcover; inversion; leaf area index (LAI); light detection and ranging (lidar) waveform; three-dimensional (3-D) model; tree height ID LASER ALTIMETER; CANOPY STRUCTURE; VEGETATION; STANDS; LEVEL; LEAF AB Due to its measurement principle, light detection and ranging (lidar) is particularly suited to estimate the horizontal as well as vertical distribution of forest structure. Quantification and characterization of forest structure is important for the understanding of the forest ecosystem functioning and, moreover, will help to assess carbon sequestration within forests. The relationship between the signal recorded by a lidar system and the canopy structure of a forest can be accurately characterized by physically based radiative transfer models (RTMs). A three-dimensional RTM is capable of representing the complex forest canopy structure as well as the involved physical processes of the lidar pulse interactions with the vegetation. Consequently, the inversion of such an RTM presents a novel concept to retrieve biophysical forest parameters that exploits the full lidar signal and underlying physical processes. A synthetic dataset and data acquired in the Swiss National Park (SNP) successfully demonstrated the feasibility and the potential of RTM inversion to retrieve forest structure from large-footprint lidar waveform data. The SNP lidar data consist of waveforms generated from the aggregation of small-footprint lidar returns. Derived forest biophysical parameters, such as fractional cover, leaf area index, maximum tree height, and the vertical crown extension, were able to describe the horizontal and vertical forest canopy structure. C1 Univ Zurich, Remote Sensing Labs, CH-8057 Zurich, Switzerland. Univ Maryland, Dept Geog, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. Univ Zurich, Geog Informat Syst, CH-8057 Zurich, Switzerland. RP Koetz, B (reprint author), Univ Zurich, Remote Sensing Labs, CH-8057 Zurich, Switzerland. EM bkoetz@geo.unizh.ch RI Morsdorf, Felix/D-1151-2010; Ranson, Kenneth/G-2446-2012 OI Ranson, Kenneth/0000-0003-3806-7270 NR 21 TC 41 Z9 43 U1 0 U2 26 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JAN PY 2006 VL 3 IS 1 BP 49 EP 53 DI 10.1109/LGRS.2005.856706 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 006LJ UT WOS:000234898700011 ER PT J AU Masek, JG Vermote, EF Saleous, NE Wolfe, R Hall, FG Huemmrich, KF Gao, F Kutler, J Lim, TK AF Masek, JG Vermote, EF Saleous, NE Wolfe, R Hall, FG Huemmrich, KF Gao, F Kutler, J Lim, TK TI A Landsat surface reflectance dataset for North America, 1990-2000 SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE atmospheric correction; Landsat; remote sensing ID OPERATIONAL ATMOSPHERIC CORRECTION; MODIS DATA; CALIBRATION; RESOLUTION; ALGORITHM; AEROSOL; IMAGERY AB The Landsat Ecosystem Disturbance Adaptive Processing System (LEDAPS) at the National Aeronautics and Space Administration (NASA) Goddard Space Flight Center has processed and released 2100 Landsat Thematic Mapper and Enhanced Thematic Mapper Plus surface reflectance scenes, providing 30-m resolution wall-to-wall reflectance coverage for North America for epochs centered on 1990 and 2000. This dataset can support decadal assessments of environmental and land-cover change, production of reflectance-based biophysical products, and applications that merge reflectance data from multiple sensors [e.g., the Advanced Spaceborne Thermal Emission and Reflection Radiometer, Multiangle Imaging Spectroradiometer, Moderate Resolution Imaging Spectroradiometer (MODIS)]. The raw imagery was obtained from the orthorectified Landsat GeoCover dataset, purchased by NASA from the Earth Satellite Corporation. Through the LEDAPS project, these data were calibrated, converted to top-of-atmosphere reflectance, and then atmospherically corrected using the MODIS/6S methodology. Initial comparisons with ground-based optical thickness measurements and simultaneously acquired MODIS imagery indicate comparable uncertainty in Landsat surface reflectance compared to the standard MODIS reflectance product (the greater of 0.5% absolute reflectance or 5% of the recorded reflectance value). The rapid automated nature of the processing stream also paves the way for routine high-level products from future Landsat sensors. C1 NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. RP Masek, JG (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. EM jeffrey.g.masek@nasa.gov RI Gao, Feng/F-3944-2010; Masek, Jeffrey/D-7673-2012; Wolfe, Robert/E-1485-2012; Vermote, Eric/K-3733-2012 OI Wolfe, Robert/0000-0002-0915-1855; NR 20 TC 425 Z9 433 U1 12 U2 90 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JAN PY 2006 VL 3 IS 1 BP 68 EP 72 DI 10.1109/LGRS.2005.857030 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 006LJ UT WOS:000234898700015 ER PT J AU Dasgupta, S Qu, JJ Hao, XJ AF Dasgupta, S Qu, JJ Hao, XJ TI Design of a susceptibility index for fire risk monitoring SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE fire susceptibility index (FSI); preignition heat energy; wildfire risk ID WATER-CONTENT; VEGETATION; SATELLITE; MODELS; REFLECTANCE AB In this letter, we present a new remote sensing fire susceptibility index (FSI) based on the physical concept of heat energy of preignition. This physical basis allows computations of ignition probabilities and comparisons of fire risk across ecoregions. The index has the flexibility to be localized to a vegetation type or ecoregion for improved performance. The computation of the index requires inputs of fuel temperature and fuel moisture content, both of which can be estimated using remote sensing techniques. While Moderate Resolution Imaging Spectrometer data for surface temperature are used as a proxy for fuel temperature, live fuel moisture is estimated by a linear regression technique utilizing the correlation between model-based live fuel moisture measurements at automated ground stations and the ratio of normalized difference vegetation index and surface temperature. FSIs are computed for the Georgia region during the spring and summer months of 2004 and validated with the well-tested fire potential index (FPI). Results show a good agreement between FSI and FPI. It suggests that FSI can be a good estimator of fire risk. C1 George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Dasgupta, S (reprint author), George Mason Univ, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. EM sdasgupt@gmu.edu; jqu@gmu.edu; xhao1@gmu.edu RI Hao, Xianjun/F-7253-2016; Hao, Xianjun/C-9543-2011 OI Hao, Xianjun/0000-0002-8186-6839; Hao, Xianjun/0000-0002-8186-6839 NR 16 TC 9 Z9 9 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JAN PY 2006 VL 3 IS 1 BP 140 EP 144 DI 10.1109/LGRS.2005.858484 PG 5 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 006LJ UT WOS:000234898700030 ER PT J AU Wen, GY Marshak, A Cahalan, RF AF Wen, GY Marshak, A Cahalan, RF TI Impact of 3-D clouds on clear-sky reflectance and aerosol retrieval in a biomass burning region of Brazil SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS LA English DT Article DE aerosols; clouds; International Intercomparison of 3D Radiation Codes (I3RC); scattering; solar radiation; threedimensional (3-D) radiative transfer ID RADIATIVE-TRANSFER; WATER CLOUDS; PRODUCTS; ATMOSPHERES; VALIDATION; TERRA AB Three-dimensional (3-D) cloud radiative effects on clear-sky reflectances and associated aerosol optical depth retrievals are quantified for a cumulus cloud field in a biomass burning region in Brazil through a Monte Carlo simulation. In this study the 1-km Moderate Resolution Imaging Spectroradiometer cloud optical depth and surface reflectance datasets are used to compute the 3-D radiation fields with ambient aerosol optical thickness of 0.1 at a wavelength of 0.66 mu m. The 3-D radiative effects range from -0.015 to 0.018 with an average of 0.004 and standard deviation of 0.006. The 3-D effects are most pronounced and variable for cloud neighboring pixels, where both large negative effects over shadows and positive effects near sunlit cloud edges are found. The clear next-to-cloud pixels, that contain similar to 83% of the clear pixel population, are affected in the most complex way and not reliable for aerosol retrieval. In the area 2 km away from clouds, the 3-D effects enhance the reflectance in clear patches. The average and variability of enhancements gradually decrease as a function of the cloud-free distance, resulting in a systematically higher aerosol optical depth estimates for pixels closer to clouds in one-dimensional (1-D) retrieval. At a distance of 3 km away from clouds, the 3-D effect is still appreciable with the average enhancement slightly less than 0.004. This enhancement will lead to an over estimate of aerosol optical thickness of similar to 0.04 in 1-D retrieval, which is significant for an ambient atmosphere with aerosol optical thickness of 0.1. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Catonsville, MD 21228 USA. RP Wen, GY (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM wen@climate.gsfc.nasa.gov RI Cahalan, Robert/E-3462-2012; Marshak, Alexander/D-5671-2012 OI Cahalan, Robert/0000-0001-9724-1270; NR 19 TC 35 Z9 36 U1 0 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1545-598X J9 IEEE GEOSCI REMOTE S JI IEEE Geosci. Remote Sens. Lett. PD JAN PY 2006 VL 3 IS 1 BP 169 EP 172 DI 10.1109/LGRS.2005.861386 PG 4 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 006LJ UT WOS:000234898700036 ER PT J AU Semmel, GS Davis, SR Leucht, KW Rowe, DA Smith, KE Boloni, L AF Semmel, GS Davis, SR Leucht, KW Rowe, DA Smith, KE Boloni, L TI Space Shuttle ground processing with monitoring agents SO IEEE INTELLIGENT SYSTEMS LA English DT Editorial Material C1 NASA, Kennedy Space Ctr, Engn Dev Directorate, Kennedy Space Ctr, FL 32899 USA. Univ Cent Florida, Sch Elect Engn & Comp Sci, Orlando, FL 32816 USA. NASA, Kennedy Space Ctr, Shuttle Proc Directorate, Kennedy Space Ctr, FL 32899 USA. RP Semmel, GS (reprint author), NASA, Kennedy Space Ctr, Engn Dev Directorate, Kennedy Space Ctr, FL 32899 USA. EM glenn.s.semmel@nasa.gov; steve.davis@nasa.gov; kurt.leucht@nasa.gov; daniel.a.rowe@nasa.gov; e.smith@nasa.gov; lboloni@cs.ucf.edu NR 9 TC 3 Z9 4 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1541-1672 J9 IEEE INTELL SYST JI IEEE Intell. Syst. PD JAN-FEB PY 2006 VL 21 IS 1 BP 68 EP 73 DI 10.1109/MIS.2006.17 PG 6 WC Computer Science, Artificial Intelligence; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 006TV UT WOS:000234921100013 ER PT B AU Chien, S Cichy, B Davies, A Tran, D Rabideau, G Castano, R Sherwood, R Nghiem, S Mandl, D Frye, S Shulman, S Ungar, S Brakke, T Ong, L Descloitres, J Jones, J Grosvenor, S AF Chien, Steve Cichy, Ben Davies, Ashley Tran, Daniel Rabideau, Gregg Castano, Rebecca Sherwood, Rob Nghiem, Son Mandl, Dan Frye, Stuart Shulman, Seth Ungar, Stephen Brakke, Thomas Ong, Lawrence Descloitres, Jacques Jones, Jeremy Grosvenor, Sandy BE Werner, B TI An autonomous earth observing sensorweb SO IEEE INTERNATIONAL CONFERENCE ON SENSOR NETWORKS, UBIQUITOUS, AND TRUSTWORTHY COMPUTING, VOL 1, PROCEEDINGS LA English DT Proceedings Paper CT IEEE International Conference on Sensor Networks, Ubiquitous, and Trustworthy Computing CY JUN 05-07, 2006 CL Tai Chung, TAIWAN SP IEEE Comp Soc, Asia Univ, Natl Sci Council, USA Force Off Sci Res, Asian Off Aerosp Res & Dev, Inst Informat Ind, Minist Educ ID MODIS AB We describe a network of sensors linked by software and the internet to an autonomous satellite observation response capability. This sensor network is designed with a flexible, modular, architecture to facilitate expansion in sensors, customization of trigger conditions, and customization of responses. This system has been used to implement a global surveillance Program of multiple science phenomena including: volcanoes, flooding, cryosphere events, and atmospheric phenomena. In this paper we describe the importance of the Earth observing sensorweb application as well as overall architecture for the network. C1 [Chien, Steve; Cichy, Ben; Davies, Ashley; Tran, Daniel; Rabideau, Gregg; Castano, Rebecca; Sherwood, Rob; Nghiem, Son] CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. [Mandl, Dan; Frye, Stuart; Shulman, Seth; Ungar, Stephen; Brakke, Thomas; Ong, Lawrence; Descloitres, Jacques; Jones, Jeremy; Grosvenor, Sandy] Goddard Space Flight Ctr, Greenbelt, MD USA. RP Chien, S (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. NR 21 TC 0 Z9 0 U1 0 U2 2 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2553-9 PY 2006 BP 178 EP + PG 2 WC Computer Science, Theory & Methods; Telecommunications SC Computer Science; Telecommunications GA BEQ69 UT WOS:000238969200023 ER PT J AU Maleki, L AF Maleki, L TI Introduction to the issue on microresonators SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS LA English DT Editorial Material C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Maleki, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 0 TC 3 Z9 3 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1077-260X J9 IEEE J SEL TOP QUANT JI IEEE J. Sel. Top. Quantum Electron. PD JAN-FEB PY 2006 VL 12 IS 1 BP 1 EP 2 DI 10.1109/JSTQE.2005.862846 PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 012WL UT WOS:000235371500001 ER PT J AU Matsko, AB Ilchenko, VS AF Matsko, AB Ilchenko, VS TI Optical resonators with whispering-gallery modes - Part I: Basics SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS LA English DT Review DE four-wave mixing; high-order optical filters; lasers; laser resonators; monolithic optical total internal reflection resonators; morphology dependent resonances; nonlinear optics; optical filters; optical resonators; parametric optics; Q-factor; solid-state lasers; spectroscopy; tunable filters; wave mixing; whispering-gallery mode (WGM) resonators ID MORPHOLOGY-DEPENDENT RESONANCES; STIMULATED RAMAN-SCATTERING; FUSED-SILICA MICROSPHERES; CHANNEL DROPPING FILTERS; INAS QUANTUM BOXES; PRISM-FILM COUPLER; NEAR-FIELD PROBE; DIELECTRIC SPHERES; DIRECTIONAL EMISSION; WAVE-GUIDES AB We briefly review basic properties of dielectric whispering gallery mode resonators that are important for applications of the resonators in optics and photonics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Matsko, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Andrey.Matsko@jpl.nasa.gov; ilcheriko@jpl.nasa.gov RI Matsko, Andrey/A-1272-2007 NR 177 TC 366 Z9 371 U1 33 U2 243 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1077-260X J9 IEEE J SEL TOP QUANT JI IEEE J. Sel. Top. Quantum Electron. PD JAN-FEB PY 2006 VL 12 IS 1 BP 3 EP 14 DI 10.1109/JSTQE.2005.862952 PG 12 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 012WL UT WOS:000235371500002 ER PT J AU Ilchenko, VS Matsko, AB AF Ilchenko, VS Matsko, AB TI Optical resonators with whispering-gallery modes - Part II: Applications SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS LA English DT Review DE four-wave mixing (FWM); high-order optical filters; lasers; laser resonators; monolithic optical total internal reflection resonators; morphology dependent resonances; nonlinear optics; optical filters; optical resonators; parametric optics; Q-factor; solid state lasers; spectroscopy; tunable filters; wave mixing; whispering-gallery mode (WGM) resonators ID STIMULATED RAMAN-SCATTERING; MORPHOLOGY-DEPENDENT RESONANCES; OPTOELECTRONIC MICROWAVE-OSCILLATOR; CAVITY QUANTUM ELECTRODYNAMICS; GLASS MICROSPHERE LASER; CYLINDRICAL MICROCAVITY LASER; POLYMER MICRORING RESONATORS; 2ND-ORDER FILTER RESPONSE; CHANNEL-DROPPING FILTERS; MICROMETER-SIZE DROPLETS AB We review photonic applications of dielectric whispering-gallery mode (WGM) resonators-tracing the growth of the technology from experiments with levitating droplets of aerosols to ultrahigh-Q solid state crystalline and integrated on-chip microresonators. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ilchenko, VS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM vladimir@jpl.nasa.gov; andery.matsko@jpl.nasa.gov RI Matsko, Andrey/A-1272-2007 NR 295 TC 303 Z9 305 U1 31 U2 260 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1077-260X J9 IEEE J SEL TOP QUANT JI IEEE J. Sel. Top. Quantum Electron. PD JAN-FEB PY 2006 VL 12 IS 1 BP 15 EP 32 DI 10.1109/JSTQE.2005.862943 PG 18 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 012WL UT WOS:000235371500003 ER PT B AU de Asis, E Ngo, Q Wong, WK Isaacson, MS Yang, CY AF de Asis, E. Ngo, Q. Wong, W. K. Isaacson, M. S. Yang, C. Y. GP IEEE TI Carbon nanostructures as interconnect and interface materials SO IEEE NMDC 2006: IEEE NANOTECHNOLOGY MATERIALS AND DEVICES CONFERENCE 2006, PROCEEDINGS LA English DT Proceedings Paper CT IEEE Nanotechnology Materials and Devices Conference CY OCT 22-25, 2006 CL Gyeongju, SOUTH KOREA SP IEEE DE carbon nanofiber; carbon nanotube; interconnect; microelectrode array; neuron ID NANOFIBERS AB Recent studies on carbon-based nanostructures have given rise to promising prospects for new applications in electrical and biological systems. In this work, our recent efforts investigating the utility of carbon nanotube (CNT) and carbon nanofiber (CNF) devices in electrical and biological interconnect systems are reviewed. Reliability measurements are performed to demonstrate the robust nature of CNFs. Concurrently, a microelectrode array (MEA) consisting of a two-dimensional (2D) pattern of CNT recording sites is used to detect in vitro the electrical signals in embryonic rat hippocampal neurons. C1 [de Asis, E.; Ngo, Q.; Yang, C. Y.] Santa Clara Univ, Ctr Nanostruct, Santa Clara, CA 95053 USA. [Ngo, Q.] NASA, Ames Res Ctr, Moffett Field, CA USA. [Wong, W. K.] Natl Univ Singapore, Dept Elect Engn, Singapore, Singapore. [Isaacson, M. S.] Univ California, Dept Elect Engn, Santa Cruz, CA USA. RP de Asis, E (reprint author), Santa Clara Univ, Ctr Nanostruct, Santa Clara, CA 95053 USA. EM cyang@scu.edu FU NASA ARC FX The authors are grateful to A. Cassell, J. Li, and M. Meyyappan at NASA Ames Research Center (ARC) for assistance in fabricating and characterizing test structures for the CNF electrical interconnects, and M. Freund at NASA ARC for financial and facilities support. NR 9 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-0540-4 PY 2006 BP 146 EP + PG 2 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology SC Engineering; Science & Technology - Other Topics GA BHM97 UT WOS:000254409500028 ER PT B AU Seo, JT Ma, SM Yang, Q Battle, R Creekmore, L Tabibi, B Yoo, KP Kim, SY Jung, SS Namkung, M AF Seo, J. T. Ma, S. M. Yang, Q. Battle, R. Creekmore, L. Tabibi, B. Yoo, K. P. Kim, S. Y. Jung, S. S. Namkung, M. GP IEEE TI Polarization-resolved cubic nonlinearity and optical power limiting of highly porous silica nanoaerogels SO IEEE NMDC 2006: IEEE NANOTECHNOLOGY MATERIALS AND DEVICES CONFERENCE 2006, PROCEEDINGS LA English DT Proceedings Paper CT IEEE Nanotechnology Materials and Devices Conference CY OCT 22-25, 2006 CL Gyeongju, SOUTH KOREA SP IEEE DE optical power limiting; nonlinear susceptibility; silica nanoaerogels ID AEROGEL AB A highly porous silica nanoacrogel has a strong optical power limiting behavior with a negative nonlinear property. The third-order nonlinear susceptibility of silica nanoaerogels was estimated to be similar to 9.6x 10(-19) m(2)/V-2 (similar to 6.9x10(-11) esu) from DFWM measurements. C1 [Seo, J. T.; Ma, S. M.; Yang, Q.; Battle, R.; Creekmore, L.; Tabibi, B.] Hampton Univ, Dept Phys, Hampton, VA 23668 USA. [Yoo, K. P.; Kim, S. Y.] Sogang Univ, Dept Chem Engn, Seoul 121742, South Korea. [Jung, S. S.] Korea Res Inst Stand & Sci, Daejeon 305600, South Korea. [Namkung, M.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. RP Seo, JT (reprint author), Hampton Univ, Dept Phys, Hampton, VA 23668 USA. EM jaetae.seo@hamptonu.edu RI Namkung, Min/E-1533-2012 FU Army Research Laboratory [DAAD17-02-C-0107]; Army Research Office [DAAD19-03-1-0011, W911NF-04-1-0393]; National Science Foundation [HRD-0630372, EEC- 0532472, HRD-0400041, PHY0139048]; Department of Energy [DE-FG02-97ER41035] FX This work at Hampton University was supported by Army Research Laboratory (DAAD17-02-C-0107), Army Research Office (DAAD19-03-1-0011, W911NF-04-1-0393), National Science Foundation (HRD-0630372, EEC- 0532472, HRD-0400041, PHY0139048), and Department of Energy (DE-FG02-97ER41035). NR 7 TC 0 Z9 0 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4244-0540-4 PY 2006 BP 534 EP + PG 2 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology SC Engineering; Science & Technology - Other Topics GA BHM97 UT WOS:000254409500192 ER PT J AU Wu, JF Jiang, SB Luo, T Geng, JH Peyghambarian, N Barnes, NP AF Wu, JF Jiang, SB Luo, T Geng, JH Peyghambarian, N Barnes, NP TI Efficient thulium-doped 2-mu m germanate fiber laser SO IEEE PHOTONICS TECHNOLOGY LETTERS LA English DT Article DE germanate glass; optical fiber lasers; slope efficiency; thulium ID CW AB We report an efficient fiber laser operating near 2 gm. The glass for the fiber is germanate that is highly doped with thulium. The effect of cross relaxation energy transfer between thulium ions as observed from emission spectrum of the glass samples results in the laser having a very high slope efficiency of 58% with respect to launched power. This corresponds to a quantum efficiency of 1.79, indicating that each pump photon leads to near 1.8 excited Tm3+ ions. C1 Npphoton Inc, Tucson, AZ 85747 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Wu, JF (reprint author), Npphoton Inc, Tucson, AZ 85747 USA. EM Jiang@npphotonics.com NR 9 TC 48 Z9 60 U1 1 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1041-1135 J9 IEEE PHOTONIC TECH L JI IEEE Photonics Technol. Lett. PD JAN-FEB PY 2006 VL 18 IS 1-4 BP 334 EP 336 DI 10.1109/LPT.2005.861970 PG 3 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 020HL UT WOS:000235899300110 ER PT J AU Elfes, A Lincoln, WP Rodriguez, G Weisbin, CR Wertz, JA AF Elfes, A Lincoln, WP Rodriguez, G Weisbin, CR Wertz, JA TI Risk-based technology portfolio optimization for early space mission design SO IEEE TRANSACTIONS ON AEROSPACE AND ELECTRONIC SYSTEMS LA English DT Article AB The successful design, development, and operation of space missions requires informed decisions to be made across a vast array of investment, scientific, technological, and operational issues. In the work reported in this paper, we address the problem of determining optimal technology investment portfolios that minimize mission risk and maximize the expected science return of the mission. We model several relationships that explicitly link investment in technologies to mission risk and expected science return. To represent and compute these causal and computational dependencies, we introduce a generalization of influence diagrams that we call inference nets. To illustrate the approach, we present results from its application to a technology portfolio investment trade study done for a specific scenario for the projected 2009 Mars MSL mission. This case study examines the impact of investments in precision landing and long-range roving technologies on the mission capability, and the associated risk, of visiting a set of preselected science sites. We show how an optimal investment strategy can be found that minimizes the mission risk given a fixed total technology investment budget, or alternatively how to determine the minimum budget required to achieve a given acceptable mission risk. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Elfes, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 198-235, Pasadena, CA 91109 USA. EM Alberto.Elfes@jpl.nasa.gov; Charles.R.Weisbin@jpl.nasa.gov RI Elfes, Alberto/E-2463-2011 OI Elfes, Alberto/0000-0003-2433-995X NR 20 TC 1 Z9 2 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9251 J9 IEEE T AERO ELEC SYS JI IEEE Trans. Aerosp. Electron. Syst. PD JAN PY 2006 VL 42 IS 1 BP 22 EP 36 DI 10.1109/TAES.2006.1603403 PG 15 WC Engineering, Aerospace; Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 025SU UT WOS:000236288000002 ER PT J AU Li, ZW Chen, L Zeng, LQ Lin, S Fong, WH AF Li, ZW Chen, L Zeng, LQ Lin, S Fong, WH TI Efficient encoding of quasi-cyclic low-density parity-check codes SO IEEE TRANSACTIONS ON COMMUNICATIONS LA English DT Article; Proceedings Paper CT IEEE Global Telecommunications Conference (GLOBECOM 05) CY NOV 28-DEC 02, 2005 CL St Louis, MO SP IEEE DE array of circulants; quasi-cyclic (QQ low-density parity-check (LDPC) codes; systematic-circulant (SC) form ID CONSTRUCTION; CAPACITY AB Quasi-cyclic (QC) low-density parity-check (LDPC) codes form an important subclass of LDPC codes. These codes have encoding advantage over other types of LDPC codes. This paper addresses the issue of efficient encoding of QC-LDPC codes. Two methods are presented to find the generator matrices of QC-LDPC codes in systematic-circulant (SC)form from their parity-check matrices, given in circulant form. Based on the SC form of the generator matrix of a QC-LDPC code, various types of encoding circuits using simple shift registers are devised. It is shown that the encoding complexity of a QC-LDPC code is linearly proportional to the number of parity bits of the code for serial encoding, and to the length of the code for high-speed parallel encoding. C1 Carnegie Mellon Univ, DSSC, Pittsburgh, PA 15213 USA. Univ Calif Davis, Dept Elect & Comp Engn, Davis, CA 95616 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Carnegie Mellon Univ, DSSC, Pittsburgh, PA 15213 USA. EM zwli@andrew.cmu.edu; leichen@ece.ucdavis.edu; lqzeng@ece.ucdavis.edu; shulin@ece.ucdavis.edu; wai.fong@gsfc.nasa.gov NR 25 TC 208 Z9 242 U1 4 U2 17 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 JAN PY 2006 VL 54 IS 1 BP 71 EP 81 DI 10.1109/TCOMM.2005.861667 PG 11 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 004LP UT WOS:000234754600013 ER PT J AU Tao, G Tang, XD Chen, SH Fei, JT Joshi, SM AF Tao, G Tang, XD Chen, SH Fei, JT Joshi, SM TI Adaptive failure compensation of two-state aircraft morphing actuators SO IEEE TRANSACTIONS ON CONTROL SYSTEMS TECHNOLOGY LA English DT Article DE actuator failure; adaptive control; morphing aircraft; stability; tracking ID FAULT-DIAGNOSIS; SYSTEMS AB An adaptive approach is developed for the compensation of uncertain failures in aircraft morphing actuators, which operate at only one of two states: "on" and "off." By modeling such actuator failures as a piecewise-linear characteristic, a compensation scheme with an adaptive inverse is thus constructed to ensure the closed-loop stability and tracking property. An application to the control of an aircraft lateral dynamic model using morphing actuators is presented with simulation results. C1 Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Tao, G (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. EM gt9s@virginia.edu; xt3f@virginia.edu; s.m.joshi@larc.nasa.gov NR 11 TC 17 Z9 20 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1063-6536 J9 IEEE T CONTR SYST T JI IEEE Trans. Control Syst. Technol. PD JAN PY 2006 VL 14 IS 1 BP 157 EP 164 DI 10.1109/TCST.2005.859639 PG 8 WC Automation & Control Systems; Engineering, Electrical & Electronic SC Automation & Control Systems; Engineering GA 003KD UT WOS:000234679700015 ER EF